FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Lyal, CHC Weitzman, AL AF Lyal, CHC Weitzman, AL TI Taxonomy: Exploring the impediment SO SCIENCE LA English DT Letter C1 Nat Hist Museum, London SW7 5BD, England. Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Lyal, CHC (reprint author), Nat Hist Museum, Cromwell Rd, London SW7 5BD, England. OI Lyal, Christopher/0000-0003-3647-6222 NR 0 TC 6 Z9 6 U1 0 U2 5 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 AUG 20 PY 2004 VL 305 IS 5687 BP 1106 EP 1106 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 849RD UT WOS:000223557400022 PM 15326335 ER PT J AU Holman, MJ Kavelaars, JJ Grav, T Gladman, BJ Fraser, WC Milisavljevic, D Nicholson, PD Burns, JA Carruba, V Petit, JM Rousselot, P Mousis, O Marsden, BG Jacobson, RA AF Holman, MJ Kavelaars, JJ Grav, T Gladman, BJ Fraser, WC Milisavljevic, D Nicholson, PD Burns, JA Carruba, V Petit, JM Rousselot, P Mousis, O Marsden, BG Jacobson, RA TI Discovery of five irregular moons of Neptune SO NATURE LA English DT Article ID ASSISTED CAPTURE; GAS-DRAG; SATELLITES; URANUS; INCLINATION; OBJECTS; JUPITER; SEARCH AB Each giant planet of the Solar System has two main types of moons. 'Regular' moons are typically larger satellites with prograde, nearly circular orbits in the equatorial plane of their host planets at distances of several to tens of planetary radii. The 'irregular' satellites (which are typically smaller) have larger orbits with significant eccentricities and inclinations. Despite these common features, Neptune's irregular satellite system, hitherto thought to consist of Triton and Nereid, has appeared unusual. Triton is as large as Pluto and is postulated to have been captured from heliocentric orbit; it traces a circular but retrograde orbit at 14 planetary radii from Neptune. Nereid, which exhibits one of the largest satellite eccentricities, is believed to have been scattered from a regular satellite orbit to its present orbit during Triton's capture(1,2). Here we report the discovery of five irregular moons of Neptune, two with prograde and three with retrograde orbits. These exceedingly faint (apparent red magnitude m(R) = 5 24.2-25.4) moons, with diameters of 30 to 50 km, were presumably captured by Neptune. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Res Council Canada, Victoria, BC V9E ZE7, Canada. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Obervatoire Besancon, F-25010 Besancon, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Holman, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mholman@cfa.harvard.edu RI Carruba, Valerio/H-5529-2012 OI Carruba, Valerio/0000-0003-2786-0740 NR 30 TC 38 Z9 39 U1 1 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 19 PY 2004 VL 430 IS 7002 BP 865 EP 867 DI 10.1038/nature02832 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 847DA UT WOS:000223369800034 PM 15318214 ER PT J AU Bonnefille, R Potts, R Chalie, F Jolly, D Peyron, O AF Bonnefille, R Potts, R Chalie, F Jolly, D Peyron, O TI High-resolution vegetation and climate change associated with Pliocene Australopithecus afarensis SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID HADAR FORMATION; HOMININ EVOLUTION; FAUNAL CHANGE; ETHIOPIA; AFRICA; PLIOPLEISTOCENE; POLLEN; MODEL; SITE; AGE AB Plio-Pleistocene global climate change is believed to have had an important influence on local habitats and early human evolution in Africa. Responses of hominin lineages to climate change have been difficult to test, however, because this procedure requires well documented evidence for connections between global climate and hominin environment. Through high-resolution pollen data from Hadar, Ethiopia, we show that the hominin Australopithecus afarensis accommodated to substantial environmental variability between 3.4 and 2.9 million years ago. A large biome shift, up to 5degreesC cooling, and a 200- to 300-mm/yr rainfall increase occurred just before 3.3 million years ago, which is consistent with a global marine delta(18)O isotopic shift. C1 Ctr Europeen Rech & Enseignement Geosci Environm, UMR 6635, CNRS, F-13545 Aix En Provence 04, France. Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. Univ Montpellier 2, CNRS, UMR 5554, Inst Sci Evolut, F-34095 Montpellier 05, France. Univ Franche Comte, Lab Chronoecol, UMR 6565, F-25030 Besancon, France. RP Bonnefille, R (reprint author), Ctr Europeen Rech & Enseignement Geosci Environm, UMR 6635, CNRS, BP 80, F-13545 Aix En Provence 04, France. EM bonnefille@cerege.fr; potts.rick@nmnh.si.edu NR 32 TC 97 Z9 99 U1 0 U2 30 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 17 PY 2004 VL 101 IS 33 BP 12125 EP 12129 DI 10.1073/pnas.0401709101 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 847QN UT WOS:000223410100040 PM 15304655 ER PT J AU Prochaska, JX Bloom, JS Chen, HW Hurley, KC Melbourne, J Dressler, A Graham, JR Osip, DJ Vacca, WD AF Prochaska, JX Bloom, JS Chen, HW Hurley, KC Melbourne, J Dressler, A Graham, JR Osip, DJ Vacca, WD TI The host galaxy of GRB 031203: Implications of its low metallicity, low redshift, and starburst nature SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : photometry; gamma rays : bursts; stars : formation ID GAMMA-RAY BURSTS; INTERNATIONAL SPECTROSCOPIC SURVEY; 29 MARCH 2003; STAR-FORMATION; LUMINOSITY FUNCTION; LIGHT-CURVE; ABUNDANCES; EMISSION; DUST; EXTINCTION AB We present Keck/NIRSPEC near-IR images and Magellan/IMACS optical spectroscopy of the host galaxy of GRB 031203. The host is an actively star-forming galaxy at z=0.1055+/-0.0001. This is the lowest redshift GRB to date, aside from GRB 980425. From the hydrogen Balmer lines, we infer an extinction of A(V)=3.62+/-0.25 or a total reddening E-T (B-V)=1.17+/-0.1 toward the sight line to the nebular regions. After correcting for reddening, we perform an emission-line analysis and derive an ISM temperature of T =13400+/-2000 K and electron density of n(e)=300 cm(-3). These imply a metallicity [O/H]=-0.72+/-0.15 dex and a roughly solar abundance pattern for N, Ne, S, and Ar. Integrating Halpha, we infer a dust-corrected star formation rate (SFR) of more than 11 M-circle dot yr(-1). These observations have the following implications: (1) The galaxy has a low K'-band luminosity Lapproximate toL*(K)/5, typical of GRB host galaxies. (2) The low redshift indicates GRB 031203 had an isotropic-equivalent gamma-ray energy release smaller than all previous confirmed GRB events. The burst discovery raises the likelihood of identifying many additional low-z, low-flux events with Swift. (3) The large SFR, low metallicity, and inferred hard radiation field are suggestive of massive star formation, supporting the collapsar model. (4) Several lines of evidence argue against the identification of GRB 031203 as an X-ray flash event. C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Carnegie Inst Washington, Carnegie Observ, Pasadena, CA 91101 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Carnegie Observ, Campanas Observ, La Serena, Chile. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Prochaska, JX (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. EM xavier@ucolick.org NR 73 TC 147 Z9 149 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2004 VL 611 IS 1 BP 200 EP 207 DI 10.1086/421988 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 845IO UT WOS:000223236000018 ER PT J AU Edmonds, PD Kahabka, P Heinke, CO AF Edmonds, PD Kahabka, P Heinke, CO TI Hubble Space Telescope discovery of an optical counterpart to the supersoft X-ray source in the globular cluster M3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; globular clusters : individual (M3); techniques : photometric; X-rays : binaries ID CATACLYSMIC VARIABLES; NGC 6397; IDENTIFICATION; STARS; ASTROMETRY; PHOTOMETRY; CENSUS; ROSAT AB We report the detection with the Hubble Space Telescope of an optical counterpart to the transient supersoft X-ray source 1E 1339.8+2837 in the globular cluster M3. The counterpart is found near the faint end of the subgiant branch in the V versus V-I color-magnitude diagram but is extremely bright in the U band. Variability is detected over a range of timescales, suggesting the presence of an accretion disk and perhaps also ellipsoidal variations of the subgiant secondary. The optical colors of the binary are similar to those of cataclysmic variables recently discovered in 47 Tuc and NGC 6397. We suggest that magnetically channeled accretion may explain the relatively low X-ray luminosity of this source's supersoft state. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Sternwarte Univ Bonn, D-53121 Bonn, Germany. RP Edmonds, PD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pedmonds@cfa.harvard.edu; pkahabka@astro.uni-bonn.de; cheinke@cfa.harvard.edu OI Heinke, Craig/0000-0003-3944-6109 NR 22 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2004 VL 611 IS 1 BP 413 EP 417 DI 10.1086/422136 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 845IO UT WOS:000223236000032 ER PT J AU Gaudi, BS Han, CG AF Gaudi, BS Han, CG TI The many possible interpretations of microlensing event OGLE 2002-BLG-055 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; planetary systems ID GRAVITATIONAL LENSING EXPERIMENT; BINARY-SOURCE; GALACTIC BULGE; EXTINCTION MAP; PLANET PHOTOMETRY; DEGENERACY; SYSTEMS; HALO; PERTURBATIONS AB Microlensing event OGLE 2002-BLG-055 is characterized by a smooth, slightly asymmetric single-lens curve with an isolated, secure data point that is similar to0.6 mag brighter than neighboring points separated by a few days. It was previously suggested that the single deviant data point and global asymmetry were best explained by a planetary companion to the primary lens with mass ratio q = 10(-3) to 10(-2) and by parallax effects induced by the motion of the Earth. We revisit the interpretation of OGLE 2002-BLG-055 and show that the data can be explained by a wide variety of models. We find that the deviant data point can be fitted by a large number of qualitatively different binary-lens models whose mass ratios range, at the similar to3 sigma level, from q similar or equal to 10(-4) to similar or equal to10(-1). This range is consistent with a planet, brown dwarf, or M dwarf companion for reasonable primary masses of M greater than or similar to 0.8 M-circle dot. A subset of these binary-lens fits consists of a family of continuously degenerate models whose mass ratios differ by an order of magnitude, but whose light curves differ by less than or similar to2% for the majority of the perturbation. The deviant data point can also be explained by a binary companion to the source, with a secondary/primary flux ratio of similar to1%. This model has the added appeal that the global asymmetry is naturally explained by the acceleration of the primary induced by the secondary. The binary-source model yields a measurement of the Einstein ring radius projected onto the source plane of (r) over cap (E) = 1.87 +/- 0.40 AU. OGLE 2002-BLG-055 is an extreme example that illustrates the difficulties and degeneracies inherent in the interpretation of weakly perturbed and/or poorly sampled microlensing light curves. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chungbuk Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. RP Gaudi, BS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sgaudi@cfa.harvard.edu; cheongho@astroph.chungbuk.ac.kr RI Gaudi, Bernard/I-7732-2012 NR 39 TC 13 Z9 13 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2004 VL 611 IS 1 BP 528 EP 536 DI 10.1086/421971 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 845IO UT WOS:000223236000040 ER PT J AU Bonanos, AZ Stanek, KZ Udalski, A Wyrzykowski, L Zebrun, K Kubiak, M Szymanski, MK Szewczyk, O Pietrzynski, G Soszynski, I AF Bonanos, A. Z. Stanek, K. Z. Udalski, A. Wyrzykowski, L. Zebrun, K. Kubiak, M. Szymanski, M. K. Szewczyk, O. Pietrzynski, G. Soszynski, I. TI WR 20a IS AN ECLIPSING BINARY: ACCURATE DETERMINATION OF PARAMETERS FOR AN EXTREMELY MASSIVE WOLF-RAYET SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries; eclipsing-binaries; spectroscopic-stars; fundamental parameters-stars; individual (WR 20a)-stars; Wolf-Rayet AB We present a high-precision I-band light curve for the Wolf-Rayet binary WR 20a, obtained as a subproject of the Optical Gravitational Lensing Experiment. Rauw et al. have recently presented spectroscopy for this system, strongly suggesting extremely large minimum masses of 70.7 +/- 4.0 and 68.8 +/- 3.8 M circle dot for the component stars, of the system, with the exact values depending strongly on the period of the system. We detect deep eclipses of about 0.4 mag in the light curve of WR 20a, confirming and refining the suspected period of P = 3.686 days and deriving an inclination angle of i = 74 degrees.5 +/- 2 degrees.0. Using these photometric data and the radial velocity data of Rauw et al., we derive the masses for the two components of WR 20a to be 83.0 +/- 5.0 and 82.0 +/- 5.0 M circle dot. Therefore,, WR 20a is confirmed to consist of two extremely massive stars and to be the most massive binary known with an accurate mass determination. C1 [Bonanos, A. Z.; Stanek, K. Z.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Udalski, A.; Wyrzykowski, L.; Zebrun, K.; Kubiak, M.; Szymanski, M. K.; Szewczyk, O.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bonanos, AZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abonanos@cfa.harvard.edu; kstanek@cfa.harvard.edu; udalski@astrouw.edu.pl; wyrzykow@astrouw.edu.pl; zebrun@astrouw.edu.pl; mk@astrouw.edu.pl; msz@astrouw.edu.pl; szewczyk@astrouw.edu.pl; pietrzyn@astrouw.edu.pl; soszynsk@astrouw.edu.pl RI Bonanos, Alceste/K-5392-2013 OI Bonanos, Alceste/0000-0003-2851-1905 FU HST [HST-GO-09810.06-A]; NASA through a grant from the Space Telescope Science Institute [HST-GO-09810.06-A]; Association of Universities for Research in Astronomy; NASA [NAS5-26555, NAG5-12212]; Polish KBN [2P03D02124]; Udalski and NSF [AST-0204908] FX We thank G. Torres for a careful reading of and comments on the manuscript and D. Sasselov and J. Devor for useful discussions. We also thank the referee, Eric Gosset, for his prompt and careful reading of the manuscript and his useful comments. A. Z. B. and K. Z. S. were partially supported by HST grant HST-GO-09810.06-A. Support for Proposal HST-GO-09810.06-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Partial support to the OGLE project was provided by the following grants: Polish KBN grant 2P03D02124 to A. Udalski and NSF grant AST-0204908 and NASA grant NAG5-12212 to B. Paczynski. NR 30 TC 88 Z9 88 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 AUG 10 PY 2004 VL 611 IS 1 DI 10.1086/423671 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V24GX UT WOS:000208400000009 ER PT J AU Camilo, F Manchester, RN Lyne, AG Gaensler, BM Possenti, A D'Amico, N Stairs, IH Faulkner, AJ Kramer, M Lorimer, DR McLaughlin, MA Hobbs, G AF Camilo, F. Manchester, R. N. Lyne, A. G. Gaensler, B. M. Possenti, A. D'Amico, N. Stairs, I. H. Faulkner, A. J. Kramer, M. Lorimer, D. R. McLaughlin, M. A. Hobbs, G. TI THE VERY YOUNG RADIO PULSAR J1357-6429 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM; individual (G309.8-2.6)-pulsars; individual (PSR J1357-6429) AB We report the discovery of a radio pulsar with a characteristic age of 7300 yr, making it one of the 10 apparently youngest Galactic pulsars known. PSR J1357-6429, with a spin period of P = 166 ms and spin-down luminosity of 3.1 x 10(36) ergs s(-1), was detected during the Parkes multibeam survey of the Galactic plane. We have measured a large rotational glitch in this pulsar, with Delta P/P = -2.4 x 10(-6), similar in magnitude to those experienced occasionally by the Vela pulsar. At a nominal distance of only similar to 2.5 kpc, based on the measured free electron column density of 127 cm(-3) pc and the electron distribution model of Cordes & Lazio, this may be, after the Crab, the nearest very young pulsar known. The pulsar is located near the radio supernova remnant candidate G309.8-2.6. C1 [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Manchester, R. N.; Hobbs, G.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Lyne, A. G.; Faulkner, A. J.; Kramer, M.; Lorimer, D. R.; McLaughlin, M. A.] Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Gaensler, B. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Possenti, A.; D'Amico, N.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. [D'Amico, N.] Univ Cagliari, Dipartimento Fis, I-90042 Monserrato, CA, Italy. [Stairs, I. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 550 W 120th St, New York, NY 10027 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 FU Commonwealth of Australia for operation as a National Facility managed by CSIRO; NSF [AST-02-05853]; NRAO; NSERC University Faculty Award; Royal Society FX The Parkes Observatory and the ATCA are part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. F. C. acknowledges useful discussions with Jules Halpern and support from NSF grant AST-02-05853 and an NRAO travel grant. I. H. S. holds an NSERC University Faculty Award and is supported by a Discovery Grant. D. R. L. is a University Research Fellow funded by the Royal Society. NR 42 TC 24 Z9 24 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 AUG 10 PY 2004 VL 611 IS 1 DI 10.1086/423620 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V24GX UT WOS:000208400000007 ER PT J AU Warrant, EJ Kelber, A Gislen, A Greiner, B Ribi, W Wcislo, WT AF Warrant, EJ Kelber, A Gislen, A Greiner, B Ribi, W Wcislo, WT TI Nocturnal vision and landmark orientation in a tropical halictid bee SO CURRENT BIOLOGY LA English DT Article ID 1ST OPTIC GANGLION; PERIPLANETA-AMERICANA; ORDER INTERNEURONES; ANGULAR SENSITIVITY; VISUAL INFORMATION; TEMPORAL SUMMATION; DARK-ADAPTATION; RETINULA CELLS; FINE-STRUCTURE; COMPOUND EYES AB Background: Some bees and wasps have evolved nocturnal behavior, presumably to exploit night-flowering plants or avoid predators. Like their day-active relatives, they have apposition compound eyes, a design usually found in diurnal insects. The insensitive optics of apposition eyes are not well suited for nocturnal vision. How well then do nocturnal bees and wasps see? What optical and neural adaptations have they evolved for nocturnal vision? Results: We studied female tropical nocturnal sweat bees (Megalopta genalis) and discovered that they are able to learn landmarks around their nest entrance prior to nocturnal foraging trips and to use them to locate the nest upon return. The morphology and optics of the eye and the physiological properties of the photoreceptors have evolved to give Megalopta's eyes almost 30 times greater sensitivity to light than the eyes of diurnal worker honeybees, but this alone does not explain their nocturnal visual behavior. This implies that sensitivity is improved by a strategy of photon summation in time and in space, the latter of which requires the presence of specialized cells that laterally connect ommatidia into groups. First-order interneurons, with significantly wider lateral branching than those found in diurnal bees, have been identified in the first optic ganglion (the lamina ganglionaris) of Megalopta's optic lobe. We believe that these cells have the potential to mediate spatial summation. Conclusions: Despite the scarcity of photons, Megalopta is able to visually orient to landmarks at night in a dark forest understory, an ability permitted by unusually sensitive apposition eyes and neural photon summation. C1 Lund Univ, Dept Cell & Organism Biol, S-22362 Lund, Sweden. Univ Principal Liechtenstein, FL-9495 Triesen, Liechtenstein. Smithsonian Trop Res Inst, Balboa, Panama. RP Warrant, EJ (reprint author), Lund Univ, Dept Cell & Organism Biol, Zool Bldg Helogonavagen 3, S-22362 Lund, Sweden. EM eric.warrant@cob.lu.se RI Kelber, Almut/H-6216-2014 OI Kelber, Almut/0000-0003-3937-2808 NR 73 TC 112 Z9 117 U1 2 U2 30 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD AUG 10 PY 2004 VL 14 IS 15 BP 1309 EP 1318 DI 10.1016/j.cub.2004.07.057 PG 10 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 846HJ UT WOS:000223306200022 PM 15296747 ER PT J AU Squyres, SW Arvidson, RE Bell, JF Bruckner, J Cabrol, NA Calvin, W Carr, MH Christensen, PR Clark, BC Crumpler, L Des Marais, DJ d'Uston, C Economou, T Farmer, J Farrand, W Folkner, W Golombek, M Gorevan, S Grant, JA Greeley, R Grotzinger, J Haskin, L Herkenhoff, KE Hviid, S Johnson, J Klingelhofer, G Knoll, A Landis, G Lemmon, M Li, R Madsen, MB Malin, MC McLennan, SM McSween, HY Ming, DW Moersch, J Morris, RV Parker, T Rice, JW Richter, L Rieder, R Sims, M Smith, M Smith, P Soderblom, LA Sullivan, R Wanke, H Wdowiak, T Wolff, M Yen, A AF Squyres, SW Arvidson, RE Bell, JF Bruckner, J Cabrol, NA Calvin, W Carr, MH Christensen, PR Clark, BC Crumpler, L Des Marais, DJ d'Uston, C Economou, T Farmer, J Farrand, W Folkner, W Golombek, M Gorevan, S Grant, JA Greeley, R Grotzinger, J Haskin, L Herkenhoff, KE Hviid, S Johnson, J Klingelhofer, G Knoll, A Landis, G Lemmon, M Li, R Madsen, MB Malin, MC McLennan, SM McSween, HY Ming, DW Moersch, J Morris, RV Parker, T Rice, JW Richter, L Rieder, R Sims, M Smith, M Smith, P Soderblom, LA Sullivan, R Wanke, H Wdowiak, T Wolff, M Yen, A TI The Spirit Rover's Athena Science Investigation at Gusev Crater, Mars SO SCIENCE LA English DT Article ID MAGNETIC-PROPERTIES EXPERIMENTS; X-RAY SPECTROMETER; MOSSBAUER SPECTROMETER; EXPLORATION ROVERS; MICROSCOPIC IMAGER; LANDING SITES; ART.; ROCKS; MISSION; FEATURES AB The Mars Exploration Rover Spirit and its Athena science payload have been used to investigate a landing site in Gusev crater. Gusev is hypothesized to be the site of a former lake, but no clear evidence for lacustrine sedimentation has been found to date. Instead, the dominant lithology is basalt, and the dominant geologic processes are impact events and eolian transport. Many rocks exhibit coatings and other characteristics that may be evidence for minor aqueous alteration. Any lacustrine sediments that may exist at this location within Gusev apparently have been buried by lavas that have undergone subsequent impact disruption. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Max Planck Inst Chem, Abt Kosmochem, D-55128 Mainz, Germany. NASA, Ames SETI Inst, Moffett Field, CA 94035 USA. Univ Nevada, Dept Geol Sci, Reno, NV 89557 USA. US Geol Survey, Menlo Pk, CA 94025 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Lockheed Martin Corp, Littleton, CO 80127 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Space Sci Inst, Boulder, CO 80301 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Honeybee Robot, New York, NY 10012 USA. Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Max Planck Inst Aeron, D-37191 Katlenburg Lindau, Germany. Johannes Gutenberg Univ Mainz, D-55099 Mainz, Germany. Harvard Univ, Bot Museum, Cambridge, MA 02138 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. Niels Bohr Inst, DK-2100 Copenhagen 0, Denmark. Malin Space Sci Syst, San Diego, CA 92191 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Deutsch Zentrum Luft & Raumfahrt, Inst Raumsimulat, D-51170 Cologne, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA. Space Sci Inst, Martinez, GA 30907 USA. RP Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM squyres@astro.cornell.edu RI Lemmon, Mark/E-9983-2010; Moersch, Jeffrey/F-7189-2010; Smith, Michael/C-8875-2012; Madsen, Morten/D-2082-2011 OI Lemmon, Mark/0000-0002-4504-5136; Madsen, Morten/0000-0001-8909-5111 NR 32 TC 237 Z9 241 U1 4 U2 48 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD AUG 6 PY 2004 VL 305 IS 5685 BP 794 EP 799 DI 10.1126/science.3050794 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 843RT UT WOS:000223104900031 PM 15297657 ER PT J AU Bell, JF Squyres, SW Arvidson, RE Arneson, HM Bass, D Blaney, D Cabrol, N Calvin, W Farmer, J Farrand, WH Goetz, W Golombek, M Grant, JA Greeley, R Guinness, E Hayes, AG Hubbard, MYH Herkenhoff, KE Johnson, MJ Johnson, JR Joseph, J Kinch, KM Lemmon, MT Li, R Madsen, MB Maki, JN Malin, M McCartney, E McLennan, S McSween, HY Ming, DW Moersch, JE Morris, RV Dobrea, EZN Parker, TJ Proton, J Rice, JW Seelos, F Soderblom, J Soderblom, LA Sohl-Dickstein, JN Sullivan, RJ Wolff, MJ Wang, A AF Bell, JF Squyres, SW Arvidson, RE Arneson, HM Bass, D Blaney, D Cabrol, N Calvin, W Farmer, J Farrand, WH Goetz, W Golombek, M Grant, JA Greeley, R Guinness, E Hayes, AG Hubbard, MYH Herkenhoff, KE Johnson, MJ Johnson, JR Joseph, J Kinch, KM Lemmon, MT Li, R Madsen, MB Maki, JN Malin, M McCartney, E McLennan, S McSween, HY Ming, DW Moersch, JE Morris, RV Dobrea, EZN Parker, TJ Proton, J Rice, JW Seelos, F Soderblom, J Soderblom, LA Sohl-Dickstein, JN Sullivan, RJ Wolff, MJ Wang, A TI Pancam multispectral imaging results from the Spirit Rover at Gusev crater SO SCIENCE LA English DT Article ID PATHFINDER LANDING SITE; MARS-PATHFINDER; REFLECTANCE SPECTRA; SOLAR-SYSTEM; DUST; MINERALOGY; ABUNDANCE AB Panoramic Camera images at Gusev crater reveal a rock-strewn surface interspersed with high-to moderate-albedo fine-grained deposits occurring in part as drifts or in small circular swales or hollows. Optically thick coatings of fine-grained ferric iron-rich dust dominate most bright soil and rock surfaces. Spectra of some darker rock surfaces and rock regions exposed by brushing or grinding show near-infrared spectral signatures consistent with the presence of mafic silicates such as pyroxene or olivine. Atmospheric observations show a steady decline in dust opacity during the mission, and astronomical observations captured solar transits by the martian moons, Phobos and Deimos, as well as a view of Earth from the martian surface. C1 Cornell Univ, Ithaca, NY 14853 USA. Washington Univ, St Louis, MO 63130 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Ames Res Ctr, Search Extraterr Intelligence Inst, Moffett Field, CA 94035 USA. Univ Nevada, Reno, NV 89501 USA. Arizona State Univ, Tempe, AZ 85287 USA. Space Sci Inst, Boulder, CO 80301 USA. Univ Copenhagen, DK-2100 Copenhagen O, Denmark. Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Aarhus Univ, DK-8000 Aarhus C, Denmark. Texas A&M Univ, College Stn, TX 77843 USA. Ohio State Univ, Columbus, OH 43210 USA. Malin Space Sci Syst Inc, San Diego, CA 92191 USA. SUNY Stony Brook, Stony Brook, NY 11794 USA. Univ Tennessee, Knoxville, TN 37996 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Bell, JF (reprint author), Cornell Univ, Ithaca, NY 14853 USA. EM jfb8@cornell.edu RI Lemmon, Mark/E-9983-2010; Moersch, Jeffrey/F-7189-2010; Madsen, Morten/D-2082-2011; Hayes, Alexander/P-2024-2014; Kinch, Kjartan/C-5742-2015; Johnson, Jeffrey/F-3972-2015; Seelos, Frank/C-7875-2016; OI Lemmon, Mark/0000-0002-4504-5136; Madsen, Morten/0000-0001-8909-5111; Hayes, Alexander/0000-0001-6397-2630; Kinch, Kjartan/0000-0002-4629-8880; Seelos, Frank/0000-0001-9721-941X; Soderblom, Jason/0000-0003-3715-6407 NR 34 TC 108 Z9 108 U1 4 U2 14 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 AUG 6 PY 2004 VL 305 IS 5685 BP 800 EP 806 DI 10.1126/science.1100175 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 843RT UT WOS:000223104900032 PM 15297658 ER PT J AU Grant, JA Arvidson, R Bell, JF Cabrol, NA Carr, MH Christensen, P Crumpler, L Des Marais, DJ Ehlmann, BL Farmer, J Golombek, M Grant, FD Greeley, R Herkenhoff, K Li, R McSween, HY Ming, DW Moersch, J Rice, JW Ruff, S Richter, L Squyres, S Sullivan, R Weitz, C AF Grant, JA Arvidson, R Bell, JF Cabrol, NA Carr, MH Christensen, P Crumpler, L Des Marais, DJ Ehlmann, BL Farmer, J Golombek, M Grant, FD Greeley, R Herkenhoff, K Li, R McSween, HY Ming, DW Moersch, J Rice, JW Ruff, S Richter, L Squyres, S Sullivan, R Weitz, C TI Surficial deposits at Gusev crater along Spirit Rover traverses SO SCIENCE LA English DT Article ID SIZE-FREQUENCY DISTRIBUTIONS; MAADIM-VALLIS; LANDING SITES; MARS; EROSION; ROCKS AB The Mars Exploration Rover Spirit has traversed a fairly flat, rock-strewn terrain whose surface is shaped primarily by impact events, although some of the landscape has been altered by eolian processes. Impacts ejected basaltic rocks that probably were part of locally formed lava flows from at least 10 meters depth. Some rocks have been textured and/or partially buried by windblown sediments less than 2 millimeters in diameter that concentrate within shallow, partially filled, circular impact depressions referred to as hollows. The terrain traversed during the 90-sol (martian solar day) nominal mission shows no evidence for an ancient lake in Gusev crater. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. NASA, Ames Res Ctr, SETI Inst, Div Space Sci, Moffett Field, CA 94035 USA. US Geol Survey, Menlo Pk, CA 94025 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. DLR, Inst Space Simulat, D-51170 Cologne, Germany. NASA Headquarters, Washington, DC 20560 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM grantj@nasm.si.edu RI Moersch, Jeffrey/F-7189-2010 NR 30 TC 53 Z9 53 U1 1 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD AUG 6 PY 2004 VL 305 IS 5685 BP 807 EP 810 DI 10.1126/science.1099849 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 843RT UT WOS:000223104900033 PM 15297659 ER PT J AU Greeley, R Squyres, SW Arvidson, RE Bartlett, P Bell, JF Blaney, D Cabrol, NA Farmer, J Farrand, B Golombek, MP Gorevan, SP Grant, JA Haldemann, AFC Herkenhoff, KE Johnson, J Landis, G Madsen, MB McLennan, SM Moersch, J Rice, JW Richter, L Ruff, S Sullivan, RJ Thompson, SD Wang, A Weitz, CM Whelley, P AF Greeley, R Squyres, SW Arvidson, RE Bartlett, P Bell, JF Blaney, D Cabrol, NA Farmer, J Farrand, B Golombek, MP Gorevan, SP Grant, JA Haldemann, AFC Herkenhoff, KE Johnson, J Landis, G Madsen, MB McLennan, SM Moersch, J Rice, JW Richter, L Ruff, S Sullivan, RJ Thompson, SD Wang, A Weitz, CM Whelley, P CA Athena Sci Team TI Wind-related processes detected by the Spirit rover at Gusev Crater, Mars SO SCIENCE LA English DT Article ID PATHFINDER LANDING SITE; SURFACES; ABRASION C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Cornell Univ, Dept Astron, Ithaca, NY USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63031 USA. Honeybee Robot, New York, NY 10012 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Colorado, Space Sci Inst, Boulder, CO 80301 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Univ Copenhagen, Niels Bohr Inst Astron Phys & Geophys, Ctr Planetary Sci, DK-2100 Copenhagen, Denmark. Univ Copenhagen, Orsted Lab, DK-2100 Copenhagen, Denmark. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Deutsch Zentrum Luft & Raumfart, German Aerosp Ctr, Inst Space Simulat, D-51170 Cologne, Germany. NASA, Washington, DC 20546 USA. RP Greeley, R (reprint author), Arizona State Univ, Dept Geol Sci, Box 871404, Tempe, AZ 85287 USA. EM Greeley@asu.edu RI Moersch, Jeffrey/F-7189-2010; Whelley, Patrick/B-9560-2012; Madsen, Morten/D-2082-2011 OI Whelley, Patrick/0000-0003-3266-9772; Madsen, Morten/0000-0001-8909-5111 NR 33 TC 66 Z9 66 U1 0 U2 3 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 AUG 6 PY 2004 VL 305 IS 5685 BP 810 EP + DI 10.1126/science.1100108 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 843RT UT WOS:000223104900034 PM 15297660 ER PT J AU Arvidson, RE Anderson, RC Bartlett, P Bell, JF Blaney, D Christensen, PR Chu, P Crumpler, L Davis, K Ehlmann, BL Fergason, R Golombek, MP Gorevan, S Grant, JA Greeley, R Guinness, EA Haldemann, AFC Herkenhoff, K Johnson, J Landis, G Li, R Lindemann, R McSween, H Ming, DW Myrick, T Richter, L Seelos, FP Squyres, SW Sullivan, RJ Wang, A Wilson, J AF Arvidson, RE Anderson, RC Bartlett, P Bell, JF Blaney, D Christensen, PR Chu, P Crumpler, L Davis, K Ehlmann, BL Fergason, R Golombek, MP Gorevan, S Grant, JA Greeley, R Guinness, EA Haldemann, AFC Herkenhoff, K Johnson, J Landis, G Li, R Lindemann, R McSween, H Ming, DW Myrick, T Richter, L Seelos, FP Squyres, SW Sullivan, RJ Wang, A Wilson, J TI Localization and physical properties experiments conducted by Spirit at Gusev crater SO SCIENCE LA English DT Article ID PATHFINDER AB The precise location and relative elevation of Spirit during its traverses from the Columbia Memorial station to Bonneville crater were determined with bundle-adjusted retrievals from rover wheel turns, suspension and tilt angles, and overlapping images. Physical properties experiments show a decrease of 0.2% per Mars solar day in solar cell output resulting from deposition of airborne dust, cohesive soil-like deposits in plains and hollows, bright and dark rock coatings, and relatively weak volcanic rocks of basaltic composition. Volcanic, impact, aeolian, and water-related processes produced the encountered landforms and materials. C1 Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Honeybee Robot, New York, NY 10012 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. US Geol Survey, Flagstaff, AZ 86001 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Deutsch Luft & Raumfahrt Inst Raumsimulat, D-51170 Cologne, Germany. RP Arvidson, RE (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. RI Seelos, Frank/C-7875-2016 OI Seelos, Frank/0000-0001-9721-941X NR 10 TC 104 Z9 108 U1 1 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 AUG 6 PY 2004 VL 305 IS 5685 BP 821 EP 824 DI 10.1126/science.1099922 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 843RT UT WOS:000223104900035 PM 15297662 ER PT J AU McSween, HY Arvidson, RE Bell, JF Blaney, D Cabrol, NA Christensen, PR Clark, BC Crisp, JA Crumpler, LS Des Marais, DJ Farmer, JD Gellert, R Ghosh, A Gorevan, S Graff, T Grant, J Haskin, LA Herkenhoff, KE Johnson, JR Jolliff, BL Klingelhoefer, G Knudson, AT McLEnnan, S Milam, KA Moersch, JE Morris, RV Rieder, R Ruff, SW de Souza, PA Squyres, SW Wanke, H Wang, A Wyatt, MB Yen, A Zipfel, J AF McSween, HY Arvidson, RE Bell, JF Blaney, D Cabrol, NA Christensen, PR Clark, BC Crisp, JA Crumpler, LS Des Marais, DJ Farmer, JD Gellert, R Ghosh, A Gorevan, S Graff, T Grant, J Haskin, LA Herkenhoff, KE Johnson, JR Jolliff, BL Klingelhoefer, G Knudson, AT McLEnnan, S Milam, KA Moersch, JE Morris, RV Rieder, R Ruff, SW de Souza, PA Squyres, SW Wanke, H Wang, A Wyatt, MB Yen, A Zipfel, J TI Basaltic rocks analyzed by the Spirit rover in Gusev Crater SO SCIENCE LA English DT Article ID CHEMICAL CLASSIFICATION; PATHFINDER SITE; VOLCANIC-ROCKS; SOILS; MARS AB The Spirit landing site in Gusev Crater on Mars contains dark, fine-grained, vesicular rocks interpreted as lavas. Pancam and Mini-Thermal Emission Spectrometer (Mini-TES) spectra suggest that all of these rocks are similar but have variable coatings and dust mantles. Magnified images of brushed and abraded rock surfaces show alteration rinds and veins. Rock interiors contain less than or equal to25% megacrysts. Chemical analyses of rocks by the Alpha Particle X-ray Spectrometer are consistent with picritic basalts, containing normative olivine, pyroxenes, plagioclase, and accessory FeTi oxides. Mossbauer, Pancam, and Mini-TES spectra confirm the presence of olivine, magnetite, and probably pyroxene. These basalts extend the known range of rock compositions composing the martian crust. C1 Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Lockheed Martin Corp, Littleton, CO 80127 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. Max Planck Inst Chem, D-55099 Mainz, Germany. Honeybee Robot, New York, NY 10012 USA. Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Univ Mainz, Inst Anorgan & Analyt Chem, D-6500 Mainz, Germany. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Co Vale Rio Doce, BR-29090900 Vitoria, ES, Brazil. RP McSween, HY (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. EM mcsween@utk.edu RI de Souza, Paulo/B-8961-2008; Moersch, Jeffrey/F-7189-2010; Johnson, Jeffrey/F-3972-2015; Crisp, Joy/H-8287-2016 OI de Souza, Paulo/0000-0002-0091-8925; Crisp, Joy/0000-0002-3202-4416 NR 16 TC 187 Z9 187 U1 2 U2 27 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 AUG 6 PY 2004 VL 305 IS 5685 BP 842 EP 845 DI 10.1126/science.1099851 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 843RT UT WOS:000223104900041 PM 15297668 ER PT J AU Piperno, DR Weiss, E Holst, I Nadel, D AF Piperno, DR Weiss, E Holst, I Nadel, D TI Processing of wild cereal grains in the Upper Palaeolithic revealed by starch grain analysis SO NATURE LA English DT Article ID STONE TOOLS; OHALO-II; PLANT REMAINS; 19,000 BP; IDENTIFICATION; ISRAEL AB Barley ( Hordeum vulgare L.) and wheat ( Triticum monococcum L. and Triticum turgidum L.) were among the principal 'founder crops' of southwest Asian agriculture(1). Two issues that were central to the cultural transition from foraging to food production are poorly understood. They are the dates at which human groups began to routinely exploit wild varieties of wheat and barley, and when foragers first utilized technologies to pound and grind the hard, fibrous seeds of these and other plants to turn them into easily digestible foodstuffs. Here we report the earliest direct evidence for human processing of grass seeds, including barley and possibly wheat, in the form of starch grains recovered from a ground stone artefact from the Upper Palaeolithic site of Ohalo II in Israel. Associated evidence for an oven-like hearth was also found at this site, suggesting that dough made from grain flour was baked. Our data indicate that routine processing of a selected group of wild cereals, combined with effective methods of cooking ground seeds, were practiced at least 12,000 years before their domestication in southwest Asia. C1 Smithsonian Trop Res Inst, Balboa, Panama. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. Harvard Univ, Peabody Museum, Dept Anthropol, Cambridge, MA 02130 USA. Univ Haifa, Archaeol Inst, IL-31905 Haifa, Israel. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. EM pipernod@tivoli.si.edu; eweiss@fas.harvard.edu RI Weiss, Ehud/F-2588-2016 OI Weiss, Ehud/0000-0002-9730-4726 NR 28 TC 152 Z9 176 U1 3 U2 33 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 5 PY 2004 VL 430 IS 7000 BP 670 EP 673 DI 10.1038/nature02734 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 843LM UT WOS:000223085400043 PM 15295598 ER PT J AU Rueda, LM AF Rueda, LM TI Pictorial keys for the identification of mosquitoes (Diptera : Culicidae) associated with dengue virus transmission SO ZOOTAXA LA English DT Article DE Diptera; Culicidae; Ochlerotatus; Aedes; aegypti; albopictus; dengue; identification key; mosquitoes AB Identification keys are provided for female adults and fourth stage larvae of the mosquito species likely to transmit dengue viruses in 4 regions of the world. The keys are illustrated with Auto-Montage(R) photomicrographs, allowing optimum depth of field and resolution. Species included for the Afrotropical Region are: Aedes (Stegomyia) aegypti (Linnaeus), Ae. (Stg.) africanus (Theobald), Ae. (Stg.) albopictus (Skuse), Ae. (Stg.) luteocephalus (Newstead), Ae. (Stg.) opok Corbet and Van Someren, Ae. (Diceromyia) furcifer (Edwards), and Ae. (Dic.) taylori Edwards; for the South Pacific Islands and Australian Region: Ae. (Stg.) aegypti, Ae. (Stg.) albopictus, Ae. (Stg.) cooki Belkin, Ae. (Stg.) hebrideus Edwards, Ae. (Stg.) hensilli Farner, Ae. (Stg.) polynesiensis Marks, Ae. (Stg.) rotumae Belkin, Ae. (Stg.) scutellaris (Walker), and Ochlerotatus (Finlaya) notoscriptus (Skuse); for the Oriental Region: Ae. (Stg.) aegypti, Ae. (Stg.) albopictus, and Oc. (Fin.) niveus subgroup; and for the American Region (North, Central and South America, including the Caribbean Islands): Ae. (Stg.) aegypti, Ae. (Stg.) albopictus, and Oc. (Gymnometopa) mediovittatus (Coquillett). C1 Walter Reed Army Inst Res, Dept Entomol, Walter Reed Biosystemat Unit, Silver Spring, MD USA. RP Rueda, LM (reprint author), Smithsonian Inst, Museum Support Ctr, Dept Entomol, Walter Reed Biosystemat Unit, 4210 Silver Hill Rd, Suitland, MD 20704 USA. EM ruedapol@msc.si.edu NR 5 TC 41 Z9 49 U1 2 U2 7 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 3 PY 2004 IS 589 BP 1 EP 60 PG 60 WC Zoology SC Zoology GA 875AH UT WOS:000225391500001 ER PT J AU Brogan, CL Goss, WM Lazendic, JS Green, AJ AF Brogan, CL Goss, WM Lazendic, JS Green, AJ TI OH (1720 MHz) maser search toward the Large Magellanic Cloud SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : individual (30 Doradus); ISM : magnetic fields; Magellanic Clouds masers; polarization; supernova remnants ID SUPERNOVA REMNANT N49; STAR-FORMING REGIONS; 30 DORADUS; MOLECULAR CLOUDS; EMISSION; SHOCK; METHANOL; IC-443; W28; MERLIN AB We have carried out a sensitive search for OH (1720 MHz) masers in the Large Magellanic Cloud (LMC) toward five regions using the Australia Telescope Compact Array. Our source list includes the 30 Doradus region and four supernova remnants (SNRs): N44, N49, N120, and N132D. These data have a typical resolution of similar to 8" and rms noise levels of 5 - 10 mJy beam(-1). We have detected OH (1720 MHz) masers in the northeast part of 30 Doradus and toward the SNR N49. The OH (1720 MHz) maser emission in 30 Doradus is coincident with a cluster of young stars known as "knot 1'' and is almost certainly of the star formation variety. Our spectral resolution (0.68 km s(-1)) is insufficient to detect the Zeeman effect from the strongest (similar to 320 mJy beam(-1)) of the 30 Doradus OH (1720 MHz) masers, leading to an upper limit to the field strength of 6 mG. The weak OH (1720 MHz) maser emission (35 mJy beam(-1)) detected toward the LMC SNR N49 is located just west of a previously identified CO cloud and is indicative of an interaction between the SNR and the molecular cloud. Although the statistics are low, the detection rate seems consistent with that seen for Galactic star-forming region and SNR type OH ( 1720 MHz) masers - both of which are low. C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Dept Astrophys, Sydney, NSW 2006, Australia. RP Brogan, CL (reprint author), Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA. EM cbrogan@ifa.hawaii.edu; mgoss@aoc.nrao.edu; lazendic@head.cfa.harvard.edu; aGreen@physics.usyd.edu.au NR 38 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2004 VL 128 IS 2 BP 700 EP 708 DI 10.1086/422351 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 843QO UT WOS:000223099600014 ER PT J AU Leinert, C van Boekel, R Waters, LBFM Chesneau, O Malbet, F Kohler, R Jaffe, W Ratzka, T Dutrey, A Preibisch, T Graser, U Bakker, E Chagnon, G Cotton, WD Dominik, C Dullemond, CP Glazenborg-Kluttig, AW Glindemann, A Henning, T Hofmann, KH de Jong, J Lenzen, R Ligori, S Lopez, B Meisner, J Morel, S Paresce, F Pel, JW Percheron, I Perrin, G Przygodda, F Richichi, A Scholler, M Schuller, P Stecklum, B van den Ancker, ME von der Luhe, O Weigelt, G AF Leinert, C van Boekel, R Waters, LBFM Chesneau, O Malbet, F Kohler, R Jaffe, W Ratzka, T Dutrey, A Preibisch, T Graser, U Bakker, E Chagnon, G Cotton, WD Dominik, C Dullemond, CP Glazenborg-Kluttig, AW Glindemann, A Henning, T Hofmann, KH de Jong, J Lenzen, R Ligori, S Lopez, B Meisner, J Morel, S Paresce, F Pel, JW Percheron, I Perrin, G Przygodda, F Richichi, A Scholler, M Schuller, P Stecklum, B van den Ancker, ME von der Luhe, O Weigelt, G TI Mid-infrared sizes of circumstellar disks around Herbig Ae/Be stars measured with MIDI on the VLTI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : circumstellar matter; techniques : interferometric; stars : formation; stars : pre-main-sequence; infrared : stars ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; PHOTOMETRIC CATALOG; ISO SPECTROSCOPY; ACCRETION DISKS; GRAIN-GROWTH; DUST; EMISSION; HD-100546; SYSTEMS AB We present the first long baseline mid-infrared interferometric observations of the circumstellar disks surrounding Herbig Ae/Be stars. The observations were obtained using the mid-infrared interferometric instrument MIDI at the European Southern Observatory (ESO) Very Large Telescope Interferometer VLTI on Cerro Paranal. The 102 m baseline given by the telescopes UTI and UT3 was employed, which provides a maximum full spatial resolution of 20 milli-arcsec (mas) at a wavelength of 10 mum. The interferometric signal was spectrally dispersed at a resolution of 30, giving spectrally resolved visibility information from 8 mum to 13.5 mum. We observed seven nearby Herbig Ae/Be stars and resolved all objects. The warm dust disk of HD 100546 could even be resolved in single-telescope imaging. Characteristic dimensions of the emitting regions at 10 Pm are found to be from 1 AU to 10 AU. The 10 mum sizes of our sample stars correlate with the slope of the 10-25 mum infrared spectrum in the sense that the reddest objects are the largest ones. Such a correlation would be consistent with a different geometry in terms of flaring or flat (self-shadowed) disks for sources with strong or moderate mid-infrared excess, respectively. We compare the observed spectrally resolved visibilities with predictions based on existing models of passive centrally irradiated hydrostatic disks made to fit the SEDs of the observed stars. We find broad qualitative agreement of the spectral shape of visibilities corresponding to these models with our observations. Quantitatively, there are discrepancies that show the need for a next step in modelling of circumstellar disks, satisfying both the spatial constraints such as are now available from the MIDI observations and the flux constraints from the SEDs in a consistent way. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Sterrenkundig Inst, B-3001 Louvain, Belgium. Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Max Planck Inst Astrophys, D-85741 Garching, Germany. Observ Meudon, Lab Etud Spatiales & Instrumentat Astrophys, F-92190 Meudon, France. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. ASTRON, NL-7990 AA Dwingeloo, Netherlands. European So Observ, D-85748 Garching, Germany. Observ Cote Azur, F-06304 Nice 4, France. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. Kiepenheuer Inst Sonnenforsch, D-79104 Freiberg, Germany. RP Leinert, C (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM leinert@mpia-hd.mpg.de OI Ligori, Sebastiano/0000-0003-4172-4606; Ratzka, Thorsten/0000-0001-9557-8232; Schoeller, Markus/0000-0002-5379-1286; Dullemond, Cornelis/0000-0002-7078-5910 NR 45 TC 169 Z9 169 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2004 VL 423 IS 2 BP 537 EP 548 DI 10.1051/0004-6361:20047178 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 850OD UT WOS:000223621400021 ER PT J AU Schild, R Masnyak, IS Hnatyk, BI Zhdanov, VI AF Schild, R Masnyak, IS Hnatyk, BI Zhdanov, VI TI Anomalous fluctuations in observations of Q0957+561 A,B: Smoking gun of a cosmic string? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : miscellaneous; gravitational lensing; galaxies : quasars : individual : Q0957+561; cosmology dark matter; elementary particles ID GRAVITATIONAL LENS; TIME-DELAY; PHOTOMETRY AB We report the detection of anomalous brightness fluctuations in the multiple image Q0957+561 A,B gravitational lens system, and consider whether such anomalies have a plausible interpretation within the framework of cosmic string theory. We study a simple model of gravitational lensing by an asymmetric rotating string. An explicit form of the lens equation is obtained and approximate relations for magnification are derived. We show that such a model with typical parameters of the GUT string can quantitatively reproduce the observed pattern of brightness fluctuations. On the other hand explanation involving a binary star system as an alternative cause requires an unacceptably large massive object at a small distance. We also discuss possible observational manifestations of cosmic strings within our lens model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Kyiv Taras Shevchenko Natl Univ, Astron Observ, UA-04053 Kiev, Ukraine. RP Schild, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rschild@cfa.harvard.edu NR 15 TC 19 Z9 21 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2004 VL 422 IS 2 BP 477 EP 482 DI 10.1051/0004-6361:20040274 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846VW UT WOS:000223348300014 ER PT J AU Greene, JE Ho, LC AF Greene, JE Ho, LC TI Active galactic nuclei with candidate intermediate-mass black holes SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : active; galaxies : nuclei; galaxies : Seyfert ID DIGITAL SKY SURVEY; LINE SEYFERT-1 GALAXIES; SURVEY PHOTOMETRIC SYSTEM; JET-INDUCED VELOCITIES; EARLY DATA RELEASE; NEARBY GALAXIES; EMISSION-LINES; EXCITATION MECHANISM; LUMINOSITY FUNCTION; VIRIAL PARAMETER AB We present an initial sample of 19 intermediate-mass black hole candidates in active galactic nuclei culled from the first data release of the Sloan Digital Sky Survey. Using the line width - luminosity mass scaling relation established for broad-line active nuclei, we estimate black hole masses in the range of M-BH approximate to 8 x (10(4)- 10(6)) M-., a regime in which only two objects are currently known. The absolute magnitudes are faint for active galactic nuclei, ranging from M-g approximate to -15 to -18 mag, while the bolometric luminosities are all close to the Eddington limit. The entire sample formally satisfies the line width criterion for so-called narrow-line Seyfert 1 galaxies; however, they display a wider range of Fe II and [O III] lambda5007 line strengths than is typically observed in this class of objects. Although the available imaging data are of insufficient quality to ascertain the detailed morphologies of the host galaxies, it is likely that the majority of the hosts are relatively late-type systems. The host galaxies have estimated g-band luminosities similar to1 mag fainter than M* for the general galaxy population at z approximate to 0.1. Beyond simply extending the known mass range of central black holes in galactic nuclei, these objects provide unique observational constraints on the progenitors of supermassive black holes. They are also expected to contribute significantly to the integrated signal for future gravitational wave experiments. C1 Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greene, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 103 TC 172 Z9 172 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2004 VL 610 IS 2 BP 722 EP 736 DI 10.1086/421719 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840AE UT WOS:000222828600010 ER PT J AU Tomsick, JA Gelino, DM Halpern, JP Kaaret, P AF Tomsick, JA Gelino, DM Halpern, JP Kaaret, P TI The low quiescent X-ray luminosity of the neutron star transient XTE J2123-058 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (XTE J2123-058, SAX J1810.8-2609); stars : neutron; X-rays : binaries; X-rays : stars ID OPTICAL LIGHT CURVES; XTE J2123-058; SAX J1810.8-2609; CHANDRA OBSERVATIONS; AQUILA X-1; EMISSION; SPECTRUM; SPECTROSCOPY; EQUILIBRIUM; COMPONENTS AB We report on the first X-ray observations of the neutron star soft X-ray transient (SXT) XTE J2123-058 in quiescence made by the Chandra X-Ray Observatory and BeppoSAX, as well as contemporaneous optical observations. In 2002, the Chandra spectrum of XTE J2123-058 is consistent with a power-law model or the combination of a blackbody plus a power law, but it is not well described by a pure blackbody. Using the interstellar value of N-H, the power-law fit gives Gamma=3.1(-0.6)(+0.7) and indicates an 0.3-8 keV unabsorbed luminosity of 9(-3)(+4) x 10(31)(d/8.5 kpc)(2) ergs s(-1) (90% confidence errors). Fits with models consisting of thermal plus power-law components indicate that the upper limit on the temperature of a 1.4 M-circle dot, 10 km radius neutron star with a hydrogen atmosphere is kT(eff)<66 eV, and the upper limit on the unabsorbed, bolometric luminosity is L-&INFIN;<1.4x10(32) ergs s(-1), assuming d=8.5 kpc. Of the neutron star SXTs that exhibit short (<1 yr) outbursts, including Aql X-1, 4U 1608-522, Cen X-4, and SAX J1810.8-2609, the lowest temperatures and luminosities are found for XTE J2123-058 and SAX J1810.8-2609. From the BeppoSAX observation of XTE J2123-058 in 2000, we obtained an upper limit on the 1-10 keV unabsorbed luminosity of 9x10(32) ergs s(-1). Although this upper limit allows for the X-ray luminosity to have decreased between 2000 and 2002, that possibility is not supported by our contemporaneous R-band observations, which indicate that the optical flux increased significantly. Motivated by the theory of deep crustal heating by Brown and coworkers, we characterize the outburst histories of the five SXTs. The low quiescent luminosity for XTE J2123-058 is consistent with the theory of deep crustal heating without requiring enhanced neutron star cooling if the outburst recurrence time is greater than or similar to70 yr. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tomsick, JA (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, Code 0424,9500 Gilman Dr, La Jolla, CA 92093 USA. EM jtomsick@ucsd.edu NR 36 TC 38 Z9 38 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2004 VL 610 IS 2 BP 933 EP 940 DI 10.1086/421865 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840AE UT WOS:000222828600028 ER PT J AU Homer, L Szkody, P Raymond, JC Fried, RE Hoard, DW Hawley, SL Wolfe, M Tramposch, JN Yirak, KT AF Homer, L Szkody, P Raymond, JC Fried, RE Hoard, DW Hawley, SL Wolfe, M Tramposch, JN Yirak, KT TI Chandra observation of V426 Ophiuchi: Weighing the evidence for a magnetic white dwarf SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; novae, cataclysmic variables; stars : individual (V426 Ophiuchi); X-rays : binaries; X-rays : stars; white dwarfs ID SECONDARY PHOTOMETRIC STANDARDS; CATACLYSMIC VARIABLES; INTERMEDIATE POLAR; RADIATIVE SHOCKS; EX HYDRAE; SPECTRA; QUIESCENCE; PERIOD; OPH AB We report the results of a 45 ks Chandra observation of the cataclysmic variable (CV) V426 Ophiuchus. The high-resolution spectrum from the high-energy transmission grating spectrometer is most consistent with a cooling flow model, placing V426 Oph among the group of CVs including U Gem and EX Hya. An uninterrupted light curve was also constructed, in which we detect a significant 4.2 hr modulation together with its first harmonic at 2.1 hr. Reanalysis of archival Ginga and ROSAT X-ray light curves also reveals modulations at periods consistent with 4.2 and/or 2.1 hr. Furthermore, optical photometry in V, simultaneous with the Chandra observation, indicates a modulation anticorrelated with the X-ray, and later more extensive R-band photometry finds a signal at similar to2.1 hr. The earlier reported X-ray periods at similar to0.5 and 1 hr appear to be only transient and quasi-periodic in nature. In contrast, the 4.2 hr period or its harmonic is stable and persistent in X-ray/optical data from 1988 to 2003. This periodicity is clearly distinct from the 6.85 hr orbit and could be due to the spin of the white dwarf. If this is the case, V426 Oph would be the first long-period intermediate polar with a ratio P-spin/P-orb of 0.6. However, this interpretation requires unreasonable values of magnetic field strength and mass accretion rate. C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Braeside Obsev, Flagstaff, AZ 86002 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Homer, L (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM homer@astro.washington.edu; szkody@astro.washington.edu; raymond@cfa.harvard.edu; hoard@ipac.caltech.edu; slh@astro.washington.edu; maw2323@u.washington.edu; jonica@u.washington.edu; ktyirak@u.washington.edu OI Hoard, Donald W./0000-0002-6800-6519 NR 26 TC 10 Z9 10 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2004 VL 610 IS 2 BP 991 EP 1000 DI 10.1086/421864 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840AE UT WOS:000222828600033 ER PT J AU Gaudi, BS AF Gaudi, BS TI Kepler and the Kuiper Belt SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper Belt; occultations; solar system : formation; techniques : photometric ID SYNOPTIC SURVEY TELESCOPE; SOLAR-SYSTEM; OBJECTS; OCCULTATIONS; PLANETS; SEARCH AB The proposed field of view of the Kepler mission is at an ecliptic latitude of similar to55degrees, where the surface density of scattered Kuiper Belt objects (KBOs) is a few percent that in the ecliptic plane. The rate of occultations of Kepler target stars by scattered KBOs with radii rgreater than or similar to10 km is similar to10(-6) to 10(-4) star(-1) yr(-1), where the uncertainty reflects the current ignorance of the thickness of the scattered KBO disk and the faint-end slope of their magnitude distribution. These occultation events will last only similar to0.1% of the planned t(exp)=15 minute integration time and thus will appear as single data points that deviate by tiny amounts. However, given the target photometric accuracy of Kepler, these deviations will nevertheless be highly significant, with typical signal-to-noise ratios (S/Ns) of similar to10. I estimate that similar to1-20 of the 10(5) main-sequence stars in Kepler's field of view will exhibit detectable occultations during its 4 yr mission. For unresolved events, the S/N of individual occultations scales as t(exp)(-1/2), and the minimum detectable radius could be decreased by an order of magnitude to similar to1 km by searching the individual 3 s readouts for occultations. I propose a number of methods by which occultation events may be differentiated from systematic effects. Kepler should measure or significantly constrain the frequency of highly inclined, similar to10 km-sized KBOs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaudi, BS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gaudi, Bernard/I-7732-2012 NR 19 TC 5 Z9 5 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2004 VL 610 IS 2 BP 1199 EP 1203 DI 10.1086/421720 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840AE UT WOS:000222828600051 ER PT J AU Esch, DN Connors, A Karovska, M van Dyk, DA AF Esch, DN Connors, A Karovska, M van Dyk, DA TI An image restoration technique with error estimates SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; techniques : high angular resolution ID MAXIMUM LIKELIHOOD; POISSON PROCESSES; PERFORMANCE; ALGORITHM; ENTROPY AB Image restoration including deconvolution techniques offers a powerful tool to improve resolution in images and to extract information on the multiscale structure stored in astronomical observations. We present a new method for statistical deconvolution, which we call expectation through Markov Chain Monte Carlo (EMC2). This method is designed to remedy several shortfalls of currently used deconvolution and restoration techniques for Poisson data. We use a wavelet-like multiscale representation of the true image to achieve smoothing at all scales of resolution simultaneously, thus capturing detailed features in the image at the same time as larger scale extended features. Thus, this method smooths the image, while maintaining the ability to effectively reconstruct point sources and sharp features in the image. We use a principled, fully Bayesian model-based analysis, which produces extensive information about the uncertainty in the fitted smooth image, allowing assessment of the errors in the resulting reconstruction. Our method also includes automatic fitting of the multiscale smoothing parameters. We show several examples of application of EMC2 to both simulated data and a real astronomical X-ray source. C1 Dept Vet Affairs, Ctr Hlth Qual Outcomes & Econ Res, Bedford, MA 01730 USA. Eureka Sci, Oakland, CA 94602 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Irvine, Dept Stat, Irvine, CA 92697 USA. RP Esch, DN (reprint author), Dept Vet Affairs, Ctr Hlth Qual Outcomes & Econ Res, 200 Spring Rd, Bedford, MA 01730 USA. EM esch@stat.harvard.edu OI Van Dyk, David/0000-0002-0816-331X NR 32 TC 30 Z9 30 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2004 VL 610 IS 2 BP 1213 EP 1227 DI 10.1086/421761 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840AE UT WOS:000222828600053 ER PT J AU Hallman, EJ Markevitch, M AF Hallman, EJ Markevitch, M TI Chandra observation of the merging cluster A168: A late stage in the evolution of a cold front SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (A168); intergalactic medium; X-rays : galaxies ID INTERGALACTIC MEDIUM; GALAXY CLUSTERS; DARK-MATTER; THERMAL CONDUCTION; MAGNETIC-FIELD; A3667; MERGER; GAS; CONSTRAINTS; SUBCLUSTER AB We present Chandra observations of the cool cluster A168, for which previous X-ray imaging and optical studies indicated a merger of two subclusters nearly in the plane of the sky. We derive a temperature map for A168, which shows that the merger has proceeded beyond the core passage and is near subcluster turnaround. It also reveals an unusual feature: the gas core of one of the subclusters forms a tonguelike structure extending ahead (in the direction of motion) of the subcluster center. The coolest cluster gas is found in a crescent-shaped region at the tip of this tongue and forms a cold front in pressure equilibrium with the external gas. In contrast with this feature's forward location, previously observed merger cold fronts (e.g., A3667, 1E 0657-56) lagged behind their host subclusters, as expected in the presence of ram pressure. We propose that A168 illustrates a much later stage in the evolution of a cold front, when its host subcluster approaches the apocenter of the merger orbit where the ram pressure on its gas drops sharply. As a result, a large chunk of the subcluster gas "slingshots" past the dark matter center, becomes unbound from the subcluster, and expands adiabatically, as seen in some recent hydrodynamic simulations. C1 Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Res Inst, Moscow 117997, Russia. RP Hallman, EJ (reprint author), Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. EM hallman@astro.umn.edu; maxim@head.cfa.harvard.edu NR 26 TC 31 Z9 31 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2004 VL 610 IS 2 BP L81 EP L84 DI 10.1086/423449 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840AF UT WOS:000222828700003 ER PT J AU Zapata, LA Rodriguez, LF Kurtz, SE O'Dell, CR Ho, PTP AF Zapata, LA Rodriguez, LF Kurtz, SE O'Dell, CR Ho, PTP TI A cluster of 1.3 centimeter continuum sources in OMC-1 South SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (Orion OMC-1S); ISM : jets and outflows; radio continuum : stars; stars : pre-main-sequence ID HERBIG-HARO OBJECTS; ORION-NEBULA; MOLECULAR OUTFLOWS; YOUNG STARS; TRAPEZIUM; CORE; PROTOSTARS; FEATURES; CENSUS; CLOUD AB We present sensitive 1.3 cm radio continuum observations of the region OMC-1 South (OMC-1S) in Orion using the Very Large Array in its B configuration. We detect 11 radio sources clustered in a 30" x 30" region, of which only three had been detected previously at radio wavelengths in deep 3.6 cm observations. The eight new radio sources are compact (theta(s) less than or equal to 0".1), and we set lower limits to their spectral indices, alpha > 0.8 +/- 0.3 (with S-nu proportional to nu(alpha)), that suggest that they may be optically thick H II regions. However, one of the new sources exhibits significant circular polarization, indicating that gyrosynchrotron emission with large positive spectral indices may be an alternative explanation. Furthermore, we find that four other sources are associated with infrared sources of low bolometric luminosity that cannot drive an H II region. Finally, two of the sources previously detected at 3.6 cm are angularly resolved in the 1.3 cm image, and their major axes have position angles that align well with large-scale outflows emanating from OMC-1S. The radio source 143-353 has a major axis with a position angle consistent with those of the HH 202 and HH 528 flows, while the radio source 134-411 has a major axis with a position angle consistent with that of the low-velocity molecular outflow associated with the far-infrared source FIR 4. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. RP Zapata, LA (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apartado Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico. EM lzapata@cfa.harvard.edu; l.rodriguez@astrosmo.unam.mx; s.kurtz@astrosmo.unam.mx; cr.odell@vanderbilt.edu; pho@cfa.harvard.edu NR 22 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2004 VL 610 IS 2 BP L121 EP L124 DI 10.1086/423428 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840AF UT WOS:000222828700013 ER PT J AU Lee, CW Myers, PC Plume, R AF Lee, CW Myers, PC Plume, R TI A survey for infall motions toward starless cores. III. CS (3-2) and DCO+(2-1) observations SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : globules; ISM : kinematics and dynamics; stars : formation ID PRE-PROTOSTELLAR CORES; INTERSTELLAR CLOUDS; DENSE CORES; CS 2-1; TAURUS; L1544; MASS AB We present CS ( 3 - 2) and DCO+ (2 - 1) observations of 94 starless cores and compare the results with previous CS ( 2 - 1) and N2H+ ( 1 - 0) observations to study inward motions in starless cores. Eighty-four cores were detected in both CS and DCO+ lines. A significant number of CS ( 3 - 2) profiles and a small number of DCO+ ( 2 - 1) lines show the classical "infall asymmetry'' similar to that seen in CS ( 2 - 1) observations. The DCO+ ( 2 - 1) lines, however, usually show a single Gaussian peak. The integrated intensity of N2H+ correlates well with that of DCO+ ( 2 - 1) but poorly with that of CS ( 2 - 1) and CS ( 3 - 2), suggesting that CS suffers significantly more depletion onto grains than do either DCO+ or N2H+. Despite these depletion effects, there is evidently enough optical depth for the CS ( 3 - 2) and CS ( 2 - 1) spectral lines to exhibit infall asymmetries. The velocity shifts of the CS ( 3 - 2) and ( 2 - 1) lines with respect to N2H+ correlate well with each other and have similar distributions. This implies that, in many cores, systematic inward motions of gaseous material may occur over a range of density of at least a factor similar to4. We identify 18 infall candidates based on observations of CS ( 3 - 2), CS ( 2 - 1), DCO+ ( 2 - 1) and N2H+ ( 1 - 0). The eight best candidates, L1355, L1498, L1521F, L1544, L158, L492, L694-2, and L1155C-1, each show at least four indications of infall asymmetry and no counterindications. Fits of the spectra to a two-layer radiative transfer model in ten infall candidates suggest that the median effective line of sight speed of the inward-moving gas is similar to0.07 km s(-1) for CS ( 3 - 2) and similar to0.04 km s(-1) for CS ( 2 - 1). Considering that the optical depth obtained from the fits is usually smaller in CS ( 3 - 2) than in ( 2 - 1) line, this may imply that CS ( 3 - 2) usually traces inner denser gas in higher inward motions than CS ( 2 - 1). However, it is also possible that this conclusion is not representative of all starless core infall candidates, because of the statistically small number analyzed here. Further line observations will be useful to test this conclusion. C1 Korea Astron Observ, Taejon 305348, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. RP Lee, CW (reprint author), Korea Astron Observ, 61-1 Hwaam Dong, Taejon 305348, South Korea. EM cwl@trao.re.kr; pmyers@cfa.harvard.edu; plume@ism.ucalgary.ca NR 27 TC 45 Z9 45 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2004 VL 153 IS 2 BP 523 EP 543 DI 10.1086/421996 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840IC UT WOS:000222850300007 ER PT J AU Robeck, TR Steinman, KJ Gearhart, S Reidarson, TR McBain, JF Monfort, SL AF Robeck, TR Steinman, KJ Gearhart, S Reidarson, TR McBain, JF Monfort, SL TI Reproductive physiology and development of artificial insemination technology in killer whales (Orcinus orca) SO BIOLOGY OF REPRODUCTION LA English DT Article DE assisted reproductive technology; follicular development; luteinizing hormone; ovulatory cycle; sperm ID BOTTLE-NOSED-DOLPHIN; TURSIOPS-TRUNCATUS; HYSTEROSCOPIC INSEMINATION; ENZYME-IMMUNOASSAY; RESOURCE BANKS; ESTROUS-CYCLE; LOW NUMBERS; SPERMATOZOA; SPERM; FERTILITY AB Research was conducted to define the basic reproductive physiology of killer whales (Orcinus orca) and to use this knowledge to facilitate the development of artificial insemination procedures. The specific objectives were 1) to determine the excretory dynamics of urinary LH and ovarian steroid metabolites during the estrous cycle; 2) to evaluate the effect of an exogenously administered, synthetic progesterone analog on reproductive hormone excretion; 3) to validate the use of transabdominal ultrasound for ovarian evaluation and timing of ovulation; 4) to examine the quality of semen after liquid storage and cryop reservation; and 5) to develop an intrauterine insemination technique. Based on urinary endocrine monitoring of 41 follicular phases and 26 complete cycles from five females, estrous cycles were 41 days long and comprised a 17-day follicular phase and a 21-day luteal phase. A consistent temporal relationship was observed between peak estrogen conjugates and the LH surge, the latter of which occurred approximately 0.5 days later. Two animals placed on oral altrenogest (three separate occasions for 30, 17, and 31 days, respectively) excreted peak urinary estrogen concentrations 25 days after withdrawal that were followed by sustained elevations in urinary pregnanediol-3alpha-glucuronide excretion. Mean preovulatory follicle diameter was 3.9 cm (n = 6), and ovulation occurred 38 h (n = 5) after the peak of the LH surge. Based on visual estimates of motility, liquidstored semen maintained 92% of its raw ejaculate sperm motility index (total progressive motility x kinetic rating [0-5 scale, where 0 = no movement and 5 = rapid progressive movement]) when held at 4degreesC for 3 days postcollection. Semen cryopreserved using a medium freezing rate demonstrated good postthaw total motility (50%), progressive motility (94%), and kinetic rating (3.5). Insemination during eight estrous cycles resulted in three pregnancies (38%), two from liquid-stored and one from cryopreserved semen. Two calves were delivered after gestation lengths of 552 and 554 days, respectively. These data demonstrate the potential of noninvasive endocrine monitoring combined with serial ultrasonography to improve our understanding of the reproductive biology of cetaceans. This fundamental knowledge was essential for ensuring the first successful conceptions, resulting in live offspring, using artificial insemination in any cetacean species. C1 SeaWorld Texas, San Antonio, TX 78251 USA. Zool Soc San Diego, Ctr Reprod Endangered Species, San Diego, CA 92112 USA. SeaWorld San Diego, San Diego, CA 92109 USA. SeaWorld Orlando, Orlando, FL 32821 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Robeck, TR (reprint author), SeaWorld Texas, 10500 SeaWorld Dr, San Antonio, TX 78251 USA. EM todd.robeck@seaworld.com NR 55 TC 39 Z9 43 U1 6 U2 47 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD AUG PY 2004 VL 71 IS 2 BP 650 EP 660 DI 10.1095/biolreprod.104.027961 PG 11 WC Reproductive Biology SC Reproductive Biology GA 841EK UT WOS:000222911900035 PM 15115725 ER PT J AU Laurance, SGW Stouffer, PC Laurance, WE AF Laurance, SGW Stouffer, PC Laurance, WE TI Effects of road clearings on movement patterns of understory rainforest birds in central Amazonia SO CONSERVATION BIOLOGY LA English DT Article DE Amazonian birds; birds and roads; roads and bird movements ID MIXED-SPECIES FLOCKS; INSECTIVOROUS BIRDS; BRAZILIAN AMAZON; FRAGMENTATION; COMMUNITIES; TERRESTRIAL; VEGETATION; IMPACT; EDGES; FIRE AB The impacts of potential linear barriers such as roads, highways, and power lines on rainforest fauna are poorly understood. In the central Brazilian Amazon, we compared the frequency of local movements (less than or equal to300 m long) of understory birds within intact forest and across a 30- to 40-m-wide road over a 2-year-period. Rainforest had regenerated along some road verges, to the extent that a nearly complete canopy was formed in some areas, so we also assessed whether this facilitated bird movement. Movement data were determined from 1212 recaptures of 3681 netted birds at six study sites. The road significantly inhibited total bird movement across roads at five of the six sites. Bird foraging guilds varied in their responses to the road and different ages of regrowth. Movements of frugivorous and edge and gap species were not inhibited at any site, whereas most forest-dependent insectivores (mixed-species flocks, terrestrial species, and army-ant followers) had markedly inhibited road-crossing movements, except at sites with extensive regrowth. Solitary understory species were especially vulnerable, rarely crossing even roads overgrown by tall regrowth. For sensitive species, road-crossing movements were inhibited because individuals tended to avoid both edge-affected habitat near the road and the road clearing itself. Our results suggest that even narrow roads with low traffic volumes can reduce local movements of many insectivorous birds in Amazonia. C1 Univ New England, Dept Nat Resources & Ecosyst Management, Armidale, NSW 2351, Australia. Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Louisiana State Univ, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. RP Laurance, SGW (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurances@tivoli.si.edu RI Laurance, Susan/G-6021-2011 OI Laurance, Susan/0000-0002-2831-2933 NR 48 TC 123 Z9 128 U1 7 U2 62 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD AUG PY 2004 VL 18 IS 4 BP 1099 EP 1109 DI 10.1111/j.1523-1739.2004.00268.x PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 842CD UT WOS:000222979400030 ER PT J AU Fearnside, PM Laurance, WF AF Fearnside, PM Laurance, WF TI Tropical deforestation and greenhouse-gas emissions SO ECOLOGICAL APPLICATIONS LA English DT Article DE Amazon; carbon emission; deforestation; global warming; tropical forest ID AMAZONIAN FOREST FRAGMENTS; BRAZILIAN-AMAZON; ABOVEGROUND BIOMASS; RAIN-FORESTS; LANDSCAPE-SCALE; CARBON; VEGETATION; CONVERSION; DYNAMICS; SOILS AB A recent (2002) analysis concluded that rates of tropical deforestation and atmospheric carbon emissions during the 1990-1997 interval were lower than previously suggested. We challenged this assertion with respect to tropical carbon emissions, but our conclusions were disputed by the authors of the original study. Here we provide further evidence to support our conclusion that the effect of tropical deforestation on greenhouse-gas emissions and global warming is substantial. At least for Brazilian Amazonia, the net impact of tropical deforestation on global warming may be more than double that estimated in the recent study. C1 Natl Inst Res Amazon, Dept Ecol, BR-69011970 Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. RP Fearnside, PM (reprint author), Natl Inst Res Amazon, Dept Ecol, CP 478, BR-69011970 Amazonas, Brazil. RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011 OI Fearnside, Philip/0000-0003-3672-9082 NR 33 TC 55 Z9 63 U1 1 U2 21 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 AUG PY 2004 VL 14 IS 4 BP 982 EP 986 DI 10.1890/03-5225 PG 5 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 844KI UT WOS:000223156600003 ER PT J AU Nascimento, HEM Laurance, WF AF Nascimento, HEM Laurance, WF TI Biomass dynamics in Amazonian forest fragments SO ECOLOGICAL APPLICATIONS LA English DT Article DE Amazon; biomass; Brazil; carbon cycling; carbon storage; decomposition; edge effects; greenhouse gases; habitat fragmentation; rainforest ID NET PRIMARY PRODUCTION; TROPICAL RAIN-FOREST; TIERRA-FIRME FOREST; BRAZILIAN AMAZON; HABITAT FRAGMENTATION; TREE COMMUNITIES; LANDSCAPE-SCALE; RIO-NEGRO; DEFORESTATION; DECOMPOSITION AB Habitat fragmentation affects aboveground biomass in Amazonian forests, with potentially important implications for carbon storage and greenhouse gas emissions. We assessed the dynamics of aboveground-biomass stocks by combining long-term (10-19 yr) data on mortality, damage, growth,. and, recruitment of large ( greater than or equal to10 cm diameter at breast height [dbh]) trees with measurements of nearly all other live and dead plant material (seedlings, saplings, small trees, palms, lianas, downed wood debris, snags, litter) in 50 1-ha plots in fragmented and continuous Amazonian forests. The key process altering biomass dynamics in fragmented forests is the chronically elevated mortality of large trees, which apparently results from microclimatic changes and increased wind turbulence near forest edges. This, in turn, accelerates the production of necromass and leads to significantly increased wood debris and litter on the forest floor. Near forest edges, frequent canopy disturbance increases the amount of light in the understory, resulting in accelerated tree recruitment, significantly higher biomass of small (510 cm dbh) trees, and higher liana densities. Surprisingly, the estimated annual turnover of wood debris increases significantly near forest edges, suggesting that decomposition is occurring more rapidly in fragmented than continuous forests. These results reveal that habitat fragmentation fundamentally alters the distribution and dynamics of aboveground biomass in Amazonian forests. The rate of carbon cycling probably increases sharply, both because long-lived canopy and emergent trees decline in favor of shorter-lived successional trees and lianas, and because necromass production and turnover,both appear to increase. Carbon storage in live vegetation also declines because small successional trees and lianas (which typically have low wood density) store substantially less carbon than do large, old-growth trees. Finally, the decline and rapid decay of live biomass in forest fragments may produce substantial atmospheric carbon emissions, above and beyond that resulting from deforestation per se. C1 INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. RP Laurance, WF (reprint author), INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012 NR 68 TC 56 Z9 60 U1 9 U2 49 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD AUG PY 2004 VL 14 IS 4 SU S BP S127 EP S138 PG 12 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 845TU UT WOS:000223269000012 ER PT J AU Carney, KM Matson, PA Bohannan, BJM AF Carney, KM Matson, PA Bohannan, BJM TI Diversity and composition of tropical soil nitrifiers across a plant diversity gradient and among land-use types SO ECOLOGY LETTERS LA English DT Article DE ammonia-oxidizing bacteria; bacteria; biodiversity; community composition; La Selva Biological Station; land-use; microbes; nitrification; soil; tropics ID AMMONIA-OXIDIZING BACTERIA; RNA GENE-SEQUENCES; COMMUNITY STRUCTURE; GEL-ELECTROPHORESIS; COSTA-RICA; MANAGEMENT REGIMENS; MOLECULAR ANALYSIS; ECOSYSTEM FUNCTION; SPECIES-DIVERSITY; NITROUS-OXIDE AB Ammonia-oxidizing bacteria (AOB) perform the rate-limiting step of nitrification, a key ecosystem process that in part determines the fate of nitrogen in ecosystems. However, little is known about the factors that determine soil AOB diversity or composition, especially in tropical systems. Using a set of study systems in Costa Rica, we examined whether plant diversity or land-use influenced AOB diversity or composition and whether AOB diversity or composition were associated with nitrification rates. We characterized the molecular diversity and composition of AOB via polymerase chain reaction amplification, cloning, and sequencing of 16S rDNA. We found that AOB diversity or composition did not change significantly across plant diversity treatments. In contrast, AOB differed among land-use types in some measures of diversity and in composition, and differences in AOB composition among land-use types were correlated with potential rates of nitrification. Our results suggest that anthropogenic changes of ecosystems can alter microbial communities in ways that may affect the processes they mediate. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA. Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA. RP Carney, KM (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM carneyk@serc.si.edu NR 58 TC 77 Z9 80 U1 3 U2 30 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD AUG PY 2004 VL 7 IS 8 BP 684 EP 694 DI 10.1111/j.1461-0248.2004.00628.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 838ME UT WOS:000222716600009 ER PT J AU Shaw, DC Franklin, JF Bible, K Klopatek, J Freeman, E Greene, S Parker, GG AF Shaw, DC Franklin, JF Bible, K Klopatek, J Freeman, E Greene, S Parker, GG TI Ecological setting of the wind river old-growth forest SO ECOSYSTEMS LA English DT Article DE old growth; temperate coniferous forest; ecological characterization; soils; geology; climate; vegetation; disturbance ID PSEUDOTSUGA-TSUGA FOREST; DOUGLAS-FIR FOREST; SOUTHWESTERN WASHINGTON; CARBON; USA; CANOPY; OREGON; EDGE; ECOSYSTEM; BALANCE AB The Wind River old-growth forest, in the southern Cascade Range of Washington State, is a cool (average annual temperature, 8.7degreesC), moist (average annual precipitation, 2223 mm), 500-year-old Douglas-fir-western hemlock forest of moderate to low productivity at 371-m elevation on a less than 10% slope. There is a seasonal snowpack (November-March), and rain-on-snow and freezing-rain events are common in winter. Local geology is characterized by volcanic rocks and deposits of Micocene/Oligocene Micocene-Oligocene (mixed) Micocene and Quaternary age, as well as intrusive rocks of Miocene age. Soils are medial, mesic, Entic Vitrands that are deep (2-3 m), well drained, loams and silt loams, generally stone free, and derived from volcanic tephra. The vegetation is transitional, between the Western Hemlock Zone and the Pacific Silver Fir Zone, and the understory is dominated by vine maple, salal, and Oregon grape. Stand structural parameters have been measured on a 4-ha plot. There are eight species of conifers, with a stand density of 427 trees ha(-1) and basal area of 82.9 m(2) ha(-1). Dominant conifers include Douglas-fir (35 trees ha(-1)), western hemlock (224 trees ha(-1)), Pacific yew (86 trees ha(-1)), western red cedar (30 trees ha(-1)), and Pacific silver fir (47 trees ha(-1)). The average height of Douglas-fir is 52.0 m (tallest tree, 64.6 m), whereas western hemlock averages 19.0 m (tallest tree, 55.7 m). The regional disturbance regime is dominated by high-severity to moderate-severity fire, from which this forest is thought to have originated. There is no evidence that fire has occurred in the forest after establishment. Primary agents of stand disturbance, which act at the individual to small groups of trees scale, are wind, snow loads, and drought, in combination and interacting with root-rot and butt-rot fungi, heart-rot fungi, dwarf mistletoe, and bark beetles. The forest composition is slowly shifting from dominance by Douglas-fir, a shade-intolerant species, to western hemlock, western red cedar, Pacific yew, and Pacific silver fir, all shade-tolerant species. The Wind River old-growth forest fits the regional definition of Douglas-fir "old growth" on western hemlock sites. C1 Univ Washington, Wind River Canopy Crane Res Facil, Carson, WA 98610 USA. Univ Washington, Coll Forest Resources, Seattle, WA 98195 USA. Arizona State Univ, Dept Plant Biol, Tempe, AZ 85287 USA. US Forest Serv, Pacific NW Res Stn, Forestry Sci Lab, Corvallis, OR 97331 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Shaw, DC (reprint author), Univ Washington, Wind River Canopy Crane Res Facil, Carson, WA 98610 USA. EM dshaw@u.washington.edu OI Parker, Geoffrey/0000-0001-7055-6491 NR 54 TC 87 Z9 88 U1 5 U2 23 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 J9 ECOSYSTEMS JI Ecosystems PD AUG PY 2004 VL 7 IS 5 BP 427 EP 439 DI 10.1007/s10021-004-0135-6 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 845TJ UT WOS:000223266900002 ER PT J AU Parker, GG Harmon, ME Lefsky, MA Chen, JQ Van Pelt, R Weis, SB Thomas, SC Winner, WE Shaw, DC Frankling, JF AF Parker, GG Harmon, ME Lefsky, MA Chen, JQ Van Pelt, R Weis, SB Thomas, SC Winner, WE Shaw, DC Frankling, JF TI Three-dimensional structure of an old-growth Pseudotsuga-tsuga canopy and its implications for radiation balance, microclimate, and gas exchange SO ECOSYSTEMS LA English DT Article DE biomass; canopy; cover; complexity; gap; hypsograph; leaf area index; old-growth forests; respiration; spatial variation; transmittance; vertical structure ID LEAF-AREA INDEX; DOUGLAS-FIR FORESTS; WESTERN HEMLOCK FOREST; PACIFIC-NORTHWEST; LIGHT TRANSMITTANCE; CONIFEROUS FOREST; CARBON STORES; PINE FOREST; ECOSYSTEM; STANDS AB We describe the three-dimensional structure of an old-growth Douglas-fir/western hemlock forest in the central Cascades of southern Washington, USA. We concentrate on the vertical distribution of foliage, crowns, external surface area, wood biomass, and several components of canopy volume. In addition, we estimate the spatial variation of some aspects of structure, including the topography of the outer surface, and of microclimate, including the within-canopy transmittance of photosynthetically active radiation (PAR). The crowns of large stems, especially of Douglas-fir, dominate the structure and many aspects of spatial variation. The mean vertical profile of canopy surfaces, estimated by five methods, generally showed a single maximum in the lower to middle third of the canopy, although the height of that maximum varied by method. The stand leaf area index was around 9 m(2) m(-2), but also varied according to method (from 6.3 to 12.3). Because of the deep narrow crowns and numerous gaps, the outer canopy surface is extremely complex, with a surface area more than 12 times that of the ground below. The large volume included below the outer canopy surface is very porous, with spaces of several qualitatively distinct environments. Our measurements are consistent with emerging concepts about the structure of old-growth forests, where a high degree of complexity is generated by diverse structural features. These structural characteristics have implications for various ecosystem functions. The height and large volume of the stand indicate a large storage component for microclimatic variables. The high biomass influences the dynamics of those variables, retarding rates of change. The complexity of the canopy outer surface influences radiation balance, particularly in reducing short-wave reflectance. The bottom-heaviness of the foliage profile indicates much radiation absorption and gas exchange activity in the lower canopy. The high porosity contributes to flat gradients of most microclimate variables. Most stand respiration occurs within the canopy and is distributed over a broad vertical range. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. Colorado State Univ, Dept Forest Sci, Ft Collins, CO 80523 USA. Univ Toledo, Toledo, OH 43606 USA. Univ Washington, Coll Forest Resources, Seattle, WA 98195 USA. Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada. Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. Wind River Canopy Crane Res Facil, Carson, WA 98610 USA. RP Parker, GG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM parkerg@si.edu RI Thomas, Sean/B-6089-2008; Chen, Jiquan/D-1955-2009; Lefsky, Michael/A-7224-2009; OI Parker, Geoffrey/0000-0001-7055-6491 NR 70 TC 81 Z9 83 U1 1 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 J9 ECOSYSTEMS JI Ecosystems PD AUG PY 2004 VL 7 IS 5 BP 440 EP 453 DI 10.1007/s10021-004-0136-5 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 845TJ UT WOS:000223266900003 ER PT J AU Ricklefs, RE Bermingham, E AF Ricklefs, RE Bermingham, E TI Application of Johnson et al.'s speciation threshold model to apparent colonization times of island biotas SO EVOLUTION LA English DT Article DE colonization; genetic divergence; Hawaiian Islands; migration; speciation; speciation-threshold model; West Indies ID LESSER ANTILLEAN AVIFAUNA; MITOCHONDRIAL-DNA; DARWINS FINCHES; TAXON CYCLES; BIOGEOGRAPHY; EVOLUTION; HYBRIDIZATION; POPULATIONS; THRASHERS; DIVERSITY AB Understanding patterns of diversity can be furthered by analysis of the dynamics of colonization, speciation, and extinction on islands using historical information provided by molecular phylogeography. The land birds of the Lesser Antilles are one of the most thoroughly described regional faunas in this context. In an analysis of colonization times, Ricklefs and Bermingham (2001) found that the cumulative distribution of lineages with respect to increasing time since colonization exhibits a striking change in slope at a genetic distance of about 2% mitochondrial DNA sequence divergence (about one million years). They further showed how this heterogeneity could be explained by either an abrupt increase in colonization rates or a mass extinction event. Cherry et al. (2002), referring to a model developed by Johnson et al. (2000), argued instead that the pattern resulted from a speciation threshold for reproductive isolation of island populations from their continental source populations. Prior to this threshold, genetic divergence is slowed by migration from the source, and species of varying age accumulate at a low genetic distance. After the threshold is reached, source and island populations diverge more rapidly, creating heterogeneity in the distribution of apparent ages of island taxa. We simulated of Johnson et al.'s speciation-threshold model, incorporating genetic divergence at rate k and fixation at rate M of genes that have migrated between the source and the island population. Fixation resets the divergence clock to zero. The speciation-threshold model fits the distribution of divergence times of Lesser Antillean birds well with biologically plausible parameter estimates. Application of the model to the Hawaiian avifauna, which does not exhibit marked heterogeneity of genetic divergence, and the West Indian herpetofauna, which does, required unreasonably high migration-fixation rates. several orders of magnitude greater than the colonization rate. However, the plausibility of the speciation-divergence model for Lesser Antillean birds emphasizes the importance of further investigation of historical biogeography on a regional scale for whole biotas, as well as the migration of genes between populations on long time scales and the achievement of reproductive isolation. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Ricklefs, RE (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. EM ricklefs@umsl.edu; eb@stri.org NR 32 TC 10 Z9 10 U1 3 U2 5 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 AUG PY 2004 VL 58 IS 8 BP 1664 EP 1673 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 850AT UT WOS:000223583900003 PM 15446421 ER PT J AU Meech, KJ Hainaut, OR Marsden, BG AF Meech, KJ Hainaut, OR Marsden, BG TI Comet nucleus size distributions from HST and Keck telescopes SO ICARUS LA English DT Article DE comets; nucleus sizes; colors; distant activity ID HUBBLE-SPACE-TELESCOPE; KUIPER-BELT OBJECTS; JUPITER-FAMILY COMETS; HYAKUTAKE C/1996 B2; SHORT-PERIOD COMETS; OUTER SOLAR-SYSTEM; OORT CLOUD; INNER COMA; COLLISIONAL EVOLUTION; PHYSICAL-PROPERTIES AB The Wide Field Camera (WFC) on the Hubble Space Telescope and the Low Resolution Imaging Spectrograph (LRIS) on the Keck 11 telescope have been used to image 21 distant dynamically new, long-period (LP) and short-period (SP) Jupiter-family (JF) comet nuclei (near aphelion), as part of a long-term program to search for physical differences between short-period comets and Oort cloud comets. WFC data were obtained on Comets C/1987 H I (Shoemaker) and C/1984 K I (Shoemaker) during Cycle 5 (1995 December) and on Cl 1988 B I (Shoemaker), C/1987 F I (Torres), and C/1983 01 (Cernis) during Cycle 6 (1997 April, May, and June). The HST comets were at heliocentric distances 20.4 < r[AU] < 29.5. Each comet observation was allocated 7 orbits, for approximate to 3.6 hrs of integration. The most difficult part of the image reduction was the removal of cosmic rays. We present our scheme for cosmic ray removal. None of the HST comet nuclei was detected to the 3-sigma level at m(R) similar to 27. The inferred upper limits to the nucleus radii are 4.0 < RN [km] < 10.5. The SP comets range in radius between 0.34 < RN [km] < 15.4, with a median value of R-N similar to 1.61 km. The LP comets ranged in size between < 4.0-56 km. Over a range of radii between 1-10 km, the nuclei can be fit with a cumulative distribution N(> R-N) proportional to R-N(-alpha) with alpha = 1.45 +/- 0.05, and for nuclei in the range 2-5 km, alpha = 1.91 +/- 0.06. Statistical analysis and modeling shows that the slopes of the observed TNO and JF comet distributions are not compatible, suggesting that the intrinsic distribution of JF comet nuclei is a differential a(-3.5) power law truncated at small nucleus radii between 0.3 and 2.0 km. (C) 2004 Elsevier Inc. All rights reserved. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. European So Observ, Santiago, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM meech@ifa.hawaii.edu RI Randall, Cora/L-8760-2014 OI Randall, Cora/0000-0002-4313-4397 NR 92 TC 77 Z9 77 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD AUG PY 2004 VL 170 IS 2 BP 463 EP 491 DI 10.1016/uj.icarus.2004.03.014 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840EH UT WOS:000222839400011 ER PT J AU Dudley, R AF Dudley, R TI Ethanol, fruit ripening, and the historical origins of human alcoholism in primate frugivory SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on In Vino Veritas - The Comparative Biology of Alcohol Consumption CY JAN 05-09, 2004 CL New Orleans, LA ID PALM ASTROCARYUM-STANDLEYANUM; VERTEBRATE-DISPERSED FRUITS; ENVIRONMENTAL ETHANOL; DENTAL MICROWEAR; FLESHY FRUITS; DROSOPHILA-MELANOGASTER; LINKAGE DISEQUILIBRIUM; MYOCARDIAL-INFARCTION; METABOLIZING GENES; PAN-TROGLODYTES AB Ethanol is a naturally occurring substance resulting from the fermentation by yeast of fruit sugars. The association between yeasts and angiosperms dates to the Cretaceous, and dietary exposure of diverse frugivorous taxa to ethanol is similarly ancient. Ethanol plumes can potentially be used to localize ripe fruit, and consumption of low-concentration ethanol within fruit may act as a feeding stimulant. Ripe and over-ripe fruits of the Neotropical palm Astrocaryum standleyanum contained ethanol within the pulp at concentrations averaging 0.9% and 4.5%, respectively. Fruit ripening was associated with significant changes in color, puncture resistance, sugar, and ethanol content. Natural consumption rates of ethanol via frugivory and associated blood levels are not known for any animal taxon. However, behavioral responses to ethanol may have been the target of natural selection for all frugivorous species, including many primates and the hominoid lineages ancestral to modern humans. Pre-existing sensory biases associating this ancient psychoactive compound with nutritional reward might accordingly underlie contemporary patterns of alcohol consumption and abuse. C1 Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Dudley, R (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM wings@socrates.berkeley.edu NR 115 TC 54 Z9 56 U1 2 U2 33 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 AUG PY 2004 VL 44 IS 4 BP 315 EP 323 DI 10.1093/icb/44.4.315 PG 9 WC Zoology SC Zoology GA 855PK UT WOS:000223986000008 PM 21676715 ER PT J AU Schwartz, DA AF Schwartz, DA TI The development and scientific impact of the Chandra X-ray observatory SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Article; Proceedings Paper CT International Workshop on Astronomy and Relativistic Astrophysics CY OCT 12-16, 2003 CL Univ Fed Pernambuco, Olinda, BRAZIL SP CAPES, CLAF, CNPq, FINEP, FAPESP HO Univ Fed Pernambuco DE X-ray astrophysics; supernova nebulae; cluster cooling flows; quasars; jets ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; ASTROPHYSICS FACILITY; EMITTING GAS; CRAB-NEBULA; RADIO LOBES; HYDRA-A; JET; GALAXIES; CLUSTERS AB I review the operational capabilities of the Chandra X-ray Observatory, including some of the spectacular results obtained by the general observer community. A natural theme of this talk is that Chandra is revealing outflows of great quantities of energy that were not previously observable. I highlight the Chandra studies of powerful X-ray jets. This subject is only possible due to the sub-arcsecond resolution of the X-ray telescope. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM das@head.cfa.harvard.edu NR 36 TC 5 Z9 5 U1 0 U2 3 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2718 J9 INT J MOD PHYS D JI Int. J. Mod. Phys. D PD AUG PY 2004 VL 13 IS 7 BP 1239 EP 1247 DI 10.1142/S0218271804005377 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 862IZ UT WOS:000224485500012 ER PT J AU Parker, GG Harding, DJ Berger, ML AF Parker, GG Harding, DJ Berger, ML TI A portable LIDAR system for rapid determination of forest canopy structure SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE canopy height profile; complexity; laser rangefinder; metrics; spatial variation; visualization ID AIRBORNE LASER ALTIMETER; FOLIAGE-HEIGHT PROFILES; BROAD-LEAVED FORESTS; TREE HEIGHTS; SCANNER DATA; VEGETATION; DIVERSITY; ACCURACY; STANDS AB 1. The functional characteristics of forests are related to the organization of their canopies. However, understanding the relationship between canopy structure and function has been limited by a paucity of methods for determining structure at scales consistent with those of function measurements. 2. We describe here a portable system, assembled from commercially available components, for acquiring measurements of distances to overhead plant surfaces. These measurements can be aggregated to assess canopy structure rapidly at scales of ecological interest. Deployed from the forest floor, the system includes a narrow-beam rapidly pulsed first-return laser rangefinder coupled with a data recording system. 3. Tests in an age sequence of broad-leaved closed-canopy forests showed that the system provides results significantly more rapidly than previous methods, at spatial scales as small as 1 m in all dimensions. The estimated mean vertical canopy structure is consistent with that found from more laborious, manual approaches, such as the foliage height profile method. The system has some biases due to beam width and range averaging but, from a variety of tests, we found these have relatively little effect on the structure estimates. 4. Various field sampling schemes and methods of aggregating the measurements yield a variety of representations of structure, including mean profiles, tomographic sections, three-dimensional distributions of canopy surface density and maximum height surfaces. Derivable summary measures include canopy cover and area index, porosity, the size distribution of overhead openings and indices of structural complexity. Moreover, the approach can provide estimates of spatial variability and covariance not previously obtainable. 5. Synthesis and applications. Portable light detection and ranging (LIDAR) systems, such as the one we describe here, provide a new tool for rapid measurement of small-scale forest structure. These can contribute efficiently and relatively inexpensively to canopy research and forestry programmes, covering a range of ecological and production needs. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. NASA, Goddard Space Flight Ctr, Geodynam Branch, Greenbelt, MD 20771 USA. RP Parker, GG (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM parkerg@si.edu RI Harding, David/F-5913-2012; OI Parker, Geoffrey/0000-0001-7055-6491 NR 50 TC 94 Z9 97 U1 1 U2 29 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 AUG PY 2004 VL 41 IS 4 BP 755 EP 767 DI 10.1111/j.0021-8901.2004.00925.x PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 838OB UT WOS:000222721600016 ER PT J AU Babich, D Creminelli, P Zaldarriaga, M AF Babich, D Creminelli, P Zaldarriaga, M TI The shape of non-Gaussianities SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE CMBR theory; inflation; physics of the early universe ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND ANISOTROPY; PERTURBATIONS; INFLATION AB We study the dependence on the configuration in momentum space of the primordial three-point function of density perturbations in several different scenarios: standard slow-roll inflation, curvaton and variable decay models, ghost inflation, models with higher derivative operators and the DBI model of inflation. We de. ne a cosine between the distributions using a measure based on the ability of experiments to distinguish between them. We find that models fall into two broad categories with fairly orthogonal distributions: models where non-Gaussianity is created on crossing the horizon during inflation and models in which the evolution beyond the horizon dominates. In the first case the three-point function is largest for equilateral triangles, while in the second the dominant contribution to the signal comes from the influence of long wavelength modes on small wavelength ones. We show that, because the distributions in these two cases are so different, translating constraints on parameters of one model to those of the other on the basis of the normalization of the three-point function for equilateral triangles can be very misleading. C1 Harvard Univ, Jefferson Phys Lab, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Babich, D (reprint author), Harvard Univ, Jefferson Phys Lab, Cambridge, MA 02138 USA. EM babich@fas.harvard.edu; creminel@carnot.harvard.edu; mzaldarr@cfa.harvard.edu NR 28 TC 274 Z9 273 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD AUG PY 2004 IS 8 AR 009 DI 10.1088/1475-7516/2004/08/009 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 850UH UT WOS:000223638500009 ER PT J AU Shrewsbury, PM Hardin, MR AF Shrewsbury, PM Hardin, MR TI Beat sampling accuracy in estimating spruce spider mite (Acari : Tetranychidae) populations and injury on juniper SO JOURNAL OF ECONOMIC ENTOMOLOGY LA English DT Article DE biological control; integrated pest management; monitoring; injury; threshold ID BIOLOGICAL-CONTROL; URTICAE ACARI; PHYTOSEIIDAE; MANAGEMENT; PLANTS AB The use of a standardized beat sampling method for estimating spruce spider mite, Oligonychus ununguis (Jacobi) (Acari: Tetranychidae), densities on a widely used evergreen ornamental plant species, Juniperus chinensis variety 'Sargentii' A. Henry (Cupressaceae), was examined. There was a significant positive relationship between total spruce spider mite densities and spider mite densities from beat sampling on juniper. The slope and intercept of the relationship may be used by pest managers to predict total spider mite densities on plants from beat sample counts. Beat sampling dramatically underestimates the total number of spider mites on a foliage sample. The relationships between spruce spider mite feeding injury and spider mite density estimates from beat sampling juniper foliage and total spider mite counts on foliage were also examined. There was a significant positive relationship between spruce spider mite density as estimated from beat sampling and injury to the plants. There was a similar positive relationship between the total number of spruce spider mites and injury to the plants, suggesting that a pest manager could use beat sampling counts to estimate plant injury and related thresholds. These findings have important implications to decision-making for spruce spider mite control, especially as it relates to threshold levels and determining rates of predator releases. Further assessment of the effectiveness of beat and other sampling methods across multiple spider mite- host plant associations needs to be examined to enable pest managers to select sampling plans that are feasible and reliable. C1 Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. Smithsonian Inst, Hort Serv Div, Washington, DC 20560 USA. RP Shrewsbury, PM (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. NR 27 TC 2 Z9 3 U1 1 U2 5 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0022-0493 J9 J ECON ENTOMOL JI J. Econ. Entomol. PD AUG PY 2004 VL 97 IS 4 BP 1444 EP 1449 PG 6 WC Entomology SC Entomology GA 847XR UT WOS:000223431900034 PM 15384359 ER PT J AU Wisely, SM Buskirk, SW Russell, GA Aubry, KB Zielinski, WJ AF Wisely, SM Buskirk, SW Russell, GA Aubry, KB Zielinski, WJ TI Genetic diversity and structure of the fisher (Martes pennanti) in a peninsular and peripheral metapopulation SO JOURNAL OF MAMMALOGY LA English DT Article DE dimensionality; fisher; genetic diversity; Martes pennanti; microsatellite DNA; peninsula; periphery; stepping-stone ID MINK MUSTELA-VISON; POPULATION-STRUCTURE; RARE ALLELES; CANADA LYNX; DISTANCE; CONSERVATION; EQUILIBRIUM; RANGE; INDIVIDUALS; ABUNDANCE AB Evolutionary processes can be strongly affected by landscape features. In vagile carnivores that disperse widely, however, genetic structure has been found to be minimal. Using microsatellite DNA primers developed for other mustelids, we found that populations of a vagile forest carnivore, the fisher (Martes pennanti), exhibit high genetic structure (F-ST = 0.45, SE = 0.07) and limited gene flow (Nm < 1) within a > 1,600-km narrow strip of forested habitat; that genetic diversity decreases from core to periphery; and that populations do not show an equilibrium pattern of isolation-by-distance. Genetic structure was greater at the periphery than at the core of the distribution and our data fit a I-dimensional model of stepping-stone range expansion. Multiple lines of paleontological and genetic evidence suggest that the fisher recently (<5,000 years ago) expanded into the mountain forests of the Pacific coast. The reduced dimensionality of the distribution of the fisher in western coastal forests appears to have contributed to the high levels of structure and decreasing diversity from north to south. These effects were likely exacerbated by human-caused changes to the environment. The low genetic diversity and high genetic structure of populations in the southern Sierra Nevada suggest that populations in this part of the geographic range are vulnerable to extinction. C1 Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. US Forest Serv, Pacific NW Res Stn, Olympia, WA 98512 USA. US Forest Serv, Pacific SW Res Stn, Arcata, CA 95521 USA. Smithsonian Inst, Genet Program, Washington, DC 20008 USA. RP Wisely, SM (reprint author), Kansas State Univ, Div Biol, Ackert Hall, Manhattan, KS 66506 USA. EM wisely@ksu.edu RI Buskirk, Steven/K-2871-2016 OI Buskirk, Steven/0000-0003-0611-6648 NR 49 TC 34 Z9 36 U1 0 U2 20 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD AUG PY 2004 VL 85 IS 4 BP 640 EP 648 DI 10.1644/BEL-011 PG 9 WC Zoology SC Zoology GA 848HH UT WOS:000223457700007 ER PT J AU Ekanayake, DK Rajapakse, RPVJ Dubey, JP Dittus, WPJ AF Ekanayake, DK Rajapakse, RPVJ Dubey, JP Dittus, WPJ TI Seroprevalence of Toxoplasma gondii in wild toque macaques (Macaca sinica) at Polonnaruwa, Sri Lanka SO JOURNAL OF PARASITOLOGY LA English DT Article ID RHESUS-MONKEYS; PRENATAL-DIAGNOSIS AB From a natural population that inhabits the dry evergreen forest at Polonnaruwa, serum samples of 170 toque macaques were examined for antibodies to Toxoplasma gondii by the modified agglutination test. Of these, 21 (12%) were found with titers of 1:16 in 9, 1: 32 in 9, 1:256 in 1, 1:1,024 in 1, and 1:4,096 in 1. There was no evidence of maternal transmission of antibodies or congenital toxoplasmosis. None of the infected macaques died within 1 yr after sampling. Toxoplasma gondii infection was closely linked to human environments where domestic cats were common. Macaques having frequent contact with human settlements showed a significantly greater (P < 0.0001) prevalence (19% infected) than macaques restricted to forest habitat, none of which was infected. Although infection with T. gondii has been noted in several species of Asian primates, this is the first report of T. gondii antibodies in toque macaques (Macaca sinica) that are endemic to the island of Sri Lanka. C1 Univ Peradeniya, Fac Vet Med & Anim Sci, Dept Vet Pathobiol, Peradeniya, Sri Lanka. Inst Fundamental Studies, Kandy, Sri Lanka. Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA. USDA ARS, ANRI, Anim Parasit Dis Lab, Beltsville, MD 20705 USA. RP Dubey, JP (reprint author), USDA ARS, ANRI, Anim Parasit Dis Lab, BARC E,Bldg 1001, Beltsville, MD 20705 USA. EM jdubey@anri.barc.usda.gov NR 15 TC 12 Z9 14 U1 0 U2 6 PU AMER SOC PARASITOLOGISTS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-3395 J9 J PARASITOL JI J. Parasitol. PD AUG PY 2004 VL 90 IS 4 BP 870 EP 871 DI 10.1645/GE-291R PG 2 WC Parasitology SC Parasitology GA 849EI UT WOS:000223521100038 PM 15357087 ER PT J AU Gering, E Atkinson, CT AF Gering, E Atkinson, CT TI A rapid method for counting nucleated erythrocytes on stained blood smears by digital image analysis SO JOURNAL OF PARASITOLOGY LA English DT Article ID AVIAN MALARIA; PATHOGENICITY; HEMATOZOA AB Measures of parasitemia by intraerythrocytic hematozoan parasites are normally expressed as the number of infected erythrocytes per n erythrocytes and are notoriously tedious and time consuming to measure. We describe a protocol for generating rapid counts of nucleated erythrocytes from digital micrographs of thin blood smears that can be used to estimate intensity of hematozoan infections in nonmammalian vertebrate hosts. This method takes advantage of the bold contrast and relatively uniform size and morphology of erythrocyte nuclei on Giemsa-stained blood smears and uses ImageJ, a java-based image analysis program developed at the U.S. National Institutes of Health and available on the internet. to recognize and count these nuclei. This technique makes feasible rapid and accurate counts of total erythrocytes in large numbers of microscope fields, which can be used in the calculation of peripheral parasitemias in low-intensity infections. C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Mol Lab, Washington, DC 20008 USA. RP Gering, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Genet Mol Lab, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM carter_atkinson@usgs.gov FU FIC NIH HHS [1-R01-TW-1581-1] NR 11 TC 37 Z9 38 U1 3 U2 14 PU AMER SOC PARASITOLOGISTS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-3395 J9 J PARASITOL JI J. Parasitol. PD AUG PY 2004 VL 90 IS 4 BP 879 EP 881 DI 10.1645/GE-222R PG 3 WC Parasitology SC Parasitology GA 849EI UT WOS:000223521100041 PM 15357090 ER PT J AU Gurgel, CFD Fredericq, S Norris, JN AF Gurgel, CFD Fredericq, S Norris, JN TI Phylogeography of Gracilaria tikvahiae (Gracilariaceae, Rhodophyta): A study of genetic discontinuity in a continuously distributed species based on molecular evidence SO JOURNAL OF PHYCOLOGY LA English DT Article DE biogeography; Gracilaria tikvahiae; Gracilariaceae; ITS; phylogeography; rbcL; rDNA; Rhodophyta ID GULF-OF-MEXICO; MITOCHONDRIAL-DNA; POPULATION-STRUCTURE; EVOLUTIONARY HISTORY; CLADOGRAM ESTIMATION; LIMULUS-POLYPHEMUS; WESTERN ATLANTIC; RBCL SEQUENCES; HORSESHOE-CRAB; UNITED-STATES AB Gracilaria tikvahiae, a highly morphologically variable red alga, is one of the most common species of Gracilariaceae inhabiting Atlantic estuarine environments and the Intracoastal Waterway of eastern North America. Populations of G. tikvahiae at the extremes of their geographic range (Canada and southern Mexico) are subjected to very different environmental regimes. In this study, we used two types of genetic markers, the chloroplast-encoded rbcL and the nuclear internal transcribed spacer (ITS) region, to examine the genetic variability within G. tikvahiae, for inferring the taxonomic and phylogenetic relationships between geographically isolated populations, and to discuss its distributional information in a phylogeographic framework. Based on rbcL and ITS phylogenies, specimens from populations collected at the extreme distributional ranges reported for G. tikvahiae are indeed part of the same species; however, rbcL- but not ITS-based phylogenies detected phylogenetic structure among the ten G. tikvahiae different haplotypes found in this study. The four distinct rbcL lineages were identified as 1) a Canadian-northeast U.S. lineage, 2) a southeast Florida lineage, 3) an eastern Gulf of Mexico lineage, and 4) a western Gulf of Mexico lineage. We found no evidence for the occurrence of G. tikvahiae in the Caribbean Sea. Observed phylogeographic patterns match patterns of genetic structures reported for marine animal taxa with continuous and quasicontinuous geographic distribution along the same geographic ranges. C1 Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. Smithsonian Inst, Dept Bot NHB 166, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Gurgel, CFD (reprint author), Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. EM f_gurgel@yahoo.com RI Gurgel, Carlos/E-6897-2014; OI Gurgel, Carlos/0000-0003-3989-1704; Gurgel, Carlos Frederico Deluqui/0000-0002-7321-6115 NR 58 TC 22 Z9 25 U1 0 U2 8 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD AUG PY 2004 VL 40 IS 4 BP 748 EP 758 DI 10.1111/j.1529-8817.2004.03070.x PG 11 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 844PK UT WOS:000223171900016 ER PT J AU Guzman, HM Tewfik, A AF Guzman, HM Tewfik, A TI Population characteristics and co-occurrence of three exploited decapods (Panulirus argus, P-guttatus and Mithrax spinosissimus) in Bocas del Toro, Panama SO JOURNAL OF SHELLFISH RESEARCH LA English DT Article DE spiny lobster; Panulirus; spider crab; Mithrax; stock assessment; overfishing; Panama; shelter; dens ID SPOTTED SPINY LOBSTER; CALLINECTES-SAPIDUS; NATIONAL-PARK; ABUNDANCE; FISHERY; DECLINE; SIZE; RECRUITMENT; MANAGEMENT; VENEZUELA AB Spiny lobster populations within the Bocas del Toro archipelago appear to be overexploited. Extensive visual surveys over a wide area of reef habitat down to 20 m in depth indicate mean lobster abundance, sizes, and percent maturity levels for both Panulirus argus and P. guttatus below other areas in the region. The almost complete absence of egg-bearing female lobsters may have serious implications for local production and recruitment and emphasizes the need for revision of management strategies for these populations, which are critical to the socio-economic wellbeing of local artisanal fishers and their dependent communities. An increase in the minimum carapace length for P. argus from 60-88 mm may allow protection for most juveniles. The implementation of a closed season or total fishing ban for lobster may also be considered to rebuild the spawning stock biomass to sustainable levels. The extensive pressure likely being exerted on lobster resources may spill over to co-occurring but poorly studied species, such as the large West Indian spider crab, Mithrax spinosissimus. This study presents the first data collected on a wild population of M. spinosissimus. More importantly, it illustrates the poor understanding we have of the inter-relationships between co-occurring species and the need to understand communities of populations that should be co-managed for the preservation of resources and biodiversity. C1 Smithsonian Trop Res Inst, U0948, Miami, FL 34002 USA. McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, U0948, APO AA, Miami, FL 34002 USA. EM guzmanh@naos.si.edu NR 33 TC 14 Z9 16 U1 2 U2 13 PU NATL SHELLFISHERIES ASSOC PI SOUTHAMPTON PA C/O DR. SANDRA E. SHUMWAY, NATURAL SCIENCE DIVISION, SOUTHAMPTON COLLEGE, SOUTHAMPTON, NY 11968 USA SN 0730-8000 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2004 VL 23 IS 2 BP 575 EP 580 PG 6 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 854TB UT WOS:000223925100031 ER PT J AU Hutchinson, A AF Hutchinson, A TI Life at the zoo: Behind the scenes with the animal doctors SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Hutchinson, A (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 2004 VL 129 IS 13 BP 115 EP 115 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 846BB UT WOS:000223288500330 ER PT J AU Sunshine, JM Bus, SJ McCoy, TJ Burbine, TH Corrigan, CM Binzel, RP AF Sunshine, JM Bus, SJ McCoy, TJ Burbine, TH Corrigan, CM Binzel, RP TI High-calcium pyroxene as an indicator of igneous differentiation in asteroids and meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID OUTER MAIN BELT; REFLECTANCE SPECTRA; SPECTROSCOPIC SURVEY; ORDINARY CHONDRITES; LASER IRRADIATION; ABSORPTION-BANDS; IRON-METEORITES; PARENT BODY; OLIVINE; MINERALOGY AB Our analyses of high quality spectra of several S-type asteroids (17 Thetis, 847 Agnia, 808 Merxia, and members of the Agnia and Merxia families) reveal that they include both low- and high-calcium pyroxene with minor amounts of olivine (<20%). In addition, we find that these asteroids have ratios of high-calcium pyroxene to total pyroxene of >similar to0.4. High-calcium pyroxene is a spectrally detectable and petrologically important indicator of igneous history and may prove critical in future studies aimed at understanding the history of asteroidal bodies. The silicate mineralogy inferred for Thetis and the Merxia and Agnia family members requires that these asteroids experienced igneous differentiation, producing broadly basaltic surface lithologies. Together with 4 Vesta (and its smaller "Vestoid" family members) and the main-belt asteroid 1489 Magnya, these new asteroids provide strong evidence for igneous differentiation of at least five asteroid parent bodies. Based on this analysis of a small subset of the near-infrared asteroid spectra taken to date with SpeX at the NASA IRTF, we expect that the number of known differentiated asteroids will increase, consistent with the large number of parent bodies inferred from studies of iron meteorites. C1 Sci Applicat Int Corp, Adv Technol Applicat Div, Chantilly, VA USA. Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Sunshine, JM (reprint author), Sci Applicat Int Corp, Adv Technol Applicat Div, Chantilly, VA USA. EM sunshinej@saic.com NR 76 TC 64 Z9 64 U1 1 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 BP 1343 EP 1357 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 849WD UT WOS:000223571200007 ER PT J AU Benedix, GK Ford, R McCoy, TJ Rushmer, T Corrigan, CM AF Benedix, GK Ford, R McCoy, TJ Rushmer, T Corrigan, CM TI Exploring the possible connection between ordinary chondrites and primitive achondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 67th Annual Meeting of the Meteoritical-Society CY AUG 02-06, 2004 CL Rio de Janeiro, BRAZIL SP Meteorit Soc C1 Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Univ Vermont, Dept Geol, Burlington, VT 05405 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM gretchen@levee.wustl.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A15 EP A15 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600013 ER PT J AU Burbine, TH McCoy, TJ Sunshine, JM Rivkin, AS Binzel, RP Bus, SJ AF Burbine, TH McCoy, TJ Sunshine, JM Rivkin, AS Binzel, RP Bus, SJ TI Near-infrared spectroscopy of vestoids SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 67th Annual Meeting of the Meteoritical-Society CY AUG 02-06, 2004 CL Rio de Janeiro, BRAZIL SP Meteorit Soc ID VESTA; METEORITES; ORIGIN C1 NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Sci Applicat Int Corp, Chantilly, VA 20151 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. EM tburbine@lepvax.gsfc.nasa.gov NR 8 TC 0 Z9 0 U1 1 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A19 EP A19 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600022 ER PT J AU Corrigan, CM Vicenzi, EP Steele, AS Amundsen, HEF McCoy, TJ Treiman, AH AF Corrigan, CM Vicenzi, EP Steele, AS Amundsen, HEF McCoy, TJ Treiman, AH TI Slab carbonates in Allan Hills 84001 and in basalts from Spitsbergen, Norway: Further examination of terrestrial analogues SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 67th Annual Meeting of the Meteoritical-Society CY AUG 02-06, 2004 CL Rio de Janeiro, BRAZIL SP Meteorit Soc ID ALH84001 C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. Univ Oslo, Dept Phys & Geol, N-0316 Oslo, Norway. Lunar & Planetary Inst, Houston, TX 77058 USA. EM corrigan.cari@nmnh.si.edu NR 5 TC 0 Z9 0 U1 1 U2 3 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A25 EP A25 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600034 ER PT J AU Dickinson, TL McCoy, TJ AF Dickinson, TL McCoy, TJ TI Experimentally determined CaS-MnS REE partitioning: Implications for aubritic oldhamite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 67th Annual Meeting of the Meteoritical-Society CY AUG 02-06, 2004 CL Rio de Janeiro, BRAZIL SP Meteorit Soc ID ELEMENTS; ORIGIN C1 Catholic Univ, Dept Phys, Washington, DC 20064 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM tdickins@nas.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A31 EP A31 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600045 ER PT J AU Fagan, TJ MacPherson, GJ Kim, GL AF Fagan, TJ MacPherson, GJ Kim, GL TI Deciphering multiple alteration events in Allende Ca-Al-rich inclusions SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 67th Annual Meeting of the Meteoritical-Society CY AUG 02-06, 2004 CL Rio de Janeiro, BRAZIL SP Meteorit Soc ID CV3 CHONDRITES; EFREMOVKA; VIGARANO; LEOVILLE C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM fagan.tim@mnnh.si.edu NR 5 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A38 EP A38 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600060 ER PT J AU Marvin, UB Whipple, FL AF Marvin, UB Whipple, FL TI Oral histories in meteoritics and planetary science: XIII: Fred L. Whipple SO METEORITICS & PLANETARY SCIENCE LA English DT Biographical-Item AB Born in Red Oak, Iowa, in 1906, Fred Lawrence Whipple earned his Ph.D. in astronomy at the University of California at Berkeley in 1931. He immediately accepted a position at the Harvard College Observatory and remained at Harvard throughout his career. In 1950, he was appointed to the Phillips Professorship in the Department of Astronomy, and in 1955, he began serving concurrently as the Director of the Smithsonian Astrophysical Observatory when it moved from Washington, D.C. to Cambridge, Massachusetts. In the 1930s, Whipple established the Harvard Meteor Project in which two cameras, 26 miles apart, simultaneously photographed the same meteors, for which he invariably derived elliptical orbits indicative of their origin within the solar system. In 1950, Whipple introduced his "dirty snowball" model of comet nuclei, which soon became widely accepted and was fully confirmed in 1986 by close-up images of comet Halley taken by the European Space Agency's Giotto spacecraft. Keenly anticipating the orbiting of satellites during the International Geophysical Year (July 1, 1957-December 31, 1958), Whipple won contracts to build a worldwide network of telescopic cameras for satellite tracking. At least one of the cameras was ready in time to photograph the Soviet Union's Sputnik I satellite in October 1957, and all 12 stations were in operation by midsummer of 1958. For his leadership role in this project, President John Kennedy honored Fred L. Whipple in June 1963 with the President's Award for Distinguished Public Service. In the 1960s, Whipple collaborated with astronomers at the University of Arizona to build a new observatory on Mt. Hopkins, 40 miles south of Tucson. Two of the most innovative instruments installed there for astrophysical research were the world's largest gamma-ray detector and the Multiple-Mirror Telescope. In 1982, the Mt. Hopkins Observatory was rededicated as the Fred Lawrence Whipple Observatory. Although he retired in 1973, Whipple was present at the dedication and until 2003, he continued to actively participate in research projects. At present, he is anticipating the return of the Stardust mission to cornet Wild 2, which will bring back to Earth samples of the comet and of interstellar dust. It is scheduled to arrive in 2006, the year of Fred Whipple's 100th birthday. Among his many honors, Fred Whipple received the Leonard Medal from the Meteoritical Society in 1970 at its meeting hosted by the Goddard Space Flight Center, in Skyland, Virginia. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marvin, UB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM umarvin@cfa.harvard.edu NR 1 TC 1 Z9 1 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A199 EP A213 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600233 ER PT J AU Marvin, UB Wasserburg, GJ AF Marvin, UB Wasserburg, GJ TI Oral histories in meteoritics and planetary science: XII. Gerald J. Wasserburg SO METEORITICS & PLANETARY SCIENCE LA English DT Biographical-Item AB In this interview, Gerald J. (Jerry) Wasserburg recounts how he entered the Geology Department at the University of Chicago in 1948 but switched to a major in physics, while maintaining links with geology, particularly geochemistry. He earned his Ph.D. in 1954 with a thesis on the new technique of potassium-argon dating under Harold C. Urey and Mark Inghram. After spending a year at Chicago as a post-doctoral research fellow with Urey, he joined the faculty at the California Institute of Technology where he ultimately advanced to the title of John D. MacArthur Professor of Geology and Geophysics. In the early 1960s, Wasserburg sought to achieve unprecedented sensitivity and precision in isotopic measurements by designing and directing the construction of the first digital output with magnet switching and on-line processing computer-controlled mass spectrometer. He promptly named his unique instrument, "Lunatic I," and his laboratory, the "Lunatic Asylum." Using that instrument and later ones, Wasserburg and his research group identified specific nucleosynthetic processes that produced isotopic anomalies in inclusions found in meteorites; investigated the origin and evolution of planetary bodies from the solar nebula; dated the oldest components in meteorites and in terrestrial and lunar rocks; and studied the oxygen in presolar grains and the astrophysical models of AGB stars. In addition to his labors in science, he served on policy-making committees and worked with other members to seek the highest standards for receiving and processing lunar samples and other planetary materials, and to forestall the elimination of the final three Apollo missions. Wasserburg has received many honors, including several honorary doctorates from universities at home and abroad, and the prestigious Crafoord Prize bestowed on him in 1986 by the Royal Swedish Academy of Sciences. In 1975, the Meteoritical Society awarded him its Leonard Medal and in 1987-1988, he served as President of the Society. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marvin, UB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM umarvin@cfa.harvard.edu NR 1 TC 1 Z9 1 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A177 EP A197 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600232 ER PT J AU Mayne, RG McCoy, TJ McSween, HY AF Mayne, RG McCoy, TJ McSween, HY TI Textures of unbrecciated eucrites: Spectral relationships? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 67th Annual Meeting of the Meteoritical-Society CY AUG 02-06, 2004 CL Rio de Janeiro, BRAZIL SP Meteorit Soc ID PARENT BODY C1 Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM rmayne@utk.edu NR 4 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A65 EP A65 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600114 ER PT J AU Pauli, E Vicenzi, EP AF Pauli, E Vicenzi, EP TI Sulfate mineralization in Nakhla: A cathodoluminescence and full-spectrum X-ray imaging study SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 67th Annual Meeting of the Meteoritical-Society CY AUG 02-06, 2004 CL Rio de Janeiro, BRAZIL SP Meteorit Soc C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. George Washington Univ, Dept Earth & Environm Sci, Washington, DC USA. EM epauli@nmnh.si.edu NR 5 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A82 EP A82 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600147 ER PT J AU Rost, D Vicenzi, EP AF Rost, D Vicenzi, EP TI The distribution of minor and trace elements within preterrestrial alteration assemblages in the Lafayette martian meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 67th Annual Meeting of the Meteoritical-Society CY AUG 02-06, 2004 CL Rio de Janeiro, BRAZIL SP Meteorit Soc C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM Rost.Detlef@nmnh.si.edu NR 5 TC 3 Z9 3 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2004 VL 39 IS 8 SU S BP A92 EP A92 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 842GB UT WOS:000222990600168 ER PT J AU Eggert, LS Mundy, NI Woodruff, DS AF Eggert, LS Mundy, NI Woodruff, DS TI Population structure of loggerhead shrikes in the California Channel Islands SO MOLECULAR ECOLOGY LA English DT Article DE endangered birds; introgression; island endemic; Lanius ludovicianus; microsatellites; mtDNA ID LANIUS LUDOVICIANUS-MEARNSI; CONSERVATION POLICY; CONTROL REGION; DNA; MARKERS; REPEATS; GENES; UNITS AB The loggerhead shrike (Lanius ludovicianus), a songbird that hunts like a small raptor, maintains breeding populations on seven of the eight California Channel Islands. One of the two subspecies, L. l. anthonyi, was described as having breeding populations on six of the islands while a second subspecies, L. l. mearnsi, was described as being endemic to San Clemente Island. Previous genetic studies have demonstrated that the San Clemente Island loggerhead shrike is well differentiated genetically from both L. l. anthonyi and mainland populations, despite the fact that birds from outside the population are regular visitors to the island. Those studies, however, did not include a comparison between San Clemente Island shrikes and the breeding population on Santa Catalina Island, the closest island to San Clemente. Here we use mitochondrial control region sequences and nuclear microsatellites to investigate the population structure of loggerhead shrikes in the Channel Islands. We confirm the genetic distinctiveness of the San Clemente Island loggerhead shrike and, using Bayesian clustering analysis, demonstrate the presence and infer the source of the nonbreeding visitors. Our results indicate that Channel Island loggerhead shrikes comprise three distinct genetic clusters that inhabit: (i) San Clemente Island, (ii) Santa Catalina Island and (iii) the Northern Channel Islands and nearby mainland; they do not support a recent suggestion that all Channel Island loggerhead shrikes should be managed as a single entity. C1 Univ Calif San Diego, Div Biol Sci, Ecol Behav & Evolut Sect, San Diego, CA 92093 USA. Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. RP Eggert, LS (reprint author), Smithsonian Inst, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM eggertl@nmnh.si.edu NR 37 TC 23 Z9 24 U1 3 U2 20 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD AUG PY 2004 VL 13 IS 8 BP 2121 EP 2133 DI 10.1111/j.1365-294X.2004.02218.x PG 13 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 835YK UT WOS:000222521300002 PM 15245388 ER PT J AU Jarvi, SI Tarr, CL McIntosh, CE Atkinson, CT Fleischer, RC AF Jarvi, SI Tarr, CL McIntosh, CE Atkinson, CT Fleischer, RC TI Natural selection of the major histocompatibility complex (Mhc) in Hawaiian honeycreepers (Drepanidinae) SO MOLECULAR ECOLOGY LA English DT Article DE avian Mhc; balancing selection; Drepanidinae; Hawaiian honeycreepers; mtDNA; Plasmodium ID CLASS-I GENES; MINIMAL ESSENTIAL MHC; RFP-Y; NUCLEOLAR ORGANIZER; PCR AMPLIFICATION; PASSERINE BIRDS; AVIAN MALARIA; POLYMORPHISM; SEQUENCES; CHICKEN AB The native Hawaiian honeycreepers represent a classic example of adaptive radiation and speciation, but currently face one the highest extinction rates in the world. Although multiple factors have likely influenced the fate of Hawaiian birds, the relatively recent introduction of avian malaria is thought to be a major factor limiting honeycreeper distribution and abundance. We have initiated genetic analyses of class II beta chain Mhc genes in four species of honeycreepers using methods that eliminate the possibility of sequencing mosaic variants formed by cloning heteroduplexed polymerase chain reaction products. Phylogenetic analyses group the honeycreeper Mhc sequences into two distinct clusters. Variation within one cluster is high, with d(N) > d(S) and levels of diversity similar to other studies of Mhc (B system) genes in birds. The second cluster is nearly invariant and includes sequences from honeycreepers (Fringillidae), a sparrow (Emberizidae) and a blackbird (Emberizidae). This highly conserved cluster appears reminiscent of the independently segregating Rfp-Y system of genes defined in chickens. The notion that balancing selection operates at the Mhc in the honeycreepers is supported by transpecies polymorphism and strikingly high d(N)/d(S) ratios at codons putatively involved in peptide interaction. Mitochondrial DNA control region sequences were invariant in the i'iwi, but were highly variable in the 'amakihi. By contrast, levels of variability of class II beta chain Mhc sequence codons that are hypothesized to be directly involved in peptide interactions appear comparable between i'iwi and 'amakihi. In the i'iwi, natural selection may have maintained variation within the Mhc, even in the face of what appears to a genetic bottleneck. C1 Univ Hawaii, Dept Biol, Hilo, HI 96720 USA. Smithsonian Inst, Natl Zool Pk, Genet Mol Lab, Washington, DC 20008 USA. Hawaii Volcanoes Natl Pk, Pacific Isl Ecosyst Res Ctr, Hawaii Natl Pk, HI USA. RP Jarvi, SI (reprint author), Univ Hawaii, Dept Biol, Hilo, HI 96720 USA. EM jarvi@hawaii.edu NR 66 TC 63 Z9 65 U1 4 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD AUG PY 2004 VL 13 IS 8 BP 2157 EP 2168 DI 10.1111/j.1365-294X.2004.02228.x PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 835YK UT WOS:000222521300005 PM 15245391 ER PT J AU Keller, GP Windsor, DM Saucedo, JM Werren, JH AF Keller, GP Windsor, DM Saucedo, JM Werren, JH TI Reproductive effects and geographical distributions of two Wolbachia strains infecting the Neotropical beetle, Chelymorpha alternans Boh. (Chrysomelidae, Cassidinae) SO MOLECULAR ECOLOGY LA English DT Article DE Chelymorpha alternans; cytoplasmic incompatibility; multiple infections; strain loss; Wolbachia ID INDUCED CYTOPLASMIC INCOMPATIBILITY; DNA-SEQUENCE DATA; DROSOPHILA-SIMULANS; BACTERIAL DENSITY; NASONIA-VITRIPENNIS; MITOCHONDRIAL-DNA; AEDES-ALBOPICTUS; MTDNA VARIATION; GENE-SEQUENCES; HEAT-SHOCK AB Wolbachia are maternally inherited endocellular bacteria known to alter insect host reproduction to facilitate their own transmission. Multiple Wolbachia infections are more common in tropical than temperate insects but few studies have investigated their dynamics in field populations. The beetle, Chelymorpha alternans, found throughout the Isthmus of Panama, is infected with two strains of Wolbachia, wCalt1 (99.2% of beetles) and wCalt2 (53%). Populations infected solely by the wCalt1 strain were limited to western Pacific Panama, whereas populations outside this region were either polymorphic for single (wCalt1) and double infections (wCalt1 +wCalt2) or consisted entirely of double infections. The wCalt2 strain was not found as a single infection in the wild. Both strains caused cytoplasmic incompatibility (CI). The wCalt1 strain caused weak CI (similar to20%) and the double infection induced moderate CI (similar to70-90%) in crosses with uninfected beetles. The wCalt1 strain rescued about 75% of eggs fertilized by sperm from wCalt2 males. Based on the relationships of beetle mtDNA and infection status, maternal transmission, and repeated population sampling we determined that the double infection invaded C. alternans populations about 100 000 years ago and that the wCalt2 strain appears to be declining in some populations, possibly due to environmental factors. This may be the first study to demonstrate an association between widespread strain loss and environmental factors in the field. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Georgia, Dept Entomol, Athens, GA USA. Univ Rochester, Dept Biol, Rochester, NY 14627 USA. RP Keller, GP (reprint author), Smithsonian Trop Res Inst, Apdo 2072, Balboa, Panama. EM Kellerg@naos.si.edu NR 58 TC 47 Z9 53 U1 2 U2 7 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD AUG PY 2004 VL 13 IS 8 BP 2405 EP 2420 DI 10.1111/j.1365-294X.2004.02213.x PG 16 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 835YK UT WOS:000222521300027 PM 15245413 ER PT J AU Orrell, TM Carpenter, KE AF Orrell, TM Carpenter, KE TI A phylogeny of the fish family Sparidae (porgies) inferred from mitochondrial sequence data SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Perciformes; Percoidei; Sparoidea; Sparidae; phylogeny; mtDNA; 16S; rRNA; cyt b ID EVOLUTION; PERCOIDEI; PERCIFORMES; TELEOSTEI AB The porgies (Sparidae) comprise a diverse group of neritic fishes with a broad geographic distribution. We used mitochondrial DNA sequences from partial 16S ribosomal RNA and cytochrome b genes to reconstruct the phylogenetic history of these fishes. Sequences from 38 sparid species, 10 species in outgroups closely related to sparids, seven basal percoid species, and a non-perciform outgroup species were analyzed with parsimony and maximum likelihood. The Sparidae were monophyletic with the inclusion of Spicara, which is currently placed in the Centracanthidae. The genera Spicara, Pagrus, and Pagellus, were not monophyletic indicating a need for revision. Two main sparid lineages were recovered in all analyses, but the previously proposed six sparid subfamilies (Boopsinae, Denticinae, Diplodinae, Pagellinae, Pagrinae, and Sparinae) were not monophyletic. This suggests that dentition and feeding modes, upon which these subfamilies are based, were independently derived multiple times within sparid fishes. There was no evidence from the 16S or combined analyses for a monophyletic Sparoidea. (C) 2004 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, NOAA, MNFA, Systemat Lab,NHB, Washington, DC 20013 USA. Old Dominion Univ, Dept Biol, Norfolk, VA 23529 USA. RP Orrell, TM (reprint author), Smithsonian Inst, NOAA, MNFA, Systemat Lab,NHB, MRC-153,POB 37012, Washington, DC 20013 USA. EM orrell.thomas@nmnh.si.edu NR 35 TC 51 Z9 64 U1 2 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD AUG PY 2004 VL 32 IS 2 BP 425 EP 434 DI 10.1016/j.ympev.2004.01.012 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 838RY UT WOS:000222732000001 PM 15223028 ER PT J AU McCormick, MK Whigham, DF O'Neill, J AF McCormick, MK Whigham, DF O'Neill, J TI Mycorrhizal diversity in photosynthetic terrestrial orchids SO NEW PHYTOLOGIST LA English DT Article DE Cephalanthera austinae; Goodyera pubescens; Liparis lilifolia; Tipularia discolor; Orchidaceae; mycorrhizal diversity ID MYCO-HETEROTROPHIC PLANTS; PHYLOGENETIC-RELATIONSHIPS; SYMBIOTIC GERMINATION; ECTOMYCORRHIZAL FUNGI; WOODY DEBRIS; IN-SITU; SPECIFICITY; IDENTIFICATION; RHIZOCTONIA; ROOTS AB Specific orchid-fungal associations are known for nonphotosynthetic orchids but fungal diversity in photosynthetic orchids is thought to be quite broad. Specific fungal associations will figure prominently in conservation efforts, while diverse associations may require less attention. We combined culture techniques with ITS and mtLSU sequences and phylogenetic analysis to determine the genetic diversity of mycorrhizal fungi associated with an evergreen, a spring-green, and a winter-green orchid and compared this diversity with that published for a nonphotosynthetic orchid. Mycorrhizal diversity in two of the three photosynthetic orchids was lower than for the nonphotosynthetic orchid. Mycorrhizal diversity in protocorms of the third species was also equal to, or less than, the fungal diversity associated with the nonphotosynthetic species, but adult fungal diversity was greater. We found that photosynthetic orchids do not necessarily have more diverse mycorrhizal associations than nonphotosynthetic orchids. Similarly, evergreen orchids do not necessarily have greater mycorrhizal diversity than seasonally green orchids. Thus, orchid mycorrhizal diversity may not be determined by adult photosynthetic capacity. (C) New Phytologist (2004). C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP McCormick, MK (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM mccormickm@si.edu OI Whigham, Dennis/0000-0003-1488-820X NR 70 TC 130 Z9 150 U1 6 U2 59 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0028-646X J9 NEW PHYTOL JI New Phytol. PD AUG PY 2004 VL 163 IS 2 BP 425 EP 438 DI 10.1111/j.1469-8137.2004.01114.x PG 14 WC Plant Sciences SC Plant Sciences GA 834PW UT WOS:000222424000019 ER PT J AU Perinati, E Barbera, M Serio, S Silver, E AF Perinati, E Barbera, M Serio, S Silver, E TI Thermalization efficiency of superconducting absorbers for thermal X-ray microcalorimeters SO PHYSICA C-SUPERCONDUCTIVITY AND ITS APPLICATIONS LA English DT Article; Proceedings Paper CT 7th International Conference on Materials and Mechanisms of Superconductive and High Temperature Superconductors CY MAY 25-30, 2003 CL Rio de Janeiro, BRAZIL DE microcalorimeters; superconducting absorbers; quasiparticles; phonons AB The persistence of long living quasiparticles created in the energy thermalization process can affect the performances of a thermal X-ray microcalorimeter with superconducting absorber. Numerical simulations indicate that in an absorber made of high-purity Sn, operated at temperatures lower than 100 mK, up to 60% of the deposited energy can remain trapped in the quasiparticle system for a time much longer than the time scale of the thermal sensor response, producing a reduction of the SNR of the detector. Other pure superconductors can present the same problem and therefore a microscopic analysis of the physical properties can be useful to identify suitable absorbing materials and optimize the detector performances. (C) 2004 Elsevier B.V. All rights reserved. C1 INAF, Osservat Astron GS Vaiana, I-90134 Palermo, Italy. Univ Palermo, Dip Sci Fis & Astron, I-90123 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perinati, E (reprint author), INAF, Osservat Astron GS Vaiana, I-90134 Palermo, Italy. EM perinati@astropa.unipa.it OI Barbera, Marco/0000-0002-3188-7420 NR 4 TC 1 Z9 1 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-4534 J9 PHYSICA C JI Physica C PD AUG PY 2004 VL 408 BP 820 EP 821 DI 10.1016/j.physc.2004.03.145 PG 2 WC Physics, Applied SC Physics GA 856NK UT WOS:000224051700345 ER PT J AU Froelich, P Jonsell, S Saenz, A Eriksson, S Zygelman, B Dalgarno, A AF Froelich, P Jonsell, S Saenz, A Eriksson, S Zygelman, B Dalgarno, A TI Leptonic annihilation in hydrogen-antihydrogen collisions SO PHYSICAL REVIEW A LA English DT Article AB We consider the question of competition between leptonic and hadronic annihilation in matter-antimatter interaction. The rate of direct positron-electron annihilation in cold hydrogen-antihydrogen collisions has been calculated. The presence of leptonic annihilation introduces an absorptive, imaginary component to the hydrogen-antihydrogen scattering length; this component is 1.4x10(-4) a.u. for the singlet state of the leptonic spins, and 1.2x10(-7) a.u. for the triplet state. Leptonic annihilation is shown to be about 3 orders of magnitude slower than proton-antiproton annihilation. C1 Uppsala Univ, Dept Quantum Chem, S-75120 Uppsala, Sweden. Umea Univ, SE-90187 Umea, Sweden. Humboldt Univ, Inst Phys, AG Moderne Opt, D-10117 Berlin, Germany. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Froelich, P (reprint author), Uppsala Univ, Dept Quantum Chem, Box 518, S-75120 Uppsala, Sweden. RI Jonsell, Svante/J-2251-2016 OI Jonsell, Svante/0000-0003-4969-1714 NR 12 TC 18 Z9 18 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD AUG PY 2004 VL 70 IS 2 AR 022509 DI 10.1103/PhysRevA.70.022509 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 851WO UT WOS:000223717400057 ER PT J AU Wang, R Mair, RW Rosen, MS Cory, DG Walsworth, RL AF Wang, R Mair, RW Rosen, MS Cory, DG Walsworth, RL TI Simultaneous measurement of rock permeability and effective porosity using laser-polarized noble gas NMR SO PHYSICAL REVIEW E LA English DT Article ID RELATIVE PERMEABILITY; MAGNETIC-RESONANCE; POROUS-MEDIA; FLOW; FIELD; XENON AB We report simultaneous measurements of the permeability and effective porosity of oil-reservoir rock cores using one-dimensional NMR imaging of the penetrating flow of laser-polarized xenon gas. The permeability result agrees well with industry standard techniques, whereas effective porosity is not easily determined by other methods. This NMR technique may have applications to the characterization of fluid flow in a wide variety of porous and granular media. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Cambridge, MA 02139 USA. RP Wang, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rmair@cfa.harvard.edu NR 25 TC 19 Z9 19 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 J9 PHYS REV E JI Phys. Rev. E PD AUG PY 2004 VL 70 IS 2 AR 026312 DI 10.1103/PhysRevE.70.026312 PN 2 PG 7 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA 852VJ UT WOS:000223784600064 PM 15447593 ER PT J AU Lorenzini, E Sanmartin, J AF Lorenzini, E Sanmartin, J TI Electrodynamic tethers in space SO SCIENTIFIC AMERICAN LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Politecn Madrid, Madrid, Spain. RP Lorenzini, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 6 Z9 6 U1 1 U2 5 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 USA SN 0036-8733 J9 SCI AM JI Sci.Am. PD AUG PY 2004 VL 291 IS 2 BP 50 EP 57 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 836WI UT WOS:000222586300027 PM 15298119 ER PT J AU Rice, RA AF Rice, RA TI Made in the shade (Coffee growing) SO SMITHSONIAN LA English DT Letter C1 Smithsonian Migratory Bird Ctr, Washington, DC USA. RP Rice, RA (reprint author), Smithsonian Migratory Bird Ctr, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD AUG PY 2004 VL 35 IS 5 BP 14 EP 14 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 840MA UT WOS:000222861500004 ER PT J AU Neal, V AF Neal, V TI Space policy and the size of the space shuttle fleet SO SPACE POLICY LA English DT Article ID DECISION AB During the space shuttle era, policy makers have repeatedly wrestled with the issue of fleet size. The number of shuttles had both practical and symbolic significance, reflecting the robustness of the space transportation system and US preeminence in space. In debating how many shuttles were needed, NASA and other government entities weighed various arguments to determine the optimum number of vehicles for human spaceflight. Deliberations and decisions about shuttle fleet size reflected changing policy priorities and attitudes about the role of the shuttle. That history frames issues that may arise again in planning for new space transportation vehicles beyond the shuttle. (C) 2004 Elsevier Ltd. All rights reserved. C1 Smithsonian Natl Air & Space Museum, Space Hist Div, Washington, DC 20013 USA. RP Neal, V (reprint author), Smithsonian Natl Air & Space Museum, Space Hist Div, POB 37012, Washington, DC 20013 USA. EM valerie.neal@nasm.si.edu NR 42 TC 1 Z9 1 U1 0 U2 0 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 AUG PY 2004 VL 20 IS 3 BP 157 EP 169 DI 10.1016/j.spacepol.2004.06.001 PG 13 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 851EU UT WOS:000223669200002 ER PT J AU Funk, VA Chan, R Keeley, SC AF Funk, VA Chan, R Keeley, SC TI Insights into the evolution of the tribe Aretoteae (Compositae : subfamily Cichorioideae s.s.) using trnL-F, ndhF, and ITS SO TAXON LA English DT Article DE Arctoteae; Asteraceae; cape floral kingdom; Cichorioideae; compositae; ITS; molecular phylocenetics; ndhF; outgroups; South Africa; trnL ID CHLOROPLAST DNA; MOLECULAR PHYLOGENY; ASTERACEAE; EREMOTHAMNEAE; POSITION; APIACEAE AB Compositae (Asteraceae) are the largest flowering plant family (23,000 to 30,000 species) and its members are found throughout the world in both temperate and tropical habitats. The Subfamilies and tribes of Compositae remained relatively constant for many years; recent molecular studies, however, have identified new subfamilial groups and identified previously Unknown relationships. Currently there are 35 tribes and 10 subfamilies (Baldwin al., 2002; Panero & Funk, 2002). Some of the tribes and subfamilies have not been tested for monophyly and without a clear understanding of the major genera that form each tribe and Subfamily, an accurate phylogeny for the family cannot be reconstructed. The tribe Arctoteae (African daisies) is a diverse and interesting group with a primarily southern African distribution (ca. 17 genera, 220 species). They are especially important in that most of the species are found in the Cape Floral Kingdom, the smallest floral kingdom and the subject of intense conservation interest. Arctoteae are part of the monophyletic subfamily Cichorioideae s.s. Other tribes in the subfamily include Eremothamneae, Gundelieae, Lactuceae, Liabeae, Moquineae, and Vernonieae, and these were all evaluated as potential outgroups. Ultimately 29 ingroup taxa and 16 outgroup taxa with a total of 130 sequences (125 newly reported), from three genetic regions, two from chloroplast DNA (trnL-F and ndhF) and one from the nuclear genome (ITS), were used to evaluate the tribe and its proposed outgroups. Each molecular region is examined separately, the chloroplast markers are examined together, and the data are combined. The data were analyzed with and Without outgroups and problem taxa using parsimony and maximum likelihood methods. The analyses showed robust support for two outgroup clades. Liabeae-Vernonieae and Gundelieae-Lactuceae and two main subtribes within Arctoteae: Arctotineae and Gorteriinae. Support for monophyly of Arctoteae is weak. Within Arctoteae, some taxa of interest are easily placed: Didelta, Cuspidia and Heterorhachis are consistently part of subtribe Gorteriinae, Cymbonotus, the Australian genus, is nested within subtribe Arctotineae, and Hoplocarpha is at the base of Arctotineae. Berkheya. Haplocarpha, and Hirpicium are probably paraphyletic. Furthermore, Platycarpha most likely does not belong in Arctoteae, and Heterolepis and the tribe Eremothamneae are within Arctoteae but not within either of the two main subtribes. After some rearrangements, the two main subtribes, Arctotineae and Gorteriinae, are monophyletic and the latter has three clades. The study shows that the unusual taxa are of critical importance, and they should be included in any molecular analysis. Adequate representation of the ingroup is also important as all previous studies of Arctoteae had involved only a few taxa from the core subtribes, and so did not reveal the problems. Multiple outgroups evaluated in an iterative manner had pronounced effects on the relationships within the ingroup, not only on the position of the root. Finally, unrooted consensus trees and unrooted phylograms were found to be very useful in analyzing the data, allowing for examination of placement of taxa without the bias of a rooted tree. C1 Smithsonian Inst, US Natl Herbarium, Washington, DC 20013 USA. Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA. RP Funk, VA (reprint author), Smithsonian Inst, US Natl Herbarium, MRC 166,POB 37012, Washington, DC 20013 USA. EM funk.vicki@nninh.si.edu; raymund@hawaii.edu; sterling@hawaii.edu NR 45 TC 38 Z9 44 U1 0 U2 6 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD AUG PY 2004 VL 53 IS 3 BP 637 EP 655 DI 10.2307/4135440 PG 19 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 860WC UT WOS:000224373500003 ER PT J AU Hawks, C Makos, K Bell, D Wambach, PE Burroughs, GE AF Hawks, C Makos, K Bell, D Wambach, PE Burroughs, GE TI An inexpensive method to test for mercury vapor in herbarium cabinets SO TAXON LA English DT Article DE corrosive sublimate; herbaria; mercuric chloride; mercury contamination; mercury detection; mercury indicator; mercury vapor AB Mercuric chloride has been used for control of insect and fungal infestations in herbarium collections for over two centuries. One of the lasting effects of this use is the long-term evolution of elemental mercury vapor from treated specimens. The vapor can contaminate untreated specimens sharing the same closed environment and can pose a human health hazard. By modifying the technique for use of a commercially available mercury indicating powder (Mallinckrodt Baker, Inc., J. T. Baker Mercury Indicator) it is possible to create an inexpensive and fairly rapid test for mercury vapor in herbarium cabinets. The indicator is mixed with deionized water and applied to glass microscope slides. One or more slides are placed inside a cabinet and any color change in the indicator is compared to unexposed controls. In the authors' experiments, the indicator results were compared against readings taken using a Jerome 431-X Mercury Vapor Analyzer and a Lumex RA-915+ Multifunctional Mercury Analyzer and were found to be broadly related to the concentration of mercury vapor present in each cabinet. The method can be used to check for mercury contamination in incoming shipments of specimens and to identify cabinets that currently contain or formerly contained contaminated specimens. Practical safety Guidelines have been developed for accessing cabinets that give a positive test for the vapor and for handling contaminated specimens. C1 Smithsonian Off Safety & Environm Management, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Bot Sect, Washington, DC 20560 USA. US DOE, Washington, DC 20585 USA. NIOSH, Robert A Taft Labs, Cincinnati, OH 45226 USA. RP Bell, D (reprint author), 2419 Barbour Rd, Falls Church, VA 22043 USA. EM cahawks@aol.com; makosk@si.edu; bell.deborah@nmnh.si.edu; paul.wambach@eh.doe.gov; geb1@cdc.gov NR 40 TC 4 Z9 4 U1 0 U2 4 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD AUG PY 2004 VL 53 IS 3 BP 783 EP 790 DI 10.2307/4135451 PG 8 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 860WC UT WOS:000224373500014 ER PT J AU Laurance, WF AF Laurance, WF TI The perils of payoff: corruption as a threat to global biodiversity SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID CONSERVATION PRIORITIES; HOTSPOTS AB Corruption is a worldwide phenomenon, particularly in many developing countries, which contain a large proportion of global biodiversity. Most alarming, from a biodiversity-conservation perspective, is the frequent corruption of government officials who manage valuable natural resources, such as timber, oil and precious minerals. A recent study by Joyotee Smith and colleagues describes rampant corruption in the timber industry of Indonesia, and shifts in the prevalence of different types of corruption as the country has become destabilized politically. By placing corruption into a conceptual framework, Smith et al. provide important insights into how developing nations and their natural resources can be besieged by corruption. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012 NR 24 TC 42 Z9 42 U1 0 U2 15 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD AUG PY 2004 VL 19 IS 8 BP 399 EP 401 DI 10.1016/j.tree.2004.06.001 PG 3 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 846EL UT WOS:000223298000001 PM 16701292 ER PT J AU Agnarsson, I AF Agnarsson, I TI Morphological phylogeny of cobweb spiders and their relatives (Araneae, Araneoidea, Theridiidae) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE Anelosimus; araneophagy; Argyrodes; Argyrodinae; cladistics; comb footed spiders; Hadrotarsinae; kleptoparasitism; Latrodectinae; maternal care; Pholcommatinae; Spintharinae; sociality; Theridiinae; web evolution ID ARGYRODES-ANTIPODIANUS ARANEAE; ANELOSIMUS-STUDIOSUS ARANEAE; ACHAEARANEA-WAU THERIDIIDAE; AUSTRALIAN REDBACK SPIDER; WEB-CONSTRUCTION BEHAVIOR; ORB-WEAVING SPIDER; DIVISION-OF-LABOR; SOCIAL SPIDER; KLEPTOPARASITIC SPIDER; BLACK-WIDOW AB This paper offers the first cladistic analysis of a wide selection of theridiid genera based on morphological data. The analysis treats 53 theridiid taxa representing 32 genera (Achaearanea, Anelosimus, Ameridion, Argyrodes, Ariamnes, Carniella, Cerocida, Chrysso, Coleosoma, Dipoena, Emertonella, Enoplognatha, Episinus, Euryopis, Faiditus, Kochiura, Latrodectus, Neospintharus, Nesticodes, Pholcomma, Phoroncidia, Rhomphaea, Robertus, Selkirkiella, Spintharus, Steatoda, Stemmops, Theridion, Theridula, Thymoites, Thwaitesia, Tidarren) and eight outgroup taxa representing the families Nesticidae (Eidmanella and Nesticus), Synotaxidae (Synotaxus, two species), Pimoidae (Pimoa), Linyphiidae (Linyphia), Tetragnathidae (Tetragnatha) and Araneidae (Argiope). The parsimony analysis of 242 morphological and behavioural characters found a single, most parsimonious tree. The monophyly of theridiids and their sister relationship with nesticids is strongly supported. The recent resurrection of Ariamnes and Rhomphaea from Argyrodes made the latter paraphyletic. However, Ariamnes and Rhomphaea are characterized by an array of characters, and Argyrodes still contains dramatically distinct clades for which names are available: Faiditus (removed from synonymy - RS) and Neospintharus (RS). These revalidations provide a classification with greater information content and utility. These three genera, along with Ariamnes, Rhomphaea and Spheropistha, comprise the subfamily Argyrodinae. The monophyly and composition of the subfamilies Hadrotarsinae, Spintharinae, Pholcommatinae, Latrodectinae and Theridiinae are discussed. Theridion is paraphyletic and in need of revision. Anelosimus as currently circumscribed is paraphyletic, a problem resolved by revalidating Selkirkiella (RS) and Kochiura (RS). Numerous new combinations are established. The results suggest the monophyletic origin of both kleptoparasitism and araneophagy in the lineage leading to Argyrodinae, negating hypotheses that either arose from the other. Sociality evolved multiple times within the family, accounting for as much as one fourth of the origins of social behaviour among all spiders. No losses of sociality are implied. The hypothesis of maternal care as the pathway to sociality receives support. Evolution of theridiid webs is complex, with multiple modifications and loss of the basic theridiid cobweb. (C) 2004 The Linnean Society of London. C1 Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Sci Biol, Washington, DC 20052 USA. RP Agnarsson, I (reprint author), Smithsonian Inst, POB 37012,NMNH E529,NHB-105, Washington, DC 20013 USA. EM ingi@gwu.edu NR 313 TC 135 Z9 155 U1 6 U2 47 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD AUG PY 2004 VL 141 IS 4 BP 447 EP 626 DI 10.1111/j.1096-3642.2004.00120.x PG 180 WC Zoology SC Zoology GA 847BG UT WOS:000223363100001 ER PT J AU Davis, CC Wurdack, KJ AF Davis, CC Wurdack, KJ TI Host-to-parasite gene transfer in flowering plants: Phylogenetic evidence from malpighiales SO SCIENCE LA English DT Article ID MITOCHONDRIAL; RAFFLESIA AB Horizontal gene transfer (HGT) between sexually unrelated species has recently been documented for higher plants, but mechanistic explanations for HGTs have remained speculative. We show that a parasitic relationship may facilitate HGT between flowering plants. The endophytic parasites Rafflesiaceae are placed in the diverse order Malpighiales. Our multigene phylogenetic analyses of Malpighiales show that mitochrodrial ( matR) and nuclear loci (18S ribosomal DNA and PHYC) place Rafflesiaceae in Malpighiales, perhaps near Ochnaceae/Clusiaceae. Mitochondrial nad1B-C, however, groups them within Vitaceae, near their obligate host Tetrastigma. These discordant phylogenetic hypotheses strongly suggest that part of the mitochondrial genome in Rafflesiaceae was acquired via HGT from their hosts. C1 Univ Michigan Herbarium, Ann Arbor, MI 48108 USA. Smithsonian Inst, Dept Bot, Suitland, MD 20746 USA. Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. RP Davis, CC (reprint author), Univ Michigan Herbarium, 3600 Vars Dr, Ann Arbor, MI 48108 USA. EM chdavis@umich.edu NR 12 TC 141 Z9 156 U1 3 U2 37 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 JUL 30 PY 2004 VL 305 IS 5684 BP 676 EP 678 DI 10.1126/science.1100671 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 842GQ UT WOS:000222992100051 PM 15256617 ER PT J AU Saetre, P Lindberg, J Leonard, JA Olsson, K Pettersson, U Ellegren, H Bergstrom, TF Vila, C Jazin, E AF Saetre, P Lindberg, J Leonard, JA Olsson, K Pettersson, U Ellegren, H Bergstrom, TF Vila, C Jazin, E TI From wild wolf to domestic dog: gene expression changes in the brain SO MOLECULAR BRAIN RESEARCH LA English DT Article DE DNA microarrays; gene expression variation; domestication; brain evolution; speciation ID NEUROPEPTIDE-Y DISTRIBUTION; REGULATORY VARIATION; PEPTIDE; EVOLUTION; HUMANS; MOUSE; RATS; NEUROENDOCRINE; QUANTIFICATION; TRANSCRIPTION AB Despite the relatively recent divergence time between domestic dogs (Canis familiaris) and gray wolves (Canis lupus), the two species show remarkable behavioral differences. Since dogs and wolves are nearly identical at the level of DNA sequence, we hypothesize that the two species may differ in patterns of gene expression. We compare gene expression patterns in dogs, wolves and a close relative, the coyote (Cams latrans), in three parts of the brain: hypothalamus, amygdala and frontal cortex, with microarray technology. Additionally, we identify genes with region-specific expression patterns in all three species. Among the wild canids, the hypothalamus has a highly conserved expression profile. This contrasts with a marked divergence in domestic dogs. Real-time PCR experiments confirm the altered expression of two neuropeptides, CALCB and NPY Our results suggest that strong selection on dogs for behavior during domestication may have resulted in modifications of mRNA expression patterns in a few hypothalamic genes with multiple functions. This study indicates that rapid changes in brain gene expression may not be exclusive to the development of human brains. Instead, they may provide a common mechanism for rapid adaptive changes during speciation, particularly in cases that present strong selective pressures on behavioral characters. (C) 2004 Elsevier B.V. All rights reserved. C1 Uppsala Univ, Dept Evolut Genomics & Systemat, S-75236 Uppsala, Sweden. Linnaeus Ctr Bioinformat, Biomed Ctr, S-75124 Uppsala, Sweden. Uppsala Univ, Dept Genet & Pathol, Med Genet Sect, Rudbeck Lab, SE-75185 Uppsala, Sweden. Swedish Univ Agr Sci, Dept Anat & Physiol, S-75007 Uppsala, Sweden. Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. RP Jazin, E (reprint author), Uppsala Univ, Dept Evolut Genomics & Systemat, Norbyvagen 18D, S-75236 Uppsala, Sweden. EM Elena.Jazin@ebc.uu.se RI Vila, Carles/H-4893-2013; Leonard, Jennifer/A-7894-2010; Bergstrom, Tomas/B-4681-2017 OI Vila, Carles/0000-0002-4206-5246; Leonard, Jennifer/0000-0003-0291-7819; Bergstrom, Tomas/0000-0002-7480-2669 NR 51 TC 78 Z9 81 U1 7 U2 76 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-328X J9 MOL BRAIN RES JI Mol. Brain Res. PD JUL 26 PY 2004 VL 126 IS 2 BP 198 EP 206 DI 10.1016/j.molbrainres.2004.05.003 PG 9 WC Neurosciences SC Neurosciences & Neurology GA 844ON UT WOS:000223168200012 ER PT J AU Campbell, BA Maxwell, TA Freeman, A AF Campbell, BA Maxwell, TA Freeman, A TI Mars orbital synthetic aperture radar: Obtaining geologic information from radar polarimetry SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; radar ID SHUTTLE IMAGING RADAR; SAR DATA; BIR-SAFSAF; PENETRATION; SCATTERING; SURFACE; BACKSCATTERING; ATTENUATION; CALIBRATION; ROUGHNESS AB Radar penetration of mantling layers, and scattering from buried objects or interfaces, is a topic of current interest in both terrestrial and planetary remote sensing. We examine the behavior of surface and subsurface scattering interfaces and the types of information that may be obtained from observations in different polarizations and wavelengths. These results are applied to the design of a future Mars orbital synthetic aperture radar (SAR), for which we draw the following conclusions. (1) Mapping of buried geologic features is best accomplished using VV polarization, at an optimal wavelength determined by the competing effects of antenna gain, attenuation in the dust, and the reduction in effective surface roughness with wavelength. P band frequencies (similar to1 GHz or less) offer the best opportunity for detection of moderately rough, buried features. (2) The relative roles of surface and subsurface scattering may be determined using measurements in HH and VV polarization, with a channel gain calibration better than 0.5 dB. (3) The thickness of a mantling layer (or ice mass) cannot be directly inferred from multiwavelength observations. Layer thickness may be inferred from the interferometric correlation of backscatter measurements collected on suitably spaced orbital passes, though the required phase measurement accuracy is challenging. While additional information may be gained by collecting scattering data in more polarizations or wavelengths, we suggest that the primary science goals of a Mars-orbiting radar could be accomplished by a single-wavelength system capable of collecting VV and HH polarizations with the calibration and orbit control needed to permit interferometric analysis. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM campbellb@nasm.si.edu NR 40 TC 10 Z9 11 U1 0 U2 2 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 JUL 23 PY 2004 VL 109 IS E7 AR E07008 DI 10.1029/2004JE002264 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 841GN UT WOS:000222917900001 ER PT J AU Gingerich, O AF Gingerich, O TI A radical reorientation SO NATURE LA English DT Editorial Material C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 22 PY 2004 VL 430 IS 6998 BP 407 EP 407 DI 10.1038/430407a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 839RD UT WOS:000222801400023 PM 15269748 ER PT J AU Beswick, RJ Peck, AB Taylor, GB Giovannini, G AF Beswick, RJ Peck, AB Taylor, GB Giovannini, G TI High-resolution imaging of the radio continuum and neutral gas in the inner kiloparsec of the radio galaxy 3C 293 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : individual : 3C 293; radio lines : galaxies ID TELESCOPE SNAPSHOT SURVEY; FREE-FREE ABSORPTION; VLBI OBSERVATIONS; HYDROGEN ABSORPTION; SOURCE COUNTERPARTS; RELATIVISTIC JETS; COMPLETE SAMPLE; MOLECULAR GAS; 3C 293; SCALE AB Using a combination of observations involving the Very Large Array (VLA), MERLIN and global Very Long Baseline Interferometry (VLBI) networks we have made a detailed study of the radio continuum and the neutral hydrogen (H I) kinematics and distribution within the central kiloparsec of the radio galaxy 3C 293. These observations trace the complex jet structure and identify the position of the steeply inverted radio core at 1.3 GHz. Strong H I absorption is detected against the majority of the inner kiloparsec of 3C 293. This absorption is separated into two dynamically different and spatially resolved systems. Against the eastern part of the inner radio jet, narrow H I absorption is detected and shown to have higher optical depths in areas cospatial with a central dust lane. Additionally, this narrow line is shown to follow a velocity gradient of similar to50 km s(-1) arcsec(-1), consistent with the velocity gradient observed in optical spectroscopy of ionized gas. We conclude that the narrow HI absorption, dust and ionized gas are physically associated and situated several kiloparsecs from the centre of the host galaxy. Against the western jet emission and core component, broad and complex H I absorption is detected. This broad and complex absorption structure is discussed in terms of two possible interpretations for the gas kinematics observed. We explore the possibility that these broad, double absorption spectra are the result of two gas layers at different velocities and distances along these lines of sight. A second plausible explanation for this absorbing structure is that the H I is situated in rotation about the core of this radio galaxy with some velocity dispersion resulting from infall and outflow of gas from the core region. If the latter explanation were correct, then the mass enclosed by the rotating disc would be at least 1.7x10(9) solar masses within a radius of 400 pc. C1 Nuffield Radio Astron Observ Labs, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Harvard Smithsonian Ctr Astrophys, SAO SMA Project, Hilo, HI 96721 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. CNR, Ist Radioastron, I-40129 Bologna, Italy. RP Beswick, RJ (reprint author), Nuffield Radio Astron Observ Labs, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. EM rbeswick@jb.man.ac.uk OI Giovannini, Gabriele/0000-0003-4916-6362 NR 30 TC 29 Z9 29 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2004 VL 352 IS 1 BP 49 EP 60 DI 10.1111/j.1365-2966.2004.07892.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 836TI UT WOS:000222578300005 ER PT J AU Nagamine, K Cen, RY Hernquist, L Ostriker, JP Springel, V AF Nagamine, K Cen, RY Hernquist, L Ostriker, JP Springel, V TI Is there a missing galaxy problem at high redshift? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : evolution; galaxies : formation; methods : numerical; stars : formation ID HUBBLE DEEP FIELD; SMOOTHED PARTICLE HYDRODYNAMICS; ULTRAVIOLET LUMINOSITY DENSITY; STAR-FORMATION HISTORY; LYMAN-BREAK GALAXIES; DARK-MATTER UNIVERSE; STELLAR MASS DENSITY; LY-ALPHA EMITTERS; PHOTOMETRIC REDSHIFTS; FORMING GALAXIES AB We study the evolution of the global stellar mass density in a Lambda cold dark matter (LambdaCDM) universe using two different types of hydrodynamic simulations (Eulerian total variation diminishing and smoothed particle hydrodynamics) and the analytical model of Hernquist & Springel. We find that the theoretical calculations all predict both a higher stellar mass density at z similar to 3 than indicated by current observations and that the peak of the cosmic star formation rate history should lie at z greater than or similar to 5. Such a star formation history implies that as much as (70%, 30%) of the total stellar mass density today must already have formed by z ( 1; 3). Our results suggest that current observations at z similar to 3 are missing as much as 50% of the total stellar mass density in the universe, perhaps because of an inadequate allowance for dust obscuration in star-forming galaxies, limited sample sizes, or cosmic variance. We also compare our results with some of the updated semianalytic models of galaxy formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Nagamine, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM knagamin@cfa.harvard.edu NR 79 TC 59 Z9 59 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 45 EP 50 DI 10.1086/421379 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700005 ER PT J AU Di Matteo, T Croft, RAC Springel, V Hernquist, L AF Di Matteo, T Croft, RAC Springel, V Hernquist, L TI The cosmological evolution of metal enrichment in quasar host galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : abundances; galaxies : evolution; methods : numerical ID SMOOTHED PARTICLE HYDRODYNAMICS; HIGH-REDSHIFT QUASARS; DARK-MATTER UNIVERSE; ACTIVE GALACTIC NUCLEI; STAR-FORMATION; ELEMENTAL ABUNDANCES; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; STELLAR SOURCES; PHYSICAL MODEL AB We study the gas metallicity of quasar hosts using cosmological hydrodynamic simulations of the LambdaCDM model. Galaxy formation in the simulations is coupled with a prescription for black hole activity, enabling us to study the evolution of the metal enrichment in quasar hosts and hence explore the relationship between star/spheroid formation and black hole growth/activity. In order to assess effects of numerical resolution, we compare simulations with different particle numbers and box sizes. We find a steep radial metallicity gradient in quasar host galaxies, with gas metallicities close to solar values in the outer parts but becoming supersolar in the center. The hosts of the rare bright quasars at z similar to 5-6 have star formation rates of several hundred M-circle dot yr(-1) and halo masses of order similar to10(12) M-circle dot. Already at these redshifts they have supersolar (Z/Z(circle dot) similar to 2-3) central metallicities, with a mild dependence of metallicity on luminosity, consistent with observed trends. The mean value of metallicity is sensitive to the assumed quasar lifetime, providing a useful new probe of this parameter. We find that lifetimes from 10(7) to 4 x 10(7) yr are favored by comparison with observational data. In both the models and observations, the rate of evolution of the mean quasar metallicity as a function of redshift is generally flat out to z similar to 4-5. Beyond the observed redshift range and out to redshift z = 6-8, we predict a slow decline of the mean central metallicity toward solar and slightly subsolar values (Z/Z(circle dot) degrees 0.4-1) as we approach the epoch of the first significant star formation activity. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. RI Di Matteo, Tiziana/O-4762-2014; Croft, Rupert/N-8707-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734; Croft, Rupert/0000-0003-0697-2583 NR 56 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 80 EP 92 DI 10.1086/421036 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700009 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, JSB Loeb, A TI Redshifted 21 centimeter signatures around the highest redshift quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; intergalactic medium; quasars : general; radio lines : general ID DIGITAL SKY SURVEY; PROBE WMAP OBSERVATIONS; COSMIC DARK-AGES; COSMOLOGICAL REIONIZATION; INTERGALACTIC MEDIUM; LUMINOUS QUASARS; BLACK-HOLES; 21-CM LINE; HYDROGEN; EMISSION AB The Lyalpha absorption spectrum of the highest redshift quasars indicates that they are surrounded by giant H II regions, a few megaparsecs in size. The neutral gas around these H II regions should emit 21 cm radiation in excess of the cosmic microwave background and enable future radio telescopes to measure the transverse extent of these H II regions. At early times, the H II regions expand with a relativistic speed. Consequently, their measured sizes along the line of sight (via Lyalpha absorption) and transverse to it ( via 21 cm emission) should have different observed values due to relativistic time delay. We show that the combined measurement of these sizes would directly constrain the neutral fraction of the surrounding intergalactic medium (IGM) as well as the quasar lifetime. Based on current number counts of luminous quasars at z greater than or similar to 6, an instrument like LOFAR should detect greater than or similar to2 redshifted 21 cm shells per field ( with a radius of 11degrees) around active quasars as bright as those already discovered by Sloan Digital Sky Survey, and greater than or similar to200 relic shells of inactive quasars per field. We show that Lyalpha photons from the quasar are unable to heat the IGM or to couple the spin and kinetic temperatures of atomic hydrogen beyond the edge of the H II region. The detection of the IGM in 21 cm emission around high-redshift quasars would therefore gauge the presence of a cosmic Lyalpha background during the reionization epoch. C1 Univ Melbourne, Parkville, Vic 3052, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wyithe, JSB (reprint author), Univ Melbourne, Parkville, Vic 3052, Australia. EM swyithe@isis.ph.unimelb.edu.au; aloeb@cfa.harvard.edu OI Wyithe, Stuart/0000-0001-7956-9758 NR 47 TC 40 Z9 40 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 117 EP 127 DI 10.1086/421042 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700012 ER PT J AU Le Bohec, S Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Catanese, M Celik, O Cui, W Daniel, M D'Vali, M Perez, ID Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Jarvis, A Jordan, M Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Linton, E Lloyd-Evans, J Milovanovic, A Moriarty, P Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J AF Le Bohec, S Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Catanese, M Celik, O Cui, W Daniel, M D'Vali, M Perez, ID Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Jarvis, A Jordan, M Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Linton, E Lloyd-Evans, J Milovanovic, A Moriarty, P Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J TI Observation of M87 at 400 GeV with the Whipple 10 meter telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (M87); gamma rays : observations ID TEV GAMMA-RAYS; BL-LACERTAE OBJECT; HIGH-RESOLUTION; GALAXY M-87; LAC OBJECT; JET; EMISSION; SPECTRUM; RADIO; POLARIZATION AB We present results from observations taken with the Whipple 10 m very high energy gamma-ray telescope with maximal sensitivity at 400 GeV during 39 hr between 2000 and 2003 in the direction of the giant radio galaxy M87. Using the entire data set, we derive a 99% confidence level upper limit on the flux of gamma-ray emission above 400 GeV from M87 to be less than or equal to 6: 9; 10(-1)2 cm(-2) s(-1). This suggests variability at the 90% confidence level when compared to the flux measured by the HEGRA collaboration in 1999 if the differential spectrum is steeper than a power law of index 3.75. Our search for a correlation between the Rossi X-Ray Timing Explorer all-sky monitor observation and a potential gamma-ray signal is inconclusive. C1 Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland, Expt Phys Dept, Dublin 4, Ireland. Natl Univ Ireland, Dept Phys, Galway, Ireland. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Le Bohec, S (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. EM lebohec@iastate.edu RI Hall, Jeter/E-9294-2015; Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 48 TC 15 Z9 15 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 JUL 20 PY 2004 VL 610 IS 1 BP 156 EP 160 DI 10.1086/421697 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700016 ER PT J AU McIntosh, DH Rix, HW Caldwell, N AF McIntosh, DH Rix, HW Caldwell, N TI Structural evidence for environment-driven transformation of the blue galaxies in local Abell clusters: A85, A496, and A754 SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : clusters : general; galaxies : clusters : individual (A85, A496, A754); galaxies : evolution; galaxies : fundamental parameters; galaxies : structure ID HUBBLE-SPACE-TELESCOPE; BAND SURFACE PHOTOMETRY; DISK DOMINATED GALAXIES; STAR-FORMATION RATE; MORPHOLOGY-DENSITY RELATION; COLOR-MAGNITUDE RELATION; RAY LUMINOSITY CLUSTERS; BUTCHER-OEMLER CLUSTERS; GROTH STRIP SURVEY; DIGITAL SKY SURVEY AB We present a detailed comparison of structural properties in the rest-frame V band of cluster and field galaxies, selected and analyzed in the same manner, to test the hypothesis that much of the current cluster galaxy membership resulted from the fairly rapid (1-2 Gyr) transformation of infalling, field spirals into red, cluster early types. Specifically, we have selected similar to140 galaxies from three nearby Abell clusters (A85, A496, and A754) that have colors significantly bluer than the red sequence population and compared them to similar to80 field galaxies with similar colors and luminosities from the Nearby Field Galaxy Survey. The comparison is based on the hypothesis that recent (1-4 Gyr) cluster arrivals were originally blue and star-forming, then stopped forming stars to dim and redden in a few gigayears. For the comparison we quantify galaxy internal structure and morphology from two-dimensional bulge/disk decompositions using GIM2D. We observe structural differences between blue galaxies in local (z < 0.06) clusters, compared to field environments. All cluster galaxies have spectroscopic membership. The majority of blue cluster members, presumably recent additions, are physically smaller and fainter than their equally colored field counterparts. At a matched size and luminosity, the newer cluster arrivals are quantifiably smoother in appearance, yet their total light is as disk dominated as in normal field spirals. Moreover, half of the blue cluster members appear to have blue cores or globally blue color profiles, in contrast with field spirals, which typically exhibit red inward color gradients. Blue cores suggest enhanced nuclear star formation, possibly a starburst, while uniformly blue profiles are consistent with an episode of fairly strong global star formation in the past few gigayears. Our previous work shows that the blue membership of local clusters is a recently infalling population that has yet to encounter the dense core. In a universe without environmentally dependent evolution outside of cluster cores, we would expect blue disk galaxies inhabiting field and cluster regions to have similar morphology, size, and color gradient distributions. Our findings show conclusively not only that the abundance of red and blue galaxies depends on environment, but also that fundamental structural and morphological galaxy properties do indeed reflect the environment in which the galaxy is found. Moreover, the data show that the transformation of accreted galaxies is not confined to the dense cluster core. The overall properties of bluer cluster members are best explained by environment-driven transformation of accreted field spirals, and our results suggest that the processes that govern color and morphological evolution occur separately. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Smithsonian Astrophys Observ, Solar & Stellar Phys Div, Cambridge, MA 02138 USA. RP McIntosh, DH (reprint author), Univ Massachusetts, Lederle Grad Res Tower, Amherst, MA 01003 USA. EM dmac@hamerkop.astro.umass.edu; rix@mpia-hd.mpg.de; caldwell@cfa.harvard.edu NR 116 TC 25 Z9 25 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 161 EP 182 DI 10.1086/421435 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700017 ER PT J AU Machacek, ME Jones, C Forman, WR AF Machacek, ME Jones, C Forman, WR TI Chandra observations of NGC 4438: An environmentally damaged galaxy in the Virgo cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : individual (NGC 4438); intergalactic medium; X-rays : galaxies ID HUBBLE-SPACE-TELESCOPE; DWARF SEYFERT NUCLEI; X-RAY-EMISSION; NEARBY GALAXIES; STAR-FORMATION; STARBURST GALAXIES; DISTANT CLUSTERS; SPIRAL GALAXIES; S0 GALAXIES; GAS AB We present results from a 25 ks Chandra ACIS-S observation of galaxies NGC 4438 and NGC 4435 in the Virgo Cluster. X-ray emission in NGC 4438 is observed in a similar to700 pc nuclear region, a similar to2.3 kpc spherical bulge, and a network of filaments extending 4-10 kpc to the west and southwest of the galaxy. The X-ray emission in all three regions is highly correlated to similar features observed in Halpha. Spectra of the filaments and bulge are well represented by a 0.4 keV MEKAL model with combined 0.3-2 keV intrinsic luminosity L-X 1.24 x 10(40) ergs s(-1), electron densities similar to0.02-0.04 cm(-3), cooling times of 400-700 Myr, and X- ray gas mass less than or similar to3.7 x 10(8) M-circle dot. In the nuclear region of NGC 4438 X- ray emission is seen from the nucleus and from two outflow bubbles extending 360 pc ( 730 pc) to the northwest (southeast) of the nucleus. The spectrum of the northwest outflow bubble plus nucleus is well fitted by an absorbed (n(H) = 1.9(-0.4)(+1.0) x 10(21) cm(-2)) 0.58(-0.10)(+0.04) keV MEKAL plasma model plus a heavily adsorbed (n(H) = 2.9(-2.0)(+3.1) x 10(22) cm(-2)) Gamma = 2, power-law component. The electron density, cooling time, and X- ray gas mass in the northwest outflow are similar to0.5 cm(-3), 30 Myr, and 3.5 x 10(6) M-circle dot, respectively. Weak X- ray emission is observed in the central region of NGC 4435 with the peak of the hard emission coincident with the galaxy's optical center, while the peak of the soft X- ray emission is displaced 316 pc to the northeast. The spectrum of NGC 4435 is well fitted by a nonthermal power law plus a thermal component from 0.2 - 0.3 keV diffuse interstellar medium gas. We argue that the X-ray properties of gas outside the nuclear region in NGC 4438 and NGC 4435 favor a high- velocity, off- center collision between these galaxies similar to100 Myr ago, while the nuclear X-ray-emitting outflow gas in NGC 4438 has been heated only recently (within similar to1-2 Myr) by shocks (v(s) similar to 600 km s(-1)) possibly powered by a central active galactic nucleus. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Machacek, ME (reprint author), Harvard Smithsonian Ctr Astrophys, MS 67,60 Garden St, Cambridge, MA 02138 USA. EM mmachacek@cfa.harvard.edu; cjf@head-cfa.cfa.harvard.edu; wrf@head-cfa.cfa.harvard.edu NR 71 TC 35 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 183 EP 200 DI 10.1086/421448 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700018 ER PT J AU Martini, P Ho, LC AF Martini, P Ho, LC TI A population of massive globular clusters in NGC 5128 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 5128); galaxies : star clusters; globular clusters : general ID HUBBLE-SPACE-TELESCOPE; CORE VELOCITY DISPERSIONS; COMPACT DWARF GALAXIES; TO-LIGHT RATIOS; ELLIPTIC GALAXIES; STRUCTURAL PARAMETERS; STELLAR-SYSTEMS; OMEGA-CENTAURI; FUNDAMENTAL PLANE; LOCAL GROUP AB We present velocity dispersion measurements of 14 globular clusters in NGC 5128 (Centarus A) obtained with the MIKE echelle spectrograph on the 6.5 m Magellan Clay telescope. These clusters are among the most luminous globular clusters in NGC 5128 and have velocity dispersions comparable to the most massive clusters known in the Local Group, ranging from 10 to 30 km s(-1). We describe in detail our cross-correlation measurements, as well as simulations to quantify the uncertainties. These 14 globular clusters are the brightest NGC 5128 globular clusters with surface photometry and structural parameters measured from the Hubble Space Telescope. We have used these measurements to derive masses and mass-to-light ratios for all of these clusters and establish that the fundamental plane relations for globular clusters extend to an order-of-magnitude higher mass than in the Local Group. The mean mass-to-light ratio for the NGC 5128 clusters is similar to3 +/- 1, higher than measurements for all but the most massive Local Group clusters. These massive clusters begin to bridge the mass gap between the most massive star clusters and the lowest mass galaxies. We find that the properties of NGC 5128 globular clusters overlap quite well with the central properties of nucleated dwarf galaxies and ultracompact dwarf galaxies. As six of these clusters also show evidence for extratidal light, we hypothesize that at least some of these massive clusters are the nuclei of tidally stripped dwarfs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. RP Martini, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 20, Cambridge, MA 02138 USA. EM pmartini@cfa.harvard.edu; lho@ociw.edu NR 68 TC 56 Z9 56 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 233 EP 246 DI 10.1086/421458 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700022 ER PT J AU Di Stefano, R Kong, AKH Greiner, J Primini, FA Garcia, MR Barmby, P Massey, P Hodge, PW Williams, BF Murray, SS Curry, S Russo, TA AF Di Stefano, R Kong, AKH Greiner, J Primini, FA Garcia, MR Barmby, P Massey, P Hodge, PW Williams, BF Murray, SS Curry, S Russo, TA TI Supersoft X-ray sources in M31. I. A Chandra survey and an extension to quasi-soft sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); X-rays : binaries; X-rays : galaxies ID LARGE MAGELLANIC CLOUD; HIGH-RESOLUTION CAMERA; ROSAT PSPC SURVEY; POINT SOURCES; SUPERNOVA-REMNANTS; EXTERNAL GALAXIES; CENTRAL REGION; POPULATION; DISCOVERY; TRANSIENT AB We report on very soft X-ray sources (VSSs) in M31. In a survey that was most sensitive to soft sources in four 80; 80 regions covered by Chandra's ACIS-S S3 CCD, we find 33 VSSs that appear to belong to M31. Fifteen VSSs have spectral characteristics mirroring the supersoft X-ray sources studied in the Magellanic Clouds and Milky Way (kT(eff) less than or equal to 100 eV); we therefore call these "classical" supersoft sources, or simply supersoft sources (SSSs). Eighteen VSSs may have either small(<10%) hard components or slightly higher effective temperatures (but still less than 350 eV). We refer to these VSSs as quasi-soft sources (QSSs). While hot white dwarf models may apply to SSSs, the effective temperatures of QSSs are too high, unless, e. g., the radiation emanates from only a small portion of surface. Two of the SSSs were first detected and identified as such through ROSAT observations. One SSS and one QSS may be identified with symbiotics and two SSSs with supernova remnants. Both SSSs and QSSs in the disk are found near star-forming regions, possibly indicating that they are young. VSSs in the outer disk and halo are likely to be old systems; in these regions, there are more QSSs than SSSs, which is opposite to what is found in fields closer to the galaxy center. The largest density of bright VSSs is in the bulge; some of the bulge sources are close enough to the nucleus to be remnants of the tidal disruption of a giant by the massive central black hole. By using Chandra data in combination with ROSAT and XMM observations, we find most VSSs to be highly variable, fading from or brightening toward detectability on timescales of months. There is evidence for VSSs with low luminosities (&SIM;10(36) ergs s(-1)). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Lowell Observ, Flagstaff, AZ 86001 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rdistefano@cfa.harvard.edu RI Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Primini, Francis/0000-0002-6077-0643 NR 53 TC 52 Z9 52 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 247 EP 260 DI 10.1086/421696 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700023 ER PT J AU Greiner, J Di Stefano, R Kong, A Primini, F AF Greiner, J Di Stefano, R Kong, A Primini, F TI Supersoft X-ray sources in M31. II. ROSAT-detected supersoft sources in the ROSAT, Chandra, and XMM-Newton eras SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; galaxies : individual (M31); novae, cataclysmic variables; X-rays : stars ID SOURCE RX J0513.9-6951; RECURRENT NOVAE; PSPC SURVEY; POPULATION; M-31; VARIABILITY; STATES; CAL-83; LMC AB We have performed Chandra observations during the past three years of five of the M31 supersoft X-ray sources discovered with ROSAT. Surprisingly, only one of these sources has been detected, despite a predicted detection of about 20-80 counts for these sources. This has motivated a thorough check of the ROSAT M31 Survey I data, including a relaxation of the hardness ratio requirement used to select supersoft sources. This increases the number of supersoft sources identified in Survey I by seven. We then carried out a comparison with the ROSAT M31 Survey II data set, which had hitherto not been explicitly investigated for supersoft X-ray sources. We find that most of the ROSAT Survey I sources are not detected, and only two new supersoft sources are identified. The low detection rate in the ROSAT Survey II and our Chandra observations imply that the variability timescale of supersoft sources is a few months. If the majority of these sources are close binary supersoft sources with shell hydrogen burning, it further implies that half of these sources predominantly experience large mass transfer rates. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Greiner, J (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM jcg@mpe.mpg.de OI Primini, Francis/0000-0002-6077-0643 NR 31 TC 25 Z9 25 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 261 EP 268 DI 10.1086/421455 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700024 ER PT J AU Nichols, JS Slavin, JD AF Nichols, JS Slavin, JD TI Shocked clouds in the Vela supernova remnant SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Vela Supernova Remnant); shock waves; supernova remnants ID HIGH-VELOCITY GAS; ABSORPTION-LINES; X-RAY; HYDRODYNAMIC INTERACTION; INTERSTELLAR ABSORPTION; CARINA NEBULA; IRAS SURVEY; ULTRAVIOLET; SPECTROSCOPY; DIRECTION AB Unusually strong high-excitation C I has been detected in 11 lines of sight through the Vela supernova remnant (SNR) by means of UV absorption line studies of IUE data. Most of these lines of sight lie near the western edge of the bright X-ray region of the SNR in a spatially distinct band approximately 1degrees by 4degrees oriented approximately north-south. The high-excitation C I (denoted C I* and C I**) is interpreted as evidence of a complex of shocked dense clouds interacting with the SNR, because of the high pressures indicated in this region. To further analyze the properties of this region of enhanced C i* and C i**, we present new HIRES-processed IRAS data of the entire Vela SNR. A temperature map calculated from the HIRES IRAS data, based on a two-component dust model, reveals the signature of hot dust at several locations in the SNR. The hot dust is anticorrelated spatially with X-ray emission, as would be expected for a dusty medium interacting with a shock wave. The regions of hot dust are strongly correlated with optical filaments, supporting a scenario of dense clouds interior to the SNR that have been shocked and are now cooling behind the supernova blast wave. With few exceptions, the lines of sight to the strong high-excitation C I pass through regions of hot dust and optical filaments. Possible mechanisms for the production of the unexpectedly large columns of high-excitation C I are discussed. Dense clouds on the back western hemisphere of the remnant may explain the relatively low X-ray emission in the western portion of the Vela SNR due to the slower forward shock velocity in regions where the shock has encountered the dense clouds. An alternate explanation for the presence of ground-state and excited-state neutrals,as well as ionized species, along the same line of sight is a magnetic precursor that heats and compresses the gas ahead of the shock. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nichols, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 34, Cambridge, MA 02138 USA. EM jnichols@cfa.harvard.edu; jslavin@cfa.harvard.edu OI Slavin, Jonathan/0000-0002-7597-6935 NR 41 TC 13 Z9 13 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 285 EP 302 DI 10.1086/421545 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700027 ER PT J AU Lada, CJ Huard, TL Crews, LJ Alves, JF AF Lada, CJ Huard, TL Crews, LJ Alves, JF TI Discovery of a dusty ring in the coalsack: A dense core caught in the act of formation? SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : clouds; ISM : globules; ISM : molecules ID SOUTHERN COALSACK; STAR-FORMATION; INFRARED EXTINCTION; DARK CLOUDS; MOLECULAR CLOUDS; BOK GLOBULE; IC 5146; FRAGMENTATION; COLLAPSE AB We present a new infrared extinction study of Globule 2, the most opaque molecular cloud core in the Coalsack complex. Using deep near-infrared imaging observations obtained with the ESO New Technology Telescope, we are able to examine the structure of the globule in significantly greater detail than previously possible. We find the most prominent structural feature of this globule to be a strong central ring of dust column density that was not evident in lower resolution studies of this cloud. This ring represents a region of high density and pressure that is likely a transient structure. For a spherical cloud geometry, the ring would correspond to a dense inner shell of high pressure that could not be in dynamical equilibrium with its surroundings, since there appear to be no sources of pressure in the central regions of the cloud that could support the shell against gravity and prevent its inward implosion. The timescale for the inward collapse of the ring would be less than 2 x 10(5) yr, suggesting that this globule is in an extremely early stage of evolution, and is perhaps being caught in the process of forming a centrally condensed dense core or Bok globule. Outside its central regions, the globule displays a well-behaved density profile whose shape is very similar to that of a stable Bonnor-Ebert sphere. Using the Swedish ESO Submillimeter Telescope, we also obtained a (CO)-O-18 spectrum toward the center of the cloud. The CO observation indicates that the globule is a gravitationally bound object. Analysis of the CO line profile reveals significant nonthermal gas motions likely due to turbulence. As a whole, the globule may be evolving to a global state of quasi-static dynamical equilibrium in which thermal and turbulent pressure balance gravity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tennessee, Dept Geol Geog & Phys, Martin, TN 38238 USA. European So Observ, D-8046 Garching, Germany. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu; thuard@cfa.harvard.edu; lcrews@utm.edu; jalves@eso.org OI Alves, Joao/0000-0002-4355-0921 NR 36 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 303 EP 312 DI 10.1086/421517 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700028 ER PT J AU Park, SQ Miller, JM McClintock, JE Remillard, RA Orosz, JA Shrader, CR Hunstead, RW Campbell-Wilson, D Ishwara-Chandra, CH Rao, AP Rupen, MP AF Park, SQ Miller, JM McClintock, JE Remillard, RA Orosz, JA Shrader, CR Hunstead, RW Campbell-Wilson, D Ishwara-Chandra, CH Rao, AP Rupen, MP TI Spectral and timing evolution of the black hole x-ray Nova 4U 1543-47 during its 2002 outburst SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; black hole physics; stars : individual (IL Lupi, 4U 1543-47); X-rays : stars ID TRANSIENT GRO J1655-40; ACTIVE GALACTIC NUCLEI; NOVA XTE J1550-564; 4U 1543-47; EMISSION-LINE; IRON LINES; REFLECTION; MODEL; RADIO; DISK AB We present an X-ray spectral and timing analysis of 4U 1543-47 during its 2002 outburst based on 49 pointed observations obtained using the Rossi X-Ray Timing Explorer. The outburst reached a peak intensity of 4.2 crab in the 2-12 keV band and declined by a factor of 32 throughout the month-long observation. A 21.9 +/- 0.6 mJy radio flare was detected at 1026.75 MHz two days before the X-ray maximum; the radio source was also detected late in the outburst, after the X-ray source entered the "hard" state. The X-ray light curve exhibits the classic shape of a rapid rise and an exponential decay. The spectrum is soft and dominated by emission from the accretion disk. The continuum is fitted with a multicolor disk blackbody (kT(max) 1: 04 keV) and a power law (Gamma similar to 2.7). Midway through the decay phase, a strong low-frequency quasi-periodic oscillation (v = 7.3-8.1 Hz) was present for several days. The spectra feature a broad Fe Kalpha line that is asymmetric, suggesting that the line is due to relativistic broadening rather than Comptonization. Relativistic Laor models provide much better fits to the line than nonrelativistic Gaussian models, particularly near the beginning and end of our observations. The line fits yield estimates for the inner disk radius that are within 6R(g); this result and additional evidence indicates that this black hole may have a nonzero angular momentum. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Park, SQ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM spark@cfa.harvard.edu; jmmiller@cfa.harvard.edu; jem@cfa.harvard.edu; rr@space.mit.edu; orosz@zwartgat.sdsu.edu; shrader@grossc.gsfc.nasa.gov; rwh@physics.usyd.edu.au; dcw@physics.usyd.edu.au; ishwar@ncra.tifr.res.in; pramesh@ncra.tifr.res.in; mrupen@zia.aoc.nrao.edu NR 51 TC 55 Z9 55 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 378 EP 389 DI 10.1086/421511 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700036 ER PT J AU Hoogerwerf, R Brickhouse, NS Mauche, CW AF Hoogerwerf, R Brickhouse, NS Mauche, CW TI The radial velocity and mass of the white dwarf of EX Hydrae measured with Chandra SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars : individual (EX Hydrae); techniques : spectroscopic; X-rays : stars ID X-RAY OBSERVATIONS; LABORATORY MEASUREMENTS; SPECTROSCOPY; EMISSION; PHOTOMETRY; PARAMETERS; ACCRETION; SPECTRUM; DENSITY; HYA AB We present the first detection of orbital motion in the cataclysmic variable EX Hydrae based on X-ray data from Chandra. The large collecting area of the telescope and the high resolution of the HETG spectrometers allow for an unprecedented velocity accuracy of similar to15 km s(-1) in the X-ray wavelength regime. We find an emission line velocity amplitude of 58.2 +/- 3.7 km s(-1) and infer a white dwarf mass of 0.49 +/- 0.13 M-., in good agreement with previous studies using optical, ultraviolet, and far-ultraviolet data. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, MS 31,60 Garden St, Cambridge, MA 02138 USA. EM rhoogerwerf@cfa.harvard.edu; nbrickhouse@cfa.harvard.edu; mauche@cygnus.llnl.gov OI Brickhouse, Nancy/0000-0002-8704-4473 NR 29 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 411 EP 415 DI 10.1086/421389 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700039 ER PT J AU Zubko, V Li, D Lim, T Feuchtgruber, H Harwit, M AF Zubko, V Li, D Lim, T Feuchtgruber, H Harwit, M TI Observations of water vapor outflow from NML Cygnus SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; stars : individual (NML Cygni, VY Canis Majoris, W Hydrae); stars : mass loss; stars : winds, outflows ID VY CANIS MAJORIS; EVOLVED STARS; W-HYDRAE; INFRARED-EMISSION; PROPER MOTIONS; DUST SHELLS; MASS-LOSS; SPECTRUM; ENVELOPE; MASERS AB We report new observations of the far-infrared and submillimeter water vapor emission of NML Cygnus based on data gathered with the Infrared Space Observatory and the Submillimeter Wave Astronomy Satellite. We compare the emission from NML Cyg to that previously published for VY CMa and W Hya in an attempt to establish the validity of recently proposed models for the outflow from evolved stars. The data obtained support the contention by Ivezic & Elitzur that the atmospheres of evolved stars obey a set of scaling laws in which the optical depth of the outflow is the single most significant scaling parameter, affecting both the radiative transfer and the dynamics of the outflow. Specifically, we provide observations comparing the water vapor emission from NML Cyg, VY CMa, and W Hya and find, to the extent permitted by the quality of our data, that the results are in reasonable agreement with a model developed by Zubko & Elitzur. Using this model we derive a mass loss based on the dust opacities, spectral line fluxes, and outflow velocities of water vapor observed in the atmospheres of these oxygen-rich giants. For VY CMa and NML Cyg, we also obtain an estimate of the stellar mass. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Cornell Univ, Ithaca, NY 14853 USA. RP Zubko, V (reprint author), NASA, Goddard Space Flight Ctr, Code 913, Greenbelt, MD 20771 USA. NR 27 TC 11 Z9 11 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP 427 EP 435 DI 10.1086/421700 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838FU UT WOS:000222699700042 ER PT J AU Jimenez-Reyes, SJ Garcia, RA Chaplin, WJ Korzennik, SG AF Jimenez-Reyes, SJ Garcia, RA Chaplin, WJ Korzennik, SG TI On the spatial dependence of low-degree solar p-mode frequency shifts from full-disk and resolved-sun observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : activity; Sun : helioseismology ID GOLF; OSCILLATIONS; VELOCITY AB We have analyzed low angular degree (low-l) solar p-mode frequency shifts extracted from two types of observations, both made by instruments on board the ESA/ NASA Solar and Heliospheric Observatory satellite during a period that covers the rising phase of activity, cycle 23 ( 1995 - 2002). The first are full-disk (Sun-as-a-star) averages made in Doppler velocity by the Global Oscillations at Low Frequency spectrophotometer; the second are Doppler velocity observations made with high spatial resolution by the Michelson Doppler Imager. We compare the eigenfrequency shifts from both sets of data and find that they are consistent at the level of precision of the observations. Furthermore, the sizes of the shifts uncovered for different mode components are found to scale in proportion to the corresponding spherical harmonic components of the observed line-of-sight surface magnetic field, with the sectoral mode components showing (as expected) the largest shifts. C1 Inst Astrofis Canarias, Tenerife 38205, Spain. Ctr Etud Saclay, CEA, DSM, DAPNIA,SAp, F-91191 Gif Sur Yvette, France. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jimenez-Reyes, SJ (reprint author), Inst Astrofis Canarias, Tenerife 38205, Spain. OI Jimenez Reyes, Sebastian/0000-0002-0317-4247; Garcia, Rafael/0000-0002-8854-3776 NR 8 TC 16 Z9 16 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP L65 EP L68 DI 10.1086/423174 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GM UT WOS:000222701500017 ER PT J AU Romani, RW Sowards-Emmerd, D Greenhill, L Michelson, P AF Romani, RW Sowards-Emmerd, D Greenhill, L Michelson, P TI Q0906+6930: The highest redshift blazar SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : general ID HOBBY-EBERLY TELESCOPE; X-RAY JETS; QUASAR GB-1508+5714; CHANDRA; SKY AB We report the discovery of a radio-loud flat-spectrum QSO at z = 5.47 with properties similar to those of the EGRET gamma-ray blazars. This source is the brightest radio QSO at z > 5, with a parsec-scale radio jet and a black hole mass estimate greater than or similar to 10(10) M-.. It appears to be the most distant blazar discovered to date. High-energy observations of this source can provide powerful probes of the background radiation in the early universe. C1 Stanford Univ, Dept Phys, Stanford, CA 94305 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romani, RW (reprint author), Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM rwr@astro.stanford.edu; dse@darkmatter.stanford.edu; lincoln@cfa.harvard.edu; peterm@stanford.edu NR 15 TC 33 Z9 33 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2004 VL 610 IS 1 BP L9 EP L11 DI 10.1086/423201 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GM UT WOS:000222701500003 ER PT J AU Guainazzi, M Siemiginowska, A Rodriguez-Pascual, P Stanghellini, C AF Guainazzi, M Siemiginowska, A Rodriguez-Pascual, P Stanghellini, C TI XMM-newton discovery of a compton-thick AGN in the GPS galaxy Mkn 668 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : individual : Mkn 668; galaxies : jets; galaxies : nuclei; galaxies : Seyfert; X-ray : galaxies ID ACTIVE GALACTIC NUCLEI; COMPACT STEEP-SPECTRUM; X-RAY-SPECTRA; WATER MASER EMISSION; SEYFERT 2 GALAXIES; RADIO-SOURCES; ASCA OBSERVATIONS; INFRARED PROPERTIES; CHANDRA DISCOVERY; CIRCINUS GALAXY AB We report the XMM-Newton discovery of the first Compton-thick obscured AGN in a Broad Line Radio Galaxy, the Gigahertz Peaked-Spectrum source Mkn 668 (OQ+208). The remarkably flat 2-10 keV X-ray spectrum (observed photon index, Gamma similar or equal to 0.7), with a prominent iron K-alpha fluorescent emission line, is a clear signature of a Compton-reflection dominated spectrum. Mkn 688 represents a remarkable example of discrepancy between X-ray spectral properties and optical classification, as its optical spectrum is characterized by broad and asymmetric Balmer lines. The obscuring matter is constrained to be located within the radio hotspots, in turn separated by about 10 pc. If the jets are piercing their way through a Compton-thick medium pervading the nuclear environment, one could be largely underestimating the radio activity dynamical age determined from the observed hotspot recession velocity. The soft X-ray spectrum is dominated by a much steeper component, which may be due to nuclear continuum electron scattering, or inverse Compton of the - remarkably large - far infrared emission. Soft X-rays are suppressed by a further Compton-thin (N-H similar to 10(21) cm(-2)) absorbing system, that we identify with matter responsible for free-free absorption of the radio lobes. C1 ESA, VILSPA, XMM, Newton Sci Operat Ctr, Madrid 28080, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist Radioastron, Noto, Italy. RP ESA, VILSPA, XMM, Newton Sci Operat Ctr, Apartado 50727, Madrid 28080, Spain. EM mguainaz@xmm.vilspa.esa.es OI Stanghellini, Carlo/0000-0002-6415-854X NR 83 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL 11 PY 2004 VL 421 IS 2 BP 461 EP 471 DI 10.1051/0004-6361:20047051 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840YY UT WOS:000222897700011 ER PT J AU Landt, H Padovani, P Perlman, ES Giommi, P AF Landt, H Padovani, P Perlman, ES Giommi, P TI A physical classification scheme for blazars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; BL Lacertae objects : general; quasars : emission lines ID BL-LACERTAE OBJECTS; ACTIVE GALACTIC NUCLEI; RILEY-I GALAXIES; RADIO-SOURCE IDENTIFICATIONS; OPTICAL CONTINUUM EMISSION; COMPLETE SAMPLE; PARENT POPULATION; SPECTRAL PROPERTIES; ASTRONOMICAL DATA; ACCRETION DISKS AB Blazars are currently separated into BL Lacertae objects (BL Lacs) and flat spectrum radio quasars based on the strength of their emission lines. This is performed rather arbitrarily by defining a diagonal line in the Ca H&K break value-equivalent width plane, following March (a) over tilde et al. We readdress this problem and put the classification scheme for blazars on firm physical grounds. We study similar to100 blazars and radio galaxies from the Deep X-ray Radio Blazar Survey (DXRBS) and 2-Jy radio survey and find a significant bimodality for the narrow emission line [O III] lambda5007. This suggests the presence of two physically distinct classes of radio-loud active galactic nuclei (AGN). We show that all radio-loud AGN, blazars and radio galaxies, can be effectively separated into weak- and strong-lined sources using the [O III] lambda5007-[O II] lambda3727 equivalent width plane. This plane allows one to disentangle orientation effects from intrinsic variations in radio-loud AGN. Based on DXRBS, the strongly beamed sources of the new class of weak-lined radio-loud AGN are made up of BL Lacs at the similar to75 per cent level, whereas those of the strong-lined radio-loud AGN include mostly (similar to97 per cent) quasars. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Hamburger Sternwarte, D-21029 Hamburg, Germany. Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. ASI Sci Data Ctr, ESRIN, I-00044 Frascati, Italy. European Space Agcy, Estec, Space Telescope Div, NL-2200 AG Noordwijk, Netherlands. RP Landt, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hlandt@cfa.harvard.edu OI giommi, paolo/0000-0002-2265-5003; Padovani, Paolo/0000-0002-4707-6841; Perlman, Eric/0000-0002-3099-1664 NR 60 TC 36 Z9 36 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 JUL 11 PY 2004 VL 351 IS 1 BP 83 EP 100 DI 10.1111/j.1365-2966.2004.07750.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831GY UT WOS:000222184100013 ER PT J AU Marconi, A Risaliti, G Gilli, R Hunt, LK Maiolino, R Salvati, M AF Marconi, A Risaliti, G Gilli, R Hunt, LK Maiolino, R Salvati, M TI Local supermassive black holes, relics of active galactic nuclei and the X-ray background SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE black hole physics; galaxies : active; galaxies : evolution; galaxies : nuclei; quasars : general; cosmology : miscellaneous ID DIGITAL SKY SURVEY; EARLY-TYPE GALAXIES; QUASI-STELLAR OBJECTS; LUMINOSITY FUNCTION; VELOCITY DISPERSION; REDSHIFT SURVEY; OBSERVATIONAL CONSTRAINTS; ULTRAVIOLET LUMINOSITY; COSMOLOGICAL EVOLUTION; COMPTON REFLECTION AB We quantify the importance of mass accretion during active galactic nuclei (AGN) phases in the growth of supermassive black holes (BHs) by comparing the mass function of black holes in the Local Universe with that expected from AGN relics, which are black holes grown entirely with mass accretion during AGN phases. The local BH mass function (BHMF) is estimated by applying the well-known correlations between BH mass, bulge luminosity and stellar velocity dispersion to galaxy luminosity and velocity functions. We find that different correlations provide the same BHMF only if they have the same intrinsic dispersion. The density of supermassive black holes in the Local Universe that we estimate is PBH = 4.6(-1.4)(+1-9)h(0.7)(2) x 10(5) M(circle dot) Mpc(-3). The relic BHMF is derived from the continuity equation with the only assumption that AGN activity is due to accretion on to massive BHs and that merging is not important. We find that the relic BHMF at z = 0 is generated mainly at z < 3 where the major part of the growth of a BH takes place. Moreover, BH growth is antihierarchical in the sense that smaller BHs (M(BH) < 10(7) M(circle dot)) grow at lower redshifts (z < 1) with respect to more massive ones (z similar to 1-3). Unlike previous work, we find that the BHMF of AGN relics is perfectly consistent with the local BHMF, indicating that local BHs were mainly grown during AGN activity. This agreement. is obtained while satisfying, at the same time, the constraints imposed from the X-ray background (XRB). The comparison between the local and relic BHMFs also suggests that the merging process is not important in shaping the relic BHMF, at least at low redshifts (z < 3), and allows us to estimate the average radiative efficiency (epsilon), the ratio between emitted and Eddington luminosity (lambda) and the average lifetime of active BHs. Our analysis thus suggests the following scenario: local BHs grew during AGN phases in which accreting matter was converted into radiation with efficiencies epsilon = 0.04-0.16 and emitted at a fraction lambda = 0.1-1.7 of the Eddington luminosity. The average total lifetime of these active phases ranges from similar or equal to 4.5 x 10(8) yr for M(BH) < 10(8) M(circle dot) to similar or equal to 1.5 x 10(8) yr for M(BH) > 10(9) M(circle dot), but can become as large as similar to10(9) yr for the lowest acceptable epsilon and lambda values. C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ist Radioastron, INAF, I-50125 Florence, Italy. RP Marconi, A (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM marconi@arcetri.astro.it RI Marconi, Alessandro/C-5880-2009; Gilli, Roberto/P-1110-2015; OI Hunt, Leslie/0000-0001-9162-2371; Marconi, Alessandro/0000-0002-9889-4238; Gilli, Roberto/0000-0001-8121-6177; Risaliti, Guido/0000-0002-3556-977X NR 114 TC 822 Z9 823 U1 1 U2 9 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 JUL 11 PY 2004 VL 351 IS 1 BP 169 EP 185 DI 10.1111/j.1365-2966.2004.07765.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831GY UT WOS:000222184100022 ER PT J AU Kim, E Lee, HM Spurzem, R AF Kim, E Lee, HM Spurzem, R TI Dynamical evolution of rotating stellar systems - III. The effect of the mass spectrum SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stellar dynamics; celestial mechanics; globular clusters : general ID FOKKER-PLANCK MODELS; ANISOTROPIC VELOCITY DISTRIBUTIONS; GLOBULAR STAR-CLUSTERS; COLLAPSE EVOLUTION; POST-COLLAPSE; PRE-COLLAPSE; M15 AB We have studied the dynamical evolution of rotating star clusters with mass spectrum using a Fokker-Planck code. As the simplest multimass model, we first investigated two-component clusters. Rotation is found to accelerate the dynamical evolution through the transfer of angular momentum outward, as well as from high masses to low masses. However, the degree of acceleration depends sensitively on the assumed initial mass function since dynamical friction, which generates mass segregation, also tends to accelerate the evolution, and the combined effect of both is not linear or multiplicative. As long as dynamical friction dominates in the competition with angular momentum exchange, the heavy masses lose random energy and angular momentum and sink towards the centre, but their remaining angular momentum is sufficient to speed them up rotationally. This is gravo-gyro instability. As a consequence, we find that the high-mass stars in the central parts rotate faster than low-mass stars. This leads to the suppression of mass segregation compared with the non-rotating clusters. From the study of multicomponent models, we observe similar trends to the two-component models in almost all aspects. The mass function changes less drastically for clusters with rotation. Unlike non-rotating clusters, the mass function depends on R and z. Our models are the only ones that can predict mass function and other quantities to be compared with new observations. C1 Seoul Natl Univ, Astron Program, SEES, Seoul 151742, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Astron Rech Inst, D-69120 Heidelberg, Germany. RP Kim, E (reprint author), Seoul Natl Univ, Astron Program, SEES, Seoul 151742, South Korea. EM ekim@cfa.harvard.edu; hmlee@astro.snu.ac.kr; spurzem@ari.uni-heidelberg.de NR 33 TC 27 Z9 27 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 JUL 11 PY 2004 VL 351 IS 1 BP 220 EP 236 DI 10.1111/j.1365-2966.2004.07776.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831GY UT WOS:000222184100027 ER PT J AU Tarchi, A Greve, A Peck, AB Neininger, N Wills, KA Pedlar, A Klein, U AF Tarchi, A Greve, A Peck, AB Neininger, N Wills, KA Pedlar, A Klein, U TI Neutral hydrogen absorption at the centre of NGC 2146 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual : NGC 2146; galaxies : ISM; galaxies : kinematics and dynamics; galaxies : starburst; radio lines : galaxies ID SPIRAL GALAXY NGC2146; STAR-FORMATION; NGC 2146; STARBURST; MERLIN; M82; GAS; VLA AB We present 1.4-GHz H I absorption line observations towards the starburst in NGC 2146, made with the Very Large Array and the Multi-Element Radio-Linked Interferometer Network. The H I gas has a rotating disc/ring structure with column densities between 6 and 18 x 10(21) atom cm(-2). The H I absorption has a uniform spatial and velocity distribution, and does not reveal any anomalous material concentration or velocity in the central region of the galaxy which might indicate an encounter with another galaxy or a far-evolved merger. We conclude that the signs of an encounter causing the starburst should be searched for in the outer regions of the galaxy. C1 CNR, Inst Radioastron, I-40129 Bologna, Italy. Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96721 USA. Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. RP Tarchi, A (reprint author), CNR, Inst Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. EM a.tarchi@ira.cnr.it OI Tarchi, Andrea/0000-0001-8540-3500 NR 26 TC 8 Z9 8 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2004 VL 351 IS 1 BP 339 EP 346 DI 10.1111/j.1365-2966.2004.07792.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831GY UT WOS:000222184100039 ER PT J AU Jonker, PG Gallo, E Dhawan, V Rupen, M Fender, RP Dubus, G AF Jonker, PG Gallo, E Dhawan, V Rupen, M Fender, RP Dubus, G TI Radio and X-ray observations during the outburst decay of the black hole candidate XTE J1908+094 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; stars : individual : XTE J1908+094; X-rays : stars ID LOW/HARD STATE; JET; BINARIES; QUIESCENCE; CHANDRA; SPECTRA; NOVAE AB Obtaining simultaneous radio and X-ray data during the outburst decay of soft X-ray transients is a potentially important tool to study the disc-jet connection. Here we report results of the analysis of (nearly) simultaneous radio [Very Large Array (VLA) or Westerbork Synthesis Radio Telescopes (WSRT)] and Chandra X-ray observations of XTE J1908 + 094 during the last part of the decay of the source after an outburst. The limit on the index of a radio-X-ray correlation that we find is consistent with the value of similar to0.7 found for other black hole candidates in the low/hard state. Interestingly, the limit that we find seems more consistent with a value of 1.4, which was recently shown to be typical for radiatively efficient accretion flow models. We further show that, when the correlation index is the same for two sources, one can use the differences in normalization in the radio-X-ray flux correlation to estimate the distance towards the sources if the distance of one of them is accurately known (assuming black hole spin and mass and jet Lorentz factor differences are unimportant or minimal). Finally, we observed a strong increase in the rate of decay of the X-ray flux. Between 2003 March 23 and April 19, the X-ray flux decayed by a factor similar to5, whereas between 2003 April 19 and May 13, the X-ray flux decreased by a factor similar to750. The source (0.5-10 keV) luminosity at the last Chandra observation was L approximate to 3 x 10(32) (d/8.5 kpc)(2) ergs(-1). C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Natl Radio Astron Observ, Socorro, NM 87801 USA. Ecole Polytech, Lab Leprince Ringuet, F-91128 Palaiseau, France. RP Jonker, PG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS83, Cambridge, MA 02138 USA. EM pjonker@cfa.harvard.edu NR 32 TC 29 Z9 29 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2004 VL 351 IS 4 BP 1359 EP 1364 DI 10.1111/j.1365-2966.2004.07873.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 834PQ UT WOS:000222423400022 ER PT J AU Di Stefano, R Kong, AKH AF Di Stefano, R Kong, AKH TI The discovery of quasi-soft and supersoft sources in external galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : individual (M51, M83, M101, NGC 4697); supernova remnants; white dwarfs; X-rays : binaries; X-rays : galaxies ID X-RAY SOURCES; SUPERNOVA-REMNANTS; SOURCE POPULATION; SPIRAL GALAXIES; BLACK-HOLE; CHANDRA; M101; MASS; EMISSION; BINARIES AB We apply a uniform procedure to select very soft sources from point sources observed by Chandra in four galaxies. This sample includes one elliptical galaxy (NGC 4967), two face-on spiral galaxies (M101 and M83), and an interacting galaxy (M51). We report on some intriguing results, including the following: 1. We have found very soft X-ray sources (VSSs) in every galaxy. Some of these fit the criteria for canonical supersoft sources (SSSs), while others are somewhat harder. These latter have characteristic values of kT less than or similar to 300 eV; we refer to them as quasi-soft sources (QSSs). We found a combined total of 149 VSSs in the four galaxies we considered; 77 were SSSs and 72 were QSSs. 2. The data are consistent with the existence of a large VSS population, most of whose members we cannot observe because of the effects of distance and obscuration. The total VSS population of sources with L > 10(37) ergs s(-1) in each galaxy could be on the order of 1000. 3. Whereas in M31 only similar to10% of all X-ray sources detected by Chandra are VSSs, more than 35% of all detectable X-ray sources in the face-on galaxy M101 fit the phenomenological definition of VSSs. This difference may be due to differences in N-H between typical lines of sight to sources in each galaxy. 4. SSSs can be super-Eddington for Chandrasekhar-mass objects. 5. We find evidence for SSSs and QSSs with luminosities of 10(36) ergs s(-1) < L < 10(37) ergs s(-1). These sources have luminosities lower than those of the similar to30 soft sources used to establish the class of SSSs. 6. In the spiral galaxies M101, M83, and M51, a large fraction of the SSSs and QSSs appear to be associated with the spiral arms. This may indicate that some SSSs are young systems, possibly younger than 10(8) yr. 7. In addition to finding hot white dwarfs and soft X-ray binaries, our method should also be efficient at selecting supernova remnants (SNRs). A small fraction of the VSSs in the spiral arms of M101 appear to be associated with SNRs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 47 TC 46 Z9 46 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 710 EP 727 DI 10.1086/421318 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200019 ER PT J AU Miller, JM Zezas, A Fabbiano, G Schweizer, F AF Miller, JM Zezas, A Fabbiano, G Schweizer, F TI XMM-Newton spectroscopy of four bright ultraluminous X-ray sources in the Antennae galaxies (NGC 4038/4039) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038/4039); X-rays : galaxies ID MASS BLACK-HOLES; CHANDRA OBSERVATIONS; SOURCE POPULATION; SPIRAL GALAXIES; CYGNUS X-1; DISCOVERY; SPECTRUM; TRANSITIONS; IC-342; STATE AB We report the results of spectral fits to four bright ultraluminous X-ray sources (ULXs) in the Antennae galaxies (NGC 4038/4039) observed for 41 ks with XMM-Newton. Although emission regions are not resolved as well as in prior Chandra observations, at least four ULXs (X-11, X-16, X-37, and X-44 in the Zezas and Fabbiano scheme) are sufficiently bright and well separated with XMM-Newton that reliable extractions and spectral analyses are possible. We find that the single-component multicolor disk blackbody models cannot describe any of the spectra. Sources X-11 and X-16 are acceptably fitted with simple power-law models. A thermal bremsstrahlung model provides a better fit to the spectrum of X-44. Including a disk blackbody component to the spectrum of X-37 improves the fit and reveals an apparently cool disk (kT = 0.13 +/- 0.02 keV). This would suggest a parallel to cool disks recently found in other very luminous ULXs, which may contain intermediate-mass black holes; however, the complex diffuse emission of the Antennae demands that this finding be regarded cautiously. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Observ, Pasadena, CA 91101 USA. RP Miller, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jmmiller@head-cfa.harvard.edu RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 42 TC 18 Z9 18 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 728 EP 734 DI 10.1086/421098 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200020 ER PT J AU Williams, BF Garcia, MR Kong, AKH Primini, FA King, AR Di Stefano, R Murray, SS AF Williams, BF Garcia, MR Kong, AKH Primini, FA King, AR Di Stefano, R Murray, SS TI A synoptic X-ray study of M31 with the Chandra High Resolution Camera SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : individual (M31); galaxies : spiral; X-rays : binaries; X-rays : galaxies; X-rays : general ID ROSAT PSPC SURVEY; BLACK-HOLE; STELLAR POPULATIONS; INTERSTELLAR-MEDIUM; GLOBULAR-CLUSTERS; ANDROMEDA GALAXY; CENTRAL REGION; POINT SOURCES; XMM-NEWTON; SUPERNOVA-REMNANTS AB We have obtained 17 epochs of Chandra High Resolution Camera (HRC) snapshot images, each covering most of the M31 disk. The data cover a total baseline of similar to2.5 yr and contain a mean effective exposure of 17 ks. We have measured the mean fluxes and long-term light curves for 166 objects detected in these data. At least 25% of the sources show significant variability. The cumulative luminosity function (CLF) of the disk sources is well fitted by a power law with a slope comparable to those observed in typical elliptical galaxies. The CLF of the bulge is a broken power law similar to measurements made by previous surveys. We note several sources in the southwestern disk with L-X > 10(37) ergs s(-1). We cross-correlate all of our sources with published optical and radio catalogs, as well as new optical data, finding counterpart candidates for 55 sources. In addition, 17 sources are likely X-ray transients. We analyze follow-up Hubble Space Telescope (HST) WFPC2 data of two X-ray transients, finding F336W (U-band equivalent) counterparts. In both cases, the counterparts are variable. In one case, the optical counterpart is transient with F336W = 22.3 +/- 0.1 mag. The X-ray and optical properties of this object are consistent with a similar to10 M. black hole X-ray nova with an orbital period of 23(-16)(+54) days. In the other case, the optical counterpart varies between F336W = 20.82 +/- 0.06 and 21.11 +/- 0.02 mag. Ground-based and HST observations show that this object is bright (V = 18.8 +/- 0.1) and slightly extended. Finally, the frequency of bright X-ray transients in the M31 bulge suggests that the ratio of neutron star to black hole primaries in low-mass X-ray binaries (NS/BH) is similar to1. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM williams@head-cfa.harvard.edu; garcia@head-cfa.harvard.edu; akong@head-cfa.harvard.edu; fap@head-cfa.harvard.edu; ark@astro.le.ac.uk; rd@head-cfa.harvard.edu; ssm@head-cfa.harvard.edu OI Primini, Francis/0000-0002-6077-0643 NR 104 TC 55 Z9 55 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 JUL 10 PY 2004 VL 609 IS 2 BP 735 EP 754 DI 10.1086/421315 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200021 ER PT J AU Bassa, C Pooley, D Homer, L Verbunt, F Gaensler, BM Lewin, WHG Anderson, SF Margon, B Kaspi, VM van der Klis, M AF Bassa, C Pooley, D Homer, L Verbunt, F Gaensler, BM Lewin, WHG Anderson, SF Margon, B Kaspi, VM van der Klis, M TI X-ray sources and their optical counterparts in the globular cluster M4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; globular clusters : general; globular clusters : individual (M4, NGC 6121); novae, cataclysmic variables; X-rays : stars ID SPACE-TELESCOPE COUNTERPARTS; ALL-SKY SURVEY; LUMINOSITY FUNCTION; MILLISECOND PULSAR; ROSAT OBSERVATIONS; EXTENSIVE CENSUS; WHITE-DWARFS; 47 TUCANAE; BINARY; PHOTOMETRY AB We report on the Chandra X-Ray Observatory ACIS-S3 imaging observation of the Galactic globular cluster M4 (NGC 6121). We detect 12 X-ray sources inside the core and 19 more within the cluster half-mass radius. The limiting luminosity of this observation is L-X approximate to 10(29) ergs s(-1) for sources associated with the cluster, the deepest X-ray observation of a globular cluster to date. We identify six X-ray sources with known objects and use ROSAT observations to show that the brightest X-ray source is variable. Archival data from the Hubble Space Telescope allow us to identify optical counterparts to 16 X-ray sources. Based on the X-ray and optical properties of the identifications and the information from the literature, we classify two (possibly three) sources as cataclysmic variables, one X-ray source as a millisecond pulsar, and 12 sources as chromospherically active binaries. Comparison of M4 with 47 Tuc and NGC 6397 suggests a scaling of the number of active binaries in these clusters with the cluster (core) mass. C1 Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Bassa, C (reprint author), Univ Utrecht, Astron Inst, POB 80 000, NL-3508 TA Utrecht, Netherlands. EM c.g.bassa@astro.uu.nl; davep@space.mit.edu; homer@astro.washington.edu; f.w.m.verbunt@astro.uu.nl; bgaensler@cfa.harvard.edu; lewin@space.mit.edu; anderson@washington.edu; margon@stsci.edu; vkaspi@hep.physics.mcgill.ca; michel@science.uva.nl RI Gaensler, Bryan/F-8655-2010; Margon, Bruce/B-5913-2012; OI Gaensler, Bryan/0000-0002-3382-9558 NR 47 TC 52 Z9 52 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 755 EP 765 DI 10.1086/421259 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200022 ER PT J AU Haverkorn, M Gaensler, BM McClure-Griffiths, NM Dickey, JM Green, AJ AF Haverkorn, M Gaensler, BM McClure-Griffiths, NM Dickey, JM Green, AJ TI Magnetic fields and ionized gas in the inner Galaxy: An outer scale for turbulence and the possible role of HII regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : structure; HII regions; ISM : structure; radio continuum : ISM; techniques : polarimetric; turbulence ID EXTRAGALACTIC RADIO-SOURCES; ROTATION MEASURE VARIATIONS; GALACTIC PLANE SURVEY; H-II REGIONS; INTERSTELLAR-MEDIUM; MAGNETOHYDRODYNAMIC TURBULENCE; ALFVENIC TURBULENCE; POWER SPECTRUM; 350 MHZ; SIMULATIONS AB We present an analysis of rotation measure (RM) fluctuations from the test region of the Southern Galactic Plane Survey (SGPS), along with emission measure (EM) fluctuations in the same field taken from the Southern Halpha Sky Survey Atlas. The structure function of RM fluctuations shows a relatively steep slope at small scales (1'-5'), a break in slope to a flatter structure function at intermediate scales (5'-60'), and a systematic variation of the strength of fluctuations as a function of position angle on the sky at the largest scales (60'-200'). The structure function of EM fluctuations shows similar behavior, although the lower resolution of the data prevents detection of a possible break in the spectrum. We interpret the anisotropy in RM/EM structure on large scales as resulting from a large-scale gradient in electron density (and possibly magnetic field) across the region. The break in the slope of the RM structure function at scales of similar to5' can be explained by contributions from two spatially distinct magnetoionized screens, most likely in the Local and Carina spiral arms. The observed structure function then implies that the outer scale of RM fluctuations in these screens is similar to2 pc. Such behavior is in striking contrast to the expectation that interstellar turbulence forms an unbroken spectrum from kiloparsec down to AU scales. We conclude that we have identified an additional source of enhanced turbulence, injected on scales of a few pc, possibly seen only in the Galactic plane. The most likely source of such turbulence is individual H II regions from relatively low mass stars, whose characteristic scale size is similar to the outer scale of turbulence inferred here. These sources may be the dominant source of density and velocity fluctuations in warm ionized gas in the Galactic plane. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP Haverkorn, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mhaverkorn@cfa.harvard.edu; bgaensler@cfa.harvard.edu; naomi.mcclure-griffiths@csiro.au; john@astro.umn.edu; agreen@physics.usyd.edu.au RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Dickey, John/0000-0002-6300-7459; Gaensler, Bryan/0000-0002-3382-9558 NR 49 TC 37 Z9 37 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 776 EP 784 DI 10.1086/421341 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200024 ER PT J AU Mohanty, S Basri, G Jayawardhana, R Allard, F Hauschildt, P Ardila, D AF Mohanty, S Basri, G Jayawardhana, R Allard, F Hauschildt, P Ardila, D TI Measuring fundamental parameters of substellar objects. I. Surface gravities SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : profiles; open clusters and associations : individual (Upper Scorpius, Taurus-Auriga); stars : fundamental parameters; stars : low-mass, brown dwarfs; stars : pre-main-sequence; techniques : spectroscopic ID LOW-MASS STARS; MAIN-SEQUENCE STARS; YOUNG BROWN DWARFS; SPECTRAL ENERGY-DISTRIBUTIONS; EXTRASOLAR GIANT PLANETS; SCORPIUS OB ASSOCIATION; NEAR-INFRARED SPECTRA; KECK HIRES SPECTRA; EVOLUTIONARY MODELS; DISK ACCRETION AB We present an analysis of high-resolution optical spectra for a sample of very young, mid- to late-M, low-mass stellar and substellar objects: 11 in the Upper Scorpius association, and two (GG Tau Ba and Bb) in the Taurus star-forming region. Effective temperatures and surface gravities are derived from a multiple-feature spectral analysis using TiO, Na I, and K I, through comparison with the latest synthetic spectra. We show that these spectral diagnostics complement each other, removing degeneracies with temperature and gravity in the behavior of each. In combination, they allow us to determine temperature to within 50 K and gravity to within 0.25 dex, in very cool young objects. Our high-resolution spectral analysis does not require extinction estimates. Moreover, it yields temperatures and gravities independent of theoretical evolutionary models ( although our estimates do depend on the synthetic spectral modeling). We find that our gravities for most of the sample agree remarkably well with the isochrone predictions for the likely cluster ages. However, discrepancies appear in our coolest targets: these appear to have significantly lower gravity ( by up to 0.75 dex) than our hotter objects, even though our entire sample covers a relatively narrow range in effective temperature ( similar to 300 K). This drop in gravity is also implied by intercomparisons of the data alone, without recourse to synthetic spectra. We consider, and argue against, dust opacity, cool stellar spots, or metallicity differences leading to the observed spectral effects; a real decline in gravity is strongly indicated. Such gravity variations are contrary to the predictions of the evolutionary tracks, causing improbably low ages to be inferred from the tracks for our coolest targets. Through a simple consideration of contraction timescales, we quantify the age errors introduced into the tracks through the particular choice of initial conditions and demonstrate that they can be significant for low-mass objects that are only a few megayears old. However, we also find that these errors appear insufficient to explain the magnitude of the age offsets in our lowest gravity targets. We venture that this apparent age offset may arise from evolutionary model uncertainties related to accretion, deuterium burning and/or convection effects. Finally, when combined with photometry and distance information, our technique for deriving surface gravities and effective temperatures provides a way of obtaining masses and radii for substellar objects independent of evolutionary models; radius and mass determinations are presented in Paper II. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Ecole Normale Super Lyon, CRAL, F-69364 Lyon, France. Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. Johns Hopkins Univ, Bloomberg Ctr Phys & Astron, Baltimore, MD 21218 USA. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smohanty@cfa.harvard.edu; basri@soleil.berkeley.edu; rayjay@astro.lsa.umich.edu; fallard@ens-lyon.fr; phauschildt@hs.uni-hamburg.de; ardila@adcam.pha.jhu.edu OI Allard, France/0000-0003-1929-9340 NR 71 TC 59 Z9 59 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 854 EP 884 DI 10.1086/420923 PN 1 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200030 ER PT J AU Mohanty, S Jayawardhana, R Basri, G AF Mohanty, S Jayawardhana, R Basri, G TI Measuring fundamental parameters of substellar objects. II. Masses and radii SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : formation; stars : fundamental parameters; stars : low-mass, brown dwarfs; stars : pre-main-sequence; techniques : spectroscopic ID YOUNG BROWN DWARFS; SCORPIUS OB ASSOCIATION; EVOLUTIONARY MODELS; MAIN-SEQUENCE; ECLIPSING BINARY; DISK ACCRETION; TAURUS-AURIGA; STARS; ATMOSPHERES; DISCOVERY AB We present mass and radius derivations for a sample of very young, mid- to late-M, low-mass stellar and substellar objects in Upper Scorpius and Taurus. In a previous paper we determined effective temperatures and surface gravities for these targets from an analysis of their high-resolution optical spectra and comparisons to the latest synthetic spectra. We now derive extinctions, radii, masses, and luminosities by combining our previous results with observed photometry, surface fluxes from the synthetic spectra, and the known cluster distances. These are the first mass and radius estimates for young, very low mass bodies that are independent of theoretical evolutionary models ( although our estimates do depend on spectral modeling). We find that for most of our sample, our derived mass-radius and mass-luminosity relationships are in very good agreement with the theoretical predictions. However, our results diverge from the evolutionary model values for the coolest, lowest mass targets: our inferred radii and luminosities are significantly larger than predicted for these objects at the likely cluster ages, causing them to appear much younger than expected. We suggest that uncertainties in the evolutionary models -e.g., in the choice of initial conditions and/or treatment of interior convection - may be responsible for this discrepancy. Finally, two of our late-M objects (USco 128 and 130) appear to have masses close to the deuterium-fusion boundary (similar to 9M(J) - 14M(J) within a factor of 2). This conclusion is primarily a consequence of their considerable faintness compared to other targets with similar extinction, spectral type, and temperature ( difference of similar to1 mag). Our result suggests that the faintest young late-M or cooler objects may be significantly lower in mass than current theoretical tracks indicate. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smohanty@cfa.harvard.edu; rayjay@umich.edu; basri@soleil.berkeley.edu NR 40 TC 54 Z9 54 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 885 EP 905 DI 10.1086/420924 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200031 ER PT J AU Hartmann, L Hinkle, K Calvet, N AF Hartmann, L Hinkle, K Calvet, N TI High-resolution near-infrared spectroscopy of FU Orionis objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared : stars; stars : formation; stars : pre-main-sequence ID Z-CANIS MAJORIS; PROTOSTELLAR DISK MODELS; SEQUENCE ACCRETION DISKS; MASS-LOSS; OBSERVATIONAL CONSTRAINTS; SPECTRUM; EVOLUTION; YOUNG; STAR; SPECTROGRAPH AB We present an analysis of recent near-infrared, high-resolution spectra of the variable FU Ori objects. During a phase of rapid fading in optical brightness during 1997, V1057 Cyg exhibited shell absorption in first-overtone (v" v' = 2-0) CO lines, blueshifted by about 50 km s(-1) from the system velocity. This shell component had not been seen previously, nor was it present in 1999, although some blueshifted absorption asymmetry is seen at the latter epoch. The appearance of this CO absorption shell is connected with the roughly contemporaneous appearance of blueshifted, low-excitation optical absorption lines with comparable low velocities; we suggest that this shell was also responsible for some of the peculiar emission features seen in red-optical spectra of V1057 Cyg. FU Ori continues to exhibit broad CO lines, with some evidence for the double-peaked profiles characteristic of an accretion disk; the line profiles are consistent with previous observations. Both FU Ori and V1057 Cyg continue to exhibit lower rotational broadening at 2.3 mum than at optical wavelengths, in agreement with the prediction of differentially rotating disk models; we have a marginal detection of the same effect in V1515 Cyg. The relative population of the first-overtone CO rotational levels in the FU Ori objects suggests low excitation temperatures. We compare disk models to the observations and find agreement with overall line strengths and rotational broadening, but the observed line profiles are generally less double-peaked than predicted. We suggest that the discrepancy in line profiles is due to turbulent motions in FU Ori disks, an effect qualitatively predicted by recent simulations of the magnetorotational instability in vertically stratified accretion disks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hartmann@cfa.harvard.edu; hinkle@noao.edu; ncalvet@cfa.harvard.edu NR 44 TC 37 Z9 37 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 906 EP 916 DI 10.1086/421317 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200032 ER PT J AU Luhman, KL Steeghs, D AF Luhman, KL Steeghs, D TI Spectroscopy of candidate members of the eta Chamaeleontis and MBM 12 young associations SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : emission-line, Be; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID LOW-MASS STARS; ORION NEBULA CLUSTER; T-TAURI STARS; BROWN DWARFS; FORMING REGION; EVOLUTIONARY MODELS; MOLECULAR CLOUD; MAIN-SEQUENCE; DISTANCE; BINARIES AB We present an analysis of candidate members of the eta Cha and MBM 12A young associations. For an area of 0.7 deg(2) toward eta Cha, we have performed a search for members of the association by combining JHK(s) photometry from the Two Micron All Sky Survey and i photometry from DENIS with follow-up optical spectroscopy at Magellan Observatory. We report the discovery of three new members with spectral types of M5.25-M5.75, corresponding to masses of 0.13 - 0.08 M-. by theoretical evolutionary models. Two and three of these members were found independently by Lyo and coworkers and Song and coworkers, respectively. Meanwhile, no brown dwarfs were detected in eta Cha down to the completeness limit of 0.015 M-.. For MBM 12A, we have obtained spectra of three of the remaining candidate members that lacked spectroscopy at the end of the survey by Luhman, all of which are found to be field M dwarfs. Ogura and coworkers have recently presented four "probable'' members of MBM 12A. However, two of these objects were previously classified as field dwarfs by the spectroscopy of Luhman. In this work, we find that the other two objects are field dwarfs as well. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu; dsteeghs@cfa.harvard.edu RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 38 TC 68 Z9 68 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 917 EP 924 DI 10.1086/421291 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200033 ER PT J AU Argiroffi, C Drake, JJ Maggio, A Peres, G Sciortino, S Harnden, FR AF Argiroffi, C Drake, JJ Maggio, A Peres, G Sciortino, S Harnden, FR TI High-resolution X-ray spectroscopy of the post-T Tauri star PZ Telescopii SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : abundances; stars : coronae; stars : individual (PZ Telescopii); stars : pre-main-sequence; techniques : spectroscopic; X-rays : stars ID EMISSION MEASURE DISTRIBUTIONS; YOUNG STELLAR OBJECTS; TEMPERATURE STRUCTURE; AB-DORADUS; EVOLUTIONARY STATUS; CORONAL ABUNDANCES; ACTIVE STARS; VARIABILITY; ASSOCIATION; ACCRETION AB We present an analysis of the Chandra High Energy Transmission Grating Spectrometer observation of the rapidly rotating (P-rot = 0.94 days) post-T Tauri (similar to20 Myr old) star PZ Telescopii, in the Tucana association. Using two different methods, we have derived the coronal emission measure distribution EM( T) and chemical abundances. The EM(T) peaks at log T = 6.9 and exhibits a significant emission measure at temperatures log T > 7. The coronal abundances are generally similar to0.5 times the solar photospheric values, which are presumed fairly representative of the composition of the underlying star. A minimum in abundance is seen at a first ionization potential (FIP) of 7 - 8 eV, with evidence for higher abundances at both lower and higher FIP, similar to patterns seen in other active stars. From an analysis of the He-like triplet of Mg xi, we have estimated electron densities of similar to 10(12) - 10(13) cm(-3). All the coronal properties found for PZ Tel are much more similar to those of AB Dor, which is slightly older than PZ Tel, than to those of the younger T Tauri star TW Hya. These results support earlier conclusions that the soft X-ray emission of TW Hya is likely dominated by accretion activity rather than by a magnetically heated corona. Our results also suggest that the coronae of pre - main- sequence stars rapidly become similar to those of older active main- sequence stars soon after the accretion stage has ended. C1 Univ Palermo, Sez Anat, Dipartimento Sci Fis & Astron, I-90134 Palermo, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. RP Univ Palermo, Sez Anat, Dipartimento Sci Fis & Astron, Piazza Parlamento 1, I-90134 Palermo, Italy. EM argi@astropa.unipa.it; jdrake@cfa.harvard.edu; maggio@astropa.unipa.it; peres@astropa.unipa.it; sciorti@astropa.unipa.it; frh@cfa.harvard.edu RI Maggio, Antonio/P-5700-2015; OI Maggio, Antonio/0000-0001-5154-6108; PERES, Giovanni/0000-0002-6033-8180; ARGIROFFI, Costanza/0000-0003-2073-1348 NR 49 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 925 EP 934 DI 10.1086/420692 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200034 ER PT J AU Torres, G Konacki, M Sasselov, DD Jha, S AF Torres, G Konacki, M Sasselov, DD Jha, S TI New data and improved parameters for the extrasolar transiting planet OGLE-TR-56b SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; planetary systems; stars : low-mass, brown dwarfs; techniques : radial velocities ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; RADIAL-VELOCITIES; HD 209458B; 51-PEG-LIKE PLANET; GALACTIC DISK; GIANT PLANETS; 2001 CAMPAIGN; PARENT STAR; ATMOSPHERE AB We report new spectroscopic observations with the Keck HIRES instrument of the recently discovered transiting planet OGLE-TR-56b. Our radial velocity measurements with errors of similar to100 m s(-1) show clear variations that are in excellent agreement with the phasing ( period and epoch) derived from the OGLE transit photometry. Careful analysis of the spectral line bisectors, along with numerical simulations of blend scenarios, supports the argument for the planetary nature of the companion. The new data, combined with measurements from the previous season, allow an improved determination of the mass of the planet, M-p = (1.45 +/- 0.23)M-Jup. All available OGLE photometry, including new measurements made during the 2003 season, have also been analyzed to derive an improved value for the planetary radius of R-p = (1.23 +/- 0.16)R-Jup. We discuss the implications of these results for the theory of extrasolar planets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. Polish Acad Sci, Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu; maciej@gps.caltech.edu; dsasselov@cfa.harvard.edu; saurabh@astron.berkeley.edu RI Konacki, Maciej/A-1220-2007 NR 32 TC 60 Z9 61 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 1071 EP 1075 DI 10.1086/421286 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200046 ER PT J AU Bensch, F Bergin, EA Bockelee-Morvan, D Melnick, GJ Biver, N AF Bensch, F Bergin, EA Bockelee-Morvan, D Melnick, GJ Biver, N TI Submillimeter Wave Astronomy Satellite monitoring of the postperihelion water production rate of comet C/1999 T1 (McNaught-Hartley) SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : general; comets : individual (C/1999 T1); radio lines : solar system; submillimeter ID H1 LEE; RADIO TELESCOPES; B2 HYAKUTAKE; ODIN; FLUORESCENCE; PHOTOMETRY; VAPOR; JCMT; IRAM AB We present observations of the pure rotational transition 1(10) --> 1(01) of ortho-H2O vapor at 556.936 GHz made with the Submillimeter Wave Astronomy Satellite (SWAS) for comet C/1999 T1 (McNaught-Hartley). The emission was monitored during the postperihelion phase from (UT) 2001 February 2.00 to 11.07 and February 23.01 to April 5.95 for a Sun-comet distance, r(h), ranging from 1.41 to 2.05 AU. The water production rate, Q(H2O), derived from the observations depends on the assumptions regarding the electron abundance in the coma. We obtain Q(H2O) similar to 4 x 10(28) s(-1) for the observations made in the first week of February (r(h) similar to 1.4 AU) using a model in which the electron abundance has been normalized to the in situ measurements obtained in 1P/Halley. The value of Q(H2O) decreases for larger r(h), and we derive similar to1.5 x 10(28) s(-1) for the observations made at r(h) similar to 2 AU in the last week of 2001 March. The inferred water production rate is larger by similar to40% for a radiative transfer model with the electron abundance reduced by 80% because of the reduced excitation of water by electron collisions in this model. A comparison to literature data suggests that the SWAS results derived with the smaller electron abundance are in better agreement with independent measurements of Q(H2O) obtained from observations of H2O photodissociation products. A chi(2) fit to the variation of Q(H2O) with the heliocentric distance gives a power-law index of similar to3.0 +/- 0.5 (statistical) +/-0.1 (systematic). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. RP Bensch, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 33 TC 11 Z9 11 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP 1164 EP 1169 DI 10.1086/421287 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835BZ UT WOS:000222456200055 ER PT J AU Abramowicz, MA Kluzniak, W McClintock, JE Remillard, RA AF Abramowicz, MA Kluzniak, W McClintock, JE Remillard, RA TI The importance of discovering a 3 : 2 twin-peak quasi-periodic oscillation in an ultraluminous x-ray source, or how to solve the puzzle of intermediate-mass black holes SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; quasars : general; relativity; X-rays : galaxies; X-rays : general ID ACCRETION DISKS; NEUTRON-STAR; BINARIES; FREQUENCIES; GALAXIES; DWARF AB Recently, twin-peak quasi-periodic oscillations (QPOs) have been observed in a 3 : 2 ratio for three Galactic black hole microquasars with frequencies that have been shown to scale as 1/M, as expected for general relativisitic motion near a black hole. It may be possible to extend this result to distinguish between the following two disparate models that have been proposed for the puzzling ultraluminous X-ray sources (ULXs): ( 1) an intermediate-mass black hole (M similar to 10(3) M-.) radiating very near the Eddington limit and (2) a conventional black hole (M similar to 10 M-.), accreting at a highly super-Eddington rate with its emission beamed along the rotation axis. We suggest that one could discriminate between these models by detecting the counterpart of a Galactic twin-peak QPO in a ULX: the expected frequency for the intermediate-mass black hole model is only about 1 Hz, whereas for the conventional black hole model the expected frequency would be the similar to 100 Hz value observed for the Galactic microquasars. C1 Chalmers Univ Technol, Sch Phys, S-41296 Gothenburg, Sweden. Zielona Gora Univ, Inst Astron, PL-65265 Zielona Gora, Poland. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Abramowicz, MA (reprint author), Chalmers Univ Technol, Sch Phys, S-41296 Gothenburg, Sweden. EM marek@fy.chalmers.se; wlodek@camk.edu.pl; jem@cfa.harvard.edu; rr@space.mit.edu NR 24 TC 41 Z9 41 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP L63 EP L65 DI 10.1086/422810 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835CA UT WOS:000222456300005 ER PT J AU Testa, P Drake, JJ Peres, G DeLuca, EE AF Testa, P Drake, JJ Peres, G DeLuca, EE TI Detection of X-ray resonance scattering in active stellar coronae SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; stars : coronae; stars : late-type; X-rays : stars ID II-PEGASI; OPTICALLY THIN; SOLAR CORONA; LINES; EMISSION; ABUNDANCES; OPACITY; PLASMAS; SPECTROSCOPY; PARAMETERS AB An analysis of Lyman series lines arising from hydrogen-like oxygen and neon ions in the coronae of the active RS CVn - type binaries II Peg and IM Peg, observed using the Chandra High Resolution Transmission Grating Spectrograph, shows significant decrements in the Lyalpha/Lybeta ratios as compared with theoretical predictions and with the same ratios observed in similar active binaries. We interpret these decrements in terms of resonance scattering of line photons out of the line of sight; these observations present the first strong evidence of this effect in active stellar coronae. The net line photon loss implies a nonuniform and asymmetric surface distribution of emitting structures on these stars. Escape probability arguments, together with the observed line ratios and estimates of the emitting plasma density, imply typical line-of-sight sizes of the coronal structures that dominate the X-ray emission of 10(10) cm at temperatures of 3 x 10(6) K and of 10(8) cm at 10(7) K. These sizes are an order of magnitude larger than predicted by simple quasi-static coronal loops models but are still very small compared to the several 10(11) cm radii of the underlying stars. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Palermo, Dipartimento Sci Fisiche & Astron, Sez Astron, I-90134 Palermo, Italy. RP Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA. EM jdrake@head.cfa.harvard.edu RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; PERES, Giovanni/0000-0002-6033-8180 NR 29 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2004 VL 609 IS 2 BP L79 EP L82 DI 10.1086/422747 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 835CA UT WOS:000222456300009 ER PT J AU Li, B Li, X Hu, YQ Habbal, SR AF Li, B Li, X Hu, YQ Habbal, SR TI A two-dimensional Alfven wave-driven solar wind model with proton temperature anisotropy SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE solar wind; 2-D MHD solar wind model; Alfven wave-driven solar wind; proton temperature anisotropy ID ION-CYCLOTRON WAVES; CORONAL HOLES; MAGNETOHYDRODYNAMIC FLOWS; MAGNETOSONIC INSTABILITY; VELOCITY DISTRIBUTIONS; RESONANT ACCELERATION; STREAMER; CONSTRAINTS; PARAMETERS; MINIMUM AB We present the first two-dimensional (2-D) Alfven wave turbulence-driven solar wind model which takes the proton temperature anisotropy into account. While the modeled proton temperature anisotropy in the fast solar wind is established in the inner corona and yields T-p(parallel to)/T-p(perpendicular to)=0.57 at 1 AU, which is comparable to measured values, T-p(parallel to) and T-p(perpendicular to) are only about half the observed values. In the slow wind, on the other hand, the modeled values for T-p(parallel to) and T-p(perpendicular to) as well as their ratio are close to those measured in interplanetary space. Curiously, the dip in the velocity that develops near the cusp at the top of the helmet streamer reduces the effect of transverse expansion and leads to a realistic electron temperature in the slow wind at 1 AU, although no explicit external heating is applied to electrons. Comparison with models with and without proton temperature anisotropy shows that by allowing the proton temperature anisotropy to develop, the average proton temperature is lower than the isotropic case primarily because of the cooling in the direction parallel to the magnetic field. These results imply that ion cyclotron resonance models with isotropic proton temperature are somewhat optimistic in assessing the role of Alfven wave turbulence in driving the fast solar wind. Inclusion of the temperature anisotropy of protons and proton thermal conduction are necessary for any physically realistic model. C1 Univ Wales, Inst Math & Phys Sci, Aberystwyth SY23 3BZ, Dyfed, Wales. Univ Sci & Technol China, Sch Earth & Space Sci, Hefei, Peoples R China. Univ Wales, Inst Math & Phys Sci, Aberystwyth, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, B (reprint author), Univ Wales, Inst Math & Phys Sci, Aberystwyth SY23 3BZ, Dyfed, Wales. EM bbl@aber.ac.uk; xxl@aber.ac.uk; huyq@ustc.edu.cn; sdh@aber.ac.uk RI Li, Bo/G-3525-2010 OI Li, Bo/0000-0003-4790-6718 NR 43 TC 25 Z9 27 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL 10 PY 2004 VL 109 IS A7 AR A07103 DI 10.1029/2003JA010313 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 837SV UT WOS:000222657300001 ER PT J AU Simbotin, I Jamieson, MJ Dalgarno, A AF Simbotin, I Jamieson, MJ Dalgarno, A TI Rayleigh scattering cross sections of O-2 at wavelengths longer than 180 nm SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Rayleigh scattering; oxygen; Schumann-Runge ID ROTATIONAL RAMAN-SCATTERING; MOLECULAR HYDROGEN; DIPOLE PROPERTIES; GASES; ABSORPTION; COEFFICIENTS; O2; POLARIZABILITIES; PREDISSOCIATION; POLARIZATION AB Rayleigh scattering of solar radiation by oxygen molecules is an important contributor to the photon flux in the atmosphere at wavelengths longer than the threshold for direct photodissociation of O-2 near 180 nm. We carry out detailed calculations of Rayleigh scattering cross sections of O-2 at wavelengths from 180 to 205 nm in the region of the discrete Schumann-Runge band system. The cross sections contain numerous resonance structures, whose characteristics we identify. Beyond 205 nm we show that the cross sections diminish rapidly before taking up the known variation as the inverse fourth power of the wavelength at long wavelengths. We present detailed results for cross sections for scattering by O-2 in individual rotational levels of the ground vibrational state sufficient to allow the calculation of the Rayleigh scattering cross sections at atmospheric temperatures. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Simbotin, I (reprint author), Univ Connecticut, Dept Phys, 2152 Hillside Rd,U-3046, Storrs, CT 06269 USA. EM simbotin@phys.uconn.edu; mjj@dcs.gla.ac.uk; dalgarno@cfa.harvard.edu NR 29 TC 3 Z9 3 U1 1 U2 9 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 JUL 9 PY 2004 VL 109 IS D13 AR D13302 DI 10.1029/2003JD004071 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 837RW UT WOS:000222654700001 ER PT J AU Pawson, DL AF Pawson, DL TI Ovalidota milleri, a new genus and species of bathyal sea cucumber from the Caribbean Sea (Echinodermata Holothuroidea: Apodida) SO ZOOTAXA LA English DT Article DE Ovalidota milleri; Holothuroidea; Apodida; Bathyal; Caribbean AB Ovalidota milleri new genus, new species, is a chiridotid holothurian with an egg-shaped body, a broad oral field surrounded by 18-19 (?20) tentacles, and body wall ossicles in the form of typical Chiridota wheels gathered into papillae and also scattered among the papillae. It is known from two localities in the Caribbean, near St. Vincent and at Grand Cayman Island, in bathyal depths of 366-414 metres. The egg-shaped body of this new genus is unique in the Order Apodida. When more material becomes available for study, Ovalidota milleri may be referred to a new family. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Pawson, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Mail Stop MRC 163, Washington, DC 20013 USA. NR 4 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 JUL 9 PY 2004 IS 561 BP 1 EP 6 PG 6 WC Zoology SC Zoology GA 872OT UT WOS:000225217200001 ER PT J AU McCarthy, MC Thorwirth, S Gottlieb, CA Thaddeus, P AF McCarthy, MC Thorwirth, S Gottlieb, CA Thaddeus, P TI Tetrasulfur, S-4: Rotational spectrum, interchange tunneling, and geometrical structure SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SO2 DISCHARGE SYSTEM; SULFUR CLUSTERS; AB-INITIO; MICROWAVE-SPECTRUM; ABSORPTION-SPECTRA; ATMOSPHERE; MOLECULES; STABILITIES; IONIZATION; ENERGIES AB The rotational spectrum of S-4 has been observed for the first time in an electrical discharge through sulfur vapor. Two techniques have been used: Fourier transform microwave spectroscopy and long-path millimeter-wave absorption spectroscopy. Small, but systematic shifts of the measured transition frequencies of the normal isotopic species indicate that S-4 has C-2v symmetry but with a low-lying transition state of D-2h symmetry, yielding interchange tunneling at 14.1(2) kHz in its ground vibrational state. From the rotational constants of the normal and the single S-34 isotopic species, an experimental (r(0)) structure has been derived: S-4 is a singlet planar trapezoid with a terminal bond length of 1.899(7) Angstrom, a central bond of 2.173(32) Angstrom, and an S-S-S angle of 103.9(8)degrees. Like thiozone (S-3), S-4 is a candidate for detection in the atmosphere of the Jovian moon Io and in other astronomical sources. (C) 2004 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 NR 41 TC 20 Z9 20 U1 0 U2 6 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 8 PY 2004 VL 121 IS 2 BP 632 EP 635 DI 10.1063/1.1769372 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 832KE UT WOS:000222265600003 PM 15260588 ER PT J AU Smith, DG AF Smith, DG TI A new genus and species of congrid eel (Teleostei : Anguilliformes : Congridae) from western Australia SO RECORDS OF THE AUSTRALIAN MUSEUM LA English DT Article AB A new genus and species of congrid eel, Castleichthys auritus, is described from a single specimen collected from 396 m off northwestern Australia. It belongs to the subfamily Congrinae and is characterized by a slender and flexible tail, a free flange on the upper lip, no plicae or other ornamentation on skin of head, large eye, uniserial maxillary and mandibular teeth, and conspicuous black pectoral fins. The vertebral formula is 15-36-128. C1 Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DG (reprint author), Smithsonian Inst, POB 37012,MRC-159, Washington, DC 20013 USA. EM smith.davidg@nmnh.si.edu NR 9 TC 0 Z9 1 U1 0 U2 0 PU AUSTRALIAN MUSEUM PI SYDNEY PA 6 COLLEGE ST, SYDNEY, NSW 2010, AUSTRALIA SN 0067-1975 J9 REC AUST MUS JI Rec. Aust. Mus. PD JUL 7 PY 2004 VL 56 IS 2 BP 143 EP 146 PG 4 WC Zoology SC Zoology GA 863QS UT WOS:000224577400002 ER PT J AU Gill, AC Jewett, SL AF Gill, AC Jewett, SL TI Eviota hoesei and E-readerae, new species of fish from the Southwest Pacific, with comments on the identity of E-corneliae Fricke (Perciformes : Gobiidae) SO RECORDS OF THE AUSTRALIAN MUSEUM LA English DT Article ID GENUS AB Eviota hoesei n.sp. is described from specimens from New Caledonia, Lord Howe Island (type locality), Norfolk Island, and Middleton and Elizabeth Reefs. It is distinguished from congeners in having the following character combination: dorsal-fin rays usually VI + I,9; anal-fin rays usually I,8; at least some pectoral-fin rays branched; cephalic sensory-pore system pattern 2; base of pectoral fin with two diffuse to prominent dark spots; fifth segmented pelvic-fin ray present, usually about 1/10 length of fourth ray; and 6 subcutaneous bars/spots on lower postanal trunk. Eviota readerae n.sp. is described from specimens from Middleton (type locality) and Elizabeth Reefs. It is distinguished from congeners in having the following combination of characters: dorsal-fin rays VI + I,9; anal-fin rays I,8; at least some pectoral-fin rays branched; fifth segmented pelvic-fin ray lacking; cephalic sensory-pore system pattern 1; male genital papilla non-fimbriate; 12-13 dark bars or saddles on trunk from origin of spinous dorsal fin to mid peduncular spot, not extending below midline; and pectoral-fin base with prominent circular dark spot dorsally. Eviota corneliae Fricke is placed in synonymy with Trimmatom eviotops (Schultz). C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20560 USA. Nat Hist Museum, Dept Zool, Fish Res Grp, London SW7 5BD, England. RP Gill, AC (reprint author), Arizona State Univ, Sch Life Sci, POB 874501, Tempe, AZ 85287 USA. EM Anthony.Gill@asu.edu; jewett.susan@nmnh.si.edu NR 21 TC 8 Z9 11 U1 1 U2 3 PU AUSTRALIAN MUSEUM PI SYDNEY PA 6 COLLEGE ST, SYDNEY, NSW 2010, AUSTRALIA SN 0067-1975 J9 REC AUST MUS JI Rec. Aust. Mus. PD JUL 7 PY 2004 VL 56 IS 2 BP 235 EP 240 PG 6 WC Zoology SC Zoology GA 863QS UT WOS:000224577400015 ER PT J AU Munroe, TA Menke, SB AF Munroe, TA Menke, SB TI Two new soleid flatfishes (Pleuronectiformes : Soleidae : Soleichthys) from Australian waters, with a re-description of Soleichthys microcephalus (Gunther) SO RECORDS OF THE AUSTRALIAN MUSEUM LA English DT Article AB Soleichthys microcephalus (Gunther, 1862) occurring in warm temperate waters off New South Wales, Australia, is re-described based on examination of a syntype and additional non-type material. This species differs from congeners in its combination of: low meristic features (43-45 vertebrae, 71-84 dorsal-fin rays, 61-71 anal-fin rays, and 81-89 lateral-line scales); in having two elongated ocular-side pectoral-fin rays of nearly equal length; with small scales present on the ocular-side pectoral-fin base and proximal halves of elongated pectoral-fin rays; in its ocular-side pigmentation consisting of a series of 8-10 mostly complete, bold, wide, dark-brown or blackish crossbands of nearly uniform width throughout their lengths and noticeably wider than the alternating lighter-coloured crossbands; and with two, conspicuous, mid-lateral white spots arranged in horizontal series. Two new species phenotypically most similar to, and with meristic features that largely overlap those of S. microcephalus, are described from specimens collected in tropical waters of northern Australia. Soleichthys serpenpellis n.sp., known from the Gulf of Carpentaria and Delambre Island, Dampier Archipelago, northwestern Australia, is easily distinguished from S. microcephalus and other congeners by its ocular-side head and body pigmentation featuring incomplete, diamond-shaped crossbands broadest in their mid-sections, fewer (about 6) ocular-side body crossbands, and with small, brown spots scattered in the interspaces between the crossbands. Soleichthys oculofasciatus n.sp. occurs off northeast Australia and is distinguished from congeners in its combination of a first elongate ocular-side pectoral-fin ray longer than the second, in lacking scales on the ocular-side pectoral-fin base and elongate pectoral-fin rays, in having a longitudinal series of crossbands (usually 11) on the ocular-side head and body, and with four conspicuous white spots on the body, two of which are arranged in a vertical series at mid-body. The new species differs further from both S. microcephalus and S. serpenpellis in having a longer and narrower head and a longer caudal fin. C1 Smithsonian Inst, NOAA, NMFS, Natl Systemat Lab, Washington, DC 20013 USA. Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92093 USA. RP Munroe, TA (reprint author), Smithsonian Inst, NOAA, NMFS, Natl Systemat Lab, POB 37021,NHB,WC 57,MRC-153, Washington, DC 20013 USA. EM Munroe.Thomas@nmnh.si.edu; smenke@biomail.ucsd.edu NR 36 TC 0 Z9 0 U1 0 U2 2 PU AUSTRALIAN MUSEUM PI SYDNEY PA 6 COLLEGE ST, SYDNEY, NSW 2010, AUSTRALIA SN 0067-1975 J9 REC AUST MUS JI Rec. Aust. Mus. PD JUL 7 PY 2004 VL 56 IS 2 BP 247 EP 258 PG 12 WC Zoology SC Zoology GA 863QS UT WOS:000224577400017 ER PT J AU Krems, RV AF Krems, RV TI Breaking van der Waals molecules with magnetic fields SO PHYSICAL REVIEW LETTERS LA English DT Article ID INELASTIC-COLLISIONS; SCATTERING; RESONANCES; ATOMS AB It is demonstrated that weakly bound van der Waals complexes can dissociate in a magnetic field through coupling between the Zeeman levels. The Zeeman predissociation process is shown to be efficient and it can be controlled by external magnetic fields. C1 Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Krems, RV (reprint author), Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. EM rkrems@cfa.harvard.edu NR 20 TC 31 Z9 31 U1 2 U2 7 PU AMERICAN 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 JUL 2 PY 2004 VL 93 IS 1 AR 013201 DI 10.1103/PhysRevLett.93.013201 PG 4 WC Physics, Multidisciplinary SC Physics GA 834DD UT WOS:000222390900013 ER PT J AU Raymond, JC AF Raymond, JC TI Imaging the Sun's eruptions in three dimensions SO SCIENCE LA English DT Editorial Material ID FLUX-ROPES 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 raymond@cfa.harvard.edu NR 6 TC 0 Z9 0 U1 1 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 JUL 2 PY 2004 VL 305 IS 5680 BP 49 EP 50 DI 10.1126/science.1100371 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 834BG UT WOS:000222386000027 PM 15232094 ER PT J AU Potts, R Behrensmeyer, AK Deino, A Ditchfield, P Clark, J AF Potts, R Behrensmeyer, AK Deino, A Ditchfield, P Clark, J TI Small mid-Pleistocene hominin associated with east African Acheulean technology SO SCIENCE LA English DT Article ID OLD HOMO CRANIUM; MIDDLE PLEISTOCENE; OLORGESAILIE FORMATION; AFAR DEPRESSION; ETHIOPIA; ERECTUS; REMAINS; AGE; CEPRANENSIS; EVOLUTION AB Hominin fossils from the African mid-Pleistocene are rare despite abundant Acheulean tools in Africa and apparently African-derived hominins in Eurasia between 1.0 and 0.5 million years ago (Ma). Here we describe an African fossil cranium constrained by Ar-40/Ar-39 analyses, magnetostratigraphy, and sedimentary features to 0.97 to 0.90 Ma, and stratigraphically associated with Acheulean handaxes. Although the cranium represents possibly the smallest adult or near-adult known between 1.7 and 0.5 Ma, it retains features observed in larger Homo erectus individuals, yet shows a distinct suite of traits indicative of wide population variation in the hominins of this period. C1 Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. Natl Museums Kenya, Div Paleontol, Nairobi, Kenya. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Berkeley Geochronol Ctr, Berkeley, CA 94709 USA. Univ Oxford, Res Lab Archaeol, Oxford OX1 3QJ, England. RP Potts, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. EM potts.rick@nmnh.si.edu NR 26 TC 56 Z9 59 U1 5 U2 14 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 JUL 2 PY 2004 VL 305 IS 5680 BP 75 EP 78 DI 10.1126/science.1097661 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 834BG UT WOS:000222386000037 PM 15232102 ER PT J AU Post, JE Heaney, PJ AF Post, JE Heaney, PJ TI Neutron and synchrotron X-ray diffraction study of the structures and dehydration behaviors of ramsdellite and "groutellite" SO AMERICAN MINERALOGIST LA English DT Article ID GAMMA-MANGANESE-DIOXIDE; POWDER DIFFRACTION; RIETVELD REFINEMENT; MNO2; PYROLUSITE; INSERTION; SYSTEM; MODEL AB The crystal structure of ramsdellite, MnO2, was refined using time-of-flight powder neutron diffraction data and the Rietveld method in order to assess the effects of reduction in cathodic battery materials. For the first time, we present a refined structure for "groutellite," a heretofore poorly characterized phase with ideal formula (Mn0.54+Mn0.53+)O-1.5(OH)(0.5). "Groutellite" is generated synthetically as an intermediate compound during the reduction of ramsdellite to groutite (MnOOH), and it also occurs as an intergrowth in certain natural specimens of ramsdellite. The Jahn-Teller distortions in "groutellite" are confined to the a-c plane, and they result in a 6.8% unit-cell volume increase relative to ramsdellite. The Mn-O bond lengths refined for "groutellite" are consistent with the replacement of half of the Mn4+ and O2- in ramsdellite by Mn3+ and (OH)(-), respectively. In addition, the high-temperature behaviors of ramsdellite and "groutellite" were investigated by temperature-resolved synchrotron powder X-ray diffraction from 298 to 720 K. Rietveld refinements revealed a gradual thermal expansion of the groutellite structure to similar to450 K. At higher temperatures, the unit-cell volume gradually decreased, primarily as a result of a decrease in c. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Post, JE (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM post.jeffrey@nmnh.si.edu NR 30 TC 20 Z9 20 U1 1 U2 12 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD JUL PY 2004 VL 89 IS 7 BP 969 EP 975 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 838IZ UT WOS:000222708200006 ER PT J AU Rosenthal, GG Rand, AS Ryan, MJ AF Rosenthal, GG Rand, AS Ryan, MJ TI The vocal sac as a visual cue in anuran communication: an experimental analysis using video playback SO ANIMAL BEHAVIOUR LA English DT Article ID TUNGARA FROGS; EVOLUTION AB Acoustic signals produced by most anurans are accompanied by inflation of a conspicuous vocal sac. We presented female tungara frogs, Physalaemus pustulosus, with acoustic playback of the male advertisement call, synchronized with a video playback of vocal sac inflation. Females significantly preferred a stimulus combination including vocal sac inflation over an identical set of stimuli with the vocal sac inflation removed. Neither a moving rectangle bearing the gross contrast and spatiotemporal properties of the vocal sac inflation sequence, nor the image of a noncalling male significantly enhanced the attractiveness of the acoustic stimulus. Both the form and spatiotemporal properties of the vocal sac thus appear to be salient to females. The results indicate that the vocal sac can serve as a visual cue, which may account for the conspicuous pigmentation found on the vocal sacs of males in many species. Gular inflation in synchrony with a call may function to facilitate female localization of individual males in an aggregation. (C) 2004 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 Boston Univ, Marine Program, Marine Biol Lab, Woods Hole, MA 02543 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. RP Rosenthal, GG (reprint author), Boston Univ, Marine Program, Marine Biol Lab, 7 MBL St, Woods Hole, MA 02543 USA. EM gil@bu.edu RI Rosenthal, Gil/E-6924-2015 OI Rosenthal, Gil/0000-0003-0342-9024 NR 17 TC 70 Z9 74 U1 0 U2 13 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 JUL PY 2004 VL 68 BP 55 EP 58 DI 10.1016/j.anbehav.2003.07.013 PN 1 PG 4 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 842GZ UT WOS:000222993000007 ER PT J AU Swanson, WF Brown, JL AF Swanson, WF Brown, JL TI International training programs in reproductive sciences for conservation of Latin American felids SO ANIMAL REPRODUCTION SCIENCE LA English DT Article; Proceedings Paper CT 15th International Congress on Animal Reproduction CY AUG 08-12, 2004 CL Porto Seguro, BRAZIL SP Brazilian Coll Anim Reprod DE cats; fecal hormones; laparoscopy; electroejaculation; cryopreservation; research training ID LAPAROSCOPIC ARTIFICIAL-INSEMINATION; JAGUARS PANTHERA-ONCA; EXOGENOUS GONADOTROPINS; ENDANGERED FELIDS; OVARIAN ACTIVITY; DOMESTIC CAT; ZOO BIOLOGY; PUMA; OVULATION; CONCOLOR AB Survival of the ten non-domestic felid species endemic to Latin America is imperiled by habitat loss, poaching and poor captive management. Over the past 10 years, conservation of these felids has been the primary focus of a reproductive research and training program conducted in Brazil, Mexico, and the USA. The objectives of this program were to: (1) provide intensive training in reproductive sciences to Latin American scientists, (2) conduct collaborative studies investigating basic and applied reproduction in endangered felids, and (3) establish a highly-trained scientific cohort to conduct independent conservation-based research. Four formal training courses, consisting of didactic lectures and hands-on instruction in research techniques, including semen collection, sperm cryopreservation and laparoscopic artificial insemination (AI), were taught in Brazil and Mexico between 1995 and 1998. Several of these scientists received further training in conducting fecal hormone analysis in the USA, and a number of research studies, many in collaboration with American scientists, were initiated in Latin American felids. Research findings have characterized basal reproductive traits in several felid species, including ocelots, margay, tigrinas and jaguars, and established that Latin American felids exhibit only minimal seasonal variation in most reproductive traits. Other studies have explored the impact of acute and chronic stressors on adrenocortical activity and demonstrated the importance of environmental enrichment in captivity, especially in small fetids. Additional research has examined ovarian and immunological responsiveness of Latin American felids to exogenous gonadotropins and assessed the impact of nutrition on sperm production and oocyte quality. Applied reproductive studies have investigated sperm cryopreservation in both captive and wild felid populations and demonstrated the production of viable offspring in ocelots and tigrinas following laparoscopic AI. Ongoing studies are investigating the potential of in vitro fertilization (IVF), embryo cryopreservation and embryo transfer for genetic management of ocelots and tigrinas. To date, over 75 Brazilian ocelot and 50 tigrina IVF embryos have been cryopreserved and two pregnancies have been established in ocelots following transfer of frozen-thawed embryos. Findings from these studies are helping to improve husbandry, population management, and breeding of Latin American felids in captivity. Continued advances in assisted reproduction eventually may provide an alternative route for exchanging genetic material among Latin American felid populations. Most importantly, this collaborative program has been essential for building scientific capacity, within Brazil and Mexico, in establishing a core group of highly-trained reproductive biologists that will continue applying their new knowledge and skills to the conservation of Latin American felids. (C) 2004 Elsevier B.V All rights reserved. C1 Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife, Cincinnati, OH 45220 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Swanson, WF (reprint author), Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife, 3400 Vine St, Cincinnati, OH 45220 USA. EM william.swanson@cincinnatizoo.org NR 51 TC 32 Z9 36 U1 3 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 EI 1873-2232 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD JUL PY 2004 VL 82-3 SI SI BP 21 EP 34 DI 10.1016/j.anireprosci.2004.05.008 PG 14 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA 845PS UT WOS:000223257400004 PM 15271441 ER PT J AU Simmons, RB Scheffer, SJ AF Simmons, RB Scheffer, SJ TI Evidence of cryptic species within the pest Copitarsia decolora (Guenee) (Lepidoptera : Noctuidae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE cryptic species; genetic variation; morphology; phylogeny; paraphyly ID DNA; AGROMYZIDAE; SEQUENCE; DIPTERA; LIMITS AB Copitarsia decolora (Guenee) is a widely distributed, highly polyphagous pest found throughout Central and South America. We examined multiple populations of C. decolora with the mitochondrial gene cytochrome oxidase I (COI). We also investigated morphological variation in adult males sampled from these populations. COI evidence suggests that C. decolora is comprised of two cryptic lineages and is paraphyletic with respect to the Chilean C. naenoides (Butler). These two lineages, which are not completely geographically isolated, display high divergence in COI sequences compared with other members of Copitarsia and other insect pest species in general. Furthermore, these lineages also possess slight morphological differences in male genitalia; however, supporting information is necessary before the taxonomy of this species is revised. C1 Smithsonian Inst, USDA ARS, Nat Hist Museum, PSI,SEL, Washington, DC 20013 USA. USDA ARS, PSI, SEL, Beltsville, MD 20705 USA. RP Simmons, RB (reprint author), Smithsonian Inst, USDA ARS, Nat Hist Museum, PSI,SEL, MRC-0168, Washington, DC 20013 USA. EM rsimmons@sel.barc.usda.gov NR 22 TC 20 Z9 21 U1 1 U2 3 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD JUL PY 2004 VL 97 IS 4 BP 675 EP 680 DI 10.1603/0013-8746(2004)097[0675:EOCSWT]2.0.CO;2 PG 6 WC Entomology SC Entomology GA 837NO UT WOS:000222642400007 ER PT J AU Solazzo, C Erhardt, D Marte, F Von Endt, D Tumosa, C AF Solazzo, C Erhardt, D Marte, F Von Endt, D Tumosa, C TI Effects of chemical and biological warfare remediation agents on the materials of museum objects SO APPLIED PHYSICS A-MATERIALS SCIENCE & PROCESSING LA English DT Article AB In the fall of 2001, anthrax-contaminated letters were sent to public figures in the United States. Chemical and radiation treatments were employed to decontaminate exposed buildings, objects, and materials. These treatments are effective, but potentially damaging to exposed objects and materials. The recommended surface chemical treatments include solutions, gels, and foams of oxidizing agents such as peroxides or chlorine bleaching agents. Such oxidizing agents are effective against a wide range of hazardous chemical and biological agents. Knowing how these reagents affect various substrates would help to anticipate and to minimize any potential damage. We are examining the effects on typical museum materials of reagents likely to be used, including hydrogen peroxide, sodium hypochlorite, and potassium peroxymonosulfate. Results so far show significant changes in a number of materials. Surface corrosion was observed on metals such as copper, silver, iron, and brass. Color changes occurred with at least one reagent in about one-fourth of the dyed fabric swatches tested, and about half of the inks. Samples of aged yellowed paper are bleached. Effects varied with both the substrate and the tested reagent. The observed changes were generally less drastic than might have been expected. Enough materials were affected, though, to preclude the use of these reagents on museum objects unless no less drastic alternative is available. It appears that many objects of lesser intrinsic value can be treated without severe loss of properties or usefulness. For example, most documents should remain legible if the appropriate reagent is used. This work will provide a basis for determining which treatment is most appropriate for a specific situation and what consequences are to be expected from other treatments. C1 Smithsonian Inst, Museum Support Ctr, Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. RP Erhardt, D (reprint author), Smithsonian Inst, Museum Support Ctr, Smithsonian Ctr Mat Res & Educ, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM erhardt@scmre.si.edu NR 6 TC 2 Z9 2 U1 0 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0947-8396 J9 APPL PHYS A-MATER JI Appl. Phys. A-Mater. Sci. Process. PD JUL PY 2004 VL 79 IS 2 BP 247 EP 252 DI 10.1007/s00339-004-2511-7 PG 6 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 828YD UT WOS:000222008800015 ER PT J AU Dussubieux, L Van Zelst, L AF Dussubieux, L Van Zelst, L TI LA-ICP-MS analysis of platinum-group elements and other elements of interest in ancient gold SO APPLIED PHYSICS A-MATERIALS SCIENCE & PROCESSING LA English DT Article ID PLASMA-MASS SPECTROMETRY AB One of the most promising methods for ancient gold analysis is laser ablation-inductively coupled plasma mass spectrometry (LA-ICP-MS). It is a quasi-non-destructive multi-elemental analytical method with detection limits in the range of ppm or below, depending on the element. Internal and external standardizations are used. Different types of standards are necessary to measure major (required for the internal standardization), minor and trace elements. High-purity gold standards doped with trace elements as well as ancient gold coins were found suitable for that purpose. The reproducibility and the accuracy of the results obtained are good enough to consider LA-ICP-MS as reliable to determine trace-element concentrations in ancient gold. C1 Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. RP Dussubieux, L (reprint author), Smithsonian Ctr Mat Res & Educ, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 4 TC 17 Z9 17 U1 1 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0947-8396 J9 APPL PHYS A-MATER JI Appl. Phys. A-Mater. Sci. Process. PD JUL PY 2004 VL 79 IS 2 BP 353 EP 356 DI 10.1007/s00339-004-2532-2 PG 4 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 828YD UT WOS:000222008800033 ER PT J AU Matthews, LD de Grus, R AF Matthews, LD de Grus, R TI Optical imaging and spectroscopy of the edge-on Sbc galaxy UGC 10043: Evidence for a galactic wind and a peculiar triaxial bulge SO ASTRONOMICAL JOURNAL LA English DT Review DE galaxies : bulges; galaxies : evolution; galaxies : individual (UGC 10043); galaxies : spiral; galaxies : structure; ISM : kinematics and dynamics ID POLAR-RING GALAXY; SURFACE BRIGHTNESS GALAXIES; DISK DOMINATED GALAXIES; DIFFUSE IONIZED-GAS; SPIRAL GALAXIES; COLOR GRADIENTS; STAR-FORMATION; STELLAR DISKS; H-I; ELLIPTICAL GALAXIES AB We present new optical imaging and spectroscopy of the peculiar, edge-on Sbc galaxy UGC 10043. Using the WIYN telescope, we have obtained B, R, and Halpha + [N II] images, together with DensePak integral field spectroscopic measurements of the stellar Ca I infrared triplet and the Halpha and [N II] lines from the ionized gas. The imaging observations show that the inner bulge of UGC 10043 ( a less than or equal to 7."5) is elongated perpendicular to the galaxy major axis. At larger r the bulge isophotes twist to become oblate and nearly circular, suggesting the bulge is triaxial. The bulge shows no clear evidence for rotation about either its major or minor axis. The inner, southwestern quadrant of the bulge is girdled by a narrow dust lane parallel to the minor axis; unsharp masking reveals that this minor-axis dust lane may be part of an inner polar ring, although we find no unambiguous kinematic evidence of orthogonally rotating material. The stellar disk of UGC 10043 has a rather low optical surface brightness [mu(0)(R,i) similar to 23.2 mag arcsec(-2)], a small scale height (h(z) = 395 pc for D = 33.4 Mpc), and a mild integral sign warp. A dusty, inner disk component that appears tilted relative to the outlying disk is also seen. The Halpha and [N II] emission lines in UGC 10043 resolve into multiple velocity components, indicating the presence of a large-scale galactic wind with an outflow velocity of V-out greater than or similar to 104 km s(-1). Halpha + [N II] imaging reaffirms this picture by revealing ionized gas extended to \z\ similar to 3.5 kpc in the form of a roughly biconical structure. The [N II]/Halpha line intensity ratio increases with increasing distance from the plane, reaching values as high as 1.7. Unlike most galaxies with large-scale winds, UGC 10043 has only a modest global star formation rate (less than or similar to1 M-. yr(-1)), implying the wind is powered by a rather feeble central starburst. We discuss evolutionary scenarios that could account for both the structural complexities of UGC 10043 and its large-scale wind. The most plausible scenarios require a major accretion or merger event at least a few gigayears ago. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. RP Matthews, LD (reprint author), Harvard Smithsonian Ctr Astrophys, MS-42,60 Garden St, Cambridge, MA 02138 USA. EM lmatthew@cfa.harvard.edu; R.DeGrijs@sheffield.ac.uk OI de Grijs, Richard/0000-0002-7203-5996 NR 140 TC 16 Z9 16 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2004 VL 128 IS 1 BP 137 EP 162 DI 10.1086/421363 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GZ UT WOS:000222702800012 ER PT J AU Mochejska, BJ Stanek, KZ Sasselov, DD Szentgyorgyi, AH Westover, M Winn, JN AF Mochejska, BJ Stanek, KZ Sasselov, DD Szentgyorgyi, AH Westover, M Winn, JN TI Planets in stellar clusters extensive search. II. Discovery of 57 variables in the cluster NGC 2158 with millimagnitude image subtraction photometry SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; delta Scuti; Hertzsprung-Russell diagram; novae, cataclysmic variables ID DELTA-SCUTI STARS; CATALOG; FREQUENCY; M67 AB We have undertaken a long-term project, Planets in Stellar Clusters Extensive Search (PISCES), to search for transiting planets in open clusters. NGC 2158 is one of the targets we have chosen - an intermediate age, populous, rather metal-poor cluster. In this paper we present the results of a search for variable stars in the data from the first season of monitoring at the FLWO 1.2 m telescope. This is the first variability search ever conducted in this cluster. We present a catalog of 57 variable stars, most with low-amplitude variability. Among the variables is a cataclysmic variable (CV) that underwent a 2.5 mag outburst. If it is a member of NGC 2158, this would be the fourth CV known in an open cluster. We have also found five delta Scuti stars, three of which have two or more detectable modes of pulsation. Of the 57 variables discovered, 28 have R-band amplitudes of 5% or below. Six of those vary at or below the 2% level, including one with 0.08% variability. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mochejska, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bmochejs@cfa.harvard.edu; kstanek@cfa.harvard.edu; sasselov@cfa.harvard.edu; saint@cfa.harvard.edu; mwestover@cfa.harvard.edu; jwinn@cfa.harvard.edu NR 27 TC 24 Z9 24 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2004 VL 128 IS 1 BP 312 EP 322 DI 10.1086/420992 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GZ UT WOS:000222702800024 ER PT J AU McCall, ML Buta, RJ Foster, TJ Huchtmeier, W Huchra, J AF McCall, ML Buta, RJ Foster, TJ Huchtmeier, W Huchra, J TI Discovery of a huge young stellar object interaction region in Camelopardalis SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : general; galaxies : individual : UGCA 92; infrared : general; stars : pre-main-sequence ID EXTENDED RED EMISSION; MILKY-WAY; SILICON NANOPARTICLES; STANDARD STARS; RADIO-SOURCES; CO SURVEY; EXTINCTION; GALAXIES; DISTANCE; CATALOG AB During the course of a wide-field VI survey of galaxies in the IC 342/Maffei Group, a large nebula, which looks like an inclined disk with a jetlike plume emerging from it, was discovered in Camelopardalis. The object is most prominent in I. The predominating disk component is 6.'8 across, which corresponds to 4.0 +/- 1.6 pc at the estimated distance of 2.0 +/- 0.8 kpc (the Perseus Arm). The plume extends 3.'8 ( 2.2 pc) outward from the core along a direction that is about 20degrees from the minor axis of the disk. The disk lies along the edge of a filament of dust and molecular gas in the Milky Way. The plume points toward the core of the filament. No large-scale emission is seen at Halpha, and the nebula is invisible in Two Micron All Sky Survey (2MASS) images. About 30" from the center of the disk is IRAS 04261+6339, which is a pair of unresolved Halpha sources whose IRAS colors and spectra reveal them to be young stellar objects (YSOs). The northern of the two exhibits a near-infrared tail, which is 15" (0.15 pc) long in H and directed 66degrees away from the plume. Although the stars are exposed, as in Class II YSOs, the spectral energy distribution of the pair rises beyond 2 mum, typical of Class I systems. It appears that they are transitional YSOs, with characteristics similar to those of Holoea (IRAS 05327+ 3404). The total brightness of the plume plus disk exceeds that of the stars by 1.6 mag in I, yet the V - I color is bluer by only 0.50 mag. Thus, the nebula cannot be a consequence of reflection, even allowing for differential extinction. It is tentatively identified as a remnant of an outflow from a binary YSO, glowing from the photoluminescence of silicon nanoparticles. C1 York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McCall, ML (reprint author), York Univ, Dept Phys & Astron, 4700 Keele St, Toronto, ON M3J 1P3, Canada. EM mccall@yorku.ca; buta@sarah.astr.ua.edu; tyler.foster@nrc-cnrc.gc.ca; huchtmeier@mpifr-bonn.mpg.de; huchra@cfa.harvard.edu NR 46 TC 1 Z9 1 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2004 VL 128 IS 1 BP 375 EP 386 DI 10.1086/421370 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GZ UT WOS:000222702800030 ER PT J AU D'Elia, V Fiore, F Elvis, M Cappi, M Mathur, S Mazzotta, P Falco, E Cocchia, F AF D'Elia, V Fiore, F Elvis, M Cappi, M Mathur, S Mazzotta, P Falco, E Cocchia, F TI The faint X-ray source population near 3C 295 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : galaxies; galaxies : clusters : individual : 3C 295; X-rays : diffuse background - cosmology : large-scale structure of Universe ID DEEP FIELD-SOUTH; COUNTING DETECTOR IMAGES; INTERGALACTIC MEDIUM; WAVELET TRANSFORMS; MISSING BARYONS; OPTICAL SURVEY; CHANDRA; GALAXIES; CLUSTERS; DISTANT AB We present a statistical analysis of the Chandra observation of the source field around the 3C 295 galaxy cluster (z = 0.46) to search for clustering of X-ray sources. We applied three different methods of analysis, all suggesting a strong clustering in the field on scales of a few arcmin. In particular 1) the log N-log S computed separately for the four ACIS-I chips reveals that there is a significant (3.2sigma in the 0.5-2 keV, 3.3sigma in the 2-10 keV and 4.0sigma in the 0.5-10 keV band) excess of sources to the North-North East and a void to the South of the central cluster; 2) the two point, two-dimensional Kolmogorov-Smirnov (KS) test, shows the probability that the sources are uniformly distributed is only a few percent; 3) a strong spatial correlation emerges from the study of the angular cot-relation function of the field: the angular correlation function (ACF) shows a clear signal on scales of 0.5 divided by 5 arcmin, correlation angle in the 0.5-7 keV band theta(0) = 8.5(-4.5)(+16.5), 90% confidence limit (assuming a power law ACF with slope gamma = 1.8). This correlation angle is 2 times higher than that of a sample of 8 ACIS-I field at the 2.5sigma confidence level. The above scales translate to 0.2 divided by 2 Mpc at the cluster redshift, higher than the typical cluster core radius, and more similar to the size of a "filament" of the large scale structure. C1 Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, IASF, I-40126 Bologna, Italy. Ohio State Univ, Columbus, OH 43210 USA. Univ Durham, Durham DH1 3LE, England. RP Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. EM delia@mporzio.astro.it RI Cappi, Massimo/F-4813-2015; Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; D'Elia, Valerio/0000-0002-7320-5862; Cappi, Massimo/0000-0001-6966-8920; Fiore, Fabrizio/0000-0002-4031-4157 NR 39 TC 17 Z9 17 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 JUL PY 2004 VL 422 IS 1 BP 11 EP 21 DI 10.1051/0004-6361:20040149 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844PE UT WOS:000223171300007 ER PT J AU Pillitteri, I Micela, G Sciortino, S Damiani, F Harnden, FR AF Pillitteri, I Micela, G Sciortino, S Damiani, F Harnden, FR TI XMM-Newton observations of the young open cluster Blanco 1 - I. X-ray spectroscopy and photometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-ray : stars; stars : activity; Galaxy : open clusters and associations : individual : Blanco I ID COUNTING DETECTOR IMAGES; ZETA-SCULPTORIS CLUSTER; WAVELET TRANSFORMS; STARS; PLEIADES; EMISSION; ROSAT; METALLICITY; DISTRIBUTIONS; DEPENDENCE AB We present an X-ray study of the high metallicity young open cluster Blanco 1 based on XMM-Newton data. X-ray spectroscopy of cluster members is presented for the first time as well as new X-ray distribution functions of late-type stars. We detected all known dF and dG stars in the EPIC field and 80% and 90% of dK and dM stars, respectively. The X-ray spectral analysis of the X-ray brightest cluster stars and X-ray color analysis of a larger sample show that a model with two temperatures (at about 0.3 and 1 keV) explains the quiescent activity phase spectra. We discuss also the nature of unidentified X-ray sources in the observed region and their X-ray spectral properties. C1 Univ Palermo, Dipartimento Astron, I-90134 Palermo, Italy. INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pillitteri, I (reprint author), Univ Palermo, Dipartimento Astron, Piazza Parlamento 1, I-90134 Palermo, Italy. EM pilli@astropa.unipa.it; giusi@astropa.unipa.it; sciorti@astropa.unipa.it; damiani@astropa.unipa.it; frh@cfa.harvard.edu RI Pillitteri, Ignazio/L-1549-2016; OI Pillitteri, Ignazio/0000-0003-4948-6550; Micela, Giuseppina/0000-0002-9900-4751; Damiani, Francesco/0000-0002-7065-3061 NR 37 TC 19 Z9 19 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2004 VL 421 IS 1 BP 175 EP 186 DI 10.1051/0004-6361:20035869 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840HD UT WOS:000222847800021 ER PT J AU Zboril, M Strassmeier, KG Avrett, EH AF Zboril, M Strassmeier, KG Avrett, EH TI An atmospheric model for UZ Librae from mean H alpha-line profiles SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : late-type; stars : activity; stars : atmospheres; stars : chromospheres; stars : individual : UZ Lib ID STELLAR SURFACE-STRUCTURE; SOLAR CHROMOSPHERE; STARS; COMPONENTS; SUN AB We present the results from fitting a semi-empirical atmospheric model including a chromosphere and a transition region to the mean (seasonal) Balmer Halpha line profiles of the RS CVn-type K0-giant UZ Librae. As a first step, a static 1D spherical model was applied to the mean component of the Ha-emission core and its profile. The main result of the fitting is that the transition region begins at a log mass depth of -1.8 g cm(-2) at a temperature of 7400 K (approximately 3000 K warmer than the photosphere) and then has a steep increase to the peak temperature of approximate to10(6) K. A stellar model in plane-parallel mode with "partial-frequency redistribution" option in the line transfer gave roughly the best fit. Subsequently, two-Gaussian fitting of the phase-dependent Halpha-line profiles yields a complex velocity field. The radial velocities, from both the absorption reversal and the main emission component, display rotational and/or orbital modulation. The largest differences between consecutive line profiles occur mostly in the red line wings, suggesting the existence of both an inward-pointed velocity field and sporadic radiation events possibly related to flares. The total Halpha emission, as derived from the equivalent width, possibly also displays rotational modulation. Indirect evidence is presented for the existence of circurnstellar matter in form of an Halpha absorption shell. Finally, a preliminary elemental abundance analysis suggests sub-solar metallicity of [M/H] approximate to -0.5 dex based on ATLAS models, or -0.7 dex based on PHOENIX models. C1 AIP, D-14482 Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, SAO, Cambridge, MA 02138 USA. RP AIP, Sternwarte 16, D-14482 Potsdam, Germany. EM mzboril@aip.de; kstrassmeier@aip.de; avrett@cfa.harvard.edu NR 26 TC 4 Z9 4 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2004 VL 421 IS 1 BP 295 EP 303 DI 10.1051/0004-6361:20034193 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840HD UT WOS:000222847800033 ER PT J AU Haverkorn, M Heitsch, F AF Haverkorn, M Heitsch, F TI Canals beyond Mars: Beam depolarization in radio continuum maps of the warm ISM SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetohydrodynamics; magnetic fields; polarization; turbulence; ISM : magnetic fields; radio continuum : ISM ID MAGNETOHYDRODYNAMIC TURBULENCE; INTERSTELLAR-MEDIUM; MOLECULAR CLOUDS; MULTIFREQUENCY POLARIMETRY; MAGNETIC-FIELD; 350 MHZ; GHZ; POLARIZATION; SIMULATIONS; EMISSION AB Multi-frequency radio polarimetric observations of the diffuse Galactic synchrotron background enable us to study the structure of the diffuse ionized gas via rotation measure maps. However, depolarization will introduce artifacts in the resulting rotation measure (RM), most notably in the form of narrow, elongated "depolarization canals". We use numerical models of a non-emitting Faraday rotating medium to study the RM distribution needed to create depolarization canals by depolarization due to a finite beam width, and to estimate the influence of this depolarization mechanism on the determination of RM. We argue that the depolarization canals indeed can be caused by beam depolarization, which in turn is a natural consequence when observing a turbulent medium with limited resolution. Furthermore, we estimate that beam depolarization can induce an additional error of about 20% in RM determinations, and considerably less in regions that are not affected by depolarization canals. C1 Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Wisconsin, Madison, WI 53706 USA. Univ Munich, Inst Astron & Astrophys, D-81679 Munich, Germany. RP Haverkorn, M (reprint author), Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands. EM mhaverkorn@cfa.harvard.edu; heitsch@usm.uni-muenchen.de NR 28 TC 12 Z9 12 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2004 VL 421 IS 3 BP 1011 EP 1019 DI 10.1051/0004-6361:20034444 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 845MX UT WOS:000223249700022 ER PT J AU Park, BG DePoy, DL Gaudi, BS Gould, A Han, C Pogge, RW Abe, F Bennett, DP Bond, IA Eguchi, S Furuta, Y Hearnshaw, JB Kamiya, K Kilmartin, PM Kurata, Y Masuda, K Matsubara, Y Muraki, Y Noda, S Okajima, K Rattenbury, NJ Sako, T Sekiguchi, T Sullivan, DJ Sumi, T Tristram, PJ Yanagisawa, T Yock, PCM AF Park, BG DePoy, DL Gaudi, BS Gould, A Han, C Pogge, RW Abe, F Bennett, DP Bond, IA Eguchi, S Furuta, Y Hearnshaw, JB Kamiya, K Kilmartin, PM Kurata, Y Masuda, K Matsubara, Y Muraki, Y Noda, S Okajima, K Rattenbury, NJ Sako, T Sekiguchi, T Sullivan, DJ Sumi, T Tristram, PJ Yanagisawa, T Yock, PCM CA muFUN Collaboration MOA Collaboration TI MOA 2003-BLG-37: A bulge jerk-parallax microlens degeneracy SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : bulge; gravitational lensing ID PLANET PHOTOMETRY; MACHO PARALLAXES; GALACTIC BULGE; SATELLITE; EVENT; LENS; HALO AB We analyze the Galactic bulge microlensing event MOA 2003-BLG-37. Although the Einstein timescale is relatively short, t(E) = 43 days, the light curve displays deviations consistent with parallax effects due to the Earth's accelerated motion. We show that the chi(2) surface has four distinct local minima that are induced by the "jerk-parallax'' degeneracy, with pairs of solutions having projected Einstein radii r(E) = 1.76 and 1.28 AU, respectively. This is the second event displaying such a degeneracy and the first toward the Galactic bulge. For both events, the jerk-parallax formalism accurately describes the offsets between the different solutions, giving hope that when extra solutions exist in future events they can easily be found. However, the morphologies of the chi(2) surfaces for the two events are quite different, implying that much remains to be understood about this degeneracy. C1 Korea Astron Observ, Taejon, South Korea. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chungbuk Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea. Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. Natl Astron Observ Japan, Tokyo, Japan. Univ Auckland, Dept Phys, Auckland, New Zealand. Univ Victoria, Sch Chem & Phys Sci, Wellington, New Zealand. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Natl Aerosp Lab, Tokyo, Japan. RP Park, BG (reprint author), Korea Astron Observ, 61-1 Whaam Dong, Taejon, South Korea. EM bgpark@boao.re.kr; depoy@astronomy.ohio-state.edu; sgaudi@cfa.harvard.edu; gould@astronomy.ohio-state.edu; cheongho@astroph.chungbuk.ac.kr; pogge@astronomy.ohio-state.edu; abe@stelab.nagoya-u.ac.jp; bennett@emu.phys.nd.edu; iab@roe.ac.uk; sado@stelab.nagoya-u.ac.jp; furuta@stelab.nagoya-u.ac.jp; john.hearnshaw@canterbury.ac.nz; kkamiya@stelab.nagoya-u.ac.jp; pam.kilmartin@canterbury.ac.nz; kurata@stelab.nagoya-u.ac.jp; kmasuda@stelab.nagoya-u.ac.jp; ymatsu@stelab.nagoya-u.ac.jp; muraki@stelab.nagoya-u.ac.jp; sachi.t.noda@nao.ac.jp; okajima@stelab.nagoya-u.ac.jp; nrat001@phy.auckland.ac.nz; sako@stelab.nagoya-u.ac.jp; sekiguchi@stelab.nagoya-u.ac.jp; denis.sullivan@vuw.ac.nz; sumi@astro.princeton.edu; paulonieka@hotmail.com; tyanagi@nal.go.jp; p.yock@auckland.ac.nz RI Gaudi, Bernard/I-7732-2012 NR 26 TC 22 Z9 22 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2004 VL 609 IS 1 BP 166 EP 172 DI 10.1086/420926 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832FO UT WOS:000222252900016 ER PT J AU Hynes, RI Steeghs, D Casares, J Charles, PA O'Brien, K AF Hynes, RI Steeghs, D Casares, J Charles, PA O'Brien, K TI The distance and interstellar sight line to GX 339-4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : distances; stars : individual (GX 339-4); X-rays : binaries; X-rays : individual (GX 339-4) ID LOW-DENSITY REGIONS; X-RAY TRANSIENTS; LOW-HARD STATES; BLACK-HOLE; OPTICAL SPECTROSCOPY; GRO J1655-40; GX 339-4; MILKY-WAY; CO SURVEY; HIGH-SOFT AB The distance to the black hole binary GX 339 - 4 remains a topic of debate. We examine high-resolution optical spectra of the Na D lines resolving the velocity structure along the line of sight. We find this to be complex, with at least nine components, mostly blueshifted, spanning a velocity range of nearly 200 km s(-1). The presence of components with a large blueshift rules out a nearby location and requires that the binary be located at or beyond the tangent point, implying a lower limit to the distance of similar to 6 kpc. The presence of a significant redshifted component at + 30 km s(-1) is even more intriguing, as GX 339 - 4 also has a slightly positive systemic velocity, suggesting that the source, and this cloud, could be on the far side of the Galaxy, where the radial velocities due to Galactic rotation become positive again. If this is the case, we require a distance of similar to 15 kpc. This is less secure than the 6 kpc lower limit, however. We discuss the implications of these possible distances for the outburst and quiescent luminosities, as well as the nature of the companion star, and argue that a large distance explains these characteristics. In particular, it would explain the nondetection of the companion star during the faintest states. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, Tenerife 38200, Spain. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. European So Observ, Santiago 19, Chile. RP Hynes, RI (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM rih@astro.asutexas.edu; dsteeghs@head-cfa.harvard.edu; jcv@ll.iac.es; pac@astro.soton.ac.uk; kobrien@eso.org RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 43 TC 89 Z9 89 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2004 VL 609 IS 1 BP 317 EP 324 DI 10.1086/421014 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832FO UT WOS:000222252900031 ER PT J AU Judge, PG Saar, SH Carlsson, M Ayres, TR AF Judge, PG Saar, SH Carlsson, M Ayres, TR TI A comparison of the outer atmosphere of the "flat activity'' star tau ceti (G8 V) with the Sun (G2 V) and alpha Centauri A (G2 V) SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : chromospheres; stars : coronae; stars : individual (alpha Centauri A, tau Ceti); Sun : general ID MAIN-SEQUENCE STARS; ULTRAVIOLET EMISSION-LINES; SOLAR-TYPE STARS; TRANSITION-REGION; FAR-ULTRAVIOLET; COOL STARS; HEATING MECHANISMS; RADIAL-VELOCITIES; MAGNETIC ACTIVITY; MAUNDER MINIMUM AB Driven by the desire to understand the roles of acoustic and magnetic mechanisms in heating the outer atmospheres of Sun-like stars, we compare solar UV spectra with archival STIS spectra from the Hubble Space Telescope of alpha Cen A (G2 V) and new STIS spectra of the extremely inactive dwarf star tau Cet (G8 V, V = 3.5). The activity of tau Cet shows occasional rotational modulations but no long-term cyclic variation. It may be in a phase analogous to the solar Maunder minimum. Solar disk center intensities from both the HRTS instrument and the SUMER instrument on SOHO were converted to Sun-as-a-star fluxes by using center-to-limb data from Dammasch and colleagues. The derived solar flux spectrum represents conditions near the minimum of the solar magnetic activity cycle. We find that the tau Cet line profiles differ systematically from those of the Sun and alpha Cen A. While lines formed in the middle chromospheres appear similar, the entire emission from the upper chromosphere to the middle transition region of tau Cet has lower flux densities by factors of approximate to 2, the line widths are significantly narrower, and, uniquely, the transition region lines are not significantly redshifted. The soft X-ray surface flux of tau Cet, measured between 0.1 and 2.4 keV, is approximate to 9 x 10(3) ergs cm(-2) s(-1), several times smaller than the median solar value. We also find that the UV spectrum of alpha Cen serves as a proxy for a Sun-as-a-star spectrum when the Sun is in an intermediate phase of its activity cycle but that its coronal emission may be somewhat smaller. We discuss the implications of these results for magnetic fields and heating mechanisms in the stars and speculate that tau Cet's UV spectrum might represent the solar spectrum during a grand minimum phase. C1 Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Theoret Astrophys, N-0315 Oslo, Norway. Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. RP Judge, PG (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. NR 71 TC 25 Z9 25 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 JUL 1 PY 2004 VL 609 IS 1 BP 392 EP 406 DI 10.1086/421044 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832FO UT WOS:000222252900038 ER PT J AU Konacki, M Torres, G Sasselov, DD Pietrzynski, G Udalski, A Jha, S Ruiz, MT Gieren, W Minniti, D AF Konacki, M Torres, G Sasselov, DD Pietrzynski, G Udalski, A Jha, S Ruiz, MT Gieren, W Minniti, D TI The transiting extrasolar giant planet around the star OGLE-TR-113 SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : profiles; planetary systems; stars : evolution; stars : individual (OGLE-TR-113); techniques : radial velocities ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; GALACTIC DISK; RADIAL-VELOCITIES; SOLAR PLANETS; 2001 CAMPAIGN; SEARCH; MASS; CANDIDATES; EVOLUTION AB We report the independent discovery of a new extrasolar transiting planet around OGLE-TR-113, a candidate star from the Optical Gravitational Lensing Experiment. Small radial velocity variations have been detected based on observations conducted with the MIKE spectrograph on the Magellan I (Baade) telescope at the Las Campanas Observatory (Chile) during 2003. We have also carried out a light-curve analysis incorporating new photometry and realistic physical parameters for the star. OGLE-TR-113b has an orbital period of only 1.43 days, a mass of (1.08 +/- 0.28)M(Jup), and a radius of (1.09 +/- 0.10)R(Jup). Similar parameters have been obtained very recently in an independent study by Bouchy et al., from observations taken a year later. The orbital period of OGLE- TR- 113b and the previously announced planet OGLE-TR-56b (P(orb) = 1.21 days) - the first two found photometrically - are much shorter than the apparent cutoff of close-in giant planets at 3 - 4 day periods found in high-precision radial velocity surveys. Along with a third case reported by Bouchy et al. (OGLE-TR-132b, P(orb) = 1.69 days), these objects appear to form a new class of "very hot Jupiters" that pose very interesting questions for theoretical study. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Concepcion, Dept Fis, Concepcion, Chile. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Chile, Dept Astron, Santiago, Chile. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. RP Konacki, M (reprint author), CALTECH, Div Geol & Planetary Sci, MS 150-21, Pasadena, CA 91125 USA. EM maciej@gps.caltech.edu RI Konacki, Maciej/A-1220-2007; Ruiz, Maria Teresa/I-5770-2016 OI Ruiz, Maria Teresa/0000-0002-6799-1537 NR 27 TC 100 Z9 101 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2004 VL 609 IS 1 BP L37 EP L40 DI 10.1086/422600 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832FY UT WOS:000222253900010 ER PT J AU Mohanty, S Jayawardhana, R Natta, A Fujiyoshi, T Tamura, M Navascues, DBY AF Mohanty, S Jayawardhana, R Natta, A Fujiyoshi, T Tamura, M Navascues, DBY TI Flared disks and silicate emission in young brown dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID T-TAURI-STARS; SPECTRAL ENERGY-DISTRIBUTIONS; RHO-OPHIUCHI CLOUD; CIRCUMSTELLAR DISKS; ACCRETION; DUST; OBJECTS; SPECTROSCOPY; ATMOSPHERES; MODELS AB We present mid-infrared photometry of three very young brown dwarfs located in the rho Ophiuchi star-forming region - GY 5, GY 11, and GY 310 - obtained with the Subaru 8 m telescope. All three sources were detected at 8.6 and 11.7 mum, confirming the presence of significant mid-infrared excess arising from optically thick dusty disks. The spectral energy distributions of both GY 310 and GY 11 exhibit strong evidence of flared disks; flat disks can be ruled out for these two brown dwarfs. The data for GY 5 show large scatter and are marginally consistent with both flared and flat configurations. Inner holes a few substellar radii in size are indicated in all three cases ( and especially in GY 11), in agreement with magnetospheric accretion models. Finally, our 9.7 mum flux for GY 310 implies silicate emission from small grains on the disk surface ( although the data do not completely preclude larger grains with no silicate feature). Our results demonstrate that disks around young substellar objects are analogous to those girdling classical T Tauri stars and that they exhibit a similar range of disk geometries and dust properties. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Natl Astron Observ, Subaru Telescope, Hilo, HI USA. Natl Astron Observ, Tokyo 1818588, Japan. INTA, Lab Astrofis Espacial & Fis Fundamental, E-2808 Madrid, Spain. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smohanty@cfa.harvard.edu RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 33 TC 44 Z9 44 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2004 VL 609 IS 1 BP L33 EP L36 DI 10.1086/422555 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832FY UT WOS:000222253900009 ER PT J AU Greene, J Lim, J Ho, PTP AF Greene, J Lim, J Ho, PTP TI Evidence for interactions in HI imaging of Seyfert galaxies SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; galaxies : active; galaxies : interactions ID ACTIVE GALACTIC NUCLEI; ATOMIC-HYDROGEN; COMPANIONS; ENVIRONMENT; GAS; MORPHOLOGY; FREQUENCY; NGC-7469; MERGERS; SAMPLE AB We still do not know the primary trigger of local active galactic nuclei. Tidal torques and nuclear bars are often invoked to explain gas infall onto the central supermassive black hole, but as yet neither has definitive observational support. Here we exploit the sensitivity and endurance of H I to trace the strength and prevalence of tidal interactions among Seyfert galaxies. To minimize selection biases, we survey the 27 northern Seyferts compiled in the comprehensive optical catalog of Veron-Cetty & Veron lying in the narrow redshift range 0.015 - 0.017. This paper is a detailed presentation of a subsample, including channel maps for all systems. In addition to the program objects, we also investigate galaxies imaged in the field. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 11529, Taiwan. RP Greene, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 10, Cambridge, MA 02138 USA. EM jgreene@cfa.harvard.edu; jlim@asiaa.sinica.edu.tw; ho@ca.harvard.edu NR 47 TC 4 Z9 5 U1 0 U2 1 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 JUL PY 2004 VL 153 IS 1 BP 93 EP 117 DI 10.1086/383316 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832GD UT WOS:000222254400004 ER PT J AU Kaplan, DL Frail, DA Gaensler, BM Gotthelf, EV Kulkarni, SR Slane, PO Nechita, A AF Kaplan, DL Frail, DA Gaensler, BM Gotthelf, EV Kulkarni, SR Slane, PO Nechita, A TI An X-ray search for compact central sources in supernova remnants. I. SNRS G093.3+6.9, G315.4-2.3, G084.2+0.8, and G127.1+0.5 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE pulsars : general; stars : neutron; supernova remnants; X-rays : stars ID PULSAR-WIND NEBULA; ISOLATED NEUTRON-STAR; ELECTRON-CAPTURE SUPERNOVAE; PHOTOMETRIC STANDARD STARS; GALACTIC PLANE SURVEY; SOFT GAMMA-REPEATERS; YOUNG RADIO PULSAR; PROPER-MOTION; CASSIOPEIA-A; RCW 86 AB Most astronomers now accept that stars more massive than about 9 M(.) explode as supernovae and leave stellar remnants, either neutron stars or black holes, with neutron stars being more prevalent. Recent modeling of the explosions suggests a significant diversity in the key natal properties - rotation rate, velocity, and magnetic field strength - of the resulting neutron stars that account for the association of active radio pulsars, pulsar wind nebulae, and magnetars with supernova remnants (SNRs). The discovery of a central X-ray source in Cas A, the youngest known Galactic SNR, dramatized the expected diversity. However, less than half of the SNRs within 5 kpc have identified central sources, and only three are identified as the remnants of Type Ia SNe. Here we report a systematic effort to search for compact central sources in the remaining 23 SNRs of this distance limited sample. Our search was inspired, on empirical considerations, by the enigmatic faint X-ray source in Cas A; motivated, on theoretical grounds, by the expectation that young neutron stars emit cooling X-ray emission; and made possible by the superb angular resolution offered by the Chandra X-ray mission and the sensitivity of the XMM-Newton mission. In this first paper we report Chandra observations of four SNRs (G093.3+6.9, G315.4 - 2.3, G084.2+ 0.8, and G127.1+0.5). We have undertaken a systematic optical / IR identification program of the X-ray sources detected in the field of each SNR. Foreground ( flare stars, active stars) and background ( active galactic nuclei) sources have identifiable IR/optical counterparts. In contrast, the counterparts of neutron stars ( or black holes) are expected to be very faint. We are able to account for all the well-detected X-ray sources and thus able to state with some confidence that there are no associated central sources down to a level of one-tenth of that of the Cas A central source, L(X) less than or similar to 10(31) ergs s(-1). We compare our limits with cooling curves for neutron stars and find that any putative neutron stars in these SNRs must be cooling faster than expected for traditional 1.35 M(.) neutron stars and that any putative pulsar must have low spin-down luminosities (E) over dot less than or similar to 10(34) ergs s(-1).. However, our limits are unable to constrain the presence or absence of more unusual options, such as relatively more massive neutron stars with M greater than or similar to 1.45 M(.), neutron stars with exotic interiors, or quiescent black holes. In subsequent papers, we will report on the X-ray and optical / IR observations of the remaining members of the 5 kpc sample. C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Astrophys Lab, New York, NY 10027 USA. Harvard Univ, Cambridge, MA 02138 USA. RP Kaplan, DL (reprint author), CALTECH, Dept Astron, MS-105-24, Pasadena, CA 91125 USA. EM dlk@astro.caltech.edu; dfrail@nrao.edu; bgaensler@cfa.harvard.edu; evg@astro.columbia.edu; srk@astro.caltech.edu; slane@cfa.harvard.edu; nechita@fas.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 231 TC 54 Z9 54 U1 0 U2 2 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 JUL PY 2004 VL 153 IS 1 BP 269 EP 315 DI 10.1086/421065 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832GD UT WOS:000222254400011 ER PT J AU Pardo, JR Wiedner, MC Serabyn, E Wilson, CD Cunningham, C Hills, RE Cernicharo, J AF Pardo, JR Wiedner, MC Serabyn, E Wilson, CD Cunningham, C Hills, RE Cernicharo, J TI Side-by-side comparison of Fourier transform spectroscopy and water vapor radiometry as tools for the calibration of millimeter/submillimeter ground-based observatories SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atmospheric effects; instrumentation : miscellaneous; radiative transfer; submillimeter ID ATMOSPHERIC TRANSMISSION; SUBMILLIMETER WAVELENGTHS; MAUNA-KEA; SPECTROMETER; OPACITY AB Measurement techniques to monitor the atmospheric transmission at millimeter and submillimeter wavelengths are necessary for the operation of instruments such as the Atacama Large Millimeter Array ( ALMA). Our previous Fourier transform spectroscopy (FTS) work at the Caltech Submillimeter Observatory (CSO) has shown that the atmospheric transmission spectrum can be accurately measured by this technique up to similar to 1100 GHz with a time resolution of a few minutes. An alternative technique is water vapor radiometry, generally using a few channels around the 183 GHz H2O line that can provide much finer time resolution but relies upon models to translate the derived water vapor columns into spectrum predictions over the required frequency ranges. Time resolutions of the order of 1 s are necessary to carry out phase correction in ground-based mm/submm interferometry that can easily be reached by water vapor radiometers but not by FTS. Water vapor radiometry has the added advantages of being easier to operate and having lower costs than an FTS. In this context, we initiated a comparison campaign between the CSO FTS on Mauna Kea and a three-channel 183 GHz water vapor monitor (WVM) mounted on one of the antennas of the Sub-Millimeter Array (SMA), some 250 m away. The data presented here were taken on 2002 March 3 under very dry conditions ( total precipitable water vapor zenith column, PWV, below 0.35 mm). The atmospheric transmission at microwaves (ATM) model described in a previous paper has been used to analyze the data. The primary conclusion is that for weather conditions allowing ground-based submillimeter interferometry to be carried out, the PWV can be measured with an agreement of about 0.01 mm between both instruments in timescales of several minutes, and therefore a combination of WVM plus an accurate mm/submm atmospheric model ( based on extensive FTS work) provides a suitable tool for ALMA calibration in those conditions. C1 CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infrarroja, E-28006 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England. CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infarroja, E-28006 Madrid, Spain. RP Pardo, JR (reprint author), CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infrarroja, Serrano 121, E-28006 Madrid, Spain. EM pardo@damir.iem.csic.es NR 9 TC 12 Z9 12 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2004 VL 153 IS 1 BP 363 EP 367 DI 10.1086/386550 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832GD UT WOS:000222254400013 ER PT J AU Morrison, SA Bolger, DT Sillett, TS AF Morrison, SA Bolger, DT Sillett, TS TI Annual survivorship of the sedentary Rufous-crowned sparrow (Aimophila ruficeps): No detectable effects of edge or rainfall in southern California SO AUK LA English DT Article ID LIFE-HISTORY VARIATION; BREEDING DISPERSAL; REPRODUCTIVE SUCCESS; MARKED ANIMALS; SURVIVAL RATES; FRAGMENTATION; POPULATION; HABITAT; FOOD; ABUNDANCE AB The Rufous-crowned Sparrow (Aimophila ruficeps) is a nonmigratory passerine that displays an area-sensitive distribution pattern of abundance in fragmented coastal sage-scrub habitat of southern California. To determine if habitat fragmentation negatively affected adult survival, we used Cormack-Jolly-Seber models to compare annual survival probabilities of adult sparrows breeding in habitat adjacent to urban-developed edges to those of birds breeding in the interior of large habitat expanses in San Diego County, 1997-2000. During that period, an El Nino event brought heavy rainfall to the study area, and a La Nina event brought drought. Annual survival probabilities were relatively high for a small passerine (females: 0.69 +/- 0.05 SE; males: 0.74 +/- 0.04 SE) but, given our data, did not differ between habitat types or with rainfall. Annual resighting probabilities for the birds were strongly associated with variation in rainfall, being high in the wet year and low in the dry year. Mate- and site-fidelity were apparently high, and surveys during the nonbreeding season documented that the sparrows stayed paired and on territories year-round. We hypothesize that the high apparent survivorship of this species is related to its nonmigratory habit and its tendency to curtail reproductive effort during periods of food scarcity. Although Our survivorship analysis suggests that the urban-wildland interface does not adversely affect survival of territorial Rufous-crowned Sparrows, our power to detect an effect of habitat edge on survival was low. Thus, we urge caution in concluding that edge effects do not have an ecologically important influence on survival rates in this species. C1 Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. Dartmouth Coll, Environm Studies Program, Hanover, NH 03755 USA. Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. RP Morrison, SA (reprint author), Nature Conservancy, 201 Mission St,4th Floor, San Francisco, CA 94105 USA. EM smorrison@tnc.org RI Piper, Walter/B-7908-2009 NR 73 TC 7 Z9 7 U1 1 U2 11 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD JUL PY 2004 VL 121 IS 3 BP 904 EP 916 DI 10.1642/0004-8038(2004)121[0904:ASOTSR]2.0.CO;2 PG 13 WC Ornithology SC Zoology GA 839SU UT WOS:000222806000024 ER PT J AU Lance, SL Peterson, AS Hagedorn, M AF Lance, SL Peterson, AS Hagedorn, M TI Developmental expression of aquaporin-3 in zebrafish embryos (Danio rerio) SO COMPARATIVE BIOCHEMISTRY AND PHYSIOLOGY C-TOXICOLOGY & PHARMACOLOGY LA English DT Article; Proceedings Paper CT Conference on Aquatic Animal Models of Human Disease CY SEP 29-OCT 02, 2003 CL Amer Type Culture Collect, Manassas, VA SP Univ Miami HO Amer Type Culture Collect DE cryobiology; cryopreservation; teleost fish; embryos; zebrafish; water permeability; cryoprotectant permeability; aquaporins ID WATER CHANNEL PROTEINS; XENOPUS OOCYTES; MOUSE OOCYTES; CULTURE MEDIA; GLYCEROL; TRANSPORT; IMPROVES; FAMILY; CELLS; UREA AB Fish embryos have never been successfully cryopreserved because of the low permeability of cryoprotectants into the yolk. Recently, we used aquaporin-3 fused with a green fluorescent protein (AQP3GFP) to modify the zebrafish embryo, and demonstrated that the pores functioned physiologically. This increased the water and cryoprotectant permeability of the membranes. We have continued our work on AQP3-modified embryos and here we report their developmental expression of AQP3, the success of various culture media on their survival and development, and their reproductive success. The AQP3GFP expression begins within 30 m after the mRNA AQP3GFP injection into the yolk of the 1- to 4-cell embryo. This expression is distributed in the membranes throughout the blastoderm and the yolk syncytial layer within 24 h. It diminishes after 96 h. We found no difference in the survival or normal development of embryos from AQP3GFP or wild-type adults. Additionally, zebrafish embryos did not require special culture medium to survive after AQP3GFP modification. In fact, they survived best in embryo medium (ca. 40 mOsm). Embryos reared entirely in embryo medium had a higher percent survival and a higher percent normal development than those exposed to a high osmolatity sucrose culture medium (ca. 330 mOsm). The mechanism whereby these embryos can maintain their internal osmolality in a hypoosmotic solution with water channels in their membranes is unknown. (C) 2004 Elsevier Inc. All rights reserved. C1 Colby Coll, Dept Biol, Waterville, ME 04901 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Conservat & Res Ctr, Washington, DC 20008 USA. RP Lance, SL (reprint author), Colby Coll, Dept Biol, 5720 Mayflower Hill, Waterville, ME 04901 USA. EM sllance@colby.edu RI Lance, Stacey/K-9203-2013 OI Lance, Stacey/0000-0003-2686-1733 FU NCRR NIH HHS [R1 RR08769] NR 30 TC 10 Z9 14 U1 2 U2 5 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1532-0456 J9 COMP BIOCHEM PHYS C JI Comp. Biochem. Physiol. C-Toxicol. Pharmacol. PD JUL PY 2004 VL 138 IS 3 BP 251 EP 258 DI 10.1016/j.cca.2004.08.004 PG 8 WC Biochemistry & Molecular Biology; Endocrinology & Metabolism; Toxicology; Zoology SC Biochemistry & Molecular Biology; Endocrinology & Metabolism; Toxicology; Zoology GA 873ZB UT WOS:000225319400004 PM 15533783 ER PT J AU Huisman, JM Norris, JN AF Huisman, JM Norris, JN TI A tribute to Isabella Aiona Abbott on the occasion of her 85th birthday. Happy birthday Izzie! SO CRYPTOGAMIE ALGOLOGIE LA English DT Biographical-Item C1 Murdoch Univ, Murdoch, WA 6150, Australia. Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Huisman, JM (reprint author), Murdoch Univ, Murdoch, WA 6150, Australia. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ADAC-CRYPTOGAMIE PI PARIS PA 12 RUE DE BUFFON, 75005 PARIS, FRANCE SN 0181-1568 J9 CRYPTOGAMIE ALGOL JI Cryptogam. Algol. PD JUL-SEP PY 2004 VL 25 IS 3 BP 219 EP 239 PG 21 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 881UY UT WOS:000225896100001 ER PT J AU Aronson, RB MacIntyre, IG Wapnick, CM O'Neill, MW AF Aronson, RB MacIntyre, IG Wapnick, CM O'Neill, MW TI Phase shifts, alternative states, and the unprecedented convergence of two reef systems SO ECOLOGY LA English DT Article DE acropora; agaricia; alternative states; Belize; coral reef; holocene; paleoecology; Panama; phase shift; porites; species dominance; species turnover ID CARIBBEAN CORAL-REEF; BOCAS DEL TORO; COMMUNITY STRUCTURE; FRINGING REEFS; STABLE STATES; WEST-INDIES; BELIZE; PANAMA; EXTINCTION; ISLANDS AB Initial conditions can generate differences in the biotic composition of spatially disjunct communities, but intense, large-scale perturbations have the potential to reduce or eliminate those historical differences. The latter possibility is of particular concern with respect to coral reefs, which have undergone dramatic changes in the last 25-30 years. This paper reports a case in which two reef systems with different biotic histories were recently perturbed to a single, novel state. We compared millennial-scale records of species dominance from reefs in Bahia Almirante, a coastal lagoon in northwestern Panama, to previously published records from reefs in the shelf lagoon of Belize. Reef cores extracted from Bahia Almirante at 5-10 in water depth revealed that the Panamanian reefs were persistently dissimilar from the Belizean reefs for at least 2000-3000 years prior to the last several decades. The Panamanian reefs were dominated continuously by branching finger corals, Porites spp. (primarily P. furcata). Shifts from the Porites-dominated state to dominance by other coral species were rare, were restricted to small areas, and lasted for decades to centuries. The Belizean reefs were dominated continuously by the staghorn coral Acropora cervicornis in the same depth range during the same period. Excursions from the Acropora-dominated state were again rare and spatially localized. Populations of Ac. cervicornis in the Belizean lagoon were nearly extirpated by an outbreak of white-band disease in the late 1980s, and changes in water quality were apparently detrimental to branching Porites in Bahia Almirante in recent decades. These large-scale perturbations caused the two reef systems to converge on a third, historically unprecedented state: dominance by the lettuce coral Agaricia tenuifolia. Ag. tenuifolia possesses life-history attributes and environmental tolerances that enabled it to become dominant in both disturbed ecosystems. Although the two phase shifts to Ag. tenuifolia differed in both their general mechanisms and specific causes, they had the effect of eliminating the salient difference in benthic composition between the Panamanian and Belizean reefs. The changes in species composition thus obliterated the influence of several thousand years of reef history. C1 Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA. Univ S Alabama, Dept Marine Sci, Mobile, AL 36688 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Aronson, RB (reprint author), Dauphin Isl Sea Lab, 101 Bienville Blvd, Dauphin Isl, AL 36528 USA. EM raronson@disl.org NR 66 TC 103 Z9 112 U1 1 U2 28 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD JUL PY 2004 VL 85 IS 7 BP 1876 EP 1891 DI 10.1890/03-0108 PG 16 WC Ecology SC Environmental Sciences & Ecology GA 843VA UT WOS:000223113500022 ER PT J AU Collin, R AF Collin, R TI Phylogenetic effects, the loss of complex characters, and the evolution of development in calyptraeid gastropods SO EVOLUTION LA English DT Article DE comparative biology; Crepidula; Crucibulum; mode of development; nurse eggs ID MARINE-INVERTEBRATES; LARVAL DEVELOPMENT; PATTERNS; MODE; POECILOGONY; CREPIDULA; SELECTION AB Despite considerable theoretical and empirical work on the population genetic effects of mode of development in benthic marine invertebrates, it is unclear what factors generate and maintain interspecific variation in mode of development and few studies have examined such variation in a phylogenetic context. Here I combine data on mode of development with a molecular phylogeny of 72 calyptraeid species to test the following hypotheses about the evolution of mode of development: (1) Is the loss of feeding larvae irreversible? (2) Is there a phylogenetic effect on the evolution of mode of development? (3) Do embryos of direct-developing species lose the structures necessary for larval feeding and swimming and, if so, is the degree of embryonic modification correlated with the genetic distance between species? The results of these analyses suggest that mode of development evolves rapidly and with little phylogenetic inertia. There are three cases of the possible regain of feeding larvae, in all cases from direct development with nurse eggs. It appears that species with planktotrophic, lecithotrophic, or direct development with nurse eggs all have equal evolutionary potential and retain the possibility of subsequent evolution of a different mode of development. However, species with direct development from large yolky eggs appear to be subject to phylogenetic constraints and may not be able to subsequently evolve a different mode of development. Finally, species that have more recently evolved direct development have less highly modified embryos than older direct-developing species. Since species with nurse eggs generally have fewer embryonic modifications than those from large yolky eggs, this embryological difference may be the underlying cause of the difference in evolutionary potential. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. Field Museum, Dept Zool, Chicago, IL 60605 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, APO,Unit 0948,AA, Miami, FL 34002 USA. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010; OI Collin, Rachel/0000-0001-5103-4460 NR 40 TC 70 Z9 72 U1 1 U2 13 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD JUL PY 2004 VL 58 IS 7 BP 1488 EP 1502 PG 15 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 842DI UT WOS:000222982800008 PM 15341151 ER PT J AU Maslakova, SA Martindale, MQ Norenburg, JL AF Maslakova, SA Martindale, MQ Norenburg, JL TI Vestigial prototroch in a basal nemertean, Carinoma tremaphoros (Nemertea; Palaeonemertea) SO EVOLUTION & DEVELOPMENT LA English DT Article ID SPIRALIAN DEVELOPMENTAL PROGRAM; CELL-LINEAGE; PHYLOGENETIC SIGNIFICANCE; TROCHOPHORAN LARVAE; PERICALYMMA LARVA; EVOLUTION; MOLLUSCA; PATELLA; MORPHOLOGY; ULTRASTRUCTURE AB Nemerteans have been alleged to belong to a protostome clade called the Trochozoa that includes mollusks, annelids, sipunculids, echiurids, and kamptozoans and is characterized by, among other things, the trochophore larva. The trochophore possesses a prototroch, a preoral belt of specialized ciliary cells, derived from the trochoblast cells. Nemertea is the only trochozoan phylum for which presence of the trochophore larva possessing a prototroch had never been shown. However, so little is known about nemertean larval development that comparing it with development of other trochozoans is difficult. Development in the nemertean clade Pilidiophora is via a highly specialized planktonic larva, the pilidium, and most of the larval body is lost during a drastic metamorphosis. Other nemerteans (hoplonemerteans and palaeonemerteans) lack a pilidium, and their development is direct, forming either an encapsulated or planktonic "planuliform" larva, producing a juvenile without a dramatic change in body plan. We show that early in the development of a member of a basal nemertean assemblage, the palaeonemertean Carinoma tremaphoros, large squamous cells cover the entire larval surface except for the apical and posterior regions. Although apical and posterior cells continue to divide, the large surface cells cleavage arrest and form a contorted preoral belt. Based on its position, cell lineage, and fate, we suggest that this belt corresponds to the prototroch of other trochozoans. Lack of differential ciliation obscures the presence of the prototroch in Carinoma, but differentiation of the trochoblasts is clearly manifested in their permanent cleavage arrest and ultimate degenerative fate. Our results allow a meaningful comparison between the development of nemerteans and other trochozoans. We review previous hypotheses of the evolution of nemertean development and suggest that a trochophore-like larva is plesiomorphic for nemerteans while a pilidium type of development with drastic metamorphosis is derived. C1 Smithsonian Inst, Natl Museum Nat Hist, MRC 163, Washington, DC 20013 USA. Univ Hawaii, Kewalo Marine Lab, Honolulu, HI 96813 USA. George Washington Univ, Dept Biol, Washington, DC 20052 USA. RP Maslakova, SA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 163, POB 37012, Washington, DC 20013 USA. EM maslak@gwu.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 56 TC 63 Z9 67 U1 0 U2 5 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 1520-541X J9 EVOL DEV JI Evol. Dev. PD JUL-AUG PY 2004 VL 6 IS 4 BP 219 EP 226 DI 10.1111/j.1525-142X.2004.04027.x PG 8 WC Evolutionary Biology; Developmental Biology; Genetics & Heredity SC Evolutionary Biology; Developmental Biology; Genetics & Heredity GA 833WM UT WOS:000222371500002 PM 15230962 ER PT J AU McCoy, T AF McCoy, T TI Meteorites SO GEOTIMES LA English DT Article C1 Smithsonian Inst, Natl Meteorite Collect, Washington, DC 20560 USA. RP McCoy, T (reprint author), Smithsonian Inst, Natl Meteorite Collect, Washington, DC 20560 USA. EM mccoy.tim@nmnh.si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 USA SN 0016-8556 J9 GEOTIMES JI Geotimes PD JUL PY 2004 VL 49 IS 7 BP 44 EP 46 PG 3 WC Geosciences, Multidisciplinary SC Geology GA 836HF UT WOS:000222545800048 ER PT J AU Haggis, DC Mook, MS Scarry, CM Snyder, LM West, WC AF Haggis, DC Mook, MS Scarry, CM Snyder, LM West, WC TI Excavations at Azoria, 2002 SO HESPERIA LA English DT Review ID ITANOS EASTERN CRETE; ARCHAEOLOGICAL RESEARCH; KAVOUSI; COLLABORATION; KASTRO; PERSPECTIVE; VROKASTRO; ECONOMY; POTTERY; AREA AB This report summarizes the results of the first season of excavation at Azoria in eastern Crete and provides an overview of the project's goals and problem orientation. Work in 2002 concentrated on the peak of the South Acropolis and the occupational phases of the seventh-sixth centuries B.C. The recovery of a possible andreion complex suggests the urban character of the site in the sixth century and forms a starting point for discussing the political economy of the Archaic city. The excavations revealed important evidence for the organization of the sixth-century settlement and for the complex stratigraphic history of the site, including the Final Neolithic, Late Prepalatial, Early Iron Age, Archaic, and Hellenistic periods. C1 Univ N Carolina, Dept Class, Chapel Hill, NC 27599 USA. Iowa State Univ, Class Studies Program, Ames, IA 50011 USA. Univ N Carolina, Dept Anthropol, Chapel Hill, NC 27599 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Washington, DC 20560 USA. RP Haggis, DC (reprint author), Univ N Carolina, Dept Class, 212 Murphy Hall,CB 3145, Chapel Hill, NC 27599 USA. EM dchaggis@email.unc.edu; msmook@iastate.edu; scarry@email.unc.edu; snyder.lynn@nmnh.si.edu; wwest@email.unc.edu NR 177 TC 21 Z9 21 U1 0 U2 0 PU AMER SCHOOL CLASSICAL STUDIES AT ATHENS PI PRINCETON PA 6-8 CHARLTON STREET, PRINCETON, NJ 08540-5232 USA SN 0018-098X J9 HESPERIA JI Hesperia PD JUL-SEP PY 2004 VL 73 IS 3 BP 339 EP 400 DI 10.2972/hesp.2004.73.3.339 PG 62 WC Archaeology SC Archaeology GA 892FT UT WOS:000226636200001 ER PT J AU Hawke, BR Blewett, DT Lucey, PG Smith, GA Bell, JF Campbell, BA Robinson, MS AF Hawke, BR Blewett, DT Lucey, PG Smith, GA Bell, JF Campbell, BA Robinson, MS TI The origin of lunar crater rays SO ICARUS LA English DT Article DE moon; surface; impact processes; cratering; spectroscopy; radar ID SOLAR-SYSTEM; MOON; STRATIGRAPHY; COPERNICUS; REFLECTANCE; ABUNDANCE; MATURITY; IMPACT; IMAGES; REGION AB Lunar rays are filamentous, high-albedo deposits occurring radial or subradial to impact craters. The nature and origin of lunar rays have long been the subjects of major controversies. We have determined the origin of selected lunar ray segments utilizing Earth-based spectral and radar data as well as FeO, TiO2, and optical maturity maps produced from Clementine UVVIS images. These include rays associated with Tycho. Olbers A, Lichtenberg, and the Messier crater complex. It was found that lunar rays are bright because of compositional contrast with the surrounding terrain, the presence of immature material, or some combination of the two. Mature "compositional" rays such as those exhibited by Lichtenberg crater, are due entirely to the contrast in albedo between ray material containing highlands-rich primary ejecta and the adjacent dark mare surfaces. "Immaturity" rays are bright due to the presence of fresh, high-albedo material. This fresh debris was produced by one or more of the following: (1) the emplacement of immature primary ejecta, (2) the deposition of immature local material from secondary craters, (3) the action of debris surges downrange of secondary clusters, and (4) the presence of immature interior walls of secondary impact craters. Both composition and state-of-maturity play a role in producing a third ("combination") class of lunar rays, The working distinction between the Eratosthenian and Copernican Systems is that Copernican craters still have visible rays whereas Eratosthenian-aged craters do not. Compositional rays can persist far longer than 1.1 Ga, the currently accepted age of the Copernican-Eratosthenian boundary. Hence, the mere presence of rays is not a reliable indication of crater age. The optical maturity parameter should be used to define the Copernican-Eratosthenian boundary. The time required for an immature surface to reach the optical maturity index saturation point could be defined as the Copernican Period. (C) 2004 Elsevier Inc. All rights reserved. C1 Univ Hawaii, Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. NovaSol, Honolulu, HI 96813 USA. Cornell Univ, Dept Astron, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. Northwestern Univ, Ctr Planetary Sci, Evanston, IL 60208 USA. RP Hawke, BR (reprint author), Univ Hawaii, Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, 1680 EW Rd, Honolulu, HI 96822 USA. EM hawke@higp.hawaii.edu RI Blewett, David/I-4904-2012 OI Blewett, David/0000-0002-9241-6358 NR 51 TC 59 Z9 68 U1 1 U2 5 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 JUL PY 2004 VL 170 IS 1 BP 1 EP 16 DI 10.1016/j.icarus.2004.02.013 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 830ZK UT WOS:000222162500001 ER PT J AU Jousselin, E Kjellberg, F Herre, EA AF Jousselin, E Kjellberg, F Herre, EA TI Flower specialization in a passively pollinated monoecious fig: A question of style and stigma? SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE allometry; coevolution; mutualism; pollination; style/stigma relationship ID HYMENOPTERA CHALCIDOIDEA; WASP MUTUALISM; FICUS MORACEAE; COEVOLUTION; DEPOSITION; EVOLUTION; CONFLICT; SEED AB The stability of the mutualism between figs and their pollinator wasps depends on the patterns of seed and wasp production. In Ficus maxima, a passively pollinated monoecious fig, we estimated the correlations among different flower characteristics and determined their relationships with pollination success and pollinator oviposition. Across flowers, stigma length shows an allometric relationship with style length, and style length correlates negatively with style width. Longer-styled flowers are more likely to be pollinated and receive higher pollen loads. This is probably explained by their larger stigmatic surface that increases their chance of receiving the passively dispersed pollen. Consistent with findings in other species, flowers with longer styles are less likely to receive a pollinator's egg. This oviposition pattern is probably explained by a combination of factors: ( 1) wasps ovipositor are too short to reach flowers with extremely long styles, and 17% of flowers are inaccessible; ( 2) sometimes, there are too few pollinators to use all accessible flowers; ( 3) oviposition is more difficult through the long stigmas and thin styles associated with long-styled flowers. Given the patterns of pollinator egg distribution, the style/stigma size relationship in F. maxima appears advantageous for the fig since it leads to preferential pollination of flowers that are not used by wasps. It might reflect flower functional specialization and contribute to the mutualism stability. C1 Univ Pretoria, Dept Genet, ZA-0002 Pretoria, South Africa. CNRS, Ctr Ecol Fonct & Evolut, F-34293 Montpellier 5, France. Smithsonian Trop Res Inst, Balboa, Panama. RP Jousselin, E (reprint author), INRA, Ctr Biol & Gest Populat, Campus Int Baillarguet,CS 30016, F-34988 Montferrier Sur Lez, France. EM ejousselin@yahoo.com NR 45 TC 18 Z9 22 U1 0 U2 9 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 EI 1537-5315 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD JUL PY 2004 VL 165 IS 4 BP 587 EP 593 DI 10.1086/386558 PG 7 WC Plant Sciences SC Plant Sciences GA 855IY UT WOS:000223968000011 ER PT J AU Suarez-Morales, E Reid, JW Fiers, F Iliffe, TM AF Suarez-Morales, E Reid, JW Fiers, F Iliffe, TM TI Historical biogeography and distribution of the freshwater cyclopine copepods (Copepoda, Cyclopoida, Cyclopinae) of the Yucatan Peninsula, Mexico SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE limnology; distributional patters; freshwater biogeography; karstic environments; zooplankton ID CRUSTACEA; AMERICAN; MESOCYCLOPS; EVOLUTION; RECORDS; CLIMATE; FAUNA; SARS AB Aim To determine and analyse the distribution of the freshwater cyclopine copepod fauna of the Yucatan Peninsula (YP) and its relationship with the geological and climatic history of this Neotropical karstic zone. Location The Yucatan Peninsula, Mexico. Methods Plotting of georeferenced sites, analysis of local and regional geological and climatic history, analysis and comparison of regional and local faunistic records. Results Distinct dispersal and/or vicariant processes seem to be linked to the current distributions of the seven genera known in the YP. In general, the endemic hypogean or benthic crevicular forms (i.e. Diacyclops chakan, D. puuc and Mesocyclops chaci), derived from epigean, tropical, widely distributed forms (some of them South American) may have been among the earliest colonizers of the subterranean habitats in the YP. The distribution of these and other endemic forms seem to be related to the Holocene dry periods that desiccated the largest bodies of water and isolated local populations of different species. These vicariant processes resulted in forms with restricted distributional areas; some of these formed sister species that speciated in geographically close localities but related to a common identifiable ancestor. Overall, the processes of cyclopine colonization of the YP show the influence of the South American fauna, as the closest relatives of some species endemic to the YP are South American forms; the Nearctic influence is low. The cyclopine fauna of the YP is formed by a mixture of Nearctic-derived (species of Acanthocyclops), Neotropical (i.e. M. edax, M. longisetus, A. panamensis, Thermocyclops inversus and T. tenuis), and epigean and hypogean endemic forms. The highly dynamic geomorphology of the YP and the recent climatic changes in the Holocene define the YP as a peculiar subregion that harbours a diverse fauna of cyclopine copepods with a high endemism. Main conclusion The current distribution of cyclopine copepods reflects relatively recent, post-Pliocene biogeographical patterns; probably older patterns are involved as well. The eastern coast of the Yucatan is the most recently colonized by cyclopine copepods. Most of the genera are linked with South American forms, and the Nearctic influence is weakly represented. This group has no marine relatives, but there is evidence of vicariant events involving cave-dwelling forms. C1 Colegio Frontera Sur ECOSUR, Chetmal 77000, Quintana Roo, Mexico. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC USA. Virginia Museum Nat Sci, Martinsville, VA USA. Royal Belgian Inst Nat Sci, Invertebrate Sect, Brussels, Belgium. Texas A&M Univ, Dept Marine Biol, Galveston, TX 77553 USA. RP Suarez-Morales, E (reprint author), Colegio Frontera Sur ECOSUR, Km 5-5,Av Centenario, Chetmal 77000, Quintana Roo, Mexico. EM esuarez@ecosur-qroo.mx NR 51 TC 24 Z9 28 U1 0 U2 7 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 JUL PY 2004 VL 31 IS 7 BP 1051 EP 1063 DI 10.1111/j.1365-2699.2004.01053.x PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 827NM UT WOS:000221906700002 ER PT J AU Vila, R Iglesias, J Canigueral, S Santana, AI Solis, PN Gupta, MP AF Vila, R Iglesias, J Canigueral, S Santana, AI Solis, PN Gupta, MP TI Constituents and biological activity of the essential oil of Eugenia acapulcensis Steud. SO JOURNAL OF ESSENTIAL OIL RESEARCH LA English DT Article DE Eugenia acapulcensis; Myrtaceae; essential oil composition ID MEXICO AB The essential oil from leaves of Eugenia acapulcensis Steud. obtained by hydrodistillation was analyzed by GC and GC/MS. From the MS data and retention indices obtained 56.7% of the oil consisting of 47 components could be identified. Eighty-five percent of the analyzed oil was comprised of sesquiterpenes, either hydrocarbons or oxygenated, among which alpha-cadinol (4.2%), spathulenol (4.2%), delta-cadinene (3.8%) and (Z)-nerolidol (3.5%) were the main ones. The oxygenated monoterpene trans-pinocarveol (4.2%) was also found as a major component of the oil. C1 Univ Barcelona, Fac Farm, Unitat Farmacol & Farmacognosia, E-08028 Barcelona, Spain. Univ Panama, Fac Farm, CIFLORPAN, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. RP Vila, R (reprint author), Univ Barcelona, Fac Farm, Unitat Farmacol & Farmacognosia, Avda Diagonal 643, E-08028 Barcelona, Spain. RI Canigueral, Salvador/O-2767-2013; OI Canigueral, Salvador/0000-0001-5056-489X; Gupta, Mahabir/0000-0002-9302-7864 NR 18 TC 5 Z9 6 U1 0 U2 0 PU ALLURED PUBL CORP PI CAROL STREAM PA 362 S SCHMALE RD, CAROL STREAM, IL 60188-2787 USA SN 1041-2905 J9 J ESSENT OIL RES JI J. Essent. Oil Res. PD JUL-AUG PY 2004 VL 16 IS 4 BP 384 EP 386 PG 3 WC Chemistry, Applied; Food Science & Technology SC Chemistry; Food Science & Technology GA 836UI UT WOS:000222580900031 ER PT J AU Snoeyenbos-West, OLO Cole, J Campbell, A Coats, DW Katz, LA AF Snoeyenbos-West, OLO Cole, J Campbell, A Coats, DW Katz, LA TI Molecular phylogeny of phyllopharyngean ciliates and their group I introns SO JOURNAL OF EUKARYOTIC MICROBIOLOGY LA English DT Article DE Chonotrichia; Ciliophora; group I introns; molecular genealogy; phyllopharyngea; ssu-rDNA; suctoria ID RIBOSOMAL-RNA GENE; EUKARYOTIC DIVERSITY; ACTIVE-SITE; CILIOPHORA; SEQUENCES; EVOLUTION; POSITION; DNA; SYSTEMATICS; FRAGMENTATION AB We analyzed small subunit ribosomal DNA (ssu-rDNA) sequences to evaluate both the monophyly of the ciliate class Phyllopharyngea de Puytorac et al. (1974), and relationships among subclasses. Classifications based on morphology and ultrastructure divide the Phyllopharyngea into four subclasses, the Phyllopharyngia, Chonotrichia, Rhynchodia, and Suctoria. Our analyses of ssu-rDNA genealogies derived from sequence data collected from diverse members representing three of the four subclasses of Phyllopharyngea (Suctoria: Ephelota spp., Prodiseophyra collini, Acineta sp.; Phyllopharyngia: Chlamydodon exocellatus, Chlamydodon tri-quetrus, Dysteria sp.; and Chonotrichia: Isochona sp.) provide strong support for the monophyly of the Phyllopharyngea, and show that the Chonotrichia emerge from within the Phyllopharyngia. Based on this initial sampling, suctorian budding types are monophyletic, and exogenous budding appears to be basal to evaginative and endogenous budding. Further, we report the discovery of a group I intron at position 891 in the Suctoria Acineta sp. and Tokophrya lemnarum, and a second group I intron at position 1506 in T. lemnarum. These introns represent only the second examples of group I introns in a ciliate ribosomal gene, since the discovery of ribozymes in the LSU rRNA gene of Tetrahymena thermophila. Phylogenetic analyses of Group I introns suggest a complex evolutionary history involving either multiple loses or gains of introns within endogenously budding Suctoria. C1 Smith Coll, Dept Biol Sci, Northampton, MA 01063 USA. Amer Type Culture Collect, Protistol Collect, Manassas, VA USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Massachusetts, Program Organ & Evolut Biol, Amherst, MA 01003 USA. RP Katz, LA (reprint author), Smith Coll, Dept Biol Sci, Northampton, MA 01063 USA. EM Lkatz@Smith.edu OI Snoeyenbos-West, Oona/0000-0001-9146-7244 NR 58 TC 23 Z9 24 U1 0 U2 8 PU SOC PROTOZOOLOGISTS PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 1066-5234 J9 J EUKARYOT MICROBIOL JI J. Eukaryot. Microbiol. PD JUL-AUG PY 2004 VL 51 IS 4 BP 441 EP 450 DI 10.1111/j.1550-7408.2004.tb00392.x PG 10 WC Microbiology SC Microbiology GA 841UO UT WOS:000222957300009 PM 15352327 ER PT J AU Buzas, MA AF Buzas, MA TI Community structure of foraminifera from two Miocene beds at Calvert Cliffs, Maryland SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID DIVERSITY AB On each of two horizontal beds in the Miocene sediments at Calvert Cliffs, Maryland, nine stations were placed in an equally spaced grid. At each station five samples were taken at random, and in each sample individuals were identified to species and counted. A list of species proportions or relative abundances constitutes a vector, p, with rank S = species richness. The statistical distribution of p is defined as the community structure. To identify community structure, species abundances are cumulated in successive samples and the species richness, S, the information function, H, and the evenness, E, are evaluated at each stage. The graph or curve of the cumulated frequency, the distribution function, is identifiable for various statistical distributions and allows for community structure identification. The entire procedure is called SHE analysis for community structure identification, SHECSI. For a log series distribution, the regression on the cumulated frequency InS = a + blnE has a value of slope b = -1 and of intercept a = H. The results obtained from both beds at Calvert Cliffs are in agreement with the expectation of a log series distribution. Comparison of the results from these fossil populations with results from living and total populations indicates that a log series distribution is the expected distribution for the structure of living and fossil shallow-water foraminiferal communities. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Buzas, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM buzas.marty@nmnh.si.edu NR 31 TC 10 Z9 11 U1 0 U2 3 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 JUL PY 2004 VL 34 IS 3 BP 208 EP 213 DI 10.2113/34.3.208 PG 6 WC Paleontology SC Paleontology GA 849SQ UT WOS:000223561400003 ER PT J AU Touwaide, A AF Touwaide, A TI Arabic urology in Byzantium SO JOURNAL OF NEPHROLOGY LA English DT Article; Proceedings Paper CT 4th Congress of the International-Association-for-the-History-of-Nephrology CY APR 24-27, 2003 CL CASSINO, ITALY SP Int Assoc Hist Nephrol DE Byzantium; The Arabic world; The middle ages; translations AB Byzantine manuscripts contain texts that are explicitly presented - or can be identified - as translations from Arabic. The present article offers a general description of these texts and a first approach to their urological contents. C1 Washington Acad Sci, Washington, DC USA. Smithsonian Inst, Washington, DC 20560 USA. RP Touwaide, A (reprint author), POB 25805, Washington, DC 20027 USA. EM atouwaide@hotmail.com NR 8 TC 3 Z9 3 U1 0 U2 0 PU WICHTIG EDITORE PI MILAN PA 72/74 VIA FRIULI, 20135 MILAN, ITALY SN 1121-8428 J9 J NEPHROL JI J. Nephrol. PD JUL-AUG PY 2004 VL 17 IS 4 BP 583 EP 589 PG 7 WC Urology & Nephrology SC Urology & Nephrology GA 854KV UT WOS:000223902600017 PM 15372424 ER PT J AU Dimichele, WA Hook, RW Nelson, WJ Chaney, DS AF Dimichele, WA Hook, RW Nelson, WJ Chaney, DS TI An unusual Middle Permian flora from the Blaine Formation (Pease River Group : Leonardian-Guadalupian Series) of King County, West Texas SO JOURNAL OF PALEONTOLOGY LA English DT Article ID NORTH-CENTRAL TEXAS; GUIZHOU PROVINCE; CHINA; GIGANTOPTERIDALES; PALEOBOTANY; TRANSITION; ANATOMY; PLANTS; GEN. AB A new Middle Permian plant assemblage from South Ash Pasture in King County, Texas, may be the youngest and is certainly the Most unusual flora known from the Permian of either West Texas or adjoining north-central Texas. Found serendipitously in the evaporite-rich upper Blaine Formation (Pease River Group, Guadalupian Series), the flora is of very low diversity despite intensive collecting efforts. and the affinities of nearly all taxa are enigmatic. The most common elements are parallel-veined leaves that resemble cordaites but that could be isolated pinnules of a pinnate leaf. Gigantopterid foliage is present but not assignable to any known taxon. A single foliar conifer specimen is too incomplete for assignment. Numerous reproductive organs, however, and an abundance of axes may represent conifers. Conchostracans, palaeoniscoid fish scales, and small heteropolar coprolites also occur in the deposit, which originated as a small, claystone-dominated channel fill in a coastal plain setting. C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Texas, Lab Vertebrate Paleontol, Texas Mem Museum, Austin, TX 78712 USA. Illinois State Geol Survey, Champaign, IL 61820 USA. RP Dimichele, WA (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM dimicheIe.bill@nmnh.si.edu; cacops@ccwf.cc.utexas.edu; jnelson@geoserv.isgs.uiuc.edu; chaney.dan@nmnh.si.edu RI DiMichele, William/K-4301-2012 NR 52 TC 34 Z9 35 U1 1 U2 3 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 2004 VL 78 IS 4 BP 765 EP 782 DI 10.1666/0022-3360(2004)078<0765:AUMPFF>2.0.CO;2 PG 18 WC Paleontology SC Paleontology GA 836UF UT WOS:000222580600012 ER PT J AU Roubik, DW AF Roubik, DW TI Sibling species of Glossura and Glossuropoda in the Amazon region (Hymenoptera : Apidae : Euglossini) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE Euglossa; Glossura; Glossuropoda; sibling species; Amazon; orchid bees AB The Euglossa subgenus Glossuropoda is examined and males of three species described, Euglossa inflata sp. nov., a small bee apparently endemic to the Guianas, E. rugilabris stat. nov., a euglossine with proportionally the longest tongue, and E. cyanochlora stat. nov., the largest Euglossa and a sibling species to the widespread E. (G.) intersecta, endemic to Bahia, Brazil. E. (Glossuropoda) juremae is synonymized under E. hugonis, sibling to E. rugilabris, and E. (Glossuropoda) nigrosignata is given new status. In the subgenus Glossura, the male of E. piliventris is described and suggested as a sibling species to E. lugubris sp. nov., being of the eastern and western Amazon, respectively. Euglossa orellana sp. nov. and E. occidentalis sp. nov. are described, both widely misidentified as E. chalybeata, which to varying degree with that species, E. flammea, E. ignita, E. imperialis, and possibly E. iopoecila stat. nov. may be considered sibling species. Euglossa tiputini sp. nov., of the E. piliventris group, is a close mimic of E. intersecta in the western Amazon region. C1 Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Roubik, DW (reprint author), Smithsonian Trop Res Inst, Balboa 2072, Panama. NR 17 TC 39 Z9 44 U1 3 U2 10 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JUL PY 2004 VL 77 IS 3 BP 235 EP 253 DI 10.2317/0308.20.1 PG 19 WC Entomology SC Entomology GA 844UW UT WOS:000223187300009 ER PT J AU Iwaniuk, AN Nelson, JE James, HF Olson, SL AF Iwaniuk, AN Nelson, JE James, HF Olson, SL TI A comparative test of the correlated evolution of flightlessness and relative brain size in birds SO JOURNAL OF ZOOLOGY LA English DT Article DE brain size; flightless; comparative method; correlated evolution; birds ID PHYLOGENETIC-RELATIONSHIPS; INDEPENDENT EVOLUTION; NUCLEUS ROTUNDUS; SEQUENCE DATA; ECOLOGY; BIOGEOGRAPHY; WATERFOWL; MAMMALS; DUCKS; MORPHOMETRICS AB Secondary flightlessness has evolved independently many times in birds. Morphological changes in the pectoral girdle and flight feathers and changes in body size have been associated with the evolution of flightlessness, and it has also been suggested that flightless birds have relatively small brains. We therefore tested whether flightlessness is related to changes in relative brain size. Relative brain size was compared between volant and flightless species using both conventional statistics and modern comparative methods within nine taxonomic groups. No significant difference was found between flightless and volant species in six of these groups, regardless of whether body mass or tibiotarsal measurements were used as estimates of body size. Species with relatively smaller brains compared with their volant relatives were the great auk Pinguinus impennis, the kakapo Strigops habroptilus and some species of penguin. Thus, we found no evidence of a general correlation between the evolution of secondary flightlessness and the evolution of relatively small brains in birds. This suggests that neural requirements are not significantly different between flightless and volant species, although our methods may have overlooked subtle neurological changes that do not result in markedly different endocranial volumes. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. Monash Univ, Sch Biol Sci, Clayton, Vic 3168, Australia. RP Iwaniuk, AN (reprint author), Univ Alberta, Dept Psychol, Edmonton, AB T6G 2E9, Canada. EM brainsize@yahoo.ca NR 68 TC 24 Z9 25 U1 7 U2 36 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0952-8369 J9 J ZOOL JI J. Zool. PD JUL PY 2004 VL 263 BP 317 EP 327 DI 10.1017/S0952836904005308 PN 3 PG 11 WC Zoology SC Zoology GA 841CY UT WOS:000222908100011 ER PT J AU Hutchinson, A AF Hutchinson, A TI No turning back: The life and death of animal species. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Hutchinson, A (reprint author), Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUL PY 2004 VL 129 IS 12 BP 113 EP 113 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 836RH UT WOS:000222572800336 ER PT J AU Aiello, A AF Aiello, A TI The Monarch butterfly: Biology & conservation. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. NR 1 TC 0 Z9 0 U1 1 U2 6 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUL PY 2004 VL 129 IS 12 BP 114 EP 114 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 836RH UT WOS:000222572800341 ER PT J AU Allan, GJ Francisco-Ortega, J Santos-Guerra, A Boerner, E Zimmer, EA AF Allan, GJ Francisco-Ortega, J Santos-Guerra, A Boerner, E Zimmer, EA TI Molecular phylogenetic evidence for the geographic origin and classification of Canary Island Lotus (Fabaceae : Loteae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Macaronesia; Canary Islands; Lotus; molecular phylogeny; ITS ID NUCLEAR RIBOSOMAL DNA; GENUS ARGYRANTHEMUM ASTERACEAE; INTERNAL TRANSCRIBED SPACERS; SEQUENCE DATA; EVOLUTION; COLONIZATION; MACARONESIA; PATTERNS; SYSTEMATICS; CHROMOSOME AB Molecular phylogenetic analyses of Macaronesian Lotus and related genera were conducted to assess their biogeographic history and taxonomy. Macaronesian Lotus, which are typically classified within one of two subgenera, Lotus subgenus Pedrosia or L. subg. Rhyncholotus, are diagnosed by the presence of a forked or toothed style and differences in corolla morphology. Maximum parsimony and Bayesian analyses of internal transcribed spacer sequences identify a well-supported northwest African-Cape Verde Island clade that includes all members of Lotus subgenus Pedrosia + L. subg. Rhyncholotus. There is modest support for two independently nested clades containing the Canary Island species and two non-Canarian species, Lotus assakensis from Africa and Lotus azoricus endemic to the Azores. Biogeographic reconstruction based on a parsimony topology unequivocally identifies an African origin for the Canary Island group with subsequent back dispersal to the African continent and a single dispersal event to the Azores. A phylogeographic assessment of colonization and diversification patterns suggests that geographic isolation via interisland colonization of ecologically similar habitats is the primary mode of species diversification in Canary Island Lotus. (C) 2003 Elsevier Inc. All rights reserved. C1 No Arizona Univ, Dept Sci Biol, Flagstaff, AZ 86011 USA. Florida Int Univ, Dept Sci Biol, Miami, FL 33199 USA. Fairchild Trop Gdn, Res Ctr, Miami, FL 33156 USA. Jardin Aclimat Orotava, E-38400 Tenerife, Spain. Arcadia Univ, Biol Dept, Glenside, PA 19038 USA. Natl Museum Nat Hist, Smithsonian Inst, Lab Analyt Biol, Museum Support Ctr, Suitland, MD 20746 USA. RP Allan, GJ (reprint author), No Arizona Univ, Dept Sci Biol, S Beaver St,Bldg 21, Flagstaff, AZ 86011 USA. EM gery.allan@nau.edu RI Zimmer, Elizabeth/G-3890-2011 NR 78 TC 63 Z9 66 U1 0 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD JUL PY 2004 VL 32 IS 1 BP 123 EP 138 DI 10.1016/j.ympev.2003.11.018 PG 16 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 832TZ UT WOS:000222291400011 PM 15186802 ER PT J AU Kawakita, A Sota, T Ito, M Ascher, JS Tanaka, H Kato, M Roubik, DW AF Kawakita, A Sota, T Ito, M Ascher, JS Tanaka, H Kato, M Roubik, DW TI Phylogeny, historical biogeography, and character evolution in bumble bees (Bombus: Apidae) based on simultaneous analysis of three nuclear gene sequences (vol 31, pg 799, 2004) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Correction C1 Kyoto Univ, Grad Sch Sci, Dept Zool, Kyoto 6068502, Japan. Kyoto Univ, Grad Sch Sci, Grad Sch Human & Environm Studies, Kyoto, Japan. Sapporo Sci & Technol Vocat Sch, Sapporo, Hokkaido, Japan. Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. Kyoto Univ, Primate Res Inst, Inuyama, Aichi 484, Japan. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Sota, T (reprint author), Kyoto Univ, Grad Sch Sci, Dept Zool, Kyoto 6068502, Japan. EM sota@terra.zool.kyoto-u.ac.jp RI Ascher, John/D-1554-2014 NR 1 TC 2 Z9 2 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD JUL PY 2004 VL 32 IS 1 BP 422 EP 423 DI 10.1016/j.ympev.2004.04.001 PG 2 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 832TZ UT WOS:000222291400036 ER PT J AU Rawlings, JMC Redman, MP Keto, E Williams, DA AF Rawlings, JMC Redman, MP Keto, E Williams, DA TI HCO(+) emission excess in bipolar outflows SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : formation; ISM : clouds; ISM : jets and outflows; ISM : molecules. ID YOUNG STELLAR OBJECTS; RADIATIVE-TRANSFER; MOLECULAR OUTFLOWS; CO OUTFLOWS; ACCRETION; ENVELOPES; CONTINUUM; MECHANISM; FLOW; JET AB A plausible model is proposed for the enhancement of the abundance of molecular species in bipolar outflow sources. In this model, levels of HCO(+) enhancement are considered based on previous chemical calculations, which are assumed to result from shock-induced desorption and photoprocessing of dust grain ice mantles in the boundary layer between the outflow jet and the surrounding envelope. A radiative transfer simulation that incorporates chemical variations within the flow shows that the proposed abundance enhancements in the boundary layer are capable of reproducing the observed characteristics of the outflow seen in HCO(+) emission in the star-forming core L1527. The radiative transfer simulation also shows that the emission lines from the enhanced molecular species, which trace the boundary layer of the outflow, exhibit complex line profiles, indicating that detailed spatial maps of the line profiles are essential in any attempt to identify the kinematics of potential infall/outflow sources. This study is one of the first applications of a full three-dimensional radiative transfer code which incorporates chemical variations within the source. C1 UCL, Dept Phys & Astron, London WC1E 6BT, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Redman, MP (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM mpr@cp.dias.ie NR 21 TC 58 Z9 58 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 JUL 1 PY 2004 VL 351 IS 3 BP 1054 EP 1062 DI 10.1111/j.1365-2966.2004.07855.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832IS UT WOS:000222261500030 ER PT J AU Kaaret, P Ward, MJ Zezas, A AF Kaaret, P Ward, MJ Zezas, A TI High-resolution imaging of the HeII lambda 4686 emission line nebula associated with the ultraluminous X-ray source in Holmberg II SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies : individual : Holmberg II; galaxies : starburst; galaxies : stellar content; X-rays : galaxies ID SOURCE NGC-5204 X-1; MASS BLACK-HOLES; OPTICAL COUNTERPART; STAR-FORMATION; DWARF GALAXY; NUCLEI; MODEL; M81 AB We present Hubble Space Telescope images of the He III region surrounding the bright X-ray source in the dwarf irregular galaxy Holmberg II. Using Chandra, we find a position for the X-ray source of alpha = 08(h) 19(m) 28(s).98, delta = + 70degrees42'19".3 (J2000) with an uncertainty of 0.6 arcsec. We identify a bright, point-like optical counterpart centred in the nebula with the X-ray source. The optical magnitude and colour of the counterpart are consistent with a star with spectral type between O4V and B3 Ib at a distance of 3.05 Mpc or reprocessed emission from an X-ray illuminated accretion disc. The nebular He II luminosity is 2.7 x 10(36) erg s(-1). The morphology of the He II, Hbeta and [O I] emission is consistent with being due to X-ray photoionization and is inconsistent with narrow beaming of the X-ray emission. A spectral model consisting of a multicolour disc blackbody with inverse-Compton emission from a hot corona gives a good fit to X-ray spectra obtained with XMM-Newton. Using the fitted X-ray spectrum, we calculate the relation between the He II and X-ray luminosity and find that the He II flux implies a lower bound on the X-ray luminosity in the range 4 to 6 x 10(39) erg s(-1) if the extrapolation of the X-ray spectrum between 54 and 300 eV is accurate. A compact object mass of at least 25 to 40 M. would be required to avoid violating the Eddington limit. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pkaaret@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 35 TC 76 Z9 78 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2004 VL 351 IS 3 BP L83 EP U1 DI 10.1111/j.1365-2966.2004.08020.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832IS UT WOS:000222261500008 ER PT J AU Morris, M AF Morris, M TI ... Successes and failures SO MUSEUM NEWS LA English DT Article C1 George Washington Univ, Washington, DC 20052 USA. Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Morris, M (reprint author), George Washington Univ, Washington, DC 20052 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD JUL-AUG PY 2004 VL 83 IS 4 BP 30 EP 35 PG 6 WC Art SC Art GA 041ZN UT WOS:000237496300016 ER PT J AU Matthews, JM Kusching, R Guenther, DB Walker, GAH Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW AF Matthews, JM Kusching, R Guenther, DB Walker, GAH Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW TI No stellar p-mode oscillations in space-based photometry of Procyon SO NATURE LA English DT Article ID GLOBAL PRESSURE OSCILLATIONS; ASTEROSEISMOLOGY; AMPLITUDES; SEARCH; STARS; LIMIT AB Pressure-driven (p-mode) oscillations at the surface of the Sun, resulting from sound waves travelling through the solar interior, are a powerful probe of solar structure, just as seismology can reveal details about the interior of the Earth. Astronomers have hoped to exploit p-mode asteroseismology(1) in Sun-like stars to test detailed models of stellar structure and evolution, but the observations are extremely difficult. The bright star Procyon has been considered one of the best candidates for asteroseismology, on the basis of models and previous reports(2-8) of p-modes detected in ground-based spectroscopy. Here we present a search for p-modes in 32 days of nearly continuous photometric satellite-based observations of Procyon. If there are p-modes in Procyon, they must have lifetimes less than 2-3 days and/or peak amplitudes <15 parts per million, which defy expectations from the Sun's oscillations and previous theoretical predictions. Target selection for future planned asteroseismology space missions may need to be reconsidered, as will the theory of stellar oscillations. C1 Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Matthews, JM (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. EM matthews@astro.ubc.ca NR 26 TC 119 Z9 119 U1 1 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 1 PY 2004 VL 430 IS 6995 BP 51 EP 53 DI 10.1038/nature02671 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 833RP UT WOS:000222356800038 PM 15229593 ER PT J AU Clubbe, C Gillman, M Acevedo-Rodriguez, P Walker, R AF Clubbe, C Gillman, M Acevedo-Rodriguez, P Walker, R TI Abundance, distribution and conservation significance of regionally endemic plant species on Anegada, British Virgin Islands SO ORYX LA English DT Article DE Acacia anegadensis; Anegada; British Virgin Islands; Cordia rupicola; endemic; Leptocereus quadricostatus; Malpighia woodburyana; Metastelma anegadense AB The conservation significance of the Caribbean island of Anegada in the British Virgin Islands is highlighted in this study of the distribution of plant species in two major habitats, sand dunes and limestone pavement. In 104 plots along 27 transects located around the western salt ponds of the Anegada Ramsar site, 133 plant species were recorded, including five regional endemics. The limestone pavement supported large populations of Acacia anegadensis, endemic to Anegada, and Cordia rupicola, known only from Anegada and Puerto Rico (although the Puerto Rican population is thought to be extirpated). The sand dunes supported a large population of Metastelma anegadense, also endemic to Anegada. Two other regional endemics were recorded within the limestone cays, Leptocereus quadricostatus, previously known from only one locality in Puerto Rico and Malpighia woodburyana, restricted to a few small populations on islands on the Puerto Rican Bank. For both of these species Anegada supports the largest known individual population. C1 Royal Bot Gardens, Richmond TW9 3AB, Surrey, England. Open Univ, Dept Biol Sci, Milton Keynes MK7 6AA, Bucks, England. Smithsonian Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. British Virgin Isl Natl Pk Trust, Tortola, VI USA. RP Clubbe, C (reprint author), Royal Bot Gardens, Richmond TW9 3AB, Surrey, England. EM c.clubbe@kew.org.uk NR 21 TC 3 Z9 7 U1 2 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0030-6053 J9 ORYX JI Oryx PD JUL PY 2004 VL 38 IS 3 BP 342 EP 346 DI 10.1017/S0030605304000596 PG 5 WC Ecology SC Environmental Sciences & Ecology GA 850BX UT WOS:000223587200024 ER PT J AU Kostrun, M AF Kostrun, M TI Hermitian-phase-operator treatment of the superfluid states in a quantum two-well problem SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATE AB We apply the Hermitian phase operator method (HPOM), as discussed by Pegg and Barnett [ D. T. Pegg and S. M. Barnett, Phys. Rev. A 39, 1665 (1989) ] to a two-well Bose-Hubbard model. Application of the HPOM formalism yields an approximate quantum phase model, or a Schrodinger-like differential equation for the phase variable theta, which is a conjugate variable to the half of the number difference between the wells, m=(N-1-N-2)/2. In the construction of the model we take care so that the Hermiticity of the original Bose-Hubbard model in number representation is inherited. We demonstrate that the quantum phase model supersedes two theoretical models suggested for the group of so-called "normal" states, for which ==0: a non-Hermitian "exact quantum phase model" by Anglin, Drummond, and Smerzi [ J. R. Anglin, P. Drummond, and A. Smerzi, Phys. Rev. A 64, 063605 (2001) ], and the "phonon model" by Javanainen and Ivanov [ J. Javanainen and M. Yu. Ivanov, Phys. Rev. A 60, 2351 (1999) ]. We apply the HPOM to the so called "superfluid" states, for which =0 and =pi, and find their superfluid phonon model. We find that the superfluid phonon model has a threshold point M=delta/(4gN)=1, at which the model diverges. Here, delta is the tunneling rate between the wells and g is the self-interaction, while N is the total number of particles. The above threshold phonon model is quite accurate in the description of the number and phase statistics of the superfluid states. We show that at the threshold point HPOM itself can be exactly solved. However, the agreement between the exact solution and the HPOM solution is poor: close to the threshold assumes values similar toN(2), thus voiding the second order expansion the HPOM is based on, much less thanN(2). C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Kostrun, M (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM kostrun@cfa.harvard.edu NR 11 TC 1 Z9 1 U1 1 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD JUL PY 2004 VL 70 IS 1 AR 012105 DI 10.1103/PhysRevA.70.012105 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 845VK UT WOS:000223273200023 ER PT J AU John, LA Phyllis, DCB Kursar, TA AF John, LA Phyllis, DCB Kursar, TA TI Cinnamoyl glucosides of catechin and dimeric procyanidins from young leaves of Inga umbellifera (Fabaceae) (vol 65, pg 351, 2004) SO PHYTOCHEMISTRY LA English DT Correction C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP John, LA (reprint author), Univ Utah, Dept Biol, 257 S 1400 E, Salt Lake City, UT 84112 USA. NR 1 TC 0 Z9 0 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0031-9422 J9 PHYTOCHEMISTRY JI Phytochemistry PD JUL PY 2004 VL 65 IS 13 BP 2013 EP 2013 DI 10.1016/j.phytochem.2004.03.023 PG 1 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA 848YM UT WOS:000223504100016 ER PT J AU Henry, TJ AF Henry, TJ TI Raglius alboacuminatus (Goeze) and Rhyparochromus vulgaris (Schilling) (Lygaeoidea : Rhyparochromidae): Two palearctic bugs newly discovered in North America SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Heteroptera; Lygaeoidea; Rhyparochromidae; Raglius alboacuminatus; Rhyparochromus vulgaris; North America; new records; California; Oregon; Utah; Washington; invasive ID HETEROPTERA AB Two invasive Palearctic rhyparochromids (Lygaeoidea: Rhyparochromidae) are recorded for the first time in North America. Raglius alboacuminatus Goeze is reported from California, Oregon, and northern Utah, and Rhyparochromus vulgaris (Schilling), from Oregon and Washington. Although not considered major agricultural pests, these invasive bugs have become serious nuisance pests, invading homes and commercial establishments in large numbers. Provided for each are a summary of the literature, notes on the biology and habitat, diagnosis, description, and photographs of the adult to help separate these nonindigenous bugs from other North American Rhyparochromidae. In addition, Xanthochilus saturnius (Rossi), a Palearctic species known in North America only from California, is reported for the first time from Oregon. C1 USDA ARS, PSI, Natl Musum Nat Hist, Smithsonian Inst,Systemat Entomol Lab, Washington, DC 20013 USA. RP Henry, TJ (reprint author), USDA ARS, PSI, Natl Musum Nat Hist, Smithsonian Inst,Systemat Entomol Lab, POB 37012,MRC-0168, Washington, DC 20013 USA. EM thenry@sel.barc.usda.gov NR 13 TC 3 Z9 3 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 JUL PY 2004 VL 106 IS 3 BP 513 EP 522 PG 10 WC Entomology SC Entomology GA 839PC UT WOS:000222796000003 ER PT J AU Gagne, RJ Posada, F Gil, ZN AF Gagne, RJ Posada, F Gil, ZN TI A new species of Bruggmanniella (Diptera : Cecidomyiidae) aborting young fruit of avocado, Persea americana (Lauraceae), in Colombia and Costa Rica SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Persea americana; avocado; Lauraceae; neotropical; gall midges AB A species new to science, Bruggmanniella perseae Gagne (Cecidomyiidae: Diptera), is reported from avocado, Persea americana, from Colombia and Costa Rica. The insect is a severe pest of avocado. Infested fruit drop to the soil when less than 2 cm in length. The new species is described, illustrated, and compared with the five previously described species of Bruggmanniella, and its biology is outlined. A key to the six species of Bruggmanniella is provided. C1 USDA ARS, Systmat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. USDA ARS, Inseect Biocontrol Lab, PSI, Beltsville, MD 20705 USA. Cenicafe, Chinchina, Caldas, Colombia. RP Gagne, RJ (reprint author), USDA ARS, Systmat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,NHB 168, Washington, DC 20013 USA. EM rgagne@sel.barc.usda.gov; francisco.posada@cafedecolombia.com; zulma.gil@cafedecolombia.com NR 8 TC 10 Z9 11 U1 1 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 JUL PY 2004 VL 106 IS 3 BP 547 EP 553 PG 7 WC Entomology SC Entomology GA 839PC UT WOS:000222796000007 ER PT J AU Neunzig, HH Solis, MA AF Neunzig, HH Solis, MA TI Exguiana, a new genus of neotropical phycitines (Lepidoptera : Pyralidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Phycitinae; taxonomy; Brazil; Costa Rica; French Guiana; Guyana AB The new genus Exguiana is proposed to receive Euzophera postflavida Dyar, n. comb, and three new species, E. beckeri, E. limonensis, and E. pitillana. Euzophera postflavida has been known only from female specimens, and its generic placement was uncertain until the recent discovery of males. A key separating the four species, habitus photographs of males, and line drawings of the wing venation, labial palpus, antenna of the male, and male and female genitalia are included. C1 N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Neunzig, HH (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. EM asolis@sel.barc.usda.gov NR 2 TC 1 Z9 1 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2004 VL 106 IS 3 BP 554 EP 563 PG 10 WC Entomology SC Entomology GA 839PC UT WOS:000222796000008 ER PT J AU Vandenberg, NJ AF Vandenberg, NJ TI Contributions to the knowledge of Olla casey (Coleoptera : Coccinellidae : Coccinellini): New species from the Galapagos Islands, updates on the distribution of O. v-nigrum (Mulsant) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Olla Coccinellini; new species; taxonomy; biological control; distribution; Galapagos ID PECAN ORCHARDS; APPLE; HEMIPTERA; PSYLLIDAE; FLORIDA; NORTH AB Olla lacrimosa, n. sp., is described from Isabela Island of the Galapagos Archipelago. Earlier, the single known example of this species was mistaken for Olla hageni Vandenberg, a closely related species which occurs on the neighboring island of Santa Cruz. A diagnosis, habitus drawing, and key details of the anatomy and morphology of the new species are provided and compared to related members of the genus. The habits and distribution of the genus are reviewed, and updated distributional data are provided for O. v-nigrum Mulsant, a widespread species of temperate and tropical America which has been released in a number of countries for biological control purposes. C1 Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, PSI,Syst Entomol Lab, Washington, DC 20013 USA. RP Vandenberg, NJ (reprint author), Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, PSI,Syst Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM nvandenb@sel.barc.usda.gov NR 22 TC 0 Z9 0 U1 1 U2 4 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 JUL PY 2004 VL 106 IS 3 BP 619 EP 626 PG 8 WC Entomology SC Entomology GA 839PC UT WOS:000222796000015 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, WN Zatwarnicki, T TI A review of two nearctic shore-fly species in the genus Psilopa Fallen that were included in the genus Cressonomyia Arnaud (Diptera : Ephydridae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE Diptera; Ephydridae; Nearctic; shore flies; Cressonomyia; Psilopa ID REVISION AB Psilopa aeneonigra Loew, a shore fly that was described in Psilopa but was for many years placed in the genus Cressonomyia Arnaud, is returned to Psilopa. A second species, P. loewi n. sp. (New Jersey. Ocean: Tuckerton (10 km N; 39degrees41.3'N, 74degrees21.6'W), that had been misidentified as P. aeneonigra is also recognized and described. The descriptions of these two species include the first illustrations of structures of the male terminalia. C1 Smithsonian Inst, Dept Syst Biol, WNM, Washington, DC 20013 USA. Polish Acad Sci, Museum & Inst Zool, PL-00679 Warsaw, Poland. Univ Opole, Dept Biosyst, PL-45052 Opole, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Syst Biol, WNM, MRC 169,BOX 37012, Washington, DC 20013 USA. EM mathis.wayne@nmnh.si.edu; zatwar@uni.opole.pl OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 12 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2004 VL 106 IS 3 BP 639 EP 648 PG 10 WC Entomology SC Entomology GA 839PC UT WOS:000222796000018 ER PT J AU Adamski, D AF Adamski, D TI A new Holcocera clemens (Lepidoptera : Gelechioidea : Coleophoridae) from mountainous southeastern Arizona SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Holcocerini; microlepidoptera; North America; taxonomy AB Holcocera fergusoni, new species, is described from two high-altitudinal collecting sites in the Santa Catalina Mountains and the Chiricahua Mountains in southeastern Arizona. A photograph of the holotype and illustrations of wing venation and male and female genitalia are provided. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Entomol, Washington, DC 20013 USA. RP Adamski, D (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Entomol, POB 37012,MRC 168, Washington, DC 20013 USA. EM dad-amski@sel.barc.usda.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2004 VL 106 IS 3 BP 649 EP 653 PG 5 WC Entomology SC Entomology GA 839PC UT WOS:000222796000019 ER PT J AU Smith, DR AF Smith, DR TI A new species of Derecyrta smith (Hymenoptera : Xiphydriidae) from Colombia and Ecuador SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE wood borer; wood wasp; Neotropical AB Derecyrta flavescens, In. sp., is described from Colombia and Ecuador. It is separated from the related species D. andrei Konow and D. pictipennis Smith. C1 Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, PSI,Syst Entomol Lab, Washington, DC 20013 USA. RP Smith, DR (reprint author), Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, PSI,Syst Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov NR 6 TC 2 Z9 4 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2004 VL 106 IS 3 BP 675 EP 678 PG 4 WC Entomology SC Entomology GA 839PC UT WOS:000222796000021 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, WN Zatwarnicki, T TI Description of a new species of Hyadina haliday (Diptera : Ephydridae) from Southern California SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Diptera; Ephydridae; shore flies; Hyadina clauseni; California AB Hyadina clauseni, new species, from Tecopa Hot Springs (California, Inyo County) is described, and information on its natural history is provided. Hyadina Haliday is redescribed, it nomenclatural status is discussed, and a revised key to known Nearctic species of the genus is provided. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. Polish Acad Sci, Museum & Inst Zool, PL-00679 Warsaw, Poland. Univ Opole, Dept Biosystemat, PL-45052 Oploe, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA. EM mathis.wayne@nmnh.si.edu; zatwar@uni.opole.pl OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 34 TC 3 Z9 3 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2004 VL 106 IS 3 BP 705 EP 716 PG 12 WC Entomology SC Entomology GA 839PC UT WOS:000222796000024 ER PT J AU Lin, J AF Lin, J TI Motions of flare ribbons and loops in various magnetic configurations SO SOLAR PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; SOLAR-FLARES; ERUPTIVE FLARES; CURRENT SHEETS; FLUX-ROPE; RECONNECTION; PHASE; FIELD; TEMPERATURE; EVOLUTION AB Kopp-Pneuman-type magnetic configurations, which include a vertical current sheet, with various background fields are investigated. Dissipation of the current sheet as a result of magnetic reconnection produces bright flare ribbons on the solar disk and a growing flare loop system in the corona. In principle, the growth of flare loop system is governed by a reconnection process only, and the behavior of flare ribbons is also controlled by the background field. The flare ribbons may appear either separate or attached to one another at the onset of the flare depending on the background field distribution on the boundary surface. We calculate the decrease in height that magnetic field lines undergo after they have reconnected to form closed loops. Following previous practice, we refer to this decrease as field line shrinkage. Unlike the motions of flare ribbons, the shrinkage of flare loops depends weakly on the background field. Individual loops always shrink fastest at the moment it is produced by reconnection and just starts to leave the current sheet. The earlier the loop forms, the more and faster it shrinks. The relevant observations are explained on the basis of our calculations, and the aspects of the explanation that need improvement are also discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jlin@cfa.harvard.edu RI LIN, JUN/B-9890-2017 NR 44 TC 38 Z9 41 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUL PY 2004 VL 222 IS 1 BP 115 EP 136 DI 10.1023/B:SOLA.0000036875.14102.39 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 843OP UT WOS:000223093800008 ER PT J AU Goodyear, AC AF Goodyear, AC TI Imagining flight: Aviation and popular culture. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst Natl Portrait Gallery, Washington, DC USA. RP Goodyear, AC (reprint author), Smithsonian Inst Natl Portrait Gallery, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2004 VL 45 IS 3 BP 627 EP 629 DI 10.1353/tech.2004.0127 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 856YT UT WOS:000224082700013 ER PT J AU Thorwirth, S Muller, HSP Lichau, H Winnewisser, G Mellau, GC AF Thorwirth, S Muller, HSP Lichau, H Winnewisser, G Mellau, GC TI The submillimeter wave spectrum of the C4H4 isomer vinylacetylene SO JOURNAL OF MOLECULAR STRUCTURE LA English DT Article DE vinylacetylene; butenyne; vinyl cyanide; submillimeter wave spectroscopy ID VINYL CYANIDE; TERAHERTZ REGION; HYPERFINE-STRUCTURE; SPECTROSCOPY; METHYLENECYCLOPROPENE; CYCLOBUTADIENE; BUTATRIENE; MILLIMETER; ENERGIES; RAMAN AB The submillimeter wave spectrum of the astrochemically relevant hydrocarbon molecule vinylacetylene (butenyne) has been investigated in selected frequency regions between 181 and 789 GHz covering the quantum numbers 19 less than or equal to J less than or equal to 87 and 0 less than or equal to K-a less than or equal to 23. A set of significantly improved spectroscopic parameters has been obtained which compares favourably with the related cyano compound vinyl cyanide for which a new comprehensive set of molecular parameters is also presented. The present investigation will aid radioastronomers in search for vinylacetylene in space. (C) 2004 Elsevier B.V. All rights reserved. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Univ Giessen, Inst Chem Phys, D-35392 Giessen, Germany. RP Thorwirth, S (reprint author), Harvard Univ, Div Engn & Appl Sci, Pierce Hall,29 Oxford St, Cambridge, MA 02138 USA. EM sthorwirth@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; Mellau, Georg Christopher/A-8886-2017; OI Thorwirth, Sven/0000-0001-8200-6710; Mellau, Georg Christopher/0000-0001-8209-5733; Mueller, Holger/0000-0002-0183-8927 NR 23 TC 8 Z9 8 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-2860 J9 J MOL STRUCT JI J. Mol. Struct. PD JUN 30 PY 2004 VL 695 SI SI BP 263 EP 267 DI 10.1016/j.molstruc.2004.01.002 PG 5 WC Chemistry, Physical SC Chemistry GA 827SV UT WOS:000221922000026 ER PT J AU Cairns, SD AF Cairns, SD TI A new shallow-water species of Javania (Scleractinia : Flabellidae) from Indonesia SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article DE Javania; Flabellidae; new species; key; Indonesia; azooxanthellate; Scleractinia; boring sponges AB A new species of azooxanthellate solitary Scleractinia, Javania erhardti, is described from relatively shallow water in Indonesia. It differs from congenerics in having six cycles of septa (192 septa), slightly concave septal axial edges, and a rudimentary columella. To aid in its identification, both a key to the 10 known Recent species in the genus and a distribution table of the 13 fossil and Recent species are given. Javania erhardti often contains commensal boring sponges in its base. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Systemat Zool Invertebrate Zool, Washington, DC 20013 USA. RP Cairns, SD (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Systemat Zool Invertebrate Zool, Washington, DC 20013 USA. NR 14 TC 2 Z9 2 U1 0 U2 1 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 JUN 30 PY 2004 VL 52 IS 1 BP 7 EP 10 PG 4 WC Zoology SC Zoology GA 843TE UT WOS:000223108600003 ER PT J AU Erwin, TL Aschiero, V AF Erwin, TL Aschiero, V TI Cicindis horni Bruch (Coleoptera : Carabidae, Cicindini): The fairy shrimp hunting beetle, its way of life on the Salinas Grandes of Argentina SO ZOOTAXA LA English DT Article DE Cicindini; Cicindis horni; Argentina; Salinas Grandes; adult beetle behavior; semiaquatic carabid beetle; anostracan fairy shrimp; Thamnocephalus sp.; the fairy shrimp hunting beetle AB Discovery of a large population of the rare and poorly known carabid beetle Cicindis horni Bruch on the Salinas Grandes of Cordoba Province, Argentina provided an opportunity to record aspects of its behavior and life history, and to test several hypotheses previously made about it way of life. This highly unusual species was known in the literature from the description of only two museum specimens and its phylogenetic relationships ambiguous. Adults spend the night in search of food or mates swimming on the water surface of alkaline water bodies. Mid-tibial natatorial setae, tarsal setal fringes, ventral vestiture, and genal/pronotal planing surfaces plus decumbent and very sharply pointed mandibles are specific adaptations that permit adults of this species to behave as swimming superspecialist predators. Therefore, there have been four independent invasions of the aquatic habitat by adephagan Coleoptera. Populations of C. horni Bruch are probably limited by the extent of the great salt flats of Argentina (550,000 hectares) located in north-central Argentina and are further limited edaphically within the overall geographic range. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Univ Nacl Tucuman, Lab Invest Ecol Las Yungas, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. RP Aschiero, V (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. NR 12 TC 12 Z9 14 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 JUN 28 PY 2004 IS 553 BP 1 EP 16 PG 16 WC Zoology SC Zoology GA 872OF UT WOS:000225215800001 ER PT J AU Dorta, E Diaz-Marrero, AR Cueto, M D'Croz, L Mate, JL Darlas, J AF Dorta, E Diaz-Marrero, AR Cueto, M D'Croz, L Mate, JL Darlas, J TI Carijenone, a novel class of bicyclic prostanoid from the eastern Pacific octocoral Carijoa multiflora SO ORGANIC LETTERS LA English DT Article ID CLAVULARIA-VIRIDIS QUOY; MARINE NATURAL-PRODUCTS; ALLENE OXIDE; SOFT CORAL; ANTITUMOR-ACTIVITY; OXYLIPINS; BIOSYNTHESIS; SYNTHASES; PATHWAY; GAIMARD AB An unprecedented biogenetically interesting bicyclic prostanoid 1, carijenone, has been isolated from the eastern Pacific octocoral Carijoa multiflora. The C-12 oxygenated function, characteristic of the coral cyclopentanone fatty acid derivatives, is involved in the formation of a five-membered oxane ring fused to the cyclopentane network. Its structure and stereochemistry were determined on the basis of spectral studies and molecular mechanics calculations. C1 CSIC, Inst Prod Nat & Agrobiol, Tenerife 38206, Spain. Smithsonian Trop Res Inst, Balboa, Panama. Univ Panama, Estafeta Univ, Dept Biol Marina & Limnol, Panama City, Panama. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. RP Dorta, E (reprint author), CSIC, Inst Prod Nat & Agrobiol, Avda Astrofis F Sanchez 3, Tenerife 38206, Spain. EM jdarlas@ipna.csic.es RI Diaz-Marrero, Ana/L-2899-2014; Cueto, MERCEDES/L-3185-2014 OI Diaz-Marrero, Ana/0000-0002-8886-7519; Cueto, MERCEDES/0000-0002-9112-6877 NR 20 TC 17 Z9 18 U1 0 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1523-7060 J9 ORG LETT JI Org. Lett. PD JUN 24 PY 2004 VL 6 IS 13 BP 2229 EP 2232 DI 10.1021/ol0492871 PG 4 WC Chemistry, Organic SC Chemistry GA 830JY UT WOS:000222119400038 PM 15200327 ER PT J AU Alvarenga, HMF Olson, SL AF Alvarenga, HMF Olson, SL TI A new genus of tiny condor from the Pleistocene of Brazil (Aves : Vulturidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new genus and species of Vulturidae (Cathartidae auct.), Wingegyps cartellei, is described from Pleistocene cave deposits in the states of Bahia and Minas Gerais, Brazil. This species is closely related to condors Gymnogyps and Vultur, particularly the former, as opposed to the smaller cathartid vultures, but is much smaller, being slightly smaller than the smallest living member of the family, the Lesser Yellow-headed Vulture Cathartes burrovianus. The Vulturidae appears to consist of two basic divisions (condors vs. other vultures) that differ profoundly in the morphology of the skull. Each appears to have been more diverse in the past and to contain larger or smaller species than survived to the present. C1 Museu Hist Nat Taubate, BR-12030520 Taubate, SP, Brazil. Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. RP Alvarenga, HMF (reprint author), Museu Hist Nat Taubate, Rua Colombia 99,Jardim Nacoes, BR-12030520 Taubate, SP, Brazil. NR 16 TC 9 Z9 9 U1 2 U2 3 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 JUN 24 PY 2004 VL 117 IS 1 BP 1 EP 9 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 833JY UT WOS:000222334800001 ER PT J AU Graves, GR AF Graves, GR TI Diagnoses of hybrid hummingbirds (Aves : Trochilidae). 13. An undescribed intrageneric combination, Heliodoxa imperatrix x Heliodoxa jacula SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID INTERGENERIC HYBRID AB An enigmatic specimen collected by Perry O. Simons, presumably on the Pacific slope of the Ecuadorian Andes, is demonstrated to be a hybrid between Heliodoxa imperatrix and Heliodoxa jacula jamesoni. This represents the only known instance of intrageneric hybridization in Heliodoxa. External measurements of the hybrid are consistent with the proposed parental hypothesis. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20013 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, MRC-116,POB 37012, Washington, DC 20013 USA. NR 20 TC 2 Z9 2 U1 0 U2 3 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 JUN 24 PY 2004 VL 117 IS 1 BP 10 EP 16 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 833JY UT WOS:000222334800002 ER PT J AU Felder, DL Kensley, B AF Felder, DL Kensley, B TI A new species of axiid shrimp from chemosynthetic communities of the Louisiana continental slope, Gulf of Mexico (Crustacea : Decapoda : Thalassinidea) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID SEEPS AB Calaxius carneyi, new species (Axiidae), is described from two male specimens collected by manned submersibles working near hydrocarbon seeps in deep waters (544 m) on the continental slope off Louisiana, in the northern Gulf of Mexico. Both specimens were taken adjacent to communities of clams that comprise a major constituent of chemosynthetic assemblages at the collection site. The new species is characterized in part by ventrally truncate abdominal pleura, as opposed to the acutely triangular or broadly rounded pleura found in other known members of Calaxius, only one of which is known to occur in the Atlantic Ocean. The new species is readily distinguished from its congeners by unique dentition of its heavy triangular rostrum and postrostral carapace, its short eyestalks and antennal acicle, the absence of well-defined teeth on the massive chelipeds, and the narrow, subtriangular telson. Chelipeds, pleopods and uropods of the two known specimens herewith described are covered extensively by long setae, many of which are plumose and densely fouled by flocculent debris. C1 Univ Louisiana, Dept Biol, Lafayette, LA 70504 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Felder, DL (reprint author), Univ Louisiana, Dept Biol, Lafayette, LA 70504 USA. EM DLF4517@louisiana.edu NR 10 TC 10 Z9 12 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 JUN 24 PY 2004 VL 117 IS 1 BP 68 EP 75 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 833JY UT WOS:000222334800008 ER PT J AU Schotte, M Heard, R AF Schotte, M Heard, R TI A new species of Synidotea (Crustacea : Isopoda : Valvifera) from the northern Gulf of Mexico SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID IDOTEIDAE AB Synidotea fosteri, n. sp., the sixth known member of the genus Synidotea from the western Atlantic Ocean, is described from shallow waters (1-2 m) adjacent to open beaches in the northern Gulf of Mexico. Its current range extends from western Florida westward to Texas. The new species is distinguished from other related species by small size, fairly straight lateral margins of first pereonite, having the posterior margin of pleotelson straight to very slightly emarginate and by details of the appendix masculina. A key to the known western Atlantic species of the genus Synidotea is also given. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. Gulf Coast Res Lab, Dept Coastal Sci, Ocean Springs, MS 39566 USA. RP Schotte, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. NR 13 TC 0 Z9 1 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 24 PY 2004 VL 117 IS 1 BP 88 EP 94 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 833JY UT WOS:000222334800010 ER PT J AU Wasshausen, DC Wood, JRI AF Wasshausen, DC Wood, JRI TI Notes on the genus Dicliptera (Acanthaceae) in Bolivia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Taxonomic notes on Dicliptera are presented in preparation for the authors' forthcoming annotated and illustrated checklist of Bolivian Acanthaceae. Two new species (D. palmariensis and D. purpurascens) are described and illustrated. Infraspecific variation of D. squarrosa is discussed. A key to all of the recognized species of Dicliptera from Bolivia is also provided. C1 Smithsonian Inst, Dept Systemat Biol Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Oxford, Dept Bot, Oxford OX1 3RB, England. RP Wasshausen, DC (reprint author), Smithsonian Inst, Dept Systemat Biol Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. EM wasshausen.dieter@nmnh.si.edu; jriwood@hotmail.com NR 2 TC 1 Z9 1 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 24 PY 2004 VL 117 IS 1 BP 140 EP 149 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 833JY UT WOS:000222334800014 ER PT J AU Carter, LM Campbell, DB Campbell, BA AF Carter, LM Campbell, DB Campbell, BA TI Impact crater related surficial deposits on Venus: Multipolarization radar observations with Arecibo SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE impact craters; radar; surface properties; Venus ID MAGELLAN; FEATURES; SURFACE; EJECTA; DEGRADATION; EMISSION AB The distribution of surficial deposits in the vicinity of impact craters on Venus was studied using measurements of the polarization properties of the reflected radar wave. Subsurface scattering of an incident circularly polarized radar signal results in a linearly polarized component in the radar echo due to the differing transmission coefficients at a smooth ( at wavelength scales) atmosphere-surface boundary for the horizontal ( H) and vertical ( V) linearly polarized components of the incident wave. Arecibo 12.6 cm wavelength radar observations in 1999 and 2001 provided images of the surface of Venus in the full Stokes polarization parameters of the reflected echo, from which images in the degree of linear polarization were derived. These images show that substantial areas of Sedna, Guinevere, and Lavinia Planitias return a radar echo with a significant degree of linear polarization, indicating that mantling deposits may be relatively widespread on the plains of Venus. The areas showing linear polarization enhancements are strongly correlated with topographic features, primarily impact craters, dome fields, and windblown deposits, including dune fields. A strong linearly polarized echo component (similar to10-40% linear polarization) is found from regions near 45 impact craters, including 5 parabolas. These linear polarization features typically correspond to diffuse, higher backscatter cross-section (bright) regions in Magellan images. The linearly polarized component in these regions is attributed to subsurface echoes from a mantled substrate or from buried rocks. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Carter, LM (reprint author), Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. EM lcarter@astro.cornell.edu; campbellb@nasm.si.edu RI Carter, Lynn/D-2937-2012 NR 28 TC 28 Z9 28 U1 0 U2 1 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 JUN 22 PY 2004 VL 109 IS E6 AR E06009 DI 10.1029/2003JE002227 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 839IP UT WOS:000222777600001 ER PT J AU Miniutti, G Fabian, AC Miller, JM AF Miniutti, G Fabian, AC Miller, JM TI The relativistic Fe emission line in XTE J1650-500 with BeppoSAX: evidence for black hole spin and light-bending effects? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; X-rays : individual : XTE J1650-500; X-rays : stars ID X-RAY ASTRONOMY; ENERGY CONCENTRATOR SPECTROMETER; XMM-NEWTON; IRON LINE; GALAXY MCG-6-30-15; ACCRETION DISK; ON-BOARD; VARIABILITY; SATELLITE; SPECTROSCOPY AB We report spectral results from three BeppoSAX observations of the black hole candidate XTE J1650-500 during its 2001/2002 outburst. We find strong evidence for the presence of a broad and strongly relativistic Fe emission line. The line profile indicates an accretion disc extending down to two gravitational radii, suggesting the presence of a rapidly rotating central Kerr black hole. Thanks to the broad-band spectral coverage of BeppoSAX, we could analyse the 1.5-200 keV spectra of the three observations and report the presence of a strong reflection component from the accretion disc, which is totally consistent with the observed broad Fe emission line. The shape of the reflection component appears to be affected by the same special and general relativistic effects that produce the broad Fe line. We study the variation of the different spectral components from the first to the third observation, and we find that they are well reproduced by a recently proposed light-bending model. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Miniutti, G (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM miniutti@ast.cam.ac.uk RI Miniutti, Giovanni/L-2721-2014 OI Miniutti, Giovanni/0000-0003-0707-4531 NR 43 TC 72 Z9 72 U1 0 U2 2 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2004 VL 351 IS 2 BP 466 EP 472 DI 10.1111/j.1365-2966.2004.07794.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 828MH UT WOS:000221976900011 ER PT J AU Gardini, A Rasia, E Mazzotta, P Tormen, G De Grandi, S Moscardini, L AF Gardini, A Rasia, E Mazzotta, P Tormen, G De Grandi, S Moscardini, L TI Simulating Chandra observations of galaxy clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; methods : N-body simulations; methods : numerical; galaxies : clusters : general; cosmology : observations; X-rays : galaxies ID X-RAY-CLUSTERS; SMOOTHED PARTICLE HYDRODYNAMICS; INTRACLUSTER MEDIUM; TEMPERATURE PROFILES; INTERGALACTIC MEDIUM; PERSEUS CLUSTER; NEARBY CLUSTERS; STAR-FORMATION; XMM-NEWTON; COLD-FRONT AB Although trivial in principle, direct comparison of galaxy clusters X-ray observations to numerical hydro-N-body simulations is not always simple, because of many possible artefacts introduced by the instrument response, sky background and instrumental noise. To address these problems, we constructed the software package X-MAS (X-ray Map Simulator), a tool devoted to simulate X-ray observations of galaxy clusters obtained from hydro-N-body simulations. One of the main features of X-MAS is the ability to generate event files following the same standards used for real observations. This implies that its simulated observations can be analysed in the same way as - and with the same tools of - real observations. In this paper we present how the X-MAS package works, and discuss its application to the simulation of Chandra ACIS-S3 observations. Using the results of high-resolution hydro-N-body simulations, we generate fake Chandra observations of a number of simulated clusters. We then compare some of the main physical properties of the input data to those derived from the simulated observations after performing a standard imaging and spectral analysis. We find that, because of the sky background, the lower surface brightness spatial substructures, which can be easily identified in the simulations, are no longer detected in the simulated observations. We also show that, when a cluster has a complex (i.e. not isothermal) thermal structure along the line of sight, then the projected spectroscopic temperature obtained from the observation is significantly lower than the emission-weighed value inferred directly from hydrodynamical simulation. This implies that much attention should be paid in the theoretical interpretation of observed temperatures. C1 Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Univ Durham, Dept Phys, Durham DH1 3LE, England. INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gardini, A (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. EM rasia@pd.astro.it RI Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; rasia, elena/0000-0003-4175-002X NR 52 TC 47 Z9 47 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2004 VL 351 IS 2 BP 505 EP 514 DI 10.1111/j.1365-2966.2004.07800.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 828MH UT WOS:000221976900014 ER PT J AU Walker, C Wood, K Lada, CJ Robitaille, T Bjorkman, JE Whitney, B AF Walker, C Wood, K Lada, CJ Robitaille, T Bjorkman, JE Whitney, B TI The structure of brown dwarf circumstellar discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; stars : low-mass, brown dwarfs; stars : pre-main-sequence; infrared : stars ID AURIGA MOLECULAR CLOUD; YOUNG STELLAR OBJECTS; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; INITIAL MASS FUNCTION; RHO-OPHIUCHI CLOUD; SIZE DISTRIBUTION; EMBEDDED-CLUSTER; FORMING REGION; BURNING LIMIT AB We present synthetic spectra for circumstellar discs that are heated by radiation from a central brown dwarf. Under the assumption of vertical hydrostatic equilibrium, our models yield scaleheights for brown dwarf discs in excess of three times those derived for classical T Tauri (CTTS) discs. If the near-IR excess emission observed from brown dwarfs is indeed due to circumstellar discs, then the large scaleheights we find could have a significant impact on the optical and near-IR detectability of such systems. Our radiation transfer calculations show that such highly flared discs around brown dwarfs will result in a large fraction of obscured sources due to extinction of direct starlight by the disc over a wide range of sightlines. The obscured fraction for a 'typical' CTTS is less than 20 per cent. We show that the obscured fraction for brown dwarfs may be double that for CTTS, but this depends on stellar and disc mass. We also comment on possible confusion in identifying brown dwarfs via colour-magnitude diagrams: edge-on CTTS display similar colours and magnitudes to face-on brown dwarf plus disc systems. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. Space Sci Inst, Boulder, CO 80303 USA. RP Walker, C (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM cw26@st-andrews.ac.uk; kw25@st-andrews.ac.uk; clada@cfa.harvard.edu; tr9@st-andrews.ac.uk; jon@astro.utoledo.edu; bwhitney@colorado.edu OI Robitaille, Thomas/0000-0002-8642-1329 NR 66 TC 48 Z9 48 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2004 VL 351 IS 2 BP 607 EP 616 DI 10.1111/j.1365-2966.2004.07807.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 828MH UT WOS:000221976900021 ER PT J AU Zaldarriaga, M Furlanetto, SR Hernquist, L AF Zaldarriaga, M Furlanetto, SR Hernquist, L TI 21 centimeter fluctuations from cosmic gas at high redshifts SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; diffuse radiation; intergalactic medium On-line material : color figures ID MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP OBSERVATIONS; COLD DARK-MATTER; REIONIZATION HISTORY; INTERGALACTIC MEDIUM; STAR-FORMATION; NEUTRAL HYDROGEN; STELLAR SOURCES; POWER SPECTRUM; LINE-PROFILE AB The relatively large Thomson optical depth, tau(es), inferred recently from the WMAP observations suggests that the universe was reionized in a more complex manner than previously believed. However, the value Of T,, provides only an integral constraint on the history of reionization and, by itself, cannot be used to determine the nature of the sources responsible for this transition. Here we show that the evolution of the ionization state of the intergalactic medium (IGM) at high redshifts can be measured statistically using fluctuations in 21 cm radiation from neutral hydrogen. By analogy with the mathematical description of anisotropies in the cosmic microwave background, we develop a formalism to quantity the variations in 21 cm emission as a function of both frequency and angular scale. Prior to and following reionization, fluctuations in the 21 cm signal are mediated by density perturbations in the distribution of matter. Between these epochs, pockets of gas surrounding luminous objects become ionized, producing large H II regions. These "bubbles" of ionized material imprint features into the 21 cm power spectrum that make it possible to distinguish them from fluctuations produced by the density perturbations. The variation of the power spectrum with frequency can be used to infer the evolution of this process. As has been emphasized previously by others, the absolute 21 cm signal from neutral gas at high redshifts is difficult to detect as a result of contamination by foreground sources. However, we argue that this source of noise can be suppressed by comparing maps closely spaced in frequency, i.e., redshift, so that 21 cm fluctuations from the IGM can be measured against a much brighter, but smoothly varying (in frequency), background. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Zaldarriaga, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mzaldarriaga@cfa.harvard.edu; sfurlane@tapir.caltech.edu; lars@cfa.harvard.edu NR 67 TC 248 Z9 248 U1 1 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2004 VL 608 IS 2 BP 622 EP 635 DI 10.1086/386327 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831HA UT WOS:000222184300002 ER PT J AU Grego, L Vrtilek, JM Van Speybroeck, L David, LP Forman, W Carlstrom, JE Reese, ED Joy, MK AF Grego, L Vrtilek, JM Van Speybroeck, L David, LP Forman, W Carlstrom, JE Reese, ED Joy, MK TI A deep Chandra observation of the distant galaxy cluster MS 1137.5+6625 SO ASTROPHYSICAL JOURNAL LA English DT Article ID MEDIUM-SENSITIVITY SURVEY; X-RAY-CLUSTERS; MICROWAVE BACKGROUND ANISOTROPY; COLD DARK-MATTER; HIGH-REDSHIFT CLUSTERS; GAS MASS FRACTIONS; HUBBLE CONSTANT; COSMOLOGICAL PARAMETERS; INTRACLUSTER MEDIUM; CL 0016+16 AB We present results from a deep Chandra observation of MS 1137.5+66, a distant (z = 0.783) and massive cluster of galaxies. Only a few similarly massive clusters are currently known at such high redshifts; accordingly, this observation provides much needed information on the dynamical state of these rare systems. The cluster appears both regular and symmetric in the X-ray image. However, our analysis of the spectral and spatial X-ray data in conjunction with interferometric Sunyaev-Zel'dovich effect data and published deep optical imaging suggests that the cluster has a fairly complex structure. The angular diameter distance we calculate from the Chandra and Sunyaev-Zei'dovich effect data assuming an isothermal, spherically symmetric cluster implies a low value for the Hubble constant for which we explore possible explanations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. RP Grego, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lgrego@cfa.harvard.edu; ldavid@cfa.harvard.edu; wforman@cfa.harvard.edu; rcese@efpa.bcrkeley.edu; marshall.joy@msfc.nasa.gov OI Forman, William/0000-0002-9478-1682 NR 68 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2004 VL 608 IS 2 BP 731 EP 741 DI 10.1086/420687 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831HA UT WOS:000222184300011 ER PT J AU Damiani, F Flaccomio, E Micela, G Sciortino, S Harnden, FR Murray, SS AF Damiani, F Flaccomio, E Micela, G Sciortino, S Harnden, FR Murray, SS TI A deep Chandra X-ray observation of the rich young cluster NGC 6530. I. The X-ray source catalog and the cluster population SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 6530); stars : coronae; stars : pre-main-sequence; X-rays : stars ID ORION NEBULA CLUSTER; H-ALPHA PHOTOMETRY; MAIN-SEQUENCE; NGC 6530; STAR-FORMATION; LAGOON NEBULA; MEMBERSHIP; EVOLUTION; NGC6530; UBVRI AB In a deep 60 ks Chandra ACIS X-ray observation of the very young cluster NGC 6530, we detect 884 X-ray point sources and argue that a very large fraction of them (90%-95%) must be pre-main-sequence (PMS) cluster members, mostly of low masses. This is a significant enlargement of the known NGC 6530 stellar population with respect to previous optical studies, including Halpha surveys. We identify 220 X-ray sources with cataloged stars down to V = 17, while most unidentified sources have fainter counterparts. Moreover, we find an infrared counterpart in the 2MASS catalog for 731 X-ray sources. The optically identified cluster X-ray sources are found in a band in the H-R diagram above the main sequence, in the locus of 0.5-1.5 Myr PMS stars, with masses down to 0.5-1.5 M-circle dot. We find evidence of an age gradient across the field from northwest to south, suggesting a sequence of star formation events qualitatively similar to that found in earlier studies of the same region, but differing in the details. A group of X-ray sources showing frequent flares may be associated with the youngest stars in the Cluster, suggesting that X-ray flaring activity is especially intense in the youngest PMS phases of low-mass stars. C1 INAF Osserv Astron Palermo GS Vaiana, I-90134 Palermo, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Damiani, F (reprint author), INAF Osserv Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy. EM damiani@oapa.astropa.umpa.it; ettoref@oapa.astropa.unipa.it; giusi@oapa.astropa.unipa.it; sciorti@oapa.astropa.unipa.it OI Flaccomio, Ettore/0000-0002-3638-5788; Damiani, Francesco/0000-0002-7065-3061 NR 31 TC 40 Z9 40 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2004 VL 608 IS 2 BP 781 EP 796 DI 10.1086/420779 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831HA UT WOS:000222184300016 ER PT J AU Goodman, AA Arce, HG AF Goodman, AA Arce, HG TI PV Cephel: Young star caught speeding? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : Herbig-Haro objects; ISM : individual (HH 315); ISM : jets and outflows; stars : formation; stars : individual (PV Cephei); stars : kinematics ID SUPERSONIC SIDE WIND; HERBIG-HARO FLOWS; T-TAURI STARS; PROPER MOTIONS; RUNAWAY STARS; STELLAR-SYSTEMS; ORION-NEBULA; DARK CLOUDS; NGC 7023; JET AB Three independent lines of evidence imply that the young star PV Cep is moving at roughly 20 km s(-1) through the interstellar medium. The first and strongest suggestion of motion comes from the geometry of the Herbig-Haro (HH) knots in the "giant" HH flow associated with PV Cep. Bisectors of lines drawn between pairs of knots at nearly equal distances from PV Cep imply an east-west motion of the source, and a plasmon model fitted to the knot positions gives a good fit of 22 km s(-1) motion for the star. The second bit of damning evidence comes from a redshifted trail of molecular gas pointing in the same east-west direction implied by the HH knot geometry. The third exhibit we offer in accusing PV Cep of speeding involves the apparent tilt in the high-velocity molecular jet now emanating from the star. This tilt is best explained if the true, current jet direction is north-south, as it is in Hubble Space Telescope WFPC2 images, and the star is moving, again at roughly 20 km s-1. Tracing the motion of PV Cep backward in time to the nearest cluster from which it might have been ejected, we find that it is very likely to have been thrown out of the massive star-forming cluster NGC 7023, more than 10 pc away. PV Cep and NGC 7023 are at similar distances, and the backward trace of PV Cep's motion is astonishingly well aligned with a dark, previously unexplained rift in NGC 7023. We propose that PV Cep was ejected, at a speed large enough to escape NGC 7023, at least 100,000 yr ago but that it did not enter the molecular cloud in which it now finds itself until more like 35,000 yr ago. Our calculations show that the currently observable molecular outflow associated with PV Cep is about 10,000 yr old, so the flow has had plenty of time to form while in its current molecular cloud. However, the question of what PV Cep was doing and what gas/disk it took along with it in the time it was traveling through the low-density region between NGC 7023 and its current home is an open one. Recent numerical simulations have suggested that condensed objects should be ejected at high velocity before they have "finished" forming in a cluster. Prior to this work, a handful of pre-main-sequence stars have been shown to be moving at speeds greater than 10 kin s-1. To the best of our knowledge, though, the analysis of PV Cep and NGC 7023 described here is the first observational work associating a speeding young star with a distant ancestral cluster. These high-speed ejection from clusters will create a class of rapidly moving young stars in molecular clouds. If these ejections are at all common, their existence confounds both calculations of clouds' star-forming efficiency and theories of star formation that do not allow for stars to move rapidly through a reservoir of star-forming material while they form. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Goodman, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM agoodman@cfa.harvard.edu; harce@astro.caltech.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 58 TC 23 Z9 24 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2004 VL 608 IS 2 BP 831 EP 845 DI 10.1086/383139 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831HA UT WOS:000222184300019 ER PT J AU Cobb, BE Bailyn, CD Van Dokkum, PG Buxton, MM Bloom, JS AF Cobb, BE Bailyn, CD Van Dokkum, PG Buxton, MM Bloom, JS TI The supernova associated with Grb 031203: Smarts optical-infrared light curves from 0.2 to 92 days SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; supernovae : general; supernovae : individual (SN 20031w) ID GAMMA-RAY BURSTS; STANDARD STARS; GRB-030329; PROSPECTS AB Optical and infrared monitoring of the afterglow site of gamma-ray burst GRB 031203 has revealed a brightening source embedded in the host galaxy, which we attribute to the presence of a supernova (SN) related to the GRB ("SN 2003lw"). We present details of the discovery and evolution of SN 2003lw from 0.2 to 92 days after the GRB, derived from SMARTS consortium photometry in I and J bands. GRB 031203 was an intrinsically faint GRB, and the optical light curve is dominated by the SN after the first few days. A template Type Ic light curve, constructed from SN 1998bw photometry, is consistent with the peak brightness of SN 20031w, although the light curves are not identical. Differential astrometry reveals that the SN, and hence the GRB, occurred less than 300 h, pc (3 a) from the apparent galaxy center. C1 Yale Univ, Dept Astron, New Haven, CT 06520 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cobb, BE (reprint author), Yale Univ, Dept Astron, POB 288101, New Haven, CT 06520 USA. EM cobb@astro.yale.edu NR 32 TC 55 Z9 57 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2004 VL 608 IS 2 BP L93 EP L96 DI 10.1086/422423 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831HB UT WOS:000222184400005 ER PT J AU Kosack, K Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Connaughton, V Cui, W Daniel, M D'Vall, M Perez, IDL Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Gutierrez, K Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Jarvis, A Jordan, M Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Linton, E Lloyd-Evans, J Milovanovic, A McEnery, J Moriarty, R Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J AF Kosack, K Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Connaughton, V Cui, W Daniel, M D'Vall, M Perez, IDL Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Gutierrez, K Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Jarvis, A Jordan, M Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Linton, E Lloyd-Evans, J Milovanovic, A McEnery, J Moriarty, R Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J TI Tev Gamma-ray observations of the galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; Galaxy : center; Galaxy : nucleus; gamma rays : observations ID SUPERMASSIVE BLACK-HOLE; SAGITTARIUS-A-ASTERISK; DARK-MATTER HALOS; MILKY-WAY; ANNIHILATION; EMISSION; DIRECTION; SPECTRA; FLARE; EAST AB We report a possible detection of TeV gamma rays from the Galactic center by the Whipple 10 m gamma-ray telescope. Twenty-six hours of data were taken over an extended period from 1995 through 2003 resulting in a total significance of 3.7 sigma. The measured excess corresponds to an integral flux of 1.6 x 10(-8) +/- 0.5 x 10(-8) (stat) +/- 0.3 x 10(-8) (sys) photons m(-2) s(-1) above an energy of 2.8 TeV, roughly 40% of the flux from the Crab Nebula at this energy. The 95% confidence region has an angular extent of about 15' and includes the position of Sgr A*. The detection is consistent with a point source and shows no evidence of variability. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Iowa State Univ Sci & Technol, Dept Phys & Astron, Ames, IA 50011 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Gamma Ray Astrophys Grp Natl Space Sci, Huntsville, AL USA. Ctr Technol, Huntsville, AL USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland Univ Coll Dublin, Dept Expt Phys, Dublin 4, Ireland. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Adler Planetarium, Dept Astron, Chicago, IL 60605 USA. Astron Museum, Chicago, IL 60605 USA. Natl Univ Ireland Univ Coll Galway, Dept Phys, Galway, Ireland. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Univ Maryland Baltimore Cty, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Mayo Inst Technol, Sch Sci, Galway, Ireland. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Kosack, K (reprint author), Washington Univ, Dept Phys, Campus Box 1105, St Louis, MO 63130 USA. EM buckley@wuphys.wustl.edu RI McEnery, Julie/D-6612-2012; Hall, Jeter/F-6108-2013; Hall, Jeter/E-9294-2015; Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 30 TC 147 Z9 147 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2004 VL 608 IS 2 BP L97 EP L100 DI 10.1086/422469 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831HB UT WOS:000222184400006 ER PT J AU Breedy, O Guzman, HM AF Breedy, O Guzman, HM TI New species of the gorgoniian genus Pacifigorgia (Coelenterata : Octocorallia : Gorgoniidae) from Pacific Panama SO ZOOTAXA LA English DT Article DE Cnidaria; Coelenterata; eastern Pacific; gorgonians; Gorgoniidae; octocorals; Pacifigorgia; Panama; soft corals; coral reefs; new species AB Four new shallow water species of the genus Pacifigorgia were found in recent surveys along the Pacific coast of Panama. One of the species was only found in dense patches at two shallow sea-mount-like localities inside the Coiba National Park, Gulf of Chiriqu. Two other species were patchily distributed at several localities in the Gulf of Chiriqu. A fourth species was widely distributed around the gulfs of Chiriqu and Panama encompassing a broad range of habitats and depths. The new species are described and illustrated in detail with scanning electron micrographs (SEM) of the sclerites, and colour photographs of the colony forms. The suspected occurrence of a particular Pacifigorgia species for this region is confirmed and two other new records are added to the species list. With the new four species, a total of 15 are established for Panama, making 31 species for the eastern Pacific to date. C1 Univ Costa Rica, Escuela Biol, Museo Zool, San Jose, Costa Rica. Smithsonian Trop Res Inst, Balboa, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Escuela Biol, Museo Zool, POB 1962-2100, San Jose, Costa Rica. EM odalisca@racsa.co.cr; guzmanh@naos.si.edu NR 11 TC 9 Z9 9 U1 1 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 18 PY 2004 IS 541 BP 1 EP 15 PG 15 WC Zoology SC Zoology GA 872NJ UT WOS:000225213600001 ER PT J AU Hutchinson, A AF Hutchinson, A TI The tower menagerie: Being the amazing true story of wild and ferocious beasts. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Hutchinson, A (reprint author), Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 15 PY 2004 VL 129 IS 11 BP 93 EP 93 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 835YH UT WOS:000222521000209 ER PT J AU Leverington, DW Maxwell, TA AF Leverington, DW Maxwell, TA TI An igneous origin for features of a candidate crater-lake system in western Memnonia, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE channel; craters; terrace ID LONG LAVA FLOWS; ERUPTION CONDITIONS; MARTIAN HIGHLANDS; SHORE PLATFORMS; THERMAL HISTORY; KILAUEA VOLCANO; LATE QUATERNARY; WRINKLE RIDGES; SINUOUS RILLES; MOUNT-ETNA AB The association of channels, inner terraces, and delta-like features with Martian impact craters has previously been interpreted as evidence in favor of the past existence of crater lakes on Mars. However, examination of a candidate crater-lake system in western Memnonia suggests instead that its features may have formed through igneous processes involving the flow and ponding of lava. Accumulations of material in craters and other topographic lows throughout much of the study region have characteristics consistent with those of volcanic deposits, and terraces found along the inner flanks of some of these craters are interpreted as having formed through drainage or subsidence of volcanic materials. Channels previously identified as inlets and outlets of the crater-lake system are interpreted instead as volcanic rilles. These results challenge previous interpretations of terrace and channel features in the study region and suggest that candidate crater lakes located elsewhere should be reexamined. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Leverington, DW (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, POB 37012,Room 3774,MRC 0315, Washington, DC 20560 USA. EM leveringtond@nasm.si.edu NR 99 TC 27 Z9 28 U1 0 U2 0 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 JUN 11 PY 2004 VL 109 IS E6 AR E06006 DI 10.1029/2004JE002237 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 829YC UT WOS:000222086900001 ER PT J AU Pawson, DL Vance, DJ AF Pawson, DL Vance, DJ TI Chiridota heheva, new species, from Western Atlantic deep-sea cold seeps and anthropogenic habitats (Echinodermata : Holothuroidea : Apodida) SO ZOOTAXA LA English DT Article DE Chiridota heheva; cold seeps; Western Atlantic; Holothuroidea; Apodida ID VENT; COMMUNITIES; BIOGEOGRAPHY; RIDGE AB Chiridota heheva new species is described from cold seeps off Georgia and Florida, a shipwreck off Georgia, and an artificial wood-block habitat near Puerto Rico, in bathyal-abyssal depths of 2,200 - 3,300 meters. C. heheva is similar in some respects to C. hydrothermica Smirnov & Gebruk from Western and Southeastern Pacific hydrothermal vents, but it differs in structure of the tentacles and in color. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Pawson, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Mail Stop MRC163, Washington, DC 20013 USA. EM pawson.david@nmnh.si.edu NR 25 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 JUN 11 PY 2004 IS 534 BP 1 EP 12 PG 12 WC Zoology SC Zoology GA 872MU UT WOS:000225212100001 ER PT J AU Cohn, JD Kochanek, CS AF Cohn, JD Kochanek, CS TI The effects of massive substructures on image multiplicities in gravitational lenses SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing ID ALL-SKY SURVEY; PHASE CALIBRATION SOURCES; DARK-MATTER SUBSTRUCTURE; LUMINOSITY FUNCTION; GALACTIC SATELLITES; SCALE STRUCTURE; CROSS-SECTIONS; GALAXIES; HALOS; SELECTION AB Surveys for gravitational lens systems have typically found a significantly larger fraction of lenses with four ( or more) images than are predicted by standard ellipsoidal lens models (50% versus 25% - 30%). We show that including the effects of smaller satellite galaxies, with an abundance normalized by the observations, significantly increases the expected number of systems with more than two images and largely explains the discrepancy. The effect is dominated by satellites with similar to 20% the luminosity of the primary lens, in rough agreement with the typical luminosities of the observed satellites. We find that the lens systems with satellites cannot be dropped from estimates of the cosmological model based on gravitational lens statistics without significantly biasing the results. C1 Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Calif Berkeley, Theoret Astrophys Ctr, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cohn, JD (reprint author), Univ Calif Berkeley, Space Sci Lab, 601 Campbell Hall, Berkeley, CA 94720 USA. EM jcohn@astron.berkeley.edu; ckochanek@cfa.harvard.edu NR 58 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2004 VL 608 IS 1 BP 25 EP 35 DI 10.1086/392491 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827EG UT WOS:000221881200004 ER PT J AU Sobolewska, MA Siemiginowska, A Zycki, PT AF Sobolewska, MA Siemiginowska, A Zycki, PT TI High-redshift radio-quiet quasars: Exploring the parameter space of accretion models. I. Hot semispherical flow SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies : high-redshift; quasars : general; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; DIGITAL SKY SURVEY; OPTICALLY SELECTED QUASARS; PALOMAR-GREEN QUASARS; BLACK-HOLE; CYGNUS X-1; DISK MODELS; ENERGY-DISTRIBUTIONS; SEYFERT-GALAXIES AB Two families of models are currently considered to describe an accretion flow onto black holes and production of the observed X-ray radiation: (1) a standard cold accretion disk with a hot corona above it and (2) an outer truncated accretion disk with a hot semispherical inner flow. We compute spectra in the scenario with a hot inner flow surrounded by a truncated accretion disk covered by a hot corona and test the results on a sample of high-redshift (z > 4) quasars observed with Chandra. We find that in order to reproduce the ratio of optical to X-ray fluxes (the alpha(ox) parameter), the optical depth of the Comptonizing plasma has to be rather low (tau = 0.02-0.25 in the corona above the disk, and tau = 0.10-0.70 in the hot inner flow). This, together with the observed X-ray photon indices, implies either a high temperature in a thermal plasma (kT(e) = 90-500 keV) or a nonthermal electron distribution in the plasma. We put an upper limit on the disk truncation radius, r(tr) less than or equal to 40R(S). The modeled accretion rate is high, (m) over dot > 0.2(M) over dot(Edd) , which may suggest that high-z radio-quiet quasars are analogs of X-ray binaries in their high or very high state. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Sobolewska, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msobolewska@cfa.harvard.edu; asiemiginowska@cfa.harvard.edu; ptz@camk.edu.pl NR 72 TC 17 Z9 17 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2004 VL 608 IS 1 BP 80 EP 94 DI 10.1086/392529 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827EG UT WOS:000221881200008 ER PT J AU Reiprich, TH Sarazin, CL Kempner, JC Tittley, E AF Reiprich, TH Sarazin, CL Kempner, JC Tittley, E TI XMM-Newton observation of the merging galaxy cluster A1644 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; cosmology : observations; galaxies : clusters : general; galaxies : clusters : individual (A1644); intergalactic medium; X-rays : galaxies : clusters ID THERMAL CONDUCTION; DARK-MATTER; COLD-FRONT; CHANDRA; TEMPERATURE; MERGER; MASS; A3667; CONSTRAINTS; SUBCLUSTER AB We present an XMM-Newton imaging spectroscopy analysis of the galaxy cluster A1644. A1644 is a complex merging system consisting of a main cluster and a subcluster. A trail of cool, metal-rich gas has been discovered close to the subcluster. The combination of results from X-ray, optical, and radio data and a comparison to a hydrodynamic simulation suggest that the subcluster has passed by the main cluster off-axis and that a fraction of its gas has been stripped off during this process. Furthermore, for this merging system simple effects are illustrated that can affect the use of clusters as cosmological probes. Specifically, double clusters may affect estimates of the cluster number density when treated as a single system. Mergers, as well as cool cores, can alter the X-ray luminosity and temperature measured for clusters, causing these values to differ from those expected in equilibrium. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Reiprich, TH (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. EM thomas@reiprich.net; sarazin@virginia.edu; jkempner@cfa.harvard.edu; ert@roe.ac.uk NR 38 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2004 VL 608 IS 1 BP 179 EP 188 DI 10.1086/386318 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827EG UT WOS:000221881200016 ER PT J AU Beuther, H Schilke, P Gueth, F AF Beuther, H Schilke, P Gueth, F TI Massive molecular outflows at high spatial resolution SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; ISM : individual (IRAS 19217+1651, IRAS 20293+3952); ISM : jets and outflows; stars : formation; techniques : interferometric ID YOUNG STELLAR OBJECTS; STAR-FORMATION REGIONS; PROTOSTELLAR CANDIDATES; CO OUTFLOWS; HYDRODYNAMIC SIMULATIONS; MULTIPLE OUTFLOWS; JET-DRIVEN; SAMPLE; EMISSION; CORES AB We present high spatial resolution Plateau de Bure Interferometer CO (2-1) and SiO (2-1) observations of one intermediate-mass and one high-mass star-forming region. The intermediate-mass region IRAS 20293+3952 exhibits four molecular outflows, one being as collimated as the highly collimated jetlike outflows observed in low-mass star formation sources. Furthermore, comparing the data with additional infrared H-2 and centimeter observations, we see indications that the nearby ultracompact H II region triggers a shock wave interacting with the outflow. The high-mass region IRAS 19217+1651 exhibits a bipolar outflow as well, and the region is dominated by the central driving source. Adding two more sources from the literature, we compare position-velocity diagrams of the intermediate-to-high-mass sources with previous studies in the low-mass regime. We find similar kinematic signatures; some sources can be explained by jet-driven outflows, whereas others are better constrained by wind-driven models. The data also allow us to estimate accretion rates varying from a few times 10(-5) M. yr(-1) for the intermediate-mass sources to a few times 10(-4) M. yr(-1) for the high-mass source, consistent with models explaining star formation of all masses via accretion processes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hbeuther@cfa.harvard.edu NR 32 TC 51 Z9 52 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2004 VL 608 IS 1 BP 330 EP 340 DI 10.1086/386543 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827EG UT WOS:000221881200029 ER PT J AU Stark, R Sandell, G Beck, SC Hogerheijde, MR van Dishoeck, EF van der Wal, P van der Tak, FFS Schafer, F Melnick, GJ Ashby, MLN de Lange, G AF Stark, R Sandell, G Beck, SC Hogerheijde, MR van Dishoeck, EF van der Wal, P van der Tak, FFS Schafer, F Melnick, GJ Ashby, MLN de Lange, G TI Probing the early stages of low-mass star formation in LDN 1689N: Dust and water in IRAS 16293-2422A, B, and E SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : clouds; ISM : individual (IRAS 16293-2422); ISM : jets and outflows; ISM : molecules; stars : formation ID SUBMILLIMETER CONTINUUM OBSERVATIONS; WAVE-ASTRONOMY-SATELLITE; CLERK-MAXWELL-TELESCOPE; MOLECULAR CLOUD CORES; YOUNG STELLAR OBJECTS; PROTOSTELLAR CORES; DEUTERATED WATER; BINARY-SYSTEM; DEUTERIUM FRACTIONATION; INTERSTELLAR-MOLECULES AB We present deep images of dust continuum emission at 450, 800, and 850 mum of the dark cloud LDN 1689N, which harbors the low-mass young stellar objects (YSOs) IRAS 16293-2422 A and B (I16293A and I16293B) and the cold prestellar object I16293E. Toward the positions of I16293A and I16293E we also obtained spectra of CO-isotopomers and deep submillimeter observations of chemically related molecules with high critical densities (HCO+, (HCO+)-C-13, DCO+, H2O, HDO, and H2D+). Toward I16293A we report the detection of the HDO 1(01)-0(00) and H2O 1(10-)1(01) ground-state transitions as broad self-reversed emission profiles with narrow absorption and a tentative detection of H2D+ 1(10)-1(11). Toward I16293E we detect weak emission of subthermally excited HDO 1(01)-0(00). Based on this set of submillimeter continuum and line data, we model the envelopes around I16293A and I16293E. The density and velocity structure of I16293A is fitted by an inside-out collapse model, yielding a sound speed of a 0: 7 kms(-1), an age of t = (0.6-2.5) x 10(4) yr, and amass of 6.1 M.. The density in the envelope of I16293E is fitted by a radial power law with index -1.0 +/- 0.2, a mass of 4.4 M., and a constant temperature of 16 K. These respective models are used to study the chemistry of the envelopes of these pre- and protostellar objects. We made a large, fully sampled CO J = 2-1 map of LDN 1689N, which clearly shows the two outflows from I16293A and I16293B and the interaction of one of the flows with I16293E. An outflow from I16293E reported elsewhere is not confirmed. Instead, we find that the motions around I16293E identified from small maps are part of a larger scale fossil flow from I16293B. Modeling of the I16293A outflow shows that the broad HDO, water ground state, and CO J = 6-5 and 7-6 emission lines originate in this flow, while the HDO and H2O line cores originate in the envelope. The narrow absorption feature in the ground-state water lines is due to cold gas in the outer envelope. The derived H2O abundance is 3 x 10(-9) in the cold regions of the envelope of I16293A (T-kin < 14 K), 2 x 10(-7) in warmer regions of the envelope (> 14 K), and 10(-8) in the outflow. The HDO abundance is constant at a few times 10(-10) throughout the envelopes of I16293A and I16293E. Because the derived H2O and HDO abundances in the two objects can be understood through shock chemistry in the outflow and ion-molecule chemistry in the envelopes, we argue that both objects are related in chemical evolution. The [HDO]/[H2O] abundance ratio in the warm inner envelope of I16293A of a few times 10(-4) is comparable to that measured in comets. This supports the idea that the [HDO]/[ H2O] ratio is determined in the cold prestellar core phase and conserved throughout the formation process of low-mass stars and planets. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Tel Aviv Univ, Dept Phys & Astron, Ramat Aviv, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Groningen, SRON, NL-9700 AV Groningen, Netherlands. RP Stark, R (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. NR 95 TC 70 Z9 70 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2004 VL 608 IS 1 BP 341 EP 364 DI 10.1086/392492 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827EG UT WOS:000221881200030 ER PT J AU Jang-Condell, H Sasselov, DD AF Jang-Condell, H Sasselov, DD TI Disk temperature variations and effects on the snow line in the presence of small protoplanets SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation; planetary systems : protoplanetary disks; radiative transfer ID ACCRETION DISKS; YOUNG OBJECTS; RADIATIVE-TRANSFER; CIRCUMSTELLAR DISKS; MASS PLANETS; GROWTH; MODELS; GAP AB We revisit the computation of a "snow line'' in a passive protoplanetary disk during the stage of planetesimal formation. We examine how shadowing and illumination in the vicinity of a planet affects where in the disk ice can form, making use of our method for calculating radiative transfer on disk perturbations with some improvements on the model. We adopt a model for the unperturbed disk structure that is more consistent with observations and use opacities for reprocessed dust instead of interstellar medium dust. We use the improved disk model to calculate the temperature variation for a range of planet masses and distances and find that planets at the gap-opening threshold can induce temperature variations of up to +/- 30%. Temperature variations this significant may have ramifications for planetary accretion rates and migration rates. We discuss in particular the effect of temperature variations near the sublimation point of water, since the formation of ice can enhance the accretion rate of disk material onto a planet. Shadowing effects can cool the disk enough that ice will form closer to the star than previously expected, effectively moving the snow line inward. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jang-Condell, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hjang@cfa.harvard.edu; dsasselov@cfa.harvard.edu OI Jang-Condell, Hannah/0000-0002-7639-1322 NR 21 TC 22 Z9 22 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2004 VL 608 IS 1 BP 497 EP 508 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827EG UT WOS:000221881200044 ER PT J AU Wcislo, WT Gonzalez, VH Arneson, L AF Wcislo, WT Gonzalez, VH Arneson, L TI A review of deviant phenotypes in bees in relation to brood parasitism, and a gynandromorph of Megalopta genalis (Hymenoptera : Halictidae) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE gynandromorph; development; deviant; brood parasitism; morphology ID TRANSVESTISM; EVOLUTION; APIDAE AB We review the occurrence of gynandromorphy in 64 species of bee, and describe the abnormal traits as deviations from the male or female wild-type. Phenodeviants occur at approximately equal frequency among the main body regions (head, thorax, metasoma). Cross-sex expression of character states occur more often among females (i.e. deviant expression of male-like traits) than among males (i.e. deviant expression of female-like traits). Such pathologies demonstrate how developmental switch mechanisms might generate novel structural traits similar to those expressed as a syndrome of brood parasitic traits. We also describe the first known gynandromorphic bee in the tribe Augochlorini, a specimen of the nocturnal bee, Megalopta genalis. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Wcislo, WT (reprint author), STRI, Unit 0948, APO, AA 34002 USA. EM WcisloW@tivoli.si.edu RI Gonzalez Betancourt, Victor /B-9528-2011; Gonzalez, Victor/B-4072-2015 NR 84 TC 25 Z9 30 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD JUN 10 PY 2004 VL 38 IS 11 BP 1443 EP 1457 DI 10.1080/0022293031000155322 PG 15 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 776GQ UT WOS:000189108600009 ER PT J AU Duda, TF Palumbi, SR AF Duda, TF Palumbi, SR TI Gene expression and feeding ecology: evolution of piscivory in the venomous gastropod genus Conus SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE gene family; adaptive evolution; differential expression; Conus; conotoxins ID RESOURCE UTILIZATION; MULTIGENE FAMILIES; MITOCHONDRIAL-DNA; SNAILS; DUPLICATION; FOOD; DIVERSIFICATION; CONOPEPTIDES; SUBSTITUTION; CONOTOXINS AB Differential expression of gene-family members is typically associated with the specific development of certain tissues and organs, but its importance in the ecological adaptation of organisms has rarely been investigated. Several specialized feeding modes have evolved within the predatory marine gastropod genus Courts, including molluscivory and piscivory. Based on phylogenetic investigations of Conus species, it has been concluded that piscivory arose at least twice in this genus. Moreover, molecular analyses of conotoxin mRNA transcripts reveal that piscivores from independent evolutionary lineages express the same subset of four-loop conotoxins, contrary to phylogenetic expectations. These results demonstrate that differential expression of gene-family members can play a key role in adaptive evolution, particularly during shifts to new ecological niches. C1 Smithsonian Trop Res Inst, Naos Marine Lab, Balboa, Ancon, Panama. Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. RP Duda, TF (reprint author), Univ Washington, Dept Biol, Seattle, WA 98195 USA. EM tfduda@u.washington.edu NR 39 TC 49 Z9 70 U1 5 U2 9 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 JUN 7 PY 2004 VL 271 IS 1544 BP 1165 EP 1174 DI 10.1098/rspb.2004.2708 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 855SN UT WOS:000223994100010 PM 15306367 ER PT J AU Yu, DW Ridley, J Jousselin, E Herre, EA Compton, SG Cook, JM Moore, JC Weiblen, GD AF Yu, DW Ridley, J Jousselin, E Herre, EA Compton, SG Cook, JM Moore, JC Weiblen, GD TI Oviposition strategies, host coercion and the stable exploitation of figs by wasps SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE cooperation; Ficus; host coercion; mutualism; pollination; virulence ID POLLINATING WASPS; MONOECIOUS FIGS; EVOLUTIONARY CONFLICTS; MOLECULAR PHYLOGENY; MUTUALISM STABILITY; FICUS-SYCOMORUS; DIOECIOUS FIGS; SEX ALLOCATION; COOPERATION; SANCTIONS AB A classic example of a mutualism is the one between fig plants (Ficus) and their specialized and obligate pollinating wasps. The wasps deposit eggs in fig ovules, which the larvae then consume. Because the wasps derive their fitness only from consumed seeds, this mutualism can persist only if the wasps are prevented from laying eggs in all ovules. The search for mechanisms that can limit oviposition and stabilize the wasp-seed conflict has spanned more than three decades. We use a simple foraging model, parameterized with data from two Ficus species, to show how fig morphology reduces oviposition rates and helps to resolve the wasp-seed conflict. We also propose additional mechanisms, based on known aspects of fig biology, which can prevent even large numbers of wasps from ovipositing in all ovules. It has been suggested that in mutualistic symbioses, the partner that controls the physical resources, in this case Ficus, ultimately controls the rate at which hosts are converted to visitors, regardless of relative evolutionary rates. Our approach provides a mechanistic implementation of this idea, with potential applications to other mutualisms and to theories of virulence. C1 Univ E Anglia, CEEC, Norwich NR4 7TJ, Norfolk, England. Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. Univ Pretoria, Dept Genet, ZA-0002 Pretoria, South Africa. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Leeds, Sch Biol, Ctr Biodivers & Conservat, Leeds LS2 9JT, W Yorkshire, England. Univ Edinburgh, Inst Cell Anim & Populat Biol, Sch Biol Sci, Ashworth Labs, Edinburgh EH9 3JT, Midlothian, Scotland. Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. Univ London Imperial Coll Sci Technol & Med, Dept Biol, Ascot SL5 7PY, Berks, England. RP Yu, DW (reprint author), Univ E Anglia, CEEC, Norwich NR4 7TJ, Norfolk, England. EM douglas.yu@uea.ac.uk RI Yu, Douglas/D-2536-2009; Cook, James/D-6423-2011 OI Cook, James/0000-0001-8447-6126 NR 62 TC 31 Z9 39 U1 1 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 JUN 7 PY 2004 VL 271 IS 1544 BP 1185 EP 1195 DI 10.1098/rspb.2003.2630 PG 11 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 855SN UT WOS:000223994100012 PM 15306369 ER PT J AU Kensley, B AF Kensley, B TI Redescription and distribution of two species of Syscenus (Crustacea, Isopoda, Aegidae) in the North Atlantic SO SARSIA LA English DT Article DE Crustacea; Isopoda; Aegidae; Syscenus attanticus; Syscenus infelix; North Atlantic ID INFELIX; FISHES AB The isopod species Syscenus atlanticus Kononenko, 1988, is recorded for the second time, from Bear Seamount off New England, western North Atlantic. The species, previously known only from the central North Atlantic, is redescribed, illustrated, and compared with the more common S. infelix Harger, 1881, which is also redescribed and illustrated. The distribution of S. infelix in a broad arc across the North Atlantic Ocean, based on 171 specimens from several museum collections, is discussed. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. RP Kensley, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. NR 32 TC 2 Z9 3 U1 0 U2 0 PU TAYLOR & FRANCIS AS PI OSLO PA CORT ADELERSGT 17, PO BOX 2562, SOLLI, 0202 OSLO, NORWAY SN 0036-4827 J9 SARSIA JI Sarsia PD JUN 2 PY 2004 VL 89 IS 3 BP 160 EP 174 DI 10.1080/00364820410005412 PG 15 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 830FQ UT WOS:000222107500002 ER PT J AU Levenback, KL AF Levenback, KL TI Virginia Woolf and the discourse of science: The aesthetics of astronomy. SO ALBION LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU APPALACHIAN STATE UNIV PI BOONE PA ALBION/HISTORY DEPT 210 WHITENER HALL, BOONE, NC 28608 USA SN 0095-1390 J9 ALBION JI Albion PD SUM PY 2004 VL 36 IS 2 BP 349 EP 350 DI 10.2307/4054263 PG 2 WC History SC History GA 970KR UT WOS:000232308000054 ER PT J AU Crowell, AL Pullar, GL Steffian, AF Haakanson, S AF Crowell, AL Pullar, GL Steffian, AF Haakanson, S TI Response to Lee and Graburn's review of looking both ways: Heritage and identity of the Alutiiq people SO AMERICAN ANTHROPOLOGIST LA English DT Editorial Material C1 Smithsonian Inst, Arctic Studies Ctr, Anchorage, AK 99501 USA. Univ Alaska, Dept Alaska Native & Rural Dev, Anchorage, AK 99508 USA. Alutiiq Museum & Archaeol Repository, Kodiak, AK 99615 USA. RP Crowell, AL (reprint author), Smithsonian Inst, Arctic Studies Ctr, 121 W 7th Ave, Anchorage, AK 99501 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 USA SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD JUN PY 2004 VL 106 IS 2 BP 431 EP 432 PG 2 WC Anthropology SC Anthropology GA 836UO UT WOS:000222581500058 ER PT J AU Cavender-Bares, J Ackerly, DD Baum, DA Bazzaz, FA AF Cavender-Bares, J Ackerly, DD Baum, DA Bazzaz, FA TI Phylogenetic overdispersion in Floridian oak communities SO AMERICAN NATURALIST LA English DT Article DE phylogenetic structure of communities; null models; ecological filtering; species interactions; conserved and convergent trait evolution; Quercus ID ECOLOGICAL CHARACTER DISPLACEMENT; RAIN-FOREST TREES; RIBOSOMAL DNA; CORRELATED EVOLUTION; NICHE CONSERVATISM; PLANT-COMMUNITIES; LIFE-HISTORY; LEAF SIZE; COEXISTENCE; FAGACEAE AB Closely related species that occur together in communities and experience similar environmental conditions are likely to share phenotypic traits because of the process of environmental filtering. At the same time, species that are too similar are unlikely to co-occur because of competitive exclusion. In an effort to explain the coexistence of 17 oak species within forest communities in North Central Florida, we examined correlations between the phylogenetic relatedness of oak species, their degree of co-occurrence within communities and niche overlap across environmental gradients, and their similarity in ecophysiological and life-history traits. We show that the oaks are phylogenetically overdispersed because co-occurring species are more distantly related than expected by chance, and oaks within the same clade show less niche overlap than expected. Hence, communities are more likely to include members of both the red oak and the oak clades than only members of one clade. white + live This pattern of phylogenetic overdispersion arises because traits important for habitat specialization show evolutionary convergence. We hypothesize further that certain conserved traits permit coexistence of distantly related congeners. These results provide an explanation for how oak diversity is maintained at the community level in North Central Florida. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA. Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. RP Cavender-Bares, J (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, 1987 Upper Buford Circle, St Paul, MN 55108 USA. EM cavender@umn.edu; dackerly@stanford.edu; dbaum@wisc.edu; fbazzaz@oeb.harvard.edu RI Ackerly, David/A-1247-2009; Cavender-Bares, Jeannine/K-5716-2013; Baum, David/D-6804-2015 OI Ackerly, David/0000-0002-1847-7398; Baum, David/0000-0001-8334-6311 NR 90 TC 362 Z9 375 U1 11 U2 160 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 JUN PY 2004 VL 163 IS 6 BP 823 EP 843 PG 21 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 832LE UT WOS:000222268200006 PM 15266381 ER PT J AU Thacker, RW Paul, VJ AF Thacker, RW Paul, VJ TI Morphological, chemical, and genetic diversity of tropical marine cyanobacteria Lyngbya spp. and Symploca spp. (Oscillatoriales) SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID 16S RIBOSOMAL-RNA; BLUE-GREEN ALGAE; PAPUA-NEW-GUINEA; SECONDARY METABOLITES; FATTY-ACIDS; STYLOCHEILUS-LONGICAUDA; ABSOLUTE-CONFIGURATION; NUTRIENT ENRICHMENT; PALAUAN COLLECTIONS; SEQUENCE-ANALYSIS AB Although diverse natural products have been isolated from the benthic, filamentous cyanobacterium Lyngbya majuscula, it is unclear whether this chemical variation can be used to establish taxonomic relationships among disparate collections. We compared morphological characteristics, secondary-metabolite compositions, and partial 16S ribosomal DNA (rDNA) sequences among several collections of L. majuscula Gomont, Lyngbya spp., and Symploca spp. from Guam and the Republic of Palau. The morphological characteristics examined were cell length, cell width, and the presence or absence of a calyptra. Secondary metabolites were analyzed by two-dimensional thin-layer chromatography. Each collection possessed a distinct cellular morphology that readily distinguished Lyngbya spp. from Symploca spp. Each collection yielded a unique chemotype, but common chemical characteristics were shared among four collections of L. majuscula. A phylogeny based on secondary-metabolite composition supported the reciprocal monophyly of Lyngbya and Symploca but yielded a basal polytomy for Lyngbya. Pairwise sequence divergence among species ranged from 10 to 14% across 605 bp of 16S rDNA, while collections of L. majuscula showed 0 to 1.3% divergence. Although the phylogeny of 16S rDNA sequences strongly supported the reciprocal monophyly of Lyngbya and Symploca as well as the monophyly of Lyngbya bouillonii and L. majuscula, genetic divergence was not correlated with chemical and morphological differences. These data suggest that 16S rDNA sequence analyses do not predict chemical variability among Lyngbya species. Other mechanisms, including higher rates of evolution for biosynthetic genes, horizontal gene transfer, and interactions between different genotypes and environmental conditions, may play important roles in generating qualitative and quantitative chemical variation within and among Lyngbya species. C1 Univ Alabama, Dept Biol, Birmingham, AL 35294 USA. Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Thacker, RW (reprint author), Univ Alabama, Dept Biol, Birmingham, AL 35294 USA. EM thacker@uab.edu NR 67 TC 40 Z9 42 U1 0 U2 21 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD JUN PY 2004 VL 70 IS 6 BP 3305 EP 3312 DI 10.1128/AEM.70.6.3305-3312.2004 PG 8 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 828NX UT WOS:000221981100015 PM 15184125 ER PT J AU Mecklenburg, MF Tumosa, CS Pride, A AF Mecklenburg, MF Tumosa, CS Pride, A TI Preserving legacy buildings SO ASHRAE JOURNAL LA English DT Article C1 Smithsonian Inst, Off Facil Reliabil, Washington, DC 20560 USA. RP Mecklenburg, MF (reprint author), Smithsonian Inst, Off Facil Reliabil, Washington, DC 20560 USA. NR 10 TC 4 Z9 4 U1 0 U2 4 PU AMER SOC HEATING REFRIGERATING AIR-CONDITIONING ENG, INC, PI ATLANTA PA 1791 TULLIE CIRCLE NE, ATLANTA, GA 30329 USA SN 0001-2491 J9 ASHRAE J JI ASHRAE J. PD JUN PY 2004 VL 46 IS 6 BP S18 EP S23 PG 6 WC Thermodynamics; Construction & Building Technology; Engineering, Mechanical SC Thermodynamics; Construction & Building Technology; Engineering GA 827ML UT WOS:000221903900011 ER PT J AU Herrnstein, RM Zhao, JH Bower, GC Goss, WM AF Herrnstein, RM Zhao, JH Bower, GC Goss, WM TI The variability of Sagittarius A* at centimeter wavelengths SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy : center; radio continuum : galaxies ID SUPERMASSIVE BLACK-HOLE; X-RAY FLARE; GALACTIC-CENTER; RADIO VARIABILITY; 1 MILLIMETER; SPECTRUM; STAR AB We present the results of a 3.3 yr project to monitor the flux density of Sagittarius A* at 2.0, 1.3, and 0.7 cm with the Very Large Array. Between 2000.5 and 2003.0, 119 epochs of data were taken with a mean separation between epochs of 8 days. After 2003.0, observations were made roughly once per month for a total of nine additional epochs. Details of the data calibration process are discussed, including corrections for opacity and elevation effects, as well as changes in the flux density scales between epochs. The fully calibrated light curves for Sgr A* at all three wavelengths are presented. Typical errors in the flux density are 6.1%, 6.2%, and 9.2% at 2.0, 1.3, and 0.7 cm, respectively. There is preliminary evidence for a bimodal distribution of flux densities, which may indicate the existence of two distinct states of accretion onto the supermassive black hole. At 1.3 and 0.7 cm, there is a tail in the distribution toward high flux densities. Significant variability is detected at all three wavelengths, with the largest amplitude variations occurring at 0.7 cm. The rms deviation of the flux density of Sgr A* is 0.13, 0.16, and 0.21 Jy at 2.0, 1.3, and 0.7 cm, respectively. During much of this monitoring campaign, Sgr A* appeared to be relatively quiescent compared with results from previous campaigns. At no point during the monitoring campaign did the flux density of Sgr A* more than double its mean value. The mean spectral index of Sgr A* is alpha = 0.20 +/- 0.01 (where S-nu proportional to nu(alpha)), with a standard deviation of 0.14. The spectral index appears to depend linearly on the observed flux density at 0.7 cm with a steeper index observed during outbursts. This correlation is consistent with the expectation for outbursts that are self-absorbed at wavelengths of 0.7 cm or longer and inconsistent with the effects of simple models for interstellar scintillation. Much of the variability of Sgr A*, including possible time lags between flux density changes at the different wavelengths, appears to occur on timescales less than the time resolution of our observations ( 8 days). Future observations should focus on the evolution of the flux density on these time-scales. C1 Columbia Univ, Dept Astron, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Herrnstein, RM (reprint author), Columbia Univ, Dept Astron, Mail Code 5246,550 W 120th St, New York, NY 10027 USA. EM herrnstein@astro.columbia.edu; jzhao@cfa.harvard.edu; gbower@astron.berkeley.edu; mgoss@aoc.nrao.edu NR 28 TC 47 Z9 48 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2004 VL 127 IS 6 BP 3399 EP 3410 DI 10.1086/420711 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 828VU UT WOS:000222002600024 ER PT J AU Braito, V Della Ceca, R Piconcelli, E Severgnini, P Bassani, L Cappi, M Franceschini, A Iwasawa, K Malaguti, G Marziani, P Palumbo, GGC Persic, M Risaliti, G Salvati, M AF Braito, V Della Ceca, R Piconcelli, E Severgnini, P Bassani, L Cappi, M Franceschini, A Iwasawa, K Malaguti, G Marziani, P Palumbo, GGC Persic, M Risaliti, G Salvati, M TI The XMM-Newton and BeppoSAX view of the Ultra Luminous Infrared Galaxy MKN 231 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : galaxies; galaxies : individual : Markarian 231 ID ACTIVE GALACTIC NUCLEI; FORMATION RATE INDICATOR; RAY REFLECTION SPECTRA; K-ALPHA LINE; MARKARIAN 231; CHANDRA SURVEY; COLD MATTER; X-RAYS; STARBURST; SPECTROSCOPY AB We discuss XMM-Newton and BeppoSAX observations of MKN 231, the lowest-redshift Broad Absorption Line (BAL) QSO known so far and one of the best-studied Ultra Luminous Infrared Galaxies. By combining the XMM-Newton spectral resolution and the high-energy bandpass of BeppoSAX we have been able to Study in more detail than previously possible its 0.2-50 keV spectral properties. The BeppoSAX PDS data unveiled, for the first time, a highly absorbed (NHsimilar to2x10(24) cm(-2)) power-law component. We find that: a) below 10 keV we are seeing only reprocessed radiation through reflection and/or scattering; b) the intrinsic 2-10 keV luminosity of MKN 231 is 1(-0.5)(+1.0)x10(44) erg s(-1), i.e. more than an order of magnitude greater than previous measurements; c) the starburst activity significantly contributes to the soft (E<2 keV) X-ray emission. C1 Osserv Astron Brera, INAF, Milan, Italy. Univ Padua, Dipartimento Astron, I-35100 Padua, Italy. CNR, IASF, I-40126 Bologna, Italy. ESA, VILSPA, SOC, XMM, Madrid, Spain. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Osserv Astron Padova, INAF, I-35122 Padua, Italy. Univ Bologna, Dipartimento Astron, I-40126 Bologna, Italy. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Braito, V (reprint author), Osserv Astron Brera, INAF, Milan, Italy. EM braito@brera.mi.astro.it RI Cappi, Massimo/F-4813-2015; OI Braito, Valentina/0000-0002-2629-4989; piconcelli, enrico/0000-0001-9095-2782; Severgnini, Paola/0000-0001-5619-5896; Cappi, Massimo/0000-0001-6966-8920; Della Ceca, Roberto/0000-0001-7551-2252; Malaguti, Giuseppe/0000-0001-9872-3378; Risaliti, Guido/0000-0002-3556-977X; Persic, Massimo/0000-0003-1853-4900; Bassani, Loredana/0000-0003-4858-6963; Marziani, Paola/0000-0002-6058-4912 NR 45 TC 90 Z9 90 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2004 VL 420 IS 1 BP 79 EP 88 DI 10.1051/0004-6361:20040061 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827WK UT WOS:000221934200009 ER PT J AU Koutchmy, S Baudin, F Bocchialini, K Daniel, JY Delaboudiniere, JP Golub, L Lamy, P Adjabshirizadeh, A AF Koutchmy, S Baudin, F Bocchialini, K Daniel, JY Delaboudiniere, JP Golub, L Lamy, P Adjabshirizadeh, A TI The August 11th, 1999 CME SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs) ID CORONAL MASS EJECTIONS; MODEL; MECHANISMS; ECLIPSE AB We present here a set of observations, space borne and ground based, at different wavelengths, of the solar corona at and after the time of the total solar eclipse of August 11th. It is used to consider some unusual features of the coronal dynamics related to a limb Coronal Mass Ejection (CME) observed after the total eclipse. The complementary aspect Of Simultaneous ground-based and space-borne observations of the corona is used to produce an accurate composite image of the White Light (W-L) corona before the CME. A high arch system (possibly a dome-like structure, with large cavities inside but without a cusp further out) which appeared on the eclipse W-L images, is suggested to be a large-scale precursor of the CME, well preceding the eruption of the top part of the brightest prominence recorded in W-L. This bright prominence is shown as a filament in absorption using the Transition Region And Corona Explorer (TRACE) images taken in different coronal lines. The analysis of the images of the Large Angle and Spectrometric Coronograph (LASCO) on board the Solar and Heliospheric Observatory (SoHO), showing the progression of the CME, is discussed in an attempt to make a connection with the surface event. A SoHO-EIT (Extreme UV Imager Telescope) image sequence details the prominence eruption and shows the sudden heating processes of the ejected parts. We found that there is no reason to assume that the huge cavity is significantly destabilised well before the eruption of the upper part of the low-lying bright twisted filament which coincides with the position of one of the leas of the high arch. Observations are still compatible with the assumption of both the break-out model and of the flux rope erupting model as a result of a shear or of an increasing poloidal magnetic flux from below. We stress the possible role of buoyancy of the giant cavity as a destabilizing factor leading to the CME, noticing that some motion of coronal material back toward the surface can be seen during at least the first phase of the CME, from both EIT and LASCO observations. C1 CNRS, Inst Astrophys Paris, F-75014 Paris, France. Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. CNRS, Lab Astron Marseille, F-13376 Marseille, France. Univ Tabriz, Dept Astron, Tabriz, Iran. RP Koutchmy, S (reprint author), CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France. EM koutchmy@iap.fr NR 23 TC 11 Z9 11 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2004 VL 420 IS 2 BP 709 EP 718 DI 10.1051/0004-6361:20040109 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 837CU UT WOS:000222606200032 ER PT J AU Lumb, DH Bartlett, JG Romer, AK Blanchard, A Burke, DJ Collins, CA Nichol, RC Giard, M Marty, PB Nevalainen, J Sadat, R Vauclair, SC AF Lumb, DH Bartlett, JG Romer, AK Blanchard, A Burke, DJ Collins, CA Nichol, RC Giard, M Marty, PB Nevalainen, J Sadat, R Vauclair, SC TI The XMM-NEWTON Omega project - I. The X-ray luminosity-temperature relation at z > 0.4 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : galaxies : clusters ID BRIGHT SHARC SURVEY; DEEP CLUSTER SURVEY; GALAXY CLUSTERS; HIGH-REDSHIFT; T RELATION; INTRACLUSTER MEDIUM; DENSITY PARAMETER; ROSAT SURVEY; EVOLUTION; CATALOG AB We describe XMM-Newton Guaranteed Time observations of a sample of eight high redshift (0.45 < z < 0.62) clusters. The goal of these observations was to measure the luminosity and the temperature of the clusters to a precision of similar to10%, leading to constraints on the possible evolution of the luminosity-temperature (L-x - T-x) relation, and ultimately on the values of the matter density, Omega(M), and, to a lesser extent, the cosmological constant Omega(Lambda). The clusters were drawn from the SHARC and 160 Square Degree (160SD) ROSAT surveys and span a bolometric (0.0-20 keV) luminosity range of 2.0 to 14.4 x 10(44) erg s(-1) (H-0 = 50, Omega(M) = 1, Omega(Lambda) = 0). Here we describe our data analysis techniques and present, for the first time with XMM-Newton, a L, - T, relation. For each of the eight clusters in the sample, we have measured total (r < r(viral)) bolometric luminosities, performed beta-model fits to the radial surface profiles and made spectral fits to a single temperature isothermal model. We describe data analysis techniques that pay particular attention to background mitigation. We have also estimated temperatures and luminosities for two known clusters (Abell 2246 and RX J1325.0-3814), and one new high redshift cluster candidate (XMMU J084701.8+345117), that were detected off-axis. Characterizing the L-x - T-x relation as L-x = L-6(T/6 keV)(alpha), we find L-6 = 15.9(-5.2)(+7.6) x 10(44) erg s(-1) and alpha = 2.7 +/- 0.4 for an Omega(Lambda) = 0.0,Omega(M) = 1.0, H-0 = 50 km s(-1) Mpc(-1) cosmology at a typical redshift z similar to 0.55. Comparing with the low redshift study by Markevitch (1998), we find a to be in agreement, and assuming L-x - T-x to evolve as (1 + z)(A), we find A = 0.68 +/- 0.26 for the same cosmology and A = 1.52(-0.27)(+0.26) for an Omega(Lambda) - 0.7, Omega(M) = 0.3 cosmology. Our A values are very similar to those found previously by Vikhlinin et al. (2002) using a compilation of Chandra observations of 0.39 < z < 1.26 clusters. We conclude that there is now evidence from both XMM-Newton and Chandra for an evolutionary trend in the L, - T, relation. This evolution is significantly below the level expected from the predictions of the self-similar model for an Omega(Lambda) = 0.0,Omega(M) = 1 -0, Cosmology, but consistent with self-similar model in an Omega(Lambda) = 0.7, Omega(M) = 0.3 cosmology. Our observations lend support to the robustness and completeness of the SHARC and 160SD surveys. C1 European Space Agcy, ESTEC, Sci Payloads & Adv Concepts Off, NL-2200 AG Noordwijk, Netherlands. Univ Paris 07, APC, PCC Coll France, F-75231 Paris 05, France. Ctr Donnees Astronom Strasbourg, F-67000 Strasbourg, France. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Observ Midi Pyrenees, Astrophys Lab, CNRS, UPS, F-31400 Toulouse, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. RP European Space Agcy, ESTEC, Sci Payloads & Adv Concepts Off, NL-2200 AG Noordwijk, Netherlands. EM dlumb@rssd.esa.int NR 76 TC 53 Z9 53 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2004 VL 420 IS 3 BP 853 EP 872 DI 10.1051/0004-6361:20035687 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 845MW UT WOS:000223249600010 ER PT J AU Crapsi, A Caselli, P Walmsley, CM Tafalla, M Lee, CW Bourke, TL Myers, PC AF Crapsi, A Caselli, P Walmsley, CM Tafalla, M Lee, CW Bourke, TL Myers, PC TI Observations of L1521F: A highly evolved starless core SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radio lines : ISM; radio continuum : ISM; submillimeter ID DENSE INTERSTELLAR CLOUDS; RADIO-ASTRONOMICAL SPECTROSCOPY; COLLAPSING PRESTELLAR CORES; TAURUS MOLECULAR CLOUD; DEUTERIUM FRACTIONATION; PROTOSTELLAR CORES; DARK CLOUD; IONIZATION FRACTION; HYPERFINE-STRUCTURE; PHYSICAL-PROPERTIES AB We observed the pre-stellar core L1521F in dust emission at 1.2 mm and in two transitions each of N2H+, N2D+, (CO)-O-18 and (CO)-O-17 in order to increase the sample of well studied centrally concentrated and chemically evolved starless cores, likely on the verge of star formation, and to determine the initial conditions for low-mass star formation in the Taurus Molecular Cloud. The dust observation allows us to infer the density structure of the core and together with measurements of CO isotopomers gives us the CO depletion. N2H+ and N2D+ lines are good tracers of the dust continuum and thus they give kinematic information on the core nucleus. We derived in this object a molecular hydrogen number density n(H-2) similar to 10(6) cm(-3) and a CO depletion factor, integrated along the line of sight, f(D) = 9.5 x 10(-5)/x(obs) (CO) similar to 15 in the central 20", similar to the pre-stellar core L1544. However, the N(N2D+)/N(N2H+) column density ratio is similar to0.1, a factor of about 2 lower than that found in L1544. The observed relation between the deuterium fractionation and the integrated CO depletion factor across the core can be reproduced by chemical models if N2H+ is slightly (factor of similar to2 in fractional abundance) depleted in the central 3000 AU. The N2H+ and N2D+ linewidths in the core center are similar to0.3 km s(-1), significantly larger than in other more quiescent Taurus starless cores but similar to those observed in the center of L1544. The kinematical behaviour of L1521F is more complex than seen in L1544, and a model of contraction due to ambipolar diffusion is only marginally consistent with the present data. Other velocity 'fields, perhaps produced by accretion of the surrounding material onto the core and/or unresolved substructure, are present. Both chemical and kinematical analyses suggest that L1521F is less evolved than L1544, but, in analogy with L1544, it is approaching the "critical" state. C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Astron Nacl IGN, Madrid 28014, Spain. Korea Astron Observ, Taeduk Radio Astron Observ, Taejon 305348, South Korea. Harvard Smithsonian Ctr Astrophys, Submillimeter Array Project, Hilo, HI 96720 USA. RP Caselli, P (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM caselli@arcetri.astro.it NR 76 TC 62 Z9 62 U1 0 U2 2 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2004 VL 420 IS 3 BP 957 EP 974 DI 10.1051/0004-6361:20035915 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 845MW UT WOS:000223249600021 ER PT J AU Eichhorn, G AF Eichhorn, G TI Ten years of the Astrophysics Data System SO ASTRONOMY & GEOPHYSICS LA English DT Article AB The Astrophysics Data System (ADS) has been on-line on the web now for 10 years. It is the search system of choice for astronomers worldwide. The searchable database contains more than 3.7 million bibliographic records. In addition the ADS has almost 2.6 million scanned article pages from more than 340 000 articles, dating back as far as 1821. There are currently more than 10 000 regular users (more than 10 queries/month). ADS users issue 2 million queries per month and receive 30 million records and 1.5 million scanned article pages per month. One important aspect of the ADS is the system of links to other data providers: there are currently 6.8 million links to other on-line resources. The ADS is accessed from almost 100 countries with a wide range of the number of queries per country. In order to improve access from different parts of the world, there are 11 mirror sites of the ADS in Argentina, Brazil, Chile, China, England, France, Germany, India, Japan, Russia, and South Korea. Automatic procedures facilitate keeping these mirror sites up-to-date over the network. The ADS is funded by NASA Grant NCC5-189. The ADS is available at ads.harvard.edu. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eichhorn, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 NR 10 TC 2 Z9 2 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1366-8781 J9 ASTRON GEOPHYS JI Astron. Geophys. PD JUN PY 2004 VL 45 IS 3 BP 7 EP 9 DI 10.1046/j.1468-4004.2003.45307.x PG 3 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA 822MY UT WOS:000221545500009 ER PT J AU Riess, AG Strolger, LG Tonry, J Casertano, S Ferguson, HC Mobasher, B Challis, P Filippenko, AV Jha, S Li, WD Chornock, R Kirshner, RP Leibundgut, B Dickinson, M Livio, M Giavalisco, M Steidel, CC Benitez, T Tsvetanov, Z AF Riess, AG Strolger, LG Tonry, J Casertano, S Ferguson, HC Mobasher, B Challis, P Filippenko, AV Jha, S Li, WD Chornock, R Kirshner, RP Leibundgut, B Dickinson, M Livio, M Giavalisco, M Steidel, CC Benitez, T Tsvetanov, Z TI Type Ia supernova discoveries at z > 1 from the Hubble Space Telescope: Evidence for past deceleration and constraints on dark energy evolution SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; distance scale; galaxies : distances and redshifts; supernovae : general ID HIGH-REDSHIFT SUPERNOVAE; FARTHEST KNOWN SUPERNOVA; PROBE WMAP OBSERVATIONS; LIGHT-CURVE SHAPES; COSMOLOGICAL CONSTANT; ACCELERATING UNIVERSE; DEEP FIELD; OPTICAL-SPECTRA; ADVANCED CAMERA; K-CORRECTIONS AB We have discovered 16 Type Ia supernovae (SNe Ia) with the Hubble Space Telescope (HST) and have used them to provide the first conclusive evidence for cosmic deceleration that preceded the current epoch of cosmic acceleration. These objects, discovered during the course of the GOODS ACS Treasury program, include 6 of the 7 highest redshift SNe Ia known, all at z > 1.25, and populate the Hubble diagram in unexplored territory. The luminosity distances to these objects and to 170 previously reported SNe Ia have been determined using empirical relations between light-curve shape and luminosity. A purely kinematic interpretation of the SN Ia sample provides evidence at the greater than 99% confidence level for a transition from deceleration to acceleration or, similarly, strong evidence for a cosmic jerk. Using a simple model of the expansion history, the transition between the two epochs is constrained to be at z = 0.46 +/- 0.13. The data are consistent with the cosmic concordance model of Omega(M) approximate to 0.3; Omega(Lambda) approximate to 0.7 (chi(dof)(2) = 1.06) and are inconsistent with a simple model of evolution or dust as an alternative to dark energy. For a flat universe with a cosmological constant, we measure Omega(M) = 0.29 +/- 0.05 (equivalently, Omega(Lambda) = 0.71). When combined with external flat-universe constraints, including the cosmic microwave background and large-scale structure, we find w = -1.02+/-(0.13)(0.19) (and w < -0.76 at the 95% confidence level) for an assumed static equation of state of dark energy, P = w rho c(2). Joint constraints on both the recent equation of state of dark energy, w(0), and its time evolution, dw/dz, are a factor of similar to 8 more precise than the first estimates and twice as precise as those without the SNe Ia discovered with HST. Our constraints are consistent with the static nature of and value of w expected for a cosmological constant (i.e., w(0) = -1.0, dw/dz = 0) and are inconsistent with very rapid evolution of dark energy. We address consequences of evolving dark energy for the fate of the universe. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. European So Observ, D-85748 Garching, Germany. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. OI Benitez, Narciso/0000-0002-0403-7455 NR 92 TC 2615 Z9 2639 U1 11 U2 64 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2004 VL 607 IS 2 BP 665 EP 687 DI 10.1086/383612 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822LC UT WOS:000221540100003 ER PT J AU Norman, C Ptak, A Hornschemeier, A Hasinger, G Bergeron, J Comastri, A Giacconi, R Gilli, R Glazebrook, K Heckman, T Kewley, L Ranalli, P Rosati, P Szokoly, G Tozzi, P Wang, JX Zheng, W Zirm, A AF Norman, C Ptak, A Hornschemeier, A Hasinger, G Bergeron, J Comastri, A Giacconi, R Gilli, R Glazebrook, K Heckman, T Kewley, L Ranalli, P Rosati, P Szokoly, G Tozzi, P Wang, JX Zheng, W Zirm, A TI The X-ray-derived cosmological star formation history and the galaxy X-ray luminosity functions in the Chandra Deep Fields North and South SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : luminosity function, mass function; surveys; X-rays : galaxies ID FORMATION RATE INDICATOR; EMISSION-LINE GALAXIES; FORMATION RATE DENSITY; H-ALPHA; REDSHIFT SURVEY; STARBURST GALAXIES; SEYFERT-GALAXIES; RADIO-SOURCES; SOURCE POPULATIONS; CONFIDENCE-LIMITS AB The cosmological star formation rate in the combined Chandra Deep Fields North and South is derived from our X-ray luminosity function for galaxies in these deep fields. Mild evolution is seen up to redshift order unity with star formation rate similar to (1 + z)(2.7). This is the first directly observed normal star-forming galaxy X-ray luminosity function (XLF) at cosmologically interesting redshifts (z > 0). This provides the most direct measure yet of the X-ray-derived cosmic star formation history of the universe. We make use of Bayesian statistical methods to classify the galaxies and the two types of active galactic nuclei (AGNs), finding the most useful discriminators to be the X-ray luminosity, X-ray hardness ratio, and X-ray to optical flux ratio. There is some residual AGN contamination in the sample at the bright end of the luminosity function. Incompleteness slightly flattens the XLF at the faint end of the luminosity function. The XLF has a lognormal distribution and agrees well with the radio and infrared luminosity functions. However, the XLF does not agree with the Schechter luminosity function for the Halpha LF, indicating that, as discussed in the text, additional and different physical processes may be involved in the establishment of the lognormal form of the XLF. The agreement of our star formation history points with the other star formation determinations in different wavebands (IR, radio, Halpha) gives an interesting constraint on the initial mass function (IMF). The X-ray emission in the Chandra band is most likely due to binary stars, although X-ray emission from nonstellar sources (e.g., intermediate-mass black holes and/or low-luminosity AGNs) remains a possibility. Under the assumption that it is due to binary stars, the overall consistency and correlations between single-star effects and binary-star effects indicate that not only is the one-parameter IMF (M) constant but also the bivariate IMF(M-1, M-2) must be constant, at least at the high-mass end. Another way to put this, quite simply, is that X-ray observations may be measuring directly the binary-star formation history of the universe. X-ray studies will continue to be useful for probing the star formation history of the universe by avoiding problems of obscuration. Star formation may therefore be measured in more detail by deep surveys with future X-ray missions. C1 Johns Hopkins Univ, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. European So Observ, D-85748 Garching, Germany. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Inst Astrophys, F-75014 Paris, France. Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. Associated Univ Inc, Washington, DC 20036 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Trieste, I-34131 Trieste, Italy. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Norman, C (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA. RI Ranalli, Piero/K-6363-2013; Glazebrook, Karl/N-3488-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015 OI Ranalli, Piero/0000-0003-3956-755X; Glazebrook, Karl/0000-0002-3254-9044; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177 NR 84 TC 78 Z9 78 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2004 VL 607 IS 2 BP 721 EP 738 DI 10.1086/383487 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822LC UT WOS:000221540100007 ER PT J AU Birzan, L Rafferty, DA McNamara, BR Wise, MW Nulsen, PEJ AF Birzan, L Rafferty, DA McNamara, BR Wise, MW Nulsen, PEJ TI A systematic study of radio-induced X-ray cavities in clusters, groups, and galaxies SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : active; galaxies : clusters : general; X-rays : galaxies; X-rays : galaxies : clusters ID NRAO PMN SURVEYS; COOLING FLOWS; INTRACLUSTER MEDIUM; CHANDRA OBSERVATION; THERMAL CONDUCTION; PERSEUS CLUSTER; HEAT-CONDUCTION; METALLICITY GRADIENTS; MAGNETIC-FIELDS; BUOYANT BUBBLES AB We present an analysis of 16 galaxy clusters, one group, and one galaxy drawn from the Chandra Data Archive. These systems possess prominent X-ray surface brightness depressions associated with cavities or bubbles that were created by interactions between powerful radio sources and the surrounding hot gas. The central galaxies in these systems harbor radio sources with luminosities ranging between similar to2 x 10(38) and 7 x 10(44) ergs s(-1). The cavities have an average radius of similar to10 kpc, and they lie at an average projected distance of similar to20 kpc from the central galaxy. The minimum energy associated with the cavities ranges from pV similar to 10(55) ergs in galaxies, groups, and poor clusters to pV similar to 10(60) ergs in rich clusters. We evaluate the hypothesis that cooling in the hot gas can be quenched by energy injected into the surrounding gas by the rising bubbles. We find that the instantaneous mechanical luminosities required to offset cooling range between 1pV and 20pV per cavity. Nearly half of the systems in this study may have instantaneous mechanical luminosities large enough to balance cooling, at least for a short period of time, if the cavities are filled with a relativistic gas. We find a trend or upper envelope in the distribution of central X-ray luminosity versus instantaneous mechanical luminosity, with the sense that the most powerful cavities are found in the most X-ray-luminous systems. Such a trend would be expected if many of these systems produce bubbles at a rate that scales in proportion to the cooling rate of the surrounding gas. Finally, we use the X-ray cavities to measure the mechanical power of radio sources over six decades of radio luminosity, independently of the radio properties themselves. We find that the ratio of the instantaneous mechanical ( kinetic) luminosity to the 1.4 GHz synchrotron luminosity ranges typically between a few and roughly a few thousand for luminous radio sources but can be several thousand for weaker sources. This wide range implies that the 1.4 GHz synchrotron luminosity is an unreliable gauge of the mechanical power of radio sources. C1 Ohio Univ, Dept Phys & Astron, Clippinger Labs, Athens, OH 45701 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Wollongong, Sch Engn Phys, Wollongong, NSW 2522, Australia. RP Birzan, L (reprint author), Ohio Univ, Dept Phys & Astron, Clippinger Labs, Athens, OH 45701 USA. NR 116 TC 507 Z9 508 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2004 VL 607 IS 2 BP 800 EP 809 DI 10.1086/383519 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822LC UT WOS:000221540100014 ER PT J AU Miller, JM Fabian, AC Miller, MC AF Miller, JM Fabian, AC Miller, MC TI Revealing a cool accretion disk in the ultraluminous X-ray source M81 X-9 (Holmberg IX X-1): Evidence for an intermediate-mass black hole SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; relativity; X-rays : binaries ID SOFT STATE; EMISSION; GALAXIES; RADIO; VARIABILITY; CANDIDATES; DISCOVERY; SPECTRA; MODEL; M81 AB We report the results of an analysis of two XMM-Newton EPIC-pn spectra of the bright ultraluminous X-ray source M81 X-9 (Holmberg IX X-1) obtained in snapshot observations. Soft thermal emission is clearly revealed in spectra dominated by hard power-law components. Depending on the model used, M81 X-9 was observed at a luminosity of L-X (1.0-1.6) x 10(40) ergs s(-1) (0.3-10.0 keV). The variability previously observed in this source signals that it is an accreting source that likely harbors a black hole. Remarkably, accretion disk models for the soft thermal emission yield very low inner disk temperatures (kT 0.17-0.29 keV, including 90% confidence errors and variations between observations and disk models) and improve the fit statistic over any single-component continuum model at the 6 sigma level of confidence. This represents much stronger evidence for a cool disk than prior evidence that combined spectra from different observatories, and the strongest evidence of a cool disk in an ultraluminous X-ray source apart from that for NGC 1313 X-1. In common with NGC 1313 X-1, scaling the temperatures measured in M81 X-9 to those commonly seen in stellar-mass Galactic black holes at their highest observed fluxes (kT similar or equal to 1 keV) may imply that M81 X-9 harbors a black hole with a mass on the order of 10(3) M-circle dot; the measured disk component normalization and broadband luminosity imply black hole masses on the order of 10(2) M-circle dot. It is therefore possible that these sources harbor 10(3) M-circle dot black holes accreting at L-X similar or equal to 0.1 x L-Edd. While these results do not represent proof that M81 X-9 harbors an intermediate-mass black hole, radio and optical observations suggest that beaming and anisotropic emission from a stellar-mass black hole are unlikely to account for the implied luminosity. We further argue that the strength of the hard emission in these sources and well-established phenomena frequently observed in stellar-mass black holes near to the Eddington limit suggest that optically thick photospheres are unlikely to be the origin of the cool thermal emission in bright ultraluminous X-ray sources. For comparison to M81 X-9, we have also analyzed the previously unpublished EPIC-pn spectrum of NGC 1313 X-1; cool disk emission is again observed, and refined spectral fit parameters and mass estimates are reported. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Miller, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jmmiller@cfa.harvard.edu NR 44 TC 87 Z9 87 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2004 VL 607 IS 2 BP 931 EP 938 DI 10.1086/383563 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822LC UT WOS:000221540100028 ER PT J AU McClure-Griffiths, NM Dickey, JM Gaensler, BM Green, AJ AF McClure-Griffiths, NM Dickey, JM Gaensler, BM Green, AJ TI A distant extended spiral arm in the fourth quadrant of the Milky Way SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : kinematics and dynamics; Galaxy : structure; ISM : structure; radio lines : ISM ID GALACTIC PLANE SURVEY; NEUTRAL HYDROGEN; STELLAR STRUCTURE; GALAXY; KINEMATICS; CLOUDS; STREAM AB Using data from the Southern Galactic Plane Survey, we present a possible distant spiral arm in the fourth quadrant of the Milky Way. The very distinct and cohesive feature can be traced for over 70degrees as the most extreme positive velocity feature in the longitude-velocity diagram. The feature is at a Galactic radius between 18 and 24 kpc and appears to be the last major structure before the end of the H I disk. We compare the feature with a Galactic spiral model and show that it is well reproduced by a spiral arm of pitch angle. The arm is i similar to 9degrees quite well confined to the Galactic plane, dropping at most 1 kpc below the Galactic equator. Over most of its length, the arm is 1-2 kpc thick. C1 CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP McClure-Griffiths, NM (reprint author), CSIRO, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. EM naomi.mcclure-griffiths@csiro.au; john@astro.umn.edu; bgaensler@cfa.harvard.edu; agreen@physics.usyd.edu.au RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Dickey, John/0000-0002-6300-7459; Gaensler, Bryan/0000-0002-3382-9558 NR 26 TC 39 Z9 39 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2004 VL 607 IS 2 BP L127 EP L130 DI 10.1086/422031 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822LD UT WOS:000221540200016 ER PT J AU Rotjan, RD Blum, J Lewis, SM AF Rotjan, RD Blum, J Lewis, SM TI Shell choice in Pagurus longicarpus hermit crabs: does predation threat influence shell selection behavior? SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE behavioral plasticity; predation risk; shell selection behavior ID SIZE; SAY; ORGANIZATION; AVOIDANCE; RESPONSES; AVAILABILITY; BERNHARDUS; IMPACT; CUES AB Pagurus longicarpus hermit crabs depend on empty gastropod shells for protection against predation. Hermit crabs avoid gastropod shells in which holes have been drilled by naticid gastropods, and hermit crabs forced to occupy drilled shells are more vulnerable to predation by green crabs, Carcinus maenas. In this study, we examined the effect of predator cues on P. longicarpus shell investigation behavior and shell choice. In paired laboratory shell choice trials, we examined hermit crab response to green crab chemical cues. We compared hermit crabs from two sites differing in the percentage of Littorina littorea shells with drill holes. The percentage of time hermit crabs spent occupying intact shells increased significantly in the presence of predator cues. The effect of predator cues on the amount of time hermit crabs spent investigating shells differed between individuals from the two sites. Predator effluent had a marginal effect on the proportion of hermit crabs initially choosing intact shells and within 15 min most hermit crabs in both treatments occupied intact shells due to shell switching. These results indicate that predation cues alter P. longicarpus shell choice behavior favoring intact shells, which provide greater protection. In summary, predation appears to be a key factor influencing hermit crab shell selection behavior. C1 Tufts Univ, Dept Biol, Medford, MA 02155 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Rotjan, RD (reprint author), Tufts Univ, Dept Biol, Medford, MA 02155 USA. EM Randi.Rotjan@tufts.edu NR 39 TC 26 Z9 27 U1 0 U2 35 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD JUN PY 2004 VL 56 IS 2 BP 171 EP 176 DI 10.1007/s00265-004-0770-0 PG 6 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 824FW UT WOS:000221672700010 ER PT J AU Morse, JL Megonigal, JP Walbridge, MR AF Morse, JL Megonigal, JP Walbridge, MR TI Sediment nutrient accumulation and nutrient availability in two tidal freshwater marshes along the Mattaponi River, Virginia, USA SO BIOGEOCHEMISTRY LA English DT Article DE nitrogen; nutrient limitation; phosphorus; sediment; tidal freshwater marsh ID CHESAPEAKE BAY; SALT MARSHES; PHOSPHORUS LIMITATION; SALINITY GRADIENT; FORESTED WETLANDS; NORTH-CAROLINA; COASTAL-PLAIN; HUMIC ACIDS; NITROGEN; VEGETATION AB Sediment deposition is the main mechanism of nutrient delivery to tidal freshwater marshes (TFMs). We quantified sediment nutrient accumulation in TFMs upstream and downstream of a proposed water withdrawal project on the Mattaponi River, Virginia. Our goal was to assess nutrient availability by comparing relative rates of carbon (C), nitrogen (N), and phosphorus (P) accumulated in sediments with the C, N, and P stoichiometries of surface soils and above ground plant tissues. Surface soil nutrient contents (0.60-0.92% N and 0.09-0.13% P) were low but within reported ranges for TFMs in the eastern US. In both marshes, soil nutrient pools and C, N, and P stoichiometries were closely associated with sedimentation patterns. Differences between marshes were more striking than spatial variations within marshes: both C, N, and P accumulation during summer, and annual P accumulation rates (0.16 and 0.04 g P m(-2) year(-1), respectively) in sediments were significantly higher at the downstream than at the upstream marsh. Nitrogen: P ratios <14 in above ground biomass, surface soils, and sediments suggest that N limits primary production in these marshes, but experimental additions of N and/or P did not significantly increase above ground productivity in either marsh. Lower soil N: P ratios are consistent with higher rates of sediment P accumulation at the downstream site, perhaps due to its greater proximity to the estuarine turbidity maximum. C1 George Mason Univ, Environm Sci & Policy Dept, Fairfax, VA 22030 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. W Virginia Univ, Dept Biol, Morgantown, WV 26506 USA. RP Morse, JL (reprint author), Univ Maryland, Dept Entomol, 4176 Plant Sci Bldg, College Pk, MD 20742 USA. EM jlmorse@umd.edu RI Morse, Jennifer/D-4410-2012; OI Morse, Jennifer/0000-0001-8872-4940 NR 93 TC 26 Z9 26 U1 2 U2 34 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD JUN PY 2004 VL 69 IS 2 BP 175 EP 206 DI 10.1023/B:BIOG.0000031077.28527.a2 PG 32 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 827UY UT WOS:000221929900003 ER PT J AU Degen, B Roubilk, DW AF Degen, B Roubilk, DW TI Effects of animal pollination on pollen dispersal, selfing, and effective population size of tropical trees: A simulation study SO BIOTROPICA LA English DT Article DE Amazon; bees; Brazil; Dipteryx; Jacaranda; model; pollination; sensitivity analysis; trees ID RAIN-FOREST TREES; DRY FOREST; HONEY-BEES; ECO-GENE; MODEL; CONSEQUENCES; PHENOLOGY; COMMUNITY; PATTERNS; DENSITY AB Animals, especially insects, are principal pollen vectors of tropical trees and have behavior patterns that affect gene dispersal. Here, we explore complex pollination systems using a new simulation model Eco-Gene and considering, among other factors, flowering synchrony. spatial distribution of trees, degree of selfing, population densities, pollinator flight distances, pollen deposition, and pollinator response to floral display size. Sensitivity analyses using two contrasting tree data sets (Jacaranda copaia and Dipteryx odorata) determined the importance of each parameter on three response variables: the proportion of seeds from self-pollination, effective population size, and pollen dispersal. Spatial considerations and attractiveness of floral displays were prominent features determining the population genetic result of pollinators, and some biological implications of the results are discussed. C1 INRA, Kourou 97387, French Guiana. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Degen, B (reprint author), INRA, Campus Agron,BP 709, Kourou 97387, French Guiana. EM degen_b@kourou.cirad.fr; roubikd@tivoli.si.edu RI Degen, Bernd/S-1730-2016 NR 52 TC 18 Z9 19 U1 1 U2 12 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JUN PY 2004 VL 36 IS 2 BP 165 EP 179 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 830AB UT WOS:000222092900006 ER PT J AU Gossel, P AF Gossel, P TI Drama and discovery: The story of histoplasmosis. SO BULLETIN OF THE HISTORY OF MEDICINE LA English DT Book Review C1 Smithsonian Inst, Amer Museum Natl Hist, Washington, DC 20560 USA. RP Gossel, P (reprint author), Smithsonian Inst, Amer Museum Natl Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0007-5140 J9 B HIST MED JI Bull. Hist. Med. PD SUM PY 2004 VL 78 IS 2 BP 503 EP 504 DI 10.1353/bhm.2004.0073 PG 2 WC Health Care Sciences & Services; History & Philosophy Of Science SC Health Care Sciences & Services; History & Philosophy of Science GA 827XP UT WOS:000221937300033 ER PT J AU Triplehorn, CA Steiner, WE Wappes, JE AF Triplehorn, CA Steiner, WE Wappes, JE TI Notes on the genus Centronopus Solier (Coleoptera : Tenebrionidae) SO COLEOPTERISTS BULLETIN LA English DT Article C1 Ohio State Univ, Dept Entomol, Museum Biol Divers, Columbus, OH 43212 USA. Smithsonian Inst, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Triplehorn, CA (reprint author), Ohio State Univ, Dept Entomol, Museum Biol Divers, 1315 Kinnear Rd, Columbus, OH 43212 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU COLEOPTERISTS SOC PI NATCHEZ PA PO BOX 767, NATCHEZ, MS 39121 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD JUN PY 2004 VL 58 IS 2 BP 245 EP 246 DI 10.1649/689 PG 2 WC Entomology SC Entomology GA 838XJ UT WOS:000222746400007 ER PT J AU Guzman, HM Guevara, CA Breedy, O AF Guzman, HM Guevara, CA Breedy, O TI Distribution, diversity, and conservation of coral reefs and coral communities in the largest marine protected area of Pacific Panama (Coiba Island) SO ENVIRONMENTAL CONSERVATION LA English DT Article DE Coiba Island; coral reef management; marine protected area; octocorals; Panama; scleractinian corals ID NINO WARMING EVENT; EASTERN PACIFIC; RESERVE SELECTION; BIODIVERSITY; MORTALITY; PATTERNS AB Sampling scale and lack of attention to taxa other than scleractinian corals have limited the capacity to protect coral reefs and coral communities in Pacific Panama. The distribution of coral habitats (live coral cover) and their species richness in the largest marine protected area of Panama, the Coiba National Park (270 125 ha), is described using quadrat transects and manta tows. The species richness of scleractinian corals and octocorals was lower in coral reefs than in coral communities, and a close relationship between richness and live coral cover was observed only in coral communities. The distribution of high live coral cover in coral communities overlapped with areas of high coral species richness. Average live coral cover in communities was 64%, compared to 28% in reefs, whereas algae cover was 30% and 49%, respectively. Twenty-two coral and 34 octocoral species were observed, many only now detected in Panama as endemic or new species. Analysis of satellite imagery showed 80% of terrestrial habitats C. were mostly primary forest, and coral reefs and coral communities covered 1701) ha, about 2% of marine habitats. Shallow marine environments (< 20 m) had up to 60% calcareous red algae cover (rhodolite beds). Based on the distribution of live coral cover and species richness, three conservation units were identified as priority, with the southern and northernmost sides of the marine protected area as the most significant. These three areas encompass most of the rare and endemic species or populations, as well as species previously regarded as endangered. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Costa Rica, Escuela Biol, Museo Zool, San Jose, Costa Rica. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM guzmanh@naos.si.edu NR 44 TC 24 Z9 26 U1 4 U2 33 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0376-8929 J9 ENVIRON CONSERV JI Environ. Conserv. PD JUN PY 2004 VL 31 IS 2 BP 111 EP 121 DI 10.1017/S0376892904001250 PG 11 WC Biodiversity Conservation; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 847ID UT WOS:000223385000003 ER PT J AU Kemp, WM Batiuk, R Bartleson, R Bergstrom, P Carter, V Gallegos, CL Hunley, W Karrh, L Koch, EW Landwehr, JM Moore, KA Murray, L Naylor, M Rybicki, NB Stevenson, JC Wilcox, DJ AF Kemp, WM Batiuk, R Bartleson, R Bergstrom, P Carter, V Gallegos, CL Hunley, W Karrh, L Koch, EW Landwehr, JM Moore, KA Murray, L Naylor, M Rybicki, NB Stevenson, JC Wilcox, DJ TI Habitat requirements for submerged aquatic vegetation in Chesapeake Bay: Water quality, light regime, and physical-chemical factors SO ESTUARIES LA English DT Review ID EELGRASS ZOSTERA-MARINA; SEAGRASS THALASSIA-TESTUDINUM; DANISH COASTAL WATERS; POTAMOGETON-PERFOLIATUS; DEPTH DISTRIBUTION; HALODULE-WRIGHTII; NUTRIENT ENRICHMENT; ESTUARINE GRADIENT; SEDIMENT SULFIDE; VASCULAR PLANTS AB We developed an algorithm for calculating habitat suitability for seagrasses and related submerged aquatic vegetation (SAV) at coastal sites where monitoring data are available for five water quality variables that govern light availability at the leaf surface. We developed independent estimates of the minimum light required for SAV survival both as a percentage of surface light passing through the water column to the depth of SAV growth (PLW(min)) and as a percentage of light reaching leaves through the epiphyte layer (PLL(min)). Values were computed by applying, as inputs to this algorithm, statistically derived values for water quality variables that correspond to thresholds for SAV presence in Chesapeake Bay. These estimates of PLW(min) and PLL(min) compared well with the values established from a literature review. Calculations account for tidal range, and total light attenuation is partitioned into water column and epiphyte contributions. Water column attenuation is further partitioned into effects of chlorophyll alpha (chl alpha), total suspended solids (TSS) and other substances. We used this algorithm to predict potential SAV presence throughout the Bay where calculated light available at plant leaves exceeded PLL(min). Predictions closely matched results of aerial photographic monitoring surveys of SAV distribution. Correspondence between predictions and observations was particularly strong in the mesohaline and polyhaline regions, which contain 75-80% of all potential SAV sites in this estuary. The method also allows for independent assessment of effects of physical and chemical factors other than light in limiting SAV growth and survival. Although this algorithm was developed with data from Chesapeake Bay, its general structure allows it to be calibrated and used as a quantitative tool for applying water quality data to define suitability of specific sites as habitats for SAV survival in diverse coastal environments worldwide. C1 Univ Maryland, Horn Point Environm Lab, CES, Cambridge, MD 21613 USA. US EPA, Chesapeake Bay Program Off, Annapolis, MD 21403 USA. US Fish & Wildlife Serv, Annapolis, MD 21401 USA. US Geol Survey, Reston, VA 22092 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Hampton Rds Sanitat Dist, Virginia Beach, VA 23471 USA. Maryland Dept Nat Resources, Annapolis, MD 21401 USA. Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. RP Kemp, WM (reprint author), Univ Maryland, Horn Point Environm Lab, CES, Cambridge, MD 21613 USA. EM kemp@hpl.umces.edu RI kemp, Michael/F-9955-2013; OI Gallegos, Charles/0000-0001-5112-0166 NR 113 TC 83 Z9 87 U1 4 U2 64 PU ESTUARINE RESEARCH FEDERATION PI PORT REPUBLIC PA 2018 DAFFODIL, PO BOX 510, PORT REPUBLIC, MD 20676 USA SN 0160-8347 J9 ESTUARIES JI Estuaries PD JUN PY 2004 VL 27 IS 3 BP 363 EP 377 PG 15 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 832UK UT WOS:000222292500001 ER PT J AU Zigler, KS Lessios, HA AF Zigler, KS Lessios, HA TI Speciation on the coasts of the new world: Phylogeography and the evolution of bindin in the sea urchin genus Lytechinus SO EVOLUTION LA English DT Article DE echinoid; gamete recognition; hybridization; selection; speciation ID MITOCHONDRIAL-DNA; STRONGYLOCENTROTUS-FRANCISCANUS; GAMETIC INCOMPATIBILITY; POPULATION-STRUCTURE; MOLECULAR EVOLUTION; ADAPTIVE EVOLUTION; GENETIC-STRUCTURE; MEMBRANE-FUSION; PROTEIN BINDIN; MASS MORTALITY AB Beginning with E. Mayr's study in 1954, tropical sea urchins have played an important role in studies of speciation in the sea, but what are the processes of cladogenesis and divergence that give rise to new species in this group? We attempt to answer this question in the genus Lytechinus. Unlike the majority of other tropical sea urchin genera, which have circumtropical distributions, Lytechinus is mostly confined to the tropics and subtropics of the New World. We sequenced a region of mitochondrial cytochrome oxidase I and the entire molecule of nuclear bindin (a sperm gamete recognition protein) of nearly all species in the genus, and we assayed isozymes of three partially sympatric closely related species and subspecies. We found that in both mitochondrial DNA (mtDNA) and in bindin the genus Lytechinus is paraphyletic, encompassing Sphaerechinus granularis as the sister species of L. euerces. The rest of the species are arranged in an Atlantic clade composed of L. williamsi and L. variegatus, and a Pacific clade containing L. anamesus L. pictus, L. semituberculatus, and L. panamensis. Divergence between these clades suggests that they were separated no later than the closure of the Isthmus of Panama, and possibly before this time. Our data confirm that L. anamesus and L. pictus from California are a single species, and provide no evidence of differentiation between L. variegatus variegatus from the Caribbean and L. variegatus atlanticus from Bermuda. Lytechinus variegatus variegatus mtDNA is distinct from that of L. variegatus carolinus from the North American seaboard and the Gulf of Mexico, whereas their bindins are very similar. However, there is clear evidence of introgression of mtDNA between the two subspecies and they share alleles in all sampled isozyme loci. Lytechinus williamsi from the Caribbean shares mtDNA haplotypes with L. variegatus variegatus, and they also share isozymes in all assayed loci. Their bindin, however. is distinct and coalesces within each morphospecies. A private clade of mtDNA in L. williamsi may be indicative of former differentiation in the process of being swamped by introgression, or of recent speciation. Recent sudden expansions in effective population size may explain the predominance of a few mitochondrial haplotypes common to the two species. Despite the high divergence of bindin (relative to differentiation of mtDNA) between L. variegatus and L. williamsi, comparison of amino acid replacement to silent substitutions by various methods uncovered no evidence for positive selection on the bindin of any clade of Lytechinus. With the possible exception of L. williamsi and L. variegatus, our results are consistent with a history of allopatric speciation in Lytechinus. The molecular results from Lytechinus, along with those of other similar studies of sea urchins, suggest that the general speciation patterns deduced in the middle of last century by Mayr from morphology and geography have held up, but also have uncovered peculiarities in the evolution of each genus. C1 Smithsonian Trop Res Inst, Balboa, Panama. Duke Univ, Dept Biol, Durham, NC 27708 USA. RP Zigler, KS (reprint author), Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. EM lessiosh@naos.si.edu NR 94 TC 56 Z9 60 U1 2 U2 12 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD JUN PY 2004 VL 58 IS 6 BP 1225 EP 1241 DI 10.1111/j.0014-3820.2004.tb01702.x PG 17 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 835VP UT WOS:000222513900008 PM 15266972 ER PT J AU Parker, GG Tibbs, DJ AF Parker, GG Tibbs, DJ TI Structural phenology of the leaf community in the canopy of a Liriodendron tulipifera L. forest in Maryland, USA SO FOREST SCIENCE LA English DT Article DE canopy cover; foliage-height profile; leaf area index; spring ephemerals ID FOLIAGE-HEIGHT PROFILES; DECIDUOUS FOREST; TREES; SUCCESSION; CLIMATE; ECOLOGY; PLANTS AB We measured the vertical dynamics of leaf area in a tall, tulip poplar (Liri-odendron tulipifera)-dominated, deciduous forest on the Maryland coastal plain over three growing seasons (one intensively) using nondestructive, ground-based observations. Leaf area index (LAI) and leaf area density (LAD) were calculated by vertical level, time, and species; the time-integrated duration of leaf display (leaf area extent, LAE) was estimated by species and vertical level. In this stand LAI rises rapidly in the spring, declines slightly during the growing season, and then rapidly in the fall. In the intensively studied year, total LAI peaked at 7.1 m(2)m(-2), LAE was 1259 m(2)m(-2) day, and the length of the canopy season (time from half-maximum LAI at leaf-out to the half-maximum at decline) was 191 days. The maximum growing season LAI, the date of leaf emergence, and the LAE differed among years, ranging 0.61 m(2)m(-2), 14 days, and 261 m(2)m(-2) day, respectively. However, the timing of leaf fall was more consistent, ranging only 6 days. Each species differs in its height distribution, density, and timing of foliar display. In the canopy, leaf number, area, and duration are the bases of species importance; these differ substantially by species from typical importance values derived from stem-based attributes (density, basal area, biomass). C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Parker, GG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM parkerg@si.edu OI Parker, Geoffrey/0000-0001-7055-6491 NR 49 TC 8 Z9 8 U1 3 U2 6 PU SOC AMER FORESTERS PI BETHESDA PA 5400 GROSVENOR LANE, BETHESDA, MD 20814 USA SN 0015-749X J9 FOREST SCI JI For. Sci. PD JUN PY 2004 VL 50 IS 3 BP 387 EP 397 PG 11 WC Forestry SC Forestry GA 841VN UT WOS:000222959900011 ER PT J AU Young, KM Walker, SL Lanthier, C Waddell, WT Monfort, SL Brown, JL AF Young, KM Walker, SL Lanthier, C Waddell, WT Monfort, SL Brown, JL TI Noninvasive monitoring of adrenocortical activity in carnivores by fecal glucocorticold analyses SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE fecal glucocorticoids; cortisol; corticosterone; enzyme immunoassay; radioimmunoassay; HPLC; ACTH; stress; carnivores ID PLASMA-CORTISOL CONCENTRATIONS; CHEETAH ACINONYX-JUBATUS; AFRICAN WILD DOGS; ADRENAL ACTIVITY; DOMESTIC LIVESTOCK; CLOUDED LEOPARD; METABOLITE CONCENTRATIONS; REPRODUCTIVE PHYSIOLOGY; POSTOPERATIVE PAIN; STRESS-RESPONSE AB Measurement of glucocorticoid metabolites in feces has become an accepted method for the noninvasive evaluation of adrenocortical activity. The objective of this study was to determine if a simple cortisol enzyme immunoassay (EIA) was suitable for monitoring adrenocortical activity in a variety of carnivore species. Performance of the cortisol EIA was gauged by comparison to a corticosterone radioimmunoassay (RIA) that has been used for measuring glucocorticoid metabolites in feces of numerous species. Tests for parallelism and extraction efficiency were used to compare the cortisol EIA and corticosterone RIA across eight species of carnivores (Himalayan black bear, sloth bear, domestic cat, cheetah, clouded leopard, black-footed ferret, slender-tailed meerkat, and red wolf). The biological relevance of immunoreactive glucocorticoid metabolites in feces was established for at least one species of each Carnivora family studied with an adrenocorticotropic hormone (ACTH) challenge. High performance liquid chromatography (HPLC) analysis of fecal extracts for each species revealed (1) the presence of multiple immunoreactive glucocorticoid metabolites in feces, but (2) the two immunoassays measured different metabolites, and (3) there were differences across species in the number and polarities of metabolites identified between assay systems. ACTH challenge studies revealed increases in fecal metabolite concentrations measured by the cortisol EIA and corticosterone RIA of similar to228-1145% and similar to231-4150% above pre-treatment baseline, respectively, within 1-2 days of injection. Concentrations of fecal glucocorticoid metabolites measured by the cortisol EIA and corticosterone RIA during longitudinal evaluation (i.e., >50 days) of several species were significantly correlated (P < 0.0025, correlation coefficient range 0.383-0.975). Adrenocortical responses to physical and psychological stressors during longitudinal evaluations varied with the type of stimulus, between episodes of the same stimulus, and among species. Significant elevations of glucocorticoid metabolites were observed following some potentially stressful situations [anesthesia (2 of 3 subjects), restraint and saline injection (2 of 2 subjects), restraint and blood sampling (2 of 6 episodes), medical treatment (1 of 1 subject)], but not in all cases [e.g., gonadotropin injection (n = 4), physical restraint only (n = 1), mate introduction/breeding (n = 1), social tension (n = 1), construction (n = 2) or relocation (n = 1)]. Results reinforced the importance of an adequate baseline period of fecal sampling and frequent collections to assess adrenocortical status. The corticosterone RIA detected greater adrenocortical responses to exogenous ACTH and stressful exogenous stimuli in the Himalayan black bear, domestic cat (female), cheetah, clouded leopard, slender-tailed rneerkat, and red wolf, whereas the cortisol EIA proved superior to resolving adrenocortical responses in the black-footed ferret and domestic cat (male). Overall results suggest the cortisol EIA tested in this study offers a practical method for laboratories restricted in the usage of radioisotopes (e.g., zoological institutions and field facilities) to integrate noninvasive monitoring of adrenocortical activity into studies of carnivore behavior and physiology. (C) 2004 Published by Elsevier Inc. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Le Zoo Granby, Granby, PQ, Canada. Point Defiance Zoo & Aquarium, Tacoma, WA USA. RP Brown, JL (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. EM jbrown@crc.si.edu NR 84 TC 125 Z9 133 U1 9 U2 70 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 JUN PY 2004 VL 137 IS 2 BP 148 EP 165 DI 10.1016/j.ygcen.2004.02.016 PG 18 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 826TJ UT WOS:000221851500004 PM 15158127 ER PT J AU Oliveira, RC Nunes, FMF Campos, APS de Vasconcelos, SM Roubik, D Goulart, LR Kerr, WE AF Oliveira, RC Nunes, FMF Campos, APS de Vasconcelos, SM Roubik, D Goulart, LR Kerr, WE TI Genetic divergence in Tetragonisca angustula Latreille, 1811 (Hymenoptera, Meliponinae, Trigonini) based on rapd markers SO GENETICS AND MOLECULAR BIOLOGY LA English DT Article DE Tetragonisca angustula; genetic divergence; molecular markers; UPGMA ID PCR; DNA; L. AB One of the commonest neotropical stingless bees is Tetragonisca angustula (Latreille, 1811), popularly known in Portuguese as jatai, which occurs invariable nesting sites from Mexico to Argentina. We used 18 primers to generate 218 RAPD markers which we used to determined the genetic distance between T angustula populations from 25 localities in three different Latin America countries, using Tetragonisca weyrauchi from the Brazilian state of Acre and the common honey bee (Apis mellifera) as outgroups. Genetic distance, calculated as the Percentage of Dissimilarity (14%), based on all markers divided the T. angustula population into eastern (group 1) and western (group 2) groups. However, we were able to separate the two groups by using only two primers that have generated five specific molecular markers. The eastern group consists of T. angustula angustula which occurs from Panama to the Brazilian states of Maranhao and northern Minas Gerais and has spread through the Brazilian Atlantic Forest as far as the southern Brazilian state of Santa Catarina. Group 2 is made up of T. angustula fiebrigi which has a more southerly and western distribution, occurring only in the western Brazilian states of Mato Grosso and Mato Grosso do Sul as well as the west of some other Brazilian states (Goias, Minas Gerais, Sao Paulo, Parana and Santa Catarina) and northeastern Argentina. C1 Univ Fed Uberlandia, Inst Genet & Bioquim, BR-38400902 Uberlandia, MG, Brazil. Univ Sao Paulo, Dept Genet, Sao Paulo, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. RP Oliveira, RC (reprint author), Univ Fed Uberlandia, Inst Genet & Bioquim, Bloco 2E 33, BR-38400902 Uberlandia, MG, Brazil. EM rosanadco@hotmail.com RI Nunes, Francis/F-5871-2010; Goulart, Luiz/G-7357-2012 OI Nunes, Francis/0000-0002-7769-3058; Goulart, Luiz/0000-0002-1803-4861 NR 12 TC 16 Z9 17 U1 0 U2 1 PU SOC BRASIL GENETICA PI RIBEIRAO PRET PA RUA CAP ADELMIO NORBET DA SILVA, 736, ALTO DA BOA VISTA, 14025-670 RIBEIRAO PRET, BRAZIL SN 1415-4757 J9 GENET MOL BIOL JI Genet. Mol. Biol. PD JUN PY 2004 VL 27 IS 2 BP 181 EP 186 DI 10.1590/S1415-47572004000200009 PG 6 WC Biochemistry & Molecular Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Genetics & Heredity GA 842FP UT WOS:000222989100009 ER PT J AU Fagan, TJ Krot, AN Keil, K Yurimoto, H AF Fagan, TJ Krot, AN Keil, K Yurimoto, H TI Oxygen isotopic evolution of amoeboid olivine aggregates in the reduced CV3 chondrites Efremovka, Vigarano, and Leoville SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ALUMINUM-RICH INCLUSIONS; EARLY SOLAR-SYSTEM; SAN-CARLOS OLIVINE; CARBONACEOUS CHONDRITES; AQUEOUS ALTERATION; PARENT-BODY; ALLENDE METEORITE; REFRACTORY INCLUSIONS; SELF-DIFFUSION; NEBULA AB Amoeboid olivine aggregates (AOAs) from the reduced CV chondrites Efremovka, Vigarano, and Leoville consist of forsteritic olivine, FeNi-metal and a refractory component composed of spinel, Al-diopside, +/- anorthite. Secondary ferrous olivine and alkali-rich minerals (nepheline and sodalite), commonly observed in the oxidized CVs, are rare. Mineralogy and chemical compositions of AOAs are similar to those predicted by equilibrium thermodynamic condensation models, suggesting that AOAs formed primarily by gas-solid condensation over a narrow temperature range, slightly below the temperatures over which most Ca-Al-rich inclusions (CAIs) formed. AOAs in the reduced CVs preserve a 1(st)-generation (16)O-rich signal (delta(17,18)O similar to -40parts per thousand) similar to that observed in many CAls, suggesting that these refractory objects originated from a common source in the solar nebula. In fact AOAs and many fine-grained CAls may have formed by the same processes, but at slightly different temperatures, and can be considered a single class of refractory objects. Alteration of the AOAs is manifested by differing extents of (16)O-depletion in original AOA minerals, FeO-enrichment in olivine, and formation of interstitial very fine grained Na-bearing phases. From the six AOAs and one fine-grained, melilite-pyroxene-rich CAI examined in this study, five distinct patterns of alteration were identified. (1) One unaltered AOA from Vigarano is characterized by (16)O-rich forsterite without FeO-rich rims and interstitial Na-bearing phases. (2) Weak alteration in the melilite-pyroxene-rich CAI is characterized by incomplete (16)O-depletion in some melilite and precipitation of Na-bearing phases near the CAI rim. (3) Oxygen isotopic composition and mineralogy are correlated in two AOAs from Leoville with (16)O-rich olivine, (16)O-poor anorthite and a range of intermediate compositions in Al-diopside. This pattern is consistent with model diffusion between original grains and a (16)O-poor reservoir during a relatively short-term ( < 60 yr), high-temperature (900-1100degreesC) event. (4) Original forsterite has been enriched in FeO, but remained (16)O-rich in one AOA from Vigarano. This result is consistent with the slower rate of diffusion of O than Fe and Mg in olivine. At least some interstitial phases are (16)O-rich, and Na-bearing phases are abundant in this AOA. (5) In contrast, oxygen isotopic composition and Fo-content are correlated in two AOAs from Eftemovka. The olivine in these AOAs tends to have forsteritic (16)O-rich cores and FeO-rich (16)O-depleted rims. The general correlation between oxygen isotopic composition and Fo-content is difficult to model by diffusion, and may have formed instead by aqueous dissolution and precipitation along the margins of preexisting olivine grains. Independent evidence for aqueous alteration of the Eftemovka AOAs is provided by OH-rich signals detected during ion beam sputtering of some of the (16)O-poor olivine. Elevated (16)OH-count rates and order of magnitude increases in (16)OH detected during single analyses reflect trapping of an aqueous phase in (16)O-depleted olivine. An elevated (16)OH signal was also detected in one analysis of relatively (16)O-poor melilite in the melilite-pyroxene CAI from Vigarano, suggesting that this object also was altered by aqueous fluid. Copyright (C) 2004 Elsevier Ltd. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. RP Fagan, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. EM fagan.tim@nmnh.si.edu NR 83 TC 32 Z9 32 U1 0 U2 3 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 JUN PY 2004 VL 68 IS 11 BP 2591 EP 2611 DI 10.1016/j.gca.2003.10.033 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 823UG UT WOS:000221638200014 ER PT J AU Heaney, PJ Vicenzi, EP Breval, E AF Heaney, PJ Vicenzi, EP Breval, E TI The origin of porosity in carbonado diamond SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 14th Annual V M Goldschmidt Conference CY JUN 05-11, 2004 CL Univ Copenhagen, Copenhagen, DENMARK SP European Assoc Geochem, Geochem Soc, Geochem Soc Japan, Mineralog Soc Amer HO Univ Copenhagen C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Mat Res Lab, University Pk, PA 16802 USA. EM heaney@geosc.psu.edu; vicenzi@volcano.si.edu; exb6@psu.edu NR 0 TC 1 Z9 1 U1 0 U2 0 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 JUN PY 2004 VL 68 IS 11 SU S BP A115 EP A115 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 827TH UT WOS:000221923400176 ER PT J AU Johnson, EA Post, JE AF Johnson, EA Post, JE TI Water in the interlayer region of birnessite: An infrared spectroscopic study SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 14th Annual V M Goldschmidt Conference CY JUN 05-11, 2004 CL Univ Copenhagen, Copenhagen, DENMARK SP European Assoc Geochem, Geochem Soc, Geochem Soc Japan, Mineralog Soc Amer HO Univ Copenhagen C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM johnson.elizabeth@nmnh.si.edu NR 0 TC 0 Z9 0 U1 1 U2 4 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 JUN PY 2004 VL 68 IS 11 SU S BP A33 EP A33 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 827TH UT WOS:000221923400021 ER PT J AU Logan, MA AF Logan, MA TI Geochemistry of cadmium in sphalerite from Creede, CO, USA: A tool to study fractionation in hydrothermal systems SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 14th Annual V M Goldschmidt Conference CY JUN 05-11, 2004 CL Univ Copenhagen, Copenhagen, DENMARK SP European Assoc Geochem, Geochem Soc, Geochem Soc Japan, Mineralog Soc Amer HO Univ Copenhagen C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. EM Logan.amelia@nmnh.si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 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 JUN PY 2004 VL 68 IS 11 SU S BP A77 EP A77 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 827TH UT WOS:000221923400104 ER PT J AU Lopano, CL Heaney, PJ Post, JE Hanson, J Komarneni, S AF Lopano, CL Heaney, PJ Post, JE Hanson, J Komarneni, S TI Time-resolved structural analysis of K-, Ba-, and Cs-exchange in synthetic birnessite using synchrotron X-ray diffraction SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 14th Annual V M Goldschmidt Conference CY JUN 05-11, 2004 CL Univ Copenhagen, Copenhagen, DENMARK SP European Assoc Geochem, Geochem Soc, Geochem Soc Japan, Mineralog Soc Amer HO Univ Copenhagen C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Brookhaven Natl Lab, Dept Chem, Upton, NY 11973 USA. Penn State Univ, Dept Crop & Soil Sci, University Pk, PA 16802 USA. Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA. EM clopano@geosc.psu.edu; heaney@geosc.psu.edu; post.jeffrey@nmnh.si.edu; hanson1@bnl.gov; komarneni@geosc.psu.edu NR 1 TC 0 Z9 0 U1 0 U2 0 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 JUN PY 2004 VL 68 IS 11 SU S BP A86 EP A86 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 827TH UT WOS:000221923400121 ER PT J AU Post, JE Heaney, PJ Hanson, J AF Post, JE Heaney, PJ Hanson, J TI In situ synchrotron X-ray diffraction study of the dehydration behaviors of Na- and K-birnessites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 14th Annual V M Goldschmidt Conference CY JUN 05-11, 2004 CL Univ Copenhagen, Copenhagen, DENMARK SP European Assoc Geochem, Geochem Soc, Geochem Soc Japan, Mineralog Soc Amer HO Univ Copenhagen C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Brookhaven Natl Lab, Dept Chem, Upton, NY 11973 USA. EM post.jeffrey@nmnh.si.edu NR 0 TC 1 Z9 1 U1 0 U2 1 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 JUN PY 2004 VL 68 IS 11 SU S BP A64 EP A64 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 827TH UT WOS:000221923400079 ER PT J AU Kavelaars, JJ Holman, MJ Grav, T Milisavljevic, D Fraser, W Gladman, BJ Petit, JM Rousselot, P Mousis, O Nicholson, PD AF Kavelaars, JJ Holman, MJ Grav, T Milisavljevic, D Fraser, W Gladman, BJ Petit, JM Rousselot, P Mousis, O Nicholson, PD TI The discovery of faint irregular satellites of Uranus SO ICARUS LA English DT Article DE irregular satellites; Uranus ID INCLINATION; EVOLUTION; ORIGIN AB We report the discovery of four new urarian irregular satellites in our deep, m(R) similar to 25.4, optical search around that planet. The orbital properties of these satellites are diverse. There is some grouping of inclinations and one of the satellites appears to be inside the Kozai resonant zone of Uranus. Further, we find that the differential size distribution of satellites is rather shallow compared to objects in the asteroid and Kuiper belts, going as similar tor(-2-4). We also report a strong coupling between semi-major axis and orbital eccentricity. We comment on the apparent paradox between the inclination grouping, shallow size distribution, and orbital correlation as they relate to the likelihood of a collisional origin for the uranian irregulars. The currently observed irregulars appear to be consistent with a disruptive formation process and a collisional origin for Uranus' obliquity. Crown Copyright (C) 2004 Published by Elsevier Inc. All rights reserved. C1 Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. McMaster Univ, Dept Phys & Astron, Hamilton, ON L8M 4S1, Canada. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Observ Besancon, F-25010 Besancon, France. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Kavelaars, JJ (reprint author), Natl Res Council Canada, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. EM jj.kavelaars@nrc-cnrc.gc.ca NR 17 TC 25 Z9 25 U1 0 U2 1 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 JUN PY 2004 VL 169 IS 2 BP 474 EP 481 DI 10.1016/j.icarus.2004.01.009 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 823IM UT WOS:000221604300015 ER PT J AU Vencl, FV AF Vencl, FV TI Allometry and proximate mechanisms of sexual selection in Photinus fireflies, and some other beetles SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Flash Communication - Fireflies at Fifty CY JAN 04-08, 2003 CL Toronto, CANADA ID COMPETITION; PERFORMANCE; DIMORPHISM; COLEOPTERA; EVOLUTION; PARADOX; SIZE; LEK AB Ever since Darwin identified it as the force responsible for the evolution of exaggerated male characters, sexual selection has been the focus of research aimed at understanding the most bizarre and intriguing morphologies and behaviors in Nature. Two congeneric species in the firefly genus Photinus, P. pyralis and P. macdermotti, afford a unique opportunity to examine the interaction between sexual and countervailing natural selection that act to shape the evolution of mating behavior and body size in closely related species with very different courtship strategies. Photinus pyralis males emit very bright Hashes during their extended patrolling flights and form 'love knots' of competing suitors, while P. macdermotti males, whose courtships seldom exceed two competing males, produce weaker flashes during a shorter patrolling period. Possibly as a consequence of their scramble competition and long flights, not only is there an extremely wide range of body sizes in P. pyralis males, but they also exhibit wing allometric slopes greater than one, and lantern allometries less than one. In contrast, P. macdermotti males do not have allometric slopes significantly different from one. Small males, when tested in an artificial scramble situation move faster than large males, an advantage in the intense competition that ensues once a female is located. Females answer several males in alternation and fail to respond to all male flashes, with the evident consequence that love knots frequently develop around such fickle females. Allometric relationships in two non-luminescent beetle species with non-visual courtship protocols are compared. Visual, sexually selected characters showed positive allometric slopes, while non-visual characters showed isometry or negative slopes. Data presented here support the existence of distinct patterns in modality-specific sexual selection. C1 SUNY Stony Brook, Stony Brook, NY 11794 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Vencl, FV (reprint author), SUNY Stony Brook, Stony Brook, NY 11794 USA. EM fvencl@life.bio.sunysb.edu NR 27 TC 20 Z9 21 U1 3 U2 14 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUN PY 2004 VL 44 IS 3 BP 242 EP 249 DI 10.1093/icb/44.3.242 PG 8 WC Zoology SC Zoology GA 846ZJ UT WOS:000223358000008 PM 21676703 ER PT J AU Biddison, D AF Biddison, D TI Protecting cultures or suppressing them? SO JOURNAL OF AMERICAN ETHNIC HISTORY LA English DT Review C1 Smithsonian Inst, Arctic Studies Ctr, Washington, DC 20560 USA. RP Biddison, D (reprint author), Smithsonian Inst, Arctic Studies Ctr, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 2 PU TRANSACTION PERIOD CONSORTIUM PI PISCATAWAY PA RUTGERS UNIV, DEPT 8010, 35 BERRUE CIRCLE, PISCATAWAY, NJ 08854-8042 USA SN 0278-5927 J9 J AM ETHNIC HIST JI J. Am. Ethn. Hist. PD SUM PY 2004 VL 23 IS 4 BP 150 EP 152 PG 3 WC Ethnic Studies; History SC Ethnic Studies; History GA 865FO UT WOS:000224688100008 ER PT J AU Launius, RD AF Launius, RD TI The national labs: Science in an American system, 1947-1974. SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD JUN PY 2004 VL 91 IS 1 BP 303 EP 304 PG 2 WC History SC History GA 830AQ UT WOS:000222094400129 ER PT J AU Sharrer, GT AF Sharrer, GT TI Valuing animals: Veterinarians and their patients in modern America. SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Sharrer, GT (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD JUN PY 2004 VL 91 IS 1 BP 336 EP 337 PG 2 WC History SC History GA 830AQ UT WOS:000222094400166 ER PT J AU Trueman, CNG Behrensmeyer, AK Tuross, N Weiner, S AF Trueman, CNG Behrensmeyer, AK Tuross, N Weiner, S TI Mineralogical and compositional changes in bones exposed on soil surfaces in Amboseli National Park, Kenya: diagenetic mechanisms and the role of sediment pore fluids SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE bone; diagenesis; crystallinity; collagen; trace elements; permineralization; amboseli ID STRONTIUM ISOTOPE RATIOS; ARCHAEOLOGICAL BONE; TRACE-ELEMENTS; FOSSIL BONE; OXYGEN ISOTOPES; RECORD; APATITE; RECONSTRUCTION; CRYSTALLINITY; PRESERVATION AB Bones exposed on tropical savannah grasslands of Amboseli National Park, Kenya undergo extensive post-mortem alteration within 40 years. A combined analytical approach involving TEM microscopy, trace metal analysis, FTIR spectroscopy, and petrographic analysis has revealed a complex, dynamic diagenetic environment operating within exposed bones, driven by evaporative transport of soil water from the bone/soil interface to the upper exposed surface of the bone. This process results in extensive bone/soil-water interaction, and is responsible for increases in the concentrations of trace elements such as Ba and La of 100 --> 1000% within 15 years. The maximum and mean size of bone crystallites increases with continued exposure. This change in mean crystallite length is correlated positively with increases in bone crystallinity, which in turn is associated with degradation of the bone protein. Microbial decomposition is rarely observed in the Amboseli bones, but where present resulted in severe dissolution-reprecipitation of bone mineral. Many bones showed extensive permineralization of the larger vascular spaces with calcite and barite and, to a lesser extent, crandallite. Permineralization of unburied bones may account for 95% reduction in macro (micron-millimeter scale) porosity in the bone within 2 years of death. We produce a model for pre-burial diagenesis of bone in and tropical environments that highlights extensive alteration of bone chemistry within 1-40 years post-mortem. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Portsmouth, Sch Earth & Environm Sci, Portsmouth PO1 3QL, Hants, England. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Washington, DC 20560 USA. Weizmann Inst Sci, Dept Biol Struct, IL-76100 Rehovot, Israel. RP Trueman, CNG (reprint author), Univ Portsmouth, Sch Earth & Environm Sci, Burnaby Bldg, Portsmouth PO1 3QL, Hants, England. EM clive.trueman@port.ac.uk RI Trueman, Clive/E-6925-2011 NR 56 TC 163 Z9 165 U1 6 U2 43 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 JUN PY 2004 VL 31 IS 6 BP 721 EP 739 DI 10.1016/j.jas.2003.11.003 PG 19 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 812AT UT WOS:000220813100006 ER PT J AU Cavanaugh, DP Sternberg, RV AF Cavanaugh, DP Sternberg, RV TI Analysis of morphological groupings using ANOPA, a pattern recognition and multivariate statistical method: A case study involving centrarchid fishes SO JOURNAL OF BIOLOGICAL SYSTEMS LA English DT Article DE empirical morphospaces; N-dimensional character state correlations; character state incongruence; taxic discontinuity; Percoidei; Centrarchidae ID EMPIRICAL REJECTION; POLARITY CRITERION; PHYLOGENY AB Morphological relationships within and among taxonomic groups can be very complicated, with anatomical data often supporting two or more incongruent groupings. One possibility is that incongruent character states are taxonomically informative, although in an N-dimensional taxic space. To test the above, morphological relationships of centrarchid fish species were examined using a new pattern recognition, multivariate correlation, and multivariate statistical analysis method (ANOPA). The objective of ANOPA is to identify N-dimensional pattern space correlations among character states, relations that cannot be detected with standard phenetic or phylogenetic approaches. ANOPA provides a solution to an inherent weakness in statistical analysis which occurs in the face of set classification ambiguity, where there is no a priori reason to assign a membership or class identification within multivariate statistical groups. This approach revealed the percoid fish family Centrarchidae to be a statistically significant, cohesive group with complicated internal relationships. Centrarchid taxa are resolved into three major generic aggregates by two and three-dimensional ANOPA, and discrete subgroups were also detected. The complex interrelationships within the Centrarchidae cannot be readily collapsed to a bifurcating tree-structure, explaining the multitude of conflicting phylogenetic hypotheses that have been presented. This is the first robust study of anatomical disparity in teleostean fishes. Applications of ANOPA to the study of morphological gaps, complex taxonomic patterns, and anatomical disparity are discussed. C1 Smithsonian Inst, Dept Zool, Washington, DC 20013 USA. RP Cavanaugh, DP (reprint author), 27329 Alberta Dr, Harvest, AL 35749 USA. NR 24 TC 1 Z9 1 U1 0 U2 3 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-3390 J9 J BIOL SYST JI J. Biol. Syst. PD JUN PY 2004 VL 12 IS 2 BP 137 EP 167 DI 10.1142/S0218339004001117 PG 31 WC Biology; Mathematical & Computational Biology SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational Biology GA 840AM UT WOS:000222829400002 ER PT J AU Rossi, AM Stiling, P Moon, DC Cattell, MV Drake, BG AF Rossi, AM Stiling, P Moon, DC Cattell, MV Drake, BG TI Induced defensive response of myrtle oak to foliar insect herbivory in ambient and elevated CO2 SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE induced defense; tannins; C : N ratio; leafminers; Quercus myrtifolia; elevated CO2 ID ATMOSPHERIC CO2; LEAF TANNINS; PAPER BIRCH; GENOTYPIC VARIATION; CONDENSED TANNIN; SEASONAL CHANGES; DECIDUOUS TREES; CARBON-DIOXIDE; CLIMATE-CHANGE; PERFORMANCE AB The rising level of atmospheric CO2 has stimulated several recent studies attempting to predict the effects of increased CO2 on ecological communities. However, most of these studies have been conducted in the benign conditions of the laboratory and in the absence of herbivores. In the current study, we utilized large octagonal chambers, which enclosed portions of an intact scrub-oak community to investigate the interactive effects of CO2 and insect herbivory on myrtle oak, Quercus myrtifolia. Specifically, we assessed the effects of ambient and elevated CO2 (2 x current concentrations) on percent foliar nitrogen, C:N ratio, total relative foliar tannin content, and the presence of leaf damage caused by leaf mining and leaf chewing insects that feed on myrtle oak. Total foliar N declined and C: N ratios increased significantly in oaks in elevated CO2 chambers. The percentages of leaves damaged by either leafminers or leaf chewers tended to be lower in elevated compared to ambient chambers, but they co-occurred on leaves less than expected, regardless of CO2 treatment. Leaves that had been either mined or chewed exhibited a similar wounding or defensive response; they had an average of 25 and 21% higher protein binding ability, which is correlated with tannin concentration, compared to nondamaged control leaves, respectively. While the protein-binding ability (expressed as total percent tannin) of leaves from elevated CO2 was slightly higher than from leaves grown in ambient chambers, this difference was not significant. C1 Univ N Florida, Dept Biol, Jacksonville, FL 32224 USA. Univ S Florida, Dept Biol, Tampa, FL 32306 USA. Univ Wisconsin, Dept Biol & Microbiol, Oshkosh, WI 54901 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21034 USA. RP Rossi, AM (reprint author), Univ N Florida, Dept Biol, Jacksonville, FL 32224 USA. EM arossi@unf.edu NR 48 TC 28 Z9 31 U1 0 U2 14 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD JUN PY 2004 VL 30 IS 6 BP 1143 EP 1152 DI 10.1023/B:JOEC.0000030268.78918.3a PG 10 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 827DS UT WOS:000221879700004 PM 15303319 ER PT J AU Stanley, JD Warne, AG Schnepp, G AF Stanley, JD Warne, AG Schnepp, G TI Geoarchaeological interpretation of the canopic, largest of the relict nile delta distributaries, Egypt SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Abu Qir Bay; archaeology; avulsion; canopic promontory; channel migration; Eastern Canopus; navigation; Nile floods; sea-level rise; subsidence; substrate failure; trade centers ID LATE QUATERNARY EVOLUTION; COAST; ALEXANDRIA; POSITION; HISTORY; ROSETTA; BRANCH; MOUTH AB The Canopic branch, the largest relict Nile distributary, once flowed across the NW Nile delta of Egypt to the Mediterranean. This study focuses on the Canopic's evolution at the delta margin and in Abu Qir Bay seaward of the coast. Information from historic documents, integrated with data from geographical, geological, and archaeological exploration in the bay, indicates that the Canopic distributary was active from similar to4000 B.C. to the end of the 1st millennium A.D. Fluvial discharge persisted through pre-Dynastic, Dynastic, Greek, Roman, Byzantine and early Arabic time. The channel flowed to two sites, Herakleion and Eastern Canopus, established by the Greeks as navigational gateways for trade in the delta and surrounding region. Eastern Canopus functioned until the mid-8th century A.D. At that time, flow in the Canopic had decreased markedly, and Nile water was diverted to the east, through the Bolbitic-Rosetta branch. By the end of the first millennium A.D., Nile water was channeled in the Rosetta and Damietta distributaries, and the Canopic branch eventually converted to a canal and drain system. The Canopic promontory across which the branch flowed, and the 2 ancient sites located at the promontory coast near Canopic channel mouths, subsided beneath the waters of the bay after the 8th century. Submergence was a response to interaction of eustatic sea-level rise, annual floods, growth-faulting, soft-sediment deformation and other natural processes. As the Canopic promontory subsided, Abu Qir Bay attainted a marked concave-seaward shape and its shoreline shifted southward. This geoarchaeological investigation helps distinguish the long-term impact of natural events from that of increased human activity. This distinction is of practical importance for the highly populated and vulnerable delta margin that continues to experience submergence and erosion. C1 Smithsonian Inst, Geoarchaeol Global Change Program, NMNH, Washington, DC 20560 USA. ARCOCEA Int, F-38170 Seyssinet Pariset, France. RP Stanley, JD (reprint author), Smithsonian Inst, Geoarchaeol Global Change Program, NMNH, E-206, Washington, DC 20560 USA. NR 46 TC 7 Z9 7 U1 0 U2 6 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD SUM PY 2004 VL 20 IS 3 BP 920 EP 930 DI 10.2112/1551-5036(2004)20[920:GIOTCL]2.0.CO;2 PG 11 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 872JN UT WOS:000225203600029 ER PT J AU Park, KD Nerem, RS Schenewerk, MS Davis, JL AF Park, KD Nerem, RS Schenewerk, MS Davis, JL TI Site-specific multipath characteristics of global IGS and CORS GPS sites SO JOURNAL OF GEODESY LA English DT Article DE GPS; multipath; post-fit phase residuals AB The site-specific multipath characteristics of 217 Global Positioning System (GPS) sites worldwide were analyzed using the variability of the post-fit phase residuals. Because the GPS satellite constellation returns to the same configuration in a sidereal day (23 h 56 min 4 s), the multipath repeats on that period. However, daily GPS position estimates are usually based on the solar day. When several days of GPS data are processed, this steady change in the orientation of the satellite constellation with respect to the station manifests itself in the form of patterns in the post-fit phase residuals which shift by 3 min 56 s per day. It was found that the mean root mean square of the time-shifted post-fit phase residuals is highly dependent on the GPS antenna type. The conclusions derived from the analysis of the time-shifted post-fit residuals were verified by performing a cross-correlation of the post-fit residuals across many days for selected sites. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Colorado, Dept Aerosp Engn Sci, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. NOAA, NNGS6, Silver Spring, MD 20910 USA. Korea Astron Observ, Taejon 305348, South Korea. RP Park, KD (reprint author), Kookmin Univ, Coll Forest Sci, 861-1 Chongnung Dong, Seoul 132702, South Korea. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 7 TC 12 Z9 15 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0949-7714 J9 J GEODESY JI J. Geodesy PD JUN PY 2004 VL 77 IS 12 BP 799 EP 803 DI 10.1007/s00190-003-0359-9 PG 5 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 827FO UT WOS:000221885100001 ER PT J AU Ibanez, R Crawford, AJ AF Ibanez, R Crawford, AJ TI A new species of Eleutherodactylus (Anura : Leptodactylidae) from the Darien Province, Panama SO JOURNAL OF HERPETOLOGY LA English DT Article AB A new species of Eleutherodactylus is described from the Serrania de Pirre, Darien Province, Panama. This species is similar to Eleutherodactylus altae and Eleutherodactylus pardalis, but can be differentiated by the lack of red or white spots on groin and limbs. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Ibanez, R (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Panama City, Panama. EM ibanezr@tivoli.si.edu NR 10 TC 7 Z9 7 U1 0 U2 0 PU SOC STUDY AMPHIBIANS REPTILES PI ST LOUIS PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST LOUIS, MO 63103 USA SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD JUN PY 2004 VL 38 IS 2 BP 240 EP 243 DI 10.1670/12-03A PG 4 WC Zoology SC Zoology GA 835AU UT WOS:000222452800012 ER PT J AU Plachta, DTT Song, JK Halvorsen, MB Popper, AN AF Plachta, DTT Song, JK Halvorsen, MB Popper, AN TI Neuronal encoding of ultrasonic sound by a fish SO JOURNAL OF NEUROPHYSIOLOGY LA English DT Article ID SHAD ALOSA-SAPIDISSIMA; DOLPHIN ECHOLOCATION CLICKS; SUPERIOR OLIVARY COMPLEX; BAT; STIMULI; CLUPEID; SPRAT AB Many species of odontocete cetaceans ( toothed whales) use high-frequency clicks (60-170 kHz) to identify objects in their environment, including potential prey. Behavioral studies have shown that American shad, Alosa sapidissima, can detect ultrasonic signals similar to those of odontocetes that are potentially their predators. American shad also show strong escape behavior in response to ultrasonic pulses between 70 and 110 kHz and can determine the location of the sound source at least in the horizontal plane. The present study examines physiological aspects of ultrasound detection by American shad and provides the first insights into the neural encoding of ultrasound signals in any nonmammalian vertebrate. The recordings were obtained by penetration through the cerebellar surface. All but two units responded exclusively to ultrasound. Ultrasound-sensitive units did not phase-couple to any stimulus frequency. Some units resembled the response of constant latency neurons found in the ventral nucleus of the lateral lemniscus of bats. We suggest that ultrasonic and sonic signals are processed along different pathways in Alosa. The ultrasonic pathway in Alosa appears to be a feature detector that is likely to be adapted ( e. g., frequency, intensity) to odontocete echolocation signals. C1 Univ Maryland, Dept Biol, College Pk, MD 20742 USA. Univ Maryland, Neurosci & Cognit Sci Program, College Pk, MD 20742 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Rhein Westfal TH Aachen, D-52074 Aachen, Germany. RP Popper, AN (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM apopper@umd.edu FU NIDCD NIH HHS [DC 03936, DC 04664]; NIMH NIH HHS [T32 MH 20048] NR 32 TC 5 Z9 8 U1 1 U2 9 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 0022-3077 J9 J NEUROPHYSIOL JI J. Neurophysiol. PD JUN PY 2004 VL 91 IS 6 BP 2590 EP 2597 DI 10.1152/jn.01200.2003 PG 8 WC Neurosciences; Physiology SC Neurosciences & Neurology; Physiology GA 819NO UT WOS:000221321900023 PM 14749304 ER PT J AU [Anonymous] AF [Anonymous] TI The second Cretaceous scorpion specimen from Burmese amber (Arachnida: Scorpiones) SO JOURNAL OF SYSTEMATIC PALAEONTOLOGY LA English DT Article AB A new specimen of Palaeoburmesebuthus grimaldii Lourenco, 2002, recently described from Cretaceous (Albian) Burmite, is reported. This is more complete thanthe holotype consisting of five scattered, unequal parts: a complete metasomawith an attached partial mesosoma bearing a visible stigma, a right pedipalp chela and three leg fragments. Comparisons to extinct and extant lineages of scorpions are made, although the partially observable trichobothrial pattern ofthe pedipalp chela precludes definitive family placement. The relative position of the fragments and the severe damage they have suffered imply that it wasdismembered by a predator and provides the oldest evidence of scorpions beingpreyed upon by other animals. RP Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC-121,POB 37012, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 1 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 1477-2019 J9 J SYST PALAEONTOL JI J. Syst. Palaeontol. PD JUN PY 2004 VL 2 IS 2 BP 147 EP 152 PG 6 WC Evolutionary Biology; Paleontology SC Evolutionary Biology; Paleontology GA 914RF UT WOS:000228244600012 ER PT J AU Rueda, LM Pecor, JE Yuen, MC Lee, MW AF Rueda, LM Pecor, JE Yuen, MC Lee, MW TI New record, habitats, and updated checklist of the mosquitoes of Hong Kong SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Article DE mosquitoes; Anopheles; Aedes; Culex; Hong Kong; Culicidae AB Mosquito collections were carried out during April 2002 in Hong Kong. Twenty-six species of mosquitoes in 9 genera were collected, including I new record, Culex (Culiciomyia) nigropunctatus. Characteristics of larval habitats of these species are described and an updated checklist is included. C1 Walter Reed Army Inst Res, Dept Entomol, Silver Spring, MD 20910 USA. Hong Kong Govt, Dept Food & Hyg, Kowloon, Hong Kong, Peoples R China. RP Rueda, LM (reprint author), Smithsonian Inst, Museum Support Ctr, Walter Reed Biosyst Unit, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 20 TC 2 Z9 2 U1 0 U2 0 PU AMER MOSQUITO CONTROL ASSOC PI EATONTOWN PA P O BOX 234, EATONTOWN, NJ 07724-0234 USA SN 8756-971X J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD JUN PY 2004 VL 20 IS 2 BP 204 EP 207 PG 4 WC Entomology SC Entomology GA 830KF UT WOS:000222120200022 PM 15264634 ER PT J AU LaPolla, JS AF LaPolla, JS TI Taxonomic review of the ant genus Pseudolasius (Formicidae : Formicinae) in the Afrotropical region SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Afrotropical region; Formicidae; Formicinae; Pseudolasius ID HYMENOPTERA AB The ant genus Pseudolasius in the Afrotropical region is reviewed. Two species are considered valid, P. bufonus and P. weissi, and diagnostic morphological characters are provided for each. Scanning electron micrographs are provided for each species, and the male genitalia of P. bufonus are illustrated for the first time. Four species are synomized with P. weissi: P. bayonii new synonym, P. bucculentus new synonym, P. gowdeyi new synonym, and P. weissi sordidus new synonym. C1 Rutgers State Univ, Dept Entomol, New Brunswick, NJ 08901 USA. RP LaPolla, JS (reprint author), Smithsonian Inst, Dept Entomol, MRC 188,POB 37012, Washington, DC 20013 USA. EM lapolla@si.edu NR 14 TC 5 Z9 6 U1 1 U2 3 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SUM-FAL PY 2004 VL 112 IS 2-3 BP 97 EP 105 DI 10.1664/0028-7199(2004)112[0097:TROTAG]2.0.CO;2 PG 9 WC Entomology SC Entomology GA 903FH UT WOS:000227410500001 ER PT J AU Henry, TJ de Paula, AS AF Henry, TJ de Paula, AS TI Rhyparochromomiris femoratus, a remarkable new genus and species of Cylapinae (Hemiptera : Heteroptera : Miridae) from ecuador SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Hemiptera; Heteroptera; Miridae; Cylapinae; new genus; new species; Ryparochromomiris femoratus; new world AB A remarkable new cylapine genus and species. Rhyparochromomiris femoratus is described new from specimens taken in canopy-fogging samples in Orellana Province, Ecuador. This myrmecomorphic taxon is unique in the Miridae in having greatly enlarged forefemora. five-segmented antennae in both sexes. and unusual male genitalia. A description, dorsal and lateral photographs of the adult mate and female. antenna, foreleg. and claw. and illustrations of the male genitalia are provided to help distinguish this new mirid from other Cylapinae. C1 Smithsonian Inst, Natl Museum Amer Hist, USDA ARS, Systemat Entomol Lab, Washington, DC 20013 USA. Unif Fed Ouro Preto, Dept Ciencias Biol, ICEB, BR-35400000 Ouro Preto, MG, Brazil. RP Henry, TJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, USDA ARS, Systemat Entomol Lab, POB 37012,MRC-0168, Washington, DC 20013 USA. EM thenry@sel.barc.usda.gov; hetalex@terra.com.br NR 7 TC 2 Z9 2 U1 0 U2 0 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SUM-FAL PY 2004 VL 112 IS 2-3 BP 176 EP 182 DI 10.1664/0028-7199(2004)112[0176:RFARNG]2.0.CO;2 PG 7 WC Entomology SC Entomology GA 903FH UT WOS:000227410500008 ER PT J AU Bush, M Raath, JP Grobler, D Klein, L AF Bush, M Raath, JP Grobler, D Klein, L TI Severe hypoxaemia in field-anaesthetised white rhinoceros (Ceratotherium simum) and effects of using tracheal insufflation of oxygen SO JOURNAL OF THE SOUTH AFRICAN VETERINARY ASSOCIATION-TYDSKRIF VAN DIE SUID-AFRIKAANSE VETERINERE VERENIGING LA English DT Article DE anaesthesia; arterial blood gases; azaperone; Ceratotherium simum; etorphine; hypercapnia; hypoxia; insufflation; intubation; oxygen; rhinoceros ID CHEMICAL IMMOBILIZATION; NASOTRACHEAL INTUBATION; ISOFLURANE ANESTHESIA; ETORPHINE ANESTHESIA; XYLAZINE AB White rhinoceros anaesthetised with etorphine and azaperone combination develop adverse physiological changes including hypoxia, hypercapnia, acidosis, tachycardia and hypertension. These changes are more marked in field-anaesthetised rhinoceros. This study was designed to develop a technique to improve safety for field-anaesthetised white rhinoceros by tracheal intubation and oxygen insufflation. Twenty-five free-ranging white rhinoceros were anaesthetised with an etorphine and azaperone combination for translocation or placing microchips in their horns. Once anaesthetised the rhinoceros were monitored prior to crating for transportation or during microchip placement. Physiological measurements included heart and respiratory rate, blood pressure and arterial blood gas samples. Eighteen rhinoceros were intubated using an equine nasogastric tube passed nasally into the trachea and monitored before and after tracheal insufflation with oxygen. Seven rhinoceros were not intubated or insufflated with oxygen and served as controls. All anaesthetised rhinoceros were initially hypoxaemic (percentage arterial haemoglobin oxygen saturation (%O2Sa) = 49 % 16 (mean +/- SD) and PaO2 = 4.666 +/- 1.200 kPa (35 +/- 9 mm Hg)), hypercapnic (PaCO2 = 8.265 +/- 1.600 kPa (62 +/- 12 mm Hg)) and acidaemic (pH(a) = 7.171 +/- 0.073). Base excess was -6.7 +/- 3.9 mmol/l, indicating a mild to moderate metabolic acidosis. The rhinoceros were also hypertensive (systolic blood pressure = 21.861 +/- 5.465 kPa (164 +/- 41 mm Hg)) and tachycardic (HR = 107 +/- 31/min). Following nasal tracheal intubation and insufflation, the %O2Sa and PaO2 increased while blood pHa and PaCO2 remained unchanged. Tracheal intubation via the nose is not difficult, andwhen oxygen is insufflated, the PaO2 and the % O2Sa increases, markedly improving the safety of anaesthesia,but thistechnique does not correctthe hypercapnoea or acidosis. Afterregaining their feet following reversal of the anaesthesia, the animals' blood gas values return towards normality. C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Penn, New Bolton Ctr, Sch Vet Med, Dept Clin Studies, Kennett Sq, PA 19348 USA. RP Bush, M (reprint author), Smithsonian Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM mbush@crc.si.edu NR 17 TC 20 Z9 22 U1 2 U2 20 PU SOUTH AFRICAN VET ASSN PI MONUMENT PARK PA PO BOX 25033, MONUMENT PARK 0105, SOUTH AFRICA SN 0038-2809 J9 J S AFR VET ASSOC JI J. S. Afr. Vet. Assoc.-Tydskr. Suid-Afr. Vet. Ver. PD JUN PY 2004 VL 75 IS 2 BP 79 EP 84 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA 853QE UT WOS:000223841300002 PM 15456163 ER PT J AU Hutchinson, A AF Hutchinson, A TI The geese of beaver bog. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Hutchinson, A (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2004 VL 129 IS 10 BP 175 EP 175 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 826GL UT WOS:000221817200244 ER PT J AU Moser, J AF Moser, J TI American drawings and a few surprises at the Smithsonian American Art Museum SO MASTER DRAWINGS LA English DT Article C1 Smithsonian Inst, Amer Art Museum, Washington, DC 20560 USA. RP Moser, J (reprint author), Smithsonian Inst, Amer Art Museum, Washington, DC 20560 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU MASTER DRAWINGS ASSN INC PI NEW YORK PA 29 E 36TH ST, NEW YORK, NY 10016 USA SN 0025-5025 J9 MASTER DRAWINGS JI Master Draw. PD SUM PY 2004 VL 42 IS 2 BP 125 EP 132 PG 8 WC Art SC Art GA 835OH UT WOS:000222492600002 ER PT J AU Fontan, F Holtstam, D De Parseval, P Permingeat, F Mason, B AF Fontan, F Holtstam, D De Parseval, P Permingeat, F Mason, B TI Elfstorpite synonymy with allactite; mineral and name discredited SO MINERALOGICAL MAGAZINE LA English DT Article DE Mn arsenate; allactite; 'elfstorpite'; Sjogruvan; Sweden AB Holotype material and other specimens of 'elfstorpite' from the Sjogruvan deposit, Orebro, Sweden have been characterized by powder X-ray diffraction and chemical analysis. The mineral is indistinguishable from allactite, which has priority, and consequently 'elfstorpite' should be discredited. The IMA Commission on New Minerals and Mineral Names has approved the proposition. C1 Univ P Sabatier, Equipe Mineral, LMTG, UMR 5563, F-31000 Toulouse, France. Swedish Museum Nat Hist, SE-10405 Stockholm, Sweden. Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Fontan, F (reprint author), Univ P Sabatier, Equipe Mineral, LMTG, UMR 5563, 39 Allees Jules Guesde, F-31000 Toulouse, France. EM fontan@lmtg.obs-mip.fr NR 10 TC 1 Z9 1 U1 0 U2 0 PU MINERALOGICAL SOCIETY PI LONDON PA 41 QUEENS GATE, LONDON SW7 5HR, ENGLAND SN 0026-461X J9 MINERAL MAG JI Mineral. Mag. PD JUN PY 2004 VL 68 IS 3 BP 523 EP 526 DI 10.1180/0026461046830203 PG 4 WC Mineralogy SC Mineralogy GA 851HG UT WOS:000223675600009 ER PT J AU Molbo, D Machado, CA Herre, EA Keller, L AF Molbo, D Machado, CA Herre, EA Keller, L TI Inbreeding and population structure in two pairs of cryptic fig wasp species SO MOLECULAR ECOLOGY LA English DT Article DE Agaonidae; breeding structure; diploid male; F-ST; hybridization; Local mate competition; Pegoscapus ID LOCAL MATE COMPETITION; OFFSPRING SEX-RATIOS; GENETIC-STRUCTURE; NASONIA-VITRIPENNIS; PARASITIC WASP; ALLOCATION; HYMENOPTERA; EVOLUTION; SELECTION; CHALCIDOIDEA AB We used recently developed microsatellites to directly estimate inbreeding levels in two pairs of coexisting cryptic fig wasp species ('Pegoscapus hoffmeyeri sp. A and sp. B', 'P. gemellus sp. A and sp. B'). Previous tests of Hamilton's local mate competition (LMC) theory in fig wasps have used the number of dead foundresses in a fig fruit to indirectly estimate the relative contribution of each to the common brood and thereby the level of local mate competition. Further, the population level of inbreeding has been indirectly estimated using the distribution of foundress numbers across broods. Our direct genetic estimates confirmed previous assumptions that the species characterized by lower foundress numbers showed higher relative levels of inbreeding. However, there were quantitative differences between the observed level of inbreeding and the expectation based on the distribution of foundress numbers in both pollinator species associated with Ficus obtusifolia. Here, genotype compositions of broods revealed that only 23% of fruits with multiple foundresses actually contained brood from more than one foundress, thus explaining at least part of the underestimate of actual sibmating. Within the four wasp species there was no evidence for genetic differentiation among the wasp populations sampled from different trees across 20 km and from different points in time. Further, no genotypic disequilibrium was detected within any of the species. Although F1 hybrids were observed between the two species pollinating F. obtusifolia, there was no evidence of genetic introgression. Finally, we found that 11% of the sons of allospecifically mated mothers were diploid hybrids suggesting a break down of the sex determination system in hybrids. C1 Smithsonian Trop Res Inst, Naos, Balboa, Panama. Univ Lausanne, Inst Ecol, CH-1015 Lausanne, Switzerland. Univ Edinburgh, Inst Cell Anim & Populat Biol, Edinburgh EH9 3JT, Midlothian, Scotland. Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. RP Molbo, D (reprint author), Smithsonian Trop Res Inst, Naos, Apartado 2072, Balboa, Panama. EM drudemolbo@hotmail.com RI Machado, Carlos/B-8855-2009; OI Machado, Carlos/0000-0003-1546-7415; keller, laurent/0000-0002-5046-9953; Molbo, Drude/0000-0003-3372-8711 NR 47 TC 39 Z9 42 U1 0 U2 24 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JUN PY 2004 VL 13 IS 6 BP 1613 EP 1623 DI 10.1111/j.1365-294X.2004.02158.x PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 819GJ UT WOS:000221302600024 PM 15140104 ER PT J AU Erickson, DL Hamrick, JL Kochert, GD AF Erickson, DL Hamrick, JL Kochert, GD TI Ecological determinants of genetic diversity in an expanding population of the shrub Myrica cerifera SO MOLECULAR ECOLOGY LA English DT Article DE colonization; gene flow; genetic diversity; maternity; paternity ID PLANT-POPULATIONS; SEED DISPERSAL; MICROSATELLITE ANALYSIS; CHAMAELIRIUM-LUTEUM; PATERNITY ANALYSIS; LOCAL-POPULATIONS; POLLEN FLOW; DIFFERENTIATION; PINE; TREE AB The ecological mechanisms that contribute to the acquisition of genetic diversity in an expanding population of the shrub, Myrica cerifera, on an island habitat were investigated. Genealogical reconstruction was used to assess the contribution of early reproductive colonists to subsequent recruitment. In addition, through determination of parentage, the source of recruiting seedlings was identified and the contribution of seed and pollen dispersal into the colonizing sites was inferred. The relative contribution of different sources of gene flow was determined directly and an investigation was made into how variability in breeding patterns may have contributed to observed levels of genetic variability. It was expected that early colonists that could flower would contribute to subsequent recruiting cohorts, and that the limited number of such early reproductive colonists would lead to variance in mating success, inbreeding, or bottlenecks which could reduce genetic diversity and increase genetic differentiation among subsequent recruiting cohorts. Analyses of parentage (with paternity exclusion probability > 95%) for all recruiting plants demonstrated that in fact, there was little contribution by the early reproductive colonists to subsequent cohorts, and that immigration from outside the study sites in the form of seed dispersal accounted for over 94% of the recruitment in the study plots, with pollen dispersal accounting for less than 3% gene flow. No genetic bottleneck or evidence of reproductive skew in the recruiting cohorts were found, suggesting that propagule dispersal was from many source individuals in other established populations. C1 Smithsonian Inst, Lab Analyt Biol, College Pk, MD 20742 USA. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Univ Georgia, Dept Genet, Athens, GA 30602 USA. RP Erickson, DL (reprint author), Smithsonian Inst, Lab Analyt Biol, 4210 Silver Hill Rd, College Pk, MD 20742 USA. EM derickso@onyx.si.edu NR 38 TC 23 Z9 23 U1 0 U2 3 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JUN PY 2004 VL 13 IS 6 BP 1655 EP 1664 DI 10.1111/j.1365-294X.2004.02139.x PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 819GJ UT WOS:000221302600028 PM 15140108 ER PT J AU Di Fiore, A Fleischer, RC AF Di Fiore, A Fleischer, RC TI Microsatellite markers for woolly monkeys (Lagothrix lagotricha) and their amplification in other New World primates (Primates : Platyrrhini) SO MOLECULAR ECOLOGY NOTES LA English DT Article DE cross-taxon amplification; Lagothrix; microsatellites; PCR; platyrrhines; woolly monkeys AB Seven polymorphic microsatellite loci were identified for woolly monkeys (Lagothrix lagotricha) from an 'enriched' genomic library. For a wild population of 66 animals, these markers averaged over 10 alleles per locus and provided a combined probability for excluding a random individual from parentage of over 98%. These loci were screened in up to 13 other genera of New World monkeys, and many were variable in multiple taxa. Few other platyrrhine-specific microsatellite markers have been identified; thus, these loci should prove valuable for studying the population genetic structure and mating system not just of Lagothrix but also of other neotropical primates. C1 NYU, Dept Anthropol, New York, NY 10003 USA. Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. RP Di Fiore, A (reprint author), NYU, Dept Anthropol, 25 Waverly Pl, New York, NY 10003 USA. EM anthony.difiore@nyu.edu NR 9 TC 13 Z9 14 U1 0 U2 12 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD JUN PY 2004 VL 4 IS 2 BP 246 EP 249 DI 10.1111/j.1471-8286.2004.00631.x PG 4 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 823TN UT WOS:000221636200033 ER PT J AU Banford, HM Bermingham, E Collette, BB AF Banford, HM Bermingham, E Collette, BB TI Molecular phylogenetics and biogeography of transisthmian and amphi-Atlantic needlefishes (Belonidae : Strongylura and Tylosurus): perspectives on New World marine speciation SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE historical biogeography; phylogenetic systematics; mitochondrial DNA; creatine kinase; speciation ID MITOCHONDRIAL-DNA EVOLUTION; OCEAN CURRENTS; TREE TOPOLOGIES; CENTRAL-AMERICA; SOUTH-AMERICA; SHORE FISHES; PANAMA; ISTHMUS; PHYLOGEOGRAPHY; AMPLIFICATION AB Phylogenetic relationships among New World and eastern Atlantic species in the belonid genera Strongylura and Tylosurus were hypothesized using 3689 bp of nucleotide sequence; including the entire mitochondrial (mtDNA) ATP synthase 6 and 8 genes; partial cytochrome b; 12S and 16S ribosomal genes; and introns and exons, 2 and 3 of the nuclear-encoded creatine kinase B gene. Concordant mtDNA and nuclear genealogies permitted well-supported inference of species relationships within Strongylura and Tylosurus, and of the chronology of diversification in the two genera. Our phylogenetic hypothesis permitted an assessment of Rosen's [Syst. Zool. 24 (1975) 431] model of species diversification across the eastern Atlantic to eastern Pacific marine biogeographic track. The spatial predictions of the Rosen model were generally supported, but not the temporal predictions. Furthermore, long branches leading to terminal Belonidae indicated that many species have persisted for millions of years or that nucleotide substitution rates were elevated for some clades. Though heterogeneity of nucleotide substitution rate was indicated across some belonid lineages, molecular clock estimates were used to hypothesize biogeographic scenarios for Strongylura across the eastern Pacific and Atlantic region. Furthermore, use of a molecular clock indicated; that early diversification among contemporary Strongylura may have been initiated by changes in Atlantic Ocean circulation precipitated by closure of the Tethys Sea; and provided approximate dates for the isolation of the freshwater species on the American continents. (C) 2003 Elsevier Inc. All rights reserved. C1 State Univ W Georgia, Dept Biol, Carrollton, GA 30118 USA. Smithsonian Trop Res Inst, Balboa, Panama. Natl Museum Nat Hist, Natl Systemat Lab, Natl Marine Fisheries Serv, Washington, DC 20560 USA. RP Banford, HM (reprint author), State Univ W Georgia, Dept Biol, Carrollton, GA 30118 USA. EM hbanford@westga.edu NR 90 TC 31 Z9 34 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD JUN PY 2004 VL 31 IS 3 BP 833 EP 851 DI 10.1016/j.ympev.2003.10.013 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 821EO UT WOS:000221443400003 PM 15120382 ER PT J AU Tormen, G Moscardini, L Yoshida, N AF Tormen, G Moscardini, L Yoshida, N TI Properties of cluster satellites in hydrodynamical simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : clusters : general; galaxies : interactions; cosmology : theory; dark matter; X-rays : galaxies ID DARK-MATTER HALOES; X-RAY-PROPERTIES; GALAXY CLUSTERS; INTERGALACTIC MEDIUM; MERGING CLUSTERS; EVOLUTION; A3667; CORE; GAS AB We analyse the dynamical and thermal evolution of dark matter and the intracluster medium in hydrodynamical N-body simulations of galaxy clusters. Starting from a sample of 17 high-resolution objects, with virial mass ranging from 3 x 10(14) to 1.7 x 10(15) h(-1) M., we follow the build-up of the systems in dark matter and hot gas through the repeated merging of satellites along their merging history trees. We measure the self-bound mass fraction of subhaloes as a function of time after the merging, estimate the satellite mean orbital properties as a function of the mass ratio with the main cluster at merging time, and study the evolution of their internal velocity dispersion, gas temperature and entropy as the substructure is disrupted by various dynamical processes, eventually reaching thermodynamic equilibrium in the gravitational potential of the main cluster. We model some relevant properties of subhalo orbits, as the time of the first pericentric and apocentric passages, and the typical distances and velocities at the corresponding times. This survival study can be used to interpret the dynamics of observed merging clusters; as an example, we apply our results to the system 1E0657-56. We show that, in the light of our results, the most likely interpretation of the data for this cluster points to the merger of a small group with mass M approximate to 1 x 10(13) h(-1) M. with a massive cluster with M approximate to 1.3 x 10(15) h(-1) M. C1 Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tormen, G (reprint author), Univ Padua, Dipartimento Astron, Vicolo Osservatorio 2, I-35122 Padua, Italy. EM tormen@pd.astro.it; moscardini@bo.astro.it; naoki@th.nao.ac.jp RI Yoshida, Naoki/A-4305-2011 NR 31 TC 69 Z9 69 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2004 VL 350 IS 4 BP 1397 EP 1408 DI 10.1111/j.1365-2966.2004.07736.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 828EY UT WOS:000221957800020 ER PT J AU Ebeling, JR Rowan, YM AF Ebeling, JR Rowan, YM TI The archaeology of the daily grind SO NEAR EASTERN ARCHAEOLOGY LA English DT Article ID STONE TOOLS; ABU-HUREYRA; RESIDUES; GRAINS; BONES AB Though they are often regarded as unglamorous, awkward, static through millennia of use, and functionally self-evident, ground stone tools nevertheless constitute a substantial part of archaeological finds recovered from most sites in the ancient Near East. They can offer insights into such diverse phenomena as changes in diet and food processing techniques, mobility and residence patterns, division of labor, and specialized activities related to cultic practices to mention but a few things. Unfortunately, the exclusion of these artifacts in past archaeological publications means that an essential part of the archaeological record remains unused and, when these tools are discarded, actually destroyed by the very archaeologists who purport to save the past. C1 Univ Evansville, Dept Archaeol & Art Hist, Evansville, IN USA. Univ Notre Dame, Notre Dame, IN 46556 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC USA. RP Ebeling, JR (reprint author), Univ Evansville, Dept Archaeol & Art Hist, Evansville, IN USA. NR 48 TC 8 Z9 8 U1 2 U2 8 PU ACADEMIC SERVICES PI CANTON PA PO BOX 531, CANTON, MA 02021-0531 USA SN 1094-2076 J9 NEAR EAST ARCHAEOL JI Near East. Archaeol. PD JUN PY 2004 VL 67 IS 2 BP 108 EP 117 DI 10.2307/4132366 PG 10 WC Archaeology SC Archaeology GA 976SB UT WOS:000232752400007 ER PT J AU D'Elia, V Fiore, F Elvis, M Cappi, M Mathur, S Mazzotta, P Falco, E AF D'Elia, V Fiore, F Elvis, M Cappi, M Mathur, S Mazzotta, P Falco, E TI X-ray sources overdensity around the 3C 295 galaxy cluster SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID DEEP FIELD-SOUTH; CHANDRA AB We present a statistical analysis of the Chandra observation of the source field around the 3C 295 galaxy cluster (z = 0.46). The logN-logS of this field is in good agreement with that computed for the Chandra Deep Field South in this work and in previous ones. Nevertheless, the logN-logS computed separately for the four ACTS-I chips reveals that there is a significant excess of sources to the North-North East and a void to the South of the central cluster. Such an asymmetric distribution is confirmed by the two-dimensional Kolmogorov-Smirnov test, which excludes (P similar to 3%) a uniform distribution. In addition, a strong spatial correlation emerges from the study of the angular correlation function of the field: the angular correlation function is above that expected for X-ray sources on a few arcmin scales. In synthesis, the present analysis may indicate a filament of the large scale structure of the Universe toward 3C 295. This kind of study may open-up a new way to map (with high efficiency) high-density peaks of large scale structures at high redshift. C1 Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, IASF, I-40126 Bologna, Italy. Ohio State Univ, Columbus, OH 43210 USA. Univ Durham, Durham DH1 3LE, England. Smithsonian Inst, Whipple Observ, AZ 85645 USA. RP D'Elia, V (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. EM fiore@mporzio.astro.it RI Cappi, Massimo/F-4813-2015; Mazzotta, Pasquale/B-1225-2016; OI Fiore, Fabrizio/0000-0002-4031-4157; Mazzotta, Pasquale/0000-0002-5411-1748; D'Elia, Valerio/0000-0002-7320-5862; Cappi, Massimo/0000-0001-6966-8920 NR 8 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 54 EP 57 DI 10.1016/j.nuclphysbps.2004.04.007 PG 4 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300008 ER PT J AU Hardcastle, MJ Worrall, DM Kraft, RP Forman, WR Jones, C Murray, SS AF Hardcastle, MJ Worrall, DM Kraft, RP Forman, WR Jones, C Murray, SS TI Particle acceleration and jet dynamics in Centaurus A SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID X-RAY JET; RADIO GALAXY 3C-31; CHANDRA OBSERVATIONS; MODELS; M87 AB New multi-epoch Chandra observations, combined with multi-epoch, high-dynamic range VLA data, have allowed us to relate the radio and X-ray structure of the jet in Cen A to the jet dynamics. We present evidence that a significant fraction of the structure in the Cen A X-ray jet is due to particle acceleration at the interaction between the jet flow and internal galactic material. C1 Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hardcastle, MJ (reprint author), Univ Bristol, Dept Phys, Tyndall Ave, Bristol BS8 1TL, Avon, England. EM m.hardcastle@bristol.ac.uk RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 20 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 116 EP 121 DI 10.1016/j.nuclphysbps.2004.04.014 PG 6 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300016 ER PT J AU Braito, V Della Ceca, R Piconcelli, E Severgnini, P Bassani, L Cappi, M Franceschini, A Iwasawa, K Malaguti, G Marziani, P Palumbo, GGC Persic, M Risaliti, G Salvati, M AF Braito, V Della Ceca, R Piconcelli, E Severgnini, P Bassani, L Cappi, M Franceschini, A Iwasawa, K Malaguti, G Marziani, P Palumbo, GGC Persic, M Risaliti, G Salvati, M TI The ultra luminous infrared galaxy Mrk 231: new clues from BeppoSAX and XMM-Newton SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID MARKARIAN 231; SPECTROSCOPY AB We present BeppoSAX and XMM-Newton observations of Mrk 231. These observations and in particular the BeppoSAX PDS data allowed us to unveil, for the first time, the highly absorbed (N-H similar to2 X 10(24) cm(-2)) AGN component. We find that: a) the AGN powering Mrk 231 has an intrinsic 2-10 keV luminosity of 1(-0.5)(+1) X 10(44) erg s(-1); b) the strong starburst activity contributes significantly in the 0.1-10 keV energy range. We propose that the starburst activity strongly contributes to the far infrared luminosity of Mrk 231; this is also suggested by the multiwavelength properties of Mrk 231. C1 Osserv Astron Brera, INAF, I-20154 Milan, Italy. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. CNR, IASF, Sez Bologna, I-40129 Bologna, Italy. ESA, VILSPA, XMN, SOC, Madrid 28080, Spain. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Osserv Astron Padova, INAF, I-35122 Padua, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Braito, V (reprint author), Osserv Astron Brera, INAF, Via Brera 28, I-20154 Milan, Italy. EM braito@brera.mi.astro.it; grisaliti@cfa.harvard.edu; grisaliti@cfa.harvard.edu RI Cappi, Massimo/F-4813-2015; OI piconcelli, enrico/0000-0001-9095-2782; Cappi, Massimo/0000-0001-6966-8920; Risaliti, Guido/0000-0002-3556-977X; Marziani, Paola/0000-0002-6058-4912; Braito, Valentina/0000-0002-2629-4989 NR 15 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 153 EP 156 DI 10.1016/j.nuclphysbps.2004.04.021 PG 4 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300023 ER PT J AU Puccetti, S Risaliti, G Fiore, F Elvis, M Nicastro, F Perola, GC Capalbi, M AF Puccetti, S Risaliti, G Fiore, F Elvis, M Nicastro, F Perola, GC Capalbi, M TI Rapid N-H changes in NGC 4151 SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID COLUMN DENSITIES AB We have analyzed two long BeppoSAX observations of the bright Seyfert galaxy NGC 4151, searching for short timescale (similar to10-200 ksec) X-ray spectral variability. The light curve of a softness ratio, chosen as most sensitive to pinpoint changes of the column density of the absorbing gas along the line of sight, shows significant variations. We try to model these variations by performing a detailed, time resolved, spectral analysis. We find significant, large (factors of 1.5-6) variations of the absorber column densities on time scales of 40-200 ksec. These values are 10-100 times shorter than those found by Risaliti et al. 2002 in a sample of Seyfert 2 galaxies, and provide strong constraints on the geometry of the obscuring medium. C1 Univ Roma Tor Vergata, Rome, Italy. INAF, Osservatorio Astron Roma, Monteporzio Catone, Rome, Italy. Osserv Astrofis Arcetri, INAF, Florence, Italy. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. Univ Roma Tor Vergata, Rome, Italy. ASI Sci Data Ctr, ESA, ESRIN, Frascati, Italy. RP Puccetti, S (reprint author), Univ Roma Tor Vergata, Rome, Italy. OI Puccetti, Simonetta/0000-0002-2734-7835; Risaliti, Guido/0000-0002-3556-977X; Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 13 TC 8 Z9 8 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 225 EP 228 DI 10.1016/j.nuclphysbps.2004.04.039 PG 4 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300041 ER PT J AU Risaliti, G AF Risaliti, G TI X-ray spectral properties of Seyfert 2s observed with BeppoSAX SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID GALAXIES AB We present the results of a homogeneous analysis of BeppoSAX observations of 19 bright Compton-thin Seyfert 2s. Using the wide spectral coverage of BeppoSAX it is possible to determine the single spectral components with unprecedented precision. We find that the intrinsic emission of Seyfert 2s is well reproduced by a power law with a photon index Gamma = 1.79 +/- 0.01, and a dispersion sigma = 0.23. A reflection component is present in most spectra. We discuss these results in the view of the unified model, and we show a stacked spectrum obtained adding up the 1-200 keV spectra of all the sources of the sample. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Risaliti, Guido/0000-0002-3556-977X NR 5 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 229 EP 231 DI 10.1016/j.nuclphysbps.2004.04.040 PG 3 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300042 ER PT J AU Uttley, P Taylor, RD Mchardy, IM Page, MJ Mason, KO Lamer, G Fruscione, A AF Uttley, P Taylor, RD Mchardy, IM Page, MJ Mason, KO Lamer, G Fruscione, A TI Catching NGC 4051 in the low state with XMM-Newton SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Energy Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID RESOLUTION X-RAY; SEYFERT-GALAXIES; SWAN SONG; NGC 4051; VARIABILITY AB The Narrow Line Seyfert I (NLS 1) galaxy NGC 4051 shows unusual low flux states, lasting several months, when the 2-10 keV X-ray spectrum becomes unusually hard (photon index< 1) while the spectrum at lower X-ray energies is dominated by a large soft excess. A Chandra TOO of the low state has shown that the soft excess and hard components are variable and well-correlated. The variability of the hard component rules out an origin in a distant reflector. Here we present results from a recent XMM-Newton TOO of NGC4051 in the low state, which allows a much more detailed examination of the nature of the hard and soft spectral components in the low state. We demonstrate that the spectral shape in the low state is consistent with the extrapolation of the spectral pivoting observed at higher fluxes. The XMM-Newton data also reveals the warm absorbing gas in emission, as the drop in the primary continuum flux unmasks prominent emission lines from a range of ion species. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Uttley, P (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. NR 10 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 240 EP 243 DI 10.1016/j.nuclphysbps.2004.04.043 PG 4 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300045 ER PT J AU Kaaret, P Corbel, S Tomsick, JA Butt, Y Fender, RP Lazendic, J Miller, JM Orosz, JA Tzioumis, AK Wijnands, R AF Kaaret, P Corbel, S Tomsick, JA Butt, Y Fender, RP Lazendic, J Miller, JM Orosz, JA Tzioumis, AK Wijnands, R TI Large-scale X-ray jets from Galactic black holes SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID XTE J1550-564; CHANDRA HETGS; EMISSION; SS-433; XTE-J1550-564; SPECTRUM; STATES; SS433 AB Observations of jets from stellar-mass sources located in our Galaxy offer a unique opportunity to study the dynamical evolution of relativistic jets on time scales inaccessible for active galactic nuclei jets, with implications for our understanding of the dynamics and energetics of relativistic jets from Galactic x-ray binaries and active galactic nuclei. We review recent observations of X-ray jets from Galactic black hole candidates. Spatially resolved X-ray spectra from SS 433 have provided evidence for re-heating in a hadronic jet and may offer an observational probe of jet collimation. A large-scale jet from the now quiescent transient 4U 1755-33 appears to indicate continual jet formation over a period of 10-30 years. Detection of a jet from XTE J1550-564 has provided the first direct measurement of gradual deceleration of a jet from a black hole and strong evidence for the re-energization of jet particles to energies up to 10 TeV at sites far from the jet origin. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Paris 07, F-91191 Gif Sur Yvette, France. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Calif San Diego, Ctr Space Sci & Astrophys, La Jolla, CA 92093 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 19 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 354 EP 362 DI 10.1016/j.nuclphysbps.2004.04.063 PG 9 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300065 ER PT J AU Zampieri, L Mucciarelli, P Falomo, R Kaaret, P Di Stefano, R Turolla, R Chieregato, A Treves, A AF Zampieri, L Mucciarelli, P Falomo, R Kaaret, P Di Stefano, R Turolla, R Chieregato, A Treves, A TI Optical counterpart of the ultraluminous X-ray source NGC 1313 X-2 SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID SOURCE NGC-5204 X-1; BLACK-HOLES; NGC 1313; IDENTIFICATION; OBJECTS AB We present new optical and Chandra observations of the field containing the ultraluminous X-ray source NGC1313 X-2. On an ESO 3.6 m image, the Chandra error box embraces a R = 21.6 mag stellar-like object and excludes a previously proposed optical counterpart. The resulting X-ray/optical flux ratio of NGC 1313 X-2 is similar to 500. The value of fx/f(opt), the X-ray variability history and spectral distribution indicate a luminous X-ray binary in NGC 1313 as a likely explanation for NGC 1313 X-2. The inferred optical luminosity (L approximate to 10(5) L-circle dot) is consistent with that of a approximate to 10M(circle dot) companion. C1 Osserv Astron Padova, INAF, I-35122 Padua, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Padua, Dipartimento Fis, I-35131 Padua, Italy. Univ Insubria, Dipartimento Sci, I-22100 Como, Italy. RP Zampieri, L (reprint author), Osserv Astron Padova, INAF, Vicolo Osservatiori 5, I-35122 Padua, Italy. OI Falomo, Renato/0000-0003-4137-6541; Zampieri, Luca/0000-0002-6516-1329 NR 22 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 387 EP 391 DI 10.1016/j.nuclphysbps.2004.04.068 PG 5 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300070 ER PT J AU Rossi, S Homan, J Miller, JM Belloni, T AF Rossi, S Homan, J Miller, JM Belloni, T TI State transitions in the 2001/2002 outburst of XTE J1650-500 SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID QUASI-PERIODIC OSCILLATIONS; BLACK-HOLE CANDIDATES; RXTE OBSERVATIONS; XTE J1650-500; J1550-564 AB We present a study of the X-ray transient and black hole candidate XTE J1650-500 during its 2001/2002 outburst. The source made two state transitions between the hard and soft states, at luminosity levels that differ by a factor of similar to5-10. The first transition, between hard and soft, lasted for similar to30 days and showed two parts; one part in which the spectral properties evolve smoothly away from the hard state and another that we identify as the,steep power law state'. The two parts showed different behavior of the Fe K emission line and QPO frequencies. The second transition, from soft to hard, lasted only similar to15 days and showed no evidence of the presence of the,steep power law state'. Comparing observations from the early rise and the decay of the outburst, we conclude that the source can be in the hard state in a range of more than 10(4) in luminosity. We briefly discuss the state transitions in the framework of a two-flow model. C1 Astron Observ Brera Merate, INAF, I-23807 Merate, LC, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rossi, S (reprint author), Astron Observ Brera Merate, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy. NR 18 TC 14 Z9 14 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 416 EP 419 DI 10.1016/j.nuclphysbps.2004.04.075 PG 4 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300077 ER PT J AU Weisskopf, MC Becker, W Swartz, DA Pavlov, GG Elsner, RF Grindlay, J Mignani, R Tennant, AF Backer, D Pulone, L Testa, V AF Weisskopf, MC Becker, W Swartz, DA Pavlov, GG Elsner, RF Grindlay, J Mignani, R Tennant, AF Backer, D Pulone, L Testa, V TI Chandra X-Ray observatory observations of the globular cluster M28 and its millisecond pulsar PSR B1821-24 SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID NEUTRON-STAR; ATMOSPHERES; EMISSION AB We discuss the results of the first Chandra X-Ray Observatory observations of the globular cluster M28 (NGC 6626). We detect 46 X-ray sources of which 12 lie within one core radius of the center. We measure the radial distribution of the X-ray sources and fit it to a King profile finding a core radius of r(c,x) approximate to 11". We measure for the first time the unconfused phase-averaged X-ray spectrum of the 3.05-ms pulsar B1821-24 and find it is best described by a power law with photon index Gamma similar or equal to 1.2. We find marginal evidence of an emission line centered at 3.3 keV in the pulsar spectrum, which could be interpreted as cyclotron emission from a Corona above the pulsar's polar cap if the magnetic field is strongly different from a centered dipole. We present a spectral analyses of the brightest unidentified source and suggest that it is a transiently accreting neutron star in a low-mass X-ray binary, in quiescence. In addition to the resolved sources, we detect fainter, unresolved X-ray emission from the central core. C1 George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. USRA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. Penn State Univ, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85740 Garching, Germany. Univ Calif Berkeley, Berkeley, CA 94720 USA. Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. RP Weisskopf, MC (reprint author), George C Marshall Space Flight Ctr, Dept Space Sci, SD 50, Huntsville, AL 35812 USA. OI Pulone, Luigi/0000-0002-5285-998X; Testa, Vincenzo/0000-0003-1033-1340 NR 14 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 566 EP 571 DI 10.1016/j.nuclphysbps.2004.04.095 PG 6 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300097 ER PT J AU Clarkson, WI Charles, PA Coe, MJ Laycock, S AF Clarkson, WI Charles, PA Coe, MJ Laycock, S TI Long-term periodicities in X-ray binaries SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 2nd BeppoSAX Conference on Restless High-Engery Universe CY MAY 05-08, 2003 CL Amsterdam, NETHERLANDS SP Royal Netherlands Acad Arts & Sci, Acad Dei Lincei Rome ID WARPED ACCRETION DISCS; HERCULIS AB A significant number of X-ray binaries are now known to exhibit long-term periodicities on timescales of similar to10 - 100 days. Several physical mechanisms have been proposed that give rise to such periodicities, one of which is radiation-driven warping and precession of the accretion disk. Recent theoretical work predicts the stability to disk warping as a function of the mass ratio, binary radius, viscosity and accretion efficiency, and we confront this theory with observed longterm behaviour of a sample of neutron star X-ray Binaries. We find good agreement, establishing this mechanism observationally for the high-luminosity systems studied here. C1 Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Clarkson, WI (reprint author), Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. NR 9 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUN PY 2004 VL 132 BP 588 EP 591 DI 10.1016/j.nuclphysbps.2004.04.099 PG 4 WC Physics, Particles & Fields SC Physics GA 845FX UT WOS:000223224300102 ER PT J AU Philpott, SM Greenberg, R Bichier, P Perfecto, I AF Philpott, SM Greenberg, R Bichier, P Perfecto, I TI Impacts of major predators on tropical agroforest arthropods: comparisons within and across taxa SO OECOLOGIA LA English DT Article DE food webs; birds; dominant arboreal ants; multi-trophic interactions; coffee agroecosystems ID EXTRAFLORAL NECTARY PLANT; PAPUA-NEW-GUINEA; FOOD-WEB; COFFEE PLANTATIONS; HERBIVORE DETERRENCE; MULTIPLE PREDATORS; TROPHIC CASCADES; ANTS HYMENOPTERA; FOREST-CANOPY; LEAF DAMAGE AB In food web studies, taxonomically unrelated predators are often grouped into trophic levels regardless of their relative importance on prey assemblages, multiple predator effects, or interactions such as omnivory. Ants and birds are important predators likely to differentially shape arthropod assemblages, but no studies have compared their effects on a shared prey base. In two separate studies, we excluded birds and ants from branches of a canopy tree (Inga micheliana) in a coffee farm in Mexico for 2 months in the dry and wet seasons of 2002. We investigated changes in arthropod densities with and without predation pressure from (1) birds and (2) ant assemblages dominated by one of two ant species (Azteca instabilis and Camponotus senex). We first analyzed individual effects of each predator (birds, Azteca instabilis, and C. senex) then used a per day effect metric to compare differences in effects across (birds vs ants) and within predator taxa (the two ant species). Individually, birds reduced densities of total and large arthropods and some arthropod orders (e.g., spiders, beetles, roaches) in both seasons. Azteca instabilis did not significantly affect arthropods (total, small, large or specific orders). Camponotus senex, however, tended to remove arthropods (total, small), especially in the dry season, and affected arthropod densities of some orders both positively and negatively. Predators greatly differed in their effects on Inga arthropods (for all, small, large, and individual orders of arthropods) both in sign (+/-) and magnitudes of effects. Birds had stronger negative effects on arthropods than ants and the two dominant ant species had stronger effects on arthropods in different seasons. Our results show that aggregating taxonomically related and unrelated predators into trophic levels without prior experimental data quantifying the sign and strengths of effects may lead to a misrepresentation of food web interactions. C1 Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. Natl Zoo, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. RP Philpott, SM (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 830 N Univ, Ann Arbor, MI 48109 USA. EM sphilpot@umich.edu RI Philpott, Stacy/F-2330-2011 NR 81 TC 59 Z9 61 U1 6 U2 32 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUN PY 2004 VL 140 IS 1 BP 140 EP 149 DI 10.1007/s00442-004-1561-z PG 10 WC Ecology SC Environmental Sciences & Ecology GA 826SZ UT WOS:000221850300016 PM 15095089 ER PT J AU Goddard, I Love, T AF Goddard, I Love, T TI Oregon, the beautiful SO OREGON HISTORICAL QUARTERLY LA English DT Article C1 Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. Linfield Coll, McMinnville, OR USA. RP Goddard, I (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 49 TC 2 Z9 2 U1 0 U2 0 PU OREGON HISTORICAL SOC PI PORTLAND PA 1230 SW PARK AVE, PORTLAND, OR 97205 USA SN 0030-4727 J9 OREG HIST QUART JI Oregon Hist. Q. PD SUM PY 2004 VL 105 IS 2 BP 238 EP 259 PG 22 WC History SC History GA 954BK UT WOS:000231128900003 ER PT J AU Budd, AE Pandolfi, JM AF Budd, AE Pandolfi, JM TI Overlapping species boundaries and hybridization within the Montastraea "annularis" reef coral complex in the Pleistocene of the Bahama Islands SO PALEOBIOLOGY LA English DT Article ID REPRODUCTIVE ISOLATION; EVOLUTIONARY HISTORY; SPAWNING CORALS; BUILDING CORAL; SCLERACTINIA; CNIDARIA; COMMUNITIES; EXTINCTION; DIVERSITY; TURNOVER AB Recent molecular analyses indicate that many reef coral species belong to hybridizing species complexes or "syngameons." Such complexes consist of numerous genetically distinct-species or lineages, which periodically split and/or fuse as they extend through time. During splitting and fusion, morphologic intermediates form and species overlap. Here we focus on processes associated with lineage fusion, specifically introgressive hybridization, and the recognition of such hybridization in the fossil record. Our approach involves comparing patterns of ecologic and morphologic overlap in genetically characterized modern species with fossil representatives of the same or closely related species. We similarly consider the long-term consequences of past hybridization on the structure of modern-day species boundaries. Our study involves the species complex Montastraea annularis s.l. and is based in the Bahamas, where, unlike other Caribbean locations, two of the three members of the complex today are not genetically distinct. We measured and collected colonies along linear transects across Pleistocene reef terraces of last interglacial age (approximately 125 Ka) on the islands of San Salvador, Andros, and Great Inagua. We performed quantitative ecologic and morphologic analyses of the fossil data, and compared patterns of overlap among species with data from modern localities where species are and are not genetically distinct. Ecologic and morphologic analyses reveal "moderate" overlap (>10%, but statistically significant differences) and sometimes "high" overlap (no statistically significant differences) among Pleistocene growth forms (= "species"). Ecologic analyses show that three species (massive, column, organ-pipe) co-occurred. Although organ-pipes had higher abundances in patch reef environments, columnar and massive species exhibited broad, completely overlapping distributions and had abundances that were not related to reef environment. For morphometric analyses, we used multivariate discriminant analysis on landmark data and linear measurements. The results show that columnar species overlap "moderately" with organ-pipe and massive species. Comparisons with genetically characterized colonies from Panama show that the Pleistocene Bahamas species have intermediate morphologies, and that the observed "moderate" overlap differs from the morphologic separation among the three modern species. In contrast, massive and columnar species from the Pleistocene of the Dominican Republic comprise distinct morphologic clusters, similar to the modern species; organ-pipe species exhibit "low" overlap (<10%, only at species margins) with columnar and massive species. Assuming that "moderate" overlap implies hybridization and "high" overlap implies more complete lineage fusion, these results support the hypothesis of hybridization among species within the complex in the Bahamas during the Pleistocene. Hybridization involved introgression of three distinct evolutionary lineages, in association with Pleistocene sea level and temperature fluctuations, and appears to have been limited geographically primarily to the Bahamas and the northern Caribbean. Thus, not only does the structure of species boundaries within the complex vary geographically, but these geographic differences may have persisted since the Pleistocene. C1 Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. RP Budd, AE (reprint author), Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. EM ann-budd@uiowa.edu; Pandolfi.john@NMNH.SI.EDU RI Pandolfi, John/A-3121-2009 OI Pandolfi, John/0000-0003-3047-6694 NR 54 TC 23 Z9 26 U1 0 U2 7 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SUM PY 2004 VL 30 IS 3 BP 396 EP 425 DI 10.1666/0094-8373(2004)030<0396:OSBAHW>2.0.CO;2 PG 30 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 844XC UT WOS:000223193400004 ER PT J AU Mikhailov, EE Sautenkov, VA Novikova, I Welch, GR AF Mikhailov, EE Sautenkov, VA Novikova, I Welch, GR TI Large negative and positive delay of optical pulses in coherently prepared dense Rb vapor with buffer gas SO PHYSICAL REVIEW A LA English DT Article ID LIGHT-PROPAGATION; GROUP-VELOCITY; SLOW LIGHT; ATOMIC GAS; MAGNETOMETRY; ULTRASLOW; REDUCTION; MEDIA AB We experimentally study the group time delay for a light pulse propagating through hot Rb-87 vapor in the presence of a strong coupling field in a Lambda configuration. We demonstrate that the ultraslow pulse propagation is transformed into superluminal propagation as the one-photon detuning of the light increases due to the change in the transmission resonance line shape. Negative group velocity as low as -c/10(6)=-80 m/s is recorded. We also find that the advance time in the regime of the superluminal propagation grows linearly with increasing laser field power. C1 Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. Texas A&M Univ, Inst Quantum Studies, College Stn, TX 77843 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. PN Lebedev Phys Inst, Moscow 119991, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mikhailov, EE (reprint author), Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. EM evmik@leona.physics.tamu.edu RI Novikova, Irina/B-9041-2008; Sautenkov, Vladimir/N-7024-2013 OI Sautenkov, Vladimir/0000-0001-8400-9405 NR 38 TC 46 Z9 46 U1 0 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 2004 VL 69 IS 6 AR 063808 DI 10.1103/PhysRevA.69.063808 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 835GT UT WOS:000222471400110 ER PT J AU Novikova, I Zibrov, AS Phillips, DF Andre, A Walsworth, RL AF Novikova, I Zibrov, AS Phillips, DF Andre, A Walsworth, RL TI Dynamic optical bistability in resonantly enhanced Raman generation SO PHYSICAL REVIEW A LA English DT Article ID NONLINEAR OPTICS; ATOMIC COHERENCE; VAPOR; LIGHT; STORAGE; PHOTONS; MEDIA AB We report observations of novel dynamic behavior in resonantly enhanced stimulated Raman scattering in Rb vapor. In particular, we demonstrate a dynamic hysteresis of the Raman scattered optical field in response to changes of the drive laser field intensity and/or frequency. This effect may be described as a dynamic form of optical bistability resulting from the formation and decay of atomic coherence. We have applied this phenomenon to the realization of an all-optical switch. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. PN Lebedev Phys Inst, Moscow 117924, Russia. RP Novikova, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Novikova, Irina/B-9041-2008; Zibrov, Alexander/G-7419-2014 NR 32 TC 14 Z9 14 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 2004 VL 69 IS 6 AR 061802 DI 10.1103/PhysRevA.69.061802 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 835GT UT WOS:000222471400006 ER PT J AU Blackman, EG Field, GB AF Blackman, EG Field, GB TI Dynamical magnetic relaxation: A nonlinear magnetically driven dynamo SO PHYSICS OF PLASMAS LA English DT Article ID MAGNETOHYDRODYNAMIC TURBULENCE; HYDROMAGNETIC TURBULENCE; ACCRETION DISKS; INVERSE CASCADE; HELICITY; FIELD; PLASMAS; SPECTRA AB A nonlinear, time-dependent, magnetically driven dynamo theory that shows how magnetically dominated configurations can relax to become helical on the largest scale available is presented. Coupled time-dependent differential equations for large-scale magnetic helicity, small-scale magnetic helicity, velocity, and the electromotive force are solved. The magnetic helicity on small scales relaxes to drive significant large-scale helical field growth on dynamical (Alfven crossing) time scales, independent of the magnitude of finite microphysical transport coefficients, after which the growing kinetic helicity slows the growth to a viscously limited pace. This magnetically driven dynamo complements the nonlinear kinetic helicity-driven dynamo; for the latter, the growing magnetic helicity fluctuations suppress, rather than drive, large-scale magnetic helicity growth. A unified set of equations accommodates both types of dynamos. (C) 2004 American Institute of Physics. C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Rochester, Laser Energet Lab, Rochester, NY 14627 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blackman, EG (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. NR 33 TC 22 Z9 22 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD JUN PY 2004 VL 11 IS 6 BP 3264 EP 3269 DI 10.1063/1.1739236 PG 6 WC Physics, Fluids & Plasmas SC Physics GA 822KW UT WOS:000221539300036 ER PT J AU Cheeseman, JM Lovelock, CE AF Cheeseman, JM Lovelock, CE TI Photosynthetic characteristics of dwarf and fringe Rhizophora mangle L. in a Belizean mangrove SO PLANT CELL AND ENVIRONMENT LA English DT Article DE oligotrophy; phosphorus fertilization; Rubisco; stomatal conductance ID CARBON ISOTOPE DISCRIMINATION; VS. PHOSPHORUS LIMITATION; GAS-EXCHANGE; AVICENNIA-MARINA; NUTRIENT ENRICHMENT; NATURAL-ENVIRONMENT; STOMATAL RESPONSES; FIELD CONDITIONS; GREY MANGROVE; SALINITY AB Twin Cays (Belize) is a highly oligotrophic mangrove archipelago dominated by Rhizophora mangle L. Ocean-fringing trees are 3-7 m tall with a leaf area index (LAI) of 2.3, whereas in the interior, dwarf zone, trees are 1.5 m or less, and the LAI is 0.7. P-fertilization of dwarf trees dramatically increases growth. As a partial explanation of these characteristics, it was hypothesized that differences in stature and growth rates would reflect differences in leaf photosynthetic capacity, as determined by the photochemical and biochemical characteristics at the chloroplast level. Gas exchange and chlorophyll fluorescence were used to compare photosynthesis of dwarf, fringe and fertilized trees. Regardless of zonation or treatment, net CO2 exchange (A) and photosynthetic electron transport were light saturated at less than 500 mumol photons m(-2) s(-1), and low-light quantum efficiencies were typical for healthy C-3 plants. On the other hand, light-saturated A was linearly related to stomatal conductance g(s). with seasonal, zonal and treatment differences in photosynthesis corresponding linearly to differences in the mean gs. Overall, photosynthetic capacity appeared to be co-regulated with stomatal conductance, minimizing the variability of C-i at ambient CO2 (and hence, C-i/C-a). Based on the results of in vitro assays, regulation of photosynthesis in R. mangle appeared to be accomplished, at least in part, by regulation of Rubisco activity. C1 Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Cheeseman, JM (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. EM j.cheese@life.uiuc.edu RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 34 TC 22 Z9 28 U1 3 U2 12 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD JUN PY 2004 VL 27 IS 6 BP 769 EP 780 DI 10.1111/j.1365-3040.2004.01181.x PG 12 WC Plant Sciences SC Plant Sciences GA 827BQ UT WOS:000221873700011 ER PT J AU Jehl, JR AF Jehl, JR TI Carnivorous Canada geese SO WILSON BULLETIN LA English DT Article AB Geese are normally herbivorous. I report an instance of Canada Geese (Branta canadensis) feeding on alkali flies (Ephydra hians) at hypersaline Mono Lake, California. The bout was brief and possibly represented exploratory behavior by inexperienced birds. C1 Natl Museum Nat Hist, Div Birds, Smithsonian Inst, Washington, DC 20560 USA. RP Jehl, JR (reprint author), Natl Museum Nat Hist, Div Birds, Smithsonian Inst, Washington, DC 20560 USA. EM grebe5k@cs.com NR 7 TC 0 Z9 0 U1 4 U2 7 PU WILSON ORNITHOLOGICAL SOC PI ANN ARBOR PA MUSEUM OF ZOOLOGY UNIV MICHIGAN, ANN ARBOR, MI 48109 USA SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD JUN PY 2004 VL 116 IS 2 BP 179 EP 180 DI 10.1676/03-127 PG 2 WC Ornithology SC Zoology GA 862OA UT WOS:000224499200010 ER PT J AU James, HF AF James, HF TI The osteology and phylogeny of the Hawaiian finch radiation (Fringillidae : Drepanidini), including extinct taxa SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE adaptive radiation; comparative anatomy; evolution; fossils; Hawaiian honeycreepers; island biogeography; morphology; palaeontology; Passeriformes ID WORLD 9-PRIMARIED OSCINES; DARWINS FINCHES; HONEYCREEPERS DREPANIDIDAE; APPENDAGE MYOLOGY; ANCIENT DNA; POO-ULI; BIRDS; AVES; SYSTEMATICS; EVOLUTION AB The monophyly and phylogeny of the adaptive radiation of Hawaiian finches (Fringillidae: Drepanidini; honeycreepers, auct.) were studied using parsimony analysis of comparative osteology, combined with Templeton (Wilcoxon signed-ranks) tests of alternative phylogenetic hypotheses. Eighty-four osteological characters were scored in 59 terminal taxa of drepanidines, including 24 fossil forms, and in 30 outgroup species. The optimal phylogenetic trees show considerable agreement, and some conflict, with independently derived ideas about drepanidine evolution. The monophyly of a large Hawaiian radiation was upheld, although one fossil taxon from Maui fell outside the drepanidine clade. The finch-billed species were placed as basal drepanidine taxa, and continental cardueline finches (Carduelini) were identified as the radiation's closest outgroups. The study found anatomical as well as phylogenetic evidence that the radiation had a finch-billed ancestor. The optimal trees identify the red-and-black plumage group as a clade, and suggest that the tubular tongue evolved only once in the radiation. Because comparative osteology provides too few characters to strongly support all the nodes of the tree, it was helpful to evaluate statistical support for alternative hypotheses about drepanidine relationships using the Templeton test. Among the alternatives that received significant statistical support are a relationship of the drepanidines with cardueline finches rather than with the Neotropical honeycreepers (Thraupini), classification of the controversial genera Paroreomyza and Melamprosops as drepanidines, and a secondary loss of the tubular tongue in Loxops mana. The hypothesis of monophyly for all the Hawaiian taxa in the study was not rejected statistically. The study provides a framework for incorporating morphological and palaeontological information in evolutionary studies of the Drepanidini. (C) 2004 The Linnean Society of London. C1 Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. Edward Grey Inst Field Ornithol, Oxford OX1 3PS, England. RP James, HF (reprint author), Smithsonian Inst, Bird Div, NHB MRC-116,POB 37012, Washington, DC 20013 USA. EM james.helen@nmnh.si.edu NR 100 TC 40 Z9 41 U1 1 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD JUN PY 2004 VL 141 IS 2 BP 207 EP 255 DI 10.1111/j.1096-3642.2004.00117.x PG 49 WC Zoology SC Zoology GA 830ZB UT WOS:000222161600003 ER PT J AU Hungate, BA Stiling, PD Dijkstra, P Johnson, DW Ketterer, ME Hymus, GJ Hinkle, CR Drake, BG AF Hungate, BA Stiling, PD Dijkstra, P Johnson, DW Ketterer, ME Hymus, GJ Hinkle, CR Drake, BG TI CO2 elicits long-term decline in nitrogen fixation SO SCIENCE LA English DT Article ID GROWTH C1 No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. No Arizona Univ, Dept Chem, Flagstaff, AZ 86011 USA. Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Univ Nevada, Dept Biol, Reno, NV 89557 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21038 USA. Dynamac Corp, Kennedy Space Ctr, FL 32899 USA. RP Hungate, BA (reprint author), No Arizona Univ, Dept Biol Sci, Box 5640, Flagstaff, AZ 86011 USA. EM bruce.hungate@nau.edu RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 5 TC 90 Z9 98 U1 4 U2 55 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAY 28 PY 2004 VL 304 IS 5675 BP 1291 EP 1291 DI 10.1126/science.1095549 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 824EV UT WOS:000221669600044 PM 15166370 ER PT J AU Cardellach, E Ao, CO Juarez, MD Hajj, GA AF Cardellach, E Ao, CO Juarez, MD Hajj, GA TI Carrier phase delay altimetry with GPS-reflection/occultation interferometry from low Earth orbiters SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID REFLECTED SIGNALS; OCEAN ALTIMETRY; SYSTEM; PARIS AB GPS signals reflected off the surface of the Earth can be detected by receivers aboard occulting Low Earth Orbiters (LEOs). In this work, carrier phase interferometry between the reflected and direct occultation signals is performed to infer its relative delay at centimetric error. Our analysis shows that submeter sensitivity on the surface heights can formally be reached with this technique. The potential applications to polar ice altimetry are discussed. C1 CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. RP Cardellach, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM ecardellach@cfa.harvard.edu; chi.o.ao@jpl.nasa.gov; mtj@jpl.nasa.gov; george.a.hajj@jpl.nasa.gov RI Cardellach, Estel/C-9418-2012 OI Cardellach, Estel/0000-0001-8908-0972 NR 13 TC 30 Z9 31 U1 1 U2 2 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 MAY 26 PY 2004 VL 31 IS 10 AR L10402 DI 10.1029/2004GL019775 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 827OK UT WOS:000221909900005 ER PT J AU Simmons, RB AF Simmons, RB TI Description of Sphecosoma pattiannae, new species, with comments on its novel male androconia (Lepidoptera : Arctiidae : Arctiinae : Euchromiini) SO ZOOTAXA LA English DT Article DE Lepidoptera; Arctiidae; Euchromiini; Sphecosoma; new species; androconia; mimicry AB A new species of the mimetic tiger moth genus Sphecosoma, S. pattiannae Simmons sp. nov., is described and illustrated. The presumed sister species, S. tarsalis (Walker), is redescribed with illustrations of the male and female genitalia. These two species bear a novel androconial structure, which is a dorsal pouch at the base of the genitalia; this structure is described and illustrated. Phylogenetic placement of S. tarsalis and S. pattiannae within Sphecosoma Butler is discussed, with male and female genital comparisons to S. cognatum (Walker). C1 Smithsonian Inst, USDA ARS, Inst Plant Sci, Systemat Entomol Lab, Washington, DC 20013 USA. RP Simmons, RB (reprint author), Smithsonian Inst, USDA ARS, Inst Plant Sci, Systemat Entomol Lab, POB 37012,Nat Hist Bldg,MRC-168, Washington, DC 20013 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 24 PY 2004 IS 519 BP 1 EP 12 PG 12 WC Zoology SC Zoology GA 869LW UT WOS:000224985900001 ER PT J AU Hamana, T Takada, M Yoshida, N AF Hamana, T Takada, M Yoshida, N TI Searching for massive clusters in weak lensing surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; galaxies : haloes; cosmology : theory; dark matter; large-scale structure of Universe ID LARGE-SCALE STRUCTURE; DARK-MATTER HALOS; COSMOLOGICAL PARAMETERS; DENSITY PROFILE; GALAXY-CLUSTER; STATISTICS; SIMULATIONS; FLUCTUATIONS; EVOLUTION AB We explore the ability of weak lensing surveys to locate massive clusters. We use both analytic models of dark matter haloes and mock weak lensing surveys generated from a large cosmological N-body simulation. The analytic models describe the average properties of weak lensing haloes and predict the number counts, enabling us to compute an effective survey selection function. We argue that the delectability of massive haloes depends not only on the halo mass but also strongly on the redshift where the halo is located. We test the model prediction for the peak number counts in weak lensing mass maps against mock numerical data, and find that the noise resulting from intrinsic galaxy ellipticities causes a systematic effect which increases the peak counts. We develop a correction scheme for the systematic effect in an empirical manner, and show that, after correction, the model prediction agrees well with the mock data. The mock data is also used to examine the completeness and efficiency of the weak lensing halo search by fully taking into account the noise and the projection effect by large-scale structures. We show that the detection threshold of S/N = 4similar to5 gives an optimal balance between completeness and efficiency. Our results suggest that, for a weak lensing survey with a galaxy number density of n(g) = 30 arcmin(-2) with a mean redshift of z = 1, the mean number of haloes which are expected to cause lensing signals above S/N = 4 is N-halo(S/N > 4) = 37 per 10 deg(2), whereas 23 of the haloes are actually detected with S/N > 4, giving the effective completeness as good as 63 per cent. Alternatively, the mean number of peaks in the same area is N-peak = 62 for a detection threshold of S/N = 4. Among the 62 peaks, 23 are caused by haloes with the expected peak height S/N > 4, 13 result from haloes with 3 < S/N < 4 and the remaining 26 peaks are either the false peaks caused by the noise or haloes with a lower expected peak height. Therefore the contamination rate is 44 per cent (this could be an overestimation). Weak lensing surveys thus provide a reasonably efficient way to search for massive clusters. C1 Inst Astrophys, F-75014 Paris, France. Natl Astron Observ Japan, Tokyo 1818588, Japan. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hamana, T (reprint author), Inst Astrophys, 98bis Blvd Arago, F-75014 Paris, France. EM hamana@iap.fr RI Takada, Masahiro/A-4364-2011; Yoshida, Naoki/A-4305-2011 NR 38 TC 107 Z9 108 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2004 VL 350 IS 3 BP 893 EP 913 DI 10.1111/j.1365-2966.2004.07691.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827PP UT WOS:000221913200014 ER PT J AU Badran, HM AF Badran, HM TI Mirror cleaning and reflectivity degradation at 1300 and 2300m above sea level at Mt. Hopkins, Arizona SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Cherenkov telescope; gamma-ray astronomy; mirror cleaning; mirror reflectivity AB The factors degrading optical performance of the atmospheric Cherenkov telescope optics are the deterioration of the reflecting coating itself on the surface and the accumulation of the contamination on the mirror surface. After an exposure of more than two and half years in the open air the mirrors cleaned monthly by just water were not subject to any considerable degradation in their reflectivity. The only drop in the reflectivity (similar to5%) was at 310 nm. The optical maintenance of the Whipple mirrors and evaluation with test mirrors at the two potential sites (1300 and 2300 m above sea level) at Mt. Hopkins are reported. Generally, the results at both sites are comparable. Sunlight seems to be an important parameter leading to mirror degradation either by itself or together with contaminants. The various cleaning methods used provided almost the same reflectivity restoration with somewhat better performance for mirrors at 1300 m asl. The present results suggest that mirror cleaning can minimize the down time for coating renewal. This is particularly important for the VERITAS project and other large arrays currently under construction. (C) 2004 Elsevier B.V. All rights reserved. C1 Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Badran, HM (reprint author), Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. EM husbadran@frcu.eun.eg NR 8 TC 6 Z9 6 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD MAY 21 PY 2004 VL 524 IS 1-3 BP 162 EP 168 DI 10.1016/j.nima.2004.01.062 PG 7 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 824IG UT WOS:000221679400017 ER PT J AU Laurance, WF Albernaz, AKM Fearnside, PM Vasconcelos, HL Ferreira, LV AF Laurance, WF Albernaz, AKM Fearnside, PM Vasconcelos, HL Ferreira, LV TI Deforestation in Amazonia SO SCIENCE LA English DT Letter ID BRAZILIAN AMAZON; ENVIRONMENT C1 Smithsonian Trop Res Inst, Balboa, Panama. Museu Paraense Emilio Goeldi, BR-66077530 Belem, Para, Brazil. Inst Nacl de Pesquisas da Amazonia, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. Univ Fed Uberlandia, Inst Biol, BR-38400902 Uberlandia, MG, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011; Vasconcelos, Heraldo/C-3353-2013; Albernaz, Ana Luisa/K-5226-2012 OI Fearnside, Philip/0000-0003-3672-9082; Vasconcelos, Heraldo/0000-0001-6969-7131; NR 14 TC 91 Z9 105 U1 4 U2 19 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAY 21 PY 2004 VL 304 IS 5674 BP 1109 EP 1109 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 822FP UT WOS:000221524500018 PM 15155931 ER PT J AU Erwin, DH Krakauer, DC AF Erwin, DH Krakauer, DC TI Insights into innovation SO SCIENCE LA English DT Editorial Material C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Santa Fe Inst, Santa Fe, NM 87501 USA. RP Erwin, DH (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM erwin@santafe.edu; krakauer@santafe.edu RI Erwin, Douglas/A-9668-2009 NR 6 TC 21 Z9 22 U1 3 U2 7 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAY 21 PY 2004 VL 304 IS 5674 BP 1117 EP 1119 DI 10.1126/science.1099385 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 822FP UT WOS:000221524500027 PM 15155937 ER PT J AU Mullis, CR Vikhlinin, A Henry, JP Forman, W Gioia, IM Hornstrup, A Jones, C McNamara, BR Quintana, H AF Mullis, CR Vikhlinin, A Henry, JP Forman, W Gioia, IM Hornstrup, A Jones, C McNamara, BR Quintana, H TI Evolution of the cluster X-ray luminosity function SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : general; X-rays : galaxies : clusters ID MEDIUM-SENSITIVITY SURVEY; ECLIPTIC POLE SURVEY; FLUX-LIMITED SAMPLE; DEGREE ROSAT SURVEY; N-LOG S; GALAXY CLUSTERS; OPTICAL IDENTIFICATIONS; SOURCE CATALOG; WARPS SURVEY; UNIVERSE AB We report measurements of the cluster X-ray luminosity function out to z = 0.8 based on the final sample of 201 galaxy systems from the 160 Square Degree ROSAT Cluster Survey. There is little evidence for any measurable change in cluster abundance out to z similar to 0.6 at luminosities of less than a few times 10(44) h(50)(-2) ergs s(-1) (0.5 - 2.0 keV). However, for 0.6 < z < 0.8 and at luminosities above 10(44) h(50)(-2) ergs s(-1), the observed volume densities are significantly lower than those of the present-day population. We quantify this cluster deficit using integrated number counts and a maximum likelihood analysis of the observed luminosity-redshift distribution fit with a model luminosity function. The negative evolution signal is more than 3 sigma regardless of the adopted local luminosity function or cosmological framework. Our results and those from several other surveys independently confirm the presence of evolution. Whereas the bulk of the cluster population does not evolve, the most luminous and presumably most massive structures evolve appreciably between z = 0.8 and the present. Interpreted in the context of hierarchical structure formation, we are probing sufficiently large mass aggregations at sufficiently early times in cosmological history, when the universe has yet to assemble these clusters to present-day volume densities. C1 European So Observ Headquarters, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow Space Res Inst, Moscow 117810, Russia. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. INAF, CNR, Ist Radioastron, I-40129 Bologna, Italy. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. RP Mullis, CR (reprint author), European So Observ Headquarters, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM cmullis@eso.org RI Gioia, Isabella/B-6982-2012; OI Gioia, Isabella/0000-0003-3127-498X; Forman, William/0000-0002-9478-1682 NR 69 TC 37 Z9 37 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2004 VL 607 IS 1 BP 175 EP 189 DI 10.1086/383234 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822FN UT WOS:000221523900014 ER PT J AU Mahdavi, A Geller, MJ AF Mahdavi, A Geller, MJ TI A redshift survey of nearby galaxy groups: The shape of the mass density profile SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : kinematics and dynamics; galaxies : statistics ID COLD DARK-MATTER; SPHERICAL STELLAR-SYSTEMS; DATA REDUCTION TECHNIQUES; X-RAY-CLUSTERS; CHANDRA OBSERVATIONS; INFALL REGION; VELOCITY DISPERSIONS; ELLIPTIC GALAXIES; RADIAL-VELOCITIES; OUTER REGIONS AB We constrain the mass profile and orbital structure of nearby groups and clusters of galaxies. Our method yields the joint probability distribution of the density slope n, the velocity anisotropy beta, and the turnover radius r(0) for these systems. The measurement technique does not use results from N-body simulations as priors. We incorporate 2419 new redshifts (included here) in the fields of 41 systems of galaxies with z < 0.04. The new groups have median velocity dispersion sigma = 360 km s(-1). We also use 979 archived redshifts in the fields of eight nearly relaxed clusters with z < 0.1. Within R less than or similar to 2r(200), the data are consistent with a single power-law matter density distribution with slope n = 1.8 2.2 for systems with sigma < 470 km s(-1) and n = 1.6-2.0 for those with sigma > 470 (95% confidence). We show that a simple, scale-free phase-space distribution function (DF) f (E, L-2) proportional to (-E)(alpha-1/2) L-2beta is consistent with the data as long as the matter density has a cusp. Using this DF, matter density profiles with constant-density cores (n = 0) are ruled out with better than 99.7% confidence. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Mahdavi, A (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM amahdavi@ifa.hawaii.edu; mgeller@cfa.harvard.edu NR 81 TC 40 Z9 41 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 MAY 20 PY 2004 VL 607 IS 1 BP 202 EP 219 DI 10.1086/383458 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822FN UT WOS:000221523900016 ER PT J AU Kempner, JC David, LP AF Kempner, JC David, LP TI A Chandra study of the core of the nearby cluster A576 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : individual (A576); intergalactic medium; X-rays : galaxies : clusters ID X-RAY OBSERVATIONS; GALAXY CLUSTER; GAS; ABELL-2052; BUBBLES AB We present data from a Chandra observation of the nearby cluster of galaxies A576. The core of the cluster shows a significant departure from dynamical equilibrium. We show that this core gas is most likely the remnant of a merging subcluster, which has been stripped of much of its gas, depositing a stream of gas behind it in the main cluster. The unstripped remnant of the subcluster is characterized by a different temperature, density, and metallicity than that of the surrounding main cluster, suggesting its distinct origin. Continual dissipation of the kinetic energy of this minor merger may be sufficient to counteract most cooling in the main cluster over the lifetime of the merger event. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kempner, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jkempner@head-cfa.harvard.edu; ldavid@head-cfa.harvard.edu NR 24 TC 10 Z9 10 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2004 VL 607 IS 1 BP 220 EP 225 DI 10.1086/383407 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822FN UT WOS:000221523900017 ER PT J AU Adelberger, KL Steidel, CC Shapley, AE Hunt, MP Erb, DK Reddy, NA Pettini, M AF Adelberger, KL Steidel, CC Shapley, AE Hunt, MP Erb, DK Reddy, NA Pettini, M TI Optical selection of star-forming galaxies at redshifts 1 < z < 3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : formation; galaxies : high-redshift ID LYMAN-BREAK GALAXIES; STELLAR MASS DENSITY; PHOTOMETRIC REDSHIFTS; LUMINOSITY DENSITY; DEEP-FIELDS; EVOLUTION; POPULATIONS; UNIVERSE AB Few galaxies have been found between the redshift ranges z less than or similar to 1 probed by magnitude-limited surveys and z greater than or similar to 3 probed by Lyman break surveys. Comparison of galaxy samples at lower and higher redshift suggests that large numbers of stars were born and the Hubble sequence began to take shape at the intermediate redshifts 1 < z < 3, but observational challenges have prevented us from observing the process in much detail. We present simple and efficient strategies that can be used to find large numbers of galaxies throughout this important but unexplored redshift range. All the strategies are based on selecting galaxies for spectroscopy on the basis of their colors in ground-based images taken through a small number of optical filters: GRi for redshifts 0.85 < z < 1.15, GRz for 1 < z < 1.5, and U(n)GR for 1.4 < z < 2.1 and 1.9 < z < 2.7. The performance of our strategies is quantified empirically through spectroscopy of more than 2000 galaxies at 1 < z < 3.5. We estimate that more than half of the UV luminosity density at 1 < z < 3 is produced by galaxies that satisfy our color selection criteria. Our methodology is described in detail, allowing readers to devise analogous selection criteria for other optical filter systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Palomar Observ, Pasadena, CA 91125 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Adelberger, KL (reprint author), Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. NR 34 TC 176 Z9 176 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2004 VL 607 IS 1 BP 226 EP 240 DI 10.1086/383221 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822FN UT WOS:000221523900018 ER PT J AU Doeleman, SS Lonsdale, CJ Kondratko, PT Predmore, CR AF Doeleman, SS Lonsdale, CJ Kondratko, PT Predmore, CR TI Using VLBI to probe the Orion KL outflow on Au scales SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Orion Kleinmann-Low); ISM : jets and outflows; masers; stars : formation; stars : winds, outflows ID SIO MASER EMISSION; 86 GHZ; MOLECULAR OUTFLOW; R-CASSIOPEIAE; STARS; IRC2; POLARIZATION; VARIABILITY; POSITIONS; PROTOSTAR AB We present the first contemporaneous 43 and 86 GHz VLBI images of the v = 1, J = 2 --> 1 and J = 1 --> 0 SiO masers in the Orion KL nebula. Both maser species exhibit the same general morphology of earlier J = 1 --> 0 maser images, which appear to trace the edges of a bipolar conical outflow. Surprisingly, the J = 2 --> 1 masers form farther from the central protostar than the J = 1 --> 0 masers, a fact not readily explained by current SiO maser pumping models. The average magnitude of offsets between corresponding regions of the two masing transitions is approximately 14% of the total radial extent of the SiO maser emission. This offset indicates that each transition must trace different physical conditions. C1 MIT, Haystack Observ, Westford, MA 01886 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Doeleman, SS (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM sdoeleman@haystack.edu; clonsdale@haystack.edu; pkondratko@cfa.harvard.edu; predmore@predmoreassociates.com NR 34 TC 9 Z9 9 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2004 VL 607 IS 1 BP 361 EP 368 DI 10.1086/383220 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822FN UT WOS:000221523900030 ER PT J AU Wargelin, BJ Markevitch, M Juda, M Kharchenko, V Edgar, R Dalgarno, A AF Wargelin, BJ Markevitch, M Juda, M Kharchenko, V Edgar, R Dalgarno, A TI Chandra observations of the "dark'' Moon and geocoronal solar wind charge transfer SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; Moon; solar wind; X-rays : diffuse background; X-rays : general ID X-RAY-EMISSION; LOCAL INTERSTELLAR-MEDIUM; MAGNETIC-FIELD; COMET HYAKUTAKE; C/1999 S4; IONS; SPECTRA; MAPS; NEUTRALS; HYDROGEN AB We have analyzed data from two sets of calibration observations of the Moon made by the Chandra X-Ray Observatory. In addition to obtaining a spectrum of the bright side that shows several distinct fluorescence lines, we also clearly detect time-variable soft X-ray emission, primarily O VII Kalpha and O VIII Lyalpha, when viewing the optically dark side. The apparent dark-side brightness varied in time by at least an order of magnitude, up to similar to2 x 10(-6) photons s(-1) arcmin(-2) cm(-2) between 500 and 900 eV, which is comparable to the typical 3/4 keV-band background emission measured in the ROSAT All-Sky Survey. The spectrum is also very similar to background spectra recorded by Chandra in low-or moderate-brightness regions of the sky. Over a decade ago, ROSAT also detected soft X-rays from the dark side of the Moon, which were tentatively ascribed to continuum emission from energetic solar wind electrons impacting the lunar surface. The Chandra observations, however, with their better spectral resolution, combined with contemporaneous measurements of solar wind parameters, strongly favor charge transfer between highly charged solar wind ions and neutral hydrogen in the Earth's geocorona as the mechanism for this emission. We present a theoretical model of geocoronal emission and show that predicted spectra and intensities match the Chandra observations very well. We also model the closely related process of heliospheric charge transfer and estimate that the total charge transfer flux observed from Earth amounts to a significant fraction of the soft X-ray background, particularly in the ROSAT 3/4 keV band. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Space Res Inst IKI, Moscow 117810, Russia. RP Wargelin, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bwargelin@cfa.harvard.edu OI Juda, Michael/0000-0002-4375-9688 NR 39 TC 101 Z9 101 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2004 VL 607 IS 1 BP 596 EP 610 DI 10.1086/383410 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822FN UT WOS:000221523900050 ER PT J AU Bobe, R Behrensmeyer, AK AF Bobe, R Behrensmeyer, AK TI The expansion of grassland ecosystems in Africa in relation to mammalian evolution and the origin of the genus Homo SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Review DE Plio-pleistocene hominins; Homo; Paranthropus; grasslands; faunal change; Turkana Basin; Lower Omo Valley ID LOWER OMO VALLEY; HOMINID EVOLUTION; LATE PLIOCENE; SHUNGURA FORMATION; EAST-AFRICA; DISPERSAL EVENTS; CLIMATIC-CHANGE; OLDUVAI GORGE; TURKANA BASIN; FAUNAL CHANGE AB The relationship between climatic change and human evolution can be framed in terms of three major hypotheses. A modem version of the long-held savanna hypothesis posits that the expansion of grassland ecosystems in Africa was driven by global climatic change and led to the divergence of hominins from the apes and to the origin of the Homo clade. A related idea suggests that hominins originated in the late Miocene, and Homo in the late Pliocene, as constituents of broader pulses of faunal turnover synchronized by episodes of global climatic change. A more recent concept, the variability selection hypothesis, emphasizes the importance of fluctuating climates and environments, rather than any single trend, in shaping human adaptation and evolution. Here we evaluate these ideas for the Plio-Pleistocene in light of new analyses of fossil mammals from the Turkana Basin of Kenya and Ethiopia. Our results show that between 4 and 1 Ma (million years ago), there were profound faunal changes in the Turkana Basin. The most important of these changes include significant shifts in the abundance of the common families of mammals, episodes of high faunal turnover, and an increase in the number and abundance of species that show adaptations to grassland ecosystems. Episodes of relatively high faunal turnover occurred in the intervals 3.4-3.2, 2.8-2.6, 2.4-2.2, and 2.0-1.8 Ma. Paranthropus and Homo appear in the Turkana Basin during successive intervals of high turnover at 2.8-2.6 and at 2.4-2.2 Ma, while the appearance of Homo erectus is coupled to a major episode of turnover and grassland expansion after 2 Ma. Thus, there was not a single turnover pulse of relevance to late Pliocene hominins, but multiple events that successively led to the appearance of Paranthropus, early Homo, and H. erectus. Our results also show evidence of large-scale, 100 ky-periodicity shifts in the fauna beginning at 2.5 Ma, during the time that Homo and lithic artifacts first appear in the Turkana Basin, lending support to the variability selection hypothesis [Science 273 (1996) 922; Potts R., 1996b. Humanity's Descent: The Consequences of Ecological Instability. Avon Books, New York.] during the latest Pliocene. The savanna hypothesis may not explain the divergence of hominins from other apes, but it could be correct in stressing the importance of grasslands to the early evolution of Homo. The fundamental importance of grasslands may lie in the complexity and heterogeneity they added to the range of habitats available to the early species of the genus Homo. The turnover pulse hypothesis [Vrba, E.S., 1988. Late Pliocene climatic events and hominid evolution. In: Grine, F.E(Ed.). Evolutionary History of the "Robust" Australopithecines. Aldine, New York, pp. 405-426; Vrba, E.S., 1995. The fossil record of African antelopes (Mammalia, Bovidae) in relation to human evolution and paleoclimate. In: Vrba, E.S., Denton, G.H., Partridge, T.C., Burckle, L.H. (Eds.). Paleoclimate and Evolution, with Emphasis on Human Origins. Yale Univ. Press, New Haven, pp. 385-424.] may be correct in linking critical events in human evolution to broader pulses of faunal change ultimately driven by climate, but our results show that any such link is complex, with at least four rather than one pulse of change during the Pliocene and early Pleistocene of the Turkana Basin. Published by Elsevier B.V. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Bobe, R (reprint author), Smithsonian Inst, Dept Paleobiol, POB 37012,NHB MRC 121, Washington, DC 20013 USA. EM bobe.rene@nmnh.si.edu; behrensmeyer.kay@nmnh.si.edu NR 122 TC 153 Z9 161 U1 11 U2 96 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 MAY 20 PY 2004 VL 207 IS 3-4 SI SI BP 399 EP 420 DI 10.1016/j.palaeo.2003.09.033 PG 22 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 828RR UT WOS:000221991000009 ER PT J AU Mihlbachler, MC Lucas, SG Emry, RJ Bayshashov, B AF Mihlbachler, MC Lucas, SG Emry, RJ Bayshashov, B TI A new brontothere (Brontotheriidae, perissodactyla, mammalia) from the eocene of the ily basin of kazakstan and a Phylogeny of Asian "Horned" brontotheres SO AMERICAN MUSEUM NOVITATES LA English DT Article ID NICHE DIFFERENTIATION; RHINOCEROS; FOOTPRINTS; TELEOCERAS; ECOLOGY; FOSSIL AB A new genus and species of "horned" brontothere, Aktautitan hippopotamopus, from the Ily Basin of Kazakstan is described from three skulls and nearly complete postcranial material. This material occurs in fluvio-lacustrine red beds of the upper part of the Eocene (Irdinmanhan) Kyzylbulak Formation at Aktau Mountain. Trackways occurring in the overlying layers are also attributed to this new brontothere. Additionally, several misleading problems in the taxonomy of Asian horned brontotheres are addressed. We conclude that Protitan khaitshinus Yanovskaya, 1980 is a junior objective synonym of Metatitan relictus Granger and Gregory, 1943. Protitan reshetovi Yanovskaya, 1980 is removed from the genus Protitan and possibly belongs within Metatitan. Brachydiastematherium transylvanicum Bockh and Maty, 1876, the only bona fide European brontothere, known from a single partial mandible, is morphologically consistent with Metatitan Granger and Gregory, 1943. Although B. transylvanicum is known from very fragmentary material, it is possible that Metatitan is a junior synonym of Brachydiastematherium. The first cladistic phylogeny of middle and late Eocene Asian horned brontotheres was constructed with 40 characters and 17 taxa. Aktautitan, Metatitan, Brachydiastematherium, and Embolotherium form a monophyletic clade, with Aktautitan hippopotamopus as the most basal member of this clade. Within this clade, there are two monophyletic trichotomies: a Metatitan relictus, M. primus, Brachydiastematherium transylvanicum clade and a "Metatitan" progressus, Embolotherium andrewsi, E. grangeri clade. The cladogram topology suggests that the elevated frontonasal horns shared by Aktautitan and Metatitan represent the ancestral morphology of the bizarre "battering-ram" of Embolotherium. We extend the subfamily name Embolotheriinae to include these taxa. The unusually shortened distal limb segments of A. hippopotamopus resemble those of a phylogenetically disparate group of large ungulates that have convergently evolved hippolike limb proportions. We conclude that these limb proportions probably do not indicate a semiaquatic lifestyle, as had been previously surmised. C1 Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA. New Mexico Museum Nat Hist, Albuquerque, NM 87104 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Kazak Acad Sci, Inst Zool, Alma Ata 480032, Kazakhstan. RP Mihlbachler, MC (reprint author), Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. EM mihlbach@amnh.org; slucas@nmmnh.state.nm.us; emry.robert@nmnh.si.edu; baybol@nursat.kz NR 79 TC 3 Z9 5 U1 0 U2 3 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD MAY 14 PY 2004 IS 3439 BP 1 EP 43 DI 10.1206/0003-0082(2004)439<0001:ANBBPM>2.0.CO;2 PG 43 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 822GH UT WOS:000221526500001 ER PT J AU Moiseyev, N Carr, LD Malomed, BA Band, YB AF Moiseyev, N Carr, LD Malomed, BA Band, YB TI Transition from resonances to bound states in nonlinear systems: application to Bose-Einstein condensates SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID COMPLEX COORDINATE METHOD; POTENTIALS; OPERATORS; ENERGIES; WIDTHS AB It is shown using the Gross-Pitaevskii equation that resonance states of Bose-Einstein condensates with attractive interactions can be stabilized into true bound states. A semiclassical variational approximation and an independent quantum variational numerical method are used to calculate the energies (chemical potentials) and linewidths of resonances of the time-independent Gross-Pitaevskii equation; both methods produce similar results. Borders between the regimes of resonances, bound states and, in two and three dimensions, collapse are identified. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Ecole Normale Super, Lab Kastler Brossel, Dept Phys, F-75231 Paris 05, France. Tel Aviv Univ, Fac Engn, Dept Interdisciplinary Studies, IL-69978 Tel Aviv, Israel. Ben Gurion Univ Negev, Dept Chem, IL-84105 Beer Sheva, Israel. Ben Gurion Univ Negev, Dept Electroopt, IL-84105 Beer Sheva, Israel. Technion Israel Inst Technol, Dept Chem, IL-32000 Haifa, Israel. Technion Israel Inst Technol, Minerva Ctr Nonlinear Phys Complex Syst, IL-32000 Haifa, Israel. RP Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Carr, Lincoln/E-3819-2016 OI Carr, Lincoln/0000-0002-4848-7941 NR 30 TC 35 Z9 35 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAY 14 PY 2004 VL 37 IS 9 BP L193 EP L200 AR PII S0953-4075(04)78005-0 DI 10.1088/0953-4075/37/3/L02 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 826MR UT WOS:000221833700002 ER PT J AU Brown, JW Adamski, D Hodges, RW Bahr, SM AF Brown, JW Adamski, D Hodges, RW Bahr, SM TI Catalog of the type specimens of Gelechioidea (Lepidoptera) in the collection of the National Museum of Natural History, Smithsonian Institution, Washington, DC SO ZOOTAXA LA English DT Article DE Lepidoptera; Gelechioidea; type specimens; catalogue; USNM ID LECITHOCERIDAE AB The collection of the National Museum of Natural History, Smithsonian Institution, Washington, D. C., is second only to that of The Natural History Museum ( formerly British Museum of Natural History), London, in the number of type specimens of the superfamily Gelechioidea ( Lepidoptera). The Smithsonian houses 1,375 gelechioid types: 1,249 holotypes, 48 lectotypes, 1 neotype, 69 species represented by one or more syntypes, and 8 species represented by one or more "pseudotypes" (i.e., specimens identified as "type" by an accompanying label that are unlikely to be the type). Three former curators are responsible for the vast majority of the type specimens: August Busck, J. F. Gates Clarke, and Ronald W. Hodges. We present a list of the species for which a type is deposited in the USNM, organized alphabetically. For each species we provide an abbreviated reference to the original description and label data. This list represents the second contribution to a larger effort to make available information on the Lepidoptera type holdings of the USNM. C1 ARS, Systemat Entomol Lab, PSI,USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. Texas A&M Univ, Dept Entomol, College Stn, TX 77843 USA. RP Brown, JW (reprint author), ARS, Systemat Entomol Lab, PSI,USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. EM jbrown@sel.barc.usda.gov NR 29 TC 5 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 MAY 14 PY 2004 IS 510 BP 1 EP 151 PG 151 WC Zoology SC Zoology GA 869LJ UT WOS:000224984500001 ER PT J AU Gates, MW Cascante-Marin, A AF Gates, MW Cascante-Marin, A TI A new phytophagous species of Eurytoma (Hymenoptera : Eurytomidae) attacking Werauhia gladioliflora (Bromeliales : Bromeliaceae) SO ZOOTAXA LA English DT Article DE Eurytomidae; Bromeliaceae; phytophagous; Eurytoma; Werauhia AB Eurytoma werauhia Gates, new species, is described and illustrated. This species was reared from the floral buds of Werauhia gladioliflora (Wendl.) (Bromeliales: Bromeliaceae), in Costa Rica. This plant represents a new host record for the genus. Eurytoma werauhia is compared with other known species of Eurytoma, primarily due to its host and metasomal coloration. C1 Natl Museum Nat Hist, MRC 168, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1090 GB Amsterdam, Netherlands. RP Gates, MW (reprint author), Natl Museum Nat Hist, MRC 168, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. EM mgates@sel.barc.usda.gov; cascante@science.uva.nl NR 20 TC 7 Z9 9 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 14 PY 2004 IS 512 BP 1 EP 10 PG 10 WC Zoology SC Zoology GA 869LL UT WOS:000224984700001 ER PT J AU Marrero, J Rodriguez, AD Baran, P Raptis, RG Sanchez, JA Ortega-Barria, E Capson, TL AF Marrero, J Rodriguez, AD Baran, P Raptis, RG Sanchez, JA Ortega-Barria, E Capson, TL TI Bielschowskysin, a gorgonian-derived biologically active diterpene with an unprecedented carbon skeleton SO ORGANIC LETTERS LA English DT Article ID PSEUDOPTEROGORGIA-KALLOS BIELSCHOWSKY; OCTOCORAL; ELISABETHAE; SYSTEM; DNA AB Bielschowskysin is a naturally occurring diterpene isolated from the Caribbean gorgonian octocoral Pseudopterogorgia kallos. Its highly oxygenated hexacyclic structure is based on a previously undescribed tricyclo[9.3.0.0(2,10)]tetradecane ring system that was established through spectroscopic analysis and X-ray crystallographic analysis. Bielschowskysin was shown to exhibit antimalarial activity against Plasmodium falciparum as well as strong anticancer activity against two human cancer cell lines. C1 Univ Puerto Rico, Dept Chem, UPR Stn, San Juan, PR 00931 USA. Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. Smithsonian Inst, Labs Analyt Biol, Washington, DC 20013 USA. Florida State Univ, Cell & Mol Biol Pathogens Unit, Inst Trop Med & Hlth Sci, Balboa, Ancon, Panama. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Rodriguez, AD (reprint author), Univ Puerto Rico, Dept Chem, UPR Stn, POB 23346, San Juan, PR 00931 USA. EM arodrig@cnnet.upr.edu RI Johnson, Selena/K-3541-2013 FU FIC NIH HHS [U01TW-01021-01] NR 15 TC 71 Z9 73 U1 3 U2 19 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1523-7060 J9 ORG LETT JI Org. Lett. PD MAY 13 PY 2004 VL 6 IS 10 BP 1661 EP 1664 DI 10.1021/ol0499495d PG 4 WC Chemistry, Organic SC Chemistry GA 818XT UT WOS:000221278500036 PM 15128261 ER PT J AU Forsberg-Taylor, NK Howard, AD Craddock, RA AF Forsberg-Taylor, NK Howard, AD Craddock, RA TI Crater degradation in the Martian highlands: Morphometric analysis of the Sinus Sabaeus region and simulation modeling suggest fluvial processes SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE craters; degradation ID RECENT VOLCANISM; INCISION MODELS; SOIL PRODUCTION; EARLY MARS; EVOLUTION; CONSTRAINTS; EROSION; RIVER; AUSTRALIA; SURFACE AB Results from simulation modeling of crater degradation by fluvial and eolian processes are compared with size-frequency and depth of infilling statistics for the heavily cratered Sinus Sabaeus quadrangle of Mars. The fractional degree of infilling of craters greater than 10 km in diameter in this region is bimodal, with a small population of post-Noachian craters with little infilling, whereas most Noachian craters are strongly infilled. This pattern is most consistent with fluvial erosion of craters, because modeling indicates that craters fill rapidly at first, but the rate of infilling diminishes through time as crater wall heights diminish and the area of deposition on the crater floor increases. Simulated rates of crater infilling by eolian processes are more constant, which would be expected to produce craters equally distributed in degree of infilling, which is not observed. The small slope of the size-frequency distribution in the 10-30 km size range is also consistent with the more rapid fluvial erosion of smaller craters. The analysis also suggests that rates of crater production and of crater degradation were in rough balance during the Noachian epoch in the 10-30 km size range. C1 Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Sci, Washington, DC 20560 USA. RP Forsberg-Taylor, NK (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM nkforsbe@artsci.wustl.edu; ah5p@virginia.edu; craddock@nasm.si.edu RI Craddock, Robert/B-3884-2013; OI Howard, Alan/0000-0002-5423-1600 NR 37 TC 74 Z9 74 U1 2 U2 14 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 MAY 12 PY 2004 VL 109 IS E5 AR E05002 DI 10.1029/2004JE002242 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 821PQ UT WOS:000221474700002 ER PT J AU Nagamine, K Springel, V Hernquist, L Machacek, M AF Nagamine, K Springel, V Hernquist, L Machacek, M TI Photometric properties of Lyman-break galaxies at z=3 in cosmological SPH simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : evolution; galaxies : formation; cosmology : theory ID HIGH-REDSHIFT GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; LY-ALPHA FOREST; DARK-MATTER UNIVERSE; STELLAR MASS DENSITY; HUBBLE DEEP FIELD; STAR-FORMATION; LUMINOSITY FUNCTION; ULTRAVIOLET LUMINOSITY; INTERGALACTIC MEDIUM AB We study the photometric properties of Lyman-break galaxies (LBGs) formed by redshift z= 3 in a set of large cosmological smoothed-particle hydrodynamics (SPH) simulations of the Lambda cold dark matter (LambdaCDM) model. Our numerical simulations include radiative cooling and heating with a uniform UV background, star formation, supernova feedback and a phenomenological model for galactic winds. Analysing a series of simulations of varying box size and particle number allows us to isolate the impact of numerical resolution on our results. We compute spectra of simulated galaxies using a population synthesis model, and derive colours and luminosity functions of galaxies at z=3 after applying local dust extinction and absorption by the intergalactic medium (IGM). We find that the simulated galaxies have U-n-G and G-R colours consistent with observations, provided that intervening absorption by the IGM is applied. The observed properties of LBGs, including their number density, colours and luminosity functions, can be explained if LBGs are identified with the most massive galaxies at z= 3, having typical stellar mass of M(star)similar to 10(10) h(-1) M-circle dot, a conclusion broadly consistent with earlier studies based on hydrodynamic simulations of the LambdaCDM model. We also find that most simulated LBGs were continuously forming stars at a high rate for more than 1 Gyr up until z= 3, but with numerous starbursts lying on top of the continuous component. Interestingly, our simulations suggest that more than 50 per cent of the total stellar mass and star formation rate in the Universe are accounted for by galaxies that are not detected in the current generation of LBG surveys. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM knagamin@cfa.harvard.edu; volker@mpa-garching.mpg.de; lars@cfa.harvard.edu; mmachacek@cfa.harvard.edu OI Nagamine, Kentaro/0000-0001-7457-8487 NR 67 TC 47 Z9 47 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 MAY 11 PY 2004 VL 350 IS 2 BP 385 EP 395 DI 10.1111/j.1365-2966.2004.07664.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 816FJ UT WOS:000221095500004 ER PT J AU Poon, MY Merritt, D AF Poon, MY Merritt, D TI A self-consistent study of triaxial black hole nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : nuclei; galaxies : structure stellar; dynamics ID DYNAMICAL EQUILIBRIUM; ELLIPTIC GALAXIES; GALACTIC NUCLEI; NUMERICAL-MODEL; STELLAR SYSTEM; ORBITS; CUSPS; HALOS AB We construct models of triaxial galactic nuclei containing central black holes using the method of orbital superposition and then verify their stability by advancing N-body realizations of the models forward in time. We assume a power-law form for the stellar density, rho proportional to r(-gamma), with gamma=1 and 2; these values correspond approximately to the nuclear density profiles of bright and faint galaxies, respectively. Equidensity surfaces are ellipsoids with fixed axis ratios. The central black hole is represented by a Newtonian point mass. We consider three triaxial shapes for each value of gamma: almost prolate, almost oblate, and maximally triaxial. Two kinds of orbital solution are attempted for each mass model: the first including only regular orbits, the second including chaotic orbits as well. We find that stable configurations exist, for both values of gamma, in the maximally triaxial and nearly oblate cases; however, steady state solutions in the nearly prolate geometry could not be found. A large fraction of the mass, of order 50% or more, could be assigned to the chaotic orbits without inducing evolution. Our results demonstrate that triaxiality may persist even within the sphere of influence of the central black hole and that chaotic orbits may constitute an important building block of galactic nuclei. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. RP Poon, MY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 30 TC 38 Z9 38 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 774 EP 787 DI 10.1086/383190 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900011 ER PT J AU Merritt, D Poon, MY AF Merritt, D Poon, MY TI Chaotic loss cones and black hole fueling SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : elliptical and lenticular, cD; galaxies : nuclei; galaxies : structure; stellar dynamics ID TRIAXIAL STELLAR-SYSTEMS; EARLY-TYPE GALAXIES; TIDAL DISRUPTION; GALACTIC NUCLEI; EVOLUTION; DYNAMICS; STARS; RATES; QSOS; QUASARS AB In classical loss cone theory, stars are supplied to a central black hole via gravitational scattering onto low angular momentum orbits. Higher feeding rates are possible if the gravitational potential near the black hole is nonaxisymmetric and the orbits are chaotic. Motivated by recently published, self-consistent models, we evaluate rates of stellar capture and disruption in triaxial nuclei. Rates are found to substantially exceed those in collisionally resupplied loss cones, as long as an appreciable fraction of the orbits are centrophilic. The mass captured by a black hole after a given time in a steep (rhosimilar tor(-2)) nucleus scales as sigma(5) with sigma the stellar velocity dispersion, and the accumulated mass in 10(10) yr is of the correct order to reproduce the M-circle-sigma relation. Triaxiality can solve the "final parsec problem'' of decaying black hole binaries by increasing the flux of stars into the binary's loss cone. C1 Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Merritt, D (reprint author), Rochester Inst Technol, Dept Phys, 84 Lomb Mem Dr, Rochester, NY 14623 USA. EM merritt@mail.r.t.edu; mpoon@cfa.harvard.edu NR 45 TC 119 Z9 119 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 788 EP 798 DI 10.1086/382497 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900012 ER PT J AU Markevitch, M Gonzalez, AH Clowe, D Vikhlinin, A Forman, W Jones, C Murray, S Tucker, W AF Markevitch, M Gonzalez, AH Clowe, D Vikhlinin, A Forman, W Jones, C Murray, S Tucker, W TI Direct constraints on the dark matter self-interaction cross section from the merging galaxy cluster 1E 0657-56 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies : clusters : individual (1E 0657-56); galaxies : formation; large-scale structure of universe ID COLLISIONAL NATURE; DENSITY PROFILE; HYPOTHESIS; HALOES AB We compare new maps of the hot gas, dark matter, and galaxies for 1E 0657-56, a cluster with a rare high-velocity merger occurring nearly in the plane of the sky. The X-ray observations reveal a bullet-like gas subcluster just exiting the collision site. A prominent bow shock gives an estimate of the subcluster velocity, 4500 km s(-1), which lies mostly in the plane of the sky. The optical image shows that the gas lags behind the subcluster galaxies. The weak-lensing mass map reveals a dark matter clump lying ahead of the collisional gas bullet but coincident with the effectively collisionless galaxies. From these observations, one can directly estimate the cross section of the dark matter self-interaction. That the darkmatter is not fluid-like is seen directly in the X-ray-lensing mass overlay; more quantitative limits can be derived from three simple independent arguments. The most sensitive constraint, sigma/m<1 cm(2) g(-1), comes from the consistency of the subcluster mass-to-light ratio with the main cluster (and universal) value, which rules out a significant mass loss due to dark matter particle collisions. This limit excludes most of the 0.5-5 cm(2) g(-1) interval proposed to explain the flat mass profiles in galaxies. Our result is only an order-of-magnitude estimate that involves a number of simplifying, but always conservative, assumptions; stronger constraints may be derived using hydrodynamic simulations of this cluster. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. Univ Bonn, Inst Astrophys & Extraterr Forsch, D-53121 Bonn, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Russian Acad Sci, Space Res Inst, Moscow 117810, Russia. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Markevitch, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM maxim@head.cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 NR 34 TC 249 Z9 249 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 819 EP 824 DI 10.1086/383178 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900015 ER PT J AU Yuan, F Quataert, E Narayan, R AF Yuan, F Quataert, E Narayan, R TI On the nature of the variable infrared emission from Sagittarius A* SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; Galaxy : center; radiation mechanisms : nonthermal ID SUPERMASSIVE BLACK-HOLE; X-RAY FLARE; NONTHERMAL SYNCHROTRON EMISSION; SHORT-TERM VARIABILITY; ACCRETION FLOWS; GALACTIC-CENTER; SGR-A; MILKY-WAY; LINEAR-POLARIZATION; CENTRAL PARSEC AB Recent infrared (IR) observations of the center of our Galaxy indicate that the supermassive black hole (SMBH) source Sgr A* is strongly variable in the IR. The timescale for the variability, similar to30 minutes, is comparable to that of the X-ray flares observed by Chandra and XMM-Newton, suggesting a common physical origin. In this paper, we investigate the nature of the IR emission in the context of models recently proposed to interpret the X-ray flares. We show that the IR emission in Sgr A* can be well explained by nonthermal synchrotron emission if a small fraction of the electrons in the innermost region of the accretion flow around the black hole are accelerated into a broken power-law distribution, perhaps through transient events such as magnetic reconnection. The model predicts differences in the variability amplitudes of flares in the IR and X-rays, in general agreement with observations. It also predicts that the IR emission should be linearly polarized, as has indeed been observed during one epoch. IR and X-ray flares analogous to those observed in Sgr A* may be detectable from other accreting SMBHs, provided Lless than or similar to10(-8) L-Edd; at higher luminosities, the flaring emission is dominated by thermal synchrotron self-Compton emission, which is likely to be less variable. C1 Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Purdue Univ, Dept Phys, 525 NW Ave, W Lafayette, IN 47907 USA. EM fyuan@physics.purdue.edu; eliot@astron.berkeley.edu; narayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 49 TC 121 Z9 121 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 MAY 10 PY 2004 VL 606 IS 2 BP 894 EP 899 DI 10.1086/383117 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900021 ER PT J AU Slavin, JD Nichols, JS Blair, WP AF Slavin, JD Nichols, JS Blair, WP TI FUSE observations of highly ionized gas in the Vela Supernova Remnant SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Vela Supernova Remnant); shock waves; supernova remnants; ultraviolet : ISM ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; ROSAT-PSPC OBSERVATION; RADIATIVE SHOCK-WAVES; HIGH-VELOCITY GAS; ABSORPTION-LINES; INTERSTELLAR ABSORPTION; NORTHEAST REGION; CYGNUS LOOP; DIRECTION; DISCOVERY AB We present Far Ultraviolet Spectroscopic Explorer (FUSE) data on O VI absorption lines observed toward nine stars behind the Vela supernova remnant (SNR). The O VI observations are compared with International Ultraviolet Explorer (IUE) observations of C IV absorption toward the same stars. All of these stars are B stars, which generally have complex continua, making the extraction of absorption lines difficult. However, four of the stars, HD 72088, HD 72089, HD 72350, and HD 72537, are rapid rotators (v sin igreater than or similar to150 km s(-1)), making the derivation of absorption column densities much easier. We present O VI and C IV column densities for the "main component'' (i.e., the low-velocity component) for these stars. In the FUSE spectra of three of the rapid rotators (HD 72088, HD 72089, and HD 72537) we find high-velocity components of O VI at similar to150 km s(-1) that we attribute to the SNR shock. HD 72350 has very strong H-2 absorption, which obscures any possible high-velocity O VI absorption. To detect the high-velocity O VI absorption in HD 72088 requires employing a technique for removing the H-2 line at 1032.35 Angstrom (121.6 km s(-1) relative to O VI). The O VI data are consistent with steady radiative shock models with v(s)approximate to150 km s(-1), but we do not detect C IV at the same velocities. Instead we find high-velocity C IV at lower velocities (similar to100 km s(-1)). We discuss the implications of our results for models of the evolution of the Vela SNR. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Slavin, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jslavin@cfa.harvard.edu; jnichols@cfa.harvard.edu; wpb@pha.jhu.edu OI Slavin, Jonathan/0000-0002-7597-6935 NR 33 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 900 EP 910 DI 10.1086/383135 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900022 ER PT J AU Hunter, TR Zhang, Q Sridharan, TK AF Hunter, TR Zhang, Q Sridharan, TK TI IRAS 18317-0757: A cluster of embedded massive stars and protostars SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : individual (AFGL 2194, G23.95+0.15, IRAS 18317-0757); stars : formation ID H-II REGIONS; ULTRACOMPACT HII-REGIONS; DENSE CLOUD CORES; RADIO-CONTINUUM; GALACTIC PLANE; INTERSTELLAR EXTINCTION; MOLECULAR CLOUD; DUST EMISSION; DARK CLOUD; GHZ AB We present high-resolution, multiwavelength-continuum, and molecular-line images of the massive star forming region IRAS 18317-0757. The global infrared through millimeter spectral energy distribution can be approximated by a two-temperature model (25 and 63 K) with a total luminosity of approximately log (L/L-circle dot)=5.2. Previous submillimeter imaging resolved this region into a cluster of five dust cores, one of which is associated with the ultracompact H II region G23.955+0.150, and another with a water maser. In our new 2.7 mm continuum image obtained with BIMA, only the UCH II region is detected, with total flux and morphology in good agreement with the free-free emission in the VLA centimeter-wave maps. For the other four objects, the nondetections at 2.7 mm and in the MSX mid-infrared bands are consistent with cool dust emission with a temperature of 13-40 K and a luminosity of 1000-40,000 L-circle dot. By combining single-dish and interferometric data, we have identified over two dozen virialized (CO)-O-18 cores in this region that contain approximate to40% of the total molecular gas mass present. While the overall extent of the (CO)-O-18 and dust emission is similar, the emission peaks do not correlate well in detail. At least 11 of the 123 infrared stars identified by 2MASS in this region are likely to be associated with the star-forming cluster. Two of these objects (both associated with the UCH II region) were previously identified as O stars via infrared spectroscopy. Most of the rest of the reddened stars have no obvious correlation with the (CO)-O-18 cores or the dust continuum sources. In summary, our observations indicate that considerable fragmentation of the molecular cloud has taken place during the time required for the UCH II region to form and for the O stars to become detectable at infrared wavelengths. Additional star formation appears to be ongoing on the periphery of the central region, where up to four B-type (proto) stars have formed among a substantial number of (CO)-O-18 cores. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, MS-78,60 Garden St, Cambridge, MA 02138 USA. EM thunter@cfa.harvard.edu OI Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 NR 61 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 929 EP 942 DI 10.1086/383181 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900025 ER PT J AU Sollins, PK Zhang, QZ Ho, PTP AF Sollins, PK Zhang, QZ Ho, PTP TI The case for local collapse in the W51 star-forming region SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : clouds; ISM : kinematics and dynamics; radio lines : ISM; stars : formation ID DYNAMICAL COLLAPSE; RADIO-CONTINUUM; MASSIVE CORES; AMMONIA MASER; OUTFLOW; CLOUDS AB We present observations of the W51 high-mass star-forming region at 86 and 110 GHz made with the Berkeley-Illinois-Maryland Association (BIMA) array. The observations include the (HCO+)-C-13(J=1-->0), SiO(J=2-->1, nu=0), SO2(8(1,7)-->8(0,8)), SO2(8(3,5)-->9(2,8)), (CO)-C-13(J=1-->0), and (CO)-O-18(J=1-->0) lines. We compare the (HCO+)-C-13(J=1-->0) data to earlier work and find that these data support the hypothesis that infall in the W51 region is taking place in several localized regions, each involving on the order of 100 M-circle dot of gas. The data do not support the hypothesis that the collapse is global, involving tens of thousands M-circle dot of gas. We calculate dust masses for two dense cores containing ultra-compact H II regions and find that these masses are consistent with the localized infall model, being on the order of 100 M-circle dot. We estimate gas column densities from the observations of CO and SO2 and find them to be consistent with the other mass estimates, assuming abundances from other hot molecular cores. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Sollins, PK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Zhang, Qizhou/0000-0003-2384-6589 NR 24 TC 25 Z9 25 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 943 EP 951 DI 10.1086/382035 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900026 ER PT J AU Blake, C Bloom, JS AF Blake, C Bloom, JS TI Optical limits on precursor emission from gamma-ray bursts with known redshift SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; gamma rays : bursts ID 29 MARCH 2003; SDSS J124602.54+011318.8; TIDAL DISRUPTION; NEUTRON-STARS; TRANSIENT; SUPERNOVA; AFTERGLOW; PROGENITORS; SYSTEM; ENERGY AB Making use of virtual observatory data, we present the first comprehensive sample of optical observations conducted before the explosion times of all gamma-ray bursts (GRBs) with known redshifts. In total, the fields of 11 such GRBs were observed by the Near-Earth Asteroid Tracking ( NEAT) program from years to hours before the bursts. Although the typical limiting magnitudes from these observations are R approximate to 20 mag, we find no evidence for a significant detection of a precursor. The deepest nondetection of precursor emission is from GRB 030329, reaching down to an absolute B-band magnitude of M-B approximate to - 18 mag from 6 to 1500 days ( rest frame) before the burst. This is of comparable brightness to supernovae, which in some scenarios for GRB progenitors are predicted to predate a GRB on similar timescales. Since sources cannot be localized to better than similar to 500 mas ( 3 sigma) with current large-area surveys, unrelated supernovae or active galactic nucleus activity in GRB hosts could be mistaken for genuine precursor emission. This possibility motivates the need for not only deep wide-field imaging, but imaging at high spatial resolution. C1 Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. RP Blake, C (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM cblake@astro.princeton.edu; jbloom@cfa.harvard.edu NR 60 TC 1 Z9 1 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 1019 EP 1028 DI 10.1086/383134 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900034 ER PT J AU Yuan, YF Narayan, R Rees, MJ AF Yuan, YF Narayan, R Rees, MJ TI Constraining alternate models of black holes: Type I X-ray bursts on accreting fermion-fermion and boson-fermion stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; dense matter; X-rays : binaries; X-rays : bursts ID SELF-GRAVITATING SYSTEMS; NEUTRON-STAR; EVENT-HORIZON; NUCLEAR-FUSION; SHELL FLASHES; DARK-MATTER; STABILITY; BINARIES; REDSHIFT AB The existence of black holes remains open to doubt until other conceivable options are excluded. With this motivation, we consider a model of a compact star in which most of the mass consists of dark particles of some kind and a small fraction of the mass is in the form of ordinary nucleonic gas. The gas does not interact with the dark matter other than via gravity, but collects at the center as a separate fermionic fluid component. Depending on whether the dark mass is made of fermions or bosons, the objects may be called fermion-fermion stars or boson-fermion stars, respectively. For appropriate choices of the mass of the dark matter particles, these objects are viable models of black hole candidates in X-ray binaries. We consider models with a dark mass of 10 M-. and a range of gas mass from 10(-6) to similar to1 M-., and analyze the bursting properties of the models when they accrete gas. We show that all the models would experience thermonuclear type I X-ray bursts at appropriate mass-accretion rates. Since no type I bursts have been reported from black hole candidates, the models are ruled out. The case for identifying black hole candidates in X-ray binaries as true black holes is thus strengthened. C1 Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. EM yfyuan@ustc.edu.cn; narayan@cfa.harvard.edu; mjr@ast.cam.ac.uk OI Narayan, Ramesh/0000-0002-1919-2730 NR 56 TC 44 Z9 44 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 1112 EP 1124 DI 10.1086/383185 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900041 ER PT J AU Chung, SM Drake, JJ Kashyap, VL Lin, LW Ratzlaff, PW AF Chung, SM Drake, JJ Kashyap, VL Lin, LW Ratzlaff, PW TI Doppler shifts and broadening and the structure of the X-ray emission from Algol SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; stars : activity; stars : individual (Algol); X-rays : stars ID LATE-TYPE STARS; CORONAL FORBIDDEN LINES; LIGHT-CURVE ANALYSIS; TRANSITION REGION; RADIO-EMISSION; RS CVN; CAPELLA; FLARE; ABUNDANCES; EVOLUTION AB In a study of Chandra High Energy Transmission Grating spectra of Algol, we clearly detect Doppler shifts caused by the orbital motion of Algol B. These data provide the first definitive proof that the X-ray emission of Algol is dominated by the secondary, in concordance with expectations that the primary B8 component should be X-ray-dark. However, the measured Doppler shifts are slightly smaller than might be expected, implying an effective orbital semimajor axis of about 10 R-circle dot instead of 11.5 R-circle dot for the Algol B center of mass. This could be caused by a small contribution of Algol A, possibly through accretion, to the observed X-ray flux, in which case such a contribution does not exceed 10%-15%. We suggest that the more likely explanation is an asymmetric corona biased toward the system center of mass by the tidal distortion of the surface of Algol B. A detailed analysis of the profiles of the strongest lines indicates the presence of excess line broadening amounting to approximately 150 km s(-1) above that expected from thermal motion and surface rotation. Possible explanations for this additional broadening include turbulence, flows or explosive events, or rotational broadening from a radially extended corona. We favor the latter scenario and infer that a significant component of the corona at temperatures less than 10(7) K has a scale height of order the stellar radius. This interpretation is supported by the shape of the X-ray light curve and tentative detection of a shallow dip at secondary eclipse. We also examine the O VII intercombination and forbidden lines in a Low Energy Transmission Grating Spectrograph observation and find no change in their relative line fluxes as the system goes from quadrature to primary eclipse. Since these lines appear to be strongly affected by UV irradiation from Algol A through radiative excitation of the 2 S-3-->2 P-3 transition, this supports the conjecture that the corona of Algol B at temperatures of several million kelvins must be significantly extended and/or located toward the poles to avoid being shadowed from Algol A during primary eclipse. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chung, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 45 TC 26 Z9 26 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP 1184 EP 1195 DI 10.1086/383195 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RJ UT WOS:000221261900047 ER PT J AU Briceno, C Vivas, AK Hernandez, J Calvet, N Hartmann, L Megeath, T Berlind, P Calkins, M Hoyer, S AF Briceno, C Vivas, AK Hernandez, J Calvet, N Hartmann, L Megeath, T Berlind, P Calkins, M Hoyer, S TI McNeil's Nebula in Orion: The outburst history SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : Herbig-Haro objects; stars : formation; stars : pre-main-sequence; stars : variables : other ID STARS; SCALE; TELESCOPE AB We present a sequence of I-band images obtained at the Venezuela 1 m Schmidt telescope during the outburst of the nebula recently discovered by J. W. McNeil in the Orion L1630 molecular cloud. We derive photometry spanning the preoutburst state and the brightening itself, which is a unique record including 14 epochs and spanning a timescale of (similar to) 5 years. We constrain the beginning of the outburst at some time between 2003 October 28 and November 15. The light curve of the object at the vertex of the nebula, the likely exciting source of the outburst, reveals that it has brightened similar to 5 mag in about 4 months. The timescale for the nebula to develop is consistent with the light-travel time, indicating that we are observing light from the central source scattered by the ambient cloud into the line of sight. We also show recent FLWO optical spectroscopy of the exciting source and of the nearby HH 22. The spectrum of the source is highly reddened; in contrast, the spectrum of HH 22 shows a shock spectrum superposed on a continuum, most likely the result of reflected light from the exciting source reaching the HH object through a much less reddened path. The blue portion of this spectrum is consistent with an early B spectral type, similar to the early outburst spectrum of the FU Orionis variable star V1057 Cygni; we estimate a luminosity of L similar to 219 L-.. The eruptive behavior of McNeil's Nebula, its spectroscopic characteristics and luminosity, suggest that we may be witnessing an FU Ori event on its way to maximum. By further monitoring this object, we will be able decide whether or not it qualifies as a member of this rare class of objects. C1 Ctr Invest Astron CIDA, Merida 5101A, Venezuela. Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. RP Briceno, C (reprint author), Ctr Invest Astron CIDA, Apartado Postal 264, Merida 5101A, Venezuela. EM briceno@cida.ve NR 16 TC 51 Z9 51 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP L123 EP L126 DI 10.1086/421395 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RL UT WOS:000221262100009 ER PT J AU Miller, JM Fabian, AC Reynolds, CS Nowak, MA Homan, J Freyberg, MJ Ehle, M Belloni, T Wijnands, R van der Klis, M Charles, PA Lewin, WHG AF Miller, JM Fabian, AC Reynolds, CS Nowak, MA Homan, J Freyberg, MJ Ehle, M Belloni, T Wijnands, R van der Klis, M Charles, PA Lewin, WHG TI Evidence of black hole spin in GX 339-4: XMM-Newton/EPIC-pn and RXTE spectroscopy of the very high state SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitation; relativity; X-rays : binaries ID X-RAY REFLECTION; ENERGY EXTRACTION; ACCRETION DISKS; EMISSION-LINE; STABLE ORBIT; CYGNUS X-1; FLUORESCENCE; MCG-6-30-15; RADIATION; SPECTRUM AB We have analyzed spectra of the Galactic black hole GX 339 - 4 obtained through simultaneous 76 ks XMM-Newton/ EPIC-pn and 10 ks Rossi X-Ray Timing Explorer observations during a bright phase of its 2002 - 2003 outburst. An extremely skewed, relativistic Fe Kalpha emission line and ionized disk reflection spectrum are revealed in these spectra. Self-consistent models for the Fe Kalpha emission-line profile and disk reflection spectrum rule out an inner disk radius compatible with a Schwarzschild black hole at more than the 8 sigma level of confidence. The best-fit inner disk radius of (2 - 3)r(g) suggests that GX 339 - 4 harbors a black hole with a greater than or equal to 0.8-0.9(where r(g) =G M/c(2) and a = cJ/GM(2), and assuming that reflection in the plunging region is relatively small). This confirms indications for black hole spin based on a Chandra spectrum obtained later in the outburst. The emission line and reflection spectrum also rule out a standard power-law disk emissivity in GX 339 - 4; a broken power-law form with enhanced emissivity inside similar to6r(g) gives improved fits at more than the 8 sigma level of confidence. The extreme red wing of the line and the steep emissivity require a centrally concentrated source of hard X-rays that can strongly illuminate the inner disk. Hard X-ray emission from the base of a jet - enhanced by gravitational light-bending effects - could create the concentrated hard X-ray emission; this process may be related to magnetic connections between the black hole and the inner disk. We discuss these results within the context of recent results from analyses of XTE J1650 - 500 and MCG - 6-30-15, and of models for the inner accretion flow environment around black holes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Villafranca Satellite Tracking Stn, XMM Newton Sci Operat Ctr, E-28080 Madrid, Spain. ESA, Res & Sci Support Dept, Noordwijk, Netherlands. Osserv Astron Brera, INAF, I-3807 Merate, Italy. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Miller, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jmmiller@cfa.harvard.edu NR 39 TC 86 Z9 86 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP L131 EP L134 DI 10.1086/421263 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RL UT WOS:000221262100011 ER PT J AU Raymond, JC Ciaravella, A AF Raymond, JC Ciaravella, A TI Densities and velocities in fast coronal mass ejections: Radiative pumping of the OVI doublet SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : activity; Sun : coronal mass ejections (CMEs) ID SOLAR MINIMUM; FLUX ROPE; ULTRAVIOLET; SPECTROMETER; SOHO; TEMPERATURE; STREAMERS; MODEL; LINES AB In very fast coronal mass ejections (CMEs), it is possible for O vi ions to scatter Lybeta photons that originate in the solar chromosphere and for the lambda1037 transition of O vi to scatter lambda1032 photons from the solar transition region. This scattering process can be identified by departures of the O VI I-1032/I-1037 intensity ratio from its collisional value of 2. We report the first detection of this effect in a CME that occurred on 2000 June 28, and we show that this pumping provides a density diagnostic for CMEs faster than 1600 km s(-1). At heliocentric distances near 3 R-., this diagnostic is useful for densities in the 5 x 10(5) - 10(7) cm(-3) range. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu; ciarave@oapa.astropa.unipa.it OI Ciaravella, Angela/0000-0002-3127-8078 NR 29 TC 16 Z9 16 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2004 VL 606 IS 2 BP L159 EP L162 DI 10.1086/421391 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818RL UT WOS:000221262100018 ER PT J AU Williams, JT Lecchini, D AF Williams, JT Lecchini, D TI Parioglossus galzini, a new species of ptereleotrid dartfish from Rapa Island (Teleostei : Gobioidei : Ptereleotridae) SO ZOOTAXA LA English DT Article DE Gobioidei; Ptereleotridae; Parioglossus galzini; Rapa Island; French Polynesia AB A new species of dart fish, Parioglossus galzini sp. nov., is described based on specimens collected in Haurei Bay, Rapa Island ( French Polynesia). It is distinguished from all other described species of Parioglossus as follows: dark lateral body stripe absent, 100 or more scales in longitudinal series from above pectoral-fin base to base of caudal fin, pectoral-fin rays 19-21, membrane of first dorsal fin attached to second dorsal fin in males and females, mature males with dorsal-fin spines 3-5 filamentous and about equal in length, fresh males with narrow yellow stripe running dorsolaterally along body from head to caudal fin. C1 Smithsonian Inst, Div Fisheries, NHB, Washington, DC 20013 USA. Univ Perpignan, Ecole Prat Hautes Etud, UMR 8046, CNRS, F-66860 Perpignan, France. Ctr Rech Insulaires & Observ Environm, Moorea, Fr Polynesia. RP Williams, JT (reprint author), Smithsonian Inst, Div Fisheries, NHB, MRC-159,POB 37012, Washington, DC 20013 USA. EM williams.jeff@nmnh.si.edu; lecchini@univ-perp.fr NR 14 TC 4 Z9 4 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 MAY 7 PY 2004 IS 506 BP 1 EP 8 PG 8 WC Zoology SC Zoology GA 869LD UT WOS:000224983800001 ER PT J AU Govoni, JJ West, MA Zivotofsky, D Zivotofsky, AZ Bowser, PR Collett, BB AF Govoni, JJ West, MA Zivotofsky, D Zivotofsky, AZ Bowser, PR Collett, BB TI Ontogeny of squamation in swordfish, Xiphias gladius SO COPEIA LA English DT Article ID RAINBOW-TROUT; ONCORHYNCHUS-MYKISS; SCALE RESORPTION; GROWTH; AGE; ESTRADIOL-17-BETA; MORPHOLOGY; ATLANTIC AB Spinoid scales appear early in the development of Swordfish, Xiphias gladius, and are first discernable in the larval stage. Scales vary in form between two principal types: small single and multispined scales and large multispined scales. Unlike the typical telcostean condition, Xiphias scales are attached along their base, not at their proximal end within scale pockets. Scales persist in juveniles and adults, that is, scales are not shed or resorbed. Scales become more deeply embedded within the dermis as the dermis thickens in ontogeny; consequently only the tips of spines protrude through the dermis of adults. A network of mucous canals with regularly spaced pores to the exterior develop in the dermis of adults, and the mucus produced further insulates scales from the surface of the integument. The ontogeny of the squamation of Xiphias differs front that of the related Istiophoridae. C1 NOAA, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC 28516 USA. Bar Ilan Univ, Brain Sci Program, Interdisciplinary Unit, IL-52100 Ramat Gan, Israel. Cornell Univ, Aquat Anim Hlth Program, Dept Microbiol & Immunol, Coll Vet Med, Ithaca, NY 14853 USA. Smithsonian Inst, Natl Mrine Fisheries Serv, Systemat Lab, Washington, DC 20013 USA. RP Govoni, JJ (reprint author), NOAA, Ctr Coastal Fisheries & Habitat Res, 101 Pivers Isl Rd, Beaufort, NC 28516 USA. EM jeff.govoni@noaa.gov NR 32 TC 3 Z9 3 U1 1 U2 3 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 MAY 5 PY 2004 IS 2 BP 391 EP 396 PG 6 WC Zoology SC Zoology GA 819SX UT WOS:000221336700020 ER PT J AU Remo, JL AF Remo, JL TI A quantitative NEO hazard mitigation scale SO ACTA ASTRONAUTICA LA English DT Article ID NEAR-EARTH OBJECTS; MOMENTUM AB A hazard mitigation scale is presented that quantifies the danger from a potential near-Earth object (NEO) impact with Earth in terms of the energy required to perturb the threatening NEO's orbit to avoid collision in the foreseeable future. The required energy is based on NEO mass, anticipated velocity change to avoid collision, and momentum coupling coefficient for the particular interaction. The momentum coefficient can be empirically determined and depends on the type, intensity, placement of the interaction energy, and target materials. Reliable experimental values for momentum coupling coefficients are provided. (C) 2003 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Remo, JL (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 18, Cambridge, MA 02138 USA. EM jremo@cfa.harvard.edu NR 27 TC 7 Z9 7 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD MAY PY 2004 VL 54 IS 10 BP 755 EP 762 DI 10.1016/j.actaastro.2003.11.001 PG 8 WC Engineering, Aerospace SC Engineering GA 806BT UT WOS:000220410100006 ER PT J AU Raboy, BE Dietz, JM AF Raboy, BE Dietz, JM TI Diet, foraging, and use of space in wild golden-headed lion tamarins SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE Leontopithecus; foraging ecology; ranging patterns; diet; golden-headed lion tamarin ID HOME RANGE SIZE; LEONTOPITHECUS-ROSALIA; CHRYSOMELAS; BEHAVIOR; ECOLOGY AB Lion tamarins (Callitrichidae: Leontopithecus) are small frugi-faunivores that defend large home ranges. We describe results from the first long-term investigation of wild golden-headed lion tamarins (L. chrysomelas; GHLTs). We present data about activity budgets, daily activity cycles, diet, daily path length, home range size, home range overlap, and territorial encounters for three groups of GHLTs that were studied for 1.5-2.5 years in Una Biological Reserve, Bahia State, Brazil, an area characterized by aseasonal rainfall. We compare our results to those from other studies of lion tamarins to identify factors that may influence foraging and ranging patterns in this genus. Ripe fruit, nectar, insects, and small vertebrates were the primary components of the GHLT diet, and gums were rarely eaten. Fruit comprised the majority of plant feeding bouts, and the GHLTs ate at least 79 different species of plants from 32 families. The most common foraging sites for animal prey were epiphytic bromeliads. The GHLTs defended large home ranges averaging 123 ha, but showed strong affinities for core areas, spending 50% of their time in approximately 11% of their home range. Encounters with neighboring groups averaged two encounters every 9 days, and they were always aggressive. Data about time budgets and daily activity cycles reveal that the GHLTs spent most of their time foraging for resources or traveling between foraging sites distributed throughout their home ranges. The GHLTs spent much less time consuming exudates compared to lion tamarins in more seasonal environments. Additionally, the GHLTs had much larger home ranges than golden lion tamarins (L. rosalia), and did not engage in territorial encounters as frequently as L. rosalta. GHLT ranging patterns appear to be strongly influenced by resource acquisition and, to a lesser extent, by resource defense. (C) 2004 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Conservat & Res Ctr, Washington, DC 20008 USA. RP Raboy, BE (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Conservat & Res Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM raboyb@nzp.si.edu NR 36 TC 42 Z9 43 U1 7 U2 51 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD MAY PY 2004 VL 63 IS 1 BP 1 EP 15 DI 10.1002/ajp.20032 PG 15 WC Zoology SC Zoology GA 824SE UT WOS:000221705900001 PM 15152369 ER PT J AU Hostetler, CM Hankerson, SJ Raboy, BE Dietz, JM AF Hostetler, C. M. Hankerson, S. J. Raboy, B. E. Dietz, J. M. TI Habitat preference and ranging patterns of Phayre's leaf monkeys (Trachypithecus phayrei) in north-eastern Thailand SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract C1 [Hostetler, C. M.; Hankerson, S. J.; Dietz, J. M.] Univ Maryland, College Pk, MD 20742 USA. [Raboy, B. E.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 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 MAY PY 2004 VL 62 IS 1 SU 1 MA 43 BP 55 EP 56 PG 2 WC Zoology SC Zoology GA V44HI UT WOS:000202993400044 ER PT J AU Hostetler, CM Hankerson, SJ Raboy, BE Dietz, JM AF Hostetler, C. M. Hankerson, S. J. Raboy, B. E. Dietz, J. M. TI Exploratory study of morphological differences in wild lion tamarin populations SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract C1 [Hostetler, C. M.; Hankerson, S. J.; Dietz, J. M.] Univ Maryland, College Pk, MD 20742 USA. [Raboy, B. E.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 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 MAY PY 2004 VL 62 IS 1 SU 1 MA 42 BP 55 EP 55 PG 1 WC Zoology SC Zoology GA V44HI UT WOS:000202993400043 ER PT J AU Post, J AF Post, J TI Presentation of the Distinguished Public Service Medal of 2003 to George Harlow SO AMERICAN MINERALOGIST LA English DT Biographical-Item C1 Smithsonian Inst, MRC NHB 119, Washington, DC 20560 USA. RP Post, J (reprint author), Smithsonian Inst, MRC NHB 119, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2004 VL 89 IS 5-6 BP 907 EP 907 PG 1 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 824IM UT WOS:000221680000031 ER PT J AU Yen, SH Solis, MA Goolsby, JA AF Yen, SH Solis, MA Goolsby, JA TI Austromusotima, a new musotimine genus (Lepidoptera : Crambidae) feeding on old world climbing fern, Lygodium microphyllum (Schizaeaceae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE cataclystiforin wing pattern; Australia; Papua New Guinea; Indonesia; Cataclysta ID TYMPANIC ORGANS; PYRALOIDEA; PYRALIDAE; AUSTRALIA; GLOSSATA; ASIA AB During the search for natural enemies of Old World climbing fern, Lygodium microphyllum (Cav.) R. Br. (Schizaeaceae), in Australia and southeastern Asia, Cataclysta camptozonale (Hampson) was found to be highly specific to this aggressive vine and was tested as a biological control agent. This musotimine moth species has long been misplaced in a European acentropine genus; therefore, we propose Austromusotima, new genus, to accommodate Austromusotima camptozonale, new combination, as the type species. The syntype series of Oligostima camptozonale is a mixture of specimens of the former species (sensu stricto) and its sibling, Austromusotima metastictalis (Hampson), new combination. A lectotype is designated for A. camptozonale to stabilize the use of the name. The immature stages of A. camptozonale are described and compared with other known musotimine immatures. The immatures of Eugauria albidenta (Hampson) and Cataclysta angulata Moore are illustrated for the first time. Austromusotima is most closely related to Cataclysta seriopunctalis Hampson based on adult morphological characters, but immatures of C. seriopunctalis are unknown, and therefore, this species is not included in Austromusotima. The important, yet incongruent, results between immature and adult characters are discussed in the context of phylogenetic relationships of Austromusotima to other taxa. C1 Univ London Imperial Coll Sci Technol & Med, Dept Biol Sci, Ascot SL5 7YP, Berks, England. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Natl Sun Yat Sen Univ, Dept Biol Sci, Kaohsiung 804, Taiwan. Smithsonian Inst, Natl Museum Nat Hist, USDA ARS, Systemat Entomol Lab, Washington, DC 20013 USA. USDA ARS, Australian Biol Control Lab, Indooroopilly, Qld, Australia. RP Yen, SH (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Biol Sci, Silwood Pk, Ascot SL5 7YP, Berks, England. EM shenhornyen@hotmail.com; asolis@sel.barc.usda.gov; john.goolsby@csiro.au NR 49 TC 11 Z9 13 U1 0 U2 1 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD MAY PY 2004 VL 97 IS 3 BP 397 EP 410 DI 10.1603/0013-8746(2004)097[0397:AANMGL]2.0.CO;2 PG 14 WC Entomology SC Entomology GA 823XF UT WOS:000221646900005 ER PT J AU Kaspi, S Brandt, WN Collinge, MJ Elvis, M Reynolds, CS AF Kaspi, S Brandt, WN Collinge, MJ Elvis, M Reynolds, CS TI Far Ultraviolet Spectroscopic Explorer spectroscopy of absorption and emission lines from the narrow-line Seyfert 1 galaxy NGC 4051 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4051); galaxies : nuclei; galaxies : Seyfert; techniques : spectroscopic; ultraviolet : galaxies ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; X-RAY VARIABILITY; INTRINSIC ABSORPTION; NGC 4051; ARAKELIAN-564; ABSORBER; NGC-5548; VELOCITY; QUASARS AB We present three Far Ultraviolet Spectroscopic Explorer (FUSE) observations of the narrow-line Seyfert 1 galaxy NGC 4051. The most prominent features in the far-ultraviolet (FUV) spectrum are the O vi emission and absorption lines and the H I Lyman series absorption lines, which are detected up to the Lyman edge. We also identify weak emission from N III, C III, and He II. The C III line shows absorption, while none is detected in the N III and He II lines. In H I and C III we detect two main absorption systems at outflow velocities of - 50 +/- 30 and - 240 +/- 40 km s(-1), as well as a possible third one at about - 450 km s(-1). These systems are consistent in velocity with the 10 absorption systems found previously in C IV, N , and Si IV, though the individual systems are blended together in the FUV spectrum. We estimate column densities of the two main absorption systems and find that the H I column density is lower for systems with larger outflow velocity. We detect no flux or spectral variations of NGC 4051 at FUV wavelengths during three epochs spanning 1 yr. This is consistent with the optical light curve, which shows no variations between the three epochs. It is also consistent with the X-ray light curve, which shows consistent flux levels at the three epochs of the FUSE observations, although the X-ray light curve shows strong variations on much shorter timescales. C1 Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Kaspi, S (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. EM shai@wise.tau.ac.il RI Brandt, William/N-2844-2015 OI Brandt, William/0000-0002-0167-2453 NR 41 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 J9 ASTRON J JI Astron. J. PD MAY PY 2004 VL 127 IS 5 BP 2631 EP 2640 DI 10.1086/383555 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 823BP UT WOS:000221585000011 ER PT J AU Olsen, KAG Miller, BW Suntzeff, NB Schommer, RA Bright, J AF Olsen, KAG Miller, BW Suntzeff, NB Schommer, RA Bright, J TI The globular cluster systems of the sculptor group SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : dwarf; galaxies : spiral; galaxies : star clusters ID LARGE-MAGELLANIC-CLOUD; SPACE-TELESCOPE OBSERVATIONS; STELLAR POPULATION-MODELS; COLOR-MAGNITUDE DIAGRAMS; STAR-CLUSTERS; GROUP GALAXIES; LMC CLUSTERS; WASHINGTON SYSTEM; NEARBY GALAXIES; STANDARD STARS AB We use CTIO 4 m Mosaic II images taken with the Washington CM and Harris R filters to identify candidate globular clusters in the six major galaxies of the Sculptor group: NGC 45, 55, 247, 254, 300, and 7793. From follow-up spectroscopy with Hydra-CTIO, we find 19 new globular clusters in NGC 55, 247, 253, and 300, bringing the total number of known Sculptor group globular clusters to 36. The newly discovered clusters have spectroscopic ages consistent with those of old Milky Way globular clusters, and the majority are metal-poor. Their luminosity function closely resembles that of the Milky Way's globular clusters; their metallicity distribution is somewhat more metal-rich, but this may be the result of our color selection of candidates. The mean [alpha/Fe] ratio in the clusters is - 0.2 +/- 0.3, which is lower than the Milky Way average. The specific frequencies S(N) are similar to those of other late-type galaxies. However, if we calculate the specific frequency using the K-band total magnitudes of the host galaxies, we find values that are more than a factor of 2 higher. The kinematics of the globular cluster systems are consistent with rotation with the H I disk in each of the four galaxies; however, only in NGC 253 is this result based on more than seven objects. We suggest that the Sculptor group galaxies add to evidence indicating that many of the first-generation globular clusters formed in disks, not halos. C1 Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. Gemini Observ, La Serena, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Olsen, KAG (reprint author), Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile. EM kolsen@noao.edu; bmiller@gemini.edu; nsuntzeff@noao.edu; rschommer@noao.edu; jbright@head-cfa.harvard.edu OI Miller, Bryan/0000-0002-5665-376X NR 73 TC 41 Z9 41 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2004 VL 127 IS 5 BP 2674 EP 2693 DI 10.1086/383297 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 823BP UT WOS:000221585000014 ER PT J AU Merin, B Montesinos, B Eiroa, C Solano, E Mora, A D'Alessio, P Calvet, N Oudmaijer, RD de Winter, D Davies, JK Harris, AW Cameron, A Deeg, HJ Ferlet, R Garzon, F Grady, CA Horne, K Miranda, LF Palacios, J Penny, A Quirrenbach, A Rauer, H Schneider, J Wesselius, PR AF Merin, B Montesinos, B Eiroa, C Solano, E Mora, A D'Alessio, P Calvet, N Oudmaijer, RD de Winter, D Davies, JK Harris, AW Cameron, A Deeg, HJ Ferlet, R Garzon, F Grady, CA Horne, K Miranda, LF Palacios, J Penny, A Quirrenbach, A Rauer, H Schneider, J Wesselius, PR TI Study of the properties and spectral energy distributions of the Herbig AeBe stars HD 34282 and HD 141569 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : pre-main sequence; stars : fundamental parameters; stars : planetary systems : protoplanetary disks ID T-TAURI STARS; MAIN-SEQUENCE STARS; INTERMEDIATE-MASS STARS; PARTICLE-SIZE DISTRIBUTION; VEGA-LIKE STARS; AE/BE STARS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; INFRARED-EMISSION; YOUNG OBJECTS AB We present a study of the stellar parameters, distances and spectral energy distributions (SEDs) of HD 34282 and HD 141569, two pre-main sequence Herbig AeBe stars. Both objects have been reported to show "anomalous positions" in the HR diagram in the sense that they appear below the main sequence. A significant result of this work is that both stars arc metal-deficient. The Hipparcos distance of HD 34282 is very uncertain and the current study places the star at the expected evolutionary position in the HR diagram, i.e. as a PMS star. The distance for HD 141569 found in this work matches the Hipparcos distance, and the problem of its anomalous position is solved as a result of the low metallicity of the object: using the right metallicity tracks, the star is in the PMS region. The SEDs are constructed using data covering ultraviolet to millimetre wavelengths. Physical, non-parametric models, have been applied in order to extract some properties of the disks surrounding the stars. The disk around HD 34282 is accreting actively, it is massive and presents large grains in the mid-plane and small grains in the surface. HD 141569 has a very low mass disk, which is in an intermediate stage towards a debris-type disk. C1 LAEFF, E-28080 Madrid, Spain. Inst Astrofis Andalucia, CSIC, E-18080 Granada, Spain. Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leeds, Dept Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. TNO, TPD Space Instrumentat, NL-2600 AD Delft, Netherlands. Royal Observ, Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. DLR, Dept Planetary Explorat, D-12489 Berlin, Germany. Univ St Andrews, Dept Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. Inst Astrophys, CNRS, F-75014 Paris, France. NASA, Goddard Space Flight Ctr, NOAO, STIS, Greenbelt, MD 20771 USA. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Observ Paris, F-92195 Meudon, France. Univ Groningen, SRON, NL-9700 AV Groningen, Netherlands. RP Merin, B (reprint author), LAEFF, Apartado 50727, E-28080 Madrid, Spain. EM bruno@laeff.esa.es RI Solano, Enrique/C-2895-2017; Montesinos, Benjamin/C-3493-2017; OI Montesinos, Benjamin/0000-0002-7982-2095; Cameron, Andrew/0000-0002-8863-7828; Deeg, Hans-Jorg/0000-0003-0047-4241; Merin, Bruno/0000-0002-8555-3012 NR 99 TC 62 Z9 62 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2004 VL 419 IS 1 BP 301 EP 318 DI 10.1051/0004-6361:20034561 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 831RH UT WOS:000222213300029 ER PT J AU Castelli, F Kurucz, RL AF Castelli, F Kurucz, RL TI Is missing FeI opacity in stellar atmospheres a significant problem? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : atmospheres; atomic processes; atomic data ID IRON PROJECT; ATOMIC DATA; STARS; PHOTOIONIZATION AB We present an empirical model-atmosphere investigation of missing Fe I opacity. Houdashelt et al. (2000) estimated that if Dragon & Mutschlecner (1980) Fe I cross sections used in the MARCS model atmospheres (Gustafsson et al. 1975) were replaced by the Bautista (1997) cross sections the solar continuous flux would be reduced by 15% in the near ultraviolet. That would imply systematic errors in models for F, G, and K stars. As a consequence, since ATLAS9 (Kurucz 1993a) uses an approximation to the same Dragon & Mutschlecner (1980) opacities, there should also be similar systematic errors in ATLAS9 models that required this investigation. Bound-free Fe I cross sections computed by Bautista (1997) in the framework of the IRON Project were used to generate the continuous Fe I absorption coefficient. It was incorporated in the Kurucz (1993a) ATLAS9 code, in place of that currently used, which is based on approximate cross sections by Kurucz. By combining Opacity Distribution Functions (ODFs) computed without the contribution of Fe I autoionization lines with the new Fe I absorption coefficient which is crowded with autoionization resonances, we obtained solar metallicity model atmospheres and energy distributions for several combinations of T-eff and log g. The comparison of these models with the standard ATLAS9 models has shown that there are no differences in the T-tau(Ross) relations, while there are some changes in the energy distributions for T-eff less than or equal to 7000 K, but limited to small wavelength regions around 2150 Angstrom, where Kurucz has less opacity, and 3350 Angstrom, where Bautista has less opacity. The differences are of the order of 25% and less than 10%, respectively. That around 2150 Angstrom disappears for T-eff less than or equal to5500 K owing to the fall of the emergent flux at these wavelengths in cool stars. This behaviour is independent of the gravity. The explanation is that our line list actually has more autoionizing opacity than Bautista's but it is treated as bound-bound line opacity rather than as bound-free opacity. C1 INAF, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. Osserv Astron Trieste, I-34131 Trieste, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Castelli, F (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, Via Fosso Cavaliere, I-00133 Rome, Italy. EM castelli@ts.astro.it; rkurucz@cfa.harvard.edu NR 21 TC 21 Z9 21 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2004 VL 419 IS 2 BP 725 EP 733 DI 10.1051/0004-6361:20040079 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827GD UT WOS:000221886800034 ER PT J AU Crane, PC Floyd, LE Cook, JW Herring, LC Avrett, EH Prinz, DK AF Crane, PC Floyd, LE Cook, JW Herring, LC Avrett, EH Prinz, DK TI The center-to-limb behavior of solar active regions at ultraviolet wavelengths SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : activity; Sun : faculae, plages; Sun : UV radiation; Sun : rotation; Sun : chromosphere; Sun : photosphere ID IRRADIANCE COMPARISON EXPERIMENT-1; TIME-SERIES; LYMAN-ALPHA; STELLAR INTERFEROMETRY; CONTINUUM RADIATION; SUSIM UARS; 300 NM; VARIABILITY; UV; FLUX AB The time series of solar ultraviolet irradiances measured by the Solar Ultraviolet Spectral Irradiance Monitor on the Upper Atmosphere Research Satellite have been analyzed to describe the center-to-limb behavior of the excess surface brightness of solar active regions over the wavelength range 142-265 nm. Comparison of these results with the analysis by Worden, Woods, and Bowman (2001, ApJ, 560, 1020) of the time series produced by the Solar-Stellar Irradiance Comparison Experiment on the same spacecraft over the wavelength range 120-170 nm shows excellent agreement. For 170-265 nm, we present new results on the center-to-limb behavior of the surface brightness of solar active regions. Comparisons with previous results for the quiet disk show roughly similar behaviors at wavelengths below 168 nm and above 210 nm, where both exhibit weak limb brightening and darkening, respectively. At intermediate wavelengths, 168-210 nm, active regions exhibit much stronger limb darkening than does the quiet disk. Our Fourier analysis and the multi-component modeling of Worden et al. (2001, ApJ, 560, 1020) are found to be complementary and could be productively combined in future work. We also compare our results with a similar analysis based upon the semi-empirical model atmospheres of Fontenla et al. (1999, ApJ, 518, 480), further improved by Avrett. We compare the measurement- and model-based analyses and suggest the direction of improvements needed in the model atmospheres. C1 USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. Interferometr Inc, Chantilly, VA 20151 USA. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Crane, PC (reprint author), USN, Res Lab, Remote Sensing Div, Code 7213, Washington, DC 20375 USA. EM patrick.crane@nrl.navy.mil; linton.floyd@nrl.navy.mil; john.cook@nrl.navy.mil; herring@susim.nrl.navy.mil; eavrett@cfa.harvard.edu NR 63 TC 16 Z9 16 U1 1 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2004 VL 419 IS 2 BP 735 EP 746 DI 10.1051/0004-6361:20040012 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827GD UT WOS:000221886800035 ER PT J AU Perrin, G Ridgway, ST du Foresto, VC Mennesson, B Traub, WA Lacasse, MG AF Perrin, G Ridgway, ST du Foresto, VC Mennesson, B Traub, WA Lacasse, MG TI Interferometric observations of the supergiant stars alpha Orionis and alpha Herculis with FLUOR at IOTA SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : supergiants; infrared : stars; techniques : interferometric ID INFRARED ANGULAR DIAMETER; STELLAR INTERFEROMETRY; DUST; VISIBILITIES; GIANTS; MODELS; CALIBRATION; CETI AB We report the observations in the K band of the red supergiant star alpha Orionis and of the bright giant star alpha Herculis with the FLUOR beamcombiner at the IOTA interferometer. The high quality of the data allows us to estimate limb-darkening and derive precise diameters in the K band which combined with bolometric fluxes yield effective temperatures. In the case of Betelgeuse, data collected at high spatial frequency although sparse are compatible with circular symmetry and there is no clear evidence for departure from circular symmetry. We have combined the K band data with interferometric measurements in the L band and at 11.15 mum. The full set of data can be explained if a 2055 K layer with optical depths tau(K) = 0.060 +/- 0.003, tau(L) = 0.026 +/- 0.002 and tau(11.15 mum) = 2.33 +/- 0.23 is added 0.33 R-star above the photosphere providing a first consistent view of the star in this range of wavelengths. This layer provides a consistent explanation for at least three otherwise puzzling observations: the wavelength variation of apparent diameter, the dramatic difference in limb darkening between the two supergiant stars, and the previously noted reduced effective temperature of supergiants with respect to giants of the same spectral type. Each of these may be simply understood as an artifact due to not accounting for the presence of the upper layer in the data analysis. This consistent picture can be considered strong support for the presence of a sphere of warm water vapor, proposed by Tsuji (2000) when interpreting the spectra of strong molecular lines. C1 Observ Paris, LESIA, UMR 8109, F-92190 Meudon, France. Natl Opt Astron Observ, Tucson, AZ 85726 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perrin, G (reprint author), Observ Paris, LESIA, UMR 8109, F-92190 Meudon, France. EM guy.perrin@obspm.fr NR 37 TC 79 Z9 79 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2004 VL 418 IS 2 BP 675 EP 685 DI 10.1051/0004-6361:20040052 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 824ER UT WOS:000221669200027 ER PT J AU Boirin, L Parmar, AN Barret, D Paltani, S Grindlay, JE AF Boirin, L Parmar, AN Barret, D Paltani, S Grindlay, JE TI Discovery of X-ray absorption features from the dipping low-mass X-ray binary XB 1916-053 with XMM-Newton SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; stars : individual : XB 1916-053; X-rays : binaries ID SOURCE GRO J1655-40; 4U 1915-05; CIRCINUS X-1; PHOTOELECTRIC ABSORPTION; GRATING SPECTROMETER; OPTICAL OBSERVATIONS; SUPERLUMINAL SOURCE; ASCA OBSERVATIONS; ACCRETION DISK; LINE FEATURES AB We report the discovery of narrow Fe XXV and Fe XXVI Kalpha X-ray absorption lines at 6.65(-0.02)(+0.05) and 6.95(-0.04)(+0.05) keV in the persistent emission of the dipping low-mass X-ray binary (LMXB) XB 1916-053 during an XMM-Newton observation performed in September 2002. In addition, there is marginal evidence for absorption features at 1.48 keV, 2.67 keV, 7.82 keV and 8.29 keV consistent with Mg XII, S XVI, Ni XXVII Kalpha and Fe XXVI Kbeta transitions, respectively. Such absorption lines from highly ionized ions are now observed in a number of high inclination (i.e. close to edge-on) LMXBs, such as XB 1916-053 where the inclination is estimated to be between 60-80degrees. This, together with the lack of any orbital phase dependence of the features (except during dips), suggests that the highly ionized plasma responsible for the absorption lines is located in a cylindrical geometry around the compact object. Using the ratio of Fe XXV and Fe XXVI column densities, we estimate the photo-ionization parameter of the absorbing material, xi, to be 10(3.92) erg cm s(-1). Only the Fe XXV line is observed during dipping intervals and the upper-limits to the Fe XXVI column density are consistent with a decrease in the amount of ionization during dipping intervals. This implies the presence of cooler material in the line of sight during dipping. We also report the discovery of a 0.98 keV absorption edge in the persistent emission spectrum. The edge energy decreases to 0.87 keV during deep dipping intervals. The detected feature may result from edges of moderately ionized Ne and/or Fe with the average ionization level decreasing from persistent emission to deep dipping. This is again consistent with the presence of cooler material in the line of sight during dipping. C1 ESA, Estec, Res & Sci Support Dept, Astrophys Miss Div, NL-2200 AG Noordwijk, Netherlands. UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Lab Astrophys Marseille, F-13376 Marseille 12, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP ESA, Estec, Res & Sci Support Dept, Astrophys Miss Div, Postbus 299, NL-2200 AG Noordwijk, Netherlands. EM L.Boirin@sron.nl OI Parmar, Arvind/0000-0002-3307-6517 NR 49 TC 44 Z9 44 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2004 VL 418 IS 3 BP 1061 EP 1072 DI 10.1051/0004-6361:20034550 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 823XB UT WOS:000221646300025 ER PT J AU Robertson, B Yoshida, N Springel, V Hernquist, L AF Robertson, B Yoshida, N Springel, V Hernquist, L TI Disk galaxy formation in a Lambda cold dark matter universe SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : formation; galaxies : spiral; methods : numerical ID SMOOTHED PARTICLE HYDRODYNAMICS; HIERARCHICALLY CLUSTERING UNIVERSES; ANGULAR-MOMENTUM PROBLEM; LYMAN-ALPHA ABSORBERS; TULLY-FISHER RELATION; DIGITAL SKY SURVEY; STAR-FORMATION; GALACTIC DISKS; PECULIAR VELOCITIES; SUPERNOVA FEEDBACK AB We describe hydrodynamic simulations of galaxy formation in a Lambda cold dark matter cosmology, performed using a subresolution model for star formation and feedback in a multiphase interstellar medium (ISM). In particular, we demonstrate the formation of a well-resolved disk galaxy. The surface brightness profile of the galaxy is exponential, with a B-band central surface brightness of 21.0 mag arcsec(-2) and a scale length of R-d = 2.0 h(-1) kpc. We find no evidence for a significant bulge component. The simulated galaxy falls within the I-band Tully-Fisher relation, with an absolute magnitude of I = -21.2 and a peak stellar rotation velocity of V-rot = 121.3 km s(-1). While the total specific angular momentum of the stars in the galaxy agrees with observations, the angular momentum in the inner regions appears to be low by a factor of similar to2. The star formation rate of the galaxy peaks at similar to7 M-circle dot yr(-1) between redshifts z = 2 and 4, with the mean stellar age decreasing from similar to10 Gyr in the outer regions of the disk to similar to7.5 Gyr in the center, indicating that the disk did not simply form inside-out. The stars exhibit a metallicity gradient from 0.7 Z(circle dot) at the edge of the disk to 1.3 Z(circle dot) in the center. Using a suite of idealized galaxy formation simulations with different models for the ISM, we show that the effective pressure support provided by star formation and feedback in our multiphase model is instrumental in allowing the formation of large, stable disk galaxies. If ISM gas is instead modeled with an isothermal equation of state, or if star formation is suppressed entirely, growing gaseous disks quickly violate the Toomre stability criterion and undergo catastrophic fragmentation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ Japan, Tokyo 1818588, Japan. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Robertson, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM brobertson@cfa.harvard.edu RI Yoshida, Naoki/A-4305-2011 NR 57 TC 194 Z9 194 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2004 VL 606 IS 1 BP 32 EP 45 DI 10.1086/382871 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SC UT WOS:000220925800003 ER PT J AU Mauche, CW Liedahl, DA Mathiesen, BF Jimenez-Garate, MA Raymond, JC AF Mauche, CW Liedahl, DA Mathiesen, BF Jimenez-Garate, MA Raymond, JC TI Reprocessing of soft X-ray emission lines in black hole accretion disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : individual (MCG-6-30-15); galaxies : Seyfert; radiative transfer; X-rays : galaxies ID DUSTY WARM ABSORBER; MCG-6-30-15; CORONA; MARKARIAN-766; SPECTRUM; PROFILES; MODEL AB By means of a Monte Carlo code that accounts for Compton scattering and photoabsorption followed by recombination, we investigate the radiation transfer of Lyalpha, Healpha, and recombination continua photons of H- and He-like C, N, O, and Ne produced in the photoionized atmosphere of a relativistic black hole accretion disk. We find that photoelectric opacity causes significant attenuation of photons with energies above the O VIII K edge, that the conversion efficiencies of these photons into lower energy lines and recombination continua are high, and that accounting for this reprocessing significantly (by factors of 21%-105%) increases the flux of the Lyalpha and Healpha emission lines of H- and He-like C and O escaping the disk atmosphere. C1 Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mauche, CW (reprint author), Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA. EM mauche@cygnus.llnl.gov; liedahl1@llnl.gov; mathiesen2@llnl.gov; mario@space.mit.edu; jraymond@cfa.harvard.edu NR 21 TC 8 Z9 8 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2004 VL 606 IS 1 BP 168 EP 172 DI 10.1086/382938 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SC UT WOS:000220925800014 ER PT J AU Furlanetto, SR Schaye, J Springel, V Hernquist, L AF Furlanetto, SR Schaye, J Springel, V Hernquist, L TI Ultraviolet line emission from metals in the low-redshift intergalactic medium SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; diffuse radiation; galaxies : formation; intergalactic medium ID LY-ALPHA FOREST; COLD DARK-MATTER; SMOOTHED PARTICLE HYDRODYNAMICS; SPECTROSCOPIC-EXPLORER DETECTION; LYMAN BREAK GALAXIES; O-VI EMISSION; STAR-FORMATION; INTERSTELLAR-MEDIUM; COSMOLOGICAL SIMULATIONS; GALACTIC SUPERWINDS AB We use a high-resolution cosmological simulation that includes hydrodynamics, multiphase star formation, and galactic winds to predict the distribution of metal line emission at z similar to 0 from the intergalactic medium (IGM). We focus on two ultraviolet doublet transitions, O vi lambdalambda1032, 1038 and C IV lambdalambda1548, 1551. Emission from filaments with moderate overdensities is orders of magnitude smaller than the background, but isolated emission from enriched dense regions with T similar to 10(5)-10(5.5) K and characteristic size similar to50-100 kpc can be detected above the background. We show that the emission from these regions is substantially greater when we use the metallicities predicted by the simulation ( which includes enrichment through galactic winds) than when we assume a uniform IGM metallicity. Luminous regions correspond to volumes that have recently been influenced by galactic winds. We also show that the line emission is clustered on scales similar to1 h(-1) Mpc. We argue that although these transitions are not effective tracers of the warm-hot intergalactic medium, they do provide a route to study the chemical enrichment of the IGM and the physics of galactic winds. C1 CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), CALTECH, Div Phys Math & Astron, Mail Code 130-33, Pasadena, CA 91125 USA. EM sfurlane@tapir.caltech.edu; schaye@ias.edu; volker@mpa-garching.mpg.de; lhernquist@cfa.harvard.edu OI Schaye, Joop/0000-0002-0668-5560 NR 77 TC 28 Z9 28 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2004 VL 606 IS 1 BP 221 EP 236 DI 10.1086/382727 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SC UT WOS:000220925800019 ER PT J AU Perna, R Gaensler, BM AF Perna, R Gaensler, BM TI Are supershells powered by multiple supernovae? Modeling the radio pulsar population produced by OB associations SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : structure; ISM : bubbles; pulsars : general; supernovae : general ID GAMMA-RAY BURSTS; LARGE-MAGELLANIC-CLOUD; ISOLATED NEUTRON-STARS; DATA-ANALYSIS SYSTEMS; H-I SUPERSHELLS; MASSIVE STARS; GALACTIC DISK; EVOLUTION; REMNANTS; SHELLS AB Traditional searches for radio pulsars have targeted individual small regions such as supernova remnants or globular clusters or have covered large contiguous regions of the sky. None of these searches have been specifically directed toward giant supershells, some of which are likely to have been produced by multiple supernova (SN) explosions from an OB association. Here we perform a Monte Carlo simulation of the pulsar population associated with supershells powered by multiple SNe. We predict that several tens of radio pulsars associated with the largest Galactic supershells ( with kinetic energies greater than or similar to10(53) ergs) could be detected with current instruments and a few pulsars associated with the smaller supershells. We test these predictions for some of the supershells that lie in regions covered by past pulsar surveys. For the smaller supershells, our results are consistent with the few detected pulsars per bubble. For the giant supershell GSH 242 - 03+ 37, we find the multiple SN hypothesis inconsistent with current data at the similar to 95% level. We stress the importance of undertaking deep pulsar surveys in correlation with supershells. Failure to detect any pulsar enhancement in the largest of them would put serious constraints on the multiple SN origin for them. Conversely, the discovery of the pulsar population associated with a supershell would allow a different, independent approach to the study of pulsar properties. C1 Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perna, R (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 66 TC 5 Z9 5 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2004 VL 606 IS 1 BP 326 EP 332 DI 10.1086/382868 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SC UT WOS:000220925800027 ER PT J AU Lipkin, YM Ofek, EO Gal-Yam, A Leibowitz, EM Poznanski, D Kaspi, S Polishook, D Kulkarni, SR Fox, DW Berger, E Mirabal, N Halpern, J Bureau, M Fathi, K Price, PA Peterson, BA Frebel, A Schmidt, B Orosz, JA Fitzgerald, JB Bloom, JS van Dokkum, PG Bailyn, CD Buxton, MM Barsony, M AF Lipkin, YM Ofek, EO Gal-Yam, A Leibowitz, EM Poznanski, D Kaspi, S Polishook, D Kulkarni, SR Fox, DW Berger, E Mirabal, N Halpern, J Bureau, M Fathi, K Price, PA Peterson, BA Frebel, A Schmidt, B Orosz, JA Fitzgerald, JB Bloom, JS van Dokkum, PG Bailyn, CD Buxton, MM Barsony, M TI The detailed optical light curve of GRB 030329 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; supernovae : general; supernovae : individual (SN 2003dh) ID GAMMA-RAY BURST; 29 MARCH 2003; IC HYPERNOVA SN-2003DH/GRB-030329; GRB 000301C; CONTINUED EVIDENCE; SUPERNOVA 2002AP; REFRESHED SHOCKS; EARLY AFTERGLOW; DUST ECHOES; ERROR BOX AB We present densely sampled BVRI light curves of the optical transient associated with the gamma-ray burst (GRB) 030329, the result of a coordinated observing campaign conducted at five observatories. Augmented with published observations of this GRB, the compiled optical data set contains 2687 photometric measurements, obtained between 78 minutes and 79 days after the burst. This data set allows us to follow the photometric evolution of the transient with unprecedented detail. We use the data to constrain the light curve of the underlying supernova (SN) 2003dh and show that it evolved faster than and was probably somewhat fainter than the Type Ic SN 1998bw, associated with GRB 980425. We find that our data can be described by a broken power-law decay perturbed by a complex variable component. The early- and late-time decay slopes are determined to be alpha(1) approximate to 1.1 and alpha(2) approximate to 2. Assuming this single-break power-law model, we constrain the break to lie between similar to3 and similar to8 days after the burst. This simple, singly broken power-law model, derived only from the analysis of our optical observations, may also account for available multiband data, provided that the break happened similar to8 days after the burst. The more complex double-jet model of Berger et al. provides a comparable fit to the optical, X-ray, millimeter, and radio observations of this event. The unique early coverage available for this event allows us to trace the color evolution of the afterglow during the first hours after the burst. We detect a significant change in optical colors during the first day. Our color analysis is consistent with a cooling-break frequency sweeping through the optical band during the first day. The light curves of GRB 030329 reveal a rich array of variations, superposed over the mean power-law decay. We find that the early variations (less than or similar to8 days after the burst) are asymmetric, with a steep rise followed by a relatively slower ( by a factor of about 2) decline. The variations maintain a similar timescale during the first 4 days and then get significantly longer. The structure of these variations is similar to those previously detected in the afterglows of several GRBs. C1 Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. Space Sci Inst, Boulder, CO 80303 USA. RP Lipkin, YM (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. EM yiftah@wise.tau.ac.il; eran@wise.tau.ac.il; avishay@wise.tau.ac.il OI Schmidt, Brian/0000-0001-6589-1287; Schmidt, Brian/0000-0002-8538-9195 NR 80 TC 115 Z9 117 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2004 VL 606 IS 1 BP 381 EP 394 DI 10.1086/383000 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SC UT WOS:000220925800032 ER PT J AU Wolk, SJ Harnden, FR Murray, SS Adams, NR Damiani, F Flaccomio, E Micela, G Sciortino, S Jeffries, RD AF Wolk, SJ Harnden, FR Murray, SS Adams, NR Damiani, F Flaccomio, E Micela, G Sciortino, S Jeffries, RD TI Coronal variability in the young cluster NGC 2516 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 2516); stars : coronae; X-rays : stars ID ORION NEBULA CLUSTER; X-RAY VARIABILITY; MAIN-SEQUENCE STARS; CHANDRA; STELLAR; PLEIADES; IC-348; PHOTOMETRY; OBJECTS; FLARES AB NGC 2516 has been observed by Chandra several times in order to correct the plate scale of the spacecraft's focal plane instruments. Because of this, Chandra has observed NGC 2516 with all four imaging arrangements available. In addition, NGC 2516 has been observed as part of the High Resolution Camera (HRC) guaranteed time program and is scheduled for return plate scale calibration visits. This makes it the best cluster to study for long-term variability. NGC 2516 is about 140 Myr old and less than 400 pc away. In our first paper, we discussed the detection of 150 X-ray sources (42% of which are identified as cluster members) in the calibration data taken during the orbital activation phase of the Chandra mission. In our second paper, we combined all the extant data sets and detected 284 sources, more than half of which are considered likely cluster members. In this our third paper, we further explore techniques of combining Advanced CCD Imaging Spectrometer (ACIS) and HRC Chandra data for timing analysis. We have been able to combine almost 70 ks of observation time, spread over five epochs, to study variability in this cluster on multiple timescales. We find that while stochastic variability rates are about the same for all objects in the sample, the timescale for detecting variability is shorter for late-type stars. Both stochastic and flare variability rates seen in NGC 2516 are similar to those seen in younger clusters IC 348, NGC 1333, and M42. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. Univ Keele, Dept Phys, Keele ST5 5BG, Staffs, England. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Flaccomio, Ettore/0000-0002-3638-5788; Micela, Giuseppina/0000-0002-9900-4751; Wolk, Scott/0000-0002-0826-9261; Damiani, Francesco/0000-0002-7065-3061 NR 27 TC 10 Z9 10 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2004 VL 606 IS 1 BP 466 EP 482 DI 10.1086/382745 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SC UT WOS:000220925800040 ER PT J AU Wijnands, R Homan, J Miller, JM Lewin, WHG AF Wijnands, R Homan, J Miller, JM Lewin, WHG TI Monitoring Chandra observations of the quasi-persistent neutron star X-ray transient MXB 1659-29 in quiescence: The cooling curve of the heated neutron star crust SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (MXB 1659-29); stars : neutron; X-rays : stars ID BURST SOURCE MXB-1659-29; KS-1731-260; EMISSION; X-1 AB We have observed the quasi-persistent neutron star X-ray transient and eclipsing binary MXB 1659 - 29 in quiescence on three occasions with Chandra. The purpose of our observations was to monitor the quiescent behavior of the source after its last prolonged (similar to 2.5 yr) outburst that ended in 2001 September. The X-ray spectra of the source are consistent with thermal radiation from the neutron star surface. We found that the bolometric flux of the source decreased by a factor of 7 - 9 over the timespan of 1.5 yr between our first and last Chandra observations. The effective temperature also decreased, by a factor of 1.6 - 1.7. The decrease in time of the bolometric flux and effective temperature can be described using exponential decay functions, with e-folding times of similar to0.7 and similar to3 yr, respectively. Our results are consistent with the hypothesis that we observed a cooling neutron star crust that was heated considerably during the prolonged accretion event and that is still out of thermal equilibrium with the neutron star core. We could only determine upper limits for any luminosity contribution because of the thermal state of the neutron star core. The rapid cooling of the neutron star crust implies that it has a large thermal conductivity. Our results also suggest that enhanced cooling processes are present in the neutron star core. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. RP Wijnands, R (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM radw@st-andrews.ac.uk; jeroen@space.mit.edu; jmmiller@head.cfa.harvard.edu; lewin@space.mit.edu NR 22 TC 48 Z9 48 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2004 VL 606 IS 1 BP L61 EP L64 DI 10.1086/421081 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SD UT WOS:000220925900016 ER PT J AU Park, YS Lee, CW Myers, PC AF Park, YS Lee, CW Myers, PC TI A CO survey toward starless cores SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : clouds; ISM : molecules; radiative transfer; radio lines : ISM; surveys ID SUBMILLIMETER CONTINUUM OBSERVATIONS; PRE-PROTOSTELLAR CORES; DENSE CORES; DARK CLOUDS; INFALL MOTIONS; MOLECULAR LINE; CS 2-1; EXCITATION; (CO)-C-13; PROFILES AB A CO survey is undertaken toward about 80% of the starless cores in the Lee & Myers catalog that can be observed in the northern hemisphere to investigate their general observational properties such as line width and intensity, from which one can deduce their environmental physical conditions. The peak (CO)-C-12 intensity implies a kinetic temperature close to 10 K, as is already known, but for some of the cores the kinetic temperature is much higher than 10 K, suggesting either that they are not really starless or that they are externally heated. We derive the ratios of peak intensities and line widths for the pairs of (CO)-C-12 and (CO)-C-13 lines and find a value of similar to1.7 for both. The linear correlations between them are most likely to be due to clumpy structure. These data are also compared with data sets of CS 2 - 1 and N2H+ 1 - 0 lines tracing high-density regions. It is found that the peak intensity and line width of (CO)-C-13 are roughly correlated with those of CS, suggesting that the outer envelope is kinematically related to the inner dense core. Confirming that the (CO)-C-12 lines seldom exhibit deep self-reversal features, whereas this is not unusual for the CS lines, we propose a heuristic model where the outer part is clumpy, but the inner part has a rather smooth density profile, with a uniform temperature and mean density decreasing outward. We apply three-dimensional radiative transfer calculations to this simple model, demonstrating that the essential observational features of the starless cores are successfully reproduced. C1 Seoul Natl Univ, SEES, Astron Program, Seoul 151747, South Korea. Korea Astron Observ, Taejon 305348, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Park, YS (reprint author), Seoul Natl Univ, SEES, Astron Program, Seoul 151747, South Korea. EM yspark@astro.snu.ac.kr NR 32 TC 16 Z9 16 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2004 VL 152 IS 1 BP 81 EP 96 DI 10.1086/382506 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SB UT WOS:000220925700004 ER PT J AU Tolls, V Melnick, GJ Ashby, MLN Bergin, EA Gurwell, MA Kleiner, SC Patten, BM Plume, R Stauffer, JR Wang, Z Zhang, YF Chin, G Erickson, NR Snell, RL Goldsmith, PF Neufeld, DA Schieder, R Winnewisser, G AF Tolls, V Melnick, GJ Ashby, MLN Bergin, EA Gurwell, MA Kleiner, SC Patten, BM Plume, R Stauffer, JR Wang, Z Zhang, YF Chin, G Erickson, NR Snell, RL Goldsmith, PF Neufeld, DA Schieder, R Winnewisser, G TI Submillimeter Wave Astronomy Satellite performance on the ground and in orbit SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE instrumentation : detectors; instrumentation : spectrographs; radio lines : general; submillimeter; techniques : spectroscopic; telescopes ID WATER-VAPOR; SPECTROMETER AB The Submillimeter Wave Astronomy Satellite (SWAS), which was launched in 1998 December, is a NASA mission dedicated to the study of interstellar chemistry and star formation. SWAS is conducting pointed observations of molecular clouds throughout our Galaxy in either the ground state or a low-lying transition of five astrophysically important species: O-2, C I, H-2 O-18, (CO)-C-13, and H-2 O-16 at approximately 487, 492, 548, 551, and 557 GHz, respectively. The SWAS instrument is comprised of a 54 cm x 68 cm off-axis Cassegrain telescope feeding two independent heterodyne receivers with Schottky barrier diode mixers, passively cooled to about 175 K. An Acousto-Optical Spectrometer (AOS) provides similar to 1 MHz (0.6 km s(-1)) frequency resolution and 1400 MHz (840 km s(-1)) total bandwidth with 350MHz (210 km s(-1)) per line for spectral analysis. SWAS was fully characterized during ground-based testing, and all performance parameters were verified on-orbit. During its on-orbit operation, SWAS observed more than 200 astronomical objects with more than 5000 lines of sight. This paper describes the tests conducted and compares the ground-based test results with the on-orbit test results. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Tolls, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vtolls@cfa.harvard.edu RI Chin, Gordon/E-1520-2012; Goldsmith, Paul/H-3159-2016 NR 19 TC 15 Z9 16 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2004 VL 152 IS 1 BP 137 EP 162 DI 10.1086/382507 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 813SB UT WOS:000220925700009 ER PT J AU Haight, RG Cypher, B Kelly, PA Phillips, S Ralls, K Possingham, HP AF Haight, RG Cypher, B Kelly, PA Phillips, S Ralls, K Possingham, HP TI Optimizing reserve expansion for disjunct populations of San Joaquin kit fox SO BIOLOGICAL CONSERVATION LA English DT Article DE endangered species; habitat protection; kit fox; reserve design; San Joaquin Valley ID NORTHERN SPOTTED OWL; BIOGEOGRAPHIC THEORY; DEMOGRAPHIC-MODELS; OPTIMIZATION; CONSERVATION; HABITAT; DESIGN; SELECTION; BIODIVERSITY; MANAGEMENT AB Expanding habitat protection is a common strategy for species conservation. We present a model to optimize the expansion of reserves for disjunct populations of all endangered species. The objective is to maximize the expected number of surviving populations subject to budget and habitat constraints. The model accounts for benefits of reserve expansion in teens of likelihood of persistence of each population and monetary cost. Solving the model with incrementally higher budgets helps prioritize sites for expansion and produces a cost curve showing funds required for incremental increases in the objective. We applied the model to the problem of allocating funds among eight reserves for the endangered San Joaquin kit fox ( Vulpes macrotis mutica) in California, USA. The priorities for reserve expansion were related to land cost and amount of already-protected habitat at each site. Western Kern and Ciervo-Panoche sites received highest priority because land costs were low and moderate amounts of already-protected habitat resulted in large reductions in extinction risk for small increments of habitat protection. The sensitivity analysis focused oil the impacts of kit fox reproductive success and home range ill non-native grassland sites. If grassland habitat is lower quality than brushland habitat resulting in higher annual variation in reproductive success or larger home ranges, then protecting habitat at the best grassland site (Ciervo-Panoche) is not cost-efficient relative to shrubland sites (Western Kern, Antelope Plain, Carrizo Plain). Finally, results suggested that lowest priority should be given to three relatively high-cost grassland sites (Camp Roberts, Contra Costa, and Western Madera) because protecting habitat at those sites would be expensive and have little effect oil the expected number of surviving kit fox populations. Published by Elsevier Ltd. C1 US Forest Serv, USDA, N Cent Res Stn, St Paul, MN 55108 USA. Calif State Univ Stanislaus, Endangered Species Recovery Program, Fresno, CA 93727 USA. Univ Queensland, Dept Zool, St Lucia, Qld 4072, Australia. Univ Queensland, Dept Math, St Lucia, Qld 4072, Australia. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. RP Haight, RG (reprint author), US Forest Serv, USDA, N Cent Res Stn, 1992 Folwell Ave, St Paul, MN 55108 USA. EM rhaight@fs.fed.us RI Possingham, Hugh/B-1337-2008 OI Possingham, Hugh/0000-0001-7755-996X NR 39 TC 26 Z9 26 U1 3 U2 18 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD MAY PY 2004 VL 117 IS 1 BP 61 EP 72 DI 10.1016/S0006-3207(03)00263-5 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 804CH UT WOS:000220276300008 ER PT J AU Harris, JS AF Harris, JS TI Use of collections can be broadened SO BIOSCIENCE LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Harris, JS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 MAY PY 2004 VL 54 IS 5 BP 380 EP 380 PG 1 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 820TJ UT WOS:000221411900003 ER PT J AU Marra, PP Griffing, S Caffrey, C Kilpatrick, AM McLean, R Brand, C Saito, E Dupuis, AP Kramer, L Novak, R AF Marra, PP Griffing, S Caffrey, C Kilpatrick, AM McLean, R Brand, C Saito, E Dupuis, AP Kramer, L Novak, R TI West Nile virus and wildlife SO BIOSCIENCE LA English DT Article DE West Nile virus; disease ecology; birds; mosquitoes; pest management ID NEW-YORK-CITY; EQUINE ENCEPHALOMYELITIS VIRUS; VECTOR COMPETENCE; EXPERIMENTAL-INFECTION; MOSQUITOS DIPTERA; CULEX MOSQUITOS; BIRDS; TRANSMISSION; CULICIDAE; IDENTIFICATION AB West Nile virus (WNV) has spread rapidly across North America, resulting in human deaths and in the deaths of untold numbers of birds, mammals, and reptiles. The virus has reached Central America and the Caribbean and may spread to Hawaii and South America. Although tens of thousands of birds have died, and studies of some bird species show local declines, few regionwide declines can be attributed to WNV Predicting future impacts of WNV on wildlife, and pinpointing what drives epidemics, will require substantial additional research into host susceptibility, reservoir competency, and linkages between climate, mosquitoes, and disease. Such work will entail a collaborative effort between scientists in governmental research groups, in surveillance and control programs, and in nongovernmental organizations. West Nile virus was not the first, and it will not be the lost, exotic disease to be introduced to the New World. Its spread in North America highlights the need to strengthen animal monitoring programs and to integrate them with research on disease ecology. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Audubon Sci, Warminster, PA 18974 USA. Consortium Conservat Med, Palisades, NY 10964 USA. US Anim & Plant Hlth Inspect Serv, Natl Wildlife Res Ctr, USDA, Ft Collins, CO 80521 USA. US Geol Survey, Natl Wildlife Hlth Ctr, Madison, WI 53711 USA. New York State Dept Hlth, Wadsworth Ctr, Arbovirus Labs, Griffin Lab, Slingerlands, NY 12159 USA. Illinois Nat Hist Survey, Champaign, IL 61820 USA. RP Marra, PP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM marrap@si.edu NR 68 TC 115 Z9 121 U1 4 U2 26 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 MAY PY 2004 VL 54 IS 5 BP 393 EP 402 DI 10.1641/0006-3568(2004)054[0393:WNVAW]2.0.CO;2 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 820TJ UT WOS:000221411900008 ER PT J AU Ralls, K Ballou, JD AF Ralls, K Ballou, JD TI Genetic status and management of California Condors SO CONDOR LA English DT Article DE California Condor; captive breeding; genetic management; Gymnogyps californianus; reintroduction ID POPULATIONS; VARIABILITY; EXTINCTION; SIMULATION; PEDIGREES; ALLELES; DNA AB The last wild California Condor (Gymnogyps californianus) was brought into captivity in 1987. Captive breeding was successful and reintroduction efforts began in 1992. The current population is descended from 14 individuals belonging to three genetic "clans." This population bottleneck led to the loss of genetic variation and changes in allele frequencies, including a probable increase in the frequency of the putative allele for chondrodystrophy, a lethal form of dwarfism. We use studbook data to analyze the current genetic and demographic status of the population and explain how it is managed to meet specific goals. In August 2002 the population consisted of 206 individuals distributed among three captive-breeding facilities and three reintroduction sites. The population is managed to preserve genetic diversity using the concept of mean kinship. Growth of the total population has been between 10% and 15% per year since 1987, but the growth of the captive population has been only about 5% per year since 1992 due to the removal of chicks for reintroduction. Assuming that founding birds within clans were half-siblings, the birds used to found the captive population theoretically contained 92% of the heterozygosity present in the hypothetical wild base population. About 99.5% of this heterozygosity has been retained in the current population. Alleles from most founders are well represented across captive-breeding facilities and reintroduction sites. The genetic status of this population compares favorably with other species that have been rescued from extinction by captive breeding. C1 Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Conservat & Res Ctr, Washington, DC 20008 USA. RP Ralls, K (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Conservat & Res Ctr, Washington, DC 20008 USA. EM rallsk@thegrid.net NR 44 TC 50 Z9 53 U1 16 U2 82 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD MAY PY 2004 VL 106 IS 2 BP 215 EP 228 DI 10.1650/7348 PG 14 WC Ornithology SC Zoology GA 818SE UT WOS:000221264000001 ER PT J AU Verbruggen, H Kooistra, WHCF AF Verbruggen, H Kooistra, WHCF TI Morphological characterization of lineages within the calcified tropical seaweed genus Halimeda (Bryopsidales, Chlorophyta) SO EUROPEAN JOURNAL OF PHYCOLOGY LA English DT Article DE Halimeda; morphology; sections; phylogeny; SSU rDNA; taxonomy ID GREAT-BARRIER-REEF; CORAL-REEFS; GREEN-ALGAE; CAULERPALES; REPRODUCTION; PHYLOGENIES; FRAGMENTS; ECOLOGY AB Halimeda Lamouroux constitutes a genus of calcified and segmented green seaweeds within the Bryopsidales. Molecular phylogenetic assessments have uncovered five principal monophyletic lineages within the genus. In the present study we define these lineages morphologically. We gathered morphological data from specimens used in the molecular analyses as well as from collections having a similar morphology and originating from the same geographical region. Starting from the lineages and their morphological synapomorphies, we define and illustrate five natural sections within Halimeda. All or most medullary siphons traversing the nodes between segments fuse into a single unit in specimens of lineage 1 (section Rhipsalis), and segments at the thallus base fuse with one another. Medullary siphons of specimens in lineage 2 (section Micronesicae) traverse the node without fusing. Medullary siphons of specimens in lineage 3 (section Halimeda) divide frequently below the nodes and become entangled among one another. The segments of specimens in this lineage possess a continuous uncorticated band along the distal perimeter instead of three or more pits as encountered in segments of specimens in all other lineages. Members of lineage 4 (section Pseudo-opuntia) possess club-shaped subperipheral utricles in their cortical region. Medullary siphons of specimens in lineage 5 (section Opuntia) fuse over only a short distance at the nodes and retain their identity. Apart from these synapomorphies, the lineages can be delimited further by a characteristic combination of symplesiomorphies and homoplasies. In addition we examined the morphology of H. bikinensis Taylor, a species not included in the molecular analyses, and discuss its ambiguous position in our sectional system. C1 State Univ Ghent, Phycol Res Grp, B-9000 Ghent, Belgium. Smithsonian Trop Res Inst, Balboa, Panama. RP Kooistra, WHCF (reprint author), State Univ Ghent, Phycol Res Grp, Krijgslaan 281-S8, B-9000 Ghent, Belgium. EM kooistra@szn.it RI Verbruggen, Heroen/C-6951-2009; OI Verbruggen, Heroen/0000-0002-6305-4749; Kooistra, Wiebe/0000-0002-8641-9739 NR 41 TC 30 Z9 30 U1 0 U2 5 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0967-0262 J9 EUR J PHYCOL JI Eur. J. Phycol. PD MAY PY 2004 VL 39 IS 2 BP 213 EP 228 DI 10.1080/026042000202163 PG 16 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 825MN UT WOS:000221762700010 ER PT J AU Froelich, P Zygelman, B Saenz, A Jonsell, S Eriksson, S Dalgarno, A AF Froelich, P Zygelman, B Saenz, A Jonsell, S Eriksson, S Dalgarno, A TI Hydrogen-antihydrogen molecule and its properties SO FEW-BODY SYSTEMS LA English DT Article; Proceedings Paper CT 3rd International Workshop on Dynamics and Structure of Critically Stable Quantum Few-Body Systems CY SEP 01-05, 2003 CL Trento, ITALY ID QUANTUM MONTE-CARLO; STABILITY; SYSTEMS; TEMPERATURES; COLLISIONS AB The metastability of the four-body system is discussed from the point of view of radiative rearrangement collisions of the hydrogen and antihydrogen. Such collisions lead to the formation of an intermediate molecular state which further decays into positronium and protonium or is destroyed via annihilation. We present calculations of the lifetime of the system and the branching ratios for Coulombic decay and annihilation. C1 Uppsala Univ, Dept Quantum Chem, SE-75120 Uppsala, Sweden. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Humboldt Univ, Inst Phys, D-10117 Berlin, Germany. Umea Univ, SE-90187 Umea, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Froelich, P (reprint author), Uppsala Univ, Dept Quantum Chem, Box 518, SE-75120 Uppsala, Sweden. EM piotr.froelich@kvac.uu.se RI Jonsell, Svante/J-2251-2016 OI Jonsell, Svante/0000-0003-4969-1714 NR 17 TC 8 Z9 8 U1 0 U2 5 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0177-7963 EI 1432-5411 J9 FEW-BODY SYST JI Few-Body Syst. PD MAY PY 2004 VL 34 IS 1-3 BP 63 EP 72 DI 10.1007/s00601-004-0053-3 PG 10 WC Physics, Multidisciplinary SC Physics GA 828YK UT WOS:000222009500012 ER PT J AU Davis, JLD Young-Williams, AC Hines, AH Zmora, O AF Davis, JLD Young-Williams, AC Hines, AH Zmora, O TI Comparing two types of internal tags in juvenile blue crabs SO FISHERIES RESEARCH LA English DT Article DE coded wire tag; visual implant elastomer; VIE; mark-recapture; blue crab; Callinectes sapidus ID CODED WIRE TAGS; CALLINECTES-SAPIDUS RATHBUN; MICROWIRE TAGS; ELASTOMER; RETENTION; SURVIVAL; GROWTH; MARKING; CRAYFISH; FISH AB Although methods to tag fish and other vertebrates have been well described, tagging crustaceans, which molt, poses a greater challenge. Tagging very small juveniles, often necessary in population recruitment or stock enhancement studies, presents an ever greater challenge. We compared the success of two tagging techniques in very small (<25 mm carapace, width) juvenile blue crabs (Callinectes sapidus): (1) microwire (also known as coded wire tags) and (2) elastomer (also known as visual implant flourescent elastomer (VIFE) tags). Although growth and long-term mortality did not differ between tagging methods. each method had certain advantages. Crabs tagged with elastomer had lower immediate mortality as a result of the tagging process. Tag retention, short- and long-term and as well as field and laboratory, was higher for microwire than elastomer. Moreover, the micowire tagging process is about 70% faster. As a result of the higher tag retention and faster rate of microwire tagging, this method is recommended for very small juvenile blue crabs and other crustaceans. However, success is likely size-dependent, as better sites of elastomer application are accessible in larger blue crabs and probably other crustaceans as well. Due to its survivorship advantages and relative inexpense, elastomer tagging should not yet be ruled out for larger crustaceans or short-term studies of juveniles. (C) 2004 Elsevier B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgwater, MD 20137 USA. Univ Maryland, Inst Biotechnol, Ctr Marine Biotechnol, Baltimore, MD 21202 USA. RP Davis, JLD (reprint author), Williams Coll Mystic Seaport, Maritime Studies Program, Mystic, CT 06355 USA. EM janalddavis@yahoo.com; younga@si.edu; hinesa@si.edu; zmorao@umbi.umd.edu NR 32 TC 34 Z9 36 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 J9 FISH RES JI Fish Res. PD MAY PY 2004 VL 67 IS 3 BP 265 EP 274 DI 10.1016/j.fishres.2003.11.005 PG 10 WC Fisheries SC Fisheries GA 815GT UT WOS:000221031500002 ER PT J AU Brown, JL Walker, SL Moeller, T AF Brown, JL Walker, SL Moeller, T TI Comparative endocrinology of cycling and non-cycling Asian (Elephas maximus) and African (Loxodonta africana) elephants SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE ultrasound; ovarian cyclicity; reproductive dysfunction; hormones; progestins ID OVARIAN FOLLICULAR CYSTS; GONADOTROPIN-RELEASING HORMONE; DAIRY-COWS; LUTEINIZING-HORMONE; SERUM PROLACTIN; ESTROUS-CYCLE; SECRETION; LH; HYPERPROLACTINEMIA; PROGESTERONE AB Up to 14% of Asian and 29% of African elephants in captivity are not cycling normally or exhibit irregular cycles based on progestin profiles. To determine if ovarian acyclicity is related to other disruptions in endocrine activity, serum pituitary, thyroid, adrenal, and ovarian hormones in weekly samples collected for 6-25 months were compared between normal cycling (n = 22 each species) and non-cycling (n 6 Asian; n = 30 African) elephants. A subset of cycling females (n = 4 Asian, 7 African) also were blood sampled daily during the follicular phase to characterize the peri-ovulatory period. In normal cycling females, two leutinizing hormone (LH) surges were observed 3 weeks apart during a normal follicular phase, with the second inducing ovulation (ovLH). Serum FSH concentrations were highest at the beginning of the non-luteal phase, declining to nadir concentrations within 4 days of the ovLH surge. FSH remained low until after the ovLH surge and then increased during the luteal phase. A species difference was noted in prolactin secretion. In the African elephant, prolactin was increased during the follicular phase, but in Asian elephants concentrations remained stable throughout the cycle. Patterns of thyroid hormones (thyroid-stimulating hormone, TSH; free and total thyroxine, T4; free and total triiodothyronine, T3) and cortisol secretion were not affected by estrous cycle stage or season in cycling elephants. In non-cycling elephants, there were no fluctuating patterns of LH, FSH, or prolactin secretion. Overall mean concentrations of all hormones were similar to those in cycling animals, with the exception of FSH, prolactin, and estradiol. Mean serum FSH concentrations were lower due to females not exhibiting normal cyclic increases, whereas serum estradiol was higher overall in most acyclic females. Prolactin concentrations were significantly increased in 11 of 30 non-cycling females, all of which were African elephants. In sum, while there were no consistent endocrine anomalies associated with ovarian acyclicity, hyperpro-lactinemia may be one cause of ovarian dysfunction. The finding of elevated estrogens in some acyclic females also deserves further investigation, especially determining how it relates to reproductive tract pathologies. (C) 2004 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, Dept Reprod Sci, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Brown, JL (reprint author), Smithsonian Inst, Dept Reprod Sci, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. EM jbrown@crc.si.edu NR 49 TC 49 Z9 49 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD MAY 1 PY 2004 VL 136 IS 3 BP 360 EP 370 DI 10.1016/j.ygcen.2004.01.013 PG 11 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 817MR UT WOS:000221182100007 PM 15081836 ER PT J AU Krot, AN Fagan, TJ Keil, K McKeegan, KD Sahijpal, S Hutcheon, ID Petaev, MI Yurimoto, H AF Krot, AN Fagan, TJ Keil, K McKeegan, KD Sahijpal, S Hutcheon, ID Petaev, MI Yurimoto, H TI Ca,Al-rich inclusions, amoeboid olivine aggregates, and Al-rich chondrules from the unique carbonaceous chondrite Acfer 094: I. Mineralogy and petrology SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID REFRACTORY INCLUSIONS; FERROMAGNESIAN CHONDRULES; CV3 CHONDRITES; SOLAR NEBULA; ISOTOPIC COMPOSITIONS; MURCHISON METEORITE; ALLENDE METEORITE; GENETIC LINK; CALCIUM; CONDENSATION AB Based on their mineralogy and petrography, similar to200 refractory inclusions studied in the unique carbonaceous chondrite, Acfer 094, can be divided into corundum-rich (0.5%), hibonite-rich (1.1%), grossite-rich (8.5%), compact and fluffy Type A (spinel-melilite-rich, 50.3%), pyroxene-anorthite-rich (7.4%), and Type C (pyroxeneanorthite-rich with igneous textures, 1.6%) Ca,Al-rich inclusions (CAIs), pyroxene-hibonite spherules (0.5%), and amoeboid olivine aggregates (AOAs, 30.2%). Melilite in some CAIs is replaced by spinel and Al-diopside and/or by anorthite. whereas spinel-pyroxene assemblages in CAIs and AOAs appear to be replaced by anorthite. Forsterite grains in several AOAs are replaced by low-Ca pyroxene. None of the CAN or AOAs show evidence for Fe-alkali metasomatic or aqueous alteration. The mineralogy, textures, and bulk chemistry of most Acfer 094 refractory inclusions are consistent with their origin by gas-solid condensation and may reflect continuous interaction with SiO and Mg of the cooling nebula gas. It appears that only a few CAls experienced subsequent melting. The Al-rich chondrules (ARCs; > 10 wt% bulk Al2O3) consist of forsteritic olivine and low-Ca pyroxene phenocrysts, pigeonite, augite, anorthitic plagioclase, +/- spinel, FeNi-metal, and crystalline mesostasis composed of plagioclase, augite and a silica phase. Most ARCs are spherical and mineralogically uniform, but some are irregular in shape and heterogeneous in mineralogy, with distinct ferromagnesian and aluminous domains. The ferromagnesian domains tend to form chondrule mantles, and are dominated by low-Ca pyroxene and forsteritic olivine, anorthitic mesostasis, and Fe,Ni-metal nodules. The aluminous domains are dominated by anorthite, high-Ca pyroxene and spinel, occasionally with inclusions of perovskite; have no or little FeNi-metal; and tend to form cores of the heterogeneous chondrules. The cores are enriched in bulk Ca and Al, and apparently formed from melting of CAI-like precursor material that did not mix completely with adjacent ferromagnesian melt. The inferred presence of CAI-like material among precursors for Al-rich chondrules is in apparent conflict with lack of evidence for melting of CAIs that occur outside chondrules, suggesting that these CAIs were largely absent from chondrule-forming region(s) at the time of chondrule formation. This may imply that there are several populations of CAIs in Acfer 094 and that mixing of "normal" CAIs that Occur outside chondrules and chondrules that accreted into the Acfer 094 parent asteroid took place after chondrule formation. Alternatively, there may have been an overlap in the CAI- and chondrule-forming regions, where the least refractory CAIs were mixed with Fe-Mg chondrule precursors. This hypothesis is difficult to reconcile with the lack of evidence of melting of AOAs which represent aggregates of the least refractory CAIs and forstefite grains. Copyright (C) 2004 Lsevier Ltd. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Inst Geophys & Planetary, Honolulu, HI 96822 USA. Tokyo Inst Technol, Tokyo 1528551, Japan. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. Punjabi Univ, Dept Phys, Chandigarh 160014, India. Lawrence Livermore Natl Lab, Livermore, CA 94451 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Krot, AN (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Inst Geophys & Planetary, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu RI McKeegan, Kevin/A-4107-2008 OI McKeegan, Kevin/0000-0002-1827-729X NR 57 TC 50 Z9 54 U1 4 U2 11 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 MAY PY 2004 VL 68 IS 9 BP 2167 EP 2184 DI 10.1016/j.gca.2003.10.025 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 815GZ UT WOS:000221032100023 ER PT J AU Teller, JT Leverington, DW AF Teller, JT Leverington, DW TI Glacial Lake Agassiz: A 5000 yr history of change and its relationship to the delta O-18 record of Greenland SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article DE Lake Agassiz; history; out-bursts; Greenland isotopic record ID LAURENTIDE ICE-SHEET; ABRUPT CLIMATE-CHANGE; FRESH-WATER INPUT; C-14 YR BP; COLD EVENT; NORTH-ATLANTIC; YOUNGER DRYAS; LAST DEGLACIATION; HOLOCENE CLIMATE; AGE CALIBRATION AB Lake Agassiz was the largest lake in North America during the last period of deglaciation; the lake extended over a total of 1.5 x 10(6) km(2) before it drained at ca. 7.7 C-14 ka (8.4 cal. [calendar] ka). New computer reconstructions-controlled by beaches, isostatic rebound data, the margin of the Laurentide Ice Sheet, outlet elevations, and a digital elevation model (DEM) of modern topographic data-show how variable the size and depth of this lake were during its 4000 C-14 yr (5000 cal. yr) history. Abrupt reductions in lake level, ranging from 8 to 110 m, occurred on at least 18 occasions when new outlets were opened, reducing the extent of the lake and sending large outbursts of water to the oceans. Three of the largest outbursts correlate closely in time with the start of large delta(18)O excursions in the isotopic records of the Greenland ice cap, suggesting that those freshwaters may have had an impact on thermohaline circulation and, in turn, on climate. C1 Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. Smithsonian Inst, Ctr Earth & Planetary Sci, Natl Air & Space Museum, Washington, DC 20560 USA. RP Teller, JT (reprint author), Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. EM tellerjt@ms.umanitoba.ca; leveringtond@nasm.si.edu NR 87 TC 100 Z9 101 U1 6 U2 29 PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER PI DENVER PA 720 S COLORADO BLVD, STE 960-S, DENVER, CO 80246 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAY-JUN PY 2004 VL 116 IS 5-6 BP 729 EP 742 DI 10.1130/B25316.1 PG 14 WC Geosciences, Multidisciplinary SC Geology GA 815MH UT WOS:000221045900015 ER PT J AU Baker, TR Phillips, OL Malhi, Y Almeida, S Arroyo, L Di Fiore, A Erwin, T Killeen, TJ Laurance, SG Laurance, WF Lewis, SL Lloyd, J Monteagudo, A Neill, DA Patino, S Pitman, NCA Silva, JNM Martinez, RV AF Baker, TR Phillips, OL Malhi, Y Almeida, S Arroyo, L Di Fiore, A Erwin, T Killeen, TJ Laurance, SG Laurance, WF Lewis, SL Lloyd, J Monteagudo, A Neill, DA Patino, S Pitman, NCA Silva, JNM Martinez, RV TI Variation in wood density determines spatial patterns in Amazonian forest biomass SO GLOBAL CHANGE BIOLOGY LA English DT Article DE AGB; Amazonia; carbon; permanent plot; tropical forests; wood specific gravity ID TROPICAL RAIN-FOREST; NET PRIMARY PRODUCTION; BRAZILIAN AMAZONIA; ABOVEGROUND BIOMASS; LANDSCAPE-SCALE; DIVERSITY; TREE; DYNAMICS; GUIANA; DEFORESTATION AB Uncertainty in biomass estimates is one of the greatest limitations to models of carbon flux in tropical forests. Previous comparisons of field-based estimates of the aboveground biomass (AGB) of trees greater than 10 cm diameter within Amazonia have been limited by the paucity of data for western Amazon forests, and the use of site-specific methods to estimate biomass from inventory data. In addition, the role of regional variation in stand-level wood specific gravity has not previously been considered. Using data from 56 mature forest plots across Amazonia, we consider the relative roles of species composition (wood specific gravity) and forest structure (basal area) in determining variation in AGB. Mean stand-level wood specific gravity, on a per stem basis, is 15.8% higher in forests in central and eastern, compared with northwestern Amazonia. This pattern is due to the higher diversity and abundance of taxa with high specific gravity values in central and eastern Amazonia, and the greater diversity and abundance of taxa with low specific gravity values in western Amazonia. For two estimates of AGB derived using different allometric equations, basal area explains 51.7% and 63.4%, and stand-level specific gravity 45.4% and 29.7%, of the total variation in AGB. The variation in specific gravity is important because it determines the regional scale, spatial pattern of AGB. When weighting by specific gravity is included, central and eastern Amazon forests have significantly higher AGB than stands in northwest or southwest Amazonia. The regional-scale pattern of species composition therefore defines a broad gradient of AGB across Amazonia. C1 Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. Max Planck Inst Biogeochem, Jena, Germany. Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. Museu Paraense Emilio Goeldi, Belem, Para, Brazil. Museo Noel Kempff Mercado, Santa Cruz, Bolivia. NYU, Dept Anthropol, New York, NY 10003 USA. Smithsonian Inst, Washington, DC 20560 USA. Conservat Int, Ctr Appl Biodivers Sci, Washington, DC USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Nacl San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. Herbario Nacl Ecuador, Missouri Bot Gardens, Quito, Ecuador. Alexander Von Humboldt Biol Res Inst, Bogota, Colombia. Duke Univ, Ctr Trop Conservat, Durham, NC 27706 USA. CIFOR, Tapajos, Brazil. EMBRAPA Amazonia Oriental, Belem, Para, Brazil. Jardin Bot Missouri, Proyecto Flora Peru, Oxapampa, Peru. RP Baker, TR (reprint author), Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. EM t.baker@geog.leeds.ac.uk RI Pitman, Nigel/A-7681-2008; Lloyd, Jonathan/F-8893-2010; Mercado, Lina /A-1890-2012; Laurance, William/B-2709-2012; Phillips, Oliver/A-1523-2011; Laurance, Susan/G-6021-2011; OI Pitman, Nigel/0000-0002-9211-2880; Lloyd, Jonathan/0000-0002-5458-9960; Phillips, Oliver/0000-0002-8993-6168; Laurance, Susan/0000-0002-2831-2933; Lewis, Simon/0000-0002-8066-6851 NR 56 TC 322 Z9 342 U1 9 U2 106 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAY PY 2004 VL 10 IS 5 BP 545 EP 562 DI 10.1111/j.1529-8817.2003.00751.x PG 18 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 820WY UT WOS:000221421600003 ER PT J AU Malhi, Y Baker, TR Phillips, OL Almeida, S Alvarez, E Arroyo, L Chave, J Czimczik, CI Di Fiore, A Higuchi, N Killeen, TJ Laurance, SG Laurance, WF Lewis, SL Montoya, LMM Monteagudo, A Neill, DA Vargas, PN Patino, S Pitman, NCA Quesada, CA Salomao, R Silva, JNM Lezama, AT Martinez, RV Terborgh, J Vinceti, B Lloyd, J AF Malhi, Y Baker, TR Phillips, OL Almeida, S Alvarez, E Arroyo, L Chave, J Czimczik, CI Di Fiore, A Higuchi, N Killeen, TJ Laurance, SG Laurance, WF Lewis, SL Montoya, LMM Monteagudo, A Neill, DA Vargas, PN Patino, S Pitman, NCA Quesada, CA Salomao, R Silva, JNM Lezama, AT Martinez, RV Terborgh, J Vinceti, B Lloyd, J TI The above-ground coarse wood productivity of 104 Neotropical forest plots SO GLOBAL CHANGE BIOLOGY LA English DT Article DE Amazonia; carbon; coarse wood productivity; GPP; growth; NPP; soil fertility; tropical forests ID NET PRIMARY PRODUCTION; FLOOD-PLAIN FORESTS; TROPICAL FORESTS; AMAZONIAN FOREST; RAIN-FOREST; PERUVIAN AMAZON; CARBON SINK; DYNAMICS; GROWTH; VARIABILITY AB The net primary production of tropical forests and its partitioning between long-lived carbon pools (wood) and shorter-lived pools (leaves, fine roots) are of considerable importance in the global carbon cycle. However, these terms have only been studied at a handful of field sites, and with no consistent calculation methodology. Here we calculate above-ground coarse wood carbon productivity for 104 forest plots in lowland New World humid tropical forests, using a consistent calculation methodology that incorporates corrections for spatial variations in tree-size distributions and wood density, and for census interval length. Mean wood density is found to be lower in more productive forests. We estimate that above-ground coarse wood productivity varies by more than a factor of three (between 1.5 and 5.5 Mg C ha(-1) a(-1)) across the Neotropical plots, with a mean value of 3.1 Mg C ha(-1) a(-1). There appear to be no obvious relationships between wood productivity and rainfall, dry season length or sunshine, but there is some hint of increased productivity at lower temperatures. There is, however, also strong evidence for a positive relationship between wood productivity and soil fertility. Fertile soils tend to become more common towards the Andes and at slightly higher than average elevations, so the apparent temperature/productivity relationship is probably not a direct one. Coarse wood productivity accounts for only a fraction of overall tropical forest net primary productivity, but the available data indicate that it is approximately proportional to total above-ground productivity. We speculate that the large variation in wood productivity is unlikely to directly imply an equivalent variation in gross primary production. Instead a shifting balance in carbon allocation between respiration, wood carbon and fine root production seems the more likely explanation. C1 Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. Max Planck Inst Biogeochem, D-07701 Jena, Germany. Univ Leeds, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. Museu Paraense Emilio Goeldi, Belem, Para, Brazil. Interconex Elect SA ISA, Equipo Gest Ambiental, Medellin, Colombia. Museo Noel Kempff Mercado, Santa Cruz, Bolivia. CNRS UPS, Lab Evolut & Divers Biol, Toulouse, France. NYU, Dept Anthropol, New York, NY 10003 USA. Inst Natl Pesquisas Amazon, Manaus, Amazonas, Brazil. Conservat Int, Ctr Appl Biodivers Sci, Washington, DC USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Nacl San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. Jardin Bot Missouri, Proyecto Flora Peru, Oxapampa, Peru. Fdn Jatun Sacha, Quito, Ecuador. Duke Univ, Ctr Trop Conservat, Durham, NC 27706 USA. Univ Brasilia, Dept Ecol, BR-70910900 Brasilia, DF, Brazil. CIFOR, Tapajos, Brazil. EMBRAPA Amazonia Oriental, Belem, Para, Brazil. Univ Los Andes, Fac Ciencias Forestales & Ambientale, INDEFOR, Merida, Venezuela. Int Plant Genet Resources Inst, Rome, Italy. RP Malhi, Y (reprint author), Univ Edinburgh, Sch Geosci, Darwin Bldg,Mayfield Rd, Edinburgh, Midlothian, Scotland. EM ymalhi@ed.ac.uk RI Pitman, Nigel/A-7681-2008; Lloyd, Jonathan/F-8893-2010; Mercado, Lina /A-1890-2012; Laurance, William/B-2709-2012; Phillips, Oliver/A-1523-2011; Laurance, Susan/G-6021-2011; OI Pitman, Nigel/0000-0002-9211-2880; Lloyd, Jonathan/0000-0002-5458-9960; Phillips, Oliver/0000-0002-8993-6168; Laurance, Susan/0000-0002-2831-2933; Lewis, Simon/0000-0002-8066-6851 NR 47 TC 232 Z9 246 U1 3 U2 56 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAY PY 2004 VL 10 IS 5 BP 563 EP 591 DI 10.1111/j.1529-8817.2003.00778.x PG 29 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 820WY UT WOS:000221421600004 ER PT J AU Jaramillo, MA Manos, PS Zimmer, EA AF Jaramillo, MA Manos, PS Zimmer, EA TI Phylogenetic relationships of the perianthless Piperales: Reconstructing the evolution of floral development SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Piperales; flower evolution; ancestral character state reconstruction; ancestral ontogeny reconstruction; floral organ merosity; carpel evolution ID SAURURUS-CERNUUS SAURURACEAE; ANCESTRAL CHARACTER STATES; RIBOSOMAL DNA-SEQUENCES; PLASTID GENE RBCL; GYNOECIUM DIVERSITY; FLOWER DEVELOPMENT; BASAL ANGIOSPERMS; NUCLEOTIDE-SEQUENCES; DISCRETE CHARACTERS; MOLECULAR-DATA AB The perianthless members of the Piperales are unique among the basal lineages of angiosperms because they are mainly herbaceous plants with over 2000 species possessing highly reduced flowers. There have been several attempts to address the evolution of the flower morphology in the group, but no previous study has included aDNA based estimate of phylogeny. Here we present a robust reconstruction of the phylogenetic relationships of the genera in the perianthless Piperales using DNA sequence data from three genes (rbcL, atpB, and 18S) and two genomes (nuclear and chloroplast). We estimated the likelihood values of ancestral character states of mature floral structures. Developmental sequences also were analyzed using step matrices under specific models of character state change to examine the origin of meristic differences of the androecium and gynoecium. Developmental lability is the general theme in the evolution of floral merosity in the perianthless Piperales, with different developmental processes giving rise to morphologically identical mature stages. Our findings confirm this notion based on several distinct patterns: ( 1) nonidentical ontogenies give rise to homoplasious, six-staminate androecia of Saururaceae and some Piperaceae most likely through terminal addition; (2) identical ontogenies produce the homoplasious two-staminate flowers in Peperomia and Piper umbellatum through deletion; and ( 3) nearly identical ontogenies produce homplasious tricarpellate gynoecia of Piper and Anemopsis + Houttuynia clade, and the apocarpous gynoecium of Saururus may be secondarily derived, both end products occurring through deletion. We note that changes in organ number and the degree of carpel fusion have been important during the evolutionary history of the perianthless Piperales as well as the basal angiosperms in general and should be studied more extensively. Overall we emphasize the lability of developmental pathways, especially in the flower, and endorse the methodological utility of developmental sequences for directing future investigations of floral evolution. C1 Smithsonian Inst, Lab Mol Systemat, Washington, DC 20560 USA. Duke Univ, Dept Biol, Durham, NC 27708 USA. RP Jaramillo, MA (reprint author), Univ Fed Rio de Janeiro, Dept Bioquim Med, BR-21940590 Rio De Janeiro, Brazil. EM jaramillo@bioqmed.ufrj.br RI Zimmer, Elizabeth/G-3890-2011 NR 81 TC 39 Z9 42 U1 2 U2 23 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD MAY PY 2004 VL 165 IS 3 BP 403 EP 416 DI 10.1086/382803 PG 14 WC Plant Sciences SC Plant Sciences GA 832AE UT WOS:000222238300007 ER PT J AU Green, DWE AF Green, DWE TI Cometography: A catalog of comets, ii: 1800-1899. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Green, DWE (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD MAY PY 2004 VL 35 BP 238 EP 240 PN 2 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 863SF UT WOS:000224581600008 ER PT J AU Gingerich, O AF Gingerich, O TI Lost stars: Lost, missing, and troublesome starsfrom the catalogues of Johannes Bayer, Nicholas-Louis de Lacaille, John Flamsteed, and sundry others. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD MAY PY 2004 VL 35 BP 244 EP 245 PN 2 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 863SF UT WOS:000224581600011 ER PT J AU Pearson, PN Nicholas, CJ Singano, JM Bown, PR Coxall, HK van Dongen, BE Huber, BT Karega, A Lees, JA Msaky, E Pancost, RD Pearson, M Roberts, AP AF Pearson, PN Nicholas, CJ Singano, JM Bown, PR Coxall, HK van Dongen, BE Huber, BT Karega, A Lees, JA Msaky, E Pancost, RD Pearson, M Roberts, AP TI Paleogene and cretaceous sediment cores from the Kilwa and Lindi areas of coastal Tanzania: Tanzania Drilling Project Sites 1-5 SO JOURNAL OF AFRICAN EARTH SCIENCES LA English DT Article DE cretaceous; Eocene; oligocene; foraminifers; nannofossils; geochemistry; palynology; magnetostratigraphy ID UNRESOLVED COMPLEX-MIXTURES; SEA-SURFACE TEMPERATURES; MAGNETIC POLARITIES; 4-METHYL STEROLS; ROCK MAGNETISM; GREIGITE; PALEOMAGNETISM; HYDROCARBONS; SECTION; OCEAN AB Initial results of scientific drilling in southern coastal Tanzania are described. A total of five sites was drilled (mostly using continuous coring) by the Tanzania Drilling Project for paleoclimate studies. The sediments are predominantly clays and claystones deposited in a deep marine shelf environment and often contain excellently preserved microfossils suitable for geochemical analysis. The studies reported here include summaries of the lithostratigraphy, biostratigraphy (planktonic foraminifers, calcareous nannofossils, benthic foraminifers, and palynology), magneto stratigraphy, and organic geochemistry. TDP Site 1 was drilled near Kilwa Masoko airstrip (8degrees54.516'S, 39degrees30.397'E). It yielded 8.55 m of barren blue-grey clays that may be Miocene in age, followed by 1.2 m of greenish-black to dark greenish-grey clay probably of the same age. The remainder of the hole cored 62.35 m of lower Oligocene sediments (nannofossil Zone NP23), which are predominantly greenish-black to dark greenish-grey clays. Total penetration was 74.10 m. The coring represents the first report of a thick Oligocene clay formation in the area. TDP Site 2 was drilled near Kilwa Masoko prison (8degrees55.277'S, 39degrees30.219'E), It yielded 92.78 m of predominantly dark greenish-grey clay with occasional allochthonous limestone beds that consist mostly of redeposited larger foraminifers. The site encompasses lower to middle Eocene planktonic foraminifer Zones P8/9 to P11 and nannofossil Subzones NP14b to NP15c. It encompasses a rarely cored interval across the Ypresian-Lutetian transition. TDP Site 3 was drilled near Mpara in the Kilwa area (8degrees51.585'S, 39degrees27.655'E). It yielded 56.4 m of predominantly dark greenish-grey clays and claystones. The site is assigned to lower Eocene planktonic foraminifer Zone P6 and nannofossil Zone NP11. TDP Site 4 was drilled near Ras Tipuli on the northwest side of Lindi creek (9degrees56.999'S, 39degrees42.985'E). It yielded 19.8 m of predominantly dark greenish-grey clay with allochthonous limestone interbeds. The site encompasses middle Eocene planktonic foraminifer Zones P12-P14 and nannofossil Zone NP17. TDP Site 5 was drilled at Machole, near Lindi, south of Kitulo Hill (10degrees01.646'S, 39degrees41.375'E). It yielded 31.6 m of predominantly greenish-black to dark greenish-grey clay assigned to the upper Cretaceous Globotruncana falsostuarti planktonic foraminifer zone and nannofossil zones UC15e-UC17 (upper Campanian-lower Maastrichtian). Paleomagnetic analysis suggests that the site straddles two magnetic reversals, between Chrons C32r.2r and C32r.1n. Samples from TDP Sites 1-5 yielded dinocyst and miospore assemblages that are integrated with the calcareous stratigraphy. Organic geochemical analyses of samples from each of the cores revealed biomarkers of predominantly terrestrial origin and an unusually low degree of thermal maturity, suggesting shallow burial depths. X-ray diffraction studies suggest that much of the Paleogene clay may be reworked from eroded Mesozoic formations. (C) 2004 Elsevier Ltd. All rights reserved. C1 Cardiff Univ, Sch Earth Ocean & Planetary Sci, Cardiff CF10 3YE, S Glam, Wales. Trinity Coll Dublin, Dept Geol, Dublin 2, Ireland. Tanzania Petr Dev Corp, Dar Es Salaam, Tanzania. UCL, Dept Earth Sci, London WC1E 6BT, England. Univ Southampton, Sch Ocean & Earth Sci, Southampton Oceanog Ctr, Southampton SO14 3ZH, Hants, England. Univ Bristol, Sch Chem, Biogeochem Res Ctr, Organ Geochem Unit, Bristol BS8 1TS, Avon, England. Smithsonian Natl Museum Nat Hist, Dept Paleobiol, MRC, Washington, DC 20012 USA. RP Pearson, PN (reprint author), Cardiff Univ, Sch Earth Ocean & Planetary Sci, Main Bldg,Pk Pl, Cardiff CF10 3YE, S Glam, Wales. EM pearson@cardiff.ac.uk RI Pearson, Paul/B-2276-2009; Bown, Paul/C-5235-2011; Roberts, Andrew/E-6422-2010; OI Pearson, Paul/0000-0003-4628-9818; Roberts, Andrew/0000-0003-0566-8117; van Dongen, Bart/0000-0003-1189-142X; LEES, JACKIE/0000-0003-0737-8826; Bown, Paul/0000-0001-6777-4463 NR 74 TC 44 Z9 53 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1464-343X J9 J AFR EARTH SCI JI J. Afr. Earth Sci. PD MAY PY 2004 VL 39 IS 1-2 BP 25 EP 62 DI 10.1016/j.jafrearsci.2004.05.001 PG 38 WC Geosciences, Multidisciplinary SC Geology GA 854BM UT WOS:000223875100002 ER PT J AU Jiggins, CD Estrada, C Rodrigues, A AF Jiggins, CD Estrada, C Rodrigues, A TI Mimicry and the evolution of premating isolation in Heliconius melpomene Linnaeus SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE Lepidoptera; mate recognition; sensory bias; sexual selection; speciation ID FEMALE MATE CHOICE; SEXUAL SELECTION; SYMPATRIC SPECIATION; MULLERIAN MIMICRY; REPRODUCTIVE ISOLATION; ADAPTIVE RADIATION; RELATIVE ABUNDANCE; NATURAL-SELECTION; HYBRID STERILITY; HOST RACES AB Ecological divergence can cause speciation if adaptive traits have pleiotropic effects on mate choice. In Heliconius butterflies, mimetic patterns play a role in mate detection between sister species, as well as signalling to predators. Here we show that male butterflies from four recently diverged parapatric populations of Heliconius melpomene are more likely to approach and court their own colour patterns as compared with those of other races. A few exceptions, where males were more attracted to patterns other than their own, suggest that some mimetic patterns are sub-optimal in mate choice. Genotype frequencies in hybrid zones between races of H. melpomene suggest that mating is random, so reinforcement is unlikely to have played a role in intra-specific divergence. In summary, co-evolved divergence of colour pattern and mate preference occurs rapidly and is likely the first step in Heliconius speciation. C1 Univ Edinburgh, Inst Cell Anim & Populat Biol, Ashworth Labs, Edinburgh EH9 3JT, Midlothian, Scotland. Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sch Biol Sci, Austin, TX 78712 USA. RP Jiggins, CD (reprint author), Univ Edinburgh, Inst Cell Anim & Populat Biol, Ashworth Labs, W Mains Rd, Edinburgh EH9 3JT, Midlothian, Scotland. EM chris.jiggins@ed.ac.uk RI Jiggins, Chris/B-9960-2008 OI Jiggins, Chris/0000-0002-7809-062X NR 71 TC 73 Z9 75 U1 4 U2 23 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD MAY PY 2004 VL 17 IS 3 BP 680 EP 691 DI 10.1111/j.1420-9101.2004.00675.x PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 817ST UT WOS:000221197900021 PM 15149410 ER PT J AU Proschan, F AF Proschan, F TI Response by Frank Proschan - On advocacy and advocates SO JOURNAL OF FOLKLORE RESEARCH LA English DT Article C1 Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. RP Proschan, F (reprint author), Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 2 PU INDIANA UNIV PI BLOOMINGTON PA FOLKLORE INST 504 NORTH FESS ST, BLOOMINGTON, IN 47405 USA SN 0737-7037 J9 J FOLKLORE RES JI J. Folk. Res. PD MAY-DEC PY 2004 VL 41 IS 2-3 BP 267 EP 273 PG 7 WC Folklore SC Arts & Humanities - Other Topics GA 879VJ UT WOS:000225746800011 ER PT J AU Ortner, DJ AF Ortner, DJ TI The bioarchaeology of tuberculosis: A global view on a reemerging disease SO JOURNAL OF HUMAN EVOLUTION LA English DT Book Review C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Ortner, DJ (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 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 MAY PY 2004 VL 46 IS 5 BP 643 EP 645 DI 10.1016/j.jhevol.2004.02.003 PG 3 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 820ZE UT WOS:000221427900010 ER PT J AU Thorwirth, S McCarthy, MC Dudek, JB Thaddeus, P AF Thorwirth, S McCarthy, MC Dudek, JB Thaddeus, P TI High resolution microwave spectroscopy of the isomeric pair vinylcyano acetylene and cyanovinylacetylene SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE carbon chain molecules; microwave spectroscopy; hyperfine structure; quantum chemical calculations ID MOLECULES; 1-CYANOBUT-3-ENE-1-YNE; CH2=CH-C=C-C=N; SPECTRA; C=N AB The carbon chain molecules vinylcyanoacetylene and cyanovinylacetylene have been investigated between 8 and 41 GHz by Fourier transform microwave spectroscopy of a supersonic molecular beam. Owing to the high spectral resolution of the present technique, significantly more accurate rotational and centrifugal distortion constants have been derived for both molecules. In addition, the dipole moments have been calculated at the B3LYP/cc-pVTZ level of theory. Because these carbon chains are similar in structure and composition to known astronomical molecules and because of their high polarity, both species are good candidates for radioastronomical detection. (C) 2004 Elsevier Inc. All rights reserved. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Thorwirth, S (reprint author), Harvard Univ, Div Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. EM sthorwirth@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 NR 13 TC 7 Z9 7 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD MAY PY 2004 VL 225 IS 1 BP 93 EP 95 DI 10.1016/j.jms.2004.01.007 PG 3 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 814UY UT WOS:000221000800012 ER PT J AU Switzer, TS Baltz, DM Allen, RL Munroe, TA AF Switzer, TS Baltz, DM Allen, RL Munroe, TA TI Habitat selection by sympatric tonguefishes (Symphurus : Cynoglossidae) in coastal Louisiana, USA: unravelling seasonal, spatial, and size-specific patterns in resource utilisation SO JOURNAL OF SEA RESEARCH LA English DT Article; Proceedings Paper CT 5th International Symposium on Flatfish Ecology CY NOV 03-07, 2002 CL ISLE OF MAN, ENGLAND DE beam-trawl; estuaries; flatfish; juveniles; nursery grounds; sympatric populations; USA; Louisiana; Barataria Bay ID GULF-OF-MEXICO; MICROHABITAT USE; NORTH-CAROLINA; EARLY LIFE; FISHES; ESTUARINE; PLEURONECTIFORMES; GROWTH; FLATFISH; RECRUITMENT AB We examined patterns of resource utilisation between young-of-the-year blackcheek tonguefish (Symphurus plagiusa) and offshore tonguefish (S. civitatium), in Barataria Bay, Louisiana, USA. A stratified monthly sampling approach was implemented to facilitate sampling of the broad saline to brackish estuary along environmental gradients. At each site several environmental variables were determined: salinity, temperature, dissolved oxygen, bottom type, median depth and distance from shore. In 594 independent beam-trawl samples, 2897 offshore tonguefish and 631 blackcheek tonguefish were collected. The distributions of both species overlapped broadly on a seasonal basis (Schoener's index of overlap = 0.78). Both species were found in the study area in all seasons, with highest abundances during fall and winter months. On a spatial basis, the species did not overlap as much (index of overlap = 0.35). Approximately 83% of blackcheek tonguefish were collected in the uppermost or landward three strata, whereas 64% of offshore tonguefish were collected in the lowermost or seaward stratum. When spatial and seasonal distributions were considered together, overlap was reduced to 0.30, and when size-class distributions were added, the overlap of comparably sized individuals was reduced to approximately 0.23. In a multivariate analysis of variance comparison of microhabitat use between species, several significant differences were detected (P < 0.05): blackcheek tonguefish generally used lower salinities, higher temperatures, finer bottom types, shallower depths, and were found nearer to shore than offshore tonguefish. Among size classes there were significant differences within and between species for all six microhabitat variables. Size-related shifts in resource utilisation along environmental gradients were evident for both species. (C) 2004 Elsevier B.V. All rights reserved. C1 Louisiana State Univ, Coastal Fisheries Inst, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA. Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA. Smithsonian Inst, NOAA, NMFS, Natl Systemat Lab,NHB, Washington, DC 20013 USA. RP Switzer, TS (reprint author), Louisiana State Univ, Coastal Fisheries Inst, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA. EM TSSwitzer@aol.com RI Baltz, Donald/A-9374-2009 NR 47 TC 6 Z9 6 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1385-1101 J9 J SEA RES JI J. Sea Res. PD MAY PY 2004 VL 51 IS 3-4 BP 229 EP 242 DI 10.1016/j.seares.2003.10.001 PG 14 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 820PA UT WOS:000221400600007 ER PT J AU Hutchinson, A AF Hutchinson, A TI Becoming a tiger: How baby animals learn to live in the wild. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Hutchinson, A (reprint author), Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 1 PY 2004 VL 129 IS 8 BP 137 EP 137 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 837VL UT WOS:000222669000181 ER PT J AU Kawakita, A Sota, T Ito, M Ascher, JS Tanaka, H Kato, M Roubik, DW AF Kawakita, A Sota, T Ito, M Ascher, JS Tanaka, H Kato, M Roubik, DW TI Phylogeny, historical biogeography, and character evolution in bumble bees (Bombus : Apidae) based on simultaneous analysis of three nuclear gene sequences SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID MITOCHONDRIAL CYTOCHROME-B; OXIDASE I SEQUENCES; COMMUNITY STRUCTURE; HYMENOPTERA; LATR C1 Kyoto Univ, Grad Sch Sci, Dept Zool, Kyoto 6068502, Japan. Kyoto Univ, Grad Sch Sci, Grad Sch Human & Environm Studies, Kyoto, Japan. Sapporo Sci & Technol Vocat Sch, Sapporo, Hokkaido, Japan. Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY USA. Kyoto Univ, Primate Res Inst, Inuyama, Aichi 484, Japan. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Sota, T (reprint author), Kyoto Univ, Grad Sch Sci, Dept Zool, Kyoto 6068502, Japan. EM sota@terra.zool.kyoto-u.ac.jp RI Ascher, John/D-1554-2014 NR 37 TC 36 Z9 43 U1 2 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAY PY 2004 VL 31 IS 2 BP 799 EP 804 DI 10.1016/j.ympev.2003.12.003 PG 6 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 814AQ UT WOS:000220948000032 PM 15062814 ER PT J AU Sokasian, A Yoshida, N Abel, T Hernquist, L Springel, V AF Sokasian, A Yoshida, N Abel, T Hernquist, L Springel, V TI Cosmic reionization by stellar sources: population III stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; intergalactic medium; galaxies : starburst ID DIGITAL SKY SURVEY; COLD DARK-MATTER; HIGH-REDSHIFT; COSMOLOGICAL REIONIZATION; INTERGALACTIC MEDIUM; IONIZING-RADIATION; GALAXY FORMATION; PRIMORDIAL GAS; HYDROGEN REIONIZATION; NUMERICAL COSMOLOGY AB We combine fast radiative transfer calculations with high-resolution hydrodynamical simulations to study an epoch of early hydrogen reionization by primordial stellar sources at redshifts 15less than or similar tozless than or similar to30. We consider the implications of various local and global feedback mechanisms using a set of models that bracket the severity of these effects to determine, qualitatively, how they may have influenced the global star formation rate and the details of hydrogen reionization. With relatively conservative assumptions, most of our models suggest that population III star formation proceeds in a self-regulated manner both locally and globally and, for a conventional LambdaCDM cosmology, can significantly reionize the intergalactic medium between 15less than or similar tozless than or similar to20 as long as a large fraction of ionizing photons can escape from these earliest galaxies. We then combine these results with our earlier work focusing on the role of population II stars in galaxies with virial temperatures greater than or similar to 10(4) K at redshifts 5less than or similar tozless than or similar to20. Hence, we construct a complete reionization history of the Universe that matches the Thomson optical depths as measured by the WMAP satellite as well as the evolution of the Gunn-Peterson optical depth as seen in the absorption spectra of the highest redshift quasars. We find that even with conservative estimates for the impact of negative feedback mechanisms, primordial stellar sources contribute significantly to early reionization. Future observations of a Thomson optical depth of tau(e)greater than or similar to0.13 would bolster the claim for the existence of population III stars similar to the ones studied here. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ Japan, Tokyo 1818588, Japan. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Sokasian, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asokasia@cfa.harvard.edu RI Yoshida, Naoki/A-4305-2011 NR 77 TC 129 Z9 129 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 MAY 1 PY 2004 VL 350 IS 1 BP 47 EP 65 DI 10.1111/j.1365-2966.2004.07636.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 814MR UT WOS:000220979300010 ER PT J AU Marsh, TR Nelemans, G Steeghs, D AF Marsh, TR Nelemans, G Steeghs, D TI Mass transfer between double white dwarfs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; gravitational waves; binaries : close; novae, cataclysmic variables; white dwarfs ID CLOSE BINARY-SYSTEMS; SHORTEST PERIOD BINARY; X-RAY BINARIES; AM CVN STARS; CATACLYSMIC VARIABLES; TRANSFER INSTABILITIES; RADIUS RELATION; ORBITAL PERIOD; TIDAL FRICTION; I SUPERNOVAE AB Three periodically variable stars have recently been discovered (V407 Vul, P=9.5 min; ES Cet, P=10.3 min; RX J0806.3+1527, P=5.3 min) with properties that suggest that their photometric periods are also their orbital periods, making them the most compact binary stars known. If true, this might indicate that close, detached, double white dwarfs are able to survive the onset of mass transfer caused by gravitational wave radiation and emerge as the semi-detached, hydrogen-deficient stars known as the AM CVn stars. The accreting white dwarfs in such systems are large compared to the orbital separations. This has two effects. First, it makes it likely that the mass-transfer stream can hit the accretor directly. Secondly, it causes a loss of angular momentum from the orbit which can destabilize the mass transfer unless the angular momentum lost to the accretor can be transferred back to the orbit. The effect of the destabilization is to reduce the number of systems which survive mass transfer by as much as one hundredfold. In this paper we analyse this destabilization and the stabilizing effect of a dissipative torque between the accretor and the binary orbit. We obtain analytical criteria for the stability of both disc-fed and direct impact accretion, and we carry out numerical integrations to assess the importance of secondary effects, the chief one being that otherwise stable systems can exceed the Eddington accretion rate. We show that to have any effect upon survival rates, the synchronizing torque must act on a time-scale of the order of 1000 yr or less. If synchronization torques are this strong, then they will play a significant role in the spin rates of white dwarfs in cataclysmic variable stars as well. C1 Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Southampton, Dept Phys & Astron, Southampton S017 1BJ, Hants, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marsh, TR (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM t.r.marsh@warwick.ac.uk RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746 NR 64 TC 133 Z9 133 U1 0 U2 2 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2004 VL 350 IS 1 BP 113 EP 128 DI 10.1111/j.1365-2966.2004.07564.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 814MR UT WOS:000220979300014 ER PT J AU Kurin, R AF Kurin, R TI Safeguarding intangible cultural heritage in the 2003 UNESCO Convention: A critical appraisal SO MUSEUM INTERNATIONAL LA English DT Article C1 Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. RP Kurin, R (reprint author), Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. NR 0 TC 57 Z9 59 U1 1 U2 15 PU BLACKWELL PUBL LTD PI OXFORD PA 108 COWLEY RD, OXFORD OX4 1JF, OXON, ENGLAND SN 1350-0775 J9 MUSEUM INT JI Mus. Int. PD MAY PY 2004 VL 56 IS 1-2 BP 66 EP 76 DI 10.1111/j.1350-0775.2004.00459.x PG 11 WC Art SC Art GA 838TR UT WOS:000222736600009 ER PT J AU Pendall, E Bridgham, S Hanson, PJ Hungate, B Kicklighter, DW Johnson, DW Law, BE Luo, YQ Megonigal, JP Olsrud, M Ryan, MG Wan, SQ AF Pendall, E Bridgham, S Hanson, PJ Hungate, B Kicklighter, DW Johnson, DW Law, BE Luo, YQ Megonigal, JP Olsrud, M Ryan, MG Wan, SQ TI Below-ground process responses to elevated CO2 and temperature: a discussion of observations, measurement methods, and models SO NEW PHYTOLOGIST LA English DT Review DE carbon sequestration; CO2 fertilization; mycorrhizas; nutrient cycling; rhizosphere; soil carbon; soil respiration; soil warming ID ATMOSPHERIC CARBON-DIOXIDE; SOIL ORGANIC-CARBON; GLOBAL ENVIRONMENTAL-CHANGE; NET PRIMARY PRODUCTIVITY; FINE-ROOT; CLIMATE-CHANGE; TERRESTRIAL ECOSYSTEMS; PINUS-TAEDA; NITROGEN CONCENTRATION; POPULUS-TREMULOIDES AB Rising atmospheric CO2 and temperatures are probably altering ecosystem carbon cycling, causing both positive and negative feedbacks to climate. Below-ground processes play a key role in the global carbon (C) cycle because they regulate storage of large quantities of C, and are potentially very sensitive to direct and indirect effects of elevated CO2 and temperature. Soil organic matter pools, roots and associated rhizosphere organisms all have distinct responses to environmental change drivers, although availability of C substrates will regulate all the responses. Elevated CO2 increases C supply below-ground, whereas warming is likely to increase respiration and decomposition rates, leading to speculation that these effects will moderate one another. However, indirect effects on soil moisture availability and nutrient supply may alter processes in unexpected directions. Detailed, mechanistic understanding and modelling of below-ground flux components, pool sizes and turnover rates is needed to adequately predict long-term, net C storage in ecosystems. In this synthesis, we discuss the current status of below-ground responses to elevated CO2 and temperature and potential feedback effects, methodological challenges, and approaches to integrating models and measurements. C1 Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. Univ Oregon, Ctr Ecol & Evolutionary Biol, Eugene, OR 97403 USA. Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. Marine Biol Lab, Ctr Ecosyst, Woods Hole, MA 02543 USA. Univ Nevada, Dept Nat Resources & Environm Sci, Reno, NV 89557 USA. Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Lund Univ, Geobiosphere Sci Ctr, S-22362 Lund, Sweden. Forest Serv Rocky Mt, USDA, Res Stn, Ft Collins, CO 80526 USA. Colorado State Univ, Dept Forest Rangeland & Watershed Stewardship, Ft Collins, CO 80523 USA. Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. Chinese Acad Sci, Inst Bot, Beijing 100093, Peoples R China. Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. RP Pendall, E (reprint author), Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. EM Pendall@uwyo.edu RI Ryan, Michael/A-9805-2008; Wan, Shiqiang/B-5799-2009; Hanson, Paul J./D-8069-2011; Hungate, Bruce/F-8991-2011; OI Ryan, Michael/0000-0002-2500-6738; Hanson, Paul J./0000-0001-7293-3561; Hungate, Bruce/0000-0002-7337-1887; Pendall, Elise/0000-0002-1651-8969; Law, Beverly/0000-0002-1605-1203 NR 131 TC 198 Z9 218 U1 13 U2 164 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0028-646X J9 NEW PHYTOL JI New Phytol. PD MAY PY 2004 VL 162 IS 2 BP 311 EP 322 DI 10.1111/j.1469-8137.2004.01053.x PG 12 WC Plant Sciences SC Plant Sciences GA 815RH UT WOS:000221058900006 ER PT J AU Giannini, NP Kalko, EKV AF Giannini, NP Kalko, EKV TI Trophic structure in a large assemblage of phyllostomid bats in Panama SO OIKOS LA English DT Article ID FRUIT-EATING BATS; CANONICAL CORRESPONDENCE-ANALYSIS; CAROLLIA-PERSPICILLATA; COMMUNITY ECOLOGY; FEEDING-BEHAVIOR; DIETARY OVERLAP; PRIMARY FORESTS; DRY FOREST; BRAZIL; CHIROPTERA AB Bats of the family Phyllostomidae are fundamental components of Neotropical mammalian diversity and display the greatest dietary diversity seen in any mammalian family. We studied trophic structure in a species-rich local assemblage of phyllostomids for which dietary data were collected during 10 years on Barro Colorado Island, Panama. Correspondence analysis of >3800 dietary records from 30 syntopic species showed a structure supporting traditional divisions of animalivorous and phytophagous phyllostomids. Putatively omnivorous species actually grouped among the latter. Phytophagous phyllostomids separated into Piper-specialists, Ficus-specialists, and eclectic plant eaters which in turn were the main consumers of flower products. Discrete dietary groups were compatible with several clades of the two current phylogenetic hypotheses of phyllostomids. We show that the trophic structure of the local contemporary assemblage is largely conservative with respect to traceable ancestral habits, strongly suggesting that overall trophic structure was likely determined historically. C1 Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. Univ Ulm, Dept Expt Ecol Bio 3, DE-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Giannini, NP (reprint author), Amer Museum Nat Hist, Dept Mammal, Cent Pk W & 79th St, New York, NY 10024 USA. EM norberto@amnh.org NR 89 TC 110 Z9 127 U1 2 U2 28 PU BLACKWELL MUNKSGAARD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0030-1299 J9 OIKOS JI Oikos PD MAY PY 2004 VL 105 IS 2 BP 209 EP 220 DI 10.1111/j.0030-1299.2004.12690.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 805RJ UT WOS:000220383100001 ER PT J AU Blackman, EG Field, GB AF Blackman, EG Field, GB TI A new approach to turbulent transport of a mean scalar (vol 15, pg L73, 2003) SO PHYSICS OF FLUIDS LA English DT Correction C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Rochester, Laser Energet Lab, Rochester, NY 14627 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blackman, EG (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD MAY PY 2004 VL 16 IS 5 BP 1830 EP 1830 DI 10.1063/1.1695583 PG 1 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 812IG UT WOS:000220832600058 ER PT J AU Eichhorn, G Kurtz, MJ AF Eichhorn, G Kurtz, MJ TI A reader answers: 'Critical mass' origin SO PHYSICS TODAY LA English DT Letter C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Eichhorn, G (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009; KURTZ, Michael /B-3890-2009 OI Eichhorn, Guenther/0000-0002-3032-1978; NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD MAY PY 2004 VL 57 IS 5 BP 18 EP 18 DI 10.1063/1.1768661 PG 1 WC Physics, Multidisciplinary SC Physics GA 816VK UT WOS:000221137200010 ER PT J AU Marsden, BG AF Marsden, BG TI Tales from the transneptunian sea SO PHYSICS WORLD LA English DT News Item C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marsden, BG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-8585 J9 PHYS WORLD JI Phys. World PD MAY PY 2004 VL 17 IS 5 BP 24 EP 25 PG 2 WC Physics, Multidisciplinary SC Physics GA 838EJ UT WOS:000222696000027 ER PT J AU Levine, MT Feller, IC AF Levine, MT Feller, IC TI Effects of forest age and disturbance on population persistence in the understory herb, Arisaema triphyllum (Araceae) SO PLANT ECOLOGY LA English DT Article DE dioecious; reproductive effort; sex ratio; succession; temporal dispersal; waiting strategy ID IN-THE-PULPIT; VEGETATIVE REPRODUCTION; ASEXUAL REPRODUCTION; UVULARIA-PERFOLIATA; WOODLAND HERB; LIFE-HISTORY; RESOURCE-ALLOCATION; ASTER-ACUMINATUS; CLONAL GROWTH; PLANT SIZE AB Long-lived understory herbs experience a highly dynamic forest over space and time, yet can persist for more than a century. To understand how these populations persist, we examined effects of forest age and disturbance on potential sexual reproduction and clonal growth in the sexually labile perennial, Arisaema triphyllum. Potential sexual reproduction (female: male ratio) was significantly greater in the Young and Old-Gap forest states compared with Old, closed-canopy sites, where it was virtually absent. In contrast, clonal growth (estimated by cormlet production) did not differ significantly among the three forest states. Of seven environmental variables measured, only light (positively) and plant density (negatively) contributed significantly to the variation in potential sexual reproduction, while no measured variables contributed significantly to the variation in number of cormlets. The larger sexual reproductive effort (flower+stalk biomass/total biomass) for males in the undisturbed, 100 yr old forest may explain the absence of females in these sites, while the invariant vegetative reproductive effort (cormlet biomass/total biomass) may explain the similarity in average number of cormlets per individual per season across forest states. These results suggest that potential sexual reproduction is resource-limited, while clonal growth may be resource-independent. By maintaining ramet production during unfavorable periods, A. triphyllum populations disperse temporally, "waiting" for conditions under which sexual reproduction may resume. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Levine, MT (reprint author), Univ Calif Davis, Populat Biol Grad Grp, 2320 Storer Hall,1 Shields Ave, Davis, CA 95616 USA. OI Feller, Ilka/0000-0002-6391-1608 NR 42 TC 9 Z9 13 U1 3 U2 20 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD MAY PY 2004 VL 172 IS 1 BP 73 EP 82 DI 10.1023/B:VEGE.0000026036.32013.7a PG 10 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 816PH UT WOS:000221121300007 ER PT J AU Hearty, PJ Olson, SL Kaufman, DS Edwards, RL Cheng, H AF Hearty, PJ Olson, SL Kaufman, DS Edwards, RL Cheng, H TI Stratigraphy and geochronology of pitfall accumulations in caves and fissures, Bermuda SO QUATERNARY SCIENCE REVIEWS LA English DT Article ID LAST INTERGLACIAL PERIOD; SEA-LEVEL HISTORY; LATE PLEISTOCENE; NORTH-ATLANTIC; CLIMATE-CHANGE; U-SERIES; BAHAMAS; LIMESTONES; SOILS; AMINOSTRATIGRAPHY AB Deep fractures ("fissures") and avens ("skylights") in limestone cave roofs create natural traps for sediments and biota. Fissures fill quickly with surface sediment and organisms soon after opening. Debris cones Lire formed as materials fall, wash, or drift on air through openings in cave skylights. Such deposits in Admiral's and Grand Canyon Cave, Bermuda contain distinct beds and are composed Of mixtures of sediment and charcoal, together with fossils of land snails, crabs, birds, reptiles, and bats. The "pitfall" accumulations were periodically sealed over by calcite flowstone. A stratigraphic record Of Surface activity and fauna through both glacial and interglacial periods has been preserved. The succession also provides an ideal setting in which to compare several geochronological methods. Calibrated 14 C ages on charcoal and shells provide dated horizons at 1600, 12,800, and about 35,000 C-14 yr BP. Thermal ionization mass spectrometric (TIMS) ages on several flowstone layers constrain the entire sequence in the Admiral's Cave sequence between 126,300 +/- 900 yr (Termination II) and historical times. A continuous relative-age record generated by amino acid epimerization (AAE) geochronology (D-alloisoleucine/L-isoleucine or alle/Ile) on the pulmonate land gastropod Poecilozonites verifies the biostratigraphy, reveals a minimal degree of mixing between stratigraphic units, and establishes an independent temporal link between the subterranean and subaerial deposits of Bermuda. This convergence between stratigraphy and geochronology yields a precisely dated succession from the oceanic island of Bermuda, and thus presents a unique opportunity to assess the rates and processes of evolutionary and climate change during that interval. (C) 2003 Elsevier Ltd. All rights reserved. C1 James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. No Arizona Univ, Dept Geol, Flagstaff, AZ 86011 USA. No Arizona Univ, Dept Environm Sci, Flagstaff, AZ 86011 USA. Univ Minnesota, Dept Geol & Geophys, Minneapolis, MN 55455 USA. RP James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia. EM paul.hearty@jcu.edu.au RI Kaufman, Darrell/A-2471-2008 OI Kaufman, Darrell/0000-0002-7572-1414 NR 50 TC 41 Z9 41 U1 1 U2 3 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 MAY PY 2004 VL 23 IS 9-10 BP 1151 EP 1171 DI 10.1016/j.quascirev.2003.09.008 PG 21 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 822ZT UT WOS:000221580200011 ER PT J AU Spindler, RE Huang, Y Howard, JG Wang, P Zhang, H Zhang, G Wildt, DE AF Spindler, RE Huang, Y Howard, JG Wang, P Zhang, H Zhang, G Wildt, DE TI Acrosomal integrity and capacitation are not influenced by sperm cryopreservation in the giant panda SO REPRODUCTION LA English DT Article ID PROTEIN-TYROSINE PHOSPHORYLATION; ZONA-PELLUCIDA PENETRATION; AILUROPODA-MELANOLEUCA; BOVINE SPERM; IN-VITRO; HAMSTER SPERMATOZOA; BOAR SPERMATOZOA; ARTIFICIAL-INSEMINATION; CAT SPERMATOZOA; SEMEN EXTENDER AB Sperm cryopreservation and artificial insemination are important management tools for giant panda breeding and the preservation of extant genetic diversity. This study examined the influence of freeze-thawing on sperm function, specifically capacitation. Sperm from nine giant pandas were assessed before and after rapid ( - 40 and - 100 degreesC/min) cryopreservation by incubation in HEPES-buffered Ham's F10 medium with and without the capacitation accelerators, 3-isobutyl-1-methylxanthine (IBMX) and dibutyryl cyclic AMP (dbcAMP). At 0, 3 and 6 h of exposure, aliquots were assessed for sperm motility traits and capacitation, defined as the proportion of sperm with intact acrosomes following exposure to solubilised zonae pellucidae (ursid or felid) or calcium ionophore subtracted from the proportion of sperm with intact acrosomes before exposure. Although mean +/- S.E.M. sperm motility post-thaw (56.1 +/- 3.9% at 0 h) was less (P < 0.05) than pre-freeze (71.7 +/- 6.0%), there was no difference (P > 0.05) in the proportion of acrosome-intact sperm (fresh, 93.0 +/- 1.7% versus cryopreserved-thawed, 81.7 +/- 4.7% at 0 h). Incidence of capacitation was greater (P < 0.05) in fresh sperm incubated with capacitation accelerators IBMX and dbcAMP (9 h: 50.9 +/- 1.1) compared with fresh sperm incubated without accelerators (9 h: 41.2 +/- 1.1 %). Frozen-thawed sperm preincubated without accelerators underwent capacitation (49.6 +/- 1.1 %) to a greater extent (P < 0.05) compared with these fresh counterparts. Thawed samples with (9 h: 45.9 +/- 1.4%) and without accelerators (9 h: 41.2 +/- 1.1 %) did not differ (P > 0.05) during the 9-h incubation. We conclude that giant panda spermatozoa (1) undergo capacitation in vitro with or without chemical accelerators and (2) withstand a rapid cryopreservation protocol, including retaining normal acrosomal integrity and functional capacitation ability. C1 Smithsonians Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. China Res & Conservat Ctr Giant Panda, Wolong, Peoples R China. RP Spindler, RE (reprint author), Smithsonians Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM rspindler@torontozoo.ca NR 76 TC 24 Z9 24 U1 2 U2 9 PU BIO SCIENTIFICA LTD PI BRISTOL PA EURO HOUSE, 22 APEX COURT WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT, ENGLAND SN 1470-1626 J9 REPRODUCTION JI Reproduction PD MAY PY 2004 VL 127 IS 5 BP 547 EP 556 DI 10.1530/rep.1.00034 PG 10 WC Developmental Biology; Reproductive Biology SC Developmental Biology; Reproductive Biology GA 825ZK UT WOS:000221797900005 PM 15129010 ER PT J AU Small, LM AF Small, LM TI Grand reunion - For the dedication of a new World War II memorial on the Mall, the Smithsonian will stage a four-day festival of reminiscence SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAY PY 2004 VL 35 IS 2 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 814YJ UT WOS:000221009700002 ER PT J AU Lovelock, CE Wright, SF Nichols, KA AF Lovelock, CE Wright, SF Nichols, KA TI Using glomalin as an indicator for arbuscular mycorrhizal hyphal growth: an example from a tropical rain forest soil SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE hyphal production; extra-radical hyphae; in-growth cores; Acaulospora morrowiae; Glomus etunicatum; Glomus intraradices; Gigaspora rosea ID FUNGAL BIOMASS; COMMUNITIES; LANDSCAPE; MYCELIUM; PROTEIN AB Glomalin concentrations of extra-radical arbuscular mycorrhizal (AM) hyphae were estimated by deploying hyphal in-growth cores ;containing glomalin-free sand in field soils in a tropical forest and in pot cultures. In field soils, glomalin was 0.044 +/- 0.013 mug m(-1) hyphae. In pot cultures glomalin concentrations were lower (range 0.0068-0.036 mug m(-1)), and varied significantly among species. Using this technique, preliminary estimates of extraradical AM hyphal production on Inceptisols were 1.91 Mg ha(-1) yr(-1) and on Oxisol were 1.47 Mg ha(-1) yr(-1), but they could range between 0.9-5.7 Mg ha(-1) yr(-1). These rates of hyphal production are approximately 10% (range 5-33%) of estimated above ground primary production of the forest. (C) 2004 Elsevier Ltd. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. USDA ARS, Sustainable Agr Syst Lab, Beltsville, MD 20705 USA. USDA ARS, No Great Plains Res Lab, Mandan, ND 58554 USA. RP Lovelock, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM lovelockc@si.edu RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 20 TC 32 Z9 35 U1 1 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD MAY PY 2004 VL 36 IS 6 BP 1009 EP 1012 DI 10.1016/j.soilbio.2004.02.010 PG 4 WC Soil Science SC Agriculture GA 826SM UT WOS:000221848900015 ER PT J AU Liang, CL Rice, JA de Pater, I Alcock, C Axelrod, T Wang, A Marshall, S AF Liang, CL Rice, JA de Pater, I Alcock, C Axelrod, T Wang, A Marshall, S TI Statistical methods for detecting stellar occultations by Kuiper Belt objects: The Taiwanese-American Occultation Survey SO STATISTICAL SCIENCE LA English DT Article DE Kuiper Belt; occultation ID DISCOVERY AB The Taiwanese-American Occultation Survey (TAOS) will detect objects in the Kuiper Belt by measuring the rate of occultations of stars by these objects, using an array of three to four 50 cm wide-field robotic telescopes. Thousands of stars will be monitored, resulting in hundreds of millions of photometric measurements per night. To optimize the success of TAOS, we have investigated various methods of gathering and processing the data, and developed statistical methods for detecting occultations. In this paper we discuss these methods. The resulting estimated detection efficiencies will be used to guide the choice of various operational parameters that determine the mode of actual observation when the telescopes come on line and begin routine observations. In particular, we show how realtime detection algorithms may be constructed, taking advantage of having multiple telescopes. We also discuss a retrospective method for estimating the rate at which occultations occur. C1 Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM rice@stat.berkeley.edu; imake@floris.berkeley.edu; taxelrod@as.arizona.edu; marshall@slac.stanford.edu NR 12 TC 7 Z9 7 U1 0 U2 0 PU INST MATHEMATICAL STATISTICS PI BEACHWOOD PA PO BOX 22718, BEACHWOOD, OH 44122 USA SN 0883-4237 J9 STAT SCI JI Stat. Sci. PD MAY PY 2004 VL 19 IS 2 BP 265 EP 274 DI 10.1214/088342304000000378 PG 10 WC Statistics & Probability SC Mathematics GA 897YM UT WOS:000227042800005 ER PT J AU Xiang, QP Zhang, XC Nicolson, DH AF Xiang, QP Zhang, XC Nicolson, DH TI On the correctability of the epithet minchegense to mingcheense... ( vol 52, pg 857, 2003) SO TAXON LA English DT Correction C1 Chinese Acad Sci, Inst Bot, Ctr Syst & Evolutionary Bot, Beijing 100093, Peoples R China. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Xiang, QP (reprint author), Chinese Acad Sci, Inst Bot, Ctr Syst & Evolutionary Bot, Beijing 100093, Peoples R China. EM Nicolson.Dan@nmnh.si.edu NR 3 TC 1 Z9 1 U1 0 U2 0 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD MAY PY 2004 VL 53 IS 2 BP 628 EP 628 DI 10.2307/4135672 PG 1 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 837MS UT WOS:000222640200040 ER PT J AU Bower, GC Falcke, H Herrnstein, RM Zhao, JH Goss, WM Backer, DC AF Bower, GC Falcke, H Herrnstein, RM Zhao, JH Goss, WM Backer, DC TI Detection of the intrinsic size of Sagittarius A* through closure amplitude imaging SO SCIENCE LA English DT Article ID SUPERMASSIVE BLACK-HOLE; SCATTER-BROADENED IMAGE; GALACTIC-CENTER; PROPER MOTION; 1 MILLIMETER; SPECTRUM; RADIO; ELECTRONS; MODEL; GHZ AB We have detected the intrinsic size of Sagittarius A*, the Galactic center radio source associated with a supermassive black hole, showing that the short-wavelength radio emission arises from very near the event horizon of the black hole. Radio observations with the Very Long Baseline Array show that the source has a size of 24 +/- 2 Schwarzschild radii at 7-millimeter wavelength. In one of eight 7-millimeter epochs, we also detected an increase in the intrinsic size of 60(-17)(+25)%. These observations place a lower limit to the mass density of Sagittarius A* of 1.4 x 10(4) solar masses per cubic astronomical unit. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. ASTRON, Radio Observ Westerbork, NL-7990 AA Dwingeloo, Netherlands. Univ Nijmegen, Dept Astron, NL-6500 GL Nijmegen, Netherlands. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Columbia Univ, Dept Astron, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA. RP Bower, GC (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM gbower@astro.berkeley.edu RI Falcke, Heino/H-5262-2012 OI Falcke, Heino/0000-0002-2526-6724 NR 37 TC 132 Z9 136 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 APR 30 PY 2004 VL 304 IS 5671 BP 704 EP 708 DI 10.1126/science.1094023 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 816JD UT WOS:000221105300036 PM 15060284 ER PT J AU Lingafelter, SW AF Lingafelter, SW TI New species of Stizocera (Coleoptera : Cerambycidae) from Bolivia SO ZOOTAXA LA English DT Article DE longhorned beetles; descriptions; Buena Vista; Cerambycidae; Bolivia; Stizocera; Elaphidiini; new species; Santa Cruz AB Two species of Stizocera ( Coleoptera: Cerambycidae: Cerambycinae: Elaphidiini) are described from Buena Vista, Ichilo Province, Santa Cruz Department, Bolivia: Stizocera delicata, new species and Stizocera ichilo, new species. Comparison of diagnostic features with the similar species Stizocera longicollis Zajciw, Stizocera rugicollis Guerin-Meneville, and Stizocera nigroapicalis Fuchs is presented. C1 ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Lingafelter, SW (reprint author), ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, MRC-168, Washington, DC 20013 USA. EM slingafe@sel.barc.usda.gov NR 9 TC 2 Z9 2 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 30 PY 2004 IS 498 BP 1 EP 11 PG 11 WC Zoology SC Zoology GA 869CB UT WOS:000224959200001 ER PT J AU Samper, C AF Samper, C TI Taxonomy and environmental policy SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Article DE convention on biological diversity; environmental policy; environmental politics; global taxonomy initiative ID GENETIC-RESOURCES; LIFE AB In 1992, with the United Nations Conference on Environment and Development in Rio de Janeiro and the subsequent Convention on Biological Diversity (CBD), the world changed for the science of taxonomy. Many taxonomists appear not to have noticed this change, but it has significantly altered the political climate in which taxonomic research is undertaken. By the late 1990s it was clear that effective implementation of the CBD needed the participation of and funding for the taxonomic community. In this paper, I chart the rise of the Global Taxonomy Initiative (GTI), review some of its goals and explore how it interacts with the CBD. The interactions of the GTI with the Global Environment Facility, a potential funding body, are explored, as are the possible synergies between the GTI and the many other global initiatives linking to taxonomy. Finally, I explore some of the challenges ahead as taxonomy begins to take a front seat in the implementation of environmental policy on the world stage. C1 Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. RP Samper, C (reprint author), Smithsonian Inst, Museum Natl Hist Nat, 10th St & Constitut Ave NW, Washington, DC 20560 USA. EM samperc@si.edu NR 17 TC 18 Z9 20 U1 0 U2 3 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD APR 29 PY 2004 VL 359 IS 1444 BP 721 EP 728 DI 10.1098/rstb.2004.1476 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 816AF UT WOS:000221082100014 PM 15253357 ER PT J AU Wright, IJ Reich, PB Westoby, M Ackerly, DD Baruch, Z Bongers, F Cavender-Bares, J Chapin, T Cornelissen, JHC Diemer, M Flexas, J Garnier, E Groom, PK Gulias, J Hikosaka, K Lamont, BB Lee, T Lee, W Lusk, C Midgley, JJ Navas, ML Niinemets, U Oleksyn, J Osada, N Poorter, H Poot, P Prior, L Pyankov, VI Roumet, C Thomas, SC Tjoelker, MG Veneklaas, EJ Villar, R AF Wright, IJ Reich, PB Westoby, M Ackerly, DD Baruch, Z Bongers, F Cavender-Bares, J Chapin, T Cornelissen, JHC Diemer, M Flexas, J Garnier, E Groom, PK Gulias, J Hikosaka, K Lamont, BB Lee, T Lee, W Lusk, C Midgley, JJ Navas, ML Niinemets, U Oleksyn, J Osada, N Poorter, H Poot, P Prior, L Pyankov, VI Roumet, C Thomas, SC Tjoelker, MG Veneklaas, EJ Villar, R TI The worldwide leaf economics spectrum SO NATURE LA English DT Article ID PHOTOSYNTHESIS-NITROGEN RELATIONS; LIFE-SPAN; FUNCTIONAL-GROUPS; USE EFFICIENCY; HIGH-RAINFALL; DRY MASS; AREA; TREE; NUTRIENT; LEAVES AB Bringing together leaf trait data spanning 2,548 species and 175 sites we describe, for the first time at global scale, a universal spectrum of leaf economics consisting of key chemical, structural and physiological properties. The spectrum runs from quick to slow return on investments of nutrients and dry mass in leaves, and operates largely independently of growth form, plant functional type or biome. Categories along the spectrum would, in general, describe leaf economic variation at the global scale better than plant functional types, because functional types overlap substantially in their leaf traits. Overall, modulation of leaf traits and trait relationships by climate is surprisingly modest, although some striking and significant patterns can be seen. Reliable quantification of the leaf economics spectrum and its interaction with climate will prove valuable for modelling nutrient fluxes and vegetation boundaries under changing land-use and climate. C1 Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA. Univ Simon Bolivar, Dept Estudios Ambientales, Caracas 1080, Venezuela. Wageningen Univ, Forest Ecol & Forest Management Grp, Dept Environm Sci, NL-6700 AH Wageningen, Netherlands. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. Vrije Univ Amsterdam, Inst Ecol Sci, Dept Syst Ecol, NL-1081 HV Amsterdam, Netherlands. Univ Zurich, Inst Umwelwissensch, Zurich, Switzerland. Univ Illes Balears, Dept Biol, Lab Fisiol Vegetal, Palma de Mallorca 07122, Illes Balears, Spain. Ctr Ecol Fonct & Evolut, CNRS, UMR 5175, F-34293 Montpellier 5, France. Curtin Univ Technol, Dept Environm Biol, Perth, WA 6845, Australia. Tohoku Univ, Grad Sch Life Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. Univ Wisconsin, Dept Biol, Eau Claire, WI 54702 USA. Landcare Res, Dunedin, New Zealand. Univ Concepcion, Dept Bot, Concepcion, Chile. Univ Cape Town, Dept Bot, ZA-7701 Rondebosch, South Africa. Univ Tartu, Dept Plant Physiol, EE-51011 Tartu, Estonia. Polish Acad Sci, Inst Dendrol, PL-62035 Kornik, Poland. Univ Tokyo, Nikko Bot Garden, Grad Sch Sci, Nikko, Tochigi 3211435, Japan. Univ Utrecht, NL-3508 TB Utrecht, Netherlands. Univ Western Australia, Sch Plant Biol, Crawley, WA 6009, Australia. Charles Darwin Univ, Key Ctr Wildlife Management, Darwin, NT 0909, Australia. Ural State Univ, Ekaterinburg, Russia. Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada. Texas A&M Univ, Dept Forest Sci, College Stn, TX 77843 USA. Univ Cordoba, Area Ecol, E-14071 Cordoba, Spain. RP Wright, IJ (reprint author), Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. EM iwright@rna.bio.mq.edu.au RI Flexas, Jaume/C-1898-2012; Gulias, Javier/N-7240-2013; Niinemets, Ulo/A-3816-2008; Thomas, Sean/B-6089-2008; Ackerly, David/A-1247-2009; Veneklaas, Erik/C-8907-2009; Poorter, Hendrik/B-8062-2010; Poot, Pieter/B-3457-2011; Prior, Lynda/A-7460-2012; Garnier, Eric/D-1650-2012; Oleksyn, Jacek/I-4539-2012; Osada, Noriyuki/K-2946-2012; Hikosaka, Kouki/A-5415-2013; Cavender-Bares, Jeannine/K-5716-2013; Wright, Ian/G-4979-2012; Villar, Rafael/F-7507-2010; Tjoelker, Mark/M-2413-2016 OI Niinemets, Ulo/0000-0002-3078-2192; Ackerly, David/0000-0002-1847-7398; Veneklaas, Erik/0000-0002-7030-4056; Poorter, Hendrik/0000-0001-9900-2433; Prior, Lynda/0000-0002-5511-2320; Garnier, Eric/0000-0002-9392-5154; Hikosaka, Kouki/0000-0003-1744-3775; Wright, Ian/0000-0001-8338-9143; Villar, Rafael/0000-0002-3895-9984; Tjoelker, Mark/0000-0003-4607-5238 NR 50 TC 2313 Z9 2605 U1 150 U2 1420 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 22 PY 2004 VL 428 IS 6985 BP 821 EP 827 DI 10.1038/nature02403 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 814CH UT WOS:000220952300031 PM 15103368 ER PT J AU Hall, JPW Robbins, RK Harvey, DJ AF Hall, JPW Robbins, RK Harvey, DJ TI Extinction and biogeography in the Caribbean: new evidence from a fossil riodinid butterfly in Dominican amber SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE amber fossils; biogeography; Dominican Republic; extinction; Riodinidae; Voltinia ID LEPIDOPTERA; VERTEBRATES; REGION; AGE AB We describe a new species of extinct riodinid butterfly, Voltinia dranaba, from Oligo-Miocene Dominican amber (15-25 Myr ago). This appears to be the first butterfly to be taxonomically described from amber, and the first adult riodinid fossil. The series of five specimens represents probably the best-preserved fossil record for any lepidopteran. The phenomenon of extant Voltinia females ovipositing on arboreal epiphytes probably explains the discovery of multiple female V dramba specimens in amber. Voltinia dramba appears to be one of many extinct butterfly species on Hispaniola. The northwestern Mexican distribution of the explicitly hypothesized sister species, the extant V. danforthi, supports the hypothesis that V dranaba reached Hispaniola by the `proto-Greater Antillean arc', dating the divergence of V. dramba and V. danforthi to 40-50 Myr ago. This date is contemporaneous with the oldest known butterfly fossils, and implies a more ancient date of origin for many of the higher-level butterfly taxa than is often conceded. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM hall.jason@nmnh.si.edu NR 42 TC 22 Z9 27 U1 0 U2 3 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 22 PY 2004 VL 271 IS 1541 BP 797 EP 801 DI 10.1098/rspb.2004.2691 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 813IM UT WOS:000220900800004 PM 15255097 ER PT J AU Ashenberg, J Lorenzini, EC AF Ashenberg, J Lorenzini, EC TI Analytical formulation of a complex mutual gravitational field SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID STEP EXPERIMENT; RELEVANCE AB The mutual gravitational potential for proximate bodies with an arbitrary mass topology is investigated. The current research is motivated by an experiment for the verification of the equivalence principle in gravitation. The gravitation model for the experiment is complex and requires high precision. The proposed methodology is to formulate the potential in terms of inertial integrals and the so-called outer integrals. The method is general and can represent any gravitational configuration. Approximating the outer integrals by radial basis functions reduces the complexity for a real-time dynamical simulation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Radio & Geoastron Div, Cambridge, MA USA. RP Ashenberg, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 2 Z9 2 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD APR 21 PY 2004 VL 21 IS 8 BP 2089 EP 2100 AR PII S0264-9381(04)70859-X DI 10.1088/0264-9381/21/8/012 PG 12 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 822GS UT WOS:000221527700013 ER PT J AU Green, PJ Aldcroft, TL Brown, WR Kuhn, O Saha, A AF Green, PJ Aldcroft, TL Brown, WR Kuhn, O Saha, A TI HS 1216+5032: a physical quasar pair with one radio-loud broad absorption line quasar SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; quasars : absorption lines; quasars : individual : HS 1216+5032; X-rays : general; X-rays : individual : HS 1216+5032. ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; STELLAR OBJECTS; EMISSION-LINE; CHANDRA OBSERVATIONS; COMPLETE SAMPLE; BINARY QUASARS; HS 1216+5032; DARK LENS AB We report on new multiwavelength observations of HS 1216+5032, a pair of quasi-stellar objects (QSOs) at z = 1.45 separated by 9.1 arcsec, which has been a perennial candidate for a massive dark lens. We explore high signal-to-noise ratio optical spectra from the MMT of both components, which show that aside from the effects of absorption, the emission-line profiles are quite similar. Near-infrared spectra from the United Kingdom Infrared Telescope show identical velocities in Hoe emission, but a significant difference in the strength of the narrow component, which is difficult to explain in a lens scenario. We highlight that, based on data from the Very Large Array Faint Images of the Radio Sky survey, HS 1216+5032B is a radio-loud broad absorption line QSO, which certifies HS 1216+5032 as a physical quasar pair. Intriguingly, both quasars show spectroscopic evidence for high accretion rates and large Eddington ratios L/L-Edd, supporting the hypothesis that close galaxy interactions trigger nuclear activity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Joint Astron Ctr, Hilo, HI 96720 USA. Natl Opt Astron Observ, Kitt Peak Natl Observ, Tucson, AZ 85726 USA. RP Green, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pgreen@cfa.harvard.edu NR 44 TC 1 Z9 1 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2004 VL 349 IS 4 BP 1261 EP 1266 DI 10.1111/j.1365-2966.2004.07592.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 815RF UT WOS:000221058700010 ER PT J AU Yoshida, N Bromm, V Hernquist, L AF Yoshida, N Bromm, V Hernquist, L TI The era of massive Population III stars: Cosmological implications and self-termination SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; galaxies : formation; intergalactic medium; stars : formation ID COLD DARK-MATTER; MICROWAVE-ANISOTROPY-PROBE; METAL-POOR STARS; SUPERMASSIVE BLACK-HOLES; 1ST STARS; INTERGALACTIC MEDIUM; GALAXY FORMATION; HIGH-REDSHIFT; LY-ALPHA; REIONIZATION HISTORY AB The birth and death of the first generation of stars have important implications for the thermal state and chemical properties of the intergalactic medium (IGM) in the early universe. Sometime after recombination, the neutral chemically pristine gas was reionized by ultraviolet photons emitted from the first stars but was also enriched with heavy elements when these stars ended their lives as energetic supernovae. Using the results from previous high-resolution cosmological simulations of early structure formation that include radiative transfer, we show that a significant volume fraction of the IGM can be metal polluted, as well as ionized, by massive Population III stars formed in small-mass (similar to10(6)-10(7) M-circle dot) halos early on. If most of the early generation stars die as pair-instability supernovae with energies up to similar to10(53) ergs, the volume-averaged mean metallicity will quickly reach Z similar to 10(-4) Z(circle dot) by a redshift of similar to15-20, possibly causing a transition to the formation of a stellar population that is dominated by low-mass stars. In this scenario, the early chemical enrichment history should closely trace the reionization history of the IGM, and the end of the Population III era is marked by the completion of reionization and preenrichment by z similar to 15. We conclude that, while the preenrichment may partially account for the "metallicity floor" in high-redshift Lyalpha clouds, it does not significantly affect the elemental abundance in the intracluster medium. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nyoshida@cfa.harvard.edu; vbromm@cfa.harvard.edu; lars@cfa.harvard.edu RI Yoshida, Naoki/A-4305-2011 NR 138 TC 104 Z9 104 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 20 PY 2004 VL 605 IS 2 BP 579 EP 590 DI 10.1086/382499 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WL UT WOS:000220801900001 ER PT J AU Munoz, JA Falco, EE Kochanek, CS McLeod, BA Mediavilla, E AF Munoz, JA Falco, EE Kochanek, CS McLeod, BA Mediavilla, E TI The extinction law in high-redshift galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; dust, extinction; galaxies : ISM; gravitational lensing ID ULTRAVIOLET LUMINOSITY DENSITY; GRAVITATIONAL LENS GALAXIES; LARGE-MAGELLANIC-CLOUD; INTERSTELLAR EXTINCTION; STARBURST GALAXIES; EINSTEIN RING; IA SUPERNOVAE; MILKY-WAY; DUST; ABSORPTION AB We estimate the dust extinction laws in two intermediate-redshift galaxies. The dust in the lens galaxy of LBQS 1009-0252, which has an estimated lens redshift of z(l) similar or equal to 0: 88, appears to be similar to that of the SMC, with no significant feature at 2175 Angstrom. Only if the lens galaxy is at a redshift of z(l) similar or equal to 0.3, which is completely inconsistent with the galaxy colors, luminosity, and location on the fundamental plane, can the data be fitted with a normal Galactic extinction curve. The dust in the z(l) = 0.68 lens galaxy for B028+357, whose reddened image lies behind a molecular cloud, requires a very flat ultraviolet extinction curve with (formally) R-V = 12+2. Both lens systems seem to have unusual extinction curves by Galactic standards. C1 Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. RP Munoz, JA (reprint author), Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. EM jmunoz@uv.es NR 50 TC 37 Z9 37 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2004 VL 605 IS 2 BP 614 EP 619 DI 10.1086/382500 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WL UT WOS:000220801900005 ER PT J AU Govoni, F Markevitch, M Vikhlinin, A VanSpeybroeck, L Feretti, L Giovannini, G AF Govoni, F Markevitch, M Vikhlinin, A VanSpeybroeck, L Feretti, L Giovannini, G TI Chandra temperature maps for galaxy clusters with radio halos SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; intergalactic medium; radio continuum : galaxies; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; HOTTEST KNOWN CLUSTER; VLA SKY SURVEY; DARK-MATTER; PARTICLE-ACCELERATION; INTERGALACTIC MEDIUM; MERGING CLUSTERS; RELIC CANDIDATES; MERGER SHOCKS; COMA CLUSTER AB We analyze Chandra temperature maps for a sample of clusters with high-quality radio halo data to study the origin of the radio halos. The sample includes A520, A665, A754, A773, A1914, A2163, A2218, A2319, and 1E 0657-56. We present new temperature maps for all but two of them (A520 and A754). All these clusters exhibit distorted X-ray morphology and strong gas temperature variations indicating ongoing mergers. Some clusters, e. g., A520, A665, 1E 0657-56, exhibit the previously reported spatial correlation between the radio halo brightness and the hot gas regions. However, it is not a general feature. While most mergers are too messy to allow us to disentangle the projection effects, we find clear counterexamples (e.g., A754 and A773) in which the hottest gas regions do not exhibit radio emission at the present sensitivity level. This cannot be explained by projection effects and therefore argues against merger shocks - at least those relatively weak ones responsible for the observed temperature structure in most clusters - as the main mechanism for the halo generation. This leaves merger-generated turbulence as a more likely mechanism. The two clusters with the clearest radio brightness temperature correlation, A520 and 1E 0657-56, are both mergers in which a small dense subcluster has just passed through the main cluster, very likely generating turbulence in its wake. The maximum radio brightness and the hot gas are both seen in these wake regions. On the other hand, the halos in 1E 0657-56 and A665 ( both high-velocity mergers) extend into the shock regions in front of the subclusters, where no strong turbulence is expected. Thus, in high-velocity (M similar or equal to 2-3) mergers, both shock and turbulence acceleration mechanisms may be significant. C1 CNR, Ist Radioastron, I-40129 Bologna, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Govoni, F (reprint author), CNR, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. OI Feretti, Luigina/0000-0003-0312-6285; Govoni, Federica/0000-0003-3644-3084; Giovannini, Gabriele/0000-0003-4916-6362 NR 86 TC 122 Z9 122 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2004 VL 605 IS 2 BP 695 EP 708 DI 10.1086/382674 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WL UT WOS:000220801900015 ER PT J AU Sun, M Seward, FD Smith, RK Slane, PO AF Sun, M Seward, FD Smith, RK Slane, PO TI Chandra view of Kesteven 79: A nearly isothermal supernova remnant with rich spatial structure SO ASTROPHYSICAL JOURNAL LA English DT Article DE conduction; ISM : individual (Kesteven 79); stars : winds, outflows; supernova remnants; X-rays : ISM ID WIND-DRIVEN BUBBLES; ASCA OBSERVATIONS; MOLECULAR CLOUDS; THERMAL CONDUCTION; EVOLUTION; G33.6+0.1; SHELL; EXPLOSIONS; MORPHOLOGY; KES-79 AB A 30 ks Chandra ACIS-I observation of Kes 79 reveals rich spatial structures, including many filaments, three partial shells, a loop, and a "protrusion." Most of them have corresponding radio features. Regardless of the different results from two nonequilibrium ionization (NEI) codes, temperatures of different parts of the remnant are all around 0.7 keV, which is surprisingly constant for a remnant with such rich structure. If thermal conduction is responsible for smoothing the temperature gradient, a lower limit on the thermal conductivity of similar to1/10 of the Spitzer value can be derived. Thus, thermal conduction may play an important role in the evolution of at least some supernova remnants (SNRs). No spectral signature of the ejecta is found, which suggests that the ejecta material has been well mixed with the ambient medium. From the morphology and the spectral properties, we suggest that the bright inner shell is a wind-driven shell (WDS) overtaken by the blast wave ( the outer shell) and estimate the age of the remnant to be similar to6 kyr for the assumed dynamics. Projection is also required to explain the complicated morphology of Kes 79. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msun@cfa.harvard.edu NR 33 TC 30 Z9 30 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2004 VL 605 IS 2 BP 742 EP 750 DI 10.1086/382666 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WL UT WOS:000220801900019 ER PT J AU Anglada, G Rodriguez, LF Osorio, M Torrelles, JM Estalella, R Beltran, MT Ho, PTP AF Anglada, G Rodriguez, LF Osorio, M Torrelles, JM Estalella, R Beltran, MT Ho, PTP TI A single circumstellar disk in the SVS 13 close binary system SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (HH 7-11, NGC 1333; SVS 13); ISM : jets and outflows; radio continuum : ISM; stars : formation ID HERBIG-HARO OBJECTS; HH 7-11 REGION; EXCITING SOURCE; PROPER MOTIONS; NGC 1333; STAR; VARIABILITY; CONTINUUM; L1551-IRS-5; ACCRETION AB We present Very Large Array observations at 7 mm of the sources IRAS 2A, IRAS 2B, MMS 2, MMS 3, and SVS 13, in the NGC 1333 region. SVS 13 is a young close binary system whose components are separated by 65 AU in projection. Our high angular resolution observations reveal that only one of the components of the SVS 13 system (VLA 4B) is associated with detectable circumstellar dust emission. This result is in contrast with the well-known case of L1551 IRS 5, a binary system of two protostars separated by 45 AU, where each component is associated with a disk of dust. In both SVS 13 and in L1551 IRS 5 the emission apparently arises from compact accretion disks, smaller than those observed around single stars, but still massive enough to form planetary systems like the solar one. These observational results confirm that the formation of planets can occur in close binary systems, either in one or in both components of the system, depending on the specific angular momentum of the infalling material. C1 CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. CSIC, IEEC, Inst Ciencias Espacio, ES-08034 Barcelona, Spain. Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. RP Anglada, G (reprint author), CSIC, Inst Astrofis Andalucia, Camino Bajo de Huetor 24, E-18008 Granada, Spain. EM guillem@iaa.es; l.rodriguez@astrosmo.unam.mx; osorio@iaa.es; torrelles@ieec.fcr.es; robert@am.ub.es; mbeltran@arcetri.astro.it; ho@cfa.harvard.edu OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626; Torrelles, Jose Maria/0000-0002-6896-6085 NR 31 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2004 VL 605 IS 2 BP L137 EP L140 DI 10.1086/420782 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WM UT WOS:000220802000013 ER PT J AU Grav, T Holman, MJ AF Grav, T Holman, MJ TI Near-infrared photometry of the irregular satellites of Jupiter and Saturn SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites : general; planets and satellites : individual (Ananke, Himalia, Pasiphae, Phoebe, Sinope) ID ASTEROID SPECTROSCOPIC SURVEY; STANDARD STARS; GAS-DRAG; PHOEBE; BELT; CAPTURE; SYSTEM AB We present JHK(s) photometry of 10 Jovian and four Saturnian irregular satellites, taken with the Near-InfraRed Imager at the 8 m Gemini North Observatory on Mauna Kea, Hawaii. The observed objects have near-infrared colors consistent with C-, P-, and D-type asteroids, although J XII Ananke and S IX Phoebe show weak indications of possible water features in the H filter. The four members of the Himalia family have similar near-infrared colors, as do the two members of the Gallic family, S XX Paaliaq and S XXIX Siarnaq. From low-resolution, normalized reflectance spectra based on the broadband colors and covering 0.4-2.2 mum, the irregular satellites are identified as C-type (J VII Pasiphae, J VI Himalia, and S IX Phoebe), P- type (J XII Ananke and J XVIII Themisto), and D-type (J IX Carme and J X Sinope), showing a diversity of origins for these objects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grav, T (reprint author), Univ Oslo, N-0316 Oslo, Norway. EM tgrav@cfa.harvard.edu; mholman@cfa.harvard.edu NR 25 TC 14 Z9 14 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2004 VL 605 IS 2 BP L141 EP L144 DI 10.1086/420881 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WM UT WOS:000220802000014 ER PT J AU Metcalfe, TS Montgomery, MH Kanaan, A AF Metcalfe, TS Montgomery, MH Kanaan, A TI Testing white dwarf crystallization theory with asteroseismology of the massive pulsating DA star BPM 37093 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : evolution; stars : individual (BPM 37093); stars : interiors; stars : oscillations; white dwarfs ID ZZ-CETI STARS; OPTICAL SPECTROSCOPY; DISCOVERY; EVOLUTION; MODELS AB It was predicted more than 40 years ago that the cores of the coolest white dwarf stars should eventually crystallize. This effect is one of the largest sources of uncertainty in white dwarf cooling models, which are now routinely used to estimate the ages of stellar populations in both the Galactic disk and the Galactic halo. We are attempting to minimize this source of uncertainty by calibrating the models, using observations of pulsating white dwarfs. In a typical mass white dwarf model, crystallization does not begin until the surface temperature reaches 6000-8000 K. In more massive white dwarf models, the effect begins at higher surface temperatures, where pulsations are observed in the ZZ Ceti (DAV) stars. We use the observed pulsation periods of BPM 37093, the most massive DAV white dwarf presently known, to probe the interior and determine the size of the crystallized core empirically. Our initial exploration of the models strongly suggests the presence of a solid core containing about 90% of the stellar mass, which is consistent with our theoretical expectations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. RP Metcalfe, TS (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 16,60 Garden St, Cambridge, MA 02138 USA. RI Metcalfe, Travis/A-9388-2008 OI Metcalfe, Travis/0000-0003-4034-0416 NR 32 TC 44 Z9 44 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2004 VL 605 IS 2 BP L133 EP L136 DI 10.1086/420884 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WM UT WOS:000220802000012 ER PT J AU Rots, AH Jahoda, K Lyne, AG AF Rots, AH Jahoda, K Lyne, AG TI Absolute timing of the Crab pulsar with the Rossi X-ray Timing Explorer SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (Crab pulsar); X-rays : stars ID RADIO; EMISSION AB We have monitored the phase of the main X-ray pulse of the Crab pulsar with the Rossi X-Ray Timing Explorer (RXTE) for almost 8 years, since the start of the mission in 1996 January. The absolute time of RXTE's clock is sufficiently accurate to allow this phase to be compared directly with the radio profile. Our monitoring observations of the pulsar took place bi-weekly (during the periods when it was at least 30degrees from the Sun), and we correlated the data with radio timing ephemerides derived from observations made at Jodrell Bank. We have determined the phase of the X-ray main pulse for each observation with a typical error in the individual data points of 50 mus. The total ensemble is consistent with a phase that is constant over the monitoring period, with the X-ray pulse leading the radio pulse by 0.0102 +/- 0.0012 periods in phase, or 344 +/- 40 mus in time. The error estimate is dominated by a systematic error of 40 ms in the radio data, arising from uncertainties in the variable amount of pulse delay due to interstellar scattering and instrumental calibration. The statistical error is 0.00015 periods, or 5 mus. The separation of the main pulse and interpulse appears to be unchanging at timescales of a year or less, with an average value of 0.4001 +/- 0.0002 periods. There is no apparent variation in these values with energy over the 2-30 keV range. The lag between the radio and X-ray pulses may be constant in phase (i.e., rotational in nature) or constant in time (i.e., due to a path-length difference). We are not (yet) able to distinguish between these two interpretations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Manchester, Dept Phys & Astron, Jodrell Bank, Macclesfield SK11 9DL, Cheshire, England. RP Rots, AH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 67, Cambridge, MA 02138 USA. EM arots@head.cfa.harvard.edu RI Jahoda, Keith/D-5616-2012; OI Rots, Arnold/0000-0003-2377-2356 NR 16 TC 50 Z9 50 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2004 VL 605 IS 2 BP L129 EP L132 DI 10.1086/420842 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WM UT WOS:000220802000011 ER PT J AU Schwartz, DA Silverman, J Birkinshaw, M Karovska, M Aldcroft, T Barkhouse, W Green, P Kim, DW Wilkes, BJ Worrall, DM AF Schwartz, DA Silverman, J Birkinshaw, M Karovska, M Aldcroft, T Barkhouse, W Green, P Kim, DW Wilkes, BJ Worrall, DM TI Discovery of a jetlike structure at the high-redshift QSO CXOMP J084128.3+131107 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : general; X-rays : galaxies ID X-RAY JET; CHANDRA MULTIWAVELENGTH PROJECT; ACTIVE GALACTIC NUCLEI; EMISSION; CLUSTERS; SPECTRUM; 3C-273 AB The Chandra Multiwavelength Project has discovered a jetlike structure associated with a newly recognized QSO at redshift z = 1.866. The system was 9'.4 off-axis during an observation of 3C 207. Although significantly distorted by the mirror point-spread function, we use both a ray trace and a nearby bright point source to show that the X-ray image must arise from some combination of point and extended sources, or else from a minimum of three distinct point sources. We favor the former situation, as three unrelated sources would have a small probability of occurring by chance in such a close alignment. We show that interpretation as a jet emitting X-rays via inverse Compton scattering on the cosmic microwave background is plausible. This would be a surprising and unique discovery of a radio-quiet QSO with an X-ray jet, since we have obtained upper limits of 100 muJy on the QSO emission at 8.46 GHz and limits of 200 muJy for emission from the putative jet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM das@head.cfa.harvard.edu OI Wilkes, Belinda/0000-0003-1809-2364 NR 20 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2004 VL 605 IS 2 BP L105 EP L108 DI 10.1086/420843 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WM UT WOS:000220802000005 ER PT J AU Schroll, S AF Schroll, S TI Decoys and disruptions: Selected writings, 1975-2001. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 15 PY 2004 VL 129 IS 7 BP 81 EP 81 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 837VK UT WOS:000222668900039 ER PT J AU Hutchinson, A AF Hutchinson, A TI Do animals think? SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Hutchinson, A (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 15 PY 2004 VL 129 IS 7 BP 120 EP 120 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 837VK UT WOS:000222668900229 ER PT J AU Olszewski, TD Erwin, DH AF Olszewski, TD Erwin, DH TI Dynamic response of Permian brachiopod communities to long-term environmental change SO NATURE LA English DT Article ID SPECIES-ABUNDANCE; NEUTRAL THEORY; BIODIVERSITY; ECOLOGY; MODEL AB The fossil record preserves numerous natural experiments that can shed light on the response of ecological communities to environmental change. However, directly observing the community dynamics of extinct organisms is not possible. As an alternative, neutral ecological models(1-3) suggest that species abundance distributions reflect dynamical processes like migration, competition, recruitment, and extinction. Live-dead comparisons suggest that such distributions can be faithfully preserved in the rock record(4). Here we use a maximum-likelihood approach to show that brachiopod (lamp shell) abundance distributions from four temporally distinct ecological landscapes from the Glass Mountains, Texas (of the Permian period), exhibit significant differences. Further, all four are better fitted by zero-sum multinomial distributions, characteristic of Hubbell's neutral model(2), than by log-normal distributions, as predicted by the traditional ecological null hypothesis(5). Using the neutral model as a guide, we suggest that sea level fluctuations spanning about 10 Myr altered the degrees of isolation and exchange among local communities within these ecological landscapes. Neither these long-term environmental changes nor higher-frequency sea level fluctuations resulted in wholesale extinction or major innovation within evolutionary lineages. C1 Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA. Smithsonian Inst, Dept Paleobiol, NMNH, Washington, DC 20013 USA. Santa Fe Inst, Santa Fe, NM 87501 USA. RP Olszewski, TD (reprint author), Texas A&M Univ, Dept Geol & Geophys, 3115 TAMU, College Stn, TX 77843 USA. EM tomo@geo.tamu.edu RI Erwin, Douglas/A-9668-2009; OI Olszewski, Thomas/0000-0002-0179-6536 NR 30 TC 35 Z9 38 U1 2 U2 14 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 15 PY 2004 VL 428 IS 6984 BP 738 EP 741 DI 10.1038/nature02464 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 812EW UT WOS:000220823800036 PM 15085129 ER PT J AU Graham, LH Swanson, WF Wildt, DE Brown, JL AF Graham, LH Swanson, WF Wildt, DE Brown, JL TI Influence of oral melatonin on natural and gonadotropin-induced ovarian function in the domestic cat SO THERIOGENOLOGY LA English DT Article DE melatonin; domestic cat; artificial insemination; ovary ID PINEAL-GLAND; INVITRO FERTILIZATION; EMBRYO; QUALITY; EMBRYOGENESIS; PHOTOPERIODS; HAMSTER; SYSTEM; PLASMA; SIGNAL AB Ovarian hyperstimulation after exogenous gonadotropin stimulation is believed to be a cause of poor success after artificial insemination (AI) in felids. The objectives of this study were to assess the effect of oral melatonin on endogenous ovarian activity in the domestic cat and subsequent eCG/hCG-induced ovarian activity. Serum melatonin concentrations peaked similar to1 h after a single oral dose of 30 mg melatonin and remained elevated above endogenous day-time concentrations for >8 h. The calculated circulating half-life (mean +/- S.E.M.) of oral melatonin was 45.4 +/- 3.5 min, and the elimination rate constant (k(10)) was 55.2 +/- 4.2 min(-1). Oral melatonin (30 mg per day) administered 3 h before lights-off effectively and reversibly suppressed estrous elevations in fecal estrogens after 25 days of treatment. There was a progressive decrease in baseline estrogen concentrations from inter-estrous concentrations after 25 days of treatment to below inter-estrous concentrations after 35 days of treatment. Oral melatonin treatment (30 mg per day for 30 days) prior to eCG/hCG administration only marginally reduced ancillary follicle development and had no significant effect on the quantity or quality of embryos produced by AI. Thus, oral melatonin effectively inhibited endogenous ovarian activity and had no adverse impact on embryo quality after AI in the domestic cat; however, this treatment was only marginally effective in minimizing eCG/hCG-induced ovarian hyperstimulation. (C) 2003 Elsevier Inc. All rights reserved. C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, Cincinnati, OH USA. RP Graham, LH (reprint author), 361A Old Finch Ave, Scarborough, ON M1B 5K7, Canada. EM endolaura@yahoo.com NR 36 TC 20 Z9 21 U1 0 U2 9 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD APR 15 PY 2004 VL 61 IS 6 BP 1061 EP 1076 DI 10.1016/j.theriogenology.2003.05.004 PG 16 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA 800EC UT WOS:000220010700007 PM 15036995 ER PT J AU Plume, R Kaufman, MJ Neufeld, DA Snell, RL Hollenbach, DJ Goldsmith, PF Howe, J Bergin, EA Melnick, GJ Bensch, F AF Plume, R Kaufman, MJ Neufeld, DA Snell, RL Hollenbach, DJ Goldsmith, PF Howe, J Bergin, EA Melnick, GJ Bensch, F TI Water absorption from line-of-sight clouds toward W49A SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : abundances; ISM : clouds; ISM : individual (W49); ISM : molecules; stars : formation ID WAVE-ASTRONOMY-SATELLITE; H-II-REGIONS; LATITUDE TRANSLUCENT CLOUD; SPIRAL-ARM CLOUDS; DISSOCIATIVE RECOMBINATION; MOLECULAR CLOUD; BRANCHING RATIOS; H2O; EMISSION; ORION AB We have observed six clouds along the line of sight toward W49A using the Submillimeter Wave Astronomy Satellite and several ground-based observatories. The ortho-H2O 1(10) --> 1(01) and OH (1665 and 1667 MHz) transitions are observed in absorption, whereas the low-J CO, (CO)-C-13, and (CO)-O-18 lines, as well as the [C I] P-3(1)-P-3(0) transition, are seen in emission. The emission lines allow us to determine the gas density (n similar to 1500 - 3000 cm(-3)) and CO column densities [N(CO) similar to 7.9 x 10(15)-2.8 x 10(17) cm(-2)] using a standard large velocity gradient analysis. By using both the o-H-2 O-18 and o-H2O absorption lines, we are able to constrain the column-averaged o-H2O abundances in each line-of-sight cloud to within about an order of magnitude. Assuming the standard N(H-2)/N(CO) ratio of 10(4), we find N(o-H2O)/N(H-2) = 8.1 x 10(-8) to 4 x 10(-7) for three clouds with optically thin water lines. In three additional clouds, the H2O lines are saturated, so we have used observations of the (H2O)-O-18 ground-state transition to find upper limits to the water abundance of 8.2 x 10(-8) to 1.5 x 10(-6). We measure the OH abundance from the average of the 1665 and 1667 MHz observations and find N(OH)/N(H-2) = 2.3 x 10(-7) to 1.1 x 10(-6). The o-H2O and OH abundances are similar to those determined for line-of-sight water absorption features toward W51 and Sgr B2 but are higher than those seen from water emission lines in molecular clouds. However, the clouds toward W49 have lower ratios of OH relative to H2O column densities than are predicted by simple models, which assume that dissociative recombination is the primary formation pathway for OH and H2O. Building on the 2002 work of Neufeld and coworkers, we present photochemistry models including additional chemical effects, which can also explain the observed OH and H2O column densities, as well as the observed H2O/CO abundance ratios. C1 Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Cornell Univ, Dept Astron, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Plume, R (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. RI Goldsmith, Paul/H-3159-2016 NR 35 TC 35 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2004 VL 605 IS 1 BP 247 EP 258 DI 10.1086/382204 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WJ UT WOS:000220801700021 ER PT J AU Woods, PM Kaspi, VM Thompson, C Gavriil, FP Marshall, HL Chakrabarty, D Flanagan, K Heyl, J Hernquist, L AF Woods, PM Kaspi, VM Thompson, C Gavriil, FP Marshall, HL Chakrabarty, D Flanagan, K Heyl, J Hernquist, L TI Changes in the X-ray emission from the magnetar candidate 1E 2259+586 during its 2002 outburst SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : general; stars : individual (1E 2259+586); stars : neutron; X-rays : bursts ID SOFT-GAMMA-REPEATER; PULSAR 1E 2259+586; PROPORTIONAL COUNTER ARRAY; VARIABLE SPIN-DOWN; 1998 AUGUST 27; NEUTRON-STARS; SGR 1900+14; VORTEX CREEP; INTERNAL TEMPERATURE; CRAB PULSAR AB An outburst of more than 80 individual bursts, similar to those seen from Soft Gamma Repeaters (SGRs), was detected from the anomalous X-ray pulsar (AXP) 1E 2259+586 in 2002 June. Coincident with this burst activity were gross changes in the pulsed flux, persistent flux, energy spectrum, pulse profile, and spin-down of the underlying X-ray source. We present Rossi X-Ray Timing Explorer and X-Ray Multi-Mirror Mission observations of 1E 2259+586 that show the evolution of the aforementioned source parameters during and following this episode and identify recovery timescales for each. Specifically, we observe an X-ray flux increase (pulsed and phase-averaged) by more than an order of magnitude having two distinct components. The first component is linked to the burst activity and decays within similar to2 days, during which the energy spectrum is considerably harder than during the quiescent state of the source. The second component decays over the year following the glitch according to a power law in time with an exponent -0.22 +/- 001. The pulsed fraction decreased initially to similar to15% rms but recovered rapidly to the preoutburst level of similar to23% within the first 3 days. The pulse profile changed significantly during the outburst and recovered almost fully within 2 months of the outburst. A glitch of size Deltanu(max) / nu = (4.24 +/- 0.11) x 10(-6) was observed in 1E 2259+586, which preceded the observed burst activity. The glitch could not be well fitted with a simple partial exponential recovery. An exponential rise of similar to20% of the frequency jump with a timescale of similar to14 days results in a significantly better fit to the data; however, contamination from a systematic drift in the phase of the pulse profile cannot be excluded. A fraction of the glitch (similar to19%) was recovered in a quasi-exponential manner having a recovery timescale of similar to16 days. The long-term postglitch spin-down rate decreased in magnitude relative to the preglitch value. The changes in the source properties of 1E 2259+586 during its 2002 outburst are shown to be qualitatively similar to changes seen during or following burst activity in two SGRs, thus further solidifying the common nature of SGRs and AXPs as magnetars. The changes in persistent emission properties of 1E 2259+586 suggest that the star underwent a plastic deformation of the crust that simultaneously impacted the superfluid interior (crustal and possibly core superfluid) and the magnetosphere. Finally, the changes in persistent emission properties coincident with burst activity in 1E 2259+586 enabled us to infer previous burst-active episodes from this and other AXPs. The nondetection of these outbursts by all-sky gamma-ray instruments suggests that the number of active magnetar candidates in our Galaxy is larger than previously thought. C1 Univ Space Res Assoc, Huntsville, AL 35805 USA. Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM peter.woods@nsstc.nasa.gov NR 78 TC 138 Z9 138 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 APR 10 PY 2004 VL 605 IS 1 BP 378 EP 399 DI 10.1086/382233 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WJ UT WOS:000220801700033 ER PT J AU Monnier, JD Millan-Gabet, R Tuthill, PG Traub, WA Carleton, NP du Foresto, VC Danchi, WC Lacasse, MG Morel, S Perrin, G Porro, IL Schloerb, FP Townes, CH AF Monnier, JD Millan-Gabet, R Tuthill, PG Traub, WA Carleton, NP du Foresto, VC Danchi, WC Lacasse, MG Morel, S Perrin, G Porro, IL Schloerb, FP Townes, CH TI High-resolution imaging of dust shells by using Keck aperture masking and the IOTA interferometer SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; instrumentation : interferometers; stars : AGB and post-AGB; stars : atmospheres; techniques : interferometric ID BISPECTRUM SPECKLE-INTERFEROMETRY; VY-CANIS-MAJORIS; HERBIG AE/BE STARS; BASE-LINE INTERFEROMETER; YOUNG STELLAR OBJECTS; M-GIANTS; RADIATIVE-TRANSFER; MIRA VARIABLES; PROPER MOTIONS; NML-CYGNI AB We present first results of an experiment to combine data from Keck aperture masking and the Infrared-Optical Telescope Array to image the circumstellar environments of evolved stars with similar to20 mas resolution. The unique combination of excellent Fourier coverage at short baselines and high-quality long-baseline fringe data allows us to determine the location and clumpiness of the innermost hot dust in the envelopes and to measure the diameters of the underlying stars themselves. We find evidence for large-scale inhomogeneities in some dust shells and also significant deviations from uniform brightness for the photospheres of the most evolved M stars. Deviations from spherically symmetric mass loss in the red supergiant NML Cyg could be related to recent evidence for dynamically important magnetic fields and/or stellar rotation. We point out that dust shell asymmetries, like those observed here, can qualitatively explain the difficulty recent workers have had in simultaneously fitting the broadband spectral energy distributions and high-resolution spatial information, without invoking unusual dust properties or multiple distinct shells (from hypothetical "superwinds''). This paper is the first to combine optical interferometry data from multiple facilities for imaging, and we discuss the challenges and potential for the future of this method, given current calibration and software limitations. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Sydney, Dept Phys, Sydney, NSW 2006, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, F-92195 Meudon, France. NASA, Goddard Space Flight Ctr, Infrared Astrophys Branch, Greenbelt, MD 20771 USA. European So Observ, D-85748 Garching, Germany. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Massachusetts, Dept Phys & Astron, Amherst, MA 01003 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Univ Michigan, Dept Astron, 941 Dennison Bldg, Ann Arbor, MI 48109 USA. EM monnier@umich.edu OI Monnier, John D/0000-0002-3380-3307 NR 93 TC 89 Z9 89 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 APR 10 PY 2004 VL 605 IS 1 BP 436 EP 461 DI 10.1086/382218 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WJ UT WOS:000220801700037 ER PT J AU Morgan, H Habbal, SR Li, X AF Morgan, H Habbal, SR Li, X TI Hydrogen Ly alpha intensity oscillations observed by the solar and heliospheric observatory ultraviolet coronagraph spectrometer SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : oscillations; Sun : UV radiation ID TRACE; WAVES; DYNAMICS; REGIONS AB We report on a search for significant oscillations in different coronal structures by applying a wavelet analysis to Solar and Heliospheric Observatory UVCS observations of the hydrogen Lyalpha 1216 Angstrom line intensity taken between 1.5 and 2.2 R.. Significant periodic oscillations, unlikely to be a result of instrumental effects, are shown to exist in a coronal hole, the quiet Sun, and a streamer. Observations made sequentially at different heights but at the same latitude often share similar power spectra. Neighboring pixels at the same radial distance also share similar power spectra. These results indicate both a localized structure to the periodicity and a long-range preservation of oscillation patterns in the radial expansion of the solar wind. We show that a preference for significant oscillations with periods of 7-8 minutes exists in three out of the four observations presented here. Other bands of preferred periodicity are observed at different heights. C1 Prifysgol Cymru, Sefydliad & Gwyddorau Math Ffisegol, Ceredigion SY23 3BZ, Cymru, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Morgan, H (reprint author), Prifysgol Cymru, Sefydliad & Gwyddorau Math Ffisegol, Ceredigion SY23 3BZ, Cymru, Wales. EM hhm01@aber.ac.uk OI Morgan, Huw/0000-0002-6547-5838 NR 12 TC 21 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2004 VL 605 IS 1 BP 521 EP 527 DI 10.1086/382203 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WJ UT WOS:000220801700044 ER PT J AU Weedman, D Charmandaris, V Zezas, A AF Weedman, D Charmandaris, V Zezas, A TI Comparing CHANDRA and SIRTF observations for obscured starbursts and active Galactic nuclei at high redshift (vol 600, pg 106, 2004) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Weedman, D (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RI Charmandaris, Vassilis/A-7196-2008; Zezas, Andreas/C-7543-2011 OI Charmandaris, Vassilis/0000-0002-2688-1956; Zezas, Andreas/0000-0001-8952-676X NR 1 TC 1 Z9 1 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2004 VL 605 IS 1 BP 578 EP 578 DI 10.1086/383142 PN 1 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WJ UT WOS:000220801700051 ER PT J AU Fabbiano, G Baldi, A King, AR Ponman, TJ Raymond, J Read, A Rots, A Schweizer, F Zezas, A AF Fabbiano, G Baldi, A King, AR Ponman, TJ Raymond, J Read, A Rots, A Schweizer, F Zezas, A TI X-raying chemical evolution and galaxy formation in the Antennae SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038/4039); galaxies : interactions; galaxies : peculiar; X-rays : binaries; X-rays : galaxies; X-rays : ISM ID YOUNG STAR-CLUSTERS; CHANDRA OBSERVATIONS; LUMINOSITY FUNCTION; INTERSTELLAR-MEDIUM; NGC 4038/4039; NGC-4038/4039; MULTIWAVELENGTH; WINDS AB We present the integrated 411 ks Chandra ACIS-S exposure of the Antennae galaxies (NGC 4038/39). Besides a rich population of pointlike sources, this spectacular image reveals a spatially and spectrally complex hot diffuse gaseous component. For the first time we detect intense line emission from Fe, Ne, Mg, and Si in the Antennae and obtain a detailed picture of spatially varied metal abundances in the hot interstellar medium (ISM) of a galaxy. In certain regions, the abundances of alpha-elements may be many times solar, while the Fe abundance is subsolar or near-solar. The differences in the local metal enrichment of the hot ISM may be related to the local star formation rates and to the degree of confinement of the enriched hot ISM. We also report large-scale gaseous features, including two gigantic, similar to10 kpc scale "loops" extending to the south of the merging disks and a low surface brightness hot halo, extending out to similar to18 kpc. These features may be related to superwinds from the starburst in the Antennae or result from the merger hydrodynamics. Their long cooling times suggest that they may persist to form the hot X-ray halo of the emerging elliptical galaxy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gfabbiano@cfa.harvard.edu; ark@astro.le.ac.uk; tjp@star.sr.bham.ac.uk; arots@cfa.harvard.edu; schweizer@ociw.edu; azezas@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Rots, Arnold/0000-0003-2377-2356 NR 25 TC 45 Z9 45 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2004 VL 605 IS 1 BP L21 EP L24 DI 10.1086/382688 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WK UT WOS:000220801800006 ER PT J AU Greenhill, LJ Gezari, DY Danchi, WC Najita, J Monnier, JD Tuthill, PG AF Greenhill, LJ Gezari, DY Danchi, WC Najita, J Monnier, JD Tuthill, PG TI High angular resolution mid-infrared imaging of young stars in Orion BN/KL SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : individual (Orion Kleinmann-Low); stars : formation; stars : pre-main-sequence ID MOLECULAR CLOUD; NEBULA CLUSTER; MASSIVE STARS; KL; ENVIRONMENT; EXTINCTION; REGION; IMAGES; IRC2 AB We present Keck Long Wavelength Spectrometer images of the Orion BN/KL star-forming region obtained in the first multiwavelength study to have 0."3 - 0."5 resolution from 4.7 to 22 mum. The young stellar objects designated infrared source n and radio source I are believed to dominate the BN/KL region. We have detected extended emission from a probable accretion disk around source n but infer a stellar luminosity on the order of only 2000 L,. Although source I is believed to be more luminous, we do not detect an infrared counterpart even at the longest wavelengths. However, we resolve the close-by infrared source, IRc2, into an arc of knots similar to10(3) AU long at all wavelengths. Although the physical relation of source I to IRc2 remains ambiguous, we suggest that these sources mark a high-density core (10(7) - 10(8) pc(-3) over similar to10(3) AU) within the larger BN/KL star-forming cluster. The high density may be a consequence of the core being young and heavily embedded. We suggest that the energetics of the BN/KL region may be dominated by this cluster core rather than one or two individual sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM greenhill@cfa.harvard.edu OI Monnier, John D/0000-0002-3380-3307 NR 34 TC 46 Z9 46 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2004 VL 605 IS 1 BP L57 EP L60 DI 10.1086/386544 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WK UT WOS:000220801800015 ER PT J AU Kukolich, SG McCarthy, MC Thaddeus, P AF Kukolich, SG McCarthy, MC Thaddeus, P TI Molecular structure of o-benzyne from microwave measurements SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID CARBON CHAINS; PHOTOELECTRON-SPECTROSCOPY; PHENYL-LITHIUM; AB-INITIO; SPECTRUM; CHEMISTRY; SPACE AB The o-benzyne molecule has been known for many years to be an important, but short-lived,, reaction intermediate in substitution reactions and more recently in cyclization reactions of enediynes. Although there has been widespread interest in this transient molecule, previous experimental structural data were very limited. In the present work, rotational transitions for o-benzyne were measured with a pulsed-beam, Fourier transform microwave spectrometer for all unique, singly substituted C-13 and single-D isotopomers. The o-benzyne was efficiently produced by flowing a dilute mixture of isotopically enriched benzene in neon through a pulsed-DC discharge beam source. The new data, combined with previous data for the normal isotopomer, provide a complete set of structural parameters for this molecule. The r(s) substitution coordinates and the coordinates from a least-squares fit are reported and are in good agreement. When using the least-squares fit to obtain structural parameters, correction terms arising from harmonic terms in the vibrational averaging were subtracted from the measured rotational constants to obtain a better representation of the planar equilibrium structure. Further improvements in the fits were obtained by applying small, mass-dependent adjustments to the atom coordinates. Structural parameters obtained from the fit to these modified rotational constants are an acetylenic C(1)equivalent toC(2) bond length of 1.264(3) Angstrom, and the other bond lengths C-2-C-3 1.390(3) Angstrom, C-3-C-4 = 1.403(3) Angstrom, C-4-C-5 = 1.404(3) Angstrom, C-3-H-1 = 1.095(9) Angstrom, and C-4-H-2 = 1.099(4) The C(1)equivalent toC(2) bond is only 0.057 Angstrom longer than the free acetylene bond. The other C-C bond lengths are within 0.01 Angstrom of those of benzene C-C bonds. New spectral data for the single-D isotopomers were used to obtain better values for the deuterium quadrupole coupling. Bond-axis deuterium quadrupole coupling constants are eQq(zz)(D-1) = 188(2) kHz, and eQq(zz)(D-2) = 185(10) kHz, which agree well with the value for benzene-D-1. The new structural parameters are compared here with theoretical parameters and with an NMR measurement of the C-1-C-2 bond length. C1 Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Kukolich, SG (reprint author), Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 29 TC 14 Z9 14 U1 3 U2 9 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD APR 8 PY 2004 VL 108 IS 14 BP 2645 EP 2651 DI 10.1021/jp031344p PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 809ME UT WOS:000220640000010 ER PT J AU McCarthy, MC Thorwirth, S Gottlieb, CA Thaddeus, P AF McCarthy, MC Thorwirth, S Gottlieb, CA Thaddeus, P TI The rotational spectrum and geometrical structure of thiozone, S-3 SO JOURNAL OF THE AMERICAN CHEMICAL SOCIETY LA English DT Article ID SOLID ARGON; SULFUR; ATMOSPHERE; VENUS; S4; S3 C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 NR 27 TC 36 Z9 36 U1 1 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0002-7863 J9 J AM CHEM SOC JI J. Am. Chem. Soc. PD APR 7 PY 2004 VL 126 IS 13 BP 4096 EP 4097 DI 10.1021/ja049645f PG 2 WC Chemistry, Multidisciplinary SC Chemistry GA 809LB UT WOS:000220637100023 PM 15053585 ER PT J AU Jones, ER Wishnie, MH Deago, J Sautu, A Cerezo, A AF Jones, ER Wishnie, MH Deago, J Sautu, A Cerezo, A TI Facilitating natural regeneration in Saccharum spontaneum (L.) grasslands within the Panama Canal Watershed: effects of tree species and tree structure on vegetation recruitment patterns SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Saccharum spontaneum; inga punctata; M. calabura; A. excelsum; cordia spp.; D. panamensis; H. crepitans; L. seemannii; understory development; natural regeneration; reforestation; tropical plantations; Panama; Panama Canal Watershed ID NATIVE FOREST REGENERATION; DEGRADED TROPICAL LANDS; OLD FIELD VEGETATION; COSTA-RICA; PUERTO-RICO; OVERSTORY COMPOSITION; WOODY REGENERATION; ABANDONED PASTURE; SEED DISPERSAL; MONTANE FOREST AB To counteract the escalating rates of tropical deforestation, it is essential that we not only minimize forest loss, but that we create effective reforestation strategies. This study investigates understory recruitment patterns in mixed native species plantations along the Panama Canal that were established in grasslands dominated by the invasive exotic species Saccharum spontaneum (L.) Graminae. We test the hypothesis that regeneration rates vary significantly by overstory tree species and overstory tree structure, and explore the mechanisms generating such patterns. Of the seven tree species sampled, Inga spp. recruits significantly more tree seedlings than any other species. Additionally, crown foliage density appears to be the most significant structural factor determining rates of understory tree species regeneration. A survey of bird activity in the plantations and in unplanted areas indicates that birds generally visit large trees and that those tree species most frequently visited by birds also have the greatest density of understory tree seedlings. These results support the hypothesis that tree structure significantly affects regeneration patterns, and suggests that bird dispersal may be a fundamental driver in seedling recruitment. Furthermore, results indicate that the presence of any tree species in a reforestation plot increases the understory species richness and species cover relative to non-reforested areas, while significantly reducing the degree of S. spontaneum dominance. While active reforestation appears to facilitate forest regeneration in areas occupied in S. spontaneum, tree species and tree structure are important factors to consider when designing reforestation programs that are intended to facilitate natural regeneration. (C) 2003 Elsevier B.V. All rights reserved. C1 Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, PRORENA, Native Species Reforestn Project, Miami, FL 34002 USA. PCC, ESMW, Panama Canal Author, Miami, FL 33102 USA. RP Wishnie, MH (reprint author), Yale Univ, Sch Forestry & Environm Studies, B2-205 Prospect St, New Haven, CT 06511 USA. EM mark.wishnie@yale.edu NR 51 TC 33 Z9 34 U1 3 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD APR 5 PY 2004 VL 191 IS 1-3 BP 171 EP 183 DI 10.1016/j.foreco.2003.12.002 PG 13 WC Forestry SC Forestry GA 806TN UT WOS:000220456300013 ER PT J AU Vrinceanu, D Granger, BE Parrott, R Sadeghpour, HR Cederbaum, LS Mody, A Tan, J Gabrielse, G AF Vrinceanu, D Granger, BE Parrott, R Sadeghpour, HR Cederbaum, LS Mody, A Tan, J Gabrielse, G TI Strongly magnetized antihydrogen and its field ionization SO PHYSICAL REVIEW LETTERS LA English DT Article ID HYDROGEN-ATOM; EXCITED ATOMS; SEPARATION; PLASMA AB Internal orbits of experimentally analyzed antihydrogen ((H) over bar) atoms depend as much on an external magnetic field as on the Coulomb force. A circular "guiding center atom" model is used to understand their field ionization. This useful model, assumed in the theory of three-body (H) over bar recombination so far, ignores the important coupling between internal and center-of-mass motion. A conserved pseudomomentum, effective potential, saddle point analysis, and numerical simulation show where the simple model is valid and classify the features of the general case, including "giant dipole states." C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Theoret Chem Phys Chem Inst, Heidelberg, Germany. RP Vrinceanu, D (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 22 TC 29 Z9 29 U1 0 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD APR 2 PY 2004 VL 92 IS 13 AR 133402 DI 10.1103/PhysRevLett.92.133402 PG 4 WC Physics, Multidisciplinary SC Physics GA 808ZE UT WOS:000220606200027 PM 15089611 ER PT J AU Viranta, S AF Viranta, S TI Habitat preferences of European Middle Miocene omnivorous ursids SO ACTA PALAEONTOLOGICA POLONICA LA English DT Article ID FAUNA AB Indarctos spp. were the first large-bodied bears with omnivorous tendencies. Two Indarctos fossils assigned to I. arctoides ssp. by Bernor, Feibel, et al. (2003) and Viranta and Werdelin (2003) show that the genus had a wide geographic range in Europe in the Middle Miocene and was represented by at least two contemporaneous species. Present work shows that the two species of Indarctos lived in a mixture of environments, and were not clearly separated into distinct habitats. Indarctos seems to have evolved during an interval of faunal turnover in Europe. The appearance of Indarctos coincided with an extinction of small omnivorous mammals and was accompanied by the appearance of other large omnivores. C1 Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA. Smithsonian Inst, Washington, DC 20013 USA. RP Viranta, S (reprint author), Howard Univ, Coll Med, Dept Anat, 520 W St NW, Washington, DC 20059 USA. EM sviranta@howard.edu RI Viranta, Suvi/B-9026-2015 OI Viranta, Suvi/0000-0003-4105-530X NR 19 TC 1 Z9 1 U1 0 U2 1 PU INSTYTUT PALEOBIOLOGII PAN PI WARSAW PA UL TWARDA 51/55, 00-818 WARSAW, POLAND SN 0567-7920 J9 ACTA PALAEONTOL POL JI Acta Palaeontol. Pol. PD APR PY 2004 VL 49 IS 2 BP 325 EP 327 PG 3 WC Paleontology SC Paleontology GA 816UA UT WOS:000221133600014 ER PT J AU Reents-Budet, D AF Reents-Budet, D TI Lost languages: The enigma of the world's undeciphered scripts SO AMERICAN JOURNAL OF ARCHAEOLOGY LA English DT Book Review C1 Smithsonian Inst, Ctr Materials Res & Educ, Washington, DC 20006 USA. RP Reents-Budet, D (reprint author), Smithsonian Inst, Ctr Materials Res & Educ, Washington, DC 20006 USA. EM BUDET@GTE.NET NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 USA SN 0002-9114 J9 AM J ARCHAEOL JI Am. J. Archaeol. PD APR PY 2004 VL 108 IS 2 BP 281 EP 282 PG 2 WC Archaeology SC Archaeology GA 818EI UT WOS:000221228000005 ER PT J AU Smith, JL Fonseca, DM AF Smith, JL Fonseca, DM TI Rapid assays for identification of members of the Culex (Culex) pipiens complex, their hybrids, and other sibling species (Diptera : Culicidae) SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID POLYMERASE-CHAIN-REACTION; WEST-NILE-VIRUS; QUINQUEFASCIATUS DIPTERA; NEW-YORK; ACETYLCHOLINESTERASE GENE; MOSQUITOS DIPTERA; AVIAN MALARIA; NORTH-AMERICA; ACE GENE; VECTOR AB Mosquitoes in the Cidex (Cidex) pipiens complex of species, known as vectors of periodic filariasis and deadly encephalitides, have recently emerged as important vectors of West Nile virus in the United States. Highly conserved morphology but marked differences in potential vectorial capacity require the development of polymerase chain reaction (PCR)-based tests that unambiguously distinguish among the different species. We introduce and describe a series of PCR-based assays that use polyrnorphisms in the second intron of the acetylcholinesterase-2 (ace-2) locus for the identification of members of the Cx. pipiens complex (Cx. pipiens, Cx. quinquefasciatus, Cx. p. pallens, Cx. australicus). two other species that are commonly mislabeled as Cx. pipiens (Cx. torrentium and Cx. pervigilans), as well as hybrids between Cx. pipiens and Cx. quinquefasciatus. C1 Natl Museum Nat Hist, Smithsonian Inst, Genet Program, Washington, DC 20560 USA. RP Smith, JL (reprint author), Acad Nat Sci Philadelphia, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA. RI Meyer, Julie/D-1021-2010; OI Meyer, Julie/0000-0003-3382-3321; Fonseca, Dina/0000-0003-4726-7100 FU NIGMS NIH HHS [1R01GM063258]; ODCDC CDC HHS [U50/CCU220532] NR 39 TC 120 Z9 127 U1 1 U2 10 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD APR PY 2004 VL 70 IS 4 BP 339 EP 345 PG 7 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA 814RI UT WOS:000220991400001 PM 15100444 ER PT J AU Johnson, EA Rossman, GR AF Johnson, EA Rossman, GR TI A survey of hydrous species and concentrations in igneous feldspars SO AMERICAN MINERALOGIST LA English DT Article ID POTASSIUM-FELDSPAR; ALKALI FELDSPARS; MANTLE MINERALS; OXYGEN ISOTOPE; HIGH-PRESSURES; WATER-CONTENT; NEW-YORK; ALBITE; MICROPROBE; ANORTHITE AB The hydrous components in 85 feldspars from various igneous environments spanning the range of naturally occurring compositions were examined with infrared spectroscopy. The feldspars contain structural OH (0-512 ppm H2O), H2O (0-1350 ppm H2O), and NH4+ (0-1500 ppm NH4+) groups as well as fluid inclusions and alteration products. Although composition and structure do influence the type of hydrous species that can be incorporated into a particular feldspar mineral, the concentration of these species is not controlled by major-element composition. Coarse perthitic microclines have a heterogeneous distribution of hydrous species, and contain H2O or NH4+ in K-rich lamellae and fluid inclusions in Na-rich areas. The structural OH in plagioclase feldspars is not associated with twin boundaries or exsolution lamellae. All of the possible structural hydrous species are found in pegmatite feldspars, whereas volcanic feldspars contain only structural OH. The variation in OH concentration within a given feldspar composition suggests that fluids in the geologic environment play a role in determining the hydrogen concentration of each sample. The vast majority of plutonic feldspars have undergone partial or total equilibration with meteoric fluids during low-temperature (400-150 degreesC) hydrothermal exchange, obliterating any structural hydrogen and creating substantial concentrations of fluid inclusions (up to 4000 ppm H2O) in the exchanged regions. The amount of water stored as fluid inclusions within feldspars in the upper crust (1 x 10(19) kg) is small compared to the 1.35.x 10(21) kg of water in the oceans, but is roughly equivalent to the reservoir of water stored in hydrous minerals in the upper crust. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20019 USA. RP Johnson, EA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM johnson.elizabeth@nmnh.si.edu OI Rossman, George/0000-0002-4571-6884 NR 69 TC 61 Z9 71 U1 4 U2 15 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD APR PY 2004 VL 89 IS 4 BP 586 EP 600 PG 15 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 809SZ UT WOS:000220657700013 ER PT J AU Kewley, LJ Geller, MJ Jansen, RA AF Kewley, LJ Geller, MJ Jansen, RA TI [O II] as a star formation rate indicator SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : fundamental parameters; galaxies : high-redshift; galaxies : starburst ID GALAXY LUMINOSITY FUNCTION; FRANCE REDSHIFT SURVEY; NEAR-INFRARED SPECTROSCOPY; FORMATION RATE ESTIMATORS; EMISSION-LINE GALAXIES; H-ALPHA; STARBURST GALAXIES; FIELD GALAXIES; FORMATION HISTORY; FORMING GALAXIES AB We investigate the [O II] emission line as a star formation rate (SFR) indicator using integrated spectra of 97 galaxies from the Nearby Field Galaxies Survey (NFGS). The sample includes all Hubble types and contains SFRs ranging from 0.01 to 100 M-. yr(-1). We compare the Kennicutt [O II] and Halpha SFR calibrations and show that there are two significant effects that produce disagreement between SFR([ O II]) and SFR(Halpha): reddening and metallicity. Differences in the ionization state of the interstellar medium do not contribute significantly to the observed difference between SFR([ O II]) and SFR(Halpha) for the NFGS galaxies with metallicities log (O/H) + 12 greater than or similar to 8.5. The Kennicutt [ O II]-SFR relation assumes a typical reddening for nearby galaxies; in practice, the reddening differs significantly from sample to sample. We derive a new SFR([ O II]) calibration that does not contain a reddening assumption. Our new SFR([ O II]) calibration also provides an optional correction for metallicity. Our SFRs derived from [ O II] agree with those derived from Halpha to within 0.03 - 0.05 dex. We show that the reddening, E( B - V), increases with intrinsic (i.e., reddening-corrected) [ O II] luminosity for the NFGS sample. We apply our SFR([ O II]) calibration with metallicity correction to two samples: high-redshift 0.8 < z < 1.6 galaxies from the NICMOS Halpha survey and 0.5 < z < 1.1 galaxies from the Canada-France Redshift Survey. The SFR([ O II]) and SFR(Halpha) for these samples agree to within the scatter observed for the NFGS sample, indicating that our SFR([ O II]) relation can be applied to both local and high-z galaxies. Finally, we apply our SFR([ O II]) to estimates of the cosmic star formation history. After reddening and metallicity corrections, the star formation rate densities derived from [ O II] and Halpha agree to within similar to 30%. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. RP Kewley, LJ (reprint author), Smithsonian Astrophys Observ, Mail Stop 20,60 Garden St, Cambridge, MA 02138 USA. EM lkewley@cfa.harvard.edu NR 100 TC 221 Z9 222 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2004 VL 127 IS 4 BP 2002 EP 2030 DI 10.1086/382723 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WI UT WOS:000220801600011 ER PT J AU Makidon, RB Rebull, LM Strom, SE Adams, MT Patten, BM AF Makidon, RB Rebull, LM Strom, SE Adams, MT Patten, BM TI Periodic variability of pre-main-sequence stars in the NGC 2264 OB association SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 2264); stars : late-type; stars : pre-main-sequence; stars : rotation ID ORION NEBULA CLUSTER; T-TAURI STARS; LOW-MASS STARS; NGC 2264; ROTATION PERIODS; ACCRETION DISKS; FORMING HISTORY; TIME-SERIES; YOUNG; PHOTOMETRY AB We summarize the results of an observing campaign to identify periodic pre-main-sequence (PMS) variables in the NGC 2264 OB association. We find 201 periodic candidates. The mean age of the NGC 2264 periodic variables is approximately 30% greater than their counterparts in the Orion Nebula cluster. Given the difference in mean age between NGC 2264 and Orion, we expect the typical periodic variable in NGC 2264 to have a period shorter by a factor of similar to 1.6, if the initial distribution of periods in the two clusters is identical and if stellar angular momentum is conserved. However, we find a period distribution indistinguishable from that found in Orion. This suggests that the angular momenta of a significant fraction of PMS stars in the age range similar to 0.4 to similar to 4 Myr must be regulated. To examine the hypothesis that disk locking regulates PMS star angular momenta, we use four different disk indicators (U - V, I-C - K-s, H - K-s, and Halpha) to search for correlations between period and disk indicator. We find no conclusive evidence that more slowly rotating stars have disk indicators, or that faster rotating stars are less likely to have disk indicators. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Univ Texas, McDonald Observ, Ft Davis, TX 79734 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Makidon, RB (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM makidon@stsci.edu OI Rebull, Luisa/0000-0001-6381-515X NR 36 TC 54 Z9 54 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2004 VL 127 IS 4 BP 2228 EP 2245 DI 10.1086/382237 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WI UT WOS:000220801600024 ER PT J AU Johnson, JA Winn, JN AF Johnson, JA Winn, JN TI The history of the mysterious eclipses of KH 15D: Asiago Observatory, 1967-1982 SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; open clusters and associations : individual (NGC 2264); stars : individual (KH 15D); stars : pre-main-sequence; techniques : photometric ID T-TAURI STAR; NGC 2264; PHOTOMETRY; YOUNG AB We are gathering archival observations to determine the photometric history of the unique and unexplained eclipses of the pre-main-sequence star KH 15D. Here we present a light curve from 1967 to 1982, based on photographic plates from Asiago Observatory. During this time, the system alternated periodically between bright and faint states, as observed today. However, the bright state was 0.9 mag brighter than the modern value, and the fractional variation between bright and faint states (DeltaI = 0.7 mag) was smaller than observed today (3.5 mag). A possible explanation for these findings is that the system contains a second star that was previously blended with the eclipsing star but is now completely obscured. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Johnson, JA (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM johnjohn@astron.berkeley.edu; jwinn@cfa.harvard.edu NR 16 TC 25 Z9 25 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2004 VL 127 IS 4 BP 2344 EP 2351 DI 10.1086/382520 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WI UT WOS:000220801600034 ER PT J AU Burke, CJ Gaudi, BS DePoy, DL Pogge, RW Pinsonneault, MH AF Burke, CJ Gaudi, BS DePoy, DL Pogge, RW Pinsonneault, MH TI Survey for transiting extrasolar planets in stellar systems. I. Fundamental parameters of the open cluster NGC 1245 SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 1245); stars : fundamental parameters; stars : luminosity function, mass function ID STAR-CLUSTERS; MASS FUNCTION; MILKY-WAY; PHOTOMETRY; HYADES; ISOCHRONES; FIELD; AGE; POPULATIONS; EXTINCTION AB We derive fundamental parameters for the old, rich, open cluster NGC 1245 using BVI photometry from the MDM 1.3 m and 2.4 m telescopes. Based on detailed isochrone fitting, we find that NGC 1245 has a slightly subsolar metallicity, [Fe/H] = - 0.05 +/- 0.03 (statistical) +/- 0.08 (systematic) and an age of 1.04 +/- 0.02 +/- 0.09 Gyr. In contrast to previous studies, we find no evidence of significant differential reddening. We determine an extinction of A(V) = 0.68 +/- 0.02 +/- 0.09 mag and a distance modulus of (m - M)(0) = 12.27 +/- 0.02 +/- 0,12 mag, which corresponds to a distance of 2.8 +/- 0.2 kpc. We derive a logarithmic mass function slope for the cluster of alpha = - 3.12 +/- 0.27, where a Salpeter slope is alpha = - 1.35. Fits to the radial surface density profile yield a core radius of r(c) = 3.'10 +/- 0.'52 (2.57 +/- 0.47 pc). NGC 1245 is highly relaxed and contains a strongly mass-segregated population. The mass function for the inner cluster has a very shallow slope, alpha = - 0.56 +/- 0.28. In contrast, the outer periphery of the cluster is enriched with low-mass members and devoid of high-mass members out to the tidal radius, r(t) = 20' (16.5 pc). Based on the observed surface density profile and an extrapolated mass function, we derive a total cluster mass, M = 1300 +/- 90 +/- 170 M-.. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Burke, CJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM cjburke@astronomy.ohio-state.edu; sgaudi@cfa.harvard.edu; depoy@astronomy.ohio-state.edu; pogge@astronomy.ohio-state.edu; pinsono@astronomy.ohio-state.edu RI Gaudi, Bernard/I-7732-2012 NR 43 TC 21 Z9 22 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2004 VL 127 IS 4 BP 2382 EP 2397 DI 10.1086/382720 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WI UT WOS:000220801600038 ER PT J AU Hogerheijde, MR de Pater, I Wright, M Forster, JR Snyder, LE Remijan, A Woodney, LM A'Hearn, MF Palmer, P Kuan, YJ Huang, HC Blake, GA Qi, CH Kessler, J Liu, SY AF Hogerheijde, MR de Pater, I Wright, M Forster, JR Snyder, LE Remijan, A Woodney, LM A'Hearn, MF Palmer, P Kuan, YJ Huang, HC Blake, GA Qi, CH Kessler, J Liu, SY TI Combined BIMA and OVRO observations of comet C/1999 S4 (LINEAR) SO ASTRONOMICAL JOURNAL LA English DT Article DE comets : individual (C/1999 S4 (LINEAR)); radiative transfer; radio lines : solar system; techniques : interferometric ID C/1996 B2 HYAKUTAKE; COMETS; DISRUPTION; PHOTOMETRY; FRAGMENTS; SPECTRA; NUCLEUS; IMAGES AB We present results from an observing campaign of the molecular content of the coma of comet C/1999 S4 (LINEAR) carried out jointly with the millimeter arrays of the Berkeley-Illinois-Maryland Association (BIMA) and the Owens Valley Radio Observatory (OVRO). Using the BIMA array in autocorrelation ("single-dish'') mode, we detected weak HCN J = 1-0 emission from comet C/1999 S4 (LINEAR) at 14 +/- 4 mK km s(-1) averaged over the 14300 beam. The 3 days over which emission was detected, 2000 July 21.9 - 24.2, immediately precede the reported full breakup of the nucleus of this comet. During this same period, we find an upper limit for HCN J = 1-0 of 144 mJy beam(-1) km s(-1) (203 mK km s(-1)) in the 9" x 12" synthesized beam of combined observations of BIMA and OVRO in cross-correlation ("imaging'') mode. Together with reported values of HCN J = 1-0 emission in the 28" IRAM 30 m beam, our data probe the spatial distribution of the HCN emission from radii of 1300 to 19,000 km. Using literature results of HCN excitation in cometary comae, we find that the relative line fluxes in the 12" x 9", 28", and 143" beams are consistent with expectations for a nuclear source of HCN and expansion of the volatile gases and evaporating icy grains following a Haser model. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Hat Creek Radio Observ, Hat Creek, CA 96040 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Lowell Observ, Flagstaff, AZ 86001 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hogerheijde, MR (reprint author), Sterrewacht Leiden, Postbus 9513, NL-2300 RA Leiden, Netherlands. EM michiel@strw.leidenuniv.nl NR 28 TC 3 Z9 3 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2004 VL 127 IS 4 BP 2406 EP 2412 DI 10.1086/382710 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811WI UT WOS:000220801600040 ER PT J AU Schuller, P Salome, P Perrin, G Mennesson, B Niccolini, G de Laverny, P Ridgway, ST du Foresto, VC Traub, WA AF Schuller, P Salome, P Perrin, G Mennesson, B Niccolini, G de Laverny, P Ridgway, ST du Foresto, VC Traub, WA TI Are dust shell models well-suited to explain interferometric data of late-type stars in the near-infrared? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric; radiative transfer; infrared : stars; stars : late-type; stars : circumstellar matter; stars : individual : alpha Orionis, SW Virginis; R Leonis ID GIANT BRANCH STARS; EVOLVED STARS; MASS-LOSS; TEMPORAL VARIATIONS; OPTICAL-PROPERTIES; SUPERGIANT STARS; MIRA VARIABLES; ALPHA-ORIONIS; 11 MICRONS; O CETI AB Recently available near-infrared interferometric data on late-type stars show a strong increase of diameter for asymptotic giant branch (AGB) stars between the K (2.0-2.4 mum) and L (3.4-4.1 mum) bands. Aiming at an explanation of these findings, we chose the objects alpha Orionis (Betelgeuse), SW Virginis, and R Leonis, which are of different spectral types and stages of evolution, and which are surrounded by circumstellar envelopes with different optical thicknesses. For these stars, we compared observations with spherically symmetric dust shell models. Photometric and 11 mum interferometric data were also taken into account to further constrain the models. - We find the following results. For all three AGB stars, the photosphere and dust shell model is consistent with the multi-wavelength photometric data. For alpha Orionis the model dust shell has a very small optical depth (0.0065 at 11 mum); the visibility data and model in K and L are essentially entirely photospheric with no significant contribution from the dust, and the visibility data at 11 mum show a strong dust signature which agrees with the model. For SW Virginis the model dust shell has a small optical depth (0.045 at 11 mum); in K the visibility data and model are essentially purely photospheric, in L the visibility data demand a larger object than the photosphere plus dust model allows, and at 11 mum there was no data available. For R Leonis the model dust shell has a moderate optical depth (0.1 at 11 mum); in K and L the visibility data and model situation is similar to that of SW Vir, and at 11 mum the visibility data and model are in agreement. - We conclude that AGB models comprising a photosphere and dust shell, although consistent with SED data and also interferometric data in K and at 11 mum, cannot explain the visibility data in L; an additional source of model opacity, possibly related to a gas component, is needed in L to be consistent with the visibility data. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, LERMA, F-75014 Paris, France. Observ Paris, LESIA, F-92195 Meudon, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Observ Cote Azur, Dept Fresnel UMR 6528, F-06304 Nice, France. Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Schuller, P (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM pschuller@cfa.harvard.edu NR 34 TC 14 Z9 14 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2004 VL 418 IS 1 BP 151 EP 162 DI 10.1051/0004-1161:20040051 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 819FH UT WOS:000221299500021 ER PT J AU Martic, M Lebrun, JC Appourchaux, T Korzennik, SG AF Martic, M Lebrun, JC Appourchaux, T Korzennik, SG TI p-mode frequencies in solar-like stars - I. Procyon A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : oscillations (including pulsations); stars : individual : Procyon A; techniques : radial velocities ID RADIAL-VELOCITY MEASUREMENTS; TIME-SERIES ANALYSIS; PHOTON-NOISE LIMIT; ETA-BOOTIS; SPACED DATA; OSCILLATIONS; AMPLITUDES; SPECTRUM; ASTEROSEISMOLOGY; SPECTROGRAPH AB As a part of an on-going program to explore the signature of p-modes in solar-like stars by means of high-resolution absorption line spectroscopy, we have Studied four stars (alphaCMi, etaCas A, zetaHer A and betaVir). We present here new results front two-site observations of Procyon A acquired over twelve nights in 1999. Oscillation frequencies for l = 1 and 0 (or 2) p-modes are detected in the power spectra of these Doppler shift measurements. A frequency analysis points out the difficulties of the classical asymptotic theory in representing the p-mode spectrum of Procyon A. C1 CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. European Space Agcy, ESTEC, Sci Payload & Adv Concept Off, NL-2200 AG Noordwijk, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Martic, M (reprint author), CNRS, Serv Aeron, BP 3, F-91371 Verrieres Le Buisson, France. EM milena@aerov.jussieu.fr NR 48 TC 53 Z9 53 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2004 VL 418 IS 1 BP 295 EP 303 DI 10.1051/0004-6361:20034574 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 819FH UT WOS:000221299500036 ER PT J AU Ness, JU Schmitt, JHMM Wolk, SJ Dennerl, K Burwitz, V AF Ness, JU Schmitt, JHMM Wolk, SJ Dennerl, K Burwitz, V TI X-ray emission from Saturn SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites : general; planets and satellites : individual : Saturn; X-rays : general ID DISCOVERY; JUPITER; CHANDRA; NEPTUNE; SPECTRA; URANUS; AURORA; SEARCH; SKY AB We report the first unambiguous detection of X-ray emission originating from Saturn with a Chandra observation, duration 65.5 ks with ACIS-S3. Beyond the pure detection we analyze the spatial distribution of X-rays on the planetary surface, the light curve, and some spectral properties. The detection is based on 162 cts extracted from the ACIS-S3 chip within the optical disk of Saturn. We found no evidence for smaller or larger angular extent. The expected background level is 56 cts, i.e., the count rate is (1.6 +/- 0.2) x 10(-3) cts/s. The extracted photons are rather concentrated towards the equator of the apparent disk. while both polar caps have a relative photon deficit. The inclination angle of Saturn during the observation was similar to-27degrees, so that the northern hemisphere was not visible during the complete observation. In addition, it was occulted by the ring system. We found a small but significant photon excess at one edge of the ring system. The light curve shows a small dip twice at identical phases, but rotational modulation cannot be claimed at a significant level. Spectral modeling results in a number of statistically, but not necessarily physically, acceptable models. The X-ray flux level we calculate from the best-fit spectral models is similar to6.8 x 10(-15) erg cm(-2) s(-1) (in the energy interval 0.1-2 keV), which corresponds to an X-ray luminosity of similar to8.7 x 10(14) erg s(-1). A combination of scatter processes of solar X-rays require a relatively high albedo favoring internal processes, but a definitive explanation remains an open issue. C1 Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Ness, JU (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM jness@hs.uni-hamburg.de OI Wolk, Scott/0000-0002-0826-9261 NR 33 TC 19 Z9 19 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2004 VL 418 IS 1 BP 337 EP 345 DI 10.1051/0004-6361:20035736 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 819FH UT WOS:000221299500040 ER PT J AU Favata, F Micela, G Baliunas, SL Schmitt, JHMM Gudel, M Harnden, FR Sciortino, S Stern, RA AF Favata, F Micela, G Baliunas, SL Schmitt, JHMM Gudel, M Harnden, FR Sciortino, S Stern, RA TI High-amplitude, long-term X-ray variability in the solar-type star HD 81809: The beginning of an X-ray activity cycle? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : x-rays ID MAIN-SEQUENCE STARS; EMISSION; MASSES; SUN AB We present the initial results from our XMM-Newton program aimed at searching for X-ray activity cycles in solar-type stars. HD 81809 is a G2-type star (somewhat more evolved than the Sun, and with a less massive companion) with a pronounced 8.2 yr chromospheric cycle, as evident from from the Mt. Wilson program data. We present here the reSU tS 1-0 11 the initial 2.5 years of XMM-Newton observations, showing that large amplitude (a factor of similar or equal to10) modulation is present in the X-ray luminosity, with a clearly defined maximum in mid 2002 and a steady decrease since then. The maximum of the chromospheric cycle took place in 2001; if the observed X-ray variability is the initial part of an X-ray cycle, this Could imply a phase shift between chromospheric and coronal activity, although the current descent into chromospheric cycle minimum is well reflected into the star's X-ray luminosity. The observations presented here provide clear evidence for the presence of large amplitude X-ray variability coherent with the activity cycle in the chromosphere in a star other than the Sun. C1 European Space Agcy, Res & Sci Support Dept, Div Astrophys, NL-2200 AG Noordwijk, Netherlands. Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. Paul Scherrer Inst, CH-5235 Wurenlingen, Switzerland. Paul Scherrer Inst, CH-5235 Villigen, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lockheed Martin Adv Technol Ctr, Palo Alto, CA USA. RP Favata, F (reprint author), European Space Agcy, Res & Sci Support Dept, Div Astrophys, Postbus 299, NL-2200 AG Noordwijk, Netherlands. EM Fabio.Favata@rssd.esa.int RI Guedel, Manuel/C-8486-2015; OI Guedel, Manuel/0000-0001-9818-0588; Micela, Giuseppina/0000-0002-9900-4751 NR 11 TC 32 Z9 33 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2004 VL 418 IS 1 BP L13 EP L16 DI 10.1051/0004-6361:20040105 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 819FH UT WOS:000221299500004 ER PT J AU Williams, SJ Fuller, GA Sridharan, TK AF Williams, SJ Fuller, GA Sridharan, TK TI The circumstellar environments of high-mass protostellar objects - I. Submillimetre continuum emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; stars : circumstellar matter; ISM : clouds; ISM : dust, extinction ID ULTRACOMPACT HII-REGIONS; MOLECULAR CLOUD CORES; YOUNG STELLAR OBJECTS; STAR-FORMATION; INTERSTELLAR GRAINS; DUST; MILLIMETER; CANDIDATES; DISKS; OUTFLOWS AB We present maps of the 850 pm and 450 pm continuum emission seen towards a sample of 68 high-mass protostellar candidates with luminosities ranging from 10(2.5) L. to similar to10(5) L. Most of these candidate high-mass stars are in the earliest stages of evolution, and have not yet developed an ultra-compact HII region. We observe a variety of continuum emission morphologies, from compact symmetric sources through to multiple cores embedded in long filaments of emission. We find on average there is a 65% probability of an IRAS point-source having a companion detection at submillimetre wavelengths. The ratio of integrated flux to peak flux for our detections shows no strong dependence on distance, suggesting the emission we have observed is primarily from scale-free envelopes with power-law density structures. Assuming a near kinematic distance projection, the clumps we detect vary in mass from similar to1 M. to over 1000 M. with a mean clump mass of 330 M. column density of 9 x 10(23) cm(-2) and diameter of similar to0.6 pc. The high luminosity and low mass of the smallest clumps suggests they are accompanied by a minimal number of stellar companions, while the most massive clumps may be examples of young protogroups and protoclusters. We measure the spectral index of the dust emission (alpha) and the spectral index of the dust grain opacity (beta) towards each object, finding clumps with morphologies suggestive of strong temperature gradients, and of grain growth in their dense inner regions. We find a mean value for beta of 0.9, significantly smaller than observed towards UCHII regions. C1 UMIST, Dept Phys, Manchester M60 1QD, Lancs, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fuller, GA (reprint author), UMIST, Dept Phys, POB 88, Manchester M60 1QD, Lancs, England. EM g.fuller@umist.ac.uk NR 53 TC 72 Z9 72 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2004 VL 417 IS 1 BP 115 EP 133 DI 10.1051/0004-6361:20031733 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 814LL UT WOS:000220976100018 ER PT J AU Clowe, D Gonzalez, A Markevitch, M AF Clowe, D Gonzalez, A Markevitch, M TI Weak-lensing mass reconstruction of the interacting cluster 1E 0657-558: Direct evidence for the existence of dark matter SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies : clusters : individual (1E 0657-556); gravitational lensing ID MODIFIED NEWTONIAN DYNAMICS; GALAXIES; FIELD; CONFIRMATION; CONSTRAINTS; HYPOTHESIS; CHANDRA; SEARCH AB We present a weak-lensing mass reconstruction of the interacting cluster 1E 0657 - 558, in which we detect both the main cluster and a subcluster. The subcluster is identified as a smaller cluster that has just undergone initial infall and pass-through of the primary cluster and has been previously identified in both optical surveys and X-ray studies. The X-ray gas has been separated from the galaxies by ram pressure - stripping during the pass-through. The detected mass peak is located between the X-ray peak and galaxy concentration, although the position is consistent with the galaxy centroid within the errors of the mass reconstruction. We find that the mass peak for the main cluster is in good spatial agreement with the cluster galaxies and is offset from the X-ray halo at 3.4 sigma significance, and we determine that the mass-to-light ratios of the two components are consistent with those of relaxed clusters. The observed offsets of the lensing mass peaks from the peaks of the dominant visible mass component ( the X-ray gas) directly demonstrate the presence, and dominance, of dark matter in this cluster. This proof of dark matter existence holds true even under the assumption of modified Newtonian dynamics (MOND); based on the observed gravitational shear - optical light ratios and the mass peak - X-ray gas offsets, the dark matter component in a MOND regime would have a total mass that is at least equal to the baryonic mass of the system. C1 Univ Bonn, Inst Astrophys & Extraterr Forsch, D-53121 Bonn, Germany. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Clowe, D (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM dclowe@as.arizona.edu NR 43 TC 207 Z9 207 U1 1 U2 9 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2004 VL 604 IS 2 BP 596 EP 603 DI 10.1086/381970 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 807SX UT WOS:000220522300013 ER PT J AU Ivanov, VD Rieke, MJ Engelbracht, CW Alonso-Herrero, A Rieke, GH Luhman, KL AF Ivanov, VD Rieke, MJ Engelbracht, CW Alonso-Herrero, A Rieke, GH Luhman, KL TI A medium-resolution near-infrared spectral library of late-type stars. I. SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE atlases; infrared : stars; stars : abundances; stars : chromospheres; stars : fundamental parameters; stars : late-type ID OLD STELLAR POPULATIONS; DETAILED ABUNDANCE ANALYSIS; FUNDAMENTAL MK STANDARDS; INITIAL MASS FUNCTION; MAIN-SEQUENCE STARS; 2.5 MU-M; GIANT STARS; COOL STARS; CLASSIFICATION SPECTROSCOPY; EFFECTIVE TEMPERATURES AB We present an empirical infrared spectral library of medium-resolution (R approximate to 2000-3000) H (1.6 mum) and K (2.2 mum) band spectra of 218 red stars, spanning a range of [Fe/H] from similar to-2.2 to similar to+0.3. The sample includes Galactic disk stars, bulge stars from Baade's window, and red giants from Galactic globular clusters. We report the values of 19 indices covering 12 spectral features measured from the spectra in the library. Finally, we derive calibrations to estimate the effective temperature, and diagnostic relationships to determine the luminosity classes of individual stars from near-infrared spectra. This paper is part of a larger effort aimed at building a near-IR spectral library to be incorporated in population synthesis models, as well as at testing synthetic stellar spectra. C1 European So Observ, D-85748 Garching, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM vivanov@eso.org; mrieke@as.arizona.edu; chad@as.arizona.edu; aalonso@as.arizona.edu; grieke@as.arizona.edu; kluhman@cfa.harvard.edu RI Alonso-Herrero, Almudena/H-1426-2015; OI Alonso-Herrero, Almudena/0000-0001-6794-2519; Ivanov, Valentin/0000-0002-5963-1283 NR 109 TC 59 Z9 59 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2004 VL 151 IS 2 BP 387 EP 397 DI 10.1086/381752 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 807SW UT WOS:000220522200009 ER PT J AU Eberhard, JR Bermingham, E AF Eberhard, JR Bermingham, E TI Phylogeny and biogeography of the Amazona ochrocephala (Aves : Psittacidae) complex SO AUK LA English DT Article ID MITOCHONDRIAL-DNA; CENTRAL-AMERICA; INTROGRESSION; SPECIATION; INFERENCE; EVOLUTION; PATTERNS; GENUS; POPULATIONS; DIVERSITY AB We present a phylogenetic analysis of relationships among members of the Amazona ochrocephala species complex of parrots, a broadly distributed group in Middle and South America that has been a "taxonomic headache." Mitochondrial DNA sequence data are used to infer phylogenetic relationships among most of the named subspecies in the complex. Sequence-based phylogenies show that Middle American subspecies included in the analysis are reciprocally monophyletic, but subspecies described for South America do not reflect patterns of genetic variation. Samples from the lower Amazon cluster with samples collected in western Amazonia-not with samples from Colombia and Venezuela, as was predicted by subspecies classification. All subspecies of the complex are more closely related to one another than to other Amazona species, and division of the complex into three species (A. ochrocephala, A. auropalliata, and A. oratrix) is not supported by our data. Divergence-date estimates suggest that these parrots arrived in Middle America after the Panama land-bridge formed, and then expanded and diversified rapidly. As in Middle America, diversification of the group in South America occurred during the Pleistocene, possibly driven by changes in distribution of forest habitat. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Eberhard, JR (reprint author), Louisiana State Univ, Dept Biol Sci, 202 Life Sci, Baton Rouge, LA 70803 USA. EM eberhard@lsu.edu NR 54 TC 69 Z9 69 U1 1 U2 9 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD APR PY 2004 VL 121 IS 2 BP 318 EP 332 DI 10.1642/0004-8038(2004)121[0318:PABOTA]2.0.CO;2 PG 15 WC Ornithology SC Zoology GA 826JE UT WOS:000221824600004 ER PT J AU Emlen, ST Wrege, PH AF Emlen, ST Wrege, PH TI Size dimorphism, intrasexual competition, and sexual selection in Wattled Jacana (Jacana jacana), a sex-role-reversed shorebird in Panama SO AUK LA English DT Article ID POTENTIAL REPRODUCTIVE RATES; BREEDING BIOLOGY; AFRICAN JACANA; LESSER JACANA; FEMALE CHOICE; POLYANDRY; BEHAVIOR; POPULATION; INTENSITY; EVOLUTION AB We studied sexual size dimorphism, intrasexual competition, and sexual selection in an individually marked population of Waffled Jacanas (Jacana jacana) in the Republic of Panama. Males are the sole incubators of eggs (28-day incubation) and primary providers of chick care (50-60 days). Females were 48% heavier than, and behaviorally dominant over, males. Females also showed greater development of secondary sexual characters (fleshy facial ornamentation and wing spurs) than males. Both sexes defended territories throughout the year against same-sex conspecifics. Competition for territorial space was intense, and many individuals of both sexes did not become breeders. Resident females further competed with one another to accumulate multiple mates, resulting in a mating system of simultaneous polyandry. Female and male residents (territory holders) were larger, heavier, and more ornamented than adult floaters of the same sex. Larger and heavier females also had more mates than smaller females. Body size was thus a critical predictor of success in intrasexual competition for territories (both sexes) and for mates (females). Three measures of sexual selection-(1) sex difference in the opportunity for sexual selection, (2) female-to-male ratio of potential reproductive rates, and (3) operational sex ratio-each indicated that sexual selection is currently operating more strongly on females than on males (female-to-male ratios ranged from 1.43:1 to 2.22:1). Values of 1.61:1 and 1.43:1 represent the first published quantitative estimates of the opportunity for sexual selection for any sex-role-reversed bird. Our study supports the theory that when increased parental care entails reduced opportunities for future reproduction, asymmetries in parental care behaviors of the sexes can influence the intensity of competition for mates and the direction and strength of sexual selection. C1 Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Emlen, ST (reprint author), Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. EM ste@cornell.edu NR 41 TC 40 Z9 42 U1 3 U2 48 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD APR PY 2004 VL 121 IS 2 BP 391 EP 403 DI 10.1642/0004-8038(2004)121[0391:SDICAS]2.0.CO;2 PG 13 WC Ornithology SC Zoology GA 826JE UT WOS:000221824600011 ER PT J AU Graves, GR AF Graves, GR TI Testicular volume and asymmetry are age-dependent in black-throated blue warblers (Dendroica caerulescens) SO AUK LA English DT Article ID SECONDARY SEXUAL CHARACTERS; DELAYED PLUMAGE MATURATION; NORTH-AMERICAN BIRDS; EXTRA-PAIR PATERNITY; MALE SPERM RESERVES; TESTIS SIZE; MIGRATORY SONGBIRD; MATING SYSTEMS; PASSER-DOMESTICUS; EJACULATE QUALITY AB Passerine birds are favored models for studies of sperm competition and extrapair paternity, yet the intraspecific chronology of testicular maturation and its empirical and theoretical consequences in avian mating systems have been largely ignored. I analyzed age-dependent variation in testicular morphology in 25 breeding populations of the Black-throated Blue Warbler (Dendroica caerulescens) distributed throughout its geographic range in eastern North America. Yearlings (first breeding season) had significantly smaller testes than older males (greater than or equal to2 years). Latitude, altitude, and Julian date had negligible effects on testicular morphology when effects of core body size were controlled. Preparator effects had significant influence on the estimation of testicular volume and asymmetry. Contrary to Moller's hypothesis that the smaller testis compensates for deficiencies in the larger, the volumes of the left and right testes were positively correlated in both yearlings and older males. Older males exhibited a higher degree of directional asymmetry because of the disproportionate enlargement of the left testis. These data suggest that testicular morphology and reproductive capacities of yearling passerines may not be equivalent to those of older males. In a broader context, these findings demonstrate that age class should be factored into quantitative models of sperm competition in birds. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, MRC 116, Washington, DC 20013 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, MRC 116, POB 37012, Washington, DC 20013 USA. EM graves.gary@nmnh.si.edu NR 77 TC 19 Z9 20 U1 1 U2 3 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD APR PY 2004 VL 121 IS 2 BP 473 EP 485 DI 10.1642/0004-8038(2004)121[0473:TVAAAA]2.0.CO;2 PG 13 WC Ornithology SC Zoology GA 826JE UT WOS:000221824600019 ER PT J AU Yavitt, JB Wright, SJ Wieder, RK AF Yavitt, JB Wright, SJ Wieder, RK TI Seasonal drought and dry-season irrigation influence leaf-litter nutrients and soil enzymes in a moist, lowland forest in Panama SO AUSTRAL ECOLOGY LA English DT Article DE litter nutrients; microbial nutrient content; neotropics; nutrient residence time; soil enzymes; tropical moist forest ID TROPICAL RAIN-FOREST; BARRO-COLORADO ISLAND; MICROBIAL BIOMASS; ORGANIC-MATTER; PLANT NUTRIENTS; DYNAMICS; NITROGEN; PHOSPHORUS; ECOSYSTEM; MINERALIZATION AB Climatic conditions should not hinder nutrient release from decomposing leaf-litter (mineralization) in the humid tropics, even though many tropical forests experience drought lasting from several weeks to months. We used a dry-season irrigation experiment to examine the effect of seasonal drought on nutrient concentrations in leaf-fall and in decomposing leaf-litter. In the experiment, soil in two 2.25-ha plots of old-growth lowland moist forest on Barro Colorado Island, Republic of Panama, was watered to maintain soil water potential at or above field capacity throughout the 4-month dry season. Wet-season leaf-fall had greater concentrations of nitrogen (N, 13.5 mg g(-1)) and calcium (Ca, 15.6 mg g(-1)) and lower concentrations of sulfur (S, 2.51 mg g(-1)) and potassium (K, 3.03 mg g(-1)) than dry-season leaf-fall (N = 11.6 mg g(-1), Ca = 13.6 mg g(-1), S = 2.98 mg g(-1), K = 5.70 mg g(-1)). Irrigation did not affect nutrient concentrations or nutrient return from forest trees to the forest floor annually (N = 18 g m(-2), phosphorus (P) = 1.06 g m(-2), S = 3.5 g m(-2), Ca = 18.9 g m(-2), magnesium = 6.5 g m(-2), K = 5.7 g m(-2)). Nutrient mineralization rates were much greater during the wet season than the dry season, except for K, which did not vary seasonally. Nutrient residence times in forest-floor material were longer in control plots than in irrigated plots, with values approximately equal to that for organic matter (210 in control plots vs 160 in irrigated plots). Calcium had the longest residence time. Forest-floor material collected at the transition between seasons and incubated with or without leaching in the laboratory did not display large pulses in nutrient availability. Rather, microorganisms immobilized nutrients primarily during the wet season, unlike observations in tropical forests with longer dry seasons. Large amounts of P moved among different pools in forest-floor material, apparently mediated by microorganisms. Arylsulfatase and phosphatase enzymes, which mineralize organically bound nutrients, had high activity throughout the dry season. Low soil moisture levels do not hinder nutrient cycling in this moist lowland forest. C1 Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. Villanova Univ, Dept Biol, Villanova, PA 19085 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Yavitt, JB (reprint author), Cornell Univ, Dept Nat Resources, Fernow Hall, Ithaca, NY 14853 USA. EM jby1@cornell.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 60 TC 51 Z9 52 U1 6 U2 40 PU BLACKWELL PUBLISHING ASIA PI CARLTON PA 54 UNIVERSITY ST, P O BOX 378, CARLTON, VICTORIA 3053, AUSTRALIA SN 1442-9985 J9 AUSTRAL ECOL JI Austral Ecol. PD APR PY 2004 VL 29 IS 2 BP 177 EP 188 DI 10.1111/j.1442-9993.2004.01334.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 809HR UT WOS:000220628300006 ER PT J AU Basset, Y Mavoungou, JF Mikissa, JB Missa, O Miller, SE Kitching, RL Alonso, A AF Basset, Y Mavoungou, JF Mikissa, JB Missa, O Miller, SE Kitching, RL Alonso, A TI Discriminatory power of different arthropod data sets for the biological monitoring of anthropogenic disturbance in tropical forests SO BIODIVERSITY AND CONSERVATION LA English DT Article DE guilds; parataxonomists; predictor sets; rarity; taxonomic resolution ID AUSTRALIAN RAIN-FOREST; DUNG BEETLES; TAXONOMIC RESOLUTION; SPECIES ASSEMBLAGES; INSECT HERBIVORES; BIOTIC INDEXES; COMMUNITIES; BIODIVERSITY; DIVERSITY; GABON AB Arthropods were monitored by local parataxonomists at 12 sites of increasing anthropogenic disturbance (old and young secondary forests, savanna and cultivated gardens) at Gamba, Gabon. We report on the discriminatory power of different data sets with regard to the classification of sites along the disturbance gradient, using preliminary data accounting for 13 surveys and 142425 arthropods collected by Malaise, pitfall and yellow-pan traps. We compared the performance of different data sets. These were based upon ordinal, familial and guild composition, or upon 22 target taxa sorted to morphospecies and either considered in toto or grouped within different functional guilds. Finally we evaluated 'predictor sets' made up of a few families or other target taxa, selected on the basis of their indicator value index. Although the discriminatory power of data sets based on ordinal categories and guilds was low, that of target taxa belonging to chewers, parasitoids and predators was much higher. The data sets that best discriminated among sites of differing degrees of disturbance were the restricted sets of indicator families and target taxa. This validates the concept of predictor sets for species-rich tropical systems. Including or excluding rare taxa in the analyses did not alter these conclusions. We conclude that calibration studies similar to ours are needed elsewhere in the tropics and that this strategy will allow to devise a representative and efficient biotic index for the biological monitoring of terrestrial arthropod assemblages in the tropics. C1 Smithsonian Trop Res Inst, Panama City, Panama. IRET, CENAREST, Libreville, Gabon. Ecole Natl Eaux & Forets, Libreville, Gabon. Griffith Univ, Australian Sch Environm Studies, Brisbane, Qld 4111, Australia. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Griffith Univ, Australian Sch Environm Studies, Cooperat Res Ctr Trop Rainforest Ecol & Managemen, Brisbane, Qld 4111, Australia. Smithsonian Inst, Monitoring & Assessment Biodivers Program, Washington, DC 20560 USA. RP Basset, Y (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Panama City, Panama. EM bassety@tivoli.si.edu RI Kitching, Roger/C-5102-2009; Missa, Olivier/G-2687-2012; Basset, Yves/B-6642-2014; OI Missa, Olivier/0000-0002-4330-5192; Miller, Scott/0000-0002-4138-1378 NR 80 TC 40 Z9 45 U1 4 U2 33 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD APR PY 2004 VL 13 IS 4 BP 709 EP 732 DI 10.1023/B:BIOC.0000011722.44714.a4 PG 24 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 762WV UT WOS:000188005900004 ER PT J AU Lydeard, C Cowie, RH Ponder, WF Bogan, AE Bouchet, P Clark, SA Cummings, KS Frest, TJ Gargominy, O Herbert, DG Hershler, R Perez, KE Roth, B Seddon, M Strong, EE Thompson, FG AF Lydeard, C Cowie, RH Ponder, WF Bogan, AE Bouchet, P Clark, SA Cummings, KS Frest, TJ Gargominy, O Herbert, DG Hershler, R Perez, KE Roth, B Seddon, M Strong, EE Thompson, FG TI The global decline of nonmarine mollusks SO BIOSCIENCE LA English DT Article DE nonmarine mollusks; biodiversity; gastropods; endangered species; hotspots ID PULMONATE LAND SNAILS; AMERICAN-SAMOA; UNITED-STATES; NEW-CALEDONIA; TREE SNAILS; BIODIVERSITY HOTSPOTS; CONSERVATION; ISLAND; RIVER; EXTINCTION AB Invertebrate species represent more than 99% of animal diversity; however, they receive much less publicity and attract disproportionately minor research effort relative to vertebrates. Nonmarine mollusks (i.e., terrestrial and fresh water) are one of the most diverse and imperiled groups of animals, although not many people other than a few specialists who study the group seem to be aware of their plight. Nonmarine mollusks include a number of phylogenetically disparate lineages and species-rich assemblages that represent two molluscan classes, Bivalvia (clams and mussels) and Gastropoda (snails, slugs, and limpets). In this article we provide an overview of global nonmarine molluscan biodiversity and conservation status, including several case studies documenting the diversity and global decline of nonmarine mollusks. We conclude with a discussion of the roles that mollusks and malacologists should play in conservation, including research, conservation management strategies, and education and outreach. C1 Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. Univ Hawaii, Ctr Conservat & Training, Honolulu, HI 96822 USA. Australian Museum, Div Invertrate Zool, Malacol Sect, Sydney, NSW 2010, Australia. N Carolina State Museum Nat Sci, Raleigh, NC 27607 USA. Museum Natl Hist Nat, F-75005 Paris, France. Illinois Nat Hist Survey, Champaign, IL 61820 USA. Deixis Consultants, Seattle, WA 98115 USA. Natal Museum, ZA-3200 Pietermaritzburg, South Africa. Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA. Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA. Natl Museum Wales, Dept Biodivers & Syst Biol, Cardiff CF1 3NP, S Glam, Wales. Univ Minnesota, Bell Museum Nat Hist, Dept Fisheries Wildlife & Conservat Biol, St Paul, MN 55108 USA. Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Lydeard, C (reprint author), Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. EM clydeard@bama.ua.edu RI Perez, Kathryn/D-6082-2013; Bogan, Arthur/G-7658-2016; OI Bogan, Arthur/0000-0003-4042-7706; Strong, Ellen/0000-0001-7181-4114 NR 83 TC 455 Z9 492 U1 11 U2 95 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 2004 VL 54 IS 4 BP 321 EP 330 DI 10.1641/0006-3568(2004)054[0321:TGDONM]2.0.CO;2 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 811EP UT WOS:000220755500010 ER PT J AU Robinson, WD Angehr, GR Robinson, TR Petit, LJ Petit, DR Brawn, JD AF Robinson, WD Angehr, GR Robinson, TR Petit, LJ Petit, DR Brawn, JD TI Distribution of bird diversity in a vulnerable neotropical landscape SO CONSERVATION BIOLOGY LA English DT Article DE biodiversity; bird diversity; economic development; Neotropics; Panama; Panama Canal ID BARRO-COLORADO ISLAND; FOREST FRAGMENTATION; INSECTIVOROUS BIRDS; CENTRAL PANAMA; BIODIVERSITY; BIOGEOGRAPHY; COMMUNITIES; EXTINCTION; GRADIENTS; AVIFAUNA AB Recent withdrawal of the US. military from the Republic of Panama has exposed 64,000 ha of lowland forest in the former Canal Zone to possible development. The forests form a 16-km-wide strip reaching 65 km from the Caribbean Sea to the Pacific Ocean and function as the water supply for the canal and as home to one of the world's richest terrestrial biotas. We present an overview of the distribution of bird diversity in the forests of the canal area based on 10 years of inventories. A total of 498 terrestrial species has been recorded, of which 177 occur only in lowland forests. More species reside in Caribbean- than in Pacific-slope forests and in the largest forest tracts. The Panamanian government, recognizing the importance of the forests for protection of biodiversity and for proper functioning of the canal, has created two national parks and a national monument in the canal area. One large park, Soberania National Park, currently contains 92% of the region's forest-dwelling species. Two large tracts on the Caribbean coast, the Achiote Road forest and the Fort Sherman forest, are not designated as national parks but are recognized as important forest areas. Those two forests harbor species found nowhere else in the canal corridor Extensive fragmentation, disconnection of forested corridors between foothills and lowlands, and anthropogenic degradation of forests near towns have altered regional bird-community dynamics. Some dynamics occur on large spatial scales, such as the poorly understood movements of elevational and transisthmian migrants. Long-term maintenance of bird species diversity in the canal area will require preservation of the large forest tracts and reestablishment of a forested connection from the canal corridor lowlands to the Chagres lowlands and foothills in the east. Such conservation activities will be challenging to execute given the region's growing human population and desires for a stronger national economy. We recommend protection of remaining forests and active enforcement of protection laws to reduce hunting and further intrusions. C1 Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. Smithsonian Trop Res Inst, APO, AA 34002 USA. Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20008 USA. Natl Pk Serv, Cuyahoga Valley Natl Pk, Brecksville, OH 44141 USA. Cleveland Metropk, Cleveland, OH 44144 USA. 113 Shelford Vivarium, Dept Anim Biol, Champaign, IL 61820 USA. RP Robinson, WD (reprint author), Oregon State Univ, Dept Fisheries & Wildlife, 104 Nash Hall, Corvallis, OR 97331 USA. EM douglas.robinson@oregonstate.edu NR 43 TC 16 Z9 17 U1 2 U2 19 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD APR PY 2004 VL 18 IS 2 BP 510 EP 518 DI 10.1111/j.1523-1739.2004.00355.x PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 808KF UT WOS:000220567300028 ER PT J AU Nansen, C Bonjour, EL Gates, MW Phillips, TW Cuperus, GW Payton, ME AF Nansen, C Bonjour, EL Gates, MW Phillips, TW Cuperus, GW Payton, ME TI Model of Cryptolestes ferrugineus flight activity outside commercial steel grain bins in central Oklahoma SO ENVIRONMENTAL ENTOMOLOGY LA English DT Article DE decision support tools; modeling; Oklahoma; stored-product beetles ID FARM-STORED WHEAT; INSECT POPULATIONS; PRODUCT INSECTS; TRAP CATCH; COLEOPTERA; INFESTATION; CUCUJIDAE; CORN; ATTRACTANTS; CAPTURE AB Unbaited sticky traps were placed on ropes in the four cardinal directions and at different heights on the outside of commercial steel bins containing stored wheat. Weekly trap catches of the rusty grain beetle, Cryptolestes ferrugineus (Stephens), were examined. The number of traps per steel bin varied due to differences in dimensions, and three height classes were established, but there was no significant difference in trap catches of C. ferrugineus among height classes. Significant yearly and between-steel bin variation was found, and these effects were removed before using a response surface regression analysis to determine how well two time variables (daylength and day number) and three weather variables (minimum and maximum temperature and precipitation) could explain the seasonal variation in C. ferrugineus flight activity. These variables were used in separate analyses of C. ferrugineus trap catches in the four cardinal directions and from the three height classes (12 separate analyses). The most robust model fit was obtained when using a subset representing 208 C. ferrugineus trap catches from the northern side at height class 3 (traps s placed at least three-quarters of bin height). The full model of the two time variables and three weather variables explained 48% of the variance in this subset of trap catches, whereas a model based on weekly means of daylength and minimum and maximum air temperatures explained 40% of the total variance in C. ferrugineus trap catches. The relative trap catch response to daylength and minimum and maximum air temperatures was evaluated. High beetle flight activity around grain bins may indicate a high risk of insect infestation of stored wheat, and the presented model can therefore be used to determine time periods with high risk of beetle immigration into commercial steel bins. C1 Oklahoma State Univ, Dept Entomol & Plant Pathol, Noble Res Ctr 127, Stillwater, OK 74078 USA. Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, PSI, Washington, DC 20013 USA. Oklahoma State Univ, Dept Stat, Stillwater, OK 74078 USA. RP Nansen, C (reprint author), Oklahoma State Univ, Dept Entomol & Plant Pathol, Noble Res Ctr 127, Stillwater, OK 74078 USA. NR 25 TC 7 Z9 7 U1 0 U2 3 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0046-225X J9 ENVIRON ENTOMOL JI Environ. Entomol. PD APR PY 2004 VL 33 IS 2 BP 426 EP 434 PG 9 WC Entomology SC Entomology GA 812RL UT WOS:000220856500039 ER PT J AU Ruber, L Britz, R Tan, HH Ng, PKL Zardoya, R AF Ruber, L Britz, R Tan, HH Ng, PKL Zardoya, R TI Evolution of mouthbrooding and life-history correlates in the fighting fish genus Betta SO EVOLUTION LA English DT Article DE brood care; bubble nesting; comparative method; mitochondrial DNA; phylogenetic generalized least-squares; phylogeny; RAG1 ID ANCESTRAL CHARACTER STATES; PARENTAL CARE; PHYLOGENETIC ANALYSIS; CICHLID FISH; LIKELIHOOD; INFERENCE; BEHAVIOR; MODEL; SIZE AB The origin of and evolutionary transitions among the extraordinary diverse forms of parental care in teleost fish remain largely unknown. The "safe harbor" hypothesis predicts that the evolution from a "guarding" to a "brooding" form of care in teleost fish is associated with shifts in reproductive and life-history features such as reduced fecundity, and increased egg volume with higher parental investment. Robust phylogenetic hypotheses may help to identify evolutionary changes in key traits associated with differences in the form of parental care. Here, we used reconstruction of ancestral character states to study the evolution of the two forms of parental care, bubble nesting and mouthbrooding in the fighting fish genus Betta. We also applied a comparative analysis using the phylogenetic generalized least-squares method to test the "safe harbor" hypothesis by evaluating differences between the two forms of parental care in standard length, life-history traits, and three habitat variables. Evolutionary hypotheses were derived from the first molecular phylogeny (nuclear and mitochondrial DNA sequence data; 4448 bp) of this speciose group. Ancestral character state reconstructions of the evolution of the form of parental care in the genus Betta, using the methods of unweighted parsimony and maximum likelihood, are uncertain and further indicate a high rate of evolutionary transitions. Applying different weights for the suspected directionality of changes, based on the consistent phenotypic and behavioral differences found between bubble nesters and mouthbrooders, recurrent origin of mouthbrooding in the genus Betta is favored using parsimony. Our comparative analyses further demonstrate that bubble nesters and mouthbrooders do not have a consistent set of life-history correlates. The form of parental care in Betta is correlated only with offspring size, with mouthbrooders having significantly bigger offspring than bubble nesters, but is not correlated with egg volume, clutch size, and broodcare duration, nor with any of the three habitat variables tested. Our results thus challenge the general predictions of the "safe harbor" hypothesis for the evolution of alternative brood care forms in the fighting fish genus Betta. C1 Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolut, E-28006 Madrid, Spain. Univ Tubingen, Lehrstuhl Spezielle Zool, D-72076 Tubingen, Germany. Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. Natl Univ Singapore, Dept Biol Sci, Singapore 119260, Singapore. RP Ruber, L (reprint author), Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolut, Jose Gutierrez Abascal 2, E-28006 Madrid, Spain. EM ruber@mncn.csic.es RI Zardoya, Rafael/B-2291-2012; Ng, Peter/J-7393-2012 OI Zardoya, Rafael/0000-0001-6212-9502; NR 74 TC 24 Z9 26 U1 3 U2 16 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD APR PY 2004 VL 58 IS 4 BP 799 EP 813 PG 15 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 818GX UT WOS:000221234700013 PM 15154556 ER PT J AU Weiss, JV Emerson, D Megonigal, JP AF Weiss, JV Emerson, D Megonigal, JP TI Geochemical control of microbial Fe(III) reduction potential in wetlands: comparison of the rhizosphere to non-rhizosphere soil SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE rhizosphere; Fe(III) reduction; Fe-reducing bacteria; Fe plaque; mineralogy; freshwater wetland ID SALT-MARSH SEDIMENTS; CRYSTALLINE IRON(III) OXIDES; IRON-OXIDIZING BACTERIA; RICE ROOTS; PHRAGMITES-AUSTRALIS; AQUATIC SEDIMENTS; FRESH-WATER; REDUCING BACTERIA; LOBELIA-DORTMANNA; OXIDATION-STATES AB We compared the reactivity and microbial reduction potential of Fe(III) minerals in the rhizosphere and non-rhizosphere soil to test the hypothesis that rapid Fe(III) reduction rates in wetland soils are explained by rhizosphere processes. The rhizosphere was defined as the area immediately adjacent to a root encrusted with Fe(III)-oxides or Fe plaque, and non-rhizosphere soil was >0.5 cm from the root surface. The rhizosphere had a significantly higher percentage of poorly crystalline Fe (66 +/- 7%) than non-rhizosphere soil (23 +/- 7%),- conversely, non-rhizosphere soil had a significantly higher proportion of crystalline Fe (50 +/- 7%) than the rhizosphere (18 +/- 7%, P < 0.05 in all cases). The percentage of poorly crystalline Fe(III) was significantly correlated with the percentage of FeRB (r = 0.76), reflecting the fact that poorly crystalline Fe(III) minerals are labile with respect to microbial. reduction. Abiotic reductive dissolution consumed about 75% of the rhizosphere Fe(III)-oxide pool in 4 h compared to 23% of the soil Fe(III)-oxide pool. Similarly, microbial reduction consumed 75-80% of the rhizosphere pool in 10 days compared to 30-40% of the non-rhizosphere soil pool. Differences between the two pools persisted when samples were amended with an electron-shuttling compound (AQDS), an Fe (III)-reducing bacterium (Geobacter metallireducens), and organic carbon. Thus, Fe(III)-oxide mineralogy contributed strongly to differences in the Fe(III) reduction potential of the two pools. Higher amounts of poorly crystalline Fe(III) and possibly humic substances, and a higher Fe(III) reduction potential in the rhizosphere compared to the non-rhizosphere soil, suggested the rhizosphere is a site of unusually active microbial Fe cycling. The results were consistent with previous speculation that rapid Fe cycling in wetlands is due to the activity of wetland plant roots. (C) 2004 Federation of European Microbiological Societies. Published by Elsevier B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Amer Type Culture Collect, Manassas, VA 22010 USA. George Mason Univ, Environm Sci & Policy Dept, Fairfax, VA 22030 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM megonigalp@si.edu NR 69 TC 81 Z9 96 U1 7 U2 69 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-6496 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD APR 1 PY 2004 VL 48 IS 1 BP 89 EP 100 DI 10.1016/j.femsec.2003.12.014 PG 12 WC Microbiology SC Microbiology GA 811LM UT WOS:000220773400009 PM 19712434 ER PT J AU Chernova, NV Stein, DL AF Chernova, NV Stein, DL TI A remarkable new species of Psednos (Teleostei : Liparidae) from the western North Atlantic Ocean SO FISHERY BULLETIN LA English DT Article AB Psednos rossi new species (Teleostei: Liparidae) is described from two specimens collected in the North Atlantic Ocean off Cape Hatteras, North Carolina, at depths of 500674 m. Psednos rossi belongs to the P. christinae group, which includes six other species and is characterized by 46-47 vertebrae and the absence of a coronal pore. Psednos rossi differs from those six species by having characters unique within the genus: straight spine, body not humpbacked at the occiput, and a very large mouth with a vertical oral cleft. Other distinguishing characters include a notched pectoral fin with 15-16 rays, eye 17-19% SL, and color in life orange-rose. With P. rossi, the genus Psednos as currently known includes 26 described and five undescribed species of small meso- or bathypelagic liparids from the Atlantic, Pacific, and Indian Oceans. C1 NOAA, NMFS, Systemat Lab, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. RP Stein, DL (reprint author), NOAA, NMFS, Systemat Lab, Smithsonian Inst,Natl Museum Nat Hist, POB 37012,MRC-0153, Washington, DC 20013 USA. EM david.stein@noaa.gov NR 8 TC 5 Z9 5 U1 0 U2 2 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD APR PY 2004 VL 102 IS 2 BP 245 EP 250 PG 6 WC Fisheries SC Fisheries GA 817MV UT WOS:000221182500002 ER PT J AU Krot, AN Petaev, MI Yurimoto, H AF Krot, AN Petaev, MI Yurimoto, H TI Amoeboid olivine aggregates with low-Ca pyroxenes: A genetic link between refractory inclusions and chondrules? SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ALUMINUM-RICH INCLUSIONS; CARBONACEOUS CHONDRITE ACFER-094; SOLAR NEBULA; FERROMAGNESIAN CHONDRULES; ALLENDE METEORITE; CO3 CHONDRITES; CONDENSATION; ORIGIN; MINERALOGY; MURCHISON AB Amoeboid olivine aggregates (AOAs) in primitive (unmetamorphosed and unaltered) carbonaceous chondrites are uniformly O-16-enriched (Delta(17)O similar to -20parts per thousand) and consist of forsterite (Fa(<2)), FeNi-metal, and a refractory component (individual CAIs and fine-grained minerals interspersed with forsterite grains) composed of Al-diopside, anorthite, +/-spinel, and exceptionally rare melilite (Angstromk(<5)); some CAIs in AOAs have compact. igneous textures. Melilite in AOAs is replaced by a fine-grained Mixture of spinel, Al-diopside. and anorthite. Spinel is corroded by anorthite or by Al-diopside. In similar to10% of > 500 AOAs studied in the CR, CV, CM, CO, CH CB, and ungrouped carbonaceous chondrites Acfer 094, Adelaide, and LEW85332. forsterite is replaced to a various degree by low-Ca pyroxene. There are three major textural Occurrences of low-Ca pyroxene in AOAs: (i) thin (<10 mum) discontinuous layers around forsterite grains or alone forsterite brain boundaries in AOA peripheries (ii) haloes and subhedral grains around FeNi-metal nodules in AOA peripheries, and (iii) thick (up to 70 Am) continuous layers with abundant tiny inclusions of FeNi-metal grains around AOAs. AOAs with low-Ca pyroxene appear to have experienced melting Of Various degrees. In the most extensively melted AOA in the CV chondrite Leoville, only spinel grains are relict: forsterite. anorthite and Al-diopside were melted. This AOA has an igneous rim of low-Ca pyroxene with abundant FeNi-metal nodules and is texturally similar to Type I chondrules. Based on these observations and thermodynamic analysis, we conclude that AOAs are aggregates of relatively low temperature solar nebular condensates originated in O-16-rich gaseous reservoir(s), probably CAI-forming region(s). Some of the CAIs were melted before aggregation into AOAs. Many AOAs must have also experienced melting. but of a much smaller degree than chondrules. Before and possibly after aggregation, melilite and spinel reacted with the gaseous SiO and Mg to form Ca-Tschermakite (CaAi(2)SiO(6))-diopside (CaMgSi2O6) solid solution and anorthite. Solid or incipiently melted olivine in some AOAs reacted with gaseous SiO in the CAI- or chondrule-forming regions to form low-Ca pyroxene: Mg2SiO6 + SiO(g) + H2O(g) = Mg2Si2O6 + H-2(g). W Some low-Ca pyroxenes in AOAs may have formed by oxidation of Si-bearing FeNi-rnetal: Mg2Si2O4 + Si-(in FeNi) +2H(2)O((g)) = Mg2Si2O6 + 2H(2(g)) and by direct gas-solid condensation: Mg-(g) + SiO(g) +H2O(g) Mg2SiO6(s) + H-2(g) from fractionated (Mg/Si ratio < solar) nebular gas. Although bulk compositions of AOAs are rather similar to those of Type I chondrules, on the projection from Spinet onto the plane Ca2SiO4 -Mg2SiO4-Al2O3, these objects plot on different sides of the anorthite-forsterite thermal divide. suggesting that Type I chondrules cannot be produced from AOAs by an igneous fractionation. Formation of low-Ca pyroxene by reaction of AOAs with gaseous SiO and by melting of silica-rich dust accreted around AOAs moves bulk compositions of the AOAs towards chondrules, and provide possible mechanisms of transformation of refractory materials into chondrules or chondrule precursors. The rare occurrences of low-Ca pyroxene in AOAs may indicate that either AOAs were isolated from the hot nebular gas before condensation of low-Ca pyroxene or that condensation of low-Ca pyroxene by reaction between forsterite and gaseous SiO was kinetically inhibited. If the latter is correct, then the common Occurrences of pyroxene-rich Type I chondrules may require either direct condensation of low-Ca pyroxenes or SiO, from fractionated nebular gas or condensation of gaseous SiO into chondrule Melts. Copyright (C) 2004 Elsevier Ltd. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Tokyo Inst Technol, Dept Earth & Planetary Sci, Tokyo 1528551, Japan. RP Krot, AN (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu NR 62 TC 22 Z9 22 U1 0 U2 5 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 APR PY 2004 VL 68 IS 8 BP 1923 EP 1941 DI 10.1016/j.gca.2003.10.026 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 813FD UT WOS:000220892100017 ER PT J AU Schneider, G Pasachoff, JM Golub, L AF Schneider, G Pasachoff, JM Golub, L TI TRACE observations of the 15 November 1999 transit of Mercury and the Black Drop effect: considerations for the 2004 transit of Venus SO ICARUS LA English DT Article DE Mercury; Venus; instrumentation ID LUNAR OCCULTATIONS; TRAVELS; TRIBULATIONS AB Historically, the visual manifestation of the "Black Drop effect," the appearance of a band linking the solar limb to the disk of a transiting planet near the point of internal tangency, had limited the accuracy of the determination of the Astronomical Unit and the scale of the Solar System in the 18th and 19th centuries. This problem was misunderstood in the case of Venus during its rare transits due to the presence of its atmosphere. We report on observations of the 15 November 1999 transit of Mercury obtained, without the degrading effects of the Earth's atmosphere, with the Transition Region and Coronal Explorer spacecraft. In spite of the telescope's location beyond the Earth's atmosphere, and the absence of a significant mercurian atmosphere, a faint Black Drop effect was detected. After calibration and removal of, or compensation for, both internal and external systematic effects, the only radially directed brightness anisotropies found resulted from the convolution of the instrumental point-spread function with the solar limb-darkened, back-lit, illumination function. We discuss these effects in light of earlier ground-based observations of transits of Mercury and of Venus (also including the effects of atmospheric "seeing") to explain the historical basis for the Black Drop effect. The methodologies we outline here for improving upon transit imagery are applicable to ground-based (adaptive optics augmented) and space-based observations of the 8 June 2004 and 5-6 June 2012 transits of Venus, providing a path to achieving high-precision measurements at and near the instants of internal limb tangencies. (C) 2004 Elsevier Inc. All rights reserved. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Williams Coll, Hop Observ, Williamstown, MA 01267 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Schneider, G (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM gschneider@as.arizona.edu OI Golub, Leon/0000-0001-9638-3082 NR 45 TC 20 Z9 20 U1 0 U2 1 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 APR PY 2004 VL 168 IS 2 BP 249 EP 256 DI 10.1016/j.icarus.2003.11.020 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 807AL UT WOS:000220474300003 ER PT J AU Valencia, R Foster, RB Villa, G Condit, R Svenning, JC Hernandez, C Romoleroux, K Losos, E Magard, E Balslev, H AF Valencia, R Foster, RB Villa, G Condit, R Svenning, JC Hernandez, C Romoleroux, K Losos, E Magard, E Balslev, H TI Tree species distributions and local habitat variation in the Amazon: large forest plot in eastern Ecuador SO JOURNAL OF ECOLOGY LA English DT Article DE Amazonian Ecuador; catena; habitat partitioning; topographic niche; tropical forest diversity; tropical trees; Yasuni National Park ID TERRA-FIRME FORESTS; RAIN-FOREST; RECRUITMENT LIMITATION; FLORISTIC PATTERNS; NEOTROPICAL FOREST; PUERTO-RICO; LONG-TERM; DIVERSITY; HETEROGENEITY; TOPOGRAPHY AB 1 We mapped and identified all trees greater than or equal to 10 mm in diameter in 25 ha of lowland wet forest in Amazonian Ecuador, and found 1104 morphospecies among 152 353 individuals. The largest number of species was mid-sized canopy trees with maximum height 10-20 m and understorey treelets with maximum height of 5-10 m. 2 Several species of understorey treelets in the genera Matisia and Rinorea dominated the forest numerically, while important canopy species were Iriartea deltoidea and Eschweilera coriacea. 3 We examined how species partition local topographic variation into niches, and how much this partitioning contributes to forest diversity. Evidence in favour of topographic niche-partitioning was found: similarity in species composition between ridge and valley quadrats was lower than similarity between two valley (or two ridge) quadrats, and 25% of the species had large abundance differences between valley and ridge-top. On the other hand, 25% of the species were generalists, with similar abundance on both valley and ridges, and half the species had only moderate abundance differences between valley and ridge. 4 Topographic niche-partitioning was not finely grained. There were no more than three distinct vegetation zones: valley, mid-slope, and upper-ridge, and the latter two differed only slightly in species composition. 5 Similarity in species composition declined with distance even within a topographic habitat, to about the same degree as it declined between habitats. This suggests patchiness not related to topographic variation, and possibly due to dispersal limitation. 6 We conclude that partitioning of topographic niches does make a contribution to the alpha-diversity of Amazonian trees, but only a minor one. It provides no explanation for the co-occurrence of hundreds of topographic generalists, nor for the hundreds of species with similar life-form appearing on a single ridge-top. C1 Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. Pontificia Univ Catolica Ecuador, Dept Biol Sci, Quito, Ecuador. Field Museum, Dept Bot, Chicago, IL 60605 USA. Univ Aarhus, Dept Systemat Bot, DK-8240 Risskov, Denmark. Smithsonian Inst, Ctr Trop Forest Sci, Washington, DC 20560 USA. RP Condit, R (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. EM condit@ctfs.si.edu RI Svenning, Jens-Christian/C-8977-2012 OI Svenning, Jens-Christian/0000-0002-3415-0862 NR 67 TC 242 Z9 282 U1 5 U2 73 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD APR PY 2004 VL 92 IS 2 BP 214 EP 229 DI 10.1111/j.0022-0477.2004.00876.x PG 16 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 805RD UT WOS:000220382500003 ER PT J AU Lovelock, CE Wright, SF Clark, DA Ruess, RW AF Lovelock, CE Wright, SF Clark, DA Ruess, RW TI Soil stocks of glomalin produced by arbuscular mycorrhizal fungi across a tropical rain forest landscape SO JOURNAL OF ECOLOGY LA English DT Article DE Costa Rica; mycorrhizas; soil carbon; soil fertility; soil nitrogen ID NITROGEN DEPOSITION; AGGREGATE STABILITY; NUTRIENT AVAILABILITY; ROOT COLONIZATION; CARBON STORAGE; ELEVATED CO2; WET FOREST; LIFE-SPAN; COMMUNITIES; HYPOTHESIS AB 1 Symbiotic arbuscular mycorrhizal (AM) fungi produce a recalcitrant AM-specific glycoprotein, glomalin, which could be a substantial contributor to soil carbon (C). In this study we made a first assessment of the standing stocks of glomalin in a tropical lowland rain forest (the La Selva Biological Station, Costa Rica) and tested whether glomalin concentrations varied over the strong fertility gradient in this forest. 2 Mean levels of glomalin in the top 10 cm of the La Selva soils were 3.94 +/- 0.16 mg cm(-3) (1.45 Mg C ha(-1)), accounting for approximately 3.2% of total soil C and 5% of soil nitrogen (N) in the 0-10 cm soil layer. 3 More fertile soils with higher concentrations of calcium, phosphorus and potassium had less glomalin, while the less fertile soils, those with high C : N ratios and high levels of iron and aluminium, had more glomalin. 4 We found higher levels of immunoreactivity, which is characteristic of young, recently produced glomalin, in the soils with higher concentrations of calcium, phosphorus and potassium. We hypothesize that AM fungal turnover, as indicated by a greater proportion of immunoreactive, recently produced glomalin, is enhanced in the more fertile soils within this tropical rain forest landscape. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. ARS, USDA, Sustainable Agr Syst Lab, Beltsville, MD 20705 USA. Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. RP Lovelock, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM lovelockc@si.edu RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 52 TC 75 Z9 96 U1 8 U2 50 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD APR PY 2004 VL 92 IS 2 BP 278 EP 287 DI 10.1111/j.0022-0477.2004.00855.x PG 10 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 805RD UT WOS:000220382500008 ER PT J AU Uriarte, M Condit, R Canham, CD Hubbell, SP AF Uriarte, M Condit, R Canham, CD Hubbell, SP TI A spatially explicit model of sapling growth in a tropical forest: does the identity of neighbours matter? SO JOURNAL OF ECOLOGY LA English DT Article DE Barro Colorado Island; density-dependence; ecological equivalence; neighbourhood effects; neutral theory ID DENSITY-DEPENDENCE; INDIVIDUAL TREES; RAIN-FOREST; HOST-SPECIFICITY; NEOTROPICAL TREE; PLANT COMMUNITY; COMPETITION; DIVERSITY; MORTALITY; RECRUITMENT AB 1 We quantified neighbourhood effects on sapling growth for 60 tree species in the 50-ha plot in Barro Colorado Island, Panama. Additionally, we tested whether target sapling growth responds to taxonomic or functional identity of neighbouring species by comparing four alternate models (that all neighbours have equivalent effects on the target; that conspecific and heterospecific neighbours have distinct effects; that heterospecific neighbours can be divided into confamilials and non-confamilials; and that they can be divided according to their response to light availability). 2 Over half of the species (34 out of 60) analysed were consistent with all neighbours having equivalent effects on the target. This may result from diffuse evolution allowing tolerance of a large number of neighbouring species or could be a statistical artefact of over-clumping species into large neighbour groups (e.g. heterospecific neighbours). 3 Other species supported models that differentiated between conspecific and heterospecific (n = 6) or between confamilial vs. non-confamilial (n = 5) neighbours and, in general, effects of neighbours were stronger if they were more closely related to the target. Where target species differentiated between neighbours from different light guilds (n = 15), effects were stronger if both belonged to the same guild (i.e. both gap requiring or both shade tolerant). 4 Despite the fact that the majority of species did not respond to the identity of neighbours, all differed in their response to the degree of crowding. Our results suggest that the response of target species to crowding, rather than individual species effects on targets, may be subject to selection. 5 Variation among species in response to crowding or to the identity of neighbouring species is likely to contribute to the maintenance of species diversity in tropical forests. C1 Inst Ecosyst Studies, Millbrook, NY 12545 USA. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. Univ Georgia, Dept Plant Biol, Athens, GA 30606 USA. RP Uriarte, M (reprint author), Inst Ecosyst Studies, Box AB, Millbrook, NY 12545 USA. EM uriartem@ecostudies.org RI Canham, Charles/F-6161-2011; Uriarte, Maria/L-8944-2013 OI Canham, Charles/0000-0001-8361-9148; NR 48 TC 147 Z9 152 U1 4 U2 62 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD APR PY 2004 VL 92 IS 2 BP 348 EP 360 DI 10.1111/j.0022-0477.2004.00867.x PG 13 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 805RD UT WOS:000220382500015 ER PT J AU Patterson, RT Fowler, AD Huber, BT AF Patterson, RT Fowler, AD Huber, BT TI Evidence of hierarchical organization in the planktic foraminiferal evolutionary record SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID SEA-SURFACE TEMPERATURES; EXTINCTION STATISTICS; SELF-ORGANIZATION; BOUNDARY; MODEL; TAXONOMY; CLIMATE; IMPACT AB The Wavelet Transform was used to analyze the evolutionary record of planktic foraminifera to distinguish specific structure not previously resolvable. Both the speciation and extinction wavelets are characterized by a major singularity at the Cretaceous-Tertiary (K-T) boundary, when there was a total breakdown in the interconnectedness of ecosystems related to sharply reduced diversity following the Chicxulub impact event. The speciation wavelet is also characterized by an interval consisting of a hierarchical array of five orders of bifurcation, which are related to repeated iterative radiation of species from the Albian to Maastrichtian. These planktic foraminiferal extinction patterns were related to quasi-periodic orogenic cycles of the Cretaceous that, in turn, produced episodic mantle CO(2)-degassing, oceanic volcanism and anoxia, and sea level fluctutations. We hypothesize that the hierarchical structure observed is a reflection of this process in an otherwise stochastic system. C1 Carleton Univ, Ottawa Carleton Geosci Ctr, Ottawa, ON K1S 5B6, Canada. Carleton Univ, Dept Earth Sci, Ottawa, ON K1S 5B6, Canada. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Patterson, RT (reprint author), Carleton Univ, Ottawa Carleton Geosci Ctr, Ottawa, ON K1S 5B6, Canada. EM tpatters@ccs.carleton.ca NR 59 TC 11 Z9 11 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 2004 VL 34 IS 2 BP 85 EP 95 DI 10.2113/0340085 PG 11 WC Paleontology SC Paleontology GA 825HK UT WOS:000221746700001 ER PT J AU Simbotin, I Stroe, M Gavrila, M AF Simbotin, I Stroe, M Gavrila, M TI Quasistationary stabilization and atomic dichotomy in superintense low-frequency fields SO LASER PHYSICS LA English DT Article; Proceedings Paper CT 12th Annual International Laser Physics Workshop CY AUG 25-29, 2003 CL Hamburg, GERMANY SP Deutsch Forsch Gemeinsch, Russian Fdn Basic Res, Russian Federat, Minist Ind, Sci & Technol, Unites States European Off Aerosp Res & Dev ID KRAMERS-HENNEBERGER APPROXIMATION; INTENSE LASER FIELDS; FLOQUET-THEORY; POLARIZATION; IONIZATION; HYDROGEN; STATES; SCATTERING AB Quasistationary (adiabatic) stabilization (QS) and atomic dichotomy have been considered as high-frequency concepts. We now show analytically and numerically that they apply also at low frequencies, on condition that the intensity is sufficiently high. The derivation is based on the iteration procedure developed earlier within the nonrelativistic high-frequency Floquet theory (HFFT) for the physical 3D hydrogen atom. We show that the successive iterations yielding the quasienergy E equivalent to W - (i/2)Gamma converge not only at large omega and arbitrary intensity (or excursion alpha(0)), which is the HFFT case, but also at sufficiently large alpha(0) and arbitrary omega. As a consequence, for linear polarization, at large alpha(0), the energies W(alpha(0)) have the familiar decrease of alpha(0)(-2/3) towards some threshold nomega, the atomic structure displays dichotomy, and the Gamma undergo QS. This shows that the iteration procedure is, in fact, a high-frequency, high-intensity Floquet theory (HI-HFFT). The general 3D results are illustrated numerically on a 1D model with a soft-core Coulomb potential. We have computed accurate Floquet quasienergies E(alpha(0)) for the lowest 18 states from alpha(0) = 0 to 100 at two low frequencies omega. It is for the first time that such an extended range of alpha(0) has been covered by a Floquet calculation. We show that the results for W(alpha(0)) and Gamma(alpha(0)) are in agreement with the predictions of HI-HFFT. In particular, F(alpha(0)) tends to zero (albeit in an oscillatory manner), thereby displaying QS. Dichotomy is illustrated by studying the behavior of the components of the Floquet solution. In view of the possibility of expanding atomic wave packets in terms of superpositions of Floquet states, the dynamical conclusion of our result is that one-electron systems become stable in superintense fields of any frequency within nonrelativistic theory. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Univ Bucharest, Dept Chem, Bucharest, Romania. FOM, Inst Atom & Mol Phys, NL-1098 SJ Amsterdam, Netherlands. RP Simbotin, I (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. EM gavrila@amolf.nl RI Stroe, Marius Cristian/D-1125-2014 NR 22 TC 4 Z9 4 U1 0 U2 1 PU INTERPERIODICA PI BIRMINGHAM PA PO BOX 1831, BIRMINGHAM, AL 35201-1831 USA SN 1054-660X J9 LASER PHYS JI Laser Phys. PD APR PY 2004 VL 14 IS 4 BP 482 EP 491 PG 10 WC Optics; Physics, Applied SC Optics; Physics GA 817ZZ UT WOS:000221216700009 ER PT J AU Schroll, S AF Schroll, S TI Jean Dubuffet: Trace of an adventure. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 1 PY 2004 VL 129 IS 6 BP 90 EP 90 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 807MD UT WOS:000220504700055 ER PT J AU Landman, NH Cochran, JK Cerrato, R Mak, J Roper, CFE Lu, CC AF Landman, NH Cochran, JK Cerrato, R Mak, J Roper, CFE Lu, CC TI Habitat and age of the giant squid (Architeuthis sanctipauli) inferred from isotopic analyses SO MARINE BIOLOGY LA English DT Article ID STATOLITH MICROSTRUCTURE; OXYGEN; GROWTH; CARBON; WATERS; FRACTIONATION; RADIOCARBON; TEMPERATURE; MORPHOLOGY; MATURITY AB The age and habitat of the giant squid, Architeuthis sanctipauli Velain, 1877, were determined based on isotopic analyses of the statoliths of three female specimens captured off Tasmania, Australia, between January and March 1996. Assuming that the aragonite of the statoliths formed in equilibrium with seawater, delta(18)O analyses indicated that the squid lived at temperatures of 10.5-12.9degreesC, corresponding to average depths of 125-250 m and maximum depths of 500 m. The capture records indicated that these squid may have occasionally ranged still deeper, to as much as 1000 m. All the statoliths were labeled with bomb C-14 (Delta(14)C=+22.9parts per thousand to +44.6parts per thousand), consistent with the depths inferred from delta(18)O. A thin section through one of the statoliths revealed 351 growth increments grouped into check-ring structures every 10-16 increments. A model for statolith growth and the pattern of temporal change in Delta(14)C in the water column was used to estimate the ages of the three specimens. These estimates were very sensitive to the choice of depth range over which Delta(14)C values were integrated. Assuming that the capture depths represented the maximum habitat depths of these individuals, the calculations suggested an age of 14 years or less. More refined age estimates require a better understanding of the variation of Delta(14)C and temperature with depth in the areas in which the squids live. C1 Amer Museum Nat Hist, New York, NY 10024 USA. SUNY Stony Brook, Marine Sci Res Ctr, Stony Brook, NY 11794 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Natl Chung Hsing Univ, Taichung 402, Taiwan. RP Landman, NH (reprint author), Amer Museum Nat Hist, 79th St & Cent Pk W, New York, NY 10024 USA. EM landman@amnh.org NR 31 TC 11 Z9 14 U1 2 U2 20 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD APR PY 2004 VL 144 IS 4 BP 685 EP 691 DI 10.1007/s00227-003-1245-y PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 808HQ UT WOS:000220560600007 ER PT J AU Ross, DJ Johnson, CR Hewitt, CL Ruiz, GM AF Ross, DJ Johnson, CR Hewitt, CL Ruiz, GM TI Interaction and impacts of two introduced species on a soft-sediment marine assemblage in SE Tasmania SO MARINE BIOLOGY LA English DT Article ID CARCINUS-MAENAS; COMMUNITY STRUCTURE; ASTERIAS-AMURENSIS; SHORE CRAB; GREEN CRAB; PREDATION; INVASION; CALIFORNIA; BIVALVES; ECOLOGY AB Introduced species are having major impacts in terrestrial, freshwater and marine ecosystems world-wide. It is increasingly recognised that effects of multiple species often cannot be predicted from the effect of each species alone, due to complex interactions, but most investigations of invasion impacts have examined only one non-native species at a time and have not addressed the interactive effects of multiple species. We conducted a field experiment to compare the individual and combined effects of two introduced marine predators, the northern Pacific seastar Asterias amurensis and the European green crab Carcinus maenas, on a soft-sediment invertebrate assemblage in Tasmania. Spatial overlap in the distribution of these invaders is just beginning in Tasmania, and appears imminent as their respective ranges expand, suggesting a strong overlap in food resources will result from the shared proclivity for bivalve prey. A. amurensis and C. maenas provide good models to test the interaction between multiple introduced predators, because they leave clear predator-specific traces of their predatory activity for a number of common prey taxa (bivalves and gastropods). Our experiments demonstrate that both predators had a major effect on the abundance of bivalves, reducing populations of the commercial bivalves Fulvia tenuicostata and Katelysia rhytiphora. The interaction between C. maenas and A. amurensis appears to be one of resource competition, resulting in partitioning of bivalves according to size between predators, with A. amurensis consuming the large and C. maenas the small bivalves. At a large spatial scale, we predict that the combined effect on bivalves may be greater than that due to each predator alone simply because their combined distribution is likely to cover a broader range of habitats. At a smaller scale, in the shallow subtidal, where spatial overlap is expected to be most extensive, our results indicate the individual effects of each predator are likely to be modified in the presence of the other as densities increase. These results further highlight the need to consider the interactive effects of introduced species, especially with continued increases in the number of established invasions. C1 Univ Tasmania, Sch Zool, Sandy Bay, Tas 7000, Australia. Univ Tasmania, Tasmanian Aquaculture & Fisheries Inst, Sandy Bay, Tas 7000, Australia. CSIRO Marine Res, Ctr Res Introduced Marine Res, Hobart, Tas 7001, Australia. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Ross, DJ (reprint author), Univ Melbourne, Dept Zool, Melbourne, Vic 3010, Australia. EM rossdj@unimelb.edu.au RI Ross, Donald/F-7607-2012; Hewitt, Chad/C-4460-2008; Johnson, Craig/E-1788-2013 OI Ruiz, Gregory/0000-0003-2499-441X; Ross, Donald/0000-0002-8659-3833; Hewitt, Chad/0000-0002-6859-6512; Johnson, Craig/0000-0002-9511-905X NR 56 TC 40 Z9 43 U1 8 U2 27 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD APR PY 2004 VL 144 IS 4 BP 747 EP 756 DI 10.1007/s00227-003-1223-4 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 808HQ UT WOS:000220560600013 ER PT J AU Bay, LK Choat, JH van Herwerden, L Robertson, DR AF Bay, LK Choat, JH van Herwerden, L Robertson, DR TI High genetic diversities and complex genetic structure in an Indo-Pacific tropical reef fish (Chlorurus sordidus): evidence of an unstable evolutionary past? SO MARINE BIOLOGY LA English DT Review ID GREAT-BARRIER-REEF; MITOCHONDRIAL-DNA VARIATION; HERBIVOROUS GRAZING FISHES; CORAL-REEF; POPULATION-STRUCTURE; CLADISTIC-ANALYSIS; WEST PACIFIC; PHENOTYPIC ASSOCIATIONS; COMPARATIVE PHYLOGEOGRAPHY; GEOGRAPHICAL-DISTRIBUTION AB Historical sea level fluctuations have influenced the genetic structure and evolutionary history of marine species and examining widespread species across their species' ranges may elucidate some of these effects. Chlorurus sordidus is a common and widespread parrotfish found on coral reefs throughout the Indo-central Pacific. We used phylogenetic, phylogeographic, and cladistic analyses to examine the genetic composition and population structure of this species across most of its latitudinal range limits. We sequenced 354 bp of the mitochondrial control region I in 185 individuals from nine populations. Populations of C. sordidus displayed high levels of genetic diversity, similar to those recorded for widespread pelagic fish species, but much greater nucleotide diversity values than those previously recorded for other demersal reef fishes. Both phylogenetic and phylogeographic analyses detected strong genetic subdivision at the largest spatial scale (i.e. among oceans). The Pacific Ocean was characterised by weak population genetic structure. Separation of the Hawaiian location from other Pacific and West Indian Ocean sites was evident in phylogenetic analyses, but not from analysis of molecular variance. NCA and isolation-by-distance tests suggested that the genetic structure of this species was the result of multiple contemporary and historical processes, including long-distance colonisation and range expansion arising from fluctuating sea levels, limited current gene flow, and isolation by distance. This pattern is to be expected when historically fragmented populations come into secondary contact. We suggest the patterns of population genetic structure recorded in C. sordidus are caused by large local population sizes, high gene flow, and a recent history of repeated fragmentation and remixing of populations resulting from fluctuating sea levels. C1 James Cook Univ N Queensland, Mol Ecol & Evolut Lab, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. Smithsonian Trop Res Inst Panama, STRI, APO, AA 34002 USA. RP Bay, LK (reprint author), James Cook Univ N Queensland, Mol Ecol & Evolut Lab, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. EM Line.bay@jcu.edu.au RI Bay, Line/D-4037-2009; van Herwerden, Lynne/I-1087-2012 OI van Herwerden, Lynne/0000-0001-6717-8995 NR 101 TC 80 Z9 83 U1 0 U2 19 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD APR PY 2004 VL 144 IS 4 BP 757 EP 767 DI 10.1007/s00227-003-1224-3 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 808HQ UT WOS:000220560600014 ER PT J AU Murphy, K Boehme, J Coble, P Cullen, J Field, P Moore, W Perry, E Sherrell, R Ruiz, G AF Murphy, K Boehme, J Coble, P Cullen, J Field, P Moore, W Perry, E Sherrell, R Ruiz, G TI Verification of mid-ocean ballast water exchange using naturally occurring coastal tracers SO MARINE POLLUTION BULLETIN LA English DT Article DE ballast water; biological invasions; chemical oceanography; optical properties; radioisotopes; metals; verification ID ATLANTIC-OCEAN; MEDITERRANEAN SEA; NORTH PACIFIC; ARABIAN SEA; ICP-MS; BARIUM; MANGANESE; MARINE; SEAWATER; RADIUM AB We examined methods for verifying whether or not ships have performed mid-ocean ballast water exchange (BWE) on four commercial vessels operating in the Pacific and Atlantic Oceans. During BWE, a ship replaces the coastal water in its ballast tanks with water drawn from the open ocean, which is considered to harbor fewer organisms capable of establishing in coastal environments. We measured concentrations of several naturally occurring chemical tracers (salinity, six trace elements, colored dissolved organic matter fluorescence and radium isotopes) along ocean transects and in ballast tanks subjected to varying degrees of BWE (0-99%). Many coastal tracers showed significant concentration changes due to BWE, and our ability to detect differences between exchanged and unexchanged ballast tanks was greatest under multivariate analysis. An expanded dataset, which includes additional geographic regions, is now needed to test the generality of our results. (C) 2003 Elsevier Ltd. All rights reserved. C1 Smithsonian Environm Res Ctr, Marine Invas Res Lab, Edgewater, MD 21037 USA. Univ S Carolina, Dept Geol Sci, Columbia, SC 29208 USA. Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. RP Smithsonian Environm Res Ctr, Marine Invas Res Lab, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM murphyka@si.edu RI Murphy, Kathleen/B-8217-2009; OI Murphy, Kathleen/0000-0001-5715-3604; Ruiz, Gregory/0000-0003-2499-441X NR 46 TC 20 Z9 20 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD APR PY 2004 VL 48 IS 7-8 BP 711 EP 730 DI 10.1016/j.marpolbul.2003.10.015 PG 20 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 811LL UT WOS:000220773300019 PM 15041428 ER PT J AU Brady, SG Danforth, BN AF Brady, SG Danforth, BN TI Recent intron gain in elongation factor-1 alpha of colletid bees (Hymenoptera : Colletidae) SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE elongation factor-1 alpha (EF-1 alpha); intron gain; bees; Apiformes; Colletidae; phylogeny ID SPLICEOSOMAL INTRONS; DROSOPHILA-MELANOGASTER; MOLECULAR PHYLOGENY; 1-ALPHA EF-1-ALPHA; GENES; EVOLUTION; POSITIONS; SEQUENCES; INSECTS; NUCLEAR AB We discovered the presence of a unique spliceosomal intron in the F1 copy of elongation factor-1alpha (EF-1alpha) restricted to the bee family Colletidae (Hymenoptera: Apoidae). The intron ranges in size from 101 to 1,044 bp and shows no positional sliding. Our data also demonstrate the complete absence of this intron from exemplars representing all other bee families, as well as from close hymenopteran relatives. A review of the literature finds that this intron is likewise absent from all other arthropods for which data are available. This provides unambiguous evidence for a relatively recent intron insertion event in the colletid common ancestor and, at least in this specific instance, lends support to the introns-late hypothesis. The comparative distribution of this novel intron also supports the monophyly of Colletidae and the exclusion of the Stenotritidae from this family, providing an example of the potential of some introns to act as robust markers of shared descent. C1 Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. RP Brady, SG (reprint author), Smithsonian Inst, Lab Analyt Biol, MRC 534, Suitland, MD 20746 USA. EM brady.sean@nmnh.si.edu NR 61 TC 24 Z9 25 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD APR PY 2004 VL 21 IS 4 BP 691 EP 696 DI 10.1093/molbev/msh062 PG 6 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 810DO UT WOS:000220685200008 PM 14739243 ER PT J AU McCartney, MA Lessios, HA AF McCartney, MA Lessios, HA TI Adaptive evolution of sperm bindin tracks egg incompatibility in neotropical sea urchins of the genus Echinometra SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article ID CODON-SUBSTITUTION MODELS; GAMETE RECOGNITION; SEXUAL SELECTION; REPRODUCTIVE ISOLATION; MOLECULAR EVOLUTION; POSITIVE SELECTION; MITOCHONDRIAL-DNA; RAPID EVOLUTION; STRONGYLOCENTROTUS-PURPURATUS; NONSYNONYMOUS SUBSTITUTION AB Bindin is a gamete recognition protein known to control species-specific sperm-egg adhesion and membrane fusion in sea urchins. Previous analyses have shown that diversifying selection on bindin amino acid sequence is found when gametically incompatible species are compared, but not when species are compatible. The present study analyzes bindin polymorphism and divergence in the three closely related species of Echinometra in Central America: E. lucunter and E. viridis from the Caribbean, and E. vanbrunti from the eastern Pacific. The eggs of E. lucunter have evolved a strong block to fertilization by sperm of its neotropical congeners, whereas those of the other two species have not. As in the Indo-West Pacific (IWP) Echinometra, the neotropical species show high intraspecific bindin polymorphism in the same gene regions as in the IWT species. Maximum likelihood analysis shows that many of the polymorphic codon sites are under mild positive selection. Of the fixed amino acid replacements, most have accumulated along the bindin lineage of E. lucunter. We analyzed the data with maximum likelihood models of variation in positive selection across lineages and codon sites, and with models that consider sites and lineages simultaneously. Our results show that positive selection is concentrated along the E. lucunter bindin lineage, and that codon sites with amino acid replacements fixed in this species show by far the highest signal of positive selection. Lineage-specific positive selection paralleling egg incompatibility provides support that adaptive evolution of sperm proteins acts to maintain recognition of bindin by changing egg receptors. Because both egg incompatibility and bindin divergence are greater between allopatric species than between sympatric species, the hypothesis of selection against hybridization (reinforcement) cannot explain why adaptive evolution has been confined to a single lineage in the American Echinometra. Instead, processes acting to varying degrees within species (e.g., sperm competition, sexual selection, and sexual conflict) are more promising explanations for lineage-specific positive selection on bindin. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP McCartney, MA (reprint author), Univ N Carolina, Dept Sci Biol, Wilmington, NC 28401 USA. EM mccartneym@unew.edu NR 78 TC 54 Z9 55 U1 2 U2 11 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD APR PY 2004 VL 21 IS 4 BP 732 EP 745 DI 10.1093/molbev/msh071 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 810DO UT WOS:000220685200013 PM 14963103 ER PT J AU Austerlitz, F Dick, CW Dutech, C Klein, EK Oddou-Muratorio, S Smouse, PE Sork, VL AF Austerlitz, F Dick, CW Dutech, C Klein, EK Oddou-Muratorio, S Smouse, PE Sork, VL TI Using genetic markers to estimate the pollen dispersal curve SO MOLECULAR ECOLOGY LA English DT Article DE gene flow; long-distance dispersal; microsatellites; plants; trees; TWOGENER ID 2-GENERATION ANALYSIS; PLANT-POPULATIONS; TROPICAL TREES; FLOW; LANDSCAPE; FOREST; SEED; DIFFERENTIATION; MITOCHONDRIAL; CALIFORNIA AB Pollen dispersal is a critical process that shapes genetic diversity in natural populations of plants. Estimating the pollen dispersal curve can provide insight into the evolutionary dynamics of populations and is essential background for making predictions about changes induced by perturbations. Specifically, we would like to know whether the dispersal curve is exponential, thin-tailed (decreasing faster than exponential), or fat-tailed (decreasing slower than the exponential). In the latter case, rare events of long-distance dispersal will be much more likely. Here we generalize the previously developed TWOGENER method, assuming that the pollen dispersal curve belongs to particular one- or two-parameter families of dispersal curves and estimating simultaneously the parameters of the dispersal curve and the effective density of reproducing individuals in the population. We tested this method on simulated data, using an exponential power distribution, under thin-tailed, exponential and fat-tailed conditions. We find that even if our estimates show some bias and large mean squared error (MSE), we are able to estimate correctly the general trend of the curve - thin-tailed or fat-tailed - and the effective density. Moreover, the mean distance of dispersal can be correctly estimated with low bias and MSE, even if another family of dispersal curve is used for the estimation. Finally, we consider three case studies based on forest tree species. We find that dispersal is fat-tailed in all cases, and that the effective density estimated by our model is below the measured density in two of the cases. This latter result may reflect the difficulty of estimating two parameters, or it may be a biological consequence of variance in reproductive success of males in the population. Both the simulated and empirical findings demonstrate the strong potential of TWOGENER for evaluating the shape of the dispersal curve and the effective density of the population (d(e)). C1 Univ Paris 11, UMR CNRS 8079, Lab Ecol Systemat & Evolut, F-91405 Orsay, France. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, Los Angeles, CA 90095 USA. INRA Bordeaux, UMR BioGEco, F-33883 Villenave Dornon, France. INRA INAPG ENGREF, UMR Biometrie & Intelligence Artificielle 518, F-75231 Paris 05, France. Off Natl Forets, Conservatoire Genet Arbres Forestiers, F-45160 Olivet, France. Rutgers State Univ, Dept Ecol Evolut & Nat Resources, New Brunswick, NJ 08903 USA. RP Austerlitz, F (reprint author), Univ Paris 11, UMR CNRS 8079, Lab Ecol Systemat & Evolut, F-91405 Orsay, France. EM Frederic.Austerlitz@ese.u-psud.fr RI Dick, Christopher/A-8744-2008; OI ODDOU-MURATORIO, Sylvie/0000-0003-2374-8313 NR 41 TC 176 Z9 185 U1 2 U2 52 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD APR PY 2004 VL 13 IS 4 BP 937 EP 954 DI 10.1111/j.1365-294X.2004.02100.x PG 18 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 802GW UT WOS:000220153000017 PM 15012767 ER PT J AU Quenouille, B Bermingham, E Planes, S AF Quenouille, B Bermingham, E Planes, S TI Molecular systematics of the damselfishes (Teleostei : Pomacentridae): Bayesian phylogenetic analyses of mitochondrial and nuclear DNA sequences SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Pomacentridae; mtDNA; ncDNA; Bayesian methods; taxonomic sampling ID V(D)J RECOMBINATION; MARQUESAS ISLANDS; INFERENCE; REEF; BIOGEOGRAPHY; EVOLUTION; RAG-1; SUBSTITUTION; LIKELIHOOD; BOOTSTRAP AB Damselfishes in the family Pomacentridae represent one of the few families of reef fishes found on coral reefs irrespective of location. At a local scale, damselfishes are often the most abundant coral reef fish, and their study has provided much of our current understanding of the ecology of tropical reef animals. The study of phylogenetic relationships among the Pomacentridae has lagged ecological investigation of the group, thus limiting historical perspective on the remarkable species richness of the family. In this study, we used 1989 bp of DNA sequence representing three mitochondrial genes and 1500 bp of the single copy nuclear RAG1 region to infer hypotheses of relationship for the group. Our analysis includes 103 Pomacentridae species in 18 genera, and three of the four named subfamilies: Amphriprioninae, Chrominae, and Pomacentrinae. The Bayesian method of phylogenetic reconstruction was applied to the data, because even with a large number of sequences it is an efficient means of analysis that provides intuitive measures of support for tree topologies and for the parameters of the nucleotide substitution model. Four Pomacentridae clades were identified with high statistical support whether the data were analyzed from a mtDNA, RAG1 or combined perspective, and in all analyses the current subfamilial classification of the Pornacentridae was rejected. At the genus level, Amphiprion, Chromis, and Chrysiptera were also rejected as natural groups. Abudefduf, Amblyglyphidodon, Dascyllus, Neoglyphidodon, Neopomacentrus, and Pomacentrus were each strongly supported as monophyletic genera but the support for monophyly is nonetheless compromised by sample size, except in the case of Dascyllus and Abudefduf for which we have sampled almost all of the described species. (C) 2003 Elsevier Inc. All rights reserved. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Perpignan, CNRS, Ecole Prat Hautes Etud, UMR 8046, Perpignan, France. RP Quenouille, B (reprint author), Smithsonian Trop Res Inst, Apdo 2072, Balboa, Panama. EM quenovib@naos.si.edu NR 77 TC 82 Z9 89 U1 1 U2 21 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2004 VL 31 IS 1 BP 66 EP 88 DI 10.1016/s1055-7903(03)00278-1 PG 23 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 807YM UT WOS:000220536800007 PM 15019609 ER PT J AU Joseph, L Wilke, T Bermingham, E Alpers, D Ricklefs, R AF Joseph, L Wilke, T Bermingham, E Alpers, D Ricklefs, R TI Towards a phylogenetic framework for the evolution of shakes, rattles, and rolls in Myiarchus tyrant-flycatchers (Aves : Passeriformes : Tyrannidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Myiarchus; systematics; phylogeny; passerines; suboscines ID MITOCHONDRIAL-DNA; MORPHOLOGY; BEHAVIOR; BIOGEOGRAPHY; RELIABILITY; SYSTEMATICS; DIVERGENCE; SPECIATION; BOOTSTRAP; TREES AB A phylogeny of 19 of the 22 currently recognized species of Myiarchus tyrant-flycatchers is presented. It is based on 842 bp of mitochondrial DNA (mtDNA) sequences from the ATPase subunit 8 and ATPase subunit 6 genes. Except for the morphologically distinct M. semirufus, mtDNAs of the remaining 18 species fall into either of two clades. One comprises predominantly Caribbean and Central and North American taxa (Clade I), and the other is of predominantly South American taxa (Clade II). The phylogeny is only very broadly concordant with some vocal characters and also with the limited morphological diversity for which the group is well known. Paraphyly in several species (M. swainsoni, M. tuberculifer, M. ferox, M. phaeocephalus, M. sagrae, M. stolidus) suggests that morphological evolution, albeit resulting in limited morphological diversity, has been more rapid than that of mtDNA, or that current taxonomy is faulty, or both. A South American origin for Myiarchus is likely. Dispersal and vicariance both appear to have been involved in generating the present-day distribution of some species. Relatively recent dispersal events out of South America are inferred to have brought species of Clades I and II into broad sympatry. Jamaica has been colonized independently at least twice by members of Clades I and II. The phylogeny brings a historical perspective that in turn suggests that ecological study of closely related species from within each major clade where they are sympatric will be especially rewarding. (C) 2003 Elsevier Inc. All rights reserved. C1 Acad Nat Sci Philadelphia, Dept Ornithol, Philadelphia, PA 19103 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Missouri, Dept Biol, St Louis, MO 63121 USA. RP Joseph, L (reprint author), Acad Nat Sci Philadelphia, Dept Ornithol, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA. EM joseph@acnatsci.org RI Joseph, Leo/F-9235-2010; Wilke, Thomas/G-1517-2012 OI Wilke, Thomas/0000-0001-8263-7758 NR 42 TC 26 Z9 26 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2004 VL 31 IS 1 BP 139 EP 152 DI 10.1016/S1055-7903(03)00259-8 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 807YM UT WOS:000220536800013 PM 15019615 ER PT J AU Arnedo, MA Coddington, J Agnarsson, I Gillespie, RG AF Arnedo, MA Coddington, J Agnarsson, I Gillespie, RG TI From a comb to a tree: phylogenetic relationships of the comb-footed spiders (Araneae, Theridiidae) inferred from nuclear and mitochondrial genes SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID HAPPY-FACE SPIDER; MULTIPLE SEQUENCE ALIGNMENT; OVATA CLERCK ARANEAE; AMINO-ACID SEQUENCE; COLOR POLYMORPHISM; SOCIAL SPIDER; MOLECULAR EVOLUTION; ANELOSIMUS-EXIMIUS; COOPERATIVE SPIDER; DATA SETS AB The family Theridiidae is one of the most diverse assemblages of spiders, from both a morphological and ecological point of view. The family includes some of the very few cases of sociality reported in spiders, in addition to bizarre foraging behaviors such as kleptoparasitism and araneophagy, and highly diverse web architecture. Theridiids are one of the seven largest families in the Araneae, with about 2200 species described. However, this species diversity is currently grouped in half the number of genera described for other spider families of similar species richness. Recent cladistic analyses of morphological, data have provided an undeniable advance in identifying the closest relatives of the theridiids as well as establishing the family's monophyly. Nevertheless, the comb-footed spiders remain an assemblage of poorly defined genera, among which hypothesized relationships have yet to be examined thoroughly. Providing a robust cladistic structure,for the Theridiidae is an essential step towards the clarification of the taxonomy of the group and the interpretation of the evolution of the diverse traits found in the family. Here we present results of a molecular phylogenetic analysis of a broad taxonomic sample of the family (40 taxa in 33 of the 79 currently recognized genera) and representatives of nine additional araneoid families, using approximately 2.5 kb corresponding to fragments of three nuclear genes (Histone 3, 18SrDNA, and 28SrDNA) and two mitochondrial genes (16SrDNA and Col). Several methods for incorporating indel information into the phylogenetic analysis are explored,;and partition support for the different clades and sensitivity of the results to different assumptions of the analysis are examined as well. Our results marginally support theridiid monophyly, although the phylogenetic structure of the outgroup is unstable and largely contradicts current phylogenetic hypotheses based on morphological data. Several groups of theridiids receive strong support in most of the analyses: latrodectines, argyrodines, hadrotarsines, a revised version of spintharines and two clades including all theridiids without trace of a colulus and those without colular setae. However, the interrelationships of these clades are sensitive to data perturbations and changes in the analysis assumptions. (C) 2003 Elsevier Inc. All rights reserved. C1 Univ Calif Berkeley, ESPM, Div Insect Biol, Berkeley, CA 94720 USA. Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Arnedo, MA (reprint author), Univ Barcelona, Dept Biol Anim, Av Diagonal 645, E-08028 Barcelona, Spain. EM marnedo@bio.ub.es; coddington.jon@nmnh.si.edu; ingi@gwu.edu; gillespi@nature.berkeley.edu NR 96 TC 96 Z9 102 U1 0 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2004 VL 31 IS 1 BP 225 EP 245 DI 10.1016/S1055-7903(03)00261-6 PG 21 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 807YM UT WOS:000220536800020 PM 15019622 ER PT J AU Kempner, JC David, LP AF Kempner, JC David, LP TI A Chandra view of the multiple merger in Abell 2744 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; shock waves; turbulence; galaxies : clusters : individual : Abell 2744; intergalactic medium; X-rays : galaxies : clusters ID GALAXY CLUSTERS; LUMINOSITY FUNCTION; RICH CLUSTERS; COMA CLUSTER; RADIO HALOS; COLD-FRONT; SKY SURVEY; EVOLUTION; PHOTOMETRY; EMISSION AB We present a Chandra observation of the merging cluster of galaxies Abell 2744. The cluster shows strong evidence for an ongoing major merger which we believe to be responsible for the radio halo. X-ray emission and temperature maps of the cluster, combined with the spatial and redshift distribution of the galaxies, indicate a roughly north-south axis for the merger, with a significant velocity component along the line of sight. The merger is occurring at a very large velocity, with M=2-3. We estimate the mass ratio of the merging subclusters to be of the order of unity. They are nearing their closest approach to each other, but with a significant impact parameter. In addition, there is a small merging subcluster toward the northwest, unrelated to the major merger, which shows evidence of a bow shock. A hydrodynamical analysis of the subcluster indicates a merger velocity corresponding to a Mach number of similar to1.2, consistent with a simple infall model. This infalling subcluster may also be re-exciting electrons in the radio halo. Its small Mach number lends support to turbulent reacceleration models for radio halo formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kempner, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jkempner@cfa.harvard.edu NR 37 TC 37 Z9 37 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 1 PY 2004 VL 349 IS 2 BP 385 EP 392 DI 10.1111/j.1365-2966.2004.07534.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 810HE UT WOS:000220694600003 ER PT J AU Jenkins, LP Roberts, TP Warwick, RS Kilgard, RE Ward, MJ AF Jenkins, LP Roberts, TP Warwick, RS Kilgard, RE Ward, MJ TI An XMM-Newton view of M101 - I. The luminous X-ray source population SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual : M101; galaxies : spiral; X-rays : binaries; X-rays : galaxies ID HYPERNOVA REMNANT CANDIDATES; NEARBY SPIRAL GALAXIES; CHANDRA OBSERVATIONS; BLACK-HOLE; SUPERNOVA-REMNANTS; EXTERNAL GALAXIES; NEUTRON-STAR; EMISSION; STARBURST; BINARIES AB We present the first results of an XMM-Newton EPIC observation of the luminous X-ray source population in the face-on supergiant spiral galaxy M101. We have studied the spectral and temporal properties of the 14 most luminous sources, all of which have intrinsic Xray luminosities exceeding the Eddington limit for a 1.4-M-circle dot neutron star, with a subset in the ultraluminous X-ray source (ULX) regime (L(x)greater than or equal to10(39) erg s(-1)). Eleven sources show evidence of short-term variability, and most vary by a factor of similar to2-4 over a baseline of 11-24 yr, providing strong evidence that these sources are accreting X-ray binary (XRB) systems. Our results demonstrate that these sources are a heterogeneous population, showing a variety of spectral shapes. Interestingly, there is no apparent spectral distinction between those sources above and below the ULX luminosity threshold. Nine sources are well fitted with either simple absorbed disc blackbody or power-law models. However, in three of the four sources best fitted with power-law models, we cannot exclude the disc blackbody fits and therefore conclude that, coupled with their high luminosities, eight out of nine single-component sources are possibly high-state XRBs. The nuclear source (XMM-10) has the only unambiguous power-law spectrum (Gammasimilar to2.3), which may be evidence for the presence of a low-luminosity active galactic nucleus (LLAGN). The remaining five sources require at least two-component spectral fits, with an underlying hard component that can be modelled by a power-law continuum or, in three cases, a hot disc blackbody (T-in=0.9-1.5 keV), plus a soft component modelled as a cool blackbody/disc blackbody/thermal plasma. We have compared the spectral shapes of nine sources covered by both this observation and an archival 100-ks Chandra observation of M101; eight show behaviour typical of Galactic XRBs (i.e. softening with increasing luminosity), the only exception being a transient source (XMM-2) which shows little change in spectral hardness despite a factor of similar to30 increase in luminosity. We find no definitive spectral signatures to indicate that these sources contain neutron star primaries, and conclude that they are likely to be stellar-mass black hole XRBs (BHXBs), with black hole masses of similar to2-23 M-circle dot if accreting at the Eddington limit. C1 Univ Leicester, Dept Phys & Astron, Xray & Obsevat Astron Grp, Leicester LE1 7RH, Leics, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jenkins, LP (reprint author), Univ Leicester, Dept Phys & Astron, Xray & Obsevat Astron Grp, Univ Rd, Leicester LE1 7RH, Leics, England. EM lej@star.le.ac.uk OI Jenkins, Leigh/0000-0001-9464-0719 NR 79 TC 26 Z9 26 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 1 PY 2004 VL 349 IS 2 BP 404 EP 424 DI 10.1111/j.1365-2966.2004.07546.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 810HE UT WOS:000220694600005 ER PT J AU O'Sullivan, E Ponman, TJ AF O'Sullivan, E Ponman, TJ TI XMM-Newton and Chandra observations of three X-ray-faint early-type galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : individual : NGC 3585; galaxies : individual : NGC 4494; galaxies : individual : NGC 5322; X-rays : galaxies ID TO-LIGHT RATIO; ELLIPTICAL GALAXIES; HOT GAS; INTERSTELLAR-MEDIUM; SPECTRAL PROPERTIES; GLOBULAR-CLUSTERS; FINE-STRUCTURE; EMISSION; EVOLUTION; CATALOG AB We present XMM-Newton observations of three X-ray-underluminous elliptical galaxies, NGC 3585, 4494 and 5322. All three galaxies have relatively large optical luminosities (log L-B=10.35-10.67 L-circle dot) but have X-ray luminosities consistent with emission from discrete sources only. In conjunction with a Chandra observation of NGC 3585, we analyse the XMM-Newton data and show that the three galaxies are dominated by discrete source emission, but do possess some X-ray-emitting gas. The gas is at relatively low temperatures, kTsimilar or equal to0.25-0.44 keV. All three galaxies show evidence of recent dynamical disturbance and formation through mergers, including kinematically distinct cores, young stellar ages and embedded stellar discs. This leads us to conclude that the galaxies formed relatively recently and have yet to build up large X-ray haloes. They are likely to be in a developmental phase where the X-ray gas has a very low density, making it undetectable outside the galaxy core. However, if the gas is a product of stellar mass loss, as seems most probable, we would expect to observe supersolar metal abundances. While abundance is not well constrained by the data, we find best-fitting abundances <0.1 Z(circle dot) for single-temperature models, and it seems unlikely that we could underestimate the metallicity by such a large factor. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ejos@head-cfa.harvard.edu OI O'Sullivan, Ewan/0000-0002-5671-6900 NR 63 TC 44 Z9 44 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 1 PY 2004 VL 349 IS 2 BP 535 EP 546 DI 10.1111/j.1365-2966.2004.07518.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 810HE UT WOS:000220694600014 ER PT J AU Parrent, JL Garbelotto, M Gilbert, GS AF Parrent, JL Garbelotto, M Gilbert, GS TI Population genetic structure of the polypore Datronia caperata in fragmented mangrove forests SO MYCOLOGICAL RESEARCH LA English DT Article ID SCHIZOPHYLLUM-COMMUNE; DIFFERENTIATION; DIVERSITY; FUNGUS; ROSEA; DNA AB Datronia caperata, a basidiomycete fungus, is one of the dominant polypore species found in neotropical mangrove forest fragments, where it is locally specialized on Laguncularia racemosa. We examined the genetic structure of D. caperata populations from four Panamanian mangrove forests using AFLP markers. Using five primer pair combinations, 145 loci were detected, 98.6 % of which were polymorphic. Each of the populations showed a high degree of genetic diversity (Nei's h ranging from 0.146 to 0.223). Results from minimum spanning trees and Mantel tests showed little evidence for small-scale spatial structure within sites. A significant amount of total genetic variation was partitioned among populations (Phi(ST) = 0.21) separated by 10s to 100s of km, a considerably greater amount than has been detected in other mushroom and wood-decaying fungi sampled at equal or greater geographic distances. These results suggest that despite production of copious basidiospores capable of long distance dispersal, some homobasidiomycete fungi may be susceptible to genetic isolation due to habitat fragmentation. C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Univ Calif Berkeley, ESPM Div Ecosyst Sci, Berkeley, CA 94720 USA. Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Parrent, JL (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA. EM jlp13@duke.edu NR 23 TC 20 Z9 21 U1 2 U2 13 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0953-7562 J9 MYCOL RES JI Mycol. Res. PD APR PY 2004 VL 108 BP 403 EP 410 DI 10.1017/S0953756204009773 PN 4 PG 8 WC Mycology SC Mycology GA 824XV UT WOS:000221721400005 PM 15209280 ER PT J AU Krennrich, F Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, D Celik, O Cui, W Daniel, M D'Vali, M Perez, IDC Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, J Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Jarvis, A Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Lang, MJ LeBohec, S Linton, E Lloyd-Evans, J Milovanovic, A Moriarty, P Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, G Swordy, SP Syson, A Vassiliev, VV Walker, G Wakely, SP Weekes, TC Zweerink, J AF Krennrich, F Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, D Celik, O Cui, W Daniel, M D'Vali, M Perez, IDC Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, J Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Horan, D Jarvis, A Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Lang, MJ LeBohec, S Linton, E Lloyd-Evans, J Milovanovic, A Moriarty, P Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, G Swordy, SP Syson, A Vassiliev, VV Walker, G Wakely, SP Weekes, TC Zweerink, J TI VERITAS: the Very Energetic Radiation Imaging Telescope Array System SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT 2nd VERITAS Symposium on TeV Astrophysics from Extragalactic Sources CY APR 24-26, 2003 CL Adler Planetarium & AStron Museum, Chicago, IL HO Adler Planetarium & AStron Museum DE gamma-ray astronomy; TeV energies; atmospheric Cherenkov detectors AB The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is the major next generation imaging atmospheric Cherenkov gamma-ray telescope in the western hemisphere and will be located in southern Arizona nearby Kitt Peak National Observatory. The VERITAS observatory will provide unprecedented sensitivity to photon energies between 50 GeV and 50 TeV. The first stage is an array of four telescopes to be fully operational in early 2006, with an expansion to seven telescopes envisioned for 2008. The construction of a prototype telescope is underway, for which first light is expected in Fall 2003. The technical concept is outlined and a progress report is given. (C) 2004 Published by Elsevier B.V. C1 Iowa State Univ Sci & Technol, Dept Phys & Astron, Ames, IA 50011 USA. Univ Leeds, Leeds LS2 9JT, W Yorkshire, England. Univ Chicago, Chicago, IL 60637 USA. Washington Univ, St Louis, MO 63130 USA. Univ Calif Los Angeles, Los Angeles, CA 90024 USA. Purdue Univ, W Lafayette, IN 47907 USA. Grinnell Coll, Grinnell, IA 50112 USA. Natl Univ Ireland Univ Coll Dublin, Dublin 4, Ireland. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Natl Univ Ireland Univ Coll Galway, Galway, Ireland. Univ Utah, Salt Lake City, UT 84112 USA. Univ Arkansas, Little Rock, AR 72204 USA. McGill Univ, Montreal, PQ H3A 2T5, Canada. Depauw Univ, Greencastle, IN 46135 USA. Galway Mayo Inst Technol, Galway, Ireland. Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. NASA, GSFC, Greenbelt, MD 20771 USA. Cork Inst Technol, Cork, AR, Ireland. RP Krennrich, F (reprint author), Iowa State Univ Sci & Technol, Dept Phys & Astron, Ames, IA 50011 USA. EM krennich@iastate.edu RI Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 7 TC 12 Z9 12 U1 1 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD APR PY 2004 VL 48 IS 5-6 BP 345 EP 349 DI 10.1016/j.newar.2003.12.050 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 815ZK UT WOS:000221080000005 ER PT J AU Horan, D AF Horan, D CA VERITAS Collaboration TI VHE observations of BL Lacertae objects: 1995-2000 SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT 2nd VERITAS Symposium on TeV Astrophysics from Extragalactic Sources CY APR 24-26, 2003 CL Adler Planetarium & AStron Museum, Chicago, IL HO Adler Planetarium & AStron Museum DE galaxies : BL Lacertae objects; gamma-ray : observations ID LAC; PHOTONS AB Over the past eight years, observations of BL Lacertae type objects have been an important part of the observing program at the Whipple Observatory 10 in gamma-ray telescope. During this time, TeV emission was detected from five Such objects: Markarian 421, Markarian 501, IES2344+514, H1426+428 and 1ES1959+650. Upper limits were placed on the TeV emission from 29 other BL Lacertae objects. Among these objects are two unconfirmed TeV sources, 3C66A and BL Lacertae. An overview of the results of these observations of BL Lacertae objects, between 1995 and 2000, at the Whipple Observatory is presented here. (C) 2003 Elsevier B.V. All rights reserved. C1 Smithsonian Astrophys Observ, Amado, AZ 85645 USA. RP Horan, D (reprint author), Smithsonian Astrophys Observ, POB 97, Amado, AZ 85645 USA. EM horan@egret.sao.arizona.edu NR 11 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD APR PY 2004 VL 48 IS 5-6 BP 391 EP 393 DI 10.1016/j.newar.2003.12.016 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 815ZK UT WOS:000221080000012 ER PT J AU Horan, D Weekes, TC AF Horan, D Weekes, TC TI Extragalactic sources of TeV gamma rays: a summary SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT 2nd VERITAS Symposium on TeV Astrophysics from Extragalactic Sources CY APR 24-26, 2003 CL Adler Planetarium & AStron Museum, Chicago, IL HO Adler Planetarium & AStron Museum DE gamma-ray astronomy; atmospheric Cherenkov radiation; AGN ID ACTIVE GALAXY MARKARIAN-421; BL-LAC OBJECTS; ENERGY-SPECTRUM; 1ES 2344+514; MKN 501; COS-B; EMISSION; VARIABILITY; TELESCOPES; H1426+428 AB The development of techniques whereby gamma rays of energy 100 GeV and above can be studied from the ground, using indirect, but sensitive, techniques has opened up a new area of high energy photon astronomy. The most exciting result that has come from these is the detection of highly variable fluxes of TeV gamma rays from the relativistic jets in nearby AGN. The recent detection of signals from a starburst galaxy and from a radio galaxy opens the possibility that the extragalactic emission of TeV gamma rays is a ubiquitous phenomenon. Here we attempt to summarize the properties of the sources detected so far. (C) 2004 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Whipple Observ, POB 97, Amado, AZ 85645 USA. EM weekes@egret.sao.arizona.edu NR 68 TC 36 Z9 36 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD APR PY 2004 VL 48 IS 5-6 BP 527 EP 535 DI 10.1016/j.newar.2003.12.057 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 815ZK UT WOS:000221080000039 ER PT J AU Pearcy, RW Valladares, F Wright, SJ de Paulis, EL AF Pearcy, RW Valladares, F Wright, SJ de Paulis, EL TI A functional analysis of the crown architecture of tropical forest Psychotria species: do species vary in light capture efficiency and consequently in carbon gain and growth? SO OECOLOGIA LA English DT Article DE crown architecture; self shading; daily photosynthesis; leaf longevity; forest gaps ID UNDERSTORY PLANTS; PETIOLE MECHANICS; BIFURCATION RATIO; LEAF INCLINATION; INTERCEPTION; MORPHOLOGY; CANOPY; SAPLINGS; PATTERN; ORIENTATION AB The crown architectures of 11 Psychotria species native to Barro Colorado Island, Panama were reconstructed from field measurements of leaf and branch geometry with the three-dimensional simulation model Y-plant. The objective was to assess the role of species differences in architecture in light capture and carbon gain in their natural understory environment. When species were grouped according to their putative light environment preference, the shade tolerant species were found to have a small but significantly higher efficiency of light capture for both diffuse and direct light as compared to the light demanding species. Within each grouping, however, there were few significant differences in light capture efficiency among species. The lower efficiencies of light demanding species was due to slightly higher self-shading and slightly lower angular efficiencies. Simulations of whole plant assimilation showed that light demanding species had greater daily assimilation in both direct and diffuse light due to the significantly greater light availability in the sites where light demanding species were found, as compared to those where shade tolerant species occurred. Among light demanding species, the above ground relative growth rate measured over a 1-year period by applying allometric equations for mass versus linear dimensions, was positively correlated with diffuse PFD and with mean daily assimilation estimated from Y-plant. For the shade tolerant plants, there was no significant correlation between RGR and mean daily assimilation or with any measure of light availability, probably because they occurred over a much narrower range of light environments. Overall, the results reveal a strong convergence in light capture efficiencies among the Psychotria species at lower values than previously observed in understory plants using similar approaches. Constraints imposed by other crown functions such as hydraulics and biomechanical support may place upper limits on light capture efficiency. C1 Univ Calif Davis, Div Biol Sci, Sect Evolut & Ecol, Davis, CA 95616 USA. Smithsonian Trop Res Inst, Balboa, Panama. CSIC, Ctr Ciencias Medioambientales, E-28006 Madrid, Spain. RP Pearcy, RW (reprint author), Univ Calif Davis, Div Biol Sci, Sect Evolut & Ecol, Davis, CA 95616 USA. EM rwpearcy@ucdavis.edu RI Wright, Stuart/M-3311-2013; Valladares, Fernando/K-9406-2014; OI Wright, Stuart/0000-0003-4260-5676; Valladares, Fernando/0000-0002-5374-4682; Lasso, Eloisa/0000-0003-4586-8674 NR 46 TC 55 Z9 56 U1 1 U2 21 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD APR PY 2004 VL 139 IS 2 BP 163 EP 177 DI 10.1007/s00442-004-1496-4 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 810SZ UT WOS:000220725300001 PM 14767753 ER PT J AU Greenwood, DR Wilf, P Wing, SL Christophel, DC AF Greenwood, DR Wilf, P Wing, SL Christophel, DC TI Paleotemperature estimation using leaf-margin analysis: Is Australia different? SO PALAIOS LA English DT Article ID ANGIOSPERM LEAVES; CLIMATE; FOREST; TERTIARY; SENSITIVITY; VEGETATION; EOCENE; FLORA; PALEOCLIMATE; TEMPERATURE AB Australia has numerous fossil floras suitable for paleoclimatic analysis, with potential to improve understanding of Southern Hemisphere climatic evolution. Leaf-margin analysis (LMA) is a widely used method that applies present-day correlations between the proportion of woody dicot species with untoothed leaves and mean annual temperature to estimate paleotemperatures from fossil megafloras. Australia's unique history and vegetation imply that its leaf-margin correlation might differ from other regions; these possible differences are investigated here to improve paleoclimatic interpretations. Australian rainforest vegetation shows nearly the same regression slope as recorded in East Asia and the Americas indicating a globally convergent evolutionary response of leaf form to temperature. However, Australian sites tend to have fewer toothed species at localities with the same temperature as Asian and American sites. The following factors, singly or in combination, may account for this difference: (1) Australia Cenozoic movement into lower latitudes, insulation from global cooling, and isolation from high-latitude cold-tolerant vegetation sources; (2) lack of high mountains as sources and refuges for cold-adapted taxa; (3) Pleistocene extinctions of cold-adapted taxa; and (4) the near absence of a cold-climate forest ecospace in Australia today. Application of Australian LMA to Australian Cenozoic floras resulted in cooler temperature estimates than other LMA regressions. However, Australian paleotemperature estimates should account for the relative importance of cold-deciduous taxa. The timing and magnitudes of the extinctions of cold-adapted lineages are not known, and the moat conservative approach is to use Australian LMA as a minimum and non-Australian LMA as a maximum temperature estimate. C1 Victoria Univ, Sustainabil Grp, Melbourne, Vic 8001, Australia. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. RP Greenwood, DR (reprint author), Victoria Univ, Sustainabil Grp, St Albans Campus,POB 14428, Melbourne, Vic 8001, Australia. EM David.Greenwood@uu.edu.au RI Greenwood, David/C-2758-2008; OI Greenwood, David/0000-0002-8569-9695; Wing, Scott/0000-0002-2954-8905 NR 68 TC 65 Z9 70 U1 2 U2 12 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD APR PY 2004 VL 19 IS 2 BP 129 EP 142 DI 10.1669/0883-1351(2004)019<0129:PEULAI>2.0.CO;2 PG 14 WC Geology; Paleontology SC Geology; Paleontology GA 807WD UT WOS:000220530700003 ER PT J AU Childress, L Sorensen, AS Lukin, MD AF Childress, L Sorensen, AS Lukin, MD TI Mesoscopic cavity quantum electrodynamics with quantum dots SO PHYSICAL REVIEW A LA English DT Article ID PHOTON NUMBER STATES; PHASE GATE; ATOMS; ENTANGLEMENT; OPERATION; MOLECULES; SPINS AB We describe an electrodynamic mechanism for coherent, quantum-mechanical coupling between spatially separated quantum dots on a microchip. The technique is based on capacitive interactions between the electron charge and a superconducting transmission line resonator, and is closely related to atomic cavity quantum electrodynamics. We investigate several potential applications of this technique which have varying degrees of complexity. In particular, we demonstrate that this mechanism allows design and investigation of an on-chip double-dot microscopic maser. Moreover, the interaction may be extended to couple spatially separated electron-spin states while only virtually populating fast-decaying superpositions of charge states. This represents an effective, controllable long-range interaction, which may facilitate implementation of quantum information processing with electron-spin qubits and potentially allow coupling to other quantum systems such as atomic or superconducting qubits. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Childress, L (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Childress, Lilian/H-1359-2012; Sorensen, Anders/L-1868-2013 OI Childress, Lilian/0000-0002-0507-6392; Sorensen, Anders/0000-0003-1337-9163 NR 36 TC 91 Z9 94 U1 1 U2 7 PU AMERICAN 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 APR PY 2004 VL 69 IS 4 AR 042302 DI 10.1103/PhysRevA.69.042302 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 818WY UT WOS:000221276400027 ER PT J AU Huan, C Yang, XY Candela, D Mair, RW Walsworth, RL AF Huan, C Yang, XY Candela, D Mair, RW Walsworth, RL TI NMR experiments on a three-dimensional vibrofluidized granular medium SO PHYSICAL REVIEW E LA English DT Article ID VELOCITY FLUCTUATIONS; EXTERNAL VIBRATIONS; MESOSCOPIC SYSTEMS; SCALING BEHAVIOR; FLOWS; GAS; SPHERES; ENERGY; BEADS; FLUIDIZATION AB A three-dimensional granular system fluidized by vertical container vibrations was studied using pulsed field gradient NMR coupled with one-dimensional magnetic resonance imaging. The system consisted of mustard seeds vibrated vertically at 50 Hz, and the number of layers Nlless than or equal to4 was sufficiently low to achieve a nearly time-independent granular fluid. Using NMR, the vertical profiles of density and granular temperature were directly measured, along with the distributions of vertical and horizontal grain velocities. The velocity distributions showed modest deviations from Maxwell-Boltzmann statistics, except for the vertical velocity distribution near the sample bottom, which was highly skewed and non-Gaussian. Data taken for three values of Nl and two dimensionless accelerations Gamma=15,18 were fitted to a hydrodynamic theory, which successfully models the density and temperature profiles away from the vibrating container bottom. A temperature inversion near the free upper surface is observed, in agreement with predictions based on the hydrodynamic parameter mu which is nonzero only in inelastic systems. C1 Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Huan, C (reprint author), Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. RI Huan, Chao/F-4735-2014 OI Huan, Chao/0000-0002-0696-4412 NR 56 TC 66 Z9 66 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 J9 PHYS REV E JI Phys. Rev. E PD APR PY 2004 VL 69 IS 4 AR 041302 DI 10.1103/PhysRevE.69.041302 PN 1 PG 13 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA 818NP UT WOS:000221252100013 PM 15169012 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, WN Zatwarnicki, T TI A revision of the shore-fly genus Cressonomyia arnaud (Diptera : ephydridae), with comments on species that have been excluded SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE review; diptera; ephydridae; shore flies; Cressonomyia AB Five species of the shore-fly genus Cressonomyia Arnaud are revised, including C. bolivia, n. sp. (Bolivia. La Paz: Tajlihui). The genus is known only from the New World tropics and subtropics and is the sister group to Peltopsilopa Cresson. Two species groups are recognized, the aciculata group (two species) and the skinneri group (three species). Psilopa aeneonigra (Loew), which had been included in Cressonomyia, is returned to Psilopa. A neotype is designated for Psilopa aciculata Loew, the senior synonym for Plagiops nitidifrons Cresson (new synonym). All species are illustrated and distribution maps are also provided. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. Polish Acad Sci, Museum Zool, PL-00679 Warsaw, Poland. Polish Acad Sci, Inst Zool, PL-00679 Warsaw, Poland. Univ Opole, Dept Biosystemat, PL-45052 Opole, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA. EM mathis.wayne@nmnh.si.edu; zatwar@uni.opole.pl OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 36 TC 4 Z9 5 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2004 VL 106 IS 2 BP 249 EP 279 PG 31 WC Entomology SC Entomology GA 810AE UT WOS:000220676400001 ER PT J AU Gagne, RJ Sosa, A Cordo, H AF Gagne, RJ Sosa, A Cordo, H TI A new neotropical species of Clinodiplosis (Diptera : cecidomyiidae) injurious to alligatorweed, Alternanthera philoxeroides (amaranthaceae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE gall midges; neotropical; biocontrol of alligatorweed AB A new species of cecidomyiid, Clinodiplosis alternantherae Gagne, is reported from alligatorweed, Alternanthera philoxeroides (Mart.) Griseb. (Amaranthaceae) in Argentina. The gall midge forms galls on branch tips and is a likely candidate to aid in the control of the invasive, alien alligatorweed in North America and Australia. The male, female, pupa and larva are described, illustrated, and compared to other Clinodiplosis species. C1 USDA ARS, Systemat Entomol Lab, PSI,Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. USDA ARS, S Amer Biol Control Lab, Hurlingham, Buenos Aires, Argentina. RP Gagne, RJ (reprint author), USDA ARS, Systemat Entomol Lab, PSI,Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM rgagne@sel.barc.usda.gov; alejsosa@mail.retina.ar; hacordo@arnet.com.ar NR 4 TC 0 Z9 2 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2004 VL 106 IS 2 BP 305 EP 311 PG 7 WC Entomology SC Entomology GA 810AE UT WOS:000220676400005 ER PT J AU Konstantinov, AS Korotyaev, BA AF Konstantinov, AS Korotyaev, BA TI Sexual dimorphism and size of aedeagi in apionid weevils (Coleoptera : apionidae) and flea beetles (Coleoptera : chrysomelidae): Why some masculine males have small aedeagi SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE apionidae; chrysomelidae; sexual dimorphism; male genitalia; copulatory courtship ID GENITALIA; SPIDERS; INSECTS; COPULATION; SELECTION AB A correlation between strongly developed sexually dimorphic external structures and the size and mechanical properties of male genitalia are described and illustrated in Trichoconapion Korotyaev (Coleoptera: Apionidae) and Normaltica Konstantinov (Coleoptera: Chrysomelidae). Sexually dimorphic structures include legs and antennae in Trichoconapion and head and mouth parts in Normaltica. These sexually dimorphic characters in our examples are likely to function as clasping (restraining) or copulatory courtship devices rather than male/male combat or precopulatory courtship devices. C1 USDA ARS, PSI, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. RP Konstantinov, AS (reprint author), USDA ARS, PSI, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM akonstan@sel.barc.usda.gov NR 26 TC 2 Z9 2 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2004 VL 106 IS 2 BP 324 EP 338 PG 15 WC Entomology SC Entomology GA 810AE UT WOS:000220676400008 ER PT J AU Costa, LAA Henry, TJ AF Costa, LAA Henry, TJ TI Fulvius chaguenus Carvalho and Costa (Heteroptera : Miridae : Cylapinae : Fulviini): Redescription and recognition of type specimens SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; Hemiptera; Heteroptera; Miridae; Cylapinae; Fulvius chaguenus description; type data; Paraguay AB Fulvius chaguenus Carvalho and Costa is redescribed and its type specimens are recognized. In 1994, Carvalho and Costa revised the New World species of Fulvius Stal and included figures of the adult holotype and male genitalia of F. chaguenus and included it in their identification key from Paraguay, but inadvertently omitted the text description and type data for this species. Provided for F. chaguenus in this paper are a formal adult description, type data for the holotype and associated paratypes, figures of the adult and male genitalia, and diagnostic information to help separate it from other New World species of Fulvius. C1 Fed Univ Rio De Janeiro, Museum Nacl, Dept Entomol, BR-20942040 Rio De Janeiro, Brazil. USDA ARS, PSI, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20250 USA. RP Costa, LAA (reprint author), Fed Univ Rio De Janeiro, Museum Nacl, Dept Entomol, BR-20942040 Rio De Janeiro, Brazil. EM tlcosta@uol.com.br; thenry@sel.barc.usda.gov NR 5 TC 1 Z9 2 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2004 VL 106 IS 2 BP 417 EP 420 PG 4 WC Entomology SC Entomology GA 810AE UT WOS:000220676400016 ER PT J AU Vandenberg, NJ AF Vandenberg, NJ TI Homonymy in the Coccinelidae (Coleoptera), or something fishy about Pseudoscymnus Chapin SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material ID COCCINELLIDAE C1 Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, Systemat Entomol Lab,PSI, Washington, DC 20013 USA. RP Vandenberg, NJ (reprint author), Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, Systemat Entomol Lab,PSI, POB 37012,MRC-168, Washington, DC 20013 USA. EM nvandenb@sel.barc.usda.gov NR 16 TC 1 Z9 3 U1 1 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 2004 VL 106 IS 2 BP 483 EP 484 PG 2 WC Entomology SC Entomology GA 810AE UT WOS:000220676400027 ER PT J AU Pedretti, E Millan-Gabet, R Monnier, JD Traub, WA Carleton, NP Berger, JP Lacasse, MG Schloerb, FP Brewer, MK AF Pedretti, E Millan-Gabet, R Monnier, JD Traub, WA Carleton, NP Berger, JP Lacasse, MG Schloerb, FP Brewer, MK TI The PICNIC interferometry camera at IOTA SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID BEAM INFRARED CAMERA; INTEGRATED-OPTICS; TELESCOPE; ENVELOPE; STARS AB We describe the control and performance of a new near-infrared camera based on a Rockwell PICNIC array detector for interferometry observations at the Infrared-Optical Telescope Array (IOTA). The camera control uses a complex programmable logic device that allows fast and stable clocking of the PICNIC array and on-the-fly reconfiguration of the readout method. We measured a read noise as low as 12.4 e per correlated double sample. The read noise can be reduced even more through nondestructive readout, and decreases as the square root of the number of successive reads. We discuss the advantages of this system for near-infrared interferometry. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts, Amherst, MA 01003 USA. RP Pedretti, E (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA. EM epedretti@cfa.harvard.edu; rafael@huey.jpl.hasa.gov; monnier@umich.edu; wtraub@cfa.harvard.edu; ncarleton@cfa.harvard.edu; Jean-Philippe.Berger@obs.ujf-grenoble.fr; mlacasse@cfa.harvard.edu; schloerb@astro.umass.edu; brewer@astro.umass.edu OI Monnier, John D/0000-0002-3380-3307 NR 28 TC 24 Z9 24 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD APR PY 2004 VL 116 IS 818 BP 377 EP 389 DI 10.1086/383528 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 810WZ UT WOS:000220735700009 ER PT J AU Garcia, RA Corbard, T Chaplin, WJ Couvidat, S Eff-Darwich, A Jimenez-Reyes, SJ Korzennik, SG Ballot, J Boumier, P Fossat, E Henney, CJ Howe, R Lazrek, M Lochard, J Palle, PL Turck-Chieze, S AF Garcia, RA Corbard, T Chaplin, WJ Couvidat, S Eff-Darwich, A Jimenez-Reyes, SJ Korzennik, SG Ballot, J Boumier, P Fossat, E Henney, CJ Howe, R Lazrek, M Lochard, J Palle, PL Turck-Chieze, S TI About the rotation of the solar radiative interior SO SOLAR PHYSICS LA English DT Article; Proceedings Paper CT 25th General Assembly of the International-Astronomical-Union CY JUL, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID P-MODE SPLITTINGS; TEMPORAL VARIATIONS; INTERNAL-ROTATION; INVERSION METHODS; GOLF; HELIOSEISMOLOGY; OSCILLATIONS; FREQUENCIES; SPECTRA; BISON AB In the modern era of helioseismology we have a wealth of high-quality data available, e.g., more than 6 years of data collected by the various instruments on board the SOHO mission, and an even more extensive ground-based set of observations covering a full solar cycle. Thanks to this effort a detailed picture of the internal rotation of the Sun has been constructed. In this paper we present some of the actions that should be done to improve our knowledge of the inner rotation profile discussed during the workshop organized at Saclay on June 2003 on this topic. In particular we will concentrate on the extraction of the rotational frequency splittings of low- and medium-degree modes and their influence on the rotation of deeper layers. Furthermore, for the first time a full set of individual |m|-component rotational splittings is computed for modes l less than or equal to 4 and 1 < ν < 2 mHz, opening new studies on the latitudinal dependence of the rotation rate in the radiative interior. It will also be shown that these splittings have the footprints of the differential rotation of the convective zone which can be extremely useful to study the differential rotation of other stars where only these low- degree modes will be available. C1 Ctr Etud Saclay, CEA, DSM,DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. Observ Cote Azur, CNRS, UMR 6529, Dept Cassini, F-06304 Nice 4, France. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Stanford Univ, HEPL, Stanford, CA 94305 USA. THEMIS SL, Tenerife 38205, Spain. Inst Astrofis Canarias, Tenerife 38205, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. Univ Nice, Dept Astrophys, UMR 6525, F-06108 Nice 2, France. Natl Solar Observ, Tucson, AZ 85726 USA. Univ Cady Ayyad Marrakech, LPHEA, Marrakech, Morocco. Observ Paris, LESIA, F-92195 Meudon, France. RP Garcia, RA (reprint author), Ctr Etud Saclay, CEA, DSM,DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. EM rgarcia@cea.fr RI Ballot, Jerome/G-1019-2010; Palle, Pere/H-4720-2015; OI Jimenez Reyes, Sebastian/0000-0002-0317-4247; Garcia, Rafael/0000-0002-8854-3776 NR 29 TC 45 Z9 45 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD APR PY 2004 VL 220 IS 2 BP 269 EP 285 DI 10.1023/B:SOLA.0000031395.90891.ce PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 827XM UT WOS:000221937000011 ER PT J AU Hardy, CR Faden, RB AF Hardy, CR Faden, RB TI Plowmanianthus, a new genus of commelinaceae with five new species from tropical America SO SYSTEMATIC BOTANY LA English DT Article ID PHYLOGENETIC-RELATIONSHIPS; CLADISTIC-ANALYSIS AB A new Neotropical genus of Commelinaceae, Plowmanianthus, is described with five new species. Karyological and morphological data, as well as results of phylogenetic studies, support its inclusion in the subtribe Dichorisandrinae (tribe Tradescantieae) with four other genera (Cochliostema, Dichorisandra, Geogenanthus, and Siderasis). The occurrence of moniliform hairs along the distal margins of the petals is evidence of an even closer relationship with Cochliostema and Geogenanthus, this character being restricted in the family to these three genera. Plowmanianthus may be uniquely characterized as comprising small, perennial rosette herbs with usually one-cymed, axillary inflorescences borne among the lower leaves, an androecium reduced to three fertile stamens, annular, papillate stigmas, and uniseriate to partially biseriate seeds. Plants of the genus are shallowly rooted, the roots not penetrating deeper than the leaf-litter or humus-rich layers of their primary rainforest habitats. Plowmanianthus is also distinctive among the Commelinaceae in the unusually high frequency of cleistogamy in the genus, with some species for which only cleistogamous flowers are known. As currently understood, two species (P. panamensis and P. dressleri) are restricted to the Isthmus of Panama, whereas the remaining four taxa (P. grandifolius subsp. grandifolius, P. grandifolius subsp. robustus, P. perforans, and P. peruvianus) are restricted to lowland Amazonia. C1 Cornell Univ, LH Bailey Hortorium, Ithaca, NY 14853 USA. New York Bot Garden, Bronx, NY 10458 USA. Museum Natl Hist Nat, US Natl Herbarium, Smithsonian Inst, MRC 166, Washington, DC 20013 USA. RP Hardy, CR (reprint author), Univ Zurich, Inst Syst Bot, Zollikerstr 107, CH-8008 Zurich, Switzerland. EM chardy@systbot.unizh.ch NR 16 TC 14 Z9 15 U1 2 U2 3 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD APR-JUN PY 2004 VL 29 IS 2 BP 316 EP 333 DI 10.1600/036364404774195511 PG 18 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 824CK UT WOS:000221661400008 ER PT J AU Xia, YM Kress, WJ Prince, LM AF Xia, YM Kress, WJ Prince, LM TI Phylogenetic analyses of amomum (Alpinioideae : zingiberaceae) using ITS and matK DNA sequence data SO SYSTEMATIC BOTANY LA English DT Article AB Comparative sequencing of the nuclear ribosomal Internal Transcribed Spacer (ITS) and the chloroplast matK coding and non-coding regions was used to examine the evolutionary relationships among 53 accessions representing 13 genera of the Zingiberaceae, including 31 accessions of Amomum (Alpinioideae). Phylogenetic analyses of the ITS and matK sequences alone and in combination using maximum parsimony methods produced a moderately supported topology within Alpinioideae. Our results indicated that Amomum as currently defined is polyphyletic with three major groups of species that do not correspond with any previously recognized sectional classification of the genus. Our analyses also identified Paramomum as sister to Elettariopsis, which are both embedded within one group of Amomum. The other two groups of Amomum share common ancestors with additional genera of the Alpinioideae. ITS and matK sequences provide new data for inferring relationships within Amomum and allow fresh interpretations of morphological characters (such as anther appendage and fruit type) that may be of value in future classifications. C1 Natl Museum Nat Hist, US Natl Herbarium, Smithsonian Inst, MRC 166, Washington, DC 20013 USA. Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Mengla 666303, Yunnan, Peoples R China. RP Kress, WJ (reprint author), Natl Museum Nat Hist, US Natl Herbarium, Smithsonian Inst, MRC 166, POB 37012, Washington, DC 20013 USA. EM kress.john@nmnh.si.edu NR 38 TC 16 Z9 26 U1 0 U2 2 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD APR-JUN PY 2004 VL 29 IS 2 BP 334 EP 344 DI 10.1600/036364404774195520 PG 11 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 824CK UT WOS:000221661400009 ER PT J AU Harasewych, MG Kantor, YI AF Harasewych, MG Kantor, YI TI The deep-sea Buccinoidea (Gastropoda : Neogastropoda) of the Scotia Sea and adjacent abyssal plains and trenches SO NAUTILUS LA English DT Article ID GENUS AB Four new genera and species of buccinoidean gastropods, Spikebuccinum stephaniae new genus, new species; Drepanodontus tatyanae new genus, new species; Muffinbuccinum catherinae new genus, new species; and Germonea cacherinae new genus, new species, are described from the Scotia tectonic plate and adjacent abyssal plains. Only Bathydomus obtectus Thiele, 1912, Tromina bella abyssicola Clarke, 1961. and T. abyssorum Lus, 1993, had previously been reported from abyssal depths off Antarctica. The latter two species were proposed in the genus Tromina, subsequently shown to belong to the family Muricidae. Therefore, a new genus, Lusitromina is proposed for these abyssal and hadal buccinoidean species. Analyses of the taxonomic placement, geographical and bathymetric distribution, and diversity of the 29 buccinoidean genera presently known from Antarctica and the Magellanic Province have shown that the abyssal (>2200 m) buccinoidean fauna of the region shares no genera with the sublittoral or bathyal faunas. None of the six abyssal genera conform readily to the subfamilies represented by the sublittoral or bathyal faunas. Credible sister taxa and likely origins for some abyssal genera occur on the adjacent continental slope. For others, closest relatives may be found on abyssal plains beyond the Antarctic Convergence. Generic diversity decreases with increasing depth for both the bathyal and abyssal buccinoidean faunas, while bathymetric range tends to increase. For abyssal buccinoideans, maximum generic diversity occurs between 2600 and 3200 meters. The proportion of monotypic genera in the Antarctic and Magellanic Provinces is extraordinarily high (48.3%), and may be an artefact of low sampling density exacerbated by difficulties in differentiating closely related species. Neither gigantism nor dwarfism is evident in the abyssal buccinoidean fauna. Rather, the range in sizes narrows with increasing depth. Genera inhabiting the base of the continental slope are smaller than those of either the tipper slope or continental rise. In the abyssal zone, maximum shell size is reached near the boundary of the continental rise and abyssal plain, and subsequently decreases with increasing depth. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. Russian Acad Sci, Severtzov Inst, Moscow 117071, Russia. RP Harasewych, MG (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. RI Kantor, Yuri/D-5259-2014 OI Kantor, Yuri/0000-0002-3209-4940 NR 61 TC 21 Z9 24 U1 0 U2 3 PU BAILEY-MATTHEWS SHELL MUSEUM PI SANIBEL PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD, SANIBEL, FL 33957 USA SN 0028-1344 J9 NAUTILUS JI Nautilus PD MAR 31 PY 2004 VL 118 IS 1 BP 1 EP 42 PG 42 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 838LW UT WOS:000222715800001 ER PT J AU Laurance, WF AF Laurance, WF TI Forest-climate interactions in fragmented tropical landscapes SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Tropical-Biology-and -Conservation CY JUL, 2002 CL Panama City, PANAMA DE atmospheric circulation; carbon dynamics; edge effects; fire; forest hydrology; microclimate ID CENTRAL AMAZONIAN FOREST; BIOSPHERE-ATMOSPHERE EXPERIMENT; GREENHOUSE-GAS EMISSIONS; RAIN-FOREST; BRAZILIAN AMAZON; EASTERN AMAZON; EL-NINO; POSITIVE FEEDBACKS; TREE COMMUNITIES; REGIONAL CLIMATE AB In the tropics, habitat fragmentation alters forest-climate interactions in diverse ways. On a local scale (less than I km), elevated desiccation and wind disturbance near fragment margins lead to sharply increased tree mortality, thus altering canopy-gap dynamics, plant community composition, biomass dynamics and carbon storage. Fragmented forests are also highly vulnerable to edge-related fires, especially in regions with periodic droughts or strong dry seasons. At landscape to regional scales (10-1000 km), habitat fragmentation may have complex effects on forest-climate interactions, with important consequences for atmospheric circulation, water cycling and precipitation. Positive feedbacks among deforestation, regional climate change and fire could pose a serious threat for some tropical forests, but the details of such interactions are poorly understood. C1 Smithsonian Trop Res Inst, Balboa, Panama. INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012 NR 103 TC 106 Z9 116 U1 6 U2 59 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD MAR 29 PY 2004 VL 359 IS 1443 BP 345 EP 352 DI 10.1098/rstb.2003.1430 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 808BR UT WOS:000220545100004 PM 15212089 ER PT J AU Baker, TR Phillips, OL Malhi, Y Almeida, S Arroyo, L Di Fiore, A Erwin, T Higuchi, N Killeen, TJ Laurance, SG Laurance, WF Lewis, SL Monteagudo, A Neill, DA Vargas, PN Pitman, NCA Silva, JNM Martinez, RV AF Baker, TR Phillips, OL Malhi, Y Almeida, S Arroyo, L Di Fiore, A Erwin, T Higuchi, N Killeen, TJ Laurance, SG Laurance, WF Lewis, SL Monteagudo, A Neill, DA Vargas, PN Pitman, NCA Silva, JNM Martinez, RV TI Increasing biomass in Amazonian forest plots SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Tropical-Biology-and -Conservation CY JUL, 2002 CL Panama City, PANAMA DE Amazonia; biomass; carbon; permanent plot; tropical forests ID TROPICAL RAIN-FOREST; BRAZILIAN AMAZON; SEVERE DROUGHT; EL-NINO; TREE; DYNAMICS; IMPACT; MORTALITY AB A previous study by Phillips et al. of changes in the biomass of permanent sample plots in Amazonian forests was used to infer the presence of a regional carbon sink. However, these results generated a vigorous debate about sampling and methodological issues. Therefore we present a new analysis of biomass change in old-growth Amazonian forest plots using updated inventory data. We find that across 59 sites, the above-ground dry biomass in trees that are more than 10 cm in diameter (AGB) has increased since plot establishment by 1.22 +/- 0.43 Mg per hectare per year (ha(-1) yr(-1), where 1 ha = 10(4) m(2)), or 0.98 +/- 0.38 Mg ha(-1) yr(-1) if individual plot values are weighted by the number of hectare years of monitoring. This significant increase is neither confounded by spatial or temporal variation in wood specific gravity, nor dependent on the allometric equation used to estimate AGB. The conclusion is also robust to uncertainty about diameter measurements for problematic trees: for 34 plots in western Amazon forests a significant increase in AGB is found even with a conservative assumption of zero growth for all trees where diameter measurements were made using optical methods and/or growth rates needed to be estimated following fieldwork. Overall, our results suggest a slightly greater rate of net stand-level change than was reported by Phillips et al. Considering the spatial and temporal scale of sampling and associated studies showing increases in forest growth and stem turnover, the results presented here suggest that the total biomass of these plots has on average increased and that there has been a regional-scale carbon sink in old-growth Amazonian forests during the previous two decades. C1 Max Planck Inst Biogeochem, D-07701 Jena, Germany. Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JU, Midlothian, Scotland. Museu Paraense Emilio Goeldi, BR-66077530 Belem, Para, Brazil. Museo Noel Kempff Mercado, Santa Cruz, Bolivia. NYU, Dept Anthropol, New York, NY 10003 USA. Smithsonian Inst, Washington, DC 20560 USA. INPA, BR-69011970 Manaus, Amazonas, Brazil. Ctr Appl Biodivers Sci, Conservat Int, Washington, DC 20036 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Nacl San Antonio Abad Del Cusco, Cuzco, Peru. Proyecto Flora Peru, Jardin Bot Missouri, Oxapampa, Peru. Missouri Bot Garden, Herbario Nacl Ecuador, Quito, Ecuador. Duke Univ, Ctr Trop Conservat, Durham, NC 27708 USA. CIFOR, Tapajos, Brazil. EMBRAPA, Amazonia Oriental, BR-66095100 Belem, Para, Brazil. RP Baker, TR (reprint author), Max Planck Inst Biogeochem, Postfach 10 01 64, D-07701 Jena, Germany. EM t.baker@geog.leeds.ac.uk RI Pitman, Nigel/A-7681-2008; Laurance, William/B-2709-2012; Phillips, Oliver/A-1523-2011; Laurance, Susan/G-6021-2011; OI Pitman, Nigel/0000-0002-9211-2880; Phillips, Oliver/0000-0002-8993-6168; Laurance, Susan/0000-0002-2831-2933; Lewis, Simon/0000-0002-8066-6851 NR 42 TC 257 Z9 272 U1 5 U2 56 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD MAR 29 PY 2004 VL 359 IS 1443 BP 353 EP 365 DI 10.1098/rstb.2003.1422 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 808BR UT WOS:000220545100005 PM 15212090 ER PT J AU Phillips, OL Baker, TR Arroyo, L Higuchi, N Killeen, TJ Laurance, WF Lewis, SL Lloyd, J Malhi, Y Monteagudo, A Neill, DA Vargas, PN Silva, JNM Terborgh, J Martinez, RV Alexiades, M Almeida, S Brown, S Chave, J Comiskey, JA Czimczik, CI Di Fiore, A Erwin, T Kuebler, C Laurance, SG Nascimento, HEM Olivier, J Palacios, W Patino, S Pitman, NCA Quesada, CA Salidas, M Lezama, AT Vinceti, B AF Phillips, OL Baker, TR Arroyo, L Higuchi, N Killeen, TJ Laurance, WF Lewis, SL Lloyd, J Malhi, Y Monteagudo, A Neill, DA Vargas, PN Silva, JNM Terborgh, J Martinez, RV Alexiades, M Almeida, S Brown, S Chave, J Comiskey, JA Czimczik, CI Di Fiore, A Erwin, T Kuebler, C Laurance, SG Nascimento, HEM Olivier, J Palacios, W Patino, S Pitman, NCA Quesada, CA Salidas, M Lezama, AT Vinceti, B TI Pattern and process in Amazon tree turnover, 1976-2001 SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Tropical-Biology-and -Conservation CY JUL, 2002 CL Panama City, PANAMA DE recruitment; mortality; tree turnover; dynamics; Amazonia; forest ID ATMOSPHERIC CO2 CONCENTRATIONS; TROPICAL RAIN-FORESTS; CARBON-DIOXIDE; ELEVATED CO2; EVALUATING TURNOVER; SPECIES RICHNESS; DYNAMICS; DIVERSITY; GROWTH; DISTURBANCE AB Previous work has shown that tree turnover, tree biomass and large liana densities have increased in mature tropical forest plots in the late twentieth century. These results point to a concerted shift in forest ecological processes that may already be having significant impacts on terrestrial carbon stocks, fluxes and biodiversity. However, the findings have proved controversial, partly because a rather limited number of permanent plots have been monitored for rather short periods. The aim of this paper is to characterize regional-scale patterns of 'tree turnover' (the rate with which trees die and recruit into a population) by using improved datasets now available for Amazonia that span the past 25 years. Specifically, we assess whether concerted changes in turnover are occurring, and if so whether they are general throughout the Amazon or restricted to one region or environmental zone. In addition, we ask whether they are driven by changes in recruitment, mortality or both. We find that: (i) trees 10 cm or more in diameter recruit and die twice as fast on the richer soils of southern and western Amazonia than on the poorer soils of eastern and central Amazonia; (ii) turnover rates have increased throughout Amazonia over the past two decades; (iii) mortality and recruitment rates have both increased significantly in every region and environmental zone, with the exception of mortality in eastern Amazonia; (iv) recruitment rates have consistently exceeded mortality rates; (v) absolute increases in recruitment and mortality rates are greatest in western Amazonian sites; and (vi) mortality appears to be lagging recruitment at regional scales. These spatial patterns and temporal trends are not caused by obvious artefacts in the data or the analyses. The trends cannot be directly driven by a mortality driver (such as increased drought or fragmentation-related death) because the biomass in these forests has simultaneously increased. Our findings therefore indicate that long-acting and widespread environmental changes are stimulating the growth and productivity of Amazon forests. C1 Univ Leeds, Earth & Biosphere Inst, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. Max Planck Inst Biogeochem, D-07701 Jena, Germany. Museo Noel Kempff Mercado, Santa Cruz, Bolivia. Missouri Bot Garden, St Louis, MO 63166 USA. Inst Natl Pesquisas Amazon, BR-69083000 Manaus, Amazonas, Brazil. Ctr Appl Biodivers Sci, Conservat Int, Washington, DC 20036 USA. Smithsonian Trop Res Inst, Balboa, Panama. Smithsonian Inst, INPA, Biol Dynam Forest Fragments Program, BR-69022970 Manaus, Amazonas, Brazil. Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland. Univ Nacl San Antonio Abad Del Cusco, Herbario Vargas, Cuzco, Peru. Proyecto Flora Peru, Jardin Bot Missouri, Oxapampa, Peru. CIFOR, Para, Brazil. EMBRAPA, Amazonia Oriental, Belem, Para, Brazil. Duke Univ, Sch Environm, Ctr Trop Conservat, Durham, NC 27705 USA. New York Bot Garden, Bronx, NY 10458 USA. Museu Paraense Emilio Goeldi, BR-66040 Belem, Para, Brazil. Winrock Int Livestock Res & Training Ctr, Arlington, VA 22209 USA. Univ Toulouse 3, CNRS, Lab Evolut & Divers Biol, UPS, F-31062 Toulouse 4, France. Smithsonian Inst, Washington, DC 20013 USA. NYU, Dept Anthropol, New York, NY 10003 USA. Fundac Jatun Sacha, Quito 002, Ecuador. Alexander Humboldt Biol Res Inst, Bogota, Colombia. Univ Brasilia, Dept Ecol, BR-70919970 Brasilia, DF, Brazil. Univ Los Andes, INDEFOR, Merida 5101, Venezuela. Int Plant Genet Resources Inst, I-00057 Rome, Italy. RP Phillips, OL (reprint author), Univ Leeds, Earth & Biosphere Inst, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. EM o.phillips@geog.leeds.ac.uk RI Pitman, Nigel/A-7681-2008; Lloyd, Jonathan/F-8893-2010; Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012; Phillips, Oliver/A-1523-2011; Laurance, Susan/G-6021-2011; OI Pitman, Nigel/0000-0002-9211-2880; Lloyd, Jonathan/0000-0002-5458-9960; Phillips, Oliver/0000-0002-8993-6168; Laurance, Susan/0000-0002-2831-2933; Lewis, Simon/0000-0002-8066-6851 NR 75 TC 250 Z9 257 U1 7 U2 74 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD MAR 29 PY 2004 VL 359 IS 1443 BP 381 EP 407 DI 10.1098/rstb.2003.1438 PG 27 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 808BR UT WOS:000220545100007 PM 15212092 ER PT J AU Chave, J Condit, R Aguilar, S Hernandez, A Lao, S Perez, R AF Chave, J Condit, R Aguilar, S Hernandez, A Lao, S Perez, R TI Error propagation and scaling for tropical forest biomass estimates SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Tropical-Biology-and -Conservation CY JUL, 2002 CL Panama City, PANAMA DE above-ground biomass; allometric equation; error propagation; sampling; tropical forest ID NET PRIMARY PRODUCTION; RAIN-FOREST; LANDSCAPE-SCALE; ABOVEGROUND BIOMASS; AMAZONIAN FORESTS; SECONDARY FORESTS; CENSUS PLOT; CARBON; DYNAMICS; BRAZIL AB The above-ground biomass (AGB) of tropical forests is a crucial variable for ecologists, biogeochemists, foresters and policymakers. Tree inventories are an efficient way of assessing forest carbon stocks and emissions to the atmosphere during deforestation. To make correct inferences about long-term changes in biomass stocks, it is essential to know the uncertainty associated with AGB estimates, yet this uncertainty is rarely evaluated carefully. Here, we quantify four types of uncertainty that could lead to statistical error in AGB estimates: (i) error due to tree measurement; (ii) error due to the choice of an allometric model relating AGB to other tree dimensions; (iii) sampling uncertainty, related to the size of the study plot(iv) representativeness of a network of small plots across a vast forest landscape. In previous studies, these sources of error were reported but rarely integrated into a consistent framework. We estimate all four terms in a 50 hectare (ha, where 1 ha = 10(4) m(2)) plot on Barro Colorado Island, Panama, and in a network of 1 ha plots scattered across central Panama. We find that the most important source of error is currently related to the choice of the allometric model. More work should be devoted to improving the predictive power of allometric models for biomass. C1 CNRS, UPS, UMR 5174, Lab Evolut & Divers Biol, F-31062 Toulouse, France. Smithsonian Trop Res Inst, Ctr Trop Forest Serv, Unit 0948, Miami, FL 34002 USA. RP Chave, J (reprint author), CNRS, UPS, UMR 5174, Lab Evolut & Divers Biol, Bat 4R3,118 Route Narbonne, F-31062 Toulouse, France. EM chave@cict.fr NR 57 TC 315 Z9 328 U1 10 U2 79 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD MAR 29 PY 2004 VL 359 IS 1443 BP 409 EP 420 DI 10.1098/rstb.2003.1425 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 808BR UT WOS:000220545100008 PM 15212093 ER PT J AU Lewis, SL Phillips, OL Baker, TR Lloyd, J Malhi, Y Almeida, S Higuchi, N Laurance, WF Neill, DA Silva, JNM Terborgh, J Lezama, AT Martinez, RV Brown, S Chave, J Kuebler, C Vargas, PN Vinceti, B AF Lewis, SL Phillips, OL Baker, TR Lloyd, J Malhi, Y Almeida, S Higuchi, N Laurance, WF Neill, DA Silva, JNM Terborgh, J Lezama, AT Martinez, RV Brown, S Chave, J Kuebler, C Vargas, PN Vinceti, B TI Concerted changes in tropical forest structure and dynamics: evidence from 50 South American long-term plots SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Tropical-Biology-and -Conservation CY JUL, 2002 CL Panama City, PANAMA DE carbon; permanent sample plot; turnover; mortality; recruitment; biomass ID NET PRIMARY PRODUCTION; ELEVATED CO2; CARBON BALANCE; EVALUATING TURNOVER; AMAZONIAN FORESTS; DECIDUOUS FOREST; ATMOSPHERIC CO2; TREE; RESPONSES; PLANTS AB Several widespread changes in the ecology of old-growth tropical forests have recently been documented for the late twentieth century, in particular an increase in stem turnover (pan-tropical), and an increase in above-ground biomass (neotropical). Whether these changes are synchronous and whether changes in growth are also occurring is not known. We analysed stand-level changes within 50 long-term. monitoring plots from across South America spanning 1971-2002. We show that: (i) basal area (BA: sum of the cross-sectional areas of all trees in a plot) increased significantly over time (by 0.10 +/- 0.04 m(2) ha(-1) yr(-1), mean +/- 95% CI); as did both (ii) stand-level BA growth rates (sum of the increments of BA of surviving trees and BA of new trees that recruited into a plot); and (iii) stand-level BA mortality rates (sum of the cross-sectional areas of all trees that died in a plot). Similar patterns were observed on a per-stem basis: (i) stem density (number of stems per hectare; 1 hectare is 10(4) m(2)) increased significantly over time (0.94 +/- 0.63 stems ha(-1) yr(-1)); as did both (ii) stem recruitment rates; and (iii) stem mortality rates. In relative terms, the pools of BA and stem density increased by 0.38 +/- 0.15% and 0.18 +/- 0.12% yr(-1), respectively. The fluxes into and out of these pools-stand-level BA growth, stand-level BA mortality, stem recruitment and stem mortality rates-increased, in relative terms, by an order of magnitude more. The gain terms (BA growth, stem recruitment) consistently exceeded the loss terms (BA loss, stem mortality) throughout the period, suggesting that whatever process is driving these changes was already acting before the plot network was established. Large long-term increases in stand-level BA growth and simultaneous increases in stand BA and stem density imply a continent-wide increase in resource availability which is increasing net primary productivity and altering forest dynamics. Continent-wide changes in incoming solar radiation, and increases in atmospheric concentrations of CO2 and air temperatures may have increased resource supply over recent decades, thus causing accelerated growth and increased dynamism across the world's largest tract of tropical forest. C1 Univ Leeds, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JU, Midlothian, Scotland. Max Planck Inst Biogeochem, D-07701 Jena, Germany. Museu Paraense Emilio Goeldi, BR-66077530 Belem, Para, Brazil. Inst Nacl Pesquisas Amazon, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. INPA Ecol, Biol Dynam Forest Fragments Program, BR-69011970 Manaus, Amazonas, Brazil. Missouri Bot Garden, Herbario Nacl Ecuador, Quito, Ecuador. CIFOR, Tapajos, Brazil. EMBRAPA, Amazonia Oriental, BR-66095100 Belem, Para, Brazil. Duke Univ, Ctr Trop Conservat, Durham, NC 27708 USA. Univ Los Andes, INDEFOR, Merida 5101, Venezuela. Jardin Bot Missouri, Proyecto Flora Peru, Oxapampa, Peru. Winrock Int Livestock Res & Training Ctr, Arlington, VA 22209 USA. UPS, CNRS, Lab Evolut & Divers Biol, F-31062 Toulouse, France. Conservat Int, Ctr Appl Biodivers Sci, Washington, DC 20036 USA. Univ Nacl San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. RP Lewis, SL (reprint author), Univ Leeds, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. EM slewis@pobox.com RI Lloyd, Jonathan/F-8893-2010; Laurance, William/B-2709-2012; Phillips, Oliver/A-1523-2011; OI Lloyd, Jonathan/0000-0002-5458-9960; Phillips, Oliver/0000-0002-8993-6168; Lewis, Simon/0000-0002-8066-6851 NR 56 TC 165 Z9 175 U1 1 U2 42 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD MAR 29 PY 2004 VL 359 IS 1443 BP 421 EP 436 DI 10.1098/rstb.2003.1431 PG 16 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 808BR UT WOS:000220545100009 PM 15212094 ER PT J AU Heaney, PJ Post, JE Lopano, C Komarneni, S Hanson, JC AF Heaney, PJ Post, JE Lopano, C Komarneni, S Hanson, JC TI Time-resolved X-ray diffraction analysis of cation exchange in Mn oxides. SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 227th National Meeting of the American-Chemical Society CY MAR 28-APR 01, 2004 CL Anaheim, CA SP Amer Chem Soc C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Crop & Soil Sci, University Pk, PA 16802 USA. Brookhaven Natl Lab, Dept Chem, Upton, NY 11973 USA. EM heaney@geosc.psu.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 28 PY 2004 VL 227 MA 155-GEOC BP U1216 EP U1217 PN 1 PG 2 WC Chemistry, Multidisciplinary SC Chemistry GA 851AJ UT WOS:000223655604018 ER PT J AU Kukolich, SG Tanjaroon, C McCarthy, MC Thaddeus, P AF Kukolich, SG Tanjaroon, C McCarthy, MC Thaddeus, P TI Microwave measurements of the molecular structure of o-benzyne SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 227th ACS National Meeting CY MAR 28-APR 01, 2004 CL Anaheim, CA SP Amer Chem Soc C1 Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA USA. EM kukolich@u.arizona.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 28 PY 2004 VL 227 MA 384-PHYS BP U317 EP U317 PN 2 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 851AK UT WOS:000223655701626 ER PT J AU Post, JE Heaney, PJ Lopano, C AF Post, JE Heaney, PJ Lopano, C TI Manganese oxide minerals: Structures and behaviors. SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 227th National Meeting of the American-Chemical Society CY MAR 28-APR 01, 2004 CL Anaheim, CA SP Amer Chem Soc C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM post.jeffrey@nmnh.si.edu NR 0 TC 0 Z9 0 U1 1 U2 3 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 28 PY 2004 VL 227 MA 154-GEOC BP U1216 EP U1216 PN 1 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 851AJ UT WOS:000223655604017 ER PT J AU Jonsell, S Saenz, A Froelich, P Zygelman, B Dalgarno, A AF Jonsell, S Saenz, A Froelich, P Zygelman, B Dalgarno, A TI Hydrogen-antihydrogen scattering in the Born-Oppenheimer approximation SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID SUB-KELVIN TEMPERATURES; CROSS-SECTIONS; LOW ENERGIES; SYSTEM; ANNIHILATION; COLLISIONS; ANTIPROTON AB We calculate the low-energy scattering between hydrogen and antihydrogen atoms in their ground states using the Born-Oppenheimer approximation. Improved results for rearrangement, direct annihilation and elastic scattering are presented. The elastic cross section agrees well with other calculations. For the rearrangement process we confirm a recent result (Armour E A G and Chamberlain C W 2002 J. Phys. B.- At. Mol. Opt. Phys. 35 L489) that rearrangement to the N = 23 state of protonium has a larger cross section than rearrangement to the N = 24 state. For both rearrangement cross sections our results are smaller than those obtained by Armour and Chamberlain. The direct annihilation, and its influence on elastic scattering, is calculated using the scattering length for the strong force between the proton and antiproton. This approach gives strong-force effects qualitatively similar, but smaller than those obtained in another recent work. C1 Umea Univ, Dept Phys, S-90187 Umea, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Uppsala Univ, Dept Quantum Chem, SE-75120 Uppsala, Sweden. Humboldt Univ, Inst Phys, AG Moderne Opt, D-10117 Berlin, Germany. RP Jonsell, S (reprint author), Umea Univ, Dept Phys, S-90187 Umea, Sweden. EM jonsell@tp.umu.se RI Jonsell, Svante/J-2251-2016 OI Jonsell, Svante/0000-0003-4969-1714 NR 20 TC 34 Z9 34 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAR 28 PY 2004 VL 37 IS 6 BP 1195 EP 1202 AR PII S0953-4075(04)70377-6 DI 10.1088/0953-4075/37/6/005 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 813AA UT WOS:000220878800008 ER PT J AU Khosrawi, F Muller, R Irie, H Engel, A Toon, GC Sen, B Aoki, S Nakazawa, T Traub, WA Jucks, KW Johnson, DG Oelhaf, H Wetzel, G Sugita, T Kanzawa, H Yokota, T Nakajima, H Sasano, Y AF Khosrawi, F Muller, R Irie, H Engel, A Toon, GC Sen, B Aoki, S Nakazawa, T Traub, WA Jucks, KW Johnson, DG Oelhaf, H Wetzel, G Sugita, T Kanzawa, H Yokota, T Nakajima, H Sasano, Y TI Validation of CFC-12 measurements from the Improved Limb Atmospheric Spectrometer (ILAS) with the version 6.0 retrieval algorithm SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE CFC-12; ILAS; validation ID PROFILE OBSERVATIONS; ARCTIC VORTEX; TRACE GASES; OZONE; STRATOSPHERE; CHLORINE; DISTRIBUTIONS; CONSTITUENTS; RATIOS; N2O AB [1] Measurements of CFC-12 were made by the Improved Limb Atmospheric Spectrometer (ILAS) between 57degreesN and 72degreesN in the Northern Hemisphere and between 64degreesS and 89degreesS in the Southern Hemisphere. ILAS was launched on 17 August 1996 on board the Advanced Earth Observing Satellite (ADEOS). The ILAS validation balloon campaigns were carried out from Kiruna, Sweden (68degreesN, 21degreesE), in February and March 1997 and from Fairbanks, Alaska (65degreesN, 148degreesW), in April and May 1997. During these validation balloon campaigns, CFC-12 was measured with the in situ instruments ASTRID, BONBON, and SAKURA and the remote sensing spectrometers MIPAS-B, FIRS-2, and MkIV. ILAS version 6.0 CFC-12 profiles obtained at the nearest location to the validation balloon measurement are compared with these validation balloon measurements. The quality of ILAS CFC-12 data processed with the version 6.0 algorithm improved significantly compared to previous versions. Low relative differences between ILAS CFC-12 and the correlative measurements of about 10% were found between 13 and 20 km. The comparison of vertical profiles shows that ILAS CFC-12 data are useful below about 20-22 km inside the vortex and below about 25 km outside the vortex. However, at greater altitudes the relative percentage difference increases very strongly with increasing altitude. Further, correlations of CFC-12 with N2O show a good agreement with the correlative measurements for N2O values of N2O > 150 ppbv. In summary, ILAS CFC-12 data are now suitable for scientific studies in the lower stratosphere. C1 Natl Inst Environm Studies, Ozone Layer Res Project, Tsukuba, Ibaraki 3050053, Japan. Forschungszentrum Julich, ICG I, D-52425 Julich, Germany. Univ Frankfurt, Inst Meteorol, D-60325 Frankfurt, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Tohoku Univ, Ctr Atmospher & Ocean Studies, Grad Sch Sci, Sendai, Miyagi 9808578, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany. RP Khosrawi, F (reprint author), Natl Inst Environm Studies, Ozone Layer Res Project, Tsukuba, Ibaraki 3050053, Japan. EM f.khosrawi@fz-juelich.de; ro.mueller@fz-juelich.de; irie.hitoshi@nies.go.jp; an.engel@meteor.uni-frankfurt.de; toon@mark4sun.jpl.nasa.gov; sen@mark4sun.jpl.nasa.gov; aoki@mail.cc.tohoku.ac.jp; nakazawa@mail.tains.tohoku.ac.jp; traub@cfa.harvard.edu; kjucks@cfa.harvard.edu; d.g.johnson@larc.nasa.gov; hermann.oelhaf@imk.fzk.de; gerald.wetzel@imk.fzk.de; tsugita@nies.go.jp; kanzawa@ihas.nagoya-u.ac.jp; yoko@nies.go.jp; hide@nies.go.jp; sasano@nies.go.jp RI Sasano, Yasuhiro/C-2927-2009; Muller, Rolf/A-6669-2013; Wetzel, Gerald/A-7065-2013; Oelhaf, Hermann/A-7895-2013; Engel, Andreas/E-3100-2014 OI Sasano, Yasuhiro/0000-0001-7470-5642; Muller, Rolf/0000-0002-5024-9977; Engel, Andreas/0000-0003-0557-3935 NR 23 TC 12 Z9 12 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 26 PY 2004 VL 109 IS D6 AR D06311 DI 10.1029/2003JD004325 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 809FN UT WOS:000220622700006 ER EF