FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Kohno, K Ishizuki, S Matsushita, S Vila-Vilaro, B Kawabe, R AF Kohno, K Ishizuki, S Matsushita, S Vila-Vilaro, B Kawabe, R TI Enhanced HCN (1-0) emission in the type-1 Seyfert galaxy NGC 1097 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies : active; galaxies : individual (NGC 1097); galaxies : ISM; galaxies : Seyfert; galaxies : starburst ID DENSE MOLECULAR GAS; ACTIVE GALACTIC NUCLEUS; BARRED SPIRAL GALAXIES; STAR-FORMING RINGS; X-RAY-EMISSION; NGC 1097; LOW-LUMINOSITY; NEARBY GALAXIES; CO SURVEY; STARBURST AB The central kpc region of the low-luminosity type-1 Seyfert galaxy NGC 1097 has been observed in the CO (1-0) and HCN (1-0) lines with the Nobeyama Millimeter Array and the NRO 45 m telescope. We have found a striking enhancement of the HCN emission toward the active nucleus of NGC 1097; a large fraction of the CO emission comes from a circumnuclear starburst ring (r similar to 10" or 700 pc at D = 14.5 Mpc), whereas the HCN emission is dominated by a strong unresolved peak at the nucleus. The HCN-to-CO integrated intensity ratio on the brightness temperature scale, R-HCN/CO, is about 0.11 in the aperture of the 45 m telescope beams (15" for CO and 19" for HCN), but reaches 0.34 in the smaller aperture (10" x 4."4). These CO and HCN properties in NGC 1097 are similar to those in the type-2 Seyfert galaxies NGC 1068 and NGC 5194 (M 5 1). C1 Univ Tokyo, Astron Inst, Mitaka, Tokyo 1810015, Japan. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Univ Tokyo, Astron Inst, Mitaka, Tokyo 1810015, Japan. EM kkohno@ioa.s.u-tokyo.ac.jp NR 50 TC 46 Z9 46 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB 25 PY 2003 VL 55 IS 1 BP L1 EP L5 DI 10.1093/pasj/55.1.L1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 653MZ UT WOS:000181441500001 ER PT J AU McCarthy, MC Fuchs, GW Kucera, J Winnewisser, G Thaddeus, P AF McCarthy, MC Fuchs, GW Kucera, J Winnewisser, G Thaddeus, P TI Rotational spectra of C4N, C6N, and the isotopic species of C3N SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID TRANSFORM MICROWAVE SPECTROSCOPY; COUPLED-CLUSTER CALCULATIONS; GAS-PHASE; HYPERFINE-STRUCTURE; ELECTRONIC-SPECTRA; CARBON CHAINS; FREE-RADICALS; MOLECULES; PARAMETERS; STATES AB Two new carbon chain radicals terminated with a nitrile group, C4N and C6N, have been detected in a supersonic molecular beam by Fourier transform microwave spectroscopy. In addition, at least three hyperfine-split rotational transitions of the singly-substituted isotopic species of C3N have also been observed. Both C4N and C6N are linear chains with (2)Pi electronic ground states, and both radicals have resolvable hyperfine structure and lambda-type doubling in their lowest rotational levels. At least four transitions in the lowest-energy fine structure component ((2)Pi(1/2)) were measured between 7 and 22 GHz for both molecules, and at most nine spectroscopic constants were required to reproduce the measured spectra to a few parts in 10(7). Precise sets of rotational, centrifugal distortion, spin-rotation, and hyperfine coupling constants were also determined for the isotopic species of C3N by combining the centimeter-wave measurements here with previous millimeter-wave data. The C-13 hyperfine coupling constants of isotopic C3N differ from those of the isoelectronic chain C4H, but are fairly close to those of isovalent C2H, indicating a nearly pure (2)Sigma electronic ground state for C3N. Although the strongest lines of C6N are more than five times less intense than those of C5N, owing to large differences in the ground state dipole moments, both new chains are more abundant than C5N. Searches for C7N have so far been unsuccessful. The absence of lines at the predicted frequencies implies that the product of the dipole moment times the abundance (mu.N-a) is more than 60 times smaller for C7N than for C5N, suggesting that the ground state of C7N may be (2)Pi, for which the dipole moment is calculated to be small. (C) 2003 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Fuchs, Guido/I-3507-2013; OI Fuchs, Guido/0000-0002-6935-059X; McCarthy, Michael/0000-0001-9142-0008 NR 34 TC 24 Z9 24 U1 3 U2 10 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 FEB 22 PY 2003 VL 118 IS 8 BP 3549 EP 3557 DI 10.1063/1.1534104 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 642KP UT WOS:000180803800014 ER PT J AU Thollesson, M Norenburg, JL AF Thollesson, M Norenburg, JL TI Ribbon worm relationships: a phylogeny of the phylum Nemertea SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE phylogenetic analysis; DNA sequence data; spiralians; phylogenetic taxonomy; Bayesian analysis ID MULTIPLE SEQUENCE ALIGNMENT; RIBOSOMAL-RNA GENE; 18S RDNA SEQUENCES; MOLECULAR PHYLOGENY; MORPHOLOGY; DNA; POSITION; SYSTEMATICS; HYPOTHESIS; TAXONOMY AB We present the most extensive phylogenetic analysis to date, to our knowledge, of higher-level nemertean relationships, based on sequence data from four different genes (the nuclear genes for nuclear large subunit rRNA (28S rRNA) and histone H3 (H3), and the mitochondrial genes for mitochondrial large subunit rRNA (16S rRNA) and cytochrome c oxidase subunit I (COI)). Well-supported clades are, in general, compatible with earlier, more limited, analyses, and current classification is largely in agreement with our results, although there are some notable exceptions. Bdellonemertea (represented by Malacobdella) is found to be a part of Monostilifera, and Polystilifera is the monophyletic sister group to Monostilifera. Cratenemertidae is the sister group to the remaining monostiliferans (including Malacobdella), a group to which we apply the new name Distromatonemertea. Heteronemertea is monophyletic and forms a clade with Hubrechtella; for this clade we introduce the name Pilidiophora. Finally, Pilidiophora and Hoplonemertea (with Malacobdella) form a monophyletic group, and we introduce the name Neonemertea to refer to this group. Palaeonemertea is found to be non-monophyletic and basal among nemerteans. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Thollesson, M (reprint author), Uppsala Univ, Dept Mol Evolut, Evolutionary Biol Ctr, Norbyvagen 18C, SE-75236 Uppsala, Sweden. EM mikael.thollesson@ebc.uu.se; norenbur@lab.si.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 62 TC 120 Z9 130 U1 2 U2 6 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 FEB 22 PY 2003 VL 270 IS 1513 BP 407 EP 415 DI 10.1098/rspb.2002.2254 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 651LC UT WOS:000181320500011 PM 12639321 ER PT J AU Sioris, CE Courreges-Lacoste, GB Stoll, MP AF Sioris, CE Courreges-Lacoste, GB Stoll, MP TI Filling in of Fraunhofer lines by plant fluorescence: Simulations for a nadir-viewing satellite-borne instrument SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE inelastic; radiative transfer ID ROTATIONAL RAMAN-SCATTERING; BLUE-GREEN FLUORESCENCE; SOLAR SPECTRUM; FERULIC ACID; ATMOSPHERE; OPACITY; IMPACT AB Solar-excited plant fluorescence in the red/near-infrared is known to fill Fraunhofer lines at ground level. In this paper, it is shown that red/near-infrared fluorescence by vegetation can fill Fraunhofer lines much more effectively than rotational Raman scattering (RRS) by air (Ring effect) for nadir viewing from satellite altitudes. Thus, similarly to RRS, plant fluorescence can be remotely sensed from an orbiting spectrometer, and may impact the retrieval of atmospheric trace gases such as water vapor by high-resolution spectroscopy over vegetated land. C1 York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 2R7, Canada. TNO TPD, Space Instrumentat Div, Delft, Netherlands. Univ Strasbourg, Lab Sci Image Informat & Teledetect, Strasbourg, France. RP Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM csioris@nimbus.yorku.ca; bazalgette@tpd.tno.nl; mpstoll@sepia.u-strasbg.fr NR 36 TC 10 Z9 10 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 21 PY 2003 VL 108 IS D4 AR 4133 DI 10.1029/2001JD001321 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 663AX UT WOS:000181983800001 ER PT J AU Springel, V Hernquist, L AF Springel, V Hernquist, L TI Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE methods : numerical; galaxies : evolution; galaxies : formation ID X-RAY-CLUSTERS; DISSIPATIVE GALAXY FORMATION; ANGULAR-MOMENTUM PROBLEM; DARK-MATTER COSMOLOGIES; HIGH-REDSHIFT GALAXIES; TULLY-FISHER RELATION; LYMAN-BREAK GALAXIES; INTERGALACTIC MEDIUM; SUPERNOVA FEEDBACK; METAL ENRICHMENT AB We present a model for star formation and supernova feedback that describes the multiphase structure of star-forming gas on scales that are typically not resolved in cosmological simulations. Our approach includes radiative heating and cooling, the growth of cold clouds embedded in an ambient hot medium, star formation in these clouds, feedback from supernovae in the form of thermal heating and cloud evaporation, galactic winds and outflows, and metal enrichment. Implemented using smoothed particle hydrodynamics, our scheme is a significantly modified and extended version of the grid-based method of Yepes et al., and enables us to achieve a high dynamic range in simulations of structure formation. We discuss properties of the feedback model in detail and show that it predicts a self-regulated, quiescent mode of star formation, which, in particular, stabilizes the star-forming gaseous layers of disc galaxies. The parametrization of this mode can be reduced to a single free quantity that determines the overall time-scale for star formation. We fix this parameter numerically to match the observed rates of star formation in local disc galaxies. When normalized in this manner, cosmological simulations employing our model nevertheless overproduce the observed cosmic abundance of stellar material. We are thus motivated to extend our feedback model to include galactic winds associated with star formation. Using small-scale simulations of individual star-forming disc galaxies, we show that these winds produce either galactic fountains or outflows, depending on the depth of the gravitational potential. In low-mass haloes, winds can greatly suppress the overall efficiency of star formation. When incorporated into cosmological simulations, our combined model for star formation and winds predicts a cosmic star formation density that is consistent with observations, provided that the winds are sufficiently energetic. Moreover, outflows from galaxies in these simulations drive chemical enrichment of the intergalactic medium - in principle, accounting for the presence of metals in the Lyman alpha forest. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Springel, V (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM volker@mpa-garching.mpg.de; lars@cfa.harvard.edu NR 119 TC 1025 Z9 1027 U1 5 U2 24 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 FEB 21 PY 2003 VL 339 IS 2 BP 289 EP 311 DI 10.1046/j.1365-8711.2003.06206.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 645HT UT WOS:000180970700003 ER PT J AU Springel, V Hernquist, L AF Springel, V Hernquist, L TI The history of star formation in a Lambda cold dark matter universe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE methods : numerical; galaxies : evolution; galaxies : starburst ID ULTRAVIOLET LUMINOSITY DENSITY; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; HUBBLE DEEP FIELD; RADIATIVE-TRANSFER; COSMOLOGICAL SIMULATIONS; ELLIPSOIDAL COLLAPSE; INTERSTELLAR-MEDIUM; CLUMPY UNIVERSE AB Employing hydrodynamic simulations of structure formation in a Lambda cold dark matter cosmology, we study the history of cosmic star formation from the 'dark ages' at redshift z similar to 20 to the present. In addition to gravity and ordinary hydrodynamics, our model includes radiative heating and cooling of gas, star formation, supernova feedback and galactic winds. By making use of a comprehensive set of simulations on interlocking scales and epochs, we demonstrate numerical convergence of our results on all relevant halo mass scales, ranging from 10(8) to 10(15) h(-1) M-.. The predicted density of cosmic star formation, , is broadly consistent with measurements, given the observational uncertainty. From the present epoch, gradually rises by approximately a factor of 10 to a peak at z similar to 5-6, which is beyond the redshift range where it has been estimated observationally. In our model, fully 50 per cent of the stars are predicted to have formed by redshift z similar or equal to 2.14, and are thus older than 10.4 Gyr, while only 25 per cent form at redshifts lower than z similar or equal to 1. The mean age of all stars at the present is approximately 9 Gyr. Our model predicts a total stellar density at z = 0 of Omega(star) = 0.004, corresponding to approximately 10 per cent of all baryons being locked up in long-lived stars, in agreement with recent determinations of the luminosity density of the Universe. We determine the 'multiplicity function of cosmic star formation' as a function of redshift; i.e. the distribution of star formation with respect to halo mass. At redshifts around z similar or equal to 10, star formation occurs preferentially in haloes of mass >10(8) -10(10) h(-1) M-., while at lower redshifts, the dominant contribution to comes from progressively more massive haloes. Integrating over time, we find that approximately 50 per cent of all stars formed in haloes less massive than 10(11.5) h(-1) M-., with nearly equal contributions per logarithmic mass interval in the range 10(10) -10(13.5) h(-1) M-., making up similar to70 per cent of the total. We also briefly examine possible implications of our predicted star formation history for reionization of hydrogen in the Universe. According to our model, the stellar contribution to the ionizing background is expected to rise for redshifts z > 3, at least up to redshift z similar to 5, in accord with estimates from simultaneous measurements of the H and He opacities of the Lyman-alpha forest. This suggests that the ultraviolet background will be dominated by stars for z > 4, provided that there are not significantly more quasars at high z than are presently known. We measure the clumping factor of the gas from the simulations and estimate the growth of cosmic H ii regions, assuming a range of escape fractions for ionizing photons. We find that the star formation rate predicted by the simulations is sufficient to account for hydrogen reionization by z similar to 6, but only if a high escape fraction close to unity is assumed. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Springel, V (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM volker@mpa-garching.mpg.de; lars@cfa.harvard.edu NR 110 TC 378 Z9 378 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 FEB 21 PY 2003 VL 339 IS 2 BP 312 EP 334 DI 10.1046/j.1365-8711.2003.06207.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 645HT UT WOS:000180970700004 ER PT J AU Groot, PJ Vreeswijk, PM Huber, ME Everett, ME Howell, SB Nelemans, G van Paradijs, J van den Heuvel, EPJ Augusteijn, T Kuulkers, E Rutten, RGM Storm, J AF Groot, PJ Vreeswijk, PM Huber, ME Everett, ME Howell, SB Nelemans, G van Paradijs, J van den Heuvel, EPJ Augusteijn, T Kuulkers, E Rutten, RGM Storm, J TI The Faint Sky Variability Survey - I. Goals and data reduction process SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; techniques : photometric; surveys; stars : variables : other; Galaxy : stellar content ID GAMMA-RAY BURST; LARGE-MAGELLANIC-CLOUD; CATACLYSMIC VARIABLES; REDSHIFT SURVEY; IMAGING SURVEY; DEEP; GALAXY; STARS; FIELD; CONSTRAINTS AB The Faint Sky Variability Survey is aimed at finding photometric and/or astrometric variable objects in the brightness range between similar to16th and similar to24th mag on time-scales between tens of minutes and years with photometric precisions ranging from 3 millimag for the brightest to 0.2 mag for the faintest objects. An area of similar to23 deg(2), located at mid and high Galactic latitudes, has been covered using the Wide Field Camera on the 2.5-m Isaac Newton Telescope on La Palma. Here we describe the main goals of the Faint Sky Variability Survey and the data reduction process. C1 Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, CHEAF, NL-1098 SJ Amsterdam, Netherlands. Planetary Sci Inst, Astrophys Grp, Tucson, AZ USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. Isaac Newton Grp Telescaopes, Santa Cruz de La Palma 38700, Canary Islands, Spain. Nord Opt Telescope, Santa Cruz de La Palma 38700, Canary Islands, Spain. ESA ESTEC, Sci Operat & Data Syst Div, SCI SDG, NL-2201 AZ Noordwijk, Netherlands. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. RP Groot, PJ (reprint author), Univ Nijmegen, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. RI Nelemans, Gijs/D-3177-2012; Groot, Paul/K-4391-2016 OI Nelemans, Gijs/0000-0002-0752-2974; Groot, Paul/0000-0002-4488-726X NR 38 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 FEB 21 PY 2003 VL 339 IS 2 BP 427 EP 434 DI 10.1046/j.1365-8711.2003.06182.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 645HT UT WOS:000180970700012 ER PT J AU Blumenschine, RJ Peters, CR Masao, FT Clarke, RJ Deino, AL Hay, RL Swisher, CC Stanistreet, IG Ashley, GM McHenry, LJ Sikes, NE van der Merwe, NJ Tactikos, JC Cushing, AE Deocampo, DM Njau, JK Ebert, JI AF Blumenschine, RJ Peters, CR Masao, FT Clarke, RJ Deino, AL Hay, RL Swisher, CC Stanistreet, IG Ashley, GM McHenry, LJ Sikes, NE van der Merwe, NJ Tactikos, JC Cushing, AE Deocampo, DM Njau, JK Ebert, JI TI Late pliocene Homo and hominid land use from western Olduvai Gorge, Tanzania SO SCIENCE LA English DT Article ID PLEISTOCENE HOMINIDS; ZINJANTHROPUS; BASIN AB Excavation in the previously little-explored western portion of Olduvai Gorge indicates that hominid land use of the eastern pateobasin extended at least episodically to the west. Finds included a dentally complete Homo maxilla (OH 65) with lower face, Oldowan stone artifacts, and butchery-marked bones dated to be between 1.84 and 1.79 million years old. The hominid shows strong affinities to the KNM ER 1470 cranium from Kenya (Homo rudolfensis), a morphotype previously unrecognized at Olduvai. ER 1470 and OH 65 can be accommodated in the H. habilis holotype, casting doubt on H. rudolfensis as a biologically valid taxon. C1 Rutgers State Univ, Dept Anthropol, Ctr Human Evolutionary Studies, New Brunswick, NJ 08901 USA. Univ Georgia, Dept Anthropol, Athens, GA 30602 USA. Univ Georgia, Inst Ecol, Athens, GA 30602 USA. Paleocultural & Environm Res, Dar Es Salaam, Tanzania. Univ Witwatersrand, Sch Med, Sch Anat Sci, ZA-2193 Johannesburg, South Africa. Berkeley Geochronol Ctr, Berkeley, CA 94709 USA. Univ Arizona, Dept Geosci, Tucson, AZ 85718 USA. Rutgers State Univ, Dept Geol Sci, Piscataway, NJ 08854 USA. Univ Liverpool, Dept Earth Sci, Liverpool L69 3BX, Merseyside, England. Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. Univ Cape Town, Dept Archaeol, ZA-7700 Rondebosch, Cape Town, South Africa. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, MRC 119, Washington, DC 20560 USA. Ebert & Associates, Albuquerque, NM 87107 USA. RP Blumenschine, RJ (reprint author), Rutgers State Univ, Dept Anthropol, Ctr Human Evolutionary Studies, 131 George St, New Brunswick, NJ 08901 USA. NR 29 TC 127 Z9 130 U1 3 U2 39 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 21 PY 2003 VL 299 IS 5610 BP 1217 EP 1221 DI 10.1126/science.1075374 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 646YY UT WOS:000181065500036 PM 12595689 ER PT J AU Nevalainen, J Lieu, R Bonamente, M Lumb, D AF Nevalainen, J Lieu, R Bonamente, M Lumb, D TI Soft X-ray excess emission in clusters of galaxies observed with XMM-Newton SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (Coma, A1795, A3112); X-rays : galaxies ID EXTREME-ULTRAVIOLET EMISSION; HOT INTERGALACTIC MEDIUM; COMA-CLUSTER; ABELL-2199; VIRGO; ABELL-1795; ABSORPTION; DISCOVERY; RADIATION; A1795 AB We present results on the spectroscopic analysis of XMM- Newton EPIC data of the central 0.5 h(50)(-1) regions of the clusters of galaxies Coma, A1795, and A3112. The temperature of the hot intracluster gas as determined by modeling the 2-7 keV PN and MOS data is consistent with that inferred from the Fe xxv/Fe xxvI line ratio. A significant warm emission component at a level above the systematic uncertainties is evident in the data and confirmed by ROSAT PSPC data for Coma and A1795. The nonthermal origin of the phenomenon cannot be ruled out at the current level of calibration accuracy, but the thermal model fits the data significantly better, with temperatures and electron densities in the range 0.6-1.3 keV and 10(-4) to 10(-3) cm(-3), respectively. In the outer parts of the clusters the properties of the warm component are marginally consistent with the results of recent cosmological simulations, which predict a large fraction of the current epoch's baryons located in a warm-hot intergalactic medium ( WHIM). However, the derived densities are too high in the cluster cores, compared to WHIM simulations, and thus more theoretical work is needed to fully understand the origin of the observed soft X-ray excess. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Alabama, Huntsville, AL 35899 USA. Estec, Noordwijk, Netherlands. RP Nevalainen, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 38 TC 34 Z9 34 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 FEB 20 PY 2003 VL 584 IS 2 BP 716 EP 728 DI 10.1086/345830 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WG UT WOS:000180884100018 ER PT J AU Raymond, JC Ghavamian, P Sankrit, R Blair, WP Curiel, S AF Raymond, JC Ghavamian, P Sankrit, R Blair, WP Curiel, S TI Far-ultraviolet spectra of a nonradiative shock wave in the Cygnus Loop SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Cygnus Loop); shock waves; supernova remnants; ultraviolet : ISM ID SUPERNOVA REMNANT; X-RAY; INTERSTELLAR-MEDIUM; EMISSION-LINES; TELESCOPE; FILAMENT; SPECTROSCOPY; PERFORMANCE; CALIBRATION; MISSION AB Spatial and spectral profiles of O VI emission behind a shock wave on the northern edge of the Cygnus Loop were obtained with the Far Ultraviolet Spectroscopic Explorer. The velocity width of the narrowest O vi profile places a tight constraint on the electron-ion and ion-ion thermal equilibration in this 350 km s(-1) collisionless shock. Unlike faster shocks in SN 1006 and in the heliosphere, this shock brings oxygen ions and protons to within a factor of 2.5 of the same temperature. Comparison with other shocks suggests that shock speed, rather than Alfven Mach number, may control the degree of thermal equilibration. We combine the O vi observations with a low-resolution far-UV spectrum from the Hopkins Ultraviolet Telescope, an H image, and ROSAT PSPC X-ray data to constrain the preshock density and the structure along the line of sight. As part of this effort, we model the effects of resonance scattering of O vi photons within the shocked gas and compute time-dependent ionization models of the X-ray emissivity. Resonance scattering affects the O vi intensities at the factor of 2 level, and the soft spectrum of the X-ray rim can be mostly attributed to departures from ionization equilibrium. The preshock density is about twice the canonical value for the Cygnus Loop X-ray emitting shocks. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Natl Autonomous Univ Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Raymond, JC (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 59 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 FEB 20 PY 2003 VL 584 IS 2 BP 770 EP 781 DI 10.1086/345741 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WG UT WOS:000180884100023 ER PT J AU Takakuwa, S Kamazaki, T Saito, M Hirano, N AF Takakuwa, S Kamazaki, T Saito, M Hirano, N TI (HCO+)-C-13 and CH3OH line observations of prestellar dense cores in the TMC-1C region. II. Internal structure SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : individual (TMC-1C); ISM : molecules; stars : formation ID L134N MOLECULAR CORE; DARK CLOUDS; INTERSTELLAR CLOUDS; PROTOSTELLAR CORES; INITIAL CONDITIONS; STAR-FORMATION; SCALE; COMPLEX; TAURUS; EVOLUTION AB We have carried out detailed (HCO+)-C-13 (J = 1-0) and CH3OH (J(K) = 2(0)-1(0) A(+)) observations of two dense cores in the TMC-1C region with the 45 m telescope at Nobeyama Radio Observatory and the Nobeyama Millimeter Array (NMA). These two cores, (HCO+)-C-13 core 2 and CH3OH core 6, were identified previously by the (HCO+)-C-13 and CH3OH mapping observations of the entire TMC-1C region and show no sign of protostar formation. We found that the internal structure of (HCO+)-C-13 core 2 is different from that of cores with class 0 protostars; this core consists of three velocity components and shows the radial column density distribution of similar tor(-0.43+/-0.08), which is flatter than that in the protostellar cores (similar tor(-1.0)). The internal structure of CH3OH core 6 is different from that of (HCO+)-C-13 core 2; the combined images of the 45 m and NMA data have revealed that there are three smaller scale CH3OH "clumps" similar to2500 AU in size inside this core. The mass of the small-scale clumps, similar to0.02 M., is much smaller than the virial mass (similar to0.3 M.), suggesting that these clumps are gravitationally unbound. The velocity dispersion observed in these small-scale clumps is 0.45-0.5 km s(-1), which is comparable to that of clumps with 0.02-0.03 pc in radius. A comparison of the velocity dispersion of the small-scale clumps and that of larger scale cores suggests that the velocity dispersion that follows the power law in the radius larger than similar to0.02-0.03 pc turns into a constant value ofsimilar to0.45-0.5 km s(-1) in the smaller size scale. The mass-size relation of the prestellar gas structures suggests that they follow the trend of constant gas density (similar to10(5) cm(-3)) in the radius from 0.006 to 0.3 pc and that the smaller scale structures tend to be gravitationally unbound. The presence of the small clumps with substellar masses in prestellar cores implies that coalescence processes are likely to play an important role in forming protostars inside the cores. The observational difference of the internal structures among CH3OH core 6, (HCO+)-C-13 core 2, and protostellar cores might represent the difference of the evolutionary stages. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Natl Astron Observ, Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. Natl Astron Observ, Tokyo 1818588, Japan. RP Takakuwa, S (reprint author), Harvard Smithsonian Ctr Astrophys, 82 Puuhonu Pl,Suite 210, Hilo, HI 96720 USA. NR 43 TC 20 Z9 20 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 FEB 20 PY 2003 VL 584 IS 2 BP 818 EP 831 DI 10.1086/345845 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WG UT WOS:000180884100027 ER PT J AU Kumar, P Narayan, R AF Kumar, P Narayan, R TI X-ray lines from gamma-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; gamma rays : theory ID AFTERGLOW; PROGENITOR AB X-ray lines have been recently detected in the afterglows of a few gamma-ray bursts. We derive general constraints on the physical conditions in the line-emitting gas and illustrate our results using as an example the multiple Kalpha lines detected by Reeves et al. in GRB 011211. We argue that photoionization models previously discussed in the literature require either a very extreme geometry or too much mass in the line-emitting region. Shock-heated models also have a serious problem since they require the emitting region to have a large optical depth unless electrons in this region are shock-heated multiple times. We propose a new model in which gamma rays from the burst and hard X-rays from the early afterglow are backscattered by an electron-positron pair screen at a distance of about 10(14)-10(15) cm from the source and irradiate the expanding outer layers of the supernova ejecta, thereby producing X-ray lines. The model suers from fewer problems compared to previous models. It also has the advantage of requiring only a single explosion to produce both the gamma-ray burst (GRB) and the supernova ejecta, in contrast to most other models for the lines that require the supernova to go off days or weeks prior to the GRB. The model, however, has difficulty explaining the greater than 10(48) ergs of energy emitted in the X-ray lines, which requires somewhat extreme choices of model parameters. The difficulties associated with the various models are not particular to GRB 011211. They are likely to pose a problem for any GRB with X-ray lines. C1 Univ Texas, Dept Astron, Austin, TX 78731 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kumar, P (reprint author), Univ Texas, Dept Astron, Austin, TX 78731 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 22 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 FEB 20 PY 2003 VL 584 IS 2 BP 895 EP 903 DI 10.1086/345892 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WG UT WOS:000180884100033 ER PT J AU Kenter, AT Murray, SS AF Kenter, AT Murray, SS TI A new technique for determining the number of X-ray sources per flux density interval SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : miscellaneous; surveys; X-rays : galaxies ID NOISE AB We present a technique for determining the number of X-ray sources per flux density interval, the log N-log S relationship, that is mathematically analogous to spectral fitting. This technique is ideal for X-ray source counts obtained using the Chandra X-ray Observatory since the telescope and the focal plane instruments have been well modeled. This technique is of general applicability. In this paper, we apply it to a wavelet source-detect analysis of a Chandra Advanced CCD Imaging Spectrometer (ACIS-I) mosaic image of a 1.35 deg(2) survey of the Lockman Hole. We verify the technique via Monte Carlo simulations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kenter, AT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 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 FEB 20 PY 2003 VL 584 IS 2 BP 1016 EP 1020 DI 10.1086/345790 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WG UT WOS:000180884100044 ER PT J AU Sokoloski, JL Kenyon, SJ AF Sokoloski, JL Kenyon, SJ TI CH Cygni. I. Observational evidence for a disk-jet connection SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : symbiotic; instabilities; stars : winds, outflows; techniques : photometric ID QUASI-PERIODIC OSCILLATIONS; X-RAY BINARIES; BLACK-HOLE; CATACLYSMIC VARIABLES; ACCRETION DISCS; GRS 1915+105; FU ORIONIS; RADIO JET; STAR; VARIABILITY AB We investigate the role of accretion in the production of jets in the symbiotic star CH Cygni. Assuming that the rapid stochastic optical variations in CH Cygni come from the accretion disk, as in cataclysmic variables, we use changes in this flickering to diagnose the state of the disk in 1997. At that time, CH Cygni dropped to a very low optical state, and Karovska et al. report that a radio jet was produced. For approximately 1 yr after the jet production, the amplitude of the fastest (timescale of minutes) variations was significantly reduced, although smooth, hour-timescale variations were still present. This light-curve evolution indicates that the inner disk may have been disrupted, or emission from this region suppressed, in association with the mass ejection event. We describe optical spectra that support this interpretation of the flickering changes. The simultaneous state change, jet ejection, and disk disruption suggest a comparison between CH Cygni and some black hole candidate X-ray binaries that show changes in the inner-disk radius in conjunction with discrete ejection events on a wide range of timescales (e.g., the microquasar GRS 1915+105 and XTE J1550-564). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sokoloski, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 56 TC 33 Z9 33 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 FEB 20 PY 2003 VL 584 IS 2 BP 1021 EP 1026 DI 10.1086/345901 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WG UT WOS:000180884100045 ER PT J AU Sokoloski, JL Kenyon, SJ AF Sokoloski, JL Kenyon, SJ TI CH Cygni. II. Optical flickering from an unstable disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : eclipsing; binaries : symbiotic; instabilities; techniques : photometric ID TRIPLE SYMBIOTIC SYSTEM; STROMGREN U-PHOTOMETRY; CATACLYSMIC VARIABLES; ACCRETION DISKS; VARIABILITY; BINARIES; ENVELOPE; MODELS; MATTER; STARS AB CH Cygni began producing rapid, stochastic optical variations with the onset of symbiotic activity in 1963. We use changes in this flickering between 1997 and 2000 to diagnose the state of the accretion disk during this time. In the 1998 high state, the luminosity of the B-band ickering component was typically more than 20 times higher than in the 1997 and 2000 low states. Therefore, the physical process or region that produces the ickering was also primarily responsible for the large optical flux increase in the 1998 high state. Assuming that the rapid, stochastic optical variations in CH Cygni come from the accretion disk, as in cataclysmic variable stars, a change in the accretion rate through the disk led to the 1998 bright state. All flickering disappeared in 1999, when the accreting white dwarf was eclipsed by the red giant orbiting with a period of approximately 14 yr, according to the ephemeris of Hinkle et al. and the interpretation of Eyres et al. We did not find any evidence for periodic or quasi-periodic oscillations in the optical emission from CH Cygni in either the high or low state, and we discuss the implications for magnetic propeller models of this system. As one alternative to propeller models, we propose that the activity in CH Cygni is driven by accretion through a disk with a thermal-viscous instability similar to the instabilities believed to exist in dwarf novae and suggested for FU Ori pre-main-sequence stars and soft X-ray transients. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sokoloski, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jsokoloski@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X NR 41 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2003 VL 584 IS 2 BP 1027 EP 1034 DI 10.1086/345902 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WG UT WOS:000180884100046 ER PT J AU Barth, AJ Sari, R Cohen, MH Goodrich, RW Price, PA Fox, DW Bloom, JS Soderberg, AM Kulkarni, SR AF Barth, AJ Sari, R Cohen, MH Goodrich, RW Price, PA Fox, DW Bloom, JS Soderberg, AM Kulkarni, SR TI Optical spectropolarimetry of the GRB 020813 afterglow SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; polarization ID GAMMA-RAY BURST; LIGHT CURVES; LINEAR-POLARIZATION; GRB 990510; REDSHIFT; SPECTROSCOPY; CONSTRAINTS; ENVIRONMENT; GRB-010222; DEPENDENCE AB The optical afterglow of gamma-ray burst GRB 020813 was observed for 3 hr with the LRIS spectropolarimeter at the Keck I telescope, beginning 4.7 hr after the burst was detected by the HETE-2. The spectrum reveals numerous metal absorption lines that we identify with two systems at z = 1.223 and z = 1.255. We also detect [O II] lambda3727 emission line at z = 1.255, and we identify this galaxy as the likely host of the GRB. After a correction for Galactic interstellar polarization, the optical afterglow has a linear polarization of 1.8%-2.4% during 4.7-7.9 hr after the burst. A measurement of p = 0.80% +/- 0.16% on the following night by Covino et al. demonstrates significant polarization variability over the next 14 hr. The lack of strong variability in the position angle of linear polarization indicates that the magnetic field in the jet is likely to be globally ordered rather than composed of a number of randomly oriented cells. Within the framework of afterglow models with collimated flows, the relatively low observed polarization suggests that the magnetic field components perpendicular and parallel to the shock front are only different by about 20%. C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA. WM Keck Observ, Kamuela, HI 96743 USA. Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barth, AJ (reprint author), CALTECH, Dept Astron, MS 105-24, Pasadena, CA 91125 USA. EM barth@astro.caltech.edu OI Barth, Aaron/0000-0002-3026-0562 NR 42 TC 81 Z9 81 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 FEB 20 PY 2003 VL 584 IS 2 BP L47 EP L51 DI 10.1086/373889 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WH UT WOS:000180884400002 ER PT J AU Bersier, D Stanek, KZ Winn, JN Grav, T Holman, MJ Matheson, T Mochejska, B Steeghs, D Walker, AR Garnavich, PM Quinn, J Jha, S Cook, KH Craig, WW Meintjes, PJ Calitz, JJ AF Bersier, D Stanek, KZ Winn, JN Grav, T Holman, MJ Matheson, T Mochejska, B Steeghs, D Walker, AR Garnavich, PM Quinn, J Jha, S Cook, KH Craig, WW Meintjes, PJ Calitz, JJ TI The unusual optical afterglow of the gamma-ray burst GRB 021004: Color changes and short-timescale variability SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID IMAGE SUBTRACTION; CCD PHOTOMETRY; GRB-990510; PROGRAM AB We report UBVRI observations of the optical afterglow of the gamma-ray burst GRB 021004. We observed significant (similar to10%-20%) deviations from a power-law decay on several timescales, ranging from a few hours down to 20-30 minutes. We also observed a significant color change starting similar to1.5 days after the burst, confirming the spectroscopic results already reported by Matheson et al. We discuss these results in the context of several models that have recently been proposed to account for the anomalous photometric behavior of this event. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Univ Orange Free State, Dept Phys, ZA-9300 Bloemfontein, South Africa. RP Bersier, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 51 TC 57 Z9 58 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 FEB 20 PY 2003 VL 584 IS 2 BP L43 EP L46 DI 10.1086/373888 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643WH UT WOS:000180884400001 ER PT J AU Kalfatovic, TMR AF Kalfatovic, TMR TI Michelangelo & the Pope's ceiling. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Kalfatovic, TMR (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 FEB 15 PY 2003 VL 128 IS 3 BP 134 EP 134 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 673WM UT WOS:000182603300059 ER PT J AU Schroll, S AF Schroll, S TI Photography: A cultural history. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Schroll, S (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 FEB 15 PY 2003 VL 128 IS 3 BP 134 EP 134 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 673WM UT WOS:000182603300062 ER PT J AU Li, LX AF Li, LX TI Evolution of magnetic fields around a Kerr black hole SO PHYSICAL REVIEW D LA English DT Article ID GLOBAL MAGNETOHYDRODYNAMIC SIMULATIONS; MARGINALLY STABLE ORBIT; ACCRETION DISK; ENERGY EXTRACTION; CONNECTION; RADIATION; MODEL; SPIN AB The evolution of magnetic fields frozen to a perfectly conducting plasma fluid around a Kerr black hole is investigated. We focus on the plunging region between the black hole horizon and the marginally stable circular orbit in the equatorial plane, where the centrifugal force is unable to stably balance the gravitational force. Adopting the kinematic approximation where the dynamical effects of magnetic fields on the fluid motion are ignored, we exactly solve Maxwell's equations with the assumptions that the geodesic motion of the fluid is stationary and axisymmetric, the magnetic field has only radial and azimuthal components and depends only on time and radial coordinates. We show that the stationary state of the magnetic field in the plunging region is uniquely determined by the boundary conditions at the marginally stable circular orbit. If the magnetic field at the marginally stable circular orbit is in a stationary state, the magnetic field in the plunging region will quickly settle into a stationary state if it is not so initially, in a time determined by the dynamical time scale in the plunging region. The radial component of the magnetic field at the marginally stable circular orbit is more important than the toroidal component in determining the structure and evolution of the magnetic field in the plunging region. Even if at the marginally stable circular orbit the toroidal component is zero, in the plunging region a toroidal component is quickly generated from the radial component by the shear motion of the fluid. Finally, we discuss the dynamical effects of magnetic fields on the motion of the fluid in the plunging region. We show that the dynamical effects of magnetic fields are unimportant in the plunging region if they are negligible on the marginally stable circular orbit. This supports the "no-torque inner boundary condition" of thin disks, contrary to the claim in the recent literature. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, LX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 36 TC 12 Z9 12 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD FEB 15 PY 2003 VL 67 IS 4 AR 044007 DI 10.1103/PhysRevD.67.044007 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 653NR UT WOS:000181443000036 ER PT J AU Piperno, DR Stothert, KE AF Piperno, DR Stothert, KE TI Phytolith evidence for early Holocene Cucurbita domestication in Southwest Ecuador SO SCIENCE LA English DT Article AB Cucurbita (squash and gourd) phytoliths recovered from two early Holocene archaeological sites in southwestern Ecuador and directly dated to 10,130 to 9320 carbon-14 years before the present (about 12,000 to 10,000 calendar years ago) are identified as derived from domesticated plants because they are considerably larger than those from modern wild taxa. The beginnings of plant husbandry appear to have been preceded by the exploitation of a wild species of Cucurbita during the terminal Pleistocene. These data provide evidence for an independent emergence of plant food production in lowland South America that was contemporaneous with or slightly before that in highland Mesoamerica. C1 Univ Texas, Ctr Archaeol Res, San Antonio, TX 78249 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 16 TC 103 Z9 112 U1 1 U2 8 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 14 PY 2003 VL 299 IS 5609 BP 1054 EP 1057 DI 10.1126/science.1080365 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 645DB UT WOS:000180960000044 PM 12586940 ER PT J AU Fearnside, PM Laurance, WF AF Fearnside, PM Laurance, WF TI Comment on "Determination of deforestation rates of the world's humid tropical forests" SO SCIENCE LA English DT Editorial Material ID BRAZILIAN AMAZONIA; ABOVEGROUND BIOMASS; CARBON C1 Natl Inst Amazonian Res INPA, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. RP Fearnside, PM (reprint author), Natl Inst Amazonian Res INPA, Dept Ecol, CP 478, BR-69011970 Manaus, Amazonas, Brazil. EM pmfearn@inpa.gov.br; laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011 OI Fearnside, Philip/0000-0003-3672-9082 NR 19 TC 4 Z9 4 U1 2 U2 17 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 14 PY 2003 VL 299 IS 5609 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 645DB UT WOS:000180960000024 ER PT J AU Gingerich, O AF Gingerich, O TI On the shoulders of giants: The great works of physics and astronomy SO NATURE LA English DT Book Review 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 1 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 13 PY 2003 VL 421 IS 6924 BP 694 EP 695 DI 10.1038/421694a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 644UP UT WOS:000180938000019 ER PT J AU Nicastro, F Zezas, A Elvis, M Mathur, S Fiore, F Cecchi-Pestellini, C Burke, D Drake, J Casella, P AF Nicastro, F Zezas, A Elvis, M Mathur, S Fiore, F Cecchi-Pestellini, C Burke, D Drake, J Casella, P TI The far-ultraviolet signature of the 'missing' baryons in the Local Group of galaxies SO NATURE LA English DT Article ID HIGH-VELOCITY CLOUDS; SPECTROSCOPIC EXPLORER OBSERVATIONS; O-VI AB The number of baryons detected in the low-redshift (z < 1) Universe is far smaller than the number detected in corresponding volumes at higher redshifts. Simulations(1-3) of the formation of structure in the Universe show that up to two-thirds of the 'missing' baryons may have escaped detection because of their high temperature and low density. One of the few ways to detect this matter directly is to look for its signature in the form of ultraviolet absorption lines in the spectra of background sources such as quasars. Here we show that the amplitude of the average velocity vector of 'high velocity' OVI (O5+) absorption clouds detected in a survey(4) of ultraviolet emission from active galactic nuclei decreases significantly when the vector is transformed to the frames of the Galactic Standard of Rest and the Local Group of galaxies. At least 82 per cent of these absorbers are not associated with any 'high velocity' atomic hydrogen complex in our Galaxy, and are therefore likely to result from a primordial warm-hot intergalactic medium pervading an extended corona around the Milky Way or the Local Group. The total mass of baryons in this medium is estimated to be up to &SIM;10(12) solar masses, which is of the order of the mass required(5) to dynamically stabilize the Local Group. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Osservatorio Astron Monteporzio, I-00040 Monte Porzio Catone, RM, Italy. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Casella, Piergiorgio/0000-0002-0752-3301; Cecchi Pestellini, Cesare/0000-0001-7480-0324; Nicastro, Fabrizio/0000-0002-6896-1364; Burke, Douglas/0000-0003-4428-7835; Fiore, Fabrizio/0000-0002-4031-4157 NR 37 TC 74 Z9 74 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 FEB 13 PY 2003 VL 421 IS 6924 BP 719 EP 721 DI 10.1038/nature01369 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 644UP UT WOS:000180938000036 PM 12610618 ER PT J AU Staveley-Smith, L Kim, S Calabretta, MR Haynes, RF Kesteven, MJ AF Staveley-Smith, L Kim, S Calabretta, MR Haynes, RF Kesteven, MJ TI A new look at the large-scale HI structure of the Large Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; Magellanic Clouds; radio lines : galaxies ID SUPERGIANT SHELL LMC-4; NEAR-INFRARED SURVEYS; STAR-FORMATION; MILKY-WAY; MOLECULAR-HYDROGEN; CONSTELLATION-III; GAS; VELOCITY; DUST; GALAXIES AB We present a Parkes multibeam H i survey of the Large Magellanic Cloud (LMC). This survey, which is sensitive to spatial structure in the range 200 pc to 10 kpc, complements the Australia Telescope Compact survey, which is sensitive to structure in the range 15-500 pc. With an rms column density sensitivity of 8 x 10(16) cm(-2) for narrow lines and 4 x 10(17) cm(-2) for typical linewidths of 40 km s(-1), emission is found to be extensive well beyond the main body of the LMC. Arm-like features extend from the LMC to join the Magellanic Bridge and the Leading Arm, a forward counterpart to the Magellanic Stream. These features, whilst not as dramatic as those in the Small Magellanic Cloud, appear to have a common origin in the Galactic tidal field, in agreement with recent 2MASS and DENIS results for the stellar population. The diffuse gas that surrounds the LMC, particularly at PAs of 90degrees-330degrees, appears to be loosely associated with tidal features, but loosening by the ram pressure of tenuous Galactic halo gas against the outer parts of the LMC cannot be discounted. High-velocity clouds, which lie between the Galaxy and the LMC in velocity and that appear in the ultraviolet spectra of some LMC stars, are found to be associated with the LMC if their heliocentric velocity exceeds approximately +100 km s(-1) . They are possibly the product of energetic outflows from the LMC disc. The H i mass of the LMC is found to be (4.8 +/- 0.2) x 10(8) M-circle dot (for an assumed distance of 50 kpc), substantially more than previous recent measurements. C1 CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. RP Staveley-Smith, L (reprint author), CSIRO, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. RI Staveley-Smith, Lister/A-1683-2011 OI Staveley-Smith, Lister/0000-0002-8057-0294 NR 83 TC 147 Z9 148 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 FEB 11 PY 2003 VL 339 IS 1 BP 87 EP 104 DI 10.1046/j.1365-8711.2003.06146.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 641JH UT WOS:000180741300011 ER PT J AU Adelberger, KL Steidel, CC Shapley, AE Pettini, M AF Adelberger, KL Steidel, CC Shapley, AE Pettini, M TI Galaxies and intergalactic matter at redshift z similar to 3: Overview SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : formation; galaxies : high-redshift; intergalactic medium; quasars : absorption lines ID LYMAN-BREAK GALAXIES; LY-ALPHA FOREST; STAR-FORMING GALAXIES; ECHELLE SPECTROGRAPH; GALACTIC WINDS; METAL ENRICHMENT; ABSORPTION-LINES; DWARF GALAXIES; EVOLUTION; TELESCOPE AB We present the first results from a survey of the relative spatial distributions of galaxies, intergalactic neutral hydrogen, and intergalactic metals at high redshift. We obtained high-resolution spectra of eight bright quasars (QSOs) at 3.1 < z < 4.1 and spectroscopic redshifts for 431 Lyman break galaxies (LBGs) at slightly lower redshifts. Comparing the locations of galaxies to the absorption lines in the QSO spectra shows that the intergalactic medium contains less neutral hydrogen than the global average within r less than or similar to 0.5 h(-1) comoving Mpc of LBGs and more than average at slightly larger distances 1 h(-1) comoving Mpc less than or similar to r less than or similar to 5 h(-1) comoving Mpc. The intergalactic medium within the largest overdensities at z similar to 3, which will presumably evolve into the intracluster medium by z similar to 0, is rich in neutral hydrogen and C IV. The lack of H I absorption at small distances from LBGs appears unlikely to be produced solely by the Lyman continuum radiation they emit; it may show that the galaxies supernova-driven winds maintain their measured outflow velocities of similar to600 km s(-1) for a few hundred million years and drive away nearby intergalactic gas. We present correlation functions of galaxies with Lyalpha forest flux decrements, with C IV systems, and with other galaxies. We describe the association of galaxies with damped Lyalpha systems and with intergalactic He II opacity. A strong observed correlation of galaxies with intergalactic metals supports the idea that LBG winds have enriched their surroundings. 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 Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 78 TC 375 Z9 376 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2003 VL 584 IS 1 BP 45 EP 75 DI 10.1086/345660 PN 1 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UH UT WOS:000180706000003 ER PT J AU Georgantopoulos, I Zezas, A Ward, MJ AF Georgantopoulos, I Zezas, A Ward, MJ TI X-ray luminous galaxies. I. Chandra observations of IRAS 00317-2142 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (IRAS 00317-2142); galaxies : nuclei; quasars : general; X-rays : galaxies ID CLASSIFICATION; BEPPOSAX; NUCLEUS; REGION; AGN AB We present Chandra observations of the enigmatic galaxy IRAS 00317-2142, which is classified as a star-forming galaxy on the basis of the ionization level of its emission lines. However, a weak broad H wing and a high X-ray luminosity give away the presence of an active nucleus. The Chandra image reveals a nuclear point source (L(2-10 keV) similar to 6 x 10(41) ergs s(-1)), contributing over 80% of the galaxy X-ray counts in the 0.3-8 keV band. This is surrounded by some fainter nebulosity extending up to 6 kpc. The nucleus does not show evidence for short-term variability. However, we detect long-term variations between the ROSAT, ASCA, and Chandra epochs. Indeed, the source has decreased its flux by over a factor of 25 in a period of about 10 yr. The nuclear X-ray spectrum is well represented by a power law with a photon index of Gamma = 1.91(-0.15)(+0.17), while the extended emission is represented by a Raymond-Smith component with a temperature of similar to0.6 keV. We find no evidence for the presence of an Fe line. The nucleus is absorbed by an intrinsic column density of N-H similar to 8 x 10(20) cm(-2). Thus, the Chandra observations suggest that at least the X-ray emission is dominated by a type 1 active galactic nucleus (AGN). Then the observed optical spectrum can be explained by the masking of the nucleus by the powerful star-forming component. These, together with previous X-ray observations of galaxies with no clear signs of AGN activity in the optical (e.g., NGC 6240), cast doubt on the optical classification scheme and have implications for the nature of the normal galaxies detected in deep Chandra X-ray surveys. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. Univ Leicester, Dept Phys & Astron, Xray Astron Grp, Leicester LE1 7RH, Leics, England. RP Georgantopoulos, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Georgantopoulos, Ioannis/L-3687-2013; Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 25 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2003 VL 584 IS 1 BP 129 EP 134 DI 10.1086/345598 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UH UT WOS:000180706000007 ER PT J AU Huang, JS Glazebrook, K Cowie, LL Tinney, C AF Huang, JS Glazebrook, K Cowie, LL Tinney, C TI The Hawaii plus Anglo-Australian Observatory K-band galaxy redshift survey. I. The local K-band luminosity function SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : luminosity function, mass function infrared : galaxies surveys ID FIELD; EVOLUTION; COUNTS; CLASSIFICATION; DENSITY; SAMPLE AB We present the K-band local luminosity function derived from a sample of 1056 bright (K < 15) K-selected galaxies from the Hawaii+ Anglo-Australian Observatory (AAO) K-band redshift survey. The Hawaii+ AAO K-band redshift survey covers four equatorial fields with a total area of 8.22 deg(2). We derive both the nonparametric and Schechter luminosity function from our data and determine M*(K) = -23.70 +/- 0.08 + 5 log(10)(h), α = -1.37 +/- 0.10, and φ* 0.013 +/- 0.003 h(3) Mpc(-3) for a universe with &UOmega;(m) = 0.3 and &UOmega;(&ULambda;) = 0.7. We also measure the K-band luminosity function for the early- and later type galaxies from our morphologically classified subsample. It appears that later type galaxies have a fainter M and a steep slope, while early- type galaxies have a much brighter M and a quite at slope in their K-band luminosity functions. This is consistent with what has been found in optical-type dependent luminosity function. The K-band luminosity density derived using our luminosity function is now measured at a similar redshift depth to optical luminosity densities in the Sloan Digital Sky Survey redshift survey. It is 2 times higher than the previous measurement from the shallower 2MASS sample and resolves the previously reported discrepancies between optical and near-infrared luminosity densities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Anglo Australian Observ, Epping, NSW 1710, Australia. RP Huang, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Glazebrook, Karl/N-3488-2015 OI Glazebrook, Karl/0000-0002-3254-9044 NR 30 TC 68 Z9 68 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 FEB 10 PY 2003 VL 584 IS 1 BP 203 EP 209 DI 10.1086/345619 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UH UT WOS:000180706000014 ER PT J AU Kamazaki, T Saito, M Hirano, N Umemoto, T Kawabe, R AF Kamazaki, T Saito, M Hirano, N Umemoto, T Kawabe, R TI Molecular outflow search in the rho Ophiuchi A and B2 regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : individual (rho Ophiuchi); ISM : jets and outflows; stars : formation; stars : winds, outflows ID YOUNG STELLAR OBJECTS; DARK CLOUD; STARS; (CO)-C-13; VLA-1623; POLARIMETRY; PROTOSTARS; EMISSION; CLUSTER; COBWEBS AB We have searched for CO molecular outflows associated with the cloud A and B2 of the rho Ophiuchi star-forming region. On the basis of single-dish (CO)-C-12 (J=3-2) and interferometric (CO)-C-12 (J=1-0) observations, we have identified three molecular outflows in the rho Oph A cloud and one in the rho Oph B2 cloud. Out of the four outflows observed in these regions, one is the known outflow driven by the Class 0 source, VLA 1623, and the other three are newly discovered ones. The inclination and opacity corrected momentum flux F-CO of newly detected outflows are roughly comparable to those of Class I objects observed by Bontemps et al. (1996). All the newly discovered outflows are likely to be driven by Class II sources or near-infrared sources, and none of them is associated with the cold submillimeter-millimeter sources without infrared counter parts. These results indicate that protostars associated with outflows whose mass and momentum flux exceed our detection limit are not formed yet in the high-density ridge of the rho Oph A region and the northeastern condensation in the rho Oph B2 region, suggesting that they are considered to be pre-protostellar cores. C1 Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Grad Univ Adv Studies, Natl Astron Observ, Dept Astron Sci, Tokyo 1818588, Japan. Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. RP Kamazaki, T (reprint author), Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. NR 23 TC 20 Z9 20 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 FEB 10 PY 2003 VL 584 IS 1 BP 357 EP 367 DI 10.1086/345659 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UH UT WOS:000180706000025 ER PT J AU Seward, FD Slane, PO Smith, RK Sun, M AF Seward, FD Slane, PO Smith, RK Sun, M TI A compact central object in the supernova remnant Kesteven 79 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Kesteven 79); stars : neutron; supernova remnants; X-rays : stars ID QUIET NEUTRON-STAR; X-RAY-EMISSION; PULSAR SURVEY; RADIO; G33.6+0.1; DISCOVERY AB A Chandra X-ray observation has detected an unresolved source at the center of the supernova remnant Kes 79. The best single-model fit to the source spectrum is a blackbody with an X-ray luminosity of L-X(0.3-8.0 keV)=7x10(33) ergs s(-1). There is no evidence for a surrounding pulsar wind nebula. There are no cataloged counterparts at other wavelengths, but the absorption is high. The source properties are similar to the central source in Cas A even though the Kes 79 remnant is considerably older. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Harvard Univ, Cambridge, MA 02138 USA. RP Seward, FD (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 35 Z9 35 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 FEB 10 PY 2003 VL 584 IS 1 BP 414 EP 417 DI 10.1086/345600 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UH UT WOS:000180706000030 ER PT J AU Drake, JJ Wagner, RM Starrfield, S Butt, Y Krautter, J Bond, HE Della Valle, M Gehrz, RD Woodward, CE Evans, A Orio, M Hauschildt, P Hernanz, M Mukai, K Truran, JW AF Drake, JJ Wagner, RM Starrfield, S Butt, Y Krautter, J Bond, HE Della Valle, M Gehrz, RD Woodward, CE Evans, A Orio, M Hauschildt, P Hernanz, M Mukai, K Truran, JW TI The extraordinary X-ray light curve of the classical nova V1494 Aquilae (1999 No. 2) in outburst: The discovery of pulsations and a burst SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae; cataclysmic variables; stars : individual (V1494 Aquilae); stars : oscillations; white dwarfs; X-rays : binaries; X-rays : bursts ID V382 VELORUM; EMISSION; ROSAT; STAR AB V1494 Aql (Nova Aql 1999 No. 2) was discovered on 1999 December 2. We obtained Chandra ACIS-I spectra on 2000 April 15 and June 7 which appear to show only emission lines. Our third observation, on August 6, showed that its spectrum had evolved to that characteristic of a Super Soft X-ray Source. We then obtained Chandra LETG+HRC-S spectra on September 28 (8 ks) and October 1 (17 ks). We analyzed the X-ray light curve of our grating observations and found both a short timescale "burst" and oscillations. Neither of these phenomena has previously been seen in the light curve of a nova in outburst. The "burst" was a factor of similar to10 rise in X-ray counts near the middle of the second observation, and which lasted about 1000 s; it exhibited at least two peaks, in addition to other structure. Our time series analysis of the combined 25 ks observation shows a peak at similar to2500 s which is present in independent analyses of both the zeroth-order image and the dispersed spectrum and is not present in similar analyses of grating data for HZ 43 and Sirius B. Further analyses of the V1494 Aql data find other periods present which implies that we are observing nonradial g(+) modes from the pulsating, rekindled white dwarf. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Large Binocular Telescope Observ, Tucson, AZ 85721 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Heidelberg Koenigstuhl Landessternwarte, D-69121 Heidelberg, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Univ Keele, Dept Phys, Keele ST5 5BG, Staffs, England. Osserv Astron Torino, I-10025 Pino Torinese, Italy. Hamburger Sternwarte, D-21029 Hamburg, Germany. CSIC, Inst Ciencias Espacio, E-08034 Barcelona, Spain. Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Hernanz, Margarita/K-1770-2014; OI Hernanz, Margarita/0000-0002-8651-7910; Della Valle, Massimo/0000-0003-3142-5020 NR 26 TC 63 Z9 64 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 FEB 10 PY 2003 VL 584 IS 1 BP 448 EP 452 DI 10.1086/345534 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UH UT WOS:000180706000034 ER PT J AU Weck, PF Schweitzer, A Stancil, PC Hauschildt, PH Kirby, K AF Weck, PF Schweitzer, A Stancil, PC Hauschildt, PH Kirby, K TI The molecular continuum opacity of (MgH)-Mg-24 in cool stellar atmospheres SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular data; molecular processes; stars : atmospheres; stars : late-type ID MODEL ATMOSPHERES; STARS; LINE AB The opacity due to photodissociation of (MgH)-Mg-24 in the atmospheres of cool stars is investigated. The lowest two electronic transitions A (2)Pi<--X (2)Sigma(+) and B' (2)Sigma(+)<--X (2)Sigma(+) are considered, where the cross sections for the latter were published previously (Weck, Stancil, & Kirby) and the former are presented in this work. Model atmospheres calculated with the PHOENIX code are used to investigate the effect of the photodissociation opacity on spectra of cool stars. The A (2)Pi<--X (2)Sigma(+) photodissociation cross sections are obtained using a combination of ab initio and experimentally derived potential curves and dipole transition moments. Partial cross sections have been evaluated over the accessible wavelength range 1770-4560 Angstrom for all rotational transitions from the vibrational levels v"=0-11. Assuming a Boltzmann distribution of the rovibrational levels of the X (2)Sigma(+) state, LTE photodissociation cross sections are presented for temperatures between 1000 and 5000 K. Shape resonances, arising from rotational predissociation of quasi-bound levels of the A (2)Pi state near threshold, characterize the LTE photodissociation cross sections. A sum rule is proposed as a check on the accuracy of the photodissociation calculations. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Weck, PF (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. OI , Philippe/0000-0002-7610-2893 NR 19 TC 19 Z9 19 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 FEB 10 PY 2003 VL 584 IS 1 BP 459 EP 464 DI 10.1086/345524 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UH UT WOS:000180706000036 ER PT J AU Rybicki, GB AF Rybicki, GB TI A new kinetic equation for Compton scattering SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; radiation mechanisms : general radiative transfer ID PLASMA AB A kinetic equation for Compton scattering is given that differs from the Kompaneets equation in several significant ways. By using an inverse differential operator, this equation allows treatment of problems for which the radiation field varies rapidly on the scale of the width of the Compton kernel. This inverse operator method describes, among other effects, the thermal Doppler broadening of spectral lines and continuum edges and automatically incorporates the process of Compton heating/cooling. It is well adapted for inclusion into a numerical iterative solution of radiative transfer problems. The equivalent kernel of the new method is shown to be a positive function and with reasonable accuracy near the initial frequency, unlike the Kompaneets kernel, which is singular and not wholly positive. It is shown that iterations of the inverse operator kernel can be easily calculated numerically, and a simple summation formula over these iterations is derived that can be efficiently used to compute Comptonized spectra. It is shown that the new method can be used for initial-value and other problems with no more numerical effort than the Kompaneets equation and that it more correctly describes the solution over times comparable to the mean scattering time. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rybicki, GB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 1 Z9 1 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 FEB 10 PY 2003 VL 584 IS 1 BP 528 EP 540 DI 10.1086/345683 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UH UT WOS:000180706000043 ER PT J AU Fabbiano, G Zezas, A King, AR Ponman, TJ Rots, A Schweizer, F AF Fabbiano, G Zezas, A King, AR Ponman, TJ Rots, A Schweizer, F TI The time-variable ultraluminous X-ray sources of "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 ID CYGNUS X-1; BLACK-HOLE; GALAXIES; MODEL AB We report the first results of the Chandra temporal monitoring of the ultraluminous X-ray sources (ULXs) in the Antennae galaxies (NGC 4038/4039). Observations at four different epochs, covering timescales of 2 yr to 2 months, show variability in seven out of nine ULXs, confirming that they are likely to be accreting compact X-ray binaries. The seven variable ULXs exhibit a variety of temporal and spectral behaviors: one has harder X-ray colors with decreasing luminosity, similar to the black hole binary Cyg X-1, but four other ULXs show the opposite behavior. We suggest that the latter may be black hole binaries accreting at very high rates. 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 Observatories, Pasadena, CA 91101 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Rots, Arnold/0000-0003-2377-2356 NR 27 TC 61 Z9 63 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 FEB 10 PY 2003 VL 584 IS 1 BP L5 EP L8 DI 10.1086/368174 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 640UJ UT WOS:000180706100002 ER PT J AU Metcalfe, TS Charbonneau, P AF Metcalfe, TS Charbonneau, P TI Stellar structure modeling using a parallel genetic algorithm for objective global optimization SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE stellar structure; parallel computation; optimization ID WHITE-DWARF GD-358; WHOLE EARTH TELESCOPE; STARS; C-12(ALPHA,GAMMA)O-16; ASTEROSEISMOLOGY; NUCLEOSYNTHESIS; PARAMETERS; INSTRUMENT; AGE AB Genetic algorithms are a class of heuristic search techniques that apply basic evolutionary operators in a computational setting. We have designed a fully parallel and distributed hardware/software implementation of the generalized optimization subroutine PIKAIA, which utilizes a genetic algorithm to provide an objective determination of the globally optimal parameters for a given model against an observational data set. We have used this modeling tool in the context of white dwarf asteroseismology, i.e., the art and science of extracting physical and structural information about these stars from observations of their oscillation frequencies. The efficient, parallel exploration of parameter-space made possible by genetic-algorithm-based numerical optimization led us to a number of interesting physical results: (1) resolution of a hitherto puzzling discrepancy between stellar evolution models and prior asteroseismic inferences of the surface helium layer mass for a DBV white dwarf; (2) precise determination of the central oxygen mass fraction in a white dwarf star, and (3) a preliminary estimate of the astrophysically important but experimentally uncertain rate for the C-12(alpha, gamma) O-16 nuclear reaction. These successes suggest that a broad class of computationally intensive modeling appfications could also benefit from this approach. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Aarhus Univ, Inst Phys & Astron, Theoret Astrophys Ctr, DK-8000 Aarhus C, Denmark. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Metcalfe, TS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Metcalfe, Travis/A-9388-2008 OI Metcalfe, Travis/0000-0003-4034-0416 NR 43 TC 54 Z9 56 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD FEB 10 PY 2003 VL 185 IS 1 BP 176 EP 193 DI 10.1016/S0021-9991(02)00053-0 PG 18 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 679WR UT WOS:000182945400009 ER PT J AU Grant, JA Schutz, AE Campbell, BA AF Grant, JA Schutz, AE Campbell, BA TI Ground-penetrating radar as a tool for probing the shallow subsurface of Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE radar; Mars; water; rover; geophysics; stratigraphy ID GLOBAL SURVEYOR; PEDOGENIC PROCESSES; ORBITER CAMERA; MOJAVE DESERT; EVOLUTION; SURFACE; IMAGES; ROCKS; SCATTERING; TOPOGRAPHY AB [1] Design and testing of an impulse ground-penetrating radar (GPR) for possible rover deployment on Mars in 2009 is well underway. The GPR has mass, power, volume, and data-rate targets of 0.5 kg, 3 W (peak), 3400 cm(3), and 0.3 Mb/d and will possess easily modified bistatic high-frequency (e.g., 500-600 MHz) and monostatic "rat-tail'' (e. g., 100 MHz) antennas. The GPR should be capable of measuring in situ radar properties on Mars to depths of up to 10-20 m, thereby helping to constrain near-surface geology and structure. Initial GPR tests at the site of the 2001 FIDO rover field trials near Cronese Lake, California, confirm the value of the instrument in defining local geologic setting and in providing context for data collected using other rover science payload elements. A rover-deployed GPR may enable three-dimensional mapping of local stratigraphy, which in turn can assist in evaluating the history of aqueous activity and the accessibility of near-surface water. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Geophys Survey Syst Inc, N Salem, NH 03073 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, 4th St & Independence Ave SW, Washington, DC 20560 USA. NR 69 TC 18 Z9 19 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 FEB 8 PY 2003 VL 108 IS E4 AR 8024 DI 10.1029/2002JE001856 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 661NQ UT WOS:000181897000001 ER PT J AU Balakrishnan, N Dalgarno, A AF Balakrishnan, N Dalgarno, A TI Nitric oxide production in collisions of hot O(P-3) atoms with N-2 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE hot oxygen; nitric oxide; thermosphere; shuttle glow; nonthermal distributions; vibrational excitation ID OXYGEN GEOCORONA; CROSS-SECTIONS; RATE CONSTANTS; KINETIC-MODEL; SURFACES; (3)A''; MARS AB [1] Energetic oxygen atoms play a central role in the heat and energy balance of the terrestrial thermosphere. The reaction between hot O(P-3) atoms and N-2 has been suggested as a source of shuttle glow in low-Earth orbits due to the formation of nitric oxide. We report cross sections and rate coefficients for the production of nitric oxide in the reaction between hot O(P-3) atoms and N-2 and show that vibrational excitation of N-2 significantly enhances the reaction rate coefficients. Results are found to be in agreement with shock-tube experiments as well as with crossed molecular beam data. C1 Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Balakrishnan, N (reprint author), Univ Nevada, Dept Chem, 4505 Maryland Pkwy, Las Vegas, NV 89154 USA. NR 26 TC 5 Z9 5 U1 1 U2 4 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 FEB 7 PY 2003 VL 108 IS A2 AR 1065 DI 10.1029/2002JA009566 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 662DW UT WOS:000181932500004 ER PT J AU Campbell, BA Ghent, RR Shepard, MK AF Campbell, BA Ghent, RR Shepard, MK TI Limits on inference of Mars small-scale topography from MOLA data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ROUGHNESS AB [1] The surface roughness of Mars at scales from 1-200 m is of interest for lander hazard and radar-sounder clutter analysis, but MOLA data are the only current source of global topographic information. We use synthetic fractal profiles to determine the uncertainties associated with deriving self-affine statistics from detrended segments of MOLA tracks. The mean Hurst exponent derived from such segments is an underestimate of the true value, H, for H > 0.5, and an overestimate for H < 0.5. Values of H from independent samples along a profile are distributed about this biased mean value. The magnitudes of the bias and variance in H increase for shorter segments. Terrestrial topography data show that extrapolation of roughness statistics to smaller scales based on self-affine relationships is uncertain. Roughness at the 1-15 m scales may be poorly correlated with topography at >100-m scales. We suggest that any extrapolation be regarded as a lower bound on the true terrain statistics. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Bloomsburg Univ Penn, Bloomsburg, PA 17815 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20560 USA. NR 12 TC 9 Z9 9 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 6 PY 2003 VL 30 IS 3 AR 1115 DI 10.1029/2002GL016550 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 661JK UT WOS:000181887300006 ER PT J AU Elosegui, P Davis, JL Mitrovica, JX Bennett, RA Wernicke, BP AF Elosegui, P Davis, JL Mitrovica, JX Bennett, RA Wernicke, BP TI Crustal loading near Great Salt Lake, Utah SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SURFACE LOADS; DEFORMATION; EARTH AB [1] Two sites of the BARGEN GPS network are located 30 km south of Great Salt Lake (GSL). Lake-level records since mid-1996 indicate seasonal water elevation variations of 0.3 m amplitude superimposed on a roughly "decadal'' feature of amplitude similar to0.6 m. Using an elastic Green's function and a simplified load geometry for GSL, we calculate that these variations translate into radial crustal loading signals of +/-0.5 mm (seasonal) and +/-1 mm (decadal). The horizontal loading signals are a factor of similar to2 smaller. Despite the small size of the expected loading signals, we conclude that we can observe them using GPS time series for the coordinates of these two sites. The observed amplitudes of the variations agree with the predicted decadal variations to <0.5 mm. The observed annual variations, however, disagree; this difference may be caused by some combination of local precipitation-induced site motion, unmodeled loading from other nearby sources, errors in the GSL model, and atmospheric errors. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Elosegui, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 11 TC 17 Z9 17 U1 1 U2 3 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 FEB 5 PY 2003 VL 30 IS 3 AR 1111 DI 10.1029/2002GL016579 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 661JJ UT WOS:000181887200005 ER PT J AU Martin, RV Jacob, DJ Yantosca, RM Chin, M Ginoux, P AF Martin, RV Jacob, DJ Yantosca, RM Chin, M Ginoux, P TI Global and regional decreases in tropospheric oxidants from photochemical effects of aerosols SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosols; ozone; heterogeneous chemistry; radiation; reactive uptake; OH ID OPTICAL-THICKNESS; LIGHT-SCATTERING; INDIAN-OCEAN; MINERAL DUST; ATMOSPHERIC PARTICLES; MODEL DESCRIPTION; PHOTOLYSIS RATES; OZONE PRODUCTION; ATLANTIC-OCEAN; MIXING RATIOS AB [1] We evaluate the sensitivity of tropospheric OH, O-3, and O-3 precursors to photochemical effects of aerosols not usually included in global models: (1) aerosol scattering and absorption of ultraviolet radiation and (2) reactive uptake of HO2,NO2, and NO3. Our approach is to couple a global 3-D model of tropospheric chemistry (GEOS-CHEM) with aerosol fields from a global 3-D aerosol model (GOCART). Reactive uptake by aerosols is computed using reaction probabilities from a recent review (gamma(HO2) = 0.2, gamma(NO2) =10(-4), gamma(NO3) = 10(-3)). Aerosols decrease the O-3 --> O(D-1) photolysis frequency by 5-20% at the surface throughout the Northern Hemisphere (largely due to mineral dust) and by a factor of 2 in biomass burning regions (largely due to black carbon). Aerosol uptake of HO2 accounts for 10-40% of total HOx radical (= OH + peroxy) loss in the boundary layer over polluted continental regions (largely due to sulfate and organic carbon) and for more than 70% over tropical biomass burning regions (largely due to organic carbon). Uptake of NO2 and NO3 accounts for 10-20% of total HNO3 production over biomass burning regions and less elsewhere. Annual mean OH concentrations decrease by 9% globally and by 5-35% in the boundary layer over the Northern Hemisphere. Simulated CO increases by 5-15 ppbv in the remote Northern Hemisphere, improving agreement with observations. Simulated boundary layer O-3 decreases by 15-45 ppbv over India during the biomass burning season in March and by 5-9 ppbv over northern Europe in August, again improving comparison with observations. We find that particulate matter controls would increase surface O-3 over Europe and other industrial regions. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 50, Cambridge, MA 02138 USA. EM rvmartin@fas.harvard.edu; djj@io.harvard.edu; bmy@io.harvard.edu; chin@rondo.gsfc.nasa.gov; ginoux@rondo.gsfc.nasa.gov RI Martin, Randall/A-2051-2008; Ginoux, Paul/C-2326-2008; Chin, Mian/J-8354-2012; Martin, Randall/C-1205-2014; Yantosca, Robert/F-7920-2014; Chem, GEOS/C-5595-2014 OI Ginoux, Paul/0000-0003-3642-2988; Martin, Randall/0000-0003-2632-8402; Yantosca, Robert/0000-0003-3781-1870; NR 84 TC 274 Z9 282 U1 10 U2 66 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 5 PY 2003 VL 108 IS D3 AR 4097 DI 10.1029/2002JD002622 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 661KE UT WOS:000181889100006 ER PT J AU Goodyear, FH AF Goodyear, FH TI Traveling the Pennsylvania Railroad: The photographs of William H. Rea SO AMERICAN STUDIES INTERNATIONAL LA English DT Book Review C1 Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. RP Goodyear, FH (reprint author), Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU GEORGE WASHINGTON UNIV PI WASHINGTON PA AMERICAN STUDIES PROGRAM, WASHINGTON, DC 20052 USA SN 0883-105X J9 AM STUD INT JI Am. Stud. Int. PD FEB PY 2003 VL 41 IS 1-2 BP 235 EP 236 PG 2 WC History SC History GA 659KW UT WOS:000181776700016 ER PT J AU Zotz, G Mikona, C AF Zotz, G Mikona, C TI Photosynthetic induction and leaf carbon gain in the tropical understorey epiphyte, Aspasia principissa SO ANNALS OF BOTANY LA English DT Article DE Aspasia principissa; Barro Colorado Island; epiphytes; induction; leaf carbon balance; light flecks.; Orchidaceae; photosynthesis ID ADENOCAULON-BICOLOR ASTERACEAE; RAIN-FOREST; DYNAMIC LIGHT; FLUCTUATING LIGHT; GAS-EXCHANGE; RESPONSES; MODEL; ENVIRONMENTS; LIGHTFLECKS; EFFICIENCY AB Gas exchange of the understorey epiphyte Aspasia principissa was studied in fluctuating light conditions both in the laboratory and in the field, testing the hypothesis that vascular epiphytes differ from most terrestrial understorey plants in showing a higher priority for water conservation. Consequently, a slow response of stomatal conductance to sudden increases in incident photon flux density (PFD) was expected, as wits a fast loss of induction after such a light fleck. Results were only partly consistent with these expectations. Full induction of photosynthesis was indeed very slow and was not reached before, respectively, 40 and 60 min of saturating PFD in the field and the laboratory. In contrast, kinetics of induction loss were comparable with those of most terrestrial species studied to date. The overall impact of light flecks on in situ carbon gain again fulfilled expectations, being rather limited: the observed carbon gain was only approx. 66% of the potential carbon gain estimated from a square-wave response model. It is concluded that in the drought-prone epiphytic habitat of a moist lowland forest, water conservation takes priority over carbon gain, which severely limits the use of light flecks for CO2 fixation in vascular epiphytes. (C) 2003 Annals of Botany Company. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. Univ Wurzburg, Lehrstuhl Bot 2, D-97082 Wurzburg, Germany. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM gerhard.zotz@unibas.ch NR 32 TC 2 Z9 3 U1 1 U2 12 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD FEB PY 2003 VL 91 IS 3 BP 353 EP 359 DI 10.1093/aob/mcg021 PG 7 WC Plant Sciences SC Plant Sciences GA 644JE UT WOS:000180913500006 PM 12547688 ER PT J AU Jarrett, TH Chester, T Cutri, R Schneider, SE Huchra, JP AF Jarrett, TH Chester, T Cutri, R Schneider, SE Huchra, JP TI The 2MASS Large Galaxy Atlas SO ASTRONOMICAL JOURNAL LA English DT Article DE atlases; galaxies : fundamental parameters; galaxies : photometry; galaxies : statistics; globular clusters : general; infrared radiation; surveys ID DUST-PENETRATED CLASSIFICATION; SPIRAL GALAXIES; STAR-FORMATION; INTERSTELLAR-MEDIUM; BARRED GALAXIES; MIDINFRARED EMISSION; BRIGHT GALAXIES; MOLECULAR GAS; M51; ARMS AB We present the largest galaxies as seen in the near-infrared (1-2 mum), imaged with the Two Micron All Sky Survey (2MASS), ranging in angular size from 1' to 1.degrees5. We highlight the 100 largest in the sample. The galaxies span all Hubble morphological types, including elliptical galaxies, normal and barred spirals, and dwarf and peculiar classes. The 2MASS Large Galaxy Atlas provides the necessary sensitivity and angular resolution to examine in detail morphologies in the near-infrared, which may be radically different from those in the optical. Internal structures such as spirals, bulges, warps, rings, bars, and star formation regions are resolved by 2MASS. In addition to large mosaic images, the atlas includes astrometric, photometric, and shape global measurements for each galaxy. A comparison of fundamental measures ( e. g., surface brightness, Hubble type) is carried out for the sample and compared with the Third Reference Catalogue. We further showcase NGC 253 and M51 ( NGC 5194/5195) to demonstrate the quality and depth of the data. The atlas represents the first uniform, all-sky, dust-penetrated view of galaxies of every type, as seen in the near-infrared wavelength window that is most sensitive to the dominant mass component of galaxies. The images and catalogs are available through the NASA/IPAC Extragalactic Database and Infrared Science Archive and are part of the 2MASS Extended Source Catalog. C1 CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP CALTECH, Ctr Infrared Proc & Anal, 100-22,770 S Wilson Ave, Pasadena, CA 91125 USA. EM jarrett@ipac.caltech.edu; tchester@ipac.caltech.edu; roc@ipac.caltech.edu; schneider@astro.umass.edu; huchra@cfa.harvard.edu NR 66 TC 614 Z9 621 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2003 VL 125 IS 2 BP 525 EP 554 DI 10.1086/345794 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NL UT WOS:000180635900011 ER PT J AU Howland, R Sarajedini, A Tiede, GP Gokas, T Djagalov, R Martins, DH AF Howland, R Sarajedini, A Tiede, GP Gokas, T Djagalov, R Martins, DH TI CCD photometry of the Galactic globular cluster NGC 6235 SO ASTRONOMICAL JOURNAL LA English DT Article DE color-magnitude diagrams; globular clusters : individual (NGC 6235); stars : abundances; stars : horizontal-branch ID ASYMPTOTIC BRANCHES; GALAXY; STARS; METALLICITIES; CATALOG; SYSTEM; GIANT; MAPS; DUST AB We present the first detailed CCD photometric study of the Galactic globular cluster NGC 6235. Our BV color-magnitude diagram extends from above the tip of the first-ascent red giant branch (RGB) to 3 mag below the horizontal branch (HB). Based on an examination of the predominantly blue HB, we conclude that there is significant differential reddening in the direction of NGC 6235. We correct the photometry for this effect. By comparing the mean location of the blue HB stars in NGC 6235 with those of other clusters of similar metallicity, we infer a mean RR Lyrae magnitude of V(RR) = 16.87 +/- 0.10. The shape and location of the RGB are used to establish a metal abundance of [Fe/H] = 1.18 +/- 0.09 on the Zinn & West scale, which translates to [Fe/H] = -0.99 +/- 0.07 by using the Carretta & Gratton scale. The mean reddening of NGC 6235, estimated using the metal abundance along with the apparent color of the RGB, is E(B-V) = 0.24 +/- 0.03. Lastly, we determine the distance of NGC 6235 to be in the range 15.47 less than or equal to (m-M)(0) less than or equal to 15.57, depending on the value we adopt for the absolute magnitude of the RR Lyrae stars. C1 Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA. Williams Coll, Williamstown, MA 01267 USA. Middlebury Coll, Middlebury, VT 05753 USA. Wesleyan Univ, Middletown, CT 06459 USA. RP Howland, R (reprint author), Buchholz High Sch, 5510 NW 27th Ave, Gainesville, FL 32606 USA. NR 29 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 FEB PY 2003 VL 125 IS 2 BP 801 EP 809 DI 10.1086/345730 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NL UT WOS:000180635900028 ER PT J AU Sandquist, EL Latham, DW Shetrone, MD Milone, AAE AF Sandquist, EL Latham, DW Shetrone, MD Milone, AAE TI The blue straggler RS Canum venaticorum star S1082 in M67: A detailed light curve and the possibility of a triple SO ASTRONOMICAL JOURNAL LA English DT Article DE blue stragglers; open clusters : individual (NGC 2682); stars : abundances ID OPEN CLUSTER M67; LINE-DEPTH RATIOS; OLD OPEN CLUSTERS; X-RAY-EMISSION; SPECTROSCOPIC BINARIES; RADIAL-VELOCITIES; ROTATIONAL AXES; CCD PHOTOMETRY; PROPER MOTIONS; CVN AB Using both photometric and spectroscopic data, we present a picture of the very unusual blue straggler S1082 in the old open cluster M67 whose light is the sum of a close binary (P = 1.0677978 days) and another cluster member. The primary of the close binary and the third star are both blue stragglers in their own rights. Using relative photometry with millimagnitude accuracy, we provide a complete V-band light curve for the system and show a number of unusual features: brightness variations at the 0.01-0.03 mag level from month to month at all phases, a narrow primary and broad secondary eclipse, brightness differences between phases 0.25 and 0. 75, and short duration (similar to1 hr) drops in brightness. Much of the light-curve variation appears to be because of spot activity on the cooler, fainter, nearly synchronized component of the close binary. We use spectra from several sources to constrain the temperatures of the three known components, the relative flux contributions, rotational velocities, and radial velocities. The data clearly show that the brightest star (narrow-line component) seen in the spectrum is on an orbit with period P = 1189 +/- 7 days and eccentricity e = 0.57 +/- 0.08, although we cannot prove that there is a dynamical link between it and the close binary. The systematic velocities of all of the stars indicate that they are members of the cluster. Our models of the system indicate that the cooler component of the close binary lies on the main sequence near the cluster turnoff, while the hotter component lies near an extension of the main sequence blueward of the turnoff, and thus qualifies as a blue straggler by itself. The reduction of the masses of the stars in the close binary compared with previous models indicates that it is possible that the more massive component of the close binary formed from a merger of just two turnoff-mass stars. C1 San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, McDonald Observ, Ft Davis, TX 79734 USA. MMT Observ, Amado, AZ 85645 USA. RP San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM erics@mintaka.sdsu.edu; dlatham@cfa.harvard.edu; shetrone@astro.as.utexas.edu; amilone@mmto.org NR 62 TC 41 Z9 42 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2003 VL 125 IS 2 BP 810 EP 824 DI 10.1086/346087 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NL UT WOS:000180635900029 ER PT J AU Torres, G Guenther, EW Marschall, LA Neuhauser, R Latham, DW Stefanik, RP AF Torres, G Guenther, EW Marschall, LA Neuhauser, R Latham, DW Stefanik, RP TI Radial velocity survey of members and candidate members of the TW Hydrae association SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; open clusters and associations : individual (TW Hydrae); stars : kinematics; stars : pre-main-sequence ID ETA-CHAMAELEONTIS CLUSTER; BROWN DWARF COMPANION; TAURI STARS; X-RAY; SPECTROSCOPIC BINARIES; SOURCE CATALOG; PROPER MOTION; EMISSION; HD-98800; SPECTRUM AB We report spectroscopic observations of stars belonging to the young nearby group known as the TW Hydrae association, as well as of a number of potential members of the association identified in kinematic and X-ray surveys. Multiple radial velocity measurements were obtained for each object, several of which turn out to be multiple systems. Orbital solutions are presented for three double-lined binaries, one single-lined binary, and a double-lined triple system, all with short periods. Effective temperatures and projected rotational velocities are presented for each visible object. None of the candidate members of the association in our sample are confirmed as a true member. The large fraction of close binaries among the candidate members has to do with their selection based on X-ray emission from ROSAT, which tends to favor the inclusion of tidally locked systems that are active but not necessarily young. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Karl Schwarzschild Observ, Thuringer Landesternwarte Tautenburg, D-07778 Tautenburg, Germany. Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 70 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 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2003 VL 125 IS 2 BP 825 EP 841 DI 10.1086/345968 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NL UT WOS:000180635900030 ER PT J AU Mermilliod, JC Latham, DW Glushkova, EV Ibrahimov, MA Batirshinova, VM Stefanik, RP James, DJ AF Mermilliod, JC Latham, DW Glushkova, EV Ibrahimov, MA Batirshinova, VM Stefanik, RP James, DJ TI Red giants in open clusters - X. NGC 1817 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE open clusters and associations : individual : NGC 1817; stars : binaries : spectroscopic; techniques : radial velocities; stars : AGB and post-AGB ID OLD OPEN CLUSTERS; STELLAR EVOLUTION; SPECTROSCOPIC BINARIES; RADIAL-VELOCITIES AB Radial-velocity and BV CCD observations of 29 red-giant candidates in the central part of the intermediate-age open cluster NGC 1817 have confirmed the membership of 21 stars. In addition, we have used radial velocities and new UBVR photoelectric photometry to investigate the membership of 59 new candidates located in an outer corona surrounding NGC 1817, identified from the POSS plates. We have confirmed 18 new members out to a distance of 27' from the centre, thus doubling the previous cluster radius. Ten definite spectroscopic-binary members have been discovered, corresponding to a binary frequency of 25.6% and four orbits have been determined so far. Three additional stars have been identified as possible spectroscopic-binary members. We derive a cluster mean velocity of +65.33 +/- 0.09 (0.52 s.e.) km s(-1) based on 29 members with no detected velocity variations plus the 3 binary members with orbital solutions. The radial distribution of the 39 red-giant members shows a strong concentration of spectroscopic binaries in the inner part of the cluster, similar to that observed in M 67, although NGC 1817 is much younger. C1 Univ Lausanne, Inst Astron, CH-1290 Chavannes Des Bois, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119899, Russia. Ukbek Acad Sci, Ulugh Beg Astron Inst, Tashkent 700052, Uzbekistan. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Mermilliod, JC (reprint author), Univ Lausanne, Inst Astron, CH-1290 Chavannes Des Bois, Switzerland. EM Jean-Claude.Mermilliod@obs.unige.ch NR 25 TC 13 Z9 13 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2003 VL 399 IS 1 BP 105 EP 112 DI 10.1051/0004-6361:20021777 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 642VZ UT WOS:000180827300016 ER PT J AU Hameury, JM Barret, D Lasota, JP McClintock, JE Menou, K Motch, C Olive, JF Webb, N AF Hameury, JM Barret, D Lasota, JP McClintock, JE Menou, K Motch, C Olive, JF Webb, N TI XMM-Newton observations of two black hole X-ray transients in quiescence SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion; accretion discs; instabilities; black hole physics; X-ray : binaries; stars : individual : GRO J1655-40; stars : individual : GRS 1009-45 ID DISC INSTABILITY MODEL; LATE-TYPE STARS; GRO J1655-40; BINARY TRANSIENTS; NEUTRON-STAR; MASS; EMISSION; OUTBURST; NOVAE; NOVA-MUSCAE-1991 AB We report on XMM-Newton observations of GRO J1655-40 and GRS 1009-45, which are two black hole X-ray transients currently in their quiescent phase. GRO J1655-40 was detected with a 0.5-10 keV luminosity of 5.9 x 10(31) erg s(-1) with 20% accuracy, taking into account both statistical errors and uncertainty on the distance. This luminosity is comparable to a previous Chandra measurement, but ten times lower than the 1996 ASCA value, most likely obtained when the source was not yet in a true quiescent state. Unfortunately, XMM-Newton failed to detect GRS 1009-45. A stringent upper limit of 8.9 x 10(30) erg s(-1) was derived by combining data from the EPIC-MOS and PN cameras. The X-ray spectrum of GRO J1655-40 is very hard as it can be fitted with a power law model of photon index similar to1.3 x 0.4. Similarly hard spectra have been observed from other systems; these rule out coronal emission from the secondary or disk flares as the origin of the observed X-rays. On the other hand, our observations are consistent with the predictions of the disc instability model in the case that the accretion flow forms an advection dominated accretion flow (ADAF) at distances less than a fraction (similar to0.1-0.3) of the circularization radius. This distance corresponds to the greatest extent of the ADAF that is thought to be possible. C1 Observ Strasbourg, CNRS, UMR 7550, F-67000 Strasbourg, France. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22937 USA. RP Hameury, JM (reprint author), Observ Strasbourg, CNRS, UMR 7550, 11 Rue Univ, F-67000 Strasbourg, France. OI Hameury, Jean-Marie/0000-0002-6412-0103 NR 66 TC 40 Z9 39 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 FEB PY 2003 VL 399 IS 2 BP 631 EP 637 DI 10.1051/0004-6361:20021746 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 643JW UT WOS:000180859000023 ER PT J AU Paltani, S Turler, M AF Paltani, S Turler, M TI Dynamics of the Ly alpha and C IV emitting gas in 3C 273 SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : profiles; quasars : emission lines; quasars : individual (3C 273); ultraviolet : galaxies ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; 3C 273; EMISSION-LINES; VARIABILITY; IUE; QUASARS; KINEMATICS; CONTINUUM; GALAXIES AB In this paper we study the variability properties of the Lyalpha and C IV emission lines in 3C 273 using archival International Ultraviolet Explorer observations. Our data show for the first time the existence of variability on timescales of several years. We study the spatial distribution and the velocity field of the emitting gas by performing detailed analyses on the line variability using correlations, one- and two-dimensional response functions, and principal component analysis. In both lines we find evidence for two components, one that has the dynamic properties of gas in Keplerian motion around a black hole with a mass on the order of 10(9) M., and one that is characterized by high, blueshifted velocities at large lag. There is no indication of the presence of optically thick emission medium in either the Lyalpha or C IV response functions. The component characterized by blueshifted velocities, which is comparatively much stronger in C IV than in Lyalpha, is more or less compatible with being the result of gas falling toward the central black hole with free-fall acceleration. We propose, however, that the line emission at high, blueshifted velocities is better explained in terms of entrainment of gas clouds by the jet. Therefore, this gas is probably collisionally excited as a result of heating due to the intense infrared radiation from the jet, which would explain the strength of this component in C IV relative to Lyalpha. This phenomenon might be a signature of disk-jet interaction. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Observ Geneva, CH-1290 Sauverny, Switzerland. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM spaltani@cfa.harvard.edu; marc.turler@obs.unige.ch NR 39 TC 11 Z9 11 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2003 VL 583 IS 2 BP 659 EP 669 DI 10.1086/345421 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300014 ER PT J AU Corbett, EA Kewley, L Appleton, PN Charmandaris, V Dopita, MA Heisler, CA Norris, RP Zezas, A Marston, A AF Corbett, EA Kewley, L Appleton, PN Charmandaris, V Dopita, MA Heisler, CA Norris, RP Zezas, A Marston, A TI COLA. II. Radio and spectroscopic diagnostics of nuclear activity in galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : starburst; infrared : galaxies; radio continuum : galaxies ID ULTRALUMINOUS INFRARED GALAXIES; SEYFERT 2 GALAXIES; STARBURST-AGN CONNECTION; LUMINOUS IRAS GALAXIES; POINT-SOURCE CATALOG; GALACTIC NUCLEI; OPTICAL SPECTROSCOPY; EMISSION; SPECTRA; COMPACT AB We present optical spectroscopic observations of 93 galaxies taken from the infrared-selected COLA (compact objects in low-power AGNs) sample. These are all galaxies for which we have previously obtained low-resolution radio observations and high-resolution (<0."05) Australian Long Baseline Array snapshots. The sample spans the range of far-IR luminosities from normal galaxies to luminous infrared galaxies and contains a significant number of galaxies involved in galaxy-galaxy interactions. Of the galaxies observed, 78 (84%) exhibit emission lines indicating that they are either AGNs or actively forming stars (starburst galaxies). Using a newly developed, theoretically based, optical emission line scheme to classify the spectra, we find that 15% of the emission-line galaxies are Seyfert galaxies, 77% are starbursts, and the rest are either borderline AGN/starburst or show ambiguous characteristics. We find little evidence for an increase in the fraction of AGNs in the sample as a function of far-IR ( FIR) luminosity, in contrast to previous studies, but our sample covers only a small range in infrared luminosity ( 10 10 : 5 L L FIR 10 11 : 7 L), and thus a weak trend may be masked. Instead, as the infrared luminosity increases, so does the fraction of metal-rich starbursts, objects that on more traditional diagnostic diagrams would have been classified as weak, low-ionization, narrow emission line regions. As a whole the Seyfert galaxies exhibit a small, but statistically significant, radio excess on the radio-FIR correlation compared to the galaxies classified as starbursts. Compact (<0."05) radio cores are detected in 55% of the Seyfert galaxies, and these galaxies exhibit a significantly larger radio excess than the Seyfert galaxies in which compact cores were not detected. Our results indicate that there may be two distinct populations of Seyfert galaxies, "radio-excess" Seyfert galaxies, which exhibit extended radio structures and compact radio cores, and "radio-quiet" Seyfert galaxies, in which the majority of the radio emission can be attributed to star formation in the host galaxy. No significant difference is seen between the IR and optical spectroscopic properties of Seyfert galaxies with and without radio cores. C1 Anglo Australian Observ, Epping, NSW 1710, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. LERMA, Observ Paris, F-75014 Paris, France. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Anglo Australian Observ, POB 296, Epping, NSW 1710, Australia. RI Charmandaris, Vassilis/A-7196-2008; Norris, Ray/A-1316-2008; Dopita, Michael/P-5413-2014; Zezas, Andreas/C-7543-2011; OI Charmandaris, Vassilis/0000-0002-2688-1956; Norris, Ray/0000-0002-4597-1906; Dopita, Michael/0000-0003-0922-4986; Zezas, Andreas/0000-0001-8952-676X; Appleton, Philip/0000-0002-7607-8766 NR 73 TC 31 Z9 31 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2003 VL 583 IS 2 BP 670 EP 688 DI 10.1086/345414 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300015 ER PT J AU Dopita, MA Groves, BA Sutherland, RS Kewley, LJ AF Dopita, MA Groves, BA Sutherland, RS Kewley, LJ TI Internal dust correction factors for star formation rates derived for dusty H II regions and starburst galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : starburst; HII regions; stars : formation ID DIFFUSE INTERSTELLAR-MEDIUM; LYMAN CONTINUUM EXTINCTION; ALPHA LUMINOSITY FUNCTION; SOLAR GRANULATION; EMITTING GALAXIES; LINE FORMATION; PHOTODESTRUCTION; SELECTION; SEQUENCE; FIELD AB Star formation rates in galaxies are frequently estimated using the Balmer line fluxes of their H II regions. However, these can be systematically underestimated because dust competes for the absorption of Lyman continuum photons in the ionized gas. This factor cannot be neglected, and in this paper we present theoretical correction factors in a simple analytic form in order to allow observers to take this effect into account when estimating star formation rates from Balmer lines. These factors scale as the product of the ionization parameter, U and the nebular O/H abundance ratio, both of which can now be derived from the observation of bright nebular line ratios. The correction factors are only somewhat dependent upon the photoelectron production by grains, but are very sensitive to the presence of complex polycyclic aromatic hydrocarbon like carbonaceous molecules in the ionized gas, providing that these can survive in such an environment. C1 Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Australian Natl Univ, Res Sch Astron & Astrophys, Private Bag,Western Creek Post Off, Weston, ACT 2611, Australia. RI Dopita, Michael/P-5413-2014 OI Dopita, Michael/0000-0003-0922-4986 NR 41 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2003 VL 583 IS 2 BP 727 EP 731 DI 10.1086/345448 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300020 ER PT J AU La Parola, V Damiani, F Fabbiano, G Peres, G AF La Parola, V Damiani, F Fabbiano, G Peres, G TI Spectral variability of the nucleus of M33 in a Chandra/ACIS observation SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M33); galaxies : nuclei; X-rays : individual (M33 X-8) ID X-RAY SOURCES; BLACK-HOLE; GALAXY; M-33; X-8 AB We have analyzed a 90 ks long observation of the bright nucleus of M33 made with Chandra/ACIS. We detected low-amplitude (similar to10%) highly significant variability on timescales of similar to5000 s. We also found associated spectral variability. The two main spectral components [a power law with Gamma similar to 2 and a multicolor disk (MCD) with kT similar to 0.9-1.2 keV] vary in relative flux. The MCD temperature also increases with increasing MCD flux. The pattern of variability is reminiscent of (but not identical to) Galactic black hole binaries. An greater than or equal to 5 M. accreting black hole may explain this source. C1 Osservatorio Astron Palermo GS Vaiana, Ist Nazl Astrofis, I-90134 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Palermo, Dipartimento Sci Fisiche & Astron, Sez Astron, I-90134 Palermo, Italy. RP La Parola, V (reprint author), Osservatorio Astron Palermo GS Vaiana, Ist Nazl Astrofis, Piazza Parlamento 1, I-90134 Palermo, Italy. OI PERES, Giovanni/0000-0002-6033-8180; La Parola, Valentina/0000-0002-8087-6488; Damiani, Francesco/0000-0002-7065-3061 NR 16 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 FEB 1 PY 2003 VL 583 IS 2 BP 758 EP 764 DI 10.1086/345505 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300023 ER PT J AU Moscadelli, L Menten, KM Walmsley, CM Reid, MJ AF Moscadelli, L Menten, KM Walmsley, CM Reid, MJ TI A high spectral resolution VLBI study of the 12 GHz methanol masers in W3(OH): Their submilliarcsecond structure and clues on saturation SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (W3); ISM : molecules; masers; radio lines : ISM; stars : formation ID STAR-FORMING REGIONS; EMISSION; DISKS AB This paper reports on the results of high velocity resolution (0.02 km s(-1)) VLBA observations of the 12 GHz methanol masers toward the ultracompact (UC) H II region W3(OH). About 50 maser features are detected, and their emission is resolved both in velocity and in space (with an angular resolution of approximate to1 mas). The maser feature spectra are very well reproduced by single Gaussian profiles, and a narrow distribution for the FWHM line widths is found from 0.14 to 0.32 km s(-1). The measured brightness temperatures distribute over the range 10(10) to 2 x 10(12) K. By performing elliptical Gaussian fits, the spot parameters ( peak position, intensity, and FWHM sizes) in the high velocity resolution maps were derived. The highest brightness temperatures occur in correspondence with the smallest spots, with FWHM size less than or equal to4 AU. For all the maser features, it is found that the channel peak positions vary smoothly with the velocity, delineating straight or arclike distributions projected onto the sky. In most cases, the channel (line-of-sight) velocities vary linearly with the peak positional shifts, with measured gradients in the range 0.05-0.65 km s(-1) mas(-1) (0.02-0.30 km s(-1) AU(-1)). Most of the maser spot spectra have very small deviations from a Gaussian profile, less than or equal to2 x 10(-3), and a trend for decreasing deviations with increasing intensities is noted. In most cases, the kurtosis of the spectral profiles is positive, with the most accurate values concentrated in the range 0.1-0.5. Comparison of these results with recent calculations of the deviations from a Gaussian pro le that occur across the line pro le of a linear maser ( as a result of the amplification process) suggests that the 12 GHz CH3OH masers are below the threshold, I-0, at which line rebroadening occurs. However, the model predicts deviations from a Gaussian pro le significantly smaller than the observed values, and this discrepancy needs to be investigated. In particular, the calculations of the deviations from a Gaussian pro le should take into account the effects of a velocity gradient through the maser features ( evidenced by our observations) that will influence the spectral pro le. The maximum output given by the pump rate of saturated masers may account for the observational result that the highest intensities are found in correspondence with the smallest sky-projected spot areas. C1 Osservatorio Astrofis Cagliari, I-09012 Capoterra, CA, Italy. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moscadelli, L (reprint author), Osservatorio Astrofis Cagliari, Loc Poggio Pini,Str 54, I-09012 Capoterra, CA, Italy. OI Moscadelli, Luca/0000-0002-8517-8881 NR 21 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 FEB 1 PY 2003 VL 583 IS 2 BP 776 EP 788 DI 10.1086/345502 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300025 ER PT J AU Harvey, DWA Wilner, DJ Myers, PC Tafalla, M Mardones, D AF Harvey, DWA Wilner, DJ Myers, PC Tafalla, M Mardones, D TI Inner structure of protostellar collapse candidate B335 derived from millimeter-wave interferometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : globules; ISM : individual (B335); ISM : jets and outflows; radio continuum : ISM; stars : formation ID SMALL-SCALE STRUCTURE; YOUNG STELLAR OBJECTS; BOK GLOBULE B335; STAR-FORMATION; INITIAL CONDITIONS; CORES; KINEMATICS; EMISSION; DYNAMICS; ENVELOPE AB We present a study of the density structure of the protostellar collapse candidate B335 using continuum observations from the IRAM Plateau de Bure Interferometer made at wavelengths of 1.2 and 3.0 mm. We analyze these data, which probe spatial scales from 5000 to 500 AU, directly in the visibility domain by comparison with synthetic observations constructed from models that assume different physical conditions. This approach allows for much more stringent constraints to be derived from the data than from analysis of images. A single radial power law in density provides a good description of the data, with a best-fit power-law density index p = 1.65 +/- 0.05. Through simulations, we quantify the sensitivity of this result to various model uncertainties, including assumptions of temperature distribution, outer boundary, dust opacity spectral index, and an unresolved central component. The largest uncertainty comes from the unknown presence of a centralized point source. The maximal point source, with 1.2 mm flux of F = 12 +/- 7 mJy, reduces the power-law density index to p = 1.47 +/- 0.07. The remaining sources of systematic uncertainty, of which the most important is the radial dependence of the temperature distribution, likely contribute a total uncertainty at the level of deltap less than or similar to 0.2. Taking into account the uncertainties, we find strong evidence that the power-law index of the density distribution within 5000 AU is significantly less than the value at larger radii, close to 2.0, from previous studies of dust emission and extinction. Images made from the data show clear departures from spherical symmetry, with the globule being slightly extended perpendicular to the outflow axis. The inclusion of a crude model of the outflow as a hollow bipolar cone of constant opening angle improves the fit and leaves the resulting density power-law index unchanged. These results conform well to the generic paradigm of isolated, low-mass star formation, which predicts a power-law density index close to p = 1.5 for an inner region of gravitational free fall onto the protostar. However, the standard inside-out collapse model does not fit the data as successfully as a simple p = 1.5 power law, because of the relative shallowness of the predicted density pro le just within the infall radius. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Astron Nacl, E-28800 Alcala De Henares, Spain. Univ Chile, Dept Astron, Santiago, Chile. RP Harvey, DWA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Mardones, Diego/I-5719-2016 NR 36 TC 36 Z9 36 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 FEB 1 PY 2003 VL 583 IS 2 BP 809 EP 818 DI 10.1086/345415 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300027 ER PT J AU Hall, TA Bond, IH Bradbury, SM Buckley, JH Carson, MJ Carter-Lewis, DA Catanese, M Dunlea, S D'Vali, M Fegan, DJ Fegan, SJ Finley, JP Gaidos, JA Gillanders, GH Hillas, AM Horan, D Kertzman, M Kieda, D Kildea, J Knapp, J Krennrich, F Lang, MJ LeBohec, S Lessard, R Lloyd-Evans, J McKernan, B Moriarty, P Muller, D Ong, R Quinn, J Reynolds, PT Rose, HJ Sembroski, GH Swordy, SP Vassiliev, VV Weekes, TC AF Hall, TA Bond, IH Bradbury, SM Buckley, JH Carson, MJ Carter-Lewis, DA Catanese, M Dunlea, S D'Vali, M Fegan, DJ Fegan, SJ Finley, JP Gaidos, JA Gillanders, GH Hillas, AM Horan, D Kertzman, M Kieda, D Kildea, J Knapp, J Krennrich, F Lang, MJ LeBohec, S Lessard, R Lloyd-Evans, J McKernan, B Moriarty, P Muller, D Ong, R Quinn, J Reynolds, PT Rose, HJ Sembroski, GH Swordy, SP Vassiliev, VV Weekes, TC TI Search for TeV emissions from pulsars in binary systems SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations; pulsars : general ID GAMMA-RAY EMISSION; SOURCE 2CG 135+01; X-RAY; MILLISECOND PULSARS; EGRET CATALOG; CENTAURUS X-3; PSR 1957+20; RADIATION; LSI+61-DEGREES-303; ACCELERATION AB A survey of binary systems containing pulsars was conducted, with the intention of detecting Galactic sources of very high energy gamma-ray emission. Observations were carried out with the Whipple 10 m imaging atmospheric Cerenkov telescope. Standard analysis techniques were applied to these sources to search for steady, unpulsed emission. Periodic tests were also performed to search for emission correlated with both the orbital and spin phases, where appropriate. Analyses indicate that the binaries in this study do not emit detectable levels of very high energy photons within the sensitivity of our instrument. The flux upper limits presented here fail to seriously constrain emission models. C1 Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Natl Univ Ireland, Expt Phys Dept, Dublin 4, Ireland. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Natl Univ Ireland, Dept Phys, Galway, Ireland. DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90024 USA. Cork Inst Technol, Dept Phys, Cork, Ireland. RP Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. EM tahall@ualr.edu OI Carson, Michael/0000-0003-0400-7819; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 60 TC 18 Z9 18 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2003 VL 583 IS 2 BP 853 EP 860 DI 10.1086/345504 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300032 ER PT J AU Kallman, TR Angelini, L Boroson, B Cottam, J AF Kallman, TR Angelini, L Boroson, B Cottam, J TI Chandra and XMM observations of the accretion disk corona source 2S 0921-63 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (2S 0921 63); X-rays : binaries; X-rays : individual (2S 0921 63) ID X-RAY BINARIES; COMPTON HEATED WINDS; EMISSION-LINES; SPECTRA; PHOTOIONIZATION; IONS AB We analyze observations of the low-mass X-ray binary (LMXB) 2S 0921-63 obtained with the gratings and CCDs on Chandra and XMM. This object is a high-inclination system showing evidence for an accretion disk corona (ADC). Such a corona has the potential to constrain the properties of the heated accretion disk in this system and other LMXBs by extension. We find evidence for line emission that is generally consistent with that found by previous experiments, although we are able to detect more lines. For the first time in this source, we find that the iron K line has multiple components. We set limits on the line widths and velocity offsets, and we fit the spectra to photoionization models and discuss the implications for ADC models. For the first time in any ADC source we use these fits, together with density constraints based on the O VII line ratio, in order to constrain the flux in the medium-ionization region of the ADC. Under various assumptions about the source luminosity this constrains the location of the emitting region. These estimates, together with estimates for the emission measure, favor a scenario in which the intrinsic luminosity of the source is comparable to what we observe. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kallman, TR (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 665, Greenbelt, MD 20771 USA. NR 32 TC 24 Z9 25 U1 1 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 FEB 1 PY 2003 VL 583 IS 2 BP 861 EP 877 DI 10.1086/345475 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300033 ER PT J AU Lobel, A Dupree, AK Stefanik, RP Torres, G Israelian, G Morrison, N de Jager, C Nieuwenhuijzen, H Ilyin, I Musaev, F AF Lobel, A Dupree, AK Stefanik, RP Torres, G Israelian, G Morrison, N de Jager, C Nieuwenhuijzen, H Ilyin, I Musaev, F TI High-resolution spectroscopy of the yellow hypergiant rho Cassiopeiae from 1993 through the outburst of 2000-2001 SO ASTROPHYSICAL JOURNAL LA English DT Article DE instabilities; stars : atmospheres; stars : oscillations; stars : variables : other; stellar dynamics; supergiants ID MASS-LOSS; SUPERGIANT ATMOSPHERES; PLANETARY-NEBULA; ALPHA-ORIONIS; ETA-CARINAE; STARS; COOL; INSTABILITY; ENVIRONMENT; PHOTOMETRY AB We present an overview of the spectral variability of the peculiar F-type hypergiant rho Cas, obtained from our long-term monitoring campaigns over the past 8.5 yr with four spectrographs in the northern hemisphere. Between 2000 June and September an exceptional variability phase occurred when the V brightness dimmed by about a full magnitude. The star recovered from this deep minimum by 2001 April. It is the third outburst of rho Cas on record in the last century. We observe TiO absorption bands in high-resolution near-IR spectra obtained with the Utrecht Echelle Spectrograph during the summer of 2000. TiO formation in the outer atmosphere occurred before the deep brightness minimum. Atmospheric models reveal that the effective temperature decreases by at least 3000 K, and the TiO shell is driven supersonically with (M) over dot similar or equal to 5.4 x 10(-2) M. yr(-1). Strong episodic mass loss and TiO have also been observed during the outbursts of 1945-1947 and 1985-1986. A detailed analysis of the exceptional outburst spectra is provided, by comparing with high-resolution optical spectra of the early M-type supergiants mu Cep (Ia) and Betelgeuse (Iab). During the outburst, central emission appears above the local continuum level in the split Na D lines. A prominent optical emission line spectrum appears in variability phases of fast wind expansion. The radial velocity curves of Halpha and of photospheric metal absorption lines signal a very extended and velocity-stratified dynamic atmosphere. The outburst spectra indicate the formation of a low-temperature, optically thick circumstellar gas shell of 3 x 10(2) M. during 200 days, caused by dynamic instability of the upper atmosphere of this pulsating massive supergiant near the Eddington luminosity limit. We observe that the mass-loss rate during the outburst is of the same order of magnitude as has been proposed for the outbursts of eta Carinae. We present calculations that correctly predict the outburst timescale, whereby the shell ejection is driven by the release of hydrogen ionization recombination energy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Canary Isl, Spain. Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA. SRON, Space Res Lab, NL-3584 CA Utrecht, Netherlands. Univ Oulu, Dept Astron, Oulu 90014, Finland. Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia. RP Lobel, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 75 TC 47 Z9 47 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 FEB 1 PY 2003 VL 583 IS 2 BP 923 EP 954 DI 10.1086/345503 PN 1 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NP UT WOS:000180636300039 ER PT J AU Bersier, D McLeod, B Garnavich, PM Holman, MJ Grav, T Quinn, J Kaluzny, J Challis, PM Bower, RG Wilman, DJ Heyl, JS Holland, ST Hradecky, V Jha, S Stanek, KZ AF Bersier, D McLeod, B Garnavich, PM Holman, MJ Grav, T Quinn, J Kaluzny, J Challis, PM Bower, RG Wilman, DJ Heyl, JS Holland, ST Hradecky, V Jha, S Stanek, KZ TI The strongly polarized afterglow of GRB 020405 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; polarization ID GAMMA-RAY BURSTS; IMAGE SUBTRACTION; LIGHT CURVES; GRB-990510; RADIATION; TELESCOPE AB We report polarization measurements and photometry for the optical afterglow of the gamma-ray burst GRB 020405. We measured a highly significant 9.9% polarization (in V band) 1.3 days after the burst and argue that it is intrinsic to the GRB. The light-curve decay is well fitted by a t(-1.72) power law; we do not see any evidence for a break between 1.24 and 4.3 days after the burst. We discuss these measurements in the light of several models of GRB afterglows. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Bersier, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wilman, David/0000-0002-1822-4462 NR 37 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 FEB 1 PY 2003 VL 583 IS 2 BP L63 EP L66 DI 10.1086/368158 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NR UT WOS:000180636500004 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 Dynamical evidence for a black hole in GX 339-4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; stars : individual (V821 Arae); X-rays : binaries ID SPECTROSCOPY; GX-339-4; EMISSION; GX339-4 AB We present outburst spectroscopy of GX 339-4 that may reveal the motion of its elusive companion star. N III lines exhibit sharp emission components moving over similar to300 km s(-1) in a single night. The most plausible interpretation of these components is that they are formed by irradiation of the companion star and the velocities indicate its orbital motion. We also detect motion of the wings of the He II 4686 Angstrom line and changes in its morphology. No previously proposed period is consistent with periodic behavior of all of these measures. However, consistent and sensible solutions are obtained for periods around 1.7 days. For the best period, 1.7557 days, we estimate a mass function of 5.8 +/-0.5 M.. Even allowing for aliases, the 95% confidence lower limit on the mass function is 2.0 M.. GX 339-4 can therefore be added to the list of dynamical black hole candidates. This is supported by the small motion in the wings of the He II line; if the compact object velocity is not larger than the observed motion, then the mass ratio is q less than or similar to 0.08, similar to other systems harboring black holes. Finally, we note that the sharp components are not always present but do seem to occur within a repeating phase range. This appears to migrate between our epochs of observation and may indicate shielding of the companion star by a variable accretion geometry such as a warp. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, Tenerife 38200, Spain. European So Observ, Santiago 19, Chile. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Hynes, RI (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 13 TC 145 Z9 146 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 FEB 1 PY 2003 VL 583 IS 2 BP L95 EP L98 DI 10.1086/368108 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NR UT WOS:000180636500012 ER PT J AU Miller, JM Wijnands, R Mendez, M Kendziorra, E Tiengo, A van der Klis, M Chakrabarty, D Gaensler, BM Lewin, WHG AF Miller, JM Wijnands, R Mendez, M Kendziorra, E Tiengo, A van der Klis, M Chakrabarty, D Gaensler, BM Lewin, WHG TI XMM-Newton spectroscopy of the accretion-driven millisecond X-ray pulsar XTE J1751-305 in outburst SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; pulsars : general; pulsars : individual (XTE J1751-305); stars : neutron; white dwarfs; X-rays : binaries ID CROSS-SECTIONS; DISCOVERY; BINARIES; ASCA AB We present an analysis of the first high-resolution spectra measured from an accretion-driven millisecond X-ray pulsar in outburst. We observed XTE J1751-305 with XMM-Newton on 2002 April 7 for approximately 35 ks. Using a simple absorbed blackbody plus power-law model, we measure an unabsorbed flux of (6.6 +/- 0.1) x 10(-10) ergs cm(-2) s(-1) (0.5-10.0 keV). A hard power-law component (Gamma = 1.44 +/- 0.01) contributes 83% of the unabsorbed flux in the 0.5-10.0 keV band, but a blackbody component (kT = 1.05 +/- 0.01 keV) is required. We find no clear evidence for narrow or broad emission or absorption lines in the time-averaged spectra, and the sensitivity of this observation has allowed us to set constraining upper limits on the strength of important features. The lack of line features is at odds with spectra measured from some other X-ray binaries that share some similarities with XTE J1751-305. We discuss the implications of these findings on the accretion flow geometry in XTE J1751-305. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Natl Inst Space Res, Space Res Org Netherlands, NL-3584 CA Utrecht, Netherlands. Univ Tubingen, Inst Astron & Astrophys, Abt Astron, D-72076 Tubingen, Germany. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Miller, JM (reprint author), MIT, Ctr Space Res, 70 Vassar St, Cambridge, MA 02139 USA. RI Gaensler, Bryan/F-8655-2010; Mendez, Mariano/C-8011-2012; OI Mendez, Mariano/0000-0003-2187-2708; Tiengo, Andrea/0000-0002-6038-1090; Gaensler, Bryan/0000-0002-3382-9558 NR 32 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2003 VL 583 IS 2 BP L99 EP L102 DI 10.1086/368105 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639NR UT WOS:000180636500013 ER PT J AU McCarthy, MC Cooksy, AL Mohamed, S Gordon, VD Thaddeus, P AF McCarthy, MC Cooksy, AL Mohamed, S Gordon, VD Thaddeus, P TI Rotational spectra of the nitrogen-sulfur carbon chains NCnS, n=1-7 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : molecules; line : identification; methods : laboratory; molecular data; molecular processes; radio lines : ISM ID TRANSFORM MICROWAVE SPECTROSCOPY; ASTRONOMICAL IDENTIFICATION; LABORATORY DETECTION; FREE-RADICALS; AB-INITIO; GAS-PHASE; MOLECULES; NCS; PARAMETERS; INTENSE AB Seven carbon chain radicals NCnS where n=1-7 have been detected in a supersonic molecular beam by Fourier transform microwave spectroscopy. Although NCCS is found to have a bent structure and an asymmetric top spectrum, the five longer chains have linear heavy-atom backbones, and like the isovalent HCnS chains, the electronic ground states of each alternate with even and odd numbers of carbon atoms: NC4S and NC6S have (2)Pi(1/2) ground states, while NC3S, NC5S, and NC7S have (2)Pi(3/2) ground states. In addition, the lowest-rotational transitions of the NCS radical have been detected in both fine-structure levels in the same supersonic molecular beam source, allowing a precise determination of the ground state hyperfine coupling constants. The centimeter-wave spectra of NC3S and the four longer chains have been fully characterized, and spectroscopic constants, including those that describe the lambda-type doubling and hyperfine structure from the nitrogen nucleus, have been determined to high precision. A complete account of the centimeter-wave spectrum of NCCS will be given by Nakajima et al. Predicted properties from UQCISD/cc-pVDZ ab initio calculations are also reported for the NCnS chains up to NC7S. All six new chains are highly polar and all are plausible candidates for astronomical detection because CnS chains up to C3S and CnN chains up to C5N are detected in both interstellar and circumstellar sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. San Diego State Univ, Dept Chem, San Diego, CA 92182 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 40 TC 24 Z9 24 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 FEB PY 2003 VL 144 IS 2 BP 287 EP 297 DI 10.1086/344727 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 636ME UT WOS:000180459200006 ER PT J AU Wcislo, WT Schatz, B AF Wcislo, WT Schatz, B TI Predator recognition and evasive behavior by sweat bees, Lasioglossum umbripenne (Hymenoptera : Halictidae), in response to predation by ants, Ectatomma ruidum (Hymenoptera : Formicidae) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE behavioral flexibility; anti-predator behavior; pattern recognition; predator-prey relationships ID PONERINE ANT; LATITUDINAL GRADIENT; ROGER FORMICIDAE; CHEMICAL CUES; SELFISH HERD; SOLITARY BEE; DIGGER WASP; DEFENSE; PREY; SOCIALITY AB Ectatomma ruidum is an abundant soil-nesting Neotropical ant, which displays extensive behavioral flexibility during foraging activities. We studied here one unusual element of their behavioral repertoire: ambush predation. A worker of E. ruidum waits near a nest of a social sweat bee, Lasioglossum umbripenne, lunging at incoming bees, or less frequently, at departing bees. However, bees detected ambushing ants and modified their behavior. Dead ants placed at bees' nest entrances significantly decreased bee activity, indicating that bees recognized dead ants as potential predators. Neither simple black models (square and rectangle) nor olfactory cues had any effect on overall bee activity. A returning bee usually approached her entrance and immediately entered, but if an ant was waiting at the nest, a bee was significantly more likely to abort the first approach flight and then to re-approach the nest on the side opposite the ant's position. As models became increasingly ant-like, returning bees more frequently aborted their first approach flight, expressing other behaviors before entering nests. These behaviors included withdrawal followed by an approach from a different direction; zigzagging flights, either from a distance or close to the entrance or even a close inspection; landing a short distance from the nest, then approaching on foot or waiting for several seconds before entering. Ants responded with effective counter-behaviors. Behavioral flexibility in nest entering/exiting by L. umbripenne and in hunting strategy by E. ruidum shows the complexity of this predator-prey relationship, and illustrates the importance of information processing by both species involved in determining the outcome of the interspecific interaction. C1 CNRS, UPR 9056, CEFE, F-34293 Montpellier, France. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Schatz, B (reprint author), CNRS, UPR 9056, CEFE, 1919 Route Mende, F-34293 Montpellier, France. EM bertrand.schatz@cefe.cnrs-mop.fr NR 52 TC 9 Z9 10 U1 0 U2 17 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 EI 1432-0762 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD FEB PY 2003 VL 53 IS 3 BP 182 EP 189 DI 10.1007/s00265-002-0564-1 PG 8 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 655KC UT WOS:000181550000006 ER PT J AU Feller, IC McKee, KL Whigham, DF O'Neill, JP AF Feller, IC McKee, KL Whigham, DF O'Neill, JP TI Nitrogen vs. phosphorus limitation across an ecotonal gradient in a mangrove forest SO BIOGEOCHEMISTRY LA English DT Review DE decomposition; mangrove ecosystem; N and P fertilization experiment; nutrient availability and cycling; nutrient limitation; nutrient resorption efficiency ID NUTRIENT-USE EFFICIENCY; SPARTINA-ALTERNIFLORA LOISEL; LEAF-LITTER DECOMPOSITION; ABOVE-GROUND PRODUCTION; RHIZOPHORA-MANGLE L; RED MANGROVE; SALT-MARSH; METROSIDEROS-POLYMORPHA; SULFIDE CONCENTRATION; SENESCING LEAVES AB Mangrove forests are characterized by distinctive tree-height gradients that reflect complex spatial, within-stand differences in environmental factors, including nutrient dynamics, salinity, and tidal inundation, across narrow gradients. To determine patterns of nutrient limitation and the effects of nutrient availability on plant growth and within-stand nutrient dynamics, we used a factorial experiment with three nutrient treatment levels (control, N, P) and three zones along a tree-height gradient (fringe, transition, dwarf) on offshore islands in Belize. Transects were laid out perpendicular to the shoreline across a mangrove forest from a fringe stand along the seaward edge, through a stand of intermediate height, into a dwarf stand in the interior of the island. At three sites, three trees were fertilized per zone for 2 yr. Although there was spatial variability in response, growth by R. mangle was generally nitrogen (N) -limited in the fringe zone; phosphorus (P) -limited in the dwarf zone; and, N- and/or P-limited in the transition zone. Phosphorus-resorption efficiency decreased in all three zones, and N- resorption efficiency increased in the dwarf zone in response to P enrichment. The addition of N had no effect on either P or N resorption efficiencies. Belowground decomposition was increased by P enrichment in all zones, whereas N enrichment had no effect. This study demonstrated that essential nutrients are not uniformly distributed within mangrove ecosystems; that soil fertility can switch from conditions of N to P limitation across narrow ecotonal gradients; and, that not all ecological processes respond similarly to, or are limited by, the same nutrient. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Louisiana State Univ, Wetland Biogeochem Inst, Baton Rouge, LA 70803 USA. RP Feller, IC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI McKee, Karen/D-1365-2014; OI McKee, Karen/0000-0001-7042-670X; Whigham, Dennis/0000-0003-1488-820X; Feller, Ilka/0000-0002-6391-1608 NR 133 TC 139 Z9 150 U1 4 U2 75 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD FEB PY 2003 VL 62 IS 2 BP 145 EP 175 DI 10.1023/A:1021166010892 PG 31 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 617LP UT WOS:000179363400002 ER PT J AU Donovan, JJ Hanchar, JM Picolli, PM Schrier, MD Boatner, LA Jarosewich, E AF Donovan, JJ Hanchar, JM Picolli, PM Schrier, MD Boatner, LA Jarosewich, E TI A re-examination of the rare-earth-element orthophosphate standards in use for electron-microprobe analysis SO CANADIAN MINERALOGIST LA English DT Article DE rare-earth elements; REE; rare-earth phosphates; orthophosphates; quantitative analysis; electron-probe micro-analysis; standards ID MONAZITE AB A re-examination of fourteen standards consisting of orthophosphates of the rare-earth elements, Sc and Y, grown at Oak Ridge National Laboratory in the 1980s and widely distributed by the Smithsonian Institution's Department of Mineral Sciences, reveals that some of the material is significantly contaminated by Pb. The origin of this impurity is the Pb2P2O7 flux that is derived from the thermal decomposition of PbHPO4. The lead pyrophosphate flux is used to dissolve the oxide starting materials at elevated temperatures (similar to1360degreesC) prior to crystal synthesis. Because these rare-earth-element standards are extremely stable under the electron beam and considered homogeneous, they have been of enormous value to the technique of electron-microprobe analysis (EMPA) whenever samples are to be analyzed for the rare-earth elements, Sc, Y, and P. The monoclinic orthophosphates (monazite structure) show a higher degree of Pb incorporation than the tetragonal orthophosphates (xenotime structure). We here describe the extent of the Ph contamination and explain the degree to which the stoichiometries have been affected by the replacement of REE by Pb within the crystal structure. C1 Univ Oregon, Dept Geol Sci, Eugene, OR 97403 USA. George Washington Univ, Dept Earth & Environm Sci, Washington, DC 20006 USA. Univ Maryland, Dept Geol, College Pk, MD 20742 USA. Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. Oak Ridge Natl Lab, Div Solid State, Oak Ridge, TN 37831 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Donovan, JJ (reprint author), Univ Oregon, Dept Geol Sci, Eugene, OR 97403 USA. OI Boatner, Lynn/0000-0002-0235-7594 NR 19 TC 40 Z9 43 U1 0 U2 5 PU MINERALOGICAL ASSOC CANADA PI OTTAWA PA PO BOX 78087, MERILINE POSTAL OUTLET, 1460 MERIVALE RD, OTTAWA, ONTARIO K2E 1B1, CANADA SN 0008-4476 J9 CAN MINERAL JI Can. Mineral. PD FEB PY 2003 VL 41 BP 221 EP 232 DI 10.2113/gscanmin.41.1.221 PN 1 PG 12 WC Mineralogy SC Mineralogy GA 663TT UT WOS:000182022500017 ER PT J AU Suarez, W Olson, SL AF Suarez, W Olson, SL TI New records of storks (Ciconiidae) from Quaternary asphalt deposits in Cuba SO CONDOR LA English DT Article DE Ciconia; Cuba; fossil birds; Mycteria; Quaternary; storks AB Storks were previously known in Cuba only from the living Wood Stork (Mycteria americana) and two bones of the extinct species Ciconia maltha from Cienfuegos Province. Newly explored Quaternary tar seep deposits in Matanzas Province have yielded fossils of M. americana, the extinct wood stork M. wetmorei, and an unidentified species of Ciconia smaller than C. maltha. These specimens provide the first verifiable fossil record of M. americana anywhere, the first of M. wetmorei outside of Florida and California, and the first instance of these two species occurring sympatrically. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. Museo Nacl Hist Nat, Havana 10100, Cuba. RP Suarez, W (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. NR 17 TC 6 Z9 7 U1 1 U2 3 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 FEB PY 2003 VL 105 IS 1 BP 150 EP 154 DI 10.1650/0010-5422(2003)105[150:NROSCF]2.0.CO;2 PG 5 WC Ornithology SC Zoology GA 648BP UT WOS:000181130200016 ER PT J AU Rappole, JH King, DI Rivera, JHV AF Rappole, JH King, DI Rivera, JHV TI Coffee and conservation SO CONSERVATION BIOLOGY LA English DT Editorial Material ID SHADE; BIRDS C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Massachusetts, US Forest Serv, NE Expt Stn, Holdsworth Nat Resources Ctr 203, Amherst, MA 01003 USA. Univ Nacl Autonoma Mexico, Inst Biol, Estac Biol Chamela, San Patrico 22630, Jalisco, Mexico. RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 19 TC 60 Z9 68 U1 0 U2 11 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2003 VL 17 IS 1 BP 334 EP 336 DI 10.1046/j.1523-1739.2003.01548.x PG 3 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 643DG UT WOS:000180846200040 ER PT J AU Lorenzetti, S Eugster, O Busemann, H Marti, K Burbine, TH McCoy, T AF Lorenzetti, S Eugster, O Busemann, H Marti, K Burbine, TH McCoy, T TI History and origin of aubrites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID RAY PRODUCTION-RATES; NOBLE-GASES; ENSTATITE METEORITES; TRACE-ELEMENTS; EXPOSURE AGES; CHONDRITES; ACHONDRITES; SOLAR; ABUNDANCES; DIOGENITES AB The cosmic ray exposure (CRE) ages of aubrites are among the longest of stone meteorites. New aubrites have been recovered in Antarctica, and these meteorites permit a substantial extension of the database on CRE ages, compositional characteristics, and regolith histories. We report He, Ne, and Ar isotopic abundances of nine aubrites and discuss the compositional data, the CRE ages, and regolith histories of this class of achondrites. A Ne three-isotope correlation reveals a solar-type ratio of Ne-20/Ne-22 = 12.1, which is distinct from the present solar wind composition and lower than most ratios observed on the lunar surface. For some aubrites, the cosmic ray-produced noble gas abundances include components produced on the surface of the parent object. The Kr isotopic systematics reveal significant neutron-capture-produced excesses in four aubrites, which is consistent with Sm and Gd isotopic anomalies previously documented in some aubrites. The nominal CRE ages confirm a non-uniform distribution of exposure times, but the evidence for a CRE age cluster appears doubtful. Six meteorites are regolith breccias with solar-type noble gases, and the observed neutron effects indicate a regolith history. ALH aubrites, which were recovered from the same location and are considered to represent a multiple fall, yield differing nominal CRE ages and, if paired, document distinct precompaction histories. Copyright (C) 2003 Elsevier Science Ltd. C1 Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. Univ Calif San Diego, La Jolla, CA 92093 USA. Smithsonian Inst, Dept Mineral Sci, MRC NHB119, Washington, DC 20560 USA. RP Lorenzetti, S (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. RI Lorenzetti, Silvio/B-1188-2009; OI Lorenzetti, Silvio/0000-0002-8339-8960; Busemann, Henner/0000-0002-0867-6908 NR 79 TC 32 Z9 32 U1 0 U2 7 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 FEB PY 2003 VL 67 IS 3 BP 557 EP 571 AR PII S0016-7037(02)01085-2 DI 10.1016/S0016-7037(02)01085-2 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 640MM UT WOS:000180692600016 ER PT J AU Libarkin, JC Chase, CG AF Libarkin, JC Chase, CG TI Timing of Colorado Plateau uplift: Initial constraints from vesicular basalt-derived paleoelevations: Comment SO GEOLOGY LA English DT Article ID LARAMIDE C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. RP Libarkin, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-71, Cambridge, MA 02140 USA. RI Libarkin, Julie/H-2316-2011 NR 4 TC 9 Z9 9 U1 0 U2 1 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD FEB PY 2003 VL 31 IS 2 BP 191 EP 192 DI 10.1130/0091-7613(2003)031<0191:TOCPUI>2.0.CO;2 PG 2 WC Geology SC Geology GA 644BQ UT WOS:000180898400024 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI Wernher von Braun and concentration camp labor - A reply SO GERMAN STUDIES REVIEW LA English DT Letter C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 3 PU ARIZ STATE UNIV PI TEMPE PA ARIZONA STATE UNIV, BOX 873204, TEMPE, AZ 85287-3204 USA SN 0149-7952 J9 GER STUD REV JI Ger. Stud. Rev. PD FEB PY 2003 VL 26 IS 1 BP 124 EP 126 PG 3 WC Area Studies; Humanities, Multidisciplinary SC Area Studies; Arts & Humanities - Other Topics GA 651ZJ UT WOS:000181353600009 ER PT J AU Arellano, C AF Arellano, C TI Habsburg Peru: Images, imagination and memory SO HISPANIC AMERICAN HISTORICAL REVIEW LA English DT Book Review RP Arellano, C (reprint author), Smithsonian Inst, Nat Museum Amer Indian Cultural Resources Ctr, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU DUKE UNIV PRESS PI DURHAM PA 905 W MAIN ST, STE 18-B, DURHAM, NC 27701 USA SN 0018-2168 J9 HISPANIC AM HIST REV JI Hisp. Am. Hist. Rev. PD FEB PY 2003 VL 83 IS 1 BP 178 EP 179 DI 10.1215/00182168-83-1-178 PG 2 WC History SC History GA 645FU UT WOS:000180966200023 ER PT J AU Stafford, BJ Thorington, RW Kawamichi, T AF Stafford, BJ Thorington, RW Kawamichi, T TI Positional behavior of Japanese giant flying squirrels (Petaurista leucogenys) SO JOURNAL OF MAMMALOGY LA English DT Article DE locomotion; musasabi; Petaurista; positional behavior; Pteromyinae ID LOCOMOTOR BEHAVIOR; MONKEYS; MECHANICS AB Positional behavior of Japanese giant flying squirrels (Petaurista leucogenys) was studied based on 3,318 positional bouts and 2,687 instantaneous samples. Resting, feeding and foraging, locomotion, and grooming were the most common behaviors. The most common locomotor behaviors were leaping, scrambling, walking, bounding, vertical bounding, and gliding. The most common postural behaviors were quadrupedal squatting, hind-limb squatting, vertical clinging, clinging, and crouching. Compared with smaller tree squirrels, Sciurus igniventris and Microsciurus flaviventer, P. leucogenys exhibited a higher frequency of "scrambling" for foraging among terminal branches. The tree squirrels foraged on terminals but fed on larger branches. They also foraged and fed more on vertical surfaces. P. leucogenys spent the most time on small supports, whereas the smallest squirrel (M. flaviventer) spent most on the largest supports. C1 Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Mammals, Washington, DC 20013 USA. Osaka City Univ, Dept Biol, Sumiyoshi Ku, Osaka 5588585, Japan. RP Stafford, BJ (reprint author), Howard Univ, Coll Med, Dept Anat, 520 W St NW, Washington, DC 20059 USA. EM stafford.brian@nmnh.si.edu NR 44 TC 16 Z9 16 U1 0 U2 10 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD FEB PY 2003 VL 84 IS 1 BP 263 EP 271 DI 10.1644/1545-1542(2003)084<0263:PBOJGF>2.0.CO;2 PG 9 WC Zoology SC Zoology GA 653BE UT WOS:000181414700025 ER PT J AU Jacquemart, D Mandin, JY Dana, V Regalia-Jarlot, L Plateaux, J Decatoire, D Rothman, LS AF Jacquemart, D Mandin, JY Dana, V Regalia-Jarlot, L Plateaux, J Decatoire, D Rothman, LS TI The spectrum of acetylene in the 5-mu m region from new line-parameter measurements SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE acetylene; infrared; vibro-rotational transitions; Fourier transform spectroscopy; transition dipole moment; line parameters ID LOW-TEMPERATURE; NU(5) BAND; C2H2; INTENSITIES AB Using Fourier Transform spectra (unapodized FWHM: 0.002 cm(-1)) of acetylene (C2H2)-C-12, absolute line positions have been obtained in the 5-mum region for about 490 lines belonging to 15 hot bands arising from the nu(4) = I or nu(5) = I lower vibrational level, improving the data available in this spectral region. Absolute line intensities have been measured for about 410 lines, from which vibrational transition dipole moments squared could be determined, as well as empirical Herman-Wallis coefficients when it was possible. The self-broadening coefficients of more than 370 lines have been measured at room temperature, showing that no vibrational dependence exists for the bands of acetylene already studied, and allowing a significant determination of their rotational dependence. Furthermore, about 120 measured values of self-shifting coefficients are tentatively proposed. Combining results published for other bands, and using the smoothed line-parameter values obtained in this work, a HITRAN-format line list of the acetylene molecule has been set up in this spectral region. (C) 2002 Elsevier Science Ltd. All rights reserved. C1 Univ Paris 06, CNRS, Lab Phys Mol & Applicat, F-75252 Paris 05, France. Univ Reims, Grp Spectrometrie Mol & Atmospher, CNRS, F-51062 Reims, France. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Dana, V (reprint author), Univ Paris 06, CNRS, Lab Phys Mol & Applicat, Case Courrier 76,Tour 13,4 Pl Jussieu, F-75252 Paris 05, France. NR 18 TC 26 Z9 26 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB 1 PY 2003 VL 76 IS 3-4 BP 237 EP 267 AR PII S0022-4073(02)00055-9 DI 10.1016/S0022-4073(02)00055-9 PG 31 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 618CV UT WOS:000179401300001 ER PT J AU Walker, A Balcomb, D Kiss, G Weaver, N Becker, MH AF Walker, A Balcomb, D Kiss, G Weaver, N Becker, MH TI Analyzing two federal building-integrated photovoltaics projects using ENERGY-10 simulations SO JOURNAL OF SOLAR ENERGY ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article AB A new version of the ENERGY-10 computer program simulates the performance of photovoltaic (PV) systems and evaluates a wide range of opportunities to improve energy.,, efficiency in buildings. This paper describes two test cases in which the beta release of, ENERGY-10 version 1.4 was used to evaluate energy efficiency and building-integrated. photovoltaics (BIPV) for two federal building projects: an office and laboratory building at the Smithsonian Astrophysical Laboratory (SAO) in Hilo, Hawaii, and housing for visiting scientists at the Smithsonian Environmental Research Center in Edgewater Mary, land The capabilities of the software, the design assistance provided by ENERGY-10, and, a synopsis of results are given. Estimates of annual energy delivery by the five PV arrays, of the SAO are compared to F-Chart to help inform a validation of ENERGY-10. Results. indicate that, by simulating both the building electrical load and simultaneous PV performance for each hour of the year ENERGY-10 facilitates a highly accurate, integrated analysis useful early in the design process. The simulation is especially useful in calculating the effect of PV on the building peak load, and associated demand cost savings. C1 Natl Renewable Energy Lab, Golden, CO 80401 USA. Kiss & Cathcart Architects, Brooklyn, NY 11201 USA. InterWeaving Consulting, Steamboat Springs, CO 80477 USA. Smithsonian Inst, Washington, DC 20024 USA. RP Walker, A (reprint author), Natl Renewable Energy Lab, 1617 Cole Blvd, Golden, CO 80401 USA. NR 10 TC 5 Z9 5 U1 0 U2 2 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0199-6231 J9 J SOL ENERG-T ASME JI J. Sol. Energy Eng. Trans.-ASME PD FEB PY 2003 VL 125 IS 1 BP 28 EP 33 DI 10.1115/1.1531643 PG 6 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA 643YC UT WOS:000180890300004 ER PT J AU Stahl, J AF Stahl, J TI Duende: A journey into the heart of flamenco. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Amer Art Museum, Washington, DC USA. RP Stahl, J (reprint author), Smithsonian Amer Art Museum, 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 FEB 1 PY 2003 VL 128 IS 2 BP 94 EP 94 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 673WL UT WOS:000182603200111 ER PT J AU Guzman, HM Guevara, CA Hernandez, IC AF Guzman, HM Guevara, CA Hernandez, IC TI Reproductive cycle of two commercial species of sea cucumber (Echinodermata : Holothuroidea) from Caribbean Panama SO MARINE BIOLOGY LA English DT Article ID SOUTHERN TAIWAN; SOLOMON-ISLANDS; BIOLOGY; REEFS; HOLOTHURIANS; FUSCOGILVA; ECOLOGY; GROWTH; MEXICO AB The reproductive status of the holothuroid species Isostichopus badionotus (Selenka, 1867) and Holothuria mexicana (Ludwig, 1875) was studied over 16 months in Bocas del Toro (Panama), from November 1999 to February 2001. Sexual reproduction was evaluated by the gonad index method, and by histology of gonad development. In addition, population structure was assessed based on sex ratio, minimum reproductive size, and length and weight distributions of males and females. The sex ratio in both species was 1:1, with a unimodal population distribution composed mainly of mature individuals. The minimum reproductive length and weight were 13-20 cm and 150 g, respectively, for both species, although reproductive individuals 10 cm in length were also found. A consistently higher gonad index was observed in H. mexicana, due to a high proportion of mature females and males and high gonad indices in most monthly samples. Gametogenesis and spawning patterns seemed to occur throughout the year, with periods of enhanced activity. Two periods of maximum reproductive activity were tentatively identified: July-November for I. badionotus and February-July for H. mexicana, but neither species had a single, sharply defined annual spawning event. Further work on these exploited holothuroids should examine the relationships between reproduction and environmental factors and between reproductive status and recruitment. C1 Smithsonian Trop Res Inst, Balboa, Panama. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Apartado Postal 2072, Balboa, Panama. NR 42 TC 21 Z9 23 U1 2 U2 16 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 FEB PY 2003 VL 142 IS 2 BP 271 EP 279 DI 10.1007/s00227-002-0939-x PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 655CY UT WOS:000181534800008 ER PT J AU Zigler, KS Lessios, HA AF Zigler, KS Lessios, HA TI Evolution of bindin in the pantropical sea urchin Tripneustes: Comparisons to bindin of other genera SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE sea urchins; bindin; speciation; gamete recognition; fertilization; Tripneustes ID POSITIVE DARWINIAN SELECTION; FULL-LENGTH CDNAS; REPRODUCTIVE ISOLATION; MOLECULAR EVOLUTION; STRONGYLOCENTROTUS-FRANCISCANUS; MITOCHONDRIAL-DNA; RAPID EVOLUTION; NONSYNONYMOUS SUBSTITUTIONS; NUCLEOTIDE SUBSTITUTIONS; FERTILIZATION PROTEINS AB Bindin, a sea urchin sperm protein, mediates sperm-egg attachment and membrane fusion and is thus important in species recognition and speciation. Patterns of bindin variation differed among three genera that had been studied previously. In two genera of the superorder Camarodonta, Echinometra and Strongylocentrotus, both of which contain sympatric species, bindin is highly variable within and between species; a region of the molecule evolves at high rates under strong positive selection. In Arbacia, which belongs to the superorder Stirodonta and whose extant species are all allopatric, bindin variation is low, and there is no evidence of positive selection. We cloned and sequenced bindin from Tripneustes, a sea urchin that belongs to the Camarodonta but whose three species are found in different oceans. Worldwide sampling of bindin alleles shows that the bindin of Tripneustes (1) contains the highly conserved core characteristic of all other bindins characterized to date, (2) has an intron in the same position, and (3) has approximately the same length. Its structure is more like that of bindin from other camarodont sea urchins than to bindin from the stirodont Arbacia. The resemblances to other camarodonts include a glycine-rich repeat structure upstream of the core and lack of a hydrophobic domain 3' of the core, a characteristic of Arbacia bindin. Yet the mode of evolution of Tripneustes bindin is more like that of Arbacia. Differences between bindins of the Caribbean Tripneustes ventricosus and the eastern Pacific T. depressus, separated for 3 my by the Isthmus of Panama, are limited to four amino acid changes and a single indel. There are no fixed amino acid differences or indels between T. depressus from the eastern Pacific and T. gratilla from the Indo-Pacific. Bindin of Tripneustes, like that of Arbacia, also shows no evidence of diversifying selection that would manifest itself in a higher proportion of amino acid replacements than of silent nucleotide substitutions. When the rate of intrageneric bindin divergence is standardized by dividing it by cytochrome oxidase I (COI) divergence, Tripneustes and Arbacia show a lower ratio of bindin to COI substitutions between the species of each genus than exists between the species of either Echinometra or Strongylocentrotus. Thus, mode of bindin evolution is not correlated with phylogenetic affinities or molecular structure, but rather with whether the species in a genus are allopatric or sympatric. For a molecule involved in gametic recognition, this would suggest a pattern of evolution via reinforcement. However, in bindin the process that gave rise to this pattern is not likely to have been selection to avoid hybridization, because there is no excess of amino acid replacements between species versus within species in the bindins of Echinometra and Strongylocentrotus, as would have been expected if specific recognition were the driving force in their evolution. We suggest instead that the pattern of reinforcement is a secondary effect of the ability of species with rapidly evolving bindins to coexist in sympatry. C1 Smithsonian Trop Res Inst, Balboa, Panama. Duke Univ, Dept Biol, Durham, NC 27706 USA. RP Zigler, KS (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 82 TC 53 Z9 54 U1 1 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 FEB PY 2003 VL 20 IS 2 BP 220 EP 231 DI 10.1093/molbev/msg020 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 646LG UT WOS:000181036100009 PM 12598689 ER PT J AU Ainsworth, EA Tranel, PJ Drake, BG Long, SP AF Ainsworth, EA Tranel, PJ Drake, BG Long, SP TI The clonal structure of Quercus geminata revealed by conserved microsatellite loci SO MOLECULAR ECOLOGY LA English DT Article DE genetic marker; microsatellite; Quercus geminata; Quercus myrtifolia; simple sequence repeat ID FLORIDA SCRUB; IDENTIFICATION; DIVERSITY; PLANT AB The scrub oak communities of the southeastern USA may have existed at their present locations for thousands of years. These oaks form suckers, and excavations of root systems suggest that clones may occupy very large areas. Resolution of the clonal nature of scrub oaks is important both to manage the tracts of this ecosystem that remain, and in conducting long-term ecological studies, where the study area must substantially exceed the area occupied by any single clone. Microsatellites were used to determine the genetic diversity of a dominant oak species within a 2-ha long-term experimental site on Merritt Island at the Kennedy Space Center. This area contains a long-term study of the effects of elevated CO2 on the ecosystem. Conservation of seven microsatellite loci, previously identified in the sessile oak, Quercus petraea , was tested in two Florida scrub oak species, Q. geminata and Q. myrtifolia . Sequence analysis revealed that all seven microsatellite loci were conserved in Q. geminata and five loci were conserved in Q. myrtifolia . Six microsatellite loci were polymorphic in Q. geminata and these were subsequently used to investigate the clonal structure of the Q. geminata population. Twenty-one unique combinations of microsatellites, or haplotypes, occurred only once, whereas the remaining 26 individuals belonged to a total of seven different haplotypes. Trees with identical haplotypes were in close proximity, supporting the interpretation that they were clones. The results showed that there is significant genetic diversity within the 2-ha experimental site. Microsatellites provided a powerful and noninvasive tool for distinguishing individual genotypes and determining an adequate area for long-term ecosystem studies. C1 Univ Illinois, Dept Crop Sci, Urbana, IL 61801 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Tranel, PJ (reprint author), Univ Illinois, Dept Crop Sci, 1201 W Gregory Dr, Urbana, IL 61801 USA. RI Long, Stephen/A-2488-2008; OI Long, Stephen/0000-0002-8501-7164; Tranel, Patrick/0000-0003-0666-4564 NR 22 TC 12 Z9 12 U1 0 U2 10 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 FEB PY 2003 VL 12 IS 2 BP 527 EP 532 DI 10.1046/j.1365-294X.2003.01749.x PG 6 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 635VT UT WOS:000180421000020 PM 12535102 ER PT J AU Argo, MK Jackson, NJ Browne, IWA York, T McKean, JP Biggs, AD Blandford, RD de Bruyn, AG Chae, KH Fassnacht, CD Koopmans, LVE Myers, ST Norbury, M Pearson, TJ Phillips, PM Readhead, ACS Rusin, D Wilkinson, PN AF Argo, MK Jackson, NJ Browne, IWA York, T McKean, JP Biggs, AD Blandford, RD de Bruyn, AG Chae, KH Fassnacht, CD Koopmans, LVE Myers, ST Norbury, M Pearson, TJ Phillips, PM Readhead, ACS Rusin, D Wilkinson, PN TI CLASS B0445+123: a new two-image gravitational lens system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; galaxies : individual : B0445+123 AB A new two-image gravitational lens system has been discovered as a result of the Cosmic Lens All-Sky Survey. Radio observations with the Very Large Array (VLA), the MultiElement Radio Linked Interferometer Network and the Very Long Baseline Array at increasingly higher resolutions all show two components with a flux density ratio of similar to7 : 1 and a separation of 1.34 arcsec. Both components are compact and have the same spectral index. Follow-up observations made with the VLA at 8.4 GHz show evidence of a feature to the south-east of the brighter component and a corresponding extension of the weaker component to the north-west. Optical observations with the William Herschel Telescope show similar to1.7-arcsec extended emission aligned in approximately the same direction as the separation between the radio components with an R -band magnitude of 21.8 +/- 0.4. C1 Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Joint INst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. CALTECH, Pasadena, CA 91125 USA. Kapteyn Lab, NL-9700 AV Groningen, Netherlands. ASTRON, NL-7990 AA Dwingeloo, Netherlands. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Argo, MK (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. RI Pearson, Timothy/N-2376-2015 OI Pearson, Timothy/0000-0001-5213-6231 NR 10 TC 10 Z9 10 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 FEB 1 PY 2003 VL 338 IS 4 BP 957 EP 961 DI 10.1046/j.1365-8711.2003.06138.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639BN UT WOS:000180607900015 ER PT J AU Biggs, AD Rusin, D Browne, IWA de Bruyn, AG Jackson, NJ Koopmans, LVE McKean, JP Myers, ST Blandford, RD Chae, KH Fassnacht, CD Norbury, MA Pearson, TJ Phillips, PM Readhead, ACS Wilkinson, PN AF Biggs, AD Rusin, D Browne, IWA de Bruyn, AG Jackson, NJ Koopmans, LVE McKean, JP Myers, ST Blandford, RD Chae, KH Fassnacht, CD Norbury, MA Pearson, TJ Phillips, PM Readhead, ACS Wilkinson, PN TI B0850+054: a new gravitational lens system from CLASS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; quasars : individual : B0850+054 ID RADIO-SOURCES; CONSTRAINTS; CONSTANT; CATALOG; SKY; VLA AB We report the discovery of a new gravitational lens system from the CLASS survey. Radio observations with the VLA, WSRT and MERLIN show that the radio source B0850+054 is composed of two compact components with identical spectra, a separation of 0.7 arcsec and a flux density ratio of 6 : 1. VLBA observations at 5 GHz reveal structures that are consistent with the gravitational lens hypothesis. The brighter of the two images is resolved into a linear string of at least six subcomponents, whilst the weaker image is radially stretched towards the lens galaxy. UKIRT K -band imaging detects an 18.7-mag extended object, but the resolution of the observations is not sufficient to resolve the lensed images and the lens galaxy. Mass modelling has not been possible with the present data and the acquisition of high-resolution optical data is a priority for this system. C1 Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. ASTRON, NL-7990 AA Dwingeloo, Netherlands. CALTECH, Pasadena, CA 91125 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Biggs, AD (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. RI Pearson, Timothy/N-2376-2015 OI Pearson, Timothy/0000-0001-5213-6231 NR 19 TC 12 Z9 12 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 FEB 1 PY 2003 VL 338 IS 4 BP 1084 EP 1088 DI 10.1046/j.1365-8711.2003.06159.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 639BN UT WOS:000180607900025 ER PT J AU Krane, S Itagaki, Y Nakanishi, K Weldon, PJ AF Krane, S Itagaki, Y Nakanishi, K Weldon, PJ TI "Venom" of the slow loris: sequence similarity of prosimian skin gland protein and Fel d 1 cat allergen SO NATURWISSENSCHAFTEN LA English DT Article ID MAJOR ALLERGEN; DOMESTIC CAT; FEL-D-1 AB Bites inflicted on humans by the slow loris (Nycticebus coucang), a prosimian from Indonesia, are painful and elicit anaphylaxis. Toxins from N. coucang are thought to originate in the brachial organ, a naked, gland-laden area of skin situated on the flexor surface of the arm that is licked during grooming. We isolated a major component of the brachial organ secretions from N. coucang, an approximately 18 kDa protein composed of two 70-90 amino-acid chains linked by one or more disulfide bonds. The N-termini of these peptide chains exhibit nearly 70% sequence similarity (37% identity, chain 1; 54% identity, chain 2) with the two chains of Fel d 1, the major allergen from the domestic cat (Felis catus). The extensive sequence similarity between the brachial organ component of N. coucang and the cat allergen suggests that they exhibit immunogenic cross-reactivity. This work clarifies the chemical nature of the brachial organ exudate and suggests a possible mode of action underlying the noxious effects of slow loris bites. C1 Columbia Univ, Dept Chem, New York, NY 10027 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Nakanishi, K (reprint author), Columbia Univ, Dept Chem, New York, NY 10027 USA. OI Krane, Sonja/0000-0002-6525-8067 NR 16 TC 13 Z9 14 U1 2 U2 48 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD FEB PY 2003 VL 90 IS 2 BP 60 EP 62 DI 10.1007/s00114-002-0394-z PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 655BN UT WOS:000181531600002 PM 12590298 ER PT J AU Jousselin, E Hossaert-McKey, M Herre, EA Kjellberg, F AF Jousselin, E Hossaert-McKey, M Herre, EA Kjellberg, F TI Why do fig wasps actively pollinate monoecious figs? SO OECOLOGIA LA English DT Article DE coevolution; mutualism; pollination behaviour; stigma ID FICUS-CARICA L; PHYLOGENETIC-RELATIONSHIPS; COMMON FIG; MUTUALISM; EVOLUTION; SEED; COEVOLUTION; CONSEQUENCES; SYCONIA AB Active pollination, although rare, has been documented in a few pollination mutualisms. Such behaviour can only evolve if it benefits the pollinator in some way. The wasps that pollinate Ficus inflorescences can be active or passive pollinators. They lay their eggs in fig flowers, so that a proportion of flowers will host a wasp larva instead of a seed. We show in an actively pollinated monoecious fig that lack of pollination does not induce fig abortion or affect wasp offspring size but results in smaller numbers of offspring. Hence, conversely to other active pollination systems, seed formation is not obligatory to sustain developing pollinator larvae; however there is a direct fitness cost to active pollinators not to pollinate. We then compared the locations of eggs and fertilised flowers of three actively pollinated Ficus species and one passively pollinated species. We found that more flowers containing wasp eggs were fertilised in the actively pollinated species relative to those of the passively pollinated one. These results along with comparison with similar studies on dioecious figs, support the hypothesis that active pollination has evolved in fig wasps to ensure that more flowers containing wasp eggs are fertilised as this may increase the chances of successful gall development. The stigmatic platform characterising actively pollinated figs is probably an adaptation to increase pollen dispersion within the fig. 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), Univ Pretoria, Dept Genet, ZA-0002 Pretoria, South Africa. EM ejousselin@yahoo.com NR 43 TC 50 Z9 56 U1 2 U2 19 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD FEB PY 2003 VL 134 IS 3 BP 381 EP 387 DI 10.1007/s00442-002-1116-0 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 657BG UT WOS:000181645100012 PM 12647146 ER PT J AU Feller, IC Whigham, DF McKee, KL Lovelock, CE AF Feller, IC Whigham, DF McKee, KL Lovelock, CE TI Nitrogen limitation of growth and nutrient dynamics in a disturbed mangrove forest, Indian River Lagoon, Florida SO OECOLOGIA LA English DT Article DE disturbance; fertilization; experiment; phosphorus; photosynthesis; resorption ID VS. PHOSPHORUS LIMITATION; RHIZOPHORA-MANGLE; ELECTRON-TRANSPORT; USE EFFICIENCY; PLANT-GROWTH; FRESH-WATER; SEDIMENTS; PATTERNS; GRADIENT; LEAVES AB The objectives of this study were to determine effects of nutrient enrichment on plant growth, nutrient dynamics, and photosynthesis in a disturbed mangrove forest in an abandoned mosquito impoundment in Florida. Impounding altered the hydrology and soil chemistry of the site. In 1997, we established a factorial experiment along a tree-height gradient with three zones, i.e., fringe, transition, dwarf, and three fertilizer treatment levels, i.e., nitrogen (N), phosphorus (P), control, in Mosquito Impoundment 23 on the eastern side of Indian River. Transects traversed the forest perpendicular to the shoreline, from a Rhizophora mangle-dominated fringe through an Avicennia germinans stand of intermediate height, and into a scrub or dwarf stand of A. germinans in the hinterland. Growth rates increased significantly in response to N fertilization. Our growth data indicated that this site is N-limited along the tree-height gradient. After 2 years of N addition, dwarf trees resembled vigorously growing saplings. Addition of N also affected internal dynamics of N and P and caused increases in rates of photosynthesis. These findings contrast with results for a R. mangle-dominated forest in Belize where the fringe is N-limited, but the dwarf zone is P-limited and the transition zone is co-limited by N and P. This study demonstrated that patterns of nutrient limitation in mangrove ecosystems are complex, that not all processes respond similarly to the same nutrient, and that similar habitats are not limited by the same nutrient when different mangrove forests are compared. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. RP Feller, IC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI McKee, Karen/D-1365-2014; Lovelock, Catherine/G-7370-2012; OI McKee, Karen/0000-0001-7042-670X; Lovelock, Catherine/0000-0002-2219-6855; Whigham, Dennis/0000-0003-1488-820X; Feller, Ilka/0000-0002-6391-1608 NR 65 TC 86 Z9 97 U1 7 U2 48 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD FEB PY 2003 VL 134 IS 3 BP 405 EP 414 DI 10.1007/s00442-002-1117-z PG 10 WC Ecology SC Environmental Sciences & Ecology GA 657BG UT WOS:000181645100015 PM 12647149 ER PT J AU Krause, GH Grube, E Virgo, A Winter, K AF Krause, GH Grube, E Virgo, A Winter, K TI Sudden exposure to solar UV-B radiation reduces net CO2 uptake and photosystem I efficiency in shade-acclimated tropical tree seedlings SO PLANT PHYSIOLOGY LA English DT Article ID ULTRAVIOLET-RADIATION; OZONE DEPLETION; PHOTOSYNTHESIS; LEAVES; PHOTOINHIBITION; PLANTS; STRESS; LIGHT; FLUORESCENCE; INHIBITION AB Tree seedlings developing in the understory of the tropical forest have to endure short periods of high-light stress when tree-fall gaps are formed, and direct solar radiation, including substantial UV light, reaches the leaves. In experiments simulating the opening of a tree-fall gap, the response of photosynthesis in leaves of shade-acclimated seedlings (Anacardium excelsum, Virola surinamensis, and Calophyllum longifolium) to exposure to direct sunlight (for 20-50 min) was investigated in Panama (9degreesN). To assess the effects of solar UV-B radiation (280-320 nm), the sunlight was filtered through plastic films that selectively absorbed UV-B or transmitted the complete spectrum. The results document a strong inhibition of CO2 assimilation by sun exposure. Light-limited and light-saturated rates of photosynthetic CO2 uptake by the leaves were affected, which apparently occurred independently of a simultaneous inhibition of potential photosystem (PS) II efficiency. The ambient UV-B light substantially contributed to these effects. The photochemical capacity of PSI, measured as absorbance change at 810 nm in saturating far-red light, was not significantly affected by sun exposure of the seedlings. However, a decrease in the efficiency of P700 photooxidation by far-red light was observed, which was strongly promoted by solar UV-B radiation. The decrease in PSI efficiency may result from enhanced charge recombination in the reaction center, which might represent an incipient inactivation of PSI, but contributes to thermal dissipation of excessive light energy and thereby to photoprotection. C1 Univ Dusseldorf, Inst Plant Biochem, D-40225 Dusseldorf, Germany. Smithsonian Trop Res Inst, Ancon, Panama. RP Krause, GH (reprint author), Univ Dusseldorf, Inst Plant Biochem, D-40225 Dusseldorf, Germany. EM ghkrause@uni-duesseldorf.de NR 41 TC 22 Z9 26 U1 0 U2 6 PU AMER SOC PLANT BIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA SN 0032-0889 EI 1532-2548 J9 PLANT PHYSIOL JI Plant Physiol. PD FEB PY 2003 VL 131 IS 2 BP 745 EP 752 DI 10.1104/pp.014076 PG 8 WC Plant Sciences SC Plant Sciences GA 645XD UT WOS:000181005000036 PM 12586898 ER PT J AU Miller, JA AF Miller, JA TI Assessing progress in systematics with continuous jackknife function analysis SO SYSTEMATIC BIOLOGY LA English DT Article DE accuracy; combined data; comparative biology; congruence; data visualization; jackknife; pseudoreplicate; stability; support; total evidence ID 12S RIBOSOMAL-RNA; DNA-SEQUENCE DATA; PHYLOGENETIC ANALYSIS; SECONDARY-STRUCTURE; SPIDERS ARANEAE; EVOLUTIONARY TREES; CONSISTENCY INDEX; CONFIDENCE-LIMITS; MISSING ENTRIES; PARSIMONY AB Systematists expect their hypotheses to be asymptotically precise. As the number of phylogenetically informative characters for a set of taxa increases, the relationships implied should stabilize on some topology. If true, this increasing stability should clearly manifest itself if an index of congruence is plotted against the accumulating number of characters. Continuous jackknife function (CJF) analysis is a new graphical method that portrays the extent to which available data converge on a specified phylogenetic hypothesis, the reference tree. The method removes characters with increasing probability, analyzes the rarefied data matrices phylogenetically, and scores the clades shared between each of the resulting trees and the reference tree. As more characters are removed, the number of shared clades must decrease, but the rate of decrease will depend on how decisively the data support the reference tree. Curves for stable phylogenies are clearly asymptotic with nearly 100% congruence for a substantial part of the curve. Less stable phylogenies lose congruent nodes quickly as characters are excluded, resulting in a more linear or even a sigmoidal relationship. Curves can be interpreted as predictors of whether the addition of new data of the same type is likely to alter the hypothesis under test. Continuous jackknife function analysis makes statistical assumptions about the collection of character data. To the extent that CJF curves are sensitive to violations of unbiased character collection, they will be misleading as predictors. Convergence of data on a reference tree does not guarantee historical accuracy, but it does predict that the accumulation of further data under the sampling model will not lead to rapid changes in the hypothesis. C1 Smithsonian Inst, Dept Systemat Biol Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Miller, JA (reprint author), Smithsonian Inst, Dept Systemat Biol Entomol, Natl Museum Nat Hist, NHB-105,POB 37012, Washington, DC 20013 USA. NR 96 TC 16 Z9 16 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD FEB PY 2003 VL 52 IS 1 BP 55 EP 65 DI 10.1080/10635150390132731 PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 635LH UT WOS:000180400000006 PM 12554440 ER PT J AU Jordan, S Simon, C Polhemus, D AF Jordan, S Simon, C Polhemus, D TI Molecular systematics and adaptive radiation of Hawaii's endemic damselfly genus Megalagrion (Odonata : Coenagrionidae) SO SYSTEMATIC BIOLOGY LA English DT Article DE Bayesian phylogenetics; Hawaii; local molecular clock; Megalagrion damselflies; species radiations ID PHYLOGENETIC ANALYSIS; MITOCHONDRIAL-DNA; COMBINING DATA; EVOLUTION; INFERENCE; TREE; SPECIATION; AGES AB Damselflies of the endemic Hawaiian genus Megalagrion have radiated into a wide variety of habitats and are an excellent model group for the study of adaptive radiation. Past phylogenetic analysis based on morphological characters has been problematic. Here, we examine relationships among 56 individuals from 20 of the 23 described species using maximum likelihood (ML) and Bayesian phylogenetic analysis of mitochondrial (1,287 bp) and nuclear (1,039 bp) DNA sequence data. Models of evolution were chosen using the Akaike information criterion. Problems with distant outgroups were accommodated by constraining the best ML ingroup topology but allowing the outgroups to attach to any ingroup branch in a bootstrap analysis. No strong contradictions were obtained between either data partition and the combined data set. Areas of disagreement are mainly confined to clades that are strongly supported by the mitochondrial DNA and weakly supported by the elongation factor 1alpha data because of lack of changes. However, the combined analysis resulted in a unique tree. Correlation between Bayesian posterior probabilities and bootstrap percentages decreased in concert with decreasing information in the data partitions. In cases where nodes were supported by single characters bootstrap proportions were dramatically reduced compared with posterior probabilities. Two speciation patterns were evident from the phylogenetic analysis. First, most speciation is interisland and occurred as members of established ecological guilds colonized new volcanoes after they emerged from the sea. Second, there are several instances of rapid radiation into a variety of specialized habitats, in one case entirely within the island of Kauai. Application of a local clock procedure to the mitochondrial DNA topology suggests that two of these radiations correspond to the development of habitat on the islands of Kauai and Oahu. About 4.0 million years ago, species simultaneously moved into fast streams and plant leaf axils on Kauai, and about 1.5 million years later another group moved simultaneously to seeps and terrestrial habitats on Oahu. Results from the local clock analysis also strongly suggest that Megalagrion arrived in Hawaii about 10 million years ago, well before the emergence of Kauai. Date estimates were more sensitive to the particular node that was fixed in time than to the model of local branch evolution used. We propose a general model for the development of endemic damselfly species on Hawaiian Islands and document five potential cases of hybridization (M. xanthomelas x M. pacificum, M. eudytum x M. vagabundum, M. orobates x M. oresitrophum, M. nesiotes x M. oahuense, and M. mauka x M. paludicola). C1 Univ Connecticut, Dept Ecol & Evolut Biol, Storrs, CT 06269 USA. Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. RP Jordan, S (reprint author), Univ Grenoble 1, Lab Ecol Alpine, CNRS, UMR 5553, BP 53, F-38041 Grenoble 9, France. NR 75 TC 98 Z9 101 U1 2 U2 25 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD FEB PY 2003 VL 52 IS 1 BP 89 EP 109 DI 10.1080/10635150390132803 PG 21 WC Evolutionary Biology SC Evolutionary Biology GA 635LH UT WOS:000180400000009 PM 12554443 ER PT J AU Soon, W Baliunas, S AF Soon, W Baliunas, S TI Proxy climatic and environmental changes of the past 1000 years SO CLIMATE RESEARCH LA English DT Review DE paleoclimate proxies; climate change; environmental change; Little Ice Age; Medieval Warm Period ID MEDIEVAL WARM PERIOD; LAST 2 MILLENNIA; NORTH-ATLANTIC OSCILLATION; SURFACE-TEMPERATURE CHANGE; QINGHAI-TIBETAN PLATEAU; TREE-RING CHRONOLOGIES; SOUTHERN SOUTH-AMERICA; ANTARCTIC ICE-SHEET; LOW ATMOSPHERIC CO2; BOREHOLE TEMPERATURES AB The 1000 yr climatic and environmental history of the Earth contained in various proxy records is reviewed. As indicators, the proxies duly represent local climate. Because each is of a different nature, the results from the proxy indicators cannot be combined into a hemispheric or global quantitative composite, However, considered as an ensemble of individual expert opinions, the assemblage of local representations of climate establishes both the Little Ice Age and Medieval Warm Period as climatic anomalies with worldwide imprints, extending earlier results by Bryson et al. (1963), Lamb (1965), and numerous intervening research efforts. Furthermore, the individual proxies can be used to address the question of whether the 20th century is the warmest of the 2nd millennium locally. Across the world, many records reveal that the 20th century is probably not the warmest nor a uniquely extreme climatic period of the last millennium. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Mt Wilson Observ, Mt Wilson, CA 91023 USA. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 16, Cambridge, MA 02138 USA. EM wsoon@cfa.harvard.edu NR 211 TC 80 Z9 92 U1 8 U2 48 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0936-577X EI 1616-1572 J9 CLIM RES JI Clim. Res. PD JAN 31 PY 2003 VL 23 IS 2 BP 89 EP 110 DI 10.3354/cr023089 PG 22 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 671UD UT WOS:000182481700001 ER PT J AU Granger, BE Greene, CH AF Granger, BE Greene, CH TI Nonclassical paths in the recurrence spectrum of diamagnetic atoms SO PHYSICAL REVIEW LETTERS LA English DT Article ID CLOSED CLASSICAL ORBITS; MAGNETIC-FIELD; HYDROGEN-ATOM; QUANTUM SPECTRA; SPECTROSCOPY; IONIZATION; SCATTERING; REGIME AB Using time-independent scattering matrices, we study how the effects of nonclassical paths on the recurrence spectra of diamagnetic atoms can be extracted from purely quantal calculations. This study reveals an intimate relationship between two types of nonclassical paths: exotic ghost orbits and diffractive orbits. This relationship proves to be a previously unrecognized reason for the success of semiclassical theories, such as closed-orbit theory, and permits a comprehensive reformulation of the semiclassical theory that elucidates its convergence properties. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Univ Colorado, Dept Phys, Boulder, CO 80309 USA. RP Granger, BE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. RI Greene, Chris/C-3821-2011 OI Greene, Chris/0000-0002-2096-6385 NR 22 TC 7 Z9 9 U1 0 U2 0 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 JAN 31 PY 2003 VL 90 IS 4 AR 043002 DI 10.1103/PhysRevLett.90.043002 PG 4 WC Physics, Multidisciplinary SC Physics GA 640TA UT WOS:000180703000011 PM 12570415 ER PT J AU Konacki, M Torres, G Jha, S Sasselov, DD AF Konacki, M Torres, G Jha, S Sasselov, DD TI An extrasolar planet that transits the disk of its parent star SO NATURE LA English DT Article ID 51-PEG-LIKE PLANET; GIANT PLANETS; HD-209458 AB Planets orbiting other stars could in principle be found through the periodic dimming of starlight as a planet moves across-or 'transits'-the line of sight between the observer and the star. Depending on the size of the planet relative to the star, the dimming could reach a few per cent of the apparent brightness of the star. Despite many searches, no transiting planet has been discovered in this way; the one known 1,2 transiting planet-HD209458b-was first discovered using precise measurements(2,3) of the parent star's radial velocity and only subsequently detected photometrically. Here we report radial velocity measurements of the star OGLE-TR-56, which was previously found to exhibit a 1.2-day transit-like light curve 4,5 in a survey looking for gravitational microlensing events. The velocity changes that we detect correlate with the light curve, from which we conclude that they are probably induced by an object of around 0.9 Jupiter masses in an orbit only 0.023 AU from its star. We estimate the planetary radius to be around 1.3 Jupiter radii and its density to be about 0.5 g cm(-3). This object is hotter than any known planet (similar to1,900 K), but is still stable against long-term evaporation or tidal disruption. C1 CALTECH, Div Geol & Planteary Sci 150 21, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Konacki, M (reprint author), CALTECH, Div Geol & Planteary Sci 150 21, Pasadena, CA 91125 USA. RI Konacki, Maciej/A-1220-2007 NR 22 TC 269 Z9 269 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 JAN 30 PY 2003 VL 421 IS 6922 BP 507 EP 509 DI 10.1038/nature01379 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 640DB UT WOS:000180670600037 PM 12556885 ER PT J AU Graham, EA Mulkey, SS Kitajima, K Phillips, NG Wright, SJ AF Graham, EA Mulkey, SS Kitajima, K Phillips, NG Wright, SJ TI Cloud cover limits net CO2 uptake and growth of a rainforest tree during tropical rainy seasons SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE El Nino; canopy; photosynthesis; light limitation ID TERRESTRIAL ECOSYSTEMS; GLOBAL RADIATION; FOREST; CANOPY; VARIABILITY; COMPONENTS; EXCHANGE; MODEL AB Recent global-scale analyses indicate that climate variability affects net carbon storage but regard temperature and precipitation to be the main contributors. Seasonal and interannual variation in light availability may also limit CO2 uptake. As an experimental test of light limitation by cloud cover during tropical rainy seasons and by the unusually heavy cloud cover associated with La Nina, we installed high-intensity lamps above the forest canopy to augment light for Luehea seemannii, a tropical canopy tree species, during cloudy periods of 1999-2000. Light augmentation only partially compensated for the reduction in photosynthetic photon flux density caused by clouds. Nonetheless, leaves acclimated to the augmented irradiance, and photosynthesis, vegetative growth, and reproduction increased significantly. Light, rather than water, temperature, or leaf nitrogen, was the primary factor limiting CO2 uptake during the rainy season. C1 Univ Florida, Dept Bot, Gainesville, FL 34002 USA. Boston Univ, Dept Geog, Boston, MA 02215 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Mulkey, SS (reprint author), Univ Florida, Dept Bot, 220 Bartram Hall, Gainesville, FL 34002 USA. RI Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013; OI Wright, Stuart/0000-0003-4260-5676; Graham, Eric/0000-0002-7495-4056 NR 31 TC 193 Z9 208 U1 7 U2 51 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 21 PY 2003 VL 100 IS 2 BP 572 EP 576 DI 10.1073/pnas.0133045100 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 638UE UT WOS:000180589000036 PM 12518044 ER PT J AU Wilf, P Johnson, KR Huber, BT AF Wilf, P Johnson, KR Huber, BT TI Correlated terrestrial and marine evidence for global climate chanaes before mass extinction at the Cretaceous-Paleogene boundary SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID TERTIARY BOUNDARY; NORTH-DAKOTA; PLANKTONIC-FORAMINIFERA; DECCAN VOLCANISM; FOSSIL FLORAS; WARMING EVENT; TEMPERATURE; EOCENE; PALEOCLIMATE; ATLANTIC AB Terrestrial climates near the time of the end-Cretaceous mass extinction are poorly known, limiting understanding of environmentally driven changes in biodiversity that occurred before bolide impact. We estimate paleotemperatures for the last approximate to1.1 million years of the Cretaceous (approximate to66.6-65.5 million years ago, Ma) by using fossil plants from North Dakota and employ paleomagnetic stratigraphy to correlate the results to foraminiferal paleoclimatic data from four middle- and high-latitude sites. Both plants and foraminifera indicate warming near 66.0 Ma, a warming peak from approximate to65.8 to 65.6 Mal, and cooling near 65.6 Ma, suggesting that these were global climate shifts. The warming peak coincides with the immigration of a thermophilic flora, maximum plant diversity, and the poleward range expansion of thermophilic foraminifera. Plant data indicate the continuation of relatively cool temperatures across the Cretaceous-Paleogene boundary; there is no indication of a major warming immediately after the boundary as previously reported. Our temperature proxies correspond well with recent pCO(2) data from paleosol carbonate, suggesting a coupling Of pCO(2) and temperature. To the extent that biodiversity is correlated with temperature, estimates of the severity of end-Cretaceous extinctions that are based on occurrence data from the warming peak are probably inflated, as we illustrate for North Dakota plants. However, our analysis of climate and facies considerations shows that the effects of bolide impact should be regarded as the most significant contributor to these plant extinctions. C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. Univ Michigan, Dept Geol Sci, Ann Arbor, MI 48109 USA. Denver Museum Nat & Sci, Dept Earth Sci, Denver, CO 80205 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Wilf, P (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM pwilf@geosc.psu.edu NR 57 TC 115 Z9 118 U1 2 U2 31 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 21 PY 2003 VL 100 IS 2 BP 599 EP 604 DI 10.1073/pnas.0234701100 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 638UE UT WOS:000180589000041 PM 12524455 ER PT J AU Kochanek, CS AF Kochanek, CS TI Gravitational lens time delays in cold dark matter SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; dark matter; distance scale; gravitational lensing ID ELLIPTIC GALAXIES; HUBBLE CONSTANT; MASS MODELS; HALOS; DEGENERACIES; PROFILES AB In standard cold dark matter (CDM) halo models, the time delay of a gravitational lens is determined by the cold baryon mass fraction, f(b) = Omega(b,cold)/Omega(0), of the visible galaxy relative to the overall halo. The observed time delays in PG 1115+080, SBS 1520+530, B1600+434, and HE 2149-2745 give Hubble constants consistent with the Hubble Space Telescope Key Project value of H-0 = 72 +/- 8 km s(-1) Mpc(-1) only if f(b) greater than or similar to 0.2 (one-sided 68% confidence), which is larger than the upper bound of f(b,max) = Omega(b)/Omega(0) = 0.15 +/- 0.05 estimated from the cosmic microwave background. If all available baryons cool and f(b) = f(b,max), then the time delays imply H-0 = 65 +/- 6 kms(-1) Mpc(-1) (95% confidence). If local inventories of cold baryons, f(b) similar or equal to 0.013/h(70), are correct, then H-0 = 52 +/- 6 km s(-1) Mpc(-1) and the halo parameters closely match isothermal mass models. Isothermal models are also consistent with strong and weak lens studies, stellar dynamics, and X-ray observations on these scales, while significantly more centrally concentrated models are not. There is a conflict between gravitational lens time delays, the local distance scale, and standard CDM halo models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 60 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 JAN 20 PY 2003 VL 583 IS 1 BP 49 EP 57 DI 10.1086/345342 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634NJ UT WOS:000180346800004 ER PT J AU Wyithe, JSB Winn, JN Rusin, D AF Wyithe, JSB Winn, JN Rusin, D TI The multiband magnification bias for gravitational lenses SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; gravitational lensing ID ALL-SKY SURVEY; COLD DARK-MATTER; COSMOLOGICAL CONSTANT; RADIO; ROSAT; QSOS; STATISTICS; EVOLUTION; CATALOG; QUASAR AB We present a generalization of the concept of magnification bias for gravitationally lensed quasars in which the quasars are selected by flux in more than one wavelength band. To illustrate the principle, we consider the case of two-band selection, in which the fluxes in the two bands are uncorrelated, perfectly correlated, or correlated with scatter. For uncorrelated fluxes, we show that the previously held result that the bias is the product of the single-band biases is generally false. We demonstrate some important properties of the multiband magnification bias using model luminosity functions inspired by observed correlations among X-ray, optical, infrared, and radio fluxes of quasars. In particular, the bias need not be an increasing function of each flux, and the bias can be extremely large for nonlinear correlations. The latter fact may account for the high lensing rates found in some X-ray/optical- and infrared/radio-selected samples. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wyithe, JSB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wyithe, Stuart/0000-0001-7956-9758 NR 47 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2003 VL 583 IS 1 BP 58 EP 66 DI 10.1086/345358 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634NJ UT WOS:000180346800005 ER PT J AU Markevitch, M Bautz, MW Biller, B Butt, Y Edgar, R Gaetz, T Garmire, G Grant, CE Green, P Juda, M Plucinsky, PP Schwartz, D Smith, R Vikhlinin, A Virani, S Wargelin, BJ Wolk, S AF Markevitch, M Bautz, MW Biller, B Butt, Y Edgar, R Gaetz, T Garmire, G Grant, CE Green, P Juda, M Plucinsky, PP Schwartz, D Smith, R Vikhlinin, A Virani, S Wargelin, BJ Wolk, S TI Chandra spectra of the soft X-ray diffuse background SO ASTROPHYSICAL JOURNAL LA English DT Article DE intergalactic medium; ISM : general; methods : data analysis; X-rays : diffuse background; X-rays : ISM ID ALL-SKY SURVEY; SOLAR-WIND; EMISSION; ROSAT; SPECTROMETER; DETECTORS; NEUTRALS; SURFACE; MAPS; GAS AB We present an exploratory Chandra ACIS-S3 study of the diffuse component of the cosmic X-ray background (CXB) in the 0.3-7 keV band for four directions at high Galactic latitudes, with emphasis on details of the ACIS instrumental background modeling. Observations of the dark Moon are used to model the detector background. A comparison of the Moon data and the data obtained with ACIS stowed outside the focal area showed that the dark Moon does not emit significantly in our band. Point sources down to 3x10(-16) ergs s(-1) cm(-2) in the 0.5-2 keV band are excluded in our two deepest observations. We estimate the contribution of fainter, undetected sources to be less than 20% of the remaining CXB flux in this band in all four pointings. In the 0.3-1 keV band, the diffuse signal varies strongly from field to field and contributes between 55% and 90% of the total CXB signal. It is dominated by emission lines that can be modeled by a kT=0.1-0.4 keV plasma. In particular, the two fields located away from bright Galactic features show a prominent line blend at Eapproximate to580 eV (O VII + O VIII) and a possible line feature at Esimilar to300 eV. The two pointings toward the North Polar Spur exhibit a brighter O blend and additional bright lines at 730-830 eV (Fe XVII). We measure the total 1-2 keV flux of (1.0-1.2+/-0.2)x10(-15) ergs s(-1) cm(-2) arcmin(-2) (mostly resolved) and the 2-7 keV flux of (4.0-4.5+/-1.5)x10(-15) ergs s(-1) cm(-2) arcmin(-2). At E>2 keV, the diffuse emission is consistent with zero, to an accuracy limited by the short Moon exposure and systematic uncertainties of the S3 background. Assuming Galactic or local origin of the line emission, we put an upper limit of similar to3x10(15) ergs s(-1) cm(-2) arcmin(-2) on the 0.3-1 keV extragalactic diffuse flux. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Markevitch, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Juda, Michael/0000-0002-4375-9688; Wolk, Scott/0000-0002-0826-9261 NR 54 TC 121 Z9 121 U1 0 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 JAN 20 PY 2003 VL 583 IS 1 BP 70 EP 84 DI 10.1086/345347 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634NJ UT WOS:000180346800007 ER PT J AU Warren, JS Hughes, JP Slane, PO AF Warren, JS Hughes, JP Slane, PO TI Revealing new physical structures in the supernova remnant N63A through Chandra imaging spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (N63A); supernova remnants; X-rays : ISM ID LARGE-MAGELLANIC-CLOUD; H-II REGIONS; HEAVY-ELEMENTS; SHOCK; ABUNDANCES; DUST AB We present Chandra X-ray observations of the supernova remnant (SNR) N63A in the Large Magellanic Cloud (LMC). N63A, one of the brightest LMC remnants, is embedded in an H II region and is probably associated with an OB association. The optical remnant consists of three lobes of emission contained within the approximately 3 times larger X-ray remnant. Our Chandra data reveal a number of new physical structures in N63A. The most striking of these are the several "crescent"-shaped structures located beyond the main shell that resemble similar features seen in the Vela SNR. In Vela, these have been interpreted as arising from high-speed clumps of supernova ejecta interacting with the ambient medium. Another distinct feature of the remnant is a roughly triangular "hole" in the X-ray emission near the location of the optical lobes and the brightest radio emission. X-ray spectral analysis shows that this deficit of emission is the result of absorption by an intervening dense cloud with a mass of similar to450 M-circle dot that is currently being engulfed by the remnant's blast wave. We also find that the rim of the remnant, as well as the crescent-shaped features, has considerably softer X-ray spectra than the interior. Limits on hard X-ray emission rule out a young, energetic pulsar in N63A, but the presence of an older or less active one, powering a wind nebula with a luminosity less than similar to4x10(34) ergs s(-1), is allowed. C1 Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Warren, JS (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. NR 24 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 JAN 20 PY 2003 VL 583 IS 1 BP 260 EP 266 DI 10.1086/345078 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634NJ UT WOS:000180346800020 ER PT J AU Hartigan, P Kenyon, SJ AF Hartigan, P Kenyon, SJ TI A spectroscopic survey of subarcsecond binaries in the Taurus-Auriga dark cloud with the Hubble Space Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; binaries : visual; stars : formation; stars : pre-main-sequence ID MAGNETIC NEUTRON STARS; DISK ACCRETION; YOUNG STARS; GG TAURI; EVOLUTIONARY MODELS; CLOSE COMPANIONS; ORION NEBULA; SEQUENCE; EMISSION; EXTINCTION AB We report the results of a spectroscopic survey of 20 close T Tauri binaries in the Taurus-Auriga dark cloud where the separations between primaries and their secondaries are less than the typical size of a circumstellar disk around a young star. Analysis of low- and medium-resolution Space Telescope Imaging Spectrograph spectra yields the stellar luminosities, reddenings, ages, masses, mass accretion rates, IR excesses, and emission-line luminosities for each star in each pair. We examine the ability of IR color excesses, H equivalent widths, [O I] emission, and veiling to distinguish between weak emission and classical T Tauri stars. Four pairs have one classical T Tauri star ( CTTS) and one weak-lined T Tauri star (WTTS); the CTTS is the primary in three of these systems. This frequency of mixed pairs among the close T Tauri binaries is similar to the frequency of mixed pairs in wider young binaries. Extinctions within pairs are usually similar; however, the secondary is more heavily reddened than the primary in some systems, where it may be viewed through the primary's disk. Mass accretion rates of primaries and secondaries are strongly correlated, and H luminosities, IR excesses, and ages also correlate within pairs. Primaries tend to have somewhat larger accretion rates than their secondaries do and are typically slightly older than their secondaries according to three different sets of modern pre main-sequence evolutionary tracks. Age differences for XZ Tau and FS Tau, systems embedded in reflection nebulae, are striking: the secondary in each pair is less massive but more luminous than the primary. The stellar masses of the UY Aur and GG Tau binaries measured from their rotating molecular disks are about 30% larger than the masses inferred from the spectra and evolutionary tracks. This discrepancy can be resolved in several ways, among them a 10% closer distance for the Taurus-Auriga dark cloud. C1 Rice Univ, Dept Space Phys & Astron, Houston, TX 77005 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartigan, P (reprint author), Rice Univ, Dept Space Phys & Astron, 6100 S Main, Houston, TX 77005 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 61 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 JAN 20 PY 2003 VL 583 IS 1 BP 334 EP 357 DI 10.1086/345293 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634NJ UT WOS:000180346800029 ER PT J AU Holder, J Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Cui, W Dowdall, C Duke, C Perez, ID Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, L Gaidos, JA Gibbs, K Gammell, S Hall, J Hall, TA Hillas, AM Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F LeBohec, S Linton, ET Lloyd-Evans, J Moriarty, P Muller, D Nagai, TN Ong, R Page, M Pallassini, R Petry, D Power-Mooney, B Quinn, J Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Vassiliev, VV Wakely, SP Walker, G Weekes, TC AF Holder, J Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Cui, W Dowdall, C Duke, C Perez, ID Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, L Gaidos, JA Gibbs, K Gammell, S Hall, J Hall, TA Hillas, AM Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F LeBohec, S Linton, ET Lloyd-Evans, J Moriarty, P Muller, D Nagai, TN Ong, R Page, M Pallassini, R Petry, D Power-Mooney, B Quinn, J Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Vassiliev, VV Wakely, SP Walker, G Weekes, TC TI Detection of TeV gamma rays from the BL Lacertae object 1ES 1959+650 with the Whipple 10 meter telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (1ES 1959+650); gamma rays : observations ID ACTIVE GALAXY MARKARIAN-421; X-RAY; ENERGY-SPECTRUM; STRONG FLARES; RADIATION; MKN-501; BLAZARS; PHOTONS; SYSTEM AB We present the first strong detection of very high energy gamma-rays from the close (z=0.048) X-ray-selected BL Lacertae object 1ES 1959+650. Observations were made with the Whipple 10 m telescope on Mount Hopkins, Arizona, using the atmospheric Cerenkov imaging technique. The flux between 2002 May and July was highly variable, with a mean of 0.64+/-0.03 times the steady flux from the Crab Nebula and reaching a maximum of 5 crab, with variability on timescales as short as 7 hr. C1 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. Iowa State Univ Sci & Technol, Dept Phys & Astron, Ames, IA 50011 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland, Dept Phys, Dublin 4, Ireland. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. Depauw Univ, Dept Phys, Greencastle, IN 46135 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Cork Inst Technol, Dept Phys, Cork, Ireland. RP Holder, J (reprint author), Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. RI Hall, Jeter/F-6108-2013; Hall, Jeter/E-9294-2015 NR 55 TC 51 Z9 51 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 JAN 20 PY 2003 VL 583 IS 1 BP L9 EP L12 DI 10.1086/367816 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634NL UT WOS:000180347000003 ER PT J AU Kaaret, P Corbel, S Prestwich, AH Zezas, A AF Kaaret, P Corbel, S Prestwich, AH Zezas, A TI Radio emission from an ultraluminous x-ray source SO SCIENCE LA English DT Article ID HIGH-RESOLUTION IMAGER; SUPER STAR-CLUSTERS; BLACK-HOLES; OPTICAL COUNTERPART; RELATIVISTIC JETS; GALAXIES; POPULATION; IDENTIFICATIONS; REGION; STATES AB The physical nature of ultraluminous x-ray sources is uncertain. Stellar-mass black holes with beamed radiation and intermediate black holes with isotropic radiation are two plausible explanations. We discovered radio emission from an ultraluminous x-ray source in the dwarf irregular galaxy NGC 5408. The x-ray, radio, and optical fluxes as well as the x-ray spectral shape are consistent with beamed relativistic jet emission from an accreting stellar black hole. If confirmed, this would suggest that the ultraluminous x-ray sources may be stellar-mass rather than intermediate-mass black holes. However, interpretation of the source as a jet-producing intermediate-mass black hole cannot be ruled out at this time. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Etud Saclay, CEA Saclay Federat APC, F-91191 Gif Sur Yvette, France. Univ Paris 07, F-91191 Gif Sur Yvette, France. 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 42 TC 123 Z9 124 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 JAN 17 PY 2003 VL 299 IS 5605 BP 365 EP 367 DI 10.1126/science.1079610 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 635YB UT WOS:000180426800036 PM 12532009 ER PT J AU Currie, CR Wong, B Stuart, AE Schultz, TR Rehner, SA Mueller, UG Sung, GH Spatafora, JW Straus, NA AF Currie, CR Wong, B Stuart, AE Schultz, TR Rehner, SA Mueller, UG Sung, GH Spatafora, JW Straus, NA TI Ancient tripartite coevolution in the attine ant-microbe symbiosis SO SCIENCE LA English DT Article ID FUNGUS-GROWING ANTS; LEAF-CUTTING ANTS; HYMENOPTERA; AGRICULTURE; FORMICIDAE; MUTUALISM; PHYLOGENY; BACTERIA AB The symbiosis between fungus-growing ants and the fungi they cultivate for food has been shaped by 50 million years of coevolution. Phylogenetic analyses indicate that this long coevolutionary history includes a third symbiont lineage: specialized microfungal parasites of the ants fungus gardens. At ancient levels, the phylogenies of the three symbionts are perfectly congruent, revealing that the ant-microbe symbiosis is the product of tripartite coevolution between the farming ants, their cultivars, and the garden parasites. At recent phylogenetic levels, coevolution has been punctuated by occasional host-switching by the parasite, thus intensifying continuous coadaptation between symbionts in a tripartite arms race. C1 Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Toronto, Dept Bot, Toronto, ON M5S 3B2, Canada. Univ Texas, Austin, TX 78712 USA. Smithsonian Inst, Natl Museum Nat Hist, MRC 188, Washington, DC 20013 USA. ARS, Insect Biocontrol Lab, USDA, Beltsville, MD 20705 USA. Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP Currie, CR (reprint author), Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. NR 23 TC 194 Z9 204 U1 9 U2 80 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 JAN 17 PY 2003 VL 299 IS 5605 BP 386 EP 388 DI 10.1126/science.1078155 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 635YB UT WOS:000180426800043 PM 12532015 ER PT J AU Bartschat, K Andersen, N AF Bartschat, K Andersen, N TI Electron-impact excitation of He 3 D-1: channel-coupling effects on the orientation, charge cloud, and cross section SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID HELIUM SCATTERING; R-MATRIX; PARAMETERS; STATES; COHERENCE; COLLISION; ENERGIES AB A violation of the propensity rule for positive angular-momentum transfer at small scattering angles in He 1 S-1 --> 3 D-1 electron-impact excitation (Cvejanovic D, McLaughlin D T and Crowe A 2000 J. Phys. B: At. Mol Opt. Phys. 33 3013) has been investigated. The analysis of results from numerical models with an increasing number of coupled states in a close-coupling expansion shows that only the most sophisticated 'convergent close-coupling' and 'R-matrix with pseudo-states' models can reproduce the experimental data. This points to channel-coupling effects as the principal reason for violation of the propensity rule, a conclusion supported by comparing predictions for the angle-integrated cross section from these models. Finally, the component of the charge cloud located along the direction perpendicular to the scattering plane becomes increasingly important with increasing energy. This can also be seen in the accompanying QuickTime movies. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Niels Bohr Inst, Orsted Lab, DK-2100 Copenhagen, Denmark. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Bartschat, K (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Bartschat, Klaus/I-2527-2012 NR 21 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD JAN 14 PY 2003 VL 36 IS 1 BP 163 EP 172 AR PII S0953-4075(03)55658-9 DI 10.1088/0953-4075/36/1/313 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 644WU UT WOS:000180944000019 ER PT J AU Bartschat, K Sadeghpour, HR AF Bartschat, K Sadeghpour, HR TI Ultralow-energy electron scattering from alkaline-earth atoms: the scattering-length limit SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID ULTRACOLD NEUTRAL PLASMA; BOSE-EINSTEIN CONDENSATION; CROSS-SECTION MEASUREMENTS; OSCILLATOR-STRENGTHS; MAGNETOOPTICAL TRAP; R-MATRIX; RESONANCES; COLLISIONS; CREATION; S-3(E) AB We use the non-relativistic R-matrix. method to treat ultralow-energy electron scattering from the alkaline-earth atoms Mg, Ca, and Sr. The sensitivity of the predictions for the scattering length is analysed by comparing results obtained from a variety of structure and collision models. We estimate the electron scattering lengths to be -2.5a(0) for e(-)-Mg, -12a(0) for e(-)-Ca, and -18 a(0) for e(-)-Sr, respectively. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Bartschat, Klaus/I-2527-2012 NR 39 TC 8 Z9 8 U1 0 U2 1 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 JAN 14 PY 2003 VL 36 IS 1 BP L9 EP L15 AR PII S0953-4075(03)54415-7 DI 10.1088/0953-4075/36/1/102 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 644WU UT WOS:000180944000002 ER PT J AU Diaferio, A Nusser, A Yoshida, N Sunyaev, RA AF Diaferio, A Nusser, A Yoshida, N Sunyaev, RA TI Superclusters with thermal Sunyaev-Zel'dovich effect surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : analytical; galaxies : clusters : general; cosmology : miscellaneous; large-scale structure of Universe ID MASS-TEMPERATURE RELATION; X-RAY-CLUSTERS; HUBBLE VOLUME SIMULATIONS; DARK-MATTER UNIVERSES; GALAXY CLUSTERS; HYDRODYNAMIC SIMULATIONS; COSMOLOGICAL PARAMETERS; STATISTICAL PROPERTIES; PECULIAR VELOCITIES; CONSTRAINTS AB We use a simple analytic model to compute the angular correlation function of clusters identified in upcoming thermal Sunyaev-Zel'dovich (SZ) effect surveys. We then compute the expected fraction of close pairs of clusters on the sky that are also close along the line of sight. We show how the expected number of cluster pairs as a function of redshift is sensitive to the assumed biasing relation between the cluster and the mass distribution. We find that, in a Lambda-cold dark matter model, the fraction of physically associated pairs is 70 per cent for angular separations smaller than 20 arcmin and clusters with a specific flux difference larger than 200 mJy at 143 GHz. The agreement of our analytic results with the Hubble volume N -body simulations is satisfactory. These results quantify the feasibility of using SZ surveys to compile catalogues of superclusters at any redshift. C1 Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10124 Turin, Italy. Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. Russian Acad Sci, Space Res Inst IKI, Moscow, Russia. RP Diaferio, A (reprint author), Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10124 Turin, Italy. EM diaferio@ph.unito.it RI Yoshida, Naoki/A-4305-2011 NR 71 TC 11 Z9 11 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2003 VL 338 IS 2 BP 433 EP 442 DI 10.1046/j.1365-8711.2003.06060.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627QP UT WOS:000179945500015 ER PT J AU Cagnoni, I Turolla, R Treves, A Huang, JS Kim, DW Elvis, M Celotti, A AF Cagnoni, I Turolla, R Treves, A Huang, JS Kim, DW Elvis, M Celotti, A TI 1WGA J1216.9+3743: Chandra finds an extremely steep ultraluminous X-ray source SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4244); galaxies : spiral; stars : individual (1WGA J1216. 9+3743); X-rays : galaxies ID GALAXIES; NGC-4244; SEARCH; FIELD AB We report the discovery of a new ultraluminous X-ray source (ULX) in the nearby galaxy NGC 4244 from Chandra archival data. The source, 1WGA J1216.9+3743, is one of the least luminous and softest ULXs discovered so far. Its X-ray spectrum is the best available for a representative of the soft ULXs, a class of sources recently discovered by Chandra and XMM-Newton. 1WGA J1216.9+3743 appears pointlike in the Chandra image and has a complex spectral shape; a multicolor disk model, suitable for brighter ULXs, is inadequate for this source. The 1WGA J1216.9+3743 spectrum is heavily absorbed (N-H similar to 1-4 x 10(21) cm(-2)) and very soft. The best-fit power-law model gives Gamma similar to 5 and implies a luminosity L(0.5-10 keV) similar to 10(39) ergs s(-1). A comparison with previous detections shows that, despite the variability displayed by the source during the Chandra observation, the 1WGA J1216.9+3743 count rate, spectral shape, and absorption are practically unchanged over a 9 yr period. We also performed deep optical imaging of the field containing the X-ray source and found a possible R similar to 23.7 counterpart. C1 Univ Insubria, Dipartimento Sci, I-22100 Como, Italy. Univ Padua, Dipartimento Fis, I-35131 Padua, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SISSA, ISAS, I-34014 Trieste, Italy. RP Cagnoni, I (reprint author), Univ Insubria, Dipartimento Sci, Via Valleggio 11, I-22100 Como, Italy. NR 21 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 JAN 10 PY 2003 VL 582 IS 2 BP 654 EP 658 DI 10.1086/344711 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700009 ER PT J AU Gillespie, EB Geller, MJ Kenyon, SJ AF Gillespie, EB Geller, MJ Kenyon, SJ TI Tidally triggered star formation in close pairs of galaxies. II. Constraints on burst strengths and ages SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : fundamental parameters; galaxies : interactions; galaxies : kinematics and dynamics; galaxies : structure ID SPIRAL GALAXIES; INTERACTING GALAXIES; MERGING GALAXIES; HIERARCHICAL UNIVERSE; ROTATION CURVES; FORMATION RATES; DISK GALAXIES; DARK MATTER; REDSHIFT; BULGES AB Galaxy-galaxy interactions rearrange the baryons in galaxies and trigger substantial star formation; the aggregate effects of these interactions on the evolutionary histories of galaxies in the universe are poorly understood. We combine B- and R-band photometry and optical spectroscopy to estimate the strengths and timescales of bursts of triggered star formation in the centers of 190 galaxies in pairs and compact groups. Based on an analysis of the measured colors and EW(Halpha), we characterize the preexisting and triggered populations separately. The best-fitting burst scenarios assume stronger reddening corrections for line emission than for the continuum and continuous star formation lasting for greater than or similar to 100 Myr. The most realistic scenarios require an initial mass function that is deficient in the highest mass stars. The color of the preexisting stellar population is the most significant source of uncertainty. Triggered star formation contributes substantially (probably greater than or similar to 50%) to the R-band flux in the central regions of several galaxies; tidal tails do not necessarily accompany this star formation. Many of the galaxies in our sample have bluer centers than outskirts, suggesting that pre- or nonmerger interactions may lead to evolution along the Hubble sequence. These objects would appear blue and compact at higher redshifts; the older, redder outskirts of the disks would be difficult to detect. Our data indicate that galaxies with larger separations on the sky contain weaker, and probably older, bursts of star formation on average. However, confirmation of these trends requires further constraints on the colors of the older stellar populations and on the reddening for individual galaxies. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Gillespie, EB (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 62 TC 49 Z9 49 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 JAN 10 PY 2003 VL 582 IS 2 BP 668 EP 688 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700011 ER PT J AU Lewis, KT Burrows, DN Hughes, JP Slane, PO Garmire, GP Nousek, JA AF Lewis, KT Burrows, DN Hughes, JP Slane, PO Garmire, GP Nousek, JA TI The radial structure of supernova remnant N103B SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Large Magellanic Cloud, N103B); Magellanic Clouds; supernova remnants; X-rays : ISM ID LARGE-MAGELLANIC-CLOUD; HEAVY-ELEMENTS; ABUNDANCES; EMISSION; SPECTROSCOPY; CHANDRA; GALAXY; IRON; IA AB We report on the results from a Chandra ACIS observation of the young, compact, supernova remnant N103B. The unprecedented spatial resolution of Chandra reveals subarcsecond structure, in both the brightness and spectral variations. Underlying these small-scale variations is a surprisingly simple radial structure in the equivalent widths of the strong Si and S emission lines. We investigate these radial variations through spatially resolved spectroscopy, using a plane-parallel, nonequilibrium ionization model with multiple components. The majority of the emission arises from components with a temperature of 1 keV: a fully ionized hydrogen component; a high ionization timescale (n(e)t > 10(12) s cm(-3)) component containing Si, S, Ar, Ca, and Fe; and a low ionization timescale (n(e)t similar to 10(11) s cm(-3)) O, Ne, and Mg component. To reproduce the strong Fe Kalpha line, it is necessary to include additional Fe in a hot ( > 2 keV), low ionization timescale (n(e)t 10(10.8) s cm(-3)) component. This hot Fe might be in the form of hot Fe bubbles, formed in the radioactive decay of clumps of Ni-56. We find no radial variation in the ionization timescales or temperatures of the various components. Rather, the Si and S equivalent widths increase at large radii because these lines, as well as those of Ar and Ca, are formed in a shell occupying the outer half of the remnant. A shell of hot Fe is located interior to this, but there is a large region of overlap between these two shells. In the inner 30% of the remnant, there is a core of cooler, 1 keV Fe. We find that the distribution of the ejecta and the yields of the intermediate-mass species are consistent with model prediction for Type Ia events. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lewis, KT (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. NR 29 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 JAN 10 PY 2003 VL 582 IS 2 BP 770 EP 782 DI 10.1086/344717 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700016 ER PT J AU Bergin, EA Kaufman, MJ Melnick, GJ Snell, RL Howe, JE AF Bergin, EA Kaufman, MJ Melnick, GJ Snell, RL Howe, JE TI A survey of 557 GHz water vapor emission in the NGC 1333 molecular cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : individual (NGC 1333 molecular cloud); ISM : jets and outflows; ISM : molecules; stars : formation; submillimeter ID WAVE-ASTRONOMY-SATELLITE; SHOCKED INTERSTELLAR CLOUDS; NONTHERMAL INTERNAL ENERGY; IR IMAGING PHOTOMETRY; C-TYPE SHOCKS; OXYGEN CHEMISTRY; STAR-FORMATION; YOUNG STARS; NGC-1333; GAS AB Using NASA's Submillimeter Wave Astronomy Satellite (SWAS), we have examined the production of water in quiescent and shocked molecular gas through a survey of the 556.936 GHz 1(10)-1(01) transition of ortho-H2O in the NGC 1333 molecular core. These observations reveal broad emission lines associated with the IRAS 2, IRAS 4, IRAS 7, and HH 7-11 outflows. Toward three positions we detect narrow (Deltav similar to 2-3 km s(-1)) emission lines clearly associated with the ambient gas. The SWAS observations, with a resolution of similar to4', are supplemented with observations from the Infrared Space Observatory (ISO) and by an unbiased survey of a similar to17' x 15' area, with similar to50" resolution, in the low-J transitions of CO, (CO)-C-13, (CO)-O-18, N2H+, CH3OH, and SiO. Using these combined data sets, with consistent assumptions, we find beam-averaged ortho-H2O abundances of greater than 10(-6) relative to H-2 for all four outflows. A comparison of SWAS and ISO water data is consistent with nondissociative shock models, provided the majority of the ortho-H2O(1(10)-1(01)) emission arises from cool postshock material with enhanced abundances. In the ambient gas the ortho-H2O abundance is found to lie between 0.1 x 10(-7) and 1 x 10(-7) relative to H-2 and is enhanced when compared to cold prestellar molecular cores. A comparison of the water emission with tracers of dense condensations and shock chemistry finds no clear correlation. However, the water emission appears to be associated with the presence of luminous external heating sources that power the reflection nebula and the photodissociation region (PDR). Simple PDR models are capable of reproducing the water and high-J (CO)-C-13 emission, suggesting that a PDR may account for the excitation of water in low-density undepleted gas, as suggested by Spaans van Dishoeck. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Bergin, EA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 65 TC 27 Z9 27 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 JAN 10 PY 2003 VL 582 IS 2 BP 830 EP 845 DI 10.1086/344674 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700021 ER PT J AU Matsuyama, I Johnstone, D AF Matsuyama, I Johnstone, D TI Viscous diffusion and photoevaporation of stellar disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; planetary systems : protoplanetary disks; stars : formation ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; GIANT PLANETS; YOUNG OBJECTS; MASSIVE STARS; ORION-NEBULA; MODELS; ULTRAVIOLET AB The evolution of a stellar disk under the influence of viscous evolution, photoevaporation from the central source, and photoevaporation by external stars is studied. We take the typical parameters of T Tauri stars (TTSs) and the Trapezium Cluster conditions. The photoionizing flux from the central source is assumed to arise from both the quiescent star and accretion shocks at the base of stellar magnetospheric columns, along which material from the disk accretes. The accretion flux is calculated self-consistently from the accretion mass-loss rate. We find that the disk cannot be entirely removed using only viscous evolution and photoionization from the disk-star accretion shock. However, when FUV photoevaporation by external massive stars is included, the disk is removed in 10(6)-10(7) yr, and when EUV photoevaporation by external massive stars is included, the disk is removed in 10(-5)-10(6) yr. An intriguing feature of photoevaporation by the central star is the formation of a gap in the disk at late stages of the disk evolution. As the gap starts forming, viscous spreading and photoevaporation work in resonance. When viscous accretion and photoevaporation by the central star and external massive stars are considered, the disk shrinks and is truncated at the gravitational radius, where it is quickly removed by the combination of viscous accretion, viscous spreading, photoevaporation from the central source, and photoevaporation by the external stars. There is no gap formation for disks nearby external massive stars because the outer annuli are quickly removed by the dominant EUV flux. On the other hand, at larger, more typical distances (d >> 0.03 pc) from the external stars the flux is FUV-dominated. As a consequence, the disk is efficiently evaporated at two different locations, forming a gap during the last stages of the disk evolution. C1 Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matsuyama, I (reprint author), Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. OI Matsuyama, Isamu/0000-0002-2917-8633 NR 35 TC 78 Z9 78 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 JAN 10 PY 2003 VL 582 IS 2 BP 893 EP 904 DI 10.1086/344638 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700025 ER PT J AU Garnavich, PM Stanek, KZ Wyrzykowski, L Infante, L Bendek, E Bersier, D Holland, ST Jha, S Matheson, T Kirshner, RP Krisciunas, K Phillips, MM Carlberg, RG AF Garnavich, PM Stanek, KZ Wyrzykowski, L Infante, L Bendek, E Bersier, D Holland, ST Jha, S Matheson, T Kirshner, RP Krisciunas, K Phillips, MM Carlberg, RG TI Discovery of the low-redshift optical afterglow of GRB 011121 and its progenitor supernova SN 2001ke SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; supernovae : general; supernovae : individual (SN 2001ke) ID GAMMA-RAY BURSTS; STELLAR PHOTOMETRY; STANDARD STARS; DUST ECHOES; SPECTRA; GALAXY; PROGRAM; WFPC2 AB We present the discovery and follow-up observations of the afterglow of the gamma-ray burst GRB 011121 and its associated supernova SN 2001ke. Images were obtained with the Optical Gravitational Lensing Experiment 1.3 m telescope in BVRI passbands, starting 10.3 hr after the burst. The temporal analysis of our early data indicates a steep decay, independent of wavelength, with F-nu proportional to t(-1.72+/-0.05). There is no evidence for a break in the light curve earlier than 2.5 days after the burst. The spectral energy distribution determined from the early broadband photometry is a power law with Fnu proportional to nu(-0.66+/-0.13) after correcting for a large reddening. Spectra obtained with the Magellan 6.5 m Baade telescope reveal narrow emission lines from the host galaxy that provide a redshift of z = 0.362 +/- 0.001 to the GRB. We also present late R - and J-band observations of the afterglow similar to7-17 days after the burst. The late-time photometry shows a large deviation from the initial decline, and our data combined with Hubble Space Telescope photometry provide strong evidence for a supernova peaking about 12 rest-frame days after the GRB. The first spectrum ever obtained of a GRB supernova at cosmological distance revealed a blue continuum. SN 2001ke was more blue near maximum than SN 1998bw and faded more quickly, which demonstrates that a range of properties are possible in supernovae that generate GRBs. The blue color is consistent with a supernova interacting with circumstellar gas, and this progenitor wind is also evident in the optical afterglow. This is the best evidence to date that classical, long GRBs are generated by core-collapse supernovae. C1 Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Pontificia Univ Catolica Chile, Santiago 22, Chile. Cerro Tololo Interamer Observ, Tucson, AZ 85719 USA. Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. Univ Toronto, Dept Astron, Toronto, ON M5S 3H8, Canada. RP Garnavich, PM (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. RI Carlberg, Raymond/I-6947-2012 OI Carlberg, Raymond/0000-0002-7667-0081 NR 65 TC 126 Z9 128 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 JAN 10 PY 2003 VL 582 IS 2 BP 924 EP 932 DI 10.1086/344785 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700029 ER PT J AU Tomsick, JA Corbel, S Fender, R Miller, JM Orosz, JA Tzioumis, T Wijnands, R Kaaret, P AF Tomsick, JA Corbel, S Fender, R Miller, JM Orosz, JA Tzioumis, T Wijnands, R Kaaret, P TI X-ray jet emission from the black hole X-ray binary XTE J1550-564 with Chandra in 2000 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; accretion, accretion disks; black hole physics; stars : individual (XTE J1550-564); stars : winds, outflows; X-rays : stars ID RELATIVISTIC JETS; GALAXY; EJECTION; STATE AB We have discovered an X-ray jet due to material ejected from the black hole X-ray transient XTE J1550-564. The discovery was first reported in 2002 by Corbel and coworkers, and here we present an analysis of the three Chandra observations made between 2000 June and September. For these observations, a source is present that moves in an eastward direction away from the point source associated with the compact object. The separation between the new source and the compact object changes from 21."3 in June to 23."4 in September, implying a proper motion of 21.2 +/- 7.2 mas day(-1), a projected separation of 0.31-0.85 pc, and an apparent jet velocity between 0.34 +/- 0.12 and 0.93 +/- 0.32 times the speed of light for a source distance range of d = 2.8-7.6 kpc. These observations represent the first time that an X-ray jet proper-motion measurement has been obtained for any accretion-powered Galactic or extragalactic source. While this work deals with the jet to the east of the compact object, the western jet has also been detected in the X-ray and radio bands. The most likely scenario is that the eastern jet is the approaching jet and that the jet material was ejected from the black hole in 1998. Along with a 1998 VLBI proper-motion measurement, the Chandra proper motion indicates that the eastern jet decelerated between 1998 and 2000. There is evidence that the eastern jet is extended by +/-2"-3" in the direction of the proper motion. The upper limit on the source extension in the perpendicular direction is +/-1."5, which corresponds to a jet opening angle of less than 7.degrees5. The X-ray jet energy spectrum is well but not uniquely described by a power law with an energy index of alpha = -0.8 +/- 0.4 (S-nu proportional to nu(alpha)) and interstellar absorption. The eastern jet was also detected in the radio band during an observation made within 7.4 days of the June Chandra observation. The overall radio flux level is consistent with an extrapolation of the X-ray power law with alpha = -0.6. The 0.3-8 keV X-ray jet luminosity is in the range (3-24) x 10(32) ergs s(-1) for the June observation using the distance range above but is a factor of similar to2-3 lower for the later observations. We cannot definitively determine the X-ray emission mechanism, but a synchrotron origin is viable and may provide the simplest explanation for the observations. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Ctr Etud Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Paris 07, F-91191 Gif Sur Yvette, France. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Space Res Ctr, Cambridge, MA 02139 USA. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tomsick, JA (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, Code 0424, La Jolla, CA 92093 USA. NR 48 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 JAN 10 PY 2003 VL 582 IS 2 BP 933 EP 944 DI 10.1086/344703 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700030 ER PT J AU Kaaret, P Corbel, S Tomsick, JA Fender, R Miller, JM Orosz, JA Tzioumis, AK Wijnands, R AF Kaaret, P Corbel, S Tomsick, JA Fender, R Miller, JM Orosz, JA Tzioumis, AK Wijnands, R TI X-ray emission from the jets of XTE J1550-564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (XTE J1550-564); stars : winds, outflows; X-rays : binaries ID RELATIVISTIC JETS; EJECTION; GALAXY AB We report on X-ray observations of the large-scale jets recently discovered in the radio and detected in X-rays from the black hole candidate X-ray transient and microquasar XTE J1550-564. On 2002 March 11, X-ray emission was detected 23" to the west of the black hole candidate and was extended along the jet axis with an FWHM of 1."2 and a full width at 10% of maximum intensity of 5". The morphology of the X-ray emission matched well to that of the radio emission at the same epoch. The jet moved by 0".52+/-0".13 between 2002 March 11 and June 19. The apparent speed during that interval was 5.2+/-1.3 mas day(-1). This is significantly less than the average apparent speed of 18.1+/-0.4 mas day(-1) from 1998 to 2002, assuming that the jet was ejected in 1998 September, and indicates that the jet has decelerated. The X-ray spectrum is adequately described by a power law with a photon index near 1.8 subject to interstellar absorption. The unabsorbed X-ray flux was 3.4x10(-13) ergs cm(-2) s(-1) in the 0.3-8 keV band in 2002 March and decreased to 2.9x10(-13) ergs cm(-2) s(-1) in June. We also detect X-rays from the eastern jet in 2002 March and show that it has decelerated and dimmed since the previous detections in 2000. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Paris 07, F-91191 Gif Sur Yvette, France. Ctr Etud Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Calif San Diego, Ctr Astrophys & Space Sci, 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. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 50 Z9 50 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 JAN 10 PY 2003 VL 582 IS 2 BP 945 EP 953 DI 10.1086/344540 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700031 ER PT J AU Weck, PF Schweitzer, A Stancil, PC Hauschildt, PH Kirby, K AF Weck, PF Schweitzer, A Stancil, PC Hauschildt, PH Kirby, K TI The molecular line opacity of MgH in cool stellar atmospheres SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular data; stars : atmospheres; stars : late-type ID MODEL ATMOSPHERES; GIANT STARS; MAGNESIUM; ABUNDANCES; SPECTRUM; HYDRIDE AB A new, complete, theoretical rotational and vibrational line list for the A (2)Pi<--X (2)Sigma(+) electronic transition in MgH is presented. The list includes transition energies and oscillator strengths for all possible allowed transitions and was computed using the best available theoretical potential energies and dipole transition moment function with the former adjusted to account for experimental data. The A<--X line list as well as new line lists for the B' (2)Sigma(+)<--X (2)Sigma(+) and the X (2)Sigma(+)<--X (2)Sigma(+) (pure rovibrational) transitions were included in comprehensive stellar atmosphere models for M, L, and T dwarfs and solar-type stars. The resulting spectra, when compared to models lacking MgH, show that MgH provides significant opacity in the visible between 4400 and 5600 Angstrom. Further comparison of the spectra obtained with the current line list to spectra obtained using the line list constructed by Kurucz show that the Kurucz list significantly overestimates the opacity due to MgH, particularly for the bands near 5150 and 4800 Angstrom, with the discrepancy increasing with decreasing effective temperature. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Weck, PF (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. OI , Philippe/0000-0002-7610-2893 NR 25 TC 46 Z9 46 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 JAN 10 PY 2003 VL 582 IS 2 BP 1059 EP 1065 DI 10.1086/344722 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700041 ER PT J AU Weck, PF Stancil, PC Kirby, K AF Weck, PF Stancil, PC Kirby, K TI B ' <- X rovibrationally resolved photodissociation of (MgH)-Mg-24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular data; molecular processes AB New accurate photodissociation cross sections have been obtained for the B' (2)Sigma(+) <-- X (2)Sigma(+) transition of (MgH)-Mg-24 using a combination of ab initio and experimentally derived potential curves and dipole transition moments. The partial cross sections have been evaluated for all rotational transitions from the vibrational levels v"=0-11 and over the entire accessible wavelength range lambdalambda1770-4560 Angstrom. In particular, all shape resonances arising from rotational predissociation of quasi-bound levels of the B' state have been obtained near threshold. Assuming a Boltzmann distribution of the rovibrational levels of the X (2)Sigma(+), LTE photodissociation cross sections are presented for temperatures between 1000 and 10,000 K. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. EM weck@physast.uga.edu; stancil@physast.uga.edu; kirby@cfa.harvard.edu OI , Philippe/0000-0002-7610-2893 NR 14 TC 13 Z9 13 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 JAN 10 PY 2003 VL 582 IS 2 BP 1263 EP 1268 DI 10.1086/344672 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KP UT WOS:000180282700056 ER PT J AU Hughes, JP Ghavamian, P Rakowski, CE Slane, PO AF Hughes, JP Ghavamian, P Rakowski, CE Slane, PO TI Iron-rich ejecta in the supernova remnant DEM L71 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (DEM L71, SNR 0505-67.9); nuclear reactions, nucleosynthesis, abundances; shock waves; supernova remnants; X-rays : ISM ID LARGE-MAGELLANIC-CLOUD; SOFT-X-RAY; ABUNDANCES; SPECTRUM AB Chandra X-ray observations of DEM L71, a supernova remnant (SNR) in the Large Magellanic Cloud (LMC), reveal a clear double-shock morphology consisting of an outer blast-wave shock surrounding a central bright region of reverse-shock-heated ejecta. The abundances of the outer shock are consistent with LMC values, while the ejecta region shows enhanced abundances of Si, Fe, and other species. However, oxygen is not enhanced in the ejecta; the Fe/O abundance ratio there is greater than or similar to5 times the solar ratio. Based on the relative positions of the blast-wave shock and the contact discontinuity in the context of SNR evolutionary models, we determine a total ejecta mass of similar to1.5 M-circle dot. Ejecta mass estimates based on emission measures derived from spectral fits are subject to considerable uncertainty because of the lack of knowledge of the true contribution of hydrogen continuum emission. Maximal mass estimates, i.e., assuming no hydrogen, result in 1.5 M-circle dot of Fe and 0.24 M-circle dot of Si. Under the assumption that an equal quantity of hydrogen has been mixed into the ejecta, we estimate 0.8 M-circle dot of Fe and 0.12 M-circle dot of Si. These characteristics support the view that in DEM L71, we see Fe-rich ejecta from a Type Ia supernova several thousand years after explosion. C1 Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hughes, JP (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. NR 18 TC 49 Z9 49 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 JAN 10 PY 2003 VL 582 IS 2 BP L95 EP L99 DI 10.1086/367760 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633KQ UT WOS:000180282800009 ER PT J AU Kemp, RA Trueman, CN AF Kemp, RA Trueman, CN TI Rare earth elements in Solnhofen biogenic apatite: geochemical clues to the palaeoenvironment SO SEDIMENTARY GEOLOGY LA English DT Article DE Solnhofen; geochemistry; coprolites; apatite; REE; palaeoenvironment ID PHOSPHATE; MINERALIZATION; TAPHONOMY; FOSSILS; OCEANS; WATERS; DECAY; BONE AB Rare earth element (REE) concentrations in biogenic apatite samples (coprolite, bone and soft-tissue) were used to investigate the environment of deposition of the celebrated Solnhofen fossil Lagerstatten. The measured REE patterns are similar between different localities, lithologies (flinz, faule) and levels in the Upper Solnhofen Plattenkalk, suggestive of a stable REE supply during deposition. The behaviour of cerium in the Solnhofen samples implies that bottom water conditions were not anoxic, and variations in the cerium anomaly can be explained by differences in burial rate. These results provide further geochemical support for current depositional models [Barthel, K.W., 1978. Solnhofen: Ein Blick in die Erdgeschichtc. Ott Verlag, Thun.; Barthel, K.W.; Swinburne, N.H.M., Conway Morris, S., 1990, Solnhofen. A Study in Mesozoic Palaeontology. Cambridge Univ. Press, Cambridge.] that propose that extra-basinal processes are responsible for the interbedded nature of the Solnhofen deposits, rather than intra-basinal processes such as water turnover events. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Olveston Court, Bristol BS35 4DU, Avon, England. Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. RP Trueman, CN (reprint author), Museum Natl Hist Nat, Smithsonian Inst, Dept Paleobiol, 10th & Constitut Ave NW, Washington, DC 20560 USA. RI Trueman, Clive/E-6925-2011 NR 45 TC 39 Z9 42 U1 0 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0037-0738 J9 SEDIMENT GEOL JI Sediment. Geol. PD JAN 10 PY 2003 VL 155 IS 1-2 BP 109 EP 127 AR PII S0037-0738(02)00163-X DI 10.1016/S0037-0738(02)00163-X PG 19 WC Geology SC Geology GA 636EH UT WOS:000180441200007 ER PT J AU Catlos, EJ Sorensen, SS AF Catlos, EJ Sorensen, SS TI Phengite-based chronology of K- and Ba-rich fluid flow in two paleosubduction zones SO SCIENCE LA English DT Article ID FRANCISCAN COMPLEX; SUBDUCTION ZONES; CALIFORNIA; ECLOGITES; SERPENTINITE; AMPHIBOLITES; METAMORPHISM; ENRICHMENT; BLUESCHIST; BLOCKS AB Subduction recycles aqueous fluids from slab and sediment to the mantle. Subduction zones are long-lived, but time scales for fluid-rock interaction within subduction complexes are uncertain. Large-ion lithophile elements (potassium and barium) were added to eclogite (subducted basalt) during high pressure/temperature metamorphism via phengite crystallization from subduction zone fluids. Phengite grains from eclogite blocks and their metasomatic selvages yielded Ar-40/Ar-39 ages across grains and between samples that indicate 25 and 60 million years of fluid-rock interaction in the Samana Complex, Dominican Republic, and the Franciscan Complex, California, respectively. C1 Oklahoma State Univ, Sch Geol, Noble Res Ctr 105, Stillwater, OK 74078 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Catlos, EJ (reprint author), Oklahoma State Univ, Sch Geol, Noble Res Ctr 105, Stillwater, OK 74078 USA. RI Catlos, Elizabeth/B-7943-2011 NR 25 TC 38 Z9 38 U1 0 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 JAN 3 PY 2003 VL 299 IS 5603 BP 92 EP 95 DI 10.1126/science.1076977 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 631JZ UT WOS:000180165800039 PM 12511647 ER PT S AU Tong, CYE Meledin, D Loudkov, D Blundell, R Erickson, N Kawamura, J Mehdi, I Gol'tsman, G AF Tong, CYE Meledin, D Loudkov, D Blundell, R Erickson, N Kawamura, J Mehdi, I Gol'tsman, G BE Thal, H TI A 1.5 THz hot-electron bolometer mixer operated by a planar diode based local oscillator SO 2003 IEEE MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM DIGEST, VOLS 1-3 SE IEEE MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM DIGEST LA English DT Proceedings Paper CT IEEE MTT-S International Microwave Symposium CY JUN 08-13, 2003 CL PHILADELPHIA, PA SP IEEE MTT S ID HETERODYNE RECEIVER AB We have developed a 1.5 THz superconducting NbN Hot-Electron Bolometer mixer. It is operated by an all-solid-state Local Oscillator comprising of a cascade of 4 planar doublers following an MMIC based W-band power amplifier. The threshold available pump power is estimated to be 1 muW. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Tong, Edward/0000-0002-7736-4203 NR 11 TC 5 Z9 5 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-645X BN 0-7803-7695-1 J9 IEEE MTT-S PY 2003 BP 751 EP 754 DI 10.1109/MWSYM.2003.1212480 PG 4 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BX04J UT WOS:000184045100227 ER PT S AU Calvet, N AF Calvet, N BE Beskin, V Henri, G Menard, F Pelletier, G Dailbard, J TI Accretion signatures in young stellar objects SO ACCRETION DISCS, JETS AND HIGH ENERGY PHENOMENA IN ASTROPHYSICS SE LES HOUCHES SUMMER SCHOOL SESSION LA English DT Proceedings Paper CT Les Houches Session 78th on Accretion Discs, Jets and High Energy Phenomena in Astrophysics CY JUL 29-AUG 23, 2002 CL Les Houches, FRANCE SP NATO Adv Study Inst, Eur Summer Sch, Ecole Themat CNRS ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; AURIGA MOLECULAR CLOUD; EMISSION-LINE DIAGNOSTICS; MAIN-SEQUENCE EVOLUTION; INTERMEDIATE-MASS STARS; HERBIG AE/BE STARS; FU-ORIONIS OBJECTS; DISK ACCRETION; MAGNETOSPHERIC ACCRETION AB Mass accretion onto the star is taken place in young stellar objects, providing the energy needed to power the excess emission observed at all wavelength bands. Signatures that allow us to identify and quantify accretion processes are reviewed in these lectures. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Calvet, N (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 88 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0924-8099 BN 3-540-20171-8 J9 LES HOUCH S PY 2003 VL 78 BP 521 EP 548 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BY82H UT WOS:000189471600011 ER PT S AU Hartmann, L AF Hartmann, L BE Beskin, V Henri, G Menard, F Pelletier, G Dailbard, J TI Evolution of YSO disks SO ACCRETION DISCS, JETS AND HIGH ENERGY PHENOMENA IN ASTROPHYSICS SE LES HOUCHES SUMMER SCHOOL SESSION LA English DT Proceedings Paper CT Les Houches Session 78th on Accretion Discs, Jets and High Energy Phenomena in Astrophysics CY JUL 29-AUG 23, 2002 CL Les Houches, FRANCE SP NATO Adv Study Inst, Eur Summer Sch, Ecole Themat CNRS ID YOUNG STELLAR OBJECTS; MAGNETIZED ACCRETION DISKS; AURIGA MOLECULAR CLOUD; X-RAY IONIZATION; T-TAURI DISKS; PROTOSTELLAR DISKS; FU ORIONIS; PROTOPLANETARY DISKS; STAR-FORMATION; SOLAR NEBULA AB As stars and planets form from accretion processes in disks, it is important to understand these processes and their evolutionary implications. While much remains unclear, it seems likely that the accretion of material through protoplanetary disks is driven by some combination of the magnetorotational instability and gravitational torques. Angular momentum transport by disk winds can be important, especially in inner disks, but this is unlikely to dominate the overall disk evolution. A key uncertainty in both disk physics and the interpretation of observations is the rate and manner of dust particle growth. Finally, the ultimate fate of the gas component in protoplanetary disks remains unclear for systems not in proximity to hot stars with strong photodonizing radiation. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hartmann, L (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 65 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0924-8099 BN 3-540-20171-8 J9 LES HOUCH S PY 2003 VL 78 BP 549 EP 582 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BY82H UT WOS:000189471600012 ER PT J AU Linares, OF AF Linares, OF TI Going to the city ... and coming back? Turnaround migration among the Jola of Senegal SO AFRICA LA English DT Article ID CASAMANCE AB The Jola of Lower Casamance in southern Senegal are involved in 'turnaround' (or circular), rural to urban migration. Using data from three Jola communities located in different geographical and cultural sub-regions, this article compares the dynamics of migration among the villages and explores variations along gender and generational lines. Special emphasis is placed on the number of young unmarried girls and boys who return to the village during the rainy season to help their parents with agricultural work. It has been argued that the movement of people from the countryside to the city has had a negative effect on local food production. 'Turnaround migration' mitigates to some extent the impact of the rural exodus on rural communities. It has important implications of its own for the future of agriculture in the various Jola sub-regions. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Linares, OF (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. NR 32 TC 12 Z9 12 U1 0 U2 4 PU EDINBURGH UNIV PRESS PI EDINBURGH PA TRADE DEPT, 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0001-9720 J9 AFRICA JI Africa PY 2003 VL 73 IS 1 BP 113 EP 132 PG 20 WC Anthropology; Area Studies SC Anthropology; Area Studies GA 700VY UT WOS:000184132900006 ER PT J AU Ubelaker, DH Owsley, DW AF Ubelaker, DH Owsley, DW TI Isotopic evidence for diet in the seventeenth-century colonial chesapeake SO AMERICAN ANTIQUITY LA English DT Article ID STABLE CARBON-ISOTOPE; BONE-COLLAGEN; TERRESTRIAL COMPONENTS; HUMAN SKELETONS; NITROGEN; RATIOS; MARINE; ANIMALS AB Excavations of colonial period sites in Maryland and Virginia have produced human remains dating to the seventeenth century. In this study, we analyze stable isotopes of carbon and nitrogen from these remains to explore aspects of the diets of the individuals represented. Analyses of both stable carbon and nitrogen isotopes were conducted on preserved protein while stable carbon isotope analysis was also conducted on preserved biological apatite. Carbon isotope values (delta(13)Cparts per thousand) ranged from -10.5 to -20.5 for collagen and -5.1 to -12.5 for bioapatite. Nitrogen isotope values (delta(15)Nparts per thousand) ranged from 9.9 to 14.4. The data suggest dietary diversity among the individuals examined. Three factors contribute to this diversity: the availability of maize, variation in immigration histories of the individuals, and the differing lengths of time they spent in the American colonies. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Anthropol, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Anthropol, MRC 112, Washington, DC 20560 USA. NR 55 TC 6 Z9 6 U1 0 U2 6 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 0002-7316 J9 AM ANTIQUITY JI Am. Antiq. PD JAN PY 2003 VL 68 IS 1 BP 129 EP 139 DI 10.2307/3557036 PG 11 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 640EN UT WOS:000180675200007 ER PT J AU Levin, RA Wagner, WL Hoch, PC Nepokroeff, M Pires, JC Zimmer, EA Sytsma, KJ AF Levin, RA Wagner, WL Hoch, PC Nepokroeff, M Pires, JC Zimmer, EA Sytsma, KJ TI Family-level relationships of Onagraceae based on chloroplast rbcL and ndhF data SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Camissonia; Megacorax; ndhF; Oenothera; Onagraceae; Onagreae; phylogeny; rbcL ID SEQUENCE DATA; PHYLOGENETIC-RELATIONSHIPS; TRIBAL RELATIONSHIPS; DNA; EVOLUTION; SYSTEMATICS; MYRTALES; INCONGRUENCE; LIMITS AB Despite intensive morphological and molecular studies of Onagraceae, relationships within the family are not fully understood. One drawback of previous analyses is limited sampling within the large tribe Onagreae. In addition, the monophyly of two species-rich genera in Onagreae, Camissonia and Oenothera, has never been adequately tested. To understand relationships within Onagraceae, test the monophyly of these two genera, and ascertain the affinities of the newly discovered genus Megacorax, we conducted parsimony and maximum likelihood analyses with rbcL and ndhF sequence data for 24 taxa representing all 17 Onagraceae genera and two outgroup Lythraceae. Results strongly support a monophyletic Onagraceae, with Ludwigia as the basal lineage and a sister-taxon relationship between Megacorax and Lopezia. Gongylocarpus is supported as sister to Epilobieae plus the rest of Onagreae, although relationships within the latter clade have limited resolution. Thus, we advocate placement of Gongylocarpus in a monogeneric tribe, Gongylocarpeae. Most relationships within Onagreae are weakly resolved, suggesting a rapid diversification of this group in western North America. Neither Camissonia nor Oenothera appears to be monophyletic; however, increased taxon sampling is needed to clarify those relationships. Morphological characters generally agree with the molecular data, providing further support for relationships. C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. Missouri Bot Garden, St Louis, MO 63166 USA. Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA. Univ Wisconsin, Dept Agron, Madison, WI 53706 USA. Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. RP Wagner, WL (reprint author), Smithsonian Inst, Dept Systemat Biol, MRC 166,POB 37012, Washington, DC 20013 USA. RI Zimmer, Elizabeth/G-3890-2011; OI Pires, J Chris/0000-0001-9682-2639 NR 45 TC 87 Z9 92 U1 5 U2 25 PU BOTANICAL SOC AMER INC PI COLUMBUS PA OHIO STATE UNIV-DEPT BOTANY, 1735 NEIL AVE, COLUMBUS, OH 43210 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD JAN PY 2003 VL 90 IS 1 BP 107 EP 115 DI 10.3732/ajb.90.1.107 PG 9 WC Plant Sciences SC Plant Sciences GA 683DQ UT WOS:000183132800012 PM 21659085 ER PT J AU Alemseged, Z Bobe, R Geraads, D AF Alemseged, Z Bobe, R Geraads, D TI Hominid environments and faunal change in the lower Omo, valley, Ethiopia: A comparison of the French and American databases. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA. Smithsonian Inst, Washington, DC 20560 USA. CNRS, Paris, France. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 57 EP 58 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000012 ER PT J AU Behrensmeyer, AK Alemseged, Z Bobe, R AF Behrensmeyer, AK Alemseged, Z Bobe, R TI Key issues in the analysis of faunal changes across the East African Pliocene. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Washington, DC 20560 USA. Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 64 EP 64 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000037 ER PT J AU Bobe, R Behrensmeyer, AK Eck, G Leakey, L AF Bobe, R Behrensmeyer, AK Eck, G Leakey, L TI A comparative approach to faunal analysis in the Hadar and Turkana regions. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Washington, Seattle, WA 98195 USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 69 EP 69 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000057 ER PT J AU Fan, J Ortner, DJ Frohlich, B Martin, D AF Fan, J Ortner, DJ Frohlich, B Martin, D TI Brucellosis in antiquity: An analysis of possible cases of brucellar sacroilitis. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Massachusetts, Amherst, MA 01003 USA. Smithsonian Inst, Washington, DC 20560 USA. Hampshire Coll, Amherst, MA 01002 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 94 EP 94 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000153 ER PT J AU Gordon, KD Schoeninger, MJ Sears, KE AF Gordon, KD Schoeninger, MJ Sears, KE TI Diet in pre-contact Central California explored through dental microwear and stable isotope analyses. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Calif San Diego, Smithsonian Inst, La Jolla, CA 92093 USA. Univ Calif San Diego, Dept Anthropol, La Jolla, CA 92093 USA. Univ Wisconsin, Dept Anthropol, Madison, WI USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 102 EP 103 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000186 ER PT J AU Mulhern, DM Jones, EB AF Mulhern, DM Jones, EB TI Evidence of subadult scurvy from Kagamil and Shiprock Islands, Alaska. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, NMNH, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 155 EP 156 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000392 ER PT J AU Ousley, SD McKeown, A AF Ousley, SD McKeown, A TI A comparison of morphometric data and methods in classification. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Off Repatriat, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 5 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 162 EP 162 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000417 ER PT J AU Ross, AH Ubelaker, DH AF Ross, AH Ubelaker, DH TI Geomorphometric study of artificially modified crania from coastal Ecuador. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Florida, Maples Ctr Forens Med, Gainesville, FL 32611 USA. Smithsonian Inst, NMNH, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 180 EP 180 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000487 ER PT J AU Weisensee, K Jantz, RL Ousley, S Sivakova, D AF Weisensee, K Jantz, RL Ousley, S Sivakova, D TI Relationships of Slovak Roma populations assessed from finger ridge counts. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA. Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. Comenius Univ, Dept Anthropol, Bratislava 81806, Slovakia. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2003 SU 36 BP 222 EP 222 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 657MB UT WOS:000181670000647 ER PT J AU Post, JE Heaney, PJ Hanson, J AF Post, JE Heaney, PJ Hanson, J TI Synchrotron X-ray diffraction study of the structure and dehydration behavior of todorokite SO AMERICAN MINERALOGIST LA English DT Article ID OCTAHEDRAL MOLECULAR-SIEVES; MANGANESE OXIDE; RIETVELD REFINEMENT; POWDER DIFFRACTION; CATION DISPLACEMENTS; CRYPTOMELANE; HOLLANDITES; CATALYSTS; NODULES; IONS AB Real-time, temperature-resolved synchrotron powder X-ray diffraction data and Rietveld refinements were used to investigate the behavior of the todorokite structure from 100 to 820 K. At 298 K, the lower valence cations, such as Mn3+, occupy large octahedral sites at the edges of the triple chains, and four water/cation sites are in the tunnels. In our heating experiments in vacuum, todorokite began to break down at similar to450 K and fully decomposed by 620 K, at which point hausmannite started to form. Our results suggest that the loss Of O-2 accompanied the reduction of Mn4+ to Mn3+ and Mn2+, and these reactions impelled a breakdown of the octahedral framework and the subsequent release of the tunnel water molecules. Rierveld refinements revealed a gradual thermal expansion of the todorokite structure to similar to450 K. At higher temperatures, the unit-cell volume gradually decreased, primarily as a result of a decrease in c, and the decline in beta with increasing temperature was accelerated. A mechanism for forming the inverse spinel hausmannite structure from todorokite is presented. 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 11793 USA. RP Post, JE (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM post.jeffrey@nmnh.si.edu RI Hanson, jonathan/E-3517-2010 NR 33 TC 36 Z9 41 U1 1 U2 10 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD JAN PY 2003 VL 88 IS 1 BP 142 EP 150 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 635DV UT WOS:000180383600017 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, WN Zatwarnicki, T TI Shore flies of the republic of Seychelles (diptera : ephydridae) SO ANNALES ZOOLOGICI LA English DT Review DE diptera; ephydridae; Seychelles; new species; taxonomy ID INDIAN-OCEAN; REVISION; ALDABRA; GENERA AB Thirty-nine species of the shore-fly family Ephydridae that occur on islands of the Republic of Seychelles are reviewed. Included are keys to the appropriate suprageneric categories, genera, and species. Distributional data for all included species are presented, and new taxa. are described and illustrated. Six new species are described (type locality in parenthesis): Psilopa victoria (Seychelles. Mahe: Roche Caiman Bird Sanctuary; 4degrees38.3'S, 55degrees28.1'E); Cerobothrium insulatum (Seychelles. Mahe: Port Launay; 4degrees39.2'S, 55degrees24.2'E); Schema aldabricum (Aldabra. South Island, Flamingo Pool); Orasiopa apiculata (Seychelles. La Digue: La Passe; 4degrees20.8'S, 55degrees49.8'E); Polytrichophora specula (Seychelles. Mahe: Arise Boileau (4degrees42.5'S, 55degrees28.7'E)); Hyadina munarii (Seychelles. Mahe: Airport). Psilopa giordanii Canzoneri is made a junior subjective synonym of Clasiopella uncinata Hendel, Enchastes scotti Lamb is made a junior subjective synonym of Placopsidella cyno-cephala Kertesz, Hecamedoides pusillus Canzoneri is made junior subjective synonym of Discocerina hepatica de Meijere, Allotrichoma outambense Canzoneri is made a junior subjective synonym of A. argentipraetextum Lamb, and Discocerina (Ditrichophora) rattii Canzoneri is made a junior subjective synonym of Hostis guamensis (Cresson). Asmeringa ligabuei Canzoneri is transferred to the genus Cerobothrium as a new combination. Lectotypes are designated for the following nine species: Discomyza similis Lamb, Ceropsilopa longicornis (Lamb), Psilopa nitidissima Lamb, Allotrichoma argentipraetextum Lamb, Hyadina fenestrata Becker, Zeros fractivirgatus (Lamb), Zeros invenatus (Lamb), Parydra tuberculifera Lamb, Scatella septemfenestrata Lamb. The shore-fly fauna of the Seychelles is diverse, comprising at least 39 species (Table 3), and the populations of these species are generally stable and intact. Most species are adventive to the islands, many apparently being introduced during the last century. Most species have biogeographic connections with the Afrotropical mainland (22 species) and to a lesser extent with the Oriental and Australasian Regions (12 species). The few apparent endemics we identified (7 species or 18%) constitute far less than half the level of endemism that was reported for insect species generally (51%). The freshwater fauna of shore flies on the Seychelles is essentially undeveloped and is comparatively depauperate. C1 Smithsonian Inst, Dept Systemat Biol, Entomol Sect, Washington, DC 20013 USA. Polish Acad Sci, Museum & Inst Zool, PL-00679 Warsaw, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Systemat Biol, Entomol Sect, NHB 169,POB 37012, Washington, DC 20013 USA. OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 138 TC 5 Z9 6 U1 0 U2 0 PU POLISH ACAD OF SCIENCES PI WARSAW PA MUSEUM & INST ZOOLOGY WILCZA 64, 00-679 WARSAW, POLAND SN 0003-4541 J9 ANN ZOOL JI Ann. Zool. PY 2003 VL 53 IS 4 BP 585 EP 650 PG 66 WC Entomology SC Entomology GA 756KC UT WOS:000187463400001 ER PT J AU Breuker, M McNamara, C Young, L Perry, T Young, A Mitchell, R AF Breuker, M McNamara, C Young, L Perry, T Young, A Mitchell, R TI Fungal growth on synthetic cloth from Apollo spacesuits SO ANNALS OF MICROBIOLOGY LA English DT Article DE Apollo spacesuits; Paecilomyces; Cladosporium; biodegradation; synthetic polymers ID MICROORGANISMS; DEGRADATION; PLASTICS; SOIL AB The United States Smithsonian Institution's National Air and Space Museum preserves the world's largest collection of spacesuits and their components relating to the American space program. Included in this collection are historically significant suits from the Apollo lunar missions which took place between 1968 and 1972. The Apollo suits are composed of multiple layers, many of which have begun to degrade. The role of microorganisms in the deterioration of the space suits was investigated in this study. Fungi belonging to the genera Paecilomyces and Cladosporium were cultured from two synthetic polymers contained within the suits. Fungal growth occurred rapidly, and isolates were capable of degrading the synthetic polymers. Scanning electron microscopy was used to observe development of fungal hyphae on individual fibers of the cloth. Our data indicate that the growth of these fungi on the suit materials was a contributing factor to the deterioration of interior layers of the Apollo spacesuits. C1 Harvard Univ, Div Engn & Appl Sci, Microbial Ecol Lab, Cambridge, MA 02138 USA. Smithsonian Inst, Natl Air & Space Museum, Paul E Garber Facil, Suitland, MD 20746 USA. RP Mitchell, R (reprint author), Harvard Univ, Div Engn & Appl Sci, Microbial Ecol Lab, 40 Oxford St, Cambridge, MA 02138 USA. NR 19 TC 7 Z9 7 U1 0 U2 5 PU INST MICROBIOLOGIA PI MILAN PA VIA CELORIA 2, 20133 MILAN, ITALY SN 1590-4261 J9 ANN MICROBIOL JI Ann. Microbiol. PY 2003 VL 53 IS 1 BP 47 EP 54 PG 8 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 670FP UT WOS:000182397000006 ER PT J AU Zanis, MJ Soltis, PS Qiu, YL Zimmer, E Soltis, DE AF Zanis, MJ Soltis, PS Qiu, YL Zimmer, E Soltis, DE TI Phylogenetic analyses and perianth evolution in basal angiosperms SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Review DE basal angiosperms; floral evolution; merosity; perianth; phylogeny ID SEED PLANT PHYLOGENY; 3 GENOMIC COMPARTMENTS; 26S RDNA SEQUENCES; PLASTID GENE RBCL; FLOWERING PLANTS; FLORAL STRUCTURE; COMPARATIVE BIOLOGY; CLADISTIC-ANALYSIS; RIBOSOMAL DNA; DATA SETS AB Using a compartmentalization approach, we conducted phylogenetic analyses of the basalmost extant angiosperms using sequences from six genes (over 12,000 bp per taxon) from all three genomes (chloroplast-atpB, rbcL; nuclear-18S rDNA, 26S rDNA; mitochondrial-matR, atpA). Trees resulting from parsimony and maximum likelihood analyses of the compartmentalized data are identical. We find strong support (100% for each node) for the earliest-branching angiosperms: Amborellaceae, Nymphaeaceae, and an Austrobaileyales clade (Illiciaceae, Schisandraceae, Trimeniaceae, Austrobaileyaceae). Whereas most recent studies using multiple genes provided poor resolution and support for relationships among the remaining basal angiosperms (Ceratophyllaceae, Chloranthaceae, Canellales (= Winterales), Piperales, monocots, Magnoliales, Laurales), with compartmentalization, we find high levels (> 90%) of bootstrap support for relationships among these clades. Canellales and Piperales form a strongly supported (100%) sister group that is, in turn, sister to a well-supported (100%) clade of Laurales and Magnoliales. Canellales + Piperales and Magnoliales + Laurales form a well-supported magnoliid clade. Ceratophyllaceae are strongly supported (100%) as sister to the monocots; the monocot/Ceratophyllaceac clade is well supported (86%) as sister to all remaining angiosperms (Chloranthaceae, the magnoliid clade, and eudicots). The addition of entire 26S rDNA sequences clearly contributed to this increased internal support. We examined the diversification of perianth phyllotaxis, merosity, and differentiation using our phylogenetic hypothesis for angiosperms. Ancestral perianth phyllotaxis and merosity are equivocal for each node of the Amborellaceac, Nymphaeaceae, Austrobaileyales grade; however, an undifferentiated perianth is reconstructed as the ancestral state for the angiosperms. Trimery and whorled perianth phyllotaxis have played a major role in basal angiosperm perianth evolution and represent the ancestral states for the large clade comprising all angiosperms other than Amborella, Nymphaeaceae, and Austrobaileyales. A differentiated perianth has apparently evolved multiple times. C1 Univ Florida, Dept Bot, Gainesville, FL 32611 USA. Univ Florida, Florida Museum Nat Hist & Genet Inst, Gainesville, FL 32611 USA. Univ Michigan, Dept Ecol & Evolut Biol, Ann Arbor, MI 48109 USA. Smithsonian Inst, Lab Mol Systemat, Washington, DC 20560 USA. Univ Florida, Inst Genet, Gainesville, FL 32611 USA. Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. RP Soltis, DE (reprint author), Univ Florida, Dept Bot, Gainesville, FL 32611 USA. RI Still, Shannon/B-5103-2010; Zimmer, Elizabeth/G-3890-2011; Soltis, Pamela/L-5184-2015 NR 168 TC 105 Z9 118 U1 2 U2 13 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 2003 VL 90 IS 2 BP 129 EP 150 DI 10.2307/3298579 PG 22 WC Plant Sciences SC Plant Sciences GA 692CT UT WOS:000183643300001 ER PT J AU Lada, CJ Lada, EA AF Lada, CJ Lada, EA TI Embedded clusters in molecular clouds SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS LA English DT Article DE clusters; star formation; initial mass function; circumstellar disks; brown dwarfs ID INITIAL MASS FUNCTION; YOUNG STELLAR OBJECTS; ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; OPHIUCHI DARK CLOUD; T-TAURI STARS; LARGE-MAGELLANIC-CLOUD; IR IMAGING PHOTOMETRY; NEAR-INFRARED SPECTRA; BROWN DWARF DISKS AB Stellar clusters are born embedded within giant molecular clouds (GMCs) and during their formation and early evolution are often only visible at infrared wavelengths, being heavily obscured by dust. Over the past 15 years advances in infrared detection capabilities have enabled the first systematic studies of embedded clusters in galactic molecular clouds. In this article we review the current state of empirical knowledge concerning these extremely young protocluster systems. From a survey of the literature we compile the first extensive catalog of galactic embedded clusters. We use the catalog to construct the mass function and estimate the birthrate for embedded clusters within similar to2 kpc of the sun. We find that the embedded cluster birthrate exceeds that of visible open clusters by an order of magnitude or more indicating a high infant mortality rate for protocluster systems. Less than 4-7% of embedded clusters survive emergence from molecular clouds to become bound clusters of Pleiades age. The vast majority (90%) of stars that form in embedded clusters form in rich clusters of 100 or more members with masses in excess of 50 M(circle dot). Moreover, observations of nearby cloud complexes indicate that embedded clusters account for a significant (70-90%) fraction of all stars formed in GMCs. We review the role of embedded clusters in investigating the nature of the initial mass function (IMF) that, in one nearby example, has been measured over the entire range of stellar and substellar mass, from OB stars to substellar objects near the deuterium burning limit. We also review the role embedded clusters play in the investigation of circumstellar disk evolution and the important constraints they provide for understanding the origin of planetary systems. Finally, we discuss current ideas concerning the origin and dynamical evolution of embedded clusters and the implications for the formation of bound open clusters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu; lada@astro.ufl.edu NR 205 TC 1421 Z9 1426 U1 1 U2 24 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2003 VL 41 BP 57 EP 115 DI 10.1146/annurev.astro.41.011802.094844 PG 63 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 742AX UT WOS:000186494000004 ER PT B AU Ubelaker, DH AF Ubelaker, DH BE Raymond, JS Burger, RL TI Health issues in the early formative of Ecuador: Skeletal biology of real alto SO ARCHAEOLOGY OF FORMATIVE ECUADOR LA English DT Proceedings Paper CT Symposium on Archaeology of Formative Ecuador CY OCT 07-08, 1995 CL Dumbarton Oaks, Washington, DC HO Dumbarton Oaks C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 43 TC 5 Z9 5 U1 0 U2 0 PU DUMBARTON OAKS RESEARCH LIBRARY PI WASHINGTON PA 1703 32ND ST NW, WASHINGTON, DC 20007 USA BN 0-88402-292-7 PY 2003 BP 259 EP 287 PG 29 WC Archaeology SC Archaeology GA BY76M UT WOS:000189457600008 ER PT J AU Kirwin, L Lord, J AF Kirwin, L Lord, J TI A toolkit of dreams: Conversations with American craft artists SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Article C1 Smithsonian Inst, Archives Amer Art, Washington, DC 20560 USA. George Washington Univ, Washington, DC 20052 USA. RP Kirwin, L (reprint author), Smithsonian Inst, Archives Amer Art, Washington, DC 20560 USA. NR 33 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 2003 VL 43 IS 1-2 BP 2 EP 24 PG 23 WC Art SC Art GA 828KM UT WOS:000221972200001 ER PT J AU Bedini, SA AF Bedini, SA TI Eastern magnificence & European ingenuity - Clocks of Late Imperial China SO ARTS OF ASIA LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARTS ASIA PUBLICATIONS LTD PI KOWLOON PA KOWLOON CENTER-SUITE 1309 29-39 ASHLEY RD, KOWLOON, HONG KONG SN 0004-4083 J9 ART ASIA JI Arts Asia PD JAN-FEB PY 2003 VL 33 IS 1 BP 114 EP 116 PG 3 WC Art; Asian Studies SC Art; Asian Studies GA 648LX UT WOS:000181153800017 ER PT J AU Mathieu, RD van den Berg, M Torres, G Latham, D Verbunt, F Stassun, K AF Mathieu, RD van den Berg, M Torres, G Latham, D Verbunt, F Stassun, K TI Sub-subgiants in the old open cluster M67? SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; color-magnitude diagrams; open clusters and associations : individual (M67) stars : evolution ID X-RAY SOURCES; BLUE STRAGGLERS; SPECTROSCOPIC BINARIES; CONTACT BINARIES; WHITE-DWARF; PHOTOMETRIC VARIABILITY; STELLAR POPULATIONS; MODEL ATMOSPHERES; GLOBULAR-CLUSTERS; RADIAL-VELOCITIES AB We report the discovery of two spectroscopic binaries in the field of the old open cluster M67-S1063 and S1113-whose positions in the color-magnitude diagram place them approximate to1 mag below the subgiant branch. A ROSAT study of M67 independently discovered these stars to be X-ray sources. Both have proper-motion membership probabilities greater than 97%; precise center-of-mass velocities are consistent with the cluster mean radial velocity. S1063 is also projected within one core radius of the cluster center. It is a single-lined binary with a period of 18.396 days and an orbital eccentricity of 0.206. S1113 is a double-lined system with a circular orbit having a period of 2.823094 days. The primary stars of both binaries are subgiants. The secondary of S1113 is likely a 0.9 M(.) main-sequence star, which implies a 1.3 M(.) primary star. We have been unable to explain securely the low apparent luminosities of the primary stars. The colors of S1063 suggest 0.15 mag higher reddening than found for either M67 or through the entire Galaxy in the direction of M67. S1063 could be explained as an extincted M67 subgiant, although the origin of such enhanced extinction is unknown. The photometric properties of S1113 are well modeled by a cluster binary with a 0.9 M(.) main-sequence secondary star. However, the low composite luminosity requires a small (2.0 R(.)) primary star that would be supersynchronously rotating, in contrast to the short synchronization timescales, the circular orbit, and the periodic photometric variability with the orbital period. Geometric arguments based on a tidally relaxed system suggest a larger (4.0 R(.)) primary star in a background binary, but such a large star violates the observed flux ratio. Thus, we have not been able to find a compelling solution for the S1113 system. We speculate that S1063 and S1113 may be the products of close stellar encounters involving binaries in the cluster environment and may de ne alternative stellar evolutionary tracks associated with mass transfer episodes, mergers, and/or dynamical stellar exchanges. C1 Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Osserv Astron Brera, I-23807 Merate, LC, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. RP Mathieu, RD (reprint author), Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53706 USA. EM mathieu@astro.wisc.edu; vdberg@merate.mi.astro.it; gtorres@cfa.harvard.edu; dlatham@cfa.harvard.edu; F.W.M.Verbunt@phys.uu.nl; keivan@astro.wisc.edu NR 54 TC 38 Z9 38 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2003 VL 125 IS 1 BP 246 EP 259 DI 10.1086/344944 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627KD UT WOS:000179931600016 ER PT J AU Carney, BW Latham, DW Stefanik, RP Laird, JB Morse, JA AF Carney, BW Latham, DW Stefanik, RP Laird, JB Morse, JA TI Spectroscopic binaries, velocity jitter, and rotation in field metal-poor red giant and red horizontal-branch stars SO ASTRONOMICAL JOURNAL LA English DT Review DE binaries : spectroscopic; Galaxy : halo; planetary systems : formation; stars : Population II; stars : rotation ID GLOBULAR-CLUSTER GIANTS; PROTON CAPTURE CHAINS; PROPER-MOTION STARS; RR-LYRAE STARS; HALO GIANTS; OXYGEN ABUNDANCES; RADIAL-VELOCITIES; DEFICIENT STARS; BRIGHT GIANTS; EXTRASOLAR PLANETS AB We summarize 2007 radial velocity measurements of 91 metal-poor field red giants. Excluding binary systems with orbital solutions, our coverage averages 13.7 yr per star, with a maximum of 18.0 yr. We report four significant findings. (1) Sixteen stars are found to be spectroscopic binaries, and we present orbital solutions for 14 of them. The spectroscopic binary frequency of the metal-poor red giants, with [Fe/H] less than or equal to -1.4, for periods less than 6000 days, is 16% +/- 4%, which is not significantly different from that of comparable-metallicity field dwarfs, 17% +/- 2%. The two CH stars in our program, BD - 1.degrees2582 and HD 135148, are both spectroscopic binaries. ( 2) Velocity jitter is present among about 40% of the giants with M-V less than or equal to -1.4. The two best-observed cases, HD 3008 and BD + 22degrees2411, show pseudoperiodicities of 172 and 186 days, longer than any known long-period variable in metal-poor globular clusters. Photometric variability seen in HD 3008 and three other stars showing velocity jitter hints that starspots are the cause. However, the phasing of the velocity data with the photometry data from Hipparcos is not consistent with a simple starspot model for HD 3008. We argue against orbital motion effects and radial pulsation, so rotational modulation remains the best explanation. The implied rotational velocities for HD 3008 and BD + 22 2411, both with M(V)less than or equal to -1.4 and R approximate to 50 R-., exceed 12 km s(-1). ( 3) Including HD 3008 and BD + 22degrees2411, we have found signs of significant excess line broadening in eight of the 17 red giants with M(V)less than or equal to -1.4, which we interpret as rotation. In three cases, BD + 30 2034, CD 37 14010, and HD 218732, the rotation is probably induced by tidal locking between axial rotation and the observed orbital motion with a stellar companion. But this cannot explain the other five stars in our sample that display signs of significant rotation. This high frequency of elevated rotational velocities does not appear to be caused by stellar mass transfer or mergers: there are too few main-sequence binaries with short enough periods. We also note that the lack of any noticeable increase in mean rotation at the magnitude level of the red giant branch luminosity function bump argues against the rapid rotation's being caused by the transport of internal angular momentum to the surface. Capture of a planetary-mass companion as a red giant expands in radius could explain the high rotational velocities. ( 4) We also find significant rotation in at least six of the roughly 15 ( 40%) red horizontal-branch stars in our survey. It is likely that the enhanced rotation seen among a significant fraction of both blue and red horizontal-branch stars arose when these stars were luminous red giants. Rapid rotation alone therefore appears insufficient cause to populate the blue side of the horizontal branch. While the largest projected rotational velocities seen among field blue and red horizontal-branch stars are consistent with their different sizes, neither are consistent with the large values we find for the largest red giants. This suggests that some form of angular momentum loss ( and possibly mass loss) has been at work. Also puzzling is the apparent absence of rotation seen in field RR Lyrae variables. Angular momentum transfer and conservation in evolved metal-poor field stars thus pose many interesting questions for the evolution of low-mass stars. C1 Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA. Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RP Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. EM bruce@physics.unc.edu; dlatham@cfa.harvard.edu; rstefanik@cfa.harvard.edu; laird@tycho.bgsu.edu; morsey@casa.colorado.edu NR 146 TC 111 Z9 113 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JAN PY 2003 VL 125 IS 1 BP 293 EP 321 DI 10.1086/345386 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627KD UT WOS:000179931600022 ER PT J AU Georgantopoulos, I Nandra, K Brotherton, M Ptak, A Zezas, A Papadakis, I AF Georgantopoulos, I Nandra, K Brotherton, M Ptak, A Zezas, A Papadakis, I TI The SHEEP survey: Observing the hardest of the hard with Chandra SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN DE X-rays; surveys ID NEARBY GALAXIES; ASCA AB Our ASCA hard (5-10 keV) SHEEP (Survey High Energy Extragalactic Populations) survey covers 39 deg(2) and contains 69 sources down to a limiting flux of 10(-13) erg cm(-2) s(-1). 35 of the sources have ROSAT counterparts and therefore reliable optical identifications. The 'soft' SHEEP/ROSAT sample appears to be dominated by QSOs and Seyfert-1 galaxies. For the remaining 34 sources we are obtaining Chandra snapshot (5 ksec) and KPNO spectroscopic observations. Here, we report some preliminary results from this campaign. Although the sample with spectroscopic identifications is still very limited, it appears that we are observing a mixture of QSOs (one at a redshift of z=0.5 is heavily obscured) and Narrow Line Galaxies. C1 Natl Observ Athens, Inst Astron & Astrophys, Athens, Greece. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Arizona, Tucson, AZ 85721 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Crete, Rethimnon, Greece. RP Georgantopoulos, I (reprint author), Natl Observ Athens, Inst Astron & Astrophys, Athens, Greece. RI Ptak, Andrew/D-3574-2012; Georgantopoulos, Ioannis/L-3687-2013; Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 10 TC 0 Z9 0 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 32 EP 35 DI 10.1002/asna.200310009 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600009 ER PT J AU Grindlay, J Zhao, P Hong, JS Jenkins, J Kim, DW Schlegel, E Drake, J Kashyap, V Edmonds, P Cohn, H Lugger, P Cool, A AF Grindlay, J Zhao, P Hong, JS Jenkins, J Kim, DW Schlegel, E Drake, J Kashyap, V Edmonds, P Cohn, H Lugger, P Cool, A TI Chandra multi-wavelength plane (ChaMPlane) survey: design and initial results SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN DE surveys; X-rays; binary : X-ray; white dwarfs; stars : neutron ID CATACLYSMIC VARIABLES; GALACTIC PLANE; EMISSION; ORIGIN AB The Chandra Multiwavength Plane (ChaMPlane) Survey of the galactic plane incorporates serendipitous sources from selected Chandra pointings in or near the galactic plane (b<12degrees; greater than or equal to20 ksec; lack of bright diffuse or point sources) to measure or constrain the luminosity function of low-luminosity accretion sources in the Galaxy. The primary goal is to detect and identify accreting white dwarfs (cataclysmic variables, with space density still uncertain by a factor of >10-100), neutron stars and black holes (quiescent low mass X-ray binaries) to constrain their space densities and thus origin and evolution, Secondary objectives are to identify Be stars in high mass X-ray binaries and constrain their space densities, and to survey the H-R diagram for stellar coronal sources. A parallel optical imaging under the NOAO Long Term Survey program provides deep optical images using the Mosaic imager on the CTIO and KPNO 4-m telescopes. The 36' x 36' optical images (Ha, R, V and I) cover similar to 5 x the area of each enclosed Chandra ACIS FOV, providing an extended survey of emission line objects for comparison with Chandra. Spectroscopic followup of optical counterparts is then conducted, thus far with WIYN and Magellan. The X-ray preliminary results from both the Chandra and optical surveys will be presented, including logN-logS vs. galactic position (l,b) and optical identifications. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. RP Grindlay, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 14 Z9 14 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 57 EP 60 DI 10.1002/asna.200310015 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600015 ER PT J AU Green, PJ Cameron, R Ghosh, H Grimes, J Kim, DW Morris, D Mossman, A Silverman, J Wilkes, B Baldwin, J Jannuzi, B Harnden, R Kashyap, V LaCluyze, A Maksym, P Schlegel, E Tananbaum, H Vikhlinin, A Smith, C Smith, M AF Green, PJ Cameron, R Ghosh, H Grimes, J Kim, DW Morris, D Mossman, A Silverman, J Wilkes, B Baldwin, J Jannuzi, B Harnden, R Kashyap, V LaCluyze, A Maksym, P Schlegel, E Tananbaum, H Vikhlinin, A Smith, C Smith, M CA ChaMP Collaboration TI The Chandra Multi-wavelength Project (ChaMP): Results and prospects SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN DE X-rays; surveys; quasars : general ID BAND AB The cosmic diffuse X-ray background radiation has been almost completely resolved into point sources by Chandra and XMM. However, the nature and evolution of those sources are just beginning to be investigated. The answers are key to our understanding of the inter-relationship over cosmic time of (a) the formation and growth of black holes, (b) star formation, and (c) hierarchical structure formation. This requires multiwavelength followup of Chandra sources over a large area. The Chandra Multiwavelength Project (ChaMP) is a serendipitous survey of the X-ray sky, covering about 14 deg(2) of sky in the X-ray flux range of -13 to -16 (log 0.5-2 keV flux, cgs) and will include about 8000 sources, 70% of which are expected to be active galactic nuclei (AGN). Using Chandra archival data, we span flux limits between those reached by previous satellites and those of the deepest small-area Chandra and XMM surveys, allowing study of larger samples of rare objects like luminous absorbed AGN, groups and clusters of galaxies, and their spatial correlations. Optical imaging and spectroscopy of the ChaMP fields are underway at a variety of telescopes using Sloan g', r', and i' filters to a flux limit matched to the X-ray such that about 75% of the X-ray sources will be optically identified. We also plan for radio and near-IR observations of subsets of the ChaMP sample to expand our multi-wavelength coverage and increase the fraction of sources identified. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Green, PJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Maksym, Walter/0000-0002-2203-7889; Wilkes, Belinda/0000-0003-1809-2364 NR 14 TC 3 Z9 3 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 93 EP 96 DI 10.1002/asna.200310024 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600024 ER PT J AU Silverman, J Green, P Wilkes, B Foltz, C Smith, P Smith, C Kim, DW Morris, D Mossman, A Cameron, R Adelberger, K AF Silverman, J Green, P Wilkes, B Foltz, C Smith, P Smith, C Kim, DW Morris, D Mossman, A Cameron, R Adelberger, K CA ChaMP Collaboration TI Optical spectroscopic followup of serendipitous Chandra sources: the Chandra Multiwavelength Project (ChaMP) SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN DE X-rays; surveys ID X-RAY; LUMINOSITY FUNCTION; DEEP SURVEY; FIELD; EVOLUTION; REDSHIFT AB A primary goal of the Chandra Multiwavelength Project (ChaMP) is to investigate the evolution of Active Galactic Nuclei (AGN) and quasars by measuring the luminosity function out to; greater than or equal to 4 including obscured AGN that have been missed by previous surveys. To do so. we are acquiring spectra of optical counterparts to serendipitious X-ray sources detected by Chandra for classification and redshift determination. We have amassed about 200 spectra using the FLWO 1.5m, WIYN 3.5m, CTIO/4m, Magellan and the MMT 6.5m. We have classified the majority of optical counterparts as 65% broad line AGN, 14% narrow emission line galaxies and 12% absorption line galaxies. The remaining counterparts are either stars (8%) or galaxy clusters (1%). We have acquired a sample of 120 AGN in 12 Chandra fields. With a limiting magnitude of r' = 22 for spectroscopic followup, we are able to detect quasars out to z similar to 5 and galaxies out to z similar to 0.7. This preliminary sample forms the foundation for our measurement of the X-ray luminosity function of AGNs out to z similar to 4. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Arizona, Multiple Mirror Telescope Observ, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. RP Silverman, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 12 TC 2 Z9 2 U1 0 U2 3 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 97 EP 100 DI 10.1002/asna.200310025 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600025 ER PT J AU Kilgard, RE Krauss, MI Kaaret, P Prestwich, AH Ward, MJ AF Kilgard, RE Krauss, MI Kaaret, P Prestwich, AH Ward, MJ TI A Chandra survey of nearby spiral galaxies SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN DE surveys; X-rays; galaxies : spiral AB We present results from a Chandra survey of I I nearby, face-on spiral galaxies. 24 observations totalling 900 ks of new and archival Chandra data reveal more than 1000 X-ray point sources associated with the galaxies, diffuse emission, and hundreds of serendipitous sources. We discuss source populations and luminosity functions and show that the slope of the X-ray luminosity function is correlated with the star formation rate in the galaxies. We also discuss ultraluminous X-ray sources in comparison with sources within the Milky Way. Finally, we discuss ongoing work on source classification based upon X-ray colors and spectra, position within the host galaxies, and multiwavelenth counterparts. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Leicester LE1 7RH, Leics, England. MIT, Dept Phys, Cambridge, MA 02139 USA. RP Kilgard, RE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 1 Z9 1 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 121 EP 123 DI 10.1002/asna.200310031 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600031 ER PT J AU Morales, R Nicastro, F Elvis, M AF Morales, R Nicastro, F Elvis, M TI Spectroscopic X-ray classification of AGNs SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN ID GALAXIES C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Morales, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 2 TC 0 Z9 0 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 152 EP 152 DI 10.1002/asna.200310051 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600051 ER PT J AU Lamer, G Schwope, A Elvis, M Burke, D Watson, MG AF Lamer, G Schwope, A Elvis, M Burke, D Watson, MG TI The XMM-Newton SSC serendipitous cluster survey SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN ID RAY C1 Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, X Ray Astron Grp, Leicester LE1 7RH, Leics, England. RP Lamer, G (reprint author), Astrophys Inst Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. OI Burke, Douglas/0000-0003-4428-7835 NR 3 TC 1 Z9 1 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 156 EP 156 DI 10.1002/asna.200310055 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600055 ER PT J AU Polletta, M Lonsdale, CJ Xu, C Wilkes, B AF Polletta, M Lonsdale, CJ Xu, C Wilkes, B TI X-Ray counts and contribution to the X-ray background of an IR population of starburst and active galaxies SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN ID LUMINOSITY FUNCTION; EMISSION C1 CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Polletta, M (reprint author), CALTECH, Infrared Proc & Anal Ctr, MS 100-22, Pasadena, CA 91125 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 8 TC 1 Z9 1 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 170 EP 170 DI 10.1002/asna.200310069 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600069 ER PT J AU Risaliti, G AF Risaliti, G TI A Chandra mini-survey of x-ray weak quasars SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN C1 INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Risaliti, G (reprint author), INAF, Osservatorio Astrofis Arcetri, L go E Fermi 5, I-50125 Florence, Italy. NR 3 TC 0 Z9 0 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 174 EP 174 DI 10.1002/asna.200310073 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600073 ER PT J AU Zhao, P Grindlay, J Edmonds, P Hong, J Jenkins, J Schlegel, E Cohn, H Lugger, P AF Zhao, P Grindlay, J Edmonds, P Hong, J Jenkins, J Schlegel, E Cohn, H Lugger, P TI Imitial optical results for the ChaMPlane Survey SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on X-ray Surveys CY SEP 04-06, 2002 CL SANTANDER, SPAIN C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Zhao, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 4 Z9 4 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 1-2 BP 176 EP 176 DI 10.1002/asna.200310075 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650JH UT WOS:000181259600075 ER PT J AU Kalkofen, W AF Kalkofen, W TI 3D wave propagation in the chromosphere SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on From the Gregory-Coude Telescope to GREGOR - A Development from Past to Future CY JUL 24-26, 2002 CL GOTTINGEN UNIV, III PHYS INST, GOTTINGEN, GERMANY SP Univ Sternwarte Gottingen HO GOTTINGEN UNIV, III PHYS INST ID ATMOSPHERE C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kalkofen, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 3 Z9 3 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2003 VL 324 IS 4 BP 409 EP 409 DI 10.1002/asna.200310149 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 689RH UT WOS:000183506400056 ER PT J AU Braito, V Franceschini, A Della Ceca, R Severgnini, P Bassani, L Cappi, M Malaguti, G Palumbo, GGC Persic, M Risaliti, G Salvati, M AF Braito, V Franceschini, A Della Ceca, R Severgnini, P Bassani, L Cappi, M Malaguti, G Palumbo, GGC Persic, M Risaliti, G Salvati, M TI XMM-Newton observations of ULIRGs: A compton-thick AGN in IRAS 19254-7245 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : starburst; X-rays : galaxies; galaxies : individual : IRAS 19254-7245 ID INFRARED GALAXIES; RAY; SUPERANTENNAE AB We present the XMM-Newton observation of the merging system IRAS 19254-7245, also known as The Superantennae, whose southern nucleus is classified as a Seyfert 2 galaxy. The XMM-Newton data have allowed us to perform a detailed X-ray imaging and spectral analysis of this system. We clearly detect, for the first time in this system, a strong (EW similar to 1.4 keV) Fe emission line at 6.49 +/- 0.1 keV (rest-frame). The X-ray spectrum requires a soft thermal component (kT similar to 0.9 keV; L0.5-2 similar to 4 x 10(41) erg s(-1)), likely associated with the starburst, and a hard power-law continuum above 2 keV (observed L2-10 similar to 4 x 10(42) erg s(-1)). We confirm the flatness of this latter component, already noted in previous ASCA data. This flatness, together with the detection of the strong Fe-Kalpha line and other broad band indicators, suggest the presence of a Compton-thick AGN with intrinsic luminosity greater than or similar to10(44) erg s(-1). We show that a Compton-thick model can perfectly reproduce the X-ray spectral properties of this object. C1 Osserv Astron Padova, INAF, I-35122 Padua, Italy. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Osserv Astron Brera, INAF, I-20121 Milan, Italy. CNR, IASF, Sez Bologna, I-40129 Bologna, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Osserv Astron Trieste, INAF, I-50125 Florence, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Braito, V (reprint author), Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. RI Cappi, Massimo/F-4813-2015; OI 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; Bassani, Loredana/0000-0003-4858-6963; Braito, Valentina/0000-0002-2629-4989 NR 29 TC 28 Z9 28 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 JAN PY 2003 VL 398 IS 1 BP 107 EP 111 DI 10.1051/0004-6361:20021633 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JL UT WOS:000180395700013 ER PT J AU Persi, P Tapia, M Roth, M Marenzi, AR Testi, L Vanzi, L AF Persi, P Tapia, M Roth, M Marenzi, AR Testi, L Vanzi, L TI Near and Mid-infrared images of the massive star forming complex G9.62+0.19 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; infrared : stars ID ULTRACOMPACT HII-REGIONS; H-II REGIONS; METHANOL MASERS; POINT SOURCES; H2O MASERS; HOT; EMISSION; PHOTOMETRY; DATABASE; AMMONIA AB A near- and mid-infrared study of the star formation complex G9.62+0.19 is presented. It includes photometrically calibrated images through wide-band JHK and narrow-band Br, H-2 and 12.5 mum filters. These were taken at Las Campanas, La Silla and OAN-San Pedro Martir. We found evidence of two embedded young clusters of O-B5 stars associated with the radio components B and C, one compact and one ultracompact HII region. The data suggest the presence of a third, more dispersed cluster of more luminous infrared stars at the southern edge of the cloud complex. A large fraction of the star members of each cluster exhibit significant infrared excess. We confirm the detection of a very red near- and mid-infrared source immersed in the molecular hot core (component F). An H-2 shocked gas knot, probably an obscured Herbig-Haro object, was found associated to the blue-shifted lobe of the high-velocity molecular outflow in this core. The properties of the individual sources are discussed in detail. C1 CNR, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22833, Baja California, Mexico. Carnegie Inst Sci, Las Campanas Observ, La Serena, Chile. Osserv Astrofis Arcetri, I-50125 Florence, Italy. European So Observ, Santiago, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP CNR, Ist Astrofis Spaziale & Fis Cosm, Via Fosso Cavaliere, I-00133 Rome, Italy. EM persi@rm.iasf.cnr.it RI Vanzi, Leonardo/D-1381-2014; OI Tapia, Mauricio/0000-0002-0506-9854 NR 21 TC 11 Z9 11 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 JAN PY 2003 VL 397 IS 1 BP 227 EP 236 DI 10.1051/0004-6361:20021480 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 624PL UT WOS:000179768500023 ER PT J AU Webb, TM Eales, S Foucaud, S Lilly, SJ McCracken, H Adelberger, K Steidel, C Shapley, A Clements, DL Dunne, L LeFevre, O Brodwin, M Gear, W AF Webb, TM Eales, S Foucaud, S Lilly, SJ McCracken, H Adelberger, K Steidel, C Shapley, A Clements, DL Dunne, L LeFevre, O Brodwin, M Gear, W TI The Canada-United Kingdom Deep Submillimeter Survey. V. The submillimeter properties of Lyman break galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; dust, extinction; galaxies : evolution; galaxies : formation; galaxies : starburst; submillimeter ID STAR-FORMATION HISTORY; HIGH-REDSHIFT GALAXIES; PHOTOMETRIC REDSHIFTS; EXTRAGALACTIC OBJECTS; STATISTICAL-ANALYSIS; STARBURST GALAXIES; SCUBA-8-MJY SURVEY; LENSING CLUSTERS; FIELD GALAXIES; NUMBER COUNTS AB We have used 850 l m maps obtained as part of the Canada-UK Deep Submillimeter Survey (CUDSS) to investigate the submillimeter properties of Lyman break galaxies (LBGs). We used three samples of LBGs: two from the Canada-France Deep Fields (CFDF) survey covering CUDSS 14 and CUDSS 03, and one from Steidel and collaborators also covering CUDSS 14. We measure a mean flux from both CFDF LBG samples at a level of similar to2 sigma of 0.414 +/- 0.263 mJy for CUDSS 03 and 0.382 +/- 0.206 mJy for CUDSS 14, but the Steidel et al. sample is consistent with zero flux. From this we place upper limits on the Lyman break contribution to the 850 l m background of similar to20%. We have also measured the cross-clustering between the LBGs and the SCUBA sources. From this measurement we infer a large clustering amplitude of r(0) = 11.5 +/- 3.0 +/- 3.0 h(-1) Mpc for the Steidel et al. sample (where the first error is statistical and the second systematic), r(0) = 4.5 +/- 7.0 +/- 5.0 h(-1) Mpc for CFDF 14, and r(0) = 7.5 +/- 7.0 +/- 5.0 h(-1) Mpc for CFDF 03. The Steidel et al. sample, for which we have the most significant detection of clustering, is also the largest of the three samples and has spectroscopically confirmed redshifts. C1 Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 1A1, Canada. Cardiff Univ, Dept Phys & Astron, Cardiff CF2 3YB, S Glam, Wales. Lab Astrophys Marseille, F-13376 Marseille 12, France. ETH Honggerberg, Inst Astron, CH-8093 Zurich, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Palomar Observ, Pasadena, CA 91125 USA. RP Univ Toronto, Dept Astron & Astrophys, 60 St George St, Toronto, ON M5S 1A1, Canada. RI Le Fevre, Olivier/G-7389-2011 NR 59 TC 70 Z9 70 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 JAN 1 PY 2003 VL 582 IS 1 BP 6 EP 16 DI 10.1086/344608 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MX UT WOS:000180000600003 ER PT J AU Di Matteo, T Allen, SW Fabian, AC Wilson, AS Young, AJ AF Di Matteo, T Allen, SW Fabian, AC Wilson, AS Young, AJ TI Accretion onto the supermassive black hole in M87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; galaxies : individual (M87); galaxies : jets; X-rays : galaxies ID ADVECTION-DOMINATED ACCRETION; X-RAY-EMISSION; ELLIPTIC GALAXIES; VLBI OBSERVATIONS; VIRGO CLUSTER; RADIO; JET; FLOWS; GAS; CONVECTION AB Chandra X-ray observations of the giant elliptical galaxy M87 resolve the thermal state of the hot interstellar medium into the accretion (Bondi) radius of its central 3 x 10(9) M-circle dot black hole. We measure the X-ray gas temperature and density profiles and calculate the Bondi accretion rate, (M)over dot(Bondi) similar to 0.1 M-circle dot yr(-1). The X-ray luminosity of the active nucleus of M87 observed with Chandra is L-X,L-0.5-7 keV similar to 7 x 10(40) ergs s(-1). This value is much less than the predicted nuclear luminosity, L-Bondi similar to5 x 10(44) ergs s(-1), for accretion at the Bondi rate with a canonical accretion radiative efficiency of 10%. If the black hole in M87 accretes at this rate it must do so at a much lower radiative efficiency than the canonical value. The multiwavelength spectrum of the nucleus is consistent with that predicted by an advection-dominated flow. However, as is likely, the X-ray nucleus is dominated by jet emission then the properties of flow must be modified, possibly by out flows. We show that the overall energetics of the system are just consistent with the predicted Bondi nuclear power. This suggests that either most of the accretion energy is released in the relativistic jet or the central engine of M87 undergoes on-off activity cycles. We show that, at present, the energy dumped into the ISM by the jet may reduce the accretion rate onto the black hole by a factor proportional to (v(j)/c(s))(-2), where v(j) is the jet velocity and c(s) the ISM sound speed, and that this is sufficient to account for the low nuclear luminosity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15231 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 58 TC 191 Z9 191 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 JAN 1 PY 2003 VL 582 IS 1 BP 133 EP 140 DI 10.1086/344504 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MX UT WOS:000180000600014 ER PT J AU Zakamska, NL Narayan, R AF Zakamska, NL Narayan, R TI Models of galaxy clusters with thermal conduction SO ASTROPHYSICAL JOURNAL LA English DT Article DE conduction; cooling flows; galaxies : clusters : general; X-rays : galaxies : clusters ID COOLING FLOWS; CHANDRA OBSERVATION; MAGNETIC MIRRORS; HEAT-CONDUCTION; MASS; TRANSPORT; GAS; INSTABILITY; ATMOSPHERE; TURBULENCE AB We present a simple model of hot gas in galaxy clusters, assuming hydrostatic equilibrium and energy balance between radiative cooling and thermal conduction. For five clusters, A1795, A1835, A2199, A2390, and RX J1347.5-1145, the model gives a good description of the observed radial profiles of electron density and temperature, provided that we take the thermal conductivity kappa to be about 30% of the Spitzer conductivity. Since the required kappa is consistent with the recent theoretical estimate of Narayan & Medvedev for a turbulent magnetized plasma, we consider a conduction-based equilibrium model to be viable for these clusters. We further show that the hot gas is thermally stable because of the presence of conduction. For five other clusters, A2052, A2597, Hydra A, Ser 159-03, and 3C 295, the model requires unphysically large values of kappa to fit the data. These clusters must have some additional source of heat, possibly an active galactic nucleus, since all the clusters have strong radio galaxies at their centers. We suggest that thermal conduction, although not dominant in these clusters, may nevertheless play a significant role by preventing the gas from becoming thermally unstable. C1 Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zakamska, NL (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 63 TC 151 Z9 153 U1 1 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 JAN 1 PY 2003 VL 582 IS 1 BP 162 EP 169 DI 10.1086/344641 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MX UT WOS:000180000600016 ER PT J AU Gardiner, TA Frank, A Hartmann, L AF Gardiner, TA Frank, A Hartmann, L TI Stellar outflows driven by magnetized wide-angle winds SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : jets and outflows; magnetic fields; MHD stars : winds, outflows ID BIPOLAR PLANETARY-NEBULAE; MOLECULAR OUTFLOWS; PROTOSTELLAR WINDS; JETS; COLLIMATION; EVOLUTION; MODELS; FLOWS; SIMULATIONS; PROPAGATION AB We present two-dimensional, cylindrically symmetric simulations of hydrodynamic and magnetohydrodynamic (MHD) wide-angle winds interacting with a collapsing environment. These simulations have direct relevance to young stellar objects. The results may also be of use in the study of collimated outflows from proto planetary and planetary nebulae. We study a range of wind configurations consistent with asymptotic MHD wind collimation. The degree of collimation is parameterized by the ratio of the wind density at the pole to that of the equator. We find that a toroidal magnetic field can have a significant influence on the resulting outflow, giving rise to a very dense, jetlike flow in the postshock region. The properties of the flow in this region are similar to the asymptotic state of a collimated MHD wind. We conclude that wide-angle MHD winds are quite likely capable of driving molecular outflows. Because of difficulty in treating MHD winds ab initio in simulations, we choose magnetic field strengths in the wind consistent with slow magnetic rotators. While MHD-launched winds will be in the fast rotator regime, we discuss how our results, which rely on toroidal pinch effects, will hold for stronger field strengths. C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Rochester, Dept Phys & Astron, 600 Wilson Blvd, Rochester, NY 14627 USA. NR 46 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2003 VL 582 IS 1 BP 269 EP 276 DI 10.1086/344609 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MX UT WOS:000180000600027 ER PT J AU Flaccomio, E Damiani, F Micela, G Sciortino, S Harnden, FR Murray, SS Wolk, SJ AF Flaccomio, E Damiani, F Micela, G Sciortino, S Harnden, FR Murray, SS Wolk, SJ TI Chandra X-ray observation of the Orion Nebula Cluster. I. Detection, identification, and determination of X-ray luminosities SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (Orion Nebula Cluster); X-rays : stars ID MOLECULAR CLOUD; BROWN DWARFS; STARS; ROTATION; VARIABILITY; POPULATION; REGION; DISKS; MODEL AB In this first of two companion papers on the Orion Nebula Cluster (ONC), we present our analysis of a 63 ks Chandra HRC-I observation that yielded 742 X-ray detections within the 30' X 30' field of view. To facilitate our interpretation of the X-ray image, here we collect a multiwavelength catalog of nearly 2900 known objects in the region by combining 17 different catalogs from the recent literature. We define two reference groups: an infrared sample, containing all objects detected in the K band, and an optical sample comprising low-extinction, well-characterized ONC members. We show for both samples that field object contamination is generally low. Our X-ray sources are primarily low-mass ONC members. The detection rate for optical sample stars increases monotonically with stellar mass from zero at the brown dwarf limit to similar to100% for the most massive stars but shows a pronounced dip between 2 and 10 M. We determine L-X and L-X/ L-bol for all stars in our optical sample and utilize this information in our companion paper to study correlations between X-ray activity and other stellar parameters. C1 Osservatorio Astron Palermo GS Vaiana, Ist Nazl Astrofis, I-90134 Palermo, Italy. Univ Palermo, Dipartimento Sci Fisiche & Astron, I-90123 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Flaccomio, E (reprint author), Osservatorio Astron Palermo GS Vaiana, Ist Nazl Astrofis, Palazzo Normanni, I-90134 Palermo, Italy. OI Flaccomio, Ettore/0000-0002-3638-5788; Wolk, Scott/0000-0002-0826-9261; Damiani, Francesco/0000-0002-7065-3061 NR 38 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 JAN 1 PY 2003 VL 582 IS 1 BP 382 EP 397 DI 10.1086/344535 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MX UT WOS:000180000600037 ER PT J AU Flaccomio, E Damiani, F Micela, G Sciortino, S Harnden, FR Murray, SS Wolk, SJ AF Flaccomio, E Damiani, F Micela, G Sciortino, S Harnden, FR Murray, SS Wolk, SJ TI Chandra X-ray observation of the Orion Nebula cluster. II. Relationship between X-ray activity indicators and stellar parameters SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (Orion Nebula Cluster); X-rays : stars ID RHO-OPHIUCHI CLOUD; DEEP FIELD-SOUTH; T-TAURI STARS; CIRCUMSTELLAR DISKS; HRI OBSERVATIONS; OPTICAL SURVEY; EMISSION; POPULATION; ROTATION; REGION AB Using the results of our first paper on the Chandra HRC observation of the Orion Nebula cluster (ONC), we explore the relation between the coronal activity of its 1 Myr-old pre-main-sequence population and stellar parameters. We find that median X-ray luminosities of low-mass stars (M/M. less than or similar to 3) increase with increasing mass and decreasing stellar age. Brown dwarfs (0.03 less than or similar to M/M. less than or similar to 0.08) follow the same trend with mass. From M similar to 0.1 to M similar to 0.5 M., median L-X/L-bol values increase by about half an order of magnitude and then remain constant at similar to10(-3.5) for the mass range from 0.5 to 3.0 M/M.. In these same two mass ranges, L-X/L-bol remains roughly constant with age, until it drops by more than 2 orders of magnitudes at the epoch when similar to2-4 M. stars are expected to become fully radiative. We find a dependence of L-X and L-X/L-bol on circumstellar accretion indicators and suggest three possible hypotheses for its origin. In spite of improved X-ray and rotational data, correlations between activity indicators and rotation remain elusive for these stars, possibly indicating that stars for which rotational periods have been measured have reached some saturation level. Our study of X-ray activity versus stellar mass leads us to propose that the few HRC X-ray sources not associated with any optical/infrared counterpart trace a yet-to-be-discovered stellar population of deeply embedded, relatively massive ONC members. C1 Osservatorio Astron Palermo GS Vaiana, Ist Nazl Astrofis, I-90134 Palermo, Italy. Univ Palermo, Dipartimento Sci Fisiche & Astron, I-90123 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Flaccomio, E (reprint author), Osservatorio Astron Palermo GS Vaiana, Ist Nazl Astrofis, Palazzo Normanni, I-90134 Palermo, Italy. OI Flaccomio, Ettore/0000-0002-3638-5788; Wolk, Scott/0000-0002-0826-9261; Damiani, Francesco/0000-0002-7065-3061 NR 37 TC 108 Z9 108 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 JAN 1 PY 2003 VL 582 IS 1 BP 398 EP 409 DI 10.1086/344536 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MX UT WOS:000180000600038 ER PT J AU Gudel, M Audard, M Kashyap, VL Drake, JJ Guinan, EF AF Gudel, M Audard, M Kashyap, VL Drake, JJ Guinan, EF TI Are coronae of magnetically active stars heated by flares? II. Extreme ultraviolet and X-ray flare statistics and the differential emission measure distribution SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : coronae; stars : flare; stars : individual (AD Leonis); stars : late-type ID QUIET SOLAR CORONA; STELLAR FLARES; TRANSIENT BRIGHTENINGS; MICROFLARING ACTIVITY; ASTRONOMY SATELLITE; ENERGY-DISTRIBUTION; TIME VARIABILITY; DM-STARS; ON-BOARD; AD-LEO AB We investigate the EUV and X-ray are rate distribution in radiated energy of the late-type active star AD Leo. Occurrence rates of solar flares have previously been found to be distributed in energy according to a power law, dN/dE proportional to E-alpha with a power-law index alpha in the range 1.5-2.6. If alpha greater than or equal to 2, then an extrapolation of the are distribution to low are energies may be sufficient to heat the complete observable X-ray/EUV corona. We have obtained long observations of AD Leo with the EUVE and BeppoSAX satellites. Numerous flares have been detected, ranging over almost 2 orders of magnitude in their radiated energy. We compare the observed light curves with light curves synthesized from model flares that are distributed in energy according to a power law with selectable index alpha. Two methods are applied, the first comparing flux distributions of the binned data and the second using the distributions of photon arrival time differences in the unbinned data (for EUVE). Subsets of the light curves are tested individually, and the quiescent flux has optionally been treated as a superposition of flares from the same are distribution. We find acceptable alpha values between 2.0 and 2.5 for the EUVE DS and the BeppoSAX LECS data. Some variation is found depending on whether or not a strong and long-lasting are occurring in the EUVE data is included. The BeppoSAX MECS data indicate a somewhat shallower energy distribution (smaller alpha) than the simultaneously observed LECS data, which is attributed to the harder range of sensitivity of the MECS detector and the increasing peak temperatures of flares with increasing total (radiative) energy. The results suggest that flares can play an important role in the energy release of this active corona. We discuss caveats related to time variability, total energy, and multiple power-law distributions. Studying the limiting case of a corona that is entirely heated by a population of flares, we derive an expression for the time-averaged coronal differential emission measure distribution (DEM) that can be used as a diagnostic for the are energy distribution. The shape of the analytical DEM agrees with previously published DEMs from observations of active stars. C1 Paul Scherrer Inst, CH-5232 Villigen, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. RP Gudel, M (reprint author), Paul Scherrer Inst, CH-5232 Villigen, Switzerland. RI Guedel, Manuel/C-8486-2015 OI Guedel, Manuel/0000-0001-9818-0588 NR 82 TC 88 Z9 88 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 JAN 1 PY 2003 VL 582 IS 1 BP 423 EP 442 DI 10.1086/344614 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MX UT WOS:000180000600041 ER PT J AU Chen, Y Esser, R Hu, Y AF Chen, Y Esser, R Hu, Y TI Formation of minor-ion charge states in the fast solar wind: Roles of differential flow speeds of ions of the same element SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; MHD; solar wind; Sun : corona ID POLAR CORONAL HOLE; ELECTRON-TEMPERATURE; HEAVY-IONS; ACCELERATION; HELIUM; DYNAMICS; PLASMAS; REGIONS; ULYSSES; OXYGEN AB To investigate the possibility of differential flow speeds between ions of the same element and their roles in the determination of ionic fractions, this paper extends our latest minor-ion model to a five-fluid model, describing the behavior of five species of minor ions of one given element in the fast solar wind. We solve the five sets of mass, momentum, and energy equations simultaneously to include the effects of ionization, recombination, and heating. The five species of minor ions are taken as test particles owing in a background plasma consisting of electrons, protons, and alpha particles. The parameters of the background gas are calculated using a previous three-fluid wave-driven magnetohydrodynamic model for the fast solar wind. These background parameters are modeled as closely as possible to observed values. Using this background of fast solar wind parameters, the five-fluid minor-ion model has no problem reproducing the frozen-in charge-state distributions observed in the fast solar wind for C and O ions, while the modeled ionic fractions of Si, Mg, and Fe show significant shifts to lower charge states compared with the observed values. It is found that the majority of C and O ions are frozen-in below 1.2 solar radii, while most Si, Mg, and Fe ions are frozen-in beyond 1.3-1.5 solar radii. Comparing the cases with and without differential flows shows that even though differential flow speeds between ions of the same element do develop beyond a certain heliocentric distance (e.g., 1.2 solar radii for Si ions), they cannot account for the high ion charge states observed in situ. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sci & Technol China, Hefei 230026, Peoples R China. Univ Tromso, Tromso, Norway. RP Chen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Chen, Yao/B-7255-2011 NR 35 TC 22 Z9 22 U1 0 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 JAN 1 PY 2003 VL 582 IS 1 BP 467 EP 474 DI 10.1086/344642 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MX UT WOS:000180000600045 ER PT J AU Greenhill, LJ Kondratko, PT Lovell, JEJ Kuiper, TBH Moran, JM Jauncey, DL Baines, GP AF Greenhill, LJ Kondratko, PT Lovell, JEJ Kuiper, TBH Moran, JM Jauncey, DL Baines, GP TI The discovery of H2O maser emission in seven active galactic nuclei and at high velocities in the Circinus galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Circinus, ESO 269-G012, IRAS F19370-0131, NGC 2824, NGC 2979, NGC 5643, NGC 6300, NGC 6926); galaxies : Seyfert; ISM : molecules masers ID BLACK-HOLE; NGC4258; SEARCH; VLBI; DISK AB We report the discovery of H2O maser emission at 1.35 cm wavelength in seven active galactic nuclei (at distances of up to 80 Mpc) during a survey conducted at the 70 m diameter antenna of the NASA Deep Space Network near Canberra, Australia. The detection rate was similar to4%. Two of the maser sources are particularly interesting because they display satellite high-velocity emission lines, which are a signature of emission from the accretion disks of supermassive black holes when seen edge-on. Three of the masers are coincident, to within uncertainties of 0."2, with continuum emission sources that we observed at about lambda = 1.3 cm. We also report the discovery of new spectral features in the Circinus galaxy H2O maser that broaden the known velocity range of emission therein by a factor of similar to1.7. If the new spectral features originate in the Circinus accretion disk, then molecular material must survive at radii similar to3 times smaller than had been believed previously (similar to0.03 pc or similar to2 x 10(5) Schwarzschild radii). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CDSCC, BAE Syst, Tidbinbilla, ACT 2620, Australia. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 60 Z9 60 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 JAN 1 PY 2003 VL 582 IS 1 BP L11 EP L14 DI 10.1086/367602 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MY UT WOS:000180000700002 ER PT J AU Matheson, T Garnavich, PM Foltz, C West, S Williams, G Falco, E Calkins, ML Castander, FJ Gawiser, E Jha, S Bersier, D Stanek, KZ AF Matheson, T Garnavich, PM Foltz, C West, S Williams, G Falco, E Calkins, ML Castander, FJ Gawiser, E Jha, S Bersier, D Stanek, KZ TI The spectroscopic variability of GRB 021004 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : distances and redshifts; galaxies : ISM; gamma rays : bursts; ultraviolet : galaxies ID GAMMA-RAY BURST; ULTRAVIOLET EXTINCTION; STANDARD STARS; SPECTROPHOTOMETRY; SPECTROGRAPH; TELESCOPE; REDSHIFT AB We present spectra of the optical transient (OT) associated with GRB 021004. The spectra show a blue continuum with superposed absorption features and one emission line. We confirm two intervening metal-line systems at z = 1.380 and z = 1.602 and and one very strong absorption system at a redshift of z = 2.323. Lyalpha emission is also seen at this redshift. While the spectrum of the OT overall cannot be simply described with a power law, the spectral index over the range 5500-8850 Angstrom is steep, F-v proportional to v(-0.96+/-0.03). Comparison of spectra from multiple epochs shows a distinct color evolution with the OT becoming redder with time over the first 3 days. This is the first clear example of color change in an OT detected spectroscopically. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Univ Arizona, Multiple Mirror Telescope Observ, Tucson, AZ 85721 USA. CSIC, Inst Estudis Espacials Catalunya, ES-08034 Barcelona, Spain. Univ Chile, Santiago, Chile. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. RP Matheson, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 46 TC 36 Z9 36 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 JAN 1 PY 2003 VL 582 IS 1 BP L5 EP L9 DI 10.1086/367601 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628MY UT WOS:000180000700001 ER PT J AU Young, PR Del Zanna, G Landi, E Dere, KP Mason, HE Landini, M AF Young, PR Del Zanna, G Landi, E Dere, KP Mason, HE Landini, M TI Chianti - An atomic database for emission lines. VI. Proton rates and other improvements SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE atomic data; stars : atmospheres; Sun : atmosphere ID ELECTRON-IMPACT-EXCITATION; FINE-STRUCTURE TRANSITIONS; EFFECTIVE COLLISION STRENGTHS; HEAVY-PARTICLE IMPACT; BE-LIKE IONS; N = 2; NITROGEN ISOELECTRONIC SEQUENCE; STRUCTURE FORBIDDEN TRANSITIONS; PHOTOIONIZATION CROSS-SECTIONS; EXPERIMENTAL LEVEL VALUES AB The CHIANTI atomic database contains atomic energy levels, wavelengths, radiative transition probabilities, and electron excitation data for a large number of ions of astrophysical interest. Version 4 has been released, and proton excitation data are now included, principally for ground configuration levels that are close in energy. The fitting procedure for excitation data, both electrons and protons, has been extended to allow nine-point spline fits in addition to the previous five-point spline fits. This allows higher quality fits to data from close-coupling calculations where resonances can lead to significant structure in the Maxwellian-averaged collision strengths. The effects of photoexcitation and stimulated emission by a blackbody radiation field in a spherical geometry on the level balance equations of the CHIANTI ions can now be studied following modi cations to the CHIANTI software. With the addition of H I He I and N I the first neutral species have been added to CHIANTI. Many updates to existing ion data sets are described, while several new ions have been added to the database, including Ar IV Fe vi and Ni XXI. The two-photon continuum is now included in the spectral synthesis routines, and a new code for calculating the relativistic free-free continuum has been added. The treatment of the free-bound continuum has also been updated. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 9EW, England. ARTEP Inc, Columbia, MD 21044 USA. USN, Res Lab, Washington, DC 20375 USA. Univ Florence, Dipartimento Astron & Sci Spazio, Florence, Italy. RP Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. RI Landi, Enrico/H-4493-2011 NR 176 TC 268 Z9 269 U1 0 U2 4 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 JAN PY 2003 VL 144 IS 1 BP 135 EP 152 DI 10.1086/344365 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627XT UT WOS:000179962500005 ER PT S AU Dubinski, J Koranyi, D Geller, M AF Dubinski, J Koranyi, D Geller, M BE Makino, J Hut, P TI The evolution of galaxies in clusters SO ASTROPHYSICAL SUPERCOMPUTING USING PARTICLE SIMULATIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 208th Symposium of the International Astronomical Union CY JUL 10-13, 2001 CL TOKYO, JAPAN SP Int Astron Union, 33, Int Astron Union, 37, Res Future Program Japan Soc Promot Sci ID FUNDAMENTAL PLANE; VIRGO CLUSTER; RICH CLUSTERS AB We report on recent numerical investigations of the dynamical evolution of galaxies in clusters. Simulations of spiral galaxies falling into forming clusters show the development of the morphology-density relationship and the formation of regular and giant elliptical galaxies. The regular elliptical merger remnants end up in a fundamental plane very similar to the observed relation. The giant ellipticals have much in common with their real counterparts but their central velocity dispersions are too high. We also quantify the amount and distribution of diffuse light in clusters. C1 Univ Toronto, Dept Astron & Astrophys, CITA, McLennan Labs, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dubinski, J (reprint author), Univ Toronto, Dept Astron & Astrophys, CITA, McLennan Labs, 60 St George St, Toronto, ON M5S 3H8, Canada. NR 13 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-139-7 J9 IAU SYMP PY 2003 IS 208 BP 237 EP 244 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW96S UT WOS:000183793400024 ER PT S AU Springel, V Hernquist, L AF Springel, V Hernquist, L BE Makino, J Hut, P TI A multi-phase model for simulations of galaxy formation SO ASTROPHYSICAL SUPERCOMPUTING USING PARTICLE SIMULATIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 208th Symposium of the International Astronomical Union CY JUL 10-13, 2001 CL TOKYO, JAPAN SP Int Astron Union, 33, Int Astron Union, 37, Res Future Program Japan Soc Promot Sci ID HYDRODYNAMICAL SIMULATIONS; SUPERNOVA FEEDBACK; STAR FORMATION AB We discuss SPH simulations of galaxy formation which use a hybrid method to describe a two-phase structure of the star forming ISM on unresolved scales. Our modeling includes radiative cooling, heating due to a UV background, growth of cold clouds embedded in an ambient hot gas, star formation out of cloud material, feedback due to supernovae in the form of thermal heating and cloud evaporation, starbursts that can lead to galactic outflows, and metal enrichment. Our particular model for the treatment of the two-phase structure is based on a modified and extended version of the grid-based approach of Yepes et al. (1997). We discuss the properties of the feedback model and show how it stabilizes star forming disk galaxies and reduces the cosmic star formation rate to a level consistent with current observational constraints. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Springel, V (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-139-7 J9 IAU SYMP PY 2003 IS 208 BP 273 EP 282 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW96S UT WOS:000183793400027 ER PT S AU Hamana, T Yoshida, N Suto, Y AF Hamana, T Yoshida, N Suto, Y BE Makino, J Hut, P TI Are cosmological N-body simulations reliable on scales below the mean separation length of particles? SO ASTROPHYSICAL SUPERCOMPUTING USING PARTICLE SIMULATIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 208th Symposium of the International Astronomical Union CY JUL 10-13, 2001 CL TOKYO, JAPAN SP Int Astron Union, 33, Int Astron Union, 37, Res Future Program Japan Soc Promot Sci AB We critically examine the reliability of clustering below the mean separation length of particles in cosmological high-resolution N-body simulations. The particle discreteness effect imposes two fundamental limitations on those scales; the lack of the initial fluctuation power and the finite mass resolution. We address this problem applying the dark matter halo approach which makes us possible to examine separately how those two limitations affect the simulation results at later epochs. We find that the reliability of the simulations on scale below the mean particle separation is primarily determined by the mass of particles. Since the small scale matter clustering is dominated by the matter in a virialized halo, it is naturally expected that the small scale clustering becomes unreliable when the characteristic nonlinear mass for gravitationally collapsed objects at that time becomes smaller than the particle mass. This is confirmed by a detailed comparison with three major cosmological simulations. The characteristic mass, M-NL(Z), is approximately given by the condition sigma(M-NL, z) = 1. This mass scale should be much larger than the simulation particle mass m(part) so as to reproduce the proper amplitude of the small scale clustering. This requirement can be translated to the criterion for the critical redshift Z(crit) when simulations reasonably resolve the clustering on scales below the mean separation: M-NL(Z(crit)) = n(halo)m(part), where we introduce a fudge factor, nhalo, of around ten. We conclude that at z > z(crit) high-resolution N-body simulations are not reliable on scales below the mean particle separation. Although it is not obvious if the opposite is true at z < Z(crit), our detailed comparison suggests that it is indeed the case at least as far as the two-point correlation functions of the matter are concerned. The detail discussions are presented in Hamana, Yoshida Suto (2001). C1 Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Dept Phys, Sch Sci, Res Ctr Early Universe RESCEU, Tokyo 1130033, Japan. RP Hamana, T (reprint author), Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-139-7 J9 IAU SYMP PY 2003 IS 208 BP 399 EP 400 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW96S UT WOS:000183793400050 ER PT S AU Kenyon, SJ Bromley, BC AF Kenyon, SJ Bromley, BC BE Makino, J Hut, P TI Evolution of planetesimals in planetary debris disks SO ASTROPHYSICAL SUPERCOMPUTING USING PARTICLE SIMULATIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 208th Symposium of the International Astronomical Union CY JUL 10-13, 2001 CL TOKYO, JAPAN SP Int Astron Union, 33, Int Astron Union, 37, Res Future Program Japan Soc Promot Sci ID VELOCITY EVOLUTION; STARS; DUST AB Dusty planetary disks can form quickly around young stars and linger, despite the depletion of dust through mechanisms such as Poynting-Robertson drag. Planetesimals in the disk can replenish the dust with an efficiency that depends on their mass and velocity distributions. Here, we describe a numerical program to track the evolution of planetesimals through merging, fragmentation and drag. Our current effort is focused on coupling a Fokker-Planck solver with N-body calculations to follow the detailed behavior of larger planetesimals. Our results demonstrate the importance of gravitational stirring in dust production. Furthermore, stirring by planets larger than Pluto can generate the large scale heights seen in several dusty disks. C1 Smithsonian Astron Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astron Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-139-7 J9 IAU SYMP PY 2003 IS 208 BP 415 EP 416 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW96S UT WOS:000183793400058 ER PT J AU Marengo, M Karovska, M Sasselov, DD Papaliolios, C Armstrong, JT Nordgren, TE AF Marengo, M Karovska, M Sasselov, DD Papaliolios, C Armstrong, JT Nordgren, TE TI Cepheid limb darkening models for the VLTI SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Workshop on the Very Large Telescope Interferometer CY SEP 05-07, 2002 CL UNIV PORTO, DEPT MATEMAT APLICADA & MATEMAT PURA, OPORTO, PORTUGAL SP Soc Portuguesa Astronomia HO UNIV PORTO, DEPT MATEMAT APLICADA & MATEMAT PURA ID DISTANCE; STAR; LINE AB We present a new method to compute wavelength- and phase-dependent limb darkening corrections for classical Cepheids. These corrections are derived from hydrodynamic simulations and radiative transfer modeling with a full set of atomic and molecular opacities. Comparison with hydrostatic models having the same stellar parameters show a larger limb darkening for most phases in our models, and temporal variations related to the hydrodynamics of the stellar pulsation. We assess the implications of our results with respect to the geometric Baade-Wesselink method, which uses interferometric measurements of Cepheid angular diameters to determine their distances and radii. The relevance of the hydrodynamic effects predicted by our model on the limb darkening of pulsating Cepheids is finally discussed in terms of the predicted capabilities of the VLTI. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. Univ Redlands, Dept Phys, Redlands, CA 92373 USA. RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 0 Z9 0 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2003 VL 286 IS 1-2 BP 185 EP 190 DI 10.1023/A:1026171925432 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 732BK UT WOS:000185920800022 ER PT J AU Karovska, M Elvis, M Marengo, M AF Karovska, M Elvis, M Marengo, M TI Distances on Cosmological Scales with VLTI SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Workshop on the Very Large Telescope Interferometer CY SEP 05-07, 2002 CL UNIV PORTO, DEPT MATEMAT APLICADA & MATEMAT PURA, OPORTO, PORTUGAL SP Soc Portuguesa Astronomia HO UNIV PORTO, DEPT MATEMAT APLICADA & MATEMAT PURA ID ACTIVE GALACTIC NUCLEI; QUASARS AB We present here a new method using interferometric measurements of quasars, that allows the determination of direct geometrical distances on cosmic scales. Quasar Broad Emission Line Regions sizes provide a 'meter rule' with which to measure the metric of the Universe. This method is less dependent of model assumptions, and even of variations in the fundamental constants ( other than c). We discuss the spectral and spatial requirements on the VLTI observations needed to carry out these measurements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmarengo@cfa.harvard.edu NR 15 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2003 VL 286 IS 1-2 BP 261 EP 266 DI 10.1023/A:1026104932701 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 732BK UT WOS:000185920800031 ER PT J AU Collins, C Brough, S Burke, D Mann, R Lynam, P AF Collins, C Brough, S Burke, D Mann, R Lynam, P TI The evolution of Brightest Cluster Galaxies SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Joint European and National Astronomical Meeting (JENAM 2002) CY SEP 02-07, 2002 CL OPORTO, PORTUGAL DE galaxies; x-rays ID SURFACE BRIGHTNESS TEST; BAND HUBBLE DIAGRAM; X-RAY-CLUSTERS; FUNDAMENTAL PLANE; ELLIPTIC GALAXIES; LUMINOUS GALAXIES; ABELL CLUSTERS; HIGH-REDSHIFT; PHOTOMETRY; MEMBERS AB In this contribution we review the properties of Brightest Cluster Galaxies (BCGs) and discuss the impact that X-ray cluster selection is having on their use as cosmological probes. BCGs form a unique galaxy population. They are located near the gravitational centre of galaxy clusters and are the most massive galaxies in the universe, being some 10 times more luminous than L* systems. Historically, BCGs have been credited with small intrinsic dispersion in their absolute magnitudes (DeltaMsimilar or equal to0.2-0.3 mag) and used as standard candles to constrain the cosmological parameters. Although indirect signs of mass accretion out to zsimilar or equal to1 have been observed, uncovering their full evolutionary picture has remained an elusive goal. Studies of BCGs based on serendipitiously discovered X-ray cluster samples, particularly from ROSAT, provide large numbers of unbiased clusters at zless than or equal to1. Furthermore X-ray emission guarantees the presence of a large gravitationally bound potential well and the X-ray information can be used to locate the centroids of clusters, aiding the identification of the BCG. We show that this has important consequences for studies of distance determination and large-scale streaming flows based on the optical properties of BCGs. Recent results based on X-ray selected clusters show large differences in near-IR BCG properties with their cluster environment; such that those in clusters with L(x)greater than or equal to1.9x10(44) erg s(-1) are brighter and more uniform than those in their low-L-x counterparts. The BCGs in high L-x systems show no evidence of having undergone mass growth, whereas those in low Lx systems show a wider range of evolution, with evidence that some have grown by a factor of 4 or more since zsimilar or equal to1. These results are a direct indication of how a single homogeneous population of galaxies evolves and are a challenge to simple semi-analytical hierarchical models. If future observations at high redshift are to seriously challenge theory then better predictions of the evolutionary process are required. C1 Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3NJ, Midlothian, Scotland. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Collins, C (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, 12 Quays House,Egerton Wharf, Birkenhead CH41 1LD, Merseyside, England. NR 50 TC 4 Z9 4 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2003 VL 285 IS 1 BP 51 EP 60 DI 10.1023/A:1024613910300 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 699TL UT WOS:000184072000008 ER PT J AU Dalgarno, A AF Dalgarno, A TI X-rays in the Solar System SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE atomic processes; comets; interplanetary medium; solar wind; X-rays : diffuse background ID WIND IONS; CHARGE-EXCHANGE; EMISSION; SPECTRA; COMETS AB Soft X-ray observations from comets are analysed on the assumption that the X-rays arise from electron captures by multiply charged ions of the solar wind in collisions with the neutral atoms and molecules of the cometary atmospheres. The collisions populate excited states of the ion formed in the transfer of charge which then decay in a cascade of radiative transitions in the soft X-ray and ultraviolet regions of the spectrum. A comparison of detailed models of the resulting spectra with observations of Comet McNaught-Hartley yield information on the solar wind ion composition. A similar process in which solar wind ions interact with neutral atoms in the heliosphere contributes to the diffuse soft X-ray background. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 2 Z9 2 U1 0 U2 3 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2003 VL 285 IS 3-4 BP 687 EP 690 DI 10.1023/A:1026161210465 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 732BH UT WOS:000185920600007 ER PT S AU Heyl, JS AF Heyl, JS BE Centrella, JM TI LMXBs may be important LIGO sources after all SO ASTROPHYSICS OF GRAVITATIONAL WAVE SOURCES SE AIP Conference Proceedings LA English DT Proceedings Paper CT Workshop on the Astrophysics of Gravitational Wave Sources CY APR 24-26, 2003 CL COLLEGE PK, MD SP NASA, NSF, Univ Maryland Phys Dept, Penn State Ctr Gratitat Wave Phys ID MILLISECOND RADIO PULSARS; ACCRETING NEUTRON-STARS; R-MODE INSTABILITY; X-RAY BINARIES; GRAVITATIONAL-RADIATION; EVOLUTION AB Andersson et al. and Bildsten proposed that the spin of accreting neutron stars is limited by removal of angular momentum by gravitational radiation which increases dramatically with the spin frequency of the star. Both Bildsten and Andersson et al. argued that the r-modes of the neutron star for sufficiently quickly rotating and hot neutron stars will grow due to the emission of gravitational radiation, thereby accounting for a time varying quadrupole component to the neutron star's mass distribution. However, Levin later argued that the equilibrium between spin-up due to accretion and spin-down due to gravitational radiation is unstable, because the growth rate of the r-modes and consequently the rate of gravitational wave emission is an increasing function of the core temperature of the star. The system executes a limit cycle, spinning up for several million years and spinning down in less than a year. However, the duration of the spin-down portion of the limit cycle depends sensitively on the amplitude at which the nonlinear coupling between different r-modes becomes important. As the duration of the spin-down portion increases the fraction of accreting neutron stars which may be emitting gravitational radiation increases while the peak flux in gravitational radiation decreases. Depending on the distribution of quickly rotating neutron stars in the Galaxy and beyond, the number of gravitational emitters detectable with LIGO may be large. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heyl, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jheyl@cfa.harvard.edu NR 31 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0157-8 J9 AIP CONF PROC PY 2003 VL 686 BP 273 EP 280 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX91T UT WOS:000186818300032 ER PT J AU Smith, TB Marra, PP Webster, MS Lovette, I Gibbs, HL Holmes, RT Hobson, KA Rohwer, S AF Smith, TB Marra, PP Webster, MS Lovette, I Gibbs, HL Holmes, RT Hobson, KA Rohwer, S TI A call for feather sampling SO AUK LA English DT Editorial Material ID BREEDING ORIGINS; ISOTOPE RATIOS; STABLE-CARBON; NORTHERN FULMARS; NITROGEN; CONNECTIVITY; POPULATIONS; WATERFOWL; INDICATE; SONGBIRD C1 Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, Ctr Trop Res, Inst Environm, Los Angeles, CA 90095 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. Cornell Univ, Ithaca, NY 14850 USA. Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. Canadian Wildlife Serv, Saskatoon, SK S7N 0X4, Canada. Univ Washington, Burke Museum, Seattle, WA 98195 USA. RP Smith, TB (reprint author), Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, 621 Charles E Young Dr S,Room LS5120,POB 951606, Los Angeles, CA 90095 USA. EM tbsmith@ucla.edu RI Lovette, Irby/P-3477-2014 NR 24 TC 38 Z9 41 U1 1 U2 17 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 JAN PY 2003 VL 120 IS 1 BP 218 EP 221 DI 10.1642/0004-8038(2003)120[0218:ACFFS]2.0.CO;2 PG 4 WC Ornithology SC Zoology GA 658AY UT WOS:000181700500028 ER PT B AU Rappole, JH Schuchmann, KL AF Rappole, JH Schuchmann, KL BE Berthold, P Gwinner, E Sonnenschein, E TI Ecology and evolution of hummingbird population movements and migration SO AVIAN MIGRATION LA English DT Proceedings Paper CT Symposium on Avian Migration CY SEP 03-06, 2001 CL UNIV KONSTANZ, CONSTANCE, GERMANY SP Max Planck Soc HO UNIV KONSTANZ ID METABOLISM; TORPOR C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. RI Schuchmann, Karl/I-1399-2015 NR 35 TC 6 Z9 6 U1 3 U2 13 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-43408-9 PY 2003 BP 39 EP 51 PG 13 WC Ornithology SC Zoology GA BX52C UT WOS:000185588600003 ER PT B AU Jehl, JR Henry, AE Ellis, HI AF Jehl, JR Henry, AE Ellis, HI BE Berthold, P Gwinner, E Sonnenschein, E TI Optimizing migration in a reluctant and inefficient flier: the Eared Grebe SO AVIAN MIGRATION LA English DT Proceedings Paper CT Symposium on Avian Migration CY SEP 03-06, 2001 CL UNIV KONSTANZ, CONSTANCE, GERMANY SP Max Planck Soc HO UNIV KONSTANZ ID WIND-TUNNEL; PODICEPS-NIGRICOLLIS; PIGEON FLIGHT; MASS; METABOLISM; ENERGETICS; ABUNDANCE; MORTALITY; BEHAVIOR; BIRDS C1 Smithsonian Inst, Natl Museum Amer Hist, Div Birds, Washington, DC 20560 USA. RP Jehl, JR (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Div Birds, Washington, DC 20560 USA. EM grebe5k@cs.com NR 44 TC 15 Z9 15 U1 0 U2 4 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-43408-9 PY 2003 BP 199 EP 209 PG 11 WC Ornithology SC Zoology GA BX52C UT WOS:000185588600013 ER PT B AU Hallager, S Ward, A Maslanka, M Boylan, J AF Hallager, S Ward, A Maslanka, M Boylan, J BE Ballentine, J Mirowitz, S TI Kori bustard nutrition and dietary husbandry SO AZA ANNUAL CONFERENCE PROCEEDINGS 2002 LA English DT Proceedings Paper CT Annual Conference of the American-Zoo-and-Aquarium-Association CY SEP 09-11, 2000 CL Ft Worth Zoo, Ft Worth, TX SP Amer Zoo Aquarium Assoc HO Ft Worth Zoo C1 Smithsonian Natl Zool Pk, Washington, DC USA. RP Hallager, S (reprint author), Smithsonian Natl Zool Pk, 3001 Connecticut Ave, Washington, DC USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU AMER ZOO & AQUARIUM ASSOC (AZA) PI SILVER SPRING PA 8403 COLESVILLE RD, SUITE 710, SILVER SPRING, MD 20910 USA PY 2003 BP 25 EP 25 PG 1 WC Biodiversity Conservation; Education, Scientific Disciplines; Zoology SC Biodiversity & Conservation; Education & Educational Research; Zoology GA BY54S UT WOS:000189405300007 ER PT B AU Howard, JG Marinari, P Wildt, DE AF Howard, JG Marinari, P Wildt, DE BE Ballentine, J Mirowitz, S TI Integration of assisted reproductive technology in the recovery of the black-footed ferret (Mustela nigripes) SO AZA ANNUAL CONFERENCE PROCEEDINGS 2002 LA English DT Proceedings Paper CT Annual Conference of the American-Zoo-and-Aquarium-Association CY SEP 09-11, 2000 CL Ft Worth Zoo, Ft Worth, TX SP Amer Zoo Aquarium Assoc HO Ft Worth Zoo ID RESOURCE BANKS; INSEMINATION; CONSERVATION; PHOTOPERIOD; PROFILES C1 Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. RP Howard, JG (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 33 TC 0 Z9 0 U1 0 U2 2 PU AMER ZOO & AQUARIUM ASSOC (AZA) PI SILVER SPRING PA 8403 COLESVILLE RD, SUITE 710, SILVER SPRING, MD 20910 USA PY 2003 BP 55 EP 60 PG 6 WC Biodiversity Conservation; Education, Scientific Disciplines; Zoology SC Biodiversity & Conservation; Education & Educational Research; Zoology GA BY54S UT WOS:000189405300013 ER PT B AU Ferster, A AF Ferster, A BE Ballentine, J Mirowitz, S TI Putting kid power to work for your zoo SO AZA ANNUAL CONFERENCE PROCEEDINGS 2002 LA English DT Proceedings Paper CT Annual Conference of the American-Zoo-and-Aquarium-Association CY SEP 09-11, 2000 CL Ft Worth Zoo, Ft Worth, TX SP Amer Zoo Aquarium Assoc HO Ft Worth Zoo C1 Smithsonian Inst, Natl Zool Pk, Off Exhibits & Outreach, Washington, DC 20008 USA. RP Ferster, A (reprint author), Smithsonian Inst, Natl Zool Pk, Off Exhibits & Outreach, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU AMER ZOO & AQUARIUM ASSOC (AZA) PI SILVER SPRING PA 8403 COLESVILLE RD, SUITE 710, SILVER SPRING, MD 20910 USA PY 2003 BP 103 EP 105 PG 3 WC Biodiversity Conservation; Education, Scientific Disciplines; Zoology SC Biodiversity & Conservation; Education & Educational Research; Zoology GA BY54S UT WOS:000189405300023 ER PT J AU Kepler, SO Nather, ER Winget, DE Nitta, A Kleinman, SJ Metcalfe, T Sekiguchi, K Xiaojun, J Sullivan, D Sullivan, T Janulis, R Meistas, EG Kalytis, R Krzesinski, J Ogloza, W Zola, S O'Donoghue, D Romero-Colmenero, E Martinez, P Dreizler, S Deetjen, J Nagel, T Schuh, SL Vauclair, G Fu, JN Chevreton, M Solheim, JE Perez, JMG Johannessen, F Kanaan, A Costa, JE Costa, AFM Wood, MA Silvestri, N Ahrens, TJ Jones, AK Collins, AE Boyer, M Shaw, JS Mukadam, AS Klumpe, EW Larrison, J Kawaler, SD Riddle, RL Ulla, A Bradley, P AF Kepler, SO Nather, ER Winget, DE Nitta, A Kleinman, SJ Metcalfe, T Sekiguchi, K Xiaojun, J Sullivan, D Sullivan, T Janulis, R Meistas, EG Kalytis, R Krzesinski, J Ogloza, W Zola, S O'Donoghue, D Romero-Colmenero, E Martinez, P Dreizler, S Deetjen, J Nagel, T Schuh, SL Vauclair, G Fu, JN Chevreton, M Solheim, JE Perez, JMG Johannessen, F Kanaan, A Costa, JE Costa, AFM Wood, MA Silvestri, N Ahrens, TJ Jones, AK Collins, AE Boyer, M Shaw, JS Mukadam, AS Klumpe, EW Larrison, J Kawaler, SD Riddle, RL Ulla, A Bradley, P TI WET observations of GD 358 in 2000 SO BALTIC ASTRONOMY LA English DT Article; Proceedings Paper CT 6th Whole Earth Telescope Workshop (WET) CY JUN 20-21, 2002 CL NAPLES, ITALY DE stars : individual : GD 358; stars : evolution ID WHITE-DWARF GD-358; WHOLE EARTH TELESCOPE; ZZ-CETI STARS AB We report on the 323 hours of nearly uninterrupted time series photometric observations of the DBV star GD 358 acquired with the Whole Earth Telescope (WET) during May 23 to June 8, 2000. We acquired more than 232000 independent measurements and detected the non-radial g-modes consistent with degree l = 1 and radial order 8 to 20 and their linear combinations up to 6th order. We also detect, for the first time, a high amplitude l = 2 mode, with a period of 796 s. In the 2000 WET data, the largest amplitude modes are similar to those detected with the WET observations of 1990 and 1994, but the highest combination order previously detected was 4th order. C1 UFRGS, Inst Fis, Porto Alegre, RS, Brazil. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Sloan Digital Sky Survey, Apache Pt Observ, Sunspot, NM 88349 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Beijing Astron Observ, Beijing 100080, Peoples R China. Univ Victoria, Wellington, New Zealand. Inst Theoret Phys & Astron, LT-2600 Vilnius, Lithuania. Cracow Pedagog Univ, Mt Suhora Observ, PL-30084 Krakow, Poland. Jagiellonian Univ, PL-30244 Krakow, Poland. S African Astron Observ, Cape Town, South Africa. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Univ Toulouse 3, Observ Midi Pyrenees, CNRS, UMR5572, F-31400 Toulouse, France. DAEC, Observ Paris Meudon, F-92195 Meudon, France. Univ Tromso, Inst Fys, N-9037 Tromso, Norway. Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. Florida Inst Technol, SARA Observ, Melbourne, FL 32901 USA. Univ Florida, Nucl Sci Ctr 202, Gainesville, FL 32611 USA. Johnson Space Ctr, Houston, TX 77058 USA. Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37132 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Vigo, Dept Fis Aplicada, Fac Ciencias, Vigo 36200, Pontevedra, Spain. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Vilnius State Univ, Astron Observ, LT-2009 Vilnius, Lithuania. RP Kepler, SO (reprint author), UFRGS, Inst Fis, Porto Alegre, RS, Brazil. RI Metcalfe, Travis/A-9388-2008; Kepler, S. O. /H-5901-2012; Ulla Miguel, Ana Maria/M-2860-2014; OI Metcalfe, Travis/0000-0003-4034-0416; Kepler, S. O. /0000-0002-7470-5703; Kawaler, Steven/0000-0002-6536-6367 NR 14 TC 1 Z9 1 U1 0 U2 1 PU INST THEORETICAL PHYSICS ASTRONOMY PI MOLETAI PA MOLETAI LT-4150, LITHUANIA SN 1392-0049 J9 BALT ASTRON JI Balt. Astron. PY 2003 VL 12 IS 1 BP 45 EP 53 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710UA UT WOS:000184698800008 ER PT J AU Stuntz, S Linder, C Linsenmair, KE Simon, U Zotz, G AF Stuntz, S Linder, C Linsenmair, KE Simon, U Zotz, G TI Do non-myrmocophilic epiphytes influence community structure of arboreal ants? SO BASIC AND APPLIED ECOLOGY LA English DT Article DE Annona glabra; ant mosaic theory; canopy; insect traps; Panama ID RAIN-FOREST; COCOA FARMS; BODY-SIZE; DIVERSITY; PATTERNS; CANOPY; MICROCLIMATE; MAINTENANCE; ARTHROPODS; FORMICIDAE AB In a one-year-survey in Panama we examined the influence of a tree crown's epiphyte assemblage on its ant fauna. Ants were collected with various types of insect traps in 25 crowns of Annona glabra trees. The study trees were assigned to three different categories according to their epiphyte load, and to an epiphyte-free control group. We collected 22,335 specimens of 91 morphospecies, 32 genera and six subfamilies. By far the most abundant species was Solenopsis zeteki, a minute Myrmicinae, which was found in each of the 25 study trees. Many other species were also rather common and widely distributed throughout the study area. Only six species were singletons. Measures of alpha- and beta-diversity, species abundance and species composition were not affected by the epiphyte load of a tree. We also made direct in situ observations of ants on 34 additional Annona glabra trees with and without epiphytes. Workers were attracted with tuna and sugar baits, and interspecific interactions and nesting sites were recorded. in total, 40 species of ants were found, all of which had also been collected in the traps. Almost half of the colonies (48%) used dead wood as nesting substrate, while 29% nested in epiphytes. Consistent with the results of the trap survey, the epiphyte load of the study trees had no influence on ant species richness and composition, but a significant correlation between ant abundance and epiphyte load was detectable. In both data sets, the lack of associations between ant species indicated that the ant assemblages were not structured in a mosaic-like fashion. We conclude that epiphytes do hardly influence the composition of ant assemblages in the studied tree crowns, probably because arboreal ants are highly opportunistic with respect to their host plants. C1 Univ Wurzburg, Lehrstuhl Bot 2, D-97082 Wurzburg, Germany. Univ Bielefeld, D-33615 Bielefeld, Germany. Univ Wurzburg, Lehrstuhl Zool 3, D-97074 Wurzburg, Germany. Tech Univ Munich, Forstwissenschaftliche Fak, D-85354 Freising Weihenstephan, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM gerhard.zotz@unibas.ch NR 51 TC 12 Z9 12 U1 1 U2 11 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1439-1791 J9 BASIC APPL ECOL JI Basic Appl. Ecol. PY 2003 VL 4 IS 4 BP 363 EP 373 DI 10.1078/1439-1791-00170 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 713VV UT WOS:000184879400009 ER PT J AU DeRivera, CE Backwell, PRY Christy, JH Vehrencamp, SL AF DeRivera, CE Backwell, PRY Christy, JH Vehrencamp, SL TI Density affects female and male mate searching in the fiddler crab, Uca beebei SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE mate searching; sexual conflict; density effects; predation effects; fiddler crabs ID MATING SYSTEM; PILLAR FUNCTION; WATER STRIDERS; PREDATION RISK; CHOICE; COURTSHIP; BEHAVIOR; OCYPODIDAE; EVOLUTION; PUGILATOR AB In most species, only one sex searches for mates while the other waits. Models, of sex-specific mate-searching behavior predict single-sex searching, but the factors that determine which sex searches are not understood. In this study, we examine the effects of density and predation risk on mate-searching behavior in the fiddler crab Uca beebei. U. beebei is one of the few fiddler-crab species in which both sexes search for mates. In a field experiment conducted in Panama, we manipulated crab density and perceived predation risk in replicate plots. Females searched more and males searched less at high densities. At high levels of-perceived predation risk, both sexes similarly reduced their search rates. Observations of plots that naturally varied in crab density show that females were more likely to search for mates in areas of higher density, where there were more males. Females may preferentially search for mates in high-density areas because the abundance of nearby burrows, into which they can run to escape predators, decreases their costs of searching and because the abundance of males and male burrows facilitates comparisons and thus may increase their benefits from searching. Males at high densities decrease their mate-searching rate perhaps in response to the increase in female searching and to the corresponding increase in the intensity of their competitors' mate-attraction signals. C1 Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Cornell Univ, Ornithol Lab, Ithaca, NY 14850 USA. Univ Calif San Diego, Dept Biol, La Jolla, CA 92093 USA. RP DeRivera, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM deriverac@si.edu RI Backwell, Patricia/C-8883-2009 NR 54 TC 43 Z9 45 U1 1 U2 9 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 EI 1432-0762 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD JAN PY 2003 VL 53 IS 2 BP 72 EP 83 DI 10.1007/s00265-002-0555-2 PG 12 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 643QL UT WOS:000180871900002 ER PT J AU Christy, JH Backwell, PRY Schober, U AF Christy, JH Backwell, PRY Schober, U TI Interspecific attractiveness of structures built by courting male fiddler crabs: experimental evidence of a sensory trap SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE landmark orientation; mate search risk; predator avoidance; sensory trap; Uca ID SEXUAL SELECTION; FEMALE CHOICE; MATE CHOICE; UCA-BEEBEI; RECEIVER BIASES; BEHAVIOR; EVOLUTION; COURTSHIP; OCYPODIDAE; SPECIATION AB Male fiddler crabs Uca musica sometimes build sand hoods and male Uca beebei sometimes build mud pillars next to their burrows to which they attract females for mating. Mate-searching females preferentially approach these structures and subsequently mate with structure builders. Here we show that the preference for structures is not species-specific and argue that it may not have evolved for mate choice. When not near burrows, many species of fiddler crabs approach and temporarily hide near objects, suggesting that hoods and pillars may attract females because they elicit this general predator-avoidance behavior. To test this sensory trap hypothesis we individually released female U. musica, U. beebei and Uca stenodactylus, a non-builder, in the center of a circular array of empty burrows to which we added hoods and pillars and then moved a model predator toward the females. All species ran to structures to escape the predator and the two builders preferred hoods. Next, we put hood replicas on male U. beebei burrows and pillar replicas on male U. musica burrows. When courted, females of both species preferentially approached hoods as they did when chased with a predator. However, males of both species with hoods did not have higher mating rates than males with pillars perhaps because hoods block more of a male's visual field so he sees and courts fewer females. Sexual selection may often favor male signals that attract females because they facilitate general orientation or navigation mechanisms that reduce predation risk in many contexts, including during mate search. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Unit 0948, APO, AA 34002 USA. Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. Univ Vet Med, Lab Ecotoxicol, Vienna, Austria. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. RI Backwell, Patricia/C-8883-2009 NR 63 TC 44 Z9 45 U1 2 U2 11 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 JAN PY 2003 VL 53 IS 2 BP 84 EP 91 DI 10.1007/s00265-002-0553-4 PG 8 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 643QL UT WOS:000180871900003 ER PT J AU Brown, JL Hildebrandt, TB AF Brown, JL Hildebrandt, TB TI The science behind elephant artificial insemination. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 36th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 19-22, 2003 CL CINCINNATI, OHIO SP Soc Study Reproduct C1 Conservat & Res Ctr, Smithsonian Natl Zool Pk, Front Royal, VA USA. Inst Zool Biol & Wildlife Res, Berlin, Germany. NR 0 TC 1 Z9 1 U1 0 U2 3 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2003 VL 68 SU 1 MA MS17 BP 95 EP 96 PG 2 WC Reproductive Biology SC Reproductive Biology GA 695FX UT WOS:000183821400028 ER PT J AU Kersey, DC Brown, JL Czekala, NM Monfort, SL AF Kersey, DC Brown, JL Czekala, NM Monfort, SL TI Fecal steroid monitoring to study the reproductive biology of endangered giant panda (Ailuropoda melanoleuca). SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 36th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 19-22, 2003 CL CINCINNATI, OHIO SP Soc Study Reproduct C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Zool Soc San Diego, Dept Res, San Diego, CA USA. NR 0 TC 4 Z9 4 U1 1 U2 4 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2003 VL 68 SU 1 MA 34 BP 125 EP 126 PG 2 WC Reproductive Biology SC Reproductive Biology GA 695FX UT WOS:000183821400090 ER PT J AU Staley, AM Blanco, JM Dufty, AM Wildt, DE Monfort, SL AF Staley, AM Blanco, JM Dufty, AM Wildt, DE Monfort, SL TI Noninvasive fecal steroid monitoring provides insight into gonadal and adrenal function in the golden eagle (Aquila chrysaetos) and peregrine falcon (Falco peregrinus). SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 36th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 19-22, 2003 CL CINCINNATI, OHIO SP Soc Study Reproduct C1 Boise State Univ, Dept Biol, Boise, ID 83725 USA. Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Sevilleja Jara, Ctr Estudios Rapaces Ibericas, Castilla Mancha, Spain. NR 0 TC 1 Z9 1 U1 1 U2 3 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2003 VL 68 SU 1 MA 35 BP 126 EP 126 PG 1 WC Reproductive Biology SC Reproductive Biology GA 695FX UT WOS:000183821400091 ER PT J AU Pukazhenthi, BS Rockett, JC Ouyang, M Dix, DJ Howard, J Georgopoulos, P Welsh, WJ Wildt, DE AF Pukazhenthi, BS Rockett, JC Ouyang, M Dix, DJ Howard, J Georgopoulos, P Welsh, WJ Wildt, DE TI Gene expression in the testes of normospermic versus teratospermic domestic cats using human cDNA microarray analyses. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 36th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 19-22, 2003 CL CINCINNATI, OHIO SP Soc Study Reproduct C1 Smithsonian Natl Zool Pk, Dept Reprod Sci, Washington, DC USA. US EPA, NHEERL, ORD, Reprod Toxicol Div, Res Triangle Pk, NC 27711 USA. Univ Med & Dent New Jersey, Inst Informat, Piscataway, NJ 08854 USA. Rutgers State Univ, Univ Med & Dent New Jersey, Environm & Occupat Hlth Sci Inst, Piscataway, NJ USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2003 VL 68 SU 1 MA 194 BP 191 EP 192 PG 2 WC Reproductive Biology SC Reproductive Biology GA 695FX UT WOS:000183821400249 ER PT J AU Comizzoli, P Wildt, DE Pukazhenthi, BS AF Comizzoli, P Wildt, DE Pukazhenthi, BS TI Enhanced in vitro nuclear maturation and developmental competence of domestic cat oocytes during the non-breeding season. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 36th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 19-22, 2003 CL CINCINNATI, OHIO SP Soc Study Reproduct C1 Smithsonian Inst, Dept Reprod Sci, Natl Zool Pk, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2003 VL 68 SU 1 MA 215 BP 199 EP 200 PG 2 WC Reproductive Biology SC Reproductive Biology GA 695FX UT WOS:000183821400270 ER PT J AU Songsasen, N Leibo, SP Wildt, DE AF Songsasen, N Leibo, SP Wildt, DE TI Effect of energy substrates on nuclear maturation of domestic dog oocytes SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 36th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 19-22, 2003 CL CINCINNATI, OHIO SP Soc Study Reproduct C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA USA. Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA. NR 0 TC 1 Z9 1 U1 1 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2003 VL 68 SU 1 MA 352 BP 257 EP 257 PG 1 WC Reproductive Biology SC Reproductive Biology GA 695FX UT WOS:000183821400406 ER PT J AU Pertola, S Faust, MA Kuosa, H Hallfors, G AF Pertola, S Faust, MA Kuosa, H Hallfors, G TI Morphology of Prorocentrum minimum (Dinophyceae) in the Baltic Sea and in Chesapeake Bay: Comparison of cell shapes and thecal ornamentation SO BOTANICA MARINA LA English DT Article DE Baltic Sea; Chesapeake Bay; dinoflagellate; morphology; Prorocentrum minimum ID DINOFLAGELLATE HETEROCAPSA-TRIQUETRA; RED-TIDE-DINOFLAGELLATE; GENERA-PROROCENTRUM; FINE-STRUCTURE; EXUVIAELLA; NOV AB Prorocentrum minimum (Dinophyceae) is a red tideforming toxinproducing planktonic microalga from coastal waters worldwide. In this study, the morphology of natural and cultured populations of P. minimum was examined to investigate whether the species can be split morphologically into more species. The diacritical features of cell shape and size, ornamentation of thecal plates, and architecture of the apical pore area and intercalary band were studied from scanning and light micrographs. Cell size of P. minimum is similar in Baltic Sea samples and a culture from the Chesapeake Bay, USA. Cell shape varies from triangular to ovalround including intermediate forms in valve view. The thecal surface is covered by evenly distributed short spines, while the circular thecal pores are mainly situated near the valve margin.The intercalary band is rimlike, striated and covered with short evenly distributed spines. The architecture of the apical pore area is ornate and more complex than previously pointed out. It is Vshaped, located on the right valve in a shallow depression and accommodates a large elongated flagellar pore, and a small round auxiliary pore. Four distinct apical features are present: next to the auxiliary pore there is a curved collar, and adjacent to the flagellar pore arise a forked double tooth, a short single tooth, and a ridged edge near the left valve margin. Our study suggests that the ornamentation of the apical pore area of P. minimum is independent of cell shape or growth place, and it is considered a stable morphological character of this cosmopolitan morphospecies. C1 Finnish Inst Marine Res, FIN-00931 Helsinki, Finland. Smithsonian Inst, Museum Support Ctr, Natl Museum Nat Hist, Dept Systemat Biol Bot, Suitland, MD 20746 USA. Univ Helsinki, Tvarminne Zool Stn, FIN-10900 Hango, Finland. RP Pertola, S (reprint author), Finnish Inst Marine Res, POB 33, FIN-00931 Helsinki, Finland. NR 46 TC 10 Z9 10 U1 1 U2 2 PU WALTER DE GRUYTER & CO PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0006-8055 J9 BOT MAR JI Bot. Marina PY 2003 VL 46 IS 5 BP 477 EP 486 DI 10.1515/BOT.2003.049 PG 10 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 719DX UT WOS:000185189300011 ER PT J AU Wasshausen, DC Wood, JRI AF Wasshausen, DC Wood, JRI TI The genus Dyschoriste (Acanthaceae) in Bolivia and Argentina SO BRITTONIA LA English DT Article DE Acanthaceae; Dyschoriste; Bolivia; Argentina AB Wasshausen, D. C. (Department of Systematic Biology-Botany, National Museum of Natural History, Smithsonian Institution, Washington, D.C. 20560, U.S.A.; email: wasshausen.dieter@nmnh.si.edu) & J. R. 1. Wood (111 Forest Road, Liss, Hampshire, GU33 7BP, Great Britain). The genus Dyschoriste (Acanthaceae) in Bolivia and Argentina. Brittonia 55: 10-18. 2003.- Recent field work in Bolivia has resulted in the recognition of new species of Dyschoriste (Acanthaceae). These novelties are introduced here for the convenience of other taxonomists prior to the publication of a treatment of the Acanthaceae of Bolivia. Three new Bolivian and one new Argentinean species of Dyschoriste, D. axillaris, D. boliviana, D. ceciliae, and D. prostrata are described, illustrated, and compared to their closest relatives. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Syst Biol, Washington, DC 20560 USA. RP Wasshausen, DC (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Syst Biol, Washington, DC 20560 USA. NR 4 TC 3 Z9 5 U1 0 U2 0 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD JAN-MAR PY 2003 VL 55 IS 1 BP 10 EP 18 DI 10.1663/0007-196X(2003)055[0010:TGDAIB]2.0.CO;2 PG 9 WC Plant Sciences SC Plant Sciences GA 690YQ UT WOS:000183578400003 ER PT S AU Bate, MR Bonnell, IA Bromm, V AF Bate, MR Bonnell, IA Bromm, V BE Martin, EL TI The formation mechanism and resulting properties of brown dwarfs SO BROWN DWARFS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 211th Symposium of the International-Astronomical-Union CY MAY 20-24, 2002 CL BIG ISL, HAWAII SP Int Astron Union ID INITIAL MASS FUNCTION AB We present results from the most complex hydrodynamical star formation calculation performed to date. It follows the collapse and fragmentation of a large-scale turbulent molecular cloud to form dozens of stars and brown dwarfs. It resolves all fragmentation down to the opacity limit, binary stars with separations as small as 1 AU, and circumstellar disks with radii down to approximate to 10 AU. In this proceedings, we examine the formation mechanism of the brown dwarfs-and compare the initial mass function and the properties of the brown dwarfs with observations. C1 Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bate, MR (reprint author), Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. NR 13 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-132-X J9 IAU SYMP PY 2003 IS 211 BP 27 EP 30 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX04E UT WOS:000184043700004 ER PT S AU Muench, AA Lada, EA Lada, CJ Alves, JF AF Muench, AA Lada, EA Lada, CJ Alves, JF BE Martin, EL TI The substellar luminosity and mass functions of the trapezium cluster down to the deuterium burning limit SO BROWN DWARFS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 211th Symposium of the International-Astronomical-Union CY MAY 20-24, 2002 CL BIG ISL, HAWAII SP Int Astron Union AB We have employed an advanced suite of Monte Carlo calculations to model the infrared luminosity function (KLF) of the Trapezium cluster and to derive its Sub-stellar Initial Mass Function down to the deuterium burning limit. Independent of the details, we find that substellar objects can account for no more than similar to 22% of the total number of likely cluster members. This cluster's substellar IMF steadily declines in a power-law fashion over most of the brown dwarf regime, however the formation of a secondary. peak in the cluster's substellar KLF suggests the existence of a corresponding secondary peak in the substellar IMF between 10 and 30 times the mass of Jupiter based upon the seemingly degenerate behavior of the theoretical substellar mass-luminosity relation. C1 Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-8574 Garching, Germany. RP Muench, AA (reprint author), Univ Florida, Dept Astron, 211 SSRB, Gainesville, FL 32611 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-132-X J9 IAU SYMP PY 2003 IS 211 BP 67 EP 68 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX04E UT WOS:000184043700011 ER PT S AU Briceno, C Luhman, KL Hartmann, L Stauffer, JR Kirkpatrick, JD AF Briceno, C Luhman, KL Hartmann, L Stauffer, JR Kirkpatrick, JD BE Martin, EL TI The brown dwarf deficit in Taurus: Evidence for a non-universal IMF SO BROWN DWARFS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 211th Symposium of the International-Astronomical-Union CY MAY 20-24, 2002 CL BIG ISL, HAWAII SP Int Astron Union AB We present the results of a deep, optical/IR wide field imaging survey of selected fields in the nearby (dsimilar to 140 pc) Taurus star-forming region. We report the discovery of 9 new members with spectral types M5.75-M9.5. We derive an Initial Mass Function encompassing 54% of the known members in Taurus. Comparison with dense regions like the Trapezium Cluster in Orion shows that Taurus has produced x2 less brown dwarfs. We suggest that the lower frequency of brown dwarfs in Taurus may result from the low-density star-forming environment, leading to larger minimum Jeans masses. C1 CIDA, Merida 5101A, Venezuela. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. CALTECH, IPAC, Pasadena, CA 91125 USA. RP Briceno, C (reprint author), CIDA, Apartado Postal 264, Merida 5101A, Venezuela. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-132-X J9 IAU SYMP PY 2003 IS 211 BP 81 EP 82 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX04E UT WOS:000184043700016 ER PT S AU Muzerolle, J Hillenbrand, L Briceno, C Calvet, N Hartmann, L AF Muzerolle, J Hillenbrand, L Briceno, C Calvet, N Hartmann, L BE Martin, EL TI Accretion in very low mass young objects SO BROWN DWARFS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 211th Symposium of the International-Astronomical-Union CY MAY 20-24, 2002 CL BIG ISL, HAWAII SP Int Astron Union AB We have investigated evidence for active accretion in a sample of similar to 30 young, very low mass objects, including at least 10 brown dwarfs. About 30% of the sample exhibits broad, asymmetric Ha emission line profiles, indicative of gas accretion via magnetospheric infall. There is a distinct lack of associated optical continuum veiling in these accretors, suggesting very low mass accretion rates. Our models yield an upper limit to the accretion rates that is several orders of magnitude smaller than typical of higher-mass T Tauri stars, suggesting a dependence of accretion rates with stellar mass. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. CIDA, Merida 5101A, Venezuela. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Muzerolle, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-132-X J9 IAU SYMP PY 2003 IS 211 BP 141 EP 142 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX04E UT WOS:000184043700029 ER PT S AU Wolk, SJ AF Wolk, SJ BE Martin, EL TI X-ray detection of brown dwarfs with Chandra SO BROWN DWARFS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 211th Symposium of the International-Astronomical-Union CY MAY 20-24, 2002 CL BIG ISL, HAWAII SP Int Astron Union ID SUBSTELLAR OBJECTS; YOUNG STELLAR; BONA-FIDE; CLUSTER; IC-348; CLOUD AB I review recent observations of brown dwarfs by the Chandra X-ray Observatory. These observations fall in 2 categories, young stellar clusters which contain brown dwarfs and brown dwarf candidates and directed pointings at brown dwarfs. and very low mass stars. Surprisingly, there axe already over 60 published detections of brown dwarfs by Chandra. A review of the X-ray, characteristics shows these objects axe subject to flaring and their temperatures and luminosities have avast range which is related to age. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-132-X J9 IAU SYMP PY 2003 IS 211 BP 447 EP 450 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX04E UT WOS:000184043700094 ER PT J AU Donlan, CJ Nelson, PA AF Donlan, CJ Nelson, PA TI Observations of invertebrate colonized flotsam in the eastern tropical Pacific, with a discussion of rafting SO BULLETIN OF MARINE SCIENCE LA English DT Article ID LONG-DISTANCE DISPERSAL; BENTHIC INVERTEBRATES; SURFACE SLICKS; PLANES-MINUTUS; INTERNAL WAVES; GRAPSID CRAB; REEF CORALS; FISHES; FRONTS; RECRUITMENT C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Comis Interamer Atun Trop, Lab Achotines, Las Tablas, Los Santos, Panama. Emory Univ, Yerkes Reg Primate Res Ctr, Atlanta, GA 30329 USA. RP Donlan, CJ (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. NR 65 TC 6 Z9 6 U1 2 U2 7 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 2003 VL 72 IS 1 BP 231 EP 240 PG 10 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 709YA UT WOS:000184653100017 ER PT J AU Puyravaud, JP Mohandass, D Chhabra, T AF Puyravaud, JP Mohandass, D Chhabra, T TI A rediscovery of Eriochrysis rangacharii C. E. C. Fisch. (Poaceae) in the Nilgiri Mountains of southern India SO CANDOLLEA LA English DT Article DE Poaceae; India; endemism; ethnobotany; conservation AB The Red Data Book of Indian Plants considers that Eriochrysis rangacharii C. E. C. Fisch. is extinct. However, this grass is very much utilized, because the Todas, a tribe of the high plateau of the Nilgiris, employ it as a thatching material for their temples and their traditional houses. It also provides fodder to their buffaloes. This plant, which thus constitutes a major resource for the perenniality, of the traditions of this ethnic group, was managed in a careful way during centuries. Today, the swamps where it grows are threatened with destruction by inappropriate management. The swamps of the Nilgiris must quickly be protected, otherwise E. rangacharii might face a second extinction which could well be final. This rediscovery - which is not a rediscovery for the Todas - shows once more that traditional knowledge should be taken into consideration for a better management of the biodiversity. C1 Smithsonian Trop Res Inst, Balboa, Panama. Pondicherry Univ, Salim Ali Sch Ecol & Environm Sci, Kalapet 605014, India. Dent Clin, Ootacamund 643001, India. RP Puyravaud, JP (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. NR 6 TC 5 Z9 5 U1 0 U2 1 PU CONSERVATOIRE ET JARDIN BOTANIQUES VILLE GENEVE PI CHAMBESY PA CASE POSTALE 60, CH-1292 CHAMBESY, SWITZERLAND SN 0373-2967 J9 CANDOLLEA JI Candollea PY 2003 VL 58 IS 1 BP 97 EP 100 PG 4 WC Plant Sciences SC Plant Sciences GA 716HG UT WOS:000185022300006 ER PT J AU Santiago-Blay, JA Alvarez-Ruiz, M Diaz-Soltero, H Medina-Gaud, S Quevedo-Bonilla, V Rosado-Alberio, J Velez, MJ Woodbury, L AF Santiago-Blay, JA Alvarez-Ruiz, M Diaz-Soltero, H Medina-Gaud, S Quevedo-Bonilla, V Rosado-Alberio, J Velez, MJ Woodbury, L TI Roy Orlo Woodbury (1913-2002): An extraordinary field biologist SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Biographical-Item C1 Museum Natl Hist Nat, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. Univ Puerto Rico, Dept Biol, Ponce, PR 00732 USA. USDA, Forest Serv, Pacific SW Res Stn, Albany, CA 94710 USA. Univ Puerto Rico, Dept Crop Protect, Rio Piedras, PR 00928 USA. Univ Puerto Rico, Agr Expt Stn, Rio Piedras, PR 00928 USA. Programa Pro Patrimonio Nat Puerto Rico, Dept Nat & Environm Resources, San Juan, PR 00906 USA. Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA. Fairchild Trop Garden, Res Ctr, Miami, FL 33156 USA. RP Santiago-Blay, JA (reprint author), Museum Natl Hist Nat, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. NR 1 TC 2 Z9 2 U1 0 U2 1 PU UNIV PUERTO RICO, PI MAYAGUEZ PA COLLEGE ARTS SCIENCES, MAYAGUEZ, PUERTO RICO 00680 USA SN 0008-6452 J9 CARIBB J SCI JI Caribb. J. Sci. PY 2003 VL 39 IS 1 BP 2 EP 10 PG 9 WC Biodiversity Conservation SC Biodiversity & Conservation GA 663TZ UT WOS:000182023300001 ER PT B AU Bergin, EA AF Bergin, EA BE Fich, M TI The chemistry of dark clouds: New astrochemical tools for star formation studies SO CHEMISTRY AS A DIAGNOSTIC OF STAR FORMATION LA English DT Proceedings Paper CT Conference on Chemistry as a Diagnostic of Star Formation CY AUG 21-23, 2002 CL Univ Waterloo, Waterloo, CANADA SP CITA, COM DEV Space, CSA HO Univ Waterloo DE astrochemistry; ISM : molecules; ISM : globules; ISM : clouds; stars : formation ID DENSE INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; PROTOSTELLAR CORES; FORMING REGIONS; CHEMICAL-MODELS; RADIATIVE-TRANSFER; INTERNAL STRUCTURE; WATER ABUNDANCE; CO DEPLETION; IC 5146 AB The past decade has led to significant improvements in our understanding of the physical structure of the molecular cores of cold dark clouds. Observational efforts, in combination with improved knowledge of cloud structure, now provide clear evidence that the chemistry of dark clouds is dominated by the depletion of gaseous species onto grain surfaces. We outline the basis of these observational efforts and show how the abundance determinations have moved beyond single point analyses to the derivation of abundance profiles. We discuss the basic physics of the interaction between molecules and grain surfaces and show that when physics is coupled into a chemical model there is excellent agreement, for a limited set of species, between theory and observations. We discuss our improved understanding of cloud chemistry can be used as a new tool for studies of the formation of stars and planetary systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 54 TC 0 Z9 0 U1 0 U2 1 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA BUILDING M-55, OTTAWA, ON KIA OR6, CANADA BN 0-660-19089-3 PY 2003 BP 63 EP 72 PG 10 WC Astronomy & Astrophysics; Chemistry, Applied SC Astronomy & Astrophysics; Chemistry GA BAU23 UT WOS:000223569400012 ER PT B AU Li, D Goldsmith, PF Melnick, GJ AF Li, D Goldsmith, PF Melnick, GJ BE Fich, M TI Large-scale mapping of the rho Ophiuchi region by SWAS SO CHEMISTRY AS A DIAGNOSTIC OF STAR FORMATION LA English DT Proceedings Paper CT Conference on Chemistry as a Diagnostic of Star Formation CY AUG 21-23, 2002 CL Univ Waterloo, Waterloo, CANADA SP CITA, COM DEV Space, CSA HO Univ Waterloo DE radio lines : ISM; ISM : individual (rho Ophiuchi) ID DARK-CLOUD; MAIN CLOUD; C I; (CO)-C-13; EXTINCTION AB We have completed a 3 square degree C I P-3(1)-P-3(0) map of the rho Ophiuchi regions using SWAS. The remarkably stable receiver and back end systems of S WAS allow for uniformly calibrated data set on this scale. Combined with (CO)-C-12, (CO)-C-13, and (CO)-O-18 maps made using FCRAO, this data set will facilitate a thorough study of the physics and chemistry in this nearby star-forming region. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, D (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA BUILDING M-55, OTTAWA, ON KIA OR6, CANADA BN 0-660-19089-3 PY 2003 BP 347 EP 349 PG 3 WC Astronomy & Astrophysics; Chemistry, Applied SC Astronomy & Astrophysics; Chemistry GA BAU23 UT WOS:000223569400071 ER PT J AU Pasteels, JM Theuring, C Windsor, DM Hartmann, T AF Pasteels, JM Theuring, C Windsor, DM Hartmann, T TI Uptake and metabolism of [C-14]rinderine and [C-14]retronecine in leaf-beetles of the genus Platyphora and alkaloid accumulation in the exocrine defensive secretions SO CHEMOECOLOGY LA English DT Article DE alkaloid sequestration; chemical defense; host-plant selection; Platyphora leaf beetles; pyrrolizidine alkaloids ID PYRROLIZIDINE ALKALOIDS; CHEMICAL DEFENSE; TRITERPENE SAPONINS; ITHOMIINE BUTTERFLIES; UTETHEISA-ORNATRIX; SEQUESTRATION; OREINA; BIOSYNTHESIS; MECHANISMS; ARTHROPODS AB Sequestration and processing of pyrrolizidine alkaloids (PAs) by leaf beetles of the genus Platyphora were investigated. Tracer experiments with labeled alkaloids were performed with R eucosma feeding on Koanophyllon panamense (Asteraceae, tribe Eupatorieae). R eucosma catalyzes the same reactions previously demonstrated for R boucardi specialized to Prestonia portobellensis (Apocynaceae): (i) epimerization of rinderine to intermedine; (ii) esterification of retronecine yielding insect-specific PAs; (iii) efficient transport of the PAs as free bases into the defensive secretions. P. bella feeding on Tournefortia cuspidata (Boraginaceae) shows the same sequestration behavior and ability to synthesize the specific retronecine esters. R ligata, a species phylogenetically closely related to the PA adapted species and clustering in the same clade, but feeding on a host plant devoid of PAs, feeds easily on PA treated host-plant leaves, but does not sequester or metabolize PAs. P kollari a species clustering outside the PA clade refused to feed on its food-plant leaves painted with PAs. The results are discussed in relation to host-plant selection of the PA adapted species and the role of PAs in chemical defense. C1 Tech Univ Carolo Wilhelmina Braunschweig, Inst Pharmazeut Biol, D-38106 Braunschweig, Germany. Free Univ Brussels, Lab Biol Anim & Cellulaire, B-1050 Brussels, Belgium. Smithsonian Trop Res Inst, Balboa, Panama. RP Pasteels, JM (reprint author), Tech Univ Carolo Wilhelmina Braunschweig, Inst Pharmazeut Biol, Mendelssohnstr 1, D-38106 Braunschweig, Germany. NR 28 TC 7 Z9 7 U1 0 U2 4 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0937-7409 J9 CHEMOECOLOGY JI Chemoecology PY 2003 VL 13 IS 1 BP 55 EP 62 PG 8 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 663PT UT WOS:000182014500007 ER PT J AU Fabbiano, G AF Fabbiano, G TI X-ray source populations in galaxies SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article; Proceedings Paper CT 5th International Workshop on Multifrequency Behaviour of High Energy Cosmic Sources CY MAY 26-31, 2003 CL Vulcano, ITALY SP INTA, MPE, IASF, USN Res Lab DE X-rays : sources; galaxies : X-rays ID HIGH-RESOLUTION IMAGER; MASS BLACK-HOLES; CHANDRA OBSERVATIONS; POINT SOURCES; BINARIES; ANTENNAE; M81; NGC-4038/4039; DISCOVERY; HISTORY AB This paper gives a short review of recent studies of the X-ray source populations of nearby galaxies. A more complete review of this subject can be found in Fabbiano & White (2003), from where this talk was partially extracted. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gfabbiano@cfa.harvard.edu NR 53 TC 1 Z9 1 U1 0 U2 0 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1009-9271 J9 CHINESE J ASTRON AST JI Chin. J. Astron. Astrophys. PY 2003 VL 3 SU S BP 193 EP 201 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 929VK UT WOS:000229374500021 ER PT S AU Drake, JJ AF Drake, JJ BE Harra, LK TI Chemical fractionation and abundances in coronal plasma SO CONNECTIONS AND RECONNECTIONS IN SOLAR AND STELLAR CORONAE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT E0 1 Symposium of COSPAR Scientific Commission E on Connections and Reconnections in Solar and Stellar Coronae held at the 34th COSPAR Scientific Assembly CY OCT 11, 2002 CL HOUSTON, TX SP ESA, CNES, ISAS ID X-RAY SPECTROSCOPY; IONIZATION-DIFFUSION PROCESSES; SOLAR CHROMOSPHERE; ELEMENT FRACTIONATION; II-PEGASI; TRANSITION REGION; ATMOSPHERE; EMISSION; BEPPOSAX; FLARES AB Much of modern astrophysics is grounded on the observed chemical compositions of stars and the diffuse plasma that pervades the space between stars, galaxies and clusters of galaxies. X-ray and EUV spectra of the hot plasma in the outer atmospheres of stars have demonstrated that these environments are subject to chemical fractionation in which the abundances of elements can be enhanced and depleted by an order of magnitude or more. These coronal abundance anomalies are discussed and some of the physical mechanisms that might be responsible for producing them are examined. It is argued that coronal abundances can provide important new diagnostics on physical processes at work in solar and stellar coronae. It seems likely that other hot astrophysical plasmas will be subject to similar effects. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Smithsonian Astrophys Observ, Mail Stop 3,60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu NR 33 TC 21 Z9 21 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2003 VL 32 IS 6 BP 945 EP 954 DI 10.1016/S0273-1177(03)00296-5 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BX89P UT WOS:000186758600007 ER PT J AU Lance, SL Maldonado, JE Bocetti, CI Pattee, OH Ballou, JD Fleischer, RC AF Lance, SL Maldonado, JE Bocetti, CI Pattee, OH Ballou, JD Fleischer, RC TI Genetic variation in natural and translocated populations of the endangered Delmarva fox squirrel (Sciurus niger cinereus) SO CONSERVATION GENETICS LA English DT Article DE endangered; microsatellite; mtDNA; squirrel; Sciurus ID TREE AB The Delmarva fox squirrel, Sciurus niger cinereus, is a federally listed endangered subspecies whose range has been reduced by 90%. In an attempt to increase both population size and range, translocation sites were established beginning in the 1960's by moving squirrels from the natural range to sites outside the current range. Although translocations have served as the primary component of the DFS recovery program, there has been very little post-release examination of the genetics of the translocation sites. In this study, we developed ten microsatellite loci, screened the three polymorphic loci, and sequenced a 330 bp fragment of the mitochondrial control region in order to assess levels of genetic variation in natural and translocated regions of Delmarva fox squirrels and to compare them to Southeastern fox squirrels (S. n. niger). Although we found low levels of microsatellite polymorphism, there were no differences in heterozygosity between natural and translocated regions, or between Delmarva and Southeastern fox squirrels. We found high levels of polymorphism in the mitochondrial control region. Our patterns of haplotype diversity suggest incomplete lineage sorting of the two subspecies. In general, our data suggest that the current levels of genetic variation in the translocated sites are representative of those found in the natural population, and we encourage the continued use of translocations as a major component of Delmarva fox squirrel recovery. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Colby Coll, Dept Biol, Waterville, ME 04901 USA. Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. USGS Patuxent Wildlife Res Ctr, California, PA USA. USGS Patuxent Wildlife Res Ctr, Laurel, MD USA. RP Lance, SL (reprint author), Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RI Lance, Stacey/K-9203-2013 OI Lance, Stacey/0000-0003-2686-1733 NR 38 TC 14 Z9 15 U1 2 U2 9 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PY 2003 VL 4 IS 6 BP 707 EP 718 DI 10.1023/B:COGE.0000006112.18846.9f PG 12 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 748ZW UT WOS:000186895000005 ER PT B AU van Ballegooijen, AA Hasan, SS AF van Ballegooijen, AA Hasan, SS BE Pevtsov, AA Uitenbroek, H TI Physics of photospheric magnetic field SO CURRENT THEORETICAL MODELS AND HIGH RESOLUTION SOLAR OBSERVATIONS: PREPARING FOR ATST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 21st Workshop on Current Theoretical Models and High Resolution Solar Observations CY MAR 11-15, 2002 CL NATL SOLAR OBSERVAT, SACRAMENTO PEAK, NM SP USAF Off Sci Res, USAF Res Lab, NASA, Natl Sci Fdn, Natl Solar Observat HO NATL SOLAR OBSERVAT ID THIN FLUX TUBES; QUIET SUN; DYNAMICS; ELEMENTS; NETWORK; CANCELLATION; OSCILLATIONS; SIMULATIONS; INSTABILITY; EXCITATION AB The magnetic field on the quiet sun is continually swept into the intergranular lanes where it is amplified by interactions with the surrounding cool downflows. The resulting kilogauss flux tubes have typical sizes of about 100 km and magnetic field strengths of around 1500 G in the photosphere. A model of the magnetic field strength as function of depth is presented. It is shown that the Reynolds stress due to the downflows are sufficient to explain the observed kilogauss field strengths. We also present simulations of vorticity in intergranular lanes and the dynamics of flux tubes in response to such vortical motions. The simulations predict that flux tubes rotate with angular velocity similar to 5 x 10(-3) rad/s. If true, this would likely result in a significant flux of Alfven waves into the solar atmosphere that would contribute to the heating of the chromosphere and corona. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA. NR 48 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-129-X J9 ASTR SOC P PY 2003 VL 286 BP 155 EP 168 PG 14 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BW47Z UT WOS:000182119600016 ER PT B AU Kalkofen, W AF Kalkofen, W BE Pevtsov, AA Uitenbroek, H TI Wave propagation in the nonmagnetic chromosphere SO CURRENT THEORETICAL MODELS AND HIGH RESOLUTION SOLAR OBSERVATIONS: PREPARING FOR ATST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 21st Workshop on Current Theoretical Models and High Resolution Solar Observations CY MAR 11-15, 2002 CL NATL SOLAR OBSERVAT, SACRAMENTO PEAK, NM SP USAF Off Sci Res, USAF Res Lab, NASA, Natl Sci Fdn, Natl Solar Observat HO NATL SOLAR OBSERVAT ID SOLAR CHROMOSPHERE; OSCILLATIONS; GRAINS; ATMOSPHERE; EXCITATION; DYNAMICS AB The paper investigates the geometrical properties of the propagation of acoustic waves in three-minute chromospheric oscillations. It finds that the excess intensity of H-2v bright points in the dynamical simulations of Carlsson and Stein is a consequence of the assumption that the waves propagate as plane waves emanating from plane sources whereas the observed increase with height of the area disturbed by the oscillations implies that they propagate as spherical waves emanating from "point" sources. The "cones" in which the waves travel upward appear to be anchored in intergranular lanes; their opening angle is about 90degrees; their walls are not sharply defined. The filling factor of the 10 - 20 such propagation cones in a supergranulation cell interior is of the order of 10(-3). in the photosphere, reaching 50% at the top of the chromosphere. The contribution of bright-point oscillations to chromospheric heating at the locations of bright points is small, and to the energy budget of the internetwork chromosphere, it is negligible. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kalkofen, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 25 TC 7 Z9 7 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-129-X J9 ASTR SOC P PY 2003 VL 286 BP 385 EP 392 PG 8 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BW47Z UT WOS:000182119600040 ER PT B AU Avrett, EH AF Avrett, EH BE Pevtsov, AA Uitenbroek, H TI The solar temperature minimum and chromosphere SO CURRENT THEORETICAL MODELS AND HIGH RESOLUTION SOLAR OBSERVATIONS: PREPARING FOR ATST SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 21st Workshop on Current Theoretical Models and High Resolution Solar Observations CY MAR 11-15, 2002 CL NATL SOLAR OBSERVAT, SACRAMENTO PEAK, NM SP USAF Off Sci Res, USAF Res Lab, NASA, Natl Sci Fdn, Natl Solar Observat HO NATL SOLAR OBSERVAT ID CO; ATMOSPHERE; LINES AB Wave motions cause the brightness temperature in the centers of strong infrared CO lines to increase and decrease by about 200 K. The. CO number density quickly decreases as T increases, but is slow to increase again as T decreases. This causes the strong CO lines to be formed in the temperature minimum region rather than at chromospheric heights. Thus there can be a chromospheric rise in temperature, accounting for UV emission lines and for other diagnostics of the temperature minimum and chromosphere, without producing emission in the CO line cores, which is not observed. We are able to reconcile minimum temperatures as low as 3800 K inferred from CO observations with the higher minimum brightness temperatures observed in the continuum near 150 pm, in the continuum near 160 nm, and in the wings of the Ca II resonance lines. The time-dependent modeling of Carlsson and Stein has been proposed as a possible resolution of these conflicting temperature determinations. We suggest that the CO observations can be reconciled with other temperature-minimum and chromospheric diagnostics by assuming temperature fluctuations no larger than the fluctuations of observed brightness temperature, i.e., fluctuations much smaller than those produced by shock waves in the Carlsson and Stein simulations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM avrett@cfa.harvard.edu NR 22 TC 10 Z9 10 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-129-X J9 ASTR SOC P PY 2003 VL 286 BP 419 EP 429 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BW47Z UT WOS:000182119600044 ER PT B AU Kalkofen, W AF Kalkofen, W BE Pevtsov, AA Uitenbroek, H TI The temperature structure of the chromosphere SO CURRENT THEORETICAL MODELS AND HIGH RESOLUTION SOLAR OBSERVATIONS: PREPARING FOR ATST SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 21st Workshop on Current Theoretical Models and High Resolution Solar Observations CY MAR 11-15, 2002 CL NATL SOLAR OBSERVAT, SACRAMENTO PEAK, NM SP USAF Off Sci Res, USAF Res Lab, NASA, Natl Sci Fdn, Natl Solar Observat HO NATL SOLAR OBSERVAT ID SOLAR CHROMOSPHERE; ATMOSPHERE; MODELS; PROPAGATION; ENERGY; WAVES; SUN AB All models of the quiet solar chromosphere are limited in the range of phenomena they are capable of describing. The static, empirical models encompass most of the temporal variation of the temperature but not the extremes, and the wave-driven models describe either only the heating or only the dynamics of the chromosphere. The limitations of the wave models most likely are due to the properties of the acoustic-wave velocity spectra used as input to the simulations. The wave model of the heating obtains its velocity spectrum from the Lighthill mechanism, which is, mainly a quadrupole source and therefore has very low power at the acoustic cutoff frequency; most power is at the higher frequencies that are important for heating. The wave model of the dynamics uses an empirical spectrum that has most of its power near the acoustic cutoff frequency, which is critical for the three-minute chromospheric oscillations; but power is lacking at the frequencies that are important for heating. This velocity spectrum appears to be that of a monopole source, a conclusion that is consistent with the small size of the sources of the waves and their presumed location in intergranular lanes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wolf@cfa.harvard.edu NR 23 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-129-X J9 ASTR SOC P PY 2003 VL 286 BP 443 EP 450 PG 8 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BW47Z UT WOS:000182119600046 ER PT B AU Kochanek, CS AF Kochanek, CS BE Livio, M TI Dynamical probes of the halo mass function SO DARK UNIVERSE: MATTER, ENERGY AND GRAVITY SE SPACE TELESCOPE SCIENCE INSTITUTE SYMPOSIUM SERIES LA English DT Proceedings Paper CT Symposium on Dark Universe CY APR 02-05, 2001 CL Baltimore, MD SP Space Telescope Sci Inst ID COLD DARK-MATTER; GALAXY LUMINOSITY FUNCTION; GRAVITATIONAL LENSING STATISTICS; SEPARATION LENSED QUASARS; X-RAY-CLUSTERS; HIERARCHICAL-MODELS; COSMOLOGICAL MODELS; ROTATION CURVES; CONSTRAINTS; EVOLUTION AB We explore the relationship between the mass function of CDM halos and dynamical probes of the mass function such as the distribution of gravitational lens separations and the local velocity function. The compression of galactic halos by the cooling baryons, a standard component of modern models, leads to a feature in the distribution of lens separations near Deltatheta = 3."0 or in the velocity function near v(c) similar or equal to 400 km s(-1). The two probes of the, mass function, lens separations and the local velocity function, are mutually consistent. Producing the observed velocity function of galaxies or the separation distribution using standard adiabatic compression models requires more cold baryons, an equivalent cosmological density of Omega(b,cool) similar or equal to 0.02 compared to a total cosmological Omega(b) similar or equal to 0.04. than are observed in standard accountings of the baryonic content of galaxies, Omega(b,gal) similar or equal to 0.006, or our Galaxy, Omega(b,Gal) less than or similar to 0.015. The requirement for a higher cold baryon density than is usually assigned to galaxies appears to be generic to models which use the standard adiabatic compression models for the transformation of the CDM halo by the cooling baryons. If real, this dynamical baryon discrepancy suggests either that we are neglecting half of the cold baryonic mass in standard galactic models (e.g. a MACHO. cold molecular or warm gas component), Or that there is a problem with standard adiabatic compression models. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St,MS-51, Cambridge, MA 02138 USA. NR 73 TC 2 Z9 2 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA BN 0-521-82227-0 J9 SPACE TEL S PY 2003 VL 15 BP 139 EP 161 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAG25 UT WOS:000222060000011 ER PT J AU Blackledge, TA Coddington, JA Gillespie, RG AF Blackledge, TA Coddington, JA Gillespie, RG TI Are three-dimensional spider webs defensive adaptations? SO ECOLOGY LETTERS LA English DT Article DE adaptive radiation; Araneidae; key innovation; Linyphiidae; orb web; sheet web; silk; Sphecidae; Theridiidae ID MUD-DAUBER WASPS; ADAPTIVE RADIATION; BUILDING SPIDERS; WEAVING SPIDERS; PREDATION; ARANEAE; FOREST; ORBICULARIAE; HYMENOPTERA; POPULATION AB Spider webs result from complex behaviours that have evolved under many selective pressures. Webs have been primarily considered to be foraging adaptations, neglecting the potential role of predation risk in the evolution of web architecture. The ecological success of spiders has been attributed to key innovations in how spiders use silk to capture prey, especially the invention of chemically adhesive aerial two-dimensional orb webs. However, araneoid sheet web weavers transformed the orb architecture into three-dimensional webs and are the dominant group of aerial web-building spiders world-wide, both in numbers and described species diversity. We argue that mud-dauber wasps are major predators of orbicularian spiders, and exert a directional selective pressure to construct three-dimensional webs such that three-dimensional webs are partly defensive innovations. Furthermore, patterns of diversification suggest that escape from wasp predators may have facilitated diversification of three-dimensional web-building spiders. C1 Univ Calif Berkeley, Div Insect Biol, Berkeley, CA 94720 USA. Smithsonian Inst, Natl Museum Nat Hist NHB 105, Washington, DC 20560 USA. RP Blackledge, TA (reprint author), Cornell Univ, Dept Entomol, Comstock Hall, Ithaca, NY 14853 USA. NR 33 TC 67 Z9 72 U1 1 U2 20 PU BLACKWELL PUBLISHING LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD JAN PY 2003 VL 6 IS 1 BP 13 EP 18 DI 10.1046/j.1461-0248.2003.00384.x PG 6 WC Ecology SC Environmental Sciences & Ecology GA 625EZ UT WOS:000179805100004 ER PT S AU Yoshida, N AF Yoshida, N BE Holt, SS Reynolds, CS TI Cosmological simulations of the formation of primordial gas clouds SO EMERGENCE OF COSMIC STRUCTURE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 13th Annual Astrophysics Conference CY OCT 07-09, 2002 CL COLLEGE PK, MD SP NASA, Goddard Space Flight Ctr, Univ Maryland AB We study the formation of primordial star-forming clouds in a ACDM universe using large N-body/SPH simulations. The simulations include non-equilibrium 9 species (e(-), H, H+, He, He+, He++, H-2, H+, H-) chemistry and hydrogen molecular cooling. We determine that the critical 2 halo mass to form primordial star-forming clouds is 5 x 10(5)h(-1)M(circle dot), with a weak dependence on redshift in a range z > 16. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoshida, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0128-4 J9 AIP CONF PROC PY 2003 VL 666 BP 147 EP 150 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW85R UT WOS:000183411200018 ER PT B AU Crocker, WH AF Crocker, William H. BE Ember, CR Ember, M TI Canela SO ENCYCLOPEDIA OF SEX AND GENDER LA English DT Article; Book Chapter C1 Smithsonian Inst, Washington, DC 20013 USA. RP Crocker, WH (reprint author), Smithsonian Inst, Washington, DC 20013 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-0-387-29907-5 PY 2003 BP 345 EP 355 DI 10.1007/0-387-29907-6_34 D2 10.1007/0-387-29907-6 PG 11 WC Anthropology; Social Sciences, Interdisciplinary SC Anthropology; Social Sciences - Other Topics GA BKM73 UT WOS:000268562400036 ER PT J AU Froeschner, RC AF Froeschner, RC TI Review of the middle American lace bug genus macrotingis (Heteroptera : tingidae), with a key and a new species from Mexico SO ENTOMOLOGICAL NEWS LA English DT Article DE Macrotingis; heteroptera; tingidae; middle America; Mexico AB The genus Macrotingis was described by Champion (1897:22) for two species. Later Drake added another species and a "variety" for one of Champion's species; that variety is herein elevated to full species status. The range of Macrotingis, previously known from Guatemala south into Panama, is extended a short distance northward into southern Mexico with the present description of the new species M. schaffneri. A key separates the five included taxa. C1 US Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Froeschner, RC (reprint author), Care Of Henry TJ, USDA ARS, Natl Museum Nat Hist, Systemat Entomol Lab,Smithsonian Inst, POB 37012,MRC-0168, Washington, DC 20013 USA. EM thenry@sel.barc.usda.gov NR 4 TC 2 Z9 2 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0013-872X J9 ENTOMOL NEWS JI Entomol. News PD JAN-FEB PY 2003 VL 114 IS 1 BP 29 EP 32 PG 4 WC Entomology SC Entomology GA 810JN UT WOS:000220700700007 ER PT J AU Hale, SS Miglarese, AH Bradley, MP Belton, TJ Cooper, LD Frame, MT Friel, CA Harwell, LM King, RE Michener, WK Nicolson, DT Peterjohn, BG AF Hale, SS Miglarese, AH Bradley, MP Belton, TJ Cooper, LD Frame, MT Friel, CA Harwell, LM King, RE Michener, WK Nicolson, DT Peterjohn, BG TI Managing troubled data: Coastal data partnerships smooth data integration SO ENVIRONMENTAL MONITORING AND ASSESSMENT LA English DT Article; Proceedings Paper CT Symposium on Coastal Monitoring Through Parterships CY 2001 CL WASHINGTON, D.C. SP US EPA, Off Res & Dev EMAP DE coastal monitoring; coastal databases; information management; data partnerships; data integration ID ECOLOGICAL RESEARCH; INFORMATION; NETWORK; PROGRAM; SYSTEM AB Understanding the ecology, condition, and changes of coastal areas requires data from many sources. Broad-scale and long-term ecological questions, such as global climate change, biodiversity, and cumulative impacts of human activities, must be addressed with databases that integrate data from several different research and monitoring programs. Various barriers, including widely differing data formats, codes, directories, systems, and metadata used by individual programs, make such integration troublesome. Coastal data partnerships, by helping overcome technical, social, and organizational barriers, can lead to a better understanding of environmental issues, and may enable better management decisions. Characteristics of successful data partnerships include a common need for shared data, strong collaborative leadership, committed partners willing to invest in the partnership, and clear agreements on data standards and data policy. Emerging data and metadata standards that become widely accepted are crucial. New information technology is making it easier to exchange and integrate data. Data partnerships allow us to create broader databases than would be possible for any one organization to create by itself. C1 US EPA, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Atlantic Ecol Div, Narragansett, RI 02882 USA. NOAA, Coastal Serv Ctr, Charleston, SC USA. US EPA, Mid Atlantic Integrated Assessment, Ft George G Meade, MD USA. NJ Dept Environm Protect, Trenton, NJ USA. So Calif Coastal Water Res Project, Westminster, CA USA. US Geol Survey, Reston, VA 22092 USA. Florida Marine Res Inst, St Petersburg, FL 33701 USA. US EPA, Gulf Breeze, FL USA. US EPA, Washington, DC 20460 USA. Univ New Mexico, Albuquerque, NM 87131 USA. Smithsonian Inst, Washington, DC 20560 USA. US Geol Survey, Laurel, MD USA. RP Hale, SS (reprint author), US EPA, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Atlantic Ecol Div, Narragansett, RI 02882 USA. NR 47 TC 7 Z9 7 U1 1 U2 6 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-6369 J9 ENVIRON MONIT ASSESS JI Environ. Monit. Assess. PD JAN-FEB PY 2003 VL 81 IS 1-3 BP 133 EP 148 DI 10.1023/A:1021372923589 PG 16 WC Environmental Sciences SC Environmental Sciences & Ecology GA 620XY UT WOS:000179560300014 PM 12620011 ER PT J AU Gopalan, A Bommels, J Gotte, S Landwehr, A Franz, K Ruf, MW Hotop, H Bartschat, K AF Gopalan, A Bommels, J Gotte, S Landwehr, A Franz, K Ruf, MW Hotop, H Bartschat, K TI A novel electron scattering apparatus combining a laser photoelectron source and a triply differentially pumped supersonic beam target: characterization and results for the He- (1s 2s(2)) resonance SO EUROPEAN PHYSICAL JOURNAL D LA English DT Article ID HIGH-RESOLUTION; CROSS-SECTIONS; FESHBACH RESONANCES; VIBRATIONAL-EXCITATION; ATOM SCATTERING; SLOW-ELECTRONS; RARE-GASES; ATTACHMENT; IMPACT; THRESHOLD AB A novel electron scattering apparatus for high resolution studies of angle-differential elastic and inelastic electron scattering from atoms and molecules in the gas phase is described and its performance characterized. It combines a laser photoelectron source, a triply differentially pumped collimated supersonic beam target (half angle 0.015 rad, background to beam density ratio < 0.01), and several electron multipliers for simultaneous detection of elastically scattered electrons and metastable atoms (or molecules) due to inelastic scattering. In detailed test measurements of the yield for the production of metastable He* (2(3)S(1)) atoms around its threshold, the dependence of the overall energy width on various experimental parameters has been investigated. So far a resolution down to 7 meV (FWHM) has been obtained. Under such conditions we have investigated the profile of the He-(1s 2s(2 2)S(1/2)) resonance at the scattering angles 22degrees, 45degrees, and 90degrees. From a consistent fit of the measured profiles by resonant scattering theory we determine a new value for the resonance energy (E-tau = 19.365(1) eV) and an accurate resonance width (Gamma = 11.2(5) meV). These results are consistent with the previously recommended values. C1 Univ Kaiserslautern, Fachbereich Phys, D-67653 Kaiserslautern, Germany. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Gopalan, A (reprint author), Univ Kaiserslautern, Fachbereich Phys, Postfach 3049, D-67653 Kaiserslautern, Germany. RI Bartschat, Klaus/I-2527-2012 NR 95 TC 42 Z9 42 U1 1 U2 1 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 1434-6060 J9 EUR PHYS J D JI Eur. Phys. J. D PD JAN PY 2003 VL 22 IS 1 BP 17 EP 29 DI 10.1140/epjd/e2002-00219-7 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 643EY UT WOS:000180850000003 ER PT B AU Barmby, P AF Barmby, P BE KisslerPatig, M TI Globular cluster systems of spirals SO EXTRA-GALACTIC GLOBULAR CLUSTER SYSTEMS SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT Workshop on Extragalactic Globular Cluster Systems CY AUG 27-30, 2002 CL GARCHING, GERMANY SP European SO Observ ID COLOR-MAGNITUDE DIAGRAMS; SPACE-TELESCOPE ARCHIVE; COMPACT STAR-CLUSTERS; LOCAL GROUP; SOMBRERO GALAXY; M31; M81; KINEMATICS; SPECTROSCOPY; CANDIDATES AB Recent observational results on the globular cluster systems of spiral galaxies are summarized. Although the number of spirals with well-studied GCSs is still small, new studies promise to increase it rapidly in the next few years. New telescopes and technology have contributed to increasingly detailed studies of GCs in Local Group galaxies like M31 and M33, and more distant spirals like M81 and M104 are finally getting the attention they deserve. The Milky Way GCS looks to be reasonably typical of spirals, and still has a lot to tell us about the history of the galaxy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barmby, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS65, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 55 TC 8 Z9 8 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-40472-4 J9 ESO ASTROPHY SYMP PY 2003 BP 143 EP 154 DI 10.1007/10857603_24 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX54C UT WOS:000185641000024 ER PT J AU Reid, RP James, NP Macintyre, IG Dupraz, CP Burne, RV AF Reid, RP James, NP Macintyre, IG Dupraz, CP Burne, RV TI Shark Bay stromatolites: Microfabrics and reinterpretation of origins SO FACIES LA English DT Article DE stromatolites; marine; microbial; precipitation; micrite; Entophysalis; Shark Bay (Australia) ID MODERN MARINE STROMATOLITES; LITHIFIED MICRITIC LAMINAE; WESTERN-AUSTRALIA; ALGAL MATS; HOLOCENE; BAHAMAS AB Detailed analysis of microfabrics in Hamelin Pool stromatolites leads to reinterpretation of the origins of these structures. Previous studies have concluded that Shark Bay stromatolites form primarily as a result of sediment trapping and binding by microorganisms. Our results suggest that microbial precipitation of microcrystalline carbonate (micrite), as both framework and cement in these stromatolites, is also a fundamental, heretofore unrecognized, process in their formation. Microbial trapping and binding is the primary mechanism of stromatolite accretion in the intertidal zone, forming grainy, calcarenite structures. Microbial precipitation is the primary accretionary mechanism in the subtidal zone, forming muddy, micritic stromatolites. Microbial precipitation also lithifies trapped and bound sediment in the calcarenite stromatolites. Recognition of microbially precipitated micrite in Shark Bay stromatolites is important, as many ancient stromatolites are micritic. C1 Miami Univ, Miami, FL 33149 USA. Queens Univ, Dept Geol Sci, Kingston, ON K7L 3N6, Canada. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. Univ Neuchatel, CH-2007 Neuchatel, Switzerland. Australian Natl Univ, Dept Geol, Canberra, ACT 0200, Australia. RP Reid, RP (reprint author), Miami Univ, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. RI Burne, , Burne, Robert V.,/B-7007-2014 OI Burne, , Burne, Robert V.,/0000-0003-0689-4298 NR 42 TC 41 Z9 43 U1 2 U2 23 PU INSTITUT PALAONTOLOGIE UNIVERSITAT ERLANGEN-NURNBERG PI ERLANGEN PA LOEWENICHSTRABE 20, D-91054 ERLANGEN, GERMANY SN 0172-9179 J9 FACIES JI Facies PY 2003 VL 49 BP 299 EP 324 PG 26 WC Geology; Paleontology SC Geology; Paleontology GA 758CR UT WOS:000187615400016 ER PT J AU Zotz, G Schultz, S Rottenberger, S AF Zotz, G Schultz, S Rottenberger, S TI Are tropical lowlands a marginal habitat for macrolichens? Evidence from a field study with Parmotrema endosulphureum in Panama SO FLORA LA English DT Article DE Barro Colorado Island; dark respiration; lichens; photosynthesis; tropical forests; water content ID WATER RELATIONS; CO2 EXCHANGE; CARBON GAIN; RAIN-FOREST; LICHENS; PHOTOSYNTHESIS AB There is a striking increase in the abundance of non-vascular organisms (mosses, liverworts, and macrolichens) with altitude in the tropics. The proposed mechanism behind this altitudinal gradient still awaits experimental verification. This study addresses this question using diel (= 24-h) time courses of CO2 exchange, thallus water relations, and microclimate of the foliose lichen, Parmotrema endosulphureum, under natural tropical lowland conditions. In addition, we studied the responses of lichen gas exchange to experimental manipulations of incident light, temperature and thallus water content. Similar to the results of the only other field study on CO2 exchange in lowland lichens, 24-h carbon gain was strongly limited by nocturnal CO2 loss: the cumulative dark respiration reached almost 90% of diurnal carbon gain. Our estimates of long-term carbon gain are consistent with direct measurements of growth, and are substantially lower than those for lichens from montane sites in the tropics. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. Univ Wurzburg, Julius von Sachs Inst Biowissesch, Lehrstuhl Bot 2, D-97070 Wurzburg, Germany. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. NR 23 TC 16 Z9 20 U1 0 U2 8 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0367-2530 J9 FLORA JI Flora PY 2003 VL 198 IS 1 BP 71 EP 77 DI 10.1078/0367-2530-00077 PG 7 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 648RT UT WOS:000181164900006 ER PT J AU Zotz, G Vollrath, B Schmidt, G AF Zotz, G Vollrath, B Schmidt, G TI Carbon relations of fruits of epiphytic orchids SO FLORA LA English DT Article DE Crassulacean acid metabolism; gas exchange; Orchidaceae; photosynthesis; reproduction; respiration; vascular epiphytes ID CRASSULACEAN ACID METABOLISM; VASCULAR EPIPHYTES; DIMERANDRA-EMARGINATA; REPRODUCTIVE EFFORT; DARK RESPIRATION; PHOTOSYNTHESIS; FLOWERS; ORIGIN; LIGHT AB While net CO2 exchange (NP) of leaves has been studied extensively in vascular epiphytes, there is little information on NP of reproductive structures. Since such information is important to evaluate the magnitude of investment in reproduction, we conducted a study with fruits of nine species of epiphytic orchids on Barro Colorado Island, Panama. Irrespective of the photosynthetic pathway of the leaves, fruits invariably showed some CAM activity as indicated by a significant nocturnal increase in titratable acidity. Photosynthetic capacity as determined in an oxygen electrode with dissected capsules was surprisingly high in some species, always showing positive net assimilation at higher PFD (photon flux density). Conversely, in situ CO2 exchange on intact fruits, which was studied in the two species Dimerandra emarginata and Caularthron bilamellatum, never yielded positive values. We estimate that internal recycling of respiratory CO2 reduces carbon losses in mature fruit by about 60% in Dimerandra emarginata, but only by 10% in Caularthron bilamellatum. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. Univ Wurzburg, Lehrstuhl Bot 2, D-8700 Wurzburg, Germany. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. NR 31 TC 5 Z9 5 U1 1 U2 7 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0367-2530 J9 FLORA JI Flora PY 2003 VL 198 IS 2 BP 98 EP 105 DI 10.1078/0367-2530-00081 PG 8 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 668XW UT WOS:000182322400002 ER PT J AU Krause, GH Galle, A Gademann, R Winter, K AF Krause, GH Galle, A Gademann, R Winter, K TI Capacity of protection against ultraviolet radiation in sun and shade leaves of tropical forest plants SO FUNCTIONAL PLANT BIOLOGY LA English DT Article DE carotenoids; chlorophyll a and b; epidermal UV shielding; UV-A PAM system; UV-absorbing compounds ID XANTHOPHYLL-CYCLE ACTIVITY; LEAF EPIDERMAL TRANSMITTANCE; CHLOROPHYLL FLUORESCENCE; UV-RADIATION; IN-SITU; PHOTOSYSTEM-II; B RADIATION; PHOTOINHIBITION; PHOTOSYNTHESIS; FIELD AB Protection of leaves of tropical forest plants against UV-A and -B radiation was studied in three lowland forests, a montane cloud forest and a mangrove stand in Panama. Leaves were classified as sun or shade leaves according to their chlorophyll a/b ratio, pool size of xanthophyll cycle pigments and alpha- and beta-carotene contents. The capacity of the leaves for protection against UV radiation was assessed by estimating epidermal UV-A shielding, by a non-invasive fluorometric method, and by the absorbance of ethanolic/aqueous leaf extracts in the UV spectral region. In all sun leaves tested, UV-A shielding by the adaxial epidermis was high, usually above 90%, whereas in shade leaves the epidermal UV-A shielding was markedly lower and varied widely between species. In most cases UV-A shielding by the abaxial epidermis was lower than by the adaxial epidermis. UV absorbance of the leaf extracts was generally higher in sun than in shade leaves, and the absorbance was much higher in the UV-B spectral region at 305 nm than in the UV-A region at 375 nm. The data demonstrate that sun leaves of tropical plants are well protected against solar UV-A and UV-B radiation. However, UV-induced damage may occur when shade leaves become exposed to full solar radiation. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Dusseldorf, Inst Plant Biochem, D-40225 Dusseldorf, Germany. RP Krause, GH (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. NR 29 TC 41 Z9 45 U1 4 U2 17 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-4408 J9 FUNCT PLANT BIOL JI Funct. Plant Biol. PY 2003 VL 30 IS 5 BP 533 EP 542 DI 10.1071/FP03047 PG 10 WC Plant Sciences SC Plant Sciences GA 686UZ UT WOS:000183340500007 ER PT S AU Kewley, LJ Dopita, M AF Kewley, LJ Dopita, M BE AvilaReese, V Firmani, C Frenk, CS Allen, YC TI The AGN-starburst connection in infrared merging galaxies SO GALAXY EVOLUTION: THEORY AND OBSERVATIONS SE REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA, SERIE DE CONFERENCIAS LA English DT Proceedings Paper CT Symposium on Galaxy Evolution CY APR 08-12, 2002 CL COZUMEL, MEXICO SP Univ Nacl Auton Mexico, Inst Astron, Univ Nacl Auton Mexico, Coordinac Investigac Cientif, Univ Nacl Auton Mexico, Direcc Gen Asuntos Person Acad, Univ Nacl Auton Mexico, Direcc Gen Estudios Posgrado DE galaxies : interactions; galaxies : active; galaxies : starburst; galaxies : evolution AB I present new results in our study of the starburst-AGN connection in the central kpc of 230 infrared galaxies. We developed theoretical optical grids for determining the relative contribution of AGN vs. starburst emission in composite galaxies. The grids are based on stellar population synthesis, photoionization and shock models. We compared the contribution from an AGN with indicators of merger evolution for our sample. Our results support an evolutionary scenario in which starburst activity is initially triggered by tidal interactions. As gas is funnelled towards the merger nucleus, an AGN is activated. Towards later stages of the merger, circumnuclear starburst activity becomes the dominant excitation mechanism. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kewley, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 4 Z9 4 U1 0 U2 0 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 BN 970-32-0609-3 J9 REV MEX AST ASTR PY 2003 VL 17 BP 83 EP 84 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX81E UT WOS:000186501900033 ER PT S AU Perna, R Belczynski, K AF Perna, R Belczynski, K BE Ricker, GR Vanderspek, RK TI Observational properties of afterglows from mergers of compact objects SO GAMMA-RAY BURST AND AFTERGLOW ASTRONOMY 2001 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Workshop Celebrating the First Year of the HETE Mission CY NOV 05-09, 2001 CL WOODS HOLE, MA SP HETE Sci Team AB Data accumulated over the years have shown that the distribution of the GRB time duration is bimodal. While there is some evidence that long bursts are associated with star-forming regions, nothing is known regarding the class of short bursts. Their very short timescales are hard to explain with the collapse of a massive star, but would be naturally produced by the merger of two compact objects, such as two neutron stars (NS), or a neutron star and a black hole (BH). As for the case of long bursts, afterglow obervations for short bursts should help reveal their origin. By using the updated population synthesis code StarTrack ([1]), we simulate a cosmological population of merging NS-NS and NS-BH, and compute the distribution of their galactic off-sets, the density distribution of their environment, and, if indeed associated with GRBs, their expected afterglow characteristics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perna, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0122-5 J9 AIP CONF PROC PY 2003 VL 662 BP 417 EP 419 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BW74S UT WOS:000183012900101 ER PT J AU Stafford, MD Frison, GC Stanford, D Zeimans, G AF Stafford, MD Frison, GC Stanford, D Zeimans, G TI Digging for the color of life: Paleoindian red ochre mining at the Powars II site, Platte County, Wyoming, USA SO GEOARCHAEOLOGY-AN INTERNATIONAL JOURNAL LA English DT Article AB The Powars II site, 48PL330, located near Sunrise, Wyoming, is a significant Paleoindian site in the Hartville Uplift area of eastern Wyoming. Intensive red ochre mining took place at Powars II, as indicated by Paleoindian materials in direct association with a natural hematite deposit. Projectile points ranging in age from Clovis to Late Paleoindian have been recovered, as well as stone and bone tools, shell and bone beads, and several pieces of incised bone. It is argued that the Powars II assemblage reflects a two-part cultural manifestation: a technological component resulting from the process of raining and processing ochre, and an ideological component derived from emic beliefs about the ochre source itself. (C) 2003 Wiley Periodicals, Inc. C1 Cranbrook Inst Sci, Bloomfield Hills, MI 48303 USA. Univ Wyoming, Dept Anthropol, Laramie, WY 82071 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Stafford, MD (reprint author), Cranbrook Inst Sci, 39221 Woodward Ave, Bloomfield Hills, MI 48303 USA. NR 42 TC 19 Z9 20 U1 1 U2 4 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0883-6353 J9 GEOARCHAEOLOGY JI Geoarchaeology PD JAN PY 2003 VL 18 IS 1 BP 71 EP 90 DI 10.1002/gea.10051 PG 20 WC Archaeology; Geosciences, Multidisciplinary SC Archaeology; Geology GA 632BP UT WOS:000180203700004 ER PT J AU Dore, S Hymus, GJ Johnson, DP Hinkle, CR Valentini, R Drake, BG AF Dore, S Hymus, GJ Johnson, DP Hinkle, CR Valentini, R Drake, BG TI Cross validation of open-top chamber and eddy covariance measurements of ecosystem CO2 exchange in a Florida scrub-oak ecosystem SO GLOBAL CHANGE BIOLOGY LA English DT Article DE eddy covariance; net ecosystem exchange; open-top chambers; scrub-oak ecosystem ID ELEVATED ATMOSPHERIC CO2; CARBON-DIOXIDE EXCHANGE; WATER-VAPOR; NET CARBON; FLUX MEASUREMENTS; BEECH FOREST; RISING CO2; RESPIRATION; PHOTOSYNTHESIS; TEMPERATE AB Simultaneous measurements of net ecosystem CO2 exchange (NEE) were made in a Florida scrub-oak ecosystem in August 1997 and then every month between April 2000 to July 2001, using open top chambers (NEEO) and eddy covariance (NEEE). This study provided a cross validation of these two different techniques for measuring NEE. Unique characteristics of the comparison were that the measurements were made simultaneously, in the same stand, with large replicated chambers enclosing a representative portion of the ecosystem (75 m(2), compared to approximately 1-2 ha measured by the eddy covariance system). The value of the comparison was greatest at night, when the microclimate was minimally affected by the chambers. For six of the 12 measurement periods, night NEEO was not significantly different to night NEEE, and for the other periods the maximum difference was 1.1 mumol m(-2)s(-1), with an average of 0.72 +/- 0.09 mumol m(-2)s(-1). The comparison was more difficult during the photoperiod, because of differences between the microclimate inside and outside the chambers. During the photoperiod, air temperature (T-air) and air vapour pressure deficits (VPD) became progressively higher inside the chambers until mid-afternoon. In the morning NEEO was higher than NEEE by about 26%, consistent with increased temperature inside the chambers. Over the mid-day period and the afternoon, NEEO was 8% higher that NEEE, regardless of the large differences in microclimate. This study demonstrates both the uses and difficulties associated with attempting to cross validate NEE measurements made in chambers and using eddy covariance. The exercise was most useful at night when the chamber had a minimal effect on microclimate, and when the measurement of NEE is most difficult. C1 Univ Tuscia, Dipartimento Forest Sci & Resources, I-01100 Viterbo, Italy. CNR, Kennedy Space Ctr, FL 32899 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Gen Dynam Corp, Kennedy Space Ctr, FL 32899 USA. RP Dore, S (reprint author), Univ Tuscia, Dipartimento Forest Sci & Resources, Via S Camillo De Lellis, I-01100 Viterbo, Italy. RI Valentini, Riccardo/D-1226-2010 OI Valentini, Riccardo/0000-0002-6756-5634 NR 43 TC 50 Z9 54 U1 0 U2 20 PU BLACKWELL PUBLISHING LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD JAN PY 2003 VL 9 IS 1 BP 84 EP 95 DI 10.1046/j.1365-2486.2003.00561.x PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 625EU UT WOS:000179804600007 ER PT J AU Li, JH Dugas, WA Hymus, GJ Johnson, DP Drake, BG Hungate, BA AF Li, JH Dugas, WA Hymus, GJ Johnson, DP Drake, BG Hungate, BA TI Direct and indirect effects of elevated CO2 on transpiration from Quercus myrtifolia in a scrub-oak ecosystem SO GLOBAL CHANGE BIOLOGY LA English DT Article DE carbon dioxide; LAI; open-top chamber; Quercus myrtifolia; sap flow; self-shading; stomatal conductance; transpiration ID CARBON-DIOXIDE ENRICHMENT; CANOPY TRANSPIRATION; STOMATAL CONDUCTANCE; GAS-EXCHANGE; PINE FOREST; STEM-FLOW; MASS-FLOW; WATER-USE; TREE; LEAF AB Elevated atmospheric carbon dioxide (C-a) usually reduces stomatal conductance, but the effects on plant transpiration in the field are not well understood. Using constant-power sap flow gauges, we measured transpiration from Quercus myrtifolia Willd., the dominant species of the Florida scrub-oak ecosystem, which had been exposed in situ to elevated C-a (350 mumol mol(-1) above ambient) in open-top chambers since May 1996. Elevated C-a reduced average transpiration per unit leaf area by 37%, 48% and 49% in March, May and October 2000, respectively. Temporarily reversing the C-a treatments showed that at least part of the reduction in transpiration was an immediate, reversible response to elevated C-a. However, there was also an apparent indirect effect of C-a on transpiration: when transpiration in all plants was measured under common C-a, transpiration in elevated C-a-grown plants was lower than that in plants grown in normal ambient C-a. Results from measurements of stomatal conductance (g(s)), leaf area index (LAI), canopy light interception and correlation between light and g(s) indicated that the direct, reversible C-a effect on transpiration was due to changes in g(s) caused by C-a, and the indirect effect was caused mainly by greater self-shading resulting from enhanced LAI, not from stomatal acclimation. By reducing light penetration through the canopy, the enhanced self-shading at elevated C-a decreased stomatal conductance and transpiration of leaves at the middle and bottom of canopy. This self-shading mechanism is likely to be important in ecosystems where LAI increases in response to elevated C-a. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Texas Agr Exptl Stn, Blackland Res Ctr, Temple, TX 76502 USA. Gen Dynam Corp, Kennedy Space Ctr, FL 32899 USA. No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. RP Li, JH (reprint author), Smithsonian CO2 Site,Mail Code DYN-2, Kennedy Space Ctr, FL 32899 USA. RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 45 TC 17 Z9 17 U1 0 U2 8 PU BLACKWELL PUBLISHING LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD JAN PY 2003 VL 9 IS 1 BP 96 EP 105 DI 10.1046/j.1365-2486.2003.00557.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 625EU UT WOS:000179804600008 ER PT B AU Worthington, WE AF Worthington, WE BE Brown, GO Garbrecht, JD Hagar, WH TI Hydraulic engineering history at the Smithsonian Institution SO HENRY P.G. DARCY AND OTHER PIONEERS IN HYDRAULICS: CONTRIBUTIONS IN CELEBRATION OF THE 200TH BIRTHDAY OF HENRY PHILIBERT GASPARD DARCY LA English DT Proceedings Paper CT Darcy Memorial Symposium on the History of Hydraulics CY JUN 24, 2003 CL PHILADELPHIA, PA SP Environment & Water Resources Inst, Surface Water Hydeol Comm, Hist & Heritage Comm AB Over the last 250 years American hydraulic engineering has taken many forms. Some techniques, practices, and inventions were adapted from abroad. Others reflected an innate creativity. These sources are explored by discussing artifacts from the collections of the National Museum of American History. The focus of the paper will be on less well known events and people who made that history. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC CIVIL ENGINEERS PI NEW YORK PA UNITED ENGINEERING CENTER, 345 E 47TH ST, NEW YORK, NY 10017-2398 USA BN 0-7844-0683-9 PY 2003 BP 252 EP 262 PG 11 WC Engineering, Civil; Engineering, Mechanical; History & Philosophy Of Science SC Engineering; History & Philosophy of Science GA BY28P UT WOS:000188784400018 ER PT S AU Karovska, M Fabbiano, G Elvis, M Nicastro, F Murray, SS Kraft, RP AF Karovska, M Fabbiano, G Elvis, M Nicastro, F Murray, SS Kraft, RP BE Li, XD Trimble, V Wang, ZR TI A Chandra view of the multi-scale structures in Centaurus A SO HIGH ENERGY PROCESSES AND PHENOMENA IN ASTROPHYSICS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 214th Symposium of the International-Astronomical-Union CY AUG 06-10, 2002 CL Suzhou, PEOPLES R CHINA SP Int Astronom Union AB Centaurus A (NGC 5128) is a giant early-type galaxy containing the nearest radio-bright AGN. The high-angular resolution Chandra images of Cen A reveal multi-scale X-ray structures with unprecedented detail and clarity. We present results from our study of X-ray structures surrounding the Cen A nuclear region, including the discovery of giant arc-like structures, extending to about 8 kpc in the direction perpendicular to the jet. We compare the X-ray structures with observations in other wavelengths and discuss their implication for a global understanding of the morphology of Cen A. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-157-5 J9 IAU SYMP PY 2003 IS 214 BP 289 EP 292 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BY65T UT WOS:000189431800048 ER PT J AU Hunter, RE AF Hunter, Robert E. BE Rollins, PC OConnor, JE TI WHO'S IN CHARGE HERE? Technology and the Presidency in Fail-Safe (1964) and Colossus (1970) SO HOLLYWOOD'S WHITE HOUSE: THE AMERICAN PRESIDENCY IN FILM AND HISTORY LA English DT Article; Book Chapter C1 [Hunter, Robert E.] Univ Illinois, Chicago, IL 60680 USA. [Hunter, Robert E.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Hunter, RE (reprint author), Univ Illinois, Chicago, IL 60680 USA. EM zpn1@earthlink.net NR 22 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS KENTUCKY PI LEXINGTON PA 102 LAFFERTY HALL, UNIVERSITY OF KENTUCKY, LEXINGTON, KY 40506 USA BN 978-0-8131-2792-7 PY 2003 BP 206 EP 222 PG 17 WC Film, Radio, Television SC Film, Radio & Television GA BAM45 UT WOS:000304681100015 ER PT B AU Dupree, AK AF Dupree, AK BE Sembach, KR Blades, JC Illingworth, GD Kennicutt, RC TI Cool stars and the future in space SO HUBBLE'S SCIENCE LEGACY: FUTURE OPTICAL/ULTRAVIOLET ASTRONOMY FROM SPACE SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Hubbles Science Legacy - Future Optical/Ultraviolet Astronomy from Space CY APR 02-05, 2002 CL UNIV CHICAGO, CHICAGO, IL SP AURA, NASA, ESA HO UNIV CHICAGO ID ALPHA-ORIONIS; AB-DORADUS; 47 TUCANAE; TELESCOPE; CHROMOSPHERE AB Recent results selected from ultraviolet spectroscopy and imaging of cool stars reveal challenging questions for future observations ranging from imaging of stellar surfaces and environments, to pursuit of faint objects populating the depths of globular cluster cores. Spectroscopy of fiducial Galactic stars and star clusters and study of abundances, atmospheric structures, winds and mass loss drive future opportunities in studies of stars and clusters. A 6-8 m class diffraction-limited ultraviolet telescope (perhaps with outriggers) will make discoveries and address fundamental problems associated with cool stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-136-2 J9 ASTR SOC P PY 2003 VL 291 BP 37 EP 44 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW77N UT WOS:000183133000007 ER PT B AU Hartmann, L AF Hartmann, L BE Sembach, KR Blades, JC Illingworth, GD Kennicutt, RC TI Problems in star and planet formation SO HUBBLE'S SCIENCE LEGACY: FUTURE OPTICAL/ULTRAVIOLET ASTRONOMY FROM SPACE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Hubbles Science Legacy - Future Optical/Ultraviolet Astronomy from Space CY APR 02-05, 2002 CL UNIV CHICAGO, CHICAGO, IL SP AURA, NASA, ESA HO UNIV CHICAGO ID T-TAURI STARS; ORION NEBULA; MOLECULAR-HYDROGEN; YOUNG STARS; DISKS; GAS; MIGRATION; ACCRETION; EMISSION; CLUSTER AB In this contribution I outline some important issues in star and planet formation which could be addressed by a space-based, optical-ultraviolet telescope of large aperture: determining the stellar initial mass function, detecting molecular hydrogen in disks and envelopes, measuring disk accretion and possibly detecting disk evaporation, and investigating details of disk structure. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-136-2 J9 ASTR SOC P PY 2003 VL 291 BP 61 EP 68 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW77N UT WOS:000183133000010 ER PT B AU Traub, WA AF Traub, WA BE Sembach, KR Blades, JC Illingworth, GD Kennicutt, RC TI Extrasolar planets and biomarkers SO HUBBLE'S SCIENCE LEGACY: FUTURE OPTICAL/ULTRAVIOLET ASTRONOMY FROM SPACE SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Hubbles Science Legacy - Future Optical/Ultraviolet Astronomy from Space CY APR 02-05, 2002 CL UNIV CHICAGO, CHICAGO, IL SP AURA, NASA, ESA HO UNIV CHICAGO ID TERRESTRIAL PLANETS AB The most important science to be done with a Hubble successor telescope could be the detection of extrasolar terrestrial planets and the search for life on those planets. A telescope which is optimized for terrestrial planet detection will also be a superb facility for ultraviolet-optical astrophysics, with a large collecting area, high angular resolution, and wide-band response. A coronagraphic Terrestrial Planet Finder (TPF) mission should be flown to explore the extrasolar planet frontier around nearby stars, much as Hubble was flown to explore the galactic frontier at the edge of the Universe. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Traub, WA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-136-2 J9 ASTR SOC P PY 2003 VL 291 BP 117 EP 124 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW77N UT WOS:000183133000017 ER PT B AU Adelberger, K AF Adelberger, K BE Sembach, KR Blades, JC Illingworth, GD Kennicutt, RC TI Measuring the influence of supernovae at high redshift SO HUBBLE'S SCIENCE LEGACY: FUTURE OPTICAL/ULTRAVIOLET ASTRONOMY FROM SPACE SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Hubbles Science Legacy - Future Optical/Ultraviolet Astronomy from Space CY APR 02-05, 2002 CL UNIV CHICAGO, CHICAGO, IL SP AURA, NASA, ESA HO UNIV CHICAGO ID GALAXY FORMATION; CLUSTERS AB Supernovae play a large but poorly understood role in our attempts to explain the evolution of the baryons in the Universe. Numerous observations throughout astronomy cannot be explained if we neglect their influence, yet our quantitative understanding of the ways in which supernovae affect the Universe remains remarkably poor. This is one of the most embarrassing gaps in our knowledge of the cosmos, and planned telescopes and surveys will probably not do much to fill it. The problem is that these surveys will be optimized to observe galaxies and intergalactic material independently of each other, while (in the author's view) by far the best information will come from simultaneous surveys of galaxies and the intergalactic material (IGM) in their vicinity. Only this will show directly how galaxies affect their surroundings and provide a rough energy scale for supernova-driven winds. Redshifts 1 less than or similar to z less than or similar to 3 are ideal for the joint galaxy/IGM surveys we advocate, because the comoving density of star formation is near its peak, because the Lyalpha forest is thin enough for QSO spectra to reveal the locations of the dominant metallic species, and because bright background QSOs are common. But a new ultraviolet (UV) spectrograph in space will be required. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Adelberger, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-136-2 J9 ASTR SOC P PY 2003 VL 291 BP 221 EP 228 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW77N UT WOS:000183133000030 ER PT B AU Kochanek, CS AF Kochanek, CS BE Sembach, KR Blades, JC Illingworth, GD Kennicutt, RC TI The whys and hows of finding 10,000 lenses SO HUBBLE'S SCIENCE LEGACY: FUTURE OPTICAL/ULTRAVIOLET ASTRONOMY FROM SPACE SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Hubbles Science Legacy - Future Optical/Ultraviolet Astronomy from Space CY APR 02-05, 2002 CL UNIV CHICAGO, CHICAGO, IL SP AURA, NASA, ESA HO UNIV CHICAGO ID GALAXIES; QUASARS; SEARCH; SUBSTRUCTURE; CONSTANT; HALOS; FIELD; SKY AB Very large samples of lenses are ideal for studying the relations between dark matter halos and astronomical objects and the evolution of these relations with cosmic epoch. Samples of 10(3) lenses are likely to be available in 10 years, but obtaining a sample of 10(4) lenses probably requires a wide-field, high resolution space telescope. C1 Smithsonian Astrophys Observ, Ctr Astrophys, Cambridge, MA 02138 USA. RP Kochanek, CS (reprint author), Smithsonian Astrophys Observ, Ctr Astrophys, MS-51,60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-136-2 J9 ASTR SOC P PY 2003 VL 291 BP 245 EP 252 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW77N UT WOS:000183133000033 ER PT J AU Jedicke, R Morbidelli, A Spahr, T Petit, JM Bottke, WF AF Jedicke, R Morbidelli, A Spahr, T Petit, JM Bottke, WF TI Earth and space-based NEO survey simulations: prospects for achieving the Spaceguard Goal SO ICARUS LA English DT Article DE asteroids ID ASTEROIDS; POPULATION AB We have used an improved model of the orbit and absolute magnitude distribution of Near Earth Objects (NEOs) to simulate the performance of asteroid surveys. Our results support general conclusions of previous studies using preliminary Near Earth Asteroid (NEA) orbit and magnitude distributions and suggest that meeting the Spaceguard Goal of 90% completion for Near Earth Objects (NEOs) greater than 1 km diameter by 2008 is impossible given contemporary surveying capabilities. The NEO model was derived from NEO detections by the Spacewatch Project. For this paper we developed a simulator for the Catalina Sky Survey (CSS) for which we had a complete pointing history and NEO detection efficiency. The good match between the output of the simulator and the actual CSS performance gives confidence that both the NEO model and simulator are correct. Then, in order to determine if existing surveys can meet the Spaceguard Goal, we developed a simulator to mimic the LINEAR survey, for which detailed performance characteristics were unavailable. This simulator serendipitously provided an estimate for the currently undiscovered population of NEOs upon which we base all our estimates of time to 90% completion. We also developed a set of idealized NEO surveys in order to constrain the best possible survey performance in contrast to more realistic systems. A 100% efficient, all-sky, every night survey, subject only to the constraints of detection above a specified air mass and when the Sun is 18degrees below the horizon provides a benchmark from which to examine the effect of imposing more restrictions and the efficacy of some simple survey strategies. Such a survey must have a limiting V-magnitude of 20.1 +/- 0.2 to meet the Spaceguard Goal. More realistic surveys, limited by latitude, the galaxy, minimum rates of NEO motion, etc., require fainter limiting magnitudes to reach the same completion. Our most realistic simulations, which have been normalized to the performance of the LINEAR detector system's operation in the period 1999-2000, indicate that it would take them another 33 +/- 5 years to reach 90% completeness for the larger asteroids ( 1 km diameter). They would need to immediately increase the limiting magnitude to about 24 in order to meet the Spaceguard Goal. The simulations suggest that there may be little need for distributing survey telescopes in longitude and latitude as long as there is sufficient sky coverage from a telescope or network of telescopes which may be geographically close. An idealized space-based survey, especially from a satellite orbit much interior to Earth, would offer an advantage over their terrestrial counterparts. We do not consider a cost-benefit analysis for any of the simulations but suspect that a local-area network of telescopes capable of covering much of the sky in a month to V similar to 21.5 may be administratively, financially, and scientifically the best compromise for reaching 90% completion of NEOs larger than I km diameter. (C) 2003 Elsevier Science (USA). All rights reserved. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Obs Cote Azur, F-06034 Nice 4, France. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. SW Res Inst, Boulder, CO 80302 USA. RP Jedicke, R (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. NR 27 TC 27 Z9 28 U1 3 U2 7 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 JAN PY 2003 VL 161 IS 1 BP 17 EP 33 AR PII S0019-1035(02)00026-X DI 10.1016/S0019-1035(02)00026-X PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 645NA UT WOS:000180983200002 ER PT B AU Nicastro, F AF Nicastro, F BE Rosenberg, JL Putman, ME TI On the intergalactic origin of the z similar to 0 absorber detected by Chandra and FUSE SO IGM/GALAXY CONNECTION: THE DISTRIBUTION OF BARYONS AT Z(EQUAL)0 SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Meeting on the IGM/Galaxy Connection - The Distribution of Baryons at z=0 CY 2002 CL NATL CTR ATMOSPHER RES, BOULDER, CO HO NATL CTR ATMOSPHER RES ID BARYONS; GAS AB In this contribution I present evidence that the HV-OVI absorbers detected by FUSE along the majority of the lines of sight track a Warm-Hot Intergalactic Medium filament in which our own Local Group is embedded. From combined Far-UV and X-ray data we conclude that this filament has a temperature of log T similar or equal to 5.8, baryon volume and column densities of n(b) = 4 - 6 x 10(-6) cm(-3) and N-b = 4.5 x 10(19)[O/H](0.3circle dot)(-1) cm(-2) respectively, and so a linear size of 2 - 4 [O/H](0.3circle dot)(-1) Mpc. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-83, Cambridge, MA 02138 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-1289-6 J9 ASTROPHYS SPACE SC L PY 2003 VL 281 BP 277 EP 282 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW93K UT WOS:000183698900050 ER PT S AU Bookbinder, J DeLuca, EE Cheimets, P Golub, L Hassler, D Korendyke, C Glenn, P Silver, E AF Bookbinder, J DeLuca, EE Cheimets, P Golub, L Hassler, D Korendyke, C Glenn, P Silver, E BE Keil, SL Avakyan, SV TI The reconnection and microscale (RAM) solar-terrestrial probe SO INNOVATIVE TELESCOPES AND INSTRUMENTATION FOR SOLAR ASTROPHYSICS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Innovative Telescopes and Instrumentation for Solar Astrophysics CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE sun; corona; reconnection; space mission; EUV spectroscopy; x-ray spectroscopy; EUV imaging; x-ray imaging; multilayers ID MAGNETIC RECONNECTION; EXPLOSIVE EVENTS; CORONA; TELESCOPE; SPECTROMETER; ABSORPTION; ATMOSPHERE; SURGES; REGION; SHEETS AB A hot, magnetized plasma such as the solar corona has the property that much of the physics governing its activity takes place on remarkably small spatial and temporal scales, while the response to this activity occurs on large scales. Observations from SMM, TRACE, SOHO and Yohkoh have shown that typical solar active regions have loops ranging in temperature from 0.5 to 10 MK, and flares up to 40MK. The spatial and temporal domains involved have been heretofore inaccessible to direct observations from Earth, so that theory has relied heavily on extrapolations from more accessible regimes, and on speculation. The RAM Solar-Terrestrial Probe consists of a set of carefully selected imaging and spectroscopic instruments that enable definitive studies of the dynamics and energetics of the solar corona. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bookbinder, J (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Golub, Leon/0000-0001-9638-3082 NR 36 TC 5 Z9 5 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4632-7 J9 P SOC PHOTO-OPT INS PY 2003 VL 4853 BP 436 EP 452 DI 10.1117/12.460300 PG 17 WC Instruments & Instrumentation; Optics; Spectroscopy SC Instruments & Instrumentation; Optics; Spectroscopy GA BW44P UT WOS:000182019000043 ER PT J AU Soucy, SL Giray, T Roubik, DW AF Soucy, SL Giray, T Roubik, DW TI Solitary and group nesting in the orchid bee Euglossa hyacinthina (Hymenoptera, Apidae) SO INSECTES SOCIAUX LA English DT Article DE nesting biology; social behaviour; social evolution; Euglossine bees ID SEX-RATIOS; ALLODAPINE BEE; COLONY STRUCTURE; SOCIAL-BEHAVIOR; HALICTINE BEE; EVOLUTION; EUSOCIALITY; ADVANTAGE; BOMBINAE; BIOLOGY AB Orchid bees (Euglossini) provide a potentially informative contrast for examining origins of advanced social behaviour in bees because they are the only tribe in the apine clade that do not form large colonies or have queens and workers. We investigated natural nests of Euglossa hyacinthina Dressier, an orchid bee that nests singly or in groups. By comparing the two types of nests, we examined if individuals in a group merely share the nest (are communal) or exhibit a level of social organization where there is reproductive division of labour among the females. Observations are consistent with communal nesting, indicating that all females in group nests are reproductively similar to the solitary nesting females because the provisioning of young, as well as the ovary development and mating status of females sharing nests were not different than that of solitary-nesting females. Also, multiple female nests did not produce a female-biased brood as predicted for nests with reproductive division of labour. We also investigated potential advantages of group nesting vs. individual nesting. We demonstrate that per capita offspring production is lower in nests with more than one female. However, we found that nests with single females were left unattended for longer periods of time during foraging, and that there was a high incidence of natural enemy attack in nests when females were absent. Group and solitary nesting may be advantageous under different conditions. C1 SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34022 USA. RP Soucy, SL (reprint author), Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. RI Giray, Tugrul/K-9570-2013 NR 48 TC 27 Z9 28 U1 1 U2 8 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PY 2003 VL 50 IS 3 BP 248 EP 255 DI 10.1007/s00040-003-0670-8 PG 8 WC Entomology SC Entomology GA 724KY UT WOS:000185487800009 ER PT S AU Szentgyorygi, AH Fabricant, DG Brown, WR Epps, HW AF Szentgyorygi, AH Fabricant, DG Brown, WR Epps, HW BE Iye, M Moorwood, AFM TI Cross dispersion and an integral field unit for Hectochelle SO INSTRUMENT DESIGN AND PERFORMANCE FOR OPTICAL/INFRARED GROUND-BASED TELESCOPES, PTS 1-3 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Instrument Design and Performance for Optical/Infrared Ground-based Telescopes CY AUG 25-28, 2002 CL WAIKOLOA, HI SP SPIE DE spectrographs; high resolution spectroscopy; integral field units; optical design ID CONVERTED MMT; OPTICAL-FIBER; SPECTROGRAPH; CELL AB We describe our plans to add cross-dispersion and an integral field unit. to the Hectochelle spectrograph, a multiobject, fiber-fed echelle spectrograph for the converted MMT. Hectochelle was originally designed without cross-dispersion to be used in a single order or overlapping orders selected by interference filters. The addition of cross-dispersion allows us to trade off multiplex advantage for spectral coverage. Our cross-disperser uses an unusual segmented, zero-deviation prism that is very compact, allowing it to fit into the existing instrument without modification. The planned integral field unit can be used with either Hectochelle or the moderate-dispersion Hectospec bench spectrograph. Both spectrographs were originally designed to be fiber-fed with a robotic fiber positioner as a front end, so adding an integral field capability is a natural enhancement. The integral field unit will use smaller diameter fibers than the robotic fiber positioner (subtending 0."16 vs. 1."5), so that both spectrographs will achieve higher spectral resolution in integral field mode. With the integral field unit Hectochelle will reach a two pixel resolution, R similar to 70, 000, and,Hectospec will reach R similar to 2000 with its 270 line mm(-1) grating. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Szentgyorygi, AH (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4620-3 J9 P SOC PHOTO-OPT INS PY 2003 VL 4841 BP 1026 EP 1035 DI 10.1117/12.459847 PN 1-3 PG 10 WC Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW44M UT WOS:000182018500100 ER PT S AU Brown, WR Fabricant, DG Boyd, DA AF Brown, WR Fabricant, DG Boyd, DA BE Iye, M Moorwood, AFM TI Thermal considerations in modern spectrograph design: the Binospec spectrograph SO INSTRUMENT DESIGN AND PERFORMANCE FOR OPTICAL/INFRARED GROUND-BASED TELESCOPES, PTS 1-3 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Instrument Design and Performance for Optical/Infrared Ground-based Telescopes CY AUG 25-28, 2002 CL WAIKOLOA, HI SP SPIE DE spectrograph design; heat transfer ID CONVERTED MMT AB We have completed a detailed thermal analysis of Binospec, a wide-field, multi-slit spectrograph being developed for the 6.5m MMT. The goals of our analysis were to minimize temperature gradients and thermally-induced deflections and achieve a >24 hr time constant in the spectrograph optics. We consider the effects of conduction, convection, and radiation with the external environment, and model the consequences of opening a spectrograph to insert new slit masks. or filters. We study when internal heat sources balance environmental effects, and the local effects of a hot motor in a spectrograph. We review the results of these thermal analyses and draw general conclusions useful to instrument builders. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brown, WR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4620-3 J9 P SOC PHOTO-OPT INS PY 2003 VL 4841 BP 1265 EP 1272 DI 10.1117/12.460098 PN 1-3 PG 8 WC Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW44M UT WOS:000182018500124 ER PT S AU Traub, WA Ahearn, A Carleton, NP Berger, JP Brewer, M Hofmann, KH Kern, P Lacasse, MG Malbet, F Millan-Gabet, R Monnier, JD Ohnaka, K Pedretti, E Ragland, S Schloerb, FP Souccar, K Weigelt, G AF Traub, WA Ahearn, A Carleton, NP Berger, JP Brewer, M Hofmann, KH Kern, P Lacasse, MG Malbet, F Millan-Gabet, R Monnier, JD Ohnaka, K Pedretti, E Ragland, S Schloerb, FP Souccar, K Weigelt, G BE Traub, WA TI New beam-combination techniques at IOTA SO INTERFEROMETRY FOR OPTICAL ASTRONOMY II, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Interferometry for Optical Astronomy II CY AUG 22-28, 2002 CL WAIKOLOA, HI SP SPIE DE interferometer; beam combination ID STARS; INTERFEROMETRY AB New beam combination techniques, using two and three telescopes, have been the focus of activity at IOTA during the past two years since our last update.(1) In particular, we have added a third telescope, made closure-phase measurements, demonstrated two- and three-beam combination with integrated optics combiners, demonstrated two-beam combination with an asymmetric coupler, and made simultaneous JHK visibility measurements with an image-plane combiner. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Traub, WA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Monnier, John D/0000-0002-3380-3307 NR 21 TC 29 Z9 29 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4617-3 J9 P SOC PHOTO-OPT INS PY 2003 VL 4838 BP 45 EP 52 DI 10.1117/12.459718 PN 1&2 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW43U UT WOS:000181980200006 ER PT S AU Millan-Gabet, R Pedretti, E Monnier, JD Traub, WA Schloerb, FP Carleton, NP Ragland, S Lacasse, MG Danchi, WC Tuthill, PG Perrin, G du Foresto, VC AF Millan-Gabet, R Pedretti, E Monnier, JD Traub, WA Schloerb, FP Carleton, NP Ragland, S Lacasse, MG Danchi, WC Tuthill, PG Perrin, G du Foresto, VC BE Traub, WA TI Recent science results from the two-telescope IOTA SO INTERFEROMETRY FOR OPTICAL ASTRONOMY II, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Interferometry for Optical Astronomy II CY AUG 22-28, 2002 CL WAIKOLOA, HI SP SPIE DE IOTA; interferometer; Mira; carbon; X-ray binaries; CI Cam; V Hydrae ID ANGULAR SIZE MEASUREMENTS; MU-M; STARS; INTERFEROMETRY; DIAMETER AB The IOTA (Infrared Optical Telescope Array) has been routinely operating with two-telescopes since 1994, a mode destined to become obsolete following its recent conversion to a three-telescope array.(1) In two-telescope mode, the IOTA has made numerous scientific and technical contributions, see e.g. our list of publications at http://cfa-www.harvard.edu/cfa/oir/IOTA/PUBLI/Publications.html. We present preliminary results on three different topics using recent data from the two-telescope IOTA: (1) measurements of Mira star diameters simultaneously in three different near-infrared spectral bands, (2) measurement of the characteristic size and shape of the source of near-infared emission in the x-ray binary system CI Cam, and (3) aperture synthesis of the Carbon star V Hydrae combining data from the IOTA and from aperture masking at the Keck-I telescope. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Millan-Gabet, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Monnier, John D/0000-0002-3380-3307 NR 19 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4617-3 J9 P SOC PHOTO-OPT INS PY 2003 VL 4838 BP 202 EP 209 DI 10.1117/12.459687 PN 1&2 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW43U UT WOS:000181980200026 ER PT S AU Berger, JP AF Berger, JP BE Traub, WA TI Guided optics in interferometry SO INTERFEROMETRY FOR OPTICAL ASTRONOMY II, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Interferometry for Optical Astronomy II CY AUG 22-28, 2002 CL WAIKOLOA, HI SP SPIE DE interferometry; fiber optics; integrated optics; imaging ID SINGLE-MODE FIBERS; ASTRONOMICAL INTERFEROMETRY; STELLAR INTERFEROMETER; INTEGRATED-OPTICS; BEAM COMBINER; LINE AB The importance of guided optics in stellar interferometry is discussed. Specificities, advantages and drawbacks are presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Berger, JP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM berger@obs.ujf-grenoble.fr NR 32 TC 1 Z9 1 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4617-3 J9 PROC SPIE PY 2003 VL 4838 BP 251 EP 265 DI 10.1117/12.456972 PN 1&2 PG 15 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW43U UT WOS:000181980200031 ER PT S 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 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 BE Traub, WA TI Aperture synthesis using multiple facilities: Keck aperture masking and the IOTA interferometer SO INTERFEROMETRY FOR OPTICAL ASTRONOMY II, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Interferometry for Optical Astronomy II CY AUG 22-28, 2002 CL WAIKOLOA, HI SP SPIE DE optical interferometry; aperture synthesis; imaging; deconvolution; maximum entropy ID ENTROPY; LEONIS AB As the number of optical interferometers increase, multi-facility observations become both feasible and scientifically interesting. For imaging of complex sources, the capability of increasing (u,v) coverage by using multiple arrays may be necessary for accurately interpreting the fringe visibility and closure phase data. Toward this end, coordinated observations with the IOTA interferometer and Keck aperture masking have been carried out to test techniques for synthesizing images using data from heterogeneous arrays with sparse (u,v) coverage. In particular, we will focus on how the image prior in the Maximum Entropy Method can be used to efficiently incorporate very high spatial frequency information with "low-resolution" data for imaging the generic prototype "Star + Dust Shell" image morphology. Preliminary results using real data for a few dusty evolved stars are presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Monnier, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Monnier, John D/0000-0002-3380-3307 NR 21 TC 5 Z9 5 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4617-3 J9 P SOC PHOTO-OPT INS PY 2003 VL 4838 BP 379 EP 386 DI 10.1117/12.459694 PN 1&2 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW43U UT WOS:000181980200043 ER PT S AU Monnier, JD Berger, JP Millan-Gabet, R Traub, WA Carleton, NP Pedretti, E Coldwell, CM Papaliolios, CD AF Monnier, JD Berger, JP Millan-Gabet, R Traub, WA Carleton, NP Pedretti, E Coldwell, CM Papaliolios, CD BE Traub, WA TI SMART precision interferometry at 794 nm SO INTERFEROMETRY FOR OPTICAL ASTRONOMY II, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Interferometry for Optical Astronomy II CY AUG 22-28, 2002 CL WAIKOLOA, HI SP SPIE DE fiber optics; optical interferometry; Cepheids; spatial filtering ID MODE FIBER OPTICS; ASTRONOMICAL INTERFEROMETRY; STELLAR INTERFEROMETER AB Single-mode fibers have been used in the near-infrared to dramatically reduce calibration error for long-baseline interferometry. We have begun an effort to apply the advantages of spatial filtering at visible wavelengths for precision measurements of pulsating Cepheids using the IOTA interferometer. Rather than employing photometric taps to calibrate fluctuating coupling efficiency, we are using an "asymmetric" coupler which allows this calibration to be done without losing photons. The Single-Mode Asymmetric Recombination Technique (SMART) experiment has finished lab-testing, and has been installed at IOTA for full commissioning in Summer 2002. We report the results of lab characterization and first sky tests, as well as first fringes on a star using a visible-wavelength single-mode coupler. With both lab and sky experience using unpolarized light, we have found that circular silica fibers are quite practical for precision interferometric measurements. We conclude that circular fibers (as opposed to polarization maintaining fibers) have an undeserved poor reputation and that birefringence effects pose no significant difficulty. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Monnier, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Monnier, John D/0000-0002-3380-3307 NR 11 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4617-3 J9 P SOC PHOTO-OPT INS PY 2003 VL 4838 BP 1127 EP 1138 DI 10.1117/12.459696 PN 1&2 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW43U UT WOS:000181980200122 ER PT S AU Ragland, S Traub, WA Millan-Gabet, R Carleton, NP Pedretti, E AF Ragland, S Traub, WA Millan-Gabet, R Carleton, NP Pedretti, E BE Traub, WA TI A low-resolution spectrograph for the IOTA interferometer SO INTERFEROMETRY FOR OPTICAL ASTRONOMY II, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Interferometry for Optical Astronomy II CY AUG 22-28, 2002 CL WAIKOLOA, HI SP SPIE ID 2.5 MU-M; ANGULAR DIAMETER; R-LEONIS; EFFECTIVE TEMPERATURES; VARIABLE-STARS; O-CETI; MIRA; SPECTRA; ATMOSPHERE; PULSATION AB The design and scientific objectives of a near infrared channeled spectrometer planned at the IOTA interferometer are discussed. The spectrometer has the flexibility to reconfigure easily for conventional broadband operations in addition to multi-channel mode. This instrument makes use of the existing PICNIC camera at the IOTA in order to be cost efficient. The spectrometer has been designed specifically for studying Mira stars. However, it will find its application in other areas of astrophysical interests such as studies of circumstellar disks around young stars and binary stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ragland, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4617-3 J9 P SOC PHOTO-OPT INS PY 2003 VL 4838 BP 1225 EP 1233 DI 10.1117/12.459321 PN 1&2 PG 9 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW43U UT WOS:000181980200133 ER PT J AU Bush, T AF Bush, T TI African American artists in Amsterdam: Sam Middleton rediscovered (plus Deborah Simon, Sherard Van Dyke and Lorina Harris) SO INTERNATIONAL REVIEW OF AFRICAN AMERICAN ART LA English DT Article C1 Smithsonian Inst, Hirshhorn Museum & Sculpture Garden, Washington, DC 20560 USA. Howard Univ, Washington, DC 20059 USA. RP Bush, T (reprint author), Smithsonian Inst, Hirshhorn Museum & Sculpture Garden, Washington, DC 20560 USA. NR 28 TC 2 Z9 2 U1 0 U2 0 PU MUSEUM AFR AMER ART PI LOS ANGELES PA 4005 CRENSHAW BLVD, LOS ANGELES, CA 90008-2534 USA SN 1045-0920 J9 INT REV AFR AM ART JI Int. Rev. Afr. Am. Art PY 2003 VL 19 IS 2 BP 2 EP 17 PG 16 WC Art SC Art GA 757YW UT WOS:000187606600001 ER PT J AU Strong, EE Harasewych, MG Haszprunar, G AF Strong, EE Harasewych, MG Haszprunar, G TI Phylogeny of the Cocculinoidea (Mollusca, Gastropoda) SO INVERTEBRATE BIOLOGY LA English DT Article DE morphology; cladistics; deep-sea ID LIMPETS MOLLUSCA; DEEP-SEA; ARCHAEOGASTROPODA; ANATOMY; COCCULINIFORMIA; AFFINITIES AB The superfamily Cocculinoidea is a group of marine, deep-water, limpet-like gastropods. Recent speculation surrounding their affinities has concentrated on their placement within the Gastropoda. However, phylogenetic relationships within the Cocculinoidea, especially the monophyly of families and genera within the group, remain poorly understood. Phylogenetic analysis of 31 morphological characters for 15 cocculinoidean taxa and 2 outgroups resulted in a single most parsimonious tree, length=70, CI=0.62, and RI=0.71. Monophyly of the Cocculinoidea, Cocculinidae, and the genera Cocculina and Coccopigya was supported; Paracocculina and Coccocrater were found to be paraphyletic. Character optimization demonstrates that many characters often cited as diagnostic of various taxa, are often homoplastic and/or synapomorphies at different hierarchical levels. C1 Univ Minnesota, Bell Museum Nat Hist, Dept Fisheries Wildlife & Conservat Biol, St Paul, MN 55108 USA. Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. Zool Staatssammlung Munchen, D-81247 Munich, Germany. RP Strong, EE (reprint author), Univ Minnesota, Bell Museum Nat Hist, Dept Fisheries Wildlife & Conservat Biol, St Paul, MN 55108 USA. NR 38 TC 6 Z9 7 U1 0 U2 4 PU AMER MICROSCOPICAL SOC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1077-8306 J9 INVERTEBR BIOL JI Invertebr. Biol. PY 2003 VL 122 IS 2 BP 114 EP 125 PG 12 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 683FK UT WOS:000183137400002 ER PT J AU Rutzler, K van Soest, RWM Alvarez, B AF Rutzler, K van Soest, RWM Alvarez, B TI Svenzea zeai, a Caribbean reef sponge with a giant larva, and Scopalina ruetzleri: a comparative fine-structural approach to classification (Demospongiae, Halichondrida, Dictyonellidae) SO INVERTEBRATE BIOLOGY LA English DT Article DE Porifera, microbial symbiosis ID SWIMMING BEHAVIOR; ULTRASTRUCTURE; METAMORPHOSIS; MORPHOLOGY; PORIFERA; GENUS; OOGENESIS; BACTERIA; CELLS AB Svenzea zeai, abundant on many deep Caribbean fore-reef habitats but of uncertain systematic position within the Demospongiae, is closely examined histologically and cytologically for evidence of its phylogenetic relationship, beyond the traditional analysis of gross morphology and skeletal structure. We document that S. zeai is a bacteriosponge containing substantial quantities of unicellular photosynthetic and autotrophic microbes; that the most abundant cell type is an unusual cell with refractile granules that only few species share and whose composition and function are still enigmatic; and that it produces the largest-by a factor of 3-embryos and larvae recorded in the phylum Porifera, A combination of characters such as the granular cells, ciliary pattern, and aspects of larval shape and behavior are comparable with those of Scopalina ruetzleri, family Dictyonellidae, a prominent member of the Caribbean mangrove community. These results support our earlier decision to establish Svenzea as a new genus in Dictyonellidae to accommodate its unprecedented skeletal structure, styles in isodictyal reticulation. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. Univ Amsterdam, Museum Zool, NL-1090 GT Amsterdam, Netherlands. Museum & Art Gallery No Terr, Darwin, NT, Australia. RP Rutzler, K (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. NR 44 TC 13 Z9 13 U1 1 U2 4 PU AMER MICROSCOPICAL SOC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1077-8306 J9 INVERTEBR BIOL JI Invertebr. Biol. PY 2003 VL 122 IS 3 BP 203 EP 222 PG 20 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 716TU UT WOS:000185045900002 ER PT J AU Davis, DR Gentili, P AF Davis, DR Gentili, P TI Andesianidae, a new family of monotrysian moths (Lepidoptera : Andesianoidea) from austral South America SO INVERTEBRATE SYSTEMATICS LA English DT Article ID PHYLOGENY AB The new family Andesianidae is proposed for the genus Andesiana, consisting of three previously described species, A. brunnea Gentili, A. lamellata Gentili and A. similis Gentili, from southern Argentina and Chile. Originally described in the ditrysian family Cossidae, Andesiana has been found to possess a monotrysian female reproductive system. The principal autapomorphies for the family are the elongate second segment of the labial palpi, presence of a male tibial pouch and associated femoral hair pencil and, within the monotrysian Heteroneura, possibly the strongly dimorphic antennae (broadly bipectinate in male, filiform in female). Other significant characters of the group include a greatly reduced haustellum, male genitalia with a broad vinculum, acuminate uncus, scutiform juxta and a pronounced saccular lobe of the valva that bears a subapical, setose appendage within a shallow, mesal cavity. The female genitalia possess a short cloaca and paired anal papillae and lack signa. Although known to be retained only in the female of A. lamellata, the presence of a two-branched Rs in the hindwing may indicate an origin of the Andesianidae basal to the Nepticuloidea. In contrast, the structure of the wing coupling apparatus for the family suggests a later appearance. Because no synapomorphy is known linking the Andesianidae with any other superfamily, the new superfamily, Andesianoidea, is proposed. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Davis, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, POB 37012, Washington, DC 20560 USA. EM davis.don@nmnh.si.edu NR 21 TC 6 Z9 9 U1 0 U2 5 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-5226 J9 INVERTEBR SYST JI Invertebr. Syst. PY 2003 VL 17 IS 1 BP 15 EP 26 DI 10.1071/IS02006 PG 12 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 659KA UT WOS:000181774800005 ER PT J AU Holloway, JD Miller, SE AF Holloway, JD Miller, SE TI The composition, generic placement and host-plant relationships of the joviana-group in the Parallelia generic complex (Lepidoptera : Noctuidae, Catocalinae) SO INVERTEBRATE SYSTEMATICS LA English DT Article DE Achaea; Bastilla; Buzara; Caranilla; Dysgonia; Grammodes; Euphorbiaceae; Malesia; Oriental; Australasian; tropics; host specialism ID NEW-GUINEA; INSECTS; FOREST AB The biosystematic position of the Parallelia generic complex is reviewed and a revised generic classification of its component taxa is presented. Bastilla Swinhoe (= Xiana Nye, syn. nov., Naxia Guenee, syn. nov.) is identified as the most appropriate genus for a large number of these taxa, including the joviana-group, which is reviewed in detail, with description of two new species, B. nielseni, sp. nov. and B. binatang, sp. nov. Parallelia prouti Hulstaert, syn. nov. and P. cuneifascia Hulstaert, syn. nov. are recognised as junior synonyms of Bastilla vitiensis Butler and two newly described Tahitian taxa are transferred into the joviana-group. Larval host records are examined in relation to this new generic system and significant preference for the Euphorbiaceae is noted for several groups: Bastilla, Buzara Walker (= Caranilla Moore, syn. nov., another segregate from Parallelia) and an Australian group within Grammodes Guenee. C1 Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Holloway, JD (reprint author), Nat Hist Museum, Dept Entomol, Cromwell Rd, London SW7 5BD, England. EM jdh@nhm.ac.uk OI Miller, Scott/0000-0002-4138-1378 NR 53 TC 4 Z9 7 U1 0 U2 2 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-5226 J9 INVERTEBR SYST JI Invertebr. Syst. PY 2003 VL 17 IS 1 BP 111 EP 128 DI 10.1071/IS02030 PG 18 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 659KA UT WOS:000181774800014 ER PT J AU Agnarsson, I AF Agnarsson, I TI The phylogenetic placement and circumscription of the genus Synotaxus (Araneae : Synotaxidae), a new species from Guyana, and notes on theridioid phylogeny SO INVERTEBRATE SYSTEMATICS LA English DT Article ID SPIDER; EVOLUTION; RICHNESS; FOREST; WEBS AB The genus Synotaxus Simon, 1895 is reviewed. Modern systematic work has challenged the classical placement of Synotaxus as an argyrodine theridiid. Its placement is evaluated in a phylogenetic analysis containing a wide selection of theridiids, including all major argyrodine genera. For the analysis, two published matrices are fused to produce a dataset containing 83 orbicularian taxa and 302 morphological characters. Although the two matrices share only 10 taxa and 33 characters, a single most parsimonious tree is obtained. The results are congruent with results from each independent matrix, and unambiguously corroborate the placement of Synotaxus outside Theridiidae. Some superficial similarities, such as the elongate abdomen extending far beyond the spinnerets, are clearly convergent in the two taxa. Synotaxus, furthermore, lacks the suite of synapomorphies defining Theridiidae. Thus, its transfer out of Theridiidae is corroborated, and a sister relationship with Chileotaxus Platnick, 1990 is proposed, based on similarities in web and somatic morphology. A synapomorphy-based circumscription of the genus is given. Synotaxus waiwai, sp. nov. is described, Synotaxus monoceros (Caporiacco, 1947), previously only known from males, is redescribed and synonymised with S. pupularum, Exline & Levi, 1965, syn. nov., previously only known from females. A description of the webs of both species is given, as well as that of Chileotaxus sans Platnick, 1990. Many further Synotaxus species remain to be described. C1 Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Agnarsson, I (reprint author), Smithsonian Inst, E-530,NHB-105,POB 37012, Washington, DC 20013 USA. EM ingi@gwu.edu NR 40 TC 31 Z9 34 U1 0 U2 4 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA SN 1445-5226 EI 1447-2600 J9 INVERTEBR SYST JI Invertebr. Syst. PY 2003 VL 17 IS 6 BP 719 EP 734 DI 10.1071/IS03002 PG 16 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 758JY UT WOS:000187632300002 ER PT S AU Ashby, MLN Surace, JA Hora, JL AF Ashby, MLN Surace, JA Hora, JL BE Mather, JC TI A realistic science data simulator for the IRAC camera on SIRTF SO IR SPACE TELESCOPES AND INSTRUMENTS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on IR Space Telescopes and Instruments CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE infrared astronomy; infrared arrays; simulations; SIRTF; IRAC; mission planning ID ARRAY AB The Infrared Array Camera (IRAC)(1) is one of three major scientific instruments to be launched aboard the Space Infrared Telescope Facility (SIRTF)(2). This document briefly describes the features, usage, and limitations of the IRAC Science Data Simulator (ISDS) that can be used to generate simulated data to anticipate data quality and reduction issues for mission operations. The software is a combination of C++ and IRAF SPP routines. that implement the features already characterized during the integration and test phase of IRAC's development. While no guarantee of accuracy is made, the intention is to replicate as faithfully as possible known characteristics and artifacts of the IRAC instrument. The many beneficial applications of the ISDS include facilitating planning of the IRAC pipeline by the SIRTF Science Center (SSC), and validating observing strategies for SIRTF Guaranteed Time Observers and Legacy teams. The simulator has already been used by mission planners to demonstrate the relative effectiveness of different approaches to data reduction. It will also be of great value in demonstrating IRAC's capabilities for-mapping and source detection, and in testing post-pipeline software currently being developed for these purposes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4629-7 J9 P SOC PHOTO-OPT INS PY 2003 VL 4850 BP 50 EP 61 DI 10.1117/12.461786 PN 1&2 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BW44N UT WOS:000182018700006 ER PT S AU Hora, JL Fazio, GG Allen, LE Ashby, MLN Barmby, P Deutsch, LK Huang, JS Megeath, ST Pahre, MA Patten, BM Wang, Z Willner, SP Hoffmann, WF Mentzell, JE Eisenhard, P Stern, D Gorjian, V Glaccum, W Lacy, M Carey, S Surace, JA Reach, WT Pipher, JL Forrest, WJ McCreight, CR AF Hora, JL Fazio, GG Allen, LE Ashby, MLN Barmby, P Deutsch, LK Huang, JS Megeath, ST Pahre, MA Patten, BM Wang, Z Willner, SP Hoffmann, WF Mentzell, JE Eisenhard, P Stern, D Gorjian, V Glaccum, W Lacy, M Carey, S Surace, JA Reach, WT Pipher, JL Forrest, WJ McCreight, CR BE Mather, JC TI Performance of the Infrared Array Camera (IRAC) for SIRTF during instrument integration and test SO IR SPACE TELESCOPES AND INSTRUMENTS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on IR Space Telescopes and Instruments CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE infrared astronomy; infrared arrays; calibration; SIRTF; IRAC ID TELESCOPE-FACILITY SIRTF AB The Infrared Array Camera (IRAC) is one of three focal plane instruments in the Space Infrared Telescope Facility (SIRTF). IRAC is a four-channel camera that obtains simultaneous images at 3.6, 4.5, 5.8, and 8 microns. Two adjacent 5.12x5.12 arcmin fields of view in the SIRTF focal plane are viewed by the four channels in pairs (3.6 and 5.8 microns; 4.5 and 8 microns). All four detector arrays in the camera are 256x256 pixels in size, with the two shorter wavelength channels using InSb and the two longer wavelength channels using Si:As IBC detectors. We describe here the results of the instrument functional and calibration tests completed at Ball Aerospace during the integration with the cryogenic telescope assembly, and provide updated estimates of the in-flight sensitivity and performance of IRAC in SIRTF. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hora, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Hora, Joseph/0000-0002-5599-4650 NR 14 TC 2 Z9 2 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4629-7 J9 P SOC PHOTO-OPT INS PY 2003 VL 4850 BP 83 EP 97 DI 10.1117/12.461791 PN 1&2 PG 15 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BW44N UT WOS:000182018700009 ER PT J AU Cederbaum, LS Moiseyev, N AF Cederbaum, LS Moiseyev, N TI On the collapse and restoration of condensates in n dimensions in the mean-field approximation SO ISRAEL JOURNAL OF CHEMISTRY LA English DT Article; Proceedings Paper CT Conference on Perspectives in Chemistry CY JUN 15-17, 2003 CL Tel Aviv, ISRAEL ID BOSE-EINSTEIN CONDENSATION; ATTRACTIVE INTERACTIONS; DARK SOLITONS AB The mean-field equation of N bosons in an external potential interacting via a short-range delta-function potential is studied. This equation is formally equivalent to the nonlinear Schrodinger equation. Virial theorems are derived and the number of possible solutions is investigated for various dimensions n. The unboundedness from below of the underlying mean-field operator for attractive nonlinearity and the related collapse of the wave function are studied in n dimensions. Within the symmetry preserving mean-field approximation, an ansatz to avoid the collapse by modifying the spherically symmetric external potential is discussed and analyzed. Other suggestions to stabilize the mean-field condensate are briefly mentioned. Illustrative numerical examples of the collapse and its restoration are given. Detailed conclusions are drawn. C1 Heidelberg Univ, Inst Phys Chem, D-69120 Heidelberg, Germany. Technion Israel Inst Technol, Dept Chem, IL-32000 Haifa, Israel. Technion Israel Inst Technol, Minerva Ctr Nonlinear Phys Complex Syst, IL-32000 Haifa, Israel. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 01238 USA. RP Cederbaum, LS (reprint author), Heidelberg Univ, Inst Phys Chem, Im Neuenheimer Feld 229, D-69120 Heidelberg, Germany. EM Lorenz.Cederbaum@urz.uni-heidelberg.de NR 19 TC 0 Z9 0 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0021-2148 EI 1869-5868 J9 ISR J CHEM JI Isr. J. Chem. PY 2003 VL 43 IS 3-4 BP 267 EP 277 DI 10.1560/UVHD-ERLQ-3YGN-VPPH PG 11 WC Chemistry, Multidisciplinary SC Chemistry GA 829FJ UT WOS:000222031600009 ER PT J AU Rappole, JH Hubalek, Z AF Rappole, JH Hubalek, Z TI Migratory birds and West Nile virus SO JOURNAL OF APPLIED MICROBIOLOGY LA English DT Article ID NORTHEASTERN UNITED-STATES; ENCEPHALITIS; MOSQUITOS; SURVEILLANCE; TRANSMISSION; ECOLOGY AB West Nile virus was first recorded in the New World during August 1999 in New York City. Aetiology of the disease in the Old World indicated birds as the likely introductory and amplifying hosts with ornithophilous mosquitoes, e.g. Culex pipiens, as the principal vectors. Speculation regarding likely agents for movement of the virus in its new environment focused on migratory birds, but evidence to date is equivocal. While spread of the disease has been fairly rapid, at a rate of roughly 70 km a month, it has not shown the kind of long-distance, leap frog movements one might expect if transient birds were the principal introductory hosts. Furthermore, movement of the disease has not been focused southward, but shows a radiating pattern with detection sites located in all directions from New York where terrestrial habitat was available. In addition, tests among potential New World, avian hosts have revealed prolonged viraemia (up to 5 days) only in the relatively nonmigratory House Sparrow (Passer domesticus). Dispersal movements by this species could account for the observed pattern of West Nile virus spread in the Western Hemisphere to date. Regardless of whether avian migration, dispersal, or some other agent is responsible, West Nile virus should reach the New World tropics in another 1-2 years, at which time a vast number of new potential introductory and amplifying avian hosts would be exposed to the disease and mosquito vectors would be available throughout most of the year, likely causing serious, long-term threats to human health and vulnerable avian populations in the region. C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA. Acad Sci Czech Republ, Lab Med Zool, Inst Vertebrate Biol, CZ-69142 Valtice, Czech Republic. RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. RI Hubalek, Zdenek/G-1111-2014 OI Hubalek, Zdenek/0000-0003-4732-0987 NR 62 TC 28 Z9 30 U1 1 U2 10 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1364-5072 J9 J APPL MICROBIOL JI J. Appl. Microbiol. PY 2003 VL 94 SU S BP 47S EP 58S PG 12 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 673DY UT WOS:000182566000007 PM 12675936 ER PT J AU Scharff, N Coddington, JA Griswold, CE Hormiga, G Bjorn, PD AF Scharff, N Coddington, JA Griswold, CE Hormiga, G Bjorn, PD TI When to quit? Estimating spider species richness in a northern European deciduous forest SO JOURNAL OF ARACHNOLOGY LA English DT Article DE biodiversity; Araneae; inventory; species richness estimation; singletons; beech forest; Denmark ID RAIN-FOREST; DIVERSITY; ABUNDANCE; COMMUNITIES; BIODIVERSITY; ASSEMBLAGES; SULAWESI; NUMBER; TREE AB Terrestrial arthropod surveys and inventories frequently suffer from undersampling bias; common species are over-represented and rare species may be missed entirely. This study compared a rapid (3 days) and intense inventory of spiders from one hectare of a mature beech forest (Fagus sylvaticus) in Hestehaven, Denmark, comprising 8,710 adult spiders of 66 species to a previous, much more thorough, bi-weekly survey of two years duration from the same site that comprised 42,273 spiders (adult and juvenile) of 141 species. Non-parametric species richness estimators were used to assess the degree of undersampling bias in various data partitions. The current study used five experienced, four novice collectors, and five semi-quantitative collecting methods. Method and time of day strongly affected numbers of species and adults per sample. Collector experience affected numbers of species but not numbers of adults per sample. Despite the intensive collecting, number of adults per sample did not decrease over the course of the study. At the end of the sampling, 31 species were still rare in the sample (singletons or doubletons). Non-parametric richness estimators suggest that the actual richness of adult spiders in the study plot at this time of year and susceptible to the methods used was about 80 species. Species turnover between the two surveys (ca 23 years) was remarkably small: the two lists were 92% identical. The baseline study suggests that the rarity of 12 of the 31 rare species was artifactual (10 due to phenology, one to method, another to spatial edge effects). The rarity of the remainder is unexplained and by default is interpreted as undersampling bias. C1 Univ Copenhagen, Dept Entomol, Zool Museum, DK-2100 Copenhagen, Denmark. Smithsonian Inst, Dept Syst Biol, Natl Museum Nat Hist, Washington, DC 20013 USA. Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA. George Washington Univ, Dept Biol, Washington, DC 20052 USA. RP Scharff, N (reprint author), Univ Copenhagen, Dept Entomol, Zool Museum, Universitetsparken 15, DK-2100 Copenhagen, Denmark. RI Hormiga, Gustavo/C-3874-2009; Scharff, Nikolaj/A-4787-2013 OI Scharff, Nikolaj/0000-0001-6809-2878 NR 65 TC 63 Z9 73 U1 1 U2 14 PU AMER ARACHNOLOGICAL SOC PI NEW YORK PA C/O NORMAN I PLATNICK, AMER MUSEUM NATURAL HISTORY, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2003 VL 31 IS 2 BP 246 EP 273 DI 10.1636/0161-8202(2003)031[0246:WTQESS]2.0.CO;2 PG 28 WC Entomology SC Entomology GA 732FB UT WOS:000185929200004 ER PT J AU Agnarsson, I AF Agnarsson, I TI Spider webs as habitat patches - The distribution of kleptoparasites (Argyrodes, theridiidae) among host webs (Nephila, tetragnathidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Habitat islands; habitat stability; ideal free distribution; orb web; patch connectivity ID ANTIPODIANA THERIDIIDAE; NEW-ZEALAND; ARANEAE; SPECIFICITY; POPULATION; CLAVIPES; BEHAVIOR AB Most adult golden orb weavers (Nephila clavipes) have kleptoparasites of the genus Argyrodes in their webs. The kleptoparasitic load correlates positively with web size. Clustered (interconnected) webs have a more predictable number of kleptoparasites than do solitary webs, but there is no difference in the mean number of kleptoparasites between the two. From the view of the kleptoparasite, host webs are habitat patches or islands. Isolated webs show characteristics of small patches, where web size is a poor indicator of kleptoparasite number and variation is high. The distribution of kleptoparasites in clustered webs, on the other hand, seems to fit the "ideal free distribution" where web size nearly entirely predicts kleptoparasitic load. Thus clustered webs, as a habitat patch, are more than merely the combination of their parts. The predictability of kleptoparasite load in clustered webs may be a function of the stability (longevity) of those habitat patches, and ease of colonization, as neighboring webs act as sources. C1 Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Agnarsson, I (reprint author), Smithsonian Inst, E-530,NHB-105,POB 37012, Washington, DC 20013 USA. NR 32 TC 24 Z9 26 U1 4 U2 21 PU AMER ARACHNOLOGICAL SOC PI NEW YORK PA C/O NORMAN I PLATNICK, AMER MUSEUM NATURAL HISTORY, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2003 VL 31 IS 3 BP 344 EP 349 DI 10.1636/s02-21 PG 6 WC Entomology SC Entomology GA 759DC UT WOS:000187722200004 ER PT J AU Summers, K Cronin, TW Kennedy, T AF Summers, K Cronin, TW Kennedy, T TI Variation in spectral reflectance among populations of Dendrobates pumilio, the strawberry poison frog, in the Bocas del Toro Archipelago, Panama SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE amphibian; neotropical; Central America; poison frog; spectral reflectance; colour; polymorphism; archipelago; aposematism; divergence ID GEOGRAPHIC-VARIATION; SEXUAL SELECTION; NATURAL-SELECTION; MATE PREFERENCE; EVOLUTION; COLORATION; MIMICRY; POLYMORPHISMS; DICHROMATISM; DIVERGENCE AB Aim The goal of this study was to quantify levels of variation in spectral reflectance within and among populations of Dendrobates pumilio , the strawberry poison frog from the Bocas del Toro Archipelago. Location This study was carried out in the Bocas del Toro Archipelago, in the Republic of Panama, Central America. Methods Spectral reflectance was measured for samples of individuals from fifteen distinct island and mainland populations, using an Ocean Optics 2000 spectrometer and a BiLink portable computer. Results Our results provide quantitative evidence for extreme polymorphism among populations, and more limited levels of polymorphism within some populations. No obvious signs of sexual dimorphism were found. All the colour morphs appear to have relatively little reflectance in the ultraviolet part of the spectrum. There is some evidence for clinal variation in colour and pattern across some mainland populations. There is also at least one area where distinctly different morphs occur in sympatry, suggesting the possibility of incipient reproductive isolation. We argue that variation in coloration may have been enhanced by sexual selection. C1 E Carolina Univ, Greenville, NC 27858 USA. Dept Biol, Greenville, NC 27858 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Maryland Baltimore Cty, Dept Biol, Baltimore, MD 21228 USA. McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP Summers, K (reprint author), E Carolina Univ, Greenville, NC 27858 USA. NR 45 TC 58 Z9 63 U1 1 U2 10 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD JAN PY 2003 VL 30 IS 1 BP 35 EP 53 DI 10.1046/j.1365-2699.2003.00795.x PG 19 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 635JC UT WOS:000180394900004 ER PT J AU Schiestl, FP Roubik, DW AF Schiestl, FP Roubik, DW TI Odor compound detection in male euglossine bees SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE euglossine bees; GC-EAD; EAG; odor compound detection ID ORCHID FLORAL FRAGRANCES AB Male euglossine bees collect fragrances from various sources, which they store and use for as yet unknown purposes. They are attracted, often specifically, to single odor compounds and blends thereof. We used gas chromatography with electroantennographic detection (GC-EAD) and electroantennography (EAG) to investigate the response to 8 odor compounds by males of two euglossine species, Euglossa cybelia Moure and Eulaema polychroma (Mocsary). In E. cybelia, we recorded EAD reactions in response to 1,8-cineole, methyl benzoate, benzyl actetate, methyl salicylate, eugenbl, and methyl cinnamate. E. polychroma responded to the same compounds in EAG experiments, while (1s)(-)alpha-pinene and beta-pinene failed to trigger EAD or EAG responses in the bees. Blends of two compounds triggered larger responses than single compounds in EAG experiments with E. polychroma, however, when alpha-pinene was added, reactions decreased. In the light of existing data on the bees' behavior towards these odor compounds, our work indicates that both peripheral and central nervous processes influence the attraction of euglossine bees to odors. C1 ETH, Geobot Inst, CH-8008 Zurich, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Schiestl, FP (reprint author), ETH, Geobot Inst, Zollikerstr 107, CH-8008 Zurich, Switzerland. NR 10 TC 36 Z9 37 U1 2 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 JAN PY 2003 VL 29 IS 1 BP 253 EP 257 DI 10.1023/A:1021932131526 PG 5 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 635GX UT WOS:000180392100018 PM 12647866 ER PT J AU deRivera, CE AF deRivera, CE TI Causes of a male-biased operational sex ratio in the fiddler crab Uca crenulata SO JOURNAL OF ETHOLOGY LA English DT Article DE fiddler crab; mating synchrony; operational sex ratio; reproductive cycle; Uca ID REPRODUCTIVE-BEHAVIOR; GENUS UCA; PUGILATOR; POPULATION; HISTORY; CYCLES; CONSEQUENCES; DIMORPHISM; PUGNAX; SMITH AB This research investigates the causes of a male-biased operational sex ratio in a population of the California fiddler crab, Uca crenulata. Mensurative studies revealed there were almost twice as many adult males as females, mating occurred across half of the days within the breeding season, and females had much longer individual reproductive cycles than males. Therefore, many more males than females were available for mating on each breeding day. Perhaps as a consequence, males spent a large proportion of their time fighting with neighbors and rapidly waving their large claws when females passed by. C1 Univ Calif San Diego, Dept Biol, La Jolla, CA 92093 USA. RP deRivera, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 31 TC 7 Z9 8 U1 0 U2 10 PU SPRINGER-VERLAG TOKYO PI TOKYO PA 3-3-13, HONGO, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 0289-0771 J9 J ETHOL JI J. Ethol. PY 2003 VL 21 IS 2 BP 137 EP 144 DI 10.1007/s10164-002-0090-7 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 672RF UT WOS:000182534700011 ER PT J AU Schulz, S Kruckert, K Weldon, PJ AF Schulz, S Kruckert, K Weldon, PJ TI New terpene hydrocarbons from the alligatoridae (Crocodylia, reptilia) SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID PARACLOACAL GLAND SECRETIONS; TRIGONATUS; LIPIDS AB The contents of the paracloacal gland secretions of the alligatorids Alligator mississippiensis, A. sinensis, Paleosuchus palpebrosus, and P. trigonatus were investigated. Novel acyclic hydrocarbon terpenes with a rare trisubstituted 2,4-diene system were identified in the secretions of A. sinensis, P. palpebrosus, and P. trigonatus. The structures of the monoterpene (2E,4E)-3,7-dimethyl-2,4-octadiene (9) and the sesquiterpene (2E,4E,7S)-3,7,11-trimethyl-2,4-dodecadiene (14) were proven by synthesis and gas chromatography on a chiral phase. Several other new terpenes (11, 16, 17, 18, 19, and 20) related to these components also were present in the secretions, as well as the known compounds myrcene (6), (E)-beta-farnesene (4), (E)-beta-springene (3), squalene (5), cembrene A (1), and 11,12-dihydrocembren-10-one (2). C1 Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, D-38106 Braunschweig, Germany. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22632 USA. RP Schulz, S (reprint author), Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, Hagenring 30, D-38106 Braunschweig, Germany. EM stefan.schulz@tu-bs.de NR 16 TC 10 Z9 10 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD JAN PY 2003 VL 66 IS 1 BP 34 EP 38 DI 10.1021/np020073r PG 5 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 639HX UT WOS:000180623400008 PM 12542341 ER PT J AU Olszewski, TD Patzkowsky, ME AF Olszewski, TD Patzkowsky, ME TI From cyclothems to sequences: The record of eustasy and climate on an icehouse epeiric platform (Pennsylvanian-Permian, North American Midcontinent) SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article ID ANCESTRAL ROCKY-MOUNTAINS; SEA-LEVEL CHANGES; DEPOSITIONAL SEQUENCES; CENTRAL KANSAS; MID-CONTINENT; SOUTH-AMERICA; USA; CYCLES; STRATIGRAPHY; STRATA AB The stratigraphic succession of the North American Midcontinent contains a high-resolution (< 100,000 year) record of sea level and climate change spanning the Pennsylvanian-Permian boundary. Outcrop-based sequence stratigraphic analysis on the upper Wabaunsee, Admire, and lower Council Grove groups in Kansas and Nebraska reveals a hierarchy of fifty-one fifth-order meter-scale cycles grouped into five fourth-order composite sequences. Fifth-order cycles are bounded by subaerial unconformities in nearshore settings and correlative conformities in offshore settings, and are therefore very thin depositional sequences. Lowstand systems tracts, observed only in nearshore deposits, are expressed as sandy, incised-valley fills in these meter-scale cycles. Transgressive systems tracts, which are dominated by carbonate deposition, include coastal evaporites indicating and climatic conditions. Highstand systems tracts, which are dominated by siliciclastic deposition, include thin but persistent coals in muddy coastal successions indicating humid climatic conditions. Paleosols at sequence boundaries evolve from vertic to calcic, indicating climate change from relatively humid to relatively and conditions during subaerial exposure. This indicates that relatively and climate coincided with eustatic lows while relatively humid climate coincided with eustatic highs on this low-latitude platform. Composite sequences are bounded by subaerial, angular unconformities; and display a transgressive-regressive stacking pattern of meter-scale cycles. The high-resolution stratigraphic record of the Midcontinent helps constrain the rate and magnitude of environmental change in ancient icehouse conditions and can serve as a baseline of environmental change for comparison with other coeval successions. C1 Smithsonian Inst, NMNH, Dept Paleobiol MRC 121, Washington, DC 20013 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Olszewski, TD (reprint author), Smithsonian Inst, NMNH, Dept Paleobiol MRC 121, POB 37012, Washington, DC 20013 USA. NR 94 TC 60 Z9 61 U1 0 U2 15 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 1527-1404 J9 J SEDIMENT RES JI J. Sediment. Res. PD JAN PY 2003 VL 73 IS 1 BP 15 EP 30 DI 10.1306/061002730015 PG 16 WC Geology SC Geology GA 637BC UT WOS:000180490900003 ER PT J AU Wcislo, WT AF Wcislo, WT TI A male sleeping roost of a sweat bee, Augochlorella neglectula (Ckll.) (Hymenoptera : Halictidae), in Panama SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article ID SOLITARY BEES AB A persistent sleeping roost is described for male sweat bees, Augochlorella neglectula (Ckll.), occurring on the rootlets of a hanging plant on a 4th story apartment balcony in an urban environment in central Panama. The rootlets were used by the same males consistently within a season, as well as between seasons, although presumably different individuals were involved. Males probably do not use olfactory cues for local orientation to the sleeping rootlet, as inferred from choice tests between an un-used and used rootlet. Brief social interactions among males were generally pacific, although there was kicking and shoving when they first settled. Males became progressively more difficult to disturb further into the night. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. NR 17 TC 8 Z9 10 U1 0 U2 5 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 JAN PY 2003 VL 76 IS 1 BP 55 EP 59 PG 5 WC Entomology SC Entomology GA 643RR UT WOS:000180874700006 ER PT J AU Silvera, K Skillman, JB Dalling, JW AF Silvera, K Skillman, JB Dalling, JW TI Seed germination, seedling growth and habitat partitioning in two morphotypes of the tropical pioneer tree Trema micrantha in a seasonal forest in Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE allocation patterns; Barro Colorado Nature Monument; habitat partitioning; seed size; Trema micrantha ID GAP-PHASE REGENERATION; RIO NEGRO REGION; RAIN-FOREST; SPECIES-RICHNESS; LIFE-HISTORY; AMAZON BASIN; PUERTO-RICO; WET FOREST; SIZE; DIVERSITY AB We examined the distribution, germination, growth and photosynthetic characteristics of two co-existing morphotypes of the pioneer tree Trema micrantha at the Barro Colorado Nature Monument (BCNM), Panama. Morphotypes differed significantly in distribution and in seed characteristics. A 'large'-seeded morphotype (endocarp mass = 3.83 mg) was associated with treefall gaps in the forest interior, whereas a 'small'-seeded morphotype (endocarp mass = 1.38 mg) was found predominantly on landslides on the margins of Lake Gatun. Seeds of the small-seeded morphotype germinated faster than seeds of the large-seeded morphotype, with seedlings of the small-seeded morphotype showing both a higher Unit Leaf Rate (ULR) and a lower Specific Leaf Area (SLA). Differences in photosynthetic rates reflected differences in SLA; the small-seeded morphotype had a higher rate on a leaf area basis, while the large-seeded morphotype had a higher rate on a leaf mass basis. Although allocation patterns between morphotypes varied in a way consistent with known interspecific differences between 'sun' and 'shade' plants, relative growth rates (RGR) of the morphotypes were similar across different light conditions suggesting that factors other than light, such as water uptake efficiency, soil nutrient requirements, and perhaps seed dispersal characters may explain the habitat partitioning of morphotypes. C1 Univ Panama, Dept Bot, Panama City, Panama. Smithsonian Trop Res Inst, Balboa, Panama. Calif State Univ San Bernardino, Dept Biol, San Bernardino, CA 92407 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Silvera, K (reprint author), Univ Florida, Dept Bot, 220 Bartram Hall,POB 118526, Gainesville, FL 32611 USA. NR 51 TC 21 Z9 24 U1 0 U2 11 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 2003 VL 19 BP 27 EP 34 DI 10.1017/S0266467403003043 PN 1 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 673XM UT WOS:000182606300004 ER PT J AU Zotz, G Vollrath, B AF Zotz, G Vollrath, B TI The epiphyte vegetation of the palm Socratea exorrhiza - correlations with tree size, tree age and bryophyte cover SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Araceae; Bromeliaceae; canopy dynamics; diversity; ferns; hemi-epiphytes; moss; Orchidaceae; vascular epiphytes ID VASCULAR EPIPHYTES; CLOUD FOREST; RAIN-FOREST; COSTA-RICA; SPATIAL-DISTRIBUTION; MONTANE FOREST; SUBSTRATE USE; CANOPY; GROWTH; MEXICO AB We conducted a survey of the. epiphyte flora growing on the stilt palm Socratea exorrhiza in a primary lowland rain forest in Panama by means of a canopy crane. For each palm in a 0.9-ha plot, we determined diameter at breast height, tree height, per cent bryophyte cover and the number, identity and attachment site of all vascular epiphytes. The 118 palm trees hosted a total of 701 epiphytes and hemi-epiphytes, belonging to 66 species. Trees were estimated to be c. 20 y old before colonization with vascular epiphytes began. Epiphyte species were highly clumped and segregated along the vertical axis of the trunk. Sequential colonization led to an increased number of species and individuals as the tree grows. Epiphytes were associated with bryophyte patches much more than expected by chance, but no species seemed to depend upon them for establishment. The influence of tree size, age and bryophyte cover on the composition of the epiphyte community are discussed. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. NR 37 TC 61 Z9 68 U1 4 U2 23 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 2003 VL 19 BP 81 EP 90 DI 10.1017/S0266467403003092 PN 1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 673XM UT WOS:000182606300009 ER PT J AU Albright, B Woodburne, MO Case, JA Chaney, DS AF Albright, Barry Woodburne, Michael O. Case, Judd A. Chaney, Dan S. TI A LEATHERBACK SEA TURTLE FROM THE EOCENE OF ANTARCTICA: IMPLICATIONS FOR THE ANTIQUITY OF GIGANTOTHERMY IN DERMOCHELYIDAE SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Albright, Barry] Museum Northern Arizona, Flagstaff, AZ USA. [Woodburne, Michael O.] Univ Calif Riverside, Riverside, CA 92521 USA. [Case, Judd A.] St Marys Coll, Moraga, CA 94575 USA. [Chaney, Dan S.] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 29A EP 29A PG 1 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800003 ER PT J AU Bolat, B Lucas, SG Emry, RJ AF Bolat, Bayshashov Lucas, Spencer G. Emry, Robert J. TI THE GIANT RHINOCEROS PARACERATHERIUM IN KAZAKSTAN SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Bolat, Bayshashov] Inst Zool, Dept Minist & Akad Sci, Alma Ata, Kazakhstan. [Lucas, Spencer G.] New Mexico Museum Nat Hist, Albuquerque, NM USA. [Emry, Robert J.] Smithsonian, Natl Museum Nat Hist, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 32A EP 32A PG 1 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800026 ER PT J AU Behrensmeyer, K Harmon, EH Kimbel, WH AF Behrensmeyer, Kay Harmon, Elizabeth H. Kimbel, William H. TI ENVIRONMENTAL CONTEXT AND TAPHONOMY OF THE FIRST FAMILY HOMINID LOCALITY, HADAR, ETHIOPIA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Behrensmeyer, Kay] Smithsonian Inst, Washington, DC 20560 USA. [Harmon, Elizabeth H.; Kimbel, William H.] Arizona State Univ, Inst Human Origins, Tempe, AZ USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 33A EP 33A PG 1 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800029 ER PT J AU Bobe, R AF Bobe, Rene TI PATTERNS OF DIVERSITY IN PLIOCENE AND PLEISTOCENE BOVIDS FROM THE TURKANA BASIN, KENYA AND ETHIOPIA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Bobe, Rene] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 35A EP 35A PG 1 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800041 ER PT J AU Carrano, M Sampson, SD AF Carrano, Matthew Sampson, Scott D. TI THE EVOLUTIONARY HISTORY OF BASAL THEROPOD DINOSAURS SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Carrano, Matthew] Smithsonian Inst, Washington, DC 20560 USA. [Carrano, Matthew; Sampson, Scott D.] Univ Utah, Museum Nat Hist, Salt Lake City, UT USA. RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 0 TC 2 Z9 2 U1 0 U2 0 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 38A EP 39A PG 2 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800065 ER PT J AU Head, J AF Head, Jason TI SNAKING THROUGH SHAPE-SPACE: GEOMETRIC MORPHOMETRIC APPROACHES TO TAXONOMY AND PHYLOGENY IN ERYCINE SNAKES SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Head, Jason] Smithsonian Inst, Washington, DC 20560 USA. [Head, Jason] Univ London, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 59A EP 59A PG 1 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800189 ER PT J AU Heaton, TH Grady, F AF Heaton, Timothy H. Grady, Frederick TI THE LATE PLEISTOCENE SEA BIRD FAUNA OF ON YOUR KNEES CAVE, SOUTHEAST ALASKA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Heaton, Timothy H.] Univ S Dakota, Vermillion, SD 57069 USA. [Grady, Frederick] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 2 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 60A EP 60A PG 1 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800192 ER PT J AU O'Keefe, R Carrano, M AF O'Keefe, Robin Carrano, Matthew TI SCALING AND ECOMORPHOLOGICAL TRENDS IN THE EVOLUTION OF THE PLESIOSAUR LOCOMOTOR SYSTEM SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [O'Keefe, Robin] New York Coll Osteopath Med, Old Westbury, NY USA. [Carrano, Matthew] Smithsonian Inst, Washington, DC 20560 USA. RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 0 TC 0 Z9 0 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 84A EP 84A PG 1 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800342 ER PT J AU Sampson, S Loewen, MA Farlow, JO Carrano, MT AF Sampson, Scott Loewen, Mark A. Farlow, James O. Carrano, Matthew T. TI ECOLOGICAL AND EVOLUTIONARY IMPLICATIONS OF GIGANTISM IN THEROPOD DINOSAURS SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Meeting Abstract C1 [Sampson, Scott; Loewen, Mark A.] Utah Museum Nat Hist, Salt Lake City, UT USA. [Farlow, James O.] Indiana Purdue Univ, Ft Wayne, IN USA. [Carrano, Matthew T.] Smithsonian Inst, Washington, DC 20560 USA. RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 0 TC 1 Z9 1 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2003 VL 23 SU 3 SI SI BP 92A EP 92A PG 1 WC Paleontology SC Paleontology GA V33OT UT WOS:000209028800391 ER PT J AU Helgen, KM Wilson, DE AF Helgen, KM Wilson, DE TI Taxonomic status and conservation relevance of the raccoons (Procyon spp.) of the West Indies SO JOURNAL OF ZOOLOGY LA English DT Article DE Bahamas; Barbados; Guadeloupe; Procyon gloveralleni; Procyon maynardi; Procyon minor ID SEA-TURTLE NESTS; ISLANDS; MAMMALS AB Raccoons Procyon spp. from New Providence Island in the Bahamas and from Barbados and Guadeloupe in the Lesser Antilles have traditionally been recognized as distinctive species endemic to their respective islands. All three of these 'species' currently possess official conservation status of high concern. Bahamian and Guadeloupean raccoons are recognized as endangered species by the World Conservation Union (IUCN), which also considers the Barbados raccoon to be a recently extinct West Indian mammal. However, historical, biogeographic, genetic, and morphological evidence demonstrate that all three West Indian raccoon populations are the result of human-sponsored introductions from the eastern U.S.A. that have occurred in the past few centuries. Accordingly, these animals should not be considered either conservation priorities or recent losses of biodiversity in the Caribbean. Instead, they may actually represent ecological threats to the insular ecosystems on their respective islands. Procyonid conservation goals must be re-examined and updated accordingly. C1 Harvard Univ, Museum Comparat Zool, Dept Mammal, Cambridge, MA 02138 USA. Univ Adelaide, Dept Environm Biol, Adelaide, SA 5005, Australia. Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. RP Helgen, KM (reprint author), S Australian Museum, North Terrace, Adelaide, SA 5000, Australia. EM kristofer.helgen@adelaide.edu.au NR 73 TC 12 Z9 17 U1 1 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0952-8369 EI 1469-7998 J9 J ZOOL JI J. Zool. PD JAN PY 2003 VL 259 BP 69 EP 76 DI 10.1017/S0952836902002972 PN 1 PG 8 WC Zoology SC Zoology GA 673XR UT WOS:000182606700009 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The emblem. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Kalfatovic, MR (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 JAN PY 2003 VL 128 IS 1 BP 102 EP + PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 670QZ UT WOS:000182421400079 ER PT J AU Schroll, S AF Schroll, S TI From Millet to Leger: Essays in social art history. 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 JAN PY 2003 VL 128 IS 1 BP 102 EP 102 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 670QZ UT WOS:000182421400074 ER PT J AU Neubauer, SC Anderson, IC AF Neubauer, SC Anderson, IC TI Transport of dissolved inorganic carbon from a tidal freshwater marsh to the York River estuary SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID ORGANIC-CARBON; INTERTIDAL MARSH; SOUTHEASTERN US; MASS-BALANCE; WATER MARSH; SALT-MARSH; METABOLISM; DIOXIDE; FLUX; ECOSYSTEM AB The cycling of dissolved inorganic carbon (DIC) and the role of tidal marshes in estuarine DIC dynamics were studied in a Virginia tidal freshwater marsh and adjacent estuary. DIC was measured over diurnal cycles in different seasons in a marsh tidal creek and at the junction of the creek with the adjacent Pamunkey River. In the creek, DIC concentrations around high tide were controlled by the same processes affecting whole-estuary DIC gradients. Near low tide, DIC concentrations were 1.5-5-fold enriched relative to high tide concentrations, indicating an input of DIC from the marsh. Similar patterns (although dampened in magnitude) were observed at the creek mouth and indicated that DIC was exported from the marsh. Marsh pore-water DIC concentrations were up to 5 mmol L-1 greater than those in the creek and suggested a significant input of sediment pore water to the creek. A model of tidal marsh DIC export showed that, on a seasonal basis, DIC export rates were influenced by water temperature. The composition of exported DIC averaged 19% dissolved CO2 and 81% HCO3- and CO32-. Although CO2 can be lost to the atmosphere during transit through the estuary DIC in the form of carbonate alkalinity is subject to export from the estuary to the coastal ocean. When extrapolated to an estuarywide scale, the export of marsh-derived DIC to the York River estuary explained a significant portion (47 +/- 23%) of excess DIC production (i.e., DIC in excess of that expected from conservative mixing between seawater and freshwater and equilibrium with the atmosphere) in this system. Therefore, CO2 supersaturation, by itself, does not indicate that an estuary is net heterotrophic. C1 Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. RP Neubauer, SC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Neubauer, Scott/A-3443-2011 OI Neubauer, Scott/0000-0001-8948-2832 NR 34 TC 39 Z9 41 U1 3 U2 18 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 0024-3590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD JAN PY 2003 VL 48 IS 1 BP 299 EP 307 PG 9 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 664FA UT WOS:000182050000028 ER PT B AU Whigham, DF Olmsted, I Cano, EC Curtis, AB AF Whigham, DF Olmsted, I Cano, EC Curtis, AB BE GomezPompa, A Allen, MF Fedick, SL JimenezOsornio, JJ TI Impacts of hurricanes on the forests of Quintana Roo, Yucatan Peninsula, Mexico SO LOWLAND MAYA AREA: THREE MILLENNIA AT THE HUMAN-WILDLAND INTERFACE LA English DT Proceedings Paper CT 21st Symposium in Plant Biology CY JAN 18-20, 2001 CL UNIV CALIF, RIVERSIDE DEPT BOTANY & PLANT SCI, RIVERSIDE, CA SP Univ Calif Riverside, Dean Coll Humanities & Sopcial Sci, Univ Calif Riverside, Dean Coll Nat & Agr Sci, Univ Calif Riverside, Ctr Conservat Biol, UC MEXUS HO UNIV CALIF, RIVERSIDE DEPT BOTANY & PLANT SCI ID LUQUILLO EXPERIMENTAL FOREST; DRY TROPICAL FOREST; PUERTO-RICO; SPECIES-DIVERSITY; RAIN-FOREST; DAMAGE; NICARAGUA; DISTURBANCE; RECOVERY; HUGO C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM whigham@serc.si.edu; edgarcabrera57@hotmail.com; abcwoods@pacinfo.com NR 55 TC 14 Z9 14 U1 0 U2 1 PU FOOD PRODUCTS PRESS PI BINGHAMTON PA 10 ALICE ST, BINGHAMTON, NY 13904-1580 USA BN 1-56022-971-3 PY 2003 BP 193 EP 213 PG 21 WC Archaeology; Area Studies; Environmental Sciences; Environmental Studies SC Archaeology; Area Studies; Environmental Sciences & Ecology GA BX82U UT WOS:000186576700010 ER PT S AU Fabbiano, G AF Fabbiano, G BE Buchner, J Pevtsov, AA TI First Chandra observations of galaxies SO MAGNETIC HELICITY AT THE SUN, IN SOLAR WIND AND MAGNETOSPHERES: VISTAS FROM X-RAY OBSERVATORIES SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT Conference on Magnetic Helicity at the Sun, in Solar Wind and Magnetospheres CY OCT 14-15, 2002 CL HOUSTON, TEXAS SP Comm Space Res ID ELLIPTIC GALAXIES; ANTENNAE GALAXIES; ROSAT; NGC-4038/4039; EMISSION; M82; M31 AB Chandra's unique combination of sub-arcsecond angular resolution and spectral resolution is very well suited to the study of complex X-ray emitting systems, such as galaxies. In this talk, I give an overview of very early results on galaxies, including examples of normal spirals, actively star-forming and interacting galaxies, and E and S0 galaxies. In all cases, we can easily discriminate between the emission from a population of individual X-rays sources, hot ISM components, and nuclear sources, when present. Highlights of these early results include the detection or very stringent limits on the X-ray emission of the very massive nuclear black holes present in bulges and early-type galaxies; the detection of super-luminous (super-Eddington) sources in actively star-forming galaxies, whose counterpart may be intermediate mass black holes (10-100s M-circle dot); the detection of the debated population of XRBs in E and S0 galaxies; and the detection of a whole range of features in the hot ISM of both late and early-type galaxies. Published by Elsevier Ltd on behalf of COSPAR. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 1 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2003 VL 32 IS 10 BP 2013 EP 2020 DI 10.1016/S0273-1177(03)00914-1 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Physics, Fluids & Plasmas SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences; Physics GA BY21S UT WOS:000188280800024 ER PT J AU Jiang, XL Wang, YX Hoffmann, RS AF Jiang, XL Wang, YX Hoffmann, RS TI A review of the systematics and distribution of Asiatic short-tailed shrews, genus Blarinella (Mammalia : Soricidae) SO MAMMALIAN BIOLOGY LA English DT Article DE Blarinella; taxonomy; multivariate analysis; distribution AB The systematics and distribution of Asiatic short-tailed shrews (genus Blarinella) are confused. In this study, a taxonomic revision of Blarinella is presented. We investigated a sample of 98 specimens, 84 of which had complete skulls that were subjected to multivariate and univariate analyses. The results show that three species of Blarinella can be recognized. The species Blarinella quadraticauda occurs in Baoxin, Wenchuan, Daofu, and other localities in western Sichuan. Blarinella griselda and B. wardi, usually placed as subspecies of B. quadraticauda, are recognized as two valid species. The former has a wide distribution from southern Gansu to southern Yunnan, and northwestern Yunnan to northwestern Hubei. The tatter is restricted in northern Burma and northwestern Yunnan. The range of B. quadraticauda does not overlap that of B. wardi, white the range of B. griselda partially overlaps that of B. wardi and probably includes the entire range of B. quadraticauda. C1 Chinese Acad Sci, Kunming Inst Zool, Kunming 650223, Yunnan, Peoples R China. Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, MRC 108, Washington, DC 20013 USA. RP Jiang, XL (reprint author), Chinese Acad Sci, Kunming Inst Zool, Kunming 650223, Yunnan, Peoples R China. NR 30 TC 5 Z9 9 U1 0 U2 4 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 1616-5047 J9 MAMM BIOL JI Mamm. Biol. PY 2003 VL 68 IS 4 BP 193 EP 204 DI 10.1078/1616-5047-00085 PG 12 WC Zoology SC Zoology GA 707EX UT WOS:000184497400001 ER PT J AU Smalley, GW Coats, DW Stoecker, DK AF Smalley, GW Coats, DW Stoecker, DK TI Feeding in the mixotrophic dinoflagellate Ceratium furca is influenced by intracellular nutrient concentrations SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE dinoflagellate mixotrophy; phagotrophy; nutrient limitation; photosynthesis; Ceratium furca ID PHOTOSYNTHETIC ENERGY-CONVERSION; PHAEODACTYLUM-TRICORNUTUM BOHLIN; ISOCHRYSIS-GALBANA HAPTOPHYCEAE; NITROGEN LIMITATION; MARINE-PHYTOPLANKTON; GYRODINIUM-GALATHEANUM; PLANKTONIC PROTISTS; LIGHT-INTENSITY; CHESAPEAKE-BAY; GROWTH-RATE AB In field populations of the mixotrophic dinoflagellate Ceratium furca, feeding on microzooplankton is commonly observed and is influenced by inorganic nutrient concentrations and ratios. Using batch and 'semi-continuous' laboratory cultures, we examined in more detail the nutrient conditions that trigger feeding in C. furca. Cultures were maintained at a range of nitrogen (N) and phosphorus (P) concentrations for 31 to 36 d. Several parameters were determined at regular intervals, including inorganic nutrient concentrations of the medium, C. furca abundance and size, cellular chlorophyll a (chl a), C, N, and P contents and densities, photosynthetic rates, and ingestion of ciliate prey. We detected significant differences between treatments in all cellular parameters measured. Most notably, feeding only occurred in cultures that had been growing under N- or P-deplete conditions for 11 to 16 d, whereas nutrient-replete cells did not ingest prey. Feeding increased markedly as cellular C:N:P ratios deviated farther from those found under optimum growth conditions. Specifically, feeding in P-deplete cultures increased at C:P ratios > 130 and at N:P ratios > 19, whereas N-deplete cultures required a C:N ratio of similar to10 and an N:P ratio < 7 to commence feeding. Growth and photosynthetic rates were reduced compared to those of nutrient-replete cells regardless of the limiting nutrient. In N-limited cultures, cell size and chl a density decreased compared to nutrient-replete cells, whereas the size of P-limited cells significantly increased. This change in average cell size was caused by the development of a bimodal size distribution under N- and P-reduced conditions, raising the possibility of sexual reproduction in C. furca. Changes in cellular parameters were reversible upon nutrient addition, and feeding decreased or ceased within hours to days. The findings presented here indicate that cellular nutrient quotas and ratios are more critical than absolute inorganic nutrient concentrations in regulating feeding behavior of C. furca. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Ctr Environm Sci, Horn Point Lab, Cambridge, MD 21613 USA. RP Coats, DW (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM coatsw@si.edu RI stoecker, diane/F-9341-2013 NR 43 TC 43 Z9 45 U1 1 U2 15 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2003 VL 262 BP 137 EP 151 DI 10.3354/meps262137 PG 15 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 751TG UT WOS:000187082600011 ER PT J AU Seitz, RD Marshall, LS Hines, AH Clark, KL AF Seitz, RD Marshall, LS Hines, AH Clark, KL TI Effects of hypoxia on predator-prey dynamics of the blue crab Callinectes sapidus and the Baltic clam Macoma balthica in Chesapeake Bay SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE hypoxia; dissolved oxygen; Callinectes sapidus; blue crab; Macoma balthica; Baltic clam; predator-prey; Chesapeake Bay; benthos ID DENSITY-DEPENDENT PREDATION; COMMUNITY REGULATION; BENTHIC COMMUNITIES; FORAGING BEHAVIOR; OXYGEN DEFICIENCY; DISSOLVED-OXYGEN; PERIODIC HYPOXIA; DEMERSAL FISH; BOTTOM FAUNA; EUTROPHICATION AB In general, hypoxia (< 2 mg O-2 l(-1)) is detrimental to marine food webs because of faunal declines associated with persistent, severely low oxygen. However, transfer of benthic production to higher trophic levels could be facilitated under hypoxia if infauna migrate to shallower burial depths, increasing their availability to predators. A series of outdoor mesocosm and laboratory experiments were conducted in 3 years (1999 to 200 1) to quantify the effects of hypoxia upon (1) predation by the blue crab Callinectes sapidus on the Baltic clam Macoma balthica, a biomass dominant in Chesapeake Bay, and (2) burial depth and survival of M, balthica. For the predation experiments, 12 M. balthica were transplanted into replicate 1200 1 mesocosms at 48 clams m(-2) under normoxia (>8 mg O-2 l(-1)) or low dissolved oxygen (low DO; <2 mg O-2 l(-1)) either without or with a male blue crab that was allowed 2 d to feed upon the clams. Predation-induced proportional mortality of clams was significantly lower under low DO than under normoxia in all 3 years. Thus, under short-term hypoxia, both crab feeding efficiency and trophic transfer from M balthica to blue crabs were reduced. Changes in clam burial depth due to oxygen levels was determined by establishing normoxic and low DO treatments in replicate 208 1 aquaria in 2 years. Burial depth after exposure to oxygen treatments for 48 h did not differ as a function of oxygen level. None of the clams died after 2 d of low DO, 27 % died after -6 d, and 90 % died after 21 d. Short-lived hypoxia therefore reduces the ability of crabs to forage upon clams efficiently and increases clam survival, whereas long-term hypoxia may increase the availability of clam prey to predators through mortality and movement to the surface. Thus, short-lived hypoxia is likely to reduce the transfer of benthic prey to higher trophic levels, although longer-term exposure may increase transfer. C1 Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. Morgan State Univ, Dept Biol, Baltimore, MD 21251 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Seitz, RD (reprint author), Coll William & Mary, Virginia Inst Marine Sci, POB 1346, Gloucester Point, VA 23062 USA. EM seitz@vims.edu NR 57 TC 48 Z9 49 U1 1 U2 30 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2003 VL 257 BP 179 EP 188 DI 10.3354/meps257179 PG 10 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 717BJ UT WOS:000185065500016 ER PT J AU Ritson-Williams, R Shjegstad, S Paul, V AF Ritson-Williams, R Shjegstad, S Paul, V TI Host specificity of four corallivorous Phestilla nudibranchs (Gastropoda : Opisthobranchia) SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Phestilla; host specialization; coral predators; larval metamorphosis ID SPECIALIST MARINE HERBIVORE; SEA SLUGS; CHEMICAL DEFENSES; ALDERIA-MODESTA; PLANT CHEMISTRY; SETTLEMENT CUES; LIFE-HISTORY; LARVAE; WATERBORNE; EVOLUTION AB Nudibranchs that exclusively eat scleractinian corals provide a rare opportunity to study specialist predation in the marine environment. To measure the diet breadth of 4 Phestilla species on Guam, we offered the nudibranchs different corals in choice and no-choice feeding assays. Larval preferences were determined by measuring the percent metamorphosis in response to different coral species. We compared the specificity of larval metamorphosis to adult feeding preferences. Phestilla sibogae ate a range of Porites species (Poritidae) in the field and would not eat other coral genera in the laboratory no-choice assays. Metamorphosis was approximately 90 % in response to 4 Porites spp. Phestilla minor was found on Porites lutea and Porites annae in the field. It preferred R annae over Porites cylindrica and P. (Synaraea) rus during the choice and no-choice assays. The highest rates of metamorphosis (approx. 80 %) were in response to P. lutea, P. annae, and P, cylindrica. Phestilla sp. 1 is morphologically similar to P. minor, but it eats different Porites species. It preferred P. (S.) rus, but would eat P. cylindrica during the no-choice assays. The highest rate of metamorphosis (approx. 80 %) was in response to P. (S.) rus. Phestilla sp. 2 is distinct from the other Phestilla species studied, as it is a specialist on corals in the genus Goniopora (Poritidae). It preferred G. fruticosa and also ate G. minor and G, lobata during the feeding assays. The highest rates of metamorphosis (approx. 60 %) were in response to G. fruticosa, G. minor, and G. lobata. This study documents a range of diet breadth among Phestilla species. Phestilla spp. larvae could distinguish between coral species within a host genus and showed a tendency to have high metamorphosis on their preferred hosts, but they also metamorphosed in response to non-food coral species. C1 Univ Guam, Marine Lab, Mangilao, GU 96923 USA. RP Ritson-Williams, R (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM williams@sms.si.edu NR 48 TC 14 Z9 14 U1 1 U2 7 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2003 VL 255 BP 207 EP 218 DI 10.3354/meps255207 PG 12 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 703FD UT WOS:000184268600017 ER PT J AU Collin, R AF Collin, R TI Worldwide patterns in mode of development in calyptraeid gastropods SO MARINE ECOLOGY PROGRESS SERIES LA English DT Review DE larvae; invertebrate development; Crepidula; Crucibulum; Calyptraea ID CREPIDULA-DILATATA GASTROPODA; MARINE BENTHIC INVERTEBRATES; EGG SIZE DISTRIBUTIONS; GENE-ENZYME VARIATION; LARVAL DEVELOPMENT; SEX-CHANGE; INTRACAPSULAR DEVELOPMENT; REPRODUCTIVE STRATEGIES; PROSOBRANCH GASTROPODS; POPULATION-STRUCTURE AB The mode of development in marine invertebrates is believed to have consequences for dispersal, gene flow, geographic range, and speciation and extinction rates. The factors responsible for among-species differences in mode of development are not well understood and patterns of variation in mode of development have not been documented for many groups. I present a compiled data set of developmental characters for 78 species of calyptraeid gastropods: 53 Crejoidula, 9 Calyptraea, 11 Crucibulum and 5 other species, Analysis of this data set shows that egg- and hatching-size distributions are strongly positively skewed. As expected, egg size correlates with hatching size and time to hatching in species without nurse eggs. Egg size is not significantly different between species with planktotrophic development and species with direct development with nurse eggs. Hatching size of direct developers with and without nurse eggs do not differ. Developmental characters do not vary with adult body size among species. There are strong latitudinal effects in mode of development, the frequency of planktotrophic species decreases with increasing latitude while the proportion of direct developers increases. There is also a striking latitudinal pattern in the occurrence of nurse eggs; almost all species with nurse eggs occur in the southern hemisphere. These latitudinal patterns do not appear to be explained by sea surface temperature. Comparisons with other gastropods for which similar compilations are available show a striking difference between heterobranchs (opisthobranchs and pulmonates) and caenogastropods in developmental characteristics. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, Miami, FL 34002 USA. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010 NR 106 TC 88 Z9 94 U1 0 U2 10 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2003 VL 247 BP 103 EP 122 DI 10.3354/meps247103 PG 20 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 651KH UT WOS:000181318700010 ER PT J AU Choat, JH Robertson, DR Ackerman, JL Posada, JM AF Choat, JH Robertson, DR Ackerman, JL Posada, JM TI An age-based demographic analysis of the Caribbean stoplight parrotfish Sparisoma viride SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE age-based demographic properties; growth; maximum age; scarids; otoliths; validation; von Bertalanffy parameters; geographical variation; fishing effects ID GREAT-BARRIER-REEF; CORAL-REEFS; MARINE RESERVE; HABITAT USE; GROWTH; FISHES; REPRODUCTION; VALIDATION; BIOMASS; SIZE AB The parrotfish Sparisoma viride is an abundant and ecologically important member of the tropical NW Atlantic reef fish fauna. Sagittal otoliths of 417 individuals were analysed to estimate age-based demographic variables at 4 localities (Lee Stocking Island, Barbados, Los Roques Archipelago and the San Blas Archipelago) spanning 14degrees of latitude. The sampling localities ranged from an area protected from trap- and net-based reef fisheries (Los Roques) to an area supporting a dense human population and sustained trapping and spearing for reef fishes including S. viride (Barbados). Examination of sectioned sagittal otoliths from each locality revealed regular increments in the sagittal matrix. A preliminary validation at San Blas was consistent with these increments being annual check marks. These increments provided estimates of age structure, maximum longevities and mortality rates for the 4 study populations of S. viride. Von Bertalanffy growth functions fitted to each size-at-age plot generated similar growth curves from 3 of these 4 localities. The exception was Lee Stocking, where fish grew faster and reached a substantially larger size than those from the other 3 localities. Further analysis of the growth curves demonstrated that the differences between Lee Stocking and the other localities were attributable to more rapid growth over the first 4 yr of life. Age-based growth curves derived from the Los Roques population were very similar to a size-based curve generated by an independent study on S. viride carried out in Bonaire, adjacent to Los Roques. Maximum longevities for all 4 of our populations varied from 7 to 9 yr. Mortality rates generated from catch curve analysis were also similar among localities and suggest that maximum life spans do not exceed 12 yr. This result differs from that obtained at Bonaire, where repeated censuses of tagged fish suggest 30 yr maximum longevity. Abundances of S. viride varied 3-fold among localities, being highest at Los Roques (protected from reef fishing), lowest at Barbados (high fishing) and Lee Stocking (low fishing). Thus our age-based study suggests that S. viride is a relatively short-lived fish with consistent demographic parameters over a range of localities, latitudes and fishing intensities. C1 James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. Smithsonian Trop Res Inst, APO, AA 34002 USA. Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. RP Choat, JH (reprint author), James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. EM john.choat@jcu.edu.au NR 63 TC 51 Z9 51 U1 4 U2 22 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2003 VL 246 BP 265 EP 277 DI 10.3354/meps246265 PG 13 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 647GM UT WOS:000181085100021 ER PT J AU Estes, JA Hatfield, BB Ralls, K Ames, J AF Estes, JA Hatfield, BB Ralls, K Ames, J TI Causes of mortality in California sea otters during periods of population growth and decline SO MARINE MAMMAL SCIENCE LA English DT Article DE California sea otter; Enhydra lutris nereis; mortality; population trends; salvage of beach-cast carcasses ID PATTERNS AB Elevated mortality appears to be the main reason for both sluggish growth and periods of decline in the threatened California sea otter population. We assessed causes of mortality from salvage records of 3,105 beach-cast carcasses recovered from 1968 through 1999, contrasting two periods of growth with two periods of decline. Overall, an estimated 40%-60% of the deaths were not recovered and 70% of the recovered carcasses died from unknown causes. Nonetheless, several common patterns were evident in the salvage records during the periods of population decline. These included greater percentages of (1) prime age animals (3-10 yr), (2) carcasses killed by great white shark attacks, (3) carcasses recovered in spring and summer, and (4) carcasses for which the cause of death was unknown. Neither sex composition nor the proportion of carcasses dying of infectious disease varied consistently between periods of population increase and decline. The population decline from 1976 to 1984 was likely due to incidental mortality in a set-net fishery, and the decline from 1995 to 1999 may be related to a developing live-fish fishery. Long-term trends unrelated to periods of growth and decline included a decrease in per capita pup production and mass/length ratios of adult carcasses over the 31-yr study. The generally high proportion of deaths from infectious disease suggests that this factor has contributed to the chronically sluggish growth rate of the California sea otter population. C1 Univ Calif Santa Cruz, US Geol Survey, Santa Cruz, CA 95060 USA. Univ Calif Santa Cruz, Ctr Ocean Hlth, Santa Cruz, CA 95060 USA. US Geol Survey, San Simeon, CA 93452 USA. Smithsonian Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Calif Dept Fish & Game, Santa Cruz, CA 95060 USA. RP Estes, JA (reprint author), Univ Calif Santa Cruz, US Geol Survey, 100 Shafter Rd, Santa Cruz, CA 95060 USA. NR 21 TC 34 Z9 35 U1 3 U2 30 PU SOC MARINE MAMMALOGY PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JAN PY 2003 VL 19 IS 1 BP 198 EP 216 DI 10.1111/j.1748-7692.2003.tb01102.x PG 19 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 631ZQ UT WOS:000180198700014 ER PT B AU Monnier, JD Tuthill, PG Danchi, WC Richards, A AF Monnier, JD Tuthill, PG Danchi, WC Richards, A BE Nakada, Y Honma, M Seki, M TI High-resolution imaging of dust shells - Asymmetries and temporal evolution SO MASS-LOSING PULSATING STARS AND THEIR CIRCUMSTELLAR MATTER: OBSERVATIONS AND THEORY SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Workshop on Mass-Losing Pulsating Stars and Their Circumstellar Matter CY MAY 13-16, 2002 CL SENDAI, JAPAN SP Commemorat Assoc Japan World Exposit 1970, Saito Gratitude Fdn, Sendai Tourism & Convent Bur, Minist Educ, Culture, Sports, Sci & Technol ID VY-CANIS-MAJORIS; SPECKLE-MASKING INTERFEROMETRY; PLANETARY-NEBULA; PROPER MOTIONS; IRC+10216; TELESCOPE; STARS; ENVELOPE AB Advances in high-resolution imaging at visible, infrared, and radio wavelengths have allowed the circumstellar envelopes of evolved stars to be probed in unprecedented detail. While adequate to explain broadband spectral energy distributions, simplistic mass-loss scenarios (assuming spherical symmetry and continuous dust formation) have been shown to be grossly inadequate to understand the clumpy and often asymmetric dust shells recently revealed. In this paper, we will highlight a few sources that illustrate qualitatively new mass-loss phenomena, including the presence of circumstellar "disks" and evidence for sporadic, asymmetric mass ejections. Perhaps important physics is still missing from our picture of mass-loss on the AGB, for instance the effects of magnetic fields or large-scale convective motions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Monnier, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-1162-8 J9 ASTROPHYS SPACE SC L PY 2003 VL 283 BP 165 EP 172 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW92J UT WOS:000183622800033 ER PT B AU Reid, MJ Menten, KM AF Reid, MJ Menten, KM BE Nakada, Y Honma, M Seki, M TI Radio photospheres: Imaging and light curves SO MASS-LOSING PULSATING STARS AND THEIR CIRCUMSTELLAR MATTER: OBSERVATIONS AND THEORY SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Workshop on Mass-Losing Pulsating Stars and Their Circumstellar Matter CY MAY 13-16, 2002 CL SENDAI, JAPAN SP Commemorat Assoc Japan World Exposit 1970, Saito Gratitude Fdn, Sendai Tourism & Convent Bur, Minist Educ, Culture, Sports, Sci & Technol DE Mira variables; light curves; shocks; masers ID PERIOD VARIABLE-STARS AB Radio continuum observations of a sample of oxygen-rich Miras indicate temperatures and densities at radii near 2 R-* average approximate to 1500 K and similar to10(-12) gm cm(-3). The nearly constant radio light curves rule out strong shocks in this region, and SiO maser proper motions indicate convective-like motions with speeds of 4 km s(-1). The large amplitudes of visual light curves can be explained by the variable formation of molecular oxides (i.e., TiO). Simple models can reproduce the visual light curves and these models confirm the densities and low temperatures derived from the radio observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-1162-8 J9 ASTROPHYS SPACE SC L PY 2003 VL 283 BP 283 EP 290 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW92J UT WOS:000183622800066 ER PT B AU Shinnaga, H Claussen, MJ Lim, J Trung, DV Tsuboi, M AF Shinnaga, H Claussen, MJ Lim, J Trung, DV Tsuboi, M BE Nakada, Y Honma, M Seki, M TI Unveiling the molecular bipolar outflow of the peculiar red supergiant VY Canis Majoris SO MASS-LOSING PULSATING STARS AND THEIR CIRCUMSTELLAR MATTER: OBSERVATIONS AND THEORY SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Workshop on Mass-Losing Pulsating Stars and Their Circumstellar Matter CY MAY 13-16, 2002 CL SENDAI, JAPAN SP Commemorat Assoc Japan World Exposit 1970, Saito Gratitude Fdn, Sendai Tourism & Convent Bur, Minist Educ, Culture, Sports, Sci & Technol DE circurnstellar matter; masers; polarization; stars : individual (VY Canis Majoris); techniques : polarimetric ID INFRARED POLARIZATION; DUST SHELLS; STARS; MASERS AB We carried out polarimetric spectral-line imaging of the molecular outflow of the peculiar red supergiant VY Canis Majoris in SiO J = 1 - 0 line in the ground vibrational state, which contains highly linearly-polarized velocity components, using the Very Large Array. We succeeded in unveiling the highly linearly polarized bipolar outflow for the first time at subarcsecond spatial resolution. The results clearly show that the direction of linear polarization of the brightest maser components is parallel to the outflow axis. The results strongly suggest that the linear polarization of the SiO maser is closely related to the outflow phenomena of the star. Furthermore, the results indicate that the linear polarization observed in the optical and infrared also occur due to the outflow phenomena. C1 Harvard Smithsonian Ctr Astrophys, Submilimeter Array, Hilo, HI 96721 USA. RP Shinnaga, H (reprint author), Harvard Smithsonian Ctr Astrophys, Submilimeter Array, POB 824, Hilo, HI 96721 USA. NR 15 TC 7 Z9 7 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-1162-8 J9 ASTROPHYS SPACE SC L PY 2003 VL 283 BP 393 EP 396 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW92J UT WOS:000183622800089 ER PT B AU Pahre, MA Kochanek, CS Falco, EE Huchra, JP AF Pahre, MA Kochanek, CS Falco, EE Huchra, JP BE Bender, T Renzini, A TI The 2MASS luminosity, velocity, and mass functions of galaxies SO MASS OF GALAXIES AT LOW AND HIGH REDSHIFT SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT Workshop on the Mass of Galaxies at Low and High Redshift CY OCT 24-26, 2001 CL VENICE INT UNIV, VENICE, ITALY SP European SO Observ, Univ Sternwarte Munchen HO VENICE INT UNIV ID REDSHIFT SURVEY AB The velocity function (VF) of galaxies is analogous to the luminosity function (LF), but a more direct tool for comparing observations and theory. The 2MASS LF is calculated here for a local sample of similar to 4000 galaxies, and the VF is derived from a similar to 1000 galaxy subsample drawn from it. The observed VF follows a Schechter functional form. All current analytical, semi-analytical, and numerical galaxy formation models predict power-law (or nearly so) shapes for the VF, and hence cannot reproduce the observations. It remains an open challenge for any galaxy formation model to explain the observed VF. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pahre, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-00205-7 J9 ESO ASTROPHY SYMP PY 2003 BP 32 EP 38 DI 10.1007/10899892_9 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW39D UT WOS:000181848400009 ER PT B AU Kochanek, CS Dalal, N AF Kochanek, CS Dalal, N BE Bender, T Renzini, A TI Detection of CDM substructure SO MASS OF GALAXIES AT LOW AND HIGH REDSHIFT SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT Workshop on the Mass of Galaxies at Low and High Redshift CY OCT 24-26, 2001 CL VENICE INT UNIV, VENICE, ITALY SP European SO Observ, Univ Sternwarte Munchen HO VENICE INT UNIV ID DARK-MATTER; GALACTIC SATELLITES; MODELS; LENS AB The properties of multiple image gravitational lenses require a fractional surface mass density in satellites of f(sat) = 0.02 (0.006 less than or similar to f(sat) less than or similar to 0.07 at 90% confidence) that is consistent with the expectations for CDM. The characteristic satellite mass scale, 10(6)-10(9)M(circle dot), is also consistent with the expectations for CDM. The agreement between the observed and expected density of CDM substructure shows that most low mass galactic satellites fail to form stars, and this absence of star formation explains the discrepancy between the number of observed Galactic satellites and CDM predictions rather than any modification to the CDM theory such as self-interacting dark matter or a warm dark matter component. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA. RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02420 USA. NR 20 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-00205-7 J9 ESO ASTROPHY SYMP PY 2003 BP 178 EP 183 DI 10.1007/10899892_44 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW39D UT WOS:000181848400044 ER PT B AU Markevitch, M Vikhlinin, A Forman, WR AF Markevitch, M Vikhlinin, A Forman, WR BE Bowyer, S Hwang, CY TI A high resolution picture of the intracluster gas SO MATTER AND ENERGY IN CLUSTERS OF GALAXIES, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Matter and Energy in Clusters of Galaxies CY APR 23-27, 2002 CL NATL CENT UNIV, CHUNGLI, TAIWAN SP Natl Sci Council, Chinese Astron Soc Taiwan HO NATL CENT UNIV ID RAY-EMITTING GAS; CHANDRA OBSERVATION; GALAXY CLUSTERS; COOLING FLOWS; INTERGALACTIC MEDIUM; THERMAL CONDUCTION; MAGNETIC-FIELD; RADIO HALOS; COLD-FRONT; HYDRA-A AB Chandra has significantly advanced our knowledge of the processes in the intracluster gas. The discovery of remarkably regular "cold fronts", or contact discontinuities, in merging clusters showed that gas dynamic instabilities at the boundaries between the moving gases are often suppressed, most likely by specially structured magnetic fields. Cold fronts are not limited to mergers-Chandra observed them in the cores of more than 2/3 of the cooling flow clusters, where they often divide the cool central and the hotter ambient gas phases. The natural state of the low-entropy central gas in clusters thus appears to be to slosh subsonically in the central potential well, with several interesting implications. Hydrostatic equilibrium is not reached and the hydrostatic total mass estimates cannot be valid at small radii (r less than or similar to 100 kpc). The kinetic energy dissipated by the sloshing gas may be sufficient to compensate for radiative cooling. In the absence of a recent merger, the cause of such sloshing is unclear. It might be related to the mechanical energy generated by the central AGN, evidence of which (the bubbles) is also observed by Chandra in a large fraction of the cooling flow clusters. Heat conduction across cold fronts is suppressed completely. In the bulk of the gas, it is reduced by a factor of > 10 or more relative to the classic value, as shown by merger temperature maps. A spatial correlation between the gas temperature maps and the radio halo maps is observed in several mergers, which may provide clues for the relativistic particle acceleration mechanisms. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Markevitch, M (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. OI Forman, William/0000-0002-9478-1682 NR 37 TC 46 Z9 46 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-149-4 J9 ASTR SOC P PY 2003 VL 301 BP 37 EP 51 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX73Z UT WOS:000186286300003 ER PT B AU Vikhlinin, A Markevitch, M AF Vikhlinin, A Markevitch, M BE Bowyer, S Hwang, CY TI A cold front in A3667: Hydrodynamics and magnetic field in the intracluster medium SO MATTER AND ENERGY IN CLUSTERS OF GALAXIES, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Matter and Energy in Clusters of Galaxies CY APR 23-27, 2002 CL NATL CENT UNIV, CHUNGLI, TAIWAN SP Natl Sci Council, Chinese Astron Soc Taiwan HO NATL CENT UNIV ID KELVIN-HELMHOLTZ INSTABILITY; CLUSTER; WEAK; WIND AB This conference presentation discusses a Chandra observation of the cold front in Abell 3667. We first review our earlier results which include a measurement of the front velocity, M approximate to 1, using the ratio of exterior and interior gas pressures; observations of the hydrodynamic effects expected for a transonic front motion (weak bow shock and gas compression near the leading edge of the front); direct observation of the suppressed diffusion across the front, and estimate of the magnetic field strength near the front from suppression of the Kelvin-Helmholtz instabilities. The new results include using the 2-dimensional brightness distribution inside the cold front (a) to show that the front is stable and (b) to map the mass distribution in the gas cloud. This analysis confirms the existence of a dark matter subcluster traveling with the front. We also fix an algebraic error in our published calculations for the growth rate of the KH instability and discuss an additional effect which could stabilize the front against the small-scale perturbations. These updates only strengthen our conclusions regarding the importance of the magnetic fields for the front dynamics. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Vikhlinin, A (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 15 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-149-4 J9 ASTR SOC P PY 2003 VL 301 BP 63 EP 72 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX73Z UT WOS:000186286300005 ER PT B AU Harris, DE Krawczynski, H AF Harris, DE Krawczynski, H BE Bowyer, S Hwang, CY TI Pressure balance between thermal and non-thermal plasmas in the 3C129 cluster SO MATTER AND ENERGY IN CLUSTERS OF GALAXIES, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Matter and Energy in Clusters of Galaxies CY APR 23-27, 2002 CL NATL CENT UNIV, CHUNGLI, TAIWAN SP Natl Sci Council, Chinese Astron Soc Taiwan HO NATL CENT UNIV ID CYGNUS-A; 3C 129; GAS; 3C-129; GALAXY AB With new Chandra observations of the cluster containing the two radio galaxies 3C129 and 3C129.1, we have made a fit to the X-ray surface brightness to obtain thermal pressures. VLA data at 1.4 GHz have been obtained to complement previous maps at 0.33 GHz (Lane et al. 2002) and at 5 and 8 GHz (Taylor et al. 2001). From these radio data, we are able to derive the minimum non-thermal pressure of various emitting volumes along the tail of 3C129 and in the lobes of 3C129.1. Under the assumption that the non-thermal plasma excludes significant thermal plasma, we may expect pressure balance for most features since ram pressure should be important only close to the cores of the galaxies. Since we find that the minimum non-thermal pressures are generally only a factor of a few below estimates of the ambient thermal pressure, we conclude that it is unlikely that relativistic protons contribute significantly to the total pressure. Reasonable contributions from low energy electrons and filling factors in the range 0.1 to 1 suffice to achieve pressure balance. Although we do not find strong signatures for the exclusion of hot gas from the radio structures, we find soft features near the cores of both galaxies suggestive of cool gas stripping and hard features associated with radio jets and possibly a leading bow shock. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Harris, DE (reprint author), Smithsonian Astrophys Observ, 60 Gdn St, Cambridge, MA 02138 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-149-4 J9 ASTR SOC P PY 2003 VL 301 BP 405 EP 416 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX73Z UT WOS:000186286300031 ER PT S AU Kurucz, RL AF Kurucz, Robert L. BA Piskunov, N BF Piskunov, N BE Weiss, WW Gray, DF TI A few things we do not know about stars and model atmospheres SO Modelling of Stellar Atmospheres SE IAU SYMPOSIA LA English DT Proceedings Paper CT 210th IAU Symposium on Modelling of Stellar Atmospheres CY JUN 17-21, 2002 CL Uppsala Univ, Uppsala, SWEDEN SP Int Astron Union HO Uppsala Univ DE model atmospheres; convection; microturbulent velocity; spectroscopy; solar spectra; stellar spectra; abundances; solar abundances; atomic line data; molecular line data; Cepheids AB A similar presentation has been published in the volume New Quests in Stellar Astrophysics: The Link between Stars and Cosmology Astrophysics and Space Science Library, vol. 274 (eds. M. Chavez, A. Bressan, A. Buzzoni, and D. Mayya) Dordrecht: Kluwer, pp. 1-10, 2002. Here I quote the abstract and list only the section headings. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurucz, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 8 Z9 8 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-160-5 J9 IAU SYMP PY 2003 VL 210 BP 45 EP 46 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFN75 UT WOS:000243352400004 ER PT J AU Schroll, S AF Schroll, S TI The unmaking of fascist aesthetics SO MODERNISM-MODERNITY LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Schroll, S (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 1071-6068 J9 MODERNISM-MODERNITY JI Mod.-Mod. PD JAN PY 2003 VL 10 IS 1 BP 209 EP 210 DI 10.1353/mod.2003.0027 PG 2 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 646RR UT WOS:000181048500025 ER PT J AU Balakrishnan, CN Monfort, SL Gaur, A Sing, L Sorenson, MD AF Balakrishnan, CN Monfort, SL Gaur, A Sing, L Sorenson, MD TI Phylogeography and conservation genetics of Eld's deer (Cervus eldi) SO MOLECULAR ECOLOGY LA English DT Article DE Cervus eldi; conservation genetics; control region; endangered species; mitochondrial DNA; phylogeography ID POPULATIONS; RESTORATION; SEQUENCES; BIOLOGY; UNITS AB Eld's deer (Cervus eldi) is a highly endangered cervid, distributed historically throughout much of South Asia and Indochina. We analysed variation in the mitochondrial DNA (mtDNA) control region for representatives of all three Eld's deer subspecies to gain a better understanding of the genetic population structure and evolutionary history of this species. A phylogeny of mtDNA haplotypes indicates that the critically endangered and ecologically divergent C. eldi eldi is related more closely to C. e. thamin than to C. e. siamensis, a result that is consistent with biogeographic considerations. The results also suggest a strong degree of phylogeographic structure both between subspecies and among populations within subspecies, suggesting that dispersal of individuals between populations has been very limited historically. Haplotype diversity was relatively high for two of the three subspecies (thamin and siamensis), indicating that recent population declines have not yet substantially eroded genetic diversity. In contrast, we found no haplotype variation within C. eldi eldi or the Hainan Island population of C. eldi siamensis, two populations which are known to have suffered severe population bottlenecks. We also compared levels of haplotype and nucleotide diversity in an unmanaged captive population, a managed captive population and a relatively healthy wild population. Diversity indices were higher in the latter two, suggesting the efficacy of well-designed breeding programmes for maintaining genetic diversity in captivity. Based on significant genetic differentiation among Eld's deer subspecies, we recommend the continued management of this species in three distinct evolutionarily significant units (ESUs). Where possible, it may be advisable to translocate individuals between isolated populations within a subspecies to maintain levels of genetic variation in remaining Eld's deer populations. C1 Boston Univ, Dept Biol, Boston, MA 02215 USA. Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Ctr Cellular & Mol Biol, Hyderabad 500007, Andhra Pradesh, India. RP Balakrishnan, CN (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM cbala@bu.edu RI Sorenson, Michael/D-8065-2011; Balakrishnan, Christopher/A-3043-2014 OI Sorenson, Michael/0000-0001-5375-2917; Balakrishnan, Christopher/0000-0002-0788-0659 NR 46 TC 42 Z9 56 U1 3 U2 8 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 JAN PY 2003 VL 12 IS 1 BP 1 EP 10 DI 10.1046/j.1365-294X.2003.01751.x PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 638KV UT WOS:000180570900001 PM 12492873 ER PT J AU Blum, MJ Bermingham, E Dasmahapatra, K AF Blum, MJ Bermingham, E Dasmahapatra, K TI A molecular phylogeny of the neotropical butterfly genus Anartia (Lepidoptera : Nymphalidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID PHOSPHATE ISOMERASE GENE; DNA-SEQUENCE DATA; MITOCHONDRIAL-DNA; EVOLUTION; PATTERNS; MODEL; SUBSTITUTION; BIOGEOGRAPHY; TOPOLOGIES; SPECIATION AB While Anartia butterflies have served as model organisms for research on the genetics of speciation, no phylogeny has been published to describe interspecific relationships. Here, we present a molecular phylogenetic analysis of Anartia species relationships, using both mitochondrial and nuclear genes. Analyses of both data sets confirm earlier predictions of sister species pairings based primarily on genital morphology. Yet both the mitochondrial and nuclear gene phylogenies demonstrate that Anartia jatrophae is not sister to all other Anartia species, but rather that it is sister to the Anartia fatima-Anartia amathea lineage. Traditional biogeographic c explanations for speciation across the genus relied on A. jatrophae being sister to its congeners. These explanations invoked allopatric divergence of sister species pairs and multiple sympatric speciation events to explain why A. jatrophae flies alongside all its congeners. The molecular phylogenies are more consistent with lineage divergence due to vicariance, and range expansion of A. jatrophae to explain its sympatry with congeners. Further interpretations of the tree topologies also suggest how morphological evolution and eco-geographic adaptation may have set species range boundaries. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Duke Univ, Dept Biol, Durham, NC 27705 USA. Smithsonian Trop Res Inst, Naos Isl Mol Labs, Unit 0948, APO, AA 34002 USA. UCL, Galton Lab, Dept Biol, London NW1 2HE, England. RP Blum, MJ (reprint author), Duke Univ, Dept Biol, Durham, NC 27705 USA. EM mjblum@duke.edu NR 35 TC 18 Z9 23 U1 0 U2 5 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 JAN PY 2003 VL 26 IS 1 BP 46 EP 55 AR PII S1055-7903(02)00291-9 DI 10.1016/S1055-7903(02)00291-9 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 634GA UT WOS:000180330600006 PM 12470937 ER PT J AU Cortes-Ortiz, L Bermingham, E Rico, C Rodriguez-Luna, E Sampaio, I Ruiz-Garcia, M AF Cortes-Ortiz, L Bermingham, E Rico, C Rodriguez-Luna, E Sampaio, I Ruiz-Garcia, M TI Molecular systematics and biogeography of the Neotropical monkey genus, Alouatta SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Review DE mitochondrial DNA; Andes mountains; Panama Isthmus; riverine barriers; calmodulin; recombination activating gene 1; Ateles; Brachyteles; molecular clock ID MITOCHONDRIAL-DNA SEQUENCES; RED HOWLER MONKEY; WORLD MONKEYS; PHYLOGENETIC-RELATIONSHIPS; DISPERSAL PATTERNS; RIVERINE BARRIERS; CYTOCHROME-B; PRIMATES; PLATYRRHINI; NUCLEAR AB We take advantage of the broad distribution of howler monkeys from Mexico to Argentina to provide a historical biogeographical analysis on a regional scale that encompasses the entire Neotropics. The phylogenetic relationships among 9 of the 10 recognized Alouatta species were inferred using three mitochondrial and two nuclear genes. The nuclear gene regions provided no phylogenetic resolution among howler monkey species, and were characterized by very low levels of sequence divergence between Alouatta and the Ateles outgroup. The mtDNA genes, on the other hand, produced a well-resolved phylogeny, which indicated that the earliest split among howler monkeys separated cis- and trans-Andean clades. Eight monophyletic mtDNA haplotype clades were identified, representing six named species in South America, including Alouatta seniculus, Alouatta sara, Alouatta macconelli, Alouatta caraya, Alouatta belzebul, and Alouatta guariba, and two in Mesoamerica, Alouatta pigra and Alouatta palliata. Molecular clock-based estimates of branching times indicated that contemporary howler monkey species originated in the late Miocene and Pliocene, not the Pleistocene. The causes of Alouatta diversification were more difficult to pin down, although we posit that the initial cis-, trans-Andean split in the genus was caused by the late Miocene completion of the northern Andes. Riverine barriers to dispersal and putative forest refuges can neither be discounted nor distinguished as causes of speciation in many cases, and one, the other or both have likely played a role in the diversification of South American howler monkeys. Finally, we estimated the separation of Mesoamerican A. pigra and A. palliata at 3 Ma, which corresponds to the completion date of the Panama Isthmus promoting a role for this earth history event in the speciation of Central American howler monkeys. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. Smithsonian Trop Res Inst, Naos Labs, Unit 0948, APO, AA 34002 USA. Univ Veracruzana, Inst Neuroetol, Jalapa, Veracruz, Mexico. Fed Univ Para, BR-66059 Belem, Para, Brazil. Pontificia Univ Javeriana, Bogota, Colombia. RP Cortes-Ortiz, L (reprint author), Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. RI Rico, Ciro/K-5725-2015; CSIC, EBD Donana/C-4157-2011 OI Rico, Ciro/0000-0002-0822-336X; CSIC, EBD Donana/0000-0003-4318-6602 NR 112 TC 144 Z9 155 U1 5 U2 55 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 JAN PY 2003 VL 26 IS 1 BP 64 EP 81 AR PII S1055-7903(02)00308-1 DI 10.1016/S1055-7903(02)00308-1 PG 18 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 634GA UT WOS:000180330600008 PM 12470939 ER PT J AU McCarthy, MC Gottlieb, CA Thaddeus, P AF McCarthy, MC Gottlieb, CA Thaddeus, P TI Silicon molecules in space and in the laboratory SO MOLECULAR PHYSICS LA English DT Article ID TRIPLET GROUND-STATES; RHOMBOIDAL SIC3; THEORETICAL PREDICTIONS; ASTRONOMICAL DETECTION; ROTATIONAL SPECTRUM; SI2HN N=0-6; IRC +10216; SPECTROSCOPY; IRC+10216; RESOLUTION AB Despite the highly non-volatile nature of Si, silicon bearing molecules are a significant trace constituent of the gas associated with late-type stars and star forming regions, representing nearly 10% of the molecular species that have been identified in space. The early astronomical detection of SiO and its remarkable maser emission stimulated laboratory studies of other small silicon species that were crucial to the astronomical identifications. Although the pace of this laboratory work until recently has been slow, the application of Fourier transform microwave spectroscopy to supersonic molecular beams has overcome many experimental difficulties, yielding the detection of more than 20 new silicon chains and rings of astronomical interest during the past three years. Three of these, the rhomboidal ring SiC3 and the isovalent linear molecules SiCN and SiNC, have now been found in space, and with dedicated searches other recently discovered silicon molecules may soon be found. A number of exotic silicon molecules of astronomical and chemical interest should be amenable to laboratory detection with present techniques. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Thaddeus, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pthaddeus@cfa.harvard.edu OI McCarthy, Michael/0000-0001-9142-0008 NR 61 TC 76 Z9 77 U1 0 U2 8 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 J9 MOL PHYS JI Mol. Phys. PY 2003 VL 101 IS 4-5 BP 697 EP 704 DI 10.1080/0026897021000035197 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 657RR UT WOS:000181680600019 ER PT J AU Hardcastle, MJ Worrall, DM Birkinshaw, M Canosa, CM AF Hardcastle, MJ Worrall, DM Birkinshaw, M Canosa, CM TI Unifying B2 radio galaxies with BL Lacertae objects SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; BL Lacertae objects : general; galaxies : jets; X-rays : galaxies ID RILEY-I GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; ALTERED LUMINOSITY FUNCTIONS; TELESCOPE IMAGING SURVEY; X-RAY OBSERVATIONS; COMPLETE SAMPLE; PARENT POPULATION; RELATIVISTIC JETS; VLBI OBSERVATIONS; VLA OBSERVATIONS AB In an earlier paper we presented nuclear X-ray flux densities, measured with ROSAT, for the B2 bright sample of nearby low-luminosity radio galaxies. In this paper we construct a nuclear X-ray luminosity function for the B2 radio galaxies, and discuss the consequences of our results for models in which such radio galaxies are the parent population of BL Lacertae (BL Lac) objects. Based on our observations of the B2 sample, we use Monte Carlo techniques to simulate samples of beamed radio galaxies, and use the selection criteria of existing samples of BL Lac objects to compare our simulated results to what is observed. We find that previous analytical results are not applicable since the BL Lac samples are selected on beamed flux density. A simple model in which BL Lacs are the moderately beamed (gammasimilar to 3) counterparts of radio galaxies, with some random dispersion (similar to0.4 decades) in the intrinsic radio-X-ray relationship, can reproduce many of the features of the radio-selected and X-ray-selected BL Lac samples, including their radio and X-ray luminosity functions and the distributions of their radio-to-X-ray spectral indices. In contrast, models in which the X-ray and radio emission have systematically different beaming parameters cannot reproduce important features of the radio-galaxy and BL Lac populations, and recently proposed models in which the radio-to-X-ray spectral index is a function of source luminosity cannot in themselves account for the differences in the slopes of the radio- and X-ray-selected BL Lac luminosity functions. The redshift distribution and number counts of the X-ray-selected Einstein Medium Sensitivity Survey (EMSS) sample are well reproduced by our best models, supporting a picture in which these objects are beamed Fanaroff-Riley type I radio galaxies with intrinsic luminosities similar to those of the B2 sample. However, we cannot match the redshift distribution of the radio-selected 1-Jy sample, and it is likely that a population of Fanaroff-Riley type II radio galaxies is responsible for the high-redshift objects in this sample, in agreement with previously reported results on the sample's radio and optical emission-line properties. 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. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 71 TC 23 Z9 23 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2003 VL 338 IS 1 BP 176 EP 188 DI 10.1046/j.1365-8711.2003.06039.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627CT UT WOS:000179912000021 ER PT J AU Weil, SE AF Weil, SE TI 5 meditations - The museum, unlike beauty, can never be its own excuse for being (Some original thoughts) SO MUSEUM NEWS LA English DT Article C1 Smithsonian Inst, Ctr Educ & Museum Studies, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 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 JAN-FEB PY 2003 VL 82 IS 1 BP 26 EP + PG 0 WC Art SC Art GA 632CN UT WOS:000180206300027 ER PT B AU Edmonds, PD AF Edmonds, PD BE Piotto, G Meylan, G Djougovski, SG Riello, M TI Recent breakthroughs in detecting neutron star binaries in globular clusters SO NEW HORIZONS IN GLOBULAR CLUSTER ASTRONOMY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on New Horizons in Globular Cluster Astronomy CY JUN 24-28, 2002 CL UNIV PADOVA, PADUA, ITALY SP Inst Nazl Astrofis, Space Telescope Sci Inst, Alenia Spazio SpA, Silicon Graphics, X Technologies HO UNIV PADOVA ID X-RAY BINARY; MILLISECOND PULSARS; OPTICAL COUNTERPART; 47 TUCANAE; 47-TUCANAE; COMPANION; NGC-6397; LUMINOSITY; DISCOVERY; NGC-6652 AB Binary stars have long been considered to play a crucial role in globular cluster evolution, and offer the advantages of studying systems at the same, well-determined distances. However, early search attempts were consistently thwarted by crowding (particularly in the optical) and initial detections were limited to small numbers of low-mass X-ray binaries (LMXBs) and a handful of other systems. This resolution hurdle has been dramatically overcome by the superb spatial resolution and sensitivity of HST and Chandra (supported by advances in radio observations), enabling the detection in individual clusters of more than 10, and in some cases more than 100, binaries. This review will focus on detections of neutron star binaries, including recent optical identifications, the exciting discoveries of multiple LMXBs in quiescence (with the potential to constrain neutron star equations of state) and the detections of millisecond pulsars (MSPs) in X-ray and optical images. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pedmonds@cfa.harvard.edu NR 38 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-143-5 J9 ASTR SOC P PY 2003 VL 296 BP 255 EP 262 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX13T UT WOS:000184405600054 ER PT S AU Berger, JP AF Berger, JP BE Perrin, G Malbet, F TI An introduction to visibility modeling SO OBSERVING WITH THE VLT INTERFEROMETER SE EAS PUBLICATIONS SERIES LA English DT Proceedings Paper CT EuroWinter School on Observing with the VLT Interferometer CY FEB 03-08, 2002 CL Les Houches, FRANCE SP European Union, CNRS, Act Specif Haute Resolut Angulaire, Jean-Marie Mariotti Ctr, Lab Astrophys Grenoble, European SO Observ AB This chapter is a first step towards visibility modeling. It describes analytical expressions for visibility curves derived from "classical" brightness distributions. It describes first some general useful tools for this kind of computation and then discusses several widely used morphologies. Finally, some practical issues of visibility modeling are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Berger, JP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 4 Z9 4 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 2-86883-652-6 J9 EAS PUBLICATIONS PY 2003 VL 6 BP 23 EP 34 DI 10.1051/eas:2003002 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BBQ68 UT WOS:000227174300002 ER PT S AU Berger, JP Tatulli, E Lecoarer, E AF Berger, JP Tatulli, E Lecoarer, E BE Perrin, G Malbet, F TI Exercise #1 - Modeling an astrophysical source in preparation for interferometric observations SO OBSERVING WITH THE VLT INTERFEROMETER SE EAS PUBLICATIONS SERIES LA English DT Proceedings Paper CT EuroWinter School on Observing with the VLT Interferometer CY FEB 03-08, 2002 CL Les Houches, FRANCE SP European Union, CNRS, Act Specif Haute Resolut Angulaire, Jean-Marie Mariotti Ctr, Lab Astrophys Grenoble, European SO Observ AB The following exercices are aimed to get trained to the link between the object intensity distribution and the corresponding visibility curves. They were intended to be the practical application of the seminar "Introduction to visibility modeling" (Berger same volume). This practical session was initially meant to be done with the ASPRO software (see Duvert same volume), uv tables and the fits file can be donwloaded from the ASPRO website. However, any image processing or mathematical software (Idl, Yorick, Mathlab, Mathernatica...) associated with the object equations given in Berger can be used for most exercises. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Berger, JP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 2-86883-652-6 J9 EAS PUBLICATIONS PY 2003 VL 6 BP 43 EP 45 DI 10.1051/eas:2003004 PG 3 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BBQ68 UT WOS:000227174300004 ER PT S AU Berger, JP AF Berger, JP BE Perrin, G Malbet, F TI Interferometric observations of protoplanetary disks SO OBSERVING WITH THE VLT INTERFEROMETER SE EAS PUBLICATIONS SERIES LA English DT Proceedings Paper CT EuroWinter School on Observing with the VLT Interferometer CY FEB 03-08, 2002 CL Les Houches, FRANCE SP European Union, CNRS, Act Specif Haute Resolut Angulaire, Jean-Marie Mariotti Ctr, Lab Astrophys Grenoble, European SO Observ ID ACCRETION DISKS; APPEARANCE AB The observation of protoplanetary disks at the astronomical unit scale is one of the most exciting key programs for long baseline interferometers. Existing observations have questioned the models of circumstellar environments of young stars; but this is just the beginning. Here, to provide the reader with a sense of what can be done today in this field, actual observations of the pre-main sequence star FU Orionis with near-infrared interferometers IOTA and PTI are presented. Every step, from raw data reduction to final interpretation, is described. The limits of current observations and the promise of future contributions from the VLTI are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Berger, JP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 2-86883-652-6 J9 EAS PUBLICATIONS PY 2003 VL 6 BP 191 EP 201 DI 10.1051/eas:2003017 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BBQ68 UT WOS:000227174300017 ER PT S AU Monnier, JD AF Monnier, JD BE Perrin, G Malbet, F TI Astrophysics with closure phases SO OBSERVING WITH THE VLT INTERFEROMETER SE EAS PUBLICATIONS SERIES LA English DT Proceedings Paper CT EuroWinter School on Observing with the VLT Interferometer CY FEB 03-08, 2002 CL Les Houches, FRANCE SP European Union, CNRS, Act Specif Haute Resolut Angulaire, Jean-Marie Mariotti Ctr, Lab Astrophys Grenoble, European SO Observ ID OPTICAL APERTURE SYNTHESIS; SPECKLE MASKING; INTERFEROMETER; IMAGES AB After a brief introduction, this contribution will discuss practical strategies to exploit the unique science potential of closure phases in optical interferometry, especially in the case of only three telescopes when direct imaging is near-impossible. Prototype source morphologies will be investigated in detail (binary and "dust shell + star"), and will illustrate how closure phase measurements can be used both for "Precision Interferometry" as well as qualitatively new probes of circumstellar environments. During this meeting, the notion of a "Closure Differential Phase" came to light, and some interesting properties of this quantity are here introduced. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Monnier, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Monnier, John D/0000-0002-3380-3307 NR 19 TC 3 Z9 3 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 2-86883-652-6 J9 EAS PUBLICATIONS PY 2003 VL 6 BP 213 EP 225 DI 10.1051/eas:2003019 PG 13 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BBQ68 UT WOS:000227174300019 ER PT S AU Marengo, M Karovska, M Sasselov, D Papaliolios, C Armstrong, JT Nordgren, TE AF Marengo, M Karovska, M Sasselov, D Papaliolios, C Armstrong, JT Nordgren, TE BE Perrin, G Malbet, F TI Calibrating the Cepheid Period-Luminosity relation with the VLTI SO OBSERVING WITH THE VLT INTERFEROMETER SE EAS PUBLICATIONS SERIES LA English DT Proceedings Paper CT EuroWinter School on Observing with the VLT Interferometer CY FEB 03-08, 2002 CL Les Houches, FRANCE SP European Union, CNRS, Act Specif Haute Resolut Angulaire, Jean-Marie Mariotti Ctr, Lab Astrophys Grenoble, European SO Observ AB The VLTI is the ideal instrument for measuring the distances of nearby Cepheids with the Baade-Wesselink method, allowing an accurate recalibration of the Cepheid Period-Luminosity relation. The high accuracy required by such measurement, however, can only be reached taking into account the effects of limb darkening, and its dependence on the Cepheid pulsations. We present here our new method to compute phase- and wavelength-dependent limb darkening profiles, based on hydrodynamic simulation of Classical Cepheid atmospheres. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 2-86883-652-6 J9 EAS PUBLICATIONS PY 2003 VL 6 BP 265 EP 267 DI 10.1051/eas:2003026 PG 3 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BBQ68 UT WOS:000227174300026 ER PT J AU Stiling, P Moon, DC Hunter, MD Colson, J Rossi, AM Hymus, GJ Drake, BG AF Stiling, P Moon, DC Hunter, MD Colson, J Rossi, AM Hymus, GJ Drake, BG TI Elevated CO2 lowers relative and absolute herbivore density across all species of a scrub-oak forest SO OECOLOGIA LA English DT Article DE elevated carbon dioxide; Kennedy Space Center; leaf abscission; leaf miners; natural enemies ID ATMOSPHERIC CO2; CARBON-DIOXIDE; LEAF SENESCENCE; SOIL NUTRIENT; PERFORMANCE; FOLIAGE; AVAILABILITY; ACCLIMATION; ENRICHMENT; RESPONSES AB The unabated increase in global atmospheric CO2 is expected to induce physiological changes in plants, including reduced foliar nitrogen, which are likely to affect herbivore densities. This study employs a field-based CO2 enrichment experiment at Kennedy Space Center, Florida, to examine plant-herbivore (insect) interactions inside eight open-topped chambers with elevated CO2 (710 ppm) and eight control chambers with ambient CO2. In elevated CO2 we found decreased herbivore densities per 100 leaves, especially of leaf miners, across all five plant species we examined: the oak trees Quercus myrtifolia, Q. geminata, and Q. chapmanii, the nitrogen-fixing vine Galactia elliottii and the shrub Vaccinium myrsinites. Both direct and indirect effects of lowered plant nitrogen may influence this decrease in herbivore densities. Direct effects of lowered nitrogen resulted in increased host-plant related death and an increase in compensatory feeding: per capita herbivore leaf consumption in elevated CO2 was higher than in ambient CO2. Indirectly, compensatory feeding may have prolonged herbivore development and increased exposure to natural enemies. For all leaf miners we examined, mortality from natural enemies increased in elevated CO2, These increases in host-plant induced mortality and in attack rates by natural enemies decreased leaf miner survivorship, causing a reduction in leaf miner density per 100 leaves. Despite increased leaf production in elevated CO2 from the carbon fertilization effect, absolute herbivore abundance per chamber was also reduced in elevated CO2. Because insects cause premature leaf abscission, we also thought that leaf abscission would be decreased in elevated CO2. However, for all plant species, leaf abscission was increased in elevated CO2, suggesting a direct effect Of CO2 on leaf abscission that outweighs the indirect effects of reduced insect densities on leaf abscission. C1 Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Univ Georgia, Inst Ecol, Athens, GA 30602 USA. Univ N Florida, Dept Biol, Jacksonville, FL 33224 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Stiling, P (reprint author), Univ S Florida, Dept Biol, Tampa, FL 33620 USA. NR 33 TC 59 Z9 63 U1 1 U2 23 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JAN PY 2003 VL 134 IS 1 BP 82 EP 87 DI 10.1007/s00442-002-1075-5 PG 6 WC Ecology SC Environmental Sciences & Ecology GA 636XK UT WOS:000180482400012 PM 12647184 ER PT J AU Hubbell, SP AF Hubbell, SP TI Modes of speciation and the lifespans of species under neutrality: A response to the comment of Robert E. Ricklefs SO OIKOS LA English DT Editorial Material ID DIVERSITY; CONSEQUENCES; PATTERNS; ECOLOGY AB Ricklefs (2003) has presented a thoughtful critique of the two modes of speciation discussed in my recent book (Hubbell 2001a). His main point is that under point mutation speciation, a plethora of species is produced with extremely short lifespans, whereas under random fission speciation, lifespans are too long, particularly in large metacommunities. The issue is easily resolved if one regards point mutation speciation and random fission speciation as the theoretical extremes of a speciation continuum. The mean lifespan of a species in the theory depends upon the size of the species population at its origination. If initial population sizes are fairly small, but not as small as the extreme of individual-founded lineages as under point mutation, then intermediate distributions of species lifespans are obtained. To examine this further, I consider a third model of speciation that I call "peripheral isolate speciation." There should be a signature of peripheral isolate speciation in the distribution of metacommunity relative species abundance, just as there is in the case of point mutation speciation and random fission speciation. Other points made by Ricklefs and several others are addressed in the body of the text. C1 Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. RP Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. EM shubbell@dogwood.botany.ugq.edu NR 26 TC 42 Z9 44 U1 2 U2 10 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0030-1299 EI 1600-0706 J9 OIKOS JI Oikos PD JAN PY 2003 VL 100 IS 1 BP 193 EP 199 DI 10.1034/j.1600-0706.2003.12450.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 644AU UT WOS:000180896400020 ER PT B AU Mohanty, S Jayawardhana, R Basri, G Allard, F Hauschildt, P Ardila, D AF Mohanty, S Jayawardhana, R Basri, G Allard, F Hauschildt, P Ardila, D BE Lepine, J GregorioHetem, J TI Surface gravity & mass in young brown dwarfs and planemos SO OPEN ISSUES IN LOCAL STAR FORMATION SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Int Colloquium on Open Issues in Local Star Formation and Early Stellar Evolution CY APR 05-10, 2003 CL Ouro Preto, BRAZIL ID EVOLUTIONARY MODELS; ATMOSPHERES AB We analyse high-resolution optical spectra of a sample of low-mass, very young, mid-to late M stellar and substellar objects in Upper Scorpius and Taurus. Precise effective temperatures (+/-50K) and surface gravities (+/-0.25 dex) are derived from a multi-feature spectral analysis using TiO, NaI and KI, through comparison with the latest synthetic spectra. Our high-resolution analysis is independent of extinction estimates. Combining our T-e f f and gravities with distance and photometry information then allows us to derive extinctions, masses, radii and luminosities. We emphasize that our analysis is independent of theoretical evolutionary models. As such, it offers a new way of deriving fundamental parameters for low-mass stellar and substellar objects, and of testing the model evolutionary tracks. We find discrepancies between our results and the theoretical tracks for the coolest, lowest mass targets. Our gravities for these objects are significantly (similar to 0.75 dex) lower than for hotter ones. This is at odds with the predictions of the evolutionary models, and causes improbably low ages to be derived from the theoretical tracks for the coolest objects. Similarly, our radii and luminosities for the coolest, lowest mass objects are much larger than predicted by the evolutionary models. These results lead us to suggest that significant improvements in the evolutionary models may be necessary for very cool, ultra-low mass objects, perhaps in the treatment of convection and/or initial conditions. We also find two of our coolest targets to be planetary mass objects ("planemos"), with mass similar to7 M-J. Thus, some late-M PMS objects may be much less massive than current evolutionary models indicate. Equivalently, young planemos may be more luminous than expected. Combined with the detection of planemos by other groups, our results imply that such objects may not be too rare. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-1755-3 J9 ASTROPHYS SPACE SC L PY 2003 VL 299 BP 259 EP 266 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BY96P UT WOS:000189506300031 ER PT J AU Wooller, M Smallwood, B Scharler, U Jacobson, M Fogel, M AF Wooller, M Smallwood, B Scharler, U Jacobson, M Fogel, M TI A taphonomic study of delta C-13 and delta N-15 values in Rhizophora mangle leaves for a multi-proxy approach to mangrove palaeoecology SO ORGANIC GEOCHEMISTRY LA English DT Article ID SEA-LEVEL RISE; CARBON ISOTOPE; MOUNT-KENYA; BRAZILIAN COAST; ORGANIC-MATTER; LAKE RUTUNDU; EAST-AFRICA; FRACTIONATION; DIAGENESIS; ECOSYSTEM AB The response of mangrove ecosystems to environmental change can be examined with stable isotopic tracers of C and N. The delta(13) C and delta(15)N of a taphonomic series of Rhizophora mangle L. (Red mangrove) leaves were analyzed from Twin Cays, Belize, to facilitate reconstruction of past mangrove ecosystems. On Twin Cays, fresh leaves of dwarf R. mangle trees (similar to0.5 m high) were found to have more negative delta(15) N values (mean = -10%.) and more positive delta(13)C values (mean = -25.3parts per thousand) compared to tall R. mangle trees (mean delta(15)N = 0parts per thousand, delta(13)C= -28.3parts per thousand). These isotopic differences can be related to nitrogen and phosphorus availability [Ecology 83 (2002) 1065]. We investigated three taphonomic stages in the fossilization of R. mangle leaves into peat with the following: (1) senescent leaves; (2) fallen leaves on the surface of the peat; and (3) sub-fossil leaves found within mangrove peat. In addition, by examining natural leaf assemblages we established that VC and delta(15)N of R. mangle leaves were not altered during senescence, despite a significant (50%) decrease in the N%. Modern dwarf and tall trees could still be identified from delta(13) C and delta(15)N analyses of the leaf assemblages found directly below a tree. Dwarf and tall trees could also be identified from VC analyses of leaves that had decomposed for four months. Although dwarf and tall trees could not be statistically separated after four months according to delta(15)N analyses, leaves with very negative delta(15)N (-7parts per thousand) were only collected below dwarf trees. Leaf fragments were present in similar to50 cm long cores of peat from four sites on the island, and their isotopic compositions were determined. The ranges of delta(13)C (-29 to -22parts per thousand) and delta(15)N (-11 to +2parts per thousand) values from sub-fossil leaves were similar to the ranges from modern leaves (delta(13)C = -29 to -23parts per thousand, delta(15)N = -11 to +1parts per thousand). The sub-fossil leaf isotopic compositions were independent values, in comparison to the uniform values of the surrounding peat. Because of the stability and persistence of the stable isotopic signals, they could contribute significantly to a multi-proxy approach to mangrove palaeoenvironmental reconstruction. (C) 2003 Elsevier Ltd. All rights reserved. C1 Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. Univ So Calif, Los Angeles, CA 90089 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Wooller, M (reprint author), Univ Alaska Fairbanks, Alaska Stable Isotope Facil, Water & Environm Res Ctr, 441 Duckering Bldg,POB 755860, Fairbanks, AK 99775 USA. RI Scharler, Ursula/F-3598-2010; Fogel, Marilyn/M-2395-2015; OI Fogel, Marilyn/0000-0002-1176-3818; Wooller, Matthew/0000-0002-5065-4235 NR 51 TC 29 Z9 29 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0146-6380 J9 ORG GEOCHEM JI Org. Geochem. PY 2003 VL 34 IS 9 BP 1259 EP 1275 DI 10.1016/S0146-6380(03)00116-5 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 716UQ UT WOS:000185048000004 ER PT B AU Goddard, I AF Goddard, I GP ac BE Wolfart, HC TI Heckewelder's 1792 vocabulary from Ohio: A possible attestation of Mascouten SO PAPERS OF THE THIRTY-FOURTH ALGONQUIAN CONFERENCE SE Papers of the Algonquin Conference LA English DT Proceedings Paper CT 34th Algonquian Conference CY OCT 24-27, 2002 CL Charlotte Reinholtz & Queen Univ, KINGSTON, CANADA SP Univ Aboriginal Council HO Charlotte Reinholtz & Queen Univ ID MESKWAKI C1 Smithsonian Inst, Washington, DC 20560 USA. NR 39 TC 0 Z9 0 U1 0 U2 0 PU UNIV MANITOBA PRESS PI WINNIPEG PA 244 ENGINEERING BLDG, WINNIPEG, MANITOBA R3T 2N2, CANADA J9 PAP ALGON CONF PY 2003 VL 34 BP 165 EP 191 PG 27 WC Anthropology; Linguistics SC Anthropology; Linguistics GA BBP19 UT WOS:000226858800009 ER PT B AU Goddard, I AF Goddard, I BE Wolfart, HC TI Heckewelder's 1792 vocabulary from Ohio: A possible attestation of Mascouten SO PAPERS OF THE THIRY-FOURTH ALGONQUIAN CONFERENCE SE Papers of the Algonquin Conference LA English DT Proceedings Paper CT 34th Algonquian Conference CY OCT 24-27, 2002 CL Charlotte Reinholtz & Queen Univ, KINGSTON, CANADA SP Univ Aboriginal Council HO Charlotte Reinholtz & Queen Univ C1 Smithsonian Inst, Washington, DC 20560 USA. NR 40 TC 0 Z9 0 U1 0 U2 0 PU UNIV MANITOBA PRESS PI WINNIPEG PA 244 ENGINEERING BLDG, WINNIPEG, MANITOBA R3T 2N2, CANADA J9 PAP ALGON CONF PY 2003 VL 34 BP 165 EP 191 PG 27 WC Anthropology; Ethnic Studies; Language & Linguistics SC Anthropology; Ethnic Studies; Linguistics GA BY30G UT WOS:000188858200009 ER PT J AU Wright, SJ AF Wright, SJ TI The myriad consequences of hunting for vertebrates and plants in tropical forests SO PERSPECTIVES IN PLANT ECOLOGY EVOLUTION AND SYSTEMATICS LA English DT Article DE folivores; Janzen-Connell hypothesis; plant diversity; pollinators; seed dispersers; seed predators ID SEED DISPERSAL; NEOTROPICAL FORESTS; RECRUITMENT LIMITATION; SPECIES COEXISTENCE; AMAZONIAN FORESTS; RAIN-FORESTS; PREDATION; DIVERSITY; HERBIVORES; SURVIVAL AB Humans hunt forest vertebrates throughout the tropics. Many preferred game species consume flowers, fruit, seeds and/or leaves, and these interactions will cause their harvest to ramify through forests. Three related issues will determine how severely the harvest of forest vertebrates influences the plant community. First, the types of species selected by hunters and the intensity of the harvest will determine which vertebrates are removed and which remain. Second, the possible presence of ecologically similar, non-game species able to expand their activities to fulfill the ecological role of heavily exploited species will determine how severely the harvest disrupts ecological relationships between the community of forest vertebrates and the community of forest plants. Finally, hunters will alter plant species composition if the harvest of vertebrates differentially affects mutualists or pests of particular plant species. Hunters will also alter plant diversity if the harvest of vertebrates disrupts ecological mechanisms that permit plant species to coexist. I examine hunter selectivity, the intensity of the hunt, possible compensation by non-game species, and the types and strengths of interactions among game species and plants for tropical forests to determine when and where these outcomes occur. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 76 TC 121 Z9 129 U1 3 U2 27 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1433-8319 J9 PERSPECT PLANT ECOL JI Perspect. Plant Ecol. Evol. Syst. PY 2003 VL 6 IS 1-2 BP 73 EP 86 DI 10.1078/1433-8319-00043 PG 14 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 704MX UT WOS:000184344400006 ER PT J AU Esry, BD Sadeghpour, HR AF Esry, BD Sadeghpour, HR TI Ultraslow (p)over-bar-H collisions in hyperspherical coordinates: Hydrogen and protonium channels SO PHYSICAL REVIEW A LA English DT Article ID ANTIPROTONIC HELIUM; METASTABLE STATES; ATOMS; CAPTURE; ANNIHILATION; IONIZATION; THRESHOLD; SYSTEM; H-2 AB The collision of an antiproton and a hydrogen atom at ultralow energies is described in hyperspherical coordinates. An adiabatic approximation leads to potential-energy curves that can be used to describe the dynamics of capture in the (p) over bar -H(1s) collision. A unified formulation of the collision and capture processes leading to formation of p (p) over bar bound states emerges. Both Pn(nl)-e(-) "atomic-type" and (p) over bar -H(n(')l(')) "molecular-type" states are represented. These potential curves are calculated to more than 10 000 protonium Bohr radii, where low-energy antiprotons are stopped in collisions with hydrogen atoms. Elastic and inelastic partial and total protonium formation cross sections in the mass-scaled (p) over bar -H system are calculated. The existence of protonium negative (or positive) ion in its ground and excited states is discussed. C1 Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. Kansas State Univ, JR Macdonald Lab, Manhattan, KS 66506 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Esry, BD (reprint author), Kansas State Univ, Dept Phys, Cardwell Hall, Manhattan, KS 66506 USA. RI Esry, Brett/H-7511-2013 OI Esry, Brett/0000-0003-3207-8526 NR 31 TC 26 Z9 26 U1 0 U2 3 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 JAN PY 2003 VL 67 IS 1 AR 012704 DI 10.1103/PhysRevA.67.012704 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 642KY UT WOS:000180804600066 ER PT S AU Gomez, Y Miranda, LF Anglada, G Torrelles, JM AF Gomez, Y Miranda, LF Anglada, G Torrelles, JM BE Kwok, S Dopita, M Sutherland, R TI Water and OH maser emission from the planetary nebula k3-35 SO PLANETARY NEBULAE: THEIR EVOLUTION AND ROLE IN THE UNIVERSE SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 209th Symposium of the International-Astronomical-Union CY NOV 19-23, 2001 CL CANBERRA, AUSTRALIA SP Int Astron Union ID RADIO MORPHOLOGY AB Water-vapour masers, typical of the envelopes in giant stars, are not expected to persist in planetary nebulae due to the ultraviolet radiation of the remnant star that progressively destroys the molecules. Recently, we have reported the first unambiguous detection of water maser emission in a planetary nebula, K 3-35 (Miranda et al. 2001). The water masers in K3-35 were detected at the center of the nebula, along the minor axis, at a radius of similar to85 AU and also at the surprisingly large distance of 5000 AU from the star, at the tips of the bipolar lobes. The existence of these water molecules is puzzling, and probably we are observing the very moment of transformation of a giant star into a planetary nebula. Miranda et al. (2001) also report the presence of polarization in the OH 1665 MHz masers, which are distributed towards the central star in a torus-like structure. Here we review the main results on this source. C1 Natl Autonomous Univ Mexico, Astron Inst, Morelia 58089, Michoacan, Mexico. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Inst Ciencias Espacio, E-08034 Barcelona, Spain. CSIC, IEEC, E-08034 Barcelona, Spain. RP Gomez, Y (reprint author), Natl Autonomous Univ Mexico, Astron Inst, Apdo Postal 3-72, Morelia 58089, Michoacan, Mexico. OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 13 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-148-6 J9 IAU SYMP PY 2003 IS 209 BP 263 EP 266 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BY04E UT WOS:000187344400075 ER PT J AU Gehrig, HH Aranda, J Cushman, MA Virgo, A Cushman, JC Hammel, BE Winter, K AF Gehrig, HH Aranda, J Cushman, MA Virgo, A Cushman, JC Hammel, BE Winter, K TI Cladogram of Panamanian Clusia based on nuclear DNA: Implications for the origins of crassulacean acid metabolism SO PLANT BIOLOGY LA English DT Article DE Clusia; Clusiaceae; internal transcribed spacer (ITS); molecular phylogeny; crassulacean acid metabolism (CAM) ID RIBOSOMAL DNA; GENUS CLUSIA; NUCLEOTIDE-SEQUENCES; ISOTOPE RATIOS; TROPICAL TREES; CARBON; CAM; PHYLOGENY; UVITANA; C-3-PHOTOSYNTHESIS AB The internal transcribed spacer (ITS) region of 18-26S nuclear ribosomal DNA repeat was sequenced for 31 of the approximately 40 species of Clusia known to occur in Panama. Several species from other genera of the Clusiaceae were used as outgroups in the phylogenetic calculation. High sequence alignment and minimal length variation among ITS-1, 5.8S and ITS-2 sequences facilitated determination of positional homology of nucleotide sizes. Sequence alignment was evaluated with character state (Maximum Parsimony) and distance methods (Neighbour joining). Phylogenetic trees obtained with the two methods were largely concordant and revealed three main groups that roughly correspond to previous arrangements of species into three large morphological groups, the C. flava group, the C. minor group and the C. multiflora group. Because species of Clusia are either regular C-3 plants or exhibit crassulacean acid metabolism (CAM) involving varying proportions of CO2 fixation in the dark versus the light, we mapped photosynthetic pathways onto the cladograms. Photosynthetic pathway classification was based on measurements of C-13/C-12 ratios of plant carbon and also on information available from the literature. Both the C. flava and C. minor group contained species exhibiting CAM. distributed on distinct branches of the cladograms, whereas the third group (C. multiflora group) was composed of species which are not known to use CAM. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Nevada, Dept Biochem, Reno, NV 89557 USA. Missouri Bot Garden, St Louis, MO 63166 USA. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. NR 41 TC 29 Z9 31 U1 1 U2 6 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 1435-8603 J9 PLANT BIOLOGY JI Plant Biol. PD JAN PY 2003 VL 5 IS 1 BP 59 EP 70 DI 10.1055/s-2003-37983 PG 12 WC Plant Sciences SC Plant Sciences GA 666XZ UT WOS:000182202900007 ER PT S AU Gardner, LD Kohl, JL Daigneau, PS Smith, PL Strachan, L Howard, RA Socker, DG Davila, JM Noci, G Romoli, M Fineschi, S AF Gardner, LD Kohl, JL Daigneau, PS Smith, PL Strachan, L Howard, RA Socker, DG Davila, JM Noci, G Romoli, M Fineschi, S BE Fineschi, S TI The Advanced Spectroscopic and Coronagraphic Explorer: Science payload design concept SO POLARIMETRY IN ASTRONOMY SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Polarimetry in Astronomy CY AUG 25-28, 2002 CL WAIKOLOA, HI SP SPIE DE solar corona; UV Spectroscopy; magnetic fields; coronagraphs; UV optics; polarization ID SOLAR AB The Advanced Spectroscopic and Coronagraphic Explorer (ASCE) was proposed in, 2001 to NASA's Medium-Class Explorer (MIDEX) Program by the Smithsonian Astrophysical Observatory in collaboration with the Naval Research Laboratory, Goddard Space Flight Center, and the Italian Space Agency. It is one of four missions selected for Phase A study in 2002. ASCE is composed of three instrument units: an Advanced Ultraviolet Coronagraph Spectrograph (AUVCS), an Advanced Large Aperture Visible light Spectroscopic Coronagraph (ALASCO), and an Advanced Solar Disk Spectrometer (ASDS). ASCE makes use of a 13 m long boom that-is extended on orbit and positions the external occulters of AUVCS and ALASCO nearly 15 m in front of their respective telescope mirrors. The optical design concepts for the instruments will be discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gardner, LD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Romoli, Marco/H-6859-2012 NR 8 TC 6 Z9 6 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4622-X J9 P SOC PHOTO-OPT INS PY 2003 VL 4843 BP 1 EP 7 DI 10.1117/12.466139 PG 7 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW39A UT WOS:000181847200001 ER PT S AU Korzennik, SG Rabello-Soares, C Schou, J AF Korzennik, SG Rabello-Soares, C Schou, J BE SawayaLacoste, H TI On the characterization of high-degree modes: A lesson from MDI SO PROCEEDINGS OF SOHO 12/GONG (PLUS) 2002 ON LOCAL AND GLOBAL HELIOSEISMOLOGY: THE PRESENT AND FUTURE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Meeting on Local and Global Helioseismology CY OCT 27-NOV 01, 2002 CL BIG BEAR LAKE, CA SP SOHO 12, GONG, NASA, NSF, ESA DE helioseismology; high-degree ridge fitting ID DIFFERENTIAL ROTATION; SOLAR AB High degree power ridges (up to l = 900) were computed and fitted for several two to three-month-long time-series of full-disk observations taken with the Michelson Doppler Imager (MDI) on-board the Solar and Heliospheric Observatory between 1996 and 1999. A detailed discussion of the modeling of the ridge power distribution, and the contribution of the various observational and instrumental effects on the spatial leakage, in the context of the MDI instrument, are presented. The result of this work is a better understanding of the problems associated with the characterization of high degree modes. We present the instrumental and observational requirements needed to achieve a determination of high degree mode frequencies whose residual systematic errors associated with the accuracy of the ridge to mode correction scheme are smaller than the uncertainty of the fitting itself. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Rabello Soares, Maria Cristina/C-3207-2013 NR 8 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-827-1 J9 ESA SP PUBL PY 2003 VL 517 BP 145 EP 150 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW83S UT WOS:000183306100021 ER PT S AU Hora, JL Fazio, GG Megeath, ST Willner, SP Ashby, MLN Huang, J Wang, Z Pipher, JL Forrest, WJ McCreight, CR McKelvey, M McMurray, R Hoffmann, WF Eisenhardt, P Stauffer, JR Reach, W Surace, JA Glaccum, W Moseley, SH Arendt, RG Stewart, KP Robinson, FD AF Hora, JL Fazio, GG Megeath, ST Willner, SP Ashby, MLN Huang, J Wang, Z Pipher, JL Forrest, WJ McCreight, CR McKelvey, M McMurray, R Hoffmann, WF Eisenhardt, P Stauffer, JR Reach, W Surace, JA Glaccum, W Moseley, SH Arendt, RG Stewart, KP Robinson, FD BE Metcalfe, L Salama, A Peschke, SB Kessler, MF TI Calibration of the Infrared Array Camera (IRAC) for SIRTF SO PROCEEDINGS OF THE CONFERENCE ON THE CALIBRATION LEGACY OF THE ISO MISSION SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Conference on Calibration Legacy of the ISO Mission CY FEB 05-09, 2001 CL MADRID, SPAIN DE ISO; IRAC; SIRTF; calibration; infrared : detectors ID PERFORMANCE; FACILITY AB The Infrared Array Camera (IRAC) is one of three focal plane instruments in the Space Infrared Telescope Facility (SIRTF). IRAC is a four-channel camera that obtains simultaneous images at 3.6, 4.5, 5.8, and 8 mum. Two adjacent 5.12' x 5.12' fields of view in the SIRTF focal plane are viewed by the four channels in pairs (3.6 and 5.8 pm; 4.5 and 8 mum). All four detector arrays in the camera are 256 x 256 pixels in size, with the two shorter wavelength channels using InSb and the two longer wavelength channels using Si:As IBC detectors. We describe the results of the instrument calibration measurements completed at Goddard Space Flight Center, including the characterisation of the arrays, optical quality, and the radiometric performance of the assembled instrument. The in-flight calibration strategy is outlined, and an estimate of the point source sensitivity of IRAC in SIRTF is presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hora, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Moseley, Harvey/D-5069-2012; OI Hora, Joseph/0000-0002-5599-4650 NR 7 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-765-8 J9 ESA SP PUBL PY 2003 VL 481 BP 73 EP 76 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BX94S UT WOS:000186908900011 ER PT S AU Megeath, ST Cohen, M Stauffer, JR Hora, JL Fazio, GG Berlind, P Calkins, M AF Megeath, ST Cohen, M Stauffer, JR Hora, JL Fazio, GG Berlind, P Calkins, M BE Metcalfe, L Salama, A Peschke, SB Kessler, MF TI The ground based identification and characterization of Irac celestial calibrators SO PROCEEDINGS OF THE CONFERENCE ON THE CALIBRATION LEGACY OF THE ISO MISSION SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Conference on Calibration Legacy of the ISO Mission CY FEB 05-09, 2001 CL MADRID, SPAIN DE SIRTF; infrared calibration stars; optical spectroscopy; ground based observations; MK classification; optical photometry; infrared photometry ID STANDARDS; STARS AB We describe an ongoing campaign to identify and characterise celestial standards for the Infrared Array Camera (IRAC) which will be deployed on the Space Infrared Telescope Facility (SIRTF). These standards must extend to much fainter magnitudes than calibrator sources used for previous IR space missions, and thus, need to be identified and characterised through ground based observations. The method we have chosen is to use a combination of empirical templates of cool stars and Kurucz models of hot stars to extrapolate BVRIJHK photometry of known K giants and A dwarfs to the IRAC bands. There will be two sets of calibrators: one set near the north ecliptic pole which can be observed continuously throughout the SIRTF mission, and a second set distributed along the ecliptic plane which will be used to monitor the calibration on a day to day basis. We overview the entire selection, identification, and characterisation process. The K giants and A dwarfs are being selected from existing catalogues of stars. To verify the spectral types of these stars, we have undertaken observations of the candidates with the FAST spectrometer on the 1.5 meter Till-inghast telescope at Mt. Hopkins. By comparing the spectra of these stars with MK standards, we are able to establish the spectral type with an uncertainty of one subclass, and in the case of K giants, identify K dwarfs contaminating our sample. We are now beginning CCD camera observations to obtain accurate BVRI photometry for the selected stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Megeath, ST (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hora, Joseph/0000-0002-5599-4650 NR 14 TC 2 Z9 2 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-765-8 J9 ESA SP PUBL PY 2003 VL 481 BP 165 EP 168 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BX94S UT WOS:000186908900028 ER PT J AU Spangler, PJ Steiner, WE AF Spangler, PJ Steiner, WE TI A new species of water scavenger beetle, Coelostoma (s. str.) tina (Coleoptera : Hydrophilidae : Sphaeridiinae), from Kenya, eastern Africa SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE aquatic insects; Afrotropical fauna; extreme environments; salt lakes ID LAKE MAGADI AB A new species of African water scavenger beetle, Coelostoma tina Spangler and Steiner, is described. The specimens were collected in an eastern African section of the Rift Valley from lagoons in Lake Magadi, Kenya, and pools adjacent to the lake. The water in these habitats is hypersaline and highly alkaline and shores are salt encrusted. The adults are described and illustrated with line drawings and scanning electron micrographs. Habitat notes and photographs of the biotope are given. C1 Natl Museum Nat Hist, Dept Systemat Biol Entomol, Smithsonian Inst, Washington, DC 20560 USA. RP Spangler, PJ (reprint author), Natl Museum Nat Hist, Dept Systemat Biol Entomol, Smithsonian Inst, Washington, DC 20560 USA. NR 15 TC 0 Z9 1 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2003 VL 105 IS 1 BP 1 EP 8 PG 8 WC Entomology SC Entomology GA 636KK UT WOS:000180454500001 ER PT J AU Pogue, MG AF Pogue, MG TI New synonyms in the genus Obrima Walker (Lepidoptera : Noctuidae), with additional distribution records SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Acanthermia; Obrima didactica; Obrima pyraloides; Obrima rinconada; distribution; Costa Rica AB The monotypic genus Acanthermia Hampson 1926 is congeneric with Obrima Walker 1856 (new synonym). Two new synonymies of Obrima didactica (Dyar) 1914 (new combination) are proposed: Acanthermia dyari Hampson (1926) and Obrima cymbae Pogue (1998). Additional distributional records from Costa Rica are included. Adults of all Obrima species are illustrated to show intraspecific variation. C1 Natl Museum Nat Hist, Smithsonian Inst, Sysemat Entomol Lab, Plant Sci Lab,USDA ARS, Washington, DC 20013 USA. RP Pogue, MG (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Sysemat Entomol Lab, Plant Sci Lab,USDA ARS, POB 37012,MRC-168a, Washington, DC 20013 USA. NR 11 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 JAN PY 2003 VL 105 IS 1 BP 13 EP 21 PG 9 WC Entomology SC Entomology GA 636KK UT WOS:000180454500003 ER PT J AU Mathis, WN Trautwein, MD AF Mathis, WN Trautwein, MD TI A revision and phylogenetic study of Lipochaeta Coquillett (Diptera : Ephydridae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE revision; Diptera; Ephydridae; Lipochaetini; L. ranica; New World; phylogeny ID SHORE FLIES AB The genus Lipochaeta Coquillett is revised and a phylogenetic analysis of the genera of the tribe Lipochaetini is provided. Lipochaeta is known thus far only from the New World, Where there are now two species, The second species. L. ranica, n. sp., (type locality: California), is described herein. The species of Lipochaeta Occur in saline or alkaline habitats, especially along maritime coasts. The monophyly of Lipochaeta is well corroborated and its putative sister group is the Old World genus Homalometophus Becker. C1 Smithsonian Inst, NMNH, Dept Systemat Biol, Entomol Sect, Washington, DC 20013 USA. RP Mathis, WN (reprint author), Smithsonian Inst, NMNH, Dept Systemat Biol, Entomol Sect, POB 37012,MRC-169, Washington, DC 20013 USA. EM mathis.wayne@nmnh.si.edu; traut4@yahoo.com NR 40 TC 4 Z9 4 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2003 VL 105 IS 1 BP 30 EP 49 PG 20 WC Entomology SC Entomology GA 636KK UT WOS:000180454500005 ER PT J AU Henry, TJ AF Henry, TJ TI Proboscidotylus nigrosquamis (Maldonado) (Heteroptera : Miridae : Orthotylinae): New combination and first record for the United States SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; Heteroptera; Miridae; Orthotylinae; new combination; descriptions; distribution AB Parthenicus nigrosquamis Maldonado, described and previously known only from Puerto Rico, is reported for the first time in the United States from Key West, Florida. Based on head morphology, vestiture, and male genital structures, this species is removed from Parthenicus Reuter and transferred to the monotypic genus Proboscidotylus Henry (n. comb.), previously known only from Mexico. The type species of Proboscidotylus, P. carvalhoi Henry, and P. nigrosquamis are redescribed and their relationships are discussed. Scanning electron micrographs of selected structures, dorsal and lateral photographs, and illustrations of male genitalia for both species are provided to help facilitate recognition. C1 Natl Museum Nat Hist, Smithsonian Inst, Sysemat Entomol Lab, PSI,ARS,USDA, Washington, DC 20506 USA. RP Henry, TJ (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Sysemat Entomol Lab, PSI,ARS,USDA, Washington, DC 20506 USA. NR 4 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 JAN PY 2003 VL 105 IS 1 BP 59 EP 65 PG 7 WC Entomology SC Entomology GA 636KK UT WOS:000180454500007 ER PT J AU Adamski, D Maier, CT AF Adamski, D Maier, CT TI A new Holcocera Clemens (Lepidoptera : Gelechioidea : Coleophoridae : Holcocerini) associated with Pinaceae in North America SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Blastobasinae; conifer; pine AB Holcocera concolor, new species, is described from North America. The imago, wing venation, and male and female genitalia are illustrated. Adults have been reared from larvae collected from several species of Pinaceae. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Adamski, D (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. NR 5 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 JAN PY 2003 VL 105 IS 1 BP 144 EP 148 PG 5 WC Entomology SC Entomology GA 636KK UT WOS:000180454500018 ER PT J AU Grissell, EE Smith, DR AF Grissell, EE Smith, DR TI First report of Epitraninae (Hymenoptera : Chalcididae) in the Nearctic SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article C1 Smithsonian Inst, Museum Natl Hist Nat, USDA, Agr Res Serv,Syst Entomol Lab,PSI, Washington, DC 20560 USA. RP Grissell, EE (reprint author), Smithsonian Inst, Museum Natl Hist Nat, USDA, Agr Res Serv,Syst Entomol Lab,PSI, Washington, DC 20560 USA. NR 10 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 JAN PY 2003 VL 105 IS 1 BP 240 EP 242 PG 3 WC Entomology SC Entomology GA 636KK UT WOS:000180454500028 ER PT J AU Grissell, EE AF Grissell, EE TI Discovery of Monodontomerus osmiae Kamijo (Hymenoptera : Torymidae) in the new world SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Systemat Entomol Lab,PSI,Agr Res Serv, Washington, DC 20560 USA. RP Grissell, EE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, Systemat Entomol Lab,PSI,Agr Res Serv, Washington, DC 20560 USA. NR 7 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 JAN PY 2003 VL 105 IS 1 BP 243 EP 245 PG 3 WC Entomology SC Entomology GA 636KK UT WOS:000180454500029 ER PT J AU Smith, DR AF Smith, DR TI Expanding ranges for four species of invasive sawflies (Hymenoptera : Tenthredinidae) in eastern United States SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. NR 11 TC 2 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 JAN PY 2003 VL 105 IS 1 BP 246 EP 248 PG 3 WC Entomology SC Entomology GA 636KK UT WOS:000180454500030 ER PT J AU Soon, W Baliunas, S AF Soon, Willie Baliunas, Sallie TI Global warming SO PROGRESS IN PHYSICAL GEOGRAPHY LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wsoon@cfa.harvard.edu NR 51 TC 4 Z9 4 U1 1 U2 7 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0309-1333 J9 PROG PHYS GEOG JI Prog. Phys. Geogr. PY 2003 VL 27 IS 3 BP 448 EP 455 DI 10.1191/0309133303pp391pr PG 8 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA V43OW UT WOS:000202945400007 ER PT J AU Siemiginowska, A Aldcroft, TL Bechtold, J Brunetti, G Elvis, M Stanghellini, C AF Siemiginowska, A Aldcroft, TL Bechtold, J Brunetti, G Elvis, M Stanghellini, C TI X-ray emission from gigahertz peaked/compact steep spectrum sources SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article; Proceedings Paper CT 3rd Workshop on Compact Steep Spectrum and Gigahertz-Peaked Spectrum Radio Sources CY MAY 28-31, 2002 CL KERASTARI, GREECE DE galaxies : active; X-rays : galaxies ID RADIO-SOURCES; ABSORPTION; DISCOVERY; GALAXIES AB The high spatial resolution of the Chandra X-ray Observatory allows us to study the environment of GPS/CSS sources to within an arcsec of the strong compact core. We present the discovery of X-ray jets in two GPS quasars, PKS1127-145 and B2 0738+313, indicating that X-ray emission associated with the relativistic plasma is present at large distances from the GPS nucleus. We also discuss first results from Chandra observations of our GPS/CSS sample. We find that six out of ten sources show intrinsic absorption at a level which may be sufficient to confine the GPS source. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CNR, Inst Radioastron, I-40129 Bologna, Italy. CNR, Inst Radioastron, I-96017 Noto, Italy. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Stanghellini, Carlo/0000-0002-6415-854X; Brunetti, Gianfranco/0000-0003-4195-8613 NR 15 TC 12 Z9 12 U1 0 U2 1 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1323-3580 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PY 2003 VL 20 IS 1 BP 113 EP 117 DI 10.1071/AS02052 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685RV UT WOS:000183277800028 ER PT J AU Stothert, KE Piperno, DR Andres, TC AF Stothert, KE Piperno, DR Andres, TC TI Terminal Pleistocene Early Holocene human adaptation in coastal Ecuador: the Las Vegas evidence SO QUATERNARY INTERNATIONAL LA English DT Article; Proceedings Paper CT Meeting on the Archaeology of the Pleistocene/Holocene Transition CY DEC, 2000 CL ARGENTINA ID SANTA-ELENA PENINSULA; TROPICAL FOREST; PLANT USE; AGRICULTURE; CUCURBITA; SEA; DOMESTICATION; NEOTROPICS; EMERGENCE; AMERICA AB Preceramic sites located on the Santa Elena Peninsula in southwestern Ecuador and occupied in the Terminal Pleistocene and during the Early Holocene (10,800-6600 BP) have produced evidence of a durable Las Vegas adaptation focused on marine, estuarine and terrestrial resources. The Las Vegas people were among the earliest cultivators in America who participated in the domestication of useful plant species and progressively intensified their efforts in both fishing and horticulture. (C) 2003 Elsevier Ltd and INQUA. All rights reserved. C1 Univ Texas, Ctr Archaeol Res, San Antonio, TX 78285 USA. Smithsonian Trop Res Inst, Balboa, Panama. Cornell Univ, Ithaca, NY 14853 USA. RP Stothert, KE (reprint author), Univ Texas, Ctr Archaeol Res, San Antonio, TX 78285 USA. NR 108 TC 33 Z9 39 U1 2 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 J9 QUATERN INT JI Quat. Int. PY 2003 VL 109 BP 23 EP 43 AR PII S1040-6182(02)00200-8 DI 10.1016/S1040-6182(02)00200-8 PG 21 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 707HR UT WOS:000184505700004 ER PT J AU Piperno, DR Jones, JG AF Piperno, DR Jones, JG TI Paleoecological and archaeological implications of a Late Pleistocene/Early Holocene record of vegetation and climate from the Pacific coastal plain of Panama SO QUATERNARY RESEARCH LA English DT Article DE pleistocene; early holocene; climate and vegetation; prehistoric agriculture ID LAST GLACIAL MAXIMUM; LAKE VALENCIA BASIN; LOWLAND AMAZONIA; LATE QUATERNARY; POLLEN RECORD; RAIN-FOREST; ARIDITY; PHYTOLITHS; VENEZUELA; DIVERSITY AB A phytolith record from Monte Oscuro, a crater lake-located 10 m above sea level on the Pacific coastal plain of Panama, shows that during the Late Pleistocene the lake bed was dry and savanna-like vegetation expanded at the expense of tropical deciduous forest, the modem potential vegetation. A significant reduction of precipitation below current levels was almost certainly required to effect the changes observed. Core sediment characteristics indicate that permanent inundation of the Monte Oscuro basin with water occurred at about 10,500 C-14 yr B.P. Pollen and phytolith records show that deciduous tropical forest expanded into., the lake's watershed during the early Holocene. Significant burning of the vegetation and increases of; weedy plants at ca. 7500 to 7000 yr C-14 B.P. indicate disturbance, which most likely resulted from early human occupation of the seasonal tropical forest near Monte Oscuro, and the development of slash-and-burn methods of cultivation. (C) 2003 Elsevier Science (USA). All rights reserved. C1 Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Unit 0948, APO, AA 34002 USA. Texas A&M Univ, Dept Anthropol, Palynol Lab, College Stn, TX 77843 USA. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Unit 0948, APO, AA 34002 USA. NR 46 TC 54 Z9 59 U1 0 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD JAN PY 2003 VL 59 IS 1 BP 79 EP 87 AR PII S0033-5894(02)00021-2 DI 10.1016/S0033-5894(02)00021-2 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 652YF UT WOS:000181407900009 ER PT B AU Harris, DE AF Harris, DE BE Zensus, JA Cohen, MH Ros, E TI What can we learn about extragalactic radio jets from X-ray data? SO RADIO ASTRONOMY AT THE FRINGE, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Radio Astronomy at the Fringe CY OCT 10-12, 2002 CL NATL RADI ASTRON OBSERV, GREEN BANK, WV HO NATL RADI ASTRON OBSERV ID M87 JET; EMISSION AB We review the current status of resolved X-ray emission associated with extragalactic radio jets and hot-spots. The primary question for any particular jet is to decide if the X-rays come from the synchrotron process or from inverse Compton scattering. There is considerable evidence supporting synchrotron emission for knots in the jets of FRI galaxies. For FRII terminal hot-spots detected in the X-ray band, synchrotron self-Compton emission continues to provide viable models with one possible exception (so far). Inverse Compton scattering on photons of the cosmic microwave background is indicated for a few powerful jets, and is expected to be an important contributor if not the dominating mechanism for higher redshift objects. The application of a model generally yields physical parameters and in many cases, these include the Doppler boosting factor. C1 Smithsonian Astrophys Observ, HEA, Cambridge, MA 02138 USA. RP Harris, DE (reprint author), Smithsonian Astrophys Observ, HEA, MS-3,60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-147-8 J9 ASTR SOC P PY 2003 VL 300 BP 151 EP 158 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX69K UT WOS:000186144500022 ER PT B AU Heinke, CO Grindlay, JE Edmonds, PD Camilo, F AF Heinke, CO Grindlay, JE Edmonds, PD Camilo, F BE Bailes, M Nice, DJ Thorsett, SE TI X-ray and optical studies of millisecond pulsars in 47 Tucanae SO RADIO PULSARS, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Radio Pulsars CY AUG 26-29, 2002 CL MEDITERRANEAN AGRON INST CHANAI, Khania, GREECE HO MEDITERRANEAN AGRON INST CHANAI ID GLOBULAR-CLUSTER 47-TUCANAE; 47 TUCANAE; CORE; RADIATION; EMISSION AB Our Chandra X-ray observation of the globular cluster 47 Tuc clearly detected most of the 16 MSPs with precise radio positions, and indicates probable X-ray emission from the remainder. The MSPs ;are soft (BB kT similar to0.2-0.3 keV) and faint (L-X similar to few 10(30) ergs s(-1)), and generally consistent with thermal emission from small polar caps. An additional 40 soft X-ray sources are consistent with the known MSPs in X-ray colors, luminosity, and radial distribution within the cluster (and thus mass). We note that these MSPs display a flatter L-X to E relation than pulsars and MSPs in the field, consistent with polar cap heating models for younger MSPs and may suggest the surface magnetic field has been modified by repeated accretion episodes to include multipole components. Correlating HST images, radio timing positions, and the Chandra dataset has allowed optical searches for MSP binary companions. The MSP 47 Tuc-U is coincident with a blue star exhibiting sinusoidal variations that agree in period and phase with the heated face of the WD companion. Another blue variable star (and X-ray source) agrees in period and phase with the companion to 47 Tuc-W (which lacks an accurate timing position); this companion is probably a main sequence star. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heinke, CO (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-151-6 J9 ASTR SOC P PY 2003 VL 302 BP 367 EP 370 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX51M UT WOS:000185575800073 ER PT B AU Saar, SH AF Saar, SH BE Deming, D Seager, S TI The effects of plage on precision radial velocities SO SCIENTIFIC FRONTIERS IN RESEARCH ON EXTRASOLAR PLANETS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Scientific Frontiers in Research on Extrasolar Planets CY JUN 18-21, 2002 CL CARNEGIE INST, WASHINGTON, D.C. SP NASA Origins Solar Syst Program HO CARNEGIE INST ID MAGNETIC ACTIVITY; COOL STARS; GRANULATION; PLANET AB I present the first results of semi-empirical modeling of the effects of magnetic plage on measured radial velocities in G stars. I use solar line bisectors observed in quiet and active regions at a range of disk positions as proxies for stellar bisectors. These are then used to "warp" model line profiles and construct model stars with various v sin i and plage areas. The models predict the sun should show a maximum of Deltav(r) similar to10 m s(-1) short-term v(r) fluctuations atop similar to3 m s(-1) long-term (cyclic) modulation, while a Hyades age G dwarf with v sin i = 6 km s(-1) exhibits Deltav(r) similar to90 m s(-1) (short-term) atop similar to14 m s(-1) (long-term). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Saar, SH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 11 Z9 11 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-141-9 J9 ASTR SOC P PY 2003 VL 294 BP 65 EP 70 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX68A UT WOS:000186106100012 ER PT B AU Latham, DW AF Latham, DW BE Deming, D Seager, S TI Spectroscopic follow-up observations of planetary transit candidates identified by project vulcan SO SCIENTIFIC FRONTIERS IN RESEARCH ON EXTRASOLAR PLANETS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Scientific Frontiers in Research on Extrasolar Planets CY JUN 18-21, 2002 CL CARNEGIE INST, WASHINGTON, D.C. SP NASA Origins Solar Syst Program HO CARNEGIE INST ID MASS COMPANION AB We have used the CfA Digital Speedometers to carry out spectroscopic follow-up observations of 35 planetary transit candidates identified by project Vulcan. Nine of the candidates prove to have stellar companions with orbital motions consistent with the transits found by Vulcan. This demonstrates that Vulcan has succeeded in identifying real photometric variations of the sort expected for transits by close-in giant planets, with dips of up to a few percent and periods of up to several days. Three of the systems with orbital solutions are double-lined spectroscopic binaries, and grazing eclipses are the source of the photometric variations. Another two of the systems are triples, with a constant third star diluting the depth of the eclipses in a nearby eclipsing binary. For the four systems that are single-lined, the orbital solutions suggest that the light curves are due to eclipses by small M-dwarf companions. A few of the candidates, all with marginal transit detections, show no velocity variations at the level of about 0.5 km s(-1). If they have orbital companions responsible for the observed photometric variations, the masses must be less than about 10 Jupiter masses. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 20 Z9 20 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-141-9 J9 ASTR SOC P PY 2003 VL 294 BP 409 EP 412 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX68A UT WOS:000186106100083 ER PT B AU Saar, SH Seager, S AF Saar, SH Seager, S BE Deming, D Seager, S TI Uses of linear polarization as a probe of extrasolar planet atmospheres SO SCIENTIFIC FRONTIERS IN RESEARCH ON EXTRASOLAR PLANETS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Scientific Frontiers in Research on Extrasolar Planets CY JUN 18-21, 2002 CL CARNEGIE INST, WASHINGTON, D.C. SP NASA Origins Solar Syst Program HO CARNEGIE INST ID SCATTERING REGIONS; COOL STARS AB We point out some advantages of making observations of extrasolar planets in linearly polarized (LP) light. Older cool stars have quite low levels (similar to 10(-4) to 10(-5)) of fractional LP, while extrasolar planets can have relatively high fractional LP (similar to 0.1). Observations in LP light can therefore significantly enhance contrast between the planet and its parent star. Data on LP as a function of planetary orbital phase can be used to diagnose the properties (e.g., composition, size, and shape) of the scatterers in the planetary atmosphere. We discuss the feasibility of LP observations of extrasolar planets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Saar, SH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 16 Z9 16 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-141-9 J9 ASTR SOC P PY 2003 VL 294 BP 529 EP 534 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX68A UT WOS:000186106100103 ER PT B AU Traub, WA AF Traub, WA BE Deming, D Seager, S TI The colors of extrasolar planets SO SCIENTIFIC FRONTIERS IN RESEARCH ON EXTRASOLAR PLANETS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Scientific Frontiers in Research on Extrasolar Planets CY JUN 18-21, 2002 CL CARNEGIE INST, WASHINGTON, D.C. SP NASA Origins Solar Syst Program HO CARNEGIE INST ID TERRESTRIAL PLANETS; SPECTROMETER; EARTH AB The color of an extrasolar planet is an important property because, for the case of direct detection, color is likely to be the first post-detection quantity to be measured. We show here that color carries considerable information on planetary properties. The next most likely measurable quantity is a low resolution spectrum, and we show what additional information this carries. Several other aspects of direct detection are discussed, including the respective benefits of visible and infrared detection, techniques of visible coronagraphic detection, and the spectroscopy of an Earth-like planet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Traub, WA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 12 Z9 12 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-141-9 J9 ASTR SOC P PY 2003 VL 294 BP 595 EP 602 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX68A UT WOS:000186106100115 ER PT B AU Kuchner, MJ Spergel, DN AF Kuchner, MJ Spergel, DN BE Deming, D Seager, S TI Terrestrial planet finding with a visible light coronagraph SO SCIENTIFIC FRONTIERS IN RESEARCH ON EXTRASOLAR PLANETS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Scientific Frontiers in Research on Extrasolar Planets CY JUN 18-21, 2002 CL CARNEGIE INST, WASHINGTON, D.C. SP NASA Origins Solar Syst Program HO CARNEGIE INST AB Directly imaging extrasolar planets using a monolithic optical telescope avoids many pitfalls of space interferometry and opens up the prospect of visible light studies of extrasolar planetary systems. Future astronomical missions may require interferometry for high spatial resolution, but given that the first direct imaging missions will probably fit into a single launch vehicle, the astrophysics of planet finding calls for a visible light coronagraph as the first space mission to search for extrasolar terrestrial planets. New coronagraphic techniques place the necessary dynamic range within reach for detecting planets in reflected starlight. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kuchner, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 20,60 Garden St, Cambridge, MA 02138 USA. RI Kuchner, Marc/E-2288-2012 NR 16 TC 7 Z9 7 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-141-9 J9 ASTR SOC P PY 2003 VL 294 BP 603 EP 610 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX68A UT WOS:000186106100116 ER PT B AU Nisenson, P Melnick, GJ Geary, J Holman, M Korzennik, SG Noyes, RW Papaliolios, C Sasselov, DD Fischer, D Gezari, D Lyon, RG Gonsalves, R Hardesty, C Harwit, M Marley, MS Neufeld, DA Ridgway, ST AF Nisenson, P Melnick, GJ Geary, J Holman, M Korzennik, SG Noyes, RW Papaliolios, C Sasselov, DD Fischer, D Gezari, D Lyon, RG Gonsalves, R Hardesty, C Harwit, M Marley, MS Neufeld, DA Ridgway, ST BE Deming, D Seager, S TI The extrasolar planet imager (ESPI) SO SCIENTIFIC FRONTIERS IN RESEARCH ON EXTRASOLAR PLANETS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Scientific Frontiers in Research on Extrasolar Planets CY JUN 18-21, 2002 CL CARNEGIE INST, WASHINGTON, D.C. SP NASA Origins Solar Syst Program HO CARNEGIE INST AB ESPI has been proposed for direct imaging and spectral analysis of giant planets orbiting solar-type stars. ESPI extends the concept suggested by Nisenson and Papaliolios (2001) for a square aperture apodized telescope that has sufficient dynamic range to directly detect extrasolar planets. With a 1.5-meter square mirror, ESPI can deliver high dynamic range imagery as close as 0.3 arcseconds to bright sources, permitting a sensitive search for extrasolar planets around nearby stars and a study of their characteristics in reflected light. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01803 USA. RP Nisenson, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01803 USA. RI Lyon, Richard/D-5022-2012; Marley, Mark/I-4704-2013; OI Fischer, Debra/0000-0003-2221-0861 NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-141-9 J9 ASTR SOC P PY 2003 VL 294 BP 633 EP 638 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX68A UT WOS:000186106100120 ER PT S AU Esser, R Lie-Svendsen, O Edgar, R Chen, Y AF Esser, R Lie-Svendsen, O Edgar, R Chen, Y BE Velli, M Bruno, R Malara, F TI Observational and theoretical constraints on the heating and acceleration of the fast solar wind SO SOLAR WIND TEN, PROCEEDINGS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 10th International Solar Wind Conference CY JUN 17-21, 2002 CL PISA, ITALY SP Univ Firenze, Univ Pisa, Univ Calabria, IFSI, ASI, European Space Agcy, INAF ID POLAR CORONAL HOLE; ELECTRON-TEMPERATURE; LINES AB Constraints on coronal plasma parameters derived from remote and in situ observations are reviewed. The coronal observations include measurements of polarized white light and the widths and intensities of spectral lines. Emphasis is placed on electron temperatures derived from these measurements. In situ observations include mass flux, velocity and ion composition. Some of these observational results are in contradiction to each other. It is discussed how these contradictions could be overcome and what it means for the physical properties of the coronal plasma. The observations will are placed in context with different theoretical models of ion formation and solar wind expansion. Emphasis is placed on the fast solar wind originating in the polar coronal holes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Esser, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0148-9 J9 AIP CONF PROC PY 2003 VL 679 BP 249 EP 254 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BX72B UT WOS:000186211700058 ER PT J AU Tamisiea, ME Mitrovica, JX Davis, JL Milne, GA AF Tamisiea, ME Mitrovica, JX Davis, JL Milne, GA TI Long wavelength sea level and solid surface perturbations driven by polar ice mass variations: Fingerprinting Greenland and Antarctic ice sheet flux SO SPACE SCIENCE REVIEWS LA English DT Review ID GLACIAL ISOSTATIC-ADJUSTMENT; RISE; TRENDS; RECORDS AB Rapid ice mass variations within the large polar ice sheets lead to distinct and highly nonuniform sea-level changes that have come to be known as 'sea-level fingerprints'. We explore in detail the physics of these fingerprints by decomposing the total sea-level change into contributions from radial perturbations in the two bounding surfaces: the geoid (or sea surface) and the solid surface. In the case of a melting event, the sea-level fingerprint is characterized by a sea-level fall in the near-field of the ice complex and a gradually increasing sea-level rise (from 0.0 to 1.3 times the eustatic value) as one considers sites at progressively greater distances (up to similar to 90degrees or so) from the ice sheet. The far-field redistribution is largely driven by the relaxation of the sea-surface as the gravitational pull of the ablating ice sheet weakens. The near-field sea-level fall is a consequence of both this relaxation and ocean-plus-ice unloading of the solid surface. We argue that the fingerprints provide a natural explanation for geographic variations in sea-level (e.g., tide gauge, satellite) observations. Therefore, they furnish a methodology for extending traditional analyses of these observations to estimate not only the globally averaged sea-level rate but also the individual contributions to this rate (i.e., the sources). C1 Univ Colorado, UCB 440, Boulder, CO 80309 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Durham, Dept Geol Sci, Durham DH1 3LE, England. RP Univ Colorado, UCB 440, Boulder, CO 80309 USA. EM tamisiea@colorado.edu RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 32 TC 15 Z9 15 U1 2 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PY 2003 VL 108 IS 1-2 BP 81 EP 93 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 732AM UT WOS:000185918700009 ER PT J AU Smith, HA AF Smith, HA TI Public attitudes towards space science SO SPACE SCIENCE REVIEWS LA English DT Article DE public opinion; public understanding; space science education AB Astronomy and space science, including their associated basic research activities, enjoy broad popular backing. People generally support them, and say that they follow their results with interest. This article summarizes some of the detailed results of public surveys in the United States, focusing on popular opinions and attitudes, and the somewhat paradoxical finding that despite being interested and supportive, people are often ignorant about the basic facts. I explore some of the reasons for the popularity of space science, and suggest ways of justifying space science research in the broader context of science research. I argue that vigorous and innovative education and outreach programs are important, and can be made even more effective. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 2 Z9 2 U1 0 U2 6 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2003 VL 105 IS 1-2 BP 493 EP 505 DI 10.1023/A:1023979604016 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 683EC UT WOS:000183134000005 ER PT S AU Cosmo, ML Ashenberg, J Lorenzini, EC AF Cosmo, ML Ashenberg, J Lorenzini, EC BE Scheeres, DJ Pittelkau, ME Proulx, RJ Cangahuala, LA TI Modeling and estimation of ProSEDS decay SO SPACEFLIGHT MECHANICS 2003, PTS 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 13th Annual Space Flight Mechanics Meeting CY FEB 09-13, 2003 CL PONCE, PR SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc Space Flight Mech Tech Comm, AIAA Astrodynam Tech Comm AB Electrodynamic tethers can be used to generate power at the expense of a platform's orbital energy, which decreases as the system is decelerated by drag-like forces. Tethers using bare wires as anodes offer a much higher efficiency in collecting electrons in the ionosphere than the large spherical collectors used thus far. This new transportation technology will be demonstrated in March 2003 when the Propulsive Small Expendable Deployer System (ProSEDS) will attempt to deorbit a Delta second stage by using electrodynamic forces while simultaneously recharging the onboard batteries for operations. The aim of the paper is to present the tools developed to analyze ProSEDS, namely: (a) sophisticated numerical model to simulate the current collection mechanism and the orbital dynamics and (b) a Kalman filter to estimate the key physical parameters using the actual flight data. When compared to previous experiments, ProSEDS presents a high degree of complexity because its dynamics is strictly connected to the current distribution along the tether and its variations. The preliminary analysis shows that important information about the system dynamics can be estimated even though the system is not completely observable. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Cosmo, ML (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 1 Z9 1 U1 0 U2 2 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 J9 ADV ASTRONAUT SCI PY 2003 VL 114 BP 1667 EP 1674 PN 1-3 PG 8 WC Automation & Control Systems; Engineering, Aerospace; Mechanics SC Automation & Control Systems; Engineering; Mechanics GA BX92J UT WOS:000186831100098 ER PT S AU Lorenzini, EC Bombardelli, C Quadrelli, MB AF Lorenzini, EC Bombardelli, C Quadrelli, MB BE Scheeres, DJ Pittelkau, ME Proulx, RJ Cangahuala, LA TI Analysis and damping of lateral vibrations in a linear tethered interferometer SO SPACEFLIGHT MECHANICS 2003, PTS 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 13th Annual Space Flight Mechanics Meeting CY FEB 09-13, 2003 CL PONCE, PR SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc Space Flight Mech Tech Comm, AIAA Astrodynam Tech Comm AB The vibration modes of a linear tethered interferometer spinning around its center of mass are computed analytically. The system consists of two collectors and one combiner modeled as point masses and connected by two tether arms modeled as elastic continua. The equations of motion for small displacements are derived by means of a Lagrangian density function. The eigenvalue problem is solved analytically for the out-of-plane lateral oscillations, which are directly linked to the Optical Path Delay of the interferometer. In order to assess the tether dynamics influence upon the Optical Path Delay a convolution analysis is performed which determines the energy distribution in the lateral modes after a retargeting maneuver is completed. It is found that the maneuver can be performed in a "quasi-rigid" manner by proper choice of the thrust duration. Finally a control algorithm is presented for damping out these oscillations at the tether attachment point. The effectiveness of the damping strategy, based on an impedance matching criterion, is tested with a numerical model. C1 Harvard Smithsonian Ctr Astrophys, CfA, Cambridge, MA 02138 USA. RP Lorenzini, EC (reprint author), Harvard Smithsonian Ctr Astrophys, CfA, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 2 Z9 2 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 J9 ADV ASTRONAUT SCI PY 2003 VL 114 BP 1749 EP 1765 PN 1-3 PG 17 WC Automation & Control Systems; Engineering, Aerospace; Mechanics SC Automation & Control Systems; Engineering; Mechanics GA BX92J UT WOS:000186831100103 ER PT B AU Freeman, PE Kashyap, V Rosner, R Lamb, DQ AF Freeman, PE Kashyap, V Rosner, R Lamb, DQ BE Feigelson, ED Babu, GJ TI The statistical challenges of wavelet-based source detection SO STATISTICAL CHALLENGES IN ASTRONOMY LA English DT Proceedings Paper CT 3rd Statistical Challenges in Modern Astronomy Conference (SCMA III) CY JUL 18-21, 2001 CL PENN STATE UNIV, UNIVERSITY PK, PA SP Natl Sci Fdn, Div Math Sci, Natl Aeronaut & Space Adm, Appl Informat Syst Res Program HO PENN STATE UNIV AB Wavelet functions are proving extremely useful for detecting sources in binned, two-dimensional photon counts images. In this chapter, we describe the mission-independent source detection algorithm WAVDETECT, part of the Chandra Interactive Analysis of Observations (CIAO) software package, and discuss the statistical challenges we have faced in its development, such as: what is the best way to estimate the local background in each pixel, if it is a priori unknown? What is the best way to eliminate false detections caused by instrumental variations? And what is the significance of a detected source? C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Freeman, PE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 0-387-95546-1 PY 2003 BP 365 EP 376 DI 10.1007/0-387-21529-8_24 PG 12 WC Astronomy & Astrophysics; Statistics & Probability SC Astronomy & Astrophysics; Mathematics GA BW17K UT WOS:000181073200024 ER PT B AU Kashyap, V Drake, JJ Gudel, M Audard, M AF Kashyap, V Drake, JJ Gudel, M Audard, M BE Feigelson, ED Babu, GJ TI Modeling stellar microflares SO STATISTICAL CHALLENGES IN ASTRONOMY LA English DT Proceedings Paper CT 3rd Statistical Challenges in Modern Astronomy Conference (SCMA III) CY JUL 18-21, 2001 CL PENN STATE UNIV, UNIVERSITY PK, PA SP Natl Sci Fdn, Div Math Sci, Natl Aeronaut & Space Adm, Appl Informat Syst Res Program HO PENN STATE UNIV ID ULTRAVIOLET C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kashyap, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Guedel, Manuel/C-8486-2015 OI Guedel, Manuel/0000-0001-9818-0588 NR 3 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 0-387-95546-1 PY 2003 BP 451 EP 452 DI 10.1007/0-387-21529-8_48 PG 2 WC Astronomy & Astrophysics; Statistics & Probability SC Astronomy & Astrophysics; Mathematics GA BW17K UT WOS:000181073200048 ER PT B AU Li, D Melnick, GJ AF Li, D Melnick, GJ BE Cheng, KS Leung, KC Li, TP TI Submillimeter wave astronomy satellite and star formation SO STELLAR ASTROPHYSICS - A TRIBUTE TO HELMUT A. ABT SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT 6th Pacific Rim Stellar Conference on Stellar Astrophysics CY JUL 11-17, 2002 CL Xian, PEOPLES R CHINA SP Univ Hong Kong, Chinese Acad Sci, Inst High Energy Phys, Shaanxi Astron Observ DE ISM; star formation; submillimeter; astrochemistry ID DENSE INTERSTELLAR CLOUDS; ATOMIC OXYGEN ABUNDANCE; MOLECULAR CLOUDS AB As a successful NASA explorer mission, SWAS makes first detections of the H2O emission at a ground-state transition (1(10) --> 1(01)). The general range of the fractional water abundance ([H2O]/[H-2] similar to 6x10(-10) - 3x10(-8)) established through SWAS observations, are lower than those predicted by pure gas-phase chemistry by two orders of magnitude. SWAS does not detect O-2 with one possible exception. The sensitive limits on O-2 abundance, combined with measured H2O abundances, strongly suggest a critical role being played by dust grains in altering chemistry of relatively cold gas. C1 Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, D (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-1683-2 J9 ASTROPHYS SPACE SC L PY 2003 VL 298 BP 173 EP 177 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAA58 UT WOS:000221354700024 ER PT B AU Aufdenberg, JP Hauschildt, PH Baron, E AF Aufdenberg, JP Hauschildt, PH Baron, E BE Hubeny, I Mihalas, D Werner, K TI Spherical and expanding model atmosphere predictions for interferometry SO STELLAR ATMOSPHERE MODELING SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT International Workshop on Stellar Atmosphere Modeling CY APR 08-12, 2002 CL UNIV TUBINGEN, TUBINGEN, GERMANY HO UNIV TUBINGEN AB Long-baseline optical interferometry can test the radiation fields predicted by stellar atmosphere models in ways spectroscopy alone cannot. The observable in interferometry is the visibility. The calculation of synthetic visibilities from model atmosphere intensities is described and examples are shown for PHOENIX1 models of luminous A- and M-type stars. C1 Harvard Smithsonian Ctr Astrophys, Solar & Stellar Phys Div, Cambridge, MA 02138 USA. RP Aufdenberg, JP (reprint author), Harvard Smithsonian Ctr Astrophys, Solar & Stellar Phys Div, 60 Garden St,Mail Stop 15, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-131-1 J9 ASTR SOC P PY 2003 VL 288 BP 239 EP 242 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW53Y UT WOS:000182322800027 ER PT B AU Avrett, EH Fontenla, JM AF Avrett, EH Fontenla, JM BE Hubeny, I Mihalas, D Werner, K TI Influence of mass flows on the energy balance and structure of the solar transition region SO STELLAR ATMOSPHERE MODELING SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT International Workshop on Stellar Atmosphere Modeling CY APR 08-12, 2002 CL UNIV TUBINGEN, TUBINGEN, GERMANY HO UNIV TUBINGEN AB We have extended our previous modeling of energy balance in the chromosphere-corona transition region to include the effects of partible and mass flows. We consider quasi-steady cases satisfying the momentum and energy balance equations throughout the transition region and low corona. We include particle diffusion as well as flows in the optically thick non-LTE radiative transfer equations for the lines and continua of H, HeI, and HeII. Mass flows substantially affect the degree of ionization and the radiative losses of H and He, thereby affecting the structure and extent of the transition region. We find that the H and He line profiles are greatly affected by flows, and that line shifts are much less important than the changes in line intensity and central reversal due to the effects of flows on atmospheric structure. The Lyman alpha profiles We compute can generally explain the observed range of profiles obtained with high spectral and spatial resolution. The present paper is a brief summary of the detailed account given by Fontenla, Avrett, and Loeser (2002 FAL4). C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Avrett, EH (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-131-1 J9 ASTR SOC P PY 2003 VL 288 BP 279 EP 285 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW53Y UT WOS:000182322800037 ER PT B AU Sokoloski, JL AF Sokoloski, JL BE Corradi, RLM Mikolajewska, J Mahoney, TJ TI Rapid variability as a diagnostic of accretion and nuclear burning in symbiotic stars and supersoft X-ray sources SO SYMBIOTIC STARS PROBING STELLAR EVOLUTION SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Euroconference on Symbiotic Stars Probing Stellar Evolution CY MAY 27-31, 2002 CL Los Cancajos, SPAIN SP ING, European Commiss, Excelentisimo Cabildo Insular Palma, Patronato Turismo, Inst Astrofis Canarias ID WHITE-DWARFS; CH-CYGNI; GRS 1915+105; Z-ANDROMEDAE; PERIOD; DISK; LUMINOSITY; PHOTOMETRY; BINARIES AB Accretion disks and nuclear shell burning are present in some symbiotic stars (SSs) and probably all supersoft X-ray binaries (SSXBs). Both the disk and burning shell may be involved in the production of dramatic outbursts and, in some cases, collimated jets. A strong magnetic field may also affect the accretion flow and activity in some systems. Rapid-variability studies can probe the interesting region close to the accreting white dwarf (WD) in both SSs and SSXBs. I describe fast photometric observations of several individual systems in detail and review the results of a photometric variability survey of 35 SSs. These timing studies reveal the first clearly magnetic SS (Z And) and suggest that an accretion disk is involved in jet production in CH Cyg, as well as in the outbursts of both CH Cyg and Z And. They also support the notion that the fundamental power source in most SSs is nuclear burning on the surface of a WD and raise questions about the structure of disks in the SSXBs. Finally, spectroscopic observations of RS Oph reveal minute-timescale line strength variations, probably due to a hot boundary layer. Taken together, the rapid-timing observations explore the connections between jet-producing WDs and X-ray binaries, as well as SSs, SSXBs, and CVs. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Sokoloski, JL (reprint author), Smithsonian Astrophys Observ, MS 15,60 Garden St, Cambridge, MA 02138 USA. NR 34 TC 22 Z9 22 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-152-4 J9 ASTR SOC P PY 2003 VL 303 BP 202 EP 217 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BY80K UT WOS:000189467000035 ER PT J AU Hall, JPW AF Hall, JPW TI Phylogenetic reassessment of the five forewing radial-veined tribes of Riodininae (Lepidoptera : Riodinidae) SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID LIMITS; THISBE AB The relationships among the genera and tribal groupings of Riodininae with five forewing radial veins, and between these and tribes with four forewing radial veins, were examined using a phylogenetic analysis. Using the type species from all sixteen genera in the tribal groupings Eurybiini, Mesosemiini and incertae sedis (a presumed paraphyletic group of loosely related genera), and representatives from the four forewing radial-veined riodinine tribes, thirty-five new and traditional characters were coded from adult ecology, wing venation and pattern, the adult head and body, male and female genitalia, and early stage ecology and morphology. The majority of characters are illustrated. Phylogenetic analysis of these data produced five equally most parsimonious cladograms using equal weights and after successive weighting. The strict consensus of these confirms the monophyly of Eurybiini and Mesosemiini as currently conceived, but also indicates several higher-level relationships not previously hypothesized. Mesosemiini is here more broadly defined to also include the entire incertae sedis section, and the tribe is divided into Mesosemiina, for the previously delimited Mesosemiini plus Eunogyra and Teratophthalma, and Napaeina, subtr.n. for the incertae sedis section minus these two genera. The following hypothesis of relationships is tentatively proposed for the basal clades of Riodininae: Mesosemiini + (Eurybimi + remainder of Riodininae). These new hypotheses, and the characters supporting them, are discussed and compared with those previously proposed. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. NR 44 TC 13 Z9 18 U1 0 U2 2 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0307-6970 J9 SYST ENTOMOL JI Syst. Entomol. PD JAN PY 2003 VL 28 IS 1 BP 23 EP 37 DI 10.1046/j.1365-3113.2003.00196.x PG 15 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 643ZW UT WOS:000180894300002 ER PT J AU Ceruzzi, PE AF Ceruzzi, PE TI Driving visions: Exploring the road movie. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Ceruzzi, PE (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JAN PY 2003 VL 44 IS 1 BP 172 EP 173 DI 10.1353/tech.2003.0006 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 652YJ UT WOS:000181408200016 ER PT J AU Kidwell, PA AF Kidwell, PA TI Origins of cyberspace: A library on the history of computing, networking, and telecommunications. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Kidwell, PA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JAN PY 2003 VL 44 IS 1 BP 193 EP 194 DI 10.1353/tech.2003.0024 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 652YJ UT WOS:000181408200029 ER PT B AU Gaensler, BM AF Gaensler, BM BE Bandiera, R Maiolino, R Mannucci, F TI Shocks, outflows and bubbles: New views on pulsars and their winds SO TEXAS IN TUSCANY LA English DT Proceedings Paper CT 21st Texas Symposium on Relativistic Astrophysics CY DEC 09-13, 2002 CL Florence, ITALY SP Natl Inst Astrophys, CNR, Natl Inst Nucl Phys ID X-RAY NEBULA; CRAB-NEBULA; SUPERNOVA-REMNANTS; SYNCHROTRON NEBULA; BOW-SHOCK; PLERIONS; VELA AB A typical young pulsar slows down at an imperceptible rate, its spin period increasing by less than 10 microseconds over the course of a year. However, the inertia of a pulsar is so extreme that to effect this tiny change in rotation rate, the star must dissipate about 1046 ergs of kinetic energy. Observations of pulsars and their surroundings demonstrate that this "spin-down energy" is expelled into the pulsar's surroundings in spectacular fashion, in the form of a relativistic wind of charged particles and magnetic fields. In this review I highlight some recent observational results on pulsar winds at radio, X-ray and optical wavelengths, and explain what we can learn from these data about shock structure, particle acceleration and the interstellar medium. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-6, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010 NR 22 TC 3 Z9 3 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 981-238-580-0 PY 2003 BP 297 EP 304 DI 10.1142/9789812704009_0026 PG 8 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BCM36 UT WOS:000229995900026 ER PT S AU Traub, WA AF Traub, WA BE Lacoste, H TI Extrasolar planet characteristics in the visible wavelength range SO TOWARDS OTHER EARTHS: DARWIN/TPF AND THE SEARCH FOR EXTRASOLAR TERRESTRIAL PLANETS, PROCEEDINGS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Conference on Towards Other Earths - DARWIN/TPF and the Search for Extrasolar Terrestrial Planets CY APR 22-25, 2003 CL Heidelberg, GERMANY SP Max Planck Inst Astron, European Space Agcy, NASA DE extrasolar planets; visible wavelengths; color; color-color diagram; spectra; coronagraphs ID TERRESTRIAL PLANETS AB A coronagraph operating in the visible wavelength range to detect and characterize extrasolar planets offers advantages over any other wavelength range. The physical characteristics of a planet and its atmosphere can be derived from its color and its low-resolution spectrum, both of which are discussed. An analytic method is presented for calculating the shapes of mirrors in a pupil-mapping coronagraph. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Traub, WA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 5 Z9 5 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-849-2 J9 ESA SP PUBL PY 2003 VL 539 BP 231 EP 239 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BY94B UT WOS:000189500300024 ER PT S AU Schuller, P Vannier, M Petrov, R Lopez, B Leinert, C Henning, T AF Schuller, P Vannier, M Petrov, R Lopez, B Leinert, C Henning, T BE Lacoste, H TI Direct detection of sub-stellar companions with MIDI SO TOWARDS OTHER EARTHS: DARWIN/TPF AND THE SEARCH FOR EXTRASOLAR TERRESTRIAL PLANETS, PROCEEDINGS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Conference on Towards Other Earths - DARWIN/TPF and the Search for Extrasolar Terrestrial Planets CY APR 22-25, 2003 CL Heidelberg, GERMANY SP Max Planck Inst Astron, European Space Agcy, NASA ID PLANETS AB Current detection methods of planetary companions do not allow retrieving their spectral information properties. The method of Differential Interferometry has the potential to complement such information by comparing interferometric observables in various spectral channels. We outline the basic aspects of this method and how it can soon be realised by the Mid-infrared Interferometric instrument (MIDI) at the Very Large Telescope Interferometer (VLTI) observatory. A set of possible candidates for such direct observation has been selected among currently identified planetary companions. Differential Interferometry with MIDI would be complementary to other ground-based pro-rams. The method may also be an alternative for future space-based planetary spectroscopy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schuller, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA 02138 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-849-2 J9 ESA SP PUBL PY 2003 VL 539 BP 583 EP 587 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BY94B UT WOS:000189500300087 ER PT S AU Sozzetti, A Casertano, S Lattanzi, MG Spagna, A AF Sozzetti, A Casertano, S Lattanzi, MG Spagna, A BE Lacoste, H TI The GAIA astrometric survey of the solar neighborhood and its contribution to the target database for DARWIN/TPF SO TOWARDS OTHER EARTHS: DARWIN/TPF AND THE SEARCH FOR EXTRASOLAR TERRESTRIAL PLANETS, PROCEEDINGS SE ESA Special Publications LA English DT Proceedings Paper CT Conference on Towards Other Earths - DARWIN/TPF and the Search for Extrasolar Terrestrial Planets CY APR 22-25, 2003 CL Heidelberg, GERMANY SP Max Planck Inst Astron, European Space Agcy, NASA DE planetary systems; astrometry; stars : statistics; instrumentation : miscellaneous ID EXTRASOLAR PLANETS AB We evaluate the potential of the ESA Cornerstone Mission GAIA in helping populate the database of nearby stars (d < 25 pc) for subsequent target selection for DARWIN/TPF. The GAIA high-precision astrometric measurements will make it an ideal tool for a complete screening of the expected several thousands stars within 25 pc in order to identify and characterize (or rule out the presence of) Jupiter signposts. GAIA astrometry will be instrumental in complementing radial velocity surveys of F-G-K stars, and will more effectively search for massive planets the large database of nearby M dwarfs, which are less easily accessible with precision spectroscopy. The ability to determine the actual planet masses and inclination angles for detected systems, especially those with low-mass primaries (M < 0.6 M(circle dot)), stems as a fundamental contribution GAIA will make toward the final target selection for DARWIN/TPF, thus complementing exozodiacal dust emission observations from ground-based observatories such as Keck, LBTI, and VLTI. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sozzetti, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asozzetti@cfa.harvard.edu; stefano@stsci.edu; lattanzi@to.astro.it; spagna@to.astro.it OI Sozzetti, Alessandro/0000-0002-7504-365X; Lattanzi, Mario Gilberto/0000-0003-0429-7748 NR 8 TC 4 Z9 4 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-849-2 J9 ESA SPEC PUBL PY 2003 VL 539 BP 605 EP 610 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BY94B UT WOS:000189500300091 ER PT S AU Murray, SS AF Murray, SS CA HRC Science Team BE Trumper, JE Tananbaum, HD TI Recent scientific results from the Chandra HRC GTO program SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE x-ray astronomy; Chandra X-ray Observatory; HRC; pulsars; AGN; galaxies ID X-RAY-EMISSION; ELLIPTIC GALAXY; NEUTRON-STAR; DISCOVERY; 3C-58; PULSATIONS; CENTAURUS; REGION; M31 AB The Chandra X-ray Observatory (CXO) has now been in orbit a little over three years. During that time, the High Resolution Camera (HRC) Science Team has been carrying out a program of science observations making use of all of the capabilities of the Observatory with particular emphasis on the capabilities of the HRC for high resolution timing, and high resolution imaging. In this review of Chandra science, we present highlights of the past three years of observations including detailed studies of the Andromeda Galaxy (M31), discovery of a pulsar in the Supernova Remnant 3C58, and studies of X-ray emission from the nearby AGN Centaurus A. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Murray, SS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-2, Cambridge, MA 02138 USA. EM ssm@head-cfa.harvard.edu NR 23 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 PROC SPIE PY 2003 VL 4851 BP 17 EP 27 DI 10.1117/12.461164 PN 1&2 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600002 ER PT S AU Brickhouse, NS AF Brickhouse, NS BE Trumper, JE Tananbaum, HD TI Quantitative analysis of coronal x-ray spectra at high resolution SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE stars : coronae; techniques : spectroscopic; X-rays : stars ID CHANDRA; CAPELLA; DIAGNOSTICS; PROCYON; DENSITY; STARS AB We use Chandra observations to illustrate the X-ray spectral resolution and throughput required to probe the physical processes in stellar coronae. With today's capability, we are in a strong position to quantify the physical conditions (temperatures, abundances, and densities) for a number of stellar systems. The future holds the promise of dynamical studies to test the physical processes in the corona (heating, loop formation, winds). Diagnostic studies include measurements of electron densities in cool star atmospheres. Published measurements of electron densities from Chandra and XMM-Newton in the brightest stellar coronae disagree by more than an order of magnitude. We show that reconciling these measurements requires detailed treatment of weak satellite spectra and other line blending. While these studies provide a sobering view of electron density measurements, they also provide a strong indication of what can be learned in the future when we combine high spectral resolution with high signal-to-noise. Dynamic studies using Chandra HETC Doppler shifts are so far only reported for the most rapidly rotating cool stars. These new measurements are somewhat compromised by the presence of continuum and weak line blends, and are near the statistical limit. Nevertheless, they can provide a realistic test of the spectral synthesis such that the location(s) of coronal loops can be compared to the photospheric Doppler images. Examples of what can be learned from dynamic studies are presented. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Brickhouse, NS (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 69 EP 76 DI 10.1117/12.461418 PN 1&2 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600006 ER PT S AU Plucinsky, PP Schulz, NS Marshall, HL Grant, CE Chartas, G Sanwal, D Teter, MA Vikhlinin, AA Edgar, RJ Wise, MW Allen, GE Virani, SN DePasquale, JM Raley, MT AF Plucinsky, PP Schulz, NS Marshall, HL Grant, CE Chartas, G Sanwal, D Teter, MA Vikhlinin, AA Edgar, RJ Wise, MW Allen, GE Virani, SN DePasquale, JM Raley, MT BE Trumper, JE Tananbaum, HD TI The flight spectral response of the ACIS instrument SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE CXO; Chandra; ACIS; charge-coupled devices; CCDs; x-ray detectors; x-ray spectroscopy ID CCD IMAGING SPECTROMETER; CHARGE-TRANSFER INEFFICIENCY; X-RAY-SPECTRUM; RADIATION-DAMAGE AB We discuss the flight calibration of the spectral response of the Advanced CCD Imaging Spectrometer (ACIS) on-board the Chandra X-ray Observatory (CXO). The spectral resolution and sensitivity of the ACIS instrument have both been evolving over the course of the mission. The spectral resolution of the frontside-illuminated (FI) CCDs changed dramatically in the first month of the mission due to radiation damage. Since that time, the spectral resolution of the FI CCDs and the backside-illuminated (BI) CCDs have evolved gradually with time. We demonstrate the efficacy of charge-transfer inefficiency (CTI) correction algorithms which recover some of the lost performance. The detection efficiency of the ACIS instrument has been declining throughout the mission, presumably due to a layer of contamination building up on the filter and/or CCDs. We present a characterization of the energy dependence of the excess absorption and demonstrate software which models the time dependence of the absorption from energies of 0.4 keV and up. The spectral redistribution function and the detection efficiency are well-characterized at energies from 1.5 to 8.0 k-eV primarily due to the existence of strong lines in the ACIS calibration source in that energy range. The calibration at energies below 1.5 keV is challenging because of the lack of strong lines in the calibration source and also because of the inherent non-linear dependence with energy of the CTI and the absorption by the contamination layer. We have been using data from celestial sources with relatively simple spectra to determine the quality of the calibration below 1.5 k-eV. We have used observations of 1EO102.2-7219 (the brightest supernova remnant in the SMC), PKS2155-304 (a bright blazar), and the pulsar PSR 0656+14 (nearby pulsar with a soft spectrum), since the spectra of these objects have been well-characterized by the gratings on the CXO. The analysis of these observations demonstrate that the CTI correction recovers a significant fraction of the spectral resolution of the FI CCDs and the models of the time-dependent absorption result in consistent measurements of the flux at low energies for data from a BI (S3) CCD. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Plucinsky, PP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 34 Z9 34 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 89 EP 100 DI 10.1117/12.461473 PN 1&2 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600008 ER PT S AU Juda, M Donnelly, RH Hole, KT Kenter, AT Kraft, RP Murray, SS Pease, DO Wilton, CRA Zombeck, MV AF Juda, M Donnelly, RH Hole, KT Kenter, AT Kraft, RP Murray, SS Pease, DO Wilton, CRA Zombeck, MV BE Trumper, JE Tananbaum, HD TI Characteristics of the on-orbit background of the Chandra X-ray Observatory High Resolution Camera SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE X-ray detector; microchannel plate; MCP; particle background; HRC; CXO ID ASTROPHYSICS FACILITY AXAF; HRC AB The Chandra X-ray Observatory (CXO) High Resolution Camera (HRC) is a microchannel plate (MCP) based X-ray detector with heritage from similar detectors flown on the Einstein and ROSAT missions. The HRC consists of two detectors in a common housing. Improvements from the previous instruments include: fabricating the MCP from "low-noise" glass (glass that contains a reduced level of radioactive isotopes) and surrounding the detector housing on five sides with an active coincidence detector. Both of these improvements help to maximize the X-ray signal to background noise ratio. The on-orbit background is dominated by cosmic ray and solar-wind particles. The temporal behavior of the background has two parts: a quiescent level and a flaring component. The quiescent level slowly changes with time and is correlated with the high-energy particle flux as measured by the Electron Proton Helium Instrument (EPHIN), the CXO radiation detector. The flaring component is associated with times of elevated low-energy particle flux, primarily from the Sun. A combination of on-board vetoing and filtering during ground processing provides a substantial rejection of the non-X-ray background. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Juda, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 112 EP 123 DI 10.1117/12.461416 PN 1&2 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600010 ER PT S AU Zhao, P Van Speybroeck, LP AF Zhao, P Van Speybroeck, LP BE Trumper, JE Tananbaum, HD TI A new method to model X-ray scattering from random rough surfaces SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE X-ray scattering; random rough surface; X-ray mirror; X-ray telescope; Chandra X-ray Observatory ID MIRROR; PERFORMANCE AB This paper presents a method for modeling the X-ray scattering from random rough surfaces. An actual rough surface is (incompletely) described by its Power Spectral Density (PSD). For a given PSD, model surfaces with the same roughness as the actual surface are constructed by preserving the PSD amplitudes and assigning a random phase to each spectral component. Rays representing the incident wave are reflected from the model surface and projected onto a flat plane, which approximates the model surface, as outgoing rays and corrected for phase delays. The projected outgoing rays are then corrected for wave densities and redistributed onto an uniform grid where the model surface is constructed. The scattering is then calculated by taking the Fast Fourier Transform (FFT) of the resulting distribution. This method is generally applicable and is not limited to small scattering angles. It provides the correct asymmetrical scattering profile for grazing incident radiation. We apply this method to the mirrors of the Chandra X-ray Observatory and show the results. We also expect this method to be useful for other X-ray telescope missions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhao, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 11 Z9 11 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 124 EP 139 DI 10.1117/12.461426 PN 1&2 PG 16 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600011 ER PT S AU Pease, D Drake, JJ Kashyap, V Marshall, HL Raffauf, EL Ratzlaff, PW Wargelin, BJ AF Pease, D Drake, JJ Kashyap, V Marshall, HL Raffauf, EL Ratzlaff, PW Wargelin, BJ BE Trumper, JE Tananbaum, HD TI In-flight effective area calibration of the Chandra low energy transmission grating spectrometer SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE Chandra; X-ray; X-ray spectroscopy; transmission grating; calibration ID X-RAY; PKS-2155-304 AB We present the in-flight effective area calibration of the Low Energy Transmission Grating Spectrometer (LETGS), which comprises the High Resolution Camera Spectroscopic readout (HRC-S) and the Low Energy Transmission Grating (LETG) aboard the Chandra X-ray Observatory. Previous studies of the LETGS effective area calibration have focused on specific energy regimes: 1) the low-energy calibration for which we compared observations of Sirius B and HZ 43 with pure hydrogen non-LTE white dwarf emission models; and 2) the mid-energy calibration for which we compared observations of the active galactic nuclei PKS 2155-304 and 3C 273 with simple power-law models of their seemingly featureless continua. The residuals of the model comparisons were taken to be true residuals in the HRC-S quantum efficiency (QE) model. Additional in-flight observations of celestial sources with well-understood X-ray spectra have served to verify and fine-tune the calibration. Thus, from these studies we have derived corrections to the HRC-S QE to match the predicted and observed spectra over the full practical energy range of the LETGS. Furthermore, from pre-flight laboratory flatfield data we have constructed an HRC-S quantum efficiency uniformity (QEU) model. Application of the QEU to our semi-empirical in-flight HRC-S QE has resulted in an improved HRC-S on-axis QE. Implementation of the HRC-S QEU with the on-axis QE now allows for the computation of effective area for any reasonable Chandra/LETGS pointing. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Pease, D (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 9 Z9 9 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 157 EP 168 DI 10.1117/12.461275 PN 1&2 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600014 ER PT S AU Elvis, M Fiore, F AF Elvis, M Fiore, F CA CWE Team BE Trumper, JE Tananbaum, HD TI A high resolution intergalactic explorer for the soft X-ray/FUV SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE space missions; x-ray; ultraviolet; spectroscopy ID LY-ALPHA SYSTEMS; AFTERGLOW; ABSORPTION; GALAXIES; HISTORY AB We present a mission concept for high resolution X-ray spectroscopy with a resolving power, R similar to6000, (c.f. Rless than or similar to1000 for Chandra, XMM-Newton). This resolution is physics-driven, since it allows the thermal widths of coronal X-ray lines to be measured, and astrophysics-driven, since 50 km s(-1) resolves internal galaxy motions, and galaxy motions within larger structures. Such a mission could be small and have a rapid response allowing us to 'X-ray the Universe' using the afterglows of Gamma-ray Bursts (GRBs) as strong background sources of X-rays, and so illuminate the 'Cosmic Web'. The Cosmic Web is predicted to contain most of the normal matter (baryons) in the nearby Universe. C1 Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 377 EP 387 DI 10.1117/12.461471 PN 1&2 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600035 ER PT S AU Schnopper, HW Barbera, M Silver, E Ingram, R Christensen, FE Romaine, S Cohen, L Collura, A Murray, SS AF Schnopper, HW Barbera, M Silver, E Ingram, R Christensen, FE Romaine, S Cohen, L Collura, A Murray, SS BE Trumper, JE Tananbaum, HD TI Thin, plastic shell, X-ray optics: an update SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE X-ray optics; plastic shell X-ray optics; approximate X-ray optics; point-to-point X-ray imaging AB We present new results from a program to develop large area X-ray telescopes that are made from thin plastic shells. We use multi-shell cylindrical lenses in a point-to-point configuration to form full aperture images of the small focal spot in a an X-ray tube on a microchannel plate detector. The image data are analyzed to yield radial profiles and encircled energy curves. The derived parameters can be extrapolated to the case of a telescope that is a conical approximation to Wolter 1 optics. The plastic shells can be coated with suitable mono- or multilayers that allow for a wideband coverage of X-ray energies. Our current program is focused on the development of a large area, hard X-ray telescope for a balloon payload (see the paper 4851 - 107 by E. Silver, et al at this conference). C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Schnopper, HW (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. OI collura, alfonso/0000-0001-9534-1235; Barbera, Marco/0000-0002-3188-7420 NR 12 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 480 EP 490 DI 10.1117/12.461286 PN 1&2 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600046 ER PT S AU Gorenstein, P AF Gorenstein, P BE Trumper, JE Tananbaum, HD TI Concepts: X-ray telescopes with high angular resolution and high throughput SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE X-ray astronomy; X-ray telescopes; X-ray lenses; Fresnel zone plates ID HIGH-ENERGY ASTRONOMY; OPTICS AB The high rate at which important results are emanating from the Chandra X-Ray Observatory heightens our appreciation of the significance of high angular resolution telescopes in X-ray astronomy. However, the Chandra telescope is probably the last member of a line of high resolution telescopes with a conventional architecture. Qualitative improvement upon Chandra's resolution requires a new technology. We discuss a promising approach that is capable potentially of achieving microarcsecond resolution, possibly the highest angular resolution in astronomy of any wavelength band. It is based upon X-ray optics that focus by transmission at normal incidence rather than by reflection at grazing incidence. Its components are refractive lenses and Fresnel zone plates. Extreme chromatic aberration is intrinsic to these devices but it can be overcome in small wavelength intervals above 2 keV with a technique described by Van Speybroeck and by other methods. Like X-ray interferometry these systems have extremely long focal lengths and require "formation flying" consisting of precise positioning between the optics and detector that be aboard separate spacecraft spaced far apart. However, it is less demanding of accuracy in formation flying than X-ray interferometry. These systems have much lower mass than grazing incidence telescopes with comparable collecting area. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gorenstein, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 10 Z9 10 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 599 EP 606 DI 10.1117/12.461605 PN 1&2 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600057 ER PT S AU Jenkins, JA Narita, T Grindlay, JE Bloser, PF Stahle, C Parker, B Barthelmy, S AF Jenkins, JA Narita, T Grindlay, JE Bloser, PF Stahle, C Parker, B Barthelmy, S BE Trumper, JE Tananbaum, HD TI Background measurements from balloon-borne CZT detectors SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE CZT; background; balloon flights; hard x-ray astronomy AB We report detector characteristics and background measurements from two prototype imaging CdZnTe (CZT) detectors flown on a scientific balloon payload in May 2001. The detectors are both platinum-contact 10 mm x 10 mm x 5 mm CZT crystals, each with a 4 x 4 array of pixels tiling the anode. One is made from IMARAD horizontal Bridgman CZT, the other from eV Products high-pressure Bridgman CZT. Both detectors were mounted side-by-side in a flip-chip configuration and read out by a 32-channel IDE VA/TA ASIC preamp/shaper. We enclosed the detectors in the same 40degrees field-of-view collimator (comprising a graded passive shield and plastic scintillator) used in our previously-reported September 2000 flight. I-V curves for the detectors are diode-like, and we find that the platinum contacts adhere significantly better to the CZT surfaces than gold to previous detectors. The detectors and instrumentation performed well in a 20-hour balloon flight on 23/24 May 2001. Although we discovered a significant instrumental background component in flight, it was possible to measure and subtract this component from the spectra. The resulting IMARAD detector background spectrum (from 30 keV to similar to 450 keV) reaches similar to 5 x 10(-3) counts cm(-2)s(-1)keV(-1) at 100 keV and has a power-law index of similar to 2 at high energies. The eV Products detector has a similar spectrum, although there is more uncertainty in the energy scale because of calibration complications. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jenkins, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barthelmy, Scott/D-2943-2012 NR 5 TC 2 Z9 2 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 866 EP 874 DI 10.1117/12.461537 PN 1&2 PG 9 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600085 ER PT S AU Silver, E Schnopper, H Jones, C Forman, W Bandler, S Murray, S Romaine, S Slane, P Grindlay, J Madden, N Beeman, J Haller, EE Smith, D Barbera, M Collura, A Christensen, F Ramsey, B Woosley, S Diehl, R Tucker, G Fabregat, J Reglero, V Gimenez, A AF Silver, E Schnopper, H Jones, C Forman, W Bandler, S Murray, S Romaine, S Slane, P Grindlay, J Madden, N Beeman, J Haller, EE Smith, D Barbera, M Collura, A Christensen, F Ramsey, B Woosley, S Diehl, R Tucker, G Fabregat, J Reglero, V Gimenez, A BE Trumper, JE Tananbaum, HD TI B-MINE, the balloon-borne microcalorimeter nuclear line explorer SO X-RAY AND GAMMA-RAY TELESCOPES AND INSTRUMENTS FOR ASTRONOMY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Telescopes and Instruments for Astronomy CY AUG 24-28, 2002 CL WAIKOLOA, HI SP SPIE DE X-ray astronomy; microcalorimeter; balloon; X-ray optics; supernova ID SUPERNOVA; EMISSION AB B-MINE is a concept for a balloon mission designed to probe the deepest regions of a supernova explosion by detecting Ti-44 emission at 68 keV with spatial and spectral resolutions that are sufficient to determine the extent and velocity distribution of the Ti-44 emitting region. The payload introduces the concept of focusing optics and microcalorimeter spectroscopy to nuclear line emission astrophysics. B-MINE has a thin, plastic foil telescope multilayered to maximize the reflectivity in a 20 keV band centered at 68 keV and a microcalorimeter array optimized for the same energy band. This combination provides a reduced background, an energy resolution of 50 eV and a 3sigma sensitivity in 10(6) s of 3.3 x 10(-7) ph cm(-2) s(-1) at 68 keV. During the course of a long duration balloon flight, B-MINE could carry out a detailed study of the Ti-44 emission line centroid and width in CAS A. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Silver, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-2, Cambridge, MA 02138 USA. RI Bandler, Simon/A-6258-2010; Fabregat, Juan/F-9066-2016; OI Bandler, Simon/0000-0002-5112-8106; Fabregat, Juan/0000-0002-5986-9347; Barbera, Marco/0000-0002-3188-7420; Forman, William/0000-0002-9478-1682 NR 5 TC 5 Z9 5 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4630-0 J9 P SOC PHOTO-OPT INS PY 2003 VL 4851 BP 905 EP 912 DI 10.1117/12.461410 PN 1&2 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Imaging Science & Photographic Technology GA BW45N UT WOS:000182073600089 ER PT J AU Kaeppler, AL AF Kaeppler, AL TI An introduction to dance aesthetics SO YEARBOOK FOR TRADITIONAL MUSIC LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Kaeppler, AL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 10 TC 7 Z9 7 U1 0 U2 0 PU INT COUNCIL TRADITIONAL MUSIC PI LOS ANGELES PA UCLA/DEPT ETHNOMUSICOLOGY, 2539 SCHOENBERG, BOX 957178, LOS ANGELES, CA 90095 USA SN 0740-1558 J9 YEARB TRADIT MUSIC JI Yearb. Tradit. Mus. PY 2003 VL 35 BP 153 EP 162 DI 10.2307/4149325 PG 10 WC Music SC Music GA 758AD UT WOS:000187609600006 ER PT J AU Wisely, SM McDonald, DB Buskirk, SW AF Wisely, SM McDonald, DB Buskirk, SW TI Evaluation of the genetic management of the endangered black-footed ferret (Mustela nigripes) SO ZOO BIOLOGY LA English DT Article DE endangered species; captive propagation; reintroductions; mean kinship; microsatellite DNA; population genetics ID INBREEDING AVOIDANCE; CAPTIVE-POPULATIONS; CONSERVATION; DISPERSAL AB Empirical support for the genetic management strategies employed by captive breeding and reintroduction programs is scarce. We evaluated the genetic management plan for the highly endangered black-footed ferret (Mustela nigripes) developed by the American Zoo and Aquarium Associations (AZA) as a part of the species survival plan (SSP). We contrasted data collected from five microsatellite loci to predictions from a pedigree-based kinship matrix analysis of the captive black-footed ferret population. We compared genetic diversity among captive populations managed for continued captive breeding or reintroduction, and among wild-born individuals from two reintroduced populations. Microsatellite data gave an accurate but only moderately precise estimate of heterozygosity. Genetic diversity was similar in captive populations maintained for breeding and release, and it appears that the recovery program will achieve its goal of maintaining 80% of the genetic diversity of the founder population over 25 years. Wild-born individuals from reintroduced populations maintained genetic diversity and avoided close inbreeding. We detected small but measurable genetic differentiation between the reintroduced populations. The model of random mating predicted only slightly lower levels of heterozygosity retention compared to the SSP strategy. The random mating strategy may be a viable alternative for managing large, stable, captive populations such as that of the black-footed ferret. (C) 2003 Wiley-Liss, Inc. C1 Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. RP Wisely, SM (reprint author), Smithsonian Inst, Mol Genet Lab, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI McDonald, David/C-3195-2008; Buskirk, Steven/K-2871-2016 OI McDonald, David/0000-0001-8582-3775; Buskirk, Steven/0000-0003-0611-6648 NR 31 TC 25 Z9 26 U1 4 U2 64 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2003 VL 22 IS 3 BP 287 EP 298 DI 10.1002/zoo.10089 PG 12 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 697NX UT WOS:000183950800007 ER PT J AU Swanson, WF Johnson, WE Cambre, RC Citino, SB Ouigley, KB Brousset, DM Morals, RN Moreira, N O'Brien, SJ Wildt, DE AF Swanson, WF Johnson, WE Cambre, RC Citino, SB Ouigley, KB Brousset, DM Morals, RN Moreira, N O'Brien, SJ Wildt, DE TI Reproductive status of endemic felid species in Latin American zoos and implications for ex situ conservation SO ZOO BIOLOGY LA English DT Article DE electroejaculation; semen; cats; breeding; testosterone; cortisol; nutrition; exhibitry; cryopreservation ID LAPAROSCOPIC ARTIFICIAL-INSEMINATION; JAGUARS PANTHERA-ONCA; DOMESTIC CAT; PHYLOGEOGRAPHIC PATTERNS; MITOCHONDRIAL-DNA; ENDANGERED FELIDS; PUMA; CONCOLOR; SPERMATOZOA; EVOLUTION AB Reproductive evaluations were conducted on 185 male cats representing eight endemic Latin American species that were maintained in 44 zoos and private facilities in 12 Latin American countries. Reproductive assessments (testicular measures, ejaculate quality, and blood testosterone/cortisol concentration) were used to establish normative values for large- and small-sized cats in Latin American collections. Data also were analyzed using multiple regression to study the impact of proven breeder status, diet, and various animal housing combinations. Most felids (>95%) in the survey were of wild-born origin, and <20% had produced offspring in captivity. Larger felids had bigger testes and produced more semen, but tended to produce low-sperm-density ejaculates. The ejaculates of small felids were more sperm-concentrated, but contained fewer total spermatozoa. Sperm motility was unrelated to species size, and certain species (puma, margay, tigrina, and jaguarundi) consistently produced few (<40%) normal sperm forms. Across species, >50% of males had low sperm counts (< 1 million total sperm per ejaculate). Among large cats (jaguars and pumas), proven breeders had larger (P<0.05) testes, greater semen volume, and more normal sperm than nonbreeders. Males on adequate diets had higher (P<0.05) circulating cortisol. Among small-sized felids, proven breeders had higher (P<0.05) testosterone, and males housed alone or paired with a conspecific female had more (P<0.05) total sperm per ejaculate and greater (P<0.05) seminal and testicular volumes. Fifty-nine ejaculates (potentially representing similar to 100 artificial insemination (AI) or 26,000 in vitro fertilization (IVF) procedures) were cryopreserved for a felid genome resource bank. In conclusion, breeding success and reproductive traits for many endemic felids in Latin American zoos appear to be suboptimal, and likely would benefit from improvements in diet and exhibitry. Technology transfer and continued training of zoo staff and scientists in Latin American countries are essential if these zoos are to achieve their tremendous conservation potential for felids and other threatened endemic species. C1 Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife, Cincinnati, OH 45220 USA. NCI, Lab Genom Divers, Frederick, MD 21701 USA. Smithsonian Natl Zool Pk, Conservat & Res Ctr, Washington, DC USA. White Oak Conservat Ctr, Yulee, FL USA. Hornocker Wildlife Res Inst, Moscow, ID USA. Univ Nacl Autonoma Mexico, Fac Med Vet & Zootech, Coyoacan, Mexico. Univ Fed Parana, Setor Ciencias Biol, BR-80060000 Curitiba, Parana, Brazil. Univ Fed Parana, Curso Med Vet, Palotina, Brazil. NCI, Lab Genom Divers, Frederick, MD 21701 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 RI Moreira, Nei/C-6399-2013; Johnson, Warren/D-4149-2016; Morais, Rosana/R-4928-2016 OI Moreira, Nei/0000-0002-9236-667X; Johnson, Warren/0000-0002-5954-186X; Morais, Rosana/0000-0002-0816-4371 NR 60 TC 29 Z9 32 U1 9 U2 42 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2003 VL 22 IS 5 BP 421 EP 441 DI 10.1002/zoo.10093 PG 21 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 738UG UT WOS:000186305800001 ER PT J AU Czekala, NM MacDonald, EA Steinman, K Walker, S Garrigues, NW Olson, D Brown, JL AF Czekala, NM MacDonald, EA Steinman, K Walker, S Garrigues, NW Olson, D Brown, JL TI Estrogen and LH dynamics during the follicular phase of the estrous cycle in the Asian elephant SO ZOO BIOLOGY LA English DT Article DE elephant; urinary hormones; estrogen; luteinizing hormone; progestins; follicular development ID LOXODONTA-AFRICANA; LUTEINIZING-HORMONE; OVARIAN-FUNCTION; MAXIMUS; PROGESTERONE; SERUM; PREGNANCY; PATTERNS; EXCRETION; SECRETION AB Pituitary and corpus luteum hormone patterns throughout the elephant estrous cycle have been well characterized. By contrast, analysis of follicular maturation by measurement of circulating estrogens has been uninformative. This study tested the ability of a urinary estradiol-3-glucuronide radioimmunoassay to noninvasively assess follicular development during the nonluteal phase of the elephant estrous cycle, and to determine the relationship between estrogen production and the "double LH surge." Daily urine and serum samples were collected throughout seven estrous cycles from three Asian elephants, and urine was collected from an additional three females, for a total of 13 cycles. Serum was analyzed for luteinizing hormone (LH), and urine was analyzed for estrogens and progestins. Elephants exhibited a typical LH pattern, with an anovulatory LH (anLH) surge occurring approximately 21 days before the ovulatory LH (ovLH) surge. The urinary estrogen pattern indicated the presence of two follicular waves during the nonluteal phase. The first wave (anovulatory) began 5 days before the anLH surge and reached a maximum concentration the day before the peak. Thereafter, urinary estrogens declined to baseline for 2 weeks before increasing again to peak concentrations on the day of the ovLH surge. Urinary progestins were baseline throughout most of the follicular phase, increasing 2-3 days before the ovLH surge and continuing into the luteal phase. These results support previous ultrasound observations that two waves of follicular growth occur during the nonluteal phase of the elephant estrous cycle. Each wave is associated with an increase in estrogen production that stimulates an LH surge. Thus, in contrast to serum analyses, urinary estrogen monitoring appears to be a reliable method for characterizing follicular activity in the elephant. C1 Zool Soc San Diego, Ctr Reprod Endangered Species, San Diego, CA 92112 USA. Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA USA. Indianapolis Zoo, Indianapolis, IN USA. RP Czekala, NM (reprint author), Zool Soc San Diego, Ctr Reprod Endangered Species, POB 120551, San Diego, CA 92112 USA. NR 28 TC 14 Z9 15 U1 1 U2 3 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2003 VL 22 IS 5 BP 443 EP 454 DI 10.1002/zoo.10098 PG 12 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 738UG UT WOS:000186305800002 ER PT J AU Olson, MA Huang, Y Li, DS Spindler, R Howard, J Zhang, HM Durrant, B AF Olson, MA Huang, Y Li, DS Spindler, R Howard, J Zhang, HM Durrant, B TI Assessment of motility, acrosomal integrity, and viability of giant panda (Ailuropoda melanoleuca) sperm following short-term storage at 4 degrees C SO ZOO BIOLOGY LA English DT Article DE semen; nonfrozen storage; artificial insemination; caffeine ID ARTIFICIAL-INSEMINATION; BOVINE SEMEN; RAM SEMEN; SPERMATOZOA; CRYOPRESERVATION; FERTILITY; PRESERVATION; FRESH; EXTENDERS; CAFFEINE AB Short-term cool storage of semen affords many of the same benefits as cryopreservation, without the extensive cryoinjury to sperm associated with freezing. Semen storage for artificial insemination (AI) is an integral part of giant panda captive breeding programs. AI functions to generate offspring from males that have never bred, are underrepresented, or are unable to breed with genetically desirable females due to geographic separation. In the present study, semen was collected by electroejaculation from six giant pandas and extended in four media (TEST with 0% or 5% glycerol, or SFS with 0% or 5% glycerol). Subsequently, initial motility (MOT), speed of progression (SOP), percent live (% L), and percent normal acrosome (% NAR) values were recorded. These parameters were assessed again at 4, 8, 24, and 48 hr of incubation at 4degreesC in each medium. Motility scores (MS) were calculated as MOT x SOP2. The MS of each sample was also recorded after the addition of 20 mM caffeine. Results were expressed as a percent of the initial value (% 1). Although all three parameters decreased over time, the MS decreased at a faster rate than either the % L or the % NAR. There were significant differences between individual pandas for each measured parameter, while only % IMS was significantly affected by medium (P=.0006). The addition of caffeine increased % IMS at all time periods and reduced the differences between media to nonsignificant levels. The addition of glycerol was not beneficial for short-term semen storage. These data indicate that storage of giant panda semen at 4degreesC for up to 48 hr maintains sperm viability at a level sufficient for use in an AI program. Zoo Biol 22:529-544, 2003. (C) 2003 Wiley-Liss, Inc. C1 Zool Soc San Diego, Ctr Reprod Endangered Species, San Diego, CA 92112 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. RP Durrant, B (reprint author), Zool Soc San Diego, Ctr Reprod Endangered Species, POB 120551, San Diego, CA 92112 USA. EM bdurrant@ucsd.edu NR 35 TC 6 Z9 6 U1 1 U2 5 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2003 VL 22 IS 6 BP 529 EP 544 DI 10.1002/zoo.10113 PG 16 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 763VF UT WOS:000188120600002 ER PT J AU Tarou, LR Bashaw, MJ Maple, TL AF Tarou, LR Bashaw, MJ Maple, TL TI Failure of a chemical spray to significantly reduce stereotypic licking in a captive giraffe SO ZOO BIOLOGY LA English DT Article DE abnormal behavior; oral stereotypies; aversive conditioning; giraffe; animal welfare ID BEHAVIOR; CAMELOPARDALIS; RESTRICTION; SEPARATION; DURATION; HEIFERS; SOWS AB The repetitive licking of nonfood substrates is a common stereotypic behavior in captive giraffes. In this study we attempted to reduce stereotypic licking in a Masai giraffe (Giraffa camelopardalis tippelskirchi) by applying a bitter chemical (marketed as a taste deterrent to prevent the unwanted licking and chewing of substrates) to the areas of the fence licked most frequently by the giraffe. We hypothesized that this treatment would reduce stereotypic licking. However, there were no significant overall changes in stereotypic licking following treatment with the chemical spray. Although licking of the treated area was observed to decrease, the behavior increased in nontreated areas. These results suggest that the underlying motivation driving the behavior was not affected by the aversive stimulus. Because stereotypic licking in giraffes may be based on a motivation to use their tongues in foraging, more effective techniques for reducing stereotypic fence-licking in giraffes may include increasing feeding duration by increasing the quantity, processing time, or distribution range of food. Zoo Biol 22:601-607, 2003. (C) 2003 Wiley-Liss, Inc. C1 Zoo Atlanta, TECHlab, Atlanta, GA USA. Georgia Inst Technol, Sch Psychol, Atlanta, GA 30332 USA. Smithsonian Natl Zool Pk, Washington, DC USA. San Diego Wild Anim Pk, Ctr Reprod Endangered Species, San Diego, CA USA. RP Tarou, LR (reprint author), Grand Valley State Univ, Dept Psychol, 1 Campus Dr,2112 Au Sable Hall, Allendale, MI 49401 USA. EM taroul@gvsu.edu NR 22 TC 6 Z9 6 U1 1 U2 22 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2003 VL 22 IS 6 BP 601 EP 607 DI 10.1002/zoo.10114 PG 7 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 763VF UT WOS:000188120600007 ER PT J AU Smith, DG AF Smith, DG TI Eugenia Brandt Bohlke 1928-2001 - Obitaury SO COPEIA LA English DT Biographical-Item C1 Smithsonian Inst, NMNH, Washington, DC 20013 USA. RP Smith, DG (reprint author), Smithsonian Inst, NMNH, POB 37012,MRC 159, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD DEC 31 PY 2002 IS 4 BP 1175 EP 1179 PG 5 WC Zoology SC Zoology GA 632TF UT WOS:000180238400036 ER PT J AU Kanzawa, H Schiller, C Ovarlez, J Camy-Peyret, C Payan, S Jeseck, P Oelhaf, H Stowasser, M Traub, WA Jucks, KW Johnson, DG Toon, GC Sen, B Blavier, JF Park, JH Bodeker, GE Pan, LL Sugita, T Nakajima, H Yokota, T Suzuki, M Shiotani, M Sasano, Y AF Kanzawa, H Schiller, C Ovarlez, J Camy-Peyret, C Payan, S Jeseck, P Oelhaf, H Stowasser, M Traub, WA Jucks, KW Johnson, DG Toon, GC Sen, B Blavier, JF Park, JH Bodeker, GE Pan, LL Sugita, T Nakajima, H Yokota, T Suzuki, M Shiotani, M Sasano, Y TI Validation and data characteristics of water vapor profiles observed by the Improved Limb Atmospheric Spectrometer (ILAS) and processed with the version 5.20 algorithm SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE water vapor; polar stratosphere; validation; satellite sensor; Improved Limb Atmospheric Spectrometer (ILAS) ID POLAR STRATOSPHERIC CLOUDS; GAS EXPERIMENT-II; BALLOON-BORNE; TRACE GASES; SAGE II; OZONE; H2O; TROPOSPHERE; HYGROMETER; AEROSOL AB [1] Vertical profiles of water vapor concentration at high latitudes (57-72 degreesN; 64-89 degreesS) were observed by the Improved Limb Atmospheric Spectrometer (ILAS) solar occultation sensor aboard the Advanced Earth Observing Satellite (ADEOS). These measurements were made continuously from November 1996 through June 1997 with some additional periods in September to October 1996. A validation study of the water vapor data processed with the version 5.20 ILAS retrieval algorithm is presented in this paper. Uncertainty and general characteristics of the ILAS water vapor measurements are briefly reviewed. Comparisons are made with data obtained by (1) the ILAS validation balloon campaigns at Kiruna, Sweden and at Fairbanks, Alaska; (2) the aircraft measurements under the Photochemistry of Ozone Loss in the Arctic Region in Summer (POLARIS) campaign; and (3) available satellite measurements of the version 19 Halogen Occultation Experiment (HALOE) and the version 6 Stratospheric Aerosol and Gas Experiment II (SAGE II). The agreement between ILAS water vapor and all independent reliable correlative measurements in the altitude region of 15-60 km is better than 10% for the majority of cases and better than 20% for all comparisons, with the exception of some isolated cases detailed in this paper. Climatological comparisons of ILAS data with Upper Atmosphere Research Satellite (UARS) climatology and HALOE data show the overall consistency of ILAS water vapor data considering the known features of atmospheric circulation. The characteristics of ILAS measurements, i.e., high sampling frequency in polar latitudes with high vertical resolution along with the good data quality, make the ILAS water vapor data set valuable for various polar stratospheric research applications. C1 Natl Inst Environm Studies, Tsukuba, Ibaraki 3050053, Japan. Forschungszentrum Julich, Inst Stratosphaer Chem, D-52425 Julich, Germany. Ecole Polytech, CNRS, Meteorol Dynam Lab, F-91128 Palaiseau, France. Univ Paris 06, CNRS, Lab Phys Mol & Applicat, F-75252 Paris 05, France. Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Inst Water & Atmospher Res, Lauder, New Zealand. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Hokkaido Univ, Grad Sch Environm Earth Sci, Sapporo, Hokkaido 060, Japan. RP Kanzawa, H (reprint author), Natl Inst Environm Studies, 16-2 Onogawa, Tsukuba, Ibaraki 3050053, Japan. EM kanzawa@nies.go.jp; c.schiller@fz-juelich.de; Joelle.ovarlez@polytechnique.fr; camy@ccr.jussieu.fr; payan@ccr.jussieu.fr; jeseck@ccr.jussieu.fr; hermann.oelhaf@imk.fzk.de; markus.stowasser@imk.fzk.de; wtraub@cfa.harvard.edu; kjucks@cfa.harvard.edu; d.g.johnson@larc.nasa.gov; toon@mark4sun.jpl.nasa.gov; sen@mark4sun.jpl.nasa.gov; Jean.F.Blavier@jpl.nasa.gov; j.h.park@larc.nasa.gov; g.bodeker@niwa.cri.nz; liwen@ucar.edu; tsugita@nies.go.jp; hide@nies.go.jp; yoko@nies.go.jp; suzuki@eorc.nasda.go.jp; shiotani@kurasc.kyoto-u.ac.jp; sasano@nies.go.jp RI Pan, Laura/A-9296-2008; Sasano, Yasuhiro/C-2927-2009; Oelhaf, Hermann/A-7895-2013; Schiller, Cornelius/B-1004-2013; Johnson, David/F-2376-2015 OI Pan, Laura/0000-0001-7377-2114; Sasano, Yasuhiro/0000-0001-7470-5642; Johnson, David/0000-0003-4399-5653 NR 63 TC 16 Z9 16 U1 0 U2 2 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 DEC 31 PY 2002 VL 107 IS D24 AR 8217 DI 10.1029/2001JD000881 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 650KF UT WOS:000181262000001 ER PT J AU Petit, RE Harasewych, MG AF Petit, RE Harasewych, MG TI A new Trigonostoma (Neogastropoda : Cancellariidae) from Mozambique SO NAUTILUS LA English DT Article DE Indian Ocean; Gastropoda Scalptia ID SOUTH-AFRICA AB Trigonostoma mozambicense is described from the outer continental shelf off southern Mozambique. This new species is readily distinguished from its congeners by its combination of small adult size, its thick shell with coarsely fenestrated surface sculpture, a narrow umbilicus lined with spiral cords as well as the presence of strong but shallow apertural lirae between the suture and shoulder, and along the outer lip. This new species is provisionally assigned to the genus Trigonostoma based on characters traditionally used to define the genus, while its affinity to a western African species that has been included in the genus Scalptia is also recognized. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Petit, RE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 11 TC 2 Z9 2 U1 0 U2 0 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 DEC 31 PY 2002 VL 116 IS 4 BP 129 EP 131 PG 3 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 632UX UT WOS:000180242800003 ER PT J AU Bodo, E Scifoni, E Sebastianelli, F Gianturco, FA Dalgarno, A AF Bodo, E Scifoni, E Sebastianelli, F Gianturco, FA Dalgarno, A TI Rotational quenching in ionic systems at ultracold temperatures SO PHYSICAL REVIEW LETTERS LA English DT Article ID ATOM-MOLECULE COLLISIONS; VIBRATIONAL-RELAXATION; CLUSTER IONS; RARE-GAS; SCATTERING; CONDENSATE; STABILITY; HE-3; CO AB The behavior of the rotational quenching for a molecular ion in collision with closed-shell neutral gases is investigated. We confirm that Wigner's threshold law for inelastic scattering holds in the presence of a long-range interaction due to polarization forces decreasing as the inverse fourth power of the distance but find that, because of the contributions of the higher angular momenta, its range of applicability is markedly reduced when compared to the scattering by neutral species. The calculations of the quenching cross sections make evident the special features of ionic systems at ultralow collision energies and yield rate coefficients of the order of 10(-9) cm(3) s(-1), much larger than those found for the quenching of neutral molecules. C1 Univ Roma La Sapienza, Dept Chem, I-00185 Rome, Italy. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Gianturco, FA (reprint author), Univ Roma La Sapienza, Dept Chem, PA Moro 5, I-00185 Rome, Italy. RI Bodo, Enrico/F-4375-2012; Scifoni, Emanuele/B-5277-2013; sebastianelli, francesco/B-5718-2014 OI Scifoni, Emanuele/0000-0003-1851-5152; NR 39 TC 19 Z9 19 U1 0 U2 2 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 DEC 31 PY 2002 VL 89 IS 28 AR 283201 DI 10.1103/PhysRevLett.89.283201 PG 4 WC Physics, Multidisciplinary SC Physics GA 634AM UT WOS:000180317900016 PM 12513141 ER PT J AU Rasse, DP Stolaki, S Peresta, G Drake, BG AF Rasse, DP Stolaki, S Peresta, G Drake, BG TI Patterns of canopy-air CO2 concentration in a brackish wetland: analysis of a decade of measurements and the simulated effects on the vegetation SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE carbon dioxide concentration; CO2 rise; diurnal CO2 cycles; wetland modelling; Scirpus ID WATER-VAPOR EXCHANGE; CARBON-DIOXIDE; ATMOSPHERIC CO2; ELEVATED CO2; CLIMATE-CHANGE; ESTUARINE MARSH; FOREST; MODEL; PHOTOSYNTHESIS; ECOSYSTEM AB Photosynthetic carbon assimilation is dependent on the canopy-air CO2 concentration (Ca), which is an essential driving parameter of mechanistic models built to predict plant responses to changing environmental conditions. Short-term studies have shown that crop-canopy Ca undergoes substantial diurnal and seasonal variations as compared to Ca values measured several meters above plant canopies in well mixed conditions. Whether these canopy Ca patterns measured in crops also apply to wetland plant canopies and over long periods of time remains largely unknown. The first objective of this study was to analyze the consistency of short- and long-term Ca patterns in salt marsh canopies over a 10-year period. The second objective was to assess the impact of these canopy Ca patterns on simulated ecosystem productivity. In this study, we used Ca data collected from 1990 to 2000 in salt marsh canopies of the Chesapeake Bay, Maryland. The possible effects of short- and long-term canopy Ca patterns on plant productivity were simulated with a mechanistic model specifically adapted to the Scirpus olneyi vegetation of the salt marsh ecosystem. The annual average of daytime canopy Ca of a brackish marsh community rose by a significant (P < 0.01) 1.55 mumol CO2 mol(-1) year(-1) between 1990 and 2000, which parallels the atmospheric records of Mauna Loa over the same period of time. Annual Ca averages displayed some variability around this trend, which were highly correlated with the year-to-year variation in aboveground plant biomass (r(2) = 0.83, P < 0.001). Therefore, our study demonstrated that aboveground plant biomass is the main driver for inter-annual canopy Ca fluctuations. Daytime canopy Ca displayed maximum values in May and September and minimum values in July, with an amplitude of about 20 mumol CO2 mol(-1). The amplitude of the diurnal Ca cycle measured at the wetland appeared similar to that of North American agricultural ecosystems, exceeding 100 mumol CO2 mol(-1) in July and August and characterized by a sharp drop in the CO2 concentration shortly after dawn. Model simulations suggested that the increase in canopy Ca from 1990 to 2000 resulted in a substantial increase in Scirpus gross plant productivity (GPP) of 0.31% per year, which confirms that plant ecosystem simulations need to consider the actual increase in canopy Ca when the simulated time period exceeds a few years. Forcing the model with the measured diurnal Ca pattern increased the simulated net plant productivity (NPP) immediately after dawn and decreased it for the rest of the daytime period, which resulted in a simulated net NPP decrease of about 5% over the growing season. Published by Elsevier Science B.V. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Liege, B-4001 Liege, Belgium. RP Drake, BG (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. OI Daniel, Rasse/0000-0002-5977-3863 NR 33 TC 7 Z9 9 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD DEC 30 PY 2002 VL 114 IS 1-2 BP 59 EP 73 AR PII S0168-1923(02)00135-1 DI 10.1016/S0168-1923(02)00135-1 PG 15 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 621YF UT WOS:000179618000005 ER PT J AU Olson, SL Alvarenga, HMF AF Olson, SL Alvarenga, HMF TI A new genus of small teratorn from the middle tertiary of the Taubate Basin, Brazil (Aves : Teratornithidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new genus and species of Teratornithidae, Taubatornis campbelli, is described from deposits of the Tremembe Formation of Upper Oligocene or Lower Miocene age in the Taubate Basin of Sao Paulo State, Brazil. These fossils are much older (ca. 25 mya) than the next oldest known teratorn, Argentavis magnificens, from the late Miocene of Argentina (ca. 6 mya), and uphold the hypothesized origin of the Teratornithidae in South America. Taubatornis campbelli was smaller than other known species of the family and, as with most other occurrences of teratorns, was found syntopic with fossils of New World vultures of the family Cathartidae (Vulturidae auct.). C1 Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. Museu Hist Nat Taubate, BR-12030520 Taubate, SP, Brazil. RP Olson, SL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. NR 16 TC 4 Z9 4 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 30 PY 2002 VL 115 IS 4 BP 701 EP 705 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 632PA UT WOS:000180230700001 ER PT J AU Breedy, O Guzman, HM AF Breedy, O Guzman, HM TI A revision of the genus Pacifigorgia (Coelenterata : Octocorallia : Gorgoniidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID COLONY MORPHOLOGY; LEPTOGORGIA; CORAL AB The genus Pacifigorgia is revised based on original type-specimens and new specimens recently collected. In addition to P. irene Bayer and P. bayeri Breedy, which are the only well defined, seventeen other species are recognized as valid (P. adamsii, P. agassizii, P. arenata, P. cribrum, P. darwinii, P. douglasii, P. elegans, P. englemanni, P. exilis, P. eximia, P. gracilis, P. media, P. pulchra, P. rutila, P. stenobrochis, and P. tabogae). The species are described and illustrated in detail with photomicrographs and scanning electron micrographs of the sclerites. Lectotypes are proposed for eight species. C1 CIMAR, Cent Investigac Ciencias Mar & Limnol, San Jose, Costa Rica. Smithsonian Trop Res Inst, Balboa, Panama. RP Breedy, O (reprint author), CIMAR, Cent Investigac Ciencias Mar & Limnol, POB 1962-2100, San Jose, Costa Rica. NR 47 TC 17 Z9 19 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 DEC 30 PY 2002 VL 115 IS 4 BP 782 EP 839 PG 58 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 632PA UT WOS:000180230700011 ER PT J AU Cairns, SD Bayer, FM AF Cairns, SD Bayer, FM TI Studies on western Atlantic Octocorallia (Coelenterata : Anthozoa). Part 2: The genus Callogorgia Gray, 1858 SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Of the three species of Callogorgia now recognized in the western Atlantic, one that had been misidentified as Callogorgia verticillata, an eastern Atlantic and Mediterranean species, is now established as a new species in its own right, comprised of two subspecies. A second, C gracilis, originally reported from Guadeloupe, is redescribed on the basis of type material and additional specimens. A third species, C. linguimaris, is described as new. Records of all three species preserved in the collection of the National Museum of Natural History, Washington, D.C., are reported, and the species are illustrated by scanning electron micrography. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Invertebrate Zool, Washington, DC 20013 USA. RP Cairns, SD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Invertebrate Zool, POB 37012, Washington, DC 20013 USA. NR 23 TC 8 Z9 10 U1 1 U2 1 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 DEC 30 PY 2002 VL 115 IS 4 BP 840 EP 867 PG 28 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 632PA UT WOS:000180230700012 ER PT J AU Robinson, H Holmes, WC AF Robinson, H Holmes, WC TI New species of Mikania from Ecuador (Eupatorieae : Asteraceae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Mikania campii, M. discifera, M. dodsonii, M. farsiliflora, M. fosbergii, M. gunnarii, M. houstonioides, M. matezkii, M. ollgaardii, M. pruskii, M. rimbachioides, M. sparrei, M. websteri, and M. yanacochensis, M. zamorae are described as entirely new and M. psylobothrya Sodiro, nom. nud., is validated. C1 Natl Museum Nat Hist, Smithsonian Inst, MRC 166, Washington, DC 20013 USA. Baylor Univ, Dept Biol, Waco, TX 76798 USA. RP Robinson, H (reprint author), Natl Museum Nat Hist, Smithsonian Inst, MRC 166, POB 37012, Washington, DC 20013 USA. NR 5 TC 2 Z9 2 U1 0 U2 1 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 DEC 30 PY 2002 VL 115 IS 4 BP 878 EP 908 PG 31 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 632PA UT WOS:000180230700014 ER PT J AU Panero, JL Funk, VA AF Panero, JL Funk, VA TI Toward a phylogenetic subfamilial classification for the Compositae (Asteraceae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID SYSTEMATIC-POSITION; CHLOROPLAST DNA; HELIANTHEAE; SEQUENCES; NDHF AB Molecular studies of the flowering plant family Compositae (Asteraceae) based on comparative DNA sequence data of chloroplast genes provide new insights into the evolution and radiation of the family. The results support the creation of new groups to maintain a classification that reflects evolutionary history. We are proposing the following new names: subfamilies Corymbioideae, Gochnatioideae, Gymnarrhenoideae, Hecastocleoideae, and Pertyoideae; tribes Athroismeae, Corymbieae, Dicomeae, Gochnatieae, Gymnarrheneae, Hecastocleideae, Polymnieae; subtribe Rojasianthinae. The totals now stand at I I subfamilies and 35 tribes. Only one tribe, the Mutisieae, is non-monophyletic having two branches. Most of the new groups are derived from taxa included in tribe Mutisieae, long suspected to be a paraphyletic group. Molecular studies that support these changes are discussed elsewhere but a summary of their results is presented. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Inst, US Natl Herbarium, NMNH, MRC 166, Washington, DC 20013 USA. RP Panero, JL (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. NR 32 TC 94 Z9 108 U1 3 U2 27 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 DEC 30 PY 2002 VL 115 IS 4 BP 909 EP 922 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 632PA UT WOS:000180230700015 ER PT J AU Bartschat, K Grum-Grzhimailo, AN AF Bartschat, K Grum-Grzhimailo, AN TI Vector (e, e 'gamma) correlations in ionization-excitation of He by electron impact SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID DIFFERENTIAL CROSS-SECTIONS; R-MATRIX METHOD; HELIUM-ATOMS; STATE; ALIGNMENT; ORIENTATION; EMISSION; POLARIZATION; SCATTERING; COLLISIONS AB The general description of simultaneous electron-impact ionization-excitation processes is reformulated in,terms of an irreducible tensor representation., Using a numerical model, in which the interaction between a 'fast' ionizing projectile and the target is described by first- or second-order plane-wave and distorted-wave models, combined with a convergent close-coupling-type description of the initial bound state and the- interaction between a 'slow' ejected electron and the residual ion, new benchmark calculations for the (e, e'gamma) process have been performed. The predictions are compared with recent experimental data on ionization-excitation of helium. The similarity to results' for excitation processes and the potential extension of propensity rules is discussed. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Moscow MV Lomonosov State Univ, Inst Phys Nucl, Moscow 119992, Russia. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Bartschat, K (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Grum-Grzhimailo, Alexei/D-6274-2012; Bartschat, Klaus/I-2527-2012 NR 48 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD DEC 28 PY 2002 VL 35 IS 24 BP 5035 EP 5050 AR PII S0953-4075(02)52741-3 DI 10.1088/0953-4075/35/24/308 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 639LD UT WOS:000180629500012 ER PT J AU Biava, DA Bartschat, K Saha, HP Madison, DH AF Biava, DA Bartschat, K Saha, HP Madison, DH TI Accuracy of local exchange in the calculation of continuum wavefunctions SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID ELECTRON-IMPACT IONIZATION; DIFFERENTIAL CROSS-SECTIONS; E,2E COLLISIONS; HARTREE-FOCK; POLARIZED ELECTRONS; LOW ENERGIES; SCATTERING; XENON; ARGON; ATOMS AB It is well known that electron exchange can-play an important role in electron impact elastic, inelastic and ionization scattering from atoms and molecules. The proper theoretical treatment of exchange yields an inhomogeneous differential equation with a non-local exchange operator. To simplify the calculation, a local approximation is often made for this non-local operator. In this paper, we examine the accuracy of this approximation for the calculation of elastic scattering continuum waves in the presence of an argon ion with a single vacancy in the p-shell. It is found that one can. reliably use the local exchange approximation for ionization leading to s-state vacancies but not p state vacancies. C1 Univ Missouri, Dept Phys, Rolla, MO 65409 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Biava, DA (reprint author), Univ Missouri, Dept Phys, Rolla, MO 65409 USA. RI Bartschat, Klaus/I-2527-2012 NR 27 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD DEC 28 PY 2002 VL 35 IS 24 BP 5121 EP 5130 AR PII S0953-4075(02)39419-7 DI 10.1088/0953-4075/35/24/313 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 639LD UT WOS:000180629500017 ER PT J AU Britzi, R Johnson, GD AF Britzi, R Johnson, GD TI "Paradox lost": Skeletal ontogeny of Indostomus paradoxus and its significance for the phylogenetic relationships of indostomidae (Teleostei, Gasterosteiformes) - Introduction SO AMERICAN MUSEUM NOVITATES LA English DT Article ID OSTEOLOGICAL DEVELOPMENT; FISHES AB On the basis of an ontogenetic series of Indostomus paradoxus, we test characters that have been proposed for the phylogenetic placement of this enigmatic taxon, Contrary to previous authors, we found that the body armor of Indostomus differs from that of syngnathoids greatly and it closely resembles that of gasterosteoids in many unique details, The bud plates originate from two different sources. that is, the endoskeleton (proximal-middle radials of dorsal and anal fin, neural and hemal spines, pelvic cartilages) and the exoskeleton (postcleithra, lateral body plates, sternal plate). The median bone in the ethinoid region develop.,, from two centers and most likely represents the nasal bones that fuse during ontogeny with each other and with the vomer. Identity of the opercular bones is clarified, and it is demonstrated that Indostomus has an interopercle. The single pterygoid bone is the ectopterygoid. A parietal is lacking. There is only one cartilaginously preformed hypural element in the caudal fin. There is no parhypural, but a similar structure, termed the pseudoparhypural by us, develops as membranous outgrowths of the single hypural and the ural centrum, The pectoral radial plate fuses to the scapulocoracoid cartilage, and the pectoral radials ossify within that fused plate without prior fragmentation of the plate into individual radials, being specializations of the pectoral girdle that we think to be shared with all gasterosteoids, Indostomus shares with other gasterosteiforms the modification of the tripartite occipital condyle into tin articulation of the basioccipital and the first centrum through loss of the articulation between exoccipitals and the first centrum in all developmental stages. Indostomus lacks distal radials in all pterygiophores supporting fin spines at all developmental stages, a character shared with other gasterosteiforms, mastacembelids, and probably other smegmamorphs, We conclude that Indostomus is a gasterosteoid gasterosteiform. C1 Univ Tubingen, Lehrstuhl Spezielle Zool, D-72076 Tubingen, Germany. Amer Museum Nat Hist, Div Vertebrate Zool Ichthyol, New York, NY 10024 USA. Smithsonian Inst, Natl Museum Amer Hist, Div Fishes, Washington, DC 20560 USA. RP Britzi, R (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Div Fishes, Washington, DC 20560 USA. EM Britz.Ralf@nmnh.si.edu; Johnson.Dave@nmnh.si.edu NR 34 TC 21 Z9 23 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 DEC 27 PY 2002 IS 3383 BP 1 EP 43 DI 10.1206/0003-0082(2002)383<0001:PLSOOI>2.0.CO;2 PG 43 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 630UE UT WOS:000180127400001 ER PT J AU Smith, HA AF Smith, HA TI Why astronomy is the star of the news show SO NATURE LA English DT Letter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 26 PY 2002 VL 420 IS 6917 BP 740 EP 740 DI 10.1038/420740b PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 626WR UT WOS:000179897300028 PM 12490919 ER PT J AU Blackman, EG Field, GB AF Blackman, EG Field, GB TI New dynamical mean-field dynamo theory and closure approach SO PHYSICAL REVIEW LETTERS LA English DT Article ID TURBULENT DYNAMOS; MAGNETIC HELICITY; ALPHA; ELECTRODYNAMICS; CONSTRAINTS AB We develop a new nonlinear mean field dynamo theory that couples field growth to the time evolution of the magnetic helicity and the turbulent electromotive force, (ε) over bar. We show that the difference between kinetic and current helicities emerges naturally as the growth driver when the time derivative of (ε) over bar is coupled into the theory. The solutions predict significant field growth in a kinematic phase and a saturation rate/strength that is magnetic Reynolds number dependent/independent in agreement with numerical simulations. The amplitude of early time oscillations provides a diagnostic for the closure. C1 Univ Rochester, Dept Phys & Astron 1, 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 1, Rochester, NY 14627 USA. NR 31 TC 109 Z9 109 U1 0 U2 2 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 DEC 23 PY 2002 VL 89 IS 26 AR 265007 DI 10.1103/PhysRevLett.89.265007 PG 4 WC Physics, Multidisciplinary SC Physics GA 626NC UT WOS:000179878200029 PM 12484833 ER PT J AU Fassnacht, CD Xanthopoulos, E Koopmans, LVE Rusin, D AF Fassnacht, CD Xanthopoulos, E Koopmans, LVE Rusin, D TI A determination of H-0 with the CLASS gravitational lens B1608+656. III. A significant improvement in the precision of the time delay measurements SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; galaxies : individual (B1608+656); gravitational lensing ID HUBBLE-CONSTANT; LIGHT-CURVE; REDSHIFTS; GALAXY; QSO-0957+561; PG-1115+080; B1600+434; 0957+561A; B1422+231; OBJECTS AB The gravitational lens CLASS B1608+656 is the only four-image lens system for which all three independent time delays have been measured. This makes the system an excellent candidate for a high-quality determination of H-0 at cosmological distances. However, the original measurements of the time delays had large (12%-20%) uncertainties, due to the low level of variability of the background source during the monitoring campaign. In this paper, we present results from two additional VLA monitoring campaigns. In contrast to the similar to5% variations seen during the first season of monitoring, the source flux density changed by 25%-30% in each of the subsequent two seasons. We analyzed the combined data set from all three seasons of monitoring to improve significantly the precision of the time delay measurements; the delays are consistent with those found in the original measurements, but the uncertainties have decreased by factors of 2-3. We combined the delays with revised isothermal mass models to derive a measurement of H-0. Depending on the positions of the galaxy centroids, which vary by up to 0."1 in Hubble Space Telescope ( HST) images obtained with different filters, we obtain H-0 = 61-65 km s(-1) Mpc(-1), for (Omega(M), Omega(Lambda)) = 0.3; 0.7). The value of H-0 decreases by 6% if (Omega(M), Omega(Lambda)) = (1.0, 0.0). The formal uncertainties on H-0 due to the time-delay measurements are +/-1(+/-2) km s(-1) Mpc(-1) for the 1 sigma(2sigma) confidence limits. Thus, the systematic uncertainties due to the lens model, which are on the order of +/-15 km s(-1) Mpc(-1), now dominate the error budget for this system. In order to improve the measurement of H-0 with this lens, new models that incorporate the constraints provided by stellar dynamics and the optical/infrared Einstein ring seen in HST images must be developed. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fassnacht, CD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. NR 62 TC 88 Z9 88 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 DEC 20 PY 2002 VL 581 IS 2 BP 823 EP 835 DI 10.1086/344368 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DA UT WOS:000179914300006 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, JSB Loeb, A TI A physical model for the luminosity function of high-redshift quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : general ID DIGITAL-SKY-SURVEY; BLACK-HOLES; GRAVITATIONAL LENSES; EVOLUTION; GALAXIES; DISTRIBUTIONS; STATISTICS; POPULATION; MERGERS; FIELDS AB We provide a simple theoretical model for the quasar luminosity function at high redshifts that naturally reproduces the statistical properties of the luminous Sloan Digital Sky Survey (SDSS) quasar sample at redshifts z similar to 4.3 and z greater than or similar to 5.7. Our model is based on the assumptions that quasar emission is triggered by galaxy mergers and that the black hole mass is proportional to a power law in the circular velocity of the host galactic halo, v(c). We assume that quasars shine at their Eddington luminosity over a time proportional to the mass ratio between the small and final galaxies in the merger. This simple model fits the quasar luminosity function at z similar to 2-3, reproduces the normalization and logarithmic slope (beta similar to 2.58) at z similar to 4.3, explains the space density of bright SDSS quasars at z similar to 6.0, reproduces the black hole-halo mass relation for dormant black holes in the local universe, and matches the inferred duty cycle of quasar activity (similar to10(7) yr) in Lyman break galaxies at z similar to 3. An acceptable fit to all of these constraints requires 0.7 less than or similar to sigma(8) less than or similar to 1.0. Based on the derived luminosity function, we predict the resulting gravitational lensing rates for high-redshift quasars. The lens fractions in the SDSS samples are predicted to be similar to2% at z similar to 4.3 and similar to8% at z greater than or similar to 5.7. It is interesting to note that the limiting quasar luminosity in our best-fit relation L proportional to 5 nu(c)(5)/G scales as the binding energy of the host galaxy divided by its dynamical time, implying that feedback is the mechanism that regulates black hole growth in galactic potential wells. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wyithe, JSB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wyithe, Stuart/0000-0001-7956-9758 NR 46 TC 102 Z9 102 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 DEC 20 PY 2002 VL 581 IS 2 BP 886 EP 894 DI 10.1086/344249 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DA UT WOS:000179914300011 ER PT J AU Hardcastle, MJ Birkinshaw, M Cameron, RA Harris, DE Looney, LW Worrall, DM AF Hardcastle, MJ Birkinshaw, M Cameron, RA Harris, DE Looney, LW Worrall, DM TI Magnetic field strengths in the hot spots and lobes of three powerful Fanaroff-Riley type II radio sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (3C 263, 3C 351, 3C 330); quasars : general; radiation mechanisms : nonthermal; X-rays : galaxies ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; CYGNUS-A; CHANDRA OBSERVATIONS; SYNCHROTRON SPECTRA; 3CR QUASARS; PICTOR-A; GALAXIES; JET; DISCOVERY AB We have made deep Chandra observations of three powerful Fanaro-Riley type II (FR II) radio sources: two quasars (3C 263 and 3C 351) and one radio galaxy ( 3C 330). X-ray emission from hot spots and lobes, as well as from the active nucleus, is detected in each source. We model the hot spots synchrotron spectra using VLA, BIMA, and Hubble Space Telescope data. In 3C 263 and 3C 330, the hot spots X-ray emission is at a level consistent with being synchrotron self-Compton (SSC) emission, with a hot spot magnetic field close to the equipartition value. In the two hot spots of 3C 351, however, an SSC origin for the X-rays would require the magnetic field strength to be an order of magnitude below the equipartition value in our models; in addition, there are offsets between the radio, optical, and X-ray emission from the secondary hot spot that are hard to explain in a simple SSC model. We discuss the emission mechanisms that may be responsible for these observations. On our preferred model, the X-ray emission from the radio lobes of the three sources is due to inverse Compton scattering of the microwave background radiation. If this is the case, the magnetic field strengths in the lobes are typically about a factor of 2 below the equipartition values, assuming uniform lobe electron and magnetic field distributions. We detect extended X-ray emission, which we attribute to a cluster/group environment, around 3C 263 and 3C 330. This detection allows us to show that the lobes are close to pressure balance with their surroundings, as long as no nonradiating particles contribute to the internal pressure of the lobes. C1 Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. RP Univ Bristol, Dept Phys, Tyndall Ave, Bristol BS8 1TL, Avon, England. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 70 TC 101 Z9 101 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 DEC 20 PY 2002 VL 581 IS 2 BP 948 EP 973 DI 10.1086/344409 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DA UT WOS:000179914300016 ER PT J AU Clements, DL McDowell, JC Shaked, S Baker, AC Borne, K Colina, L Lamb, SA Mundell, C AF Clements, DL McDowell, JC Shaked, S Baker, AC Borne, K Colina, L Lamb, SA Mundell, C TI Chandra observations of ARP 220: The nuclear source SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Arp 220); galaxies : interactions; galaxies : starburst; X-rays : galaxies ID ULTRALUMINOUS INFRARED GALAXIES; MU-M; ARP-220; STARBURST; EMISSION; ULIRGS; QUASAR; ISO AB We present the first results from 60 ks of observations of Arp 220 using the ACIS-S instrument on Chandra. We report the detection of several sources near the galaxy's nucleus, including a point source with a hard spectrum that is coincident with the western radio nucleus B. This point source is mildly absorbed (N-H similar to 3 x 10(22) cm(-2)) and has an estimated luminosity of 4 x 10(40) ergs s(-1). In addition, a fainter source may coincide with the eastern nucleus A. Extended hard X-ray emission in the vicinity raises the total estimated nuclear 2-10 keV X-ray luminosity to 1.2 x 10(41) ergs s(-1), but we cannot rule out a hidden active galactic nucleus behind columns exceeding 5 x 10(24) cm(-2). We also detect a peak of soft X-ray emission to the west of the nucleus and a hard point source 2.5 kpc from the nucleus with a luminosity of 6 x 10(39) ergs s(-1). C1 Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2BW, England. Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. NASA, Raytheon Informat Technol & Sci Serv, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CSIC, Inst Estructura Mat, E-28006 Madrid, Spain. Univ Illinois, Loomis Lab Phys, Ctr Theoret Astrophys, Dept Phys, Urbana, IL 61801 USA. Liverpool John Moores Univ, Astrophys Res Inst, Wirral CH41 1LD, Cheshire, England. Univ Illinois, Loomis Lab Phys, Ctr Theoret Astrophys, Dept Astron, Urbana, IL 61801 USA. RP Clements, DL (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Phys, Prince Consort Rd, London SW7 2BW, England. NR 43 TC 53 Z9 53 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 DEC 20 PY 2002 VL 581 IS 2 BP 974 EP 980 DI 10.1086/344439 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DA UT WOS:000179914300017 ER PT J AU Strelnitski, V Alexander, J Gezari, S Holder, BP Moran, JM Reid, MJ AF Strelnitski, V Alexander, J Gezari, S Holder, BP Moran, JM Reid, MJ TI H2O masers and supersonic turbulence SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : jets and outflows; masers; turbulence ID PROPER MOTIONS; DEVELOPED TURBULENCE; W49N; DISTANCE; CLOUDS; GALAXY; MODEL AB We use unpublished and published VLBI results to investigate the geometry and the statistical properties of the velocity field traced by H2O masers in five galactic regions of star formation: Sgr B-2(M), W49N, W51(MAIN), W51N, and W3(OH). In all sources the angular distribution of the H2O hot spots demonstrates approximate self-similarity (fractality) over almost 4 orders of magnitude in scale, with the calculated fractal dimension d between approximate to0.2 and 1.0. In all sources, the lower order structure functions for the line-of-sight component of the velocity field are satisfactorily approximated by power laws, with the exponents near their classic Kolmogorov values for high Reynolds number incompressible turbulence. These two facts, as well as the observed significant excess of large deviations of the two-point velocity increments from their mean values, strongly suggest that the H2O masers in regions of star formation trace turbulence. We propose a new conceptual model of these masers in which maser hot spots originate at the sites of ultimate dissipation of highly supersonic turbulence produced in the ambient gas by the intensive gas out flow from a newly born star. Because of the high brightness and small angular sizes of masing hot spots and the possibility of measuring their positions and velocities with high precision, they become a unique probe of supersonic turbulence. C1 Maria Mitchell Observ, Nantucket, MA 02554 USA. New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. Brown Univ, Providence, RI 02912 USA. Wesleyan Univ, Middletown, CT 06459 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Strelnitski, V (reprint author), Maria Mitchell Observ, 3 Vestal St, Nantucket, MA 02554 USA. NR 59 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2002 VL 581 IS 2 BP 1180 EP 1193 DI 10.1086/344244 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DA UT WOS:000179914300035 ER PT J AU Kastner, JH Li, JQ Vrtilek, SD Gatley, I Merrill, KM Soker, N AF Kastner, JH Li, JQ Vrtilek, SD Gatley, I Merrill, KM Soker, N TI On the asymmetries of extended X-ray emission from planetary nebulae SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary nebulae : individual (BD+30 degrees 3639, NGC 7027); stars : AGB and post-AGB; stars : mass loss; stars : winds, outflows; X-rays : ISM ID PHOTODISSOCIATION REGION; BD +30-DEGREES-3639; BD+30-DEGREES-3639; NGC-7027; RESOLUTION AB Chandra X-Ray Observatory (CXO) images have revealed that the X-ray-emitting regions of the molecule-rich young planetary nebulae (PNe) BD + 30degrees3639 and NGC 7027 are much more asymmetric than their optical nebulosities. To evaluate the potential origins of these X-ray asymmetries, we analyze X-ray images of BD + 30degrees3639, NGC 7027, and another PN resolved by CXO, NGC 6543, within specific energy bands. Image resolution has been optimized by subpixel repositioning of individual X-ray events. The resulting subarcsecond resolution images reveal that the soft (E < 0.7 keV) X-ray emission from BD + 30&DEG;3639 is more uniform than the harder emission, which is largely confined to the eastern rim of the optical nebula. In contrast, soft X-rays from NGC 7027 are highly localized and this PN is more axially symmetric in harder emission. The broadband X-ray morphologies of BD + 30&DEG;3639 and NGC 7027 are highly anticorrelated with their distributions of visual extinction, as determined from high-resolution, space-and ground-based optical and infrared imaging. Hence, it is likely that the observed X-ray asymmetries of these nebulae are due in large part to the effects of nonuniform intranebular extinction. However, the energy-dependent X-ray structures in both nebulae and NGC 6543-which is by far the least dusty and molecule-rich of the three PNe and displays very uniform intranebular extinction suggest that other mechanisms, such as the action of collimated outflows and heat conduction, are also important in determining the detailed X-ray morphologies of young PNe. C1 Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Dept Phys, IL-36006 Oranim, Tivon, Israel. RP Kastner, JH (reprint author), Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. NR 30 TC 23 Z9 23 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 DEC 20 PY 2002 VL 581 IS 2 BP 1225 EP 1235 DI 10.1086/344363 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DA UT WOS:000179914300038 ER PT J AU Bergin, EA Snell, RL AF Bergin, EA Snell, RL TI Sensitive limits on the water abundance in cold low-mass molecular cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : molecules; stars : formation ID WAVE-ASTRONOMY-SATELLITE; STAR-FORMATION; INITIAL CONDITIONS; EMISSION; CLOUDS; ABSORPTION; H2O; EXTINCTION; CHEMISTRY; REGIONS AB We present Submillimeter Wave Astronomy Satellite observations of water vapor in two cold starless clouds, B68 and core D in rho Ophiuchi. Sensitive nondetections of the 1(10)-1(01) transition of o-H2O are reported for each source. Both molecular cores have been previously examined by detailed observations that have characterized the physical structure. Using these rather well-defined physical properties and a Monte Carlo radiation transfer model, we have removed one of the largest uncertainties from the abundance calculation and set the lowest water abundance limit to date in cold low-mass molecular cores. These limits are x(o-H2O) <3 x 10(-8) (relative to H-2) and x(o-H2O) < in 8 x 10(-9) in B68 and rho Oph D, respectively. Such low abundances confirm the general lack of ortho-water vapor in cold (T < 20 K) cores. Provided that the ortho/para ratio of water is not near zero, these limits are well below theoretical predictions and appear to support the suggestion that most of the water in dense low-mass cores is frozen onto the surfaces of cold dust grains. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Bergin, EA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 30 TC 39 Z9 39 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 DEC 20 PY 2002 VL 581 IS 2 BP L105 EP L108 DI 10.1086/346014 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DB UT WOS:000179914500011 ER PT J AU Elvis, M Karovska, M AF Elvis, M Karovska, M TI Quasar parallax: A method for determining direct geometrical distances to quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; HUBBLE-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; ACCELERATING UNIVERSE; LUMINOSITY FUNCTION; STELLAR OBJECTS; EMISSION-LINES; NGC 5548; SUPERNOVAE AB We describe a novel method to determine direct geometrical distances to quasars that can measure the cosmological constant, Lambda, with minimal assumptions. This method is equivalent to geometric parallax, with the "standard length" being the size of the quasar broad emission line region (BELR) as determined from the light-travel time measurements of reverberation mapping. The effect of nonzero Lambda on angular diameter is large, 40% at z = 2, so mapping angular diameter distances versus redshift will give Lambda with (relative) ease. In principle, these measurements could be made in the UV, optical, near-infrared, or even X-ray bands. Interferometers with a resolution of 0.01 mas are needed to measure the size of the BELR in z = 2 quasars, which appear plausible given reasonable short-term extrapolations of current technology. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM elvis@cfa.harvard.edu NR 52 TC 27 Z9 27 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2002 VL 581 IS 2 BP L67 EP L70 DI 10.1086/346015 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DB UT WOS:000179914500002 ER PT J AU Kuraszkiewicz, JK Green, PJ AF Kuraszkiewicz, JK Green, PJ TI Evidence of a strong N v/C IV correlation between emission and absorption lines in active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : active; quasars : absorption lines; quasars : emission lines ID QUASI-STELLAR OBJECTS; CHEMICAL EVOLUTION; DISK WINDS; SYSTEMS; ABUNDANCES; REDSHIFT; SPECTRA; QSOS; SAMPLE AB The narrow absorption lines (NALs) that are seen in the rest-frame ultraviolet near the systemic redshift of active galactic nuclei (AGNs) are not always intrinsic to the near-nuclear region but may originate in the host galaxy or in neighboring galaxies intervening along the line of sight. A variety of criteria have been sought-and several identified-as evidence of an intrinsic origin. We have measured both emission and absorption lines in a Hubble Space Telescope Faint Object Spectrograph sample of objects with both C IV and N V NALs within +/-5000 km s(-1) of the systemic redshift. We find a strong (>99.5% confidence) linear correlation between the N V/C IV ratio in broad emission lines and that in NALs. A control sample of AGNs with NALs separated by larger velocities shows no such correlation. Our finding thus identifies an additional test for the intrinsic nature of NALs in any given object. The correlation shows that the chemical-enrichment histories and/or ionization parameters of the NAL clouds are closely related to those of clouds that produce the broad emission lines. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kuraszkiewicz, JK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 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 DEC 20 PY 2002 VL 581 IS 2 BP L77 EP L80 DI 10.1086/346017 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DB UT WOS:000179914500004 ER PT J AU Loinard, L Rodriguez, LF D'Alessio, P Wilner, DJ Ho, PTP AF Loinard, L Rodriguez, LF D'Alessio, P Wilner, DJ Ho, PTP TI Orbital proper motions in the protobinary system L1527/IRAS 04368+2557? SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; binaries : general; ISM : jets and outflows; stars : formation ID LOW-MASS PROTOSTARS; DISK; TAURUS; STARS AB Using high angular resolution 7 mm Very Large Array (VLA) observations, we show that the low-mass protostellar object IRAS 04368+2557 in L1527 is composed of two radio sources separated in projection by 25 AU. One of the two components is extended in the direction perpendicular to the outflow powered by IRAS 04368+2557 and is, most likely, a compact accretion disk (R similar to 20 AU), similar to those found in L1551 IRS 5 by Rodriguez et al. As in L1551 IRS 5, the disk found here is small compared to those around T Tauri stars. Tidal interactions with nearby companions provide a natural way of truncating disks, and we argue that the two millimeter-wavelength sources in L1527 trace a compact binary system, where the disk surrounding one of the components has been truncated by the tidal influence of the other. A comparison between observations obtained in 1996 and 2002 reveals large proper motions, which can be only partly attributed to the overall large-scale motion of the region in which IRAS 04368+2557 is located. The remaining "residual" proper motions might trace the orbital motion of the binary and would suggest a total mass for the system larger than 0.2 M. and likely of the order of 0.5-2 M. This mass (only a small fraction of which is in the disk) is of the same order as that of the extended surrounding envelope of gas and dust traced by far-infrared and submillimeter observations (M-env similar to 0.5 M.), implying that the stars that will eventually form out of IRAS 04368+2557 would have already acquired a significant fraction of their final masses. It is worth noting that multiepoch VLA studies of nearby protobinary systems similar to that presented here could provide direct mass estimates in most nearby star-forming sites. Combined with submillimeter observations of the surrounding envelopes, this would provide a more reliable measure of the evolutionary status of binary protostars. C1 Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Loinard, L (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 72-3 Xangari, Morelia 58089, Michoacan, Mexico. NR 19 TC 28 Z9 28 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 DEC 20 PY 2002 VL 581 IS 2 BP L109 EP L113 DI 10.1086/345940 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DB UT WOS:000179914500012 ER PT J AU Patsourakos, S Habbal, SR Hu, YQ AF Patsourakos, S Habbal, SR Hu, YQ TI Ion effective temperatures in polar coronal holes: Observations versus ion-cyclotron resonance SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : corona; Sun : UV radiation ID FAST SOLAR-WIND; ALFVEN WAVES; HEAVY-IONS; ACCELERATION; REGIONS; ELEMENTS; OUTFLOW; LINES; SUMER; SOHO AB The resonant cyclotron interaction between ion-cyclotron waves and solar wind species is considered nowadays to be a strong candidate for heating and acceleration of protons, alpha-particles, and heavy ions. A crucial physical parameter for determining the amount and the location of significant heating and acceleration, which the different solar wind ions receive from the waves in the frame of the ion-cyclotron mechanism, is their charge-to-mass ratio q/m. Therefore, comparisons of ion temperatures derived from spectroscopic observations and calculated by ion-cyclotron models, for ions that span a broad range in q/m, would provide a rigorous test for such models. By using an ion-cyclotron model, we calculate the effective temperatures for 10 different ions that cover the range 0.16-0.37 in q/m. Effective temperatures correspond to unresolved thermal motions and wave motions. The good agreement between our calculations, based on the specific mechanism that we employed here (ion-cyclotron resonance) and on spectroscopic observations of effective temperatures in polar coronal holes, provides support that the above mechanism accounts for the energetics and kinematics of fast solar wind heavy ions. However, such an agreement does not prove that other potential mechanisms can be excluded. C1 USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Univ Wales, Dept Phys, Aberystwyth SW23 3BZ, Ceredigion, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sci & Technol China, Dept Earth & Space Sci, Anhua 230026, Peoples R China. RP Patsourakos, S (reprint author), USN, Res Lab, Div Space Sci, 4555 Overlook Ave SW,Code 7670P, Washington, DC 20375 USA. EM patsourakos@nrl.navy.mil NR 24 TC 6 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2002 VL 581 IS 2 BP L125 EP L127 DI 10.1086/345976 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 627DB UT WOS:000179914500015 ER PT J AU Rufus, J Yoshino, K Thorne, AP Murray, JE Imajo, T Ito, K Matsui, T AF Rufus, J Yoshino, K Thorne, AP Murray, JE Imajo, T Ito, K Matsui, T TI The application of a vacuum ultraviolet Fourier transform spectrometer and synchrotron radiation source to measurements of: V. The beta(11,0) band of NO SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID NITRIC-OXIDE; HIGH-RESOLUTION; SYSTEM; BETA; SPECTROSCOPY; O-2; OD AB The beta(11,0) band of NO was measured at high resolution (0.06 cm(-1)) by the vacuum ultraviolet Fourier transform spectrometer from Imperial College, London, using synchrotron radiation at the Photon Factory, KEK, Japan, as a continuum light source. Such resolution facilitates a line by line analysis of the NO beta(11,0) band which yields accurate rotational line positions and term values as well as the photoabsorption cross sections. The molecular constants of the B(11) (2)Pi(r) level are found to be T-0=55 983.203+/-0.017 cm(-1), A=47.977+/-0.024, B-v=1.010 77+/-0.000 37 cm(-1), D-v=(6.7+/-0.8)x10(-6) cm(-1) and A(D)=0.0438+/-0.0035 cm(-1). The sum of the line strengths for all rotational transitions of the NO beta(11,0) band is determined as 3.04x10(-16) cm(2) cm(-1), corresponding to a band oscillator strength of (3.44+/-0.21)x10(-4). (C) 2002 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Japan Womens Univ, Tokyo 1128681, Japan. KEK, Photon Factory, Tsukuba, Ibaraki 3050801, Japan. RP Rufus, J (reprint author), Space & Atmospher Phys, London SW7 2AZ, England. NR 31 TC 7 Z9 5 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 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 15 PY 2002 VL 117 IS 23 BP 10621 EP 10626 DI 10.1063/1.1520535 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 619UC UT WOS:000179495000022 ER PT J AU Bartschat, K AF Bartschat, K TI Convergent R-matrix with pseudostates calculations for electron-impact ionization of the n=2 states in helium SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article AB We have used the R-matrix with pseudostates method to calculate angle-integrated cross-sections for electron-impact ionization of the n = 2 states in helium. Good agreement with the convergent close-coupling results of Fursa and Bray (J. Phys. B: At. Mol. Opt. Phys. 30 (1997) 757) is obtained, thereby confirming the discrepancy with the experimental data of Dixon et al (J. Phys. B: At. Mol. Phys. 9 (1976) 2617). C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Bartschat, K (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Bartschat, Klaus/I-2527-2012 NR 6 TC 13 Z9 14 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD DEC 14 PY 2002 VL 35 IS 23 BP L527 EP L529 AR PII S0953-4075(02)54879-3 DI 10.1088/0953-4075/35/23/104 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 635CT UT WOS:000180381000004 ER PT J AU Lin, J van Ballegooijen, AA Forbes, TG AF Lin, J van Ballegooijen, AA Forbes, TG TI Evolution of a semicircular flux rope with two ends anchored in the photosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE sun; corona; magnetic structure; equilibrium; evolution; catastrophe ID CORONAL MASS EJECTIONS; MAGNETIC-FIELD EVOLUTION; ERUPTIVE FLARES; SOLAR-FLARES; MODEL AB We investigated a coronal magnetic configuration including a semicircular flux rope with two ends anchored in the photosphere. The background field is produced by two source regions on the photosphere. We study the evolution of this configuration in response to the gradual change in the background field, which is modeled by varying either the strength of the source or the distance between the source regions on the photosphere. Our results indicate that the evolution due to the change in source strength shows the likelihood of catastrophic loss of equilibrium, and that the evolution due to the change in the distance is smooth and does not manifest any tendency to lose equilibrium. In the former case, the current sheet starts developing fairly early; it forms even before the evolution reaches the maximum current state. We notice that the effect of the curvature of flux rope on the evolution of the system is significant, such that the equilibrium curve does not form a cusp-catastrophic structure but a simple fold-catastrophic structure even if the evolution is ideal MHD and a current sheet attached to the boundary surface occurs. The curvature strengthens the magnetic compression between the flux rope and the photosphere and makes the loss of equilibrium easier. However, the question of how the system behaves after the loss of equilibrium is still open since the flux rope is not likely to remain semicircular at the stage of fast evolution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI LIN, JUN/B-9890-2017 NR 32 TC 16 Z9 16 U1 0 U2 0 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 DEC 12 PY 2002 VL 107 IS A12 AR 1438 DI 10.1029/2002JA009486 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 649AM UT WOS:000181184800002 ER PT J AU Vaisanen, P Morel, T Rowan-Robinson, M Serjeant, S Oliver, S Sumner, T Crockett, H Gruppioni, C Tollestrup, EV AF Vaisanen, P Morel, T Rowan-Robinson, M Serjeant, S Oliver, S Sumner, T Crockett, H Gruppioni, C Tollestrup, EV TI Near- and mid-infrared colours of star-forming galaxies in European large area ISO survey fields SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies : evolution; galaxies : starburst; infrared : galaxies; infrared : stars ID EXTREMELY RED GALAXIES; HUBBLE-DEEP-FIELD; ENERGY-DISTRIBUTIONS; SOURCE COUNTS; IR EMISSION; DUST; BAND; QUASARS; SAMPLE; ULTRAVIOLET AB We present J- and K-band near-infrared (near-IR) photometry of a sample of mid-infrared (mid-IR) sources detected by the Infrared Space Observatory (ISO) as part of the European Large Area ISO Survey (ELAIS) and study their classification and star-forming properties. We have used the Preliminary ELAIS Catalogue for the 6.7-mum (LW2) and 15-mum (LW3) fluxes. All of the high-reliability LW2 sources and 80 per cent of the LW3 sources are identified in the near-IR survey reaching K approximate to 17.5 mag. The near-IR/mid-IR flux ratios can effectively be used to separate stars from galaxies in mid-IR surveys. The stars detected in our survey region are used to derive a new accurate calibration for the ELAIS ISOCAM data in both the LW2 and LW3 filters. We show that near- to mid-IR colour-colour diagrams can be used to classify galaxies further, as well as to study star formation. The ELAIS ISOCAM survey is found mostly to detect strongly star-forming late-type galaxies, possibly starburst-powered galaxies, and it also picks out obscured active galactic nuclei. The ELAIS galaxies yield an average mid-IR flux ratio LW2/LW3 = 0.67 +/- 0.27. We discuss the f(v)(6.7 mum)/f(v)(15 mum) ratio as a star formation tracer using ISO and IRAS data of a local comparison sample. We find that the f(v) (2.2 mum)/f(v)(15 mum) ratio is also a good indicator of activity level in galaxies and conclude that the drop in the f(v)(6.7 mum)/f(v)(15 mum) ratio seen in strongly star-forming galaxies is a result of both an increase of 15-mum emission and an apparent depletion of 6.7-mum emission. Near-IR together with the mid-IR data make it possible to estimate the relative amount of interstellar matter in the galaxies. C1 Univ Helsinki Observ, Helsinki, Finland. European So Observ, Santiago 19, Chile. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2BZ, England. IUCAA, Pune 411007, Maharashtra, India. Osserv Astron Palermo, I-90134 Palermo, Italy. Univ Sussex, Sch CPES, Phys & Astron Subject Grp, Ctr Astron, Brighton BN1 9QJ, E Sussex, England. Osserv Astron Padova, I-35122 Padua, Italy. Osservatorio Astron Bologna, I-40127 Bologna, Italy. Boston Univ, Dept Astron, Boston, MA 02215 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Helsinki Observ, POB 14, Helsinki, Finland. EM pvaisane@eso.org OI Gruppioni, Carlotta/0000-0002-5836-4056 NR 57 TC 18 Z9 18 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 DEC 11 PY 2002 VL 337 IS 3 BP 1043 EP 1058 DI 10.1046/j.1365-8711.2002.06006.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 622LG UT WOS:000179648100031 ER PT J AU Croft, RAC Weinberg, DH Bolte, M Burles, S Hernquist, L Katz, N Kirkman, D Tytler, D AF Croft, RAC Weinberg, DH Bolte, M Burles, S Hernquist, L Katz, N Kirkman, D Tytler, D TI Toward a precise measurement of matter clustering: Ly alpha forest data at redshifts 2-4 SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : observations; large-scale structure of universe; quasars : absorption lines ID LINEAR POWER SPECTRUM; LARGE-SCALE STRUCTURE; WARM DARK-MATTER; INTERGALACTIC MEDIUM; MASS FLUCTUATIONS; COSMOLOGICAL PARAMETERS; DEUTERIUM ABUNDANCE; RADIATIVE-TRANSFER; GALAXY FORMATION; COLUMN DENSITY AB We measure the filling factor, correlation function, and power spectrum of transmitted flux in a large sample of Lyalpha forest spectra, comprised of 30 Keck HIRES spectra and 23 Keck LRIS spectra. We infer the linear matter power spectrum P(k) from the flux power spectrum P-F(k), using an improved version of the method of Croft et al. that accounts for the influence of redshift-space distortions, nonlinearity, and thermal broadening on the shape of P-F(k). The evolution of the shape and amplitude of P(k) over the redshift range of the sample (zapproximate to2-4) is consistent with the predictions of gravitational instability, implying that non-gravitational fluctuations do not make a large contribution to structure in the Lyalpha forest. Our fiducial measurement of P(k) comes from a subset of the data with 2.3=2.72, and total path length Deltazapproximate to25. It has a dimensionless amplitude Delta(2)(k(p))=0.74(-0.16)(+0.20) at wavelength number k(p)=0.03 (km s(-1))(-1) and is well described by a power law of index nu=-2.43+/-0.06 or by a CDM-like power spectrum with shape parameter Gamma'=1.3(0.5)(0.7)x10(-3) (km s(-1))(-1) at z=2.72 (all error bars 1 sigma). The correspondence to present-day P(k) parameters depends on the adopted cosmology. For Omega(m)=0.4, Omega(Lambda)=0.6, the best-fit shape parameter is Gamma=0.16 h Mpc(-1), in good agreement with measurements from the 2dF Galaxy Redshift Survey, and the best-fit normalization is sigma(8)=0.82(Gamma/0.15)(-0.44). Matching the observed cluster mass function and our measured Delta(2) (k(p)) in spatially at cosmological models requires Omega(m)=0.38(-0.08)(+0.10) + 2.2(Gamma-0.15). Matching Delta(2) (k(p)) in COBE-normalized, at CDM models with no tensor fluctuations requires Omega(m)=(0.29+/-0.04)n(-2.89) h(65)(-1.9), and models that satisfy this constraint are also consistent with our measured logarithmic slope. The Lyalpha forest complements other observational probes of the linear matter power spectrum by constraining a regime of redshift and length scale not accessible by other means, and the consistency of these inferred parameters with independent estimates provides further support for a cosmological model based on inflation, cold dark matter, and vacuum energy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Board Studies Astron & Astrophys, Santa Cruz, CA 95064 USA. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60615 USA. Univ Massachusetts, Dept Phys & Astron, Lederle Grad Res Ctr 640, Amherst, MA 01003 USA. RP Croft, RAC (reprint author), Carnegie Mellon Univ, Dept Phys, 7325 Wean Hall,5000 Forbes Ave, Pittsburgh, PA 15213 USA. RI Croft, Rupert/N-8707-2014 OI Croft, Rupert/0000-0003-0697-2583 NR 116 TC 284 Z9 286 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 DEC 10 PY 2002 VL 581 IS 1 BP 20 EP 52 DI 10.1086/344099 PN 1 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500003 ER PT J AU Reese, ED Carlstrom, JE Joy, M Mohr, JJ Grego, L Holzapfel, WL AF Reese, ED Carlstrom, JE Joy, M Mohr, JJ Grego, L Holzapfel, WL TI Determining the cosmic distance scale from interferometric measurements of the Sunyaev-Zeldovich effect SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmic microwave background; cosmology : observations; distance scale; galaxies : clusters : general; techniques : interferometric ID X-RAY-CLUSTER; MICROWAVE BACKGROUND ANISOTROPY; MEDIUM-SENSITIVITY SURVEY; VLA SKY SURVEY; HUBBLE-CONSTANT; GALAXY CLUSTERS; COOLING FLOWS; COMA CLUSTER; RADIO HALOS; RELATIVISTIC CORRECTIONS AB We determine the distances to 18 galaxy clusters with redshifts ranging from zsimilar to0.14 to 0.78 from a maximum likelihood joint analysis of 30 GHz interferometric Sunyaev-Zeldovich effect(SZE) and X-ray observations. We model the intracluster medium (ICM) using a spherical isothermal beta model. We quantify the statistical and systematic uncertainties inherent to these direct distance measurements, and we determine constraints on the Hubble parameter for three different cosmologies. These distances imply a Hubble constant of 60(-4-18)(+4+13) km s(-1) Mpc(-1) for an Omega(M)=0.3, Omega(Lambda)=0.7 cosmology, where the uncertainties correspond to statistical followed by systematic at 68% confidence. With a sample of 18 clusters, systematic uncertainties clearly dominate. The systematics are observationally approachable and will be addressed in the coming years through the current generation of X-ray satellites (Chandra and XMM-Newton) and radio observatories (Owens Valley Radio Observatory, Berkeley-Illinois-Maryland Association, and Very Large Array). Analysis of high-redshift clusters detected in future SZE and X-ray surveys will allow a determination of the geometry of the universe from SZE-determined distances. C1 Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reese, ED (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. RI Holzapfel, William/I-4836-2015 NR 155 TC 170 Z9 171 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 DEC 10 PY 2002 VL 581 IS 1 BP 53 EP 85 DI 10.1086/344137 PN 1 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500004 ER PT J AU Peterson, BM Berlind, P Bertram, R Bischoff, K Bochkarev, NG Borisov, N Burenkov, AN Calkins, M Carrasco, L Chavushyan, VH Chornock, R Dietrich, M Doroshenko, VT Ezhkova, OV Filippenko, AV Gilbert, AM Huchra, JP Kollatschny, W Leonard, DC Li, W Lyuty, VM Malkov, YF Matheson, T Merkulova, NI Mikhailov, VP Modjaz, M Onken, CA Pogge, RW Pronik, VI Qian, B Romano, P Sergeev, SG Sergeeva, EA Shapovalova, AI Spiridonova, OI Tao, J Tokarz, S Valdes, JR Vlasiuk, VV Wagner, RM Wilkes, BJ AF Peterson, BM Berlind, P Bertram, R Bischoff, K Bochkarev, NG Borisov, N Burenkov, AN Calkins, M Carrasco, L Chavushyan, VH Chornock, R Dietrich, M Doroshenko, VT Ezhkova, OV Filippenko, AV Gilbert, AM Huchra, JP Kollatschny, W Leonard, DC Li, W Lyuty, VM Malkov, YF Matheson, T Merkulova, NI Mikhailov, VP Modjaz, M Onken, CA Pogge, RW Pronik, VI Qian, B Romano, P Sergeev, SG Sergeeva, EA Shapovalova, AI Spiridonova, OI Tao, J Tokarz, S Valdes, JR Vlasiuk, VV Wagner, RM Wilkes, BJ TI Steps toward determination of the size and structure of the broad-line region in active galactic nuclei. XVI. A 13 year study of spectral variability in NGC 5548 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 5548); galaxies : nuclei; galaxies : Seyfert ID NGC 5548; OPTICAL WAVELENGTHS; SEYFERT-GALAXIES; EMISSION-LINES; LONG-TERM; CONTINUUM; QUASARS; ULTRAVIOLET; LUMINOSITY; ACCURACY AB We present the final installment of an intensive 13 year study of variations of the optical continuum and broad Hbeta emission line in the Seyfert 1 galaxy NGC 5548. The database consists of 1530 optical continuum measurements and 1248 Hbeta measurements. The Hbeta variations follow the continuum variations closely, with a typical time delay of about 20 days. However, a year-by-year analysis shows that the magnitude of emission-line time delay is correlated with the mean continuum flux. We argue that the data are consistent with the simple model prediction between the size of the broad-line region and the ionizing luminosity, rproportional toL(ion)(1/2). Moreover, the apparently linear nature of the correlation between the Hbeta response time and the nonstellar optical continuum F-opt arises as a consequence of the changing shape of the continuum as it varies, specifically F(opt)proportional toF(UV)(0.56). . C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Sternwarte Gottingen, D-37083 Gottingen, Germany. Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 357147, Karachai Cherke, Russia. Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Crimean Lab, UA-98409 Nauchnyi, Crimea, Ukraine. Uzbek Acad Sci, Ulugbek Astron Inst, Tashkent 700052, Uzbekistan. Crimean Astrophys Observ, UA-98409 Crimea, Ukraine. Shanghai Astron Observ, Shanghai 200030, Peoples R China. RP Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM peterson@astronomy.ohio-state.edu; pberlind@cfa.harvard.edu; rayb@as.arizona.edu; bischoff@uni-sw.gwdg.de; boch@sai.msu.ru; ban@sao.ru; carrasco@inaoep.mx; vahram@inaoep.mx; rchornock@astro.berkeley.edu; dietrich@astro.ufl.edu; doroshen@sai.crimea.ua; oezh@sai.msu.ru; alex@astro.berkeley.edu; agilbert@astro.berkeley.edu; huchra@cfa.harvard.edu; wkollat@gwdg.de; leonard@nova.astro.umass.edu; wli@astro.berkeley.edu; lyuty@sai.crimea.ua; tmatheson@cfa.harvard.edu; nelly@astro.crao.crimea.ua; mvp@sao.ru; mmodjaz@cfa.harvard.edu; onken@astronomy.ohio-state.edu; pogge@astronomy.ohio-state.edu; vpronik@crao.crimea.ua; promano@astronomy.ohio-state.edu; selena@crao.crimea.ua; sergeev@crao.crimea.ua; ashap@sao.ru; ospir@sao.ru; taojun@center.shao.ac.cn; jvaldes@inaoep.mx; vvlas@sao.ru; rmw@as.arizona.edu; belinda@cfa.harvard.edu OI Onken, Christopher/0000-0003-0017-349X; Romano, Patrizia/0000-0003-0258-7469; Wilkes, Belinda/0000-0003-1809-2364 NR 34 TC 102 Z9 102 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2002 VL 581 IS 1 BP 197 EP 204 DI 10.1086/344197 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500013 ER PT J AU Wiedner, MC Wilson, CD Harrison, A Hills, RE Lay, OP Carlstrom, JE AF Wiedner, MC Wilson, CD Harrison, A Hills, RE Lay, OP Carlstrom, JE TI Interferometric observations of the nuclear region of ARP 220 at submillimeter wavelengths SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (Arp 220); galaxies : ISM; galaxies : peculiar; galaxies : starburst; submillimeter; techniques : interferometric ID ULTRALUMINOUS INFRARED GALAXIES; MOLECULAR CLOUDS; LUMINOUS GALAXIES; STAR-FORMATION; IRAS GALAXIES; ARP-220; STARBURSTS; GAS; IC-4553; DISKS AB We report the first submillimeter interferometric observations of an ultraluminous infrared galaxy. We observed Arp 220 in the CO J=3-2 line and 342 GHz continuum with the single-baseline CSO-JCMT interferometer consisting of the Caltech Submillimeter Observatory (CSO) and the James Clerk Maxwell Telescope (JCMT). Models were fitted to the measured visibilities to constrain the structure of the source. The morphologies of the CO J=3-2 line and 342 GHz continuum emission are similar to those seen in published maps at 230 and 110 GHz. We clearly detect a binary source separated by similar to1" in the east-west direction in the 342 GHz continuum. The CO J=3-2 visibility amplitudes, however, indicate a more complicated structure, with evidence for a compact binary at some velocities and rather more extended structure at others. Less than 30% of the total CO J=3-2 emission is detected by the interferometer, which implies the presence of significant quantities of extended gas. We also obtained single-dish CO J=2-1, CO J=3-2, and HCN J=4-3 spectra. The HCN J=4-3 spectrum, unlike the CO spectra, is dominated by a single redshifted peak. The HCN J=4-3/CO J=3-2, HCN J=4-3/HCN J=10, and CO J=3-2/2-1 line ratios are larger in the redshifted (eastern) source, which suggests that the two sources may have different physical conditions. This result might be explained by the presence of an intense starburst that has begun to deplete or disperse the densest gas in the western source, while the eastern source harbors undispersed high-density gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. McMaster Univ, Hamilton, ON L8S 4M1, Canada. Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Wiedner, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. NR 42 TC 15 Z9 15 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 DEC 10 PY 2002 VL 581 IS 1 BP 229 EP 240 DI 10.1086/344106 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500016 ER PT J AU Seth, AC Greenhill, LJ Holder, BP AF Seth, AC Greenhill, LJ Holder, BP TI Water masers as tracers of protostellar disks and outflows in the intermediate-mass star-forming region NGC 2071 SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (NGC 2071); ISM : jets and outflows; masers; stars : formation ID YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; HIGH-RESOLUTION; H2O MASERS; BIPOLAR OUTFLOW; RADIO-CONTINUUM; CEPHEUS-A; IRS 1; NGC-2071; EMISSION AB We have mapped the water maser emission associated with the infrared centers IRS 1 and IRS 3 of the NGC 2071IR star-forming region at four epochs over similar to4 months with the Very Long Baseline Array. We detected 269 maser features with similar to1 km s(-1) line widths and measured 30 proper motions. In each infrared center, the water maser emission appears to trace parts of a protostellar disk and collimated outflow. The disk components are similar to9 and similar to17 AU long in IRS 3 and IRS 1, respectively, and similar to2 AU wide. They are identified as disks by their compact size, elongation parallel to the direction of known IR polarization, central location in the maser maps, small internal proper motions, and proximity to lambda1.3 cm continuum emission. The outflows have axes perpendicular to the disks and exhibit proper motions of up to similar to42 km s(-1). They are outlined by maser emission up to similar to260 AU from the protostars. The IRS 3 outflow appears to be conical on one side, while the IRS 1 outflow comprises a narrowly collimated bipolar flow surrounded by outward-facing, funnel-shaped cavities. The detection of water maser emission tracing such compact disk components and specifically conical or funnel-shaped structures is unusual. The fact that the distributions are similar in IRS 3 and IRS 1 may indicate that the two infrared centers are roughly coeval. NGC 2071IR provides a rare opportunity to resolve the structures and dynamics of disks and outflows together and to do so for two protostars that are only similar to2000 AU apart (in projection) in a deeply embedded star-forming region of intermediate luminosity. C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, Dept Phys, Austin, TX 78712 USA. RP Seth, AC (reprint author), Univ Washington, Dept Astron, Stevens Way,Box 351580, Seattle, WA 98195 USA. NR 42 TC 34 Z9 34 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 DEC 10 PY 2002 VL 581 IS 1 BP 325 EP 334 DI 10.1086/344225 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500023 ER PT J AU Grindlay, JE Camilo, F Heinke, CO Edmonds, PD Cohn, H Lugger, P AF Grindlay, JE Camilo, F Heinke, CO Edmonds, PD Cohn, H Lugger, P TI Chandra study of a complete sample of millisecond pulsars in 47 Tucanae and NGC 6397 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; globular clusters : general; globular clusters : individual (47 Tucanae); pulsars : general; stars : neutron; X-rays : stars ID GLOBULAR-CLUSTER 47-TUCANAE; SINGLE-STAR SCATTERING; X-RAY-EMISSION; DYNAMICAL PROPERTIES; BINARY; COMPANION; CORE; MASS; EVOLUTION; NGC-6397 AB We report Chandra observations of the complete sample of millisecond pulsars (MSPs) with precise radio positions in the globular clusters 47 Tuc (NGC 104) and NGC 6397. The X-ray luminosities and colors are derived or constrained and compared to X-ray MSPs previously detected in the field as well as one previously detected in a globular cluster (M28). The 47 Tuc MSPs are predominantly soft sources suggestive of thermal emission from small (r(X) < 0.6 km) polar caps on the neutron star rather than magnetospheric emission and are a relatively homogeneous sample, with most X-ray luminosities in a surprisingly narrow range [L-X &SIM; (1-4) x 10(30) ergs s(-1)]. We use previously derived intrinsic (P) over dot values and find a new relation between L-X and spin-down luminosity, (E) over dot : L-X &PROP; E-β, with β &SIM; 0.5 +/- 0.2 versus &SIM;1.0 for both pulsars and MSPs in the field. Adding the single MSP in NGC 6397 constrains β to 0.5 +/- 0.15. This L-X-(E) over dot relation and also the L-X/(E) over dot versus spin-down age are each similar to that found by Harding & Muslimov for thermal emission from polar cap heating. However, the cluster MSPs are relatively longer lived ( in thermal X-rays) than either the models or field MSPs, which may have additional magnetospheric (nonthermal) components. We suggest that the cluster MSPs may have altered surface magnetic field topology (e.g., multipole), or their neutron stars are more massive from repeated accretion episodes due to encounters and repeated exchange interactions. MSP binary companions on or just off the main sequence (e.g., NGC 6397) are likely to have been reexchanged and might show anomalous (P) over dot and (E) over dot values due to relaxation of misaligned core-crust spins. The radial distribution of &SIM;40 soft Chandra sources in 47 Tuc is consistent with a &SIM;1.4 M-. component in a multimass King model and with the identified MSP sample. The implied total MSP population in 47 Tuc with L-X &GSIM; 10(30) ergs s(-1) is &SIM;35-90 and can constrain the relative beaming in radio versus soft X-rays. NGC 6397 is relatively deficient in MSPs: its single detected example may have been reexchanged out of the cluster core. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Heinke, Craig/0000-0003-3944-6109 NR 55 TC 99 Z9 99 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 DEC 10 PY 2002 VL 581 IS 1 BP 470 EP 484 DI 10.1086/344150 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500034 ER PT J AU Smith, RK Edgar, RJ Shafer, RA AF Smith, RK Edgar, RJ Shafer, RA TI The X-ray halo of GX 13+1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; scattering; X-rays : binaries; X-rays : ISM ID INTERSTELLAR GRAINS; ENERGY-SPECTRA; BINARIES; DUST; SCATTERING; GX-13+1; DISCOVERY; RADIO; LINE AB We present observations of the X-ray halo around the low-mass X-ray binary GX 13+1 from the Chandra X-ray telescope. The halo is caused by scattering in interstellar dust grains, and we use it to diagnose the line-of-sight position, size distribution, and density of the grains. Using the intrinsic energy resolution of Chandra's ACIS CCDs and the recent calibration observation of the Chandra point-spread function, we were able to extract the halo fraction as a function of energy and off-axis angle. We de ne a new quantity, the "halo coefficient", or the total halo intensity relative to the source extrapolated to 1 keV, and measure it to be 1.5(-0.1)(+0.5) for GX 13+1. We find a relationship between this value and the dust size, density, and hydrogen column density along the line of sight to GX 13+1. We also conclude that our data do not agree with "fluffy" dust models that earlier X-ray halo observations have supported and that models including an additional large dust grain population are not supported by these data. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Lab Astron & Space Phys, Greenbelt, MD 20771 USA. RP Smith, RK (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 50 Z9 50 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 DEC 10 PY 2002 VL 581 IS 1 BP 562 EP 569 DI 10.1086/344151 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500041 ER PT J AU Tomsick, JA Heindl, WA Chakrabarty, D Kaaret, P AF Tomsick, JA Heindl, WA Chakrabarty, D Kaaret, P TI Rotational broadening measurement for the neutron star X-ray transient XTE J2123-058 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (XTE J2123-058); stars : neutron; stars : rotation; X-rays : bursts; X-rays : stars ID COMPANION STAR; RADIO PULSARS; AQUILA X-1; MASS; SPECTROSCOPY; CYGNI; SPEED; CURVE AB We used optical spectroscopy of the neutron star X-ray transient XTE J2123-058 to measure the rotational broadening of the binary companion's stellar absorption lines and determined that the companion's projected rotational velocity is v sin i = 121(-29)(+21) km s(-1). This value is considerably larger than the measurements of v sin i obtained previously for three other neutron star systems, where the values were between 34 and 65 km s(-1). The larger value is likely due to the combination of high binary inclination and short ( 6 hr) orbital period for XTE J2123-058. Along with previously measured parameters, the rotational broadening measurement allowed us to determine the binary parameters, including the ratio of the neutron star mass to the companion mass, q = M-1/M-2 = 2.7(-0.9)(+1.3) the neutron star mass M-1 = 1.46(-0.39)(+0.30) M-., and the companion mass M-2 = 0.53(-0.39)(+0.28) M-., assuming a Roche lobe-filling companion synchronously rotating with the binary orbit. These values are consistent with a previous measurement in which the H emission line was used to determine the semiamplitude of the neutron star's radial velocity curve (K-1). It is a significant result that the two methods give consistent values. We also report the first measurement of the XTE J2123-058 companion's radius. Assuming synchronous rotation, we obtain R-2 = 0.62(-0.15)(+0.11) R-., which is in line with that expected for a late K-type star on or close to the main sequence. Finally, we report the first precise spectroscopic determination of the binary orbital period (P-orb = 21, 442.3 +/- 1.8 s). C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Space Res Ctr, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tomsick, JA (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, Code 0424, La Jolla, CA 92093 USA. NR 23 TC 10 Z9 11 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 DEC 10 PY 2002 VL 581 IS 1 BP 570 EP 576 DI 10.1086/344130 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500042 ER PT J AU Koenigsberger, G Kurucz, RL Georgiev, L AF Koenigsberger, G Kurucz, RL Georgiev, L TI The photospheric absorption lines in the ultraviolet spectrum of the multiple system HD 5980 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; Magellanic Clouds; stars : atmospheres; stars : individual (HD 5980) ID SMALL-MAGELLANIC-CLOUD; WOLF-RAYET STARS; BINARY HD-5980; O-STARS; OPTICAL-SPECTRUM; SMC; MICROTURBULENCE; SPECTROSCOPY; ATMOSPHERES; SUPERGIANTS AB We search for radial velocity variations in the ultraviolet spectra of the erupting Wolf-Rayet/luminous blue variable system HD 5980, located in the Small Magellanic Cloud. We obtain an average radial velocity of 22 +/- 22 km s(-1) for five observations in 1999 at different orbital phases, -39 +/- 24 km s(-1) for one observation in 2001, and 20 +/- 45 km s(-1) for one observation in 2002. These velocities are with respect to the SMC O3 star MPG 355, which is used as one of the templates. Hence, radial velocity variations on the 19.265 day (star A+ star B) orbital timescale attributable to the erupting star ( star A) of the system are not detected, thus confirming that the visible absorption lines in the spectrum have their origin in a third stellar component ( star C). We propose that star A has very broad (v sin i similar to 250 km s(-1)) absorption lines, which would escape detection in the complicated emission-line spectrum of the system. Such broad lines, combined with the 128 km s(-1) orbital motion, would lead to a lower amplitude fictitious radial velocity curve when the stationary set of absorption lines is measured. We conclude that line pro le variations at orbital phase 0.0 from one epoch of observations to another are associated with these broad underlying absorption lines, arising in the unstable photosphere of star A. The analysis is performed with the aid of synthetic UV spectra that are calculated from LTE line-blanketed atmosphere models, and the HST Space Telescope Imaging Spectrograph spectra of four O-type stars in the cluster NGC 346, to which HD 5980 is believed to belong. We estimate T-eff and obtain values of v sin i and the mean radial velocity for MPG 324 [O4 V((f))], MPG 368 [O4-5 V((f))], MPG 355 [O3 V(f*)], and MPG 113 (OC 6Vz). C1 Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62251, Morelos, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Autonomous Univ Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Koenigsberger, G (reprint author), Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62251, Morelos, Mexico. NR 35 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2002 VL 581 IS 1 BP 598 EP 609 DI 10.1086/344215 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500045 ER PT J AU Redfield, S Linsky, JL Ake, TB Ayres, TR Dupree, AK Robinson, RD Wood, BE Young, PR AF Redfield, S Linsky, JL Ake, TB Ayres, TR Dupree, AK Robinson, RD Wood, BE Young, PR TI A Far Ultraviolet Spectroscopic Explorer Survey of late-type dwarf stars SO ASTROPHYSICAL JOURNAL LA English DT Article ID HIGH-RESOLUTION SPECTROGRAPH; X-RAY-EMISSION; LOCAL INTERSTELLAR-MEDIUM; NEIGHBORHOOD FLARE STARS; HUBBLE-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; A-TYPE STARS; TRANSITION REGION; CONVECTION ZONES; THIN PLASMAS AB We describe the 910-1180 Angstrom spectra of seven late-type dwarf stars obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite. The stars include Altair (A7 IV), Procyon (F5 IV V),alpha Cen A (G2 V), AB Dor (K1 V),alpha Cen B (K2 V),epsilon Eri (K2 V), and AU Mic (M0 V). We present line identifications, fluxes, Doppler shifts, and widths. Doppler shifts are measured with respect to heliocentric wavelength scales determined from interstellar absorption lines, and are compared with transition region line shifts seen in Hubble Space Telescope (HST) ultraviolet spectra. For the warmer stars the O vi lines extend the trend of increasing redshift with line formation temperature, but for the cooler stars the O vi line redshifts are essentially zero. The C III and O vi lines of most stars in the sample are best fit with two Gaussians, and we confirm the correlation of increasing importance of the broad component with increasing stellar activity. The nonthermal velocities of the narrow component are subsonic and exhibit a trend toward larger velocities with decreasing surface gravity, while the nonthermal velocities of the broad components show no obvious trend with stellar gravity. The C III and O vi lines of Altair show unique broad horned profiles. Two flares were observed on AU Mic. One shows increasing continuum flux to shorter wavelengths, which we interpret as free-free emission from hot plasma, and relatively narrow, redshifted C III and O vi emission. The other shows very broad line profiles. C1 Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Natl Inst Stand & Technol, Boulder, CO 80309 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. RP Redfield, S (reprint author), Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. NR 78 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 DEC 10 PY 2002 VL 581 IS 1 BP 626 EP 653 DI 10.1086/344153 PN 1 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623AU UT WOS:000179681500047 ER PT J AU Linares, OF AF Linares, OF TI African rice (Oryza glaberrima): History and future potential SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article AB The African species of rice (Oryza glaberrima) was cultivated long before Europeans arrived in the continent. At present, O. glaberrima is being replaced by the introduced Asian species of rice, Oryza sativa. Some West African farmers, including the Jola of southern Senegal, still grow African rice for use in ritual contexts. The two species of rice have recently been crossed, producing a promising hybrid. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Linares, OF (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. NR 24 TC 87 Z9 90 U1 3 U2 18 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 DEC 10 PY 2002 VL 99 IS 25 BP 16360 EP 16365 DI 10.1073/pnas.252604599 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 624VY UT WOS:000179783400096 PM 12461173 ER PT J AU Kitajima, K Mulkey, SS Samaniego, M Wright, SJ AF Kitajima, K Mulkey, SS Samaniego, M Wright, SJ TI Decline of photosynthetic capacity with leaf age and position in two tropical pioneer tree species SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE leaf age; leaf longevity; leaf nitrogen content; leaf position; photosynthetic capacity; self-shading; tropical trees ID NITROGEN USE EFFICIENCY; CARBON GAIN; CANOPY TREE; LIFE SPANS; LEAVES; FOREST; LIGHT; PLANTS; LONGEVITY; PATTERN AB The effect of leaf age on photosynthetic capacity, a critical parameter in the theory of optimal leaf longevity, was studied for two tropical pioneer tree species, Cecropia longipes and Urera caracasana, in a seasonally dry forest in Panama. These species continuously produce short-lived leaves (74 and 93 d, respectively) during the rainy season (May-December) on orthotropic branches. However, they differ in leaf production rate, maximum number of leaves per branch, light environment experienced by the leaves, leaf mass per unit area, and nitrogen content. Light-saturated photosynthetic rates for marked leaves of known ages (+/-1 wk) were measured with two contrasting schemes (repeated measurements vs. chronosequence within branch), which overall produced similar results. In both species, photosynthetic rates and nitrogen use efficiency were negatively correlated with leaf age and positively correlated with light availability. Photosynthetic rates declined faster with leaf age in Cecropia than in Urera as predicted by the theory. The rate of decline was faster for leaves on branches with faster leaf turnover rates. Nitrogen per unit leaf area decreased with leaf age only for Urera. Leaf mass per unit area increased with leaf age, either partly (in Cecropia) or entirely (in Urera) due to ash accumulation. C1 Univ Florida, Dept Bot, Gainesville, FL 32611 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Kitajima, K (reprint author), Univ Florida, Dept Bot, Gainesville, FL 32611 USA. RI Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 33 TC 82 Z9 94 U1 7 U2 27 PU BOTANICAL SOC AMER INC PI COLUMBUS PA OHIO STATE UNIV-DEPT BOTANY, 1735 NEIL AVE, COLUMBUS, OH 43210 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD DEC PY 2002 VL 89 IS 12 BP 1925 EP 1932 DI 10.3732/ajb.89.12.1925 PG 8 WC Plant Sciences SC Plant Sciences GA 683DN UT WOS:000183132500007 PM 21665621 ER PT J AU Johnston, PF AF Johnston, PF TI A million pounds of sandalwood: The history of Cleopatra's-Barge in Hawaii (Vessel built by George Crowninshield and America's first yacht) SO AMERICAN NEPTUNE LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Johnston, PF (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 32 TC 0 Z9 0 U1 0 U2 1 PU PEABODY MUSEUM PI SALEM PA E INDIA MARINE HALL, SALEM, MA 01970 USA SN 0003-0155 J9 AM NEPTUNE JI Am. Neptune PD WIN PY 2002 VL 62 IS 1 BP 5 EP 45 PG 41 WC History SC History GA 756UD UT WOS:000187501000001 ER PT J AU Nickles, S AF Nickles, S TI More is better: Mass consumption, gender, and class identity in postwar America SO AMERICAN QUARTERLY LA English DT Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Nickles, S (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 151 TC 25 Z9 25 U1 0 U2 3 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0003-0678 J9 AM QUART JI Am. Q. PD DEC PY 2002 VL 54 IS 4 BP 581 EP 622 DI 10.1353/aq.2002.0040 PG 42 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 628PH UT WOS:000180004600003 ER PT J AU Kewley, LJ Geller, MJ Jansen, RA Dopita, MA AF Kewley, LJ Geller, MJ Jansen, RA Dopita, MA TI The H alpha and infrared star formation rates for the Nearby Field Galaxy Survey SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : spiral; galaxies : starburst ID SPIRAL GALAXIES; IRAS OBSERVATIONS; HUBBLE SEQUENCE; INTERSTELLAR-MEDIUM; STARBURST GALAXIES; FORMATION HISTORY; EMISSION; REDSHIFT; SAMPLE; PHOTOMETRY AB We investigate the Halpha and infrared star formation rate (SFR) diagnostics for galaxies in the Nearby Field Galaxy Survey (NFGS). For the 81 galaxies in our sample, we derive Halpha fluxes (included here) from integrated spectra. There is a strong correlation between the ratio of far-infrared to optical luminosities L(FIR)/L(Halpha) and the extinction E(B-V) measured with the Balmer decrement. Before reddening correction, the SFR(IR) and SFR(Halpha) are related to each other by a power law: SFR(IR) = (2.7 +/- 0.3) SFR(Halpha) 1.30 +/- 0.06. Correction of the SFR(Halpha) for extinction using the Balmer decrement and a classical reddening curve both reduces the scatter in the SFR(IR)-SFR(Halpha) correlation and results in a much closer agreement between the two SFR indicators; SFR(IR) = (0.91 +/- 0.04) SFR(Halpha(corr))(1.07+/-0.03). SFR(IR) and SFR(Halpha) agree to similar to10%. This SFR relationship spans 4 orders of magnitude and holds for all Hubble types with IRAS detections in the NFGS. A constant ratio between the SFR(IR) and SFR(Halpha) for all Hubble types, including early types (S0-Sab), suggests that the IR emission in all these objects results from a young stellar population. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Kewley, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS-20,60 Garden St, Cambridge, MA 02138 USA. EM lkewley@cfa.harvard.edu RI Dopita, Michael/P-5413-2014 OI Dopita, Michael/0000-0003-0922-4986 NR 64 TC 145 Z9 145 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2002 VL 124 IS 6 BP 3135 EP 3143 DI 10.1086/344487 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 617KW UT WOS:000179361700010 ER PT J AU Bragg, AE Kenyon, SJ AF Bragg, AE Kenyon, SJ TI HII emission from a complete spectroscopic survey of Be stars in h and chi Persei SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 869, NGC 884); stars : early-type; stars : emission-line, Be ID OPEN CLUSTERS; STANDARD STARS; PHOTOMETRY; SPECTRA AB We describe data for emission-line B stars observed in a spectroscopic survey of h and chi Persei. The survey is complete to V = 12.5 and covers an area of similar to1100 arcmin(2) roughly centered on the two clusters. We detect 32 Be stars; some have low Halpha emission strength. Seven of these are new identifications; seven others are confirmations of Be stars previously identified using photometry. Five of the observed Be stars show significant Halpha profile variations from epoch to epoch. We show that spectral indices yield physical characteristics of the H II emission region. This automatic method is robust and easily applied to large spectroscopic samples. We infer Halpha : Hbeta flux ratios of 2-5 and observe a linear relationship between Halpha emission and J-K color for these stars. We include a Hertzsprung-Russell diagram for the B-type stars in the clusters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bragg, AE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 40 TC 15 Z9 15 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 DEC PY 2002 VL 124 IS 6 BP 3289 EP 3298 DI 10.1086/344306 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 617KW UT WOS:000179361700019 ER PT J AU Winn, JN Morgan, ND Hewitt, JN Kochanek, CS Lovell, JEJ Patnaik, AR Pindor, B Schechter, PL Schommer, RA AF Winn, JN Morgan, ND Hewitt, JN Kochanek, CS Lovell, JEJ Patnaik, AR Pindor, B Schechter, PL Schommer, RA TI PMN J1632-0033: A new gravitationally lensed quasar (vol 123, pg 10, 2002) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, Australia Telescope Natl Facil, Dickson, ACT, Australia. Max Planck Inst Radioastron, D-5300 Bonn, Germany. Princeton Univ Observ, Princeton, NJ 08544 USA. Cerro Tololo Interamer Observ, La Serena, Chile. RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2002 VL 124 IS 6 BP 3485 EP 3485 DI 10.1086/367729 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 617KW UT WOS:000179361700041 ER PT J AU Pentericci, L Kurk, JD Carilli, CL Harris, DE Miley, GK Rottgering, HJA AF Pentericci, L Kurk, JD Carilli, CL Harris, DE Miley, GK Rottgering, HJA TI A Chandra study of X-ray sources in the field of the z=2.16 radio galaxy MRC 1138-262 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : clusters : general; X-rays : galaxies : clusters; X-rays : general ID LUMINOSITY FUNCTION; OPTICAL SURVEY; PROTO-CLUSTER; SPECTROSCOPY; POPULATION; SEARCH; SOUTH AB We present results from a Chandra X-ray Observatory study of the field X-ray source population in the vicinity of the radio galaxy MRC 1138-262. Many serendipitous X-ray sources are detected in an area of 8' x 8' around the radio source and 90% are identified in our deep VLT images. The space density of such sources is higher than expected on the basis of the statistics of ROSAT and Chandra deep surveys. The most likely explanation is in terms of a concentration of AGN associated with the protocluster at z = 2.16 which was found around the radio galaxy in previous studies. Two sources have a confirmed spectroscopic redshift close to that of the radio galaxy, and for three more sources other observations suggest that they are associated with the protocluster. Four of these five X-ray sources form, together with the radio galaxy, a filament in the plane of the sky. The direction of the filament is similar to that of the radio source axis, the large scale distribution of the other protocluster members, the 150 kpc-sized emission-line halo and the extended X-ray emission associated with the radio galaxy. The majority of optically identified X-ray sources in this field have properties consistent with type I AGN, a few could be soft, low luminosity galaxies, one is probably an obscured (type II) AGN and one is a star. These statistics are consistent with the results of deep X-ray surveys. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astron Observ, Cambridge, MA 02138 USA. RP Pentericci, L (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. NR 28 TC 54 Z9 54 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 DEC PY 2002 VL 396 IS 1 BP 109 EP 115 DI 10.1051/0004-6361:20021368 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 617YB UT WOS:000179387600010 ER PT J AU Bianchi, S Matt, G Fiore, F Fabian, AC Iwasawa, K Nicastro, F AF Bianchi, S Matt, G Fiore, F Fabian, AC Iwasawa, K Nicastro, F TI Flux and spectral variations in the Circinus Galaxy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : individual : Circinus; galaxies : Seyfert X-rays : galaxies; X-rays : individuals : CG X-1 x-rays : individuals : CG X-2 ID ACTIVE GALACTIC NUCLEI; NEARBY SPIRAL GALAXIES; X-RAY-SPECTRUM; COLD MATTER; VARIABILITY; CHANDRA; REFLECTION; NGC-1068; BEPPOSAX; LINE AB We report on a dramatic flux (similar to 50% increase in the LECS and MECS band) and spectral variation between two BeppoSAX observations of the Circinus Galaxy performed almost three years apart. Through the analysis of all Chandra observations available in the archive, including a new DDT observation on May 2001, we show that a high flux state of an extremely variable Ultra Luminous X-ray source (CG X-1: Bauer et al. 2001), which is within the adopted BeppoSAX source extraction region of 20, is the most likely explanation for most of the observed variation. However, the presence of a high flux 6.7 keV line and the spectral variation of the PDS in the new BeppoSAX data could be partly due to intrinsic variation of the nucleus. Comparing the longest Chandra observation and the BeppoSAX one, we find that the long-term flux variability of CG X-1 is not accompanied by a significant spectral variability. We also re-analysed the Chandra HEG nuclear spectra and report on the presence of a Compton shoulder with a flux of about 20% the line core, in agreement with theoretical expectations for Compton-thick matter. C1 Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. Osserv Astron Roma, I-00044 Monte Porzio Catone, Italy. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bianchi, S (reprint author), Univ Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy. RI Bianchi, Stefano/B-4804-2010; OI Bianchi, Stefano/0000-0002-4622-4240; Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 27 TC 22 Z9 22 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 DEC PY 2002 VL 396 IS 3 BP 793 EP 799 DI 10.1051/0004-6361:20021414 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 622DE UT WOS:000179630600007 ER PT J AU Ventura, R Spadaro, D Uzzo, M Suleiman, R AF Ventura, R Spadaro, D Uzzo, M Suleiman, R TI UV line intensity and flow velocity distributions in two coronal mass ejections as deduced by UVCS-SOHO observations (vol 383, pg 1032, 2002) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction ID SOLAR CORONA; SPECTROMETER; SIGNATURES; UVCS/SOHO; ERUPTION; EMISSION; FLARES AB The Ultraviolet Coronagraph Spectrometer (UVCS) instrument onboard the SOHO satellite observed two coronal mass ejections on November 2 and 3, 2000, related to the eruptions of a large filament structure in an active region close to the West limb of the Sun, and of a prominence near the South Pole, respectively. Intensity and profile of the O VI resonance doublet lines at 1032 and 1037 Angstrom and of Lybeta (1026 Angstrom) line, together with the intensity of some other minor ions, were observed using the O VI channel of UVCS. We analsed these spectroscopic observations in order to get information about the distributions of ionic densities and flow velocities in the solar coronal plasma ejected during these transient events. Emission in ions ranging from C II to O VI indicates a temperature range between 10(4.5) and 10(5.5) K. The morphology of the bright emission regions suggests the development of several strands of plasma irregularly distributed inside the CME structures, whose temporal evolution is significantly different from each other. The velocities determined for each bright element also give a complex picture of the plasma kinematics characterizing these coronal mass ejections. C1 Citta Univ Catania, Osservatorio Astrofis Catania, I-95125 Catania, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ventura, R (reprint author), Citta Univ Catania, Osservatorio Astrofis Catania, Via S Sofia 78, I-95125 Catania, Italy. NR 28 TC 0 Z9 0 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 DEC PY 2002 VL 395 IS 3 BP 975 EP U18 DI 10.1051/0004-6361:20021369 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 616ER UT WOS:000179291200026 ER PT J AU Croft, RAC Hernquist, L Springel, V Westover, M White, M AF Croft, RAC Hernquist, L Springel, V Westover, M White, M TI High-redshift galaxies and the Ly alpha forest in a cold dark matter universe SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; cosmology : theory; intergalactic medium; large-scale structure of universe; methods : N-body simulations; quasars : absorption lines ID LYMAN-BREAK GALAXIES; INTERGALACTIC MEDIUM; RADIATIVE-TRANSFER; COSMOLOGICAL REIONIZATION; NUMERICAL COSMOLOGY; SUPERNOVA FEEDBACK; METAL ENRICHMENT; SCALE STRUCTURE; POWER SPECTRUM; DWARF GALAXIES AB We use a cosmological hydrodynamic simulation of a cold dark matter universe to investigate theoretically the relationship between high-redshift galaxies and the Lyalpha forest at redshift z = 3. Galaxies in the simulation are surrounded by halos of hot gas, which nevertheless contain enough neutral hydrogen to cause a Lyalpha flux decrement, its strength increasing with galaxy mass. A comparison with recent observational data by Adelberger et al. on the Lyalpha forest around galaxies reveals that actual galaxies may have systematically less Lyalpha absorption within 1 Mpc of them than our simulated galaxies. In order to investigate this possibility, we add several simple prescriptions for galaxy feedback on the intergalactic medium (IGM) to the evolved simulation. These include the effect of photoionizing background radiation coming from galactic sources, galactic winds whose only effect is to deposit thermal energy into the IGM, and another, kinetic model for winds, which are assumed to evacuate cavities in the IGM around galaxies. We find that only the latter is able to produce a large effect, enough to match the tentative observational data, given the energy available from star formation in the simulated galaxies. Another intriguing possibility is that a selection effect is responsible, so that galaxies with low Lyalpha absorption are preferentially included in the sample. This is also viable but predicts galaxy properties (including clustering) that are very different from the other scenarios. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Max Planck Inst Astrophys, D-85748 Garching, Germany. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Croft, RAC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI White, Martin/I-3880-2015; Croft, Rupert/N-8707-2014 OI White, Martin/0000-0001-9912-5070; Croft, Rupert/0000-0003-0697-2583 NR 80 TC 53 Z9 53 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 DEC 1 PY 2002 VL 580 IS 2 BP 634 EP 652 DI 10.1086/343889 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DG UT WOS:000179458300002 ER PT J AU Kim, S Martin, CL Stark, AA Lane, AP AF Kim, S Martin, CL Stark, AA Lane, AP TI Antarctic Submillimeter Telescope and Remote Observatory observations of CO J=7 -> 6 and J=4 -> 3 emission toward the Galactic center region SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : abundances; Galaxy : center; ISM : general; ISM : molecules; submillimeter ID C-12/C-13 ISOTOPE RATIO; CENTER MOLECULAR CLOUDS; GAS; KINEMATICS; GALAXY; AST/RO; GHZ AB We present position-velocity strip maps of the Galactic center region in the CO J = 7 --> 6 and J = 4 --> 3 transitions observed with the Antarctic Submillimeter Telescope and Remote Observatory located at the Amundsen-Scott South Pole Station. Emission from the two rotational transitions of (CO)-C-12 was mapped at b = 0degrees for 3.degrees5 > l > -1.degrees5 on a 1' grid with a FWHM beam size of 58" at 806 GHz and 105" at 461 GHz. Previous observations of CO J = 4 --> 3 (C. L. Martin et al., in preparation) and of [C I] emission (Ojha et al.) from this region show that these lines are distributed in a manner similar to CO J = 1 --> 0 (Stark et al.); the (CO J = 4 -->3)/(CO J = 1 --> 0) line ratio map is almost featureless across the entire Galactic center region. In contrast, the CO J = 7 --> 6 emission from the Galactic center is strongly peaked toward the Sgr A and Sgr B molecular complexes. A large velocity gradient analysis shows that, aside from the two special regions Sgr A and Sgr B, the photon-dominated regions within a few hundred parsecs of the Galactic center are remarkably uniform in mean density and kinetic temperature at n = 2500-4000 cm(-3) and T = 30-45 K. The (CO J = 7 --> 6)/(CO J = 4 --> 3) line temperature ratios near Sgr B are a factor of 2 higher than those observed in the nuclear region of the starburst galaxy M82 (Mao et al.), while the CO(J = 7 --> 6)/CO(J = 4 --> 3) line temperature ratios around Sgr A are similar to M82. The line ratio on large scales from the Galactic center region is an order of magnitude less than that from M82. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 26 Z9 26 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 DEC 1 PY 2002 VL 580 IS 2 BP 896 EP 903 DI 10.1086/343842 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DG UT WOS:000179458300024 ER PT J AU Slane, P Chen, Y Lazendic, JS Hughes, JP AF Slane, P Chen, Y Lazendic, JS Hughes, JP TI An ASCA study of the high-luminosity supernova remnant G349.7+0.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiation mechanisms : thermal; supernovae : individual (G349.7+0.2); X-rays : ISM ID X-RAY; MOLECULAR CLOUDS; GALACTIC PLANE; MASER EMISSION; N132D; BUBBLES AB We present ASCA observations of supernova remnant (SNR) G349.7+0.2. The remnant has irregular shell morphology and is interacting with a molecular cloud, evident from the presence of OH (1720 MHz) masers and shocked molecular gas. The X-ray morphology is consistent with that at radio wavelengths, with a distinct enhancement in the south. The X-ray emission from the SNR is well described by a model of a thermal plasma that has yet to reach ionization equilibrium. The hydrogen column of similar to6.0 x 10(22) cm(-2) is consistent with the large distance to the remnant of similar to22 kpc estimated from the maser velocities. We derive an X-ray luminosity of L-X(0.5-10.0 keV) = 1.8 x 10(37) d(22)(2) ergs s(-1), which makes G349.7+0.2 one of the most X-ray luminous shell-type SNRs known in the Galaxy. The age of the remnant is estimated to be similar to2800 yr. The ambient density and pressure conditions appear similar to those inferred for luminous compact SNRs found in starburst regions of other galaxies and provide support for the notion that these may be the result of SNR evolution in the vicinity of dense molecular clouds. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 29 TC 19 Z9 19 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 DEC 1 PY 2002 VL 580 IS 2 BP 904 EP 908 DI 10.1086/343891 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DG UT WOS:000179458300025 ER PT J AU Keto, E AF Keto, E TI On the evolution of ultracompact HII regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; HII regions; hydrodynamics ID STARS AB The classic model for the pressure-driven expansion of H II regions is reevaluated to include the gravitational force of the star responsible for the H II region. The model shows that the gravitational attraction of the star maintains a steep density gradient and accretion flow within the ionized gas and prevents the H II region from expanding hydrodynamically unless the radius of ionization equilibrium is beyond the radius where the sound speed of the ionized gas approximates the escape velocity. Once past this critical radius, the H II region will expand rapidly and the accretion flow through the H II region is quickly reduced. However, in contrast to the model without gravity in which the velocity of the ionized gas is everywhere outward, in the model with gravity, the velocity within the H II region is always inward. Newly formed massive stars within dense molecular cores may initially form very small H II regions that at first evolve slowly through an increase in ionizing flux, as would be caused by an increase in the mass or number of stars through continuing accretion through the H II region. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 79 Z9 79 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 DEC 1 PY 2002 VL 580 IS 2 BP 980 EP 986 DI 10.1086/343794 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DG UT WOS:000179458300033 ER PT J AU Remillard, RA Muno, MP McClintock, JE Orosz, JA AF Remillard, RA Muno, MP McClintock, JE Orosz, JA TI Evidence for harmonic relationships in the high-frequency quasi-periodic oscillations of XTE J1550-564 and GRO J1655-40 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (GRO J1655-40, XTE J1550-564); stars : oscillations; X-rays : stars ID RELATIVISTIC DISKOSEISMOLOGY; RXTE OBSERVATIONS; GRS-1915+105; OUTBURST; MODES AB We continue to investigate the X-ray properties of the black hole binary XTE J1550-564. By grouping observations (1998-1999) according to the type of low-frequency quasiperiodic oscillation (LFQPO) identified in a previous paper, we show evidence that two high-frequency QPOs (HFQPOs) occur simultaneously near 184 and 276 Hz. We can model the QPO profiles while assuming that the central frequencies are related by a 3:2 ratio. In one group, there is some evidence of a broad feature at the fundamental frequency of 92 Hz. We also investigate the 2000 April outburst, and we confirm the suggestion of Miller et al. that a 270 Hz QPO is accompanied by a second feature near 180 Hz. The histogram for the 28 individual HFQPO detections in XTE J1550-564 shows two peaks near 184 and 276 Hz, while there is a notable exception in the 143 Hz QPO detected on 1998 October 15. Similarly, all of the 13 HFQPO detections in the black hole binary GRO J1655-40 occur at two frequencies that are related by a 3:2 ratio. We next investigate all of the energy spectra for XTE J1550-564, and we find a systematic increase in the strength of the power-law component as the stronger of the two HFQPOs shifts from 276 to 184 Hz. A strikingly similar result is seen in the spectra of GRO J1655-40 when the stronger HFQPO shifts from 450 to 300 Hz. The fundamental HFQPO frequencies for the two X-ray sources scale as M-1, which is consistent with the hypotheses that these HFQPOs represent some kind of oscillation rooted in general relativity (GR) and that the two black holes have similar values of the dimensionless spin parameter. We discuss physical mechanisms that may explain these HFQPOs. A resonance between orbital and radial coordinate frequencies is one possibility suggested by Abramowicz & Kluzniak. For XTE J1550-564, this would imply moderate values for the dimensionless spin parameter (0.1 < a(*) < 0.6), with similar results for GRO J1655-40. A resonance between polar and radial coordinate frequencies allows additional values for a(*) above 0.9. There remain serious uncertainties regarding the physical mechanism whereby resonances in coordinate frequencies may produce HFQPOs. We also discuss models for "diskoseismic'' oscillations. In this case, the concept that the inner disk behaves as a resonance cavity in GR has certain attractions for explaining HFQPOs, but integral harmonics are not predicted for the three types of diskoseismic modes derived for adiabatic perturbations in a thin accretion disk. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Utrecht, Inst Astron, NL-3508 TA Utrecht, Netherlands. RP Remillard, RA (reprint author), MIT, Ctr Space Res, Cambridge, MA 02139 USA. NR 40 TC 121 Z9 121 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 DEC 1 PY 2002 VL 580 IS 2 BP 1030 EP 1042 DI 10.1086/343791 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DG UT WOS:000179458300038 ER PT J AU Galloway, DK Sokoloski, JL Kenyon, SJ AF Galloway, DK Sokoloski, JL Kenyon, SJ TI Correlated radial velocity and X-ray variations in HD 154791/4U 1700+24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : symbiotic; stars : individual (HD 154791); stars : neutron; X-rays : binaries ID MAGNETIC NEUTRON STARS; ACCRETION; GX-1+4; PERIOD; V2116-OPHIUCHI; VARIABILITY; CATALOG; PULSAR AB We present evidence for approximately 400 day variations in the radial velocity of HD 154791 (V934 Her), the suggested optical counterpart of 4U 1700+24. The variations are correlated with the previously reported approximate to400 day variations in the X-ray flux of 4U 1700+24, which supports the association of these two objects, as well as the identi. cation of this system as the second known X-ray binary in which a neutron star accretes from the wind of a red giant. The HD 154791 radial velocity variations can be fitted with an eccentric orbit with period 404 +/- 3 days, amplitude K = 0.75 +/- 0.12 km s(-1), and eccentricity e = 0.26 +/- 0.15. There are also indications of variations on longer timescales e 2000 days. We have reexamined all available All-Sky Monitor (ASM) data following an unusually large X-ray outburst in 1997-1998 and confirm that the 1 day averaged 2-10 keV X-ray flux from 4U 1700+24 is modulated with a period of 400 +/- 20 days. The mean pro. le of the persistent X-ray variations was approximately sinusoidal, with an amplitude of 0.108 +/- 0.012 ASM counts s(-1) (corresponding to 31% rms). The epoch of X-ray maximum was approximately 40 days after the time of periastron, according to the eccentric orbital fit. If the 400 day oscillations from HD 154791/4U 1700+24 are due to orbital motion, then the system parameters are probably close to those of the only other neutron star symbiotic-like binary, GX 1+4. We discuss the similarities and differences between these two systems. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Galloway, DK (reprint author), MIT, Ctr Space Res, Cambridge, MA 02139 USA. OI Galloway, Duncan/0000-0002-6558-5121; Kenyon, Scott/0000-0003-0214-609X NR 24 TC 18 Z9 19 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 DEC 1 PY 2002 VL 580 IS 2 BP 1065 EP 1069 DI 10.1086/343798 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DG UT WOS:000179458300042 ER PT J AU Kashyap, VL Drake, JJ Gudel, M Audard, M AF Kashyap, VL Drake, JJ Gudel, M Audard, M TI Flare heating in stellar coronae SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; methods : statistical; stars : coronae; stars : flare; stars : late-type; X-rays : stars ID X-RAY-EMISSION; WAITING-TIME DISTRIBUTION; CANUM-VENATICORUM SYSTEMS; LATE-TYPE STARS; SOLAR-FLARES; STATISTICAL FLARE; ACTIVE STARS; ULTRAVIOLET OBSERVATIONS; FREQUENCY-DISTRIBUTIONS; MICROFLARING ACTIVITY AB An open question in the field of solar and stellar astrophysics is the source of heating that causes stellar coronae to reach temperatures of millions of degrees. One possibility is that the coronae are heated by a large number of small flares. On the Sun, flares with energies as low as those of micro flares are distributed with energy as a power law of the form (dN/dE) proportional to E(-alpha), with alpha approximate to 1.8, and alpha appears to increase to values of 2.2-2.7 for flares of lower energy. If the slope exceeds the critical value of 2, then in principle the entire coronal energy input can be ascribed to flares that are increasingly less energetic but are more numerous. Previous analyses of flares in light curves of active stars have shown that this index generally is greater than 2, although it may be as low as 1.6 when strong flares alone are considered. Here we investigate the contribution of very weak flares, covering the milliflare energy range, to the coronal luminosity of low-mass active stars. We analyze Extreme Ultraviolet Explorer/Deep Survey events data from FK Aqr, V1054 Oph, and AD Leo and conclude that in all these cases, the coronal emission is dominated by flares to such an extent that in some cases, the entire emission can be ascribed to. are heating. We have developed a new method to directly model for the first time stochastically produced. are emission, including undetectable flares, and their effects on the observed photon arrival times. We find that alpha(FK) (Aqr) = 2.60 +/- 0.34, alpha(V1054) (Oph) = 2.74 +/- 0.35, and alpha(AD) (Leo) = 2.03-2.32, and the flare component accounts for a large fraction (generally greater than 50%) of the total flux. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Paul Scherrer Inst, Astrophys Lab, CH-5232 Villigen, Switzerland. RP Kashyap, VL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vkashyap@cfa.harvard.edu; jdrake@cfa.harvard.edu; guedel@astro.phys.ethz.ch; audard@astro.phys.ethz.ch RI Guedel, Manuel/C-8486-2015 OI Guedel, Manuel/0000-0001-9818-0588 NR 69 TC 58 Z9 58 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 DEC 1 PY 2002 VL 580 IS 2 BP 1118 EP 1132 DI 10.1086/343869 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DG UT WOS:000179458300047 ER PT J AU Gaensler, BM Jones, DH Stappers, BW AF Gaensler, BM Jones, DH Stappers, BW TI An optical bow shock around the nearby millisecond pulsar J2124-3358 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : general; pulsars : individual (PSR J2124-3358); stars : neutron; stars : winds, outflows ID H-I AB We report the discovery of an Halpha-emitting bow shock nebula powered by the nearby millisecond pulsar J2124-3358. The bow shock is very broad and is highly asymmetric about the pulsar's velocity vector. This shape is not consistent with that expected for the case of an isotropic wind interacting with a homogeneous ambient medium. Models that invoke an anisotropy in the pulsar wind, a bulk flow of the surrounding gas, or a density gradient in the ambient medium either perpendicular or parallel to the pulsar's direction of motion also fail to reproduce the observed morphology. However, we find an ensemble of good fits to the nebular morphology when we consider a combination of these effects. In all such cases, we find that the pulsar is propagating through an ambient medium of mean density 0.8-1.3 cm(-3) and bulk flow velocity similar to15-25 km s(-1) and that the star has recently encountered an increase in density by 1-10 cm(-3) over a scale less than or similar to0.02 pc. The wide variety of models that fit the data demonstrate that in general there is no unique set of parameters that can be inferred from the morphology of a bow shock nebula. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, Santiago 19, Chile. Univ Chile, Observ Cerro Calan, Dept Astron, Santiago, Chile. Stichting ASTRON, Dwingeloo, Netherlands. Sterrenkunding Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 20 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 DEC 1 PY 2002 VL 580 IS 2 BP L137 EP L141 DI 10.1086/345750 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DL UT WOS:000179458700011 ER PT J AU Kong, AKH Garcia, MR Primini, FA Murray, SS AF Kong, AKH Garcia, MR Primini, FA Murray, SS TI The discovery of a spatially resolved supernova remnant in M31 with Chandra SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); supernova remnants; X-rays : ISM ID X-RAY SPECTROSCOPY; NOVA REMNANTS; ROSAT HRI; ABUNDANCES; CANDIDATES; GALAXY; M-31 AB Chandra observations of M31 allow the first spatially resolved X-ray image of a supernova remnant (SNR) in an external spiral galaxy. CXOM31 J004327.7 + 411829 is a slightly elongated ring-shaped object with a diameter of similar to11" (42 pc). In addition, the X-ray image hints that the chemical composition of the SNR is spatial dependent. The X-ray spectrum of the SNR can be well fitted with a Raymond-Smith model or a nonequilibrium ionization model. Depending on the spectral model, the 0.3-7 keV luminosity is between and 3.2 x 10(36) and 4.5 x 10(37) ergs s(-1). The age of the SNR is estimated to be 3210-22,300 yr, and the number density of ambient gas is similar to0.003-0.3 cm(-3). This suggests that the local interstellar medium around the SNR is low. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Primini, Francis/0000-0002-6077-0643 NR 22 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 DEC 1 PY 2002 VL 580 IS 2 BP L125 EP L128 DI 10.1086/345610 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DL UT WOS:000179458700008 ER PT J AU Millan-Gabet, R Monnier, JD AF Millan-Gabet, R Monnier, JD TI Discovery of a near-infrared jetlike feature in the Z Canis Majoris system SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; instrumentation : adaptive optics; planetary systems : protoplanetary disks; stars : formation; techniques : high angular resolution ID KECK-II-TELESCOPE; Z-CMA; MOLECULAR OUTFLOWS; BINARY STAR; IMAGES; INTERFEROMETRY; COMPANION; OBJECTS; SCALE; JET AB We present near-infrared high-resolution observations of the young binary system Z Canis Majoris using the adaptive optics system at the Keck II telescope. Both components are unresolved at 1.25 and 1.65 mum, although high dynamic range images reveal a previously unknown jetlike feature in the circumstellar environment. We argue that this feature probably arises from light scattered off the walls of a jet-blown cavity, and proper-motion studies of this feature can probe the dynamics of the bipolar outflow. Potentially, the morphology of the dust-laden cavity walls offers a new probe of the momentum profile and collimation of bipolar winds from young stellar objects. We also derive high-precision binary parameters, which when combined with historical data have allowed the first detection of orbital motion. Finally, our observations confirm the high degree of flux variability in the system; the northwest binary component is dominant at the H band, in contrast to all previous observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Millan-Gabet, R (reprint author), CALTECH, Interferometry Sci Ctr, Pasadena, CA 91125 USA. OI Monnier, John D/0000-0002-3380-3307 NR 26 TC 15 Z9 15 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 DEC 1 PY 2002 VL 580 IS 2 BP L167 EP L170 DI 10.1086/345590 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DL UT WOS:000179458700017 ER PT J AU Wolk, SJ Bourke, TL Smith, RK Spitzbart, B Alves, J AF Wolk, SJ Bourke, TL Smith, RK Spitzbart, B Alves, J TI Discovery of nonthermal X-ray emission from the embedded massive star-forming region RCW 38 SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (RCW 38); stars : formation; X-rays : diffuse background; X-rays : stars ID H-II REGIONS; SUPERNOVA-REMNANTS; SOUTHERN; CLUSTER AB We report on results of a 96.7 ks Chandra observation of one of the youngest, most embedded and massive young stellar clusters studied to date in X-rays-RCW 38. We find a region of extended emission about 1.25 x 1.75 pc. The emission is consistent with synchrotron emission. The power index of the emission steepens toward 1.75 the cluster core, implying that the magnetic field originates there. This is the first evidence of synchrotron emission filling a region of active star formation. The source of the necessary magnetic field is unclear. We measure the hydrogen column to the emission and find that N-H increases from 7.6 x 10(21) to 1.61 x 10(22) cm(-2), increasing from the northwest to the southeast quadrants of the cluster, consistent with near-infrared extinction data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Munich, Germany. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261; Alves, Joao/0000-0002-4355-0921 NR 22 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 DEC 1 PY 2002 VL 580 IS 2 BP L161 EP L165 DI 10.1086/345611 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619DL UT WOS:000179458700016 ER PT J AU Kuraszkiewicz, JK Green, PJ Forster, K Aldcroft, TL Evans, IN Koratkar, A AF Kuraszkiewicz, JK Green, PJ Forster, K Aldcroft, TL Evans, IN Koratkar, A TI Emission line properties of active galactic nuclei from a pre-costar Faint Object Spectrograph Hubble Space Telescope spectral atlas SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : active; quasars : emission lines; quasars : general; ultraviolet : galaxies ID OPTICALLY SELECTED QUASARS; X-RAY PROPERTIES; REDSHIFT QUASARS; COMPLETE SAMPLE; QSOS; IONIZATION; EVOLUTION; CONTINUUM; REGION; LIMITS AB UV/optical emission lines offer some of the most detailed information obtainable about the intrinsic properties of quasars. Studies of the density, ionization and metal abundance of gas near the accreting black hole are probed through an intriguing but poorly understood complex of correlations between emission lines and overall quasar spectral energy distributions that has long suffered from a lack of large, consistently measured samples. As part of a broader effort to expand and systematize the data upon which these studies are built, we present measurements of the UV/optical emission line parameters in a sample of 158 active galactic nuclei observed with the Faint Object Spectrograph on the Hubble Space Telescope (HST), prior to the installation of COSTAR. We use an automated technique that accounts for galactic reddening, includes iron emission blends, galactic and intrinsic absorption lines, and performs multicomponent fits to the emission line profiles. We present measured line parameters ( equivalent width and FWHM) for a large number (28) of different UV/optical lines, including upper limits for undetected lines. We also study the relations between the emission line equivalent widths and luminosity (the Baldwin effect), as well as redshift ( evolution). We compare results from this HST FOS sample with our previous measurements of 993 QSOs in the Large Bright Quasar Survey using the same analysis technique and sum the samples to achieve better coverage of the luminosity-redshift plane. We confirm a significant Baldwin effect for UV iron emission from Green et al. and find that evolution dominates the effect for iron and for Si IV emission. The values of the Baldwin effect slopes for all UV emission lines and the dependence of the slopes on the sample's luminosity range point to a change of the SED as the cause of the Baldwin effect in the FOS sample. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Kuraszkiewicz, JK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 43 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 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2002 VL 143 IS 2 BP 257 EP 276 DI 10.1086/342789 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 617KX UT WOS:000179361800002 ER PT J AU Moegenburg, SM AF Moegenburg, SM TI Spatial and temporal variation in hydrochory in Amazonian floodplain forest SO BIOTROPICA LA English DT Article ID SEED DISPERSAL; TUPELO SWAMP; REGENERATION; RIVERS; WATER; ANTS; RAIN AB The hypothesis that water depth, plant species, and the presence of submerged substrates influence seed dispersal by water was tested in a whitewater tributary of the Tocantins River of the Amazon Basin. Seed dispersal was greatest when water depth was greatest, which occurred during the new moon. Seeds of buoyant species with smaller seeds required less water for dispersal than large seeded species. Submerged objects reduced the distance dispersed but not the probability of dispersal. C1 Univ Florida, Dept Zool, Gainesville, FL 32611 USA. RP Moegenburg, SM (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. NR 32 TC 16 Z9 18 U1 3 U2 13 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD DEC PY 2002 VL 34 IS 4 BP 606 EP 612 DI 10.1111/j.1744-7429.2002.tb00581.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 637XV UT WOS:000180539800015 ER PT J AU Lin, J AF Lin, J TI Energetics and propagation of coronal mass ejections in different plasma environments SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article DE Sun : CMEs; Sun : atmosphere; Sun : magnetic fields ID YOHKOH SXT IMAGES; CURRENT SHEET; SOLAR CORONA; FLARE; RECONNECTION; DENSITY; ARCHES AB Based on previous work, we investigate the propagation of CMEs in a more realistic plasma environment than the isothermal atmosphere, and find that it is a slightly faster reconnection for flux ropes to break free. The average Alfven Mach number M(A) for the inflow into the reconnection site has to be at least 0.013 in order to give a plausible eruption (compared to M(A) = 0.005 for the isothermal atmosphere). Taking M(A) = 0.1, we find that the energy output and the electric field induced inside the current sheet match the temporal behavior inferred from the energetic, long duration, CME-associated X-ray events. The results indicate that catastrophic loss of equilibrium in the coronal magnetic field provides the most promising mechanism for major solar eruptions, and that the more energetic the eruption is, the earlier the associated flare peaks. The variation of the output power with the background field strength revealed by our calculations implies the poor correlation between slow CMEs and solar flares. This work also further confirms the explanation we proposed for the peculiar motion of giant X-ray arches and anomalous post-flare loops. Their kinematic pattern and observed heights are determined by the local Alfven speed and its variation with height. 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 29 TC 56 Z9 61 U1 1 U2 1 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1009-9271 J9 CHINESE J ASTRON AST JI Chin. J. Astron. Astrophys. PD DEC PY 2002 VL 2 IS 6 BP 539 EP 556 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 631YJ UT WOS:000180195600006 ER PT J AU Hall, JPW Harvey, DJ AF Hall, JPW Harvey, DJ TI Basal subtribes of the Nymphidiini (Lepidoptera : Riodinidae): phylogeny and myrmecophily SO CLADISTICS LA English DT Article ID LARGE DATA SETS; BUTTERFLIES; REVISION; THISBE; TREES; ANTS; INFERENCE; ECOLOGY; CHARIS; LIMITS AB Three cladistic analyses, based predominantly on adult morphology, are presented for myrmecophilous riodinid butterflies in the tribe Nymphidiini, The first is a species-level analysis of all 22 species recognized here in Aricoris ( = Audre auctt.) using 27 characters. The second is a species-level analysis of all 24 species recognized here in Synargis using 53 characters. The third is a generic-level analysis of all six genera (Aricoris, Ariconias n. gen., Lemonias. Thishe, Juditha, and Synargis) recognized here as belonging in the basal clades of the Nymphidiini (=Lemoniadina auctt.) using 17 characters. with members of the Theopeina and Nymphidiina included with the ingroup to assess the monophyly of subtribes. Almost all characters are illustrated. The first analysis indicates that Aricoris consists of five monophyletic species groups, with the relationship ((constantius gr. + colchis gr.) + (chilensis gr. + (aurinia gr. + epulus gr.))), and contains the type species of Eiseleia and Audre. which are synonymized with Aricoris (n. syns.), The second analysis indicates that Synargis consists Of four monophyletic species groups. with the relationship (phliasus gr. + (regulus gr. + (pittheus gr. + abaris gr.))). and contains the type species of Ematurgina and Thysamota. which are synonymized with Synargis (n. syns.). The third analysis indicates that the Lemoniadina, or basal clades of the Nymphidiini, are paraphyletic with respect to the Theopeina and Nymphidiina. with the generic relationship ((Aricoris + Ariconias) + (((Lemonias + Thishe) + (Juditha + Synargis))+ (Theopeina + Nymphidiina))). We therefore restrict the Lemoniadina to include Lemonias, Thishe. Juditha, and Synargis and provide the name Aricorina n. subtribe for Aricoris and Ariconias. All nymphidiine subtribes are characterized and a synonymic checklist for the Aricorina and Lemoniadina is presented. A "supertree" composed of the species-level phylogenies derived here for Aricoris and Synargis. and those derived elsewhere for Ariconias. Lemonias, Thishe, and Juditha, is used to map the distribution of larval host plant and attending ant taxa and the occurrence of aphytophagy. Observed patterns are discussed. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. EM jpwhall@hotmail.com NR 86 TC 16 Z9 16 U1 1 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0748-3007 EI 1096-0031 J9 CLADISTICS JI Cladistics PD DEC PY 2002 VL 18 IS 6 BP 539 EP 569 AR PII S0748-3007(02)00105-6 DI 10.1016/S0748-3007(02)00105-6 PG 31 WC Evolutionary Biology SC Evolutionary Biology GA 629YV UT WOS:000180081000001 ER PT J AU Krell, FT Simon, U Zotz, G AF Krell, FT Simon, U Zotz, G TI Cetoniinae developing in a living stalk of Bromeliaceae (Coleoptera : Scarabaeidae : Cetoniinae : Gymnetini) SO COLEOPTERISTS BULLETIN LA English DT Article AB Larvae of Desicasta laevicostata (van de Poll 1886) (Coleoptera: Scarabaeidae: Cetoniinae: Gymnetini) were found developing in living stalk tissue of the bromeliad Vriesea sanguinolenta Cogn. and Marchal (Bromeliaceae) in Panama. This is the first record of Cetoniinae using living plant tissue as a larval substratum. The male of this species is described for the first time and its aedeagus is figured. C1 Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Tech Univ Munich, Lehrstuhl Landnutzungsplanung & Naturschutz, D-85354 Freising Weihenstephan, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Krell, FT (reprint author), Nat Hist Museum, Dept Entomol, Cromwell Rd, London SW7 5BD, England. OI Krell, Frank-Thorsten/0000-0001-6065-0812 NR 11 TC 5 Z9 6 U1 0 U2 1 PU COLEOPTERISTS SOC PI NATCHEZ PA PO BOX 767, NATCHEZ, MS 39121 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD DEC PY 2002 VL 56 IS 4 BP 533 EP 539 DI 10.1649/0010-065X(2002)056[0533:CDIALS]2.0.CO;2 PG 7 WC Entomology SC Entomology GA 630DN UT WOS:000180092400008 ER PT J AU Alarie, Y Spangler, PJ Steiner, WE AF Alarie, Y Spangler, PJ Steiner, WE TI Larval morphology of Agabetes Crotch (Coleoptera : Adephaga : Dytiscidae): The hypothesis of sister-group relationship with the subfamily Laccophilinae revisited SO COLEOPTERISTS BULLETIN LA English DT Article ID NEARCTIC COLYMBETINAE COLEOPTERA; PHYLOGENETIC-RELATIONSHIPS; GENERA; SHARP AB Description of all larval instars of Agabetes acuductus (Harris) is presented including a detailed chaetotaxic and porotaxic analysis of the cephalic capsule, head appendages, legs, last abdominal segment and urogomphi. A parsimony analysis based on the 43 informative larval characteristics was conducted with PAUP. Boostrap values indicate strong support for the monophyly of the clade containing the genus Agabetes Crotch and members of the subfamily Laccophilinae. This is supported by five synapomorphies: (i) egg bursters positioned posteriorly, contiguous to the coronal suture, (ii) presence of two lamellae clypeales in instar I, (iii) absence of the primary setae LA10 and LA12, (iv) absence of a ventroapical spinula on antennomere 3, and (v) abdominal venter 6 sclerotized. C1 Laurentian Univ, Dept Biol, Sudbury, ON P3E 2C6, Canada. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Alarie, Y (reprint author), Laurentian Univ, Dept Biol, Ramsey Lake Rd, Sudbury, ON P3E 2C6, Canada. NR 25 TC 11 Z9 12 U1 0 U2 1 PU COLEOPTERISTS SOC PI NATCHEZ PA PO BOX 767, NATCHEZ, MS 39121 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD DEC PY 2002 VL 56 IS 4 BP 547 EP 567 DI 10.1649/0010-065X(2002)056[0547:LMOACC]2.0.CO;2 PG 21 WC Entomology SC Entomology GA 630DN UT WOS:000180092400011 ER PT J AU Hooper, E Condit, R Legendre, P AF Hooper, E Condit, R Legendre, P TI Responses of 20 native tree species to reforestation strategies for abandoned farmland in Panama SO ECOLOGICAL APPLICATIONS LA English DT Article DE abandoned farmland; exotic grasses; fire effects; natural regeneration; Panama; Saccharum spontaneum; secondary succession; shade tolerance; tropical reforestation ID COSTA-RICA; RAIN-FOREST; PLANT SUCCESSION; EASTERN AMAZONIA; GROWTH; ESTABLISHMENT; PASTURE; PLANTATIONS; SURVIVAL; RESTORATION AB Deforestation in the tropics often leads to unproductive agriculture and results in abandoned, degraded grasslands that tree species recolonize poorly. To evaluate why forests do not regenerate naturally and to identify potential species for use in reforestation of degraded areas, we planted 15 000 seeds of 20 native tree species, varying in seed size and shade tolerance, in abandoned Panamanian farmland dominated by the exotic grass, Saccharum spontaneum. To determine the effects of above- and belowground constraints on tree seedling germination, survival, and growth, we used four mowing and shading treatments of the Saccharum. Shading the Saccharum effectively eliminated it, whereas mowing led to increased light aboveground, but did not reduce Saccharum growth rate. Germination, survival, and growth of tree seedlings approximately doubled in shade treatments compared to the unshaded control, but were lowest when the Saccharum was mowed three times. Fire significantly decreased germination and survival. Some species did not follow these general trends, however: we identified four species groups that varied in their response to Saccharum competition. Very small-seeded, light-demanding species performed poorly, and we do not recommend their use in reforestation because they tolerate neither above- nor belowground constraints imposed by the Saccharum. Light-demanding species with large seeds were limited by aboveground constraints, namely, shading. Small-seeded, shade-tolerant species were limited by belowground constraints imposed by the Saccharum. Large-seeded, moderately to highly shade-tolerant species performed well in the Saccharum; we recommend a reforestation strategy that includes planting this last group. C1 McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. Univ Montreal, Dept Sci Biol, Montreal, PQ H3C 3J7, Canada. RP Hooper, E (reprint author), Univ Illinois, Dept Biol Sci, M-C 066,845 W Taylor St, Chicago, IL 60607 USA. NR 50 TC 97 Z9 109 U1 5 U2 40 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 DEC PY 2002 VL 12 IS 6 BP 1626 EP 1641 DI 10.1890/1051-0761(2002)012[1626:RONTST]2.0.CO;2 PG 16 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 628HD UT WOS:000179986700006 ER PT J AU Sheehy, D AF Sheehy, D TI Poetry and violence: The ballad tradition of Mexico's Costa Chica SO ETHNOMUSICOLOGY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Sheehy, D (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC ETHNOMUSICOLOGY INC PI BLOOMINGTON PA MORRISON HALL, ROOM 005 INDIANA UNIVERSITY, BLOOMINGTON, IN 47405 USA SN 0014-1836 J9 ETHNOMUSICOLOGY JI Ethnomusicology PD WIN PY 2002 VL 46 IS 1 BP 177 EP 179 DI 10.2307/852816 PG 3 WC Music SC Music GA 513NV UT WOS:000173385400015 ER PT J AU Ross, AH Ubelaker, DH Falsetti, AB AF Ross, AH Ubelaker, DH Falsetti, AB TI Craniometric variation in the Americas SO HUMAN BIOLOGY LA English DT Article DE New World; craniometrics; multivariate statistics; human variation ID PREHISTORIC ANDEAN POPULATIONS; AZAPA VALLEY; GENE FLOW; CHILE; MICROEVOLUTION; AFFINITIES; PATTERNS; KINSHIP; ORIGINS; SHAPE AB Craniofacial variation is investigated in Latin America and the Caribbean. The samples included in this study are two historic and one prehistoric sample from Ecuador; prehistoric and modem Cuban samples; a prehistoric Peruvian sample; two prehistoric Mexican samples and one contemporary admixed Mexican sample; a 16th/17th-century Spanish sample; and Terry blacks. Biological distance is investigated using traditional craniometrics by computing size and shape variables according to Mosimann and colleagues. This study shows that there is much biological variation within the Americas. C1 Univ Florida, CA Pound Human Identificat Lab, Gainesville, FL 32611 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Anthropol, Washington, DC 20560 USA. RP Ross, AH (reprint author), Univ Florida, CA Pound Human Identificat Lab, Gainesville, FL 32611 USA. OI Ross, Ann/0000-0001-8780-1414 NR 48 TC 14 Z9 14 U1 0 U2 7 PU WAYNE STATE UNIV PRESS PI DETROIT PA 4809 WOODWARD AVE, DETROIT, MI 48201-1309 USA SN 0018-7143 J9 HUM BIOL JI Hum. Biol. PD DEC PY 2002 VL 74 IS 6 BP 807 EP 818 DI 10.1353/hub.2003.0010 PG 12 WC Biology; Genetics & Heredity SC Life Sciences & Biomedicine - Other Topics; Genetics & Heredity GA 652LJ UT WOS:000181380400005 PM 12617490 ER PT J AU Krasnopolsky, VA Christian, DJ Kharchenko, V Dalgarno, A Wolk, SJ Lisse, CM Stern, SA AF Krasnopolsky, VA Christian, DJ Kharchenko, V Dalgarno, A Wolk, SJ Lisse, CM Stern, SA TI X-ray emission from Comet McNaught-Hartley (C/1999 T1) SO ICARUS LA English DT Article ID EXTREME-ULTRAVIOLET EMISSION; SELECTIVE ELECTRON-CAPTURE; SOLAR-WIND IONS; HALE-BOPP; SLOW COLLISIONS; CHARGE-TRANSFER; HYAKUTAKE; O1; SPECTROSCOPY; SUBSHELLS AB Comet McNaught-Hartley was observed in five 1-h exposures on January 8-14 2001 using the advanced CCD imaging spectrometer on board the Chandra X-ray Observatory. The X-ray image of the comet does not show a crescent-like shape. The brightest region is offset from the nucleus between the sunward and comet velocity directions. The comet mean X-ray luminosity is equal to 7.8 x 10(15) erg s(-1) for photon energy E > 150 eV and aperture rho = 1.5 x 10(5) km where the comet X-ray brightness exceeds 20% of the peak value. Gas production rate was 10(29) s(-1) during the observations, and the efficiency of X-ray excitation was equal to 4 x 10(-14) erg AU(3/2). Dayto-day variations in X-rays reached a factor of 5. The strongest short-term variation was by a factor of 1.75 for 1600 s. This variation may be explained by a decline in the solar-wind flux by the same factor in approximate to800 s. The comet and Earth were seeing different faces of the Sun, and time delay in the solar-wind events on the Earth and the comet was long, equal to 6 days. The best correlation between the comet X-ray luminosity and the solar-wind proton density is for the time delay of 5.5 days and may be explained by the higher velocity of heavy ions. Careful background subtraction made it possible to extract the comet spectrum from 150 to 1000 eV. No signal was detected at E > 1000 eV, and a 3sigma upper limit to any emission with E > 1000 eV is 0.3% of the photon emission at 150-1000 eV. The best chi(2)-fit model to the spectrum consists of nine narrow emission features. The emission energies and intensities are in good agreement with a charge exchange spectrum calculated by us for the slow solar wind. Using this spectrum, we identify the observed emissions as (Ne(7+) + Mg(7+) + Mg(8+)) at 195 eV, (Mg(8+) + Mg(9+) + Si(8+)) at 250 eV, C(5+) at 370 and 460 eV, O(6+) at 560 eV, 071 at 650, 780, and 840 eV, and Ne(8+) at 940 eV. X-ray spectroscopy of comets may be used to diagnose the solar-wind composition and its interaction with comets. (C) 2002 Elsevier Science (USA). C1 Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. RP Krasnopolsky, VA (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave, Washington, DC 20064 USA. EM vkrasn@verizonmail.com RI Krasnopolsky, Vladimir/L-5085-2013; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Wolk, Scott/0000-0002-0826-9261; Christian, Damian/0000-0003-1746-3020 NR 39 TC 48 Z9 48 U1 0 U2 3 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 DEC PY 2002 VL 160 IS 2 BP 437 EP 447 DI 10.1006/icar.2002.6965 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 628HR UT WOS:000179988000015 ER PT J AU Bermingham, E AF Bermingham, E TI Evolutionary assembly of the Mesoamerican freshwater fish fauna. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Smithsonian Trop Res Inst, Balboa, Panama. NR 0 TC 2 Z9 2 U1 2 U2 2 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 DEC PY 2002 VL 42 IS 6 BP 1195 EP 1195 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600076 ER PT J AU Buskirk, SW Wisely, SM Russell, GA Aubry, KB Zielinski, WJ AF Buskirk, SW Wisely, SM Russell, GA Aubry, KB Zielinski, WJ TI Phylogeography of fishers in the Pacific Northwest. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Univ Wyoming, Laramie, WY 82071 USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 1 U2 2 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 DEC PY 2002 VL 42 IS 6 BP 1204 EP 1205 PG 2 WC Zoology SC Zoology GA 669ND UT WOS:000182356600121 ER PT J AU Johnson, GD AF Johnson, GD TI Diversity of the Acanthomorpha. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 DEC PY 2002 VL 42 IS 6 BP 1251 EP 1251 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600355 ER PT J AU Kohn, AJ Duda, TF AF Kohn, AJ Duda, TF TI Genetic, morphological and ecological differentiation in Conus ebraeus, a Pan-Indo-Pacific zoogeographic species. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Smithsonian Trop Res Stn, Washington, DC USA. Univ Washington, Seattle, WA 98195 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 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 DEC PY 2002 VL 42 IS 6 BP 1259 EP 1259 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600391 ER PT J AU Lynch, K Rand, AS Ryan, M Wilczynski, W AF Lynch, K Rand, AS Ryan, M Wilczynski, W TI The interaction between motivation to mate and permissiveness in female mate choice. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Univ Texas, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 DEC PY 2002 VL 42 IS 6 BP 1269 EP 1269 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600443 ER PT J AU Nichols, SA Barnes, PAG Hickman, CS AF Nichols, SA Barnes, PAG Hickman, CS TI Biodiversity, and distribution with respect to substrate and depth, of marine sponges of the Caribbean coast of Panama. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Univ Calif Berkeley, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 DEC PY 2002 VL 42 IS 6 BP 1285 EP 1285 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600520 ER PT J AU Parenti, LR Grier, HJ AF Parenti, LR Grier, HJ TI Evolution and phylogeny of gonad morphology in bony fishes. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Natl Museum Nat Hist, Washington, DC 20560 USA. Smithsonian Inst, Washington, DC 20560 USA. Florida Marine Res Inst, Stock Enhancement Res Facil, St Petersburg, FL USA. NR 0 TC 0 Z9 0 U1 0 U2 1 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 DEC PY 2002 VL 42 IS 6 BP 1291 EP 1291 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600550 ER PT J AU Stach, TG AF Stach, TG TI Evolution of the serotonergic nervous system in Chordata. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 DEC PY 2002 VL 42 IS 6 BP 1317 EP 1317 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600677 ER PT J AU Suarez, RK Darveau, CA O'Brien, DM Roubik, DW AF Suarez, RK Darveau, CA O'Brien, DM Roubik, DW TI Heirarchical and metabolic regulation in the evolution of metabolic scaling. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. Swarthmore Coll, Swarthmore, PA 19081 USA. Smithsonian Trop Res Inst, Balboa, Panama. NR 0 TC 0 Z9 0 U1 0 U2 3 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 DEC PY 2002 VL 42 IS 6 BP 1320 EP 1321 PG 2 WC Zoology SC Zoology GA 669ND UT WOS:000182356600692 ER PT J AU Sweeney, A Jiggins, C Johnsen, S AF Sweeney, A Jiggins, C Johnsen, S TI Bio-optics and visual ecology of Heliconius color patterns. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Duke Univ, Durham, NC 27706 USA. Smithsonian Trop Res Inst, Balboa, Panama. RI Jiggins, Chris/B-9960-2008 OI Jiggins, Chris/0000-0002-7809-062X NR 0 TC 1 Z9 1 U1 0 U2 2 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 DEC PY 2002 VL 42 IS 6 BP 1321 EP 1321 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600696 ER PT J AU Thacker, RW Erwin, PM Bevis, KP Paul, VJ AF Thacker, RW Erwin, PM Bevis, KP Paul, VJ TI Effects of reduced light availability on a sponge-cyanobacterial symbiosis. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 Univ Alabama, Birmingham, AL USA. Smithsonian Marine Stn, Ft Pierce, FL USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 DEC PY 2002 VL 42 IS 6 BP 1323 EP 1323 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600704 ER PT J AU Vencl, F AF Vencl, F TI Sexually selected allometries in Photinus fireflies SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 SUNY Stony Brook, Stony Brook, NY 11794 USA. Smithsonian Trop Res Inst, Bilbao, Spain. NR 0 TC 0 Z9 0 U1 0 U2 1 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 DEC PY 2002 VL 42 IS 6 BP 1327 EP 1327 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600723 ER PT J AU Wolcott, TG Wolcott, DL Hines, AH Medici, DA AF Wolcott, TG Wolcott, DL Hines, AH Medici, DA TI Migration of adult female blue crabs from mating areas to the maternity suite: when, where, and who cares? SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol C1 N Carolina State Univ, Raleigh, NC 27695 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 DEC PY 2002 VL 42 IS 6 BP 1337 EP 1337 PG 1 WC Zoology SC Zoology GA 669ND UT WOS:000182356600773 ER PT J AU Marvin, UB AF Marvin, UB TI Plate tectonics: An insider's history of the modern theory of the earth. SO ISIS LA English DT Book Review 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. NR 1 TC 0 Z9 0 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD DEC PY 2002 VL 93 IS 4 BP 754 EP 755 DI 10.1086/376063 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 657UR UT WOS:000181685200113 ER PT J AU Kaeppler, AL AF Kaeppler, AL TI Hawaiki, Ancestral Polynesia: An essay in historical anthropology. SO JOURNAL OF ANTHROPOLOGICAL RESEARCH LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Kaeppler, AL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV NEW MEXICO PI ALBUQUERQUE PA DEPT ANTHROPOLOGY, ALBUQUERQUE, NM 87131-1561 USA SN 0091-7710 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD WIN PY 2002 VL 58 IS 4 BP 565 EP 566 PG 2 WC Anthropology SC Anthropology GA 634CR UT WOS:000180322900017 ER PT J AU Dudley, R Winter, Y AF Dudley, R Winter, Y TI Hovering flight mechanics of neotropical flower bats (Phyllostomidae : Glossophaginae) in normodense and hypodense gas mixtures SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE aerodynamics; bat; density; flight; glossophagine; hovering; hyperoxia; Leptonycteris curasoae; power ID NECTAR-FEEDING BAT; INSECT FLIGHT; ENERGETIC COST; BODY-MASS; PERFORMANCE; HUMMINGBIRDS; AERODYNAMICS; SORICINA; HELIOX; POWER AB Existing estimates of flight energetics in glossophagine flower bats, the heaviest hovering vertebrate taxon, suggest disproportionately high expenditure of mechanical power. We determined wingbeat kinematics and mechanical power expenditure for one of the largest flower bats (Leptonycteris curasoae Martinez and Villa) during hovering flight in normodense and hypodense gas mixtures. Additional experiments examined the effects of supplemental oxygen availability on maximum flight performance. Bats failed to sustain hovering flight at normoxic air densities averaging 63% that of normodense air. Kinematic responses to hypodense aerodynamic challenge involved increases in wing positional angles and in total stroke amplitude; wingbeat frequency was unchanged. At near-failure air densities, total power expenditure assuming perfect elastic energy storage was 17-42% greater than that for hovering in normodense air, depending on the assumed value for the profile drag coefficient. Assuming a flight muscle ratio of 26%, the associated muscle-mass-specific power output at the point of near-failure varied between 90.8 W kg(-1) (profile drag coefficient of 0.02) to 175.6 W kg(-1) (profile drag coefficient of 0.2). Hyperoxia did not enhance hovering performance in hypodense air, and, with the exception of a small increase (10%) in stroke plane angle, yielded no significant change in any of the kinematic parameters studied. Revised energetic estimates suggest that mechanical power expenditure of hovering glossophagines is comparable with that in slow forward flight. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Munich, Dept Biol, D-80333 Munich, Germany. RP Dudley, R (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. NR 43 TC 9 Z9 11 U1 2 U2 10 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD DEC PY 2002 VL 205 IS 23 BP 3669 EP 3677 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 625VA UT WOS:000179835200010 PM 12409493 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Vanished splendors: A memoir. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 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 DEC PY 2002 VL 127 IS 20 BP 115 EP 115 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 624JT UT WOS:000179757100057 ER PT J AU Mair, RW Rosen, MS Wang, R Cory, DG Walsworth, RL AF Mair, RW Rosen, MS Wang, R Cory, DG Walsworth, RL TI Diffusion NMR methods applied to xenon gas for materials study SO MAGNETIC RESONANCE IN CHEMISTRY LA English DT Article DE NMR; Xe-129; He-3; diffusion; gases; laser polarization; porous media; gas-phase diffusion; gas flow; restricted diffusion ID NUCLEAR-MAGNETIC-RESONANCE; GRADIENT SPIN-ECHO; LASER-POLARIZED XE-129; HYPERPOLARIZED HE-3 GAS; TO-VOLUME RATIO; POROUS-MEDIA; SELF-DIFFUSION; NOBLE-GAS; LONGITUDINAL RELAXATION; MONOLITHIC CATALYSTS AB We report initial NMR studies of (i) xenon gas diffusion in model heterogeneous porous media and (ii)continuous flow laser-polarized xenon gas. Both areas utilize the pulsed gradient spin-echo (PGSE) techniques in the gas phase, with the aim of obtaining more sophisticated information than just translational self-diffusion coefficients - a brief overview of this area is provided in the Introduction. The heterogeneous or multiple-length scale model porous media consisted of random packs of mixed glass beads of two different sizes. We focus on observing the approach of the time-dependent gas diffusion coefficient, D(t) (an indicator of mean squared displacement), to the long-time asymptote, with the aim of understanding the long-length scale structural information that may be derived from a heterogeneous porous system. We find that D(t) of imbibed xenon gas at short diffusion times is similar for the mixed bead pack and a pack of the smaller sized beads alone, hence reflecting the pore surface area to volume ratio of the smaller bead sample. The approach of D(t) to the long-time limit follows that of a pack of the larger sized beads alone, although the limiting D(t) for the mixed bead pack is lower, reflecting the lower porosity of the sample compared to that of a pack of mono-sized glass beads. The Pade approximation is used to interpolate D(t) data between the short- and long-time limits. Initial studies of continuous flow laser-polarized xenon gas demonstrate velocity-sensitive imaging of much higher flows than can generally be obtained with liquids (20-200 mm s(-1)). Gas velocity imaging is, however, found to be limited to a resolution of about 1 mm s(-1) owing to the high diffusivity of gases compared with liquids. We also present the first gas-phase NMR scattering, or diffusive-diffraction, data, namely flow-enhanced structural features in the echo attenuation data from laser-polarized xenon flowing through a 2 mm glass bead pack. Copyright (C) 2002 John Wiley Sons, Ltd. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Nucl Engn, Cambridge, MA 02139 USA. RP Mair, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 59, Cambridge, MA 02138 USA. NR 86 TC 24 Z9 24 U1 2 U2 9 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX PO19 1UD, ENGLAND SN 0749-1581 J9 MAGN RESON CHEM JI Magn. Reson. Chem. PD DEC PY 2002 VL 40 SI SI BP S29 EP S39 DI 10.1002/mrc.1114 PG 13 WC Chemistry, Multidisciplinary; Chemistry, Physical; Spectroscopy SC Chemistry; Spectroscopy GA 621MP UT WOS:000179593900006 PM 12807139 ER PT J AU Guzman, HM Guevara, CA AF Guzman, HM Guevara, CA TI Annual reproductive cycle, spatial distribution, abundance, and size structure of Oreaster reticulatus (Echinodermata : Asteroidea) in Bocas del Toro, Panama SO MARINE BIOLOGY LA English DT Article ID CORAL-REEFS; CONSERVATION STATUS; CONTINENTAL REEFS; SAND BOTTOMS; POPULATIONS; LIGHT AB The structure, distribution, and population abundance of Oreaster reticulatus (Linnaeus, 1758) in 47,157 ha of shallow-water habitat in the archipelago of Bocas del Toro, Panama, were assessed from May to October 2000. The reproductive cycle of the sea star was studied in Isla Solarte, from February 2000 to February 2001. In total, 4,818 sea stars were recorded with a mean density of 149.7 ind. ha(-1), and a population of over 7 million was estimated for the archipelago. O. reticulatus was absent in ca. 50% of the evaluated areas, possibly due to high runoff and sedimentation; highest density was observed in an intermediate-runoff regime (255 ind. ha 1). About 45% of the population was found in substrata dominated by seagrass (Thalassia testudinum) and coarse, calcareous sand, 51% occurred in habitats where coral reef patches were mixed with seagrass, and 4% exclusively on coral reefs. The average size, based on the major radius, was 9.5 cm (3-21 cm), with a population structure composed of ca. 83% juveniles and 17% adults. The average reproductive size, measured as major radius, was 15 cm, and the minimum was 7 cm. Both males and females with a maximum stage (IV) of gonad development were observed throughout the year. The gonad index showed three peaks of maximum reproductive activity, which is not comparable to studies from other localities. The reproductive cycle did not seem to be related to water temperature, which ranged from 27 C to 30 C, but may respond more closely to changes in local rainfall. This relationship was not statistically significant based on this 1-year study. These data provide a useful baseline for management of local populations in the face of an increasing harvest for the aquarium trade and as souvenirs. C1 Smithsonian Trop Res Inst, Balboa, Panama. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. NR 28 TC 24 Z9 26 U1 3 U2 14 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 DEC PY 2002 VL 141 IS 6 BP 1077 EP 1084 DI 10.1007/s00227-002-0898-2 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 629HM UT WOS:000180044300010 ER PT J AU Guzman, HM Garcia, EM AF Guzman, HM Garcia, EM TI Mercury levels in coral reefs along the Caribbean coast of Central America SO MARINE POLLUTION BULLETIN LA English DT Article DE mercury; coral reefs; pollution; Siderastrea siderea; Costa Rica; Panama ID ATMOSPHERIC MERCURY; METAL CONTENT; HEAVY-METALS; CONTAMINATION; POLLUTION; SEDIMENTS; GOLD; EMISSIONS; BRAZIL; SILVER AB Sediment and coral skeleton samples from 23 coral reefs along the Caribbean coast of Costa Rica and Panama (1497 km) were evaluated for total mercury (Hg). High levels of pollution were found in the entire region with averages of 18.9 and 71.3 ppb in coral skeletons and sediments respectively. Significantly higher contamination was found in Panamanian corals (21.4 ppb) while compared to Costa Rican reef sediments (85.9 ppb). Hg from several processes and non-point sources (e.g., erosion, runoff, flooding, mining, overuse of agrochemicals, industrial waste, ports, and refineries) may have affected the entire region. The widespread observed distribution suggests that Hg is being carried along long distances within the region due to its high concentrations found in "pristine" reefs. Forest burning and colonial mining residues may be considered as possible contamination factors. Published by Elsevier Science Ltd. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. RP Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM guzmanh@naos.si.edu NR 45 TC 28 Z9 30 U1 0 U2 15 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 DEC PY 2002 VL 44 IS 12 BP 1415 EP 1420 AR PII S0025-326X(02)00318-1 DI 10.1016/S0025-326X(02)00318-1 PG 6 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 627JB UT WOS:000179929100026 PM 12523547 ER PT J AU Marvin, UB Cosmo, ML AF Marvin, UB Cosmo, ML TI Domenico Troili(1766): "The true cause of the fall of a stone in Albereto is a subterranean explosion that hurled the stone skyward" SO METEORITICS & PLANETARY SCIENCE LA English DT Article AB In mid-July, 1766, a stone fell at Villa Albareto near Modena in northern Italy. A sudden explosion like a cannon shot followed by fierce whistling sounds frightened people over a wide area. Some saw a fiery body falling from the sky; others said it was dark and smoky. The ground shook when the stone plunged into the soil making a hole nearly a meter deep. The Abbe Domenico Troili collected eyewitness reports, examined the stone, and reported the presence of marchesita, an old name for pyrite. A century later, this mineral, which proved to be iron sulfide (FeS), was named "troilite" in his honor. Troili's description is unquestionably that of a meteorite fall, and therefore some scientists have argued that it is Troili, rather than Ernst F. F. Chladni, to whom we should give credit as the first person to record the fall of a stone from space. However, Troili, himself, had no such an idea; he wrote that a subterranean explosion had hurled the stone high into the sky from a vent in the Earth. He stoutly defended this explanation against his opponents, including the Bishop of Modena, who believed that the stone had been hurled aloft by a bolt of lightning. Both hypotheses reflect a conviction, held well into the nineteenth century, that any rocky objects that fall from the sky must originate on the Earth or in the atmosphere. In 1794, Chladni calculated that meteors and mereoritic fireballs course down the sky at such extremely high velocities that the bodies forming them must originate in space. He listed all the falls that he found credible in historic records. Partly through his efforts, meteorites had gained widespread acceptance by 1803, but the idea of their origin in space had not. For the next half century many scientists continued to argue that meteorites either consolidate in the upper atmosphere or are ejected by volcanoes on the Moon. Recent efforts to transfer honors from Chladni to Troili for being the first to describe meteorites as bodies falling from space are unwarranted. 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. NR 26 TC 3 Z9 3 U1 1 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 DEC PY 2002 VL 37 IS 12 BP 1857 EP 1864 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633FT UT WOS:000180272400015 ER PT J AU Marvin, UB AF Marvin, UB TI Oral histories in meteoritics and planetary science: VIII. Friedrich Begemann SO METEORITICS & PLANETARY SCIENCE LA English DT Editorial Material AB In this interview, taped in 2001 during The Meteoritical Society meeting in Rome, Friedrich Begemann recalls that after he earned his doctorate in physics under the direction of Professor Friedrich G. Houtermans, first in Gottingen and then in Bern, Switzerland, he began his career as what he calls a low-level gas counting man, specializing in tritium (H-3). In 1954 he accepted an invitation from Professor Willard F. Libby to run his gas-counting laboratory at the University of Chicago. Begemann spent 3 years there during which he traced the distribution in the world's atmosphere and waters of tritium from two sources, natural cosmic radiation and the detonation of the first thermonuclear device. During his time at Chicago he was drawn into Harold C. Urey's group of scientists studying meteorites. Begemann found that he could measure tritium in meteorites, and by coupling his values with those of He-3, he and his collaborators initiated a new branch of meteoritics by determining the first cosmic-ray exposure age of a meteorite-Norton County, which fell in 1947. In 1957, Begemann joined the group led by Friedrich A. Paneth at the Max-Planck-Institut fur Chemie at Mainz, Germany, where he continued his studies of gas isotopes for the remainder of his career. His research led to the discovery of primitive noble gases in the diamond-graphite aggregates in ureilites, where their presence in presumably deep-seated igneous rocks still remains to be explained. With the advent of the Apollo missions, Begemann extended his studies to the lunar rocks and soils in an effort to learn as much as possible about the interaction of solids with the space environment. He also became heavily involved in measuring the s-process isotope abundance patterns of medium-heavy chemical elements as they occur in interstellar grains. In 1995 at the meeting in Washington, D.C., The Meteoritical Society presented Friedrich Begemann with the Leonard Medal for his contributions to our understanding of the radiation encountered by bodies as they orbit through space. 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. NR 27 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 DEC PY 2002 VL 37 IS 12 SU S BP B69 EP B77 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 634JY UT WOS:000180337300010 ER PT J AU Marvin, UB AF Marvin, UB TI Oral histories in meteoritics and planetary science: V1. Stuart Ross Taylor SO METEORITICS & PLANETARY SCIENCE LA English DT Editorial Material AB In this interview, Ross Taylor describes how his interest in planetary science was aroused by proofreading Brian Mason's book on geochemistry. Born and raised in New Zealand, Ross majored in chemistry at Canterbury College in Christchurch. While there, he took a course in geology and was strongly tempted to change his major, but he resolved the problem by becoming a geochemist. For his doctoral studies, Ross joined Mason at Indiana University where he learned the basics of trace element analysis on the emission spectrograph. Subsequently, he set up emission spectrographic laboratories and used them to pursue his research at Oxford University and the University of Cape Town. As techniques became more sensitive, he set up a spark-source mass spectrograph at the Australian National University in Canberra. Ross always has retained an interest in terrestrial rocks, but he is most widely known for his investigations of tektites and lunar rocks. He became one of the earliest and strongest advocates of tektites as molten terrestrial sediments sent aloft by high-energy impacts. As a member of the preliminary examination team that analyzed the samples returned by the Apollo missions, Ross gained an intimate knowledge of lunar chemistry and petrology and wrote three books about the Moon. He also has written a book about the chemical evolution of the solar system, a topic on which such rapid progress was made in 10 years that his second edition is practically a different book from the first one. Ross has written Destiny or Chance, a philosophical consideration of the likelihood that as sentient beings we may well be alone in the universe. Ross served as the president of The Meteoritical Society in 1989 and 1990, and at its annual meeting in Dublin, Ireland, in 1998, the Society presented him with its Leonard Medal. 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. NR 13 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 DEC PY 2002 VL 37 IS 12 SU S BP B47 EP B56 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 634JY UT WOS:000180337300008 ER PT J AU Marvin, UB AF Marvin, UB TI Oral histories in meteoritics and planetary science: V. Brian Mason SO METEORITICS & PLANETARY SCIENCE LA English DT Editorial Material AB In this interview, Brian Mason describes the sudden awakening of his interest in meteorites during his student days at Canterbury College in New Zealand when he read a paper on the cosmic abundances of the elements by Victor M. Goldschmidt. Subsequently, he won a scholarship for graduate study abroad and wrote to Goldschmidt asking if he could do a thesis with him in Norway. Shortly after he began his research in Oslo, he fled the city, ahead of the German invasion of Norway, and completed his doctorate in Stockholm with a thesis on the iron-manganese minerals of the Langban Mine. After the war he taught for 3 years at Canterbury College where he gave courses on mineralogy and geology (into which he inserted lectures on geochemistry) and led students in extensive field studies. In 1947, Mason accepted a professorship of mineralogy at Indiana University. While there, he wrote the landmark book, Principles of Geochemistry, which appeared in 1952. The following year he moved to New York City where he served as the Curator of Minerals at the American Museum of Natural History and an adjunct professor at Columbia University. He became fascinated with the museum's meteorite collection and discussed meteorites in his lectures, which inspired some of his outstanding students to enter the field. During a sabbatical year he spent as a Fulbright Professor in Japan, he gave an advanced level seminar on meteorites and based his book, Meteorites, on his lecture notes. Mason developed a rapid method of optically classifying chondritic meteorites that he applied to major collections in many countries, thus enabling curators to replace uninformative labels such as "stone" or "chondrite" with species names, and to recognize which of their meteorites were rare types demanding serious study. In 1965 he moved to the Smithsonian Institution in Washington, D.C. where he remained for the rest of his career. Early in 1968, he collected specimens from the spectacular fall of the Allende meteorite in Mexico, which proved to be a carbonaceous chondrite containing rare types of inclusions enriched in calcium and aluminum. His analyses showed how these inclusions could be divided into groups on the basis of their differing rare earth element patterns. Masons studies of Allende continued while he investigated lunar samples returned by the Apollo missions and coauthored a book on them. Beginning in the latter 1970s, he applied his rapid classification of stony meteorites to the large numbers of specimens collected each year by U.S. teams on the Antarctic ice sheet. In 1992 he capped his career with a biography of Victor M. Goldschmidt. In recognition of his many fundamental contributions, The Meteoritical Society honored Brian Mason with its Leonard Medal at its meeting in 1972 at the University of Chicago. 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. NR 14 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 DEC PY 2002 VL 37 IS 12 SU S BP B35 EP B45 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 634JY UT WOS:000180337300007 ER PT J AU Marvin, UB AF Marvin, UB TI Oral histories in meteoritics and planetary science: IX. Heinrich Wanke SO METEORITICS & PLANETARY SCIENCE LA English DT Editorial Material ID TERRESTRIAL PLANETS AB In this interview, Heinrich Wanke, a nuclear physicist, describes how he first encountered meteorite studies in 1953 when, after finishing his Ph.D. thesis in Vienna, he joined the research group of Professor Friedrich Paneth at the University of Durham, England. There, he worked on problems relating to uranium-helium ages of iron meteorites. A year later, Wanke moved with Paneth to the Max-Planck-Institut fur Chemie at Mainz in Germany. He continued meteorite research but also conducted experiments to measure noble gases in the stratosphere, a project that brought him to America in 1956 where he first met Professor Harold C. Urey, with whom he formed a lasting friendship. After Paneth's early death in 1958, Wanke remained at the Institute in Mainz and pursued research on topics such as the isotopic compositions of cosmogenic noble gases in iron meteorites and the abundances of primordial rare gases implanted by solar wind particles in brecciated stony meteorites. In 1969, Wanke was appointed to fill Paneth's position as a director of the Max-Planck-Institut fur Chemie just in time for him to lead a wide spectrum of research projects on the lunar rocks and soils. From the geochemical evidence these studies provided, he theorized on the formation of the Moon by the giant impact hypothesis, and proposed a two-component model for the cosmic composition of the Earth's mantle. His group also investigated the isotopic chemistry of martian meteorites and its bearing on the origin and evolution of Mars, which he viewed as a cored planet that underwent early differentiation without subsequent convective homogenization. In 1980, the Meteoritical Society awarded the Leonard Medal to Heinrich Wanke for his numerous contributions of fundamental importance to meteoritics and planetary science. 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. NR 19 TC 0 Z9 0 U1 0 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 DEC PY 2002 VL 37 IS 12 SU S BP B79 EP B88 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 634JY UT WOS:000180337300011 ER PT J AU Marvin, UB AF Marvin, UB TI Oral histories in meteoritics and planetary science: VII. Alastair G. W. Cameron SO METEORITICS & PLANETARY SCIENCE LA English DT Editorial Material AB In this interview, Alastair Cameron recounts how he started his career as a nuclear physicist but taught himself astrophysics after he read a paper that required an astrophysical explanation for the presence of technetium in red giant stars. Subsequently, as new analytical data became available, he periodically updated the Suess-Urey tables of elemental abundances to enhance the value of the systematic approach they provided to understanding individual processes of nucleosysthesis. Since many of these new data were based on analyses of carbonacous chondrites, he taught himself meteoritics. In recent decades, Cameron has focused his research interests on problems such as the provenance of certain components of meteorites (calcium-aluminum-rich inclusions, FUN (fractionated and unknown nuclear) anomalous inclusions, amoeboid olivine aggregates, and presolar grains) that he believes to have formed in the supernova envelope prior to formation of the solar nebula, the origin of chondrules in the primitive solar nebula, and the origins of the solar system and of the Earth-Moon system. To investigate these subjects he has pioneered the use of advanced computer technology to make lengthy calculations of nucleosysthesis in complicated networks. After teaching courses and advising graduate students at several research institutes and colleges, Cameron served as a Professor of Astronomy at Harvard University from 1973 to 1997 when he was appointed to the Donald H. Menzel Research Professorship of Astrophysics. In 1994, The Meteoritical Society honored him with the Leonard Medal at its meeting in Prague, the Czech Republic. 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. NR 12 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 DEC PY 2002 VL 37 IS 12 SU S BP B57 EP B67 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 634JY UT WOS:000180337300009 ER PT J AU Beltran, M Jiggins, CD Bull, V Linares, M Mallet, J McMillan, WO Bermingham, E AF Beltran, M Jiggins, CD Bull, V Linares, M Mallet, J McMillan, WO Bermingham, E TI Phylogenetic discordance at the species boundary: Comparative gene genealogies among rapidly radiating Heliconius butterflies SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE coalescence; hybridization; phylogeny; mitochondrial DNA; nuclear genes; Taq error ID MITOCHONDRIAL-DNA SEQUENCES; PASSION-VINE BUTTERFLIES; RIBOSOMAL-RNA GENES; HYBRID ZONE; POPULATION-GENETICS; CLADISTIC-ANALYSIS; NATURAL-SELECTION; NUCLEAR GENE; LEPIDOPTERA; NYMPHALIDAE AB Recent adaptive radiations provide excellent model systems for understanding speciation, but rapid diversification can cause problems for phylogenetic inference. Here we use gene genealogies to investigate the phylogeny of recent speciation in the heliconiine butterflies. We sequenced three gene regions, intron 3 (approximate to550 bp) of sex-linked triosephosphate isomerase (Tpi), intron 3 (approximate to450 bp) of autosomal mannose-phosphate isomerase (Mpi), and 1,603 bp of mitochondrial cytochrome oxidase subunits I and II (COI and COII), for 37 individuals from 25 species of Heliconius and related genera. The nuclear intron sequences evolved at rates similar to those of mitochondrial coding sequences, but the phylogenetic utility of introns was restricted to closely related geographic populations and species due to high levels of indel variation. For two sister species pairs, Heliconius erato-Heliconius himera and Heliconius melpoinene-Heliconius cydno, there was highly significant discordance between the three genes. At mtDNA and Tpi, the hypotheses of reciprocal monophyly and paraphyly of at least one species with respect to its sister could not be distinguished. In contrast alleles sampled from the third locus, Mpi, showed polyphyletic relationships between both species pairs. In all cases, recent coalescence of mtDNA lineages within species suggests that polyphyly of nuclear genes is not unexpected. In addition, very similar alleles were shared between melpomene and cydno, implying recent gene flow. Our finding of discordant genealogies between genes is consistent with models of adaptive speciation with ongoing gene How and highlights the need for multiple locus comparisons to resolve phylogeny among closely related species. C1 Smithsonian Trop Res Inst, AA-2072 Balboa, Panama. Univ Puerto Rico, Dept Biol, San Juan, PR 00936 USA. UCL, Dept Biol, Galton Lab, London, England. RP Beltran, M (reprint author), Smithsonian Trop Res Inst, AA-2072 Balboa, Panama. EM beltranm@naos.si.edu RI Jiggins, Chris/B-9960-2008; mallet, james/B-5114-2008; Linares, Mauricio/I-3509-2016; OI Jiggins, Chris/0000-0002-7809-062X; Linares, Mauricio/0000-0002-1021-0226; Mallet, James/0000-0002-3370-0367 NR 53 TC 114 Z9 120 U1 2 U2 19 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 DEC PY 2002 VL 19 IS 12 BP 2176 EP 2190 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 625AT UT WOS:000179795100014 PM 12446809 ER PT J AU Husband, R Herre, EA Turner, SL Gallery, R Young, JPW AF Husband, R Herre, EA Turner, SL Gallery, R Young, JPW TI Molecular diversity of arbuscular mycorrhizal fungi and patterns of host association over time and space in a tropical forest SO MOLECULAR ECOLOGY LA English DT Article DE AM1; arbuscular mycorrhiza; community composition; diversity; SSU; tropical forest ID PLANT COMMUNITY STRUCTURE; TALLGRASS PRAIRIE; GLOMUS-MOSSEAE; GROWTH; SPORES; SUCCESSION; GRASSLAND; GLOMALES; COLONIZATION; PRODUCTIVITY AB We have used molecular techniques to investigate the diversity and distribution of the arbuscular mycorrhizal (AM) fungi colonizing tree seedling roots in the tropical forest on Barro Colorado Island (BCI), Republic of Panama. In the first year, we sampled newly emergent seedlings of the understory treelet Faramea occidentalis and the canopy emergent Tetragastris panamensis, from mixed seedling carpets at each of two sites. The following year we sampled surviving seedlings from these cohorts. The roots of 48 plants were analysed using AM fungal-specific primers to amplify and clone partial small subunit (SSU) ribosomal RNA gene sequences. Over 1300 clones were screened for random fragment length polymorphism (RFLP) variation and 7% of these were sequenced. Compared with AM fungal communities sampled from temperate habitats using the same method, the overall diversity was high, with a total of 30 AM fungal types identified. Seventeen of these types have not been recorded previously, with the remainder being similar to types reported from temperate habitats. The tropical mycorrhizal population showed significant spatial heterogeneity and nonrandom associations with the different hosts. Moreover there was a strong shift in the mycorrhizal communities over time. AM fungal types that were dominant in the newly germinated seedlings were almost entirely replaced by previously rare types in the surviving seedlings the following year. The high diversity and huge variation detected across time points, sites and hosts, implies that the AM fungal types are ecologically distinct and thus may have the potential to influence recruitment and host composition in tropical forests. C1 Univ York, Dept Biol, York YO10 5YW, N Yorkshire, England. Smithsonian Trop Res Inst, Balboa, Panama. CEH Oxford, Oxford, England. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Husband, R (reprint author), Univ York, Dept Biol, POB 373, York YO10 5YW, N Yorkshire, England. RI Turner, Sarah/K-4683-2012; Young, Peter/C-1446-2012 OI Turner, Sarah/0000-0002-8937-6922; Young, Peter/0000-0001-5259-4830 NR 49 TC 222 Z9 240 U1 15 U2 98 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 DEC PY 2002 VL 11 IS 12 BP 2669 EP 2678 DI 10.1046/j.1365-294X.2002.01647.x PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 619TD UT WOS:000179492800019 PM 12453249 ER PT J AU Molbo, D Krieger, MJB Herre, EA Keller, L AF Molbo, D Krieger, MJB Herre, EA Keller, L TI Species-diagnostic microsatellite loci for the fig wasp genus Pegoscapus SO MOLECULAR ECOLOGY NOTES LA English DT Article DE cross-species amplification; cryptic species; fig wasp; microsatellites; Pegoscapus; primers AB To obtain tools for the estimation of inbreeding and assignment of offspring to matrilines, we developed 13 microsatellite loci from the fig wasps that pollinate Ficus obtusifolia. Based on morphological studies, it was thought that a single species (Pegoscapus hoffmeyer) pollinated this fig. However, our data revealed the presence of two coexisting cryptic species. Several diagnostic microsatellite markers may be used to distinguish these two cryptic species. The new microsatellites can be used across a wide range of fig-pollinating wasp species for both evolutionary and population genetic studies. C1 Univ Lausanne, Inst Ecol, CH-1015 Lausanne, Switzerland. Univ Georgia, Dept Entomol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balbao, Panama. RP Molbo, D (reprint author), Univ Lausanne, IE ZEA, Batiment Biol, CH-1015 Lausanne, Switzerland. OI keller, laurent/0000-0002-5046-9953 NR 11 TC 11 Z9 12 U1 0 U2 10 PU BLACKWELL PUBLISHING LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD DEC PY 2002 VL 2 IS 4 BP 440 EP 442 DI 10.1046/j.1471-8286.2002.00268.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 622ZM UT WOS:000179678400019 ER PT J AU Ortega, J Maldonado, JE Arita, HT Wilkinson, GS Fleischer, RC AF Ortega, J Maldonado, JE Arita, HT Wilkinson, GS Fleischer, RC TI Characterization of microsatellite loci in the Jamaican fruit-eating bat Artibeus jamaicensis and cross-species amplification SO MOLECULAR ECOLOGY NOTES LA English DT Article DE Artibeus jamaicensis; cross-species amplification; heterozygosity; microsatellite; Phyllostomidae AB Artibeus jamaicensis is one of the most common bat species in the neotropics, with a well-defined polygynous social structure in caves. In order to study behaviour and to examine patterns of paternity and relatedness between different harem groups, we developed 14 microsatellite loci from two different enriched genomic libraries. We screened 125 individuals from two different bat colonies and found that polymorphism ranged from five to 13 alleles. Heterozygosity ranged from 63 to 95%. The primers amplified across 14 bat species, indicating their potential utility for population-level studies in several closely related bat species. C1 Smithsonian Inst, Genet Lab, Natl Museum Natl Hist, Washington, DC 20008 USA. Univ Maryland, Dept Biol, College Pk, MD 20742 USA. Univ Nacl Autonoma Mexico, Inst Ecol, Mexico City 04510, DF, Mexico. RP Ortega, J (reprint author), Smithsonian Inst, Genet Lab, Natl Museum Natl Hist, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Wilkinson, Gerald/E-4424-2011; ARITA, HECTOR/I-6161-2012 OI Wilkinson, Gerald/0000-0001-7799-8444; NR 6 TC 15 Z9 16 U1 0 U2 3 PU BLACKWELL PUBLISHING LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD DEC PY 2002 VL 2 IS 4 BP 462 EP 464 DI 10.1046/j.1471-8286.2002.00278.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 622ZM UT WOS:000179678400026 ER PT J AU Stach, T Turbeville, JM AF Stach, T Turbeville, JM TI Phylogeny of Tunicata inferred from molecular and morphological characters SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID EVOLUTIONARY HISTORY; BODY-PLAN; 18S RDNA; SEQUENCES; ASCIDIANS; CHORDATA; ULTRASTRUCTURE; INVERTEBRATES; UROCHORDATA; PITUITARY AB The phylogeny of the Tunicata was reconstructed using molecular and morphological characters. Mitochondrial cytochrome oxidase I (cox1) and 18S rDNA sequences were obtained for 14 and 4 tunicate species, respectively. 18S rDNA sequences were aligned with gene sequences obtained from GenBank of 57 tunicates, a cephalochordate, and a selachian craniate. Cox1 sequences were aligned with the sequence of two ascidians and a cephalochordate obtained from GenBank. Traditional, morphological, life history, and biochemical characters of larval and adult stages were compiled from the literature and analyzed cladistically. Separate and simultaneous parsimony analyses of molecular and morphological data were carried out. Aplousobranch ascidians from three different families were included in a molecular phylogenetic analysis for the first time. Analysis of the morphological, life history, and biochemical characters results in a highly unresolved tree. Aplousobranchiata form a strongly supported monophylum in the analysis of the 18S rDNA data, the morphological data, and the combined data set. Cionidae is not included in the Aplousobranchiata but nests within the Phlebobranchiata. Appendicularia (= Larvacea) nest within the 'Ascidiacea' as the sister taxon of Aplousobranchiata in the parsimony analysis of the 18S rDNA data and the combined analysis. A potential morphological synapomorphy of Aplousobranchiata plus Appendicularia is the horizontal orientation of the larval tail. In the 18S rDNA and the combined analysis, Thaliacea is included in the 'Ascidiacea' as the sister group to Phlebobranchiata. Pyrosomatida is found to be the sister taxon to the Salpidae in analyses of 18S rDNA and combined data, whereas the analysis of the morphological data recovers a sister group relationship between Doliolidae and Salpidae. Results of cox1 analyses are incongruent with both the 18S rDNA and the morphological phylogenies. Cox1 sequences may evolve too rapidly to resolve relationships of higher tunicate taxa. However, the cox1 data may be useful at lower taxonomic levels. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Univ Arkansas, Dept Biol Sci, Fayetteville, AR 72701 USA. RP Stach, T (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. NR 96 TC 79 Z9 80 U1 1 U2 14 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 DEC PY 2002 VL 25 IS 3 BP 408 EP 428 AR PII S1055-7903(02)00305-6 DI 10.1016/S1055-7903(02)00305-6 PG 21 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 622AQ UT WOS:000179624400003 PM 12450747 ER PT J AU Scappini, F Casu, S Cecchi-Pestellini, C Olberg, M AF Scappini, F Casu, S Cecchi-Pestellini, C Olberg, M TI The discovery of clumpy structure in the diffuse gas towards Cyg OB2No. 12 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : individual : Cyg OB2No. 12; ISM : clouds; ISM : molecules ID INTERSTELLAR-MEDIUM; ASSOCIATION; ABSORPTION; H-3(+); CO; COEFFICIENTS; EMISSION; STARS AB We have mapped the (CO)-C-13 (1-0) line in a region of sky towards the star Cyg OB2 No. 12. The observations rule out the possibility that the molecular material along the line of sight is distributed over a long path of very dilute gas. Instead, we present unambiguous evidence of well-defined kinematical structures, which might be assembled to form a cloud complex. The chemistry that leads to H-3(+) appears decoupled from that responsible for the production of heavier species. C1 CNR, Ist Studio Mat Nanostrutturati, I-40129 Bologna, Italy. Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, Italy. Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Onsala Space Observ, S-43900 Onsala, Sweden. RP Scappini, F (reprint author), CNR, Ist Studio Mat Nanostrutturati, Via P Gobetti 101, I-40129 Bologna, Italy. OI Cecchi Pestellini, Cesare/0000-0001-7480-0324; Casu, Silvia/0000-0002-0154-3571 NR 18 TC 12 Z9 12 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 DEC PY 2002 VL 337 IS 2 BP 495 EP 498 DI 10.1046/j.1365-8711.2002.05928.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619TT UT WOS:000179494100012 ER PT J AU Roberts, TP Warwick, RS Ward, MJ Murray, SS AF Roberts, TP Warwick, RS Ward, MJ Murray, SS TI A Chandra observation of the interacting pair of galaxies NGC 4485/4490 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual : NGC 4485; galaxies : individual : NGC 4490; galaxies : interactions; X-rays : galaxies ID X-RAY SOURCES; NEARBY SPIRAL GALAXIES; ROSAT PSPC OBSERVATIONS; HIGH-RESOLUTION IMAGER; BLACK-HOLES; INTERSTELLAR-MEDIUM; STAR-FORMATION; NGC-4485; CATALOG AB We report the results of a 20-ks Chandra ACIS-S observation of the galaxy pair NGC 4485/4490. This is an interacting system containing a late-type spiral with an enhanced star formation rate (NGC 4490), and an irregular companion that possesses a disturbed morphology. A total of 29 discrete X-ray sources are found coincident with NGC 4490, but only one is found within NGC 4485. The sources range in observed X-ray luminosity from similar to2 x 10(37) to 4 x 10(39) erg s(-1). The more luminous sources appear, on average, to be spectrally harder than the fainter sources, an effect that is attributable to increased absorption in their spectra. Extensive diffuse X-ray emission is detected coincident with the disc of NGC 4490, and in the tidal tail of NGC 4485, which appears to be thermal in nature and hence the signature of a hot interstellar medium in both galaxies. However, the diffuse component accounts for only similar to10 per cent of the total X-ray luminosity of the system (2 x 10(40) erg s(-1), 0.5-8 keV), which arises predominantly in a handful of the brightest discrete sources. This diffuse emission fraction is unusually low for a galaxy pair which has many characteristics that would lead it to be classified as a starburst system, possibly as a consequence of the small gravitational potential well of the system. The discrete source population, on the other hand, is similar to that observed in other starburst systems, possessing a flat luminosity function slope of similar to-0.6 and a total of six ultraluminous X-ray sources (ULX). Five of the ULX are identified as probable black hole X-ray binary systems, and the sixth (which is coincident with a radio continuum source) is identified as an X-ray luminous supernova remnant. The ULX all lie in star formation regions, providing further evidence of the link between the ULX phenomenon and active star formation. Importantly, this shows that even in star-forming regions, the ULX population is dominated by accreting systems. We discuss the implications of this work for physical models of the nature of ULX, and in particular how it argues against the intermediate-mass black hole hypothesis. C1 Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Roberts, TP (reprint author), Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Univ Rd, Leicester LE1 7RH, Leics, England. NR 59 TC 55 Z9 55 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 DEC PY 2002 VL 337 IS 2 BP 677 EP 692 DI 10.1046/j.1365-8711.2002.05950.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619TT UT WOS:000179494100028 ER PT J AU Ewe, SML Sternberg, LDL AF Ewe, SML Sternberg, LDL TI Seasonal water-use by the invasive exotic, Schinus terebinthifolius, in native and disturbed communities SO OECOLOGIA LA English DT Article DE Brazilian pepper; delta O-18; everglades; water potentials; stable isotopes; water source ID ROOT HYDRAULIC CONDUCTIVITY; PLANTS; EXPANSION; OXYGEN; ABA; SAP AB Schinus terebinthifolius Raddi (Anacardiaceae) is an aggressive invader found in both disturbed and native habitats of Florida. The purpose of this study was to compare Schinus water uptake patterns to those of four native species in a disturbed previously farmed area versus a native pineland community. Although neither of the study sites was flooded, soils in both sites were saturated with water at the end of the wet season. Isotopic analysis of stem water showed that almost all the native species in both sites showed a seasonal change in plant water uptake; plants utilized mainly groundwater during the dry season but shifted to a high proportion of soil water during the wet season. In the pineland community, Schinus showed no seasonal shift in water uptake source. In the disturbed community, however, Schinus was not isotopically distinct from the native species with regard to water source. Despite greater soil water availability in the wet season, predawn water potentials were significantly lower in the wet than in the dry season for native species at both sites. The counterintuitive decrease in water potentials during the wet season in both study sites could be the response of native plants to root flooding. Predawn water potentials of Schinus in both study areas however, remained constant across seasons. Predawn and noontime water potential differences were smaller in Schinus than in the native species at both sites during the wet season, but this pattern was found only in the disturbed area during the dry season. Schinus was most likely less affected by seasonality and more tolerant of root flooding than the native species studied. C1 Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Ewe, SML (reprint author), Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. NR 35 TC 27 Z9 30 U1 2 U2 18 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD DEC PY 2002 VL 133 IS 4 BP 441 EP 448 DI 10.1007/s00442-002-1047-9 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 623ZA UT WOS:000179733800001 ER PT J AU Covington, AM Aguilar, A Covington, IR Gharaibeh, MF Hinojosa, G Shirley, CA Phaneuf, RA Alvarez, I Cisneros, C Dominguez-Lopez, I Sant'Anna, MM Schlachter, AS McLaughlin, BM Dalgarno, A AF Covington, AM Aguilar, A Covington, IR Gharaibeh, MF Hinojosa, G Shirley, CA Phaneuf, RA Alvarez, I Cisneros, C Dominguez-Lopez, I Sant'Anna, MM Schlachter, AS McLaughlin, BM Dalgarno, A TI Photoionization of Ne+ using synchrotron radiation SO PHYSICAL REVIEW A LA English DT Article ID R-MATRIX THEORY; CROSS-SECTIONS; ATOMIC FLUORINE; IONS; NEON; C+ AB Absolute measurements of cross sections for photoionization of a statistical admixture of Ne+ in the P-2(3/2)0 ground state and the P-2(1/2)0 metastable state are reported in the energy range 40-71 eV at photon energy resolutions ranging from 22 meV to 2 meV. The experiments were performed using synchrotron radiation from an undulator beamline of the Advanced Light Source with a newly developed ion-photon-beam endstation. The data are characterized by multiple Rydberg series of autoionizing resonances superimposed upon a direct photoionization background cross section where some of the observed resonance line shapes show evidence of interference between the direct and indirect photoionization channels. The resonance features are assigned spectroscopically, and their energies and quantum defects are tabulated. The experimental photoionization cross sections are in satisfactory agreement with the predictions from theoretical calculations performed in intermediate coupling using the semirelativistic Breit-Pauli approximation with ten states. The resonances nearest to the ionization thresholds exhibit anomalous behavior with respect to their positions and strengths due to the presence of interloping resonances associated with higher-lying ionic states causing disruption of the regular Rydberg, spectral pattern. C1 Univ Nevada, Dept Phys, Reno, NV 89557 USA. Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico. Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Univ Nevada, Dept Phys, MS 220, Reno, NV 89557 USA. RI Sant'Anna, Marcelo/B-9355-2013; Dominguez-Lopez, Ivan/B-6072-2016 OI Sant'Anna, Marcelo/0000-0001-5342-5799; Dominguez-Lopez, Ivan/0000-0001-8084-8711 NR 32 TC 103 Z9 103 U1 0 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD DEC PY 2002 VL 66 IS 6 AR 062710 DI 10.1103/PhysRevA.66.062710 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 639YA UT WOS:000180656800062 ER PT J AU Rigazio, M Kharchenko, V Dalgarno, A AF Rigazio, M Kharchenko, V Dalgarno, A TI X-ray emission spectra induced by hydrogenic ions in charge transfer collisions SO PHYSICAL REVIEW A LA English DT Article ID SELECTIVE ELECTRON-CAPTURE; SOLAR-WIND IONS; COMET HALE-BOPP; EXCHANGE COLLISIONS; CROSS-SECTIONS; C/1995 O1; JUPITER; IMPACT; HE; PRECIPITATION AB Theoretical models are constructed of the hard x-ray spectra resulting from electron capture by fully stripped Ne10+ ions traversing the gases Ne, He, H-2, CO2, and H2O. The measured spectra are superposiiions of individual lines of Ne9+. An exact description of the radiative cascade is used. Initial excited populations that reproduce the measured spectra are derived and quantitative predictions of the energies Bind intensities of lines in the soft x-ray and extreme ultraviolet regions are made. These lines when observed will be powerful diagnostic probes of the capture mechanism and of the diverse range of laboratory and astrophysical plasmas in which it occurs. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Rigazio, M (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 53 TC 25 Z9 25 U1 0 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 DEC PY 2002 VL 66 IS 6 AR 064701 DI 10.1103/PhysRevA.66.064701 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 639YA UT WOS:000180656800117 ER PT J AU Pope, NA AF Pope, NA TI Special delivery: Canada's postal heritage SO PUBLIC HISTORIAN LA English DT Book Review C1 Smithsonian Inst, Natl Postal Museum, Washington, DC USA. RP Pope, NA (reprint author), Smithsonian Inst, Natl Postal Museum, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA C/O JOURNALS DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD WIN PY 2002 VL 24 IS 1 BP 95 EP 97 PG 3 WC History SC History GA 543AG UT WOS:000175077800026 ER PT J AU Crouch, TD AF Crouch, TD TI Challenge to Apollo: The Soviet Union and the space race, 1945-1974 SO PUBLIC HISTORIAN LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Crouch, TD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CALIF PRESS PI BERKELEY PA C/O JOURNALS DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD WIN PY 2002 VL 24 IS 1 BP 108 EP 109 PG 2 WC History SC History GA 543AG UT WOS:000175077800033 ER PT J AU Van Dyk, SD Garnavich, PM Filippenko, AV Hoflich, P Kirshner, RP Kurucz, RL Challis, P AF Van Dyk, SD Garnavich, PM Filippenko, AV Hoflich, P Kirshner, RP Kurucz, RL Challis, P TI The progenitor of supernova 1993J revisited SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ETA-CARINAE ANALOG; SN 1993J; STELLAR PHOTOMETRY; M81; SN-1993J; MASS; SUPERGIANT; EMISSION; SPECTRA; MODELS AB From Hubble Space Telescope images with 0."05 resolution, we identify four stars brighter than V = 25 mag within 2."5 of SN 1993J in M81, which contaminated previous ground-based brightness estimates for the supernova progenitor. Correcting for the contamination, we find that the energy distribution of the progenitor is consistent with that of an early K-type supergiant star with M-V approximate to -7.0 +/- 0.4 mag and an initial mass of 13-22 M.. The brightnesses of the nearby stars are sufficient to account for the excess blue light seen from the ground in preexplosion observations. Therefore, the SN 1993J progenitor did not necessarily have a blue companion, although by 2001, fainter blue stars are seen in close proximity to the supernova. These observations do not strongly limit the mass of a hypothetical companion. A blue dwarf star with a mass up to 30 M. could have been orbiting the progenitor without being detected in the ground-based images. Explosion models and observations show that SN 1993J progenitor had a helium-rich envelope. To test whether the helium abundance could influence the energy distribution of the progenitor, we calculated model supergiant atmospheres with a range of plausible helium abundances. The models show that the presupernova colors are not strongly affected by the helium abundance longward of 4000 Angstrom, and abundances ranging between solar and 90% helium (by number) are all consistent with the observations. C1 CALTECH, IPAC, Pasadena, CA 91125 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP CALTECH, IPAC, Mailcode 100-22, Pasadena, CA 91125 USA. EM vandyk@ipac.caltech.edu; pgarnavi@miranda.phys.nd.edu; alex@astro.berkeley.edu; pah@astro.as.utexas.edu; rkirshner@cfa.harvard.edu; rkurucz@cfa.harvard.edu; pchallis@cfa.harvard.edu NR 44 TC 51 Z9 51 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 2002 VL 114 IS 802 BP 1322 EP 1332 DI 10.1086/344382 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 617ZD UT WOS:000179390300003 ER PT J AU Brown, WR Fabricant, DG Boyd, DA AF Brown, WR Fabricant, DG Boyd, DA TI A detailed thermal analysis of the Binospec spectrograph SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID CONVERTED MMT; LENSES AB Refractive optics in astronomical instruments are potentially sensitive to temperature gradients and temperature transients. This sensitivity arises from thermally dependent refractive indices, lens spacings, and lens dimensions. In addition, thermal gradients in the instrument structure can cause undesirable image shifts at the detector that degrade instrument calibration. We have therefore undertaken a detailed thermal analysis of Binospec, a wide-field optical spectrograph under development for the converted Multiple Mirror Telescope (MMT). Our goals are to predict the temperature gradients that will be present in the Binospec optics and structure under realistic operating conditions and to determine how design choices affect these gradients. We begin our analysis by deriving thermal time constants for instrument subassemblies to estimate the magnitude of temperature gradients in the instrument and to determine where detailed thermal models are required. We then generate a low-resolution finite-difference model of the entire instrument and high-resolution models of sensitive subassemblies. This approach to thermal analysis is applicable to a variety of other instruments. We use measurements of the ambient temperature in the converted MMT's dome to model Binospec's thermal environment. In moderate conditions, the external temperature changes by up to 8degreesC over 48 hr, while in extreme conditions the external temperature changes by up to 17degreesC in 24 hr. During moderate conditions, we find that the Binospec lens groups develop similar to0.14degreesC axial and radial temperature gradients and that lens groups of different mass develop similar to0.5degreesC temperature differences; these numbers are doubled for the extreme conditions. Internal heat sources do not significantly affect these results; heat flow from the environment dominates. The instrument must be periodically opened to insert new aperture masks, but we find that the resulting temperature gradients and thermal stresses in the optics are small. Image shifts at the detector caused by thermal deflections of the Binospec optical bench structure are similar to0.1 pixel hr(-1). We conclude that the proposed Binospec design has acceptable thermal properties, and we briefly discuss design changes to further reduce temperature gradients. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brown, WR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 2 Z9 2 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 DEC PY 2002 VL 114 IS 802 BP 1389 EP 1400 DI 10.1086/344383 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 617ZD UT WOS:000179390300009 ER PT J AU Shayt, DH AF Shayt, DH TI Just the right touch - By introducing a note of modesty, Marilyn Monroe's gloves actually heightened her come-hither allure SO SMITHSONIAN LA English DT Article C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Shayt, DH (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD DEC PY 2002 VL 33 IS 9 BP 22 EP + PG 0 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 621MY UT WOS:000179594800011 ER PT J AU Litwak, RS AF Litwak, RS TI The new calculus of pre-emption SO SURVIVAL LA English DT Article AB Under the Bush administration's 2002 National Security Strategy document, military pre-emption against 'rogue states' and terrorist groups has been elevated to official doctrine. But the conditions under which pre-emption would be undertaken remain unclear. Military action against terrorist groups, such as al-Qaeda, enjoys broad international legitimacy, but that consensus breaks down over the use of force against a state violating non-proliferation norms. A comparative analysis of historical cases reveals force to be as problematic as its non-military alternatives. Inadequate intelligence, concern over collateral damage to civilian populations and the fear of triggering a broader conflict have been major constraints on the use of force to prevent the proliferation of weapons of mass destruction. In the post-11 September era, pre-emption should be a rarely invoked policy option, and successful prevention strategies, employing non-military instruments, might forestall the need to resort to it. C1 Smithsonian Inst, Woodrow Wilson Int Ctr Scholars, Washington, DC 20560 USA. RP Litwak, RS (reprint author), Smithsonian Inst, Woodrow Wilson Int Ctr Scholars, Washington, DC 20560 USA. NR 47 TC 24 Z9 24 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0039-6338 J9 SURVIVAL JI Survival PD WIN PY 2002 VL 44 IS 4 BP 53 EP + DI 10.1080/00396330212331343492 PG 28 WC International Relations; Political Science SC International Relations; Government & Law GA 617ZF UT WOS:000179390600004 ER PT J AU Pryer, KM Schneider, H Zimmer, EA Banks, JA AF Pryer, KM Schneider, H Zimmer, EA Banks, JA TI Deciding among green plants for whole genome studies SO TRENDS IN PLANT SCIENCE LA English DT Editorial Material ID CLOSEST LIVING RELATIVES; NUCLEAR-DNA AMOUNTS; RICE GENOME; MITOCHONDRIAL GENOME; EVOLUTIONARY HISTORY; CHLOROPLAST GENOMES; COMPARATIVE BIOLOGY; DRAFT SEQUENCE; LAND PLANTS; ARABIDOPSIS AB Recent comparative DNA-sequencing studies of chloroplast, mitochondrial and ribosomal genes have produced an evolutionary tree relating the diversity of green-plant lineages. By coupling this phylogenetic framework to the explosion of information on genome content, plant-genomic efforts can and should be extended beyond angiosperm crop and model systems. Including plant species representative of other crucial evolutionary nodes would produce the comparative information necessary to understand fully the organization, function and evolution of plant genomes. The simultaneous development of genomic tools for green algae, bryophytes,'seed-free' vascular plants and gymnosperms should provide insights into the bases of the complex morphological, physiological, reproductive and biochemical innovations that have characterized the successful transition of green plants to land. C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Univ Gottingen, Albrecht von Haller Inst Pflanzenwissensch, Abt Sayst Bot, D-37073 Gottingen, Germany. Smithsonian Inst, Natl Museum Natl Hist, Labs Analyt Biol, Washington, DC 20560 USA. Purdue Univ, Dept Bot & Plant Pathol, W Lafayette, IN 47907 USA. RP Pryer, KM (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA. EM pryer@duke.edu RI Zimmer, Elizabeth/G-3890-2011; Schneider, Harald/B-6681-2008 OI Schneider, Harald/0000-0002-4548-7268 NR 52 TC 62 Z9 66 U1 0 U2 10 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 1360-1385 J9 TRENDS PLANT SCI JI Trends Plant Sci. PD DEC PY 2002 VL 7 IS 12 BP 550 EP 554 AR PII S1360-1385(02)02375-0 DI 10.1016/S1360-1385(02)02375-0 PG 5 WC Plant Sciences SC Plant Sciences GA 624XW UT WOS:000179788200013 PM 12475497 ER PT J AU Novotny, V Miller, SE Basset, Y Cizek, L Drozd, P Darrow, K Leps, J AF Novotny, V Miller, SE Basset, Y Cizek, L Drozd, P Darrow, K Leps, J TI Predictably simple: assemblages of caterpillars (Lepidoptera) feeding on rainforest trees in Papua New Guinea SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE insect herbivory; host specificity; Malesia; sample size; temporal and spatial variability; species richness ID HOST-SPECIFICITY; TROPICAL FOREST; INSECTS; COMMUNITIES; BIODIVERSITY; SEASONALITY; HERBIVORES; DIVERSITY; ABUNDANCE; RICHNESS AB Predictability in the composition of tropical assemblages of insect herbivores was studied using a sample of 35 952 caterpillars (Lepidoptera) from 534 species, feeding on 69 woody species from 45 genera and 23 families in a lowland rainforest in Papua New Guinea. Caterpillar assemblages were strongly dominated by a single species (median 48% of individuals and 49% of biomass). They were spatially and temporally constant (median normalized expected species shared (NESS) similarity between assemblages from the same host was greater than or equal to 0.85 for three sites 8-17 km apart as well as for three four-month periods of the year). Further, the median presence of species was I I months per year. Assemblages on hosts from different families and genera were virtually disjunct (NESS similarity less than 0.05) as the caterpillars were mostly specialized to a single plant family (77% of species) and, within families, to a single genus (66% of species), while capable of feeding on multiple congeneric hosts (89% of species). The dominance of caterpillar assemblages by a small number of specialized species, which also exhibited low spatial and temporal variability, permitted robust and reliable estimates of assemblage composition and between-assemblage similarity from small samples, typically less than 300 individuals per host plant. By contrast, even considerably larger samples were insufficient for estimates of species richness. A sample of 300 individuals was typically obtained from 1050 m(2) of foliage sampled during 596 tree inspections (i.e. a particular tree sampled at a particular time) in the course of 19 sampling days (median values from 69 assemblages). These results demonstrate that, contrary to some previous suggestions, insect herbivore assemblages in tropical rainforests have a predictable structure and, as such, are amenable to study. C1 Acad Sci Czech Republic, Inst Entomol, CR-37005 Ceske Budejovice, Czech Republic. Univ S Bohemia, Fac Biol, CR-37005 Ceske Budejovice, Czech Republic. Smithsonian Inst, Natl Museum Amer Hist, Dept Systemat Biol, Washington, DC 20560 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Ostrava, Dept Biol, Ostrava 70103, Czech Republic. RP Novotny, V (reprint author), Acad Sci Czech Republic, Inst Entomol, Branisovska 31, CR-37005 Ceske Budejovice, Czech Republic. EM novotny@entu.cas.cz RI Leps, Jan/B-6913-2013; Drozd, Pavel/J-3943-2013; Basset, Yves/B-6642-2014; Cizek, Lukas/G-7905-2014; Novotny, Vojtech/G-9434-2014; Cizek, Lukas/K-7111-2015; OI Leps, Jan/0000-0002-4822-7429; Drozd, Pavel/0000-0002-4602-8856; Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 49 TC 46 Z9 52 U1 4 U2 8 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 NOV 22 PY 2002 VL 269 IS 1507 BP 2337 EP 2344 DI 10.1098/rspb.2002.2166 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 621GN UT WOS:000179580300008 PM 12495501 ER PT J AU Leonard, JA Wayne, RK Wheeler, J Valadez, R Guillen, S Vila, C AF Leonard, JA Wayne, RK Wheeler, J Valadez, R Guillen, S Vila, C TI Ancient DNA evidence for Old World origin of New World dogs SO SCIENCE LA English DT Article ID DOMESTIC DOG; CANIS-LUPUS; EVOLUTION; WOLF AB Mitochondrial DNA sequences isolated from ancient dog remains from Latin America and Alaska showed that native American dogs originated from multiple Old World lineages of dogs that accompanied late Pleistocene humans across the Bering Strait. One clade of dog sequences was unique to the New World, which is consistent with a period of geographic isolation. This unique clade was absent from a large sample of modern dogs, which implies that European colonists systematically discouraged the breeding of native American dogs. C1 Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, Los Angeles, CA 90095 USA. CONOPA, Coordinadora Invest & Desarrollo Camelidos, Lima 19, Peru. Univ Nacl Autonoma Mexico, Inst Invest Antropol, Lab Paleozool, Mexico City 04510, DF, Mexico. Bioanthropol Fdn Peru, Ctr Mallqui, Lima 11, Peru. Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. RP Leonard, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Vila, Carles/H-4893-2013; Leonard, Jennifer/A-7894-2010 OI Vila, Carles/0000-0002-4206-5246; Leonard, Jennifer/0000-0003-0291-7819 NR 27 TC 212 Z9 230 U1 9 U2 103 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 NOV 22 PY 2002 VL 298 IS 5598 BP 1613 EP 1616 DI 10.1126/science.1076980 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 617KV UT WOS:000179361600047 PM 12446908 ER PT J AU Stancil, PC Loeb, A Zaldarriaga, M Dalgarno, A Lepp, S AF Stancil, PC Loeb, A Zaldarriaga, M Dalgarno, A Lepp, S TI Cosmological recombination of lithium and its effect on the microwave background anisotropies SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; cosmic microwave background; cosmology : theory; early universe; nuclear reactions, nucleosynthesis, abundances ID EARLY UNIVERSE; ATOMIC DATA; CHEMISTRY; ASTROPHYSICS; MOLECULES; DEUTERIUM; IONS; LI AB The cosmological recombination history of lithium, produced during big bang nucleosynthesis, is presented using updated chemistry and cosmological parameters consistent with recent cosmic microwave background (CMB) measurements. For the popular set of cosmological parameters, about a fifth of the lithium ions recombine into neutral atoms by a redshift zsimilar to400. The neutral lithium atoms scatter resonantly the CMB at 6708 Angstrom and distort its intensity and polarization anisotropies at observed wavelengths around similar to300 mum, as originally suggested by Loeb. The modified anisotropies resulting from the lithium recombination history are calculated for a variety of cosmological models and found to result primarily in a suppression of the power spectrum amplitude. Significant modification of the power spectrum occurs for models that assume a large primordial abundance of lithium. While detection of the lithium signal might prove difficult, it offers the possibility of inferring the lithium primordial abundance and is the only probe proposed to date of the large-scale structure of the universe for zsimilar to500-100. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NYU, Dept Phys, New York, NY 10003 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. RP Stancil, PC (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. NR 30 TC 15 Z9 15 U1 3 U2 7 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 NOV 20 PY 2002 VL 580 IS 1 BP 29 EP 35 DI 10.1086/343070 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 616ET UT WOS:000179291400004 ER PT J AU Petry, D Bond, IH Bradbury, SM Buckley, JH Carter-Lewis, DA Cui, W Duke, C Perez, ID Falcone, A Fegan, DJ Fegan, SJ Finley, JP Gaidos, JA Gibbs, K Gammell, S Hall, J Hall, TA Hillas, AM Holder, J Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krennrich, F LeBohec, S Moriarty, P Muller, D Nagai, TN Ong, R Page, M Pallassini, R Power-Mooney, B Quinn, J Reay, NW Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Sidwell, R Stanton, N Swordy, SP Vassiliev, VV Wakely, SP Walker, G Weekes, TC AF Petry, D Bond, IH Bradbury, SM Buckley, JH Carter-Lewis, DA Cui, W Duke, C Perez, ID Falcone, A Fegan, DJ Fegan, SJ Finley, JP Gaidos, JA Gibbs, K Gammell, S Hall, J Hall, TA Hillas, AM Holder, J Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krennrich, F LeBohec, S Moriarty, P Muller, D Nagai, TN Ong, R Page, M Pallassini, R Power-Mooney, B Quinn, J Reay, NW Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Sidwell, R Stanton, N Swordy, SP Vassiliev, VV Wakely, SP Walker, G Weekes, TC TI The TeV spectrum of H1426+428 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (H1426+428); gamma rays : observations ID RAY; OBJECTS AB The BL Lac object H1426+428 was recently detected as a high-energy gamma-ray source by the VERITAS collaboration (Horan et al.). We have reanalyzed the 2001 portion of the data used in the detection in order to examine the spectrum of H1426+428 above 250 GeV. We find that the time-averaged spectrum agrees with a power law of the shape (dF/dE) (E)=10(-7.31+/-0.15 stat +/-0.16 syst) E-3.50+/-0.35 stat +/-0.05 syst m(-2) s(-1) TeV-1. The statistical evidence from our data for emission above 2.5 TeV is 2.6 sigma. At the 95% confidence level, the integral flux of H1426+428 above 2.5 TeV is larger than 3% of the corresponding flux from the Crab Nebula. The spectrum is consistent with the (noncontemporaneous) measurement by Aharonian et al. both in shape and in normalization. Below 800 GeV, the data clearly favor a spectrum steeper than that of any other TeV blazar observed so far, indicating a difference in the processes involved either at the source or in the intervening space. C1 Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland, Dept Phys, Dublin 4, Ireland. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. Depauw Univ, Dept Phys, Greencastle, IN 46135 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. Cork Inst Technol, Dept Phys, Cork, Ireland. RP Petry, D (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Hall, Jeter/F-6108-2013; Hall, Jeter/E-9294-2015; OI Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383 NR 16 TC 49 Z9 49 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 NOV 20 PY 2002 VL 580 IS 1 BP 104 EP 109 DI 10.1086/343102 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 616ET UT WOS:000179291400012 ER PT J AU Harris, DE Finoguenov, A Bridle, AH Hardcastle, MJ Laing, RA AF Harris, DE Finoguenov, A Bridle, AH Hardcastle, MJ Laing, RA TI X-ray detection of the inner jet in the radio galaxy M84 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (M84); galaxies : jets; radiation mechanisms : nonthermal; radio continuum : galaxies; X-rays : galaxies AB During the course of an investigation of the interaction of the radio galaxy M84 and its ambient cluster gas, we found excess X-ray emission aligned with the northern radio jet. The emission extends from the X-ray core of the host galaxy as a weak bridge and then brightens to a local peak coincident with the first detectable radio knot at approximate to2."5 from the core. The second radio knot at 3."3 is brighter in both radio and X-ray. The X-ray jet terminates 3."9 from the core. Although all the evidence suggests that Doppler favoritism augments the emission of the northern jet, it is unlikely that the excess X-ray emission is produced by inverse Compton emission. We find many similarities between the M84 X-ray jet and recent jet detections from Chandra data of low-luminosity radio galaxies. For most of these current detections, synchrotron emission is the favored explanation for the observed X-rays. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Univ Oxford, Dept Astrophys, Nucl & Astrophys Lab, Oxford OX1 3RH, England. RP Harris, DE (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 9 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 NOV 20 PY 2002 VL 580 IS 1 BP 110 EP 113 DI 10.1086/343112 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 616ET UT WOS:000179291400013 ER PT J AU Perna, R Lazzati, D AF Perna, R Lazzati, D TI Time-dependent photoionization in a dusty medium. I. Code description and general results SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; X-rays : general ID GAMMA-RAY BURST; CROSS-SECTIONS; DIELECTRONIC RECOMBINATION; INTERSTELLAR GRAINS; ABSORPTION; DESTRUCTION; SPECTRUM; H-2; ENVIRONMENTS; FLUORESCENCE AB We present a time-dependent photoionization code that combines self-consistently metal evolution and dust destruction under an intense X-ray UV radiation field. First, we extend the mathematical formulation of the time-dependent evolution of dust grains under an intense radiation flux with the inclusion of the process of ion field emission (IFE). We determine the relative importance of IFE with respect to X-ray and UV sublimation as a function of grain size, intensity, and hardness of the incident spectrum. We then combine the processes of dust destruction with a photoionization code that follows the evolution of the ionization states of the metals and the relative radiative transitions. Our code treats, self-consistently, the gradual recycling of metals into gas as dust is sublimated away; it allows for any initial dust grain distribution and follows its evolution in space and time. In this first paper, we use our code to study the time-dependent behavior of the X-ray and optical opacities in the nearby environment of a gamma-ray burst and show how the time variability of the low- and high-energy opacities can yield powerful clues on the characteristics of the medium in which the bursts occur. C1 Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Perna, R (reprint author), Harvard Soc Fellows, 74 Mt Auburn St, Cambridge, MA 02138 USA. NR 38 TC 78 Z9 78 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 NOV 20 PY 2002 VL 580 IS 1 BP 261 EP 277 DI 10.1086/343081 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 616ET UT WOS:000179291400025 ER PT J AU Briceno, C Luhman, KL Hartmann, L Stauffer, JR Kirkpatrick, JD AF Briceno, C Luhman, KL Hartmann, L Stauffer, JR Kirkpatrick, JD TI The initial mass function in the Taurus star-forming region SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : luminosity function, mass function; stars : pre-main-sequence ID YOUNG BROWN DWARFS; ORION NEBULA CLUSTER; AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE STARS; IMAGING SURVEY; OPTICAL SPECTROSCOPY; STELLAR POPULATION; EXTINCTION LAW; BINARY STARS; DARK CLOUD AB By combining a deep optical imaging (I, z') survey of 8 deg(2) in the Taurus star-forming region with data from the Two-Micron All-Sky Survey (2MASS) and follow-up spectroscopy, we have performed a search for low-mass Taurus members that is complete to 0.02M. for reddenings of A(V) less than or similar to 4. We report the discovery of nine new members with spectral types of M5.75-M9.5, corresponding to masses of 0.1-0.015 M. by recent evolutionary models. The new M9.5 member is the least massive brown dwarf found to date in the Taurus star-forming region. We derive an initial mass function (IMF) for the fields surveyed in this work and in our previous studies, which encompass 54% of the known Taurus membership. We compare the Taurus IMF with a similarly derived one for the Trapezium Cluster and to mass functions for the M35 and Pleiades open clusters. While the IMFs in all of these regions flatten near similar to0.8M., the mass function in Taurus is more narrow and sharply peaked at this mass. Our survey indicates that Taurus has similar to2 x fewer brown dwarfs at 0.02-0.08 M. than the Trapezium. We discuss the implications of these results for theories of the IMF, and suggest that the lower frequency of brown dwarfs in Taurus relative to the Trapezium may result from the low-density star-forming environment, leading to larger minimum Jeans masses. C1 Ctr Invest Astron, Merida 5101A, Venezuela. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Briceno, C (reprint author), Ctr Invest Astron, Apartado Postal 264, Merida 5101A, Venezuela. NR 94 TC 263 Z9 263 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 NOV 20 PY 2002 VL 580 IS 1 BP 317 EP 335 DI 10.1086/343127 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 616ET UT WOS:000179291400029 ER PT J AU Eff-Darwich, A Korzennik, SG Jimenez-Reyes, SJ Hernandez, FP AF Eff-Darwich, A Korzennik, SG Jimenez-Reyes, SJ Hernandez, FP TI An upper limit on the temporal variations of the solar interior stratification SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : helioseismology; Sun : interior; Sun : magnetic fields ID HELIOSEISMIC INVERSIONS; MODE FREQUENCIES; CONVECTION ZONE; CYCLE VARIATION; P-MODES; ASPHERICITY; TACHOCLINE; ROTATION; GONG AB We have analyzed changes in the acoustic oscillation eigenfrequencies measured over the past 7 years by the GONG, MDI, and LOWL instruments. The observations span the period from 1994 to 2001 that corresponds to half a solar cycle, from minimum to maximumsolar activity. These data were inverted to look for a signature of the activity cycle on the solar stratification. A one-dimensional structure inversion was carried out to map the temporal variation of the radial distribution of the sound speed at the boundary between the radiative and convective zones. Such variation could indicate the presence of a toroidal magnetic field anchored in this region. We found no systematic variation with time of the strati. cation at the base of the convection zone. However, we can set an upper limit to any fractional change of the sound speed at the level of 3 x 10(-5). C1 Inst Astrofis Canarias, Tenerife 38205, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. RP Univ La Laguna, Dept Soil Sci & Geol, Tenerife 38205, Spain. OI Jimenez Reyes, Sebastian/0000-0002-0317-4247 NR 36 TC 23 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 NOV 20 PY 2002 VL 580 IS 1 BP 574 EP 578 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 616ET UT WOS:000179291400053 ER EF