FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Riley, S AF Riley, S TI Wild thorn. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst Libs, 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 NOV 15 PY 2002 VL 127 IS 19 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 615TU UT WOS:000179263500235 ER PT J AU Herting, C Hanne, GF Bartschat, K Grum-Grzhimailo, AN Muktavat, K Srivastava, R Stauffer, AD AF Herting, C Hanne, GF Bartschat, K Grum-Grzhimailo, AN Muktavat, K Srivastava, R Stauffer, AD TI Orientation propensities in spin-resolved electron-impact excitation of mercury SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID POLARIZED ELECTRONS; COINCIDENCE; RESONANCES; PACKAGE AB The atomic orientation J(perpendicular to)(+) Hg (6s(2))S-1(0) --> (6s6p)P-3(1) is studied using the electron-photon coincidence technique. J(perpendicular to)(+) shows a significant dependence on the spin projection of the incident electrons. Experimental results are compared with theoretical predictions employing a semi-relativistic five-state R-matrix (close-coupling) description and the relativistic distorted-wave approximation. The experimental data show, in qualitative agreement with the calculations, that the well established orientation propensity rules for light atoms are apparently violated if the electron spin is initially down with respect to the scattering plane. The applicability of the propensity rules to electron-impact excitation of heavy atoms is analysed. The observed apparent violation is attributed to a quantum mechanical interference caused by 'intermediate coupling' within the excited state. A re-evaluation of the data supports the validity of the orientation propensity rules. C1 Univ Munster, Inst Phys, D-48149 Munster, Germany. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. Moscow MV Lomonosov State Univ, Inst Nucl Phys, Moscow 119992, Russia. Indian Inst Technol, Dept Phys, Roorkee 247667, Uttar Pradesh, India. York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. RP Herting, C (reprint author), Univ Munster, Inst Phys, Wilhelm Klemm Str 10, D-48149 Munster, Germany. RI Grum-Grzhimailo, Alexei/D-6274-2012; Bartschat, Klaus/I-2527-2012 NR 25 TC 13 Z9 13 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 NOV 14 PY 2002 VL 35 IS 21 BP 4439 EP 4451 AR PII S0953-4075(02)38588-2 DI 10.1088/0953-4075/35/21/309 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 618VC UT WOS:000179437100011 ER PT J AU Andersen, N Bartschat, K AF Andersen, N Bartschat, K TI Search for relativistic effects in electron-impact S -> P excitation of heavy alkali atoms: polarization, alignment and orientation in Cs SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID SCATTERING; SYSTEMS AB This work analyses in detail to what extent relativistic effects can be studied in electron-impact excitation of the (2)S(1/2) --> (2)P(1/2,3/2)(o) resonance transitions in heavy alkali atoms. For Cs at 10 eV impact energy as an example, numerical results were obtained in a 40-state semi-relativistic Breit-Pauli R-matrix calculation. For comparison, results were generated in the corresponding 23-state non-relativistic LS model. The standard Stokes parameters obtained with unpolarized electron beams are found to be extremely insensitive to the inclusion of relativistic effects. This insensitivity explains the success of non-relativistic theories in reproducing experimental results for heavy alkali atoms. If spin-polarized electrons are used, however, the generalized Stokes parameters and other spin-asymmetry parameters display small but experimentally accessible relativistic effects. Implications for future experimental studies of these systems are discussed and recommendations are given. C1 Niels Bohr Inst, Orsted Lab, DK-2100 Copenhagen, Denmark. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Andersen, N (reprint author), Niels Bohr Inst, Orsted Lab, Univ Pk 5, DK-2100 Copenhagen, Denmark. RI Bartschat, Klaus/I-2527-2012 NR 22 TC 17 Z9 17 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD NOV 14 PY 2002 VL 35 IS 21 BP 4507 EP 4525 AR PII S0953-4075(02)52407-X DI 10.1088/0953-4075/35/21/313 PG 19 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 618VC UT WOS:000179437100015 ER PT J AU Santos, MR Bromm, V Kamionkowski, M AF Santos, MR Bromm, V Kamionkowski, M TI The contribution of the first stars to the cosmic infrared background SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : formation; galaxies : formation; cosmology : theory; diffuse radiation; early Universe; infrared : general ID COLD DARK-MATTER; COSMOLOGICAL REIONIZATION; INTERMEDIATE ENERGIES; HIERARCHICAL-MODELS; UNIVERSE; FRAGMENTATION; SCATTERING; SPECTRUM; HYDROGEN; GALAXIES AB We calculate the contribution to the cosmic infrared background from very massive metal-free stars at high redshift. We explore two plausible star formation models and two limiting cases for the reprocessing of the ionizing stellar emission. We find that Population III stars may contribute significantly to the cosmic near-infrared background if the following conditions are met. (i) The first stars were massive, with M greater than or similar to 100 M-.. (ii) Molecular hydrogen can cool baryons in low-mass haloes. (iii) Population III star formation is ongoing, and not shut off through negative feedback effects. (iv) Virialized haloes form stars at similar to40 per cent efficiency up to the redshift of reionization, zsimilar to7. (v) The escape fraction of the ionizing radiation into the intergalactic medium is small. (vi) Nearly all of the stars end up in massive black holes without contributing to the metal enrichment of the Universe. C1 CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Santos, MR (reprint author), CALTECH, Mail Code 130-33, Pasadena, CA 91125 USA. NR 45 TC 145 Z9 145 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 NOV 11 PY 2002 VL 336 IS 4 BP 1082 EP 1092 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610VC UT WOS:000178981200005 ER PT J AU Gonzalez, AH Zaritsky, D Simard, L Clowe, D White, SDM AF Gonzalez, AH Zaritsky, D Simard, L Clowe, D White, SDM TI Tests of the Las Campanas Distant Cluster Survey from confirmation observations for the ESO Distant Cluster Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : high-redshift ID BAND HUBBLE DIAGRAM; GALAXIES; EVOLUTION; MODELS AB The ESO Distant Cluster Survey (EDisCS) is a photometric and spectroscopic study of the galaxy cluster population at two epochs, zsimilar or equal to0.5 and zsimilar or equal to0.8, drawn from the Las Campanas Distant Cluster Survey (LCDCS). We report results from the initial candidate-confirmation stage of the program and use these results to probe the properties of the LCDCS. Of the 30 candidates targeted, we find statistically significant overdensities of red galaxies near 28. Of the 10 additional candidates serendipitously observed within the fields of the targeted 30, we detect red galaxy overdensities near six. We test the robustness of the published LCDCS estimated redshifts to misidentification of the brightest cluster galaxy ( BCG) in the survey data and measure the spatial alignment of the published cluster coordinates, the peak red galaxy overdensity, and the BCG. We conclude that for LCDCS clusters out to zsimilar to0.8, (1) the LCDCS coordinates agree with the centroid of the red galaxy overdensity to within 25"(similar to150 h(-1) kpc) for 34 out of 37 candidates with 3sigma galaxy overdensities, (2) BCGs are typically coincident with the centroid of the red galaxy population to within a projected separation of 200 h(-1) kpc (32 out of 34 confirmed candidates), ( 3) the red galaxy population is strongly concentrated, and ( 4) the misidentification of the BCG in the LCDCS causes a redshift error greater than 0.1 in 15%-20% of the LCDCS candidates. These findings together help explain the success of the surface brightness fluctuations detection method. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Bonn, Inst Astrophys & Extraterr Forsch, D-53121 Bonn, Germany. Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Gonzalez, AH (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. NR 23 TC 12 Z9 12 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 10 PY 2002 VL 579 IS 2 BP 577 EP 586 DI 10.1086/342792 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 612EZ UT WOS:000179062700010 ER PT J AU Tucci, M Carretti, E Cecchini, S Nicastro, L Fabbri, R Gaensler, BM Dickey, JM McClure-Griffiths, NM AF Tucci, M Carretti, E Cecchini, S Nicastro, L Fabbri, R Gaensler, BM Dickey, JM McClure-Griffiths, NM TI Polarization angular spectra of Galactic synchrotron emission on arcminute scales SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; methods : statistical; polarization; radio continuum : ISM ID PLANCK SURVEYOR MISSION; RADIO-CONTINUUM; 2.4 GHZ; ANISOTROPIES; FOREGROUNDS; LIMIT AB We study the angular power spectra of the polarized component of the Galactic synchrotron emission in the 28 deg(2) test region of the Southern Galactic Plane Survey at 1.4 GHz. These data were obtained by the Australia Telescope Compact Array and allow us to investigate angular power spectra down to arcminute scales. We find that, at this frequency, the polarization spectra for E- and B-modes seem to be affected by Faraday rotation produced in compact foreground screens. A different behavior is shown by the angular spectrum of the polarized intensity PI=(Q(2)+U-2)(1/2). This is well fitted by a power law (C-PIl proportional to l(-alphaPI)) with slopesimilar to1.7, which agrees with higher frequency results and can probably be more confidently extrapolated to the cosmological window. C1 Univ Milano Bicocca, Dipartimento Fis G Occhialini, I-20126 Milan, Italy. Ist Nazl Fis Nucl, I-20133 Milan, Italy. Inst Fis Cantabria, Santander 39005, Spain. CNR, Sez Bologna, Inst Astrophys Spatiale, I-40129 Bologna, Italy. CNR, Sez Palermo, Inst Astrophys Spatiale, I-90146 Palermo, Italy. Univ Florence, Dipartimento Fis, I-50019 Sesto Fiorentino, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Commonwealth Sci & Ind Res Org, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy. RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; Nicastro, Luciano/F-5866-2015; OI Nicastro, Luciano/0000-0001-8534-6788; McClure-Griffiths, Naomi/0000-0003-2730-957X; Dickey, John/0000-0002-6300-7459; Gaensler, Bryan/0000-0002-3382-9558 NR 40 TC 25 Z9 25 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2002 VL 579 IS 2 BP 607 EP 615 DI 10.1086/342793 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 612EZ UT WOS:000179062700014 ER PT J AU Wang, L Wheeler, JC Hoflich, P Khokhlov, A Baade, D Branch, D Challis, P Filippenko, AV Fransson, C Garnavich, P Kirshner, RP Lundqvist, P McCray, R Panagia, N Pun, CSJ Phillips, MM Sonneborn, G Suntzeff, NB AF Wang, L Wheeler, JC Hoflich, P Khokhlov, A Baade, D Branch, D Challis, P Filippenko, AV Fransson, C Garnavich, P Kirshner, RP Lundqvist, P McCray, R Panagia, N Pun, CSJ Phillips, MM Sonneborn, G Suntzeff, NB TI The axisymmetric ejecta of supernova 1987A SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernova remnants; supernovae : individual (SN 1987A) ID GAMMA-RAY BURSTS; SN 1987A; NEUTRINO RADIATION; SN-1987A; SPECTROPOLARIMETRY; POLARIZATION; EXPLOSIONS; EMISSION; LINE; JET AB Extensive early observations proved that the ejecta of supernova 1987A (SN 1987A) are aspherical. The most important of these early observations include (1) the "Bochum event" that revealed small-scale spectroscopic structure indicating chemical inhomogeneities of the ejecta, (2) spectropolarimetry that showed deviations from spherical symmetry, and ( 3) speckle observations that revealed both the asymmetry of the ejecta and the "mystery spot" manifested as a secondary source off center from the bulk of the supernova ejecta. Fifteen years after the supernova explosion, the Hubble Space Telescope has resolved the rapidly expanding ejecta. The late-time images and spectroscopy provide a geometrical picture that is consistent with early observations and suggests a highly structured, axially symmetric geometry. We present here a new synthesis of the old and new data. We show that the Bochum event, presumably a clump of Ni-56, and the late-time image, the locus of excitation by Ti-44, are most naturally accounted for by sharing a common position angle of about 14degrees the same as the mystery spot and early speckle data on the ejecta, and that they are both oriented along the axis of the inner circumstellar ring at 45degrees to the plane of the sky. We also demonstrate that the polarization represents a prolate geometry with the same position angle and axis as the early speckle data and the late-time image, and hence that the geometry has been fixed in time and throughout the ejecta. The Bochum event and the Doppler kinematics of the [Ca II]/[O II] emission in spatially resolved Hubble Space Telescope spectra of the ejecta can be consistently integrated into this geometry. The radioactive clump is deduced to fall approximately along the axis of the inner circumstellar ring and therefore to be redshifted in the north, whereas the [Ca II]/[O II] 7300 Angstrom emission is redshifted in the south. We present a jet-induced model for the explosion and argue that such a model can account for many of the observed asymmetries. In the jet models, the oxygen and calcium are not expected to be distributed along the jet but primarily in an expanding torus that shares the plane and northern blue shift of the inner circumstellar ring. C1 Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. USN, Computat Phys & Fluid Dynam Lab, Res Lab, Washington, DC 20375 USA. European So Observ, D-85748 Garching, Germany. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Stockholm Observ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. ESA, Dept Space Sci, F-75738 Paris 15, France. NASA, Goddard Space Flight Ctr, Lab Astron & Space Phys, Greenbelt, MD 20771 USA. Carnegie Observ, Campanas Observ, La Serena, Chile. Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile. RP Wang, L (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, 50-232,1 Cyclotron Rd, Berkeley, CA 94720 USA. RI Sonneborn, George/D-5255-2012 NR 59 TC 132 Z9 134 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 NOV 10 PY 2002 VL 579 IS 2 BP 671 EP 677 DI 10.1086/342824 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 612EZ UT WOS:000179062700019 ER PT J AU Monnier, JD Millan-Gabet, R AF Monnier, JD Millan-Gabet, R TI On the interferometric sizes of young stellar objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; instrumentation : interferometers; radiative transfer; stars : formation; stars : pre-main-sequence ID HERBIG AE/BE STARS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; INFRARED-EMISSION; MASSIVE STARS; ENVELOPES; GRAINS AB Long-baseline optical interferometers can now detect and resolve hot dust emission thought to arise at the inner edge of circumstellar disks around young stellar objects (YSOs). We argue that the near-infrared sizes being measured are closely related to the radius at which dust is sublimated by the stellar radiation field. We consider how realistic dust optical properties and gas opacity dramatically affect the predicted location of this dust destruction radius, an exercise routinely done in other contexts but so far neglected in the analysis of near-infrared sizes of YSOs. We also present the accumulated literature of near-infrared YSO sizes in the form of a size-luminosity diagram and compare with theoretical expectations. We find evidence that large (greater than or similar to 1.0 mum) dust grains predominate in the inner disks of T Tauri and Herbig Ae/Be stars, under the assumption that the innermost gaseous disks are optically thin at visible wavelengths. 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 34 TC 129 Z9 129 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 10 PY 2002 VL 579 IS 2 BP 694 EP 698 DI 10.1086/342917 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 612EZ UT WOS:000179062700022 ER PT J AU Di Matteo, T Perna, R Narayan, R AF Di Matteo, T Perna, R Narayan, R TI Neutrino trapping and accretion models for gamma-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; gamma rays : bursts; neutrinos; scattering ID BLACK-HOLES; PHYSICAL MODELS; STAR MERGERS; EMISSION; ENERGY; DISKS; STEP; NUCLEOSYNTHESIS; BREMSSTRAHLUNG AB Many models of gamma-ray bursts (GRBs) invoke a central engine consisting of a black hole of a few solar masses accreting matter from a disk at a rate of a fraction to a few solar masses per second. Popham et al. and Narayan et al. have shown that, for (M) over dot greater than or similar to 0.1 M. s(-1), accretion proceeds via neutrino cooling and neutrinos can carry away a significant amount of energy from the inner regions of the disks. We improve on these calculations by including a simple prescription for neutrino transfer and neutrino opacities in such regions. We find that the flows become optically thick to neutrinos inside a radius R similar to 6R(S)-40 R-S for (M) over dot in the range of 0.1-10 M. s(-1), where R-S is the black hole Schwarzchild radius. Most of the neutrino emission comes from outside this region, and the neutrino luminosity stays roughly constant at a value L-nu similar to 10(53) ergs s(-1). We show that, for (M) over dot greater than or similar to 1 M. s(-1), neutrinos are sufficiently trapped that energy advection becomes the dominant cooling mechanism in the flow. These results imply that nu(ν) over bar annihilation in hyperaccreting black holes is an inefficient mechanism for liberating large amounts of energy. Extraction of rotational energy by magnetic processes remains the most viable mechanism. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. RP Di Matteo, T (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. OI Narayan, Ramesh/0000-0002-1919-2730 NR 43 TC 203 Z9 204 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 NOV 10 PY 2002 VL 579 IS 2 BP 706 EP 715 DI 10.1086/342832 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 612EZ UT WOS:000179062700024 ER PT J AU Edmonds, PD Gilliland, RL Camilo, F Heinke, CO Grindlay, JE AF Edmonds, PD Gilliland, RL Camilo, F Heinke, CO Grindlay, JE TI A millisecond pulsar optical counterpart with large-amplitude variability in the globular cluster 47 Tucanae SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; globular clusters : individual (47 Tucanae); pulsars : general; pulsars : individual (PSR J0024-7204W); techniques : photometric ID 47-TUCANAE; COMPANION; BINARIES; EVOLUTION; CORE; CALIBRATION; EMISSION; NGC-6397; TERZAN-5; STARS AB Using extensive Hubble Space Telescope imaging, combined with Chandra X-ray and Parkes radio data, we have detected the optical binary companion to a second millisecond pulsar (MSP) in the globular cluster 47 Tucanae. This faint (V = 22.3) blue (V-I = 0.7) star shows a large-amplitude (60%-70%) sinusoidal variation in both V and I. The period (3.19066 hr) and phase of the variation match those of the MSP 47 Tuc W (which does not have an accurate radio timing position) to within 0.5 s and 1.2 minutes, respectively, well within the 1 sigma errors. The phase dependence of the intensity and color implies that heating of a tidally locked companion causes the observed variations. The eclipsing nature of this MSP in the radio, combined with the relatively large companion mass (greater than 0.13 M.) and the companion s position in the color-magnitude diagram, suggests that the companion is a main-sequence star, a rare circumstance for an MSP companion. This system is likely to have had a complex evolution and represents an interesting case study in MSP irradiation of a close companion. We present evidence for another optical variable with similar properties to the companion of 47 Tuc W. This variable also may be an MSP companion, although no radio counterpart has yet been detected. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Edmonds, PD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Heinke, Craig/0000-0003-3944-6109 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 NOV 10 PY 2002 VL 579 IS 2 BP 741 EP 751 DI 10.1086/342985 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 612EZ UT WOS:000179062700027 ER PT J AU Herrnstein, RM Ho, PTP AF Herrnstein, RM Ho, PTP TI Hot molecular gas in the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; ISM : clouds; ISM : molecules; radio lines : ISM ID APERTURE SYNTHESIS OBSERVATIONS; SAGITTARIUS-A COMPLEX; CENTER REGION; GALAXY; RESOLUTION; PARSECS; CLOUD; SUBMILLIMETER; AMMONIA; IC-443 AB Using the new 23 GHz receivers at the Very Large Array (VLA), we have detected NH3 (6, 6) emission (v = 25.056025 GHz) from hot (>150 K) molecular clouds in the central 10 pc of the Galaxy. This is the first successful detection of NH3 (6, 6) with the VLA. The brightest emission comes from a region interior to the "circumnuclear disk" (CND), less than 1.5 pc in projected distance from Sagittarius A*. This region does not show molecular emission from lower energy transitions such as NH3 (1, 1) and (2, 2), HCN (1-0), and HCO+ (1-0). Line ratios of NH3 (6, 6) and (3, 3) emission as well as NH3 (6, 6) line widths have peak values within 1.5 pc of Sgr A*, indicating that the gas is physically close to the nucleus. NH3 (6, 6) is also detected toward many features outside the CND observed in NH3 (1, 1), (2, 2), and (3, 3). These features tend to lie along ridges of gas associated with Sgr A East or the massive "molecular ridge" that connects the "20 km s(-1)" and "50 km s(-1)" giant molecular clouds. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Herrnstein, RM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 26 Z9 26 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2002 VL 579 IS 2 BP L83 EP L86 DI 10.1086/345289 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 612FG UT WOS:000179063400008 ER PT J AU Kidun, O Fominykh, N Berakdar, J AF Kidun, O Fominykh, N Berakdar, J TI Scattering and bound-state problems with non-local potentials: application of the variable-phase approach SO JOURNAL OF PHYSICS A-MATHEMATICAL AND GENERAL LA English DT Article AB Following the framework of the variable-phase approach, we derive an equation for determining the scattering amplitude of a non-relativistic quantum particle in a non-local potential. Its solution implies the integration of the Volterra integro-differential equation of the first kind and allows determination of bound-state. energies and wavefunctions. A fast numerical scheme for the solution of these equations is suggested and it is demonstrated that the proposed method requires the numerical efforts of the same order as in the local potential case. C1 Max Planck Inst Mikrostrukturphys, D-06120 Halle Saale, Germany. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Kidun, O (reprint author), Max Planck Inst Mikrostrukturphys, Weinberg 2, D-06120 Halle Saale, Germany. OI Berakdar, Jamal/0000-0001-8727-3981 NR 13 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0305-4470 J9 J PHYS A-MATH GEN JI J. Phys. A-Math. Gen. PD NOV 8 PY 2002 VL 35 IS 44 BP 9413 EP 9424 AR PII S0305-4470(02)36609-5 DI 10.1088/0305-4470/35/44/310 PG 12 WC Physics, Multidisciplinary; Physics, Mathematical SC Physics GA 622WJ UT WOS:000179670300010 ER PT J AU Shoemaker, DD Machado, CA Molbo, D Werren, JH Windsor, DM Herre, EA AF Shoemaker, DD Machado, CA Molbo, D Werren, JH Windsor, DM Herre, EA TI The distribution of Wolbachia in fig wasps: correlations with host phylogeny, ecology and population structure SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Agaonidae; fig; fig wasp; horizontal transfer; Wolbachia; wsp ID CYTOPLASMIC INCOMPATIBILITY; NEW-WORLD; HORIZONTAL TRANSMISSION; MOLECULAR PHYLOGENIES; NEMATODE PARASITES; POLLINATING WASPS; WSP GENE; EVOLUTION; INSECT; PARTHENOGENESIS AB We surveyed for the presence and identity of Wolbachia in 44 species of chalcid wasps associated with 18 species of Panamanian figs. We used existing detailed knowledge of the population structures of the host wasps, as well as the ecological and evolutionary relationships among them, to explore the relevance of each of these factors to Wolbachia prevalence and mode of transmission. Fifty-nine per cent of these wasp species have Wolbachia infections, the highest proportion reported for any group of insects. Further, neither the presence nor the frequency of Wolbachia within hosts was correlated with the population structure of pollinator hosts. Phylogenetic analyses of wsp sequence data from 70 individuals representing 22 wasp species show that neither the close phylogenetic relationship nor close ecological association among host species is consistently linked to close phylogenetic affinities of the Wolbachia associated with them. Moreover, no genetic variation was detected within any Wolbachia strain from a given host species. Thus, the spread of Wolbachia within host species exceeds the rate of horizontal transmission among species and both exceed the rate of mutation of the wsp gene in Wolbachia. The presence and, in some cases, high frequency of Wolbachia infections within highly inbred species indicate that the Wolbachia either directly increase host fitness or are frequently horizontally transferred within these wasp species. However, the paucity of cospeciation of Wolbachia and their wasp hosts indicates that Wolbachia do not persist within a given host lineage for long time-periods relative to speciation times. C1 Western Michigan Univ, Dept Sci Biol, Kalamazoo, MI 49008 USA. Rutgers State Univ, Nelson Biol Labs, Dept Genet, Piscataway, NJ 08854 USA. Univ Lausanne, IE ZEA, CH-1015 Lausanne, Switzerland. Univ Rochester, Dept Biol, Rochester, NY 14627 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Shoemaker, DD (reprint author), Univ Wisconsin, Dept Entomol, 1630 Linden Dr,643 Russell Labs, Madison, WI 53706 USA. EM dshoemak@entomology.wisc.edu RI Machado, Carlos/B-8855-2009; OI Machado, Carlos/0000-0003-1546-7415; Molbo, Drude/0000-0003-3372-8711 NR 57 TC 63 Z9 65 U1 2 U2 25 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 7 PY 2002 VL 269 IS 1506 BP 2257 EP 2267 DI 10.1098/rspb.2002.2100 PG 11 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 615LB UT WOS:000179245700010 PM 12427319 ER PT J AU Elliott, WC Haynes, JT AF Elliott, WC Haynes, JT TI The chemical character of fluids forming diagenetic illite in the Southern Appalachian Basin SO AMERICAN MINERALOGIST LA English DT Article ID LATE PALEOZOIC REMAGNETIZATION; K-AR AGES; ILLINOIS BASIN; OXYGEN-ISOTOPE; SEDIMENTARY BASINS; BRINE MIGRATION; PLATE-TECTONICS; CARBONATE ROCKS; NORTH-AMERICA; SMECTITE AB Diagenetic illite (mixed layer illite-smectite, I-S) from Ordovician and Devonian potassium bentonite (K-bentonite) and shales was studied in the proximal southern Appalachian Basin (Alabama through Virginia) to understand in more detail the timing of illite formation as well as attempt to describe the chemistry of the fluids that formed illite during the Alleghanian Orogeny through combined K/Rb and oxygen isotope analyses. The clay fraction of the K-bentonites is composed predominantly of illite-smectite (I-S) and chlorite. Most I-S exhibited Kalkberg order (IISI) with >85% illite layers. The K-Ar dates of I-S from Ordovician K-bentonites and Devonian K-bentonites mostly range from 260-310 Ma and indicate I-S formed during the Alleghanian Orogeny. Internally concordant dates and similar percentages of illite layers of I-S are measured from several samples collected within a thick (1 m) Ordovician K-bentonite at Fort Payne, Alabama. The oxygen isotopic values (delta(18)O) of I-S range from 18-23parts per thousandSMOW. At lowest levels of thermal maturity and burial, as seen by conodont alteration index values (CAI) of 1.5-2.0, the range in delta(18)O values of water in equilibrium with I-S is 2.5-3.5parts per thousand. At higher thermal maturity (CAI = 2.5-4.5), the delta(18)O of water in equilibrium with I-S is from 4.5 to 12parts per thousand. The delta(18)O analyses are mostly consistent with I-S having formed in the presence of orogenic (i.e., saline) waters. The mean K/Rb of the Appalachian illites from this study is 325 (N = 20). This mean K/Rb is also consistent with the formation of diagenetic I-S in the presence of a saline fluids having higher K activities than meteoric waters. The combined data indicate these diagenetic illites in K-bentonites formed from saline/orogenic waters during the Alleghanian Orogeny along the Valley and Ridge Province in the southern Appalachian Basin. Although the data rule out formation of diagenetic illite in the presence of meteoric water or long-term reaction with connate formation waters, the combined data cannot distinguish the source and the mechanism (tectonic push or flush from tectonic highlands) for the movement of saline fluids in the Appalachian Basin. C1 Georgia State Univ, Dept Geol, Atlanta, GA 30303 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Pomfret Sch, Pomfret, CT 06258 USA. RP Elliott, WC (reprint author), Georgia State Univ, Dept Geol, Atlanta, GA 30303 USA. EM geowce@panther.Gsu.edu NR 53 TC 11 Z9 11 U1 2 U2 6 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 NOV-DEC PY 2002 VL 87 IS 11-12 BP 1519 EP 1527 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 618JZ UT WOS:000179416100002 ER PT J AU Woo, R Habbal, SR AF Woo, R Habbal, SR TI The origin of the solar wind - A novel way of looking at the solar corona reveals a hidden "imprint" of the Sun SO AMERICAN SCIENTIST LA English DT Article ID SLOW C1 CALTECH, NASAs Jet Prop Lab, Pasadena, CA USA. Univ Wales, Aberystwyth, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Woo, R (reprint author), JPL, 4800 oak Grove Dr,MS 238-725, Pasadena, CA 91109 USA. EM richard.woo@jpl.nasa.gov NR 17 TC 6 Z9 7 U1 0 U2 1 PU SIGMA XI-SCI RES SOC PI RES TRIANGLE PK PA PO BOX 13975, RES TRIANGLE PK, NC 27709 USA SN 0003-0996 J9 AM SCI JI Am. Scientist PD NOV-DEC PY 2002 VL 90 IS 6 BP 532 EP 539 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 603HR UT WOS:000178553700016 ER PT J AU Wielebnowski, NC Ziegler, K Wildt, DE Lukas, J Brown, JL AF Wielebnowski, NC Ziegler, K Wildt, DE Lukas, J Brown, JL TI Impact of social management on reproductive, adrenal and behavioural activity in the cheetah (Acinonyx jubatus) SO ANIMAL CONSERVATION LA English DT Article ID NORTH-AMERICAN ZOOS; ADRENOCORTICAL FUNCTION; CORTISOL METABOLITES; DOMESTIC CAT; SUPPRESSION; FELIDS; STEROIDS; HORMONE; QUALITY; MAMMALS AB Cheetahs (Acinonyx jubatus) held ex situ can provide an important resource for obtaining new biological information that usually cannot be gleaned from free-living individuals. However, consistent captive propagation of the cheetah, a prerequisite for establishing a self-sustaining population, has not been accomplished so far. This study examined the effect of a husbandry regimen commonly used in ex situ facilities on female cheetahs. Although generally solitary in the wild, zoos frequently house cheetahs in pairs or groups. Using non-invasive hormone monitoring and quantitative behavioural observations, we studied the impact of such enforced social conditions on behaviour and ovarian/adrenal activity. Eight female cheetahs were evaluated for two consecutive 6-month periods, first while maintained in pairs and then as individuals. Subsequently four females were regrouped into two new pairs and monitored for another 6 months. Females in five of six pairings demonstrated prolonged anoestrus and displayed agonistic behaviours. After pair separation all females rapidly resumed oestrous cyclicity. Females in the sixth pair continued cycling throughout the year while consistently displaying affiliative grooming and no agonistic behaviours. Faecal corticoid patterns varied significantly among individuals, but appeared unrelated to behavioural or ovarian hormone patterns. Thus, data appear to indicate that same-sex pair-maintenance of behaviourally incompatible female cheetahs may lead to suppressed ovarian cyclicity. This suppression appears linked to agonistic behaviours but not to any particular adrenal hormone excretion pattern. Results clearly demonstrate the value of applying knowledge about in situ social behaviour to ex situ management practices. Conversely, however, non-invasive hormone monitoring conducted ex situ may help us to identify physiological phenomena of potential relevance for future in situ studies. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. White Oak Conservat Ctr, Yulee, FL 32097 USA. RP Wielebnowski, NC (reprint author), Brookfield Zoo, Chicago Zool Soc, 3300 Golfr Rd, Brookfield, IL 60513 USA. NR 65 TC 56 Z9 63 U1 6 U2 59 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD NOV PY 2002 VL 5 BP 291 EP 301 DI 10.1017/S1367943002004043 PN 4 PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 622TZ UT WOS:000179664300004 ER PT J AU Pogue, MG AF Pogue, MG TI Identity of a sugar cane pest, Scolecocampa mochisa (Schaus), in Mexico, and a new generic synonym (Lepidoptera : Noctuidae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Scolecocampa; sugar cane; pest; egg; larva; pupa AB A sugar cane pest in Mexico, Scolecocampa mochisa (Schaus) (new combination), was originally described in the monotypic genus Saccharaphagos Schaus (1923), which is considered a new synonym of Scolecocampa Guenee (1852). The adult and larva are illustrated. The genitalia, egg, and pupa are described and illustrated. The closely related species, Scolecocampa stygialis (Smith), is a new combination. C1 Smithsonian Inst, Systemat Entomol Lab, Inst Plant Sci, ARS,USDA,NMNH, Washington, DC 20013 USA. RP Pogue, MG (reprint author), Smithsonian Inst, Systemat Entomol Lab, Inst Plant Sci, ARS,USDA,NMNH, MRC-168,POB 37012, Washington, DC 20013 USA. NR 9 TC 2 Z9 3 U1 0 U2 2 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD NOV PY 2002 VL 95 IS 6 BP 653 EP 657 DI 10.1603/0013-8746(2002)095[0653:IOASCP]2.0.CO;2 PG 5 WC Entomology SC Entomology GA 625NJ UT WOS:000179822300001 ER PT J AU Leonard, DC Filippenko, AV Li, WD Matheson, T Kirshner, RP Chornock, R Van Dyk, SD Berlind, P Calkins, ML Challis, PM Garnavich, PM Jha, S Mahdavi, A AF Leonard, DC Filippenko, AV Li, WD Matheson, T Kirshner, RP Chornock, R Van Dyk, SD Berlind, P Calkins, ML Challis, PM Garnavich, PM Jha, S Mahdavi, A TI A study of the Type II-plateau supernova 1999gi and the distance to its host galaxy, NGC 3184 SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; galaxies : individual (NGC 3184); supernovae : individual (SN 1999gi) ID EXPANDING PHOTOSPHERE METHOD; LARGE MAGELLANIC CLOUD; STANDARD STARS; SPIRAL GALAXIES; HUBBLE CONSTANT; PROGENITOR; TELESCOPE; SPECTRA; SPECTROPHOTOMETRY; 1993J AB We present optical spectra and photometry sampling the first 6 months after discovery of supernova (SN) 1999gi in NGC 3184. SN 1999gi is shown to be a Type II-plateau event with a photometric plateau lasting until about 100 days after discovery. Using the expanding photosphere method (EPM), we derive a distance to SN 1999gi of 11.1(-1.8)(+2.0) Mpc and an explosion date of 1999 December 5.8(-3.1)(+3.0), or 4.1(-3.1)(+3.0) days prior to discovery. This distance is consistent with a Tully-Fisher distance recently derived to NGC 3184 (Dapproximate to11.59 Mpc), but it is somewhat closer than the Cepheid distances recently derived to two galaxies that have generally been assumed to be associated with the group containing NGC 3184 (NGC 3319, D=13.30+/-0.55 Mpc, and NGC 3198, D=13.80+/-0.51 Mpc). From many lines of evidence, we conclude that SN 1999gi is only minimally reddened. A comparison between the color of SN 1999gi at early times and that of an infinitely hot blackbody restricts the reddening to E(B-V)<0.45 mag, while a comparison between the color evolution of SN 1999gi and the well-observed ( and extensively modeled) Type II-P SN 1999em implies an even more restrictive upper reddening limit of E (B-V)<0.3 mag. A variety of other, independent reddening estimates are consistent with these upper limits and yield a probable reddening of E (B-V)=0.21+/-0.09 mag. We reconsider the upper mass limit (9(-2)(+3) M-circle dot) recently placed on the progenitor star of SN 1999gi by Smartt et al. in light of these results. Following the same procedures, but using the new data presented here, we arrive at a less restrictive upper mass limit of 15(-3)(+5) M-circle dot for the progenitor. The increased upper limit results mainly from the larger distance derived through the EPM than was assumed by the Smartt et al. analyses, which relied on less precise (and less recent) distance measurements to NGC 3184. Finally, we confirm the existence of "complicated" P Cygni line profiles in early-time and later photospheric-phase spectra of SN 1999gi. These features, first identified by Baron et al. in spectra of SN 1999em as high-velocity absorptions, in addition to the "normal" lower velocity component, are here verified to be true P Cygni profiles consisting of both an absorption trough and an emission peak at early times. In the earliest spectrum, taken less than a day after discovery, the features extend out to nearly -30,000 km s(-1), indicating the existence of very high velocity material in the outer envelope of SN 1999gi. C1 Univ Massachusetts, Five Coll Astron Dept, Amherst, MA 01003 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Leonard, DC (reprint author), Univ Massachusetts, Five Coll Astron Dept, Amherst, MA 01003 USA. NR 82 TC 111 Z9 112 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2002 VL 124 IS 5 BP 2490 EP 2505 DI 10.1086/343771 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607AL UT WOS:000178768200009 ER PT J AU Larsen, SS Brodie, JP Sarajedini, A Huchra, JP AF Larsen, SS Brodie, JP Sarajedini, A Huchra, JP TI Structural parameters and dynamical masses for globular clusters in M33 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M33); galaxies : star clusters ID HUBBLE-SPACE-TELESCOPE; TO-LIGHT RATIOS; STAR-CLUSTERS; VELOCITY DISPERSIONS; FUNDAMENTAL PLANE; RADIAL-VELOCITIES; INDIVIDUAL STARS; STELLAR-SYSTEMS; RELATIVE AGES; GALAXY AB Using high-dispersion spectra from the HIRES echelle spectrograph on the Keck I telescope, we measure velocity dispersions for four globular clusters (GCs) in M33. Combining the velocity dispersions with integrated photometry and structural parameters derived from King-Michie model fits to Wide Field Planetary Camera 2 images, we obtain mass-to-light ratios for the clusters. The mean value is M/L-V=1.53+/-0.18, very similar to the M/L-V of Milky Way and M31 GCs. The M33 clusters also fit very well into the fundamental plane and binding energy luminosity relations derived for Milky Way GCs. Dynamically and structurally, the four M33 clusters studied here appear virtually identical to Milky Way and M31 GCs. C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Larsen, SS (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. NR 58 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 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2002 VL 124 IS 5 BP 2615 EP 2624 DI 10.1086/344110 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607AL UT WOS:000178768200019 ER PT J AU Di Francesco, J Hogerheijde, MR Welch, WJ Bergin, EA AF Di Francesco, J Hogerheijde, MR Welch, WJ Bergin, EA TI Abundances of molecular species in Barnard 68 SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : globules; ISM : individual (Barnard 68); ISM : molecules; stars : formation ID BOK GLOBULES; DARK CLOUDS; STAR-FORMATION; CHEMISTRY; EMISSION; CORES; CANDIDATES; AMMONIA; PHYSICS; LINES AB Abundances for five molecules ((CO)-O-18, CS, NH3, H2CO, and C3H2) and one molecular ion (N2H+) and upper limits for the abundances of one molecule ((CO)-C-13) and one molecular ion (HCO+) are derived for gas within the Bok globule Barnard 68 (B68). The abundances were determined using our own BIMA millimeter interferometer data and single-dish data gathered from the literature, in conjunction with a Monte Carlo radiative transfer model. Since B68 is the only starless core to have its density structure strongly constrained via extinction mapping, a major uncertainty has been removed from these determinations. All abundances for B68 are lower than those derived for translucent and cold dense clouds, but perhaps significantly only for N2H+, NH3, and C3H2. Depletion of CS toward the extinction peak of B68 is hinted at by the large offset between the extinction peak and the position of maximum CS line brightness. Abundances derived here for (CO)-O-18 and N2H+ are consistent with other, recently determined values at positions observed in common. C1 Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94705 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Francesco, J (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. NR 34 TC 17 Z9 17 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2002 VL 124 IS 5 BP 2749 EP 2755 DI 10.1086/344078 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607AL UT WOS:000178768200028 ER PT J AU Chagnon, G Mennesson, B Perrin, G du Foresto, VC Salome, P Borde, P AF Chagnon, G Mennesson, B Perrin, G du Foresto, VC Salome, P Borde, P TI L '-band interferometric observations of evolved stars SO ASTRONOMICAL JOURNAL LA English DT Article DE stars : AGB and post-AGB; stars : late-type; techniques : interferometric ID MODE GUIDED OPTICS; STELLAR INTERFEROMETER; IOTA INTERFEROMETER; DIFFRACTION LIMIT; R-LEONIS; SURFACE; GIANTS; INSTRUMENT; TELESCOPE; SPACE AB Ten bright Miras, six semiregular variable giants, and two semiregular variable supergiants have been observed with the Infrared-Optical Telescope Array interferometer in the L' band (from 3.4 to 4.1 mum). Observations were carried out in 2000 March and November with the FLUOR/TISIS instrument, using optimized single-mode waveguides for optical recombination and a dedicated chopping system for accurate subtraction of slow thermal background drifts. Four of the sources (the Mira stars R Leo and R Cnc, alpha Ori, and RS Cnc) were observed in both runs. We report on visibility measurements and derive L' broadband uniform disk (UD) diameter best fits for all 18 stars in our sample. We also detect strong departures from UD models in some peculiar cases. C1 Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chagnon, G (reprint author), Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, 5 Pl Jules Janssen, F-92195 Meudon, France. NR 24 TC 23 Z9 23 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2002 VL 124 IS 5 BP 2821 EP 2832 DI 10.1086/343057 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607AL UT WOS:000178768200033 ER PT J AU Strolger, LG Smith, RC Suntzeff, NB Phillips, MM Aldering, G Nugent, P Knop, R Perlmutter, S Schommer, RA Ho, LC Hamuy, M Krisciunas, K Germany, LM Covarrubias, R Candia, P Athey, A Blanc, G Bonacic, A Bowers, T Conley, A Dahlen, T Freedman, W Galaz, G Gates, E Goldhaber, G Goobar, A Groom, D Hook, IM Marzke, R Mateo, M McCarthy, P Mendez, J Muena, C Persson, SE Quimby, R Roth, M Ruiz-Lapuente, P Seguel, J Szentgyorgyi, A von Braun, K Wood-Vasey, WM York, T AF Strolger, LG Smith, RC Suntzeff, NB Phillips, MM Aldering, G Nugent, P Knop, R Perlmutter, S Schommer, RA Ho, LC Hamuy, M Krisciunas, K Germany, LM Covarrubias, R Candia, P Athey, A Blanc, G Bonacic, A Bowers, T Conley, A Dahlen, T Freedman, W Galaz, G Gates, E Goldhaber, G Goobar, A Groom, D Hook, IM Marzke, R Mateo, M McCarthy, P Mendez, J Muena, C Persson, SE Quimby, R Roth, M Ruiz-Lapuente, P Seguel, J Szentgyorgyi, A von Braun, K Wood-Vasey, WM York, T TI The Type Ia supernova 1999aw: A probable 1999aa-like event in a low-luminosity host galaxy SO ASTRONOMICAL JOURNAL LA English DT Article DE supernovae : general; supernovae : individual (SN 1999aw) ID LIGHT CURVES; PEAK BRIGHTNESS; STANDARD STARS; HUBBLE DIAGRAM; DECLINE RATE; PHOTOMETRY; PHYSICS; LAMBDA; CALIBRATION; EXTINCTION AB SN 1999aw was discovered during the first campaign of the Nearby Galaxies Supernova Search project. This luminous, slow-declining [Deltam(15)(B) = 0.81 +/- 0.03] Type Ia supernova was noteworthy in at least two respects. First, it occurred in an extremely low luminosity host galaxy that was not visible in the template images nor in initial subsequent deep imaging. Second, the photometric and spectral properties of this supernova indicate that it very likely was similar to the subclass of Type Ia supernovae whose prototype is SN 1999aa. This paper presents the BVRI and J(s)HK(s) light curves of SN 1999aw ( through similar to100 days past maximum light), as well as several epochs of optical spectra. From these data, we calculate the bolometric light curve and give estimates of the luminosity at maximum light and the initial (56)Ni mass. In addition, we present deep BVI images obtained recently with the Baade 6.5 m telescope at Las Campanas Observatory that reveal the remarkably low-luminosity host galaxy. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. Observ Carnegie Inst Washington, Observ Las Campanas, La Serena, Chile. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. European So Observ, Santiago 19, Chile. Univ Washington, Dept Astron, Seattle, WA 98195 USA. CEA, DSM, DAPNIA,Ctr Etud Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Pontificia Univ Catolica Chile, Santiago 22, Chile. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Stockholm Observ, SCFAB, Dept Phys, SE-10691 Stockholm, Sweden. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. Univ Oxford, Dept Phys, Oxford OX1 3RH, England. Univ Barcelona, Dept Astron, E-08028 Barcelona, Spain. Isaac Newton Grp, E-38780 Tenerife, Spain. Univ Concepcion, Dept Fis, Concepcion, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Strolger, LG (reprint author), Univ Michigan, Dept Astron, 830 Dennison Bldg, Ann Arbor, MI 48109 USA. EM loust@umich.edu RI Hamuy, Mario/G-7541-2016; Perlmutter, Saul/I-3505-2015 OI Perlmutter, Saul/0000-0002-4436-4661 NR 62 TC 70 Z9 70 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2002 VL 124 IS 5 BP 2905 EP 2919 DI 10.1086/343058 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607AL UT WOS:000178768200041 ER PT J AU Henkel, C Braatz, JA Greenhill, LJ Wilson, AS AF Henkel, C Braatz, JA Greenhill, LJ Wilson, AS TI Discovery of water vapor megamaser emission from Mrk 1419 (NGC 2960): An analogue of NGC 4258? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : individual : Mrk 1419 (NGC 2960, UGC 05159); galaxies : ISM; galaxies : nuclei masers; radio lines : galaxies ID H2O MASER EMISSION; GALAXY NGC4258; SEYFERT-GALAXIES; BLACK-HOLE; DISK; NGC-4258; NUCLEUS; DISTANCE AB Water vapor emission at 22 GHz is reported from the nucleus of the LINER galaxy Mrk 1419 (NGC 2960). Single-dish spectra of the maser source show properties that are similar to those seen in NGC 4258, namely (1) a cluster of systemic (V similar to V-sys) H2O features, (2) two additional H2O clusters, one red- and one blue-shifted with respect to V-sys, (3) a likely acceleration of the systemic features (dV/dt = 2.8 +/- 0.5 km s(-1) yr(-1)), and (4) no detectable velocity drifts (<1 km s(-1) yr(-1)) in the red- and blue-shifted features. Interpreting the data in terms of the paradigm established for NGC 4258, i.e. assuming the presence of an edge-on Keplerian circumnuclear annulus with the systemic emission arising from the near side of its inner edge, the following parameters are derived: V-rot = 330-600 km s(-1), R &SIM; 0.13-0.43 pc, binding mass M &SIM; 10(7) M., and mass density inside the disk ρ &SIM; 10(9) M. pc(-3). With the galaxy being approximately ten times farther away than NGC 4258, a comparison of linear and angular scales (the latter via Very Long Baseline Interferometry) may provide an accurate geometric distance to Mrk 1419 that could be used to calibrate the cosmic distance scale. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Natl Radio Astron Observ, Green Bank, WV 24944 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Henkel, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. NR 16 TC 29 Z9 29 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 NOV PY 2002 VL 394 IS 2 BP L23 EP L26 DI 10.1051/0004-6361:20021297 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 603TD UT WOS:000178575300001 ER PT J AU Furlanetto, SR Loeb, A AF Furlanetto, SR Loeb, A TI The 21 centimeter forest: Radio absorption spectra as probes of minihalos before reionization SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : active; intergalactic medium; large-scale structure of universe; radio lines : general ID HIGH-REDSHIFT; COSMOLOGICAL REIONIZATION; INTERGALACTIC MEDIUM; 21-CM LINE; H-I; GALAXY; ABSORBERS; UNIVERSE; HYDROGEN; PROFILE AB We study the absorption along lines of sight toward high-z radio sources caused by the 21 cm transition of neutral hydrogen in the intergalactic medium (IGM) before reionization. Using semianalytic methods, we compute the number density of observable features caused by both "minihalos" ( bound objects that are unable to cool efficiently because of their small virial temperatures) and protogalactic disks. We show that both sets of features should be observable by the next generation of low-frequency radio telescopes, including the Low Frequency Array and the Square Kilometer Array, provided that sufficiently bright background sources exist. The statistics of minihalo absorption features seen along lines of sight to radio-loud quasars offer a way to measure the evolution of the radiation background and the IGM temperature with cosmic time. Intersections with disks are much less common but cause significantly deeper absorption features that would be visible in the spectra of both radio-loud quasars and gamma-ray bursts (GRBs). The absorption feature caused by H I in the host galaxy of a GRB should be observable, offering a route to determine spectroscopically the burst redshift. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 41 TC 81 Z9 81 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2002 VL 579 IS 1 BP 1 EP 9 DI 10.1086/342757 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607XZ UT WOS:000178817200001 ER PT J AU White, M Hernquist, L Springel, V AF White, M Hernquist, L Springel, V TI Simulating the Sunyaev-Zeldovich effect(s): Including radiative cooling and energy injection by galactic winds SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : theory; galaxies : clusters : general; large-scale structure of universe; methods : numerical ID COLD DARK-MATTER; HYDRODYNAMICAL SIMULATIONS; POWER SPECTRUM; UNIVERSE AB We present results on the thermal and kinetic Sunyaev-Zeldovich (SZ) effects from a sequence of high-resolution hydrodynamic simulations of structure formation, including cooling, feedback, and metal injection. These simulations represent a self-consistent thermal model that incorporates ideas from the "preheating " scenario while preserving good agreement with the low-density intergalactic medium at z similar to 3 probed by the Lyalpha forest. Four simulations were performed, at two different resolutions with and without radiative effects and star formation. The long-wavelength modes in each simulation were the same, so we can compare the results on an object-by-object basis. We demonstrate that our simulations are converged to the subarcminute level. The effect of the additional physics is to suppress the mean Comptonization parameter by 20% and to suppress the angular power spectrum of fluctuations by just under a factor of 2 in this model, while leaving the source counts and properties relatively unchanged. We quantify how non-Gaussianity in the SZ maps increases the sample variance over the standard result for Gaussian fluctuations. We identify a large scatter in the Y-M relation that will be important in searches for clusters using the SZ effect(s). C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85748 Garching, Germany. RP White, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 NR 37 TC 127 Z9 127 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 1 PY 2002 VL 579 IS 1 BP 16 EP 22 DI 10.1086/342756 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607XZ UT WOS:000178817200003 ER PT J AU Cagnoni, I Elvis, M Kim, DW Nicastro, F Celotti, A AF Cagnoni, I Elvis, M Kim, DW Nicastro, F Celotti, A TI ROSAT blank field sources. I. Sample selection and archival data SO ASTROPHYSICAL JOURNAL LA English DT Review DE BL Lacertae objects : general; galaxies : active; galaxies : nuclei; galaxies : Seyfert; X-rays : galaxies; X-rays : galaxies : clusters ID X-RAY SOURCES; ISOLATED NEUTRON-STAR; ALL-SKY SURVEY; MEDIUM SENSITIVITY SURVEY; LUMINOUS GALAXY CLUSTER; BL LACERTAE OBJECTS; T TAURI STARS; SPIRAL GALAXIES; SOURCE CATALOG; BLACK-HOLES AB We have identified a population of "blank field sources" (or "blanks") among the ROSAT bright unidentified X-ray sources with faint optical counterparts. The extreme X-ray over optical flux ratio of blanks is not compatible with the main classes of X-ray emitters except for extreme BL Lacertae objects. From the analysis of ROSAT archival data we found no indication of variability, and evidence for only three sources, out of 16, needing absorption in excess of the Galactic value. We also found evidence for an extended nature for only one of the five blanks with a serendipitous HRI detection; this source (1WGA J1226.9+3332) was confirmed as a z = 0.89 cluster of galaxies. Palomar images reveal the presence of a red (O-E greater than or equal to 2) counterpart in the X-ray error circle for six blanks. The identification process brought to the discovery of another high-z cluster of galaxies, one (possibly extreme) BL Lac, two ultraluminous X-ray sources in nearby galaxies, and two apparently normal type 1 active galactic nuclei (AGNs). These AGNs, together with four more AGN-like objects, seem to form a well-defined group: they present unabsorbed X-ray spectra but red Palomar counterparts. We discuss the possible explanations for the discrepancy between the X-ray and optical data, among which are a suppressed big blue bump emission, an extreme dust-to-gas ratio (similar to40-60 times the Galactic ratio), a high-redshift (z greater than or equal to 3.5) quasar nature, an atypical dust grain size distribution, and a dusty warm absorber. These AGN-like blanks seem to be the bright ( and easier to study) analogs of the sources that are found in deep Chandra observations. Three more blanks still have an unknown nature. C1 Univ Insubria, Dipartimento Sci, I-22100 Como, Italy. SISSA, I-34014 Trieste, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cagnoni, I (reprint author), Univ Insubria, Dipartimento Sci, Via Valleggio 11, I-22100 Como, Italy. EM ilaria.cagnoni@uninsubria.it OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 120 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2002 VL 579 IS 1 BP 148 EP 168 DI 10.1086/342678 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607XZ UT WOS:000178817200012 ER PT J AU Welty, DE Jenkins, EB Raymond, JC Mallouris, C York, DG AF Welty, DE Jenkins, EB Raymond, JC Mallouris, C York, DG TI Intermediate- and high-velocity ionized gas toward zeta orionis SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : general; stars : individual (zeta Orionis, tau Canis majoris); ultraviolet : ISM ID INTERSTELLAR ABSORPTION-LINES; VELA SUPERNOVA REMNANT; INTER-STELLAR MEDIUM; X-RAY ENHANCEMENT; SHOCK-WAVES; COPERNICUS-SATELLITE; ELEMENTAL ABUNDANCE; GRAIN DESTRUCTION; EXPANDING SHELL; H-I AB We combine near-UV spectra obtained with the Hubble Space Telescope GHRS echelle with far-UV spectra obtained with the Interstellar Medium Absorption Pro le Spectrograph and Copernicus to study the abundances and physical conditions in the predominantly ionized gas seen at high velocity ( 105 km s(-1) less than or similar to v(circle dot) less than or similar to 65 km s(-1)) and at intermediate velocity (-60 km s(-1) less than or similar to v(circle dot) less than or similar to -10 km s(-1)) along the line of sight to the star zeta Ori. We have high-resolution (FWHM similar to 3.3-4.5 km s(-1)) and/or high signal-to-noise ratio spectra for at least two significant ions of C, N, Al, Si, S, and Fe enabling accurate estimates for both the total N (H II) and the elemental depletions. C, N, and S have essentially solar relative abundances; Al, Si, and Fe appear to be depleted by about 0.8, 0.3-0.4, and 0.95 dex, respectively, relative to C, N, and S. While various ion ratios would be consistent with collisional ionization equilibrium (CIE) at temperatures of 25,000-80,000 K, the widths of individual high-velocity absorption components indicate that T similar to 9000 +/- 2000 K-so the gas is not in CIE. Analysis of the C II ne-structure excitation equilibrium, at that temperature, yields estimates for the densities (n(e) similar to n(H) similar to 0.1-0.2 cm(-3)), thermal pressures (2n(H)T similar to 2000-4000 cm(-3) K), and thicknesses (0.5-2.7 pc) characterizing the individual clouds. We compare the abundances and physical properties derived for these clouds with those found for gas at similar velocities toward 23 Ori and tau CMa and also with several different models for shocked gas. While the shock models can reproduce some features of the observed line profiles and some of the observed ion ratios, there are also significant differences between the models and the data. The measured depletions suggest that roughly 10% of the Al, Si, and Fe originally locked in dust in the preshock medium may have been returned to the gas phase, consistent with recent predictions for the destruction of silicate dust in a 100 km s(-1) shock. The observed near-solar gas-phase abundance of carbon, however, appears to be inconsistent with the predicted longer timescales for the destruction of graphite grains. C1 Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Welty, DE (reprint author), Univ Chicago, Ctr Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. RI Jenkins, Edward/P-5684-2014 OI Jenkins, Edward/0000-0003-1892-4423 NR 78 TC 23 Z9 23 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 NOV 1 PY 2002 VL 579 IS 1 BP 304 EP 326 DI 10.1086/342755 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607XZ UT WOS:000178817200025 ER PT J AU Mennesson, B Perrin, G Chagnon, G du Foresto, VC Ridgway, S Merand, A Salome, P Borde, P Cotton, W Morel, S Kervella, P Traub, W Lacasse, M AF Mennesson, B Perrin, G Chagnon, G du Foresto, VC Ridgway, S Merand, A Salome, P Borde, P Cotton, W Morel, S Kervella, P Traub, W Lacasse, M TI Evidence for very extended gaseous layers around O-rich Mira variables and M giants SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; instrumentation : interferometers; stars : atmospheres; stars : variables : other; techniques : interferometric ID MASS-LOSS RATES; ANGULAR DIAMETER; R-LEONIS; INTERFEROMETRIC OBSERVATIONS; DIFFRACTION LIMIT; 11 MICRONS; COOL STARS; CETI; SPECTROSCOPY; ATMOSPHERE AB Nine bright O-rich Mira stars and five semiregular variable cool M giants have been observed with the Infrared and Optical Telescope Array (IOTA) interferometer in both K' (similar to2.15 mum) and L' (similar to3.8 mum) broadband filters, in most cases at very close variability phases. All of the sample Mira stars and four of the semiregular M giants show strong increases, from similar or equal to20% to similar or equal to100%, in measured uniform-disk (UD) diameters between the K' and L' bands. (A selection of hotter M stars does not show such a large increase.) There is no evidence that K' and L/ broadband visibility measurements should be dominated by strong molecular bands, and cool expanding dust shells already detected around some of these objects are also found to be poor candidates for producing these large apparent diameter increases. Therefore, we propose that this must be a continuum or pseudocontinuum opacity effect. Such an apparent enlargement can be reproduced using a simple two-component model consisting of a warm ( 1500 2000 K), extended (up to similar or equal to3 stellar radii), optically thin (tau similar to 0.5) layer located above the classical photosphere. The Planck weighting of the continuum emission from the two layers will suffice to make the L' UD diameter appear larger than the K' UD diameter. This two-layer scenario could also explain the observed variation of Mira UD diameters versus infrared wavelength outside of strong absorption bands as already measured inside the H, K, L, and N atmospheric windows. This interpretation is consistent with the extended molecular gas layers (H2O, CO, etc.) inferred around some of these objects from previous IOTA K'-band interferometric observations obtained with the Fiber Linked Unit for Optical Recombination (FLUOR) and from Infrared Space Observatory and high-resolution ground-based FTS infrared spectra. The two-component model has immediate implications. For example, the Mira photosphere diameters are smaller than previously recognized this certainly implies higher effective temperatures, and it may favor fundamental mode pulsation. Also, the UD model fails generally to represent the brightness distribution and has very limited applicability for Mira stars. The presence of a very extended gas layer extending up to 3 stellar radii seems now well established on a fair sample of asymptotic giant branch stars ranging from late-type giants to long-period variables, with some probable impact on stellar model atmospheres and mass-loss mechanisms. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. European So Observ, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mennesson, B (reprint author), CALTECH, Jet Prop Lab, MS 306-388,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 40 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 NOV 1 PY 2002 VL 579 IS 1 BP 446 EP 454 DI 10.1086/342671 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607XZ UT WOS:000178817200037 ER PT J AU Camilo, F Manchester, RN Gaensler, BM Lorimer, DR AF Camilo, F Manchester, RN Gaensler, BM Lorimer, DR TI Heartbeat of the Mouse: A young radio pulsar associated with the axisymmetric nebula G359.23-0.82 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G359.23-0.82); pulsars : individual (PSR J1747-2958) ID GALACTIC-CENTER; B1757-24; SEARCH AB We report the discovery of PSR J1747-2958, a radio pulsar with period P = 98 ms and dispersion measure DM = 101 cm(-3) pc, in a deep observation with the Parkes telescope of the axially symmetric "Mouse" radio nebula (G359.23-0.82). Timing measurements of the newly discovered pulsar reveal a characteristic age P/2(P) over dot kyr and spin-down luminosity (E) over dot = 2.5 x 10(36) ergs s(-1). The pulsar (timing) position is consistent with that of the Mouse's "head." The distance derived from the DM (approximate to2 kpc) is consistent with the Mouse's distance limit from H I absorption (<5.5 kpc). Also, the X-ray energetics of the Mouse are compatible with being powered by the pulsar. Therefore, we argue that PSR J1747-2958, moving at supersonic speed through the local interstellar medium, powers this unusual nonthermal nebula. The pulsar is a weak radio source, with a period-averaged flux density at 1374 MHz of 0.25 mJy and a luminosity of &SIM;1 mJy kpc(2). C1 Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 23 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 NOV 1 PY 2002 VL 579 IS 1 BP L25 EP L28 DI 10.1086/344832 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607YB UT WOS:000178817400007 ER PT J AU Warren, HP Winebarger, AR Hamilton, PS AF Warren, HP Winebarger, AR Hamilton, PS TI Hydrodynamic modeling of active region loops SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona ID SOLAR CORONAL LOOPS; TRANSITION REGION; TEMPORAL VARIATIONS; FLARING LOOPS; DYNAMICS; TEMPERATURE; PLASMAS; TRACE AB Recent observations with the Transition Region and Coronal Explorer (TRACE) have shown that many apparently cool (T-e similar to 1-1.5 MK) active region loops are much brighter and have flatter temperature profiles than static loop models predict. Observations also indicate that these loops can persist much longer than a characteristic cooling time. Using time-dependent hydrodynamic simulations, we explore the possibility that these active region loops are actually a collection of small-scale filaments that have been impulsively heated and are cooling through the TRACE 171 Angstrom (Fe IX/X) and 195 Angstrom (Fe XII) bandpasses. We find that an ensemble of independently heated filaments can be significantly brighter than a static uniformly heated loop and would have a flat filter ratio temperature when observed with TRACE. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. Computat Phys Inc, Springfield, VA 22151 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM hwarren@nrl.navy.mil RI Hamilton, Paul/E-7891-2015 OI Hamilton, Paul/0000-0001-6080-632X NR 21 TC 89 Z9 90 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2002 VL 579 IS 1 BP L41 EP L44 DI 10.1086/344921 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607YB UT WOS:000178817400011 ER PT J AU Wood, WF Weldon, PJ AF Wood, WF Weldon, PJ TI The scent of the reticulated giraffe (Giraffa camelopardalis reticulata) SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Article DE Giraffa camelopardalis reticulata; giraffe; scent; anti-ectoparasitic agents; antimicrobial activity ID FATTY-ACIDS; ANTIMICROBIAL ACTIVITY; ESSENTIAL OILS; COMPONENTS; AGENTS AB The giraffe (Giraffa camelopardalis) emits a scent that can be detected by humans over considerable distances. Dichloromethane extracts of hair samples from adult male and female reticulated giraffes (G. c. reticulata) were analysed by gas chromatography-mass spectrometry. Two highly odoriferous compounds, indole and 3-methylindole, identified in these extracts appear to be primarily responsible for the giraffe's strong scent. Other major compounds identified were octane, benzaldehyde, heptanal, octanal, nonanal, p-cresol, tetradecanoic acid, hexadecanoic acid, and 3,5-androstadien-17-one; the last compound has not previously been identified from a natural source. These compounds may deter microorganisms or ectoparasitic arthropods. Most of these compounds are known to possess bacteriostatic or fungistatic properties against mammalian skin pathogens or other microorganisms. The levels of p-cresol in giraffe hair are sufficient to repel some ticks. (C) 2002 Elsevier Science Ltd. All rights reserved. C1 Humboldt State Univ, Dept Chem, Arcata, CA 95521 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Wood, WF (reprint author), Humboldt State Univ, Dept Chem, Arcata, CA 95521 USA. OI Wood, William/0000-0002-2991-0054 NR 20 TC 15 Z9 16 U1 1 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0305-1978 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD NOV PY 2002 VL 30 IS 10 BP 913 EP 917 AR PII S0305-1978(02)00037-6 DI 10.1016/S0305-1978(02)00037-6 PG 5 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 607UF UT WOS:000178808600002 ER PT J AU Waycott, M Freshwater, DW York, RA Calladine, A Kenworthy, WJ AF Waycott, M Freshwater, DW York, RA Calladine, A Kenworthy, WJ TI Evolutionary trends in the seagrass genus Halophila (thouars): Insights from molecular phylogeny SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT 4th International Seagrass Biology Workshop CY SEP 26-OCT 02, 2000 CL CORSICA, FRANCE SP Univ Corsica, Coastal Ecosyst Team, Ischia Lab, Staz Zool Anton Dohrn ID ANGIOSPERM PHYLOGENY; HYDROCHARITACEAE; BIOGEOGRAPHY; SEQUENCES; REGION; RBCL AB Relationships among members of the seagrass genus Halophila (Hydrocharitaceae) were investigated using phylogenetic analysis of the internal transcribed spacer (ITS) region of the nuclear ribosomal DNA. The final aligned ITS sequence data set of 705 base pairs from 36 samples in 11z currently recognised species included 18.7% parsimony informative characters. Phylogenetic analysis yielded two most parsimonious trees with strong support for six groups within the genus. Evolutionary trends in Halophila appear to be toward a more reduced simple phyllotaxy. In addition, this study indicates that long distance 'jump' dispersal between major ocean systems may have occurred at least in the globally distributed H. decipiens. Results of ITS analyses also indicate that the widespread pacific species H. ovalis is paraphyletic and may contain cryptic species. Likewise, the geographically restricted species H. hawaiiana and H. johnsonii could not be distinguished from H. ovalis with these data and warrant further investigation. C1 James Cook Univ N Queensland, Sch Trop Biol, Townsville, Qld 4811, Australia. James Cook Univ N Queensland, Sch Trop Environm Studies Geog & Trop Biol, Townsville, Qld 4811, Australia. Smithsonian Trop Res Inst, Balboa 2072, Panama. Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28409 USA. NOAA, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC 28516 USA. RP Waycott, M (reprint author), James Cook Univ N Queensland, Sch Trop Biol, Townsville, Qld 4811, Australia. NR 26 TC 33 Z9 34 U1 0 U2 12 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 NOV PY 2002 VL 71 IS 3 BP 1299 EP 1308 PG 10 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 696BM UT WOS:000183865300016 ER PT J AU Smith, DR Dapoto, G Giganti, H AF Smith, DR Dapoto, G Giganti, H TI A new species of Periclista (Hymenoptera : Tenthredinidae) associated with Nothofagus (Fagaceae) in Argentina and Chile SO ENTOMOLOGICAL NEWS LA English DT Article AB Periclista dapotoae, Smith, n. sp., is described from Argentina and Chile and separated from the described species of Periclista from South America. It was reared from Nothofagus antarctica (Fagaceae). Periclista leucoma is a new combination. C1 ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. Univ Nacl Comahue, Dept Biol Aplicada, RA-8303 Cinco Saltos, RN, Argentina. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. NR 5 TC 1 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 NOV-DEC PY 2002 VL 113 IS 5 BP 328 EP 331 PG 4 WC Entomology SC Entomology GA 666NZ UT WOS:000182184500010 ER PT J AU Ibanez, R Condit, R Angehr, G Aguilar, S Garcia, T Martinez, R Sanjur, A Stallard, R Wright, SJ Rand, AS Heckadon, S AF Ibanez, R Condit, R Angehr, G Aguilar, S Garcia, T Martinez, R Sanjur, A Stallard, R Wright, SJ Rand, AS Heckadon, S TI An ecosystem report on the Panama Canal: Monitoring the status of the forest communities and the watershed SO ENVIRONMENTAL MONITORING AND ASSESSMENT LA English DT Article DE environmental assessment; forest communities; human population; hydrological aspects; Panama Canal; vertebrate populations; watershed monitoring ID TROPICAL FOREST; POPULATION DECLINES; SEED DISPERSAL; PUERTO-RICO; DIVERSITY; TREES; CONSERVATION; BIODIVERSITY; LANDSLIDES; MORTALITY AB In 1996, the Smithsonian Tropical Research Institute and the Republic of Panama's Environmental Authority, with support from the United States Agency for International Development, undertook a comprehensive program to monitor the ecosystem of the Panama Canal watershed. The goals were to establish baseline indicators for the integrity of forest communities and rivers. Based on satellite image classification and ground surveys, the 2790 km(2) watershed had 1570 km(2) of forest in 1997, 1080 km(2) of which was in national parks and nature monuments. Most of the 490 km(2) of forest not currently in protected areas lies along the west bank of the Canal, and its management status after the year 2000 turnover of the Canal from the U.S. to Panama remains uncertain. In forest plots designed to monitor forest diversity and change, a total of 963 woody plant species were identified and mapped. We estimate there are a total of 850-1000 woody species in forests of the Canal corridor. Forests of the wetter upper reaches of the watershed are distinct in species composition from the Canal corridor, and have considerably higher diversity and many unknown species. These remote areas are extensively forested, poorly explored, and harbor an estimated 1400-2200 woody species. Vertebrate monitoring programs were also initiated, focusing on species threatened by hunting and forest fragmentation. Large mammals are heavily hunted in most forests of Canal corridor, and there was clear evidence that mammal density is greatly reduced in hunted areas and that this affects seed predation and dispersal. The human population of the watershed was 113 000 in 1990, and grew by nearly 4% per year from 1980 to 1990. Much of this growth was in a small region of the watershed on the outskirts of Panama City, but even rural areas, including villages near and within national parks, grew by 2% per year. There is no sewage treatment in the watershed, and many towns have no trash collection, thus streams near large towns are heavily polluted. Analyses of sediment loads in rivers throughout the watershed did not indicate that erosion has been increasing as a result of deforestation, rather, erosion seems to be driven largely by total rainfall and heavy rainfall events that cause landslides. Still, models suggest that large-scale deforestation would increase landslide frequency, and failure to detect increases in erosion could be due to the gradual deforestation rate and the short time period over which data are available. A study of runoff showed deforestation increased the amount of water from rainfall that passed directly into streams. As a result, dry season flow was reduced in a deforested catchment relative to a forested one. Currently, the Panama Canal watershed has extensive forest areas and streams relatively unaffected by humans. But impacts of hunting and pollution near towns are clear, and the burgeoning population will exacerbate these impacts in the next few decades. Changes in policies regarding forest protection and pollution control are necessary. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Condit, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, Miami, FL 34002 USA. EM ctfs@tivoli.si.edu RI Wright, Stuart/M-3311-2013; Stallard, Robert/H-2649-2013 OI Wright, Stuart/0000-0003-4260-5676; Stallard, Robert/0000-0001-8209-7608 NR 59 TC 37 Z9 40 U1 11 U2 36 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-6369 J9 ENVIRON MONIT ASSESS JI Environ. Monit. Assess. PD NOV PY 2002 VL 80 IS 1 BP 65 EP 95 DI 10.1023/A:1020378926399 PG 31 WC Environmental Sciences SC Environmental Sciences & Ecology GA 595FH UT WOS:000178097200005 PM 12437064 ER PT J AU Collin, R de Maintenon, M AF Collin, R de Maintenon, M TI Integrative approaches to biogeography: Patterns and processes on land and in the sea SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol ID HAPLOTYPES AB At the 2002 SICB meeting in Anaheim, we brought together some of the leaders in terrestrial and marine phylogeography for a day-long symposium. This symposium combined presentations from ten scientists whose question-driven research focuses on testing hypotheses about patterns and processes in biogeography in both vertebrate and invertebrate animals and including marine, terrestrial, and freshwater systems. The papers gathered here cover the breadth of the presentations. By explicitly seeking to combine marine and terrestrial workers into a single symposium we hoped that the different patterns and processes that predominate in major biomes and the different assumptions made by the workers in those areas would be highlighted. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. Univ Hawaii, Dept Marine Sci, Hilo, HI 96720 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Collin, Rachel/G-2001-2010 NR 14 TC 2 Z9 2 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 NOV PY 2002 VL 42 IS 5 BP 911 EP 912 DI 10.1093/icb/42.5.911 PG 2 WC Zoology SC Zoology GA 661AV UT WOS:000181869800001 PM 21680370 ER PT J AU Williams, ST Jara, J Gomez, E Knowlton, N AF Williams, ST Jara, J Gomez, E Knowlton, N TI The marine Indo-West Pacific break: Contrasting the resolving power of mitochondrial and nuclear genes SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 02-07, 2002 CL ANAHEIM, CALIFORNIA SP Soc Integrat & Comparat Biol ID GLOBAL POPULATION-STRUCTURE; STARFISH LINCKIA-LAEVIGATA; SOUTHEASTERN INDIAN-OCEAN; HIGH-DISPERSAL STARFISH; SHRIMP GENUS ALPHEUS; TUNA THUNNUS-OBESUS; PENAEUS-MONODON; DNA VARIATION; CRASSOSTREA-VIRGINICA; MOLECULAR PHYLOGENY AB Simultaneous studies of both nuclear and mitochondrial markers were undertaken in two widespread Indo-West Pacific (IWP) marine invertebrates to compare and contrast the ability of these markers to resolve genetic structure. In particular, we were interested in the resolution of a genetic break between the Indian and Pacific Oceans due to historical isolation. Sequence variation from the nuclear gene encoding myosin heavy chain (MyHC) and the mitochondrial gene cytochrome oxidase I (COI) were examined for the snapping shrimp Alpheus lottini from wide-ranging populations throughout the Indian and Pacific Oceans. A previously identified genetic break between oceans based on COI sequences appears to have been an artifact caused by the inadvertent inclusion of pseudogene sequences; our new COI data provide evidence only of a break between IWP and East Pacific populations. Distribution of a single nucleotide polymorphism in MyHC, on the other hand, shows evidence of a cline between Indian and Pacific Oceans. New allozyme and mtDNA sequence data were also obtained for the starfish Linckia laevigata. Allozyme data show a clear genetic break between Indian Ocean populations and Pacific (including western Australian) populations, whereas the distribution of mtDNA haplotypes shows a region of overlap in the central IWP. Comparisons of our data for both Alpheus and Linckia with data from other population genetic studies in the IWP suggest that nuclear markers (allozymes, sequence data and morphological characters) may in some instances reveal historical patterns of genetic population structure whereas mtDNA variation better reflects present day patterns of gene flow. C1 Nat Hist Museum, Dept Zool, London SW7 5BD, England. Smithsonian Trop Res Inst, Naos Marine Lab, Panama City, Panama. Univ Calif San Diego, Scripps Inst Oceanog, Marine Biol Res Div 0202, La Jolla, CA 92093 USA. RP Williams, ST (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England. RI Williams, Suzanne/A-9604-2008 OI Williams, Suzanne/0000-0003-2995-5823 NR 76 TC 53 Z9 55 U1 0 U2 16 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 NOV PY 2002 VL 42 IS 5 BP 941 EP 952 DI 10.1093/icb/42.5.941 PG 12 WC Zoology SC Zoology GA 661AV UT WOS:000181869800005 PM 21680374 ER PT J AU Bergin, EA AF Bergin, EA TI Molecules and the process of star formation SO JOURNAL DE PHYSIQUE IV LA English DT Article; Proceedings Paper CT European Research Course on Atmospheres CY 2002 CL GRENOBLE, FRANCE ID DENSE INTERSTELLAR CLOUDS; GRAIN-SURFACE-CHEMISTRY; YOUNG STELLAR OBJECTS; FORMING REGIONS; DARK CLOUDS; CHEMICAL EVOLUTION; PROTOSTELLAR CORES; ORGANIC-MOLECULES; WATER ICE; IONIZATION FRACTION AB Stars are born inside clouds of gas and dust which are predominantly molecular in composition. The chemistry and physics of these molecules are important contributors to the overall evolution of the parent clouds and on the formation of the stellar systems. We review the methods and techniques through which molecules are used to probe the process of star formation. We also detail our current understanding of the chemical processes active in molecular clouds preceding and during the initial stages of stellar birth. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02137 USA. RP Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02137 USA. NR 144 TC 2 Z9 2 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1155-4339 J9 J PHYS IV JI J. Phys. IV PD NOV PY 2002 VL 12 IS PR10 BP 307 EP 325 DI 10.1051/jp4:20020466 PG 19 WC Physics, Multidisciplinary SC Physics GA 639MQ UT WOS:000180633400021 ER PT J AU Kornicker, LS AF Kornicker, LS TI Comparative morphology of the fifth limb (second maxilla) of myodocopid Ostracoda SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB The anatomy of the fifth limb of Isocypridina quatuorsetae Kornicker, 1975, is described and illustrated in detail, and it is concluded that the appendage is biramous. The interpretation of the morphology of the fifth limb of I.quatuorsetae is then extrapolated to the fifth limbs of selected members of the families Rutidermatidae, Sarsiellidae, and Cylindroleberididae, which are described and illustrated, and it is concluded that they ire also biramous. Members of the Philomedidae have fifth limbs similar to those of the Rutidermatidae and are also biramous. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 35 TC 10 Z9 10 U1 1 U2 3 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD NOV PY 2002 VL 22 IS 4 BP 798 EP 818 DI 10.1651/0278-0372(2002)022[0798:CMOTFL]2.0.CO;2 PG 21 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 613JH UT WOS:000179128800012 ER PT J AU Gunderson, JH John, SA Boman, WC Coats, DW AF Gunderson, JH John, SA Boman, WC Coats, DW TI Multiple strains of the parasitic dinoflagellate Amoebophrya exist in Chesapeake Bay SO JOURNAL OF EUKARYOTIC MICROBIOLOGY LA English DT Article DE alveolate; biological control; blooms; host specificity; parasite; PCR; red tides; rRNA; small subunit; Syndiniophyceae ID SUBUNIT RIBOSOMAL-RNA; GYMNODINIUM-SANGUINEUM; CERATII; PHYLOGENY; SEQUENCES AB Small subunit rRNA sequences were amplified from Amoebophrya strains infecting Karlodinium micrum, Gymnodinium instriatum and an unidentified Scrippsiella species in Chesapeake Bay. The alignable parts of the sequences differed from each other and from the previously reported rRNA sequence of the Amoebophrya strain infecting Akashiwo sanguinea in Chesapeake Bay by 4 to 10%. This is a greater degree of difference than sometimes found between sequences from separate genera of free-living dinoflagellates. These sequence differences indicate that the Amoebophrya strains parasitizing dinoflagellates in Chesapeake Bay do not all belong to the same species. In spite of their relative dissimilarity, the sequences do group together into a single clade with high bootstrap support in phylogenetic trees constructed from the sequences. C1 Tennessee Technol Univ, Dept Biol, Cookeville, TN 38505 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Gunderson, JH (reprint author), Tennessee Technol Univ, Dept Biol, Cookeville, TN 38505 USA. EM jgunderson@tntech.edu NR 22 TC 27 Z9 28 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1066-5234 EI 1550-7408 J9 J EUKARYOT MICROBIOL JI J. Eukaryot. Microbiol. PD NOV-DEC PY 2002 VL 49 IS 6 BP 469 EP 474 DI 10.1111/j.1550-7408.2002.tb00230.x PG 6 WC Microbiology SC Microbiology GA 626GK UT WOS:000179863300007 PM 12503682 ER PT J AU Tyree, MT Vargas, G Engelbrecht, BMJ Kursar, TA AF Tyree, MT Vargas, G Engelbrecht, BMJ Kursar, TA TI Drought until death do us part: a case study of the desiccation-tolerance of a tropical moist forest seedling-tree, Licania platypus (Hemsl.) Fritsch SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Article DE desiccation tolerance; drought resistance; hydraulic conductance; Licania platypus; water potential ID HYDRAULIC CONDUCTANCE; ROOT; EMBOLISM AB Studies of the desiccation tolerance of 15-month-old Licania platypus (Hemsl.) Fritsch seedlings were performed on potted plants. Pots were watered to field capacity and then dehydrated for 23-46 d to reach various visible wilting stages from slightly-wilted to dead. Root hydraulic conductance, k(r), was measured with a high-pressure flow meter and whole-stem hydraulic conductance, k(ws), was measured by a vacuum chamber method. Leaf punches were harvested for measurement of leaf water potential by a thermocouple psychrometer and for measurement of fresh- and dry-weight. L. platypus was surprisingly desiccation-tolerant, suggesting that most species of central Panama may be well adapted to the seasonality of rainfall in the region. The slightly-wilted stage corresponded to leaf water potentials and relative water contents of -2.7 MPa and 0.85, respectively, but plants did not die until these values fell to -7.5 MPa and 0.14, respectively. As desiccation proceeded k(r) and k(ws) declined relative to irrigated controls, but k(ws) was more sensitive to desiccation than k(r). Values of k(ws) declined by 70-85%. in slightly-wilted to dead plants, respectively. By comparison, k(r) showed no significant change in slightly-wilted plants and fell by about 50% in plants having severely-wilted to dead shoots. C1 USDA, Forest Serv, Burlington, VT 05402 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Tyree, MT (reprint author), USDA, Forest Serv, POB 968, Burlington, VT 05402 USA. RI Engelbrecht, Bettina/E-9914-2012 NR 12 TC 53 Z9 57 U1 1 U2 25 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-0957 J9 J EXP BOT JI J. Exp. Bot. PD NOV PY 2002 VL 53 IS 378 BP 2239 EP 2247 DI 10.1093/jxb/erf078 PG 9 WC Plant Sciences SC Plant Sciences GA 610JT UT WOS:000178957500013 PM 12379791 ER PT J AU Craddock, RA Howard, AD AF Craddock, RA Howard, AD TI The case for rainfall on a warm, wet early Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review DE Mars; Martian; erosion; climate; hydrology; fluvial ID ORBITER LASER ALTIMETER; SMALL MARTIAN VALLEYS; HILLSLOPE EVOLUTION MODEL; EARTHS EARLY ATMOSPHERE; PIPING SAPPING EROSION; CHANNEL NETWORK GROWTH; CARBON-DIOXIDE CLOUDS; GLOBAL SURVEYOR; FLUVIAL VALLEYS; SUN PARADOX AB [1] Valley networks provide compelling evidence that past geologic processes on Mars were different than those seen today. The generally accepted paradigm is that these features formed from groundwater circulation, which may have been driven by differential heating induced by magmatic intrusions, impact melt, or a higher primordial heat flux. Although such mechanisms may not require climatic conditions any different than today's, they fail to explain the large amount of recharge necessary for maintaining valley network systems, the spatial patterns of erosion, or how water became initially situated in the Martian regolith. In addition, there are no clear surface manifestations of any geothermal systems (e. g., mineral deposits or phreatic explosion craters). Finally, these models do not explain the style and amount of crater degradation. To the contrary, analyses of degraded crater morphometry indicate modification occurred from creep induced by rain splash combined with surface runoff and erosion; the former process appears to have continued late into Martian history. A critical analysis of the morphology and drainage density of valley networks based on Mars Global Surveyor data shows that these features are, in fact, entirely consistent with rainfall and surface runoff. The necessity for a cold, dry early Mars has been predicated on debatable astronomical and climatic arguments. A warm, wet early climate capable of supporting rainfall and surface runoff is the most plausible scenario for explaining the entire suite of geologic features in the Martian cratered highlands. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. RP Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Room 3762,MRC-315, Washington, DC 20560 USA. EM craddock@nasm.si.edu RI Craddock, Robert/B-3884-2013; OI Howard, Alan/0000-0002-5423-1600 NR 238 TC 240 Z9 240 U1 7 U2 52 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV PY 2002 VL 107 IS E11 AR 5111 DI 10.1029/2001JE001505 PG 36 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 639RQ UT WOS:000180643400023 ER PT J AU Maria, A Carey, S AF Maria, A Carey, S TI Using fractal analysis to quantitatively characterize the shapes of volcanic particles SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE fractal analysis; morphology; volcanic particles; magma fragmentation ID SCANNING ELECTRON-MICROSCOPY; TRANSPORTATION MECHANISMS; SURFACE-FEATURES; DIMENSION; FRAGMENTATION; MORPHOLOGY; DEPOSITS; PATTERNS; LIPARI; IMAGES AB [1] The shapes of volcanic particles reflect numerous eruptive parameters (e. g., magma viscosity, volatile content, and degree of interaction with water) and are useful for understanding fragmentation and transport processes associated with volcanic eruptions. However, quantitative analysis of volcanic particle shapes has proven difficult because of their morphological complexity and variability. Here a newly developed procedure for shape analysis based on fractal geometry is described and tested. Although volcanic particle shapes are not truly fractal, their complexity can be effectively characterized in terms of fractal values (pseudofractal dimensions) reflecting morphological invariance over discrete ranges of scale. Using fractal data produced by dilation of a particle's two-dimensional boundary, a spectrum of fractal dimensions is calculated for each particle by taking the first derivative of the dilation data. Compared with fractal methods that express shape in terms of only one or two fractal dimensions, typically derived from the slope of data on a Richardson plot, this technique results in better discrimination between samples. In addition, use of multiple fractal values allows incorporation of multivariate statistical analysis, further strengthening the differentiating power of the technique. This fractal spectrum technique yields promising results for samples of sideromelane shards from Iceland and is likely to be effective at characterizing other kinds of volcanic particle shapes. C1 Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. RP Maria, A (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012,NHB-119, Washington, DC 20013 USA. EM maria@volcano.si.edu; scarey@gso.uri.edu NR 47 TC 20 Z9 22 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD NOV PY 2002 VL 107 IS B11 AR 2283 DI 10.1029/2001JB000822 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 637RR UT WOS:000180527200018 ER PT J AU Chen, Y Esser, R Hu, YQ AF Chen, Y Esser, R Hu, YQ TI A theoretical model for O5+ (O7+) ions in the fast solar wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID POLAR CORONAL HOLE; ELECTRON-TEMPERATURE; CHARGE STATES; HEAVY-IONS; ULYSSES; SWICS; ACCELERATION; OXYGEN; FLOW; SOHO AB [1] We present a theoretical model for O5+ (O7+) ions as test particles in the fast solar wind using a previous turbulence-driven four-fluid model to establish the background solar wind, which consists of electrons, protons, alpha particles, and O6+ ions. The O5+ (O7+) ions in our model and the O6+ ions in the background are driven by the same mechanism, say, the resonant cyclotron interaction or an exponential heating addition. The ionization and recombination processes of O ions are taken into account. It is shown that the differential flow speeds between O6+ and O-5, or O7+, which are found to be in the range of 0.3-2, play very different roles in the formation of O charge states. This is due to discrepancy between the freezing-in distances of the two ion species. O7+ forms predominantly below 1.2 R-S too close to the Sun to develop a differential streaming between O ions. O5+, on the other hand, freezes-in at about 1.8 R-S where differential flows are well developed and therefore important for the formation of O5+ ions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sci & Technol China, Hefei 230026, Peoples R China. RP Chen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Chen, Yao/B-7255-2011 NR 32 TC 6 Z9 6 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV PY 2002 VL 107 IS A11 AR 1368 DI 10.1029/2002JA009341 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634UU UT WOS:000180360500035 ER PT J AU Grappin, R Leorat, J Habbal, SR AF Grappin, R Leorat, J Habbal, SR TI Large-amplitude Alfven waves in open and closed coronal structures: A numerical study SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE solar wind; Alfven waves; acceleration; nonlinear coupling; numerical simulations; MHD ID SOLAR-WIND ACCELERATION; PROPAGATION; STREAMER; SLOW AB [1] We present the first simulations of the coronal response to Alfven wave injection using transparent boundaries in a classical one-fluid, isothermal axisymmetric model including both closed and open magnetic field structures. The aim of the work is first to study how Alfven waves change the contrast between the equatorial and high-latitude wind, and second, how they modify the geometry of the wind and its global stability. We integrate the full time-dependent MHD equations, and inject large-amplitude (150 km/s), low-frequency (20 min period) waves at 1.8 R-s, both in open and in closed field line regions, except within narrow regions around the poles and the equator. The domain considered extends up to 16 R-s. Our principal results are the following: (1) The assumption of a latitude-independent Alfven wave amplitude compatible with observations leads to a large acceleration both of the high-latitude and equatorial wind; as a consequence, the contrast between slow and fast wind speeds at 16 R-s is not as large as the observed values if extrapolated to 1 AU, a result which could potentially change with the use of better resolved, less dissipative simulations; (2) an initial delay in the Alfven flux onset in one hemisphere generates a stable global circulation in the closed loops region, which after a long enough time produces a global north-south asymmetry and changes the structure of the corona as a whole. C1 Observ Meudon, Dept Astrophys Extragalact & Cosmol, F-92195 Meudon, France. Univ Coll Wales, Dept Phys, Aberystwyth SY23 3BZ, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grappin, R (reprint author), Observ Meudon, Dept Astrophys Extragalact & Cosmol, F-92195 Meudon, France. NR 15 TC 12 Z9 12 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 NOV PY 2002 VL 107 IS A11 AR 1380 DI 10.1029/2001JA005062 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634UU UT WOS:000180360500047 ER PT J AU Sanmartin, JR Estes, RD AF Sanmartin, JR Estes, RD TI Magnetic self-field effects on current collection by an ionospheric bare tether SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ionospheric tethers; bare tethers; magnetic self-field of tethers; magnetic effects on current collection; orbital-motion-limited current; magnetic topology ID CYLINDRICAL LANGMUIR PROBES; MOTION-LIMITED REGIME AB [1] It was recently suggested that the magnetic field created by the current of a bare tether strongly reduces its own electron-collection capability when a magnetic separatrix disconnecting ambient magnetized plasma from tether extends beyond its electric sheath. It is here shown that current reduction by the self-field depends on the ratio L-*/L-t parameterizing bias and current profiles along the tether (L-t = tether length, L-* = characteristic length gauging ohmic effects) and on a new dimensionless number K-s involving ambient and tether parameters. Current reduction is weaker the lower K-s and L-* /L-t, which depend critically on the type of cross section: K-s varies as R-5/3, h(2/3) R, and h(2/3) x 1/4 width for wires, round tethers conductive only in a thin layer, and thin tapes, respectively; L-* varies as R-2/3 for wires and as h(2/3) for tapes and round tethers conductive in a layer (R = radius, h = thickness). Self-field effects are fully negligible for the last two types of cross sections whatever the mode of operation. In practical efficient tether systems having L-*/L-t, low, maximum current reduction in case of wires is again negligible for power generation; for deorbiting, reduction is <1% for a 10 km tether and similar to 15% for a 20 km tether. In the reboost mode there are no effects for K-s below some threshold; moderate effects may occur in practical but heavy reboost-wire systems that need no dedicated solar power. C1 Univ Politecn Madrid, Escuela Tecn Super Ingn Aeronaut, E-28040 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Politecn Madrid, Escuela Tecn Super Ingn Aeronaut, E-28040 Madrid, Spain. EM Ors@faia.upm.es; estes@onscreen-sci.com NR 18 TC 7 Z9 7 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV PY 2002 VL 107 IS A11 AR 1335 DI 10.1029/2002JA009344 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634UU UT WOS:000180360500002 ER PT J AU Pelaez, J Ruiz, M Lopez-Rebollal, O Lorenzini, EC Cosmo, ML AF Pelaez, J Ruiz, M Lopez-Rebollal, O Lorenzini, EC Cosmo, ML TI Two-bar model for the dynamics and stability of electrodynamic tethers SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article AB Previously a new dynamic instability that affected electrodynamic tethers in inclined orbits was studied, with a simple one-bar model that neglected the contribution of the tether lateral dynamics. The flexibility of the tether (lateral dynamics), however, plays an important role in the overall motion of the system as shown by numerical simulations of a bare-tether generator in a circular inclined orbit. The same analytical techniques of the previous work are now applied to investigate the dynamics and stability of an electrodynamic tether system modeled by two articulated bars that account for the lowest lateral modes of the tether. The analysis, which can be directly extended to any electrodynamic tether system, has been focused on two particular, but important cases: the combination of a conductive and a nonconductive leader tether (as in the Propulsive Small Expendable Deployment System) and a homogeneous, conductive tether. The lateral dynamics is extremely rich, with skip rope motion, instability peaks, and chains of bifurcations for different regions of the parameter space. The same energy pumping mechanism that destabilizes the rigid model (one bar) is found to drive an even faster instability of the lateral modes. Damping, which has not been included in the analysis, could change this unstable behavior. C1 Univ Politecn Madrid, Escuela Tecn Super Ingn Aeronaut, E-28040 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pelaez, J (reprint author), Univ Politecn Madrid, Escuela Tecn Super Ingn Aeronaut, Pl Cardenal Cisneros 3, E-28040 Madrid, Spain. EM jpelaez@faia.upm.es; mrd@faia.upm.es; oscar@faia.upm.es; elorenzini@cfa.harvard.edu; mcosmo@cfa.harvard.edu NR 17 TC 28 Z9 30 U1 1 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV-DEC PY 2002 VL 25 IS 6 BP 1125 EP 1135 DI 10.2514/2.4992 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 613CB UT WOS:000179112600016 ER PT J AU Eberhard, WG AF Eberhard, WG TI Physical restraint or stimulation? The function(s) of the modified front legs of male Archisepsis diversiformis (Diptera, Sepsidae) SO JOURNAL OF INSECT BEHAVIOR LA English DT Article DE sexual selection; sepsid flies; lock-and-key; male-female conflict of interests ID SEXUAL SELECTION; MATING-BEHAVIOR; FEMALE CHOICE; FLY; CYNIPSEA; CONFLICT; SUCCESS; ODONATA; INSECT; FLIES AB Four hypotheses that could explain the elaborate species-specific morphology of the clasping organs on the front legs of male Archisepsis diversiformis flies were tested: direct male-male combat, mechanical fit, male-female conflict of interests, and male stimulation of the female. Experimental modification of the shape of the male clasper and of the female wing base where the male clasped the female both strongly reduced the chances that a mount would result in copulation. This reduction was not predicted by the male-male combat hypothesis but was predicted by the others. Males in the field did nave to fight other males to remain mounted on females, as expected by the male-male combat hypothesis. Reduced male copulatory success was not due to inferior male ability to grasp and hold onto the female's wings, as predicted by the mechanical fit and male-female conflict hypotheses but to a reduction in the likelihood that the female would allow intromission, as predicted by the stimulation hypothesis. By a process of elimination, and in combination with data from a previous morphological study, the data support the hypothesis that the species-specific aspects of grasping organs in these flies function to stimulate females. Further behavioral data will be needed to test alternative possibilities. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. NR 48 TC 32 Z9 32 U1 0 U2 5 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0892-7553 J9 J INSECT BEHAV JI J. Insect Behav. PD NOV PY 2002 VL 15 IS 6 BP 831 EP 850 DI 10.1023/A:1021161915227 PG 20 WC Entomology SC Entomology GA 617KB UT WOS:000179359900008 ER PT J AU Gonzalez, S Alvarez-Valin, F Maldonado, JE AF Gonzalez, S Alvarez-Valin, F Maldonado, JE TI Morphometric differentiation of endangered pampas deer (Ozotoceros bezoarticus), with description of new subspecies from Uruguay SO JOURNAL OF MAMMALOGY LA English DT Article DE genetic differentiation; geographic variation; morphometry; Ozotoceros bezoarticus; pampas deer; sexual dimorphism ID CONSERVATION; GENETICS AB The pampas deer, Ozotoceros bezoarticus, was, until the recent past, widespread in South America from 5degreesS to 41degreesS; however, it is now considered to be one of the most endangered South American cervids because of habitat destruction and fragmentation. A comparative craniometrical study using univariate and multivariate analyses was performed to determine whetherd populations of pampas deer show patterns of sexual dimorphism and geographic variation. We found that pampas deer exhibit strong sexual dimorphism. Although the species showed high levels of intrapopulation morphological variability, most of it can be attributed to males, which are highly variable within populations. The 4 populations analyzed in this work, which correspond to 4 geographic regions in South America, are. significantly differentiated, with females contributing most to differentiation among populations. Furthermore, results of our morphometric analysis were in concordance with genetic levels of differentiation previously found among populations. This study also supports the recognition of 2 separate subspecies in the Uruguayan northwestern grassland (Salto Department) and the Uruguayan east grassland (Rocha Department). C1 IIBCE, Dept Citogenet, Inst Biol, Unidad Asociada,Fac Ciencias, Montevideo 11600, Uruguay. Fac Ciencias, Secc Biomatemat, Montevideo 11400, Uruguay. Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. RP Gonzalez, S (reprint author), IIBCE, Dept Citogenet, Inst Biol, Unidad Asociada,Fac Ciencias, Av Italia 3318, Montevideo 11600, Uruguay. NR 32 TC 25 Z9 30 U1 0 U2 2 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD NOV PY 2002 VL 83 IS 4 BP 1127 EP 1140 DI 10.1644/1545-1542(2002)083<1127:MDOEPD>2.0.CO;2 PG 14 WC Zoology SC Zoology GA 621HP UT WOS:000179583200021 ER PT J AU Jarosewich, E AF Jarosewich, E TI Smithsonian Microbeam Standards SO JOURNAL OF RESEARCH OF THE NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY LA English DT Article; Proceedings Paper CT Workshop on the Accuracy Barrier in Quantitative EPMA and the Role of Standards CY APR 08-11, 2002 CL NATL INST STAND & TECHNOL, GAITHERSBURG, MD SP Natl Inst Stand & Technol, Chem Sci & Technol Lab, Surface & Microanal Sci Div, Microbeam Anal Soc HO NATL INST STAND & TECHNOL DE electron microprobe standards; microbeam standards; mineral standards; reference materials AB This is a short history of the Smithsonian Microbeam Standards; their sources, selection, preparation, and analyses. Fifty-eight minerals, natural glasses, and synthetic samples have been characterized in the past 25 years. During that time, over 750 requests were received for approximately 11 000 individual samples. These reference samples are referred to as the Smithsonian Microbeam Standards. C1 Smithsonian Inst, NMNH, Dept Mineral Sci, Washington, DC 20560 USA. RP Jarosewich, E (reprint author), Smithsonian Inst, NMNH, Dept Mineral Sci, Washington, DC 20560 USA. NR 10 TC 54 Z9 54 U1 0 U2 17 PU US GOVERNMENT PRINTING OFFICE PI WASHINGTON PA SUPERINTENDENT DOCUMENTS,, WASHINGTON, DC 20402-9325 USA SN 1044-677X J9 J RES NATL INST STAN JI J. Res. Natl. Inst. Stand. Technol. PD NOV-DEC PY 2002 VL 107 IS 6 BP 681 EP 685 DI 10.6028/jres.107.054 PG 5 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 643NJ UT WOS:000180867100018 PM 27446760 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 Contamination an the rare-earth element orthophosphate reference samples SO JOURNAL OF RESEARCH OF THE NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY LA English DT Article; Proceedings Paper CT Workshop on the Accuracy Barrier in Quantitative EPMA and the Role of Standards CY APR 08-11, 2002 CL NATL INST STAND & TECHNOL, GAITHERSBURG, MD SP Natl Inst Stand & Technol, Chem Sci & Technol Lab, Surface & Microanal Sci Div, Microbeam Anal Soc HO NATL INST STAND & TECHNOL DE EPMA; microanalysis; orthophosphates; quantitative analysis; rare earth elements; rare earth phosphates; REE; standards ID ELECTRON-MICROPROBE ANALYSIS AB Several of the fourteen rare-earth element (plus Sc and Y) orthophosphate standards grown at Oak Ridge National Laboratory in the 1980s and widely distributed by the Smithsonian Institution's Department of Mineral Sciences, are 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 (approximate to 1360 degreesC) prior to the crystal synthesis. Because these rare-earth element standards are extremely stable under the electron beam and considered homogenous, they have been of enormous value to electron probe microanalysis (EPMA). The monoclinic, monazite structure, orthophosphates show a higher degree of Pb incorporation than the tetragonal xenotime structure, orthophosphates. This paper will attempt to describe and rationalize the extent of the Pb contamination in these otherwise excellent materials. 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. EM donovan@oregon.uoregon.edu RI Boatner, Lynn/I-6428-2013 OI Boatner, Lynn/0000-0002-0235-7594 NR 16 TC 3 Z9 3 U1 0 U2 5 PU US GOVERNMENT PRINTING OFFICE PI WASHINGTON PA SUPERINTENDENT DOCUMENTS,, WASHINGTON, DC 20402-9325 USA SN 1044-677X J9 J RES NATL INST STAN JI J. Res. Natl. Inst. Stand. Technol. PD NOV-DEC PY 2002 VL 107 IS 6 BP 693 EP 701 DI 10.6028/jres.107.056 PG 9 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 643NJ UT WOS:000180867100020 PM 27446762 ER PT J AU Vicenzi, EP Eggins, S Logan, A Wysoczanski, R AF Vicenzi, EP Eggins, S Logan, A Wysoczanski, R TI Microbeam characterization of coming archeological reference glasses: New additions to the Smithsonian Microbeam Standard collection SO JOURNAL OF RESEARCH OF THE NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY LA English DT Article; Proceedings Paper CT Workshop on the Accuracy Barrier in Quantitative EPMA and the Role of Standards CY APR 08-11, 2002 CL NATL INST STAND & TECHNOL, GAITHERSBURG, MD SP Natl Inst Stand & Technol, Chem Sci & Technol Lab, Surface & Microanal Sci Div, Microbeam Anal Soc HO NATL INST STAND & TECHNOL DE chemical heterogeneity; electron probe microanalysis; glass; laser ablation ICP-MS; microbeam; microscale characterization; secondary ion mass spectrometry AB An initial study of the minor element, trace element, and impurities in Corning archeological references glasses have been performed using three microbeam techniques: electron probe microanalysis (EPMA), laser ablation ICP-mass spectrometry (LA ICP-MS), and secondary ion mass spectrometry (SIMS). The EPMA results suggest a significant level of heterogeneity for a number of metals. Conversely, higher precision and a larger sampling volume analysis by LA ICP-MS indicates a high degree of chemical uniformity within all glasses, typically <2 % relative (1 sigma). SIMS data reveal that small but measurable quantities of volatile impurities are present in the glasses, including H at roughly the 0.0001 mass fraction level. These glasses show promise for use as secondary standards for minor and trace element analyses of insulating materials such as synthetic ceramics, minerals, and silicate glasses. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. RP Vicenzi, EP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM vicenzi@volcano.si.edu RI Wysoczanski, Richard/C-2930-2009; Wysoczanski, Richard/I-7730-2012; Eggins, Stephen/H-6943-2016 OI Eggins, Stephen/0000-0002-0007-5753 NR 12 TC 40 Z9 40 U1 0 U2 13 PU US GOVERNMENT PRINTING OFFICE PI WASHINGTON PA SUPERINTENDENT DOCUMENTS,, WASHINGTON, DC 20402-9325 USA SN 1044-677X J9 J RES NATL INST STAN JI J. Res. Natl. Inst. Stand. Technol. PD NOV-DEC PY 2002 VL 107 IS 6 BP 719 EP 727 DI 10.6028/jres.107.058 PG 9 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 643NJ UT WOS:000180867100022 PM 27446764 ER PT J AU Schroll, S AF Schroll, S TI Couture culture: A study in modern art and fashion. SO LIBRARY JOURNAL 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 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 NOV 1 PY 2002 VL 127 IS 18 BP 88 EP 88 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 608ZN UT WOS:000178878100069 ER PT J AU Marko, PB AF Marko, PB TI Fossil calibration of molecular clocks and the divergence times of geminate species pairs separated by the Isthmus of Panama SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Review DE bivalves; calibration; cytochrome oxidase-1; histone-3; fossil record; molecular clock; molluscs; speciation dates; substitution models ID MITOCHONDRIAL-DNA EVOLUTION; NUCLEOTIDE SUBSTITUTION; MAXIMUM-LIKELIHOOD; GENETIC-DIVERGENCE; TROPICAL AMERICA; RAPID EVOLUTION; EASTERN PACIFIC; SEA-URCHINS; SPECIATION; HISTORY AB Calibration of nucleotide sequence divergence rates provides an important method by which to test many hypotheses of evolution. In the absence of an adequate fossil record, geological events, rather than the first appearances of sister taxa in the geological record, are often used to calibrate molecular clocks. The formation of the Isthmus of Panama, which isolated the tropical western Atlantic and eastern Pacific oceans, is one such event that is frequently used to infer rates of nucleotide sequence divergence. Isthmian calibrations assume that morphologically similar "geminate" species living now on either side of the isthmus were isolated geographically by the latest stages of seaway closure 3.1-3.5 MYA. Here, I have applied calibration dates from the fossil record to cytochrome c oxidase-1 (CO1) and nuclear histone-3 (H3) divergences among six pairs of geminates in the Arcidae to test this hypothesis. Analysis of CO1 first and third positions yield geminate divergences that predate final seaway closure, and on the basis of CO1 first positions, times for all six geminates are significantly greater than 3.5 Myr. H3 sequences produce much more recent geminate divergences, some that are younger than 3.1 Myr. But H3-derived estimates for all arcid geminates are not significantly different from both 0 and 15 Myr. According to CO1, one of the two most divergent pairs, Arca mutabilis and A. imbricata, split more than 30 MYA. This date is compatible with the fossil record, which indicates that these species were morphologically distinct at least 16-21 MYA. Across all CO1 nucleotide sites, divergence rates for arcids are slower than the rates reported for other taxa on the basis of isthmian calibrations, with the exception of rates determined from the least divergent species pair in larger surveys of multiple transisthmian pairs. Rate differences between arcids and some taxa may be real, but these data suggest that divergence rates can be greatly overestimated when dates corresponding to final closure of the Central American Seaway are used to calibrate the molecular clocks of marine organisms. C1 Smithsonian Trop Res Inst, Naos Marine Lab, Balboa, Panama. Nat Hist Museum Los Angeles, Mol Systemat Lab, Los Angeles, CA USA. RP Marko, PB (reprint author), Univ N Carolina, Dept Marine Sci, 12-7 Venable Hall,CB 3300, Chapel Hill, NC 27599 USA. NR 106 TC 210 Z9 215 U1 4 U2 29 PU SOC MOLECULAR BIOLOGY EVOLUTION PI LAWRENCE PA PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD NOV PY 2002 VL 19 IS 11 BP 2005 EP 2021 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 617NF UT WOS:000179367200018 PM 12411609 ER PT J AU Bate, MR Bonnell, IA Bromm, V AF Bate, MR Bonnell, IA Bromm, V TI The formation of close binary systems by dynamical interactions and orbital decay SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; hydrodynamics; binaries : close; binaries : spectroscopic; circumstellar matter; stars : formation ID ROTATING INTERSTELLAR CLOUDS; SMOOTHED PARTICLE HYDRODYNAMICS; ELONGATED CYLINDRICAL CLOUDS; MASS-RATIO DISTRIBUTION; STAR-FORMATION; SPECTROSCOPIC BINARIES; PROTOSTELLAR FORMATION; FORMATION MECHANISM; STELLAR-SYSTEMS; PROTOBINARY SYSTEMS AB We present results from the first hydrodynamical star formation calculation to demonstrate that close binary stellar systems (separations less than or similar to 10 au) need not be formed directly by fragmentation. Instead, a high frequency of close binaries can be produced through a combination of dynamical interactions in unstable multiple systems and the orbital decay of initially wider binaries. Orbital decay may occur as a result of gas accretion and/or the interaction of a binary with its circumbinary disc. These three mechanisms avoid the problems associated with the fragmentation of optically thick gas to form close systems directly. They also result in a preference for close binaries to have roughly equal-mass components because dynamical exchange interactions and the accretion of gas with high specific angular momentum drive mass ratios towards unity. Furthermore, because of the importance of dynamical interactions, we find that stars with greater masses ought to have a higher frequency of close companions, and that many close binaries ought to have wide companions. These properties are in good agreement with the results of observational surveys. C1 Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, 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, Stocker Rd, Exeter EX4 4QL, Devon, England. EM mbate@astro.ex.ac.uk NR 58 TC 162 Z9 162 U1 1 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2002 VL 336 IS 3 BP 705 EP 713 DI 10.1046/j.1365-8711.2002.05775.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 608RK UT WOS:000178860300005 ER PT J AU Pappa, A Georgantopoulos, I Ward, M Zezas, AL AF Pappa, A Georgantopoulos, I Ward, M Zezas, AL TI The BeppoSAX spectrum of the composite galaxy Mrk 609 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : individual : Mrk 609; galaxies : starburst; X-rays : galaxies ID X-RAY OBSERVATIONS; SEYFERT-GALAXIES; LINE REGION; EMISSION; ROSAT; CLASSIFICATION; STARBURST AB We present BeppoSAX observations of the starburst/Seyfert composite galaxy Mrk 609. This enigmatic object has an optical spectrum dominated by the features of starburst galaxies, yet its X-ray luminosity (6 3 x 10(42) erg s(-1)) is typical of an active galactic nucleus (AGN). The X-ray spectrum of Mrk 609 can be parametrized by a single-power-law model with a photon index Gamma similar to 1.6 +/- 0 1 and no evidence for significant absorption above the Galactic value. Long-term variability in both the 0.1-2 and 2-10 keV energy bands is detected, again suggesting that the X-ray emission is dominated by an AGN. The observed broad H component is a factor of 40 below that predicted by the X-ray flux, implying a deficit of ionizing ultraviolet photons. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pappa, A (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RI Georgantopoulos, Ioannis/L-3687-2013; Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 20 TC 7 Z9 7 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 NOV 1 PY 2002 VL 336 IS 3 BP 714 EP 720 DI 10.1046/j.1365-8711.2002.05629.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 608RK UT WOS:000178860300006 ER PT J AU Lile, S AF Lile, S TI Solving the history mystery (The History Lab project of the Washington State History Museum in Tacoma) SO MUSEUM NEWS LA English DT Article C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Lile, S (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD NOV-DEC PY 2002 VL 81 IS 6 BP 61 EP 62 PG 2 WC Art SC Art GA 609PA UT WOS:000178913100037 ER PT J AU Sozzetti, A Casertano, S Brown, RA Lattanzi, MG AF Sozzetti, A Casertano, S Brown, RA Lattanzi, MG TI Narrow-angle astrometry with the Space Interferometry Mission: The search for extrasolar planets. I. Detection and characterization of single planets SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID LOW-MASS COMPANIONS; METROLOGY TESTBED MAM; SUB-STELLAR OBJECTS; GIANT PLANETS; SUBSTELLAR COMPANIONS; UPSILON-ANDROMEDAE; SOLAR PLANETS; BROWN DWARF; HIPPARCOS OBSERVATIONS; ORBITAL ELEMENTS AB A decade after the publication of the Hipparcos Catalogue, the Space Interferometry Mission (SIM) will be capable of making selected high-precision astrometric measurements about 3 orders of magnitude more accurate than the Hipparcos survey. We present results from a detailed set of end-to-end numerical simulations of SIM narrow-angle astrometric measurements and data analysis to illustrate the enormous potential that SIM has for the discovery and characterization of planets outside the solar system. Utilizing a template observing scenario, we quantify SIM sensitivity to single planets orbiting single normal nearby stars as a function of measurement errors and properties of the planet: SIM will detect over 95% of the planets with periods between a few days and the 5 yr nominal mission lifetime that produces astrometric signatures similar to2.2 times larger than the single-measurement accuracy. We provide accuracy estimates of full-orbit reconstruction and planet mass determination: at twice the discovery limit, orbital elements will be determined with a typical accuracy of 20%-30%; the astrometric signature must be 10 and 15 times the minimum signal required for detection to derive mass and inclination-angle estimates accurate to 10%. We quantify the impact of different observing strategies on the boundaries for secure detection and accurate orbit estimation: the results scale with the square root of both the number of observations and the number of reference stars. We investigate SIM discovery space, to gauge the instrument ability in detecting very low mass planets: around the nearest stars, SIM will find planets as small as Earth, if they are present. Some of these might be orbiting inside the parent star's habitable zone. Extrasolar planets figure prominently among SIM scientific goals: our results reaffirm the importance of high-precision astrometric measurements as a unique complement to spectroscopic surveys based on radial velocity. For example, establishing the existence of rocky, perhaps habitable planets would constitute both a fundamental test of theoretical models and progress toward the understanding of formation and evolution processes of planetary systems. Such discoveries would also provide the Terrestrial Planet Finder with prime targets to investigate with direct spectroscopy in terms of the potential for life. C1 Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Osserv Astron Torino, I-10025 Pino Torinese, Italy. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Sozzetti, A (reprint author), Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. EM alex@phyast.pitt.edu; stefano@stsci.edu; rbrown@stsci.edu; lattanzi@to.astro.it OI Sozzetti, Alessandro/0000-0002-7504-365X; Lattanzi, Mario Gilberto/0000-0003-0429-7748 NR 96 TC 24 Z9 24 U1 0 U2 2 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 NOV PY 2002 VL 114 IS 801 BP 1173 EP 1196 DI 10.1086/343823 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610QP UT WOS:000178972200002 ER PT J AU Epps, HW Fabricant, DG AF Epps, HW Fabricant, DG TI Athermalizing refractive optics with fluid lenses SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID LIQUIDS; DISPERSION; INDEXES AB Astronomical optics may encounter a wide range of nighttime temperatures (similar to-10degreesC to +20degreesC) at mountaintop observatories. Complex refractive optics used in high-performance spectrographs and focal reducers may perform poorly at temperature extremes unless special care is taken in their design. Refocusing will not always restore image quality, and thermally induced focal length changes may introduce troublesome image motion. We describe the techniques that we have used to predict the thermal behavior of the Binospec Spectrograph, an instrument under development for the converted Multiple Mirror Telescope. This thermal analysis must account for (1) the change in optical power due to thermal expansion of the optical elements, (2) thermal variations in the refractive indices of the optical elements, and (3) element respacings due to the interplay between the thermal expansions of the optical elements and cell materials. Binospec's multiplets are fluid coupled to reduce the reflection losses that would occur at glass-air surfaces; to athermalize the Binospec optics, we form weak lenses in the optical coupling fluid within multiplets. The large variation of the coupling fluid's refractive index with temperature allows these weak fluid lenses to correct thermal changes in the optical elements and cell. This athermalization technique is attractive because it introduces no additional mechanical complexity. C1 Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Epps, HW (reprint author), Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA. NR 18 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 NOV PY 2002 VL 114 IS 801 BP 1252 EP 1259 DI 10.1086/343218 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610QP UT WOS:000178972200009 ER PT J AU Small, LM AF Small, LM TI Cultivating delight (An introduction to the Smithsonian's Horticulture Services Division) SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, 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 NOV PY 2002 VL 33 IS 8 BP 20 EP 20 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 607LH UT WOS:000178792700002 ER PT J AU Zygelman, B Dalgarno, A AF Zygelman, B Dalgarno, A TI Shape resonance enhancement of dipolar relaxation in ultra-cold atomic gases SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID BOSE-EINSTEIN CONDENSATION; FESHBACH RESONANCES; COLLISIONS; SCATTERING; RB-85 AB We demonstrate that shape resonances can enhance the dipolar relaxation rate of atomic gases in the zero-temperature limit. We show that the rate coefficients exhibit resonance features as a bias magnetic field is swept through a region characterized by the resonances. Unlike Feshbach resonances which also enhance dipolar relaxation rates, the shape resonance mechanism does not affect the value of the collision s-wave scattering length. We discuss possible applications of the proposed mechanism in cold atomic gases or bosonic condensates. C1 Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. MIT, Harvard Ctr Ultra Cold Atoms, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zygelman, B (reprint author), Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. NR 22 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD OCT 28 PY 2002 VL 35 IS 20 BP L441 EP L446 AR PII S0953-4075(02)52715-2 DI 10.1088/0953-4075/35/20/101 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 620UV UT WOS:000179551600001 ER PT J AU Norman, JA Christidis, L Joseph, L Slikas, B Alpers, D AF Norman, JA Christidis, L Joseph, L Slikas, B Alpers, D TI Unravelling a biogeographical knot: origin of the 'leapfrog' distribution pattern of Australo-Papuan sooty owls (Strigiformes) and logrunners (Passeriformes) SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE leapfrog; comparative phylogeography; speciation; mitochondrial DNA; Aves; systematics ID CYTOCHROME-B GENE; NUCLEOTIDE-SEQUENCES; EVOLUTIONARY RATES; SPECIATION PROCESS; SPECTRAL-ANALYSIS; PHYLOGENETIC DATA; VERTEBRATES; MUTATION; BIRDS AB Molecular analysis of two Australo-Papuan rainforest birds exhibiting correlated 'leapfrog' patterns were used to elucidate the evolutionary origin of this unusual pattern of geographical differentiation. In both sooty owls (Tyto) and logrunners (Orthonyx), phenotypically similar populations occupy widely disjunct areas (central-eastern Australia and upland New Guinea) with a third, highly distinctive population, occurring between them in northeastern Queensland. Two mechanisms have been proposed to explain the origin of leapfrog patterns in avian distributions: recent shared ancestry of terminal populations and unequal rates or phenotypic change among populations. As the former should generate correlated patterns of phenotypic and genetic differentiation, we tested for a sister relationship between populations from New Guinea and central-eastern Australia using nuclear and mitochondrial DNA sequences. The resulting phylogenies not only refute recent ancestry as an explanation for the leapfrog pattern, but provide evidence of vastly different spatio-temporal histories for sooty owls and logrunners within the Australo-Papuan rainforests. This incongruence indicates that the evolutionary processes responsible for generating leapfrog patterns in these co-distributed taxa are complex, possibly involving a combination of selection and drift in sooty owls and convergence or retention of ancestral characteristics in logrunners. C1 Museum Victoria, Dept Sci, Melbourne, Vic 3001, Australia. Acad Nat Sci Philadelphia, Dept Ornithol, Philadelphia, PA 19103 USA. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. RP Christidis, L (reprint author), Museum Victoria, Dept Sci, GPO Box 666E, Melbourne, Vic 3001, Australia. EM lchrist@museum.vic.gov.au RI Joseph, Leo/F-9235-2010; Slikas, Beth/E-7275-2013 NR 42 TC 28 Z9 28 U1 3 U2 12 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 OCT 22 PY 2002 VL 269 IS 1505 BP 2127 EP 2133 DI 10.1098/rspb.2002.2136 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 607WX UT WOS:000178814700008 PM 12396487 ER PT J AU Hartmann, L AF Hartmann, L TI Flows, fragmentation, and star formation. I. Low-mass stars in Taurus SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : structure; stars : formation; stars : pre-main-sequence ID MOLECULAR CLOUD CORES; MAIN-SEQUENCE STARS; MAGNETIC-FIELD STRUCTURE; SHEET-LIKE CLOUDS; DARK CLOUDS; GRAVITATIONAL COLLAPSE; FORMING REGIONS; DENSE CORES; STELLAR CLUSTERS; MAGNETOHYDRODYNAMIC TURBULENCE AB The remarkably filamentary spatial distribution of young stars in the Taurus molecular cloud has significant implications for understanding low-mass star formation in relatively quiescent conditions. The large scale and regular spacing of the laments suggests that small-scale turbulence is of limited importance, which could be consistent with the driving on large scales by flows that produced the cloud. The small spatial dispersion of stars from gaseous laments indicates that the low-mass stars are generally born with small velocity dispersions relative to their natal gas, of the order of the sound speed or less. The spatial distribution of the stars exhibits a mean separation of about 0.25 pc, comparable to the estimated Jeans length in the densest gaseous laments, and is consistent with roughly uniform density along the laments. The efficiency of star formation in laments is much higher than elsewhere, with an associated higher frequency of protostars and accreting T Tauri stars. The protostellar cores are generally aligned with the laments, suggesting that they are produced by gravitational fragmentation, resulting in initially quasi-prolate cores. Given the absence of massive stars that could strongly dominate cloud dynamics, Taurus provides important tests of theories of dispersed low-mass star formation and numerical simulations of molecular cloud structure and evolution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hartmann@cfa.harvard.edu NR 86 TC 150 Z9 150 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2002 VL 578 IS 2 BP 914 EP 924 DI 10.1086/342657 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 604JR UT WOS:000178617600021 ER PT J AU Ko, YK Raymond, JC Li, J Ciaravella, A Michels, J Fineschi, S Wu, R AF Ko, YK Raymond, JC Li, J Ciaravella, A Michels, J Fineschi, S Wu, R TI Solar and Heliospheric Observatory ultraviolet coronagraph spectrometer and Yohkoh Soft X-ray Telescope observations of the high-temperature corona above an active region complex SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : abundances; Sun : corona; Sun : UV radiation ID FE-XVII; SOHO; STREAMERS; ABUNDANCE; WIND; UVCS/SOHO; DENSITY; LINES; DIAGNOSTICS; ANGSTROM AB We present the results of Solar and Heliospheric Observatory Ultraviolet Coronagraph Spectrometer ( SOHO / UVCS) and Yohkoh Soft X-Ray Telescope (SXT) observations above an active region complex (AR 8194, 8195, and 8198) at the southeast limb on 1998 April 6-7. This active region complex appears to be the base of a small streamer seen by the Large Angle and Spectrometric Coronagraph Experiment (LASCO/C2) at the southeast limb. The UVCS was offset-pointed to observe low in the corona from 1.22 up to 1.6 R-. with normal pointing. High-temperature lines such as [ Fe xvIII] lambda974 and Ne ix lambda1248 were present in this region, implying that the electron temperature is higher than that in the quiet-Sun corona. This region of the corona is also seen as particularly bright in the Yohkoh / SXT, SOHO EUV Imaging Telescope high-temperature filter ( Fe xv lambda284) and SOHO/LASCO C1. The electron temperature analysis indicates a two-temperature structure, one of similar to1.5 x 10(6) K, which is similar to that observed in quiet-Sun streamers, and the other at a high temperature of similar to3.0 x 10(6) K. This two-temperature region likely corresponds to two distinct coronal regions overlapping in the line of sight. We compare the electron temperature and emission measure results from the SOHO / UVCS data with those from the Yohkoh / SXT data. The absolute elemental abundances show a general first ionization potential effect and decrease with height for all the elements. This is consistent with the effect of gravitational settling, which, however, cannot totally account for the observed elemental abundances. Other mechanisms that are likely to affect the coronal elemental abundance are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Ko, YK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 49 TC 38 Z9 38 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2002 VL 578 IS 2 BP 979 EP 995 DI 10.1086/342616 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 604JR UT WOS:000178617600028 ER PT J AU Jayawardhana, R Mohanty, S Basri, G AF Jayawardhana, R Mohanty, S Basri, G TI Probing disk accretion in young brown dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID LOW-MASS STARS; T-TAURI STARS; SCORPIUS OB ASSOCIATION; CLUSTER; ROTATION; MODELS; ORION AB We present high-resolution optical spectra of 15 objects near or below the substellar limit in the Upper Scorpius and rho Ophiuchus star-forming regions. These spectra, obtained with the High Resolution Echelle Spectrometer on the Keck I telescope, are used to investigate disk accretion, rotation, and activity in young very low mass objects. We report the detection of a broad, asymmetric H emission line in the rho Oph source GY 5, which is also known to harbor mid-infrared excess, consistent with the presence of an accreting disk. The Halpha profiles of the Upper Sco objects suggest little or no ongoing accretion. Our results imply that if most brown dwarfs are born with disks, their accretion rates decrease rapidly, at timescales comparable to or smaller than those for T Tauri disks. The Upper Sco brown dwarfs appear to be rotating faster than their somewhat younger counterparts in Taurus, consistent with spin-up due to contraction following disk unlocking. The H activity is comparable to saturated activity levels in field M dwarfs with similar spectral type and rotation rates. Comparison of our data with published (albeit lower resolution) spectra of a few of the same objects from other epochs suggests possible variability in accretion/activity indicators. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Jayawardhana, R (reprint author), Univ Michigan, Dept Astron, 830 Dennison Bldg, Ann Arbor, MI 48109 USA. NR 26 TC 54 Z9 54 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2002 VL 578 IS 2 BP L141 EP L144 DI 10.1086/344707 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 604JU UT WOS:000178617800012 ER PT J AU Vikhlinin, A VanSpeybroeck, L Markevitch, M Forman, WR Grego, L AF Vikhlinin, A VanSpeybroeck, L Markevitch, M Forman, WR Grego, L TI Evolution of the cluster X-ray scaling relations since z > 0.4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; surveys; X-rays : galaxies ID LUMINOSITY-TEMPERATURE RELATION; GALAXY CLUSTERS AB We derive correlations between X-ray temperature, luminosity, and gas mass for a sample of 22 distant, z > 0.4, galaxy clusters observed with Chandra. We detect evolution in all three correlations between z > 0.4 and the present epoch. In particular, in the Omega = 0.3 Lambda = 0.7, cosmology, the luminosity corresponding to a fixed temperature scales approximately as (1 + z)(1.5+/-0.3); the gas mass for a fixed luminosity scales as (1 + z)(-1.8+/-0.4) and the gas mass for a fixed temperature scales as (1 + z)(-0.5+/-0.4) (all uncertainties are 90% confidence). We briefly discuss the implication of these results for cluster evolution models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 33 TC 76 Z9 76 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 OCT 20 PY 2002 VL 578 IS 2 BP L107 EP L111 DI 10.1086/344591 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 604JU UT WOS:000178617800004 ER PT J AU Ghent, RR Tibuleac, IM AF Ghent, RR Tibuleac, IM TI Ribbon spacing in Venusian tessera: Implications for layer thickness and thermal state SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EVOLUTION; LITHOSPHERE; TERRAIN; DEFORMATION; EXTENSION; BOUDINAGE; CLIMATE; REGIO; MODEL; BASIN AB [1] We report on measurements of characteristic extensional wavelength represented by ribbons in Venusian tessera terrain. Fourier power spectra for ribbons in 35 areas from 9 geographic regions show dominant wavelengths of 2 to 6 km. We used these values to estimate mechanical layer thickness during ribbon formation at 0.6 to 2.9 km. Because ribbons accommodate extension of a single strong layer overlying a ductile substrate, we conclude that the base of this mechanical layer corresponded to the local brittle- ductile transition (BDT) during ribbon formation. Maintaining a BDT at <3 km depth for a significant length of time requires a locally hot environment, as over a plume impinging on thin lithosphere. These results indicate that locally hot conditions prevailed at widely distinct locations in the past. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Western Geophys Corp, Lexington, MA 02420 USA. RP Ghent, RR (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, POB 37012, Washington, DC 20013 USA. NR 26 TC 7 Z9 7 U1 0 U2 0 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 OCT 15 PY 2002 VL 29 IS 20 AR 2000 DI 10.1029/2002GL015994 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 639BL UT WOS:000180607700061 ER PT J AU Spurr, RJD AF Spurr, RJD TI Simultaneous derivation of intensities and weighting functions in a general pseudo-spherical discrete ordinate radiative transfer treatment SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE radiative transfer; discrete ordinates; linearization; pseudo-spherical ID OZONE PROFILES; RAYLEIGH-SCATTERING; TROPOSPHERIC OZONE; ACCURATE SOLUTION; PLANE-PARALLEL; TRANSFER MODEL; RETRIEVAL; POLARIZATION; ALGORITHM; GOME AB The retrieval of atmospheric constituents from measurements of backscattered light requires a radiative transfer forward model that can simulate both intensities and weighting functions (partial derivatives of intensity with respect to atmospheric parameters being retrieved). The radiative transfer equation is solved in a multi-layer multiply-scattering atmosphere using the discrete ordinate method. In an earlier paper dealing with the upwelling top-of-the-atmosphere radiation field, it was shown that a full internal perturbation analysis of the plane-parallel discrete ordinate solution leads in a natural way to the simultaneous generation of analytically-derived weighting functions with respect to a wide range of atmospheric variables. In the present paper, a more direct approach is used to evaluate explicitly all partial derivatives of the intensity field. A generalization of the post-processing function is developed for the derivation of weighting functions at arbitrary optical depth and stream angles for both upwelling and downwelling directions. Further, a complete treatment is given for the pseudo-spherical approximation of the direct beam attenuation; this is an important extension to the range of viewing geometries encountered in practical radiative transfer applications. The numerical model LIDORT developed for this work is able to generate intensities and weighting functions for a wide range of retrieval scenarios, in addition to the passive remote sensing application from space. We present a number of examples in an atmosphere with O-3 absorption in the UV, for satellite (upwelling radiation) and ground-based (downwelling radiation) applications. In particular, we examine the effect of various pseudo-spherical parameterizations on backscatter intensities and weighting functions with respect to O-3 volume mixing ratio. In addition, the use of layer-integrated multiple scatter output from the model is shown to be important for satellite instruments with wide-angle off nadir viewing geometries. Published by Elsevier Science Ltd. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Spurr, RJD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 39 TC 68 Z9 70 U1 0 U2 7 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 OCT 15 PY 2002 VL 75 IS 2 BP 129 EP 175 AR PII S0022-4073(01)00245-X DI 10.1016/S0022-4073(01)00245-X PG 47 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 580ET UT WOS:000177222700001 ER PT J AU van Oss, RF Spurr, RJD AF van Oss, RF Spurr, RJD TI Fast and accurate 4 and 6 stream linearized discrete ordinate radiative transfer models for ozone profile retrieval SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE discrete ordinates; linearization; 4/6 stream; ozone profile retrieval ID BIOMASS BURNING SMOKE; MONITORING EXPERIMENT; RAYLEIGH-SCATTERING; TROPOSPHERIC OZONE; GOME; APPROXIMATION; ATMOSPHERES; PARAMETERS; ALGORITHM; GEOMETRY AB The global and long-term measurement of ozone vertical and horizontal distributions is one of the most important tasks in the monitoring of the earth's atmosphere. A number of satellite instruments are capable of delivering ozone profile distributions from UV nadir backscatter measurements. Retrieval algorithms should be efficient enough to deliver profiles in real-time without compromising accuracy. Such algorithms require a radiative transfer model that can generate quickly and accurately both simulated radiances and Jacobian matrices of weighting functions. We develop fast and analytic 4 stream and 6 stream linearized discrete ordinate models designed to satisfy performance and accuracy requirements for such an algorithm. The models have the pseudo-spherical treatment of the direct beam attenuation. For anisotropic scattering we use the delta-M scaling method to deal with strong forward scattering peaks. We demonstrate that the accuracy of the models is improved greatly upon application of a single scatter correction based on an exact specification of the phase function. For wide-angle off-nadir viewing, a sphericity correction is developed to deal more precisely with attenuation in a curved atmosphere. Radiances and weighting functions for the 4 and 6 stream models are compared with 20 stream output from the LIDORT model. We show that for the UV range pertinent to ozone profile retrieval from space, the 4 stream model generates backscatter radiances to an accuracy > 1.25% for all viewing situations in a clear sky Rayleigh and background aerosol reference atmosphere, and up to 1.75% for a number of special scenarios with optically thick particulate layers. Six stream radiances are accurate to the 0.25% level for clear sky situations, and 0.65% for the special cases; weighting functions for the 6 stream output are accurate to 2% in all cases. We discuss the implications of these comparisons regarding the performance and accuracy of the radiative transfer forward model in the ozone profile retrieval context. (C) 2002 Elsevier Science Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. RP Spurr, RJD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 35 TC 30 Z9 31 U1 1 U2 2 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 OCT 15 PY 2002 VL 75 IS 2 BP 177 EP 220 AR PII S0022-4073(01)00246-1 DI 10.1016/S0022-4073(01)00246-1 PG 44 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 580ET UT WOS:000177222700002 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The feud that sparked the renaissance: How Brunelleschi and Ghiberti changed the art world. 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 2 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 OCT 15 PY 2002 VL 127 IS 17 BP 70 EP 70 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 602ZF UT WOS:000178533800037 ER PT J AU Riley, S AF Riley, S TI As high as the scooter can fly. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst, Libs, 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 OCT 15 PY 2002 VL 127 IS 17 BP 94 EP 95 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 602ZF UT WOS:000178533800187 ER PT J AU Carleton, MD Sanchez, O Vidales, GU AF Carleton, MD Sanchez, O Vidales, GU TI A new species of Habromys (Muroidea : Neotominae) from Mexico, with generic review of species definitions and remarks on diversity patterns among Mesoamerican small mammals restricted to humid montane forests SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Review ID CENTRAL AMERICAN HERPETOFAUNA; SMALL-EARED SHREW; PEROMYSCUS-BOYLII; MORPHOLOGICAL EVOLUTION; GROUP RODENTIA; ADAPTIVE RADIATION; TAXONOMIC STATUS; MURIDAE; SYSTEMATICS; CRICETIDAE AB A new species of Habromys, H. delicatulus, is described from an isolated patch of cloud forest situated on a northern exposure of the Cordillera Neovolcanica, Estado de Mexico. The species is the smallest so far known in the genus and is further characterized by its delicate cranial features. Morphometric comparisons with the five other species-group taxa currently allocated to the genus recommend the elevation of ixtlani Goodwin, 1964. as a species distinct from Habromys lepturus (Merriam, 1898). Habromys lophurus (Merriam, 1908), known from highlands east of the Isthmus of Tehuantepec, appears to be the sister taxon to the former pair, each restricted in separate Oaxaean ranges west of the Isthmus. Habromys chinanteco (Robertson & Mussel, 1976) is retained as a species, but its possible status as it junior synonym under H. simulatus (Osgood, 1904) warrants continued investigation with improved samples. The montane distribution of Habromys in naturally discontinuous humid-forest associations of northern Mesoamerica is considered in the context of diversity patterns summarized for other small terrestrial mammals confined to such forests. C1 Col Sanchez, Mexico City 50040, DF, Mexico. Univ Nacl Autonoma Mexico, Dept Zool, Mexico City 04510, DF, Mexico. RP Carleton, MD (reprint author), Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, Washington, DC 20560 USA. NR 103 TC 23 Z9 28 U1 0 U2 5 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 OCT 14 PY 2002 VL 115 IS 3 BP 488 EP 533 PG 46 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 605NB UT WOS:000178683000002 ER PT J AU Hastings, PA Springer, VG AF Hastings, PA Springer, VG TI Pholidichthys anguilliformis Lockington, 1881 (Teleostei : Pholidae), a junior synonym of Pholis ornata (Girard, 1854) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The identity of Pholidichthys anguilliformis Lockington, 1881, has been unclear since its original description and subsequent loss of the holotype and only known specimen. We consider it conspecific with Gunnellus ornatus Girard, 1854 (= Pholis ornata [Girard]) and designate the holotype of G. ornatus as neotype of P. anguilliformis, thereby making the latter name a junior objective synonym of the former. C1 Univ Calif San Diego, Div Marine Biol Res, Scripps Inst Oceanog 0208, La Jolla, CA 92093 USA. Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. RP Hastings, PA (reprint author), Univ Calif San Diego, Div Marine Biol Res, Scripps Inst Oceanog 0208, 9500 Gilman Dr, La Jolla, CA 92093 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 14 PY 2002 VL 115 IS 3 BP 543 EP 545 PG 3 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 605NB UT WOS:000178683000004 ER PT J AU Campos, MR Lemaitre, R AF Campos, MR Lemaitre, R TI A new species of freshwater crab of the genus Potamocarcinus H. Milne Edwards, 1853 (Crustacea : Decapoda : Brachyura : Pseudothelphusidae) from Panama SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID MEXICO AB A new species of freshwater crab from Panama of the genus Potamocarcinus H. Milne Edwards, P. lobulatus, is described and illustrated, bringing to 1 l the total number of known species in the genus. The new species is distinguished from other congeners by the morphology of the male first gonopod, especially the presence on the cephalic surface of it prominent and wide distal lobe, and a deep, transverse depression narrowing the spermatic channel. C1 Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, Washington, DC 20560 USA. RP Campos, MR (reprint author), Univ Nacl Colombia, Inst Ciencias Nat, AA 103698, Bogota, Colombia. NR 17 TC 2 Z9 3 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 14 PY 2002 VL 115 IS 3 BP 600 EP 604 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 605NB UT WOS:000178683000010 ER PT J AU Schotte, M AF Schotte, M TI Speocirolana prima, a new species from Tamaulipas, Mexico with a key to known species of the genus (Crustacea : Isopoda : Cirolanidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The twelfth species of Speocirolana is described, distinguished from its cogener S. pubens by the morphology of the male uropods. A key to the known species of the genus is given. A distribution map of species in the genus, known only froth northeastern Mexico, is also presented. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. RP Schotte, M (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. NR 12 TC 2 Z9 3 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 OCT 14 PY 2002 VL 115 IS 3 BP 628 EP 635 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 605NB UT WOS:000178683000014 ER PT J AU Walter, TC Ohtsuka, S Putchakarn, S Pinkaew, K Chullasorn, S AF Walter, TC Ohtsuka, S Putchakarn, S Pinkaew, K Chullasorn, S TI Redescription of two species of Pseudodiaptomus from Asia and Australia (Crustacea : Copepoda : Calanoida : Pseudodiaptomidae) with discussion of the female genital structure and zoogeography of Indo-West Pacific species SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID MORPHOLOGY; AREA; KEY AB Many species of Pseudodiaptomus tire known from the southeast Asia region. An ongoing review of this genus has produced 58 species front the eastern Indian Ocean and western Pacific Ocean coasts. front Japan to Australia. Range extensions for P. ornatus and P. andamanensis are noted for Australia and Japan, and for Thailand respectively. The previously unknown male of P. ornatus and the female genital structure of both species are described; the zoogeography of the genus is discussed. C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. Hiroshima Univ, Fishery Lab, Hiroshima 725, Japan. Burapha Univ, Inst Marine Sci, Chon Buri 20131, Thailand. Rhamkhamhaeng Univ, Dept Biol, Fac Sci, Bangkok 10240, Thailand. RP Walter, TC (reprint author), Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. NR 53 TC 11 Z9 14 U1 0 U2 2 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 OCT 14 PY 2002 VL 115 IS 3 BP 650 EP 669 PG 20 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 605NB UT WOS:000178683000016 ER PT J AU Amaral, FD Broadhurst, MK Cairns, SD Schlenz, E AF Amaral, FD Broadhurst, MK Cairns, SD Schlenz, E TI Skeletal morphometry of Millepora occurring in Brazil, including a previously undescribed species SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID REEF; COELENTERATA; HYDROZOA AB The aims of this study were to identify the species of Millepora occurring in Brazil and compare the skeletal morphology of M. braziliensis from Brazil and M. squarrosa from the Caribbean (to address confusion over their synonymy). One hundred and three colonies of Millepora were collected from various sites along the Brazilian coast. In an attempt to facilitate delineation among species, diameters of the gastropores and dactylopores were compared in addition to other morphological characters. We proposed that the colonies collected from Brazil comprised four species: M. alcicornis (34 colonies), M. braziliensis (45), M. nitida (13), and one previously undescribed species (11). Analyses of variance of the diameters of gastropores and dactylopores among the various species showed considerable intra-specific variability and some inter-specific spatial variation. At the Abrolhos Islands, significant differences were detected between M. alcicornis, M. braziliensis and M. nitida for the mean diameter of the dactylopores, but not the gastropores. In contrast, significant differences in mean diameter of the gastropores were detected between M. braziliensis and M. alcicornis across three other locations. We hypothesized that Caribbean M. squarrosa is a species distinct from M. braziliensis, although the use of molecular systematics may be required to eliminate doubts about their synonymy. C1 Univ Fed Rural Pernambuco, Dept Biol, Area Zool, Lab Ambientaes Recifais, BR-52171030 Recife, PE, Brazil. Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. Univ Sao Paulo, Inst Biociencias, Dept Zool, BR-05422970 Sao Paulo, SP, Brazil. RP Amaral, FD (reprint author), Univ Fed Rural Pernambuco, Dept Biol, Area Zool, Lab Ambientaes Recifais, Av Dom Manuel Medeiros S-N, BR-52171030 Recife, PE, Brazil. RI Amaral, Fernanda/I-2633-2012; Broadhurst, Matt/I-6783-2015 OI Broadhurst, Matt/0000-0003-0184-7249 NR 52 TC 8 Z9 11 U1 0 U2 9 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 OCT 14 PY 2002 VL 115 IS 3 BP 681 EP 695 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 605NB UT WOS:000178683000019 ER PT J AU Wasshaussen, DC AF Wasshaussen, DC TI New species of Ruellia (Acanthaceae) from French Guiana and adjacent Brazil SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Two new species, Ruellia amapensis and R. schnellii, are described, illustrated and compared with their closest relatives. A key to all the known species of Ruellia from the Guianas is also provided. C1 Natl Museum Nat Hist, Dept Systemat Biol Bot, Smithsonian Inst, Washington, DC 20560 USA. RP Wasshaussen, DC (reprint author), Natl Museum Nat Hist, Dept Systemat Biol Bot, Smithsonian Inst, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 14 PY 2002 VL 115 IS 3 BP 696 EP 700 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 605NB UT WOS:000178683000020 ER PT J AU Kochanek, CS AF Kochanek, CS TI What do gravitational lens time delays measure? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; dark matter; distance scale; galaxies : halos; gravitational lensing ID HUBBLE-CONSTANT; MASS MODELS; DARK HALO; Q0957+561; GALAXIES; DEGENERACIES; PG-1115+080; PARAMETER; B1600+434; H-0 AB Gravitational lens time delays depend on the Hubble constant, the observed image positions, and the surface mass density of the lens in the annulus between the images. Simple time delay lenses like PG 1115+80, SBS 1520+530, B1600+434, PKS 1830-211, and HE 2149-2745 have H-0 = A(1 - [kappa]) + B[kappa](eta - 1), where the two coefficients A similar or equal to 90 km s(-1) Mpc(-1) and B similar or equal to 10 km s(-1) Mpc(-1) depend on the measured delays and the observed image positions, [kappa] is the mean surface density in the annulus between the images, and there is a small correction from the logarithmic slope eta similar or equal to 2 of the density profile, kappa proportional to R1-eta, in the annulus. These five systems are very homogeneous since for fixed H-0 = 100 h km s(-1) Mpc(-1) they must have the same surface density, [kappa] = 1.11 - 1.22 h +/- 0.04, with an upper bound sigma(kappa) < 0.07 on any dispersion in [κ] beyond those due to the measurement errors. If the lenses have their expected dark halos, [κ] &SIME; 0.5 and H0 &SIME; 51 +/- 5 km s(-1) Mpc(-1), while if they have constant mass-to-light ratios, [κ] &SIME; 0.1-0.2 and H-0 &SIME; 73 +/- 8 km s(-1) Mpc(-1). More complicated lenses with multiple components or strong perturbations from nearby clusters, like RX J0911+0551 and Q0957+561, are easily recognized because they have significantly different coefficients. 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, Cambridge, MA 02138 USA. NR 55 TC 110 Z9 110 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 OCT 10 PY 2002 VL 578 IS 1 BP 25 EP 32 DI 10.1086/342476 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500003 ER PT J AU Harris, DE Krawczynski, H Taylor, GB AF Harris, DE Krawczynski, H Taylor, GB TI X-ray detection of the inner jet in the radio galaxy 3C 129 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (3C 129); galaxies : jets; radiation mechanisms : nonthermal radio continuum : galaxies; X-rays : galaxies ID CLUSTER; 3C-129 AB During the course of an investigation of the interaction of the radio galaxy 3C 129 and its ambient cluster gas, we found excess X-ray emission aligned with the northern radio jet. The emission extends from the weak X-ray core of the host galaxy approximate to2."5 to the first resolved radio knot. On a smaller scale, we have also detected a weak radio extension in the same position angle with the VLBA. 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 3C 129 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. Yale Univ, New Haven, CT 06520 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Harris, DE (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 13 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 OCT 10 PY 2002 VL 578 IS 1 BP 60 EP 63 DI 10.1086/342346 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500006 ER PT J AU Romano, P Mathur, S Pogge, RW Peterson, BM Kuraszkiewicz, J AF Romano, P Mathur, S Pogge, RW Peterson, BM Kuraszkiewicz, J TI Far-Ultraviolet Spectroscopic Explorer Observations of the narrow-line Seyfert 1 galaxy Arakelian 564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Arakelian 564) galaxies : nuclei; galaxies : Seyfert; ultraviolet : galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY; ABSORPTION-LINES; VARIABILITY; SPECTRUM; IONIZATION; COMPONENTS; EMISSION; NGC-5548; ABSORBER AB We present a 63 ks FUSE observation of the narrow-line Seyfert 1 galaxy Arakelian 564. The spectrum is dominated by the strong emission in the O VI lambdalambda1032, 1038 resonance doublet. Strong, heavily saturated absorption troughs due to Lyman series of hydrogen, O VI and C III lambda977 at velocities near the systemic redshift of Ark 564 are also observed. We used the column densities of O VI and C III in conjunction with the published column densities of species observed in the UV and X-ray bands, to derive constraints on the physical parameters of the absorber through photoionization modeling. The available data suggest that the UV and X-ray absorbers in Ark 564 are physically related and possibly identical. The combination of constraints indicates that the absorber is characterized by a narrow range in total column density N-H and U, centered at log N-H approximate to 21 and log U approximate to -1.5, and may be spatially extended along the line of sight. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romano, P (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. NR 44 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 OCT 10 PY 2002 VL 578 IS 1 BP 64 EP 73 DI 10.1086/342403 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500007 ER PT J AU Finoguenov, A Jones, C Bohringer, H Ponman, TJ AF Finoguenov, A Jones, C Bohringer, H Ponman, TJ TI ASCA observations of groups at radii of low overdensity: Implications for the cosmic preheating SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general galaxies : evolution; intergalactic medium; supernovae : general; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; EARLY-TYPE GALAXIES; ROSAT PSPC OBSERVATIONS; ACTIVE GALACTIC NUCLEI; HYDRA-A CLUSTER; INTRACLUSTER MEDIUM; RICH CLUSTERS; ELEMENTAL ABUNDANCES; INTERGALACTIC MEDIUM; ELLIPTIC GALAXIES AB Through a three-dimensional modeling of ASCA observations, we performed a spatially resolved X-ray spectroscopic study, extending to radii exceeding 150 kpc, for a sample of nine groups of galaxies. Combined with published ROSAT results, we conclude that these systems generally exhibit a strong temperature decline at outer radii. In our best case, NGC 3268, this corresponds to a flattening of the entropy pro le at a level of similar to400 keV cm(2). This value is high compared both to the observed entropy floor of similar to100 keV cm(2) and to the expected value from gravitational heating. We suggest that the observed entropy profile in most groups at densities exceeding 500 times the critical is driven purely by nongravitational heating processes. After comparison with a larger sample of groups and clusters, we conclude that there is a variation in the level of nongravitational heating between similar to100 and similar to400 keV cm(2) within every system. Using models of cluster formation as a reference frame, we established that the accreted gas reaches an entropy level of 400 keV cm(2) by redshift 2.0-2.5, while such high entropies where not present at redshifts higher than 2.8-3.5, favoring nearly instantaneous preheating. Adopting galactic winds as a source of preheating and scaling the released energy by the observed metal abundance, the variation in the preheating could be ascribed mostly to variation in the typical overdensity of the energy injection, from 30 for an entropy floor of 100 keV cm(2) to similar to5 for an entropy of 400 keV cm(2). C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Finoguenov, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. NR 87 TC 52 Z9 52 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2002 VL 578 IS 1 BP 74 EP 89 DI 10.1086/342472 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500008 ER PT J AU Kaaret, P AF Kaaret, P TI A Chandra high resolution camera observation of X-ray point sources in M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31, NGC 224) galaxies : spiral; X-rays : binaries; X-rays : galaxies; X-rays : general ID HUBBLE-SPACE-TELESCOPE; GLOBULAR-CLUSTERS; CENTRAL REGION; BINARIES; GALAXIES; PHOTOMETRY; ASTRONOMY; SEARCHES; ROSAT AB We present results from a 47 ks observation of the Andromeda galaxy, M31, using the High Resolution Camera of the Chandra X-Ray Observatory. We detect 142 point sources spanning 3 orders of magnitude in luminosity, from L-X = 2 x 10(35) to 2 x 10(38) ergs s(-1) in the 0.1-10 keV band. The X-ray source location accuracy is better than 1" in the central regions of the galaxy. One source lies within 1."3 of SN 1885 but does not coincide with the UV absorption feature identified as the supernova remnant. However, there is an optical transient, which is likely an optical nova, at the location of the X-ray source. There is a weak source, L-X similar to 4 x 10(36) ergs cm(-2) s(-1), coincident with the nucleus of M31 and 14 sources coincident with globular clusters. Our observation has very high efficiency down to luminosities of 1.5 x 10(36) ergs s(-1) for sources within 5' of the nucleus. Comparing with a ROSAT observation made 11 yr earlier, we find that 0.46 +/- 0.26 of the sources with L-X > 5 x 10(36) ergs s(-1) are variable. We find no evidence for X-ray pulsars in this region, indicating that the population is likely dominated by low-mass X-ray binaries. The source density radial pro le follows a power-law distribution with an exponent of 1.25 +/- 0.10 and is inconsistent with the optical surface brightness profile. The X-ray point-source luminosity function is well fitted by a differential broken power law with a break at a luminosity of (4.5(-2.2)(+11)) x 10(37) ergs s(-1). The luminosity function is consistent with a model of an aging population of X-ray binaries. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 49 TC 67 Z9 67 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 OCT 10 PY 2002 VL 578 IS 1 BP 114 EP 125 DI 10.1086/342475 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500012 ER PT J AU McClure-Griffiths, NM Dickey, JM Gaensler, BM Green, AJ AF McClure-Griffiths, NM Dickey, JM Gaensler, BM Green, AJ TI The Galactic distribution of large HI shells SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : kinematics and dynamics Galaxy : structure; ISM : bubbles; ISM : structure; radio lines : ISM ID INTERSTELLAR-MEDIUM; SPIRAL STRUCTURE; STAR-FORMATION; MILKY-WAY; I SHELLS; SUPERNOVA-REMNANTS; SCALE STRUCTURES; OB ASSOCIATIONS; PLANE SURVEY; HOLMBERG-II AB We report the discovery of 19 new H I shells in the Southern Galactic Plane Survey (SGPS). These shells, which range in radius from 40 pc to 1 kpc, were found in the low-resolution Parkes portion of the SGPS data set covering Galactic longitudes l = 253degrees to l = 358degrees. Here we give the properties of individual shells, including positions, physical dimensions, energetics, masses, and possible associations. We also examine the distribution of these shells in the Milky Way and find that several of the shells are located between the spiral arms of the Galaxy. We offer possible explanations for this effect, in particular, that the density gradient away from spiral arms, combined with the many generations of sequential star formation required to create large shells, could lead to a preferential placement of shells on the trailing edges of spiral arms. Spiral density wave theory is used in order to derive the magnitude of the density gradient behind spiral arms. We find that the density gradient away from spiral arms is comparable to that out of the Galactic plane and therefore suggest that this may lead to exaggerated shell expansion away from spiral arms and into interarm regions. C1 CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Dept Astrophys, Sydney, NSW 2006, Australia. RP McClure-Griffiths, NM (reprint author), CSIRO, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Dickey, John/0000-0002-6300-7459; Gaensler, Bryan/0000-0002-3382-9558 NR 57 TC 78 Z9 79 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 OCT 10 PY 2002 VL 578 IS 1 BP 176 EP 193 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500016 ER PT J AU Wargelin, BJ Drake, JJ AF Wargelin, BJ Drake, JJ TI Stringent X-ray constraints on mass loss from Proxima Centauri SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : coronae; stars : individual (Proxima Centauri); stars : late-type; stars : mass loss; X-rays : stars ID HUBBLE-SPACE-TELESCOPE; LOCAL INTERSTELLAR-MEDIUM; BINARY V471 TAURI; SOLAR-WIND; CHARGE-EXCHANGE; LAMBDA-ANDROMEDAE; ALPHA-CENTAURI; CROSS-SECTIONS; STELLAR WINDS; EPSILON-INDI AB We have analyzed data from two Chandra imaging observations of Proxima Centauri, searching for an Xray halo arising from charge exchange between highly charged ions in its stellar wind and neutral gas in the surrounding interstellar medium. Based upon our model of Proxima Cen's charge exchange emission, the absence of any detectable charge exchange signal places a statistical 3 upper limit of similar to3 x 10(13) M. yr(-1) (14 (M) over dot .) on the mass-loss rate (9 (M) over dot . for the 2 sigma limit and 4 (M) over dot . for 1 sigma), with a model uncertainty of roughly a factor of 3. This is orders of magnitude smaller than the upper limits that have been placed on late-type dwarf stars using radio observations, and it supports a recent mass-loss result for Proxima Cen based on Lyalpha absorption profiles. We have also studied the coronal spectrum, both in quiescence and during a prominent flare. Results are consistent with those obtained in previous X-ray observations, but a firm determination of coronal metal abundances remains elusive. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Wargelin, BJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 63 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 OCT 10 PY 2002 VL 578 IS 1 BP 503 EP 514 DI 10.1086/342270 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500043 ER PT J AU Longcope, DW Van Ballegooijen, AA AF Longcope, DW Van Ballegooijen, AA TI A three-dimensional dynamical model of current sheet formation in a coronal loop SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; Sun : corona; Sun : magnetic fields ID FREE MAGNETIC-FIELDS; FLUX-TUBES; SOLAR CORONA; RECONNECTION; TOPOLOGY; ELEMENTS; MAGNETOHYDRODYNAMICS AB We develop a three-dimensional model for the time evolution of a slender coronal loop anchored in multiple isolated photospheric flux elements. As a result of the composite photospheric boundaries, the coronal field comprises multiple flux domains. The model shows that motion at the footpoints results in current singularities developing along separators between domains. Motion at one end of the loop creates a nonsingular Alfvenic pulse. Repeated reflections from the complex photospheric boundaries change the pulse's current into a surface singularity traveling along the separator ribbon. Final relaxation leads to an equilibrium that is current-free within all of the coronal domains and contains a separator current sheet. The relation of the equilibrium current to the footpoint displacements confirms previous quasi-static models of three-dimensional separator current sheets. C1 Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Longcope, DW (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. NR 32 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2002 VL 578 IS 1 BP 573 EP 589 DI 10.1086/342399 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500049 ER PT J AU Reeves, KK Warren, HP AF Reeves, KK Warren, HP TI Modeling the cooling of postflare loops SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : flares; Sun : X-rays, gamma rays ID POST-FLARE LOOPS; X-RAY FLARES; 26 JUNE 1992; TRANSITION REGION; CORONAL EXPLORER; SOLAR-FLARES; MAGNETIC RECONNECTION; YOHKOH OBSERVATIONS; FINE-STRUCTURE; TEMPERATURE AB We present a model for the cooling of post are loops. In our model, we form an arcade that consists of hundreds of loops with offset formation times to simulate a rising reconnection site. An initial temperature and density is assumed in each loop, and then the scaling laws of Cargill, Mariska, & Antiochos are used to determine the evolution of the temperature and density in the loop. Once these quantities are found, they are passed through the instrument response functions for TRACE and the Yohkoh Soft X-Ray Telescope (SXT) to obtain intensities, which are integrated over the arcade to give a simulated light curve. This light curve is then compared to observed light curves from the 2000 July 14 X6 flare. We find that this multiloop, multithermal approach to simulating the are cooling fits the observed data much better than a single-loop model. There are some discrepancies between our simulations and the observed data in the decay phase of the are, however, which may be due to residual late-phase heating. We also find that the temperatures calculated by using SXT filter ratios are generally lower than the initial loop temperatures needed in the simulation to give a good fit to the observed data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. RI Reeves, Katharine/P-9163-2014 NR 45 TC 48 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 OCT 10 PY 2002 VL 578 IS 1 BP 590 EP 597 DI 10.1086/342310 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500050 ER PT J AU Lepson, JK Beiersdorfer, P Brown, GV Liedahl, DA Utter, SB Brickhouse, NS Dupree, AK Kaastra, JS Mewe, R Kahn, SM AF Lepson, JK Beiersdorfer, P Brown, GV Liedahl, DA Utter, SB Brickhouse, NS Dupree, AK Kaastra, JS Mewe, R Kahn, SM TI Emission lines of Fe VII-Fe X in the extreme ultraviolet region, 60-140 angstrom SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : identification; methods : analytical; methods : laboratory; stars : coronae; ultraviolet : stars ID STELLAR CORONAL ABUNDANCES; COOL STARS; EUV SPECTROSCOPY; ALPHA-CENTAURI; SPECTRUM; PLASMAS AB We report on emission spectra of iron in the extreme ultraviolet recorded at an electron density of similar to5 x 10(11) cm(-3) at the Lawrence Livermore electron beam ion trap EBIT-II. We present a summary of observed emission lines, including wavelengths and emission intensities. We also illustrate our technique for isolating pure charge states of the desired ion and present spectra of pure Fe VII-Fe X. Our measurements add a large number of newly identified lines to existing line lists in the extreme-ultraviolet region, 60-140 Angstrom. While many of these lines are quite weak, they add up to a significant flux that can seriously affect interpretations of global fitting models, especially when applied to stars with material at the appropriate temperatures, such as Procyon, alpha Cen, and the Sun. C1 Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Lawrence Livermore Natl Lab, Div High Temp Phys, Livermore, CA 94550 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Columbia Univ, Dept Phys, New York, NY 10027 USA. RP Lepson, JK (reprint author), Univ Calif Berkeley, Space Sci Lab, Grizzly Peak & Centennial Dr, Berkeley, CA 94720 USA. NR 22 TC 48 Z9 48 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 OCT 10 PY 2002 VL 578 IS 1 BP 648 EP 656 DI 10.1086/342274 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XH UT WOS:000178301500054 ER PT J AU Greiner, J Di Stefano, R AF Greiner, J Di Stefano, R TI Chandra observations of the recurrent nova CI Aquilae after its 2000 April outburst SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; novae, cataclysmic variables; stars : individual (CI Aquilae); X-rays : stars ID ACCRETING WHITE-DWARFS; X-RAY-EMISSION; U-SCORPII; MODEL AB We report the results of two Chandra observations of the recurrent nova CI Aql at 14 and 16 months after its outburst in 2000 April. The X-ray emission is faint in both cases, without any noticeable change in spectrum or intensity. Although the emission is very soft, it is not luminous enough to be due to late-time H burning. This implies that the luminous supersoft phase ended even before the time predicted by the most recent calculations. The details of the X-ray spectrum, together with the fact that the observed X-ray intensity is brighter than preoutburst (1992/1993), suggest that the observed X-ray emission is either due to ionization of the circumstellar material or due to the shocks within the wind and/or with the surrounding medium. C1 Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Greiner, J (reprint author), Astrophys Inst Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. NR 26 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 OCT 10 PY 2002 VL 578 IS 1 BP L59 EP L62 DI 10.1086/344565 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598XQ UT WOS:000178302200014 ER PT J AU Chae, KH Biggs, AD Blandford, RD Browne, IWA de Bruyn, AG Fassnacht, CD Helbig, P Jackson, NJ King, LJ Koopmans, LVE Mao, S Marlow, DR McKean, JP Myers, ST Norbury, M Pearson, TJ Phillips, PM Readhead, ACS Rusin, D Sykes, CM Wilkinson, PN Xanthopoulos, E York, T AF Chae, KH Biggs, AD Blandford, RD Browne, IWA de Bruyn, AG Fassnacht, CD Helbig, P Jackson, NJ King, LJ Koopmans, LVE Mao, S Marlow, DR McKean, JP Myers, ST Norbury, M Pearson, TJ Phillips, PM Readhead, ACS Rusin, D Sykes, CM Wilkinson, PN Xanthopoulos, E York, T TI Constraints on cosmological parameters from the analysis of the Cosmic Lens All Sky Survey radio-selected gravitational lens statistics SO PHYSICAL REVIEW LETTERS LA English DT Article ID LUMINOSITY FUNCTION; COMMISSIONING DATA; SUPERNOVAE; GALAXIES; CONSTANT; UNIVERSE AB We derive constraints on cosmological parameters and the properties of the lensing galaxies from gravitational lens statistics based on the final Cosmic Lens All Sky Survey data. For a flat universe with a classical cosmological constant, we find that the present matter fraction of the critical density is Omega(m)=0.31(-0.14)(+0.27) (68%)(-0.10)(+0.12) (syst). For a flat universe with a constant equation of state for dark energy w=p(x)(pressure)/rho(x)(energy density), we find w<-0.55(-0.11)(+0.18) (68%). C1 Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. CALTECH, Pasadena, CA 91125 USA. Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Bonn, D-53121 Bonn, Germany. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chae, KH (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; Helbig, Phillip/0000-0003-3637-0057 NR 28 TC 77 Z9 77 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 OCT 7 PY 2002 VL 89 IS 15 AR 151301 DI 10.1103/PhysRevLett.89.151301 PG 4 WC Physics, Multidisciplinary SC Physics GA 596ZC UT WOS:000178195500006 PM 12365978 ER PT J AU Eggert, LS Rasner, CA Woodruff, DS AF Eggert, LS Rasner, CA Woodruff, DS TI The evolution and phylogeography of the African elephant inferred from mitochondrial DNA sequence and nuclear microsatellite markers SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE forest elephant; savannah elephant; mammal evolution; molecular scatology; speciation ID ASIAN ELEPHANT; POPULATIONS; DIVERGENCE; SENSITIVITY; GENOTYPES; MAXIMUS; EASTERN; LOCI AB Recent genetic results support the recognition of two African elephant species: Loxodonta africana, the savannah elephant, and Loxodonta cyclotis, the forest elephant. The study, however, did not include the populations of West Africa, where the taxonomic affinities of elephants have been much debated. We examined mitochondrial cytochrome b control region sequences and four microsatellite loci to investigate the genetic differences between the forest and savannah elephants of West and Central Africa. We then combined our data with published control region sequences from across Africa to examine patterns at the continental level. Our analysis reveals several deeply divergent lineages that do not correspond with the currently recognized taxonomy: (i) the forest elephants of Central Africa-, (ii) the forest and savannah elephants of West Africa; and (iii) the savannah elephants of eastern, southern and Central Africa. We propose that the complex phylogeographic patterns we detect in African elephants result from repeated continental-scale climatic changes over their five-to-six million year evolutionary history. Until there is consensus on the taxonomy, we suggest that the genetic and ecological distinctness of these lineages should be an important factor in conservation management planning. C1 Univ Calif San Diego, Div Biol, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA. RP Eggert, LS (reprint author), Smithsonian Inst, Genet Mol Lab, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM eggertl@nmnh.si.edu NR 65 TC 86 Z9 92 U1 9 U2 52 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD OCT 7 PY 2002 VL 269 IS 1504 BP 1993 EP 2006 DI 10.1098/rspb.2002.2070 PG 14 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 604AN UT WOS:000178593600005 PM 12396498 ER PT J AU Corbel, S Fender, RP Tzioumis, AK Tomsick, JA Orosz, JA Miller, JM Wijnands, R Kaaret, P AF Corbel, S Fender, RP Tzioumis, AK Tomsick, JA Orosz, JA Miller, JM Wijnands, R Kaaret, P TI Large-scale, decelerating, relativistic X-ray jets from the microquasar XTE J1550-564 SO SCIENCE LA English DT Article ID ASCA OBSERVATIONS; RADIO; SS-433; SYSTEM; STATES; GALAXY; ROSAT AB We have detected, at x-ray and radio wavelengths, large-scale moving jets from the microquasar XTE J1550-564. Plasma ejected from near the black hole traveled at relativistic velocities for at least 4 years. We present direct evidence for gradual deceleration in a relativistic jet. The broadband spectrum of the jets is consistent with synchrotron emission from high-energy (up to 10 tera-electron volts) particles that were accelerated in the shock waves formed within the relativistic ejecta or by the interaction of the jets with the interstellar medium. XTE J1550-564 offers a rare opportunity to study the dynamical evolution of relativistic jets on time scales inaccessible for active galactic nuclei jets, with implications for our understanding of relativistic jets from Galactic x-ray binaries and active galactic nuclei. C1 Univ Paris 07, F-75221 Paris 05, France. Ctr Etud Saclay, CEA, Serv Astrophys, 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. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Corbel, S (reprint author), Univ Paris 07, F-75221 Paris 05, France. NR 34 TC 168 Z9 169 U1 0 U2 2 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 OCT 4 PY 2002 VL 298 IS 5591 BP 196 EP 199 DI 10.1126/science.1075857 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 600BJ UT WOS:000178370500057 PM 12364800 ER PT J AU Kress, WJ Prince, LM Williams, KJ AF Kress, WJ Prince, LM Williams, KJ TI The phylogeny and a new classification of the gingers (Zingiberaceae): Evidence from molecular data SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE classificatiom gingers; ITS; matK; phylogeny; tropical; Zingiberaceae; Zingiberales ID GENUS; SEQUENCES; BORNEO; TREES; MATK AB The pantropical Zingiberaceae is the largest family in the order Zingiberales with 53 genera and over 1200 species. Classifications of the family first proposed in 1889 and refined by others since that time recognize four tribes (Globbeae, Hedychieae, Alpinieae, and Zingibereae) based on morphological features, such as number of locules and placentation in the ovary, development of staminodia, modifications of the fertile anther, and rhizome-shoot-leaf orientation. New phylogenetic analyses based on DNA sequences of the nuclear internal transcribed spacer (ITS) and plastid matK regions suggest that at least some of these morphological traits are homoplasious and three of the tribes are paraphyletic, The African genus Siphonochilus and Bornean genus Tamijia are basal clades. The former Alpinieae and Hedychieae for the most part are monophyletic taxa with the Globbeae and Zingibereae included within the latter, The results of these phylogenetic investigations are used to propose a new classification of the Zingiberaceae that recognizes four subfamilies and four tribes: Siphonochiloideae (Siphonochileae), Tamijioideae (Tamijieae), Alpinioideae (Alpinieae, Riedelieae), and Zingiberoideae (Zingibereae, Globbeae). Morphological features congruent with this classification and the taxonomic status of various monotypic genera are discussed. C1 Smithsonian Inst, US Natl Herbarium, Natl Museum Nat Hist, Washington, DC 20013 USA. Duke Univ, Dept Biol, Durham, NC 27708 USA. RP Kress, WJ (reprint author), Smithsonian Inst, US Natl Herbarium, Natl Museum Nat Hist, MRC-166,POB 37012, Washington, DC 20013 USA. NR 58 TC 136 Z9 184 U1 4 U2 17 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 OCT PY 2002 VL 89 IS 10 BP 1682 EP 1696 DI 10.3732/ajb.89.10.1682 PG 15 WC Plant Sciences SC Plant Sciences GA 683DH UT WOS:000183131800014 PM 21665595 ER PT J AU Pasachoff, JM AF Pasachoff, JM TI Haystack radio telescope SO AMERICAN JOURNAL OF PHYSICS LA English DT Letter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Williams Coll, Hopkins Observ, Williamstown, MA 02167 USA. RP Pasachoff, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC PHYSICS TEACHERS AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0002-9505 J9 AM J PHYS JI Am. J. Phys. PD OCT PY 2002 VL 70 IS 10 BP 983 EP 983 DI 10.1119/1.1498892 PG 1 WC Education, Scientific Disciplines; Physics, Multidisciplinary SC Education & Educational Research; Physics GA 595KJ UT WOS:000178107800002 ER PT J AU Mueller, UG AF Mueller, UG TI Ant versus fungus versus mutualism: Ant-cultivar conflict and the deconstruction of the attine ant-fungus symbiosis SO AMERICAN NATURALIST LA English DT Review DE attine ants; conflict; cooperation; fungiculture; mutualism; symbiosis ID LEAF-CUTTING ANT; ATTA-CEPHALOTES L; GROWING ANTS; SEX-RATIO; ACROMYRMEX-OCTOSPINOSUS; DIET SELECTION; LIVE NEST; EVOLUTION; FORMICIDAE; HYMENOPTERA AB A century of research on fungus-growing ants (Attini, Formicidae) has ignored the cultivated fungi as passive domesticates and viewed the attine fungicultural symbiosis as an integrated unit dominated by the evolutionary interests of the ant farmers. This article takes a different perspective and explores first the evolutionary interests and leverages of the fungal cultivars, then dissects eight potential evolutionary conflicts between ants and cultivars. Three types of antcultivar conflict are examined in depth. First, ant-cultivar conflict over the ant sex ratio is predicted because the cultivars are dispersed by female foundresses but not by males; cultivars thus may be selected to bias the ant sex ratio toward females. Second, ant-cultivar conflict over fungal sexual reproduction exists if the fungi are able to escape from the symbiosis and live independently, as is implied by phylogenetic analyses of the fungi; this conflict is exacerbated in colonies that experience queen death or senescence. A literature review reveals that sexual fruiting of attine cultivars is more common than has been traditionally realized and often occurs in moribund colonies. Third, the routine transplanting of fungal mycelium by ants could generate, through sensory-biased symbiont choice, selection favoring fungal features that increase the likelihood of transplantation within nests (symbiont drive) but that are detrimental to the survival of the whole colony. A balanced perspective incorporating both ant and fungal interests emerges as a more appropriate framework than the traditional myrmicocentric perspective. Indeed, the attine symbiosis offers unique experimental opportunities (cultivar switch experiments) to unravel the evolutionary dynamics of conflict and cooperation between ant and fungal partners. C1 Univ Texas, Sect Integrat Biol, Patterson Labs, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Mueller, UG (reprint author), Univ Texas, Sect Integrat Biol, Patterson Labs, Austin, TX 78712 USA. NR 165 TC 86 Z9 88 U1 2 U2 31 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD OCT PY 2002 VL 160 SU S BP S67 EP S98 DI 10.1086/342084 PG 32 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 604HQ UT WOS:000178613600006 PM 18707454 ER PT J AU Zotz, G Reichling, P Valladares, F AF Zotz, G Reichling, P Valladares, F TI A simulation study on the importance of size-related changes in leaf morphology and physiology for carbon gain in an epiphytic bromeliad SO ANNALS OF BOTANY LA English DT Article DE crown architecture; ecophysiology; epiphytes; light capture; modelling; photosynthesis; plant size; scaling; Vriesea sanguinolenta(4) ID CROWN ARCHITECTURE MODEL; LIGHT INTERCEPTION; PLANT SIZE; HETEROMELES ARBUTIFOLIA; SHADE PLANTS; PHOTOSYNTHESIS; CAPTURE; CONSEQUENCES; WATER; SUN AB This study addresses the question of how size-related changes in leaf morphology and physiology influence light absorption and carbon gain of the epiphytic bromeliad Vriesea sanguinolenta. A geometrically based computer model, Y-plant. was used for the three-dimensional reconstruction of entire plants and for calculation of whole plant light interception and carbon gain, Plants of different sizes were reconstructed, and morphological and physiological attributes of young and old leaves. and small and large plants were combined to examine the individual effects of each factor on light absorption and carbon gain of the plant, The influence of phyllotaxis on light absorption was also explored. Departure of measured divergence angles between successive leaves from the ideal 137.5degrees slightly decreased light absorption. The only morphological parameter that consistently changed with plant size was leaf shape: larger plants produced more slender foliage. which substantially reduced self-shading. Nevertheless. self-shading increased with plant size. While the maximum rate of net CO2 uptake of leaves increased linearly with plant size by a factor of two from the smallest to the largest individual, the potential plant carbon gain (based on total foliage area) showed a curvilinear relationship. but with similar numerical variation. We conclude that leaf physiology has a greater impact on plant carbon gain than leaf and plant morphology in this epiphytic bromeliad. (C) 2002 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-8700 Wurzburg, Germany. CSIC, Ctr Ciencias Medioambientales, E-28006 Madrid, Spain. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. RI Valladares, Fernando/K-9406-2014 OI Valladares, Fernando/0000-0002-5374-4682 NR 37 TC 14 Z9 15 U1 0 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 OCT PY 2002 VL 90 IS 4 BP 437 EP 443 DI 10.1093/mcf208 PG 7 WC Plant Sciences SC Plant Sciences GA 603ZG UT WOS:000178590700002 PM 12324266 ER PT J AU Warner, DJ AF Warner, DJ TI Political geodesy: the Army, the Air Force, and the World Geodetic System of 1960 SO ANNALS OF SCIENCE LA English DT Review AB Since military planners must know the size and shape of the earth if they hope to track earth-orbiting satellites and to target missiles on distant lands, geodesy was an important concern of the two superpowers during the Cold War. The most important geodetic product in the United States was a series of increasingly powerful World Geodetic Systems, the first of which ( WGS 60) was published for the Department of Defense in 1960. Although WGS 60 was created because of intense international rivalries, it reflected the intense rivalries between America's Army and its Air Force, and it introduced the notion of 'political geodesy'. My attention to American events does not indicate a lack of interest in the Soviet story; rather, I hope that historians with better language skills and better access to Soviet documents will examine geodetic research on the other side of the former Iron Curtain. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Warner, DJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 123 TC 5 Z9 5 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0003-3790 J9 ANN SCI JI Ann. Sci. PD OCT PY 2002 VL 59 IS 4 BP 363 EP 389 DI 10.1080/0003790110044756 PG 27 WC History & Philosophy Of Science SC History & Philosophy of Science GA 591AY UT WOS:000177858600002 ER PT J AU Balog, Z Kenyon, SJ AF Balog, Z Kenyon, SJ TI Spectroscopic survey of the galactic open cluster NGC 6871. I. New emission-line stars SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 6871); stars : emission line, Be ID T-TAURI STARS; NORTHERN MILKY-WAY; INTERSTELLAR EXTINCTION; OB ASSOCIATIONS; YOUNG STARS; LOW-MASS; EVOLUTION; DISKS; CLASSIFICATION; ACCRETION AB We analyze spectra of 44 emission-line stars detected in a low-resolution optical spectroscopic survey of the galactic open cluster NGC 6871. The survey of 1217 stars is complete to V=14.9 and includes stars with V<16.5 between the zero-age main sequence and the 10(7) yr pre-main-sequence (PMS) isochrone. Of the 44 emission-line stars in this survey, 28 show obvious emission in Hα and 16 have weak Hα absorption (compared with Hγ). We use the reddening to separate foreground and background stars from the cluster members; the position in the HR diagram or the presence of forbidden emission lines ([N II] and [S II]) then yields the evolutionary status of the emission-line stars. A comparison of the Hα spectral index distribution in NGC 6871 with the distribution of young stars in the Taurus-Auriga molecular cloud indicates that the late-type PMS stars in our sample may be weak-line T Tauri stars. Many of these stars show [S II] ( 36%) and [N II] (45%) emission. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Balog, Z (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 45 TC 6 Z9 6 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 OCT PY 2002 VL 124 IS 4 BP 2083 EP 2092 DI 10.1086/342938 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 596BF UT WOS:000178143400020 ER PT J AU Patnaude, DJ Fesen, RA Raymond, JC Levenson, NA Graham, JR Wallace, DJ AF Patnaude, DJ Fesen, RA Raymond, JC Levenson, NA Graham, JR Wallace, DJ TI An isolated, recently shocked ISM cloud in the Cygnus Loop supernova remnant SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : individual (Cygnus Loop); ISM : kinematics and dynamics; supernova remnants ID X-RAY; OPTICAL-EMISSION; INTERSTELLAR CLOUDS; EINSTEIN OBSERVATIONS; BLAST WAVE; ROSAT PSPC; ULTRAVIOLET; DYNAMICS; NOVA AB Spatially resolved ROSAT X-ray and ground-based optical data for the southwestern region of the Cygnus Loop supernova remnant (SNR) reveal in unprecedented detail the very early stages of a blast-wave interaction with an isolated interstellar cloud. Numerous internal cloud shock fronts near the upstream flow and along the cloud edges are visible optically as sharp laments of enhanced Halpha emission. Faint X-ray emission is seen along a line of Balmer-dominated shock laments north and south of the cloud with an estimated X-ray gas temperature of 1.2 x 10(6) K (0.11 keV), corresponding to a shock velocity of 290 km s(-1). The main cloud body itself exhibits little or no X-ray flux. Instead, X-ray emission is confined along the northern and southernmost cloud edges, with the emission brightest in the downstream regions farthest from the shock front's current position. We estimate an interaction age of similar to1200 yr, based on the observed shock-cloud morphology. Overall, the optical and X-ray properties of this shocked interstellar medium (ISM) cloud show many of the principal features predicted for a young SNR shock ISM cloud interaction. In particular, one sees shocklet formation and diffraction inside the inhomogenous cloud, along with partial main blast-wave engulfment. However, several significant differences from model predictions are also present, including no evidence for turbulence along cloud edges, diffuse rather than filamentary [O III] emission within the main body of the cloud, unusually strong downstream [S II] emission in the postshock cloud regions, and confinement of X-ray emission to the cloud's outer boundaries. C1 Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Kentucky, Dept Phys & Astron, Lexington, KY 40507 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. RP Patnaude, DJ (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. NR 36 TC 24 Z9 24 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2002 VL 124 IS 4 BP 2118 EP 2134 DI 10.1086/342537 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 596BF UT WOS:000178143400023 ER PT J AU Racca, G Gomez, M Kenyon, SJ AF Racca, G Gomez, M Kenyon, SJ TI A near-infrared imaging survey of Coalsack Globule 2 SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; ISM : globules; ISM : individual (Coalsack); stars : formation; stars : pre-main-sequence ID SOUTHERN COALSACK; DARK CLOUDS; INTERSTELLAR EXTINCTION; PROTOSTELLAR COLLAPSE; MOLECULAR CLOUDS; BIPOLAR OUTFLOW; STANDARD STARS; BOK GLOBULES; LOW-MASS; B335 AB We describe a near-infrared imaging survey of Globule 2 in the Coalsack. This Bok globule is the highest-density region of this southern hemisphere molecular cloud and is the most likely location for young stars in this complex. The survey is complete for K < 14.0, H < 14.5, and J < 15.5, several magnitudes more sensitive than previous observations of this globule. From the large number of background stars, we derive an accurate near-infrared extinction law for the cloud. Our result, EJ-H/EH-K = 2.08 +/- 0.03, is significantly steeper than results for other southern clouds. We use the J-H/H-K color-color diagram to identify two potential young stars with K < 14.0 in the region. We apply H-band star counts to derive the density pro le of Coalsack Globule 2 and use a polytropic model to describe the internal structure of this small cloud. For a gas temperature T similar to 15 K, this globule is moderately unstable. C1 Observ Astron, RA-5000 Cordoba, Argentina. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Nacl Cordoba, Fac Matemat Astron & Fis, RA-5000 Cordoba, Argentina. RP Observ Astron, Laprida 854, RA-5000 Cordoba, Argentina. EM german@oac.uncor.edu; mercedes@oac.uncor.edu; skenyon@cfa.harvard.edu RI Racca, German/K-4798-2012; OI Kenyon, Scott/0000-0003-0214-609X NR 52 TC 30 Z9 30 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2002 VL 124 IS 4 BP 2178 EP 2184 DI 10.1086/342738 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 596BF UT WOS:000178143400028 ER PT J AU Greene, TP Lada, CJ AF Greene, TP Lada, CJ TI Spectroscopic detection of a stellar-like photosphere in an accreting protostar SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared radiation; stars : atmospheres; stars : formation; stars : rotation; techniques : spectroscopic ID RHO-OPHIUCHI CLOUD; MAIN-SEQUENCE STARS; NEAR-INFRARED SPECTRA; T-TAURI STARS; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; YOUNG STARS; LOW-MASS; OBJECTS; DISKS; ROTATION AB We present high-resolution (R similar or equal to 18,000), high signal-to-noise 2 mum spectra of two luminous, X-ray flaring Class I protostars in the rho Ophiuchi cloud acquired with the NIRSPEC spectrograph of the Keck II telescope. We present the first spectrum of a highly veiled, strongly accreting protostar, which shows photospheric absorption features and demonstrates the stellar nature of its central core. We find the spectrum of the luminous (L-bol = 10 L.) protostellar source, YLW 15, to be stellar-like with numerous atomic and molecular absorption features, indicative of a K5 IV/V spectral type and a continuum veiling r(k) = 3.0. Its derived stellar luminosity (3 L.) and stellar radius (3.1 R.) are consistent with those of a 0.5 M. pre-main-sequence star. However, 70% of its bolometric luminosity is due to mass accretion, whose rate we estimate to be 1.6 x 10(6) M. yr(-1), onto the protostellar core. We determine that excess infrared emission produced by the circumstellar accretion disk, the inner infalling envelope, and accretion shocks at the surface of the stellar core of YLW 15 all contribute significantly to its near-IR continuum veiling. Its projected rotation velocity v sin i = 50 km s(-1) is comparable to those of at-spectrum protostars, but considerably higher than those of classical T Tauri stars in the rho Oph cloud. The protostar may be magnetically coupled to its circumstellar disk at a radius of 2 R-*. It is also plausible that this protostar can shed over half its angular momentum and evolve into a more slowly rotating classical T Tauri star by remaining coupled to its circumstellar disk (at increasing radius) as its accretion rate drops by an order of magnitude during the rapid transition between the Class I and Class II phases of evolution. The spectrum of WL6 does not show any photospheric absorption features, and we estimate that its continuum veiling is r(k)greater than or equal to4.6. Its low bolometric luminosity (2 L.) and high veiling dictate that its central protostar is very low mass, M similar to 0.1 M.. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greene, TP (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. NR 43 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 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2002 VL 124 IS 4 BP 2185 EP 2193 DI 10.1086/342861 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 596BF UT WOS:000178143400029 ER PT J AU Reipurth, B Hartmann, L Kenyon, SJ Smette, A Bouchet, P AF Reipurth, B Hartmann, L Kenyon, SJ Smette, A Bouchet, P TI Evolution of the FU Orionis object BBW 76 SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; stars : fundamental parameters; stars : individual (BBW 76); stars : pre-main-sequence ID Z-CANIS-MAJORIS; T-TAURI STARS; PROTOSTELLAR DISK MODELS; HARO ENERGY-SOURCES; ACCRETION DISKS; OBSERVATIONAL CONSTRAINTS; VELOCITY-FIELD; OUTER GALAXY; ESO-SYSTEM; MASS-LOSS AB We have carried out a long-term photometric and spectroscopic monitoring program of the southern FU Orionis type object BBW 76 spanning the period from 1982 to 1997. BBW 76 has the same radial velocity as the small cloud toward which it is projected, and for which a kinematic distance of about 1.8 kpc has been derived. We have determined a large reddening of E (B-V) similar to 0.7 for BBW 76. Optical and infrared spectra show the change toward later spectral type with increasing wavelength characteristic of FU Orionis stars and indicative of a hot luminous disk. High-resolution echelle spectra of BBW 76 show P Cygni profiles with extended blueshifted absorption troughs at the H and sodium lines from a neutral, supersonic wind. Comparison of such spectra obtained at six different epochs between 1985 and 1997 reveals major changes in these Halpha and sodium line profiles. For a period of 10 years from 1985, the massive absorption troughs diminished in extent and depth, until by 1994 they had all but disappeared, while at the same time the blueshifted emission peak in the Halpha line increased markedly in strength. However, when observed in 1997, the absorption had increased again and the emission had diminished. We interpret this in terms of an extended period during which accretion through a circumstellar disk decreased, with a resulting decrease in wind production. But the increased activity by 1997 shows that this is not a constant decay and that the star was not about to revert to its presumably original T Tauri stage. We monitored the star with optical photometry from 1983 to 1994, during which period it decreased almost monotonically in brightness by 0.2 mag in V. Infrared J, H, and K photometry from 1983 to 1991 shows a period of monotonic fading between 1984 and 1988, followed by more irregular behavior. In a search of the Harvard plate archives we have found a plate from the year 1900 on which BBW 76 is seen at approximately its present brightness, certainly not 2 mag brighter as expected if the optical decline between 1983 and 1994 had persisted during the whole century. Also, a plate taken for the Franklin-Adams charts in 1927 again shows BBW 76 at approximately the same brightness. This historical light curve makes BBW 76 the FU Orionis star with the longest-documented period in a high state. Overall, the observations suggest that BBW 76 is virtually identical to the prototype of its class, FU Orionis itself, in all respects except that BBW 76 has not shown the regular fading that FU Orionis has displayed after its eruption in 1936. This may be due to continued replenishment of the circumstellar accretion disk. C1 Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. Cerro Tololo Interamer Observ, La Serena, Chile. RP Reipurth, B (reprint author), Univ Hawaii, Astron Inst, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 76 TC 26 Z9 26 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2002 VL 124 IS 4 BP 2194 EP 2206 DI 10.1086/342740 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 596BF UT WOS:000178143400030 ER PT J AU Kawamura, J Hunter, TR Tong, CYE Blundell, R Papa, DC Patt, F Peters, W Wilson, TL Henkel, C Gol'tsman, G Gershenzon, E AF Kawamura, J Hunter, TR Tong, CYE Blundell, R Papa, DC Patt, F Peters, W Wilson, TL Henkel, C Gol'tsman, G Gershenzon, E TI Ground-based terahertz CO spectroscopy towards orion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : molecules; ISM : individual objects : orion KL; submillimeter ID BOLOMETER MIXER RECEIVER; KLEINMANN-LOW NEBULA; HETERODYNE SPECTROSCOPY; MOLECULAR CLOUD; ATMOSPHERIC TRANSMISSION; SUBMILLIMETER; EMISSION; OUTFLOW; LINE; GAS AB Using a superconductive hot-electron bolometer heterodyne receiver on the 10-m Heinrich Hertz Telescope on Mount Graham, Arizona, we have obtained velocity-resolved 1.037 THz CO (J = 9 --> 8) spectra toward several positions along the Orion Molecular Cloud (OMC-1) ridge. We confirm the general results of prior observations of high-J CO lines that show that the high temperature, T-kin greater than or equal to 130 K, high density molecular gas, n greater than or equal to 10(6) cm(-3), is quite extended, found along asimilar to4' region centered on BN/KL. However, our observations have significantly improved angular resolution, and with a beam size of theta(FWHP) approximate to 9" we are able to spatially and kinematically discriminate the emission originating in the extended quiescent ridge from the very strong and broadened emission originating in the compact molecular outflow. The ridge emission very close to the BN/KL region appears to originate from two distinct clouds along the line of sight with v(LSR) approximate to+ 6(1) km s(-1) and approximate to+10(1) km s(-1). The former component dominates the emission to the south of BN/KL and the latter to the north, with a turnover point coincident with or near BN/KL. Our evidence precludes a simple rotation of the inner ridge and lends support to a model in which there are multiple molecular clouds along the line of sight towards the Orion ridge. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Submillimeter Inst Radioastron, Tucson, AZ 85721 USA. Moscow State Pedag Univ, Moscow 119435, Russia. Max Planck Inst Radioastron, D-53010 Bonn, Germany. RP Kawamura, J (reprint author), CALTECH, Jet Prop Lab, MS 168-314, Pasadena, CA 91109 USA. OI Tong, Edward/0000-0002-7736-4203; Hunter, Todd/0000-0001-6492-0090 NR 36 TC 24 Z9 25 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 OCT PY 2002 VL 394 IS 1 BP 271 EP 274 DI 10.1051/0004-6361:20021090 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 603TB UT WOS:000178575000033 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, JSB Loeb, A TI Measuring the size of quasar broad-line clouds through time-delay light-curve anomalies of gravitational lenses SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : emission lines; quasars : general ID ACTIVE GALACTIC NUCLEI; MICROLENSING VARIABILITY; LENSING EXPERIMENT; ACCRETION DISKS; EMISSION-LINES; Q2237+0305; QSO-2237+0305; SYSTEM; REGION AB Intensive monitoring campaigns have recently attempted to measure the time delays between multiple images of gravitational lenses. Some of the resulting light curves show puzzling low-level, rapid variability that is unique to individual images, superposed on (and concurrent with) longer timescale intrinsic quasar variations that repeat in all images. We demonstrate that both the amplitude and variability timescale of the rapid light-curve anomalies are naturally explained by stellar microlensing of a smooth accretion disk that is occulted by optically thick broad-line clouds. This model also explains the observed correlation between microlensing and intrinsic variability. The rapid timescale is caused by the high velocities of the clouds (similar to5 x 10(3) km s(-1)), and the low-amplitude results from the large number of clouds covering the magnified or demagnified parts of the disk. The observed amplitudes of variations in specific lenses implies that the number of broad-line clouds that cover similar to10% of the quasar sky is similar to10(5) per 4pi sr. This is comparable to the expected number of broad-line clouds in models where the clouds originate from bloated stars. 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 37 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 OCT 1 PY 2002 VL 577 IS 2 BP 615 EP 625 DI 10.1086/342121 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WT UT WOS:000178300000006 ER PT J AU Piro, L Frail, DA Gorosabel, J Garmire, G Soffitta, P Amati, L Andersen, MI Antonelli, LA Berger, E Frontera, F Fynbo, J Gandolfi, G Garcia, MR Hjorth, J In't Zand, J Jensen, BL Masetti, N Moller, P Pedersen, H Pian, E Wieringa, MH AF Piro, L Frail, DA Gorosabel, J Garmire, G Soffitta, P Amati, L Andersen, MI Antonelli, LA Berger, E Frontera, F Fynbo, J Gandolfi, G Garcia, MR Hjorth, J In't Zand, J Jensen, BL Masetti, N Moller, P Pedersen, H Pian, E Wieringa, MH TI The bright gamma-ray burst of 2000 February 10: A case study of an optically dark gamma-ray burst SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; gamma-rays : bursts ID MOLECULAR CLOUDS; RADIO AFTERGLOW; EMISSION FEATURE; STAR-FORMATION; HOST GALAXY; BEPPOSAX; DUST; ABSORPTION; LINE; DISCOVERY AB The gamma-ray burst GRB 000210 had the highest gamma-ray peak flux of any event localized by BeppoSAX as yet, but it did not have a detected optical afterglow, despite prompt and deep searches down to R(lim) approximate to 23.5. It is therefore one of the events recently classified as dark GRBs, whose origin is still unclear. Chandra observations allowed us to localize the X-ray afterglow of GRB 000210 to within approximate to1", and a radio transient was detected with the Very Large Array. The precise X-ray and radio positions allowed us to identify the likely host galaxy of this burst and to measure its redshift, z = 0.846. The probability that this galaxy is a field object is approximate to1.6 x 10(-2). The X-ray spectrum of the afterglow shows significant absorption in excess of the Galactic one corresponding, at the redshift of the galaxy, to N(H) = (5 +/- 1) x 10(21) cm(-2). The amount of dust needed to absorb the optical flux of this object is consistent with the above H I column density, given a dust-to-gas ratio similar to that of our Galaxy. We do not find evidence for a partially ionized absorber expected if the absorption takes place in a giant molecular cloud. We therefore conclude that either the gas is local to the GRB but is condensed in small-scale high-density (n greater than or similar to 10(9) cm(-3)) clouds, or the GRB is located in a dusty, gas-rich region of the Galaxy. Finally, we examine the hypothesis that GRB 000210 lies at z greater than or similar to 5 (and therefore that the optical flux is extinguished by Lyalpha forest clouds), but we conclude that the X-ray absorbing medium would have to be substantially thicker from that observed in GRBs with optical afterglows. C1 CNR, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. Natl Radio Astron Observ, Socorro, NM 87801 USA. Danish Space Res Inst, DK-2100 Copenhagen, Denmark. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. CNR, Ist Astrofis Spaziale & Fis Cosm, Sez Bologna, I-40129 Bologna, Italy. Univ Oulu, Div Astron, FIN-90014 Oulu, Finland. Osserv Astron Roma, INAF, I-00040 Rome, Italy. CALTECH, Palomar Observ 105 24, Pasadena, CA 91125 USA. Univ Ferrara, Dipartmento Fis, I-44100 Ferrara, Italy. European So Observ, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Copenhagen, Astron Observ, DK-2100 Copenhagen O, Denmark. Space Res Org Netherlands, NL-3584 CA Utrecht, Netherlands. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Paul Wild Observ, Narrabri, NSW 2390, Australia. RP Piro, L (reprint author), CNR, Ist Astrofis Spaziale & Fis Cosm, Via Fosso Cavaliere, I-00133 Rome, Italy. RI PIRO, LUIGI/E-4954-2013; Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Jensen, Brian Lindgren/E-1275-2015; Amati, Lorenzo/N-5586-2015; OI PIRO, LUIGI/0000-0003-4159-3984; Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306; Jensen, Brian Lindgren/0000-0002-0906-9771; Amati, Lorenzo/0000-0001-5355-7388; Soffitta, Paolo/0000-0002-7781-4104; Pian, Elena/0000-0001-8646-4858 NR 72 TC 98 Z9 102 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 OCT 1 PY 2002 VL 577 IS 2 BP 680 EP 690 DI 10.1086/342226 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WT UT WOS:000178300000011 ER PT J AU Zezas, A Fabbiano, G Rots, AH Murray, SS AF Zezas, A Fabbiano, G Rots, AH Murray, SS TI Chandra observations of "the antennae" galaxies (NGC 4038/4039). III. X-ray properties and multiwavelength associations of the X-ray source population SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038/4039) galaxies : interactions galaxies : peculiar; X-rays : galaxies ID YOUNG STAR-CLUSTERS; HIGH-RESOLUTION IMAGER; BLACK-HOLE CANDIDATES; ROSAT OBSERVATIONS; NGC 4038/4039; GALACTIC DISTRIBUTION; STELLAR POPULATIONS; LUMINOSITY FUNCTION; NEARBY GALAXIES; SPECTRAL STATES AB We investigate the nature of the luminous X-ray source population detected in a (72 ks) Chandra ACIS-S observation of NGC 4038/4039, the Antennae galaxies. We derive the average X-ray spectral properties of sources in different luminosity ranges, and we correlate the X-ray positions with radio, IR, and optical (Hubble Space Telescope) data. The X-ray sources are predominantly associated with young stellar clusters, indicating that they belong to the young stellar population. Based on both their co-added X-ray spectrum and the lack of associated radio emission, we conclude that the ultraluminous X-ray sources (ULXs), with L(X) greater than or equal to 10(39) ergs s(-1), are not young compact supernova remnants (SNRs) but accretion binaries. While their spectrum is consistent with those of ULXs studied in nearby galaxies and interpreted as the counterparts of intermediate-mass black holes (M > 10-1000 M.), comparison with the position of star clusters suggests that some of the ULXs may be runaway binaries, thus suggesting lower mass binary systems. The co-added spectrum of the sources in the 3 x 10(38) to 10(39) ergs s(-1) luminosity range is consistent with those of Galactic black hole candidates. These sources are also on average displaced from neighboring star clusters. The softer spectrum of the less luminous sources suggests the presence of SNRs or of hot interstellar medium in the Chandra source extraction area. Comparison with H I and CO observations shows that most sources are detected in the outskirts of large concentrations of gas. The absorbing columns inferred from these observations would indeed absorb X-rays up to 5 keV, so there may be several hidden X-ray sources. Associated with these obscured regions, we find six sources with heavily absorbed X-ray spectra and absorption-corrected luminosities in the ULX range. We detect the nuclei of both galaxies, with luminosities in the 10(39) ergs s(-1) range and soft, possibly thermal X-ray spectra. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zezas, A (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 NR 62 TC 128 Z9 128 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 OCT 1 PY 2002 VL 577 IS 2 BP 710 EP 725 DI 10.1086/342160 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WT UT WOS:000178300000014 ER PT J AU Zezas, A Fabbiano, G AF Zezas, A Fabbiano, G TI Chandra observations of "the antennae" galaxies (NGC 4038/4039). IV. The X-ray source luminosity function and the nature of ultraluminous X-ray sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038/4039) galaxies : interactions galaxies : peculiar; X-rays : galaxies ID THICK ACCRETION DISKS; MASS BLACK-HOLES; NEARBY SPIRAL GALAXIES; HIGH-RESOLUTION CAMERA; DENSE STAR-CLUSTERS; SOURCE POPULATION; LIKELIHOOD ESTIMATION; ROSAT OBSERVATIONS; RELATIVISTIC JETS; GALACTIC NUCLEI AB We derive the X-ray luminosity function (XLF) of the X-ray source population detected in the Chandra observation of NGC 4038/4039 (the Antennae). We explicitly include photon-counting and spectral parameter uncertainties in our calculations. The cumulative XLF is well represented by a at power law (alpha = -0.47), similar to those describing the XLFs of other star-forming systems (e.g., M82, the disk of M81) but different from those of early-type galaxies. This result associates the X-ray source population in the Antennae with young high-mass X-ray binaries. In comparison with less actively star-forming galaxies, the XLF of the Antennae has a highly significant excess of sources with luminosities above 10(39) ergs s(-1) (ultraluminous sources; ULXs). We discuss the nature of these sources, based on the XLF and on their general spectral properties, as well as their optical counterparts discussed in Paper III. We conclude that the majority of the ULXs cannot be intermediate-mass black hole (M > 10 1000 M.) binaries, unless they are linked to the remnants of massive Population III stars (the Madau & Rees model). Instead, their spatial and multiwave-length properties can be well explained by beamed emission as a consequence of supercritical accretion. Binaries with a neutron star or moderate-mass black hole (up to 20 M.) and B2 to A type star companions would be consistent with our data. In the beaming scenario, the XLF should exhibit characteristic breaks that would be visible in future deeper observations of the Antennae. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zezas, A (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 NR 78 TC 106 Z9 106 U1 0 U2 3 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 OCT 1 PY 2002 VL 577 IS 2 BP 726 EP 737 DI 10.1086/342135 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WT UT WOS:000178300000015 ER PT J AU Kong, AKH Garcia, MR Primini, FA Murray, SS Di Stefano, R McClintock, JE AF Kong, AKH Garcia, MR Primini, FA Murray, SS Di Stefano, R McClintock, JE TI X-ray point sources in the central region of M31 as seen by Chandra SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); X-rays : galaxies; X-rays : stars ID SUPERNOVA REMNANT CANDIDATES; PLANETARY-NEBULAE; GALAXY; FIELD; STARS; M-31; POPULATION; BINARIES; EMISSION AB We report on Chandra observations of the central region of M31. By combining eight Chandra ACIS-I observations taken between 1999 and 2001, we have identified 204 X-ray sources within the central similar to17' x 17' region of M31, with a detection limit of similar to2 x 10(35) ergs s(-1). Of these 204 sources, 22 are identified with globular clusters, two with supernova remnants, nine with planetary nebula, and nine with supersoft sources. By comparing individual images, about 50% of the sources are variable on timescales of months. We also found 13 transients, with light curves showing a variety of shapes. We also extracted the energy spectra of the 20 brightest sources; they can be well fitted by a single power law with a mean photon index of 1.8. The spectral shapes of 12 sources are shown to be variable, suggesting that they went through state changes. The luminosity function of all the point sources is consistent with previous observations (a broken power law with a luminosity break at 1.7 x 10(37) ergs s(-1)). However, when the X-ray sources in different regions are considered separately, different luminosity functions are obtained. This indicates that the star formation history might be different in different regions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 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 66 TC 105 Z9 105 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 OCT 1 PY 2002 VL 577 IS 2 BP 738 EP 756 DI 10.1086/342116 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WT UT WOS:000178300000016 ER PT J AU McGary, RS Ho, PTP AF McGary, RS Ho, PTP TI NH3 in the central 10 parsecs of the galaxy. II. Determination of opacity for gas with large line widths SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy : center; ISM : kinematics and dynamics ISM : molecules ID GALACTIC-CENTER REGION; MOLECULAR CLOUD; A EAST; SGR-A; SAGITTARIUS; AMMONIA; SUBMILLIMETER; DYNAMICS; COMPLEX AB The 23 GHz emission lines from the NH3 rotation inversion transitions are widely used to investigate the kinematics and physical conditions in dense molecular clouds. The line pro le is composed of hyperfine components that can be used to calculate the opacity of the gas. For intrinsic line widths of a few km s(-1), the 18 magnetic hyperfine components blend together to form a line profile composed of five quadrupole hyperfine lines. If the intrinsic line width exceeds one-half of the separation of these quadrupole hyperfine components (similar to5-10 km s(-1)), these five lines blend together and the observed line widths greatly overestimate the intrinsic line widths. If uncorrected, these artificially broad line widths will lead to artificially high opacities. We have observed this effect in our NH3 data from the central 10 pc of the Galaxy where uncorrected NH3 (1, 1) line widths of similar to30 km s(-1) exaggerate the intrinsic line widths by more than a factor of 2. Models of the effect of blending on the line pro le enable us to solve for the intrinsic line width and opacity of NH3 using the observed line width and intensity of two NH3 rotation inversion transitions. By using the observed line width instead of the entire line pro le, our method may also be used to correct line widths in historical data where detailed information on the shape of the line profile is no longer available. We present the result of the application of this method to our Galactic center data. We successfully recover the intrinsic line width ([Deltav(int)] approximate to 15 km s(-1)) and opacity of the gas. Clouds close to the nucleus in projected distance as well as those that are being impacted by Sgr A East show the highest intrinsic line widths. The cores of the "southern streamer" and the "50 km s(-1)" giant molecular cloud have the highest opacities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McGary, RS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 22 TC 12 Z9 12 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2002 VL 577 IS 2 BP 757 EP 767 DI 10.1086/342233 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WT UT WOS:000178300000017 ER PT J AU Zhu, C Krems, R Dalgarno, A Balakrishnan, N AF Zhu, C Krems, R Dalgarno, A Balakrishnan, N TI Chemistry of hydrogen fluoride in the interstellar medium SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : molecules; molecular data; molecular processes ID POTENTIAL-ENERGY SURFACE; DER-WAALS COMPLEXES; OPEN-SHELL ATOMS; F+H-2 REACTION; F+H-2->HF+H REACTION; DIABATIC REPRESENTATIONS; SCATTERING; MOLECULE; DISTRIBUTIONS; COLLISIONS AB A comprehensive account is given of the chemistry of HF in interstellar clouds. Calculations are presented of the rate coefficients for the quenching of F(P-2(1/2)) and for the reaction of F(P-2(3/2)) atoms in collisions with H-2. They confirm the conclusions of Neufeld and coworkers that gaseous fluorine exists in interstellar clouds almost entirely in the form of the molecule HF. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. RP Zhu, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 27 Z9 27 U1 1 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 OCT 1 PY 2002 VL 577 IS 2 BP 795 EP 797 DI 10.1086/342240 PN 1 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WT UT WOS:000178300000020 ER PT J AU Tuthill, PG Monnier, JD Danchi, WC Hale, DDS Townes, CH AF Tuthill, PG Monnier, JD Danchi, WC Hale, DDS Townes, CH TI Imaging the disk around the luminous young star LkH alpha 101 with infrared interferometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; stars : individual (LkH alpha 101); stars : mass loss; techniques : interferometric ID HERBIG-AE/BE STARS; INTERMEDIATE-MASS STARS; T-TAURI STARS; ECCENTRIC GRAVITATIONAL INSTABILITIES; CIRCUMSTELLAR DISKS; STELLAR OBJECTS; PROTOSTELLAR DISKS; HIGH-RESOLUTION; ORION NEBULA; AB AURIGAE AB The Herbig Ae/Be star LkHalpha 101 has been imaged at high angular resolution at a number of wavelengths in the near-infrared (from 1 to similar to3 mum), using the Keck I Telescope, and also observed in the mid-infrared ( 11.15 mum), using the UC Berkeley Infrared Spatial Interferometer (ISI). The resolved circular disk with a central hole or cavity reported by Tuthill, Monnier, & Danchi is confirmed. This is consistent with an almost face-on view (inclination of less than or similar to35degrees) onto a luminous pre-main-sequence or early main-sequence object surrounded by a massive circumstellar disk. With a multiple-epoch study spanning almost 4 years, relative motion of the binary companion has been detected, together with evidence of changes in the brightness distribution of the central disk/star. The resolution of the LkHalpha 101 disk by ISI mid-infrared interferometry constitutes the first such measurement of a young stellar object in this wavelength region. The angular size was found to increase only slowly from 1.6 to 11.15 mum, inconsistent with standard power-law temperature proles usually encountered in the literature, supporting instead models with a hot inner cavity and relatively rapid transition to a cool or tenuous outer disk. The radius of the dust-free inner cavity is consistent with a model of sublimation of dust in equilibrium with the stellar radiation field. Measurements from interferometry have been combined with published photometry, enabling an investigation of the energetics and fundamental properties of this prototypical system. C1 Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Tuthill, PG (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. NR 65 TC 46 Z9 46 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 OCT 1 PY 2002 VL 577 IS 2 BP 826 EP 838 DI 10.1086/342235 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WT UT WOS:000178300000022 ER PT J AU Henry, GW Donahue, RA Baliunas, SL AF Henry, GW Donahue, RA Baliunas, SL TI A false planet around HD 192263 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : individual (HD 192263); stars : late-type; stars : rotation; stars : spots; stars : variables : other ID MAIN-SEQUENCE STARS; MAGNETIC ACTIVITY; COOL STARS; VARIABILITY; SEARCH AB We present new high-precision Stromgren photometry and Ca II H and K spectrophotometry of HD 192263. Based on radial velocity variations detected previously by two groups, this K2 V star was thought to host a 0.75 M-Jup (minimum mass) planetary companion in a 24 day orbit. Our photometric observations reveal periodic variations that match the purported planetary orbital period, while the Ca II H and K emission fluxes are modulated on half the planetary period. This suggests that rotational modulation of the visibility of stellar surface activity is the source of the observed radial velocity variations. Therefore, HD 192263 should be removed from lists of stars with well-established planetary companions unless further observations and analysis can support the existence of the planet in spite of the star's intrinsic variations. C1 Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37203 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. Mt Wilson Observ, Pasadena, CA 91106 USA. RP Henry, GW (reprint author), Tennessee State Univ, Ctr Excellence Informat Syst, 330 10th Ave N, Nashville, TN 37203 USA. NR 19 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 OCT 1 PY 2002 VL 577 IS 2 BP L111 EP L114 DI 10.1086/344291 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598WY UT WOS:000178300500009 ER PT J AU Zezas, A Fabbiano, G Rots, AH Murray, SS AF Zezas, A Fabbiano, G Rots, AH Murray, SS TI Chandra observations of the Antennae galaxies (NGC 4038/4039). II. Detection and analysis of galaxian X-ray sources SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : individual (NGC 4038/4039); galaxies : interactions; galaxies : peculiar; X-rays : galaxies ID NGC-4038/4039; EMISSION AB We report the detailed analysis of the X-ray properties of the discrete sources detected in a long (72 ks) Chandra ACIS-S observation of the Antennae galaxies. We detect 49 sources, down to a detection limit of similar to10(38) ergs s(-1); 18 sources have L-X > 10(39) ergs s(-1) ( ultraluminous X-ray sources; ULXs). Six of the 49 sources have an extended component. Two sources show evidence for variability during this observation, and three sources exhibit long-term variability in timescales of a few years. The spectra of the discrete sources are diverse, suggesting different emission mechanisms, broadly correlated with the source luminosity: the most luminous sources exhibit harder emission, while the spectra of fainter sources appear softer. Spectra and variability suggest that the ULXs may be binary accretion sources; Supernova remnants or hot interstellar medium in the Chandra beam may be responsible for some of the softer sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zezas, A (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 NR 29 TC 63 Z9 63 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 OCT PY 2002 VL 142 IS 2 BP 239 EP 260 DI 10.1086/342010 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 596YM UT WOS:000178194100004 ER PT J AU Jehl, JR Boyd, WS Paul, DS Anderson, DW AF Jehl, JR Boyd, WS Paul, DS Anderson, DW TI Massive collapse and rapid rebound: Population dynamics of eared grebes (Podiceps nigricollis) during an ENSO event SO AUK LA English DT Article ID CALIFORNIA; ABUNDANCE; MIGRATION AB In autumn, >99% of North American Eared Grebes (Podiceps nigricollis) stage at Mono Lake, California, and Great Salt Lake, Utah, creating an exceptional opportunity to measure population trends in a common and otherwise widely distributed species. Aerial photocounts showed that numbers at both lakes fluctuated in parallel, from a total of similar to3.56 million in 1997, then crashing to 1.60 million in 1998. The decline was coincident with a major El Nino, during which hundreds of thousands starved in the Gulf of California. The population rebounded to 3.27 million by 2000, illustrating the species' potentially high survivorship throughout the year. Catastrophic events are evidently the major factors affecting proximate changes in population size. Factors that set the ultimate limit to the population can be clarified through long-term studies at staging areas. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Canadian Wildlife Serv, Pacific Wildlife Res Ctr, Delta, BC V4K 3N2, Canada. Utah Div Wildlife Resources, Salt Lake City, UT 84116 USA. Univ Calif Davis, Dept Wildlife & Conservat Biol, Davis, CA 95616 USA. RP Jehl, JR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 17 TC 11 Z9 13 U1 1 U2 7 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2002 VL 119 IS 4 BP 1162 EP 1166 DI 10.1642/0004-8038(2002)119[1162:MCARRP]2.0.CO;2 PG 5 WC Ornithology SC Zoology GA 639VC UT WOS:000180649200028 ER PT J AU Davis, BK Henderson, RA Lindsay, M Wysoczanski, R AF Davis, BK Henderson, RA Lindsay, M Wysoczanski, R TI Deformation history and timing of granite emplacement in the Butchers Hill - Helenvale region, northern Hodgkinson Province, Queensland SO AUSTRALIAN JOURNAL OF EARTH SCIENCES LA English DT Article DE deformation history; emplacement mechanism; geochronology; granite; Hodgkinson Province; Hunter-Bowen Orogeny; porphyroblast ID TASMAN OROGENIC ZONE; ENGLAND FOLD BELT; U-TH-PB; METAMORPHIC ROCKS; AUSTRALIA; ROTATION; TERRANES; VEINS AB Granite plutons of the Whypalla Supersuite in the Butchers Hill - Helenvale region of north Queensland were intruded into the upper crust of the Hodgkinson Formation during contractional deformation associated with the Permian-Triassic Hunter-Bowen Orogeny. A four-stage structural history has been resolved for the area, with fabric overprinting relationships, porphyroblast-matrix microstructural geometries and isotopic ages being consistent with granite emplacement during D-4 shortening at ca 274 Ma. Microstructural relationships suggest the possibility of a minor syn-D-3 phase of granite emplacement. The deformation-emplacement history of the Butchers Hill - Helenvale area is consistent with that recognised regionally for the Hodgkinson Province, indicating province-wide synchronous syntectonic granite intrusion during a major phase of contractional deformation. Intense syn-emplacement deformation partitioning was ongoing in the country rocks during progressive D-4 and was associated with upward translation of country rock from the microscale to the macroscale along D-4 cleavages and shears. Kinematic indicators show that this progressive uplift, at the scale of the area examined, was east-side-up. C1 AurionGold, Kalgoorlie, WA 6433, Australia. James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Davis, BK (reprint author), AurionGold, POB 862, Kalgoorlie, WA 6433, Australia. RI Wysoczanski, Richard/C-2930-2009; Wysoczanski, Richard/I-7730-2012 NR 29 TC 6 Z9 6 U1 0 U2 3 PU BLACKWELL PUBLISHING ASIA PI CARLTON PA 54 UNIVERSITY ST, P O BOX 378, CARLTON, VICTORIA 3053, AUSTRALIA SN 0812-0099 J9 AUST J EARTH SCI JI Aust. J. Earth Sci. PD OCT PY 2002 VL 49 IS 5 BP 775 EP 785 DI 10.1046/j.1440-0952.2002.00953.x PG 11 WC Geosciences, Multidisciplinary SC Geology GA 599NM UT WOS:000178341600002 ER PT J AU Wasshausen, DC AF Wasshausen, DC TI New species of Justicia (Acanthaceae) from the Guianas SO BRITTONIA LA English DT Article DE Acanthaceae; Justicia; Guianas; taxonomy AB Wasshausen, Dieter C. (Department of Botany, NHB-166, Smithsonian Institution, Washington, DC 20560-0166, U.S.A.; email: wasshausen.dieter@nmnh. si.edu). New species of Justicia (Acanthaceae) from the Guianas. Brittonia 54: 286-297. 2002.-Four new species, Justicia oldemanii, J. mcdowellii, J. wilhelminensis, and J. prevostiae are described, illustrated, and compared with their closest relatives. A key to species of Justicia from the Guianas is also provided. C1 Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Wasshausen, DC (reprint author), Smithsonian Inst, Dept Bot, NHB-166, Washington, DC 20560 USA. NR 8 TC 1 Z9 1 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 OCT-DEC PY 2002 VL 54 IS 4 BP 286 EP 297 DI 10.1663/0007-196X(2003)54[286:NSOJAF]2.0.CO;2 PG 12 WC Plant Sciences SC Plant Sciences GA 670AE UT WOS:000182383700009 ER PT J AU Feuillet, C Skog, LE AF Feuillet, C Skog, LE TI Novae Gesneriaceae Neotropicarum XI. New genera and species from the Guianas SO BRITTONIA LA English DT Article DE Cremersia; Episcieae; French Guiana; Gesneriaceae; Guyana; Lampadaria; Lembocarpus ID PHYLOGENETIC-RELATIONSHIPS; NDHF SEQUENCES AB Feuillet, C. & L. E. Skog. (Department of Systematic Biology-Botany, MRC-166, Smithsonian Institution, PO. Box 37012, Washington, DC 20013-7012, U.S.A.; emails: bihorel@concentric.net; skog.larry@Pnmnh.si.edu). Novae Gesneriaceae Neotropicarum XI. New genera and species from the Guianas. Brittonia 54: 344-351. 2002.-Two new genera of Gesneriaceae are described, Lampadaria and Cremersia, each with one new species: Lampadaria rupestris from Guyana and Cremersia platula from French Guiana, both belonging to the tribe Episcieae. The placement of Lembocarpus in the Episcieae near Cremersia and Rhoogeton is proposed. C1 Smithsonian Inst, Dept Systemat Biol Bot, Washington, DC 20013 USA. RP Feuillet, C (reprint author), Smithsonian Inst, Dept Systemat Biol Bot, MRC-166,POB 37012, Washington, DC 20013 USA. NR 16 TC 0 Z9 2 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 OCT-DEC PY 2002 VL 54 IS 4 BP 344 EP 351 DI 10.1663/0007-196X(2003)54[344:NGNXNG]2.0.CO;2 PG 8 WC Plant Sciences SC Plant Sciences GA 670AE UT WOS:000182383700018 ER PT J AU Feuillet, C Skog, LE AF Feuillet, C Skog, LE TI Novae Gesneriaceae Neotropicarum XII. New species of Gesneriaceae from the Guianas SO BRITTONIA LA English DT Article DE Episcieae; French Guiana; Gesneriaceae; Guyana; Napeantheae; Napeanthus; Nautilocalyx; Paradrymonia AB Feuillet, C. & L. E. Skog. (Department of Systematic Biology-Botany, MRC-166, Smithsonian Institution, PO. Box 37012, Washington, DC 20013-7012, U.S.A.; emails: bihorel@concentric.net; skog.larry@nmnh.si.edu). Novae Gesneriaceae Neotropicarum XII. New species of Gesneriaceae from the Guianas. Brittonia 54: 352-361. 2002.-Five new species of Gesneriaceae are described from the Guianas: Nautilocalyx coccineus, Paradrymonia anisophylla, and Paradrymonia barbata in the tribe Episcieae, from Guyana; Napeanthus angustifolius from French Guiana and Napeanthus rupicola from Guyana in the tribe Napeantheae. C1 Smithsonian Inst, Dept Systemat Biol Bot, Washington, DC 20013 USA. RP Feuillet, C (reprint author), Smithsonian Inst, Dept Systemat Biol Bot, MRC-166,POB 37012, Washington, DC 20013 USA. NR 5 TC 0 Z9 2 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 OCT-DEC PY 2002 VL 54 IS 4 BP 352 EP 361 DI 10.1663/0007-196X(2003)54[352:NGNXNS]2.0.CO;2 PG 10 WC Plant Sciences SC Plant Sciences GA 670AE UT WOS:000182383700019 ER PT J AU Linares, OF AF Linares, OF TI Cultural evolution: Contemporary viewpoints SO CAMBRIDGE ARCHAEOLOGICAL JOURNAL LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Linares, OF (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM LINARES@tivoli.si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0959-7743 J9 CAMB ARCHAEOL J JI Camb. Archaeol. J. PD OCT PY 2002 VL 12 IS 2 BP 277 EP 279 DI 10.1017/S0959774302250143 PG 3 WC Archaeology SC Archaeology GA 617TK UT WOS:000179376800011 ER PT J AU Groat, LA Marshall, DD Giuliani, G Murphy, DC Piercey, SJ Jambor, JL Mortensen, JK Ercit, TS Gault, RA Mattey, DP Schwarz, D Maluski, H Wise, MA Wengzynowski, W Eaton, DW AF Groat, LA Marshall, DD Giuliani, G Murphy, DC Piercey, SJ Jambor, JL Mortensen, JK Ercit, TS Gault, RA Mattey, DP Schwarz, D Maluski, H Wise, MA Wengzynowski, W Eaton, DW TI Mineralogical and geochemical study of the Regal Ridge emerald showing, southeastern Yukon SO CANADIAN MINERALOGIST LA English DT Article DE emerald deposit; geology; mineralogy; geochemistry; fluid inclusions; stable isotopes; Finlayson Lake; Yukon; Canada ID FLUID INCLUSIONS; STABLE-ISOTOPE; OXYGEN-ISOTOPE; GRANITIC PEGMATITE; TANANA TERRANE; COLOMBIAN EMERALDS; CRYSTAL-CHEMISTRY; SOUTH-AFRICA; MINERALIZATION; EVOLUTION AB In September, 1998, one of the authors (WW) discovered a major occurrence of emerald in the Finlayson Lake district of southeastern Yukon. The Regal Ridge showing occurs in complexly deformed metavolcanic rocks in the Yukon-Tanana Terrane, near their contact with a mid-Cretaceous granitic pluton. The emerald crystals occur where quartz veins cut mica-rich layers in a shallowly dipping mica schist of the Upper Devonian Fire Lake mafic metavolcanic unit. At least eight such veins have been found. Most are surrounded by a much more extensive, overlapping mass of fine, dark tourmaline crystals. The tourmaline crystals are locally associated with minor amounts of scheelite, and small amounts of sulfides have been observed to occur within the quartz veins. A zone of sparse, disseminated sulfides apparently coincides with the tourmaline zone, which is surficially marked by ochreous products of oxidation. Green beryl crystals up to 4 cm in length occur in tourmaline zones and, rarely, in the quartz veins. Some of the smaller crystals, and sections of larger crystals, are of gem quality. The Cr content (average 3208 ppm) shows that it is the predominant chromophore. Fluid-inclusion data indicate that the emerald precipitated from a fluid whose maximum salinity was 3 wt.% NaCl equivalent. The oxygen isotopic composition of the emerald is highly variable (12.3 to 14.8parts per thousand), but there is little difference in corresponding deltaD values (-57.3 and-59.8parts per thousand, respectively), which suggests the presence of an isotopically homogeneous fluid that underwent isotopic exchange with the host rocks without achieving homogenization. The delta(18)O values for coexisting quartz and tourmaline from the quartz veins yield temperatures of formation of approximately 365 and 498degreesC. Based on fluid-inclusion isochoric data, these temperatures correspond to pressures of 1.0 to 2.5 kbar, and inferred depths of 3 to 7.7 km. The close proximity of the granite suggests that it is the source of the Be, although the Be content is low (12 and 13.2 ppm). The source of the Cr is the schist (520 ppm Cr). An Ar-40/Ar-39 age of 109 Ma for a mica sample from the schist could either reflect a thermal overprint age related to the event that produced the emerald crystals, or cooling following intrusion of the adjacent pluton, or both. C1 Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada. Simon Fraser Univ, Dept Earth Sci, Burnaby, BC V5A 1S6, Canada. IRD, F-54501 Vandoeuvre Les Nancy, France. CNRS, Ctr Rech Petrog & Geochim, UPR 2300, F-54501 Vandoeuvre Les Nancy, France. Govt Yukon, Yukon Geol Program, Whitehorse, YT Y1A 2C6, Canada. Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada. Canadian Museum Nat, Div Res, Ottawa, ON K1P 6P4, Canada. Univ London, Royal Holloway & Bedford New Coll, Dept Geol, Egham TW20 0EX, Surrey, England. Gubelin Gemmol Lab, CH-6000 Luzern 9, Switzerland. Univ Montpellier 2, Lab Geochronol, F-34095 Montpellier, France. Smithsonian Inst, Washington, DC 20560 USA. Expatriate Resources Ltd, Vancouver, BC V6B 1L8, Canada. Archer Cathro & Associates 1981 Ltd, Vancouver, BC V6B 1L8, Canada. RP Groat, LA (reprint author), Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada. NR 91 TC 27 Z9 28 U1 2 U2 7 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 OCT PY 2002 VL 40 BP 1313 EP 1338 DI 10.2113/gscanmin.40.5.1313 PN 5 PG 26 WC Mineralogy SC Mineralogy GA 619MU UT WOS:000179480400003 ER PT J AU McKeown, DA Post, JE Etz, ES AF McKeown, DA Post, JE Etz, ES TI Vibrational analysis of palygorskite and sepiolite SO CLAYS AND CLAY MINERALS LA English DT Article DE FTIR; palygorskite; Raman; sepiolite ID ACID TREATMENT; FT-IR; ATTAPULGITE; SILICATES; SPECTRA; RAMAN; MICA AB Lattice dynamic calculations for the sepiolite and palygorskite structures using polarized Raman and FTIR spectra provide a fundamental basis for interpreting spectral features by assigning vibrational modes. The Si-O stretch and O-Si-O bond bending force constants determined for palygorskite are similar to equivalent values calculated previously for other phyllosilicates. The Mg-O bond stretch values, on the other hand, are about half of those determined for the equivalent Al-O and Mg-O bond stretch environments in other phyllosilicates, suggesting that the bonding within the octahedral ribbons in palygorskite and sepiolite is weaker than that in the continuous octahedral sheets in micas. The weaker bonding allows more flexible octahedral environments in palygorskite and sepiolite, giving rise to higher probabilities for cation substitutions and vacancies relative to the micas. Above similar to700 cm(-1) in the IR and 750 cm(-1) in the Raman spectra, the eigenmodes are dominated by atomic displacements within the silicate sheets. Below 700 cm(-1) the eigenmodes become mixed with motions among the Mg octahedra and the silicate sheets; the eigenmodes assigned to the most prominent peaks in the Raman spectra (near 700 cm(-1)) belong to this group. As mode frequencies decrease, the corresponding eigenmodes evolve from more localized Mg-O stretch, O-Mg-O bend and O-Si-O bend motions to longer-range motions such as silicate sheet deformations caused by silicate tetrahedra rotation and silicate sheet shearing around the Mg-octahedral sheets. C1 Catholic Univ Amer, Vitreous State Lab, Washington, DC 20064 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. NIST, Surface & Microanalysis Sci Div, Gaithersburg, MD 20899 USA. RP McKeown, DA (reprint author), Catholic Univ Amer, Vitreous State Lab, 620 Michigan Ave,NE, Washington, DC 20064 USA. EM davidm@vsl.cua.edu NR 30 TC 56 Z9 58 U1 2 U2 27 PU CLAY MINERALS SOC PI CHANTILLY PA 3635 CONCORDE PKWY, STE 500, CHANTILLY, VA 20151-1125 USA SN 0009-8604 EI 1552-8367 J9 CLAY CLAY MINER JI Clay Clay Min. PD OCT PY 2002 VL 50 IS 5 BP 667 EP 680 DI 10.1346/000986002320679549 PG 14 WC Chemistry, Physical; Geosciences, Multidisciplinary; Mineralogy; Soil Science SC Chemistry; Geology; Mineralogy; Agriculture GA 610EJ UT WOS:000178947500013 ER PT J AU Bruna, EM Kress, WJ AF Bruna, EM Kress, WJ TI Habitat fragmentation and the demographic structure of an Amazonian understory herb (Heliconia acuminata) SO CONSERVATION BIOLOGY LA English DT Article ID RAIN-FOREST FRAGMENTS; OLD-GROWTH FOREST; MATRIX MODELS; PLANT; POLLINATION; TREE; DYNAMICS; CONSEQUENCES; CONSERVATION; VEGETATION AB Little is known about the demographic consequences of fragmentation for plant populations. By assessing the population structure of a common herb (Heliconia acuminata) in an experimentally fragmented landscape in the central Amazon, we tested the predictions that fragmentation could reduce population density, alter population structure, and reduce reproductive effort. Population density in continuous forest varied six-fold, some areas having high density and others low density. Population density in small fragments and on the edges of large fragments was often low, but it was within the range of densities found in continuous forest, and the difference between locations was not significant. Heliconia populations in forest fragments were skewed toward smaller demographic size classes, however. Because reproduction in H. acuminata is positively correlated with plant size, these shifts were predicted to result in fewer flowering plants in forest fragments. The proportion of the population flowering in forest fragments and continuous forest was not significantly different, although there was a trend toward proportionately greater flowering in continuous forest. For plants that did flower, per-individual reproductive success (measured as developing fruit set) was the same in forest fragments and continuous forests. Our results suggest that per-individual and population-level reproduction by understory herbs in tropical forest fragments may be resistant to the detrimental consequences of fragment isolation. Our study also highlights the need to consider how fragmentation influences aspects of population structure and demography beyond abundance and fruit production, because these alternative measures of population structure can be modified in forest fragments in subtle, unexpected ways. C1 Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. Univ Calif Davis, Ctr Populat Biol, Davis, CA 95616 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Bot, Washington, DC 20560 USA. Natl Inst Res Amazon, INPA, Biol Dynam Forest Fragments Project, BR-69011 Manaus, Amazonas, Brazil. RP Bruna, EM (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, POB 110430, Gainesville, FL 32611 USA. RI Bruna, Emilio/H-2769-2012 OI Bruna, Emilio/0000-0003-3381-8477 NR 60 TC 50 Z9 55 U1 4 U2 28 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 2002 VL 16 IS 5 BP 1256 EP 1266 DI 10.1046/j.1523-1739.2002.99494.x PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 596UC UT WOS:000178183600012 ER PT J AU Haight, RG Cypher, B Kelly, PA Phillips, S Possingham, HP Ralls, K Starfield, AM White, PJ Williams, D AF Haight, RG Cypher, B Kelly, PA Phillips, S Possingham, HP Ralls, K Starfield, AM White, PJ Williams, D TI Optimizing habitat protection using demographic models of population viability SO CONSERVATION BIOLOGY LA English DT Article ID JOAQUIN KIT FOXES; NORTHERN SPOTTED OWL; MANAGEMENT; CONSERVATION; OPTIMIZATION; DISTRIBUTIONS; REPRODUCTION; ABUNDANCE; PREY; GIS AB Expanding habitat protection is a common tactic for species conservation. When unprotected habitat is privately owned, decisions must be made about which areas to protect by land purchase or conservation easement. To address this problem, we developed an optimization framework for choosing the habitat-protection strategy that minimizes the risk of population extinction subject to an upper bound on funding. The framework is based on the idea that an extinction-risk function that predicts the relative effects of varying the quantity and quality of habitat can be estimated from the results of a demographic model of population viability. We used the framework to address the problem of expanding the protected habitat of a core population of the endangered San Joaquin kit fox (Vulpes macrotis mutica) in the Panoche area in central California. We first developed a stochastic demographic model of the kit fox population. Predictions from the simulation model were used to estimate an extinction-risk function that depended on areas of good- and fair-quality habitat. The risk function was combined with costs of habitat protection to determine cost-efficient protection strategies and risk-cost curves showing how extinction risk could be reduced at minimum cost for increasing levels of funding. One important result was that cost-efficient shares of the budget used to protect different types of habitat changed as the budget increased and depended on the relative costs of available habitat and the relative effects of habitat protection on extinction risk. Another important finding was the sensitivity of the location and slope of the risk-cost curve to assumptions about the spatial configuration of available habitat. When the location and slope of the risk-cost curve are sensitive to model assumptions, resulting predictions of extinction risk and risk reduction per unit cost should be used very cautiously in ranking conservation options among different species or populations. The application is an example of how the results of a complex demographic model of population viability can be synthesized for use in optimization analyses to determine cost-efficient habitat-protection strategies and risk-cost tradeoffs. C1 US Forest Serv, N Cent Res Stn, St Paul, MN 55108 USA. Calif State Univ Stanislaus, Endangered Species Recovery Program, Bakersfield, CA 93389 USA. Calif State Univ Stanislaus, Endangered Species Recovery Program, Fresno, CA 93727 USA. Univ Queensland, Dept Zool, St Lucia, Qld 4072, Australia. Univ Queensland, Dept Math, St Lucia, Qld 4072, Australia. Smithsonian Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Univ Minnesota, St Paul, MN 55108 USA. US Fish & Wildlife Serv, Carlsbad, CA 92008 USA. Calif State Univ Stanislaus, Dept Biol Sci, Turlock, CA 95382 USA. RP Haight, RG (reprint author), US Forest Serv, N Cent Res Stn, 1992 Folwell Ave, St Paul, MN 55108 USA. RI Possingham, Hugh/B-1337-2008 OI Possingham, Hugh/0000-0001-7755-996X NR 44 TC 39 Z9 40 U1 3 U2 20 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 2002 VL 16 IS 5 BP 1386 EP 1397 DI 10.1046/j.1523-1739.2002.99510.x PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 596UC UT WOS:000178183600025 ER PT J AU Ainsworth, EA Davey, PA Hymus, GJ Drake, BG Long, SP AF Ainsworth, EA Davey, PA Hymus, GJ Drake, BG Long, SP TI Long-term response of photosynthesis to elevated carbon dioxide in a Florida scrub-oak ecosystem SO ECOLOGICAL APPLICATIONS LA English DT Article DE canopy closure; climate change; elevated CO2; Florida scrub oak; intergeneric variation; interspecific variation; photosynthesis; Quercus; Rubisco ID ATMOSPHERIC CO2 CONCENTRATION; PINE PINUS-TAEDA; QUERCUS-MYRTIFOLIA; NATIVE ENVIRONMENT; ACCLIMATION; PLANTS; FOREST; TREE; MODEL; METAANALYSIS AB The response of photosynthesis was analyzed during canopy closure in a Florida scrub-oak ecosystem exposed to elevated [CO2] (704 mumol CO2/mol air; concentration Of CO2). The species were measured on six occasions, covering different seasons, during the third. and fourth year of exposure to elevated [CO2]. The entire regrowth cycle of this community has been under elevated [CO2], providing a rare opportunity to assess the differential responses of species during the critical phase of canopy closure. Measurements were taken in order to determine both season-specific and species-specific differences' in the response of photosynthesis to elevated [CO2]. Photosynthesis was measured with an open-gas exchange system, and in vivo rates of Rubisco carboxylation (V-c,V-max) and electron transport (J(max)) were derived to assess changes in the photosynthetic capacity in the co-dominant, evergreen oak species. Quercus myrtifolia did not show any change in photosynthetic capacity with prolonged exposure to elevated [CO2] during any season, and as a result the increase in photosynthesis due to the increased Supply Of CO2 was sustained at 72%. The codominant, Q. geminata, showed a loss of photosynthetic capacity with growth at elevated [CO2], such that during most measurement periods light-saturated photosynthesis in leaves grown and measured at elevated [CO2] was no higher than in leaves grown and measured at ambient CO2. A third oak, Q. chapmanii, showed a response similar to that of Q. myrtifolia. This suggests that at the critical phase of canopy closure in a woody community,, elevation Of [CO2] causes a species-dependent and time-dependent change in the capacity of the codominants to acquire carbon and energy. C1 Univ Illinois, Edward R Madigan Lab 190, Dept Crop Sci, Urbana, IL 61801 USA. Univ Illinois, Edward R Madigan Lab 190, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. RP Long, SP (reprint author), Univ Illinois, Edward R Madigan Lab 190, Dept Crop Sci, 1201 W Gregory Dr, Urbana, IL 61801 USA. RI Long, Stephen/A-2488-2008 OI Long, Stephen/0000-0002-8501-7164 NR 34 TC 26 Z9 27 U1 4 U2 20 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 OCT PY 2002 VL 12 IS 5 BP 1267 EP 1275 DI 10.2307/3099970 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 614PM UT WOS:000179198600003 ER PT J AU Pearson, TRH Burslem, DFRP Mullins, CE Dalling, JW AF Pearson, TRH Burslem, DFRP Mullins, CE Dalling, JW TI Germination ecology of neotropical pioneers: Interacting effects of environmental conditions and seed size SO ECOLOGY LA English DT Article DE Burro Colorado Island, Panama; emergence potential; germination cue; niche diffierentiation; pioneer species; tropical diversity ID TROPICAL RAIN-FOREST; LIGHT; TREE; ESTABLISHMENT; LITTER; SOIL; REGENERATION; DISPERSAL; DIVERSITY; RESPONSES AB Germination provides many potentially unrecognized sources of variation in the regeneration niche. In this study we relate germination requirements and seed size for 16 species of pioneer trees to microclimatic conditions present in gaps in semi-deciduous rain forest in Panama. We found that, whereas increased duration of direct irradiance can be an effective indicator of the presence of a canopy gap across all scales of canopy openness, diel fluctuations in soil temperature effectively discriminate both understory sites and small gaps (25 m(2)) from larger gaps. Germination response was significantly related to seed size. Small-seeded species (seed mass <2 mg) showed significantly greater germination in response to irradiance of 22.3 mumol.m(-2).s(-1) than in complete darkness. Their germination was unaffected by an increasing magnitude of diel temperature fluctuation up to a species-specific threshold, above which it declined. Large-seeded species (seed mass >2 mg) germinated equally in light and darkness (with one exception) and either showed a positive germination response to an increasing magnitude of temperature fluctuation (four species) or no significant response (four species). The maximum seed burial depth from which seedlings could emerge successfully was strongly positively associated with seed mass. We conclude that photoblastic germination of tropical pioneer trees results in small-seeded species germinating in gaps only when seeds are located in microsites that are suitable for seedling emergence. A positive germination response to increasing temperature fluctuation can stimulate germination of larger-seeded species in larger gaps and when they are buried beneath an opaque soil or litter layer. Therefore, seed size differences constrain the physiological mechanisms of canopy gap detection in tropical pioneer trees and might contribute to observed differences in the distribution of adult plants in relation to canopy gap size. C1 Univ Aberdeen, Dept Plant & Soil Sci, Aberdeen AB24 3UU, Scotland. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Pearson, TRH (reprint author), Univ Aberdeen, Dept Plant & Soil Sci, Cruickshank bldg,St Machar Dr, Aberdeen AB24 3UU, Scotland. OI Burslem, David/0000-0001-6033-0990 NR 42 TC 139 Z9 164 U1 4 U2 50 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD OCT PY 2002 VL 83 IS 10 BP 2798 EP 2807 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 617ER UT WOS:000179348800013 ER PT J AU Stine, JK AF Stine, JK TI Placing environmental history on display SO ENVIRONMENTAL HISTORY LA English DT Article; Proceedings Paper CT Joint American-Society-for-Environmental-History/Forest-History-Society Conference CY MAR 20, 2001 CL DURHAM, NORTH CAROLINA SP Amer Soc Environm Hist, Forest Hist Soc C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Stine, JK (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 41 TC 7 Z9 7 U1 0 U2 0 PU ENVIRONMENTAL HISTORY PI DURHAM PA 701 VICKERS AVE, DURHAM, NC 27701-3147 USA SN 1084-5453 J9 ENVIRON HIST JI Environ. Hist. PD OCT PY 2002 VL 7 IS 4 BP 566 EP 588 DI 10.2307/3986057 PG 23 WC Environmental Studies; History SC Environmental Sciences & Ecology; History GA 616MD UT WOS:000179306800002 ER PT J AU Blum, MJ AF Blum, MJ TI Rapid movement of a Heliconius hybrid zone: Evidence for phase III of Wright's shifting balance theory? SO EVOLUTION LA English DT Article DE dominance drive; Heliconius; moving hybrid zone; shifting balance ID WARNING-COLOR; GENE FLOW; EVOLUTION; MIMICRY; PERSPECTIVE; BUTTERFLIES; SPECIATION; SELECTION; DISPERSAL; DIVERSITY AB It has been proposed that a moving hybrid zone can be a mechanism for the spread of adaptive traits in phase III of Wright's shifting balance model of evolution. Here I present an example of a moving hybrid zone in warningly colored Heliconius butterflies, a system which is considered to be a possible case of shifting balance evolution. Having moved approximately 47 km in 17 years, the hybrid zone shift has led to the H. erato hydara color pattern rapidly displacing the adjacent H. erato petiverana pattern. The movement is potentially due to dominance drive augmenting a slight selective advantage of H. erato hydara over H. erato petiverana, which is largely consistent with theoretical conditions favoring the success of phase III. C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Smithsonian Trop Res Inst, Naos Isl Mol Labs, Unit 0948, APO, AA 34002 USA. RP Blum, MJ (reprint author), Duke Univ, Dept Biol, POB 90338, Durham, NC 27708 USA. NR 39 TC 39 Z9 40 U1 0 U2 9 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD OCT PY 2002 VL 56 IS 10 BP 1992 EP 1998 PG 7 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 615JH UT WOS:000179241700011 PM 12449486 ER PT J AU Husband, R Herre, EA Young, JPW AF Husband, R Herre, EA Young, JPW TI Temporal variation in the arbuscular mycorrhizal communities colonising seedlings in a tropical forest SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE arbuscular mycorrhiza; small subunit; AM1; diversity; succession; seedling recruitment ID HYACINTHOIDES NON-SCRIPTA; ENDOMYCORRHIZAL FUNGI; MOLECULAR DIVERSITY; GROWTH; PRODUCTIVITY; POPULATIONS; STRATEGIES; DYNAMICS; ROOTS AB in order to investigate temporal variation in the arbuscular mycorrhizal (AM) fungal community in a tropical forest in the Republic of Panama, seedlings of the canopy emergent Tetragastris panamensis were sampled three times over a period of 3 years. We used AM-specific primers to amplify and clone partial small subunit ribosomal RNA gene sequences. Over 550 clones were classified into 18 AM fungal types. As the seedlings matured, the fungal diversity decreased and there was a significant shift so that previously rare types replaced formerly dominant fungal types. Further, seedlings of different ages sampled at the same time point were colonised by significantly different fungal populations. Our results indicate that both time and host age may influence the mycorrhizal population. (C) 2002 Federation of European Microbiological Societies. Published by Elsevier Science B.V. All rights reserved. C1 Univ York, Dept Biol, York YO10 5YW, N Yorkshire, England. Smithsonian Trop Res Inst, Balboa, Panama. RP Husband, R (reprint author), Univ York, Dept Biol, POB 373, York YO10 5YW, N Yorkshire, England. RI Young, Peter/C-1446-2012 OI Young, Peter/0000-0001-5259-4830 NR 30 TC 78 Z9 84 U1 3 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-6496 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD OCT PY 2002 VL 42 IS 1 BP 131 EP 136 AR PII S0168-6496(02)00323-9 DI 10.1111/j.1574-6941.2002.tb01002.x PG 6 WC Microbiology SC Microbiology GA 604GD UT WOS:000178607900013 PM 19709272 ER PT J AU Megonigal, JP Schlesinger, WH AF Megonigal, JP Schlesinger, WH TI Methane-limited methanotrophy in tidal freshwater swamps SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article DE methane emissions; methane oxidation; temperature responses; forested wetland; global warming; methanogenesis ID NORTH CENTRAL ALBERTA; CAREX DOMINATED FEN; CARBON REMINERALIZATION; RICE MICROCOSMS; OXIDATION; RHIZOSPHERE; PEATLANDS; EMISSION; WETLAND; FLUX AB [1] We investigated the relationship between CH4 production and oxidation in two tidal freshwater wetland forests in order to determine whether CH4 oxidation efficiency was limited by O-2 or CH4. Methane oxidation was measured in situ over a 16-month period with bi-monthly applications of the inhibitor CH3F. Oxidation consumed 52 +/- 10 and 81 +/- 9% of diffusive CH4 emissions on the two sites. Methane oxidation rates were linearly related to gross CH4 emissions on both sites (r(2) = 0.96), demonstrating the process was CH4-limited. This interpretation is consistent with the fact that the apparent activation energies for the potential CH4 production and oxidation differed by <4 kJ mol(-1). Apparent activation energies calculated from field emissions data were also similar for the two processes. The high CH4 oxidation efficiency on these sites may be attributed to relatively low rates of methane production, a deep oxidizing zone (5-10 cm), and low cover of understory vegetation capable of CH4 transport. If our results are typical of forested wetlands, CH4 oxidation efficiency in forested wetlands will not change in response to soil warming. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 45 TC 26 Z9 29 U1 3 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD OCT-NOV PY 2002 VL 16 IS 4 AR 1088 DI 10.1029/2001GB001594 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 643RK UT WOS:000180874100035 ER PT J AU Hymus, GJ Pontailler, JY Li, J Stiling, P Hinkle, CR Drake, BG AF Hymus, GJ Pontailler, JY Li, J Stiling, P Hinkle, CR Drake, BG TI Seasonal variability in the effect of elevated CO2 on ecosystem leaf area index in a scrub-oak ecosystem SO GLOBAL CHANGE BIOLOGY LA English DT Article DE elevated CO2; leaf area index; leaf expansion; leaf fall; open-top chambers; scrub-oak ecosystem ID LONG-TERM CO2; ATMOSPHERIC CO2; QUERCUS-MYRTIFOLIA; GAS-EXCHANGE; NATIVE ENVIRONMENT; BIOMASS PRODUCTION; GROWTH; ENRICHMENT; TEMPERATURE; SENESCENCE AB We report effects of elevated atmospheric CO2 concentration (C-a) on leaf area index (LAI) of a Florida scrub-oak ecosystem, which had regenerated after fire for between three and five years in open-top chambers (OTCs) and was yet to reach canopy closure. LAI was measured using four nondestructive methods, calibrated and tested in experiments performed in calibration plots near the OTCs. The four methods were: PAR transmission through the canopy, normalized difference vegetation index (NDVI), hemispherical photography, and allometric relationships between plant stem diameter and plant leaf area. Calibration experiments showed: (1) Leaf area index could be accurately determined from either PAR transmission through the canopy or hemispherical photography. For LAI determined from PAR transmission through the canopy, ecosystem light extinction coefficient (k) varied with season and was best described as a function of PAR transmission through the canopy. (2) A negative exponential function described the relationship between NDVI and LAI; (3) Allometric relationships overestimated LAI. Throughout the two years of this study, LAI was always higher in elevated C-a, rising from, 20% during winter, to 55% during summer. This seasonality was driven by a more rapid development of leaf area during the spring and a relatively greater loss of leaf area during the winter, in elevated C-a. For this scrub-oak ecosystem prior to canopy closure, increased leaf area was an indirect mechanism by which ecosystem C uptake and canopy N content were increased in elevated C-a. In addition, increased LAI decreased potential reductions in canopy transpiration from decreases in stomatal conductance in elevated C-a. These findings have important implications for biogeochemical cycles of C, N and H2O in woody ecosystems regenerating from disturbance in elevated C-a. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Paris 11, CNRS, UPR ESA 8079, Dept Ecophysiol Vegetale, F-91405 Orsay, France. Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Gen Dynam Corp, Kennedy Space Ctr, FL 32899 USA. RP Hymus, GJ (reprint author), Smithsonian Environm Res Ctr, Mail Code DYN-2, Kennedy Space Ctr, FL 32899 USA. NR 42 TC 20 Z9 22 U1 2 U2 7 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD OCT PY 2002 VL 8 IS 10 BP 931 EP 940 DI 10.1046/j.1365-2486.2002.00526.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 590YT UT WOS:000177853000001 ER PT J AU Burbine, TH Binzel, RP AF Burbine, TH Binzel, RP TI Small main-belt asteroid spectroscopic survey in the near-infrared SO ICARUS LA English DT Article DE asteroids; composition ID SPECTRAL PROPERTIES; ORDINARY CHONDRITE; S-TYPE; PARENT BODY; VESTA; METEORITES; OLIVINE; REFLECTANCE; DISCOVERY; ELEMENTS AB Near-infrared spectra (similar to0.90 to similar to1.65 mum) are presented for 181 main-belt asteroids, more than half having diameters less than 20 km. These spectra were measured using a specialized grism at the NASA Infrared Telescope Facility, where the near-infrared wavelength coverage is designed to complement visible wavelength CCD measurements for enhanced mineralogic interpretation. We have focused our analysis on asteroids that appear to have surfaces dominated by olivine or pyroxene since these objects can be best characterized with spectral coverage only out to 1.65 mum. Olivine-dominated A-type asteroids have distinctly redder slopes than olivine found in meteorites, possibly due to surface alteration effects such as micro-meteoroid bombardment simulated by laser irradiation laboratory experiments. K-type asteroids observed within the Eos family tend to be well matched by laboratory spectra of CO3 chondrites, while those independent of the Eos family have a variety of spectral properties. The revealed structure of the 1-mum band for 3628 Boznemcova appears to refute its previously proposed match to ordinary chondrite meteorites. Boznemcova displays a 1-mum band that is unlike that for any currently measured meteorite; however, spectra out to 2.5 mum are needed to conclusively argue that Boznemcova has a surface mineralogy different from that of ordinary chondrites. Extending the spectral coverage of Vestoids out to similar to1.65 mum continues to be consistent with the "genetic" relationship of almost all observed Vestoids with Vesta and the howardites, eucrites, and diogenites. Eucrites/howardites provide the best spectral matches to the observed Vestoids. (C) 2002 Elsevier Science (USA). C1 Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Burbine, TH (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 51 TC 71 Z9 71 U1 1 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 OCT PY 2002 VL 159 IS 2 BP 468 EP 499 DI 10.1006/icar.2002.6902 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 601JE UT WOS:000178442000019 ER PT J AU Santos-Granero, F AF Santos-Granero, F TI Boundaries are made to be crossed: The magic and politics of the long-lasting Amazon/Andes divide SO IDENTITIES-GLOBAL STUDIES IN CULTURE AND POWER LA English DT Article DE Amazon; Andes; Peru; boundaries; borderlands; discourse; identity; alterity AB The construction of Amazonia as a distinct entity, opposed to the Andes, results from processes associated with the expansion of Andean-centered state formations. Analysis of five short texts on the Amazon region, written in colonial and postcolonial Peru by a a diversity of social actors, reveals a pervasive rhetoric of alterity whose content varies according to the particular objectives the authors had in mind. In all cases, however, the aim is the same, namely the imposition of boundaries of differentiation as justification for state integration, expressed in the commodification and symbolic consumption of the Amazonian Other. It the politics of boundary making consist in "peripheralizing" and "othering" the Amazon and its people, the magic of boundary making resides in the discursive sleight of hand through which contemporary agents conceal the fact that the Amazon has long ago been incorporated into the nation-state. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, Unit 0948,APO AA, Miami, FL 34002 USA. NR 32 TC 3 Z9 4 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1070-289X J9 IDENTITIES-GLOB STUD JI Identities-Glob. Stud. Cult. Power PD OCT-DEC PY 2002 VL 9 IS 4 BP 545 EP 569 DI 10.1080/10702890290091651 PG 25 WC Ethnic Studies SC Ethnic Studies GA 641XY UT WOS:000180773400006 ER PT J AU Weiss, IM Tuross, N Addadi, L Weiner, S AF Weiss, IM Tuross, N Addadi, L Weiner, S TI Mollusc larval shell formation: Amorphous calcium carbonate is a precursor phase for aragonite SO JOURNAL OF EXPERIMENTAL ZOOLOGY LA English DT Article ID EMBRYOGENESIS; CALCIFICATION; CLAM AB The larval shells of the marine bivalves Mercenaria mercenaria and Crassostrea gigas are investigated by polarized light microscopy, infrared spectroscopy, Raman imaging spectroscopy, and scanning electron microscopy. Both species contain similar shell ultrastructures. We show that larval shells contain amorphous calcium carbonate (ACC), in addition to aragonite. The aragonite is much less crystalline than nonbiogenic aragonite. We further show that the initially deposited mineral phase is predominantly ACC that subsequently partially transforms into aragonite. The postset juvenile shell, as well as the adult shell of Mercenaria also contains aragonite that is less crystalline than nonbiogenic aragonite. We conclude that ACC fulfills an important function in mollusc larval shell formation. It is conceivable that ACC may also be involved in adult shell formation. (C) 2002 Wiley-Liss, Inc. C1 Weizmann Inst Sci, Dept Biol Struct, IL-76100 Rehovot, Israel. Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. RP Weiner, S (reprint author), Weizmann Inst Sci, Dept Biol Struct, IL-76100 Rehovot, Israel. NR 37 TC 357 Z9 370 U1 11 U2 111 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0022-104X J9 J EXP ZOOL JI J. Exp. Zool. PD OCT 1 PY 2002 VL 293 IS 5 BP 478 EP 491 DI 10.1002/jez.90004 PG 14 WC Zoology SC Zoology GA 589EE UT WOS:000177744900005 PM 12486808 ER PT J AU Dixon, T Decaix, J Farina, F Furlong, K Malservisi, R Bennett, R Suarez-Vidal, F Fletcher, J Lee, J AF Dixon, T Decaix, J Farina, F Furlong, K Malservisi, R Bennett, R Suarez-Vidal, F Fletcher, J Lee, J TI Seismic cycle and rheological effects on estimation of present-day slip rates for the Agua Blanca and San Miguel-Vallecitos faults, northern Baja California, Mexico SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE fault slip rates and the seismic cycle; northern Baja California ID POSITIONING SYSTEM CONSTRAINTS; SOUTHERN CALIFORNIA; POSTSEISMIC RELAXATION; SURFACE DEFORMATION; EARTHQUAKE CYCLE; TENSILE FAULTS; ANDREAS FAULT; HALF-SPACE; MOTION; MODEL AB [1] Geodesy can be used to infer long-term fault slip rates, assuming a model for crust and upper mantle rheology. We examine the sensitivity of fault slip rate estimates to assumed rheology for the Agua Blanca and San Miguel-Vallecitos faults in northern Baja California, Mexico, part of the Pacific-North America plate boundary zone. The Agua Blanca fault is seismically quiet, but offset alluvial fans indicate young activity. Current seismicity is confined to the nearby San Miguel-Vallecitos fault, a small offset fault better aligned with plate motion. GPS measurements between 1993 and 1998 suggest that both faults are active, with a combined slip rate of 4-8 mm yr(-1) regardless of rheological model. However, slip rate estimates for the individual faults are sensitive to assumed rheology. Elastic half-space models yield 2-3 mm yr(-1) for the Agua Blanca fault, and somewhat faster rates for the San Miguel-Vallecitos fault, 2-4 mm yr(-1), with uncertainties of about 1 mm yr(-1). Models incorporating viscoelastic rheology and seismic cycle effects suggest a faster slip rate for the Agua Blanca fault, 6 +/- 1 mm yr(-1), and a slower rate for the San Miguel-Vallecitos fault, 1 +/- 1 mm yr(-1), in better agreement with geological data, but these rates are sensitive to assumed rheology. Numerical simulations with a finite element model suggest that for similar rheological and friction conditions, slip on the San Miguel-Vallecitos fault should be favored due to better alignment with plate motion. Long-term faulting processes in the larger offset Agua Blanca fault may have lowered slip resistance, allowing accommodation of motion despite misalignment with plate motion. C1 Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. Penn State Univ, Dept Geosci, Geodynam Res Grp, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Cent Washington Univ, Dept Geol Sci, Ellensburg, WA USA. Ctr Invest Cient & Educ Super Ensenada, Ensenada, Baja California, Mexico. RP Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM tdixon@rsmas.miami.edu NR 62 TC 26 Z9 28 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD OCT PY 2002 VL 107 IS B10 AR 2226 DI 10.1029/2000JB000099 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 637RC UT WOS:000180525500020 ER PT J AU Poletto, G Suess, ST Biesecker, DA Esser, R Gloeckler, G Ko, YK Zurbuchen, TH AF Poletto, G Suess, ST Biesecker, DA Esser, R Gloeckler, G Ko, YK Zurbuchen, TH TI Low-latitude solar wind during the Fall 1998 SOHO-Ulysses quadrature SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE SOHO-Ulysses quadrature; low-latitude solar wind; oxygen flow speed; proton flow speed; in situ data ID POLAR CORONAL HOLE; WHOLE SUN MONTH; PHYSICAL-PROPERTIES; STRAY-LIGHT; TEMPERATURE; UVCS/SOHO; MINIMUM; REGIONS; SPECTROMETER; STREAMERS AB The Fall 1998 Solar and Heliospheric Observatory (SOHO)-Ulysses quadrature occurred when Ulysses was at 5.2 AU, 17.4degreesS of the equator, and off the west limb of the Sun. SOHO coronal observations, at heliocentric distances of a few solar radii, showed that the line through the solar center and Ulysses crossed, over the first days of observations, a dark, weakly emitting area and through the northern edge of a streamer complex during the second half of the quadrature campaign. Ulysses in situ observations showed this transition to correspond to a decrease from higher-speed wind typical of coronal hole flow to low-speed wind. Physical parameters of the low-latitude coronal plasma sampled over the campaign are determined using constraints from what is the same plasma measured later in situ and simulating the intensities of the hydrogen Lyman-alpha and OVI 1032 and 1037 Angstrom lines, measured by the Ultraviolet Coronagraph Spectrometer on SOHO. It appears that low-latitude wind from small coronal holes and polar wind have different characteristics in the corona, differences well known at interplanetary distances through in situ experiments. Small, low-latitude coronal holes have a higher expansion factor than typical polar holes, and their plasma moves at a lower speed than plasma from polar holes, reaching, at 3.5 R-sun, only about one-fifth of the terminal speed. Wind emanating from bright regions, above streamer complexes, is, at the altitudes we analyzed (i.e., 3.5 and 4.5 R-sun), about a factor 3 slower than the low-latitude coronal hole wind, implying a shift to even higher altitudes of the region where plasma gets accelerated. We surmise that open field regions, interspersed amidst closed coronal loops/streamers, may be at least partially responsible for the well-known slow wind speed variability. As in polar fast wind, OVI ions move faster than protons, over the range of altitudes we sampled, and are frozen-in at temperatures of approximate to1.3-1.5 10(6) K, depending on the site where the outflow originates. An oxygen abundance variation from a value of 8.55, in low-latitude holes, to 8.73 in bright areas, has also been inferred. C1 Osserv Astrofis Arcetri, I-50125 Florence, Italy. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NASA, Goddard Space Flight Ctr, Commun Analyt Corp L3, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Poletto, G (reprint author), Osserv Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. NR 50 TC 10 Z9 10 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD OCT PY 2002 VL 107 IS A10 AR 1300 DI 10.1029/2001JA000275 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634RF UT WOS:000180353900035 ER PT J AU Hacker, BC AF Hacker, BC TI Technology, disease and colonial conquests, sixteenth to eighteenth centuries: Essays reappraising the guns and germs theories SO JOURNAL OF MILITARY HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC MILITARY HISTORY PI LEXINGTON PA C/O VIRGINIA MILITARY INST, GEORGE C MARSHALL LIBRARY, LEXINGTON, VA 24450-1600 USA SN 0899-3718 J9 J MILITARY HIST JI J. Mil. Hist. PD OCT PY 2002 VL 66 IS 4 BP 1194 EP 1195 DI 10.2307/3093276 PG 2 WC History SC History GA 597QC UT WOS:000178231400018 ER PT J AU Child, CA AF Child, CA TI Some Pycnogonida from the Eastern (Hasa) District of Saudi Arabia SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Pycnogonida; Saudi Arabia; Ascorhynchus dietheus; Nymphon enteonum AB Seven pycnogonid species are described from the Arabian (Persian) Gulf coast of Saudi Arabia in its Eastern (Hasa) District. Two new species, Ascorhynchus dietheus and Nymphon enteonum, are fully described, illustrated and compared with similar congeners. Distributions and remarks are given for all seven species. A key is given for the 22 species in one of four discrete groups of the genus Ascorhynchus, including the new species. This group has longitarsal distal leg segments and scapes of one segment only. A parasitic juvenile Ascorhynchus species is described and illustrated, but left unnamed for lack of a presumed adult specimen. It is compared with the few other known parasitic specimens in this genus. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Child, CA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 27 TC 2 Z9 3 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD OCT PY 2002 VL 36 IS 15 BP 1805 EP 1821 DI 10.1080/00222930110075189 PG 17 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 597WA UT WOS:000178242700004 ER PT J AU Eberhard, WG AF Eberhard, WG TI The relation between aggressive and sexual behavior and allometry in Palaeosepsis dentatiformis Flies (Diptera : Sepsidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE sexual selection; sepsid flies; allometry ID MALE MATING SUCCESS; REPRODUCTIVE-BEHAVIOR; FUNCTIONAL-MORPHOLOGY; ONE SIZE; FLY; CYNIPSEA; DISPLAY; MICROSEPSIS; EVOLUTION; GENITALIA AB Male Palaeosepsis dentatiformis (Duda) (Diptera: Sepsidae) fought near dung pats that were used as feeding and mating sites by males and females. Males stilted and displayed their sexually dimorphic wing spots during stereotyped threat displays; they fought using rapid pulling and slamming movements of their front legs, and head butting. Males performed several apparent courtship movements during copulation, including tapping the female with their sternal brushes and genitalic squeezing. Allometric slopes of body parts used in aggression (wing spots) were steeper than control values, as is typical of weapons in other species. The slope of sternal brush length was lower, as in the genitalia of this and many other species. C1 Univ Costa Rica, Smithsonian Trop Res Inst, Santiago, Chile. Univ Costa Rica, Escuela Biol, Santiago, Chile. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, Santiago, Chile. NR 43 TC 26 Z9 27 U1 1 U2 4 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 OCT PY 2002 VL 75 IS 4 BP 317 EP 332 PG 16 WC Entomology SC Entomology GA 622UT UT WOS:000179666000011 ER PT J AU Ivanova, MA Petaev, MI MacPherson, GJ Nazarov, MA Taylor, LA Wood, JA AF Ivanova, MA Petaev, MI MacPherson, GJ Nazarov, MA Taylor, LA Wood, JA TI The first known natural occurrence of calcium monoaluminate, in a calcium-aluminum-rich inclusion from the CH chondrite Northwest Africa 470 SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID SOLAR NEBULA; METAL GRAINS; CONDENSATION; CHONDRULES; SYSTEM; ABUNDANCES; CHEMISTRY; METEORITE; ORIGIN AB Natural calcium monoaluminate, CaAl2O4, has been found in a grossite-rich calcium-aluminum-rich inclusion (CAI) from the CH chondrite Northwest Africa 470. The calcium monoaluminate occurs as colorless similar to10 mum subhedral grains intergrown with grossite, perovskite, and melilite. Nebular condensation is the most likely origin for the precursor materials of this CAI, but calculations suggest that dust/gas ratios substantially enhanced over solar are required to stabilize CaAl2O4. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Russian Acad Sci, Vernadsky Inst, Moscow 117795, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. RP MacPherson, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 41 TC 9 Z9 9 U1 1 U2 4 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 OCT PY 2002 VL 37 IS 10 BP 1337 EP 1344 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 608YY UT WOS:000178877100004 ER PT J AU Perdices, A Bermingham, E Montilla, A Doadrio, I AF Perdices, A Bermingham, E Montilla, A Doadrio, I TI Evolutionary history of the genus Rhamdia (Teleostei : Pimelodidae) in Central America SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE catfishes; neotropical freshwater fishes; mitochondrial DNA; ATP synthase; cytochrome b; phylogeography; molecular systematics ID FRESH-WATER FISHES; MITOCHONDRIAL-DNA; CYPRINODONTIFORMES; PHYLOGENY; SEQUENCES; CATFISH AB We constructed phylogenetic hypotheses for Mesoamerican Rhamdia, the only genus of primary freshwater fish represented by sympatric species across Central America. Phylogenetic relationships were inferred from analysis of 1990 base pairs (bp) of mitochondrial DNA (mtDNA), represented by the complete nucleotide sequences of the cytochrome b (cyt b) and the ATP synthase 8 and 6 (ATPase 8/6) genes. We sequenced 120 individuals from 53 drainages to provide a comprehensive geographic picture of Central American Rhamdia systematics and phylogeography. Phylogeographic analysis distinguished multiple Rhamdia mtDNA lineages, and the geographic congruence across evolutionarily independent Rhamdia clades indicated that vicariance has played a strong role in the Mesoamerican diversification of this genus. Phylogenetic analyses of species-level relationships provide strong support for the monophyly of a trans-Andean clade of three evolutionarily equivalent Rhamdia taxa: R. guatemalensis, R. laticauda, and R. cinerascens. Application of fish-based mitochondrial DNA clocks ticking at 1.3-1.5% sequence divergence per million years (Ma), suggests that the split between cis- and trans-Andean Rhamdia extends back about 8 Ma, and the three distinct trans-Andean Rhamdia clades split about 6 Ma ago. Thus the mtDNA divergence observed between cis- and trans-Andean Rhamdia species is too low to support an ancient colonization of Central America in the Late Cretaceous or Paleocene as had been hypothesized in one colonization model for Mesoamerican fishes. Rather the mtDNA data indicate that Rhamdia most likely colonized Central America in the late Miocene or Pliocene, promoting a strong role for the Isthmus of Panama in the Mesoamerican expansion of this genus. Basal polytomies suggest that both the R. laticauda and R. guatemalensis clades spread rapidly across the Central American landscape, but differences in the average mtDNA genetic distances among clades comprising the two species, indicate that the R. laticauda spread and diversified across Mesoamerica about I million years before R. guatemalensis. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Smithsonian Trop Res Inst, Balboa, Panama. CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. RP Perdices, A (reprint author), Smithsonian Trop Res Inst, Apto 2072, Balboa, Panama. RI Montilla, Antonia/J-4116-2012; OI Montilla, Antonia/0000-0003-2117-6999; Doadrio, Ignacio/0000-0003-4863-9711 NR 54 TC 115 Z9 122 U1 0 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2002 VL 25 IS 1 BP 172 EP 189 AR PII S1055-7903(02)00224-5 DI 10.1016/S1055-7903(02)00224-5 PG 18 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 611QC UT WOS:000179028400014 PM 12383759 ER PT J AU Pierce, S Winter, K Griffiths, H AF Pierce, S Winter, K Griffiths, H TI Carbon isotope ratio and the extent of daily CAM use by Bromeliaceae SO NEW PHYTOLOGIST LA English DT Article DE Bromeliad; carbon pathway; crassulacean acid metabolism (CAM); delta C-13; epiphyte; photosynthesis ID CRASSULACEAN-ACID-METABOLISM; GUZMANIA-MONOSTACHIA; EPIPHYTIC BROMELIAD; VASCULAR EPIPHYTES; RESPONSES AB Use of carbon isotope ratio (delta(13)C) to resolve photosynthetic pathways (C-3, C-4 or CAM) has limitations imposed by the use of intermediate photosynthetic modes by certain plant taxa. Diel gas-exchange patterns, leaf delta(13)C values and nocturnal tissue acidification were determined for 50 Bromeliaceae. delta(13)C values for well watered plants reflected the proportion of daily CO2 uptake occurring at night. Thirteen per cent of species with delta(13)C values typical of C-3 plants (i.e. from -22.6 to -31.5parts per thousand) showed nocturnal acidification and either a small proportion (< 10%) of daily CO2 uptake occurring nocturnally or internal CO2 recycling during part of the night. None altered CAM expression in response to short-term drought, but the contribution of CAM to daily carbon gain became proportionally more important as C-3 CO2 uptake failed. Surveys of plant communities using solely the carbon isotope technique underestimate the number of CAM-equipped plants. C1 Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. Smithsonian Trop Res Inst, Panama City, Panama. RP Pierce, S (reprint author), Univ Cambridge, Dept Plant Sci, Downing St, Cambridge CB2 3EA, England. OI Pierce, Simon/0000-0003-1182-987X NR 29 TC 45 Z9 50 U1 2 U2 21 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0028-646X J9 NEW PHYTOL JI New Phytol. PD OCT PY 2002 VL 156 IS 1 BP 75 EP 83 DI 10.1046/j.1469-8137.2002.00489.x PG 9 WC Plant Sciences SC Plant Sciences GA 592XK UT WOS:000177962000009 ER PT J AU Lovelock, CE Robinson, SA AF Lovelock, CE Robinson, SA TI Surface reflectance properties of Antarctic moss and their relationship to plant species, pigment composition and photosynthetic function SO PLANT CELL AND ENVIRONMENT LA English DT Article DE Bryum pseudotriquetrum; Ceratodon purpureus; Grimmia antarctici; chlorophyll; chlorophyll fluorescence; photochemical reflectance index; xanthophyll cycle pigments ID RADIATION-USE EFFICIENCY; SPECTRAL REFLECTANCE; RED EDGE; CHLOROPHYLL FLUORESCENCE; CONTINENTAL ANTARCTICA; SUNFLOWER LEAVES; CANOPY-LEVEL; VEGETATION; LEAF; PHOTOINHIBITION AB In this study the variations in surface reflectance properties and pigment concentrations of Antarctic moss over species, sites, microtopography and with water content were investigated. It was found that species had significantly different surface reflectance properties, particularly in the region of the red edge (approximately 700 nm), but this did not correlate strongly with pigment concentrations. Surface reflectance of moss also varied in the visible region and in the characteristics of the red edge over different sites. Reflectance parameters, such as the photochemical reflectance index (PRI) and cold hard band were useful discriminators of site, microtopographic position and water content. The PRI was correlated both with the concentrations of active xanthophyll-cycle pigments and the photosynthetic light use efficiency, F-v/F-m, measured using chlorophyll fluorescence. Water content of moss strongly influenced the amplitude and position of the red-edge as well as the PRI, and may be responsible for observed differences in reflectance properties for different species and sites. All moss showed sustained high levels of photoprotective xanthophyll pigments, especially at exposed sites, indicating moss is experiencing continual high levels of photochemical stress. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Wollongong, Inst Conservat Biol, Wollongong, NSW 2522, Australia. RP Lovelock, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Robinson, Sharon/B-2683-2008; Lovelock, Catherine/G-7370-2012 OI Robinson, Sharon/0000-0002-7130-9617; Lovelock, Catherine/0000-0002-2219-6855 NR 54 TC 56 Z9 58 U1 2 U2 23 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD OCT PY 2002 VL 25 IS 10 BP 1239 EP 1250 DI 10.1046/j.1365-3040.2002.00916.x PG 12 WC Plant Sciences SC Plant Sciences GA 595YA UT WOS:000178134800004 ER PT J AU Gwinn, N AF Gwinn, N TI Evidence in hand: Report of the task force on the artifact in library collections. SO PORTAL-LIBRARIES AND THE ACADEMY LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Gwinn, N (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 1531-2542 J9 PORTAL-LIBR ACAD JI Portal-Libr. Acad PD OCT PY 2002 VL 2 IS 4 BP 676 EP 678 DI 10.1353/pla.2002.0078 PG 3 WC Information Science & Library Science SC Information Science & Library Science GA 636CB UT WOS:000180436000016 ER PT J AU Hall, JPW Harvey, DJ AF Hall, JPW Harvey, DJ TI A revision of the Neotropical butterfly genus Seco Hall and Harvey (Lepidoptera : Riodinidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Charis; Neotropics; Riodinini; Seco; xeric habitats AB The South American riodinid genus Seco Hall and Harvey is revised. The taxonomy and biology of its species are discussed, locality data and range maps are given, and the adults and male and female genitalia (where known) are illustrated for all species. 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 17 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 OCT PY 2002 VL 104 IS 4 BP 941 EP 947 PG 7 WC Entomology SC Entomology GA 601GA UT WOS:000178437100011 ER PT J AU Polhemus, DA AF Polhemus, DA TI Two new species of orsilline Lygaeidae (Heteroptera) from the Hawaiian Islands SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Lygaeidae; Hawaii; Oceanides; Nesius; new species; illustrations; key AB Two new species of orsilline Lygacidae are described from the Hawaiian Islands: Oceanides gruneri, taken in canopy fogging samples from ohia trees (Metrosideros polymorpha) on eastern Molokai; and Nesius (Physonysius) poepoe, collected from understory vegetation in the upper elevations of the West Maui Mountains. Shaded habitus drawings and distribution maps are provided for both new species, the male paramere of N. (Physonysius) poepoe is illustrated, and a revised key to the species in the subgenus Physonysius is included. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Polhemus, DA (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Systemat Biol Entomol, Washington, DC 20560 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2002 VL 104 IS 4 BP 955 EP 963 PG 9 WC Entomology SC Entomology GA 601GA UT WOS:000178437100013 ER PT J AU Adamski, D Brown, JW AF Adamski, D Brown, JW TI A new species of Frumenta Busck (Lepidoptera : Gelechiidae : Gnorimoschemini) from Mexico: A potential biocontrol agent against Solanum elaeagnifolium (Solanaccae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Gelechiidae; Solarium; biocontrol ID HOST-SPECIFIC HERBIVORE; MAURITIANUM SCOP AB Frumenta solanophaga, new species, is described from San Luis Potosi, Mexico. It was reared from Solanum elaeagnifolium Cavanilles (Solanaceae) as part of a survey for potential biocontrol agents against this introduced weed in southern Africa. Frumenta also includes two previously described species from southern United States; the group appears to feed exclusively on Solanum. Photographs and illustrations of F. solanophaga depict the imago, wing venation, intersegmental abdominal lobes of the female, and male and female genitalia. A key to the species of Frumenta is provided. C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. RP Adamski, D (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. NR 31 TC 1 Z9 1 U1 3 U2 9 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2002 VL 104 IS 4 BP 1029 EP 1035 PG 7 WC Entomology SC Entomology GA 601GA UT WOS:000178437100020 ER PT J AU Nowicke, JW Takahashi, M AF Nowicke, JW Takahashi, M TI Pollen morphology, exine structure and systematics of Acalyphoideae (Euphorbiaceae), Part 4 SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY LA English DT Article DE Acalyphoidea; exine structure; pollen; systematics ID TRIBES; PLUKENETIEAE; EVOLUTION; PHYLOGENY; SYNOPSIS; RICINUS; WETRIA AB This is the fourth, last and largest installment of a palynological study of the Acalyphoideae that examined in light, scanning electron and transmission electron microscopy, the pollen of a grand total of 460 collections representing 372 species from 112 of the 116 assigned genera. Part 4 describes the pollen of tribe Acalypheae pro parte, subtribes Claoxylinae (Erythrococca, Claoxylon, Claoxylopsis, Mareya, Mareyopsis. Discoclaoxylon, Micrococca, Amyrea), Lobaniliinae (Lobanilia), Rottlerinae (Mallotus, Deuteromallotus, Cordemoya, Cococceras, Trewia, Neotrewia, Rockinghamia, Octospermum), Acalyphinae (Acalypha), Lasiococcinae (Lasiococca, Spathiostemon, Homonoia), tribe Plukenetieae, subtribe Plukenetiinae (Haematostemon, Astrococcus, Angostyles, Romanoa, Eleutherostigma, Plukenetia, Vigia); subtribe Tragiinae (Cnesmone, Megistostigma, Sphaerortylis, Tragiella, Platygyna, Tragia, Acidoton, (Pachystylidium); subtribe Dalechampiinae (Dalechampia) and tribe Omphaleae (Omphalea). None of the above multigeneric tribes or subtribes have uniform morphology or exine structure, but, with the notable exception of Plukenetieae, neither do they have any genera with outstanding palynological distinctions. Most members of Cloaxylinae have pollen of a generalized type. although the data support the separation of Mareyopsis from Mareya. Pollen of Amyrea is distinguished by a striate sculpture. Pollen of Mallotus is uniform and representative of the subtribe Rottlerinae: punctate-microspinulose tecta. thin foot layers, small columellae and thick continuous tecta. Pollen of Acalypha is small, brevicolp(or)ate, and mostly angulaperturate in polar view. One genus of subtribe Lasiococcinae, Spathiostemon, has a supratectal sculpture of lirae with cross striations, while a second, Homonoia, has a tectum. composed of elongate, vertically oriented individual rods with acute tips. The exine structure of the large tribe Plukenetieae is strikingly diverse with most variants unique in the Acalyphoideae if not the family. Pollen of most members of Plukenetiinae is of either the Conophora type (punctate tecta, prominent columellae, and granular area under the tectum) or the Loretensis type (reticulate exines, crenate muri, unremarkable structure). Pollen of subtribe Tragiinae is more diverse than Plukenetiinae. Three Asian genera, Cnesmone, Megistostigma and Pachystylidium, have poorly defined apertures, and reduced exines. Inaperturate pollen is present in Platygyna, two species of Acidoton and Tragia sellowiana, all of which have exines consisting mostly of columellae, Three pollen types are recognized in Tragia: (1) the Ramosa type is three-colpate, intectate, and has exines or large columellae and thick foot layers; (2) the Lukafuensis type is three-colpate and has reticulate exines with arched colpal margins at the equator; (3) the Urens type has poorly defined apertures, is tectate with exines lacking foot layers. Pollen of Tragiella is very similar to the Lukafuensis type of Tragia. The large grains of the monogeneric subtribe Dalechampiinae are characterized by two prominent equatorial bands (costae). In Plukenetieae, the pollen data support: the reduction of three monotypic genera, Eleutherostigma, Romanoa and Vigia to species of Plukenetia: a close relationship among Cnesmone. Megistostigma and Pachystylidium; a congeneric treatment of Platygyna and Acidoton microphyllus and A. urens, or at least the restriction of Acidoton to these two species; separate generic status for Tragia sect. Tragia which has the Ramosa pollen type; a congeneric treatment of Tragiella and those species of Tragia (T sect. Tagira) with the Lukafuensis pollen type; separate tribal status for Dalechampia. Pollen of Omphaleae is three-colpate, has irregular columellae and foot layers, and a non-apertural endexine that, after acetolysis, separates from the ectexine like the aperturate pollen of Crotonoideae. The results of the pollen study of the entire Acalyphoideae are discussed and Parts 1, 2 and 3 are summarized. Of the multigeneric tribes and subtribes, there are significant pollen differences among the taxa of Ampereae, of Chrozophoreae (subtribe Ditaxinae), of Pycnocomeae (subtribe Pycnocominae), and of Adelieae, as well as taxa of Plukenetieae. The nearly identical pollen of Ricininae and Adrianinae would support their treatment as one subtribe. The subtribes Mercurialinae and Dysopsidinae share similar pollen that is sufficiently distinct from the remaining Acalypheae to merit their treatment as one subtribe. Most pollen of Acalyphoideae is three-colporate with a lalongate endoaperture and punctate-microspinulose or punctate sculpture. Most exines consist of thin foot layers, modest columellae and continuous, mostly thick tecta. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Niigata Univ, Fac Sci, Dept Environm Sci, Niigata 9502181, Japan. RP Nowicke, JW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, NHB 166, Washington, DC 20560 USA. NR 27 TC 27 Z9 30 U1 1 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0034-6667 J9 REV PALAEOBOT PALYNO JI Rev. Palaeobot. Palynology PD OCT PY 2002 VL 121 IS 3-4 BP 231 EP 336 AR PII S0034-6667(02))00087-8 DI 10.1016/S0034-6667(02)00087-8 PG 106 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA 613MQ UT WOS:000179136400003 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI Stalin's V-2 - Technology transfer and German remote control systems in the USSR and the development of the Soviet missile industry 1945-1959 SO TECHNOLOGY AND CULTURE LA English DT Book Review 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 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 OCT PY 2002 VL 43 IS 4 BP 820 EP 822 DI 10.1353/tech.2002.0165 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 621AM UT WOS:000179566400030 ER PT J AU Hall, JPW Harvey, DJ AF Hall, JPW Harvey, DJ TI A survey of androconial organs in the Riodinidae (Lepidoptera) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE abdominal androconia; alar androconia; coremata; courtship; leg androconia; morphology; perching; pheromones; scale structure ID CHEMICAL COMMUNICATION; BUTTERFLIES; NYMPHIDIINI; MORPHOLOGY; COURTSHIP; EVOLUTION AB A comprehensive survey of the occurrence and morphology of alar, abdominal and appendage androconial organs in the Riodinidae is presented based on light microscopy and scanning electron microscopy. Although historically poorly studied, the group actually possesses among the greatest diversity of androconial organs in the butterflies, including coremata, reported here for the first time outside the Lycaenidae and Nymphalidae, and hindleg hair-pencils, reported here for the first time in the true butterflies, Twenty-five percent of riodinid species are reported to have androconial organs. The mode of function of these organs and their role in courtship is discussed where known, based on field observations. A number of taxonomic changes are made at the tribal, generic and species level, predominantly in the Symmachiini, based on the occurrence and structure of androconia. (C) 2002 The Linnean Society of London. C1 Smithsonian Inst, Dept Systemat Biol Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Dept Systemat Biol Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 75 TC 34 Z9 43 U1 2 U2 10 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD OCT PY 2002 VL 136 IS 2 BP 171 EP 197 DI 10.1046/j.1096-3642.2002.00003.x PG 27 WC Zoology SC Zoology GA 596LF UT WOS:000178165800001 ER PT J AU Gavrila, M AF Gavrila, M TI Atomic stabilization in superintense laser fields SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Review ID FREQUENCY FLOQUET-THEORY; SHORT-RANGE POTENTIALS; ABOVE-THRESHOLD PHOTODETACHMENT; INTENSE ELECTROMAGNETIC-FIELDS; DEPENDENT SCHRODINGER-EQUATION; CIRCULARLY-POLARIZED FIELD; EXCITED HYDROGEN-ATOMS; ADIABATIC STABILIZATION; MODEL-ATOM; RYDBERG ATOMS AB Atomic stabilization is a highlight of superintense laser-atom physics. A wealth of information has been gathered on it; established physical concepts have been revised in the process; points of contention have been debated. Recent technological breakthroughs are opening exciting perspectives of experimental study. With this in mind, we present a comprehensive overview of the phenomenon. We discuss the two forms of atomic stabilization identified theoretically. The first one, 'quasistationary (adiabatic) stabilization' (QS), refers to the limiting case of plane-wave monochromatic radiation. QS characterizes the fact that ionization rates, as calculated from single-state Floquet theory, decrease with intensity (possibly in an oscillatory manner) at high values of the field. We present predictions for QS from various forms of Floquet theory: high frequency (that has led to its discovery and offers the best physical insight), complex scaling, Sturmian, radiative close coupling and R-matrix. These predictions all agree quantitatively, and high-accuracy numerical results have been obtained for hydrogen. Predictions from non-Floquet theories are also discussed. Thereafter, we analyse the physical origin of QS. The alternative form of stabilization, 'dynamic stabilization' (DS), is presented next. Ibis expresses the fact that the ionization probability at the end of a laser pulse of fixed shape and duration does not approach unity as the peak intensity is increased, but either starts decreasing with the intensity (possibly in an oscillatory manner), or flattens out at a value smaller than unity. We review the extensive research done on one-dimensional models, that has provided valuable insights into the phenomenon; two- and three-dimensional models are also considered. Full three-dimensional Coulomb calculations have encountered severe numerical handicaps in the past, and it is only recently that a comprehensive mapping of DS could be made for hydrogen. An adiabatic variation of the laser-pulse envelope keeps the system in the Floquet state associated with the initial state, that allows calculation of the ionization probability in terms of the corresponding rate. A nonadiabatic variation can excite other Floquet states, either discrete ('shake-up') or continuous ('shake-off'), with considerable consequences for DS. A unitary interpretation of these aspects of DS is presented in terms of 'multistate Floquet theory'. We then comment on the points of contention raised in connection with DS. Further, we review the extent to which the classical approach has been successful in describing DS. We next examine the concern that nonrelativistic (NR) predictions for stabilization may be inadequate in superintense fields, because relativistic corrections would invalidate them. It turns out that, although the relativistic corrections do limit stabilization, there is an ample 'window' of intensities for which the NR predictions remain valid. Finally, we discuss the experimental evidence in favour of stabilization. For lack of adequate lasers to study ground states of single-active-electron atoms, the experiments so far have been performed on low-lying Rydberg states. Two state-of-the-art experiments have determined ionization yields for pulses with adiabatic envelopes. Their results concur, are in agreement with the theoretical predictions and represent a clear-cut confirmation of DS. Our conclusion is that superintense field stabilization is firmly established, both theoretically and experimentally. Nevertheless, further research is desirable to solve interesting open problems, some of which we identify. Their research is made timely by the superintense high-frequency light sources that are being developed, such as VUV-FELs, or attosecond pulses from high-harmonic generation. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. FOM, Inst Atom & Mol Phys, NL-1098 SJ Amsterdam, Netherlands. RP Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 204 TC 139 Z9 144 U1 2 U2 18 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 SEP 28 PY 2002 VL 35 IS 18 BP R147 EP R193 AR PII S0953-4075(02)89858-3 DI 10.1088/0953-4075/35/18/201 PG 47 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 606CA UT WOS:000178714500002 ER PT J AU Granger, BE Kral, P Sadeghpour, HR Shapiro, M AF Granger, BE Kral, P Sadeghpour, HR Shapiro, M TI Highly extended image states around nanotubes SO PHYSICAL REVIEW LETTERS LA English DT Article ID METAL-SURFACES; POTENTIAL STATES; CARBON NANOTUBES; SPECTROSCOPY; CHARGE; MOLECULES; LIFETIME; ATOMS; WALL AB We predict that freely suspended, linear molecular conductors or dielectrics, such as carbon nanotubes, can support electronic states that are localized far from the surface. These "tubular image states" are formed in extended potential wells resulting from the tug of war between the external electron's attraction to its image charge in the nanotube, and its repulsion from the tube due to its transverse angular momentum. The displacement of these states (>10 nm) away from the surface prevents their wave functions from collapsing, resulting in long lifetimes at low temperatures. We predict that tubular image states with binding energies of 1-10 meV can be formed via radiative recombination. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. RP Granger, BE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. EM bgranger@cfa.harvard.edu; kral@weizmann.ac.il; hsadeghpour@cfa.harvard.edu; moshe.shapiro@weizmann.ac.il NR 38 TC 66 Z9 66 U1 3 U2 9 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 SEP 23 PY 2002 VL 89 IS 13 AR 135506 DI 10.1103/PhysRevLett.89.135506 PG 4 WC Physics, Multidisciplinary SC Physics GA 594VH UT WOS:000178071800029 PM 12225038 ER PT J AU Yoshida, N Stoehr, F Springel, V White, SDM AF Yoshida, N Stoehr, F Springel, V White, SDM TI Gas cooling in simulations of the formation of the galaxy population SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : N-body simulations; galaxies : clusters : general; galaxies : evolution ID DARK-MATTER; COSMOLOGICAL SIMULATIONS; NUMERICAL RESOLUTION; CLUSTER; HALOS; EVOLUTION; UNIVERSE; BIAS; Z=0 AB We compare two techniques for following the cooling of gas and its condensation into galaxies within high-resolution simulations of cosmologically representative regions. Both techniques treat the dark matter using N-body methods. One follows the gas using smoothed particle hydrodynamics (SPH) while the other uses simplified recipes from semi-analytic (SA) models. We compare the masses and locations predicted for dense knots of cold gas (the 'galaxies') when the two techniques are applied to evolution from the same initial conditions and when the additional complications of star formation and feedback are ignored. We find that above the effective resolution limit of the two techniques, they give very similar results both for global quantities such as the total amount of cooled gas and for the properties of individual 'galaxies'. The SA technique has systematic uncertainties arising from the simplified cooling model adopted, while details of the SPH implementation can produce substantial systematic variations in the galaxy masses it predicts. Nevertheless, for the best current SPH methods and the standard assumptions of the SA model, systematic differences between the two techniques are remarkably small. The SA technique gives adequate predictions for the condensation of gas into 'galaxies' at less than one per cent of the computational cost of obtaining similar results at comparable resolution using SPH. C1 Max Planck Inst Astrophys, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoshida, N (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. EM nyoshida@cfa.harvard.edu RI Yoshida, Naoki/A-4305-2011 NR 29 TC 73 Z9 73 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 SEP 21 PY 2002 VL 335 IS 3 BP 762 EP 772 DI 10.1046/j.1365-8711.2002.05661.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 598NR UT WOS:000178283100029 ER PT J AU Finch, TK Carlivati, LP Winn, JN Schechter, PL AF Finch, TK Carlivati, LP Winn, JN Schechter, PL TI Analytic expressions for mean magnification by a quadrupole gravitational lens SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; methods : analytical ID MODELS; STATISTICS; QUASARS AB We derive an analytic expression for the mean magnification due to strong gravitational lensing, using a simple lens model: a singular isothermal sphere embedded in an external shear field. We compute separate expressions for two-image and four-image lensing. For four-image lensing, the mean magnification takes a particularly simple form: (mu(4)) = 3.6/[gamma(1-gamma(2))], where gamma is the external shear. We compare our analytic results with a numerical evaluation of the full magnification distribution. The results can be used to understand the magnification bias that favors the discovery of four-image systems over two-image systems in flux-limited lens surveys. C1 MIT, Cambridge, MA 02139 USA. Howard Univ, Washington, DC 20059 USA. Harvard Univ, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Finch, TK (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 25 TC 19 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 SEP 20 PY 2002 VL 577 IS 1 BP 51 EP 56 DI 10.1086/342163 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594DJ UT WOS:000178033200005 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, JSB Loeb, A TI Gravitational lensing of the Sloan Digital Sky Survey high-redshift quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : high-redshift; gravitational lensing; quasars : general ID ELLIPTICAL POTENTIAL WELLS; LUMINOSITY FUNCTION; COSMOLOGICAL CONSTANT; COMMISSIONING DATA; GALAXIES; EVOLUTION; LENSES; DISTRIBUTIONS; STATISTICS; UNIVERSE AB We predict the effects of gravitational lensing on the color-selected flux-limited samples of z(s) similar to 4.3 and zs e 5 : 8 quasars, recently published by the Sloan Digital Sky Survey (SDSS). Our main findings are the following: ( 1) The lensing probability should be 1 2 orders of magnitude higher than for conventional surveys. The expected fraction of multiply imaged quasars is highly sensitive to redshift and the uncertain slope of the bright end of the luminosity function, beta(h). For beta(h) = 2.58 (3.43) we find that at z(s) similar to 4.3 and i* < 20.0 the fraction is &SIM;4% (13%), while at z(s) &SIM; 6 and z* < 20.2 the fraction is similar to7% (30%). (2) The distribution of magnifications is heavily skewed; sources having the redshift and luminosity of the SDSS zs e 5 : 8 quasars acquire median magnifications of med(mu(obs)) similar to1.1-1.3 and mean magni cations of (mu(obs)) similar to 5-50. Estimates of the quasar luminosity density at high redshift must therefore filter out gravitationally lensed sources. ( 3) The flux in the Gunn-Peterson trough of the highest redshift (z(s) = 6.28) quasar is known to be f(lambda) < 3 x 10(-19) ergs s(-1) cm(-2) &ANGS;(-1). Should this quasar be multiply imaged, we estimate a 40% chance that light from the lens galaxy would have contaminated the same part of the quasar spectrum with a higher flux. Hence, spectroscopic studies of the epoch of reionization need to account for the possibility that a lens galaxy, which boosts the quasar flux, also contaminates the Gunn-Peterson trough. (4) Microlensing by stars should result in &SIM;1/3 of multiply imaged quasars in the z(s) &GSIM; 5.8 catalog varying by more than 0.5 mag over the next decade. The median emission-line equivalent width of multiply imaged quasars would be lowered by &SIM;20% with respect to the intrinsic value because of differential magni cation of the continuum and emission-line regions. 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 57 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 SEP 20 PY 2002 VL 577 IS 1 BP 57 EP 68 DI 10.1086/342181 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594DJ UT WOS:000178033200006 ER PT J AU Karovska, M Fabbiano, G Nicastro, F Elvis, M Kraft, RP Murray, SS AF Karovska, M Fabbiano, G Nicastro, F Elvis, M Kraft, RP Murray, SS TI X-ray arc structures in Chandra images of NGC 5128 (Centaurus A) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Centaurus A, NGC 5128); X-rays : galaxies ID GALAXY; NGC-5128; ATLAS AB We describe results from our initial study of the diffuse X-ray emission structures in NGC 5128 (Centaurus A) using the Chandra X-ray Observatory observations. The high angular resolution Chandra images reveal multiscale X-ray structures with unprecedented detail and clarity. The large-scale structures suggest complex symmetry, including a component possibly associated with the inner radio lobes, and a separate component with an orthogonal symmetry that may be associated with the galaxy as a whole. We detect arclike soft X-ray structures, extending to similar to8 kpc in the direction perpendicular to the jet. These arcs appear to be tracing an ellipse, or a ring seen in projection, and are enclosed between the dust and H I-emitting gas in the central region of the galaxy and the optical and H I shell fragments at a distance of about 8 10 kpc. The diffuse X-ray and the optical emission in the arcs could originate in a region of interaction ( possibly a shock) between the infalling material from the outer regions of the galaxy and the cool dust and H I-emitting material in the center or from an equatorial outflow resulting from an outburst of nuclear activity similar to10(7) yr ago. 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. OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 24 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 SEP 20 PY 2002 VL 577 IS 1 BP 114 EP 119 DI 10.1086/342126 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594DJ UT WOS:000178033200011 ER PT J AU Sun, M Murray, SS AF Sun, M Murray, SS TI Chandra view of the dynamically young cluster of galaxies A1367. II. Point sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (A1367); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; X-RAY-EMISSION; OPTICAL SURVEY; RICH CLUSTERS; ABELL-1367; ROSAT; COMA; STATISTICS; ASCA AB A40ks Chandra ACIS-S observation of the dynamically young cluster A1367 yields new insights on X-ray emission from cluster member galaxies. We detect 59 pointlike sources in the ACIS field, of which eight are identified with known cluster member galaxies. Thus, in total 10 member galaxies are detected in X-rays when three galaxies discussed in Paper I (NGC 3860 is discussed in both papers) are included. The superior spatial resolution and good spectroscopy capability of Chandra allow us to constrain the emission nature of these galaxies. Central nuclei, thermal halos, and stellar components are revealed in their spectra. Two new low-luminosity active galactic nuclei (LLAGNs) are found, including an absorbed one ( NGC 3861). Besides these two for sure, two new LLAGN candidates are also found. This discovery makes the LLAGN/AGN content in this part of A1367 very high (greater than or similar to12%). Thermal halos with temperatures around 0.5-0.8 keV are revealed in the spectra of NGC 3842 and NGC 3837, which suggests that galactic coronae can survive in clusters and that heat conduction must be suppressed. The X-ray spectrum of NGC 3862 (3C 264) resembles a BL Lac object with a photon index of similar to2.5. We also present an analysis of other point sources in the field and discuss the apparent source excess (similar to2.5 sigma) in the central field. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 38 TC 23 Z9 23 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 SEP 20 PY 2002 VL 577 IS 1 BP 139 EP 149 DI 10.1086/342156 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594DJ UT WOS:000178033200014 ER PT J AU Narayan, R Quataert, E Igumenshchev, IV Abramowicz, MA AF Narayan, R Quataert, E Igumenshchev, IV Abramowicz, MA TI The magnetohydrodynamics of convection-dominated accretion flows SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; convection; instabilities; MHD; turbulence ID BLACK-HOLES; 3 DIMENSIONS; INSTABILITY; STABILITY; DISKS; TURBULENCE; TRANSPORT AB Radiatively inefficient accretion flows onto black holes are unstable due to both an outwardly decreasing entropy ("convection") and an outwardly decreasing rotation rate (the "magnetorotational instability" [MRI]). Using a linear MHD stability analysis, we show that long-wavelength modes with lambda/H >> beta(-1/2) are primarily destabilized by the entropy gradient and that such convective modes transport angular momentum inward (lambda is the wavelength of the mode, H is the scale height of the disk, and beta is the ratio of the gas pressure to the magnetic pressure). Moreover, the stability criteria for the "convective" modes are the standard Hoiland criteria of hydrodynamics. By contrast, shorter wavelength modes with lambda/H similar to beta(-1/2) are primarily destabilized by magnetic tension and differential rotation. These "MRI" modes transport angular momentum outward. The convection-dominated accretion flow (CDAF) model, which has been proposed for radiatively inefficient accretion onto a black hole, posits that inward angular momentum transport and outward energy transport by long-wavelength convective fluctuations are crucial for determining the structure of the accretion flow. Our analysis suggests that the CDAF model is applicable to an MHD accretion flow provided that the magnetic field saturates at a value sufficiently below equipartition (beta >> 1), so that long-wavelength convective fluctuations with lambda/H >> beta(-1/2) can fit inside the accretion disk. Numerical MHD simulations are required to determine whether such a subequipartition field is in fact obtained. C1 Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08540 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Rochester, Laser Energet Lab, Rochester, NY 14623 USA. Chalmers Univ Technol, Goteborg Univ, Dept Astron & Astrophys, S-41296 Gothenburg, Sweden. Harvard Smithsonian Ctr Astrophys, Dept Astron, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08540 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 30 TC 65 Z9 65 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 SEP 20 PY 2002 VL 577 IS 1 BP 295 EP 301 DI 10.1086/342159 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594DJ UT WOS:000178033200027 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, SJ Bromley, BC TI Dusty rings: Signposts of recent planet formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; solar system : formation; stars : formation ID ACCRETIONAL EVOLUTION; PROTOPLANETARY DISK; CIRCUMSTELLAR DISK; SOLAR NEBULA; KUIPER-BELT; STARS; PLANETESIMALS; SWARM; FRAGMENTATION; HR-4796A AB Many nearby stars are surrounded by a bright ring or disk of cold dust. Our calculations show that these disks and rings of dust are signposts of recent planet formation. Bright rings appear because dust associated with the formation of a planet absorbs and scatters light from the central star. The calculations explain the rings observed so far and predict that all nascent solar systems have dusty rings. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 39 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 SEP 20 PY 2002 VL 577 IS 1 BP L35 EP L38 DI 10.1086/344084 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594DQ UT WOS:000178033800009 ER PT J AU Sanz, ME McCarthy, MC Thaddeus, P AF Sanz, ME McCarthy, MC Thaddeus, P TI Laboratory detection of HSiCN and HSiNC SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; line : identification; molecular data; molecular processes; radio lines : ISM ID ASTRONOMICAL DETECTION; SPECTRA; SICN; IDENTIFICATION; IRC-+10216; IRC+10216; SIS AB Two new silicon-bearing molecules, the closed-shell asymmetric tops cyanosilylene HSiCN and its isomer HSiNC, have been detected in a laboratory discharge by molecular beam Fourier transform microwave spectroscopy. The rotational spectra of the normal and deuterated isotopic species of both molecules have been analyzed to derive precise spectroscopic constants, which allow the astronomically most interesting transitions up to 120 GHz to be calculated to an accuracy better than 1 km s(-1) in equivalent radial velocity. Both molecules are good candidates for astronomical detection, closely related in structure and composition to known astronomical molecules, and they are highly polar, with estimated dipole moments of 3.5 D for HSiCN and 2.5 D for HSiNC. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Sanz, ME (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Sanz, Maria Eugenia/F-7054-2013; OI McCarthy, Michael/0000-0001-9142-0008 NR 22 TC 18 Z9 18 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 SEP 20 PY 2002 VL 577 IS 1 BP L71 EP L74 DI 10.1086/344083 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594DQ UT WOS:000178033800017 ER PT J AU Stahl, J AF Stahl, J TI Katherine Dunham: Dancing a life. 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 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 SEP 15 PY 2002 VL 127 IS 15 BP 63 EP 63 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 754JN UT WOS:000187312800050 ER PT J AU Nandra, K Mushotzky, RF Arnaud, K Steidel, CC Adelberger, KL Gardner, JP Teplitz, HI Windhorst, RA AF Nandra, K Mushotzky, RF Arnaud, K Steidel, CC Adelberger, KL Gardner, JP Teplitz, HI Windhorst, RA TI X-ray properties of Lyman break galaxies in the Hubble Deep Field North Region SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : evolution; galaxies : high-redshift; galaxies : nuclei; X-rays : galaxies ID STAR-FORMATION HISTORY; ULTRAVIOLET LUMINOSITY DENSITY; SPECTRAL ENERGY-DISTRIBUTIONS; HIGH-REDSHIFT GALAXIES; BLACK-HOLE MASS; INFRARED GALAXIES; FORMING GALAXIES; VELOCITY DISPERSION; SOURCE COUNTS; CHANDRA AB We describe the X-ray properties of a large sample of z similar to 3 Lyman break galaxies (LBGs) in the region of the Hubble Deep Field North, derived from the 1 Ms public Chandra observation. Of our sample of 148 LBGs, four are detected individually. This immediately gives a measure of the bright AGN fraction in these galaxies of similar to3%, which is in agreement with that derived from the UV spectra. The X-ray color of the detected sources indicates that they are probably moderately obscured. Stacking of the remainder shows a significant detection (6sigma) with an average luminosity of 3.4 x 10(41) ergs s(-1) per galaxy in the rest-frame 2-10 keV band. We have also studied a comparison sample of 95 z similar to 1 "Balmer break" galaxies. Eight of these are detected directly, with at least two clear AGNs based on their high X-ray luminosity and very hard X-ray spectra. The remainder are of relatively low luminosity (<10(42) ergs s(-1)), and the X-rays could arise from either AGNs or rapid star formation. The X-ray colors and evidence from other wave bands favor the latter interpretation. Excluding the clear AGNs, we deduce a mean X-ray luminosity of 6.6 x 10(40) ergs s(-1), a factor of &SIM;5 lower than the LBGs. The average ratio of the UV and X-ray luminosities of these star-forming galaxies L-UV/L-X, however, is approximately the same at z = 1 as it is at z = 3. This scaling implies that the X-ray emission follows the current star formation rate, as measured by the UV luminosity. We use our results to constrain the star formation rate at z &SIM; 3 from an X-ray perspective. Assuming the locally established correlation between X-ray and far-IR luminosity, the average inferred star formation rate in each LBG is found to be approximately 60 M. yr(-1), in excellent agreement with the extinction-corrected UV estimates. This provides an external check on the UV estimates of the star formation rates and on the use of X-ray luminosities to infer these rates in rapidly star-forming galaxies at high redshift. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. CALTECH, Palomar Observ, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. RP Nandra, K (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2BW, England. NR 98 TC 111 Z9 111 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 SEP 10 PY 2002 VL 576 IS 2 BP 625 EP 639 DI 10.1086/341888 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590EF UT WOS:000177804800002 ER PT J AU Steidel, CC Hunt, MP Shapley, AE Adelberger, KL Pettini, M Dickinson, M Giavalisco, M AF Steidel, CC Hunt, MP Shapley, AE Adelberger, KL Pettini, M Dickinson, M Giavalisco, M TI The population of faint optically selected active galactic nuclei at z similar to 3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : evolution; galaxies : nuclei; quasars : general ID REDSHIFT RADIO GALAXIES; QUASI-STELLAR OBJECTS; LYMAN-BREAK GALAXIES; LUMINOSITY FUNCTION; BLACK-HOLES; EVOLUTION; SPECTRA; CUTOFF; COLORS; LIMIT AB We discuss a sample of 29 active galactic nuclei (AGNs) (16 narrow-lined and 13 broad-lined) discovered in a spectroscopic survey of similar to1000 star-forming Lyman break galaxies ( LBGs) at z similar or equal to 3. Reaching apparent magnitudes of R-AB = 25.5, the sample includes broad-lined AGNs approximately 100 times less UV luminous than in most surveys to date covering similar redshifts and in the first statistical sample of UV/optically selected narrow-lined AGNs at high redshift. The fraction of objects in our survey with clear evidence for AGN activity is similar or equal to3%. A substantial fraction, perhaps even most, of these objects would not have been detected in even the deepest existing X-ray surveys. We argue that these AGNs are plausibly hosted by the equivalent of LBGs. The UV luminosities of the broad-lined AGNs in the sample are compatible with Eddington-limited accretion onto black holes that satisfy the locally determined M-BH versus M-bulge relation given estimates of the stellar masses of LBGs. The clustering properties of the AGNs are compatible with their being hosted by objects similar to LBGs. The implied lifetime of the active AGN phase in LBGs, if it occurs some time during the active star formation phase, is similar to10(7) yr. C1 CALTECH, Astron Opt, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Astron Inst, Cambridge CB3 0HA, England. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Steidel, CC (reprint author), CALTECH, Astron Opt, MS 105-24, Pasadena, CA 91125 USA. NR 48 TC 111 Z9 111 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 SEP 10 PY 2002 VL 576 IS 2 BP 653 EP 659 DI 10.1086/341789 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590EF UT WOS:000177804800004 ER PT J AU Sun, M Murray, SS AF Sun, M Murray, SS TI Chandra view of the dynamically young cluster of galaxies A1367. I. Small-scale structures SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (A1367); galaxies : individual (NGC 3860, NGC 3860B, NGC 6697); X-rays : galaxies ID X-RAY-EMISSION; STARBURST GALAXIES; SPIRAL GALAXIES; COMA CLUSTER; ABELL-1367; ROSAT; GAS; A-1367; RADIO AB The 40 ks Chandra ACIS-S observation of A1367 provides new insights into small-scale structures and point sources in this dynamically young cluster. Here we concentrate on small-scale extended structures. A ridgelike structure around the center ( the ridge) is significant in the Chandra image. The ridge, with a projected length of similar to8' (or 300 h(0.5)(-1) kpc), is elongated from northwest to southeast, as is the X-ray surface brightness distribution on much larger scales (similar to2 h(0.5)(-1) Mpc). The ridge is cooler than its western and southern surroundings, while the differences from its eastern and northern surroundings are small. We also searched for small-scale structures with sizes of about an arcminute. Nine extended features, with sizes from similar to0.'5 to 1.'5, were detected at significance levels above 4 sigma. Five of the nine features are located in the ridge and form local crests. The nine extended features can be divided into two types. Those associated with galaxies (NGC 3860B, NGC 3860, and UGC 6697) are significantly cooler than their surroundings (0.3-0.9 keV vs. 3-4.5 keV). The masses of their host galaxies are sufficient to bind the extended gas. These extended features are probably related to thermal halos or galactic superwinds of their host galaxies. The existence of these relatively cold halos implies that galaxy coronae can survive in a cluster environment (e.g., Vikhlinin and coworkers in 2001). Features of the second type are not apparently associated with galaxies. Their temperatures may not be significantly different from those of their surroundings. This class of extended features may be related to the ridge. We consider several possibilities for the ridge and the second type of extended features. The merging scenario is preferred. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 36 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 SEP 10 PY 2002 VL 576 IS 2 BP 708 EP 719 DI 10.1086/341756 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590EF UT WOS:000177804800009 ER PT J AU Li, LX Narayan, R Menou, K AF Li, LX Narayan, R Menou, K TI The giant X-ray flare of NGC 5905: Tidal disruption of a star, a brown dwarf, or a planet? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : nuclei ID MASSIVE BLACK-HOLE; ACTIVE GALACTIC NUCLEI; EMISSION-SPECTRUM; ACCRETION DISKS; GALAXIES; APPEARANCE; OUTBURST; NGC-5905; MASSES; RATES AB We model the 1990 giant X-ray are of the quiescent galaxy NGC 5905 as the tidal disruption of a star by a supermassive black hole. From the observed rapid decline of the luminosity, over a timescale of a few years, we argue that the are was powered by the fallback of debris rather than subsequent accretion via a thin disk. The fallback model allows constraints to be set on the black hole mass and the mass of debris. The latter must be very much less than a solar mass to explain the very low luminosity of the are. The observations can be explained either as the partial stripping of the outer layers of a low-mass main-sequence star or as the disruption of a brown dwarf or a giant planet. We find that the X-ray emission in the are must have originated within a small patch rather than over the entire torus of circularized material surrounding the black hole. We suggest that the patch corresponds to the "bright spot" where the stream of returning debris impacts the torus. Interestingly, although the peak luminosity of the are was highly sub-Eddington, the peak flux from the bright spot was close to the Eddington limit. We speculate on the implications of this result for observations of other are events. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. RP Li, LX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 45 TC 54 Z9 55 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2002 VL 576 IS 2 BP 753 EP 761 DI 10.1086/341890 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590EF UT WOS:000177804800013 ER PT J AU Janiuk, A Czerny, B Siemiginowska, A AF Janiuk, A Czerny, B Siemiginowska, A TI Radiation pressure instability driven variability in the accreting black holes SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; instabilities; stars : individual (GRS 1915+105); X-rays : bursts ID ACTIVE GALACTIC NUCLEI; X-RAY BINARIES; RXTE OBSERVATIONS; GRS 1915+105; SPECTRAL VARIABILITY; SUPERLUMINAL SOURCE; VERTICAL STRUCTURE; DISK ACCRETION; CYG X-1; GRS-1915+105 AB The time-dependent evolution of the accretion disk around the black hole is computed. The classical description of the alpha-viscosity is adopted so the evolution is driven by the instability operating in the innermost radiation pressure dominated part of the accretion disk. We assume that the optically thick disk always extends down to the marginally stable orbit, so it is never evacuated completely. We include the effect of the advection, coronal dissipation, and vertical outflow. We show that the presence of the corona and/or the outflow reduces the amplitude of the outburst. If only about half of the energy is dissipated in the disk ( with the other half dissipated in the corona and carried away by the outflow), the outburst amplitude and duration are consistent with observations of the microquasar GRS 1915+ 105. Viscous evolution explains in a natural way the lack of direct transitions from the state C to the state B in the color-color diagram of this source. Further reduction of the fraction of energy dissipated in the optically thick disk switches off the outbursts, which may explain why they are not seen in all high accretion rate sources being in the very high state. C1 Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Janiuk, A (reprint author), Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. RI Czerny, Bozena/A-2363-2015 OI Czerny, Bozena/0000-0001-5848-4333 NR 85 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 SEP 10 PY 2002 VL 576 IS 2 BP 908 EP 922 DI 10.1086/341804 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590EF UT WOS:000177804800027 ER PT J AU Puyravaud, JP AF Puyravaud, JP TI A modification of the prevalence index SO CURRENT SCIENCE LA English DT Article C1 Smithsonian Trop Res Inst, Tupper, Balboa, Panama. RP Puyravaud, JP (reprint author), Smithsonian Trop Res Inst, Tupper, Box 2072, Balboa, Panama. NR 1 TC 0 Z9 0 U1 0 U2 1 PU CURRENT SCIENCE ASSN PI BANGALORE PA C V RAMAN AVENUE, PO BOX 8005, BANGALORE 560 080, INDIA SN 0011-3891 J9 CURR SCI INDIA JI Curr. Sci. PD SEP 10 PY 2002 VL 83 IS 5 BP 565 EP 565 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 595CT UT WOS:000178089800018 ER PT J AU Soon, W Baliunas, S Idso, SB Kondratyev, KY Posmentier, ES AF Soon, W Baliunas, S Idso, SB Kondratyev, KY Posmentier, ES TI Modeling climatic effects of anthropogenic carbon dioxide emissions: unknowns and uncertainties. Reply to Risbey (2002) SO CLIMATE RESEARCH LA English DT Editorial Material C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Mt Wilson Observ, Mt Wilson, CA 91023 USA. US Water Conservat Lab, Phoenix, AZ 85040 USA. Russian Acad Sci, Res Ctr Ecol Safety, St Petersburg 197110, Russia. Long Isl Univ, Brooklyn, NY 11201 USA. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 1 Z9 1 U1 0 U2 4 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0936-577X J9 CLIMATE RES JI Clim. Res. PD SEP 6 PY 2002 VL 22 IS 2 BP 187 EP 188 DI 10.3354/cr022187 PG 2 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 608EW UT WOS:000178833200009 ER PT J AU Park, MG Cooney, SK Kim, JS Coats, DW AF Park, MG Cooney, SK Kim, JS Coats, DW TI Effects of parasitism on diel vertical migration, phototaxis/geotaxis, and swimming speed of the bloom-forming dinoflagellate Akashiwo sanguinea SO AQUATIC MICROBIAL ECOLOGY LA English DT Article DE parasitism; diel vertical migration; taxis; swimming speed; behavior; red tide; Akashiwo sanguinea ID GYMNODINIUM-SANGUINEUM; AMOEBOPHRYA SP; RED-TIDE; CHESAPEAKE BAY; REPRODUCTION; ENVIRONMENT; INFECTION; CERATII; NITRATE AB Eukaryotic parasites are believed to play important roles in bloom dynamics of red-tide dinoflagellates; however, little is known about their impact on host behavior. To address this issue, we examined the influence of the parasitic dinoflagellate Amoebophrya sp. on diel vertical migration (DVM), phototaxis/geotaxis, and swimming speed of the bloom-forming dinoflagellate Akashiwo sanguinea. Uninfected A. sanguinea exhibited strong DVM, yielding subsurface aggregations during the day and evenly dispersed populations at night. DVM of parasitized A. sanguinea was comparable to that of uninfected host for much of the infection cycle; however, subsurface accumulations of host cells were dramatically reduced or eliminated as parasites matured. The absence of DVM in the latter part of the infection cycle appeared to be associated with changes in phototaxic response and swimming speed of parasitized cells. While uninfected A. sanguinea exhibited strong positive phototaxis, hosts with late-stage infections exhibited strong negative phototaxis. By contrast, infected and uninfected A. sanguinea did not differ in geotaxis or sinking. Swimming speed of infected A. sanguinea decreased with parasite age, differing significantly from that of uninfected hosts 24 h after initiation of infections. A. sanguinea with late-stage infections exhibited a 37.3 % lower swimming speed than uninfected hosts. Results indicate that parasitism by Amoebophrya sp. disrupts 'internal' factors that control DVM in dinoflagellates. Data also suggest that modification of host behavior by parasitism may contribute to vertical variations in phytoplankton species-composition and -abundance, particularly during epidemics when late-stage infections are prevalent. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Kunsan Natl Univ, Red Tide Res Ctr, Coll Ocean Sci & Technol, Dept Oceanog, Kunsan 573701, South Korea. RP Park, MG (reprint author), Kunsan Natl Univ, Red Tide Res Ctr, Coll Ocean Sci & Technol, Dept Oceanog, Kunsan 573701, South Korea. NR 40 TC 28 Z9 32 U1 1 U2 11 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0948-3055 J9 AQUAT MICROB ECOL JI Aquat. Microb. Ecol. PD SEP 3 PY 2002 VL 29 IS 1 BP 11 EP 18 DI 10.3354/ame029011 PG 8 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 595JY UT WOS:000178106600002 ER PT J AU Doris, DT AF Doris, DT TI The good, the bad, and the beautiful - Discourse about values in Yoruba Culture SO AFRICAN ARTS LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Doris, DT (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD FAL PY 2002 VL 35 IS 3 BP 7 EP + PG 0 WC Art SC Art GA 645CT UT WOS:000180959200002 ER PT J AU Harney, E AF Harney, E TI The Ecole de Dakar: Pan-Africanism in paint and textile (First generation of Senegalese painters who made their public debut at the 1966 exhibition Tendances et Confrontations) SO AFRICAN ARTS LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Harney, E (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 53 TC 4 Z9 4 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD FAL PY 2002 VL 35 IS 3 BP 12 EP + PG 0 WC Art SC Art GA 645CT UT WOS:000180959200004 ER PT J AU Norconk, MA Oftedal, OT Power, ML Jakubasz, M Savage, A AF Norconk, MA Oftedal, OT Power, ML Jakubasz, M Savage, A TI Digesta passage and fiber digestibility in captive white-faced sakis (Pithecia pithecia) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE transit time (TT); mean retention time (MRT); seed predator; neutral detergent fiber; acid detergent fiber; chromic oxide (Cr2O3); particulate marker; Chiropotes; Cacajao ID FEEDING ECOLOGY; SEED DISPERSAL; DIETARY; STRATEGIES; PRIMATES; CHIMPANZEES; CHIROPOTES; MONKEYS; FOREST; FRUIT AB Wild white-faced sakis (Pithecia pithecia) ingest primarily seeds that provide a diet that is lipid-rich and moderately high in dietary fiber. Although little anatomical information is available on sakis, evidence from other vertebrate seed predators suggests that such a diet is, correlated with adaptations in gut morphology or physiology. Milton [1984] reported a 20 hr transit time (TT = transit time or time of first appearance in feces) of a particulate marker for a single monk saki (Pithecia monachus). This suggests that TT for Pithecia sakis may be four to five times longer than what has been reported for soft-fruit-eating platyrrhines, such as Ateles and Cebus. During a captive study, we calculated an average TT of 14.7 +/- 0.4 hr (n = 5 trials started in the evening) for a chromic oxide (Cr2O3) marker that follows liquid digesta and TTs of 14.5 hr (trial started the previous evening) and 23.0 hr (trial started the previous morning) for two trials using particulate markers. Mean retention time (MRT) for the liquid marker ranged from 15.3 hr to 37.7 hr in four trials that lasted longer than 90 hr. Marker recovery was incomplete for the particulate markers in these trials, and thus MRT could only be determined for the liquid phase marker. Three 5-day trials on a low-fiber, blended diet revealed high fiber fraction digestibilities (neutral detergent fiber (NDF) = 77.4% and acid detergent fiber (ADF) = 74.4%). Data collected for this study and nutritional data from wild sakis suggest that pitheciin seed predators may have a potential for fiber digestibility that is intermediate between ripe-pulp frugivores and folivores. (C) 2002 Wiley-Liss, Inc. C1 Kent State Univ, Dept Anthropol, Kent, OH 44242 USA. Smithsonian Inst, Dept Conservat Biol, Washington, DC USA. Disneys Anim Kingdom, Dept Educ & Sci, Lake Buena Vista, FL USA. RP Norconk, MA (reprint author), Kent State Univ, Dept Anthropol, 228 Lowry Hall, Kent, OH 44242 USA. OI Power, Michael/0000-0002-6120-3528 NR 43 TC 11 Z9 12 U1 1 U2 12 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD SEP PY 2002 VL 58 IS 1 BP 23 EP 34 DI 10.1002/ajp.10048 PG 12 WC Zoology SC Zoology GA 601NF UT WOS:000178452100002 PM 12325116 ER PT J AU Klamer, M Roberts, MS Levine, LH Drake, BG Garland, JL AF Klamer, M Roberts, MS Levine, LH Drake, BG Garland, JL TI Influence of elevated CO2 on the fungal community in a coastal scrub oak forest soil investigated with terminal-restriction fragment length polymorphism analysis SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID GRADIENT GEL-ELECTROPHORESIS; RIBOSOMAL-RNA GENES; T-RFLP ANALYSIS; ATMOSPHERIC CO2; MICROBIAL COMMUNITY; CARBON-DIOXIDE; ECTOMYCORRHIZAL FUNGI; ENVIRONMENTAL-SAMPLES; BACTERIAL COMMUNITIES; POPULUS-GRANDIDENTATA AB Sixteen open-top chambers (diameter, 3.66 m) were established in a scrub oak habitat in central Florida where vegetation was removed in a planned burn prior to chamber installation. Eight control chambers have been continuously exposed to ambient air and eight have been continuously exposed to elevated CO2 at twice-ambient concentration (similar to700 ppm) for 5 years. Soil cores were collected from each chamber to examine the influence of elevated atmospheric CO, on the fungal community in different soil fractions. Each soil sample was physically fractionated into bulk soil, rhizosphere soil, and roots for separate analyses. Changes in relative fungal biomass were estimated by the ergosterol technique. In the bulk soil and root fractions, a significantly increased level of ergosterol was detected in the elevated CO, treatments relative to ambient controls. Fungal community composition was determined by terminal-restriction fragment length polymorphism (T-RFLP) analysis of the internal transcribed spacer (ITS) region. The specificities of different ITS primer sets were evaluated against plant and fungal species isolated from the experimental site. Changes in community composition were assessed by principal component analyses of T-RFLP profiles resolved by capillary electrophoresis. Fungal species richness, defined by the total number of terminal restriction fragments, was not significantly affected by either CO2 treatment or soil fraction. C1 Univ Cent Florida, Dept Biol, Kennedy Space Ctr, FL 32899 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Dynamac Corp, Kennedy Space Ctr, FL 32899 USA. RP Klamer, M (reprint author), Lund Univ, Dept Ecol, Ecol Bldg,Getingegatan 60, S-22362 Lund, Sweden. NR 68 TC 98 Z9 106 U1 1 U2 25 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD SEP PY 2002 VL 68 IS 9 BP 4370 EP 4376 DI 10.1128/AEM.68.9.4370-4376.2002 PG 7 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 588TX UT WOS:000177718000028 PM 12200289 ER PT J AU Wilson, G Cowie, LL Barger, AJ Burke, DJ AF Wilson, G Cowie, LL Barger, AJ Burke, DJ TI Star formation history since z=1.5 as inferred from rest-frame ultraviolet luminosity density evolution SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : distances and redshifts galaxies : evolution; galaxies : formation; galaxies : luminosity function, mass function ID GALAXY REDSHIFT SURVEY; HUBBLE-DEEP-FIELD; FAINT GALAXIES; COUNTS; ESTIMATORS; RESOLUTION; COLORS; SAMPLE; BAND AB We investigate the evolution of the universal rest-frame ultraviolet luminosity density from z = 1.5 to the present. We analyze an extensive sample of multicolor data (U'(AB), B-AB, V-AB = 24.5) plus spectroscopic redshifts from the Hawaii Survey Fields and the Hubble Deep Field. Our multicolor data allow us to select our sample in the rest- frame ultraviolet (2500 Angstrom) over the entire redshift range to z = 1.5. We conclude that the evolution in the luminosity density is a function of the form (1 + z)(1.7 +/- 1.0) for a at lambda (Omega(m0) = 0.3, Omega(lambda0) = 0.7) cosmology and (1 + z)(2.4 +/- 1.0) for an Einstein de Sitter cosmology. C1 Brown Univ, Dept Phys, Providence, RI 02912 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilson, G (reprint author), Brown Univ, Dept Phys, 182 Hope St, Providence, RI 02912 USA. NR 34 TC 83 Z9 83 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 SEP PY 2002 VL 124 IS 3 BP 1258 EP 1265 DI 10.1086/341818 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 586ND UT WOS:000177589300002 ER PT J AU Rines, K Geller, MJ Diaferio, A Mahdavi, A Mohr, JJ Wegner, G AF Rines, K Geller, MJ Diaferio, A Mahdavi, A Mohr, JJ Wegner, G TI Mass profile of the infall region of the Abell 2199 supercluster SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : individual (Abell 2197, Abell 2199); galaxies : kinematics and dynamics ID PECULIAR VELOCITY-FIELD; ALL-SKY SURVEY; X-RAY SOURCES; GALAXY CLUSTERS; FUNDAMENTAL PLANE; RICH CLUSTERS; HOT PLASMA; ROSAT; TEMPERATURE; DENSITY AB Using a redshift survey of 1323 galaxies ( 1092 new or remeasured) in a region of 95 deg(2) centered on the nearby galaxy cluster Abell 2199, we analyze the supercluster containing A2199, A2197, and an X-ray group. The caustic technique accurately reproduces the true mass profiles of simulated simple superclusters (i.e., superclusters for which the virial mass of one cluster is 2 10 times the virial mass of all other clusters in the supercluster). We calculate the masses of the two main components of A2197 ( A2197W and A2197E) by using archival X-ray observations and demonstrate that the A2199 supercluster is simple ( the mass of A2199 is 5 and 12 times larger than A2197W and A2197E, respectively) and thus that the caustic technique should yield an accurate mass pro le. The masses of A2199, A2197W, and A2197E within r(500) (the radius within which the enclosed density is 500 times the critical density) are 22.0, 3.8, and 1.7 times 10(13) h(-1) M-., respectively. The mass profile is uncertain by similar to30% within 3 h(-1) Mpc and by a factor of 2 within 8 h(-1) Mpc and is one of only a few for a supercluster on such large scale. Independent X-ray mass estimates agree with our results at all radii where they overlap. The mass pro le strongly disagrees with an isothermal sphere pro le but agrees with profiles suggested by simulations. We discuss the interplay of the supercluster dynamics and the dynamics of the bound subclusters. The agreement between the infall mass pro le and other techniques shows that the caustic technique is surprisingly robust for simple superclusters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smithsonian Astrophys Observ, Solar & Stellar Phys Div, Cambridge, MA 02138 USA. Univ Turin, Dipartimento Fis Gen, Turin, Italy. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Rines, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 75 TC 47 Z9 50 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2002 VL 124 IS 3 BP 1266 EP 1282 DI 10.1086/342344 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 586ND UT WOS:000177589300003 ER PT J AU Contreras, ME Sicilia-Aguilar, A Muzerolle, J Calvet, N Berlind, P Hartmann, L AF Contreras, ME Sicilia-Aguilar, A Muzerolle, J Calvet, N Berlind, P Hartmann, L TI A study of intermediate-mass stars in Trumpler 37 SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; color-magnitude diagrams; stars : early-type; stars : emission-line, Be ID ALPHA EMISSION STARS; CIRCUMSTELLAR DISKS; PROTOSTELLAR DISKS; CLUSTER TRUMPLER-37; DUST PROPERTIES; AE/BE STARS; AE STARS; PHOTOEVAPORATION; SYSTEMS; RESOLUTION AB We present results from optical spectra for intermediate-mass stars in the young cluster Trumpler 37. The spectroscopy presented helps to re ne the membership, reddening ( A(V) similar to 1.5 +/- 0.5), and distance modulus [ (m-M) = 9. 7 +/- 0.2] to this cluster. Only three new emission-line stars were found in our sample, resulting in a total of four stars in the cluster with emission lines and spectral type earlier than G. One of these emission-line stars, LkHalpha 349, is probably not a member of the central cluster, since it lies within a dark globule on the periphery of the H II region IC 1396. Thus, at an age of about 3 Myr, as estimated from the expansion age of molecular material around the cluster, emission-line phenomena possibly driven by disk accretion are extremely rare through spectral types F (masses not greater than or equal to 1.5 M-circle dot). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Contreras, ME (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 45 TC 42 Z9 42 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2002 VL 124 IS 3 BP 1585 EP 1592 DI 10.1086/341825 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 586ND UT WOS:000177589300022 ER PT J AU Kassis, M Deutsch, LK Campbell, MF Hora, JL Fazio, GG Hoffmann, WF AF Kassis, M Deutsch, LK Campbell, MF Hora, JL Fazio, GG Hoffmann, WF TI Mid-infrared observations of M17 SO ASTRONOMICAL JOURNAL LA English DT Article DE HII regions; infrared radiation; ISM : individual (M17); stars : formation ID H-II REGIONS; INTERSTELLAR DUST CLOUDS; 21 MICRON EMISSION; HIGH-RESOLUTION; PHOTODISSOCIATION REGIONS; RADIATION TRANSPORT; CLUMPY STRUCTURE; STELLAR OBJECTS; MOLECULAR CLOUD; ARRAY CAMERA AB Mosaics of the M17 southwest photodissociation region (PDR) at the mid-infrared wavelengths 9.8, 10.53, 11.7, and 20.6 mum are presented. Maps of hydrocarbon and ionized gas emission were derived by subtracting the continuum at 9.8 mum from the 10.5 and 11.7 mum maps, respectively. Comparisons of the emission from hydrocarbons and ionized gas to the 9.8 mum/20.6 mum color temperature and 9.8 mum opacity maps show that regions of hotter 9.8 mum/20.6 mum color temperatures have increased emission from ionized gas, while the hydrocarbons are found in cooler regions with high 9.8 mum opacities. Emission at 20.6 mum is spatially correlated with 11.3 mum hydrocarbon emission. Two bright point sources found in the southwest PDR are high-mass young stellar objects caught at distinctly different early evolutionary phases. M17-UC1 appears to be older than IRS 5 because it has less maser emission and has an observable H II region in radio continuum. Both sources are modeled with a radiative transfer code, which takes advantage of both the spatial and spectral information available. Models that best match the profiles and spectral energy distribution of the ultra-compact H II region, M17-UC1, have central stars with a luminosity and temperature equal to that of a zero-age main-sequence (ZAMS) B0 star, an outer radius less than 0.032 pc, an inner radius about the same size as the radio observed H II region, and a total shell mass of 0.6-3.4 M. The best-fit models underestimate the total observed flux found at near-infrared wavelengths, which suggests that a small, hot disk may be present in M17-UC1. A second source, identified with the near-infrared source IRS 5, has comparable mid-infrared emission to M17-UC1. The best-fitting model to IRS 5 has a central star with a luminosity and temperature equal to that of a ZAMS B0 star, an outer radius on the order of 1 pc, a small inner radius ( 0.001 pc), and a total shell mass of 70 M.. C1 Boston Univ, Dept Astron, Boston, MA 02215 USA. Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Kassis, M (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. OI Hora, Joseph/0000-0002-5599-4650 NR 60 TC 9 Z9 9 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2002 VL 124 IS 3 BP 1636 EP 1650 DI 10.1086/341819 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 586ND UT WOS:000177589300026 ER PT J AU Torres, G Boden, AF Latham, DW Pan, M Stefanik, RP AF Torres, G Boden, AF Latham, DW Pan, M Stefanik, RP TI Testing models of stellar evolution for metal-poor stars: An interferometric-spectroscopic orbit for the binary HD 195987 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; stars : abundances; stars : fundamental parameters; stars : individual (HD 195987) ID PROPER-MOTION STARS; PALOMAR TESTBED INTERFEROMETER; LOW-MASS STARS; ALPHA-ELEMENT ABUNDANCES; LOWER MAIN-SEQUENCE; VISUAL ORBIT; GLOBULAR-CLUSTERS; RADIAL-VELOCITIES; GALACTIC DISK; SOLAR NEIGHBORHOOD AB We report spectroscopic and interferometric observations of the moderately metal-poor double-lined binary system HD195987, with an orbital period of 57.3 days. By combining our radial-velocity and visibility measurements, we determine the orbital elements and derive absolute masses for the components of M(A) = 0.844 +/- 0.018 M. and M(B) = 0.6650 +/- 0.0079 M., with relative errors of 2% and 1%, respectively. We also determine the orbital parallax, pi(orb) = 46.08 +/- 0.27 mas, corresponding to a distance of 21.70 +/- 0.13 pc. The parallax and the measured brightness difference between the stars in V, H, and K yield the component absolute magnitudes in those bands. We also estimate the effective temperatures of the stars as T(eff)(A) = 5200 100 K and T(eff)(B) = 4200 +/- 200 K. Together with detailed chemical abundance analyses from the literature giving [Fe/H] approximate to -0.5 (corrected for binarity) and [alpha/Fe] = +0.36, we use these physical properties to test current models of stellar evolution for metal-poor stars. Among the four that we considered, we find that no single model fits all observed properties at the measured composition, although we identify the assumptions in each one that account for the discrepancy, and we conclude that a model with the proper combination of assumptions should be able to reproduce all the radiative properties. The indications from the isochrone fits and the pattern of enhancement of the metals in HD 195987 are consistent with this being a thick disk object, with an age of 10-12 Gyr. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Interferometry Sci Ctr, Pasadena, CA 91125 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu NR 88 TC 43 Z9 45 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2002 VL 124 IS 3 BP 1716 EP 1737 DI 10.1086/342018 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 586ND UT WOS:000177589300031 ER PT J AU Li, LX AF Li, LX TI Observational signatures of the magnetic connection between a black hole and a disk SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE black hole physics; accretion disks; magnetic fields; galaxies : active; galaxies : Seyfert ID EXTRACTING ENERGY; ACCRETION DISK AB We use a simple model to demonstrate the observational signatures of the magnetic connection between a black hole and a disk: (1) with the existence of the magnetic connection, more energy is dissipated in and radiated away from regions close to the center of the disk; (2) the magnetic connection can produce a very steep emissivity compared to the standard disk accretion; (3) the observational spectral signature of the magnetic connection can be robust. These signatures can be identified by the observations of Chandra and XMM-Newton. In fact, the steep emissivity index for the Seyfert 1 galaxies MCG-6-30-15 and Mrk-766 inferred from the recent XMM-Newton observations is very difficult to be explained with a standard accretion disk but can be easily explained with the magnetic connection between a black hole and a disk. 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 18 TC 48 Z9 50 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 SEP PY 2002 VL 392 IS 2 BP 469 EP 472 DI 10.1051/00046361:20020958 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 593PJ UT WOS:000178001100007 ER PT J AU Schmidt, RW Kundic, T Pen, UL Turner, EL Wambsganss, J Bergeron, LE Colley, WN Corson, C Hastings, NC Hoyes, T Long, DC Loomis, KA Malhotra, S Rhoads, JE Stanek, KZ AF Schmidt, RW Kundic, T Pen, UL Turner, EL Wambsganss, J Bergeron, LE Colley, WN Corson, C Hastings, NC Hoyes, T Long, DC Loomis, KA Malhotra, S Rhoads, JE Stanek, KZ TI Optical monitoring of the gravitationally lensed quasar Q2237+0305 from APO between June 1995 and January 1998 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing; dark matter; quasars : individual : Q2237+0305; cosmology : observations ID LENSING EXPERIMENT; EINSTEIN-CROSS; SYSTEM; MODELS AB We present a data set of images of the gravitationally lensed quasar Q2237+0305, that was obtained at the Apache Point Observatory (APO) between June 1995 and January 1998. Although the images were taken under variable, often poor seeing conditions and with coarse pixel sampling, photometry is possible for the two brighter quasar images A and B with the help of exact quasar image positions from HST observations. We obtain a light curve with 73 data points for each of the images A and B. There is evidence for a long ( greater than or similar to 100 day) brightness peak in image A in 1996 with an amplitude of about 0.4 to 0.5 mag (relative to 1995), which indicates that microlensing has been taking place in the lensing galaxy. Image B does not vary much over the course of the observation period. The long, smooth variation of the light curve is similar to the results from the OGLE monitoring of the system (Wozniak et al. 2000a). C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Potsdam, Inst Phys, D-14469 Potsdam, Germany. Renaissance Technol, Moscow 117333, Russia. Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Princeton Univ Observ, Princeton, NJ 08544 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. MIT, Lincoln Lab, Lexington, MA 02420 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Apache Point Observ, Sunspot, NM 88349 USA. Mesa Community Coll, Mesa, AZ 85202 USA. Johns Hopkins Univ, Baltimore, MD 21210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schmidt, RW (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RI Turner, Edwin/A-4295-2011 NR 23 TC 15 Z9 15 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 SEP PY 2002 VL 392 IS 3 BP 773 EP 779 DI 10.1051/0004-6361:20020957 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594MM UT WOS:000178054400001 ER PT J AU Hynes, RI Clark, JS Barsukova, EA Callanan, PJ Charles, PA Cameron, AC Fabrika, SN Garcia, MR Haswell, CA Horne, K Miroshnichenko, A Negueruela, I Reig, P Welsh, WF Witherick, DK AF Hynes, RI Clark, JS Barsukova, EA Callanan, PJ Charles, PA Cameron, AC Fabrika, SN Garcia, MR Haswell, CA Horne, K Miroshnichenko, A Negueruela, I Reig, P Welsh, WF Witherick, DK TI Spectroscopic observations of the candidate sgB[e]/X-ray binary CI Camelopardalis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : individual : CI Cam; stars : emission line, B[e]; stars : radio emission stars : CI Cam; binaries : close ID DIFFUSE INTERSTELLAR BANDS; EMISSION-LINE STARS; XTE J0421+560; ACCRETION-DISK; SS 433; OUTBURST; CAM; PECULIAR; BRIGHT; EXTINCTION AB We present a compilation of spectroscopic observations of the sgB[e] star CI Cam, the optical counterpart of XTE J0421+560. This includes data from before, during, and after its 1998 outburst, with quantitative results spanning 37 years. The object shows a rich emission line spectrum originating from circumstellar material, rendering it difficult to determine the nature of either star involved or the cause of the outburst. We collate all available pre-outburst data to determine the state of the system before this occurred and provide a baseline for comparison with outburst and post-outburst data. During the outburst all lines become stronger, and hydrogen and helium lines become significantly broader and asymmetric. After the outburst, spectral changes persist for at least three years, with Fe II and [N II] lines still a factor of similar to 2 above the pre-outburst level and He I, He II, and N II lines suppressed by a factor of 2-10. We find that the spectral properties of CI Cam are similar to other sgB[e] stars and therefore suggest that the geometry of the circumstellar material is similar to that proposed for the other objects: a two component outflow, with a fast, hot, rarefied polar wind indistinguishable from that of a normal supergiant and a dense, cooler equatorial outflow with a much lower velocity. Based on a comparison of the properties of CI Cam with the other sgB[e] stars we suggest that CI Cam is among the hotter members of the class and is viewed nearly pole-on. The nature of the compact object and the mechanism for the outburst remain uncertain, although it is likely that the compact object is a black hole or neutron star, and that the outburst was precipitated by its passage through the equatorial material. We suggest that this prompted a burst of supercritical accretion resulting in ejection of much of the material, which was later seen as an expanding radio remnant. The enhanced outburst emission most likely originated either directly from this supercritical accretion, or from the interaction of the expanding remnant with the equatorial material, or from a combination of both mechanisms. C1 Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. UCL, Dept Phys & Astron, London WC1E 6BT, England. Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia. Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. Pulkovo Observ, St Petersburg 196140, Russia. Observ Strasbourg, F-67000 Strasbourg, France. Univ Crete, Dept Phys, Iraklion 71003, Greece. Fdn Res & Technol Hellas, Iraklion 71110, Greece. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Univ Texas, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM rih@astro.as.utexas.edu RI Reig, Pablo/A-1198-2014; Witherick, Dugan/C-9403-2014; Negueruela, Ignacio/L-5483-2014 OI Reig, Pablo/0000-0002-6446-3050; Witherick, Dugan/0000-0002-9175-0151; Negueruela, Ignacio/0000-0003-1952-3680 NR 60 TC 33 Z9 36 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2002 VL 392 IS 3 BP 991 EP 1013 DI 10.1051/0004-6361:20020979 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 594MM UT WOS:000178054400022 ER PT J AU van den Bosch, FC Abel, T Croft, RAC Hernquist, L White, SDM AF van den Bosch, FC Abel, T Croft, RAC Hernquist, L White, SDM TI The angular momentum of gas in protogalaxies. I. Implications for the formation of disk galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies : formation; galaxies : halos; galaxies : structure; methods : n-body simulations ID HIERARCHICAL FORMATION SCENARIO; WEAK-LENSING MEASUREMENTS; COLD DARK-MATTER; STAR-FORMATION; TIDAL TORQUES; EVOLUTION; HALOS; DYNAMICS; FEEDBACK; ORIGIN AB We use numerical simulations of structure formation in a cold dark matter cosmology to compare the angular momentum distributions of dark matter and nonradiative gas in a large sample of halos. We show that the two components have identical spin parameter distributions and that their angular momentum distributions within individual halos are very similar, all in excellent agreement with standard assumptions. Despite these similarities, however, we find that the angular momentum vectors of the gas and dark matter are poorly aligned, with a median misalignment angle of similar to30degrees, which might have important implications for spin correlation statistics used in weak lensing studies. We present distributions for the component of the angular momentum that is aligned with the total angular momentum of each halo and find that for between 5% and 50% of the mass, this component is negative. This disagrees with the generally adopted universal angular momentum distribution, for which the mass fraction with negative specific angular momentum is zero. We discuss the implications of our results for the formation of disk galaxies. Since galactic disks generally do not contain counterrotating stars or gas, disk formation cannot occur under detailed conservation of specific angular momentum. We suggest that the material with negative specific angular momentum combines with positive angular momentum material to build a bulge component, and we show that in such a scenario the remaining material can form a disk with a density distribution that is very close to exponential. C1 Max Planck Inst Astron, D-85741 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van den Bosch, FC (reprint author), Max Planck Inst Astron, Karl Schwarzschild Str 1,Postfach 1317, D-85741 Garching, Germany. RI Croft, Rupert/N-8707-2014 OI Croft, Rupert/0000-0003-0697-2583 NR 62 TC 160 Z9 161 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 SEP 1 PY 2002 VL 576 IS 1 BP 21 EP 35 DI 10.1086/341619 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 586NB UT WOS:000177589100002 ER PT J AU Lin, J van Ballegooijen, AA AF Lin, J van Ballegooijen, AA TI Catastrophic and noncatastrophic mechanisms for coronal mass ejections SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : coronal mass ejections (CMEs) Sun : flares; Sun : magnetic fields; Sun : prominences ID FLUX-ROPE MODELS; ERUPTIVE FLARES; MAGNETIC-FIELD; LASCO; RECONNECTION; ACCELERATION; PROMINENCE; EVOLUTION AB It has been suggested that coronal mass ejections (CMEs) are triggered by the loss of equilibrium of a coronal magnetic field configuration containing a twisted flux rope. We propose that there are two types of CMEs: fast CMEs that are triggered by a catastrophic loss of equilibrium and slow CMEs that do not involve a true catastrophe, but nevertheless show rapid evolution of the system. As an extension of the 1991 work by Forbes and Isenberg, we investigated the evolution of a magnetic configuration taking into account deviations from ideal MHD. We find that the non ideal MHD evolution makes it easier for the catastrophic loss of equilibrium to occur, and the catastrophic behavior of the system is no longer constrained by the radius of the flux rope. For ideal-MHD evolution, we find that noncatastrophic solutions can account for slow CMEs. We also discuss the conditions under which the ideal-MHD approximation holds. 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. RI LIN, JUN/B-9890-2017 NR 27 TC 19 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 SEP 1 PY 2002 VL 576 IS 1 BP 485 EP 492 DI 10.1086/341737 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 586NB UT WOS:000177589100044 ER PT J AU Hagedorn, M Lance, SL Fonseca, DM Kleinhans, FW Artimov, D Fleischer, R Hoque, ATMS Hamilton, MB Pukazhenthi, BS AF Hagedorn, M Lance, SL Fonseca, DM Kleinhans, FW Artimov, D Fleischer, R Hoque, ATMS Hamilton, MB Pukazhenthi, BS TI Altering fish embryos with aquaporin-3: An essential step toward successful cryopreservation SO BIOLOGY OF REPRODUCTION LA English DT Article DE embryo ID BRACHYDANIO-RERIO EMBRYOS; WATER CHANNEL PROTEINS; PERMEABILITY BARRIER; OSMOMETRIC BEHAVIOR; ZEBRAFISH EMBRYOS; XENOPUS OOCYTES; EXPRESSION; GLYCEROL; FAMILY; CELLS AB Fish populations are globally threatened by over-harvesting and habitat degradation. The ability to bank fish embryos by cryopreservation could be crucial for preserving species diversity, for aquaculture (allowing circannual fish farming), and for managing fish models used in human biomedical research. However, no nonmammalian embryo has ever been successfully cryopreserved. For fish, low membrane permeability prevents cryoprotectants from entering the yolk to prevent cryodamage. Here, we present evidence of a membrane mechanism hindering cryopreservation of fish and propose a novel solution to this obstacle. Zebrafish (Danio rerio) embryos have rectifying membranes that allow water to leave but not to reenter readily. This feature may be an evolutionary trait that allows freshwater embryos to grow in hypo-osmotic environments without osmoregulatory organs. However, this trait may also prevent successful fish embryo cryopreservation because both water and cryoprotectants must move into and out of cells. As a solution, we injected zebrafish embryos with mRNA for the aquaporin-3 water channel protein and demonstrated increased membrane permeability to water and to a cryoprotectant. Modeling indicates that sufficient cryoprotectant enters aquaporin-3-expressing zebrafish embryos to allow cryopreservation. C1 Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. Smithsonian Inst, Conservat & Res Ctr, Washington, DC 20008 USA. Walter Reed Army Inst Res, Dept Entomol, Silver Spring, MD 20910 USA. Indiana Univ Purdue Univ, Dept Phys, Indianapolis, IN 46202 USA. Johns Hopkins Univ, Sch Med, Dept Radiol, Baltimore, MD 21205 USA. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. Smithsonian Inst, Natl Zool Pk, Mol Genet Lab, Washington, DC 20008 USA. US FDA, Ctr Biol Evaluat & Res, Lab Plasma Derivat, Div Hematol, Bethesda, MD 20892 USA. Georgetown Univ, Dept Biol, Washington, DC 20057 USA. RP Hagedorn, M (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM hagedornm@nzp.si.edu RI Lance, Stacey/K-9203-2013; OI Lance, Stacey/0000-0003-2686-1733; Fonseca, Dina/0000-0003-4726-7100 FU NCRR NIH HHS [K01 RR00135, R01 RR08769] NR 38 TC 54 Z9 59 U1 2 U2 10 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD SEP PY 2002 VL 67 IS 3 BP 961 EP 966 DI 10.1095/biolreprod.101.002915 PG 6 WC Reproductive Biology SC Reproductive Biology GA 587WZ UT WOS:000177668200036 PM 12193408 ER PT J AU Lucky, A Erwin, TL Witman, JD AF Lucky, A Erwin, TL Witman, JD TI Temporal and spatial diversity and distribution of arboreal Carabidae (Coleoptera) in a western Amazonian rain forest SO BIOTROPICA LA English DT Article DE Amazon; canopy; Carabidae; distribution; diversity; Ecuador; lowland tropical rain forest; species richness ID PAPUA-NEW-GUINEA; SPECIES-DIVERSITY; COMMUNITIES; RICHNESS; TREE; BIODIVERSITY; HERBIVORES; DIMENSIONS; ABUNDANCE; INSECTS AB Diversity of arboreal carabid beetles was sampled by fumigation in 100 3 x 3 m stations within a 100 x 1000 m terra firme forest plot in Ecuadorian Amazonia. Nine sampling dates from January 1994 to October 1996 yielded 2329 individuals belonging to 318 species of which more than 50 percent were undescribed species. A high percentage of the species sampled were rare; the proportion that occurred once per sampling date (singletons) ranged from 50.0 to 62.5 percent. Estimates of species richness were from 82 to 282 species of arboreal carabids in the study plot on a given sampling date. Most richness values were greater than 173 species. Species accumulation curves attained asymptotes for all but one sampling date, indicating that an adequate level of sampling effort was used to characterize the diversity of carabid fauna. Total accumulation curves based on pooled data failed to reach asymptotes. There was a high turnover in species composition between sampling dates; less than 50 percent of the species between the majority of sampling dates were shared, suggesting that the total species pool may be extremely large. Although species composition changed seasonally, species richness varied little. Spatial autocorrelation analysis revealed that the structure of this species assemblage was significantly patterned at distances below 280 m. Taken together, the large percentage of undescribed species, the failure of the overall species accumulation curves to level off, and the high turnover in species composition indicate that the species diversity of carabid beetles is far higher than previously thought. C1 Brown Univ, Dept Ecol & Evolut Biol, Providence, RI 02912 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Lucky, A (reprint author), Brown Univ, Dept Ecol & Evolut Biol, Box G-W, Providence, RI 02912 USA. NR 35 TC 33 Z9 34 U1 1 U2 14 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD SEP PY 2002 VL 34 IS 3 BP 376 EP 386 DI 10.1111/j.1744-7429.2002.tb00551.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 609JB UT WOS:000178898900005 ER PT J AU Gilbert, GS Sousa, WP AF Gilbert, GS Sousa, WP TI Host specialization among wood-decay polypore fungi in a Caribbean mangrove forest SO BIOTROPICA LA English DT Article DE Avicennia; Datronia; fungal ecology; host specialization; Laguncularia; mangrove forest; Panama; Phellinus; Rhizophora; Trichaptum ID INHABITING FUNGI; TROPICAL FOREST; RAIN-FOREST; DIVERSITY; SPECIFICITY; ENDOPHYTES; PATTERNS; BIODIVERSITY; MICROFUNGI; COMMUNITY AB Host specialization in highly diverse tropical forests may be limited by the low local abundance of suitable hosts. To address whether or not fungi in a low-diversity tropical forest were released from this restriction, fruiting bodies of polypore basidiomycete fungi were collected from three species of mangroves (Avicennia germinans, Laguncularia racemosa, and Rhizophora mangle) in a Caribbean mangrove forest in Panama. Unlike other tropical forests, the polypore assemblage in this mangrove forest was strongly dominated by a few host-specialized species. Three fungal species, each with strong preference for a different mangrove host species, comprised 88 percent of all fungi collected. C1 Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. RP Gilbert, GS (reprint author), Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. EM ggilbert@cats.ucsc.edu RI Gilbert, Gregory/C-2595-2008 NR 47 TC 45 Z9 49 U1 3 U2 18 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD SEP PY 2002 VL 34 IS 3 BP 396 EP 404 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 609JB UT WOS:000178898900007 ER PT J AU Vecchione, M Roper, CFE Widder, EA Frank, TM AF Vecchione, M Roper, CFE Widder, EA Frank, TM TI In situ observations on three species of large-finned deep-sea squids SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Cephalopod International Advisory Council Symposium and Workshops (CIAC 2000) CY JUL 03-07, 2000 CL UNIV ABERDEEN, ABERDEEN, SCOTLAND HO UNIV ABERDEEN ID CEPHALOPODA; VERRILL AB The manned submersible JOHNSON SEA-LINK 11 Was used for a series of dives on the continental slope of the eastern Gulf of Mexico in September 1995. The deep-sea squids Mastigoteuthis hjorti Chun, 1913 and Octopoteuthis megaptera (Verrill, 1885) were repeatedly observed at depths of 600-850 m. Both species were videotaped alive, in situ, for the first time during these dives. These species share the characteristic of very large fins, almost as long as the mantle length, but their swimming behavior observed in the vicinity of the submersible differed greatly. Throughout most of the videotaped sequences of O. megaptera, it swam with its body oriented obliquely with the head upward, arms flexed laterally and dorsally. The fins flapped in the arc between overlapping ventrally and extending laterally, never traversing dorsally above the body plane. Conversely, the near-bottom observations of M. hjorti showed it to behave similarly to previous descriptions of Mastigoteuthis magna, orienting vertically with the head down and tentacles extended to the sediment. This orientation is maintained by gentle, complex undulation of the fins. A third species with very large fins and extremely long arms was observed near the bottom from an ROV at approximately 2200 In in January 2000. While it differed from any previously known family, it behaved similarly to a mastigoteuthid. We now believe this specimen was a 'big-fin', family Magnapinnidae Vecchione and Young, 1998. If so, this observation and a similar squid recently observed and video-taped from a submersible in the Indian Ocean extend the known distribution of the recently discovered family to deep waters in subtropical areas around the globe. C1 Natl Museum Nat Hist, NMFS, Natl Systemat Lab, Washington, DC 20560 USA. Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. Harbor Branch Oceanog Inst Inc, Ft Pierce, FL 34946 USA. RP Vecchione, M (reprint author), Natl Museum Nat Hist, NMFS, Natl Systemat Lab, Washington, DC 20560 USA. NR 12 TC 14 Z9 14 U1 0 U2 5 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 SEP PY 2002 VL 71 IS 2 BP 893 EP 901 PG 9 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 677BT UT WOS:000182787600023 ER PT J AU Eberhard, WG AF Eberhard, WG TI Natural history and behavior of Chymomyza mycopelates and C-exophthalma (Diptera : Drosophilidae), and allometry of structures used as signals, weapons, and spore collectors SO CANADIAN ENTOMOLOGIST LA English DT Article ID STALK-EYED FLIES; CYRTODIOPSIS-WHITEI DIOPSIDAE; HAWAIIAN DROSOPHILA; ONE SIZE; DISPLAY; GENITALIA; EVOLUTION; INSECTS; SPIDERS; CHOICE AB Males of Chymomyza mycopelates Grimaldi and Chymomyza exophthalma Grimaldi battled at sites where females fed and mated (but did not oviposit). Both sexes in the two species waved their brightly marked front legs during aggressive interactions, and males used these legs to strike and grasp opponents forcefully. During intense battles, male C. mycopelates also butted or pushed with their heads, whereas male C. exophthalma used their more strikingly wide heads to threaten with stereotyped displays, during which they also held their front legs folded against the sides of their eyes. Courtship behavior by male C. mycopelates involved tactile and perhaps visual displays with the tips of their front legs. Both species also fed by sweeping their front legs over the surface of fruiting fungi and by removing the spores from their legs with their mouthparts. Although male head width in C. exophthalma showed positive allometry, portions of the front legs that were used as signals and as weapons did not, and thus were not in accord with theoretical predictions that weapons and display devices would have steeper allometries. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. EM archisepsis@biologia.ucr.ac.cr NR 41 TC 20 Z9 21 U1 0 U2 7 PU ENTOMOL SOC CANADA PI OTTAWA PA 393 WINSTON AVE, OTTAWA, ONTARIO K2A 1Y8, CANADA SN 0008-347X J9 CAN ENTOMOL JI Can. Entomol. PD SEP-OCT PY 2002 VL 134 IS 5 BP 667 EP 687 PG 21 WC Entomology SC Entomology GA 603CZ UT WOS:000178542400008 ER PT J AU Wisely, SM Ososky, JJ Buskirk, SW AF Wisely, SM Ososky, JJ Buskirk, SW TI Morphological changes to black-footed ferrets (Mustela nigripes) resulting from captivity SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID GEOGRAPHIC-VARIATION; GROWTH; SELECTION; SIZE AB Captive breeding of endangered species carries risks associated with small population size and domestication. The black-footed ferret (Mustela nigripes) was among the first endangered species bred in captivity. We documented morphological changes to the species after >10 years of captive breeding. We measured 9 dental or cranial traits on 109 skulls; 85 specimens were collected prior to captivity and 24 specimens were of captive-born animals. Skulls of captive animals were 5-6% smaller than skulls from precaptive animals and were 3-10% smaller than skulls of animals collected near the founding population, suggesting that changes occurred in captivity rather than from sample bias in the founders of the captive population. Skull size did not correlate with inbreeding coefficients of captive animals, eliminating the possibility that black-footed ferrets were smaller because of the effects of inbreeding depression or overdominance. Although reintroduced animals were smaller than historical animals, we recommended no alterations to the current management because intentional selection for body size might further reduce genetic variation in a genetically impoverished species. We hypothesize that reintroduced individuals will return to historical body sizes rapidly, owing either to release of environmental stresses or to natural selection for larger size. C1 Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. RP Wisely, SM (reprint author), Smithsonian Inst, Genet Mol Lab, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Buskirk, Steven/K-2871-2016 OI Buskirk, Steven/0000-0003-0611-6648 NR 29 TC 6 Z9 7 U1 3 U2 35 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD SEP PY 2002 VL 80 IS 9 BP 1562 EP 1568 DI 10.1139/Z02-160 PG 7 WC Zoology SC Zoology GA 607YC UT WOS:000178817500009 ER PT J AU Perez, M AF Perez, M TI The political 'flying bus': Nationalism, identity, status, citizenship and Puerto Ricans SO CRITIQUE OF ANTHROPOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the American-Ethnological-Society CY APR 17-21, 1996 CL SAN JUAN, PUERTO RICO SP Amer Ethnolog Soc DE citizenship; immigration; nationalism; Puerto Ricans; United States AB The colonial political relationship of Puerto Rico to the United States has established certain contexts which Stimulate debates about citizenship, culture and Puerto Ricanness, The US Congress has been a space where these issues have been contested since 1898, when Puerto Rico became part of the United States. I analyze the discursive contests that took place during 1990 in Congress overjust who were the Puerto Ricans entitled to vote in a plebiscite to decide Puerto Rico's political status. I examine the ways in which the transnational and highly problematic Puerto Rican identity was constructed and contested in this context between Puerto Ricans in the United States and Puerto Ricans in Puerto Rico. C1 Amer Museum Natl Hist, Smithsonian Inst, Washington, DC USA. RP Perez, M (reprint author), Amer Museum Natl Hist, Smithsonian Inst, Washington, DC USA. NR 23 TC 2 Z9 2 U1 0 U2 5 PU SAGE PUBLICATIONS LTD PI LONDON PA 6 BONHILL STREET, LONDON EC2A 4PU, ENGLAND SN 0308-275X J9 CRIT ANTHROPOL JI Crit. Anthropol. PD SEP PY 2002 VL 22 IS 3 BP 305 EP 322 DI 10.1177/0308275X02022003760 PG 18 WC Anthropology SC Anthropology GA 596TG UT WOS:000178181500004 ER PT J AU Flint, OS AF Flint, OS TI Studies on neotropical caddisflies, LX: Three new species of the Chilean genus Microthremma, with a review of the genus (Trichoptera : Helicophidae) SO ENTOMOLOGICAL NEWS LA English DT Article AB The genus Microthremma is confined to Argentina and Chile, and has contained five species. Two new species, M. angulatum and M. patagonicum, both placed in the crassifimbriatum complex, and a third new species, M. lobatum, placed in the griseum complex, are described and figured. Also M. crassifimbriatum is redescribed and figured. A key to males, diagnostic characters, and distributional records is given for all eight species. C1 Natl Museum Nat Hist, Smithsonian Inst, Sect Entomol, Washington, DC 20013 USA. RP Flint, OS (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Sect Entomol, Washington, DC 20013 USA. NR 7 TC 5 Z9 6 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 SEP-OCT PY 2002 VL 113 IS 4 BP 225 EP 232 PG 8 WC Entomology SC Entomology GA 664RB UT WOS:000182073400001 ER PT J AU Dilustro, JJ Day, FP Drake, BG Hinkle, CR AF Dilustro, JJ Day, FP Drake, BG Hinkle, CR TI Abundance, production and mortality of fine roots under elevated atmospheric CO2 in an oak-scrub ecosystem SO ENVIRONMENTAL AND EXPERIMENTAL BOTANY LA English DT Article DE CO2; minirhizotrons; root growth; root length density; root mortality; root turnover ID CARBON-DIOXIDE; MINERAL-NUTRITION; SOIL-NITROGEN; RESPONSES; ENRICHMENT; GROWTH; SEEDLINGS; RHIZOSPHERE; PONDEROSA; INCREASES AB Atmospheric carbon dioxide levels are increasing and are predicted to double this century. The implications of this rise on vegetation structure and function are not well understood. Measurement of root growth response to elevated atmospheric carbon dioxide is critical to understanding plant responses and soil carbon input. We investigated the effects of elevated carbon dioxide on fine root growth using open top chambers with both ambient and elevated (700 ppm) CO2 treatments in an oak-palmetto scrub ecosystem at Kennedy Space Center, FL. Minirhizotron tubes installed in each elevated and control chamber were sampled for root length density (mm cm(-2)) every 3 months. Carbon dioxide enrichment of the chambers began May 15, 1996. By December 1997, root length density (RLD) increased to 7.53 mm cm(-2) for the control chambers and 21.36 mm cm(-2) for the enriched chambers in the top 101-cm of soil. Vertical distribution of fine roots was unchanged under elevated carbon dioxide. Fine root production increased with elevated carbon dioxide, and mortality and turnover were higher in the elevated chambers by the last sample date in 1997. The increased rates of fine root growth coupled with no change in decomposition rate suggest a potential increased rate of carbon input into the soil. However, these results only represent the first 21 months post-fire and recovery to root closure could just be faster in the elevated CO2 atmosphere. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Dynam Corp, Kennedy Space Ctr, FL 32899 USA. Univ Georgia, Savannah River Ecol Lab, Aiken, SC 29802 USA. RP Day, FP (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. NR 39 TC 25 Z9 28 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0098-8472 J9 ENVIRON EXP BOT JI Environ. Exp. Bot. PD SEP PY 2002 VL 48 IS 2 BP 149 EP 159 AR PII S0098-8472(02)00020-5 DI 10.1016/S0098-8472(02)00020-5 PG 11 WC Plant Sciences; Environmental Sciences SC Plant Sciences; Environmental Sciences & Ecology GA 584CD UT WOS:000177448900006 ER PT J AU Nascimento, HEM Laurance, WF AF Nascimento, HEM Laurance, WF TI Total aboveground biomass in central Amazonian rainforests: a landscape-scale study SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Amazon basin; biomass; carbon cycle; carbon storage; global warming; terra-firme forest; tropical rainforest ID RAIN-FOREST FRAGMENTATION; GREENHOUSE-GAS EMISSIONS; TIERRA-FIRME FOREST; BRAZILIAN AMAZON; TROPICAL FORESTS; LAND-USE; CARBON-DIOXIDE; RIO-NEGRO; DEFORESTATION; SOILS AB Amazonian forests play a key role in the global carbon cycle, but there is much uncertainty about the quantity and distribution of carbon stored in these forests. We quantified total aboveground dry biomass (TAGB) in undisturbed central Amazonian rainforests, based on detailed estimates of all live and dead plant material within 20 1 ha plots spanning an extensive (ca. 1000 km(2)) study area. TAGB values in our study area were very high, averaging 397.7 +/- 30.0 Mg ha(-1). The most important component of aboveground biomass was large (greater than or equal to10 cm diameter-at-breast-height (DBH)) trees, which comprised 81.9% of TAGB, followed by downed wood debris (7.0%), small trees, saplings, and seedlings (<10 cm DBH; 5.3%), lianas (2.1%), litter (1.9%), snags (1.5%), and stemless palms (0.3%). Among large trees, aboveground biomass was greatest in intermediate-sized (20-50 cm DBH) stems (46.7% of TAGB), with very large (greater than or equal to60 cm DBH) trees also containing substantial biomass (13.4% of TAGB). There were no significant correlations between large tree biomass and that of any other live or dead biomass component. An analysis based on the variability of our samples suggested that just 3-4 randomly positioned I ha plots would be sufficient to provide a reasonable estimate of mean TAGB in a landscape such as ours (with 95% confidence intervals being <10% of the mean). This suggests that efforts to quantify Amazon forest biomass should be extensive rather than intensive; researchers should sample many geographically separate areas with a few plots each, rather than sampling a small number of areas more intensively. Published by Elsevier Science B.V. C1 Natl Inst Amazonian Res, INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. RP Laurance, WF (reprint author), Natl Inst Amazonian Res, INPA, Biol Dynam Forest Fragments Project, CP 478, BR-69011970 Manaus, Amazonas, Brazil. RI Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012 NR 75 TC 96 Z9 103 U1 2 U2 23 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD SEP 1 PY 2002 VL 168 IS 1-3 BP 311 EP 321 AR PII S0378-1127(01)00749-6 DI 10.1016/S0378-1127(01)00749-6 PG 11 WC Forestry SC Forestry GA 584QJ UT WOS:000177478900025 ER PT J AU Luhr, JF Logan, MAV AF Luhr, JF Logan, MAV TI Sulfur isotope systematics of the 1982 El Chichon trachyandesite: An ion microprobe study SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ILMENITE-SERIES GRANITOIDS; MAGNETITE-SERIES; SUBDUCTION ZONES; VOLCANIC-ROCKS; MEXICO; ERUPTIONS; CHIAPAS; DEPOSITS; MAGMAS; ANHYDRITE C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Luhr, JF (reprint author), Smithsonian Inst, Dept Mineral Sci, NHB-119, Washington, DC 20560 USA. EM luhr@volcano.si.edu NR 64 TC 37 Z9 37 U1 0 U2 6 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 SEP PY 2002 VL 66 IS 18 BP 3303 EP 3316 AR PII S0016-7037(02)00931-6 DI 10.1016/S0016-7037(02)00931-6 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 594BW UT WOS:000178029700011 ER PT J AU Ricklefs, RE Bermingham, E AF Ricklefs, RE Bermingham, E TI The concept of the taxon cycle in biogeography SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE co-evolution; colonization; extinction; habitat distribution; island biogeography; Lesser Antilles; phylogeography; taxon cycles ID LESSER ANTILLEAN AVIFAUNA; CHARACTER DISPLACEMENT; WEST-INDIES; EVOLUTION; BIRDS; EXTINCTION; ISLAND; SPECIATION; ANOLIS; DIFFERENTIATION AB Taxon cycles are sequential phases of expansion and contraction of the ranges of species, associated generally with shifts in ecological distribution. The important contribution of the taxon cycle to biogeographical analysis is its emphasis on evolutionary and ecological interactions among colonizing and resident species, which influence their extinction dynamics and establish patterns of geographical distribution. Taxon cycles were inferred originally from the distribution of species across island archipelagos, where a correlation was noted between gaps in island occupancy and the degree of phenotypic differentiation. This pattern implied that phases of colonization were followed by range contraction, while endemic Antillean species that were undifferentiated between islands suggested secondary expansion and the beginning of a new cycle. This interpretation was met with scepticism, but reconstruction of phylogenetic relationships from gene sequences has now permitted us to characterize taxon cycles in Lesser Antillean birds. The relative timing of phases of the cycle can be deduced from genetic divergence between island populations. We have found that taxon cycles have periods in the order of 10(6) years and that cycles in different lineages occur independently of each other and independently of Pleistocene climate cycles. Individual island populations may persist for several millions of years on the larger islands of the Lesser Antilles; occasional expansion phases lead to the replacement of island populations that have disappeared, thus reducing the archipelago-wide rate of extinction to nil. What drives taxon cycles is unknown, but we speculate that they may be caused by co-evolution with enemy populations, and a probable mechanism would involve infrequent mutations influencing parasite virulence and avian host disease resistance. Taxon cycles undoubtedly occur on continents, but the geographical configuration of island archipelagos reveals more clearly their presence and invites their study. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Ricklefs, RE (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. NR 69 TC 107 Z9 114 U1 2 U2 35 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0960-7447 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD SEP PY 2002 VL 11 IS 5 BP 353 EP 361 DI 10.1046/j.1466-822x.2002.00300.x PG 9 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 596WQ UT WOS:000178189800001 ER PT J AU Lefsky, MA Cohen, WB Harding, DJ Parker, GG Acker, SA Gower, ST AF Lefsky, MA Cohen, WB Harding, DJ Parker, GG Acker, SA Gower, ST TI Lidar remote sensing of above-ground biomass in three biomes SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE above-ground biomass; biomass measurement; carbon storage; global carbon cycle; forest biomass; interbiome comparison; lidar remote sensing; SLICER sensor ID LEAF-AREA INDEX; DECIDUOUS FORESTS; LASER ALTIMETER; VEGETATION; CANOPY; ECOSYSTEM AB Estimation of the amount of carbon stored in forests is a key challenge for understanding the global carbon cycle, one which remote sensing is expected to help address. However, estimation of carbon storage in moderate to high biomass forests is difficult for conventional optical and radar sensors. Lidar (light detection and ranging) instruments measure the vertical structure of forests and thus hold great promise for remotely sensing the quantity and spatial organization of forest biomass. In this study, we compare the relationships between lidar-measured canopy structure and coincident field measurements of above-ground biomass at sites in the temperate deciduous, temperate coniferous, and boreal coniferous biomes. A single regression for all three sites is compared with equations derived for each site individually. The single equation explains 84% of variance in above-ground biomass (P < 0.0001) and shows no statistically significant bias in its predictions for any individual site. C1 Oregon State Univ, Forest Sci Lab, Corvallis, OR 97331 USA. US Forest Serv, USDA, Forest Sci Lab, Corvallis, OR 97331 USA. NASA, Goddard Space Flight Ctr, Geodynam Branch, Greenbelt, MD 20771 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Natl Pk Serv, Seattle, WA 98104 USA. Univ Wisconsin, Dept Forest Ecol & Management, Madison, WI 53706 USA. RP Lefsky, MA (reprint author), Colorado State Univ, Dept Forestry Sci, Forestry Bldg 131, Ft Collins, CO 80523 USA. RI Lefsky, Michael/A-7224-2009; Harding, David/F-5913-2012; OI Parker, Geoffrey/0000-0001-7055-6491 NR 24 TC 233 Z9 253 U1 8 U2 96 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0960-7447 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD SEP PY 2002 VL 11 IS 5 BP 393 EP 399 DI 10.1046/j.1466-822x.2002.00303.x PG 7 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 596WQ UT WOS:000178189800004 ER PT J AU Lellouch, E Bezard, B Moses, JI Davis, GR Drossart, P Feuchtgruber, H Bergin, EA Moreno, R Encrenaz, T AF Lellouch, E Bezard, B Moses, JI Davis, GR Drossart, P Feuchtgruber, H Bergin, EA Moreno, R Encrenaz, T TI The origin of water vapor and carbon dioxide in Jupiter's stratosphere SO ICARUS LA English DT Article DE Jupiter's atmosphere; spectroscopy ID WAVE-ASTRONOMY-SATELLITE; ISO-SWS OBSERVATIONS; COMET SHOEMAKER-LEVY-9; UPPER-ATMOSPHERE; GIANT PLANETS; IMPACT; MONOXIDE; SATURN; OXYGEN; PHOTOCHEMISTRY AB Observations of H2O rotational lines from the Infrared Space Observatory (ISO) and the Submillimeter Wave Astronomy Satellite (SWAS) and of the CO2 nu(2) band by ISO are analyzed jointly to determine the origin of water vapor and carbon dioxide in Jupiter's stratosphere. Simultaneous modelling of ISO/LWS and ISO/SWS observations acquired in 1997 indicates that most of the stratospheric jovian water is restricted to pressures less than 0.5 +/- 12 mbar, with a disk-averaged column density of (2.0 +/- 0.5) x 10(15) cm(-2). Disk-resolved observations of CO2 by ISO/SWS reveal latitudinal variations of the CO2 abundance, with a decrease of at least a factor of 7 from mid-southern to mid-northern latitudes, and a disk-center column density of (3.4 +/- 0.7) x 10(14) cm(-2). These results strongly suggest that the observed. H2O and CO2 primarily result from the production, at midsouthern latitudes, of oxygenated :material in the form of CO and H2O by the Shoemaker-Levy 9 (SL9) impacts in July 1994 and subsequent chemical and transport evolution, rather than from a permanent interplanetary dust particle or satellite source. This conclusion is supported by quantitative evolution model calculations. Given the characteristic vertical mixing times in Jupiter's stratosphere, material deposited at similar to0.1 mbar by the SL9 impacts is indeed expected to diffuse down to the similar to0.5 mbar level after 3 years. A coupled chemical-horizontal transport model indicates that the stability of water vapor against photolysis and conversion to CO2 is maintained over typically similar to50 years by the decrease of the local CO mixing ratio associated with horizontal spreading. A model with an initial (i.e., SL9-produced) H2O/CO mass mixing ratio of 0.07, not inconsistent with immediate postimpact observations, matches the observed H2O abundance and CO2 horizontal distribution 3 years after the impacts. In contrast, the production Of CO2 from SL9-produced CO and a water component deriving from an interplanetary dust component is insufficient to account for the observed CO2 amounts. The observations can further be used to place a stringent upper limit (8 x 10(4) cm(-2) s(-1)) on the permanent water influx into Jupiter. This may indicate that the much larger flux observed at Saturn derives dominantly from a ring source, or that the ablation of micrometeoroids leads dominantly to different species at Saturn (H2O) and Jupiter (CO). Finally, the SWAS H2O spectra do not appear fully consistent with the ISO data and should be confirmed by future ODIN and Herschel observations. (C) 2002 Elsevier Science (USA). C1 Observ Paris, F-92195 Meudon, France. Lunar & Planetary Inst, Houston, TX 77058 USA. Univ Saskatchewan, Saskatoon, SK S7N 5E2, Canada. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Radio Astron Millimetr, F-38400 St Martin Dheres, France. RP Lellouch, E (reprint author), Observ Paris, F-92195 Meudon, France. RI Moses, Julianne/I-2151-2013 OI Moses, Julianne/0000-0002-8837-0035 NR 68 TC 58 Z9 58 U1 1 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD SEP PY 2002 VL 159 IS 1 BP 112 EP 131 DI 10.1006/icar.2002.6929 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 593LE UT WOS:000177992100008 ER PT J AU Finn, B AF Finn, B TI Eloges - Brooke Hindle, 28 September 1918-3 June 2001 SO ISIS LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20560 USA. RP Finn, B (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD SEP PY 2002 VL 93 IS 3 BP 454 EP 456 DI 10.1086/374063 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 626HP UT WOS:000179866000004 ER PT J AU Forman, P AF Forman, P TI The measurement of time: Time, frequency, and the atomic clock. SO ISIS LA English DT Book Review C1 Smithsonian Inst, Amer Museum Nat Hist, Modern Phys Collect, Washington, DC 20560 USA. RP Forman, P (reprint author), Smithsonian Inst, Amer Museum Nat Hist, Modern Phys Collect, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD SEP PY 2002 VL 93 IS 3 BP 522 EP 523 DI 10.1086/374131 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 626HP UT WOS:000179866000075 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI A history of the European space agency, 1958-1987, vol 1, The story of ESRO and ELDO, 1958-1973, vol 2, The story of ESA, 1973-1987. SO ISIS LA English DT Book Review 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 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD SEP PY 2002 VL 93 IS 3 BP 528 EP 529 DI 10.1086/374138 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 626HP UT WOS:000179866000083 ER PT J AU West-Eberhard, MJ AF West-Eberhard, MJ TI On Stephen Jay Gould SO JOURNAL OF BIOSCIENCES LA English DT Biographical-Item C1 Smithsonian Trop Res Inst, Unit 2511, APO, AA 34020 USA. RP West-Eberhard, MJ (reprint author), Smithsonian Trop Res Inst, Unit 2511, APO, AA 34020 USA. NR 1 TC 0 Z9 0 U1 1 U2 7 PU INDIAN ACADEMY SCIENCES PI BANGALORE PA P B 8005 C V RAMAN AVENUE, BANGALORE 560 080, INDIA SN 0250-5991 J9 J BIOSCIENCES JI J. Biosci. PD SEP PY 2002 VL 27 IS 5 BP 447 EP 447 DI 10.1007/BF02705035 PG 1 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 596VC UT WOS:000178186300005 ER PT J AU Stanley, JD Jorstad, TR AF Stanley, JD Jorstad, TR TI Iron-coated quartz as a provenance and paleoclimatic marker in the Rhone delta, France SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE archaeology; climatic cycles; coastal processes; Costieres; Crau; distal sediment; floods; Gulf of Lion; Holocene; iron oxides; Pleistocene; proximal sediment; quartz coating; sediment dispersal; size-sorting; source terrains; weathering ID SEA-LEVEL RISE; GULF-OF-LIONS; CONTINENTAL-SHELF; ALLUVIAL DEPOSITS; STAINED-QUARTZ; SEDIMENT; HOLOCENE; PLEISTOCENE; RIVER; AREA AB Analyses of 430 surficial and core sediment samples in the Rhone delta and adjacent region in southern France record similar average proportions of iron-stained quartz (ISQ) on the delta plain and in the Rhone and Durance rivers (similar to30%). These two rivers, largely responsible for the formation of the Holocene delta, carried most of their sediment load from distal source terrains. The much higher ISQ values in sand on the delta's modern coast (to >40%) and on older sand strand deposits (56%) subaerially exposed in the central and southern delta plain are primarily the result of post-depositional in situ formation of iron coating on quartz particles. However, some subsurface delta plain core samples with high stained-grain content (>40%) have a different origin. These layers were derived from Pleistocene and older sediment in proximal terrains, characterized by very high ISQ values (67%), that were transported to the delta plain. Evidence indicating displacement of highly-stained material eroded from these more local source areas is quartz with high ISQ values (50%) in the Vidourle and Gardon rivers with headwaters in adjacent uplands. Strata with large ISQ values (>40%) in Holocene core sections are attributed primarily to periodically increased hydrological fluxes that resulted from marked paleoclimatic changes and, possibly, effects of human activity as seen in the archaeological record in southern France. Wetter climatic conditions increased the erosion and reworking of proximal ISQ-enriched terrigenous sediment to the delta. This study indicates that the stained-grain method can be used to help identify changes in sediment provenance and dispersal patterns related to Holocene paleoclimatic fluctuations and/or human activity in the Rhone delta region. C1 Smithsonian Inst, NMNH, Deltas Global Change Program, Washington, DC 20560 USA. RP Stanley, JD (reprint author), Smithsonian Inst, NMNH, Deltas Global Change Program, E-206, Washington, DC 20560 USA. NR 68 TC 2 Z9 2 U1 0 U2 4 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD FAL PY 2002 VL 18 IS 4 BP 712 EP 729 PG 18 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 618JJ UT WOS:000179414700011 ER PT J AU Ubelaker, DH Ward, DC Braz, VS Stewart, J AF Ubelaker, DH Ward, DC Braz, VS Stewart, J TI The use of SEM/EDS analysis to distinguish dental and osseus tissue from other materials SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; forensic anthropology; SEM/EDS analysis; X-ray spectra; bone and tooth identification AB With increasing frequency, relatively small, fragmentary evidence thought to be osseous or dental tissue of human origin is submitted to the forensic laboratory for DNA analysis with the request for positive identification. Prior to performing DNA analysis, however, it is prudent to first perform a presumptive test or "screen" to determine whether the questioned material may be eliminated from further consideration. When material is shown not to be consistent with bone/teeth, DNA testing is not performed. When such determinations cannot be made from gross morphological features, elemental analysis can be indicative. This presumptive test is made possible by applying scanning electron microscopy/energy dispersive X-ray spectroscopy (SEM/EDS) in conjunction with an X-ray spectral database recently developed by the FBI laboratory. This database includes spectra for many different materials including known examples of bone and tooth from many different contexts and representing the full range of taphonomic conditions Results of SEM/EDS analysis of evidence can be compared to these standards to determine if they are consistent with bone and/or tooth and, if not, then what the material might represent. Analysis suggests that although the proportions and amounts of calcium and phosphorus are particularly important in differentiating bone and tooth from other materials, other minor differences in spectral profile can also provide significant discrimination Analysis enables bone and tooth to be successfully distinguished from other materials in most cases. Exceptions appear to be ivory, mineral apatite, and perhaps some types of corals. C1 Smithsonian Inst, NMNH, Dept Anthropol, Washington, DC 20560 USA. Fed Bur Invest, Washington, DC USA. Fed Univ Rio De Janeiro, Biol Anthropol Div, Rio De Janeiro, Brazil. RP Ubelaker, DH (reprint author), Smithsonian Inst, NMNH, Dept Anthropol, MRC 112, Washington, DC 20560 USA. NR 4 TC 18 Z9 19 U1 0 U2 6 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 USA SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD SEP PY 2002 VL 47 IS 5 BP 940 EP 943 PG 4 WC Medicine, Legal SC Legal Medicine GA 596UY UT WOS:000178185800003 PM 12353578 ER PT J AU Jucks, KW Johnson, DG Chance, KV Traub, WA Margitan, JM Stachnik, R Sasano, Y Yokota, T Kanzawa, H Shibasaki, K Suzuki, M Ogawa, T AF Jucks, KW Johnson, DG Chance, KV Traub, WA Margitan, JM Stachnik, R Sasano, Y Yokota, T Kanzawa, H Shibasaki, K Suzuki, M Ogawa, T TI Validation of ILAS v5.2 data with FIRS-2 balloon observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LIMB-ATMOSPHERIC-SPECTROMETER; HALOGEN OCCULTATION EXPERIMENT; UARS PLATFORM; STRATOSPHERE; OZONE; HO2; H2O AB [1] Comparisons of remote sensing stratospheric mixing ratio profiles for O-3,H2O, N2O, HNO3, and NO2 are shown between data (version 5.2) obtained by the Improved Limb Atmospheric Spectrometer (ILAS) on board the Japanese Advanced Earth Observing Satellite (ADEOS) and the Smithsonian Astrophysical Observatory far-infrared spectrometer (FIRS)-2 balloon-borne spectrometer from a flight on 30 April 1997 originating in Fairbanks, Alaska. Submillimeter wave remote sensing and UV in situ observations of mixing ratios of O-3 from Jet Propulsion Laboratory (JPL) instruments obtained on board the same balloon gondola are also used for comparison with ILAS mixing ratios of O-3. The remote sensing balloon observations occurred roughly 5 latitude, and the in situ 2 latitude, north of the nearest ILAS observations and were taken between 0700 and 1300 local solar time (LST), while the ILAS data were taken at the previous local sunset (near 2100 LST). Back trajectories from the locations and times of balloon data sets to the prior local sunset were within 2 latitude and 10 longitude of the nearest ILAS occultation; the validation therefore effectively occurred in very nearly the same air mass as was observed with ILAS, and well within a 1-day time interval. The mixing ratio profiles of all of the compared molecules (O-3, HNO3,N2O, H2O, and NO2) agree to within the combined uncertainties with only minor systematic offsets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Jet Propuls Lab, Pasadena, CA USA. Japan Environm Agcy, Natl Inst Environm Studies, Tsukuba, Ibaraki 305, Japan. Kokugakuin Univ, Shibuya Ku, Tokyo 1508440, Japan. NASDA, Earth Observat Res Ctr, Tokyo, Japan. RP Jucks, KW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Sasano, Yasuhiro/C-2927-2009; Johnson, David/F-2376-2015 OI Sasano, Yasuhiro/0000-0001-7470-5642; Johnson, David/0000-0003-4399-5653 NR 26 TC 6 Z9 6 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP-OCT PY 2002 VL 107 IS D24 AR 8207 DI 10.1029/2001JD000578 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 637BN UT WOS:000180491900003 ER PT J AU Martin, RV Chance, K Jacob, DJ Kurosu, TP Spurr, RJD Bucsela, E Gleason, JF Palmer, PI Bey, I Fiore, AM Li, QB Yantosca, RM Koelemeijer, RBA AF Martin, RV Chance, K Jacob, DJ Kurosu, TP Spurr, RJD Bucsela, E Gleason, JF Palmer, PI Bey, I Fiore, AM Li, QB Yantosca, RM Koelemeijer, RBA TI An improved retrieval of tropospheric nitrogen dioxide from GOME SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING EXPERIMENT; ABSORPTION CROSS-SECTIONS; SENSING REFERENCE DATA; MARINE BOUNDARY-LAYER; 231-794 NM RANGE; REACTIVE NITROGEN; RAMAN-SCATTERING; UNITED-STATES; NORTH-AMERICA; MODEL AB We present a retrieval of tropospheric nitrogen dioxide (NO2) columns from the Global Ozone Monitoring Experiment (GOME) satellite instrument that improves in several ways over previous retrievals, especially in the accounting of Rayleigh and cloud scattering. Slant columns, which are directly fitted without low-pass filtering or spectral smoothing, are corrected for an artificial offset likely induced by spectral structure on the diffuser plate of the GOME instrument. The stratospheric column is determined from NO2 columns over the remote Pacific Ocean to minimize contamination from tropospheric NO2. The air mass factor (AMF) used to convert slant columns to vertical columns is calculated from the integral of the relative vertical NO2 distribution from a global 3-D model of tropospheric chemistry driven by assimilated meteorological data (Global Earth Observing System (GEOS)-CHEM), weighted by altitude-dependent scattering weights computed with a radiative transfer model (Linearized Discrete Ordinate Radiative Transfer), using local surface albedos determined from GOME observations at NO2 wavelengths. The AMF calculation accounts for cloud scattering using cloud fraction, cloud top pressure, and cloud optical thickness from a cloud retrieval algorithm (GOME Cloud Retrieval Algorithm). Over continental regions with high surface emissions, clouds decrease the AMF by 20-30% relative to clear sky. GOME is almost twice as sensitive to tropospheric NO2 columns over ocean than over land. Comparison of the retrieved tropospheric NO2 columns for July 1996 with GEOS-CHEM values tests both the retrieval and the nitrogen oxide radical (NOx) emissions inventories used in GEOS-CHEM. Retrieved tropospheric NO2 columns over the United States, where NOx emissions are particularly well known, are within 18% of GEOS-CHEM columns and are strongly spatially correlated (r = 0.78, n = 288, p < 0.005). Retrieved columns show more NO2 than GEOS-CHEM columns over the Transvaal region of South Africa and industrial regions of the northeast United States and Europe. They are lower over Houston, India, eastern Asia, and the biomass burning region of central Africa, possibly because of biases from absorbing aerosols. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Space Res Org Netherlands, NL-3584 Utrecht, Netherlands. RP Harvard Univ, Div Engn & Appl Sci, G3D Pierce Hall,29 Oxford St, Cambridge, MA 02138 USA. EM rvmartin@fas.harvard.edu RI Martin, Randall/A-2051-2008; Palmer, Paul/F-7008-2010; Gleason, James/E-1421-2012; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; NR 73 TC 210 Z9 223 U1 3 U2 29 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 SEP-OCT PY 2002 VL 107 IS D20 AR 4437 DI 10.1029/2001JD001027 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 636PY UT WOS:000180466200100 ER PT J AU Sugita, T Yokota, T Nakajima, H Kanzawa, H Nakane, H Gernandt, H Yushkov, V Shibasaki, K Deshler, T Kondo, Y Godin, S Goutail, F Pommereau, JP Camy-Peyret, C Payan, S Jeseck, P Renard, JB Bosch, H Fitzenberger, R Pfeilsticker, K von Konig, M Bremer, H Kullmann, H Schlager, H Margitan, JJ Stachnik, B Toon, GC Jucks, K Traub, WA Johnson, DG Murata, I Fukunishi, H Sasano, Y AF Sugita, T Yokota, T Nakajima, H Kanzawa, H Nakane, H Gernandt, H Yushkov, V Shibasaki, K Deshler, T Kondo, Y Godin, S Goutail, F Pommereau, JP Camy-Peyret, C Payan, S Jeseck, P Renard, JB Bosch, H Fitzenberger, R Pfeilsticker, K von Konig, M Bremer, H Kullmann, H Schlager, H Margitan, JJ Stachnik, B Toon, GC Jucks, K Traub, WA Johnson, DG Murata, I Fukunishi, H Sasano, Y TI Validation of ozone measurements from the Improved Limb Atmospheric Spectrometer SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE ILAS; solar occultation; stratosphere; ozone ID HALOGEN OCCULTATION EXPERIMENT; GAS EXPERIMENT-II; STRATOSPHERIC AEROSOL; POLAR OZONE; POAM-II; SOLAR OCCULTATION; HETERODYNE MEASUREMENTS; VERTICAL-DISTRIBUTION; NORTHERN EUROPE; TRACE-GAS AB [1] Vertical profiles of ozone concentration in the high latitudes were observed by the Improved Limb Atmospheric Spectrometer (ILAS) aboard the Advanced Earth Observing Satellite (ADEOS) from November 1996 to June 1997. The ozone data obtained by the version 5.20 ILAS retrieval algorithm are compared with those obtained by the version 19 Halogen Occultation Experiment (HALOE), the version 6 Stratospheric Aerosol and Gas Experiment (SAGE) II, and the version 6 Polar Ozone and Aerosol Measurement (POAM) II retrieval algorithms. The ILAS data are also compared with ozone data measured by ozonesondes, instruments on board balloons or an aircraft, and ground-based instruments. The ILAS ozone data generally agree with its correlative data between 11 and 64 km with some exceptions. Quantitatively, the median value of the relative difference (absolute difference divided by its mean value) for these comparisons was within +/-10%. Relative differences (18%) exceeding the combined measurement errors were found around 45-55 km altitude from comparisons with the HALOE and SAGE II data in January 1997 in the Southern Hemisphere (SH). Larger relative differences (around 50%) were also found below 15 km from comparisons with the HALOE and POAM II data in November 1996 in the SH, but these absolute differences were 0.10-0.16 ppmv as the median value. The ozone data processed by the version 5.20 were improved compared to the former version 3.10, which is available to the general public. The version 5.20 ozone data can be used for scientific analysis purposes based on the accuracy of the data in comparison with these other instruments. C1 Natl Inst Environm Studies, Ozone Layer Res Project, Tsukuba, Ibaraki 3058506, Japan. Alfred Wegener Inst Polar & Marine Res, D-2850 Bremerhaven, Germany. Cent Aerol Observ, Dolgoprudnyi, Russia. Kokugakuin Univ, Fac Letters, Tokyo, Japan. Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. Univ Tokyo, Adv Sci & Technol Res Ctr, Tokyo, Japan. CNRS, Serv Aeron, Paris, France. CNRS, Lab Phys Mol & Applicat, Paris, France. CNRS, Lab Phys & Chim Environm, F-45071 Orleans, France. Univ Heidelberg, Inst Umweltphys, D-6900 Heidelberg, Germany. Univ Bremen, Inst Umweltphys, Bremen, Germany. DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany. CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tohoku Univ, Dept Geophys, Sendai, Miyagi 980, Japan. RP Sugita, T (reprint author), Natl Inst Environm Studies, Ozone Layer Res Project, 16-2 Onogawa, Tsukuba, Ibaraki 3058506, Japan. RI Sasano, Yasuhiro/C-2927-2009; Kondo, Yutaka/D-1459-2012; Sinnhuber, Miriam/A-7252-2013; Johnson, David/F-2376-2015; Boesch, Hartmut/G-6021-2012 OI Sasano, Yasuhiro/0000-0001-7470-5642; Johnson, David/0000-0003-4399-5653; NR 59 TC 24 Z9 25 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP-OCT PY 2002 VL 107 IS D24 AR 8212 DI 10.1029/2001JD000602 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 637BN UT WOS:000180491900010 ER PT J AU Grant, JA Parker, TJ AF Grant, JA Parker, TJ TI Drainage evolution in the Margaritifer Sinus region, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; water; valleys; channels; rainfall; sapping ID MARTIAN IMPACT CRATERS; ISIDIS BASIN; VALLEYS; DEGRADATION; SURFACE; WATER; AGE AB [1] Margaritifer Sinus, Mars, records a complex history of water transport, storage, and release extending from the late Noachian into at least the mid-Hesperian. Collection, transport, and discharge of water were accomplished by systems of differing character flanking opposite sides of the Chryse Trough. Drainage on the western side of the trough was via the segmented Uzboi-Ladon-Margaritifer mesoscale outflow system that heads in Argyre Basin and incises and fills as it crosses ancient multiringed impact basins. By contrast, Samara and Parana-Loire Valles, two of the largest and best integrated valley systems on Mars, dominated drainage on the eastern trough flank. Valley morphometry suggests formation was due to precipitation-recharged groundwater sapping. All systems discharged into Margaritifer Basin, located along the Chryse Trough axis, and caused ponding that persisted into the early Hesperian. The Uzboi-Ladon-Margaritifer system dominated discharge that was coincident with widespread geomorphic activity on Mars. As channel and valley formation ended, some water in Margaritifer Basin infiltrated the subsurface. Collapse and release of water began shortly thereafter and persisted into mid-Hesperian times, thereby forming Margaritifer and Iani Chaos and incising Ares Vallis. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 54 TC 58 Z9 58 U1 0 U2 4 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 SEP PY 2002 VL 107 IS E9 AR 5066 DI 10.1029/2001JE001678 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 639LP UT WOS:000180630500004 ER PT J AU Diogo, R Chardon, M Vandewalle, P AF Diogo, R Chardon, M Vandewalle, P TI Osteology and myology of the cephalic region and pectoral girdle of the Chinese catfish Cranoglanis bouderius, with a discussion on the autapomorphies and phylogenetic relationships of the Cranoglanididae (Teleostei : Siluriformes) SO JOURNAL OF MORPHOLOGY LA English DT Article DE autapomorphies; catfish; Cranoglanididae; myology; osteology; phylogeny; Siluriformes ID BIOGEOGRAPHY; ANATOMY; MUSCLES; FISHES; OSTARIOPHYSI; SILUROIDEI; HOMOLOGIES; SYNONYMY; ORIGIN AB The cephalic and pectoral girdle structures of the Chinese catfish Cranoglanis bouderius are described and compared with those of other catfishes as the foundation for an analysis on the Cranoglanididae autapomorphies and also for a discussion on the phylogenetic relationships between the cranoglanidids and the other catfishes. Our observations and comparisons indicate that cranoglanidids are defined, at least, by four autapomorphies, namely: 1) the cartilages associated with the mandibular barbels are broad, somewhat circular; 2) epioccipital with a well-developed posterodorsal process, which presents a large, deep, circular posterior concavity; 3) a well-defined, deep, anteroposteriorly elongated concavity formed by both the frontal and the lateral ethmoid to receive the anteromedial surface of the metapterygoid; 4) the adductor mandibulae A3" is dorsally divided into two bundles and partially inserted on the posterior portion of the primordial ligament. With respect to the phylogenetic relationships of the Cranoglanididae, this study strongly suggests that these fishes are probably closely related to the Ariidae and the Claroteidae. (C) 2002 Wiley-Liss, Inc. C1 Univ Liege, Inst Chim, Lab Funct & Evolutionary Morphol, B-4000 Sart Tilman Par Liege, Liege, Belgium. RP Diogo, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM R.Diogo@student.ulg.ac.be OI Diogo, Rui/0000-0002-9008-1910 NR 51 TC 14 Z9 17 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD SEP PY 2002 VL 253 IS 3 BP 229 EP 242 DI 10.1002/jmor.10000 PG 14 WC Anatomy & Morphology SC Anatomy & Morphology GA 579QN UT WOS:000177189500003 PM 12125062 ER PT J AU Johnson, JS AF Johnson, JS TI First aid for finds, 3rd edition. SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Cultural Resources Ctr, Suitland, MD 20746 USA. RP Johnson, JS (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Cultural Resources Ctr, 4220 Silver Hill Rd, Suitland, MD 20746 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD FAL-WIN PY 2002 VL 41 IS 3 BP 296 EP 298 DI 10.2307/3179928 PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 770ER UT WOS:000188710700010 ER PT J AU Polhemus, DA AF Polhemus, DA TI An initial review of Orthotylus in the Hawaiian Islands, with descriptions of twenty-one new species (Heteroptera : Miridae) SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE plant bugs; Orthotylus; Hawaii; new species; host plant associations AB The plant bug genus Orthotylus has undergone extensive insular radiation in the Hawaiian Islands. Based on male paramere structure and dorsal setiferation, at least four major clades appear to be present, each of which has sequentially tracked particular host plant families along the island chain in geological and evolutionary time. In this work, 21 new species of Hawaiian Orthorylus are described, arranged by host plant affiliation. The new species and their host plant associations are as follows: O. pisoniae from Oahu, on Pisonia umbellifera and Pisonia sandwicensis; O. pisonioides, from Hawaii, on Pisonia brunoniana; O. hedyoti from Oahu, on Hedyotis terminalis; O. hedyotiopsis from Oahu, on Hedyotis acuminata; O. hedyoticola from Hawaii, on Hedyotis terminalis; O. psychotriae from Hawaii, on Psychotria hawaiiensis; O. psychotrioides from Hawaii, on Psychotria hawaiiensis; O. psychotricola from Oahu, on Psychotria mariniana; O. coprosmae from Maui, on Coprosma foliosa and Coprosma pubens; O. coprosmoides from Oahu, on Coprosma ochracea; O. ilicis from Maui, on flex anomala; O. neoilicis from Hawaii, on Ilex anomala; O. urerae from Oahu, on Urera kaalae; O. pipturi from Hawaii, on Pipturus albidus; O. pipturoides from Maui, on Pipturus albidus; O. pseudotantali from Maui, on Pipturus albidus; O. clermontiae from Hawaii, on Clermontia clermontioides; O. xylosmae from Hawaii, on Xylosma hawaiiense; O. diospyri from Hawaii, on Diospyros sandwicensis; and O. hibisci from Oahu, on Hibiscus arnottianus. Redescriptions are also given for 5 previously described species: O. kanakanus (Kirkaidy) from Hawaii, on Coprosma rhynchocarpa; O. perkinsi Kirkaldy from Hawaii, on flex anomala; O. tantali (Perkins) from Oahu on Pipturus albidus; O. iolani Kirkaldy from Hawaii, on Clermontia clermontioides; and O. daphne (Kirkaldy) from Oahu on Xylosma hawaiiense. Shaded dorsal habitus drawings are provided for O. hedyotiopsis and O. psychotrioides. Figures of the male genitalic structures and distribution maps are provided for all species treated, accompanied by a table of species and host plant relationships. C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. RP Polhemus, DA (reprint author), Smithsonian Inst, Dept Systemat Biol, MRC 105,POB 37012, Washington, DC 20013 USA. NR 10 TC 7 Z9 8 U1 1 U2 2 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD FAL-WIN PY 2002 VL 110 IS 3-4 BP 270 EP 340 DI 10.1664/0028-7199(2002)110[270:AIROOI]2.0.CO;2 PG 71 WC Entomology SC Entomology GA 670ZX UT WOS:000182441100002 ER PT J AU Zobin, VM Luhr, JF Taran, YA Breton, M Cortes, A De La Cruz-Reyna, S Dominguez, T Galindo, I Gavilanes, JC Muniz, JJ Navarro, C Ramirez, JJ Reyes, GA Ursua, M Velasco, J Alatorre, E Santiago, H AF Zobin, VM Luhr, JF Taran, YA Breton, M Cortes, A De La Cruz-Reyna, S Dominguez, T Galindo, I Gavilanes, JC Muniz, JJ Navarro, C Ramirez, JJ Reyes, GA Ursua, M Velasco, J Alatorre, E Santiago, H TI Overview of the 1997-2000 activity of Volcan de Colima, Mexico SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Volcan de Colima; Mexico; lava flows; pyroclastic flows; monitoring; eruption ID DE-COLIMA; PLATE; ERUPTION AB This overview of the 1997-2000 activity of Volcan de Colima is designed to serve as an introduction to the Special Issue and a summary of the detailed studies that follow. New andesitic block lava was first sighted from a helicopter on the morning of 20 November 1998, forming a rapidly growing dome in the summit crater. Numerous antecedents to the appearance of the dome were recognized, starting more than a year in advance, including: (1) pronounced increases in S/Cl and deltaD values at summit fumaroles in mid-1997; (2) five earthquake swarms between November-December 1997 and October-November 1998, with hypocenters that ranged down to 8 km beneath the summit and became shallower as the eruption approached; (3) steady inflation of the volcano reflected in shortening of geodetic survey line lengths beginning in November-December 1997 and continuing until the start of the eruption; (4) air-borne correlation spectrometer measurements Of SO2 that increased from the background values of < 30 tons/day recorded since 1995 to reach 400 tons/day on 30 October 1998 and 1600 tons/day on 18 November 1998; and (5) small ash emissions detected by satellite-borne sensors beginning on 22 November 1997. The seismic and other trends were the basis of a short-term forecast of an eruption, announced on 13 November 1998, with a forecast window of 16-18 November. Although the lava dome actually appeared on 20 November, this forecast is considered to have been a major success, and the first of its kind at Volcan de Colima. Based in part on this forecast, orderly evacuations of Yerbabuena, Juan Barragan, and other small proximal communities took place on 18 November. The lava dome grew rapidly (similar to4.4 m(3)/s) on 20 November, and was spilling over the SW rim of the crater by the morning of 21 November to feed block-and-ash flows (pyroclastic flows) ahead of an advancing lobe of andesitic block lava. The pyroclastic flows were initially generated at intervals of 3-5 min, reached speeds of 80-90 km/h, and extended out to 4.5 km from the crater. The block lava flow was already similar to150 m long by the afternoon of 21 November. It ultimately split into three lobes that flowed down the three branches of Barranca el Cordoban on the SSW flank of Volcan de Colima; the lava advanced atop previously emplaced pyroclastic-flow deposits from the same eruptive event, whose total volume is estimated as 24 X 10(5) m(3). The three lava lobes ultimately reached 2.8-3.8 km from the crater, had flow fronts similar to30 m high, and an estimated total volume of 39 X 106 in'. By early February 1999 the lava flows were no longer being fed from the summit crater, but the flow fronts continued their slow advance driven by gravitational draining of their partially molten interiors. The 1998-1999 andesites continued a compositional trend toward relatively higher SiO2 and lower MgO that began with the 1991 lava eruption, completing the reversal of an excursion to more mafic compositions (lower SiO2 and higher MgO) that occurred during 1976-1982. Accordingly, the 19981999 andesites show no signs of a transition toward the more mafic magmas that have characterized the major explosive eruptions of Volcan de Colima, such as those of 1818 and 1913. A large explosion on 10 February 1999 blasted a crater through the 1998-1999 lava dome and marked the beginning of a new explosive stage of activity at Volcan de Colima. Incandescent blocks showered the flanks out to 5 km distance, forming impact craters and triggering numerous forest fires. Similar large explosions occurred on 10 May and 17 July 1999, interspersed with numerous smaller explosions of white steam or darker ash-bearing steam. Intermittent minor explosive activity continued through the year 2000, and another large explosion took place on 22 February, 2001. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Univ Colima, Observ Vulcanol, Colima 28052, Mexico. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Univ Colima, Ctr Univ Invest Ciencias Ambiente, Colima 28000, Mexico. Univ Colima, Coordinac Gen Invest Cient, Colima 28040, Mexico. Consejo Estatal Protecc Civil Colima, Colima 28010, Mexico. Natl Autonomous Univ Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. RP Zobin, VM (reprint author), Univ Colima, Observ Vulcanol, Av Gonzalo Sandoval 333,Col Las Viboras, Colima 28052, Mexico. RI Namikawa, Laercio/C-5559-2013 OI Namikawa, Laercio/0000-0001-7847-1804 NR 39 TC 51 Z9 51 U1 1 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD SEP PY 2002 VL 117 IS 1-2 BP 1 EP 19 AR PII S0377-0273(02)00232-9 DI 10.1016/S0377-0273(02)00232-9 PG 19 WC Geosciences, Multidisciplinary SC Geology GA 608PQ UT WOS:000178855900003 ER PT J AU Luhr, JF AF Luhr, JF TI Petrology and geochemistry of the 1991 and 1998-1999 lava flows from Volcan de Colima, Mexico: implications for the end of the current eruptive cycle SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Volcan de Colima; pyroclastic flows; petrology; geochemistry ID MOUNT-ST-HELENS; PARTITION-COEFFICIENTS; ELEMENT PARTITION; BASALTIC MAGMAS; COMPLEX SYSTEMS; ORTHO-PYROXENE; WATER-CONTENT; NEW-ZEALAND; DE-COLIMA; CRYSTALLIZATION AB Point-counted modes, representative mineral analyses, and whole-rock major- and trace-element compositions determined by X-ray fluorescence spectroscopy and inductively coupled plasma mass spectroscopy (ICP-MS) are presented for 11 samples of the hornblende-andesite block-lava flows erupted from Volcan de Colima in 1991 and 1998-1999. New ICP-MS trace-element data are also presented for 37 andesites erupted between 1869 and 1982, described in previous publications. These data are used to evaluate mineralogical and whole-rock compositional changes during two well-defined historical eruption cycles: 1818-1913 and 1913-present. The eruptive cycles of Volcan de Colima are dominated by andesitic lavas with similar to61 wt% SiO2, but terminate with major explosive eruptions, as occurred in 1818 and 1913, involving relatively mafic andesites with similar to58% SiO2. Following eruptions of andesitic block-lava flows with similar to61% SiO2 in 1961-1962 and 1975-1976, a trend toward lower SiO2 contents began in 1976 and peaked in 1981, probably as a small volume of deeper, more mafic magma ascended into the shallower andesitic reservoir beneath the volcano. Since then, however, andesitic lavas have become progressively richer in SiO2 through the 1991 and 1998-1999 eruptions. Andesites erupted between 1961 and 1999 show many subtle but important differences compared to those erupted between 1869 and 1913. Based on rocks of similar SiO2 content, the 1961-1999 andesites are richer in modal plagioclase and in the elements Y, Nb, Tb, Ho, Er, Yb, and Ta, and they are poorer in modal hornblende and in the elements Ba and Sr. All of these observations are consistent with the interpretation that the magmas of 1961-1999 had significantly lower water contents compared to those erupted in 1869-1913, which diminished the role of hornblende crystallization and enhanced the role of plagioclase crystallization. The relatively lower magmatic water contents for the 1961-1999 andesites imply that the explosive eruption anticipated to terminate the current eruptive cycle will be less powerful than the 1913 eruption. Of equal importance to this question, however, is the role of magmatic degassing. The relatively higher viscosities of andesitic magmas with similar to61% SiO2 likely lead to relatively slow ascent rates and more thorough degassing prior to arrival of the magma at the summit crater and its eruption as block lava. In contrast, the lower viscosities of more mafic andesitic magmas with similar to58% SiO2 result in faster ascent and greater retention of volatiles, so that they erupt explosively upon reaching the summit crater. Published by Elsevier Science B.V. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Luhr, JF (reprint author), Smithsonian Inst, Dept Mineral Sci, NHB-119, Washington, DC 20560 USA. NR 78 TC 61 Z9 61 U1 3 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD SEP PY 2002 VL 117 IS 1-2 BP 169 EP 194 AR PII S0377-0273(02)00243-3 PG 26 WC Geosciences, Multidisciplinary SC Geology GA 608PQ UT WOS:000178855900014 ER PT J AU Schroll, S AF Schroll, S TI Wifredo Lam and the International Avant-Garde, 1923-1982. SO LIBRARY JOURNAL 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 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 SEP 1 PY 2002 VL 127 IS 14 BP 174 EP 174 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 589AD UT WOS:000177734500070 ER PT J AU Burbine, TH McCoy, TJ Nittler, LR Benedix, GK Cloutis, EA Dickinson, TL AF Burbine, TH McCoy, TJ Nittler, LR Benedix, GK Cloutis, EA Dickinson, TL TI Spectra of extremely reduced assemblages: Implications for Mercury SO METEORITICS & PLANETARY SCIENCE LA English DT Article; Proceedings Paper CT Workshop on Mercury CY OCT 04-05, 2001 CL FIELD MUSEUM, CHICAGO, ILLINOIS HO FIELD MUSEUM ID SILICATE FRACTIONATION; SOLAR-SYSTEM; AUBRITE; REFLECTANCE; METEORITES; MISSION; SURFACE; SPECTROSCOPY; OBJECTIVES; ASTEROIDS AB We investigate the possibility that Mercury's crust is very reduced with FeO concentrations of less than similar to0.1 wt%. We believe that such a surface could have a composition of enstatite, plagioclase, diopside, and sulfide, similar to the mineral assemblages found in aubritic meteorites. To test this hypothesis, we investigated the spectra of aubrites and their constituent minerals as analogs for the surface of Mercury. We found that some sulfides have distinctive absorption features in their spectra shortwards of similar to0.6 mum that may be apparent in the spectrum of such an object. Determination of the surface composition of Mercury using orbital x-ray spectroscopy should easily distinguish between a lunar highlands and enstatite basalt composition since these materials have significant differences in concentrations of Al, Mg, S, and Fe. The strongest argument against Mercury having an enstatite basalt composition is its extreme spectral redness. Significant reddening of the surface of an object (such as Mercury) is believed to require reduction of FeO to nanophase iron, thus requiring a few percent FeO in the material prior to alteration. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Burbine, TH (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. OI Benedix, Gretchen/0000-0003-0990-8878 NR 83 TC 76 Z9 76 U1 1 U2 8 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 SEP PY 2002 VL 37 IS 9 BP 1233 EP 1244 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 598FU UT WOS:000178265900008 ER PT J AU Prohl, H Adams, RMM Mueller, U Rand, S Ryan, MJ AF Prohl, H Adams, RMM Mueller, U Rand, S Ryan, MJ TI Polymerase chain reaction primers for polymorphic microsatellite loci from the tungara frog Physalaemus pustulosus SO MOLECULAR ECOLOGY NOTES LA English DT Article DE anuran; genotyping; microsatellite marker; PCR; Physalaernus pustulosus; primer ID ALLOZYME AB We developed eight PCR-primer pairs of polymorphic microsatellite loci for the tungara frog Physalaemus pustulosus. Genomic libraries were enriched for one of four microsatellite repeat sequences (CA(n), GA(n), ATG(n) and TAGA(n)). Following characterization of microsatellite loci by sequencing, primers were designed and PCR conditions optimized. Microsatellite PCR-amplification was tested in 37 frogs from 8 populations in Costa Rica and Panama. Primer sequences, PCR conditions, allelelic diversities and observed as well as expected heterozygosities in the screened populations are described. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Prohl, H (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. RI Adams, Rachelle/J-8846-2013 OI Adams, Rachelle/0000-0002-0918-9861 NR 9 TC 11 Z9 11 U1 1 U2 5 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD SEP PY 2002 VL 2 IS 3 BP 341 EP 343 DI 10.1046/j.1471-8286.2002.00240.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 592YK UT WOS:000177964300047 ER PT J AU Metchev, SA Grindlay, JE AF Metchev, SA Grindlay, JE TI A two-dimensional Kolmogorov-Smirnov test for crowded field source detection: ROSAT sources in NGC 6397 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; methods : statistical; globular clusters : individual : NGC 6397; X-rays : stars ID X-RAY SOURCES; GLOBULAR-CLUSTERS; NGC-6397; DISCOVERY; ASTRONOMY; MULTIPLE; CORE AB We present a two-dimensional version of the classical one-dimensional Kolmogorov-Smirnov (KS) test, extending an earlier idea due to Peacock and an implementation proposed by Fasano and Franceschini. The two-dimensional KS test is used to optimize the goodness of fit in an iterative source-detection scheme for astronomical images. The method is applied to a ROSAT/HRI X-ray image of the post-core-collapse globular cluster NGC 6397 to determine the most probable source distribution in the cluster core. Comparisons to other widely used source-detection methods, and to a Chandra image of the same field, show that our iteration scheme is superior in measuring statistics-limited sources in severely crowded fields. C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Metchev, SA (reprint author), CALTECH, Dept Astron, Pasadena, CA 91125 USA. NR 30 TC 15 Z9 15 U1 0 U2 3 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 SEP PY 2002 VL 335 IS 1 BP 73 EP 83 DI 10.1046/j.1365-8711.2002.05595.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 589ZB UT WOS:000177790700016 ER PT J AU Elizondo, MSG Enriquez, ILL Wagner, WL AF Elizondo, MSG Enriquez, ILL Wagner, WL TI Megacorax gracielanus (Onagraceae), a new genus and species from Durango, Mexico SO NOVON LA English DT Article DE Megacorax; Mexico; Onagraceae AB Megacorax gracielanus, a distinctive new genus and species from the Sierra de Coneto in central Durango, Mexico, is described and illustrated. Its distinctive characters include: leaves linear, petals presented to one side of the flower, and capsule wall thin and distended by the seeds. It appears to be most closely related to Lopezia Cavanilles based on possession of 4-merous flowers, deciduous sepals, a capitate stigma, stipules, and a tendency toward the structural zygomorphy in the flowers found in Lopezia. In addition, the capsules of Megacorax gracielanus are very similar in, shape and structure to the capsules of certain species of Lopezia. Because Megacorax has distinctive morphological characters and does not have the unique synapomorphies of Lopezia (2 fertile stamens or 1 fertile stamen and 1 staminode, and petals unequal), it is here described as a related genus. C1 Inst Politecn Nacl, CIIDIR, Durango 34000, Dgo, Mexico. Smithsonian Inst, US Natl Herbarium, Dept Systemat Biol Bot, Washington, DC 20013 USA. RP Elizondo, MSG (reprint author), Inst Politecn Nacl, CIIDIR, Apdo Postal 738, Durango 34000, Dgo, Mexico. NR 15 TC 5 Z9 5 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD FAL PY 2002 VL 12 IS 3 BP 360 EP 365 DI 10.2307/3393079 PG 6 WC Plant Sciences SC Plant Sciences GA 600ZM UT WOS:000178421700009 ER PT J AU Roa, AR Skog, LE AF Roa, AR Skog, LE TI Novae Gesneriaceae Neotropicarum X: A new species of Achimenes from Mexico SO NOVON LA English DT Article DE Achimenes; Gesnerjaceae; Mexico AB A new species of Achimenes Persoon, A. hintoniana, is described from western Mexico and distinguished from the closely related A. mexicana by the pilose indumentum of the stem, leaves, and pedicels, the linear-lanceolate calyx lobes, and the slightly saccate purple or rarely white corolla. C1 Univ Nacl Autonoma Mexico, Fac Ciencias, Herbario Nacl Mexico, Mexico City 04510, DF, Mexico. Smithsonian Inst, US Natl Herbarium, Washington, DC 20013 USA. RP Roa, AR (reprint author), Univ Nacl Autonoma Mexico, Fac Ciencias, Herbario Nacl Mexico, Mexico City 04510, DF, Mexico. NR 1 TC 1 Z9 2 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD FAL PY 2002 VL 12 IS 3 BP 382 EP 384 DI 10.2307/3393084 PG 3 WC Plant Sciences SC Plant Sciences GA 600ZM UT WOS:000178421700014 ER PT J AU Robinson, H AF Robinson, H TI Additions to Neocuatrecasia (Eupatorieae : Asteraceae) SO NOVON LA English DT Article DE Asteraceae; Bolivia; Eupatorieae; Neocuatrecasia; Peru AB Neocuatrecasia sandiensis H. Robinson and N. yungasensis H. Robinson from high elevations in Peru and Bolivia and N. tysonii H. Robinson from lower elevations in Bolivia are described as new. A key is furnished to the 12 species of the as yet inadequately collected genus. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Robinson, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC-166,Box 37012, Washington, DC 20013 USA. NR 6 TC 1 Z9 1 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD FAL PY 2002 VL 12 IS 3 BP 388 EP 392 DI 10.2307/3393086 PG 5 WC Plant Sciences SC Plant Sciences GA 600ZM UT WOS:000178421700016 ER PT J AU Robinson, H AF Robinson, H TI Three new species of Piptocarpha (Asteraceae : Vernonieae) from Ecuador and Peru SO NOVON LA English DT Article DE Asteraceae; Ecuador; Peru; Piptocarpha; Vernonieae AB Piptocarpha geraldsmithii H. Robinson, P. klugii G. Lom. Smith ex H. Robinson, and P vasquezii H. Robinson are described as new from northern Peru and southern Ecuador. The first relates to an otherwise strictly Guyana Highland group of species, and the third has terminal panicles with uniquely formed urn-shaped heads. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Robinson, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC-166,Box 37012, Washington, DC 20013 USA. NR 6 TC 2 Z9 2 U1 0 U2 1 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD FAL PY 2002 VL 12 IS 3 BP 393 EP 398 DI 10.2307/3393087 PG 6 WC Plant Sciences SC Plant Sciences GA 600ZM UT WOS:000178421700017 ER PT J AU Coley, PD Massa, M Lovelock, CE Winter, K AF Coley, PD Massa, M Lovelock, CE Winter, K TI Effects of elevated CO2 on foliar chemistry of saplings of nine species of tropical tree SO OECOLOGIA LA English DT Article DE phenolic compounds; elevated CO2; tropical trees; fertilization; Panama ID CARBON-NUTRIENT BALANCE; INSECT HERBIVORE INTERACTIONS; ATMOSPHERIC CO2; DECIDUOUS TREES; SECONDARY METABOLISM; PHENOLIC-COMPOUNDS; NO3 AVAILABILITY; LEAF QUALITY; PERFORMANCE; RESPONSES AB This study examined the effects of elevated CO2 on secondary metabolites for saplings of tropical trees. In the first experiment, nine species of trees were grown in the ground in open-top chambers in central Panama at ambient and elevated CO2 (about twice ambient). On average, leaf phenolic contents were 48% higher under elevated CO2. Biomass accumulation was not affected by CO2, but starch, total non-structural carbohydrates and C/N ratios all increased. In a second experiment with Ficus, an early successional species, and Virola, a late successional species, treatments were enriched for both CO2 and nutrients. For both species, nutrient fertilization increased plant growth and decreased leaf carbohydrates, C/N ratios and phenolic contents, as predicted by the carbon/nutrient balance hypothesis. Changes in leaf C/N levels were correlated with changes in phenolic contents for Virola (r=0.95, P<0.05), but not for Ficus. Thus, elevated CO2 particularly under conditions of low soil fertility, significantly increased phenolic content as well as the C/N ratio of leaves. The magnitude of the changes is sufficient to negatively affect herbivore growth, survival and fecundity, which should have impacts on plant/herbivore interactions. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Coley, PD (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 49 TC 38 Z9 47 U1 3 U2 25 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD SEP PY 2002 VL 133 IS 1 BP 62 EP 69 DI 10.1007/s00442-002-1005-6 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 597MA UT WOS:000178224300009 PM 24599370 ER PT J AU O'Dea, A Jackson, JBC AF O'Dea, A Jackson, JBC TI Bryozoan growth mirrors contrasting seasonal regimes across the Isthmus of Panama SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Cupuladriidae; growth; zooid; seasonality; tropical America ID PHENOTYPIC VARIATION; ZOOID SIZE; TEMPERATURE; COLONY; ENVIRONMENTS; OCEANOGRAPHY; ECTOTHERMS; HISTORY; SEA AB Two highly environmentally contrasting localities on either side of the Isthmus of Panama were chosen to investigate the response of zooid size to differing seasonal regimes within colonies of cupuladriid bryozoans. The Bocas del Toro region in the southern Caribbean experiences a very low mean annual range of temperature (MART) while, as a result of seasonal upwelling, the Gulf of Panama in the eastern Pacific experiences a high MART. Profiles of zooid size, from ancestrula to colony margins, were made on colonies from both localities. Results reveal that in colonies from the Gulf of Panama zooid size varies cyclically, while in colonies from the Bocas del Toro region no strong trends are observed, hence paralleling the respective seasonal temperature regimes. These data support previous evidence that zooid size varies inversely with temperature. We propose that given good taxonomic understanding, profiling zooid size in this way could provide important information on aspects of life histories in both fossil and Recent cupuladriids. We were also able to show that the amount of variation in zooid size within cupuladriid colonies correlates well with the MART which the colony experiences. This approach may be used to provide data on absolute MARTs over geological time by analysing zooid sizes in fossil cupuladriids. The abundance of cupuladriids in the Neogene of Central America suggests that this technique could provide important corroborative data on regional environmental changes associated with the closure of the Central American Isthmus. (C) 2002 Published by Elsevier Science B.V. C1 Scripps Inst Oceanog, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Panama. RP O'Dea, A (reprint author), 14 Ninetree Hill, Bristol BS1 3SQ, Avon, England. RI O'Dea, Aaron/D-4114-2011 NR 61 TC 39 Z9 43 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD SEP 1 PY 2002 VL 185 IS 1-2 BP 77 EP 94 AR PII S0031-0182(02)00278-X DI 10.1016/S0031-0182(02)00278-X PG 18 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 593YC UT WOS:000178021200005 ER PT J AU Kooistra, WHCF AF Kooistra, WHCF TI Molecular, phylogenies of Udoteaceae (Bryopsidales, Chlorophyta) reveal nonmonophyly for Udotea, Penicillus and Chlorodesmis SO PHYCOLOGIA LA English DT Article ID GREEN-ALGAE; CORAL-REEFS; MORPHOLOGICAL DEFENSES; TEMPORAL PATTERNS; SPECIES TREES; NUCLEAR RDNA; GENE TREES; HERBIVORY; HALIMEDA; EVOLUTION AB Generic delineation within and among the udoteacean genera Udotea, Penicillus, Rhipocephalus and Chlorodesmis has remained provisional because of conflicting evidence from different sets of traits, especially between reproductive structures and vegetative morphology. The ribosomal DNA phylogeny presented here contradicts the classical generic concepts within the Udoteaceae by revealing traditional genera to be polyphyletic. Based on this study, it was reported that the brush of Penicillus is essentially an uncorticated Udotea blade in which siphons have lost adherence. In fact, this Penicillus morphology arises twice independently. Similarly, the simple uniaxial thallus of Chlorodesmis has evolved through secondary reduction or neoteny. Siphon anatomy of vegetative thalli does not delineate natural groups perfectly. However, the shape of reproductive structures and the size of macrogametes appear to circumscribe natural taxa well. Overall sequence divergence within Udotea and its allied species in Chlorodesmis, Penicillus and Rhipocephalus is low and indicates relatively young and rapidly diversifying lineages. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Kooistra, WHCF (reprint author), Staz Zool Anton Dohrn, Villa Comunale, I-80121 Naples, Italy. EM kooistra@alpha.szn.it OI Kooistra, Wiebe/0000-0002-8641-9739 NR 74 TC 28 Z9 28 U1 0 U2 6 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD SEP PY 2002 VL 41 IS 5 BP 453 EP 462 DI 10.2216/i0031-8884-41-5-453.1 PG 10 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 611ZE UT WOS:000179047600002 ER PT J AU Krems, RV Zgid, D Chalasinski, G Klos, J Dalgarno, A AF Krems, RV Zgid, D Chalasinski, G Klos, J Dalgarno, A TI Possibility of buffer-gas cooling of paramagnetic carbon to ultracold temperatures SO PHYSICAL REVIEW A LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; COUPLED-CLUSTER; INTRAMULTIPLET TRANSITIONS; ATOMIC-COLLISIONS; WAVE-FUNCTIONS; STATES; HE; RELAXATION AB We demonstrate that the rate constant for the collisional relaxation of C(P-3(1)) in a buffer gas of He vanishes as the temperature decreases below 1 K. This suggests that the buffer-gas loading technique can be used for trapping excited paramagnetic C(P-3(1)) atoms at ultracold temperatures. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Warsaw Univ, Fac Chem, PL-03093 Warsaw, Poland. Univ Nijmegen, NSRIM, Inst Theoret Chem, NL-6525 ED Nijmegen, Netherlands. Oakland Univ, Dept Chem, Rochester, MI 48309 USA. RP Krems, RV (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. RI Klos, Jacek/A-6457-2008 OI Klos, Jacek/0000-0002-7407-303X NR 20 TC 4 Z9 4 U1 0 U2 1 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 SEP PY 2002 VL 66 IS 3 AR 030702 DI 10.1103/PhysRevA.66.030702 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 600GP UT WOS:000178382500004 ER PT J AU Stoner, RE Walsworth, RL AF Stoner, RE Walsworth, RL TI Measurement of the Ne-21 Zeeman frequency shift due to Rb-Ne-21 collisions SO PHYSICAL REVIEW A LA English DT Article ID NOBLE-GAS MASER; HYPERPOLARIZED HE-3 GAS; ELECTRIC-DIPOLE MOMENT; SPIN-EXCHANGE; DIFFUSION MEASUREMENTS; XE-129; LORENTZ; POLARIZATION; VIOLATION; SEARCH AB Using a Ne-21-He-3 Zeeman maser, we compared the frequency shift of the Ne-21 nuclear Zeeman resonance induced by polarized Rb vapor to the shift induced in the He-3 nuclear Zeeman resonance. The He-3-Rb shift has recently been measured with high precision [M.V. Romalis and G.D. Cates, Phys. Rev. A 58, 3004 (1998)], permitting the conversion of our differential measurement to an absolute value for the Ne-21-Rb shift. We report a value of kappa(21)=32.0+/-2.9 for the Rb-Ne-21 contact shift enhancement factor at a temperature of approximately 128(degrees)C. We also propose high-precision differential contact shift measurements, the absolute accuracy of which could be limited by the error in the He-3 contact shift. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stoner, RE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Stoner, Richard/0000-0001-7949-6747 NR 38 TC 10 Z9 10 U1 0 U2 1 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 SEP PY 2002 VL 66 IS 3 AR 032704 DI 10.1103/PhysRevA.66.032704 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 600GP UT WOS:000178382500063 ER PT J AU Pierce, S Winter, K Griffiths, H AF Pierce, S Winter, K Griffiths, H TI The role of CAM in high rainfall cloud forests: an in situ comparison of photosynthetic pathways in Bromeliaceae SO PLANT CELL AND ENVIRONMENT LA English DT Article DE Aechmea; Werauhia; bromeliad; Crassulacean acid metabolism; epiphyte; montane forest ID CARBON; ECOPHYSIOLOGY; NITROGEN; EPIPHYTE AB Crassulacean acid metabolism (CAM), an advanced photosynthetic pathway conferring water conservation to plants in arid habitats, has enigmatically been reported in some species restricted to extremely wet tropical forests. Of these, epiphytic Bromeliaceae may possess absorbent foliar trichomes that hinder gas-exchange when wetted, imposing further limitations on carbon dioxide (CO2) uptake. The hypothesis that the metabolic plasticity inherent to CAM confers an ecological advantage over conventional C-3 plants, when constant rainfall and mist might inhibit gas-exchange was investigated. Gas-exchange, fluorometry and organic acid and mineral nutrient contents were compared for the bromeliads Aechmea dactylina (CAM) and Werauhia capitata (C-3 ) in situ at the Cerro Jefe cloud forest, Panama (annual rainfall > 4 m). Daily carbon gain and photosynthetic nutrient use efficiencies were consistently higher for A. dactylina , due to a greater CO2 uptake period, recycling of CO2 from respiration and a dynamic response of CO2 uptake to wetting of leaf surfaces. During the dry season CAM also had water conserving and photoprotective roles. A paucity of CAM species at Cerro Jefe suggests a recent radiation of this photosynthetic pathway into the wet cloud forest, with CAM extending diversity in form and function for epiphytes. C1 Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. Smithsonian Trop Res Inst, Panama City, Panama. RP Pierce, S (reprint author), Univ Sheffield, Dept Anim & Plant Sci, Alfred Denny Bldg,Western Bank, Sheffield S10 2TN, S Yorkshire, England. OI Pierce, Simon/0000-0003-1182-987X NR 39 TC 29 Z9 35 U1 1 U2 13 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD SEP PY 2002 VL 25 IS 9 BP 1181 EP 1189 DI 10.1046/j.1365-3040.2002.00900.x PG 9 WC Plant Sciences SC Plant Sciences GA 584KN UT WOS:000177465900009 ER PT J AU Post, JE Heaney, PJ Hanson, J AF Post, JE Heaney, PJ Hanson, J TI Rietveld refinement of a triclinic structure for synthetic Na-birnessite using synchrotron powder diffraction data SO POWDER DIFFRACTION LA English DT Article DE birnessite; synchrotron; Rietveld; manganese oxide ID MANGANESE-OXIDE; HEXAGONAL BIRNESSITE; RICH BIRNESSITE; TRANSFORMATION; SPECTROSCOPY; CONSTRAINTS; MINERALOGY; MECHANISM; EXCHANGE; VARNISH AB Rietveld refinement using synchrotron powder X-ray diffraction data revealed that the crystal structure of synthetic Na-birnessite is triclinic (C (1) over bar), not monoclinic as was previously reported. The Mn-O octahedra have elongated axial bonds, consistent with Jahn-Teller distortion resulting from partial occupancy by Mn3+. Mean Mn-O distances indicate that Mn sites are similar to2/3 Mn4+ and similar to1/3 Mn3+. The interlayer Na cations and H2O molecules occupy a split site that shows evidence of considerable disorder. (C) 2002 International Centre for Diffraction Data. 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. RI Hanson, jonathan/E-3517-2010 NR 28 TC 33 Z9 33 U1 1 U2 19 PU J C P D S-INT CENTRE DIFFRACTION DATA PI NEWTOWN SQ PA 12 CAMPUS BLVD, NEWTOWN SQ, PA 19073-3273 USA SN 0885-7156 EI 1945-7413 J9 POWDER DIFFR JI Powder Diffr. PD SEP PY 2002 VL 17 IS 3 BP 218 EP 221 DI 10.1154/1.1498279 PG 4 WC Materials Science, Characterization & Testing SC Materials Science GA 592GU UT WOS:000177929200009 ER PT J AU Bakos, GA Lazar, J Papp, I Sari, P Green, EM AF Bakos, GA Lazar, J Papp, I Sari, P Green, EM TI System description and first light curves of the Hungarian Automated Telescope, an autonomous observatory for variability search SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ALL-SKY; VARIABLE-STARS; PHOTOMETRY; CEPHEID; CATALOG; FIELDS AB Having been operational at Kitt Peak for more than a year, the prototype (HAT-1) of the Hungarian Automated Telescope (HAT) has been used for an all-sky variability search of the northern hemisphere. This small autonomous observatory is recording the brightness of stars in the range of mag with a telephoto I-c approximate to 6-13 lens and its 9degrees x 9degrees field of view, yielding a data rate of similar to10(-6) photometric measurements per night. We give brief hardware and software descriptions of the system, controlled by a single PC running RealTime Linux OS. We provide an overview of site-specific details and quantify the astrometric and photometric capabilities of HAT. As a demonstration of system performance, we give a sample of 60 short-period variables in a single selected field, all bright, with I<13 mag, where only 14 were known before. Depending on the observing strategy, a search for extrasolar planet transits is also a feasible observing program. We conclude with a short discussion on future directions. Further information can be found at the HAT Web page.(3) C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hungarian Astron Assoc, H-1461 Budapest, Hungary. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Bakos, GA (reprint author), Konkoly Observ Budapest, POB 67, H-1525 Budapest, Hungary. NR 50 TC 93 Z9 94 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 SEP PY 2002 VL 114 IS 799 BP 974 EP 987 DI 10.1086/342382 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 585PK UT WOS:000177533600003 ER PT J AU Chave, J Leigh, EG AF Chave, J Leigh, EG TI A spatially explicit neutral model of beta-diversity in tropical forests SO THEORETICAL POPULATION BIOLOGY LA English DT Article DE data diversity; long-distance dispersal; neutral model; tropical forest ID TREE SPECIES-DIVERSITY; STEPPING STONE MODEL; NEOTROPICAL FOREST; VOTER MODEL; FLORISTIC COMPOSITION; GENETIC-VARIABILITY; SEED DISPERSAL; RAIN-FORESTS; PATTERNS; POPULATION AB To represent species turnover in tropical rain forest, we use a neutral model where a tree's fate is not affected by what species it belongs to, seeds disperse a limited distance from their parents, and speciation is in equilibrium with random extinction. We calculate the similarity function, the probability F(r) that two trees separated by a distance r belong to the same species, assuming that the dispersal kernel P(r), the distribution of seeds about their parents and the prospects of mortality and reproduction, are the same for all trees regardless of their species. If P(r) is radially symmetric Gaussian with mean-square dispersal distance a, F(r) can be expressed in closed form. If P(r) is a radially symmetric Cauchy distribution, then, in two-dimensional space, F(r) is proportional to 1/r for large r. Analytical results are compared with individual-based simulations, and the relevance to field observations is discussed. (C) 2002 Elsevier Science (USA). C1 Lab Ecol Terr, CNRS, UMR 5552, F-31029 Toulouse 4, France. Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Lab Ecol Terr, CNRS, UMR 5552, 13 Ave Colonel Roche, F-31029 Toulouse 4, France. EM chave@cict.fr NR 90 TC 154 Z9 159 U1 4 U2 52 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0040-5809 EI 1096-0325 J9 THEOR POPUL BIOL JI Theor. Popul. Biol. PD SEP PY 2002 VL 62 IS 2 BP 153 EP 168 DI 10.1006/tpbi.2002.1597 PG 16 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 589CD UT WOS:000177739700005 PM 12167354 ER PT J AU Cordero, RA Nilsen, ET AF Cordero, RA Nilsen, ET TI Effects of summer drought and winter freezing on stem hydraulic conductivity of Rhododendron species from contrasting climates SO TREE PHYSIOLOGY LA English DT Article DE Appalachians; cavitation; evergreen shrubs; freezing temperature; Oregon Cascades; xylem diameter ID XYLEM EMBOLISM; WATER-STRESS; ACER-SACCHARUM; SOUTHERN APPALACHIANS; CHAPARRAL SHRUBS; THAW CYCLES; CAVITATION; VULNERABILITY; ARCHITECTURE; DYSFUNCTION AB We studied the limits to maximum water transport in three diffuse-porous evergreen shrubs exposed to frequent winter freeze-thaw events (Rhododendron maximum L. and R. catawbiense Michaux from the Appalachian Mountains) and to a severe summer drought (R. macrophyllum G. Don. from the Oregon Cascades). Percent loss of hydraulic conductivity (PLC), vulnerability curves to xylem embolism and freezing point temperatures of stems were measured over 2 years. Controlled freeze-thaw experiments were also conducted to determine the effect of thaw rate on PLC. During both years, native PLC was significantly higher in winter than in summer for R. macrophyllum. Seasonal changes in PLC were variable in both R. catawbiense and R. maximum. Only R. maximum plants growing in gaps or clearings showed higher PLC than understory plants. A rapid (2-4 day) natural recovery of high native PLC during the winter was observed in both R. maximum and R. macrophyllum. Compared with the bench-dehydration method, vulnerability curves based on the air-injection method consistently had less negative slopes and greater variation. Fifty percent PLC (PLC50) obtained from vulnerability curves based on the dehydration method occurred at -1.75, -2.42 and -2.96 MPa for R. catawbiense, R. maximum and R. macrophyllum, respectively. Among the study species, R. macrophyllum, which commonly experiences a summer drought, had the most negative water potential at PLC50. In all species, stem freezing point temperatures were not consistently lower in winter than in summer. A single fast freeze thaw event significantly increased PLC, and R. catawbiense had the highest PLC in response to freezing treatments. Recovery to control PLC values occurred if a low positive hydraulic pressure was maintained during thawing. Rhododendron macrophyllum plants, which commonly experience few freeze thaw events, had large stem diameters, whereas plants of R. catawbiense, which had small stem diameters, suffered high embolism in response to a single freeze-thaw event. Both drought-induced and winter-induced embolism caused a significant reduction in hydraulic conductivity in all species during periods when drought or freeze-thaw events occurred in their native habitats. However, rapid recovery of PLC following freezing or drought maintained the species above their relatively low margins of safety for complete xylem dysfunction. C1 Virginia Polytech Inst & State Univ, Dept Biol, Blacksburg, VA 24061 USA. RP Cordero, RA (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. RI Cordero Solorzano, Roberto A./H-8273-2016 OI Cordero Solorzano, Roberto A./0000-0001-7270-104X NR 41 TC 19 Z9 20 U1 1 U2 28 PU HERON PUBLISHING PI VICTORIA PA 202, 3994 SHELBOURNE ST, VICTORIA, BC V8N 3E2, CANADA SN 0829-318X J9 TREE PHYSIOL JI Tree Physiol. PD SEP PY 2002 VL 22 IS 13 BP 919 EP 928 PG 10 WC Forestry SC Forestry GA 609RG UT WOS:000178917900003 PM 12204848 ER PT J AU Whigham, D Pittek, M Hofmockel, KH Jordan, T Pepin, AL AF Whigham, D Pittek, M Hofmockel, KH Jordan, T Pepin, AL TI Biomass and nutrient dynamics in restored wetlands on the outer coastal plain of Maryland, USA SO WETLANDS LA English DT Article DE restoration; Maryland; depressional wetlands; aboveground biomass; nutrient concentrations; nutrient standing stock; agricultural landscape ID SOUTH-CAROLINA; SELF-DESIGN; VEGETATION; PLANT; MARSH; RESTORATION; MATTER; WATER; SOIL AB A three-year study of aboveground biomass and nutrient dynamics in twelve restored depressional wetlands of different ages demonstrated significant annual variability among sites. Annual variations appeared to be primarily due to differences in hydrologic conditions over the three years of the study. Differences among wetlands were not related to time since restoration. When data for all sites were combined, annual differences in biomass and most measurements of nutrients (concentrations and standing stocks) did not, however, differ significantly. These results suggest that differences that are measured at individual wetland sites may be less important at the landscape level. Biomass decreased from the outer temporary to inner submersed zone, and there were few differences among wetlands when the temporary, seasonal, and submersed zones were compared. Nutrient concentrations in the plant. biomass increased from the temporary zone to the submersed zone, resulting in few differences in nutrient standing crops across zones. Results from this study demonstrate that some measurements of restoration success (i.e., biomass production) should be used cautiously because they are likely to be highly variable among sites and across years and thus may be of limited use in post-restoration monitoring. Other ecosystem parameters (e.g., nutrient concentrations of biomass) are much more constant spatially and temporally, indicating that nutrient cycling processes in vegetation were established quickly following restoration. Nutrient characteristics of wetland vegetation thus may be a useful metric for evaluating restoration success or failure. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Whigham, D (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. OI Whigham, Dennis/0000-0003-1488-820X NR 42 TC 20 Z9 21 U1 2 U2 6 PU SOC WETLAND SCIENTISTS PI LAWRENCE PA 810 E TENTH ST, P O BOX 1897, LAWRENCE, KS 66044 USA SN 0277-5212 J9 WETLANDS JI Wetlands PD SEP PY 2002 VL 22 IS 3 BP 562 EP 574 DI 10.1672/0277-5212(2002)022[0562:BANDIR]2.0.CO;2 PG 13 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 604DP UT WOS:000178600900012 ER PT J AU Santini, F Tyler, JC AF Santini, F Tyler, JC TI Phylogeny and biogeography of the extant species of triplespine fishes (Triacanthidae, Tetraodontiformes) SO ZOOLOGICA SCRIPTA LA English DT Article AB A new phylogenetic hypothesis for the living species of triplespine fishes of the Indo-Western Pacific family Triacanthidae (Tetraodontiformes, Teleostei) is proposed. A data set of 55 morphological characters (34 osteological and 21 morphometric) was constructed. A cladistic analysis of the osteological data set yielded a single most-parsinionious tree. This cladogram does not support the monophyly of one of the four genera, Tripodichthys, but Bremer values for this analysis are low. The osteological data set was then combined with a data set of 21 metphometric characters that had previously been used to diagnose the four genera. The analysis of the combined data set produced the same phylogenetic hypothesis, but with greater nodal support. The biogeographical distribution of the living species is then interpreted with the use of this new phylogenetic information. C1 Univ Toronto, Dept Zool, Ramsay Wright Zool Labs, Toronto, ON M5S 3G5, Canada. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Santini, F (reprint author), Univ Toronto, Dept Zool, Ramsay Wright Zool Labs, 25 Harbord St, Toronto, ON M5S 3G5, Canada. EM fsantini@zoo.utoronto.ca; tyler.jim@nmnh.si.edu NR 33 TC 9 Z9 11 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0300-3256 EI 1463-6409 J9 ZOOL SCR JI Zool. Scr. PD SEP PY 2002 VL 31 IS 4 BP 321 EP 330 DI 10.1046/j.1463-6409.2002.00097.x PG 10 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 576WK UT WOS:000177029600001 ER PT J AU Chave, J Muller-Landau, HC Condit, R Pitman, N Terborgh, J Hubbell, SP Leigh, EG AF Chave, J Muller-Landau, HC Condit, R Pitman, N Terborgh, J Hubbell, SP Leigh, EG TI Beta-diversity in tropical forests - Response SO SCIENCE LA English DT Editorial Material C1 CNRS, Lab Ecol Terr, UMR 5552, F-31029 Toulouse, France. Princeton Univ, Dept Ecol & Evolut Biol, Princeton, NJ 08544 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Duke Univ, Ctr Trop Conservat, Durham, NC 27708 USA. Univ Georgia, Dept Bot, Athens, GA 30602 USA. RP Chave, J (reprint author), CNRS, Lab Ecol Terr, UMR 5552, 13 Ave Colonel Roche,BP 4072, F-31029 Toulouse, France. RI Pitman, Nigel/A-7681-2008 OI Pitman, Nigel/0000-0002-9211-2880 NR 4 TC 0 Z9 0 U1 1 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 AUG 30 PY 2002 VL 297 IS 5586 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 588JA UT WOS:000177697300002 ER PT J AU Duivenvoorden, JF Svenning, JC Wright, SJ AF Duivenvoorden, JF Svenning, JC Wright, SJ TI Beta-diversity in tropical forests - Response SO SCIENCE LA English DT Editorial Material C1 Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1090 GB Amsterdam, Netherlands. Univ Aarhus, Dept Systemat Bot, DK-8240 Risskov, Denmark. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Duivenvoorden, JF (reprint author), Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, Postbus 94062, NL-1090 GB Amsterdam, Netherlands. RI Svenning, Jens-Christian/C-8977-2012; Wright, Stuart/M-3311-2013 OI Svenning, Jens-Christian/0000-0002-3415-0862; Wright, Stuart/0000-0003-4260-5676 NR 4 TC 0 Z9 0 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 AUG 30 PY 2002 VL 297 IS 5586 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 588JA UT WOS:000177697300003 ER PT J AU Cote, R Kharchenko, V Lukin, MD AF Cote, R Kharchenko, V Lukin, MD TI Mesoscopic molecular ions in Bose-Einstein condensates SO PHYSICAL REVIEW LETTERS LA English DT Article ID FROZEN RYDBERG GAS; LIQUID-HELIUM; ATOMS; RECOMBINATION; SCATTERING; SUPERFLUIDITY; EXCITATIONS; COLLISIONS; RESONANCES; DYNAMICS AB We study the possible formation of large (mesoscopic) molecular ions in an ultracold degenerate bosonic gas doped with charged particles (ions). We show that the polarization potentials produced by the ionic impurities are capable of capturing hundreds of atoms into loosely bound states. We describe the spontaneous formation of these hollow molecular ions via phonon emission and suggest an optical technique for coherent stimulated transitions of condensate atoms into a specific bound state. These results open up new possibilities for manipulating tightly confined ensembles. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Cote, R (reprint author), Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06269 USA. NR 39 TC 75 Z9 75 U1 1 U2 16 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 AUG 26 PY 2002 VL 89 IS 9 AR 093001 DI 10.1103/PhysRevLett.89.093001 PG 4 WC Physics, Multidisciplinary SC Physics GA 585MR UT WOS:000177529000013 PM 12190393 ER PT J AU Vardi, A Moore, MG AF Vardi, A Moore, MG TI Directional "superradiant" collisions: Bosonic amplification of atom pairs emitted from an elongated Bose-Einstein condensate SO PHYSICAL REVIEW LETTERS LA English DT Article ID ENTANGLEMENT; SCATTERING; MOLECULES; STATES AB We study spontaneous directionality in the bosonic amplification of atom pairs emitted from an elongated Bose-Einstein condensate, an effect analogous to superradiant emission of atom-photon pairs. Using a simplified model, we make analytic predictions regarding directional effects for both atom-atom and atom-photon emission. These are confirmed by numerical mean-field simulations, demonstrating the feasibility of nearly perfect directional emission along the condensate axis. The dependence of the emission angle on the pump strength for atom-atom pairs is significantly different than for atom-photon pairs. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Vardi, A (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Vardi, Amichay/D-8189-2011 OI Vardi, Amichay/0000-0002-8992-2129 NR 17 TC 23 Z9 23 U1 0 U2 1 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 AUG 26 PY 2002 VL 89 IS 9 AR 090403 DI 10.1103/PhysRevLett.89.090403 PG 4 WC Physics, Multidisciplinary SC Physics GA 585MR UT WOS:000177529000003 PM 12190383 ER PT J AU Kohno, K Tosaki, T Matsushita, S Vila-Vilaro, B Shibatsuka, T Kawabe, R AF Kohno, K Tosaki, T Matsushita, S Vila-Vilaro, B Shibatsuka, T Kawabe, R TI Diffuse and gravitationally stable molecular gas in the post-starburst galaxy NGC 5195 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : individual (NGC 5195); galaxies : ISM; galaxies : starburst ID POSTSTARBURST GALACTIC NUCLEUS; BARRED SPIRAL GALAXIES; H-II REGIONS; STAR-FORMATION; CO EMISSION; PHYSICAL CONDITIONS; S0 GALAXIES; NGC-5195; DISK; M51 AB The Nobeyama Millimeter Array (NMA) has been used to make aperture synthesis CO(1 - 0) observations of the post-starburst galaxy NGC 5195. CO(1 - 0) and HCN(1 - 0) observations of NGC 5195 using the Nobeyama 45 m telescope are also presented. High-resolution (1."9 x 1."8 or 86 pc x 81 pc resolution at D = 9.3 Mpc) NMA maps show a strong concentration of CO emission toward the central a few x 100pc region of NGC 5195, despite the fact that the current massive star formation is suppressed there. The face-on gas surface density, Sigma(gas), within the r < 2" or 90pc region reaches 3.7 x 10(3) Mcircle dot pc(-2) if a Galactic N-H2/l(CO) conversion factor is applied. The extent of the central CO peak is about 5", or 230pc, and is elongated along the E-W direction with two-armed spiral-like structures, which are typical for barred disk galaxies. The HCN-to-CO integrated intensity ratio on the brightness temperature scale, R-HCN/CO, is about 0.02 within the central r < 400 pc region. This RHCN/CO is smaller than those in starburst regions by a factor of 5-15. These molecular-gas properties would explain why NGC 5195 is in a post-starburst phase; most of the dense molecular cores (i.e., the very sites of massive star formation) have been consumed away by a past starburst event, and therefore a burst of massive star formation can no longer last, although a large amount of low density gas still exists. We find a steep rise of the rotation velocity toward the center of NGC 5195. As a consequence, the critical gas surface density for a local gravitational instability of the gas disk becomes very high (Sigma(crit) similar to 6.9 x 10(3) M(circle dot)pc(-2)), Suggesting that the molecular gas in the central region of NGC 5195 is gravitationally stable, in contrast to that of starburst galaxies. We propose that dense molecular gas can not be formed from remaining diffuse molecular gas because the molecular gas in the center of NGC 5195 is too stable to form dense cores via gravitational instabilities of diffuse molecular gas. The deduced very high threshold density seems to be due to a high mass concentration in NGC 5195. The known trends on the occurrence and luminosity of nuclear star formation in early-type galaxies can be understood naturally if the high threshold density is characteristic for early-type galaxies. C1 Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. Gunma Astron Observ, Gunma 3770702, Japan. Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. RP Univ Tokyo, Inst Astron, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan. EM kkohno@ioa.s.u-tokyo.ac.jp; tomoka@astron.pref.gunma.jp; smatsu@sma.hawaii.edu; bvila@as.arizona.edu; shiba@nro.nao.ac.jp; kawabe@nro.nao.ac.jp NR 84 TC 23 Z9 23 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 AUG 25 PY 2002 VL 54 IS 4 BP 541 EP 553 DI 10.1093/pasj/54.4.541 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590UT UT WOS:000177842700010 ER PT J AU White, M van Waerbeke, L Mackey, J AF White, M van Waerbeke, L Mackey, J TI Completeness in weak-lensing searches for clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; gravitational lensing; large-scale structure of universe ID LARGE-SCALE STRUCTURE; DARK-MATTER CONCENTRATIONS; GALAXY-CLUSTER; POWER-SPECTRUM; COSMIC SHEAR; CONSTRAINTS AB Using mock observations of numerical simulations, we investigate the completeness and efficiency of searches for galaxy clusters in weak-lensing surveys. While it is possible to search for high-mass objects directly as density enhancements using weak lensing, we find that line-of-sight projection effects can be quite serious. For the search methods that we consider, to obtain high completeness requires acceptance of a very high false positive rate. The false positive rate can be reduced only by significantly degrading the completeness. Both completeness and efficiency are dependent on the filter used in the search and the desired mass threshold, emphasizing that a measurement of the three-dimensional mass function from gravitational lensing is affected by a number of biases that mix cosmological and observational issues. C1 Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Inst Astrophys Paris, F-75014 Paris, France. Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM mwhite@astron.berkeley.edu RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 NR 35 TC 82 Z9 83 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2002 VL 575 IS 2 BP 640 EP 649 DI 10.1086/341351 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583VF UT WOS:000177430600004 ER PT J AU Arce, HG Goodman, AA AF Arce, HG Goodman, AA TI The great PV Cephei outflow: A case study in outflow-cloud interaction SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : Herbig-Haro objects; ISM : individual (HH 315, PV Cephei); ISM : jets and outflows; stars : formation ID MAIN-SEQUENCE OBJECTS; MOLECULAR CLOUDS; PROTOSTELLAR OUTFLOWS; CO OUTFLOWS; YOUNG STARS; EVOLUTION; DRIVEN AB We present a set of detailed molecular-line maps of the region associated with the giant Herbig-Haro flow HH 315 from the young star PV Cephei, aimed at studying the outflow-cloud interaction. Our study clearly shows that the HH 315 flow is affecting the kinematics of its surrounding medium and has been able to redistribute considerable amounts of the surrounding medium-density (similar to10(3) cm(-3)) gas in its star-forming core as well at parsec-scale distances from the source. The single-dish observations include a map of the outflow in the (CO)-C-12 (2-1) line, with a beam size of 27", and more extended maps of the outflow region in the (CO)-C-12 (1-0) and (CO)-C-13 (1-0) lines, with 45" and 47" beam sizes, respectively. A companion paper published in this issue presents higher resolution (IRAM 30 m) observations and discusses their implications. The giant molecular outflow HH 315 is a highly asymmetric bipolar flow with a projected linear extent of about 2 pc. Our results indicate that the two outflow lobes are each interacting with the ambient medium in different ways. The southern (redshifted) lobe, with a mass of 1.8 M-., interacts with a dense ambient medium, very close to the young stellar outflow source, and its kinetic energy is comparable to both the turbulent and gravitational binding energy of its host cloud (of order 10(44) ergs). In addition, we find evidence that the southern lobe is responsible for the creation of a cavity in the (CO)-C-13 emission. In contrast, the northern ( mainly blueshifted) outflow lobe, with a total mass of 4.8 M-., extends farther from PV Cep and interacts with ambient gas much less dense than the southern lobe. There is very little (CO)-C-13 emission north of the outflow source, and the only prominent (CO)-C-13 emission is a shell-like structure coincident with the outer edge of the northern lobe, about 1.2 pc northwest of PV Cep. It appears that the northern lobe of the HH315 outflow has been able to push aside a substantial fraction of the gas in the area, piling it in a dense shell-like structure at its edges. In addition, we find that about 50% of the gas in the region of the northern lobe has been put into motion by the outflow and that the northern outflow lobe is responsible for a velocity gradient in the ambient gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Arce, HG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 35 TC 31 Z9 32 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2002 VL 575 IS 2 BP 911 EP 927 DI 10.1086/341427 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583VF UT WOS:000177430600025 ER PT J AU Arce, HG Goodman, AA AF Arce, HG Goodman, AA TI Bow shocks, wiggling jets, and wide-angle winds: A high-resolution study of the entrainment mechanism of the PV Cephei molecular (CO) outflow SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : Herbig-Haro objects; ISM : individual (HH 315, PV Cephei); ISM : jets and outflows; stars : formation ID HERBIG-HARO FLOWS; NUMERICAL SIMULATIONS; PROTOSTELLAR JETS; BIPOLAR OUTFLOWS; STELLAR JETS; HYDRODYNAMIC SIMULATIONS; PROMPT ENTRAINMENT; MIXING LAYERS; YOUNG STARS; HH-111 JET AB We present a new set of high-resolution molecular-line maps of the gas immediately surrounding various Herbig-Haro (HH) knots of the giant HH flow HH 315 from the young star PV Cephei. The observations, aimed at studying the entrainment mechanism of the 2.6 pc long HH 315 flow, include IRAM 30 m maps of the (CO)-C-12 (2-1), (CO)-C-12 (1-0), and (CO)-C-13 (1-0) lines, with beam sizes of 11", 21", and 22", respectively. We compare the morphology and the kinematics of the outflow gas, as well as the temperature and momentum distribution of the molecular outflow, with those predicted by different entrainment models. With our detailed study we are able to conclude that jet bow shock entrainment by an episodic stellar wind, with a time-varying axis, produces most of the high-velocity molecular outflow observed far from the source. In addition, near PV Cep we find evidence for a poorly collimated, wide-angle molecular outflow and a collimated, wiggling jet like molecular outflow. We propose that the poorly collimated component is entrained by a wide-angle wind and the collimated component is entrained by a variable jet with internal working surfaces. If this picture is true, then a stellar wind model that allows for the coexistence of a wide-angle component and a collimated (jetlike) stellar wind component is needed to explain the observed properties of the PV Cep outflow. The wiggling axis of the redshifted molecular outflow lobe indicates that the outflow ejection axis is changing over time. We find that the timescale of the axis variation shown by the molecular outflow lobe is about a factor of 10 less than that shown by the large-scale optical HH knots. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Arce, HG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 67 TC 30 Z9 31 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 AUG 20 PY 2002 VL 575 IS 2 BP 928 EP 949 DI 10.1086/341426 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583VF UT WOS:000177430600026 ER PT J AU Gerardy, CL Fesen, RA Nomoto, K Garnavich, PM Jha, S Challis, PM Kirshner, RP Hoflich, P Wheeler, JC AF Gerardy, CL Fesen, RA Nomoto, K Garnavich, PM Jha, S Challis, PM Kirshner, RP Hoflich, P Wheeler, JC TI Extraordinary late-time infrared emission of type IIn supernovae SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; infrared : stars; supernovae : individual (SN 1995N, SN 1997ab; SN1998S, SN 1999Z, SN 1999el) ID DUST GRAINS; SN-1987A; EJECTA; ECHO; CONTINUUM; RADIATION; SPECTRA; SN1998S; LINE; NOVA AB Near-infrared observations are presented for five Type IIn supernovae (SN 1995N, SN 1997ab, SN 1998S, SN 1999Z, and SN 1999el) that exhibit strong infrared excesses at late times (tgreater than or similar to100 days). H- and K-band emission from these objects is dominated by a continuum that rises toward longer wavelengths. The data are interpreted as thermal emission from dust, probably situated in a preexisting circumstellar nebula. The IR luminosities implied by single-temperature blackbody fits are quite large, greater than or similar to10(41)-10(42) ergs s(-1), and the emission evolves slowly, lasting for years after maximum light. For SN 1995N, the integrated energy release via IR dust emission was approximate to0.5-1 x 10(50) ergs. A number of dust heating scenarios are considered, the most likely being an infrared echo powered by X-ray and UV emissions from the shock interaction with a dense circumstellar medium. C1 Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Gerardy, CL (reprint author), Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. RI Nomoto, Ken'ichi/A-4393-2011 NR 55 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 AUG 20 PY 2002 VL 575 IS 2 BP 1007 EP 1017 DI 10.1086/341430 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583VF UT WOS:000177430600031 ER PT J AU Kaaret, P In't Zand, JJM Heise, J Tomsick, JA AF Kaaret, P In't Zand, JJM Heise, J Tomsick, JA TI Discovery of millisecond variability in the neutron star X-ray transient SAX J1750.8-2900 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; gravitation; relativity; stars : individual (SAX J1750.8-2900); stars : neutron; X-rays : stars ID OSCILLATIONS; EMISSION; BINARIES; SPECTRA; BURSTS; ASCA AB We report the discovery of millisecond oscillations in the X-ray emission from the X-ray transient SAX J1750.8-2900. Millisecond quasiperiodic oscillations were present in the persistent emission with frequencies ranging from 543 to 1017 Hz. Oscillations at a frequency of 600.75 Hz were present in the brightest X-ray burst observed. We derive an upper limit on the source distance of 6.3 +/- 0.7 kpc from this X-ray burst. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 36 Z9 36 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2002 VL 575 IS 2 BP 1018 EP 1024 DI 10.1086/341336 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583VF UT WOS:000177430600032 ER PT J AU Wood, BE Karovska, M Raymond, JC AF Wood, BE Karovska, M Raymond, JC TI Analysis of H-2 emission from Mira B in ultraviolet spectra from the Hubble Space Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; stars : individual (o Ceti); stars : winds, outflows; ultraviolet : stars ID MOLECULAR-HYDROGEN; INTERSTELLAR-MEDIUM; EVOLVED STARS; FINAL ARCHIVE; O-CETI; WIND; VARIABLES; LYMAN; CO; DISSOCIATION AB We analyze Lyalpha fluoresced H-2 lines observed in the UV spectrum of Mira B. We identify 13 different sequences fluoresced by 13 different H-2 transitions within the Lyalpha line. The observed H-2 line ratios within these sequences imply significant line opacity, so we use a Monte Carlo radiative transfer code to model the line ratios, correcting for opacity effects. We find that the observed line ratios can best be reproduced by assuming that the H-2 is fluoresced in a layer between the observer and Mira B with a temperature and column density of T = 3600 K and log N(H-2) = 17.3, respectively. The strengths of H-2 absorption features within the Lyalpha line are roughly consistent with this temperature and column. We use the total flux fluoresced within the 13 sequences to infer the Lyalpha profile seen by the H-2. In order to explain differences between the shape of this and the observed profile, we have to assume that the observed profile suffers additional interstellar (or circumstellar) H I Lyalpha absorption with a column density of about log N (H I) = 20.35. We also have to assume that the observed pro le is about a factor of 2.5 lower in flux than the pro le seen by the H-2, and a couple of possible explanations for this behavior are presented. Several lines of evidence lead us to tentatively attribute the fluoresced emission to H-2 that is heated in a photodissociation front within Mira A's wind a few AU from Mira B, although it is possible that interaction between the winds of Mira A and B may also play a role in heating the H-2. We estimate a Mira B mass-loss rate of (M) over dot = 5 x 10(-13) M-. yr(-1) and a terminal velocity of V-infinity = 250 km s(-1), based on wind absorption features in the Mg II h and k lines. We note, however, that the wind is variable and IUE Mg II spectra suggest significantly higher mass-loss rates during the IUE era. C1 Univ Colorado, JILA, Boulder, CO 80309 USA. NIST, Boulder, CO 80309 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Wood, BE (reprint author), Univ Colorado, JILA, Boulder, CO 80309 USA. NR 61 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 AUG 20 PY 2002 VL 575 IS 2 BP 1057 EP 1077 DI 10.1086/341478 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583VF UT WOS:000177430600037 ER PT J AU Hussain, GAJ van Ballegooijen, AA Jardine, M Collier Cameron, A AF Hussain, GAJ van Ballegooijen, AA Jardine, M Collier Cameron, A TI The coronal topology of the rapidly rotating K0 dwarf AB Doradus. I. Using surface magnetic field maps to model the structure of the stellar corona SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : coronae; stars : rotation ID ACTIVE STARS; POLAR SPOTS; DOPPLER AB We reanalyze spectropolarimetric data of AB Dor taken in 1996 December using a surface imaging code that can model the magnetic field of the star as a nonpotential current-carrying magnetic field. We find that a nonpotential field needs to be introduced in order to fit the data set at this epoch. This nonpotential component takes the form of a strong unidirectional azimuthal field of a similar strength to the radial field. This azimuthal field is concentrated around the boundary of the dark polar spot recovered at the surface of the star using Doppler imaging. As polarization signatures from the center of starspots are suppressed, it is unclear whether or not this nonpotential component genuinely represents electric current at the unspotted surface or whether it results from the preferred detection of horizontal field in starspot penumbrae. This model contains 20% more energy than the corresponding potential field model at the surface. This amount of free energy drops to under 1% about 1 R-* above the photosphere. We use these surface maps to model the coronal structure of the star. The mixed radial polarities at the pole in the surface maps support closed coronal loops in the high-latitude regions, indicating that a component of the X-ray emission may originate in this area. Assuming that the field remains closed out to 5 R-*, we find stable surfaces where prominences may form out to the observed distances using this coronal model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ghussain@cfa.harvard.edu; vanballe@cfa.harvard.edu; mmj@st-andrews.ac.uk; acc4@st-andrews.ac.uk NR 35 TC 50 Z9 50 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2002 VL 575 IS 2 BP 1078 EP 1086 DI 10.1086/341429 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583VF UT WOS:000177430600038 ER PT J AU Ciaravella, A Raymond, JC Li, J Reiser, P Gardner, LD Ko, YK Fineschi, S AF Ciaravella, A Raymond, JC Li, J Reiser, P Gardner, LD Ko, YK Fineschi, S TI Elemental abundances and post-coronal mass ejection current sheet in a very hot active region SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : abundances; Sun : activity; Sun : corona; Sun : coronal mass ejections (CMEs); Sun : UV radiation ID LINE INTENSITY RATIOS; X-RAY TELESCOPE; FE-XVII; SOLAR; SPECTROMETER; EMISSION; SOHO; DIAGNOSTICS; IONS; RECONNECTION AB A peculiar young active region was observed in 1998 March with the Ultraviolet Coronagraph Spectrometer ( UVCS) over the southwest limb. The spectra showed strong emission in the 974 line of fluorine-like iron, [Fe XVIII], which is brightest at an electron temperature of 10(6.8) K, and lines of Ne IX [Ca XIV], [Ca XV], Fe XVII [Ni xiv, and [Ni xv]. It is the only active region so far observed to show such high temperatures 0.5 R-. above the solar limb. We derive the emission measure and estimate elemental abundances. The active region produced a number of coronal mass ejections (CMEs). After one CME on March 23, a bright post-CME arcade was seen in EIT and Yohkoh/SXT images. Between the arcade and the CME core, UVCS detected a very narrow, very hot feature, most prominently in the [ Fe XVIII] line. This feature seems to be the reconnection current sheet predicted by flux rope models of CMEs. Its thickness, luminosity, and duration seem to be consistent with the expectations of the flux rope models for CME. The elemental abundances in the bright feature are enhanced by a factor of 2 compared to those in the surrounding active region, i.e., a first ionization potential enhancement of 7-8 compared to the usual factor of 3-4. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Palermo GS Vaiana, I-90134 Palermo, Italy. Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. Interferomet Inc, Chantilly, VA 20151 USA. Osserv Astron Torino, I-10125 Turin, Italy. RP Ciaravella, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 45 TC 103 Z9 107 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2002 VL 575 IS 2 BP 1116 EP 1130 DI 10.1086/341473 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583VF UT WOS:000177430600042 ER PT J AU Hussein, MS Pato, MP Wells, JC AF Hussein, MS Pato, MP Wells, JC TI Causal classical theory of radiation damping SO MODERN PHYSICS LETTERS A LA English DT Article DE self-interaction; electrodynamics ID LORENTZ-DIRAC EQUATION; COMPTON-SCATTERING AB It is shown how initial conditions can be appropriately defined for the integration of Lorentz-Dirac equations of motion. The integration is performed forward in time. The theory is applied to the case of the motion of an electron in an intense laser pulse, relevant to nonlinear Compton scattering. C1 Univ Sao Paulo, Inst Fis, BR-05315970 Sao Paulo, Brazil. Univ Calif Santa Barbara, Inst Theoret Phys, Santa Barbara, CA 93106 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Hussein, MS (reprint author), Univ Sao Paulo, Inst Fis, CP 66318, BR-05315970 Sao Paulo, Brazil. RI Wells, Jack/D-3675-2016 OI Wells, Jack/0000-0002-5083-3030 NR 14 TC 0 Z9 0 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA JOURNAL DEPT PO BOX 128 FARRER ROAD, SINGAPORE 912805, SINGAPORE SN 0217-7323 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD AUG 20 PY 2002 VL 17 IS 25 BP 1635 EP 1642 DI 10.1142/S021773230200806X PG 8 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 594KZ UT WOS:000178050200003 ER PT J AU Tumosa, CS Erhardt, D Von Endt, DW Mecklenburg, MF El-Easely, ASM Hopwood, WR AF Tumosa, CS Erhardt, D Von Endt, DW Mecklenburg, MF El-Easely, ASM Hopwood, WR TI Irradiation of mail: Effects on museum materials. SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 Smithsonian Inst, Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 18 PY 2002 VL 224 MA 130-AGFD BP U84 EP U84 PN 1 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 583RL UT WOS:000177422200274 ER PT J AU Bradley, BA Sakimoto, SEH Frey, H Zimbelman, JR AF Bradley, BA Sakimoto, SEH Frey, H Zimbelman, JR TI Medusae Fossae Formation: New perspectives from Mars Global Surveyor SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; Medusae Fossae Formation; Mars Global Surveyor; layering; volcanism ID ORBITER LASER ALTIMETER; TOPOGRAPHY; THARSIS; RECORD; REGION; CAMERA; ICE AB [1] The nature and origin of the Medusae Fossae Formation (MFF) on Mars has been debated since the return of the first Viking images. The MFF's young age, distinctive surface texture, and lack of obvious source have prompted multiple hypotheses for its origin. This study uses data from the Mars Global Surveyor (MGS) mission to examine the MFF at all available scales. We discuss and quantify observations from Mars Orbiter Laser Altimeter (MOLA) topography and Mars Orbiter Camera (MOC) images to better constrain the origin of the MFF. Topographic grid estimates yield a present extent of 2.1 x 10(6) km(2) and a volume of 1.4 x 10(6) km(3); however, remnant yardang deposits observed far from the thicker lobes of MFF material suggest that it may have once covered up to 5 x 10(6) km(2). We do not find compelling evidence for extensive fluvial reworking of the MFF; however, in several regions, buried channels are apparent in the MFF because the formation is draped over underlying topography. Layering is apparent at all scales, from submeter to hundreds of meters, with variable resistance to weathering. Continuity of layers appears to be local to regional, but not likely formation-wide. Yardangs form both parallel and bidirectional patterns, with resistant layers and jointing probably influencing their orientations. A comparative study of MFF regional topography and surface expression indicates that the MFF is quantitatively dissimilar to Martian polar layered deposits. The material is most likely a friable and irregularly consolidated air fall deposit of probable volcanic origin. C1 NASA, Goddard Space Flight Ctr, Geodynam Branch, GEST, Greenbelt, MD 20771 USA. Smithsonian Inst, Natl Air & Space Museum, CEPS, Washington, DC 20560 USA. RP Bradley, BA (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA. RI Bradley, Bethany/B-1964-2008 OI Bradley, Bethany/0000-0003-4912-4971 NR 42 TC 52 Z9 52 U1 3 U2 3 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 AUG 17 PY 2002 VL 107 IS E8 AR 5058 DI 10.1029/2001JE001537 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 622HP UT WOS:000179641700001 ER PT J AU Emmons, LH Leite, YLR Kock, D Costa, LP AF Emmons, LH Leite, YLR Kock, D Costa, LP TI A review of the named forms of Phyllomys (Rodentia : Echimyidae) with the description of a new species from coastal Brazil SO AMERICAN MUSEUM NOVITATES LA English DT Article AB To clarify the taxonomy and serve as a foundation for future systematic studies, we searched for the type material associated with all named forms of Brazilian Atlantic tree rats of the genus Phyllomys. For the following ten taxa we found either the originally designated holotypes, syntype series, or contemporary specimens likely to have been seen by the authors: P. blainvilii, P. brasiliensis, P. fossilis, P. nigrispinus, P. unicolor, P. dasythrix, P. lamarum, P. medius, P. thomasi, and P. kerri. For five species the holotype was unambiguously identified. For five other named forms no holotype was originally designated but we found several candidate specimens and for all of these we designate lectotypes. We identify the type localities for all named Phyllomys species and amend those which are ambiguous. We review the taxonomy, diagnosing and redescribing all the named forms of the genus. After examining the type material, we concluded that the rusty-sided tree rat from coastal Brazil, usually identified in the literature as P. brasiliensis, belongs to an unnamed species. We describe and name it here. C1 Amer Museum Nat Hist, Dept Vertebrate Zool Mammal, New York, NY 10024 USA. Smithsonian Inst, Div Mammals NHB 390, Washington, DC 20560 USA. Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. Forschungsinst Senckenberg, Abt Terr Zool, Sekt Mammal 2, D-60325 Frankfurt, Germany. RP Emmons, LH (reprint author), Amer Museum Nat Hist, Dept Vertebrate Zool Mammal, New York, NY 10024 USA. EM emmons.louise@nmnh.si.edu; yuri_leite@yahoo.com; dkock@sng.uni-frankfurt.de RI Leite, Yuri/D-4667-2009; Costa, Leonora/G-4259-2011 OI Leite, Yuri/0000-0002-0248-8738; NR 57 TC 16 Z9 21 U1 0 U2 5 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 AUG 16 PY 2002 IS 3380 BP 1 EP 40 DI 10.1206/0003-0082(2002)380<0001:AROTNF>2.0.CO;2 PG 40 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 612FC UT WOS:000179063000001 ER PT J AU Orrell, TM Carpenter, KE Musick, JA Graves, JE AF Orrell, TM Carpenter, KE Musick, JA Graves, JE TI Phylogenetic and biogeographic analysis of the Sparidae (Perciformes : Percoidei) from cytochrome b sequences SO COPEIA LA English DT Article ID CENTROMERIC SATELLITE DNA; FAMILY PISCES; EVOLUTION; GENE; TELEOSTEI; FISHES AB We used complete sequence of the mitochondrial cytochrome b gene to test monophyly of the Sparoidea, Sparidae, six subfamilies of Sparidae, and to elucidate the interrelationships of the 33 recognized sparid genera. The analysis included 40 sparid species, 10 closely related species, 10 basal percoids, and two nonperciform out-group species. The aligned 1140 base pairs of cytochrome b yielded 542 parsimony informative characters. Mutational analysis revealed that third codon position transitions were saturated and, therefore, of questionable use in phylogenetic analysis. However, the third codon position transversions and all first and second codon substitutions were not saturated and thus judged more reliable for inferring evolutionary relationship. Parsimony analysis of the equally weighted nucleotide data, weighted nucleotide data set (saturated position transitions given a weight of zero) supported a monophyletic Sparidae with the inclusion of Spicara, which is traditionally included in Centracanthidae. The previously proposed composition of genera within the six sparid subfamilies (Boopsinae, Denticinae, Diplodinae, Pagellinae, Pagrinae, and Sparinae) were not monophyletic in all analyses. This suggests the feeding types on which the subfamilies are based were independently derived multiple times within sparid fishes. In all analyses, Lethrinidae were sister to Sparidae. Sparoidea (Sparidae, Centracanthidae, Lethrinidae, and Nemipteridae) were monophyletic only in the weighted nucleotide phylogeny. C1 Virginia Inst Marine Sci, Dept Fisheries Sci, Gloucester Point, VA 23062 USA. Old Dominion Univ, Dept Biol, Norfolk, VA USA. RP Orrell, TM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, NMFS Systemat Lab, POB 37012,WC57,MCR-153, Washington, DC 20013 USA. NR 46 TC 33 Z9 41 U1 3 U2 10 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 AUG 15 PY 2002 IS 3 BP 618 EP 631 DI 10.1643/0045-8511(2002)002[0618:PABAOT]2.0.CO;2 PG 14 WC Zoology SC Zoology GA 588ED UT WOS:000177687400005 ER PT J AU Fernandez, L Vari, RP AF Fernandez, L Vari, RP TI New species of Trichomycterus from the Andes of Argentina with a redescription of Trichomycterus alterus (Siluriformes : Trichomycteridae) SO COPEIA LA English DT Article ID TELEOSTEI AB Trichomycterus belensis, new species, is described from a tributary to Laguna Blanca, a high-elevation drainage in the Departamento Belen, Provincia de Catamarca, Argentina. The new species is distinguished from other members of the apparently nonmonophyletic genus Trichomycterus by a combination of features involving the premaxilla, dentition, barbel form, pigmentation, and morphometrics. Trichomycterus alterus, whose original description was based on a limited number of specimens, is redescribed based on numerous specimens from localities in the central and northwestern portions of Argentina. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Consejo Nacl Invest Cient & Tecn, Fundac Miguel Lillo, Div Ictiol, RA-4000 San Miguel De Tucuman, Argentina. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. EM majose@unt.edu.ar; vari.richard@nmnh.si.edu NR 28 TC 12 Z9 12 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD AUG 15 PY 2002 IS 3 BP 739 EP 747 DI 10.1643/0045-8511(2002)002[0739:NSOTFT]2.0.CO;2 PG 9 WC Zoology SC Zoology GA 588ED UT WOS:000177687400015 ER PT J AU Svenning, JC Macia, MJ AF Svenning, JC Macia, MJ TI Harvesting of Geonoma macrostachys Mart. leaves for thatch: an exploration of sustainability SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE extractivism; non-timber forest products; palm leaves; sustainable management; transition matrix analysis; tropical rain forest ID IMPACT; FOREST; ECUADOR; LIGHT AB Palm leaves are an important source of roof thatch for rural communities in many parts of the tropics. Often leaves are harvested from wild populations, and as a non-timber forest product may promote local commitment to forest conservation. Nevertheless, reports suggest that at least some wild populations are declining due to over-harvesting. In Amazonian Ecuador the understory palm Geonoma macrostachys Mart. is often the preferred species for thatching. Here we explore the limits to sustainable harvesting of this species combining ethnobotanical data on the use of this species by the Huaorani indigenous group with ecological data and transition matrix modeling. We find that due to severe light limitation there seems to be little scope for sustainable harvesting of this species from old-growth forest. Instead high rates of sustainable harvesting could probably be achieved in semi-open anthropogenic habitats, e.g. agroforestry systems or young secondary forests. We also find that harvesting scheme has a strong impact on sustainable harvesting rates; if only adults (leaf length 100-223 cm) are harvested, while subadults (leaf length 35-99 cm) are left unharvested, two to three times as much leaf material can be harvested per area (at a fixed density) as when subadults are also harvested. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Univ Aarhus, Dept Systemat Bot, DK-8240 Risskov, Denmark. Real Jardin Bot, E-28014 Madrid, Spain. RP Svenning, JC (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Svenning, Jens-Christian/C-8977-2012; Macia, Manuel/H-4631-2012 OI Svenning, Jens-Christian/0000-0002-3415-0862; Macia, Manuel/0000-0002-4676-612X NR 44 TC 35 Z9 38 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD AUG 15 PY 2002 VL 167 IS 1-3 BP 251 EP 262 AR PII S0378-1127(01)00699-5 DI 10.1016/S0378-1127(01)00699-5 PG 12 WC Forestry SC Forestry GA 576UH UT WOS:000177023700020 ER PT J AU Phillips, OL Martinez, RV Arroyo, L Baker, TR Killeen, T Lewis, SL Malhi, Y Mendoza, AM Neill, D Vargas, PN Alexiades, M Ceron, C Di Fiore, A Erwin, T Jardim, A Palacios, W Saldias, M Vinceti, B AF Phillips, OL Martinez, RV Arroyo, L Baker, TR Killeen, T Lewis, SL Malhi, Y Mendoza, AM Neill, D Vargas, PN Alexiades, M Ceron, C Di Fiore, A Erwin, T Jardim, A Palacios, W Saldias, M Vinceti, B TI Increasing dominance of large lianas in Amazonian forests SO NATURE LA English DT Article ID ATMOSPHERIC CARBON-DIOXIDE; TROPICAL FORESTS; RAIN-FOREST; PATTERNS; BIOMASS; SINK AB Ecological orthodoxy suggests that old-growth forests should be close to dynamic equilibrium, but this view has been challenged by recent findings that neotropical forests are accumulating carbon(1,2) and biomass(3,4), possibly in response to the increasing atmospheric concentrations of carbon dioxide(5,6). However, it is unclear whether the recent increase in tree biomass has been accompanied by a shift in community composition. Such changes could reduce or enhance the carbon storage potential of old-growth forests in the long term. Here we show that non-fragmented Amazon forests are experiencing a concerted increase in the density, basal area and mean size of woody climbing plants (lianas). Over the last two decades of the twentieth century the dominance of large lianas relative to trees has increased by 1.7-4.6% a year. Lianas enhance tree mortality and suppress tree growth(7), so their rapid increase implies that the tropical terrestrial carbon sink may shut down sooner than current models suggest(8-10). Predictions of future tropical carbon fluxes will need to account for the changing composition and dynamics of supposedly undisturbed forests. C1 Univ Leeds, Sch Geog, Ctr Biodivers & Conservat, Leeds LS2 9JT, W Yorkshire, England. Jardin Bot Missouri, Jaen, Peru. Missouri Bot Garden, St Louis, MO 63166 USA. Museo Hist Nat Moel Kempff Mercado, Santa Cruz, Bolivia. Conservat Int, Washington, DC 20036 USA. Univ Edinburgh, Sch Earth Environm & Geog Sci, Edinburgh EH9 3JU, Midlothian, Scotland. Univ San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. Fdn Jatun Sacha, Quito, Ecuador. Univ Cent Ecuador, Escuela Biol, Herbario QAP, Quito, Ecuador. New York Bot Garden, Bronx, NY 10458 USA. NYU, Dept Anthropol, New York, NY 10003 USA. Smithsonian Inst, Museum Nat Hist, Washington, DC 20560 USA. RP Phillips, OL (reprint author), Univ Leeds, Sch Geog, Ctr Biodivers & Conservat, Leeds LS2 9JT, W Yorkshire, England. RI Phillips, Oliver/A-1523-2011; OI Phillips, Oliver/0000-0002-8993-6168; Lewis, Simon/0000-0002-8066-6851 NR 29 TC 285 Z9 317 U1 9 U2 58 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 15 PY 2002 VL 418 IS 6899 BP 770 EP 774 DI 10.1038/nature00926 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 583UF UT WOS:000177428000037 PM 12181565 ER PT J AU Johansson, JM Davis, JL Scherneck, HG Milne, GA Vermeer, M Mitrovica, JX Bennett, RA Jonsson, B Elgered, G Elosegui, P Koivula, H Poutanen, M Ronnang, BO Shapiro, II AF Johansson, JM Davis, JL Scherneck, HG Milne, GA Vermeer, M Mitrovica, JX Bennett, RA Jonsson, B Elgered, G Elosegui, P Koivula, H Poutanen, M Ronnang, BO Shapiro, II TI Continuous GPS measurements of postglacial adjustment in Fennoscandia - 1. Geodetic results SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE glacial isostacy; space geodesy; vertical motion; sea level change ID GLOBAL POSITIONING SYSTEM; COMPUTING 3-DIMENSIONAL DEFORMATIONS; GLACIAL ISOSTATIC-ADJUSTMENT; SEA-LEVEL; SPECTRAL FORMALISM; SIGNAL SCATTERING; MANTLE VISCOSITY; SITE POSITIONS; SURFACE LOADS; MODEL AB [1] Project BIFROST (Baseline Inferences for Fennoscandian Rebound Observations, Sea-level, and Tectonics) combines networks of continuously operating GPS receivers in Sweden and Finland to measure ongoing crustal deformation due to glacial isostatic adjustment (GIA). We present an analysis of data collected between August 1993 and May 2000. We compare the GPS determinations of three-dimensional crustal motion to predictions calculated using the high-resolution Fennoscandian deglaciation model recently proposed by Lambeck et al. [1998a, 1998b]. We find that the maximum observed uplift rate (similar to10 mm yr(-1)) and the maximum predicted uplift rate agree to better than 1 mm yr(-1). The patterns of uplift also agree quite well, although significant systematic differences are evident. The root-mean-square residual rate for a linear error model yields estimates of rate accuracy of 0.4 mm yr(-1) for east, 0.3 mm yr(-1) for north, and 1.3 mm yr(-1) for up; these figures incorporate model errors, however. We have also compared the values for the observed radial deformation rates to those based on sea level rates from Baltic tide gauges. The observational error for the vertical GPS rates required to give a reduced chi(2) of unity is 0.8 mm yr(-1). The time series do exhibit temporal variations at seasonal frequencies, as well as apparent low-frequency noise. An empirical orthogonal function analysis indicates that the temporal variations are highly correlated among the sites. The correlation appears to be regional and falls off only slightly with distance. Some of this correlated noise is associated with snow accumulation on the antennas or, for those antennas with radomes, on the radomes. This problem has caused us to modify the radomes used several times, leading to one of our more significant sources of uncertainty. C1 Chalmers Univ Technol, Onsala Space Observ, S-43992 Onsala, Sweden. Natl Land Survey, Div Geodet Res, S-80182 Gavle, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Finnish Geodet Inst, FIN-02430 Masala, Finland. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Johansson, JM (reprint author), Chalmers Univ Technol, Onsala Space Observ, S-43992 Onsala, Sweden. EM jmj@oso.chalmers.se; jdavis@cfa.harvard.edu; hgs@oso.chalmers.se; G.A.Milne@durham.ac.uk; Martin.Vermeer@hut.fi; jxm@physics.utoronto.ca; rbennett@cfa.harvard.edu; bo.jonsson@lm.se; kge@oso.chalmers.se; pelosegui@cfa.harvard.edu; Hannu.Koivula@fgi.fi; Markku.Poutanen@fgi.fi; bor@oso.chalmers.se; ishapiro@cfa.harvard.edu RI Davis, James/D-8766-2013; Vermeer, Martin/G-2468-2013; Elgered, Gunnar/B-7052-2016 OI Davis, James/0000-0003-3057-477X; Vermeer, Martin/0000-0003-3107-6342; Elgered, Gunnar/0000-0001-5711-0073 NR 59 TC 77 Z9 78 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD AUG 14 PY 2002 VL 107 IS B8 AR 2157 DI 10.1029/2001JB000400 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 610ZY UT WOS:000178993000004 ER PT J AU Winn, JN Kochanek, CS McLeod, BA Falco, EE Impey, CD Rix, HW AF Winn, JN Kochanek, CS McLeod, BA Falco, EE Impey, CD Rix, HW TI PKS 1830-211: A face-on spiral galaxy lens SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; gravitational lensing; quasars : individual (PKS 1830-211) ID REDSHIFTED MOLECULAR ABSORPTION; RADIO-SOURCE PKS1830-211; GRAVITATIONAL LENS; HUBBLE CONSTANT; ROTATION CURVES; EINSTEIN RING; PKS-1830-211; IMAGES; SYSTEM; MODELS AB We present new Hubble Space Telescope images of the gravitational lens PKS 1830-211, which allow us to characterize the lens galaxy and update the determination of the Hubble constant (H-0) from this system. The I-band image shows that the lens galaxy is a face-on spiral galaxy with clearly delineated spiral arms. The southwestern image of the background quasar passes through one of the spiral arms, explaining the previous detections of large quantities of molecular gas and dust in front of this image. The lens galaxy photometry is consistent with the Tully-Fisher relation, suggesting the lens galaxy is a typical spiral galaxy for its redshift. The lens galaxy position, which was the main source of uncertainty in previous attempts to determine H-0, is now known precisely. Given the current time delay measurement and assuming the lens galaxy has an isothermal mass distribution, we compute H-0 = 44 +/- 9 km s(-1) Mpc(-1) for an Omega(m) = 0.3 flat cosmological model. We describe some possible systematic errors and how to reduce them. We also discuss the possibility raised by Courbin et al. (2002), that what we have identified as a single lens galaxy is actually a foreground star and two separate galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smithsonian Inst, Whipple Observ, Amado, AZ USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 61 TC 51 Z9 51 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2002 VL 575 IS 1 BP 103 EP 110 DI 10.1086/341265 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581BH UT WOS:000177270900010 ER PT J AU Getman, KV Feigelson, ED Townsley, L Bally, J Lada, CJ Reipurth, B AF Getman, KV Feigelson, ED Townsley, L Bally, J Lada, CJ Reipurth, B TI Chandra study of young stellar objects in the NGC 1333 star-forming cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 1333); stars : early-type; stars : pre-main-sequence; X-rays : stars ID RHO-OPHIUCHI CLOUD; IR IMAGING PHOTOMETRY; MAIN-SEQUENCE STARS; HERBIG-HARO FLOWS; X-RAY-EMISSION; T-TAURI STARS; DARK CLOUD; INTERSTELLAR EXTINCTION; CORONAL TEMPERATURES; LUMINOSITY FUNCTIONS AB NGC 1333, a highly active star formation region within the Perseus molecular cloud complex, has been observed with the ACIS-I detector on board the Chandra X-Ray Observatory. In our image with a sensitivity limit of similar to10(28) ergs s(-1), we detect 127 X-ray sources, most with subarcsecond positional accuracy. While 32 of these sources appear to be foreground stars and extragalactic background, 95 X-ray sources are identified with known cluster members. The X-ray luminosity function of the discovered young stellar object (YSO) population spans a range of log L-X similar or equal to 28.0-31.5 ergs s(-1) in the 0.5-8 keV band, and absorption ranges from log N-H similar or equal to 20 to 23 cm(-2). Most of the sources have plasma energies between 0.6 and 3 keV, but a few sources show higher energies up to similar to7 keV. Comparison with K-band source counts indicates that we detect all of the known cluster members with K < 12 and about half of the members with K > 12. K similar or equal to 11, the peak of the K-band luminosity function, corresponds to 0.2-0.4 M. stars for a cluster age of similar to1 Myr. We detect seven of the 20 known YSOs in NGC 1333 producing jets or molecular outflows as well as one deeply embedded object without outflows. No evident difference in X-ray emission of young stars with and without outflows is found. Based on the complete subsample of T Tauri stars, we also find no difference in X-ray properties and X-ray production mechanism of stars with and without K-band excess disks. Several other results are obtained. We suggest that the X-ray emission from two late B stars that illuminate the reflection nebula originates from unresolved late-type companions. Two T Tauri stars are discovered in the ACIS images as previously unknown components of visual binaries. A good correlation L-X proportional to J is seen, which confirms the well-known relation L-X proportional to L-bol found in many star-forming regions. Based on spectral analysis for the X-ray counterpart of SVS 16, we establish that the column density NH is much lower than that expected from near-IR photometry so that its X-ray luminosity, log L-X similar or equal to 30.6 ergs s(-1), is not unusually high. C1 Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. NR 83 TC 82 Z9 82 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2002 VL 575 IS 1 BP 354 EP 377 DI 10.1086/341219 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581BH UT WOS:000177270900032 ER PT J AU Ozel, F AF Ozel, F TI Timing properties of magnetars SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiation mechanisms : thermal; stars : magnetic fields; stars : neutron; X-rays : stars ID X-RAY PULSARS; MAGNETIZED NEUTRON-STARS; SPECTRA; FIELDS; MODELS; 1E-1048.1-5937; EMISSION AB We study the pulse morphologies and pulse amplitudes of thermally emitting neutron stars with ultrastrong magnetic fields. The beaming of the radiation emerging from a magnetar was recently shown to be predominantly nonradial, with a small pencil and a broad fan component. We show that the combination of this radiation pattern with the effects of strong lensing in the gravitational field of the neutron star yields pulse profiles that show a qualitatively different behavior compared to that of the radially peaked beaming patterns explored previously. Specifically, we find that (i) the pulse profiles of magnetars with a single hot emission region on their surface exhibit 1-2 peaks, whereas those with an antipodal emission geometry have 1-4 peaks, depending on the neutron star compactness, the observer's viewing angle, and the size of the hot regions; (ii) the energy dependence of the beaming pattern may give rise to weakly or strongly energy-dependent pulse profiles and may introduce phase lags between different energy bands; (iii) the nonradial beaming pattern can give rise to high pulsed fractions even for very relativistic neutron stars; (iv) the pulsed fraction may not vary monotonically with neutron star compactness; (v) the pulsed fraction does not decrease monotonically with the size of the emitting region; (vi) the pulsed fraction from a neutron star with a single hot pole has, in general, a very weak energy dependence, in contrast to the case of an antipodal geometry. Comparison of these results to the observed properties of anomalous X-ray pulsars strongly suggests that they are neutron stars with a single hot region of ultrastrong magnetic field. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Ozel, F (reprint author), Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA. NR 25 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 AUG 10 PY 2002 VL 575 IS 1 BP 397 EP 406 DI 10.1086/340900 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581BH UT WOS:000177270900035 ER PT J AU Krennrich, F Bond, IH Bradbury, SM Buckley, JH Carter-Lewis, DA Cui, W Perez, ID Fegan, DJ Fegan, SJ Finley, JP Gaidos, JA Gibbs, K Gillanders, GH Hall, TA Hillas, AM Holder, J Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Lang, MJ LeBohec, S Moriarty, P Muller, D Ong, RA Pallassini, R Petry, D Quinn, J Reay, NW Reynolds, PT Rose, HJ Sembroski, GH Sidwell, R Stanton, N Swordy, SP Vassiliev, VV Wakely, SP Weekes, TC AF Krennrich, F Bond, IH Bradbury, SM Buckley, JH Carter-Lewis, DA Cui, W Perez, ID Fegan, DJ Fegan, SJ Finley, JP Gaidos, JA Gibbs, K Gillanders, GH Hall, TA Hillas, AM Holder, J Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Lang, MJ LeBohec, S Moriarty, P Muller, D Ong, RA Pallassini, R Petry, D Quinn, J Reay, NW Reynolds, PT Rose, HJ Sembroski, GH Sidwell, R Stanton, N Swordy, SP Vassiliev, VV Wakely, SP Weekes, TC TI Discovery of spectral variability of Markarian 421 at TeV energies SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (Markarian 421); gamma rays : observations ID ACTIVE GALAXY MARKARIAN-421; CHERENKOV TELESCOPE SYSTEM; X-RAY; CAT OBSERVATIONS; GAMMA-RAYS; MKN-501; FLARE; PHOTONS; MKN-421; CUTOFF AB The detection of spectral variability of the gamma-ray blazar Mrk 421 at TeV energies is reported. Observations with the Whipple Observatory 10 m gamma-ray telescope taken in 2000/2001 revealed exceptionally strong and long-lasting flaring activity. Flaring levels of 0.4-13 times that of the Crab Nebula flux provided sufficient statistics for a detailed study of the energy spectrum between 380 GeV and 8.2 TeV as a function of the flux level. These spectra are well described by a power law with an exponential cutoff: dN/dE proportional to E(-alpha)e(-E/Eo) m(-2) s(-1) TeV-1. There is no evidence for variation in the cutoff energy with flux, and all spectra are consistent with an average value for the cutoff energy of 4.3 TeV. The spectral index varies between 1.89 +/- 0.04(stat) +/- 0.05(syst) in a high flux state and 2.72 +/- 0.11(stat) +/- 0.05(syst) in a low state. The correlation between spectral index and flux is tight when averaging over the total 2000/ 2001 data set. Spectral measurements of Mrk 421 from previous years (1995/1996 and 1999) by the Whipple collaboration are consistent with this flux-spectral index correlation, which suggests that this may be a constant or a long-term property of the source. If a similar flux-spectral index correlation were found for other gamma-ray blazars, this universal property could help disentangle the intrinsic emission mechanism from external absorption effects. 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. 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. Natl Univ Ireland, Dept Phys, Galway, Ireland. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. Depauw Univ, Dept Phys, 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 90095 USA. Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. Cork Inst Technol, Dept Phys, Cork, Ireland. RP Krennrich, F (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. OI Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 33 TC 67 Z9 67 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2002 VL 575 IS 1 BP L9 EP L13 DI 10.1086/342700 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581BJ UT WOS:000177271000003 ER PT J AU Villesen, P Murakami, T Schultz, TR Boomsma, JJ AF Villesen, P Murakami, T Schultz, TR Boomsma, JJ TI Identifying the transition between single and multiple mating of queens in fungus-growing ants SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE fungus-growing ants; microsatellite markers; multiple mating; paternity; relatedness; attine ants ID ACROMYRMEX ECHINATIOR; PHYLOGENETIC ANALYSIS; SOCIAL HYMENOPTERA; ATTA-COLOMBICA; STINGLESS BEES; MATE NUMBER; POLYANDRY; PATERNITY; RELATEDNESS; EVOLUTION AB Obligate mating of females (queens) with multiple males has evolved only rarely in social Hymenoptera (ants, social bees, social wasps) and for reasons that are fundamentally different from those underlying multiple mating in other animals. The monophyletic tribe of ('attine') fungus-growing ants is known to include evolutionarily derived genera with obligate multiple mating (the Acromyrmex and Atta leafcutter ants) as well as phylogenetically basal genera with exclusively single mating (e.g. Apterostigma, Cyphomyrmex, Myrmicocrypta). All attine genera share the unique characteristic of obligate dependence on symbiotic fungus gardens for food, but the sophistication of this symbiosis differs considerably across genera. The lower attine genera generally have small, short-lived colonies and relatively non-specialized fungal symbionts (capable of living independently of their ant hosts), whereas the four evolutionarily derived higher attine genera have highly specialized, long-term clonal symbionts. In this paper, we investigate whether the transition from single to multiple mating occurred relatively recently in the evolution of the attine ants, in conjunction with the novel herbivorous 'leafcutter' niche acquired by the common ancestor of Acromyrmex and Atta, or earlier, at the transition to rearing specialized long-term clonal fungi in the common ancestor of the larger group of higher attines that also includes the genera Trachymyrmex and Sericomyrmex. We use DNA microsatellite analysis to provide unambiguous evidence for a single, late and abrupt evolutionary transition from exclusively single to obligatory multiple mating. This transition is historically correlated with other evolutionary innovations, including the extensive use of fresh vegetation as substrate for the fungus garden, a massive increase in mature colony size and morphological differentiation of the worker caste. C1 Aarhus Univ, Dept Ecol & Genet, DK-8000 Aarhus C, Denmark. Univ Texas, Patterson Labs, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. Univ Copenhagen, Inst Zool, Dept Populat Ecol, DK-2100 Copenhagen, Denmark. RP Boomsma, JJ (reprint author), Aarhus Univ, Dept Ecol & Genet, DK-8000 Aarhus C, Denmark. EM jjboomsma@zi.ku.dk RI Boomsma, Jacobus/M-2785-2014 OI Boomsma, Jacobus/0000-0002-3598-1609 NR 60 TC 77 Z9 80 U1 0 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 AUG 7 PY 2002 VL 269 IS 1500 BP 1541 EP 1548 DI 10.1098/rspb.2002.2044 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 585DR UT WOS:000177508300004 PM 12184823 ER PT J AU Piperno, DR Holst, I Wessel-Beaver, L Andres, TC AF Piperno, DR Holst, I Wessel-Beaver, L Andres, TC TI Evidence for the control of phytolith formation in Cucurbita fruits by the hard rind (Hr) genetic locus: Archaeological and ecological implications SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID SILICON; PALEOETHNOBOTANY; EVOLUTION; PLANTS; PEPO AB Many angiosperms, both monocotyledons and dicotyledons, heavily impregnate their vegetative and reproductive organs with solid particles of silicon dioxide (SiO2) known as opaline phytoliths. The underlying mechanisms accounting for the formation of phytoliths in plants are poorly understood, however. Using wild and domesticated species in the genus Cucurbita along with their F, and F-2 progeny, we have demonstrated that the production of large diagnostic phytoliths in fruit rinds exhibits a one-to-one correspondence to the lignification of these structures. We propose that phytolith formation in Cucurbita fruits is primarily determined by a dominant genetic locus, called hard rind (Hr), previously shown to code for lignin deposition. If true, this evidence represents a demonstration of genetic control over phytolith production in a dicotyledon and provides considerable support to hypotheses that silica phytoliths constitute another important system of mechanical defense in plants. Our research also identifies Hr as another single locus controlling more than one important phenotypic difference between wild and domesticated plants, and establishes rind tissue cell structure and hardness under the effects of Hr as an important determinant of phytolith morphology. When recovered from pre-Columbian archaeological sites, Cucurbita phytoliths represent genetically controlled fossil markers of exploitation and domestication in this important economic genus. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Puerto Rico, Dept Agron & Soils, Mayaguez, PR 00681 USA. Cucurbit Network, Bronx, NY 10471 USA. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. NR 31 TC 57 Z9 63 U1 0 U2 14 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 6 PY 2002 VL 99 IS 16 BP 10923 EP 10928 DI 10.1073/pnas.152275499 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 582HC UT WOS:000177343200125 PM 12149443 ER PT J AU Bishop, RL Blackman, MJ AF Bishop, RL Blackman, MJ TI Instrumental neutron activation analysis of archaeological ceramics: Scale and interpretation SO ACCOUNTS OF CHEMICAL RESEARCH LA English DT Review ID STANDARDIZATION; SPECIALIZATION; POTTERY AB Instrumental neutron activation analysis has become a standard technique for the study of the production and distributional patterns of archaeological pottery. Questions once framed within the context of long distance exchange are now focused on issues of subregional and even intrasite levels. The increasing specificity at which these questions are poised requires a,high level of analytical precision as we seek to observe statistically and archaeologically significant differences among groups of pottery produced from geographically closely spaced resources or the compositional differences that arise from production behaviors of the producers of the pottery. C1 Smithsonian Inst, Smithsonian Ctr Mat Res & Educ, Suitland, MD 20569 USA. RP Blackman, MJ (reprint author), Smithsonian Inst, Smithsonian Ctr Mat Res & Educ, 4210 Silver Hall Rd, Suitland, MD 20569 USA. NR 28 TC 29 Z9 29 U1 0 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0001-4842 J9 ACCOUNTS CHEM RES JI Accounts Chem. Res. PD AUG PY 2002 VL 35 IS 8 BP 603 EP 610 DI 10.1021/ar000199k PG 8 WC Chemistry, Multidisciplinary SC Chemistry GA 586RW UT WOS:000177599700004 PM 12186564 ER PT J AU Santos-Granero, F AF Santos-Granero, F TI Consuming grief: Compassionate cannibalism in an Amazonian society. SO AMERICAN ETHNOLOGIST LA English DT Book Review C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 USA SN 0094-0496 J9 AM ETHNOL JI Am. Ethnol. PD AUG PY 2002 VL 29 IS 3 BP 723 EP 724 DI 10.1525/ae.2002.29.3.723 PG 2 WC Anthropology SC Anthropology GA 607MF UT WOS:000178794800011 ER PT J AU Mulhern, DM AF Mulhern, DM TI Probable case of Binder syndrome in a skeleton from Quarai, New Mexico SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE maxillonasal dysplasia; midfacial hypoplasia; developmental malformation ID MAXILLONASAL; MALFORMATIONS; FACE AB Binder syndrome (maxillonasal dysplasia) is a not uncommon disorder reported in the clinical literature and is characterized by hypoplastic development of the midface. An extensive review of the paleopathology literature did not reveal any examples of Binder syndrome. In this paper, a probable case of Binder syndrome in a female skeleton, 16-17 years at age of death, from Quarai, New Mexico (ca. AD 1375-1450) is presented. This case was identified during standard documentation prior to repatriation at the National Museum of Natural History, Smithsonian Institution. The skull of this individual (381243) exhibits unusual facial features, including an underdeveloped midface, flattened glabella, absent nasal spine, and apparent alveolar prognathism, in addition to a vertebral anomaly. All of these characteristics are consistent with skeletal dysmorphologies associated with Binder syndrome. Measurements of the Quarai skull are compared with published data on Binder patients and normal control groups in order to quantify the nature of the observed morphology. Univariate analysis of craniometric/cephalometric data provides further support for a diagnosis of Binder syndrome, as critical measurements on the Quarai skull are consistent with those reported in Binder patients and significantly different from those reported for normal control groups. In addition to presenting a probable prehistoric case of Binder syndrome, this paper demonstrates the applicability of using direct comparisons of clinical data to help identify unusual conditions in skeletal remains. (C) 2002 Wiley-Liss, Inc. C1 Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Mulhern, DM (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, NMNH MRC 138,10th & Constitut Ave NW, Washington, DC 20560 USA. NR 23 TC 3 Z9 4 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. PD AUG PY 2002 VL 118 IS 4 BP 371 EP 377 DI 10.1002/ajpa.10065 PG 7 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 577TG UT WOS:000177077500005 PM 12124916 ER PT J AU Neubauer, SC Emerson, D Megonigal, JP AF Neubauer, SC Emerson, D Megonigal, JP TI Life at the energetic edge: Kinetics of circumneutral iron oxidation by lithotrophic iron-oxidizing bacteria isolated from the wetland-plant rhizosphere SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID ORGANIC-MATTER; FERRIC IRON; OXYGENATION; PH; DEPOSITION; REDUCTION; SEDIMENTS; MARSHES; DENMARK; AARHUS AB Batch cultures of a lithotrophic Fe(II)-oxidizing bacterium, strain BrT, isolated from the rhizosphere of a wetland plant, were grown in bioreactors and used to determine the significance of microbial Fe(II) oxidation at circumneutral pH and to identify abiotic variables that affect the partitioning between microbial oxidation and chemical oxidation. Strain BrT grew only in the presence of an Fe(II) source, with an average doubling time of 25 h. In one set of experiments, Fe(II) oxidation rates were measured before and after the cells were poisoned with sodium azide. These experiments indicated that strain BrT accounted for 18 to 53% of the total iron oxidation, and the average cellular growth yield was 0.70 g of CH2O per mol of Fe(II) oxidized. In a second set of experiments, Fe(II) was constantly added to bioreactors inoculated with live cells, killed cells, or no cells. A statistical model fitted to the experimental data demonstrated that metabolic Fe(II) oxidation accounted for up to 62% of the total oxidation. The total Fe(II) oxidation rates in these experiments were strongly limited by the rate of Fe(II) delivery to the system and were also influenced by O-2 and total iron concentrations. Additionally, the model suggested that the microbes inhibited rates of abiotic Fe(II) oxidation, perhaps by binding Fe(II) to bacterial exopolymers. The net effect of strain BrT was to accelerate total oxidation rates by up to 18% compared to rates obtained with cell-free treatments. The results suggest that neutrophilic Fe(II)oxidizing bacteria may compete for limited O-2 in the rhizosphere and therefore influence other wetland biogeochemical cycles. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Amer Type Culture Collect, Manassas, VA 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 35 TC 117 Z9 125 U1 3 U2 44 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD AUG PY 2002 VL 68 IS 8 BP 3988 EP 3995 DI 10.1128/AEM.68.8.3988-3995.2002 PG 8 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 580WV UT WOS:000177260500043 PM 12147500 ER PT J AU Tuross, N AF Tuross, N TI Alterations in fossil collagen SO ARCHAEOMETRY LA English DT Article; Proceedings Paper CT 4th International Meeting on Bone Diagenesis CY MAY, 2000 CL TERUEL, SPAIN DE ancient DNA; Pleistocene; racemization; aspartic acid; collagen ID BONE; PRESERVATION; MECHANISM; PROTEIN; CAVE; DIET AB Fossil collagens isolated from fauna excavated at Kent's Cavern, Torquay, England, present a number of chemical and biochemical changes relative to modern collagens, including increased atomic C/N values, differential loss of some amino acids, alterations in molecular weights, altered response to diagnostic staining and increased fluorescence. In the aggregate, these changes suggest primarily chemical as opposed to microbiological impacts, and autohumification by compounds containing carbohydrate and/or nucleic acids. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Tuross, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 29 TC 27 Z9 28 U1 2 U2 6 PU BLACKWELL PUBL LTD PI OXFORD PA 108 COWLEY RD, OXFORD OX4 1JF, OXON, ENGLAND SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD AUG PY 2002 VL 44 BP 427 EP 434 DI 10.1111/1475-4754.00075 PN 3 PG 8 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA 600JR UT WOS:000178387300013 ER PT J AU Holland, ST Soszynski, I Gladders, MD Barrientos, LF Berlind, P Bersier, D Garnavich, PM Jha, S Stanek, KZ AF Holland, ST Soszynski, I Gladders, MD Barrientos, LF Berlind, P Bersier, D Garnavich, PM Jha, S Stanek, KZ TI The optical afterglow of the gamma-ray burst GRB 012111 SO ASTRONOMICAL JOURNAL LA English DT Article DE gamma rays : bursts ID INTERSTELLAR-MEDIUM; ENERGY; PHOTOMETRY; DIVERSITY AB We present early-time optical photometry and spectroscopy of the optical afterglow of the gamma-ray burst GRB 011211. The spectrum of the optical afterglow contains several narrow metal lines that are consistent with the burst's occurring at a redshift of 2.14 +/- 0.001. The optical afterglow decays as a power law with a slope of alpha = 0.83 +/- 0.04 for the first approximate to2 days after the burst, at which time there is evidence of a break. The slope after the break is greater than or equal to 1.4. There is evidence of rapid variations in the R-band light approximately 0.5 days after the burst. These variations suggest that there are density fluctuations near the gamma-ray burst on spatial scales of approximately 40-125 AU. The magnitude of the break in the light curve, the spectral slope, and the rate of decay in the optical suggest that the burst expanded into an ambient medium that is homogeneous on large scales. We estimate that the local particle density is between approximately 0.1 and 10 cm(-3) and that the total gamma-ray energy in the burst was (1.2-1.9) x 10(50) ergs. This energy is smaller than, but consistent with, the "standard" value of (5 +/- 2) x 10(50) ergs. Comparing the observed color of the optical afterglow with predictions of the standard beaming model suggests that the rest-frame V-band extinction in the host galaxy is less than or similar to0.03 mag. C1 Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Uniwersytet Warszawski, Obserwatorium Astron, PL-00478 Warsaw, Poland. Carnegie Observ, Pasadena, CA 91101 USA. Pontificia Univ Catolica Chile, Dept AStron & Astrofis, Santiago 22, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Holland, ST (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. NR 36 TC 62 Z9 62 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2002 VL 124 IS 2 BP 639 EP 645 DI 10.1086/341388 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574KQ UT WOS:000176888900001 ER PT J AU Reipurth, B Rodriguez, LF Anglada, G Bally, J AF Reipurth, B Rodriguez, LF Anglada, G Bally, J TI Radio continuum maps of deeply embedded protostars: Thermal jets, multiplicity, and variability SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : general; ISM : jets and outflows; radio continuum; stars : formation; stars : pre-main-sequence ID HARO ENERGY-SOURCES; YOUNG STELLAR OBJECTS; TELESCOPE NICMOS IMAGES; SMALL-SCALE STRUCTURE; HH 7-11 REGION; EXCITING SOURCES; STAR-FORMATION; VLA DETECTION; MOLECULAR OUTFLOWS; NGC-1333 IRAS-4 AB We have carried out a deep, 3.6 cm radio continuum survey of young outflow sources using the Very Large Array in its A configuration providing subarcsecond resolution. The seven regions observed are L1448-N, IRAS 2 and 4 in NGC 1333, L1551-NE, SSV 63 in L1630, HH 124 IRS in NGC 2264, and B335 IRS. The first three of these objects are known from submillimeter observations to be multiple sources, and we detect almost all known submillimeter components at 3.6 cm. The L1551-NE source is confirmed to be a subarcsecond binary. We find a third radio source in the SSV 63 system, which drives the multiple HH 24 jets. HH 124 IRS is embedded in a cometary cloud, where we detect a small cluster of six time-variable radio continuum sources. Six of the observed sources are resolved into compact thermal radio jets. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Nacl Autonoma Mexico, Astron Inst, Morelia 58089, Michoacan, Mexico. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. RP Reipurth, B (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM reipurth@ifa.hawaii.edu; l.rodriguez@astrosmo.unam.mx; guillem@iaa.es; bally@casa.colorado.edu NR 79 TC 91 Z9 91 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2002 VL 124 IS 2 BP 1045 EP 1053 DI 10.1086/341172 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574KQ UT WOS:000176888900031 ER PT J AU Kenyon, SJ Groot, PJ Benson, P AF Kenyon, SJ Groot, PJ Benson, P TI The eclipsing binary BG Geminorum: Improved constraints on the orbit and the structure of the accretion disk SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : emission-line, Be; stars : evolution; stars : individual (BG Geminorum) ID SPECTRAL ENERGY-DISTRIBUTIONS; DOPPLER TOMOGRAPHY; SYMBIOTIC STARS; VARIABLES; REDSHIFTS; IMAGES AB We describe new optical photometric and spectroscopic observations of the semidetached eclipsing binary BG Geminorum. A large change in the amount of Mg I absorption at secondary maximum indicates the presence of cool material in the outer edge of the disk surrounding the unseen primary star. Detection of weak He I emission implies a hot radiation source at the inner edge of the disk. If the velocity variations in the Hbeta emission-line track the orbital motion of the primary star, the primary star has, an orbital semiamplitude of K-1 = KHbeta = 16.0+/-4.6 km s(-1). This result yields a mass ratio q=0.22+/-0.07, consistent with the q=0.1 derived from the large ellipsoidal variation. Despite this progress, the nature of the primary star-B type star or black hole-remains uncertain. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Wellesley Coll, Whitin Observ, Wellesley, MA 02181 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Groot, Paul/K-4391-2016; OI Groot, Paul/0000-0002-4488-726X; Kenyon, Scott/0000-0003-0214-609X NR 28 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 AUG PY 2002 VL 124 IS 2 BP 1054 EP 1059 DI 10.1086/341651 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574KQ UT WOS:000176888900032 ER PT J AU Goldberg, D Mazeh, T Latham, DW Stefanik, RP Carney, BW Laird, JB AF Goldberg, D Mazeh, T Latham, DW Stefanik, RP Carney, BW Laird, JB TI A survey of proper-motion stars. XV. Orbital solutions for 34 double-lined spectroscopic binaries SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; Galaxy : halo; techniques : radial velocities ID PRIMORDIAL LITHIUM ABUNDANCE; EXTRASOLAR PLANET CANDIDATES; MASS-RATIO DISTRIBUTION; POPULATION-II BINARIES; METAL-POOR STARS; SOLAR-TYPE STARS; RADIAL-VELOCITIES; CROSS-CORRELATION; STELLAR-SYSTEMS; HALO STARS AB We present orbital solutions for 34 double-lined spectroscopic binaries found in the Carney-Latham sample of 1464 stars selected for high proper motion. We use TODCOR, a two-dimensional correlation technique, to extract the velocities for the primary and secondary stars and their light ratio. For our single-order echelle spectra, obtained with the Center for Astrophysics Digital Speedometers, we find that we can reach secondaries that are as much as 2 mag fainter than their primaries. The ratio of the primary to secondary velocity residuals from the orbital fit equals approximately the secondary-to-primary light ratio, as would be expected for the photon-limited case. We use our mass and light ratios to evaluate the mass-luminosity relation for metal-poor main-sequence dwarfs in the mass range 0.55-0.8 M(circle dot). We assume an Lproportional toM(beta) relation and find that the exponent at around 5200 Angstrom is 7.4+/-0.6. We find this is in good agreement with the slope of the corresponding theoretical M(V)-M 14 Gyr isochrones from the VandenBerg & Bell models for metal-poor stars. C1 Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA. RP Goldberg, D (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. EM dorit@wise.tau.ac.il; mazeh@wise.tau.ac.il; dlatham@cfa.harvard.edu; rstefanik@cfa.harvard.edu; bruce@astro.unc.edu; laird@tycho.bgsu.edu NR 68 TC 52 Z9 56 U1 0 U2 3 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 AUG PY 2002 VL 124 IS 2 BP 1132 EP 1143 DI 10.1086/341385 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574KQ UT WOS:000176888900040 ER PT J AU Latham, DW Stefanik, RP Torres, G Davis, RJ Mazeh, T Carney, BW Laird, JB Morse, JA AF Latham, DW Stefanik, RP Torres, G Davis, RJ Mazeh, T Carney, BW Laird, JB Morse, JA TI A survey of proper-motion stars. XVI. Orbital solutions for 171 single-lined spectroscopic binaries SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; Galaxy : halo ID LOW-MASS COMPANIONS; RADIAL-VELOCITIES; SOLAR NEIGHBORHOOD; ECCENTRIC ORBITS; SYSTEMS; HALO; FREQUENCY; SAMPLE; PLANETS; TODCOR AB We report 25,563 radial velocity measurements for 1359 single-lined stars in the Carney-Latham sample of 1464 stars selected for high proper motion. For 171 of these, we present spectroscopic orbital solutions. We find no obvious difference between the binary characteristics in the halo and the disk populations. The observed frequency is the same, and the period distributions are consistent with the hypothesis that the two sets of binaries were drawn from the same parent population. This suggests that metallicity in general, and radiative opacities in particular, have little influence over the fragmentation process that leads to short-period binaries. All the binaries with periods shorter than 10 days have nearly circular orbits, while the binaries with periods longer than 20 days exhibit a wide range of eccentricities and a median value of 0.37. For the metal-poor high-velocity halo binaries in our sample, the transition from circular to eccentric orbits appears to occur at about 20 days, supporting the conclusion that tidal circularization on the main sequence is important for the oldest binaries in the Galaxy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 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 Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 52 TC 222 Z9 229 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2002 VL 124 IS 2 BP 1144 EP 1161 DI 10.1086/341384 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574KQ UT WOS:000176888900041 ER PT J AU Kuchner, MJ Brown, ME Holman, M AF Kuchner, MJ Brown, ME Holman, M TI Long-term dynamics and the orbital inclinations of the classical Kuiper belt objects SO ASTRONOMICAL JOURNAL LA English DT Article DE celestial mechanics; comets : general; Kuiper belt; methods : N-body simulations; planetary systems : formation ID SHORT-PERIOD COMETS; OUTER SOLAR-SYSTEM; SECULAR RESONANCES; CHAOTIC MOTION; NEPTUNE; ORIGIN; ACCRETION; DELIVERY; DISK; AU AB We numerically integrated the orbits of 1458 particles in the region of the classical Kuiper belt (41 AU less than or equal to a less than or equal to 47 AU) to explore the role of dynamical instabilities in sculpting the inclination distribution of the classical Kuiper belt objects (KBOs). We find that the selective removal of low-inclination objects by overlapping secular resonances (nu(17) and nu(18)) acts to raise the mean inclination of the surviving population of particles over 4 billion yr of interactions with Jupiter, Saturn, Uranus, and Neptune, though these long-term dynamical effects do not themselves appear to explain the discovery of KBOs with inclinations near 30degrees. Our integrations also imply that after 3 billion yr of interaction with the massive planets, high-inclination KBOs more efficiently supply Neptune-encountering objects, the likely progenitors of short-period comets, Centaurs, and scattered KBOs. The secular resonances at low inclinations may indirectly cause this effect by weeding out objects unprotected by mean motion resonances during the first 3 billion yr. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Planetary Sci, Pasadena, CA 91125 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 39 TC 31 Z9 32 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2002 VL 124 IS 2 BP 1221 EP 1230 DI 10.1086/341643 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574KQ UT WOS:000176888900046 ER PT J AU Laurent, E Rousselet-Perraut, K Benech, P Berger, JP Gluck, S Haguenauer, P Kern, P Malbet, F Schanen-Duport, I AF Laurent, E Rousselet-Perraut, K Benech, P Berger, JP Gluck, S Haguenauer, P Kern, P Malbet, F Schanen-Duport, I TI Integrated optics for astronomical interferometry - V. Extension to the K band SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric ID LATE-TYPE STARS; EFFECTIVE TEMPERATURES; IOTA INTERFEROMETER; INTERFEROGRAMS; GIANTS; IV AB We report laboratory and on sky characterizations of planar integrated optics beam combiners in the K ([2.0 mum; 2.4 mum]) and K' ([2.02 mum; 2.30 mum]) bands. Because of the strong scientific interests of the K band, we have extended the integrated optics technologies available in the telecom range (i.e. at 0.8 mum, 1.3 mum and 1.5 mum) to 2.0-2.5 mum. Ion exchange components optimized for these atmospheric bands provide stable contrasts higher than 95% with a laboratory white-light source and global throughputs of 35% in this spectral range. These results are completed with first stellar interferograms obtained with a silica-on-silicon two-way beam combiner on the IOTA interferometer. We characterized in the H and K bands the throughput of this beam combiner optimized for the H band ([1.47 mum; 1.78 mum]). On-sky fringes obtained on iotaAur in the H and K' bands clearly demonstrate a high instrumental contrast (larger than 50%) in both bands. This shows that integrated optics works with high performance outside its usual wavelength domain and provides good solutions for astronomical interferometry in a large wavelength range. We have measured single-mode ranges over 1 mum on our components which would allow to observe in two spectral bands simultaneously or to integrate both metrology reference and science signals in a single chip for astrometric applications. C1 Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. Inst Microelect Eletromagnetisme & Photon, F-38016 Grenoble, France. Alcatel Space Ind, F-06156 Cannes La Bocca, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lab Electron Technol & Informat, F-38054 Grenoble 9, France. RP Laurent, E (reprint author), Observ Grenoble, Astrophys Lab, BP 53, F-38041 Grenoble 9, France. NR 24 TC 23 Z9 23 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2002 VL 390 IS 3 BP 1171 EP 1176 DI 10.1051/0004-6361:20020404 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 579MR UT WOS:000177182200036 ER PT J AU Motta, V Mediavilla, E Munoz, JA Falco, E Kochanek, CS Arribas, S Garcia-Lorenzo, B Oscoz, A Serra-Ricart, M AF Motta, V Mediavilla, E Munoz, JA Falco, E Kochanek, CS Arribas, S Garcia-Lorenzo, B Oscoz, A Serra-Ricart, M TI Detection of the 2175 angstrom extinction feature at z=0.83 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; gravitational lensing; quasars : individual (SBS 0909+532) ID OPTICAL-FIBER SYSTEM; GRAVITATIONAL LENS; INTERSTELLAR EXTINCTION; MAGELLANIC-CLOUD; ULTRAVIOLET EXTINCTION; STARBURST GALAXIES; DUST; SPECTROSCOPY; SPECTRA; QUASAR AB We determine the extinction curve in the z(l) = 0.83 lens galaxy of the gravitational lens SBS 0909+532 from the wavelength dependence of the flux ratio between the lensed quasar images (z(s) = 1.38) from 3400 to 9200 Angstrom. It is the first measurement of an extinction curve at a cosmological distance of comparable quality to those obtained within the Galaxy. The extinction curve has a strong 2175 Angstrom feature, a noteworthy fact because it has been weak or nonexistent in most estimates of extinction curves outside the Galaxy. The extinction curve is fitted well by a standard R(V) = 2.1 +/- 0.9 Galactic extinction curve. If we assume standard Galactic extinction laws, the estimated dust redshift of z = 0.88 +/- 0.02 is in good agreement with the spectroscopic redshift of the lens galaxy. The widespread assumption that SMC extinction curves are more appropriate models for cosmological dust may be incorrect. C1 Inst Astrofis Canarias, Tenerife 38200, Spain. Fac Ciencias, Dept Astron, Montevideo 11400, Uruguay. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. ESA, Space Telescope Sci Inst, Res & Sci Support Dept, Baltimore, MD 21218 USA. Consejo Super Invest Cientif, Barcelona, Spain. Isaac Newton Grp Telescopes, La Palma 38700, Spain. RP Motta, V (reprint author), Inst Astrofis Canarias, Via Lactea S-N, Tenerife 38200, Spain. EM vmotta@ll.iac.es; emg@ll.iac.es RI Garcia-Lorenzo, Maria Begona/E-7011-2010 OI Garcia-Lorenzo, Maria Begona/0000-0002-7228-7173 NR 28 TC 76 Z9 77 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 AUG 1 PY 2002 VL 574 IS 2 BP 719 EP 725 DI 10.1086/341118 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581BC UT WOS:000177270400015 ER PT J AU Finoguenov, A Jones, C AF Finoguenov, A Jones, C TI Chandra observation of low-mass X-ray binaries in the elliptical galaxy M84 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; galaxies : elliptical and lenticular, cD; galaxies : individual (M84 NGC 4374); X-rays : galaxies; X-rays : stars ID BLACK-HOLES; COMPTONIZATION; POPULATION; ACCRETION; CLUSTER; NOVAE AB We present characteristics of the X-ray point-source population in the M84 galaxy observed by the Chandra Advanced CCD Imaging Spectrometer S-Array. We find an excess in the number of sources centered on M84 with a spatial distribution closely corresponding to the M84 stellar light. Given an absence of recent star formation, accreting binaries are the only candidates for the M84 X-ray sources. The majority of M84 sources (with luminosities exceeding 10(38) ergs s(-1)) exhibit hardness ratios expected from multi-temperature blackbody disk emission. The most luminous sources, which we attribute to accreting black holes, exhibit X-ray colors typical of a blackbody spectrum. We also identify the sources whose X-ray colors match the expectations for constituents of the cosmic X-ray background. The number of such sources agrees with that expected to be background sources. After correcting for incompleteness in the source detection, we find a log N-log S for M84 similar to that of the elliptical galaxy NGC 4697, i.e., having a break at a luminosity of L-b = 2.4(-0.3)(+0.6) x 10(38) ergs s(-1), approximately the Eddington limit on the isotropic luminosity for accretion onto a neutron star. The slope of the luminosity function above the break provides evidence for a mass distribution in the M84 accreting black holes. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Finoguenov, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr Postfach 1312, D-85748 Garching, Germany. NR 39 TC 30 Z9 30 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2002 VL 574 IS 2 BP 754 EP 761 DI 10.1086/340997 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581BC UT WOS:000177270400018 ER PT J AU Szkody, P Nishikida, K Raymond, JC Seth, A Hoard, DW Long, KS Sion, EM AF Szkody, P Nishikida, K Raymond, JC Seth, A Hoard, DW Long, KS Sion, EM TI Chandra spectra of the prototype dwarf nova U geminorum at quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars : individual (U Geminorum); X-rays : stars ID HOPKINS-ULTRAVIOLET-TELESCOPE; X-RAY-SPECTRUM; WHITE-DWARF; CATACLYSMIC VARIABLES; ACCRETION DISKS; BOUNDARY-LAYERS; SS CYGNI; OUTBURST; EMISSION; PLASMA AB We have observed the prototypical dwarf nova U Gem at quiescence with the Chandra medium- and high-resolution gratings to accomplish the first study of resolved X-ray emission lines in a disk-accreting cataclysmic variable. Doppler tomograms constructed from optical spectra obtained close in time to the X-ray observation show a typical quiescent disk structure with an irradiated secondary but no prominent disk hot spot. The unprecedented spectral resolution of Chandra over past X-ray telescopes reveals prominent narrow emission lines of O, Ne, Mg, Si, S, and Fe. The line fluxes, ratios, and widths indicate that X-ray emission arises from a range of temperatures in a high-density (greater than 10(14) cm(-3)) gas, moving at low (less than 300 km s(-1)) velocity, with a small ( less than 10(7) cm) scale height compared to the white dwarf radius. Simple models with cooling flows, cooling flows plus isothermal zones, and thermal conduction give reasonable agreement with the low-temperature emission lines, but a good fit to the entire range of lines will require a better understanding of all the parameters that affect the boundary layer. C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. RP Szkody, P (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. NR 42 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2002 VL 574 IS 2 BP 942 EP 949 DI 10.1086/341006 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581BC UT WOS:000177270400035 ER PT J AU Narayan, R Heyl, JS AF Narayan, R Heyl, JS TI On the lack of type I X-ray bursts in black hole X-ray binaries: Evidence for the event horizon? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays : binaries; X-rays : bursts ID ACCRETING NEUTRON-STARS; THERMAL EVOLUTION; NUCLEAR-FUSION; FLASHES; ENVELOPES; DISCOVERY; CAPTURE; MASS AB Type I X-ray bursts are very common in neutron star X-ray binaries, but no type I burst has been seen in the dozen or so binaries in which the accreting compact star is too massive to be a neutron star and is therefore identified as a black hole candidate. We have carried out a global linear stability analysis of the accumulating fuel on the surface of a compact star to identify the conditions under which thermonuclear bursts are triggered. Our analysis, which improves on previous calculations, reproduces the gross observational trends of bursts in neutron star systems. It further shows that, if black hole candidates have surfaces, they would very likely exhibit instabilities similar to those that lead to type I bursts on neutron stars. The lack of bursts in black hole candidates is thus significant and indicates that these objects have event horizons. We discuss possible caveats to this conclusion. C1 Inst Adv Study, Princeton, NJ 08540 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA. EM rnarayan@cfa.harvard.edu; jheyl@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 32 TC 40 Z9 40 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 AUG 1 PY 2002 VL 574 IS 2 BP L139 EP L142 DI 10.1086/342502 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581BF UT WOS:000177270700008 ER PT J AU Matthews, LD Gallagher, JS AF Matthews, LD Gallagher, JS TI High-resolution optical rotation curves of low-luminosity spiral galaxies SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : fundamental parameters galaxies : general; galaxies : kinematics and dynamics galaxies : spiral ID SURFACE BRIGHTNESS GALAXIES; MATTER-DOMINATED GALAXIES; H-I; MASS-DISTRIBUTION; DISK GALAXIES; STAR CLUSTER; DARK-HALO; SOUTHERN; NUCLEI; KINEMATICS AB We present optical long-slit spectroscopic observations of 21 low-luminosity, extreme late-type spiral galaxies. Our sample is comprised of Sc-Sm Local Supercluster spirals with moderate-to-low optical surface brightnesses and with luminosities at the low end for spiral disk galaxies (M-V greater than or equal to -18.8). For each galaxy we have measured high spatial resolution position-velocity (P-V) curves using the Halpha emission line, and for 15 of the galaxies we also derive major-axis rotation curves. In similar to50% of our sample, the P-V curves show significant asymmetries in shape, extent, and/or amplitude on the approaching and receding sides of the disk. A number of the P-V curves are still rising to the last measured point or reach a clear turnover on only one side. In most instances we find good agreement between the kinematic centers of extreme late-type spirals as defined by the global H I emission profile and by their optical continuum, although in a few cases we see evidence of possible real offsets. In spite of their shallow central gravitational potentials, at least six of the galaxies in our sample possess semi-stellar nuclei that appear to be compact nuclear star clusters; in five of these cases we see kinematic signatures in the P-V curves at the location of the nucleus. Finally, we find that like giant spirals, our sample galaxies have higher specific angular momenta than predicted by current cold dark matter models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Matthews, LD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. NR 68 TC 30 Z9 30 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2002 VL 141 IS 2 BP 429 EP 442 DI 10.1086/340647 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 575ZN UT WOS:000176978500006 ER PT J AU Johnson, WR Savukov, IM Safronova, UI Dalgarno, A AF Johnson, WR Savukov, IM Safronova, UI Dalgarno, A TI E1 transitions between states with n=1-6 in helium-like carbon, nitrogen, oxygen, neon, silicon, and argon SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic data; plasmas ID CONFIGURATION-INTERACTION CALCULATIONS; SELECTIVE CHARGE-TRANSFER; WIND-COMET INTERACTIONS; X-RAY; SOLAR-WIND; OSCILLATOR-STRENGTHS; ENERGY-LEVELS; IONS; EMISSION; JUPITER AB Wavelengths and transition rates are given for E1 transitions between singlet (1)S, (1)P, (1)D, and (1)F states, between triplet (3)S, (3)P, and (3)D states, and between triplet (3)P(1) and singlet (1)S(0) states in ions of astrophysical interest: helium-like carbon, nitrogen, oxygen, neon, silicon, and argon. All possible E1 transitions between states with J less than or equal to 3 and n less than or equal to 6 are considered. Energy levels and wave functions used in calculations of the transition rates are obtained from relativistic configuration-interaction calculations that include both Coulomb and Breit interactions. C1 Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Johnson, WR (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland,Sci Hall, Notre Dame, IN 46556 USA. EM johnson@nd.edu; adalgarno@cfa.harvard.edu NR 27 TC 20 Z9 20 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2002 VL 141 IS 2 BP 543 EP 557 DI 10.1086/340547 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 575ZN UT WOS:000176978500012 ER PT J AU Estrada, C Jiggins, CD AF Estrada, C Jiggins, CD TI Patterns of pollen feeding and habitat preference among Heliconius species SO ECOLOGICAL ENTOMOLOGY LA English DT Article DE co-evolution; ecological isolation; Lepidoptera; pollen feeding; speciation ID PASSION-VINE BUTTERFLIES; SYMPATRIC SPECIATION; MIMICRY; NYMPHALIDAE; EVOLUTION; LEPIDOPTERA; ADAPTATIONS; SEQUENCES; BEHAVIOR; BIOLOGY AB 1. The ecological circumstances that precipitate speciation remain poorly understood. Here, a community of Heliconius butterflies in lowland Panama was studied to investigate patterns of pollen use, and more specifically the ecological changes associated with the recent divergence of Heliconius melpomene (Linnaeus) and H. cydno (Doubleday). 2. Considering the seven commonest Heliconius species in the community, 32 types of pollen or spore were encountered in pollen loads but only five pollen species were common. Systematic exploitation of pollen was therefore confined to a small proportion of the flowers visited. 3. Most of the variation in pollen load composition between individuals was explained by differences in collecting locality. The exception was Psiguria, which was used in all habitats by the melpomene/hecale clade far more than by the erato/sapho clade. This may suggest an ancestral switch within Heliconius towards increased reliance on Psiguria pollen. 4. Heliconius cydno and H. melpomene differed significantly in pollen load composition for three of the five most commonly collected pollen species. This is most probably explained by differences in habitat preference; H. melpomene and its co-mimic H. erato are found in open habitat while H. cydno and its co-mimic H. sapho are found in closed-canopy forest. 5. As melpomene and cydno are known to hybridise occasionally, such differences in adult microhabitat contribute to pre-mating isolation. Habitat divergence between H. cydno and H. melpomene, which is associated with changes in mimicry, must have played a role in their recent speciation. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Jiggins, CD (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. RI Jiggins, Chris/B-9960-2008; Marion-Poll, Frederic/D-8882-2011 OI Jiggins, Chris/0000-0002-7809-062X; Marion-Poll, Frederic/0000-0001-6824-0180 NR 36 TC 41 Z9 43 U1 1 U2 18 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0307-6946 J9 ECOL ENTOMOL JI Ecol. Entomol. PD AUG PY 2002 VL 27 IS 4 BP 448 EP 456 DI 10.1046/j.1365-2311.2002.00434.x PG 9 WC Entomology SC Entomology GA 568YJ UT WOS:000176572300008 ER PT J AU De Steven, D Wright, SJ AF De Steven, D Wright, SJ TI Consequences of variable reproduction for seedling recruitment in three neotropical tree species SO ECOLOGY LA English DT Article DE Barro Colorado Island, Panama; density dependence; Quararibea asterolepis; recruitment limitation; seed production; seedling demography; Tetragastris panamensis; Trichilia tuberculata; tropical tree demography ID RAIN-FOREST TREE; NINO SOUTHERN-OSCILLATION; JANZEN-CONNELL MODEL; TROPICAL FOREST; DENSITY-DEPENDENCE; PLANT-POPULATIONS; SPATIAL PATTERNS; DISPERSAL; DIVERSITY; DYNAMICS AB Variable seed production may have important consequences for recruitment but is poorly documented for frugivore-dispersed tropical trees. Recruitment limitation may also be a critical spatial process affecting forest dynamics, but it is rarely assessed at the scale of individual trees. Over an 11-yr period, we studied the consequences of variable seed production for initial seedling recruitment in three shade-tolerant tree species (Quararibea asterolepis, Tetragastris panamensis, and Trichilia tuberculata) on Barro Colorado Island, Panama. We measured annual seed production for a permanent sample of focal trees and censused annual new seedling establishment within a restricted dispersal neighborhood of each tree. We analyzed temporal and spatial variability in recruitment and compared recruitment limitations among species. Annual seed production in Quararibea and Tetragastris fluctuated widely, whereas Trichilia had more, consistent seed production across years. Within species, trees were synchronized in seed production, and synchrony appeared partly influenced by El Nino climatic events. Seedling recruitment varied temporally and spatially. At the population scale, all species had greater recruitment in productive seed years, and individual trees had differing contributions to this temporal pattern. At the focal-tree scale, recruitment patterns differed among species. Quararibea and Tetragastris trees with higher average seed production recruited more seedlings in their local neighborhoods than did less fecund trees. In contrast, Trichilia seedling recruitment did not increase with seed crop size, suggesting negative density dependence. At the tree neighborhood scale, no species showed evidence of density dependence in first-year survival. Comparatively, recruitment was more seed-limited in Quararibea and Tetragastris and more establishment-limited in Trichilia. Overall, our results indicated that: (1) variable seed production influenced seedling recruitment both temporally and spatially, and (2) species differed in limitations to recruitment. C1 Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP De Steven, D (reprint author), USDA, Forest Serv, So Res Stn, Ctr Forested Wetlands Res, 2730 Savannah Highway, Charleston, SC 29414 USA. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 55 TC 33 Z9 36 U1 2 U2 19 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD AUG PY 2002 VL 83 IS 8 BP 2315 EP 2327 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 583WP UT WOS:000177434200025 ER PT J AU Gallegos, CL Jordan, TE AF Gallegos, CL Jordan, TE TI Impact of the Spring 2000 phytoplankton bloom in Chesapeake Bay on optical properties and light penetration in the Rhode River, Maryland SO ESTUARIES LA English DT Article ID SUBMERSED AQUATIC VEGETATION; DIFFUSE ATTENUATION; ESTUARY; ABSORPTION; WATER; PHOTOSYNTHESIS; PRODUCTIVITY; CHLOROPHYLL; TRANSPORT; NUTRIENTS AB Accelerating eutrophication manifest as increasing frequency and magnitude of phytoplankton blooms threatens living resources in many estuaries. Effects of large blooms can be difficult to document because blooms are often unexpected and do not always coincide with scheduled sampling programs. Here we use continuously monitored salinity distributions and optical properties to study the spring bloom of the red tide dinoflagellate, Prorocentrum minimum, in the Rhode River, Maryland, a tributary embayment of upper Chesapeake Bay. Salinity distributions, together with weekly cruise measurements of nutrient concentrations, indicate that the bloom commenced with an influx of nitrate at the mouth due to the arrival of a freshet from the Susquehanna River. Arrival of this freshet at the mouth set up an unstable, inverse salinity gradient within the Rhode River. Continuously monitored absorption and scattering spectra indicated that increases in chlorophyll within the Rhode River initially were due to the influx of chlorophyll that had developed in the main stem of the bay. After the influx, much higher concentrations and steep spatial gradients developed within the Rhode River, subsequent to reduced mixing that accompanied re-establishment of a normal estuarine salinity gradient. We used the monitored absorption and scattering coefficients to determine the effect of the bloom on light attenuation coefficients in the Rhode River. The bloom resulted in a nearly three-fold increase in attenuation coefficient. Attenuation was dominated by chlorophyll in the early stages of the bloom and by detritus after the termination of the bloom. Although the bloom lasted only 20 d, the elevated attenuation coefficients due to the bloom exceeded values that would permit growth of submersed vascular plants for a period of about 45 d. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. OI Gallegos, Charles/0000-0001-5112-0166 NR 31 TC 32 Z9 35 U1 0 U2 9 PU ESTUARINE RES FEDERATION PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0160-8347 J9 ESTUARIES JI Estuaries PD AUG PY 2002 VL 25 IS 4A BP 508 EP 518 DI 10.1007/BF02804886 PG 11 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 602WK UT WOS:000178527300002 ER PT J AU Johnson, RC Johnston, WJ Golob, CT Nelson, MC Soreng, RJ AF Johnson, RC Johnston, WJ Golob, CT Nelson, MC Soreng, RJ TI Characterization of the USDA Poa pratensis collection using RAPD markers and agronomic descriptors SO GENETIC RESOURCES AND CROP EVOLUTION LA English DT Article DE cluster analysis; diversity; germplasm evaluation; Kentucky bluegrass; Poa pratensis; RAPD analysis ID GERMPLASM COLLECTION; GENETIC-MARKERS; DNA; IDENTIFICATION; POPULATIONS; ACCESSIONS AB Characterization of germplasm collections is critical to assess collection diversity and enhance utilization. A Poa pratensis L. germplasm collection of 228 accessions representing 26 countries, along with 17 commercial check cultivars, was characterized using 86 random amplified polymorphic DNA (RAPD) markers and 17 agronomic descriptors. The Dice similarity coefficient used for RAPD data ranged from 0.56 to 0.95 and average Euclidean distance used for agronomic data ranged from 0.28 to 2.52. No two accessions had a similarity of one or a distance of zero, showing there were no duplicate entries. Cluster analysis of RAPD data using the unweighted pair-group method using arithmetic averages (UPGMA) revealed 11 accessions with particularly low similarity values. These were subsequently found to be misidentified Poa species (one each of P. alpina, P. compressa, P. glauca, P. urssulensis and seven P. trivialis). For RAPD data, 62% of the entries were in one large cluster with 46 additional clusters containing one to 13 accessions. For agronomic data, 89% of the entries were in four main clusters. This clustering pattern for RAPD and agronomic data suggested unique genotypes were generally under represented in the collection. The agronomic-based clusters showed some broad separation by accession origin, but in general, origin did not correspond closely with the clustering pattern. The correlation between the RAPD and agronomic-based distance matrices, excluding misidentified accessions, was highly significant (P <0.01) (n = 234, r = - 0.14). However, the correlation represented a relatively small fraction of the total variation, indicating that both molecular and agronomic characterizations were needed to assess overall diversity. C1 Washington State Univ, USDA, Western Reg Plant Introduct Stn, Pullman, WA 99164 USA. UD Dept Golf Assoc, Twin Falls, ID 83303 USA. Smithsonian Inst, NMNH, Dept Bot, Washington, DC 20560 USA. RP Johnson, RC (reprint author), Washington State Univ, USDA, Western Reg Plant Introduct Stn, Pullman, WA 99164 USA. NR 29 TC 24 Z9 29 U1 1 U2 4 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0925-9864 J9 GENET RESOUR CROP EV JI Genet. Resour. Crop Evol. PD AUG PY 2002 VL 49 IS 4 BP 349 EP 361 PG 13 WC Agronomy; Plant Sciences SC Agriculture; Plant Sciences GA 603GG UT WOS:000178550100002 ER PT J AU Naisbit, RE Jiggins, CD Linares, M Salazar, C Mallet, J AF Naisbit, RE Jiggins, CD Linares, M Salazar, C Mallet, J TI Hybrid sterility, Haldane's rule and speciation in Heliconius cydno and H. melpomene SO GENETICS LA English DT Article ID PASSION-VINE BUTTERFLIES; REPRODUCTIVE ISOLATION; DROSOPHILA-SIMULANS; SEXUAL SELECTION; GENE FLOW; EVOLUTION; MIMICRY; ZONES; CHROMOSOMES; PASSIFLORA AB Most genetic studies of Haldane's rule, in which hybrid sterility or inviability affects the heterogametic sex preferentially, have focused on Drosophila. It therefore remains unclear to what extent the conclusions of that work apply more generally, particularly in female-heterogametic taxa such as birds and Lepidoptera. Here we present a genetic analysis of Haldane's rule in Heliconius butterflies. Female F, hybrids between Heliconius melpomene and H. cydno are completely sterile, while males have normal to mildly reduced fertility. In backcrosses of male F-1 hybrids, female offspring range from completely sterile to fully fertile. Linkage analysis using the Z-linked triose-phosphate isomerase locus demonstrates a "large X" (Z) effect on sterility. Expression of female sterility varies among crosses in this and a previous study of Heliconius. Sterility may result from the production of normal but infertile eggs, production of small infertile eggs, or from a complete failure to develop ovarioles, which suggests multiple routes to the evolution of hybrid sterility in these Heliconius species. These results conform to the expectations of the "dominance" rather than "faster male" theories of Haldane's rule and suggest that relatively few loci are responsible. The two species are broadly sympatric and hybridize in the wild, so that female hybrid sterility forms one of several strong but incomplete barriers to gene flow in nature. The effect of female sterility is comparable to that of selection against non-mimetic hybrids, while mate choice forms a much stronger barrier to gene transfer. C1 UCL, Galton Lab, Dept Biol, London NW1 2HE, England. Smithsonian Trop Res Inst, Balboa, Panama. Univ Los Andes, Inst Genet, Bogota, Colombia. RP Mallet, J (reprint author), UCL, Galton Lab, Dept Biol, 4 Stephenson Way, London NW1 2HE, England. EM j.mallet@ucl.ac.uk RI Jiggins, Chris/B-9960-2008; Naisbit, Russell/B-9658-2011; Salazar, camilo/A-1647-2010; mallet, james/B-5114-2008; Linares, Mauricio/I-3509-2016; OI Jiggins, Chris/0000-0002-7809-062X; Naisbit, Russell/0000-0003-0190-9323; Salazar, camilo/0000-0001-9217-6588; Linares, Mauricio/0000-0002-1021-0226; Mallet, James/0000-0002-3370-0367 NR 52 TC 65 Z9 68 U1 5 U2 27 PU GENETICS SOC AM PI BETHESDA PA 9650 ROCKVILLE AVE, BETHESDA, MD 20814 USA SN 0016-6731 J9 GENETICS JI Genetics PD AUG PY 2002 VL 161 IS 4 BP 1517 EP 1526 PG 10 WC Genetics & Heredity SC Genetics & Heredity GA 588WT UT WOS:000177725700014 PM 12196397 ER PT J AU Brouwer, FM Sorensen, SS AF Brouwer, FM Sorensen, SS TI Whole-rock and mineral trace element distributions in Alpine and Franciscan eclogites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract ID SUBDUCTION C1 Univ Bern, Inst Geol, CH-3012 Bern, Switzerland. NMNH, Smithsonian Inst, Dept Mineral Sci, Washington, DC USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2002 VL 66 IS 15A SU 1 BP A105 EP A105 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 583RX UT WOS:000177423400205 ER PT J AU Handler, MR Sorensen, S Vicenzi, EP AF Handler, MR Sorensen, S Vicenzi, EP TI Microanalytical characterisation of hydrothermal fluid interaction with feldspar phenocrysts, Alta andesite, Comstock Lode region, Nevada SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2002 VL 66 IS 15A SU 1 BP A307 EP A307 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 583RX UT WOS:000177423400597 ER PT J AU Wang, PL Rumble, D McCoy, TJ AF Wang, PL Rumble, D McCoy, TJ TI Oxygen isotopic composition of IVA iron meteorites and its implications SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract C1 Carnegie Inst Washington, Geophys Lab, Washington, DC 20005 USA. Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2002 VL 66 IS 15A SU 1 BP A821 EP A821 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 583RX UT WOS:000177423401605 ER PT J AU Wysoczanski, RJ Hauri, EH Gamble, JA Luhr, JF Eggins, S Wright, IC AF Wysoczanski, RJ Hauri, EH Gamble, JA Luhr, JF Eggins, S Wright, IC TI Volatile elements in pillow lava glasses from the Kermadec Arc - Havre Trough and offshore Taupo Volcanic Zone, southwest Pacific SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Victoria Univ Wellington, Sch Earth Sci, Wellington, New Zealand. Australian Natl Univ, Sch Earth Sci, Canberra, ACT 2601, Australia. Natl Inst Water & Atmospher Res, Wellington, New Zealand. RI Wright, Ian/B-9643-2008; Wysoczanski, Richard/I-7730-2012 OI Wright, Ian/0000-0002-6660-0493; NR 0 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD AUG PY 2002 VL 66 IS 15A SU 1 BP A848 EP A848 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 583RX UT WOS:000177423401659 ER PT J AU Allibone, A Wysoczanski, R AF Allibone, A Wysoczanski, R TI Initiation of magmatism during the Cambrian-Ordovician Ross orogeny in southern Victoria Land, Antarctica SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article DE Antarctica; dating; granitoid; orthogneiss; Ross orogeny; Victoria Land ID CENTRAL TRANSANTARCTIC MOUNTAINS; DRY VALLEYS AREA; KOETTLITZ GROUP; TAYLOR VALLEY; GLACIER AREA; PALEO-PACIFIC; MARGIN; GRANITOIDS; EVOLUTION; AUSTRALIA AB Sensitive high-resolution ion-microprobe (SHRIMP) U-Pb zircon dating of four gneissic granitoid intrusions, whose field relationships indicate that they are among the oldest plutonic rocks exposed in the Dry Valleys region of southern Victoria Land, Antarctica, gives ages between 531 10 and 502 9 Ma. Two samples from 1- to 3-km-scale gneissic plutons characterized by the distinctive enrichment in Sr and depletion in Y (DV1b suite) typical of "adakitic" igneous rocks yielded dates of 531 10 Ma and 516 10 Ma, respectively. Two other samples of gneissic, K-feldspar-megacrystic granodiorite intercalated with the Skelton Group country rocks that are characterized by more typical Cordilleran I-type chemistries (DV1a suite) yielded dates of 505 9 Ma and 502 9 Ma, respectively. A fifth sample from the large Bonney pluton (DV1a suite) emplaced at the peak of magmatic activity during the Ross orogeny, gave a date of 499 6 Ma. The new dates indicate that subduction and magmatism associated with the Ross orogeny had begun by ca. 530 Ma along this segment of the East Antarctic margin. They also require cessation by this time of the Neoproterozoic-Cambrian rifting that predated the Ross orogeny. None of the gneissic granitoid plutons was emplaced during a Neoproterozoic Beardmore orogeny, as has been suggested by some previous workers. Emplacement of small plutons characterized by an "adakitic" chemistry, punctuated by folding events, continued for 10-30 m.y. after ca. 530 Ma before major, more typical Cordilleran-style magmatism occurred between 505 and 499 Ma. Large volumes of calc-alkalic plutonic rocks in the Ross orogen south of the Dry Valleys region were emplaced 10-40 m.y. earlier than those in the Dry Valleys region, indicating marked variations in the timing of calc-alkalic granitoid magmatism parallel to the Ross orogen. The full extent and significance of these variations remain to be defined. C1 James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. RP Allibone, A (reprint author), James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia. RI Wysoczanski, Richard/C-2930-2009; Wysoczanski, Richard/I-7730-2012 NR 60 TC 56 Z9 57 U1 0 U2 3 PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER PI COLLEGE STN PA TEXAS A & M UNIV, DEPT GEOLOGY & GEOPHYSICS, COLLEGE STN, TX 77843-3115 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD AUG PY 2002 VL 114 IS 8 BP 1007 EP 1018 DI 10.1130/0016-7606(2002)114<1007:IOMDTC>2.0.CO;2 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 583DA UT WOS:000177389400007 ER PT J AU Benner, LAM Ostro, SJ Hudson, RS Rosema, KD Jurgens, RF Yeomans, DK Campbell, DB Chandler, JF Shapiro, II AF Benner, LAM Ostro, SJ Hudson, RS Rosema, KD Jurgens, RF Yeomans, DK Campbell, DB Chandler, JF Shapiro, II TI Radar observations of asteroid 3908 Nyx SO ICARUS LA English DT Article DE asteroids; radar ID SHAPE; INVERSION; DISCOVERY AB We report Doppler-only (cw) radar observations of basaltic near-Earth asteroid 3908 Nyx obtained at Arecibo and Goldstone in September and October of 1988. The circular polarization ratio of 0.75 +/- 0.03 exceeds similar to90% of those reported among radar-detected near-Earth asteroids and it implies an extremely rough near-surface at centimeter-to-decimeter spatial scales. Echo power spectra over narrow longitudinal intervals show a central dip indicative of at least one significant concavity. Inversion of cw spectra yields two statistically indistinguishable shape models that have similar shapes and dimensions but pole directions that differ by similar to100degrees. We adopt one as our working model and explore its implications. It has an effective diameter of 1.0 +/- 0.15 km and radar and visual geometric albedos of 0.15 +/- 0.075 and 0.16(-0.05)(+0.08). The visual albedo supports the interpretation by D. P. Cruikshank et al. (1991, Icarus 89, 1-13) that Nyx has a thermal inertia consistent with that of bare rock. The model is irregular, modestly asymmetric, and topographically rugged. (C) 2002 Elsevier Science (USA). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99164 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Benner, LAM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 22 TC 15 Z9 15 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2002 VL 158 IS 2 BP 379 EP 388 DI 10.1006/icar.2002.6869 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 592ZK UT WOS:000177966600008 ER PT J AU Campbell, BA AF Campbell, BA TI Comment on "Regolith layer thickness mapping of the moon by radar and optical data," by Y. G. Shkuratov and N. V. Bondarenko SO ICARUS LA English DT Article DE moon; surface; regolith; radar AB In a recent Icarus article, Shkuratov and Bondarenko (2001) propose a model for the depth of the lunar regolith based on 70-cm radar observations and near-infrared spectroscopy. This model treats the regolith as a single homogeneous layer of lossy dust, and ignores scattering by buried rocks. There is also an implicit assumption that the regolith substrate is everywhere of uniform morphology. Radar scattering from this substrate is treated using averaged Fresnel coefficients, with little explanation of how such a model might produce the observed lunar polarization properties. Taken together, these issues weaken the validity of the published regolith depth map. (C) 2002 Elsevier Science (USA). C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 5 TC 6 Z9 6 U1 0 U2 2 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 AUG PY 2002 VL 158 IS 2 BP 560 EP 561 DI 10.1006/icar.2001.6807 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 592ZK UT WOS:000177966600021 ER PT J AU Dalling, JW Muller-Landau, HC Wright, SJ Hubbell, SP AF Dalling, JW Muller-Landau, HC Wright, SJ Hubbell, SP TI Role of dispersal in the recruitment limitation of neotropical pioneer species SO JOURNAL OF ECOLOGY LA English DT Article DE dispersal limitation; gap; seed limitation; seedling distribution pattern; seedling establishment ID GAP-PHASE REGENERATION; TROPICAL FOREST; SEED DISPERSAL; TREE; PATTERNS; COMPETITION; ECOLOGY; LITTER; ESTABLISHMENT; GERMINATION AB 1 We examined the importance of seed dispersal in predicting the pioneer seedling composition in recent gaps in a forest plot on Barro Colorado Island (BCI), Panama. We characterize seed dispersal for 13 taxa from seed rain data collected over 13 years in 200 mesh traps, and for an additional species from germination from soil samples collected in one year. We describe seedling distribution patterns from a complete census of all seedlings of these 14 taxa present in 36 treefall gaps. 2 A maximum likelihood model, incorporating both distance to adult trees and tree size, fitted observed seed rain to traps quite well for all taxa. 3 The ability to predict seedling recruit number per gap varied greatly among taxa. For 8 of 14 taxa, regression models incorporating predicted seed rain were significantly better predictors of seedling recruitment than models in which recruitment probability was assumed constant in all sites. 4 To see if variation in local dispersal patterns determined the community composition of gaps, we examined the relative abundances of these 14 pioneer taxa in the 36 gaps. We found that taxon abundances were significantly positively correlated with abundances predicted from seed dispersal models and seed-seedling regressions for 27 out of 36 gaps. 5 Overall, we find evidence that limited seed dispersal is an important factor contributing, together with factors affecting post-dispersal recruitment success, to seedling distribution patterns in gaps. C1 Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Georgia, Dept Bot, Athens, GA 30602 USA. RP Dalling, JW (reprint author), Univ Illinois, Dept Plant Biol, 265 Morrill Hall,505 S Goodwin Ave, Urbana, IL 61801 USA. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 53 TC 164 Z9 194 U1 2 U2 46 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD AUG PY 2002 VL 90 IS 4 BP 714 EP 727 DI 10.1046/j.1365-2745.2002.00706.x PG 14 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 582TZ UT WOS:000177368400013 ER PT J AU Altshuler, DL Dudley, R AF Altshuler, DL Dudley, R TI The ecological and evolutionary interface of hummingbird flight physiology SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Review DE aerodynamics; biomechanics; evolutionary physiology; flight; hovering; hummingbird ID SEXUAL SIZE DIMORPHISM; HOVERING MODEL HAWKMOTH; TROPICAL HUMMINGBIRDS; OXYGEN-CONSUMPTION; INSECT FLIGHT; GAS-MIXTURES; LEADING-EDGE; BODY-MASS; RUFOUS HUMMINGBIRDS; PHYLOGENETIC TREES AB The hovering ability, rapidity of maneuvers and upregulated aerobic capacity of hummingbirds have long attracted the interest of flight biologists. The range of intra- and interspecific variation in flight performance among hummingbirds, however, is equally impressive. A dominant theme in hummingbird evolution is progressive invasion of higher-elevation habitats. Hypobaric challenge is met behaviorally through compensatory changes in wingbeat kinematics, particularly in stroke amplitude. Over evolutionary time scales, montane colonization is associated with increases in body mass and relative wing area. Hovering ability has been well-studied in several North American hummingbird taxa, yet the broad range of interspecific variation in hummingbird axial and appendicular anatomy remains to be assessed mechanistically. Such varied features as tail length, molt condition and substantial weight change due to lipid-loading can dramatically alter various features of the flight envelope. Compared with our present knowledge of hovering performance in hummingbirds, the mechanics of forward flight and maneuvers is not well understood. Relationships among flight-related morphology, competitive ability and foraging behavior have been the focus of numerous studies on tropical and temperate hummingbirds. Ecologists have hypothesized that the primary selective agents on hummingbird flight-related morphology are the behaviors involved in floral nectar consumption. However, flight behaviors involved in foraging for insects may also influence the evolution of wing size and shape. Several comparisons of hummingbird communities across elevational gradients suggest that foraging strategies and competitive interactions within and among species vary systematically across elevations as the costs of flight change with body size and wing shape. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Altshuler, DL (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. EM colibri@socrates.berkeley.edu OI Altshuler, Douglas/0000-0002-1364-3617 NR 108 TC 68 Z9 69 U1 13 U2 67 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 EI 1477-9145 J9 J EXP BIOL JI J. Exp. Biol. PD AUG PY 2002 VL 205 IS 16 BP 2325 EP 2336 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 590ZW UT WOS:000177855700001 PM 12124359 ER PT J AU Bushmann, PJ Burns, JR Weitzman, SH AF Bushmann, PJ Burns, JR Weitzman, SH TI Gill-derived glands in glandulocaudine fishes (Teleostei : Characidae : Glandulocaudinae) SO JOURNAL OF MORPHOLOGY LA English DT Article DE glandulocaudines; gill gland; chemical signals ID SOCIAL-CONTROL; INSPECTION BEHAVIOR; SWORDTAIL CHARACIN; CORYNOPOMA-RIISEI; MATURATION; INHIBITION; PISCES AB The Glandulocaudinae is a subfamily of neotropical characid fishes from Central and South America. A unifying feature of the subfamily is the caudal gland, found almost exclusively in males. The gland consists of tissue on the base of the caudal fin covered in part by hypertrophied scales. Scale movement as the caudal fin is flexed appears to facilitate the release of chemical compounds from the glandular tissue. We describe here a different structure, found in the gill cavity of mature males in 12 of 17 glandulocaudine genera examined. Termed a gill gland, it develops as a male secondary sex character and appears morphologically suited to release chemical signals. The gland forms by the growth of tissue over and around 4-13 anterior gill filaments on the first gill arch, forming chambers with ventral openings. Within the gland chambers, gill secondary lamellae usually shorten and may disappear. When secondary lamellae persist, simple columnar epithelial cells develop between them. In the absence of secondary lamellae, the gland chambers are lined with a simple cuboidal or columnar epithelium. Gland size and the degree of gill modification vary among species. Gill glands appear absent in five glandulocaudine genera, suggesting character reversals based on current phylogenetic hypotheses and systematic classification. Gill gland morphology suggests that this structure releases chemical compounds into the gill current. The presence of gill glands only in mature males suggests a function in reproduction and/or male aggression. Together with studies of the caudal gland, this research suggests that chemical signals may play important roles in glandulocaudine reproduction. (C) 2002 Wiley-Liss, Inc. C1 Anne Arundel Community Coll, Dept Biol, Arnold, MD 21012 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Bushmann, PJ (reprint author), Anne Arundel Community Coll, Dept Biol, Arnold, MD 21012 USA. NR 28 TC 14 Z9 15 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 0362-2525 J9 J MORPHOL JI J. Morphol. PD AUG PY 2002 VL 253 IS 2 BP 187 EP 195 DI 10.1002/jmor.1120 PG 9 WC Anatomy & Morphology SC Anatomy & Morphology GA 569GQ UT WOS:000176593400007 PM 12112132 ER PT J AU Kensley, B Schotte, M AF Kensley, B Schotte, M TI New species and records of Asellota from the Indian Ocean (Crustacea : Peracarida : Isopoda) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Crustacea; Peracarida; Isopoda; Asellota; Indian Ocean ID MARINE; STENETRIIDAE; FLORIDA; FAMILY AB In this study of asellote Isopoda from the Indian Ocean, 29 species in 11 genera and seven families are recorded. Twenty-one species are described as new: family Gnathostenetroididae, Maresiella aldabrana; family Janiridae, Carpias mossambica; family Joeropsidae, Joeropsis algensis, J. arpedes, J. dimorpha, J. hamatilis, J. lentigo, J. pentagona, J. pleurion; family Pleurocopidae, Pleurocope wilsoni; family Pseudojaniridae, Pseudojanira meganesus; family Santiidae, Santia spicata, S. urospinosa; family Stenetriidae, Hansenium aldabrae, H. expansa, H. remocarpus; Mizothenar serratum, Stenetrium assumentum, S. quinquedens, S. zanzibarica, Stenobermuda brucei. The first record of the family Pleurocopidae (Pleurocope wilsoni) and the genus Mizothenar (family Stenetriidae) from the Indian Ocean are included. Diagnoses of the genera and species are provided, and keys to the Indian Ocean species of most of the genera. The material comes primarily from Aldabra Atoll, the granitic Seychelles islands, Zanzibar Island, the Comoro Islands, and Phuket in Thailand. A few samples are from material of the International Indian Ocean Expedition carried out in the mid-1960s. C1 Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Kensley, B (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 58 TC 16 Z9 16 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD AUG PY 2002 VL 36 IS 12 BP 1421 EP 1461 DI 10.1080/00222930110050401 PG 41 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 579JC UT WOS:000177174000003 ER PT J AU Schmidt, G Zotz, G AF Schmidt, G Zotz, G TI Inherently slow growth in two Caribbean epiphytic species: A demographic approach SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Aspasia; epiphyte; plant size; Panama; RGR; Vriesea ID VRIESEA-SANGUINOLENTA; PLANT SIZE; CARBON; ORCHID AB In relation to the drought-prone and nutrient-poor habitat, vascular epiphytes are routinely referred to as inherently slow-growing plants, although actual evidence is rare. To test this notion we measured in situ growth of the understorey orchid Aspasia principissa and the tank bromeliad Vriesea sanguinolenta, and, for the latter species, also the growth under favourable conditions in the greenhouse. Using growth analysis we show: (1) that in an intraspecific comparison, small to intermediate individuals yield the highest relative,growth rates (RGR) in situ A. principissa: 1.6 10(-3) d(-1); V. sanguinolenta: 3.3 10(-3) d(-1); (2) that the bromeliad reaches maximum size after ca. 15 yr, while the orchid needs at least 20 yr; and (3) small V. sanguinolenta plants exhibit a highly plastic growth response to favourable conditions in the greenhouse, reaching an almost 10-fold increase in RGR. In spite of a substantial increase in growth under more favourable conditions, our results are consistent with the notion that epiphytes are inherently slow growing organisms. C1 Univ Wurzburg, Lehrstuhl Bot 2, D-97082 Wurzburg, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Wurzburg, Lehrstuhl Bot 2, D-97082 Wurzburg, Germany. NR 27 TC 46 Z9 51 U1 3 U2 12 PU OPULUS PRESS UPPSALA AB PI LANNA PA MALMEN, S-740 11 LANNA, SWEDEN SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD AUG PY 2002 VL 13 IS 4 BP 527 EP 534 DI 10.1111/j.1654-1103.2002.tb02079.x PG 8 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 610LN UT WOS:000178961700008 ER PT J AU Laurance, WF AF Laurance, WF TI Hyperdynamism in fragmented habitats SO JOURNAL OF VEGETATION SCIENCE LA English DT Article ID AMAZONIAN FOREST FRAGMENTS; TROPICAL RAIN-FOREST; LANDSCAPE FRAGMENTATION; ECOSYSTEM FUNCTION; TREE COMMUNITIES; NEST PREDATION; EDGE; EXTINCTION; BIRDS; RESPONSES AB Are the dynamics of most ecological processes fundamentally increased in frequency or magnitude in fragmented habitats? Hyperdynamism could alter a wide range of population, community, and landscape phenomena, and appears to be evident in fragmented tropical, temperate, and boreal Communities. I suggest some potential causes and consequences of hyperdynamism, and argue that the responses of many species and ecological processes to habitat fragmentation can be understood in this context. C1 Smithsonian Trop Res Inst, Balboa, Panama. INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. RI Laurance, William/B-2709-2012 NR 97 TC 70 Z9 71 U1 5 U2 18 PU OPULUS PRESS UPPSALA AB PI LANNA PA MALMEN, S-740 11 LANNA, SWEDEN SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD AUG PY 2002 VL 13 IS 4 BP 595 EP 602 DI 10.1111/j.1654-1103.2002.tb02086.x PG 8 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 610LN UT WOS:000178961700015 ER PT J AU McLellan, WA Koopman, HN Rommel, SA Read, AJ Potter, CW Nicolas, JR Westgate, AJ Pabst, DA AF McLellan, WA Koopman, HN Rommel, SA Read, AJ Potter, CW Nicolas, JR Westgate, AJ Pabst, DA TI Ontogenetic allometry and body composition of harbour porpoises (Phocoena phocoena, L.) from the western North Atlantic SO JOURNAL OF ZOOLOGY LA English DT Article DE ontogeny; allometry; harbour porpoise; Phocoena phocoena; energetics ID RATTUS-NORVEGICUS; GROWTH; FUNDY; BAY; DOLPHINS; MUSCLES; SIMILARITY; MORPHOLOGY; MAMMALS; MAINE AB North Atlantic harbour porpoises Phocoena phocoena (L.) face considerable energetic challenges, as they are relatively small marine mammals with an intense reproductive schedule and a cold-water habitat. Postnatal growth of these porpoises was described using ontogenetic allometry and body composition techniques. The cross-sectional sample contained robust calves, immature, and mature porpoises (n = 122) incidentally killed in commercial fishing operations between 1992 and 1998. Total mass and the mass of 26 body components were measured using a standard dissection protocol. Most body components grew similarly in female and male porpoises. Blubber, brain and skull were negatively allometric, while muscle and reproductive tissues exhibited positive allometry. Female heart, liver, intestine and mesenteric lymph node grew at significantly higher rates than in males. Male locomotor muscle and pelvic bones grew significantly faster than in females. High growth rates for visceral and reproductive organs in porpoises, relative to other mammals, may underlie their early maturation and support their intensive, annual reproductive schedule. Relative to other cetaceans, porpoises seem to allocate a larger percentage of their total body mass to blubber. This allocation to blubber, which is greatest in calves (37% of body mass), may provide harbour porpoises with the thermal insulation required to live in cold water. The factors influencing growth rates and differential investments in body composition seem to change at various stages of a porpoise's life. Energy allocation in porpoises seems to shift from an emphasis on developing an insulative blubber layer in young animals to preparing the body for annual reproduction at sexual maturity. C1 Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28403 USA. Duke Univ, Marine Lab, Nicholas Sch Environm, Beaufort, NC 28516 USA. Marine Mammal Pathobiol Lab, Florida Dept Environm Protect, St Petersburg, FL 33711 USA. Smithsonian Inst, Div Mammals, Washington, DC 20560 USA. NE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Woods Hole, MA 02543 USA. RP McLellan, WA (reprint author), Univ N Carolina, Ctr Marine Sci, 601 S Coll Rd, Wilmington, NC 28403 USA. NR 57 TC 56 Z9 60 U1 1 U2 29 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 AUG PY 2002 VL 257 BP 457 EP 471 DI 10.1017/S0952836902001061 PN 4 PG 15 WC Zoology SC Zoology GA 586QE UT WOS:000177595100004 ER PT J AU Schroll, S AF Schroll, S TI Roy Lichtenstein: Brushstrokes; four decades. SO LIBRARY JOURNAL 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 BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 2002 VL 127 IS 13 BP 86 EP 86 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 584WF UT WOS:000177491200060 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Demons and angels: A life of Jacob Epstein. 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 AUG PY 2002 VL 127 IS 13 BP 89 EP 89 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 584WF UT WOS:000177491200068 ER PT J AU Riley, S AF Riley, S TI Ruby river. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst Libs, 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 AUG PY 2002 VL 127 IS 13 BP 145 EP 145 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 584WF UT WOS:000177491200355 ER PT J AU McCafferty, S Bermingham, E Quenouille, B Planes, S Hoelzer, G Asoh, K AF McCafferty, S Bermingham, E Quenouille, B Planes, S Hoelzer, G Asoh, K TI Historical biogeography and molecular systematics of the Indo-Pacific genus Dascyllus (Teleostei : Pomacentridae) SO MOLECULAR ECOLOGY LA English DT Article DE damselfish; Indo-West Pacific; life history evolution; mitochondrial DNA; molecular systematics; phylogeography ID CORAL-REEF FISH; SEX-CHANGE; POPULATION-STRUCTURE; MAXIMUM-LIKELIHOOD; GENETIC-STRUCTURE; MATING SYSTEMS; EVOLUTION; DAMSELFISH; SPECIATION; DISPERSAL AB The phylogeographical and systematic relationships among species in the tropical marine fish genus Dascyllus were inferred using mitochondrial DNA (mtDNA) sequence data. Although our results were generally consistent with previously published phylogenies based on both morphological and mitochondrial data, our broad taxonomic and geographical sampling design revealed novel insights into the phylogenetic history of Dascyllus that had escaped previous notice. These results include: (a) the polyphyletic nature of D. reticulatus mtDNAs, representing two divergent and geographically separated lineages, one shared with D. flavicaudus and the second forming the sister lineage of D. carneus ; (b) the paraphyly of D. trimaculatus relative to the closely related D. abisella ; and (c) phylogeographical structure within the widespread taxa D. aruanus and D. trimaculatus . Application of a molecular clock permits us to posit a causative role for tectonic and oceanic changes regarding some Dascyllus speciation events. Finally, we mapped body size and the presence or absence of protogynous sex change on the mtDNA tree, and tested published hypotheses regarding determinants of the evolution of mating system and protogyny in the genus. Our data rejected a model based on body size but not one based on phylogenetic inertia. The ability to change sex arose once in the ancestor to the entire genus, and was lost once in the ancestor of the D. trimaculatus complex. For taxa that are as geographically widespread as many Indo-Pacific genera, this study highlights the importance of adequate geographical sampling when inferring patterns of species diversification and life history evolution. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Perpignan, Ecole Prat Hautes Etud, CNRS, ESA 8046, F-66860 Perpignan, France. Univ Nevada, Dept Biol, Reno, NV 89557 USA. Univ Hawaii Manoa, Dept Zool, Honolulu, HI 96822 USA. RP Bermingham, E (reprint author), STRL, Unit 0948, APO, AA 34002 USA. NR 70 TC 57 Z9 60 U1 0 U2 16 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD AUG PY 2002 VL 11 IS 8 BP 1377 EP 1392 DI 10.1046/j.1365-294X.2002.01533.x PG 16 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 577XA UT WOS:000177086900012 PM 12144659 ER PT J AU Butt, YM Torres, DF Romero, GE Dame, TM Combi, JA AF Butt, YM Torres, DF Romero, GE Dame, TM Combi, JA TI Astrophysics - Supernova-remnant origin of cosmic rays? SO NATURE LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. Inst Argentino Radioastron, RA-1894 Buenos Aires, DF, Argentina. RP Butt, YM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Torres, Diego/O-9422-2016 OI Torres, Diego/0000-0002-1522-9065 NR 9 TC 36 Z9 36 U1 0 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 1 PY 2002 VL 418 IS 6897 BP 499 EP 499 DI 10.1038/418499a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 579EE UT WOS:000177162800029 PM 12152068 ER PT J AU Moller, AP Jennions, MD AF Moller, AP Jennions, MD TI How much variance can be explained by ecologists and evolutionary biologists? SO OECOLOGIA LA English DT Article DE ecology; effect size; evolution; meta-analysis; sample size ID PUBLICATION BIAS; SEXUAL SELECTION; FLUCTUATING ASYMMETRY; METAANALYSIS; PARADIGM; HERITABILITIES; SIZE AB The average amount of variance explained by the main factor of interest in ecological and evolutionary studies is an important quantity because it allows evaluation of the general strength of research findings. It also has important implications for the planning of studies. Theoretically we should be able to explain 100% of the variance in data, but randomness and noise may reduce this amount considerably in biological studies. We performed a meta-analysis using data from 43 published meta-analyses in ecology and evolution with 93 estimates of mean effect size using Pearson's r and 136 estimates using Hedges' d or g. This revealed that (depending on the exact analysis) the mean amount of variance (r(2)) explained was 2.51-5.42%. The various 95% confidence intervals fell between 1.99 and 7.05%. There was a strongly positive relationship between the fail-safe number (the number of null results needed to nullify an effect) and the coefficient of determination (r(2)) or effect size. Analysis at the level of individual tests of null hypotheses showed that the amount of variance key factors explained differed among fields with the largest amount in physiological ecology, lower amounts in ecology and the lowest in evolutionary studies. In all fields though, the hypothesized relationship (e.g. main effect of a fixed treatment) explained little of the variation in the trait of interest. Our finding has important implications for the interpretation of scientific studies. Across studies, the average effect size reported is between Pearson r=0.180 and 0.193 and Hedges' d=0.631 and 0.721. Thus the average sample sizes needed to conclude that a particular relationship is absent with a power of 80% and alpha=0.05 (two-tailed) are considerably larger than usually recorded in studies of evolution and ecology. For example, to detect r=0.193, the required sample size is 207. C1 Univ Paris 06, Lab Ecol Evolut Parasitaire, CNRS, UMR 7103, F-75252 Paris 05, France. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. RP Moller, AP (reprint author), Univ Paris 06, Lab Ecol Evolut Parasitaire, CNRS, UMR 7103, 7 Quai St Bernard,Case 237, F-75252 Paris 05, France. RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 40 TC 228 Z9 230 U1 5 U2 61 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD AUG PY 2002 VL 132 IS 4 BP 492 EP 500 DI 10.1007/s00442-002-0952-2 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 591EE UT WOS:000177866100002 ER PT J AU Chu, X Dalgarno, A AF Chu, X Dalgarno, A TI Molecular transition moments at large internuclear distances SO PHYSICAL REVIEW A LA English DT Article ID NOBLE GAS MOLECULES; DYNAMIC POLARIZABILITIES; DIPOLE-MOMENTS; POTENTIALS; STATES; ATOMS; SPECTRA AB The behavior of the dipole moments of molecular transitions is analyzed as a function of the internuclear distance R and it is shown that for allowed transitions the departure of the dipole moment from the value for the unperturbed atom varies as R-3 with a coefficient that can be obtained from the dynamic polarizability of one atom evaluated at the unperturbed transition frequency of the other. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Chu, X (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 19 TC 11 Z9 11 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 AUG PY 2002 VL 66 IS 2 AR 024701 DI 10.1103/PhysRevA.66.024701 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 591HA UT WOS:000177872600140 ER PT J AU Gingerich, O AF Gingerich, O TI Kepler's singular harmony SO PHYSICS TODAY LA English DT Letter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD AUG PY 2002 VL 55 IS 8 BP 76 EP 76 DI 10.1063/1.1510308 PG 1 WC Physics, Multidisciplinary SC Physics GA 579KK UT WOS:000177177000039 ER PT J AU Winter, K Holtum, JAM AF Winter, K Holtum, JAM TI How closely do the delta(13)C values of crassulacean acid metabolism plants reflect the proportion of CO(2) fixed during day and night? SO PLANT PHYSIOLOGY LA English DT Article ID CARBON-ISOTOPE DISCRIMINATION; DIFFERENT ENVIRONMENTAL-CONDITIONS; KALANCHOE-DAIGREMONTIANA; VASCULAR EPIPHYTES; CAM PLANTS; PHOTOSYNTHETIC PATHWAYS; DIOXIDE FIXATION; PARTIAL-PRESSURE; LIFE-FORMS; RATIOS AB The extent to which Crassulacean acid metabolism (CAM) plant delta(13)C values provide an index of the proportions of CO(2) fixed during daytime and nighttime was assessed. Shoots of seven CAM species (Aloe vera, Hylocereus monocanthus, Kalanchoe beharensis, Kalanchoe daigremontiana, Kalanchoe pinnata, Vanilla pauciflora, and Xerosicyos danguyi) and two C(3) species (teak [Tectona grandis] and Clusia sp.) were grown in a cuvette and net CO(2) exchange was monitored for g to 51 d. In species exhibiting net dark CO(2) fixation, between 14% and 73.3% of the carbon gain occurred in the dark. delta(13)C values of tissues formed inside the cuvette ranged between -28.7parts per thousand and -11.6parts per thousand, and correlated linearly with the percentages of carbon gained in the light and in the dark. The 8130 values for new biomass obtained solely during the dark and light were estimated as -8.7parts per thousand and -26.9parts per thousand, respectively. For each 10% contribution of dark CO(2) fixation integrated over the entire experiment, the delta(13)C content of the tissue was, thus, approximately 1.8parts per thousand less negative. Extrapolation of the observations to plants previously surveyed under natural conditions suggests that the most commonly expressed version of CAM in the field, "the typical CAM plant," involves plants that gain about 71% to 77% of their carbon by dark fixation, and that the isotopic signals of plants that obtain one-third or less of their carbon in the dark may be confused with C(3) plants when identified on the basis of carbon isotope content alone. C1 Smithsonian Trop Res Inst, Ancon, Panama. James Cook Univ N Queensland, Sch Trop Biol, Dept Trop Plant Sci, Townsville, Qld 4811, Australia. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Ancon, Panama. EM winterk@tivoli.si.edu RI Holtum, Joseph/B-3063-2012 OI Holtum, Joseph/0000-0001-6568-8019 NR 47 TC 94 Z9 98 U1 2 U2 19 PU AMER SOC PLANT BIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD AUG PY 2002 VL 129 IS 4 BP 1843 EP 1851 DI 10.1104/pp.002915 PG 9 WC Plant Sciences SC Plant Sciences GA 585AZ UT WOS:000177502100044 PM 12177497 ER PT J AU Brown, TM Libbrecht, KG Charbonneau, D AF Brown, TM Libbrecht, KG Charbonneau, D TI A search for CO absorption in the transmission spectrum of HD 209458b SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GIANT PLANET TRANSITS; SIGNATURES; TELESCOPE; HD-209458; EXOSPHERE AB We observed one transit of the extrasolar planet HD 209458b with the NIRSPEC spectrograph on the Keck II telescope. Using time series of low-noise observations in the wavelength range 2.0-2.5 mum, we searched for extra absorption from the first-overtone rotation-vibration band of CO near 2.3 mum. This was not detected with a detection limit that fails to test simple models of the planetary atmosphere by a factor of about 3. Great improvements in the detectability of the CO spectrum features could be realized by observing a transit that is centered near stellar meridian passage, and in better weather. Since it appears that similar observations taken under better circumstances might succeed, we describe our analysis procedures in detail. C1 Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brown, TM (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, 3450 Mitchell Lane, Boulder, CO 80307 USA. OI Charbonneau, David/0000-0002-9003-484X NR 19 TC 43 Z9 43 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 AUG PY 2002 VL 114 IS 798 BP 826 EP 832 DI 10.1086/341717 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574PE UT WOS:000176898100004 ER PT J AU Cranmer, SR AF Cranmer, SR TI Coronal holes and the high-speed solar wind SO SPACE SCIENCE REVIEWS LA English DT Review ID ION-CYCLOTRON WAVES; INTERPLANETARY MAGNETIC-FIELD; NONLINEAR ALFVEN WAVES; FARADAY-ROTATION MEASUREMENTS; SLOW MAGNETOSONIC WAVES; VELOCITY DISTRIBUTION-FUNCTIONS; ANISOTROPIC PROTON TEMPERATURE; KELVIN-HELMHOLTZ INSTABILITIES; MODE MAGNETOHYDRODYNAMIC WAVES; REMOTE-SENSING MEASUREMENTS AB Coronal holes are the lowest density plasma components of the Sun's outer atmosphere, and are associated with rapidly expanding magnetic fields and the acceleration of the high-speed solar wind. Spectroscopic and polarimetric observations of the extended corona, coupled with interplanetary particle and radio sounding measurements going back several decades, have put strong constraints on possible explanations for how the plasma in coronal holes receives its extreme kinetic properties. The Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliospheric Observatory (SOHO) spacecraft has revealed surprisingly large temperatures, outflow speeds, and velocity distribution anisotropies for positive ions in coronal holes. We review recent observations, modeling techniques, and proposed heating and acceleration processes for protons, electrons, and heavy ions. We emphasize that an understanding of the acceleration region of the wind (in the nearly collisionless extended corona) is indispensable for building a complete picture of the physics of coronal holes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 589 TC 155 Z9 158 U1 1 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD AUG PY 2002 VL 101 IS 3-4 BP 229 EP 294 DI 10.1023/A:1020840004535 PG 66 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 606CX UT WOS:000178716600001 ER PT J AU Nicolson, DH Gandhi, KN AF Nicolson, DH Gandhi, KN TI Cecil John Saldanha (1926-2002) - In Memoriam SO TAXON LA English DT Biographical-Item C1 Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. Harvard Univ Hebaria, Cambridge, MA 02138 USA. RP Nicolson, DH (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Bot MRC-166, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD AUG PY 2002 VL 51 IS 3 BP 585 EP 587 PG 3 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 603WB UT WOS:000178583000019 ER PT J AU Gallegos, CL Neale, PJ AF Gallegos, CL Neale, PJ TI Partitioning spectral absorption in case 2 waters: discrimination of dissolved and particulate components SO APPLIED OPTICS LA English DT Article ID DIFFUSE ATTENUATION COEFFICIENT; SUBMERSED AQUATIC VEGETATION; NATURAL PHYTOPLANKTON; OPTICAL-PROPERTIES; RHODE RIVER; CHLOROPHYLL; ESTUARY; MATTER; VARIABILITY; NUTRIENTS AB A series of three mathematical procedures is derived to discriminate the light absorption by phytoplankton, colored dissolved organic matter, and nonpigmented particulates in waters in which absorption is dominated by factors other than phytoplankton (i.e., case 2 waters). The procedures utilize normalized absorption cross-sectional spectra of the absorption components and matrix inversion to solve for the coefficients that scale the normalized spectra. The procedures differ in the amount of ancillary measurements incorporated to reduce the variability of the estimates. The procedure that incorporates no ancillary information is expected to be unbiased only over long time periods. Application of the procedures to a 15-day time series of continuously monitored data from the Rhode River, Maryland, revealed the presence of large (approximately twofold) changes in absorption at 440 nm over periods of a few hours. Hourly sampling over a 24-h period confirmed that the changes in measured optical coefficients corresponded to changes in water quality. Errors in estimates of absorption components were of a magnitude consistent with those observed in development of the procedures and confirmed the progressive improvement achieved by incorporation of additional information. Over the time period observed, changes in optical properties appeared to be driven by advective processes. (C) 2002 Optical Society of America. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gallegos@serc.si.edu RI Neale, Patrick/A-3683-2012; OI Gallegos, Charles/0000-0001-5112-0166 NR 38 TC 47 Z9 55 U1 0 U2 2 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JUL 20 PY 2002 VL 41 IS 21 BP 4220 EP 4233 DI 10.1364/AO.41.004220 PG 14 WC Optics SC Optics GA 575WU UT WOS:000176972100002 PM 12148749 ER PT J AU White, M Kochanek, CS AF White, M Kochanek, CS TI Completeness in photometric and spectroscopic searches for clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : clusters : general large-scale structure of universe ID GALAXY FORMATION; REDSHIFT SURVEY; COSMOLOGICAL PARAMETERS; LUMINOSITY FUNCTION; CATALOG; EVOLUTION; UNIVERSE; HALO; BIAS; CONSTRAINTS AB We investigate, using simulated galaxy catalogs, the completeness of searches for massive clusters of galaxies in redshift surveys or imaging surveys with photometric redshift estimates, i.e., what fraction of clusters (M > 10(14) h(-1) M-.) are found in such surveys. We demonstrate that the matched filter method provides an efficient and reliable means of identifying massive clusters even when the redshift estimates are crude. In true redshift surveys the method works extremely well. We demonstrate that it is possible to construct catalogs with high completeness and low contamination, where both vary little with redshift. C1 Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP White, M (reprint author), Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA. EM mwhite@astron.berkeley.edu; ckochanek@cfa.harvard.edu RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 NR 47 TC 26 Z9 26 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2002 VL 574 IS 1 BP 24 EP 37 DI 10.1086/340944 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 575ZK UT WOS:000176978200004 ER PT J AU Woolf, NJ Smith, PS Traub, WA Jucks, KW AF Woolf, NJ Smith, PS Traub, WA Jucks, KW TI The spectrum of earthshine: A pale blue dot observed from the ground SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; Moon; planetary systems AB We report the visible reflection spectrum of the integrated Earth, illuminated as it would be seen as a spatially unresolved extrasolar planet. The spectrum was derived from observation of lunar earthshine in the range 4800-9200 Angstrom at a spectral resolution of about 600. We observe absorption features of ozone, molecular oxygen, and water. We see enhanced reflectivity at short wavelengths from Rayleigh scattering and apparently negligible contributions from aerosol and ocean water scattering. We also see enhanced reflectivity at long wavelengths starting at about 7300 Angstrom, corresponding to the well-known red reflectivity edge of vegetation because of its chlorophyll content; however, this signal is not conclusive because of the breakdown of our simple model at wavelengths beyond 7900 Angstrom. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Woolf, NJ (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NR 6 TC 131 Z9 132 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 JUL 20 PY 2002 VL 574 IS 1 BP 430 EP 433 DI 10.1086/340929 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 575ZK UT WOS:000176978200036 ER PT J AU Heyl, JS AF Heyl, JS TI Low-mass X-ray binaries may be important laser interferometer gravitational-wave observatory sources after all SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational waves; stars : neutron; stars : oscillations ID MILLISECOND RADIO PULSARS; ACCRETING NEUTRON-STARS; R-MODE INSTABILITY; EVOLUTION; RADIATION; RUNAWAY AB Andersson et al. and Bildsten proposed that the spin of accreting neutron stars is limited by the removal of angular momentum by gravitational radiation that 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 as a result of 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 are 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 that 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 the Laser Interferometer Gravitational-Wave Observatory may be large. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heyl, JS (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 51,60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 26 Z9 26 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2002 VL 574 IS 1 BP L57 EP L60 DI 10.1086/342263 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 575ZL UT WOS:000176978300013 ER PT J AU Kuchner, MJ Lecar, M AF Kuchner, MJ Lecar, M TI Halting planet migration in the evacuated centers of protoplanetary disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; circumstellar matter; planetary systems : formation; planetary systems : protoplanetary disks; stars : formation ID HERBIG AE/BE STARS; YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; MAGNETOROTATIONAL INSTABILITY; SYSTEMS; SIMULATIONS; EVOLUTION; ORIGIN; NEBULA AB Precise Doppler searches for extrasolar planets find a surfeit of planets with orbital periods of 3-4 days and no planets with orbital periods less than 3 days. The circumstellar distance R-0, where small grains in a proto- planetary disk reach sublimation temperatures (similar to1500 K), corresponds to a period of 6 days. Interior to, R-0 turbulent accretion due to magnetorotational instability may evacuate the disk center. We suggest that planets with orbital periods of 3-4 days are so common because migrating planets halt once this evacuated region contains the sites of their exterior 2 : 1 Lindblad resonances. 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 43 TC 41 Z9 42 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2002 VL 574 IS 1 BP L87 EP L89 DI 10.1086/342370 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 575ZL UT WOS:000176978300021 ER PT J AU Peslier, AH Luhr, JF Post, J AF Peslier, AH Luhr, JF Post, J TI Low water contents in pyroxenes from spinel-peridotites of the oxidized, sub-arc mantle wedge SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE water; Fourier transform infrared spectroscopy; pyroxene group; mantle; xenoliths ID NOMINALLY ANHYDROUS MINERALS; OVERLYING SUBDUCTION ZONES; OXIDATION-STATE; TECTONIC TERRANES; OXYGEN FUGACITY; EARTHS MANTLE; VENT LOCATION; HYDROGEN; PRESSURE; OH AB Pyroxene water contents measured by Fourier transform infrared spectrometry for Mexican and Simcoe (WA, USA) spinel-peridotite xenoliths range from 140 to 528 ppm in clinopyroxenes and 39 to 265 ppm in orthopyroxenes. Correlations between these water contents and major-element compositional data for the pyroxenes, associated spinels, and whole-rock xenoliths demonstrate that these water contents record mantle values that have not been perturbed since the xenoliths were brought to the surface by their host magmas. Broad positive correlations of pyroxene water contents with whole-rock Al2O3 are consistent with water behaving as an incompatible element during peridotite melting. The main control on the range of pyroxene water contents, however, appears to be the redox state of the peridotite, because estimates of oxygen fugacity from Mossbauer (Simcoe) and microprobe data (Mexico) on spinels are negatively correlated with water contents. This is consistent with the dominant mechanism of H incorporation into pyroxene, which is dependent on the oxidation-reduction of iron. Metasomatism of sub-arc mantle-wedge peridotites by oxidized fluids or melts rising from the slab raises the oxygen fugacity of the peridotites, and where temperature is high enough, induces them to partially melt. The oxidation, in turn, lowers the solubility of water in the peridotite minerals, causing more than half of the original water to be expelled. That water enters the hydrous partial melts and these ascend through the lithosphere to feed the arc magmatic system in the upper crust. Low water contents in pyroxenes from sub-arc mantle-wedge peridotites, such as those from Simcoe and some western Mexican sites, therefore appear to be complementary to the high water contents that characterize subduction-zone magmas and fuel their explosive eruptions. An estimate of water budget in subduction zones, however, indicates that the amount of water coming from the dehydration of mantle-wedge anhydrous minerals probably accounts for less than 5% of the total water present in subduction-related magmas. The high water contents of arc magmas thus are mainly attributed to fluids or melts from the slab proper. The relatively dry sub-arc mantle wedge appears to be an effective medium through which subducted water is transported from slabs toward the surface. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Peslier, AH (reprint author), Univ Houston, Texas Ctr Superconduct, Houston, TX 77204 USA. RI Peslier, Anne/F-3956-2010 NR 56 TC 126 Z9 151 U1 1 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JUL 15 PY 2002 VL 201 IS 1 BP 69 EP 86 AR PII S0012-821X(02)00663-5 DI 10.1016/S0012-821X(02)00663-5 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 572NY UT WOS:000176782800007 ER PT J AU Mebel, AM Halasz, GJ Vibok, A Alijah, A Baer, M AF Mebel, AM Halasz, GJ Vibok, A Alijah, A Baer, M TI Quantization of the 3x3 nonadiabatic coupling matrix for three coupled states of the C2H molecule SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID DIABATIC TRANSFORMATION MATRIX; SINGLE-SURFACE APPROXIMATIONS; UNUSUAL CONICAL INTERSECTIONS; BORN-OPPENHEIMER EQUATION; POTENTIAL-ENERGY SURFACES; AB-INITIO; SCATTERING PROCESSES; ELECTRONIC STATES; REACTIVE SYSTEMS; GEOMETRIC PHASE AB The three ab initio nonadiabatic coupling terms related to the three strongly coupled states of the C2H molecule, i.e., 2 (2)A('), 3 (2)A('), and 4 (2)A('), were studied applying the line integral technique [M. Baer, Chem. Phys. Lett. 35, 112 (1975)]. The following was verified: (1) Due to the close proximity of the conical intersections between these three states, two-state quantization cannot always be satisfied between two successive states. (2) It is shown that in those cases where the two-state quantization fails a three-state quantization is satisfied. This three-state quantization is achieved by applying the 3x3 nonadiabatic coupling matrix that contains the three relevant nonadiabatic coupling terms. The quantization is shown to be satisfied along four different contours (in positions and sizes) surrounding the relevant conical intersections. (C) 2002 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Soreq NRC, Dept Appl Math & Phys, IL-81800 Yavne, Israel. Univ Debrecen, Inst Math & Informat, Debrecen, Hungary. Univ Debrecen, Dept Theoret Phys, Debrecen, Hungary. Univ Bielefeld, Dept Chem, D-4800 Bielefeld, Germany. RP Baer, M (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Mebel, Alexander/A-5234-2009; Alijah, Alexander/A-4079-2013 OI Alijah, Alexander/0000-0002-4915-0558 NR 59 TC 29 Z9 29 U1 1 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 15 PY 2002 VL 117 IS 3 BP 991 EP 1000 DI 10.1063/1.1483854 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 569KA UT WOS:000176600500004 ER PT J AU Heyl, JS Shaviv, NJ AF Heyl, JS Shaviv, NJ TI QED and the high polarization of the thermal radiation from neutron stars SO PHYSICAL REVIEW D LA English DT Article ID X-RAY POLARIMETER; MAGNETIC-FIELD; RADIO PULSARS; VACUUM; BIREFRINGENCE; LIGHT; DICHROISM; DETECT AB The thermal emission of strongly magnetized neutron-star atmospheres is thought to be highly polarized. However, because of the different orientations of the magnetic field over the surface of the neutron star (NS), it is commonly assumed that the net observed polarization will be significantly reduced as the polarization from different regions will cancel each other. We show that the birefringence of the magnetized QED vacuum decouples the polarization modes in the magnetosphere; therefore, the direction of the polarization follows the direction of the magnetic field up to a large distance from the stellar surface. At this distance, the rays that leave the surface and are destined for our detectors pass through only a small solid angle; consequently, the polarization direction of the emission originating in different regions will tend to align together. The net observed polarization of the thermal radiation of NSs should therefore be very large. Measurement of this polarization will be the first direct evidence of the birefringence of the magnetized vacuum due to QED and a direct probe of behavior of the vacuum at magnetic fields of order of and above the critical QED field of 4.4x10(13) G. The large observable polarization will also help us learn more about the atmospheric properties of NSs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. RP Harvard Smithsonian Ctr Astrophys, MS-51,60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 27 Z9 27 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUL 15 PY 2002 VL 66 IS 2 AR 023002 DI 10.1103/PhysRevD.66.023002 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 581HJ UT WOS:000177285600006 ER PT J AU Gingerich, O AF Gingerich, O TI The correspondence of John Flamsteed, first astronomer royal, vol 3, 1703-1719 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 JUL 11 PY 2002 VL 418 IS 6894 BP 128 EP 129 DI 10.1038/418128a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 571GV UT WOS:000176710400018 ER PT J AU Eff-Darwich, A Korzennik, SG Jimenez-Reyes, SJ AF Eff-Darwich, A Korzennik, SG Jimenez-Reyes, SJ TI Inversion of the internal solar rotation rate SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : interior; Sun : rotation ID ANGULAR-MOMENTUM EVOLUTION; STELLAR RADIATIVE ZONES; DIFFERENTIAL ROTATION; STARS; MODELS; CORE; OSCILLATIONS; PARAMETERS; IPHIR; SUN AB Accurate determination of the rotation rate in the inner radiative zone (0.2 < r/R-. < 0.5) of the Sun from helioseismic observations requires rotational frequency splittings of exceptional quality. Indeed, only the very low degree modes are sensitive to the dynamics of the deep interior. Low- and intermediate-degree splittings have been estimated from a variety of instruments and different data analysis procedures. Therefore, it is not surprising that these determinations present significant differences. We have attempted to build consistent data sets to constrain the dynamics of the solar core, excluding features in the data that are not common to all sets as well as excluding modes for frequencies for which such measurements are not reliable. Our inferences of the solar internal rotation pro le were obtained from a full two-dimensional numerical inversion based on the optimal mesh distribution methodology, a variant of the regularized least-squares technique. Our results show that the radiative zone rotates at a rate of approximately 435 nHz, slowing down slightly in the core (r/R-. < 0.35). We also did not find any significant angular differential rotation below the base of the convective zone (r/R-. &AP;0.7). We can rule out any departure of the rotation rate in the solar deep interior, 0.2 < r/R-. < 0.4, by more than 20% of the surface rotation rate at midlatitude. This result is in clear disagreement with the theoretical hydrodynamical models that expect a much faster rotation rate in the solar core, some 10-50 times faster than the surface rate. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, E-38205 Tenerife, Canary Isl, Spain. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Eff-Darwich, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Jimenez Reyes, Sebastian/0000-0002-0317-4247 NR 32 TC 33 Z9 33 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2002 VL 573 IS 2 BP 857 EP 863 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 570MX UT WOS:000176663000037 ER PT J AU Rubidge, BS Sidor, CA AF Rubidge, BS Sidor, CA TI On the cranial morphology of the basal therapsids Burnetia and Proburnetia (Therapsida : burnetiidae) SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID PRIMITIVE CYNODONT PROCYNOSUCHUS; SOUTH-AFRICA; EVOLUTION; GONDWANA AB The poorly known genera Burnetia and Proburnetia, which are the only members of the therapsid family Burnetiidae, are redescribed and revised generic diagnoses are provided. Both genera are similar in having a prominent antorbital depression, a parasagittal ridge on the basicranial taunts of the pterygoid that extends from the transverse processes to the basisphenoid, a small temporal fenestra with no external area for adductor muscle attachment, and the same complement of bony protuberances on the skull roof including characteristic posteriorly projecting supratemporal "horns" formed by the squamosal and parietal bones. The morphology identified here is consistent with grouping the Burnetiidae in the Biarmosuchia, rather than in the Dinocephalia or Gorgonopsia as has been previously suggested. C1 Univ Witwatersrand, Bernard Price Inst Palaeontol Res, ZA-2050 Wits, South Africa. Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol, Washington, DC 20560 USA. RP Rubidge, BS (reprint author), New York Inst Technol, New York Coll Osteopath Med, Dept Anat, Old Westbury, NY 11568 USA. EM 106gar@cosmos.wits.ac.za; casidor@iris.nyit.edu OI Rubidge, Bruce/0000-0003-2477-1873 NR 34 TC 18 Z9 20 U1 0 U2 2 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD JUL 8 PY 2002 VL 22 IS 2 BP 257 EP 267 DI 10.1671/0272-4634(2002)022[0257:OTCMOT]2.0.CO;2 PG 11 WC Paleontology SC Paleontology GA 572KA UT WOS:000176772200004 ER PT J AU Arroyo-Cabrales, J Gregorin, R Schlitter, DA Walker, A AF Arroyo-Cabrales, J Gregorin, R Schlitter, DA Walker, A TI The oldest African molossid bat cranium (Chiroptera : Molossidae) SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID OUTGROUPS; PROCONSUL; HOMOLOGY; KENYA AB A fossil cranium from Rusinga Island, Kenya, is described as a new species of free-tailed hat, Tadarida rusingae (Chiroptera, Molossidae). The sediments where the skull was found are dated by Potassium-Argon assay at about 17.5-18.0 million years before present (early Miocene). Comparisons with fossil molossids and all the extant species of Tadarida show that T. rusingae is distinguished by its large size, well developed posterior sagittal crest, deeply domed palate, and several features of the Upper molars. This skull represents one of the most complete fossil molossid bats known. C1 INAH, Lab Paleozool, Mexico City 06060, DF, Mexico. Smithsonian Inst, Natl Museum Nat Hist, Biodivers Programs Off, Washington, DC 20560 USA. Univ Sao Paulo, Museu Zool, BR-04299970 Sao Paulo, Brazil. Texas A&M Univ, Dept Wildlife & Fisheries Sci, Texas Cooperat Wildlife Collect, College Stn, TX 77843 USA. Penn State Univ, Dept Anthropol & Biol, University Pk, PA 16803 USA. RP Arroyo-Cabrales, J (reprint author), INAH, Lab Paleozool, Moneda 16,Col Ctr, Mexico City 06060, DF, Mexico. RI Santos Pompeu, Paulo/G-8032-2014; Gregorin, Renato/D-8072-2016; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 NR 42 TC 8 Z9 9 U1 2 U2 3 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD JUL 8 PY 2002 VL 22 IS 2 BP 380 EP 387 DI 10.1671/0272-4634(2002)022[0380:TOAMBC]2.0.CO;2 PG 8 WC Paleontology SC Paleontology GA 572KA UT WOS:000176772200014 ER PT J AU Woodman, N AF Woodman, N TI A new species of small-eared shrew from Colombia and Venezuela (Mammalia : Soricomorpha : Soricidae : genus Cryptotis) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID INSECTIVORA; ANDES AB Populations of small-eared shrews inhabiting the northern Cordillera Oriental of Colombia and adjoining Venezuelan highlands in the vicinity of Paramo de Tama have been referred alternatively to Cryptotis thomasi or Cryptotis meridensis. Morphological and morphometrical study of this population indicates that it belongs to neither taxon, but represents a distinct, previously unrecognized species. I describe this new species as Cryptotis tamensis and redescribe C. meridensis. Recognition of the population at Paramo de Tama as a separate taxon calls into question the identities of populations of shrews currently represented only by single specimens from Cerro Pintado in the Sierra de Perija, Colombia, and near El Junquito in the coastal highlands of Venezuela. C1 Natl Museum Nat Hist, USGS, Patuxent Wildlife Res Ctr, Smithsonian Inst, Washington, DC 20013 USA. RP Woodman, N (reprint author), Natl Museum Nat Hist, USGS, Patuxent Wildlife Res Ctr, Smithsonian Inst, POB 37012,NHB 378,MRC-111, Washington, DC 20013 USA. NR 53 TC 11 Z9 21 U1 1 U2 2 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 JUL 2 PY 2002 VL 115 IS 2 BP 249 EP 272 PG 24 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 571AK UT WOS:000176692500001 ER PT J AU Ivanov, VA Bigatti, G Penchaszadeh, PE Norenburg, JL AF Ivanov, VA Bigatti, G Penchaszadeh, PE Norenburg, JL TI Malacobdella arrokeana (Nemertea : Bdellonemertea), a new species of nemertean from the Southwestern Atlantic Ocean entocommensal in Panopea abbreviata (Bivalvia, Heterodonta, Hiatellidae) in Argentina SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Malacobdella arrokeana, a new species of entocommensal nemertean is described from the mantle cavity of the bivalve Panopea abbreviata in Argentine waters. This discovery expands the distribution of the genus, including the Southern Hemisphere for the first time, and represents a new host record. Malacobdella arrokeana can be differentiated from all other species in the genus by the following combination of characters: worm size, length of rhynchocoel, proboscis and retractor muscle of proboscis, gonad distribution and coloration, and position of excretory pores. C1 Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Ciencias Biol, RA-1428 Buenos Aires, DF, Argentina. Consejo Nacl Invest Cient & Tecn, Buenos Aires, DF, Argentina. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Ivanov, VA (reprint author), Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Ciencias Biol, Ciudad Univ,Pabellon 2,Piso 4, RA-1428 Buenos Aires, DF, Argentina. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 27 TC 10 Z9 11 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL 2 PY 2002 VL 115 IS 2 BP 359 EP 367 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 571AK UT WOS:000176692500008 ER PT J AU Kornicker, LS Harrison-Nelson, E AF Kornicker, LS Harrison-Nelson, E TI Ontogeny of Rutiderma darbyi (Crustacea : Ostracoda : Myodocopida : Rutidermatidae) and comparisons with other Myodocopina SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The carapaces and appendages of instars I-IV of Rutiderma darbyi Kornicker, 1983, are described and illustrated. The species has five growth stages including a single stage for the adult. A key to identification of stages by differences in appendage morphologies is presented. The morphologies of appendages at each stage of R. darbyi and R. arx Kornicker, 1992 are compared and found quite similar indicating that the two species develop in the same manner. The numbers of bristles on the 9th joint of the 2nd antenna of species of Rutiderma are useful for identifying the stage of development: 2 bristles on instar I, 3 on instar II, 4 on instar IV, and 5 on instar V. Natatory hairs are absent on bristles of the exopodite of the 2nd antenna of juveniles and present on adults; this distribution is useful for identifying them, and also indicates that the juveniles are restricted to the substrate. The presence of both a greater number of natatory bristles and a stouter protopodite on adult male rutidermatids indicate that the adult male is a stronger swimmer than the adult female. A similarity in the distribution of bristles on the 1st antennae and 6th and 7th limbs of instars I-III of R. darbyi (Rutidermatidae), which has five growth stages, and Skogsbergia lerneri (Kornicker, 1958) (Cypridinidae), which has six growth stages, suggests that the extra stage in species having six stages is added after instar III. The total number of bristles, claws, and teeth on appendages of each stage of R. darbyi (Rutidermatidae: Rutidermatinae), S. lerneri (Cypridinidae: Cypridininae), Gigantocypris muelleri Skogsberg, 1920 (Cypridinidae: Gigantocypridininae), and Tetragonodon rex Kornicker & Harrison-Nelson, 1999 (Philomedidae: Pseudophilomedinae), are compared. The rate of increase of the total number of bristles, claws and teeth at each stage is greater in the earlier stages of R. darbyi, S. lerneri, and T. rex, but greater in the later stages of G. muelleri, primarily because of a large increase in the number of bristles on the 7th limb of G. muelleri in the later stages. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 53 TC 1 Z9 1 U1 0 U2 2 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 JUL 2 PY 2002 VL 115 IS 2 BP 426 EP 471 PG 46 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 571AK UT WOS:000176692500016 ER PT J AU Thompson, FG Hershler, R AF Thompson, FG Hershler, R TI Two genera of North American freshwater snails: Marstonia Baker, 1926, resurrected to generic status, and Floridobia, new genus (Prosobranchia : Hydrobiidae : Nymphophilinae) SO VELIGER LA English DT Article ID GASTROPODA C1 Univ Florida, Florida Museum Nat Hist, Div Malacol, Gainesville, FL 32611 USA. Smithsonian Inst, Ntl Museum Nat Hist, Dept Syst Biol, Washington, DC 20560 USA. RP Thompson, FG (reprint author), Univ Florida, Florida Museum Nat Hist, Div Malacol, Gainesville, FL 32611 USA. NR 12 TC 8 Z9 8 U1 0 U2 2 PU CALIF MALACOZOOLOGICAL SOC INC PI SANTA BARBARA PA SANTA BARBARA MUSEUM NATURAL HISTORY, 2559 PUESTA DEL SOL RD, SANTA BARBARA, CA 93105 USA SN 0042-3211 J9 VELIGER JI Veliger PD JUL 2 PY 2002 VL 45 IS 3 BP 269 EP 271 PG 3 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 571HP UT WOS:000176712200013 ER PT J AU Kelloff, CL Skog, J Adamkewicz, L Werth, CR AF Kelloff, CL Skog, J Adamkewicz, L Werth, CR TI Differentiation of Eastern North American Athyrium filix-femina taxa: Evidence from allozymes and spores SO AMERICAN FERN JOURNAL LA English DT Article ID POLYSTICHUM DRYOPTERIDACEAE; HOMOSPOROUS FERNS; GENETIC-VARIATION; SPECIES CONCEPTS; HYBRID SWARMS; PTERIDOPHYTES; DELIMITATION; POPULATIONS AB Athyrium filix-femina (Lady Fern) comprises a complex of homoploid (n = 40) taxa, distributed over much of the northern hemisphere and extending into South America, whose evolutionary relationships are poorly understood and whose taxonomic treatment is problematic. The A. filix-femina complex of North America comprises as many as four taxa with overlapping ranges and provides an especially suitable context for exploring patterns and processes of divergent evolution and its taxonomic consequences in ferns. We addressed differentiation of two eastern North American taxa distinguished on the basis of growth form, frond shape, and spore color, and most recently treated as varieties A. angustum and A. asplenioides (Northern and Southern Lady Fern respectively). Although, these two taxa have been long perceived as closely related, they have been known to intergrade and recombine to form a hybrid zone in their relatively narrow region of overlap. This perception is supported by the data from the present study. Collections from 17 populations, 9 of A. angustum from Quebec to Pennsylvania and 8 of A. asplenioides from New Jersey to North Carolina, were examined for spores using LM, SEM, and TEM, and/or allozymes (16 loci coding 10 enzymes). The two taxa exhibited highly distinct perispore surfaces: all A. angustum individuals had papillose surfaces, whereas most A. asplenioides individuals were rugose with a reticulum of inflated folds. Spores from the northernmost A. asplenioides population sampled (Shirley, NJ) showed varying degrees of intermediacy suggestive of introgressive hybridization with A. angustum. Levels of allozyme polymorphism in populations (means: P=36.5%, A=1.97, H-E=0.129) were near means for angiosperms and ferns. Genotype frequencies at most loci in all populations were in Hardy-Weinberg equilibrium indicating an outcrossing mating system. Most alleles were shared among all populations. However, at the four most polymorphic loci (Idh-1, Pgi-2, Pgm-2, and Tpi-2) allele frequencies were significantly divergent between populations of A. angustum and A. asplenioides, especially Idh-1 which approached fixation for alternate alleles. Values for F-ST ranged from 0.008 to 0.459 for individual loci (0.255 across loci) with especially high values for Idh-1, Pgi-2, Pgm-2, and Tpi-2. Hierarchical FST analysis indicated that differences between the two taxa (F-XY=0.216) accounted for most allele frequency divergence among populations (F-XY=0.238). UPGMA analysis of paired Rogers' Similarity (S) values resulted in two principal clusters each comprising populations of one taxon. Populations of A. angustum and A. asplenioides were joined within their clusters at S=0.938 and S=0.945 respectively, while the two taxon clusters were joined at S=0.848. The spore and isozyme data indicate substantial divergence between A. angustum and A. asplenioides, suggesting that they merit distinction at the rank of subspecies or species. Additional study of populations in their region of sympatry is required to determine the nature and extent of hybridization. C1 George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. Smithsonian Inst, US Natl Herbarium, Washington, DC 20560 USA. Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. RP Kelloff, CL (reprint author), George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. NR 66 TC 2 Z9 2 U1 2 U2 5 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 USA SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD JUL-SEP PY 2002 VL 92 IS 3 BP 185 EP 213 DI 10.1640/0002-8444(2002)092[0185:DOENAA]2.0.CO;2 PG 29 WC Plant Sciences SC Plant Sciences GA 609MY UT WOS:000178910600001 ER PT J AU Ceruzzi, PE AF Ceruzzi, PE TI From whirlwind to MITRE: the R&D story of the SAGE Air Defense computer. SO ANNALS OF SCIENCE LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. RP Ceruzzi, PE (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, MRC 311, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0003-3790 J9 ANN SCI JI Ann. Sci. PD JUL PY 2002 VL 59 IS 3 BP 327 EP 328 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 561RD UT WOS:000176155500005 ER PT J AU Hall, JPW Harvey, DJ AF Hall, JPW Harvey, DJ TI A phylogenetic review of Charis and Calephelis (Lepidoptera : Riodinidae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Calephelis; Charis; cladistics; foodplants; neotropics ID REVISION; LIMITS AB A phylogenetic analysis of the Neotropical riodinid butterfly genera Charis Hubner and Calephelis Grote & Robinson is presented. Cladistic analyses using 31 characters of male and female genitalia and external facies generated cladograrns indicating that Charis is paraphyletic with respect to Calephelis, The analyses highlight the existence of four major clades, the ocellata Hewitson, cleonus Stoll, anius Cramer, and virginiensis Guerin-Meneville groups, which we treat as genera. The generic names Charis and Calephelis are applicable to the last two groups, but new genera are described for the first two: Seco n. gen. for the ocellata group and Detritivora n. gen, for the cleonus group. Each genus is diagnosed and provided with illustrations of representative adults and male and female genitalia, a synonymic checklist and list of all known foodplants. The following taxa are misplaced in the analyzed clade: aerigera Stichel and xanthosa Stichel axe transferred from Charis to Emesis F. (n. combs.), and myrtis H. Druce is transferred from Charis to Exoplisia Godman & Salvin (n. combs.). Charis irina Stichel is synonymized with Charis iris Staudinger (n. syn.) and Charis cadytis acroxantha Stichel is synonymized with nominate C. cadytis Hewitson (n. syn,). The taxon candiope H. Druce is transferred from Charis to Calephelis for the first time (n. comb.) and iris and velutina Godman and Salvin are returned to Calephelis from Charis (rev. combs.). 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 41 TC 6 Z9 7 U1 0 U2 0 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD JUL PY 2002 VL 95 IS 4 BP 407 EP 421 DI 10.1603/0013-8746(2002)095[0407:APROCA]2.0.CO;2 PG 15 WC Entomology SC Entomology GA 600CQ UT WOS:000178373400001 ER PT J AU Da Costa, GS Armandroff, TE Caldwell, N AF Da Costa, GS Armandroff, TE Caldwell, N TI The dwarf spheroidal companions to M31: WFPC2 observations of Andromeda III SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : dwarf; galaxies : individual (Andromeda III); galaxies : photometry; galaxies : stellar content; Local Group ID STAR-FORMATION HISTORY; HORIZONTAL-BRANCH STARS; SURFACE-BRIGHTNESS PROFILES; CHARGE-TRANSFER EFFICIENCY; COLOR MAGNITUDE DIAGRAM; GLOBULAR-CLUSTER SYSTEM; CARINA DSPH GALAXY; STELLAR POPULATIONS; VARIABLE-STARS; LOCAL GROUP AB The Hubble Space Telescope Wide Field Planetary Camera 2 has been used to image Andromeda III, a dwarf spheroidal ( dSph) companion to M31. The resulting color-magnitude diagrams ( CMDs) reveal for the first time the morphology of the horizontal branch (HB) in this dwarf galaxy. We find that like Andromeda I and Andromeda II, and like most of the Galactic dSph companions, the HB morphology of And III is predominantly red, redder indeed than that of both And I and And II, despite And III having a lower mean metallicity. The And III HB morphology is also somewhat redder than that of the Galactic dSph Draco, which has a similar mean abundance to And III. We interpret this red HB morphology as indicating that the bulk of the And III population is similar to3 Gyr younger than the age of the majority of Galactic globular clusters. Nevertheless, the And III CMD does reveal the presence of a few blue HB stars, and a number of RR Lyrae variables are also evident in the data. This indicates that And III does contain an old population of age comparable to that of the Galactic globular clusters. There is no evidence, however, for any young stars in And III despite a claimed association between this dSph and an H I cloud. As was the case for And II, but not And I, no radial gradient was detected in the And III HB morphology. The mean V magnitude of the HB is 25.06 +/- 0.04, leading to (m - M)(0) = 24.38 +/- 0.06 for this dwarf. And III is then similar to75 kpc from the center of M31, comparable to the Galactocentric distances of Sculptor and Draco. Comparison with standard globular cluster red giant branches indicates a mean abundance for And III of h [Fe/ H] = -1.88 +/- 0.11, the lowest mean abundance of any of M31's companions. This value, however, is consistent with the absolute magnitude mean abundance relation followed by dSph galaxies. The same comparison yields an intrinsic abundance dispersion for And III of sigma(int) ([Fe/H]) = 0.12, a low value compared to And I and And II and to the Galactic dSph's of comparable luminosity to And III. If confirmed by future spectroscopic studies, this low value would suggest that And III retained relatively little of the enrichment products generated during its evolutionary history. The list of candidate variables reveals one definite and one probable anomalous Cepheid variable star in And III. Such variables are common in Galactic dSph's, so their discovery in And III is not unexpected. C1 Australian Natl Univ, Inst Adv Studies, Sch Phys Astron & Astrophys, Weston, ACT 2611, Australia. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Da Costa, GS (reprint author), Australian Natl Univ, Inst Adv Studies, Sch Phys Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia. NR 79 TC 30 Z9 30 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2002 VL 124 IS 1 BP 332 EP 348 DI 10.1086/340965 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 563UA UT WOS:000176272900020 ER PT J AU Paulson, DB Saar, SH Cochran, WD Hatzes, AP AF Paulson, DB Saar, SH Cochran, WD Hatzes, AP TI Searching for planets in the Hyades. II. Some implications of stellar magnetic activity SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (Hyades); planetary systems : general; stars : activity; stars : chromospheres; techniques : radial velocities ID LOWER MAIN-SEQUENCE; EXTRA-SOLAR PLANETS; LATE-TYPE STARS; SUN-LIKE STARS; RADIAL-VELOCITY; COOL STARS; CHROMOSPHERIC EMISSION; ROTATIONAL VELOCITIES; CORALIE SURVEY; NEARBY STARS AB The Hyades constitute a homogeneous sample of stars ideal for investigating the dependence of planet formation on the mass of the central star. Because of their youth, Hyades members are much more chromospherically active than stars traditionally surveyed for planets using high-precision radial velocity techniques. Therefore, we have conducted a detailed investigation of whether magnetic activity of our Hyades target stars will interfere with our ability to make precise radial velocity (v(rad)) searches for substellar companions. We measure chromospheric activity (which we take as a proxy for magnetic activity) by computing the equivalent of the R'(HK) activity index (which is corrected for photospheric contributions) from the Ca II K line. The value of [R'(HK)] is not constant in the Hyades: we confirm that it decreases with increasing temperature in the F stars and also find it decreases for stars cooler than mid K. We examine correlations between simultaneously measured R'(HK) and radial velocities using both a classical statistical test and a Bayesian odds ratio test. We find that there is a significant correlation between R'(HK) and the radial velocity in only five of the 82 stars in this sample. Thus, simple R'(HK)-v(rad) correlations will generally not be effective in correcting the measured vrad values for the effects of magnetic activity in the Hyades. We argue that this implies long-timescale activity variations (of order a few years; i.e., magnetic cycles or growth and decay of plage regions) will not significantly hinder our search for planets in the Hyades if the stars are closely monitored for chromospheric activity. The trends in the radial velocity scatter (sigma'(v)) with [R'(HK)], v sin i, and P-rot for our stars is generally consistent with those found in field stars in the Lick planet search data, with the notable exception of a shallower dependence of sigma'(v) on [R'(HK)] for F stars. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. RP Paulson, DB (reprint author), Univ Texas, Dept Astron, RLM 15308, Austin, TX 78712 USA. NR 59 TC 62 Z9 63 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2002 VL 124 IS 1 BP 572 EP 582 DI 10.1086/341171 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 563UA UT WOS:000176272900040 ER PT J AU Platais, I Kozhurina-Platais, V Girard, TM van Altena, WF Klemola, AR Stauffer, JR Armandroff, TE Mighell, KJ Dell'Antonio, IP Falco, EE Sarajedini, A AF Platais, I Kozhurina-Platais, V Girard, TM van Altena, WF Klemola, AR Stauffer, JR Armandroff, TE Mighell, KJ Dell'Antonio, IP Falco, EE Sarajedini, A TI WIYN Open Cluster Study. VIII. The geometry and stability of the NOAO CCD Mosaic Imager SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; catalogs; instrumentation : detectors; open clusters and associations : individual (NGC 188) ID HUBBLE-SPACE-TELESCOPE; PROPER-MOTION; ATMOSPHERIC DISPERSION; METER TELESCOPE; DATA REDUCTION; FIELD; ASTROMETRY; MEMBERSHIP; PHOTOMETRY; PROGRAM AB The field of direct imaging is experiencing a considerable growth in the number of available CCD mosaic imagers, especially on large telescopes. To fully exploit the astrometric potential of these imaging devices, we develop a technique, utilizing an astrometric standard, for precision transformation of pixel coordinates into a global coordinate system. We have constructed a new astrometric standard set of 1863 stars in the field of NGC 188 to derive the CCD chip constants for the NOAO CCD Mosaic Imager. The multiple-epoch data on the Mosaic's metrics indicate that this CCD mosaic device may have experienced a one-time nonelastic expansion. We also present a new determination of the pixel scale and the optical field angle distortion constants for the KPNO Mayall 4 m telescope prime focus field corrector. To establish a reliable history of the CCD mosaic imager metrics for current and potential future astrometric applications, we recommend obtaining astrometric calibrations for CCD mosaic imagers on a regular basis. Apart from mechanical positioning of the CCD mosaic camera on the telescope, noticeable changes in the thermal environment of CCD mosaic chips should also prompt new astrometric calibrations. It is shown that, following all precautions, the NOAO CCD Mosaic Imager can produce excellent astrometric results on the Mayall 4 m telescope. C1 Univ Space Res Assoc, Div Astron & Space Phys, Washington, DC 20024 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. CALTECH, IPAC, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Brown Univ, Dept Phys, Providence, RI 02912 USA. Smithsonian Inst, Whipple Observ, Amado, AZ 85645 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Platais, I (reprint author), Free Univ Brussels, Inst Astron & Astrophys, CP 226,Blvd Triomphe, B-1050 Brussels, Belgium. NR 37 TC 11 Z9 11 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2002 VL 124 IS 1 BP 601 EP 611 DI 10.1086/340953 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 563UA UT WOS:000176272900043 ER PT J AU Arnaud, M Majerowicz, S Lumb, D Neumann, DM Aghanim, N Blanchard, A Boer, M Burke, DJ Collins, CA Giard, M Nevalainen, J Nichol, RC Romer, AK Sadat, R AF Arnaud, M Majerowicz, S Lumb, D Neumann, DM Aghanim, N Blanchard, A Boer, M Burke, DJ Collins, CA Giard, M Nevalainen, J Nichol, RC Romer, AK Sadat, R TI XMM-Newton observation of the distant (z=0.6) galaxy cluster RX J1120.1+4318 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : clusters : general; galaxies : intergalactic medium; cosmology : observations; cosmology : dark matter; cosmological parameters; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; LUMINOSITY-TEMPERATURE RELATION; INTRACLUSTER MEDIUM; HIGH-REDSHIFT; T RELATION; GAS; MASS; EMISSION; ENTROPY AB We report on a 20 ks XMM observation of the distant cluster RX J1120.1+4318, discovered at z = 0.6 in the SHARC survey. The cluster has a regular spherical morphology, suggesting it is in a relaxed state. The combined fit of the EPIC/MOS&pn camera gives a cluster mean temperature of kT = 5.3 +/- 0.5 keV with an iron abundance of 0.47 +/- 0.19. The temperature profile, measured for the first time at such a redshift, is consistent with an isothermal atmosphere up to half the virial radius. The surface brightness profile, measured nearly up to the virial radius, is well fitted by a beta-model, with beta = 0.78(-0.04)(+0.06) and a core radius of theta(c) = 0.44(-0.04)(+0.06) arcmin. We compared the properties of RX J1120.1+4318 with the properties of nearby clusters for two cosmological models. an Einstein-de Sitter Universe and a flat low density Universe with Omega(0) = 0.3. For both models, the scaled emission measure profile beyond the core, the gas mass fraction and luminosity are consistent with the expectations of the self-similar model of cluster formation, although a slightly better agreement is obtained for a low density Universe. There is no evidence of a central cooling flow, in spite of the apparent relaxed state of the cluster. This is consistent with its estimated cooling time, larger than the age of the Universe at the cluster redshift. The entropy profile shows a flat core with a central entropy of similar to140 keV cm(2), remarkably similar to the entropy floor observed in nearby clusters, and a rising profile beyond typically 0.1 virial radius. Implications of our results, in terms of non-gravitational physics in cluster formation, are discussed. C1 CEA, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. European Space Agcy, ESTEC, Sci Payloads Technol Div, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. UPS, CNRS, UMR5572, Observ Midi Pyrenees,Lab Astrophys, F-31400 Toulouse, France. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead L41 1LD, Merseyside, England. European Space Agcy, ESTEC, Res & Sci Support Div, NL-2200 AG Noordwijk, Netherlands. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Arnaud, M (reprint author), CEA, DSM, DAPNIA, Serv Astrophys, LOrme Merisiers,Bat 709, F-91191 Gif Sur Yvette, France. OI Burke, Douglas/0000-0003-4428-7835; Boer, Michel/0000-0001-9157-4349 NR 51 TC 99 Z9 99 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2002 VL 390 IS 1 BP 27 EP 38 DI 10.1051/0004-6361:20020669 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 576AE UT WOS:000176980000006 ER PT J AU Beuther, H Walsh, A Schilke, P Sridharan, TK Menten, KM Wyrowski, F AF Beuther, H Walsh, A Schilke, P Sridharan, TK Menten, KM Wyrowski, F TI CH3OH and H2O masers in high-mass star-forming regions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE masers; stars : formation; ISM : dust, extinction; ISM : jets and outflows; infrared : ISM; radio continuum : ISM ID ULTRACOMPACT HII-REGIONS; GHZ METHANOL MASERS; H-II-REGIONS; VLBI OBSERVATIONS; HIGH-RESOLUTION; ENVIRONMENT; EMISSION; CONTINUUM; OUTFLOWS; DISKS AB We present a comparison of Class II CH3OH (6.7 GHz) and H2O (22.2 GHz) masers at high spatial resolution in a sample of 29 massive star-forming regions. Absolute positions of both maser types are compared with mm dust continuum, cm continuum and mid-infrared sources. All maser features - regardless of the species - are associated with massive mm cores, but only 3 out of 18 CH3OH masers and 6 out of 22 H2O masers are associated with cm emission likely indicating the presence of a recently ignited massive star. These observations of a homogenous sample of massive, young star-forming regions confirm earlier results, obtained for each maser species separately, that both maser types are signposts of high-mass star formation in very early evolutionary stages. The data are consistent with models that explain CH3OH maser emission by radiative pumping in moderately hot cores, requiring the absence, or only weak, free-free cm continuum radiation due to recently ignited stars. Mid-infrared sources are associated with both maser types in approximately 60% of the observed fields. Thus, mid-infrared objects may power maser sites, but the detection of strong mid-infrared emission is not strictly necessary because it might be heavily extincted. A comparison of the spatial separations between the different observed quantities and other properties of the star-forming regions does not reveal any correlation. Our data suggest that CH3OH and H2O masers need a similar environment (dense and warm molecular gas), but that, due to the different excitation processes (radiative pumping for CH3OH and collisional pumping for H2O), no spatial correlations exist. Spatial associations are probably coincidences due to insufficient angular resolution and projection effects. The kinematic structures we find in the different maser species show no recognizable pattern, and we cannot draw firm conclusions as to whether the features are produced in disks, outflows or expanding shock waves. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beuther, H (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. RI Walsh, Andrew/B-5627-2013 OI Walsh, Andrew/0000-0001-9506-0855 NR 39 TC 115 Z9 115 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2002 VL 390 IS 1 BP 289 EP 298 DI 10.1051/0004-6361:20020710 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 576AE UT WOS:000176980000034 ER PT J AU Rodriguez, LF Anglada, G Torrelles, JM Mendoza-Torres, JE Haschick, AD Ho, PTP AF Rodriguez, LF Anglada, G Torrelles, JM Mendoza-Torres, JE Haschick, AD Ho, PTP TI VLA observations of water maser emission associated with SVS 13 and other sources in NGC 1333 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : Herbig-Haro objects; ISM : jets and outflows; masers; stars : pre-main sequence ID HERBIG-HARO OBJECTS; HH 7-11 REGION; STAR; VICINITY AB The young stellar object SVS 13 is believed to power the chain formed by the HH 7-11 objects. Recent observations have revealed that in the radio continuum (3.6-cm) the source is a binary with components separated by about 0."3 in the east-west direction. The members of the binary are named VLA 4A (western component) and VLA 4B (eastern component). In an attempt to ascertain which of the two components of the binary is the most likely candidate to drive the outflow, we obtained accurate positions for the H(2)O maser spots toward this source, also known as H(2)O(A), derived from Very Large Array observations in its highest angular resolution A configuration. We detected a total of eleven spots over four observational sessions (made in the years 1983, 1985, 1988, and 1989). The spots are segregated in two velocity groups: a velocity group with v(LSR) similar to that of the ambient cloud (v(LSR) similar or equal to 8 km s(-1)), for which we detected five features (with v(LSR) in the range of 6.5 to 12.2 km s(-1)) and a blueshifted velocity group (six features with vLSR in the range of -25.4 to 5.6 km s(-1)). Remarkably, all the spots in the first velocity group are associated with VLA 4A, while all the spots in the blueshifted velocity group are associated with VLA 4B. We discuss the possible implications of this observation. We also present accurate positions of the H(2)O maser HH 7(B) and of the masers associated with IRAS4B (VLA 28) and IRAS7 (VLA 27, the exciting source of HH 6). C1 Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, IEEC, ES-08034 Barcelona, Spain. CSIC, Inst Ciencias Espacio, ES-08034 Barcelona, Spain. Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico. MIT, Haystack Observ, Westford, MA 01886 USA. RP Rodriguez, LF (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Campus Morelia,Apdo Postal 3-72, Morelia 58089, Michoacan, Mexico. EM luisfr@astrosmo.unam.mx; guillem@iaa.es; torrelles@ieec.fcr.es; mend@inaoep.mx; ho@cfa.harvard.edu OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 28 TC 17 Z9 17 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 JUL PY 2002 VL 389 IS 2 BP 572 EP 576 DI 10.1051/0004-6361:20020619 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 573EW UT WOS:000176817200028 ER PT J AU Tuthill, PG Men'shchikov, AB Schertl, D Monnier, JD Danchi, WC Weigelt, G AF Tuthill, PG Men'shchikov, AB Schertl, D Monnier, JD Danchi, WC Weigelt, G TI Bispectrum speckle interferometry of the Red Rectangle: Diffraction-limited near-infrared images reconstructed from Keck telescope speckle data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : image processing; circumstellar matter; stars : individual : Red Rectangle; stars : mass-loss; stars : AGB and post-AGB; infrared : stars ID RESOLUTION; EVOLUTION; EMISSION; MASKING; NEBULAE AB We present new near-infrared (2.1-3.3 mum) images of the Red Rectangle with unprecedented diffraction-limited angular resolutions of 46-68 mas; 4 times higher than that of the Hubble space telescope and almost a factor of two improvement over the previous 6 m SAO telecope speckle images presented by Men'shchikov et al. (1998). The new images, which were reconstructed from Keck telescope speckle data using the bispectrum speckle interferometry method, clearly show two bright lobes above and below the optically thick dark lane obscuring the central binary. X-shaped spikes, thought to trace the surface of a biconical flow, change the intensity distribution of the bright lobes, making them appear broadened or with an east-west double-peak in images with the highest resolution. The striking biconical appearance of the Red Rectangle is preserved on scales from 50 mas to 10 and from the visible (red) to at least 10 mum, implying that large grains of at least several microns in size dominate scattering. The new images supplement previous 76 mas resolution speckle reconstructions at shorter wavelengths of 0.6-0.8 mum (Osterbart et al. 1997) and 0.7-2.2 mum (Men'shchikov et al. 1998), allowing a more detailed analysis of the famous bipolar nebula. The intensity distribution of the images is inconsistent with a at disk geometry frequently used to model the bipolar nebulae. Instead, a geometrically thick torus-like density distribution with bipolar conical cavities is preferred. The extent of the bright lobes indicates that the dense torus has a diameter of greater than or similar to 100 AU, for an assumed distance of 330 pc. This torus may be the outer reaches of a flared thick disk tapering inwards to the central star, however such a density enhancement on the midplane is not strictly required to explain the narrow dark lane obscuring the central stars. C1 Univ Sydney, Sch Phys, Dept Astron, Sydney, NSW 2006, Australia. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Smithsonian Astrophys Observ MS 42, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tuthill, PG (reprint author), Univ Sydney, Sch Phys, Dept Astron, Sydney, NSW 2006, Australia. NR 19 TC 26 Z9 27 U1 0 U2 2 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2002 VL 389 IS 3 BP 889 EP 895 DI 10.1051/0004-6361:20020292 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574FL UT WOS:000176877800019 ER PT J AU Jones, DH Stappers, BW Gaensler, BM AF Jones, DH Stappers, BW Gaensler, BM TI Discovery of an optical bow-shock around pulsar B0740-28 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : general; pulsars : individual : B0740-28 ID PROPER MOTIONS; RADIO PULSARS; NEBULA; STANDARDS; EMISSION AB We report the discovery of a faint Halpha pulsar wind nebula (PWN) powered by the radio pulsar B0740-28. The characteristic bow-shock morphology of the PWN implies a direction of motion consistent with the previously measured velocity vector for the pulsar. The PWN has a flux density more than an order of magnitude lower than for the PWNe seen around other pulsars, but, for a distance 2 kpc, it is consistent with propagation through a medium of atomic density n(H) similar to 0.25 cm(-3), and neutral fraction of 1%. The morphology of the PWN in the area close to the pulsar is distinct from that in downstream regions, as is also seen for the PWN powered by PSR B2224+65. In particular, the PWN associated with PSR B0740-28 appears to close at its rear, suggesting that the pulsar has recently passed through a transition from low density to high density ambient gas. The faintness of this source underscores that deep searches are needed to find further examples of optical pulsar nebulae. C1 European So Observ, Santiago 19, Chile. Univ Chile, Observ Cerro Calan, Dept Astron, Santiago, Chile. Stichting ASTRON, NL-7990 AA Dwingeloo, Netherlands. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jones, DH (reprint author), European So Observ, Casilla 19001, Santiago 19, Chile. RI Gaensler, Bryan/F-8655-2010 NR 26 TC 16 Z9 16 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2002 VL 389 IS 1 BP L1 EP L5 DI 10.1051/0004-6361:20020651 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 568UA UT WOS:000176561500001 ER PT J AU Tarchi, A Henkel, C Peck, AB Menten, KM AF Tarchi, A Henkel, C Peck, AB Menten, KM TI The association between water kilomasers and compact radio sources in the starburst galaxy NGC 2146 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : individual : NGC 2146; galaxies : starburst; galaxies : ISM; masers; radio lines : ISM; radio lines : galaxies ID H2O MASER EMISSION; DRIVEN SUPERWIND; NGC-2146; NUCLEUS; M51 AB We report the detection of 22 GHz water vapor emission toward the starburst galaxy NGC 2146, made using the Effelsberg 100-m telescope. Interferometric observations with the Very Large Array (VLA) show that a part of the emission originates from two prominent sites of star formation that are associated with compact radio continuum sources, likely ultra-compact HII regions. It is concluded that the emission arises from the most luminous and distant H2O "kilomasers" detected so far. Our data increase the number of water maser detections in northern galaxies (Dec > -30degrees) with IRAS point source fluxes S-100mum > 50 Jy to 18%. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. CNR, Ist Radioastron, I-40129 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tarchi, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. OI Tarchi, Andrea/0000-0001-8540-3500 NR 26 TC 11 Z9 11 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2002 VL 389 IS 1 BP L39 EP L42 DI 10.1051/0004-6361:20020719 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 568UA UT WOS:000176561500010 ER PT J AU Bloser, PF Chou, Y Grindlay, JE Narita, J Monnelly, G AF Bloser, PF Chou, Y Grindlay, JE Narita, J Monnelly, G TI Development of an XSPEc-based spectral analysis system for the coded-aperture hard X-ray balloon payload EXITE2 SO ASTROPARTICLE PHYSICS LA English DT Article DE balloons; gamma rays; observations; instrumentation; detectors; methods; data analysis; nebulae; individual (Crab nebula) ID PHOSWICH DETECTOR TELESCOPE; ASTRONOMY AB We present the spectral analysis system for the second-generation energetic X-ray imaging telescope experiment (EXITE2) balloon payload. EXITE2 is an imaging hard X-ray telescope using a coded-aperture mask and a NaI/CsI phoswich detector operating in the energy range 20-600 keV. The instrument was flown on a high-altitude scientific balloon from Ft. Sumner, NM on 7-8 May, 1997. We describe the details of the EXITE2 spectral analysis system, with emphasis on those aspects peculiar to coded-aperture instruments. In particular. we have made our analysis compatible with the standard X-ray spectral fitting package XSPEC by generating a response matrix in the appropriate format including all the effects of a coded-aperture system, The use of XSPEC, which may be a first for coded-aperture data, permits great flexibility in the fitting of spectral models. The additional effects of our phoswich system, or any other detector-specific considerations, may be easily included as well. We test our spectral analysis using observations of the Crab Nebula, and find that the EXITE2 Crab spectrum is consistent with those recorded by previous instruments operating in this energy range. (C) 2002 Elsevier Science B,V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Bloser, PF (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. RI Chou, Yi/C-4922-2008 OI Chou, Yi/0000-0002-8584-2092 NR 19 TC 3 Z9 4 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD JUL PY 2002 VL 17 IS 4 BP 393 EP 400 AR PII S0937-6505(01)00165-7 DI 10.1016/S0927-6505(01)00165-7 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 562LR UT WOS:000176198700001 ER PT J AU Kilgard, RE Kaaret, P Krauss, MI Prestwich, AH Raley, MT Zezas, A AF Kilgard, RE Kaaret, P Krauss, MI Prestwich, AH Raley, MT Zezas, A TI A minisurvey of X-ray point sources in starburst and nonstarburst galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : spiral; galaxies : starburst; surveys; X-rays : galaxies ID CHANDRA OBSERVATIONS; BINARIES AB We present a comparison of X-ray point-source luminosity functions of three starburst galaxies ( the Antennae, M82, and NGC 253) and four nonstarburst spiral galaxies ( NGC 3184, NGC 1291, M83, and IC 5332). We find that the luminosity functions of the starbursts are flatter than those of the spiral galaxies; the starbursts have relatively more sources at high luminosities. This trend extends to early-type galaxies that have steeper luminosity functions than spirals. We show that the luminosity function slope is correlated with 60 mum luminosity, a measure of star formation. We suggest that the difference in luminosity functions is related to the age of the X-ray binary populations, and we present a simple model that highlights how the shape of the luminosity distribution is affected by the age of the underlying X-ray binary population. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kilgard, RE (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 NR 24 TC 85 Z9 85 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2002 VL 573 IS 1 BP 138 EP 143 DI 10.1086/340490 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564YD UT WOS:000176340400014 ER PT J AU Nicastro, F Zezas, A Drake, J Elvis, M Fiore, F Fruscione, A Marengo, M Mathur, S Bianchi, S AF Nicastro, F Zezas, A Drake, J Elvis, M Fiore, F Fruscione, A Marengo, M Mathur, S Bianchi, S TI Chandra discovery of a tree in the X-ray forest toward PKS 2155-304: The local filament? SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : halo; intergalactic medium; quasars : absorption lines; X-rays : ISM ID INTERGALACTIC MEDIUM; RELATIVISTIC JETS; CORONAL GAS; GALAXY; ABSORPTION; DUST; SPECTRA; ATOMS AB We present the first X-ray detection of resonant absorption from warm/hot local gas either in our Galaxy, or in the intergalactic space surrounding our Galaxy, along the line of sight toward the blazar PKS 2155-304. The Chandra HRCS/LETG spectrum of this z = 0 : 116 source clearly shows, at 5 level, unresolved (FWHM less than or equal to 800 km s(-1) at a 2 sigma confidence level) O VII Kalpha and Ne IX Kalpha resonant absorption lines at 21.603(-0.024)(+0.014) and 13.448(-0.024)(+0.022) Angstrom (i.e., cz = 14(-330)(+190) km s(-1) in the rest frame, from the O VII Kalpha line). O VIII Kalpha and O VII K from the same system are also detected at a lower significance level (i.e., similar to3 sigma), while upper limits are set on O VIII Kbeta, Ne x Kalpha, and Ne IX Kbeta. The Far Ultraviolet Spectroscopic Explorer spectrum of this source shows complex O VI 2s-->2p absorption at the same redshift as the X-ray system, made by at least two components: one relatively narrow (FWHM = 106 +/- 9 km s(-1)) and slightly redshifted (cz = 36 +/- 6 km s(-1)), and one broader ( FWHM = 158 +/- 26 km s(-1)) and blueshifted (cz = 135 +/- 14 km s(-1)). We demonstrate that the physical states of the UV and X-ray absorbers are hard to reconcile with a single, purely collisionally ionized, equilibrium plasma. We propose instead that the X-ray and at least the broader and blueshifted UV absorber are produced in a low-density intergalactic plasma, collapsing toward our Galaxy, consistent with the predictions of a warm-hot intergalactic medium from numerical simulations. We find that any reasonable solution requires overabundance of Ne compared to O by a factor of similar to2, with respect to the solar value. We propose several scenarios to account for this observation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Roma, I-00040 Rome, Italy. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Bianchi, Stefano/B-4804-2010; Zezas, Andreas/C-7543-2011; OI Bianchi, Stefano/0000-0002-4622-4240; Zezas, Andreas/0000-0001-8952-676X; Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 48 TC 180 Z9 180 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2002 VL 573 IS 1 BP 157 EP 167 DI 10.1086/340489 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564YD UT WOS:000176340400016 ER PT J AU Pooley, D Lewin, WHG Verbunt, F Homer, L Margon, B Gaensler, BM Kaspi, VM Miller, JM Fox, DW van der Klis, M AF Pooley, D Lewin, WHG Verbunt, F Homer, L Margon, B Gaensler, BM Kaspi, VM Miller, JM Fox, DW van der Klis, M TI Chandra observation of the globular cluster NGC 6440 and the nature of cluster X-ray luminosity functions SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; globular clusters : individual (NGC 6440); novae cataclysmic variables; stars : neutron ID BINARIES; ROSAT; POPULATION; NGC-6440; LIMITS; CORE AB As part of our campaign to determine the nature of the various source populations of the low-luminosity globular cluster X-ray sources, we have obtained a Chandra X-Ray Observatory ACIS-S3 image of the globular cluster NGC 6440. We detect 24 sources to a limiting luminosity of similar to2 x 10(31) ergs s(-1) (0.5-2.5 keV) inside the cluster's half-mass radius, all of which lie within 2 core radii of the cluster center. We also find excess emission in and around the core that could be due to unresolved point sources. Based on X-ray luminosities and colors, we conclude that there are 4-5 likely quiescent low-mass X-ray binaries and that most of the other sources are cataclysmic variables. We compare these results to Chandra results from other globular clusters and find the X-ray luminosity functions differ among the clusters. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Univ Utrecht, Inst Astron, NL-3508 TA Utrecht, Netherlands. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. RP MIT, Ctr Space Res, Cambridge, MA 02139 USA. EM davep@space.mit.edu; lewin@space.mit.edu; F.W.M.Verbunt@astro.uu.nl; homer@astro.washington.edu; margon@stsci.edu; bgaensler@cfa.harvard.edu; vkaspi@physics.mcgill.ca; jmm@space.mit.edu; derekfox@astro.caltech.edu; michiel@astro.uva.nl RI Gaensler, Bryan/F-8655-2010; Margon, Bruce/B-5913-2012; OI Gaensler, Bryan/0000-0002-3382-9558 NR 34 TC 57 Z9 57 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2002 VL 573 IS 1 BP 184 EP 190 DI 10.1086/340498 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564YD UT WOS:000176340400019 ER PT J AU Beltran, MT Girart, JM Estalella, R Ho, PTP Palau, A AF Beltran, MT Girart, JM Estalella, R Ho, PTP Palau, A TI IRAS 21391+5802: The molecular outflow and its exciting source SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; ISM : individual (JC 1396N, IRAS 21391+5802); radio continuum : ISM; stars : formation ID YOUNG STELLAR OBJECTS; INTERMEDIATE-MASS STARS; HERBIG-HARO OBJECTS; RADIATION-DRIVEN IMPLOSION; RIMMED GLOBULE IC1396N; T-TAURI STARS; CONTINUUM EMISSION; RADIO-CONTINUUM; HIGH-RESOLUTION; CIRCUMSTELLAR ENVIRONMENT AB We present centimeter and millimeter observations of gas and dust around IRAS 21391+5802, an intermediate-mass source embedded in the core of IC 1396N. Continuum observations from 3.6 cm to 1.2 mm are used to study the embedded objects and overall distribution of the dust, while molecular line observations of CO, CS, and CH3OH are used to probe the structure and chemistry of the outflows in the region. The continuum emission at centimeter and millimeter wavelengths has been resolved into three sources separated 15 00 from each other, and with one of them, BIMA 2, associated with IRAS 21391+5802. The dust emission around this source shows a very extended envelope, which accounts for most of the circumstellar mass of 5.1 M. This source is powering a strong molecular outflow, elongated in the east-west direction, which presents a complex structure and kinematics. While at high outflow velocities the outflow is clearly bipolar, at low outflow velocities the blueshifted and redshifted emission are highly overlapping and the strongest emission shows a V-shaped morphology. The outflow as traced by CS and CH3OH exhibits two well-differentiated and clumpy lobes, with two prominent northern blueshifted and redshifted clumps. The curved shape of the clumps and the spectral shape at these positions are consistent with shocked material. In addition, CS and CH3OH are strongly enhanced toward these positions with respect to typical quiescent material abundances in other star-forming regions. This kinematical and chemical evidence suggests that the clumps are tracing gas entrained within the surface of interaction between the molecular outflow and the dense ambient quiescent core and that the morphology of the molecular outflow is a result of this interaction. The circumstellar mass together with the power-law index of the dust emissivity measured, beta = 1.1 +/- 0.3, and the fact that the source is driving a molecular outflow are consistent with the source BIMA 2 being an embedded intermediate-mass protostar. In addition, the source fits very well correlations between source and outflow properties found for low-mass Class 0 objects. The other two sources in the region, BIMA 1 and BIMA 3, have a mass of 0.07 M-. each, and their dust emissivity index, beta < 0.3 and β = 0.1 +/- 0.3, respectively, is consistent with more evolved objects. BIMA 1 is also driving a very collimated and small bipolar outflow elongated in the north-south direction. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Catalunya, Spain. RP Beltran, MT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Beltran Sorolla, Maria Teresa/0000-0003-3315-5626 NR 70 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 JUL 1 PY 2002 VL 573 IS 1 BP 246 EP 259 DI 10.1086/340592 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564YD UT WOS:000176340400024 ER PT J AU Muench, AA Lada, EA Lada, CJ Alves, J AF Muench, AA Lada, EA Lada, CJ Alves, J TI The luminosity and mass function of the Trapezium cluster: From B stars to the deuterium-burning limit SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; open clusters and associations : individual (Trapezium); stars : low-mass, brown dwarfs; stars : luminosity function, mass function; stars : pre main-sequence ID ORION NEBULA CLUSTER; EQUATION-OF-STATE; STELLAR TURBULENT CONVECTION; MAIN-SEQUENCE TRACKS; YOUNG BROWN DWARFS; MOLECULAR CLOUD; CIRCUMSTELLAR DISKS; IC 348; CARBON-MONOXIDE; FLUID HYDROGEN AB We use the results of a new multiepoch, multiwavelength, near-infrared census of the Trapezium cluster in Orion to construct and analyze the structure of its infrared (K-band) luminosity function. Specifically, we employ an improved set of model luminosity functions to derive this cluster's underlying initial mass function (IMF) across the entire range of mass from OB stars to substellar objects down to near the deuterium-burning limit. We derive an IMF for the Trapezium cluster that rises with decreasing mass, having a Salpeter-like IMF slope until near similar to0.6 M-circle dot where the IMF flattens and forms a broad peak extending to the hydrogen-burning limit, below which the IMF declines into the substellar regime. Independent of the details, we find that substellar objects account for no more than similar to22% of the total number of likely cluster members. Further, the substellar Trapezium IMF breaks from a steady power-law decline and forms a significant secondary peak at the lowest masses ( 10 20 times the mass of Jupiter). This secondary peak may contain as many as similar to30% of the substellar objects in the cluster. Below this substellar IMF peak, our K-band luminosity function (KLF) modeling requires a subsequent sharp decline toward the planetary mass regime. Lastly, we investigate the robustness of pre-main-sequence luminosity evolution as predicted by current evolutionary models, and we discuss possible origins for the IMF of brown dwarfs. C1 Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. RP Univ Florida, Dept Astron, POB 112055,211 Bryant Space Sci Ctr, Gainesville, FL 32611 USA. EM muench@astro.ufl.edu; lada@astro.ufl.edu; clada@cfa.harvard.edu; jalves@eso.org NR 69 TC 281 Z9 281 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2002 VL 573 IS 1 BP 366 EP 393 DI 10.1086/340554 PN 1 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564YD UT WOS:000176340400035 ER PT J AU Beasley, AJ Gordon, D Peck, AB Petrov, L MacMillan, DS Fomalont, EB Ma, C AF Beasley, AJ Gordon, D Peck, AB Petrov, L MacMillan, DS Fomalont, EB Ma, C TI The VLBA Calibrator Survey - VCSI SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrometry; radio continuum : general; reference systems; surveys; techniques : interferometric ID COMPACT SYMMETRIC OBJECTS; BASE-LINE INTERFEROMETRY; MHZ SKY SURVEY; ASTROMETRIC SURVEY; HIPPARCOS-CATALOG; REFERENCE-FRAME; RADIO-SOURCES; COINS SAMPLE; MISSION; GALAXY AB A catalog containing milliarcsecond-accurate positions of 1332 extragalactic radio sources distributed over the northern sky is presented the Very Long Baseline Array Calibrator Survey ( VCS1). The positions have been derived from astrometric analysis of dual-frequency 2.3 and 8.4 GHz VLBA snapshot observations; in a majority of cases, images of the sources are also available. These radio sources are suitable for use in geodetic and astrometric experiments, and as phase-reference calibrators in high-sensitivity astronomical imaging. The VCS1 is the largest high-resolution radio survey ever undertaken and triples the number of sources available to the radio astronomy community for VLBI applications. In addition to the astrometric role, this survey can be used in active galactic nuclei, Galactic, gravitational lens, and cosmological studies. C1 CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Raytheon ITSS, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NVI Inc, Greenbelt, MD 20771 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Beasley, AJ (reprint author), CALTECH, Owens Valley Radio Observ, POB 968, Big Pine, CA 93513 USA. RI Ma, Chopo/D-4751-2012 NR 39 TC 188 Z9 190 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2002 VL 141 IS 1 BP 13 EP 21 DI 10.1086/339806 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564XW UT WOS:000176339700002 ER PT J AU Bakos, GA Sahu, KC Nemeth, P AF Bakos, GA Sahu, KC Nemeth, P TI Revised coordinates and proper motions of the stars in the Luyten Half-Second catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrometry; astronomical data bases : miscellaneous; catalogs ID SPACE INTERFEROMETRY MISSION; LUMINOSITY FUNCTION; DARK-MATTER AB We present refined coordinates and proper-motion data for the high proper-motion (HPM) stars in the Luyten Half-Second (LHS) catalog. The positional uncertainty in the original Luyten catalog is typically greater than 10" and is often greater than 30". We have used the digital scans of the POSS I and POSS II plates to derive more accurate positions and proper motions of the objects. Out of the 4470 candidates in the LHS catalog, 4323 objects were manually reidentified in the POSS I and POSS II scans. A small fraction of the stars were not found because of the lack of finder charts and digitized POSS II scans. The uncertainties in the revised positions are typically similar to2" but can be as high as similar to8" in a few cases, which is a large improvement over the original data. Cross-correlation with the Tycho-2 and Hipparcos catalogs yielded 819 candidates (with m(R) less than or similar to 12). For these brighter sources, the position and proper-motion data were replaced with the more accurate Tycho-2/Hipparcos data. In total, we have revised proper-motion measurements and coordinates for 4040 stars and revised coordinates for 4330 stars. The electronic version of the paper(5) contains the updated information on all 4470 stars in the LHS catalog. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Konkoly Observ Budapest, H-1525 Budapest, Hungary. JATE Univ, Dept Expt Phys, H-6720 Szeged, Hungary. RP Bakos, GA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RI Nemeth, Peter/E-4515-2016 OI Nemeth, Peter/0000-0003-0963-0239 NR 19 TC 66 Z9 67 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2002 VL 141 IS 1 BP 187 EP 193 DI 10.1086/340115 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564XW UT WOS:000176339700011 ER PT J AU Lovette, IJ Bermingham, E AF Lovette, IJ Bermingham, E TI What is a wood-warbler? Molecular characterization of a monophyletic parulidae SO AUK LA English DT Article ID DENDROICA-WARBLERS; MITOCHONDRIAL-DNA; CYTOCHROME-B; EVOLUTION; BIRDS; DIFFERENTIATION; BIOGEOGRAPHY; PHYLOGENETICS; SYSTEMATICS; TANAGERS AB The wood-warblers (family Parulidae) fall within a radiation of passerine birds commonly known as the New World nine-primaried oscines. Defining familial relationships within that radiation has previously been challenging because of its extremely high diversity, a paucity of phylogenetically informative morphological characters, and an apparent high rate of cladogenesis early in the radiation's history. Here, analyses of mitochondrial and nuclear DNA sequences demonstrate that the 25 extant genera traditionally placed in the Parulidae do not form a monophyletic group. Instead, all reconstructions identify a well-resolved clade of 19 genera (Vermivora, Parula, Dendroica, Catharopeza, Mniotilta, Setophaga, Protonotaria, Helmitheros, Limnothlypis, Seiurus, Oporornis, Geothlypis, Wilsonia, Cardellina, Ergaticus, Myioborus, Euthlypis, Basileuterus, and Phaeothlypis) that are all morphologically typical wood-warblers traditionally placed in the Parulidae. Six genera traditionally assigned to the Parulidae-Microligea, Teretistris, Zeledonia, Icteria, Granatellus, and Xenoligea-fall outside this highly supported clade in all mtDNA-based and nuclear DNA-based reconstructions, and each is probably more closely allied to taxa traditionally placed in other nine-primaried oscine families. The long, well-supported, and independently confirmed internode at the base of this wood-warbler clade provides the opportunity to define a monophyletic Paruliclae using several complementary molecular phylogenetic criteria. Support for those relationships comes from reconstructions based on a range of nucleotide-intensive (from 894 to 3,638 nucleotides per taxon) and taxon-intensive (45 to 128 species) analyses of mtDNA sequences, as well as independent reconstructions based on nucleotide substitutions in the nuclear-encoded c-mos gene. Furthermore, the 19 typical wood-warbler genera share a synapomorphic one-codon c-mos deletion not found in other passerines. At a slightly deeper phylogenetic level, our mtDNA-based reconstructions are consistent with previous morphologic and genetic studies in suggesting that many nine-primaried oscine taxa have unanticipated affinities, that many lineages arose during an early and explosive period of cladogenesis, and that the generation of a robust nine-primaried oscine phylogeny will require robust taxonomic sampling and extensive phylogenetic information. C1 Cornell Univ, Cornell Lab Ornithol, Ithaca, NY 14850 USA. Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14850 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Lovette, IJ (reprint author), Cornell Univ, Cornell Lab Ornithol, 159 Sapsucker Woods Rd, Ithaca, NY 14850 USA. EM ijl2@cornell.edu RI Lovette, Irby/P-3477-2014 NR 71 TC 70 Z9 80 U1 0 U2 8 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 JUL PY 2002 VL 119 IS 3 BP 695 EP 714 DI 10.1642/0004-8038(2002)119[0695:WIAWWM]2.0.CO;2 PG 20 WC Ornithology SC Zoology GA 593FL UT WOS:000177980300009 ER PT J AU Friesen, VL Anderson, DJ Steeves, TE Jones, H Schreiber, EA AF Friesen, VL Anderson, DJ Steeves, TE Jones, H Schreiber, EA TI Molecular support for species status of the Nazca Booby (Sula granti) SO AUK LA English DT Article ID MITOCHONDRIAL-DNA; POPULATION DIFFERENTIATION; MARBLED MURRELETS; EVOLUTION; SEQUENCES; LIMITS; RATES AB Pitman and Jehl (1998) recently argued that Masked Boobies (formerly Sula dactylatra granti) breeding on the Nazca Plate in the eastern Pacific Ocean are morphologically and ecologically distinct from other Masked Boobies and may represent a full species. The American Ornithologists' Union subsequently elevated that subspecies to a full species: the Nazca Booby (S. granti). To evaluate that change in classification, we compared sequence variation in the mitochondrial cytochrome-b gene among 75 Nazca Boobies and 37 Masked Boobies representing three subspecies from the central and eastern Pacific and Atlantic oceans. Results indicated strong differentiation of cytochrome-b variation among taxa. Sequences constituted three distinct groups: Nazca Boobies, Masked Boobies from the central and eastern Pacific (S. d. personata and S. d. californica), and Masked Boobies (S. d. dactylatra) from the Caribbean and Atlantic. Those three groups probably diverged within a very short period, 400,000-500,000 years ago. Our results support the proposal that S. granti represents a distinct species. C1 Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20008 USA. RP Friesen, VL (reprint author), Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. EM friesenv@biology.queensu.ca NR 30 TC 23 Z9 26 U1 1 U2 5 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 JUL PY 2002 VL 119 IS 3 BP 820 EP 826 DI 10.1642/0004-8038(2002)119[0820:MSFSSO]2.0.CO;2 PG 7 WC Ornithology SC Zoology GA 593FL UT WOS:000177980300022 ER PT J AU Vecchione, M Collins, MA Sweeney, MJ AF Vecchione, M Collins, MA Sweeney, MJ TI Systematics, ecology and biology of cirrate octopods: Workshop report SO BULLETIN OF MARINE SCIENCE LA English DT Editorial Material ID CEPHALOPODA AB Cirrate octopods are conspicuous members of the benthopelagic and bathypelagic communities and include some of the largest invertebrates of the deep-sea. Although they have often been considered to be rare members of deep-sea communities, recent trawling has shown that the relative abundance of some cirrates, especially opisthoteuthids, may be locally or regionally high (e.g., Boyle et al., 1998). Cirrates also are presumed to be primitive, morphologically similar to ancestral octopods (Young et al., 1998), although recent observations indicate unexpected adaptations such as bioluminescence (Johnsen et al., 1999) and possibly diverse feeding modes (Vecchione and Young, 1997). Therefore, knowledge of cirrates may contribute substantially to understanding cephalopod evolution as well as deep-sea biology and ecology. However, because they are fragile, the condition of specimens collected up until the past decade generally has been very poor, and our knowledge of the group is rudimentary. New methods, such as video-tapes recorded in-situ and gentle collection by submersibles, have allowed substantial new observations and renewed interest in the group. C1 Natl Museum Nat Hist, Natl Marine Fisheries Serv, Systemat Lab, Washington, DC 20560 USA. Univ Aberdeen, Dept Zool, Aberdeen AB24 2TN, Scotland. Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Vecchione, M (reprint author), Natl Museum Nat Hist, Natl Marine Fisheries Serv, Systemat Lab, Washington, DC 20560 USA. NR 10 TC 5 Z9 5 U1 0 U2 5 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 JUL PY 2002 VL 71 IS 1 BP 79 EP 94 PG 16 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 674CU UT WOS:000182619900008 ER PT J AU Debski, I Burslem, DFRP Palmiotto, PA Lafrankie, JV Lee, HS Manokaran, N AF Debski, I Burslem, DFRP Palmiotto, PA Lafrankie, JV Lee, HS Manokaran, N TI Habitat preferences of Aporosa in two Malaysian forests: Implications for abundance and coexistence SO ECOLOGY LA English DT Article DE Aporosa; coexistence; habitat preference; Malaysia; niche; rain forest; random drift; Ripley's K function; spatial pattern; species diversity; tropical forest ID TROPICAL RAIN-FOREST; JANZEN-CONNELL MODEL; TREE DIVERSITY; DISTRIBUTION PATTERNS; SPATIAL-DISTRIBUTION; DIPTEROCARP FOREST; NEOTROPICAL FOREST; GROWTH; RECRUITMENT; MAINTENANCE AB Theories accounting for the maintenance of high tree diversity in tropical rain forests range from those proposing that tropical trees are highly co-evolved niche specialists, to those proposing that they are mostly generalist, undergoing random drift. We test these hypotheses at a meaningful, community-wide scale using data on the spatial patterns and habitat preferences of all species of Aporosa (Euphorbiaceae) growing on two large rain forest plots in Malaysia. Second-order spatial pattern analyses using a method based on Ripley's K function showed that Aporosa species formed spatially distinct assemblages, and a randomization procedure suggested that these assemblages were explained by biases in their distributions in relation to habitat types. Soil type, as determined by parent material, was an important determinant of habitat preferences, although topography and forest structure also accounted for some variation. We conclude that niche differentiation is an important mechanism contributing to the coexistence of Aporosa species at the community scale. However, spatial separation due to these differential habitat biases accounted for only a portion of the high species richness observed in this genus, so other mechanisms must also be sought to account fully for the maintenance of tropical tree species richness. C1 Univ Aberdeen, Dept Plant & Soil Sci, Aberdeen AB24 3UU, Scotland. Univ Malaysia Sarawak, Inst Biodivers & Environm Conservat, Sarawak, Malaysia. Bates Coll, Lewiston, ME 04240 USA. Nanyang Technol Univ, NIE, Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Singapore, Singapore. Sarawak Forest Dept, Kuching, Sarawak, Malaysia. Forest Res Inst Malaysia, Kuala Lumpur 52109, Malaysia. RP Burslem, DFRP (reprint author), Univ Aberdeen, Dept Plant & Soil Sci, Cruickshank Bldg,St Machar Dr, Aberdeen AB24 3UU, Scotland. EM d.burslem@abdn.ac.uk OI Burslem, David/0000-0001-6033-0990 NR 62 TC 42 Z9 52 U1 2 U2 21 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD JUL PY 2002 VL 83 IS 7 BP 2005 EP 2018 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 571LD UT WOS:000176718100019 ER PT J AU Hall, JPW Harvey, DJ AF Hall, JPW Harvey, DJ TI The phylogeography of Amazonia revisited: New evidence from riodinid butterflies SO EVOLUTION LA English DT Article DE Amazon; area cladograms; biogeography; Charis; endemism; phylogeny; Riodinidae ID RIVERINE BARRIER HYPOTHESIS; VICARIANCE BIOGEOGRAPHY; HELICONIUS BUTTERFLIES; PHYLOGENETIC INFERENCE; PARSIMONY ANALYSIS; AREA-RELATIONSHIPS; RAW DISTRIBUTIONS; RACE FORMATION; SPECIATION; PATTERNS AB A fully resolved cladogram for 19 species in the Charis cleonus group of riodinid butterflies, which have closely parapatric ranges throughout the Amazon basin, is used to derive an area cladogram for the region. This represents the first comprehensive species-level analysis using insects and results in a hypothesis of Amazonian area relationships that is the most detailed to date. The Charis area cladogram is interpreted as supporting an historical vicariant split between the Guianas and the remainder of the Amazon and then between the upper and lower Amazon. The latter two clades can be further divided into the six most widely recognized areas of endemism and even smaller endemic centers within these, some of which, especially along the Madeira and lower Amazon Rivers, have never been previously hypothesized for butterflies. The overall pattern of historical interrelationships indicated is Guiana + ((Rond (o) over cap nia + (Para + Belem)) + (Imeri + (Napo + Inambari))). The area relationships for riodinid butterflies show substantial congruence with those presented from the literature for amphibians, reptiles, birds, primates, rodents, and marsupials, suggesting a common vicariant history for these organisms. A summary area cladogram generated by combining area cladograms for all the aforementioned groups of organisms indicated the pattern of historical interrelationships to be (Guiana + (Rond (o) over cap nia + (Para + Belem))) + (Imeri + (Napo + Inambari)). Charis cleonus group species distributions are noticeably larger around the upland periphery of Amazonia and smaller in the central and lower regions. A significant positive correlation between the proportion of range area above 100 m and total range size for each species is used to suggest that past sea-level rises may explain smaller range sizes in low-lying regions and that riverine barriers have been important in shaping the current distribution of C. cleonus group species. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Entomol, Washington, DC 20560 USA. EM jpwhall@hotmail.com NR 100 TC 81 Z9 86 U1 0 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD JUL PY 2002 VL 56 IS 7 BP 1489 EP 1497 PG 9 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 583WR UT WOS:000177434400016 PM 12206248 ER PT J AU Stiling, P Cattell, M Moon, DC Rossi, A Hungate, BA Hymus, G Drake, B AF Stiling, P Cattell, M Moon, DC Rossi, A Hungate, BA Hymus, G Drake, B TI Elevated atmospheric CO2 lowers herbivore abundance, but increases leaf abscission rates SO GLOBAL CHANGE BIOLOGY LA English DT Article DE elevated CO2; insect herbivory; Kennedy Space Center; leaf abscission; Quercus myrtifolia ID LONG-TERM EXPOSURE; CARBON-DIOXIDE; INSECT PERFORMANCE; DECIDUOUS TREES; LITTER QUALITY; GAS-EXCHANGE; RESPONSES; GROWTH; PHYTOCHEMISTRY; ENRICHMENT AB Increased levels of atmospheric carbon dioxide (CO2 ) are likely to affect the trophic relationships that exist between plants, their herbivores and the herbivores' natural enemies. This study takes advantage of an open-top CO2 fertilization experiment in a Florida scrub oak community at Kennedy Space Center, Florida, consisting of eight chambers supplied with ambient CO2 (360 ppm) and eight chambers supplied with elevated CO2 (710 ppm). We examined the effects of elevated CO2 on herbivore densities and levels of leaf consumption, rates of herbivore attack by natural enemies and effects on leaf abscission. Cumulative levels of herbivores and herbivore damage were significantly lower in elevated CO2 than in ambient CO2 . This may be because leaf nitrogen levels are lower in elevated CO2 . More herbivores die of host plant-induced death in elevated CO2 than in ambient CO2 . Attack rates of herbivores by parasitoids are also higher in elevated CO2 , possibly because herbivores need to feed for a longer time in order to accrue sufficient nitrogen (N), thus exposing themselves longer to natural enemies. Insect herbivores cause an increase in abscission rates of leaves throughout the year. Because of the lower insect density in elevated CO2 , we thought, abscission rates would be lower in these chambers. However, abscission rates were significantly higher in elevated CO2 . Thus, the direct effects of elevated CO2 on abscission are greater than the indirect effects on abscission mediated via lower insect densities. A consequence of increased leaf abscission in elevated CO2 is that nutrient deposition rates to the soil surface are accelerated. C1 Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Univ N Florida, Dept Nat Sci, Jacksonville, FL 33224 USA. No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Stiling, P (reprint author), Univ S Florida, Dept Biol, Tampa, FL 33620 USA. RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 49 TC 56 Z9 61 U1 1 U2 20 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD JUL PY 2002 VL 8 IS 7 BP 658 EP 667 DI 10.1046/j.1365-2486.2002.00501.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 559ZD UT WOS:000176055800005 ER PT J AU Krems, R Dalgarno, A AF Krems, R Dalgarno, A TI Electronic and rotational energy transfer in F(P-2(1/2))+H-2 collisions at ultracold temperatures SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID BOSE-EINSTEIN CONDENSATION; DILUTE ATOMIC VAPOR; DER-WAALS COMPLEXES; OPEN-SHELL ATOMS; VIBRATIONAL-RELAXATION; DIABATIC REPRESENTATIONS; MAGNETIC TRAP; MOLECULES; COLD; HCL AB The dynamics of F(P-2(1/2))+H-2 scattering at ultracold temperatures is studied. It is shown that both the rotational and vibrational excitation of H-2 molecules decrease substantially the efficiency of spin-orbit relaxation in F+H-2 collisions. It is observed that the near-resonant electronic transition leading to rotational excitation of H-2(j=0) is of the same magnitude at high energies as the off-resonant transition in which the rotational angular momentum of H-2 is preserved but becomes dominant in ultracold collisions. The zero temperature rate constant for spin-orbit relaxation of F is computed and suggestions are made as to the chemical reactivity of F(P-2(1/2)) atoms at ultracold temperatures. It is found that rotational relaxation of excited H-2 molecules is significantly enhanced by electronic transitions in F atoms and the electronic relaxation in F(P-2(1/2))+H-2(j>0) collisions is suppressed by rotational relaxation of H-2. (C) 2002 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krems, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 40 TC 22 Z9 26 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 1 PY 2002 VL 117 IS 1 BP 118 EP 123 DI 10.1063/1.1480004 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 563UT UT WOS:000176275700016 ER PT J AU Krems, RV Buchachenko, AA Markovic, N Nordholm, S AF Krems, RV Buchachenko, AA Markovic, N Nordholm, S TI Resonance and reversibility of vibrational relaxation of HF in high temperature Ar bath gas SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MOLECULAR-SCATTERING THEORY; ENERGY-TRANSFER; CROSS-SECTIONS; RATE CONSTANTS; STATES APPROXIMATION; CHEMI-LUMINESCENCE; COLLISIONS; ATOMS; DYNAMICS; H-2 AB The Boltzmann averaged rate constants for total vibrational relaxation of HF(v=1) in collisions with Ar are computed in the range of temperatures between 100 and 1500 K. The computed rate constants overestimate the experimental measurements at high temperatures by a large factor. It is concluded that the deviation between theory and experiment cannot be explained by inaccuracy of the PES or dynamical approximations made. It is shown that increasing initial rotational energy enhances a resonant character of the vibrational energy transfer to a great extent. An assumption is made that total vibrational relaxation of HF(v=1) at high temperatures is determined by competition between vibrational relaxation to a resonant level (v=0,j(res)), vibrational excitation from the resonant level, and purely rotational relaxation of HF(v=0,j(res)). It is demonstrated that at high temperatures the latter process can be significantly slower than vibrationally inelastic transitions and rotational relaxation of HF(v=0,j(res)) may in fact be a rate-limiting stage of vibrational relaxation. (C) 2002 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow MV Lomonosov State Univ, Dept Chem, Lab Mol Struct & Quantum Mech, Moscow 119899, Russia. Chalmers Univ Technol, Dept Phys Chem, SE-41296 Gothenburg, Sweden. Univ Gothenburg, Dept Chem, SE-41296 Gothenburg, Sweden. RP Krems, RV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Nordholm, Sture/A-8506-2010; Buchachenko, Alexei/C-8452-2012 OI Buchachenko, Alexei/0000-0003-0701-5531 NR 57 TC 10 Z9 10 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 1 PY 2002 VL 117 IS 1 BP 166 EP 171 DI 10.1063/1.1482373 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 563UT UT WOS:000176275700022 ER PT J AU Hoelzel, AR Fleischer, RC Campagna, C Le Boeuf, BJ Alvord, G AF Hoelzel, AR Fleischer, RC Campagna, C Le Boeuf, BJ Alvord, G TI Impact of a population bottleneck on symmetry and genetic diversity in the northern elephant seal SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE bottleneck; fluctuating asymmetry; genetic diversity; marine mammal ID FLUCTUATING ASYMMETRY; VARIABILITY; GHOST; MICE AB The northern elephant seal (NES) suffered a severe population bottleneck towards the end of the nineteenth century. Theoretical expectations for the impact of population bottlenecks include the loss of genetic diversity and a loss of fitness (e.g. through a disruption of developmental stability); however, there are few direct demonstrations in natural populations. Here, we report on the comparison of archive samples collected prior to and following the NES population bottleneck. Measures of genetic diversity show a loss of variation consistent with expectations and suggest a strong disruption in the pattern of allele frequencies following the bottleneck. Measures of bilateral characters show an increase in fluctuating asymmetry. C1 Univ Durham, Dept Biol Sci, Durham DH1 3LE, England. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. Consejo Nacl Invest Cient & Tecn, Ctr Nacl Patagonico, RA-9120 Puerto Madryn, Chubut, Argentina. Univ Calif Santa Cruz, Dept Biol, Santa Cruz, CA 95064 USA. NCI, Data Management Serv Inc, FCRDC, Frederick, MD 21702 USA. RP Hoelzel, AR (reprint author), Univ Durham, Dept Biol Sci, South Rd, Durham DH1 3LE, England. OI Campagna, Claudio/0000-0002-7971-5062 NR 51 TC 66 Z9 68 U1 3 U2 51 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD JUL PY 2002 VL 15 IS 4 BP 567 EP 575 DI 10.1046/j.1420-9101.2002.00419.x PG 9 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 564NE UT WOS:000176319800008 ER PT J AU Irwin, RP Howard, AD AF Irwin, RP Howard, AD TI Drainage basin evolution in Noachian Terra Cimmeria, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; highlands; drainage basins; erosion; valleys ID SMALL MARTIAN VALLEYS; MARGARITIFER SINUS; CHANNELS; MORPHOLOGY; HIGHLANDS; SURFACE; AGE AB [1] Geomorphic mapping of a similar to1 million square kilometer section of Terra Cimmeria on Mars (1: 1M scale) indicates that prolonged, intense fluvial erosion occurred during the period of heavy bombardment. Crater counts date the termination of ubiquitous, intense erosion to the late Noachian, although some valleys may have continued downcutting into the early Hesperian. Stratigraphic and topographic relationships indicate that early erosional processes created large, integrated drainage basins, affected primarily by large impact basin structures and regional slopes. This terrain is not consistent with an origin purely by volcanic or impact processes. Cratering competed with drainage basin development, minimizing valley length, catchment area, and valley network integration. Drainage basin disruption resulted from impacts on valley thalwegs, or when the ejecta of large (usually >75 km) craters created low divides. Near-level upland intercrater plains are lightly dissected, in part because smaller craters could interrupt flow paths on gently sloping or flat terrain. Some closed drainage basins became integrated by continued erosion of drainage divides and stream capture, overflow of the divides, or headward growth of valleys fed by groundwater collected in closed basins. Drainage divide breaching was most effective on steeper (>0.5degrees) regional slopes, where observed drainage density is also highest. This is due to greater runoff volumes and velocity encouraging valley incision, as well as steep slopes allowing valleys to bypass or breach superimposed craters. Valley systems commonly extend nearly to the crests of sharp drainage divides, and spatially ubiquitous valley source points throughout the higher elevations suggest that runoff derived largely from precipitation. C1 Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Irwin, RP (reprint author), Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA. NR 49 TC 59 Z9 59 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUL PY 2002 VL 107 IS E7 AR 5056 DI 10.1029/2001JE001818 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 610UB UT WOS:000178978400001 ER PT J AU Oftedal, OT AF Oftedal, OT TI The mammary gland and its origin during synapsid evolution SO JOURNAL OF MAMMARY GLAND BIOLOGY AND NEOPLASIA LA English DT Review DE mammary gland; cutaneous gland; evolution; Synapsida; monotreme; marsupial ID MARSUPIAL MILK OLIGOSACCHARIDES; MACROPUS-EUGENII; TAMMAR WALLABY; MONODELPHIS-DOMESTICA; TRICHOSURUS-VULPECULA; LACTOSE BIOSYNTHESIS; ALPHA-LACTALBUMIN; SEBACEOUS GLANDS; PARENTAL CARE; LACTATION AB Lactation appears to be an ancient reproductive trait that predates the origin of mammals. The synapsid branch of the amniote tree that separated from other taxa in the Pennsylvanian (>310 million years ago) evolved a glandular rather than scaled integument. Repeated radiations of synapsids produced a gradual accrual of mammalian features. The mammary gland apparently derives from an ancestral apocrine-like gland that was associated with hair follicles. This association is retained by monotreme mammary glands and is evident as vestigial mammary hair during early ontogenetic development of marsupials. The dense cluster of mammo-pilo-sebaceous units that open onto a nipple-less mammary patch in monotremes may reflect a structure that evolved to provide moisture and other constituents to permeable eggs. Mammary patch secretions were coopted to provide nutrients to hatchlings, but some constituents including lactose may have been secreted by ancestral apocrine-like glands in early synapsids. Advanced Triassic therapsids, such as cynodonts, almost certainly secreted complex, nutrient-rich milk, allowing a progressive decline in egg size and an increasingly altricial state of the young at hatching. This is indicated by the very small body size, presence of epipubic bones, and limited tooth replacement in advanced cynodonts and early mammaliaforms. Nipples that arose from the mammary patch rendered mammary hairs obsolete, while placental structures have allowed lactation to be truncated in living eutherians. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Conservat Biol, Washington, DC 20008 USA. RP Oftedal, OT (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Conservat Biol, Washington, DC 20008 USA. NR 146 TC 89 Z9 94 U1 7 U2 43 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1083-3021 J9 J MAMMARY GLAND BIOL JI J. Mammary Gland Biol. Neoplasia PD JUL PY 2002 VL 7 IS 3 BP 225 EP 252 DI 10.1023/A:1022896515287 PG 28 WC Oncology; Endocrinology & Metabolism; Physiology SC Oncology; Endocrinology & Metabolism; Physiology GA 654PR UT WOS:000181505700002 PM 12751889 ER PT J AU Oftedal, OT AF Oftedal, OT TI The origin of lactation as a water source for parchment-shelled eggs SO JOURNAL OF MAMMARY GLAND BIOLOGY AND NEOPLASIA LA English DT Article DE lactation; egg physiology; water balance; endothermy; evolution; monotreme ID REPTILIAN EGGS; MAMMALIAN ENDOTHERMY; BIRD EGGS; EVOLUTION; INCUBATION; EMBRYOS; PLACENTATION; CONDUCTANCE; ENERGY; CYNOGNATHUS AB Available evidence indicates that mammary gland secretions first evolved in synapsids that laid parchment-shelled eggs. Unlike the rigid-shelled eggs of birds and some other sauropsids, parchment-shelled eggs lose water very rapidly when exposed to ambient air of lower vapor pressure, whether due to differences in relative humidity or to differences in temperature. This precludes endothermic incubation of parchment-shelled eggs in an open nest. Synapsids may have avoided egg desiccation by incubating eggs in a pouch, but this would limit maternal activity. Parchment-shelled eggs are able to take up liquid water across the eggshell. I propose that mammary secretion originally evolved as a means of supplying water to eggs, and as such was essential to the evolution of endothermy among the egg-laying cynodonts that were ancestral to mammals. It is possible that synapsid eggs, like parchment-shelled squamate eggs, were also capable of uptake of some nutrients, such as sodium and ionic calcium. Living monotremes still produce parchment-shelled eggs. The porous eggshell and bilaminar yolk sac membrane of these eggs permit substantial uptake of uterine secretions during the intrauterine period, and might also facilitate uptake of mammary secretions during egg incubation. In its simplest form, mammary secretion may be an ancient trait of egg-laying synapsids, having had an important role long before milk became obligatory for suckling young. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Conservat Biol, Washington, DC 20008 USA. RP Oftedal, OT (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Conservat Biol, Washington, DC 20008 USA. NR 96 TC 54 Z9 55 U1 4 U2 23 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1083-3021 J9 J MAMMARY GLAND BIOL JI J. Mammary Gland Biol. Neoplasia PD JUL PY 2002 VL 7 IS 3 BP 253 EP 266 DI 10.1023/A:1022848632125 PG 14 WC Oncology; Endocrinology & Metabolism; Physiology SC Oncology; Endocrinology & Metabolism; Physiology GA 654PR UT WOS:000181505700003 PM 12751890 ER PT J AU Murphy, KR Ritz, D Hewitt, CL AF Murphy, KR Ritz, D Hewitt, CL TI Heterogeneous zooplankton distribution in a ship's ballast tanks SO JOURNAL OF PLANKTON RESEARCH LA English DT Article ID VERTICAL MIGRATION; MARINE ORGANISMS; INVASION; WATER AB We examined the vertical distribution of zooplankton in a ship's ballast water. Some crustacean taxa were more abundant at 0.5 m and 2 m than at 6 m depths. Non-random distributions affect population size estimations and are an important consideration for invasion risk assessment. C1 Univ Tasmania, Dept Zool, Hobart, Tas 7001, Australia. CSIRO Marine Res, Ctr Res Introduced Marine Pests, Hobart, Tas 7001, Australia. RP Murphy, KR (reprint author), Smithsonian Environm Res Ctr, Marine Invas Res Lab, POB 28, Edgewater, MD 21037 USA. RI Murphy, Kathleen/B-8217-2009; Hewitt, Chad/C-4460-2008 OI Murphy, Kathleen/0000-0001-5715-3604; Hewitt, Chad/0000-0002-6859-6512 NR 26 TC 25 Z9 28 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0142-7873 J9 J PLANKTON RES JI J. Plankton Res. PD JUL PY 2002 VL 24 IS 7 BP 729 EP 734 DI 10.1093/plankt/24.7.729 PG 6 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 574VD UT WOS:000176909500010 ER PT J AU Engelbrecht, BMJ Wright, SJ De Steven, D AF Engelbrecht, BMJ Wright, SJ De Steven, D TI Survival and ecophysiology of tree seedlings during El Nino drought in a tropical moist forest in Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE El Nino Southern Oscillation; tropical forest; Panama; Quararibea asterolepis; seedling survival; stomatal conductance; Tetragastris panamensis; Trichilia tuberculata; water relations ID RAIN-FOREST; SEASONAL DROUGHT; CARBON-DIOXIDE; UNDERSTORY; RESPONSES; IMPACT; GROWTH; GAP AB In tropical forests, severe droughts caused by El Nino events may strongly influence the water relations of tree seedlings and thereby increase their mortality. Data on known-aged seedlings of three common shade-tolerant canopy tree species (Trichilia tuberculata, Tetragastris panamensis and Quararibea asterolepis) in a Panamanian moist forest are presented. Seedling survival during a severe El Nino dry season (1997-98) was compared with prior long-term survival data, and levels of drought stress were assessed by measuring plant water potentials and gas exchange characteristics. Contrary to prediction, dry-season seedling survival was not dramatically reduced in any species compared with that expected in 'normal' years. In Trichilia and Quararibea, pre-dawn water potentials averaged -2 MPa and midday water potentials about -3 MPa. Stomatal conductances were very low, averaging 26 mmol m(-2) s(-1) for Tetragastris and 11-13 mmol m(-2) s(-1) for Trichilia and Quararibea. Photosynthetic rates also were very low but consistently positive, averaging 0.8-1.1 mumol m(-2) s(-1). The findings suggest that, once established, seedlings of common tree species in this semi-deciduous forest may be tolerant of drought events. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. US Forest Serv, USDA, So Res Stn, Ctr Forested Wetlands Res, Charleston, SC 29414 USA. RP Engelbrecht, BMJ (reprint author), Smithsonian Trop Res Inst, Apdo 2072, Balboa, Panama. RI Engelbrecht, Bettina/E-9914-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 30 TC 18 Z9 21 U1 0 U2 16 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 JUL PY 2002 VL 18 BP 569 EP 579 DI 10.1017/S0266467402002377 PN 4 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 582KK UT WOS:000177349500005 ER PT J AU Cook, RC Cook, JG Garrott, RA Irwin, LL Monfort, SL AF Cook, RC Cook, JG Garrott, RA Irwin, LL Monfort, SL TI Effects of diet and body condition on fecal progestagen excretion in elk SO JOURNAL OF WILDLIFE DISEASES LA English DT Article DE abortion; Cervus elaphus; condition; elk; nutrition; pregnancy detection; progesterone; reproduction ID PAPIO-CYNOCEPHALUS-CYNOCEPHALUS; NUTRITIONAL CONDITION; STEROID METABOLITES; BEEF HEIFERS; PROGESTERONE; DYNAMICS; MODELS; FECES; FLOW; DEER AB Recent research demonstrated the utility of fecal progestagens (P-4) for detecting pregnancy in elk (Cervus elaphus) during mid- to late gestation. Several factors, however, may influence fecal P-4 excretion and limit its use in free-ranging animals. We investigated the effects of nutrition and body condition (percent ingesta-free body fat) on fecal P-4 concentrations and incidence of abortion. During mid-gestation (late December 1997 through early March 1998), 40 gravid cow elk varying in body condition were placed on three diets (high, medium, and low) in which the amount of food offered varied. Feces were collected periodically and analyzed for P-4 via radioimmunoassay. We found no significant effect of dietary treatment on P-4 concentrations, but as body condition declined, P-4 concentrations declined significantly. This decline did not impede the ability to detect pregnancy based on previously reported criteria, even for elk in such poor condition that they aborted. However, fecal P-4 concentrations in 10% (4/39) of samples collected from 13 non-pregnant animals maintained on a high plane of nutrition were false-positive for pregnancy. We suggest alternate criteria for determining pregnancy in elk using fecal P-4 values: >1.25 mug/g feces as pregnant, <1.0 μg/g feces as non-pregnant, and 1.0-1.25 μg/g feces as inconclusive. Finally, two cows that aborted did not abort until weeks after being classified as emaciated and near death, suggesting that nutrition-associated abortion in elk may not occur during mid-gestation except under extremely harsh conditions. C1 Natl Council Air & Stream Improvement, Forestry & Range Sci Lab, La Grande, OR 97850 USA. Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA. Natl Council Air & Stream Improvement, Bozeman, MT 59870 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Cook, RC (reprint author), Natl Council Air & Stream Improvement, Forestry & Range Sci Lab, 1401 Gekeler Lane, La Grande, OR 97850 USA. NR 30 TC 15 Z9 16 U1 4 U2 12 PU WILDLIFE DISEASE ASSN, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD JUL PY 2002 VL 38 IS 3 BP 558 EP 565 PG 8 WC Veterinary Sciences SC Veterinary Sciences GA 593UX UT WOS:000178013100010 PM 12238373 ER PT J AU Riley, S AF Riley, S TI The middle ages. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst Libs, 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 JUL PY 2002 VL 127 IS 12 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 572UB UT WOS:000176792400274 ER PT J AU Dalebout, ML Mead, JG Baker, CS Baker, AN van Helden, AL AF Dalebout, ML Mead, JG Baker, CS Baker, AN van Helden, AL TI A new species of beaked whale Mesoplodon perrini sp N. (Cetacea : Ziphiidae) discovered through phylogenetic analyses of mitochondrial DNA sequences SO MARINE MAMMAL SCIENCE LA English DT Article DE molecular genetics and systematics; morphology; external appearance; natural history; distribution; Mesoplodon perrini; Perrin's beaked whale ID MOLECULAR-GENETIC IDENTIFICATION; POPULATION-STRUCTURE; NORTH PACIFIC; ANCIENT DNA; MORPHOLOGY; EXTRACTION; WATERS; BONES AB Mesoplodon perrini, a new species of beaked whale is described on the basis of five animals stranded on the coast of California (between 32degrees55'N, 117degrees15'W and 36degrees37'N, 121degrees55'W) from May 1975 to September 1997. Four of these animals were initially identified as Hector's beaked whales M. hectori based on cranial morphology (Mead 1981). A fifth specimen was initially identified as a neonate Cuvier's beaked whale Ziphius cavirostris based on external features. These specimens were first recognized as representatives of an undescribed species through phylogenetic analysis of mitochondrial (mt) DNA control region and cytochrome b sequence data. Although similar morphologically, the genetic data do not support a close evolutionary relationship between M. perrini and M. hectori, Instead, these data suggest a possible sister-species relationship with the lesser beaked whale M, peruvianus. Sightings of two small beaked whales off California in the 197 Os which were tentatively identified as M. hectori are also likely to be M, perrini, We suggest that M. hectori is confined to the Southern Hemisphere, while M. perrini is known to date only from the North Pacific. C1 Univ Auckland, Sch Biol Sci, Auckland 1000, New Zealand. Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. Dept Conservat, Sci & Res Unit, Wellington, New Zealand. Museum New Zealand Te Papa Tongarewa, Wellington, New Zealand. RP Baker, CS (reprint author), Univ Auckland, Sch Biol Sci, Private Bag 92019, Auckland 1000, New Zealand. NR 46 TC 69 Z9 85 U1 0 U2 12 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 JUL PY 2002 VL 18 IS 3 BP 577 EP 608 DI 10.1111/j.1748-7692.2002.tb01061.x PG 32 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 569YF UT WOS:000176630200001 ER PT J AU Benedix, GK McCoy, TJ AF Benedix, GK McCoy, TJ TI Aqueous alteration in CM chondrites from elephant moraine. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 7 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 JUL PY 2002 VL 37 IS 7 SU S BP A14 EP A14 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700013 ER PT J AU Burbine, TH McCoy, TJ Jarosewich, E Sunshine, JM AF Burbine, TH McCoy, TJ Jarosewich, E Sunshine, JM TI How much compositional information can be derived from the reflectance spectrum of an asteroid? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Sci Applicat Int Corp, Adv Technol Applicat Div, Chantilly, VA 20151 USA. NR 4 TC 0 Z9 0 U1 2 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2002 VL 37 IS 7 SU S BP A27 EP A27 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700039 ER PT J AU Bus, SJ Sunshine, JM Burbine, TH McCoy, TJ Binzel, RP AF Bus, SJ Sunshine, JM Burbine, TH McCoy, TJ Binzel, RP TI Spectral evidence for the igneous nature of Agnia and Merxia family asteroids. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract C1 Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. Sci Applicat Int Corp, Chantilly, VA 20151 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. NR 4 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 JUL PY 2002 VL 37 IS 7 SU S BP A28 EP A28 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700040 ER PT J AU Clarke, RS Plotkin, H AF Clarke, RS Plotkin, H TI Frederick C. Leonard (1896-1960): First UCLA astronomer and founding father of the meteoritical society. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Univ Western Ontario, Dept Philosophy, London, ON N6A 3K7, Canada. NR 1 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 JUL PY 2002 VL 37 IS 7 SU S BP A34 EP A34 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700053 ER PT J AU Cosarinsky, M Leshin, LA MacPherson, GJ Krot, AN Guan, Y AF Cosarinsky, M Leshin, LA MacPherson, GJ Krot, AN Guan, Y TI Oxygen isotopic composition of olivines from matrices and accretionary rims around Ca-Al-rich inclusions in CV chondrites. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Arizona State Univ, Ctr Meteorites Studies, Tempe, AZ 85287 USA. Smithsonian Inst, NMNH, Dept Mineral Sci, Washington, DC 20560 USA. Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. NR 7 TC 4 Z9 4 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 JUL PY 2002 VL 37 IS 7 SU S BP A38 EP A38 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700061 ER PT J AU French, BM AF French, BM TI Craters in the mainstream: The new role of meteorite impact as a normal geological process. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. NR 0 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 JUL PY 2002 VL 37 IS 7 SU S BP A50 EP A50 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700084 ER PT J AU Guan, Y Huss, GR MacPherson, GJ Leshin, LA AF Guan, Y Huss, GR MacPherson, GJ Leshin, LA TI Rare earth elements of calcium-aluminum-rich inclusions in unequilibrated enstatite chondrites: Characteristics and implications. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract ID SOLAR NEBULA; OXYGEN ISOTOPES C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Arizona State Univ, Ctr Meteorite Studies, Tempe, AZ 85287 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 7 TC 2 Z9 2 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 JUL PY 2002 VL 37 IS 7 SU S BP A59 EP A59 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700102 ER PT J AU Huss, GR MacPherson, GJ Davis, AM Krot, AN Ulyanov, AA AF Huss, GR MacPherson, GJ Davis, AM Krot, AN Ulyanov, AA TI Microdistribution of REE in fine-grained group IICAIs in Efremovka. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract ID RARE-EARTH ELEMENTS; SOLAR NEBULA; FRACTIONATION; CONDENSATION; METEORITE C1 Moscow MV Lomonosov State Univ, Moscow 117999, Russia. Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. Smithsonian Inst, US Museum Nat Hist, Washington, DC 20560 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. NR 5 TC 6 Z9 6 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 JUL PY 2002 VL 37 IS 7 SU S BP A68 EP A68 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700118 ER PT J AU Kim, GL MacPherson, GJ Rumble, D AF Kim, GL MacPherson, GJ Rumble, D TI In situ oxygen isotope analysis of HED breccias with UV-laser microprobe. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract C1 Geophys Lab, Washington, DC 20015 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 7 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 JUL PY 2002 VL 37 IS 7 SU S BP A77 EP A77 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700137 ER PT J AU Krot, AN Hohenberg, CM Meshik, AP Pravdivtseva, OV Hiyagon, H Petaev, MI Weisberg, MK Meibom, A Keil, K AF Krot, AN Hohenberg, CM Meshik, AP Pravdivtseva, OV Hiyagon, H Petaev, MI Weisberg, MK Meibom, A Keil, K TI Two-stage asteroidal alteration of the allende dark inclusions. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract ID CHONDRITES C1 Stanford Univ, Stanford, CA 94305 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Tokyo, Japan. Washington Univ, St Louis, MO 63130 USA. Univ Hawaii, Honolulu, HI 96822 USA. NR 2 TC 4 Z9 4 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 JUL PY 2002 VL 37 IS 7 SU S BP A82 EP A82 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700147 ER PT J AU Lentz, RCF McCoy, TJ AF Lentz, RCF McCoy, TJ TI Insights on mixed basaltic shergottites from a xenolith-bearing Hawaiian basalt. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract ID METEORITES C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Univ Tennessee, Dept Geol Sci, Knoxville, TN 37996 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2002 VL 37 IS 7 SU S BP A86 EP A86 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700154 ER PT J AU MacPherson, GJ Krot, AN AF MacPherson, GJ Krot, AN TI Distribution of Ca-Fe-silicates in CV3 chondrites: Possible controls by parent-body compaction. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract C1 Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Smithsonian Inst, US Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 4 TC 15 Z9 15 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 JUL PY 2002 VL 37 IS 7 SU S BP A91 EP A91 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700165 ER PT J AU Vicenzi, EP Fish, MR Treiman, A Wilson, S AF Vicenzi, EP Fish, MR Treiman, A Wilson, S TI Comparison of clay minerals produced during low-temperature alteration of mafic rocks from Earth and Mars. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract ID LAFAYETTE SNC METEORITE; AQUEOUS ALTERATION C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Oregon State Univ, Coll Ocean & Atm Sci, Corvallis, OR 97331 USA. Lunar & Planetary Inst, Houston, TX USA. NR 3 TC 2 Z9 2 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 JUL PY 2002 VL 37 IS 7 SU S BP A144 EP A144 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 581CZ UT WOS:000177274700270 ER PT J AU Kooistra, WHCF Coppejans, EGG Payri, C AF Kooistra, WHCF Coppejans, EGG Payri, C TI Molecular systematics, historical ecology, and phylogeography of Halimeda (Bryopsidales) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Review DE calcareous algae; cognate; convergence; dispersal; fossil; Halimeda; historical ecology; iterative evolution; ITS; phylogeny; phylogeography; rDNA; vicariance ID TRANSCRIBED SPACER SEQUENCES; MESSINIAN SALINITY CRISIS; NUCLEAR RIBOSOMAL DNA; GREEN-ALGAE; CORAL-REEFS; MORPHOLOGICAL DEFENSES; GLOBAL PHYLOGEOGRAPHY; CONCERTED EVOLUTION; SECONDARY STRUCTURE; CAULERPA-TAXIFOLIA AB Halimeda (Bryopsidales), a genus of calcified, segmented green seaweeds, abounds in reefs and lagoons throughout the tropics. To investigate phylogenetic, phylogeographic, and historic ecological relationships of the genus, the nuclear rDNA including the SSU and both ITS regions were sequenced. A maximum likelihood tree revealed the following: (1) there were anatomical and morphological synapomorphies for five well-supported lineages; (2) the last common ancestor of one lineage invaded sandy substrata; those of two other lineages established in wave-affected habitats, whereas the cenancestor of the remaining two lineages occupied sheltered rocky slopes. Yet, several species adapted to new habitats subsequently, resulting in several cases of convergence; (3) all lineages separated into Atlantic and Indo-Pacific daughters, likely resulting from the rise of the Panamanian Isthmus. Each daughter pair gave rise to additional convergent species in similar habitats in different oceans; (4) Halimeda opuntia, the only monophyletic pantropical species detected so far, dispersed from the Indo-Pacific into the Atlantic well after the closure event; (5) minor SSU-sequence differences across species and phylogeographic patterns of vicariance indicated a relatively recent diversification of the extant diversity. Cretaceous and Early Tertiary fossil look-alikes of modern species must then have resulted from iterative convergence. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Ghent, Dept Bot, Res Grp Phycol, B-9000 Ghent, Belgium. Univ Francaise Pacifique, Lab Ecol Marine, Tahiti, Fr Polynesia. RP Kooistra, WHCF (reprint author), Staz Zool Anton Dohrn, I-80121 Naples, Italy. EM kooistra@alpha.szn.it OI Kooistra, Wiebe/0000-0002-8641-9739 NR 122 TC 48 Z9 51 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 JUL PY 2002 VL 24 IS 1 BP 121 EP 138 AR PII S1055-7903(02)00221-X DI 10.1016/S1055-7903(02)00221-X PG 18 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 580KN UT WOS:000177233900011 PM 12128033 ER PT J AU Springel, V Hernquist, L AF Springel, V Hernquist, L TI Cosmological smoothed particle hydrodynamics simulations: the entropy equation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : evolution; galaxies : starburst ID GALAXY FORMATION; INTERGALACTIC MEDIUM; ALPHA FOREST; SPH CODE; EVOLUTION; TREESPH; STARS; GAS; CONSERVATION; METHODOLOGY AB We discuss differences in simulation results that arise between the use of either the thermal energy or the entropy as an independent variable in smoothed particle hydrodynamics (SPH). In this context, we derive a new version of SPH that, when appropriate, manifestly conserves both energy and entropy if smoothing lengths are allowed to adapt freely to the local mass resolution. To test various formulations of SPH, we consider point-like energy injection, as in certain models of supernova feedback, and find that powerful explosions are well represented by SPH even when the energy is deposited into a single particle, provided that the entropy equation is integrated. If the thermal energy is instead used as an independent variable, unphysical solutions can be obtained for this problem. We also examine the radiative cooling of gas spheres that collapse and virialize in isolation, and of haloes that form in cosmological simulations of structure formation. When applied to these problems, the thermal energy version of SPH leads to substantial overcooling in haloes that are resolved with up to a few thousand particles, while the entropy formulation is biased only moderately low for these haloes under the same circumstances. For objects resolved with much larger particle numbers, the two approaches yield consistent results. We trace the origin of the differences to systematic resolution effects in the outer parts of cooling flows. When the thermal energy equation is integrated and the resolution is low, the compressional heating of the gas in the inflow region is underestimated, violating entropy conservation and improperly accelerating cooling. The cumulative effect of this overcooling can be significant. In cosmological simulations of moderate size, we find that the fraction of baryons which cool and condense can be reduced by up to a factor similar to2 if the entropy equation is employed rather than the thermal energy equation, partly explaining discrepancies with semi-analytic treatments of galaxy formation. We also demonstrate that the entropy method leads to a greatly reduced scatter in the density-temperature relation of the low-density Lyalpha forest relative to the thermal energy approach, in accord with theoretical expectations. 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 51 TC 618 Z9 621 U1 1 U2 9 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL PY 2002 VL 333 IS 3 BP 649 EP 664 DI 10.1046/j.1365-8711.2002.05445.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 568EX UT WOS:000176530400017 ER PT J AU Lira, P Ward, MJ Zezas, A Murray, SS AF Lira, P Ward, MJ Zezas, A Murray, SS TI Chandra HRC and HST observations of NGC 6240: resolving the active galactic nucleus and starburst SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : individual : NGC 6240; galaxies : starburst; X-rays : galaxies ID INFRARED GALAXY NGC-6240; X-RAY-EMISSION; ENERGY-DISTRIBUTIONS; DUST; ARP-220 AB We present high spatial resolution X-ray Chandra HRC and HST WFPC2 Halpha observations of the prototypical infrared-luminous galaxy NGC 6240. The central region of this system shows a remarkably complex morphology, with filaments and loops observed in the optical and X-rays. The total X-ray luminosity is dominated by the extended emission. Both nuclei are clearly detected in the HRC image and both appear to be extended. The energetics of the nuclei imply that the southern nucleus is the more plausible counterpart to the obscured active galactic nucleus. The overall spectral energy distribution of the galaxy is in good agreement with a blend of starburst and AGN components that have similar bolometric luminosities, L (bol) similar to5x10(45) erg s(-1), with the starburst dominating the observed continuum in the near-infrared (K band), optical and soft X-ray bands. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Chile, Dept Astron, Santiago, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lira, P (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RI Lira, Paulina/G-8536-2016; Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 27 TC 34 Z9 34 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL PY 2002 VL 333 IS 3 BP 709 EP 714 DI 10.1046/j.1365-8711.2002.05456.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 568EX UT WOS:000176530400022 ER PT J AU Gardner, JB Merritt, E AF Gardner, JB Merritt, E TI Collections planning: Pinning down a strategy SO MUSEUM NEWS LA English DT Article C1 Smithsonian Inst, Natl Museum Amer Hist, Behring Ctr, Washington, DC 20560 USA. RP Gardner, JB (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Behring Ctr, Washington, DC 20560 USA. NR 0 TC 1 Z9 2 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD JUL-AUG PY 2002 VL 81 IS 4 BP 30 EP + PG 0 WC Art SC Art GA 609NU UT WOS:000178912500026 ER PT J AU Butt, YM Torres, DF Combi, JA Dame, T Romero, GE AF Butt, YM Torres, DF Combi, JA Dame, T Romero, GE TI Acceleration of cosmic ray protons in the supernova remnant RX J1713.7-3946? SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Workshop of the Max-Planck-Gesellschaft CY MAY, 2001 CL RINGBERG CASTLE, GERMANY SP Max Planck Gesell DE cosmic rays; interstellar medium; supernova remnants C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. Inst Argentino Radioastron, RA-1894 Buenos Aires, DF, Argentina. RP Butt, YM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Torres, Diego/O-9422-2016 OI Torres, Diego/0000-0002-1522-9065 NR 0 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD JUL PY 2002 VL 46 IS 8-10 BP 565 EP 565 AR PII S1387-6473(02)00202-6 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 582VT UT WOS:000177372400021 ER PT J AU Gilbert, GS Mejia-Chang, M Rojas, E AF Gilbert, GS Mejia-Chang, M Rojas, E TI Fungal diversity and plant disease in mangrove forests: salt excretion as a possible defense mechanism SO OECOLOGIA LA English DT Article DE Avicennia germinans; Laguncularia racemosa; Panama; plant disease resistance; Rhizophora mangle ID RAIN-FOREST; DENSITY; TREE; ENDOPHYTES; SEEDLINGS; INFECTION; DISTANCE; ECOLOGY; LIGHT; RUST AB Salt excretion in leaves of some mangrove species may serve as an important defense against fungal attack, reducing the vulnerability of typically high-density, monospecific forest stands to severe disease pressure. In field surveys of a Caribbean mangrove forest in Panama, Avicennia germinans suffered much less damage from foliar diseases than did Laguncularia racemosa or Rhizophora mangle. Similarly, Avicennia leaves supported the least superficial fungal growth, endophytic colonization, and diversity, followed by Laguncularia and Rhizophora. Host specificity of leaf-colonizing fungi was greater than expected at random. We hypothesize that the different salt tolerance mechanisms in the three mangrove species may differentially regulate fungal colonization. The mangroves differ in their salt tolerance mechanisms such that Avicennia (which excretes salt through leaf glands) has the highest salinity of residual rain water on leaves, Laguncularia (which accumulates salt in the leaves) has the greatest bulk salt concentration, and Rhizophora (which excludes salt at the roots) has little salt associated with leaves. The high salt concentrations associated with leaves of Avicennia and Laguncularia, but not the low salinity of Rhizophora, were sufficient to inhibit the germination of many fungi associated with mangrove forests. C1 Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. RP Gilbert, GS (reprint author), Univ Calif Santa Cruz, Dept Environm Studies, 1156 High St, Santa Cruz, CA 95064 USA. EM ggilbert@cats.ucsc.edu RI Gilbert, Gregory/C-2595-2008 NR 34 TC 20 Z9 30 U1 3 U2 35 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 JUL PY 2002 VL 132 IS 2 BP 278 EP 285 DI 10.1007/s00442-002-0966-9 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 580PL UT WOS:000177242900017 ER PT J AU Chung, HK Dalgarno, A AF Chung, HK Dalgarno, A TI Diffusion of hydrogen atoms in helium gas and helium atoms in hydrogen gas SO PHYSICAL REVIEW A LA English DT Article ID H-HE AB The potential of Meyer and Frommhold describing the interaction between hydrogen and helium atoms is used to calculate the diffusion coefficients of hydrogen atoms in helium gas and helium atoms in hydrogen gas as functions of temperature, taking into account higher-order corrections of transport theory. Comparison with experiment suggests that the interaction potential should be steepened at small nuclear separations. Calculations of the diffusion coefficients for temperatures between zero and 1000 K with the modified potential are reported. The corresponding H-He scattering length resulting from the zero-temperature value of the diffusion coefficients has the magnitude 0.359a(0). Direct calculation shows it to be negative. C1 Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chung, HK (reprint author), Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. NR 10 TC 0 Z9 0 U1 2 U2 5 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 JUL PY 2002 VL 66 IS 1 AR 012712 DI 10.1103/PhysRevA.66.012712 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 579WH UT WOS:000177200800058 ER PT J AU Krems, RV Dalgarno, A AF Krems, RV Dalgarno, A TI Shape resonances and nonadiabatic dynamics in O(P-3(j))+He collisions at cold and ultracold temperatures SO PHYSICAL REVIEW A LA English DT Article ID FINE-STRUCTURE TRANSITIONS; BOSE-EINSTEIN CONDENSATION; ATOM-MOLECULE COLLISIONS; VIBRATIONAL-RELAXATION; INTRAMULTIPLET TRANSITIONS; ELECTRON-SCATTERING; ENERGY-TRANSFER; EXCITED-STATES; QUANTUM; MATRIX AB The dynamics of the elastic and inelastic scattering of helium atoms in collisions with oxygen atoms in different fine-structure levels O(P-3(j)) at cold and ultracold temperatures is investigated using two sets of interaction potentials of the molecule HeO in the ground Sigma and Pi states. Scattering resonances occur in the collisions at low energies. The positions and shapes of the resonance peaks in the inelastic channels do not always mirror those in the elastic channels. The real parts of the scattering lengths are all positive with values in the range 2.5-4.2 Angstrom. The rate coefficients for the quenching of the P-3(0) and P-3(1) fine-structure levels decrease almost by one order of magnitude as the temperature decreases from 1 to 0 K and their zero temperature values are, respectively, 3.09x10(-12) and 3.27x10(-12) cm(3) sec(-1). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krems, RV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 7 Z9 7 U1 1 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL PY 2002 VL 66 IS 1 AR 012702 DI 10.1103/PhysRevA.66.012702 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 579WH UT WOS:000177200800048 ER PT J AU Yelin, SF Hemmer, PR AF Yelin, SF Hemmer, PR TI Resonantly enhanced nonlinear optics in semiconductor quantum wells: An application to sensitive infrared detection SO PHYSICAL REVIEW A LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; PHASE CONJUGATION; FANO INTERFERENCE; SCATTERING; EXCITATIONS; EFFICIENT; PHONONS; SODIUM AB A novel class of coherent nonlinear optical phenomena, involving induced transparency in semiconductor quantum wells, is considered in the context of a particular application to sensitive long-wavelength infrared detection. It is shown that the strongest decoherence mechanisms can be suppressed or mitigated, resulting in substantial enhancement of nonlinear optical effects in semiconductor quantum wells. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Hanscom Air Force Res Lab, Sensors Directorate, Bedford, MA 01731 USA. Texas A&M Univ, Dept Elect Engn, College Stn, TX 77843 USA. RP Yelin, SF (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 27 Z9 27 U1 0 U2 1 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 JUL PY 2002 VL 66 IS 1 AR 013803 DI 10.1103/PhysRevA.66.013803 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 579WH UT WOS:000177200800113 ER PT J AU Norrbom, AL AF Norrbom, AL TI A new species and key for the genus Zonosemata Benjamin (Diptera : Tephritidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Zonosentata; fruit flies; taxonomy; host plant; distribution; Solanum AB New taxonomic, host, and distribution data for species of Zonosemata are presented. One new species. Z. guybushi, reared from fruit of Solanum lanceifolium in Costa Rica. is described, and a revised key to the eight known species of this genus is provided. A neotype is designated for Z. electa (Say). C1 USDA, Smithsonian Inst, Natl Museum Nat Hist, PSI,Systemat Entomol Lab, Washington, DC 20560 USA. RP Norrbom, AL (reprint author), USDA, Smithsonian Inst, Natl Museum Nat Hist, PSI,Systemat Entomol Lab, Washington, DC 20560 USA. NR 21 TC 3 Z9 3 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2002 VL 104 IS 3 BP 614 EP 623 PG 10 WC Entomology SC Entomology GA 570DG UT WOS:000176642900008 ER PT J AU Smith, DR Shinohara, A AF Smith, DR Shinohara, A TI A new genus and new species of Cephidae (Hymenoptera) from Sulawesi Utara, Indonesia SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Sulawesius; Indonesia; Athetocephinae AB Sulawesius grandoculus, n. gen., n. sp.. is described from Sulawesi Utara, Indonesia. The genus does not fit into the current classification of the Cephidae, but it is provisionally placed in the Athetocephinae, a subfamily previously known only from Madagascar. C1 USDA, Smithsonian Inst, Natl Museum Nat Hist, PSI,Systemat Entomol Lab, Washington, DC 20560 USA. RP Smith, DR (reprint author), USDA, Smithsonian Inst, Natl Museum Nat Hist, PSI,Systemat Entomol Lab, Washington, DC 20560 USA. NR 9 TC 4 Z9 6 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2002 VL 104 IS 3 BP 624 EP 628 PG 5 WC Entomology SC Entomology GA 570DG UT WOS:000176642900009 ER PT J AU Polhemus, DA AF Polhemus, DA TI A new species of micropterous damsel bug (Heteroptera : Nabidae) from Nuku Hiva, Marquesas Islands SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Heteroptera; Nabidae; Marquesas Islands ID HAWAIIAN AB A new species of micropterous damsel bug. Nabis nukuhiva, is described from the summit area of Nuku Hiva in the Marquesas Islands, and compared to other endemic Marquesan Nabidae. Illustrations of the male paramere, male endosoma, and female dorsal habitus are provided. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Polhemus, DA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 5 TC 0 Z9 1 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2002 VL 104 IS 3 BP 640 EP 645 PG 6 WC Entomology SC Entomology GA 570DG UT WOS:000176642900011 ER PT J AU Robbins, RK AF Robbins, RK TI Replacement names in the Eumaeini (Lepidoptera : Lycaenidae : Theclinae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article C1 Natl Museum Nat Hist, Entomol Sect, Dept Syst Biol, Smithsonian Inst, Washington, DC 20560 USA. RP Robbins, RK (reprint author), Natl Museum Nat Hist, Entomol Sect, Dept Syst Biol, Smithsonian Inst, Washington, DC 20560 USA. NR 3 TC 1 Z9 6 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2002 VL 104 IS 3 BP 820 EP 821 PG 2 WC Entomology SC Entomology GA 570DG UT WOS:000176642900027 ER PT J AU Baltay, C Snyder, JA Andrews, P Emmet, W Schaefer, B Sinnott, J Bailyn, C Coppi, P Oemler, A Sabbey, CN Sofia, S van Altena, W Vivas, AK Abad, C Bongiovanni, A Briceno, C Bruzual, G Della Prugna, F Magris, G Sanchez, G Sanchez, G Schenner, H Stock, J Adams, B Gebhard, M Honeycutt, RK Musser, J Rengstorff, A Ferrin, I Fuenmayor, F Hernandez, J Naranjo, O Rosenzweig, P Harris, F Geary, J AF Baltay, C Snyder, JA Andrews, P Emmet, W Schaefer, B Sinnott, J Bailyn, C Coppi, P Oemler, A Sabbey, CN Sofia, S van Altena, W Vivas, AK Abad, C Bongiovanni, A Briceno, C Bruzual, G Della Prugna, F Magris, G Sanchez, G Sanchez, G Schenner, H Stock, J Adams, B Gebhard, M Honeycutt, RK Musser, J Rengstorff, A Ferrin, I Fuenmayor, F Hernandez, J Naranjo, O Rosenzweig, P Harris, F Geary, J TI A large-area CCD camera for the Schmidt telescope at the Venezuelan National Astronomical Observatory SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID DISCOVERY AB We have designed, constructed, and put into operation a large-area CCD camera that covers a large fraction of the image plane of the 1 m Schmidt telescope at Llano del Hato in Venezuela. The camera consists of 16 CCD devices arranged in a 4 x 4 mosaic covering 2.degrees3 x 3.degrees5 of sky. The CCDs are 2048 x 2048 LORAL devices with 15 mum pixels. The camera is optimized for drift-scan photometry and objective-prism spectroscopy. The design considerations, construction features, and performance parameters are described in the following paper. C1 Yale Univ, Dept Phys, New Haven, CT 06520 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Ctr Investigac Astron, Merida 5101-A, Venezuela. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. Univ Los Andes, Merida 5251, Venezuela. USN Observ, Univ Space Res Assoc, Flagstaff, AZ 86002 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Observ, Pasadena, CA 91101 USA. RP Andrews, P (reprint author), Yale Univ, Dept Phys, POB 208121, New Haven, CT 06520 USA. EM charles.baltay@yale.edu; jeffrey.snyder@yale.edu; peter.andrews@yale.edu; william.emmet@yale.edu; schaefer@astro.as.utexas.edu; jps39@cornell.edu; bailyn@astro.yale.edu; coppi@astro.yale.edu; oemler@ociw.edu; cns@boglefunds.com; sofia@astro.yale.edu; vanalten@astro.yale.edu; vivas@astro.yale.edu; abad@cida.ve; abongiov@cid.ve; briceno@cida.ve; bruzual@cida.ve; dellap@cida.ve; magris@cida.ve; gerardo@cida.ve; sanchez@cida.ve; hans@cida.ve; stock@cida.ve; adams@astro.indiana.edu; gebhard@astro.indiana.edu; honey@astro.indiana.edu; musser@astro.indiana.edu; arengsto@astro.indiana.edu; ferrin@ciens.ula.ve; franfuen@ciens.ula.ve; hernandj@ciens.ula.ve; naranjo@ciens.ula.ve; patricia@ciens.ula.ve; fhh@nofs.navy.mil; jgeary@cfa.harvard.edu RI Bongiovanni, Angel/J-6176-2012; OI Vivas, Kathy/0000-0003-4341-6172 NR 14 TC 32 Z9 33 U1 0 U2 3 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 JUL PY 2002 VL 114 IS 797 BP 780 EP 794 DI 10.1086/341705 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 566QZ UT WOS:000176440900010 ER PT J AU Roalson, EH Senters, AE Skog, LE Zimmer, EA AF Roalson, EH Senters, AE Skog, LE Zimmer, EA TI A morphological cladistic analysis of the neotropical flowering plant genus Gasteranthus (Gesneriaceae) SO SYSTEMATIC BOTANY LA English DT Article ID PHYLOGENETIC ANALYSIS; POLLINATION SYSTEMS; EVOLUTION; ECUADOR; CHARACTERS; CONFIDENCE; INFERENCE; SEQUENCES; NDHF AB Gasteranthus (Gesneriaceae; Beslerieae) includes 38 species restricted to the New World tropics. The genus has a limited distribution in Central and South America, with a center of diversity in western Ecuador. This study investigates cladistic relationships among species of Gasteranthus using floral and vegetative morphological data. Corolla shape in Gasteranthus ranges from funnelform to urceolate and ventricose, with additional variation in corolla spur and corolla ventral pouch morphology, Our analysis revealed that there were likely single primary, innovations of the three major corolla types, although only one of the three types forms a monophyletic group. Apparently, ventricose corollas were derived from funnelform corollas and urceolate corollas were derived from ventricose corollas, making the funnelform and ventricose corolla groups both paraphyletic. Spurs have been lost twice in Gasteranthus. Conspicuousness of stomatal clusters is quite homoplastic given the phylogenetic hypothesis. C1 Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. Smithsonian Inst, Natl Museum Nat Hist, Bot Unit, Dept Systemat Biol, Washington, DC 20560 USA. RP Roalson, EH (reprint author), Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. RI Zimmer, Elizabeth/G-3890-2011 NR 33 TC 5 Z9 6 U1 1 U2 4 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 2002 VL 27 IS 3 BP 573 EP 591 PG 19 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 594BR UT WOS:000178029300011 ER PT J AU Kim, HG Loockerman, DJ Jansen, RK AF Kim, HG Loockerman, DJ Jansen, RK TI Systematic implications of ndhF sequence variation in the Mutisieae (Asteraceae) SO SYSTEMATIC BOTANY LA English DT Article ID CHLOROPLAST DNA; PHYLOGENETIC IMPLICATIONS; SUNFLOWER FAMILY; EVOLUTION; TRIBE AB Mutisieae are considered one of the most important tribes for understanding the systematics and evolution of the Asteraceae because of their basal position within the family. The tribe is extremely diverse morphologically and biogeographically, consisting of 84 genera and 900 species. Despite extensive studies using macromorphological, palynological, and molecular approaches, tribal and subtribal delimitation and relationships of Mutisieae remain controversial. Phylogenetic analyses of DNA sequences of the chloroplast gene ndhF were performed using 53 species representing 31 genera of Mutisieae, 11 genera from the remaining five tribes of Cichorioideae, and five genera from the Asteroideae, The ndhF phylogeny of the Mutisieae provides insights into the circumscription anti relationship., of the tribe, subtribes, and taxonomic placement of several morphologically anomalous genera. The ndhF tree indicates, that Mutisicae are polyphyletic, The subtribes Gochnatiinae and Mutisiinae are not monophyletic, whereas the Nassauviinae are monophyletic, The majority of the South American genera and the Chinese genus Nouelia of the Gochnatiinae are positioned in a basal position in the Mutisieae. Furthermore, intergeneric relationships are resolved in several cases. C1 Smithsonian Museum Support Ctr, Lab Mol Systemat, Suitland, MD 20746 USA. Crime Lab Serv, Codis Sect, Austin, TX 78765 USA. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Univ Texas, Inst Mol & Cellular Biol, Austin, TX 78712 USA. RP Kim, HG (reprint author), Smithsonian Museum Support Ctr, Lab Mol Systemat, 4210 Silver Hill Rd, Suitland, MD 20746 USA. RI Jansen, Robert/F-6272-2011 NR 73 TC 32 Z9 40 U1 1 U2 2 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 2002 VL 27 IS 3 BP 598 EP 609 PG 12 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 594BR UT WOS:000178029300013 ER PT J AU Harvey, DJ Hall, JPW AF Harvey, DJ Hall, JPW TI Phylogenetic revision of the Charis cleonus complex (Lepidoptera : Riodinidae) SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID LIMITS AB A revision of the Charis cleonus group of Neotropical riodinid butterflies is presented, including discussions on the taxonomy, biogeography and biology of its species, and illustrations of the adults and male and female genitalia (where known) of all taxa. We recognize twenty-two species, including nineteen new species: C. ariquemes sp.n., C. brasilia sp.n., C. breves sp.n., C. cacaulandia sp.n., C. cuiaba sp.n., C. humaita sp.n., C. ipiranga sp.n., C. iquitos sp.n., C. ma sp.n., C. manicore sp.n., C. manu sp.n., C. matic sp.n., C. maues sp.n., C. negro sp.n., C. palcazu sp.n., C. rocana sp.n., C. santarem sp.n., C. tapajos sp.n and C. tefe sp.n. A cladistic analysis using thirty-six characters of male and female genitalia and external facies generated a single most parsimonious cladogram highlighting the existence of two clades, the major and cleonus subgroups. As each species largely occupies a parapatric range, this cladogram provides the opportunity to reassess historical relationships among areas of endemism in the Amazon basin. 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 43 TC 6 Z9 6 U1 0 U2 1 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 JUL PY 2002 VL 27 IS 3 BP 265 EP 300 DI 10.1046/j.1365-3113.2002.00173.x PG 36 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 568FN UT WOS:000176531900001 ER PT J AU Sallum, MAM Schultz, TR Foster, PG Aronstein, K Wirtz, RA Wilkerson, RC AF Sallum, MAM Schultz, TR Foster, PG Aronstein, K Wirtz, RA Wilkerson, RC TI Phylogeny of Anophelinae (Diptera : Culicidae) based on nuclear ribosomal and mitochondrial DNA sequences SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID D2 VARIABLE REGION; GENE-SEQUENCES; COMBINING DATA; ARTHROPOD PHYLOGENY; ANIMAL KINGDOM; RNA; CHARACTERS; SYSTEMATICS; EVOLUTION; 18S AB Phylogenetic relationships among thirty-two species of mosquitoes in subfamily Anophelinae are inferred from portions of the mitochondrial genes COI and COII, the nuclear 18S small subunit rRNA gene and the expansion D2 region of the nuclear large subunit 28S rRNA gene. Sequences were obtained from the genera Anopheles, Bironella and Chagasia . Representatives of all six subgenera of Anopheles were included: Anopheles, Cellia, Kerteszia, Lophopodomyia, Nyssorhynchus and Stethomyia. Using parsimony and maximum likelihood methods, various combinations of these DNA sequence data were analysed separately: 18S, 28S, combined 18S and 28S, combined COI and COII, and combined 18S, 28S, COI and COII ('total evidence'). The combined rDNA data contain strong phylogenetic signal, moderately to strongly supporting most clades in MP and ML analyses; however, the mtDNA data (analysed as either nucleotide or amino acid sequences) contain little phylogenetic signal, except for relationships of very recently derived groups of species and, at the deepest level, for the monophyly of Anophelinae. The paraphyly of Anopheles relative to Bironella is confirmed by most analyses and statistical tests. Support for the monophyly of subgenera Anopheles, Cellia , Kerteszia and Nyssorhynchus is indicated by most analyses. Subgenus Lophopodomyia is reconstructed as the sister to Bironella, nested within a clade also containing Nyssorhynchus and Kerteszia. The most basal relationships within genus Anopheles are not well resolved by any of the data partitions, although the results of statistical analyses of the rDNA data (S-H-tests, likelihood ratio tests for monophyly and Bayesian MCMC analyses) suggest that the clade consisting of Bironella, Lophopodomyia, Nyssorhynchus and Kerteszia is the sister to the clade containing Cellia and Anopheles. C1 Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, BR-01246904 Sao Paulo, Brazil. Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. Museum Nat Hist, Dept Zool, London, England. Smithsonian Inst, Dept Entomol, Walter Reed Army Inst Res, Washington, DC 20560 USA. Ctr Dis Control, Natl Ctr Infect Dis, Entomol Branch, Div Parasit Dis, Atlanta, GA 30333 USA. RP Sallum, MAM (reprint author), Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, Av Dr Arnaldo 715, BR-01246904 Sao Paulo, Brazil. RI Sallum, Maria/B-8537-2012 NR 63 TC 79 Z9 88 U1 1 U2 7 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 JUL PY 2002 VL 27 IS 3 BP 361 EP 382 DI 10.1046/j.1365-3113.2002.00182.x PG 22 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 568FN UT WOS:000176531900005 ER PT J AU Jehl, JR Johansson, C AF Jehl, JR Johansson, C TI Autumnal migration of Eared Grebes (Podiceps nigricollis) through southwestern Wyoming: A key to assessing the size of the North American population SO WESTERN NORTH AMERICAN NATURALIST LA English DT Article DE Eared Grebe; Podiceps nigricollis; Great Salt Lake; Mono Lake; migration; population; monitoring ID UTAH AB In autumn the vast majority of the North American population of Eared Grebes (Podiceps nigricollis) congregates for several months at Great Salt Lake, Utah, and Mono Lake, California. Because the lakes are so large, it has not been possible to monitor grebe migration with sufficient accuracy to determine when peak numbers are reached. To clarify migration phenology, we analyzed data from 2 isolated wetland areas in southwestern Wyoming where grebes land en route between breeding areas in the interior and Great Salt Lake. Occasional birds, probably non-breeders or failed breeders, begin moving southward as early as mid-June. Migration of postbreeding birds starts in late July, peaks in late August and September, and is largely completed by the end of October, with very small numbers arriving into,November. The pattern of migration and number of birds encountered varied annually, but 95% of the migration was usually completed by 15 October. As a result, censuses at the major staging lake made on or after 15 October but before the grebes depart for wintering areas can be used to study trends in size of the North American population. C1 Hubbs SeaWorld Res Inst, San Diego, CA 92109 USA. Fresno city coll, Dept Biol, Fresno, CA 93741 USA. RP Jehl, JR (reprint author), Smithsonian Inst, US Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. NR 13 TC 7 Z9 7 U1 0 U2 2 PU BRIGHAM YOUNG UNIV PI PROVO PA 290 LIFE SCIENCE MUSEUM, PROVO, UT 84602 USA SN 1527-0904 J9 WEST N AM NATURALIST JI West. North Am. Naturalist PD JUL PY 2002 VL 62 IS 3 BP 335 EP 340 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 584LN UT WOS:000177468200009 ER PT J AU Forrey, RC Kharchenko, V Dalgarno, A AF Forrey, RC Kharchenko, V Dalgarno, A TI On the statistical averaging procedure for the refractive index of matter waves SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID ATOMIC WAVES; GASES; POTENTIALS AB A discrepancy concerning the statistical averaging procedure is resolved for the refractive index of matter waves travelling in a dilute gas. C1 Penn State Univ, Berks Lehigh Valley Coll, Reading, PA 19610 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Forrey, RC (reprint author), Penn State Univ, Berks Lehigh Valley Coll, Reading, PA 19610 USA. NR 12 TC 7 Z9 7 U1 0 U2 2 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 JUN 28 PY 2002 VL 35 IS 12 BP L261 EP L264 AR PII S0953-4075(02)36223-0 DI 10.1088/0953-4075/35/12/103 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 576QL UT WOS:000177016200003 ER PT J AU Walton, WC MacKinnon, C Rodriguez, LF Proctor, C Ruiz, GA AF Walton, WC MacKinnon, C Rodriguez, LF Proctor, C Ruiz, GA TI Effect of an invasive crab upon a marine fishery: green crab, Carcinus maenas, predation upon a venerid clam, Katelysia scalarina, in Tasmania (Australia) SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE nonindigenous; predation; shellfish; Carcinus maenas; Katelysia scalarina AB Nonindigenous species are increasingly recognized as altering marine and estuarine communities, causing significant changes in abundance and distribution of native species. Such effects are of particular concern to coastal fisheries. We experimentally determined the effect of the nonindigenous European green crab, Carcinus maenas, upon the stepped venerid clam, Katelysia scalarina, the basis for a fledgling clam fishery in Tasmania, Australia. First, we observed a trend of decreased juvenile (< 13-mm shell length or SL) abundance of K. scalarina at sites with C maenas relative to those without this invasive predator. Additionally, relative predation intensity on these juveniles was significantly higher in invaded areas. To better understand the dynamics of predation by this invader, we conducted a number of manipulative experiments. In cage experiments testing per capita predation rates, we found that: (1) of the various sizes of C maenas, large C maenas were the most significant predators; (2) the smallest size class of K. scalarina tested (6-12-mm SL) was preferred by C. maenas; (3) C. maenas had much higher predation rates than any native predator tested, and (4) while the native shore crab, Paragrapsus gaimardii, was found to have a constant predation rate over an eightfold range of densities of juvenile K. scalarina (16 - 128 individuals.m(2)), C. maenas significantly increased its per capita predation with increasing prey density. Notably, in open Field plots at a site where C maenas was abundant, predation was constant over the range of tested prey densities. We predict, therefore, that the invasion of C maenas will have significant negative consequences for the Tasmanian K. scalarina fishery. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. CSIRO, Ctr Res Introduced Marine Pests, Hobart, Tas 7001, Australia. AC, Inst Biol Ecol & Conservat, Zapopan 45070, Jalisco, Mexico. Univ Calif Davis, Dept Environm Sci & Policy, Grad Grp Ecol, Davis, CA 95616 USA. RP Walton, WC (reprint author), Wellfleet Shellfish Dept, 300 Main St, Wellflect, MA 02667 USA. RI Proctor, Craig/I-3710-2016; OI Ruiz, Gregory/0000-0003-2499-441X NR 28 TC 65 Z9 72 U1 3 U2 54 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD JUN 24 PY 2002 VL 272 IS 2 BP 171 EP 189 AR PII S0022-0981(02)00127-2 DI 10.1016/S0022-0981(02)00127-2 PG 19 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 566GL UT WOS:000176418500005 ER PT J AU Botschwina, P Sanz, ME McCarthy, MC Thaddeus, P AF Botschwina, P Sanz, ME McCarthy, MC Thaddeus, P TI Ab initio theory and rotational spectra of linear carbon chains SiCnS SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; LABORATORY DETECTION; ASTRONOMICAL IDENTIFICATION; SILICON CARBIDES; WAVE-FUNCTIONS; IRC+10216; CHEMISTRY; SIS; SULFUR AB On the basis of extensive coupled cluster calculations, the rotational spectra of the linear silicon- and sulfur-containing carbon chains SiC2nS (n=1-3) in their singlet electronic ground state and SiC3S in its triplet electronic ground state have been detected and characterized by means of molecular beam Fourier transform microwave spectroscopy. Rotational and centrifugal distortion constants have been determined to high accuracy as well as the spin-spin coupling constant for triplet SiC3S. In addition, the Si-29, S-34, and both C-13 isotopic species of SiC2S have been detected, allowing the determination of both an effective r(0) structure, as well as a mixed experimental-theoretical structure resulting from the combination of the measured rotational constants with the vibration-rotation coupling constants calculated ab initio. Several rotational satellite lines have also been observed for SiC2S and, on the basis of their predicted vibration-rotation and l-type doubling constants, were assigned to the two highest-frequency stretching modes v(1) and v(2), and to a progression in the second lowest-frequency bending mode v(4) up to 3v(4). Equilibrium structures and various spectroscopic properties are predicted for all SiCnS species with n=1-8. (C) 2002 American Institute of Physics. C1 Univ Gottingen, Inst Phys Chem, D-37077 Gottingen, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Botschwina, P (reprint author), Univ Gottingen, Inst Phys Chem, Tammannstr 6, D-37077 Gottingen, Germany. EM pbotsch@gwdg.de RI Sanz, Maria Eugenia/F-7054-2013; OI McCarthy, Michael/0000-0001-9142-0008 NR 51 TC 16 Z9 16 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD JUN 22 PY 2002 VL 116 IS 24 BP 10719 EP 10729 DI 10.1063/1.1473807 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 560DF UT WOS:000176066200018 ER PT J AU Irwin, RP Maxwell, TA Howard, AD Craddock, RA Leverington, DW AF Irwin, RP Maxwell, TA Howard, AD Craddock, RA Leverington, DW TI A large paleolake basin at the head of Ma'adim Vallis, Mars SO SCIENCE LA English DT Article ID MARGARITIFER SINUS; CRATER; EVOLUTION; DRAINAGE; MODELS AB At 8 to 15 kilometers wide, Ma'adim Vallis is one of the largest valleys in the martian highlands. Although a groundwater source was previously suggested, the channel originates at a spillway in the divide of a similar to3,000,000-square-kilometer closed drainage basin. The interior morphology of this source basin, including likely shoreline features following topographic contours, suggests that Ma'adim Vallis was created through catastrophic overflow of a similar to1,100,000-square-kilometer highland lake. The size, constant levels, and interior morphology of three regional paleolake basins require a warmer paleoclimate and a long-term, recharged, stable highland water table more than similar to3.5 billion years ago. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. RP Irwin, RP (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RI Craddock, Robert/B-3884-2013; OI Howard, Alan/0000-0002-5423-1600 NR 27 TC 88 Z9 88 U1 2 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUN 21 PY 2002 VL 296 IS 5576 BP 2209 EP 2212 DI 10.1126/science.1071143 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 565PQ UT WOS:000176379000055 PM 12077414 ER PT J AU Rusin, D AF Rusin, D TI The expected properties of dark lenses SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; gravitational lensing; quasars general ID GRAVITATIONAL LENS; BINARY QUASAR; MATTER HALOS; GALAXIES; CANDIDATE; CLUSTERS; MODELS; CONSTRAINTS; STATISTICS; DISCOVERY AB We investigate the properties of multiple-image gravitational lens systems formed by dark matter halos. Both the Navarro-Frenk-White (NFW) and Moore et al. mass profiles are considered, and the effects of quadrupole perturbations to the lensing potential are taken into account. The systems produced by dark halos exhibit two generic properties that serve as powerful benchmarks for scrutinizing individual lens candidates: small flux ratios between the two brightest images in triples and detectable odd images. In contrast, most currently ambiguous quasar pairs consist of two components with flux ratios greater than or equal to3 : 1. Such systems are statistical outliers in the expected distribution of dark lenses and are therefore likely to be binary quasars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rusin, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. NR 60 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 JUN 20 PY 2002 VL 572 IS 2 BP 705 EP 712 DI 10.1086/340367 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 560FC UT WOS:000176071200002 ER PT J AU Alcalde, D Mediavilla, E Moreau, O Munoz, JA Libbrecht, C Goicoechea, LJ Surdej, J Puga, E De Rop, Y Barrena, R Gil-Merino, R McLeod, BA Motta, V Oscoz, A Serra-Ricart, M AF Alcalde, D Mediavilla, E Moreau, O Munoz, JA Libbrecht, C Goicoechea, LJ Surdej, J Puga, E De Rop, Y Barrena, R Gil-Merino, R McLeod, BA Motta, V Oscoz, A Serra-Ricart, M TI QSO 2237+0305 VR light curves from Gravitational Lenses International Time Project optical monitoring SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : photometry; gravitational lensing; quasars : individual (Q2237+0305) ID LENSING EXPERIMENT; Q2237+0305; TELESCOPE; SYSTEM AB We present VR observations of QSO 2237+ 0305 conducted by the Gravitational Lensing International Time Project collaboration from 1999 October 1 to 2000 February 3. The observations were made with the 2.56 m Nordic Optical Telescope at Roque de los Muchachos Observatory, La Palma ( Spain). The pointspread function ( PSF) fitting method and an adapted version of the ISIS subtraction method have been used to derive the VR light curves of the four components ( A D) of the quasar. The mean errors range in the intervals 0.01-0.04 mag ( PSF fitting) and 0.01-0.02 mag ( ISIS subtraction), with the faintest component ( D) having the largest uncertainties. We address the relatively good agreement between the A and D light curves derived using different filters, photometric techniques, and telescopes. The new VR light curves of component A extend the time coverage of a high-magnification microlensing peak, which was discovered by the OGLE team. C1 Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain. Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. Univ Lille 1, Lab Astron, Impasse Observ, F-59000 Lille, France. Univ Cantabria, Dept Fis Moderna, E-39005 Santander, Spain. Univ Potsdam, Inst Phys, Lehrstuhl Astrophys, D-14469 Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Fac Ciencias, Dept Astron, Montevideo 11400, Uruguay. RP Alcalde, D (reprint author), Inst Astrofis Canarias, C Via Lactea S-N, E-38205 San Cristobal la Laguna, Spain. NR 12 TC 31 Z9 32 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2002 VL 572 IS 2 BP 729 EP 734 DI 10.1086/340343 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 560FC UT WOS:000176071200004 ER PT J AU Furlanetto, SR Loeb, A AF Furlanetto, SR Loeb, A TI Emission of positron annihilation line radiation by clusters of galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; elementary particles; galaxies : clusters : general; galaxies : jets; X-rays : galaxies : clusters ID COSMIC-RAY ELECTRONS; SNR RX J1713.7-3946; BLACK-HOLE MASS; SHOCK ACCELERATION; COMA-CLUSTER; MAGNETIC-FIELDS; RADIO HALOS; CENTAURUS-A; SKY SURVEY; ENERGY AB Clusters of galaxies are enriched with positrons from jets of active galactic nuclei (AGNs) or from the interaction of cosmic rays with the intracluster gas. We follow the cooling of these positrons and show that their eventual annihilation with cluster electrons yields a narrow annihilation line. Unlike annihilation in the interstellar medium of galaxies, the line produced in clusters is not smeared by three-photon decay of positronium because positronium formation is suppressed at the high (greater than or similar to1 keV) temperature of the cluster electrons. We show that if AGN jets are composed of e(+)e(-) pairs, then the annihilation line from rich clusters within a distance of 100 Mpc might be detectable with future space missions, such as the International Gamma-Ray Astrophysical Laboratory or the Energetic X-Ray Imaging Survey Telescope. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 66 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 JUN 20 PY 2002 VL 572 IS 2 BP 796 EP 809 DI 10.1086/340384 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 560FC UT WOS:000176071200010 ER PT J AU Ghavamian, P Winkler, PF Raymond, JC Long, KS AF Ghavamian, P Winkler, PF Raymond, JC Long, KS TI The optical spectrum of the SN 1006 supernova remnant revisited SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (SN 1006); ISM : kinematics and dynamics; shock waves; supernova remnants ID LOCAL INTERSTELLAR-MEDIUM; FAST MODE SHOCKS; NONRADIATIVE SHOCKS; CROSS-SECTIONS; SN-1006; EMISSION; IONIZATION; COLLISIONLESS; WAVE; NOVA AB We present the deepest optical spectrum acquired to date of Balmer-dominated shocks in the northwest rim of SN 1006. We detect the broad and narrow components of Halpha, Hbeta, and Hgamma and report the first detection of the He I lambda6678 emission line in this supernova remnant. We may have detected, at the 1.5 sigma level, faint He II lambda4686 emission. We measure a full width at half-maximum of 2290 +/- 80 km s(-1) in the broad-component Halpha line, with broad-to-narrow flux ratios of 0.84(-0.01)(+0.03) and 0.93(-0.16)(+0.18) in Halpha and Hbeta, respectively. To match these observations, our nonradiative shock models require a low degree of electron-proton equilibration at the shock front, T-e/T-p less than or equal to 0.07, and a shock speed of 2890 +/- 100 km s(-1). These results agree well with an earlier analysis of ultraviolet lines from SN 1006. The He I/Halpha and He i /He II flux ratios also indicate low equilibration. Furthermore, our models match the observations for mostly ionized (similar to90%) preshock H and mostly neutral (greater than or similar to70%) preshock He, respectively. We conclude that the high H ionization fraction cannot be explained by either photoionization from the reverse shock or relic ionization from EUV photons released in the A.D. 1006 supernova. The most plausible explanation appears to be photoionization from the Galactic Lyman continuum. C1 Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Ghavamian, P (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. NR 40 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 JUN 20 PY 2002 VL 572 IS 2 BP 888 EP 896 DI 10.1086/340437 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 560FC UT WOS:000176071200016 ER PT J AU Pun, CSJ Michael, E Zhekov, SA McCray, R Garnavich, PM Challis, PM Kirshner, RP Baron, E Branch, D Chevalier, RA Filippenko, AV Fransson, C Leibundgut, B Lundqvist, P Panagia, N Phillips, MM Schmidt, B Sonneborn, G Suntzeff, NB Wang, LF Wheeler, JC AF Pun, CSJ Michael, E Zhekov, SA McCray, R Garnavich, PM Challis, PM Kirshner, RP Baron, E Branch, D Chevalier, RA Filippenko, AV Fransson, C Leibundgut, B Lundqvist, P Panagia, N Phillips, MM Schmidt, B Sonneborn, G Suntzeff, NB Wang, LF Wheeler, JC TI Modeling the Hubble Space Telescope ultraviolet and optical spectrum of spot 1 on the circumstellar ring of SN 1987A SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; supernova remnants; supernovae : individual (SN 1987A) ID LARGE-MAGELLANIC-CLOUD; RADIATIVE SHOCK-WAVES; VELOCITY LY-ALPHA; X-RAY; INTERSTELLAR EXTINCTION; SUPERNOVA REMNANT; NEUTRINO BURST; EMISSION-LINES; RADIO REMNANT; H-ALPHA AB We report and interpret Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph ( STIS) long-slit observations of the optical and ultraviolet ( 1150 10270 A) emission line spectra of the rapidly brightening spot 1 on the equatorial ring of SN 1987A between 1997 September and 1999 October ( days 3869 4606 after outburst). The emission is caused by radiative shocks created where the supernova blast wave strikes dense gas protruding inward from the equatorial ring. We measure and tabulate line identifications, fluxes, and, in some cases, line widths and shifts. We compute flux correction factors to account for substantial interstellar line absorption of several emission lines. Nebular analysis shows that optical emission lines come from a region of cool (T-e approximate to10(4) K) and dense (n(e) approximate to10(6) cm(-3)) gas in the compressed photoionized layer behind the radiative shock. The observed line widths indicate that only shocks with shock velocities V-s < 250 km s(-1) have become radiative, while line ratios indicate that much of the emission must have come from yet slower (V-s &LSIM; 135 km s(-1)) shocks. Such slow shocks can be present only if the protrusion has atomic density n &GSIM; 3 x 10(4) cm(-3), somewhat higher than that of the circumstellar ring. We are able to fit the UV fluxes with an idealized radiative shock model consisting of two shocks (V-s = 135 and 250 km s(-1)). The observed UV flux increase with time can be explained by the increase in shock surface areas as the blast wave overtakes more of the protrusion. The observed flux ratios of optical to highly ionized UV lines are greater by a factor of &SIM;2-3 than predictions from the radiative shock models, and we discuss the possible causes. We also present models for the observed Hα line widths and profiles, which suggest that a chaotic flow exists in the photoionized regions of these shocks. We discuss what can be learned with future observations of all the spots present on the equatorial ring. C1 Natl Opt Astron Observ, Tucson, AZ 85726 USA. NASA, Goddard Space Flight Ctr, Lab Astron & Space Phys, Greenbelt, MD 20771 USA. Univ Colorado, JILA, Boulder, CO 80309 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Stockholm Observ, SCFAB, Dept Astron, SE-10691 Stockholm, Sweden. European So Observ, D-85784 Garching, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Las Campanas Observ, Carnegie Inst Washington, La Serena, Chile. Mt Stromlo & Siding Spring Observ, Canberra, ACT 2611, Australia. Cerro Tololo Interamer Observ, La Serena, Chile. EO Lawrence Berkeley Natl Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Pun, CSJ (reprint author), Univ Hong Kong, Dept Phys, 518 Chong Yuet Ming Phys Bldg,Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. RI Baron, Edward/A-9041-2009; OI Baron, Edward/0000-0001-5393-1608; Schmidt, Brian/0000-0001-6589-1287; Schmidt, Brian/0000-0002-8538-9195 NR 81 TC 50 Z9 50 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 JUN 20 PY 2002 VL 572 IS 2 BP 906 EP 931 DI 10.1086/340453 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 560FC UT WOS:000176071200018 ER PT J AU Drake, JJ Marshall, HL Dreizler, S Freeman, PE Fruscione, A Juda, M Kashyap, V Nicastro, F Pease, DO Wargelin, BJ Werner, K AF Drake, JJ Marshall, HL Dreizler, S Freeman, PE Fruscione, A Juda, M Kashyap, V Nicastro, F Pease, DO Wargelin, BJ Werner, K TI Is RX J1856.5-3754 a quark star? SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (RX J1856.5-3754); stars : neutron; X-rays : stars ID ISOLATED NEUTRON-STAR; STRANGE STAR; COMPACT OBJECTS; MATTER; PULSARS AB Deep Chandra Low Energy Transmission Grating and High Resolution Camera spectroscopic observations of the isolated neutron star candidate RX J1856.5-3754 have been analyzed to search for metallic and resonance cyclotron spectral features and for pulsation behavior. As found from earlier observations, the X-ray spectrum is well represented by an similar to60 eV (7 x 10(5) K) blackbody. No unequivocal evidence of spectral line or edge features has been found, arguing against metal-dominated models. The data contain no evidence for pulsation, and we place a 99% confidence upper limit of 2.7% on the unaccelerated pulse fraction over a wide frequency range from 10(-4) to 100 Hz. We argue that the derived interstellar medium neutral hydrogen column density of 8 x 10(19) cm(-2) less than or equal to N-H less than or equal to 1.1 x 10(20) cm(-2) favors the larger distance from two recent Hubble Space Telescope parallax analyses, placing RX J1856.5-3754 at 140 pc instead of similar to60 pc and in the outskirts of the R CrA dark molecular cloud. That such a comparatively rare region of high interstellar matter (ISM) density is precisely where an isolated neutron star reheated by accretion of ISM would be expected is either entirely coincidental or current theoretical arguments excluding this scenario for RX J1856.5-3754 are premature. Taken at face value, the combined observational evidence-a lack of spectral and temporal features and an implied radius of R-infinity = 3.8-8.2 km that is too small for current neutron star models points to a more compact object, such as allowed for quark matter equations of state. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA. OI Juda, Michael/0000-0002-4375-9688; Nicastro, Fabrizio/0000-0002-6896-1364 NR 44 TC 171 Z9 174 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2002 VL 572 IS 2 BP 996 EP 1001 DI 10.1086/340368 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 560FC UT WOS:000176071200025 ER PT J AU Libarkin, JC Quade, J Chase, CG Poths, J McIntosh, W AF Libarkin, JC Quade, J Chase, CG Poths, J McIntosh, W TI Measurement of ancient cosmogenic Ne-21 in quartz from the 28 Ma Fish Canyon Tuff, Colorado SO CHEMICAL GEOLOGY LA English DT Article DE cosmogenic isotopes; neon; erosion; Colorado ID SURFACE EXPOSURE AGES; NUCLIDE PRODUCTION; PRODUCTION-RATES; DRY VALLEYS; EROSION; HE-3; NEON AB Measurement of Ne-21 in quartz from the 28 Ma buried Fish Canyon Tuff of Colorado yielded a maximum of 2.75 +/- 0.57 x 10(6) Ne-21 atoms (g SiO2)(-1) above nucleogenic and modem concentrations. This quantity represents cosmogenic Ne-21 produced on the Fish Canyon Tuff surface prior to the deposition of the overlying Carpenter Ridge Tuff. Ancient Ne-21 was isolated through the analysis and identification of (1) background Ne-21 produced from alpha-particle interactions or inherited; and (2) cosmogenic Ne-21 produced from modem radiation. Multiple samples of Fish Canyon Tuff shielded during both exposure periods, 28 Ma ago and in modem time, yielded the background that was then subtracted from all samples. Likewise, samples of Fish Canyon exposed today, but well below the Fish Canyon-Carpenter Ridge contact and therefore shielded 28 Ma ago, yielded a modem component that was also removed from all sample concentrations. The presence of an ancient cosmogenic isotope in a buried surface has several potential applications, including the quantification of paleoelevation, paleolatitude, and pre-Quaternary erosion rates. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA. Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. New Mexico Inst Min & Technol, NM Bur Mines, NM Geochronol Res Lab, Socorro, NM 87801 USA. RP Libarkin, JC (reprint author), Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, 60 Garden St,MS-71, Cambridge, MA 02138 USA. RI Libarkin, Julie/H-2316-2011 NR 32 TC 15 Z9 16 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 J9 CHEM GEOL JI Chem. Geol. PD JUN 15 PY 2002 VL 186 IS 3-4 BP 199 EP 213 AR PII S0009-2541(01)00411-9 DI 10.1016/S0009-2541(01)00411-9 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 573PN UT WOS:000176840200002 ER PT J AU Siebert, L Carrasco-Nunez, G AF Siebert, L Carrasco-Nunez, G TI Late-Pleistocene to precolumbian behind-the-arc mafic volcanism in the eastern Mexican Volcanic Belt; implications for future hazards SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Mexican Volcanic Belt; Cofre de Perote volcano; lava flows; volcanic risk; alkali basalts; calc-alkaline composition ID PICO-DE-ORIZABA; PLUME-RELATED MAGMATISM; CALC-ALKALIC VOLCANISM; ISLAND BASALT TYPE; CITLALTEPETL VOLCANO; ACTIVE MARGIN; CINDER CONES; COSTA-RICA; FLOW-FIELD; ROCKS AB An area of widespread alkaline-to-subalkaline volcanism lies at the northern end of the Cofre de Perote-Citlaltepetl (Pico de Orizaba) volcanic chain in the eastern Mexican Volcanic Belt (MVB). Two principal areas were active. About a dozen latest-Pleistocene to precolumbian vents form the 11-km-wide, E-W-trending Cofre de Perote vent cluster (CPVC) at 2300-2800 in elevation on the flank of the largely Pleistocene Cofre de Perote shield volcano and produced an extensive lava field that covers > 100 km(2). More widely dispersed vents form the Naolinco volcanic field (NVF) in the Sierra de Chiconquiaco north of the city of Jalapa (Xalapa). Three generations of flows are delineated by cone and lava-flow morphology, degree of vegetation and cultivation, and radiocarbon dating. The flows lie in the behind-the-are portion of the northeastern part of the MVB and show major- and trace-element chemical patterns transitional between intraplate and subduction zone environments. Flows of the oldest group originated from La Joya cinder cone (radiocarbon ages similar to 42 000 yr BP) at the eastern end of the CPVC. This cone fed an olivine-basaltic flow field of similar to 20 km(2) that extends about 14 km southeast to underlie the heavily populated northern outskirts of Jalapa, the capital city of the state of Veracruz. The Central Cone Group (CCG), of intermediate age, consists of four morphologically youthful cinder cones and associated vents that were the source of a lava field > 27 km(2) of late-Pleistocene or Holocene age. The youngest group includes the westernmost flow, from Cerro Colorado, and a lava flow similar to 2980 BP from the Rincon de Chapultepec scoria cone of the NVF. The latest eruption, from the compound El Volcancillo scoria cone, occurred about 870 radiocarbon years ago and produced two chemically and rheologically diverse lava flows that are among the youngest precolumbian flows in Mexico and resemble paired aa-pahoehoe flows from Mauna Loa volcano. The El Volcancillo eruption initially produced the high effusion rate, short-duration Toxtlacuaya alkaline aa lava flow from the southeastern crater. This 12-km-long hawaiite (average 50.5% SiO2) flow Was followed by extrusion of the cale-alkaline Rio Naolinco lava flow from the northwestern crater. This large-volume (similar to 1.3 km(3)) tube-fed basaltic pahoehoe flow (average SiO2 49%) traveled 50 kin. Inferred effusion rates suggest emplacement over a decade-long period. Flows of all three age groups are transected by Highway 140 and the railway that form major transportation arteries between Jalapa and Puebla. This area has not previously been considered to be at volcanic risk, but volcanism here has continued into precolumbian time. Future eruptions of similar magnitude and location to those documented here could pose significant hazards to transportation corridors and to densely populated areas in and to the north of Jalapa. Slight variations in vent locations could produce future flows down one or more of more than a half dozen drainages with widely varying population densities. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Smithsonian Inst, Global Volcanism Program, Washington, DC 20560 USA. Univ Nacl Autonoma Mexico, Unidad Invest Ciencias Tierra, Mexico City 04510, DF, Mexico. RP Siebert, L (reprint author), Smithsonian Inst, Global Volcanism Program, Washington, DC 20560 USA. NR 58 TC 39 Z9 39 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD JUN 15 PY 2002 VL 115 IS 1-2 BP 179 EP 205 AR PII S0377-0273(01)00316-X DI 10.1016/S0377-0273(01)00316-X PG 27 WC Geosciences, Multidisciplinary SC Geology GA 569NJ UT WOS:000176608200010 ER PT J AU Schroll, S AF Schroll, S TI Barnett Newman. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Schroll, S (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 JUN 15 PY 2002 VL 127 IS 11 BP 61 EP 61 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 564QW UT WOS:000176325900028 ER PT J AU Roubik, DW AF Roubik, DW TI Tropical agriculture - The value of bees to the coffee harvest SO NATURE LA English DT Article C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Roubik, DW (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 5 TC 82 Z9 86 U1 1 U2 39 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 13 PY 2002 VL 417 IS 6890 BP 708 EP 708 DI 10.1038/417708a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 561QY UT WOS:000176154700035 PM 12066176 ER PT J AU Buzas, MA Collins, LS Culver, SJ AF Buzas, MA Collins, LS Culver, SJ TI Latitudinal difference in biodiversity caused by higher tropical rate of increase SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID SPECIES RICHNESS; EXTINCTION; DIVERSITY; PATTERNS; MOLLUSKS AB Tropical diversity has generally exceeded temperate diversity in the present and at points in the past, but whether measured differences have remained relatively constant through time has been unknown. Here we examine tropical vs. temperate diversities from the Neogene to Recent using the within-habitat diversity measure Fisher's alpha of Cenozoic benthic foraminifera from the temperate Central Atlantic Coastal Plain and the tropical Central American Isthmus. During the Neogene, the mean value of alpha at temperate latitudes increased 1.4 times or 40%, whereas in the tropics it increased 2.1 times or 106%. Thus, while both areas exhibit an increase of diversity with time, past differences in the rate of increase have generated a more pronounced gradient today (164%) than existed in the Miocene (80%). These data disagree with the suggestion that the world reached an equilibrium number of species during the Paleozoic and demonstrate the need to consider both temperate and tropical components in global diversity assessments. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Florida Int Univ, Dept Earth Sci, Miami, FL 33199 USA. Florida Int Univ, Dept Sci Biol, Miami, FL 33199 USA. E Carolina Univ, Dept Geol, Greenville, NC 27858 USA. RP Buzas, MA (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. NR 30 TC 54 Z9 56 U1 0 U2 7 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 JUN 11 PY 2002 VL 99 IS 12 BP 7841 EP 7843 DI 10.1073/pnas.122241499 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 562UQ UT WOS:000176217700009 PM 12060730 ER PT J AU Graves, GR Romanek, CS Navarro, AR AF Graves, GR Romanek, CS Navarro, AR TI Stable isotope signature of philopatry and dispersal in a migratory songbird SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID THROATED BLUE WARBLERS; TROPHIC RELATIONSHIPS; DENDROICA-CAERULESCENS; MONARCH BUTTERFLIES; WINTERING GROUNDS; BREEDING ORIGINS; N-15 ABUNDANCE; NATAL ORIGINS; FOOD WEBS; CARBON AB Stable isotope analysis is widely promoted as a practical method for tracing the geographic origins of migratory birds. However, the extent to which geospatial patterns of isotope ratios in avian tissues are influenced by age-specific, altitudinal, and temporal factors remains largely unexplored. We measured carbon (C-13/C-12) and nitrogen (N-15/N-14) isotope ratios in feathers of black-throated blue warblers (Dendroica caerulescens) breeding along a relatively steep altitudinal gradient in the Appalachian Mountains to evaluate the effects of altitude and year on the isotopic signatures of yearling (first breeding season) and older males (>2 years). Breeding males (n = 302) collected during 7 consecutive years exhibited significant age-specific and altitudinal effects in delta(13)C values and age-specific and temporal effects in delta(15)N values. The delta(13)C values of older males increased with altitude at the rate of approximate to1.3%(o) per 1,000 m, suggesting a high degree of year-to-year philopatry to narrow altitudinal zones, if not to breeding territories. In contrast, absence of altitudinal patterns in yearlings most likely reflects natal dispersal. Carbon isotope variation (delta(13)C = -26.07 to -20.86%.) observed along a single altitudinal transect (755 m) nearly brackets the range of delta(13)C values recorded in feathers across the North American breeding range of the warbler from Georgia to New Brunswick (110 of latitude) and from New Brunswick to Michigan (22degrees of longitude). These data indicate that age-specific and altitudinal effects must be considered when using delta(13)C values to delineate the geographic origin of avian species with large altitudinal and latitudinal ranges. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Univ Georgia, Dept Geol, Athens, GA 30602 USA. Savannah River Ecol Lab, Aiken, SC 29802 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, MRC-116, Washington, DC 20560 USA. NR 70 TC 48 Z9 50 U1 10 U2 30 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUN 11 PY 2002 VL 99 IS 12 BP 8096 EP 8100 DI 10.1073/pnas.082240899 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 562UQ UT WOS:000176217700054 PM 12034868 ER PT J AU Dalal, N Kochanek, CS AF Dalal, N Kochanek, CS TI Direct detection of cold dark matter substructure SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; dark matter; galaxies : formation; gravitational lensing; large-scale structure of universe ID 4-IMAGE GRAVITATIONAL LENS; DENSITY PROFILES; GALAXIES; EVOLUTION; MODELS AB We devise a method to measure the abundance of satellite halos in gravitational lens galaxies and apply our method to a sample of seven lens systems. After using Monte Carlo simulations to verify the method, we find that substructure comprises f(sat) = 0.02 (median, 0.006 < f(sat) < 0.07 at 90% confidence) of the mass of typical lens galaxies, in excellent agreement with predictions of cold dark matter (CDM) simulations. We estimate a characteristic critical radius for the satellites of 0."0001 < b < 0."006 (90% confidence). For a dn/dM proportional to M-1.8 (M-low < M < M-high) satellite mass function, the critical radius provides an estimate for the upper mass limit of 10(6) M-. less than or similar to M-high less than or similar to 10(9) M-.. Our measurement confirms a generic prediction of CDM models and may obviate the need to invoke alternatives to CDM such as warm dark matter or self-interacting dark matter. C1 Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dalal, N (reprint author), Univ Calif San Diego, Dept Phys, Code 0350,9500 Gilman Dr, La Jolla, CA 92093 USA. NR 42 TC 314 Z9 317 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2002 VL 572 IS 1 BP 25 EP 33 DI 10.1086/340303 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100003 ER PT J AU Caselli, P Benson, PJ Myers, PC Tafalla, M AF Caselli, P Benson, PJ Myers, PC Tafalla, M TI Dense cores in dark clouds. XIV. N2H+ (1-0) maps of dense cloud cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : molecules; ISM : structure; molecular data; radio lines : ISM ID PRE-PROTOSTELLAR CORES; SMALL-SCALE STRUCTURE; MASS STAR-FORMATION; MOLECULAR CLOUDS; AMBIPOLAR DIFFUSION; NH3 OBSERVATIONS; INTERNAL STRUCTURE; INITIAL CONDITIONS; MAGNETIC BRAKING; PRESTELLAR CORES AB We present results of an extensive mapping survey of N2H+ (1-0) in about 60 low-mass cloud cores already mapped in the NH3 ( 1, 1) inversion transition line. The survey has been carried out at the FCRAO antenna with an angular resolution of 54", about 1.5 times finer than the previous ammonia observations made at the Haystack telescope. The comparison between N2H+ and NH3 maps shows strong similarities in the size and morphology of the two molecular species, indicating that they are tracing the same material, especially in starless cores. Cores with stars typically have map sizes about a factor of 2 smaller for N2H+ than for NH3, indicating the presence of denser and more centrally concentrated gas compared to starless cores. The mean aspect ratio is similar to2. Significant correlations are found between NH3 and N2H+ column densities and excitation temperatures in starless cores, but not in cores with stars, suggesting a different chemical evolution of the two species. Starless cores are less massive ( M vir hi 3 M) than cores with stars ( M vir hi 9 M). Velocity gradients range between 0.5 and 6 km s(-1) pc(-1), similar to what has been found with NH3 data, and the ratio beta of rotational kinetic energy to gravitational energy has magnitudes between similar to10(-4) and 0.07, indicating that rotation is not energetically dominant in the support of the cores. Local velocity gradients show significant variation in both magnitude and direction, suggesting the presence of complex motions not interpretable as simple solid-body rotation. Integrated intensity profiles of starless cores present a central flattening and are consistent with a spherically symmetric density law n proportional to r(-alpha), where alpha = 1.2 for r < r(break) and alpha = 2 for r > r(break), with r(break) similar to0.03 pc. Cores with stars are better modeled with single density power laws with alpha greater than or equal to2, in agreement with observations of submillimeter continuum emission. Line widths change across the core, but we did not find a general trend: there are cores with significant positive as well as negative linear correlations between D v and the impact parameter b. The deviation in line width correlates with the mean line width, suggesting that the line of sight contains 10 coherence lengths. The corresponding value of the coherence length, similar to0.01 pc, is similar to the expected cutoff wavelength for MHD waves. This similarity may account for the increased coherence of line widths on small scales. Despite finer angular resolution, the majority of N2H+ and NH3 maps show a similar simple structure, with single peaks and no elongation. C1 Osserv Astrofis Arcetri, I-50125 Florence, Italy. Wellesley Coll, Whitin Observ, Wellesley, MA 02181 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Astron Nacl IGN, E-28014 Madrid, Spain. RP Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy. NR 72 TC 323 Z9 327 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 JUN 10 PY 2002 VL 572 IS 1 BP 238 EP 263 DI 10.1086/340195 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100022 ER PT J AU Fransson, C Chevalier, RA Filippenko, AV Leibundgut, B Barth, AJ Fesen, RA Kirshner, RP Leonard, DC Li, WD Lundqvist, P Sollerman, J Van Dyk, SD AF Fransson, C Chevalier, RA Filippenko, AV Leibundgut, B Barth, AJ Fesen, RA Kirshner, RP Leonard, DC Li, WD Lundqvist, P Sollerman, J Van Dyk, SD TI Optical and ultraviolet spectroscopy of SN1995N: Evidence for strong circumstellar interaction SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars : mass loss; supernovae : individual (SN 1995N) ID ACTIVE GALACTIC NUCLEI; VY-CANIS-MAJORIS; GAMMA-RAY BURST; 25 APRIL 1998; SUPERNOVA 1988Z; RADIO-EMISSION; II SUPERNOVAE; FE-VII; YOUNG SUPERNOVA; COOL HYPERGIANT AB Optical and ultraviolet observations of the Type IIn supernova SN 1995N at epochs between 321 and 1799 days after the explosion show three distinct velocity components. The narrow lines come from circumstellar gas and show both low and high ionization. This component has a low filling factor and is photoionized by X-rays from the shock. The intermediate component, which is dominated by newly processed oxygen, originates in a shell with velocity of 2500-5000 km s(-1) and most likely comes from the ejecta. The hydrogen- and helium-dominated gas has a low ionization, a high density, and velocities that extend out to e 10,000 km s(-1). Strong signatures of Lyalpha-pumped fluorescence lines of Fe II are seen in the near-infrared and ultraviolet. The He/H ratio, similar to0.3 by number, and the nitrogen overabundance provide strong evidence for CNO-burning products. The fluxes of the broad hydrogen and helium lines decrease considerably faster than the oxygen lines. The Halpha line pro le shows strong evolution, with the red wing decreasing faster than the blue. Possible scenarios, involving either a clumpy circumstellar medium or an aspherical distribution of the surrounding gas, are discussed based on the line profiles and physical conditions. Finally, we propose that Type IIn supernovae have their origin in red supergiants in a superwind phase. C1 Stockholm Observ, SE-13336 Saltsjobaden, Sweden. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. European So Observ, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Fransson, C (reprint author), Stockholm Observ, SE-13336 Saltsjobaden, Sweden. OI Sollerman, Jesper/0000-0003-1546-6615; Barth, Aaron/0000-0002-3026-0562; Van Dyk, Schuyler/0000-0001-9038-9950 NR 81 TC 88 Z9 88 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2002 VL 572 IS 1 BP 350 EP 370 DI 10.1086/340295 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100030 ER PT J AU Chatterjee, P Hernquist, L Loeb, A AF Chatterjee, P Hernquist, L Loeb, A TI Dynamics of a massive black hole at the center of a dense stellar system SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; celestial mechanics; galaxies : kinematics and dynamics; methods : n-body simulations; stellar dynamics ID SAGITTARIUS A-ASTERISK; GALACTIC NUCLEI; SPHERICAL SYSTEMS; PROPER-MOTION; FRICTION; GALAXIES; STARS; MODES AB We develop a simple physical model to describe the dynamics of a massive pointlike object, such as a black hole, near the center of a dense stellar system. It is shown that the total force on this body can be separated into two independent parts, one of which is the slowly varying influence of the aggregate stellar system, and the other being the rapidly fluctuating stochastic force due to discrete encounters with individual stars. For the particular example of a stellar system distributed according to a Plummer model, it is shown that the motion of the black hole is then similar to that of a Brownian particle in a harmonic potential, and we analyze its dynamics using an approach akin to Langevin's solution of the Brownian motion problem. The equations are solved to obtain the average values, time autocorrelation functions, and probability distributions of the black hole's position and velocity. By comparing these results with N-body simulations, we demonstrate that this model provides a very good statistical description of the actual black hole dynamics. As an application of our model, we use our results to derive a lower limit on the mass of the black hole Sgr A* in the Galactic center. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pchatterjee@cfa.harvard.edu; lars@cfa.harvard.edu; aloeb@cfa.harvard.edu NR 37 TC 51 Z9 51 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 JUN 10 PY 2002 VL 572 IS 1 BP 371 EP 381 DI 10.1086/340224 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100031 ER PT J AU Belczynski, K Kalogera, V Bulik, T AF Belczynski, K Kalogera, V Bulik, T TI A comprehensive study of binary compact objects as gravitational wave sources: Evolutionary channels, rates, and physical properties SO ASTROPHYSICAL JOURNAL LA English DT Review DE binaries : close; black hole physics; gravitational waves; stars : evolution; stars : neutron ID COMMON ENVELOPE EVOLUTION; NEUTRON-STAR ACCRETION; GAMMA-RAY BURSTS; BLACK-HOLE FORMATION; LOW-MASS STARS; PRESUPERNOVA EVOLUTION; STELLAR EVOLUTION; RADIO PULSARS; GALACTIC DISK; EVENT RATES AB A new generation of ground-based interferometric detectors for gravitational waves is currently under construction or has entered the commissioning phase ( Laser Interferometer Gravitational-wave Observatory [LIGO], VIRGO, GEO600, TAMA300). The purpose of these detectors is to observe gravitational waves from astrophysical sources and help improve our understanding of the source origin and physical properties. In this paper we study the most promising candidate sources for these detectors: inspiraling double compact objects. We use population synthesis methods to calculate the properties and coalescence rates of compact object binaries: double neutron stars, black hole neutron star systems, and double black holes. We also examine the formation channels available to double compact object binaries. We explicitly account for the evolution of low-mass helium stars and investigate the possibility of common-envelope evolution involving helium stars as well as two evolved stars. As a result we identify a significant number of new formation channels for double neutron stars, in particular, leading to populations with very distinct properties. We discuss the theoretical and observational implications of such populations, but we also note the need for hydrodynamical calculations to settle the question of whether such common-envelope evolution is possible. We also present and discuss the physical properties of compact object binaries and identify a number of robust, qualitative features as well as their origin. Using the calculated coalescence rates we compare our results to earlier studies and derive expected detection rates for LIGO. We find that our most optimistic estimate for the first LIGO detectors reach a couple of events per year and our most pessimistic estimate for advanced LIGO detectors exceed similar or equal to10 events per year. C1 Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Belczynski, K (reprint author), Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. NR 116 TC 372 Z9 373 U1 7 U2 16 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2002 VL 572 IS 1 BP 407 EP 431 DI 10.1086/340304 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100034 ER PT J AU Ransom, RR Bartel, N Bietenholz, MF Lebach, DE Ratner, MI Shapiro, II AF Ransom, RR Bartel, N Bietenholz, MF Lebach, DE Ratner, MI Shapiro, II TI Possible corotation of the milliarcsecond radio structure of the close binary HR 1099 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; radio continuum : stars; stars : activity; stars : imaging; stars : individual (V711 Tauri); techniques : interferometric ID RS-CANUM-VENATICORUM; CVN SYSTEM HR-1099; UX ARIETIS; VLBI OBSERVATIONS; MAIN-SEQUENCE; FLUX-DENSITY; EMISSION; STARS; ALGOL; POLARIZATION AB We present the first VLBI images of the RS CVn binary star HR 1099 ( = V711 Tauri, HD 22468) obtained from observations at 8.4 GHz in 1996 May and September made in support of the NASA/Stanford Gravity Probe B project. The first set of observations was made during a decay stage of a are event. The second set of observations was made during a quiescent period. The detected emission region for the active epoch had an estimated major-axis length ( FWHM) of 2.7 +/- 0.2 mas. This region consisted of a halo and two superimposed compact condensations that were oriented approximately east-west. The centers of the compact condensations were separated by 1.7 +/- 0.1 mas. Compared to the similar to1.3 mas separation on the sky at this epoch of the centers of the stellar components of the binary, the observed separation of the condensations differs by only 0.4 mas, which is less than the similar to0.6 mas angular radius of the larger component. During the observations, the compact western condensation rotated north-northwestward by 24degrees +/- 4degrees, or by 0.7 +/- 0.1 mas, relative to the eastern condensation. We speculate that ( 1) either both condensations originate from the corona of the larger stellar component or one condensation is close to the surface of each of the two stellar components of the binary and (2) the relative rotation of the two condensations is a consequence of the rotation of the binary system. We speculate further that the halo is a consequence of flare-energized electrons conned by the magnetosphere of the larger stellar component or by the combined magnetospheres of the two stellar components. Our quiescent epoch, in contrast, was characterized by a single emission region with a major axis estimated to be 1.7 +/- 0.1 mas ( FWHM). C1 York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, DEMIRM, F-75014 Paris, France. RP Ransom, RR (reprint author), York Univ, Dept Phys & Astron, 4700 Keele St, N York, ON M3J 1P3, Canada. NR 51 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 JUN 10 PY 2002 VL 572 IS 1 BP 487 EP 502 DI 10.1086/340300 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100040 ER PT J AU Fontenla, JM Avrett, EH Loeser, R AF Fontenla, JM Avrett, EH Loeser, R TI Energy balance in the solar transition region. IV. Hydrogen and helium mass flows with diffusion SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffusion; hydrodynamics; line : formation; radiative transfer; Sun : transition region ID CORONAL LOOPS; QUIET SUN; MODELS; CHROMOSPHERE; IONIZATION; ATMOSPHERE; EMISSION; LINE; HE AB In this paper we extend our previous modeling of energy balance in the chromosphere-corona transition region to cases with particle and mass flows. The cases considered here are quasi-steady and satisfy the momentum and energy balance equations in the transition region. We assume one-dimensional geometry and include the flow velocity terms in all equations, but we neglect the partial derivatives with respect to time. We present a complete and physically consistent formulation and method for solving the non-LTE and energy balance equations in these situations, including both particle diffusion and flows of Hand He. Our calculations include partial frequency redistribution in the Lyalpha and Lybeta lines. Our results show quantitatively how mass flows affect the ionization and radiative losses of H and He, thereby affecting the structure and extent of the transition region. Furthermore, our computations show that the H and He line profiles are greatly affected by flows. We find that line shifts are much less important than the changes in line intensity and central reversal as a result of the influence of flows on the excitation and ionization. In this paper we use fixed conditions at the base of the transition region and in the underlying chromosphere. Our intent is to show the physical effects of flows on the transition region, not to match any particular observations. However, our computed Lyalpha profiles can account for the range of observed high spectral and spatial resolution from the quiet Sun. We suggest that dedicated modeling of specific sequences of observations based on physically consistent methods like those presented here will substantially improve our understanding of the energy balance in the chromosphere and corona. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP 1874 MacCullen Dr, Erie, CO 80516 USA. EM jfonten750@earthlink.net; eavrett@cfa.harvard.edu; rloeser@cfa.harvard.edu NR 37 TC 55 Z9 56 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 JUN 10 PY 2002 VL 572 IS 1 BP 636 EP 662 DI 10.1086/340227 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100051 ER PT J AU Field, GB Blackman, EG AF Field, GB Blackman, EG TI Dynamical quenching of the alpha(2) dynamo SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : magnetic fields; ISM : magnetic fields; methods : numerical; MHD; stars : magnetic fields; turbulence ID MEAN-FIELD ELECTRODYNAMICS; TURBULENT DYNAMOS; MAGNETIC HELICITY AB We present a two-scale approximation for the dynamics of a nonlinear alpha(2) dynamo. Solutions of the resulting nonlinear equations agree with the numerical simulations of Brandenburg and show that alpha is quenched by the buildup of magnetic helicity at the forcing scale 1/k(2) as the alpha effect transfers it from the large scale 1/k(1)(>1/k(2)). For times t>(k(1)/k(2))Re-M,Re-2 in eddy turnover units (where Re-M,Re-2 is the magnetic Reynolds number of the forcing scale), alpha is limited resistively in the form predicted for the steady state case. However, for tmuch less thanRe(M,2), alpha takes on its kinematic value independent of Re-M,Re-2, allowing the production of large-scale magnetic energy equal to k(1)/k(2) times equipartition. Thus, the dynamic theory of predicts substantial fast growth of a large-scale field despite being slow at large times. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Rochester, Laser Energet Lab, Rochester, NY 14627 USA. RP Field, GB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 23 TC 84 Z9 84 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2002 VL 572 IS 1 BP 685 EP 692 DI 10.1086/340233 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100055 ER PT J AU Reid, MJ Goldston, JE AF Reid, MJ Goldston, JE TI How Mira variables change visual light by a thousandfold (vol 568, pg 931, 2002) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2002 VL 572 IS 1 BP 694 EP 694 DI 10.1086/341093 PN 1 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BQ UT WOS:000176005100057 ER PT J AU Soria, R Kong, AKH AF Soria, R Kong, AKH TI XMM-Newton observations of the spiral galaxy M74 (NGC 628) SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : individual (M74, NGC 628); galaxies : spiral; supernovae : individual (SN 2002ap); X-rays : binaries; X-rays : galaxies ID X-RAY SOURCES; HIGH-RESOLUTION CAMERA; MASS BLACK-HOLE; SURFACE PHOTOMETRY; STARBURST GALAXY; ENERGY-SPECTRA; M81 X-9; H I; CHANDRA; DISCOVERY AB The face-on spiral galaxy M74 (NGC 628) was observed by XMM-Newton on 2002 February 2. In total, 21 sources are found in the inner 5' from the nucleus (after rejection of a few sources associated to foreground stars). Hardness ratios suggest that about half of them belong to the galaxy. The higher luminosity end of the luminosity function is fitted by a power law of slope -0.8. This can be interpreted as evidence of ongoing star formation, in analogy with the distributions found in disks of other late-type galaxies. A comparison with previous Chandra observations reveals a new ultraluminous X-ray transient (L(x) approximate to 1.5 x 10(39) ergs s(-1) in the 0.3-8 keV band) about 4' north of the nucleus. We find another bright transient source (L(x) approximate to 5 x 10(38) ergs s(-1)) about 5' northwest of the nucleus. The UV and X-ray counterparts of SN 2002ap are also found in this XMM-Newton observation; the hardness ratio of the X-ray counterpart suggests that the emission comes from the shocked circumstellar matter. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Soria, R (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM rs1@mssl.ucl.ac.uk; akong@cfa.harvard.edu NR 39 TC 25 Z9 25 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2002 VL 572 IS 1 BP L33 EP L37 DI 10.1086/341445 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559BW UT WOS:000176005600008 ER PT J AU Paxinos, EE James, HF Olson, SL Ballou, JD Leonard, JA Fleischer, RC AF Paxinos, EE James, HF Olson, SL Ballou, JD Leonard, JA Fleischer, RC TI Prehistoric decline of genetic diversity in the nene SO SCIENCE LA English DT Article ID POPULATIONS C1 Smithsonian Inst, Conservat & Res Ctr, Washington, DC 20008 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Univ Calif Los Angeles, Dept Ecol Evolut & Organismal Biol, Los Angeles, CA 90095 USA. RP Fleischer, RC (reprint author), Smithsonian Inst, Conservat & Res Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Leonard, Jennifer/A-7894-2010 OI Leonard, Jennifer/0000-0003-0291-7819 NR 7 TC 48 Z9 49 U1 1 U2 20 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 JUN 7 PY 2002 VL 296 IS 5574 BP 1827 EP 1827 DI 10.1126/science.296.5574.1827 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 559YP UT WOS:000176054300035 PM 12052947 ER PT J AU Remo, JL AF Remo, JL TI Characterizing the near-Earth object hazard and its mitigation SO ACTA ASTRONAUTICA LA English DT Article ID MOMENTUM; ORBITS AB Within observational constraints and analytic orbit determinations, potential NEO hazards and mitigations are characterized in terms of orbit displacements to establish (arbitrary) "safe" closest approach distances and corresponding energies that must be externally applied to achieve appropriate orbit displacements from the Earth. Required orbital velocity changes depend on projected closest Earth approach distances and time to (near) impact. Energy to achieve orbital displacement depends on NEO mass, required orbital velocity change, and the energy-momentum coupling coefficient. Errors in these parameters introduce uncertainties into hazard index and mitigation procedures. Hazard avoidance levels and mitigation indices for nine near-Earth asteroids, including 1997 XF11 and 1999 AN(10), with non-zero Earth-impact probabilities are computed as examples of the proposed methodology, generating insight into the dilemma of predicting near impacts. This zeroth order approximation should not be construed as solving an orbital mechanics problem, nor establishing a particular set of criteria for mitigation action, but rather as a "survival index". (C) 2002 Published by Elsevier Science Ltd. C1 Harvard Smithsonian Ctr Astrophys, Planetary Sci Div, Cambridge, MA 02138 USA. RP Remo, JL (reprint author), Harvard Smithsonian Ctr Astrophys, Planetary Sci Div, Mail Stop 18,60 Garden St, Cambridge, MA 02138 USA. NR 22 TC 5 Z9 5 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN PY 2002 VL 50 IS 12 BP 737 EP 746 AR PII S0094-5765(02)00017-6 DI 10.1016/S0094-5765(02)00017-6 PG 10 WC Engineering, Aerospace SC Engineering GA 569QQ UT WOS:000176613900003 ER PT J AU Krebs, E AF Krebs, E TI High noon in the rain forest SO AMERICAN ANTHROPOLOGIST LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Krebs, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 6 TC 0 Z9 0 U1 1 U2 1 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 USA SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD JUN PY 2002 VL 104 IS 2 BP 649 EP 651 DI 10.1525/aa.2002.104.2.649 PG 3 WC Anthropology SC Anthropology GA 573RW UT WOS:000176845500023 ER PT J AU Pisano, DA AF Pisano, DA TI Wingless eagle: US army aviation through World War I. SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Pisano, DA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER HISTORICAL REVIEW PI WASHINGTON PA 400 A ST SE, WASHINGTON, DC 20003 USA SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD JUN PY 2002 VL 107 IS 3 BP 894 EP 895 DI 10.1086/532552 PG 2 WC History SC History GA 565HB UT WOS:000176362800060 ER PT J AU Des Marais, DJ Harwit, MO Jucks, KW Kasting, JF Lin, DNC Lunine, JI Schneider, J Seager, S Traub, WA Woolf, NJ AF Des Marais, DJ Harwit, MO Jucks, KW Kasting, JF Lin, DNC Lunine, JI Schneider, J Seager, S Traub, WA Woolf, NJ TI Remote sensing of planetary properties and biosignatures on extrasolar terrestrial planets SO ASTROBIOLOGY LA English DT Article DE spectroscopy; biosignatures; extrasolar planets; Terrestrial Planet Finder; Darwin; habitable planets ID HABITABLE ZONES; LIFE; EVOLUTION; EARTH; ATMOSPHERE; SIGNATURE; SEARCH; VENUS; STARS AB The major goals of NASA's Terrestrial Planet Finder (TPF) and the European Space Agency's Darwin missions are to detect terrestrial-sized extrasolar planets directly and to seek spectroscopic evidence of habitable conditions and life. Here we recommend wavelength ranges and spectral features for these missions. We assess known spectroscopic molecular band features of Earth, Venus, and Mars in the context of putative extrasolar analogs. The preferred wavelength ranges are 7-25 mum in the mid-IR and 0.5 to similar to1.1 mum in the visible to near-IR. Detection of O-2 or its photolytic product O-3 merits highest priority. Liquid H2O is not a bioindicator; but it is, considered essential to life. Substantial CO2 indicates an atmosphere and oxidation state typical of a terrestrial planet. Abundant CH4 might require a biological source, yet abundant CH4 also can arise from a crust and upper mantle more reduced than that of Earth: The range of characteristics of extrasolar rocky planets might far exceed that of the Solar System. Planetary size and mass are very important indicators of habitability and can be estimated in the mid-IR and potentially also in the visible to near-IR. Additional spectroscopic features merit study, for example, features created by other biosignature compounds in the atmosphere or on the surface and features due to Rayleigh scattering. In summary, we find that both the mid-IR and the visible to near-IR wavelength ranges offer valuable information regarding biosignatures and planetary properties; therefore both merit serious scientific consideration for TPF and Darwin. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Cornell Univ, Ithaca, NY USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, State Coll, PA USA. Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. Univ Arizona, Tucson, AZ USA. Observ Paris, Meudon, France. Inst Adv Study, Princeton, NJ 08540 USA. RP Des Marais, DJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 44 TC 246 Z9 248 U1 8 U2 51 PU MARY ANN LIEBERT INC PUBL PI LARCHMONT PA 2 MADISON AVENUE, LARCHMONT, NY 10538 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD SUM PY 2002 VL 2 IS 2 BP 153 EP 181 DI 10.1089/15311070260192246 PG 29 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 671KJ UT WOS:000182463700002 PM 12469366 ER PT J AU Lacy, M Gregg, M Becker, RH White, RL Glikman, E Helfand, D Winn, JN AF Lacy, M Gregg, M Becker, RH White, RL Glikman, E Helfand, D Winn, JN TI The reddest quasars. II. A gravitationally lensed FeLoBAL quasar SO ASTRONOMICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : absorption lines; quasars : individual (J100424.9+122922); radio continuum ID BROAD ABSORPTION-LINE; STELLAR OBJECTS; LUMINOSITY FUNCTION; RADIO GALAXIES; SKY SURVEY; QSO; DUST; EXTINCTION; EVOLUTION; REDSHIFT AB We report the discovery of a z = 2.65 low-ionization iron broad absorption line quasar, FIRST J100424.9+122922, which is gravitationally lensed by a galaxy at z approximate to 0.95. The object was discovered as part of a program to find very red quasars by matching the FIRST radio survey with the Two Micron All Sky Survey in the near-infrared. J100424.9+122922 is the second lensed system to be found in this program, suggesting that many gravitational lenses are probably missed from conventional optical quasar surveys. We have made a simple lens model and a rough estimate of the reddening in the immediate environment of the quasar which suggests that the quasar is intrinsically very luminous and is accreting at close to the Eddington limit of its similar to10(9) M. black hole. The lensing galaxy has a small amount of dust, which is responsible for some excess reddening observed in the fainter image of the quasar, but is otherwise a fairly typical massive elliptical galaxy. We model the selection effects working against the detection of red quasars in both lensed and unlensed samples. We show that these selection effects are very effective at removing even lightly reddened high-redshift quasars from magnitude-limited samples, whether they are lensed or not. This suggests that the red quasar population in general could be very large, and in particular the class of iron broad absorption line quasars of which J100424.9+122922 is a member may be much larger than their rarity in magnitude-limited samples would suggest. C1 Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94550 USA. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lacy, M (reprint author), Lawrence Livermore Natl Lab, IGPP, L-413, Livermore, CA 94550 USA. NR 43 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 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2002 VL 123 IS 6 BP 2925 EP 2935 DI 10.1086/340568 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556BW UT WOS:000175830300003 ER PT J AU Ramella, M Geller, MJ Pisani, A da Costa, LN AF Ramella, M Geller, MJ Pisani, A da Costa, LN TI The UZC-SSRS2 group catalog SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : distances and redshifts ID REDSHIFT-SPACE NEIGHBORHOODS; PERSEUS-PISCES SURVEY; LUMINOSITY FUNCTION; GALAXY GROUPS; LOOSE GROUPS; MAGNITUDE SCALE; CCD CALIBRATION; NEARBY GROUPS; X-RAY; SAMPLE AB We apply a friends-of-friends algorithm to the combined Updated Zwicky Catalog and Southern Sky Redshift Survey to construct a catalog of 1168 groups of galaxies; 411 of these groups have five or more members within the redshift survey. The group catalog covers 4.69 sr, and all groups exceed the number density contrast threshold deltarho/rho = 80. We demonstrate that the groups catalog is homogeneous across the two underlying redshift surveys; the catalog of groups and their members thus provides a basis for other statistical studies of the large-scale distribution of groups and their physical properties. The median physical properties of the groups are similar to those for groups derived from independent surveys, including the ESO Key Programme and the Las Campanas Redshift Survey. We include tables of groups and their members. C1 Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Ist Istruz Statale Classico Dante Alighieri, I-34170 Goriza, Italy. European So Observ, D-85748 Garching, Germany. RP Ramella, M (reprint author), Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34131 Trieste, Italy. OI Ramella, Massimo/0000-0001-5446-4749 NR 58 TC 94 Z9 94 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2002 VL 123 IS 6 BP 2976 EP 2984 DI 10.1086/340357 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556BW UT WOS:000175830300006 ER PT J AU Lane, WM Kassim, NE Ensslin, TA Harris, DE Perley, RA AF Lane, WM Kassim, NE Ensslin, TA Harris, DE Perley, RA TI 3C 129 at 90 centimeters: Evidence for a radio relic? SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : clusters : individual (4U 0446+44); galaxies : jets ID CLUSTER; GALAXIES; 3C-129 AB We present a new wide-field map of the radio galaxy 3C 129 and its companion galaxy 3C 129.1 at lambda = 90 cm. We see a distinct steep-spectrum feature near the head of 3C 129, extending in a direction perpendicular to the radio tails. We propose that this Crosspiece might consist of fossil radio plasma, which has been re-energized by the compression of the bow shock of the supersonically moving galaxy 3C 129. One possible origin of the fossil radio plasma could be the tail of a nearby head-tail radio galaxy. We discuss the implications of and give testable predictions for this scenario. C1 USN, Res Lab, Washington, DC 20375 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Lane, WM (reprint author), USN, Res Lab, Code 7213,4555 Overlook Ave SW, Washington, DC 20375 USA. NR 20 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2002 VL 123 IS 6 BP 2985 EP 2989 DI 10.1086/340359 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556BW UT WOS:000175830300007 ER PT J AU Harvey, DWA Wilner, DJ Di Francesco, J Lee, CW Myers, PC Williams, JP AF Harvey, DWA Wilner, DJ Di Francesco, J Lee, CW Myers, PC Williams, JP TI Limits on radio continuum emission from a sample of candidate contracting starless cores SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : globules; ISM : jets and outflows; radio continuum; stars : formation ID YOUNG STELLAR OBJECTS; INFALL MOTIONS; IRAS SOURCES; CLOUD; STARS; PROTOSTARS; COLLAPSE; REGIONS; DUST AB We have used the NRAO Very Large Array to search for 3.6 cm continuum emission from embedded protostars in a sample of eight nearby starless cores that show spectroscopic evidence for infalling motions in molecular emission lines. We detect a total of 13 compact sources in the eight observed fields to 5sigma limiting flux levels of typically 0.09 mJy. None of these sources lie within 1 0 of the central positions of the cores, and they are all likely background objects. Based on an extrapolation of the empirical correlation between the bolometric luminosity and 3.6 cm luminosity for the youngest protostars, these null detections place upper limits of similar to0.1 L-. (d /140 pc)(2) on the luminosities of protostellar sources embedded within these cores. These limits, together with the extended nature of the inward motions inferred from molecular line mapping, are inconsistent with the inside-out collapse model of singular isothermal spheres and suggest a less centrally condensed phase of core evolution during the earliest stages of star formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Harvey, DWA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Williams, Jonathan/B-1643-2009; OI Williams, Jonathan/0000-0001-5058-695X NR 27 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 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2002 VL 123 IS 6 BP 3325 EP 3328 DI 10.1086/340468 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556BW UT WOS:000175830300026 ER PT J AU Park, S Kenyon, SJ AF Park, S Kenyon, SJ TI Extended near-infrared emission from candidate protostars in the Taurus-Auriga molecular cloud SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared radiation; reflection nebulae; stars : formation; stars : pre main-sequence ID YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; ORION NEBULA CLUSTER; LOW-MASS PROTOSTARS; PROTOSTELLAR DISKS; SUBMILLIMETER CONTINUUM; PHOTOMETRIC VARIABILITY; IMAGING POLARIMETRY; EMBEDDED SOURCES; BINARY-SYSTEM AB We describe near-IR imaging data for a sample of 23 Class I sources in the Taurus-Auriga dark clouds. Combining our data with previous photometry, we detect brightness variations of similar to0.1-0.5 mag in many sources. The near-IR morphologies are consistent with millimeter continuum measurements. Most (similar to60%) of the sample are true protostars; the rest may be objects in transition between Class I and Class II, T Tauri stars with edge-on disks, or heavily reddened T Tauri stars. C1 Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Park, S (reprint author), Univ Calif Berkeley, Dept Phys, 366 LeConte Hall, Berkeley, CA 94720 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 79 TC 28 Z9 28 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2002 VL 123 IS 6 BP 3370 EP 3379 DI 10.1086/340467 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556BW UT WOS:000175830300030 ER PT J AU Mochejska, BJ Stanek, KZ Sasselov, DD Szentgyorgyi, AH AF Mochejska, BJ Stanek, KZ Sasselov, DD Szentgyorgyi, AH TI Planets in stellar clusters extensive search. I. Discovery of 47 low-amplitude variables in the metal-rich cluster NGC 6791 with millimagnitude image subtraction photometry SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; color-magnitude diagrams; novae, cataclysmic variables; stars : variables : other ID NGC-6791; STARS; OLD; SYSTEMS; MASS AB We have undertaken a long-term project, the Planets in Stellar Clusters Extensive Search ( PISCES), to search for transiting planets in open clusters. As our first target, we have chosen NGC 6791 a very old, populous, metal-rich cluster. We present the results of a test observing run at the F. L. Whipple Observatory's 1.2 m telescope. Our primary goal is to demonstrate the feasibility of obtaining the accuracy required for planetary-transit detection using image subtraction photometry on data collected with a 1 m class telescope. We present a catalog of 62 variable stars, 47 of them newly discovered, most with low-amplitude variability. Among those there are several BY Draconis type variables. We have also observed outbursts in the cataclysmic variables B7 and B8. C1 Centrum Astron Mikolaja Kopernika, PL-00716 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mochejska, BJ (reprint author), Centrum Astron Mikolaja Kopernika, Ulica Bartycka 18, PL-00716 Warsaw, Poland. NR 34 TC 62 Z9 62 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2002 VL 123 IS 6 BP 3460 EP 3472 DI 10.1086/340695 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556BW UT WOS:000175830300037 ER PT J AU Walsh, W Beck, R Thuma, G Weiss, A Wielebinski, R Dumke, M AF Walsh, W Beck, R Thuma, G Weiss, A Wielebinski, R Dumke, M TI Molecular gas in NGC 6946 SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE ISM : molecules; galaxies : spiral; radio lines : galaxies; submillimeter ID SPIRAL GALAXY NGC-6946; MASSIVE STAR FORMATION; NEARBY GALAXIES; H-I; INTERSTELLAR-MEDIUM; INFRARED-EMISSION; DISK GALAXIES; EXTENDED DISTRIBUTION; VERTICAL EQUILIBRIUM; SURFACE BRIGHTNESS AB We present imaging of molecular gas emission in the star-forming spiral galaxy NGC 6946. Our (CO)-C-12(1-0) and (CO)-C-12(3-2) images, made at 22" resolution with the IRAM 30-m and the Heinrich Hertz 10-m radio telescopes, are the most extensive observations of molecular gas in this galaxy and are among the most extensive observations of molecular gas in any spiral galaxy. The (CO)-C-12(1-0) emission shows a central concentration aligned in a north-south ellipse, an extended diffuse component plus concentrations in the outer spiral arms. (CO)-C-12(1-0) is detected across most of the optical disk out to a projected radius of nearly 300". The molecular component in NGC6946 is unusually massive, with M-H2/M-HI = 0.57. The scale length of the disk in (CO)-C-12(1-0) is the same, to within 5%, as the VRI, Halpha, 15 mum, and FIR disks. The (CO)-C-12(3-2) data shows broadly similar structure to the (CO)-C-12(1-0) image out to the observed limit of 200", although the arm-interarm contrast of (CO)-C-12(3-2) is significantly larger than that of (CO)-C-12(1-0) which suggests that molecules in the spiral arms are warmer or reside longer there. The rotation curve derived from the (CO)-C-12(1-0) velocity field agrees, within the uncertainties, with the H I rotation curve. The velocity dispersion is 40 +/- 10 km s(-1) in the inner 2 kpc and 8 +/- 3 km s(-1) in the disk, without tendency to increase in the spiral arms. Spectra of the (CO)-C-13(1-0), (CO)-C-13(2-1), (CO)-C-12-O-18(1-0) isotopomers for several positions are used for line ratio studies of the state of the molecular ISM in NGC 6946. In the centre of NGC 6946 our LVG analysis suggests that the beam-averaged gas kinetic temperature is 40 +/- 5 K, the molecular gas density is (3.3 +/- 0.3) x 10(3) cm(-3) and that line opacities are high, with tau12(CO(3-2)) similar to 10. A star formation efficiency image for NGC 6946, made from the Halpha image divided by the molecular gas image, ranges by over two orders of magnitude with highest values found in the northeastern spiral arm. The lambda6 cm polarized emission image, which traces the regular part of the magnetic field, appears anti-correlated with the star formation efficiency. We present an analysis of the ISM in NGC 6946's disk by making 1-D and 2-D comparisons of images made in several wavebands. Using a point-by-point correlation technique, we investigate the distribution and kinematics of the molecular gas and its relation to the neutral and ionized gas, the mid-infrared-emitting dust, the radio continuum and the magnetic field, and find that the molecular gas is closely associated with the 7 mum-emitting dust. The highest correlation between any pair of tracers is found between the mid-infrared emission and the total radio continuum emission at lambda6 cm. This cannot be due to dust heating and gas ionization in star-forming regions because the thermal radio emission is less correlated with the mid-infrared emission than the nonthermal emission. A coupling of magnetic fields to gas clouds is proposed as a possible scenario. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. Univ Arizona, Steward Observ, SMTO, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Walsh, W (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. NR 151 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 JUN PY 2002 VL 388 IS 1 BP 7 EP 28 DI 10.1051/0004-6361:20020467 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 557GX UT WOS:000175901700008 ER PT J AU Girart, JM Viti, S Williams, DA Estalella, R Ho, PTP AF Girart, JM Viti, S Williams, DA Estalella, R Ho, PTP TI The molecular condensations ahead of Herbig-Haro objects - I. Multi-transition observations of HH 2 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : individual objects : HH 2; ISM : abundances; ISM : clouds; ISM : molecules; radio lines : ISM; stars : formation ID STAR-FORMING REGIONS; HYPERFINE ANOMALIES; CHEMICAL EVOLUTION; VLA OBSERVATIONS; LINE EMISSION; HCO+ EMISSION; SPECTRAL-LINE; DARK CLOUDS; CHEMISTRY; MODELS AB We present a CSO and BIMA molecular line survey of the dense, quiescent molecular environment ahead of HH 2. The molecular gas is cold, 13 K, and moderately dense, 3 x 10(5) cm(-3). A total of 14 species has been detected (including different isotopes and deuterated species). The relative abundances of the clump are compared with other dense molecular environments, including quiescent dark clouds, and active low and high mass star forming regions. This comparison confirms the peculiar chemical composition of the quiescent gas irradiated by the HH objects. Thus, from this comparison, we found that the HCO(+), CH(3)OH and H(2)CO are strongly enhanced. SO and SO(2) are weakly enhanced, whereas HCN and CS are underabundant. The CN abundance is within the range of values found in starless dark clouds, but it is low with respect to high mass star forming regions. Finally, the chemical composition of HH 2 confirms the qualitative results of the Viti & Williams (1999) complex chemical model that follows the chemical behavior of a molecular clump irradiated by a HH object. C1 Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. UCL, Dept Phys & Astron, London WC1E 6BT, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Girart, JM (reprint author), Univ Barcelona, Dept Astron & Meteorol, Av Diagonal 647, E-08028 Barcelona, Spain. EM jgirart@am.ub.es RI Girart, Josep/O-1638-2014 OI Girart, Josep/0000-0002-3829-5591 NR 62 TC 36 Z9 36 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2002 VL 388 IS 3 BP 1004 EP 1015 DI 10.1051/0004-6361:20020536 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 566RD UT WOS:000176441300021 ER PT J AU De Rosa, A Piro, L Fiore, F Grandi, P Maraschi, L Matt, G Nicastro, F Petrucci, PO AF De Rosa, A Piro, L Fiore, F Grandi, P Maraschi, L Matt, G Nicastro, F Petrucci, PO TI The BeppoSAX broad-band spectrum and variability of the Seyfert 1 NGC 3783 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : individual : NGC 3783; galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEUS; XMM-NEWTON OBSERVATION; RAY-ABSORPTION LINES; IRON LINE; ASCA OBSERVATIONS; GALAXY NGC-5548; WARM ABSORBER; NGC-3783; EMISSION; DISK AB BeppoSAX observed the Seyfert 1 galaxy NGC 3783 for similar to5 days from 1998 June 6 to 1998 June 10. The average flux during the observation was F2-10 keV similar to 6 x 10(-11) erg cm(-2) s(-1). The long exposure provided a very high quality spectrum that exhibits all the typical features of Seyfert 1s. The high energy cut-off of the intrinsic continuum, at E-c = 340+/-(560)(107) keV, was detected for the first time in this object. During the observation the source showed modest flux variations (similar to20% in 2-10 keV) and spectral variability that can be completely explained by a change of the intrinsic slope DeltaGamma similar to 0.1. NGC 3783 is one of the few Seyfert 1s that exhibits a soft emission component in the BeppoSAX spectrum. This soft excess is well reproduced by a black body component with temperature kT similar to 0.2 keV. A warm absorber is also required to fit the soft X-ray spectrum. Both reprocessing features, the Compton reflection hump and the Fe emission line, were detected in our observation. In addition to a narrow iron line (as observed by Chandra) a broad component with sigma = 0.72+/-(1.28)(0.27) keV and EW = 115 +/- 76 eV, is required to fit the line. The observed Compton hump and the Fe line are well reproduced with the ionized (log xi = 2.73+/-(0.04)(0.05)) disc reflection model of Ross & Fabian. In this case the soft excess observed below 2 keV can be accounted for by the disc emissivity and no additional soft X-rays component is required to fit the spectrum. C1 CNR, Inst Astrophys Spaziale, Rome, Italy. Osserv Astron Roma, Monte Porzio Catone, Italy. Univ Study Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. Osserv Astron Brera, Milan, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Astrophys Lab, Grenoble, France. RP De Rosa, A (reprint author), CNR, Inst Astrophys Spaziale, Via Fosso Cavaliere, Rome, Italy. RI PIRO, LUIGI/E-4954-2013; OI PIRO, LUIGI/0000-0003-4159-3984; Nicastro, Fabrizio/0000-0002-6896-1364; Grandi, Paola/0000-0003-1848-6013; De Rosa, Alessandra/0000-0001-5668-6863; Fiore, Fabrizio/0000-0002-4031-4157 NR 44 TC 27 Z9 27 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2002 VL 387 IS 3 BP 838 EP 849 DI 10.1051/0004-6361:20020444 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 557GT UT WOS:000175901300008 ER PT J AU Beuther, H Schilke, P Gueth, F McCaughrean, M Andersen, M Sridharan, TK Menten, KM AF Beuther, H Schilke, P Gueth, F McCaughrean, M Andersen, M Sridharan, TK Menten, KM TI IRAS 05358+3543: Multiple outflows at the earliest stages of massive star formation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE molecular data; stars : early-type; stars : formation; stars : individual : IRAS 05358+3543; ISM : jets and outflows ID MOLECULAR OUTFLOWS; (PROTO)STAR IRAS-20126+4104; REGIONS; CLOUDS; GALAXY; LINE; DISK; ACCRETION; CLUSTERS; EMISSION AB We present a high-angular-resolution molecular line and millimeter continuum study of the massive star formation site IRAS 05358+3543. Observations with the Plateau de Bure Interferometer in CO 1-0, SiO 2-1 and (HCO+)-C-13 1-0 reveal at least three outflows which cannot be separated in single-dish data. Observations at millimeter and sub-millimeter wavelengths from the IRAM 30 m telescope and the CSO provide additional information on the region. The most remarkable feature is a highly collimated (collimation factor similar to10) and massive (>10 M.) bipolar outflow of similar to1 pc length, which is part of a quadrupolar outflow system. The three observed molecular outflows forming the IRAS 05358+3543 outflow system resemble, in structure and collimation, those typical of low-mass star-forming regions. They might therefore, just like low-mass outflows, be explained by shock entrainment models of jets. We estimate a mass accretion rate of similar to10(-4) M./yr, sufficient to overcome the radiative pressure of the central object and to build up a massive star, lending further support to the hypothesis that massive star formation occurs similarly to low-mass star formation, only with higher accretion rates and energetics. In the millimeter continuum, we find three sources near the center of the quadrupolar outflow, each with a mass of 75-100 M.. These cores are associated with a complex region of infrared reflection nebulosities and their embedded illuminating sources. The molecular line data show that SiO is found mostly in the outflows, whereas (HCO+)-C-13 traces core-like structures, though likely with varying relative abundances. Thermal CH3OH comprises both features and can be disentangled into a core-tracing component at the line center, and wing emission following the outflows. A CO line-ratio study (using data of the J = 1-0, 2-1 and 6-5 transitions) reveals local temperature gradients. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beuther, H (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. NR 56 TC 123 Z9 124 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2002 VL 387 IS 3 BP 931 EP 943 DI 10.1051/0004-6361:20020319 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 557GT UT WOS:000175901300015 ER PT J AU Greiner, J Di Stefano, R AF Greiner, J Di Stefano, R TI X-ray off states and optical variability in CAL 83 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-ray : stars; accretion, accretion disks; stars : binaries : close; stars : individual : CAL 83 ID LARGE MAGELLANIC CLOUD; SOURCE RX J0513.9-6951; ACCRETION DISK; LMC; NOVA; BINARIES; EMISSION; EVOLUTION; MODELS; WINDS AB CAL 83 was one of the first supersoft X-ray binaries (SSBs) to be discovered and is considered to be the prototype of its class. In 15 X-ray observations between 1983-1997 it was observed to have nearly constant X-ray luminosity and temperature, with the exception of one off-state in 1996 (Kahabka et al. 1996). We report on a second X-ray off-state, discovered with a Chandra ACIS-S observation in November 1999. We consider the long-term X-ray and MACHO optical light curves. We find that, during more than 7 years of monitoring by the MACHO team, CAL 83 has exhibited distinct and well-defined low, intermediate, and high optical states. Transitions between states are not accompanied by color variations. We also find that both X-ray off states were observed during optical high states and were followed by optical low states within similar to50 days. We discuss possible explanations for the observed optical and X-ray variations. While photospheric adjustments might account for the variations in soft X-ray flux, optical variations can be explained only by invoking changes in the accretion disk, which is the primary source of optical radiation. C1 Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greiner, J (reprint author), Astrophys Inst Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. NR 44 TC 26 Z9 26 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2002 VL 387 IS 3 BP 944 EP 954 DI 10.1051/0004-6361:20020463 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 557GT UT WOS:000175901300016 ER PT J AU Dobrzycki, A Bechtold, J Scott, J Morita, M AF Dobrzycki, A Bechtold, J Scott, J Morita, M TI A uniform analysis of the Ly alpha Forest at z=0-5. IV. The clustering and evolution of clouds at z <= 1.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE intergalactic medium; quasars : absorption lines ID LINE KEY PROJECT; LOW-REDSHIFT; ABSORPTION SYSTEMS; ABSORBERS; SPECTRUM; SAMPLE AB We present results on the evolution and clustering of Lyalpha lines at low redshift as part of our series A Uniform Analysis of the Lyalpha Forest at z = 0-5." The sample analyzed in this paper contains 1298 Lyalpha absorption lines from 165 quasar spectra mined from the archives of the Faint Object Spectrograph on the Hubble Space Telescope (HST). Our sample extends to z approximate to1.7, slightly higher than the sample analyzed by the HST Quasar Absorption Line Key Project. We confirm the result from the Key Project that the number density evolution of Lyalpha lines at low redshifts can be described by a power law that is significantly flatter than that found at high z. We find that the evolution is somewhat steeper than obtained previously. Specifically, we find gamma = 0.54 +/- 0.21 for lines with equivalent widths greater than 0.24 Angstrom and gamma = 0.60 +/- 0.14 using a variable equivalent width threshold. We find that the difference between our and Key Project results is likely attributable to different redshift coverage of the two samples. The results concerning the number density evolution are not significantly affected if one includes Lyalpha lines which are members of metal systems. Object-to-object fluctuations in the number of lines detected are small, indicating a high degree of uniformity in the intergalactic medium on large scales. We find marginal evidence that weak and strong lines undergo different evolution. We find weak clustering for Lyalpha lines at velocity separations DeltaV less than or equal to 500 km s(-1), weaker than the level predicted from an earlier analysis by Ulmer of a small subsample of the Key Project data. We see no correlations for metal system-Lyalpha forest or extensive metal system-Lyalpha forest combinations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Dobrzycki, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 70, Cambridge, MA 02138 USA. NR 40 TC 14 Z9 14 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2002 VL 571 IS 2 BP 654 EP 664 DI 10.1086/339983 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556CB UT WOS:000175830800008 ER PT J AU Scott, J Bechtold, J Morita, M Dobrzycki, A Kulkarni, VP AF Scott, J Bechtold, J Morita, M Dobrzycki, A Kulkarni, VP TI A uniform analysis of the Ly alpha Forest at z=0-5. V. The extragalactic ionizing background at low redshift SO ASTROPHYSICAL JOURNAL LA English DT Review DE diffuse radiation; intergalactic medium; quasars : absorption lines ID HUBBLE-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; QUASI-STELLAR OBJECTS; LINE KEY PROJECT; ULTRAVIOLET EMISSION PROPERTIES; RADIO-LOUD QUASARS; MG-II ABSORPTION; HYDROGEN CLOUDS; HIGH-RESOLUTION; GASEOUS EXTENT AB In Paper III of our series, "A Uniform Analysis of the Lyalpha Forest at z = 0-5," we presented a set of 270 quasar spectra from the archives of the Faint Object Spectrograph ( FOS) on the Hubble Space Telescope (HST). A total of 151 of these spectra, yielding 906 lines, are suitable for using the proximity effect signature to measure J(nu(o)), the mean intensity of the hydrogen-ionizing background radiation field, at low redshift. Using a maximum-likelihood technique and the best estimates possible for each QSO's Lyman limit flux and systemic redshift, we find J(nu(o)) = 7.6(-3.0)(+9.4) x 10(-23) erg s(-1) cm(-2) Hz(-1) sr(-1) at 0.03 < z < 1.67. This is in good agreement with the mean intensity expected from models of the background which incorporate only the known quasar population. When the sample is divided into two subsamples, consisting of lines with z < 1 and z > 1, the values of J(nu(o)) found are 6.5(-1.6)(+38.) x 10(-23) erg s(-1) cm(-2) Hz(-1) sr(-1), and 1.0(-0.2)(+3.8) x 10(-22) erg s(-1) cm(-2) Hz(-1) sr(-1), respectively, indicating that the mean intensity of the background is evolving over the redshift range of this data set. Relaxing the assumption that the spectral shapes of the sample spectra and the background are identical, the best-fit H I photoionization rates are found to be 6.7 x 10(-13) s(-1) for all redshifts, and 1.9 x 10(-13) and 1.3 x 10(-12) s(-1) for z < 1 and z > 1, respectively. The inclusion of blazars, associated absorbers, or damped Lyalpha absorbers, or the consideration of a LambdaCDM cosmology rather than one in which Omega(Lambda)= 0 has no significant effect on the results. The result obtained using radio-loud objects is not significantly different from that found using radio-quiet objects. Allowing for a variable equivalent width threshold gives a consistently larger value of J(nu(o)) than the constant threshold treatment, though this is found to be sensitive to the inclusion of a small number of weak lines near the QSO emission redshifts. This work confirms that the evolution of the number density of Lyalpha lines is driven by a decrease in the ionizing background from z similar to 2 to z similar to 0 as well as by the formation of structure in the intergalactic medium. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ S Carolina, Dept Phys & Astron, Columbia, SC 29208 USA. RP Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM jscott@as.arizona.edu; jbechtold@as.arizona.edu; mmorita@as.arizona.edu; adobrzycki@cfa.harvard.edu; varsha@mail.psc.sc.edu NR 143 TC 58 Z9 58 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2002 VL 571 IS 2 BP 665 EP 692 DI 10.1086/339982 PN 1 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556CB UT WOS:000175830800009 ER PT J AU Green, PJ Kochanek, C Siemiginowska, A Kim, DW Markevitch, M Silverman, J Dosaj, A Jannuzi, BT Smith, C AF Green, PJ Kochanek, C Siemiginowska, A Kim, DW Markevitch, M Silverman, J Dosaj, A Jannuzi, BT Smith, C TI Chandra observations of the QSO pair Q2345+007: Binary or massive dark lens? SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : absorption lines; quasars : individual (Q2345+007); X-rays : general; X-rays : individual (Q2345+007) ID BRIGHT QUASAR SURVEY; OPTICALLY SELECTED QUASARS; HIGH-REDSHIFT CLUSTER; X-RAY PROPERTIES; ROSAT OBSERVATIONS; STELLAR OBJECTS; COMPLETE SAMPLE; GALAXY; SYSTEM; Q1634+267A,B AB The components of the wide (7."3) separation quasar pair Q2345+007A, B (z = 2.15) have the most strikingly similar optical spectra seen to date (Steidel & Sargent) yet no detected lensing mass, making this system the best candidate known for a massive (similar to10(14) M-.) dark matter lens system. Here we present results from a 65 ks Chandra observation designed to investigate whether it is a binary quasar or a gravitational lens. We find no X-ray evidence for a lensing cluster to a (0.5-2 keV) flux limit of 2 x 10(-15) ergs cm(-2) s(-1), which is consistent with lensing only for a reduced baryon fraction. Using the Chandra X-ray observations of the quasars themselves, together with new and published optical measurements, we use the observed emission properties of the quasars for further tests between the lens and binary hypotheses. Assuming similar line-of-sight absorption to the images, we find that their X-ray continuum slopes are inconsistent (Gamma(A) = 2.30(-0.30)(+0.36) and Gamma(B) = 0.83(-0.44)(+0.49)) as are their X-ray to optical flux ratios. The probability that B suffers intrinsic absorption sufficient to account for these spectral differences is negligible. We present new optical evidence that the flux ratio of the pair is variable, so the time delay in a lens scenario could cause some of the discrepancies. However, adequately large variations in overall spectral energy distribution are rare in individual QSOs. All new evidence here weighs strongly toward the binary interpretation. Q2345+ 007 thus may represent the highest redshift example known of an interaction-triggered but as-yet unmerged luminous active galactic nucleus. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. RP Green, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 70 TC 19 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 JUN 1 PY 2002 VL 571 IS 2 BP 721 EP 732 DI 10.1086/340051 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556CB UT WOS:000175830800012 ER PT J AU Horan, D Badran, HM Bond, IH Bradbury, SM Buckley, JH Carson, MJ Carter-Lewis, DA Catanese, M Cui, W Dunlea, S Das, D Perez, ID D'Vali, M Fegan, DJ Fegan, SJ Finley, JP Gaidos, JA Gibbs, K Gillanders, GH Hall, TA Hillas, AM Holder, J Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krennrich, F Lang, MJ LeBohec, S Lessard, R Lloyd-Evans, J McKernan, B Moriarty, P Muller, D Ong, R Pallassini, R Petry, D Quinn, J Reay, NW Reynolds, PT Rose, HJ Sembroski, GH Sidwell, R Stanton, N Swordy, SP Vassiliev, VV Wakely, SP Weekes, TC AF Horan, D Badran, HM Bond, IH Bradbury, SM Buckley, JH Carson, MJ Carter-Lewis, DA Catanese, M Cui, W Dunlea, S Das, D Perez, ID D'Vali, M Fegan, DJ Fegan, SJ Finley, JP Gaidos, JA Gibbs, K Gillanders, GH Hall, TA Hillas, AM Holder, J Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krennrich, F Lang, MJ LeBohec, S Lessard, R Lloyd-Evans, J McKernan, B Moriarty, P Muller, D Ong, R Pallassini, R Petry, D Quinn, J Reay, NW Reynolds, PT Rose, HJ Sembroski, GH Sidwell, R Stanton, N Swordy, SP Vassiliev, VV Wakely, SP Weekes, TC TI Detection of the BL Lacertae object H1426+428 at TeV gamma-ray energies SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (1ES 1426+42.8) gamma rays : observations ID BLAZARS; MARKARIAN-421; SPECTRUM; EMISSION; LAC; PHOTONS; SYSTEM AB A very high energy gamma-ray signal has been detected at the 5.5sigma level from H1426+ 428, an X-ray-selected BL Lacertae object at a redshift of 0.129. The object was monitored from 1995 to 1998 with the Whipple 10 m imaging atmospheric Cerenkov telescope as part of a general blazar survey; the results of these observations, although not statistically significant, were consistently positive. X-ray observations of H1426+ 428 during 1999 with the BeppoSAX instrument revealed that the peak of its synchrotron spectrum occurs at greater than 100 keV, leading to the prediction of observable TeV emission from this object. H1426+ 428 was monitored extensively at the Whipple Observatory during the 1999, 2000, and 2001 observing seasons. The strongest TeV signals were detected in 2000 and 2001. During 2001, an integral flux of 2.04 +/- 0.35 x 10(-11) cm(-2) s(-1) above 280 GeV was recorded from H1426+ 428. The detection of H1426+ 428 supports the idea that, as also seen in Mrk 501 and 1ES 2344+ 514, BL Lacertae objects with extremely high synchrotron peak frequencies produce gamma-rays in the TeV range. C1 Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Natl Univ Ireland Univ Coll Dublin, Expt Phys Dept, Dublin 4, Ireland. Tanta Univ, Dept Phys, Tanta, Egypt. 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. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Natl Univ Ireland Univ Coll Galway, Dept Phys, Galway, Ireland. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. 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 Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Cork Inst Technol, Dept Phys, Cork, Ireland. RP Horan, D (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, POB 97, Amado, AZ 85645 USA. OI Carson, Michael/0000-0003-0400-7819; Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 46 TC 89 Z9 90 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2002 VL 571 IS 2 BP 753 EP 762 DI 10.1086/340019 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556CB UT WOS:000175830800014 ER PT J AU Warren, HP Warshall, AD AF Warren, HP Warshall, AD TI Temperature and density measurements in a quiet coronal streamer SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona ID X-RAY TELESCOPE; SOLAR CORONA; EXTREME-ULTRAVIOLET; IONIZATION BALANCE; ELECTRON-DENSITIES; TRANSITION REGION; SUMER TELESCOPE; SOHO; SPECTROMETER; SPECTRA AB Many previous studies have used emission line or broadband filter ratios to infer the presence of temperature gradients in the quiet solar corona. Recently it has been suggested that these temperature gradients are not real, but result from the superposition of isothermal loops with different temperatures and density scale heights along the line of sight. A model describing this hydrostatic weighting bias has been developed by Aschwanden & Acton. In this paper we present the application of the Aschwanden & Acton differential emission measure model to Solar and Heliospheric Observatory Solar Ultraviolet Measurement of Emitted Radiation (SUMER) observations of a quiet coronal streamer. Simultaneous Yohkoh soft X-ray telescope (SXT) observations show increases in the filter ratios with height above the limb, indicating an increase in temperature. The application of the Aschwanden & Acton model to these SUMER data, however, show that the temperature is constant with height and that the distribution of temperatures in the corona is much too narrow for the hydrostatic weighting bias to have any effect on the SXT filter ratios. We consider the possibility that there is a tenuous hot component (similar to3 MK) that accounts for the SXT observations. We find that a hot plasma with an emission measure sufficient to reproduce the observed SXT fluxes would also produce significant count rates in the high-temperature emission lines in the SUMER wavelength range. These lines are not observed, and we conclude that the SUMER spectra are not consistent with the SXT filter ratio temperatures. Calculations from a hydrodynamic loop model suggest that nonuniform footpoint heating may be consistent with the temperatures and densities observed at most heights, consistent with the recent analysis of relatively cool (similar to1 MK) active region loops. We also find, however, that at the lowest heights the observed densities are smaller than those predicted by uniform or footpoint heating. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 58, Cambridge, MA 02138 USA. EM hwarren@cfa.harvard.edu NR 35 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2002 VL 571 IS 2 BP 999 EP 1007 DI 10.1086/340069 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556CB UT WOS:000175830800035 ER PT J AU Strachan, L Suleiman, R Panasyuk, AV Biesecker, DA Kohl, JL AF Strachan, L Suleiman, R Panasyuk, AV Biesecker, DA Kohl, JL TI Empirical densities, kinetic temperatures, and outflow velocities in the equatorial streamer belt at solar minimum SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : corona; Sun : UV radiation; techniques : spectroscopic ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; WHOLE-SUN-MONTH; MAGNETIC-FIELD; SOURCE REGIONS; WIND; MODEL; SLOW; ACCELERATION; UVCS/SOHO; ORIGINS AB We use combined Ultraviolet Coronagraph Spectrometer and Large Angle Spectroscopic Coronagraph data to determine the O5+ outflow velocities as a function of height along the axis of an equatorial streamer at solar minimum and as a function of latitude (at 2.3 R-circle dot from Sun center). The results show that outflow increases rather abruptly in the region between 3.6 and 4.1 R-circle dot near the streamer cusp and gradually increases to similar to90 km s(-1) at similar to5 R-circle dot in the streamer stalk beyond the cusp. The latitudinal variation at 2.3 R-circle dot shows that there is no outflow (within the measurement uncertainties) in the center of the streamer, called the core, and that a steep increase in outflow occurs just beyond the streamer legs, where the O VI gimel1032 intensity relative to H I gimel1216 (Lyalpha) is higher than in the core. Velocity variations in both height and latitude show that the transitions from no measurable outflow to positive outflow are relatively sharp and thus can be used to infer the location of the transition from closed to open field lines in streamer magnetic field topologies. Such information, including the densities and kinetic temperatures derived from the observations, provides hard constraints for realistic theoretical models of streamers and the source regions of the slow solar wind. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Emergent Informat Technol Inc, Greenbelt, MD 20771 USA. RP Strachan, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 38 TC 105 Z9 110 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2002 VL 571 IS 2 BP 1008 EP 1014 DI 10.1086/339984 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556CB UT WOS:000175830800036 ER PT J AU Cecchi-Pestellini, C Bodo, E Balakrishnan, N Dalgarno, A AF Cecchi-Pestellini, C Bodo, E Balakrishnan, N Dalgarno, A TI Rotational and vibrational excitation of CO molecules by collisions with He-4 atoms SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; molecular data; molecular processes ID INTERACTION ENERGY SURFACE; INELASTIC-COLLISIONS; INFRARED-SPECTRUM; CARBON-MONOXIDE; UNIMOLECULAR DISSOCIATION; COORDINATE DEPENDENCE; SPECTROSCOPY; SCATTERING; RELAXATION; DEACTIVATION AB Full close-coupled calculations are carried out of the cross sections for energy transfer between rotational levels of carbon monoxide in collision with He-4 atoms with energies between 5 and 600 cm(-1). At low energies, the cross sections are dominated by contributions from shape resonances. The calculated cross sections are in satisfactory agreement with the experimental data measured at an energy of 570 cm(-1). Calculations using the infinite order sudden approximation are carried out of cross sections for energy transfer between vibrational levels of CO. Vibrational energy transfer is dominated by transitions in which the vibrational quantum number changes by unity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cecchi-Pestellini, C (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, Largo E Fermi 5, I-50125 Florence, Italy. RI Bodo, Enrico/F-4375-2012; OI Cecchi Pestellini, Cesare/0000-0001-7480-0324 NR 33 TC 35 Z9 35 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 JUN 1 PY 2002 VL 571 IS 2 BP 1015 EP 1020 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556CB UT WOS:000175830800037 ER PT J AU Schwartz, DA AF Schwartz, DA TI A Chandra search for X-ray jets in z approximate to 6 quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : general; quasars : individual (SDSSp J083643.85+005453.3, SDSSp J103027.10+052455.0, SDSSp J130608.26+035626.3); X-rays : galaxies ID PKS-0637-752; SPECTRA AB We have searched for X-ray jets in the recent Chandra observations of three Sloan Digital Sky Survey (SDSS) quasars at redshift z approximate to 6. All three quasars were detected in X-rays in these relatively short observations. SDSS 1030+0524 is not consistent with a point source and may be a gravitationally lensed system. We find a possible jetlike feature 23" from the quasar SDSS 1306+0356. We can explain the emission by inverse Compton scattering off the cosmic microwave background, assuming that the intrinsic properties of the system are similar to X-ray jets at z<1. Deeper observations to investigate the jet interpretation will be practical. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 24 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 JUN 1 PY 2002 VL 571 IS 2 BP L71 EP L75 DI 10.1086/341359 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556CE UT WOS:000175831100001 ER PT J AU Bechtold, J Dobrzycki, A Wilden, B Morita, M Scott, J Dobrzycka, D Tran, KV Aldcroft, TL AF Bechtold, J Dobrzycki, A Wilden, B Morita, M Scott, J Dobrzycka, D Tran, KV Aldcroft, TL TI A uniform analysis of the Ly alpha forest at z=0-5. III. Hubble Space Telescope faint object spectrograph spectral atlas SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE intergalactic medium; quasars : absorption lines; ultraviolet : general ID LINE KEY PROJECT; BRIGHT QSO SURVEY; QUASI-STELLAR OBJECTS; REDSHIFT MG-II; ABSORPTION SYSTEMS; LYMAN-ALPHA; HIGH-RESOLUTION; COSMOLOGICAL EVOLUTION; EQUATORIAL FIELDS; GALAXIES AB We analyzed the absorption line spectra of all quasars observed with the high-resolution gratings of the Faint Object Spectrograph on board the Hubble Space Telescope. We examined 788 spectra for 334 quasars and present line lists and identifications of absorption lines in the spectra of 271 of them. Analysis of the statistics of the Lyalpha and metal absorption systems are presented in companion papers. The data and several analysis products are available electronically and on the authors Web site. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bechtold, J (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NR 74 TC 46 Z9 46 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2002 VL 140 IS 2 BP 143 EP 238 DI 10.1086/342489 PG 96 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556LG UT WOS:000175850400002 ER PT J AU Bersier, D AF Bersier, D TI Fundamental parameters of Cepheids. V. Additional photometry and radial velocity data for southern Cepheids SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE Cepheids; techniques : photometric; techniques : radial velocities ID COLOR EXCESSES; G-SUPERGIANTS AB I present photometric and radial velocity data for Galactic Cepheids, most of them being in the southern hemisphere. There are 1250 Geneva seven-color photometric measurements for 62 Cepheids, the average uncertainty per measurement is better than 0.01 mag. A total of 832 velocity measurements have been obtained with the CORAVEL radial velocity spectrograph for 46 Cepheids. The average accuracy of the radial velocity data is 0.38 km s(-1). There are 33 stars with both photometry and radial velocity data. I discuss the possible binarity or period change that these new data reveal. I also present reddenings for all Cepheids with photometry. The data are available electronically. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bersier, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 23 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2002 VL 140 IS 2 BP 465 EP 468 DI 10.1086/342487 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556LG UT WOS:000175850400011 ER PT J AU Gilbert, GS Ferrer, A Carranza, J AF Gilbert, GS Ferrer, A Carranza, J TI Polypore fungal diversity and host density in a moist tropical forest SO BIODIVERSITY AND CONSERVATION LA English DT Article; Proceedings Paper CT 7th Meeting of the Subsidiary Body on Scientific, Technical and Technological Advice of the Convention on Biological Diversity CY NOV 12-16, 2001 CL MONTREAL, CANADA DE Barro Colorado Island; density dependence; fungi; Panama; polypores ID WOOD-INHABITING FUNGI; NEOTROPICAL FOREST; SPECIES-DIVERSITY; RAIN-FOREST; ABUNDANCE; BIODIVERSITY; CONSERVATION; SPECIFICITY; MORTALITY; SEEDLINGS AB In a moist tropical forest in Panama, the wood-decay polypore fungi comprise many rare species (more than half found only once) and exhibit diversity that exceeds that of the supporting tree community. The most abundant fungal species were non-specialists, each found on several host species from multiple plant families. In diverse fungal communities, each of many species should infect a given host species in a density-dependent manner, so that the infected proportion of a host population should increase with host density. Applied across host species, hosts with denser populations should support greater fungal diversity. For 10 tree species, fungal incidence and diversity increased with abundance of the host in the community, consistent with across-species density-dependent infection. Fungal diversity associated with individual trunks did not, however, vary with host-species density. Both host density and persistence of decaying logs may be important in determining fungal diversity associated with tree species. C1 Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. SUNY Coll Environm Sci & Forestry, Dept Environm & Forest Biol, Syracuse, NY 13210 USA. Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. RP Gilbert, GS (reprint author), Univ Calif Santa Cruz, Dept Environm Studies, 481 Nat Sci 2, Santa Cruz, CA 95064 USA. RI Gilbert, Gregory/C-2595-2008 NR 31 TC 42 Z9 46 U1 3 U2 16 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD JUN PY 2002 VL 11 IS 6 BP 947 EP 957 DI 10.1023/A:1015896204113 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 562EP UT WOS:000176184700002 ER PT J AU Liu, AZ Li, DZ Wang, H Kress, WJ AF Liu, AZ Li, DZ Wang, H Kress, WJ TI Ornithophilous and chiropterophilous pollination in Musa itinerans (Musaceae), a pioneer species in tropical rain forests of Yunnan, southwestern China SO BIOTROPICA LA English DT Article DE chiropterophily; Musa itinerans; ornithophily; pioneer species; pollination ecology; Yunnan ID DISPERSAL; MORPHOLOGY; PHENOLOGY; HELICONIA; ECOLOGY; TREE AB The role of bats and sunbirds in the pollination ecology of Musa itinerans Cheesman (Musaceae) was studied in the tropical seasonal rain forests of Xishuangbanna, southern Yunnan, China, It was found that both long-tongued fruit bats (Macroglossus sobrinus) and sunbirds (Arachnothera longirostris) were effective pollinators of M. itinerans. Nectar production had two peaks, one during the day and one during night (0800-1200 h and 2000-2400 h), which allowed the two different foragers to visit at specific times, The visitation patterns of the two foragers coincided with both flowering time and nectar production. By measuring the differences in fruit weight and seed production among different bagging experiments, we found that birds and bats were equally effective as pollinators of this species. C1 Chinese Acad Sci, Kunming Inst Bot, Kunming 620204, Peoples R China. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Li, DZ (reprint author), Chinese Acad Sci, Kunming Inst Bot, Kunming 620204, Peoples R China. EM dzl@mail.kib.ac.cn RI Liu, aizhong/F-1770-2010; Li, De-Zhu/G-8203-2011 NR 31 TC 16 Z9 24 U1 1 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JUN PY 2002 VL 34 IS 2 BP 254 EP 260 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 569EE UT WOS:000176587000007 ER PT J AU Leverington, DW Teller, JT Mann, JD AF Leverington, DW Teller, JT Mann, JD TI A GIS method for reconstruction of late Quaternary landscapes from isobase data and modern topography SO COMPUTERS & GEOSCIENCES LA English DT Article DE geographic information system (GIS); paleo-topographic model; isostatic rebound; late Quaternary ID LAST GLACIAL MAXIMUM; CANADIAN ARCTIC ARCHIPELAGO; INNUITIAN ICE-SHEET; NORTH-AMERICA; DEVON-ISLAND; LAKE AGASSIZ; CONSTRAINT; GREENLAND; SUPPORT; VOLUME AB Digital reconstructions of late Quaternary landscapes can be produced using a geographic information system (GIS) method that subtracts interpolated isobase values from modern elevations and bathymetry. The principal utility of the GIS method for reconstructing late Quaternary landscapes is in the relative ease and rapidity with which high-resolution, quantitative. and georeferenced databases of paleo-topography can be generated. These databases can be used for many purposes. including the generation of paleo-topographic maps, the estimation of the areas and volumes of individual water bodies and landforms, and the approximation of paleo-shoreline positions. GIS-based estimates of the dimensions of water bodies and landforms can be used to help constrain hydrological and climatic models of the late Quaternary. (C) 2002 Elsevier Science Ltd. All rights reserved. C1 Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. RP Leverington, DW (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 45 TC 33 Z9 33 U1 1 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0098-3004 J9 COMPUT GEOSCI-UK JI Comput. Geosci. PD JUN PY 2002 VL 28 IS 5 BP 631 EP 639 AR PII S0098-3004(01)00097-8 DI 10.1016/S0098-3004(01)00097-8 PG 9 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA 559EZ UT WOS:000176013800005 ER PT J AU Laurance, WF Lovejoy, TE Vasconcelos, HL Bruna, EM Didham, RK Stouffer, PC Gascon, C Bierregaard, RO Laurance, SG Sampaio, E AF Laurance, WF Lovejoy, TE Vasconcelos, HL Bruna, EM Didham, RK Stouffer, PC Gascon, C Bierregaard, RO Laurance, SG Sampaio, E TI Ecosystem decay of Amazonian forest fragments: A 22-year investigation SO CONSERVATION BIOLOGY LA English DT Review ID TROPICAL RAIN-FOREST; GREENHOUSE-GAS EMISSIONS; HABITAT FRAGMENTATION; INSECTIVOROUS BIRDS; SPECIES RICHNESS; BRAZILIAN AMAZON; TREE COMMUNITIES; EUGLOSSINE BEES; BREEDING BIRDS; CLIMATE-CHANGE AB We synthesized key findings from the Biological Dynamics of Forest Fragments Project, the world's largest and longest-running experimental study of habitat fragmentation. Although initially designed to assess the influence of fragment area on Amazonian biotas, the project has yielded insights that go far beyond the original scope of the study. Results suggest that edge effects play a key role in fragment dynamics, that the matrix has a major influence on fragment connectivity and functioning, and that many Amazonian species avoid even small (<100-m-wide) clearings. The effects of fragmentation are highly eclectic, altering species richness and abundances, species invasions, forest dynamics, the trophic structure of communities, and a variety of ecological and ecosystem processes. Moreover, forest fragmentation appears to interact synergistically with ecological changes such as hunting, fires, and logging, collectively posing an even greater threat to the rainforest biota. C1 Smithsonian Trop Res Inst, Balboa, Panama. Natl Inst Amazonian Res, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. H John Heinz III Ctr Sci Econ & Environm, Washington, DC 20004 USA. Univ Canterbury, Dept Zool, Christchurch 1, New Zealand. SE Louisiana Univ, Dept Biol Sci, Hammond, LA 70402 USA. Conservat Int, Washington, DC 20036 USA. Univ N Carolina, Dept Biol, Charlotte, NC 28223 USA. Univ New England, Dept Ecosyst Management, Armidale, NSW 2351, Australia. Univ Tubingen, Dept Zoophysiol, D-72076 Tubingen, Germany. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. RI Didham, Raphael/B-5953-2011; Laurance, William/B-2709-2012; Bruna, Emilio/H-2769-2012; Vasconcelos, Heraldo/C-3353-2013; Laurance, Susan/G-6021-2011 OI Bruna, Emilio/0000-0003-3381-8477; Vasconcelos, Heraldo/0000-0001-6969-7131; Laurance, Susan/0000-0002-2831-2933 NR 127 TC 796 Z9 881 U1 54 U2 384 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD JUN PY 2002 VL 16 IS 3 BP 605 EP 618 DI 10.1046/j.1523-1739.2002.01025.x PG 14 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 556CP UT WOS:000175832000009 ER PT J AU Pukazhenthi, B Spindler, R Wildt, D Bush, LM Howard, J AF Pukazhenthi, B Spindler, R Wildt, D Bush, LM Howard, J TI Osmotic properties of spermatozoa from felids producing different proportions of pleiomorphisms: influence of adding and removing cryoprotectant SO CRYOBIOLOGY LA English DT Article DE felid; spermatozoa; osmolality; viability; motility ID DOMESTIC CATS; ARTIFICIAL-INSEMINATION; TERATOSPERMIC DONORS; MOUSE SPERMATOZOA; BOAR SPERMATOZOA; RESOURCE BANKS; SWIM-UP; CRYOPRESERVATION; SPERM; GLYCEROL AB The spermatozoon of felids (cats) survives cryopreservation inconsistently. Using ejaculates from three species (domestic cat [normospermic versus teratospermic], the normospermic serval and the teratospermic clouded leopard), this study (1) determined the influence of adding and removing two permeating cryoprotectants (glycerol and dimethylsulfoxide) and (2) assessed the impact of one-step versus multi-step cryoprotectant removal on sperm motility and membrane integrity. Spermatozoa were exposed in a single step to various anisotonic solutions or to 1M solutions of glycerol or dimethylsulfoxide. In both cases, sperm then were returned to near isotonic conditions in a single or multi-step with de-ionized water, Ham's F10 medium or saline. Percentage of sperm motility was measured subjectively, and plasma membrane integrity was assessed using a dual fluorescent stain and flow cytometry. Sperm motility was more sensitive to anisotonic conditions than membrane integrity. Rapid dilution into various test solutions and removal of cryoprotectant with de-ionized water reduced (P < 0.01) sperm motility compared to control spermatozoa, maintained in Ham's F10. Exposing sperm from all species to a 1M solution of either cryoprotectant resulted in >85%,, spermatozoa retaining intact membranes. However, return to isotonicity with de-ionized water in a single step or multiple steps always caused severe plasma membrane disruption. In contrast, sperm motility and membrane integrity in all species and populations remained unaffected (P > 0.05) when spermatozoa were returned to isotonicity in multiple steps with Ham's F10 medium or 0.9% sodium chloride. Results demonstrate that: (1) felid spermatozoa are resistant to hypertonic stress, (2) sperm motility is more sensitive to changes in osmolality than membrane integrity; and (3) removal of cryoprotectant in multiple steps with an isotonic solution minimizes loss of sperm motility and membrane disruption in both normospermic and teratospermic males. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Pukazhenthi, B (reprint author), Smithsonian Natl Zool Pk, Dept Reprod Sci, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM pukazhenthib@nzp.si.edu FU NCRR NIH HHS [K01 RR00135] NR 54 TC 32 Z9 33 U1 1 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 EI 1090-2392 J9 CRYOBIOLOGY JI Cryobiology PD JUN PY 2002 VL 44 IS 3 BP 288 EP 300 AR PII S0011-2240(02)00035-4 DI 10.1016/S0011-2240(02)00035-4 PG 13 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 601YG UT WOS:000178476400011 PM 12237094 ER PT J AU Santos-Granero, F AF Santos-Granero, F TI Saint Christopher in the Amazon: Child sorcery, colonialism, and violence among the southern Arawak SO ETHNOHISTORY LA English DT Article; Proceedings Paper CT Annual Meeting of the American-Anthropological-Association CY DEC 02-06, 1998 CL PHILADELPHIA, PENNSYLVANIA SP Amer Anthropol Assoc AB The killing of alleged children sorcerers has been widely reported among the Arawak of eastern Peru. Accusations of child sorcery multiplied at junctures of increased outside pressures marked by violence, displacement, and epidemics. Mythical foundations for this belief are found in the legend of Saint Christopher and the Child Christ. Appropriated through mimetic image in colonial times, the tale of this "plague saint" was transformed into the myth of a cannibalistic giant and his evil infant son. The notion that children could become potent witches was reinforced in postcolonial times by epidemics affecting mostly adults. An example of mimesis gone wrong, the belief in child sorcery is one of those unforeseen and tragic products of the colonial encounter. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 94 TC 8 Z9 9 U1 0 U2 0 PU DUKE UNIV PRESS PI DURHAM PA 905 W MAIN ST, STE 18-B, DURHAM, NC 27701 USA SN 0014-1801 J9 ETHNOHISTORY JI Ethnohistory PD SUM PY 2002 VL 49 IS 3 BP 507 EP 543 DI 10.1215/00141801-49-3-507 PG 37 WC Anthropology; History SC Anthropology; History GA 598ZG UT WOS:000178307000002 ER PT J AU Marko, PB Moran, AL AF Marko, PB Moran, AL TI Correlated evolutionary divergence of egg size and a mitochondrial protein across the isthmus of panama SO EVOLUTION LA English DT Article DE effective population size; geminate species; life-history evolution; molecular clock; nearly neutral evolution ID TROPICAL AMERICAN MOLLUSKS; SITE RATE VARIATION; DNA-SEQUENCES; NONSYNONYMOUS SUBSTITUTIONS; NUCLEOTIDE SUBSTITUTION; MOLECULAR CLOCK; NEUTRAL THEORY; 2 SIDES; MODELS; BIOGEOGRAPHY AB An explicit assumption of studies that employ a mitochondrial DNA (mtDNA) molecular clock is that mtDNA evolves independently of morphology. Here we report a very strong correlation between egg size divergence and cytochrome c oxidase-1 (CO1) amino acid sequence divergence among sister species of bivalve molluscs separated by the Central American Isthmus (i.e., "geminate" species). Analyses of the molecular data reveal that CO1 sequences likely did not diverge as a function of time or evolve in response to positive natural selection. Given that an excess of CO1 amino acid polymorphism exists within species (as expected if most mutations are only slightly deleterious), a third hypothesis is that reductions in effective population size could simultaneously increase the fixation rate of nearly neutral mtDNA polymorphisms and in some way also facilitate egg size evolution. The remarkable strength of the relationship between egg size and CO1 amino acid sequence demonstrates that, even in the absence of an obvious functional relationship or clock-like evolution, the amounts of molecular and morphological change can be tightly correlated, and therefore may reflect common processes. Accordingly, the assumption that the evolutionary divergence of molecules and morphology are independent must always be carefully examined. C1 Smithsonian Trop Res Inst, Balbao, Panama. Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. RP Marko, PB (reprint author), Univ N Carolina, Dept Marine Sci, Chapel Hill, NC 27599 USA. EM pmarko@unc.edu; amoran@unc.edu RI Moran, Amy/F-7072-2011 NR 85 TC 21 Z9 21 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD JUN PY 2002 VL 56 IS 6 BP 1303 EP 1309 PG 7 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 573GL UT WOS:000176820900021 PM 12144030 ER PT J AU Park, KD Nerem, RS Davis, JL Schenewerk, MS Milne, GA Mitrovica, JX AF Park, KD Nerem, RS Davis, JL Schenewerk, MS Milne, GA Mitrovica, JX TI Investigation of glacial isostatic adjustment in the northeast US using GPS measurements SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID COMPUTING 3-DIMENSIONAL DEFORMATIONS; SEA-LEVEL CHANGE; SPECTRAL FORMALISM; SURFACE LOADS; MODEL; FIELD AB [1] We have been observing three-dimensional site velocities at over 60 permanent GPS stations in the northeastern U. S for the purpose of inferring mantle viscosity and thus improving current models of glacial isostatic adjustment (GIA). We estimate the upper and lower mantle viscosity by comparing radial site velocities from a subset of continuous GPS measurements with numerical GIA predictions. Our inferences are consistent with previous estimates obtained using different methods and data sets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Colorado, Dept Aerosp Engn Sci, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. NOAA, Natl Geodet Survey, Silver Spring, MD 20910 USA. Univ Durham, Dept Geol Sci, Durham DH1 3LE, England. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Park, KD (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 20 TC 9 Z9 9 U1 0 U2 1 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 JUN 1 PY 2002 VL 29 IS 11 AR 1509 DI 10.1029/2001GL013782 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 610MN UT WOS:000178964000051 ER PT J AU Watters, TR Schultz, RA Robinson, MS Cook, AC AF Watters, TR Schultz, RA Robinson, MS Cook, AC TI The mechanical and thermal structure of Mercury's early lithosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EFFECTIVE ELASTIC THICKNESS; LOBATE SCARPS; CONTINENTAL LITHOSPHERE; FOCAL DEPTHS; FAULTS; DEFORMATION; EARTHQUAKES; EVOLUTION; MARS; CALIFORNIA AB [1] Insight into the mechanical and thermal structure of Mercury's early lithosphere has been obtained from forward modeling of the largest lobate scarp known on the planet. Our modeling indicates the structure overlies a thrust fault that extends deep into Mercury's lithosphere. The best-fitting fault parameters are a depth of faulting of 35 to 40 km, a fault dip of 30degrees to 35degrees, and a displacement of similar to2 km. The Discovery Rupes thrust fault probably cut the entire elastic and seismogenic lithosphere when it formed (similar to4.0 Gyr ago). On Earth, the maximum depth of faulting is thermally controlled. Assuming the limiting isotherm for Mercury's crust is 300 to 600degreesC and it occurred at a depth of similar to40 km, the corresponding heat flux at the time of faulting was similar to10 to 43 mW m(-2). This is less than old terrestrial oceanic lithosphere but greater than the present heat flux on the Moon. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Nevada, Mackay Sch Mines, Dept Geol Sci, Reno, NV 89557 USA. Northwestern Univ, Dept Geol Sci, Evanston, IL 60208 USA. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RI Schultz, Richard/J-4015-2015 OI Schultz, Richard/0000-0003-3198-5263 NR 38 TC 38 Z9 38 U1 0 U2 1 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 JUN 1 PY 2002 VL 29 IS 11 AR 1542 DI 10.1029/2001GL014308 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 610MN UT WOS:000178964000018 ER PT J AU Gladman, B Holman, M Grav, T Kavelaars, J Nicholson, P Aksnes, K Petit, JM AF Gladman, B Holman, M Grav, T Kavelaars, J Nicholson, P Aksnes, K Petit, JM TI Evidence for an extended scattered disk SO ICARUS LA English DT Article DE Kuiper Belt objects; trans-neptunian objects; comets; dynamics ID KUIPER-BELT OBJECTS; RESTRICTED 3-BODY PROBLEM; TRANS-NEPTUNIAN OBJECTS; JUPITER-FAMILY COMETS; OUTER SOLAR-SYSTEM; DYNAMICAL LIFETIMES; SYMPLECTIC MAPS; CHAOTIC MOTION; PERIOD COMETS; PLANETESIMALS AB By telescopic tracking, we have established that the transneptunian object (TNO) 2000 CR(105) has a semimajor axis of 220 +/- 1 AU and perihelion distance of 44.14 +/- 0.02 AU, beyond the domain which has heretofore been associated with the "scattered disk" of Kuiper Belt objects interacting via gravitational encounters with Neptune. We have also firmly established that the TNO 1995 TL(8) has a high perihelion (of 40.08 +/- 0.02 AU). These objects, and two other recent discoveries which appear to have perihelia outside 40 AU, have probably been placed on these orbits by a gravitational interaction which is not strong gravitational scattering off of any of the giant planets on their current orbits. Their existence may thus have profound cosmogonic implications for our understanding of the formation of the outer Solar System. We discuss some viable scenarios which could have produced these objects, including long-term diffusive chaos and scattering off of other massive bodies in the outer Solar System. This discovery implies that there must be a large population of TNOs in an "extended scattered disk" with perihelia above the previously suggested 38 AU boundary. The total population is difficult to estimate due to the ease with which such objects would have been lost. This illustrates the great value of frequent and well time-sampled recovery observations of trans-neptunian objects within their discovery opposition. (C) 2002 Elsevier Science (USA). C1 Observ Cote Azur, F-06304 Nice 4, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. McMaster Univ, Dept Phys & Astron, Hamilton, ON L8K 2P4, Canada. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Observ Cote Azur, F-06304 Nice 4, France. RP Gladman, B (reprint author), Observ Cote Azur, BP 4229, F-06304 Nice 4, France. EM gladman@obs-nice.fr NR 39 TC 92 Z9 93 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JUN PY 2002 VL 157 IS 2 BP 269 EP 279 DI 10.1006/icar.2002.6860 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 568NK UT WOS:000176548300001 ER PT J AU Hacker, BC AF Hacker, BC TI War machines: Transforming technologies in the US military, 1920-1940. SO ISIS LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD JUN PY 2002 VL 93 IS 2 BP 343 EP 343 DI 10.1086/345037 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA 581FK UT WOS:000177280300078 ER PT J AU Stiner, MC Munro, ND AF Stiner, MC Munro, ND TI Approaches to prehistoric diet breadth, demography, and prey ranking systems in time and space SO JOURNAL OF ARCHAEOLOGICAL METHOD AND THEORY LA English DT Review DE zooarchaeology; diet breadth; demography; Mediterranean Basin; hunter-gatherers; Middle Paleolithic; Upper Paleolithic; Epi-Paleolithic; Natufian ID BROAD-SPECTRUM REVOLUTION; FORAGING EFFICIENCY; FOOD-PRODUCTION; CAVE ISRAEL; POPULATION; LEVANT; EXPLOITATION; ASSEMBLAGES; AURIGNACIAN; SUBSISTENCE AB Zooarchaeological data on small game use hold much potential for identifying and dating Paleolithic demographic pulses in time and space, such as those associated with modern human origins and the evolution of food-producing economies. Although small animals were important to human diets throughout the Middle, Upper, and Epi-Paleolithic periods int he Mediterranean Basin, the types of small prey emphasized by foragers shifted dramatically over the last 200,000 years. Slow-growing, slow-moving tortoises, and marine mollusks dominate the Middle Paleolithic records of small game exploitation. Later, agile, fast-maturing animals became increasingly important in human diets, first birds in the early Upper Paleolithic, and soon thereafter hares and rabbits. While the findings of this study are consistent with the main premise of Flannery's Broad Spectrum Revolution (BSR) hypothesis (Flannery, K.V. (1969). In Ucko, P.J., and Dimbleby, G.W. (eds.), The Domestication and Exploitation of Plants and Animals, Aldine Publishing Company, Chicago, pp. 73-100), its is now clear that human diet breadth began to expand much earlier than the Pleistocene/Holocene transition. Ranking small prey in terms of work of capture (in the absence of special harvesting tools) proves far more effective in this investigation of human diet breadth than taxonomy-based diversity analyses published previously. Our analyses expose a major shift in human predator-prey dynamics involving small game animals by 50-40 KYA in the Mediterranean Basin, with earliest population growth pulses occurring in the Levant. In a separate application to the Natufian period (13-10 KYA), just prior to the rise of Neolithic societies in the Levant, great intensification is apparent from small game use. This effect is most pronounced at the onset of this short culture period, and is followed by an episode of local depopulation during the Younger Dryas, without further changes in the nature of Natufian hunting adaptations. An essential feature of the diachronic and synchronic approaches outlined here is controlling the potentially conflating effects of spatial (biogeographic) and temporal variation in the faunal data sets. C1 Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA. Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Stiner, MC (reprint author), Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA. EM mstiner@u.arizona.edu NR 101 TC 98 Z9 102 U1 1 U2 21 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1072-5369 J9 J ARCHAEOL METHOD TH JI J. Archaeol. Method Theory PD JUN PY 2002 VL 9 IS 2 BP 181 EP 214 DI 10.1023/A:1016530308865 PG 34 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 586YZ UT WOS:000177614900004 ER PT J AU Dunlap, WJ Wysoczanski, R AF Dunlap, WJ Wysoczanski, R TI Thermal evidence for early Cretaceous metamorphism in the Shyok suture zone and age of the Khardung volcanic rocks, Ladakh, India SO JOURNAL OF ASIAN EARTH SCIENCES LA English DT Article DE Shyok suture; Shiguanhe suture; Bangong suture ID KARAKORAM FAULT; HIMALAYA; EVOLUTION; AUSTRALIA; COLLISION; PAKISTAN; GEOLOGY; SCALE; INDUS; ARC AB The Dras island arc (NW India) is intruded by the Ladakh Batholith and rimmed along its southern margin by the Indus suture zone, which developed ca. 50 Ma at the start of the India-Asia collision. Along its northern margin the Ladakh Batholith intrudes the Shyok Formation, a series of folded and faulted metasedimentary and metavolcanic rocks that are thought to mark an older suture of Cretaceous age. Restoration of Miocene and younger strike-slip movement of similar to150 km on the Karakoram fault suggests that the Shiquanhe suture in China was once continuous with the Shyok suture in Kohistan, but no geochronologic evidence for this connection has been demonstrated in the intervening region in Ladakh. The Khardung calc-alkaline volcanic rocks were deposited unconformably on the Shyok Formation and are thought to be of Late Cretaceous age on the basis of fossils and regional correlations, yet no reliable radiometric ages have been published. New Sensitive High Resolution Ion Microprobe (SHRIMP) U/Pb ages on single zircon grains from Khardung volcanic rocks have confirmed that a similar to7 km thick section was deposited between 67.4 and 60.5 Ma. The underlying Shyok Formation has been difficult to date due to strong thermal overprinting related to both intrusion by the ca. 102-50 Ma Ladakh granites and movement on the younger Karakoram fault. Near Digar a series of metasedimentary and metavolcanic rocks in structural and metamorphic continuity with the Shyok Formation has experienced less thermal overprinting and a muscovite from a marble unit yields a Ar-40/Ar-39 maximum age ca. 124 Ma, which indicates that greenschist facies metamorphism took place prior to this time. The geochronological evidence is consistent with an Early Cretaceous age for the Shyok Formation, but it further suggests an Early Cretaceous metamorphic and deformational event related to convergence in an oceanic arc setting between the Dras island arc and the Shiquanhe island arc. This metamorphism was followed in the Late Cretaceous by suturing of the Dras island arc to the continental rocks of the Qiangtang block in westernmost Tibet along the Bangong suture. (C) 2002 Elsevier Science Ltd. All rights reserved. C1 Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Dunlap, WJ (reprint author), Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. RI Wysoczanski, Richard/C-2930-2009; Wysoczanski, Richard/I-7730-2012 NR 21 TC 39 Z9 44 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1367-9120 J9 J ASIAN EARTH SCI JI J. Asian Earth Sci. PD JUN PY 2002 VL 20 IS 5 BP 481 EP 490 AR PII S1367-9120(01)00042-6 DI 10.1016/S1367-9120(01)00042-6 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 551QJ UT WOS:000175572300004 ER PT J AU Bodo, E Gianturco, FA Dalgarno, A AF Bodo, E Gianturco, FA Dalgarno, A TI F+D-2 reaction at ultracold temperatures SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CROSS-SECTIONS; MOLECULES; SCATTERING; SURFACE; F+H-2 AB We present a quantum mechanical study of the reaction F+D-2 at ultracold temperatures based on the potential energy surface of Stark and Werner. The reaction cross section at low energies is controlled by the tunneling through the activation barrier, a mechanism that is favored by the long duration of the collision at those energies. Differences are found in the behavior of the reactive cross section compared to that for F+H-2, due to the changed mass and zero point energy. A new feature is detected in the reaction probabilities and is attributed to a Feshbach resonance corresponding to a metastable state in the exit channel. (C) 2002 American Institute of Physics. C1 Univ Roma La Sapienza, Dept Chem, I-00185 Rome, Italy. Univ Roma La Sapienza, INFM, 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 NR 34 TC 88 Z9 89 U1 1 U2 4 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 JUN 1 PY 2002 VL 116 IS 21 BP 9222 EP 9227 DI 10.1063/1.1472515 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 550DA UT WOS:000175487300011 ER PT J AU Klos, J Chalasinski, G Krems, RV Buchachenko, AA Aquilanti, V Pirani, F Cappelletti, D AF Klos, J Chalasinski, G Krems, RV Buchachenko, AA Aquilanti, V Pirani, F Cappelletti, D TI Ab initio potentials for the S(P-3(j))-rare gas dimers: Implementation for elastic and inelastic collisions and comparison with scattering potentials SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID KINETIC-ENERGY SPECTROSCOPY; LOWEST EXCITED-STATES; FINE-STRUCTURE TRANSITIONS; OPEN-SHELL SYSTEMS; QUANTUM-MECHANICAL TREATMENT; DER-WAALS COMPLEXES; WEAK-INTERACTIONS; MOLECULAR-BEAM; INTRAMULTIPLET TRANSITIONS; TRANSPORT-PROPERTIES AB The interaction potentials between the ground state S(P-3) atom and rare gas atoms Rg (He, Ne, Ar, Kr, and Xe) in (3)Pi and (3)Sigma(-) states are calculated ab initio using an unrestricted CCSD(T) level of theory and extended correlation consistent basis sets augmented by bond functions. For NeS, the effects of extending the basis set, of a more accurate treatment of triple excitations within the coupled cluster method, and of the frozen core approximation are analyzed. The spin-orbit interaction is taken into account by the commonly used atomic model, whose validity is verified by the direct ab initio calculations of spin-orbit coupling matrix elements. The ab initio potentials are tested in the calculations of the absolute total scattering cross sections measured in molecular beams and compared with the potentials derived from the same data. This comparison, along with an analysis in terms of correlation formulas, proves the high accuracy of ab initio potentials and characterizes the sensitivity of scattering cross sections to the properties of interaction potentials. Both ab initio and scattering derived potentials are implemented in the study of inelastic fine structure transitions in S+Rg collisions. The relaxation rate constants are calculated and compared with those for O+Rg collisions. (C) 2002 American Institute of Physics. C1 Warsaw Univ, Fac Chem, PL-03093 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow MV Lomonosov State Univ, Dept Chem, Moscow 119899, Russia. Univ Perugia, Dipartimento Chim, I-06123 Perugia, Italy. Univ Perugia, Dipartimento Ingn Civile & Ambientale, I-06125 Perugia, Italy. Oakland Univ, Dept Chem, Rochester, MI 48309 USA. INFM, Unita Perugia, I-06123 Perugia, Italy. RP Klos, J (reprint author), Univ Nijmegen, NSRIM, Inst Theoret Chem, Toernooiveld 1, NL-6525 ED Nijmegen, Netherlands. RI Buchachenko, Alexei/C-8452-2012; Klos, Jacek/A-6457-2008; Cappelletti, David/C-5782-2009; Pirani, Fernando/E-8125-2014 OI Buchachenko, Alexei/0000-0003-0701-5531; Klos, Jacek/0000-0002-7407-303X; Cappelletti, David/0000-0002-9652-2457; Pirani, Fernando/0000-0003-3110-6521 NR 63 TC 15 Z9 15 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUN 1 PY 2002 VL 116 IS 21 BP 9269 EP 9280 DI 10.1063/1.1476009 PG 12 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 550DA UT WOS:000175487300018 ER PT J AU Stanley, JD AF Stanley, JD TI Andrew George Warne SO JOURNAL OF COASTAL RESEARCH LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20560 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD SUM PY 2002 VL 18 IS 3 BP 596 EP 596 PG 1 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 589JZ UT WOS:000177756400017 ER PT J AU Dalling, JW Hubbell, SP AF Dalling, JW Hubbell, SP TI Seed size, growth rate and gap microsite conditions as determinants of recruitment success for pioneer species SO JOURNAL OF ECOLOGY LA English DT Article DE gap phase regeneration; herbivory; seedling emergence; seedling establishment; trade-off ID TROPICAL RAIN-FOREST; PAPUA-NEW-GUINEA; PHASE REGENERATION; SHADE TOLERANCE; STEM-BORERS; WET FOREST; LONG-TERM; TREE; SOIL; LIGHT AB 1 We examined how seed size and seedling growth rate influence recruitment success of neotropical pioneer species. We investigated the soil seed bank, and followed seedlings from emergence and establishment to the sapling stage in artificially created gaps in secondary forest on the Barro Colorado Nature Monument, Panama. 2 To simulate microsite variation within gaps, litter addition/removal and soil disturbance treatments were applied to seedling plots in a factorial design. 3 Seedling emergence was almost three-fold higher in litter-free plots than in control plots. 4 We found a negative relationship between seed mass and seed abundance in the soil, seed mass was positively correlated with seedling emergence success from the seed bank and with seedling survival through to the end of the first dry season. 5 In the 18 months following the first dry season we observed an uncoupling of seed mass from seedling performance. Seedling mortality was now a function of maximum relative growth rate, with higher mortality of fast-growing species attributable to herbivory, notably by shoot-borers. 6 We propose that a seed size-dependent trade-off between dispersal success (selecting for large seed number), and emergence-establishment success (selecting for large seed size) can explain the maintenance of wide variation in seed size among pioneer species. Secondarily, a trade-off between growth rate and susceptibility to herbivores acting at the post-establishment phase may contribute to observed differences in light requirements among pioneer species. C1 Smithsonian Trop Res Inst, Balboa, Panama. Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. RP Dalling, JW (reprint author), Univ Illinois, Dept Plant Biol, 265 Morrill Hall,505 S Goodwin Ave, Urbana, IL 61801 USA. EM dallingj@life.uiuc.edu NR 74 TC 195 Z9 231 U1 7 U2 87 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD JUN PY 2002 VL 90 IS 3 BP 557 EP 568 DI 10.1046/j.1365-2745.2002.00695.x PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 553GG UT WOS:000175666900013 ER PT J AU Mair, RW Sen, MN Hurlimann, MD Patz, S Cory, DG Walsworth, RL AF Mair, RW Sen, MN Hurlimann, MD Patz, S Cory, DG Walsworth, RL TI The narrow pulse approximation and long length scale determination in xenon gas diffusion NMR studies of model porous media SO JOURNAL OF MAGNETIC RESONANCE LA English DT Article DE xenon; diffusion; PGSE; tortuosity; porous media ID FIELD-GRADIENT NMR; TO-VOLUME RATIO; RESTRICTED DIFFUSION; COEFFICIENT; PROBE; RELAXATION; TORTUOSITY; FLUIDS; WIDTHS; ROCKS AB We report a systematic study of xenon gas diffusion NMR in simple model porous media, random packs of mono-sized glass beads, and focus on three specific areas peculiar to gas-phase diffusion. These topics are: (i) diffusion of spins on the order of the pore dimensions during the application of the diffusion encoding gradient pulses in a PGSE experiment (breakdown of the narrow pulse approximation and imperfect background gradient cancellation), (ii) the ability to derive long length scale structural information, and (iii) effects of finite sample size. We find that the time-dependent diffusion coefficient, D(t), of the imbibed xenon gas at short diffusion times in small beads is significantly affected by the gas pressure. In particular, as expected, we find smaller deviations between measured D(t) and theoretical predictions as the gas pressure is increased, resulting from reduced diffusion during the application of the gradient pulse. The deviations are then completely removed when water D(t) is observed in the same samples. The use of gas also allows us to probe D(t) over a wide range of length scales and observe the long time asymptotic limit which is proportional to the inverse tortuosity of the sample, as well as the diffusion distance where this limit takes effect (similar to1-1.5 bead diameters). The Pade approximation can be used as a reference for expected xenon D(t) data between the short and the long time limits, allowing us to explore deviations from the expected behavior at intermediate times as a result of finite sample size effects. Finally, the application of the Pade interpolation between the long and the short time asymptotic limits yields a fitted length scale (the Pade length), which is found to be similar to0.13b for all bead packs, where b is the bead diameter. (C) 2002 Elsevier Science (USA). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Dept Nucl Engn, Cambridge, MA 02139 USA. Schlumberger Doll Res Ctr, Ridgefield, CT 06877 USA. Brigham & Womens Hosp, Dept Radiol, Boston, MA 02115 USA. RP Mair, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Patz, Samuel/I-2879-2012 FU NCRR NIH HHS [R21 RR014297-01A1, R21 RR014297-01A18280, R21 RR014297-02] NR 32 TC 55 Z9 55 U1 2 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1090-7807 J9 J MAGN RESON JI J. Magn. Reson. PD JUN PY 2002 VL 156 IS 2 BP 202 EP 212 DI 10.1006/jmre.2002.2540 PG 11 WC Biochemical Research Methods; Physics, Atomic, Molecular & Chemical; Spectroscopy SC Biochemistry & Molecular Biology; Physics; Spectroscopy GA 584RB UT WOS:000177480900006 PM 12165255 ER PT J AU Coats, DW AF Coats, DW TI Dinoflagellate life-cycle complexities SO JOURNAL OF PHYCOLOGY LA English DT Editorial Material ID PFIESTERIA-PISCICIDA; BEHAVIOR; MECHANISMS; PREY C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Coats, DW (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 32 TC 15 Z9 15 U1 1 U2 3 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD JUN PY 2002 VL 38 IS 3 BP 417 EP 419 DI 10.1046/j.1529-8817.2002.03832.x PG 3 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 563AY UT WOS:000176232300001 ER PT J AU Lesser, MP Barry, TM Banaszak, AT AF Lesser, MP Barry, TM Banaszak, AT TI Effects of UV radiation on a chlorophyte alga (Scenedesmus sp.) isolated from the fumarole fields of Mt. Erebus, Antarctica SO JOURNAL OF PHYCOLOGY LA English DT Article DE antarctica; carbon fixation; chlorophyte; photosynthesis; photosystem II; UV radiation ID ULTRAVIOLET-B RADIATION; GENE SEQUENCE DATA; MARINE DIATOM; OZONE DEPLETION; ABSORBING COMPOUNDS; VASCULAR PLANTS; AMINO-ACIDS; PHOTOSYNTHESIS; PHYTOPLANKTON; INHIBITION AB Acclimation to UV radiation (UVR) was examined in a unicellular chlorophyte isolated from fumarole fields adjacent to Mt. Erebus, Antarctica. Long-term exposure to UVR (14 days) initially reduced the efficiency of photosynthetic energy conversion measured as the dark adapted quantum yield of PSII fluorescence (F-v/F-m) when compared with cultures not exposed to UVR. However, the UVR exposed cultures recovered to pre-UVR exposure levels of photosynthetic efficiency by the end of the experimental period. Additionally, neither growth rates nor cell size were significantly affected by exposure to UVR. In contrast, the maximum rate of carbon fixation on a chl a basis was significantly reduced at the end of the experiment and was accompanied by a significant decrease in chl a concentrations. These results suggest a transient effect of UVR on primary photochemistry consistent with damage to PSII, possibly at the D1 protein, with more chronic effects on carbon fixation that did affect maximum photosynthetic capacity. Ultrastructural and molecular (18s rDNA) data show that this isolate from the fumoral fields of Mt. Erebus, Antarctica is a member of the genus Scenedesmus . C1 Univ New Hampshire, Dept Zool, Durham, NH 03824 USA. Univ New Hampshire, Ctr Marine Biol, Durham, NH 03824 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Lesser, MP (reprint author), Univ New Hampshire, Dept Zool, Durham, NH 03824 USA. NR 49 TC 21 Z9 22 U1 0 U2 4 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD JUN PY 2002 VL 38 IS 3 BP 473 EP 481 DI 10.1046/j.1529-8817.2002.t01-1-01171.x PG 9 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 563AY UT WOS:000176232300006 ER PT J AU Coats, DW Park, MG AF Coats, DW Park, MG TI Parasitism of photosynthetic dinoflagellates by three strains of Amoebophrya (Dinophyta): Parasite survival, infectivity, generation time, and host specificity SO JOURNAL OF PHYCOLOGY LA English DT Article DE Akashiwo sanguinea; Gymnodinium instriatum; Karlodinium micrum; plankton; protist; red tide ID CHESAPEAKE-BAY; GYMNODINIUM-SANGUINEUM; POPULATION-DYNAMICS; CERATIUM; REPRODUCTION; LAKES AB Amoebophrya ceratii (Koeppen) Cachon is an obligate parasite of dinoflagellates and may represent a species complex. However, little is known about the biology and host range of different strains of Amoebophrya Cachon. Here, we determined parasite generation time and dinospore infectivity, survival, and ability to infect nonprimary hosts for strains of Amoebophrya from Akashiwo sanguinea (Hirasaka) G. Hansen et Moestrup, Gymnodinium instriatum (Freudenthal et Lee) Coats comb. nov., and Karlodinium micrum (Leadbeater et Dodge) J. Larsen. Akashiwo sanguinea was readily infected, with parasite prevalence reaching 100% in dinospore:host inoculations above a 10:1 ratio. Parasitism also approached 100% in G. instriatum , but only when inoculations exceeded a 40:1 ratio. Karlodinium micrum appeared partially resistant to infection, as parasite prevalence saturated at 92%. Parasite generation time differed markedly among Amoebophrya strains. Survival and infectivity of dinospores decreased over time, with strains from G. instriatum and A. sanguinea unable to initiate infections after 2 and 5 days, respectively. By contrast, dinospores from Amoebophrya parasitizing K. micrum remained infective for up to 11 days. Akashiwo sanguinea and G. instriatum were not infected when exposed to dinospores from nonprimary Amoebophrya strains. Karlodinium micrum , however, was attacked by dinospores of Amoebophrya from the other two host species, but infections failed to reach maturity. Observed differences in host-parasite biology support the hypothesis that Amoebophrya ceratii represents a complex of host-specific species. Results also suggest that Amoebophrya strains have evolved somewhat divergent survival strategies that may encompass sexuality, heterotrophy during the "free-living" dinospore stage, and dormancy. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Coats, DW (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 31 TC 75 Z9 81 U1 1 U2 13 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD JUN PY 2002 VL 38 IS 3 BP 520 EP 528 DI 10.1046/j.1529-8817.2002.t01-1-01200.x PG 9 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 563AY UT WOS:000176232300011 ER PT J AU FitzHugh, EW AF FitzHugh, EW TI Artists' pigments, c. 1600-1835 SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Book Review C1 Smithsonian Inst, Dept Conservation & Sci Res, Washington, DC 20560 USA. RP FitzHugh, EW (reprint author), Smithsonian Inst, Dept Conservation & Sci Res, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SUM PY 2002 VL 41 IS 2 BP 187 EP 189 DI 10.2307/3179793 PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 592EP UT WOS:000177924000007 ER PT J AU Johnson, JS AF Johnson, JS TI Leather wet and dry: Current treatments in the conservation of waterlogged and desiccated archaeological leather SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Book Review C1 Smithsonian Inst, Natl Mus Am Indian, Cultural Resources Ctr, Suitland, MD 20746 USA. RP Johnson, JS (reprint author), Smithsonian Inst, Natl Mus Am Indian, Cultural Resources Ctr, Suitland, MD 20746 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SUM PY 2002 VL 41 IS 2 BP 189 EP 191 DI 10.2307/3179794 PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 592EP UT WOS:000177924000008 ER PT J AU Ubelaker, DH AF Ubelaker, DH TI The origins of native Americans: evidence from anthropological genetics. SO JOURNAL OF THE ROYAL ANTHROPOLOGICAL INSTITUTE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROYAL ANTHROPOLOGICAL INST PI LONDON PA 50 FITZROY STREET, LONDON W1P 5HS, ENGLAND SN 1359-0987 J9 J ROY ANTHROPOL INST JI J. R. Anthropol. Inst. PD JUN PY 2002 VL 8 IS 2 BP 387 EP 388 PG 2 WC Anthropology SC Anthropology GA 565PR UT WOS:000176379100025 ER PT J AU Malhi, Y Phillips, OL Lloyd, J Baker, T Wright, J Almeida, S Arroyo, L Frederiksen, T Grace, J Higuchi, N Killeen, T Laurance, WF Leano, C Lewis, S Meir, P Monteagudo, A Neill, D Vargas, PN Panfil, SN Patino, S Pitman, N Quesada, CA Rudas-Ll, A Salomao, R Saleska, S Silva, N Silveira, M Sombroek, WG Valencia, R Martinez, RV Vieira, ICG Vinceti, B AF Malhi, Y Phillips, OL Lloyd, J Baker, T Wright, J Almeida, S Arroyo, L Frederiksen, T Grace, J Higuchi, N Killeen, T Laurance, WF Leano, C Lewis, S Meir, P Monteagudo, A Neill, D Vargas, PN Panfil, SN Patino, S Pitman, N Quesada, CA Rudas-Ll, A Salomao, R Saleska, S Silva, N Silveira, M Sombroek, WG Valencia, R Martinez, RV Vieira, ICG Vinceti, B TI An international network to monitor the structure, composition and dynamics of Amazonian forests (RAINFOR) SO JOURNAL OF VEGETATION SCIENCE LA English DT Article; Proceedings Paper CT IGBP Terrestrial Transects Workshop CY JUL 12-16, 1999 CL DARWIN, AUSTRALIA DE Amazon; basal area; carbon; climate; long-term monitoring; permanent plot; soil; tropical forest ID TROPICAL FORESTS; CARBON-DIOXIDE; CO2; BALANCE AB The Amazon basin is likely to be increasingly affected by environmental changes: higher temperatures, changes in precipitation, CO2 fertilization and habitat fragmentation. To examine the important ecological and biogeochemical consequences of these changes, we are developing an international network, RAINFOR, which aims to monitor forest biomass and dynamics across Amazonia in a co-ordinated fashion in order to understand their relationship to soil and climate. The network will focus on sample plots established by independent researchers, some providing data extending back several decades. We will also conduct rapid transect studies of poorly monitored regions. Field expeditions analysed local soil and plant properties in the first phase (2001-2002). Initial results suggest that the network has the potential to reveal much information on the continental-scale relations between forest and environment. The network will also serve as a forum for discussion between researchers, with the aim of standardising sampling techniques and methodologies that will enable Amazonian forests to be monitored in a coherent manner in the coming decades. C1 Univ Edinburgh, Inst Ecol & Resource Management, Edinburgh EH9 3JU, Midlothian, Scotland. Univ Leeds, Sch Geog, Ctr Biodivers & Conservat, Leeds LS2 9JT, W Yorkshire, England. Museu Paraense Emilio Goeldi, Belem, Para, Brazil. Proyecto BOLFOR, Santa Cruz, Bolivia. Inst Nacl de Pesquisas da Amazonia, Dept Silvicultura Trop, Manaus, Amazonas, Brazil. Conservat Int, Ctr Appl Biodivers Sci, Washington, DC USA. Smithsonian Trop Res Inst, Balboa, Panama. Natl Inst Amazonian Res, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. Max Planck Inst Biogeochem, D-07701 Jena, Germany. Univ Nacl San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. Fdn Jatun Sacha, Quito, Ecuador. Missouri Bot Garden, St Louis, MO USA. Univ Georgia, Dept Bot, Athens, GA 30602 USA. Duke Univ, Ctr Trop Conservat, Durham, NC USA. Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. Harvard Univ, Cambridge, MA 02138 USA. CIFOR, Tapajos, Para, Brazil. EMBRAPA Amazonia Oriental, Belem, Para, Brazil. Univ Brasilia, Dept Ecol, Brasilia, DF, Brazil. ISRIC, Wageningen, Netherlands. Pontificia Univ Catolica Ecuador, Herbario QCA, Dept Ciencias Biol, Quito, Ecuador. Jardin Bot Missouri, Proyecto Flora Peru, Jaen, Cajamarca, Peru. Museo Noel Kempff Mercado, Santa Cruz, Bolivia. Alexander von Humboldt Inst, Bogota, DC, Colombia. Univ Fed Acre, Dept Ciencias Nat Parque Zoobot, Rio Branco, AC, Brazil. RP Malhi, Y (reprint author), Univ Edinburgh, Inst Ecol & Resource Management, Darwin Bldg,Mayfield Rd, Edinburgh EH9 3JU, Midlothian, Scotland. RI Laurance, William/B-2709-2012; Meir, Patrick/J-8344-2012; Wright, Jim/C-7881-2013; Phillips, Oliver/A-1523-2011; Silveira, Marcos/H-7906-2013; Pitman, Nigel/A-7681-2008; Lloyd, Jonathan/F-8893-2010 OI Wright, Jim/0000-0002-8842-2181; Phillips, Oliver/0000-0002-8993-6168; Silveira, Marcos/0000-0003-0485-7872; Lewis, Simon/0000-0002-8066-6851; Pitman, Nigel/0000-0002-9211-2880; Lloyd, Jonathan/0000-0002-5458-9960 NR 26 TC 139 Z9 147 U1 4 U2 33 PU OPULUS PRESS UPPSALA AB PI LANNA PA MALMEN, S-740 11 LANNA, SWEDEN SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD JUN PY 2002 VL 13 IS 3 BP 439 EP 450 DI 10.1111/j.1654-1103.2002.tb02068.x PG 12 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 601CF UT WOS:000178428000015 ER PT J AU Burger, RL Matos Mendieta, R AF Burger, RL Matos Mendieta, R TI Atalla: A center on the periphery of the Chavin horizon SO LATIN AMERICAN ANTIQUITY LA English DT Article ID PERU; HUANTAR AB The emergence of public architecture in Peru's central highlands occurred during the mid-first millennium BC and is correlated with the expansion of the Chavin sphere of interaction. Atalla, a high-altitude site in Huancavelica, represents one of the first known centers with large-scale masonry constructions. Analysis of the ceramic assemblage reveals many similarities between the local ceramics and the Janabarriu phase pottery from Chavin de Huantar, located 450 km to the north. The inhabitants of Atalla emulated the ceramic style and cut-stone masonry of the much larger northern civic-ceremonial centers, like Chavin de Huantas, while maintaining local traits such as circular dwellings and burials in or adjacent to domestic architecture. Utilizing a core-periphery perspective, the unprecedented formation in the central highlands of a community like Atalla is hypothesized to be an independent response to demands for exotic goods from the more complex societies in the north. The largest mercury deposits in Latin America are located 15 km to the west of Atalla, and the center would have been in an excellent position to procure cinnabar and distribute the bright red vermilion pigment. Production of the pigment itself would have occurred at small villages like Chuncuimarca located in the zones of the mercury deposits. C1 Yale Univ, Peabody Museum, New Haven, CT 06520 USA. Smithsonian Inst, Natl Mus Amer Indian Cultural Resource Ctr, Suitland, MD 20746 USA. RP Burger, RL (reprint author), Yale Univ, Peabody Museum, New Haven, CT 06520 USA. NR 81 TC 25 Z9 26 U1 1 U2 6 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD JUN PY 2002 VL 13 IS 2 BP 153 EP 177 DI 10.2307/971912 PG 25 WC Archaeology SC Archaeology GA 569WX UT WOS:000176626600002 ER PT J AU Reents-Budet, D AF Reents-Budet, D TI The decipherment of ancient Maya writing SO LATIN AMERICAN ANTIQUITY LA English DT Book Review C1 Smithsonian Inst, Ctr Material Res & Educ, Washington, DC 20560 USA. RP Reents-Budet, D (reprint author), Smithsonian Inst, Ctr Material Res & Educ, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD JUN PY 2002 VL 13 IS 2 BP 241 EP 242 DI 10.2307/971919 PG 2 WC Archaeology SC Archaeology GA 569WX UT WOS:000176626600009 ER PT J AU Schroll, S AF Schroll, S TI Ben Schonzeit paintings. SO LIBRARY JOURNAL 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 BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2002 VL 127 IS 10 BP 144 EP 144 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 559DT UT WOS:000176010400058 ER PT J AU Duda, TF Vanhoye, D Nicolas, P AF Duda, TF Vanhoye, D Nicolas, P TI Roles of diversifying selection and coordinated evolution in the evolution of amphibian antimicrobial peptides SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE antimicrobial peptides; gene family; diversifying selection; coordinated evolution ID DERMASEPTIN-FAMILY; MOLECULAR-CLONING; RANA-RUGOSA; FROG-SKIN; INNATE IMMUNITY; PRECURSORS; ANTIBIOTICS; CATESBEIANA; VERTEBRATES; LIKELIHOOD AB Antimicrobial peptides are expressed in the skin of amphibian,, and are used to prevent infection by microorganisms. Frog species store distinct collections of antimicrobial peptides that show variation in size. charge. conformation, and bactericidal activity, and so the evolution of antimicrobial peptide gene families may reflect the adaptive diversification of these loci. We examined the molecular evolution of antimicrobial peptide transcripts front hylid and ranid frog species. Our results show that after the gene family arose in file common ancestor of the Hylidae and Ranidae, before the divergence of these families in the Mesozoic. it Subsequently diversified within these groups, with numerous duplication events and divergence of loci. Moreover, we provide evidence that suggests that member.,, of the antimicrobial peptide gene family have been subject to diversifying, selection, within both propiece and mature domains of hylids and solely within the mature domain of ranids, Finally, our results suggest that coordinated and compensatory amino acid replacements hake occurred within the acidic propiece and cationic mature domain of hylid antimicrobial peptide precursors. as has been observed for mammalian defensin genes, but not among those of ranid precursors. C1 Smithsonian Trop Res Inst, Naos Marine Lab, Balboa, Ancon, Panama. Inst Jacques Monod, Lab Bioactivat Peptides, Paris, France. RP Duda, TF (reprint author), Smithsonian Trop Res Inst, Naos Marine Lab, Apartado 2072, Balboa, Ancon, Panama. RI Nicolas, Pierre/C-7908-2009 NR 37 TC 110 Z9 115 U1 0 U2 14 PU SOC MOLECULAR BIOLOGY EVOLUTION PI LAWRENCE PA PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD JUN PY 2002 VL 19 IS 6 BP 858 EP 864 PG 7 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 562RA UT WOS:000176211700008 PM 12032242 ER PT J AU Axner, E Pukazhenthi, BS Wildt, DE Linde-Forsberg, C Spindler, RE AF Axner, E Pukazhenthi, BS Wildt, DE Linde-Forsberg, C Spindler, RE TI Creatine phosphokinase in domestic cat epididymal spermatozoa SO MOLECULAR REPRODUCTION AND DEVELOPMENT LA English DT Article DE creatine phosphokinase immunostaining; epididymal spermatozoa; sperm maturation; sperm morphology ID SWIM-UP; SPERM; MORPHOLOGY; EJACULATE; FERTILIZATION; CAPACITATION; TRANSPORT; MOTILITY; DUCT AB Mammalian spermatozoa that have not completed final testicular sperm maturation have residual cytoplasm and increased creatine phosphokinase (CK) content. This study determined: (1) if CK could be detected by immunostaining cat spermatozoa from the caput, corpus, and cauda epididymis, (2) fluctuations in the proportions of spermatozoa with mature or immature CK-staining patterns during epididymal sperm transit, and (3) how well sperm maturity (as determined by a CK marker) correlated with testicular or epididymal dysfunctions associated with morphological sperm abnormalities. One epididymis was collected from each of 37 cats after orchiectomy and processed immediately to allow sperm morphology evaluations on a 'regional' basis. Sperm released from the contralateral epididymis were evaluated for motility, sperm membrane integrity, and immunostaining with CK-B antibodies. Proportions of spermatozoa with malformed or detached heads, proximal droplets and acrosomal or midpiece abnormalities decreased (P < 0.05) from the caput to the cauda epididymis. In contrast, proportions of spermatozoa that were motile, membrane-intact or with flagellar abnormalities or distal droplets increased (P < 0.05) from the caput to cauda region. Percentages of spermatozoa with an immature CK-staining pattern also decreased (P<0.05) with epididymal transit (which differs from that reported for the human and stallion). There was no correlation (P > 0.05) between sperm morphology and the CK-staining patterns. In summary, the results reveal that some specific sperm malformations in the domestic cat are of testicular origin, whereas others develop during epididymal transit. (C) 2002 Wiley-Liss, Inc. C1 Swedish Univ Agr Sci, Ctr Reprod Biol Uppsala, Fac Med Vet, Dept Obstet & Gynaecol, SE-75007 Uppsala, Sweden. Natl Zool Pk, Conservat & Res Ctr, Smithsonian Inst, Front Royal, VA USA. RP Axner, E (reprint author), Swedish Univ Agr Sci, Ctr Reprod Biol Uppsala, Fac Med Vet, Dept Obstet & Gynaecol, Box 7039, SE-75007 Uppsala, Sweden. FU NCRR NIH HHS [K01 RR00135] NR 31 TC 12 Z9 13 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1040-452X EI 1098-2795 J9 MOL REPROD DEV JI Mol. Reprod. Dev. PD JUN PY 2002 VL 62 IS 2 BP 265 EP 270 DI 10.1002/mrd.10070 PG 6 WC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology SC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology GA 548RN UT WOS:000175403300014 PM 11984837 ER PT J AU Mackey, J White, M Kamionkowski, M AF Mackey, J White, M Kamionkowski, M TI Theoretical estimates of intrinsic galaxy alignment SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; cosmology : theory; large-scale structure of Universe ID LARGE-SCALE STRUCTURE; ANGULAR-MOMENTUM; POWER SPECTRA; COSMIC SHEAR; STATISTICS; PROTOGALAXIES; ELLIPTICITIES; POLARIZATION AB It has recently been argued that the observed ellipticities of galaxies may be determined at least in part by the primordial tidal gravitational field in which the galaxy formed. Long-range correlations in the tidal field could thus lead to an ellipticity-ellipticity correlation for widely separated galaxies. We present a new model relating ellipticity to angular momentum, which can be calculated in linear theory. We use this model to calculate the angular power spectrum of intrinsic galaxy shape correlations. We show that, for low-redshift galaxy surveys, our model predicts that intrinsic correlations will dominate correlations induced by weak lensing, in good agreement with previous theoretical work and observations. We find that our model produces 'E -mode' correlations enhanced by a factor of 3.5 over B -modes on small scales, making it harder to disentangle intrinsic correlations from those induced by weak gravitational lensing. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Mackey, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 NR 41 TC 56 Z9 56 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2002 VL 332 IS 4 BP 788 EP 798 DI 10.1046/j.1365-8711.2002.05337.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 557KQ UT WOS:000175908100006 ER PT J AU Hart, AG Bot, ANM Brown, MJF AF Hart, AG Bot, ANM Brown, MJF TI A colony-level response to disease control in a leaf-cutting ant SO NATURWISSENSCHAFTEN LA English DT Article ID SOCIAL INSECT; TERMITE AB Parasites and pathogens often impose significant costs on their hosts. This is particularly true for social organisms, where the genetic structure of groups and the accumulation of contaminated waste facilitate disease transmission. In response, hosts have evolved many mechanisms of defence against parasites. Here we present evidence that Atta colombica, a leaf-cutting ant, may combat Escovopsis, a dangerous parasite of Atta's garden fungus, through a colony-level behavioural response. In A. colombica, garden waste is removed from within the colony and transported to the midden - an external waste dump - where it is processed by a group of midden workers. We found that colonies infected with Escovopsis have higher numbers of workers on the midden, where Escovopsis is deposited. Further, midden workers are highly effective in dispersing newly deposited waste away from the dumping site. Thus, the colony-level task allocation strategies of the Atta superorganism may change in response to the threat of disease to a third, essential party. C1 Smithsonian Trop Res Inst, Panama City, Panama. Univ Aarhus, Dept Genet & Ecol, DK-8000 Aarhus, Denmark. Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. Univ Dublin Trinity Coll, Dept Zool, Dublin 2, Ireland. RP Brown, MJF (reprint author), Swiss Fed Inst Technol, Zurich, Switzerland. RI Brown, Mark/E-7644-2010 NR 14 TC 23 Z9 23 U1 0 U2 12 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD JUN PY 2002 VL 89 IS 6 BP 275 EP 277 DI 10.1007/s00114-002-0316-0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 571ZA UT WOS:000176748000007 PM 12146794 ER PT J AU Rasmussen, HN Whigham, DF AF Rasmussen, HN Whigham, DF TI Phenology of roots and mycorrhiza in orchid species differing in phototrophic strategy SO NEW PHYTOLOGIST LA English DT Article DE corallorhiza; galearis; goodyera; heterotrophy; liparis; terrestrial; orchids; mycotrophy; Orchidaceae; Tipularia ID GOODYERA-REPENS; PLANTS AB The mycorrhiza of orchids represents an energy source that may replace or supplement photosynthesis. Dependency on mycotrophy in adult life stages would thus be expected to be inversely related to the prevalence of phototrophic structures. The phenology of underground parts and mycorrhizal infection were monitored in five terrestrial species differing in leaf phenology (and thus in phototrophic strategy): Goodyera pubescens (evergreen), Tipularia discolor (wintergreen), Galearis spectabilis and Liparis lilifolia (summergreen) and Corallorhiza odontorhiza (chlorophyll deficient), growing sympatrically in a North American deciduous forest. Mycorrhizal infection was extensive in T. discolor roots and C. odontorhiza rhizomes. Only the proximal part of roots was infected in G. pubescens, and mycorrhizal colonisation was patchy in roots and tubers of G, spectabilis and localized in the rhizome in L. lilifolia. Mycotrophic roots were long-lived (1.5-3 yrs) determinate structures and mycorrhizal infection reached maximum intensity 2-6 months after development. Mycotrophy appeared to be active all year round in mature organs. The phenology of mycotrophic roots and patterns of mycorrhizal infection were not related to the leafy season. The hypothesis that phototrophic and mycotrophic nutrition alternate through the seasons could not be confirmed. (C) New Phytologist (2002) 154: 797-807. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Rasmussen, HN (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Rasmussen, Hanne/P-5485-2014; OI Rasmussen, Hanne/0000-0002-0181-9304; Whigham, Dennis/0000-0003-1488-820X NR 29 TC 30 Z9 35 U1 4 U2 27 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0028-646X J9 NEW PHYTOL JI New Phytol. PD JUN PY 2002 VL 154 IS 3 BP 797 EP 807 DI 10.1046/j.1469-8137.2002.00422.x PG 11 WC Plant Sciences SC Plant Sciences GA 555GP UT WOS:000175786600023 ER PT J AU Pawson, DL AF Pawson, DL TI A new species of bathyal elasipod sea cucumber from New Zealand (Echinodermata : Holothuroidea) SO NEW ZEALAND JOURNAL OF MARINE AND FRESHWATER RESEARCH LA English DT Article DE Holothuroidea; New Zealand; new species; Orphnurgus dorisae; key to Orphnurgus; lecithotrophy AB Orphnurgus dorisae new species is described from bathyal depths to the north of New Zealand, near the Kermadec Islands. It is distinctive in possessing spatulate rods and spinous rods dorsally, and spinous rods and perforated plates ventrally. A key to Orphnurgus species is provided. Egg size suggests that this species, and other Orphnurgus species, may have planktonic lecithotrophic embryos. C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Pawson, DL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. NR 13 TC 1 Z9 1 U1 1 U2 2 PU SIR PUBLISHING PI WELLINGTON PA PO BOX 399, WELLINGTON, NEW ZEALAND SN 0028-8330 J9 NEW ZEAL J MAR FRESH JI N. Z. J. Mar. Freshw. Res. PD JUN PY 2002 VL 36 IS 2 BP 333 EP 338 PG 6 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA 577EV UT WOS:000177049300008 ER PT J AU Clark, JL Skog, LE AF Clark, JL Skog, LE TI Novae Gesneriaceae neotropicarum VIII: Alloplectus grandicalyx, a new species from Colombia and Ecuador SO NOVON LA English DT Article DE Alloplectus; Colombia; Ecuador; Gesneriaceae AB A new species, Alloplectus grandica-lyx J. L. Clark & L. E. Skog, is described from northern Ecuador and Southern Colombia. Alloplectus grandicalyx is differentiated from other similar species on the basis of larger calyx lobes, longer pedicels, and villous pubescence on the stems, leaves, petioles, and calyx lobes. A key is provided to help distinguish A. grandicalyx from other shrubby and resupinate flowered Alloplectus species. In addition, the commonly confused and widely spread Alloplectus tetragonoides Mansfeld is discussed and neotypified. C1 George Washington Univ, Washington, DC 20052 USA. Natl Museum Nat Hist, Smithsonian Inst, Bot Sect Systemat Biol, Washington, DC 20013 USA. RP Clark, JL (reprint author), George Washington Univ, 2023 G St NW, Washington, DC 20052 USA. NR 5 TC 1 Z9 1 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SUM PY 2002 VL 12 IS 2 BP 173 EP 178 DI 10.2307/3392952 PG 6 WC Plant Sciences SC Plant Sciences GA 571YX UT WOS:000176747700005 ER PT J AU Skog, LE Kvist, LP AF Skog, LE Kvist, LP TI Novae Gesneriaceae neotropicarum IX: Cremospermopsis, a new genus from Colombia SO NOVON LA English DT Article DE Colombia; Cremosperma; Cremospermopsis; Gesneriaceae AB A new genus in the Gesneriaceae, Cremospermopsis L. E. Skog & L. P Kvist, is described from the very humid forests in the Colombian departments of Antioquia and adjacent Bolivar. The new genus of two species, C. cestroides and C. parviflora, is similar and may be related to Cremosperma, but differs in having inflorescence bracts, unequal calyx lobes, and spherical papillate seeds. C1 Smithsonian Inst, US Natl Herbarium, MRC 166, Washington, DC 20013 USA. Royal Vet & Agr Univ, Unit Forestry, DK-1871 Frederiksberg C, Denmark. RP Skog, LE (reprint author), Smithsonian Inst, US Natl Herbarium, MRC 166, POB 37012, Washington, DC 20013 USA. NR 4 TC 1 Z9 3 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SUM PY 2002 VL 12 IS 2 BP 262 EP 269 DI 10.2307/3392965 PG 8 WC Plant Sciences SC Plant Sciences GA 571YX UT WOS:000176747700018 ER PT J AU Jennions, MD Telford, SR AF Jennions, MD Telford, SR TI Life-history phenotypes in populations of Brachyrhaphis episcopi (Poeciliidae) with different predator communities SO OECOLOGIA LA English DT Article DE guppy; life-history variation; offspring size; Poecilia reticulata; population differences ID SIZE-SELECTIVE PREDATION; REPRODUCTIVE EFFORT; OPTIMAL ALLOCATION; OFFSPRING SIZE; EVOLUTION; AGE; GUPPIES; NUMBER; RETICULATA; MORTALITY AB Variation among populations in extrinsic mortality schedules selects for different patterns of investment in key life-history traits. We compared life-history phenotypes among 12 populations of the live-bearing fish Brachyrhaphis episcopi. Five populations co-occurred with predatory fish large enough to prey upon adults, while the other seven populations lacked these predators. At sites with large predatory fish, both sexes reached maturity at a smaller size. Females of small to average length that co-occurred with predators had higher fecundity and greater reproductive allotment than those from populations that lacked predators, but the fecundity and reproductive allotment of females one standard deviation larger than mean body length did not differ among sites. In populations with large predatory fish, offspring mass was significantly reduced. In each population, fecundity, offspring size and reproductive allotment increased with female body size. When controlling for maternal size, offspring mass and number were significantly negatively correlated, indicating a phenotypic trade-off. This trade-off was non-linear, however, because reproductive allotment still increased with brood size after controlling for maternal size. Similar differences in life-history phenotypes among populations with and without large aquatic predators have been reported for Brachyrhaphis rhabdophora in Costa Rica and Poecilia reticulata (a guppy) in Trinidad. This may represent a convergent adaptation in life-history strategies attributable to predator-mediated effects or environmental correlates of predator presence. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. RP Jennions, MD (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 58 TC 56 Z9 57 U1 2 U2 24 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUN PY 2002 VL 132 IS 1 BP 44 EP 50 DI 10.1007/s00442-002-0942-4 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 572JR UT WOS:000176771300005 ER PT J AU Osterman, LE Buzas, MA Hayek, LAC AF Osterman, LE Buzas, MA Hayek, LAC TI SHE analysis for biozonation of benthic foraminiferal assemblages from Western Arctic Ocean SO PALAIOS LA English DT Article AB Benthic foraminiferal species abundance in samples from three Mendeleyev Ridge box cores were analyzed by cluster analysis and the newer method of SHE analysis. Previously, the latter technique only has been used on foraminiferal data from depth transacts of modern surface sediment samples. Unlike most methods, which initially compare all possible pairs of samples, the SHE procedure results in a linear pattern if a sequence of samples are from the same statistical distribution. A change in slope indicates a statistical change in community structure and/or a change in species composition. The research reported herein is the first application of SHE for the purpose of identifying biozones in sediment core samples for the purpose of stratigraphic correlation. Both cluster analysis and the SHE method provided zonation within cores. However, the cluster method often produced clusters that were difficult to identify and also contained a mixture of samples without stratigraphic continuity. In contrast, SHE resulted in easily identifiable biozones and ensured temporal continuity within them. In general, the cluster analysis produced more zones than the SHE analysis. About 87% of the cluster zones and 64% of the SHE zones were correlated across more than one core. The average age range for correlated biozone boundaries among the three cores, based on radiocarbon dates, was 821 years using cluster analysis and 296 years using SHE. The sequential nature of the analysis, ease in choosing boundaries, and correlation of these boundaries across cores makes SHE the preferred technique. C1 US Geol Survey, Reston, VA 20192 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Osterman, LE (reprint author), US Geol Survey, MS 926A, Reston, VA 20192 USA. NR 12 TC 9 Z9 10 U1 1 U2 3 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD JUN PY 2002 VL 17 IS 3 BP 297 EP 303 DI 10.1669/0883-1351(2002)017<0297:SAFBOB>2.0.CO;2 PG 7 WC Geology; Paleontology SC Geology; Paleontology GA 576FG UT WOS:000176991700009 ER PT J AU Vrinceanu, D Sadeghpour, HR AF Vrinceanu, D Sadeghpour, HR TI He(1 S-1)-He(2 S-3) collision and radiative transition at low temperatures SO PHYSICAL REVIEW A LA English DT Article ID POTENTIAL-ENERGY CURVES; FINE-STRUCTURE; METASTABLE HELIUM; TRIPLET-STATES; HE-4 CLUSTERS; LIQUID-HELIUM; IONIZATION; SPECTROSCOPY; SCATTERING; ATOMS AB There has been considerable recent interest in low-temperature interrogation of quantum helium nanodroplets. We consider the interaction of helium ground and metastable states, employing the best known molecular dimer potentials. Radiative transitions between different metastable rovibrational levels are compared with the discharge emission transition lines and good agreement is found. Collisional interactions between helium ground and metastable atoms are studied and elastic scattering, metastability excitation transfer and diffusion cross sections and rate coefficients are calculated at ultralow energies. The integral elastic cross section at ultralow energies is about 5000 Angstrom(2). Effect of shape resonances that form in the potential barriers, on the cross sections is investigated. We find that some shape resonances live for longer than 100 s. Long-range potential wells could support "shelf" levels. We discuss their collisional and spectroscopic properties. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Vrinceanu, D (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 53 TC 6 Z9 6 U1 1 U2 6 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 JUN PY 2002 VL 65 IS 6 AR 062712 DI 10.1103/PhysRevA.65.062712 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 572FT UT WOS:000176763600065 ER PT J AU Svenning, JC Skov, F AF Svenning, JC Skov, F TI Mesoscale distribution of understorey plants in temperate forest (Kalo, Denmark): the importance of environment and dispersal SO PLANT ECOLOGY LA English DT Article DE dispersal limitation; dispersal mode; edaphic conditions; field layer vegetation; overstorey effects; spatial autocorrelation ID TROPICAL RAIN-FORESTS; RECRUITMENT LIMITATION; SPATIAL PATTERNS; SEED DISPERSAL; ANCIENT WOODLAND; SPECIES RICHNESS; MANAGED FOREST; CORAL-REEFS; HISTORY; MIGRATION AB We studied the influence of environmental heterogeneity and dispersal processes on mesoscale distribution patterns of understorey plants in a 330 ha ancient, managed temperate forest area. Similarity matrix regression analysis showed that overall species similarity was affected by site (the two disjunct halves of the forest area), spatial autocorrelation at the 100 m scale, edaphic conditions, stand type and stand structure, and the occurrence of open areas, but not by stand age or topography. Using autologistic regression we analysed the influence of clumping, site, edaphic conditions, stand composition, open areas, and stand structure on the individual distribution patterns of the 60 most abundant species. Only five species had distributions that were not significantly related to any of the explanatory variables. A large number of species showed significant, and often differing, relationships to at least one of the environmental parameters. At least 20 species exhibited clumping at the 100 m scale that was independent of the environmental parameters. Principal coordinate analysis and an analysis using the Ellenberg ecological indicator values suggested that no important gradients had been overlooked. Dispersal ability (estimated from dispersal mode) and clumping independent of environmental heterogeneity were related. Poor dispersers exhibited stronger clumping at the 100 m scale than good dispersers. Our results support the joint importance of environmental heterogeneity and dispersal processes in shaping the mesoscale distribution patterns of forest herbs. We conclude that the distribution of plant species, and species coexistence and species composition in plant communities, cannot be explained without simultaneously considering environmental heterogeneity and dispersal. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Natl Environm Res Inst, Dept Landscape Ecol, DK-8410 Ronde, Denmark. RP Svenning, JC (reprint author), Univ Aarhus, Dept Systemat Bot, Nordlandsvej 68, DK-8410 Risskov, Denmark. RI Svenning, Jens-Christian/C-8977-2012; Skov, Flemming/I-2665-2013 OI Svenning, Jens-Christian/0000-0002-3415-0862; Skov, Flemming/0000-0002-9490-8663 NR 75 TC 48 Z9 50 U1 0 U2 18 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD JUN PY 2002 VL 160 IS 2 BP 169 EP 185 DI 10.1023/A:1015885321263 PG 17 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 562YJ UT WOS:000176226300004 ER PT J AU Gardner, JB Henry, SM AF Gardner, JB Henry, SM TI September-11 and the mourning after: Reflections on collecting and interpreting the history of tragedy SO PUBLIC HISTORIAN LA English DT Article C1 Smithsonian Inst, NMAH, Washington, DC 20560 USA. Mus City NY, New York, NY USA. RP Gardner, JB (reprint author), Smithsonian Inst, NMAH, Washington, DC 20560 USA. NR 4 TC 7 Z9 7 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 SUM PY 2002 VL 24 IS 3 BP 37 EP 52 DI 10.1525/tph.2002.24.3.37 PG 16 WC History SC History GA 613UM UT WOS:000179149900004 PM 14558577 ER PT J AU Rogers, J AF Rogers, J TI The fireproof building: Technology and public safety in the nineteenth-century American city SO PUBLIC HISTORIAN LA English DT Book Review C1 Smithsonian Inst, Natl Mus Amer Hist, Washington, DC USA. RP Rogers, J (reprint author), Smithsonian Inst, Natl Mus Amer Hist, 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 SUM PY 2002 VL 24 IS 3 BP 83 EP 85 PG 3 WC History SC History GA 613UM UT WOS:000179149900024 ER PT J AU Sokoloski, JL Bildsten, L Chornock, R Filippenko, AV AF Sokoloski, JL Bildsten, L Chornock, R Filippenko, AV TI Four new delta Scuti pulsators from a variability survey of 131 stars SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GRAVITATIONAL LENSING EXPERIMENT; PERIODIC VARIABLE-STARS; BAADES WINDOW FIELDS; GALACTIC BULGE; CATALOG; LUMINOSITY; MODELS; SEARCH; GAIA AB In a photometric variability survey of 131 stars with B less than or similar to 14 mag, we have found four new delta Scuti stars. We were sensitive to oscillation amplitudes as low as a few millimagnitudes (mmag). The detection rate of short-period (P < 0.1 days) pulsating variable stars, which may be relevant for planned large-variability surveys such as the Global Astrometric Interferometer for Astrophysics, the Panoramic Optical Imager, and even the Large-Aperture Synoptic Survey Telescope, was therefore 3%. All four new variable stars have low pulsation amplitude (tens of mmag), and one has a very short period (0.0198 days). This star is one of the fastest known d Scuti pulsators. The short period of this variable star makes it observationally tractable, and it may therefore be a particularly good candidate for asteroseismological studies. All four new variable stars will add to the cadre of low-amplitude and relatively short period δ Scuti stars that are potentially useful for learning about the structure of stars on or near the main sequence, slightly more massive than the Sun. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Santa Barbara, Inst Theoret Phys, Santa Barbara, CA 93106 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Sokoloski, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 3 Z9 3 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 JUN PY 2002 VL 114 IS 796 BP 636 EP 644 DI 10.1086/341689 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551ZJ UT WOS:000175593600007 ER PT J AU Hueber, FM Galtier, J AF Hueber, FM Galtier, J TI Symplocopteris wyattii n. gen. et n. sp.: a zygopterid fern with a false trunk from the Tournaisian (Lower Carboniferous) of Queensland, Australia SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY LA English DT Article DE early fern; false trunk; Lower Carboniferous; Australia ID ARTHROPOD AB Fossil remains of a fern were collected from the basalmost Carboniferous Tournaisian, Hardwick Formation of Queensland, Australia. The fern is described as an erect false trunk composed of intertwined branch systems and phyllophores embedded in a mesh of adventitious roots. The base of the trunk attained up to 50 cm in diameter and was composed almost totally of roots. Branching of the stems is isotomous. Each subsequent branch gives rise to a phyllophore and a geotropic adventitious root. Smaller roots arise from the bases of the phyllophores, as well as the larger roots, and all are covered with hairs and are directed horizontally. The two forms of roots are functionally complementary, the larger for support and absorption of water from the soil, the smaller for absorption in the humidity within the trunk. The repetitive branching of the stems concomitant with the increase of phyllophores and the two forms of adventitious roots comprised the oldest tree fern with false trunk known to this time. The phyllophores have no apparent phyllotaxy and many are abortive before reaching the exterior of the trunk. The cauline xylem strand, in transverse section, is a solid centrarch protostele while the phyllophore traces are simple and clepsydroid in outline. Xylem strands in the roots have four, rarely three or five, exarch protoxylem points. The combination of the very primitive anatomy with the arborescent habit is unique and the name Symplocopteris wyattii n. gen. et n. sp. is proposed. This plant is the oldest known zygopterid fern showing the clear anatomical and morphological distinction between stems, leaves and roots. (C) 2002 Elsevier Science B.V. All rights reserved. C1 CIRAD, Lab Bot & Bioinformat Plantes, F-34398 Montpellier 05, France. Smithsonian Inst, Dept Paleobiol MRC121, Washington, DC 20560 USA. RP Galtier, J (reprint author), CIRAD, Lab Bot & Bioinformat Plantes, TA40-PS2,Blvd Lironde, F-34398 Montpellier 05, France. NR 46 TC 19 Z9 20 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0034-6667 J9 REV PALAEOBOT PALYNO JI Rev. Palaeobot. Palynology PD JUN PY 2002 VL 119 IS 3-4 BP 241 EP 273 AR PII S0034-6667(01)00100-2 DI 10.1016/S0034-6667(01)00100-2 PG 33 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA 587CD UT WOS:000177622200004 ER PT J AU Eberhard, WG AF Eberhard, WG TI The function of female resistance behavior: Intromission by male coercion vs. female cooperation in sepsid flies (Diptera : Sepsidae) SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE sexual selection; cryptic female choice; male-female conflict; Sepsidae ID DROSOPHILA-MELANOGASTER FEMALES; SEXUAL SELECTION; WATER STRIDER; FORCED COPULATION; MATING SUCCESS; SEAWEED FLY; HIND LEGS; CONFLICT; COURTSHIP; MATE AB Female resistance behavior that occurs prior to intromission does not by itself imply forced copulation. Such behavior may function instead as a test of the male in order to favor some males over others, or to induce the male to desist. Thus, male persistence and forcefulness may sometimes be better described as persuasion rather than coercion. Under the persuasion hypothesis, the male only gains intromission due to an active response of the female. Under the coercion hypothesis, male and female are opposed in a physical battle which the female loses if copulation occurs. In species in which males are morphologically incapable of forcing intromission without active female cooperation (I argue here that this is probably a very common situation), data on the behavioral and ecological context in which resistance occurs can distinguish between the two possibilities. Partially congruent functions of resistance, seen from the female point of view, are female resistance to screen (male persuasion), and female resistance to avoid males non-selectively (male coercion). Sepsid flies illustrate these ideas. Females often struggle energetically in apparent attempts to dislodge mounted males and to prevent intromission, and males grasp females with powerful species-specific structures on their front legs and genitalia. This suggests the possibility of coerced intromission. But behavioral and morphological evidence demonstrate that active female cooperation occurs at the moment of intromission, and that males are probably dependent on this cooperation because they are not morphologically equipped to force their genitalia into those of an uncooperative female. Despite the impression from previous publications, male insects in general may seldom be able to achieve intromission by genitalic force. The species-specific forms of the grasping genitalia of male sepsids are probably not the result of an evolutionary arms race between coercive males and unselectively resistant females. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. NR 90 TC 61 Z9 62 U1 1 U2 16 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD JUN PY 2002 VL 50 IS 2 BP 485 EP 505 PG 21 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 583AY UT WOS:000177384400009 PM 12298280 ER PT J AU Davis, DR Landry, B Roque-Albelo, L AF Davis, DR Landry, B Roque-Albelo, L TI Two new Neotropical species of Bucculatrix leaf miners (Lepidoptera : Bucculatricidae) reared from Cordia (Boraginaceae) SO REVUE SUISSE DE ZOOLOGIE LA English DT Article DE larva; leaf mining; hypermetamorphosis; pupa; Belize; Mexico; Galapagos Islands AB Two new species of Bucculatrix, each initially mining and later externally skeletonizing the leaves of two different Neotropical species of Cordia (Boraginaceae), are described and illustrated. Bucculatrix caribbea Davis & Landry, sp. n. was reared from the leaves of Cordia sebestena L. on Glovers Reef, Belize and Cozumel, Mexico. The biology of this species is briefly summarized and all primary stages, except that of the egg, are illustrated. The adult of Bucculatrix cordiaella Davis & Landry, sp. n. is described from six islands of the Galapagos archipelago. This represents the first record for Bucculatricidae from the Galapagos. The larva feeds on the leaves of Cordia lutea Lam. Both species are morphologically allied to Bucculatrix ilecella Busck, a leaf miner on Ilex sp. from southern Texas, USA. C1 Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. Museum Hist Nat, CH-1211 Geneva 6, Switzerland. Charles Darwin Res Stn, Quito, Ecuador. RP Davis, DR (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, NHB 169, Washington, DC 20560 USA. NR 13 TC 4 Z9 5 U1 0 U2 1 PU MUSEUM HISTOIRE NATURELLE PI GENEVA 6 PA CASE POSTALE 6434, ATTN:DENISE MAIER ADMN REV SUISSE DE ZOOLOGIE, CH-L211 GENEVA 6, SWITZERLAND SN 0035-418X J9 REV SUISSE ZOOL JI Rev. Suisse Zool. PD JUN PY 2002 VL 109 IS 2 BP 277 EP 294 PG 18 WC Zoology SC Zoology GA 573HJ UT WOS:000176823100004 ER PT J AU Pasachoff, JM Babcock, BA Russell, KD Seaton, DB AF Pasachoff, JM Babcock, BA Russell, KD Seaton, DB TI Short-period waves that heat the corona detected at the 1999 eclipse SO SOLAR PHYSICS LA English DT Article ID REGION TRANSIENT BRIGHTENINGS; HIGH-FREQUENCY OSCILLATIONS; TOTAL SOLAR ECLIPSE; LOOPS AB As a part of a study of the cause of solar coronal heating, we searched for high-frequency (similar to1 Hz) intensity oscillations in coronal loops in the [Fe XIV] coronal green line. We summarize results from observations made at the 11 August 1999 total solar eclipse from Ramnicu-Valcea, Romania, through clear skies. We discuss the image reduction and analysis through two simultaneous series of coronal CCD images digitized at 10 Hz for a total time of about 140 s. One series of images was taken through a 3.6 Angstrom filter isolating the 5303 Angstrom [Fe XIV] coronal green line and the other through a 100 Angstrom filter in the nearby K-corona continuum. Previous observations, described in Pasachoff et al. (2000), showed no evidence for oscillations in the [Fe XIV] green line at a level greater than 2% of coronal intensity. We describe several improvements made over the 1998 eclipse that led to increased image clarity and sensitivity. The corona was brighter in 1999 with the solar maximum, further improving the data. We use Fourier analysis to search in the [Fe XIV] channel for intensity oscillations in loops at the base of the corona. Such oscillations in the 1-Hz range are predicted as a result of density fluctuations from the resonant absorption of MHD waves. The dissipation of a significant amount of mechanical energy from the photosphere into the corona through this mechanism could provide sufficient energy to heat the corona. A Monte Carlo model of the data suggests the presence of enhanced power, particularly in the 0.75-1.0 Hz range, and we conclude that MHD waves remain a viable method for coronal heating. C1 Williams Coll, Hopkins Observ, Williamstown, MA 01267 USA. RP Pasachoff, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI SEATON, DANIEL/0000-0002-0494-2025 NR 27 TC 22 Z9 22 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2002 VL 207 IS 2 BP 241 EP 257 DI 10.1023/A:1016297800478 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 573AG UT WOS:000176806700004 ER PT J AU Graves, GR AF Graves, GR TI Habitat characteristics in the core breeding range of the swainson's warbler SO WILSON BULLETIN LA English DT Article ID GEOGRAPHIC-VARIATION; FORAGING BEHAVIOR; FOREST; POPULATIONS; SELECTION; WINTER AB I investigated the physiognomic and floristic characteristics of Swainson's Warbler (Limnothlypis swainsonii) territories at five localities within its core breeding range in Arkansas, Mississippi, Louisiana, and Florida. The warbler attained its greatest abundance (10-20 territorial males/km(2)) in floodplain forest characterized by small (<25 cm dbh) trees (ca 620-820 stems/ha) and understory thickets of saplings, vines, and shrubs (ca 35,000-48,000 small woody stems/ha). Territories in mature forest typically were associated with disturbance gaps. Canopy height, basal area, and floristics appear to be relatively unimportant factors in habitat selection, provided that understory requirements are met, which explains the warbler's occurrence in regenerating clearcuts as well as in relic tracts of old growth forest. Giant cane (Arundinaria gigantea), hypothesized to be an essential habitat requisite along the northern periphery of its breeding range, was sparse or absent in the prime breeding locations surveyed in this study. Selective thinning and clearcutting are viable habitat management techniques for the Swainson's Warbler. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, MRC-116,POB 37012, Washington, DC 20013 USA. EM graves.gary@nmnh.si.edu NR 60 TC 24 Z9 26 U1 1 U2 7 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD JUN PY 2002 VL 114 IS 2 BP 210 EP 220 DI 10.1676/0043-5643(2002)114[0210:HCITCB]2.0.CO;2 PG 11 WC Ornithology SC Zoology GA 620LV UT WOS:000179535600008 ER PT J AU Kress, WJ O'Connor, JD DePriest, P AF Kress, WJ O'Connor, JD DePriest, P TI The globalization of nature SO SCIENCE LA English DT Letter C1 Natl Museum Nat Hist, US Natl Herbarium, Washington, DC 20560 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Kress, WJ (reprint author), Natl Museum Nat Hist, US Natl Herbarium, MRC-166, Washington, DC 20560 USA. RI DePriest, Paula/K-6633-2015 NR 1 TC 1 Z9 1 U1 0 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAY 31 PY 2002 VL 296 IS 5573 BP 1612 EP 1612 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 558PR UT WOS:000175976200024 PM 12041534 ER PT J AU Krebs, E AF Krebs, E TI Borges and Argentine history ("biographia literaria" vs. regular biography) SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Letter C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Krebs, E (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU TIMES SUPPLEMENTS LIMITED PI MARKET HARBOROUGH PA TOWER HOUSE, SOVEREIGN PARK, MARKET HARBOROUGH LE87 4JJ, ENGLAND SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD MAY 31 PY 2002 IS 5174 BP 17 EP 17 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 559UX UT WOS:000176044700023 ER PT J AU Leigh, EG Vermeij, GJ AF Leigh, EG Vermeij, GJ TI Does natural selection organize ecosystems for the maintenance of high productivity and diversity? SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Review DE evolution of productivity; evolution of diversity; economics; ecosystems; Adam Smith ID CRETACEOUS-TERTIARY BOUNDARY; PERMIAN-TRIASSIC EXTINCTION; POPULATION-GENETICS; TROPICAL FOREST; WATER-BALANCE; RAIN-FOREST; SEA OTTERS; EVOLUTION; COMMUNITIES; HISTORY AB Three types of evidence suggest that natural ecosystems are organized for high productivity and diversity: (i) changes not previously experienced by a natural ecosystem, such as novel human disturbances, tend to diminish its productivity and/or diversity, just as 'random' changes in a machine designed for a function usually impair its execution of that function; (ii) humans strive to recreate proper-ties of natural ecosystems to enhance productivity of artificial ones, as farmers try to recreate properties of natural soils in their fields; and (iii) productivity and diversity have increased during the Earth's history as a whole, and after every major biotic crisis. Natural selection results in ecosystems organized to maintain high productivity of organic matter and diversity of species, just as competition among individuals in Adam Smith's ideal economy favours high production of wealth and diversity of occupations. In nature, poorly exploited energy attracts more efficient users. This circumstance favours the opening of new ways of life and more efficient recycling of resources, and eliminates most productivity-reducing 'ecological monopolies'. Ecological dominants tend to be replaced by successors with higher metabolism, which respond to more stimuli and engage in more varied interactions. Finally, increasingly efficient predators and herbivores favour faster turnover of resources. C1 Smithsonian Trop Res Inst, U0948, Balboa 34002, Panama. Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. RP Leigh, EG (reprint author), Smithsonian Trop Res Inst, U0948, Apartado 2072, Balboa 34002, Panama. NR 120 TC 17 Z9 18 U1 1 U2 22 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD MAY 29 PY 2002 VL 357 IS 1421 BP 709 EP 718 DI 10.1098/rstb.2001.0990 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 557JG UT WOS:000175905000010 PM 12079531 ER PT J AU Bodo, E Gianturco, FA Dalgarno, A AF Bodo, E Gianturco, FA Dalgarno, A TI The reaction of F+D-2 at ultra-low temperatures: the effect of rotational excitation SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID STATE POTASSIUM MOLECULES; BOSE-EINSTEIN CONDENSATE; PHOTOASSOCIATION AB We report an ab initio study of the dynamics of the reaction F + D-2 --> DF + D, where D-2 is initially in a rotationally excited state (j = 2). The possibility of obtaining ultra-cold molecules and of investigating reaction dynamics at ultra-low temperature relies on the production of molecules in a well defined quantum state and it is important to know the relative efficiency of the rotational quenching and of the chemical reaction. We examine here a reaction with an activation barrier, the reaction of F with D-2, and we find that quenching dominates the reaction when the initial rotational level lies energetically below the barrier, so severe trap loss may occur before the reaction can take place. C1 Univ Roma La Sapienza, NEC, Dept Chem, I-00185 Rome, Italy. Univ Roma La Sapienza, INFM, 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, NEC, Dept Chem, P A Moro 5, I-00185 Rome, Italy. RI Bodo, Enrico/F-4375-2012 NR 18 TC 25 Z9 25 U1 0 U2 2 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 MAY 28 PY 2002 VL 35 IS 10 BP 2391 EP 2396 AR PII S0953-4075(02)35975-3 DI 10.1088/0953-4075/35/10/316 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 560GZ UT WOS:000176075500021 ER PT J AU Hamilton, EL Greene, CH Sadeghpour, HR AF Hamilton, EL Greene, CH Sadeghpour, HR TI Shape-resonance-induced long-range molecular Rydberg states SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID ULTRACOLD NEUTRAL PLASMA; ATOMS; COLLISIONS; GAS; SCATTERING; SPECTRA; S-3(E); COLD; RB; CS AB When an excited atomic electron interacts with a neutral perturbing atom or molecule that possesses a shape resonance, it generates a characteristic class of Bom-Oppenheimer potential curves that rise with internuclear distance. We document this effect, and predict the existence of a diverse class of stable, strongly bound atom-atom and atom-molecule states that result from this phenomenon. For the specific case in which Rb is the perturbing atom, we show that such states should be observable in the spectroscopy of an ultracold gas or condensate. C1 Univ Colorado, Dept Phys, Boulder, CO 80309 USA. Univ Colorado, JILA, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Hamilton, EL (reprint author), Univ Colorado, Dept Phys, Boulder, CO 80309 USA. RI Greene, Chris/C-3821-2011 OI Greene, Chris/0000-0002-2096-6385 NR 24 TC 65 Z9 65 U1 0 U2 4 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 MAY 28 PY 2002 VL 35 IS 10 BP L199 EP L206 AR PII S0953-4075(02)36053-X DI 10.1088/0953-4075/35/10/102 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 560GZ UT WOS:000176075500002 ER PT J AU Lepp, S Stancil, PC Dalgarno, A AF Lepp, S Stancil, PC Dalgarno, A TI Atomic and molecular processes in the early Universe SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Review ID STIMULATED RADIATIVE ASSOCIATION; POTENTIAL-ENERGY SURFACE; RATE COEFFICIENTS; CHARGE-TRANSFER; DISSOCIATIVE RECOMBINATION; MUTUAL NEUTRALIZATION; HYDROGEN MOLECULES; GALAXY FORMATION; CROSS-SECTIONS; GAS CLOUDS AB Most of the information about the environment of the early Universe comes to us from radiation emitted from atoms and molecules. An understanding of the relevant atomic and molecular processes is needed to correctly interpret this radiation. Atomic and molecular process also control the evolution of the early Universe. In this paper, we review the atomic and molecular processes that are important in the early Universe. C1 Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. 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 Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. EM lepp@physics.unlv.edu; stancil@physast.uga.edu; adalgarno@cfa.harvard.edu NR 119 TC 133 Z9 134 U1 3 U2 27 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAY 28 PY 2002 VL 35 IS 10 BP R57 EP R80 AR PII S0953-4075(02)93670-9 DI 10.1088/0953-4075/35/10/201 PG 24 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 560GZ UT WOS:000176075500005 ER PT J AU Halasz, G Vibok, A Mebel, AM Baer, M AF Halasz, G Vibok, A Mebel, AM Baer, M TI Ab initio non-adiabatic coupling elements: the conical intersection between the 2(2)A ' and the 3(2)A ' of the H+H-2 system SO CHEMICAL PHYSICS LETTERS LA English DT Article ID SINGLE-SURFACE APPROXIMATIONS; GEOMETRIC PHASE; SCATTERING PROCESSES; C2H MOLECULE; CONSEQUENCES; STATES AB The conical intersections between the 1(2)A' and 2(2)A' electronic states and the 2(2)A' and 3(2)A' electronic states of the H-2 + H system were characterized by line-integral calculations using ab initio non-adiabatic coupling terms. The calculations confirmed that when a contour surrounds the {1(2)A',2(2)A'} conical intersection but does not approach, too closely, the {22 A', 32 A'} conical intersections the line-integral produces for the topological phase, the expected pi-value [Chem. Phys. Lett., 319 (2000) 489]. Estimating the location of {2(2)A', 3(2)A'} conical intersection, the line-integral procedure was employed again - this time for the {2(2)A', 3(2)A'} system - confirming, in the same way, also the existence of the {2(2)A', 3(2)A'} conical intersections. (C) 2002 Published by Elsevier Science B.V. C1 Harvard Smithsonian Ctr Astrophys, Inst Atom & Mol Sci, Cambridge, MA 02138 USA. Soreq NRC, Dept Phys & Appl Math, IL-81800 Yavne, Israel. RP Baer, M (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Atom & Mol Sci, 60 Garden St, Cambridge, MA 02138 USA. RI Mebel, Alexander/A-5234-2009 NR 31 TC 29 Z9 29 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD MAY 24 PY 2002 VL 358 IS 1-2 BP 163 EP 169 AR PII S0009-2614(02)00623-1 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 564GH UT WOS:000176306300025 ER PT J AU Carpenter, KE Johnson, GD AF Carpenter, KE Johnson, GD TI A phylogeny of sparoid fishes (Perciformes, Percoidei) based on morphology SO ICHTHYOLOGICAL RESEARCH LA English DT Article DE Nemipteridae; Lethrinidae; Sparidae; phylogeny; osteologgy AB The putative percoid superfamily Sparoidea includes the Nemipteridae, Lethrinidae, Sparidae, and Centracanthidae. Although a rigorous cladistic analysis has never been attempted, two hypotheses regarding relationships among these families have been proposed. One early noncladistic hypothesis considered the Sparidae to be intermediate between the more primitive Nemipteridae and the more derived Lethrinidae. A later nonformal phylogenetic treatment provided evidence for a close relationship between Sparidae and Centranthidae and suggested a closer affinity between the Nemipteridae and Lethrinidae. We examine 54 osteological, ligament, and squamation characters in representatives of all 45 genera of these families and 4 outgroup taxa. The results of our cladistic analysis are congruent with a cladistic interpretation of the earlier hypothesis, with strong support for the phyletic sequence Nemipteridae, Lethrinidae, Sparidae plus Centracanthidae, with placement of centracanthids unresolved with respect to sparid genera. C1 Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Washington, DC 20560 USA. RP Carpenter, KE (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. NR 22 TC 14 Z9 17 U1 3 U2 10 PU SPRINGER-VERLAG TOKYO PI TOKYO PA 3-3-13, HONGO, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 1341-8998 J9 ICHTHYOL RES JI Ichthyol. Res. PD MAY 24 PY 2002 VL 49 IS 2 BP 114 EP 127 DI 10.1007/s102280200015 PG 14 WC Zoology SC Zoology GA 559ET UT WOS:000176013200003 ER EF