FN Thomson Reuters Web of Science™ VR 1.0 PT S AU Jerius, D Gaetz, TJ Karovska, M AF Jerius, D Gaetz, TJ Karovska, M BE Flanagan, KA Siegmund, OHW TI Calibration of Chandra's near on-axis performance SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE X-ray optics; PSF; Chandra AB The Chandra X-Ray telescope has excellent angular resolution for on-axis sources. While its Wolter type I design optimizes on-axis performance, there is a relatively large region in which 0.5" to 1" imaging is possible. The Chandra PSF was first characterized during ground calibration and, most recently, from actual on-orbit measurements. The ground calibration provided data with the highest signal to noise but, because of gravity-induced distortions of the optics, could not completely characterize their performance. We present the results of on-orbit calibrations of the optics' performance, focusing on the near on-axis field of view. We present for the first time an analysis of the energy dependence of the on-orbit PSF. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Jerius, D (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 5 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 433 EP 444 DI 10.1117/12.509359 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700042 ER PT S AU Beckerman, E Aldcroft, T Gaetz, TJ Jerius, D Nguyen, D Tibbetts, M AF Beckerman, E Aldcroft, T Gaetz, TJ Jerius, D Nguyen, D Tibbetts, M BE Flanagan, KA Siegmund, OHW TI Positional accuracy as a measure of Chandra's optical distortions SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE Chandra; HRMA; optical distortions; positional accuracy; X-ray optics ID ORION NEBULA CLUSTER AB We present a study of Chandra's optical distortions by examining the positional accuracy of observed sources on the HRC-I. We investigate the Chandra mirror and detector models' ability to reproduce the detector locations of observed sources by simulating similar to160 calibration observations of AR Lac, HR 1099, and LMC X-1. To study the optical distortions of the mirrors more directly, we compare a 63 ksec observation of the Orion Nebular Cluster (ONC) with positions based on the well-determined optical astrometry of the cluster. We simulate observations of 100 reasonably bright sources from the Hillenbrand 1997(1) catalog of the ONC and compare the simulated positions with their observed positions. Offsets between the optical positions and the observed X-ray positions help determine a map of the optical distortions of the Chandra mirrors. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beckerman, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 445 EP 456 DI 10.1117/12.509381 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700043 ER PT S AU Graessle, DE Soufli, R Aquila, AL Gullikson, EM Blake, RL Burek, AJ AF Graessle, DE Soufli, R Aquila, AL Gullikson, EM Blake, RL Burek, AJ BE Flanagan, KA Siegmund, OHW TI Iridium optical constants for the Chandra X-ray Observatory from reflectance measurements of 0.05-12 keV SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE Chandra X-ray Observatory; iridium; optical constants; reflectance; X-ray mirrors; grazing incidence ID SCATTERING AB We present optical constants derived from synchrotron reflectance measurements of iridium-coated X-ray witness mirrors over 0.05-12 keV, relevant to the Chandra X-ray Observatory effective area calibration. In particular we present for the first time analysis of measurements taken at the Advanced Light Source Beamline 6.3.2 over 50-1000 eV, Chandra's lower-energy range. Refinements to the currently tabulated iridium optical constants (B. L. Henke et al., At. Data Nucl. Data Tables 54, 181-343, 1993 and on the Web at http://www-cxro.lbl.gov/optical-constants/) will become important as the low-energy calibration of Chandra's X-ray detectors and gratings are further improved, and as possible contaminants on the Chandra mirror assembly are considered in the refinement of the in-flight Ir absorption edge depths. The goal of this work has been to provide an improved tabulation of the Ir optical constants over the full range of Chandra using a self-consistent mirror model, including metallic layers, interface roughness, contaminating overlayer, and substrate. The low-energy data present us with a considerable challenge in the modeling of the overlayer composition, as the K-absorption features of C, O, and N are likely to be present in the similar to10A overlayer. The haphazard contamination and chemical shifts may significantly affect optical constants attributed to this overlayer, which will distort the iridium optical constants derived. Furthermore, the witness mirror contamination may be considerably different from that deposited on the flight optics. The more complex modeling required to deal with low-energy effects must reduce to the simpler model applied at the higher energies, which has successfully derived optical constants for iridium in the higher energy range, including the iridium M-edges, already used in the Chandra calibration. We present our current results, and the state of our modeling and analysis, and our approach to a self-consistent tabulation. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Graessle, DE (reprint author), Smithsonian Astrophys Observ, MS-70, Cambridge, MA 02138 USA. NR 7 TC 5 Z9 5 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 469 EP 481 DI 10.1117/12.506132 PG 13 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700045 ER PT S AU Zhao, P Jerius, D Edgar, RJ Gaetz, TJ Van Speybroeck, LP Biller, B Beckerman, E Marshall, HL AF Zhao, P Jerius, D Edgar, RJ Gaetz, TJ Van Speybroeck, LP Biller, B Beckerman, E Marshall, HL BE Flanagan, KA Siegmund, OHW TI Chandra X-ray Observatory mirror effective area SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE Chandra X-ray Observatory; HRMA; X-ray telescopes; X-ray mirrors; calibration; effective area ID AXAF CALIBRATION; DETECTORS AB Chandra X-ray Observatory (CXO) - the third of NASA's Great Observatories - has now been successfully operated for four years and has brought us fruitful scientific results with many exciting discoveries. The major achievement comparing to previous X-ray missions lies in the heart of the CXO - the High Resolution Mirror Assembly. Its unprecedented spatial resolution and well calibrated performing characteristics are the keys for its success. We discuss the effective area of the CXO mirrors, based on the ground calibration measurements made at the X-Ray Calibration Facility in Marshall Space Flight Center before launch. We present the derivations of both on-axis and off-axis effective areas, which are currently used by Chandra observers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhao, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 9 Z9 9 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 482 EP 496 DI 10.1117/12.509379 PG 15 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700046 ER PT S AU Wargelin, BJ Ratzlaff, PW Pease, DO Kashyap, VL Drake, JJ AF Wargelin, BJ Ratzlaff, PW Pease, DO Kashyap, VL Drake, JJ BE Flanagan, KA Siegmund, OHW TI Chandra LETG higher order diffraction efficiencies SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE Chandra; LETG; diffraction efficiency; calibration AB Accurate calibration of the Chandra Low Energy Transmission Grating (LETG) higher-order (\m\ > 1) diffraction efficiencies is vital for proper analysis of spectra obtained with the LETG's primary detector, the HRC-S, which lacks the energy resolution to distinguish different orders. Pre-flight ground calibration of the LETG was necessarily limited to sampling a relatively small subset of spectral orders and wavelengths, and virtually no higher-order data are available in the critical region between 6 and 10 Angstrom. In this paper, we describe an analysis of diffraction efficiencies based on in-flight data obtained using the LETG's secondary detector, the ACIS-S. Using ACIS, the relative efficiency of each order can be studied out to \mlambda\ similar to 80 Angstrom, which is nearly one-half of the LETG/HRC-S wavelength coverage. We find that the current models match our results well but can be improved., particularly for the even orders just longward of the Au-M edge at 6 Angstrom. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Wargelin, BJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 509 EP 517 DI 10.1117/12.509361 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700048 ER PT S AU Chung, SM Drake, JJ Kashyap, VL Ratzaff, PW Wargelin, BJ AF Chung, SM Drake, JJ Kashyap, VL Ratzaff, PW Wargelin, BJ BE Flanagan, KA Siegmund, OHW TI Characterizing non-linearities in the Chandra LETG plus HRC-S dispersion relation SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE AB The dispersion relation for the Chandra Low Energy Transmission Grating Spectrometer (LETGS) is known to better than 1 part in 1000 over the wavelength range 5-150 Angstrom. A recent resolution of a data processing software bug that lead to a systematic error in the computation of photon wavelengths has allowed us to trace further discrepancies in the dispersion relation to the boundaries between different microchannel plate segments of the HRC-S imaging detector. However, data acquired during in-flight calibration with the HRC-S detector have always shown the presence of additional non-linear deviations in the positions of some spectral lines by as much as 0.05 Angstrom, which is of the order of a full width half maximum (FWHM) of a line profile. These latter effects are thought to be caused by spatial non-linearities in the imaging characteristics of the HRC-S detector. Here, we present an improved dispersion relation for the LETG+HRC-S and new methods to help characterize the spatial non-linearities. We also describe an empirical approach that might be used to help improve the position determination of photon events. C1 Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, Cambridge, MA 02138 USA. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 518 EP 529 DI 10.1117/12.509360 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700049 ER PT S AU Virani, SN DePasquale, JM Schwartz, DA Cameron, RA Plucinsky, PP O'Dell, SL Minow, JI Blackwell, WC AF Virani, SN DePasquale, JM Schwartz, DA Cameron, RA Plucinsky, PP O'Dell, SL Minow, JI Blackwell, WC BE Flanagan, KA Siegmund, OHW TI Improving the science observing efficiency of the Chandra X-ray observatory via the Chandra radiation model SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE Chandra; space missions; radiation environment; radiation belts; radiation models ID ENVIRONMENT AB The Chandra X-ray Observatory (CXO), NASA's latest "Great Observatory", was launched on July 23, 1999 and reached its final orbit on August 7, 1999. The CXO is in a highly elliptical orbit, with an apogee altitude of 120,000 km and a perigee altitude of 20,000 km, and has a period of approximately 63.5 hours (approximate to 2.65 days). It transits the Earth's Van Allen belts once per orbit during which no science observations can be performed due to the high radiation environment. The Chandra X-ray Observatory Center currently uses the National Space Science Data Center's "near Earth" AP-8/AE-8 radiation belt model to predict the start and end times of passage through the radiation belts. Our earlier analysis (Virani et al, 2000) demonstrated that our implementation of the AP-8/AE-8 model (a simple dipole model of the Earth's magnetic field) does not always give sufficiently accurate predictions of the start and end times of transit of the Van Allen belts. This led to a change in our operating procedure whereby we "padded" the start and end times of transit as determined by the AE-8 model by 10 ks so that ACIS, the Advanced CCD Imaging Spectrometer and the primary science instrument on-board Chandra, would not be exposed to the "fringes" of the Van Allen belts on ingress and egress for any given transit. This additional 20 ks per orbit during which Chandra is unable to perform science observations integrates to approximately 3 Ms of "lost" science time per year and therefore reduces the science observing efficiency of the Observatory. To address the need for a higher fidelity radiation model appropriate for the Chandra orbit, the Chandra Radiation Model (CRM) was developed. The CRM is an ion model for the outer magnetosphere and is based on data from the EPIC/ICS instrument on-board the Geotail satellite as well as data from the CEPPAD/IPS instrument on-board the Polar satellite. With the production and implementation of the CRM Version 2.3, we present the results of a study designed to investigate the science observing time that may be recovered by using the CRM for science mission planning purposes. In this paper, we present a scheme using the CRM such that for a modest increase in ACIS CTI, approximately 500 ks can be recovered each year for new science observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Virani, SN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 5 TC 2 Z9 2 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 530 EP 541 DI 10.1117/12.505878 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700050 ER PT S AU DePasquale, JM Virani, SN Schwartz, DA Cameron, RA Plucinsky, PP O'Dell, SL Minow, JI Blackwell, WC AF DePasquale, JM Virani, SN Schwartz, DA Cameron, RA Plucinsky, PP O'Dell, SL Minow, JI Blackwell, WC BE Flanagan, KA Siegmund, OHW TI A study of the seasonal variations of the Chandra X-ray observatory radiation model SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE Chandra; space missions; radiation environment; radiation belts; radiation models AB The Chandra X-ray Observatory (CXO), launched in July of 1999, contains two focal-plane imaging detectors and two transmission-grating spectrometers. Maintaining an optimal performance level for the observatory is the job of the Chandra X-ray Center (CXC), located in Cambridge, MA. One very important aspect of the observatory's performance is the science observing efficiency. The single largest factor which reduces the observing efficiency of the observatory is the interruption of observations due to passage through the Earth's radiation belts approximately every 2 2/3 days. During radiation belt passages, observations are suspended on average for over 15 hours and the Advanced CCD Imaging Spectrometer (ACIS) is moved out of the focus of the telescope to minimize damage from low-energy (100-200 keV) protons. The CXC has been using the National Space Science Data Center's "near Earth" AE-8/AP-8 radiation belt model to predict the entry and exit from the radiation belts. However, it was discovered early in the mission that the AE-8/AP-8 model predictions were inadequate for science scheduling purposes and a 10 ks "pad time" was introduced on ingress and egress of perigee to ensure protection from radiation darnage.(1) This pad time, totaling 20 ks per orbit, has recently been the subject of much analysis to determine if it can be reduced to maximize science observing efficiency. A recent analysis evaluating a possible correlation between the Chandra Radiation Model (CRM) and the Electron Proton Helium Instrument (EPHIN) found a greatest lower bound (GLB) in lieu of a correlation for the ingress and egress of each perigee.(2) The GLB is a limit imposed on the CRM such that when the CRM exceeds this limit on ingress, this defines the new safing time and similarly for egress. We have shown that using this method we can regain a significant amount of lost science time at the expense of minimal radiation exposure. The GLB analysis also found that different GLBs produce varied results and hint that there could be a time dependence associated with the GLB, possibly related to the orientation of the Observatory's orbit. Utilizing CRM V2.3, we present the search for a seasonal dependence on the value of the GLB; we find a seasonal effect that appears to depend on the orientation of Chandra's orbit with respect to the Earth's magnetic field. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP DePasquale, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 3 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 554 EP 564 DI 10.1117/12.516469 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700053 ER PT S AU Schnopper, HW Ingram, R Silver, E Barbera, M Candia, R Christensen, FE Jensen, CP Romaine, S Vernani, D Cotroneo, V Varisco, S Artale, MA Madsen, KK Callura, A AF Schnopper, HW Ingram, R Silver, E Barbera, M Candia, R Christensen, FE Jensen, CP Romaine, S Vernani, D Cotroneo, V Varisco, S Artale, MA Madsen, KK Callura, A BE MacDonald, CA Macrander, AT Ishikawa, T Morawe, C Wood, JL TI Thin shell plastic lenses for space and laboratory applications SO X-RAY SOURCES AND OPTICS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Sources and Optics CY AUG 02-03, 2004 CL Denver, CO SP SPIE DE X-ray optics; X-ray telescopes; X-ray lenses; X-ray imaging; X-ray collimation; medical diagnostics; microanalysis ID ASTROPHYSICS AB We have identified an inexpensive, readily available, mechanically stable, extremely smooth, elastic, and mechanically uniform plastic suitable for thin film X-ray optics. Polyethylene terephthalate (PET) is easily deformed without losing its elastic properties or surface smoothness. Most important, PET can be coated with mono- or multilayers that reflect X-rays at grazing incidence. We have used these properties to produce X-ray optics made either as a concentric nest of cylinders or as a spiral. We have produced accurately formed shells in precisely machined vacuum mandrels or used a pin and wheel structure to form a continuously wound spiral. The wide range of medical, industrial and scientific applications for our technology includes: a monochromatic X-ray collimator for medical diagnostics, a relay optic to transport an X-ray beam from the target in a scanning electron microscope to a lithium-drifted silicon and microcalorimeter detectors and a satellite mounted telescope to collect celestial X-rays. A wide variety of mono- and multilayer coatings allow X-rays up to similar to 100 keV to be reflected. Our paper presents data from a variety of diagnostic measurements on the properties of the PET foil and imaging results form single- and multi-shell lenses. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Schnopper, HW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI collura, alfonso/0000-0001-9534-1235; Barbera, Marco/0000-0002-3188-7420; Madsen, Kristin/0000-0003-1252-4891; Varisco, Salvatore/0000-0002-6891-8390 NR 10 TC 7 Z9 7 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5475-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5537 BP 82 EP 93 DI 10.1117/12.559774 PG 12 WC Optics SC Optics GA BBJ12 UT WOS:000225736100010 ER PT S AU Rots, AH AF Rots, AH BE Kaaret, P Lamb, FK Swank, JH TI 2800 days of monitoring the timing of PSR b1509-58 with RXTE SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project AB We have analyzed 90 observations of the young pulsar B 1509-58 made by RXTE over 7.6 years. The pulse profile can be described as a combination of two systems. The first consists of two narrow components separated by 0.14 period with an amplitude ratio of 10:3; the second consists of a single broader component. The two systems appear to be shifting with respect to each other as a function of energy. We have derived a single timing ephemeris on the basis of the X-ray observations, using terms up to the third derivative. There is no indication that a fourth derivative is required. The resulting value of the first braking index is consistent with that derived from radio observations, but the second braking index is twice its expected value. This casts some doubt on the significance of the pulsar's characteristic age (1700 years). The phase residuals have been fit with sine components, resulting in an estimate of the proper motion (45 +/- 25 mas/yr at a position angle of 45 45) and of masses and orbital radii (ranging from 0.7 to 2 AU and 0.25 to 2.5 earth masses) of planetary material - if that is the cause of these phase excursions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Rots, AH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 67, Cambridge, MA 01238 USA. NR 7 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 309 EP 312 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800057 ER PT S AU Vrtilek, SD AF Vrtilek, SD BE Kaaret, P Lamb, FK Swank, JH TI Long-term X-ray variability and the importance of the ASM SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID ACCRETION DISCS; SMC X-1; BINARIES AB From determining the log(N)-log(S) distribution of XRBs in the Milky Way, to testing radio/X-ray correlations of microquasars and BHCs, studying long term variability, and acting as a trigger for observations of transient sources, the ASM on RXTE has proved an invaluable resource. I will briefly discuss some highlights of the many results that have been possible only because of the ASM. The fact that the number of papers per year (over 100) that have relied on ASM data has remained steady over the 8-year lifetime of the RXTE is an indication of the enduring usefulness of all-sky X-ray monitoring. I argue that the permanent presence in space of an ASM-like instrument is a major benefit to numerous active branches of astrophysics, that there is no substitute (ground-based or in other parts of the electromagnetic spectrum) for this capability, and that the planning process for future missions ought to take into account the ongoing scientific need for all-sky X-ray monitoring. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vrtilek, SD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 331 EP 336 PG 6 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800060 ER PT S AU Grindlay, JE AF Grindlay, JE BE Kaaret, P Lamb, FK Swank, JH TI Hard X-ray timing with EXIST SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID DISRUPTION; LUMINOSITY; GALAXIES; MISSION AB The Energetic X-ray Timing Survey Telescope (EXIST) mission concept is under study as the Black Hole Finder Probe (BHFP), one of the three Einstein Probe missions in the Beyond Einstein Program in the current NASA Strategic Plan. EXIST would conduct an all-sky imaging hard X-ray (similar to10-600 keV) survey with unprecedented sensitivity: about 5 x 10(-13) cgs over any factor of 2 bandwidth, or comparable to that achieved at soft X-rays in the ROSAT survey. The proposed angular resolution of 5arcmin, temporal resolution of 10microsec, energy resolution of 1-4 keV over the broad band, and duty cycle of 0.2-0.5 for continuous coverage of any source provide an unprecedented phase space for timing and spectral studies of black holes -from stellar to supermassive, as well as neutron stars and accreting white dwarfs. The large sky coverage allows intrinsically rare events to be studied. One particularly exciting example is the possible detection of tidal disruption of stars near quiescent AGN. Super flares from SGRs could be detected out to the Virgo cluster. The large duty cycle and all sky monitor nature of the mission will enable QPOs from luminous AGN and BH X-ray binaries to be studied on timescales not possible before. I provide an overview of the mission concept and Reference Design, the X-ray timing science prospects for EXIST, and how these might be further optimized in the current Study for EXIST as the BHFP so that EXIST might include many of the desirable features of a next-generation timing mission. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM josh@cfa.harvard.edu NR 19 TC 10 Z9 10 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 413 EP 420 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800074 ER PT S AU Kaaret, P AF Kaaret, P BE Kaaret, P Lamb, FK Swank, JH TI Silicon-based large-area X-ray detectors SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID QUASI-PERIODIC OSCILLATION; GRO J1655-40; DISCOVERY; BREAKDOWN; DIODES; HZ; PHOTODIODES; EXPLORER; VOLTAGE; MISSION AB The great success of the Rossi X-Ray Timing Explorer (RXTE) has shown that X-ray timing is an excellent tool for study of the physics of strong gravitational fields and for measurement of fundamental physical properties of black holes and neutron stars. In order to provide a qualitative advance in X-ray timing capabilities, the next generation X-ray timing mission will require an effective area near 10 square meters with sensitivity extending into the hard X-ray band an order of magnitude increase in effective area over RXTE. Achieving such a large effective area at reasonable cost will require advances in detector technology. Silicon-based detectors have a long heritage in space applications and can be fabricated in the large numbers needed for a large area detector by industry with existing facilities and at reasonable cost. I describe current work on the development of silicon-based detectors suitable for a next generation X-ray timing mission. 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 29 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 423 EP 430 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800075 ER PT S AU Gorenstein, P AF Gorenstein, P BE Kaaret, P Lamb, FK Swank, JH TI A focusing X-ray timing observatory SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID QUASI-PERIODIC OSCILLATION; DISCOVERY AB The next generation X-ray timing observatory will be a more powerful and versatile facility if it is based upon focusing optics rather than large area detectors. With X-ray CCDs or active pixel detectors (or possibly even microcalorimeters) in the focal plane(s) the spectral resolution will be significantly superior to the RXTE PCA making it possible to study the dynamics of the gravitationally redshifted Fe line in great detail. With orders of magnitude reduction of background the ability to study temporal variations of fainter sources in external galaxies will be much greater than with large area counters of the same collecting area. Furthermore, source confusion will not be an issue as it may be when large area detectors observe sources near the galactic center or in other galaxies. Focusing detectors do require larger open apertures than counters and their bandwidth is smaller. However, they are not necessarily heavier and in fact one candidate optic would be much lighter. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gorenstein, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 431 EP 438 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800076 ER PT S AU Di Stefano, R AF Di Stefano, R BE Kaaret, P Lamb, FK Swank, JH TI The importance of monitoring soft X-ray sources SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID LARGE-MAGELLANIC-CLOUD; CAL-87; BINARY; MODELS; GALAXY AB The next generation of X-ray monitoring missions should include detectors sensitive to X-rays with energies below 2 keV This capability will allow us to explore the physics associated with soft sources, including hot white dwarfs, intermediate-mass black holes, soft active galactic nuclei, soft emission in gamma-ray burst afterglows, and many X-ray active stars. I also show, using Chandra data from 4 galaxies, that more than half of the photons from even so-called "canonical" X-ray sources (with strong emission signatures above 2 keV) have energies below 2 keV This suggests that soft-X-ray monitoring can open new doors to our understanding of even well-studied sources. C1 Tufts Univ, Harvard Smithsonian Ctr Astrophys, Medford, MA 02155 USA. RP Di Stefano, R (reprint author), Tufts Univ, Harvard Smithsonian Ctr Astrophys, Medford, MA 02155 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 451 EP 454 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800080 ER PT S AU Elvis, M AF Elvis, M BE Kaaret, P Lamb, FK Swank, JH TI An extreme physics MIDEX SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID NEUTRON-STARS AB A moderate sized mission to use bright X-ray sources as physics labs is described. A combination of microchannel plate optics and a 32x32 pixel microcalorimeter would allow the successor to the Rossi XTE to explore new domains of spectroscopic timing in a MIDEX class mission. With similar to10 times the area and similar to100 times the spectral resolution of the PCA (and 10 times that of silicon detectors) such a mission would be able to explore spectral line shifts in magnetars, neutron stars and black holes. Adding a polarimeter would create a powerful and unique capability. Such a mission would make numerous tests of basic physics, both quantum electrodynamics/chromodynamics (QED/QCD) and general relativity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 459 EP 462 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800082 ER PT S AU Gelfand, JD Lazio, TJW Gaensler, BM AF Gelfand, JD Lazio, TJW Gaensler, BM BE Camilo, F TI A 330 MHz survey for pulsars and supernova remnants in m31 SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union AB In the radio band, supernova remnants (SNRs) and pulsars are best identified at low frequencies due to their steep spectra. Motivated by this fact, we have carried out a deep 330-MHz observation of M31 using the VLA. Achieving a sensitivity of 0.6 mJy at 6" resolution over the entire optical disk of M31, we identified 405 distinct radio sources. While most of these are unresolved background radio galaxies, we found five SNR candidates, three pulsar wind nebula (PWN) candidates, and three pulsar candidates in our source list. The properties of these sources are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Washington, DC 20375 USA. RP Gelfand, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-10, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010 NR 7 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 91 EP 92 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000024 ER PT S AU Seward, F Smith, R Hagler, J Portolese, L Gaetz, T Slane, P Koo, BC Lee, JJ AF Seward, F Smith, R Hagler, J Portolese, L Gaetz, T Slane, P Koo, BC Lee, JJ BE Camilo, F TI The Chandra supernova remnant catalog SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union AB We show some examples from a WWW-based catalog, containing Chandra archive data, that is now under construction. Many remnants show manifestations of internal neutron stars, which are of particular interest to this conference. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Seoul Natl Univ, SEES, Seoul, South Korea. RP Seward, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 93 EP 94 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000025 ER PT S AU Kaplan, DL Kulkarni, SR Rail, DA Gaensler, BM Slane, PO Gotthelf, EV AF Kaplan, DL Kulkarni, SR Rail, DA Gaensler, BM Slane, PO Gotthelf, EV BE Camilo, F TI Searching for compact objects in supernova remnants: Initial results SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID X-RAY SOURCES; RADIO PULSARS AB Most astronomers now accept that stars more massive than about 9 M-(c) explode as supernovae and leave stellar remnants, either neutron stars or black holes. However, less than half of the SNRs within 5 kpc have identified central sources. Here, we discuss a systematic effort to search for compact central sources in the remaining 23 SNRs of this distance-limited sample. As the first part of this survey, we are able to state with some confidence that there are no associated central sources down to a level of one tenth of that of the Cas A central source Lx less than or similar to 10(31) ergs s-1, in four SNRs (G093.3+6.9, G315.4-2.3, G084.2+0.8, and G127.1+0.5). We compare our limits with cooling curves for neutron stars and find that any putative neutron stars in these SNRs must be cooling faster than expected for traditional 1.35 M-circle dot neutron stars. C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Kaplan, DL (reprint author), CALTECH, Dept Astron, 105-24, Pasadena, CA 91125 USA. RI Gaensler, Bryan/F-8655-2010 NR 13 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 123 EP 126 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000030 ER PT S AU Gaensler, BM AF Gaensler, BM BE Camilo, F TI Shocks and wind bubbles around energetic pulsars SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID HUBBLE-SPACE-TELESCOPE; SUPERNOVA-REMNANTS; CRAB-NEBULA; BOW SHOCKS; SIMULATIONS; EMISSION; LIMITS; JET AB The Crab Nebula demonstrates that neutron stars can interact with their environments in spectacular fashion, their relativistic winds generating nebulae observable across the electromagnetic spectrum. At many previous conferences, astronomers have discussed, debated and puzzled over the complicated structures seen in the Crab, but have been limited to treating most other pulsar wind nebulae (PWNe) as simple calorimeters for a pulsar's spin-down energy. However, with the wealth of high-quality data which have now become available, this situation has changed dramatically. I here review some of the main observational themes which have emerged from these new measurements. Highlights include the ubiquity of pulsar termination shocks, the unambiguous presence of relativistic jets in PWNe, complicated time variability seen in PWN structures, and the use of bow shocks to probe the interaction of pulsar winds with the ambient medium. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010 NR 29 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 151 EP 158 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000039 ER PT S AU Slane, P AF Slane, P BE Camilo, F TI High resolution X-ray observations of 3C 58 SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID PULSAR WIND NEBULAE; REMNANT 3C 58; NEUTRON-STAR; CONSTRAINTS AB As the presumed remnant of SN 1181, 3C 58 houses one of the youngest known neutron stars in the Galaxy. The properties of this young pulsar and its associated pulsar wind nebula (PWN) differ considerably from those of the Crab Nebula, and may well offer a more typical example of the endpoint of massive star collapse. High resolution X-ray studies reveal structures in the inner nebula that may be associated with the pulsar wind termination shock, a jet that may be aligned with the rotation axis, and other regions of enhanced emission. Spectral variations in the PWN are consistent with the expected evolution of the postshock flow, and complex loops of emission are seen in the nebula interior. Limits on the neutron star surface temperature fall below standard cooling models, indicating that some more rapid neutrino cooling process is required. The outer regions of 3C 58 show thermal emission with enhanced levels of neon, indicative of shocked ejecta bounding the PWN. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 185 EP 188 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000047 ER PT S AU Hughes, JP Friedman, RB Slane, P Park, S AF Hughes, JP Friedman, RB Slane, P Park, S BE Camilo, F TI An X-ray pulsar, metal-rich Ejecta, and shocked ambient medium in the supernova remnant G292.0+1.8 SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union AB We report the discovery of pulsed X-ray emission from the compact object CXOU J112439.1-591620 within the Galactic supernova remnant G292.0+1.8 using the High Resolution Camera on the Chandra X-Ray Observatory. The X-ray period is consistent with the extrapolation of the radio period and spindown rate of PSR J1124-5916. The X-ray pulse is single peaked and broad. There is no optical counterpart to a limit of M-V similar to 26. The pressure in the pulsar wind nebula is considerably less than that in the reverse-shock-heated ejecta and circumstellar medium, indicating that the reverse shock has not yet begun to interact with the nebula. C1 Rutgers State Univ, Piscataway, NJ 08855 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, University Pk, PA 16802 USA. RP Hughes, JP (reprint author), Rutgers State Univ, Piscataway, NJ 08855 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 199 EP 202 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000051 ER PT S AU Harrus, I Bernstein, JP Slane, PO Gaensler, B Hughes, JP Moffett, D Dodson, R AF Harrus, I Bernstein, JP Slane, PO Gaensler, B Hughes, JP Moffett, D Dodson, R BE Camilo, F TI Chandra study of the central object associated with the supernova remnant MSH 11-62 SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID NEBULAE; PULSARS AB We present results from our analysis of Chandra data on the supernova remnant MSH 11-62 (also known as G291.0-0.1). Our previous ASCA analysis showed that MSH 11-62 is most likely a composite remnant whose strong non-thermal emission is powered by a compact object, most probably a pulsar. The present analysis confirms in a spectacular fashion the earlier detection of a compact source. The Chandra data reveal a small region with a hard non-thermal spectrum located at the tip of the central radio emission seen in data taken at the Australia Telescope Compact Array (ATCA). This source is likely the young rapidly rotating neutron star powering the synchrotron nebula in MSH 11-62. Compared to other young rotation-powered pulsars the Chandra spectrum of MSH 11-62 implies an energy loss rate of E similar to 5 x 10(36) ergs s(-1). C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutgers State Univ, Piscataway, NJ 08854 USA. Furman Univ, Greenville, SC 29613 USA. Japan Aerosp Explorat Agcy, JAXA, Kanagawa 2298510, Japan. RP Harrus, I (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Gaensler, Bryan/F-8655-2010 NR 7 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 203 EP 206 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000052 ER PT S AU Bock, DCJ Gaensler, BM AF Bock, DCJ Gaensler, BM BE Camilo, F TI Millimeter-wave imaging of pulsar wind nebulae SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID SUPERNOVA-REMNANTS AB We have observed the supernova remnants G16.7+0.1 and G29.7-0.3 at millimeter wavelengths with the Berkeley-Illinois-Maryland Association array, measuring total flux densities of the pulsar wind nebulae in the remnants. Our results imply a break at similar to 50 GHz in the spectrum of the PWN in C29.7-0.3, lower than previously estimated. The PWN in C16.7+0.1 either has a break < 100 GHz, or a steep radio spectrum. C1 Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bock, DCJ (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Gaensler, Bryan/F-8655-2010 NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 207 EP 210 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000053 ER PT J AU Brown, JL Goritz, F Pratt-Hawkes, N Hermes, R Galloway, M Graham, LH Gray, C Walker, SL Gomez, A Moreland, R Murray, S Schmitt, DL Howard, J Lehnhardt, J Beck, B Bellem, A Montali, R Hildebrandt, TB AF Brown, JL Goritz, F Pratt-Hawkes, N Hermes, R Galloway, M Graham, LH Gray, C Walker, SL Gomez, A Moreland, R Murray, S Schmitt, DL Howard, J Lehnhardt, J Beck, B Bellem, A Montali, R Hildebrandt, TB TI Successful artificial insemination of an Asian elephant at the National Zoological Park SO ZOO BIOLOGY LA English DT Article DE hormones; ultrasound; assisted reproduction; pregnancy; LH ID LOXODONTA-AFRICANA ELEPHANTS; LUTEINIZING-HORMONE; REPRODUCTIVE FUNCTION; ENZYME-IMMUNOASSAY; SERUM PROGESTERONE; UROGENITAL TRACT; IMPORTANT TOOL; MAXIMUS; PREGNANCY; ULTRASONOGRAPHY AB For decades, attempts to breed elephants using artificial insemination (AI) have failed despite considerable efforts and the use of various approaches. However, recent advances in equipment technology and endocrine-monitoring techniques have resulted in 12 elephants conceiving by AI within a 4-year period (19982002). The successful AT technique employs a unique endoscope-guided catheter and transrectal ultrasound to deliver semen into the anterior vagina or cervix, and uses the "double LH surge" (i.e., identifying the anovulatory LH (anLH) surge that predictably occurs 3 weeks before the ovulatory LH (ovLH) surge to time insemination. This study describes the 6-year collaboration between the National Zoological Park (NZP) and the Institute for Zoo Biology and Wildlife Research (IZW), Berlin, Germany, that led to the refinement of this AI technique and subsequent production of an Asian elephant calf. The NZP female was the first elephant to be inseminated using the new AI approach, and was the fifth to conceive. A total of six AI trials were conducted beginning in 1995, and conception occurred in 2000. Semen was collected by manual rectal stimulation from several bulls in North America. Sperm quality among the bulls was variable and was thus a limiting factor for AI. For the successful AI, semen quality was good to excellent (75-90% motile sperm), and sperm was deposited into the anterior vagina on the day before and the day of the ovLH surge. Based on transrectal ultrasound, ovulation occurred the day after the ovLH surge. Pregnancy was monitored by serum and urinary progestagen, and serum prolactin analyses in samples collected weekly. Fetal development was assessed at 12, 20, and 28 weeks of gestation using transrectal ultrasound. Elevated testosterone measured in the maternal circulation after 36 weeks of gestation reliably predicted the calf was a male. Parturition was induced by administration of 40 IU oxytocin 3 days after serum progestagens dropped to undetectable baseline levels. We conclude that AI has potential as a supplement to natural breeding, and will be invaluable for improving the genetic management of elephants, provided that problems associated with inadequate numbers of trained personnel and semen donors are resolved. (C) 2004 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. Inst Zoo Biol & Wildlife Res, Berlin, Germany. Disneys Anim Kingdom, Lake Buena Vista, FL USA. Natl Zool Pk, Dept Biol Programs, Washington, DC USA. African Lion Safari, Cambridge, ON, Canada. SW Missouri State Univ, Dept Agr, Springfield, MO USA. Natl Zool Pk, Dept Pathol, Washington, DC USA. RP Brown, JL (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, 1500 Remont Rd, Front Royal, VA 22630 USA. EM jbrown@crc.si.edu NR 37 TC 30 Z9 32 U1 4 U2 17 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2004 VL 23 IS 1 BP 45 EP 63 DI 10.1002/zoo.10116 PG 19 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 778XU UT WOS:000189267300004 ER PT J AU Brown, JL Olson, D Keele, M Freeman, EW AF Brown, JL Olson, D Keele, M Freeman, EW TI Survey of the reproductive cyclicity status of Asian and African elephants in north America SO ZOO BIOLOGY LA English DT Article DE ultrasound; ovarian cyclicity; reproductive dysfunction; hormones; progestagens ID OVARIAN FOLLICULAR CYSTS; GONADOTROPIN-RELEASING HORMONE; DAIRY-COWS; ENDOCRINE; SUPPRESSION; TOOL AB The Asian and African elephant populations in North America are not self-sustaining, and reproductive rates remain low. One problem identified from routine progestagen analyses is that some elephant females do not exhibit normal ovarian cycles. To better understand the extent of this problem, the Elephant TAG/SSP conducted a survey to determine the reproductive status of the captive population based on hormone and ultrasound evaluations. The survey response rates for facilities with Asian and African elephants were 81% and 71%, respectively, for the studbook populations, and nearly 100% for the SSP facilities. Of the elephants surveyed, 49% of Asian and 62% of African elephant females were being monitored for ovarian cyclicity via serum or urinary progestagen analyses on a weekly basis. Of these, 14% of Asian and 29% of African elephants either were not cycling at all or exhibited irregular cycles. For both species, ovarian inactivity was more prevalent in the older age categories (> 30 years); however, acyclicity was found in all age groups of African elephants. Fewer elephant females (similar to30%) had been examined by transrectal ultrasound to assess reproductive-tract integrity, and corresponding hormonal data were available for about three-quarters of these females. Within this subset, most (similar to75%) cycling females had normal reproductive-tract morphologies, whereas at least 70% of noncycling females exhibited some type of ovarian or uterine pathology. In summary, the survey results suggest that ovarian inactivity is a significant reproductive problem for elephants held in zoos, especially African elephants. To increase the fecundity of captive elephants, females should be bred at a young age, before reproductive pathologies occur. However, a significant number of older Asian elephants are still not being reproductively monitored. More significantly, many prime reproductive-age (10-30 years) African females are not being monitored. This lack of information makes it difficult to determine what factors affect the reproductive health of elephants, and to develop mitigating treatments to reinitiate reproductive cyclicity. (C) 2004 whey-Liss, Inc. C1 Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. Indianaplis Zoo, Dept Conservat & Sci, Indianapolis, IN USA. Oregon Zoo, Portland, OR USA. RP Brown, JL (reprint author), Conservat & Res Ctr, Dept Reprod Sci, 1500 Remount Rd,Natl Zool Pk, Front Royal, VA 22630 USA. EM jbrown@crc.si.edu NR 26 TC 26 Z9 27 U1 2 U2 18 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2004 VL 23 IS 4 BP 309 EP 321 DI 10.1002/zoo.20006 PG 13 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 848SR UT WOS:000223487900003 ER PT J AU Freeman, EW Weiss, E Brown, JL AF Freeman, EW Weiss, E Brown, JL TI Examination of the interrelationships of behavior, dominance status, and ovarian activity in captive Asian and African elephants SO ZOO BIOLOGY LA English DT Article DE behavioral profile; dominance status; ovarian cyclicity; management; progestagens ID LOXODONTA-AFRICANA; REPRODUCTIVE SUPPRESSION; ESTROGEN EXCRETION; DWARF MONGOOSES; MAXIMUS; ULTRASONOGRAPHY; PROGESTERONE; MANAGEMENT; CYCLICITY; CHEETAHS AB Ovarian inactivity has been identified in captive African (Loxodonta africana) and Asian (Elephas maximus) elephants and is thought to be mediated in part by social influences. Thus, a survey was conducted to determine how behavior and dominance status relate to each other and to ovarian cyclicity. For both Asian and African elephants, dominance status was positively correlated with relative size, age, temperament, disciplinary nature, and willingness to share novel objects. Relative size and temperament were also related to disciplinary nature toward herdmates. Behavior toward keepers was a good indicator of the willingness of elephants to follow commands, whereas sharing novel objects was positively correlated with object curiosity. Finally, dominance status, temperament, and disciplinary nature were all correlated with willingness to share. Comparisons of ovarian cyclicity status with behavior rankings were conducted only for African elephants because of the low number of noncycling Asian elephants surveyed. Overall, social status appeared to be the best predictor of ovarian activity in African elephants. Noncycling African elephant females ranked higher in the dominance hierarchy and gave more discipline to herdmates than cycling cohorts. It remains to be determined whether these are cause or effect relationships, but clearly it is important to understand how physical and social attributes impact physiological processes, such as reproduction. Captive management now needs to focus on optimizing social and environmental conditions to maximize reproductive potential in elephants. (C) 2004 Wiley-Liss, Inc. C1 Smithsonian Inst, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. Sedgwick Cty Zoo, Wichita, KS USA. RP Brown, JL (reprint author), Smithsonian Inst, Conservat & Res Ctr, Dept Reprod Sci, Natl Zool Pk, Front Royal, VA 22630 USA. EM jbrown@crc.si.edu NR 49 TC 32 Z9 34 U1 4 U2 37 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2004 VL 23 IS 5 BP 431 EP 448 DI 10.1002/zoo.20025 PG 18 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 867NX UT WOS:000224850400004 ER PT J AU Allen, ME Ullrey, DE AF Allen, ME Ullrey, DE TI Relationships among nutrition and reproduction and relevance for wild animals SO ZOO BIOLOGY LA English DT Article DE food restriction; energy; protein; minerals; vitamins; spermatogenesis ID VITAMIN-E-DEFICIENCY; MATERNAL UNDERNUTRITION; ACID-COMPOSITION; EGG-PRODUCTION; ASCORBIC-ACID; SELENIUM; GROWTH; SHEEP; DIETS; MICE AB This review discusses aspects of feeding ecology, nutrition, and dietary husbandry that are particularly relevant to reproductive success in wild animals. Emphasis has been placed on recently published literature. Special attention has been given to requirements for energy and protein and the unique roles of essential amino acids, essential fatty acids, calcium, phosphorus, zinc, copper, selenium, and vitamins A, C, D, and E. Information has been drawn from research with mammals, birds, reptiles, amphibians, and fish, including the domestic and laboratory species that play such a large role in elucidating mechanisms connecting nutrition and reproduction. (C) 2004 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Michigan State Univ, Comparat Nutr Grp, E Lansing, MI 48824 USA. RP Allen, ME (reprint author), 5320 Olney Laytonsville Rd, Olney, MD 20832 USA. EM meallennzp@aol.com NR 60 TC 18 Z9 18 U1 5 U2 38 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2004 VL 23 IS 6 BP 475 EP 487 DI 10.1002/zoo.20029 PG 13 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 886FD UT WOS:000226211400001 ER PT J AU Gomez, A Jewell, E Walker, SL Brown, JL AF Gomez, A Jewell, E Walker, SL Brown, JL TI Use of salivary steroid analyses to assess ovarian cycles in an Indian rhinoceros at the National Zoological Park SO ZOO BIOLOGY LA English DT Article DE hormones; estrus; androgens; estrogens; progestins ID DICEROS-BICORNIS; CERATOTHERIUM-SIMUM; WHITE RHINOCEROS; DICERORHINUS-SUMATRENSIS; MONACHUS-SCHAUINSLANDI; REPRODUCTIVE FUNCTION; SUMATRAN-RHINOCEROS; FECAL PROGESTERONE; ESTRONE SULFATE; PREGNANCY AB Saliva samples were collected from a female Indian rhinoceros (Rhinoceros unicornis) housed at the National Zoological Park, and ether-extracted for analyses of androgen, estrogen, and progestin metabolites to assess ovarian cycles. Analyses of both salivary androgens and estrogens were found to reliably monitor follicular activity. Although the temporal patterns of the two steroids were significantly correlated (r = 0.62; P < 0.05), they differed slightly. Salivary androgens increased earlier during the follicular phase, although both peaked at the same time in association with behavioral estrus. Based on salivary androgen profiles, the mean duration of the follicular phase was 11.4 days (ranged = 7-15 days; n = 17 cycles). Estrous cycle length, as measured by the time between consecutive androgen peaks, was 47.4 +/- 3.4 days (range = 37-86 days). Salivary progestin measurements were effective for monitoring luteal function. The mean duration of the luteal phase was 15.5 +/- 1.5 days (range = 10-23 days). In sum, assays were identified for measuring salivary steroids to assess ovarian function in Indian rhinoceroses. However, not all of the assay systems tested were effective, perhaps because of interfering matrix effects. Mate introductions in the Indian rhinoceros often require careful monitoring, and a technique for monitoring hormones in saliva could be an alternative to urine or fecal analyses for identifying estrus and timing breeding in this species. Such a technique would be particularly useful for situations in which it is difficult to collect uncontaminated urine and feces. (C) 2004 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. RP Brown, JL (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, 1500 Remount Rd, Front Royal, VA 22630 USA. EM jbrown@crc.si.edu NR 26 TC 14 Z9 15 U1 0 U2 6 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2004 VL 23 IS 6 BP 501 EP 512 DI 10.1002/zoo.20028 PG 12 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 886FD UT WOS:000226211400003 ER PT J AU Mclaughlin, PA Lemaitre, R AF Mclaughlin, PA Lemaitre, R TI The discovery of two new species of Lithopagurus Provenzano, 1968 (Crustacea, Decapoda, Anomura, Paguroidea, Paguridae) and the first records of the genus in the western Pacific SO ZOOSYSTEMA LA English DT Article DE Crustacea; Decapoda; Anomura; Paguridae; Lithopagurus; western Pacific; new species ID CRUISE AB Two new species of the hermit crab genus Lithopagurus Provenzano, 1968 are described and illustrated together with an illustrated and detailed diagnosis of the type species, L. yucatanicus Provenzano, 1968 that is included for comparative purposes. This genus, heretofore monotypic and known only from off the Atlantic coast of Mexico, is now reported from two widely separated Pacific areas, the Indonesian Kai Islands and the Fiji Islands. In having 13 pairs of gills and one pair of pleopods modified as gonopods, Lithopagurus is included in the Pylopaguropsis group within the family Paguridae, and would appear most closely allied to the monotypic Tomopaguroides Balss, 1912. Species of Lithopagurus are very characteristic, with large operculate or semioperculate right chelipeds, reduced and somewhat bulbous pleons; males with paired and modified second pleopods, but lacking all unpaired pleopods; females with only unpaired pleopods 2-4; and telsons without lateral indentations and with terminal margins lacking median clefts. Lithopagurus boucheti n. sp., from the Fiji Islands, is morphologically quite similar to its Atlantic counterpart, L. yucatanicus, whereas L. tribulomanus n. sp., from the Kai Islands, is very distinctive. All three now recognized species have been collected from relatively deep water, 146-540 m, but little is known about their habitats other than one specimen of L. yucatanicus reportedly was occupying a piece of lithistid sponge at the time of collection. C1 Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, Washington, DC 20013 USA. RP Mclaughlin, PA (reprint author), Western Washington Univ, Shannon Point Marine Ctr, 1900 Shannon Point Rd, Anacortes, WA 98221 USA. EM hermit@fidalgo.net; lemaitre.rafael@nmnh.si.edu NR 14 TC 2 Z9 2 U1 0 U2 1 PU PUBLICATIONS SCIENTIFIQUES DU MUSEUM, PARIS PI PARIS CEDEX 05 PA CP 39-57, RUE CUVIER, F-75231 PARIS CEDEX 05, FRANCE SN 1280-9551 J9 ZOOSYSTEMA JI Zoosystema PY 2004 VL 26 IS 3 BP 483 EP 494 PG 12 WC Zoology SC Zoology GA 863CN UT WOS:000224538100008 ER PT J AU Steiner, G Kabat, AR AF Steiner, G Kabat, AR TI Catalog of species-group names of Recent and fossil Scaphopoda (Mollusca) SO ZOOSYSTEMA LA English DT Article DE Mollusca; scaphopoda; nomenclature ID PACIFIC; INJURY; SYSTEM; COLOR; SEA AB This catalog lists names of Recent and fossil species-group taxa of the molluscan class Scaphopoda. Of a total of 1965 entries, 517 are attributed to valid Recent taxa, 816 to valid fossil taxa, 543 are invalid names, and 89 were subsequently excluded from the Scaphopoda. The authorship and complete bibliographic references are provided for each name. The original and current generic allocation, type locality, and type material depositories, as far as available, are provided. Synonyms, geographic distributions, and bathymetric ranges are provided for Recent taxa. Cross references to junior synonyms are based upon published opinions. Eight species taxa are newly synonymized herein: Dentalium tessellatum is a junior synonym of Entalinopsis habutae; Dentalium caudani is a junior synonym of Fissidentalium candidum; F. ergasticum, F. milneedwardsi, and F. scamnatum are junior synonyms of F. capillosum; F. exuberans is a junior synonym of F. paucicostatum; and Cadulus halius is a junior synonym of C podagrinus. Three subspecific taxa are synonymized with the respective nominate species: Antalis cerata tenax, Polyschides rushii arne, and Gadila agassizii hatterasensis. Further, eight new generic combinations are proposed: Paradentalium americanum n. comb., Coccodentalium cancellatum n. comb., Fissidentalium peruvianum n. comb., Pulsellum teres n. comb., Polyschides poculum n. comb., Polyschides foweyensis n. comb., Polyschides portoricensis n. comb., and Polyschides nitidus n. comb. Thirteen junior homonyms are renamed and listed in the appendix 1. C1 Univ Vienna, Inst Zool, A-1090 Vienna, Austria. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Steiner, G (reprint author), Univ Vienna, Inst Zool, Althanstr 14, A-1090 Vienna, Austria. EM gerhard.steiner@univie.ac.at; AlanKabat@aol.com OI Steiner, Gerhard/0000-0001-9845-1026 NR 77 TC 24 Z9 34 U1 1 U2 4 PU PUBLICATIONS SCIENTIFIQUES DU MUSEUM, PARIS PI PARIS CEDEX 05 PA CP 39-57, RUE CUVIER, F-75231 PARIS CEDEX 05, FRANCE SN 1280-9551 J9 ZOOSYSTEMA JI Zoosystema PY 2004 VL 26 IS 4 BP 549 EP 726 PG 178 WC Zoology SC Zoology GA 890XP UT WOS:000226544900001 ER PT J AU Zeng, T Wang, YH Chance, K Browell, EV Ridley, BA Atlas, EL AF Zeng, T Wang, YH Chance, K Browell, EV Ridley, BA Atlas, EL TI Widespread persistent near-surface ozone depletion at northern high latitudes in spring SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ARCTIC BOUNDARY-LAYER; POLAR SUNRISE; BRO CONCENTRATIONS; TROPOSPHERIC BRO; BROMINE; CHEMISTRY; MODEL; DESTRUCTION; RELEASE; EVENTS AB Springtime near-surface ozone depletion has been observed at northern high latitudes. Due to limited observations, the spatial and temporal extent of low O-3 concentrations near the surface is still unknown. A regional 3-D chemistry and transport model is applied to simulate surface O-3 depletion catalyzed by bromine radicals at northern high latitudes in March and April 2000. Satellite observations of BrO column by the ESA Global Ozone Monitoring Experiment (GOME) were processed to specify the BrO concentrations in the lower troposphere. In view of the GOME measurement and model uncertainties, the model results show an adequate agreement with the O-3 depletion events observed at two surface sites, Alert, Canada (82.5degreesN, 62.3degreesW) and Barrow, Alaska (71.3degreesN, 156.6degreesW), and by airborne in situ and DIAL instrument during the TOPSE experiments at northern high latitudes. Low O-3 events at Alert appear to be mostly driven by transport of O-3-poor air from high BrO regions. Model results indicate that low O-3 concentrations (<20 ppbv) near the surface cover similar to 60% of the northern high latitudes and that the depleted O-3 concentrations (<10 ppbv) cover similar to20% of the region in April. The high BrO events tend to be large-scale and persistent (1-2 weeks). We find that they are correlated with low temperature, a condition conducive for heterogeneous reactions on frozen snow or aerosol surfaces. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. RP Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM ywang@eas.gatech.edu RI Wang, Yuhang/B-5578-2014; Atlas, Elliot/J-8171-2015 NR 28 TC 38 Z9 38 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 31 PY 2003 VL 30 IS 24 AR 2298 DI 10.1029/2003GL018587 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 761HZ UT WOS:000187896600005 ER PT J AU Graves, GR AF Graves, GR TI Diagnoses of hybrid hummingbirds (Aves : Trochilidae). 12. Amazilia bangsi Ridgway, 1910, is an intrageneric hybrid, Amazilia tzacatl x Amazilia rutila SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID INTERGENERIC HYBRID AB Amazilia bangsi Ridgway, 1910, collected at Volcan de Miravalles, Costa Rica, is shown to be a hybrid between Amazilia tzacatl and Amazilia rutila. C1 Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, Washington, DC 20013 USA. RP Graves, GR (reprint author), Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, POB 37012, Washington, DC 20013 USA. NR 23 TC 0 Z9 0 U1 0 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 31 PY 2003 VL 116 IS 4 BP 847 EP 852 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 761VQ UT WOS:000187936500001 ER PT J AU Woodman, N AF Woodman, N TI A new small-eared shrew of the Cryptotis nigrescens-group from Colombia (Mammalia : Soricomorpha : Soricidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID INSECTIVORA AB Cryptotis colombiana Woodman & Timm, 1993 previously was known from few specimens from two isolated regions in the Cordillera Central and Cordillera Oriental of Colombia. Recent collecting in the northern Cordillera Central and review of older collections from the central Cordillera Oriental in the vicinity of Bogota yielded additional specimens that permit reevaluation of the two geographic populations of these small-eared shrews. Morphological and morphometrical studies indicate that the population inhabiting the Cordillera Oriental represents a distinct, previously unrecognized species that I describe herein as Cryptotis brachyonyx. Study of 54 specimens of shrews from the Cordillera Oriental in systematic collections in North America, South America, and Europe yielded only four specimens of the new species, all collected before 1926. The paucity of modern specimens suggests that C. brachyonyx may be extremely restricted in distribution, or possibly extinct. C1 USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Woodman, N (reprint author), USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. NR 30 TC 3 Z9 9 U1 0 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 31 PY 2003 VL 116 IS 4 BP 853 EP 872 PG 20 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 761VQ UT WOS:000187936500002 ER PT J AU Ng, PKL Manning, RB AF Ng, PKL Manning, RB TI On two new genera of pea crabs parasitic in holothurians (Crustacea : Decapoda : Brachyura : Pinnotheridae) from the Indo-West Pacific, with notes on allied genera SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID GENUS AB Two new genera of pea crabs of the family Pinnotheridae, Holotheres and Buergeres, members of which are parasites of sea cucumbers, are described from the Indo-West Pacific. Species of Holotheres are characterized by having all the dactyli of the walking legs of females short and subequal in length, with the spatuliform dactylus of the third maxilliped inserted very near or at the base of the propodus. Species of Buergeres are characterized by having the last dactyli of the walking legs of females elongate and longer than those of the other legs, with the subspatuliform dactylus of the third maxilliped inserted distinctly before the base of the propodus. Holotheres and Buergeres are compared to other genera whose members are associated with holothurians, Holothuriophilus Nauck, 1880, and Alain Manning, 1998 (obligate parasites); as well as Pinnaxodes Heller, 1865 (facultative parasites). C1 Natl Univ Singapore, Dept Sci Biol, Singapore 119260, Singapore. Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20560 USA. RP Manning, RB (reprint author), Natl Univ Singapore, Dept Sci Biol, Kent Ridge, Singapore 119260, Singapore. EM dbsngkl@nus.edu.sg RI Ng, Peter/J-7393-2012 NR 39 TC 14 Z9 16 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 31 PY 2003 VL 116 IS 4 BP 901 EP 919 PG 19 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 761VQ UT WOS:000187936500006 ER PT J AU Wang, J Liu, X Christopher, SA Reid, JS Reid, E Maring, H AF Wang, J Liu, X Christopher, SA Reid, JS Reid, E Maring, H TI The effects of non-sphericity on geostationary satellite retrievals of dust aerosols SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SCATTERING; PARTICLES AB Using data collected during the Puerto Rico Dust Experiment ( PRIDE), we examine the effect of non-spherical phase functions on dust aerosol retrievals from geostationary satellites. We utilize a statistical model based on Scanning Electron Micrograph (SEM) analysis of individual dust particles. Using T-matrix calculations and assuming that dust particles are randomly-orientated oblate spheroids we compute the dust phase function and scattering properties. Although the non-spherical function developed in this study compares well with the synthetic non-spherical phase functions [Liu et al., 2003], new retrievals using the non-spherical phase function only show slight improvement at scattering angles (Theta) from 110degrees similar to 150degrees, and become worse for Theta between 150degrees similar to 170degrees. However the retrievals are greatly improved at all angles when retrieval algorithms account for the combined effect of both spherical and non-spherical phase functions. C1 Univ Alabama, NSSTC, Dept Atmospher Sci, Huntsville, AL 35806 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Naval Res Lab, Marine Meteorol Div, Monterey, CA USA. Univ Miami, Div Marine & Atmospher Chem, Miami, FL 33152 USA. RP Wang, J (reprint author), Univ Alabama, NSSTC, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35806 USA. EM wangjun@nsstc.uah; sundar@nsstc.uah.edu RI Christopher, Sundar/E-6781-2011; Reid, Jeffrey/B-7633-2014; Liu, Xiong/P-7186-2014; Wang, Jun/A-2977-2008 OI Reid, Jeffrey/0000-0002-5147-7955; Liu, Xiong/0000-0003-2939-574X; Wang, Jun/0000-0002-7334-0490 NR 17 TC 34 Z9 34 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 30 PY 2003 VL 30 IS 24 AR 2293 DI 10.1029/2003GL018697 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 761HX UT WOS:000187896400004 ER PT J AU Furuya, RS Shinnaga, H Nakanishi, K Momose, M Saito, M AF Furuya, RS Shinnaga, H Nakanishi, K Momose, M Saito, M TI A giant flare on a T Tauri star observed at millimeter wavelengths SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE radio continuum : stars; stars : flare; stars : individual (GMR-A); stars : pre-main sequence; techniques : interferometric ID EMISSION MEASURE; STELLAR FLARES; MASS FUNCTION; ORION NEBULA; TEMPERATURE; CLUSTER; SOLAR AB We have conducted multi-epoch synthesis imaging of lambda = 2 and 3 millimeter (mm) continuum emission and near-infrared K-band (2.2 mum) imaging of a flare event in 2003 January that occurred on the young stellar object GMR-A, which is suggested to be a weak-line T Tauri star in the Orion cluster. Our turn data showed that the flare activity lasted for at least over 13 days, whereas the K-band magnitude did not change during this event. In addition, we have succeeded in detecting short time variations of flux on time scales of 15 minutes. The total energy of the flare is estimated to be similar to10(35-36)erg, which makes it one of the most energetic flares reported to date. Comparing the mm continuum luminosities with reported X-ray luminosities, we conclude that the mm flare was similar in nature to solar and other stellar flares. Our results will be a crucial step toward understanding magnetically induced stellar surface activities in T Tauri stars. C1 Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Harvard Smithsonian Ctr Astrophys, Hilo, HI 96721 USA. Nobeyama Radio Observ, Nagano 3841305, Japan. Ibaraki Univ, Inst Astrophys & Planetary Sci, Mito, Ibaraki 3108512, Japan. RP CALTECH, Div Phys Math & Astron, MS 105-24, Pasadena, CA 91125 USA. EM rsf@astro.caltech.edu NR 16 TC 11 Z9 11 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 DEC 25 PY 2003 VL 55 IS 6 BP L83 EP L87 DI 10.1093/pasj/55.6.L83 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758EB UT WOS:000187619200004 ER PT J AU Narayan, R Igumenshchev, IV Abramowicz, MA AF Narayan, R Igumenshchev, IV Abramowicz, MA TI Magnetically arrested disk: An energetically efficient accretion flow SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; galaxies : nuclei; galaxies : quasars : general magnetic fields; magnetohydrodynamics : MHD ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE; EXTRACTING ENERGY; COLLAPSING STAR; FIELD; EVOLUTION; MATTER AB We consider an accretion flow model originally proposed by Bisnovatyi-Kogan and Ruzmaikin (1974), which has been confirmed in recent 3D MHD simulations. In the model, the accreting gas drags in a strong poloidal magnetic field to the center such that the accumulated field disrupts the axisymmetric accretion flow at a relatively large radius. Inside the disruption radius, the gas accretes as discrete blobs or streams with a velocity much less than the free-fall velocity. Almost the entire rest mass energy of the gas is released as heat, radiation and mechanical/magnetic energy. Even for a non-rotating black hole, the efficiency of converting mass to energy is of order 50% or higher. The model is thus a practical analog of an idealized engine proposed by Geroch and Bekenstein. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Rochester, Laser Energet Lab, Rochester, NY 14623 USA. Gothenburg Univ, Dept Astron & Astrophys, S-41296 Gothenburg, Sweden. Chalmers, S-41296 Gothenburg, Sweden. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rnarayan@cfa.harvard.edu; iigu@lle.rochester.edu; marek@fy.chalmers.se OI Narayan, Ramesh/0000-0002-1919-2730 NR 27 TC 113 Z9 113 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 DEC 25 PY 2003 VL 55 IS 6 BP L69 EP L72 DI 10.1093/pasj/55.6.L69 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758EB UT WOS:000187619200001 ER PT J AU Albright, LB Woodburne, MO Case, JA Chaney, DS AF Albright, LB Woodburne, MO Case, JA Chaney, DS TI A leatherback sea turtle from the Eocene of Antarctica: Implications for antiquity of gigantothermy in Dermochelyidae SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID CORIACEA; PSEPHOPHORUS; TEMPERATURES; EVOLUTION; ISLAND; MA C1 Museum No Arizona, Dept Geol, Flagstaff, AZ 86001 USA. Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. St Marys Coll, Dept Biol, Moraga, CA 94575 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Albright, LB (reprint author), Museum No Arizona, Dept Geol, Flagstaff, AZ 86001 USA. NR 37 TC 12 Z9 12 U1 2 U2 9 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 DEC 24 PY 2003 VL 23 IS 4 BP 945 EP 949 DI 10.1671/1886-19 PG 5 WC Paleontology SC Paleontology GA 760PR UT WOS:000187843300019 ER PT J AU Arnold, AE Mejia, LC Kyllo, D Rojas, EI Maynard, Z Robbins, N Herre, EA AF Arnold, AE Mejia, LC Kyllo, D Rojas, EI Maynard, Z Robbins, N Herre, EA TI Fungal endophytes limit pathogen damage in a tropical tree SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID ARBUSCULAR MYCORRHIZAL FUNGI; PLANT-PATHOGEN; PUERTO-RICO; HOST; DIVERSITY; FOREST; RESISTANCE; SYMBIOSIS; MUTUALISM; LEAVES AB Every plant species examined to date harbors endophytic fungi within its asymptomatic aerial tissues, such that endophytes represent a ubiquitous, yet cryptic, component of terrestrial plant communities. Fungal endophytes associated with leaves of woody angiosperms are especially diverse; yet, fundamental aspects of their interactions with hosts are unknown. In contrast to the relatively species-poor endophytes that are vertically transmitted and act as defensive mutualists of some temperate grasses, the diverse, horizontally transmitted endophytes of woody angiosperms are thought to contribute little to host defense. Here, we document high diversity, spatial structure, and host affinity among foliar endophytes associated with a tropical tree (Theobroma cacao, Malvaceae) across lowland Panama. We then show that inoculation of endophyte-free leaves with endophytes isolated frequently from naturally infected, asymptomatic hosts significantly decreases both leaf necrosis and leaf mortality when T. cacao seedlings are challenged with a major pathogen (Phytophthora sp.). In contrast to reports of fungal inoculation inducing systemic defense, we found that protection was primarily localized to endophyte-infected tissues. Further, endophyte-mediated protection was greater in mature leaves, which bear less intrinsic defense against fungal pathogens than do young leaves. In vitro studies suggest that host affinity is mediated by leaf chemistry, and that protection may be mediated by direct interactions of endophytes with foliar pathogens. Together, these data demonstrate the capacity of diverse, horizontally transmitted endophytes of woody angiosperms to play an important but previously unappreciated role in host defense. C1 Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Arnold, AE (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA. EM aearnold@duke.edu NR 66 TC 468 Z9 532 U1 23 U2 201 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD DEC 23 PY 2003 VL 100 IS 26 BP 15649 EP 15654 DI 10.1073/pnas.2533483100 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 757GL UT WOS:000187554600066 PM 14671327 ER PT J AU Collin, R Cipriani, R AF Collin, R Cipriani, R TI Dollo's law and the re-evolution of shell coiling SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE gastropod; calyptraeid; atavism; evolutionary reversal ID CALYPTRAEID GASTROPODS; CHARACTERS; GEOMETRY AB Gastropods have lost the quintessential snail feature, the coiled shell, numerous times in evolution. In many cases these animals have developed a limpet morphology with a cap-shaped shell and a large foot. Limpets thrive in marginal habitats such as hydrothermal vents, the high-energy rocky intertidal areas and fresh water, but they are considered to be evolutionary dead-ends, unable to re-evolve a coiled shell and therefore unable to give rise to the diversity seen among coiled snails. The re-evolution of a coiled shell, or any complex character, is considered unlikely or impossible (Dollo's law) because the loss of the character is followed by the loss of the genetic architecture and developmental mechanisms that underlie that character. Here, we quantify the level of coiling in calyptraeids, a family of mostly uncoiled limpets, and show that coiled shells have re-evolved at least once within this family. These results are the first demonstration, to our knowledge, of the re-evolution of coiling in a gastropod, and show that the developmental features underlying coiling have not been lost during 20-100 Myr of uncoiled evolutionary history. This is the first example of the re-evolution of a complex character via a change in developmental timing (heterochrony) rather than a change in location of gene expression (heterotopy). C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Simon Bolivar, Dept Estudios Ambientales, Caracas 1080, Venezuela. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010 NR 23 TC 57 Z9 58 U1 4 U2 29 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 DEC 22 PY 2003 VL 270 IS 1533 BP 2551 EP 2555 DI 10.1098/rspb.2003.2517 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 762NW UT WOS:000187989900003 PM 14728776 ER PT J AU Perez, ID Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Cui, W Dowdall, C Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, L Gaidos, JA Gibbs, K Gammell, S Hall, J Hall, TA Hillas, AM Holder, J Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F LeBohec, S Linton, ET Lloyd-Evans, J Moriarty, P Muller, D Nagai, TN Ong, RA Page, M Pallassini, R Petry, D Power-Mooney, B Quinn, J Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Vassiliev, VV Wakely, SP Walker, G Weekes, TC AF Perez, ID Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Cui, W Dowdall, C Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, L Gaidos, JA Gibbs, K Gammell, S Hall, J Hall, TA Hillas, AM Holder, J Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F LeBohec, S Linton, ET Lloyd-Evans, J Moriarty, P Muller, D Nagai, TN Ong, RA Page, M Pallassini, R Petry, D Power-Mooney, B Quinn, J Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Vassiliev, VV Wakely, SP Walker, G Weekes, TC TI Search for high-energy gamma rays from an X-ray-selected blazar sample SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (RGB J0214+517, RGB J1117+202, RGB J1725+118, IES 0033+595, 1ES 0120+340; 1ES 0229+200, 1ES 0806+524, 1ES 1426+428, 1ES 1553+113, 1ES 1959+650); gamma rays : observations ID ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; TEV ENERGIES; EMISSION; RADIATION; TELESCOPE; FLARE; MARKARIAN-501; ABSORPTION; DISCOVERY AB Our understanding of blazars has been greatly increased in recent years by extensive multiwavelength observations, particularly in the radio, X-ray, and gamma-ray regions. Over the past decade the Whipple 10 m telescope has contributed to this with the detection of five BL Lacertae objects at very high gamma-ray energies. The combination of multiwavelength data has shown that blazars follow a well-defined sequence in terms of their broadband spectral properties. Together with providing constraints on emission models, this information has yielded a means by which potential sources of TeV emission may be identified and predictions made as to their possible gamma-ray flux. We have used the Whipple telescope to search for TeV gamma-ray emission from eight objects selected from a list of such candidates. No evidence has been found for very high energy emission from the objects in our sample, and upper limits have been derived for the mean gamma-ray flux above 390 GeV. These flux upper limits are compared with the model predictions, and the implications of our results for future observations are discussed. C1 Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland, Dept Phys, Dublin 4, Ireland. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. De Pauw Univ, Dept Phys, Greencastle, IN 46135 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Cork Inst Technol, Dept Phys, Cork, Ireland. RP Perez, ID (reprint author), Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. RI Hall, Jeter/F-6108-2013; Hall, Jeter/E-9294-2015; OI Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383 NR 48 TC 20 Z9 20 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 909 EP 917 DI 10.1086/379544 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500015 ER PT J AU Bloom, JS Fox, D van Dokkum, PG Kulkarni, SR Berger, E Djorgovski, SG Frail, DA AF Bloom, JS Fox, D van Dokkum, PG Kulkarni, SR Berger, E Djorgovski, SG Frail, DA TI The first two host galaxies of X-ray flashes: XRF 011030 and XRF 020427 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; X-rays : bursts ID HUBBLE-SPACE-TELESCOPE; GAMMA-RAY; GRB 990123; BURSTS; EMISSION; MODEL AB Given the paucity of empirical constraints, the nature of the newly recognized phenomena called X-ray. ashes (XRFs) has been an open question. However, with the recent detections of radio and X-ray afterglow it is finally possible to study the large- and small-scale environments of XRFs. We present Chandra, Hubble Space Telescope (HST), and Keck observations of the fields of XRFs 011030 and 020427. Astrometric comparisons of the X-ray transient positions and the HST images reveal the XRFs to be associated with faint blue galaxies. Photometric evidence of these putative hosts suggests that these two XRFs originated from redshifts less than z similar to 3.5, and thus cannot be due to GRBs at very high redshifts. In both host-burst offsets and host properties, these XRFs could have been drawn from distributions similar to those measured of gamma-ray bursts (GRBs). We conclude with a discussion of the implications of this XRF-GRB host connection for the possible progenitors of XRFs. C1 Harvard Smithsonian Ctr Astrophys, MC 20, Cambridge, MA 02138 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. CALTECH, Palomar Observ, Pasadena, CA 91125 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Bloom, JS (reprint author), Harvard Smithsonian Ctr Astrophys, MC 20, 60 Garden St, Cambridge, MA 02138 USA. NR 46 TC 29 Z9 29 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 957 EP 963 DI 10.1086/379310 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500019 ER PT J AU Di Stefano, R Kong, AKH VanDalfsen, ML Harris, WE Murray, SS Delain, KM AF Di Stefano, R Kong, AKH VanDalfsen, ML Harris, WE Murray, SS Delain, KM TI X-ray point sources in the Sombrero galaxy: Very soft sources, the globular cluster/low-mass X-ray binary connection, and an overview SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M104); X-rays : binaries; X-rays : galaxies ID LARGE MAGELLANIC CLOUD; NEBULA LUMINOSITY FUNCTION; NUCLEAR ACCRETION; SOURCE CATALOGS; CHANDRA; M31; DISCOVERY; CAL-83; POPULATION; REMNANTS AB We report on the population of point sources discovered during an 18.5 ks Chandra ACIS-S observation of the Sombrero galaxy. We present the luminosity function and the spectra of the six brightest sources, consider correlations with globular clusters (GCs) and with planetary nebulae, and study the galaxy's population of very soft sources. We detected 122 sources. Twenty-two sources are identified as very soft; of these, five appear to be classical luminous supersoft X-ray sources (SSSs), while 17 may belong to the slightly harder class referred to as quasi-soft (QSSs). There is an overdensity of very soft sources within 2 kpc of the nucleus, which is itself the brightest X-ray source. Very soft sources are also found in the disk and halo, with one QSS in a globular cluster (GC). This source is somewhat harder than most SSSs; the energy distribution of its photons is consistent with what is expected from an accreting intermediate-mass black hole. Several sources in the Sombrero's halo are good candidates for SSS models in which the accretor is a nuclear-burning white dwarf. In total, 32 X-ray sources are associated with GCs. The majority of sources with luminosity greater than 10(38) ergs s(-1) are in GCs. These results for M104, an Sa galaxy, are similar to what has been found for elliptical galaxies and for the late-type spiral M31. We find that those optically bright GCs with X-ray sources house only the brightest X-ray sources. We find that, in common with other galaxies, there appears to be a positive connection between young (metal-rich) GCs and X-ray sources but that the brightest X-ray sources are equally likely to be in metal-poor GCs. The luminosity function of X-ray sources in GCs has a cut-off near the Eddington luminosity for a 1.4 M. object. We propose a model that can explain the trends seen in the data sets from the Sombrero and other galaxies. Thermal timescale mass transfer can occur in some of the younger clusters in which the turnoff mass is slightly greater than 0.8M.; multiplicity may play a role in some of the most massive clusters; accretion from giant stars may be the dominant mechanism in some older, less massive and less centrally concentrated clusters. Key elements of the model can be tested. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 47 TC 31 Z9 31 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 1067 EP 1081 DI 10.1086/379245 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500028 ER PT J AU Kim, WT Ostriker, EC Stone, JM AF Kim, WT Ostriker, EC Stone, JM TI Magnetorotationally driven galactic turbulence and the formation of giant molecular clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; instabilities; ISM : kinematics and dynamics; ISM : magnetic fields; MHD; stars : formation ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; WEAKLY MAGNETIZED DISKS; LOCAL SHEAR INSTABILITY; SPIRAL DENSITY WAVE; 2 SPACE DIMENSIONS; H-II REGIONS; GRAVITATIONAL COLLAPSE; INTERSTELLAR-MEDIUM; ACCRETION DISKS; STAR-FORMATION AB Giant molecular clouds (GMCs), where most stars form, may originate from self-gravitating instabilities in the interstellar medium. Using local three-dimensional magnetohydrodynamic simulations, we investigate ways in which galactic turbulence associated with the magnetorotational instability (MRI) may influence the formation and properties of these massive, self-gravitating clouds. Our disk models are vertically stratified with both gaseous and stellar gravity and subject to uniform shear corresponding to a. at rotation curve. Initial magnetic fields are assumed to be weak and purely vertical. For simplicity, we adopt an isothermal equation of state with sound speed c(s) = 7 km s(-1). We find that MRI-driven turbulence develops rapidly, with the saturated-state Shakura & Sunyaev parameter alpha similar to 0.15-0.3 dominated by Maxwell stresses. Many of the dimensionless characteristics of the turbulence (e.g., the ratio of the Maxwell to Reynolds stresses) are similar to results from previous MRI studies of accretion disks, hence insensitive to the degree of vertical disk compression, shear rate, and the presence of self-gravity-although self-gravity enhances fluctuation amplitudes slightly. The density-weighted velocity dispersions in non- or weakly self-gravitating disks are sigma(x) similar to sigma(y) similar to (0.4-0.6)c(s) and sigma(z) similar to (0.2-0.3)c(s), suggesting that MRI can contribute significantly to the observed level of galactic turbulence. The saturated-state magnetic field strength (β) over bar similar to 2 muG is similar to typical galactic values. When self-gravity is strong enough, MRI-driven high-amplitude density perturbations are swing-amplified to form Jeans-mass (similar to10(7) M.) bound clouds. Compared to previous unmagnetized or strongly magnetized disk models, the threshold for nonlinear instability in the present models occurs for surface densities at least 50% lower, corresponding to the Toomre parameter Q(th) similar to 1.6. We present evidence that self-gravitating clouds like GMCs formed under conditions similar to our models can lose much of their original spin angular momenta by magnetic braking, preferentially via fields threading nearly perpendicularly to their spin axes. Finally, we discuss the present results within the larger theoretical and observational context, outlining directions for future study. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Harvard Univ, Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. Univ Cambridge, DAMTP, Cambridge CB3 9EW, England. RP Kim, WT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 68 TC 66 Z9 66 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 DEC 20 PY 2003 VL 599 IS 2 BP 1157 EP 1172 DI 10.1086/379367 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500033 ER PT J AU Keto, E AF Keto, E TI The formation of massive stars by accretion through trapped hypercompact HII regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; HII regions; stars : formation ID H-II REGIONS; RECOMBINATION LINE OBSERVATIONS; IRAS POINT SOURCES; CONTINUUM OBSERVATIONS; FORMING REGION; PHYSICAL-PROPERTIES; MOLECULAR CLOUDS; VLA OBSERVATIONS; STELLAR MODELS; MAIN-SEQUENCE AB The formation of massive stars may take place at relatively low accretion rates over a long period of time if the accretion can continue past the onset of core hydrogen ignition. The accretion may continue despite the formation of an ionized H II region around the star if the H II region is small enough that the gravitational attraction of the star dominates the thermal pressure of the H II region. The accretion may continue despite radiation pressure acting against dust grains in the molecular gas if the momentum of the accretion flow is sufficient to push the dust grains through a narrow zone of high dust opacity at the ionization boundary and into the H II region where the dust is sublimated. This model of massive star formation by continuing accretion predicts a new class of gravitationally trapped, long-lived, hypercompact H II regions. The observational characteristics of the trapped hypercompact H II regions can be predicted for comparison with observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 57 TC 120 Z9 120 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 1196 EP 1206 DI 10.1086/379545 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500036 ER PT J AU Mazzali, PA Deng, JS Tominaga, N Maeda, K Nomoto, K Matheson, T Kawabata, KS Stanek, KZ Garnavich, PM AF Mazzali, PA Deng, JS Tominaga, N Maeda, K Nomoto, K Matheson, T Kawabata, KS Stanek, KZ Garnavich, PM TI The type Ic hypernova SN 2003dh/GRB 030329 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; nuclear reactions, nucleosynthesis; abundances supernovae : general; supernovae : individual (SN 2003dh) ID GAMMA-RAY BURST; 25 APRIL 1998; OPTICAL AFTERGLOW; SN 1998BW; SUPERNOVA; SPECTRA; NUCLEOSYNTHESIS; GRB-011121; EXPLOSIONS; DISCOVERY AB The spectra of SN 2003dh, identified in the afterglow of GRB 030329, are modeled using radiation transport codes. It is shown that SN 2003dh had a high explosion kinetic energy (similar to4 x 10(52) ergs in spherical symmetry), making it one of the most powerful hypernovae observed so far and supporting the case for association between hypernovae and gamma-ray bursts. However, the light curve derived from fitting the spectra suggests that SN 2003dh was not as bright as SN 1998bw, ejecting only similar to0.35 M. of (56)Ni. The spectra of SN 2003dh resemble those of SN 1998bw around maximum, but later they look more like those of the less energetic hypernova SN 1997ef. The spectra and the inferred light curve can be modeled adopting a density distribution similar to that used for SN 1998bw at v < 25,000 km s(-1) but more like that of SN 1997ef at lower velocities. The mass of the ejecta is similar to 8 M., somewhat less than in the other two hypernovae. The progenitor must have been a massive star (M similar to 35-40 M.), as for other hypernovae. The need to combine different one-dimensional explosion models strongly indicates that SN 2003dh was an asymmetric explosion. C1 Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NAOJ, Opt & Infrared Astron Div, Tokyo 1818588, Japan. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. RP Mazzali, PA (reprint author), Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. EM mazzali@ts.astro.it; deng@astron.s.u-tokyo.ac.jp; ntominaga@astron.s.u-tokyo.ac.jp; maeda@astron.s.u-tokyo.ac.jp; nomoto@astron.s.u-tokyo.ac.jp; tmatheson@cfa.harvard.edu; koji.kawabata@nao.ac.jp; kstanek@cfa.harvard.edu; pgarnavi@miranda.phys.nd.edu RI Nomoto, Ken'ichi/A-4393-2011 NR 27 TC 108 Z9 108 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP L95 EP L98 DI 10.1086/381259 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EE UT WOS:000187452200011 ER PT J AU Perlman, ES Harris, DE Biretta, JA Sparks, WB Macchetto, FD AF Perlman, ES Harris, DE Biretta, JA Sparks, WB Macchetto, FD TI Month-timescale optical variability in the M87 jet SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : general; galaxies : active; galaxies : individual (M87); galaxies : jets; magnetic fields; radiation mechanisms : nonthermal ID BL LACERTAE OBJECT; X-RAY VARIABILITY; SPACE-TELESCOPE OBSERVATIONS; ACTIVE GALACTIC NUCLEI; PKS 2155-304; EMISSION; BLAZARS; RESOLUTION AB A previously inconspicuous knot in the M87 jet has undergone a dramatic outburst and now exceeds the nucleus in optical and X-ray luminosity. Monitoring of M87 with the Hubble Space Telescope and Chandra X-Ray Observatory during 2002-2003, has found month-timescale optical variability in both the nucleus and HST-1, a knot in the jet 0."82 from the nucleus. We discuss the behavior of the variability timescales as well as spectral energy distribution of both components. In the nucleus, we see nearly energy-independent variability behavior. Knot HST-1, however, displays weak energy dependence in both X-ray and optical bands but with nearly comparable rise/decay timescales at 220 nm and 0.5 keV. The flaring region of HST-1 appears stationary over 8 months of monitoring. We consider various emission models to explain the variability of both components. The flares we see are similar to those seen in blazars, albeit on longer timescales, and so could, if viewed at smaller angles, explain the extreme variability properties of those objects. C1 Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. European Space Agcy, ESTEC, Space Telescope Div, Noordwijk, Netherlands. RP Perlman, ES (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. OI Perlman, Eric/0000-0002-3099-1664 NR 24 TC 55 Z9 55 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP L65 EP L68 DI 10.1086/381191 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EE UT WOS:000187452200004 ER PT J AU Zezas, A Hernquist, L Fabbiano, G Miller, J AF Zezas, A Hernquist, L Fabbiano, G Miller, J TI NGC 4261 and NGC 4697: Rejuvenated elliptical galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : individual (NGC 4261, 3C 270) galaxies : interactions; X-rays : binaries; X-rays : galaxies ID SPACE-TELESCOPE IMAGES; CHANDRA OBSERVATIONS; STELLAR POPULATIONS; MERGER REMNANTS; SHELL GALAXIES; TRANSFORMATIONS; MORPHOLOGIES; PROGENITORS; GASDYNAMICS; POTENTIALS AB Chandra images present evidence of a nonuniform spatial distribution of discrete X-ray sources in the elliptical galaxy NGC 4261. This nonuniform distribution is inconsistent with the optical morphology of NGC 4261 at greater than a 99.9% confidence level. Similar evidence is seen in one more elliptical galaxy (NGC 4697; 98% confidence level) out of five cases we investigated. NGC 4261 and NGC 4697 have old stellar populations (9-15 Gyr) and fine-structure parameters of 1 and 0, respectively, suggesting that no recent merging activity occurred. On the basis of simulations of galaxy interactions, we propose that the X-ray sources responsible for the nonuniform distribution are associated with young stellar populations, related to the rejuvenating fallback of material in tidal tails onto a relaxed merger remnant or to shock-induced star formation along the tidal tails. 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 40 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 DEC 20 PY 2003 VL 599 IS 2 BP L73 EP L77 DI 10.1086/380895 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EE UT WOS:000187452200006 ER PT J AU Meggers, BJ AF Meggers, BJ TI Revisiting Amazonia circa 1492 SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Meggers, BJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012,MRC-112, Washington, DC 20013 USA. EM meggers.betty@nmnh.si.edu NR 14 TC 13 Z9 14 U1 1 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD DEC 19 PY 2003 VL 302 IS 5653 BP 2067 EP 2067 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 755CB UT WOS:000187385200019 PM 14684803 ER PT J AU Povich, MS Raymond, JC Jones, GH Uzzo, M Ko, YK Feldman, PD Smith, PL Marsden, BG Woods, TN AF Povich, MS Raymond, JC Jones, GH Uzzo, M Ko, YK Feldman, PD Smith, PL Marsden, BG Woods, TN TI Doubly ionized carbon observed in the plasma tail of comet Kudo-Fujikawa SO SCIENCE LA English DT Article ID BETA-PICTORIS; SOLAR; DUST; CO AB Comet C/2002 X5 (Kudo-Fujikawa) was observed near its perihelion of 0.19 astronomical unit by the Ultraviolet Coronagraph Spectrometer aboard the Solar and Heliospheric Observatory spacecraft. Images of the comet reconstructed from high-resolution spectra reveal a quasi-spherical cloud of neutral hydrogen and a variable tail of C+ and C2+ that disconnects from the comet and subsequently regenerates. The high abundance of C2+ and C+, at least 24% relative to water, cannot be explained by photodissociation of carbon monoxide and is instead attributed to the evaporation and subsequent photoionization of atomic carbon from organic refractory compounds present in the cometary dust grains. This result serves to strengthen the connection between comets and the material from which the Solar System formed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. RP Povich, MS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Jones, Geraint/C-1682-2008; OI Jones, Geraint/0000-0002-5859-1136 NR 21 TC 17 Z9 17 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 DEC 12 PY 2003 VL 302 IS 5652 BP 1949 EP 1952 DI 10.1126/science.1092142 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 752NL UT WOS:000187174000056 PM 14671299 ER PT J AU Bajcsy, M Zibrov, AS Lukin, MD AF Bajcsy, M Zibrov, AS Lukin, MD TI Stationary pulses of light in an atomic medium SO NATURE LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; NONLINEAR OPTICS; ULTRASLOW; ENTANGLEMENT; COHERENCE; STORAGE; PHOTONS; GAS AB Physical processes that could facilitate coherent control of light propagation are under active exploration(1-5). In addition to their fundamental interest, these efforts are stimulated by practical possibilities, such as the development of a quantum memory for photonic states(6 - 8). Controlled localization and storage of photonic pulses may also allow novel approaches to manipulating of light via enhanced nonlinear optical processes(9). Recently, electromagnetically induced transparency(10) was used to reduce the group velocity of propagating light pulses(11,12) and to reversibly map propagating light pulses into stationary spin excitations in atomic media(13 - 16). Here we describe and experimentally demonstrate a technique in which light propagating in a medium of Rb atoms is converted into an excitation with localized, stationary electromagnetic energy, which can be held and released after a controllable interval. Our method creates pulses of light with stationary envelopes bound to an atomic spin coherence, offering new possibilities for photon state manipulation and nonlinear optical processes at low light levels. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. PN Lebedev Phys Inst, Moscow 117924, Russia. RP Lukin, MD (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Zibrov, Alexander/G-7419-2014 NR 30 TC 380 Z9 393 U1 3 U2 29 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 11 PY 2003 VL 426 IS 6967 BP 638 EP 641 DI 10.1038/nature02176 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 752DY UT WOS:000187132800034 PM 14668857 ER PT J AU Matheson, T Garnavich, PM Stanek, KZ Bersier, D Holland, ST Krisciunas, K Caldwell, N Berlind, P Bloom, JS Bolte, M Bonanos, AZ Brown, MJI Brown, WR Calkins, ML Challis, P Chornock, R Echevarria, L Eisenstein, DJ Everett, ME Filippenko, AV Flint, K Foley, RJ Freedman, DL Hamuy, M Harding, P Hathi, NP Hicken, M Hoopes, C Impey, C Jannuzi, BT Jansen, RA Jha, S Kaluzny, J Kannappan, S Kirshner, RP Latham, DW Lee, JC Leonard, DC Li, W Luhman, KL Martini, P Mathis, H Maza, J Megeath, ST Miller, LR Minniti, D Olszewski, EW Papenkova, M Phillips, MM Pindor, B Sasselov, DD Schild, R Schweiker, H Spahr, T Thomas-Osip, J Thompson, I Weisz, D Windhorst, R Zaritsky, D AF Matheson, T Garnavich, PM Stanek, KZ Bersier, D Holland, ST Krisciunas, K Caldwell, N Berlind, P Bloom, JS Bolte, M Bonanos, AZ Brown, MJI Brown, WR Calkins, ML Challis, P Chornock, R Echevarria, L Eisenstein, DJ Everett, ME Filippenko, AV Flint, K Foley, RJ Freedman, DL Hamuy, M Harding, P Hathi, NP Hicken, M Hoopes, C Impey, C Jannuzi, BT Jansen, RA Jha, S Kaluzny, J Kannappan, S Kirshner, RP Latham, DW Lee, JC Leonard, DC Li, W Luhman, KL Martini, P Mathis, H Maza, J Megeath, ST Miller, LR Minniti, D Olszewski, EW Papenkova, M Phillips, MM Pindor, B Sasselov, DD Schild, R Schweiker, H Spahr, T Thomas-Osip, J Thompson, I Weisz, D Windhorst, R Zaritsky, D TI Photometry and spectroscopy of GRB 030329 and its associated supernova 2003dh: The first two months SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : distances and redshifts; gamma rays : bursts; supernovae : general; supernovae : individual (SN 2003dh) ID GAMMA-RAY BURST; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; OPTICAL AFTERGLOW; STAR-FORMATION; ULTRAVIOLET EXTINCTION; IMAGE SUBTRACTION; MAGELLANIC CLOUDS; CCD PHOTOMETRY; HOST GALAXIES; LIGHT-CURVE AB We present extensive optical and infrared photometry of the afterglow of gamma-ray burst (GRB) 030329 and its associated supernova (SN) 2003dh over the first two months after detection (2003 March 30-May 29 UT). Optical spectroscopy from a variety of telescopes is shown and, when combined with the photometry, allows an unambiguous separation between the afterglow and SN contributions. The optical afterglow of the GRB is initially a power-law continuum but shows significant color variations during the first week that are unrelated to the presence of an SN. The early afterglow light curve also shows deviations from the typical power-law decay. An SN spectrum is first detectable similar to7 days after the burst and dominates the light after similar to11 days. The spectral evolution and the light curve are shown to closely resemble those of SN 1998bw, a peculiar Type Ic SN associated with GRB 980425, and the time of the SN explosion is close to the observed time of the GRB. It is now clear that at least some GRBs arise from core-collapse SNe. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Carnegie Inst Sci, Las Campanas Observ, La Serena, Chile. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. FL Whipple Observ, Amado, AZ 85645 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Univ Arizona, Steward Observ, Tucson, AZ 85718 USA. Planetary Sci Inst, Tucson, AZ 85705 USA. Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. Carnegie Observ, Pasadena, CA 91101 USA. Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Massachusetts, Five Coll Astron Observ, Amherst, MA 01003 USA. Univ Chile, Dept Astron, Santiago, Chile. Pontificia Univ Catolica Chile, Santiago 22, Chile. Princeton Univ Observ, Princeton, NJ 08544 USA. WIYN Consortium Inc, Tucson, AZ 85719 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tmatheson@cfa.harvard.edu; pgarnavi@miranda.phys.nd.edu; kstanek@cfa.harvard.edu; dbersier@cfa.harvard.edu; sholland@milkyway.gsfc.nasa.gov; kevin@ctiosz.ctio.noao.edu; ncaldwell@cfa.harvard.edu; pberlind@cfa.harvard.edu; jbloom@cfa.harvard.edu; bolte@ucolick.org; abonanos@cfa.harvard.edu; mbrown@noao.edu; wbrown@cfa.harvard.edu; mcalkins@cfa.harvard.edu; pchallis@cfa.harvard.edu; chornock@astron.berkeley.edu; luis.echevarria@asu.edu; eisenste@as.arizona.edu; everett@psi.edu; alex@astron.berkeley.edu; flint@dtm.ciw.edu; rfoley@astron.berkeley.edu; dfreedman@cfa.harvard.edu; mhamuy@ociw.edu; harding@billabong.astr.cwru.edu; nphathi@asu.edu; mhicken@cfa.harvard.edu; choopes@pha.jhu.edu; impey@as.arizona.edu; jannuzi@noao.edu; rolf.jansen@asu.edu; alex@astron.berkeley.edu; jka@camk.edu.pl; sheila@astro.as.utexas.edu; rkirshner@cfa.harvard.edu; dlatham@cfa.harvard.edu; jlee@as.arizona.edu; leonard@nova.astro.umass.edu; weidong@astron.berkeley.edu; kluhman@cfa.harvard.edu; martini@ociw.edu; hmathis@noao.edu; jose@das.uchile.cl; tmegeath@cfa.harvard.edu; mmiller@noao.edu; dante@astro.puc.cl; edo@as.arizona.edu; marina@ugastro.berkeley.edu; mmp@lco.cl; pindor@astro.princeton.edu; dsasselov@cfa.harvard.edu; rschild@cfa.harvard.edu; heidis@noao.edu; tspahr@cfa.harvard.edu; jet@lco.cl; ian@ociw.edu; dweisz@u.clink.berkeley.edu; rogier.windhorst@asu.edu; dzaritsky@as.arizona.edu RI Bonanos, Alceste/K-5392-2013; Brown, Michael/B-1181-2015; Maza, Jose/I-5722-2016; Hamuy, Mario/G-7541-2016; Hathi, Nimish/J-7092-2014 OI Bonanos, Alceste/0000-0003-2851-1905; Brown, Michael/0000-0002-1207-9137; Maza, Jose/0000-0003-2068-1328; Hathi, Nimish/0000-0001-6145-5090 NR 115 TC 190 Z9 192 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2003 VL 599 IS 1 BP 394 EP 407 DI 10.1086/379228 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FN UT WOS:000187149600032 ER PT J AU Narayan, R Heyl, JS AF Narayan, R Heyl, JS TI Thermonuclear stability of material accreting onto a neutron star SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : neutron; X-rays : binaries; X-rays : bursts ID X-RAY-BURSTS; HELIUM-BURNING FLASHES; RADIUS-EXPANSION; SHELL FLASHES; MAGNETIC-FIELD; NUCLEAR FUSION; ENVELOPES; HYDROGEN; OSCILLATIONS; EVOLUTION AB We present a global linear stability analysis of nuclear fuel accumulating on the surface of an accreting neutron star, and we identify the conditions under which thermonuclear bursts are triggered. The analysis reproduces all the recognized regimes of hydrogen and helium bursts and in addition shows that at high accretion rates, near the limit of stable burning, there is a regime of "delayed mixed bursts" that is distinct from the more usual "prompt mixedbursts." In delayed mixed bursts, a large fraction of the fuel is burned stably before the burst is triggered. Bursts thus have longer recurrence times but at the same time have somewhat smaller fluences. Therefore, the parameter a, which measures the ratio of the energy released via accretion to that generated through nuclear reactions in the burst, is up to an order of magnitude larger than for prompt bursts. This increase in alpha near the threshold of stable burning has been seen in observations. We explore a wide range of mass accretion rates, neutron star radii, and core temperatures and calculate a variety of burst properties. From a preliminary comparison with data, we suggest that bursting neutron stars may have hot cores, with T-core greater than or similar to 10(7.5) K, consistent with interior cooling via the modified Urca or similar low-efficiency process, rather than T-core similar to 10(7) K, as expected for the direct Urca process. There is also an indication that neutron star radii are somewhat small, less than or similar to10 km. Both of these conclusions need to be confirmed by comparing more careful calculations with better data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 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 DEC 10 PY 2003 VL 599 IS 1 BP 419 EP 449 DI 10.1086/379211 PN 1 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FN UT WOS:000187149600034 ER PT J AU Traub, WA Vanderbei, RJ AF Traub, WA Vanderbei, RJ TI Two-mirror apodization for high-contrast imaging SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation : high angular resolution AB Direct detection of extrasolar planets will require imaging systems capable of unprecedented contrast. Apodized pupils provide an attractive way to achieve such contrast, but they are difficult, perhaps impossible, to manufacture to the required tolerance, and they absorb about 90% of the light in order to create the apodization, which of course lengthens the exposure times needed for planet detection. A recently proposed alternative is to use two mirrors to accomplish the apodization. With such a system, no light is lost. In this paper, we provide a careful mathematical analysis, using one-dimensional mirrors, of the on-axis and off-axis performance of such a two-mirror apodization system. There appear to be advantages and disadvantages to this approach. In addition to not losing any light, we show that the nonuniformity of the apodization implies an extra magnification of off-axis sources and thereby makes it possible to build a real system with about half the aperture that one would otherwise require or, equivalently, resolve planets at about half the angular separation as one can achieve with standard apodization. More specifically, ignoring pointing error and stellar disk size, a planet at 1.7 lambda/D ought to be at the edge of detectability. However, we show that the non-zero size of a stellar disk pushes the threshold for high contrast so that a planet must be at least 2.5 lambda/D from its star to be detectable. The off-axis analysis of two-dimensional mirrors is left for future study. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ, Princeton, NJ 08544 USA. RP Traub, WA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Vanderbei, Robert/A-9779-2009 NR 5 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 DEC 10 PY 2003 VL 599 IS 1 BP 695 EP 701 DI 10.1086/379152 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FN UT WOS:000187149600055 ER PT J AU Edwards, S Fischer, W Kwan, J Hillenbrand, L Dupree, AK AF Edwards, S Fischer, W Kwan, J Hillenbrand, L Dupree, AK TI HeI lambda 10830 as a probe of winds in accreting young stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : protoplanetary disks; stars : formation; stars : pre-main-sequence; stars : winds, outflows ID T-TAURI STARS; VELOCITY MOLECULAR GAS; CLASS-I PROTOSTARS; DISK ACCRETION; MAGNETOSPHERIC ACCRETION; ECHELLE SPECTROSCOPY; EMISSION; REGIONS; INFALL; MODEL AB He I lambda10830 profiles acquired with Keck's NIRSPEC for six young low-mass stars with high disk accretion rates (AS 353A, DG Tau, DL Tau, DR Tau, HL Tau, and SVS 13) provide new insight into accretion-driven winds. In four of the stars, the profiles have the signature of resonance scattering, and they possess a deep and broad blueshifted absorption that penetrates more than 50% into the 1 mum continuum over a continuous range of velocities from near the stellar rest velocity to the terminal velocity of the wind, unlike inner wind signatures seen in other spectral features. This deep and broad absorption provides the first observational tracer of the acceleration region of the inner wind and suggests that this acceleration region is situated such that it occults a significant portion of the stellar disk. The remaining two stars also have blue absorption extending below the continuum, although here the profiles are dominated by emission, requiring an additional source of helium excitation beyond resonant scattering. This is likely the same process that produces the emission profiles seen at He I 5876 Angstrom. C1 Smith Coll, Coll Astron 5, Northampton, MA USA. Univ Massachusetts, Coll Astron Dept 5, Amherst, MA 01003 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Edwards, S (reprint author), Smith Coll, Coll Astron 5, McConnell Hall, Northampton, MA USA. NR 25 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 DEC 10 PY 2003 VL 599 IS 1 BP L41 EP L44 DI 10.1086/381077 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FP UT WOS:000187149800011 ER PT J AU Furlanetto, SR Schaye, J Springel, V Hernquist, L AF Furlanetto, SR Schaye, J Springel, V Hernquist, L TI Mapping the cosmic web with Ly alpha emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; diffuse radiation; galaxies : formation; intergalactic medium ID STAR-FORMATION; COOLING RADIATION; GALAXIES; FOREST; SIMULATIONS; UNIVERSE; HISTORY; MODEL; LIMIT AB We use a high-resolution cosmological simulation to predict the distribution of H I Lyalpha emission from the low-redshift (zless than or similar to0.5) intergalactic medium (IGM). Our simulation can be used to reliably compute the emission from optically thin regions of the IGM but not that of self-shielded gas. We therefore consider several models that bracket the expected emission from self-shielded regions. Most galaxies are surrounded by extended (greater than or similar to10(2) kpc) "coronae" of optically thin gas with Lyalpha surface brightness close to the expected background. Most of these regions contain smaller cores of dense, cool gas. Unless self-shielded gas is able to cool to T < 10(41), these cores are much brighter than the background. The Lyα coronae represent "cooling flows" of IGM gas accreting onto galaxies. We also estimate the number of Lyα photons produced through the reprocessing of stellar ionizing radiation in the interstellar medium of galaxies; while this mechanism is responsible for the brightest Lya emission, it occurs on small physical scales and can be separated using high-resolution observations. In all cases, we find that Lyα emitters are numerous ( with a space density of &SIM;0.1 h(3) Mpc(-3)) and closely trace the filamentary structure of the IGM, providing a new way to map gas inside the cosmic web. C1 CALTECH, Pasadena, CA 91125 USA. Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), CALTECH, Mail Code 130-33, Pasadena, CA 91125 USA. NR 21 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 DEC 10 PY 2003 VL 599 IS 1 BP L1 EP L4 DI 10.1086/381140 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 752FP UT WOS:000187149800001 ER PT J AU Campbell, BA Shepard, MK AF Campbell, BA Shepard, MK TI Coherent and incoherent components in near-nadir radar scattering: Applications to radar sounding of Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE radar; scattering; MARSIS; SHARAD; Mars ID SURFACE; BACKSCATTERING; TOPOGRAPHY; SCALE; MOON AB [1] We examine the relative importance of coherent and incoherent echo components in near-nadir radar scattering from self-affine surfaces. The coherent component, important only for observations at small incidence angles (nadir-looking sounders and altimeters), is a function of both surface roughness and scattering area. Models for the incoherent component require a minimum scattering area for validity; for smaller regions, the radar echo is overestimated. We propose a simple criterion for the horizontal scale that defines this shift in applicable scattering model and show the range of roughness parameters for which MARSIS, SHARAD, and possibly JIMO radar sounder measurements may be modeled using the two approaches. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Bloomsburg Univ Penn, Dept Geog & Earth Sci, Bloomsburg, PA 17815 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 19 TC 9 Z9 9 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-PLANET JI J. Geophys. Res.-Planets PD DEC 10 PY 2003 VL 108 IS E12 AR 5132 DI 10.1029/2003JE002164 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 756QU UT WOS:000187493100002 ER PT J AU Golombek, MP Grant, JA Parker, TJ Kass, DM Crisp, JA Squyres, SW Haldemann, AFC Adler, M Lee, WJ Bridges, NT Arvidson, RE Carr, MH Kirk, RL Knocke, PC Roncoli, RB Weitz, CM Schofield, JT Zurek, RW Christensen, PR Fergason, RL Anderson, FS Rice, JW AF Golombek, MP Grant, JA Parker, TJ Kass, DM Crisp, JA Squyres, SW Haldemann, AFC Adler, M Lee, WJ Bridges, NT Arvidson, RE Carr, MH Kirk, RL Knocke, PC Roncoli, RB Weitz, CM Schofield, JT Zurek, RW Christensen, PR Fergason, RL Anderson, FS Rice, JW TI Selection of the Mars Exploration Rover landing sites SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review DE Mars Exploration Rover; landing sites; remote sensing; aqueous climatic and geologic histories; Meridiani; Gusev ID ORBITER LASER ALTIMETER; THERMAL EMISSION SPECTROMETER; GENERAL-CIRCULATION MODEL; SIZE-FREQUENCY DISTRIBUTIONS; REMOTE-SENSING DATA; GLOBAL SURVEYOR; PHYSICAL-PROPERTIES; MARTIAN ATMOSPHERE; MAADIM-VALLIS; SCALE ROUGHNESS AB [1] The selection of Meridiani Planum and Gusev crater as the Mars Exploration Rover landing sites took over 2 years, involved broad participation of the science community via four open workshops, and narrowed an initial -155 potential sites (80-300 x 30 km) to four finalists based on science and safety. Engineering constraints important to the selection included (1) latitude (10degreesN-15degreesS) for maximum solar power, (2) elevation (less than -1.3 km) for sufficient atmosphere to slow the lander, (3) low horizontal winds, shear, and turbulence in the last few kilometers to minimize horizontal velocity, (4) low 10-m-scale slopes to reduce airbag spin-up and bounce, (5) moderate rock abundance to reduce abrasion or strokeout of the airbags, and (6) a radar-reflective, load-bearing, and trafficable surface safe for landing and roving that is not dominated by fine-grained dust. The evaluation of sites utilized existing as well as targeted orbital information acquired from the Mars Global Surveyor and Mars Odyssey. Three of the final four landing sites show strong evidence for surface processes involving water and appear capable of addressing the science objectives of the missions, which are to determine the aqueous, climatic, and geologic history of sites on Mars where conditions may have been favorable to the preservation of evidence of possible prebiotic or biotic processes. The evaluation of science criteria placed Meridiani and Gusev as the highest-priority sites. The evaluation of the three most critical safety criteria (10-m-scale slopes, rocks, and winds) and landing simulation results indicated that Meridiani and Elysium Planitia are the safest sites, followed by Gusev and Isidis Planitia. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Washington Univ, Dept Earth & Space Sci, St Louis, MO 63130 USA. US Geol Survey, Menlo Pk, CA 94025 USA. US Geol Survey, Geol Div, Branch Astrogeol, Flagstaff, AZ 86001 USA. NASA Headquarters, Washington, DC 20546 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mgolombek@jpl.nassa.gov; grantj@nasm.si.edu; timothy.j.parker@jpl.nasa.gov; david.m.kass@jpl.nasagov; joy.crisp@jpl.nasa.gov; squyres@astrosun.tn.cornell.edu; albert@shannon.jpl.nasa.gov; joy@glassy.jpl.nasa.gov; wayne@cranberry.jpl.nasa.gov; nathan.bridges@jpl.nasa.gov; arvidson@wunder.wustl.edu; carr@usgs.gov; rkirk@usgs.gov; philip.c.knocke@jpl.nasa.gov; ralph.b.roncoli@jpl.nasa.gov; cweitz@hq.nasa.gov; tim@scn1.jpl.nasa.gov; rzurek@jpl.nasa.gov; phil.christensen@asu.edu; robin.fergason@asu.edu; anderson@higp.hawaii.edu; james.rice@asu.edu RI Bridges, Nathan/D-6341-2016; Crisp, Joy/H-8287-2016 OI Crisp, Joy/0000-0002-3202-4416 NR 120 TC 86 Z9 88 U1 1 U2 10 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 DEC 10 PY 2003 VL 108 IS E12 AR 8072 DI 10.1029/2003JE002074 PG 48 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 756QU UT WOS:000187493100001 ER PT J AU Sanz, ME McCarthy, MC Thaddeus, P AF Sanz, ME McCarthy, MC Thaddeus, P TI Rotational transitions of SO, SiO, and SiS excited by a discharge in a supersonic molecular beam: Vibrational temperatures, Dunham coefficients, Born-Oppenheimer breakdown, and hyperfine structure SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ELECTRIC DIPOLE MOMENT; AB-INITIO THEORY; MICROWAVE-SPECTRUM; CARBON CHAINS; DIATOMIC-MOLECULES; RELAXATION; SPECTROSCOPY; STATES; IRC+10216; CONSTANTS AB Fourier transform microwave spectroscopy has been used to investigate vibrational excitation and relaxation of diatomic molecules produced by an electric discharge in the throat of a supersonic nozzle. Rotational transitions of SO, SiO, and SiS, in vibrational states up to v=33 for (SO)-S-32-O-16, v=45 for (SiO)-Si-28-O-16, and v=51 for (SiS)-Si-28-S-32 in their ground electronic states have been detected. The isotopic species (SO)-S-33-O-16, (SO)-S-34-O-16, (SiO)-Si-29-O-16, (SiO)-Si-28-O-18, (SiS)-Si-29-S-32, and (SiS)-Si-28-S-34 have also been observed in highly excited vibrational states. Microwave transitions include up to v=22 for the second lowest excited electronic state b (1)Sigma(+) of SO (similar to10 510 cm-1 above ground) have also been detected. Effective vibrational temperatures have been derived for each species, and a general model is proposed to qualitatively explain the observations. Vibrational excitation is caused by inelastic collisions with the hot electrons produced in the discharge. The subsequent vibrational populations are largely determined by vibration-vibration energy transfer via molecule-molecule binary collisions. Two regions can be inferred from the data: one characterized by a temperature of around 1000 K and a second region with a temperature of several thousand degrees Kelvin. Improved Dunham coefficients and correction terms for the breakdown of the Born-Oppenheimer approximation have been determined for b (1)Sigma(+) SO, X (1)Sigma(+) SiO, and X (1)Sigma(+) SiS. Nuclear spin-rotation hyperfine structure for the Si-29 isotopic species of SiO and SiS has been observed in all highly excited vibrational states. (C) 2003 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Sanz, ME (reprint author), Univ Valladolid, Fac Ciencias, Dept Quim Fis, Prado Magdalena S-N, E-47005 Valladolid, Spain. RI Sanz, Maria Eugenia/F-7054-2013; OI McCarthy, Michael/0000-0001-9142-0008 NR 64 TC 34 Z9 34 U1 1 U2 16 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 8 PY 2003 VL 119 IS 22 BP 11715 EP 11727 DI 10.1063/1.1612481 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 746PZ UT WOS:000186755900025 ER PT J AU Stein, DL Bond, CE Misitano, D AF Stein, DL Bond, CE Misitano, D TI Liparis adiastolus (Teleostei, Liparidae): A new snailfish species from the littoral zone of the Northeastern Pacific, and redescription of Liparis rutteri (Gilbert and Snyder, 1898) SO COPEIA LA English DT Article ID SCORPAENIFORMES AB Liparis adiastolus, a previously undescribed species from the coasts of Oregon and Washington, northwest United States, is described. The new species has probably been consistently confused with Liparis rutteri, which has a more northerly distribution. Liparis adiastolus is clearly distinguishable from all similar species in having 41-70 pyloric caeca, 35-39 vertebrae, 30-33 dorsal-fin rays, 32-35 pectoral-fin rays, disk 67-77% HL, and other distinctive characters. In addition to describing the new species, we select a lectotype of L. rutteri, provide an expanded diagnosis for that species, and discuss the confusion previously existing with regard to its identification. C1 NOAA, NMFS Systemat Lab, Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. Gen Delivery, Clinton, WA 98236 USA. RP Stein, DL (reprint author), NOAA, NMFS Systemat Lab, Smithsonian Inst, Natl Museum Nat Hist, POB 37012,MRC 0153, Washington, DC 20013 USA. EM david.stein@noaa.gov NR 19 TC 0 Z9 3 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 DEC 4 PY 2003 IS 4 BP 818 EP 823 PG 6 WC Zoology SC Zoology GA 751LR UT WOS:000187069000014 ER PT J AU Menezes, NA Weitzman, SH Burns, JR AF Menezes, NA Weitzman, SH Burns, JR TI A systematic review of Planaltina (Teleostei : Characiformes : Characidae : Glandulocaudinae : Diapomini) with a description of two new species from the upper rio Parana, Brazil SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID ALARM SUBSTANCE CELLS; FISHES TELEOSTEI; FRIGHT REACTION; OSTARIOPHYSI AB Two new species, Planaltina glandipedis and Planaltina britskii, glandulocaudine fishes of the family Characidae, tribe Diapomini, are described herein. They were collected from tributaries of the rio Grande and or the rio Tiete, both tributaries of the upper rio Parana in the State of Sao Paulo, Brazil. The previously described species, Planaltina myersi, until now known almost exclusively from the holotype, is here redescribed from 47 specimens taken from. tributaries of the rio Corumba, a tributary of the upper rio Parana. The two new species differ most prominently from the previously known species by possession of three somewhat elongate scales along the dorsal border of the male's caudal pouch opening. There is only one elongate scale in P. myersi. Planaltina glandipedis differs from P. britskii in having six or seven horizontal scale rows between the dorsal-fin origin and the lateral line versus five in the later species. The possible phylogenetic relationships among the three inseminating species within the tribe Diapomini, subfamily Glandulocaudinae, are discussed along with the putative phylogenetic relationships of the Diapomini to the newly recognized glandulocaudine outgroup containing the characid genera Knodus and a new genus related to Attonitus. Brief comments are presented concerning the geographical distribution and ecology of the species of Planaltina. C1 Univ Sao Paulo, Museu Zool, BR-04299970 Sao Paulo, SP, Brazil. Natl Museum Nat Hist, Dept Syst Biol, Div Fishes, Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Menezes, NA (reprint author), Univ Sao Paulo, Museu Zool, Caixa Postal 42694, BR-04299970 Sao Paulo, SP, Brazil. RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 NR 25 TC 11 Z9 15 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 DEC 2 PY 2003 VL 116 IS 3 BP 557 EP 600 PG 44 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 752CN UT WOS:000187129600004 ER PT J AU Cairns, SD Bayer, FM AF Cairns, SD Bayer, FM TI Studies on western Atlantic octocorallia (Coelenterata : Anthozoa). Part 3: The genus Narella gray, 1870 SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The seven species of Narella known from the North Atlantic are described and illustrated, often with the aid of stereo SEM photomicrographs in order to show the shape and relationships of the body wall sclerites. Two species are described as new: N. alvinae and N. spectabilis, the former the deepest known representative of this genus. Two keys, tabular and dichotomous, are provided for the seven species. The types of all but one of the species were examined; only photographs of the syntype were studied of N. bellissima. New material is reported for all but one species, based primarily on collections housed at the USNM and MCZ. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Invertebrate Zool, Washington, DC 20013 USA. RP Cairns, SD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Invertebrate Zool, POB 37012, Washington, DC 20013 USA. NR 31 TC 5 Z9 8 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 DEC 2 PY 2003 VL 116 IS 3 BP 617 EP 648 PG 32 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 752CN UT WOS:000187129600006 ER PT J AU Ivanenko, VN Ferrari, FD AF Ivanenko, VN Ferrari, FD TI Redescription of adults and description of copepodid development of Dermatomyzon nigripes (Brady & Robertson, 1876) and of Asterocheres lilljeborgi Boeck, 1859 (Copepoda : Siphonostomatoida : Asterocheridae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID RIDGEWAYIA-KLAUSRUETZLERI; SETAL NUMBERS; SWIMMING LEGS; HOMOLOGIES; FAMILY AB Adult and immature copepodids of Dermatomyzon nigripes (Brady & Robertson, 1876) and Asterocheres lilljeborgi Boeck, 1859 were collected by SCUBA from the White Sea. All copepodids of D. nigripes were found on the bryozoan Flustra foliacea (Linnaeus, 1758); adults of D. nigripes also were washed out from the sponge Halichondria panicea (Pallas, 1766), the ophiuroid Ophiopholis aculeata (Linnaeus, 1767), and were collected among hydrozoans and other invertebrates from dead shells swept by tidal cur-rents. Copepodids of A. lilljeborgi were washed from the starfish Henricia sanguinolenta (O. E Muller, 1776). Comparative analysis of development of D. nigripes and A. lilljeborgi with the related Scottomyzon gibberum (Scott & Scott, 1894) shows that both genders of A. lilljeborgi and S. gibberum suppress the formation of fourth abdominal somite. Females of A. lilljeborgi and D. nigripes develop a simple segmental complex when the arthrodial membrane separating the genital somite from the second abdominal somite fails to form; this arthrodial membrane develops on females of S. gibberum so that there is no genital complex. The antennule of A. lilljeborgi with a single, proximal complex of three segments appears most similar to the ancestral siphonostomatoid. The antennule of D. nigripes has a proximal complex of two segments and a distal complex of three segments; the antennule of S. gibberum has a proximal complex of three segments and a distal complex of four segments. Setation of the maxilliped of D. nigripes and A. lilljeborgi are identical and appear similar to the ancestral siphonostomatoid; the maxilliped of S. gibberum differs in that it fails to add a seta to its syncoxa and loses a seta on the penultimate endopodal segment. Asterocheres lilljeborgi and S. gibberum share derived states of setation on the exopod of swimming legs 1-4, leg 5 and leg 6; D. nigripes and S. gibberum share derived states of setation on the endopod of swimming legs 3 and 4. C1 Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, Museum Support Ctr, Suitland, MD 20746 USA. RP Ivanenko, VN (reprint author), Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. RI Ivanenko, Viatcheslav/B-8198-2008 OI Ivanenko, Viatcheslav/0000-0003-1255-0491 NR 51 TC 16 Z9 17 U1 1 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 2 PY 2003 VL 116 IS 3 BP 661 EP 691 PG 31 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 752CN UT WOS:000187129600008 ER PT J AU Vari, RP Ferraris, CJ Keith, P AF Vari, RP Ferraris, CJ Keith, P TI A new Pseudocetopsis species (Siluriformes : Cetopsidae) from Suriname and French Guiana SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID SOUTH-AMERICA AB Pseudocetopsis orientale, a new catfish species of small body size of the cetopsid subfamily Cetopsinae is described from several Atlantic-slope rivers of Suriname and French Guiana. The combination of the presence of a dorsal fin with an ossified spinelet, the possession of pectoral- and dorsal-fin spines, the length of the pelvic and pectoral fins, the relative depth of the body, and the alignment of the dorsal and ventral profiles of the portion of the body posterior of the dorsal-fin base serve to distinguish the new species from all other cetopsines. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Syst Engn Fishes, Washington, DC 20560 USA. Natl Museum Nat Hist, Dept Syst Biol Fishes, Smithsonian Inst, Washington, DC 20560 USA. Museum Natl Hist Nat, Lab Ichtyol, F-75231 Paris, France. RP Vari, RP (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Syst Engn Fishes, Washington, DC 20560 USA. NR 8 TC 5 Z9 6 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 2 PY 2003 VL 116 IS 3 BP 692 EP 698 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 752CN UT WOS:000187129600009 ER PT J AU Olson, SL AF Olson, SL TI First fossil record of a finfoot (Aves : Heliornithidae) and its biogeographical significance SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID GRUIFORMES AB The distal end of a humerus from the Lee Creek Mine in North Carolina is identified with the modern Neotropical species as Heliornis aff. fulica and provides the first fossil record for the family Heliornithidae. The fossil was determined to come from the Middle Miocene (14 Ma) Pungo River Formation based on sedimentary, preservational, and other lines of evidence. This in turn implies that Heliornis did not spread into South America until after the isthmian land connection about 3 Ma and that the interchange of Heliornithidae between the Old and New World probably took place through the Northern Hemisphere in the Paleogene. C1 Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. RP Olson, SL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. NR 12 TC 6 Z9 6 U1 1 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 2 PY 2003 VL 116 IS 3 BP 732 EP 736 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 752CN UT WOS:000187129600013 ER PT J AU Arroyo-Cabrales, J Gardner, AL AF Arroyo-Cabrales, J Gardner, AL TI The type specimen of Anoura geoffroyi lasiopyga (Chiroptera : Phyllostomidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB In 1868, Wilhelm Peters described Glossonycteris lasiopyga, based on a specimen provided by Henri de Saussure and collected in Mexico. The type specimen was presumed to be among those housed in the collections of the Zoologisches Museum of the Humboldt, Universitat, in Berlin, Germany. Our study of one of Saussure's specimens from Mexico, discovered in the collections of the Museum d'Histoire Naturelle, Geneva, Switzerland, demonstrates that it and not one of the Berlin specimens is the holotype. C1 M&C Ticul Alvarez Solorzano, INAH, Lab Arqueozool, Mexico City 06060, DF, Mexico. Smithsonian Inst, Biodivers Program Off, Washington, DC 20560 USA. Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20560 USA. RP Arroyo-Cabrales, J (reprint author), M&C Ticul Alvarez Solorzano, INAH, Lab Arqueozool, Modena 16 Col Ctr, Mexico City 06060, DF, Mexico. NR 19 TC 2 Z9 3 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 DEC 2 PY 2003 VL 116 IS 3 BP 737 EP 741 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 752CN UT WOS:000187129600014 ER PT J AU Graves, GR AF Graves, GR TI Diagnoses of hybrid hummingbirds (Aves : Trochilidae). 11. Documentation of an intergeneric woodstar hybrid, Calliphlox mitchellii x Chaetocercus mulsant SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID SYSTEMATICS; ORIGIN; GOULD AB A specimen in the Museum Alexander Koenig collected in Colombia is shown to be a hybrid between Calliphlox mitchelhi and Chaetocercus mulsant. This is the first known example of intergeneric hybridization between species in these presumably closely related genera. External measurements of the hybrids are consistent with the proposed parental hypothesis. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. RP Graves, GR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, MRC-116,POB 37012, Washington, DC 20013 USA. NR 20 TC 2 Z9 2 U1 0 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 2 PY 2003 VL 116 IS 3 BP 820 EP 826 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 752CN UT WOS:000187129600019 ER PT J AU Dick, CW Abdul-Salim, K Bermingham, E AF Dick, CW Abdul-Salim, K Bermingham, E TI Molecular systematic analysis reveals cryptic tertiary diversification of a widespread tropical rain forest tree SO AMERICAN NATURALIST LA English DT Article DE internal transcribed spacer (ITS); phylogeography; molecular clock; fossils; long-distance dispersal; tropical trees ID MAHOGANY SWIETENIA-MACROPHYLLA; SYMPHONIA-GLOBULIFERA CLUSIACEAE; INTERNAL TRANSCRIBED SPACER; NUCLEAR RIBOSOMAL DNA; MESOAMERICAN POPULATIONS; NEOTROPICAL PALEOBOTANY; POLLINATION BIOLOGY; GENETIC DIVERSITY; DIVERGENCE TIMES; CENTRAL-AMERICA AB The broad geographic range of many Neotropical rain forest tree species implies excellent dispersal abilities or range establishment that preceded the formation of current dispersal barriers. In order to initiate historical analyses of such widespread Neotropical trees, we sequenced the nuclear ribosomal spacer (ITS) region of Symphonia globulifera L.f. (Clusiaceae) from populations spanning the Neotropics and western Africa. This rain forest tree has left unmistakable Miocene fossils in Mesoamerica (15.5-18.2 Ma) and in South America (similar to15 Ma). Although marine dispersal of S. globulifera is considered improbable, our study establishes three marine dispersal events leading to the colonization of Mesoamerica, the Amazon basin, and the West Indies, thus supporting the paleontological data. Our phylogeographic analysis revealed the spatial extent of the three Neotropical S. globulifera clades, which represent trans-Andes (Mesoamerica + west Ecuador), cis-Andes (Amazonia + Guiana), and the West Indies. Strong phylogeographic structure found among trans-Andean populations of S. globulifera stands in contrast to an absence of ITS nucleotide variation across the Amazon basin and indicates profound regional differences in the demographic history of this rain forest tree. Drawing from these results, we provide a historical biogeographic hypothesis to account for differences in the patterns of beta diversity within Mesoamerican and Amazonian forests. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Harvard Univ Herbaria, Cambridge, MA 02138 USA. RP Dick, CW (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM dickc@naos.si.edu RI Dick, Christopher/A-8744-2008 NR 70 TC 129 Z9 135 U1 1 U2 16 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD DEC PY 2003 VL 162 IS 6 BP 691 EP 703 DI 10.1086/379795 PG 13 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 759ED UT WOS:000187724600001 PM 14737707 ER PT J AU Gingerich, O AF Gingerich, O TI Mapping Mars: Science, imagination, and the birth of a world SO AMERICAN SCHOLAR LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU PHI BETA KAPPA SOC PI WASHINGTON PA 1785 MASSACHUSETTS AVENUE, N W FOURTH FL,, WASHINGTON, DC 20036 USA SN 0003-0937 J9 AM SCHOLAR JI Am. Sch. PD WIN PY 2003 VL 72 IS 1 BP 148 EP 150 PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 637RW UT WOS:000180527600024 ER PT J AU Olin, JS AF Olin, JS TI Evidence that the Vinland Map is medieval SO ANALYTICAL CHEMISTRY LA English DT Letter ID PARCHMENT AB The Vinland Map has been proposed to date to the mid-fifteenth century and is significant in showing the north Atlantic area of what is now North America about 50 years before the voyages of Columbus. It has been confirmed by radiocarbon dating that the map was drawn on a fifteenth century parchment; however, controversy regarding the ink of the map has persisted. Analytical studies of the ink of the map have been interpreted to show that the map is a twentieth century forgery because of the presence of carbon and anatase in the ink. However, carbon is known to have been added to medieval iron gallotannate inks, and the presence of anatase in a medieval ink can be explained by examining the process of making medieval inks. C1 Smithsonian Inst, Washington, DC 20560 USA. RP Olin, JS (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 14 TC 13 Z9 13 U1 1 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 J9 ANAL CHEM JI Anal. Chem. PD DEC 1 PY 2003 VL 75 IS 23 BP 6745 EP 6747 DI 10.1021/ac034533c PG 3 WC Chemistry, Analytical SC Chemistry GA 750HV UT WOS:000186986000058 PM 16468159 ER PT J AU Lynnerup, N Meldgaard, J Jakobsen, J Appelt, M Koch, A Frohlich, B AF Lynnerup, N Meldgaard, J Jakobsen, J Appelt, M Koch, A Frohlich, B TI Human Dorset remains from Igloolik, Canada SO ARCTIC LA English DT Article DE graves; Alarnerk (NhHd-1); early and late Dorset; physical anthropology; dental anthropology AB Skeletal remains of four Dorset Palaeo-Eskimo individuals were found at Alarnerk (NhHd-1), Melville Peninsula, in 1954 by the joint Danish National Museum-University of Pennsylvania Expedition, which was excavating Dorset and pre-Dorset sites. These remains included one complete mandible, two fragmentary mandibles, and a cranial fragment. One of the mandibular fragments, found in a grave, was from a child approximately nine months old. The other remains were found in middens at the site. These remains add to the otherwise very sparse Dorset human material. Analysis of the dental morphology, as well as morphometric analysis of the complete mandible, shows Eskimoid characters and resemblance with later period Greenlandic human skeletal remains. C1 Univ Copenhagen, Panum Inst, Inst Forens Med, Lab Biol Anthropol, DK-2200 Copenhagen, Denmark. Natl Museum Denmark, SILA Greenland Res Ctr, DK-1220 Copenhagen, Denmark. Univ Copenhagen, Panum Inst, Inst Odontol, Lab Dent Anthropol, DK-2200 Copenhagen, Denmark. Statens Serum Inst, Danish Epidemiol Ctr, Dept Epidemiol Res, DK-2300 Copenhagen S, Denmark. Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Lynnerup, N (reprint author), Univ Copenhagen, Panum Inst, Inst Forens Med, Lab Biol Anthropol, Blegdamsvej 3, DK-2200 Copenhagen, Denmark. EM n.lynnerup@antrolab.ku.dk NR 32 TC 6 Z9 6 U1 0 U2 1 PU ARCTIC INST N AMER PI CALGARY PA UNIV OF CALGARY 2500 UNIVERSITY DRIVE NW 11TH FLOOR LIBRARY TOWER, CALGARY, ALBERTA T2N 1N4, CANADA SN 0004-0843 J9 ARCTIC JI Arctic PD DEC PY 2003 VL 56 IS 4 BP 349 EP 358 PG 10 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 764FX UT WOS:000188197700005 ER PT J AU Williams, BF Hogan, CJ Barris, B Candia, P Challis, P Clocchiatti, A Coil, AL Filippenko, AV Garnavich, P Kirshner, RP Holland, ST Jha, S Krisciunas, K Leibundgut, B Li, WD Matheson, T Maza, J Phillips, MM Riess, AG Schmidt, BP Schommer, RA Smith, RC Sollerman, J Spyromilio, J Stubbs, C Suntzeff, NB Tonry, JL AF Williams, BF Hogan, CJ Barris, B Candia, P Challis, P Clocchiatti, A Coil, AL Filippenko, AV Garnavich, P Kirshner, RP Holland, ST Jha, S Krisciunas, K Leibundgut, B Li, WD Matheson, T Maza, J Phillips, MM Riess, AG Schmidt, BP Schommer, RA Smith, RC Sollerman, J Spyromilio, J Stubbs, C Suntzeff, NB Tonry, JL TI Imaging and demography of the host galaxies of high-redshift type Ia supernovae SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmological parameters; galaxies : high redshift; supernovae : general ID BVRI LIGHT CURVES; COSMOLOGICAL CONSTANT; PEAK LUMINOSITY; HUBBLE DIAGRAM; EVOLUTION; MORPHOLOGY; UNIVERSE; LAMBDA; OMEGA; CONSEQUENCES AB We present the results of a study of the host galaxies of high-redshift Type Ia supernovae (SNe Ia). We provide a catalog of 18 hosts of SNe Ia observed with the Hubble Space Telescope (HST) by the High-z Supernova Search Team, including images, scale lengths, measurements of integrated (Hubble-equivalent) BVRIZ photometry in bands where the galaxies are brighter than mapproximate to25 mag, and galactocentric distances of the supernovae. We compare the residuals of SN Ia distance measurements from cosmological fits with measurable properties of the supernova host galaxies that might be expected to correlate with variable properties of the progenitor population, such as host-galaxy color and position of the supernova. We find mostly null results; the current data are generally consistent with no correlations of the distance residuals with host-galaxy properties in the redshift range 0.4210 plant families. 4. The assemblage on P. aduncum was dominated by a single species (Herpetogramma sp. near licarsisalis, Crambidae), which represented 48% of individuals, and also had a high proportion (34%) of rare species, collected as single individuals. This community structure was indistinguishable from that of a typical native host. In contrast, the P. umbellatum assemblage was unusual as no species represented >10% of individuals. 5. The aggressive invasion by P. aduncum of early successional vegetation is not explained by a competitive advantage due to low herbivore load, as the abundance of caterpillars feeding on it was comparable to that of native pioneer plants. 6. The caterpillar assemblage on P. aduncum demonstrated that an assemblage indistinguishable from native assemblages in density, species richness, and dominance structure (but not in host specificity) can originate from the existing species pool in lowland rainforests on a recently established tree species in <50 years. C1 Acad Sci Czech Republ, Inst Entomol, CZ-37005 Ceske Budejovice, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice, Czech Republic. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Smithsonian Trop Res Inst, Ancon, Panama. Univ Minnesota, St Paul, MN 55108 USA. RP Novotny, V (reprint author), Acad Sci Czech Republ, Inst Entomol, Branisovska 31, CZ-37005 Ceske Budejovice, Czech Republic. RI Leps, Jan/B-6913-2013; Cizek, Lukas/G-7905-2014; Novotny, Vojtech/G-9434-2014; Basset, Yves/B-6642-2014; Cizek, Lukas/K-7111-2015; Janda, Milan/H-7216-2014 OI Leps, Jan/0000-0002-4822-7429; Miller, Scott/0000-0002-4138-1378; Novotny, Vojtech/0000-0001-7918-8023; NR 66 TC 33 Z9 35 U1 1 U2 7 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 DEC PY 2003 VL 28 IS 6 BP 704 EP 716 DI 10.1111/j.1365-2311.2003.00558.x PG 13 WC Entomology SC Entomology GA 753XR UT WOS:000187257300009 ER PT J AU Wright, SJ Muller-Landau, HC Condit, R Hubbell, SP AF Wright, SJ Muller-Landau, HC Condit, R Hubbell, SP TI Gap-dependent recruitment, realized vital rates, and size distributions of tropical trees SO ECOLOGY LA English DT Article DE Barro Colorado Island, Panama; functional groups; gap dependence; guilds; life history; ontogenetic shifts; Panama; shade tolerance; size distribution; tree-fall gap; tropical trees; wood density ID RAIN-FOREST TREES; NEOTROPICAL FOREST; SPECIES-DIVERSITY; FUNCTIONAL TYPES; LIFE-HISTORY; DISTURBANCE; DYNAMICS; DIAMETER; GROWTH; CANOPY AB In closed-canopy forests, plant morphology and physiology determine shade tolerance and potential growth and mortality rates; potential vital rates and ongoing gap dependence determine realized vital rates; and realized vital rates determine individual size distributions. This hypothesis was evaluated for the 73 most abundant canopy tree species from Barro Colorado Island, Panama. The percentage of recruits located in tree-fall gaps (P), sapling growth (G), and mortality (M) rates, and the coefficient of skewness of size distributions (g(1)) were determined from censuses of all individuals >10 mm dbh in a 50-ha plot, Seven qualitative, bivariate predictions relating g(1), G, M, P, and wood density (W) were evaluated. Six of the seven predictions were substantiated in pairwise analyses. A path analysis integrated all seven predictions and explained 51% of the interspecific variation in g,. Size distributions with many large individuals and a long tail of relatively rare, small individuals (g(1) < 0) characterized gap-dependent species with large fecundity, seed mortality, seedling mortality, G, M, and P. Size distributions with many small individuals and a long tail of relatively rare, large individuals (g(1) > 0) characterized shade-tolerant species with the opposite traits. The percentage of tropical tree species that require tree-fall gaps to regenerate has been estimated to range from <20% to >70% for old-growth forests. Our analyses suggest that there are not large numbers of functionally equivalent species at either extreme of the regeneration continuum. Rather, there are very few extremely shade-tolerant and extremely light-demanding species. Most species have intermediate light requirements and lifestyles. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. Univ Georgia, Dept Bot, Athens, GA 30602 USA. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 53 TC 197 Z9 211 U1 6 U2 52 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 DEC PY 2003 VL 84 IS 12 BP 3174 EP 3185 DI 10.1890/02-0038 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 762LN UT WOS:000187973500008 ER PT J AU Baker, ME Wiley, MJ Carlson, ML Seelbach, PW AF Baker, ME Wiley, MJ Carlson, ML Seelbach, PW TI A GIS model of subsurface water potential for aquatic resource inventory, assessment, and environmental management SO ENVIRONMENTAL MANAGEMENT LA English DT Article DE groundwater hydrology; GIS; modeling; stream ecology; wetlands ID GROUNDWATER-FLOW; STREAM FISHES; PREDICTION; QUALITY; LANDSCAPE; PROFILES; SYSTEMS AB Biological, chemical, and physical attributes of aquatic ecosystems are often strongly influenced by groundwater sources. Nonetheless, widespread access to predictions of subsurface contributions to rivers, lakes, and wetlands at a scale useful to environmental managers is generally lacking. In this paper, we describe a "neighborhood analysis" approach for estimating topographic constraints on spatial patterns of recharge and discharge and discuss how this index has proven useful in research, management, and conservation contexts. The Michigan Rivers Inventory subsurface flux model (MRI-DARCY) used digital elevation and hydraulic conductivity inferred from mapped surficial geology to estimate spatial patterns of hydraulic potential. Model predictions were calculated in units of specific discharge (meters per day) for a 30-m-cell raster map and interpreted as an index of potential subsurface water flux (shallow groundwater and event through-flow). The model was evaluated by comparison with measurements of groundwater-related attributes at watershed, stream segment, and local spatial scales throughout Lower Michigan (USA). Map-based predictions using MRI-DARCY accounted for 85% of the observed variation in base flow from 128 USGS gauges, 69% of the observed variation in discharge accrual from 48 river segments, and 29% of the residual variation in local groundwater flux from 33 locations as measured by hyporheic temperature profiles after factoring out the effects of climate. Although it does not incorporate any information about the actual water table surface, by quantifying spatial variation of key constraints on groundwater-related attributes, the model provides strata for more intensive study, as well as a useful spatial tool for regional and local conservation planning, fisheries management, wetland characterization, and stream assessment. C1 Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Michigan Dept Nat Resources, Fisheries Res Inst, Ann Arbor, MI 48109 USA. RP Baker, ME (reprint author), Univ Michigan, Sch Nat Resources & Environm, 430 E Univ, Ann Arbor, MI 48109 USA. EM bakerm@si.edu RI Wiley, Michael/A-6853-2012; Baker, Matthew/I-2839-2014 OI Baker, Matthew/0000-0001-5069-0204 NR 83 TC 32 Z9 32 U1 1 U2 22 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0364-152X J9 ENVIRON MANAGE JI Environ. Manage. PD DEC PY 2003 VL 32 IS 6 BP 706 EP 719 DI 10.1007/s00267-003-0018-1 PG 14 WC Environmental Sciences SC Environmental Sciences & Ecology GA 800SA UT WOS:000220046800004 PM 15160896 ER PT J AU King, FM Johnson, EA Post, JE AF King, FM Johnson, EA Post, JE TI Diamonds - A comparison of three historic blue diamonds. SO GEMS & GEMOLOGY LA English DT News Item C1 GIA Gem Lab, New York, NY USA. Smithsonian Inst, Washington, DC 20560 USA. RP King, FM (reprint author), GIA Gem Lab, New York, NY USA. EM jking@gia.edu NR 0 TC 2 Z9 2 U1 0 U2 1 PU GEMOLOGICAL INST AMERICA PI CARLSBAD PA 5345 ARMADA DRIVE, CARLSBAD, CA 92008 USA SN 0016-626X J9 GEMS GEMOL JI Gems Gemol. PD WIN PY 2003 VL 39 IS 4 BP 322 EP 325 PG 4 WC Mineralogy SC Mineralogy GA 802OS UT WOS:000220173400014 ER PT J AU Hymus, GJ Johnson, DP Dore, S Anderson, HP Hinkle, CR Drake, BG AF Hymus, GJ Johnson, DP Dore, S Anderson, HP Hinkle, CR Drake, BG TI Effects of elevated atmospheric CO2 on net ecosystem CO2 exchange of a scrub-oak ecosystem SO GLOBAL CHANGE BIOLOGY LA English DT Article DE elevated CO2; NEE; open-top chambers; respiration; scrub-oak ecosystem ID LONG-TERM ELEVATION; OPEN-TOP CHAMBER; RISING CO2; QUERCUS-MYRTIFOLIA; CALCAREOUS GRASSLAND; NATIVE ENVIRONMENT; ALPINE GRASSLAND; CARBON-DIOXIDE; GAS-EXCHANGE; TREE GROWTH AB We report the results of a 2-year study of effects of the elevated (current ambient plus 350 mumol CO2 mol(-1)) atmospheric CO2 concentration (C-a) on net ecosystem CO2 exchange (NEE) of a scrub-oak ecosystem. The measurements were made in open-top chambers (OTCs) modified to function as open gas-exchange systems. The OTCs enclosed samples of the ecosystem (ca. 10 m(2) surface area) that had regenerated after a fire, 5 years before, in either current ambient or elevated C-a. Throughout the study, elevated C-a increased maximum NEE (NEEmax) and the apparent quantum yield of the NEE (phi(NEE)) during the photoperiod. The magnitude of the stimulation of NEEmax, expressed per unit ground area, was seasonal, rising from 50% in the winter to 180% in the summer. The key to this stimulation was effects of elevated C-a, and their interaction with the seasonal changes in the environment, on ecosystem leaf area index, photosynthesis and respiration. The separation of these factors was difficult. When expressed per unit leaf area the stimulation of the NEEmax ranged from 7% to 60%, with the increase being dependent on increasing soil water content (W-soil). At night, the CO2 effluxes from the ecosystem (NEEnight) were on an average 39% higher in elevated C-a. However, the increase varied between 6% and 64%, and had no clear seasonality. The partitioning of NEEnight into its belowground (R-below) and aboveground (R-above) components was carried out in the winter only. A 35% and 27% stimulation of NEEnight in December 1999 and 2000, respectively, was largely due to a 26% and 28% stimulation of R-below in the respective periods, because R-below constituted ca. 87% of NEEnight. The 37% and 42% stimulation of R-above in December 1999 and 2000, respectively, was less than the 65% and 80% stimulation of the aboveground biomass by elevated C-a at these times. An increase in the relative amount of the aboveground biomass in woody tissue, combined with a decrease in the specific rate of stem respiration of the dominant species Quercus myrtifolia in elevated C-a, was responsible for this effect. Throughout this study, elevated C-a had a greater effect on carbon uptake than on carbon loss, in terms of both the absolute flux and relative stimulation. Consequently, for this scrub-oak ecosystem carbon sequestration was greater in the elevated C-a during this 2-year study period. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. CNR, Kennedy Space Ctr, FL 32899 USA. Dynam Corp, Kennedy Space Ctr, FL 32899 USA. RP Drake, BG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 44 TC 18 Z9 19 U1 1 U2 12 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 DEC PY 2003 VL 9 IS 12 BP 1802 EP 1812 DI 10.1046/j.1529-8817.2003.00675.x PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 753XZ UT WOS:000187274800010 ER PT J AU Xiao, KC Ogawa, H Fukui, Y AF Xiao, KC Ogawa, H Fukui, Y TI An experimental study of harmonic SIS mixing at 205-235 GHz SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE harmonic quantum mixing; noise temperature; superconducting tunnel junctions; superconductor-insulator-superconductor (SIS) mixers ID TUNNEL-JUNCTIONS; CONVERSION GAIN; RADIO ASTRONOMY; RECEIVER; MIXERS AB A 230-GHz subharmonically pumped waveguide mixer employing superconducting tunnel junctions has been developed. We present, in this paper, an experimental study of harmonic superconductor-insulator-superconductor (SIS) mixing at 230 GHz, focusing mainly on its noise behavior. The mixer has a double-tuned waveguide structure and employs an array of four 1.7-mum(2) Nb-AlOx-Nb SIS junctions in series, with omegaR(n)C(j) similar to 3 at 230 GHz. Harmonic quantum mixing occurred over an experimental frequency range of 205-235 GHz (local oscillator: 112.5-117.5 GHz), exhibiting corresponding double sideband noise temperatures of lower than 150 K, with a lowest value of 75 K at similar to230 GHz. The measured mixer noise is believed to be the lowest yet reported for a mixer using subharmonic-pump configuration at this frequency. A phenomenon that we attribute to the third harmonic SIS mixing has also been observed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nagoya Univ, Dept Astrophys, Nagoya, Aichi 4648602, Japan. RP Xiao, KC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kxiao@cfa.harvard.edu NR 14 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD DEC PY 2003 VL 13 IS 4 BP 3856 EP 3861 DI 10.1109/TASC.2003.820510 PG 6 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 761DZ UT WOS:000187886100006 ER PT J AU McFadden, CS Sanchez, JA France, SC AF McFadden, CS Sanchez, JA France, SC TI The evolution of colony morphology in Octocorallia: A phylogenetic approach. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Smithsonian Inst, Washington, DC 20560 USA. Harvey Mudd Coll, Claremont, CA 91711 USA. Coll Charleston, Charleston, SC 29401 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 804 EP 804 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200007 ER PT J AU Ward, JR Bruno, J Harvell, CD Mullen, K Petes, LE Rypien, KL Sanchez, J Smith, G AF Ward, JR Bruno, J Harvell, CD Mullen, K Petes, LE Rypien, KL Sanchez, J Smith, G TI Patterns of coral diversity and disease in the Caribbean SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Cornell Univ, Ithaca, NY 14853 USA. Univ N Carolina, Chapel Hill, NC 27515 USA. Oregon State Univ, Corvallis, OR 97331 USA. Smithsonian Inst, Washington, DC 20560 USA. Univ S Carolina, Columbia, SC 29208 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 820 EP 820 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200070 ER PT J AU Srygley, RB AF Srygley, RB TI Locomotor mimicry and energetic costs of aposematic signaling in butterflies SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Smithsonian Inst, Washington, DC 20560 USA. Seoul Natl Univ, Seoul 151, South Korea. NR 0 TC 1 Z9 2 U1 0 U2 5 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 823 EP 823 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200083 ER PT J AU Hochberg, R AF Hochberg, R TI Evolutionary morphology of the head in Thaumastodermatidae (Gastrotricha). Fluid mechanics and evolutionary constraints drive historical transformation of the feeding apparatus SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Smithsonian Marine Stn, Ft Pierce, FL USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 930 EP 930 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200513 ER PT J AU Santagata, S AF Santagata, S TI Functional design of ciliary swimming in non-feeding bryozoan larvae SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Smithsonian Marine Stn, Ft Pierce, FL USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 936 EP 936 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200534 ER PT J AU Schulze, A Rice, ME AF Schulze, A Rice, ME TI Muscle development in larvae and juveniles of four Sipunculan species SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Harvard Univ, Cambridge, MA 02138 USA. Smithsonian Marine Stn, Ft Pierce, FL USA. NR 0 TC 1 Z9 1 U1 0 U2 3 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 936 EP 936 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200537 ER PT J AU Hochberg, R AF Hochberg, R TI New insights on the structure and function of gastrotrich helicoidal muscles - Evolutionary biomechanics of a contractile helix SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Smithsonian Marine Stn, Ft Pierce, FL USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 952 EP 952 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200598 ER PT J AU Hillenius, WJ Rehorek, SJ Dawson, S AF Hillenius, WJ Rehorek, SJ Dawson, S TI The preorbital apparatus of Muntjacs 2: Facial musculature SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Coll Charleston, Charleston, SC 29401 USA. Slippery Rock Univ, Slippery Rock, PA 16057 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RI Rehorek, Susan/C-3534-2009 NR 0 TC 0 Z9 0 U1 0 U2 3 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 953 EP 953 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200604 ER PT J AU West-Eberhard, MJ AF West-Eberhard, MJ TI Phenotypic accommodation: Adaptive innovation due to developmental plasticity, with or without genetic change SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 Smithsonian Trop Res Inst, Balboa, Panama. NR 0 TC 11 Z9 11 U1 9 U2 76 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 970 EP 970 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200667 ER PT J AU Wolcott, TG Wolcott, DL Hines, AH AF Wolcott, TG Wolcott, DL Hines, AH TI Exploring migration of female blue crabs to spawning grounds, using biotelemetry and CTD dataloggers. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY 2004 CL New Orleans, LA SP Soc Integrative Comparative Biol C1 N Carolina State Univ, Raleigh, NC 27695 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2003 VL 43 IS 6 BP 1001 EP 1001 PG 1 WC Zoology SC Zoology GA 831ZI UT WOS:000222235200792 ER PT J AU Shrewsbury, PM Hardin, MR AF Shrewsbury, PM Hardin, MR TI Evaluation of predatory mite (Acari : Phytoseiidae) releases to suppress spruce spider mites, Oligonychus ununguis (Acari : Tetranychidae), on Juniper SO JOURNAL OF ECONOMIC ENTOMOLOGY LA English DT Article DE augmentative biological control; natural enemies; ornamentals; integrated pest management; cost analysis ID NEOSEIULUS-FALLACIS ACARI; PEST-MANAGEMENT PROGRAM; BIOLOGICAL-CONTROL; ORNAMENTAL PLANTS; PERSIMILIS; URTICAE; ROSES; HUMIDITY; INJURY; PREFERENCE AB A laboratory trial evaluated four phytoseiid species for their potential as biological control agents of spruce spider mite, Oligonychus ununguis (Jacobi) (Acari: Tetranychidae). An augmentative biological control approach, using the predatory mites Neoseiulus fallacis Garman and Galendromus occidentalis Nesbitt (Acari: Phytoseiidae), was evaluated for reducing pest mite densities and injury, and economic costs on Juniperus chinensis 'Sargentii' A. Henry (Cupressaceae) in an outdoor nursery. Sequential releases of predator species, individually and in combination, were tested and compared with two commonly used miticides, a low-toxicity miticide, horticultural oil, and a conventional miticide, hexythiazox. Timing of treatments was based on grower-determined need, and predator release rates were based on guidelines in literature received from producers of beneficial organisms. Predator releases were more expensive and provided less effective suppression of spruce spider mites, resulting in greater spider mite injury to plants, compared with conventional pesticides. However, spider mite damage to plants did not differ in an economically meaningful way between treatments. Unsatisfactory levels of control seem related to under estimations of actual spider mite abundance based on grower perceptions and the beat sampling technique used to estimate predator release rates. These data suggest that when initial populations of spruce spider mite are high, it is unlikely that sequential releases of predator species, individually or in combination, will suppress spider mite populations. In this trial, augmentative biological control was 2.5-7 times more expensive than chemical controls. C1 Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. Smithsonian Inst, Hort Serv Div, Washington, DC 20560 USA. RP Shrewsbury, PM (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. EM pshrewsb@umd.edu NR 55 TC 10 Z9 12 U1 0 U2 5 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0022-0493 J9 J ECON ENTOMOL JI J. Econ. Entomol. PD DEC PY 2003 VL 96 IS 6 BP 1675 EP 1684 DI 10.1603/0022-0493-96.6.1675 PG 10 WC Entomology SC Entomology GA 767RY UT WOS:000188467500008 PM 14977103 ER PT J AU Greenberg, R AF Greenberg, R TI The use of nest departure calls for surveying Swamp Sparrows SO JOURNAL OF FIELD ORNITHOLOGY LA English DT Article DE bird census; bird population estimates; female vocalizations; marsh birds; point counts AB Female Swamp Sparrows (Melospiza georgiana) give a loud series of chips as they leave their nest during incubation and brooding. I tested the efficacy of basing breeding population surveys on the nest departure call (NDC). For a subset of point-count surveys designed to estimate the abundance and distribution of Swamp Sparrows in the coastal mid-Atlantic States, I surveyed singing males and (in a longer survey) the number of different females uttering NDCs. A set of 31 points was surveyed in early June and a subset of 21 in early July. The number of NDCs was well correlated with the number of singing males detected in the early season. The number of females giving NDCs was consistently smaller than the number of singing males. In part, this is because the detection distance for NDC is significantly shorter than for male song. However, even within a small fixed circular plot, more males were detected. Singing-male surveys provide more data over a shorter period of time and are appropriate for large-scale surveys. However, female NDCs provide an index of actual reproductive activity with no unmated birds included. Although a longer survey period is required, the surveys can be conducted throughout the day. It is suggested that female vocalizations related to nesting activity are more widespread than is generally appreciated and, when possible, should be used at least as complementary data to singing-male surveys. C1 Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20008 USA. RP Greenberg, R (reprint author), Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20008 USA. NR 6 TC 1 Z9 2 U1 0 U2 2 PU ASSOC FIELD ORNITHOLOGISTS PI STATESBORO PA GEORGIA SOUTHERN UNIV, DEPT BIOLOGY, STATESBORO, GA 30460-8042 USA SN 0273-8570 J9 J FIELD ORNITHOL JI J. Field Ornithol. PD WIN PY 2003 VL 74 IS 1 BP 12 EP 16 PG 5 WC Ornithology SC Zoology GA 652JP UT WOS:000181376300002 ER PT J AU Wisely, SM Golightly, RT AF Wisely, SM Golightly, RT TI Behavioral and ecological adaptations to water economy in two plethodontid salamanders, Ensatina eschscholtzii and Batrachoseps attenuatus SO JOURNAL OF HERPETOLOGY LA English DT Article ID ABSORPTION RESPONSE; ANURAN-AMPHIBIA; CALIFORNIA; MOISTURE; BUFO; FROG; SKIN AB Amphibians in general, and plethodontid salamanders in particular, are highly susceptible to cutaneous water loss. We compared behavior, habitat use, and physiology of Batrachoseps attenuatus (Eschscholtz) and Ensatina eschscholtzii (Gray) in Humboldt County, California, to identify adaptations of water economy. Both species lost more body water in a dry environment than in a wet one. In the field, sites with salamanders had higher relative humidity than sites without salamanders. In behavioral experiments, both species used water-conserving postures; they positioned themselves deep in leaf litter in dry environments while remaining on the surface of leaf litter in wet environments. The slender morphology of B. attenuatus may aid in habitat partitioning by plethodontid salamanders; in the field we found B. attenuatus closer to the surface of the leaf litter than E. eschscholtzii. The evolution of a slender body shape appears to be unconstrained by microclimates typically encountered by this species. C1 Humboldt State Univ, Dept Wildlife, Arcata, CA 95519 USA. RP Wisely, SM (reprint author), Smithsonian Inst, Genet Program, Washington, DC 20008 USA. NR 24 TC 7 Z9 8 U1 0 U2 15 PU SOC STUDY AMPHIBIANS REPTILES PI ST LOUIS PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST LOUIS, MO 63103 USA SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD DEC PY 2003 VL 37 IS 4 BP 659 EP 665 DI 10.1670/5-03A PG 7 WC Zoology SC Zoology GA 756YM UT WOS:000187513400005 ER PT J AU Williams, C Espinosa, OA Montenegro, H Cubilla, L Capson, TL Ortega-Barria, E Romero, LI AF Williams, C Espinosa, OA Montenegro, H Cubilla, L Capson, TL Ortega-Barria, E Romero, LI TI Hydrosoluble formazan XTT: its application to natural products drug discovery for Leishmania SO JOURNAL OF MICROBIOLOGICAL METHODS LA English DT Article DE XTT; Leishmania; natural products; drug discovery; aegeline; Sarcorhachis naranjoana ID PROMASTIGOTES; ASSAY AB A colorimetric method for measuring the viability of Leishmania promastigotes is described that is based on the reduction of the tetrazolium salt, XTT, to a water-soluble formazan. Values obtained by the XTT method correlated well with parasite number (r = 0.965) and with methods that rely upon the reduction of MTT or NITS (r = 0.96 and 0.97, respectively). The IC50 values obtained by XTT method with amphotericin-B, miltefosine and ketoconazole were similar to those previously reported by other methods. The XTT method proved to be a reliable and convenient method for the screening of methanolic extracts from 1059 plants and was used for the bioassay-guided fractionation of the alkaloid aegeline from Sarcorhachis naranjoana. (C) 2003 Elsevier B.V. All rights reserved. C1 Inst Invest Cientificas Avanzadas & Serv Alta Tec, Secretaria Nacl Ciencia & Tecnol, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. Univ Panama, Lab Nat Prod, Panama City, Panama. RP Romero, LI (reprint author), Inst Invest Cientificas Avanzadas & Serv Alta Tec, Secretaria Nacl Ciencia & Tecnol, POB 7250,Zona 5, Panama City, Panama. FU FIC NIH HHS [U01 TW 01021-05] NR 11 TC 42 Z9 43 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-7012 J9 J MICROBIOL METH JI J. Microbiol. Methods PD DEC PY 2003 VL 55 IS 3 BP 813 EP 816 DI 10.1016/j.mimet.2003.08.013 PG 4 WC Biochemical Research Methods; Microbiology SC Biochemistry & Molecular Biology; Microbiology GA 747UP UT WOS:000186823500029 PM 14607426 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, MC Thaddeus, P TI Geometrical structure of monobridged disilyene Si(H)SiH SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID SILICON-CONTAINING MOLECULES; LASER SPECTROSCOPY; SI2HN N=0-6; MICROWAVE; SPECTRUM; STATE; SIH3; WAVE AB By means of Fourier transform microwave spectroscopy of a supersonic molecular beam, we have detected the more abundant rare isotopic species of monobridged Si(H)SiH, and determined of its geometrical structure by isotopic substitution. Unexpected abundance anomalies of the singly deuterated isotopic species with respect to normal and Si(D)SiD were observed with equal mixtures of SiH4 and SiD4. This nonstatistical distribution is consistent with Si(H)SiH formation which is dominated by the reaction of a bare Si atom or ion with either SiH2 or SiH4. Dedicated laboratory searches were also undertaken for the remaining singlet isomer, H2SiSi, so far without success. From the absence of lines at the expected frequencies we conclude that H2SiSi is at least 50 times less abundant than Si(H)SiH. Because it is only slightly less stable than Si(H)SiH and because the barrier to isomerization is calculated to be quite low, H2SiSi may rearrange on the timescale of the supersonic expansion to Si(H)SiH. (C) 2003 Elsevier Inc. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu; pthaddeus@cfa.harvard.edu OI McCarthy, Michael/0000-0001-9142-0008 NR 26 TC 13 Z9 13 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 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD DEC PY 2003 VL 222 IS 2 BP 248 EP 254 DI 10.1016/S0022-2852(03)00231-5 PG 7 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 750JY UT WOS:000186988600012 ER PT J AU Komarneni, S Newalkar, BL Li, DS Gheyi, T Lopano, CL Heaney, PJ Post, JE AF Komarneni, S Newalkar, BL Li, DS Gheyi, T Lopano, CL Heaney, PJ Post, JE TI Anionic clays as potential slow-release fertilizers: Nitrate ion exchange SO JOURNAL OF POROUS MATERIALS LA English DT Article DE nitrate; anion exchange; anionic clay; slow-release fertilizer; synchrotron XRD ID SATURATED CLINOPTILOLITE; NATURAL ZEOLITES; PHOSPHATE ROCK; HYDROTALCITE; HYDROXIDE; OCCLUSION; MIXTURES; SAND; MICA; ZN AB Several nitrate containing anionic clays were synthesized at different temperatures and the kinetics of NO3- release were determined to test their suitability as slow-release N fertilizers. A sample (Mg:Al = 2: 1) synthesized at 60degreesC with smaller particle size released 75, 86 and 100% of its NO3- in 1, 3 and 7 days, respectively when equilibrated with a simulated soil solution. On the other hand, the 175degreesC/2 hrs sample with larger particle size released 65, 77 and 84% of its nitrate in 1, 3 and 7 days, respectively. Another anionic clay ( synthesized at 175degreesC/24 hrs) of higher charge density (Mg:Al = 2:1) containing NO3- was equilibrated with a 0.012 N NaCl or Na2CO3 to test the role of different anions in releasing the NO3- anion from the interlayers. The results showed that Cl- released more NO3- than did CO32- from this anionic clay after all the treatment times probably as a result of the CO32- anion blocking the release of NO3- from the interior of the crystals. When a lower charge density (Mg: Al = 3:1) sample (synthesized at 175degreesC/48 hrs) was equilibrated with 0.02N solution of anions the release of nitrate was as follows: Cl- < F- < SO4= less than or equal to CO32-. These results suggest that the divalent SO4= and CO32- anions are more effective in the release of NO3- from this lower charge density anionic clay. Time-resolved structural analysis of NO3- exchange with CO32- in the above anionic clay using synchrotron x-ray diffraction showed that ion exchange is rapid because of small crystal size and lower charge density. Thus the release of NO3- from anionic clays is an interplay among the type of anions present in soil solution, their concentration, pH of soil solution, the charge density and crystal size of anionic clay etc. C1 Penn State Univ, Mat Res Lab, Dept Crop & Soil Sci, University Pk, PA 16802 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Komarneni, S (reprint author), Penn State Univ, Mat Res Lab, Dept Crop & Soil Sci, University Pk, PA 16802 USA. EM komarneni@psu.edu NR 21 TC 21 Z9 23 U1 5 U2 15 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1380-2224 J9 J POROUS MAT JI J. Porous Mat. PD DEC PY 2003 VL 10 IS 4 BP 243 EP 248 DI 10.1023/B:JOPO.0000011385.19108.49 PG 6 WC Chemistry, Applied; Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA 761XC UT WOS:000187939900006 ER PT J AU Tewfik, A Guzman, HM AF Tewfik, A Guzman, HM TI Shallow-water distribution and population characteristics of Strombus gigas and S. costatus (Gastropoda : Strombidae) in Bocas del Toro, Panama SO JOURNAL OF SHELLFISH RESEARCH LA English DT Article DE queen conch; stock assessment; overfishing; Panama; Allee effect; Strombus ID QUEEN CONCH; SEAGRASS MEADOWS; COMPETITION; ABUNDANCE; BIOLOGY; FISHERY AB Extensive visual surveys for the economically and ecologically significant queen conch (Strombus gigas) and milk conch (Strombus costatus) were conducted within the Bocas del Toro archipelago. Overall population densities are among the lowest recorded in the region (S. gigas 1.43 conch ha(-1); S. costatus 1.27 conch ha(-1)), and are likely the result of overexploitation by both commercial and subsistence fishing. The very low adult densities (S. gigas 0.30 conch ha(-1)) and the lack of reproductive behaviors observed are a serious concern when one considers the "Allee effect" and the resultant negative per capita population growth rates reported elsewhere in the literature. This information has provided some of the rationale for establishing the recently announced 5-y ban on conch exploitation on the Caribbean coast of Panama. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, Miami, FL 34002 USA. EM guzmanh@naos.si.edu NR 46 TC 10 Z9 13 U1 1 U2 7 PU NATL SHELLFISHERIES ASSOC PI SOUTHAMPTON PA C/O DR. SANDRA E. SHUMWAY, NATURAL SCIENCE DIVISION, SOUTHAMPTON COLLEGE, SOUTHAMPTON, NY 11968 USA SN 0730-8000 J9 J SHELLFISH RES JI J. Shellfish Res. PD DEC PY 2003 VL 22 IS 3 BP 789 EP 794 PG 6 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 766GD UT WOS:000188365100029 ER PT J AU Reinert, JF AF Reinert, JF TI Transfer of Heizmannia thelmae from subgenus Mattinglyia to subgenus Heizmannia of genus Heizmannia and new characters for separating the two subgenera SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Article DE Culicidae; Heizmannia; Heizmannia thelmae; Mattinglyia; mosquito AB Heizmannia thelmae is formally transferred from subgenus Mattinglyia and assigned to subgenus Heizmannia. Rationale for this action is provided. New characters of the adults, female genitalia, and pupae are listed for separating the 2 subgenera of Heizmannia. C1 USDA ARS, Ctr Med Agr & Vet Entomol, CMAVE, Gainesville, FL 32608 USA. Natl Museum Nat Hist, Walter Reed Biosystemat Unit, Smithsonian Inst, Washington, DC 20560 USA. RP Reinert, JF (reprint author), USDA ARS, Ctr Med Agr & Vet Entomol, CMAVE, 1600-1700 SW 23rd Dr, Gainesville, FL 32608 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU AMER MOSQUITO CONTROL ASSOC PI EATONTOWN PA P O BOX 234, EATONTOWN, NJ 07724-0234 USA SN 8756-971X J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD DEC PY 2003 VL 19 IS 4 BP 433 EP 434 PG 2 WC Entomology SC Entomology GA 758CC UT WOS:000187614100023 PM 14710749 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The life of Henry Moore. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD DEC PY 2003 VL 128 IS 20 BP 104 EP 104 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 754YQ UT WOS:000187361400036 ER PT J AU Hutchinson, A AF Hutchinson, A TI Wolves: Behavior; ecology, and conservation. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Hutchinson, A (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 5 U2 19 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD DEC PY 2003 VL 128 IS 20 BP 158 EP 158 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 754YQ UT WOS:000187361400288 ER PT J AU Carlin, JL Robertson, DR Bowen, BW AF Carlin, JL Robertson, DR Bowen, BW TI Ancient divergences and recent connections in two tropical Atlantic reef fishes Epinephelus adscensionis and Rypticus saponaceous (Percoidei : Serranidae) SO MARINE BIOLOGY LA English DT Article ID HUMAN MITOCHONDRIAL-DNA; CYTOCHROME-B GENE; POPULATION-GROWTH; CONTINENTAL-SHELF; OCEAN CURRENTS; MARINE FISHES; PHYLOGEOGRAPHY; EVOLUTION; TELEOSTEI; RESTRICTION AB Reef habitats of the tropical Atlantic are separated by river outflows and oceanic expanses that may preclude larval dispersal or other population connections in shorefishes. To examine the impact of these habitat discontinuities on the intraspecific phylogeography of reef-associated species we conducted range-wide surveys of two amphi-Atlantic reef fishes that have dispersive pelagic larval stages. Based on 593 bp of mtDNA cytochrome b from the rock hind Epinephelus adscensionis and 682 bp from the greater soapfish Rypticus saponaceous (n=109 and 86, respectively), we found evidence of relatively ancient separations as well as recent surmounting of biogeographic barriers by dispersal or colonization. Rock hind showed slight but significant population genetic differentiation across much of the tropical Atlantic Ocean (Phi(ST)=0.056), but deep divergence between the southeastern United States and seven other localities from the Bahamas to the south, central and east Atlantic (mean pairwise d=0.040, overall Phi(ST)=0.867). The geographic distribution of the two rock hind lineages is highly unusual in genetic studies of Caribbean Sea reef fishes, because those lineages are separated by less than 250 km of open water within a major biogeographic region. In contrast, highly significant population genetic structure was observed among greater soapfish from the SW Caribbean, Brazil, and mid-Atlantic ridge (Phi(ST)=0.372), with a deep evolutionary separation distinguishing putative R. saponaceous from West Africa (mean pairwise d=0.044, overall Phi(ST)=0.929). Both species show evidence for a potential connection between the Caribbean and Brazilian provinces. While widespread haplotype sharing in rock hind indicates that larvae of this species cross oceanic expanses of as much as 2000 km, such a situation is difficult to reconcile with the isolation of populations in Florida and the Bahamas separated by only 250 km. These findings indicate that populations of some species in disjunct biogeographic zones may be isolated for long periods, perhaps sufficient for allopatric speciation, but rare gene flow between zones may preclude such evolutionary divergence in other species. C1 Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. Whitman Coll, Dept Biol, Walla Walla, WA 99362 USA. Smithsonian Trop Res Inst Panama, APO, AA 34002 USA. RP Univ Hawaii, Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA. EM bbowen@hawaii.edu NR 78 TC 35 Z9 35 U1 0 U2 21 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD DEC PY 2003 VL 143 IS 6 BP 1057 EP 1069 DI 10.1007/s00227-003-1151-3 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 749XB UT WOS:000186954400003 ER PT J AU Lampert, KP Rand, AS Mueller, UG Ryan, MJ AF Lampert, KP Rand, AS Mueller, UG Ryan, MJ TI Fine-scale genetic pattern and evidence for sex-biased dispersal in the tungara frog, Physalaemus pustulosus SO MOLECULAR ECOLOGY LA English DT Article DE gene-flow barrier; male-biased dispersal; metapopulation; microsatellite marker; population genetics ID METAPOPULATION PROCESSES; MICROSATELLITE ANALYSIS; POPULATION-STRUCTURE; NATTERJACK TOAD; RANA-TEMPORARIA; BUFO-CALAMITA; DIFFERENTIATION; EVOLUTION; MAMMALS; FLOW AB Tungara frogs (Physalaemus pustulosus) are a model system for sexual selection and communication. Population dynamics and gene flow are of major interest in this species because they influence speciation processes and microevolution, and could consequently provide a deeper understanding of the evolutionary processes involved in mate recognition. Although earlier studies have documented genetic variation across the species' range, attempts to investigate dispersal on a local level have been limited to mark-recapture studies. These behavioural studies indicated high mobility at a scale of several hundred metres. In this study we used seven highly polymorphic microsatellite loci to investigate fine-scaled genetic variation in the tungara frog. We analysed the influence of geographical distance on observed genetic patterns, examined the influence of a river on gene flow, and tested for sex-biased dispersal. Data for 668 individuals from 17 populations ranging in distance from 0.26 to 11.8 km revealed significant levels of genetic differentiation among populations. Genetic differentiation was significantly correlated with geographic distance. A river acted as an efficient barrier to gene flow. Several tests of sex-biased dispersal were conducted. Most of them showed no difference between the sexes, but variance of Assignment Indices exhibited a statistically significant male bias in dispersal. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Lampert, KP (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. NR 42 TC 90 Z9 92 U1 2 U2 23 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD DEC PY 2003 VL 12 IS 12 BP 3325 EP 3334 DI 10.1046/j.1365-294X.2003.02016.x PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 744TF UT WOS:000186648400012 PM 14629349 ER PT J AU Dumbacher, JP Pratt, TK Fleischer, RC AF Dumbacher, JP Pratt, TK Fleischer, RC TI Phylogeny of the owlet-nightjars (Aves : Aegothelidae) based on mitochondrial DNA sequence SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Aegothelidae; owlet-nightjar; phylogeny; mitochondrial DNA; biogeography; maximum likelihood; molecular systematics; systematics ID ANCIENT DNA; MODEL; CAPRIMULGIFORMES; PHYLOGEOGRAPHY; SUBSTITUTION; EVOLUTION; ALLIES AB The avian family Aegothelidae (Owlet-nightjars) comprises nine extant species and one extinct species, all of which are currently classified in a single genus, Aegotheles. Owlet-nightjars are secretive nocturnal birds of the South Pacific. They are relatively poorly studied and some species are known from only a few specimens. Furthermore, their confusing morphological variation has made it difficult to cluster existing specimens unambiguously into hierarchical taxonomic units. Here we sample all extant owlet-nightjar species and all but three currently recognized subspecies. We use DNA extracted primarily from museum specimens to obtain mitochondrial gene sequences and construct a molecular phylogeny. Our phylogeny suggests that most species are reciprocally monophyletic, however A. albertisi appears paraphyletic. Our data also suggest splitting A. bennettii into two species and splitting A. insignis and A. tatei as suggested in another recent paper. (C) 2003 Elsevier Science (USA). All rights reserved. C1 Smithsonian Inst, Dept Conservat Biol, Conservat & Res Ctr, Washington, DC 20008 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Genet Program, Washington, DC 20008 USA. RP Dumbacher, JP (reprint author), Smithsonian Inst, Dept Conservat Biol, Conservat & Res Ctr, Washington, DC 20008 USA. NR 37 TC 39 Z9 39 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD DEC PY 2003 VL 29 IS 3 BP 540 EP 549 DI 10.1016/S1055-7903(03)00135-0 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 746GE UT WOS:000186738000013 PM 14615192 ER PT J AU O'Sullivan, E Vrtilek, JM Read, AM David, LP Ponman, TJ AF O'Sullivan, E Vrtilek, JM Read, AM David, LP Ponman, TJ TI An XMM-Newton observation of the galaxy group MKW 4 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : individual : MKW4; galaxies : individual : NGC 4073; X-rays : galaxies; X-rays : galaxies : clusters ID REFLECTION GRATING SPECTROMETER; X-RAY SPECTROSCOPY; POOR CLUSTERS; HIGH-RESOLUTION; COOLING FLOWS; CHANDRA; INTERSTELLAR; PROFILES; ASCA; GAS AB We present an X-ray study of the galaxy group or poor cluster MKW 4. Working with XMM-Newton data we examine the distribution and properties of the hot gas which makes up the group halo. The inner halo shows some signs of structure, with circular or elliptical beta models providing a poor fit to the surface brightness profile. This may be evidence of large-scale motion in the inner halo, but we do not find evidence of sharp fronts or edges in the emission. The temperature of the halo declines in the core, with deprojected spectral fits showing a central temperature of similar to1.3 keV compared to similar to3 keV at 100 kpc. In the central similar to30 kpc of the group, multitemperature spectral models are required to fit the data, but they indicate a lack of gas at low temperatures. Steady-state cooling flow models provide poor fits to the inner regions of the group and the estimated cooling time of the gas is long except within the central dominant galaxy, NGC 4073. Abundance profiles show a sharp increase in the core of the group, with mean abundance rising by a factor of 2 in the centre of NGC 4073. Fitting individual elements shows the same trend, with high values of Fe, Si and S in the core. We estimate that similar to50 per cent of the Fe in the central 40 kpc was injected by Type Ia supernovae, in agreement with previous ASCA studies. Using our best-fitting surface brightness and temperature models, we calculate the mass, gas fraction, entropy and mass-to-light ratio of the group. At 100 kpc (similar to0.1 virial radius) the total mass and gas entropy of the system (similar to2 x 10(13) M-. and similar to300 keV cm(2)) are quite comparable to those of other systems of similar temperature, but the gas fraction is rather low (similar to1 per cent). We conclude that MKW 4 is a fairly relaxed group, which has developed a strong central temperature gradient but not a large-scale cooling flow. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI O'Sullivan, Ewan/0000-0002-5671-6900 NR 53 TC 21 Z9 21 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2003 VL 346 IS 2 BP 525 EP 539 DI 10.1046/j.1365-2966.2003.07108.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745QE UT WOS:000186698700022 ER PT J AU Little, AEF Murakami, T Mueller, UG Currie, CR AF Little, AEF Murakami, T Mueller, UG Currie, CR TI The infrabuccal pellet piles of fungus-growing ants SO NATURWISSENSCHAFTEN LA English DT Article ID FORMICIDAE; HYMENOPTERA; POCKET AB Fungus-growing ants (Attini) live in an obligate mutualism with the fungi they cultivate for food. Because of the obligate nature of this relationship, the success of the ants is directly dependent on their ability to grow healthy fungus gardens. Attine ants have evolved complex disease management strategies to reduce their garden's exposure to potential parasitic microbes, to prevent the establishment of infection in their gardens, and to remove infected garden sections. The infrabuccal pocket, a filtering device located in the oral cavity of all ants, is an integral part of the mechanisms that leaf-cutter ants use to prevent the invasion and spread of general microbial parasites and the specific fungal-garden parasite Escovopsis. Fungus-growing ants carefully groom their garden, collecting general debris and pathogenic spores of Escovopsis in their infrabuccal pocket, the contents of which are later expelled in dump chambers inside the nest or externally. In this study we examined how a phylogenetically diverse collection of attine ants treat their infrabuccal pellets. Unlike leaf-cutters that deposit their infrabuccal pellets directly in refuse piles, ants of the more basal attine lineages stack their infrabuccal pellets in piles located close to their gardens, and a separate caste of workers is devoted to the construction, management, and eventual disposal of these piles. C1 Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Univ Texas, Patterson Labs, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Little, AEF (reprint author), Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. NR 12 TC 20 Z9 23 U1 1 U2 18 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD DEC PY 2003 VL 90 IS 12 BP 558 EP 562 DI 10.1007/s00114-003-0480-x PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 754HK UT WOS:000187309900003 PM 14676952 ER PT J AU Feuillet, C AF Feuillet, C TI Three new species of Cordia (Boraginaceae) from the Guianas SO NOVON LA English DT Article DE Boraginaceae; Cordia; french Guiana; Guyana; sect. Myxa; sect. Varrornia AB Three new species of Cordia (Boraginaceae) are described from the Guianas. Cordia cremersii and C. marioniae belong in section Varronia, and C. fanchoniae in section Myxa. Cordia marioniae is known from the Rupununi savanna in the south of Guyana; the two other species have been collected in French Guiana. C1 Smithsonian Inst, Dept Syst Biol Bot, MRC 166, Washington, DC 20013 USA. RP Feuillet, C (reprint author), Smithsonian Inst, Dept Syst Biol Bot, MRC 166, POB 3712, Washington, DC 20013 USA. NR 12 TC 0 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 WIN PY 2003 VL 13 IS 4 BP 433 EP 437 DI 10.2307/3393375 PG 5 WC Plant Sciences SC Plant Sciences GA 753BU UT WOS:000187212500011 ER PT J AU Harlow, GE Sisson, VB Lallemant, HGA Sorensen, SS Seitz, R AF Harlow, GE Sisson, VB Lallemant, HGA Sorensen, SS Seitz, R TI High-pressure, metasomatic rocks along the Motagua fault zone, Guatemala SO OFIOLITI LA English DT Article; Proceedings Paper CT IGCP 433 Workshop/2nd Italian-Latin American Geological Meeting CY JAN 28, 2002 CL CIUDAD DE GUATEMALA, GUATEMALA DE jadeitite; eclogite; serpentinite; plate boundary; suture zone; high P/T; metasomatism; Guatemala ID NORTH-AMERICAN PLATES; RELATIVE MOTION; GEOTHERMOMETER; SERPENTINITE; CALIBRATION; DEFORMATION; JADEITITES; INCLUSIONS; ECLOGITES; ALBITITES AB The Motagua River of Guatemala follows the Motagua fault zone, the present plate boundary zone between the North American (Maya block) and Caribbean (Chortis block) plates. The central Motagua River valley is bordered by E-W-striking tectonic slices of serpentinite, some of which contain blocks of high pressure/low temperature (high P/T) eclogite, garnet amphibolite, and jadeitite. Recent exploration for commercial jadeitite (jade) has discovered considerable quantities of high P/T rocks in serpentinite bodies both further along and farther from the river. The southern bodies, south of the Motagua fault zone and adjacent to Chortis basement, also contain abundant eclogite, glaucophane eclogite, blueschist, jadeitite, and other high P/T rocks. The northern bodies, adjacent to Maya basement, include abundant jadeitite, albitite, and garnet amphibolite, but rare eclogite. Our initial studies find metasomatic signatures in most of the high-P/T rocks (e.g., phengite and quartz in veins, oscillatory zoning of jadeite and phengite, etc.). Mineralogical differences between jadeitites from the northern and southern bodies, and the different lithotectonic assemblages on the two sides of the Motagua fault zone suggest that either two high P/T events have occurred, or the two belts may be a single unit disrupted by strike slip duplexing. C1 Rice Univ, Dept Earth Sci, Houston, TX 77005 USA. Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. Natl Museum Nat Hist, Dept Mineral Sci, NHB 119, Smithsonian Inst, Washington, DC 20560 USA. RP Sisson, VB (reprint author), Rice Univ, Dept Earth Sci, MS-126, Houston, TX 77005 USA. NR 46 TC 21 Z9 22 U1 0 U2 6 PU OFIOLITI PI FIRENZE PA DIPARTIMENTO DI SCIENZE DELLA TERRA, UNIVERSITA DI FIRENZE, VIA G LA PIRA 4,, 50121 FIRENZE, ITALY SN 0391-2612 J9 OFIOLITI JI Ofioliti PD DEC PY 2003 VL 28 IS 2 BP 115 EP 120 PG 6 WC Geology SC Geology GA 760BM UT WOS:000187790700004 ER PT J AU Greenstein, BJ Pandolfi, JM AF Greenstein, BJ Pandolfi, JM TI Taphonomic alteration of reef corals: Effects of reef environment and coral growth form II: The Florida Keys SO PALAIOS LA English DT Article ID GREAT-BARRIER-REEF; CAVITY-DWELLERS COELOBITES; PAPUA-NEW-GUINEA; COMMUNITY STRUCTURE; DAMSELFISH TERRITORIALITY; DEATH ASSEMBLAGES; INTERNAL BIOEROSION; CONTINENTAL-SHELF; HUON PENINSULA; RUBBLE AB In a companion study to earlier work in the Indo-Pacific, taphonomic alteration in reef-coral death assemblages was assessed in four distinct reef habitats ranging from 2-30 m water depth in the Florida Keys reef tract. Physical and biological taphonomic attributes measured from coral specimens showed great variability with respect to reef environment. Physico-chemical degradation (abrasion and dissolution) was greatest in reef-crest and patch-reef environments. With the exception of encrusting foraminifera, coverage by epi- and endobionts was higher in deep-reef environments (20 m and 30 m). Variability in dissolution and abrasion is likely the result of the different energy regimes present in the reef habitats examined. Variability in biological attributes results from a combination of increased residence time of coral skeletons on substrates in deep-reef environments, higher overall coral skeletal densities of corals inhabiting deep reef environments, and increased nutrient availability in the deep reefs sampled. Clear gradients in the degree of taphonomic alteration of reef corals with reef habitat indicate the utility of corals as taphofacies indicators in ancient reef settings. In contrast to shallow-water reefs on the Great Barrier Reef, taphonomic alteration of corals in the Florida Keys was equitable across growth forms. C1 Cornell Coll, Dept Geol, Mt Vernon, IA 52314 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Greenstein, BJ (reprint author), Cornell Coll, Dept Geol, Mt Vernon, IA 52314 USA. RI Pandolfi, John/A-3121-2009 OI Pandolfi, John/0000-0003-3047-6694 NR 90 TC 23 Z9 25 U1 0 U2 6 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 DEC PY 2003 VL 18 IS 6 BP 495 EP 509 DI 10.1669/0883-1351(2003)018<0495:TAORCE>2.0.CO;2 PG 15 WC Geology; Paleontology SC Geology; Paleontology GA 758TF UT WOS:000187665700003 ER PT J AU Sims, HJ AF Sims, HJ TI Measures of global biodiversity dynamics (past and present) are meaningless... or are they? Introductory comments SO PALEOBIOLOGY LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Sims, HJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. NR 0 TC 2 Z9 4 U1 1 U2 2 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD WIN PY 2003 VL 29 IS 1 BP 1 EP 2 DI 10.1666/0094-8373(2003)029<0001:MOGBDP>2.0.CO;2 PG 2 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 644MN UT WOS:000180922000001 ER PT J AU Behrensmeyer, AK Stayton, CT Chapman, RE AF Behrensmeyer, AK Stayton, CT Chapman, RE TI Taphonomy and ecology of modern avifaunal remains from Amboseli Park, Kenya SO PALEOBIOLOGY LA English DT Article ID FOSSIL; DISARTICULATION; ASSEMBLAGE; SEDIMENTS; PATTERNS; RECORD; BIRDS AB Avian skeletal remains occur in many fossil assemblages, and in spite of small sample sizes and incomplete preservation, they may be a source of valuable paleoecological information. In this paper, we examine the taphonomy of a modern avian bone assemblage and test the relationship between ecological data based on avifaunal skeletal remains and known ecological attributes of a living bird community. A total of 54 modern skeletal occurrences and a sample of 126 identifiable bones from Amboseli Park, Kenya, were analyzed for weathering features and skeletal part preservation in order to characterize preservation features and taphonomic biases. Avian remains, with the exception of ostrich, decay more rapidly than adult mammal bones and rarely reach advanced stages of weathering. Breakage and the percentage of anterior limb elements serve as indicators of taphonomic overprinting that may affect paleoecological signals. Using ecomorphic categories including body weight, diet, and habitat, we compared species in the bone assemblage with the living Amboseli avifauna. The documented bone sample is biased toward large body size, representation of open grassland habitats, and grazing or scavenging diets. In spite of this, multidimensional scaling analysis shows that the small faunal sample (16 out of 364 species) in the pre-fossil bone assemblage accurately represents general features of avian ecospace in Amboseli. This provides a measure of the potential fidelity of paleoecological reconstructions based on small samples of avian remains. In the Cenozoic, the utility of avian fossils is enhanced because bird eco-morphology is relatively well known and conservative through time, allowing back-extrapolations of habitat preferences, diet, etc. based on modern taxa. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Univ Chicago, Dept Geol & Geophys, Chicago, IL 60637 USA. Smithsonian Inst, Natl Museum Nat Hist, Appl Morphometr Lab, Washington, DC 20560 USA. RP Behrensmeyer, AK (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Box 37012, Washington, DC 20013 USA. NR 47 TC 45 Z9 49 U1 0 U2 2 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD WIN PY 2003 VL 29 IS 1 BP 52 EP 70 DI 10.1666/0094-8373(2003)029<0052:TAEOMA>2.0.CO;2 PG 19 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 644MN UT WOS:000180922000013 ER PT J AU Royer, DL Hickey, LJ Wing, SL AF Royer, DL Hickey, LJ Wing, SL TI Ecological conservatism in the "living fossil" Ginkgo SO PALEOBIOLOGY LA English DT Review ID PLATANUS-OCCIDENTALIS SEEDLINGS; POTENT INSECTICIDAL ACTIVITY; RIBOSOMAL-RNA SEQUENCES; PALEOBOTANICAL EVIDENCE; NILAPARVATA-LUGENS; BILOBA LEAVES; LAND PLANTS; SEED SIZE; VEGETATION; PHYLOGENY AB The living species Ginkgo biloba is phylogenetically isolated, has a relictual distribution, and is morphologically very similar to Mesozoic and Cenozoic congenerics. To investigate what adaptations may have allowed this lineage to persist with little or no morphological change for over 100 Myr, we analyzed both sedimentological and floral data from 51 latest Cretaceous to middle Miocene Ginkgo-bearing fossil plant sites in North America and northern Europe. The resulting data indicate that throughout the late Cretaceous and Cenozoic Ginkgo was largely confined to disturbed streamside and levee environments, where it occurred with a consistent set of other plants. These inferred habitats are surprising because the life-history traits of Ginkgo (e.g., slow growth rate, late reproductive maturity, extended reproductive cycle, large and complex seeds, large and slowly developing embryos) are counter to those considered advantageous in modern disturbed habitats. Many flowering plant lineages first appeared or became common in disturbed riparian habitats, and are inferred to have had reproductive and growth traits (e.g., rapid reproduction, small easily dispersed seeds, rapid growth) suited to such habitats. Paleoecological inferences based on both morphology and sedimentary environments thus support the idea that Ginkgo was displaced in riparian habitats by angiosperms with better adaptations to frequent disturbance. C1 Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Royer, DL (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. OI Royer, Dana/0000-0003-0976-953X; Wing, Scott/0000-0002-2954-8905 NR 121 TC 73 Z9 91 U1 4 U2 35 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD WIN PY 2003 VL 29 IS 1 BP 84 EP 104 DI 10.1666/0094-8373(2003)029<0084:ECITLF>2.0.CO;2 PG 21 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 644MN UT WOS:000180922000015 ER PT J AU Hora, JL AF Hora, JL TI Right place, wrong time SO PHOTONICS SPECTRA LA English DT Letter C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Hora, JL (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU LAURIN PUBL CO INC PI PITTSFIELD PA BERKSHIRE COMMON PO BOX 1146, PITTSFIELD, MA 01202 USA SN 0731-1230 J9 PHOTON SPECTRA JI Photon. Spect. PD DEC PY 2003 VL 37 IS 12 BP 12 EP 12 PG 1 WC Optics SC Optics GA 768VP UT WOS:000188556000003 ER PT J AU Humphrey, MA Phillips, DF Mattison, EM Vessot, RFC Stoner, RE Walsworth, RL AF Humphrey, MA Phillips, DF Mattison, EM Vessot, RFC Stoner, RE Walsworth, RL TI Testing CPT and Lorentz symmetry with hydrogen masers SO PHYSICAL REVIEW A LA English DT Article ID HIGHER-DIMENSIONAL THEORIES; VIOLATION; STRINGS; TRANSITIONS; INVARIANCE; ELECTRON; MODEL AB In a recent paper [Phys. Rev. D 63, 111101 (2001)] we reported a new limit on CPT (charge, parity, and time reversal) and Lorentz violation of the proton by using a hydrogen maser to search for a sidereal variation of the F=1, Deltam(F)=+/-1 Zeeman frequency in atomic hydrogen. Here we discuss the theoretical interpretation of this recent experiment, the operating principles of the maser, and the double-resonance technique used to measure the Zeeman frequency. We also describe the characterization of systematic effects and details of the data analysis. We conclude by comparing our result to other recent experiments, and discussing potential improvements to the hydrogen maser double-resonance technique. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 35 TC 70 Z9 70 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD DEC PY 2003 VL 68 IS 6 AR 063807 DI 10.1103/PhysRevA.68.063807 PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 761DP UT WOS:000187885000102 ER PT J AU Marian, P Marian, TA Scutaru, H AF Marian, P Marian, TA Scutaru, H TI Bures distance as a measure of entanglement for two-mode squeezed thermal states SO PHYSICAL REVIEW A LA English DT Article ID CONTINUOUS VARIABLE SYSTEMS; SEPARABILITY CRITERION; STATISTICAL DISTANCE; GAUSSIAN STATES; QUANTUM STATES; NOISE; TELEPORTATION; FIDELITY; COHERENT; INSEPARABILITY AB We propose a reliable entanglement measure for a two-mode squeezed thermal state of the quantum electromagnetic field in terms of its Bures distance to the set of all separable states of the same kind. The requisite fidelity of a pair of two-mode squeezed thermal states is exactly evaluated. By applying the Peres-Simon criterion of separability, we find the closest separable state. This enables us to establish an insightful expression of the amount of entanglement. We also derive the relative entropy of a two-mode squeezed thermal state with respect to another one. This quantity is exploited in the pure-state case by undertaking a similar approximation for the entropic entanglement of a two-mode squeezed vacuum state. Comparison with previous work lends support to our approach that replaces the reference set of all separable Gaussian states by its subset consisting only of the squeezed thermal ones. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. Univ Bucharest, Dept Chem, R-030018 Bucharest, Romania. Univ Bucharest, Dept Phys, R-077125 Bucharest, Romania. Romanian Acad, Ctr Adv Studies Phys, R-050711 Bucharest, Romania. RP Marian, P (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 49 TC 60 Z9 60 U1 0 U2 4 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD DEC PY 2003 VL 68 IS 6 AR 062309 DI 10.1103/PhysRevA.68.062309 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 761DP UT WOS:000187885000027 ER PT J AU Eltz, T Roubik, DW Whitten, MW AF Eltz, T Roubik, DW Whitten, MW TI Fragrances, male display and mating behaviour of Euglossa hemichlora: a flight cage experiment SO PHYSIOLOGICAL ENTOMOLOGY LA English DT Article DE copulatory behaviour; female choice; fragrance exposure; mating; GC-MS; orchid bees; sexual selection; territorial behaviour; velvet area ID MALE ORCHID BEES; APIDAE; HYMENOPTERA; COLLECTION AB Male euglossine bees (Apidae: Euglossini) collect volatile substances (fragrances) from floral and nonfloral sources and store them in hair-filled cavities in their hind tibiae. Over time, males accumulate large quantities of complex and species-specific blends of fragrances. Various hypotheses have been put forward to explain this behaviour, including the idea that fragrance stores reflect the genetic quality of individual males and have evolved through sexual selection and female choice. Clear support of this hypothesis is lacking, largely because male-female interactions are both rare and difficult to observe in nature. Here, we report a flight cage experiment performed in Panama that permitted mating between virgin females (raised from brood cells) and males captured in the forest at fragrance baits. In the cage, eight individually marked males defended small territories around vertical perch sites and showed a characteristic display, which included a previously unreported 'leg-crossing' movement, possibly related to fragrance release. A total of six copulations and three copulatory attempts by Euglossa hemichlora were observed and partly recorded on video. The copulations, all of which were initiated by the female landing on a male perch, were short (4-10 s) and showed no signs of the transfer of chemical substances from male to female. In some cases, the male hovered directly over the female before descending to mount her, possibly facilitating fragrance evaluation by the female. After the experiment, the contents of the males' hind legs were analysed by gas chromatography-mass spectroscopy, which detected complex mixtures of terpenoids and aromatics (totalling 70 different compounds) dominated by hexahydrofarnesyl acetone, farnesene epoxide, ocimene and p-dimethoxy benzene. Individual total amounts of fragrances were neither related to display activity or perch occupancy by given males, nor to the frequency of matings achieved. Display activity was the only positive correlate of mating frequency. Generally, individuals had uniformly large amounts of stored fragrances in comparison to a previous study of three other species of Panamanian Euglossa. C1 Univ Dusseldorf, Dept Neurobiol, D-40225 Dusseldorf, Germany. Smithsonian Trop Res Inst, Balboa, Panama. Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Eltz, T (reprint author), Univ Dusseldorf, Dept Neurobiol, Univ Str 1, D-40225 Dusseldorf, Germany. NR 22 TC 33 Z9 34 U1 5 U2 11 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0307-6962 J9 PHYSIOL ENTOMOL JI Physiol. Entomol. PD DEC PY 2003 VL 28 IS 4 BP 251 EP 260 DI 10.1111/j.1365-3032.2003.00340.x PG 10 WC Entomology SC Entomology GA 753XL UT WOS:000187256800002 ER PT J AU Symmes, M AF Symmes, M TI Splendid pages: The Molly and Walter Bareiss Collection of modern illustrated books SO PRINT QUARTERLY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Symmes, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PRINT QUART LTD PI LONDON PA 80 CARLTON HILL, LONDON NW8 0ER, ENGLAND SN 0265-8305 J9 PRINT Q JI Print Q. PD DEC PY 2003 VL 20 IS 4 BP 428 EP 434 PG 7 WC Art SC Art GA 766ZA UT WOS:000188412600039 ER PT J AU Comizzoli, P Wildt, DE Pukazhenthi, BS AF Comizzoli, P Wildt, DE Pukazhenthi, BS TI Overcoming poor in vitro nuclear maturation and developmental competence of domestic cat oocytes during the non-breeding season SO REPRODUCTION LA English DT Article ID FOLLICLE-STIMULATING-HORMONE; INTRACYTOPLASMIC SPERM INJECTION; EMBRYO DEVELOPMENT; BOVINE OOCYTES; ASCORBIC-ACID; PIG OOCYTES; PROTEIN SUPPLEMENTATION; MALE PRONUCLEUS; GROWTH-HORMONE; FERTILIZATION AB The domestic cat experiences circannual variations in ovarian activity and intrafollicular oocyte quality. One result is poor nuclear and cytoplasmic maturation during in vitro maturation (IVM) conducted during the annual non-breeding season (July through November). In an attempt to overcome this seasonal phenomenon immature oocytes were collected from July through November and cultured in a conventional IVM medium (IVM1) or in IVM1 supplemented with different FSH concentrations and antioxidant (ascorbic acid or cysteine). Nuclear status of oocytes was assessed after IVM or IVF. Embryo stage and blastocyst quality were evaluated after 7 days of in vitro culture. Although the addition of antioxidant alone had no effect, the presence of 10 mug FSH ml(-1) improved nuclear maturation (75.4 +/- 4.1% versus 48.7 +/- 8.8% in IVM1; P<0.05) and fertilization success (47.9 +/- 3.2% versus 35.0 +/- 5.1% in IVM1; P<0.05). Furthermore, developmental competence of fertilized oocytes was enhanced (P < 0.05) only in the presence of ascorbic acid (30.6 +/- 6.7%) or cysteine (33.6 +/- 5.1%) compared with IVM1 (8.1 +/- 8.8%). Consequently, blastocyst yield (17% of total oocytes cultured) was highest when oocytes were matured in medium containing higher FSH concentration and antioxidants. The results of this study demonstrate that meiotic and developmental competences are inherent to the immature cat oocyte collected during the non-breeding season. However, appropriate mechanisms (perhaps seasonal variation in FSH receptors or lack of antioxidant capacity of the cumulus-oocyte complex) are inadequate during this period of gonadal quiescence. Regardless, this compromised oocyte function during the non-breeding season can be overridden by altering in vitro culture conditions to include supplemental FSH and antioxidant. C1 Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. RP Comizzoli, P (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM comizzolip@nzp.si.edu FU NCRR NIH HHS [K01 RR00135] NR 49 TC 35 Z9 36 U1 0 U2 8 PU BIOSCIENTIFICA LTD PI BRISTOL PA EURO HOUSE, 22 APEX COURT WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT, ENGLAND SN 1470-1626 J9 REPRODUCTION JI Reproduction PD DEC PY 2003 VL 126 IS 6 BP 809 EP 816 DI 10.1530/rep.0.1260809 PG 8 WC Developmental Biology; Reproductive Biology SC Developmental Biology; Reproductive Biology GA 762MU UT WOS:000187976800013 PM 14748700 ER PT J AU Litwak, RS AF Litwak, RS TI Non-proliferation and the dilemmas of regime change SO SURVIVAL LA English DT Article AB The Iraq war was unprecedented in at least one respect: it was the first case in which forcible regime change was the means employed to achieve non-proliferation ends. In addressing the current proliferation crises with North Korea and Iran, however, the Bush administration confronts major constraints on both the use of force and the US ability to bring about regime change. This has prompted a shift in strategy to the alternative combination of deterrence and reassurance. Implementing a strategy of deterrence and reassurance requires effective policy coordination to ensure that the two components are in sync. Military moves for purposes of deterrence should not undercut the message of political reassurance and thereby provide further incentive for either country to cross the nuclear threshold. C1 Smithsonian Inst, Woodrow Wilson Ctr, Washington, DC 20560 USA. RP Litwak, RS (reprint author), Smithsonian Inst, Woodrow Wilson Ctr, Washington, DC 20560 USA. NR 37 TC 11 Z9 11 U1 1 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0039-6338 J9 SURVIVAL JI Survival PD WIN PY 2003 VL 45 IS 4 BP 7 EP + DI 10.1080/00396330312331343566 PG 26 WC International Relations; Political Science SC International Relations; Government & Law GA 753KY UT WOS:000187231600001 ER PT J AU Nepokroeff, M Sytsma, KJ Wagner, WL Zimmer, EA AF Nepokroeff, M Sytsma, KJ Wagner, WL Zimmer, EA TI Reconstructing ancestral patterns of colonization and dispersal in the Hawaiian understory tree genus Psychotria (Rubiaceae): A comparison of parsimony and likelihood approaches SO SYSTEMATIC BIOLOGY LA English DT Review DE ancestral character state reconstruction; biogeography; ETS; Hawai'i; island evolution; ITS; molecular systematics; Psychotria ID NUCLEAR RIBOSOMAL DNA; EXTERNAL TRANSCRIBED SPACER; NORTH-AMERICAN ORIGIN; PHYLOGENETIC ANALYSES; DISCRETE CHARACTERS; MAXIMUM-LIKELIHOOD; SEQUENCE DATA; 18S-26S RDNA; MOLECULAR SYSTEMATICS; CONCERTED EVOLUTION AB Systematic and biogeographical relationships within the Hawaiian clade of the pantropical understory shrub genus Psychotria ( Rubiaceae) were investigated using phylogenetic analysis of 18S - 26S ribosomal DNA internal ( ITS) and external ( ETS) transcribed spacers. Phylogenetic analyses strongly suggest that the Hawaiian Psychotria are monophyletic and the result of a single introduction to the Hawaiian Islands. The results of phylogenetic analyses of ITS and ETS partitions alone give slightly different topologies among basal lineages of the Hawaiian clade; however, such differences are not well supported. Relationships in the section Straussia clade in particular are not well resolved because of few nucleotide changes on internal branches, suggesting extremely rapid radiation in the lineage. Parsimony and likelihood reconstructions of ancestral geographical distributions using the topologies inferred from both parsimony and likelihood analysis of combined data and using different combinations of models and branch lengths gave highly congruent results. However, for one internal node ( corresponding to the majority of the " greenwelliae" clade), parsimony reconstructions were unable to distinguish between three possible island states, whereas likelihood reconstructions resulted in clear ordering of possible states, with the island of O` ahu slightly more probable than other islands under all but one model and branch length combination considered ( the Jukes - Cantor- like model with branch lengths inferred under parsimony, under which conditions Maui Nui is more probable). A pattern of colonization from oldest to youngest islands was inferred from the phylogeny, using maximum parsimony and maximum likelihood. Additionally, a much higher incidence of intraisland versus interisland speciation was inferred. C1 Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA. Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Smithsonian Inst, MRC 534, MSC, Lab Analyt Biol, Suitland, MD 20746 USA. RP Nepokroeff, M (reprint author), Univ S Dakota, Dept Biol, 414 E Clark St, Vermillion, SD 57069 USA. RI Zimmer, Elizabeth/G-3890-2011 NR 102 TC 63 Z9 63 U1 0 U2 19 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD DEC PY 2003 VL 52 IS 6 BP 820 EP 838 DI 10.1080/10635150390251072 PG 19 WC Evolutionary Biology SC Evolutionary Biology GA 752UH UT WOS:000187185200006 PM 14668119 ER PT J AU Cambra, RA Quintero, D AF Cambra, RA Quintero, D TI Description of the previously unknown male of the neotropical genus Hoplognathoca suarez and new distribution records (Hymenoptera : Mutillidae : Sphaeropthalminae) SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Hoplognathoca; male description; systematics AB The male of the Neotropical genus Hoplognathoca Suarez is described and illustrated for the first time, based on sex association of Hoplognathoca nodifrons (Gerstaecker, 1874) from Panama. Comments about the association of the sexes are made. Hoplognathoca costarricensis Suarez, 1962 and H. nodifrons, are recorded for the first time from Panama, both species were known previously only from their female holotypes, from Costa Rica and Colombia, respectively. C1 Univ Panama, Estafeta Univ, Museo Invertebrados GB Fairchild, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. RP Cambra, RA (reprint author), Univ Panama, Estafeta Univ, Museo Invertebrados GB Fairchild, Panama City, Panama. EM rcambra@ancon.up.ac.pa; QUINTERD@tivoli.si.edu NR 5 TC 3 Z9 3 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD DEC PY 2003 VL 129 IS 3-4 BP 487 EP 495 PG 9 WC Entomology SC Entomology GA 763DN UT WOS:000188059600006 ER PT J AU Cambra, RA Quintero, D AF Cambra, RA Quintero, D TI Tallium lattkei n. sp (Hymenoptera : Mutillidae) from Venezuela and Colombia, the northernmost distribution record for this Neotropical genus SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE mutillidae; Tallium; neotropical; taxonomy AB Tallium lattkei n. sp., male and female, is described and illustrated. This new species represents the first record of Tallium for Venezuela and Colombia and the northernmost distribution record for this Neotropical genus. C1 Univ Panama, Estafeta Univ, Museo Invertebrados GB Fairchild, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. RP Cambra, RA (reprint author), Univ Panama, Estafeta Univ, Museo Invertebrados GB Fairchild, Panama City, Panama. EM rcambra@ancon.up.ca.pa; QUINTERD@tivoli.si.edu NR 7 TC 0 Z9 0 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD DEC PY 2003 VL 129 IS 3-4 BP 497 EP 502 PG 6 WC Entomology SC Entomology GA 763DN UT WOS:000188059600007 ER PT J AU Perez-Gelabert, DE Otte, D AF Perez-Gelabert, DE Otte, D TI Melanoplus sanguinipes (Fabricius) (Orthoptera : Acrididae : Melanoplinae), a pest grasshopper introduced to Dominican Republic, Hispaniola SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE grasshopper; Melanoplus; invasive species; insect pests; Dominican Republic; Hispaniola AB The invasive grasshopper species Melanoplus sanguinipes (F.) is reported to have been accidentally introduced over 30 years ago into Dominican Republic. This species has been found in several mountain localities around the town of Constanza, Cordillera Central. The complete extent of its distribution in the Dominican Republic remains to be mapped, but the species appears to be absent from the country's lowlands. C1 Smithsonian Inst, Natl Museum Nat Hist, Entomol Sect, Dept Systemat Biol, Washington, DC 20560 USA. Acad Nat Sci Philadelphia, Dept Entomol, Philadelphia, PA 19103 USA. RP Perez-Gelabert, DE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Entomol Sect, Dept Systemat Biol, Washington, DC 20560 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD DEC PY 2003 VL 129 IS 3-4 BP 543 EP 548 PG 6 WC Entomology SC Entomology GA 763DN UT WOS:000188059600010 ER PT J AU Ferrari, FD Grygier, MJ AF Ferrari, FD Grygier, MJ TI Comparative morphology among trunk limbs of Caenestheriella gifiurensis and Leptestheria kawachiensis (Crustacea : Branchiopoda : Spinicaudata) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE appendages development; homologies; spinicaudatan ID CYCLESTHERIA-HISLOPI BAIRD; RIDGEWAYIA-KLAUSRUETZLERI; PHYLOGENETIC ANALYSIS; DROSOPHILA LEG; AXIS FORMATION; SWIMMING LEGS; SETAL NUMBERS; DISTAL-LESS; CONCHOSTRACA; SUBDIVISION AB Morphological differences among groups of the 24 trunk limbs of Caenestheriella gifuensis (Ishikawa, 1895) and differences between males and females are described and illustrated. A setose attenuate lobe located proximally near enditic lobe 1 and a discoid lobe covered with small setae proximal to enditic lobe 1 are newly described. The five ventral enditic lobes, endopod, exopod, and dorsal exite of traditional spinicaudatan morphology are redescribed. Trunk limbs 1-4 of females bear a palp, on enditic lobe 5 and trunk limbs 1-15 of males bear a similar palp. A second, articulating palp is associated with the base of the endopod of trunk limbs 1-2 of males. The proximal part of trunk limbs 19-24, bearing enditic lobe 1, articulates by an arthrodial membrane with the remainder of the limb, and the exite is distal to this arthrodial membrane. Development of trunk limbs, ascertained through an examination of early juvenile instars of Leptestheria kawachiensis Ueno, 1927, includes an asetose limb followed in time by a series of setose limbs that increase in morphological complexity with age. The number of lobes on the asetose limb varies from seven (corresponding to five enditic lobes, an endopod, and an exopod) on anterior limbs to five on trunk limb 24, which lacks the lobes corresponding to enditic lobe 4 and the endopod; these two structures are added later to setose limbs. The attenuate lobe, the discoid lobe, the exite of all trunk limbs, and the palps of the anterior trunk limbs are added to the setose limbs. Development of anterior limbs is accelerated relative to that of posterior limbs, and development of the more posterior limbs is truncated relative to that of limbs immediately anterior to them. Enditic lobe 4 and the endopod of limbs like trunk limb 24 develop from, or are patterned by, enditic lobe 5; the articulating palp of male trunk limbs 1-2 also may be added in this way. A comparison of these observations with development of the copepod maxilliped suggests that the spinicaudatan trunk limb is composed of a praecoxa with three lobes, a coxa and a basis each with one lobe, and an endopod of three segments in females and four in males. This is similar to the homology scheme previously proposed by Hansen in 1925. A critique is given of attempts to homologize parts of arthropod limbs based on developmental gene expression patterns. Stenopodal to phyllopodal transformations of maxillipeds in copepods provide a model at least partly applicable to spinicaudatans, and a 'multibranched' interpretation of spinicaudatan (and by extension branchiopodan) limb morphology is rejected. There is nothing intrinsic to the structure of the adult trunk limbs suggesting that they are similar to the adult limbs of the ancestral branchiopod or the ancestral crustacean, but early developmental steps of more posterior limbs are good matches for the morphology of an ancestral crustacean biramal limb predicted by a hypothesis of duplication of the proximo-distal axis. (C) 2003 The Linnean Society of London, Zoological Journal of the Linnean Society, 2003, 139, 547-564. No claim to original US government works. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Syst Biol, Museum Support Ctr, Suitland, MD 20746 USA. Lake Biwa Museum, Shiga 5250001, Japan. RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Syst Biol, Museum Support Ctr, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 46 TC 21 Z9 23 U1 1 U2 3 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD DEC PY 2003 VL 139 IS 4 BP 547 EP 564 DI 10.1046/j.0024-4082.2003.00083.x PG 18 WC Zoology SC Zoology GA 753CR UT WOS:000187214700003 ER PT J AU Santini, F Tyler, JC AF Santini, F Tyler, JC TI A phylogeny of the families of fossil and extant tetraodontiform fishes (Acanthomorpha, Tetraodontiformes), Upper Cretaceous to recent SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE miocene; Monte bolca; oligocene; tethys; zeiformes ID MISSING DATA; EVOLUTIONARY RELATIONSHIPS; NORTH-CAROLINA; CHARACTERS; MOLIDAE; EOCENE; GENUS; RECONSTRUCTION; BIOGEOGRAPHY; OSTRACIIDAE AB A data matrix is presented of 210 morphological characters (mostly osteological, some external) for 20 extant taxa of the ten Recent families of tetraodontiform fishes and 36 fossil tetraodontiforms. The oldest of these are from the Upper Cretaceous (95 Mya); most are from the Lower to Middle Eocene (50-58 Mya). There are two outgroup taxa, (a zeiform and a caproid). A cladistic analysis of this matrix for only the extant taxa produced two equally parsimonious trees that call into question the monophyly of some of the previously accepted major higher-level tetraodontiform clades. Inclusion in the analysis of the large number of available fossil taxa helps to resolve relationships between family level clades. The new phylogenetic hypothesis, together with stratigraphic and biogeographical data, is used to discuss scenarios of the origin and evolution of the major clades of the order. (C) 2003 The Linnean Society of London, Zoological Journal of the Linnean Society, 2003, 139, 565-617. C1 Univ Toronto, Dept Zool, Ramsay Wright Zool Labs, Toronto, ON M5S 3G5, Canada. Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Santini, F (reprint author), Museum Natl Hist Nat, Dept Syst & Evolut, 43 Rue Cuvier, F-75005 Paris, France. EM fsantini@mnhn.fr NR 89 TC 78 Z9 85 U1 2 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD DEC PY 2003 VL 139 IS 4 BP 565 EP 617 DI 10.1111/j.1096-3642.2003.00088.x PG 53 WC Zoology SC Zoology GA 753CR UT WOS:000187214700004 ER PT J AU Castro, P Williams, AB Cooper, LL AF Castro, P Williams, AB Cooper, LL TI Revision of the family Latreilliidae Stimpson, 1858 (Crustacea, Decapoda, Brachyura) SO ZOOSYSTEMA LA English DT Review DE Crustacea; Decapoda; Brachyura; Latreilliidae; biogeography; carrying behaviour; phylogeny; revision ID FIJIAN ARCHIPELAGO; MEGALOPA STAGE; CRUISE; STATIONS; LIST; PODOTREMATA; CRABS AB A study of specimens from around the world and the re-examination of additional material used by Williams for his revision of Latreillia Roux, 1830 have lead to a revision of the family Latreilliidae Stimpson, 1858 (Crustacea, Decapoda, Brachyura). The family now consists of two genera: Latreillia, with five species (L. elegans Roux, 1830, L. metanesa Williams, 1982, L. pennifera Alcock, 1900, L. valida de Haan, 1839, and L. williamsi Melo, 1990), and Eplumula Williams, 1982, with two species (E australiensis (Henderson, 1888) and E phalangium (de Haan, 1839)). Latreillia manningi Williams, 1982, which was described as a western Atlantic species distinct from the Mediterranean and eastern Atlantic populations of L. elegans, is now regarded as a very close geographical variant of L. elegans because the differences between the two populations are insignificant and overlapping. The revision has resulted in an updated and more detailed definition of the Latreilliidae with the addition of characters such as the type of abdominal holding system and the morphology of the coxae of the last pair of pereopods (P5) of males. The revision has also re-examined our current knowledge of the phylogeny and biogeography of the family. It also reviews carrying behaviour, the use of the P5 for carrying living organisms or non-living objects for camouflaging, among its member species. C1 Calif State Polytech Univ Pomona, Dept Biol Sci, Pomona, CA 91768 USA. Smithsonian Inst, Natl Marine Fisheries Serv Systemat Lab, Natl Museum Nat Hist, Washington, DC 20560 USA. Fisheries & Oceans Canada, Biodivers Sci Branch, Ottawa, ON K1A 0E6, Canada. RP Castro, P (reprint author), Calif State Polytech Univ Pomona, Dept Biol Sci, Pomona, CA 91768 USA. EM pcastro@csupomona.edu NR 117 TC 12 Z9 14 U1 0 U2 3 PU PUBLICATIONS SCIENTIFIQUES DU MUSEUM, PARIS PI PARIS CEDEX 05 PA CP 39-57, RUE CUVIER, F-75231 PARIS CEDEX 05, FRANCE SN 1280-9551 EI 1638-9387 J9 ZOOSYSTEMA JI Zoosystema PD DEC PY 2003 VL 25 IS 4 BP 601 EP 634 PG 34 WC Zoology SC Zoology GA 763EN UT WOS:000188062100003 ER PT J AU Chu, X Jamieson, MJ Dalgarno, A AF Chu, X Jamieson, MJ Dalgarno, A TI Scattering lengths for collisions of hydrogen and deuterium atoms SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID POTENTIAL-ENERGY CURVES; GROUND-STATE; MOLECULE; APPROXIMATION; MASS; H-2 AB The scattering lengths for hydrogen and deuterium atoms interacting via the potentials of the X (1)Sigma(g)(+), b (3)Sigma(u)(+) and e (3)Sigma(u)(+) molecular. states are calculated. An estimate of the uncertainty in the X (1)Sigma(g)(+) scattering length arising from the coupling to the (1)Sigma(u)(+) states is made. The recommended scattering lengths are -0.67 and 148 bohr for the b (3)Sigma(u)(+) and e (3)Sigma(u)(+) interaction potentials, respectively, and 11.1 bohr for the X (1)Sigma(g)(+) interaction potential. It is suggested that deuterium atoms would be cooled efficiently by collisions with metastable hydrogen atoms. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. RP Chu, X (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 2 Z9 2 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 NOV 28 PY 2003 VL 36 IS 22 BP L415 EP L418 AR PII S0953-4075(03)67963-0 DI 10.1088/0953-4075/36/22/L01 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 757KX UT WOS:000187562400001 ER PT J AU Pandolfi, JM Bradbury, RH Sala, E Hughes, TP Bjorndal, KA Cooke, RG McArdle, D McClenachan, L Newman, MJH Paredes, G Warner, RR Jackson, JBC AF Pandolfi, JM Bradbury, RH Sala, E Hughes, TP Bjorndal, KA Cooke, RG McArdle, D McClenachan, L Newman, MJH Paredes, G Warner, RR Jackson, JBC TI Causes of coral reef degradation - Response SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Australian Natl Univ, Ctr Resource & Environm Studies, Canberra, ACT 0200, Australia. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. James Cook Univ N Queensland, Sch Marine Biol, Ctr Coral Reef Biodivers, Townsville, Qld 4811, Australia. Univ Florida, Dept Zool, Archie Carr Ctr Sea Turtle Res, Gainesville, FL 32611 USA. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. Univ Calif Cooperat Extens, Calif Sea Grant, Santa Barbara, CA 93105 USA. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. RP Pandolfi, JM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC-121,POB 37012, Washington, DC 20013 USA. RI Pandolfi, John/A-3121-2009; Hughes, Terry/L-4721-2013; Warner, Robert/M-5342-2013 OI Pandolfi, John/0000-0003-3047-6694; Hughes, Terry/0000-0002-5257-5063; Warner, Robert/0000-0002-3299-5685 NR 0 TC 2 Z9 2 U1 1 U2 12 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD NOV 28 PY 2003 VL 302 IS 5650 BP 1502 EP 1503 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 747JV UT WOS:000186802200016 ER PT J AU Hughes, TP Baird, AH Bellwood, DR Connolly, SR Folke, C Grosberg, R Hoegh-Guldberg, O Jackson, JBC Kleypas, J Lough, JM Marshall, P Nystrom, M Palumbi, SR Pandolfi, JM Rosen, B Roughgarden, J AF Hughes, TP Baird, AH Bellwood, DR Connolly, SR Folke, C Grosberg, R Hoegh-Guldberg, O Jackson, JBC Kleypas, J Lough, JM Marshall, P Nystrom, M Palumbi, SR Pandolfi, JM Rosen, B Roughgarden, J TI Causes of coral reef degradation - Response SO SCIENCE LA English DT Letter C1 James Cook Univ N Queensland, Ctr Coral Reef Biodivers, Townsville, Qld 4811, Australia. Stockholm Univ, Dept Syst Ecol, SE-10691 Stockholm, Sweden. Univ Calif Davis, Ctr Populat Biol, Div Biol Sci, Sect Evolut & Ecol, Davis, CA 95616 USA. Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4070, Australia. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Australian Inst Marine Sci, Townsville, Qld 4810, Australia. Great Barrier Reef Marine Pk Author, Townsville, Qld 4810, Australia. Stanford Univ, Hopkins Marine Stn, Dept Biol Sci, Pacific Grove, CA 93950 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Nat Hist Museum, Dept Zool, London SW7 5BD, England. Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA. RP Hughes, TP (reprint author), James Cook Univ N Queensland, Ctr Coral Reef Biodivers, Townsville, Qld 4811, Australia. RI Baird, Andrew/C-8449-2009; Connolly, Sean/E-7773-2011; Pandolfi, John/A-3121-2009; Hoegh-Guldberg, Ove/H-6169-2011; Lough, Janice/L-1682-2013; Hughes, Terry/L-4721-2013 OI Baird, Andrew/0000-0001-8504-4077; Connolly, Sean/0000-0003-1537-0859; Pandolfi, John/0000-0003-3047-6694; Hoegh-Guldberg, Ove/0000-0001-7510-6713; Hughes, Terry/0000-0002-5257-5063 NR 0 TC 2 Z9 2 U1 1 U2 17 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD NOV 28 PY 2003 VL 302 IS 5650 BP 1503 EP 1504 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 747JV UT WOS:000186802200017 ER PT J AU Heinz, S Churazov, E Forman, W Jones, C Briel, UG AF Heinz, S Churazov, E Forman, W Jones, C Briel, UG TI Ram pressure stripping and the formation of cold fronts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : clusters : individual : A3667; galaxies : general; X-rays : galaxies : clusters ID RADIATION MAGNETOHYDRODYNAMICS CODE; 2 SPACE DIMENSIONS; CHANDRA OBSERVATION; INTERGALACTIC MEDIUM; ASTROPHYSICAL FLOWS; GALAXY CLUSTER; A3667; SUBCLUSTER; ALGORITHMS; ZEUS-2D AB Chandra and XMM-Newton observations of many clusters reveal sharp discontinuities in the surface brightness, which, unlike shocks, have lower gas temperature on the X-ray brighter side of the discontinuity. For this reason, these features are called 'cold fronts'. It is believed that some cold fronts are formed when a subcluster merges with another cluster and the ram pressure of gas flowing outside the subcluster gives the contact discontinuity the characteristic curved shape. While some edges may not arise directly from mergers, as was argued by Dupke & White for the case of A496, this paper focuses on those which arise as contact discontinuities between a merging subcluster and the ambient cluster gas. We argue that the flow of gas past the merging subcluster induces slow motions inside the cloud. These motions transport gas from the central parts of the subcluster towards the interface. Because in a typical cluster or group (even an isothermal one) the entropy of the gas in the central regions is significantly lower than in the outer regions, the transport of the low entropy gas towards the interface and the associated adiabatic expansion makes the gas temperature immediately inside the interface lower than in any other place in the system, thus enhancing the temperature jump across the interface and making the 'tip' of the contact discontinuity cool. We illustrate this picture with the XMM-Newton gas temperature map of the A3667 cluster. C1 Max Planck Inst Astrophys, D-85741 Garching, Germany. Space Res Inst, Moscow 117997, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Heinz, S (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. RI Churazov, Eugene/A-7783-2013; OI Heinz, Sebastian/0000-0002-8433-8652; Forman, William/0000-0002-9478-1682 NR 21 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 NOV 21 PY 2003 VL 346 IS 1 BP 13 EP 17 DI 10.1046/j.1365-2966.2003.07066.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 742TA UT WOS:000186533100004 ER PT J AU van den Bosch, FC Abe, T Hernquist, L AF van den Bosch, FC Abe, T Hernquist, L TI The angular momentum of gas in protogalaxies - II. The impact of pre-heating SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : formation; galaxies : haloes; galaxies : structure; dark matter ID X-RAY-EMISSION; DARK-MATTER HALOES; GALAXY FORMATION; DISC GALAXIES; DWARF GALAXIES; STAR-FORMATION; INTRACLUSTER MEDIUM; SIMULATIONS; CLUSTERS; EVOLUTION AB We examine the effect of pre-heating of the intergalactic medium on galaxy formation using cosmological hydrodynamical simulations. By performing simulations both with and without a simple model for pre-heating, we analyse and compare the angular momentum distributions of the dark matter and the baryons. Pre-heating unbinds baryons from their dark-matter haloes, yielding a baryonic mass fraction that declines with decreasing halo mass. In addition, the spin parameter of the gas is reduced with respect to the case without pre-heating, while the misalignment between the angular momentum directions of the gas and dark matter increases strongly. The angular momentum distributions of individual haloes reveal that pre-heating decreases (increases) the mass fraction with low (negative) specific angular momentum. We discuss the implications of these findings for the formation of disc galaxies in a pre-heated intergalactic medium, and compare our results to the predictions of Maller & Dekel, who propose an alternative interpretation for the origin of the angular momentum of (proto)galaxies. C1 Max Planck Inst Astrophys, D-85741 Garching, Germany. Penn State Univ, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van den Bosch, FC (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. NR 57 TC 28 Z9 28 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 NOV 21 PY 2003 VL 346 IS 1 BP 177 EP 185 DI 10.1046/j.1365-2966.2003.07079.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 742TA UT WOS:000186533100019 ER PT J AU Kong, AKH AF Kong, AKH TI XMM-Newton observation of the X-ray point source population of the starburst galaxy IC 342 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual : IC 342; galaxies : starburst; X-rays : binaries; X-rays : galaxies ID FORMATION RATE INDICATOR; STAR-FORMATION; BLACK-HOLES; BINARIES; CHANDRA; MASS; EMISSION; LUMINOSITY AB We present the results of an XMM-Newton observation of the starburst galaxy IC 342. Thirty-seven X-ray point sources were detected down to a luminosity limit Of similar to10(37) erg s(-1). Most of the sources are located near the spiral arms. The X-ray point source luminosity function is consistent with a power-law shape with a slope of 0.55, typical of starburst galaxies. We also present the energy spectra of several ultraluminous X-ray sources (ULXs), including the luminous X-ray source in the galactic nucleus. Except for the nucleus and a luminous supersoft X-ray source, other ULXs can generally be fitted with a simple power-law spectral model. The nucleus is very luminous (similar to10(40) erg s(-1) in 0.2-12 keV) and requires disc blackbody and power-law components to describe the X-ray emission. The spectral fit reveals a cool accretion disc (kT = 0.11 keV) and suggests that the source harbours either an intermediate-mass black hole or a stellar-mass black hole with outflow. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 34 TC 22 Z9 22 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 21 PY 2003 VL 346 IS 1 BP 265 EP 272 DI 10.1046/j.1365-2966.2003.07086.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 742TA UT WOS:000186533100025 ER PT J AU Basu, AR Petaev, MI Poreda, RJ Jacobsen, SB Becker, L AF Basu, AR Petaev, MI Poreda, RJ Jacobsen, SB Becker, L TI Chondritic meteorite fragments associated with the Permian-Triassic boundary in Antarctica SO SCIENCE LA English DT Article ID GIGANTIC RELEASE; MASS EXTINCTION; SIBERIAN TRAPS; BOLIDE IMPACT; FLOOD BASALTS; NOBLE-GASES; FULLERENES; MICROMETEORITES; CATASTROPHE; SULFUR AB Multiple chondritic meteorite fragments have been found in two sedimentary rock samples from an end-Permian bed at Graphite Peak in Antarctica. The Ni/Fe, Co/Ni, and P/Fe ratios in metal grains; the Fe/Mg and Mn/Fe ratios in olivine and pyroxene; and the chemistry of Fe-, Ni-, P-, and S-bearing oxide in the meteorite fragments are typical of CM-type chondritic meteorites. In one sample, the meteoritic fragments are accompanied by more abundant discrete metal grains, which are also found in an end-Permian bed at Meishan, southern China. We discuss the implications of this finding for a suggested global impact event at the Permian-Triassic boundary. C1 Univ Rochester, Dept Earth & Environm Sci, Rochester, NY 14627 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Santa Barbara, Dept Geol, Inst Crustal Studies, Santa Barbara, CA 93106 USA. RP Basu, AR (reprint author), Univ Rochester, Dept Earth & Environm Sci, Rochester, NY 14627 USA. RI Jacobsen, Stein/B-1759-2013 NR 33 TC 85 Z9 101 U1 5 U2 29 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD NOV 21 PY 2003 VL 302 IS 5649 BP 1388 EP 1392 DI 10.1126/science.1090852 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 745HP UT WOS:000186683500050 PM 14631038 ER PT J AU Zentner, AR Bullock, JS AF Zentner, AR Bullock, JS TI Halo substructure and the power spectrum SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; dark matter; galaxies : formation; galaxies : halos; galaxies : structure ID COLD DARK-MATTER; SURFACE BRIGHTNESS GALAXIES; PROBE WMAP OBSERVATIONS; LARGE-SCALE STRUCTURE; LY-ALPHA FOREST; RESOLUTION ROTATION CURVES; DIGITAL SKY SURVEY; LOW-MASS GALAXIES; X-RAY-CLUSTERS; DWARF GALAXIES AB We present a semianalytic model to investigate the merger history, destruction rate, and survival probability of substructure in hierarchically formed dark matter halos and use it to study the substructure content of halos as a function of input primordial power spectrum. For a standard cold dark matter "concordance" cosmology (LambdaCDM; n = 1, sigma(8) = 0.95) we successfully reproduce the subhalo velocity function and radial distribution pro. le seen in N-body simulations and determine that the rate of merging and disruption peaks similar to10-12 Gyr in the past for Milky Way-like halos, while surviving substructures are typically accreted within the last similar to0-8 Gyr. We explore power spectra with normalizations and spectral "tilts" spanning the ranges sigma(8) similar or equal to 1-0.65 and n similar or equal to 1-0.8, and include a "running-index" model with dn/d ln k = -0.03 similar to the best-fit model discussed in the first-year Wilkinson Microwave Anisotropy Probe (WMAP) report. We investigate spectra with truncated small-scale power, including a broken-scale inflation model and three warm dark matter cases with m(W) = 0.75-3.0 keV. We find that the mass fraction in substructure is relatively insensitive to the tilt and overall normalization of the primordial power spectrum. All of the CDM-type models yield projected substructure mass fractions that are consistent with, but on the low side, of published estimates from strong lens systems: f(9) = 0.4%-1.5% (64th percentile) for subhalos smaller than 10(9) M-circle dot within projected cylinders of radius r < 10 kpc. Truncated models produce significantly smaller fractions, f(9) = 0.02%-0.2% for m(W) &SIME; 1 keV, and are disfavored by lensing estimates. This suggests that lensing and similar probes can provide a robust test of the CDM paradigm and a powerful constraint on broken-scale inflation/warm particle masses, including masses larger than the &SIM;1 keV upper limits of previous studies. We compare our predicted subhalo velocity functions with the dwarf satellite population of the Milky Way. Assuming that dwarfs have isotropic velocity dispersions, we find that the standard n = 1 model overpredicts the number of Milky Way satellites at V-max &LSIM; 35 km s(-1\), as expected. Models with less small-scale power do better because subhalos are less concentrated and the mapping between observed velocity dispersion and halo Vmax is significantly altered. The running-index model, or a fixed tilt with σ(8) &SIM; 0.75, can account for the local dwarfs without the need for differential feedback (for V-max &GSIM; 20 km s(-1)); however, these comparisons depend sensitively on the assumption of isotropic velocities in satellite galaxies. C1 Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zentner, AR (reprint author), Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. RI Bullock, James/K-1928-2015 OI Bullock, James/0000-0003-4298-5082 NR 150 TC 289 Z9 291 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 49 EP 72 DI 10.1086/378797 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700005 ER PT J AU Yoshida, N Sokasian, A Hernquist, L Springel, V AF Yoshida, N Sokasian, A Hernquist, L Springel, V TI Early structure formation and reionization in a cosmological model with a running primordial power spectrum SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; early universe; galaxies : formation; large-scale structure of universe; methods : n-body simulations ID COLD DARK-MATTER; SMOOTHED PARTICLE HYDRODYNAMICS; PROBE WMAP OBSERVATIONS; INITIAL MASS FUNCTION; LYMAN-ALPHA FOREST; STAR-FORMATION; HIGH-REDSHIFT; LY-ALPHA; NUMERICAL COSMOLOGY; BLACK-HOLES AB We study high-redshift structure formation and reionization in a LambdaCDM universe under the assumption that the spectral power index of primordial density fluctuations is a function of length scale. We adopt a particular formulation of the "running" spectral index (RSI) model as suggested by the combined analysis of the recent Wilkinson Microwave Anisotropy Probe (WMAP) data and two other large-scale structure observations. We carry out high-resolution cosmological simulations and use them to study the formation of primordial gas clouds where the first stars are likely to form. While early structure forms hierarchically in the RSI model, quite similar to the standard power-law LambdaCDM model, the reduced power on small scales causes a considerable delay in the formation epoch of low-mass (similar to10(6) M-circle dot) "minihalos" compared with the LambdaCDM model. The abundance of primordial star-forming gas clouds in such halos also differs by more than an order of magnitude at z > 15 between the two models. The extremely small number of gas clouds in the RSI model indicates that reionization is initiated later than z < 15, generally resulting in a smaller total Thomson optical depth than in the Lambda CDM model. By carrying out radiative transfer calculations, we also study reionization by stellar populations formed in galaxies. We show that, in order to reionize the universe by z similar to 7, the escape fraction of ultraviolet photons from galaxies in the RSI model must be as high as 0.6 throughout the redshift range 5 < z < 18 for a stellar population similar to that of the local universe. Even with a top-heavy initial mass function representing an early population of massive stars and/or an extraordinarily high photon emission rate from galaxies, the total optical depth can only be as large as tau(e) similar to 0.1 for reasonable models of early star formation. The RSI model is thus in conflict with the large Thomson optical depth inferred by the WMAP satellite. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ Japan, Tokyo 1868588, Japan. Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Yoshida, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nyoshida@cfa.harvard.edu; asokasia@cfa.harvard.edu; lhernqui@cfa.harvard.edu; volker@mpa-garching.mpg.de RI Yoshida, Naoki/A-4305-2011 NR 84 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 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 73 EP 85 DI 10.1086/378852 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700006 ER PT J AU Sun, M Forman, W Vikhlinin, A Hornstrup, A Jones, C Murray, SS AF Sun, M Forman, W Vikhlinin, A Hornstrup, A Jones, C Murray, SS TI CHANDRA observations of the NGC 1550 galaxy group: Implication for the temperature and entropy profiles of 1 keV galaxy groups SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 1550); hydrodynamics; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; XMM-NEWTON OBSERVATION; INTRACLUSTER MEDIUM; NEARBY CLUSTERS; INTRAGROUP MEDIUM; SCALING PROJECT; GROUP NGC-5044; COOLING FLOW; SKY SURVEY; T RELATION AB We present a detailed Chandra study of the galaxy group NGC 1550. For its temperature (1.37 +/- 0.01 keV) and velocity dispersion (similar to300 km s(-1)), the NGC 1550 group is one of the most luminous known galaxy groups (L-bol = 1.65 x 10(43) ergs s(-1) within 200 kpc, or 0.2r(vir)). We find that within similar to 60 kpc, where the gas cooling time is less than a Hubble time, the gas temperature decreases continuously toward the center, implying the existence of a cooling core. The temperature also declines beyond similar to 100 kpc (or 0.1r(vir)). The temperature pro. le of NGC 1550 is remarkably similar to those of two other 1 keV groups with accurate temperature determination. The temperature begins to decline at 0.07r(vir) - 0.1r(vir), while in hot clusters the decline begins at or beyond 0.2rvir. Thus, there are at least some 1 keV groups that have temperature profiles significantly different from those of hot clusters, which may reflect the role of nongravitational processes in intracluster medium/intergalactic medium evolution. NGC 1550 has no isentropic core in its entropy pro. le, in contrast to the predictions of "entropy floor'' simulations. We compare the scaled entropy profiles of three 1 keV groups ( including NGC 1550) and three 2 - 3 keV groups. The scaled entropy profiles of 1 keV groups show much larger scatter than those of hotter systems, which implies varied preheating levels. We also discuss the mass content of the NGC 1550 group and the abundance pro. le of heavy elements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. RP Sun, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 53 TC 36 Z9 36 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 250 EP 259 DI 10.1086/378887 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700019 ER PT J AU Fabbiano, G Krauss, M Zezas, A Rots, A Neff, S AF Fabbiano, G Krauss, M Zezas, A Rots, A Neff, S TI The multicolored hot interstellar medium of ''the antennae'' galaxies (NGC 4038/4039) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038; NGC 4039, Antennae); galaxies : interactions; galaxies : peculiar; X-rays : galaxies ID YOUNG STAR-CLUSTERS; X-RAY-EMISSION; CHANDRA OBSERVATIONS; LUMINOSITY FUNCTION; METAL ABUNDANCE; NGC 4038/39; ASCA; MULTIWAVELENGTH; REGIONS; GAS AB We report the results of the analysis of the extended soft emission discovered in the Chandra ACIS pointing at the merging system NGC 4038/4039 ("the Antennae''). We present a multicolor X-ray image that suggests both extensive absorption by the dust in this system, peaking in the contact region, as well as variations in the temperature of different emitting regions of the hot interstellar medium (ISM). Spectral fits to multicomponent thermal emission models confirm this picture and give a first evaluation of the parameters of the hot plasma. We compare the diffuse X-ray emission with radio continuum (6 cm), H I, CO, and Halpha images to take a first look at the multiphase ISM of "the Antennae'' galaxies. We find that the hot (X-ray) and cold (CO) gas have comparable thermal pressures in the two nuclear regions. We also conclude that the displacement between the peak of the diffuse X-ray emission in the north of the galaxy system, toward the inner regions of the northern spiral arm (as defined by Halpha, radio continuum, and H I), could result from ram pressure of infalling H I clouds. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 43 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 272 EP 287 DI 10.1086/378791 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700021 ER PT J AU Yuan, F Quataert, E Narayan, R AF Yuan, F Quataert, E Narayan, R TI Nonthermal electrons in radiatively inefficient accretion flow models of Sagittarius A SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; Galaxy : center; radiation mechanisms : nonthermal; radiation mechanisms : thermal ID SUPERMASSIVE BLACK-HOLE; X-RAY FLARE; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; OUTER BOUNDARY-CONDITION; ACTIVE GALACTIC NUCLEI; LINEAR-POLARIZATION; SGR-A; SYNCHROTRON EMISSION; SUBMILLIMETER EMISSION; CIRCULAR-POLARIZATION AB We investigate radiatively inefficient accretion flow models for Sgr A*, the supermassive black hole in our Galactic center, in light of new observational constraints. Confirmation of linear polarization in the submillimeter emission argues for accretion rates much less than the canonical Bondi rate. We consider models with low accretion rates and calculate the spectra produced by a hybrid electron population consisting of both thermal and nonthermal particles. The thermal electrons produce the submillimeter emission and can account for its linear polarization properties. As noted in previous work, the observed low-frequency radio spectrum can be explained if a small fraction (approximate to 1.5%) of the electron thermal energy resides in a soft powerlaw tail. In the innermost region of the accretion flow, turbulence and/or magnetic reconnection events may occasionally accelerate a fraction of the electrons into a harder power-law tail. We show that the synchrotron emission from these electrons, or the Compton upscattering of synchrotron photons by the same electrons, may account for the X-ray flares observed by Chandra. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Yuan, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM fyuan@cfa.harvard.edu; eliot@astron.berkeley.edu; narayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 75 TC 369 Z9 371 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 301 EP 312 DI 10.1086/378716 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700023 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 X-ray burst oscillations from a neutron star X-ray transient in the globular cluster NGC 6440 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters : individual (NGC 6440); stars : individual ( SAX J1748.9-2021) stars : neutron; X-rays : binaries ID PHOTOSPHERIC RADIUS EXPANSION; MILLISECOND PULSAR; NGC 6440; VARIABILITY; EVOLUTION; BINARIES AB We report the discovery of millisecond oscillations in an X-ray burst from the X-ray transient SAX J1748.9 - 2021 in the globular cluster NGC 6440. Oscillations at a frequency of 409.7 +/- 0.3 Hz were present in one of 15 X-ray bursts observed with the Proportional Counter Array on the Rossi X-Ray Timing Explorer during the outburst that occurred in 2001. The burst was relatively dim and had the second longest duration and decay time. The average peak luminosity of two bursts showing radius expansion is (3.6 +/- 0.4) x 10(38) ergs s(-1), consistent with the Eddington luminosity for a 1.4 M-. and 10 km radius neutron star burning hydrogen-poor matter. We speculate that the dichotomy observed between sources with burst oscillations at once versus twice the frequency difference of kHz quasiperiodic oscillations in the persistent emission may be related to the magnetic field geometry of the neutron stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pkaaret@cfa.harvard.edu NR 29 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 481 EP 485 DI 10.1086/375053 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700039 ER PT J AU Heinke, CO Grindlay, JE Lugger, PM Cohn, HN Edmonds, PD Lloyd, DA Cool, AM AF Heinke, CO Grindlay, JE Lugger, PM Cohn, HN Edmonds, PD Lloyd, DA Cool, AM TI Analysis of the quiescent low-mass X-ray binary population in Galactic globular clusters SO ASTROPHYSICAL JOURNAL LA English DT Review DE globular clusters : general; globular clusters : individual (NGC 6440); novae, cataclysmic variables; stars : neutron; stellar dynamics; X-rays : binaries ID HUBBLE-SPACE-TELESCOPE; SEQUENCE LUMINOSITY FUNCTION; XMM-NEWTON OBSERVATIONS; BLUE STRAGGLER STARS; NEUTRON-STAR; CATACLYSMIC VARIABLES; CHANDRA OBSERVATION; MILLISECOND PULSAR; 47 TUCANAE; EXTENSIVE CENSUS AB Quiescent low-mass X-ray binaries (qLMXBs) containing neutron stars have been identified in several globular clusters using Chandra or XMM X-ray observations, via their distinctive soft thermal spectra. We report a complete census of the qLMXB population in these clusters, identifying three additional probable qLMXBs in NGC 6440. We conduct several analyses of the qLMXB population and compare it with the harder, primarily cataclysmic variable (CV), population of low-luminosity X-ray sources with 1031 ergs s(-1) < L-X < 10(32.5) ergs s(-1). The radial distribution of our qLMXB sample suggests an average system mass of 1.5(-0.2)(+0.3) M-., consistent with a neutron star and low-mass companion. Spectral analysis reveals that no globular cluster qLMXBs, other than the transient in NGC 6440, require an additional hard powerlaw component, as often observed in field qLMXBs. We identify an empirical lower luminosity limit of similar to10(32) ergs s(-1) among globular cluster qLMXBs. The bolometric luminosity range of qLMXBs implies (in the deep crustal heating model of Brown and collaborators) low time-averaged mass-transfer rates, below the disk stability criterion. The X-ray luminosity functions of the CV populations alone in NGC 6397 and 47 Tuc are shown to differ. The distribution of qLMXBs among globular clusters is consistent with their dynamical formation by either tidal capture or exchange encounters, allowing us to estimate that 7 times more qLMXBs than bright LMXBs reside in globular clusters. The distribution of harder sources ( primarily CVs) has a weaker dependence on density than that of the qLMXBs. Finally, we discuss possible effects of core collapse and globular cluster destruction on X-ray source populations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. San Francisco State Univ, San Francisco, CA 94132 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cheinke@cfa.harvard.edu; josh@cfa.harvard.edu; lugger@indiana.edu; cohn@indiana.edu; pedmonds@cfa.harvard.edu; dlloyd@cfa.harvard.edu; cool@sfsu.edu OI Heinke, Craig/0000-0003-3944-6109 NR 105 TC 103 Z9 103 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 501 EP 515 DI 10.1086/378885 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700042 ER PT J AU Heinke, CO Grindlay, JE Edmonds, PD Lloyd, DA Murray, SS Cohn, HN Lugger, PM AF Heinke, CO Grindlay, JE Edmonds, PD Lloyd, DA Murray, SS Cohn, HN Lugger, PM TI A Chandra X-ray study of the globular cluster M80 SO ASTROPHYSICAL JOURNAL LA English DT Article DE blue stragglers; globular clusters : individual (NGC 6093); novae, cataclysmic variables; stars : neutron; X-rays : binaries ID SPACE-TELESCOPE COUNTERPARTS; BLUE STRAGGLER STARS; CATACLYSMIC VARIABLES; 47 TUCANAE; EXTENSIVE CENSUS; CCD PHOTOMETRY; NEUTRON-STARS; CORE; POPULATION; NGC-6397 AB We report our analysis of a Chandra X-ray observation of the rich globular cluster M80, in which we detect some 19 sources to a limiting 0.5 - 2.5 keV X-ray luminosity of 7 x 10(30) ergs s(-1) within the half-mass radius. X-ray spectra indicate that two of these sources are quiescent low-mass X-ray binaries containing neutron stars. We identify five sources as probable cataclysmic variables (CVs), one of which seems to be heavily absorbed, implying high inclination. The brightest CV may be the X-ray counterpart of nova 1860 T Sco. The concentration of the X-ray sources within the cluster core implies an average mass of 1.2 +/- 0.2 M-., consistent with the binary nature of these systems and very similar to the radial distribution of the blue stragglers in this cluster. The X-ray and blue straggler source populations in M80 are compared to those in the similar globular cluster 47 Tuc. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Heinke, CO (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Heinke, Craig/0000-0003-3944-6109 NR 53 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 NOV 20 PY 2003 VL 598 IS 1 BP 516 EP 526 DI 10.1086/378884 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700043 ER PT J AU Perna, R McDowell, J Menou, K Raymond, J Medvedev, MV AF Perna, R McDowell, J Menou, K Raymond, J Medvedev, MV TI Chandra observations of the dwarf nova WX Hydri in quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars : individual (WX Hydri); X-rays : stars ID X-RAY-EMISSION; ION LINE-INTENSITIES; HELIUM-LIKE IONS; CATACLYSMIC VARIABLES; ACCRETION DISKS; HOT ACCRETION; WHITE-DWARFS; EXTREME-ULTRAVIOLET; BOUNDARY-LAYERS; SHOCK-WAVES AB We report Chandra observations of the dwarf nova WX Hyi in quiescence. The X-ray spectrum displays strong and narrow emission lines of N, O, Mg, Ne, Si, S, and Fe. The various ionization states implied by the lines suggest that the emission is produced within a flow spanning a wide temperature range, from T similar to 10(6) K to T greater than or similar to 10(8) K. Line diagnostics indicate that most of the radiation originates from a very dense region, with n similar to 10(13) - 10(14) cm(-3). The Chandra data allow the first tests of specific models proposed in the literature for the X-ray emission in quiescent dwarf novae. We have computed the spectra for a set of models ranging from hot boundary layers, to hot settling flow solutions, to X-ray-emitting coronae. WX Hyi differs from other dwarf novae observed at minimum in having much stronger low-temperature lines, which prove difficult to fit with existing models, and possibly a very strong, broad O VII line, perhaps produced in a wind moving at a few times 10(3) km s(-1). The accretion rate inferred from the X-rays is lower than the value inferred from the UV. The presence of high-velocity mass ejection could account for this discrepancy while at the same time explaining the presence of the broad O VII line. If this interpretation is correct, it would provide the first detection of a wind from a dwarf nova in quiescence. C1 Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Virginia Inst Theoret Astron, Charlottesville, VA 22903 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. RP Perna, R (reprint author), Harvard Soc Fellows, 74 Mt Auburn St, Cambridge, MA 02138 USA. NR 52 TC 18 Z9 18 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP 545 EP 552 DI 10.1086/378855 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KW UT WOS:000186688700045 ER PT J AU Siemiginowska, A Smith, RK Aldcroft, TL Schwartz, DA Paerels, F Petric, AO AF Siemiginowska, A Smith, RK Aldcroft, TL Schwartz, DA Paerels, F Petric, AO TI An X-ray jet discovered by Chandra in the z=4.3 radio-selected quasar GB 1508+5714 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : individual (GB 1508+5714); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; INVERSE COMPTON; LOUD QUASARS; SPECTRUM; RADIATION; Z-GREATER-THAN-4; ABSORPTION; ELECTRONS; REDSHIFT; EMISSION AB We report the Chandra discovery of an X-ray jet associated with the z = 4.3 radio-loud quasar GB 1508 +5714. The jet X-ray emission peaks similar to2" to the southwest of the quasar core. We present archival Hubble Space Telescope Wide Field Planetary Camera 2 data of the quasar field that show no optical emission at the location of the Xray jet. We discuss possible emission mechanisms and give constraints to the magnetic field and energy densities for synchrotron radiation or for Compton scattering of the cosmic microwave background radiation as the jet Xray emission process. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Columbia Univ, Dept Phys, New York, NY 10027 USA. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 37 Z9 37 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2003 VL 598 IS 1 BP L15 EP L18 DI 10.1086/380497 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745KX UT WOS:000186688800004 ER PT J AU Skinner, G Gorenstein, P AF Skinner, G Gorenstein, P TI Astronomy - Black holes, fleas and microlithography SO NATURE LA English DT Editorial Material ID HIGH-ENERGY ASTRONOMY; OPTICS C1 Ctr Etud Spatiale Rayonnements, F-31208 Toulouse, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Skinner, G (reprint author), Ctr Etud Spatiale Rayonnements, F-31208 Toulouse, France. NR 8 TC 3 Z9 3 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 20 PY 2003 VL 426 IS 6964 BP 245 EP 246 DI 10.1038/426245b PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 744YQ UT WOS:000186660800032 PM 14628040 ER PT J AU Sahai, R Morris, M Knapp, GR Young, K Barnbaum, C AF Sahai, R Morris, M Knapp, GR Young, K Barnbaum, C TI A collimated, high-speed outflow from the dying star V Hydrae SO NATURE LA English DT Article ID BIPOLAR PLANETARY-NEBULAE; ASYMPTOTIC GIANT BRANCH; CARBON STAR; BOW SHOCK; JET; BUBBLES; WIND AB Stars with masses in the range 1-8 solar masses (M.) live ordinary lives for similar to10(9)-10(10) years, but die extraordinary deaths. First, during their death throes as asymptotic giant branch (AGB) stars they eject, over 10(4)-10(5) years, half or more of their mass in slowly expanding, spherical winds, and then, in a short (a few 100-1,000 years) and poorly understood phase, they are transformed into aspherical planetary nebula. Recent studies support the idea that high-speed, jet-like flows play a crucial role in this transformation(1). Evidence for such outflows is indirect, however; this phase is so short that few nearby stars are likely to be caught in the act. Here we report the discovery of a newly launched, high-speed jet-like outflow in the nearby AGB star, V Hydrae. We have detected both proper motions and ongoing evolution in the jet. These results support a model in which the jet is driven by an accretion disk around an unseen, compact companion. We also find a central, dense equatorial disk-like structure which may enable and/or enhance the formation of the accretion disk. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Div Astron, Dept Phys & Astrophys, Los Angeles, CA 90095 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Valdosta State Univ, Dept Phys Astron & Geosci, Valdosta, GA 31698 USA. RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 24 TC 38 Z9 38 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 20 PY 2003 VL 426 IS 6964 BP 261 EP 264 DI 10.1038/nature02086 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 744YQ UT WOS:000186660800036 PM 14628044 ER PT J AU Jaenicke-Despres, V Buckler, ES Smith, BD Gilbert, MTP Cooper, A Doebley, J Paabo, S AF Jaenicke-Despres, V Buckler, ES Smith, BD Gilbert, MTP Cooper, A Doebley, J Paabo, S TI Early allelic selection in maize as revealed by ancient DNA SO SCIENCE LA English DT Article ID BRANCH CHAIN-LENGTH; PROLAMIN BOX; DOMESTICATION; STARCH; EVOLUTION; DETERMINANT; DOMINANCE; DIVERSITY; GENES AB Maize was domesticated from teosinte, a wild grass, by similar to6300 years ago in Mexico. After initial domestication, early farmers continued to select for advantageous morphological and biochemical traits in this important crop. However, the timing and sequence of character selection are, thus far, known only for morphological features discernible in corn cobs. We have analyzed three genes involved in the control of plant architecture, storage protein synthesis, and starch production from archaeological maize samples from Mexico and the southwestern United States. The results reveal that the alleles typical of contemporary maize were present in Mexican maize by 4400 years ago. However, as recently as 2000 years ago, allelic selection at one of the genes may not yet have been complete. C1 Max Planck Inst Evolutionary Anthropol, D-04103 Leipzig, Germany. ARS, USDA, Raleigh, NC 27695 USA. N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. Univ Oxford, Dept Zool, Henry Wellcome Ancient Biomol Ctr, Oxford OX1 3PS, England. Univ Wisconsin, Genet Lab, Madison, WI 53706 USA. RP Paabo, S (reprint author), Max Planck Inst Evolutionary Anthropol, Deutsch Pl 6, D-04103 Leipzig, Germany. RI Cooper, Alan/E-8171-2012; Gilbert, Marcus/A-8936-2013 OI Cooper, Alan/0000-0002-7738-7851; Gilbert, Marcus/0000-0002-5805-7195 NR 24 TC 136 Z9 146 U1 6 U2 40 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD NOV 14 PY 2003 VL 302 IS 5648 BP 1206 EP 1208 DI 10.1126/science.1089056 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 742XW UT WOS:000186544300053 PM 14615538 ER PT J AU Campbell, BA Campbell, DB Chandler, JF Hine, AA Nolan, MC Perillat, PJ AF Campbell, BA Campbell, DB Chandler, JF Hine, AA Nolan, MC Perillat, PJ TI Radar imaging of the lunar poles - Long-wavelength measurements reveal a paucity of ice in the Moon's polar craters. SO NATURE LA English DT Editorial Material C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Cornell Univ, Ithaca, NY 14853 USA. Arecibo Observ, Arecibo, PR 00612 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Box 37012, Washington, DC 20013 USA. RI Nolan, Michael/H-4980-2012 OI Nolan, Michael/0000-0001-8316-0680 NR 9 TC 27 Z9 28 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 NOV 13 PY 2003 VL 426 IS 6963 BP 137 EP 138 DI 10.1038/426137a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 742LA UT WOS:000186517200028 PM 14614491 ER PT J AU Greiner, J Klose, S Reinsch, K Schmid, HM Sari, R Hartmann, DH Kouveliotou, C Rau, A Palazzi, E Straubmeier, C Stecklum, B Zharikov, S Tovmassian, G Barnbantner, O Ries, C Jehin, E Henden, A Kaas, AA Grav, T Hjorth, J Pedersen, H Wijers, RAMJ Kaufer, A Park, HS Williams, G Reimer, O AF Greiner, J Klose, S Reinsch, K Schmid, HM Sari, R Hartmann, DH Kouveliotou, C Rau, A Palazzi, E Straubmeier, C Stecklum, B Zharikov, S Tovmassian, G Barnbantner, O Ries, C Jehin, E Henden, A Kaas, AA Grav, T Hjorth, J Pedersen, H Wijers, RAMJ Kaufer, A Park, HS Williams, G Reimer, O TI Evolution of the polarization of the optical afterglow of the gamma-ray burst GRB030329 SO NATURE LA English DT Article ID 29 MARCH 2003; GRB 990510; SPECTROPOLARIMETRY; GRB-020405; GRB-030329; EMISSION AB The association of a supernova with GRB030329(1,2) strongly supports the 'collapsar' model(3) of gamma-ray bursts, where a relativistic jet(4) forms after the progenitor star collapses. Such jets cannot be spatially resolved because gamma-ray bursts lie at cosmological distances; their existence is instead inferred from 'breaks' in the light curves of the afterglows, and from the theoretical desire to reduce the estimated total energy of the burst by proposing that most of it comes out in narrow beams. Temporal evolution of the polarization of the afterglows(5-7) may provide independent evidence for the jet structure of the relativistic outflow. Small-level polarization (similar to1-3 per cent)(8-17) has been reported for a few bursts, but its temporal evolution has yet to be established. Here we report polarimetric observations of the afterglow of GRB030329. We establish the polarization light curve, detect sustained polarization at the per cent level, and find significant variability. The data imply that the afterglow magnetic field has a small coherence length and is mostly random, probably generated by turbulence, in contrast with the picture arising from the high polarization detected in the prompt gamma-rays from GRB021206 (ref. 18). C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. Univ Sternwarte Gottingen, D-37083 Gottingen, Germany. ETH, Inst Astron, CH-8092 Zurich, Switzerland. CALTECH, Pasadena, CA 91125 USA. Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. NSSTC, Huntsville, AL 35805 USA. CNR, Ist Astrofis Spaziale & Fis Cosm, Sez Bologna, I-40129 Bologna, Italy. Univ Cologne, Inst Phys, D-50937 Cologne, Germany. Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, Baja California, Mexico. Univ Sternwarte, Wendelstein Observ, D-81679 Munich, Germany. European So Observ, Santiago 19, Chile. USN Observ, Univ Space Res Assoc, Flagstaff, AZ 86002 USA. Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Copenhagen, NBIfAFG, Astron Observ, DK-2100 Copenhagen O, Denmark. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. Univ Arizona, Multiple Mirror Telescope Observ, Tucson, AZ 85721 USA. Ruhr Univ Bochum, D-44780 Bochum, Germany. RP Greiner, J (reprint author), Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. EM jcg@mpe.mpg.de RI Reimer, Olaf/A-3117-2013; Hjorth, Jens/M-5787-2014; Palazzi, Eliana/N-4746-2015; OI Reimer, Olaf/0000-0001-6953-1385; Hjorth, Jens/0000-0002-4571-2306; Wijers, Ralph/0000-0002-3101-1808; Palazzi, Eliana/0000-0002-8691-7666 NR 28 TC 89 Z9 89 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD NOV 13 PY 2003 VL 426 IS 6963 BP 157 EP 159 DI 10.1038/nature02077 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 742LA UT WOS:000186517200036 PM 14614499 ER PT J AU Krawczynski, H Harris, DE Grossman, R Lane, W Kassim, N Willis, AG AF Krawczynski, H Harris, DE Grossman, R Lane, W Kassim, N Willis, AG TI Thermal and non-thermal plasmas in the galaxy cluster 3C 129 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : clusters : individual : 3C 129; galaxies : jets; radio continuum : galaxies; X-rays : galaxies; X-rays : galaxies; clusters ID TAILED RADIO-SOURCES; X-RAY OBSERVATIONS; GALACTIC PLANE SURVEY; 3C 129; INTRACLUSTER MEDIUM; ELLIPTIC GALAXIES; CHANDRA; EMISSION; GAS; GHZ AB We describe new Chandra spectroscopy data of the cluster which harbours the prototypical 'head-tail' radio galaxy 3C 129 and the weaker radio galaxy 3C 129.1. We combined the Chandra data with Very Large Array (VLA) radio data taken at 0.33, 5 and 8 GHz (archival data) and 1.4 GHz (new data). We also obtained new H I observations at the Dominion Radio Astrophysical Observatory (DRAG) to measure the neutral hydrogen column density in the direction of the cluster with arcmin angular resolution. The Chandra observation reveals extended X-ray emission from the radio galaxy 3C 129.1 with a total luminosity of 1.5x10(41) erg s(-1). The X-ray excess is resolved into an extended central source of similar or equal to2 arcsec (1 kpc) diameter and several point sources with individual luminosities up to 2.1x10(40) erg s(-1). There is no evidence for a correlation between the 3C 129.1 X-ray and radio morphology. In the case of the radio galaxy 3C 129, the Chandra observation shows, in addition to core and jet X-ray emission reported in an earlier paper, some evidence for extended, diffuse X-ray emission from a region east of the radio core. The 12 x 36 arcsec2 (6 kpc x 17 kpc) region lies 'in front' of the radio core, in the same direction into which the radio galaxy is moving. We use the radio and X-ray data to study in detail the pressure balance between the non-thermal radio plasma and the thermal intracluster medium (ICM) along the tail of 3C 129 which extends over 15 arcmin (427 kpc). Depending on the assumed lower energy cut-off of the electron energy spectrum, the minimum pressure of the radio plasma lies a factor of between 10 and 40 below the ICM pressure for a large part of the tail. We discuss several possibilities to explain the apparent pressure mismatch. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada. RP Krawczynski, H (reprint author), Washington Univ, Dept Phys, 1 Brookings Dr,Campus Box 1105, St Louis, MO 63130 USA. NR 53 TC 3 Z9 3 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 2003 VL 345 IS 4 BP 1255 EP 1265 DI 10.1046/j.1365-2966.2003.07041.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743HG UT WOS:000186565900016 ER PT J AU Winn, JN Hall, PB Schechter, PL AF Winn, JN Hall, PB Schechter, PL TI Mass and dust in the disk of a spiral lens galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; dust, extinction; galaxies : spiral, structure, halos gravitational lensing; quasars : individual (PMN J2004-1349) ID GRAVITATIONAL LENS; DARK-MATTER; SYSTEM; MODELS; CURVES; IMAGE; PKS-1830-211; SUBSTRUCTURE; EXTINCTION; B1600+434 AB Gravitational lensing is a potentially important probe of spiral galaxy structure, but only a few cases of lensing by spiral galaxies are known. We present Hubble Space Telescope and Magellan observations of the two-image quasar PMN J2004-1349, revealing that the lens galaxy is a spiral galaxy. One of the quasar images passes through a spiral arm of the galaxy and suffers 3 mag of V-band extinction. Using simple lens models, we show that the mass quadrupole is well aligned with the observed galaxy disk. A more detailed model with components representing the bulge and disk gives a bulge-to-disk mass ratio of 0.16+/-0.05. The addition of a spherical dark halo, tailored to produce an overall. at rotation curve, does not change this conclusion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. MIT, Dept Phys, Cambridge, MA 02139 USA. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 53 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 NOV 10 PY 2003 VL 597 IS 2 BP 672 EP 679 DI 10.1086/378637 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700004 ER PT J AU Aldcroft, TL Siemiginowska, A Elvis, M Mathur, S Nicastro, F Murray, SS AF Aldcroft, TL Siemiginowska, A Elvis, M Mathur, S Nicastro, F Murray, SS TI Chandra observation of 3C 212: A new look at the X-ray and ultraviolet absorbers SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars : absorption lines; quasars : individual (3C 212); ultraviolet : galaxies; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; MG-II ABSORPTION; INTRINSIC ABSORPTION; RADIO-SOURCES; QUASARS; SPECTRUM; SPECTROSCOPY; NGC-5548; EMISSION; SAMPLE AB The red quasar 3C 212 (z=1.049) is one of the most distant and most luminous active galactic nuclei that have shown evidence of an X-ray warm absorber. In order to further investigate this unusual quasar, we used Chandra/ACIS-S to observe 3C 212 for 19.5 ks, resulting in a net detection of similar to4000 counts. The Chandra data confirm the presence of an excess absorbing column N(H)approximate to4x10(21) cm(-2) at the quasar redshift, but we find no compelling evidence for a warm absorber. Using both the Chandra and archival ROSAT PSPC data, we obtain very good fits for both a partially covered neutral absorber and a low-ionization (U=0.03) photoionized absorber. In the ultraviolet, 3C 212 shows a strong associated Mg II absorber. Based on a moderate-resolution (80 km s(-1)) MMT spectrum we show that the absorber is highly saturated and has a covering fraction less than 60%, implying that the absorber is truly intrinsic to the quasar. Photoionization modeling of the Mg II absorber yields a constraint on the ionization parameter of U<0.03, inconsistent with a warm UV/X-ray absorber. In addition to our spectral analysis, we find evidence in the ACIS image data for weak extended emission surrounding the quasar as well as emission corresponding to the radio lobes at a distance of 5&DPRIME; from 3C 212. The statistical significance of these features is low, but we briefly explore the implications if the detections are valid. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Aldcroft, TL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 46 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 NOV 10 PY 2003 VL 597 IS 2 BP 751 EP 758 DI 10.1086/378640 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700009 ER PT J AU Krongold, Y Nicastro, F Brickhouse, NS Elvis, M Liedahl, DA Mathur, S AF Krongold, Y Nicastro, F Brickhouse, NS Elvis, M Liedahl, DA Mathur, S TI Toward a self-consistent model of the ionized absorber in NGC 3783 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 3783); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; X-RAY-ABSORPTION; TRANSMISSION GRATING SPECTROMETER; WARM ABSORBER; EMISSION-LINE; INTRINSIC ABSORPTION; SEYFERT-1 GALAXIES; PHOTOIONIZED GASES; XMM-NEWTON AB We present a detailed model for the ionized absorbing gas evident in the 900 ks Chandra HETGS spectrum of NGC 3783. The analysis was carried out with PHASE, a new tool designed to model X-ray and UV absorption features in ionized plasmas. The 0.5-10 keV intrinsic continuum of the source is well represented by a single power law (Gamma=1.53) and a soft blackbody component (kTsimilar to0.1 keV). The spectrum contains over 100 features, which are well fitted by PHASE with just six free parameters. The model consists of a simple two-phase absorber with a difference of approximate to35 in the ionization parameter and a difference of approximate to4 in the column density of the phases. The two absorption components turned out to be in pressure equilibrium and are consistent with a single outflow (approximate to750 km s(-1)), a single turbulent velocity (300 km s(-1)), and solar elemental abundances. The main features of the low-ionization phase are an FeM-shell unresolved transition array (UTA) and the O VII lines. The O VII features, usually identified with the O VIII and a warm absorber, are instead produced in a cooler medium that also produces O VI lines. The UTA sets tight constraints on the ionization degree of the absorbers, making the model more reliable. The high-ionization phase is required by the O VIII and the Fe L-shell lines, and there is evidence for an even more ionized component in the spectrum. A continuous range of ionization parameters is disfavored by the fits, particularly to the UTA. Our model indicates a severe blending of the absorption and emission lines, as well as strong saturation of the most intense O absorption lines. This is in agreement with the O VII (taulambda=0.33) and O VIII (taulambda=0.13) absorption edges required to fit the spectrum. The low-ionization phase can be decomposed into three subcomponents on the basis of the outflow velocity, FWHM, and H column densities found for three of the four UV absorbers detected in NGC 3783. However, the ionization parameters are systematically smaller in our model than those derived from UV data, indicating a lower degree of ionization. Finally, our model predicts a Ca XVI line for the feature observed at around 21.6 Angstrom (a feature formerly identified as O VII), constraining the contribution from a zero-redshift absorber. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lawrence Livermore Natl Lab, Dept Phys & Adv Technol, Livermore, CA 94550 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Krongold, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Nicastro, Fabrizio/0000-0002-6896-1364; Brickhouse, Nancy/0000-0002-8704-4473 NR 65 TC 140 Z9 140 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 2003 VL 597 IS 2 BP 832 EP 850 DI 10.1086/378639 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700016 ER PT J AU Qi, CH Kessler, JE Koerner, DW Sargent, AI Blake, GA AF Qi, CH Kessler, JE Koerner, DW Sargent, AI Blake, GA TI Continuum and CO/HCO+ emission from the disk around the T Tauri star LkCa 15 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : molecules; planetary systems : protoplanetary disks; radio lines : stars; stars : individual (LkCa 15) ID MAIN-SEQUENCE STARS; YOUNG-STELLAR-OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MONTE-CARLO METHOD; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; HL-TAURI; MOLECULAR-EXCITATION; RADIATIVE-TRANSFER AB We present Owens Valley Radio Observatory Millimeter Array lambda = 3: 4 1: 2 mm dust continuum and spectral line observations of the accretion disk encircling the T Tauri star LkCa 15. The 1.2 mm dust continuum emission is resolved and gives a minimum diameter of 190 AU and an inclination angle of 57degrees +/- 5degrees. There is a noticeable but, at present, poorly constrained decrease in the continuum spectral slope with frequency that may result from the coupled processes of grain growth and dust settling. Imaging of the fairly intense emission from the lowest rotational transitions of CO, (CO)-C-13, and HCO+ reveals a rotating disk substantially larger than that observed in the dust continuum. Emission extends to similar to750 AU and the characteristic radius of the disk is determined to be similar to425 AU (HWHM), based on model fits to the CO velocity field. The measured line ratios demonstrate that the emission from these species is optically thick, while that from (CO)-O-18 and (HCO+)-C-13 is optically thin, or nearly so. The disk mass derived from the CO isotopologues with typical dense cloud abundances is still nearly 2 orders of magnitude less than that inferred from the dust emission, the most probable explanation being extensive molecular depletion in the cold, dense disk midplane. Thus, while CO, HCO+, and their isotopologues are excellent tracers of the disk velocity field, they are not reliable tracers of the disk mass. N2H+ 1 --> 0 emission has also been detected which, along with HCO+, sets a lower limit to the fractional ionization of 10(-8) in the near-surface regions of protoplanetary disks. This first detection of N2H+ in circumstellar disks has also made possible a determination of the N-2/CO ratio (similar to2) that is at least an order of magnitude larger than those in the envelopes of young stellar objects and dense clouds. The large N-2/CO ratio indicates that our observations probe disk layers in which CO is depleted but some N-2 remains in the gas phase. Such differential depletion can lead to large variations in the fractional ionization with height in the outer reaches of circumstellar disks and may help to explain the relative nitrogen deficiency observed in comets. C1 CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Qi, CH (reprint author), CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. NR 58 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 10 PY 2003 VL 597 IS 2 BP 986 EP 997 DI 10.1086/378494 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700029 ER PT J AU Pfahl, E Rappaport, S Podsiadlowski, P AF Pfahl, E Rappaport, S Podsiadlowski, P TI The galactic population of low- and intermediate-mass X-ray binaries SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; pulsars : general; stars : neutron; X-rays : stars ID COMMON ENVELOPE EVOLUTION; BLACK-HOLE BINARIES; MILLISECOND PULSARS; RADIO PULSARS; CYGNUS X-2; CLOSE BINARIES; HELIUM STARS; VELOCITY DISTRIBUTION; STELLAR EVOLUTION; COMPACT BINARIES AB We present the first study that combines binary population synthesis in the Galactic disk and detailed evolutionary calculations of low- and intermediate-mass X-ray binaries (L/IMXBs). Our approach allows us to follow completely the formation of incipient L/IMXBs and their evolution through the mass-transfer phase to the point when they become binary millisecond pulsars (BMPs). We show that the formation probability of IMXBs with initial donor masses of 1.5-4 M-circle dot is typically greater than or similar to5 times higher than that of standard LMXBs with initial donor masses of less than 1.5 M-circle dot. Since IMXBs evolve to resemble observed LMXBs, we suggest that the majority of the observed systems may have descended from IMXBs. Distributions at the current epoch of the orbital periods, donor masses, and mass accretion rates of L/IMXBs have been computed, as have orbital-period distributions of BMPs. This is a major step forward over previous theoretical population studies of L/IMXBs that utilized only crude representations of the binary evolution through the X-ray phase. Several significant discrepancies between the theoretical and observed distributions are discussed. We find that the total number of luminous (L-X > 10(36) ergs s(-1)) X-ray sources at the current epoch and the period distribution of BMPs are very sensitive to the parameters in the analytic formula describing the common-envelope phase that precedes the formation of the neutron star. The orbital-period distribution of observed BMPs strongly favors cases in which the common envelope is more easily ejected. However, this leads to an approximately hundredfold overproduction of the theoretical number of luminous X-ray sources relative to the total observed number of LMXBs. As noted by several groups prior to our study, X-ray irradiation of the donor star may result in a dramatic reduction in the X-ray active lifetime of L/IMXBs, and we suggest that irradiation may resolve the overproduction problem as well as the long-standing BMP/LMXB birthrate problem. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. RP Pfahl, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 81 TC 99 Z9 99 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2003 VL 597 IS 2 BP 1036 EP 1048 DI 10.1086/378632 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700034 ER PT J AU Still, M Hussain, G AF Still, M Hussain, G TI Coronal element abundances of the post-common-envelope binary V471 Tauri with ASCA SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; stars : individual (V471 Tauri); stars : magnetic fields; white dwarfs; X-rays : binaries ID V471 TAURI; X-RAY; ECLIPSING BINARY; WHITE-DWARF; ENERGETIC PARTICLES; CLOSE BINARIES; RADIO-EMISSION; HYADES CLUSTER; STARS; MASS AB We report on ASCA observations of the coronally active companion star in the post-common-envelope binary V471 Tau. Evolutionary calculations indicate that there should be no peculiar abundances on the companion star resulting from the common-envelope epoch. Indeed, we find no evidence for peculiar abundances, although uncertainties are high. We find that a single-temperature plasma model does not fit the data. Two-temperature models with decoupled elemental abundances suggest that Fe is underabundant compared to the Hyades photospheric mean. In the absence of a measurement of photospheric Ne abundance in the cluster, we find that Ne is overabundant compared to the solar photospheric value. This is indicative of the inverse first ionization potential effect. Differences between coronal and photospheric abundances are believed to result from the fractionation of ionized and neutral material in the upper atmosphere of the star. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Still, M (reprint author), Univ Space Res Assoc, Columbia, MD USA. NR 49 TC 7 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 NOV 10 PY 2003 VL 597 IS 2 BP 1059 EP 1064 DI 10.1086/378507 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700036 ER PT J AU Konacki, M Torres, G Sasselov, DD Jha, S AF Konacki, M Torres, G Sasselov, DD Jha, S TI High-resolution spectroscopic follow-up of OGLE planetary transit candidates in the Galactic bulge: Two possible Jupiter-mass planets and two blends SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; planetary systems; stars : low-mass, brown dwarfs techniques : radial velocities ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; EXTRASOLAR PLANET; 51-PEG-LIKE PLANET; RADIAL-VELOCITIES; 2001 CAMPAIGN; PARENT STAR; SEARCH; DISK; ATMOSPHERE AB We report the results of our campaign to follow up spectroscopically several candidate extrasolar transiting planets from the OGLE-III survey in the direction of the Galactic center, announced in 2001. All of these objects present shallow and periodic dips in brightness that may be due to planetary companions. Our Keck I/High Resolution Echelle Spectrometer ( HIRES) observations have revealed two interesting cases (OGLE-TR-10 with a period of 3.1 days and OGLE-TR-58 with a period of 4.3 days) that show no radial velocity variations at the level of 100-200 m s(-1). If orbited by companions, their masses would be similar to Jupiter. With the information in hand ( including the light curves) we are not able to rule out that these candidates are instead the result of contamination from an eclipsing binary in the same line of sight (a "blend"). We also discuss the case of OGLE-TR-56, which was recently reported by Konacki et al. to have a Jupiter-size companion, on the basis of an earlier analysis of our data and we present supporting information. Two other candidates, OGLE-TR-3 and OGLE-TR-33, show clear evidence that they are blends. We describe tests carried out to characterize the stability of the HIRES spectrograph and its impact on the determination of precise velocities for faint stars (V greater than or equal to 15 mag) using exposures of a thorium-argon lamp as the wavelength reference. Systematic effects are at the level of 100 m s(-1) or smaller and tend to dominate the total error budget. We also evaluate the precision attainable using the iodine gas absorption cell as an alternative fiducial, and we propose a simplified version of the standard procedure employed for high-precision Doppler planet searches that is very promising. Results from both this method and the classical ThAr technique show the feasibility of spectroscopic follow-up for faint targets in the range V = 14-17. We point out also that the high incidence of contamination from blends and other false positives in the OGLE-III survey already mentioned by Konacki et al. is potentially a serious concern not only for other similar surveys of relatively faint stars but also for future space missions to search for transits due to extrasolar planets as small as the Earth. C1 CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. Polish Acad Sci, Nicholaus Copernicus Astron Ctr, PL-87100 Torun, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Konacki, M (reprint author), CALTECH, Dept Geol & Planetary Sci, MS 150-21, Pasadena, CA 91125 USA. RI Konacki, Maciej/A-1220-2007 NR 40 TC 62 Z9 62 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 2003 VL 597 IS 2 BP 1076 EP 1091 DI 10.1086/378561 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700039 ER PT J AU Raymond, JC Ciaravella, A Dobrzycka, D Strachan, L Ko, YK Uzzo, M Raouafi, NE AF Raymond, JC Ciaravella, A Dobrzycka, D Strachan, L Ko, YK Uzzo, M Raouafi, NE TI Far-ultraviolet spectra of fast coronal mass ejections associated with X-class flares SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : activity; Sun : corona; Sun : coronal mass ejections (CMEs) ID 21 APRIL 2002; STREAMER BELT; ELEMENTAL ABUNDANCES; ATOMIC DATABASE; EMISSION-LINES; ACTIVE-REGION; CURRENT SHEET; SOLAR CORONA; FLUX ROPES; SPECTROMETER AB The Ultraviolet Coronagraph Spectrometer (UVCS) on board the Solar and Heliospheric Observatory satellite has observed very fast coronal mass ejections (CMEs) associated with X-class flares. These events show spectral signatures different from those seen in most other CMEs in terms of very rapid disruption of the pre-CME streamer, very high Doppler shifts, and high-temperature plasma visible in the [Fe XVIII] emission line. This paper describes three very similar events on 2002 April 21, July 23, and August 24 associated with X-class flares. We determine the physical parameters of the pre-CME streamers and discuss the geometric and physical nature of the streamer blowouts. In the April 21 event, the hot plasma seen as [Fe XVIII] is not related to the structure seen in [Fe XXI] by the Solar Ultraviolet Measurement of Emitted Radiation (SUMER) instrument at lower heights. It has the form of a rapidly expanding fan, quite likely a current sheet. In the August event, on the other hand, the [Fe XVIII] is probably a bubble of hot plasma formed by reconnection in the wake of the CME. C III emission from the July 23. are is detected as stray light in the UVCS aperture. It precedes the hard X-ray brightening by about 2 minutes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Aeron, D-37191 Katlenburg Lindau, Germany. European So Observ, D-85748 Garching, Germany. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Raouafi, Nour/C-2286-2016 OI Raouafi, Nour/0000-0003-2409-3742 NR 54 TC 80 Z9 83 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2003 VL 597 IS 2 BP 1106 EP 1117 DI 10.1086/378663 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700042 ER PT J AU Ciaravella, A Raymond, JC van Ballegooijen, A Strachan, L Vourlidas, A Li, J Chen, J Panasyuk, A AF Ciaravella, A Raymond, JC van Ballegooijen, A Strachan, L Vourlidas, A Li, J Chen, J Panasyuk, A TI Physical parameters of the 2000 February 11 coronal mass ejection: Ultraviolet spectra versus white-light images SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : UV radiation ID MAGNETIC-FLUX ROPE; X-RAY TELESCOPE; SOLAR CORONA; SOHO; SPECTROMETER; LASCO; PROMINENCES; TRANSIENTS; GEOMETRY; EIT AB We present spectra of a three-part coronal mass ejection (CME) observed by the Ultraviolet Coronagraph Spectrometer aboard SOHO on 2000 February 11. Images of the CME in different spectral lines show how the morphology depends on the temperature, density, and outflow speed of the ejected plasma. The H I Lyalpha is the line that best resembles the white-light data, although it can be rather different where the outflow speed severely dims its radiative component. We estimate the ranges of temperature and density in the front, prominence core, and void. We also estimate the outflow speed that is the true speed of the ejecta as obtained from the Doppler dimming technique, its component projected on the plane of the sky, and the line-of-sight speed for the three components of the CME. The plasma in the front was denser, cooler, and more depleted in O and Si than the ambient coronal streamer. These characteristics indicate that it originated in the closed field core of the pre-CME streamer. The leading edge was not the projection of a simple spherical shell onto the plane of the sky. The line profiles suggest a wide looplike structure, although a more complete shell that was brighter in some areas could also match the data. The prominence has a structure in temperature and density with the hotter top end emitting in the Mg x and Si XII lines while the bottom end was much cooler and visible only in the H I Lyman lines. Emission in the void was rather faint. The outflow speed obtained from Doppler dimming of the radiative lines, the line-of-sight speed measured from the Doppler shift of the lines, and the plane-of-the-sky speed estimated from the comparison of the images taken at 2.3 and 2.6 R-circle dot give speeds much lower than those estimated at greater heights (>4 R-circle dot) from LASCO and indicate a stronger acceleration at lower heights. C1 Osservatorio Astron GS Vaiana, INAF, I-90134 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Div Plasma Phys, Washington, DC 20375 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Ciaravella, A (reprint author), Osservatorio Astron GS Vaiana, INAF, Piazza Parlamento 1, I-90134 Palermo, Italy. RI Vourlidas, Angelos/C-8231-2009 OI Vourlidas, Angelos/0000-0002-8164-5948 NR 53 TC 34 Z9 34 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 2003 VL 597 IS 2 BP 1118 EP 1134 DI 10.1086/381220 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700043 ER PT J AU Frazin, RA Cranmer, SR Kohl, JL AF Frazin, RA Cranmer, SR Kohl, JL TI Empirically determined anisotropic velocity distributions and outflows of O5+ ions in a coronal streamer at solar minimum SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : UV radiation ID POSITIVE ESTIMATION; NEUTRAL HYDROGEN; MAGNETIC-FIELD; INNER CORONA; STRAY-LIGHT; WIND; SPECTROMETER; UVCS/SOHO; MODEL; ACCELERATION AB Empirical constraints on the O5+ velocity distributions and outflow speeds in a solar minimum equatorial streamer between 2.6 and 5.1 R-circle dot are determined using a spectral synthesis code that includes O VI Doppler dimming. These constraints follow directly from UV spectra taken on 1996 October 12 with the Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO) satellite and three-dimensional electron densities derived from tomography applied to a time series of polarized white-light images taken with the Large Angle and Spectrometric Coronagraph (LASCO) also on SOHO. Four conclusions result from this work: (1) our analysis shows O5+ velocity distribution anisotropy in the streamer legs and stalk and gives strong evidence that the microscopic velocity distribution (which excludes wave motions that equally affect all charged particles) is anisotropic, where the most probable speed perpendicular to the magnetic field direction exceeds that in the parallel direction; (2) there is preferential heating of the O5+ ions over the protons in the streamer stalk and legs; (3) there is no evidence for preferential O5+ heating in the core; and (4) the outflow velocity of the O5+ ions is determined at heights above 4.6 R-circle dot. All results have a confidence level of at least 70%. C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Frazin, RA (reprint author), Univ Illinois, Dept Elect & Comp Engn, 1406 W Green St, Urbana, IL 61801 USA. RI Frazin, Richard/J-2625-2012 NR 38 TC 57 Z9 58 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2003 VL 597 IS 2 BP 1145 EP 1157 DI 10.1086/378558 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZG UT WOS:000186432700045 ER PT J AU Laursen, LT Stanek, KZ AF Laursen, LT Stanek, KZ TI High-precision photometry of the gamma-ray burst GRB 020813: The smoothest afterglow yet SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID OPTICAL AFTERGLOW; IMAGE SUBTRACTION; VARIABILITY AB We report results of our precise reduction of the high signal-to-noise ratio VRI observations of the optical afterglow of the gamma-ray burst GRB 020813 obtained by Gladders & Hall with the Magellan 6.5 m telescope 3.9-4.9 hr after the burst. These observations are very well fitted locally by a power-law curve, providing the tightest constraints yet on how smooth the afterglows can be in some cases: the rms deviations range from 0.005 mag (0.5%) for the R band to 0.007 mag for the I band, only marginally larger than the rms scatter for nearby nonvariable stars. This scatter is a factor of several smaller than the smallest reported rms of 0.02 mag for GRB 990510 (Stanek et al.). These observations are in strong contrast to those of afterglows of GRB 011211 and GRB 021004, for which large, greater than 10% variability has been observed on timescales from similar to20 minutes to several hours. If interstellar medium (ISM) density fluctuations near the GRB are indeed causing the bumps and wiggles observed in some bursts, very uniform regions of ISM near some bursts must be present as well. This result also constrains the intrinsic smoothness of the afterglow itself. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Laursen, LT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 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 NOV 10 PY 2003 VL 597 IS 2 BP L107 EP L108 DI 10.1086/380297 PN 2 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZL UT WOS:000186433200005 ER PT J AU Martini, P Schneider, DP AF Martini, P Schneider, DP TI Multiepoch sky surveys and the lifetime of quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; quasars : general; surveys ID MASSIVE BLACK-HOLES; HIGH-REDSHIFT; GALAXIES; VARIABILITY; NUCLEI; QSOS AB We present a new method for measuring the episodic lifetime of quasars with current and future large-scale sky surveys. Future photometric observations of large samples of confirmed quasars can provide a direct measurement (or interesting lower limit) to the lifetime of an individual episode of quasar activity (t(Q)) and potentially enable the study of postquasar host galaxies. Photometric observations of the quasars found by the Sloan Digital Sky Survey (SDSS) and Two-Degree Field Survey could, with a time baseline of 10 years, determine t(Q) to within a factor of 2 if t(Q)<10(5) yr or set a lower limit to the quasar lifetime. Multiple-epoch precise photometry with the proposed Large Synoptic Survey Telescope could test more complex models for quasar variability and mean quasar luminosity evolution. These observations could also constrain the rate that tidal disruptions of single stars produce quasar luminosities. It is possible to reverse the order of this investigation; previous-epoch plate material, such as the Digitized Sky Survey, can be used to determine if any of the SDSS quasars had not yet turned on at the time of these prior observations. Measurements of the entire SDSS quasar sample over the &SIM;50 yr baseline provided by these plates potentially can be used to estimate t(Q) to within a factor of 2 if t(Q)<10(5.5) yr, provided quasar variability can be accurately characterized and the detection efficiency and photometric calibration of the plate material can be well determined. These measurements of t(Q) will have comparable quality to existing, more indirect estimates of the quasar lifetime. Analysis of the 3814 quasars in the SDSS Early Data Release finds that t(Q) must be larger than approximately 20,000 yr. C1 Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RP Martini, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS20, 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 2003 VL 597 IS 2 BP L109 EP L112 DI 10.1086/379888 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZL UT WOS:000186433200006 ER PT J AU Muzerolle, J Calvet, N Hartmann, L D'Alessio, P AF Muzerolle, J Calvet, N Hartmann, L D'Alessio, P TI Unveiling the inner disk structure of T Tauri stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared : stars; stars : formation; stars : pre-main-sequence; techniques : spectroscopic ID HERBIG AE/BE STARS; YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; ACCRETION DISKS; MAGNETOSPHERIC ACCRETION; CIRCUMSTELLAR DISKS; EMISSION; TESTS; MODEL; CONSTRAINTS AB We present near-infrared spectra of the excess continuum emission from the innermost regions of classical T Tauri disks. In almost all cases, the shape of the excess is consistent with that of a single-temperature blackbody with Tsimilar to1400 K, similar to the expected dust sublimation temperature for typical dust compositions. The amount of excess flux roughly correlates with the accretion luminosity in objects with similar stellar properties. We compare our observations with the predictions of simple disk models having an inner rim located at the dust sublimation radius, including irradiation heating of the dust from both the stellar and accretion luminosities. The models yield inner rim radii in the range 0.07-0.54 AU, increasing with higher stellar and accretion luminosities. Using typical parameters that fit our observed sample, we predict a rim radius similar to0.2 AU for the T Tauri star DG Tau, which agrees with recent Keck near-infrared interferometric measurements. For large mass accretion rates, the inner rim lies beyond the corotation radius at (or within) which magnetospheric accretion flows are launched, which implies that pure gaseous disks must extend inside the dust rim. Thus, for a significant fraction of young stars, dust cannot exist in the innermost disk, calling into question theories in which solid particles are ejected by a wind originating at the magnetospheric radius. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Muzerolle, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM jamesm@as.arizona.edu; ncalvet@cfa.harvard.edu; hartmann@cfa.harvard.edu; p.dalessio@astrosmo.unam.mx NR 40 TC 151 Z9 151 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 10 PY 2003 VL 597 IS 2 BP L149 EP L152 DI 10.1086/379921 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZL UT WOS:000186433200016 ER PT J AU Tomsick, JA Corbel, S Fender, R Miller, JM Orosz, JA Rupen, MP Tzioumis, T Wijnands, R Kaaret, P AF Tomsick, JA Corbel, S Fender, R Miller, JM Orosz, JA Rupen, MP Tzioumis, T Wijnands, R Kaaret, P TI Chandra detections of two quiescent black hole X-ray transients SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars : individual (V4641 Sgr, XTE J1859+226); stars : winds, outflows; X-rays : stars ID LOW/HARD STATE; SPECTRAL STATE; XTE J1550-564; JETS; EMISSION; BINARIES; RADIO; J1819.3-2525; TRANSITION; MODEL AB Using the Chandra X-Ray Observatory, we have detected the black hole transients V4641 Sgr and XTE J1859+226 in their low-luminosity quiescent states. The 0.3-8 keV luminosities are (4.0(-2.4)(+3.3))x10(31) (d/7 kpc)(2) ergs s(-1) and (4.2(-2.2)(+4.8))x10(31) (d/11 kpc)(2) ergs s(-1) for V4641 Sgr and XTE J1859+226, respectively. With the addition of these two systems, 14 out of the 15 transients with confirmed black holes (via compact object mass measurements) now have measured quiescent luminosities or sensitive upper limits. The only exception is GRS 1915+105, which has not been in quiescence since its discovery in 1992. The luminosities for V4641 Sgr and XTE J1859+226 are consistent with the median luminosity of 2x10(31) ergs s(-1) for the systems with previous detections. Our analysis suggests that the quiescent X-ray spectrum of V4641 Sgr is harder than for the other systems in this group, but because of the low statistical quality of the spectrum, it is not clear if V4641 Sgr is intrinsically hard or if the column density is higher than the interstellar value. Focusing on V4641 Sgr, we compare our results to theoretical models for X-ray emission from black holes in quiescence. Also, we obtain precise X-ray positions for V4641 Sgr and XTE J1859+226 via cross-correlation of the X-ray sources detected near our targets with IR sources in the Two Micron All Sky Survey catalog. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Paris 07, F-91191 Gif Sur Yvette, France. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Tomsick, JA (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, Code 0424, La Jolla, CA 92093 USA. NR 43 TC 28 Z9 28 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2003 VL 597 IS 2 BP L133 EP L136 DI 10.1086/380088 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740ZL UT WOS:000186433200012 ER PT J AU He, FL Hubbell, SP AF He, FL Hubbell, SP TI Percolation theory for the distribution and abundance of species SO PHYSICAL REVIEW LETTERS LA English DT Article ID LANDSCAPES AB We develop and test new models that unify the mathematical relationships among the abundance of a species, the spatial dispersion of the species, the number of patches occupied by the species, the edge length of the occupied patches, and the scale on which the distribution of species is mapped. The models predict that species distributions will exhibit percolation critical thresholds, i.e., critical population abundances at which the fragmented patches (as measured by the number of patches and edge length) start to coalesce to form large patches. C1 Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC V8Z 1M5, Canada. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP He, FL (reprint author), Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. NR 17 TC 26 Z9 27 U1 0 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 NOV 7 PY 2003 VL 91 IS 19 AR 198103 DI 10.1103/PhysRevLett.91.198103 PG 4 WC Physics, Multidisciplinary SC Physics GA 740VR UT WOS:000186422700053 PM 14611621 ER PT J AU Bilby, K AF Bilby, K TI Divine utterances: The performance of Afro-Cuban Santeria. SO AMERICAN ETHNOLOGIST LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Bilby, K (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 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 NOV PY 2003 VL 30 IS 4 BP 628 EP 629 DI 10.1525/ae.2003.30.4.628 PG 2 WC Anthropology SC Anthropology GA 748EA UT WOS:000186848100023 ER PT J AU Axsmith, BJ Serbet, R Krings, M Taylor, TN Taylor, EL Mamay, SH AF Axsmith, BJ Serbet, R Krings, M Taylor, TN Taylor, EL Mamay, SH TI The enigmatic Paleozoic plants Spermopteris and Phasmatocycas reconsidered SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE carboniferous; cycads; Permian; Phasmatocyas; pteridosperms; Spermopteris; Taeniopteris ID CYCADALEAN AFFINITY; TAENIOPTERID LAMINA; CYCADS; KANSAS; CHINA; GENUS AB Ovule-bearing leaves from the Paleozoic of North America assigned to Spernopteris and Phasmatocycas have been interpreted as primitive cycad megasporophylls. According to this hypothesis, Cycas megasporophylls were derived from a Spermopteris-like ancestor via Phasmatocycas and various other taeniopterid forms. This putative transformation entailed the phyletic shift of ovule attachment from the abaxial lamina surface of Spermopteris to the leaf midrib in Phasinatocyas. However, reexamination of the original Spermopteris specimens from the Lawrence Shale of Kansas has shown that the ovules are attached to the leaf midrib. Therefore, Spemopteris and Phasinatocyas differ only in a few details of lamina morphology. The apical cleft of the ovules of both forms is interpreted as an original feature rather than a preservational artifact; however, the abaxial flange is probably a result of compression of a terete midrib. Spermopteris is typified by sterile specimens of Taeniopteris coriacea from Europe, which are of uncertain affinity to the fertile leaves. Therefore, we propose that the ovule-bearing leaves now known as Spermopteris coriacea be named as a new species of Phasmatocycas (Phasmatocycas bridwellii sp. nov.). The new concept of Phasmatocyas is less cycad-like than previously thought, and the phylogenetic position of the genus is unclear. C1 Univ S Alabama, Dept Biol Sci, Mobile, AL 36688 USA. Museum Hist Nat, Div Paleobot, Lawrence, KS 66045 USA. Biodivers Res Ctr, Lawrence, KS 66045 USA. Bayer Staatssammlung Palaontol & Geol, Funktionseinheit Palaontol, D-80333 Munich, Germany. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Univ Kansas, Museum Nat Hist, Lawrence, KS 66045 USA. Univ Kansas, Biodivers Ctr, Lawrence, KS 66045 USA. Museum Natl Hist Nat, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. RP Axsmith, BJ (reprint author), Univ S Alabama, Dept Biol Sci, LSCB 124, Mobile, AL 36688 USA. NR 22 TC 19 Z9 21 U1 0 U2 1 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 NOV PY 2003 VL 90 IS 11 BP 1585 EP 1595 DI 10.3732/ajb.90.11.1585 PG 11 WC Plant Sciences SC Plant Sciences GA 744PB UT WOS:000186639900005 PM 21653333 ER PT J AU Morley, RJ Dick, CW AF Morley, RJ Dick, CW TI Missing fossils, molecular clocks, and the origin of the Melastomataceae SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE chloroplast DNA; Melastomataceae; palynology; plate tectonics; synonymous substitution rates; tropical rain forests ID NUCLEOTIDE SUBSTITUTION; CHLOROPLAST; EVOLUTION; RATES; PHYLOGENY; DISPERSAL AB In a recent analysis of the historical biogeography of Melastomataceae, Renner, Clausing, and Meyer (2001; American Journal of Botany 88(7): 1290-1300) rejected the hypothesis of a Gondwana origin. Using a fossil-calibrated chloroplast DNA (ndhF) phylogeny, they placed the early diversification of Melastomataceae in Laurasia at the Paleocene/Eocene boundary (ca. 55 Ma) and suggested that long-distance oceanic dispersals in the Oligocene and Miocene (34 to 5 Ma) account for its range expansion into South America, Africa, and Madagascar. Their critical assumption-that oldest northern mid-latitude melastome fossils reflect tribal ages and their geographic origins-may be erroneous, however, because of the sparse fossil record in the tropics. We show that rates of synonymous nucleotide substitutions derived by the Renner et al. (2001) model are up to three times faster than most published rates. Under a Gondwana-origin model advocated here, which includes dispersals from Africa to Southeast Asia via the "Indian ark" and emphasizes filter rather than either sweepstakes dispersal or strict vicariance, rates of nucleotide substitution fall within the range of published rates. We suggest that biogeographic reconstructions need to consider the paucity of Gondwanan fossils and that frequently overlooked interplate dispersal routes provide alternatives to vicariance, boreotropical dispersal, and long-distance oceanic dispersal as explanations for the amphi-oceanic disjunctions of many tropical rain forest plants. C1 Monash Univ, Sch Geog & Environm Sci, Clayton, Vic 3800, Australia. Univ London Royal Holloway & Bedford New Coll, Dept Geol, Egham TW20 0EX, Surrey, England. Smithsonian Trop Res Inst, Miami, FL 34002 USA. RP Morley, RJ (reprint author), Palynova PT Eksindo Pratama,Villa Indah Pajajaran, Bogor 16153, Indonesia. RI Dick, Christopher/A-8744-2008 NR 43 TC 44 Z9 47 U1 1 U2 9 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 NOV PY 2003 VL 90 IS 11 BP 1638 EP 1644 DI 10.3732/ajb.90.11.1638 PG 7 WC Plant Sciences SC Plant Sciences GA 744PB UT WOS:000186639900011 PM 21653339 ER PT J AU Jonsdottir, B Ortner, DJ Frohlich, B AF Jonsdottir, B Ortner, DJ Frohlich, B TI Probable destructive meningioma in an archaeological adult male skull from Alaska SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE intracranial tumor; cranial base lesions AB Several intracranial pathological conditions can affect the bones of the skull. The most common cause of these conditions is tumor, but infection and other diseases are also known to affect the bones of the skull. Distinguishing between the various causes of intracranial skeletal pathology in archaeological human remains is usually a challenging exercise, and a specific diagnosis will often be impossible. Meningiomas are tumors that arise in arachnoid tissues embedded in the outer layer of the dura. Because of this association, they occur almost exclusively in the skull and vertebral column. Usually meningiomas are slow-growing tumors that do not metastasize to other organs and tissues of the body. However, rare cases can be malignant and, even when meningiomas are benign, their presence and growth can adversely affect the nervous and vascular supply to other tissues in the skull and vertebral column. Their effect on adjacent bone tissue varies from stimulating bone-forming lesions to causing highly destructive lesions. A few examples of meningioma have been described in the paleopathological literature. Most of these cases are bone-stimulating meningiomas. The case presented here is a probable example of a highly destructive meningioma of the skull base, with unilateral extension into the left side of the cranium. This case is compared with a modern clinical case of destructive intracranial meningioma that was documented both radiographically and pathologically. Destructive meningiomas can be confused with other pathological conditions, including benign and malignant tumors. Criteria for differentiating the diagnostic options are reviewed. (C) 2003 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. Rontgen Domus Medica, Reykjavik, Iceland. Univ Bradford, Dept Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England. RP Ortner, DJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 8 TC 6 Z9 6 U1 1 U2 4 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 NOV PY 2003 VL 122 IS 3 BP 232 EP 239 DI 10.1002/ajpa.10285 PG 8 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 734CV UT WOS:000186038400004 PM 14533181 ER PT J AU Harris, TR Monfort, SL AF Harris, TR Monfort, SL TI Behavioral and endocrine dynamics associated with infanticide in a black and white Colobus monkey (Colobus guereza) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE Colobus guereza; infanticide; urinary hormones; mating behavior ID LANGURS PRESBYTIS-ENTELLUS; ENZYME-IMMUNOASSAY; STRATEGIES; FEMALES; MALES; ADULT AB Infanticide has been observed in several colobines, but only one infanticide has previously been documented for black and white colobus monkeys (Colobus guereza). This report describes an infanticide observed in Kibale National Park, Uganda, in the summer of 2001. An adult male from a neighboring group attacked and killed a young infant whose mother subsequently remained in her own group and was observed mating 10 days later. She engaged in two mating periods of several days each, separated by approximately 1 month, during which she copulated frequently with the dominant male within her group. Urinary estrogen (EC) and progesterone metabolite (PdG) excretion patterns demonstrated that the female resumed ovarian cycling soon after the infanticide. Because the infanticidal male did not attempt to mate with the victim's mother, his actions were not consistent with the predictions of the sexual-selection hypothesis. We speculate that infanticide associated with intergroup aggression may help secure access to high-quality resources for the infanticidal male's group. (C) 2003 Wiley-Liss, Inc. C1 Conservat & Res Ctr, Front Royal, VA 22630 USA. Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. RP Monfort, SL (reprint author), Conservat & Res Ctr, 1500 Remount Rd,Smithsonian Natl Zool Pk, Front Royal, VA 22630 USA. NR 26 TC 13 Z9 13 U1 2 U2 7 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 NOV PY 2003 VL 61 IS 3 BP 135 EP 142 DI 10.1002/ajp.10116 PG 8 WC Zoology SC Zoology GA 748VT UT WOS:000186882300004 PM 14610731 ER PT J AU Post, JE Heaney, PJ Cahill, CL Finger, LW AF Post, JE Heaney, PJ Cahill, CL Finger, LW TI Woodruffite: A new Mn oxide structure with 3 x 4 tunnels SO AMERICAN MINERALOGIST LA English DT Article ID OCTAHEDRAL MOLECULAR-SIEVES; MANGANESE OXIDE; CATION DISPLACEMENTS; RIETVELD REFINEMENT; TODOROKITE; CRYPTOMELANE; HOLLANDITES; CATALYSTS; BEHAVIOR; NODULES AB The mineral woodruffite, Zn-x/2(2+) (Mn-1-x(4+) Mn-x(3+))O-2.yH(2)O, xsimilar to0.4 and ysimilar to0.7, is the first known example of a new type of Mn oxide characterized by large tunnels that measure 3 and 4 octahedra (6.9x9.2 Angstrom) on a side. These tunnels are rectangular in cross-section and are the largest of any yet reported in natural or synthetic Mn oxides. The thermal stability of woodruffite is comparable to that of todorokite and other large-tunnel Mn oxide phases, breaking down at similar to300degreesC and eventually transforming to a spinel-type structure. The woodruffite structure may serve as a model for a new class of octahedral molecular sieves with enhanced capabilities as catalysts and selective cation-exchange agents. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. George Washington Univ, Dept Chem, Washington, DC 20052 USA. Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. RP Post, JE (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM post.jeffrey@nmnh.si.edu NR 28 TC 7 Z9 8 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 2003 VL 88 IS 11-12 BP 1697 EP 1702 PN 1 PG 6 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 747UZ UT WOS:000186824400009 ER PT J AU Smith, DA Ralls, K Hurt, A Adams, B Parker, M Davenport, B Smith, MC Maldonado, JE AF Smith, DA Ralls, K Hurt, A Adams, B Parker, M Davenport, B Smith, MC Maldonado, JE TI Detection and accuracy rates of dogs trained to find scats of San Joaquin kit foxes (Vulpes macrotis mutica) SO ANIMAL CONSERVATION LA English DT Article ID MOLECULAR TRACKING; FECES; DNA AB Specially trained detection dogs have been used to locate faeces (scats) for faecal analyses but their effectiveness has not been quantified. We evaluated detection and accuracy rates of dogs trained to find scats of endangered San Joaquin kit foxes (Vulpes macrotis mutica). Four dogs found from 0.43 to 5.37 presumptive kit fox scats per km of transect searched in two field sites where kit foxes and coyotes (Canis latrans) but not non-native red foxes (V. vulpes) were present. The unusually low detection rate (0.43 scats per km) by one dog (probably due to excessive panting in hot weather) was still similar to the average scat detection rate of two experienced humans. DNA tests of 1298 scats showed that all dogs were 100% accurate at distinguishing kit fox scats under our field conditions. Because red foxes are sympatric with kit foxes in some areas, we also conducted controlled discrimination experiments to see if trained dogs could distinguish between scats from kit and red foxes. Four dogs were 100% accurate at choosing a kit fox scat when red fox scats were present (n = 64 trials), but were less accurate at ignoring red fox scats in trials where a kit fox scat was absent. C1 Univ Washington, Dept Ecosyst Sci, Seattle, WA 98195 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. Univ Louisiana, Dept Biol, Lafayette, LA 70504 USA. Univ Montana, Sch Forestry, Wildlife Biol Program, Missoula, MT 59812 USA. Packleader Dog Training, Steilacoom, WA 98388 USA. Washington Dept Fish & Wildlife, LaConner, WA 98257 USA. Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. RP Smith, DA (reprint author), Univ Washington, Dept Ecosyst Sci, Seattle, WA 98195 USA. NR 34 TC 73 Z9 78 U1 3 U2 29 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD NOV PY 2003 VL 6 BP 339 EP 346 DI 10.1017/S136794300300341X PN 4 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 750GR UT WOS:000186983400008 ER PT J AU Leimgruber, P Gagnon, JB Wemmer, C Kelly, DS Songer, MA Selig, ER AF Leimgruber, P Gagnon, JB Wemmer, C Kelly, DS Songer, MA Selig, ER TI Fragmentation of Asia's remaining wildlands: implications for Asian elephant conservation SO ANIMAL CONSERVATION LA English DT Article ID VALIDATION; DYNAMICS; DATABASE; ROADS AB Habitat loss and fragmentation are main causes for Asian elephant population declines. We mapped wildlands - large, unfragmented and undeveloped areas - asking: (1) Where are the largest wildlands that constitute elephant habitats? (2) What proportion of these wildlands is protected? (3) What is their potential for elephant conservation? Our study demonstrates that wildlands constitute only 51% of the Asian elephant range. Myanmar has the largest wildland (similar to170,000 km(2)), followed by Thailand and India. In Principal Components Analysis (PCA), the first two components explained 73% of the variation in fragmentation among ranges. We identified three fragmentation clusters from the PCA. Cluster A contains large ranges with unfragmented wildlands; cluster B includes ranges with well-developed transportation networks and large human populations; and cluster C contains ranges with severely fragmented wildlands. In cluster A, we identified four ranges with elephant populations >1000 animals: ARYO, MYTJC, BNMH and BITE. Together with ranges that support >1000 elephants in cluster B, these A ranges have great potential for long-term elephant conservation. We propose that fragmentation clusters and population size can be used to identify different elephant monitoring and management zones. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Leimgruber, P (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 NR 47 TC 47 Z9 50 U1 7 U2 45 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD NOV PY 2003 VL 6 BP 347 EP 359 DI 10.1017/S1367943003003421 PN 4 PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 750GR UT WOS:000186983400009 ER PT J AU Rines, K Geller, MJ Kurtz, MJ Diaferio, A AF Rines, K Geller, MJ Kurtz, MJ Diaferio, A TI CAIRNS: The Cluster and Infall Region Nearby Survey. I. Redshifts and mass profiles SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : general; galaxies : kinematics and dynamics ID FLUX-LIMITED SAMPLE; X-RAY-CLUSTERS; GALAXY CLUSTERS; RICH CLUSTERS; COMA CLUSTER; HIERARCHICAL UNIVERSE; VELOCITY DISPERSIONS; TEMPERATURE RELATION; MATTER DISTRIBUTION; INTRACLUSTER MEDIUM AB The CAIRNS (Cluster and Infall Region Nearby Survey) project is a spectroscopic survey of the infall regions surrounding eight nearby, rich, X-ray-luminous clusters of galaxies. We have collected 15,654 redshifts (3471 new or remeasured) within similar to5-10 h(-1) Mpc of the centers of the clusters, making it the largest study of the infall regions of clusters. We determine cluster membership and the mass profiles of the clusters based on the phase-space distribution of the galaxies. All of the clusters display decreasing velocity dispersion profiles. The mass profiles are fitted well by functional forms based on numerical simulations but exclude an isothermal sphere. Specifically, NFW and Hernquist models provide good descriptions of cluster mass profiles to their turnaround radii. Our sample shows that the predicted infall pattern is ubiquitous in rich, X-ray-luminous clusters over a large mass range. The caustic mass estimates are in excellent agreement with independent X-ray estimates at small radii and with virial estimates at intermediate radii. The mean ratio of the caustic mass to the X-ray mass is 1.03+/-0.11, and the mean ratio of the caustic mass to the virial mass (when corrected for the surface pressure term) is 0.93+/-0.07. We further demonstrate that the caustic technique provides reasonable mass estimates even in merging clusters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smithsonian Astrophys Observ, Opt & Infrared Div, Cambridge, MA 02138 USA. Univ Turin, Dipartimento Fis GAen Amedeo Avogadro, I-10125 Turin, Italy. RP Rines, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI KURTZ, Michael /B-3890-2009; OI Kurtz, Michael/0000-0002-6949-0090 NR 81 TC 154 Z9 154 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 NOV PY 2003 VL 126 IS 5 BP 2152 EP 2170 DI 10.1086/378599 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 742AZ UT WOS:000186494200006 ER PT J AU Brandt, S Budtz-Jorgensen, C Lund, N Westergaard, NJ Rasmussen, IL Andersen, KH Chenevez, J Hornstrup, A Jensen, PA Laursen, S Omo, K Oxborrow, CA Pedersen, SM Polny, J Andersson, H Andersson, T Vilhu, O Huovelin, J Maisala, S Morawski, M Juchnikowski, G Costa, E Feroci, M Rubini, A Rapisarda, M Morelli, E Frontera, F Pelliciari, C Loffredo, G Carassiti, V Reglero, V Nunez, SM Larsson, S Svensson, R Zdziarski, AA Castro-Tirado, A Goria, M Giulianelli, G Rezazad, M Cordero, F Schmidt, M Carli, R Jensen, PL Sarri, G Gomez, C Orr, A Much, R Schnopper, HW Kretschmar, P AF Brandt, S Budtz-Jorgensen, C Lund, N Westergaard, NJ Rasmussen, IL Andersen, KH Chenevez, J Hornstrup, A Jensen, PA Laursen, S Omo, K Oxborrow, CA Pedersen, SM Polny, J Andersson, H Andersson, T Vilhu, O Huovelin, J Maisala, S Morawski, M Juchnikowski, G Costa, E Feroci, M Rubini, A Rapisarda, M Morelli, E Frontera, F Pelliciari, C Loffredo, G Carassiti, V Reglero, V Nunez, SM Larsson, S Svensson, R Zdziarski, AA Castro-Tirado, A Goria, M Giulianelli, G Rezazad, M Cordero, F Schmidt, M Carli, R Jensen, PL Sarri, G Gomez, C Orr, A Much, R Schnopper, HW Kretschmar, P TI JEM-X inflight performance SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation : detectors; X-rays : general AB We summarize the inflight performance of JEM-X, the X-ray monitor on the INTEGRAL mission during the initial ten months of operations. The JEM-X instruments have now been tuned to stable operational conditions. The performance is found to be close to the pre-launch expectations. The ground calibrations and the inflight calibration data permit to determine the instruments characteristics to fully support the scientific data analysis. C1 Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. Metorex Int Oy, Espoo 02631, Finland. Univ Helsinki, Observ, FIN-00014 Helsinki, Finland. Space Res Ctr, PL-00716 Warsaw, Poland. CNR, Inst Astrofis, I-00133 Rome, Italy. ENEA, Frascati UTS Fus, I-00045 Frascati, Italy. IASF Bologna, I-40129 Bologna, Italy. Univ Ferrara, Dipartmento Fis, I-44100 Ferrara, Italy. Univ Valencia, GACE, Valencia 46071, Spain. Stockholm Univ, S-10691 Stockholm, Sweden. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Alenia Spazio, Space Div, I-10146 Turin, Italy. ESOC, D-64293 Darmstadt, Germany. European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. INTEGRAL Sci Data Ctr, Versoix, Switzerland. RP Brandt, S (reprint author), Danish Space Res Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. RI Chenevez, Jerome/F-5380-2010; OI Costa, Enrico/0000-0003-4925-8523; Feroci, Marco/0000-0002-7617-3421; Castro-Tirado, A. J./0000-0003-2999-3563; Kretschmar, Peter/0000-0001-9840-2048 NR 21 TC 16 Z9 16 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 NOV PY 2003 VL 411 IS 1 BP L243 EP L251 DI 10.1051/0004-6361:20031363 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800040 ER PT J AU Courvoisier, TJL Beckmann, V Bourban, G Chenevez, J Chernyakova, M Deluit, S Favre, P Grindlay, JE Lund, N O'Brien, P Page, K Produit, N Turler, M Turner, MJL Staubert, R Stuhlinger, M Walter, R Zdziarski, AA AF Courvoisier, TJL Beckmann, V Bourban, G Chenevez, J Chernyakova, M Deluit, S Favre, P Grindlay, JE Lund, N O'Brien, P Page, K Produit, N Turler, M Turner, MJL Staubert, R Stuhlinger, M Walter, R Zdziarski, AA TI Simultaneous observations of the quasar 3C 273 with INTEGRAL, XMM-Newton and RXTE SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-rays : observations; galaxies : active; quasars : general; quasars : individual : 3C 273 ID 3C-273 AB INTEGRAL has observed the bright quasar 3C 273 on 3 epochs in January 2003 as one of the first observations of the open programme. The observation on January 5 was simultaneous with RXTE and XMM-Newton observations. We present here a first analysis of the continuum emission as observed by these 3 satellites in the band from similar or equal to3 keV to similar or equal to500 keV. The continuum spectral energy distribution of 3C 273 was observed to be weak and steep in the high energies during this campaign. We present the actual status of the cross calibrations between the instruments on the three platforms using the calibrations available in June 2003. C1 INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Observ Geneva, CH-1290 Sauverny, Switzerland. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Courvoisier, TJL (reprint author), INTEGRAL Sci Data Ctr, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. RI Chenevez, Jerome/F-5380-2010 NR 18 TC 31 Z9 31 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 2003 VL 411 IS 1 BP L343 EP L348 DI 10.1051/0004-6361:20031206 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800055 ER PT J AU Lund, N Budtz-Jorgensen, C Westergaard, NJ Brandt, S Rasmussen, IL Hornstrup, A Oxborrow, CA Chenevez, J Jensen, PA Laursen, S Andersen, KH Mogensen, PB Rasmussen, I Omo, K Pedersen, SM Polny, J Andersson, H Andersson, T Kamarainen, V Vilhu, O Huovelin, J Maisala, S Morawski, M Juchnikowski, G Costa, E Feroci, M Rubini, A Rapisarda, M Morelli, E Carassiti, V Frontera, F Pelliciari, C Loffredo, G Nunez, SM Reglero, V Velasco, T Larsson, S Svensson, R Zdziarski, AA Castro-Tirado, A Attina, P Goria, M Giulianelli, G Cordero, F Rezazad, M Schmidt, M Carli, R Gomez, C Jensen, PL Sarri, G Tiemon, A Orr, A Much, R Kretschmar, P Schnopper, HW AF Lund, N Budtz-Jorgensen, C Westergaard, NJ Brandt, S Rasmussen, IL Hornstrup, A Oxborrow, CA Chenevez, J Jensen, PA Laursen, S Andersen, KH Mogensen, PB Rasmussen, I Omo, K Pedersen, SM Polny, J Andersson, H Andersson, T Kamarainen, V Vilhu, O Huovelin, J Maisala, S Morawski, M Juchnikowski, G Costa, E Feroci, M Rubini, A Rapisarda, M Morelli, E Carassiti, V Frontera, F Pelliciari, C Loffredo, G Nunez, SM Reglero, V Velasco, T Larsson, S Svensson, R Zdziarski, AA Castro-Tirado, A Attina, P Goria, M Giulianelli, G Cordero, F Rezazad, M Schmidt, M Carli, R Gomez, C Jensen, PL Sarri, G Tiemon, A Orr, A Much, R Kretschmar, P Schnopper, HW TI JEM-X: The X-ray monitor aboard INTEGRAL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation : detectors; X-rays : general AB The JEM-X monitor provides X-ray spectra and imaging with arcminute angular resolution in the 3 to 35 keV band. The good angular resolution and the low energy response of JEM-X plays an important role in the identification of gamma ray sources and in the analysis and scientific interpretation of the combined X-ray and gamma ray data. JEM-X is a coded aperture instrument consisting of two identical, coaligned telescopes. Each of the detectors has a sensitive area of 500 cm(2), and views the sky through its own coded aperture mask. The two coded masks are inverted with respect to each other and provides an angular resolution of 3' across an effective field of view of about 10degrees diameter. C1 Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. Metorex Int Oy, Espoo 02631, Finland. Univ Helsinki, Observ, FIN-00014 Helsinki, Finland. Space Res Ctr, PL-00716 Warsaw, Poland. CNR, Inst Astrofis, I-00133 Rome, Italy. ENEA, Frascati UTS Fus, I-00045 Frascati, Italy. IASF Bologna, I-40129 Bologna, Italy. Univ Ferrara, Dipartmento Fis, I-44100 Ferrara, Italy. Univ Valencia, GACE, Valencia 46071, Spain. Stockholm Univ, S-10691 Stockholm, Sweden. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Alenia Spazio, Space Div, I-10146 Turin, Italy. ESOC, D-64293 Darmstadt, Germany. European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. MPI Extraterr Phys, D-85748 Garching, Germany. ISDC, Versoix, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lund, N (reprint author), Danish Space Res Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. RI Chenevez, Jerome/F-5380-2010; OI Costa, Enrico/0000-0003-4925-8523; Feroci, Marco/0000-0002-7617-3421; Castro-Tirado, A. J./0000-0003-2999-3563; Kretschmar, Peter/0000-0001-9840-2048 NR 18 TC 308 Z9 311 U1 0 U2 3 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 2003 VL 411 IS 1 BP L231 EP L238 DI 10.1051/0004-6361:20031358 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800038 ER PT J AU Vilhu, O Hjalmarsdotter, L Zdziarski, AA Paizis, A McCollough, ML Beckmann, V Courvoisier, TJL Ebisawa, K Goldoni, P Hakala, P Hannikainen, D Kretschmar, P Westergaard, NJ AF Vilhu, O Hjalmarsdotter, L Zdziarski, AA Paizis, A McCollough, ML Beckmann, V Courvoisier, TJL Ebisawa, K Goldoni, P Hakala, P Hannikainen, D Kretschmar, P Westergaard, NJ TI First INTEGRAL observations of Cygnus X-3 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : observations; radiation mechanisms : non-thermal; stars : individual : Cyg X-3; X-rays : binaries; X-rays : general; X-rays : stars ID X-RAY; X-1; DISCOVERY; PLASMAS AB We present the first INTEGRAL results on Cyg X-3 from the PV phase observations of the Cygnus region. The source was clearly detected by the JEM-X, ISGRI and SPI. The INTEGRAL observations were supported by simultaneous pointed RXTE observations. Their lightcurves folded over the 4.8 hour binary period are compatible with the mean RXTE/ASM and CGRO/BATSE light curves. We fit our broad-band X-ray/gamma-ray spectra with a physical model, which represents the first such published model for Cyg X-3. The main physical processes in the source are thermal Comptonization and Compton reflection with parameters similar to those found for black-hole binaries at high Eddington rates. C1 INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Univ Helsinki Observ, Helsinki 00014, Finland. Centrum Astron M Kopernika, PL-00716 Warsaw, Poland. CNR, IASF, Sez Milano, I-20133 Milan, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Observ Geneva, CH-1290 Sauverny, Switzerland. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Ctr Etud Saclay, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. RP Vilhu, O (reprint author), INTEGRAL Sci Data Ctr, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. OI Kretschmar, Peter/0000-0001-9840-2048; Paizis, Adamantia/0000-0001-5067-0377 NR 27 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 NOV PY 2003 VL 411 IS 1 BP L405 EP L410 DI 10.1051/0004-6361:20031257 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800066 ER PT J AU Winkler, C Courvoisier, TJL Di Cocco, G Gehrels, N Gimenez, A Grebenev, S Hermsen, W Mas-Hese, JM Lebrun, F Lund, N Palumbo, GGC Paul, J Roques, JP Schnopper, H Schonfelder, V Sunyaev, R Teegarden, B Ubertini, P Vedrenne, G Dean, AJ AF Winkler, C Courvoisier, TJL Di Cocco, G Gehrels, N Gimenez, A Grebenev, S Hermsen, W Mas-Hese, JM Lebrun, F Lund, N Palumbo, GGC Paul, J Roques, JP Schnopper, H Schonfelder, V Sunyaev, R Teegarden, B Ubertini, P Vedrenne, G Dean, AJ TI The INTEGRAL mission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray astronomy; space observatory AB The ESA observatory INTEGRAL (International Gamma-Ray Astrophysics Laboratory) is dedicated to the fine spectroscopy (2.5 keV FWHM @ 1 MeV) and fine imaging (angular resolution: 12 arcmin FWHM) of celestial gamma-ray sources in the energy range 15 keV to 10 MeV with concurrent source monitoring in the X-ray (3-35 keV) and optical (V-band, 550 nm) energy ranges. INTEGRAL carries two main gamma-ray instruments, the spectrometer SPI (Vedrenne et al. 2003)-optimized for the high-resolution gamma-ray line spectroscopy (20 keV-8 MeV), and the imager IBIS (Ubertini et al. 2003)-optimized for high-angular resolution imaging (15 keV-10 MeV). Two monitors, JEM-X (Lund et al. 2003) in the (3-35) keV X-ray band, and OMC (Mas-Hesse et al. 2003) in optical Johnson V-band complement the payload. The ground segment includes the Mission Operations Centre at ESOC, ESA and NASA ground stations, the Science Operations Centre at ESTEC and the Science Data Centre near Geneva. INTEGRAL was launched on 17 October 2002. The observing programme is well underway and sky exposure (until June 2003) reaches similar to1800 ks in the Galactic plane. The prospects are excellent for the scientific community to observe the high energy sky using state-of-the-art gamma-ray imaging and spectroscopy. This paper presents a high-level overview of INTEGRAL. C1 ESA, Estec, Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. INTEGRAL, Sci Data Ctr, CH-1290 Versoix, Switzerland. CNR, IASF, Sez Bologna, I-40129 Bologna, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Space Res Inst, Moscow 117810, Russia. SRON Utrecht, NL-3584 CA Utrecht, Netherlands. LAEFF INTA, Madrid 28080, Spain. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. DSRI, DK-2100 Copenhagen OE, Denmark. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Ctr Etud Spatiale Rayonnements, F-31029 Toulouse, France. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. CNR, IASF, I-00133 Rome, Italy. Max Planck Inst Astrophys, D-85741 Garching, Germany. Univ Southampton, Dept Phys, Astron Grp, Southampton SO17 1BJ, Hants, England. CSIC, INTA, Ctr Astrobiol, Torrejon De Ardoz 28850, Spain. Observ Geneva, CH-1290 Sauverny, Switzerland. RP Winkler, C (reprint author), ESA, Estec, Res & Sci Support Dept, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM Christoph.Winkler@rssd.esa.int RI Gehrels, Neil/D-2971-2012; Mas-Hesse, J. Miguel /K-6805-2014 OI Mas-Hesse, J. Miguel /0000-0002-8823-9723 NR 13 TC 668 Z9 675 U1 2 U2 11 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 NOV PY 2003 VL 411 IS 1 SI SI BP L1 EP L6 DI 10.1051/0004-6361:20031288 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737JZ UT WOS:000186227800002 ER PT J AU Walsh, AJ Macdonald, GH Alvey, NDS Burton, MG Lee, JK AF Walsh, AJ Macdonald, GH Alvey, NDS Burton, MG Lee, JK TI Observations of warm dust near methanol masers SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; ISM : dust, extinction; submillimeter; infrared : ISM ID H-II REGIONS; ULTRACOMPACT HII-REGIONS; MASSIVE STAR-FORMATION; 1.3MM CONTINUUM OBSERVATIONS; CLERK-MAXWELL-TELESCOPE; VELOCITY MOLECULAR GAS; IRAS POINT SOURCES; H2O MASERS; HIGH-RESOLUTION; RADIO-CONTINUUM AB Continuum emission at 450 and 850 mum from warm dust has been mapped in the fields of 71 methanol masers. Within these fields lie 30 centimetre-wave radio continuum sources and an additional 13 methanol maser sites. Sub-mm emission is detected at all but one of the maser sites, confirming the association of methanol maser emission with deeply embedded objects. Measured bolometric luminosities confirm that methanol maser emission is an excellent signpost of high-mass star formation. Examples of nearby isolated maserless dust cores may be harbouring massive protostars at an earlier evolutionary stage. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Kent, Dept Elect, Canterbury CT2 7NT, Kent, England. Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. RP Walsh, AJ (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; Burton, Michael/0000-0001-7289-1998 NR 54 TC 61 Z9 61 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 2003 VL 410 IS 2 BP 597 EP 610 DI 10.1051/0004-6361:20031191 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZX UT WOS:000185917300023 ER PT J AU Naef, D Mayor, M Korzennik, SG Queloz, D Udry, S Nisenson, P Noyes, RW Brown, TM Beuzit, JL Perrier, C Sivan, JP AF Naef, D Mayor, M Korzennik, SG Queloz, D Udry, S Nisenson, P Noyes, RW Brown, TM Beuzit, JL Perrier, C Sivan, JP TI The ELODIE survey for northern extra-solar planets - II. A Jovian planet on a long-period orbit around GJ 777A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : radial velocities; stars : individual : GJ 777 A; stars : individual : HD 190360; stars : planetary systems ID STARS; SPECTROGRAPH AB We present radial-velocity measurements obtained with the ELODIE and AFOE spectrographs for GJ777A (HD190360), a metal-rich ([Fe/H] = 0.25) nearby (d = 15.9 pc) star in a stellar binary system. A long-period low radial-velocity amplitude variation is detected revealing the presence of a Jovian planetary companion. Some of the orbital elements remain weakly constrained because of the smallness of the signal compared to our instrumental precision. The detailed orbital shape is therefore not well established. We present our best fitted orbital solution: an eccentric (e = 0.48) 10.7-year orbit. The minimum mass of the companion is 1.33 M-Jup. C1 Observ Geneva, CH-1290 Sauverny, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Univ Grenoble 1, Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. Observ Haute Provence, F-04870 St Michel lObservatoire, France. RP Naef, D (reprint author), Observ Geneva, 51 Ch Maillettes, CH-1290 Sauverny, Switzerland. NR 27 TC 32 Z9 32 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 2003 VL 410 IS 3 BP 1051 EP 1054 DI 10.1051/0004-6361:20031341 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 733GH UT WOS:000185991200036 ER PT J AU Ostriker, JP Nagamine, K Cen, R Fukugita, M AF Ostriker, JP Nagamine, K Cen, R Fukugita, M TI The probability distribution function of light in the universe: Results from hydrodynamic simulations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation; large-scale structure of universe; methods : numerical ID LOGNORMAL MODEL; REDSHIFT SURVEY; ONE-POINT; MATTER; EVOLUTION; VOIDS; GALAXIES; FLUCTUATIONS AB While second and higher order correlations of the light distribution have received extensive study, the lowest order probability distribution function (PDF) - the probability that a unit volume of space will emit a given amount of light - has received very little attention. We estimate this function with the aid of hydrodynamic simulations of the LambdaCDM model, finding it significantly different from the mass density PDF, and not simply related to it by linear bias or any of the other prescriptions commonly adopted. If the optical light PDF is, in reality, similar to what we find in the simulations, then some measures of Omega(m) based on the mass-to-light ratio and the cosmic virial theorem will have significantly underestimated Omega(m). Basically, the problem is one of selection bias, with galaxy-forming regions being unrepresentative of the dark matter distribution in a way not described by linear bias. Knowledge of the optical PDF and the plausible assumption of a lognormal distribution for the matter PDF will allow one to correct for these selection biases. We find that this correction ( which amounts to 20% - 30%) brings the values of Omega(m) estimated by using the mass-to-light ratio and the cosmic virial theorem to the range Omega(m) = 0.2 0.3, in better agreement with the Wilkinson Microwave Anisotropy Probe result than the uncorrected estimates. In addition, the relation between mass and light PDFs gives us insight concerning the nature of the void phenomenon. In particular, our simulation indicates that 20% of mass is distributed in voids, which occupy 85% of volume in the universe. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Dept Astrophys, Princeton, NJ 08544 USA. Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. RP Ostriker, JP (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. NR 30 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 NOV 1 PY 2003 VL 597 IS 1 BP 1 EP 8 DI 10.1086/378320 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800001 ER PT J AU Taylor, GB Peck, AB AF Taylor, GB Peck, AB TI Identifying compact symmetric objects in the southern sky SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : ISM; galaxies : jets; galaxies : nuclei; radio continuum : galaxies ID EXTRAGALACTIC RADIO-SOURCES; ACTIVE GALACTIC NUCLEI; BANK VLBI SURVEY; SAMPLE; YOUNG; JETS AB We present results of multifrequency polarimetric VLBA observations of 20 compact radio sources. The observations represent the northern and southern extensions of a large survey undertaken to identify compact symmetric objects (CSOs) observed in the northern sky. CSOs are young radio galaxies whose jet axes lie close to the plane of the sky and whose appearance is therefore not dominated by relativistic beaming effects. The small linear sizes of CSOs make them valuable for studies of both the evolution of radio galaxies and testing unified schemes for active galactic nuclei. In this paper we report on observations of 20 new CSO candidates discovered in the northern and southern extremities of the VLBA Calibrator Survey. We identify four new CSOs, and discard 12 core-jet sources. The remaining four sources remain candidates pending further investigation. We present continuum images at 5 and 15 GHz and, where relevant, images of the polarized flux density and spectral index distributions for the eight new CSOs and CSO candidates. C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, SAO SMA Project, Hilo, HI 96720 USA. RP Taylor, GB (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA. NR 25 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 157 EP 165 DI 10.1086/378267 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800014 ER PT J AU Pellegrini, S Baldi, A Fabbiano, G Kim, DW AF Pellegrini, S Baldi, A Fabbiano, G Kim, DW TI An XMM-Newton and Chandra investigation of the nuclear accretion in the Sombrero galaxy (NGC 4594) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4594); galaxies : nuclei; X-rays : galaxies; X-rays : ISM ID ACTIVE GALACTIC NUCLEI; ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; X-RAY OBSERVATIONS; SEYFERT 1 GALAXIES; NEARBY GALAXIES; COOLING FLOWS; ENERGY-DISTRIBUTIONS; ELLIPTIC GALAXIES AB We present an analysis of the XMM-Newton and Chandra ACIS-S observations of the LINER nucleus of the Sombrero galaxy, and we discuss possible explanations for its very sub-Eddington luminosity by complementing the X-ray results with high angular resolution observations in other bands. The X-ray investigation shows a hard (Gamma = 1.89) and moderately absorbed (N-H = 1.8 x 10(21) cm(-2)) nuclear source of 1x5 x 10(40) ergs s(-1) in the 2 - 10 keV band, surrounded by hot gas at a temperature of similar to0.6 keV. The bolometric nuclear luminosity is at least similar to 200 times lower than expected if mass accreted on the supermassive black hole, which Hubble Space Telescope shows to reside at the center of this galaxy, at the rate predicted by the spherical and adiabatic Bondi accretion theory and with the high radiative efficiency of a standard accretion disk. The low luminosity, coupled to the observed absence of Fe K emission in the nuclear spectrum, indicates that such a disk is not present. This nucleus also differs from bright unobscured active galactic nuclei in the lack of high flux variability and prominent broad Halpha emission. However, it is also too faint for the predictions of simple radiatively inefficient accretion taking place at the Bondi rate; it could instead be too radio bright for radiatively inefficient accretion that includes strong mass outflows or convection. This discrepancy could be solved by the possible presence of nuclear radio jets. An alternative explanation of the low luminosity, in place of radiative inefficiency, could be unsteady accretion. C1 Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pellegrini, S (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy. NR 62 TC 36 Z9 36 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 175 EP 185 DI 10.1086/378235 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800016 ER PT J AU Harvey, DWA Wilner, DJ Myers, PC Tafalla, M AF Harvey, DWA Wilner, DJ Myers, PC Tafalla, M TI Inner structure of starless core L694-2 derived from millimeter-wave interferometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : globules; ISM : individual (L694); radio continuum : ISM; stars : formation ID MOLECULAR CLOUD CORES; YOUNG STELLAR OBJECTS; PROTOSTELLAR COLLAPSE; CONTINUUM EMISSION; INFALL MOTIONS; MODELS; MASS; ACCRETION AB We study the density structure of the candidate contracting starless core L694-2 using 1.3 mm dust continuum observations from the IRAM Plateau de Bure Interferometer (PdBI) and the Berkeley-Illinois-Maryland Association (BIMA) array, which probe spatial scales from 10,000 to 500 AU. The long-baseline PdBI observations detect no emission from the core and limit the maximum contamination from a compact component: F-c < 2.7 mJy. The flux limit corresponds to a very small disk mass, M-disk &LSIM; 5 x 10(-4) M. (60 K/T-disk), and bolsters the "starless'' interpretation of the L694-2 core. The shorter baseline BIMA data are compared to a series of density models using a physically motivated temperature distribution with a central minimum. This analysis provides clear evidence for a turnover from the steep density pro. le observed in the outer regions in dust extinction to substantially more shallow behavior in the inner regions (< 7500 AU). The best-fit Bonnor-Ebert, Plummer-like, broken power law, and end-on cylinder models produce very similar flattened profiles and cannot be distinguished. We quantify the sensitivity of the inferred structure to various uncertainties, including the temperature distribution, the accuracy of the central position, and the presence of a weak, unresolved central component. The largest uncertainty comes from the temperature assumption; an isothermal model modifies the best-fit parameters by similar to2 sigma, with the inferred density profiles more shallow. Dust emission and extinction profiles are reproduced by an embedded isothermal cylinder with scale height H = 13."5 inclined at a small angle to the line of sight. The turnover observed in the L694-2 density distribution suggests that pressure forces still support the core and that it has not fully relaxed, as in the inside-out collapse model, despite the extended inward motions inferred from molecular line observations by Lee, Myers, & Tafalla. In the context of the cylindrical density model, these inward motions may represent the contraction of a prolate core along its major axis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Astron Nacl, E-28014 Madrid, Spain. RP Harvey, DWA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 424 EP 433 DI 10.1086/378237 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800037 ER PT J AU Wilson, TL Boboltz, DA Gaume, RA Megeath, ST AF Wilson, TL Boboltz, DA Gaume, RA Megeath, ST TI High-resolution continuum imaging at 1.3 and 0.7 centimeters of the W3IRS 5 region SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (W3); radio continuum : ISM; stars : formation ID ULTRACOMPACT HII-REGIONS; THERMAL RADIO JET; H2O MASER SOURCE; PROPER MOTIONS; WATER MASERS; W3 IRS-5; GHZ; CONDENSATIONS; KINEMATICS; RADIATION AB High-resolution images of the hypercompact H II (HC H II) regions in W3 IRS 5 taken with the Very Large Array (VLA) at 1.3 and 0.7 cm are presented. Four HC H II regions were detected with sufficient signal-to-noise ratios to allow the determination of relevant parameters, such as source position, size, and flux density. The sources are slightly extended in our similar to0."2 beams; the deconvolved radii are less than 240 AU. A comparison of our data with VLA images taken at epoch 1989.1 shows proper motions for sources IRS 5a and IRS 5f. Between 1989.1 and 2002.5, we find a proper motion of 210 mas at a position angle of 12degrees for IRS 5f and a proper motion of 190 mas at a position angle of 50degrees for IRS 5a. At the assumed distance to W3 IRS 5, 1.83 +/- 0.14 kpc, these offsets translate to proper motions of similar to135 and similar to122 km s(-1), respectively. These sources are either shock-ionized gas in an outflow or ionized gas ejected from high-mass stars. We find no change in the positions of IRS 5d1/d2 and IRS 5b, and we show through a comparison with archival NICMOS 2.2 mum images that these two radio sources coincide with the infrared double constituting W3 IRS 5. These sources contain B or perhaps O stars. The flux densities of the four sources have changed compared to the epoch 1989.1 results. In our epoch 2002.5 data, none of the spectral indices obtained from flux densities at 1.3 and 0.7 cm are consistent with optically thin free-free emission; IRS 5d1/d2 shows the largest increase in flux density from 1.3 to 0.7 cm. This may be an indication of free-free optical depth within an ionized wind, a photoevaporating disk, or an accretion flow. It is less likely that this increase is caused by dust emission at 0.7 cm. C1 Max Planck Inst Radioastron, D-53010 Bonn, Germany. USN Observ, Washington, DC 20392 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilson, TL (reprint author), Max Planck Inst Radioastron, Postfach 2024, D-53010 Bonn, Germany. NR 34 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 NOV 1 PY 2003 VL 597 IS 1 BP 434 EP 442 DI 10.1086/378233 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800038 ER PT J AU Butt, YM Benaglia, P Combi, JA Corcoran, M Dame, TM Drake, J Bernado, MK Milne, P Miniati, F Pohl, M Reimer, O Romero, GE Rupen, M AF Butt, YM Benaglia, P Combi, JA Corcoran, M Dame, TM Drake, J Bernado, MK Milne, P Miniati, F Pohl, M Reimer, O Romero, GE Rupen, M TI Chandra/Very Large Array follow-up of TeV J2032+4131, the only unidentified TeV gamma-ray source SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations ID STARBURST GALAXY NGC-253; COSMIC-RAYS; CYGNUS OB2; SUPERNOVA-REMNANTS; PARTICLE-ACCELERATION; STELLAR WINDS; SHOCK ACCELERATION; GALACTIC PLANE; MASSIVE STARS; MILKY-WAY AB The High Energy Gamma Ray Astronomy (HEGRA) Cerenkov telescope array group recently reported a steady and extended unidentified TeV gamma-ray source lying at the outskirts of Cygnus OB2. This is the most massive stellar association known in the Galaxy, estimated to contain similar to 2600 OB-type members alone. It has been previously argued that the large-scale shocks and turbulence induced by the multiple interacting supersonic winds from the many young stars in such associations may play a role in accelerating Galactic cosmic rays. Indeed, Cyg OB2 also coincides with the nonvariable MeV - GeV range unidentified EGRET source, 3EG 2033+ 4118. We report on the near-simultaneous follow-up observations of the extended TeV source region with the Chandra X-Ray Observatory and the Very Large Array radio telescope, obtained in order to explore this possibility. Analysis of the CO, H I, and IRAS 100 mum emissions shows that the TeV source region coincides with an outlying subgroup of powerful OB stars that have evacuated or destroyed much of the ambient atomic, molecular, and dust material and that may be related to the very high energy emissions. An interesting supernova-remnant - like structure is also revealed near the TeV source region in the CO, H I, and radio emission maps. Applying a numerical simulation that accurately tracks the radio to gamma-ray emission from primary hadrons as well as primary and secondary e(+/-), we find that the broadband spectrum of the TeV source region favors a predominantly nucleonic - rather than electronic - origin for the high-energy flux, although deeper X-ray and radio observations will help confirm this. A very reasonable, similar to 0.1%, conversion efficiency of Cyg OB2' s extreme stellar wind mechanical luminosity to nucleonic acceleration to similar to PeV (10(15) eV) energies is sufficient to explain the multifrequency emissions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Argentino Radioastron, RA-1894 Buenos Aires, DF, Argentina. Univ Space Res Assoc, Seabrook, MD 20706 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. Ruhr Univ Bochum, Inst Theoret Phys, D-44780 Bochum, Germany. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Butt, YM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Reimer, Olaf/A-3117-2013 OI Reimer, Olaf/0000-0001-6953-1385 NR 75 TC 55 Z9 55 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2003 VL 597 IS 1 BP 494 EP 512 DI 10.1086/378121 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736KW UT WOS:000186170800044 ER PT J AU Diego, JM Mazzotta, P Silk, J AF Diego, JM Mazzotta, P Silk, J TI Kinetic Sunyaev-Zel'dovich effect and cosmic microwave background polarization from subsonic bulk motions of dense gas clouds in galaxy cluster cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; intergalactic medium; submillimeter; X-rays : galaxies : clusters ID PECULIAR VELOCITIES; CHANDRA OBSERVATION; QUADRUPOLE; FLOWS AB Recent Chandra observations have revealed the presence of cold fronts in many clusters of galaxies. The cold fronts are believed to be produced by the bulk motions of massive, dense, cold gas clouds with respect to the hotter, more rarefied ambient gas at velocities that can be as high as the speed of sound. This phenomenon may produce a significant contamination of both the kinetic Sunyaev-Zel'dovich (SZ) effect and the cosmic microwave background (CMB) polarization pattern observed in the direction of a cluster. We estimate the contributions to the kinetic SZ effect and to the CMB polarization toward galaxy clusters produced by the bulk motions of the gas in the inner parts of galaxy clusters. The observed cold fronts probe the absolute velocities of the gas motion, while the induced polarization and the kinetic SZ effect probe the transverse and the radial components, respectively. We show that these signals may be easily detected with sensitive future experiments, opening an exciting new window for studies of galaxy cluster internal dynamics and eventually facilitating reconstruction of the intrinsic cluster polarization of the CMB and the associated measure of the local CMB quadrupole. C1 Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England. Univ Durham, Dept Phys, Durham DH1 3LE, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Diego, JM (reprint author), Univ Oxford, Dept Phys Astrophys, Denys Wilkinson Bldg,1 Keble Rd, Oxford OX1 3RH, England. RI Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; silk, joe/0000-0002-1566-8148 NR 25 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 NOV 1 PY 2003 VL 597 IS 1 BP L1 EP L4 DI 10.1086/379638 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736LF UT WOS:000186171700001 ER PT J AU Gioia, IM Henry, JP Mullis, CR Bohringer, H Briel, UG Voges, W Huchra, JP AF Gioia, IM Henry, JP Mullis, CR Bohringer, H Briel, UG Voges, W Huchra, JP TI The ROSAT North Ecliptic Pole survey: The optical identifications SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE BL Lacertae objects : general; catalogs; galaxies : clusters : general; surveys; X-rays : general; X-rays : stars ID ALL-SKY SURVEY; MEDIUM-SENSITIVITY SURVEY; X-RAY DATA; BRIGHTEST CLUSTER SAMPLE; ACTIVE GALACTIC NUCLEI; RADIO-LOUD QUASARS; SOURCE CATALOG; HIGH-REDSHIFT; GALAXY CLUSTERS; STANDARD STARS AB The X-ray data around the North Ecliptic Pole (NEP) of the ROSAT All Sky Survey have been used to construct a contiguous area survey consisting of a sample of 445 individual X-ray sources above a flux of similar to2 x 10(-14) ergs cm(-2) s(-1) in the 0.5-2.0 keV energy band. The NEP survey is centered at alpha(2000) = 18(h)00(m), delta(2000) = +66degrees33' and covers a region of 80.7 deg(2) at a moderate Galactic latitude of b = 29.degrees8. Hence, the NEP survey is as deep and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. We have identified 99.6% of the sources and determined redshifts for the extragalactic objects. In this paper we present the optical identifications of the NEP catalog of X-ray sources including basic X-ray data and properties of the sources. We also describe with some detail the optical identification procedure. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGNs) (similar to49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (similar to34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. C1 CNR, Ist Radioastron, I-40129 Bologna, Italy. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. European So Observ, D-85740 Garching, Germany. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gioia, IM (reprint author), CNR, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. RI Gioia, Isabella/B-6982-2012 OI Gioia, Isabella/0000-0003-3127-498X NR 84 TC 52 Z9 52 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2003 VL 149 IS 1 BP 29 EP 51 DI 10.1086/378229 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736LL UT WOS:000186172200002 ER PT J AU Krupnick, GA Kress, WJ AF Krupnick, GA Kress, WJ TI Hotspots and ecoregions: a test of conservation priorities using taxonomic data SO BIODIVERSITY AND CONSERVATION LA English DT Article DE biodiversity; ecoregions; endemism; hotspots; Indo-Pacific mapping; museum collections; plants ID BLUME EUPHORBIACEAE; REVISION; BIODIVERSITY; ERICACEAE; MALAYSIA; PHYLOGENY; CLEISTANTHUS; DIVERSITY; RICHNESS; PATTERNS AB The loss of biodiversity is now recognized as a global problem of significant magnitude [Wilson (2000) Science 289: 2279]. Conservation efforts focus on measuring species diversity and distribution, assessing biodiversity threats, and managing habitats to maintain that diversity. The accuracy of measuring species diversity depends on the quality and scale of the data. Recently indirect estimates of diversity based on the skilled opinions of international taxonomic authorities were used to define 25 global conservation hotspots [Myers et al. (2000) Nature 403: 853-858] and 871 ecoregions [Olson et al. (2001) Bioscience 51: 933-938]. These data, originating from first-hand fieldwork and museum study, are readily available, but not necessarily repeatable nor testable. If this type of information prevails for conservation purposes, it is critical that we test the quality of this information with verifiable data at finer scales (e. g., regional inventories, specimen records, and accumulated distribution data). Here we perform such a test for the hotspots and ecoregions found in the Indo-Pacific by comparing the estimates of the expert scientists with authenticated published diversity data on flowering plants. We found a high correlation between our counts of species richness and endemism with the experts' estimates, but surprisingly found less congruity among the seven families examined. A revised list of conservation priority regions based on our plant data is provided. C1 US Natl Herbarium Bot, MRC 166, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Krupnick, GA (reprint author), US Natl Herbarium Bot, MRC 166, Natl Museum Nat Hist, Smithsonian Inst, POB 37012, Washington, DC 20013 USA. OI Krupnick, Gary/0000-0002-1357-4826 NR 81 TC 24 Z9 26 U1 0 U2 14 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD NOV PY 2003 VL 12 IS 11 BP 2237 EP 2253 DI 10.1023/A:1024582529645 PG 17 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 696TM UT WOS:000183903600006 ER PT J AU Penfold, LM Jost, L Evenson, DP Wildt, DE AF Penfold, LM Jost, L Evenson, DP Wildt, DE TI Normospermic versus teratospermic domestic cat sperm chromatin integrity evaluated by flow cytometry and intracytoplasmic sperm injection SO BIOLOGY OF REPRODUCTION LA English DT Article DE assisted reproductive technology; gamete biology; in vitro fertilization; sperm ID IN-VITRO FERTILIZATION; ZONA-PELLUCIDA; ACROSOME REACTION; STRUCTURE ASSAY; METHYL METHANESULFONATE; REDUCED FERTILIZATION; STRICT CRITERIA; SWIM-UP; SPERMATOZOA; OOCYTES AB Teratospermia (>60% of morphologically abnormal spermatozoa) is well documented in felids. Even morphologically normal spermatozoa from teratospermic ejaculates have reduced ability to undergo tyrosine phosphorylation, acrosome react, and bind and penetrate oocytes compared with normospermic (<40% abnormal spermatozoa) counterparts. However, it is unknown whether fertilization deficiencies originate at a nuclear level. This study examined whether fertilization failure also was attributable to abnormal sperm chromatin, using the sperm chromatin structure assay (SCSA), in vitro fertilization (IVF), and intracytoplasmic sperm injection (ICSI). Aliquots of unprocessed and swim-up-processed (to isolate morphologically normal spermatozoa) spermatozoa from teratospermic and normospermic domestic cats were analyzed by the flow cytometric SCSA. Swim-up-processed sperm were incubated with in vivo-matured oocytes or used for ICSI. Teratospermic ejaculates expressed more (P < 0.05) chromatin heterogeneity (abnormal chromatin structure) than their normospermic counterparts, both in unprocessed and swim-up-processed samples. Fertilization success in vitro was higher (P < 0.05) from normo- compared with teratospermic inseminates. Similar (P > 0.05) proportions of oocytes fertilized after ICSI using spermatozoa from normo- and teratospermic cats. Results reveal that teratospermia in the cat is expressed at the nuclear level as increased sperm chromatin heterogeneity, but ICSI showed that this does not apparently affect fertilization rates if the zona pellucida and oolemma can be bypassed. C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. S Dakota State Univ, Dept Chem & Biochem, Brookings, SD 57007 USA. RP Penfold, LM (reprint author), White Oak Conservat Ctr, 2823 Owens Rd, Yulee, FL 32097 USA. EM Lindap@wogilman.com FU NICHD NIH HHS [R01 HD 23853] NR 45 TC 28 Z9 29 U1 1 U2 3 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD NOV PY 2003 VL 69 IS 5 BP 1730 EP 1735 DI 10.1095/biolreprod.103.016089 PG 6 WC Reproductive Biology SC Reproductive Biology GA 736AK UT WOS:000186147700036 PM 12890738 ER PT J AU Wikelski, M Hau, M Robinson, WD Wingfield, JC AF Wikelski, M Hau, M Robinson, WD Wingfield, JC TI Reproductive seasonality of seven neotropical passerine species SO CONDOR LA English DT Article DE breeding season; gonad cycles; hormones; Panama; rainforest; seasonality; tropical ID BROWED SPARROW WEAVER; CENTRAL PANAMA; TERRITORIAL AGGRESSION; PLOCEPASSER-MAHALI; FOREST BIRD; OPPORTUNISTIC BREEDER; PLASMA TESTOSTERONE; LOXIA-CURVIROSTRA; SEXUAL SELECTION; HORMONAL-CONTROL AB We investigated gonad sizes, nesting patterns, and plasma hormone concentrations of seven Neotropical passerine species in a lowland tropical rainforest (Panama) at 9degreesN latitude over at least one annual cycle. All species had entirely regressed gonads for several months of the year (October to January), coinciding with the end of heavy rainfall. Gonadal recrudescence started in the dry season between January and March. Nesting began earlier (March) for open-habitat species than for forest-interior species (April), and lasted until August or December, respectively. Species differed widely in maximal relative testes sizes and reproductive hormone concentrations, but both measures were lower than in most temperate-zone species. Although we cannot provide a phylogenetically controlled comparison, polygynous and group-living species appeared to have larger testes than monogamous species, possibly indicating sperm competition. Testosterone concentrations were highest in polygynous species, intermediate in socially monogamous species, and lowest in a group-living species, indicating that testosterone is more influenced by social systems than by gonad cycles. Tropical birds may generally maintain low testosterone concentrations and relatively small gonads to decrease overall energy expenditure compared to temperate-zone relatives. C1 Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. Smithsonian Trop Res Inst, Balboa, Panama. Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. Univ Washington, Dept Zool, Seattle, WA 98195 USA. RP Wikelski, M (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, Guyot Hall 303, Princeton, NJ 08544 USA. NR 71 TC 69 Z9 70 U1 1 U2 28 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD NOV PY 2003 VL 105 IS 4 BP 683 EP 695 DI 10.1650/7251 PG 13 WC Ornithology SC Zoology GA 741TX UT WOS:000186477400006 ER PT J AU Ferrer, A Gilbert, GS AF Ferrer, A Gilbert, GS TI Effect of tree host species on fungal community composition in a tropical rain forest in Panama SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE fungal diversity; host preference; wood-inhabiting fungi ID WOOD-INHABITING FUNGI; DECAY; SPECIFICITY AB To determine whether host species influence the composition of fungal communities, the ascomycetes and basidiomycetes present on three tree species (Prioria copaifera (Fabaceae), Quararibea asterolepis (Bombacaceae), and Trichilia tuberculata (Meliaceae)) were sampled on the 50-ha Forest Dynamics Project plot in lowland moist tropical forest on Barro Colorado Island, Panama. The most abundant fungal morphotypes of both ascomycetes and basidiomycetes were generalists found on all three hosts, but detrended correspondence analysis revealed distinct differences in fungal community composition among host trees. These differences among hosts were constant across census years. Randomization tests revealed that there were significantly fewer host-generalist fungi than expected for ascomycetes but not for basidiomycetes. These results indicate that host composition plays a role in structuring both ascomycete and basidiomycete fungal communities, but that the most successful fungal morphotypes are capable of colonizing multiple host species. C1 SUNY Syracuse, Coll Environm Sci & Forestry, Syracuse, NY 13210 USA. Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Ferrer, A (reprint author), SUNY Syracuse, Coll Environm Sci & Forestry, 1 Forestry Dr, Syracuse, NY 13210 USA. NR 37 TC 23 Z9 27 U1 1 U2 11 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD NOV PY 2003 VL 9 IS 6 BP 455 EP 468 DI 10.1046/j.1472-4642.2003.00039.x PG 14 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 735MH UT WOS:000186118800004 ER PT J AU Cudnik, BM Dunham, DW Palmer, DM Cook, A Venable, R Gural, PS AF Cudnik, BM Dunham, DW Palmer, DM Cook, A Venable, R Gural, PS TI Ground-based observations of lunar meteoritic phenomena SO EARTH MOON AND PLANETS LA English DT Article DE hypervelocity impacts; Leonid meteors; lunar impact phenomena; Moon; transient lunar phenomena ID LEONID IMPACT FLASHES; LARGE METEOROIDS; STREAM; MOON AB The occurrence and visibility of meteoroid impacts on the moon as seen from the earth were little more than speculation prior to November 1999. The best evidence of present-day impact activity came from the seismic experiments left on the Moon during the Apollo era. Past systematic attempts at earth-based observations to document lunar impacts revealed nothing conclusive. However, during the Leonid storms of 1999 and 2001, lunar impact events were for the first time confirmed by multiple independent observers. A total of 15 meteoritic impact flash events have been verified during these storms, with an additional 12 unconfirmed but likely events awaiting confirmation. Estimates of the mass of these meteoroids range from less than one gram for the faintest flashes to more than 10 kg for the brightest observed flash. The fraction of visible light to total energy produced by these events, a quantity known as luminous efficiency, averages about 0.001 for the established events. The confirmation of lunar meteoritic events on the Moon opens a new avenue in lunar and planetary research, one which could help bridge the gap between atmospheric sampling of the smallest components of meteoroid streams and interplanetary debris to the larger scale objects accessible to ground-based telescopes. C1 Prairie View A&M Univ, Dept Phys, Prairie View, TX 77446 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Los Alamos Natl Lab, Los Alamos, NM 87544 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Sci Applicat Int Corp, Chantilly, VA 20151 USA. RP Cudnik, BM (reprint author), Prairie View A&M Univ, Dept Phys, Prairie View, TX 77446 USA. NR 17 TC 4 Z9 4 U1 0 U2 4 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD NOV PY 2003 VL 93 IS 3 BP 145 EP 161 DI 10.1023/B:MOON.0000047475.61749.c1 PG 17 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 869NK UT WOS:000224991100001 ER PT J AU Santiago-Blay, JA AF Santiago-Blay, JA TI Acknowledgments to reviewers of articles published in Entomological News (volume 114) and to volunteers SO ENTOMOLOGICAL NEWS LA English DT Editorial Material C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist MRC121, Washington, DC 20013 USA. RP Santiago-Blay, JA (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist MRC121, POB 37012, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 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 2003 VL 114 IS 5 BP 294 EP 297 PG 4 WC Entomology SC Entomology GA 858MQ UT WOS:000224196300012 ER PT J AU Ryan, MJ Rand, AS AF Ryan, MJ Rand, AS TI Sexual selection in female perceptual space: How female tungara frogs perceive and respond to complex population variation in acoustic mating signals SO EVOLUTION LA English DT Article DE animal communication; mate recognition; perception; Physalaemus pustulosus; sexual selection ID RED JUNGLE FOWL; PHYSALAEMUS-PUSTULOSUS; MATE CHOICE; TREE FROGS; PREFERENCES; CALL; RECOGNITION; CHARACTERS; CUES; DISCRIMINATION AB Female preferences for male mating signals are often evaluated on single parameters in isolation or small suites of characters. Most signals, however, are composites of many individual parameters. In this study we quantified multivariate traits in the advertisement call of the tungara frog, Physalaemus pustulosus. We represented the calls in multidimensional scaling space and chose nine test calls to represent the range of population variation. We then tested females for phonotactic preference between calls in each pair of the nine test calls. We used statistics developed for paired comparisons in such "round robin" competitions to evaluate the null hypothesis of equal attractiveness, and to examine the degree to which females responded to calls as being different from or similar to one another in attractiveness. We then examined the attractiveness of each test call relative to all other test calls as a function of their location in multivariate acoustic space (the acoustic landscape) to visualize sexual selection on calls. Finally, we used methods from cognitive psychology to illustrate the females' perception of call attractiveness in multivariate space, and compared this perceptual landscape to the acoustic landscape of quantitative call variation. We show that correlations between individual call characters are not strong and thus there are few biomechanical constraints on their independent evolution. Most call variables differed among males, and there was high repeatability of call characters within males. Females often discriminated between pairs of calls from the population, and there were significant differences among calls in their attractiveness. Female preferences for calls were not stabilizing. The region of the acoustic landscape that was most attractive to females included the mean call but was not centered around it. The females' perceptual or preference landscape did not correlate with the call's acoustic landscape, and female perception of calls decreased rather than enhanced call differences. C1 Univ Texas, Sect Integrat Biol C0930, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Ryan, MJ (reprint author), Univ Texas, Sect Integrat Biol C0930, Austin, TX 78712 USA. NR 48 TC 89 Z9 89 U1 0 U2 16 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD NOV PY 2003 VL 57 IS 11 BP 2608 EP 2618 DI 10.1111/j.0014-3820.2003.tb01503.x PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 748WZ UT WOS:000186885100015 PM 14686535 ER PT J AU Lagarde, F Bonnet, X Henen, B Nagy, K Corbin, J Lacroix, A Trouve, C AF Lagarde, F Bonnet, X Henen, B Nagy, K Corbin, J Lacroix, A Trouve, C TI Plasma steroid and nutrient levels during the active season in wild Testudo horsfieldi SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Testudo horsfieldi; testosterone; progesterone; calcium; phosphorus; phospholipid; cholesterol; triglyceride; total protein; albumin; reproductive cycle; physiology; breeding season; time constraint ID PSEUDEMYDURA-UMBRINA TESTUDINES; ANNUAL REPRODUCTIVE-CYCLE; FEMALE DESERT TORTOISES; TURTLE CARETTA-CARETTA; COMMON SNAPPING TURTLE; FRESH-WATER TURTLE; STERNOTHERUS-ODORATUS; CHRYSEMYS-PICTA; KINOSTERNON-FLAVESCENS; CHELYDRA-SERPENTINA AB Plasma concentrations of sex steroids (testosterone and progesterone), proteins (total protein and albumin), lipids (phospholipids, cholesterol, and triglycerides), and minerals (calcium and phosphorus) were measured in wild Testudo horSfieldi in Uzbekistan, during the short, 3-month activity period (March-May, 1998). Testosterone concentration in males was highest (52 ng/ml) when they had just emerged from brumation (hibernation) in mid-March, which was also the beginning of the mating period, and fell in April. In females, progesterone peaked in mid-April (at 10 ng/ml),just before ovulation of the first clutches at the end of April and beginning of May. Testosterone levels in females and progesterone levels in males were low (<3 ng/ml) throughout the activity period. In general, the plasma concentrations of proteins, lipids, and phosphorus increased slowly in males, but more rapidly in females, during the activity season. These increases were particularly strong in females in the second half of April, coinciding with the peaks in female hormone levels. The changes in plasma hormones and nutrients reflected the timing of the different behaviours. The four first weeks of above-ground activity (mid-March to mid-April) by males, when they had high testosterone levels, were primarily allocated to fighting other males, courtship, and mating, while females spent much of that time feeding. Thereafter, both sexes concentrated on feeding. Females were probably preparing to ovulate in late-April, when their progesterone levels were highest and when plasma nutrient levels increased considerably. (C) 2003 Elsevier Inc. All rights reserved. C1 CNRS, Ctr Etudes Biol Chize, F-79360 Villiers En Bois, France. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. Univ Western Cape, Dept Zool Biodivers & Conservat Biol, ZA-7535 Bellville, South Africa. Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, Los Angeles, CA 90095 USA. RP Lagarde, F (reprint author), CNRS, Ctr Etudes Biol Chize, F-79360 Villiers En Bois, France. EM lagarde@cebc.cnrs.fr RI Henen, Brian/S-6552-2016 OI Henen, Brian/0000-0003-3412-4944 NR 62 TC 11 Z9 12 U1 2 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD NOV PY 2003 VL 134 IS 2 BP 139 EP 146 DI 10.1016/S0016-6480(03)00245-4 PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 734KC UT WOS:000186053800007 PM 14511984 ER PT J AU Grav, T Holman, MJ Gladman, BJ Aksnes, K AF Grav, T Holman, MJ Gladman, BJ Aksnes, K TI Photometric survey of the irregular satellites SO ICARUS LA English DT Article DE photometry; satellite of Jupiter; satellite of Saturn; satellite of Uranus; surfaces; satellite ID KUIPER-BELT OBJECTS; OUTER JOVIAN-SATELLITES; TRANSNEPTUNIAN OBJECTS; MULTICOLOR PHOTOMETRY; CAPTURE; PHOEBE; URANUS; SPECTROSCOPY; ASTEROIDS; DISCOVERY AB We present BVRI colors of 13 jovian and 8 saturnian irregular satellites obtained with the 2.56 m Nordic Optical Telescope on La Palma, the 6.5 m Magellan Baade Telescope on La Campanas, and the 6.5 m MMT on Mt. Hopkins. The observations were performed from December 2001 to March 2002. The colors of the irregular satellites vary from grey to light red. We have arbitrarily divided the known irregular satellites into two classes based on their colors. One, the grey color class, has similar colors to the C-type asteroids, and the other, the light red color class, has colors similar to P/D-type asteroids. We also find at least one object, the jovian irregular J XXIII Kalyke, that has colors similar to the red colored Centaurs/TNOs, although its classification is insecure. We find that there is a correlation between the physical properties and dynamical properties of the irregular satellites. Most of the dynamical clusters have homogeneous colors, which points to single homogeneous progenitors being cratered or fragmented as the source of each individual cluster. The heterogeneously colored clusters are most easily explained by assuming that there are several dynamical clusters in the area, rather than just one, or that the parent body was a differentiated, heterogeneous body. By analyzing simple cratering/fragmentation scenarios, we show that the heterogeneous colored S IX Phoebe cluster, is most likely two different clusters, a grey colored cluster centered on S IX Phoebe and a light red colored cluster centered on S/2000 S 1. To which of these two clusters the remaining saturnian irregulars with inclinations close to 174degrees belong is not clear from our analysis, but determination of their colors should help constrain this. We also show through analysis of possible fragmentation and dispersion of the six known uranian irregulars that they most likely make up two clusters, one centered on U XVI Caliban and another centered on U XVII Sycorax. We further show that, although the two objects have similar colors, a catastrophic fragmentation event creating one cluster containing both U XVI Caliban and U XVII Sycorax would have involved a progenitor with a diameter of similar to 395 km. While such an event is not impossible it seems rather improbable, and we further show that such an event would leave 5-6 fragments with sizes comparable to or larger than U XVI Caliban. The stable region around Uranus has been extensively searched to limiting magnitudes far beyond that of U XVI Caliban. The fact that only U XVI Caliban, the larger U XVII Sycorax and four much smaller objects have been found leaves us with a distribution not compatible with a catastrophic event with such a large progenitor. The most likely solution is therefore two separate events creating two uranian dynamical clusters. (C) 2003 Elsevier Inc. All rights reserved. C1 Univ Oslo, Inst Theoret Astrophys, N-0359 Oslo, Norway. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Grav, T (reprint author), Univ Oslo, Inst Theoret Astrophys, Postbox 1029 Blindern, N-0359 Oslo, Norway. EM tommy.grav@astro.uio.no NR 61 TC 42 Z9 42 U1 1 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 2003 VL 166 IS 1 BP 33 EP 45 DI 10.1016/j.icarus.2003.07.005 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743TL UT WOS:000186589600003 ER PT J AU Meledin, D Tong, CYE Blundell, R Goltsman, G AF Meledin, D Tong, CYE Blundell, R Goltsman, G TI Measurement of intermediate frequency bandwidth of hot electron bolometer mixers atterahertz frequency range SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE hot-electron bolometer; intermediate frequency bandwidth; submillimeter waves AB We have developed a new experimental setup for measuring the IF bandwidth of superconducting hot electron bolometer mixers. In our measurement system we use a chopped hot filament as a broadband signal source, and can perform a high-speed IF scan with no loss of accuracy when compared to coherent methods. Using this technique we have measured the 3 dB IF bandwidth of hot electron bolometer mixers, designed for THz frequency operation, and made from 3-4 nm thick NbN film deposited on an MgO buffer layer over crystalline quartz. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow State Pedag Univ, Moscow 119891, Russia. RP Meledin, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Tong, Edward/0000-0002-7736-4203 NR 9 TC 2 Z9 2 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD NOV PY 2003 VL 13 IS 11 BP 493 EP 495 DI 10.1109/LMWC.2003.817133 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 740KQ UT WOS:000186401900013 ER PT J AU Fernandez-Marin, H Zimmermann, JK Wcislo, WT AF Fernandez-Marin, H Zimmermann, JK Wcislo, WT TI Nest-founding in Acromyrmex octospinosus (Hymenoptera, Formicidae, Attini): demography and putative prophylactic behaviors SO INSECTES SOCIAUX LA English DT Article DE Attini; metapleural gland; leg grooming ID FUNGUS-GROWING ANTS; LEAF-CUTTING ANTS; METAPLEURAL GLANDS; ATTA-TEXANA; SYMBIOSIS; BACTERIA; SECRETION AB Foundresses of the leaf-cutting ant Acromyrmex octospinosus in central Panamaa forage for leaves as garden substrate (semi-claustral foundation). The fungal pellet and substrate usually are attached to rootlets, which are used as a platform for the garden. This arrangement keeps the garden suspended away from the earthen chamber of the underground nest during early colony growth, and we hypothesize that it serves to minimize contact between the garden and contaminants. A. octospinosus foundresses produce from 3 to 7 workers in 2.7 months after founding the nest, but workers do not forage for substrate at this time. Incipient nests died or were abandoned at a monthly rate of ca. 50%. We show that ants routinely clean their legs before manipulating the garden substrate. We also describe how foundresses use their fore-legs to rub the surface of the metapleural gland (MPG), and they then use typical grooming behaviors to pass the forelegs through the mouthparts, after which the ant then licks the garden substrate. Similarly, ants apparently use their mouths to transfer fecal droplets to their legs. We briefly discuss the functional significance of these grooming behaviors, and hypothesize that they are prophylactic behaviors that may help the foundress maintain a hygienic garden. C1 Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. Inst Trop Ecosyst Studies, San Juan, PR 00936 USA. Smithsonian Trop Res Inst, Ancon, Panama. RP Fernandez-Marin, H (reprint author), Univ Puerto Rico, Dept Biol, POB 23360, San Juan, PR 00931 USA. NR 31 TC 26 Z9 27 U1 1 U2 16 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PD NOV PY 2003 VL 50 IS 4 BP 304 EP 308 DI 10.1007/s00040-003-0687-z PG 5 WC Entomology SC Entomology GA 752UL UT WOS:000187185500002 ER PT J AU Kornicker, LS AF Kornicker, LS TI Morphology and musculature of the fifth and sixth limbs of Halocyprida (Ostracoda : Myodocopa) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article ID SPELAEOECIA-BERMUDENSIS; CAVE AB Intrinsic musculature of the fifth and sixth limbs of selected halocyprid ostracodes is used to identify the basis and, also, bristles that could be interpreted to represent an exopod. It is concluded that, in general, species of the Halocyprida bear bristles that could be interpreted to represent an exopod. Taxa that bear an unsegmented exopod lobe on the sixth limb are restricted to the deep sea and anchialine caves, and this suggests their antiquity. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, POB 37012, Washington, DC 20013 USA. NR 25 TC 6 Z9 6 U1 0 U2 0 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 2003 VL 23 IS 4 BP 765 EP 776 DI 10.1651/C-2406 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 740YM UT WOS:000186430900003 ER PT J AU Pawlowski, J Holzmann, M Fahrni, J Richardson, SL AF Pawlowski, J Holzmann, M Fahrni, J Richardson, SL TI Small subunit ribosomal DNA suggests that the xenophyophorean Syringammina corbicula is a foraminiferan SO JOURNAL OF EUKARYOTIC MICROBIOLOGY LA English DT Article DE deep-sea; foraminifera; phylogeny; ribosomal RNA; protista xenophyophorea ID MOLECULAR PHYLOGENY; PROTISTA; ECOLOGY; SEA; CLASSIFICATION; MORPHOLOGY; SEQUENCES; CERCOZOA; SAMPLES; ORIGIN AB Xenophyophorea are giant deep-sea rhizopodial protists of enigmatic origins. Although species were described as Foraminifera or sponges in the early literature, the xenophyophoreans are currently classified either as a class of Rhizopoda or an independent phylum. To establish the phylogenetic position of Xenophyophorea, we analysed the small subunit (SSU) rRNA gene sequence of Syringammina corbicula Richardson, a newly described xenophyophorean species from the Cape Verde Plateau. The SSUrDNA analyses showed that S. corbicula is closely related to Rhizammina algaeformis, a tubular deep-sea foraminiferan. Both species branch within a group of monothalamous (single-chambered) Foraminifera, which include also such agglutinated genera as Toxisarcon, Rhabdammina, and Saccammina, and the organic-walled genera Gloiogullmia and Cylindrogullmia. Our results are congruent with observations of similar cytoplasmic organisation in Rhizammina and Syringammina. Thus, the Xenophyophorea appear to be a highly specialised group of deep-sea Foraminifera. C1 Univ Geneva, Dept Zool & Anim Biol, CH-1211 Geneva 4, Switzerland. Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Pawlowski, J (reprint author), Univ Geneva, Dept Zool & Anim Biol, CH-1211 Geneva 4, Switzerland. EM jan.pawlowski@zoo.unige.ch NR 35 TC 25 Z9 30 U1 0 U2 3 PU SOC PROTOZOOLOGISTS PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 1066-5234 J9 J EUKARYOT MICROBIOL JI J. Eukaryot. Microbiol. PD NOV-DEC PY 2003 VL 50 IS 6 BP 483 EP 487 DI 10.1111/j.1550-7408.2003.tb00275.x PG 5 WC Microbiology SC Microbiology GA 736QP UT WOS:000186184900013 PM 14733441 ER PT J AU Viranta, S AF Viranta, S TI Geographic and temporal ranges of Middle and Late Miocene carnivores SO JOURNAL OF MAMMALOGY LA English DT Article DE carnivora; distribution; ecomorphology; extinction risk; longevity; Miocene ID COMMUNITY STRUCTURE; LOWER PLEISTOCENE; DIVERSITY; PREDATORS; EVOLUTION; TURNOVER; PATTERNS; MAMMALIA; CANIDS; SIZE AB Carnivores are ecologically diverse mammals. Dietary adaptations vary from strict herbivory to pure carnivory. These adaptations have evolved independently several times within families, so evolution within the order is iterative. I used 2 databases to examine whether ecological adaptations have an effect on longevity or spatial distributions of fossil carnivores. Miocene hypercarnivorous species had, on average, the widest spatial distributions. Their temporal distributions were not significantly longer than those of other carnivores. Body size also had a significant interaction with maximum spatial distribution. Large-bodied carnivores, regardless of feeding adaptations, had larger geographical ranges, but did not have greater longevity. However, when all the data were pooled, temporal distribution had a significant correlation with spatial distribution. The position of hypercarnivores at the top of the food chain and their specialized adaptations for meat eating probably increased their extinction risk to the same level of more narrowly distributed, less specialized carnivores. C1 Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA. Smithsonian Inst, Washington, DC 20013 USA. RP Viranta, S (reprint author), Howard Univ, Coll Med, Dept Anat, 520 W St NW, Washington, DC 20059 USA. EM sviranta@howard.edu RI Viranta, Suvi/B-9026-2015 OI Viranta, Suvi/0000-0003-4105-530X NR 51 TC 8 Z9 8 U1 0 U2 1 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 2003 VL 84 IS 4 BP 1267 EP 1278 DI 10.1644/BJK-035 PG 12 WC Zoology SC Zoology GA 749JP UT WOS:000186916800011 ER PT J AU Rodriguez, N Vasquez, Y Hussein, AA Coley, PD Solis, PN Gupta, MP AF Rodriguez, N Vasquez, Y Hussein, AA Coley, PD Solis, PN Gupta, MP TI Cytotoxic cucurbitacin constituents from Sloanea zuliaensis SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID TRADITIONAL MEDICINE AB A new cucurbitacin D analogue, 2-deoxycucurbitacin D (1), as well as cucurbitacin D (2) and 25-acetylcucurbitacin F (3) were isolated from Sloanea zuliaensis. Compound 1 was found only in the young leaves of the plant and not in the mature leaves, and its structure was established using spectroscopic means. Compounds 1-3 demonstrated potent cytotoxic activity against breast (MCF-7), lung (H-460), and central nervous system (SF-268) human cancer cell lines. C1 Univ Panama, Ctr Invest Farmacognost Flora Panamena, Fac Farm, Estafeta Univ, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Gupta, MP (reprint author), Univ Panama, Ctr Invest Farmacognost Flora Panamena, Fac Farm, Estafeta Univ, Apartado 10767, Panama City, Panama. EM cytedqff@ancon.up.ac.pa OI Gupta, Mahabir/0000-0002-9302-7864; Hussein, Ahmed/0000-0002-3877-9959 FU FIC NIH HHS [1 U01-TW01021-01] NR 11 TC 13 Z9 13 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD NOV PY 2003 VL 66 IS 11 BP 1515 EP 1516 DI 10.1021/np0303106 PG 2 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 749GW UT WOS:000186912400024 PM 14640532 ER PT J AU Aguilera, O De Aguilera, DR AF Aguilera, O De Aguilera, DR TI Two new otolith-based sciaenid species of the genus Plagioscion from South American Neogene marine sediments SO JOURNAL OF PALEONTOLOGY LA English DT Article AB Two new Neogene South American croakers of the genus Plagioscion (Perciformes, Sciaenidae) from marine sediments, Plagioscion marinus and Plagioscion urumacoensis, are described. These are otoliths from the lower Miocene Castillo, Cantaure and upper Miocene Urumaco Formations of the Neogene Venezuelan basin, respectively. An additional undetermined fossil species of Plagioscion was also collected from the upper Miocene to lower Pliocene Cubagua Formation. Using the function total fish length = 13.7187 + 50.8399 * Ln otolith size, the total length of P. marinus n. sp. is inferred to be from 6.05 to 38.1 cm, and for the specimens of P. urumacoensis n. sp. it is 63.3 cm. The length distribution of the fossil species overlaps the length distribution of the living freshwater species. C1 Univ Nacl Expt Francisco de Miranda, Ctr Invest Ciencias Basicas, Coro 4101, Estado Falcon, Venezuela. Smithsonian Trop Res Inst, Balboa, Panama. RP Aguilera, O (reprint author), Univ Nacl Expt Francisco de Miranda, Ctr Invest Ciencias Basicas, Complejo Docente Perozos,Carretera Variente Sur, Coro 4101, Estado Falcon, Venezuela. NR 29 TC 9 Z9 10 U1 0 U2 2 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD NOV PY 2003 VL 77 IS 6 BP 1133 EP 1138 DI 10.1666/0022-3360(2003)077<1133:TNOSSO>2.0.CO;2 PG 6 WC Paleontology SC Paleontology GA 744PN UT WOS:000186641000009 ER PT J AU Rothman, LS Chance, K Goldman, A AF Rothman, LS Chance, K Goldman, A TI Special issue - Hitran - Preface SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material C1 Harvard Smithsonian Ctr Astrophys, Astrophys Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Denver, Dept Phys, Denver, CO 80208 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Astrophys Atom & Mol Phys Div, MS 50,60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 18 Z9 18 U1 0 U2 1 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 1 EP 2 DI 10.1016/S0022-4073(03)00145-6 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800001 ER PT J AU Rothman, LS Barbe, A Benner, DC Brown, LR Camy-Peyret, C Carleer, MR Chance, K Clerbaux, C Dana, V Devi, VM Fayt, A Flaud, JM Gamache, RR Goldman, A Jacquemart, D Jucks, KW Lafferty, WJ Mandin, JY Massie, ST Nemtchinov, V Newnham, DA Perrin, A Rinsland, CP Schroeder, J Smith, KM Smith, MAH Tang, K Toth, RA Vander Auwera, J Varanasi, P Yoshino, K AF Rothman, LS Barbe, A Benner, DC Brown, LR Camy-Peyret, C Carleer, MR Chance, K Clerbaux, C Dana, V Devi, VM Fayt, A Flaud, JM Gamache, RR Goldman, A Jacquemart, D Jucks, KW Lafferty, WJ Mandin, JY Massie, ST Nemtchinov, V Newnham, DA Perrin, A Rinsland, CP Schroeder, J Smith, KM Smith, MAH Tang, K Toth, RA Vander Auwera, J Varanasi, P Yoshino, K TI The HITRAN molecular spectroscopic database: edition of 2000 including updates through 2001 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Review DE HITRAN; spectroscopic database; molecular spectroscopy; molecular absorption; absorption cross-sections; aerosol refractive indices ID ABSORPTION CROSS-SECTIONS; TUNABLE DIODE-LASER; HETERODYNE FREQUENCY MEASUREMENTS; FOURIER-TRANSFORM SPECTROSCOPY; ABSOLUTE LINE-INTENSITIES; MULTISPECTRUM FITTING PROCEDURE; CARBONYL SULFIDE TRANSITIONS; AIR-BROADENING COEFFICIENTS; COMPLEX REFRACTIVE-INDEXES; INFRARED OPTICAL-CONSTANTS AB This paper describes the status circa 2001, of the HITRAN compilation that comprises the public edition available through 2001. The HITRAN compilation consists of several components useful for radiative transfer calculation codes: high-resolution spectroscopic parameters of molecules in the gas phase, absorption cross-sections for molecules with very dense spectral features, aerosol refractive indices, ultraviolet line-by-line parameters and absorption cross-sections, and associated database management software. The line-by-line portion of the database contains spectroscopic parameters for 38 molecules and their isotopologues and isotopomers suitable for calculating atmospheric transmission and radiance properties. Many more molecular species are presented in the infrared cross-section data than in the previous edition, especially the chlorofluorocarbons and their replacement gases. There is now sufficient representation so that quasi-quantitative simulations can be obtained with the standard radiance codes. In addition to the description and justification of new or modified data that have been incorporated since the last edition of HITRAN (1996), future modifications are indicated for cases considered to have a significant impact on remote-sensing experiments. (C) 2003 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Paris 06, Lab Phys Mol & Applicat, F-75252 Paris, France. Univ Libre Brussels, Lab Chim Phys Mol, B-1050 Brussels, Belgium. Univ Paris 06, Serv Aeron, F-75252 Paris, France. Catholic Univ Louvain, Lab Spect Mol, B-1348 Louvain, Belgium. Univ Paris 11, CNRS, Photophys Mol Lab, F-91405 Orsay, France. Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. Univ Denver, Dept Phys, Denver, CO 80208 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. SUNY Stony Brook, Stony Brook, NY 11794 USA. Rutherford Appleton Lab, Didcot OX11 OQX, Oxon, England. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Ontar Corp, N Andover, MA 01845 USA. NIST, Opt Technol Div, Gaithersburg, MD 20899 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu RI clerbaux, cathy/I-5478-2013; OI Rothman, Laurence/0000-0002-3837-4847; Chance, Kelly/0000-0002-7339-7577 NR 178 TC 792 Z9 822 U1 7 U2 52 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 5 EP 44 DI 10.1016/S0022-4073(03)00146-8 PG 40 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800002 ER PT J AU Goldman, A Stephen, TM Rothman, LS Giver, LP Mandin, JY Gamache, RR Rinsland, CP Murcray, FJ AF Goldman, A Stephen, TM Rothman, LS Giver, LP Mandin, JY Gamache, RR Rinsland, CP Murcray, FJ TI The 1-mu m CO2 bands and the O-2 (0-1) X-3 Sigma(-)(g) a(1)Delta(g) and (1-0) X-3 Sigma(-)(g)- b(1)Sigma g(+) bands in the Earth atmosphere SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article ID INTEGRATED ABSORPTION INTENSITIES; INTERACTING VIBRATIONAL-STATES; IMPROVED SPECTRAL PARAMETERS; COLLISION-INDUCED ABSORPTION; LINE POSITIONS; PRESSURE-SHIFT; BROADENING COEFFICIENTS; MOLECULAR-OXYGEN; WAVE-NUMBERS; MU-M AB The CO2 triad of bands in the 9300-9700 cm(-1) region have been observed in near infrared 0.05 cm(-1) resolution ground-based solar absorption spectra. This interval is a portion of spectra taken in the 900012,000 cm(-1) region, at large solar zenith angles. Considering the available line positions and pressure line shifts for CO2, H2O and O-2 in this region as of 2000, it was concluded that these observations show significant inconsistencies among the line positions of the species as listed in the atmospheric spectroscopy databases. The spectra allow a better definition of the O-2 (0-1) X(3)Sigma(g)(-) - a(1)Delta(g) band, with the discrete (0-1) transitions observable in the 9300-9450 cm(-1), superimposed on a collision-induced continuum covering the 9200-9700 cm(-1) region. This continuum, as well as the (0-0) continuum in the 7900 cm(-1) region, have been previously studied only from atmospheric spectra with much lower spectral resolution. The discrete O-2 (1-0) transitions of the X(3)Sigma(g)(-) - b(1)Sigma(g)(+) atmospheric B-band are observed in the 11,500-11,600 cm(-1) region, but no evidence is found for an underlying continuum. A recent laboratory study of the 2v(1) + 3v(3) (CO2)-C-12 triad significantly improves the consistency between the O-2, H2O and CO2 lines in the atmospheric spectra. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Denver, Dept Phys, Denver, CO 80208 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. NASA, Ames Res Ctr, Atmospher Phys Branch, Moffett Field, CA 94035 USA. Univ Paris 06, CNRS, Lab Phys Mol & Applicat, F-75252 Paris 05, France. Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23681 USA. RP Goldman, A (reprint author), Univ Denver, Dept Phys, 2112 E Wesley Ave, Denver, CO 80208 USA. EM goldman@acd.ucar.edu NR 41 TC 12 Z9 12 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV-DEC PY 2003 VL 82 IS 1-4 BP 197 EP 205 DI 10.1016/S0022-4073(03)00153-5 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800009 ER PT J AU Rinsland, CP Flaud, JM Perrin, A Birk, A Wagner, G Goldman, A Barbe, A De Backer-Barilly, MR Mikhailenko, SN Tyuterev, VG Smith, MAH Devi, VM Benner, DC Schreier, F Chance, KV Orphal, J Stephen, TM AF Rinsland, CP Flaud, JM Perrin, A Birk, A Wagner, G Goldman, A Barbe, A De Backer-Barilly, MR Mikhailenko, SN Tyuterev, VG Smith, MAH Devi, VM Benner, DC Schreier, F Chance, KV Orphal, J Stephen, TM TI Spectroscopic parameters for ozone and its isotopes: recent measurements, outstanding issues, and prospects for improvements to HITRAN SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE laboratory spectroscopy; ozone; remote sensing ID ABSORPTION CROSS-SECTIONS; HIGH-RESOLUTION MEASUREMENTS; ATMOSPHERIC TRACE GASES; FTIR SOLAR SPECTRA; LINE POSITIONS; TEMPERATURE-DEPENDENCE; ABSOLUTE INTENSITIES; SHIFT COEFFICIENTS; NU(1)+NU(3) BANDS; CM(-1) REGION AB In this article we review ozone spectroscopy from the microwave to the ultraviolet since the release of the 1996 HITRAN database. Uncertainties, deficiencies, areas of potential improvement, and anticipated new spectral line parameters datasets are highlighted. Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Paris 11, CNRS, Photophys Mol Lab, F-91405 Orsay, France. German Aerosp Ctr, Remote Sensing Technol Inst, Oberpfaffenhofen, Germany. Univ Denver, Dept Phys, Denver, CO 80208 USA. UFR Sci, CNRS, UMR 6089, Grp Spectrometrie Mol & Atmospher, F-51687 Reims 2, France. Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634055, Russia. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 402, Hampton, VA 23681 USA. RI Orphal, Johannes/A-8667-2012; OI Orphal, Johannes/0000-0002-1943-4496; Chance, Kelly/0000-0002-7339-7577 NR 73 TC 19 Z9 20 U1 1 U2 3 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 207 EP 218 DI 10.1016/S0022-4073(03)00154-7 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800010 ER PT J AU Goldman, A Coffey, MT Hannigan, JW Mankin, WG Chance, KV Rinsland, CP AF Goldman, A Coffey, MT Hannigan, JW Mankin, WG Chance, KV Rinsland, CP TI HBr and HI line parameters update for atmospheric spectroscopy databases SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HBr; HI; infrared; line parameters; spectroscopic databases ID INFRARED-EMISSION-SPECTROSCOPY; SUBMILLIMETER; SPECTRUM AB Recent work on new line parameters for the X(1)Sigma(+)(0-0),(0-1) (HBr)-Br-79, (HBr)-Br-81 bands and the X(1)Sigma(+)(0-0), (0-1) HI bands, which include hyperfine structure components, has been extended for an update of spectroscopic databases in use for atmospheric spectroscopy. The updated line parameters, now incorporated in HITRAN 2001, are discussed in comparison to HITRAN 1996. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Denver, Dept Phys, Denver, CO 80208 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80303 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23681 USA. RP Goldman, A (reprint author), Univ Denver, Dept Phys, Denver, CO 80208 USA. OI Chance, Kelly/0000-0002-7339-7577 NR 20 TC 8 Z9 8 U1 1 U2 1 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 313 EP 317 DI 10.1016/S0022-4073(03)00160-2 PG 5 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800016 ER PT J AU Jacquemart, D Mandin, JY Dana, V Claveau, C Vander Auwera, J Herman, A Rothman, LS Regalia-Jarlot, L Barbe, A AF Jacquemart, D Mandin, JY Dana, V Claveau, C Vander Auwera, J Herman, A Rothman, LS Regalia-Jarlot, L Barbe, A TI The IR acetylene spectrum in HITRAN: update and new results SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE acetylene; infrared; vibro-rotational transitions; line parameters; databases ID VIBRATIONAL-ENERGY PATTERN; DIODE-LASER MEASUREMENTS; FOURIER-TRANSFORM SPECTROMETER; EFFECTIVE OPERATOR APPROACH; INTERNAL PARTITION SUMS; 13.7 MU-M; LINE-INTENSITIES; LOW-TEMPERATURES; NU(5) BAND; APPROXIMATE CONSTANTS AB The 2000 HITRAN edition, with the updates of 2001, contains improved and new data on the acetylene molecule. The main changes concern the 13.6- and 7.5-mum spectral regions (improved line intensities), and the 5-mum region (previously absent from the database). These changes are reviewed, and the key problem of the validation of line intensities is dealt with. The status of the currently available line parameters is critically examined, and recommendations for future improvements are given. (C) 2603 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Paris 06, CNRS, Lab Phys Mol & Applicat, F-75252 Paris, France. Free Univ Brussels, Lab Chim Phys Mol, B-1050 Brussels, Belgium. Univ Reims, CNRS, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. OI Rothman, Laurence/0000-0002-3837-4847 NR 68 TC 36 Z9 36 U1 1 U2 5 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 363 EP 382 DI 10.1016/S0022-4073(03)00163-8 PG 20 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800019 ER PT J AU Fischer, J Gamache, RR Goldman, A Rothman, LS Perrin, A AF Fischer, J Gamache, RR Goldman, A Rothman, LS Perrin, A TI Total internal partition sums for molecular species in the 2000 edition of the HITRAN database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE total internal partition sums; partition functions; atmospheric molecular species; HITRAN; temperature dependence of partition functions ID FAR-INFRARED-SPECTRUM; LINEAR-MOLECULES; TOP MOLECULES; INTENSITIES; H2O2 AB Total internal partition sums (TIPS) are calculated for all molecular species in the 2000 HITRAN database. In addition, the TIPS for 13 other isotopomers/isotopologues of ozone and carbon dioxide are presented. The calculations address the corrections suggested by Goldman et al. (JQSRT 66 (2000) 455). The calculations consider the temperature range 70-3000 K to be applicable to a variety of remote sensing needs. The method of calculation for each molecular species is stated and comparisons with data from the literature are discussed. A new method of recall for the partition sums, Lagrange 4-point interpolation, is developed. This method, unlike previous versions of the TIPS code, allows all molecular species to be considered. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Massachusetts Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. Univ Denver, Dept Phys, Denver, CO 80208 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Paris 11, Photophys Mol Lab, F-91405 Orsay, France. RP Gamache, RR (reprint author), Univ Massachusetts Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. OI Rothman, Laurence/0000-0002-3837-4847 NR 19 TC 122 Z9 137 U1 4 U2 18 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 401 EP 412 DI 10.1016/S0022-4073(03)00166-3 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800022 ER PT J AU Orphal, J Chance, K AF Orphal, J Chance, K TI Ultraviolet and visible absorption cross-sections for HITRAN SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Review DE cross-section; ultraviolet visible; remote sensing; trace gases; atmosphere ID OZONE MONITORING EXPERIMENT; FOURIER-TRANSFORM MEASUREMENT; SENSING REFERENCE DATA; REGION 205-240 NM; TEMPERATURE-DEPENDENCE; WAVELENGTH RANGE; ABSOLUTE INTENSITIES; LINE PARAMETERS; A-BAND; 220 K AB Ultraviolet-visible absorption cross-sections are important reference data for remote sensing of atmospheric trace gases including O(3), NO(2), BrO, H(2)CO, OClO, SO(2), and NO(3) using optical instruments. In this paper, the reference absorption cross-sections for the HITRAN database are presented and needs for future improvements are addressed. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ Paris Sud Mol, UPR, CNRS, Photophys Mol Lab, F-91405 Orsay, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Orphal, J (reprint author), Univ Paris Sud Mol, UPR, CNRS, Photophys Mol Lab, Bat 350 Ctr Orsay, F-91405 Orsay, France. EM johannes.orphal@ppm.u-psud.fr RI Orphal, Johannes/A-8667-2012; OI Orphal, Johannes/0000-0002-1943-4496; Chance, Kelly/0000-0002-7339-7577 NR 112 TC 55 Z9 59 U1 3 U2 12 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 NOV-DEC PY 2003 VL 82 IS 1-4 BP 491 EP 504 DI 10.1016/S0022-4073(03)00173-0 PG 14 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 711KG UT WOS:000184738800029 ER PT J AU Sharrer, GT AF Sharrer, GT TI In old Virginia: Slavery, farming, and society in the journal of John Walker. SO JOURNAL OF SOUTHERN HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Sharrer, GT (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOUTHERN HISTORICAL ASSOC PI ATHENS PA UNIV GEORGIA, HISTORY DEPT, ATHENS, GA 30602 USA SN 0022-4642 J9 J SOUTHERN HIST JI J. South. Hist. PD NOV PY 2003 VL 69 IS 4 BP 905 EP 906 PG 2 WC History SC History GA 740YQ UT WOS:000186431200040 ER PT J AU Trueman, C Chenery, C Eberth, DA Spiro, B AF Trueman, C Chenery, C Eberth, DA Spiro, B TI Diagenetic effects on the oxygen isotope composition of bones of dinosaurs and other vertebrates recovered from terrestrial and marine sediments SO JOURNAL OF THE GEOLOGICAL SOCIETY LA English DT Article DE bones; isotope; oxygen; dinosaurs; diagenesis ID JUDITH RIVER FORMATION; SOUTHERN ALBERTA; PROVINCIAL-PARK; STABLE ISOTOPES; CANADA; PHOSPHATE; APATITE; THERMOREGULATION; FRACTIONATION; PALEOECOLOGY AB Assessing effects of diagenesis on oxygen isotope composition of bone is essential to its use in reconstructing habitats and lifestyles of ancient vertebrates. These effects are a matter of controversy, particularly in the case of extinct animals such as dinosaurs. To investigate the effects of diagenesis on isotopic composition of fossil bone, bone samples from both marine and terrestrial Campanian sediments from Alberta, Canada, have been analysed. The isotopic compositions of oxygen (delta(18)O(SMOW)) were determined in bones sampled from articulated skeletons of exclusively terrestrial animals recovered from the terrestrial Dinosaur Park Formation, and compared with bones from the marine Bearpaw Formation. The articulated skeleton of an exclusively terrestrial dinosaur (hadrosaur) found in marine sediments yielded similar delta(18)O values for both structural carbonate and phosphate fractions (mean delta(18)O(SMOW) values 22.6parts per thousand and 16.9parts per thousand, respectively) in bone to marine reptiles (mosasaurs) recovered from the same locality (mean delta(18)O(SMOW) values 24.2parts per thousand and 17.3parts per thousand, respectively). The isotopic composition of both skeletons recovered from marine sediments was significantly more positive than that of articulated hadrosaur skeletons recovered from contemporaneous terrestrial sediments (mean phosphate delta(18)O(SMOW) value 12.9parts per thousand), and outside the range of phosphate delta(18)O(SMOW) values previously reported for terrestrial dinosaur skeletons (c. 9-14parts per thousand). These data suggest that the isotopic composition of oxygen in the phosphate and structural carbonate ions in the bone apatite was altered during diagenesis and can be used for neither palaeoclimate nor physiological reconstruction. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. British Geol Survey, NERC, Isotope Geosci Lab, Keyworth NG12 5GG, Notts, England. Royal Tyrrell Museum Palaeontol, Drumheller, AB T0J 0Y0, Canada. Nat Hist Museum, Dept Mineral, London SW7 5BD, England. RP Trueman, C (reprint author), Univ Portsmouth, Sch Earth & Environm Sci, Burnaby Bldg,Burnaby Rd, Portsmouth PO1 3QL, Hants, England. RI Trueman, Clive/E-6925-2011; OI Chenery, Carolyn Ann/0000-0001-9592-051X NR 43 TC 21 Z9 22 U1 1 U2 5 PU GEOLOGICAL SOC PUBL HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CENTRE, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0016-7649 J9 J GEOL SOC LONDON JI J. Geol. Soc. PD NOV PY 2003 VL 160 BP 895 EP 901 DI 10.1144/0016-764903-019 PN 6 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 745WD UT WOS:000186713000007 ER PT J AU Endo, H Kimura, J Oshida, T Stafford, BJ Rerkamnuaychoke, W Nishida, T Sasaki, M Hayashida, A Hayash, Y AF Endo, H Kimura, J Oshida, T Stafford, BJ Rerkamnuaychoke, W Nishida, T Sasaki, M Hayashida, A Hayash, Y TI Geographical variation of skull morphology and its functional significances in the red-cheeked squirrel SO JOURNAL OF VETERINARY MEDICAL SCIENCE LA English DT Article DE Dremomys rufigenis; geographical variation; osteometry; red-cheeked squirrel; skull ID COMMON TREE SHREW; THAILAND; ISTHMUS; KRA AB Skulls of the red-cheeked squirrel (Dremomys rufigenis) from various geographical locations: Malaysia (peninsular area), Vietnam (south district)-Laos, and Thailand (north district) were osteometrically examined. The skull size of the squirrels in the southern (Malaysia) population was fundamentally larger than that in the northern (Vietnam, Laos and Thailand) populations. The proportion indices indicated that the splanchnocranium was relatively longer in the Malaysia population, and that the interorbital space was narrower in Vietnam-Laos, and Thailand populations. We suggest that the long nose and laterally-oriented orbits in the skull may be better adapted for terrestrial-insectivorous life in the Malaysia population and the binocular sense facilitated by rostrally-oriented eyes contributes to the arboreal-fruit eating behavior in the two northern populations. The Malaysia population was clearly distinguished from the other populations by the principal component analysis. We suggest that the geographical barrier of the Isthmus of Kra influences the morphological variation of the skull among the squirrel populations. C1 Natl Sci Museum, Dept Zool, Shinjuku Ku, Tokyo 1690073, Japan. Nihon Univ, Coll Bioresource Sci, Dept Vet Anat, Kanagawa 2528610, Japan. Tunghai Univ, Dept Biol, Lab Mol Ecol, Taichung 407, Taiwan. Smithsonian Inst, Natl Museum Nat Hist, Mammal Div, Washington, DC 20560 USA. Howard Univ, Coll Med, Dept Anat, Washington, DC USA. Kasetsart Univ, Fac Vet Med, Dept Vet Anat, Bangkok, Thailand. Obihiro Univ Agr & Vet Med, Dept Vet Anat, Obihiro, Hokkaido 0808555, Japan. Univ Tokyo, Grad Sch Agr & Life Sci, Tokyo 1138657, Japan. RP Endo, H (reprint author), Natl Sci Museum, Dept Zool, Shinjuku Ku, 3-23-1 Hyakunin Cho, Tokyo 1690073, Japan. NR 12 TC 7 Z9 9 U1 0 U2 2 PU JAPAN SOC VET SCI PI TOKYO PA UNIV TOKYO, 1-1-1 YAYOI, BUNKYO-KU, TOKYO, 103, JAPAN SN 0916-7250 J9 J VET MED SCI JI J. Vet. Med. Sci. PD NOV PY 2003 VL 65 IS 11 BP 1179 EP 1183 DI 10.1292/jvms.65.1179 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA 753FR UT WOS:000187221900005 PM 14665745 ER PT J AU Schroll, S AF Schroll, S TI Aaron Siskind 100. SO LIBRARY JOURNAL LA English DT Book Review 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 2003 VL 128 IS 18 BP 79 EP 80 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 736UY UT WOS:000186192600076 ER PT J AU Aiello, A AF Aiello, A TI For love of insects. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. 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 2003 VL 128 IS 18 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 736UY UT WOS:000186192600253 ER PT J AU Hutchinson, A AF Hutchinson, A TI The beast in the garden: A modern parable of man and nature. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Hutchinson, A (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 1 PY 2003 VL 128 IS 18 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 736UY UT WOS:000186192600251 ER PT J AU Myers, KJ AF Myers, KJ TI Mr. Whistler's gallery: The art of displaying art SO MAGAZINE ANTIQUES LA English DT Article C1 Smithsonian Inst, Arthur M Sackler Gallery, Washington, DC 20560 USA. RP Myers, KJ (reprint author), Smithsonian Inst, Arthur M Sackler Gallery, Washington, DC 20560 USA. NR 30 TC 0 Z9 0 U1 0 U2 1 PU BRANT PUBL, INC PI NEW YORK PA 575 BROADWAY, NEW YORK, NY 10012 USA SN 0161-9284 J9 MAG ANTIQUES JI Mag. Antiq. PD NOV PY 2003 VL 164 IS 5 BP 140 EP 151 PG 12 WC Art SC Art GA 737UM UT WOS:000186250200018 ER PT J AU Ingolfsson, A Agnarsson, I AF Ingolfsson, A Agnarsson, I TI Amphipods and isopods in the rocky intertidal: dispersal and movements during high tide SO MARINE BIOLOGY LA English DT Article ID POLLOCK POLLACHIUS-VIRENS; CARCINUS-MAENAS; SHORE CRAB; ZONE; MIGRATION; BEHAVIOR; ICELAND; RATHKE AB Animals in the intertidal, both mobile and sessile, generally exhibit some zonation pattern, in which each species shows a preference for, or is confined to, some height levels. The study of zonation patterns is, however, almost exclusively based on surveys made during low tide, when many animals are relatively inactive. We studied zonation patterns of amphipods and isopods on rocky shores in southwestern Iceland, both by traditional sampling at low tide as well as by sampling during high tide. The distributional patterns seen at high tide differed significantly from that at low tide. One amphipod, Anonyx sarsi, was common around baits at all levels at high tide but absent from the intertidal at low tide. Several other species were either relatively more common or tended to be recorded higher, or in one instance, lower on the shore when the tide was in than at low tide. There was also evidence of some species changing habitats within the intertidal with the tidal cycle. Many species, however, moved little away from their respective zones occupied at low tide, and for some species, including some capable of rapid swimming, very limited mobility was indicated. We conclude that low-tide surveys of the intertidal give an incomplete picture of the community structure, and even key species may be missed in such surveys. C1 Univ Iceland, Inst Biol, IS-108 Reykjavik, Iceland. Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Ingolfsson, A (reprint author), Univ Iceland, Inst Biol, Grensasvegur 12, IS-108 Reykjavik, Iceland. EM agnaring@hi.is NR 31 TC 13 Z9 17 U1 0 U2 6 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD NOV PY 2003 VL 143 IS 5 BP 859 EP 866 DI 10.1007/s00227-003-1132-6 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 741NH UT WOS:000186463800004 ER PT J AU Novick, RR Dick, CW Lemes, MR Navarro, C Caccone, A Bermingham, E AF Novick, RR Dick, CW Lemes, MR Navarro, C Caccone, A Bermingham, E TI Genetic structure of Mesoamerican populations of Big-leaf mahogany (Swietenia macrophylla) inferred from microsatellite analysis SO MOLECULAR ECOLOGY LA English DT Article DE mahogany; Meliaceae; Mesoamerica; microsatellites; population genetics; Swietenia macrophylla ID TROPICAL TREE; FRAGMENTED POPULATIONS; DIFFERENTIATION; MARKERS; KING; FLOW; MELIACEAE; DIVERSITY; AMERICA; ECOLOGY AB While microsatellites have been used to examine genetic structure in local populations of Neotropical trees, genetic studies based on such high-resolution markers have not been carried out for Mesoamerica as a whole. Here we assess the genetic structure of the Mesoamerican mahogany Swietenia macrophylla King (big-leaf mahogany), a Neotropical tree species recently listed as endangered in CITES which is commercially extinct through much of its native range. We used seven variable microsatellite loci to assess genetic diversity and population structure in eight naturally established mahogany populations from six Mesoamerican countries. Measures of genetic differentiation (F-ST and R-ST) indicated significant differences between most populations. Unrooted dendrograms based on genetic distances between populations provide evidence of strong phylogeographic structure in Mesoamerican mahogany. The two populations on the Pacific coasts of Costa Rica and Panama were genetically distant from all the others, and from one another. The remaining populations formed two clusters, one comprised of the northern populations of Mexico, Belize and Guatemala and the other containing the southern Atlantic populations of Nicaragua and Costa Rica. Significant correlation was found between geographical distance and all pairwise measures of genetic divergence, suggesting the importance of regional biogeography and isolation by distance in Mesoamerican mahogany. The results of this study demonstrate greater phylogeographic structure than has been found across Amazon basin S. macrophylla. Our findings suggest a relatively complex Mesoamerican biogeographic history and lead to the prediction that other Central American trees will show similar patterns of regional differentiation. C1 Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06511 USA. Smithsonian Trop Res Inst, Ancon, Panama. Inst Nacl de Pesquisas da Amazonia, Lab Genet & Biol Reprod Plantas, BR-69011970 Manaus, Amazonas, Brazil. Trop Agr Ctr Res & Higher Educ CATIE, Turrialba 7170, Costa Rica. RP Novick, RR (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, OML 165 Prospect St, New Haven, CT 06511 USA. RI Dick, Christopher/A-8744-2008 NR 48 TC 69 Z9 74 U1 2 U2 18 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 NOV PY 2003 VL 12 IS 11 BP 2885 EP 2893 DI 10.1046/j.1365-294X.2003.01951.x PG 9 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 734UR UT WOS:000186076800003 PM 14629370 ER PT J AU McCartney, MA Acevedo, J Heredia, C Rico, C Quenoville, B Bermingham, E McMillan, WO AF McCartney, MA Acevedo, J Heredia, C Rico, C Quenoville, B Bermingham, E McMillan, WO TI Genetic mosaic in a marine species flock SO MOLECULAR ECOLOGY LA English DT Article DE coral reef fishes; hamlets; hybridization; microsatellites; mtDNA; speciation ID SERRANID FISH HYPOPLECTRUS; MICROSATELLITE NULL ALLELE; MITOCHONDRIAL-DNA; DARWINS FINCHES; CICHLID FISHES; PHENOTYPIC ASSOCIATIONS; HAMLETS HYPOPLECTRUS; CLADISTIC-ANALYSIS; MOLECULAR-BASIS; LAKE MALAWI AB We used molecular approaches to study the status of speciation in coral reef fishes known as hamlets (Serranidae: Hypoplectrus). Several hamlet morphospecies coexist on Caribbean reefs, and mate assortatively with respect to their strikingly distinct colour patterns. We provide evidence that, genetically, the hamlets display characteristics common in species flocks on land and in freshwaters. Substitutions within two mitochondrial DNA (mtDNA) protein-coding genes place hamlets within a monophyletic group relative to members of two related genera (Serranus and Diplectrum), and establish that the hamlet radiation must have been very recent. mtDNA distances separating hamlet morphospecies were slight (0.6 +/- 0.04%), yielding a coalescent estimate for the age of the hamlet flock of approximately 430 000 years. Morphospecies did not sort into distinct mtDNA haplotype phylogroups, and alleles at five hypervariable microsatellite loci were shared broadly across species boundaries. None the less, molecular variation was not distributed at random. Analyses of mtDNA haplotype frequencies and nested clades in haplotype networks revealed significant genetic differences between geographical regions and among colour morphospecies. We also observed significant microsatellite differentiation between geographical regions and in Puerto Rico, among colour morphospecies; the latter providing evidence for reproductive isolation between colour morphospecies at this locale. In our Panama collection, however, colour morphospecies were mostly genetically indistinguishable. This mosaic pattern of DNA differentiation implies a complex interaction between population history, mating behaviour and geography and suggests that porous boundaries separate species in this flock of brilliantly coloured coral reef fishes. C1 Univ N Carolina, Dept Biol Sci, Wilmington, NC 28403 USA. Univ Puerto Rico, Dept Biol, San Juan, PR 00936 USA. Univ E Anglia, Sch Biol Sci, Norwich NR4 7T3, Norfolk, England. Smithsonian Trop Res Inst, NAOS Marine Lab, Balboa, Panama. RP McCartney, MA (reprint author), Univ N Carolina, Dept Biol Sci, 601 S Coll Rd, Wilmington, NC 28403 USA. EM mccartneym@uncwil.edu RI Rico, Ciro/K-5725-2015; CSIC, EBD Donana/C-4157-2011 OI Rico, Ciro/0000-0002-0822-336X; CSIC, EBD Donana/0000-0003-4318-6602 NR 73 TC 57 Z9 58 U1 1 U2 9 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD NOV PY 2003 VL 12 IS 11 BP 2963 EP 2973 DI 10.1046/j.1365-294X.2003.01946.x PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 734UR UT WOS:000186076800010 PM 14629377 ER PT J AU Suh, SO Marshall, CJ McHugh, JV Blackwell, M AF Suh, SO Marshall, CJ McHugh, JV Blackwell, M TI Wood ingestion by passalid beetles in the presence of xylose-fermenting gut yeasts SO MOLECULAR ECOLOGY LA English DT Article DE Enteroramus dimorphus; evolution; LSU rDNA; SSU rDNA; symbiosis; wood decomposition ID ASCOMYCETOUS YEASTS; COLEOPTERA; SEQUENCES; FUNGI AB During a survey of insect gut micro-organisms, we consistently isolated Pichia stipitis-like yeasts (Fungi: Ascomycota, Saccharomycetes) from the wood-ingesting beetles, Odontotaenius disjunctus and Verres sternbergianus (Coleoptera: Passalidae). The yeasts were isolated from passalid beetles over a wide area, including the eastern and midwestern USA and Panama. Phylogenetic analyses of the nuclear encoded small and large subunit rRNA gene (rDNA) sequences distinguished a well-supported clade consisting of the passalid yeasts and Pichia stipitis, P. segobiensis, Candida shehatae and C. ergatensis. Members of this clade have the ability to ferment and assimilate xylose or to hydrolyse xylan, major components of the polysaccharide, hemicellulose. Sexual reproduction was present in the passalid isolates but was rare among the gut yeasts of other beetles to which they were compared. Minor genetic and phenotypic variation among some of the passalid yeasts was detected using markers from the internal transcribed spacer region of the rDNA repeat unit, morphology, and in vitro metabolic tests. The consistent association of xylose-fermenting yeasts of almost identical genotypes with passalid beetles across a broad geographical distribution, suggests a significant symbiotic association. C1 Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Entomol, Washington, DC 20560 USA. Univ Georgia, Dept Entomol, Athens, GA 30602 USA. RP Blackwell, M (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RI McHugh, Joseph/P-7417-2015 OI McHugh, Joseph/0000-0002-7954-6254 NR 37 TC 90 Z9 94 U1 2 U2 17 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 NOV PY 2003 VL 12 IS 11 BP 3137 EP 3145 DI 10.1046/j.1365-294X.2003.01973.x PG 9 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 734UR UT WOS:000186076800025 PM 14629392 ER PT J AU Kilkenny, D Reed, MD O'Donoghue, D Kawaler, SD Mukadam, A Kleinman, SJ Nitta, A Metcalfe, TS Provencal, JL Watson, TK Sullivan, DJ Sullivan, T Shobbrook, R Jiang, XJ Joshi, S Ashoka, BN Seetha, S Leibowitz, E Ibbetson, P Mendelson, H Meistas, E Kalytis, R Alisauskas, D Martinez, P van Wyk, F Stobie, RS Marang, F Zola, S Krzesinski, J Ogloza, W Moskalik, P Silvotti, R Piccioni, A Vauclair, G Dolez, N Chevreton, M Dreizler, S Schuh, SL Deetjen, JL Solheim, JE Perez, JMG Ulla, A Ostensen, R Manteiga, M Suarez, O Burleigh, M Kepler, SO Kanaan, A Giovannini, O AF Kilkenny, D Reed, MD O'Donoghue, D Kawaler, SD Mukadam, A Kleinman, SJ Nitta, A Metcalfe, TS Provencal, JL Watson, TK Sullivan, DJ Sullivan, T Shobbrook, R Jiang, XJ Joshi, S Ashoka, BN Seetha, S Leibowitz, E Ibbetson, P Mendelson, H Meistas, E Kalytis, R Alisauskas, D Martinez, P van Wyk, F Stobie, RS Marang, F Zola, S Krzesinski, J Ogloza, W Moskalik, P Silvotti, R Piccioni, A Vauclair, G Dolez, N Chevreton, M Dreizler, S Schuh, SL Deetjen, JL Solheim, JE Perez, JMG Ulla, A Ostensen, R Manteiga, M Suarez, O Burleigh, M Kepler, SO Kanaan, A Giovannini, O TI A Whole Earth Telescope campaign on the pulsating subdwarf B binary system PG 1336-018 (NY Vir) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : individual : PG 1336-018; stars : oscillations; stars : variables : other ID EC 14026 STARS; UNEQUALLY-SPACED DATA; SDB STAR; MULTISITE CAMPAIGN; ECLIPSING BINARY; FOURIER-ANALYSIS; ASTEROSEISMOLOGY; PG-2131+066; PERIODS AB We present results from a multisite ('Whole Earth Telescope') photometric campaign on PG 1336-018, the close eclipsing binary system containing a pulsating subdwarf B (sdB) star. The main part of the campaign (1999 April) resulted in similar to172 h of observations, representing a coverage of about 47 per cent, and additional data were obtained outside the core campaign. Periodogram analysis shows that the light variations are dominated by three frequencies near 5757, 5585 and 5369 muHz (similar to174, 179 and 186 s, respectively), although many frequencies are present, particularly in the range 5000-6000 muHz (similar to200-170 s). We identify, with some confidence, 28 frequencies down to a semi-amplitude of 0.0005 in fractional intensity (equivalent to about 0.5 mmag). It is clear that the pulsation frequencies of PG 1336-018 have changed substantially since the 1996 discovery observations were made, and that amplitude changes occur, at least in the dominant three frequencies, on relatively short time-scales (of the order of a day). On the assumption that the pulsating star is phase-locked in the binary system, we have searched for rotational splitting of frequencies near the orbital and half of the orbital period, but the results are confused by aliasing at those frequencies (due to the data gaps caused by the eclipses). A preliminary model qualitatively matches the distribution of frequencies in PG 1336-018, with some good individual correspondences, but cannot be considered adequate because geometric cancellation should hide some of the modes which are apparently detected. Analysis of the pulsations during eclipse recovers three of the strongest modes, but the limited eclipse data - which can, at best, be only about 9 per cent of the total - do not allow mode identification at this stage. Simulations indicate that an overall coverage of about 80 per cent would be required for this to be viable. An attempt was made to determine phase shifts in the pulsation frequencies as a way of directly measuring the size of the binary orbit, but the uncertainties in the method are comparable to the light travel time across the orbit (probably less than a second). C1 S African Astron Observ, ZA-7935 Observatory, South Africa. SW Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65804 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Apache Point Observ, Sunspot, NM 88349 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Delaware, Newark, DE 19716 USA. Southwestern Univ, Georgetown, TX 78626 USA. Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. Univ Sydney, Sch Phys, Chatterton Astron Dept, Sydney, NSW 2006, Australia. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Uttar Pradesh State Observ, Naini Tal 263129, India. Indian Space Res Org, Bangalore 560017, Karnataka, India. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Inst Theoret Phys & Astrophys, LT-2600 Vilnius, Lithuania. Vilnius State Univ, Inst Mat Res & Appl Sci, LT-2009 Vilnius, Lithuania. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. Krakow Pedag Univ, Mt Suhora Observ, Krakow, Poland. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Osserv Astron Capodimonte, I-80131 Naples, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Univ Toulouse 3, Observ Midi Pyrenees, CNRS, UMR5572, F-31400 Toulouse, France. Observ Paris, DAEC, F-92195 Meudon, France. Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. Univ Tromso, Inst Fys, N-9037 Tromso, Norway. Univ Vigo, Fac Ciencias, Dept Fis, Vigo 36200, Spain. Isaac Newton Grp Telescopes, E-37800 Santa Cruz de La Palma, Spain. Civil Univ A Coruna, Dept Ciencias Navegac & Tierra ES Marina, E-15011 Acoruna, Spain. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Fed Rio Grande do Sul, Inst Fis, BR-91501900 Porto Alegre, RS, Brazil. Univ Fed Santa Catarina, Florianopolis, SC, Brazil. Univ Caixas do Sul, Dept Quim & Fis, BR-95001970 Caxias do Sul, RS, Brazil. RP Kilkenny, D (reprint author), S African Astron Observ, POB 9, ZA-7935 Observatory, South Africa. EM dmk@saao.ac.za RI Metcalfe, Travis/A-9388-2008; Kepler, S. O. /H-5901-2012; Ulla Miguel, Ana Maria/M-2860-2014; Manteiga, Minia/K-9773-2014; OI Metcalfe, Travis/0000-0003-4034-0416; Kepler, S. O. /0000-0002-7470-5703; Manteiga, Minia/0000-0002-7711-5581; Silvotti, Roberto/0000-0002-1295-8174; Kawaler, Steven/0000-0002-6536-6367 NR 29 TC 40 Z9 40 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2003 VL 345 IS 3 BP 834 EP 846 DI 10.1046/j.1365-8711.2003.07007.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736JX UT WOS:000186168600015 ER PT J AU Weil, SE AF Weil, SE TI Beyond big and awesome - Outcome-based evaluation (The impact of museums on their visitors) SO MUSEUM NEWS LA English DT Article C1 Smithsonian Inst, Ctr Educ & Museum Studies, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 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 2003 VL 82 IS 6 BP 40 EP + PG 0 WC Art SC Art GA 738EA UT WOS:000186272700008 ER PT J AU Kyllo, DA Velez, V Tyree, MT AF Kyllo, DA Velez, V Tyree, MT TI Combined effects of arbuscular mycorrhizas and light on water uptake of the neotropical understory shrubs, Piper and Psychotria SO NEW PHYTOLOGIST LA English DT Article DE arbuscular mycorrhiza (AM); high pressure flow meter (HPFM); hydraulic conductance; Piper; Psychotria; tropical forest ID TROPICAL MOIST FOREST; SHOOT HYDRAULIC CONDUCTANCE; HIGH-PRESSURE FLOWMETER; RAIN-FOREST; ROOT ARCHITECTURE; VA MYCORRHIZAL; ROSE PLANTS; DROUGHT; GROWTH; NUTRIENT AB Root hydraulic conductance (K-r) was measured for five understory shrub species of the neotropical moist forest to determine the effects of arbuscular mycorrhizas (AM) for both carbon-rich and carbon-limited host plants. K-r was measured using a high pressure flow meter (HPFM) for potted plants grown in a factorial combination of AM fungi (presence/absence) and light (3.5 and 30% of full sun, low/high). AM colonization improved Kr for the more shade-tolerant species plants when growing in low light. By contrast, water uptake efficiency of the light-demanding species was significantly decreased by AM fungi in high light. Regardless of AM colonization, light-demanding species had a lower capacity than shade-tolerant species to meet transpirational demands, and they allocated substantially more to fine root production relative to leaf area when colonized. The differential effects of AM colonization and light on a species' root hydraulic conductance in relation to phylogeny and light adaptation demonstrate that AM fungi may be critical in determining early plant succession and community composition not only due to effects on nutrient uptake, but on water uptake as well. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, Balboa, Panama. US Forest Serv, USDA, Aiken Forestry Sci Lab, S Burlington, VT 05402 USA. RP Kyllo, DA (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. NR 54 TC 15 Z9 20 U1 2 U2 13 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 NOV PY 2003 VL 160 IS 2 BP 443 EP 454 DI 10.1046/j.1469-8137.2003.00896.x PG 12 WC Plant Sciences SC Plant Sciences GA 739BH UT WOS:000186322000017 ER PT J AU Pearson, TRH Burslem, DFRP Goeriz, RE Dalling, JW AF Pearson, TRH Burslem, DFRP Goeriz, RE Dalling, JW TI Regeneration niche partitioning in neotropical pioneers: effects of gap size, seasonal drought and herbivory on growth and survival SO OECOLOGIA LA English DT Article DE Panama; seedling; species richness; trade-off; tropical forest ID LOWLAND TROPICAL FOREST; SHADE TOLERANCE; PHYSIOLOGICAL ECOLOGY; RELATIVE IMPORTANCE; PLANT-COMMUNITIES; POPLAR SEEDLINGS; LIGHT GRADIENT; TREE SEEDLINGS; CHANGE RANK; SEED SIZE AB Adaptive trade-offs underlie the specialisation that permits habitat partitioning in species rich plant communities. We investigated the influence of the trade-offs that determine differences in growth and survival among six species of neotropical pioneer trees in gaps in semideciduous forest in Panama. Seedlings of Miconia argentea, Cecropia insignis, Luehea seemannii, Trema micrantha, Ochroma pyramidale and Croton bilbergianus were planted into artificial small (25 m(2)), medium (64 m(2)) and large (225 m(2)) gaps in secondary forest in the Barro Colorado Nature Monument. Trema and Ochroma suffered greater than or equal to50% mortality across all gap sizes, while Cecropia had high mortality only during the dry season and in the small gaps, and Miconia and Croton suffered low to zero mortality across all environments. The highest growth rates in large gaps were attained by Cecropia seedlings and in the smaller gaps by Miconia seedlings, although there were indications that Trema and Ochroma required gaps that were larger than any used in this study. Variation in growth and mortality could not be attributed to differences in foliar herbivore damage. Instead, there was strong evidence of a trade-off between maximum growth in the wet season and the ability to survive seasonal drought, particularly in small gaps. We conclude that variation in allocation in response to multiple limiting resources may be as important as allocation to growth and defence in determining the habitat preferences of neotropical pioneers. C1 Univ Aberdeen, Dept Plant & Soil Sci, Aberdeen AB24 3UU, Scotland. Smithsonian Trop Res Inst, U0948, APO, AA 34002 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Winrock Int Livestock Res & Training Ctr, 1621 N Kent St,Suite 1200, Arlington, VA 22209 USA. EM tpearson@winrock.org OI Burslem, David/0000-0001-6033-0990 NR 53 TC 36 Z9 43 U1 1 U2 34 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD NOV PY 2003 VL 137 IS 3 BP 456 EP 465 DI 10.1007/s00442-003-1361-x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 735CA UT WOS:000186093800018 PM 12920642 ER PT J AU Florescu, V Gavrila, M AF Florescu, V Gavrila, M TI Extreme relativistic compton scattering by K-shell electrons SO PHYSICAL REVIEW A LA English DT Article ID COULOMB GREENS FUNCTION; HIGH-ENERGIES; RADIATIVE-CORRECTIONS; MOMENTUM DISTRIBUTION; ELASTIC-SCATTERING; CROSS-SECTION; PHOTONS; APPROXIMATION; LASER; RETARDATION AB We have derived cross sections for Compton scattering of very hard incident photons (homega(1)>mc(2)) from K-shell electrons, exact in the nuclear charge Z. The nuclear potential was taken to be of Coulomb form. The calculation of the extreme relativistic (ER) S-matrix element involved was carried out analytically. In the present case, this is the viable alternative to an impracticable ab initio numerical computation. In order to obtain the dominant behavior of the matrix element in the large omega(1) limit, the momentum transferred to the nucleus needs to be ascribed a constant (albeit arbitrary) value in the limiting process. The result depends critically on the spectral range in which the scattered-photon energy omega(2) is situated. We start by considering the omega(2) range covering the Compton line, for which the ratio omega(2)/omega(1) needs to be kept finite. We show that in the ER limit the Dirac electron spinors and Green's operator entering the S-matrix element can be replaced by their relativistically modified Schrodinger counterparts. This allows the application of integration methods developed by us earlier for the nonrelativistic matrix element. Remarkably enough, the sixfold integrals of the ER matrix element can eventually be reduced to single integrals, expressible in terms of generalized hypergeometric functions. The doubly differential cross section d(2)sigma/domega(2) dOmega(2) for the range of Compton line finally results as a twofold integration, requiring a simple numerical computation. This is a rather unique example of a most elaborate Coulomb problem that could be solved analytically, essentially in closed form. We subsequently consider the low- (omega(2)-->0) and high-frequency (omega(2)-->omega(2)(max)) ends of the scattered photon spectrum. For omega(2)-->0 we find the expected infrared divergence, and verify the soft-photon theorem, which represents an important check on our calculation. Finally, we present our numerical results for d(2)sigma/domega(2) dOmega(2), analyzed at fixed omega(2) (angular distributions), or fixed photon scattering angle (spectral distributions). We discuss the "defect" and the width of the Compton line for both distributions. C1 Univ Bucharest, Dept Phys, Bucharest 76900, Romania. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Florescu, V (reprint author), Univ Bucharest, Dept Phys, MG11, Bucharest 76900, Romania. RI FLORESCU, Viorica/A-2394-2014 NR 39 TC 3 Z9 3 U1 0 U2 0 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 NOV PY 2003 VL 68 IS 5 AR 052709 DI 10.1103/PhysRevA.68.052709 PG 17 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 750BF UT WOS:000186970900050 ER PT J AU Krems, RV Sadeghpour, HR Dalgarno, A Zgid, D Klos, J Chalasinski, G AF Krems, RV Sadeghpour, HR Dalgarno, A Zgid, D Klos, J Chalasinski, G TI Low-temperature collisions of NH(X3 Sigma(-)) molecules with He atoms in a magnetic field: An ab initio study SO PHYSICAL REVIEW A LA English DT Article ID GAUSSIAN-BASIS SETS; COUPLED-CLUSTER; ULTRACOLD MOLECULES; DERIVATIVE METHOD; WAVE-FUNCTIONS; PHOTOASSOCIATION; SCATTERING; THRESHOLD AB Ab initio calculations of cross sections and rate constants for elastic scattering and Zeeman relaxation in collisions of NH(X (3)Sigma(-)) molecules with He-3 atoms in a magnetic field are presented and the mechanism for Zeeman transitions in ground-state (3)Sigma molecules is established. The potential surface for He-NH interaction is obtained using all-electron coupled-cluster calculations with single, double, and noniterative triple excitations in a basis set augmented by bond functions. The ratio of the rates for elastic energy transfer and Zeeman relaxation in NH-He-3 collisions exceeds 10(5) at temperatures between 0.5 and 1 K. C1 Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. 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 Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. RI Klos, Jacek/A-6457-2008 OI Klos, Jacek/0000-0002-7407-303X NR 34 TC 54 Z9 54 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 NOV PY 2003 VL 68 IS 5 AR 051401 DI 10.1103/PhysRevA.68.051401 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 750BF UT WOS:000186970900006 ER PT J AU Blackman, EG Field, GB AF Blackman, EG Field, GB TI A new approach to turbulent transport of a mean scalar SO PHYSICS OF FLUIDS LA English DT Article ID DIFFUSION; EQUATION AB We develop a simple mean field approach to the transport of a passive scalar for which the fundamental equation is a second order differential equation in the transported quantity, not a first order equation. Triple correlations are included, as they must be for any realistic description of turbulence. No correlation time enters the theory, only an eddy turnover time. The approach is simpler than standard approaches which incorporate triple correlations, but more realistic than Gaussian or short correlation time closures which do not. A similar approach has proven useful in magnetohydrodynamics. (C) 2003 American Institute of Physics. C1 Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Rochester, Laser Energet Lab, Rochester, NY 14627 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blackman, EG (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. NR 26 TC 39 Z9 39 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD NOV PY 2003 VL 15 IS 11 BP L73 EP L76 DI 10.1063/1.1613281 PG 4 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 731BY UT WOS:000185865700001 ER PT J AU Harwit, M AF Harwit, M TI The growth of astrophysical understanding SO PHYSICS TODAY LA English DT Article; Proceedings Paper CT Meeting of the American-Physical-Society CY APR, 2003 CL PHILADELPHIA, PENNSYLVANIA SP Amer Phys Soc ID PROBE WMAP OBSERVATIONS AB A stroll through three millennia of astronomic and discovery reminds us that inspired guesses enough. Progress comes primarily,from the introduction of new observational and theoretical tools. C1 Cornell Univ, Ithaca, NY 14853 USA. Smithsonian Natl Air & Space Museum, Washington, DC USA. RP Harwit, M (reprint author), Cornell Univ, Ithaca, NY 14853 USA. NR 20 TC 5 Z9 5 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD NOV PY 2003 VL 56 IS 11 BP 38 EP 43 DI 10.1063/1.1634532 PG 6 WC Physics, Multidisciplinary SC Physics GA 738HQ UT WOS:000186281500022 ER PT J AU Holtum, JAM Winter, K AF Holtum, JAM Winter, K TI Photosynthetic CO2 uptake in seedlings of two tropical tree species exposed to oscillating elevated concentrations of CO2 SO PLANTA LA English DT Article DE CO2 oscillations; elevated CO2 concentrations; free-air CO2 enrichment (FACE) systems; photosynthesis; tropical trees ID SHORT-TERM FLUCTUATIONS; AFFECT LEAF RESPIRATION; ATMOSPHERIC CO2; ENRICHMENT FACE; DARK RESPIRATION; SYSTEM; PLANTS; ACCLIMATION; VEGETATION; RESPONSES AB Do short-term fluctuations in CO2 concentrations at elevated CO2 levels affect net CO2 uptake rates of plants? When exposed to 600 mul CO2 l(-1), net CO2 uptake rates in shoots or leaves of seedlings of two tropical C-3 tree species, teak (Tectona grandis L. f.) and barrigon [Pseudobombax septenatum (Jacq.) Dug.], increased by 28 and 52% respectively. In the presence of oscillations with half-cycles of 20 s, amplitude of ca. 170 mul CO2 l(-1) and mean of 600 mul CO2 l(-1), the stimulation in net CO2 uptake by the two species was reduced to 19 and 36%, respectively, i.e. the CO2 stimulation in photosynthesis associated with a change in exposure from 370 to 600 mul CO2 l(-1) was reduced by a third in both species. Similar reductions in CO2-stimulated net CO2 uptake were observed in T. grandis exposed to 40-s oscillations. Rates of CO2 efflux in the dark by whole shoots of T. grandis decreased by 4.8% upon exposure of plants grown at 370 mul CO2 l(-1) to 600 mul CO2 l(-1). The potential implications of the observations on CO2 oscillations and dark respiration are discussed in the context of free-air CO2 enrichment (FACE) systems in which short-term fluctuations of CO2 concentration are a common feature. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. RI Holtum, Joseph/B-3063-2012 OI Holtum, Joseph/0000-0001-6568-8019 NR 31 TC 39 Z9 43 U1 0 U2 7 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0032-0935 J9 PLANTA JI Planta PD NOV PY 2003 VL 218 IS 1 BP 152 EP 158 DI 10.1007/s00425-003-1089-1 PG 7 WC Plant Sciences SC Plant Sciences GA 743TH UT WOS:000186589300018 PM 12905026 ER PT J AU Golub, L AF Golub, L TI Solar observation from space SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Review ID EOS SORCE MISSION; TRANSITION REGION; CORONAL EXPLORER; HELIOSEISMOLOGY; OSCILLATIONS; ATMOSPHERE; FIELDS; VIEW AB Solar observations are carried out in space when necessary for technical reasons, such as detection of wavelengths that do not reach the ground, or to provide observing conditions that are difficult or impossible to achieve on the ground. Examples in the first category are observations at far ultraviolet or soft x-ray wavelengths and direct detection of solar wind particles; in the latter are precise measurements of variations in the solar luminosity and stereo observations of coronal mass ejections. This article samples the wide variety of techniques presently being used to study the Sun. We begin with an overview of the observational problem presented by the particular scientific questions involved in improving our understanding of the Sun, and of solar activity in particular. We then discuss the need for and advantages of observations from space, and give examples of scientific objectives which can only be met by such observations. We then describe in detail some representative examples of space missions and specific space-based experiments for solar studies. (C) 2003 American Institute of Physics. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Golub, L (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Golub, Leon/0000-0001-9638-3082 NR 32 TC 2 Z9 2 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 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD NOV PY 2003 VL 74 IS 11 BP 4583 EP 4600 DI 10.1063/1.1618011 PG 18 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 737XE UT WOS:000186256400001 ER PT J AU Terrell, EE Robinson, H AF Terrell, EE Robinson, H TI Survey of Asian and Pacific species of Hedyotis and Exallage (Rubiaceae) with nomenclatural notes on Hedyotis types SO TAXON LA English DT Article DE Asia; Exallage; Hedyotis; morphology; pacific; Oldenlandia; rubiaceae; typification; taxonomy ID RUBIOIDEAE RUBIACEAE; PHYLOGENY AB Selection of a type species for the wide-ranging genus Hedyotis (Hedyotideae; Rubiaceae) has involved a longstanding controversy over two species, Hedyotis auricularia L. and H. fruticosa L. Nomenclatural and morphological data support the selection of H. fruticosa as type. The choice of H. auricularia would have caused considerable taxonomic confusion by upsetting previously established names and overturning the names of the many species of Oldenlandia. The General Committee on nornenclature recently has approved Hedyolis fruticosa as the conserved type of Hedyotis. The morphology and taxonomy of the genus Exallage, based on H. auricularia, is surveyed, and we conclude that at least three of the species are better treated as a new subgenus of Oldenlandia. The synonymy of these species is listed, and two new combinations are published in the genus Oldenlandia. A detailed survey of the species related to Hedyotis fruticosa begins with the 24 Sri Lankan species, most of which exhibit morphological characters similar to Hedyotis fruticosa. The capsules of these species have been termed diplophragmous in allusion to the partial apical loculicidal dehiscence followed by complete septicidal dehiscence, resulting in two separate capsular halves or cocci. The seeds of these species are dorsiventrally compressed with a ventral hilar ridge topped by a punctiform apical hilum. Many other Asian and Pacific, particularly Micronesian, species show similar diplophragmous capsules and fruticosa-type seeds. The recognition of this newly circumscribed group, Hedyotis subgenus Hedyotis, ranging from China and India to Micronesia, establishes a firm basis for comparative studies of Hawaiian and American species, which are known to differ in morphology from the typical subgenus. C1 Smithsonian Inst, Dept Systemat Biol Bot, Museum Natl Hist Nat, Washington, DC 20013 USA. RP Terrell, EE (reprint author), Smithsonian Inst, Dept Systemat Biol Bot, Museum Natl Hist Nat, MRC-166,POB 37012, Washington, DC 20013 USA. NR 33 TC 11 Z9 20 U1 1 U2 1 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 NOV PY 2003 VL 52 IS 4 BP 775 EP 782 DI 10.2307/3647351 PG 8 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 754XA UT WOS:000187357400012 ER PT J AU Faden, RB AF Faden, RB TI Lectotypification of two African species of Commelina (Commelinaceae), with the description of new taxa from Madagascar and Tanzania SO TAXON LA English DT Editorial Material DE Africa; Commelina purpurea; Commelina scandens; Commelinaceae; lectotypification AB Commelina scandens C.B. Clarke and Commelina purpurea C.B. Clarke were typified by syntypes that belong to different species. Accordingly, each species is lectotypified, and the taxonomic consequences of the lectotypifications are discussed. Commelina scandens is lectotypified by a specimen from Angola, with the result that the species is confined to continental Africa. A new subspecies, Commelina diffusa Burm.f. subsp. violacea Faden, is described for the Madagascan element in Clarke's C. scandens. Commelina purpurea is lectotypified by the syntype from Kenya, resulting in C. lugardii Bullock and C. kabarensis De Wild. being placed in synonymy under C. purpurea. The other element in Clarke's C. purpurea is described as a new species C. pseudopurpurea Faden. C1 US Natl Herbarium, Dept Systemat Biol Bot, Museum Natl Hist Nat, Smithsonian Inst, Washington, DC 20013 USA. RP Faden, RB (reprint author), US Natl Herbarium, Dept Systemat Biol Bot, Museum Natl Hist Nat, Smithsonian Inst, MRC-166,POB 37012, Washington, DC 20013 USA. NR 19 TC 2 Z9 3 U1 1 U2 1 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 NOV PY 2003 VL 52 IS 4 BP 831 EP 836 DI 10.2307/3647356 PG 6 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 754XA UT WOS:000187357400017 ER PT J AU Xiang, QP Zhang, XC Nicolson, DH AF Xiang, QP Zhang, XC Nicolson, DH TI Correctability of the epithet minchegense to mingcheense in Lycopodium (Lycopodiaceae) and lectotypification of Lycopodium mingcheense SO TAXON LA English DT Editorial Material DE Huperzia; lectotypification; Lycopodium; nomenclature; Phlegmariurus ID HUPERZIA AB The long overlooked synonym Lycopodium "minchegense" Ching has one month's priority over Phlegmariurus mingcheensis Ching on which Huperzia mingcheensis (Ching) Holub is based. It is argued that the older binomial has a typesetter's error (misplaced "g") and is correctable to L. mingcheense. A new combination in Huperzia would be a later homonym of Holub's combination. A lectotype is designated for L. mingcheense. C1 Chinese Acad Sci, Inst Bot, Ctr Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Zhang, XC (reprint author), Chinese Acad Sci, Inst Bot, Ctr Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. NR 7 TC 2 Z9 2 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 NOV PY 2003 VL 52 IS 4 BP 857 EP 858 DI 10.2307/3647361 PG 2 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 754XA UT WOS:000187357400022 ER PT J AU Nicolson, DH AF Nicolson, DH TI Robert William Read (1931-2003) SO TAXON LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Nicolson, DH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 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 NOV PY 2003 VL 52 IS 4 BP 869 EP 869 PG 1 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 754XA UT WOS:000187357400025 ER PT J AU Narayan, R AF Narayan, R TI Black holes - Sparks of interest SO NATURE LA English DT Article ID SAGITTARIUS-A-ASTERISK; X-RAY FLARE; STAR C1 Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 10 TC 5 Z9 5 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 30 PY 2003 VL 425 IS 6961 BP 908 EP 909 DI 10.1038/425908a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 737KY UT WOS:000186230600024 PM 14586450 ER PT J AU Britz, R Kottelat, M AF Britz, R Kottelat, M TI Descriptive Osteology of the Family Chaudhuriidae (Teleostei, Synbranchiformes, Mastacembeloidei), with a Discussion of its Relationships SO AMERICAN MUSEUM NOVITATES LA English DT Article ID FISHES; EEL AB The little known earthworm eel family Chaudhuriidae consists of nine small to minute species of Asian freshwater fishes. In this paper, the osteology of seven representatives of the family is described in detail for the first time. We propose a list of 21 synapomorphies to support chaudhuriid monophyly. Reductive characters are: loss of basisphenoid, pterosphenoid, endopterygoid, dermopalatine, pars autopalatina, posttemporal, gill rakers, toothplate on pharyngobranchial two, distal pectoral radials, lateral line canals, dorsal- and anal-fin spines and their supporting pterygiophores, epurals, uroneurals, parhypural, and reduction in numbers of epicentrals and hypurals. Progressive characters are: presence of a long membrane bone process on autosphenotic, a boomerang-shaped ectopterygoid with a long preorbital extension, an anterior process of membrane bone of the metapterygoid, a unique arrangement of dorsal gill arch elements, separate foramina for the three trigeminal branches, and a ventromedian keel on the first vertebra. The new information is used to critically reevaluate previous hypotheses of chaudhuriid relationships. Finally, the issue of miniaturization in chaudhuriid fishes is addressed and discussed. C1 Univ Tubingen, Lehrstuhl Spezielle Zool, D-72076 Tubingen, Germany. Amer Museum Nat Hist, Dept Ichthyol, New York, NY 10024 USA. RP Britz, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. EM britz.ralf@nmnh.si.edu NR 50 TC 15 Z9 17 U1 0 U2 3 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD OCT 29 PY 2003 IS 3418 BP 1 EP 62 DI 10.1206/0003-0082(2003)418<0001:DOOTFC>2.0.CO;2 PG 62 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 738QG UT WOS:000186298900001 ER PT J AU Turner, HV Wolcott, DL Wolcott, TG Hines, AH AF Turner, HV Wolcott, DL Wolcott, TG Hines, AH TI Post-mating behavior, intramolt growth, and onset of migration to Chesapeake Bay spawning grounds by adult female blue crabs, Callinectes sapidus Rathbun SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE female blue crab; Callinectes sapidus; foraging; growth; energetics; migration; telemetry; Chesapeake Bay; USA ID ULTRASONIC TELEMETRY; VERTICAL MIGRATION; SITE FIDELITY; MEGALOPAE; CONSTRAINTS; COMPETITION; ABUNDANCE; MOVEMENTS; VARIABLES; TRANSPORT AB After molting to maturity, female blue crabs must rebuild muscles atrophied to permit molting and grow larger ones commensurate with the larger exoskeleton. They also must acquire energy for oogenesis and for migration to high-salinity spawning habitat, a distance of >150 kin for females mating in the Upper Chesapeake Bay. Using telemetry and mark-recapture techniques, post-copulatory females in the upper bay were shown to forage at high rates, alternating between meandering and directed movement in the area of mating for weeks to months, and to begin migrating in October. Consequently, females from the Upper Chesapeake Bay probably do not spawn until the season after mating. Their priority seems to be to acquire energy before migrating. After molting, energy was allocated first into somatic tissue and eventually into hepatopancreas and gonads. Telemetry of feeding and movement showed that habitat utilization, traveling velocities, foraging patterns, and movements were similar to those already determined for males. However, females appeared to invest proportionally more energy (calories per gram dry weight) into their somatic and reproductive tissues than did males. A newly designed transmitter that telemetered depth showed that females moved during both ebbs and floods and remained at or near the bottom of the water column. (C) 2003 Elsevier B.V. All rights reserved. C1 N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Wolcott, DL (reprint author), N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Box 8208, Raleigh, NC 27695 USA. NR 53 TC 38 Z9 40 U1 0 U2 6 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 OCT 28 PY 2003 VL 295 IS 1 BP 107 EP 130 DI 10.1016/S0022-0981(03)00290-9 PG 24 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 717NA UT WOS:000185094900006 ER PT J AU Hu, YQ Habbal, SR Chen, Y Li, X AF Hu, YQ Habbal, SR Chen, Y Li, X TI Are coronal holes the only source of fast solar wind at solar minimum? art. no. 1377 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE coronal holes; fast solar wind; 2-D MHD solar wind model; Alfven wave driven solar wind ID FLUX-CORRECTED TRANSPORT; MAGNETIC-FIELD STRENGTH; LONG-TERM VARIATION; ALFVEN WAVES; MAGNETOHYDRODYNAMIC FLOWS; INTERPLANETARY SPACE; TRANSITION REGION; MODEL; ULYSSES; STREAMER AB A two-dimensional (2-D) MHD model of an Alfven-wave-driven solar wind in the heliospheric meridional plane is presented whereby the consequences of a magnetic field distribution at the Sun that digresses from the standard dipole structure, often used in 2-D MHD models, are explored. The latitudinal distribution of open magnetic flux is specified at the solar surface, with a clear distinction between the polar coronal hole and the neighboring quiet Sun. The region of strictly closed magnetic structures at the coronal base is limited in latitude to +/-30degrees. Alfven waves are assumed to emanate from the solar surface above 30degrees latitude so as to open the field lines anchored there, as well as heat and accelerate the solar wind. The field lines anchored at the solar surface below 30degrees latitude, where the plasma is thermally conductive, remain closed, resulting in the formation of the helmet streamer astride the solar equator. The solution obtained is characterized by a helmet streamer in magnetostatic equilibrium, centered at the solar equator, and a steady solar wind outside. With the assumption that the contribution of the polar coronal hole and the quiet Sun to the interplanetary magnetic flux is evenly split between them during solar minimum, a fast wind solution is obtained that matches the latitudinal distribution of the solar wind parameters observed by Ulysses and SOHO and extends from the pole to 9degrees latitude. The larger fraction (approximate to60%) of the fast wind (above 30degrees latitude at 1 AU) emerges from the polar coronal hole, while the remainder is associated with the quiet Sun. While the actual fraction of the fast solar wind originating from polar coronal holes relies on an accurate estimate of the contribution of the open magnetic flux from polar coronal holes to the total IMF flux, this model shows that extending the source of open magnetic flux at the Sun beyond the traditionally assumed polar coronal holes can readily account for the latitudinal distribution of fast wind measured by Ulysses at solar minimum. C1 Univ Wales, Inst Math & Phys Sci, Aberystwyth SY23 3BZ, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sci & Technol China, Sch Earth & Space Sci, Hefei 230026, Peoples R China. RP Univ Wales, Inst Math & Phys Sci, Aberystwyth SY23 3BZ, Dyfed, Wales. EM huyq@ustc.edu.cn; sdh@aber.ac.uk; yachen@cfa.harvard.edu; xxl@aber.ac.uk RI Chen, Yao/B-7255-2011 NR 61 TC 27 Z9 30 U1 1 U2 3 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 OCT 28 PY 2003 VL 108 IS A10 AR 1377 DI 10.1029/2002JA009776 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 740HX UT WOS:000186397900001 ER PT J AU Olson, SL Hearty, PJ AF Olson, SL Hearty, PJ TI Probable extirpation of a breeding colony of Short-tailed Albatross (Phoebastria albatrus) on Bermuda by Pleistocene sea-level rise SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID HISTORY; PLIOCENE; BAHAMAS AB Albatrosses (Diomedeidae) do not occur in the North Atlantic Ocean today except as vagrants, although five species were present in the early Pliocene. No fossil breeding sites of albatrosses were known previously. The timing of extinction of albatrosses in the North Atlantic was likewise unknown. Deposits that formed near present-day sea level along the southeastern shore of Bermuda contain remains of a former breeding colony and include intact eggshells and bones of embryos, juveniles, and adults of Short-tailed Albatross (Phoebastria albatrus), a critically endangered species now confined to a few islets in the northwestern Pacific Ocean. These deposits are correlated with the middle Pleistocene Lower Town Hill Formation, which at other sites have a radiometric age of approximate to405,000 years ago. This equates with the marine isotope stage 11 interglacial, which culminated in a rise in sea-level to >+20 m. Bones of a juvenile Short-tailed Albatross were also found in beach deposits at +21.3 m from this same interglacial. We interpret the extirpation of albatrosses on Bermuda as probably resulting from lack of nesting sites protected from storm surges over the little emergent land that remained at the height of the marine isotope stage 11 sea level rise. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, POB 37012, Washington, DC 20013 USA. NR 23 TC 37 Z9 38 U1 2 U2 9 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD OCT 28 PY 2003 VL 100 IS 22 BP 12825 EP 12829 DI 10.1073/pnas.1934576100 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 738RF UT WOS:000186301100058 PM 14566060 ER PT J AU Cheung, ASC Wong, AL Lo, DHY Leung, KWS Yoshino, K Thorne, AP Murray, JE Imajo, T Ito, K Matsui, T AF Cheung, ASC Wong, AL Lo, DHY Leung, KWS Yoshino, K Thorne, AP Murray, JE Imajo, T Ito, K Matsui, T TI Application of a VUV Fourier transform spectrometer and synchrotron radiation source to measurements of. VI. The epsilon(0,0) band of NO SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID FINE STRUCTURE ANALYSIS; NITRIC-OXIDE; OSCILLATOR-STRENGTHS; HIGH-RESOLUTION; ULTRAVIOLET; MOLECULE; SYSTEMS; PREDISSOCIATION; FLUORESCENCE; TRANSITION AB The epsilon(0,0) (D (2)Sigma(+)-X (2)Pi(r)) band of NO has been recorded by using a vacuum ultraviolet Fourier transform spectrometer from Imperial College, London, with synchrotron radiation at the Photon Factory, KEK, Japan, as a continuum light source. Analysis of the epsilon(0,0) band provides accurate rotational line positions and term values as well as the photoabsorption cross sections. Molecular constants of the v=0 level of the D (2)Sigma state have been determined as T-0=53 291.10+/-0.10 cm(-1), B-0=1.991 07+/-0.000 05 cm(-1), and D-0=(6.6+/-0.1)x10(-6) cm(-1). Accurate rotational line strengths have also been obtained and the sum of the line strengths for all rotational lines is determined as 2.18x10(-15) cm(2) cm(-1). The band oscillator strength of the epsilon(0,0) band is determined to be (2.47+/-0.12)x10(-3). (C) 2003 American Institute of Physics. C1 Univ Hong Kong, Dept Chem, Hong Kong, Hong Kong, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Japan Womens Univ, Tokyo 1128681, Japan. Natl Lab High Energy Phys, KEK, Photon Factory, Tsukuba, Ibaraki 305, Japan. RP Cheung, ASC (reprint author), Univ Hong Kong, Dept Chem, Hong Kong, Hong Kong, Peoples R China. NR 28 TC 7 Z9 5 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 OCT 22 PY 2003 VL 119 IS 16 BP 8373 EP 8378 DI 10.1063/1.1611171 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 731BW UT WOS:000185865500020 ER PT J AU Weitz, CM Parker, TJ Bulmer, MH Anderson, FS Grant, JA AF Weitz, CM Parker, TJ Bulmer, MH Anderson, FS Grant, JA TI Geology of the Melas Chasma landing site for the Mars Exploration Rover mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Valles Marineris; Melas Chasma; MER; landslides; valleys; mass wasting ID VALLES MARINERIS MARS; SUBMARINE LANDSLIDES; LAYERED DEPOSITS; DEBRIS FLOWS; SPECTROMETER; TOPOGRAPHY; TECTONICS; EVOLUTION; PATTERNS; ORIGIN AB [1] The Melas Chasma landing site was considered a high-priority site for the Mars Exploration Rover ( MER) mission because of the opportunity to land on and study potential layered sedimentary deposits. Though no longer considered a candidate site because of safety concerns, the site remains a scientifically interesting area that provides insight into the geologic history of Valles Marineris. Within the landing ellipse are dunes, landslide material, and unusual blocky deposits. The blocky deposits are composed of rounded blocks, some of which have meter-scale layering, and they show evidence of ductile deformation, including bending and distortion of coherent blocks around each other. The morphologic characteristics of the blocks are unique, and they appear to have no terrestrial analogue. However, the gross morphology of these blocky deposits and their superposition on adjacent wallrock is consistent with the blocks having been transported downslope. Given the existence of other large mass failures in the area, we propose the blocky deposits may also have originated from mass movement events. The size of the blocks coupled with the distances they traveled indicates high mobility. The distances the blocks were transported and their rounded, irregular shapes suggest either water in the source material or deposition in a subaqueous environment. The source for the main blocky deposit inside the landing ellipse is considered to be the wallrock to the south, while the other two blocky deposits have source regions along the northern canyon walls. The southern wallrock of Melas Chasma contains numerous valleys not seen elsewhere in Valles Marineris. The identification of valley networks along the southern wallrock suggests that a source of water existed below the surface of the plateau and produced the valleys after intersecting the edge of the exposed canyon walls. C1 Planetary Sci Inst, Tucson, AZ 85719 USA. NASA Headquarters, Washington, DC USA. Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Weitz, CM (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. NR 77 TC 23 Z9 23 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT 22 PY 2003 VL 108 IS E12 AR 8082 DI 10.1029/2002JE002022 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 736YE UT WOS:000186200200001 ER PT J AU Chen, Y Esser, R Hu, YQ AF Chen, Y Esser, R Hu, YQ TI Numerical modeling of the halo electrons in the fast solar wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE solar wind; electron velocity distribution functions; transport phenomena ID VELOCITY DISTRIBUTION-FUNCTIONS; HELIOS PLASMA-EXPERIMENT; POLAR CORONAL HOLE; HEAT-FLUX; GLOBAL PROCESSES; INSTABILITIES; TEMPERATURE; STREAMS; DEPLETIONS; ULYSSES AB [1] A one-dimensional magnetohydrodynamic solar wind model is constructed to describe the behavior of the halo electrons in the fast electron-proton solar wind, assuming that the electrons are composed of two populations: the core and halo. The halo component is separated from the core electrons by increasing the heat deposition. It is shown that the model including only Coulomb collisions yields a much faster halo drift than observed if the halo temperature is in agreement with measured values. This supports the previous argument that some anomalous frictional processes caused by microinstabilities and/or wave-particle interactions exist in the solar wind. We show that these anomalous frictional processes can be approximated by enhanced Coulomb collisions together with a heat deposition that has a very large damping length. We find that beyond a certain heliocentric distance, say 20 R-S, the anomalous frictional forces acting on the halo population are more important than the electric field force and the Coulomb collisional forces and become the dominant factor inhibiting the core-halo drift. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sci & Technol China, Sch Earth & Space Sci, Anhua 230026, Peoples R China. Univ Tromso, Tromso, Norway. RP Chen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Chen, Yao/B-7255-2011 NR 41 TC 4 Z9 4 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 OCT 22 PY 2003 VL 108 IS A10 AR 1371 DI 10.1029/2003JA009957 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 736YL UT WOS:000186200800003 ER PT J AU Rodenhouse, NL Sillett, TS Doran, PJ Holmes, RT AF Rodenhouse, NL Sillett, TS Doran, PJ Holmes, RT TI Multiple density-dependence mechanisms regulate a migratory bird population during the breeding season SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE population regulation; density dependence; migratory bird ID THROATED BLUE WARBLERS; LIMITATION; SONGBIRD; TRENDS; FOREST; CONSERVATION; DYNAMICS; WINTER; CYCLE AB The mechanisms regulating bird populations are poorly understood and controversial. We provide evidence that a migratory songbird, the black-throated blue warbler (Dendroica caerulescens), is regulated by multiple density-dependence mechanisms in its breeding quarters. Evidence of regulation includes: stability in population density during 1969-2002, strong density dependence in time-series analyses of this period, an inverse relationship between warbler density and annual fecundity, and a positive relationship between annual fecundity and recruitment of yearlings in the subsequent breeding season. Tests of the mechanisms causing regulation were carried out within the Hubbard Brook Experimental Forest, New Hampshire, during 1997-1999. When individuals from abutting territories were experimentally removed in a homogeneous patch of high-quality habitat, the fecundity of focal pairs nearly doubled, revealing a locally operating crowding mechanism. A site-dependence mechanism was indicated by an inverse relationship between population size and mean territory quality, as well as by greater annual fecundity on the sites that were most frequently occupied and of highest quality. These site-dependence relationships were revealed by intensive monitoring of territory quality and demography at the landscape spatial scale. Crowding and site-dependence mechanisms, therefore, acted simultaneously but at different spatial scales to regulate local abundance of this migratory bird population. C1 Wellesley Coll, Dept Biol Sci, Wellesley, MA 02481 USA. Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. RP Rodenhouse, NL (reprint author), Wellesley Coll, Dept Biol Sci, Wellesley, MA 02481 USA. EM nrodenho@wellesley.edu NR 41 TC 89 Z9 93 U1 2 U2 37 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD OCT 22 PY 2003 VL 270 IS 1529 BP 2105 EP 2110 DI 10.1098/rspb.2003.2438 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 734QA UT WOS:000186067000003 PM 14561272 ER PT J AU King, AR Pounds, KA AF King, AR Pounds, KA TI Black hole winds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; quasars : general; X-rays : binaries; X-rays : galaxies AB We show that black holes accreting at or above the Eddington rate probably produce winds that are optically thick in the continuum, whether in quasars or in X-ray binaries. The photospheric radius and outflow speed are proportional to (M) over dot (2)(out) out and (M)over dot (-1)(out) out respectively, where (M) over dot (out) is the mass outflow rate. The momentum outflow rate is always of the order of L(Edd)c. Blackbody emission from these winds may provide the big blue bump in some quasars and active galactic nuclei, as well as ultrasoft X-ray components in ultraluminous X-ray sources. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP King, AR (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NR 6 TC 246 Z9 246 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 OCT 21 PY 2003 VL 345 IS 2 BP 657 EP 659 DI 10.1046/j.1365-8711.2003.06980.x PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731FG UT WOS:000185873400025 ER PT J AU Kim, WT Narayan, R AF Kim, WT Narayan, R TI Thermal instability in clusters of galaxies with conduction SO ASTROPHYSICAL JOURNAL LA English DT Article DE conduction; cooling flows; galaxies : clusters : general; hydrodynamics instabilities; X-rays : galaxies : clusters ID X-RAY HALO; COOLING FLOWS; HEAT-CONDUCTION; MAGNETIC-FIELD; XMM-NEWTON; INTERGALACTIC MEDIUM; CHANDRA OBSERVATION; HIGH-RESOLUTION; COLD FRONTS; MODELS AB We consider a model of galaxy clusters in which the hot gas is in hydrostatic equilibrium and maintains energy balance between radiative cooling and heating by thermal conduction. We analyze the thermal stability of the gas using a Lagrangian perturbation analysis. For thermal conductivity at the level of similar to 20% - 40% of Spitzer conductivity, consistent with previous estimates for cluster gas, we find that the growth rate of the most unstable global radial mode is similar to 6-9 times lower than the growth rate of local isobaric modes at the cluster center in the absence of conduction. The growth time in typical clusters is similar to 2-5 Gyr, which is comparable to the time since the last major merger episode, when the gas was presumably well mixed. Thus, we suggest that thermal instability is not dynamically significant in clusters, provided that there is an adequate level of thermal conduction. On the other hand, if the heating of the gas is not the result of thermal conduction or any other diffusive process such as turbulent mixing, then the thermal instability has a growth time under a gigayear in the central regions of the cluster and is a serious threat to equilibrium. We also analyze local nonradial modes and show that the Lagrangian technique leads to the same dispersion relation as the Eulerian approach, provided that clusters are initially in strict thermal equilibrium. Because cluster gas is convectively stable, nonradial modes always have a smaller growth rate than equivalent radial modes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, WT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 72 TC 53 Z9 53 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2003 VL 596 IS 2 BP 889 EP 902 DI 10.1086/378153 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZH UT WOS:000185916000014 ER PT J AU Edmonds, PD Gilliland, RL Heinke, CO Grindlay, JE AF Edmonds, PD Gilliland, RL Heinke, CO Grindlay, JE TI An extensive census of Hubble Space Telescope counterparts to Chandra X-ray sources in the globular cluster 47 Tucanae. I. Astrometry and photometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; globular clusters : individual (47 Tucanae); novae, cataclysmic variables; stars : chromospheres; techniques : photometric; X-rays : binaries ID ECLIPSING MILLISECOND PULSAR; ANGSTROM ATLAS; FAINT SYSTEMS; CCD SPECTROPHOTOMETRY; CATACLYSMIC VARIABLES; DENSITY PROFILE; 47-TUCANAE; CORE; STARS; COMPANION AB We report in this study of 47 Tucanae the largest number of optical identifications of X-ray sources yet obtained in a single globular cluster. Using deep Chandra ACIS-I imaging and extensive Hubble Space Telescope studies with Wide Field Planetary Camera 2 (WFPC2; including a 120 orbit program giving superb V and I images), we have detected optical counterparts to at least 22 cataclysmic variables (CVs) and 29 chromospherically active binaries (BY Dra and RS CVn systems) in 47 Tuc. These identifications are all based on tight astrometric matches between X-ray sources and objects with unusual (non-main-sequence [non-MS]) optical colors and/or optical variability. Several other CVs and active binaries have likely been found, but these have marginal significance because of larger offsets between the X-ray and optical positions, or colors and variability that are not statistically convincing. These less secure optical identifications are not subsequently discussed in detail. In the U versus U-V color-magnitude diagram (CMD), where the U band corresponds to either F336W or F300W, the CVs all show evidence for blue colors compared with the MS, but most of them fall close to the main sequence in the V versus V-I CMD, showing that the secondary stars dominate the optical light. The X-ray-detected active binaries have magnitude offsets above the MS (in both the U versus U-V or V versus V-I CMDs) that are indistinguishable from those of the much larger sample of optical variables (eclipsing and contact binaries and BY Dra variables) detected in the recent WFPC2 studies of Albrow et al. We also present the results of a new, deeper search for optical companions to millisecond pulsars (MSPs). One possible optical companion to an MSP (47 Tuc T) was found, adding to the two optical companions already known. Finally, we study several blue stars with periodic variability from Albrow et al. that show little or no evidence for X-ray emission. The optical colors of these objects differ from those of 47 Tuc (and field) CVs. An accompanying paper will present time series results for these optical identifications and will discuss X-ray-to-optical flux ratios, spatial distributions, and an overall interpretation of the results. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 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 50 TC 64 Z9 64 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2003 VL 596 IS 2 BP 1177 EP 1196 DI 10.1086/378193 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZH UT WOS:000185916000034 ER PT J AU Edmonds, PD Gilliland, RL Heinke, CO Grindlay, JE AF Edmonds, PD Gilliland, RL Heinke, CO Grindlay, JE TI An extensive census of Hubble Space Telescope counterparts to Chandra X-ray sources in the globular cluster 47 Tucanae. II. Time series and analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; globular clusters : individual (47 Tucanae); novae, cataclysmic variables; techniques : photometric; X-rays : binaries ID ECLIPSING MILLISECOND PULSAR; ALL-SKY SURVEY; ACTIVE BINARY CORONAE; CATACLYSMIC VARIABLES; BLUE STRAGGLERS; ORBITAL PERIOD; WHITE-DWARFS; CORE; 47-TUCANAE; COMPANION AB We report time series and variability information for the optical identifications of X-ray sources in 47 Tucanae reported in Paper I (at least 22 cataclysmic variables [CVs] and 29 active binaries). The radial distribution of the CVs is indistinguishable from that of the millisecond pulsars (MSPs) detected by Freire et al. A study of the eight CVs with secure orbital periods (two obtained from the Chandra study of Grindlay et al.) shows that the 47 Tuc CVs have fainter accretion disks, in the V band, than field CVs with similar periods. These faint disks and the faint absolute magnitudes (M-V) of the 47 Tuc CVs suggests they have low accretion rates. One possible explanation is that the 47 Tuc objects may be a more representative sample of CVs, down to our detection threshold, than the CVs found in the field (where many low accretion rate systems are believed to be undiscovered), showing the advantages of deep globular cluster observations. The median F-X/F-opt value for the 47 Tuc CVs is higher than that of all known classes of field CV, partly because of the faint M-V values and partly because of the relatively high X-ray luminosities (L-X). The latter are only seen in DQ Her systems in the field, but the 47 Tuc CVs are much fainter optically than most field DQ Her's. Previous work by Edmonds et al. has shown that the four brightest CVs in NGC 6397 have optical spectra and broadband colors that are consistent with DQ Her's having lower than average accretion rates. Some combination of magnetic behavior and low accretion rates may be able to explain our observations, but the results at present are ambiguous, since no class of field CV has distributions of both L-X and M-V that are consistent with those of the 47 Tuc CVs. The radial distribution of the X-ray detected active binaries is indistinguishable from that of the much larger sample of optical variables (eclipsing and contact binaries and BY Dra variables) detected in previous Wide Field Planetary Camera 2 (WFPC2) studies by Albrow et al. The X-ray properties of these objects (luminosity, hardness ratios, and variability) are consistent with those of active binaries found in field studies, and the F-X/F-opt distribution is significantly different from those of the CVs and the MSPs that are detected (or possibly detected) in the optical. Despite these results, we examine the possibility that a few of the active binaries are MSPs with main-sequence companions resulting from double exchanges in the crowded core of 47 Tuc. No solid evidence is found for a significant population of such objects, and therefore, using the methods of Grindlay et al., we estimate that the number of MSPs in 47 Tuc with luminosities above 10(30) ergs s(-1) is similar to30-40, near the previous lower limit. We present the results of a new, deeper search for faint low-mass X-ray binaries (LMXBs) in quiescence. One reasonable and one marginal candidate for optical identification of a quiescent LMXB was found (one is already known). Finally, it is shown that the periods of the blue variables showing little or no evidence for X-ray emission are too long for Roche lobe filling (if the variations are ellipsoidal). These blue variables also show no evidence for the large flickering levels seen in comparably bright CVs. At present we have no satisfactory explanation for these objects, although some may be detached white dwarf-main-sequence star binaries. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 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 52 TC 53 Z9 53 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2003 VL 596 IS 2 BP 1197 EP 1219 DI 10.1086/378194 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZH UT WOS:000185916000035 ER PT J AU Sasselov, DD AF Sasselov, DD TI The new transiting planet OGLE-TR-56b: Orbit and atmosphere SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; planetary systems; stars : individual (OGLE-TR-56); stars : interiors; stellar dynamics ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; IN EXTRASOLAR PLANETS; CLOSE BINARY STARS; SOLAR-TYPE STAR; TIDAL CIRCULARIZATION; GALACTIC DISK; GIANT PLANETS; 2001 CAMPAIGN; PARENT STAR AB Motivated by the identification of the very close-in extrasolar giant planet OGLE-TR-56b (P = 1.2 days, a = 0.023 AU, M-p = 0.9 M-J), we explore implications of its existence for problems of tidal dissipation, planet migration, and atmospheric stability. The small orbit of OGLE-TR-56b makes the planet an interesting test particle case for tidal dissipation in stellar convection zones. We show that it favors prescriptions of suppressed convective eddy viscosity. Precise timing of the transits of OGLE-TR-56b might place interesting constraints on stellar convection theory if orbital period change is detected in the near future. Another interesting issue related to the new planet is the origin of its close orbit; OGLE-TR-56b may be a survivor of Roche lobe overflow mass loss. Living in such close proximity to its parent star, OGLE-TR-56b should have temperatures in the dayside hemisphere reaching 1900 K, and we find that only few condensates could form clouds, if at all, under those conditions-mostly Al2O3 and Fe(s). We explore the issue of atmosphere evaporation and find that the planet's atmosphere is stable over its lifetime. The large size of the planet (R-p = 1.3 +/- 0.15 R-J) might also require additional energy, similar to HD 209458b. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sasselov, DD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 36 TC 72 Z9 73 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 2003 VL 596 IS 2 BP 1327 EP 1331 DI 10.1086/378145 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZH UT WOS:000185916000044 ER PT J AU Bromm, V Yoshida, N Hernquist, L AF Bromm, V Yoshida, N Hernquist, L TI The first supernova explosions in the universe SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation; hydrodynamics; intergalactic medium; stars : formation; supernovae : general ID SMOOTHED PARTICLE HYDRODYNAMICS; EARLY METAL ENRICHMENT; INTERGALACTIC MEDIUM; GALAXY FORMATION; COSMOLOGICAL SIMULATIONS; PREGALACTIC OUTFLOWS; HYDROGEN MOLECULES; PRIMORDIAL STAR; POPULATION-III; DARK-MATTER AB We investigate the supernova explosions that end the lives of massive Population III stars in low-mass minihalos (M similar to 10(6) M-.) at redshifts z similar to 20. Employing the smoothed particle hydrodynamics method, we carry out numerical simulations in a cosmological setup of pair-instability supernovae with explosion energies of E-SN = 10(51) and 10(53) ergs. Whereas the lower explosion energy leaves part of the halo intact, we find that the more 51 10 energetic explosion leads to the complete disruption of the gas in the minihalo and expels greater than or similar to90% of the stellar metals into a region similar to1 kpc across over a timescale of 3-5 Myr. Because of this burstlike initial star formation episode, a large fraction of the universe could have been endowed with a metallicity floor, Z(min) greater than or similar to 10(-4) Z(.), already at z greater than or similar to 15. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bromm, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Yoshida, Naoki/A-4305-2011 NR 49 TC 142 Z9 142 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 2003 VL 596 IS 2 BP L135 EP L138 DI 10.1086/379359 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZJ UT WOS:000185916100003 ER PT J AU Kim, WT Narayan, R AF Kim, WT Narayan, R TI Turbulent mixing in clusters of galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; hydrodynamics; instabilities; turbulence; X-rays : galaxies ID X-RAY-CLUSTERS; COOLING FLOWS; INTRACLUSTER MEDIUM; THERMAL CONDUCTION; INTERGALACTIC GAS; SCALING RELATIONS; MAGNETIC-FIELDS; HEAT-CONDUCTION; HIGH-RESOLUTION; ENTROPY AB We present a spherically symmetric, steady state model of galaxy clusters in which radiative cooling from the hot gas is balanced by heat transport through turbulent mixing. We assume that the gas is in hydrostatic equilibrium and describe the turbulent heat diffusion by means of a mixing length prescription with a dimensionless parameter alpha(mix). Models with alpha(mix) similar to 0.01 - 0.03 yield reasonably good fits to the observed density and temperature profiles of cooling core clusters. Making the strong simplification that alpha(mix) is time independent and that it is roughly the same in all clusters, the model reproduces remarkably well the observed scalings of X-ray luminosity, gas mass fraction, and entropy with temperature. The break in the scaling relations at kT similar to 1-2 keV is explained by the break in the cooling function at around this temperature, and the entropy floor observed in galaxy groups is reproduced naturally. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, WT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 58 TC 43 Z9 43 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 2003 VL 596 IS 2 BP L139 EP L142 DI 10.1086/379342 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 731ZJ UT WOS:000185916100004 ER PT J AU Bergeman, T Moore, MG Olshanii, M AF Bergeman, T Moore, MG Olshanii, M TI Atom-atom scattering under cylindrical harmonic confinement: Numerical and analytic studies of the confinement induced resonance SO PHYSICAL REVIEW LETTERS LA English DT Article ID GUIDING NEUTRAL ATOMS; IMPENETRABLE BOSONS; GASES AB It was recently predicted [Phys. Rev. Lett. 81, 938 (1998)10.1103/PhysRevLett.81.938] that atom-atom scattering under transverse harmonic confinement is subject to a "confinement-induced resonance" where the effective one-dimensional coupling strength diverges at a particular ratio of the confinement and scattering lengths. As the initial prediction made use of the zero-range pseudopotential approximation, we now report numerical results for finite-range interaction potentials that corroborate this resonance. In addition, we now present a physical interpretation of this effect as a novel type of Feshbach resonance in which the transverse modes of the confining potential assume the roles of "open" and "closed" scattering channels. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Univ So Calif, Dept Phys, Los Angeles, CA 90089 USA. RP Bergeman, T (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Olshanii, Maxim/M-2830-2013 OI Olshanii, Maxim/0000-0003-3629-6002 NR 29 TC 234 Z9 235 U1 0 U2 10 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 17 PY 2003 VL 91 IS 16 AR 163201 DI 10.1103/PhysRevLett.91.163201 PG 4 WC Physics, Multidisciplinary SC Physics GA 734QP UT WOS:000186068300016 PM 14611401 ER PT J AU Stanley, JD AF Stanley, JD TI Effective protection may alter the look of Venice - Those seeking to rescue Venice are caught between the devil and the deep-blue sea. SO NATURE LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Geoarchaeol Program, Washington, DC 20560 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Geoarchaeol Program, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 16 PY 2003 VL 425 IS 6959 BP 661 EP 661 DI 10.1038/425661a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 732DA UT WOS:000185924500013 PM 14562075 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The gothic enterprise: A guide to understanding the medieval cathedral. 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 OCT 15 PY 2003 VL 128 IS 17 BP 66 EP 66 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 729CL UT WOS:000185753700046 ER PT J AU Riley, S AF Riley, S TI You look nice today. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 2003 VL 128 IS 17 BP 95 EP 95 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 729CL UT WOS:000185753700215 ER PT J AU Ouerdane, H Jamieson, MJ Vrinceanu, D Cavagnero, MJ AF Ouerdane, H Jamieson, MJ Vrinceanu, D Cavagnero, MJ TI The variable phase method used to calculate and correct scattering lengths SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID EFFECTIVE-RANGE; MOLECULAR PHYSICS; POTENTIALS; COLLISIONS; ATOMS; COLD AB It is shown that the scattering length can be obtained by solving a Riccati equation derived from variable phase theory. Two methods of solving it are presented. The equation is used to predict how long-range interactions influence the scattering length, and upper and lower bounds on the scattering length are determined. The predictions are compared with others and it is shown how they may be obtained from secular perturbation theory. C1 Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Ouerdane, H (reprint author), Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. RI Ouerdane, Henni/A-2263-2010 OI Ouerdane, Henni/0000-0002-1914-0244 NR 25 TC 23 Z9 26 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 OCT 14 PY 2003 VL 36 IS 19 BP 4055 EP 4063 AR PII S0953-4075(03)65364-2 DI 10.1088/0953-4075/36/19/013 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 739MC UT WOS:000186349600019 ER PT J AU Mazzotta, P Edge, AC Markevitch, M AF Mazzotta, P Edge, AC Markevitch, M TI A Chandra study of the complex structure in the core of 2A 0335+096 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general galaxies : clusters : individual (2A 0335+096); X-rays : galaxies ID FLOW CLUSTER 2A-0335+096; XMM-NEWTON OBSERVATIONS; X-RAY SPECTROSCOPY; COOLING FLOW; INTERGALACTIC MEDIUM; COLD-FRONT; CENTAURUS CLUSTER; PERSEUS CLUSTER; MAGNETIC-FIELD; H-I AB We present a Chandra observation of the central (r<200 kpc) region of the cluster of galaxies 2A 0335+096, rich in interesting phenomena. On large scales (r>40 kpc), the X-ray surface brightness is symmetric and slightly elliptical. The cluster has a cool, dense core; the radial temperature gradient varies with position angle. The radial metallicity profile shows a pronounced central drop and an off-center peak. Similarly to many clusters with dense cores, 2A 0335+096 hosts a cold front at rapproximate to40 kpc south of the center. The gas pressure across the front is discontinuous by a factor A(P)=1.6+/-0.3, indicating that the cool core is moving with respect to the ambient gas with a Mach number Mapproximate to0.75+/-0.2. The central dense region inside the cold front shows an unusual X-ray morphology, which consists of a number of X-ray blobs and/or filaments on scales greater than or similar to3 kpc, along with two prominent X-ray cavities. The X-ray blobs are not correlated with either the optical line emission (Halpha+[N II]), member galaxies, or radio emission. The deprojected temperature of the dense blobs is consistent with that of the less dense ambient gas, so these gas phases do not appear to be in thermal pressure equilibrium. An interesting possibility is a significant, unseen nonthermal pressure component in the interblob gas, possibly arising from the activity of the central active galactic nucleus (AGN). We discuss two models for the origin of the gas blobs-hydrodynamic instabilities caused by the observed motion of the gas core and "bubbling'' of the core caused by multiple outbursts of the central AGN. C1 Univ Durham, Dept Phys, Durham DH1 3LE, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mazzotta, P (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. RI Mazzotta, Pasquale/B-1225-2016 OI Mazzotta, Pasquale/0000-0002-5411-1748 NR 65 TC 52 Z9 52 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2003 VL 596 IS 1 BP 190 EP 203 DI 10.1086/377633 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DQ UT WOS:000185814300016 ER PT J AU Lazendic, JS Dickel, JR Jones, PA AF Lazendic, JS Dickel, JR Jones, PA TI Supernova remnant candidates in the 30 Doradus nebula SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; HII regions; ISM : individual (30 Doradus) Magellanic Clouds; supernova remnants ID LARGE-MAGELLANIC-CLOUD; H-II-REGION; 30 DORADUS REGION; X-RAY PULSAR; OB ASSOCIATIONS; STAR-FORMATION; NEARBY GALAXIES; NOVA REMNANTS; H2O MASERS; RADIO AB We have searched the 30 Doradus nebula, a giant extragalactic H II region, for the presence of embedded supernova remnants using high-resolution radio, optical, and X-ray images. Radio images obtained at 6 and 3.5 cm with the Australia Telescope Compact Array have an angular resolution of similar to2". We compare our radio images with the optical images from the Cerro Tololo Inter-American Observatory to distinguish thermal and possible nonthermal components in the nebula. We have also mapped, for the first time, the extinction across the region at high angular resolution. We identify two sources as supernova remnant candidates in the nebula. Derived physical parameters for the adiabatic phase imply relatively young remnants (similar to10(3) yr) evolving in a very dense environment (greater than or similar to10(2) cm(-3)). We compare our results with high-resolution data from the Chandra X-Ray Observatory, but with only a short exposure these preliminary X-ray data lack the sensitivity to resolve our supernova remnant candidates from intervening hot gas of the diffuse thermal X-ray component of the nebula. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Lazendic, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 62 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 OCT 10 PY 2003 VL 596 IS 1 BP 287 EP 298 DI 10.1086/377630 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DQ UT WOS:000185814300023 ER PT J AU Fish, VL Reid, MJ Argon, AL Menten, KM AF Fish, VL Reid, MJ Argon, AL Menten, KM TI Interstellar hydroxyl masers in the Galaxy. II. Zeeman pairs and the galactic magnetic field SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : disk; HII regions; ISM : magnetic fields; masers; radio lines : ISM ID ROTATION MEASURES; OH MASERS; STAR FORMATION; MOLECULAR CLOUDS; INNER GALAXY; MILKY-WAY; REGIONS; W3(OH); LINE; ABSORPTION AB We have identified and classified Zeeman pairs in the survey by Argon, Reid, & Menten of massive star-forming regions with 18 cm ((II3/2)-I-2; J=3/2) OH maser emission. We have found a total of more than 100 Zeeman pairs in more than 50 massive star-forming regions. The magnetic field deduced from the Zeeman splitting has allowed us to assign an overall line-of-sight magnetic field direction to many of the massive star-forming regions. Combining these data with other data sets obtained from OH Zeeman splitting, we have looked for correlations of magnetic field directions between star-forming regions scattered throughout the Galaxy. Our data do not support a uniform, Galactic-scale field direction, nor do we find any strong evidence of magnetic field correlations within spiral arms. However, our data suggest that in the solar neighborhood the magneticfield outside the solar circle is oriented clockwise as viewed from the north Galactic pole, while inside the solar circle it is oriented counterclockwise. This pattern, including the magnetic field reversal near the Sun, is in agreement with results obtained from pulsar rotation measures. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Fish, VL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 51 TC 54 Z9 54 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 2003 VL 596 IS 1 BP 328 EP 343 DI 10.1086/377081 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DQ UT WOS:000185814300027 ER PT J AU Cyganowski, CJ Reid, MJ Fish, VL Ho, PTP AF Cyganowski, CJ Reid, MJ Fish, VL Ho, PTP TI Dual cometary HII regions in DR 21: Bow shocks or champagne flows? SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (DR 21); ISM : kinematics and dynamics; ISM : molecules; radio lines : ISM ID H-II REGIONS; RECOMBINATION LINE OBSERVATIONS; PHYSICAL-PROPERTIES; OUTFLOW SOURCE; GAS-DYNAMICS; EMISSION; MODEL; H-2 AB The DR 21 massive star-forming region contains two cometary H II regions, aligned nearly perpendicular to each other on the sky. This others a unique opportunity to discriminate among models of cometary H II regions. We present hydrogen recombination and ammonia line observations of DR 21 made with the Very Large Array. The velocity of the molecular gas, measured from NH3 emission and absorption lines, is constant to within +/-1 km s(-1) across the region. However, the radial velocity of the ionized material, measured from hydrogen recombination lines, differs by approximate to9 km s(-1) between the "heads'' of the two cometary H II regions and by up to similar to7 km s(-1) from that of the molecular gas. These findings indicate a supersonic velocity difference between the compact heads of the cometary regions and between each head and the ambient molecular material. This suggests that the observed cometary morphologies are created largely by the motion of wind-blowing, ionizing stars through the molecular cloud, as in a bow shock model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cyganowski, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 25 Z9 25 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 10 PY 2003 VL 596 IS 1 BP 344 EP 349 DI 10.1086/377688 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DQ UT WOS:000185814300028 ER PT J AU Harvey, DWA Wilner, DJ Myers, PC Tafalla, M AF Harvey, DWA Wilner, DJ Myers, PC Tafalla, M TI Disk properties and density structure of the star-forming dense core B335 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; ISM : globules; ISM : individual (B335); radio continuum : ISM; stars : formation ID YOUNG STELLAR OBJECTS; PROTOSTELLAR COLLAPSE; SUBARCSECOND SURVEY; CLOUDS; ENVELOPE; PROTOSTARS; EMISSION; DYNAMICS; MAPS AB We present subarcsecond-resolution dust continuum observations of the protostellar collapse candidate B335 made with the IRAM Plateau de Bure Interferometer at wavelengths of 1.2 and 3.0 mm. These observations probe to less than 100 AU size scales and reveal a compact source component that we identify with a circumstellar disk. We analyze these data in concert with previous lower resolution interferometer observations and find a best-fit density structure for B335 that consists of a power-law envelope with index p=1.55+/-0.04 (rless than or similar to5000 AU) together with a disk (r<100 AU) of flux F(1.2mm)=21 +/- 2 mJy. We estimate a systematic uncertainty in the power-law index delta p less than or similar to 0.15, where the largest error comes from the assumed form of the dust temperature falloff with radius. This determination of the inner density structure of B335 has a precision unique among protostellar cores, and it is consistent with the r(-1.5) profile of gravitational free fall, in accord with basic expectations for the formation of a star. The flux (and implied mass) of the compact component in B335 is typical of the disks around T Tauri stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Astron Nacl, E-28014 Madrid, Spain. RP Harvey, DWA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dharvey@cfa.harvard.edu; dwilner@cfa.harvard.edu; pmyers@cfa.harvard.edu; m.tafalla@oan.es NR 28 TC 39 Z9 39 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 OCT 10 PY 2003 VL 596 IS 1 BP 383 EP 388 DI 10.1086/377581 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DQ UT WOS:000185814300031 ER PT J AU Wilner, DJ Bourke, TL Wright, CM Jorgensen, JK van Dishoeck, EF Wong, T AF Wilner, DJ Bourke, TL Wright, CM Jorgensen, JK van Dishoeck, EF Wong, T TI Disks around the young stars TW Hydrae and HD 100546 imaged at 3.4 millimeters with the Australia Telescope Compact Array SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : protoplanetary disks; stars : individual (TW Hydrae, HD 100546) ID HERBIG AE/BE STARS; FU-ORIONIS STARS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; TAURI STARS; HD-100546; DUST; DISTRIBUTIONS; ENVIRONMENT; EMISSION AB We present observations of the young stars TW Hya and HD 100546 made with the Australia Telescope Compact Array at 89 GHz with similar to2" resolution and similar to3 mJy continuum sensitivity. Compact thermal dust continuum emission is detected from disks surrounding both stars. HD 100546 also shows hints of extended emission, presumably a residual protostellar envelope, which is also visible in scattered light at optical wavelengths. For TW Hya, HCO+ J=1-0 line emission from the circumstellar disk is detected and spatially resolved. The observed size and intensity are in good agreement with model calculations based on an irradiated disk with substantial depletions derived previously from single-dish observations of higher J HCO+ transitions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ New S Wales, Sch Phys, Univ Coll, ADFA, Canberra, ACT 2600, Australia. Leiden Observ, NL-2300 RA Leiden, Netherlands. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 36 TC 44 Z9 44 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2003 VL 596 IS 1 BP 597 EP 602 DI 10.1086/377627 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DQ UT WOS:000185814300049 ER PT J AU King, A AF King, A TI Black holes, galaxy formation, and the M-BH-sigma relation SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : formation; galaxies : nuclei; quasars : general ID COOLING FLOWS; QUASARS; GROWTH; NUCLEI; ORIGIN AB Recent X-ray observations of intense high-speed outflows in quasars suggest that supercritical accretion on to the central black hole may have an important effect on a host galaxy. I revisit some ideas of Silk & Rees and assume that such flows occur in the final stages of building up the black hole mass. It is now possible to model explicitly the interaction between the outflow and the host galaxy. This is found to resemble a momentum-driven stellar wind bubble, implying a relation M-BH=(f(g)kappa/2piG(2))sigma(4)similar or equal to1.5x10(8)sigma(200)(4) M-circle dot between black hole mass and bulge velocity dispersion (f(g)=gas fraction of total matter density, kappa=electron scattering opacity), without free parameters. This is remarkably close to the observed relation in both slope and normalization. This result suggests that the central black holes in galaxies gain most of their mass in phases of super-Eddington accretion, which are presumably obscured or at high redshift. Observed super-Eddington quasars are apparently late in growing their black hole masses. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP King, A (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. NR 19 TC 356 Z9 358 U1 1 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2003 VL 596 IS 1 BP L27 EP L29 DI 10.1086/379143 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DT UT WOS:000185814500007 ER PT J AU Kuchner, MJ AF Kuchner, MJ TI Volatile-rich earth-mass planets in the habitable zone SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; planetary systems ID GALILEAN SATELLITES; IMPACT EROSION; GIANT PLANETS; SOLAR NEBULA; ATMOSPHERES; EVOLUTION; SYSTEMS; JUPITER; INSTABILITIES; COMPANION AB A small planet is not necessarily a terrestrial planet. Planets that form beyond the snow line with too little mass to seed rapid gas accretion (less than or similar to 10(+)) should be rich in volatile ices like H2O and NH3. Some of these planets should migrate inward by interacting with a circumstellar disk or with other planets. Such objects can retain their volatiles for billions of years or longer at similar to 1 AU as their thick steam atmospheres undergo slow hydrodynamic escape. These objects could appear in future surveys for extrasolar Earth analogs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kuchner, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Kuchner, Marc/E-2288-2012 NR 47 TC 72 Z9 72 U1 0 U2 6 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 2003 VL 596 IS 1 BP L105 EP L108 DI 10.1086/378397 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DT UT WOS:000185814500027 ER PT J AU Lecar, M Sasselov, DD AF Lecar, M Sasselov, DD TI Dispersing the gaseous protoplanetary disk and halting type II migration SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation; planetary systems : protoplanetary disks ID PLANET MIGRATION; MASS; NEBULA AB More than 30 extrasolar Jupiter-like planets have shorter periods than the planet Mercury. It is generally accepted that they formed farther out, past the "snow line" (similar to 1 AU), and migrated inward. In order to be driven by tidal torques from the gaseous disk, the disk exterior to the planet had to contain about a planetary mass. The fact that the planets stopped migrating means that their outer disk was removed. We suggest, following the simulation by Kley and Bate et al., that the outer disk was accreted by the planet. This not only halts migration but removes the outer disk. For planets exterior to about 2 AU, the outer disk could have been removed by photoevaporation (Matsuyama et al.). Furthermore, as also shown by Bate et al., this process also provides an upper limit to planetary masses in agreement with the analysis of observed planetary masses by Zucker & Mazeh. In this scenario, the endgame is a race. The central star is accreting the inner disk and the planet, while the planet is accreting the outer disk. The planet survives if it accretes its outer disk before being accreted by the star. The winner is determined solely by the ratio of the mass of the outer disk to the local surface density of the disk. Some planets certainly lose the race and are eaten by the central star. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lecar, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 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 OCT 10 PY 2003 VL 596 IS 1 BP L99 EP L100 DI 10.1086/379207 PN 2 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 730DT UT WOS:000185814500025 ER PT J AU Sanchez, JA Lasker, HR AF Sanchez, JA Lasker, HR TI Patterns of morphological integration in marine modular organisms: supra-module organization in branching octocoral colonies SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE modularity; phenotypic integration; branching colonies; octocoral; phylogeny; comparative analysis ID PHENOTYPIC INTEGRATION; ARABIDOPSIS-THALIANA; HOX GENES; EVOLUTION; EXPRESSION; ALLOMETRY; PHYLOGENIES; CNOX-2 AB Despite the relative simplicity of their modular growth, marine invertebrates such as arborescent gorgonian octocorals (Octocorallia: Cnidaria) generate complex colonial forms. Colony form in these taxa is a consequence of modular (polyp) replication, and if there is a tight integration among modular and supramodular traits (e.g. polyp aperture, inter-polyp spacing, branch thickness, internode and branch length), then changes at the module level may lead to changes in colony architecture. Alternatively, different groups of traits may evolve semi-independently (or conditionally independent). To examine the patterns of integration among morphological traits in Caribbean octocorals, we compared five morphological traits across 21 species, correcting for the effects of phylogenetic relationships among the taxa. Graphical modelling and phylogenetic independence contrasts among the five morphological characters indicate two groups of integrated traits based on whether they were polyp- or colony-level traits. Although all characters exhibited bivariate associations, multivariate analyses (partial correlation coefficients) showed the strongest integration among the colony-level characters (internode distance and branch length). It is a quantitative demonstration that branching characters within the octocorals studied are independent of characters of the polyps. Despite the universally recognized modularity of octocorals at the level of polyps, branching during colony development may represent an emergent level of integration and modularity. C1 SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA. RP Sanchez, JA (reprint author), Smithsonian Inst, Dept Systemat Biol, NMNH, POB 37012,MRC-0163, Washington, DC 20013 USA. EM sanchez.juan@nmnh.si.edu NR 37 TC 41 Z9 43 U1 3 U2 7 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 2003 VL 270 IS 1528 BP 2039 EP 2044 DI 10.1098/rspb.2003.2471 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 728WP UT WOS:000185739600008 PM 14561292 ER PT J AU Hershler, R Frest, TJ Liu, HP Johannes, EJ AF Hershler, R Frest, TJ Liu, HP Johannes, EJ TI Rissooidean snails from the Pit River basin, California SO VELIGER LA English DT Article ID WESTERN UNITED-STATES; FRESH-WATER SNAILS; PHYLOGENETIC-RELATIONSHIPS; MITOCHONDRIAL-DNA; GENUS PYRGULOPSIS; GREAT-BASIN; HYDROBIIDAE; GASTROPODA; TRYONIA; REGION AB A recent field survey of the Pit River basin in northeastern California resulted in the discovery of numerous undescribed populations of aquatic rissooidean snails which are treated in this paper. Based on morphological study and analysis of mitochondrial DNA sequences we describe a new species of the genus Colligyrus (family Amnicolidae) and four new species of the genus Pyrgulopsis (Hydrobiidae). Phylogenetic analysis of sequence data suggests that the new species of Colligyrus is sister to an undescribed congener from the Klamath basin. The four new species of Pyrgulopsis do not form a monophyletic group but instead are variously related to other regional congeners. We also describe Pit River basin populations of two species of Pyrgulopsis which were previously considered to be endemic to the northwestern Great Basin (P. eremica) and Klamath basin (P. archimedis). C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. DEIXIS Consultants, Seattle, WA 98115 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Systemat Biol, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. NR 50 TC 18 Z9 18 U1 0 U2 0 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 OCT 6 PY 2003 VL 46 IS 4 BP 275 EP 304 PG 30 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 732EJ UT WOS:000185927600001 ER PT J AU Losi, CJ Siccama, TG Condit, R Morales, JE AF Losi, CJ Siccama, TG Condit, R Morales, JE TI Analysis of alternative methods for estimating carbon stock in young tropical plantations SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE carbon sequestration; techniques; carbon; biomass; allometric equations AB Estimates of carbon stock in forest plantations are generally based on allometric equations relating either carbon or biomass to diameter at breast height (DBH). These equations are usually based on measurement of the fresh mass of each tree with sub-samples taken to determine moisture content to convert to dry weight. However, drying time and the number of sub-samples varies between studies. Furthermore, the carbon concentration of different tree parts is rarely measured directly, but generally assumed to be 50% of dry weight. This study analyzed those assumptions and determined their effect on regression equations and on species-specific stand level estimates of carbon stock for Anacardium excelsum and Dipteryx panamensis growing in 7-year-old mixed-species plantations in Panama. Four methods were used to develop above ground carbon estimates for the same sample of trees. Results indicated that the drying time, the number of sub-samples taken, and whether or not carbon was measured directly had only a small effect on the estimate of carbon stock for the entire cohort of trees. None of the methods developed using the same sample of Panamanian trees gave stand level estimates of carbon stock that differed by more than 10% from the best estimate for either species. Another sample of slightly larger D. panamensis trees growing in 5- and 6-year-old mixed-species plantations in Costa Rica [J. Trop. For. Sci. 13 (3) (2001) 450] was used to develop a second set of regression equations. We hypothesized that a regression equation would give a more accurate estimate of carbon stock if the range of tree sizes used to produce the regression more closely matched the range of sizes that the regression was being applied to. When the Costa Rican equation developed using the full range of trees was compared to a Panamanian equation developed using the full range of tree diameters that we sampled, the estimates of carbon stock for the Panamanian plantation differed by 10.2%. However, when two additional regression equations were created using the range of tree diameters that overlapped, the estimates of carbon stock for the Panamanian plantation differed by only 5.2%, supporting our hypothesis. (C) 2003 Elsevier Science B.V. All rights reserved. C1 Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. RP Losi, CJ (reprint author), Allegheny Natl Forest, Bradford Dist,HC 1 Box 88, Bradford, PA 16701 USA. NR 13 TC 34 Z9 40 U1 0 U2 12 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 OCT 3 PY 2003 VL 184 IS 1-3 BP 355 EP 368 DI 10.1016/S0378-1127(03)00160-9 PG 14 WC Forestry SC Forestry GA 718WZ UT WOS:000185170600028 ER PT J AU Mulhern, DM Ubelaker, DH AF Mulhern, DM Ubelaker, DH TI Histologic examination of bone development in juvenile chimpanzees SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE osteon; bone microstructure; hominoid; Pan troglodytes ID DENTAL DEVELOPMENT; CORTICAL BONE; PAN-TROGLODYTES; AGE; GROWTH; DEATH; HOMO AB The purpose of this study is to determine whether histologic skeletal development in chimpanzees (Pan troglodytes) differs from that in humans. Currently, minimal quantitative data are available on the bone histology of great apes. In addition to providing baseline data on juvenile chimpanzee bone histology, the data generated by this study have potential applications for studying the comparative development between chimpanzees and humans and other primates, as well as investigating the evolution of human bone development, differences in development among limb elements, and differences in histology related to locomotor function. The study sample includes thin sections from the femoral, tibial, and fibular midshafts of 13 chimpanzees originally prepared by Kerley ([1966] Tulane Stud. Zool. 13:71-82) as part of a study on skeletal age changes in the chimpanzee. Twelve juveniles, ranging in known age from 2-15.3 years, and one adult, with a known age of 35 years, are represented. For each specimen, numbers of osteons, osteon fragments, and non-Haversian canals were counted, and percent lamellar bone was estimated. Results were compared with data extracted from Kerley ([1965] Am. J. Phys. Anthropol. 23:149-164) on a juvenile human sample. Results indicate that juvenile chimpanzees and humans exhibit similar age-related changes in histologic variables. However, age is not as strong a predictor of variation in microstructural variables in chimpanzees as it is in humans. (C) 2003 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Mulhern, DM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012,NMNH MRC 138, Washington, DC 20013 USA. NR 24 TC 15 Z9 15 U1 0 U2 6 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 OCT PY 2003 VL 122 IS 2 BP 127 EP 133 DI 10.1002/ajpa.10294 PG 7 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 722VZ UT WOS:000185399900004 PM 12949833 ER PT J AU Koch-Muller, M Dera, P Fei, YW Reno, B Sobolev, N Hauri, E Wysoczanski, R AF Koch-Muller, M Dera, P Fei, YW Reno, B Sobolev, N Hauri, E Wysoczanski, R TI OH- in synthetic and natural coesite SO AMERICAN MINERALOGIST LA English DT Article ID ELECTRON LOCALIZATION FUNCTION; EARTHS DEEP INTERIOR; HIGH-PRESSURE; QUANTITATIVE-ANALYSIS; SILICA POLYMORPHS; X-RAY; MANTLE; HYDROXYL; MINERALS; PYROPE AB The incorporation of hydrogen into the coesite structure was investigated at pressures ranging from 4.0-9.0 GPa and temperatures from 750-1300 degreesC using Al and B doped SiO2 starting materials. The spectra show four sharp bands (nu(1), nu(2a), nu(2b), and nu(3)) in the energy range of 3450-3580 cm(-1), consistent with the hydrogarnet substitution [Si4+(T2) + 4O(2-) = va(T2) + 4OH(-)], two weak sharp bands at 3537 and 3500 cm(-1) (nu(6a) and nu(6b)) attributed to B-based point defects, and two weaker and broad bands at 3300 and 3210 cm(-1) (nu(4) and nu(5)) attributed to substitution of Si4+ by Al3+ + H. More than 80% of the dissolved water is incorporated via the hydrogarnet substitution mechanism. The hydrogen solubility in coesite increases with pressure and temperature. At 7.5 GPa and 1100 degreesC, 1335 H/10(6) Si is incorporated into the coesite structure. At 8.5 GPa and 1200 degreesC, the incorporation mechanism changes: in the IR spectra four new sharp bands appear in the energy range of 3380-3460 cm(-1) (nu(7)-nu(10)) and the nu(1)-nu(3) bands disappear. Single crystal X-ray diffraction, Raman spectroscopy, polarized single-crystal and in situ high-pressure FTIR spectroscopy confirm that the new bands are due to OH- in coesite. The polarization and high-pressure behavior of the nu(7)-nu(10) OH bands is quite different from that of the nu(1)-nu(3) bands, indicating that the H incorporation in coesite changes dramatically at these P and T conditions. Quantitative determination of hydrogen solubility in synthetic coesite as a function of pressure, temperature, and chemical impurity allow us to interpret observations in natural coesite. Hydrogen has not previously been detected in natural coesite samples from ultra high-pressure metamorphic rocks. In this study, we report the first FTIR spectrum of a natural OH-bearing coesite. The dominant substitution mechanism in this sample is the hydrogarnet substitution and the calculated hydrogen content is about 900 zeta+/- 300 H/10(6) Si. The coesite occurs as an inclusion in diamond together with an OH-bearing omphacite. The shift of the OH-bands of coesite and omphacite to lower energies indicates that the minerals are still under confining pressure. C1 Geoforschungszentrum Potsdam, Sekt 4 1, D-14473 Potsdam, Germany. Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. Trinity Univ, Dept Geosci, San Antonio, TX 78212 USA. Russian Acad Sci, Siberian Branch, Inst Mineral & Petrog, Novosibirsk 630090, Russia. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Koch-Muller, M (reprint author), Geoforschungszentrum Potsdam, Sekt 4 1, D-14473 Potsdam, Germany. RI Wysoczanski, Richard/C-2930-2009; Fei, Yingwei/F-3709-2011; Wysoczanski, Richard/I-7730-2012; Dera, Przemyslaw/F-6483-2013 OI Fei, Yingwei/0000-0001-9955-5353; NR 36 TC 30 Z9 33 U1 0 U2 5 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD OCT PY 2003 VL 88 IS 10 BP 1436 EP 1445 PG 10 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 731PK UT WOS:000185895500008 ER PT J AU Knowlton, N Rohwer, F AF Knowlton, N Rohwer, F TI Multispecies microbial mutualisms on coral reefs: The host as a habitat SO AMERICAN NATURALIST LA English DT Article DE microbe; zooxanthellae; reef; mutualism; bacteria ID GYMNODINIUM MICROADRIATICUM FREUDENTHAL; FIXATION ACETYLENE-REDUCTION; SYMBIODINIUM-MICROADRIATICUM; MARINE-INVERTEBRATES; GENUS SYMBIODINIUM; GENETIC-VARIATION; BACTERIAL COMMUNITIES; MONTASTRAEA-ANNULARIS; SYMBIONT SPECIFICITY; PHOTOSYSTEM-II AB Reef-building corals associate with a diverse array of eukaryotic and noneukaryotic microbes. Best known are dinoflagellates in the genus Symbiodinium ("zooxanthellae"), which are photosynthetic symbionts found in all reef-building corals. Once considered a single species, they are now recognized as several large, genetically diverse groups that often co-occur within a single host species or colony. Variation among Symbiodinium in host identities, tolerance to stress, and ability to colonize hosts has been documented, but there is little information on the ecology of zooxanthellar free-living stages and how different zooxanthellae perform as partners. Other microbial associates of reef corals are much less well known, but studies indicate that individual coral colonies host diverse assemblages of bacteria, some of which seem to have species-specific associations. This diversity of microbial associates has important evolutionary and ecological implications. Most mutualisms evolve as balanced reciprocations that allow partners to detect cheaters, particularly when partners are potentially diverse and can be transmitted horizontally. Thus, environmental stresses that incapacitate the ability of partners to reciprocate can destabilize associations by eliciting rejection by their hosts. Coral bleaching (the loss of zooxanthellae) and coral diseases, both increasing over the last several decades, may be examples of stress-related mutualistic instability. C1 Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. RP Knowlton, N (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers, La Jolla, CA 92093 USA. NR 77 TC 169 Z9 171 U1 9 U2 95 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 2003 VL 162 IS 4 SU S BP S51 EP S62 DI 10.1086/378684 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 744XJ UT WOS:000186657900005 PM 14583857 ER PT J AU Pisani, A Ramella, M Geller, MJ AF Pisani, A Ramella, M Geller, MJ TI The mass function and distribution of velocity dispersions for UZC groups of galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology : observations; cosmology : theory; galaxies : clusters : general large-scale structure of universe ID REDSHIFT-SPACE NEIGHBORHOODS; RAY TEMPERATURE FUNCTION; FLUX-LIMITED SAMPLE; X-RAY; LOOSE GROUPS; LUMINOSITY FUNCTION; POWER-SPECTRUM; RICH CLUSTERS; NEARBY GROUPS; HIERARCHICAL UNIVERSE AB We measure the distribution of velocity dispersions of groups of galaxies identified in the Updated Zwicky Catalog, and we use the distribution to derive the group mass function. We introduce a new method that makes efficient use of the entire magnitude-limited catalog. Our determination of n(greater than or equal tosigma(T)) includes a significant contribution from low-luminosity systems that would be missing in a volume-limited sample. We start from a model for the probability density function of the total number of group members and reproduce the observed distribution. We take several effects, such as the local fluctuations in volume density, limited sampling, and group selection, into account. We estimate the relation between total number of members, total luminosity, and true velocity dispersion. We can then reproduce not only the observed distribution of sigma(v), but also the distributions of the number of group members, the total group luminosity, and virial mass. The best fit to the data in the true velocity dispersion range 100 km s(-1) less than or equal to sigma(T) less than or equal to 750 km s(-1) is a power-law model with a slope d log n(greater than or equal tosigma(T))/d log sigma(T) = -3.4 (-2.1, -5) and a normalization n(sigma(T) greater than or equal to 750 km s(-1)) = (1.27 +/- 0.21) x 10(-5) h(3) Mpc(-3), where sigma(T) is the true velocity dispersion of a group. The predictions of cold dark matter models are consistent with the mass function we derive from this distribution of velocity dispersions. C1 Univ Trieste, Dipartimento Astron, I-34131 Trieste, Italy. Sci Duca Abruzzi & Magistrale S Slataper, Ist Istruz Statale Class Dante Alighieri, I-34170 Gorizia, Italy. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Pisani, A (reprint author), Univ Trieste, Dipartimento Astron, Via GB Tiepolo 11, I-34131 Trieste, Italy. OI Ramella, Massimo/0000-0001-5446-4749 NR 68 TC 12 Z9 13 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 2003 VL 126 IS 4 BP 1677 EP 1689 DI 10.1086/377621 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TM UT WOS:000185676200003 ER PT J AU Strateva, IV Strauss, MA Hao, L Schlegel, DJ Hall, PB Gunn, JE Li, LX Ivezic, Z Richards, GT Zakamska, NL Voges, W Anderson, SF Lupton, RH Schneider, DP Brinkmann, J Nichol, RC AF Strateva, IV Strauss, MA Hao, L Schlegel, DJ Hall, PB Gunn, JE Li, LX Ivezic, Z Richards, GT Zakamska, NL Voges, W Anderson, SF Lupton, RH Schneider, DP Brinkmann, J Nichol, RC TI Double-peaked low-ionization emission lines in active galactic nuclei SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : active; accretion disks ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; ACCRETION DISKS; RADIO GALAXIES; BLACK-HOLE; 3C 390.3; 1ST SURVEY; LONG-TERM; REGION; PROFILES AB We present a new sample of 116 double-peaked Balmer line active galactic nuclei (AGNs) selected from the Sloan Digital Sky Survey. Double-peaked emission lines are believed to originate in the accretion disks of AGNs, a few hundred gravitational radii (R-G) from the supermassive black hole. We investigate the properties of the candidate disk emitters with respect to the full sample of AGNs over the same redshifts, focusing on optical, radio, and X-ray flux, broad-line shapes and narrow-line equivalent widths, and line flux ratios. We find that the disk emitters have medium luminosities (similar to10(44) ergs s(-1)) and FWHM on average 6 times broader than the AGNs in the parent sample. The double-peaked AGNs are 1.6 times more likely to be radio sources and are predominantly (76%) radio-quiet, with about 12% of the objects classified as LINERs. Statistical comparison of the observed double-peaked line profiles with those produced by axisymmetric and nonaxisymmetric accretion disk models allows us to impose constraints on accretion disk parameters. The observed Halpha line profiles are consistent with accretion disks with inclinations smaller than 50degrees, surface emissivity slopes of 1.0-2.5, outer radii larger than similar to2000R(G), inner radii of (200-800) R-G, and local turbulent broadening of 780-1800 km s(-1). The comparison suggests that 60% of accretion disks require some form of asymmetry ( e. g., elliptical disks, warps, spiral shocks, or hot spots). C1 Princeton Univ Observ, Princeton, NJ 08544 USA. Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 504, University Pk, PA 16802 USA. Apache Point Observ, Sunspot, NM 88349 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Strateva, IV (reprint author), Princeton Univ Observ, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA. NR 89 TC 140 Z9 140 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 OCT PY 2003 VL 126 IS 4 BP 1720 EP 1749 DI 10.1086/378367 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TM UT WOS:000185676200007 ER PT J AU Lacy, CHS Torres, G Claret, A Sabby, JA AF Lacy, CHS Torres, G Claret, A Sabby, JA TI Absolute properties of the main-sequence eclipsing binary star BP Vulpeculae SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : evolution; stars : fundamental parameters; stars : individual (BP Vulpeculae) ID LIMB-DARKENING COEFFICIENTS; LIGHT CURVES; SYNCHRONIZATION TIMES; PHOTOMETRY; CIRCULARIZATION; SYSTEMS AB We present 5236 differential observations in the V filter measured by a robotic telescope, as well as radial velocities from spectroscopic observations, of the detached, eccentric 1.9 day double-lined eclipsing binary star BP Vul. Absolute dimensions of the components are determined with high precision (better than 1% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 1.737 +/- 0.015 M. and 1.852 +/- 0.014 R. for the primary, and 1.408 +/- 0.009 M. and 1.489 +/- 0.014 R. for the secondary. The effective temperatures and interstellar reddening of the stars are accurately determined from uvbybeta photometry: 7700 +/- 150 K for the primary, 6800 +/- 150 K for the secondary-corresponding to spectral types of A7m and F2m-and 0.022 mag for Eb-y. The metallic-lined character of the stars is revealed by high-resolution spectroscopy and uvbybeta photometry. Spectral line widths give rotational velocities that are synchronous with the orbital motion for the secondary component, but subsynchronous for the primary component, in a slightly eccentric orbit (e = 0.0345). Apsidal motion based on times of minimum light appears to be negative with a period of about 75 years based on recent observations of minima, but this result is not confirmed by the radial velocity measurements, and it is indeterminate when older photographic and visual data are included. The components of BP Vul are main-sequence stars with an age of about 1 Gyr according to models. C1 Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. RP Lacy, CHS (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. NR 38 TC 13 Z9 14 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 2003 VL 126 IS 4 BP 1905 EP 1915 DI 10.1086/378058 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TM UT WOS:000185676200020 ER PT J AU Porras, A Christopher, M Allen, L Di Francesco, J Megeath, ST Myers, PC AF Porras, A Christopher, M Allen, L Di Francesco, J Megeath, ST Myers, PC TI A catalog of young stellar groups and clusters within 1 kiloparsec of the Sun SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : general; open clusters and associations : general; stars : formation ID VELA MOLECULAR CLOUDS; STAR-FORMING REGIONS; NEAR-INFRARED IMAGES; HERBIG-AE/BE STARS; IR IMAGING PHOTOMETRY; ORION TRAPEZIUM CLUSTER; BRIGHT-RIMMED CLOUDS; OPHIUCHI DARK CLOUD; MAIN-SEQUENCE STARS; RHO-OPHIUCHI AB We present a catalog of near-infrared surveys of young (less than or similar to a few 10(6) yr) stellar groups and clusters within 1 kpc from the Sun, based on an extensive search of the literature from the past ten years. We find 143 surveys from 69 published articles, covering 73 different regions. The number distribution of stars in a region has a median of 28 and a mean of 100. About 80% of the stars are in clusters with at least 100 members. By a rough classification of the groups and clusters based on the number of their associated stars, we show that most of the stars form in large clusters. The spatial distribution of cataloged regions in the Galactic plane shows a relative lack of observed stellar groups and clusters in the range 270degrees < l < 60degrees of Galactic longitude, reflecting our location between the Local and Sagittarius arms. This compilation is intended as a useful resource for future studies of nearby young regions of multiple star formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Porras, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 87 TC 99 Z9 99 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2003 VL 126 IS 4 BP 1916 EP 1924 DI 10.1086/377623 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TM UT WOS:000185676200021 ER PT J AU Fiore, F Elvis, M Maiolino, R Nicastro, F Siemiginowska, A Stratta, G D'Elia, V AF Fiore, F Elvis, M Maiolino, R Nicastro, F Siemiginowska, A Stratta, G D'Elia, V TI The X-ray absorber of PKS 2126-158 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE quasars : general; X-rays : galaxies ID HIGH-REDSHIFT QUASARS; LY-ALPHA SYSTEMS; ENERGY CONCENTRATOR SPECTROMETER; SPECTRUM RADIO-SOURCES; ASTRONOMY SATELLITE; METAL ABUNDANCES; HIGH-RESOLUTION; WGACAT QUASARS; STAR-FORMATION; ON-BOARD AB BeppoSAX observed the z = 3.27 quasar PKS 2126-158 on May 24-28 1999 when its 2-10 keV and 0.1-2.5 keV fluxes were 1.1 X 10(-11) and 4.4 X 10(-12) erg cm(-2) s(-1) respectively, a factor of 2 higher than in all previous ROSAT and ASCA observations and 40% higher than in two more recent Chandra and XMM-Newton observations. The shortest detected rest frame variability timescale is of a few months, comparable to the causal timescale associated with an emission region of similar to10 Schwarzschild radii around a fewX10(10) M. black hole. The source is detected with a signal to noise ratio S/N greater than or similar to 3 up to similar to50 keV, 215 keV rest frame. The BeppoSAX observations confirm the presence of low energy absorption along the line of sight, independent of the continuum model adopted, at a high confidence level. Despite the limited spectral resolution of the BeppoSAX LECS and MECS it is possible to put constraints on different absorption and continuum models, but not to unambiguously determine the redshift of the absorber. If the absorber is not significantly ionized the BeppoSAX data do prefer an absorber at z less than or similar to 2.7. Strong and complex metal line systems along the line of sight to PKS 2126-158 have been found at z = 0.6631 and at 2.64 < z < 2.82. They could well be associated with the X-ray absorption. Conversely, an ionized ("warm") absorber at the quasar redshift provides a good fit only if the iron abundance is smaller than similar to0.3 solar, while that of the other elements is fixed to the solar value. Lower iron metallicity would imply a lower dust to gas ratio, since iron aggregates easily in dust. This can help in solving the apparent paradox of the lack of significant ultraviolet reddening in this source while strong absorption is detected in X-rays. Low iron abundance would be at odds with the supersolar abundances derived from the broad emission lines. C1 Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Univ Roma La Sapienza, I-00185 Rome, Italy. RP Fiore, F (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. RI Stratta, Maria Giuliana/L-3045-2016; OI Stratta, Maria Giuliana/0000-0003-1055-7980; D'Elia, Valerio/0000-0002-7320-5862; Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 44 TC 7 Z9 7 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 2003 VL 409 IS 1 BP 57 EP 64 DI 10.1051/0004-6361:20031018 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 721LQ UT WOS:000185318200006 ER PT J AU Fiore, F Brusa, M Cocchia, F Baldi, A Carangelo, N Ciliegi, P Comastri, A La Franca, F Maiolino, R Matt, G Molendi, S Mignoli, M Perola, GC Severgnini, P Vignali, C AF Fiore, F Brusa, M Cocchia, F Baldi, A Carangelo, N Ciliegi, P Comastri, A La Franca, F Maiolino, R Matt, G Molendi, S Mignoli, M Perola, GC Severgnini, P Vignali, C TI The HELLAS2XMM survey - IV. Optical identifications and the evolution of the accretion luminosity in the Universe SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-ray : diffuse background; X-ray : galaxies; quasars : general; surveys ID LARGE-AREA SURVEY; X-RAY SOURCES; STAR-FORMATION HISTORY; FIELD NORTH SURVEY; ROSAT DEEP SURVEY; SPECTRAL PROPERTIES; MULTIWAVELENGTH OBSERVATIONS; REDSHIFT EVOLUTION; SPACE DISTRIBUTION; SOURCE POPULATION AB We present results from the photometric and spectroscopic identification of 122 X-ray sources recently discovered by XMM-Newton in the 2-10 keV band (the HELLAS2XMM 1dF sample). Their flux cover the range 8 X 10(-15)-4 X 10(-13) erg cm(-2) s(-1) and the total area surveyed is 0.9 square degrees. One of the most interesting results (which is found also in deeper sourveys) is that about 20% of the hard X-ray selected sources have an X-ray to optical flux ratio (X/O) ten times or more higher than that of optically selected AGN. Unlike the faint sources found in the ultra-deep Chandra and XMM-Newton surveys, which reach X-ray (and optical) fluxes more than one order of magnitude lower than the HELLAS2XMM survey sources, many of the extreme X/O sources in our sample have R less than or similar to 25 and are therefore accessible to optical spectroscopy. We report the identification of 13 sources with X/O greater than or similar to 10 (to be compared with 9 sources known from the deeper, pencil-beam surveys). Eight of them are narrow line QSO (seemingly the extension to very high luminosity of the type 2 Seyfert galaxies), four are broad line QSO. The results from our survey are also used to make reliable predictions about the luminosity of the sources not yet spectroscopically identified, both in our sample and in deeper Chandra and XMM-Newton samples. We then use a combined sample of 317 hard X-ray selected sources (HELLAS2XMM 1dF, Chandra Deep Field North 1Msec, Chandra SSA13 and XMM-Newton Lockman Hole flux limited samples), 221 with measured redshifts, to evaluate the cosmological evolution of the hard X-ray source's number and luminosity densities. Looking backward in time, the low luminosity sources (log L2-10 keV = 43-44 erg s(-1)) increase in number at a much slower rate than the very high luminosity sources (log L2-10 keV > 44.5 erg s(-1)), reaching a maximum around z = 1 and then levelling off beyond z = 2. This translates into an accretion driven luminosity density which is dominated by sources with log L2-10 keV < 44.5 erg s(-1) up to at least z = 1, while the contribution of the same sources and of those with log L2-10 keV > 44.5 erg s(-1) appear, with yet rather large uncertainties, to be comparable between z = 2 and 4. C1 Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. CNR, IASF, Milan, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Osserv Astron Brera, INAF, I-20121 Milan, Italy. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Fiore, F (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. EM fiore@mporzio.astro.it RI La Franca, Fabio/G-9631-2012; Vignali, Cristian/J-4974-2012; Mignoli, Marco/O-9426-2015; Comastri, Andrea/O-9543-2015; OI Vignali, Cristian/0000-0002-8853-9611; Fiore, Fabrizio/0000-0002-4031-4157; Mignoli, Marco/0000-0002-9087-2835; Comastri, Andrea/0000-0003-3451-9970; Ciliegi, Paolo/0000-0002-0447-4620; Severgnini, Paola/0000-0001-5619-5896; La Franca, Fabio/0000-0002-1239-2721; Molendi, Silvano/0000-0002-2483-278X; Brusa, Marcella/0000-0002-5059-6848 NR 54 TC 222 Z9 222 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2003 VL 409 IS 1 BP 79 EP 90 DI 10.1051/0004-6361:20031031 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 721LQ UT WOS:000185318200008 ER PT J AU Li, LX Ostriker, JP AF Li, LX Ostriker, JP TI Gravitational lensing by a compound population of halos: Standard models SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : halos; gravitational lensing ID COLD DARK-MATTER; DIGITAL SKY SURVEY; SUPERMASSIVE COMPACT OBJECTS; GALAXY REDSHIFT SURVEY; DENSITY PROFILE; COSMOLOGICAL ABUNDANCE; ENERGY COMPONENT; POWER SPECTRUM; CLUSTER SURVEY; MASS PROFILES AB Based on observed rotation curves of galaxies and theoretical simulations of dark matter halos, there are reasons for believing that at least three different types of dark matter halos exist in the universe classified by their masses M and the inner slope of mass density -alpha: population A (galaxies): 10(10) h(-1) M(.) less than or similar to M less than or equal to 2 x 10(13) h(-1) M(.), alpha approximate to 2; population B (cluster halos): M greater than or similar to 2 x 10(13) h(-1) M(.), alpha approximate to 1.3; and population C (dwarf halos): M less than or similar to 10(10) h(-1) M(.), alpha approximate to 1.3. In this paper we calculate the lensing probability produced by such a compound population of dark halos for both image separation and time delay, assuming that the mass function of halos is given by the Press-Schechter function and the universe is described by a cold dark matter (CDM) LCDM, OCDM, or SCDM model. The LCDM model is normalized to the Wilkinson Microwave Anisotropy Probe observations; OCDM and SCDM models are normalized to the abundance of rich clusters. We compare the predictions of the different cosmological models with observational data and show that both LCDM and OCDM models are marginally consistent with the current available data, but the SCDM model is ruled out. The fit of the compound model to the observed correlation between splitting angle and time delay is excellent, but the fit to the number versus splitting angle relation is only adequate using the small number of sources in the objective Jodrell-VLA Astrometric Survey/Cosmic Lens All-Sky Survey. A larger survey of the same type would have great power in discriminating among cosmological models. Furthermore, population C in a LCDM model has a unique signature in the time domain, an additional peak at similar to3 s potentially observable in GRBs, which makes it distinguishable from variants of CDM scenarios, such as warm dark matter, repulsive dark matter, or collisional dark matter. For image separations greater than 1000 the differently normalized LCDM models predict significantly different lensing probabilities, affording an additional lever to break the degeneracies in the CMB determination of cosmological parameters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Li, LX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lli@cfa.harvard.edu; jpo@ast.cam.ac.uk NR 70 TC 23 Z9 23 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2003 VL 595 IS 2 BP 603 EP 613 DI 10.1086/377489 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TJ UT WOS:000185675800003 ER PT J AU Siemiginowska, A Stanghellini, C Brunetti, G Fiore, F Aldcroft, TL Bechtold, J Elvis, M Murray, SS Antonelli, LA Colafrancesco, S AF Siemiginowska, A Stanghellini, C Brunetti, G Fiore, F Aldcroft, TL Bechtold, J Elvis, M Murray, SS Antonelli, LA Colafrancesco, S TI Chandra discovery of an X-ray jet and extended X-ray structure in the z=0.63 quasar B2 0738+313 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : individual (B2 0738+313); X-rays : galaxies ID SPECTRUM RADIO-SOURCES; ACTIVE GALACTIC NUCLEI; LY-ALPHA ABSORPTION; VLA OBSERVATIONS; COMPLETE SAMPLE; ACCRETION DISK; STEEP-SPECTRUM; EMISSION; GHZ; PERFORMANCE AB We have made a similar to 30 ks Chandra observation of the redshift z = 0.63 gigahertz-peaked spectrum (GPS) quasar B2 0738+313. We detected X-ray emission from the core and have discovered a 200 kpc (projected on the sky) X-ray jet. The X-ray jet is narrow and curves, following the extended radio structure to the south of the quasar, and ending with a hot spot at the southernmost part of the radio lobe. The jet has a knot at similar to13" away from the core. The knot emission is consistent with the X-rays being created by the inverse Compton scattering of the cosmic microwave background (CMB) photons and requires jet bulk Lorentz factors of a few (Gamma(bulk) similar to 5-7). We discuss the emission mechanisms that may be responsible for the jet emission. We present new VLA data of the core and jet, and discuss the relation between the extended radio and X-ray emission. Extended emission observed in several GPS sources has been interpreted as a signature of the source past activity, while the GPS source is young and newly expanded. We argue that B2 0738+313 may be an example of a new class of radio sources similar to the FR II radio galaxies in their high jet bulk velocities, but with a powerful GPS-like nucleus. B2 0738+ 313 also has two damped Lyalpha systems along the line of sight, at z(abs) = 0.0912 and 0.2212. We discuss the possible connection between the X-ray absorption (7.2 +/- 0.9 x 10(20) cm(-2)) detected in the ACIS spectrum and these two intervening absorbers. We also investigate an extended structure within the central 10" of the core in the relation to structure seen in the optical. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist Radioastron, Noto, Italy. CNR, Ist Radioastron, I-40126 Bologna, Italy. Osserv Astron Roma, INAF, I-00136 Rome, Italy. Univ Arizona, Steward Observ, Tucson, AZ USA. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Stanghellini, Carlo/0000-0002-6415-854X; Fiore, Fabrizio/0000-0002-4031-4157 NR 48 TC 27 Z9 27 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 2003 VL 595 IS 2 BP 643 EP 655 DI 10.1086/377369 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TJ UT WOS:000185675800007 ER PT J AU Uttley, P Fruscione, A McHardy, I Lamer, G AF Uttley, P Fruscione, A McHardy, I Lamer, G TI Catching NGC 4051 in the low state with Chandra SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4051); galaxies : Seyfert; X-rays : galaxies ID X-RAY VARIABILITY; SEYFERT 1 GALAXIES; SPECTRAL VARIABILITY; ASCA OBSERVATIONS; BLACK-HOLE; SWAN SONG; IRON LINE; NGC 4051; MCG-6-30-15; REFLECTION AB We report the results from a Chandra target-of-opportunity observation of the low-luminosity narrow-line Seyfert 1 galaxy NGC 4051, obtained during a 6 week duration low-flux state in 2001 February. During the Chandra observation, the 2 - 10 keV source flux was 7 x 10(-12) ergs cm(-2) s(-1), corresponding to a 2 - 10 keV luminosity of similar to8 x 10(40) ergs s(-1). We confirm the absence of strong extended soft X-ray emission in NGC 4051 and that the low-state spectrum is dominated by the central point source. The X-ray spectrum has an unusual, hybrid shape, very soft below similar to3 keV (and which we model with a blackbody of temperature of 0.14 keV) and very hard at higher energies (power-law slope of Gamma similar to 1). The light curves in both soft and hard bands are significantly variable and correlated, implying a connection between hard and soft components and proving that the hard component is dominated by primary continuum emission and is not due to pure reflection from distant cold material. However, a comparison with RXTE data obtained during the same 2001 low state suggests the presence of unusually prominent disk reflection features, which may help to explain the apparent upward curvature and extreme hardness of the Chandra spectrum above a few keV. The shape of the 2001 low-state spectrum is consistent with that observed in a brief (< 3 days) low-flux excursion during the source's normal state in 2000 April, suggesting that emission processes during the low state are not significantly different to those in the normal state. The unusual spectral shape observed in the low state may be a continuation to low fluxes of the normal, flux-dependent spectral variability of the source. C1 Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. RP Uttley, P (reprint author), Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. EM pu@astro.soton.ac.uk; antonell@head-cfa.harvard.edu; imh@astro.soton.ac.uk; glamer@aip.de NR 23 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2003 VL 595 IS 2 BP 656 EP 664 DI 10.1086/377468 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TJ UT WOS:000185675800008 ER PT J AU Grogin, NA Koekemoer, AM Schreier, EJ Bergeron, J Giacconi, R Hasinger, G Kewley, L Norman, C Rosati, P Tozzi, P Zirm, A AF Grogin, NA Koekemoer, AM Schreier, EJ Bergeron, J Giacconi, R Hasinger, G Kewley, L Norman, C Rosati, P Tozzi, P Zirm, A TI Hubble Space Telescope imaging in the Chandra Deep Field-South. III. Quantitative morphology of the 1 million second Chandra counterparts and comparison with the field population SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : fundamental parameters; galaxies : structure; surveys; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY; LUMINOSITY FUNCTION; WFPC2 OBSERVATIONS; SEYFERT-GALAXIES; EVOLUTION; MERGERS; NORTH; COMPANIONS; EXPOSURE AB We present quantitative morphological analyses of 37 Hubble Space Telescope (HST)/WFPC2 counterparts of X-ray sources in the 1 Ms Chandra Deep Field - South (CDFS). We investigate (1) one-dimensional surface brightness profiles via isophotal ellipse fitting; (2) two-dimensional, point-spread function convolved, bulge+ disk+ nucleus profile fitting; (3) asymmetry and concentration indices compared with all similar to 3000 sources in our three WFPC2 fields; and (4) near-neighbor analyses comparing local environments of X-ray sources versus the field control sample. Significant nuclear point-source optical components appear in roughly half of the resolved HST/WFPC2 counterparts, showing a narrow range of F(X)/F(opt,nuc) consistent with the several HST-unresolved X-ray sources (putative type 1 active galactic nuclei [AGNs]) in our fields. We infer that roughly half of the HST/WFPC2 counterparts host unobscured AGNs, comparable to analogous low-redshift AGN samples and suggesting no steep decline in the type 1/ type 2 ratio out to the redshifts z similar to 0.5-1 typical of our sources. The concentration indices of the CDFS counterparts are clearly larger on average than those of the field distribution, at 5 sigma, suggesting that the strong correlation between central black hole mass and host galaxy properties ( including concentration index) observed in nearby galaxies is already evident by z similar to 0.5-1. By contrast, the asymmetry index distribution of the 21 resolved CDFS sources at I < 23 is indistinguishable from that of the I < 23 field. Moreover, the frequency of I < 23 near neighbors around the CDFS counterparts is not significantly different from that of the field sample. These results, combined with previous similar findings for local samples, suggest that recent merger/interaction history is not a good indicator of AGN activity over a substantial range of look-back time. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Associated Univ Inc, Washington, DC 20036 USA. European So Observ, D-85748 Garching, Germany. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Trieste, I-34131 Trieste, Italy. RP Grogin, NA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. OI Koekemoer, Anton/0000-0002-6610-2048 NR 37 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2003 VL 595 IS 2 BP 685 EP 697 DI 10.1086/377450 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TJ UT WOS:000185675800010 ER PT J AU Prestwich, AH Irwin, JA Kilgard, RE Krauss, MI Zezas, A Primini, F Kaaret, P Boroson, B AF Prestwich, AH Irwin, JA Kilgard, RE Krauss, MI Zezas, A Primini, F Kaaret, P Boroson, B TI Classifying X-ray sources in external galaxies from X-ray colors SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : spiral; galaxies : starburst; surveys; X-rays : galaxies; X-rays : general ID SUPER-NOVA REMNANTS; CHANDRA OBSERVATIONS; MAGELLANIC-CLOUD; CENTRAL REGION; POINT SOURCES; EMISSION; M31; POPULATIONS; STARBURST; BINARIES AB The X-ray populations of Local Group galaxies have been classified in detail by Einstein, ROSAT, and ASCA, revealing a mix of binaries, supernova remnants (SNRs), and H II regions. However, these observatories were unable to resolve X-ray sources in galaxies beyond the Local Group. With Chandra's exquisite spatial resolution, we are able to resolve sources in a sample of nearby galaxies. We show that there are highly significant differences in the X-ray colors of sources in bulge and disk systems. In particular, we find that there is a population of X-ray - soft, faint sources in disk galaxies not seen in bulges and a smaller population of hard sources also seen preferentially in disk systems. These differences can be used as a basis to classify sources as low- and high-mass X-ray binaries, SNRs, and supersoft sources. We suggest that the soft sources seen preferentially in disks are probably dominated by SNRs, although we cannot rule out the possibility that they are a new population of absorbed, faint, supersoft accretion sources associated with the young stellar population. The hard sources seen in disks but not bulges we identify as high-mass X-ray binaries. While it is impossible to classify any individual source on the basis of X-ray color alone, the observations presented here suggest that it is possible to separate sources into groups dominated by one or two source types. This classification scheme is likely to be very useful in population studies, where it is crucial to distinguish between different classes of objects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Ann Arbor, MI 48109 USA. MIT, Ctr Space Res, Cambridge, MA 02138 USA. RP Prestwich, AH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Primini, Francis/0000-0002-6077-0643 NR 32 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2003 VL 595 IS 2 BP 719 EP 726 DI 10.1086/377366 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TJ UT WOS:000185675800013 ER PT J AU Immler, S Wang, QD Leonard, DC Schlegel, EM AF Immler, S Wang, QD Leonard, DC Schlegel, EM TI A deep Chandra X-ray observation of NGC 1637 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : general; galaxies : individual (NGC 1637); galaxies : spiral; X-rays : galaxies; X-rays : general ID HUBBLE-SPACE-TELESCOPE; MEDIUM SENSITIVITY SURVEY; NEARBY SPIRAL GALAXIES; SOURCE NGC-5204 X-1; POINT SOURCES; OPTICAL COUNTERPART; GLOBULAR-CLUSTERS; SOURCE POPULATION; SUPERNOVA 1979C; STAR-CLUSTERS AB We present a deep (168 ks) Chandra observation of the nearby face-on spiral galaxy NGC 1637 and study the X-ray source population. A total of 32 X-ray sources are detected within the D-25 ellipse of NGC 1637, each of which is found to be variable during the 629 day period covered by the observations. Deep Hubble Space Telescope WFPC2 observations of NGC 1637, nearly simultaneous with the Chandra data, were used to search for optical counterparts to the X-ray sources. An ultraluminous (L-X = 2.2 x 10(39) ergs s(-1); 0.3 - 7 keV) and variable (factor of 1.4) X-ray source is found to positionally coincide with an optical faint and extended (similar to25 pc FWHM) counterpart in the HST images (m(V) similar to 22.8 mag, m(I) similar to 21.1 mag). Given the multiband properties of this source, it likely represents a stellar-mass (similar to8 M-.) black hole candidate located in an OB association in an outer spiral arm of NGC 1637. Our analysis further reveals large amounts of diffuse emission filling the entire extent of the galaxy. The spectrum of the inner less than or similar to 300 pc region is best described by a two-temperature thermal plasma emission, with a low-temperature/ low-absorption component (kT(low) similar to 0.3 keV) and a high-temperature/high-absorption component (kT(high) similar to 0.7-0.8 keV), likely associated with an outflow of hot gas into the halo of NGC 1637. Comparison of the multiwavelength properties of a number of nearby galaxies shows that NGC 1637 has remarkably high L-X/L-FIR and L-X/L-B ratios, suggesting a recent epoch with an enhanced star formation rate. C1 Penn State Univ, Dept Astron & Astrophys, DAvey Lab 525, University Pk, PA 16802 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Univ Massachusetts, Coll Astron Dept 5, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Immler, S (reprint author), Penn State Univ, Dept Astron & Astrophys, DAvey Lab 525, University Pk, PA 16802 USA. NR 64 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 1 PY 2003 VL 595 IS 2 BP 727 EP 742 DI 10.1086/377474 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TJ UT WOS:000185675800014 ER PT J AU Huenemoerder, DP Canizares, CR Drake, JJ Sanz-Forcada, J AF Huenemoerder, DP Canizares, CR Drake, JJ Sanz-Forcada, J TI The coronae of AR Lacertae SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; stars : abundances; stars : coronae; stars : individual (AR Lacertae); X-rays : binaries; X-rays : stars ID RS-CANUM-VENATICORUM; X-RAY SPECTROSCOPY; HELIUM-LIKE IONS; XMM-NEWTON VIEW; EMISSION MEASURE DISTRIBUTIONS; ACTIVE BINARY-SYSTEMS; STELLAR CORONAE; FUNDAMENTAL LIMITATIONS; TEMPERATURE STRUCTURE; PLASMA TEMPERATURE AB We observed the coronally active eclipsing binary AR Lac with the High Energy Transmission Grating on Chandra for a total of 97 ks, spaced over five orbits, at quadratures and conjunctions. Contemporaneous and simultaneous EUV spectra and photometry were also obtained with the Extreme Ultraviolet Explorer. Significant variability in both X-ray and EUV fluxes were observed, dominated by at least one X-ray flare and one EUV flare. We saw no evidence of primary or secondary eclipses, but exposures at these phases were short and intrinsic variability compromised detection of any geometric modulation. X-ray flux modulation was largest at high temperature, indicative of. are heating of coronal plasma rather than changes in emitting volume or global emission measure. Analysis of spectral line widths interpreted in terms of Doppler broadening suggests that both binary stellar components are active. On the basis of line fluxes obtained from total integrated spectra, we have modeled the emission measure and abundance distributions. The EUV spectral line fluxes were particularly useful for constraining the parameters of the "cool'' (less than or equal to2 x 10(6) K) plasma. A strong maximum was found in the differential emission measure, characterized by two apparent peaks at log T = 6.9 and 7.4, together with a weak but significant cooler maximum near log T = 6.2 and a moderately strong hot tail from log T = 7.6-8.2. Coronal abundances have a broad distribution and show no simple correlation with first ionization potential. While the resulting model spectrum generally agrees very well with the observed spectrum, there are some significant discrepancies, especially among the many Fe L lines. Both the emission measure and abundance distributions are qualitatively similar to prior determinations from other X-ray and ultraviolet spectra, indicating some long-term stability in the overall coronal structure. C1 MIT, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Palermo, I-90134 Palermo, Italy. RP Huenemoerder, DP (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI Sanz-Forcada, Jorge/C-3176-2017 OI Sanz-Forcada, Jorge/0000-0002-1600-7835 NR 61 TC 45 Z9 45 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2003 VL 595 IS 2 BP 1131 EP 1147 DI 10.1086/377490 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TJ UT WOS:000185675800046 ER PT J AU Zhang, M Golub, L AF Zhang, M Golub, L TI The dynamical morphologies of flares associated with the two types of solar coronal mass ejections SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : flares ID POLARIZATION; TRANSIENTS; ORIGIN AB In this paper we study the high-cadence TRACE observations of a sample of 28 X- and M-class flares, with particular focus on the relation between. are morphology and the two types (fast and slow) of solar coronal mass ejections (CMEs). Among the 28 flares studied, 10 are associated with fast CMEs, 10 are associated with slow CMEs, and 8 are loosely associated with a CME. We find that flares associated with fast and slow CMEs show different morphologies as groups. While all flares associated with fast CMEs show clear footpoint-separating, two-ribbon brightenings during the flare, this feature is less often seen in flares associated with slow CMEs or flares without CMEs. Meanwhile, while flares associated with slow CMEs sometimes show tubular emission structures during the flare, this feature is not found in our sample of flares associated with fast CMEs. This observational result suggests that the morphologies of flares, and hence possibly the magnetic field topologies, are different for events associated with fast and with slow CMEs. C1 Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Chinese Acad Sci, Natl Astron Observ, Beijing 100864, Peoples R China. RP Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. EM zhm@hao.ucar.edu; lgolub@head-cfa.cfa.harvard.edu OI Golub, Leon/0000-0001-9638-3082 NR 21 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2003 VL 595 IS 2 BP 1251 EP 1258 DI 10.1086/377466 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TJ UT WOS:000185675800053 ER PT J AU Skory, S Weck, PF Stancil, PC Kirby, K AF Skory, S Weck, PF Stancil, PC Kirby, K TI New theoretical line list for the B ' (2)Sigma(+)<- X (2)Sigma(+) system of (MgH)-Mg-24 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE molecular data; stars : atmospheres; stars : late-type ID LYING ELECTRONIC STATES; MAGNESIUM HYDRIDE; GIANT STARS; MGH; SPECTRUM; COEFFICIENTS; TRANSITIONS; ABUNDANCES AB Fully quantum-mechanical techniques have been applied to compute the complete line list for the B' (2)Sigma(+) <-- X (2)Sigma(+) system of (MgH)-Mg-24. The list includes transition energies and oscillator strengths over the wavelength range 11,850-32,130 cm(-1), for all possible allowed transitions from the ground electronic state vibrational levels upsilon" = 0-11. This list was computed using the best available ab initio potential energies and dipole transition moment function, with the former adjusted to account for experimental data. The agreement of the current calculations with previous theoretical results and the line list of Kurucz is discussed. Although spectroscopic accuracy for a particular line cannot be claimed for our calculations, comparison is made with the recent astronomical measurements of Wallace et al. A line list for pure rovibrational transitions in the X (2)Sigma(+) state is also presented. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Skory, S (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. RI Mahalingam, Arjun/G-8586-2011 NR 29 TC 27 Z9 27 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2003 VL 148 IS 2 BP 599 EP 606 DI 10.1086/376834 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 727TN UT WOS:000185676300017 ER PT J AU James, HF Olson, SL AF James, HF Olson, SL TI A giant new species of nukupuu (Fringillidae : Drepanidini : Hemignathus) from the island of Hawaii SO AUK LA English DT Article ID GEESE AB We describe a new species of drepanidine bird from a fossil found in a lava tube cave on the island of Hawaii. The bill of the new species combines a long, scimitar-like maxillary rostrum with a much shorter mandibular rostrum, giving the bird a most unusual appearance. The general bill form is shared with members of the drepanidine genus Hemignathus, to which the new species is referred, although it is quite distinct from other species of Hemignathus in aspects of its bill morphology and in its much larger body size. The scimitar-like maxilla appears to be adapted to probing in cracks or crevices and possibly to moving loose material, such as leaf detritus, to obtain invertebrate prey. The species became extinct <3,000 years ago. Received I October 2000, accepted 20 April 2003. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. RP James, HF (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, POB 37012, Washington, DC 20013 USA. NR 28 TC 0 Z9 0 U1 1 U2 1 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 2003 VL 120 IS 4 BP 971 EP 981 PG 11 WC Ornithology SC Zoology GA 739HE UT WOS:000186338400004 ER PT J AU Robbins, MB Braun, MJ Finch, DW AF Robbins, MB Braun, MJ Finch, DW TI Discovery of a population of the endangered Red Siskin (Carduelis cucullata) in Guyana (vol 120, pg 291, 2003) SO AUK LA English DT Correction C1 Univ Kansas, Museum Hist Nat, Div Birds, Lawrence, KS 66045 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Syst Biol, Suitland, MD 20746 USA. Smithsonian Inst, Museum Natl Hist Nat, Lab Analyt Biol, Suitland, MD 20746 USA. WINGS, Tucson, AZ 85712 USA. RP Robbins, MB (reprint author), Univ Kansas, Museum Hist Nat, Div Birds, Lawrence, KS 66045 USA. NR 2 TC 0 Z9 0 U1 1 U2 2 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 2003 VL 120 IS 4 BP 1211 EP 1211 PG 1 WC Ornithology SC Zoology GA 739HE UT WOS:000186338400028 ER PT J AU Puyravaud, JP Davidar, P Pascal, JP Ramesh, BR AF Puyravaud, JP Davidar, P Pascal, JP Ramesh, BR TI Analysis of threatened endemic trees of the Western Ghats of India sheds new light on the Red Data Book of Indian Plants SO BIODIVERSITY AND CONSERVATION LA English DT Article DE endemic species; India; rainforest; Red Data Book; semi-evergreen rainforest; threatened species ID EVERGREEN FOREST; BIODIVERSITY; DIVERSITY AB The Red Data Book of Indian Plants (RDB) is a reference manual that lists threatened angiosperms, gymnosperms and pterydophytes. Because it is widely used as an analytical tool and is a major reference for impact assessments on vegetation, it is important that the RDB be as comprehensive and up to date as possible. This study is an attempt to cross-check the listings in the RDB using vegetation inventories and another reference manual, the Atlas of Endemics of the Western Ghats, India [Ramesh and Pascal 1997. Atlas of Endemics of the Western Ghats ( India). French Institute of Pondicherry, India]. Field inventories across the Western Ghats gave an estimate of the species relative abundances and the Atlas provided quantitative information on the number of records for the endemic species in herbaria, literature, and during field surveys. The results of this analysis indicate that the RDB and the Atlas agree statistically regarding the conservation status of endemic trees. However, the proportion of threatened species per Atlas record category behaves erratically, indicating that some threatened endemic trees are not listed in the RDB. Our results suggest that the status of threatened plant species should be reexamined on a priority basis using quantitative methodology. An updating of the RDB is urgently needed, particularly for the endemic plants of the Western Ghats. We provide a list of species that are likely to be threatened, yet are not listed. C1 Smithsonian Trop Res Inst, Balboa, Panama. Pondicherry Univ, Salim Ali Sch Ecol & Environm Sci, Pondicherry 605014, India. Univ Lyon 1, CNRS, UMR 5558, F-69622 Villeurbanne, France. French Inst Pondicherry, Pondicherry 605001, India. RP Puyravaud, JP (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. OI Davidar, Priya/0000-0003-2463-6743 NR 23 TC 5 Z9 7 U1 0 U2 5 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD OCT PY 2003 VL 12 IS 10 BP 2091 EP 2106 DI 10.1023/A:1024184814545 PG 16 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 688PL UT WOS:000183444400007 ER PT J AU Parkinson, WH Yoshino, K AF Parkinson, WH Yoshino, K TI Absorption cross-section measurements of water vapor in the wavelength region 181-199 nm SO CHEMICAL PHYSICS LA English DT Article DE water vapor; cross-sections ID MARTIAN ATMOSPHERE; PHOTODISSOCIATION; MARS; PHOTOABSORPTION; STABILITY; SPECTRUM; D2O; H2O AB Laboratory measurements of the relative absorption cross-sections of H2O at the temperature 295 K have been made throughout the wavelength region 181-199 nm. Laboratory measurements of the absolute absorption cross-sections of H2O at 295 K have been made at 15 different wavelengths, and these absolute values have been used to put the relative cross-section measurements of H2O at 295 K on an absolute basis, In combination with our previous measurements [Chem. Phys. 211 (1996) 387; 215 (1997) 429], the absorption cross-section of H2O are available in the wavelength region 118-199 nm at 295 K. (C) 2003 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoshino, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-50, Cambridge, MA 02138 USA. NR 20 TC 17 Z9 18 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD OCT 1 PY 2003 VL 294 IS 1 BP 31 EP 35 DI 10.1016/S0301-0104(03)00361-6 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 726HM UT WOS:000185593000003 ER PT J AU Guzman, HM Guevara, C Castillo, A AF Guzman, HM Guevara, C Castillo, A TI Natural disturbances and mining of Panamanian coral reefs by indigenous people SO CONSERVATION BIOLOGY LA English DT Article ID COMMUNITY STRUCTURE; DIADEMA-ANTILLARUM; SAN-BLAS; RECOVERY; GROWTH AB Before the 1980s, coral reefs were considered relatively stable and healthy in Kuna-Yala, Caribbean Panama. During the 1980s, however, several natural disturbances changed the reef's community structure. We evaluated historical changes in coral cover and for the first time provide quantitative evidence of a large-scale process of reef degradation. This process started long before the onset of these disturbances as a result of demographic growth and the traditional practices of the Kuna people. Living coral cover declined 79% in 30 years (1970-2001) while the indigenous population increased 62%. We measured 20 km of seawall built with mined reef corals (16,000 m 3) and an increase in island surface area of 6.23 ha caused by coral land filling. Consequently, coastal erosion has increased as a result of the lack of a protective natural barrier and a 2.0 cm/year local increase in sea level. Coral-mining and land-filling practices to accommodate population expansion and mismanagement of resources have significantly modified the reef ecosystem and will have serious long-term consequences. We propose eight priority conservation areas within the Indian reserve, based on reef conservation status. The Kuna people and their leaders are considering a cultural change, which may include a gradual and organized migration to the mainland, and have optimistically accepted our results. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 28 TC 17 Z9 18 U1 3 U2 17 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 2003 VL 17 IS 5 BP 1396 EP 1401 DI 10.1046/j.1523-1739.2003.02308.x PG 6 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 724DZ UT WOS:000185473000024 ER PT J AU Toscano, MA Macintyre, IG AF Toscano, MA Macintyre, IG TI Corrected western Atlantic sea-level curve for the last 11,000 years based on calibrated C-14 dates from Acropora palmata framework and intertidal mangrove peat SO CORAL REEFS LA English DT Article DE sea-level rise; Acropora palmata; mangrove peat; radiocarbon calibration; paleo water depths; corrected Holocene sea-level curve; glacio-hydroisostacy ID MID-PACIFIC ISLAND; RADIOCARBON AGE CALIBRATION; RECENT SEDIMENTARY RECORD; REEF GROWTH; SOUTHWESTERN COAST; GLACIAL MAXIMUM; MARINE SAMPLES; CLIMATE-CHANGE; PAST 14KY; FLORIDA AB A corrected western Atlantic Holocene sea-level curve was constructed from 145 calibrated C-14 and TIMS U-Th dates from shallow Acropora palmata framework and intertidal Rhizopora mangle peat from the Florida Keys, Belize, and the wider Caribbean. Data include both previously published and newly reported coral and peat dates. With the elevations of corals restricted to positions below sea level and those of peats to intertidal and higher levels, a curve bracketed by corals below and peat above effectively delineates the positions of a rising Holocene sea. From 3-11 ka, the corrected curve shifts progressively to older calibrated ages, reaching an similar to1-kyr increase at -21 m MSL (mean sea level). Elevations and calibrated ages of samples from each locality in the wider Caribbean region constitute an important database for future refinement with glacio-hydro-isostatic elevation corrections from 3-D Earth models. In future studies of the history of western Atlantic coral reefs, scientists will be able to relate calibrated radiocarbon dates to this sea-level curve to determine paleo water depths and rates of sea-level rise. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 125, Washington, DC 20560 USA. RP Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 125, Washington, DC 20560 USA. EM mtoscano@sprintmail.com NR 55 TC 169 Z9 185 U1 2 U2 39 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD OCT PY 2003 VL 22 IS 3 BP 257 EP 270 DI 10.1007/s00338-003-0315-4 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 727YK UT WOS:000185688300009 ER PT J AU Cudnik, BM Dunham, DW Palmer, DM Cook, A Venable, R Gural, PS AF Cudnik, BM Dunham, DW Palmer, DM Cook, A Venable, R Gural, PS TI The observation and characterization of lunar meteoroid impact phenomena SO EARTH MOON AND PLANETS LA English DT Article DE hypervelocity impacts; Leonid meteors; lunar impact phenomena; moon; professional-amateur collaboration; signal detection technology ID MOON; FLASHES AB Confirmed observations of meteoroids from the Leonid stream impacting the Moon in 1999 and 2001 have opened up new opportunities in observational and theoretical astronomy. These opportunities could help bridge the gap between the ground-based ( atmospheric) sampling of the smallest meteoroids and the larger objects observable with ground-based telescopes. The Moon provides a laboratory for the study of hypervelocity impacts, with collision velocities not yet possible in ground-based laboratories. Development of automatic detection software removes the time-intensive activity of laboriously reviewing data for impact event signatures, freeing the observer to engage in other activities. The dynamics of professional-amateur astronomer collaboration have the promise of advancing the study of lunar meteoritic phenomenon considerably. These three factors will assist greatly in the development of a systematic, comprehensive program for monitoring the Moon for meteoroid impacts and determining the physical nature of these impacts. C1 Prairie View A&M Univ, Dept Phys, Prairie View, TX 77446 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Los Alamos Natl Lab, Los Alamos, NM 87544 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Sci Appl Intl Corp, Chantilly, VA 20151 USA. RP Cudnik, BM (reprint author), Prairie View A&M Univ, Dept Phys, Prairie View, TX 77446 USA. NR 16 TC 2 Z9 2 U1 2 U2 8 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD OCT PY 2003 VL 93 IS 2 BP 97 EP 106 DI 10.1023/B:MOON.0000034498.32831.3c PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 837CG UT WOS:000222604200002 ER PT J AU Johnson, DW Hungate, BA Dijkstra, P Hymus, G Hinkle, CR Stiling, P Drake, BG AF Johnson, DW Hungate, BA Dijkstra, P Hymus, G Hinkle, CR Stiling, P Drake, BG TI The effects of elevated CO2 on nutrient distribution in a fire-adapted scrub oak forest SO ECOLOGICAL APPLICATIONS LA English DT Article DE CO2, elevated; fire; nutrients; O horizon; scrub oak; Florida; soils; uptake ID ATMOSPHERIC CARBON-DIOXIDE; PONDEROSA PINE; POPULUS-TREMULOIDES; CO2-ENRICHED ATMOSPHERE; NITROGEN-FERTILIZATION; N FERTILIZATION; SOIL; GROWTH; ENRICHMENT; DECOMPOSITION AB Elevated carbon dioxide (CO2) caused greater accumulation of carbon (C) and nutrients in both vegetation and O horizons over a 5-yr sampling period in a scrub oak ecosystem in Florida. Elevated CO2 had no effect on any measured soil property except extractable phosphorus (P), which was lower with elevated CO2 after five years. Anion and cation exchange membranes showed lower available nitrogen (N) and zinc (Zn) with elevated CO2. Soils in both elevated and ambient CO2 showed decreases in total C, N, sulfur (S), and cation exchange capacity, and increases in base saturation, exchangeable Ca2+, and Mg2+ over the 5-yr sampling period. We hypothesize that these soil changes were a delayed response to prescribed fire, which was applied to the site just before the initiation of the experiment. In the ambient CO2 treatment, the increases in vegetation and O horizon C, N, and S were offset by the losses of soil total C, N, and S, resulting in no statistically significant net changes in ecosystem C, N, or S over time. In the elevated CO2 treatment the increases in vegetation and O horizon C content outweighed the losses in soil C, resulting in a statistically significant net increase in ecosystem C content. Nitrogen and S contents showed no statistically significant change over time in the elevated CO2 treatment, however. Comparisons of vegetation contents and soil pools of potassium (K), calcium (Ca), and magnesium (Mg) suggest that a substantial proportion of these nutrients were taken up from either groundwater or deep soil horizons. This study demonstrates that changes in ecosystem C sequestration due elevated CO2 or any other factor cannot be accurately assessed in the absence of data on changes in soils. C1 Univ Nevada, Reno, NV 89557 USA. No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Dynamac, Kennedy Space Ctr, FL 32899 USA. Univ S Florida, Tampa, FL 33620 USA. RP Johnson, DW (reprint author), Univ Nevada, Reno, NV 89557 USA. RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 48 TC 37 Z9 40 U1 0 U2 14 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 2003 VL 13 IS 5 BP 1388 EP 1399 DI 10.1890/02-5139 PG 12 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 743XT UT WOS:000186599400017 ER PT J AU Mas, AH Dietsch, TV AF Mas, AH Dietsch, TV TI An index of management intensity for coffee agroecosystems to evaluate butterfly species richness SO ECOLOGICAL APPLICATIONS LA English DT Article DE agroecology; agroforestry; biodiversity; Chiapas; Mexico; coffee agroecosystems; fruit-feeding butterflies; intensity gradient; management index; shade-grown coffee ID BIRD POPULATIONS; SHADE COFFEE; BIODIVERSITY; FOREST; PLANTATIONS; TAXA; DISTURBANCE; INDICATORS; COMMUNITY; DIVERSITY AB In spite of the attention that has been focused on the importance of traditional, shade coffee production for biodiversity, little is known about the relative conservation value of different systems of managing the shade canopy. We surveyed fruit-feeding butterfly species richness and vegetation structure on different shade coffee management systems in Chiapas, Mexico, that ranged from intensive commercial to traditional, rustic systems. The impact, of management on the diversity and structure of the shade canopy in each coffee production system was quantified and compared using a Management Index. This Management Index revealed statistically significant differences between management systems that previously were distinguished by researchers using qualitative, "gestalt" categories. Butterfly species richness was found to decline as management intensity increased, but a significant drop was found between the rustic system and the other more intensive systems, corroborating the importance of preserving rustic, shade coffee production for the conservation of biodiversity. Fruit-feeding butterflies were found to be very sensitive to the intensification of management of the shade canopy, so they may be an effective way to monitor ecological changes that accompany intensification within the coffee agroecosystem. Additionally, the vegetation Management Index may prove useful for quantifying management practices to evaluate certification criteria for conservation benefits. C1 Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. RP Dietsch, TV (reprint author), Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, 3001 Connecticut Ave, Washington, DC 20008 USA. NR 37 TC 58 Z9 58 U1 1 U2 24 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 2003 VL 13 IS 5 BP 1491 EP 1501 DI 10.1890/01-5229 PG 11 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 743XT UT WOS:000186599400023 ER PT J AU Moegenburg, SM Levey, DJ AF Moegenburg, SM Levey, DJ TI Do frugivores respond to fruit harvest? An experimental study of short-term responses SO ECOLOGY LA English DT Article DE Amazonia; Brazil; Euterpe oleracea; extractive reserves; fruit-frugivore interactions; fruit harvest; fruit tracking; non-timber forest products; palm trees; parrots; vertebrate population ecology ID EATING BIRDS STAY; TEMPORAL VARIATION; RESOURCE AVAILABILITY; FOOD AVAILABILITY; TROPICAL FOREST; ELEVATIONAL GRADIENT; EXTRACTIVE RESERVES; DISPERSED PLANTS; OLIVE ORCHARDS; FLESHY FRUITS AB Many nonexperimental studies have shown positive correlations between resource abundance and vertebrate abundance. These relationships, however, are difficult to interpret because of confounding factors that may independently determine the abundance of vertebrates and their resources. Moreover, verifying links between vertebrate and resource abundance is complex because human perception of resource abundance may differ from that of nonhuman vertebrates and because manipulating resource abundance on an ecologically meaningful scale is difficult. We studied the dependency of frugivores on fruit abundance in eastern Amazonian floodplain forests dominated by one species of palm tree (Euterpe oleracea) from which people harvest fruit. We first compared spatial and temporal use by frugivorous parrots of four sites dominated by E. oleracea and four sites with no E. oleracea. Parrots spent 48-92% more time in the former, where their activity over the fruiting season mirrored the abundance of fruits. To test whether fruit abundance was the mechanism underlying these patterns, we removed fruit at two intensities in replicated 1.8-ha plots, and then monitored responses of frugivorous birds and mammals. High-intensity removal (75% of ripe fruit harvested) significantly reduced the number of frugivorous bird individuals by 29% and the length of frugivorous bird visits by 68%, relative to controls. In contrast, low-intensity removal (41% of ripe fruit removed) had no impact on these metrics. Frugivore species richness did not differ among treatments and controls, but the composition of the frugivore community was altered by harvest, with the presence of 11 species being linked to fruit abundance. Nonfrugivorous birds did not respond to either intensity of fruit harvest. The number of fruit-eating mammal species was 58% lower in both the low- and high-removal treatments, relative to control plots. These results verify that fruit abundance influences the species composition of frugivore communities and the abundance and foraging behavior of individual species. They also document short-term dependency of fruit-eating mammals on fruit abundance. Harvest of fruit from forest systems, a common practice in tropical forests, therefore can affect populations of fruit-eating animals. C1 Univ Florida, Dept Zool, Gainesville, FL 32611 USA. RP Moegenburg, SM (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. EM moegenburas@nzp.si.edu NR 95 TC 71 Z9 73 U1 0 U2 17 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD OCT PY 2003 VL 84 IS 10 BP 2600 EP 2612 DI 10.1890/02-0063 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 743XR UT WOS:000186599300011 ER PT J AU Banks, AN Srygley, RB AF Banks, AN Srygley, RB TI Orientation by magnetic field in leaf-cutter ants, Atta colombica (Hymenoptera : Formicidae) SO ETHOLOGY LA English DT Article ID PATH-INTEGRATION; WOOD ANTS; NAVIGATION; COMPASS; HONEYBEES; MECHANISMS; INSECTS; VISION; MEMORY AB Leaf-cutter ants (Atta colombica) use trail following to travel between foraging sites and the home nest. However, this combination of pheromone and visual cues is likely to be complemented by a directional reference system such as a compass, used not only when foraging but also during colony formation, where foraging trails degrade or where ants become displaced. One candidate system is the magnetic polarity compass. We tested the orientation of leaf-cutter ants under a magnetic field of reversed-polarity, with the prediction that the ants would show 180degrees deflection compared with control ants in an unchanged geomagnetic field. When the sun's disc was unobstructed by clouds, orientation was the same as that of control ants, implying that magnetic cues were not used to orient. However, when the sky was overcast, ants in the experimental treatment significantly shifted their mean orientation both in comparison with controls and reversed-polarity ants under the sun. Although a total reversal in orientation was not induced, the results demonstrate that Atta respond to magnetic reversal in the absence of sunlight cues, and suggest a role for magnetic cues in determining direction during orientation. C1 British Trust Ornithol, Thetford IP24 2PU, Norfolk, England. Univ Oxford, Dept Zool, Oxford OX1 3PS, England. Smithsonian Trop Res Inst, Balboa, Panama. RP Banks, AN (reprint author), British Trust Ornithol, Nunnery, Thetford IP24 2PU, Norfolk, England. NR 32 TC 32 Z9 39 U1 5 U2 25 PU BLACKWELL VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0179-1613 J9 ETHOLOGY JI Ethology PD OCT PY 2003 VL 109 IS 10 BP 835 EP 846 DI 10.1046/j.0179-1613.2003.00927.x PG 12 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 733EG UT WOS:000185986500005 ER PT J AU Zigler, KS Raff, EC Popodi, E Raff, RA Lessios, HA AF Zigler, KS Raff, EC Popodi, E Raff, RA Lessios, HA TI Adaptive evolution of bindin in the genus Heliocidaris is correlated with the shift to direct development SO EVOLUTION LA English DT Article DE evolution of development; fertilization; gamete recognition; sea urchin ID DEVELOPING SEA-URCHIN; MITOCHONDRIAL-DNA; NUCLEOTIDE SUBSTITUTIONS; MOLECULAR EVOLUTION; POSITIVE SELECTION; EASTERN PACIFIC; DIFFERENT MODES; PROTEIN BINDIN; SPERM BINDIN; ERYTHROGRAMMA AB Sea urchins are widely used to study both fertilization and development. In this study we combine the two fields to examine the evolution of reproductive isolation in the genus Heliocidaris. Heliocidaris tuberculata develops indirectly via a feeding larva, whereas the only other species in the genus, H. erythrogramma, has evolved direct development through a nonfeeding larva. We estimated the time of divergence between H. erythrogrannna and H. tuberculata from mitochondrial DNA divergence, quantified levels of gametic compatibility between the two species in cross-fertilization assays, and examined the mode of evolution of the sperm protein bindin by sequencing multiple alleles of the two species. Bindin is the major component of the sea urchin sperm acrosomal vesicle, and is involved in sperm-egg attachment and fusion. Based on our analyses, we conclude that: the two species of Hetiocidaris diverged less than five million years ago, indicating that direct development can evolve rapidly in sea urchins; since their divergence, the two species have become gametically incompatible; Heliocidaris bindin has evolved under positive selection; and this positive selection is concentrated on the branch leading to H. erythrogramma. Three hypotheses can explain the observed pattern of selection on bindin: (1) it is a correlated response to the evolution of direct development in H. erythrogramma; (2) it is the result of an intraspecific process acting in H. erythrogramma but not in H. tuberculata: or (3) it is the product of reinforcement on the species that invests more energy into each egg to avoid hybridization. C1 Smithsonian Trop Res Inst, Balboa, Panama. Duke Univ, Dept Biol, Durham, NC 27708 USA. Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. Indiana Univ, Inst Mol Biol, Bloomington, IN 47405 USA. RP Zigler, KS (reprint author), Friday Harbor Labs, 620 Univ Rd, Friday Harbor, WA 98250 USA. EM ziglerk@u.washington.edu; eraff@bio.indiana.edu; epopodi@bio.indiana.edu; rraff@bio.indiana.edu; lessiosh@naos.si.edu NR 56 TC 60 Z9 60 U1 0 U2 11 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 OCT PY 2003 VL 57 IS 10 BP 2293 EP 2302 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 740PG UT WOS:000186410300009 PM 14628917 ER PT J AU Coley, PD Heller, MV Aizprua, R Arauz, B Flores, N Correa, M Gupta, M Solis, PN Ortega-Barria, E Romero, LI Gomez, B Ramos, M Cubilla-Rios, L Capson, TL Kursar, TA AF Coley, PD Heller, MV Aizprua, R Arauz, B Flores, N Correa, M Gupta, M Solis, PN Ortega-Barria, E Romero, LI Gomez, B Ramos, M Cubilla-Rios, L Capson, TL Kursar, TA TI Using ecological criteria to design plant collection strategies for drug discovery SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Review ID TROPICAL RAIN-FORESTS; ECOGEOGRAPHIC PERSPECTIVE; NATURAL-PRODUCTS; LEAF DEVELOPMENT; MEDICINAL PLANT; BIODIVERSITY; HERBIVORY; DEFENSE; COEVOLUTION; CONVERGENCE AB Tropical forests are one of the most diverse and endangered habitats on earth. They have also been portrayed as a source of future pharmaceuticals, yet finding useful compounds can be both scientifically and politically challenging. Increasingly, over the past decade, the potential value of medicinal compounds derived from plants, microorganisms, and animals has been proposed as a tangible benefit of biodiversity and therefore a basis for promoting its preservation. Ecological theories of plant defense can increase the probability of discovering compounds with activity in bioassays against human disease targets. In addition, conducting research in tropical countries with local scientists provides immediate and lasting benefits for the sustainable use of biodiversity. This new approach to drug discovery has been effective in identifying bioactive leads. It is both an important step towards understanding the medicinal value of biodiversity, and a practical way to link drug discovery with conservation. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Panama, Natl Herbarium, Panama City, Panama. Univ Panama, Sch Pharm, CIFLOR PAN, Panama City, Panama. Inst Adv Sci Invest & High Technol, Panama City, Panama. Univ Panama, Sch Med, Dept Microbiol, Panama City, Panama. Univ Panama, Fac Nat & Exact Sci & Technol, Lab Nat Product, Panama City, Panama. RP Coley, PD (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. OI Gupta, Mahabir/0000-0002-9302-7864 NR 61 TC 35 Z9 37 U1 1 U2 20 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD OCT PY 2003 VL 1 IS 8 BP 421 EP 428 DI 10.2307/3868139 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 825XG UT WOS:000221791500017 ER PT J AU Laube, S Zotz, G AF Laube, S Zotz, G TI Which abiotic factors limit vegetative growth in a vascular epiphyte? SO FUNCTIONAL ECOLOGY LA English DT Article DE growth; ontogenetic drift; Panama; rainforest; RGR ID RAIN-FOREST; DIMERANDRA-EMARGINATA; BIOMASS ALLOCATION; CARBON GAIN; BROMELIACEAE; SIZE; BIOGEOGRAPHY; TEMPERATURE; ONTOGENY; ORCHID AB 1. Vegetative growth in vascular epiphytes is assumed to be severely limited by intermittent supply of water and nutrients, but experimental evidence for this notion is meagre. The effects of water, nutrient supply and light on growth were studied in an epiphytic bromeliad, Vriesea sanguinolenta Cogn. & Marchal (syn. Werauhia sanguinolenta) in a large forest gap in a lowland forest of Panama, in a full-factorial design. To investigate ontogenetic drift, three plant-size classes (approximate to5, 15 and 35 cm leaf length) were included in the experiment. 2. Water supply had the strongest influence on growth, but the magnitude of this effect differed considerably among size classes. Nutrient supply affected growth only in small and intermediate-sized plants. More light (60% of direct irradiation) tended to decrease growth rates compared to 30% irradiation. 3. Small plants showed by far the highest potential to adjust their relative growth rate (RGR) in response to favourable growing conditions. 4. Despite these size-related differences, absolute RGRs were extremely low compared to studies with other plant groups, confirming the notion that vascular epiphytes are inherently slow-growing plants. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Fachbereich Biol, Abt Allgemeine Bot 13 274, D-67653 Kaiserslautern, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. NR 41 TC 51 Z9 56 U1 1 U2 23 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD OCT PY 2003 VL 17 IS 5 BP 598 EP 604 DI 10.1046/j.1365-2435.2003.00760.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 726JL UT WOS:000185595900004 ER PT J AU Gilmour, I French, BM Franchi, IA Abbott, JI Hough, RM Newton, J Koeberl, C AF Gilmour, I French, BM Franchi, IA Abbott, JI Hough, RM Newton, J Koeberl, C TI Geochemistry of carbonaceous impactites from the Gardnos impact structure, Norway SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID SHOCK COMPRESSION; SOUTHERN-NORWAY; GRAPHITE; DIAMOND; SAMPLES; CRATER; SEDIMENTATION; METAMORPHISM; INCLUSIONS; TRANSITION AB The Gardnos impact structure in southern Norway is one of only two known impact structures (among similar to175) whose impactites contain significant amounts (typically 0.2-1.0 wt.%) of carbon, or 5 to 10 times the amount present in the target rocks; Sudbury, Canada is the other. This study extends a previous investigation of the geochemistry and petrology of Gardnos impactites (French et al., 1997) with additional sampling and a detailed investigation of the nature and possible origin of the carbonaceous material present. Two principal carbon components have been identified in Gardnos impactites: (1) impact-produced diamonds, 0.5 to 1 mum in size, with a cubic crystal structure, predominantly hexagonal morphologies with platey layers and an estimated concentration of < 0.19 ppm in Gardnos suevites and (2) graphitic carbon ranging from poorly ordered to moderately crystalline. Geochemical data suggests that there are no suitable target rocks that could provide a single source for the carbon in Gardnos impactites. However, Raman spectroscopy, stable isotope analysis and transmission electron microscopy of the impact diamonds and graphitic carbon suggests that there were at least two episodes of C emplacement in Gardnos impactites: an impact-related incorporation and shock transformation of graphitic material from target rocks followed by later mobilization of C, possibly during postimpact cooling or later regional metamorphism. Copyright (C) 2003 Elsevier Ltd. C1 Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. Smithsonian Inst, Washington, DC 20560 USA. Univ Vienna, Inst Geochem, A-1090 Vienna, Austria. RP Gilmour, I (reprint author), Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. RI Newton, Jason/A-9536-2009; OI Newton, Jason/0000-0001-7594-3693; Gilmour, Iain/0000-0002-2860-9489 NR 49 TC 23 Z9 23 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 OCT PY 2003 VL 67 IS 20 BP 3889 EP 3903 DI 10.1016/S0016-7037(03)00123-8 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 734JR UT WOS:000186052600008 ER PT J AU Rudran, R Fernandez-Duque, E AF Rudran, R Fernandez-Duque, E TI Demographic changes over thirty years in a red howler population in Venezuela SO INTERNATIONAL JOURNAL OF PRIMATOLOGY LA English DT Article DE density; rate of increase; population size; group composition; age structure; sex ratios ID MONKEYS ALOUATTA-SENICULUS; LOCAL RESOURCE COMPETITION; RICAN DRY FOREST; SEX-RATIO; DISPERSAL PATTERNS; HOWLING MONKEYS; BIRTH DATA; CONSERVATION; PALLIATA; DYNAMICS AB During a 30-year span (1969 - 1999) the annual growth rate of a Venezuelan red howler (Alouatta seniculus) population fluctuated irregularly, but its size increased, remained stable for a short while, and finally declined sharply. The increase took place in three stages, and began as an increase in the size of established groups. The next two stages of population increase were due to the formation of new groups and their subsequent increases in size. These two stages likely occurred because of habitat regeneration, which increased the areas where newly formed groups could establish home ranges. The population decline of 74% was most likely due to disease. However, new groups died out more rapidly than established groups, indicating that food shortages, especially in recently regenerated areas, may also have contributed to the population crash. The food shortages could have been caused by unpredictable periods of drought, which may explain the irregular size fluctuations of the study population. Since many howler species show irregular size fluctuations and sharp declines, their demographic features may reflect adaptations to unpredictable events like droughts and disease epidemics. On this premise we explain the preponderance of unimale groups and female-biased birth sex ratios at low densities and the dispersal of both sexes as adaptations for increasing a population rapidly after a decline. Within the population, mortality of small juvenile females was higher in multimale than in unimale groups, though medium juvenile and older immature females were better represented in multimale than in unimale groups. These results may be explained in terms of group composition and the mating systems in red howlers. C1 Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA. Zool Soc San Diego, Ctr Reprod Endangered Species, San Diego, CA 92112 USA. RP Rudran, R (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA. NR 65 TC 27 Z9 35 U1 1 U2 20 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0164-0291 J9 INT J PRIMATOL JI Int. J. Primatol. PD OCT PY 2003 VL 24 IS 5 BP 925 EP 947 DI 10.1023/A:1026241625910 PG 23 WC Zoology SC Zoology GA 735QV UT WOS:000186126800001 ER PT J AU Pearson, TRH Burslem, DFRP Goeriz, RE Dalling, JW AF Pearson, TRH Burslem, DFRP Goeriz, RE Dalling, JW TI Interactions of gap size and herbivory on establishment, growth and survival of three species of neotropical pioneer trees SO JOURNAL OF ECOLOGY LA English DT Article DE Barro Colorado Island; germination; niche partitioning; seedling; tropical forest regeneration ID TROPICAL FOREST; SEED SIZE; RAIN-FOREST; PLANT; DIVERSITY; GERMINATION; SEEDLINGS; LIGHT; ECOLOGY; DEFENSE AB 1 The difference in gap size requirements observed for neotropical pioneer species is a classic example of habitat partitioning among tropical tree species. Previous research has shown that the three species Miconia argentea, Cecropia insignis and Trema micrantha differ in the minimum gap size that they occupy as adult plants in semi-deciduous tropical forest in Panama. Here we test whether these differences result from variation in seed germination and seedling establishment requirements, or from differences in susceptibility to herbivores. 2 We planted seeds of Miconia argentea and Trema micrantha into artificially created small (25 m(2)), medium ( 64 m(2)) and large (225 m(2)) gaps in secondary forest, and transplanted seedlings of all three species into small and large gaps inside and outside mesh cages that excluded invertebrate herbivores. 3 Miconia seedlings emerged and established successfully across a broad range of gap sizes, and transplanted seedlings grew slowly but survived well in all gap sizes. By contrast, emergence and survival of Trema seedlings occurred only in the large gaps and transplants died in small gaps. Survival of Cecropia seedlings was intermediate between Trema and Miconia in the small gaps and growth was greater than either species in the large gaps. 4 Herbivore exclosures reduced foliar herbivory on all three species. The median lifespan of Trema seedlings in small gaps was reduced when the seedlings were exposed to herbivores, but survival of the other species was not affected by the exclosure treatment in either gap size. The growth of Miconia seedlings was lower outside exclosures in both gap sizes. 5 Differences in germination and establishment could generate the contrasting gap size distributions observed between Miconia and Trema, but they are partially offset by measured differences in seed bank density. However, patterns of seedling growth and survival reinforce differences among species at the establishment phase and provide a mechanism for the observed differences in gap size distribution at the sapling stage. 'Cross-overs' in species growth rates result in specialization to different environments and reduce their survival in unfavourable conditions. We found no evidence for a definitive influence of herbivory as a mechanism driving differences in gap size distribution among species. C1 Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland. Smithsonian Trop Res Inst, Miami, FL 34002 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Pearson, TRH (reprint author), Winrock Int Livestock Res & Training Ctr, 1621 N Kent St,Suite 1200, Arlington, VA 22209 USA. OI Burslem, David/0000-0001-6033-0990 NR 34 TC 39 Z9 51 U1 2 U2 22 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 OCT PY 2003 VL 91 IS 5 BP 785 EP 796 DI 10.1046/j.1365-2745.2003.00803.x PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 723RW UT WOS:000185446200007 ER PT J AU Hayward, BW Buzas, MA Buzas-Stephens, P Holzmann, M AF Hayward, BW Buzas, MA Buzas-Stephens, P Holzmann, M TI The lost types of Rotalia beccarii var. tepida Cushman 1926 SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID FORAMINIFERA; AMMONIA AB In 1926, Cushman described Rotalia beccarii var. tepida from San Juan Harbor, Puerto Rico. His publication illustrates a strew slide with many individuals, and no holotype was designated. Consequently, over the years, researchers have assumed that no holotype exists. A search of the Cushman Collection, however, discovered a slide labeled as holotype and it is so recorded in the Cushman Catalog of 1929. Here, this specimen is re-described and designated as a lectotype. All nine of the other surviving syntypes from the original collection in San Juan Harbor, Puerto Rico, now become paralectotypes. Hopefully, the designation of formal types for Ammonia tepida (Cushman) will help stabilize the taxonomy of this important species. Our study shows that the lectotype is morphologically distinguishable from other Ammonia types and that the distribution of Ammonia tepida is restricted to tropical shallow-water environments. C1 Univ Auckland, Dept Geol, Auckland 1, New Zealand. Smithsonian Inst, NMNH, Dept Paleobiol, Washington, DC 20560 USA. Midwestern State Univ, Dept Biol, Wichita Falls, TX 76308 USA. Univ Geneva, Stn Zool, CH-1224 Chene Bougeries, Switzerland. RP Hayward, BW (reprint author), Univ Auckland, Dept Geol, Private Bag 92019, Auckland 1, New Zealand. EM b.hayward@geomarine.org.nz NR 12 TC 11 Z9 12 U1 0 U2 1 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 2003 VL 33 IS 4 BP 352 EP 354 DI 10.2113/0330352 PG 3 WC Paleontology SC Paleontology GA 761DK UT WOS:000187884600007 ER PT J AU Moigis, AG Gocke, K AF Moigis, AG Gocke, K TI Primary production of phytoplankton estimated by means of the dilution method in coastal waters SO JOURNAL OF PLANKTON RESEARCH LA English DT Article ID RED-SEA; BACTERIA; GROWTH; PHOTOSYNTHESIS; PLANKTON; SEAWATER; ESTUARY; C-14 C1 Univ Kiel, Inst Meereskunde, D-24105 Kiel, Germany. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Moigis, AG (reprint author), Ulmenstr 73, D-24306 Plon, Germany. NR 37 TC 7 Z9 8 U1 0 U2 2 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 OCT PY 2003 VL 25 IS 10 BP 1291 EP 1300 DI 10.1093/plankt/fbg089 PG 10 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 733ZN UT WOS:000186030900008 ER PT J AU Bolon, CR AF Bolon, CR TI Art from Thailand. SO JOURNAL OF THE AMERICAN ORIENTAL SOCIETY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Bolon, CR (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ORIENTAL SOCIETY PI ANN ARBOR PA HARLAN HATCHER GRADUATE LIB UNIV OF MICHIGAN, ANN ARBOR, MI 48109-1205 USA SN 0003-0279 J9 J AM ORIENTAL SOC JI J. Am. Orient. Soc. PD OCT-DEC PY 2003 VL 123 IS 4 BP 906 EP 907 DI 10.2307/3589998 PG 2 WC Asian Studies SC Asian Studies GA 873HN UT WOS:000225270600038 ER PT J AU Bolon, CR AF Bolon, CR TI The dvaravati wheels of the law and the indianization of South East Asia. SO JOURNAL OF THE AMERICAN ORIENTAL SOCIETY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Bolon, CR (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ORIENTAL SOCIETY PI ANN ARBOR PA HARLAN HATCHER GRADUATE LIB UNIV OF MICHIGAN, ANN ARBOR, MI 48109-1205 USA SN 0003-0279 J9 J AM ORIENTAL SOC JI J. Am. Orient. Soc. PD OCT-DEC PY 2003 VL 123 IS 4 BP 906 EP 907 DI 10.2307/3589998 PG 2 WC Asian Studies SC Asian Studies GA 873HN UT WOS:000225270600037 ER PT J AU Wcislo, WT Gonzalez, VH Engel, MS AF Wcislo, WT Gonzalez, VH Engel, MS TI Nesting and social behavior of a wood-dwelling neotropical bee, Augochlora isthmii (Schwarz), and notes on a new species, A-alexanderi Engel (Hymenoptera : Halictidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE Apoidea; Halictidae; Augochlora; nesting biology; social behavior; taxonomy ID SWEAT BEE; EVOLUTION; APOIDEA; ARCHITECTURE; NEOCORYNURA; SOLITARY AB The nesting biology and social behavior are described for Augochlora (Augochlora) isthmii Schwarz at the species' type locality (Barro Colorado Island, Republic of Panama). Bees nested in a fallen log with wood that was still solid. Nests of A. isthmii sometimes contained more than one female, suggesting some form of social behavior, while other females nested alone. Pollen taken from nest cells was almost exclusively (>95%) from a single species of Rubiaceae (nr. Warscewiczia coccinea) that is rare on BCI. An occupied nest of a second, related species (A. alexanderi Engel, new species) was discovered in a tree branch in southern Colombia, supporting the conclusion that females of the repandirostris species-group regularly use wood as a nesting substratum. We provide the first taxonomic descriptions of the male of A. isthmii and both sexes of A. alexanderi; we also redescribe the female of A. isthmii. The evolution of social behavior in the "Augochlora group" is briefly considered in light of available information. C1 Smithsonian Trop Res Inst, Balboa, Panama. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Kansas, Museum Nat Hist, Div Entomol, Lawrence, KS 66045 USA. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM WcisloW@tivoli.si.edu; vhgonzales@rocketmail.com RI Gonzalez Betancourt, Victor /B-9528-2011; Engel, Michael/C-5461-2012; Gonzalez, Victor/B-4072-2015 OI Engel, Michael/0000-0003-3067-077X; NR 38 TC 10 Z9 10 U1 0 U2 5 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD OCT PY 2003 VL 76 IS 4 BP 588 EP 602 PG 15 WC Entomology SC Entomology GA 800SZ UT WOS:000220049300006 ER PT J AU O'Dea, A AF O'Dea, A TI Seasonality and zooid size variation in Panamanian encrusting bryozoans SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article ID GROWTH AB A model describing the positive correlation between variation in zooid size within bryozoan colonies and the amount of seasonal variation in temperature is tested in Panamanian encrusting bryozoans from contrasting seasonal regimes. Results reveal that in a natural setting the model provides accurate estimates of the level of seasonality experienced by the colonies. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM odeaa@ancon.si.edu RI O'Dea, Aaron/D-4114-2011 NR 5 TC 13 Z9 13 U1 1 U2 2 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD OCT PY 2003 VL 83 IS 5 BP 1107 EP 1108 DI 10.1017/S0025315403008348h PG 2 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 740VH UT WOS:000186421900034 ER PT J AU Bowen, WD Ellis, SL Iverson, SJ Boness, DJ AF Bowen, WD Ellis, SL Iverson, SJ Boness, DJ TI Maternal and newborn life-history traits during periods of contrasting population trends: implications for explaining the decline of harbour seals (Phoca vitulina), on Sable Island SO JOURNAL OF ZOOLOGY LA English DT Article DE pinniped; Phoca vitulina; interannual variation; life-history traits; population decline ID ANTARCTIC FUR SEALS; SCOTIAN SHELF; GREY SEALS; LACTATION PERFORMANCE; HALICHOERUS-GRYPUS; DECADAL CHANGES; BIRTH; AGE; MASS; CANADA AB Annual censuses of the number of harbour seal Phoca vitulina pups born on Sable Island Canada showed an increasing trend during the 1980s, but a rapid decline through the 1990s from 625 pups in 1989 to only 32 by 1997. Weekly surveys of the North Beach of the island during the 1991-98 breeding seasons showed that the number of adults and juveniles also declined during the 1990s. Despite the dramatic demographic changes, maternal postpartum mass, pup birth mass, relative birth mass, lactation duration, pup weaning mass and relative weaning mass showed no significant trends during 1987-96. However, two traits did change. The age structure of parturient females increased significantly, indicating reduced recruitment to the breeding population. Mean birth date increased by 7 days during the early 1990s, suggesting nutritional stress of females and later implantation dates. This nutritional stress may in turn have been caused by increased competition from the rapidly increasing grey seal population on Sable Island. Although minimum estimates of shark-inflicted mortality can account for much of the decline, evidence suggests that food shortage arising from interspecific competition may have also played a role in causing the decline of the population through effects on fecundity and juvenile survival. C1 Fisheries & Oceans Canada, Bedford Inst Oceanog, Marine Fish Div, Dartmouth, NS B2Y 4A2, Canada. Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. Lobster Conservancy, Friendship, ME 04547 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. RP Bowen, WD (reprint author), Fisheries & Oceans Canada, Bedford Inst Oceanog, Marine Fish Div, POB 1006, Dartmouth, NS B2Y 4A2, Canada. EM bowen@mar.dfo-mfo.gc.ca RI Bowen, William/D-2758-2012 NR 44 TC 52 Z9 55 U1 9 U2 54 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0952-8369 J9 J ZOOL JI J. Zool. PD OCT PY 2003 VL 261 BP 155 EP 163 DI 10.1017/S0952836903004047 PN 2 PG 9 WC Zoology SC Zoology GA 739DV UT WOS:000186327700005 ER PT J AU Schroll, S AF Schroll, S TI American photography. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 1 PY 2003 VL 128 IS 16 BP 72 EP 72 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 724AP UT WOS:000185464300035 ER PT J AU Hutchinson, A AF Hutchinson, A TI You belong in a zoo!: Tales from a lifetime spent with cobras, crocs, and other creatures. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Hutchinson, A (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 1 PY 2003 VL 128 IS 16 BP 111 EP 111 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 724AP UT WOS:000185464300206 ER PT J AU Wilkinson, SL McCoy, TJ McCamant, JE Robinson, MS Britt, DT AF Wilkinson, SL McCoy, TJ McCamant, JE Robinson, MS Britt, DT TI Porosity and density of ordinary chondrites: Clues to the formation of friable and porous ordinary chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROID 433 EROS; ELEMENTAL COMPOSITION; PHYSICAL-PROPERTIES; SHOCK METAMORPHISM; INTERNAL STRUCTURE; PARENT BODIES; BULK-DENSITY; 253 MATHILDE; METEORITES; FEATURES AB Densities and porosities of meteorites are physical properties that can be used to infer characteristics of asteroid interiors. We report density and porosity measurements of 42 pieces of 30 ordinary chondrites and provide a quantification of the errors of the gas pycnometer method used in this study. Based on our measurements, we find that no significant correlation exists between porosity and petrologic grade, chemical group, sample mass, bulk and grain density, or shock level. To investigate variations in porosity and density between pieces of a meteorite, we examined stones from two showers, Holbrook and Pultusk. Examination of nine samples of Holbrook suggests relative homogeneity in porosity and density between pieces of this shower. Measurements of three samples of Pultusk show homogeneity in bulk density, in contrast to Wilkison and Robinson (2000), a study that reported significant variations in bulk density between 11 samples of Pultusk. Finally, examination of two friable ordinary chondrites, Bjurbole and Allegan, reveal variability in friability and porosity among pieces of the same fall. We suggest that friable ordinary chondrites may have formed in a regolith or fault zone of an asteroid. C1 Northwestern Univ, Dept Geol Sci, Evanston, IL 60208 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Williams Coll, Williamstown, MA 01267 USA. Northwestern Univ, Ctr Planetary Sci, Evanston, IL 60208 USA. Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. RP Northwestern Univ, Dept Geol Sci, 1850 Campus Dr, Evanston, IL 60208 USA. EM sarah@earth.northwestern.edu NR 68 TC 21 Z9 21 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD OCT PY 2003 VL 38 IS 10 BP 1533 EP 1546 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 759RZ UT WOS:000187751800010 ER PT J AU Crawford, AJ AF Crawford, AJ TI Huge populations and old species of Costa Rican and Panamanian dirt frogs inferred from mitochondrial and nuclear gene sequences SO MOLECULAR ECOLOGY LA English DT Review DE c-myc intron; effective population size; Eleutherodactylus; F-ST; molecular clock; mtDNA; Neotropics; phylogenetics ID BUFO-BUFO; ELEUTHERODACTYLUS-BRANSFORDII; DROSOPHILA-MELANOGASTER; MOLECULAR PHYLOGENY; FREQUENCY-SPECTRUM; AMPHIBIAN DECLINES; FINITE POPULATION; DNA POLYMORPHISM; RANA-TEMPORARIA; AMERICAN FROGS AB Molecular genetic data were used to investigate population sizes and ages of Eleutherodactylus (Anura: Leptodactylidae), a species-rich group of small leaf-litter frogs endemic to Central America. Population genetic structure and divergence was investigated for four closely related species surveyed across nine localities in Costa Rica and Panama. DNA sequence data were collected from a mitochondrial gene (ND2) and a nuclear gene (c-myc). Phylogenetic analyses yielded concordant results between loci, with reciprocal monophyly of mitochondrial DNA haplotypes for all species and of c-myc haplotypes for three of the four species. Estimates of genetic differentiation among populations (F-ST) based upon mitochondrial data were always higher than nuclear-based F-ST estimates, even after correcting for the expected fourfold lower effective population size (N-e) of the mitochondrial genome. Comparing within-population variation and the relative mutation rates of the two genes revealed that the N-e of the mitochondrial genome was 15-fold lower than the estimate of the nuclear genome based on c-myc. Nuclear F-ST estimates were approximate to0 for the most proximal pairs of populations, but ranged from 0.5 to 1.0 for all other pairs, even within the same nominal species. The nuclear locus yielded estimates of N-e within localities on the order of 10(5). This value is two to three orders of magnitude larger than any previous N-e estimate from frogs, but is nonetheless consistent with published demographic data. Applying a molecular clock model suggested that morphologically indistinguishable populations within one species may be 10(7) years old. These results demonstrate that even a geologically young and dynamic region of the tropics can support very old lineages that harbour great levels of genetic diversity within populations. The association of high nucleotide diversity within populations, large divergence between populations, and high species diversity is also discussed in light of neutral community models. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. RP Smithsonian Trop Res Inst, Apartado Postal 2072, Balboa, Abcon, Panama. EM crawfordaj@naos.si.edu NR 123 TC 92 Z9 94 U1 0 U2 8 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD OCT PY 2003 VL 12 IS 10 BP 2525 EP 2540 DI 10.1046/j.1365-294X.2003.01910.x PG 16 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 720GE UT WOS:000185252400002 PM 12969459 ER PT J AU Liu, HP Hershler, R Clift, K AF Liu, HP Hershler, R Clift, K TI Mitochondrial DNA sequences reveal extensive cryptic diversity within a western American springsnail SO MOLECULAR ECOLOGY LA English DT Article DE cryptic species; freshwater; Gastropoda; mtDNA; phylogenetics; western North America ID PHYLOGENETIC-RELATIONSHIPS; SOUTHEASTERN CALIFORNIA; AQUATIC GASTROPODS; ASH MEADOWS; HYDROBIIDAE; RISSOOIDEA; SYSTEM; VALLEY; PYRGULOPSIS; DISPERSAL AB We analysed cytochrome c oxidase subunit I and NADH dehydrogenase subunit I sequence variation among 29 populations of a widely ranging southwestern springsnail (Pyrgulopsis micrococcus) and 18 regional congeners. Cladistic analyses of these sequences depict P. micrococcus as a polyphyletic composite of five well-supported clades. Sequence divergences among these clades and subclades imply the possible occurrence of as many as seven or eight cryptic species in addition to P. micrococcus. Our finding that P. micrococcus contains multiple, genetically distinct and geographically restricted lineages suggests that diversification within this highly speciose aquatic genus has been structured in large part by the operation of terrestrial barriers to gene flow. However, these sequence data also indicate that recent dispersal among hydrographically separated areas has occurred within one of these lineages, which we attribute to passive transport on migratory waterbirds. C1 Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. SW Missouri State Univ, Dept Biol, Springfield, MO 65804 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Systemat Biol, POB 37012,NHB W-305,MRC163, Washington, DC 20013 USA. EM hershler.robert@nmnh.si.edu NR 52 TC 71 Z9 71 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD OCT PY 2003 VL 12 IS 10 BP 2771 EP 2782 DI 10.1046/j.1365-294X.2003.01949.x PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 720GE UT WOS:000185252400022 PM 12969479 ER PT J AU Dearborn, DC Anders, AD Schreiber, EA Adams, RMM Mueller, UG AF Dearborn, DC Anders, AD Schreiber, EA Adams, RMM Mueller, UG TI Inter-island movements and population differentiation in a pelagic seabird SO MOLECULAR ECOLOGY LA English DT Article DE AFLP; Bayesian; frigatebird; genetics; island; mark-resight ID GENE FLOW; MITOCHONDRIAL-DNA; WANDERING ALBATROSSES; COLONIES; ATLANTIC; BIRDS; FRIGATEBIRD; DIMORPHISM; SHEARWATER; MURRELETS AB We used mark-resight data and amplified fragment length polymorphism (AFLP) markers to assess movements and gene flow between Central Pacific breeding colonies of the great frigatebird, Fregata minor. Of 715 adult frigatebirds marked on Tern Island and Johnston Atoll, 21.3% were resighted at other frigatebird colonies at least 582 km away. Mark-resight data indicated regular movement of males and females between Tern Island and Johnston Atoll (873 km apart), and less frequent movements to other islands; no birds marked on Tern or Johnston were seen on Christmas Island, but one was seen in the Philippines, 7627 km from where it was marked. Despite the regular occurrence of interisland movements, Bayesian analyses of AFLP data showed significant genetic differentiation between Tern Island and Johnston Atoll, and more pronounced differentiation between these two islands and the more distant Christmas Island. The AFLP profiles of three birds breeding on Tern Island fell within the profile-cluster typical for Christmas Island birds, both in a nonmetric multidimensional scaling analysis and in a population assignment test, suggesting dispersal events from Christmas Island to Tern Island. Several factors could explain the persistence of genetic structure despite frequent movements between colonies: many movements occurred during the nonbreeding season, many breeding-season movements did not involve mate-acquisition behaviours and individuals that do disperse may be selected against, as suggested by morphometric differences between colonies. The persistence of genetic structure among breeding colonies despite significant interisland movements suggests limits to the effectiveness of migration as a homogenizing force in this broadly distributed, extremely mobile species. C1 Bucknell Univ, Dept Biol, Lewisburg, PA 17837 USA. Bucknell Univ, Program Anim Behav, Lewisburg, PA 17837 USA. Penn State Univ, Program Ecol, University Pk, PA 16802 USA. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Dearborn, DC (reprint author), Bucknell Univ, Dept Biol, Lewisburg, PA 17837 USA. RI Adams, Rachelle/J-8846-2013 OI Adams, Rachelle/0000-0002-0918-9861 NR 49 TC 40 Z9 48 U1 2 U2 14 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 OCT PY 2003 VL 12 IS 10 BP 2835 EP 2843 DI 10.1046/j.1365-294X.2003.01931.x PG 9 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 720GE UT WOS:000185252400028 PM 12969485 ER PT J AU Sanjur, OI Carmona, JA Doadrio, I AF Sanjur, OI Carmona, JA Doadrio, I TI Evolutionary and biogeographical patterns within Iberian populations of the genus Squalius inferred from molecular data SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID FRESH-WATER FISHES; CHUB LEUCISCUS-CEPHALUS; CYTOCHROME-B GENE; PHYLOGENETIC-RELATIONSHIPS; MITOCHONDRIAL-DNA; MAXIMUM-LIKELIHOOD; BALKAN PENINSULA; CYPRINIDAE; PISCES; SEQUENCES AB Origins and biogeography of the chub, genus Squalius (formerly within the genus Leuciscus), in the Iberian Peninsula were inferred from comparison between patterns of geographic distribution and phylogenetic relationships among populations belonging to 14 European Squalius species. The phylogeny recovered was based on the complete sequence of the mitochondrial cytochrome b gene. Squalius species were grouped into three major clades. The basal clade, included species distributed across the ancient Paratethys Sea. The second clade included species from Central and East Europe and the northern areas of the Mediterranean basin towards Minor Asia. The third clade included species from the Mediterranean Peninsulas (Iberian, Italy, and Balkans). The Iberian Squalius species do not constitutes a monophyletic group. Our data indicate that the Iberian Peninsula was colonized at least twice by two different monophyletic lineages, a meridional group and a Central Europe group. The amount of species diversity found in the Iberian Peninsula and the phylogenetic relationships among these species, together with their geographic distribution, suggest that the Central Europe lineage colonized the Iberian Peninsula at a latter time. Our data indicate that the northeastern Iberian lineage is phylogenetically close to Greek populations of Squalius cephalus, while the second lineage formed a monophyletic group including Squalius pyrenaicus, Squalius carolitertii, Squalius aradensis, and Squalius torgalensis. The speciation process that. generated these species and the geographic structure of their populations, principally in S. pyrenaicus, can be attributed to paleo-geographical events like the ancient endorrheism and the development of hydrographic basins. (C) 2003 Elsevier Science (USA). All rights reserved. C1 CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad, E-28006 Madrid, Spain. Smithsonian Trop Res Inst, Balboa, Panama. RP Doadrio, I (reprint author), CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad, C-Jose Gutierrez Abascal 2, E-28006 Madrid, Spain. OI Doadrio, Ignacio/0000-0003-4863-9711 NR 54 TC 50 Z9 53 U1 0 U2 8 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 2003 VL 29 IS 1 BP 20 EP 30 DI 10.1016/S1055-7903(03)00088-5 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 722XP UT WOS:000185403600002 PM 12967604 ER PT J AU Sanchez, JA Lasker, HR Taylor, DJ AF Sanchez, JA Lasker, HR Taylor, DJ TI Phylogenetic analyses among octocorals (Cnidaria): mitochondrial and nuclear DNA sequences (lsu-rRNA, 16S and ssu-rRNA, 18S) support two convergent clades of branching gorgonians SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID SECONDARY-STRUCTURE; SARCOPHYTON GLAUCUM; GENE; CHARACTERS; MUTS; GORGONACEA; ALIGNMENT; ANTHOZOA; CLUSTAL; HOMOLOG AB Gorgonian octocorals lack corroborated hypotheses of phylogeny. This study reconstructs genealogical relationships among some octocoral species based on published DNA sequences from the large ribosomal subunit of the mitochondrial RNA (Isu-rRNA, 16S: 524 bp and 21 species) and the small subunit of the nuclear RNA (ssu-rRNA, 18S: 1815 bp and 13 spp) using information from insertions-deletions (INDELS) and the predicted secondary structure of the lsu-rRNA (16S). There were seven short (3-10bp) INDELS in the 18S with consistent phylogenetic information. The INDELS in the 16S corresponded to informative signature sequences homologous to the G13 helix found in Escherichia coli. We found two main groups of gorgonian octocorals using a maximum parsimony analysis of the two genes. One group corresponds to deep-water taxa including species from the suborders Calcaxonia and Scleraxonia characterized by an enlargement of the G13 helix. The second group has species from Alcyoniina, Holaxonia and again Scleraxonia characterized by insertions in the 18S. Gorgonian corals, branching colonies with a gorgonin-containing flexible multilayered axis (Holaxonia and Calcaxonia), do not form a monophyletic group. These corroborated results from maternally inherited (16S) and biparentally inherited (18S) genes support a hypothesis of independent evolution of branching in the two octocoral clades. (C) 2003 Elsevier Science (USA). All rights reserved. C1 SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA. RP Sanchez, JA (reprint author), Smithsonian Inst, Dept Systemat Biol, NMNH, POB 37012,MRC-0163, Washington, DC 20013 USA. NR 57 TC 38 Z9 42 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 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2003 VL 29 IS 1 BP 31 EP 42 DI 10.1016/S1055-7903(03)00090-3 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 722XP UT WOS:000185403600003 ER PT J AU Warren, BH Bermingham, E Bowie, RCK Prys-Jones, RP Thebaud, C AF Warren, BH Bermingham, E Bowie, RCK Prys-Jones, RP Thebaud, C TI Molecular phylogeography reveals island colonization history and diversification of western Indian Ocean sunbirds (Nectarinia : Nectariniidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE sunbirds; phylogeography; island colonization; molecular clock; Indian Ocean; Madagascar; Comoros; Seychelles ID MITOCHONDRIAL-DNA SEQUENCES; DAVIE-FRACTURE-ZONE; CANARY-ISLANDS; MOZAMBIQUE CHANNEL; CYTOCHROME-B; COMORES ARCHIPELAGO; EVOLUTIONARY RELATIONSHIPS; SYMPATRIC SPECIATION; DARWINS FINCHES; MTDNA SEQUENCES AB We constructed a phylogenetic hypothesis for western Indian Ocean sunbirds (Nectarinia) and used this to investigate the geographic pattern of their diversification among the islands of the Indian Ocean. A total of 1309 bp of mitochondrial sequence data was collected from the island sunbird taxa of the western Indian Ocean region, combined with sequence data from a selection of continental (African and Asian) sunbirds. Topological and branch length information combined with estimated divergence times are used to present hypotheses for the direction and sequence of colonization events in relation to the geological history of the Indian Ocean region. Indian Ocean sunbirds fall into two well-supported clades, consistent with two independent colonizations from Africa within the last 3.9 million years. The first clade contains island populations representing the species Nectarinia notata, while the second includes Nectarinia souimanga, Nectarinia humbloti, Nectarinia dussumieri, and Nectarinia coquereli. With respect to the latter clade, application of Bremer's [Syst. Biol. 41 (1992) 436] ancestral areas method permits us to posit the Comoros archipelago as the point of initial colonization in the Indian Ocean. The subsequent expansion of the souimanga clade across its Indian Ocean range occurred rapidly, with descendants of this early expansion remaining on the Comoros and granitic Seychelles. The data suggest that a more recent expansion from Anjouan in the Comoros group led to the colonization of Madagascar by sunbirds representing the souimanga clade. In concordance with the very young geological age of the Aldabra group, the sunbirds of this archipelago have diverged little from the Madagascar population; this is attributed to colonization of the Aldabra archipelago in recent times, in one or possibly two or more waves originating from Madagascar. The overall pattern of sunbird radiation across Indian Ocean islands indicates that these birds disperse across ocean barriers with relative ease, but that their subsequent evolutionary success probably depends on a variety of factors including prior island occupation by competing species. (C) 2003 Elsevier Science (USA). All rights reserved. C1 Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. Smithsonian Trop Res Inst, UNit 0948, Miami, FL 34002 USA. Museum Hist Nat, Bird Grp, Tring HP23 6AP, Herts, England. Univ Cape Town, Percy FitzPatrick Inst, ZA-7925 Cape Town, South Africa. UMR Evolut & Diversite Biol, F-31062 Toulouse 4, France. RP Warren, BH (reprint author), Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. EM warrenb@naos.si.edu RI Thebaud, Christophe/N-3916-2016; OI Thebaud, Christophe/0000-0002-8586-1234; Bowie, Rauri/0000-0001-8328-6021 NR 80 TC 78 Z9 82 U1 1 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2003 VL 29 IS 1 BP 67 EP 85 DI 10.1016/S1055-7903(03)00063-0 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 722XP UT WOS:000185403600006 PM 12967608 ER PT J AU Gillespie, JJ Kjer, KM Duckett, CN Tallamy, DW AF Gillespie, JJ Kjer, KM Duckett, CN Tallamy, DW TI Convergent evolution of cucurbitacin feeding in spatially isolated rootworm taxa (Coleoptera : Chrysomelidae; Galerucinae, Luperini) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Review DE pharmacophagy; convergence; cucurbitacins; pseudoreplicate reweighting; Bayesian analysis; loose receptor hypothesis; rRNA secondary structure ID WESTERN CORN-ROOTWORM; DIABROTICA-VIRGIFERA-VIRGIFERA; MOTH UTETHEISA-ORNATRIX; LEAF BEETLES COLEOPTERA; RNA SECONDARY STRUCTURE; POLLEN AMINO-ACIDS; RIBOSOMAL-RNA; PYRROLIZIDINE ALKALOIDS; PHYLOGENETIC ANALYSES; OPHRAELLA COLEOPTERA AB Historically, chemical ecologists assumed that cucurbitacin feeding and sequestration in rootworm leaf beetles is a remnant of an ancient association between the Luperini (Coleoptera: Chrysomelidae; Galerucinae) and Cucurbitaceae (ancestral host hypothesis). Under this premise, rootworms that do not develop on cucurbits but undergo pharmacophagous forays for cucurbitacins are thought to do so to supplement novel host diets that lack these bitter compounds. The ancestral host hypothesis is supported from studies of pyrrolizidine alkaloid pharmacophagy in Lepidoptera but has not been subjected to phylogenetic analysis within the Luperini. New evidence that this feeding behavior is better correlated with an adult affinity for pollen than with larval host offers the possibility that Old and New World rootworm species with an affinity for cucurbitacins converged on this behavior through apomorphic taste receptor modifications (loose receptor hypothesis). Here we test the monophyly of cucurbitacin feeding within the Luperini by using nuclear and mitochondrial sequence data to infer phylogenetic relationships among 49 taxa representing tribes of the Galerucinae and subtribes of the Luperini. The resulting phylogenetic hypothesis is mostly concordant with existing tribal and subtribal delineations within the Subfamily Galerucinae sensu stricto (Galerucinae not including the flea beetles). The establishment of ancestry among the subtribes of the Luperini refutes the monophyly of cucurbitacin feeding and cucurbit specialization, with the New World Diabroticina being paraphyletic to the Old World Aulacophorina and cosmopolitan Luperina. These data unambiguously support the convergent evolution of cucurbitacin feeding in rootworms and are inconsistent with the ancestral host hypothesis. (C) 2003 Elsevier Inc. All rights reserved. C1 Univ Delaware, Dept Entomol & Appl Ecol, Newark, DE 19717 USA. Texas A&M Univ, Dept Entomol, College Stn, TX 77843 USA. Rutgers State Univ, Dept Entomol, New Brunswick, NJ 08901 USA. Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Gillespie, JJ (reprint author), Univ Delaware, Dept Entomol & Appl Ecol, Newark, DE 19717 USA. OI Gillespie, Joseph/0000-0002-5447-7264 NR 101 TC 25 Z9 29 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2003 VL 29 IS 1 BP 161 EP 175 DI 10.1016/S1055-7903(03)00256-2 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 722XP UT WOS:000185403600015 PM 12967617 ER PT J AU Metcalfe, TS Montgomery, MH Kawaler, SD AF Metcalfe, TS Montgomery, MH Kawaler, SD TI Probing the core and envelope structure of DBV white dwarfs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : evolution; stars : individual : GD 358; stars : individual : CBS 114; stars : interiors; stars : oscillations; white dwarfs ID WHOLE EARTH TELESCOPE; STARS; ASTEROSEISMOLOGY; GD-358; C-12(ALPHA; EVOLUTION; RICH AB We investigate the global pulsation properties of DBV white dwarf models that include the double-layered envelope structure expected from time-dependent diffusion calculations, as well as a non-uniform C/O core expected from prior nuclear burning. We compare these models with otherwise identical models containing a pure C core to determine whether the addition of core structure leads to any significant improvement. Our double-layered envelope model fit to GD 358 that includes an adjustable C/O core is significantly better than our pure C core fit (7sigma improvement). We find a comparable improvement from fits to a second DBV star, CBS 114, though the values of the derived parameters may be more difficult to reconcile with stellar evolution theory. We find that our models are systematically cooler by 1900 K relative to the similar models of Fontaine & Brassard (2002). Although a fit to their model reproduces the mass and envelope structure almost exactly, we are unable to reproduce the absolute quality of their fit to GD 358. Differences between the constitutive physics employed by the two models may account for both the temperature offset and the period residuals. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. RP Metcalfe, TS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Metcalfe, Travis/A-9388-2008 OI Metcalfe, Travis/0000-0003-4034-0416 NR 30 TC 22 Z9 22 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 OCT 1 PY 2003 VL 344 IS 4 BP L88 EP L92 DI 10.1046/j.1365-8711.2003.07128.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 725GU UT WOS:000185536100008 ER PT J AU Schwartz, DA Marshall, HL Miller, BP Worrall, DM Birkinshaw, M Lovell, JEJ Jauncey, DL Perlman, ES Murphy, DW Preston, RA AF Schwartz, DA Marshall, HL Miller, BP Worrall, DM Birkinshaw, M Lovell, JEJ Jauncey, DL Perlman, ES Murphy, DW Preston, RA TI CHANDRA observations of X-ray jet structure on kpc to Mpc scales SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Meeting on the Physics of Relativistic Jets in the Chandra and XMM Era CY SEP 23-27, 2002 CL BOLOGNA, ITALY ID INVERSE COMPTON; RADIATION; EMISSION AB With its exquisite spatial resolution of better than 0.5 arcsec, the Chandra observatory is uniquely capable of resolving and studying the spatial structure of extragalactic X-ray jets on scales of a few to a few hundred kilo-parsec. Our analyses of four recent Chandra images of quasar jets interpret the X-ray emission as inverse Compton scattering of high energy electrons on the cosmic microwave background. We infer that these jets are in bulk relativistic motion, carrying kinetic powers upwards of 10(46) ergs s(-1) to distances of hundreds of kpc, with very high efficiency. (C) 2003 Elsevier B.V. All rights reserved. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Cambridge, MA 02139 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Schwartz, DA (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 8 Z9 9 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 OCT PY 2003 VL 47 IS 6-7 BP 461 EP 465 DI 10.1016/S1387-6473(03)00072-1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737CH UT WOS:000186210600012 ER PT J AU Siemiginowska, A Stanghellini, C Brunetti, G Aldcroft, TL Bechtold, J Elvis, M Harris, DE AF Siemiginowska, A Stanghellini, C Brunetti, G Aldcroft, TL Bechtold, J Elvis, M Harris, DE TI Discovery of X-ray jets in GPS sources SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Meeting on the Physics of Relativistic Jets in the Chandra and XMM Era CY SEP 23-27, 2002 CL BOLOGNA, ITALY DE quasars : individual (PKS1127-145, B2 0738+313); galaxies : jets; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRUM RADIO-SOURCES; CHANDRA DISCOVERY; PERFORMANCE; EMISSION AB Giga-Hertz Peaked Spectrum (GPS) and Compact Steep Spectrum (CSS) sources have compact radio morphologies (<1 to 10 kpc, respectively). They have been interpreted as either young counterparts of FR I radio galaxies or as 'frustrated' AGN, in which the radio jets are not able to penetrate the host galaxy's gas and dust. The high spatial resolution of Chandra allows us to study the environment of these sources within arcsec of the strong compact core. Here, we present the discovery of X-ray jets in the two GPS quasars, indicating that X-ray emission associated with relativistic plasma is present at large distances from the GPS quasar. (C) 2003 Elsevier B.V. All rights reserved. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CNR, I-40126 Bologna, Italy. CNR, Noto, Italy. RP Siemiginowska, A (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. OI Stanghellini, Carlo/0000-0002-6415-854X; Brunetti, Gianfranco/0000-0003-4195-8613 NR 16 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD OCT PY 2003 VL 47 IS 6-7 BP 467 EP 469 DI 10.1016/S1387-6473(03)00073-3 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737CH UT WOS:000186210600013 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 Moving relativistic large-scale X-ray jets in the microquasar XTE J1550-564 SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Meeting on the Physics of Relativistic Jets in the Chandra and XMM Era CY SEP 23-27, 2002 CL BOLOGNA, ITALY ID EMISSION; RADIO AB We have discovered large-scale moving X-ray and radio jets from the microquasar XTE J1550 - 564. Using X-ray and radio observations performed between 2000 and 2002, we showed that plasma ejected from XTE J1550 - 564 has been able to travel at relativistic velocities during many years, with evidence for gradual deceleration. The broadband spectrum of the jets is consistent with synchrotron emission from high energy particles accelerated in shocks. Full details can be found in Corbel et al. [Science 298 (2002a) 196], Karret et al. [ApJ 582 (2003) 933] and Tomsick et al. [ApJ (2003) 945]. (C) 2003 Elsevier B.V. All rights reserved. C1 CEA Saclay, Serv Astrophys Fed APC, 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, Inst Astron, NL-3508 TA Utrecht, Netherlands. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Corbel, S (reprint author), CEA Saclay, Serv Astrophys Fed APC, F-91191 Gif Sur Yvette, France. NR 10 TC 3 Z9 3 U1 0 U2 1 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 OCT PY 2003 VL 47 IS 6-7 BP 477 EP 480 DI 10.1016/S1387-6473(03)00075-7 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737CH UT WOS:000186210600015 ER PT J AU Cagnoni, I Nicastro, F Maraschi, L Treves, A Tavecchio, F AF Cagnoni, I Nicastro, F Maraschi, L Treves, A Tavecchio, F TI XMM-Newton observations of absorption features towards PKS 2155-304 SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Meeting on the Physics of Relativistic Jets in the Chandra and XMM Era CY SEP 23-27, 2002 CL BOLOGNA, ITALY DE BL lacertae objects; individual (PKS 2155-304); intergalactic medium; large-scale structure of universe; quasars; absorption lines ID X-RAY FOREST; ATOMIC OXYGEN; ULTRAVIOLET; VICINITY; CLOUDS; EDGE AB We present XMM-Newton grating spectra of the bright BL Lac object PKS 2155 - 304 taken in November 2000. Various absorption features are detected in the range 5-38 A. The results are compared with those recently obtained with Chandra gratings [ApJ 573 (2002) 157; Nature, 421 (2003) 719]. We discuss whether the absorption occurs at the source (in the host galaxy or in a jet), in the Galactic halo, or in the intervening cluster. We are not able to confirm the proposal by [ApJL 572 (2002) L127] that a hot medium is responsible for an absorption feature at an intermediate redshift. (C) 2003 Elsevier B.V. All rights reserved. C1 Univ Insubria, Dip Sci, I-22100 Como, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Brera, I-20121 Milan, Italy. RP Cagnoni, I (reprint author), Univ Insubria, Dip Sci, Via Valleggio 11, I-22100 Como, Italy. OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 17 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD OCT PY 2003 VL 47 IS 6-7 BP 561 EP 563 DI 10.1016/S1387-6473(03)00093-9 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737CH UT WOS:000186210600033 ER PT J AU Kraft, RP Hardcastle, MJ Forman, WR Jones, C Murray, SS Worrall, DM AF Kraft, RP Hardcastle, MJ Forman, WR Jones, C Murray, SS Worrall, DM TI High resolution X-ray observation and monitoring of the X-ray jet and radio lobes of centaurus A SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Meeting on the Physics of Relativistic Jets in the Chandra and XMM Era CY SEP 23-27, 2002 CL BOLOGNA, ITALY DE active galaxies; individual galaxies (Centaurus A, NGC 5128); early-type galaxies; extragalactic jets; X-rays AB We summarize the results of our Chandra AO-1 observations of the X-ray jet in the nearby radio galaxy Centaurus A, and discuss preliminary results from our ongoing monitoring campaign, the first observation of which was made in September, 2002. Our AO-1 observations demonstrate that there are small but significant differences in the X-ray and radio morphologies of the jet in this prototypical FR I radio galaxy. We conclude that the X-ray emission was due to synchrotron radiation from a population of ultra-relativistic electrons, and that the morphological differences can be explained by physical separation of the radio and X-ray emitting electron populations through aging and diffusion. This synchrotron hypothesis can be tested because the lifetime of the X-ray emitting electrons is only a few tens of years. Statistically significant spectral and intensity variations in the knots of the jet should be detectable with Chandra on the timescales of years. As part of our monitoring campaign, we are searching for super-luminal motion in the knots of the jet to evaluate the importance of bulk relativistic motion. Finally, we also discuss the nature of the X-ray enhancement in the vicinity of the outer half of the inner SW radio lobe. (C) 2003 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. RP Kraft, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012; OI Hardcastle, Martin/0000-0003-4223-1117; Forman, William/0000-0002-9478-1682 NR 5 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD OCT PY 2003 VL 47 IS 6-7 BP 625 EP 628 DI 10.1016/S1387-6473(03)00108-8 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737CH UT WOS:000186210600048 ER PT J AU Yuan, F Markoff, S Falcke, H Biermann, PL AF Yuan, F Markoff, S Falcke, H Biermann, PL TI Jet-disk coupling model for low luminosity AGNs SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Meeting on the Physics of Relativistic Jets in the Chandra and XMM Era CY SEP 23-27, 2002 CL BOLOGNA, ITALY DE accretion; accretion disks; galaxies : active; galaxies : nuclei ID ACTIVE GALACTIC NUCLEI; A-ASTERISK; NGC-4258 AB Low-luminosity AGNs (LLAGNs) are a very important class of sources since they occur in a significant fraction of local galaxies. Their spectra differ significantly from the canonical luminous AGNs, most notably by the absence of the 'big blue bump'. Up until now there is no model which can explain the spectra of LLAGNs. Taking NGC 4258 as an example, we propose a coupled jet-disk model for some LLAGNs. (C) 2003 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Max Planck Inst Radioastron, D-5300 Bonn, Germany. RP Yuan, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. RI Falcke, Heino/H-5262-2012 OI Falcke, Heino/0000-0002-2526-6724 NR 9 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD OCT PY 2003 VL 47 IS 6-7 BP 705 EP 707 DI 10.1016/S1387-6473(03)00127-1 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737CH UT WOS:000186210600067 ER PT J AU Esry, BD Sadeghpour, HR AF Esry, BD Sadeghpour, HR TI Split diabatic representation SO PHYSICAL REVIEW A LA English DT Article ID ATOMIC-COLLISIONS; CHARGE-TRANSFER; HE AB A split diabatic representation is proposed as a technique for generating diabatic potential curves with the maximal physical content and favorable computational characteristics. This method is a mixed adiabatic-diabatic representation, in which smoothly varying couplings appear in both the kinetic- and potential-energy matrices. It requires the solution of the first-order differential equation for the transformation matrix of the standard strict diabatic representation for which an efficient numerical scheme is also presented. A transformation propagator, akin to the Cayley-Hamiltonian time evolution operator, is employed to obtain the diabatic states while preserving unitarity. Several examples illustrate the advantages of the proposed split diabatic representation. C1 Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. Kansas State Univ, JR Macdonald Lab, Manhattan, KS 66506 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Esry, BD (reprint author), Kansas State Univ, Dept Phys, Cardwell Hall, Manhattan, KS 66506 USA. RI Esry, Brett/H-7511-2013 OI Esry, Brett/0000-0003-3207-8526 NR 23 TC 1 Z9 1 U1 0 U2 4 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 OCT PY 2003 VL 68 IS 4 AR 042706 DI 10.1103/PhysRevA.68.042706 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 750PJ UT WOS:000187004700064 ER PT J AU Henry, TJ Brambila, J AF Henry, TJ Brambila, J TI First report of the neotropical damsel bug Alloeorhynchus trimacula (Stein) in the United States, with new records for two other nabid species in Florida (Heteroptera : Nabidae : Prostemmatinae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; Hemiptera; Nabidae; damsel bug; Alloeorhynchus trimacula; Pagasa confusa; Phorticus collaris; new records; United States; Florida ID NORTH-AMERICA AB The first report of the prostemmatine nabid Alloeorhynchus trimacula (Stein) in the United States is given based on specimens collected in two counties of Florida. We diagnose the genus Alloeorhynchus, redescribe and provide photographs of the adult male and female of A. trimacula, and give other diagnostic information to help separate this newly discovered immigrant from other North American Nabidae. Also given are the first report of Phorticus collaris (Stal) in Florida and additional Florida records for Pagasa confusa Kerzhner. C1 Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, Systemat Entomol Lab,PSI, Washington, DC 20560 USA. Florida Dept Agr & Consumer Serv, Florida State Collect Anthropods, Div Plant Ind, Gainesville, FL 32614 USA. RP Henry, TJ (reprint author), Smithsonian Inst, Museum Natl Hist Nat, USDA ARS, Systemat Entomol Lab,PSI, POB 37012,MRC-168, Washington, DC 20560 USA. NR 25 TC 3 Z9 3 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2003 VL 105 IS 4 BP 801 EP 808 PG 8 WC Entomology SC Entomology GA 732WV UT WOS:000185969300001 ER PT J AU Flint, OS AF Flint, OS TI The genus Macrostemum kolenati (Trichoptera : Hydropsychidae) in Sri Lanka SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Macrostemum; Hydropsychidae; Sri Lanka; new species; descriptions; illustrations; wings AB Based on the study of types and, mostly, new material collected between 1970 and 1980, nine species of Macrostemum Kolenati are recognized on the island of Sri Lanka. The species Macronema multifarium (Walker), M. nebulosum (Hagen), and M. sepultum (Hagen) are redescribed based on the first material collected since the original types in the 1850s, and are formally transferred to Macrostemum (all n. comb.). Macrostemum splendidum (Hagen) and M. pseudoneura (Brauer) are redescribed, and M. ethelda (Banks) from southern India is reduced to a subspecies of the latter (n. status). Macrostemum indistinctum (Banks), a species widespread in southeastern Asia, is newly recorded from the island and M. saowapa Malicky is placed in its synonymy (n. syn.). Macrostemum barnardi, M. krombeini, and M. malickyi are newly described. All species are described, the male genitalia figured (M. krombeini and M. multifarium are known only from females), and photos of the wing patterns presented. The species Macronema obliquum Hagen is transferred to the genus Marilia in the Odontoceridae (n. comb.). C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. RP Flint, OS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. NR 16 TC 1 Z9 1 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2003 VL 105 IS 4 BP 816 EP 831 PG 16 WC Entomology SC Entomology GA 732WV UT WOS:000185969300003 ER PT J AU Miller, SE Novotny, V Basset, Y AF Miller, SE Novotny, V Basset, Y TI Studies on New Guinea moths. 1. Introduction (Lepidoptera) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE malesia; Papua new guinea; Lepidoptera; biodiversity; rearing; community ecology ID PAPUA-NEW-GUINEA; RAIN-FOREST; COMMUNITIES; HERBIVORES; INSECTS AB This is the first in a series of papers providing taxonomic data in support of ecological and biogeographic studies of moths in New Guinea. The primary study is an extensive inventory of the caterpillar fauna of a lowland rainforest site near Madang, Papua New Guinea, from 1994-2001. The inventory focused on the Lepidoptera community on 71 woody plant species representing 45 genera and 23 families. During the study, 46,457 caterpillars representing 585 species were sampled, with 19,660 caterpillars representing 441 species reared to adults. This introductory contribution is intended to provide background on the project, including descriptions of the study site, sampling methods, and taxonomic methods. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Acad Sci Czech Republic, Inst Entomol, CR-37005 Ceske Budejovice, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice 37005, Czech Republic. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Miller, SE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. EM miller.scott@nmnh.si RI Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; OI Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 36 TC 9 Z9 9 U1 0 U2 3 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 2003 VL 105 IS 4 BP 1034 EP 1042 PG 9 WC Entomology SC Entomology GA 732WV UT WOS:000185969300022 ER PT J AU Terio, KA Marker, L Overstrom, EW Brown, JL AF Terio, KA Marker, L Overstrom, EW Brown, JL TI Analysis of ovarian and adrenal activity in Namibian cheetahs SO SOUTH AFRICAN JOURNAL OF WILDLIFE RESEARCH LA English DT Article DE cheetah; faecal steroids; estrogen; progestagen; corticoid; reproduction ID NORTH-AMERICAN ZOOS; ACINONYX-JUBATUS; ADRENOCORTICAL FUNCTION; INDUCED OVULATION; CLOUDED LEOPARD; FECAL STEROIDS; STRESS; REPRODUCTION; PROGESTERONE; METABOLISM AB Captive breeding of cheetahs (Acinonyx jubatus) has had limited success because a high percentage of captive females exhibit a lack of ovarian activity. This study examined concentrations of ovarian and adrenal hormones in wild-caught cheetahs (n = 3) housed in large outdoor enclosures on private game ranches in Namibia. Cheetahs were monitored for a 16-month period to investigate the effect of season on ovarian and adrenal function. Secretory profiles of oestradiol, progestagen, and cortisol metabolites were quantified non-invasively using faecal steroid analysis. All three cheetahs exhibited ovarian activity; however, none cycled continuously. Periods of anoestrus occurred during overlapping periods between August and December 1994, but not during the same time period in 1995. Mean duration of the oestrous cycle, oestrus period and baseline concentrations of reproductive hormones were consistent with those observed in other captive cheetah populations. Concentrations of faecal corticoids were lower than those from captive cheetahs in North America. There was no correlation between adrenal activity and ovarian function. Spontaneous ovulation was documented in one cheetah. These findings support those of earlier studies that even under natural and, therefore, presumably ideal environmental conditions, reproductive activity in captive cheetahs is not continuous. C1 Univ Calif Davis, Sch Vet Med, Davis, CA 95616 USA. Tufts Univ, Sch Vet Med, Grafton, MA USA. Cheetah Conservat Fund, Windhoek, Namibia. Natl Zool Pk, Conservat & Res Ctr, Smithsonian Inst, Front Royal, VA USA. RP Terio, KA (reprint author), Univ Calif Davis, Sch Vet Med, Davis, CA 95616 USA. NR 32 TC 10 Z9 11 U1 1 U2 17 PU SOUTHERN AFRICAN WILDLIFE MANAGEMENT ASSOC PI BLOUBERGSTRAND PA P O BOX 217, BLOUBERGSTRAND 7437, SOUTH AFRICA SN 0379-4369 J9 S AFR J WILDL RES JI South Afr. J. Wildl. Res. PD OCT PY 2003 VL 33 IS 2 BP 71 EP 78 PG 8 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 758NW UT WOS:000187641000003 ER PT J AU Collin, R AF Collin, R TI Phylogenetic relationships among calyptraeid gastropods and their implications for the biogeography of marine speciation SO SYSTEMATIC BIOLOGY LA English DT Review DE biogeographic barriers; Calyptraea; Crepidula; Crucibulum; cytochrome oxidase I; 16S; sympatric speciation ID LENGTH DIFFERENCE TEST; POPULATION-STRUCTURE; CREPIDULA-FORNICATA; DISCRETE CHARACTERS; LIKELIHOOD APPROACH; MOLECULAR-GENETICS; HABITAT SELECTION; SPECIES COMPLEX; DNA-SEQUENCES; SEX-CHANGE AB Although calyptraeid gastropods are not well understood taxonomically, in part because their simple plastic shells are the primary taxonomic character, they provide an ideal system to examine questions about evolution in the marine environment. I conducted a phylogenetic analysis of calyptraeid gastropods using DNA sequence data from mitochondrial cytochrome oxidase I (COI) and 16S genes and the nuclear 28S gene. The resultant phylogeny was used to examine the biogeographic patterns of speciation in the Calyptraeidae. Parsimony and Bayesian analyses of the combined data sets for 94 calyptraeid operational taxonomic units and 24 outgroups produced well-resolved phylogenies. Both approaches resulted in identical sister-species relationships, and the few differences in deeper topology did not affect biogeographic inferences. The geographic distribution of the species included here demonstrate numerous dispersal events both between the Pacific and Atlantic oceans and across the equator. When parsimony is used to reconstruct the movement from the Pacific to the Atlantic oceans on the phylogeny, there are 12 transitions between oceans, primarily from the Pacific to the Atlantic. When the latitude is coded as north versus south of the equator, the most-parsimonious reconstruction gives the origin of calyptraeids in the north followed by 15 dispersal events to regions south of the equator and no returns to the north. Many clades of the most closely related species are either sympatric or occur along a single coastline. Closely related species can, however, occur in such divergent regions as Southern California and South Africa. There is little evidence for sister-species pairs or larger clades having been split by the Isthmus of Panama or the Benguela upwelling, but the East Pacific Barrier appears to separate the most basal taxa from the rest of the family. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Collin, Rachel/G-2001-2010; OI Collin, Rachel/0000-0001-5103-4460 NR 124 TC 77 Z9 80 U1 3 U2 17 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD OCT PY 2003 VL 52 IS 5 BP 618 EP 640 DI 10.1080/10635150390235430 PG 23 WC Evolutionary Biology SC Evolutionary Biology GA 728TM UT WOS:000185732500004 PM 14530130 ER PT J AU Stine, JK AF Stine, JK TI Me, myself and infrastructure: Private lives and public works in America - The National Building Museum, Washington, DC SO TECHNOLOGY AND CULTURE LA English DT Review C1 Smithsonian Inst, Amer Museum Nat Hist, Washington, DC 20560 USA. RP Stine, JK (reprint author), Smithsonian Inst, Amer Museum Nat Hist, Washington, DC 20560 USA. NR 2 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 2003 VL 44 IS 4 BP 778 EP 785 DI 10.1353/tech.2003.0185 PG 8 WC History & Philosophy Of Science SC History & Philosophy of Science GA 752PZ UT WOS:000187177500006 ER PT J AU Hacker, BC AF Hacker, BC TI Throwing fire: Projectile technology through history. SO TECHNOLOGY AND CULTURE 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 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 2003 VL 44 IS 4 BP 802 EP 803 DI 10.1353/tech.2003.0162 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 752PZ UT WOS:000187177500011 ER PT J AU Finn, B AF Finn, B TI Sir Charles Wheatstone, FRS, 1802-1875. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Finn, B (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 2003 VL 44 IS 4 BP 820 EP 822 DI 10.1353/tech.2003.0158 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 752PZ UT WOS:000187177500022 ER PT J AU Keita, SOY AF Keita, SOY TI A study of vault porosities in early Upper Egypt from the Badarian through Dynasty I SO WORLD ARCHAEOLOGY LA English DT Article DE palaeopathology; predynastic Egypt; porotic hyperostosis; schistosomiasis; hookworm ID POROTIC HYPEROSTOSIS; CHILDHOOD; DISEASE; ANEMIA; SCHISTOSOMIASIS; HYPOPLASIAS; IRON AB Predynastic and Early Dynastic Upper Egyptian adult crania were assessed for porotic hyperostosis. This lesion (in adults) is believed most often to reflect iron deficiency anaemia that has occurred in childhood. The results indicate an increase in frequency from the Badarian to Naqada I with a subsequent decline to Dynasty I. This pattern is discussed in terms of subsistence change and its possible relationship to exposure to schistosomiasis, hookworm, and various possible adaptive responses. C1 Howard Univ, Natl Human Genome Ctr, Washington, DC 20059 USA. Smithsonian Inst, Nat Hist Museum, Dept Anthropol, Washington, DC 20560 USA. RP Keita, SOY (reprint author), Howard Univ, Natl Human Genome Ctr, Washington, DC 20059 USA. NR 48 TC 3 Z9 3 U1 0 U2 2 PU ROUTLEDGE TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0043-8243 J9 WORLD ARCHAEOL JI World Archaeol. PD OCT PY 2003 VL 35 IS 2 BP 210 EP 222 DI 10.1080/0043824032000111380 PG 13 WC Archaeology SC Archaeology GA 734BJ UT WOS:000186035100005 ER PT J AU Rusin, D Kochanek, CS Keeton, CR AF Rusin, D Kochanek, CS Keeton, CR TI Self-similar models for the mass profiles of early-type lens galaxies SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : elliptical and lenticular, cD; galaxies : structure; gravitational lensing ID DIGITAL SKY SURVEY; SURFACE BRIGHTNESS GALAXIES; DARK-MATTER SUBSTRUCTURE; FIELD ELLIPTIC GALAXIES; GRAVITATIONAL LENS; FUNDAMENTAL PLANE; TIME-DELAY; HUBBLE CONSTANT; LUMINOSITY EVOLUTION; INTERNAL STRUCTURE AB We introduce a self-similar mass model for early-type galaxies and constrain it using the aperture mass-radius relations determined from the geometries of 22 gravitational lenses. The model consists of two components: a concentrated component, which traces the light distribution, and a more extended power-law component (rho proportional to r(-n)), which represents the dark matter. We find that lens galaxies have total mass profiles that are nearly isothermal, or slightly steeper, on the several-kiloparsec radial scale spanned by the lensed images. In the limit of a single-component, power-law radial profile, the model implies n = 2.07 +/- 0.13, consistent with isothermal ( n = 2). Models in which mass traces light are excluded at higher than 99% confidence. An n = 1 cusp (such as the Navarro-Frenk-White profile) requires a projected dark matter mass fraction of f(cdm) = 0.22 +/- 0.10 inside two effective radii. These are the best statistical constraints yet obtained on the mass profiles of lenses and provide clear evidence for a small but nonzero dark matter mass fraction in the inner regions of early-type galaxies. In addition, we derive the first strong-lensing constraint on the relation between the stellar mass-to-light ratio Y and galaxy luminosity L, Y proportional to L0.14(-0.12)(+0.16) which is consistent with the relation suggested by the fundamental plane. Finally, we apply our self-similar mass models to current problems regarding the interpretation of time delays and flux ratio anomalies in gravitational lens systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Rusin, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 113 TC 125 Z9 125 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 2003 VL 595 IS 1 BP 29 EP 42 DI 10.1086/377356 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 721VC UT WOS:000185338300004 ER PT J AU Risaliti, G Maiolino, R Marconi, A Bassani, L Berta, S Braito, V Della Ceca, R Franceschini, A Salvati, M AF Risaliti, G Maiolino, R Marconi, A Bassani, L Berta, S Braito, V Della Ceca, R Franceschini, A Salvati, M TI Revealing the active galactic nucleus in the superantennae through L-band spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (IRAS 19254-7245); infrared : galaxies ID ULTRALUMINOUS INFRARED GALAXIES; X-RAY; IRAS-19254-7245; ABSORPTION; EMISSION; STARBURSTS; SPECTRA AB We present an L-band spectrum of the ultraluminous infrared galaxy IRAS 19254 - 7245 ( the Superantennae), obtained with the Infrared Spectrometer and Array Camera on the Very Large Telescope. The high signal-to-noise ratio allows us to study the main spectral features with unprecedented detail for an extragalactic source. We argue that the main energy source in the IR is an obscured active galactic nucleus. This is indicated by the low equivalent width of the 3.3 mum polycyclic aromatic hydrocarbon feature, the broad absorption feature at 3.4 mum, and the steep continuum at lambda > 3.7 mum (f(lambda)proportional tolambda(2.7)). The substructure of the 3.4 mum absorption feature indicates that the absorption is due to hydrocarbon chains of six to seven carbon atoms. C1 INAF, Osservatorio Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist Tecnol & Studio Radiaz Extraterr, I-40129 Bologna, Italy. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. INAF, Osservatorio Astron Brera, I-20121 Milan, Italy. RP Risaliti, G (reprint author), INAF, Osservatorio Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; Risaliti, Guido/0000-0002-3556-977X; Braito, Valentina/0000-0002-2629-4989 NR 21 TC 22 Z9 22 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2003 VL 595 IS 1 BP L17 EP L20 DI 10.1086/378842 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 721VE UT WOS:000185338500005 ER PT J AU Balakrishnan, N Dalgarno, A AF Balakrishnan, N Dalgarno, A TI On the isotope effect in F+HD reaction at ultracold temperatures SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID POTENTIAL-ENERGY SURFACES; BOSE-EINSTEIN CONDENSATE; F+H-2->HF+H REACTION; CROSS-SECTIONS; COLLISIONS; MOLECULES; DYNAMICS; RELAXATION; EXCITATION; RESONANCE AB Isotope branching in the F + HD reaction is investigated at ultracold temperatures. It is found that in the limit of zero temperatures, the rate coefficient for HF formation in the F + HD (v = 0, j = 0) reaction is a factor of 5.5 greater than that of DF formation. The difference is attributed to the more efficient tunneling of the lighter atom. For HD molecules initially in the j = I excited rotational level, a clear preference is seen for chemical reaction leading to HF and DF products with an HF/DF branching ratio of 5.2 rather than for nonreactive rotational quenching. C1 Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Univ Nevada, Dept Chem, 4505 Maryland Pkwy, Las Vegas, NV 89154 USA. EM naduvala@unlv.edu NR 42 TC 35 Z9 35 U1 0 U2 7 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD SEP 18 PY 2003 VL 107 IS 37 BP 7101 EP 7105 DI 10.1021/jp022654v PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 721XY UT WOS:000185344800006 ER PT J AU Sari, L McCarthy, MC Schaefer, HF Thaddeus, P AF Sari, L McCarthy, MC Schaefer, HF Thaddeus, P TI Mono- and dibridged isomers of Si2H3 and Si2H4: the true ground state global minima. Theory and experiment concert SO JOURNAL OF THE AMERICAN CHEMICAL SOCIETY LA English DT Article ID SILICON-CONTAINING MOLECULES; ELECTRONIC-STRUCTURE; HARTREE-FOCK; SPECTRA; ABINITIO; DISILENE; CARBON; DECOMPOSITION; SILYLSILYLENE; ENTHALPIES AB Highly correlated ab initio coupled-cluster theories (e.g., CCSD(T), CCSDT) were applied on the ground electronic states Of Si2H3 and Si2H4, with substantive basis sets. A total of 10 isomers, which include mono- and dibridged structures, were investigated. Scalar relativistic corrections and zero-point vibrational energy corrections were included to predict reliable energetics. For Si2H3, we predict an unanticipated monobridged H2Si-H-Si-like structure (C-s, (2)A") to be the lowest energy isomer, in constrast to previous studies which concluded that either H3Si-Si (C-s, (2)A") or near-planar H2Si-SiH (C-1, (2)A) is the global minimum. Our results confirm that the disilene isomer, H2Si-SiH2, is the lowest energy isomer for Si2H4 and that it has a trans-bent structure (C-2h, Ag-1). In addition to the much studied silylsilylene, H3Si-SiH, we also find that a new monobridged isomer H2Si-H-SiH (C-1, (1)A, designated 2c) is a minimum on the potential energy surface and that it has comparable stability; both isomers are predicted to lie about 7 kcal/mol above disilene. By means of Fourier transform microwave spectroscopy of a supersonic molecular beam, the rotational spectrum of this novel Si2H4 isomer has recently been measured in the laboratory, as has that of the planar H2Si-SiH radical. Harmonic vibrational frequencies as well as infrared intensities of all 10 isomers were determined at the cc-pVTZ CCSD(T) level. C1 Univ Georgia, Ctr Computat Quantum Chem, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schaefer, HF (reprint author), Univ Georgia, Ctr Computat Quantum Chem, Athens, GA 30602 USA. NR 45 TC 47 Z9 48 U1 2 U2 12 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0002-7863 J9 J AM CHEM SOC JI J. Am. Chem. Soc. PD SEP 17 PY 2003 VL 125 IS 37 BP 11409 EP 11417 DI 10.1021/ja0300923 PG 9 WC Chemistry, Multidisciplinary SC Chemistry GA 721WQ UT WOS:000185341800063 PM 16220964 ER PT J AU Schroll, S AF Schroll, S TI Art: A new history. SO LIBRARY JOURNAL LA English DT Book Review C1 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 15 PY 2003 VL 128 IS 15 BP 54 EP 54 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 720ZV UT WOS:000185293300040 ER PT J AU Hutchinson, A AF Hutchinson, A TI True grizz: Glimpses of Fernie, Stahr, Easy, Dakota, and other real bears in the modern world. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Hutchinson, A (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 15 PY 2003 VL 128 IS 15 BP 87 EP 87 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 720ZV UT WOS:000185293300223 ER PT J AU Riley, S AF Riley, S TI Love me. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Riley, 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 15 PY 2003 VL 128 IS 15 BP 92 EP 92 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 720ZV UT WOS:000185293300247 ER PT J AU Steeghs, D AF Steeghs, D TI Extending emission-line Doppler tomography: mapping modulated line flux SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; line : profiles; techniques : spectroscopic; binaries : close; stars : individual : IP Peg; novae, cataclysmic variables ID ACCRETION DISKS; OUTBURST; MAXIMUM AB Emission-line Doppler tomography is a powerful tool that resolves the accretion flow in binaries on micro-arcsecond scales using time-resolved spectroscopy. I present an extension to Doppler tomography that relaxes one of its fundamental axioms and permits the mapping of time-dependent emission sources. Significant variability on the orbital period is a common characteristic of the emission sources that are observed in the accretion flows of cataclysmic variables and X-ray binaries. Modulation Doppler tomography maps sources varying harmonically as a function of the orbital period through the simultaneous reconstruction of three Doppler tomograms. One image describes the average flux distribution as is done in standard tomography, while the two additional images describe the variable component in terms of its sine and cosine amplitudes. I describe the implementation of such an extension in the form of the maximum entropy based fitting code MODMAP. Test reconstructions of synthetic data illustrate that the technique is robust and well constrained. Artefact-free reconstructions of complex emission distributions can be achieved under a wide range of signal-to-noise levels. An application of the technique is illustrated by mapping the orbital modulations of the asymmetric accretion disc emission in the dwarf nova IP Pegasi. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Southampton, Dept Phys & Astron, Southampton S017 1BJ, Hants, England. RP Steeghs, D (reprint author), Harvard Smithsonian Ctr Astrophys, MS-67,60 Garden St, Cambridge, MA 02138 USA. RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 16 TC 20 Z9 20 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 11 PY 2003 VL 344 IS 2 BP 448 EP 454 DI 10.1046/j.1365-8711.2003.06917.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 719EP UT WOS:000185190900014 ER PT J AU Yoshida, N Sugiyama, N Hernquist, L AF Yoshida, N Sugiyama, N Hernquist, L TI The evolution of baryon density fluctuations in multicomponent cosmological simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : N-body simulations; intergalactic medium; cosmology : theory; early Universe ID N-BODY SIMULATIONS; BACKGROUND ANISOTROPIES; PERTURBATIONS; DISCRETENESS; REIONIZATION; CODE AB We critically examine how the evolution of the matter density field in cosmological simulations is affected by details of setting up initial conditions. We show that it is non-trivial to realize an initial distribution of matter in N-body/hydrodynamic simulations so that the baryon and dark matter density fluctuations and their velocities evolve consistently as theoretically predicted. We perform a set of cosmological simulations and use them to distinguish and verify an appropriate method for generating initial conditions. We show that a straightforward way of applying the Zel'dovich approximation to each component using distinct transfer functions results in an incorrect growth of density fluctuations and that it is necessary to correct velocities at the initial epoch. The unperturbed uniform particle distribution must be also generated appropriately to avoid tight coupling of the baryonic and dark matter components. We recommend using independent 'glass' particle distributions, using distinct transfer functions for baryons and dark matter, and taking into account the difference in the velocity fields at the initialization epoch. The proposed method will be useful for studies of the evolution of the intergalactic medium and the formation of the first cosmological objects using numerical simulations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ, Tokyo 1818588, Japan. RP Yoshida, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Yoshida, Naoki/A-4305-2011 NR 41 TC 25 Z9 25 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 SEP 11 PY 2003 VL 344 IS 2 BP 481 EP 491 DI 10.1046/j.1365-8711.2003.06829.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 719EP UT WOS:000185190900019 ER PT J AU Sokasian, A Abel, T Hernquist, L Springel, V AF Sokasian, A Abel, T Hernquist, L Springel, V TI Cosmic reionization by stellar sources: Population II stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; intergalactic medium; quasars : general; diffuse radiation ID PARTICLE HYDRODYNAMICS SIMULATIONS; DIGITAL SKY SURVEY; RADIATIVE-TRANSFER; INTERGALACTIC MEDIUM; IONIZING-RADIATION; CLUMPY UNIVERSE; GALAXIES; HISTORY; QUASARS; Z-SIMILAR-TO-6 AB We study the reionization of the Universe by stellar sources using a numerical approach that combines fast 3D radiative transfer calculations with high-resolution hydrodynamical simulations. By supplementing a one-step radiative transfer code specifically designed for following ionization processes with an adaptive ray-tracing algorithm, we are able to speed up the calculations significantly to the point where handling a vast number of sources becomes technically feasible. This allows us to study how dim low-mass sources, excluded in previous investigations owing to computational limitations, affect the morphological evolution of the reionization process. Ionizing fluxes for the sources are derived from intrinsic star formation rates computed in the underlying hydrodynamical simulations. Analysis of numerically converged results for star formation rates and halo mass functions allows us to assess the consequences of not including low-mass objects and enables us to correct for resolution effects. With these corrections, we are able to reduce the effective mass resolution limit for sources to M similar to 4.0 x 10(7) h(-1) M-circle dot in a 10 h(-1) Mpc comoving box. Our calculations reveal that the process by which ionized regions in the intergalactic medium (IGM) percolate is complex and is especially sensitive to the inclusion of dim sources. Moreover, we find that, given the same level of cosmic star formation, the number of ionizing photons required to reionize the Universe is significantly overestimated if sources with masses below similar to10(9) h(-1) M-circle dot are excluded. This result stems from the fact that low-mass sources preferentially reside in less clumpy environments than their massive counterparts. Consequently, their exclusion has the net effect of concentrating more of the cosmic ionizing radiation in regions which have higher recombination rates. We present the results of our reionization simulation assuming a range of escape fractions for ionizing photons and make statistical comparisons with observational constraints on the neutral fraction of hydrogen at z similar to 6 derived from the z = 6.28 Sloan Digital Sky Survey (SDSS) quasar of Becker and coworkers. We find that, given the amplitude and form of the underlying star formation predictions, an escape fraction near f(esc) = 0.10-0.20 is most consistent with the observational results. In these models, reionization is expected to have occurred between z similar to 7-8, although the IGM remains fairly opaque until z similar or equal to 6. Our method is also capable of handling the simultaneous reionization of the helium component in the IGM, allowing us to explore the plausibility of the scenario where sources with harder spectra are primarily responsible for reionization. In this case, we find that if the sources responsible for reionizing hydrogen by z similar to 8 had spectra similar to active galactic nuclei, then the helium component of the IGM should have been reionized by z similar to 6. We find that such an early reionization epoch for helium does not necessarily conflict with observational constraints obtained at z similar to 3, but may be challenged by future observations at higher redshifts. The recent WMAP measurements of the electron scattering optical depth (tau(e) = 0.17 +/- 0.04 according to the 'model independent' analysis of Kogut et al.) appear to be inconsistent with the relatively late onset of reionization by the normal Population II type stars that we consider. In order to simultaneously match the observations from the z = 6.28 SDSS quasar and the optical depth measurement from WMAP with the sources modelled here, we require a boosting factor for the number of ionizing photons released in the f(esc) = 0.20 model which evolves from unity at z = 6 to greater than or similar to50 by z similar to 18. Such a steep enhancement in the stellar production rate of ionizing photons would be consistent with an IMF that becomes more and more top heavy with increasing redshift. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Sokasian, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 147 Z9 147 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 SEP 11 PY 2003 VL 344 IS 2 BP 607 EP 624 DI 10.1046/j.1365-8711.2003.06847.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 719EP UT WOS:000185190900030 ER PT J AU Montgomery, MH Metcalfe, TS Winget, DE AF Montgomery, MH Metcalfe, TS Winget, DE TI The core/envelope symmetry in pulsating stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : analytical; stars : individual : GD358; stars : interiors; stars : oscillations; white dwarfs ID WHITE-DWARF GD-358; ASTEROSEISMOLOGY; C-12(ALPHA AB We demonstrate that there is an inherent symmetry in the way high-overtone stellar pulsations sample the core and the envelope, which can potentially lead to an ambiguity in the asteroseismologically derived locations of internal structures. We provide an intuitive example of the source of this symmetry by analogy with a vibrating string. For the stellar case, we focus on the white dwarf stars, establishing the practical consequences for high-order white dwarf pulsations both analytically and numerically. In addition, we verify the effect empirically by cross-fitting two different structural models, and we discuss the consequences that this approximate symmetry may have for past and present asteroseismological fits of the pulsating DBV, GD 358. Finally, we show how the signatures of composition transition zones that are brought about by physically distinct processes may be used to help alleviate this potential ambiguity in our asteroseismological interpretation of the pulsation frequencies observed in white dwarf stars. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Montgomery, MH (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RI Metcalfe, Travis/A-9388-2008 OI Metcalfe, Travis/0000-0003-4034-0416 NR 17 TC 42 Z9 42 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 11 PY 2003 VL 344 IS 2 BP 657 EP 664 DI 10.1046/j.1365-8711.2003.06853.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 719EP UT WOS:000185190900035 ER PT J AU Bloom, JS Frail, DA Kulkarni, SR AF Bloom, JS Frail, DA Kulkarni, SR TI Gamma-ray burst energetics and the gamma-ray burst Hubble diagram: Promises and limitations SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmological parameters; cosmology : miscellaneous; cosmology : observations; distance scale; gamma rays : bursts; supernovae : individual (SN 1998bw) ID STANDARD ENERGY RESERVOIR; RELATIVISTIC BLAST WAVES; BRIGHT OPTICAL AFTERGLOW; WIND INTERACTION-MODELS; BROAD-BAND AFTERGLOW; RICH GRB 981226; 25 APRIL 1998; HOST GALAXY; RADIO AFTERGLOW; SPACE-TELESCOPE AB We present a complete sample of 29 gamma- ray bursts ( GRBs) for which it has been possible to determine temporal breaks ( or limits) from their afterglow light curves. We interpret these breaks within the framework of the uniform conical jet model, incorporating realistic estimates of the ambient density and propagating error estimates on the measured quantities. In agreement with our previous analysis of a smaller sample, the derived jet opening angles of those 16 bursts with redshifts result in a narrow clustering of geometrically corrected gamma- ray energies about E gamma = 1.33 x 10(51) ergs; the burst- to- burst variance about this value is 0.35 dex, a factor of 2.2. Despite this rather small scatter, we demonstrate in a series of GRB Hubble diagrams that the current sample cannot place meaningful constraints upon the fundamental parameters of the universe. Indeed, for GRBs to ever be useful in cosmographic measurements, we argue the necessity of two directions. First, GRB Hubble diagrams should be based upon fundamental physical quantities such as energy, rather than empirically derived and physically ill- understood distance indicators ( such as those based upon prompt burst time- profiles and spectra). Second, a more homogeneous set should be constructed by culling subclasses from the larger sample. These subclasses, although now first recognizable by deviant energies, ultimately must be identifiable by properties other than those directly related to energy. We identify a new subclass of GRBs (" f- GRBs '') that appear both underluminous by factors of at least 10 and exhibit a rapid fading ( f(nu) proportional to t(-2)) at early times ( t less than or similar to 0.5 day). About 10% - 20% of observed long- duration bursts appear to be f- GRBs. C1 Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, MC 20, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. CALTECH, Palomar Observ 105 24, Pasadena, CA 91125 USA. RP Bloom, JS (reprint author), Harvard Soc Fellows, 78 Mt Auburn St, Cambridge, MA 02138 USA. NR 114 TC 320 Z9 322 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2003 VL 594 IS 2 BP 674 EP 683 DI 10.1086/377125 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600002 ER PT J AU Munoz, JA Falco, EE Kochanek, CS Lehar, J Mediavilla, E AF Munoz, JA Falco, EE Kochanek, CS Lehar, J Mediavilla, E TI The redshift distribution of flat-spectrum radio sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : distances and redshifts; gravitational lensing; radio continuum : galaxies ID GRAVITATIONALLY LENSED QUASAR; PHASE CALIBRATION SOURCES; LUMINOSITY FUNCTION; SUPERNOVAE; REGIONS; SKY AB The redshift distribution of flat- spectrum radio sources with 5 GHz flux densities S-5 greater than or similar to 5 mJy is a key component in using current radio lens surveys to probe the cosmological model. We have constructed the first flat- spectrum radio sample in the flux density range 3 - 20 mJy. Our new sample has 33 sources; we have determined the redshifts of 14 of these ( 42% complete). The low mean redshift, similar or equal to 0.75, of our faintest sample needs to be confirmed by further observations to improve the sample completeness. We also increased the redshift completeness of several surveys of brighter flat- spectrum sources. While the mean redshift similar or equal to 1.1 of flat- spectrum samples fainter than 1 Jy is nearly constant, the fraction of the sources identifiable as quasars steadily drops from similar to 80% to similar to 10% as the. flux density of the sources decreases. C1 Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. RP Munoz, JA (reprint author), Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. 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 SEP 10 PY 2003 VL 594 IS 2 BP 684 EP 694 DI 10.1086/377077 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600003 ER PT J AU Georgantopoulos, I Zezas, A AF Georgantopoulos, I Zezas, A TI Chandra observations of NGC 4698: A Seyfert 2 galaxy with no absorption SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4698); galaxies : nuclei; quasars : general ID ACTIVE GALACTIC NUCLEI; BROAD-LINE EMISSION; X-RAY-SPECTRA; LUMINOSITY; REGIONS; VISIBILITY; CATALOG; SAMPLE; TORUS AB We present Chandra ACIS- S observations of the enigmatic Seyfert 2 galaxy NGC 4698. This object, together with several other bona. de Seyfert 2 galaxies, shows no absorption in the low spatial resolution ASCA data, in contrast to the standard unification models. Our Chandra observations of NGC 4698 probe directly the nucleus, allowing us to check whether nearby sources contaminate the ASCA spectrum. Indeed, the Chandra observations show that the ASCA spectrum is dominated by two nearby AGNs. The X- ray flux of NGC 4698 is dominated by a nuclear source with luminosity L0.3-8 keV similar to 10(39) ergs s(-1), coincident with the radio nucleus. Its spectrum is well represented by a power law, Gamma approximate to 2.2, obscured by a small column density of 5 x 10(20) cm(-2), suggesting that NGC 4698 is an atypical Seyfert galaxy. On the basis of its low luminosity, we then interpret NGC 4698 as a Seyfert galaxy that lacks a broad- line region. C1 Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Georgantopoulos, I (reprint author), Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. RI Georgantopoulos, Ioannis/L-3687-2013; Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 36 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 SEP 10 PY 2003 VL 594 IS 2 BP 704 EP 708 DI 10.1086/377120 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600005 ER PT J AU Becker, W Swartz, DA Pavlov, GG Elsner, RF Grindlay, J Mignani, R Tennant, AF Backer, D Pulone, L Testa, V Weisskopf, MC AF Becker, W Swartz, DA Pavlov, GG Elsner, RF Grindlay, J Mignani, R Tennant, AF Backer, D Pulone, L Testa, V Weisskopf, MC TI Chandra X-ray observatory observations of the globular cluster M28 and its millisecond pulsar PSR B1821-24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters : individual (M28); pulsars : general; stars : neutron; X-rays : stars ID ACCRETING NEUTRON-STARS; CATACLYSMIC VARIABLES; EMISSION; NGC-6397; QUIESCENCE; DISCOVERY; GALAXY; CORE; ATMOSPHERES; PHOTOMETRY AB We report here the results of the first Chandra X- Ray Observatory observations of the globular cluster M28 ( NGC 6626). We detect 46 X- ray sources, of which 12 lie within 1 core radius of the center. We show that the apparently extended X- ray core emission seen with the ROSAT HRI is due to the superposition of multiple discrete sources, for which we determine the X- ray luminosity function down to a limit of about 6 x 1030 ergs s(-1). We measure the radial distribution of the X- ray sources and fit it to a King profile finding a core radius of r(c), x approximate to 1 1". We measure for the first time the unconfused phase- averaged X- ray spectrum of the 3.05 ms pulsar B1821 - 24 and find that it is best described by a power law with photon index Gamma similar or equal to 1.2. We find marginal evidence of an emission line centered at 3.3 keV in the pulsar spectrum, which could be interpreted as cyclotron emission from a corona above the pulsar's polar cap if the magnetic field is strongly different from a centered dipole. The unabsorbed pulsar flux in the 0.5 - 8.0 keV band is approximate to 3. 5 x 10(-13) ergs s(-1) cm(-2). We present spectral analyses of the five brightest unidentified sources. Based on the spectral parameters of the brightest of these sources, we suggest that it is a transiently accreting neutron star in a low- mass X- ray binary, in quiescence. Fitting its spectrum with a hydrogen neutron star atmosphere model yields the effective temperature T-eff(infinity) = 90(-10)(+30) eV and the radius R-NS(infinity) = 14.5(-3.8)(+6.9) km. In addition to the resolved sources, we detect fainter, unresolved X- ray emission from the central core. Using the Chandra- derived positions, we also report on the result of searching archival Hubble Space Telescope data for possible optical counterparts. C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. NASA, USRA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Penn State Univ, Davey Lab 525, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85740 Garching, Germany. Univ Calif Berkeley, Berkeley, CA 94720 USA. Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. RP Becker, W (reprint author), Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. OI Pulone, Luigi/0000-0002-5285-998X; Testa, Vincenzo/0000-0003-1033-1340 NR 52 TC 74 Z9 74 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2003 VL 594 IS 2 BP 798 EP 811 DI 10.1086/376967 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600011 ER PT J AU McClure-Griffiths, NM Dickey, JM Gaensler, BM Green, AJ AF McClure-Griffiths, NM Dickey, JM Gaensler, BM Green, AJ TI Loops, drips, and walls in the galactic chimney GSH 277+00+36 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : kinematics and dynamics; Galaxy : structure; ISM : bubbles; ISM : structure; radio lines : ISM ID SUPERNOVA-REMNANTS; GRAVITATIONAL INSTABILITIES; 3-DIMENSIONAL EVOLUTION; INTERSTELLAR-MEDIUM; MAGELLANIC-CLOUD; OB ASSOCIATIONS; DISK GALAXIES; MILKY-WAY; SCALE; SUPERBUBBLES AB We present new high- resolution H i images of the Galactic chimney GSH 277+ 00+ 36. The chimney is at a distance of similar to 6.5 kpc, is more than 600 pc in diameter, and extends at least 1 kpc above and below the Galactic midplane. Using the Australia Telescope Compact Array and the Parkes Radiotelescope as part of the Southern Galactic Plane Survey, we have imaged the H i associated with this chimney, with a spatial resolution of similar to 6 pc. These are among the highest spatial resolution images of an H i chimney. We find very narrow well-defined shell walls, a remarkably empty interior, and complex small- scale structures. The shell walls show a very steep reduction in emission at the interior edge and a more gradual decline toward the exterior. We suggest that this structure is characteristic of compression and may be used to distinguish stellar by- product shells from shell- like structures resulting from random turbulent motions. The shell and chimney walls also exhibit a great deal of small- scale structure, which we discuss in the context of hydrodynamic instabilities. We find that these structures are primarily cold gas with narrow line widths in the range 1.5 - 2.5 km s(-1). C1 CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP McClure-Griffiths, NM (reprint author), CSIRO, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. 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 41 TC 32 Z9 32 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 2003 VL 594 IS 2 BP 833 EP 843 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600013 ER PT J AU Frisch, PC Slavin, JD AF Frisch, PC Slavin, JD TI The chemical composition and gas-to-dust mass ratio of nearby interstellar matter SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : abundances ID LINE-OF-SIGHT; HUBBLE-SPACE-TELESCOPE; EPSILON-CANIS-MAJORIS; IN-SITU MEASUREMENTS; ZETA-OPHIUCHI; HELIOSPHERIC INTERFACE; ELEMENTAL ABUNDANCES; ULTRAVIOLET OBSERVATIONS; SOLAR NEIGHBORHOOD; PHASE ABUNDANCES AB We use recent results on interstellar gas toward nearby stars and interstellar by- products within the solar system to select among the equilibrium radiative transfer models of the nearest interstellar material presented in Slavin & Frisch. For the assumption that O/ H similar to 400 parts per million, models 2 and 8 are found to yield good fits to available data on interstellar material inside and outside of the heliosphere, with the exception of the Ne abundance in the pickup ion and anomalous cosmic- ray populations. For these models, the interstellar medium ( ISM) at the entry point to the heliosphere has n(H-0) = 0.202 - 0.208 cm(-3), n(He-0) = 0.0137-0.0152 cm(-3), and ionizations chi(H) = 0.29-0.30, chi(He) = 0.47-0.51. These best models suggest that the chemical composition of the nearby ISM is similar to 60% - 70% subsolar if S is undepleted. Both H-0 and H+ need to be included when evaluating abundances of ions found in warm diffuse clouds. Models 2 and 8 yield an H filtration factor of similar to 0.46. Gas- to- dust mass ratios for the ISM toward epsilon CMa are R-gd = 178 - 183 for solar abundances of Holweger or R-gd = 611-657 for an interstellar abundance standard 70% solar. Direct observations of dust grains in the solar system by Ulysses and Galileo yield R-gd similar or equal to 115 for models 2 and 8, supporting earlier results ( Frisch and coworkers). If the local ISM abundances are subsolar, then gas and dust are decoupled over small spatial scales. The inferred variation in R-gd over parsec length scales is consistent with the fact that the ISM near the Sun is part of a dynamically active cluster of cloudlets flowing away from the Sco- Cen association. Observations toward stars within similar to 500 pc show that R-gd correlates with the percentage of the dust mass that is carried by iron, suggesting that an Fe- rich grain core ( by mass) remains after grain destruction. Evidently large dust grains (> 10(-13) g) and small dust grains (< 10(-13) g) are not well mixed over parsec length spatial scales in the ISM. It also appears that very small C- dominated dust grains have been destroyed in the ISM within several parsecs of the Sun, since C appears to be essentially undepleted. However, if gas- dust coupling breaks down over the cloud lifetime, the missing mass arguments applied here to determine R-gd and dust grain mineralogy are not appropriate. C1 Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Chicago, Dept Astron & Astrophys, 5460 S Ellis Ave, Chicago, IL 60637 USA. OI Slavin, Jonathan/0000-0002-7597-6935 NR 66 TC 39 Z9 39 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2003 VL 594 IS 2 BP 844 EP 858 DI 10.1086/376689 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600014 ER PT J AU Szentgyorgyi, A Raymond, J Franco, J Villaver, E Lopez-Martin, L AF Szentgyorgyi, A Raymond, J Franco, J Villaver, E Lopez-Martin, L TI The high-excitation planetary nebula NGC 246: Optical and near-ultraviolet observations and two-dimensional numerical models SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; hydrodynamics; ISM : kinematics and dynamics planetary nebulae : individual (NGC 246) ID INTERMEDIATE-MASS STARS; ASYMPTOTIC GIANT BRANCH; X-RAY OBSERVATIONS; H-II REGIONS; MAGNETIC-FIELDS; INTERSTELLAR BUBBLES; DYNAMICAL EVOLUTION; ROSAT OBSERVATIONS; CIRCUMSTELLAR GAS; GALACTIC DISK AB We have imaged the planetary nebula ( PN) NGC 246 in the near- ultraviolet wavelengths [ Ne v] 342.6 nm, the Bowen fluorescence line of O iii at 344.4 nm, and a nearby line- free region centered on 338.6 nm, as well as Halpha, [ O iii] 500.7 nm, and [ S ii] 673.0 and 671.5 nm. Imaging in the 344.4 nm line is necessary to deconvolve contamination of the [ Ne v] images by O iii 342.9 nm. The emission from the shell and inner parts of the nebula is detected in [ Ne v]. The radial profiles of the [ Ne v] brightness decrease with radius from the exciting star, indicating that the bulk of the emission from this ion is due to the hard UV stellar radiation field, with a ( probably) marginal contribution from collisional ionization in a shock between the PN shell and the interstellar medium ( ISM). In contrast, the radial profiles of the emission in Halpha, [ O iii] 500.7 nm, and [ S ii] are flatter and peak at the location of the shell. The emission of [ S ii] probably traces the interaction of the PN with the ambient ISM. We also present two- dimensional numerical simulations for this PN- ISM interaction. The simulations consider the stellar motion with respect to the ambient ISM, with a velocity of 85 km s(-1), and include the time evolution of the wind parameters and UV radiation field from the progenitor star. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Space Telescope Sci Inst, Baltimore, MD 21218 USA. DEMIRM, Observ Paris, F-75014 Paris, France. RP Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM saint@cfa.harvard.edu; jraymond@cfa.harvard.edu; pepe@astroscu.unam.mx; villaver@stsci.edu; luislm@ll.iac.es RI Villaver, Eva/G-5710-2012 OI Villaver, Eva/0000-0003-4936-9418 NR 68 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2003 VL 594 IS 2 BP 874 EP 887 DI 10.1086/377123 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600017 ER PT J AU Perna, R Narayan, R Rybicki, G Stella, L Treves, A AF Perna, R Narayan, R Rybicki, G Stella, L Treves, A TI Bondi accretion and the problem of the missing isolated neutron stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; X-rays : ISM; X-rays : stars ID SAGITTARIUS-A-ASTERISK; MAGNETIC-FIELD DECAY; MASSIVE BLACK-HOLES; VELOCITY DISTRIBUTION; SPHERICAL ACCRETION; ELLIPTIC GALAXIES; 3 DIMENSIONS; FLOWS; MODEL; PULSARS AB A large number of neutron stars (NSs), similar to10(9), populate the Galaxy, but only a tiny fraction of them is observable during the short radio pulsar lifetime. The majority of these isolated NSs, too cold to be detectable by their own thermal emission, should be visible in X-rays as a result of accretion from the interstellar medium. The ROSAT All-Sky Survey has, however, shown that such accreting isolated NSs are very elusive: only a few tentative candidates have been identified, contrary to theoretical predictions that up to several thousand should be seen. We suggest that the fundamental reason for this discrepancy lies in the use of the standard Bondi formula to estimate the accretion rates. We compute the expected source counts using updated estimates of the pulsar velocity distribution, realistic hydrogen atmosphere spectra, and a modified expression for the Bondi accretion rate, as suggested by recent MHD simulations and supported by direct observations in the case of accretion around supermassive black holes in nearby galaxies and in our own. We find that, whereas the inclusion of atmospheric spectra partly compensates for the reduction in the counts due to the higher mean velocities of the new distribution, the modified Bondi formula dramatically suppresses the source counts. The new predictions are consistent with a null detection at the ROSAT sensitivity. C1 Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. Univ Insubria, Dipartimento Sci, I-22100 Como, Italy. RP Harvard Soc Fellows, 74 Mt Auburn St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 71 TC 54 Z9 54 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 2003 VL 594 IS 2 BP 936 EP 942 DI 10.1086/377091 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600022 ER PT J AU Wijnands, R Nowak, M Miller, JM Homan, J Wachter, S Lewin, WHG AF Wijnands, R Nowak, M Miller, JM Homan, J Wachter, S Lewin, WHG TI Chandra observation of the neutron star X-ray transient and eclipsing binary MXB 1659-29 in quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : eclipsing; stars : individual (MXB 1659-29); stars : neutron; X-rays : stars ID BURST SOURCE MXB-1659-29; BLACK-HOLE CANDIDATE; ANOMALOUS LOW-STATE; XMM-NEWTON; CENTAURUS X-4; SAX J1808.4-3658; MXB 1659-29; LUMINOSITY; DISCOVERY; EMISSION AB After almost 2.5 yr of actively accreting, the neutron star X-ray transient and eclipsing binary MXB 1659-29 returned to quiescence in 2001 September. We report on a Chandra observation of this source taken a little over a month after this transition. The source was detected at an unabsorbed 0.5-10 keV flux of only (2.7-3.6) x 10(-13) ergs cm(-2) s(-1), which implies a 0.5-10 keV X-ray luminosity of approximately (3.2-4.3) x 10(33) (d/10 kpc)(2) ergs s(-1), with d the distance to the source in kiloparsecs. Its spectrum had a thermal shape and could be well fitted by either a blackbody with a temperature kT of similar to0.3 keV or a neutron star atmosphere model with a kT of similar to0.1 keV. The luminosity and spectral shape of MXB 1659-29 are very similar to those observed of the other neutron star X-ray transients when they are in their quiescent state. The source was variable during our observation, exhibiting a complete eclipse of the inner part of the system by the companion star. Dipping behavior was observed before the eclipse, likely due to obscuration by an extended feature in the outer part of a residual accretion disk. We discuss our observation in the context of the cooling neutron star model proposed to explain the quiescent properties of neutron star X-ray transients. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. Osserv Astron Brera, I-23807 Merate, LC, Italy. Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. RP Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM rudy@space.mit.edu NR 62 TC 37 Z9 37 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 2003 VL 594 IS 2 BP 952 EP 960 DI 10.1086/377122 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600024 ER PT J AU Mukadam, AS Kepler, SO Winget, DE Nather, RE Kilic, M Mullally, F von Hippel, T Kleinman, SJ Nitta, A Guzik, JA Bradley, PA Matthews, J Sekiguchi, K Sullivan, DJ Sullivan, T Shobbrook, RR Birch, P Jiang, XJ Xu, DW Joshi, S Ashoka, BN Ibbetson, P Leibowitz, E Ofek, EO Meistas, EG Janulis, R Alisauskas, D Kalytis, R Handler, G Kilkenny, D O'Donoghue, D Kurtz, DW Muller, M Moskalik, P Ogloza, W Zola, S Krzesinski, J Johannessen, F Gonzales-Perez, JM Solheim, JE Silvotti, R Bernabei, S Vauclair, G Dolez, N Fu, JN Chevreton, M Manteiga, M Suarez, O Ulla, A Cunha, MS Metcalfe, TS Kanaan, A Fraga, L Costa, AFM Giovannini, O Fontaine, G Bergeron, P O'Brien, MS Sanwal, D Wood, MA Ahrens, TJ Silvestri, N Klumpe, EW Kawaler, SD Riddle, R Reed, MD Watson, TK AF Mukadam, AS Kepler, SO Winget, DE Nather, RE Kilic, M Mullally, F von Hippel, T Kleinman, SJ Nitta, A Guzik, JA Bradley, PA Matthews, J Sekiguchi, K Sullivan, DJ Sullivan, T Shobbrook, RR Birch, P Jiang, XJ Xu, DW Joshi, S Ashoka, BN Ibbetson, P Leibowitz, E Ofek, EO Meistas, EG Janulis, R Alisauskas, D Kalytis, R Handler, G Kilkenny, D O'Donoghue, D Kurtz, DW Muller, M Moskalik, P Ogloza, W Zola, S Krzesinski, J Johannessen, F Gonzales-Perez, JM Solheim, JE Silvotti, R Bernabei, S Vauclair, G Dolez, N Fu, JN Chevreton, M Manteiga, M Suarez, O Ulla, A Cunha, MS Metcalfe, TS Kanaan, A Fraga, L Costa, AFM Giovannini, O Fontaine, G Bergeron, P O'Brien, MS Sanwal, D Wood, MA Ahrens, TJ Silvestri, N Klumpe, EW Kawaler, SD Riddle, R Reed, MD Watson, TK TI Constraining the evolution of ZZ Ceti SO ASTROPHYSICAL JOURNAL LA English DT Article ID WHITE-DWARF STARS; WHOLE EARTH TELESCOPE; PERIOD CHANGE; STELLAR OSCILLATIONS; TIME-SCALE; MASS-LOSS; G117-B15A; ASTEROSEISMOLOGY; MODELS; STABILITY AB We report our analysis of the stability of pulsation periods in the DAV star (pulsating hydrogen atmosphere white dwarf) ZZ Ceti, also called R548. On the basis of observations that span 31 years, we conclude that the period 213.13 s observed in ZZ Ceti drifts at a rate dP/dt less than or equal to (5.5 +/- 1.9) x 10(-15) s s(-1), after correcting for proper motion. Our results are consistent with previous (P) over dot values for this mode and an improvement over them because of the larger time base. The characteristic stability timescale implied for the pulsation period is \P/(P) over dot\greater than or equal to 1.2 Gyr, comparable to the theoretical cooling timescale for the star. Our current stability limit for the period 213.13 s is only slightly less than the present measurement for another DAV, G117-B15A, for the period 215.2 s, establishing this mode in ZZ Ceti as the second most stable optical clock known, comparable to atomic clocks and more stable than most pulsars. Constraining the cooling rate of ZZ Ceti aids theoretical evolutionary models and white dwarf cosmochronology. The drift rate of this clock is small enough that we can set interesting limits on reflex motion due to planetary companions. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. McDonald Observ, Ft Davis, TX 79734 USA. Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. Apache Point Observ, Sunspot, NM 88349 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Perth Observ, Bickley, WA 6076, Australia. Beijing Astron Observ, Beijing 100012, Peoples R China. Natl Astron Observ, Joint Labs Opt Astron, Beijing 100012, Peoples R China. Uttar Pradesh State Observ, Naini Tal 263129, India. ISRO, Tech Phys Div, Satellite Ctr, Bangalore 560017, Karnataka, India. Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Inst Theoret Phys & Astron, LT-2600 Vilnius, Lithuania. Vilnius Univ Observ, LT-2009 Vilnius, Lithuania. S African Astron Observ, ZA-7935 Cape Town, South Africa. Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. Observ Midi Pyrenees, F-31400 Toulouse, France. Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. Polish Acad Sci, N Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Cracow Pedag Univ, Mt Suhora Observ, PL-30084 Krakow, Poland. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. Univ Tromso, Inst Fys, N-9037 Tromso, Norway. Osserv Astron Capodimonte, Inst Nazl Astrofis, I-80131 Naples, Italy. Osservatorio Astron Bologna, Inst Nazl Astrofis, I-40127 Bologna, Italy. Observ Paris, F-92195 Meudon, France. Univ A Coruna, Dept Ciencias Naut & Terra, Coruna, Spain. Univ Vigo, Dept Fis Aplicada, Vigo, Spain. Univ Porto, Ctr Astrofis, P-4150 Oporto, Portugal. Inst Super Maia, P-4475690 Avioso S Pedro, Portugal. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. Univ Caxias do Sul, Dept Quim & Fis, BR-95001970 Caxias Do Sul, RS, Brazil. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. Florida Inst Technol, SARA Observ, Melbourne, FL 32901 USA. Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37132 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. SW Missouri State Univ, Springfield, MO 65807 USA. Southwestern Univ, Informat Technol Serv, Georgetown, TX 78626 USA. RP Univ Texas, Dept Astron, 1 Univ Stn,C1400, Austin, TX 78712 USA. RI Kepler, S. O. /H-5901-2012; Fraga, Luciano/K-9075-2013; Ulla Miguel, Ana Maria/M-2860-2014; Manteiga, Minia/K-9773-2014; Metcalfe, Travis/A-9388-2008 OI Kepler, S. O. /0000-0002-7470-5703; Manteiga, Minia/0000-0002-7711-5581; Cunha, Margarida/0000-0001-8237-7343; Kawaler, Steven/0000-0002-6536-6367; Metcalfe, Travis/0000-0003-4034-0416 NR 55 TC 38 Z9 38 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2003 VL 594 IS 2 BP 961 EP 970 DI 10.1086/377044 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600025 ER PT J AU Ko, YK Raymond, JC Lin, J Lawrence, G Li, J Fludra, A AF Ko, YK Raymond, JC Lin, J Lawrence, G Li, J Fludra, A TI Dynamical and physical properties of a post-coronal mass ejection current sheet SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs) ID X-RAY TELESCOPE; SOLAR-FLARE; MAGNETIC RECONNECTION; ELEMENTAL ABUNDANCES; DENSITY STRUCTURE; ERUPTIVE FLARES; ATOMIC DATABASE; EMISSION-LINES; ACTIVE-REGION; FLUX ROPE AB In the eruptive process of the Kopp-Pneuman type, the closed magnetic field is stretched by the eruption so much that it is usually believed to be "open'' to infinity. Formation of the current sheet in such a configuration makes it possible for the energy in the coronal magnetic field to quickly convert into thermal and kinetic energies and cause significant observational consequences, such as growing postflare/CME loop system in the corona, separating bright. are ribbons in the chromosphere, and fast ejections of the plasma and the magnetic flux. An eruption on 2002 January 8 provides us a good opportunity to look into these observational signatures of and place constraints on the theories of eruptions. The event started with the expansion of a magnetic arcade over an active region, developed into a coronal mass ejection (CME), and left some thin streamer-like structures with successively growing loop systems beneath them. The plasma outflow and the highly ionized states of the plasma inside these streamer-like structures, as well as the growing loops beneath them, lead us to conclude that these structures are associated with a magnetic reconnection site, namely, the current sheet, of this eruptive process. We combine the data from the Ultraviolet Coronagraph Spectrometer, Large Angle and Spectrometric Coronagraph Experiment, EUV Imaging Telescope, and Coronal Diagnostic Spectrometer on board the Solar and Heliospheric Observatory, as well as from the Mauna Loa Solar Observatory Mark IV K-coronameter, to investigate the morphological and dynamical properties of this event, as well as the physical properties of the current sheet. The velocity and acceleration of the CME reached up to 1800 km s(-1) and 1 km s(-2), respectively. The acceleration is found to occur mainly at the lower corona (< 2.76 R.). The post-CME loop systems showed behaviors of both post. are loops (upward motion with decreasing speed) and soft X-ray giant arches (upward motion with constant speed, or acceleration) according to the definition of Svestka. In the current sheet, the presence of highly ionized ions, such as Fe+17 and Ca+13, suggests temperature as high as (3-4) x 10(6) K, and the plasma outflows have speeds ranging from 300 to 650 km s(-1). Absolute elemental abundances in the current sheet show a strong first ionization potential effect and have values similar to those found in the active region streamers. The magnetic field strength in the vicinity of the current sheet is found to be of the order of 1 G. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Catholic Univ Amer, Ctr Solar Phys & Space Weather, Washington, DC 20064 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Rutherford Appleton Lab, Didcot 0X11 0QX, Oxon, England. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI LIN, JUN/B-9890-2017 NR 91 TC 139 Z9 147 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2003 VL 594 IS 2 BP 1068 EP 1084 DI 10.1086/376982 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JL UT WOS:000185257600034 ER PT J AU Gaensler, BM Hendrick, SP Reynolds, SP Borkowski, KJ AF Gaensler, BM Hendrick, SP Reynolds, SP Borkowski, KJ TI Discovery of a new pulsar wind nebula in the Large Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (B0453-685); Magellanic Clouds; radio continuum : ISM; stars : neutron; supernova remnants; X-rays : ISM ID X-RAY PULSAR; SUPERNOVA-REMNANTS AB We present new high-resolution radio and X-ray observations of the supernova remnant (SNR) B0453 - 685 in the Large Magellanic Cloud, carried out with the Australia Telescope Compact Array and the Chandra X-Ray Observatory, respectively. Embedded in the SNR shell is a compact central nebula producing both flat-spectrum polarized radio emission and nonthermal X-rays; we identify this source as a pulsar wind nebula (PWN) powered by an unseen central neutron star. We present a new approach by which the properties of a SNR and PWN can be used to infer upper limits on the initial spin period and surface magnetic field of the unseen pulsar, and we conclude that this star was an initial rapid rotator with current properties similar to those of the Vela pulsar. As is the case for other similarly aged sources, there is currently an interaction taking place between the PWN and the SNR's reverse shock. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-6, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 18 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2003 VL 594 IS 2 BP L111 EP L114 DI 10.1086/378687 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JM UT WOS:000185257700012 ER PT J AU Ness, JU Starrfield, S Burwitz, V Wichmann, R Hauschildt, P Drake, JJ Wagner, RM Bond, HE Krautter, J Orio, M Hernanz, M Gehrz, RD Woodward, CE Butt, Y Mukai, K Balman, S Truran, JW AF Ness, JU Starrfield, S Burwitz, V Wichmann, R Hauschildt, P Drake, JJ Wagner, RM Bond, HE Krautter, J Orio, M Hernanz, M Gehrz, RD Woodward, CE Butt, Y Mukai, K Balman, S Truran, JW TI A Chandra low energy transmission grating spectrometer observation of V4743 Sagittarii: A supersoft X-ray source and a violently variable light curve SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars : individual (V4743 Sagittarii); stars : oscillations; white dwarfs; X-rays : binaries ID NOVAE; DISCOVERY; EMISSION; ROSAT AB V4743 Sagittarii ( Nova Sgr 2002 No. 3) was discovered on 2002 September 20. We obtained a 5 ks ACIS-S spectrum in 2002 November and found that the nova was faint in X-rays. We then obtained a 25 ks Chandra Low Energy Transmission Grating Spectrometer (LETGS) observation on 2003 March 19. By this time, it had evolved into the supersoft X-ray phase exhibiting a continuous spectrum with deep absorption features. The light curve from the observation showed large-amplitude oscillations with a period of 1325 s ( 22 minutes) followed by a decline in the total count rate after similar to13 ks of observations. The count rate dropped from similar to 40 counts s(-1) to practically zero within similar to 6 ks and stayed low for the rest of the observation (similar to 6 ks). The spectral hardness ratio changed from maxima to minima in correlation with the oscillations and then became significantly softer during the decay. Strong H-like and He-like lines of oxygen, nitrogen, and carbon were found in absorption during the bright phase, indicating temperatures between 1 and 2 MK, but they were shifted in wavelength corresponding to a Doppler velocity of - 2400 km s(-1). The spectrum obtained after the decline in count rate showed emission lines of C vi, N vi, and N VII, suggesting that we were seeing expanding gas ejected during the outburst, probably originating from CNO-cycled material. An XMM-Newton Target of Opportunity observation, obtained on 2002 April 4 and a later LETGS observation from 2003 July 18 also showed oscillations, but with smaller amplitudes. C1 Hamburger Sternwarte, D-21029 Hamburg, Germany. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Large Binocular Telescope Observ, Tucson, AZ 85721 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Heidelberg Konigstuhl Landessternwarte, D-69117 Heidelberg, Germany. INAF Turin Observ, I-10025 Pino Torinese, Italy. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. CSIC, Inst Ciencias Espacio, E-08034 Barcelona, Spain. Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Ness, JU (reprint author), Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. RI Hernanz, Margarita/K-1770-2014 OI Hernanz, Margarita/0000-0002-8651-7910 NR 16 TC 75 Z9 75 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 2003 VL 594 IS 2 BP L127 EP L130 DI 10.1086/378664 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JM UT WOS:000185257700016 ER PT J AU Yuan, F AF Yuan, F TI Luminous hot accretion flows: Thermal equilibrium curve and thermal stability SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; galaxies : nuclei; hydrodynamics ID ADVECTION-DOMINATED ACCRETION; BLACK-HOLES; DISKS; CLUSTERS; INSTABILITY; GALAXIES; CONDUCTION; CLOUDS; DISCS AB In a previous paper, we presented the global solution of a new accretion flow model, namely, luminous hot accretion flows (LHAFs). In this Letter, we first show the corresponding thermal equilibrium curve of LHAFs in the mass accretion rate versus surface density diagram. Then we examine its thermal stability against local perturbations. We find that LHAFs are thermally unstable when thermal conduction is neglected. However, when the accretion rate is not very large, the timescale of the growth of perturbations is longer than the accretion timescale; therefore, the instability has no dynamical effect on the accretion flow. When the accretion rate is large, the perturbations can grow very fast at a certain radius. As a result, some cold clumps may form and the accretion flow will become multiphase. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yuan, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 30 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 SEP 10 PY 2003 VL 594 IS 2 BP L99 EP L102 DI 10.1086/378666 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 720JM UT WOS:000185257700009 ER PT J AU Vari, RP Lima, RCT AF Vari, RP Lima, RCT TI New species of Creagrutus (Teleostei : Characiformes : Characidae) from the Rio Uaupes basin, Brazil SO COPEIA LA English DT Article AB A new species of Creagrutus is described from the western portions of the Rio Uaupes basin near the Brazilian-Colombian border region. The species is most closely related to, and most similar externally to, Creagrutus amoenus and Creagrutus kunturus, but differs from those species in details of pigmentation, meristics, and morphometrics. C1 Smithsonian Inst, Natl Museum Amer Hist, Sect Vertebrate Zool Fishes, Washington, DC 20560 USA. Univ Sao Paulo, Museu Zool, BR-94299970 Sao Paulo, Brazil. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Sect Vertebrate Zool Fishes, Washington, DC 20560 USA. RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 NR 4 TC 6 Z9 8 U1 0 U2 1 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 SEP 5 PY 2003 IS 3 BP 583 EP 587 PG 5 WC Zoology SC Zoology GA 721AE UT WOS:000185294200013 ER PT J AU Abbot, DS Palmer, PI Martin, RV Chance, KV Jacob, DJ Guenther, A AF Abbot, DS Palmer, PI Martin, RV Chance, KV Jacob, DJ Guenther, A TI Seasonal and interannual variability of North American isoprene emissions as determined by formaldehyde column measurements from space SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OZONE MONITORING EXPERIMENT; CHEMISTRY; GOME; MODEL AB [1] Formaldehyde ( HCHO) columns measured from space by solar UV backscatter allow mapping of reactive hydrocarbon emissions. The principal contributor to these emissions during the growing season is the biogenic hydrocarbon isoprene, which is of great importance for driving regional and global tropospheric chemistry. We present seven years (1995-2001) of HCHO column data for North America from the Global Ozone Monitoring Experiment (GOME), and show that the general seasonal and interannual variability of these data is consistent with knowledge of isoprene emission. There are some significant regional discrepancies with the seasonal patterns predicted from current isoprene emission models, and we suggest that these may reflect flaws in the models. The interannual variability of HCHO columns observed by GOME appears to follow the interannual variability of surface temperature, as expected from current isoprene emission models. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. RP Abbot, DS (reprint author), Harvard Univ, Div Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. RI Martin, Randall/A-2051-2008; Palmer, Paul/F-7008-2010; Abbot, Dorian/J-6352-2012; Martin, Randall/C-1205-2014; Guenther, Alex/B-1617-2008 OI Martin, Randall/0000-0003-2632-8402; Guenther, Alex/0000-0001-6283-8288 NR 22 TC 67 Z9 68 U1 2 U2 13 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 SEP 5 PY 2003 VL 30 IS 17 AR 1886 DI 10.1029/2003GL017336 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 722DX UT WOS:000185361100001 ER PT J AU Martin, RV Jacob, DJ Chance, K Kurosu, TP Palmer, PI Evans, MJ AF Martin, RV Jacob, DJ Chance, K Kurosu, TP Palmer, PI Evans, MJ TI Global inventory of nitrogen oxide emissions constrained by space-based observations of NO2 columns SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE emissions; GOME; nitrogen oxides; biomass burning; retrieval; remote sensing ID OZONE MONITORING EXPERIMENT; TROPOSPHERIC OZONE; REACTIVE NITROGEN; GOME MEASUREMENTS; MODEL DESCRIPTION; GOCART MODEL; SATELLITE; CHEMISTRY; AEROSOLS; SULFUR AB [1] We use tropospheric NO2 columns from the Global Ozone Monitoring Experiment (GOME) satellite instrument to derive top-down constraints on emissions of nitrogen oxides (NOx = NO + NO2), and combine these with a priori information from a bottom-up emission inventory ( with error weighting) to achieve an optimized a posteriori estimate of the global distribution of surface NOx emissions. Our GOME NO2 retrieval improves on previous work by accounting for scattering and absorption of radiation by aerosols; the effect on the air mass factor (AMF) ranges from + 10 to -40% depending on the region. Our AMF also includes local information on relative vertical profiles (shape factors) of NO2 from a global 3-D chemical transport model (GEOS-CHEM); assumption of a globally uniform shape factor, as in most previous retrievals, would introduce regional biases of up to 40% over industrial regions and a factor of 2 over remote regions. We derive a top-down NOx emission inventory from the GOME data by using the local GEOS-CHEM relationship between NO2 columns and NOx emissions. The resulting NOx emissions for industrial regions are aseasonal,despite large seasonal variation in NO2 columns, providing confidence in the method. Top-down errors in monthly NOx emissions are comparable with bottom-up errors over source regions. Annual global a posteriori errors are half of a priori errors. Our global a posteriori estimate for annual land surface NOx emissions (37.7 Tg N yr(-1)) agrees closely with the GEIA-based a priori (36.4) and with the EDGAR 3.0 bottom-up inventory (36.6), but there are significant regional differences. A posteriori NOx emissions are higher by 50-100% in the Po Valley, Tehran, and Riyadh urban areas, and by 25-35% in Japan and South Africa. Biomass burning emissions from India, central Africa, and Brazil are lower by up to 50%; soil NOx emissions are appreciably higher in the western United States, the Sahel, and southern Europe. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM rvmartin@fizz.phys.dal.ca; djj@io.harvard.edu; kchance@cfa.harvard.edu; tkurosu@cfa.harvard.edu; pip@io.harvard.edu; mje@io.harvard.edu RI Martin, Randall/A-2051-2008; Palmer, Paul/F-7008-2010; Evans, Mathew/A-3886-2012; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Evans, Mathew/0000-0003-4775-032X; Martin, Randall/0000-0003-2632-8402; NR 61 TC 225 Z9 231 U1 3 U2 61 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 5 PY 2003 VL 108 IS D17 AR 4537 DI 10.1029/2003JD003453 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 722EC UT WOS:000185361600003 ER PT J AU McCarthy, MC AF McCarthy, MC TI Silicon carbides, silicon clusters, and exotic silicon hydrides. SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 226th National Meeting of the American-Chemical-Society CY SEP 07-11, 2003 CL NEW YORK, NY SP Amer Chem Soc C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP PY 2003 VL 226 MA 371-INOR BP U730 EP U730 PN 1 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 751JF UT WOS:000187062403481 ER PT J AU Ekanayake, DK Horadagoda, NU Sanjeevani, GKM Arulkanthan, A Gunatilake, KAS Dittus, WPJ AF Ekanayake, DK Horadagoda, NU Sanjeevani, GKM Arulkanthan, A Gunatilake, KAS Dittus, WPJ TI Hematology of a natural population of toque macaques (Macaca sinica) at Polonnaruwa, Sri Lanka SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE toque macaque; Macaca sinica; hematology; wild population; erythrocyte sedimentation rate; Sri Lanka ID SERUM BIOCHEMICAL VALUES; MONKEY MACACA; SEX; FASCICULARIS; COMPETITION; PARAMETERS; MALARIA; RADIATA; MULATTA; GROWTH AB Hematological studies were conducted in three wild groups of toque macaques (Macaca sinica) inhabiting the Polonnaruwa Sanctuary in northeastern Sri Lanka. The macaques were temporarily trapped and anesthetized, and femoral blood was drawn from 35 males and 37 females (age range: 0.33-24.5 yr). Statistically significant (P<0.05) differences were observed by sex for total plasma proteins (PP), and by age for red blood cell (RBC) counts, hemoglobin (Hb), mean corpuscular volume (MCV), mean corpuscular Hb (MCH), mean corpuscular Hb concentration (MCHC), PP, erythrocyte sedimentation rate (ESR), differential and absolute neutrophil counts, differential lymphocyte counts, and absolute eosinophil counts. In general, the results were similar to those reported for other species of colony-bred and free-ranging macaques. However, there also were differences. First, in contrast to earlier studies of nonhuman primates, we examined the hematology of infants. Compared to other age classes, infants (< 1 yr old) had lower RBC, Hb, MCHC, and ESR values, and a higher MCV. These findings were similar to those obtained in human infants. Second, we observed variations in hematology among social groups in relation to their ecology. Two groups (IH3 and M3) had ready access to water throughout the dry season (the period of sampling), whereas the third group (J) did not. The Hb, RBC, and PP values obtained in groups IH3 and M3 were similar to those reported in other macaque species. However, these parameters in group J were significantly (P < 0.01) higher, which suggests that this group (representing about 26% of the sample) had been dehydrated during the dry season. Finally, two indices indicative of injury and infection-the ESR and leukocyte counts-were higher in the wild toque macaques than has been reported for other species of macaques held in captivity, and about 15% of the toque macaques sampled had extreme outlier values for these parameters; however, none were visibly ill or died. These results suggest that wild toque macaques are subject to a wide array of physical and biological insults that are unique to natural populations. (C) 2003 Wiley-Liss, Inc. C1 Smithsonian Inst, Primate Project, Kandy, CP, Sri Lanka. Univ Peradeniya, Fac Vet Med & Anim Sci, Dept Vet Pathobiol, Peradeniya, Sri Lanka. Inst Fundamental Studies, Kandy, Sri Lanka. Smithsonian Inst, Natl Zool Pk, Dept Conversat Biol, Washington, DC 20008 USA. RP Dittus, WPJ (reprint author), Smithsonian Inst, Primate Project, 140-12 Mapanawathura Rd, Kandy, CP, Sri Lanka. NR 34 TC 7 Z9 7 U1 0 U2 5 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 2003 VL 61 IS 1 BP 13 EP 28 DI 10.1002/ajp.10105 PG 16 WC Zoology SC Zoology GA 729DX UT WOS:000185758000003 PM 12966516 ER PT J AU Grupe, D Mathur, S Elvis, M AF Grupe, D Mathur, S Elvis, M TI XMM-Newton observations of two broad absorption line QSOs: Q1246-057 and SBS 1542+541 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : active; quasars : general; quasars : individual (Q1246-057, SBS 1542+541) ID ACTIVE GALACTIC NUCLEI; SPECTRUM ROSAT SOURCES; QUASI-STELLAR OBJECTS; X-RAY SPECTROSCOPY; EMISSION-LINE; ULTRAVIOLET-SPECTRA; CHANDRA DETECTS; NGC 5548; GALAXIES; APM-08279+5255 AB We report on the results of XMM-Newton observations of two broad absorption line quasars (BAL QSOs), Q1246 - 057 and SBS 1542+ 541. The unprecedented sensitivity of XMM-Newton allows spectral analysis of these X-ray-weak sources. The X-ray spectral data of these sources can be fitted by a power law with alpha(X) = 1.0 - 1.2 and either a partially covering absorber or an ionized absorber model. Rest-frame UV spectroscopy together with polarimetry favors the model with a partially covering absorber with column density a few times 10(22) cm(-2) and a covering fraction of about 0.80. After correcting for absorption, the X-ray loudness of these BAL QSOs appears to be similar to other, unabsorbed quasars. The mystery of X-ray weakness of BAL QSOs appears to be all but solved, with strong absorption being the primary reason. With the available X-ray data, however, the issue of whether BAL QSOs represent highly accreting/younger population of quasars remains unsettled. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM dgrupe@astronomy.ohio-state.edu; smita@astronomy.ohio-state.edu NR 57 TC 33 Z9 33 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 SEP PY 2003 VL 126 IS 3 BP 1159 EP 1166 DI 10.1086/377141 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 718EJ UT WOS:000185131900003 ER PT J AU Sawicki, M Mallen-Ornelas, G AF Sawicki, M Mallen-Ornelas, G TI Redshifts in the Hubble Deep Field South SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; cosmology : observations; galaxies : distances and redshifts; galaxies : photometry ID PHOTOMETRIC REDSHIFTS; SPECTROSCOPY; GALAXIES AB We present a catalog of 97 spectroscopic redshifts of z < 1 galaxies in the Hubble Deep Field South (HDF-S) and its flanking fields (FFs). In the HDF-S proper we observed approximately half the galaxies brighter than I-814(AB) = 24 and obtained redshifts for 76% of them. Targets in our HDF-S sample were pre-selected to be at z < 1 based on photometric redshifts, while in the FFs a simple magnitude cut was used. The photometric redshift preselection in the HDF-S resulted in a spectroscopic success rate that is significantly higher than in the FFs, where no preselection was applied. The rms precision of our redshift measurements, determined from repeat observations, is deltaz = 0.0003. We present the photometry and redshifts for the 97 objects for which we secured spectroscopic redshifts and describe the basic properties of this sample. C1 Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Pontificia Univ Catolica Chile, Santiago 22, Chile. RP Sawicki, M (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. NR 12 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 SEP PY 2003 VL 126 IS 3 BP 1208 EP 1216 DI 10.1086/377317 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 718EJ UT WOS:000185131900006 ER PT J AU Williams, BF AF Williams, BF TI The recent star formation history of the M31 disk SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : individual (M31); galaxies : stellar content ID HUBBLE-SPACE-TELESCOPE; SPIRAL ARM; WFPC2 PHOTOMETRY; NEARBY GALAXIES; DIRECT PROJECT; H-ALPHA; DISTANCE; M-31; ASSOCIATIONS; CEPHEIDS AB The star formation history of the northern and southern M31 disk is measured using samples of BV photometry for 4' x 4' regions taken from the KPNO/CTIO Local Group Survey. The distances, mean reddening values, and age distributions of the stars in these regions were measured using the routines of Dolphin. Independent measurements of overlapping fields show that the results are stable for most samples. A slight distance gradient is seen across the major axis of the southern disk, and a mean distance of 24.47 +/- 0.03 is found by combining the results. Higher mean reddening values are seen to follow the spiral structure. The stellar age distributions are consistent with episodic star formation confined mainly to the gas-rich arm regions. If these episodes were caused by propagating density waves, the waves did not cause significant star formation episodes in the gas-poor interarm regions. A combination of all of the results provides the total star formation rate for 1.4 deg(2) of the M31 disk for six epochs. These results suggest that star formation in the disk declined by similar to50% from similar to250 to similar to50 Myr ago. The lowest star formation rate occurred similar to25 Myr ago, followed by a similar to20% increase to the present. The mean star formation rate for this large portion of M31 over the past 60 Myr is 0.63 +/- 0.07 M-. yr(-1), suggesting a total mean rate for the disk of similar to1 M-. yr(-1). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, MS 67,60 Garden St, Cambridge, MA 02138 USA. NR 34 TC 43 Z9 44 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 2003 VL 126 IS 3 BP 1312 EP 1325 DI 10.1086/377347 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 718EJ UT WOS:000185131900015 ER PT J AU Brown, WR Prieto, CA Beers, TC Wilhelm, R Geller, MJ Kenyon, SJ Kurtz, MJ AF Brown, WR Prieto, CA Beers, TC Wilhelm, R Geller, MJ Kenyon, SJ Kurtz, MJ TI The Century Survey Galactic Halo Project. I. Stellar spectral analysis SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy : halo; Galaxy : stellar content; stars : abundances; stars : horizontal-branch ID HORIZONTAL-BRANCH STARS; RR LYRAE STARS; DIGITAL SKY SURVEY; METAL-POOR STARS; A-TYPE STARS; SURVEY COMMISSIONING DATA; MILKY-WAY; DWARF STARS; GLOBULAR-CLUSTERS; RADIAL-VELOCITY AB The Century Survey Galactic Halo Project is a photometric and spectroscopic survey from which we select relatively blue stars ( V - R < 0.30 mag) as probes of the MilkyWay halo. The survey strip spans the range of Galactic latitude 35&DEG; < b < 88&DEG;, allowing us to study the nature of populations of stars and their systematic motions as a function of Galactic latitude. One of our primary goals is to use blue horizontal-branch stars to trace potential star streams in the halo, and to test the hierarchical model for the formation of the Galaxy. In this paper we discuss spectroscopy and multipassband photometry for a sample of 764 blue stars in the Century Survey region. Our sample consists predominantly of A- and F-type stars. We describe our techniques for determination of radial velocities, effective temperatures, metallicities, and surface gravities. Based on these measurements, we derive distance estimates by comparison with a set of calibrated isochrones. We devote special attention to the classification of blue horizontal-branch stars, and compare the results obtained from the application of the techniques of Kinman et al., Wilhelm et al., and Clewley et al. We identify 55 blue horizontal-branch stars. Our large sample of stars also uncovers a number of unusual objects, including three carbon-enhanced stars, a late B-type star located 0.8 kpc above the Galactic plane, and a DZ white dwarf. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Brown, WR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI KURTZ, Michael /B-3890-2009; OI Kenyon, Scott/0000-0003-0214-609X; Kurtz, Michael/0000-0002-6949-0090 NR 83 TC 22 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 SEP PY 2003 VL 126 IS 3 BP 1362 EP 1380 DI 10.1086/377143 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 718EJ UT WOS:000185131900018 ER PT J AU Branch, D Garnavich, P Matheson, T Baron, E Thomas, RC Hatano, K Challis, P Jha, S Kirshner, RP AF Branch, D Garnavich, P Matheson, T Baron, E Thomas, RC Hatano, K Challis, P Jha, S Kirshner, RP TI Optical spectra of the type Ia supernova 1998aq SO ASTRONOMICAL JOURNAL LA English DT Article DE supernovae : general; supernovae : individual (SN 1998aq) ID 1994D; SN-1998AQ; NGC-3982; CARBON; MODELS AB We present 29 optical spectra of the normal Type Ia SN 1998aq, ranging from 9 days before to 241 days after the time of maximum brightness. This spectrocopic data set, together with photometric data presented elsewhere, makes SN 1998aq one of the best observed Type Ia supernovae at optical wavelengths. We use the parameterized supernova synthetic-spectrum code SYNOW to study line identifications in the early photospheric-phase spectra. The results include evidence for lines of singly ionized carbon, at ejection velocities as low as 11,000 km s(-1). Implications for SN Ia explosion models are discussed. C1 Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Univ Notre Dame, Dept Phys & Astron, Notre Dame, IN 46556 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Dept Astron, Sch Sci, Tokyo 113, Japan. RP Branch, D (reprint author), Univ Oklahoma, Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. RI Baron, Edward/A-9041-2009 OI Baron, Edward/0000-0001-5393-1608 NR 34 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 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2003 VL 126 IS 3 BP 1489 EP 1498 DI 10.1086/377016 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 718EJ UT WOS:000185131900027 ER PT J AU Lang, CC Cyganowski, C Goss, WM Zhao, JH AF Lang, Cornelia C. Cyganowski, Claudia Goss, W. M. Zhao, Jun-Hui TI High-resolution HI Absorption Observations towards the Central 200 pc of the Galaxy SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE interstellar medium; Galactic Center AB We report the first results of an HI absorption survey of the central 200 pc of the Galaxy. These Very Large Array (VLA) data have a resolution of similar to 15 '' (0.6 pc at the Galactic Center (GC) distance) and a velocity resolution of similar to 2.5 km s(-1). This study provides HI data with high spatial resolution, comparable with the many high resolution observations which have been made of GC sources over the past ten years. Information on the velocities, relative distances of sources and HI column densities will be studied. Such data serves to clarify the nature of physical associations between the unique radio continuum features in this region and the atomic and molecular components. In particular, we are interested in the arrangement of sources in the active Radio Arc region: the atomic, ionized and molecular gas and their relation to the massive stellar clusters and magnetic filaments. C1 [Lang, Cornelia C.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Cyganowski, Claudia; Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lang, CC (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM cornelia-lang@uiowa.edu NR 15 TC 2 Z9 2 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD SEP PY 2003 VL 324 SU 1 BP 1 EP 7 DI 10.1002/asna.200385065 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V23UK UT WOS:000208367500001 ER PT J AU Martin, CL Walsh, WM Xiao, KC Lane, AP Walker, CK Stark, AA AF Martin, Christopher L. Walsh, Wilfred M. Xiao, Kecheng Lane, Adair P. Walker, Christopher K. Stark, Antony A. TI The Inner 200pc: Hot Dense Gas SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE Galaxy:center; Galaxy:kinematics and dynamics; ISM:atoms; ISM:general; ISM:molecules AB We present fully-sampled maps of 461 GHz CO J - 4 -> 3, 807 GHz CO J - 7 -> 6, and 492 GHz [CI] P-3(1) -> P-3(0) emission from the inner 3 degrees of the Galactic Center region taken with the Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) in 2001-2002. The data cover -1 degrees.3 < l < 2 degrees, -0 degrees.3 < b < 0 degrees.2 with 0.5' spacing, resulting in spectra in 3 transitions at over 24,000 positions on the sky. The CO J = 4 -> 3 emission is found to be essentially coextensive with lower-J transitions of CO. The CO J = 7 -> 6 emission is spatially confined to a far smaller region than the lower-J CO lines. The [C I] P-3(1) -> P-3(0) emission has a spatial extent similar to the low-J CO emission, but is more diffuse. Bright CO J = 7 -> 6 emission is detected in the well-known Galactic Center clouds Sgr A and Sgr B. Analyzing our CO J = 7 -> 6 and CO J = 4 -> 3 data in conjunction with J = 1 -> 0 (CO)-C-12 and (CO)-C-13 data previously observed with the Bell Laboratories 7-m antenna, we apply a Large Velocity Gradient (LVG) model to estimate the kinetic temperature and density of molecular gas in the inner 200 pc of the Galactic Center region. Typical pressures in the Galactic Center gas are n(H-2) center dot T-kin similar to 10(5.2) K cm(-3). We present an (l, b) map of molecular hydrogen column density derived from our LVG results. C1 [Martin, Christopher L.; Walsh, Wilfred M.; Xiao, Kecheng; Lane, Adair P.; Stark, Antony A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walker, Christopher K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Martin, CL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-12, Cambridge, MA 02138 USA. EM cmartin@cfa.harvard.edu NR 40 TC 1 Z9 1 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD SEP PY 2003 VL 324 SU 1 BP 93 EP 99 DI 10.1002/asna.200385109 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V23UK UT WOS:000208367500014 ER PT J AU Lee, S Pak, S Davis, CJ Herrnstein, RM Geballe, TR Ho, PTP Wheeler, JC AF Lee, Sungho Pak, Soojong Davis, Christopher J. Herrnstein, Robeson M. Geballe, T. R. Ho, Paul T. P. Wheeler, J. Craig TI Interaction between the Northeastern Boundary of Sgr A East and Giant Molecular Clouds: Excitation Mechanisms of the H-2 Emission SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE Galaxy: centre; ISM: individual(Sgr A East), molecules; infrared: ISM: lines and bands AB We have detected the v = 1 -> 0 S(1) (lambda = 2.1218 mu m) and v = 2 -> 1 S(1) (lambda = 2.2477 mu m) lines of H-2 in a region between the northeastern boundary of Sgr A East and the giant molecular cloud (GMC) M-0.02-0.07, in the Galactic centre. The broad line widths, the low peak velocities relative to the molecular clouds, and the moderate H-2 v = 2 -> 1 S(1) to v = 1 -> 0 S(1) line ratios can be best explained by a combination of C-type shocks and fluorescence. The detection of shocked H-2 in this region is clear evidence that Sgr A East is driving material into both the GMC M-0.02-0.07 and the northern ridge found by McGary, Coil, & Ho (2001). C1 [Lee, Sungho] Seoul Natl Univ, Astron Program SEES, Seoul 151742, South Korea. [Lee, Sungho; Pak, Soojong] Korea Astron Observ, Taejon 305348, South Korea. [Davis, Christopher J.] Joint Astron Ctr, Hilo, HI 96720 USA. [Herrnstein, Robeson M.; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Geballe, T. R.] Gemini Observ, Hilo, HI 96720 USA. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Lee, S (reprint author), Seoul Natl Univ, Astron Program SEES, Seoul 151742, South Korea. EM leesh@astro.snu.ac.kr NR 31 TC 0 Z9 0 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD SEP PY 2003 VL 324 SU 1 BP 189 EP 195 DI 10.1002/asna.200385068 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V23UK UT WOS:000208367500028 ER PT J AU Zhao, JH AF Zhao, Jun-Hui TI Intrinsic Radio Variability of Sgr A* SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE Black hole; radio continuum; accretion disk AB We review and summarize the results on the variability of Sgr A* based on the recent monitoring programs with the SMA at 1.3 and 0.87 mm, and the VLA at 2, 1.3 and 0.7 cm. We discuss the flares at 1.3 mm and a cross-correlation of the SMA flux density at 1.3 mm with the VLA data at 1.3 cm. We also present a preliminary result on the double quasi-periodic oscillation (DQPO) in flux density of Sgr A* based on our analysis of radio light curves observed with the VLA at 1.3 cm. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM jzhao@cfa.harvard.edu NR 19 TC 4 Z9 4 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD SEP PY 2003 VL 324 SU 1 BP 355 EP 361 DI 10.1002/asna.200385096 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V23UK UT WOS:000208367500054 ER PT J AU Yuan, F Markoff, S Falcke, H AF Yuan, F. Markoff, S. Falcke, H. TI A Jet-ADAF Model for Sgr A* SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: nuclei; Galaxy: center; hydrodynamics AB We briefly review the observations and theoretical models for Sgr A*, the supermassive black hole in the center of our Galaxy, emphasizing the coupled jet plus accretion disk model for this source. In this model, the accretion flow is described as an ADAF fed by hot plasma in the Galactic Center region. At the innermost region of the accretion flow, a small fraction of the accretion flow is ejected out and forms a jet. Because the accretion flow is supersonic at the innermost region, during this process a standing shock occurs. As a result, the electron temperature increases to similar to 2 x 10(11) K, which is about 10 times higher than the highest temperature attained in the ADAF, therefore leading to strong radiation via synchrotron and the Compton scattering processes. The emergent spectrum of Sgr A* is the sum of the emission from jet and underlying ADAF. Specifically, the submm-bump is produced by the base of the jet, while the radio spectrum is due to the outer part of the jet. The X-ray flux in the quiescent state is the sum of the bremsstrahlung emission from the underlying accretion flow and SSC from the jet. We also briefly discuss the application of our model to another low-luminosity AGN, NGC4258. C1 [Yuan, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Markoff, S.] MIT, Ctr Space Res, Cambridge, MA 02139 USA. [Falcke, H.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Yuan, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM fyuan@cfa.harvard.edu RI Falcke, Heino/H-5262-2012 OI Falcke, Heino/0000-0002-2526-6724 NR 24 TC 1 Z9 1 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD SEP PY 2003 VL 324 SU 1 BP 453 EP 458 DI 10.1002/asna.200385044 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V23UK UT WOS:000208367500069 ER PT J AU Reid, MJ Menten, KM Genzel, R Ott, T Schodel, R Brunthaler, A AF Reid, Mark J. Menten, Karl M. Genzel, Reinhard Ott, Thomas Schoedel, Rainer Brunthaler, Andreas TI The Position, Motion, and Mass of Sgr A* SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE Sgr A*; black holes; proper motions; SiO masers AB We report progress on measuring the position of Sgr A* on infrared images, placing limits on the motion of the central star cluster relative to Sgr A*, and measuring the proper motion of Sgr A* itself. The position of Sgr A* has been determined to within 10 mas on infrared images. To this accuracy, the gravitational source (sensed by stellar orbits) and the radiative source (Sgr A*) are coincident. Proper motions of four stars measured both in the infrared and radio indicate that the central star cluster moves with Sgr A* to within 70 km s(-1). Finally, combining stellar orbital information with an upper limit of 8 km s(-1) for the intrinsic proper motion of Sgr A* (perpendicular to the Galactic plane), we place a lower limit on the mass of Sgr A* of 4 x 10(5) M-circle dot. C1 [Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, Karl M.; Brunthaler, Andreas] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Genzel, Reinhard; Ott, Thomas; Schoedel, Rainer] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mreid@cfa.harvard.edu RI Schoedel, Rainer/D-4751-2014 OI Schoedel, Rainer/0000-0001-5404-797X NR 11 TC 12 Z9 12 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD SEP PY 2003 VL 324 SU 1 BP 505 EP 511 DI 10.1002/asna.200385084 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V23UK UT WOS:000208367500076 ER PT J AU Ohnaka, K Beckmann, U Berger, JP Brewer, MK Hofmann, KH Lacasse, MG Malanushenko, V Millan-Gabet, R Monnier, JD Pedretti, E Schertl, D Schloerb, FP Shenavrin, VI Traub, WA Weigelt, G Yudin, BF AF Ohnaka, K Beckmann, U Berger, JP Brewer, MK Hofmann, KH Lacasse, MG Malanushenko, V Millan-Gabet, R Monnier, JD Pedretti, E Schertl, D Schloerb, FP Shenavrin, VI Traub, WA Weigelt, G Yudin, BF TI JHK '-band IOTA interferometry of the circumstellar environment of R CrB SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric; stars : circumstellar matter; stars : mass-loss; stars : individual : R CrB; stars :; variable : general; infrared : stars ID CORONAE-BOREALIS STARS; AMORPHOUS-CARBON GRAINS; PHOTOMETRY; ENVELOPE; MINIMUM AB We report the first long-baseline interferometry of the circumstellar dust environment of R CrB. The observations were carried out with the Infrared Optical Telescope Array (IOTA), using our new JHK' beam combiner which enables us to record fringes in the J, H, and K' bands simultaneously. The circumstellar dust envelope of R CrB is resolved at a baseline of 21 m along a position angle of similar to170degrees, and the visibilities in the J, H, and K' bands are 0.97 +/- 0.06, 0.78 +/- 0.06, and 0.61 +/- 0.03, respectively. These observed visibilities, together with the K'-band visibility obtained by speckle interferometry with baselines of up to 6 m, and the spectral energy distribution are compared with predictions from spherical dust shell models which consist of the central star and an optically thin dust shell. The comparison reveals that the observed J- and H-band visibilities are in agreement with those predicted by these models, and the inner radius and inner boundary temperature of the dust shell were derived to be 60-80 R-* and 950-1050 K, respectively. However, the predicted K'-band visibilities are found to be similar to10% smaller than the one obtained with IOTA. Given the simplifications adopted in our models and the complex nature of the object, this can nevertheless be regarded as rough agreement. As a hypothesis to explain this small discrepancy, we propose that there might be a group of newly formed dust clouds, which may appear as a third visibility component. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. Univ Massachusetts, Dept Phys & Astron, Amherst, MA 01003 USA. Crimean Astrophys Observ, UA-98409 Crimea, Ukraine. CALTECH, Pasadena, CA 91125 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119899, Russia. RP Ohnaka, K (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kohnaka@mpifr-bonn.mpg.de OI Monnier, John D/0000-0002-3380-3307 NR 20 TC 7 Z9 7 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2003 VL 408 IS 2 BP 553 EP 558 DI 10.1051/0004-6361:20031002 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716AM UT WOS:000185006700014 ER PT J AU Beuther, H Schilke, P Stanke, T AF Beuther, H Schilke, P Stanke, T TI Multiple outflows in IRAS 19410+2336 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; stars : early type; stars : formation; ISM : jets and outflows ID MASS PROTOSTELLAR CANDIDATES; STAR-FORMATION; MOLECULAR OUTFLOWS; BIPOLAR OUTFLOWS; PRECESSING JET; EMISSION; IRAS-20126+4104; COLLAPSE; REGIONS; SAMPLE AB Plateau de Bure Interferometer high-spatial resolution CO observations combined with near-infrared H-2 data disentangle at least seven (possibly even nine) molecular outflows in the massive star-forming region IRAS 19410 + 2336. Position velocity diagrams of the outflows reveal Hubble-like relationships similar to outflows driven by low-mass objects. Estimated accretion rates are of the order of 10(-4) M-circle dot yr(-1), sufficiently high to overcome the radiation pressure and form massive stars via disk-mediated accretion processes. The single-dish large-scale mm continuum cores fragment into several compact condensations at the higher spatial resolution of the PdBI which is expected due to the clustering in massive star formation. While single-dish data give a simplified picture of the source, sufficiently high spatial resolution resolves the structures into outflows resembling those of low-mass star-forming cores. We interpret this as further support for the hypothesis that massive stars do form via disk-accretion processes similar to low-mass stars. 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. NR 36 TC 39 Z9 39 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2003 VL 408 IS 2 BP 601 EP 610 DI 10.1051/0004-6361:20030795 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 716AM UT WOS:000185006700017 ER PT J AU Wilhelm, K Kalkofen, W AF Wilhelm, K Kalkofen, W TI Observations of the upper solar chromosphere with SUMER SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE Sun : chromosphere; Sun : transition region; Sun : corona; Sun : UV radiation ID HIGH-RESOLUTION OBSERVATIONS; UNRESOLVED FINE-STRUCTURES; TRANSITION REGION LINES; HYDROGEN LYMAN LINES; QUIET-SUN; MAGNETIC-FIELDS; EMISSION-LINES; VELOCITY FIELDS; K-GRAINS; MG-I AB The structure and dynamics of the solar chromosphere are still matters of debate. The chromospheric network reflecting the supergranulation of the outer convection zone of the Sun is a prominent feature of the lower solar atmosphere that extends into the transition zone between chromosphere and corona. In particular, the physics of the so-called "nonmagnetic" chromosphere in internetwork regions as well as the physics of the magnetic network are not yet fully understood. Here we present observations of the H I Lyman continuum obtained in areas of the undisturbed Sun by the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) instrument on the Solar and Heliospheric Observatory (SOHO). The observing sequences are unique in the sense that they cover the spectral range from 67 nm to 93 nm with the highest cadence the SUMER spectrometer can achieve operating near the limit of its mechanism performance, telemetry allocation, and memory capabilities. In this wavelength range not only the Lyman continuum but also many extreme-ultraviolet emission lines (N II, N III, S IV, O II, O III, O IV, O V, Ne VIII, and Mg IX) are prominent, allowing the investigation of radiation formed at temperatures representative of regions from the chromosphere to the corona. Brightenings have been identified that are presumed to be related to the well-known 3 min oscillations as seen, for instance, in Ca II H-2v and K-2v observations. The relative temporal variations of the continuum radiance near 77 nm were typically 20% to 40%, whereas simultaneously recorded transition-region lines varied by about 40% of their lowest values in phase with the continuum. In the corona, the Ne VIII and Mg IX lines with formation temperatures of 620000 K and 950000 K, respectively, experienced relative changes of approximate to10% and displayed no phase relationship with the transition-region lines or the continuum. Radiance variations in the spatial regime across the solar disk show a higher correlation between the chromosphere and the corona than between the transition region and the corona. The observations will be discussed with a view towards providing constraints for modelling chromospheric structure and dynamics. C1 Max Planck Inst Aeron, D-37191 Katlenburg Lindau, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Max Planck Inst Aeron, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany. EM wilhelm@linmpi.mpg.de; wolf@cfa.harvard.edu NR 116 TC 15 Z9 16 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 2003 VL 408 IS 3 BP 1137 EP 1154 DI 10.1051/0004-6361:20030956 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 719PQ UT WOS:000185212600034 ER PT J AU Tonry, JL Schmidt, BP Barris, B Candia, P Challis, P Clocchiatti, A Coil, AL Filippenko, AV Garnavich, P Hogan, C Holland, ST Jha, S Kirshner, RP Krisciunas, K Leibundgut, B Li, WD Matheson, T Phillips, MM Riess, AG Schommer, R Smith, RC Sollerman, J Spyromilio, J Stubbs, CW Suntzeff, NB AF Tonry, JL Schmidt, BP Barris, B Candia, P Challis, P Clocchiatti, A Coil, AL Filippenko, AV Garnavich, P Hogan, C Holland, ST Jha, S Kirshner, RP Krisciunas, K Leibundgut, B Li, WD Matheson, T Phillips, MM Riess, AG Schommer, R Smith, RC Sollerman, J Spyromilio, J Stubbs, CW Suntzeff, NB TI Cosmological results from high-z supernovae SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmological parameters; cosmology : observations; distance scale; galaxies : distances and redshifts; supernovae : general ID GALAXY REDSHIFT SURVEY; FARTHEST KNOWN SUPERNOVA; OPTICAL LIGHT CURVES; IA SUPERNOVAE; ACCELERATING UNIVERSE; HUBBLE CONSTANT; INFRARED PHOTOMETRY; CCD PHOTOMETRY; POWER SPECTRUM; STANDARD STARS AB The High-z Supernova Search Team has discovered and observed eight new supernovae in the redshift interval z = 0.3-1.2. These independent observations, analyzed by similar but distinct methods, confirm the results of Riess and Perlmutter and coworkers that supernova luminosity distances imply an accelerating universe. More importantly, they extend the redshift range of consistently observed Type Ia supernovae (SNeIa) to z approximate to 1, where the signature of cosmological effects has the opposite sign of some plausible systematic effects. Consequently, these measurements not only provide another quantitative confirmation of the importance of dark energy, but also constitute a powerful qualitative test for the cosmological origin of cosmic acceleration. We find a rate for SN Ia of (1.4 +/- 0.5) x 10(-4) h(3) Mpc(-3) yr(-1) at a mean redshift of 0.5. We present distances and host extinctions for 230 SN Ia. These place the following constraints on cosmological quantities: if the equation of state parameter of the dark energy is w = -1, then H(0)t(0) = 0.96 +/- 0.04, and Omega(Lambda) - 1.4Omega(M) = 0.35 +/- 0/14. Including the constraint of a. at universe, we find Omega(M) = 0.28 +/- 0.05, independent of any large-scale structure measurements. Adopting a prior based on the Two Degree Field (2dF) Redshift Survey constraint on Omega(M) and assuming a. at universe, we find that the equation of state parameter of the dark energy lies in the range -1.48 < w < -0.72 at 95% confidence. If we further assume that w > -1, we obtain w < -0.73 at 95% confidence. These constraints are similar in precision and in value to recent results reported using the WMAP satellite, also in combination with the 2dF Redshift Survey. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Cerro Tololo Interamer Observ, La Serena, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Las Campanas Observ, La Serena, Chile. European So Observ, D-85748 Garching, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. SCFAB, Stockholm Observ, SE-10691 Stockholm, Sweden. RP Tonry, JL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Schmidt, Brian/0000-0001-6589-1287 NR 110 TC 1253 Z9 1261 U1 1 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 SEP 1 PY 2003 VL 594 IS 1 BP 1 EP 24 DI 10.1086/376865 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400001 ER PT J AU Colley, WN Schild, RE AF Colley, WN Schild, RE TI A rapid microlensing event in the Q0957+561A, B gravitational lens system SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : halos; gravitational lensing; quasars : individual (Q957+561) ID TIME-DELAY; CLOCK OBSERVATIONS; QUASAR Q0957+561; VARIABILITY; QSO-0957+561; PHOTOMETRY; A,B AB We reanalyze brightness data sampled intensively over five nights at two epochs separated by the quasar lens time delay to examine the nature of the observed microlensing. We find strong evidence for a microlensing event with an amplitude of 1% and a timescale of 12 hr. The existence of such rapid microlensing, albeit at low amplitude, imposes constraints on the nature of the quasar and of the baryonic dark matter. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Colley, WN (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. NR 19 TC 17 Z9 17 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2003 VL 594 IS 1 BP 97 EP 100 DI 10.1086/376832 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400007 ER PT J AU Finoguenov, A Burkert, A Bohringer, H AF Finoguenov, A Burkert, A Bohringer, H TI Role of clusters of galaxies in the evolution of the metal budget in the universe SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : clusters : general; galaxies : evolution; intergalactic medium ID MORPHOLOGY-DENSITY RELATION; INITIAL MASS FUNCTION; X-RAY-CLUSTERS; LY-ALPHA FOREST; STAR-FORMATION; INTERGALACTIC MEDIUM; ELLIPTIC GALAXIES; DARK-MATTER; INTRACLUSTER MEDIUM; CHEMICAL EVOLUTION AB Using the guidelines on supernova element production provided by XMM-Newton, we summarize the results of ASCA observations on the element abundance in groups and clusters of galaxies. We show that while the metal production in groups could be described by a stellar population with a standard local initial mass function (IMF), clusters of galaxies require a more top-heavy IMF. We attribute an excess heavy-element production to an IMF evolution with redshift. Dating the galaxy formation in clusters by observations of the star formation rate, we conclude that the IMF variations have occurred preferentially at z greater than or similar to 4. We further combine our metallicity measurements with the mass function of clusters to estimate the role of clusters in the evolution of the metal content of the universe. We argue that at no epoch stars are a major container of metals, unless groups of galaxies are not representative for the star formation. This lends further support for the reduced (0.6 solar) mass-averaged oxygen abundance in the stellar population. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM alexis@head-cfa.harvard.edu NR 71 TC 32 Z9 33 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 1 PY 2003 VL 594 IS 1 BP 136 EP 143 DI 10.1086/376778 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400012 ER PT J AU Mullis, CR McNamara, BR Quintana, H Vikhlinin, A Henry, JP Gioia, IM Hornstrup, A Forman, W Jones, C AF Mullis, CR McNamara, BR Quintana, H Vikhlinin, A Henry, JP Gioia, IM Hornstrup, A Forman, W Jones, C TI The 160 Square Degree ROSAT Survey: The revised catalog of 201 clusters with spectroscopic redshifts SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies : clusters : general; surveys; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; MEDIUM-SENSITIVITY SURVEY; DISTANT GALAXY CLUSTERS; COLD DARK-MATTER; ALL-SKY SURVEY; OPTICAL IDENTIFICATIONS; RICH CLUSTERS; COOLING FLOWS; HOT PLASMA; EVOLUTION AB We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z(median) = 0.25, and the median X-ray luminosity is L-X,L-median = 4.2 x 10(43) h(50)(-2) s(-1) (0.5 - 2.0 keV). This is the largest high-redshift sample of X-ray - selected clusters published to date. There are 73 objects at z > 0.3 and 22 objects at z > 0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4 x 10(-13) ergs cm(-2) s(-1). We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches. C1 European So Observ Headquarters, D-85748 Garching, Germany. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. CNR, Ist Radioastron, I-40129 Bologna, Italy. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. RP European So Observ Headquarters, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM cmullis@eso.org RI Gioia, Isabella/B-6982-2012 OI Gioia, Isabella/0000-0003-3127-498X NR 93 TC 80 Z9 80 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 1 PY 2003 VL 594 IS 1 BP 154 EP 171 DI 10.1086/376866 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400014 ER PT J AU Gaensler, BM Wallace, BJ AF Gaensler, BM Wallace, BJ TI A multifrequency radio study of supernova remnant G292.0+1.8 and its pulsar wind nebula SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G292.0+1.8); pulsars : individual (PSR J1124-5916); radio continuum : ISM; stars : neutron; supernova remnants ID SPECTRAL INDEX VARIATIONS; DIFFUSIVE SHOCK ACCELERATION; X-RAY NEBULA; NOVA REMNANT; GALACTIC PLANE; CRAB-NEBULA; MAGNETIC-FIELDS; PSR J1124-5916; LINE EMISSION; CASSIOPEIA-A AB We present a detailed radio study of the young supernova remnant (SNR) G292.0+1.8 and its associated pulsar PSR J1124-5916, using the Australia Telescope Compact Array at observing wavelengths of 20, 13, and 6 cm. We find that the radio morphology of the source consists of three main components: a polarized flat-spectrum central core coincident with the pulsar J1124-5916, a surrounding circular steep-spectrum plateau with sharp outer edges, and superposed on the plateau, a series of radial. laments with spectra significantly flatter than their surroundings. H I absorption argues for a lower limit on the distance to the system of 6 kpc. The core clearly corresponds to radio emission from a pulsar wind nebula powered by PSR J1124-5916, while we conclude that the plateau represents the surrounding SNR shell. The plateau's sharp outer rim delineates the SNR's forward shock, while the thickness of the plateau region demonstrates that the forward and reverse shocks are well separated. Assuming a distance of 6 kpc and an age for the source of 2500 yr, we infer an expansion velocity for the SNR of similar to1200 km s(-1), an ambient density similar to0.9 cm(-3), an ejected mass similar to5.9 M-., and a supernova explosion energy similar to1.1 x 10(51) ergs. We interpret the flat-spectrum radial. laments superposed on the steeper spectrum plateau as Rayleigh-Taylor unstable regions between the forward and reverse shocks of the SNR. The. at radio spectrum seen for these features results from efficient second-order Fermi acceleration in strongly amplified magnetic fields. Overall, SNR G292.0+1.8 shows an unusual set of properties not seen in any other SNR. This source may reflect a unique stage in evolution, seen only for systems at an age of similar to2500 yr and only when there is both a bright SNR shell and an energetic associated pulsar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Def R&D Canada Ottawa, Ottawa, ON K1A 0Z4, Canada. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-6, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 86 TC 47 Z9 47 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2003 VL 594 IS 1 BP 326 EP 339 DI 10.1086/376861 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400024 ER PT J AU Perna, R Sari, R Frail, D AF Perna, R Sari, R Frail, D TI Jets in gamma-ray bursts: Tests and predictions for the structured jet model SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; gamma rays : bursts ID STANDARD ENERGY RESERVOIR; AFTERGLOW LIGHT CURVES; STAR-FORMATION HISTORY; LUMINOSITY; GALAXIES; SUPERSHELLS; GRB-990510; GRB-980519; REMNANTS; UNIVERSE AB The two leading interpretations of achromatic breaks that are observed in the light curves of GRBs afterglow are (1) the manifestation of the edge of a jet, which has a roughly uniform energy profile and a sharp edge, and (2) a line-of-sight effect in jets with a variable energy profile. The first scenario requires the inner engine to produce a jet with a different opening angle each explosion, while the latter requires a standard engine. The physical structure of the jet is a crucial factor in understanding GRB progenitors, and therefore discriminating the two jet scenarios is particularly relevant. In the structured jet case, specific predictions can be made for the distribution of observed break angles theta(br), while that distribution is arbitrary in the first scenario. We derive the theoretical distribution for the structured jet model. Specifically, we predict the most common angle to be about 0.12 rad, in rough agreement with the sample. If this agreement holds as the sample size increases, it would strengthen the case for the standard jet hypothesis. We show that a prediction of this model is that the average viewing angle is an increasing function of the survey sensitivity and in particular that a mission such as Swift will find the typical viewing angle to be about 0.3 rad. The local event rate predicted by this model is R-GRB(z = 0) similar to 0.5 Gpc(-3) yr(-1). C1 Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Perna, R (reprint author), Harvard Soc Fellows, 74 Mt Auburn St, Cambridge, MA 02138 USA. NR 27 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 1 PY 2003 VL 594 IS 1 BP 379 EP 384 DI 10.1086/376772 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400028 ER PT J AU Heyrovsky, D AF Heyrovsky, D TI Measuring stellar limb darkening by gravitational microlensing SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; methods : data analysis; stars : atmospheres ID EVENT MACHO 98-SMC-1; PLANET PHOTOMETRY; RED GIANT; ECLIPSING BINARIES; ANGULAR DIAMETER; PULSATION MODES; LIGHT CURVES; STARS; HD-209458; TRANSIT AB Observations of microlensing transit events can be used to measure the limb darkening of the lensed star. We discuss the advantages and drawbacks of several microlensing light-curve inversion methods. The method of choice in this work is inversion by means of decomposition of the stellar surface brightness profile. We construct an ideal basis by principal component analysis of brightness profiles obtained from model atmosphere calculations. Limb-darkening approximations using such a basis are superior to those using standard power-law limb-darkening laws. We perform a full analysis of simulated single-lens microlensing transit events including a detailed error analysis of the method. In realistic events with a low impact parameter the brightness profile of the source can be recovered with a relative accuracy of 2% from the center of the source disk to 0.9 of the disk radius. We show that in the particular case of the observed MACHO Alert 9530 event the intrinsic complex variability of the lensed red giant hinders efforts to recover its surface features. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heyrovsky, D (reprint author), Stahlavce 6, Prague 16000 6, Czech Republic. RI Heyrovsky, David/A-2031-2015 OI Heyrovsky, David/0000-0002-5198-5343 NR 58 TC 17 Z9 17 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 2003 VL 594 IS 1 BP 464 EP 482 DI 10.1086/376787 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400038 ER PT J AU Drake, JJ AF Drake, JJ TI From the heart of the ghoul: C and N abundances in the corona of Algol B SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : abundances; stars : activity; stars : coronae; stars : late-type; Sun : corona; X-rays : stars ID RS-CANUM-VENATICORUM; X-RAY-EMISSION; PHOTOSPHERIC METAL ABUNDANCES; OPTICALLY THIN PLASMAS; LIGHT-CURVE ANALYSIS; BINARY-SYSTEMS; CHEMICAL-COMPOSITION; MAGNETIC ACTIVITY; NITROGEN ABUNDANCES; CONTINUUM EMISSION AB Chandra Low Energy Transmission Grating Spectrograph observations of Algol have been used to determine the abundances of C and N in the secondary star for the first time. In order to minimize errors arising from an uncertain coronal differential emission measure as a function of temperature, the analysis was performed relative to similar observations of an adopted "standard'' star, HR 1099. It is demonstrated that HR 1099 and Algol are coronal twins in many respects and that their X-ray spectra are very similar in nearly all details, except for the observed strengths of C and N lines. The H-like 2p P-2(3/2,1/2) --> 1s S-2(1/2) transitions of C and N in the coronae of Algol and HR 1099 demonstrate that the surface abundances of Algol B have been strongly modified by CN processing, as shown earlier by Schmitt & Ness. It is found that N is enhanced in Algol B by a factor of 3 compared with HR 1099. No C lines are detected in the Algol spectrum, indicating a C depletion relative to HR 1099 by a factor of 10 or more. These C and N abundances indicate that Algol B must have lost at least half of its initial mass and are consistent with predictions of evolutionary models that include nonconservative mass transfer and angular momentum loss through magnetic activity. Based on H-like and He-like transitions in O and Ne, it is estimated that Algol is slightly metal poor, by 0.2 dex in terms of the coronal abundances of light elements relative to HR 1099, while the Fe XVII 2p(5)3d P-1(1) --> 2p(6) S-1(0) transition indicates a very similar Fe abundance. In reviewing coronal abundance results for active stars in the literature and drawing on an earlier Chandra study of the coronal abundances of HR 1099, it is concluded that Fe is very likely depleted in the coronae of both Algol and HR 1099 by 0.5 dex relative to their photospheric compositions, but that Ne is enhanced by a similar magnitude. Light elements such as C, N, and O are likely depleted in both stars by of order 0.3 dex. The similarities in these large-abundance anomalies in HR 1099 and Algol are notable. Despite such compositional fractionation in these coronae, the relative C and N abundances in HR 1099, determined by comparing observed line strengths with theoretical C/N line ratios, are consistent with recent solar values, indicating that differential fractionation between these elements is not significant and that little or no dredge-up of material subjected to CN processing has occurred on the subgiant component. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA. NR 72 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 1 PY 2003 VL 594 IS 1 BP 496 EP 509 DI 10.1086/375837 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400040 ER PT J AU Cranmer, SR van Ballegooijen, AA AF Cranmer, SR van Ballegooijen, AA TI Alfvenic turbulence in the extended solar corona: Kinetic effects and proton heating SO ASTROPHYSICAL JOURNAL LA English DT Review DE MHD; plasmas; solar wind; Sun : corona; turbulence; waves ID ION-CYCLOTRON WAVES; PHASE-SPACE HOLES; ELECTROSTATIC SOLITARY WAVES; DOMINATED ACCRETION FLOWS; LOW-FREQUENCY WAVES; MAGNETOHYDRODYNAMIC TURBULENCE; MAGNETIC-FIELD; WIND PLASMA; VELOCITY DISTRIBUTIONS; PARTICLE-ACCELERATION AB We present a model of magnetohydrodynamic (MHD) turbulence in the extended solar corona that contains the effects of collisionless dissipation and anisotropic particle heating. Recent observations have shown that preferential heating and acceleration of positive ions occur in the first few solar radii of the high-speed solar wind. Measurements made by the Ultraviolet Coronagraph Spectrometer aboard SOHO have revived interest in the idea that ions are energized by the dissipation of ion cyclotron resonant waves, but such high-frequency (i.e., small-wavelength) fluctuations have not been observed. A turbulent cascade is one possible way of generating small-scale fluctuations from a preexisting population of low-frequency MHD waves. We model this cascade as a combination of advection and diffusion in wavenumber space. The dominant spectral transfer occurs in the direction perpendicular to the background magnetic field. As expected from earlier models, this leads to a highly anisotropic fluctuation spectrum with a rapidly decaying tail in the parallel wavenumber direction. The wave power that decays to high enough frequencies to become ion cyclotron resonant depends on the relative strengths of advection and diffusion in the cascade. For the most realistic values of these parameters, however, there is insufficient power to heat protons and heavy ions. The dominant oblique fluctuations ( with dispersion properties of kinetic Alfven waves) undergo Landau damping, which implies strong parallel electron heating. We discuss the probable nonlinear evolution of the electron velocity distributions into parallel beams and discrete phase-space holes ( similar to those seen in the terrestrial magnetosphere), which can possibly heat protons via stochastic interactions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 161 TC 133 Z9 133 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2003 VL 594 IS 1 BP 573 EP 591 DI 10.1086/376777 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400048 ER PT J AU Kuchner, MJ Spergel, DN AF Kuchner, MJ Spergel, DN TI Notch-filter masks: Practical image masks for planet-finding coronagraphs SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; instrumentation : adaptive optics; planetary systems ID EXTRASOLAR TERRESTRIAL PLANETS; EARTH-LIKE PLANETS; ADAPTIVE OPTICS; DEFORMABLE MIRROR; SPACE TELESCOPE; PERFORMANCE; STARLIGHT AB An ideal coronagraph with a band-limited image mask can efficiently image off-axis sources while removing identically all of the light from an on-axis source. However, strict mask construction tolerances limit the utility of this technique for directly imaging extrasolar terrestrial planets. We present a variation on the basic band-limited mask design - a family of "notch-filter'' masks - that mitigates this problem. These robust and trivially achromatic masks can be easily manufactured by cutting holes in opaque material. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. RP Kuchner, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS 20,60 Garden St, Cambridge, MA 02138 USA. RI Kuchner, Marc/E-2288-2012; Spergel, David/A-4410-2011 NR 27 TC 28 Z9 28 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2003 VL 594 IS 1 BP 617 EP 626 DI 10.1086/375836 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KJ UT WOS:000185087400051 ER PT J AU Drake, JJ Sarna, MJ AF Drake, JJ Sarna, MJ TI X-ray evidence of the common envelope phase of V471 Tauri SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; novae, cataclysmic variables; stars : abundances; stars : activity; stars : coronae; X-rays : stars ID BD&16 DEGREES 516; CHEMICAL ABUNDANCES; LITHIUM DEPLETION; RATE COEFFICIENTS; EVOLVED STARS; WHITE-DWARF; EVOLUTION; BINARIES; GIANTS; ROTATION AB Chandra Low Energy Transmission Grating Spectrograph observations of the precataclysmic binary V471 Tauri have been used to estimate the C/N abundance ratio of the K dwarf component for the first time. While the white dwarf component dominates the spectrum longward of 50 Angstrom, at shorter wavelengths the observed X-ray emission is entirely due to coronal emission from the K dwarf. The H-like 2p P-2(3.2, 1/2) --> 1s S-2(1/2) resonance lines of C and N yield an estimate of their logarithmic abundance ratio relative to the Sun of [C/N] = -0.38 +/- 0.15-half of the currently accepted solar value. We interpret this result as the first clear observational evidence for the presumed common envelope phase of this system, during which the surface of the K dwarf was contaminated by CN cycle-processed material dredged up into the red giant envelope. We use the measured C/N ratio to deduce that 0.015-0.04 M-. was accreted by the K dwarf while engulfed and to show that this is consistent with a recent tentative detection of C-13 in the K dwarf photosphere and with the measured Li abundance in the scenario in which the red giant companion was Li-rich during the common envelope phase. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Polish Acad Sci, Nicolas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA. NR 38 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 SEP 1 PY 2003 VL 594 IS 1 BP L55 EP L58 DI 10.1086/378577 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KM UT WOS:000185087700014 ER PT J AU Gaensler, BM Fogel, JKJ Slane, PO Miller, JM Wijnands, R Eikenberry, SS Lewin, WHG AF Gaensler, BM Fogel, JKJ Slane, PO Miller, JM Wijnands, R Eikenberry, SS Lewin, WHG TI Untwisting the tornado: X-ray imaging and spectroscopy of G357.7-0.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G357.7-0.1); supernova remnants; X-rays : ISM ID MORPHOLOGY SUPERNOVA-REMNANTS; MHZ MASER EMISSION; OH; SYSTEM; MICROQUASAR; EVOLUTION; PULSARS; SHOCK; ROSAT AB We report on the detection of X-ray emission from the unusual Galactic radio source G357.7-0.1 (the "Tornado"). Observations made with the Chandra X-Ray Observatory demonstrate the presence of up to three sources of X-ray emission from the Tornado: a relatively bright region of dimensions 2' x 1' coincident with and interior to the brightest radio emission at the " head" of the Tornado, plus two fainter extended regions possibly associated with the Tornado's "tail." No X-ray point sources associated with the Tornado are seen down to a 3 sigma luminosity (0.5-10 keV) of 1 x 10(33) ergs s(-1), for a distance to the system of 12 kpc. The spectrum of the brightest region of X-rays is consistent with a heavily absorbed (N-H approximate to 10(23) cm(-2)) thermal plasma of temperature kT similar to 0.6 keV; an absorbed power law can also fit the data but implies an extremely steep photon index. From these data we tentatively conclude that the Tornado is a supernova remnant (SNR), although we are unable to rule out the possibility that the Tornado is powered either by outflows from an X-ray binary or by the relativistic wind of an unseen pulsar. Within the SNR interpretation, the head of the Tornado is a limb-brightened radio shell that contains centrally filled thermal X-rays and that is interacting with a molecular cloud. We therefore propose that the Tornado is a "mixed morphology" supernova remnant. The unusual tail component of the Tornado remains unexplained in this interpretation but might result from expansion of the SNR into an elongated progenitor wind bubble. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Univ, Cambridge, MA 02138 USA. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, MS 6,60 Garden St, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 30 TC 10 Z9 10 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2003 VL 594 IS 1 BP L35 EP L38 DI 10.1086/378260 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KM UT WOS:000185087700009 ER PT J AU Zezas, A Ward, MJ Murray, SS AF Zezas, A Ward, MJ Murray, SS TI Chandra observations of the X-ray-luminous star-forming galaxy merger ARP 299 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Arp 299, IC 694, NGC 3690); galaxies : interactions; galaxies : peculiar; X-rays : binaries; X-rays : galaxies ID STARBURST GALAXIES; POPULATIONS AB We report the results of a Chandra observation of the X-ray-luminous star-forming galaxy Arp 299 (NGC 3690/IC 694). We detect 18 discrete X-ray sources with luminosities above similar to10(39) ergs s(-1) (0.5-8.0 keV band), which contribute similar to40% of the total galactic emission in this band. The remaining emission is associated with a diffuse component spatially coincident with regions of widespread star formation. We detect X-ray emission from both nuclei. One of the discrete sources within the complex nuclear region of NGC 3690 is found to have a very hard spectrum, and therefore we associate it with the origin of the active galactic nucleus-like spectrum that has also been detected at high X-ray energies using BeppoSAX. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Xray Astron Grp, Leicester LE2 7RH, Leics, England. 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 19 TC 47 Z9 47 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2003 VL 594 IS 1 BP L31 EP L34 DI 10.1086/378144 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KM UT WOS:000185087700008 ER PT J AU Reed, DH O'Grady, JJ Brook, BW Ballou, JD Frankham, R AF Reed, DH O'Grady, JJ Brook, BW Ballou, JD Frankham, R TI Estimates of minimum viable population sizes for vertebrates and factors influencing those estimates SO BIOLOGICAL CONSERVATION LA English DT Article DE demographic stochasticity; endangered species; extinction; minimum viable population size; population variability; population viability analysis ID SPATIAL PVA MODELS; INBREEDING DEPRESSION; DENSITY-DEPENDENCE; CONSERVATION BIOLOGY; VIABILITY ANALYSIS; EXTINCTION RISK; BUTTERFLY METAPOPULATION; ORB SPIDERS; VARIABILITY; DYNAMICS AB Population size is a major determinant of extinction risk. However, controversy remains as to how large populations need to be to ensure persistence. It is generally believed that minimum viable population sizes (MVPs) would be highly specific, depending on the environmental and life history characteristics of the species. We used population viability analysis to estimate MVPs for 102 species. We define a minimum viable population size as one with a 99% probability of persistence for 40 generations. The models are comprehensive and include age-structure, catastrophes, demographic stochasticity, environmental stochasticity, and inbreeding depression. The mean and median estimates of MVP were 7316 and 5816 adults, respectively. This is slightly larger than, but in general agreement with, previous estimates of MVP. MVPs did not differ significantly among major taxa, or with latitude or trophic level, but were negatively correlated with population growth rate and positively correlated with the length of the study used to parameterize the model. A doubling of study duration increased the estimated MVP by approximately 67%. The increase in extinction risk is associated with greater temporal variation in population size for models built from longer data sets. Short-term studies consistently underestimate the true variances for demographic parameters in populations. Thus, the lack of long-term studies for endangered species leads to widespread underestimation of extinction risk. The results of our simulations suggest that conservation programs, for wild populations, need to be designed to conserve habitat capable of supporting approximately 7000 adult vertebrates in order to ensure long-term persistence. (C) 2003 Elsevier Science Ltd. All rights reserved. C1 Macquarie Univ, Dept Sci Biol, Key Ctr Biodivers & Bioresources, N Ryde, NSW 2109, Australia. No Terr Univ, Key Ctr Trop Wildlife Management, Darwin, NT 0909, Australia. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Conservat Biol, Washington, DC 20008 USA. RP Univ Mississippi, Dept Biol, POB 1848, University, MS 38677 USA. RI Brook, Barry/G-2686-2011 OI Brook, Barry/0000-0002-2491-1517 NR 92 TC 197 Z9 212 U1 20 U2 146 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD SEP PY 2003 VL 113 IS 1 BP 23 EP 34 AR PII S0006-3207(02)00346-4 DI 10.1016/S0006-3207(02)00346-4 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 691EC UT WOS:000183591000003 ER PT J AU Leverington, D Teller, J AF Leverington, D Teller, J TI Paleotopographic reconstructions of the eastern outlets of glacial Lake Agassiz SO CANADIAN JOURNAL OF EARTH SCIENCES LA English DT Article ID LAURENTIDE ICE-SHEET; ABRUPT CLIMATE-CHANGE; C-14 YR BP; 3-OUTLET CONTROL; LARGE BEACHES; VOLUME; BASIN; SEDIMENTATION; SASKATCHEWAN; BATHYMETRY AB Paleotopographic reconstructions of the eastern outlets of glacial Lake Agassiz provide a foundation for understanding the complex manner in which terrain morphology controlled the routing of overflow through the eastern outlets during the lake's Nipigon Phase (ca. 9400-8000 C-14 years BP) and for understanding the causes of outlet-driven declines in lake level during that period. Although flow paths across the divide between the Agassiz and Nipigon basins were numerous, eastward releases from Lake Agassiz to glacial Lake Kelvin (modern Lake Nipigon) were channeled downslope into a relatively small number of major channels that included the valleys of modern Kopka River, Ottertooth Creek, Vale Creek, Whitesand River, Pikitigushi River, and Little Jackfish River. From Lake Kelvin, these waters overflowed into the Superior basin. The numerous lowerings in lake level between stages of the Nipigon Phase, controlled by topography and the position of the retreating southern margin of the Laurentide Ice Sheet, had magnitudes of between 8 and 58 m, although some of these drawdowns may have occurred as multiple individual events that could have been as small as several metres. The total volumes of water released in association with these drops were as great as 8100 km(3), and for all Nipigon stages were probably between about 140 and 250 km(3) per metre of lowering. The topographic reconstructions demonstrate that Lake Agassiz occupied the area of glacial Lake Nakina (located northeast of modern Lake Nipigon) by the The Pas stage (ca. 8000 C-14 years BP) and that Lake Agassiz drainage through the Nipigon basin to the Great Lakes ended before the succeeding Gimli stage. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. RP Leverington, D (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 49 TC 40 Z9 40 U1 1 U2 10 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4077 J9 CAN J EARTH SCI JI Can. J. Earth Sci. PD SEP PY 2003 VL 40 IS 9 BP 1259 EP 1278 DI 10.1139/E03-043 PG 20 WC Geosciences, Multidisciplinary SC Geology GA 727DH UT WOS:000185640900006 ER PT J AU Stern, SA Kenyon, SJ AF Stern, SA Kenyon, SJ TI Collisions, accretion, and erosion in the Kuiper Belt SO COMPTES RENDUS PHYSIQUE LA English DT Article DE Kuiper Belt; collisions; accretion ID OUTER SOLAR-SYSTEM; PLANET FORMATION; TIME SCALES; OBJECTS; NEPTUNE; FRAGMENTATION; EVOLUTION; CENTAURS; COMETS; PLUTO AB Collisional modeling has been a fertile area of Kuiper Belt research for almost a decade. Such modeling has yielded important results concerning expected KBO surface properties, the KBO size distribution, the origin of KBOs and the properties of the primoridal Kuiper Belt, and most recently, the formation of KBO satellites. In what follows we briefly review some isolated aspects of these research results. A far more comprehensive, but older review of this topic was provided by Farinella et al. (in: Protostars and Planets IV, Mannings et al. (Eds.), University of Arizona Press, 2001). C1 SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. Smithsonian Astrophys Observ, Cambridge, MA USA. RP Stern, SA (reprint author), SW Res Inst, Dept Space Studies, 1050 Walnut St,Suite 400, Boulder, CO 80302 USA. EM astern@swri.edu NR 31 TC 3 Z9 3 U1 0 U2 0 PU EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0705 J9 CR PHYS JI C. R. Phys. PD SEP PY 2003 VL 4 IS 7 BP 803 EP 808 DI 10.1016/j.crhy.2003.10.008 PG 6 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA 769CB UT WOS:000188607900009 ER PT J AU Thompson, FC Marinoni, L AF Thompson, FC Marinoni, L TI Copestylum circumdatum (Walker) (Diptera : Syrphidae): Redescription of a neotropical flower fly, with lectotype designations, and new synonyms SO ENTOMOLOGICAL NEWS LA English DT Article DE Diptera; Syrphidae; Copestylum; Neotropics; lectotype; synonyms AB Copestylum circumdatum (Walker) (Diptera: Syrphidae) is redescribed. Lectotypes are designated for two names and one new synonym is proposed (Volucella mus Williston 1888 = circumdatum Walker 1857). C1 USDA ARS, Systemat Entomol Lab, Smithsonian Inst, Washington, DC 20560 USA. Univ Fed Parana, Dept Zool, BR-80060000 Curitiba, Parana, Brazil. RP Thompson, FC (reprint author), USDA ARS, Systemat Entomol Lab, Smithsonian Inst, NHB-168, Washington, DC 20560 USA. EM cthompso@sel.barc.usdad.gov; lmarinoni@ufpr.br RI Marinoni, Luciane /C-5720-2013 NR 14 TC 1 Z9 3 U1 0 U2 1 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 2003 VL 114 IS 4 BP 217 EP 223 PG 7 WC Entomology SC Entomology GA 849LV UT WOS:000223541000007 ER PT J AU Lessios, HA Kane, J Robertson, DR AF Lessios, HA Kane, J Robertson, DR TI Phylogeography of the pantropical sea urchin Tripneustes: Contrasting patterns of population structure between oceans SO EVOLUTION LA English DT Article DE Benguela; cytochrome oxidase I; Eastern Pacific Barrier; gene flow; Isthmus of Panama; sea urchins; speciation ID TROPICAL EASTERN PACIFIC; HIGH-DISPERSAL STARFISH; HUMAN MITOCHONDRIAL-DNA; GLOBAL PHYLOGEOGRAPHY; GENETIC-DIFFERENCES; MOLECULAR VARIANCE; XIPHIAS-GLADIUS; SOUTH-AMERICA; EL-NINO; EVOLUTION AB To understand how allopatric speciation proceeds, we need information on barriers to gene flow, their antiquity, and their efficacy. For marine organisms with planktonic larvae, much of this information can only be obtained through the determination of divergence between populations. We evaluated the importance of ocean barriers by studying the mitochondrial DNA phylogeography of Tripneustes, a pantropical genus of shallow water sea urchin. A region of cytochrome oxidase I (COI) was sequenced in 187 individuals from locations around the globe. The COI phylogeny agreed with a previously published phylogeny of bindin that barriers important to the evolution of Tripneustes are: (1) the cold water upwelling close to the tip of South Africa, (2) the Isthmus of Panama, (3) the long stretch of deep water separating the eastern from the western Atlantic, and (4) the freshwater plume of the Orinoco and the Amazon rivers between the Caribbean and the coast of Brazil. These barriers have previously been shown to be important in at least a subset of the shallow water marine organisms in which phylogeography has been studied. In contrast, the Eastern Pacific Barrier, 5000 km of deep water between the central and the eastern Pacific that has caused the deepest splits in other genera of sea urchins, is remarkably unimportant as a cause of genetic subdivision in Tripneustes. There is also no discernible subdivision between the Pacific and Indian Ocean populations of this genus. The most common COI haplotype is found in the eastern, central, and western Pacific as well as the Indian Ocean. Morphology, COI, and bindin data agree that T. depressus from the eastern Pacific and T. gratilla from the western Pacific are, in fact, the same species. The distribution of haplotype differences in the Indo-Pacific exhibits characteristics expected from a sea urchin genus with ephemeral local populations, but with high fecundity, dispersal, and growth: there is little phylogenetic structure, and mismatch distributions conform to models of recent population expansion on a nearly global scale. Yet, comparisons between local populations produce large and significant F-ST values, indicating nonrandom haplotype distribution. This apparent local differentiation is only weakly reflected in regional divergence, and there is no evidence of isolation by distance in correlations between FST values and either geographical or current distance. Thus, Tripneustes in the Indo-Pacific (but not in the Atlantic) seems to be one large metapopulation spanning two oceans and containing chaotic, nonequilibrium local variation, produced by the haphazard arrival of larvae or by unpredictable local extinction. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Lessios, HA (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. NR 91 TC 142 Z9 148 U1 2 U2 30 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD SEP PY 2003 VL 57 IS 9 BP 2026 EP 2036 DI 10.1554/02-681 PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 727TB UT WOS:000185674500006 PM 14575324 ER PT J AU Skeans, MH AF Skeans, MH TI Identifying tribes of waterfowl (Anseriformes : Anatidae) by microscopic examination of feather down morphology SO FORENSIC SCIENCE INTERNATIONAL LA English DT Meeting Abstract CT 3rd European-Academy-of-Forensic-Science Meeting CY SEP 22-27, 2003 CL ISTANBUL, TURKEY SP European Acad Forens Sci, Istanbul Univ, Inst Forens Sci DE feather; ornithology; waterfowl C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 2 U2 2 PU ELSEVIER SCI IRELAND LTD PI CLARE PA CUSTOMER RELATIONS MANAGER, BAY 15, SHANNON INDUSTRIAL ESTATE CO, CLARE, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD SEP PY 2003 VL 136 SU 1 BP 385 EP 385 PG 1 WC Medicine, Legal SC Legal Medicine GA 725HM UT WOS:000185538200854 ER PT J AU Skeans, MH AF Skeans, MH TI Adding up feather evidence - Solving a case of forensic ornithology SO FORENSIC SCIENCE INTERNATIONAL LA English DT Meeting Abstract CT 3rd European-Academy-of-Forensic-Science Meeting CY SEP 22-27, 2003 CL ISTANBUL, TURKEY SP European Acad Forens Sci, Istanbul Univ, Inst Forens Sci DE feather; forensic ornithology C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. Fed Bur Invest, Trace Evidence Unit, Quantico, VA 22135 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI IRELAND LTD PI CLARE PA CUSTOMER RELATIONS MANAGER, BAY 15, SHANNON INDUSTRIAL ESTATE CO, CLARE, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD SEP PY 2003 VL 136 SU 1 BP 386 EP 387 PG 2 WC Medicine, Legal SC Legal Medicine GA 725HM UT WOS:000185538200856 ER PT J AU MacPherson, GJ Huss, GR Davis, AM AF MacPherson, GJ Huss, GR Davis, AM TI Extinct (10)Be in type a calcium-aluminum-rich inclusions from CV chondrites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EARLY SOLAR-SYSTEM; REFRACTORY INCLUSIONS; ALLENDE METEORITE; COSMIC-RAYS; ISOTOPIC SYSTEMATICS; LIGHT-ELEMENTS; GAMMA-RAYS; CHONDRULES; MAGNESIUM; ABUNDANCES AB We have found clear evidence of live (10)Be in five normal Type A Calcium-aluminum-rich inclusions (CAIs), one normal Type B CAI, and one FUN Type A CAI, all from CV3 chondrites. The ((10)Be/(9)Be)(0) ratios range from similar to0.36 X 10(-3) to similar to0.77 X 10(-3) and are similar to those found by previous workers. The ((10)Be/(9)Be)(0) ratios do not correlate in a temporal fashion with ((26)Al/(27)Al)(0), suggesting that (10)Be and (26)Al were produced by different mechanisms. An examination of possible sources for the short-lived radionuclides indicates that production of (10)Be was almost certainly by particle irradiation, possibly within the solar system, and was probably accompanied by significant production of (41)Ca and (53)Mn. In contrast, all of the (60)Fe, most of the (26)Al, and some of the (53)Mn were probably produced in stars and were imported into the solar system within presolar dust grains. Copyright (C) 2003 Elsevier Ltd. C1 Smithsonian Inst, Museum Hist Nat, Dept Mineral Sci, Washington, DC 20560 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Arizona State Univ, Ctr Meteorite Studies, Tempe, AZ 85287 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. RP MacPherson, GJ (reprint author), Smithsonian Inst, Museum Hist Nat, Dept Mineral Sci, Washington, DC 20560 USA. EM glenn@volcano.si.edu OI Davis, Andrew/0000-0001-7955-6236 NR 55 TC 55 Z9 55 U1 2 U2 13 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 2003 VL 67 IS 17 BP 3165 EP 3179 DI 10.1016/S0016-7037(02)01298-X PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 717VJ UT WOS:000185111200006 ER PT J AU Vicenzi, EP Heaney, PJ Ketcham, RA Rivers, M AF Vicenzi, EP Heaney, PJ Ketcham, RA Rivers, M TI High resolution X-ray microtomography of polycrystalline diamond SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 13th Annual VM Goldschmidt Conference CY SEP 07-12, 2003 CL KURASHIKI, JAPAN C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. Argonne Natl Lab, Argonne, IL 60439 USA. EM vicenzi@volcano.si.edu; heaney@geosc.psu.edu; ketcham@mail.utexas.edu; rivers@cars.uchicago.edu RI Ketcham, Richard/B-5431-2011 OI Ketcham, Richard/0000-0002-2748-0409 NR 0 TC 1 Z9 1 U1 0 U2 2 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 2003 VL 67 IS 18 SU 1 BP A513 EP A513 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 724ZF UT WOS:000185517601010 ER PT J AU Schimmelmann, A Lange, CB Meggers, BJ AF Schimmelmann, A Lange, CB Meggers, BJ TI Palaeoclimatic and archaeological evidence for a similar to 200-yr recurrence of floods and droughts linking California, Mesoamerica and South America over the past 2000 years SO HOLOCENE LA English DT Review DE flood; drought; climatic change; solar variability; periodicity; teleconnection; cultural transition; Holocene; Santa Barbara Basin; California; Mesoamerica; South America ID TREE-RING RECORDS; SOUTHWESTERN UNITED-STATES; NORTHERN GREAT-PLAINS; STABLE-ISOTOPE RECORD; LATE-HOLOCENE CLIMATE; GREENLAND ICE-SHEET; SAN-FRANCISCO BAY; LAST MILLENNIUM; ENVIRONMENTAL-CHANGE; VOLCANIC-ERUPTIONS AB Conspicuous grey, clay-rich flood deposits in the predominantly olive, varved sediment in the central Santa Barbara Basin, California, were dated via varve-counting to c. AD 212, 440, 603, 1029, 1418 and 1605. The similar to 200-yr quasi-periodicity and the timing of individual floods match time periods of known supraregional climatic changes and the documented similar to200-yr periodicity in palaeoclimate records elsewhere. The floods of c. ad 440 and ad 1418 occurred during global reorganizations of atmospheric circulation. Cold spells seem to have accompanied the floods of c. AD 1029 and ad 1605. California floods and other palaeoclimate records suggest that expressions of regional climates are modulated by solar variability with a similar to 200-yr periodicity. Our compilation of palaeoclimatic and Mesoamerican and South American archaeological records provides evidence that palaeoenvironmental and cultural changes were often coincident within their respective dating uncertainties and occurred in similar to 200-yr steps. The matching pattern supports the hypothesis that manifestations of changing climates, such as drought or flooding, served as destabilizing cofactors in transitions of precolumbian cultures. Extrapolation of the similar to 200-yr recurrence pattern of Santa Barbara flooding suggests that catastrophic flooding in southern California may be expected for the early part of this century. C1 Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. Univ Concepcion, Dept Oceanog, Ctr Invest Oceanog Pacifico SurOriental, FONDAP, Concepcion 3, Chile. Smithsonian Inst, Washington, DC 20013 USA. RP Schimmelmann, A (reprint author), Indiana Univ, Dept Geol Sci, 1001 E 10th St, Bloomington, IN 47405 USA. EM aschimme@indiana.edu NR 152 TC 46 Z9 46 U1 7 U2 24 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0959-6836 EI 1477-0911 J9 HOLOCENE JI Holocene PD SEP PY 2003 VL 13 IS 5 BP 763 EP 778 DI 10.1191/0959683603hl661rp PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 721MK UT WOS:000185320000011 ER PT J AU Zhang, W Tong, CYE Shi, SC AF Zhang, W Tong, CYE Shi, SC TI Scaled model measurement of the embedding impedance of a 660-GHz waveguide SIS mixer with a 3-standard deembedding method SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE deembedding method; embedding impedance; scaled model; SIS mixer; time domain gating AB In this paper, I the. embedding impedance of a 660-GHz superconductor-insulator-superconducter (SIS) mixer is investigated using a 100-times scalled-model with a new 3-standard deembedding technique. The mixer embedding impedance is extracted from the reflection coefficients, measured at the waveguide port of the mixer for three different terminations at the SIS junction's feed point. The three standards chosen are open-circuit, short-circuit and resistive load. Measured results are compared with those simulated by high-frequency structure simulator (HFSS). C1 Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, W (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. OI Tong, Edward/0000-0002-7736-4203 NR 10 TC 4 Z9 5 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD SEP PY 2003 VL 13 IS 9 BP 376 EP 378 DI 10.1109/LMWC.2003.817112 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 722UZ UT WOS:000185397500006 ER PT J AU Launius, RD AF Launius, RD TI Perfect worlds, perfect societies: The persistent goal of utopia in human spaceflight SO JBIS-JOURNAL OF THE BRITISH INTERPLANETARY SOCIETY LA English DT Article DE utopia; spaceflight; Gerard K. O'Neill; Robert Zubrin; solar power satellite; space colonies ID SPACE-SHUTTLE; DECISION AB This essay sets about the task of exploring three basic aspects of the persistent goal of Utopia in human spaceflight. First, after briefly considering the rise of spaceflight in the United States, this essay will discuss the rise of a zealous pro-space movement in the 1970s and the resulting efforts to justify space exploration using a range of arguments that at their base contain a strong element of utopianism. Second, this paper shall investigate the radical ideas of spaceflight utopianism contained in the work of Gerard K. O'Neill and extending to the present with advocates such as Robert Zubrin. Finally, this essay will explore flaws in the utopian impulse in favor of space exploration. Like all works of advocacy, those who seek to "sell" spaceflight as a positive good overstate their cases. Clearly the radical utopian ideal of creating a perfect society has numerous effective detractors and may be debunked using any number of methodologies: history, psychology, economics, political theory, and technological hubris. At the same time, spaceflight advocates have some untapped aspects to their utopian arguments that would greatly strengthen their position should they effectively articulate them. C1 Smithsonian Inst, Div Space Hist, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Div Space Hist, POB 37012,NASM Room 3550,MRC 311, Washington, DC 20013 USA. EM launiusr@nasm.si.edu NR 64 TC 6 Z9 6 U1 1 U2 3 PU BRITISH INTERPLANETARY SOC PI LONDON PA 27-29 S LAMBETH RD, LONDON SW8 1SZ, ENGLAND SN 0007-084X J9 JBIS-J BRIT INTERPLA JI JBIS-J. Br. Interplanet. Soc. PD SEP-OCT PY 2003 VL 56 IS 9-10 BP 338 EP 349 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Engineering; Astronomy & Astrophysics; Geology GA 761XP UT WOS:000187941000006 ER PT J AU Altshuler, DL Dudley, R AF Altshuler, DL Dudley, R TI Kinematics of hovering hummingbird flight along simulated and natural elevational gradients SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE air density; elevation; flight; hummingbird; hyperoxia; hypoxia; kinematics; load lifting; oxygen concentration; wingbeat frequency; stroke amplitude ID INDEPENDENT CONTRASTS; GAS-MIXTURES; PERFORMANCE; HELIOX; ENERGETICS; LIMITS; HEART AB Hovering flight is one of the most energetically demanding forms of animal locomotion. Despite the cost, hummingbirds regularly hover at high elevations, where flight is doubly challenging because of reduced air density and oxygen availability. We performed three laboratory experiments to examine how air density and oxygen partial pressure influence wingbeat kinematics. In the first study, we experimentally lowered air density but maintained constant oxygen partial pressure. Under these hypodense but normoxic conditions, hummingbirds increased stroke amplitude substantially and increased wingbeat frequency slightly. In the second experiment, we maintained constant air density but decreased oxygen partial pressure. Under these normodense but hypoxic conditions, hummingbirds did not alter stroke amplitude but instead reduced wingbeat frequency until they could no longer generate enough vertical force to offset body weight. In a final combined experiment, we decreased air density but increased oxygen availability, and found that the wingbeat kinematics were unaffected by supplemental oxygen. We also studied hovering and maximally loaded flight performance for 43 hummingbird species distributed along a natural elevational gradient in Peru. During free hovering flight, hummingbirds showed increased stroke amplitude interspecifically at higher elevations, mirroring the intra-individual responses in our first laboratory experiment. During loaded flight, hummingbirds increased both wingbeat frequency and wing stroke amplitude by 19% relative to free-flight values at any given elevation. We conclude that modulation of wing stroke amplitude is a major compensatory mechanism for flight in hypodense or hypobaric environments. By contrast, increases in wingbeat frequency impose substantial metabolic demands, are only elicited transiently and anaerobically, and cannot be used to generate additional sustained lift at high elevations. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Altshuler, DL (reprint author), CALTECH, Mail Code 138-78,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM doug@caltech.edu OI Altshuler, Douglas/0000-0002-1364-3617 NR 22 TC 48 Z9 48 U1 1 U2 22 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 SEP PY 2003 VL 206 IS 18 BP 3139 EP + DI 10.1242/jeb.00540 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 755FR UT WOS:000187393300007 PM 12909695 ER PT J AU Dominy, NJ Lucas, PW Wright, SJ AF Dominy, NJ Lucas, PW Wright, SJ TI Mechanics and chemistry of rain forest leaves: canopy and understorey compared SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Article; Proceedings Paper CT 5th International Workshop in Field Techniques for Environmental Physiology CY MAR 16-22, 2003 CL TENERITE, SPAIN DE Barro Colorado island; canopy crane; fracture toughness; herbivory; Panama ID LEAF OPTICAL-PROPERTIES; EXTREME-SHADE PLANTS; FRACTURE-TOUGHNESS; DYE-BINDING; HERBIVORY; PROTEIN; TREES; DEFENSES; VISION; ASSAY AB Despite the potential for changes during transit or preservation, the physicochemical properties of leaves are typically measured in a laboratory setting. A suite of laboratory methods adapted for use in the field is described here. The equipment is portable and operable in remote environments. Each technique has been validated against laboratory standards and has been tested throughout the tropics in a variety of ecological contexts. The properties of canopy and understorey leaves from Central Panama are reported here. The results show clear differences between leaves growing in different light regimes. Canopy leaves are tougher and possess greater concentrations of protein, phenols, and tannins. The implication of these results to the resource availability hypothesis, which proposes trade-offs between physiology and defences against herbivory, is discussed. C1 Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA. Univ Hong Kong, Dept Anat, Hong Kong, Hong Kong, Peoples R China. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Dominy, NJ (reprint author), Univ Chicago, Dept Ecol & Evolut, 1101 E 57th St, Chicago, IL 60637 USA. RI Wright, Stuart/M-3311-2013; OI Wright, Stuart/0000-0003-4260-5676; Dominy, Nathaniel/0000-0001-5916-418X NR 46 TC 46 Z9 46 U1 1 U2 10 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 SEP PY 2003 VL 54 IS 390 BP 2007 EP 2014 DI 10.1093/jxb/erg224 PG 8 WC Plant Sciences SC Plant Sciences GA 717AU UT WOS:000185064100002 PM 12867549 ER PT J AU Lee, V Gu, XM Hou, YL AF Lee, V Gu, XM Hou, YL TI The treatment of Chinese ancestor portraits: An introduction to Chinese painting conservation techniques SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article AB In 1991, the Arthur M. Sackler Gallery, Smithsonian Institution, acquired a collection of 83 Chinese ancestor portraits in the format of hanging scrolls. The museum decided to make 34 of the scrolls the subject of an exhibition called Worshiping the Ancestors: Chinese Conuneinorative Portraits, which opened in the summer of 2001. The condition of the paintings was evaluated, and it was determined that some paintings required a complete remounting while others required minimal stabilization. In this article, some specifics of Chinese painting conservation will be discussed, and a complete remounting process will be thoroughly described. It is our hope that this article will provide a better understanding of Chinese painting conservation while making its techniques more familiar to Western conservators. C1 Smithsonian Inst, Freer Gallery Art & Arthur M Sackler Gallery, Washington, DC 20560 USA. RP Lee, V (reprint author), Smithsonian Inst, Freer Gallery Art & Arthur M Sackler Gallery, Washington, DC 20560 USA. NR 17 TC 2 Z9 2 U1 0 U2 6 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 2003 VL 42 IS 3 BP 463 EP + DI 10.2307/3179868 PG 20 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 988JU UT WOS:000233591700009 ER PT J AU Henson, PM AF Henson, PM TI 'What holds the earth together': Agnes Chase and American agrostology SO JOURNAL OF THE HISTORY OF BIOLOGY LA English DT Article DE botany; Agnes Chase; fieldwork; Latin America; research schools; women in science ID SCIENCE; WOMEN; HISTORY AB Geison's model of a research school is applied to the case of Agnes Chase ( 1869 - 1963), agrostologist at the Bureau of Plant Industry, United States Department of Agriculture, and curator, U. S. National Herbarium, Smithsonian Institution. Chase developed a geographically dispersed research school in systematic agrostology across the Americas in the first half of the twentieth century. Despite her gender- based lack of institutional power, Chase used her scientific expertise, mentoring skills, and relationships based on women's groups to develop a cohesive school of grass specialists focused on her research program to collect, observe, describe, identify, and classify the grasses of the Americas. Geison's model is extended to encompass geographically dispersed schools led by a non- university based mentor without institutional power. C1 Smithsonian Inst Archives, Inst Hist Div, Washington, DC 20560 USA. RP Henson, PM (reprint author), Smithsonian Inst Archives, Inst Hist Div, Washington, DC 20560 USA. NR 67 TC 2 Z9 3 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0022-5010 J9 J HIST BIOL JI J. Hist. Biol. PD FAL PY 2003 VL 36 IS 3 BP 437 EP 460 DI 10.1023/B:HIST.0000004568.11609.2d PG 24 WC Biology; History & Philosophy Of Science SC Life Sciences & Biomedicine - Other Topics; History & Philosophy of Science GA 744ZA UT WOS:000186661700001 ER PT J AU Ollivet-Courtois, F Lecu, A Yates, RA Spelman, LH AF Ollivet-Courtois, F Lecu, A Yates, RA Spelman, LH TI Treatment of a sole abscess in an Asian elephant (Elephas maximus) using regional digital intravenous perfusion SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Asian elephant; Elephas maximus; sole; abscess; regional digital intravenous perfusion ID LOXODONTA-AFRICANA; LIMB; ANTIBIOTICS AB Regional digital i.v. perfusion was used to treat a severe sole abscess associated with a wire foreign body in a 19-yr-old female Asian elephant (Elephas maximus) housed at the Paris Zoo. The cow presented with acute right forelimb lameness and swelling that persisted despite 4 days of anti-inflammatory therapy. Under anesthesia, a 10- X 0.5- X 0.5-cm wire was extracted from the sole of the right foot. There was a 2-cm-deep, 7-cm-diameter abscess pocket that was subsequently debrided. Regional digital i.v. perfusion was performed and repeated 15 days later, using cefoxitin and gentamicin on both occasions. Between treatments, the cow received trimethoprim-sulfamethoxazole and phenylbutazone orally. Within 2 days of administering anesthesia and the first perfusion treatment, the lameness improved dramatically. When phenylbutazone was discontinued 1 wk after the first treatment, the lameness had completely resolved. At the second treatment, there was no evidence of further soft tissue infection, and the abscess pocket had resolved. C1 Museum Natl Hist Nat, F-75012 Paris, France. Smithsonian Natl Zool Pk, Washington, DC 20016 USA. RP Ollivet-Courtois, F (reprint author), Museum Natl Hist Nat, Parc Zool Paris,53 Ave St Maurice, F-75012 Paris, France. NR 13 TC 3 Z9 4 U1 1 U2 2 PU AMER ASSOC ZOO VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD SEP PY 2003 VL 34 IS 3 BP 292 EP 295 DI 10.1638/01-103 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA 729EL UT WOS:000185759600012 PM 14582794 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The Burlington magazine: A centenary anthology. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Kalfatovic, MR (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 SEP 1 PY 2003 VL 128 IS 14 BP 161 EP 161 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 716ZR UT WOS:000185060900068 ER PT J AU Ortega, J Maldonado, JE Wilkinson, GS Arita, HT Fleischer, RC AF Ortega, J Maldonado, JE Wilkinson, GS Arita, HT Fleischer, RC TI Male dominance, paternity, and relatedness in the Jamaican fruit-eating bat (Artibeus jamaicensis) SO MOLECULAR ECOLOGY LA English DT Article DE Artibeus jamaicensis; genetic structure; male dominance; microsatellites; paternity; relatedness ID COMMON VAMPIRE BAT; PHYLLOSTOMUS-HASTATUS; SOCIAL-ORGANIZATION; POLYGYNOUS BAT; GENETIC CONSEQUENCES; CYNOPTERUS SPHINX; PLECOTUS-AURITUS; MATING SYSTEMS; CHIROPTERA; MITOCHONDRIAL AB We analysed variation at 14 nuclear microsatellite loci to assess the genetic structure, relatedness, and paternity of polygynous Jamaican fruit-eating bats. A total of 84 adults captured in two caves exhibited little genetic differentiation between caves (F-ST = 0.008). Average relatedness among adult females in 10 harem groups was very low (R = 0.014 +/- 0.011), providing no evidence of harem structure. Dominant and subordinate males shared paternity in large groups, while dominant and satellite males shared paternity in smaller groups. However, our results suggest that male rank influences paternity. Dominant males fathered 69% of 40 offspring, followed by satellite (22%) and subordinate males (9%). Overall adult male bats are not closely related, however, in large harem groups we found that subordinate and dominant males exhibited relatedness values consistent with a father-offspring relationship. Because dominant and subordinate males also sired all the pups in large groups, we propose that their association provides inclusive fitness to them. C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. Univ Maryland, Dept Biol, College Pk, MD 20742 USA. Univ Nacl Autonoma Mexico, Inst Ecol, Mexico City 04510, DF, Mexico. RP Ortega, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Genet Program, 3001 Connecticut Ave, Washington, DC 20008 USA. RI Wilkinson, Gerald/E-4424-2011; ARITA, HECTOR/I-6161-2012 OI Wilkinson, Gerald/0000-0001-7799-8444; NR 42 TC 49 Z9 53 U1 0 U2 11 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 SEP PY 2003 VL 12 IS 9 BP 2409 EP 2415 DI 10.1046/j.1365-294X.2003.01924.x PG 7 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 720HZ UT WOS:000185256500011 PM 12919478 ER PT J AU Ascunce, MS Cortes-Ortiz, L Mudry, MD AF Ascunce, MS Cortes-Ortiz, L Mudry, MD TI The mitochondrial control region of the black howler monkey, Alouatta caraya (Primates, Platyrrhini), and the development of new primers SO MOLECULAR ECOLOGY NOTES LA English DT Article DE D-loop; howler monkeys; mitochondrial DNA; platyrrhines; population genetics; specific primers ID DNA; EVOLUTION; PATTERN AB The analysis of polymorphic genetic markers is necessary to assess the genetic variability of natural populations in order to develop effective conservation strategies. However, the molecular genetic variability of most neotropical primates is not well known. Therefore, we describe 13 primers for the amplification and sequencing of the mitochondrial control region that were developed for Alouatta caraya. Six of these primers gave unique bands on four other platyrrhine species (Alouatta palliata, Ateles paniscus, Ateles belzebuth and Saimiri boliviensis) showing their utility for control region amplification and sequencing in these platyrrhine species. C1 Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Ecol Genet & Evoluc, GIBE, RA-1428 Buenos Aires, DF, Argentina. Smithsonian Trop Res Inst, NAOS Marine Labs, Isla Naos, Calzada Amador, Panama. RP Ascunce, MS (reprint author), Univ Florida, Dept Anthropol, 1112 Turlington Hall,POB 117305, Gainesville, FL 32611 USA. NR 12 TC 3 Z9 5 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 2003 VL 3 IS 3 BP 372 EP 375 DI 10.1046/j.1471-8286.2003.00454.x PG 4 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 719VG UT WOS:000185225300015 ER PT J AU Jones, FA Hubbell, SP AF Jones, FA Hubbell, SP TI Isolation and characterization of microsatellite loci in the tropical tree Jacaranda copaia (Bignoniaceae) SO MOLECULAR ECOLOGY NOTES LA English DT Article DE Jacaranda copaia; microsatellite; Panama; paternity and maternity analysis; tropical tree ID SEED DISPERSAL; FOREST AB We isolated 10 microsatellite loci for jacaranda copaia for direct measurement of seed and pollen movement within the 50 ha Forest Dynamics Plot on Barro Colorado Island, Panama, and for studies of population genetic structure and gene flow across the Isthmus of Panama. Enriched repeat libraries were screened for microsatellite repeats and polymorphic primer pairs were developed. A total of 110 adult individuals were screened for allelic diversity and loci showed high levels of heterozygosity. These loci show both high maternal and paternal exclusion probabilities. C1 Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Jones, FA (reprint author), Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. RI Jones, Andy/C-3460-2009 NR 11 TC 11 Z9 11 U1 0 U2 1 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 2003 VL 3 IS 3 BP 403 EP 405 DI 10.1046/j.1471-8286.2003.00465.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 719VG UT WOS:000185225300025 ER PT J AU Humphrey, PJ Fabbiano, G Elvis, M Church, MJ Balucinska-Church, M AF Humphrey, PJ Fabbiano, G Elvis, M Church, MJ Balucinska-Church, M TI Ultraluminous X-ray source populations in normal galaxies: a preliminary survey with Chandra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; binaries : close; X-rays : galaxies; X-rays : stars ID ELLIPTIC GALAXY; NEARBY GALAXIES; GLOBULAR-CLUSTERS; BLACK-HOLES; MASS; NGC-4697; STARBURST; BINARIES; COMPACT; PERFORMANCE AB We present results of a Chandra survey of the ultraluminous X-ray sources (ULX) in 13 normal galaxies, in which we combine source detection with X-ray flux measurement. 22 ULX were detected, i.e. with L-x > 1 x 10(39) erg s(-1) (L-10) and 39 other sources were detected with L-x > 5 x 10(38) erg s(-1) (L-5). We also use radial intensity profiles to remove extended sources from the sample. The majority of sources are not extended, which for a typical distance constrains the emission region size to less than 50 pc. X-ray colour-colour diagrams and spectral fitting results were examined for indicators of the ULX nature. In the case of the brighter sources, spectral fitting generally requires two-component models. In only a few cases do colour-colour diagrams or spectral fitting provide evidence of a black hole nature. We find no evidence of a correlation with stellar mass, however, there is a strong correlation with star formation as indicated by the 60-mum flux as found in previous studies. C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. RP Humphrey, PJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. NR 60 TC 32 Z9 32 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 PY 2003 VL 344 IS 1 BP 134 EP 148 DI 10.1046/j.1365-8711.2003.06802.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KZ UT WOS:000185088800017 ER PT J AU Jonker, PG Nelemans, G Wang, Z Kong, AKH Chakrabarty, D Garcia, M Groot, PJ van der Klis, M Kerr, T Mobasher, B Sullivan, M Augusteijn, T Stappers, BW Challis, P Kirshner, RP Hjorth, J Delsanti, A AF Jonker, PG Nelemans, G Wang, Z Kong, AKH Chakrabarty, D Garcia, M Groot, PJ van der Klis, M Kerr, T Mobasher, B Sullivan, M Augusteijn, T Stappers, BW Challis, P Kirshner, RP Hjorth, J Delsanti, A TI A search for the optical and near-infrared counterpart of the accreting millisecond X-ray pulsar XTE J1751-305 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : individual : XTE J1751-305; stars : neutron; X-rays : stars ID LOW-MASS; BINARIES; DISCOVERY; PERIOD; STARS AB We have obtained optical and near-infrared images of the field of the accreting millisecond X-ray pulsar XTE J1751-305. There are no stars in the 0.7-arcsec error circle (0.7 arcsec is the overall uncertainty arising from tying the optical and X-ray images and from the intrinsic uncertainty in the Chandra X-ray astrometric solution). We derive limiting magnitudes for the counterpart of R > 23.1, I > 21.6, Z > 20.6, J > 19.6 and K > 19.2. We compare these upper limits with the magnitudes one would expect for simple models for the possible donor stars and the accretion disc subject to the reddening observed in X-rays for XTE J1751-305 and when put at the distance of the Galactic Centre (8.5 kpc). We conclude that our non-detection does not constrain any of the models for the accretion disc or possible donor stars. Deep, near-infrared images obtained during quiescence will, however, constrain possible models for the donor stars in this ultracompact system. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nijmegen, Dept Astrophys, Nijmegen, Netherlands. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Joint Astron Ctr, Hilo, HI 96720 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Durham, Dept Phys, Sci Labs, Durham DH1 3LE, England. Nord Opt Telescope, Santa Cruz De La Palma 38700, Canary Islands, Spain. Univ Copenhagen, Astron Observ, DK-2100 Copenhagen O, Denmark. European So Observ, Santiago 19, Chile. RP Jonker, PG (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RI Nelemans, Gijs/D-3177-2012; Hjorth, Jens/M-5787-2014; Groot, Paul/K-4391-2016; OI Nelemans, Gijs/0000-0002-0752-2974; Hjorth, Jens/0000-0002-4571-2306; Groot, Paul/0000-0002-4488-726X; Sullivan, Mark/0000-0001-9053-4820 NR 26 TC 9 Z9 9 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 PY 2003 VL 344 IS 1 BP 201 EP 206 DI 10.1046/j.1365-8711.2003.06814.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 717KZ UT WOS:000185088800024 ER PT J AU Flannery, MR Vrinceanu, D AF Flannery, MR Vrinceanu, D TI Quantal and classical radiative cascade in Rydberg plasmas SO PHYSICAL REVIEW A LA English DT Article ID ATOMS; LIFETIME AB Atoms in high-(n,l) states formed in cold Rydberg plasmas decay to the ground state in a succession of radiative transitions populating intermediate excited states. A classical treatment presents radiative cascade in a physically transparent way and reveals the "trajectory" in nl space obeyed by the cascade, scaling rules, and other aspects hidden within the quantal approach. Quantal-classical correspondence in radiative decay is directly demonstrated. Classical transition probabilities are also presented and are in excellent agreement with quantal transition probabilities, even for moderate quantum numbers. C1 Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. NR 18 TC 26 Z9 27 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD SEP PY 2003 VL 68 IS 3 AR 030502 DI 10.1103/PhysRevA.68.030502 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 728KQ UT WOS:000185716700002 ER PT J AU Gorenstein, P Tananbaum, H AF Gorenstein, P Tananbaum, H TI Leon Van Speybroeck - Obituary SO PHYSICS TODAY LA English DT Biographical-Item C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gorenstein, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 1 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 0031-9228 J9 PHYS TODAY JI Phys. Today PD SEP PY 2003 VL 56 IS 9 BP 78 EP 79 DI 10.1063/1.1620845 PG 2 WC Physics, Multidisciplinary SC Physics GA 716MF UT WOS:000185032200034 ER PT J AU Bedini, SA AF Bedini, SA TI Brooke Hindle - 28 September 1918 3 June 2001 SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Bedini, SA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 USA SN 0003-049X J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD SEP PY 2003 VL 147 IS 3 BP 281 EP 285 PG 5 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 730YV UT WOS:000185858500007 PM 14606492 ER PT J AU Challinor, D AF Challinor, D TI S. Dillon Ripley - 20 September 1913 12 March 2001 SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20560 USA. RP Challinor, D (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 USA SN 0003-049X J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD SEP PY 2003 VL 147 IS 3 BP 297 EP 302 PG 6 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 730YV UT WOS:000185858500010 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. II. Detection and characterization of planetary systems SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Review ID 47 URSAE-MAJORIS; UPSILON-ANDROMEDAE; HABITABLE ZONES; RADIAL-VELOCITY; OUTER PLANETS; V-ANDROMEDAE; SUBSTELLAR COMPANIONS; PROTOPLANETARY DISKS; EXOPLANETARY SYSTEMS; TERRESTRIAL PLANETS AB We utilize (1) detailed end-to-end numerical simulations of sample narrow-angle astrometric observing campaigns with the Space Interferometry Mission (SIM) and the subsequent data analysis process and (2) the set of extrasolar planetary systems discovered so far by radial velocity surveys as templates to provide meaningful estimates of the limiting capabilities of SIM for the detection and measurement of multiple-planet systems around solar-type stars in the solar neighborhood. We employ standard chi(2) statistics, periodograms, and Fourier analysis to evaluate SIM's ability to detect multiple planetary signatures; the probability of detecting additional companions is essentially unchanged from the single-planet configurations, but after fitting and subtraction of orbits with astrometric signal-to-noise ratio, alpha/sigma(d) --> 1, the false detection rates can be enhanced by up to a factor of 2. The periodogram approach results in robust multiple-planet detection for systems with periods shorter than the SIM mission length, even at low values of alpha/sigma(d), while the least-squares technique combined with Fourier series expansions is arguably preferable in the long-period regime. We explore the three-dimensional parameter space defined by astrometric signature, orbital period, and eccentricity to derive general conclusions on the capability of SIM to accurately measure the full set of orbital parameters and masses for a variety of configurations of planetary systems; the accuracy of multiple-planet orbit reconstruction and mass determination suffers a typical degradation of 30%-40% from single-planet solutions; mass and orbital inclination can be measured to better than 10% for periods as short as 0.1 yr and for alpha/sigma(d) as low as similar to5, while alpha/sigma(d) similar or equal to 100 is required in order to measure with similar accuracy systems harboring objects with periods as long as 3 times the mission duration. We gauge the potential of SIM for meaningful coplanarity measurements via determination of the true geometry of multiple-planet orbits. For systems with all components producing alpha/sigma(d) similar or equal to 10 or greater, quasi-coplanarity can be reliably established with uncertainties of a few degrees, for periods in the range 0.1 yr less than or similar to T less than or equal to 15 yr; in systems where at least one component has alpha/sigma(d) --> 1, coplanarity measurements are compromised, with typical uncertainties on the mutual inclinations on the order of 30degrees-40degrees. We quantify the improvement derived in full-orbit reconstruction and planet mass determination by constraining the multiple-planet orbital fits to SIM observations with the nominal orbital elements obtained from the radial velocity measurements; the uncertainties on orbital elements and masses can be reduced by up to an order of magnitude, especially for long-period orbits in face-on configurations and for low-amplitude orbits seen edge-on. Our findings are illustrative of the importance of the contribution SIM will make, complementing other ongoing and planned spectroscopic, astrometric, and photometric surveys, in order to fulfill the expectations for ground-breaking science in the fields of formation and evolution of planetary systems during the next decade. 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. OI Sozzetti, Alessandro/0000-0002-7504-365X; Lattanzi, Mario Gilberto/0000-0003-0429-7748 NR 102 TC 17 Z9 17 U1 1 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 SEP PY 2003 VL 115 IS 811 BP 1072 EP 1104 DI 10.1086/376872 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 714GA UT WOS:000184902900005 ER PT J AU Vrtilek, SD Raymond, JC Boroson, B McCray, R Smale, A Kallman, T Nagase, F AF Vrtilek, SD Raymond, JC Boroson, B McCray, R Smale, A Kallman, T Nagase, F TI Simultaneous ASCA and Hubble Space Telescope GHRS observations of Cygnus X-2/V1341 Cygni SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID X-RAY BINARIES; MULTIWAVELENGTH CAMPAIGN; EMISSION-LINES; X-2; SPECTRUM; IUE; HERCULES-X-1; SPECTROMETER; SCORPIUS-X-1; PERIODICITY AB We present results from ultraviolet and X-ray observations of the low-mass X-ray binary Cygnus X-2. The simultaneous Hubble Space Telescope/GHRS and ASCA observations took place during the low state of an 82 day cycle. We compare our observations as well as archival IUE and RXTE data with models that predict ultraviolet and optical continuum emission from an X-ray-heated disk and a Roche lobe-filling star. The model predictions are consistent with observed optical, ultraviolet, and X-ray variations over both orbital and long-term periods. The X-ray spectral state, the luminosities implied by fits to the X-ray data, the ultraviolet continuum and line fluxes, and the mass accretion rates obtained from fits to the ultraviolet continuum are consistent with location of our observations on the normal and horizontal branches of the Z-shaped X-ray color- color diagram. A combination of changes to mass accretion rate and obstruction by a warped disk can be invoked as a possible explanation for the motion of the "Z" in the color- color plane. The GHRS/G160M measurements concentrated on N v (lambda1238.8; lambda1242.8) and He II (lambda1640.5). The low-resolution (GHRS/G140L) observations captured Si IV (lambda1393.8; lambda1402.8), N IVv (lambda1486.5), and C IV (lambda1548); absorption lines detected in the spectra are interstellar. Although the relative line fluxes are consistent with emission from an X-ray-heated accretion disk corona, predictions from models of line emission from simple disks do not fit the observed emission-line profiles. The lack of double peaks suggests that most of the line emission is from the surface of the companion and the radial velocities (80-130 km s(-1)) are consistent with emission from the optical star at the orbital phase (0.70-0.74) of our observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Cambridge, MA 02138 USA. Univ Colorado, JILA, Boulder, CO 80309 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20177 USA. Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. RP Vrtilek, SD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 11 Z9 11 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 2003 VL 115 IS 811 BP 1124 EP 1134 DI 10.1086/377089 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 714GA UT WOS:000184902900008 ER PT J AU Early, J AF Early, J TI TransAfrica: An interview with Bill Fletcher Jr. SO RADICAL HISTORY REVIEW LA English DT Editorial Material C1 Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. RP Early, J (reprint author), Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU DUKE UNIV PRESS PI DURHAM PA 905 W MAIN ST, STE 18-B, DURHAM, NC 27701 USA SN 0163-6545 J9 RADICAL HIST REV JI Radic. Hist. Rev. PD FAL PY 2003 IS 87 BP 127 EP 137 PG 11 WC History SC History GA 733UW UT WOS:000186019900008 ER PT J AU Ralls, K White, PJ AF Ralls, K White, PJ TI Diurnal spacing patterns in kit foxes, a monogamous canid SO SOUTHWESTERN NATURALIST LA English DT Article ID DIK-DIK; COYOTE; PREY AB Kit foxes (Vulpes macrotis) are socially monogamous and live in male-female pairs or small family groups. These small desert foxes are nocturnal and spend the day in an underground den. Mated pairs often shared the same den on the same day. However, on days when they did not share the same den, mated pairs did not occupy dens that were closer together (or farther apart) than expected by chance. Closely related foxes on adjacent home ranges also occasionally shared dens. However, foxes living on adjacent home ranges, even when closely related, also did not occupy dens that were closer together or farther apart than expected by chance. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Yellowstone Ctr Resources, Yellowstone Natl Pk, WY 82190 USA. RP Ralls, K (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. NR 17 TC 3 Z9 3 U1 0 U2 3 PU SOUTHWESTERN ASSN NATURALISTS PI SAN MARCOS PA SOUTHWEST TEXAS STATE UNIV, DEPT BIOLOGY, 601 UNIVERSITY DR, SAN MARCOS, TX 78666 USA SN 0038-4909 J9 SOUTHWEST NAT JI Southw. Natural. PD SEP PY 2003 VL 48 IS 3 BP 432 EP 436 DI 10.1894/0038-4909(2003)048<0432:DSPIKF>2.0.CO;2 PG 5 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 724DJ UT WOS:000185471600014 ER PT J AU Eberhard, WG Cordero, C AF Eberhard, WG Cordero, C TI Sexual conflict and female choice SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter ID BENEFITS C1 Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, Costa Rica. Univ Costa Rica, Escuela Biol, Ciudad Univ, Costa Rica. Univ Nacl Autonoma Mexico, Inst Ecol, Mexico City 04510, DF, Mexico. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, Costa Rica. NR 11 TC 48 Z9 49 U1 1 U2 32 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD SEP PY 2003 VL 18 IS 9 BP 438 EP 439 DI 10.1016/S0169-5347(03)00180-0 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 721HW UT WOS:000185311800004 ER PT J AU Ellis, HI Jehl, JR AF Ellis, HI Jehl, JR TI Temperature regulation and the constraints of climate in the Eared Grebe SO WATERBIRDS LA English DT Article DE Eared Grebe; Black-Necked Grebe; temperature regulation; BMR; thermal conductance; climate; distribution; Podiceps nigricollis ID PODICEPS-NIGRICOLLIS; THERMAL CONDUCTANCE; METABOLIC-RATE; MIGRATION; MOLT; BIRDS; COST AB Eared Grebes (Podiceps nigricollis) encounter a variety of climatic regimes in their annual cycle. The most dramatic occur while on staging areas in autumn. We investigated the thermoregulatory abilities of the Eared Grebe to determine how they coped with these climate changes during staging. The basal metabolic rate (BMR) was higher than predicted. Mass-specific BMR was 1.212 mL O-2/g(.)h for birds averaging 317 g. The thermoneutral zone is wide and extended from 15degreesC to 38degreesC. Minimal thermal conductance and average body temperature were not unusual. We conclude that Eared Grebes live most of the year under thermoneutral conditions and that food availability, not temperature extremes, determines the timing of their winter migration. C1 Univ San Diego, Dept Biol, San Diego, CA 92110 USA. Univ San Diego, Marine & Environm Studies Program, San Diego, CA 92110 USA. Smithsonian Inst, US Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. RP Ellis, HI (reprint author), Univ San Diego, Dept Biol, San Diego, CA 92110 USA. NR 20 TC 5 Z9 5 U1 2 U2 9 PU WATERBIRD SOC PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 1524-4695 J9 WATERBIRDS JI Waterbirds PD SEP PY 2003 VL 26 IS 3 BP 275 EP 279 DI 10.1675/1524-4695(2003)026[0275:TRATCO]2.0.CO;2 PG 5 WC Ornithology SC Zoology GA 731DK UT WOS:000185869100004 ER PT J AU Launius, RD AF Launius, RD TI Bound for Santa Fe: The road to New Mexico and the American conquest, 1806-1848. SO WESTERN HISTORICAL QUARTERLY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU WESTERN HISTORY ASSOCIATION PI LOGAN PA UTAH STATE UNIV, UMC 0740, LOGAN, UT 84322 USA SN 0043-3810 J9 WESTERN HIST QUART JI West. Hist. Q. PD FAL PY 2003 VL 34 IS 3 BP 382 EP 383 PG 2 WC History SC History GA 717RY UT WOS:000185105200028 ER PT J AU Whigham, DF Jordan, TE AF Whigham, DF Jordan, TE TI Isolated wetlands and water quality SO WETLANDS LA English DT Article DE isolated wetlands; water quality; nutrients; hydrology; depressional wetlands; slope wetlands; playas; prairie potholes; Carolina bays; cypress swamps; mineral flats; organic flats ID PRAIRIE-POTHOLE WETLANDS; NORTH-DAKOTA; GROUND-WATER; PINHOOK BOG; NEW-YORK; CHEMISTRY; HYDROLOGY; CAROLINA; MICHIGAN; PEATLAND AB Isolated wetlands occur in many hydrogeomorphic settings, and while they appear to be physically isolated from other water bodies, they are almost never completely decoupled from surface-water or groundwater systems. In this paper, we examine water-quality data for isolated wetlands in three hydrogeomorphic classes (depressions, slopes, flats). Some isolated wetlands are dominated by atmospheric exchanges and have little ground-water or surface-water connections with adjacent systems. Other isolated wetlands are dominated by ground-water inputs and have intermittent or continuous hydrologic connections to adjacent systems. Water-quality characteristics of isolated wetlands are highly variable and depend primarily on the sources of water, substrate characteristics, and land uses associated with the wetland watershed. We were unable to identify any general pattern of water-quality characteristics within or between isolated wetlands in the three hydrogeomorphic classes. Alteration of hydrologic conditions (e.g., ditching, filling), however, usually results in increased nutrient export to downstream systems. From a water-quality perspective, we conclude that so-called isolated wetlands are rarely isolated, and isolation is a term that is not very useful from an ecosystem perspective. Isolated wetlands are nutrient sinks and, because most are hydrologically connected to other waters and wetlands, the loss of isolated wetlands would potentially have negative impacts on the water quality of downstream systems. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Whigham, DF (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM whighamd@si.edu RI Gebauer, Radek/G-6749-2015; OI Whigham, Dennis/0000-0003-1488-820X NR 78 TC 58 Z9 60 U1 3 U2 54 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 J9 WETLANDS JI Wetlands PD SEP PY 2003 VL 23 IS 3 BP 541 EP 549 DI 10.1672/0277-5212(2003)023[0541:IWAWQ]2.0.CO;2 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 730CR UT WOS:000185812100006 ER PT J AU Olshanii, M Dunjko, V AF Olshanii, M Dunjko, V TI Short-distance correlation properties of the Lieb-Liniger system and momentum distributions of trapped one-dimensional atomic gases SO PHYSICAL REVIEW LETTERS LA English DT Article ID IMPENETRABLE BOSONS; BOSE-GAS; DENSITY-MATRIX; QUANTUM FLUIDS; GROUND STATE; TEMPERATURE; CONFINEMENT; MODELS; TIME AB We derive exact closed-form expressions for the first few terms of the short-distance Taylor expansion of the one-body correlation function of the Lieb-Liniger gas. As an intermediate result, we obtain the high-p asymptotics of the momentum distribution of both free and harmonically trapped atoms and show that it obeys a universal 1/p(4) law for all values of the interaction strength. We discuss the ways to observe the predicted momentum distributions experimentally, regarding them as a sensitive identifier for the Tonks-Girardeau regime of strong correlations. C1 Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. EM olshanii@physics.usc.edu RI Olshanii, Maxim/M-2830-2013 OI Olshanii, Maxim/0000-0003-3629-6002 NR 35 TC 100 Z9 100 U1 3 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 29 PY 2003 VL 91 IS 9 AR 090401 DI 10.1103/PhysRevLett.91.090401 PG 4 WC Physics, Multidisciplinary SC Physics GA 719ZJ UT WOS:000185235000001 PM 14525162 ER PT J AU Sorensen, AS Molmer, K AF Sorensen, AS Molmer, K TI Measurement induced entanglement and quantum computation with atoms in optical cavities SO PHYSICAL REVIEW LETTERS LA English DT Article ID DECOHERENCE; SCHEME AB We propose a method to prepare entangled states and implement quantum computation with atoms in optical cavities. The internal states of the atoms are entangled by a measurement of the phase of light transmitted through the cavity. By repeated measurements an entangled state is created with certainty, and this entanglement can be used to implement gates on qubits which are stored in different internal degrees of freedom of the atoms. This method, based on measurement induced dynamics, has a higher fidelity than schemes making use of controlled unitary dynamics. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Aarhus, Dept Phys & Astron, Danish Natl Res Fdn, Ctr Quantum Opt, DK-8000 Aarhus C, Denmark. RP Sorensen, AS (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Sorensen, Anders/L-1868-2013 OI Sorensen, Anders/0000-0003-1337-9163 NR 19 TC 66 Z9 66 U1 1 U2 6 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 29 PY 2003 VL 91 IS 9 AR 097905 DI 10.1103/PhysRevLett.91.097905 PG 4 WC Physics, Multidisciplinary SC Physics GA 719ZJ UT WOS:000185235000052 PM 14525213 ER PT J AU Kanzawa, H Sugita, T Nakajima, H Bodeker, GE Oelhaf, H Stowasser, M Wetzel, G Engel, A Schmidt, U Levin, I Toon, GC Sen, B Blavier, JF Aoki, S Nakazawa, T Jucks, KW Johnson, DG Traub, WA Camy-Peyret, C Payan, S Jeseck, P Murata, I Fukunishi, H von Konig, M Bremer, H Kullmann, H Park, JH Pan, LL Yokota, T Suzuki, M Shiotani, M Sasano, Y AF Kanzawa, H Sugita, T Nakajima, H Bodeker, GE Oelhaf, H Stowasser, M Wetzel, G Engel, A Schmidt, U Levin, I Toon, GC Sen, B Blavier, JF Aoki, S Nakazawa, T Jucks, KW Johnson, DG Traub, WA Camy-Peyret, C Payan, S Jeseck, P Murata, I Fukunishi, H von Konig, M Bremer, H Kullmann, H Park, JH Pan, LL Yokota, T Suzuki, M Shiotani, M Sasano, Y TI Validation and data characteristics of nitrous oxide and methane profiles observed by the Improved Limb Atmospheric Spectrometer (ILAS) and processed with the Version 5.20 algorithm SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE nitrous oxide; methane; polar stratosphere; validation; satellite sensor; Improved Limb Atmospheric Spectrometer (ILAS) ID TUNABLE DIODE-LASER; TRACE GAS OBSERVATIONS; POLAR VORTEX; LOWER STRATOSPHERE; HETERODYNE SPECTROMETER; RETRIEVAL ALGORITHM; POTENTIAL VORTICITY; UPPER TROPOSPHERE; CH4 MEASUREMENTS; ARCTIC VORTEX AB Vertical profiles of nitrous oxide and methane at high latitudes (57-72degreesN; 64-89degreesS) were observed by the Improved Limb Atmospheric Spectrometer (ILAS) solar occultation sensor aboard Advanced Earth Observing Satellite. These measurements were made continuously from November 1996 through June 1997 with some additional periods in September-October 1996. A validation study of the nitrous oxide and methane data processed with the Version 5.20 ILAS retrieval algorithm is presented in this paper. Comparisons are made with (1) nitrous oxide and methane obtained by the ILAS validation balloon campaigns at Kiruna, Sweden, and at Fairbanks, Alaska, in the Arctic; (2) nitrous oxide and methane by the Photochemistry of Ozone Loss in the Arctic Region in Summer aircraft campaign in the Arctic; (3) nitrous oxide by the ground-based spectroscopic measurements and by the aircraft-based remote sensing measurements in the Arctic; and (4) methane by satellite measurements of the Version 19 Halogen Occultation Experiment in the Arctic and Antarctic. Comparisons of ILAS nitrous oxide and methane with Upper Atmosphere Research Satellite Reference Atmosphere data are also made. The results of the comparisons and additional ILAS internal consistency analyses are as follows: (1) the uncertainty of ILAS nitrous oxide is better than 10% over 10-30 km in altitude, and is larger than 50% over 30-40 km, which is comparable to the expected total errors of the ILAS measurements; (2) the uncertainty of ILAS methane is better than 10% over 10-50 km, except for 15-30 km in winter with positive biases exceeding 20%, which is smaller than or comparable to the expected total errors of the ILAS measurements (the quality of ILAS methane in the polar lower stratosphere is better in summer than in winter). In summary, the characteristics of ILAS measurements, i.e., high sampling frequency in polar latitudes with high vertical resolution, along with the good quality of ILAS Version 5.20 nitrous oxide for 10-40 km and the good quality of ILAS Version 5.20 methane for 10-50 km except for 15-30 km in winter, make the ILAS nitrous oxide and methane data set valuable for scientific study of various polar stratospheric phenomena. C1 Natl Inst Environm Studies, Tsukuba, Ibaraki 3050053, Japan. Natl Inst Water & Atmospher Res, Lauder, New Zealand. Univ Karlsruhe, Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany. Univ Frankfurt, Inst Meteorol, D-60054 Frankfurt, Germany. Univ Heidelberg, Inst Umweltphys, D-69120 Heidelberg, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Tohoku Univ, Grad Sch Sci, Ctr Atmospher & Ocean Studies, Sendai, Miyagi 9808578, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Paris 06, CNRS, Lab Phys Mol & Applicat, F-75252 Paris 05, France. Tohoku Univ, Grad Sch Sci, Dept Geophys, Sendai, Miyagi 9808578, Japan. Univ Bremen, Inst Umweltphys, D-28359 Bremen, Germany. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Hokkaido Univ, Grad Sch Environm Earth Sci, Sapporo, Hokkaido 060, Japan. RP Kanzawa, H (reprint author), Nagoya Univ, Grad Sch Environm Studies, Dept Hydrospher Atmospher Sci, Div Earth & Environm Sci,Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan. EM kanzawa@ihas.nagoya-u.ac.jp; tsugita@nies.go.jp; hide@nies.go.jp; g.bodeker@niwa.co.nz; hermann.oelhaf@imk.fzk.de; markus.stowasser@imk.fzk.de; gerald.wetzel@imk.fzk.de; an.engel@meteor.uni-frankfurt.de; u.schmidt@meteor.uni-frankfurt.de; ingeborg.levin@iup.uni-heidelberg.de; aoki@mail.cc.tohoku.ac.jp; nakazawa@mail.cc.tohoku.ac.jp; kjucks@cfa.harvard.edu; d.g.johnson@larc.nasa.gov; wtraub@cfa.harvard.edu; murata@pat.geophys.tohoku.ac.jp; fuku@pat.geophys.tohoku.ac.jp; miriam@florian.physik.uni-bremen.de; bremer@florian.physik.uni-bremen.de; hkuell@uni-bremen.de; j.h.park@larc.nasa.gov; liwen@ucar.edu; yoko@nies.go.jp; suzuki@eorc.nasda.go.jp; shiotani@kurasc.kyoto-u.ac.jp; sasano@nies.go.jp RI Pan, Laura/A-9296-2008; Sasano, Yasuhiro/C-2927-2009; Wetzel, Gerald/A-7065-2013; Sinnhuber, Miriam/A-7252-2013; Oelhaf, Hermann/A-7895-2013; Engel, Andreas/E-3100-2014 OI Pan, Laura/0000-0001-7377-2114; Sasano, Yasuhiro/0000-0001-7470-5642; Engel, Andreas/0000-0003-0557-3935 NR 68 TC 20 Z9 20 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 28 PY 2003 VL 108 IS D16 AR 8003 DI 10.1029/2002JD002458 PG 35 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 720FV UT WOS:000185251500001 ER PT J AU Schippers, S Muller, A McLaughlin, BM Aguilar, A Cisneros, C Emmons, ED Gharaibeh, MF Phaneuf, RA AF Schippers, S Muller, A McLaughlin, BM Aguilar, A Cisneros, C Emmons, ED Gharaibeh, MF Phaneuf, RA TI Photoionization studies of the B+ valence shell: experiment and theory SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID CONFIGURATION INTERACTION; CROSS-SECTION; IONS AB We have investigated L-shell photoionization (PI) of IS ground-state and 3 p, metastable states of the Be-like ion, B+, in the photon energy range 22.4-31.3 eV, at an experimental energy resolution of 25 meV Absolute PI cross sections have been measured using a photon-ion merged-beams arrangement at the Advanced Light Source. Detailed calculations using the semi-relativistic Breit-Pauli R-matrix approach suggest a fraction of 29% of metastable ions in the primary beam of the experiment. Excellent agreement is observed between the theoretical predictions and the experimental high-resolution PI cross sections. The present results are compared with earlier experimental and theoretical work. The cross section for PI of B+ ground-state ions can be very well described by an analytic formula derived from quantum defect theory. C1 Univ Giessen, Inst Kernphys, D-35392 Giessen, Germany. Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Nevada, Dept Phys, Reno, NV 89557 USA. Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico. RP Univ Giessen, Inst Kernphys, D-35392 Giessen, Germany. EM Stefan.E.Schippers@strz.uni-giessen.de RI Schippers, Stefan/A-7786-2008; Muller, Alfred/A-3548-2009 OI Schippers, Stefan/0000-0002-6166-7138; Muller, Alfred/0000-0002-0030-6929 NR 31 TC 30 Z9 30 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD AUG 28 PY 2003 VL 36 IS 16 BP 3371 EP 3381 AR PII S0953-4075(03)63256-6 DI 10.1088/0953-4075/36/16/301 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 725KQ UT WOS:000185542700005 ER PT J AU Volkov, I Banavar, JR Hubbell, SP Maritan, A AF Volkov, I Banavar, JR Hubbell, SP Maritan, A TI Neutral theory and relative species abundance in ecology SO NATURE LA English DT Article ID SAMPLING THEORY; DIVERSITY; ALLELES AB The theory of island biogeography(1) asserts that an island or a local community approaches an equilibrium species richness as a result of the interplay between the immigration of species from the much larger metacommunity source area and local extinction of species on the island (local community). Hubbell(2) generalized this neutral theory to explore the expected steady-state distribution of relative species abundance (RSA) in the local community under restricted immigration. Here we present a theoretical framework for the unified neutral theory of biodiversity(2) and an analytical solution for the distribution of the RSA both in the metacommunity (Fisher's log series) and in the local community, where there are fewer rare species. Rare species are more extinction-prone, and once they go locally extinct, they take longer to re-immigrate than do common species. Contrary to recent assertions(3), we show that the analytical solution provides a better fit, with fewer free parameters, to the RSA distribution of tree species on Barro Colorado Island, Panama(4), than the lognormal distribution(5,6). C1 Penn State Univ, Dept Phys, University Pk, PA 16802 USA. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balboa, Panama. Scuola Int Super Studi Avanzati, SISSA, I-34014 Trieste, Italy. INFM, Trieste, Italy. Abdus Salam Int Ctr Theoret Phys, Trieste, Italy. RP Banavar, JR (reprint author), Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA. NR 28 TC 370 Z9 396 U1 20 U2 264 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 28 PY 2003 VL 424 IS 6952 BP 1035 EP 1037 DI 10.1038/nature01883 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 715QR UT WOS:000184984200038 PM 12944964 ER PT J AU Davis, JLD Metcalfe, WJ Hines, AH AF Davis, JLD Metcalfe, WJ Hines, AH TI Implications of a fluctuating fish predator guild on behavior, distribution, and abundance of a shared prey species: the grass shrimp Palaemonetes pugio SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE refuge; predator-prey interactions; Morone saxatilis; Fundulus heteroclitus ID CHESAPEAKE-BAY; SOUTH-CAROLINA; BLUE CRABS; COMMUNITIES; SUBESTUARY; POPULATION; RESPONSES; EVOLUTION; HABITAT; ECOLOGY AB In some systems, the identity of a prey species' dominant predator(s) may not be constant over time. In cases in which a prey species exhibits different responses to various predator species, such changes in predator identity may have population-wide consequences. Our goals were to determine (1) whether mortality of and refuge use by the grass shrimp, Palaemonetes pugio, were predator-specific, and (2) how effects of prey size and habitat interacted with predator type. Striped bass (Morone saxatilis) exerted twice as much predation pressure as mummichog (Fundulus heteroclitus), although not equally as great on large (female) and small (male) shrimp. Mummichog, which fed preferentially on large shrimp, forced a partitioning of habitat between the two shrimp size classes. In contrast, large and small shrimp occupied similar habitats when subjected to striped bass, which fed on both size classes equally. Refuge use of grass shrimp depended on predator type. In the presence of mummichog, which occupied shallower depths in the water column than striped bass, shrimp stayed deep and close to structural habitat. Striped bass, which were deeper, caused shrimp to move high in the water column away from structural habitat. When both predators were present, shrimp distribution was similar to that when only striped bass were present, striped bass predation rate was enhanced, and overall mortality was higher than with either predator alone. Results suggest that at times when mummichogs are the dominant predators, large (female) shrimp experience higher predation than small (male) shrimp and are physically separated from their potential mates. When striped bass are more abundant, male and female shrimp may share a similar, shallow, less structure-oriented distribution and be subjected to higher mortality. When both predators are present, mortality rates may be higher still. This predator-, size-, and habitat-specificity of grass shrimp behavior suggests significant population and distribution consequences of fluctuating predator guilds and fluctuating cover of structural habitats in the field. (C) 2003 Published by Elsevier B.V. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Davis, JLD (reprint author), Williams Coll Mystic Seaport, Marine Studies Program, POB 6000, Mystic, CT 06355 USA. NR 33 TC 17 Z9 17 U1 0 U2 13 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 AUG 26 PY 2003 VL 293 IS 1 BP 23 EP 40 DI 10.1016/S0022-0981(03)00122-9 PG 18 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 706XP UT WOS:000184480600002 ER PT J AU Gazzola, KE AF Gazzola, KE TI Letter from the publisher SO AVIATION WEEK & SPACE TECHNOLOGY LA English DT News Item C1 Smithsonian Air & Space Museum, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MCGRAW HILL INC PI NEW YORK PA 1221 AVENUE OF THE AMERICAS, NEW YORK, NY 10020 USA SN 0005-2175 J9 AVIAT WEEK SPACE TEC JI Aviat. Week Space Technol. PD AUG 25 PY 2003 VL 159 IS 8 BP 32 EP 32 PG 1 WC Engineering, Aerospace SC Engineering GA 715TD UT WOS:000184987600012 ER PT J AU Tamisiea, ME Mitrovica, JX Davis, JL AF Tamisiea, ME Mitrovica, JX Davis, JL TI A method for detecting rapid mass flux of small glaciers using local sea level variations SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE glacier mass balance; sea level variations; geoid variations ID ICE SHEETS; EARTH; BALANCE AB There is increasing evidence that the global reservoir of small (or mountain) glaciers is presently experiencing an accelerated phase of net melting, perhaps linked to climatic warming. We argue that relative sea level and sea surface fingerprints local to such events provide a potentially powerful, integrated diagnostic for the mass imbalance. For example, we demonstrate, using an inference of glacier mass balance near Alaska over the last 50 years, that the present-day relative sea level fall at nearby sites can reach amplitudes that are similar to 2 orders of magnitude greater than the ongoing eustatic sea level rise associated with the melting. The peak sea surface subsidence is a factor of similar to 15 greater than the eustatic amplitude. We find that the predicted present-day sea surface change arising from the 50-year loading history is sensitive only to the ongoing rate of accelerated melting. In contrast, the present-day relative sea level fingerprint becomes increasingly sensitive to the 'history' of the recent loading when the viscosity of the asthenosphere adopted in the prediction is progressively reduced below 10(20) Pa s. Specifically, the relative sea level fingerprint becomes more localized, and reaches higher amplitudes, close to the glacier system as viscous effects become active. Our results have application in efforts to constrain small glacier mass balance using tide gauge records of relative sea level change or satellite-derived constraints on sea surface (geoid) rates. (C) 2003 Elsevier B.V. All rights reserved. C1 Univ Colorado, Boulder, CO 80305 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tamisiea, ME (reprint author), Univ Colorado, 440 UCB, Boulder, CO 80305 USA. EM tamisiea@colorado.edu RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 23 TC 10 Z9 11 U1 1 U2 5 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 AUG 25 PY 2003 VL 213 IS 3-4 BP 477 EP 485 DI 10.1016/S0012-821X(03)00301-7 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 716ZJ UT WOS:000185060100024 ER PT J AU Kukolich, SG Tanjaroon, C McCarthy, MC Thaddeus, P AF Kukolich, SG Tanjaroon, C McCarthy, MC Thaddeus, P TI Microwave spectrum of o-benzyne produced in a discharge nozzle SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID BERGMAN CYCLIZATION; AB-INITIO; ENEDIYNES; MOLECULES AB The microwave spectrum for o-benzyne was obtained by passing a dilute (<1%) mixture of benzene in neon through a pulsed-DC discharge nozzle source into a pulsed-beam, Fourier transform spectrometer. Rotational transitions were measured for the normal isotopomer, the two unique single-D isotopomers, and the C-13 isotopomer and one of the C-13 isotopomers. Benzynes have been known as reactive intermediates in organic reactions for many years, and have recently been implicated in gasoline combustion reactions and antitumor activity of enediynes. Twenty-seven b-type transitions for the normal isotopomer were fit to obtain A=6989.7292(6), B=5706.8062(6), and C=3140.3708(4) MHz, and five centrifugal distortion constants. The inertial defect is Delta=0.069 4 amu A(2), consistent with a planar structure. Hyperfine structure for the D-1 (closest to the CdropC bond) and D-2 (furthest from the CdropC bond), was analyzed to obtain deuterium quadrupole coupling strengths eQq(aa)(D-1)=185(3) kHz, eQq(bb)(D-1)=-85(2) kHz, eQq(aa)(D-2)=5(13), and eQq(bb)(D-2)=86(13) kHz. The C-D, bond axis quadrupole coupling strengths are compared with values for benzene. Spectra for the C-13(6) and one of the C-13(1) isotopomers were analyzed to obtain rotational constants. Kraitchman analysis and least-squares fitting provided nearly all of the structural parameters. The preliminary structural analysis yields an acetylenic Cequivalent toC bond length of 1.24 A, in agreement with a recent NMR value. Density functional theory (DFT) calculations were used to obtain structural parameters, and values obtained are in very good agreement with present experimental results. (C) 2003 American Institute of Physics. C1 Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Appl Sci, Cambridge, MA 02138 USA. RP Kukolich, SG (reprint author), Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 25 TC 21 Z9 21 U1 2 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 AUG 22 PY 2003 VL 119 IS 8 BP 4353 EP 4359 DI 10.1063/1.1593015 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 710HW UT WOS:000184675600029 ER PT J AU Franceschini, A Braito, V Persic, M Della Ceca, R Bassani, L Cappi, M Malaguti, P Palumbo, GGC Risaliti, G Salvati, M Severgnini, P AF Franceschini, A Braito, V Persic, M Della Ceca, R Bassani, L Cappi, M Malaguti, P Palumbo, GGC Risaliti, G Salvati, M Severgnini, P TI An XMM-Newton hard X-ray survey of ultraluminous infrared galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies : active; galaxies : evolution; galaxies : starburst; infrared : galaxies; X-rays : galaxies ID LUMINOUS STARBURST GALAXIES; DEEP SUBMILLIMETER SURVEY; BROAD-LINE REGIONS; ASCA OBSERVATIONS; EMISSION; EVOLUTION; CHANDRA; SEARCH; IRAS-19254-7245; SUPERANTENNAE AB XMM-Newton observations of 10 ultraluminous infrared galaxies (ULIRGs) from a 200-ks mini-survey programme are reported. The aim is to investigate in hard X-rays a complete ULIRG sample selected from the bright IRAS 60-mum catalogue. All sources are detected in X-rays, five of which for the first time. These observations confirm that ULIRGs are intrinsically faint X-ray sources, their observed X-ray luminosities being typically L (2-10 keV) less than or equal to 10(42) -10(43) erg s(-1) , whereas their bolometric (mostly infrared) luminosities are L (bol) > 10(45) erg s(-1). In all sources we find evidence for thermal emission from hot plasma with a rather constant temperature kT similar or equal to 0.7 keV, dominating the X-ray spectra below 1 keV, and probably associated with a nuclear or circumnuclear starburst. This thermal emission appears uncorrelated with the far-infrared luminosity, suggesting that, in addition to the ongoing rate of star formation, other parameters may also affect it. The soft X-ray emission appears to be extended on a scale of similar to30 kpc for Mrk 231 and IRAS 19254-7245, possible evidence of galactic superwinds. In these two sources, IRAS 20551-4250 and 23128-5919, we find evidence for the presence of hidden active galactic nuclei (AGNs), while a minor AGN contribution may be suspected also in IRAS 20100-4156. In particular, we have detected a strong (EW similar to 2 keV) Fe K line at 6.4 keV in the spectrum of IRAS 19254-7245 and a weaker one in Mrk 231, suggestive of deeply buried AGNs. For the other sources, the X-ray luminosities and spectral shapes are consistent with hot thermal plasma and X-ray binary emissions of mainly starburst origin. We find that the 2-10 keV luminosities in these sources, most probably due to high-mass X-ray binaries, are correlated with L (FIR) : both luminosities are good indicators of the current global star formation rate in the Galaxy. The composite nature of ULIRGs is then confirmed, with hints for a predominance of the starburst over the AGN phenomenon in these objects even when observed in hard X-rays. C1 Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Osserv Astron Padova, INAF, I-35122 Padua, Italy. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Osserv Astron Brera, INAF, I-20121 Milan, Italy. CNR, IASF, Sez Bologna, I-40129 Bologna, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Franceschini, A (reprint author), Univ Padua, Dipartimento Astron, Vicolo Osservatorio 2, I-35122 Padua, Italy. EM franceschini@pd.astro.it RI Cappi, Massimo/F-4813-2015; OI Severgnini, Paola/0000-0001-5619-5896; Cappi, Massimo/0000-0001-6966-8920; Della Ceca, Roberto/0000-0001-7551-2252; Risaliti, Guido/0000-0002-3556-977X; Bassani, Loredana/0000-0003-4858-6963; Braito, Valentina/0000-0002-2629-4989 NR 68 TC 125 Z9 125 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 AUG 21 PY 2003 VL 343 IS 4 BP 1181 EP 1194 DI 10.1046/j.1365-8711.2003.06744.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710DM UT WOS:000184665600015 ER PT J AU Clarkson, WI Charles, PA Coe, MJ Laycock, S AF Clarkson, WI Charles, PA Coe, MJ Laycock, S TI Long-term properties of accretion discs in X-ray binaries - II. Stability of radiation-driven warping SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; pulsars : general; X-rays : binaries ID UNEVENLY SPACED DATA; TIME-SERIES ANALYSIS; ANOMALOUS LOW-STATE; 35 DAY CYCLE; NEUTRON-STAR; CYGNUS X-2; HERCULIS X-1; OAO 1657-415; MASS; HERCULES-X-1 AB A significant number of X-ray binaries (XRBs) are now known to exhibit long-term 'superorbital' periodicities on time-scales of similar to10-100 d. Several physical mechanisms have been proposed that give rise to such periodicities, in particular warping and/or precession of the accretion disc. Recent theoretical work predicts the stability to disc warping of XRBs as a function of the mass ratio, binary radius, viscosity and accretion efficiency, and here we examine the constraints that can be placed on such models by current observations. In Paper I we used a dynamic power spectrum (DPS) analysis of long-term X-ray data sets (Compton Gamma Ray Observatory , Rossi X-Ray Timing Explorer ), focusing on the remarkable, smooth variations in the superorbital period exhibited by SMC X-1. Here we use a similar DPS analysis to investigate the stability of the superorbital periodicities in the neutron star XRBs Cyg X-2, LMC X-4 and Her X-1, and thereby confront stability predictions with observation. We find that the period and nature of superorbital variations in these sources are consistent with the predictions of warping theory. We also use a dynamic light-curve analysis to examine the behaviour of Her X-1 as it enters and leaves the 1999 anomalous low state (ALS). This reveals a significant phase shift some 15 cycles before the ALS, which indicates a change in the disc structure or profile leading into the ALS. C1 Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Clarkson, WI (reprint author), Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. NR 58 TC 36 Z9 37 U1 1 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 AUG 21 PY 2003 VL 343 IS 4 BP 1213 EP 1223 DI 10.1046/j.1365-8711.2003.06761.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710DM UT WOS:000184665600018 ER PT J AU Clarke, CJ Bromm, V AF Clarke, CJ Bromm, V TI The characteristic stellar mass as a function of redshift SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : formation; galaxies : formation; cosmology : theory; early Universe ID EARLY STAR-FORMATION; GLOBULAR-CLUSTERS; MOLECULAR CLOUDS; BROWN DWARFS; 1ST STARS; FRAGMENTATION; UNIVERSE; EVOLUTION; GAS; REIONIZATION AB We present a model for the star formation process during the initial collapse of dark matter haloes at redshifts z = 0-30. We derive a simple formula for the characteristic stellar mass scale during this initial burst of star formation. In our picture, this characteristic scale reflects both the minimum temperature to which the gas can cool (determined by the metallicity and the temperature of the cosmic microwave background) and the pressure of overlying baryons in the collapsing halo. This prescription reproduces both the large mass scales found in simulations of Population III star formation and the near-solar values observed for star formation at low redshift. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Clarke, CJ (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. NR 53 TC 31 Z9 31 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 AUG 21 PY 2003 VL 343 IS 4 BP 1224 EP 1230 DI 10.1046/j.1365-8711.2003.06765.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710DM UT WOS:000184665600019 ER PT J AU Hamana, T Kayo, I Yoshida, N Suto, Y Jing, YP AF Hamana, T Kayo, I Yoshida, N Suto, Y Jing, YP TI Modelling peculiar velocities of dark matter haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : general; cosmology : theory; dark matter; large-scale structure of Universe ID N-BODY SIMULATIONS; GALAXY CLUSTERS; LOGNORMAL MODEL; BULK FLOWS; ONE-POINT; FLUCTUATIONS; MOTIONS AB We present a simple model that accurately describes various statistical properties of peculiar velocities of dark matter haloes. We pay particular attention to the following two effects. First, the evolution of the halo peculiar velocity depends on the local matter density, instead of the global density. Secondly, dark matter haloes are biased tracers of the underlying mass distribution, thus haloes tend to be located preferentially at high density regions. For the former, we develop an empirical model calibrated with N -body simulations while, for the latter, we use a conventional halo bias model based on the extended Press-Schechter model combined with an empirical lognormal probability distribution function of the mass density distribution. We find that, compared with linear theory, the present model significantly improves the accuracy of predictions of statistical properties of the halo peculiar velocity field including the velocity dispersion, the probability distribution function, and the pairwise velocity dispersion at large separations. Thus, our model predictions may be useful in analysing future observations of the peculiar velocities of galaxy clusters. C1 Inst Astrophys, F-75014 Paris, France. Natl Astron Observ Japan, Tokyo 1818588, Japan. Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan. MPI Astrophys, Shanghai Astron Observ, Shanghai 200030, Peoples R China. RP Hamana, T (reprint author), Inst Astrophys, 98bis Blvd Arago, F-75014 Paris, France. RI Yoshida, Naoki/A-4305-2011; Kayo, Issha/A-4389-2011; Jing, Yipeng/P-3678-2015 NR 46 TC 22 Z9 22 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 AUG 21 PY 2003 VL 343 IS 4 BP 1312 EP 1318 DI 10.1046/j.1365-8711.2003.06787.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710DM UT WOS:000184665600028 ER PT J AU Somerville, RS Bullock, JS Livio, M AF Somerville, RS Bullock, JS Livio, M TI The epoch of reionization in models with reduced small-scale power SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : evolution; intergalactic medium ID WARM DARK-MATTER; SURFACE BRIGHTNESS GALAXIES; INITIAL MASS FUNCTION; STAR-FORMATION; 1ST STARS; COSMOLOGICAL REIONIZATION; POPULATION-III; HIGH-REDSHIFT; INTERGALACTIC MEDIUM; RADIATIVE FEEDBACK AB Reducing the power on small scales relative to the "standard'' Lambda cold dark matter (LambdaCDM) model alleviates a number of possible discrepancies with observations and is favored by the recent analysis of the Wilkinson Microwave Anisotropy Probe (WMAP) plus galaxy and Lyalpha forest data. Here we investigate the epoch of reionization in several models normalized to WMAP on large scales and with sufficiently reduced power on small scales to solve the halo concentration and substructure problems. These include a tilted model, the WMAP running-index model, and a warm dark matter model. We assume that the universe was reionized by stellar sources composed of a combination of supermassive (similar to200 M.) Population III stars and Population II stars with a "normal'' initial mass function (IMF). We find that in all of these models, structure formation and hence reionization occurs late, certainly at redshifts below 10, and more probably at z less than or similar to 6. This is inconsistent (at 2 sigma) with the determination of z(reion) similar or equal to 17 from the WMAP temperature-polarization data and is only marginally consistent with Sloan Digital Sky Survey quasar observations. The tension between the galactic-scale observations, which favor low-power models, and the early reionization favored by WMAP can only be resolved if the efficiency of Population III star formation is dramatically higher than any current estimate or if there is an exotic population of ionizing sources such as miniquasars. Otherwise, we may have to live with the standard LambdaCDM power spectrum and solve the small-scale problems in some other way. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Somerville, RS (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM somerville@stsci.edu; jbullock@cfa.harvard.edu; mlivio@stsci.edu RI Bullock, James/K-1928-2015 OI Bullock, James/0000-0003-4298-5082 NR 72 TC 64 Z9 64 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 20 PY 2003 VL 593 IS 2 BP 616 EP 621 DI 10.1086/376686 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400003 ER PT J AU Matthews, LD Wood, K AF Matthews, LD Wood, K TI High-latitude HI in the low surface brightness galaxy UGC 7321 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : halos; galaxies : individual (UGC 7321); galaxies : ISM; galaxies : spiral ID DIFFUSE IONIZED-GAS; ALPHA ABSORPTION SYSTEMS; DISK COLOR GRADIENTS; INTERSTELLAR-MEDIUM; NEUTRAL HYDROGEN; SPIRAL GALAXIES; SUPERTHIN GALAXIES; GLOBAL PROPERTIES; ROTATION CURVE; GASEOUS EXTENT AB From the analysis of sensitive H I 21 cm line observations, we find evidence for vertically extended H I emission (\z\ less than or similar to 2.4 kpc) in the edge-on, low surface brightness spiral galaxy UGC 7321. Three-dimensional modeling suggests that the H I disk of UGC 7321 is both warped and flared, but that neither effect can fully reproduce the spatial distribution and kinematics of the highest z-height gas. We are able to model the high-latitude emission as an additional H I component in the form of a "thick disk'' or "halo'' with a FWHM of similar to3.3 kpc. We find tentative evidence that the vertically extended gas declines in rotational velocity as a function of z, although we are unable to completely rule out models with constant V(z). In spite of the low star formation rate of UGC 7321, energy from supernovae may be sufficient to sustain this high-latitude gas. However, alternative origins for this material, such as slow, sustained infall, cannot yet be excluded. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Dept Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Matthews, LD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. NR 56 TC 56 Z9 58 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 2003 VL 593 IS 2 BP 721 EP 732 DI 10.1086/376602 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400012 ER PT J AU Michael, E McCray, R Chevalier, R Filippenko, AV Lundqvist, P Challis, P Sugerman, B Lawrence, S Pun, CSJ Garnavich, P Kirshner, R Crotts, A Fransson, C Li, WD Panagia, N Phillips, M Schmidt, B Sonneborn, G Suntzeff, N Wang, LF Wheeler, JC AF Michael, E McCray, R Chevalier, R Filippenko, AV Lundqvist, P Challis, P Sugerman, B Lawrence, S Pun, CSJ Garnavich, P Kirshner, R Crotts, A Fransson, C Li, WD Panagia, N Phillips, M Schmidt, B Sonneborn, G Suntzeff, N Wang, LF Wheeler, JC TI Hubble Space Telescope observations of high-velocity Ly alpha and H alpha emission from supernova remnant 1987A: The structure and development of the reverse shock SO ASTROPHYSICAL JOURNAL LA English DT Article DE shock waves; supernovae : individual (SN 1987A); supernova remnants ID LARGE-MAGELLANIC-CLOUD; X-RAY REMNANT; SN 1987A; CIRCUMSTELLAR RING; INTERSTELLAR EXTINCTION; LINE EMISSION; HOT-SPOTS; SN-1987A; EVOLUTION; EJECTA AB We present two-dimensional line profiles of high-velocity (similar to+/-12,000 km s(-1)) Lyalpha and Halpha emission from supernova remnant 1987A obtained with the Space Telescope Imaging Spectrograph between 1997 September and 2001 September (days 3869-5327 after the explosion). This emission comes from hydrogen in the debris that is excited and ionized as it passes through the remnant's reverse shock. We use these profiles to measure the geometry and development of the reverse-shock surface. The observed emission is confined within similar to+/-30degrees about the remnant's equatorial plane. At the equator, the reverse shock has a radius of similar to75% of the distance to the equatorial ring. We detect marginal differences (6% +/- 3%) between the location of the reverse-shock front in the northeast and southwest parts of the remnant. The radius of the reverse shock surface increases for latitudes above the equator, a geometry consistent with a model in which the supernova debris expands into a bipolar nebula. Assuming that the outer supernova debris has a power-law density distribution, we can infer from the reverse-shock emission light curve an expansion rate ( in the northeast part of the remnant) of 3700 +/- 900 km s(-1), consistent with the expansion velocities determined from observations in radio ( Manchester et al.) and X-ray ( Park et al.; Michael et al.) wavelengths. However, our most recent observation ( at day 5327) suggests that the rate of increase of mass flux across the northeast sector of the reverse shock has accelerated, perhaps because of deceleration of the reverse shock caused by the arrival of a reflected shock created when the blast wave struck the inner ring. Resonant scattering within the supernova debris causes Lyalpha photons created at the reverse shock to be directed preferentially outward, resulting in a factor of similar to5 difference in the observed brightness of the reverse shock in Lyalpha between the near and far sides of the remnant. Accounting for this effect, we compare the observed reverse-shock Lyalpha and Halpha fluxes to infer the amount of interstellar extinction by dust as E(B - V) = 0.17 +/- 0.01 mag. We also notice extinction by dust in the equatorial ring with E(B - V) approximate to 0.02-0.08 mag, which implies dust-to-gas ratios similar to that of the LMC. Since Halpha photons are optically thin to scattering, the observed asymmetry in brightness of Halpha from the near and far sides of the remnant represents a real asymmetry in the mass flux through the reverse shock of similar to30%. We discuss future observational strategies that will permit us to further investigate the reverse-shock dynamics and resonant scattering of the Lyalpha line and to constrain better the extinction by dust within and in front of the remnant. C1 Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Dept Astron, Stockholm Observ, SCFAB, SE-10691 Stockholm, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hofstra Univ 151, Dept Phys & Astron, Hempstead, NY 11590 USA. NASA, Lab Astron & Space Phys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. STScI, Baltimore, MD 21218 USA. Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Weston, ACT 2611, Australia. Cerro Tololo Interamer Observ, La Serena, Chile. Univ Calif Berkeley, Lawrence Berkeley Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Michael, E (reprint author), Univ Colorado, Joint Inst Lab Astrophys, Campus Box 440, Boulder, CO 80309 USA. NR 39 TC 39 Z9 40 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 2003 VL 593 IS 2 BP 809 EP 830 DI 10.1086/376725 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400017 ER PT J AU Argon, AL Reid, MJ Menten, KM AF Argon, AL Reid, MJ Menten, KM TI A class of interstellar OH masers associated with protostellar outflows SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (W3); ISM : jets and outflows; masers; radiation mechanisms : nonthermal; radio lines : ISM; stars : formation ID PROPER MOTIONS; HYDROXYL MASERS; REGION W3(OH); ORION-KL; EMISSION; KINEMATICS; DISTANCES; GALAXY; SHOCK AB Using the Very Large Array, we have detected weak OH maser emission near the Turner-Welch protostellar source in the W3 OH region. Unlike typical interstellar OH masers, which are associated with ultracompact H II regions, our measured positions and proper motions (from very long baseline interferometry) indicate that these OH masers are associated with a bipolar outflow traced by strong H2O masers. These OH masers may be part of a class of interstellar OH masers that are associated with very young stars that have yet to, or may never, create ultracompact H II regions. This class of OH masers appears to form near the edges of very dense material ( within which H2O masers form), where total densities drop precipitously and interstellar UV radiation is sufficient to dissociate the H2O molecules. Observations of this class of OH masers may be an important way to probe the distribution of this important molecule in interstellar shocks at arcsecond resolution or better. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Argon, AL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. NR 29 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 AUG 20 PY 2003 VL 593 IS 2 BP 925 EP 930 DI 10.1086/376592 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400023 ER PT J AU Li, LX Goodman, J Narayan, R AF Li, LX Goodman, J Narayan, R TI Nonaxisymmetric g-mode and p-mode instability in a hydrodynamic thin accretion disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; instabilities; waves; X-rays : binaries ID QUASI-PERIODIC OSCILLATIONS; X-RAY BINARIES; BLACK-HOLE; RELATIVISTIC DISKOSEISMOLOGY; COUETTE FLOW; WAVES; EXCITATION AB It has been suggested that quasi-periodic oscillations of accreting X-ray sources may relate to the modes named in the title. We consider nonaxisymmetric linear perturbations to an isentropic, isothermal, unmagnetized thin accretion disk. The radial wave equation, in which the number of vertical nodes (n) appears as a separation constant, admits a wave action current that is conserved except, in some cases, at corotation. Waves without vertical nodes amplify when reflected by a barrier near corotation. Their action is conserved. As was previously known, this amplification allows the n = 0 modes to be unstable under appropriate boundary conditions. In contrast, we find that waves with n > 0 are strongly absorbed at corotation rather than amplified; their action is not conserved. Therefore, nonaxisymmetric p-modes and g-modes with n > 0 are damped and stable even in an inviscid disk. This eliminates a promising explanation for quasi-periodic oscillations in neutron star and black hole X-ray binaries. 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 32 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 AUG 20 PY 2003 VL 593 IS 2 BP 980 EP 991 DI 10.1086/376695 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400029 ER PT J AU Narita, T Grindlay, JE Bloser, PF Chou, Y AF Narita, T Grindlay, JE Bloser, PF Chou, Y TI X-ray dip monitoring of XB 1916-053 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; X-rays : binaries ID ADVECTION-DOMINATED ACCRETION; ACTIVE GALACTIC NUCLEI; 4U 1915-05; BEPPOSAX OBSERVATION; SPECTRAL VARIATIONS; DISK CORONAE; BLACK-HOLES; CYGNUS X-1; BINARIES; ABSORPTION AB We report on the long-term monitoring of X-ray dips from the ultracompact low-mass X-ray binary (LMXB) XB 1916-053. Roughly one-month interval observations were carried out with the Rossi X-ray Timing Explorer (RXTE) during 1996, during which the source varied between dim, hard states and more luminous, soft states. The dip spectra and dip light curves were compared against both the broadband luminosity and the derived mass accretion rate ((M)over dot). The dips spectra could be fitted by an absorbed blackbody plus cutoff power-law nondip spectral model, with additional absorption ranging from 0 to > 100 x 10(22) cm(-2). The amount of additional blackbody absorption was found to vary with the source luminosity. Our results are consistent with an obscuration of the inner disk region by a partially ionized outer disk. The size of the corona, derived from the dip ingress times, was found to be similar to10(9) cm. The corona size did not correlate with the coronal temperature, but seemed to increase when (M)over dot also increased. We discuss our. ndings in the context of an evaporated accretion disk corona model and an ADAF-type model. C1 Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Cent Univ, Grad Inst Astron, Taoyuan, Taiwan. RP Narita, T (reprint author), Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA. RI Chou, Yi/C-4922-2008 OI Chou, Yi/0000-0002-8584-2092 NR 47 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2003 VL 593 IS 2 BP 1007 EP 1012 DI 10.1086/376693 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400031 ER PT J AU Lloyd, DA Hernquist, L Heyl, JS AF Lloyd, DA Hernquist, L Heyl, JS TI Optical and X-ray properties of cooling neutron stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; stars : atmospheres; stars : neutron; X-rays : stars ID PULSAR 4U 0142+61; MAGNETIZED PLASMA; RCW 103; EMISSION; COUNTERPART; GEMINGA; MODEL; PSR-1055-52; ATMOSPHERES; MAGNETARS AB Blackbody fits to the soft X-ray spectra of cooling neutron stars will, in general, overestimate the surface temperature of the source. We examine blackbody fits to the spectra predicted by light-element neutron star model atmospheres folded with the ACIS response matrices and quantify the inferred temperature error for a range of magnetic field strengths representative of the broad populations of isolated cooling neutron stars. Results for the Position Sensitive Proportional Counter are derived for comparative purposes. In each example, the blackbody temperature systematically overestimates the underlying flux temperature of the model and is an unreliable gauge by which to estimate the surface properties of neutron stars. We demonstrate a linear relationship between flux temperature and peak energy, similar to Wien displacement, as a function of magnetic field strength for the model atmospheres. We calculate the excess optical magnitude predicted from the model atmospheres with respect to the Rayleigh-Jeans portion of the fitted blackbody. We detail the nature and magnitude of these discrepancies and identify their origin in the opacity of the atmospheric plasma, the magnitude of interstellar absorption, and the instrumental response function. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lloyd, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dlloyd@cfa.harvard.edu; lhernquist@cfa.harvard.edu; jsheyl@cfa.harvard.edu NR 38 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2003 VL 593 IS 2 BP 1024 EP 1031 DI 10.1086/376589 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400033 ER PT J AU Luhman, KL Stauffer, JR Muench, AA Rieke, GH Lada, EA Bouvier, J Lada, CJ AF Luhman, KL Stauffer, JR Muench, AA Rieke, GH Lada, EA Bouvier, J Lada, CJ TI A census of the young cluster IC 348 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : luminosity function, mass function; stars : pre-main-sequence ID LOW-MASS STARS; T-TAURI STARS; MAIN-SEQUENCE EVOLUTION; ORION NEBULA CLUSTER; SPECTRAL ENERGY-DISTRIBUTIONS; NEAR-INFRARED IMAGES; BROWN DWARFS; SUBSTELLAR OBJECTS; IC 348; SPECTROSCOPIC BINARIES AB We present a new census of the stellar and substellar members of the young cluster IC 348. We have obtained images at I and Z for a 42' x 28' field encompassing the cluster and have combined these measurements with previous optical and near-infrared photometry. From spectroscopy of candidate cluster members appearing in these data, we have identified 122 new members, 15 of which have spectral types of M6.5-M9, corresponding to masses of similar to0.08-0.015 M-circle dot by recent evolutionary models. The latest census for IC 348 now contains a total of 288 members, 23 of which are later than M6 and thus are likely to be brown dwarfs. From an extinction-limited sample of members (A(V) less than or equal to 4) for a 16' x 14' field centered on the cluster, we construct an initial mass function (IMF) that is unbiased in mass and nearly complete for M/M-circle dot greater than or equal to 0.03 (less than or similar toM8). In logarithmic units where the Salpeter slope is 1.35, the mass function for IC 348 rises from high masses down to a solar mass, rises more slowly down to a maximum at 0.1-0.2 M-circle dot, and then declines into the substellar regime. In comparison, the similarly derived IMF for Taurus from Briceno et al. and Luhman et al. rises quickly to a peak near 0.8 M-circle dot and steadily declines to lower masses. The distinctive shapes of the IMFs in IC 348 and Taurus are reflected in the distributions of spectral types, which peak at M5 and K7, respectively. These data provide compelling, model-independent evidence for a significant variation of the IMF with star-forming conditions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Muench, August/0000-0003-0666-6367 NR 93 TC 418 Z9 419 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 2003 VL 593 IS 2 BP 1093 EP 1115 DI 10.1086/376594 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400039 ER PT J AU Jang-Condell, H Sasselov, DD AF Jang-Condell, H Sasselov, DD TI Radiative transfer on perturbations in protoplanetary disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation; planetary systems : protoplanetary disks; radiative transfer ID SPECTRAL ENERGY-DISTRIBUTIONS; T-TAURI STARS; ACCRETION DISKS; YOUNG OBJECTS; IRRADIATION AB We present a method for calculating the radiative transfer on a protoplanetary disk perturbed by a protoplanet. We apply this method to determine the effect on the temperature structure within the photosphere of a passive circumstellar disk in the vicinity of a small protoplanet of up to 20 Earth masses. The gravitational potential of a protoplanet induces a compression of the disk material near it, resulting in a decrement in the density at the disk's surface. Thus, an isodensity contour at the height of the photosphere takes on the shape of a well. When such a well is illuminated by stellar irradiation at grazing incidence, it results in cooling in a shadowed region and heating in an exposed region. For typical stellar and disk parameters relevant to the epoch of planet formation, we find that the temperature variation due to a protoplanet at 1 AU separation from its parent star is about 4% (5 K) for a planet of 1 Earth mass, about 14% (19 K) for planet of 10 Earth masses, and about 18% (25 K) for planet of 20 Earth masses, We conclude that even such relatively small protoplanets can induce temperature variations in a passive disk. Therefore, many of the processes involved in planet formation should not be modeled with a locally isothermal equation of state. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jang-Condell, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Jang-Condell, Hannah/0000-0002-7639-1322 NR 14 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2003 VL 593 IS 2 BP 1116 EP 1123 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400040 ER PT J AU Bemporad, A Poletto, G Suess, ST Ko, YK Parenti, S Riley, P Romoli, M Zurbuchen, TZ AF Bemporad, A Poletto, G Suess, ST Ko, YK Parenti, S Riley, P Romoli, M Zurbuchen, TZ TI Temporal evolution of a streamer complex: Coronal and in situ plasma parameters SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : abundances; Sun : corona; Sun : UV radiation ID UPPER SOLAR ATMOSPHERE; WHOLE SUN MONTH; ELEMENTAL ABUNDANCES; QUIET-SUN; WIND; SPECTROMETER; SOHO; MINIMUM; TEMPERATURES; DENSITIES AB We report on observations acquired by the Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliospheric Observatory (SOHO), from 2000 June 10 to June 17 at the time of a SOHO-Sun-Ulysses quadrature. UVCS took data at 1.6 and 1.9 R-circle dot with a slit normal to the solar radius and centered along the radial to Ulysses. A streamer complex was sampled by UVCS throughout the quadrature campaign, giving us the opportunity to derive plasma parameters in different streamers and to compare them with plasma properties measured in situ. Large Angle Spectroscopic Coronagraph images above 2 R-circle dot helped us understand the temporal evolution of the streamer complex. We derive densities, temperatures, and elemental abundances in two streamers, which have different temperatures and element abundances. In spite of these differences, both structures have the same first ionization potential (FIP) bias. The Fe/O ratio, which may be considered a proxy for the FIP effect, was measured in situ by the Solar Wind Ion Composition Spectrometer aboard the Ulysses spacecraft. Values of Fe/O measured in the corona at the sites where in situ plasma originated agree with in situ Fe/O values. C1 Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Osserv Astrofis Arcetri, I-50125 Florence, Italy. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Sci Applicat Int Corp, San Diego, CA 92121 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Univ Florence, Dipartimento Astron & Sci Spazio, Largo Fermi 5, I-50125 Florence, Italy. EM bemporad76@arcetri.astro.it; poletto@arcetri.astro.it; steve.suess@nsstc.nasa.gov; yko@cfa.harvard.edu; susanna.parenti@medoc-ias.u-psud.fr; pete.riley@saic.co; romoli@arcetri.astro.it; thomasz@umich.edu RI Romoli, Marco/H-6859-2012; OI Bemporad, Alessandro/0000-0001-5796-5653 NR 51 TC 24 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2003 VL 593 IS 2 BP 1146 EP 1163 DI 10.1086/376605 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400043 ER PT J AU Winebarger, AR Warren, HP Seaton, DB AF Winebarger, AR Warren, HP Seaton, DB TI Evolving active region loops observed with the Transition Region and Coronal Explorer. I. Observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : UV radiation ID FLARING LOOPS; SOLAR CORONA; TRACE DATA; TEMPERATURE; DYNAMICS; EVOLUTION; PROFILES; FLARES; FLOWS; VIEW AB Observations made with TRACE have detected a class of persistent active region loops that have. at 195/171 Angstrom filter ratios. The intensity of these loops implies a density that is as much as 3 orders of magnitude larger than the densities of static solutions to the hydrodynamic equations. It has recently been suggested that these loops are bundles of impulsively heated strands that are cooling through the TRACE passbands. This scenario implies that the loops would appear in the hotter ( Fe XV 284 Angstrom or Fe XII 195 Angstrom) TRACE filter images before appearing in the cooler (Fe IX/X 171 Angstrom) TRACE filter images. In this paper, we test this hypothesis by examining the temporal evolution of five active region loops in multiple TRACE EUV filter images. We find that all the loops appear in the hotter filter images before appearing in cooler filter images. We then use the measured delay to estimate a cooling time and find that four of the five loops have lifetimes greater than the expected lifetime of a cooling loop. These results are consistent with the hypothesis that each apparent loop is a bundle of sequentially heated strands; other explanations will also be discussed. To facilitate comparisons between these loops and hydrodynamic simulations, we use a new technique to estimate the loop length and geometry. C1 Computat Phys Inc, Springfield, VA 22151 USA. USN, Res Lab, Washington, DC 20375 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Computat Phys Inc, 8001 Braddock Rd,Suite 210, Springfield, VA 22151 USA. EM winebarger@nrl.navy.mil; hwarren@nrl.navy.mil; dseaton@cfa.harvard.edu OI SEATON, DANIEL/0000-0002-0494-2025 NR 27 TC 85 Z9 86 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 2003 VL 593 IS 2 BP 1164 EP 1173 DI 10.1086/376679 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XA UT WOS:000184823400044 ER PT J AU Mohanty, S Jayawardhana, R Navascues, DBY AF Mohanty, S Jayawardhana, R Navascues, DBY TI Magellan echelle spectroscopy of TW Hydrae brown dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; open clusters and associations : individual (TW Hydrae); stars : low-mass, brown dwarfs; stars : pre-main-sequence ID LOW-MASS STARS; ASSOCIATION; CANDIDATE; ACCRETION; DISCOVERY; MEMBERS; DISK AB We present high-resolution optical spectroscopy of four candidate members of the nearby TW Hydrae young association including three brown dwarfs ( 2MASS 1207-3932, 2MASS 1139-3159, and TWA 5B) and one T Tauri multiple star (TWA 5A). Using echelle spectra from the Magellan Baade 6.5 m telescope, we confirm the pre-main-sequence status and cluster membership of the substellar candidates, through the detection of Li I, Na I consistent with low gravity, and radial velocity. Given their late spectral type (similar toM8) and the youth of the association (age similar to 10 Myr), cluster membership certifies these three objects as young brown dwarfs. One of them (2MASS 1207-3932) shows strong emission both in the hydrogen Balmer series (Halpha to Hepsilon) and in He I (4471, 5876, 6678, and 7065 Angstrom), compared with other young brown dwarfs of similar spectral type. The Halpha line is also relatively broad (10% width similar to200 km s(-1)) and asymmetric. These characteristics suggest that 2MASS 1207-3932 is a (weak) accretor. While we cannot rule out activity, comparison with a flaring field dwarf implies that such activity would have to be quite anomalous. The verification of accretion would make it the oldest actively accreting brown dwarf known to date, suggesting that inner-disk lifetimes in substellar objects can be comparable to those in stars, consistent with a similar formation mechanism. The close triple TWA 5A also appears to be a variable accretor, implying that long-lived disks can exist in multiple systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. INTA, Lab Astofis Espacial & Fis Fundamental, Madrid 28080, Spain. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 17 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2003 VL 593 IS 2 BP L109 EP L112 DI 10.1086/378315 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XD UT WOS:000184823900013 ER PT J AU Winn, JN Garnavich, PM Stanek, KZ Sasselov, DD AF Winn, JN Garnavich, PM Stanek, KZ Sasselov, DD TI Limits on eclipses of the pre-main-sequence star KH 15D in the first half of the 20th century SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 2264); planetary systems : protoplanetary disks; stars : individual (KH 15D); stars : pre-main-sequence ID KH 15D; YOUNG; MASS; DUST AB Over the last decade, the pre-main-sequence star KH 15D has exhibited periodic eclipses that are surprisingly deep (similar to3 mag) and long-lasting (similar to40% of the 48.4 day period). The cause of the eclipses is unknown, but it could be a feature in a nearly edge-on protoplanetary disk. Here we report on an analysis of archival photographs of KH 15D from the Harvard College Observatory plate collection, most of which were taken during the years 1913-1951. During this time range, the data are consistent with no eclipses; the duty cycle of 1 mag eclipses was less than 20%. The decadal timescale of this change in eclipse behavior is compatible with the expected timescale of protoplanet/disk interactions. Archival images from more recent epochs should reveal the onset of the eclipses. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Notre Dame, IN 46556 USA. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 25 Z9 25 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2003 VL 593 IS 2 BP L121 EP L124 DI 10.1086/378314 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 712XD UT WOS:000184823900016 ER PT J AU Clarke, G Leverington, D Teller, J Dyke, A AF Clarke, G Leverington, D Teller, J Dyke, A TI Superlakes, megafloods, and abrupt climate change SO SCIENCE LA English DT Editorial Material ID LAURENTIDE ICE-SHEET; GLACIAL LAKE AGASSIZ; COLD EVENT; YR BP; DEGLACIATION; INSTABILITY; RECORD; EUROPE C1 Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada. Smithsonian Inst, Ctr Earth & Planetray Studies, Natl Air & Space Museum, Washington, DC 20560 USA. Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. Geol Survey Canada, Terain Sci Div, Ottawa, ON K1A 0E8, Canada. RP Clarke, G (reprint author), Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada. NR 14 TC 83 Z9 83 U1 3 U2 31 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 15 PY 2003 VL 301 IS 5635 BP 922 EP 923 DI 10.1126/science.1085921 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 711RY UT WOS:000184755900022 PM 12920285 ER PT J AU Hughes, TP Baird, AH Bellwood, DR Card, M Connolly, SR Folke, C Grosberg, R Hoegh-Guldberg, O Jackson, JBC Kleypas, J Lough, JM Marshall, P Nystrom, M Palumbi, SR Pandolfi, JM Rosen, B Roughgarden, J AF Hughes, TP Baird, AH Bellwood, DR Card, M Connolly, SR Folke, C Grosberg, R Hoegh-Guldberg, O Jackson, JBC Kleypas, J Lough, JM Marshall, P Nystrom, M Palumbi, SR Pandolfi, JM Rosen, B Roughgarden, J TI Climate change, human impacts, and the resilience of coral reefs SO SCIENCE LA English DT Review ID GREAT-BARRIER-REEF; MARINE RESERVES; BIODIVERSITY; ECOSYSTEMS; EVOLUTION; FUTURE; PERSPECTIVES; DISTURBANCE; MORTALITY; DIVERSITY AB The diversity, frequency, and scale of human impacts on coral reefs are increasing to the extent that reefs are threatened globally. Projected increases in carbon dioxide and temperature over the next 50 years exceed the conditions under which coral reefs have flourished over the past half-million years. However, reefs will change rather than disappear entirely, with some species already showing far greater tolerance to climate change and coral bleaching than others. International integration of management strategies that support reef resilience need to be vigorously implemented, and complemented by strong policy decisions to reduce the rate of global warming. C1 James Cook Univ, Ctr Coral Reef Biodivers, Townsville, Qld 4811, Australia. Environm Protect Agcy, Old Quarantine Stn, Townsville, Qld 4810, Australia. Stockholm Univ, Dept Syst Ecol, SE-10691 Stockholm, Sweden. Univ Calif Davis, Ctr Populat Biol, Div Biol Sci, Sect Ecol & Evolut, Davis, CA 95616 USA. Univ Queensland, Ctr Marine Studies, St Lucia, Qld, Australia. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Australian Inst Marine Sci, Townsville, Qld 4810, Australia. Great Barrier Reef Marine Pk Author, Townsville, Qld 4810, Australia. Stanford Univ, Hopkins Marine Stn, Dept Biol Sci, Pacific Grove, CA 93950 USA. Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. Nat Hist Museum, Dept Zool, London SW7 5BD, England. Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA. RP Hughes, TP (reprint author), James Cook Univ, Ctr Coral Reef Biodivers, Townsville, Qld 4811, Australia. RI Baird, Andrew/C-8449-2009; Connolly, Sean/E-7773-2011; Pandolfi, John/A-3121-2009; Hoegh-Guldberg, Ove/H-6169-2011; Lough, Janice/L-1682-2013; Hughes, Terry/L-4721-2013; kohki, sowa/D-2955-2011 OI Baird, Andrew/0000-0001-8504-4077; Connolly, Sean/0000-0003-1537-0859; Pandolfi, John/0000-0003-3047-6694; Hoegh-Guldberg, Ove/0000-0001-7510-6713; Hughes, Terry/0000-0002-5257-5063; NR 50 TC 1672 Z9 1747 U1 344 U2 1844 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 15 PY 2003 VL 301 IS 5635 BP 929 EP 933 DI 10.1126/science.1085046 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 711RY UT WOS:000184755900027 PM 12920289 ER PT J AU Pandolfi, JM Bradbury, RH Sala, E Hughes, TP Bjorndal, KA Cooke, RG McArdle, D McClenachan, L Newman, MJH Paredes, G Warner, RR Jackson, JBC AF Pandolfi, JM Bradbury, RH Sala, E Hughes, TP Bjorndal, KA Cooke, RG McArdle, D McClenachan, L Newman, MJH Paredes, G Warner, RR Jackson, JBC TI Global trajectories of the long-term decline of coral reef ecosystems SO SCIENCE LA English DT Article ID CLIMATE-CHANGE; BELIZE; DISEASES; ECOLOGY; FUTURE; SCALE AB Degradation of coral reef ecosystems began centuries ago, but there is no global summary of the magnitude of change. We compiled records, extending back thousands of years, of the status and trends of seven major guilds of carnivores, herbivores, and architectural species from 14 regions. Large animals declined before small animals and architectural species, and Atlantic reefs declined before reefs in the Red Sea and Australia, but the trajectories of decline were markedly similar worldwide. All reefs were substantially degraded long before outbreaks of coral disease and bleaching. Regardless of these new threats, reefs will not survive without immediate protection from human exploitation over large spatial scales. C1 Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Australian Natl Univ, Ctr Resource & Environm Studies, Canberra, ACT 0200, Australia. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. James Cook Univ, Ctr Coral Reef Biodivers, Sch Marine Biol, Townsville, Qld 4811, Australia. Univ Florida, Archie Carr Ctr Sea Turtle Res, Dept Zool, Gainesville, FL 32611 USA. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. Univ Calif Santa Barbara, Calif Sea Grant, Cooperat Extens, Santa Barbara, CA 93105 USA. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. RP Pandolfi, JM (reprint author), Natl Museum Nat Hist, Dept Paleobiol, MRC-121,POB 37012, Washington, DC 20013 USA. EM pandolfi.john@nmnh.si.edu RI Pandolfi, John/A-3121-2009; Hughes, Terry/L-4721-2013; Warner, Robert/M-5342-2013; OI Pandolfi, John/0000-0003-3047-6694; Hughes, Terry/0000-0002-5257-5063; Warner, Robert/0000-0002-3299-5685; Bjorndal, Karen/0000-0002-6286-1901 NR 19 TC 858 Z9 909 U1 70 U2 551 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 15 PY 2003 VL 301 IS 5635 BP 955 EP 958 DI 10.1126/science.1085706 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 711RY UT WOS:000184755900036 PM 12920296 ER PT J AU Narayan, R Medvedev, MV AF Narayan, R Medvedev, MV TI Self-similar hot accretion on to a spinning neutron star: matching the outer boundary conditions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars : neutron; stars : rotation ID X-RAY-EMISSION; FLOWS; CONVECTION; SPECTRA; DWARFS AB Medvedev & Narayan have described a hot accretion flow on to a spinning neutron star in which the gas viscously brakes the spin of the star. Their self-similar solution has the surprising property that the density, temperature and angular velocity of the gas at any radius are completely independent of the outer boundary conditions. Hence, the solution cannot be matched to a general external medium. We resolve this paradoxical situation by showing that there is a second self-similar solution which bridges the gap between the original solution and the external medium. This new solution has an extra degree of freedom which permits it to match general outer boundary conditions. We confirm the main features of the analytical results with a full numerical solution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 21 TC 4 Z9 4 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 AUG 11 PY 2003 VL 343 IS 3 BP 1007 EP 1012 DI 10.1046/j.1365-8711.2003.06747.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706ZT UT WOS:000184485500036 ER PT J AU Wasshausen, DC Wood, JRI AF Wasshausen, DC Wood, JRI TI Notes on the genus Ruellia (Acanthaceae) in Bolivia, Peru and Brazil SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Taxonomic notes on Ruellia are presented in preparation for the authors' forthcoming annotated checklist of Bolivian Acanthaceae. Four new species (R. antiquorum, R. beckii, R. dolichosiphon and R. exserta) are described and illustrated, two new combinations are made and variation in R. haenkeana is discussed leading to the recognition of two varieties and two forms in the species. The little-known R. pearcei is described, illustrated and discussed in relation to the widespread R. brevifolia. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Bot, DCW, Washington, DC 20560 USA. JRIW, Liss GU33 7BP, Hants, England. RP Wasshausen, DC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Bot, DCW, Washington, DC 20560 USA. NR 1 TC 6 Z9 6 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 AUG 11 PY 2003 VL 116 IS 2 BP 263 EP 274 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 712FJ UT WOS:000184786500001 ER PT J AU Graves, GR AF Graves, GR TI Diagnoses of hybrid hummingbirds (Aves : Trochilidae). 10. Cyanomyia salvini Brewster, 1893, is an intergeneric hybrid of Amazilia violiceps and Cynanthus latirostris SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID ORIGIN; GOULD AB Cyanomyia salvini Brewster, 1893, collected in Sonora, Mexico, is shown to be a hybrid between Amazilia violiceps ellioti and Cynanthus latirostris magicus, whose breeding ranges overlap extensively in northwestern Mexico. This specimen represents the only known intergeneric hybrid between species currently placed in Amazilia and Cynanthus (Sibley and Monroe 1990). C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, MRC 116, 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. NR 24 TC 0 Z9 0 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 AUG 11 PY 2003 VL 116 IS 2 BP 293 EP 300 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 712FJ UT WOS:000184786500003 ER PT J AU Suarez, W Olson, SL AF Suarez, W Olson, SL TI A new species of caracara (Milvago) from Quaternary asphalt deposits in Cuba, with notes on new material of Caracara creightoni Brodkorb (Aves : Falconidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB An extinct caracara, Milvago carbo, new species, is described from Quaternary asphalt deposits of Las Breas de San Felipe, northern Matanzas Province, Cuba, from tarsometatarsi, tibiotarsi, and a notarium. This species was much larger than other species of the genus, living or extinct. New material of the extinct species Caracara creightoni provides additional information on its characters and distribution. C1 Museo Nacl Hist Nat, WS, Havana 10100, Cuba. Smithsonian Inst, Natl Museum Nat Hist, SLO, Washington, DC 20560 USA. RP Suarez, W (reprint author), Museo Nacl Hist Nat, WS, Obispo 61,Plaza Armas, Havana 10100, Cuba. NR 19 TC 7 Z9 7 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 AUG 11 PY 2003 VL 116 IS 2 BP 301 EP 307 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 712FJ UT WOS:000184786500004 ER PT J AU Heyer, WR Junca, FA AF Heyer, WR Junca, FA TI Leptodactylus caatingae, a new species of frog from eastern Brazil (Amphiba : Anura : Leptodactylidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new species of frog of the genus Leptodactylus is described from eastern Brazil. The new species differs little morphologically from L. latinasus, but the advertisement calls are very different. The geographic distribution of L. latinasus and the new species, together with the respective levels of differentiation of morphology and call, is mirrored in the species pair L. bufonius and L. troglodytes. Presumably the same historical event or events lead to differentiation of these species pairs. C1 Smithsonian Inst, WRH, MRC 162, Washington, DC 20013 USA. Univ Estadual Feira Santana, Dept Ciencias Biol, Lab Anim Peconhentos & Herpetol, FAJ, BR-44031460 Salvador, Brazil. RP Heyer, WR (reprint author), Smithsonian Inst, WRH, MRC 162, POB 37012, Washington, DC 20013 USA. RI Junca, Flora/I-3732-2012 OI Junca, Flora/0000-0002-7622-6968 NR 12 TC 10 Z9 15 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 AUG 11 PY 2003 VL 116 IS 2 BP 317 EP 329 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 712FJ UT WOS:000184786500006 ER PT J AU Britz, R Favorito, S Johnson, GD AF Britz, R Favorito, S Johnson, GD TI The hyopalatine arch of a 25 mm larva of Synbranchus and homology of the single pterygoid in the Synbranchidae (Teleostei : Synbranchiformes) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Identity of the single pterygoid bone in Synbranchidae is evaluated based on a 25 mm larva of Synbranchus. Two hypotheses have been proposed as to its homology: it is 1) the endopterygoid or 2) the ectopterygoid. We show that the bone in question develops in the position of the ectopterygoid and therefore represents the homologue of this bone in other teleosts. Thus synbranchids lack the endopterygoid, an observation that invalidates a previously proposed synapomorphy of this family and the channids (snakeheads). C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, RB, Washington, DC 20560 USA. Univ Tubingen, Lehrstuhl Spezielle Zool, D-72076 Tubingen, Germany. Univ Sao Paulo, Museu Zool, BR-04299970 Sao Paulo, SP, Brazil. Smithsonian Inst, Museum Natl Hist Nat, Div Fishes, GDJ, Washington, DC 20560 USA. RP Britz, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, RB, Washington, DC 20560 USA. EM britz.ralf@nmnh.si.edu; favorito@uniban.br; johnson.dave@nmnh.si.edu RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 NR 15 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 AUG 11 PY 2003 VL 116 IS 2 BP 337 EP 340 PG 4 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 712FJ UT WOS:000184786500008 ER PT J AU Lemaitre, R McLaughlin, PA AF Lemaitre, R McLaughlin, PA TI Revision of Pylopagurus and Tomopagurus (Crustacea : Decapoda : Paguridae), with descriptions of new genera and species. Addendum and taxonomic summary SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID HERMIT-CRAB; EASTERN PACIFIC; ANOMURA; GENUS; MCLAUGHLIN AB The discovery of two new species, Enallopagurus provenzanoi, and Enallopaguropsis williamsi, has required an addendum and concluding part to the revisionary study of the "Pylopagurus-Tomopagurus" group of genera. The diagnoses of Enallopagurus McLaughlin and Enallopaguropsis McLaughlin, are emended, and a corrected key to the genera is provided. The discovery of additional specimens of Phimochirus randalli (Provenzano) from the Gulf of Mexico has provided supplemental information on the morphology, color, and distribution of this uncommon species; it is rediagnosed and illustrated. Also provided is a summary of the original taxonomic assignments in part 1 (published in 1981) of this revisionary study, and the subsequent changes, corrections, deletions, and additions that have occurred since then. An updated list of the 13 genera, two subgenera, and 64 valid species currently recognized in the "Pylopagurus-Tomopagurus" group, is presented. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 56 TC 6 Z9 7 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 AUG 11 PY 2003 VL 116 IS 2 BP 464 EP 486 PG 23 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 712FJ UT WOS:000184786500016 ER PT J AU Di Matteo, T Croft, RAC Springel, V Hernquist, L AF Di Matteo, T Croft, RAC Springel, V Hernquist, L TI Black hole growth and activity in a Lambda cold dark matter universe SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : evolution; galaxies : nuclei; methods : numerical ID HIGH-REDSHIFT QUASARS; DIGITAL SKY SURVEY; PARTICLE HYDRODYNAMICS SIMULATIONS; LUMINOSITY FUNCTION; GALACTIC NUCLEI; GALAXY FORMATION; STAR-FORMATION; VELOCITY DISPERSION; COSMOLOGICAL SIMULATIONS; EVOLUTION AB The observed properties of supermassive black holes suggest a fundamental link between their assembly and the formation of their host spheroids. We model the growth and activity of black holes in galaxies using Lambda cold dark matter cosmological hydrodynamic simulations by following the evolution of the baryonic mass component in galaxy potential wells. We find that the observed steep relation between black hole mass and spheroid velocity dispersion, M-BH proportional to sigma(4), is reproduced if the gas mass in bulges is linearly proportional to the black hole mass. To a good approximation, this is equivalent to assuming the conversion of a fixed fraction of gas mass into black hole mass. In this model, star formation and supernova feedback in the gas are sufficient for regulating and limiting the growth of the central black hole and of its gas supply. Black hole growth saturates because of the competition with star formation and, in particular, feedback, both of which determine the gas fraction available for accretion. Unless other processes also operate, we predict that the M-BH-sigma relation is not set in primordial structures but is fully established at low redshifts, z less than or similar to 2, and is shallower at earlier times. Once this relation is established, we find that central black hole masses are related to their dark matter halos simply via M-BH approximate toproportional to M-DM(4/3). We assume that galaxies undergo a quasar phase with a typical lifetime, t(Q) similar to 2 x 10(7) yr, the only free parameter of the model, and show that star formation - regulated depletion of gas in spheroids is sufficient to explain, for the most part, the decrease of the quasar population at redshift z < 3 in the optical blue band. However, with the simplest assumption of a redshift-independent quasar lifetime, the model slightly over-predicts optical quasar numbers at high redshifts, although it yields the observed evolution of number density of X-ray - faint quasars over the whole redshift range 1 < z < 6. Finally, we find that the majority of black hole mass is assembled in galaxies by z &SIM; 3 and that the black hole accretion rate density peaks in rough correspondence to the star formation rate density at z &SIM; 4-5. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Matteo, T (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. RI Croft, Rupert/N-8707-2014; Di Matteo, Tiziana/O-4762-2014 OI Croft, Rupert/0000-0003-0697-2583; Di Matteo, Tiziana/0000-0002-6462-5734 NR 61 TC 109 Z9 109 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 AUG 10 PY 2003 VL 593 IS 1 BP 56 EP 68 DI 10.1086/376501 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 708TN UT WOS:000184585600005 ER PT J AU Hardcastle, MJ Worrall, DM Kraft, RP Forman, WR Jones, C Murray, SS AF Hardcastle, MJ Worrall, DM Kraft, RP Forman, WR Jones, C Murray, SS TI Radio and X-ray observations of the jet in Centaurus A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Centaurus A; NGC 5128); galaxies : nuclei; radio continuum : galaxies; X-rays : galaxies ID HIGH-RESOLUTION; M87 JET; CHANDRA OBSERVATIONS; GALAXY 3C-31; 3C 66B; EMISSION; DISCOVERY; NGC-5128; MOTIONS; NUCLEUS AB We present new, high dynamic range VLA images of the inner jet of the closest radio galaxy, Centaurus A. Over a 10 yr baseline we detect apparent subluminal motions (v similar to 0.5c) in the jet on scales of hundreds of parsecs. The inferred speeds are larger than those previously determined using VLBI on smaller scales and provide new constraints on the angle made by the jet to the line of sight if we assume jet-counterjet symmetry. The new images also allow us to detect faint radio counterparts to a number of previously unidentified X-ray knots in the inner part of the jet and counterjet, showing conclusively that these X-ray features are genuinely associated with the outflow. However, we find that the knots with the highest X-ray/radio flux density ratios do not have detectable proper motions, suggesting that they may be related to standing shocks in the jet; we consider some possible internal obstacles that the jet may encounter. Using new, high-resolution Chandra data, we discuss the radio to X-ray spectra of the jet and the discrete features that it contains, and we argue that the compact radio and X-ray knots are privileged sites for the in situ particle acceleration that must be taking place throughout the jet. We show that the offsets observed between the peaks of the radio and X-ray emission at several places in the Cen A jet are not compatible with the simplest possible models involving particle acceleration and downstream advection together with synchrotron and expansion losses. C1 Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hardcastle, MJ (reprint author), Univ Bristol, Dept Phys, Tyndall Ave, Bristol BS8 1TL, Avon, England. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 34 TC 135 Z9 135 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 2003 VL 593 IS 1 BP 169 EP 183 DI 10.1086/376519 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 708TN UT WOS:000184585600013 ER PT J AU Kempner, JC Sarazin, CL Markevitch, M AF Kempner, JC Sarazin, CL Markevitch, M TI Chandra observation of the merging cluster A2034 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : individual (A2034); intergalactic medium; shock waves; X-rays : galaxies : clusters ID COLD-FRONT; INTERGALACTIC MEDIUM; GALAXY CLUSTERS; MAGNETIC-FIELD; ACO CLUSTERS; TEMPERATURE; A3667; CONDUCTION; PROFILES; MERGER AB We present an analysis of a Chandra observation of A2034. The cluster has multiple signatures of an ongoing merger, including a cold front and probable significant heating of the intracluster medium above its equilibrium temperature. We find no evidence for the large cooling rate previously determined for the cluster and, in fact, find it to be roughly isothermal, although with numerous small-scale inhomogeneities, out to a radius of similar to700 kpc. The cold front appears to be in the process of being disrupted by gasdynamic instability and perhaps by shock heating. We find weak evidence for inverse Compton hard X-ray emission from the radio relic suspected to be associated with the cold front. Finally, we study the emission to the south of the cluster, which was previously thought to be a merging subcluster. We find no evidence that this "subcluster'' is interacting with the main A2034 cluster. On the other hand, the properties of this region are inconsistent with an equilibrium cluster at the redshift of A2034 or less. We explore the possibility that it is a disrupted merging subcluster but find its luminosity to be significantly lower than expected for such a scenario. We suggest that the emission to the south of the cluster may actually be a moderate to high redshift (0.3 less than or similar to z less than or similar to 1.25) background cluster seen in projection against A2034. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kempner, JC (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. NR 25 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2003 VL 593 IS 1 BP 291 EP 300 DI 10.1086/376358 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 708TN UT WOS:000184585600021 ER PT J AU McClintock, JE Narayan, R Garcia, MR Orosz, JA Remillard, RA Murray, SS AF McClintock, JE Narayan, R Garcia, MR Orosz, JA Remillard, RA Murray, SS TI Multiwavelength spectrum of the black hole XTE J1118+480 in quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; black hole physics; stars : individual (A0620-00, XTE J1118+480); X-rays : stars ID ADVECTION-DOMINATED ACCRETION; X-RAY TRANSIENTS; NOVA MUSCAE 1991; BROAD-BAND SPECTRUM; STREAM-DISK IMPACT; XTE J1118+480; CATACLYSMIC VARIABLES; INTERACTING BINARIES; 2 DIMENSIONS; FLOWS AB We present an X-ray/UV/optical spectrum of the black hole primary in the X-ray nova XTE J1118+480 in quiescence at L-X approximate to 4 x 10(-9) L-Edd. The Chandra, Hubble Space Telescope, and Multiple Mirror Telescope spectroscopic observations were performed simultaneously on 2002 January 12 UT. Because this 4.1 hr binary is located at b = 62degrees, the transmission of the interstellar medium is very high (e.g., 70% at 0.3 keV). We present many new results for the quiescent state, such as the first far-UV spectrum and evidence for a 0.35 mag orbital modulation in the near-UV flux. However, the centerpiece of our work is the multiwavelength spectrum of XTE J1118+480, which we argue represents the canonical spectrum of a stellar-mass black hole radiating at L-X similar to 10(-8.5) L-Edd. This spectrum is composed of two apparently disjoint components: a hard X-ray spectrum with a photon index Gamma = 2.02 +/- 0.16 and an optical/UV continuum that resembles a 13,000 K disk blackbody spectrum punctuated by several strong emission lines. We present a model of the source in which the accretion flow has two components: (1) an X-ray-emitting interior region where the flow is advection-dominated and (2) a thin exterior accretion disk with a truncated inner edge (R-tr similar to 10(4) Schwarzschild radii) that is responsible for the optical/UV spectrum. For D = 1.8 kpc, the luminosity of the X-ray component is L-X approximate to 3.5 x 10(30) ergs s(-1) (0.3-7 keV); the bolometric luminosity of the optical/UV component is approximate to20 times greater. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jmcclintock@cfa.harvard.edu; rnarayan@cfa.harvard.edu; mgarcia@cfa.harvard.edu; orosz@zwartgat.sdsu.edu; rr@space.mit.edu; smurray@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 99 TC 74 Z9 74 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 AUG 10 PY 2003 VL 593 IS 1 BP 435 EP 451 DI 10.1086/376406 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 708TN UT WOS:000184585600034 ER PT J AU Lazendic, JS Slane, PO Gaensler, BM Plucinsky, PP Hughes, JP Galloway, DK Crawford, F AF Lazendic, JS Slane, PO Gaensler, BM Plucinsky, PP Hughes, JP Galloway, DK Crawford, F TI X-ray observations of the compact central object in supernova remnant G347.3-0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G347.3-0.5); pulsars : individual (PSR J1713-3945); stars : neutron; supernova remnants; X-rays : stars ID QUIET NEUTRON-STAR; MILLISECOND PULSATIONS; MAGNETIC-FIELDS; RADIO; EMISSION; ROSAT AB We present Chandra, XMM-Newton, and Rossi X-Ray Timing Explorer observations of 1WGA J1713.4-3949, a compact source at the center of the Galactic supernova remnant (SNR) G347.3-0.5. The X-ray spectrum of the source is well fitted by the sum of a blackbody component with a temperature of similar to0.4 keV plus a power-law component with a photon index of similar to4. We found no pulsations down to 4% in the 0.01-0.16 Hz range nor down to 25% in the 0.01-128 Hz range. This source resembles other compact central objects in SNRs, and we suggest that 1WGA J1713.4-3949 is the associated neutron star for G347.3-0.5. We also measured the properties of the adjacent radio pulsar PSR J1713-3945 with a 392 ms period, and we show that it is not associated with 1WGA J1713.4-3949 nor, most probably, is it associated with SNR G347.3-0.5. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. RP Lazendic, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jlazendic@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Galloway, Duncan/0000-0002-6558-5121; Gaensler, Bryan/0000-0002-3382-9558 NR 22 TC 34 Z9 34 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 10 PY 2003 VL 593 IS 1 BP L27 EP L30 DI 10.1086/378183 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 708TR UT WOS:000184585900007 ER PT J AU Duncan, BN Bey, I Chin, M Mickley, LJ Fairlie, TD Martin, RV Matsueda, H AF Duncan, BN Bey, I Chin, M Mickley, LJ Fairlie, TD Martin, RV Matsueda, H TI Indonesian wildfires of 1997: Impact on tropospheric chemistry SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Review DE Indonesia; biomass burning; wildfires; aerosols; radiative forcing; long-range transport ID GROUND-BASED OBSERVATIONS; BIOMASS BURNING SMOKE; LONG-RANGE TRANSPORT; 1997-1998 EL-NINO; CARBON-MONOXIDE; FOREST-FIRES; OPTICAL-PROPERTIES; TOMS MEASUREMENTS; DEEP CONVECTION; MAUNA-LOA AB The Indonesian wildfires of 1997 released large amounts of trace gases and aerosols (e.g., similar to130 Tg of carbon monoxide (CO)) from September to November. Using the GEOS-CHEM model of tropospheric chemistry and transport, we conducted a study of this burning event, including sensitivity simulations, to estimate the impacts of the trace gas and aerosol emissions on tropospheric chemistry. The emissions from the fires were estimated using the Total Ozone Mapping Spectrometer (TOMS) Aerosol Index (AI) data product and fire-count data from the Along Track Scanning Radiometer (ATSR) World Fire Atlas as surrogates for biomass burning. The model captures most of the daily variations of CO and ozone (O-3) observed in the region affected by the pollution. Export of the pollution from the Indonesian region was primarily in the prevailing easterlies in the free troposphere to the tropical Indian Ocean where the bulk of the pollution lay between 20degreesN to 20degreesS from September to November. The model's tropospheric CO and O3 columns were elevated by more than 50% and 10%, respectively, over the tropical Indian Ocean in a simulation with emissions from the fires relative to a simulation without the emissions. Another important export pathway was to the tropical and subtropical South Pacific Ocean in the southern subtropical jet. A more episodic pathway occurred to the tropics and subtropics of the North Pacific Ocean. By December, the tropospheric CO column from the fires had mixed zonally and somewhat symmetrically about the equator impacting both the Northern and Southern Hemisphere similarly. The model's CO column was elevated by 10-20% from 30degreesN to 45degreesS in December, by 5-10% poleward of 45degreesS, and by less than 5% poleward of 45degreesN. The relative impact of the fires was lower in the Northern Hemisphere, as the background CO column is typically higher there. The fires decreased the concentration of the hydroxyl radical (OH) in the model by more than 20% over much of the tropical Indian Ocean through consumption by CO, heterogeneous loss of odd-oxygen radicals (HOx) on black (BC) and organic carbon (OC) aerosols, and reduction of UV light by the aerosols. The net direct, shortwave radiative forcing at the top of the atmosphere of OC and BC aerosols from the fires was relatively small, as their forcings were similar, but of opposite signs. The net forcing at the surface, however, was large, about -10 W m(-2) over most of the tropical Indian Ocean and as low as -150 W m(-2) over the burning regions in Indonesia, indicating that aerosols from the fires significantly perturbed the tropical radiative budget. The calculated forcing of O3 was minor relative to those of BC and OC aerosols. C1 Ecole Polytech Fed Lausanne, Lab Modelisat Chim Atmospher, CH-1015 Lausanne, Switzerland. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23665 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Meteorol Res Inst, Geochem Res Dept, Tsukuba, Ibaraki 3050052, Japan. RP Duncan, BN (reprint author), Ecole Polytech Fed Lausanne, Lab Modelisat Chim Atmospher, CH-1015 Lausanne, Switzerland. EM bryan.duncan@epfl.ch; isabelle.bey@epfl.ch; chin@rondo.gsfc.nasa.gov; ljm@io.harvard.edu; tdf@io.harvard.edu; rvmartin@fas.harvard.edu; hmatsued@mri-jma.go.jp RI Martin, Randall/A-2051-2008; Duncan, Bryan/A-5962-2011; Chin, Mian/J-8354-2012; Mickley, Loretta/D-2021-2012; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Mickley, Loretta/0000-0002-7859-3470; Martin, Randall/0000-0003-2632-8402; NR 123 TC 79 Z9 80 U1 0 U2 19 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 AUG 7 PY 2003 VL 108 IS D15 AR 4458 DI 10.1029/2002JD003195 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 712PK UT WOS:000184805900004 ER PT J AU Britz, R Bartsch, P AF Britz, R Bartsch, P TI The myth of dorsal ribs in gnathostome vertebrates SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE dorsal ribs; ventral ribs; polypterids; gnathostomes ID INTERRELATIONSHIPS AB Traditionally, two types of rib are distinguished in gnathostomes: dorsal (upper) and ventral (lower, pleural) ribs. They are defined according to their position in the connective tissue system of the body: dorsal ribs develop at the intersection of the serially arranged myosepta with the horizontal septum that separates epaxial from hypaxial musculature, whereas ventral ribs develop at the intersection of myosepta with the peritoneum and usually encircle the body cavity. Distribution of rib types among gnathostomes has traditionally been reported as follows: elasmobranchs have dorsal ribs; all Actinopterygii have only ventral ribs with the exception of polypterids, and two subgroups of teleosts, which supposedly also have dorsal ribs; within Sarcopterygii tetrapods have dorsal ribs, whereas dipnoans have ventral ribs. Here, we report the development of ribs in polypterids, a taxon playing a crucial role in discussions on rib homology. We demonstrate that putative dorsal ribs of polypterids have a unique ontogeny and represent an autapomorphy of this taxon. We discuss previous hypotheses of rib homology and offer a more plausible (i.e. more parsimonious) alternative to the conventional interpretation. We conclude that dorsal ribs do not exist and that ribs of gnathostomes are ventral ribs. C1 Univ Tubingen, Lehrstuhl Spezielle Zool, D-72076 Tubingen, Germany. Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. Inst Systemat Zool, Museum Nat Kunde, D-10115 Berlin, Germany. RP Britz, R (reprint author), Univ Tubingen, Lehrstuhl Spezielle Zool, Morgenstelle 28, D-72076 Tubingen, Germany. EM britz.ralf@nmnh.si.edu; peter.bartsch@museum.hu-berlin.de NR 21 TC 7 Z9 7 U1 0 U2 4 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 2003 VL 270 SU 1 BP S1 EP S4 DI 10.1098/rsbl.2003.0035 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 712FL UT WOS:000184786900001 PM 12952620 ER PT J AU Harrison, RD AF Harrison, RD TI Fig wasp dispersal and the stability of a keystone plant resource in Borneo SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Ficus; Agaonidae; pollination; mutualism; pollen dispersal ID POLLINATING WASPS; PHYLOGENETIC-RELATIONSHIPS; EL-NINO; MUTUALISM; CONSEQUENCES; SIMULATION; EVOLUTION; DROUGHT AB The stability of interactions in remaining rainforest fragments is an issue of considerable concern for conservation. Figs are a pre-eminent tropical keystone resource because of their importance for wildlife, but are dependent on tiny (1-2 mm) species-specific wasps for pollination. To investigate fig wasp dispersal I trapped insects at various heights (5-75 m) in an isolated fragment (ca. 4500 ha) of Bornean rain forest. Fig wasps constituted the majority of captures above the canopy (pollinators 47%, non-pollinators 5%). However, genera were not evenly represented. There were 50% more species of monoecious fig pollinator than there were host species in the fragment, indicating some must have arrived from forests with different assemblages of figs at least 30 km away. Dioecious fig pollinators were poorly represented suggesting more limited dispersal, which could account for higher endemism and vulnerability to catastrophic disturbance in these figs. Diurnal activity and flight height also varied among genera. Most non-pollinating fig wasps were very rare. C1 Kyoto Univ, Ctr Ecol Res, Otsu, Shiga 5202113, Japan. RP Harrison, RD (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM harrisonr@tivoli.si.edu NR 21 TC 46 Z9 48 U1 2 U2 30 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 2003 VL 270 SU 1 BP S76 EP S79 DI 10.1098/rsbl.2003.0018 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 712FL UT WOS:000184786900023 PM 12952642 ER PT J AU Jennions, MD Backwell, PRY Murai, M Christy, JH AF Jennions, MD Backwell, PRY Murai, M Christy, JH TI Hiding behaviour in fiddler crabs: how long should prey hide in response to a potential predator? SO ANIMAL BEHAVIOUR LA English DT Article ID ANTIPREDATORY BEHAVIOR; EUMECES LATICEPS; MATING-BEHAVIOR; RISK; DECISIONS; LIZARD; VULNERABILITY; COURTSHIP; PUGILATOR; REFUGE AB Do predator-prey 'waiting games' where prey hide from potential predators have inherently unstable evolutionary outcomes, making it impossible to generate quantitative predictions about hiding times? Fiddler crabs, Uca lactea perplexa, respond to potential predators by retreating into their burrows. Time inside the burrow during unprovoked retreats during normal activity provides a 'null model' to test whether sex, tidal cycle and body size affect hiding time from potential predators. Using experimentally created predator-like stimuli we found that males hid for significantly longer than females, and larger crabs of both sexes also hid for longer. This differs from burrow use during unprovoked retreats, suggesting hiding time varies depending on the potential risk of predation on re-emergence. If risk prior to hiding predicts risk on emergence, the closer the proximity of a predator-like stimulus when first encountered the longer crabs should hide. We confirmed this experimentally (stimuli at 0.5 versus 2.5 m). Finally, we tested whether males hide for longer when a predator-like stimulus approaches them directly rather than tangentially. None of three pairwise comparisons was statistically significant, but crabs hid less as the angle of approach became more tangential. These results suggest prey can use stimuli prior to hiding to predict predation risk on re-emergence, but studies on predators are required to test this claim. Finally, theoretical models must explain why hiding time has a lognormal distribution and low variance such that a predator can predict when most prey will re-emerge. For example, 95% of crabs re-emerged within 2.3 min of hiding. (C) 2003 Published by Elsevier Ltd on behalf of The Association for the Study of Animal Behaviour. C1 Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. Univ Ryukyus, Trop Biosphere Res Ctr, Okinawa 90502, Japan. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Jennions, MD (reprint author), Australian Natl Univ, Sch Bot & Zool, GPO Box 4, Canberra, ACT 0200, Australia. RI Jennions, Michael/C-7560-2009; Backwell, Patricia/C-8883-2009 OI Jennions, Michael/0000-0001-9221-2788; NR 36 TC 45 Z9 45 U1 1 U2 24 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD AUG PY 2003 VL 66 BP 251 EP 257 DI 10.1006/anbe.2003.2190 PN 2 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 714EP UT WOS:000184899600007 ER PT J AU Bloomsmith, MA Tarou, LR Lambeth, SP Haberstroh, MD AF Bloomsmith, MA Tarou, LR Lambeth, SP Haberstroh, MD TI Maternal response to mother-offspring separation in the chimpanzee (Pan troglodytes) SO ANIMAL WELFARE LA English DT Article DE animal welfare; behavioural management; chimpanzees; despair; protest; social separation ID INFANT SQUIRREL-MONKEYS; RHESUS; ENVIRONMENT; DEPRESSION; TERM AB For management and/or research purposes, chimpanzee mothers and their offspring are Often physically separated from one another at an earlier age than they would be in the wild. Studies of the behavioural and physiological effects of mother-infant separation on infant behaviour have been conducted in both human and nonhuman primates. However, few studies have been conducted to examine the response of the mother to separation from her infant, particularly in great apes. The current study opportunistically examined the response of twelve chimpanzee mothers to separation from 15 of their offspring ranging from 1.8 to 5.4 years of age. Behavioural data (proximity of the mother to other group members, and fifteen behaviours representing six categories [agonistic, prosocial, vocalisations, abnormal, locomotor, inactive]) were collected for three weeks prior to and three to five weeks following the permanent removal of the offspring from their mothers. A repeated measures MANOVA conducted on all subjects revealed no significant change in behaviour following separation. There was a significant increase in inactivity following separation of the offspring (F-2.21 = 5.47, P < 0.05) in a subgroup of mothers (n = 8) that was studied more intensively on the first day of separation. Maternal age, infant age, presence of other offspring, and past experience with mother-offspring separation had no effect on response to separation. These results contradict those of mother-infant separation studies in monkeys and indicate that most behavioural indicators of well-being are stable in chimpanzee mothers that remain in their familiar environment and social group following offspring separation. C1 TECHlab, Zoo Atlanta, Atlanta, GA 30315 USA. Emory Univ, Yerkes Natl Primate Res Ctr, Atlanta, GA 30329 USA. Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA. Univ Texas, MD Anderson Canc Ctr, Dept Vet Sci, Bastrop, TX 78602 USA. RP Bloomsmith, MA (reprint author), TECHlab, Zoo Atlanta, 800 Cherokee Ave SE, Atlanta, GA 30315 USA. NR 27 TC 0 Z9 0 U1 3 U2 6 PU UNIV FEDERATION ANIMAL WELFARE PI WHEATHAMPSTEAD PA OLD SCHOOL, BREWHOUSE HILL, WHEATHAMPSTEAD AL4 8AN, HERTS, ENGLAND SN 0962-7286 J9 ANIM WELFARE JI Anim. Welf. PD AUG PY 2003 VL 12 IS 3 BP 359 EP 368 PG 10 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 702GB UT WOS:000184215200006 ER PT J AU Schild, R Vakulik, V AF Schild, R Vakulik, V TI Microlensing of a ring model for quasar structure SO ASTRONOMICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (QSO 0957+561) ID GRAVITATIONALLY LENSED QUASAR; Q0957+561 TIME-DELAY; CLOCK OBSERVATIONS; VARIABILITY; STARS; A,B AB Microlensing observations of QSO 0957+561A and QSO 0957+561B have consistently shown evidence for structure in the quasar that has not been evident in available microlensing models, where the luminous source has been consistently modeled as a single large, round structure. We show that the microlensing features can easily be reproduced by a luminous quasar model motivated by observations: a luminous inner accretion disk edge and outer ring-shaped structures where the emission lines form. Such a model can explain all of the features known from 24 years of QSO 0957+561 microlensing observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Kharkov Natl Univ, Inst Astron, UA-61022 Kharkov, Ukraine. RP Schild, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 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 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2003 VL 126 IS 2 BP 689 EP 695 DI 10.1086/376472 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706GU UT WOS:000184446600007 ER PT J AU Dobrzycki, A Stanek, KZ Macri, LM Groot, PJ AF Dobrzycki, A Stanek, KZ Macri, LM Groot, PJ TI New X-ray quasars behind the Small Magellanic Cloud SO ASTRONOMICAL JOURNAL LA English DT Article DE Magellanic Clouds; quasars : general ID GRAVITATIONAL LENSING EXPERIMENT; VARIABILITY-SELECTED QUASARS; ACTIVE GALACTIC NUCLEI; SEYFERT 1 GALAXIES; HEAVY-ELEMENTS; SMC REGION; DISTANCE; CATALOG; SPECTRA; ASCA AB We present five X-ray quasars behind the Small Magellanic Cloud, increasing the number of known quasars behind the SMC by similar to40%. They were identified via follow-up spectroscopy of serendipitous sources from the Chandra X-Ray Observatory matched with objects from the OGLE database. All quasars lie behind dense parts of the SMC and could be very useful for proper-motion studies. We analyze X-ray spectral and timing properties of the quasars. We discuss applications of those and other recently discovered quasars behind the SMC to the studies of absorption properties of the Cloud, its proper motion, and for establishing the geometrical distance to the SMC. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. RP Dobrzycki, A (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. RI Groot, Paul/K-4391-2016 OI Groot, Paul/0000-0002-4488-726X NR 32 TC 10 Z9 10 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2003 VL 126 IS 2 BP 734 EP 741 DI 10.1086/376740 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706GU UT WOS:000184446600011 ER EF