FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Adams, RM AF Adams, RM TI Catastrophe & culture - The anthropology of disaster SO SCIENCE LA English DT Book Review C1 Univ Calif San Diego, Dept Anthropol, La Jolla, CA 92093 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Adams, RM (reprint author), Univ Calif San Diego, Dept Anthropol, 9500 Gilman Dr, La Jolla, CA 92093 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAY 24 PY 2002 VL 296 IS 5572 BP 1404 EP 1405 DI 10.1126/science.1072171 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 557LP UT WOS:000175910300026 ER PT J AU Simmons, RB Weller, SJ AF Simmons, RB Weller, SJ TI What kind of signals do mimetic tiger moths send? A phylogenetic test of wasp mimicry systems (Lepidoptera : Arctiidae : Euchromiini) SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE comparative biology; Arctiinae; Mullerian mimicry; evolution of mimicry ID MULLERIAN MIMICRY; HELICONIUS BUTTERFLIES; MUELLERIAN MIMICRY; SEQUENCE DATA; EVOLUTION; PERMUTATION; ADAPTATION; DIVERSITY; PREDATOR; DYNAMICS AB Mimicry has been examined in field and laboratory studies of butterflies and its evolutionary dynamics have been explored in computer simulations. Phylogenetic studies examining the evolution of mimicry, however, are rare. Here, the phylogeny of wasp-mimicking tiger moths, the Sphecosoma group, was used to test evolutionary predictions of computer simulations of conventional Mullerian mimicry and quasi-Batesian mimicry dynamics. We examined whether mimetic traits evolved individually, or as suites of characters, using concentrated change tests. The phylogeny of these moth mimics revealed that individual mimetic characters were conserved, as are the three mimetic wasp forms: yellow Polybia, black Polybia and Parachartergus mimetic types. This finding was consistent with a 'supergene' control of linked loci and the Nicholson two-step model of mimicry evolution. We also used a modified permutation-tail probability approach to examine the rate of mimetic-type evolution. The observed topology, hypothetical Mullerian and Batesian scenarios, and 1000 random trees were compared using Kishino-Hasegawa tests. The observed phylogeny was more consistent with the predicted Mullerian distribution of mimetic traits than with that of a quasi-Batesian scenario. We suggest that the range of discriminatory abilities of the predator community plays a key role in shaping mimicry dynamics. C1 Univ Minnesota, Dept Entomol, St Paul, MN 55016 USA. Univ Minnesota, JF Bell Museum Nat Hist, St Paul, MN 55016 USA. RP Simmons, RB (reprint author), USDA ARS, PSI, Systemat Entomol Lab, Smithsonian Inst,NMNH, Room E-525,0168, Washington, DC 20013 USA. EM rsimmons@sel.barc.usda.gov NR 53 TC 15 Z9 15 U1 0 U2 11 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 MAY 22 PY 2002 VL 269 IS 1495 BP 983 EP 990 DI 10.1098/rspb.2002.1970 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 556AW UT WOS:000175826100001 PM 12028753 ER PT J AU Weinberg, DH Hernquist, L Katz, N AF Weinberg, DH Hernquist, L Katz, N TI High-redshift galaxies in cold dark matter models SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies : evolution; galaxies : formation; large-scale structure of universe; stars : formation ID LYMAN-BREAK GALAXIES; HUBBLE DEEP FIELD; LY-ALPHA FOREST; STAR-FORMATION HISTORY; MICROWAVE BACKGROUND ANISOTROPIES; SMOOTHED PARTICLE HYDRODYNAMICS; ULTRAVIOLET LUMINOSITY DENSITY; LARGE-SCALE STRUCTURE; MASS FLUCTUATIONS; POWER SPECTRUM AB We use hydrodynamic cosmological simulations to predict the star formation properties of high-redshift galaxies (z = 2-6) in five variants of the inflationary cold dark matter scenario, paying particular attention to z = 3, the redshift of the largest Lyman break galaxy (LBG) samples. Because we link the star formation timescale to the local gas density, the rate at which a galaxy forms stars is governed mainly by the rate at which it accretes cooled gas from the surrounding medium. At z = 3, star formation in most of the simulated galaxies is steady on similar to200 Myr timescales, and the instantaneous star formation rate (SFR) is correlated with total stellar mass. However, there is enough scatter in this correlation that a sample selected above a given SFR threshold may contain galaxies with a fairly wide range of masses. The redshift history and global density of star formation in the simulations depend mainly on the amplitude of mass fluctuations in the underlying cosmological model. The three models whose mass fluctuation amplitudes agree with recent analyses of the Lyalpha forest also reproduce the observed luminosity function of LBGs reasonably well, although the dynamic range of the comparison is small and the theoretical and observational uncertainties are large. The models with higher and lower amplitudes appear to predict too much and too little star formation, respectively, although they are not clearly ruled out. The intermediate amplitude models predict SFR 30 40 M yr(-1) for galaxies with a surface density of similar to1 arcmin(-2) per unit redshift at z = 3. They predict much higher surface densities at lower SFR, and significant numbers of galaxies with SFR > 10 M-. yr(-1) at z greater than or equal to 5. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts, Dept Phys & Astron, Amherst, MA 01003 USA. RP Weinberg, DH (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. NR 92 TC 38 Z9 38 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2002 VL 571 IS 1 BP 15 EP 29 DI 10.1086/339841 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TJ UT WOS:000175519000002 ER PT J AU Norman, C Hasinger, G Giacconi, R Gilli, R Kewley, L Nonino, M Rosati, P Szokoly, G Tozzi, P Wang, JX Zheng, W Zirm, A Bergeron, J Gilmozzi, R Grogin, N Koekemoer, A Schreier, E AF Norman, C Hasinger, G Giacconi, R Gilli, R Kewley, L Nonino, M Rosati, P Szokoly, G Tozzi, P Wang, JX Zheng, W Zirm, A Bergeron, J Gilmozzi, R Grogin, N Koekemoer, A Schreier, E TI A classic type 2 QSO SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars : emission lines; quasars : individual (CXOCDFS J033229.9-275106); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; REDSHIFT RADIO GALAXIES; DEEP FIELD-SOUTH; X-RAY SOURCES; SEYFERT-GALAXIES; QUASAR; EMISSION; CHANDRA; EVOLUTION; SPECTRA AB In the Chandra Deep Field South 1 Ms exposure, we have found, at redshift 3.700 +/- 0.005, the most distant type 2 active galactic nucleus ever detected. It is the source with the hardest X-ray spectrum with redshift z > 3. The optical spectrum has no detected continuum emission to a 3 detection limit of 3 10 19 ergs s(-1) cm(-2) Angstrom(-1) and shows narrow lines of Lyalpha, C IV N v He II O vI [O III], and C III]. Their FWHM line widths have a range of similar to700-2300 km s(-1) with an average of approximately similar to1500 km s(-1). The emitting gas is metal-rich (Z similar or equal to 2.5-3 Z(.)). In the X-ray spectrum of 130 counts in the 0.5-7 keV band, there is evidence for intrinsic absorption with N-H greater than or similar to 10(24) cm(-2). An iron Kalpha line with rest-frame energy and equivalent width of similar to6.4 keV and similar to1 keV, respectively, in agreement with the obscuration scenario, is detected at a 2sigma level. If confirmed by our forthcoming XMM-Newton observations, this would be the highest redshift detection of Fe Kalpha. Depending on the assumed cosmology and the X-ray transfer model, the 2-10 keV rest frame luminosity corrected for absorption is similar to10(45 +/- 0.5) ergs cm(-2) s(-1), which makes our source a classic example of the long-sought type 2 QSO. From standard population synthesis models, these sources are expected to account for a relevant fraction of the black hole powered QSO distribution at high redshift. C1 Johns Hopkins Univ, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Associated Univ Inc, Washington, DC 20036 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Trieste, I-34131 Trieste, Italy. European So Observ, D-85748 Garching, Germany. RP Norman, C (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA. RI Gilli, Roberto/P-1110-2015; OI Gilli, Roberto/0000-0001-8121-6177; Nonino, Mario/0000-0001-6342-9662; Koekemoer, Anton/0000-0002-6610-2048 NR 59 TC 201 Z9 201 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2002 VL 571 IS 1 BP 218 EP 225 DI 10.1086/339855 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TJ UT WOS:000175519000013 ER PT J AU Risaliti, G Elvis, M Nicastro, F AF Risaliti, G Elvis, M Nicastro, F TI Ubiquitous variability of X-ray absorbing column densities in Seyfert 2 galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; HIGH-ENERGY SPECTRA; ASCA OBSERVATIONS; BEPPOSAX OBSERVATIONS; ESO 103-G35; CENTAURUS-A; THICK TORI; ABSORPTION; NGC-7582; EMISSION AB We present a study of the variations in the absorbing column density of 25 X-ray defined Seyfert 2 galaxies, as inferred from hard X-ray observations, on timescales from months to several years. We show that a significant variation of N-H (from 20% to 80%) is observed in almost all ( 22 of 25) of the sources with multiple X-ray observations, although X-ray absorption never vanishes. For a subsample of 11 sources observed at least five times, the typical variation time, as defined by a structure function, is less than 1 yr for both heavily absorbed (N-H similar to10(23) cm(-2)) and moderately absorbed (N-H similar to 10(22) cm(-2)) sources. These variations rule out the simplest version of the unified models, based on a homogeneous obscuring torus, and suggest the presence of clumpy circumnuclear material on a scale well below a parsec. We propose a modi cation of the torus model in which an overabundance of slightly dusty broad emission-line region (BELR) clouds obscures the BELR. The BELR needs, like the torus, to have an axisymmetric structure. This model is closely related to that of Elvis for type 1 active galactic nuclei (AGNs). For lightly obscured AGNs (N-H similar to 10(22) cm(-2)), the structure function shows an increase at a timescale of similar to5 yr, indicating a second absorber, most probably on a 5-10 pc scale associated with the host galaxy. C1 Osserv Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Risaliti, G (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. OI Risaliti, Guido/0000-0002-3556-977X; Nicastro, Fabrizio/0000-0002-6896-1364 NR 71 TC 196 Z9 196 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2002 VL 571 IS 1 BP 234 EP 246 DI 10.1086/324146 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TJ UT WOS:000175519000015 ER PT J AU Kim, S Reach, WT AF Kim, S Reach, WT TI The origin of far-infrared [C II] emission in the Large Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; infrared : galaxies; ISM : lines and bands; Magellanic Clouds; radio lines : galaxies ID 158 MICRON LINE; PHOTODISSOCIATION REGIONS; MOLECULAR CLOUDS; GAS; GALAXIES; COBE; ABUNDANCES AB We compare the distribution of H I 21 cm, H II 6563 Angstrom, and [C II] 157.7 mum line emission over the entire Large Magellanic Cloud (LMC). Bright [C II] emission is associated with H II regions and their surroundings, with a good correlation between [C II] and Halpha laments. Faint [C II] emission is also detected in regions with no H II emission. We found a reasonably good correlation between the extended [C II] emission and H I emission. Using the slope of the [C II] versus H I correlation in regions with low Halpha brightness, 4piI(C II)/N (H) I = 6.0 +/- 3.0 x 10(-26) ergs s(-1) ( H atom)(-1), and the total H I column density away from H II regions, the luminosity of [C II] from the atomic medium is 1.14 +/- 0.57 x 10(6) L-., which amounts to 20% of the total [ C ii luminosity from the LMC. The [ C ii emission per unit H I column density from the atomic regions of the LMC is similar to, but somewhat higher than, that in the Milky Way, because of the cancelling effects of lower C abundance and higher radiation field in the LMC. Significant deviations between the H I and [ C ii in some regions suggest that part of the [ C ii emission comes from ionized regions. Subtracting the contribution to the [ C II] luminosity from bright H II regions, an upper limit of 46% of the [ C II] luminosity could be due to diffuse ionized gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, SIRTF Sci Ctr, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Kim, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Reach, William/0000-0001-8362-4094 NR 28 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2002 VL 571 IS 1 BP 288 EP 292 DI 10.1086/339936 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TJ UT WOS:000175519000021 ER PT J AU Wyithe, JSB Wilson, RE AF Wyithe, JSB Wilson, RE TI Photometric solutions for semidetached eclipsing binaries: Selection of distance indicators in the Small Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; distance scale; Magellanic Clouds ID STAR LIGHT; CURVES; MODELS AB Estimation of distances to nearby galaxies by the use of eclipsing binaries as standard candles has recently become feasible because of new large-scale instruments and the discovery of thousands of eclipsing binaries as spin-off from Galactic microlensing surveys. Published measurements of distances to detached eclipsing binaries in the Large Magellanic Cloud combine stellar surface areas ( in absolute units) determined from photometric light and radial velocity curves with surface brightnesses from model atmospheres and observed spectra. The method does not require the stars to be normal or undistorted and is not limited in its applicability to the well-detached systems that have traditionally been considered. We discuss the potential usefulness of semidetached vis a vis detached eclipsing binaries for distance determination and examine and quantify criteria for their selection from large catalogs. Following our earlier paper on detached binaries in the Small Magellanic Cloud (SMC), we carry out semidetached light-curve solutions for SMC binaries discovered by the OGLE collaboration, identify candidates for SMC distance estimation that can be targets of future high-quality observations, and tabulate results of OGLE light-curve solutions. We point out that semidetached binaries have important advantages over well-detached systems as standard candles, although this idea runs counter to the usual view that the latter are optimal distance indicators. Potential advantages are that ( 1) light-curve solutions can be strengthened by exploiting lobe-filling configurations, ( 2) only single-lined spectra may be needed for radial velocities because the mass ratio can be determined from photometry in the case of complete eclipses, and ( 3) nearly all semidetached binaries have sensibly circular orbits, which is not true for detached binaries. We carry out simulations with synthetic data to see if semidetached binaries can be reliably identified and to quantify the accuracy of solutions. The simulations were done for detached as well as semidetached binaries so as to constitute a proper controlled study. The simulations demonstrate two additional advantages for semidetached distance determination candidates; ( 4) the well-known difficulty in distinguishing solutions with interchanged radii ( aliasing) is much less severe for semidetached than for detached binaries and ( 5) the condition of complete eclipse ( which removes a near degeneracy between inclination and the ratio of the radii) is identified with improved reliability. In many cases we find that parameters are accurately determined ( e. g., relative errors in radii smaller than 10%) and that detached and semidetached systems can be distinguished. We select 36 candidate semidetached systems ( although seven of these are doubtful because of large mass ratios or periods) from the OGLE SMC eclipsing binary catalog. We expected that most semidetached candidates would have light curves similar to those of common Algol binaries, but that turned out not to be the case, and we note that fully Algol-like light curves are nearly absent in the OGLE sample. We discuss possible explanations for the near absence of obvious Algols in OGLE, including whether their paucity is real or apparent. C1 Princeton Univ Observ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. RP Wyithe, JSB (reprint author), Princeton Univ Observ, Peyton Hall, Princeton, NJ 08544 USA. OI Wyithe, Stuart/0000-0001-7956-9758 NR 28 TC 38 Z9 38 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2002 VL 571 IS 1 BP 293 EP 319 DI 10.1086/339877 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TJ UT WOS:000175519000022 ER PT J AU Ballesteros-Paredes, J Vazquez-Semadeni, E Goodman, AA AF Ballesteros-Paredes, J Vazquez-Semadeni, E Goodman, AA TI Velocity structure of the interstellar medium as seen by the spectral correlation function SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : kinematics and dynamics; methods : data analysis; methods : statistical turbulence ID STAR-FORMING REGIONS; MOLECULAR CLOUDS; DENSITY-FLUCTUATIONS; TURBULENT MODEL; STATISTICS; GAS; SIMULATIONS; EVOLUTION; FLOWS AB We use the statistical tool known as the "spectral correlation function" (SCF) to intercompare simulations and observations of the atomic interstellar medium ( ISM). The simulations considered, which mimic three distinct sets of physical conditions, are each calculated for a 300 pc(3) box centered at the Galactic plane. The "ISM" run is intended to represent a mixture of cool and warm atomic gas and includes self-gravity and magnetic fields in the calculations. The "ISM-IT" run is more representative of molecular clouds, in which the gas is presumed isothermal. The third run "IT" is for purely isothermal gas, with zero magnetic field and no self-gravity. Forcing in the three cases is accomplished by including simulated effects of stellar heating (ISM), stellar winds (ISM-IT), or random compressible fluctuations (IT). For each simulation, H I spectral line maps are simulated, and it is these maps that are intercompared, both with each other and with observations, using the SCF. For runs where the separation of velocity features is much greater than the "thermal" width of a line, density-weighted velocity histograms are decent estimates of H I spectra. When thermal broadening is large in comparison with fine-scale turbulent velocity structure, this broadening masks subthermal velocity substructure in observed spectra. So, simulated spectra for runs in which thermal broadening is important must be calculated by convolving density-weighted histograms with Gaussians whose width represents the thermal broadening. The H I observations we use for comparison are of the north celestial pole (NCP) loop, a region chosen to minimize line-of-sight confusion on scales greater than 100 pc. None of the simulations match the NCP loop data very well, for a variety of reasons described in the paper. Most of the reasons for simulation/observation discrepancy are predictable and understandable, but one is particularly interesting: the most realistic sets of line profiles and SCF statistics come from artificially expanding the velocity axis of the ISM run by a factor of 6. Without rescaling, the low-velocity dispersion associated with much of the gas in the ISM run causes almost all of the spectra to appear as virtually identical Gaussians whose width is determined solely by temperature-all velocity structure is smeared out by thermal broadening. However, if the velocity axis is expanded by a factor of 6, the SCF distributions of the ISM run and the NCP loop match up fairly well. This means that the ratio of thermal to turbulent pressure in the ISM simulation is much too large as it stands, and that the simulation is deficient in turbulent energy. This is a consequence of the ISM run not including the effects of supernovae. This paper concludes that the SCF is a useful tool for understanding and fine-tuning simulations of interstellar gas, and in particular that realistic simulations of the atomic ISM need to include the effects of energetic stellar winds (e. g., supernovae) in order for the ratio of thermal-to-turbulent pressure to give spectra representative of the observed ISM in our Galaxy. C1 Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Amer Museum Nat Hist, Dept Astrophys, Cent Pk W & 79th St, New York, NY 10024 USA. EM javierbp@amnh.org RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 42 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2002 VL 571 IS 1 BP 334 EP 355 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TJ UT WOS:000175519000025 ER PT J AU Belczynski, K Bulik, T Rudak, B AF Belczynski, K Bulik, T Rudak, B TI Study of gamma-ray burst binary progenitors SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; black hole physics; gamma rays : bursts; stars : evolution; stars : neutron white dwarfs ID STAR-FORMATION HISTORY; NEUTRON-STAR; BLACK-HOLE; GRB 990510; MASS-LOSS; STELLAR PARAMETERS; OPTICAL AFTERGLOW; COMPACT OBJECTS; RADIO PULSARS; I SUPERNOVAE AB Recently much work in studying gamma-ray bursts (GRBs) has been devoted to revealing the nature of outburst mechanisms and to studies of GRB afterglows. These issues have also been closely followed by the quest to identify GRB progenitors. Several types of progenitors have been proposed for GRBs: the most promising objects seem to be collapsars, compact object binaries, mergers of compact objects with helium cores of evolved stars in common envelope episodes, and also the recently discussed connection of GRBs with supernovae. In this paper we consider the binary star progenitors of GRBs: white dwarf neutron star (WD-NS) binaries, white dwarf black hole (WD-BH) binaries, helium core neutron star (He-NS) mergers, helium core black hole (He-BH) mergers, and double neutron star (NS-NS) and neutron star black hole binaries (NS-BH). Using population synthesis methods we calculate merger rates of these binary progenitors and compare them to the observed BATSE GRB rate. For the binaries considered, we also calculate the distribution of merger sites around host galaxies and compare them to the observed locations of GRB afterglows with respect to their hosts. We find that the rates of binary GRB progenitors in our standard model are lower than the observed GRB rates if GRBs are highly collimated. However, the uncertainty in the population synthesis results is too large to make this a firm conclusion. Although some observational signatures seem to point to collapsars as progenitors of long GRBs, we find that mergers of WD-NS, He-NS, He-BH, and NS-NS systems also trace the star formation regions of their host galaxies, as it is observed for long GRBs. We also speculate about possible progenitors of short-duration GRBs. For these, the most likely candidates are still mergers of compact objects. We find that the locations of NS-NS and NS-BH mergers with respect to their hosts are significantly different. This may allow us to distinguish between these two progenitor models once current and near future missions, such as HETE-2 or Swift, measure the locations of short GRBs. C1 Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd,No F325, Evanston, IL 60208 USA. EM belczynski@northwestern.edu; bulik@camk.edu.pl; bronek@ncac.torun.pl NR 75 TC 57 Z9 57 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2002 VL 571 IS 1 BP 394 EP 412 DI 10.1086/339860 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TJ UT WOS:000175519000029 ER PT J AU Protassov, R van Dyk, DA Connors, A Kashyap, VL Siemiginowska, A AF Protassov, R van Dyk, DA Connors, A Kashyap, VL Siemiginowska, A TI Statistics, handle with care: Detecting multiple model components with the likelihood ratio test SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : statistical ID GAMMA-RAY BURST; LINE SEARCH; PARAMETER-ESTIMATION; BAYES FACTORS; CANDIDATES; ABSORPTION; ASTRONOMY; SPECTRUM; FEATURES; STARS AB The likelihood ratio test (LRT) and the related F-test, popularized in astrophysics by Eadie and coworkers in 1971, Bevington in 1969, Lampton, Margon, & Bowyer, in 1976, Cash in 1979, and Avni in 1978, do not ( even asymptotically) adhere to their nominal 2 and F-distributions in many statistical tests common in astrophysics, thereby casting many marginal line or source detections and nondetections into doubt. Although the above authors illustrate the many legitimate uses of these statistics, in some important cases it can be impossible to compute the correct false positive rate. For example, it has become common practice to use the LRT or the F-test to detect a line in a spectral model or a source above background despite the lack of certain required regularity conditions. (These applications were not originally suggested by Cash or by Bevington.) In these and other settings that involve testing a hypothesis that is on the boundary of the parameter space, contrary to common practice, the nominal 2 distribution for the LRT or the F-distribution for the F-test should not be used. In this paper, we characterize an important class of problems in which the LRT and the F test fail and illustrate this nonstandard behavior. We briefly sketch several possible acceptable alternatives, focusing on Bayesian posterior predictive probability values. We present this method in some detail since it is a simple, robust, and intuitive approach. This alternative method is illustrated using the gamma-ray burst of 1997 May 8 (GRB 970508) to investigate the presence of an Fe K emission line during the initial phase of the observation. There are many legitimate uses of the LRT and the F-test in astrophysics, and even when these tests are inappropriate, there remain several statistical alternatives (e. g., judicious use of error bars and Bayes factors). Nevertheless, there are numerous cases of the inappropriate use of the LRT and similar tests in the literature, bringing substantive scientific results into question. C1 Harvard Univ, Dept Stat, Cambridge, MA 02138 USA. Eureka Sci, Oakland, CA 94602 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Protassov, R (reprint author), Harvard Univ, Dept Stat, 1 Oxford St, Cambridge, MA 02138 USA. OI Van Dyk, David/0000-0002-0816-331X NR 41 TC 343 Z9 343 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2002 VL 571 IS 1 BP 545 EP 559 DI 10.1086/339856 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TJ UT WOS:000175519000043 ER PT J AU Jayawardhana, R Luhman, KL D'Alessio, P Stauffer, JR AF Jayawardhana, R Luhman, KL D'Alessio, P Stauffer, JR TI Discovery of an edge-on disk in the MBM 12 young association SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; circumstellar matter; open clusters and associations : individual (MBM 12); stars : pre-main-sequence; techniques : high angular resolution ID OPTICAL SPECTROSCOPY; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISK; ACCRETION DISKS; MOLECULAR CLOUD; STARS; SYSTEM; MULTIPLICITY; OBJECTS; TAURI AB We report the discovery of a spatially resolved edge-on protoplanetary disk in the similar to2 Myr old MBM 12 young association. Our near-infrared images of LkHalpha 263C (MBM 12A 3C), obtained with the Hokupa' a adaptive optics system on the Gemini North telescope, clearly show two elongated reflection nebulosities separated by a dark lane, a morphology well matched by scattered-light models of an optically thick (at near-infrared wavelengths) edge-on disk. An optical spectrum of the scattered-light nebulosity obtained with the Keck II telescope exhibits a spectral type of M0 +/- 0.5 (T(eff) = 3850 +/- 100 K) for the central star and contains H and forbidden emission lines, which may indicate the presence of a jet. The absence of a near-infrared point source implies A(g) > 9.5 K toward the unseen central star. The disk is flared and has a radius of similar to150 AU (at a distance of 275 pc) and an inclination of 87degrees. The aspect ratio of the model disk in the J band is 0.72. There is possible evidence of dust settling to the disk midplane. LkHalpha 263C is 4."115 from the 0."415 binary LkHalpha 263 A and B (MBM 12A 3A and 3B), which is itself 15."5 from LkHalpha 262 (MBM 12A 2). Thus, LkHalpha 263C may be the first disk to be clearly resolved around an individual star in a young quadruple system. The detection of a faint edge-on disk near a bright star demonstrates both the high angular resolution and the high sensitivity that can be achieved with adaptive optics imaging on large telescopes. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. CALTECH, Ctr Sci, SIRTF, Pasadena, CA 91125 USA. RP Jayawardhana, R (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. NR 25 TC 34 Z9 34 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 MAY 20 PY 2002 VL 571 IS 1 BP L51 EP L54 DI 10.1086/341202 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TQ UT WOS:000175519700011 ER PT J AU Slane, PO Helfand, DJ Murray, SS AF Slane, PO Helfand, DJ Murray, SS TI New constraints on neutron star cooling from Chandra observations of 3C 58 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (3C 58); pulsars : individual (PSR J0205+6449); stars : neutron; supernova; remnants; X-rays : general ID X-RAY-EMISSION; REMNANT 3C 58; SUPERNOVA; DISCOVERY; PULSARS AB 3C 58 is a young Crab-like supernova remnant. Historical evidence strongly suggests an association of the remnant with supernova SN 1181, which would make 3C 58 younger than the Crab Nebula. Recent Chandra observations have identified the young 65 ms pulsar J0205+6449 at its center, embedded in a compact nebula that, as we show here, appears to be confined by the pulsar wind termination shock. We present new Chandra observations of this compact nebula and the embedded pulsar that set strong upper limits on the thermal emission originating from the neutron star surface. These limits fall far below predictions of standard neutron star cooling, requiring the presence of exotic cooling processes in the neutron star core. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Slane, PO (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 98 Z9 98 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 MAY 20 PY 2002 VL 571 IS 1 BP L45 EP L49 DI 10.1086/341179 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550TQ UT WOS:000175519700010 ER PT J AU Johansson, M Coats, DW AF Johansson, M Coats, DW TI Ciliate grazing on the parasite Amoebophrya sp decreases infection of the red-tide dinoflagellate Akashiwo sanguinea SO AQUATIC MICROBIAL ECOLOGY LA English DT Article DE parasitic dinoflagellate; harmful algal bloom; ciliate grazing; Amoebophrya sp.; Akashiwo sanguinea; Strobilidium sp.; Chesapeake bay ID HARMFUL ALGAL BLOOMS; CHESAPEAKE BAY; GYMNODINIUM-SANGUINEUM; PHYTOPLANKTON BLOOMS; GROWTH; RATES; POPULATIONS; REPRODUCTION; SIZE; MICROZOOPLANKTON AB Parasitic dinoflagellates of the genus Amoebophrya commonly infect free-living dinoflagellates, some of which cause toxic or otherwise harmful red tides. These parasites prevent reproduction of their hosts and kill infected cells on a time scale of days, Thus, epidemic outbreaks of Amoebophrya spp. are thought to facilitate the decline of red tides by causing mass mortality of host taxa, However, little is known about biotic and abiotic factors that regulate epidemic occurrence of Amoebophrya spp. in nature. We addressed the hypothesis that grazing by ciliate microzooplankton on the infective stage of Amoebophrya sp. can regulate parasite prevalence in the bloom-forming dinoflagellate Akashiwo sanguinea. In culture, the choreotrich ciliate Strobilidium sp. rapidly ingested and digested infective dinospores of Amoebophrya sp. ex A. sanguinea. Laboratory experiments also showed that grazing by Strobilidium sp. could decrease infection of A, sanguinea by 70 to 80% relative to controls. Field experiments using plankton assemblages from Chesapeake Bay, USA, indicated that grazing by natural populations of ciliates may contribute to the regulation of parasitism in A. sanguinea, Thus, grazing by ciliates and other microzooplankton may indirectly influence the occurrence of red tides by limiting the spread of parasites like Amoebophrya sp. C1 Univ Stockholm, Dept Syst Ecol, S-10691 Stockholm, Sweden. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Johansson, M (reprint author), Univ Stockholm, Dept Syst Ecol, Svante Arrhenius Vag 21A, S-10691 Stockholm, Sweden. NR 51 TC 28 Z9 32 U1 0 U2 6 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0948-3055 J9 AQUAT MICROB ECOL JI Aquat. Microb. Ecol. PD MAY 16 PY 2002 VL 28 IS 1 BP 69 EP 78 DI 10.3354/ame028069 PG 10 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 556RQ UT WOS:000175863100006 ER PT J AU Tait, EJ AF Tait, EJ TI Better communication is in everyone's interests - Scientists will find it's worth making the effort to explain what they're doing to the public. SO NATURE LA English DT Letter C1 Smithsonian Inst, Off Publ Affairs, Washington, DC 20560 USA. RP Tait, EJ (reprint author), Smithsonian Inst, Off Publ Affairs, 1000 Jefferson Dr SW, Washington, DC 20560 USA. NR 2 TC 1 Z9 1 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 MAY 16 PY 2002 VL 417 IS 6886 BP 221 EP 221 DI 10.1038/417221a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 551YT UT WOS:000175592100014 PM 12015569 ER PT J AU Meier, RR Warren, HP Nicholas, AC Bishop, J Huba, JD Drob, DP Lean, JL Picone, JM Mariska, JT Joyce, G Judge, DL Thonnard, SE Dymond, KF Budzien, SA AF Meier, RR Warren, HP Nicholas, AC Bishop, J Huba, JD Drob, DP Lean, JL Picone, JM Mariska, JT Joyce, G Judge, DL Thonnard, SE Dymond, KF Budzien, SA TI Ionospheric and dayglow responses to the radiative phase of the Bastille Day flare SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MODEL; ATMOSPHERE; SPECTRUM; EUV AB [1] The Sun's Bastille Day flare on July 14, 2000 produced a variety of geoeffective events. This solar eruption consisted of an X-class flare followed by a coronal mass ejection that produced a major geomagnetic storm. We have undertaken a study of this event beginning with an analysis of the effects of the radiative phase of the flare on the dayglow and the ionosphere. The key new enabling work is a novel method of evaluating the X-ray and extreme ultraviolet (EUV) solar spectral irradiance changes associated with the flare. We find that the solar radiative output enhancements modeled during the flare are consistent with measurements of both solar EUV irradiance and far UV Earth thermospheric dayglow. We use the SAMI2 model to predict global ionospheric changes along a magnetic meridian that show significantly different northern and southern effects, suggesting that flares can be used to study ionospheric dynamics. C1 USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Div Plasma Phys, Washington, DC 20375 USA. Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. RP Meier, RR (reprint author), USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. RI Drob, Douglas/G-4061-2014; Meier, Robert/G-4749-2014 OI Drob, Douglas/0000-0002-2045-7740; Meier, Robert/0000-0001-8497-7115 NR 16 TC 31 Z9 32 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 15 PY 2002 VL 29 IS 10 AR 1461 DI 10.1029/2001GL013956 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 609DL UT WOS:000178888300045 ER PT J AU Siemiginowska, A Bechtold, J Aldcroft, TL Elvis, M Harris, DE Dobrzycki, A AF Siemiginowska, A Bechtold, J Aldcroft, TL Elvis, M Harris, DE Dobrzycki, A TI Chandra discovery of a 300 kiloparsec X-ray jet in the gigahertz-peaked spectrum quasar PKS 1127-145 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : individual (PKS 1127 145); X-rays : galaxies ID ACCRETION-DISK INSTABILITIES; HUBBLE-SPACE-TELESCOPE; COMPACT STEEP-SPECTRUM; RADIO-SOURCES; EXTRAGALACTIC OBJECTS; REFERENCE FRAME; ABSORPTION; GHZ; PKS-0637-752; PERFORMANCE AB We have discovered an X-ray jet with Chandra imaging of the z=1.187 radio-loud quasar PKS 1127-145. In this paper we present the Chandra X-ray data, follow-up Very Large Array observations, and optical imaging using the Hubble Space Telescope Wide Field Planetary Camera 2. The X-ray jet contains 273+/-5 net counts in 27 ks and extends similar to30" from the quasar core, corresponding to a minimum projected linear size of similar to330 h(50)(-1) kpc. The evaluation of the X-ray emission processes is complicated by the observed offsets between X-ray and radio brightness peaks. We discuss the problems posed by these observations to jet models. In addition, PKS 1127-145 is a gigahertz-peaked spectrum (GPS) radio source, a member of the class of radio sources suspected to be young or "frustrated" versions of FR I radio galaxies. However, the discovery of an X-ray and radio jet extending well outside the host galaxy of PKS 1127-145 suggests that activity in this and other GPS sources may be long-lived and complex. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 63 TC 84 Z9 84 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2002 VL 570 IS 2 BP 543 EP 556 DI 10.1086/339629 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WJ UT WOS:000175527100008 ER PT J AU Di Stefano, R Kong, AKH Garcia, MR Barmby, P Greiner, J Murray, SS Primini, FA AF Di Stefano, R Kong, AKH Garcia, MR Barmby, P Greiner, J Murray, SS Primini, FA TI Bright X-ray sources in M31 globular clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); galaxies : star clusters; Galaxy : globular clusters : general; X-rays : galaxies; X-rays : stars ID HUBBLE-SPACE-TELESCOPE; LUMINOSITY FUNCTION; ASTRONOMICAL DATA; UPPER LIMITS; BLACK-HOLES; BINARIES; SYSTEM; METALLICITY; EMISSION; DEPENDENCE AB We have conducted Chandra observations of similar to2560 arcmin(2) (similar to131 kpc(2)) of M31 and find that the most luminous X-ray sources in most of our fields are in globular clusters. Of the 28 globular cluster X-ray sources in our fields, 15 are newly discovered. Approximately one-third of all the sources have L-X([0.5-7] keV)>10(37) ergs s(-1), and approximately one-tenth of all the sources have L-X([0.5-7] keV) close to or above 10(38) ergs s(-1). The most luminous source, in the globular cluster Bo 375, is consistently observed to have L-X greater than 2x10(38) ergs s(-1). (1) We present data on the spectra and/or light curves of the five most luminous M31 globular cluster sources. (2) We explore possible explanations for the high X-ray luminosities of the brightest sources. These include that the X-ray sources may be composites, the radiation we receive may be beamed, metallicity effects could be at work, or the sources may be accreting black holes. We weigh each of these possibilities against the data. In addition, we introduce a neutron star model in which mass transfer proceeds on the thermal timescale of the donor star. Our model can produce luminosities of several times 10(38) ergs s(-1) and leads to a set of well-defined predictions. (3) We compute the X-ray luminosity function and the distribution of counts in wavebands that span the range of energies to which Chandra is sensitive. We find the peak X-ray luminosity is higher and that systems with L-X>10(37) ergs s(-1) constitute a larger fraction of all GC sources than in our Galaxy. (4) We study the possible reasons for this difference between M31 and Galactic globular cluster X-ray sources and identify three promising explanations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Astron Inst Potsdam, D-14482 Potsdam, Germany. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Primini, Francis/0000-0002-6077-0643 NR 69 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 MAY 10 PY 2002 VL 570 IS 2 BP 618 EP 636 DI 10.1086/339283 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WJ UT WOS:000175527100013 ER PT J AU Yusef-Zadeh, F Law, C Wardle, M Wang, QD Fruscione, A Lang, CC Cotera, A AF Yusef-Zadeh, F Law, C Wardle, M Wang, QD Fruscione, A Lang, CC Cotera, A TI Detection of X-ray emission from the arches cluster near the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; Galaxy : center; stars : mass loss; stars : winds, outflows; X-rays : ISM ID MASSIVE STARS; QUINTUPLET CLUSTER; COLLIDING WINDS; STELLAR WINDS; LINE STARS; HOT; REGION; CHANDRA; GAS AB The Arches cluster is an extraordinarily compact massive star cluster with a core radius of about 10" (similar to0.4 pc) and consisting of more than 150 O star candidates with initial stellar masses greater than 20 M(circle dot) near G0.12-0.02. X-ray observations of the radio Arc near the Galactic center at lsimilar to0.degrees2, which contains the Arches cluster, have been carried out with the Advanced CCD Imaging Spectrometer (ACIS) on board Chandra X-Ray Observatory. We report the detection of two X-ray sources from the Arches cluster embedded within a bath of diffuse X-ray emission extending beyond the edge of the cluster to at least 90" x 60" (3.6 pc x 2.4 pc). The brightest component of the X-ray emission coincides with the core of the cluster and can be fitted with a two-temperature thermal spectrum with a soft and hard component of 0.8 and 6.4 keV, respectively. The core of the cluster coincides with several ionized stellar wind sources that have previously been detected at radio wavelengths, suggesting that the X-ray emission from the core arises from stellar wind sources. The diffuse emission beyond the boundary of the cluster is discussed in the context of combined shocked stellar winds escaping from the cluster. We argue that the expelled gas from young clusters such as the Arches cluster may be responsible for the hot and extended X-ray emitting gas detected throughout the inner degree of the Galactic center. C1 Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Univ Massachusetts, Amherst, MA 01003 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Yusef-Zadeh, F (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. EM zadeh@northwestern.edu; claw@head-cfa.harvard.edu; wardle@physics.usyd.edu.au; wqd@hnr.astro.umass.edu; antonell@head-cfa.harvard.edu; clang@ocotillo.astro.umass.edu; cotera@as.arizona.edu OI Wardle, Mark/0000-0002-1737-0871 NR 36 TC 73 Z9 73 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 MAY 10 PY 2002 VL 570 IS 2 BP 665 EP 670 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WJ UT WOS:000175527100017 ER PT J AU Molinari, S Testi, L Rodriguez, LF Zhang, QZ AF Molinari, S Testi, L Rodriguez, LF Zhang, QZ TI The formation of massive stars. I. High-resolution millimeter and radio studies of high-mass protostellar candidates SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : jets and outflows; ISM : molecules; radio continuum : ISM; stars : formation; submillimeter ID MAGNETOCENTRIFUGALLY DRIVEN FLOWS; ULTRACOMPACT HII-REGIONS; LUMINOUS IRAS SOURCES; YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; HYDRODYNAMIC SIMULATIONS; BIPOLAR OUTFLOWS; JET-DRIVEN; SEARCH; SAMPLE AB We used the Owens Valley Millimeter Array and the Very Large Array to obtain interferometric maps at millimeter and centimeter wavelengths in both the continuum and various lines [HCO+ (1-0), (HCO+)-C-13 (1-0), SiO (v = 0, J = 2-1) and (HCN)-C-13(1-0)] toward a sample of 11 high-mass protostellar candidates. These sources are known from a previous study to be associated with dense gas and dust and to not be associated with H II regions. All 11 sources were detected in HCO+ (1-0), nine in the millimeter continuum and five (of eight observed) in the centimeter continuum. The derived physical parameters confirm the high-mass nature of these molecular clumps and suggest they are gravitationally bound. Molecular outflows were detected toward six sources, with flow masses and momenta much higher than in low-mass young stellar objects. In many of the sources the molecular emission is organized in substructures, resolved both spatially and in velocity. We find that the sources may be characterized by their degree of fragmentation, turbulence, and outflow activity, with the sample dividing into two groups: group 1 cores have multiple peaks but with a clearly dominant component and larger line widths and are systematically associated with outflows, while group 2 cores have several comparable subentities, smaller line widths, and no association with outflows. We speculate that more massive cores may form from smaller cores via coalescence or competitive accretion. Even conservative estimates of outflow mass-loss rates, however, indicate that accretion is the dominant process in the later formation of massive protostars from such cores. We find a flattening of the outflow mass spectra with increasing flow velocities, at variance with previous studies that suggest a steepening with increasing flow velocities. In the light of this result we suggest a reevaluation of the wide-angle wind momentum-driven flow models to describe the acceleration of outflows in the earliest stages of massive star formation. C1 Ist Fis Spazio Interplanetario, CNR, I-00133 Rome, Italy. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58190, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Molinari, S (reprint author), CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA. RI Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Zhang, Qizhou/0000-0003-2384-6589 NR 53 TC 65 Z9 65 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2002 VL 570 IS 2 BP 758 EP 778 DI 10.1086/339630 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WJ UT WOS:000175527100025 ER PT J AU Sanz-Forcada, J Brickhouse, NS Dupree, AK AF Sanz-Forcada, J Brickhouse, NS Dupree, AK TI Quiescent and flaring structure in RS canum venaticorum stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : coronae; stars : individual (sigma Geminorum, UX Arietis, II Pegasi, V711 Tauri, AB Doradus, beta Ceti); stars : late-type; ultraviolet : stars; X-rays : stars ID LOCAL INTERSTELLAR-MEDIUM; BINARY-II-PEGASI; X-RAY FLARE; AB DORADUS; ROTATIONAL MODULATION; AR-LACERTAE; UX ARIETIS; TEMPERATURE STRUCTURE; MAGNETIC ACTIVITY; EMISSION MEASURE AB Four of the most active RS CVn stars (V711 Tau, II Peg, sigma Gem, and UX Ari) have been observed for a total of 3 Ms with the Extreme Ultraviolet Explorer satellite (EUVE) between 1992 and 2000 January. Flaring and quiescent states of extreme ultraviolet spectra (lambdalambda70-740) and light curves (lambdalambda75-175) have been analyzed to provide emission measure distributions ( EMD) for these systems in the range log T-e(K) similar to 5.6-7.4, based principally on iron lines. Flux measurements obtained with IUE and the Orbiting and Retrievable Far and Extreme Ultraviolet Spectrometer (ORFEUS) complete the EMD in the lower temperature range [log T-e(K) similar to 4.0-5.6]. Frequent flaring activity has been found in the systems, including an increase during the rise phase by a factor of similar to9 in the flux of sigma Gem, the largest are enhancement observed with EUVE. Analyses of the EUVE emission in the active single star AB Dor and the low-rotation giant star beta Cet are also included. The EMDs are remarkably similar among all the stars, showing a narrow enhancement or "bump" around log T-e(K) similar to 6.9. These narrow bumps are apparently unrelated to rotation rate, spectral type, binarity, or evolutionary stage. Significant material is found at log T-e(K)greater than or similar to7.0 for the most active stars. Modulation of the EUV flux outside of flaring occurs in four of the stars (sigma Gem, V711 Tau, UX Ari, AB Dor). The electron density ranges between N-e similar to 10(12) and similar to10(13) cm(-3), measured at log T-e(K) similar to 7.0, and may reach higher values during flares. These densities and EMD values imply small scale sizes for emitting regions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sanz-Forcada, J (reprint author), Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy. RI Sanz-Forcada, Jorge/C-3176-2017; OI Sanz-Forcada, Jorge/0000-0002-1600-7835; Brickhouse, Nancy/0000-0002-8704-4473 NR 81 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 MAY 10 PY 2002 VL 570 IS 2 BP 799 EP 819 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WJ UT WOS:000175527100029 ER PT J AU Kuchner, MJ Traub, WA AF Kuchner, MJ Traub, WA TI A coronagraph with a band-limited mask for finding terrestrial planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; circumstellar matter; instrumentation : adaptive optics; planetary systems; techniques : interferometric ID ADAPTIVE OPTICS; CORONOGRAPHY AB Several recent designs for planet-finding telescopes use coronagraphs operating at visible wavelengths to suppress starlight along the telescope's optical axis while transmitting any off-axis light from circumstellar material. We describe a class of graded coronagraphic image masks that can, in principle, provide perfect elimination of on-axis light, while simultaneously maximizing the Lyot stop throughput and angular resolution. These "band-limited" masks operate on the intensity of light in the image plane, not the phase. They can work with almost any entrance pupil shape, provided that the entrance pupil transmissivity is uniform, and can be combined with an apodized Lyot stop to reduce the sensitivity of the coronagraph to imperfections in the image mask. We discuss some practical limitations on the dynamic range of coronagraphs in the context of a space-based terrestrial-planet finder telescope and emphasize that fundamentally, the optical problem of imaging planets around nearby stars is a matter of precision fabrication and control, not Fraunhofer diffraction theory. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 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 NR 14 TC 201 Z9 201 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2002 VL 570 IS 2 BP 900 EP 908 DI 10.1086/339625 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WJ UT WOS:000175527100035 ER PT J AU Bergin, EA Alves, J Huard, T Lada, CJ AF Bergin, EA Alves, J Huard, T Lada, CJ TI N2H+ and (CO)-O-18 depletion in a cold dark cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : abundances; ISM : clouds; ISM : individual (B68); ISM : molecules; stars : formation ID PRESTELLAR CORES; DUST EXTINCTION; CHEMICAL-MODELS; STAR-FORMATION; MOLECULAR GAS; EVOLUTION; CHEMISTRY AB We present sensitive, high angular resolution molecular line observations of (CO)-O-18 and N2H+ toward the dark globule B68. We directly compare these data with the near-infrared extinction measurements of Alves, Lada, & Lada to derive the first evidence for the depletion of N2H+, and by inference N-2, in a prestellar dark cloud. We also find widespread (CO)-O-18 depletion throughout the centrally condensed core of the B68 cloud. Specifically, we find the N2H+ emission to peak in a shell partially surrounding the peak of dust extinction. Moreover, N2H+ peaks inside the much larger (CO)-O-18 depletion hole and has a smaller depletion zone, confirming theoretical predictions. These data are analyzed through a direct coupling of time-dependent chemical models to a radiation transfer code. This analysis highlights the importance of photodissociation at cloud edges and suggests that the CO abundance declines by 2 orders of magnitude from edge to center. In contrast, N2H+ declines in abundance, at minimum, by at least a factor of 2. Indeed, it is entirely possible that both N2H+ and N-2 are completely absent from the central regions of the B68 core. The depletion of N2H+, and its parent molecule N-2, opens up the possibility that the centers of dense cores, prior to the formation of a star, may evade detection by conventional methods of probing cores using molecular emission. Under these conditions, H2D+ may be the sole viable molecular probe of the innermost regions of star-forming cores. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. RP Bergin, EA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 236 Z9 236 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2002 VL 570 IS 2 BP L101 EP L104 DI 10.1086/340950 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WM UT WOS:000175527500013 ER PT J AU Ransom, SM Gaensler, BM Slane, PO AF Ransom, SM Gaensler, BM Slane, PO TI A deep search for pulsations from the nearby isolated neutron star RX J1856.5-3754 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (RX J1856.5-3754); stars : neutron; X-rays : stars ID PERIODIC SIGNAL; HOT SPOTS; EMISSION; DISCOVERY; FIELD AB We present the results of a deep search for pulsations from the nearby isolated neutron star RX J1856.5-3754 using the 450 ks director's discretionary time Chandra observation completed on 2001 October 15. No pulsations were detected. We find a 99% confidence upper limit on the pulsed fraction of similar to4.5% for worst-case sinusoidal pulsations with frequency less than or similar to50 Hz and frequency derivatives -5 x 10(-10) Hz s(-1) less than or equal to f less than or equal to 0 Hz s(-1). The nondetection of pulsations is most likely due to an unfavorable viewing angle or emitting geometry. Such emitting geometries are much more likely to occur for more "compact" neutron stars, which show increased gravitational light-bending effects. In this case, the nondetection implies a radius-to-mass ratio for RX J1856.5-3754 of R/M less than or similar to 10 km M-.(-1). C1 McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ransom, SM (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. RI Gaensler, Bryan/F-8655-2010; OI Ransom, Scott/0000-0001-5799-9714; Gaensler, Bryan/0000-0002-3382-9558 NR 28 TC 30 Z9 30 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2002 VL 570 IS 2 BP L75 EP L78 DI 10.1086/340973 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WM UT WOS:000175527500007 ER PT J AU Winebarger, AR Updike, AC Reeves, KK AF Winebarger, AR Updike, AC Reeves, KK TI Correlating transition region explosive events with extreme-ultraviolet brightenings SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : activity; Sun : corona ID CORONAL EXPLORER; ENERGY-DISTRIBUTION; MAGNETIC NETWORK; SUMER TELESCOPE; SOLAR CORONA; QUIET SUN; MICROFLARES; NANOFLARES; SPECTROMETER; ATMOSPHERE AB Frequent small-scale reconnection events have been proposed as a possible mechanism to heat the solar corona. It has not yet been demonstrated, however, that the smallest reconnection events can heat the plasma to coronal temperatures. In this Letter, we use explosive events in the spectral line C IV lambda1548 observed by the Solar Ultraviolet Measurement of Emitted Radiation instrument flown aboard the Solar and Heliospheric Observatory to locate areas of reconnection in Active Region 8536 on 1999 May 13. We then examine coaligned Transition Region and Coronal Explorer (TRACE) 171 Angstrom images for a response to the reconnection. We find that short-term (<5 minute) fluctuations are on average 2.2 times larger in regions of reconnection than in comparison (nonevent) regions. These fluctuations are statistically significant (3 σ above the mean intensity fluctuation in the nonevent regions) in 35% of the reconnection regions. We find two possible explanations for the 171 &ANGS; intensity fluctuations: (1) the explosive event plasma could be heated to 1 MK, or (2) the emission measure of the O vi λ172 line could increase because of a surge of transition region material that would, in turn, increase the 171 &ANGS; intensity. The latter explanation would imply that not all transient brightenings in the TRACE data are associated with plasma at coronal temperatures. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smith Coll, Northampton, MA 01063 USA. RP Winebarger, AR (reprint author), USN, Res Lab, Code 7673W, Washington, DC 20375 USA. RI Reeves, Katharine/P-9163-2014 NR 20 TC 9 Z9 9 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2002 VL 570 IS 2 BP L105 EP L108 DI 10.1086/341121 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550WM UT WOS:000175527500014 ER PT J AU Ricklefs, RE Bermingham, E AF Ricklefs, RE Bermingham, E TI Islands, equilibria, and speciation - Response SO SCIENCE LA English DT Editorial Material ID LESSER ANTILLEAN AVIFAUNA; BIOGEOGRAPHY C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. Smithsonian Trop Res Inst, Balboa, Panama. RP Ricklefs, RE (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. NR 6 TC 0 Z9 0 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 MAY 10 PY 2002 VL 296 IS 5570 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 551MG UT WOS:000175565000002 ER PT J AU Zotz, G Vollrath, B AF Zotz, G Vollrath, B TI Substrate preferences of epiphytic bromeliads: an experimental approach SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY LA English DT Article DE Barro Colorado Island; seedling ecology; survival; tropical moist forest; vascular epiphytes ID SEEDLING ESTABLISHMENT; WATER RELATIONS; COSTA-RICA; ORCHID; DISPERSAL; FOREST AB Based on the known vertical distributions of three epiphyte species we tested the hypothesis that observed interspecific differences are determined at a very early ontogenetic stage. We attached 1296 first-year seedlings of the three species Guzmania monostachya, Tillandsia fasciculata, and Vriesea sanguinolenta (Bromeliaceae) to substrates differing in orientation and relative position within the crown of the host tree, Annona glabra. Surprisingly, we found no evidence for differential mortality on different substrate types for any of the three species. Hence, differences in vertical distribution cannot be explained by interspecific differences in site-specific survival at this stage. This suggests that spatial distribution patterns are determined even earlier, probably resulting from species differences in seed dispersal or during germination. (C) 2002 Editions scientifiques et medicales Elsevier SAS. All rights reserved. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. NR 30 TC 22 Z9 25 U1 0 U2 9 PU GAUTHIER-VILLARS/EDITIONS ELSEVIER PI PARIS PA 23 RUE LINOIS, 75015 PARIS, FRANCE SN 1146-609X J9 ACTA OECOL JI Acta Oecol.-Int. J. Ecol. PD MAY PY 2002 VL 23 IS 2 BP 99 EP 102 AR PII S1146-609X(02)01139-6 DI 10.1016/S1146-609X(02)01139-6 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 568VK UT WOS:000176565400006 ER PT J AU Post, J AF Post, J TI Acceptance of the Mineralogical Society of America's Public Service Medal for 2001 SO AMERICAN MINERALOGIST LA English DT Editorial Material C1 Smithsonian Inst, Dept Mineral Sci, MRC, NHB 119, Washington, DC 20560 USA. RP Post, J (reprint author), Smithsonian Inst, Dept Mineral Sci, MRC, NHB 119, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2002 VL 87 IS 5-6 BP 798 EP 798 PG 1 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 553DN UT WOS:000175660500031 ER PT J AU Carbone, C Christie, S Conforti, K Coulson, T Franklin, N Ginsberg, JR Griffiths, M Holden, J Kinnaird, M Laidlaw, R Lynam, A MacDonald, DW Martyr, D McDougal, C Nath, L O'Brien, T Seidensticker, J Smith, JLD Tilson, R Shahruddin, WNW AF Carbone, C Christie, S Conforti, K Coulson, T Franklin, N Ginsberg, JR Griffiths, M Holden, J Kinnaird, M Laidlaw, R Lynam, A MacDonald, DW Martyr, D McDougal, C Nath, L O'Brien, T Seidensticker, J Smith, JLD Tilson, R Shahruddin, WNW TI The use of photographic rates to estimate densities of cryptic mammals: response to Jennelle et al. SO ANIMAL CONSERVATION LA English DT Article ID SIZE C1 Zool Soc London, Inst Zool, London NW1 4RY, England. Zool Soc London, London Zoo, London NW1 4RY, England. Smithsonian Natl Zool Pk, Washington, DC 20008 USA. Univ Cambridge, Dept Zool, Large Anim Res Grp, Cambridge CB2 3EJ, England. Univ York, Dept Biol, York YO1 5DD, N Yorkshire, England. Sumatran Tiger Project, Lampung 34101, Sumatra, Indonesia. Wildlife Conservat Soc, Int Programs, Bronx, NY 10460 USA. Leuser Dev Programme, Medan 20154, Sumatra, Indonesia. Fauna & Flora Int, Cambridge CB1 2DT, England. Univ Oxford, Dept Zool, Wildlife Conservat Res Unit, Oxford OX1 3PS, England. Tiger Tops, Kathmandu, Nepal. Dept Fisheries & Wildlife, St Paul, MN 55108 USA. RP Carbone, C (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. OI Lynam, Antony/0000-0002-8395-7902; Coulson, Tim/0000-0001-9371-9003 NR 9 TC 34 Z9 34 U1 2 U2 19 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD MAY PY 2002 VL 5 BP 121 EP 123 DI 10.1017/S1367943002002172 PN 2 PG 3 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 559VD UT WOS:000176045300006 ER PT J AU Stuart, J AF Stuart, J TI C.C. Wang, singing brush and dancing ink SO ARTS OF ASIA LA English DT Article C1 Smithsonian Inst, Freer Gallery Art & Arthur M Sackler Gallery, Washington, DC 20560 USA. RP Stuart, J (reprint author), Smithsonian Inst, Freer Gallery Art & Arthur M Sackler Gallery, Washington, DC 20560 USA. NR 5 TC 6 Z9 6 U1 0 U2 0 PU ARTS ASIA PUBLICATIONS LTD PI KOWLOON PA KOWLOON CENTER-SUITE 1309 29-39 ASHLEY RD, KOWLOON, HONG KONG SN 0004-4083 J9 ART ASIA JI Arts Asia PD MAY-JUN PY 2002 VL 32 IS 3 BP 44 EP 52 PG 9 WC Art; Asian Studies SC Art; Asian Studies GA 561MG UT WOS:000176144100003 ER PT J AU Kannappan, SJ Fabricant, DG Franx, M AF Kannappan, SJ Fabricant, DG Franx, M TI Physical sources of scatter in the Tully-Fisher relation SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; galaxies : evolution; galaxies : fundamental parameters; galaxies : general; galaxies : interactions; galaxies : kinematics and dynamics ID URSA-MAJOR CLUSTER; EXTRAGALACTIC DISTANCE SCALE; OPTICAL-ROTATION CURVES; NEARBY FIELD GALAXIES; SPIRAL GALAXIES; VELOCITY-FIELD; STAR-FORMATION; LOCAL SUPERCLUSTER; LUMINOSITY FUNCTION; DWARF GALAXIES AB We analyze residuals from the Tully-Fisher relation for the emission-line galaxies in the Nearby Field Galaxy Survey, a broadly representative survey designed to fairly sample the variety of galaxy morphologies and environments in the local universe for luminosities from M-B = 15 to -23. For a subsample consisting of the spiral galaxies brighter than M-R(i) = -18, we find strong correlations between Tully-Fisher residuals and both B-R color and EW(Halpha). The extremes of the correlations are populated by Sa galaxies, which show consistently red colors, and spiral galaxies with morphological peculiarities, which are often blue. If we apply an EW(Halpha)-dependent or B-R color-dependent correction term to the Tully-Fisher relation, the scatter in the relation no longer increases from R to B to U but instead drops to a nearly constant level in all bands, close to the scatter we expect from measurement errors. We argue that these results probably reflect correlated offsets in luminosity and color as a function of star formation history. Broadening the sample in morphology and luminosity, we find that most nonspiral galaxies brighter than M-R(i) = -18 follow the same correlations between Tully-Fisher residuals and B R color and EW( H) as do spirals, albeit with greater scatter. However, the color and EW(Halpha) correlations do not apply to galaxies fainter than M-R(i) = -18 or to emission-line S0 galaxies with anomalous gas kinematics. For the dwarf galaxy population, the parameters controlling Tully-Fisher residuals are instead related to the degree of recent evolutionary disturbance: overluminous dwarfs have higher rotation curve asymmetries, brighter U-band effective surface brightnesses, and shorter gas consumption timescales than their underluminous counterparts. As a result, sample selection strongly affects the measured faint-end slope of the Tully-Fisher relation, and a sample limited to include only passively evolving, rotationally supported galaxies displays a break toward steeper slope at low luminosities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Kannappan, SJ (reprint author), Univ Texas, McDonald Observ, 2511 Speedway,RLM 15-308 C1400, Austin, TX 78712 USA. NR 87 TC 87 Z9 87 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 MAY PY 2002 VL 123 IS 5 BP 2358 EP 2386 DI 10.1086/339972 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547AZ UT WOS:000175311200015 ER PT J AU Schroder, LL Brodie, JP Kissler-Patig, M Huchra, JP Phillips, AC AF Schroder, LL Brodie, JP Kissler-Patig, M Huchra, JP Phillips, AC TI Spectroscopy of globular clusters in M81 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M31, M81, NGC 3031); galaxies : spiral; globular clusters : general ID STAR-CLUSTERS; RADIAL-VELOCITIES; ANDROMEDA GALAXY; SYSTEM; M31; METALLICITY; KINEMATICS; DISK; PHOTOMETRY; FIELD AB We present moderate-resolution spectroscopy of globular clusters around the Sa/Sb spiral galaxy M81 (NGC 3031). Sixteen candidate clusters were observed with the Low Resolution Imaging Spectrograph on the Keck I telescope. All are confirmed as bona de globular clusters, although one of the clusters appears to have been undergoing a transient event during our observations. In general, the M81 globular cluster system is found to be very similar to the Milky Way and M31 systems, both chemically and kinematically. A kinematic analysis of the velocities of 44 M81 globular clusters ( the 16 presented here and 28 from previous work) strongly suggests that the red metal-rich clusters are rotating in the same sense as the gas in the disk of M81. The blue metal-poor clusters have halo-like kinematics, showing no evidence for rotation. The kinematics of clusters whose projected galactocentric radii lie between 4 and 8 kpc suggests that they are rotating much more than those with projected galactocentric radii outside these bounds. We suggest that these rotating, intermediate-distance clusters are analogous to the kinematic subpopulation in the metal-rich, disk globular clusters observed in the Milky Way, and we present evidence for the existence of a similar subpopulation in the metal-rich clusters of M31. With one exception, all of the M81 clusters in our sample have ages that are consistent with Milky Way and M31 globular clusters. One cluster may be as young as a few Gyr. The correlations between absorption-line indices established for Milky Way and M31 globular clusters also hold in the M81 cluster system, at least at the upper end of the metallicity distribution ( which our sample probes). On the whole, the mean metallicity of the M81 globular cluster system is similar to the metallicity of the Milky Way and M31 globular cluster systems. To within a factor of 2, the projected mass of M81 is similar to the masses of the Milky Way and M31. Its mass pro le indicates the presence of a dark matter halo. C1 Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. European So Observ, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Schroder, LL (reprint author), Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. NR 60 TC 38 Z9 38 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2002 VL 123 IS 5 BP 2473 EP 2489 DI 10.1086/322994 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547AZ UT WOS:000175311200022 ER PT J AU Perrett, KM Bridges, TJ Hanes, DA Irwin, MJ Brodie, JP Carter, D Huchra, JP Watson, FG AF Perrett, KM Bridges, TJ Hanes, DA Irwin, MJ Brodie, JP Carter, D Huchra, JP Watson, FG TI The kinematics and metallicity of the M31 globular cluster system SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M31); galaxies : stellar content; Galaxy : formation; Galaxy : kinematics and dynamics; techniques : spectroscopic ID INFRARED PHOTOMETRY; STELLAR POPULATIONS; GALAXY FORMATION; OUTER HALO; MILKY-WAY; MASS; BULGE; DISK; M-31; INNER AB With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12 km s(-1)) and metallicities (+/-0.26 dex) for over 200 members of the M31 globular cluster population out to a radius of 1.degrees5 from the galaxy center. Many of these clusters have no previous published radial velocity or [ Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters. We find that the abundance distribution of the cluster system is consistent with a bimodal distribution with peaks at [Fe/H] similar to1.4 and -0.5. The metal-rich clusters demonstrate a centrally concentrated spatial distribution with a high rotation amplitude, although this population does not appear significantly flattened and is consistent with a bulge population. The metal-poor clusters tend to be less spatially concentrated and are also found to have a strong rotation signature. C1 Queens Univ, Dept Phys, Kingston, ON K7L 3N6, Canada. Anglo Australian Observ, Epping, NSW 1710, Australia. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Liverpool John Moores Univ, Birkenhead CH41 1LD, Merseyside, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perrett, KM (reprint author), Queens Univ, Dept Phys, Kingston, ON K7L 3N6, Canada. NR 64 TC 140 Z9 141 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 MAY PY 2002 VL 123 IS 5 BP 2490 EP 2510 DI 10.1086/340186 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547AZ UT WOS:000175311200023 ER PT J AU Barbera, M Bocchino, F Damiani, F Micela, G Sciortino, S Favata, F Harnden, FR AF Barbera, M Bocchino, F Damiani, F Micela, G Sciortino, S Favata, F Harnden, FR TI ROSAT PSPC/HRI observations of the open cluster NGC 2422 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE open clusters and associations : individual : NGC 2422; stars : coronae; X-rays : stars ID UVBY-BETA-PHOTOMETRY; COUNTING DETECTOR IMAGES; X-RAY SURVEY; ULTRAVIOLET SENSITIVITY; WAVELET TRANSFORMS; STARS; PLEIADES; PRAESEPE; HRI; NGC-2422 AB We present the results of a ROSAT study of NGC 2422, a southern open cluster at a distance of about 470 pc, with an age close to the Pleiades. Source detection was performed on two observations, a 10-ks PSPC and a 40-ks HRI pointing, with a detection algorithm based on wavelet transforms, particularly suited to detecting faint sources in crowded fields. We have detected 78 sources, 13 of which were detected only with the HRI, and 37 detected only with the PSPC. For each source, we have computed the 0:2 2:0 keV X-ray flux. Using optical data from the literature and our own low-dispersion spectroscopic observations, we find candidate optical counterparts for 62 X-ray sources, with more than 80% of these counterparts being late type stars. We have assigned to the optical sources an astrometric and/or a photometric membership flag, depending on which data are available to us. The number of sources (38 of 62) with high membership probability counterparts is consistent with that expected for Galactic plane observations at our sensitivity. We have computed maximum likelihood X-ray luminosity functions (XLF) for F and early-G type stars with high membership probability. Heavy data censoring due to our limited sensitivity permits determination of only the high-luminosity tails of the XLFs; the distributions are indistinguishable from those of the nearly coeval Pleiades cluster. C1 Osservatorio Astron Palermo GS Vaiana, INAF, I-90134 Palermo, Italy. European Space Agcy, European Space Res & Technol Ctr, Dept Space Sci, Div Astrophys, NL-2200 AG Noordwijk, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barbera, M (reprint author), Osservatorio Astron Palermo GS Vaiana, INAF, Piazza Parlamento 1, I-90134 Palermo, Italy. OI Bocchino, Fabrizio/0000-0002-2321-5616; Micela, Giuseppina/0000-0002-9900-4751; Damiani, Francesco/0000-0002-7065-3061; Barbera, Marco/0000-0002-3188-7420 NR 45 TC 7 Z9 8 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2002 VL 387 IS 2 BP 463 EP 478 DI 10.1051/004-6361:20020380 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 556PM UT WOS:000175858200014 ER PT J AU Finoguenov, A Kudritzki, RP Jones, C AF Finoguenov, A Kudritzki, RP Jones, C TI Probing the intracluster star-light with Chandra SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : binaries : close; X-rays : stars; cosmology : observations ID X-RAY-CLUSTERS; PLANETARY-NEBULAE; VIRGO CLUSTER; GALAXIES; IRON AB We propose a method to test for the presence of intracluster star-light using X-ray binaries as a trace population. We discuss a particular application of this method to observations of the Virgo cluster. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Finoguenov, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. NR 29 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2002 VL 387 IS 1 BP L10 EP L12 DI 10.1051/0004-6361:20020430 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 548XP UT WOS:000175415400003 ER PT J AU Risaliti, G AF Risaliti, G TI The BeppoSAX view of bright Compton-thin Seyfert 2 galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : Seyfert; X-rays : galaxies ID X-RAY ASTRONOMY; ENERGY CONCENTRATOR SPECTROMETER; ASCA OBSERVATIONS; ALPHA LINE; ON-BOARD; AGN; SATELLITE; NUCLEUS; VARIABILITY; ABSORBER AB We present the analysis of 31 observations (17 of which are published here for the first time) of 20 bright Compton thin Seyfert 2 s, in the 0.1-200 keV band, performed with the BeppoSAX satellite. The sample consists of all Seyfert 2 s in the BeppoSAX public archive, with a 2-10 keV flux higher than 5 x 10(-12) erg cm(-2) s(-1). The good statistics available and the broad energy band permit a detailed study of the main continuum components of these sources, i.e. the primary power-law, the reflected component, the soft emission and the high-energy cut-off. The main results of our analysis are: (1) the 3-200 keV intrinsic power-law has a mean photon index Gamma= 1.79+/-0.01, with a dispersion of sigma = 0.23. (2) The high-energy exponential cut-off at E similar to 100-300 keV is not an ubiquitous property of Seyfert galaxies: in similar to30% of the objects the continuum power-law does not drop up to energies of 300 keV or more. (3) A reflected component is present in almost all the sources (17 out of 21). The small variations of this component with respect to the intrinsic continuum, in objects with multiple observations, suggests that the reflector is not the accretion disk, but must be located much farther from the nucleus. (4) The range of ratios between the reflected and intrinsic components suggests that the circumnuclear medium is not homogeneous, and a significant fraction of the solid angle is covered by a gas thicker than that along the line of sight. (5) The iron Kalpha line is present is all but one the sources. The equivalent width is in the typical range of Seyfert 1 s (EW = 100 300 eV) in sources with low absorption (N(H) < 3 x 10(23) cm(-2)), and increases in more absorbed objects, as expected according to unified models. (6) The energy resolution of BeppoSAX is in general too low to measure the iron line width. However, in 6 cases we measured a significant line broadening. C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Risaliti, G (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM risaliti@arcetri.astro.it OI Risaliti, Guido/0000-0002-3556-977X NR 35 TC 102 Z9 102 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2002 VL 386 IS 2 BP 379 EP 398 DI 10.1051/0004-6361:20020170 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543YX UT WOS:000175132400001 ER PT J AU Vanzi, L Bagnulo, S Le Floc'h, E Maiolino, R Pompei, E Walsh, W AF Vanzi, L Bagnulo, S Le Floc'h, E Maiolino, R Pompei, E Walsh, W TI Multi-wavelength study of IRAS 19254-7245 - The Superantennae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : individual : IRAS 19254-7245; infrared : galaxies; radio lines : galaxies; galaxies : Seyfert ID ULTRALUMINOUS INFRARED GALAXIES; CO-TO-H-2 CONVERSION FACTOR; MOLECULAR GAS; INTERACTING GALAXIES; SPIRAL GALAXIES; LINE EMISSION; CO; NGC-6240; MERGERS; SPECTROSCOPY AB We present observations in the optical, near-infrared and millimetre bands of the Ultraluminous Infrared galaxy IRAS 19254-7245, also known as "The Superantennae". This galaxy is an interacting system with a double nucleus and long tails extending for about 350 kpc. We studied in detail the southern component of the system which is optically classified as a Sy2 galaxy. We have developed a method to determine the parameters of the emission lines in a spectrum in the case of multiple components and severe blending. Our data allow us to build a picture of the environment around the nucleus of the galaxy with unprecedented detail. The optical lines show a complex dynamical structure that is not observable in the near-infrared. In addition we find typical features of AGN such as the coronal lines of [FeVII]5721 and [SiVI]1.96. We also detect strong emission from [FeII]1.64 and H-2. C1 European So Observ, Santiago, Chile. Osservatorio Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vanzi, L (reprint author), European So Observ, Alonso de Cordova 3107, Santiago, Chile. RI Vanzi, Leonardo/D-1381-2014 NR 40 TC 12 Z9 12 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2002 VL 386 IS 2 BP 464 EP 471 DI 10.1051/0004-6361:20020291 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543YX UT WOS:000175132400007 ER PT J AU Barrena, R Biviano, A Ramella, M Falco, EE Seitz, S AF Barrena, R Biviano, A Ramella, M Falco, EE Seitz, S TI The dynamical status of the cluster of galaxies 1E0657-56 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : clusters : individual : 1E0657-56; galaxies : clusters : general; galaxies : distances and redshifts ID COLOR-MAGNITUDE RELATION; COMA CLUSTER; VIRGO CLUSTER; REDSHIFT; EVOLUTION; MASS; SUBSTRUCTURE; CONSEQUENCES; PHOTOMETRY; DEPENDENCE AB We present the results of a new spectroscopic and photometric survey of the hot X-ray cluster 1E0657-56, at z = 0.296. We determine the presence of a low velocity dispersion subcluster, which is offset from the main cluster position by 0.7 Mpc and similar or equal to600 km s(-1). We determine the virial masses and total luminosities of the cluster and its subcluster, and solve for the two-body dynamical model. With additional constraints from the results of the analysis of the cluster X-ray emission by Markevitch et al. (2001), we find that the subcluster passed through the cluster centre similar or equal to0.15 Gyr ago. Taken at face value the mass of the subcluster is typical of a loose group. It is however difficult to establish the pre-merger mass of the colliding system. We provide tentative evidence that the subcluster is in fact the remnant core of a moderately massive cluster, stripped by the collision with 1E0657-56. The main cluster dynamics does not seem to have suffered from this collision. On the contrary, the cluster X-ray properties seem to have been significantly affected. We also discuss the effect of the subcluster collision in relation to starburst events and the cluster radio halo. C1 Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Inst Astrofis Canarias, Tenerife 38200, Spain. Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. Univ Sternwarte, D-81679 Munich, Germany. RP Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34131 Trieste, Italy. EM biviano@ts.astro.it OI Ramella, Massimo/0000-0001-5446-4749; Biviano, Andrea/0000-0002-0857-0732 NR 64 TC 65 Z9 65 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2002 VL 386 IS 3 BP 816 EP 828 DI 10.1051/0004-6361:20020244 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546HZ UT WOS:000175269800006 ER PT J AU Sollerman, J Holland, ST Challis, P Fransson, C Garnavich, P Kirshner, RP Kozma, C Leibundgut, B Lundqvist, P Patat, F Filippenko, AV Panagia, N Wheeler, JC AF Sollerman, J Holland, ST Challis, P Fransson, C Garnavich, P Kirshner, RP Kozma, C Leibundgut, B Lundqvist, P Patat, F Filippenko, AV Panagia, N Wheeler, JC TI Supernova 1998bw - the final phases SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE supernovae : individual (SN 1998bw); nuclear reactions, nucleosynthesis, abundances; Gamma rays : bursts ID GAMMA-RAY BURST; 25 APRIL 1998; SN 1998BW; LIGHT-CURVE; CCD PHOTOMETRY; LATE TIMES; EMISSION; 1987A; SN-1998BW/GRB-980425; TEMPERATURE AB The probable association with GRB 980425 immediately put SN 1998bw at the forefront of supernova research. Here, we present revised late-time BVRI light curves of the supernova, based on template images taken at the VLT. To follow the supernova to the very last observable phases we have used HST/STIS. Deep images taken in June and November 2000 are compared to images taken in August 2001. The identification of the supernova is firmly established. This allows us to measure the light curve to similar to 1000 days past explosion. The main features are a rapid decline up to more than 500 days after explosion, with no sign of complete positron trapping from the Co-56 decay. Thereafter, the light curve flattens out significantly. One possible explanation is powering by more long lived radioactive isotopes, if they are abundantly formed in this energetic supernova. C1 European So Observ, D-85748 Garching, Germany. Stockholm Observ, Dept Astron, SCFAB, S-10691 Stockholm, Sweden. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Sollerman, J (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. OI Sollerman, Jesper/0000-0003-1546-6615 NR 44 TC 42 Z9 42 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2002 VL 386 IS 3 BP 944 EP 956 DI 10.1051/0004-6361:20020326 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546HZ UT WOS:000175269800023 ER PT J AU Weekes, TC Badran, H Biller, SD Bond, I Bradbury, S Buckley, J Carter-Lewis, D Catanese, M Criswell, S Cui, W Dowkontt, P Duke, C Fegan, DJ Finley, J Fortson, L Gaidos, J Gillanders, GH Grindlay, J Hall, TA Harris, K Hillas, AM Kaaret, P Kertzman, M Kieda, D Krennrich, F Lang, MJ LeBohec, S Lessard, R Lloyd-Evans, J Knapp, J McKernan, B McEnery, J Moriarty, P Muller, D Ogden, P Ong, R Petry, D Quinn, J Reay, NW Reynolds, PT Rose, J Salamon, M Sembroski, G Sidwell, R Slane, P Stanton, N Swordy, SP Vassiliev, VV Wakely, SP AF Weekes, TC Badran, H Biller, SD Bond, I Bradbury, S Buckley, J Carter-Lewis, D Catanese, M Criswell, S Cui, W Dowkontt, P Duke, C Fegan, DJ Finley, J Fortson, L Gaidos, J Gillanders, GH Grindlay, J Hall, TA Harris, K Hillas, AM Kaaret, P Kertzman, M Kieda, D Krennrich, F Lang, MJ LeBohec, S Lessard, R Lloyd-Evans, J Knapp, J McKernan, B McEnery, J Moriarty, P Muller, D Ogden, P Ong, R Petry, D Quinn, J Reay, NW Reynolds, PT Rose, J Salamon, M Sembroski, G Sidwell, R Slane, P Stanton, N Swordy, SP Vassiliev, VV Wakely, SP TI VERITAS: the Very Energetic Radiation Imaging Telescope Array System SO ASTROPARTICLE PHYSICS LA English DT Article DE gamma-ray astronomy; gamma-ray telescopes; atmospheric Cherenkov radiation; pulsars; AGN; supernova remnants; galactic plane; neutralinos ID GAMMA-RAY ASTRONOMY; VERY-HIGH-ENERGY; AIR CERENKOV TELESCOPES; PRIMORDIAL BLACK-HOLES; SUPERNOVA-REMNANTS; GALACTIC PLANE; TEV; GALAXY; MARKARIAN-421; ACCELERATION AB The Very Energetic Radiation Imaging Telescope Array System (VERITAS) represents an important step forward in the study of extreme astrophysical processes in the universe. It combines the power of the atmospheric Cherenkov imaging technique using a large optical reflector with the power of stereoscopic observatories using at-rays of separated telescopes looking at the same shower. The seven identical telescopes in VERITAS. each of aperture 10 m, will be deployed in a filled hexagonal pattern of side 80 m, each telescope will have a camera consisting of 499 pixels with a field of view of 3.5degrees. VERITAS will substantially increase the catalog of very high energy (E > 100 GeV) gamma-ray sources and greatly improve measurements of established sources. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. Univ Oxford, Dept Phys, Oxford OX1 3RH, England. Univ Leeds, Dept Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland Univ Coll Dublin, Dept Expt Phys, Dublin 4, Ireland. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Natl Univ Ireland Univ Coll Galway, Dept Expt Phys, Galway, Ireland. Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. Galway Mayo Inst Technol, Galway, Ireland. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90024 USA. Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. Cork Inst Technol, Cork, Ireland. RP Harvard Smithsonian Ctr Astrophys, Whipple Observ, POB 97, Amado, AZ 85645 USA. EM weekes@cfa.harvard.edu RI McEnery, Julie/D-6612-2012; OI Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 81 TC 210 Z9 210 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD MAY PY 2002 VL 17 IS 2 BP 221 EP 243 AR PII S0927-6505(01)00152-9 DI 10.1016/S0927-6505(01)00152-9 PG 23 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 559TL UT WOS:000176041400010 ER PT J AU Perna, R Belczynski, K AF Perna, R Belczynski, K TI Short gamma-ray bursts and mergers of compact objects: Observational constraints SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays : bursts ID NEUTRON-STAR BINARIES; MASS-LOSS; BLACK-HOLES; OPTICAL COUNTERPART; STELLAR PARAMETERS; FORMING REGIONS; AFTERGLOW; EVOLUTION; ABSORPTION; GALAXIES AB Gamma-ray burst (GRB) data accumulated over the years have shown that the distribution of their time duration is bimodal. While there is some evidence that long bursts are associated with star-forming regions, nothing is known regarding the class of short bursts. Their very short timescales are hard to explain with the collapse of a massive star but would be naturally produced by the merger of two compact objects, such as two neutron stars (NS-NS), or a neutron star and a black hole (NS-BH). As for the case of long bursts, afterglow obervations for short bursts should help reveal their origin. By using updated population synthesis code calculations, we simulate a cosmological population of merging NS-NS and NS-BH and compute the distribution of their galactic offsets, the density distribution of their environment, and, if indeed associated with GRBs, their expected afterglow characteristics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist Astrofis Spaziale, I-00133 Rome, Italy. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Perna, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 101 TC 59 Z9 59 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 MAY 1 PY 2002 VL 570 IS 1 BP 252 EP 263 DI 10.1086/339571 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547AG UT WOS:000175309300023 ER PT J AU Kong, AKH McClintock, JE Garcia, MR Murray, SS Barret, D AF Kong, AKH McClintock, JE Garcia, MR Murray, SS Barret, D TI The X-ray spectra of black hole X-ray novae in quiescence as measured by Chandra SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (A0620-00, GRO J1655-40, V404 Cygni, XTE J1550-564); X-rays : binaries ID OPTICAL LIGHT-CURVE; SOURCE GRO J1655-40; PARAMETER-ESTIMATION; ROSAT OBSERVATIONS; V404 CYGNI; EMISSION; TRANSIENTS; ASTRONOMY; BEPPOSAX; A0620-00 AB We present Chandra observations of black hole X-ray novae V404 Cyg, A0620-00, GROJ1655-40, and XTE J1550-564 in quiescence. Their quiescent spectra can be well fitted by a power-law model with number slope alphasimilar to2. While a coronal (Raymond-Smith) model is also a statistically acceptable representation of the spectra, the best-fit temperatures of these models is similar to5 times higher than that seen in active stellar coronae. These four spectra of quiescent X-ray novae are all consistent with that expected for accretion via an advection-dominated accretion flow and inconsistent with that expected from a stellar corona. This evidence for continued accretion in quiescence further strengthens the case for the existence of event horizons in black holes. Both A0620-00 and GROJ1655-40 were fainter than in previous observations, while V404 Cyg was more luminous and varied by a factor of 2 in a few kiloseconds. A reanalysis of the X-ray data for XTE J1550-564 shows that (like V404 Cyg and A0620-00) its luminosity exceeds the maximum prediction of the coronal model by a large factor. The 0.3-7 keV luminosities of the four sources studied are in the range from similar to10(30) to 10(33) ergs s(-1). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 45 TC 110 Z9 109 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2002 VL 570 IS 1 BP 277 EP 286 DI 10.1086/339501 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547AG UT WOS:000175309300025 ER PT J AU Aufdenberg, JP Hauschildt, PH Baron, E Nordgren, TE Burnley, AW Howarth, ID Gordon, KD Stansberry, JA AF Aufdenberg, JP Hauschildt, PH Baron, E Nordgren, TE Burnley, AW Howarth, ID Gordon, KD Stansberry, JA TI The spectral energy distribution and mass-loss rate of the A-type supergiant Deneb SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : numerical; radio continuum : stars; stars : atmospheres; stars : individual (Deneb); stars : winds, outflows; techniques : interferometric ID EARLY-TYPE STARS; STELLAR ANGULAR DIAMETERS; VISUAL SURFACE BRIGHTNESS; RADIO-CONTINUUM EMISSION; OR-EQUAL-TO; ALPHA-CYGNI; H-ALPHA; OPTICAL INTERFEROMETER; ATMOSPHERIC PARAMETERS; ULTRAVIOLET EXTINCTION AB A stellar wind module has been developed for the PHOENIX stellar atmosphere code for the purpose of computing non-LTE, line-blanketed, expanding atmospheric structures and detailed synthetic spectra of hot luminous stars with winds. We apply the code to observations of Deneb, for which we report the first positive detections of millimeter and centimeter emission ( obtained using the Submillimeter Common-User Bolometric Array and the Very Large Array) as well a strong upper limit on the 870 mum flux (using the Heinrich Hertz Telescope). The slope of the radio spectrum shows that the stellar wind is partially ionized. We report a uniform-disk angular diameter measurement theta(UD) = 2.40 +/- 0.06 mas from the Navy Prototype Optical Interferometer (NPOI). The measured bolometric flux and corrected NPOI angular diameter yield an effective temperature of 8600 +/- 500 K. Least-squares comparisons of synthetic spectral energy distributions from 1220 Angstrom to 3.6 cm with the observations provide estimates for the effective temperature and the mass-loss rate of similar or equal to8400 +/- 100 K and (8+/-3) 10(-7) M(.) yr(-1), respectively. This range of mass-loss rates is consistent with that derived from high-dispersion UV spectra when non-LTE metal-line blanketing is considered. We are unable achieve a reasonable fit to a typical Halpha P Cygni profile with any model parameters over a reasonable range. This is troubling because the Halpha profile is the observational basis for the wind momentum luminosity relationship. C1 Harvard Smithsonian Ctr Astrophys, Solar & Stellar Phys Div, Cambridge, MA 02138 USA. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Univ Redlands, Dept Phys, Redlands, CA 92373 USA. UCL, Dept Phys & Astron, London WC1E 6BT, England. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Aufdenberg, JP (reprint author), Harvard Smithsonian Ctr Astrophys, Solar & Stellar Phys Div, 60 Garden St,Mail Stop 15, Cambridge, MA 02138 USA. EM jaufdenberg@cfa.harvard.edu; yeti@hal.physast.uga.edu; baron@nhn.ou.edu; tyler_nordgren@redlands.edu; awxb@star.ucl.ac.uk; idh@star.ucl.ac.uk; kgordon@as.arizona.edu; stansber@as.arizona.edu RI Baron, Edward/A-9041-2009 OI Baron, Edward/0000-0001-5393-1608 NR 88 TC 37 Z9 38 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 MAY 1 PY 2002 VL 570 IS 1 BP 344 EP 368 DI 10.1086/339740 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547AG UT WOS:000175309300030 ER PT J AU Frazin, RA Janzen, P AF Frazin, RA Janzen, P TI Tomography of the solar corona. II. Robust, regularized, positive estimation of the three-dimensional electron density distribution from LASCO-C2 polarized white-light images SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; Sun : corona ID WHOLE SUN MONTH; SPECTROMETER; MINIMUM; HOLE AB Solar rotational tomography is used to determine the three-dimensional electron density distribution of the solar corona from 2.4 to 6.0 R-.. The robust, regularized, positive estimation method, described in a previous paper, is demonstrated on test cases and on LASCO-C2 data. Because the solar rotational pole is inclined to the plane of the ecliptic by about 7degrees, the tomographic inversion requires a full three-dimensional treatment instead of a series of two-dimensional inversions. The LASCO data are taken from the first Whole Sun Month, which was a period of low solar activity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Frazin, RA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Frazin, Richard/J-2625-2012 NR 17 TC 54 Z9 54 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2002 VL 570 IS 1 BP 408 EP 422 DI 10.1086/339572 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547AG UT WOS:000175309300036 ER PT J AU Mathur, S Wilkes, BJ Ghosh, H AF Mathur, S Wilkes, BJ Ghosh, H TI Chandra detection of highest redshift (z not similar to 6) quasars in X-rays SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; quasars : individual (SDSSp J083643+005453, SDSSp J103027+052455, SDSSp J130608+035626); X-rays : galaxies ID DIGITAL SKY SURVEY; EVOLUTION AB We report on Chandra observations of the three quasars SDSSp J083643+005453, SDSSp J103027+052455, and SDSSp J130608+035626 at redshifts 5.82, 6.28, and 5.99, respectively. All three sources are clearly detected in the X-ray band, up to rest-frame energies of similar to55 keV. These observations demonstrate the unprecedented sensitivity of Chandra to detect faint sources in relatively short exposure times (5.7-8.2 ks). The broadband X-ray properties of these highest redshift quasars do not appear to be any different from their lower redshift cousins, implying little or no evolution for these few sources out to z similar to 6, at redshifts where the optical space density is falling. Spectra of the sources could not be determined with only a few counts detected. Observations with XMM-Newton will be able to constrain the spectral shapes, if they are simple. Determination of complex spectra in a reasonable amount of time, however, will have to await the next generation of X-ray missions. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mathur, S (reprint author), Ohio State Univ, Dept Astron, 174 W 18th Ave, Columbus, OH 43210 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 22 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 MAY 1 PY 2002 VL 570 IS 1 BP L5 EP L8 DI 10.1086/340831 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547AN UT WOS:000175309900002 ER PT J AU Moos, HW Sembach, KR Vidal-Madjar, A York, DG Friedman, SD Hebrard, G Kruk, JW Lehner, N Lemoine, M Sonneborn, G Wood, BE Ake, TB Andre, M Blair, WP Chayer, P Gry, C Dupree, AK Ferlet, R Feldman, PD Green, JC Howk, JC Hutchings, JB Jenkins, EB Linsky, JL Murphy, EM Oegerle, WR Oliveira, C Roth, K Sahnow, DJ Savage, BD Shull, JM Tripp, TM Weiler, EJ Welsh, BY Wilkinson, E Woodgate, BE AF Moos, HW Sembach, KR Vidal-Madjar, A York, DG Friedman, SD Hebrard, G Kruk, JW Lehner, N Lemoine, M Sonneborn, G Wood, BE Ake, TB Andre, M Blair, WP Chayer, P Gry, C Dupree, AK Ferlet, R Feldman, PD Green, JC Howk, JC Hutchings, JB Jenkins, EB Linsky, JL Murphy, EM Oegerle, WR Oliveira, C Roth, K Sahnow, DJ Savage, BD Shull, JM Tripp, TM Weiler, EJ Welsh, BY Wilkinson, E Woodgate, BE TI Abundances of deuterium, nitrogen, and oxygen in the local interstellar medium: Overview of first results from the FUSE mission SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; Galaxy : abundances; ISM : abundances; ISM : evolution; ultraviolet : ISM ID ON-ORBIT PERFORMANCE; D/H RATIO; WHITE-DWARF; SPATIAL VARIATIONS; SIGHT; LINE; ABSORPTION; HYDROGEN; STARS; SPECTROGRAPH AB Observations obtained with the Far Ultraviolet Spectroscopic Explorer ( FUSE) have been used to determine the column densities of D I, N I, and O I along seven sight lines that probe the local interstellar medium (LISM) at distances from 37 to 179 pc. Five of the sight lines are within the Local Bubble, and two penetrate the surrounding H I wall. Reliable values of N ( H I were determined for five of the sight lines from Hubble Space Telescope (HST) data, International Ultraviolet Explorer (IUE) data, and published Extreme Ultraviolet Explorer ( EUVE) measurements. The weighted mean of D I/H I for these five sight lines is (1.52 +/- 0.08) x 10(-5) (1 sigma uncertainty in the mean). It is likely that the D I/H I ratio in the Local Bubble has a single value. The D I/ O I ratio for the five sight lines within the Local Bubble is (3.76 +/- 0.20) x 10(-2). It is likely that O I column densities can serve as a proxy for H I in the Local Bubble. The weighted mean for O I H I for the seven FUSE sight lines is (3.03 +/- 0.21) x 10(-4), comparable to the weighted mean (3.43 +/- 0.15) x 10(-4) reported for 13 sight lines probing larger distances and higher column densities. The FUSE weighted mean of N I/H I for five sight lines is half that reported by Meyer and colleagues for seven sight lines with larger distances and higher column densities. This result combined with the variability of O I/N I ( six sight lines) indicates that at the low column densities found in the LISM, nitrogen ionization balance is important. Thus, unlike O I, N I cannot be used as a proxy for H I or as a metallicity indicator in the LISM. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Inst Astrophys, F-75014 Paris, France. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Natl Inst Stand & Technol, Boulder, CO 80309 USA. Comp Sci Corp, Lanham, MD 20706 USA. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. ESA, Div Astrophys, ISO Data Ctr, Madrid 28080, Spain. Astron Spatiale Lab, F-13376 Marseille 12, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V8X 4M6, Canada. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Gemini Observ, No Operat Ctr, Hilo, HI 96720 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. NASA Headquarters, Washington, DC 20546 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Moos, HW (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RI Oegerle, William/C-9070-2012; Sonneborn, George/D-5255-2012; Woodgate, Bruce/D-2970-2012; Kruk, Jeffrey/G-4047-2012; Howk, Jay/D-2577-2013; Jenkins, Edward/P-5684-2014; OI Jenkins, Edward/0000-0003-1892-4423; Howk, J. Christopher/0000-0002-2591-3792; Murphy, Edward/0000-0003-2925-738X NR 89 TC 142 Z9 142 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2002 VL 140 IS 1 BP 3 EP 17 DI 10.1086/339133 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 541XU UT WOS:000175012500002 ER PT J AU Christy, JH Backwell, PRY Goshima, S Kreuter, T AF Christy, JH Backwell, PRY Goshima, S Kreuter, T TI Sexual selection for structure building by courting male fiddler crabs: an experimental study of behavioral mechanisms SO BEHAVIORAL ECOLOGY LA English DT Article DE behavioral mechanisms; bowers; courtship; female preferences; fiddler crabs; male-built ornaments; sexual selection; Uca musica ID FEMALE CHOICE; MATE CHOICE; UCA-BEEBEI; REPRODUCTIVE SUCCESS; GENUS UCA; OCYPODIDAE; COURTSHIP; SIZE; TERPSICHORES; RESOLUTION AB Males of the fiddler crab Uca musica sometimes build sand hoods at the entrances of their burrows, to which they attract females for mating with claw waving and other displays. Females significantly more often approached males with hoods than males without hoods, but once at a burrow, they were just as likely to stay and mate whether the male had a hood or not. To determine how hoods affect male attractiveness, we conducted experiments that controlled for other differences in courtship behavior between builders and nonbuilders; we removed hood builders' hoods and we added hood models to nonbuilders' burrows. We then measured the attractiveness of hood builders and nonbuilders with and without hoods. Neither manipulation measurably affected male courtship behavior. The presence of a hood did not increase male-female encounter rates, suggesting that hoods do not attract distant females into a male's courtship range. However, once a male courted a female, she was significantly more likely to approach if he had a real or model hood. We obtained direct evidence that females orient to hoods by replacing them with hood models positioned about 3 cm away from the openings to males' burrows. Females approached the models, not the courting males, about 27% of the time. We conclude that hood building is sexually selected because courted females differentially approach hoods, not because hoods attract distant females and not because females prefer to mate with hood builders. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Unit 0948, APO, AA 34003 USA. Hokkaido Univ, Fac Fisheries, Dept Marine Biol Sci, Hakodate, Hokkaido 0418611, Japan. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Backwell, Patricia/C-8883-2009 NR 41 TC 50 Z9 53 U1 3 U2 18 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD MAY PY 2002 VL 13 IS 3 BP 366 EP 374 DI 10.1093/beheco/13.3.366 PG 9 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 552ZK UT WOS:000175650200010 ER PT J AU Garcia, G Alvarez-Valin, F Gomez, N AF Garcia, G Alvarez-Valin, F Gomez, N TI Mitochondrial genes: signals and noise in the phylogenetic reconstruction of the annual killifish genus Cynolebias (Cyprinodontiformes, Rivulidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Cynolebias; killifish; mtDNA; phylogeny ID RIBOSOMAL-RNA; EVOLUTION; DNA; SEQUENCES; PATTERNS; RATES; ATHERINOMORPHA; AMPLIFICATION; COMPILATION; MORPHOLOGY AB The genus Cynolebias (Cyprinodontiformes: Rivulidae) is a locally endemic and speciose group of Neotropical fishes with an annual life cycle. Members of the genus vary greatly in morphology and behaviour, and extensive interspecific karyotypic divergence has been documented among species from Uruguay, Argentina and Rio Grande do Sul, Brazil. We present a molecular systematic hypothesis of the relationships between these Cynolebias species based on phylogenetic analysis of a combined dataset containing 1825 base pairs of DNA sequence, representing three mitochondrial genes. The protein-coding cytochrome-b gene, the 12S and 16S rRNA mitochondrial genes, alone and in combination, yield robust support for monophyly within Cynolebias. Furthermore, our analyses identify two major Cynolebias clades, one of which contains at least four monophyletic groups. Corrected mtDNA genetic distances range from 5.2 to 17.5% between Cynolebias species, and application of a molecular clock suggests the occurrence of two pulses of cladogenesis, one in the late Miocene and another in the Pliocene-Pleistocene. (C) 2002 The Linnean Society of London. C1 Smithsonian Trop Res Inst, Naos Labs, Panama City, Panama. Fac Ciencias, Secc Genet Evol, Montevideo, Uruguay. RP Garcia, G (reprint author), Fac Ciencias, Secc Genet Evol, Igua 4225,CP 11400, Montevideo, Uruguay. NR 50 TC 22 Z9 22 U1 1 U2 7 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD MAY PY 2002 VL 76 IS 1 BP 49 EP 59 DI 10.1111/j.1095-8312.2002.tb01713.x PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 554DK UT WOS:000175718400005 ER PT J AU Jennions, MD Moller, AP AF Jennions, MD Moller, AP TI Publication bias in ecology and evolution: an empirical assessment using the 'trim and fill' method SO BIOLOGICAL REVIEWS LA English DT Article DE effect size; fail-safe number; fluctuating asymmetry; funnel plots; meta-analysis; publication bias; trim and fill ID SEXUAL SELECTION; FLUCTUATING ASYMMETRY; DEVELOPMENTAL STABILITY; BIOLOGICAL-RESEARCH; DRAWER PROBLEM; CLUTCH-SIZE; METAANALYSIS; POPULATIONS; PARADIGM; FITNESS AB Recent reviews of specific topics, such as the relationship between male attractiveness to females and fluctuating asymmetry or attractiveness and the expression of secondary sexual characters, suggest that publication bias might be a problem in ecology and evolution. In these cases, there is a significant negative correlation between the sample size of published studies and the magnitude or strength of the research findings (formally the 'effect size'). If all studies that are conducted are equally likely to be published. irrespective of their findings, there should not be a directional relationship between effect size and sample size: only a decrease in the variance in effect size as sample size increases due to a reduction in sampling error. One interpretation of these reports of negative correlations is that studies with small sample sizes and weaker findings (smaller effect sizes) are less likely to be published. If the biological literature is systematically biased this could undermine the attempts of reviewers to summarise actual biology relationships by inflating estimates of average effect sizes. But how common is this problem? And does it really affect the general conclusions of literature reviews? Here, we examine data sets of effect sizes extracted from 40 peer-reviewed. published meta-analyses. We estimate how many studies are missing using the newly developed 'trim and fill' method. This method uses asymmetry in plots of effect size against sample size ('funnel plots') to detect 'missing' studies. For random-effect models of meta-analysis 38% (15/40) of data sets had a significant number of 'missing' studied. After correcting for potential publication bias, 21% (8/38) of weighted mean effects were no longer significantly greater than zero, and 15% (5/34) were no longer statistically robust when we used random-effects models in a weighted meta-analysis. The mean correlation between sample size and the magnitude of standardised effect size was also significantly negative, (r(s) = -0.20, P < 0.0001). Individual correlations were significantly negative (P<0.10) in 35% (14/40) of cases. Publication bias may therefore affect the main conclusions, of at least 15-21% of meta-analyses. We suggest that future literature reviews assess the robustness of their main conclusions by correcting for potential publication bias using the 'trim and fill' method. C1 Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. Smithsonian Trop Res Inst, APO, AA 34002 USA. Univ Paris 06, CNRS FRE 2365, Lab Ecol Evolut Parasitaire, F-75252 Paris, France. RP Jennions, MD (reprint author), Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 70 TC 95 Z9 96 U1 1 U2 28 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 1464-7931 J9 BIOL REV JI Biol. Rev. PD MAY PY 2002 VL 77 IS 2 BP 211 EP 222 DI 10.1017/S1464793101005875 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 558LA UT WOS:000175966600003 PM 12056747 ER PT J AU McCoy, TJ Robinson, MS Nittler, LR Burbine, TH AF McCoy, TJ Robinson, MS Nittler, LR Burbine, TH TI The near earth asteroid rendezvous mission to asteroid 433 Eros: A milestone in the study of asteroids and their relationship to meteorites SO CHEMIE DER ERDE-GEOCHEMISTRY LA English DT Review DE meteorites; asteroids; 433 Eros; NEAR MISSION; spacecraft missions; asteroid chemistry; asteroid geology; meteorite-asteroid links ID NEAR-SHOEMAKER SPACECRAFT; SMALL-SCALE FEATURES; EJECTA BLOCKS; MULTISPECTRAL IMAGER; RAY SPECTROMETER; MAGNETIC-FIELD; 433-EROS; INSTRUMENTATION; 253-MATHILDE; REGOLITH AB A milestone in the study of asteroids occurred on 14 Feb 2000, when the NEAR spacecraft entered orbit around the asteroid 433 Eros for a year of detailed observation of the geology, mineralogy and chemistry of the surface, before landing on the surface on 12 Feb 2001 and conducting the first science on the surface of a small Solar System body. This paper reviews the scientific results of THE NEAR MISSION. Eros is irregularly shaped, can be described by a best fit ellipse measuring 35 by 10.2 by 10.2 km, with a complex surface that includes a global regolith, asymmetrically distributed population of boulders, heavily cratered surface at diameters above 200 m, and grooves and ridges thought to record broad scale tectonic deformation. Significant albedo differences are associated with steeply sloping surfaces, indicating downslope movement of "relatively dark" regolith, leaving behind "fresher," "less-altered" material. The spectrally-derived mineral compositions and olivine: pyroxene ratio. absence of a global magnetic field, and the Mg/Si, Al/Si and Ca/Si ratios and K concentrations point to a primitive, chondritic body (most likely an ordinary chondrite), while a strong apparently-global depletion in sulfur and lower Fe/Si and Fe/O ratios at the landing site relative to ordinary chondrites are likely due to metal and sulfide migration due to partial melting throughout the entire asteroid or, more likely. through processing of the regolith layer by micrometeorite bombardment, sputtering and/or size/density segregations. Synthesis of the spectral and chemical data suggest the most likely meteoritic analog is either an ordinary chondritic composition that experienced alteration at the surface or less likely a primitive achondrite formed from an ordinary chondritic precursor. The markedly different compositions from the X-ray and gamma-ray experiments can be reconciled with a common silicate mineralogy through variable abundances of metal and/or sulfide. As we begin our detailed exploration of the diverse group of small bodies that make up the asteroid belt, NEAR has provided both a technical and scientific blueprint for the future. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP McCoy, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 72 TC 9 Z9 9 U1 1 U2 2 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0009-2819 J9 CHEM ERDE-GEOCHEM JI Chem Erde-Geochem. PD MAY PY 2002 VL 62 IS 2 BP 89 EP 121 DI 10.1078/0009-2819-00004 PG 33 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 584KJ UT WOS:000177465500001 ER PT J AU Helly, JJ Elvins, TT Sutton, D Martinez, D Miller, SE Pickett, S Ellison, AM AF Helly, JJ Elvins, TT Sutton, D Martinez, D Miller, SE Pickett, S Ellison, AM TI Controlled publication of digital scientific data SO COMMUNICATIONS OF THE ACM LA English DT Article ID LIBRARIES; WEB C1 Univ Calif San Diego, San Diego Supercomp Ctr, San Diego, CA 92103 USA. Oracle Corps Voice Lab, San Diego, CA USA. Univ Calif San Diego, San Diego Supercomp Ctr, San Diego, CA USA. Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC USA. Inst Ecosyst Studies, Millbrook, NY 12545 USA. Mt Holyoke Coll, S Hadley, MA 01075 USA. RP Helly, JJ (reprint author), Univ Calif San Diego, San Diego Supercomp Ctr, San Diego, CA 92103 USA. OI Ellison, Aaron/0000-0003-4151-6081; Miller, Scott/0000-0002-4138-1378 NR 12 TC 2 Z9 2 U1 0 U2 2 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036 USA SN 0001-0782 J9 COMMUN ACM JI Commun. ACM PD MAY PY 2002 VL 45 IS 5 BP 97 EP 101 DI 10.1145/506218.506222 PG 5 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 544NC UT WOS:000175165600028 ER PT J AU Eberhard, JR AF Eberhard, JR TI Cavity adoption and the evolution of coloniality in cavity-nesting birds SO CONDOR LA English DT Article DE Anseriformes; birds; cavity nesting; colonial nesting; comparative method ID LIFE-HISTORY TRAITS; CORRELATED EVOLUTION; CHARACTERS; FOOD; PREDATION; SITES AB Among cavity-nesting birds, a distinction can he made between excavators, which dig their own cavities, and cavity-adopters. which nest in pre-existing cavities. Historically, these two types of species have been grouped together as "cavity-nesters," but it has become clear that the two nesting habits are associated with very different suites of life-history characters. This paper tests the hypothesis that cavity-adopters differ from excavators and other nest-building species in their propensity to evolve colonial breeding. Because of their dependence on pre-existing cavities, cavity-adopters presumably have less control than excavators over the location of their nests, and this could limit their ability to nest near conspecifics. A literature survey of the nesting behavior of 842 species in 17 bird families shows that coloniality almost never occurs in species that arc obligate cavity-adopters. A phylogeny-based comparative analysis of nesting behavior in the Anseriformes indicates that in this group. colonial breeding has evolved less frequently in lineages of cavity-adopters than would he expected by chance. Together; this evidence support, the hypothesis that colonial breeding systems are unlikely to evolve in lineages of cavity-adopters. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Eberhard, JR (reprint author), Cornell Univ, Ornithol Lab, Macaulay Lib Nat Sounds, 159 Sapsucker Woods Rd, Ithaca, NY 14850 USA. NR 36 TC 12 Z9 12 U1 1 U2 10 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD MAY PY 2002 VL 104 IS 2 BP 240 EP 247 DI 10.1650/0010-5422(2002)104[0240:CAATEO]2.0.CO;2 PG 8 WC Ornithology SC Zoology GA 548RF UT WOS:000175402500002 ER PT J AU South, JM Wright, TF AF South, JM Wright, TF TI Nestling sex ratios in the Yellow-naped Amazon: No evidence for adaptive modification SO CONDOR LA English DT Article DE Amazona auropalliata; CHD gene; molecular sexing; sex ratio; Yellow-naped Amazon ID LOCAL RESOURCE COMPETITION; ALLOCATION; POPULATION; PARROTS; BIRDS; IDENTIFICATION; SWALLOWS; DIALECTS AB Many birds, including some parrots, may adjust the sex ratio of their offspring in relation to the relative fitness benefits of sons and daughters. We investigated nestling sex ratios in Yellow-naped Amazons (Amazona auropalliata) using a molecular sexing technique that amplifies intronic regions of the CHD-W and CHD-Z genes in birds. We examined all nestlings in 37 complete clutches comprising 77 chicks. The overall nestling sex ratio did not differ from unity. Sex allocation was not associated with hatch date, sequence of hatching, or clutch size. We also found no difference in sex ratio between two regional dialects. Female Yellow-naped Amazons may be unable to control their hatchling sex ratio. Alternatively, there may be no fitness benefits to females producing more of one sex in relation to the factors we measured here. C1 Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Wright, TF (reprint author), Smithsonian Inst, Genet Mol Lab, Natl Zool Pk,3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Munshi-South, Jason/A-3385-2009 NR 24 TC 15 Z9 15 U1 2 U2 4 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD MAY PY 2002 VL 104 IS 2 BP 437 EP 440 DI 10.1650/0010-5422(2002)104[0437:NSRITY]2.0.CO;2 PG 4 WC Ornithology SC Zoology GA 548RF UT WOS:000175402500021 ER PT J AU Aronson, RB Macintyre, IG Precht, WF Murdoch, TJT Wapnick, CM AF Aronson, RB Macintyre, IG Precht, WF Murdoch, TJT Wapnick, CM TI The expanding scale of species turnover events on coral reefs in Belize SO ECOLOGICAL MONOGRAPHS LA English DT Review DE Acropora; Agaricia; Belilze; Caribbean; coral bleaching; coral disease; coral reef; Holocene; paleoecology; patch dynamics; species turnover; white-band disease ID CARIBBEAN PLATE MOVEMENTS; COMMUNITY STRUCTURE; SOUTHERN LAGOON; ACROPORA-CERVICORNIS; MACROALGAL COVER; JUVENILE CORALS; HOLOCENE REEF; WEST-INDIES; ZONATION; PATTERNS AB Beginning in the late 1980s, white-band disease nearly eliminated the staghorn coral Acropora cervicornis from reefs in the central shelf lagoon of Belize. The lettuce coral Agaricia tenuifolia replaced Acropora cervicornis in the early 1990s, but anomalously high water temperatures in 1998 caused severe bleaching and catastrophic mortality of Agaricia tenuifolia. The short-lived transition in dominance from Acropora cervicornis to Agaricia tenuifolia left an unambiguous signature in the fossil record of these uncemented lagoonal reefs. Analysis of 38 cores, extracted from 22 sampling stations in a 375-km(2) area of the central lagoon. showed that Acropora cervicornis dominated continuously for at least 3000 years prior to the recent events. Agaricia tenuifolia occasionally grew in small patches, but no coral-to-coral replacement sequence occurred over the entire area until the late 1980s. Within a decade, the scale of species turnover increased from tens of square meters or less to hundreds of square kilometers or more. This unprecedented increase in the scale of turnover events is rooted in the accelerating pace of ecological change on coral reefs at the regional level. C1 Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA. Univ S Alabama, Dept Marine Sci, Mobile, AL 36688 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. PBS&J, Miami, FL 33172 USA. RP Aronson, RB (reprint author), Dauphin Isl Sea Lab, 101 Bienville Blvd,Dauphin Isl, Dauphin Isl, AL 36528 USA. EM raronson@disl.org RI kohki, sowa/D-2955-2011 NR 106 TC 102 Z9 114 U1 2 U2 29 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9615 EI 1557-7015 J9 ECOL MONOGR JI Ecol. Monogr. PD MAY PY 2002 VL 72 IS 2 BP 233 EP 249 DI 10.1890/0012-9615(2002)072[0233:TESOST]2.0.CO;2 PG 17 WC Ecology SC Environmental Sciences & Ecology GA 544FP UT WOS:000175147800005 ER PT J AU Moegenburg, SM Levey, DJ AF Moegenburg, SM Levey, DJ TI Prospects for conserving biodiversity in Amazonian extractive reserves SO ECOLOGY LETTERS LA English DT Article DE Amazonia; biodiversity; Euterpe oleracea; extractive reserves; frugivores; fruit harvest; non-timber forest products ID TROPICAL FOREST; ECONOMIC VALUE; RAIN-FOREST; ESTUARY; PATTERNS; FUTURE; BRAZIL; IMPOVERISHMENT; CONSERVATION; STRATEGIES AB Non-timber forest product (NTFP) extraction is a popular alternative to timber extraction that figures prominently in efforts to utilize tropical forests sustainably. But the ability to conserve biodiversity through NTFP management, particularly in extractive reserves in Amazonia, has remained untested. We found that intensive management of Euterpe oleracea (Palmae) fruit, one of the most important extractive products in the Amazon, has substantial impacts on biodiversity, whereas moderate management does not. We mimicked traditional levels of fruit harvest in a replicated experiment over one fruiting season. High-intensity harvest (75% of fruits removed) reduced avian frugivore species diversity by 22%. Low-intensity harvest (40% of fruits removed), however, had no effect on diversity. On a larger scale, we found that forests with enriched densities of E. oleracea supported more fruit-eating birds but fewer non fruit-eating birds than non-enriched forests. Taken together, these results suggest that intensive NTFP management to meet market demands may trigger substantial ecological impacts, at least at the level of our study. E. oleracea harvest should be limited where conservation of biodiversity is a goal. 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. NR 35 TC 22 Z9 24 U1 0 U2 20 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD MAY PY 2002 VL 5 IS 3 BP 320 EP 324 DI 10.1046/j.1461-0248.2002.00323.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 549YV UT WOS:000175476200002 ER PT J AU Dallmeier, F Alonso, A Jones, M AF Dallmeier, F Alonso, A Jones, M TI Planning an adaptive management process for biodiversity conservation and resource development in the Camisea River basin SO ENVIRONMENTAL MONITORING AND ASSESSMENT LA English DT Article DE adaptive management; Amazon Basin; biodiversity; conservation; resource exploration AB The Smithsonian Institution's Monitoring and Assessment of Biodiversity Program joined Shell Prospecting and Development Peru (SPDP) to protect biodiversity during a natural gas exploration project. Emphasis was on long-term societal and environmental benefits in addition to financial gain for the company. The systematic, cyclical adaptive management process was used to generate feedback for SPDP managers. Adaptive management enables ongoing improvement of management policies and practices based on lessons learned from operational activities. Previous to this study, very little information about the local biodiversity was available. Over a 2-year period, the team conducted biological assessments of six taxonomic groups at five sites located within 600 km(2). A broad range of management options such as location, timing and technology were developed from the beginning of the project. They were considered in conjunction with emerging lessons from the biodiversity assessments. Critical decisions included location of a gas plant and the cost of helicopter access versus roads to service the full field development. Both of these decisions were evaluated to ensure that they were economically and environmentally feasible. Project design changes, addressed in the planning stage, were accepted once consensus was achieved. Stakeholders were apprised of the implications of the baseline biodiversity assessments. C1 Natl Zool Pk, Conservat & Res Ctr, Monitoring & Assessment Biodivers Program, Smithsonian Inst, Washington, DC 20560 USA. RP Dallmeier, F (reprint author), Natl Zool Pk, Conservat & Res Ctr, Monitoring & Assessment Biodivers Program, Smithsonian Inst, 1100 Jefferson Dr SW,Suite 3123, Washington, DC 20560 USA. NR 34 TC 9 Z9 9 U1 1 U2 13 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-6369 J9 ENVIRON MONIT ASSESS JI Environ. Monit. Assess. PD MAY PY 2002 VL 76 IS 1 BP 1 EP 17 DI 10.1023/A:1015256119375 PG 17 WC Environmental Sciences SC Environmental Sciences & Ecology GA 545JK UT WOS:000175213600001 PM 12125744 ER PT J AU Campbell, P Comiskey, J Alonso, A Dallmeier, F Nunez, P Beltran, H Baldeon, S Nauray, W De La Colina, R Acurio, L Udvardy, S AF Campbell, P Comiskey, J Alonso, A Dallmeier, F Nunez, P Beltran, H Baldeon, S Nauray, W De La Colina, R Acurio, L Udvardy, S TI Modified whittaker plots as an assessment and monitoring tool for vegetation in a lowland tropical rainforest SO ENVIRONMENTAL MONITORING AND ASSESSMENT LA English DT Article DE assessment; modified Whittaker plots; monitoring; tropical forests ID STATISTICAL POWER ANALYSIS; RAIN-FOREST; AMAZONIAN FORESTS; SPECIES RICHNESS; SAMPLING METHOD; DIVERSITY; PATTERNS; TREE; MANAGEMENT; TRENDS AB Resource exploitation in lowland tropical forests is increasing and causing loss of biodiversity. Effective evaluation and management of the impacts of development on tropical forests requires appropriate assessment and monitoring tools. We propose the use of 0.1-ha multi-scale, modified Whittaker plots (MWPs) to assess and monitor vegetation in lowland tropical rainforests. We established MWPs at 4 sites to: (1) describe and compare composition and structure of the sites using MWPs, (2) compare these results to those of 1-ha permanent vegetation plots (BDPs), and (3) evaluate the ability of MWPs to detect changes in populations (statistical power). We recorded more than 400 species at each site. Species composition among the sites was distinctive, while mean abundance and basal area was similar. Comparisons between MWPs and BDPs show that they record similar species composition and abundance and that both perform equally well at detecting rare species. However, MWPs tend to record more species, and power analysis studies show that MWPs were more effective at detecting changes in the mean number of species of trees greater than or equal to10 cm in diameter at breast height (dbh) and in herbaceous plants. Ten MWPs were sufficient to detect a change of 11% in the mean number of herb species, and they were able to detect a 14% change in the mean number of species of trees greater than or equal to10 cm dbh. The value of MWPs for assessment and monitoring is discussed, along with recommendations for improving the sampling design to increase power. C1 Natl Zool Pk, Conservat Res Ctr, Monitoring & Assessment Biodivers Program, Smithsonian Inst, Washington, DC 20560 USA. RP Campbell, P (reprint author), Natl Zool Pk, Conservat Res Ctr, Monitoring & Assessment Biodivers Program, Smithsonian Inst, 1100 Jefferson Dr SW,Suite 3123, Washington, DC 20560 USA. NR 51 TC 9 Z9 10 U1 1 U2 11 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-6369 J9 ENVIRON MONIT ASSESS JI Environ. Monit. Assess. PD MAY PY 2002 VL 76 IS 1 BP 19 EP 41 DI 10.1023/A:1015264720284 PG 23 WC Environmental Sciences SC Environmental Sciences & Ecology GA 545JK UT WOS:000175213600002 PM 12125748 ER PT J AU Angehr, GR Siegel, J Aucca, C Christian, DG Pequeno, T AF Angehr, GR Siegel, J Aucca, C Christian, DG Pequeno, T TI An assessment and monitoring program for birds in the Lower Urubamba Region, Peru SO ENVIRONMENTAL MONITORING AND ASSESSMENT LA English DT Article DE adaptive management; assessment; birds; development; monitoring; tropical forests ID BARRO-COLORADO ISLAND; TRANSECT COUNTS; FOREST; DENSITIES; COMMUNITY; EDGE; ORGANIZATION; POPULATIONS; PREDATION; CORRIDOR AB We developed an assessment and monitoring plan for birds in connection with the exploration and potential development of a large natural gas field in the Lower Urubamba drainage of Peru, a project of Shell Prospecting and Development Peru (SPDP). Our objectives were to: (1) inventory the birds in the area, including information on habitat use and abundance, and (2) devise long-term monitoring protocols for birds. We sampled birds through a combination of visual and auditory surveys and mist-netting at 4 well sites and 3 sites along the Urubamba and Camisea rivers. We recorded 420 species during 135 days of field work. We consider the highest priorities for a future monitoring program to be: (1) establish whether edge effects are occurring at well sites, along roads and along the planned pipeline route and determine the significance and extent of these effects and (2) assess the impact of increased human access to the area on game and other exploited species. The remoteness of the area, its rugged terrain and dense vegetation and the lack of trained personnel limit the choice of survey and monitoring methods. We recommend use of mist-netting and transects for monitoring edge effects and use of transects for monitoring game and other exploited species. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Angehr, GR (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 62 TC 2 Z9 2 U1 1 U2 7 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-6369 J9 ENVIRON MONIT ASSESS JI Environ. Monit. Assess. PD MAY PY 2002 VL 76 IS 1 BP 69 EP 87 DI 10.1023/A:1015220921192 PG 19 WC Environmental Sciences SC Environmental Sciences & Ecology GA 545JK UT WOS:000175213600005 PM 12125751 ER PT J AU Mateos, M Sanjur, OI Vrijenhoek, RC AF Mateos, M Sanjur, OI Vrijenhoek, RC TI Historical biogeography of the livebearing fish genus Poeciliopsis (Poeciliidae : Cyprinodontiformes) SO EVOLUTION LA English DT Article DE Bayesian inference; mitochondrial; molecular clocks; parametric bootstrap; phylogeny; phylogeography; vicariance ID NADH DEHYDROGENASE SUBUNIT-2; MEXICAN VOLCANIC BELT; MOLECULAR PHYLOGENETICS; CONSERVATION GENETICS; PARAMETRIC BOOTSTRAP; NUCLEOTIDE-SEQUENCES; MITOCHONDRIAL-DNA; WESTERN MEXICO; EVOLUTION; INFERENCE AB To assess the historical biogeography of freshwater topminnows in the genus Poeciliopsis, we examined sequence variation in two mitochondrial genes, cytochrome b (1140 bp) and NADH subunit 2 (1047 bp). This widespread fish genus is distributed from Arizona to western Colombia, and nearly half of its 21 named species have distributions that border on the geologically active Trans-Mexican Volcanic Belt (TMVB), a region that defines the uplifted plateau (Mesa Central) of Mexico. We used the parametric bootstrap method to test the hypothesis that a single vicariant event associated with the TMVB was responsible for divergence of taxa found to the north and south of this boundary. Because the single-event hypothesis was rejected as highly unlikely, we hypothesize that at least two geological events were responsible for divergence of these species. The first (8-16 million years ago) separated ancestral populations that were distributed across the present TMVB region. A second event (2.8-6.4 million years ago) was associated with northward dispersal and subsequent vicariance of two independent southern lineages across the TMVB. The geological history of this tectonically and volcanically active region is discussed and systematic implications for the genus are outlined. C1 Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. Smithsonian Trop Res Inst, Naos Marine Lab Unit 0948, APO, AA 34002 USA. RP Mateos, M (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. RI Mateos, Mariana/B-5235-2008 OI Mateos, Mariana/0000-0001-5738-0145 NR 74 TC 71 Z9 76 U1 1 U2 15 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD MAY PY 2002 VL 56 IS 5 BP 972 EP 984 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 560JH UT WOS:000176078600010 PM 12093032 ER PT J AU Anderson, RP Handley, CO AF Anderson, RP Handley, CO TI Dwarfism in insular sloths: Biogeography, selection, and evolutionary rate SO EVOLUTION LA English DT Review DE Bradypus; body size; darwins; haldanes; island; selection differential; selection intensity ID QUANTITATIVE-GENETIC-ANALYSIS; BRADYPUS-TORQUATUS XENARTHRA; BODY-SIZE; MORPHOLOGICAL EVOLUTION; PHYLOGENETIC ANALYSIS; ISLAND BIOGEOGRAPHY; FRENCH-GUIANA; HOUSE MICE; MAMMALS; EXTINCTION AB The islands of Bocas del Toro, Panama, were sequentially separated from the adjacent mainland by rising sea levels during the past 10,000 years. Three-toed sloths (Bradypus) from five islands are smaller than their mainland counterparts, and the insular populations themselves vary in mean body size. We first examine relationships between body size and physical characteristics of the islands, testing hypotheses regarding optimal body size, evolutionary equilibria, and the presence of dispersal in this system. To do so, we conduct linear regressions of body size onto island area, distance from the mainland, and island age. Second, we retroactively calculate two measures of the evolutionary rate of change in body size (haldanes and darwins) and the standardized linear selection differential, or selection intensity (i). We also test the observed morphological changes against models of evolution by genetic drift. The results indicate that mean body size decreases linearly with island age, explaining up to 97% of the variation among population means. Neither island area nor distance from the mainland is significant in multiple regressions that include island age. Thus, we find no evidence for differential optimal body size among islands, or for dispersal in the system. In contrast, the dependence of body size on island age suggests uniform directional selection for small body size in the insular populations. Although genetic drift cannot be discounted as the cause for this evolution in body size, the probability is small given the consistent direction of evolution (repeated dwarfism). The insular sloths show a sustained rate of evolution similar to those measured in haldanes over tens of generations, appearing to unite micro- and macroevolutionary time scales. Furthermore, the magnitude and rate of this example of rapid differentiation fall within predictions of theoretical models from population genetics. However, the linearity of the relationship between body size and island age is not predicted, suggesting that either more factors are involved than those considered here, or that theoretical advances are necessary to explain constant evolutionary rates over long time spans in new selective environments. C1 Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. Univ Kansas, Museum Nat Hist, Lawrence, KS 66045 USA. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. RP Anderson, RP (reprint author), Amer Museum Nat Hist, Div Vertebrate Zool Mammal, Cent Pk W & 79th St, New York, NY 10024 USA. NR 101 TC 62 Z9 65 U1 3 U2 36 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD MAY PY 2002 VL 56 IS 5 BP 1045 EP 1058 PG 14 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 560JH UT WOS:000176078600016 PM 12093018 ER PT J AU Christensen, LE Okumura, M Sander, SP Salawitch, RJ Toon, GC Sen, B Blavier, JF Jucks, KW AF Christensen, LE Okumura, M Sander, SP Salawitch, RJ Toon, GC Sen, B Blavier, JF Jucks, KW TI Kinetics of HO2+HO2 -> H2O2+O-2: Implications for stratospheric H2O2 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TEMPERATURE-DEPENDENCE; SELF-REACTION; ATMOSPHERIC CHEMISTRY; HO2; RADICALS; O-3; PRESSURES; HO2+HO2; DO2 AB [1] The reaction HO2 + HO2 --> H2O2 + O-2 (1) has been studied at 100 Torr and 222 K to 295 K. Experiments employing photolysis of Cl-2/CH3OH/O-2/N-2 and F-2/H-2/O-2/N-2 gas mixtures to produce HO2 confirmed that methanol enhanced the observed reaction rate. At 100 Torr, zero methanol, k(1) = (8.8 +/- 0.9) 10(-13) x exp[(210 +/- 26)/T] cm(3) molecule(-1) s(-1) (2 uncertainties), which agrees with current recommendations at 295 K but is nearly 2 times slower at 231 K. The general expression for k(1), which includes the dependence on bath gas density, is k(1) = (1.5 +/- 0.2) x 10(-12) exp[(19 +/- 31)/T] + 1.7 x 10(-33) [M] x exp[1000/T], where the second term is taken from the JPL00-3 recommendation. The revised rate largely accounts for a discrepancy between modeled and measured [H2O2] in the lower to middle stratosphere. C1 CALTECH, Arthur Amos Noyes Lab Chem Phys, Div Chem & Chem Engn, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP CALTECH, Arthur Amos Noyes Lab Chem Phys, Div Chem & Chem Engn, Pasadena, CA 91125 USA. RI Salawitch, Ross/B-4605-2009; Okumura, Mitchio/I-3326-2013 OI Salawitch, Ross/0000-0001-8597-5832; Okumura, Mitchio/0000-0001-6874-1137 NR 16 TC 37 Z9 38 U1 1 U2 14 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 MAY 1 PY 2002 VL 29 IS 9 AR 1299 DI 10.1029/2001GL014525 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 609DH UT WOS:000178888000063 ER PT J AU Rasse, DP AF Rasse, DP TI Nitrogen deposition and atmospheric CO2 interactions on fine root dynamics in temperate forests: a theoretical model analysis SO GLOBAL CHANGE BIOLOGY LA English DT Article DE atmospheric nitrogen deposition; below-ground allocation; elevated CO2; root demography; root longevity; soil respiration ID SOIL-N AVAILABILITY; NORTHERN HARDWOOD FORESTS; ELEVATED CO2; POPULUS-TREMULOIDES; PINUS-RADIATA; CARBON ALLOCATION; SPRUCE SEEDLINGS; NUTRIENT-UPTAKE; PONDEROSA PINE; LIFE-SPAN AB Fine root turnover is a critical component of below-ground forest ecology, which regulates nutrient dynamics, forest net primary productivity, carbon input to soils, and soil respiration. Understanding fine root responses to changing environmental conditions is critical for predicting the productivity and carbon sequestration potential of forest ecosystems during the 21st century. The first objective of this study is to demonstrate that a mechanistic model can realistically simulate spatial and temporal fine root demography in temperate forests on the basis of two hypotheses: (1) absorption of mineral N (N) stimulates the production of new roots, and (2) fine root longevity decreases with increasing N availability. Based on this model, my second objective is to predict fine root responses to changing atmospheric CO2 levels and N deposition rates. To meet these objectives, an extensive description of the N cycle and the new fine root module were implemented in the ASPECTS model. In agreement with a wide body of literature information, the new model predicted: (1) a preferential colonisation by fine roots of the uppermost soil layer, and (2) a flush of fine root growth in the spring. The simulations indicate that fine root biomass will increase in response to elevated CO2 under the double effect of (1) an increase in root longevity due to increased N stress, and (2) larger amounts of assimilates available to the growth of plant tissue due to increased photosynthesis. Although the simulated total fine root biomass increased under both increasing N deposition rates and atmospheric CO2 concentrations, the model predicts that the distribution of fine roots among soil layers will be altered. This suggests that experimental studies must consider the full depth of the root system in order to accurately assess effects of environmental changes on fine root dynamics. The model also suggests that fine root longevity is a plastic parameter, which varied from less than 1 year to more than 3 years depending on forcing values of N deposition rates and atmospheric CO2 concentrations. Finally, the model indicates that the increase in net ecosystem exchange (NEE) and soil respiration in temperate forests under elevated CO2 will be proportional to the amount of available N, with little to no response in low N conditions and up to +28% for both NEE and soil respiration under the highest deposition rate (7.0 g N m(-2) y(-1)). C1 Univ Liege, Lab Planetary & Atmospher Phys, B-4000 Liege, Belgium. RP Rasse, DP (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. OI Daniel, Rasse/0000-0002-5977-3863 NR 76 TC 20 Z9 23 U1 0 U2 23 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAY PY 2002 VL 8 IS 5 BP 486 EP 503 DI 10.1046/j.1365-2486.2002.00481.x PG 18 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 549CE UT WOS:000175426300006 ER PT J AU DiMichele, WA Phillips, TL Nelson, WJ AF DiMichele, WA Phillips, TL Nelson, WJ TI Place vs. time and vegetational persistence: a comparison of four tropical mires from the Illinois Basin during the height of the Pennsylvanian ice age SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Article DE paleoecology; coal; coal ball; ecosystem stability; Pennsylvanian; Illinois Basin; Springfield coal; Herrin coal; Baker coal; Danville coal ID COAL-SWAMP VEGETATION; SPRINGFIELD COAL; CLASTIC-SWAMP; PEAT; COMMUNITIES; EURAMERICA; PATTERNS; INDIANA; PLANTS; USA AB Coal balls were collected from four coal beds in the southeastern part of the Illinois Basin. Collections were made from the Springfield, Herrin, and Baker coals in western Kentucky, and from the Danville Coal in southwestern Indiana. These four coal beds are among the principal mineable coals of the Illinois Basin and belong to the Carbondale and Shelburn Formations of late Middle Pennsylvanian age. Vegetational composition was analyzed quantitatively. Coal-ball samples from the Springfield, Herrin, and Baker are dominated by the lycopsid tree Lepidophloios, with lesser numbers of Psaronius tree ferns, medullosan pteridosperms, and the lycopsid trees Synchysidendron and Diaphorodendron. This vegetation is similar to that found in the Springfield and Herrin coals elsewhere in the Illinois Basin, as reported in previous studies. The Danville coal sample, which is considerably smaller than the others, is dominated by Psaronius with the lycopsids Sigillaria and Synchysidendron as subdominants. Coal balls from the Springfield coal were collected in zones directly from the coal bed and their zone-by-zone composition indicates three to four distinct plant assemblages. The other coals were analyzed as whole-seam random samples, averaging the landscape composition of the parent mire environments. This analysis indicates that these coals, separated from each other by marine and terrestrial-clastic deposits, have essentially the same floristic composition and, thus, appear to represent a common species pool that persisted throughout the late Middle Pennsylvanian, despite changes in baselevel and climate attendant the glacial-interglacial cyclicity of the Pennsylvanian ice age. Patterns of species abundance and diversity are much the same for the Springfield, Herrin, and Baker, although each coal, both in the local area sampled, and regionally, has its own paleobotanical peculiarities. Despite minor differences, these coals indicate a high degree of recurrence of assemblage and landscape organization. The Danville departs dramatically from the dominance-diversity composition of the older coals, presaging patterns of tree-fern and Sigillaria dominance of Late Pennsylvanian coals of the eastern United States, but, nonetheless, built on a species pool shared with the older coals. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Smithsonian Inst, Museum Natl Hist Nat, NMNH, Dept Paleobiol, Washington, DC 20560 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Illinois State Geol Survey, Basin Anal Sect, Champaign, IL 61820 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, Museum Natl Hist Nat, NMNH, Dept Paleobiol, Washington, DC 20560 USA. RI DiMichele, William/K-4301-2012 NR 54 TC 34 Z9 34 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD MAY PY 2002 VL 50 IS 1-4 BP 43 EP 72 AR PII S0166-5162(02)00113-1 DI 10.1016/S0166-5162(02)00113-1 PG 30 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA 612HD UT WOS:000179067600003 ER PT J AU Novotny, V Basset, Y Miller, SE Drozd, P Cizek, L AF Novotny, V Basset, Y Miller, SE Drozd, P Cizek, L TI Host specialization of leaf-chewing insects in a New Guinea rainforest SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE herbivore communities; insect-plant interactions; Papua New Guinea; species richness; tropical forests ID PAPUA-NEW-GUINEA; PHYTOPHAGOUS INSECTS; SPECIES RICHNESS; DECIDUOUS FOREST; HERBIVORES; COMMUNITIES; SPECIFICITY; DIVERSITY; FICUS; ABUNDANCE AB 1. Data on host use by herbivorous insects in the tropics cannot be cross-referenced between the studies as only a fraction of the species can be formally identified. It is thus imperative for each study to include a wide range of plant and insect taxa, but this requirement has rarely been met because of logistical difficulties. 2. A novel approach using mass insect collecting and rearing by parataxonomists was applied to study the use of 59 species, 39 genera and 18 families of woody plants by 58 588 individuals and 1010 species of leaf-chewing insects in a lowland rainforest. 3. Most species had wide host plant ranges with reference to congeneric plants. The modal host range for a herbivore feeding on a particular genus (Ficus, Macaranga or Psychotria) included >90% of congeneric species studied. Only 3.7% of species feeding on these genera were monophagous. 4. Most herbivores were specialized with respect to confamilial plant genera, with modal host range of 1 genus from 9 studied in Euphorbiaceae and 13 in Rubiaceae. This pattern was corroborated by modal host range of 1 plant family from 18 studied. 5. Because of the overlap among the herbivore communities on congeneric plants, the total number of herbivores on speciose plant genera was relatively small. For example, although 336 species of leaf-chewers used the 13 study species of Ficus, the 35 additional Ficus species present locally would support only estimated 163 additional species. 6. Since large genera constitute a significant proportion of tropical floras, these results have implications for regional estimates of herbivore species richness. Our estimate of 10.6-24.1 leaf-chewing species effectively specialized to a rainforest tree species is an order of magnitude lower than previously suggested. 7. The number of new herbivore species (y) resulting from the addition of the xth plant species to the compound community (x = 1, 2, 3,..., n where n is the total number of plants studied) can be described as y = cx(k), where c and k are constants. k is a useful descriptor of similarity among herbivore communities from different hosts. C1 Acad Sci Czech Republic, Inst Entomol, CZ-37005 Ceske Budejovice, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice 37005, Czech Republic. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Int Ctr Insect Physiol & Ecol, Nairobi, Kenya. Univ Ostrava, Dept Biol, Ostrava 70103, Czech Republic. RP Novotny, V (reprint author), Acad Sci Czech Republic, Inst Entomol, Branisovska 31, CZ-37005 Ceske Budejovice, Czech Republic. EM novotny@entu.cas.cz RI Drozd, Pavel/J-3943-2013; Basset, Yves/B-6642-2014; Cizek, Lukas/G-7905-2014; Novotny, Vojtech/G-9434-2014; Cizek, Lukas/K-7111-2015; OI Drozd, Pavel/0000-0002-4602-8856; Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 70 TC 66 Z9 70 U1 4 U2 22 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0021-8790 J9 J ANIM ECOL JI J. Anim. Ecol. PD MAY PY 2002 VL 71 IS 3 BP 400 EP 412 DI 10.1046/j.1365-2656.2002.00608.x PG 13 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 551AE UT WOS:000175536600003 ER PT J AU Laurance, WF Albernaz, AKM Schroth, G Fearnside, PM Bergen, S Venticinque, EM Da Costa, C AF Laurance, WF Albernaz, AKM Schroth, G Fearnside, PM Bergen, S Venticinque, EM Da Costa, C TI Predictors of deforestation in the Brazilian Amazon SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Amazon; Brazil; deforestation; government policy; habitat fragmentation; highways; human population size; rainfall; rainforest; roads; soil fertility ID RAIN-FOREST FRAGMENTATION; TROPICAL DEFORESTATION; HABITAT FRAGMENTATION; CONSERVATION; BIOMASS; CARBON; SCALE; FIRE AB Aim and Location We assessed the effects of biophysical and anthropogenic predictors on deforestation in Brazilian Amazonia. This region has the world's highest absolute rates of forest destruction and fragmentation. Methods Using a GIS, spatial data coverages were developed for deforestation and for three types of potential predictors: (1) human-demographic factors (rural-population density, urban-population size); (2) factors that affect physical accessibility to forests (linear distances to the nearest paved highway, unpaved road and navigable river), and (3) factors that may affect land-use suitability for human occupation and agriculture (annual rainfall, dry-season severity, soil fertility, soil waterlogging, soil depth). To reduce the effects of spatial autocorrelation among variables, the basin was subdivided into >1900 quadrats of 50 x 50 km, and a random subset of 120 quadrats was selected that was stratified on deforestation intensity. A robust ordination analysis (non-metric multidimensional scaling) was then used to identify key orthogonal gradients among the ten original predictor variables. Results The ordination revealed two major environmental gradients in the study area. Axis 1 discriminated among areas with relatively dense human populations and highways, and areas with sparse populations and no highways; whereas axis 2 described a gradient between wet sites having low dry-season severity, many navigable rivers and few roads, and those with opposite values. A multiple regression analysis revealed that both factors were highly significant predictors, collectively explaining nearly 60% of the total variation in deforestation intensity (F (2,117) = 85.46, P < 0.0001). Simple correlations of the original variables were highly concordant with the multiple regression model and suggested that highway density and rural-population size were the most important correlates of deforestation. Main conclusins These trends suggest that deforestation in the Brazilian Amazon is being largely determined by three proximate factors: human population density, highways and dry-season severity, all of which increase deforestation. At least at the spatial scale of this analysis, soil fertility and waterlogging had little influence on deforestation activity, and soil depth was only marginally significant. Our findings suggest that current policy initiatives designed to increase immigration and dramatically expand highway and infrastructure networks in the Brazilian Amazon are likely to have important impacts on deforestation activity. Deforestation will be greatest in relatively seasonal, south-easterly areas of the basin, which are most accessible to major population centres and where large-scale cattle ranching and slash-and-burn farming are most easily implemented. C1 Smithsonian Trop Res Inst, Balboa, Panama. Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. Natl Inst Amazonian Res INPA, Dept Ecol, Manaus, Amazonas, Brazil. Mt Holyoke Coll, Ctr Environm Literacy, S Hadley, MA 01075 USA. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011; Albernaz, Ana Luisa/K-5226-2012; Venticinque, Eduardo/G-8961-2015 OI Fearnside, Philip/0000-0003-3672-9082; NR 68 TC 154 Z9 164 U1 19 U2 158 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD MAY-JUN PY 2002 VL 29 IS 5-6 BP 737 EP 748 DI 10.1046/j.1365-2699.2002.00721.x PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 570HF UT WOS:000176652300016 ER PT J AU Kornicker, LS AF Kornicker, LS TI Orientation of the maxilla of the Sarsiellinae (Ostracoda) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB The maxillae (fourth limbs) of myodocopine Ostracoda are difficult to interpret correctly because of their complexity, which has led to inaccurate descriptions of the limb in the literature. Maxillae of species of the Sarsiellinae are described and illustrated herein in their natural orientation on the body of the animal, and clues are presented to assist in more accurate descriptions of the limb when compressed under a cover slip. It is shown that the anterior-to-posterior sequence of the three endites of the protopod in the Sarsiellinae is the reverse of that in the Cypridinidae, Philomedidae, and Rutidermatidae. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Systemet Biol, Invertebrate Zool Sect, Washington, DC 20560 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Systemet Biol, Invertebrate Zool Sect, Washington, DC 20560 USA. NR 20 TC 3 Z9 3 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 MAY PY 2002 VL 22 IS 2 BP 268 EP 278 DI 10.1651/0278-0372(2002)022[0268:OOTMOT]2.0.CO;2 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 556TY UT WOS:000175866100005 ER PT J AU Stafford, BJ Thorington, RW Kawamichi, T AF Stafford, BJ Thorington, RW Kawamichi, T TI Gliding behavior of Japanese giant flying squirrels (Petaurista leucogenys) SO JOURNAL OF MAMMALOGY LA English DT Article DE aerodynamics; flying squirrels; gliding; locomotion; musasabi; Petaurista; Pteromyinae ID GLAUCOMYS; ANATOMY AB Gliding behavior of Japanese giant flying squirrels, Petaurista leucogenys, was studied at Nara Park, Japan. We observed 150 glides. We were able to calculate glide ratios on 57 glides and airspeeds on 29 glides. Glide ratios (distance/[altitude lost]) averaged 1.87, and a glide ratio of 3-3.5 seems to represent an upper performance limit for P. leucogenys. Airspeeds (4.39-9.47 m/s) were substantially lower than reported in other studies, and glide angles were higher (17.74-34.99). Aspect ratios of the animals in mid-glide averaged 1.42. C1 Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA. Natl Museum Nat Hist, Dept Vertebrate Zool, Div Mammals, Smithsonian Inst, Washington, DC 20560 USA. Osaka City Univ, Dept Biol, Sumiyoshi Ku, Osaka 5588585, Japan. RP Stafford, BJ (reprint author), Howard Univ, Coll Med, Dept Anat, 520 W St NW, Washington, DC 20059 USA. NR 28 TC 31 Z9 32 U1 0 U2 14 PU AMER SOC MAMMALOGISTS PI PROVO PA BRIGHAM YOUNG UNIV, DEPT OF ZOOLOGY, PROVO, UT 84602 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD MAY PY 2002 VL 83 IS 2 BP 553 EP 562 DI 10.1644/1545-1542(2002)083<0553:GBOJGF>2.0.CO;2 PG 10 WC Zoology SC Zoology GA 556UC UT WOS:000175866500023 ER PT J AU Hotton, N Feldmann, RM Hook, RW Dimichele, WA AF Hotton, N Feldmann, RM Hook, RW Dimichele, WA TI Crustacean-bearing continental deposits in the Petrolia formation (Leonardian Series, Lower Permian) of North-Central Texas SO JOURNAL OF PALEONTOLOGY LA English DT Article AB Numerous pygocephalomorph crustaceans Occur with conchostracans. plants. fishes. amphibians, and amniotes in the Petrolia Formation (Leonardian Series. Lower Permian) of Baylor and Archer counties. Texas. Two pygocephalomorph species are represented Mamayocaris serendipitous. new species, by hundreds of specimens that appear to be molted exoskeletons. and Paulocaris schrami, new species. by only a few specimens. Mamayocaris has been reported previously from the Lower Permian of Texas and South Dakota and the Upper Carboniferous Of Illinois; Paulocaris was previously known only from South America. Associated plant assemblages are dominated by conifers accompanied by other Early Permian and some Late Carboniferous elements. Accompanying vertebrate remains include aquatic to fully terrestrial forms with close taxonomic ties to genera or families recorded in Upper Carboniferous deposits. The fossils are preserved in local deposits of thin (<2 cm). lenticular to nodular beds of limestone and thin (< 15 cm) intervals of dark-gray claystone. These deposits accumulated in abandoned, standing-water segments of suspended-load fluvial channels. The archaic nature of these plant and animal assemblages supports previous interpretations that the Permian Petrolia Formation contains paleoenvironmentally isolated biotic elements characteristic of the Carboniferous and underscore,; prior depictions of the assemblages as relictual. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Kent State Univ, Dept Geol, Kent, OH 44242 USA. Univ Texas, Vertebrate Paleontol Lab, Texas Mem Museum, Austin, TX 78758 USA. RP Feldmann, RM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RI DiMichele, William/K-4301-2012 NR 34 TC 10 Z9 11 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 MAY PY 2002 VL 76 IS 3 BP 486 EP 494 DI 10.1666/0022-3360(2002)076<0486:CBCDIT>2.0.CO;2 PG 9 WC Paleontology SC Paleontology GA 548PV UT WOS:000175398500007 ER PT J AU Daniel, P AF Daniel, P TI Race, rock, and Elvis SO JOURNAL OF SOUTHERN HISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Daniel, P (reprint author), Smithsonian Inst, Natl Museum Amer Hist, 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 MAY PY 2002 VL 68 IS 2 BP 501 EP 503 DI 10.2307/3069999 PG 3 WC History SC History GA 549FD UT WOS:000175433100067 ER PT J AU Cochrane, MA Laurance, WF AF Cochrane, MA Laurance, WF TI Fire as a large-scale edge effect in Amazonian forests SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Amazon; Brazil; conservation; carbon emissions; deforestation; drought; fire; habitat fragmentation; logging; rain forest; remote sensing; tropical forest ID RAIN-FOREST; BRAZILIAN AMAZON; EASTERN AMAZON; TROPICAL FORESTS; CLIMATE-CHANGE; EL-NINO; FRAGMENTATION; DEFORESTATION; COMMUNITIES; BIOMASS AB Amazonian forests are being rapidly cleared, and the remaining forest fragments appear unusually vulnerable to fire. This occurs because forest remnants have dry, Ere-prone edges, are juxtaposed with frequently burned pastures, and are often degraded by selective logging, which increases forest desiccation and fuel loading. Here we demonstrate that in eastern Amazonia, fires are operating as a large-scale edge effect in the sense that most fires originate outside fragments and penetrate considerable distances into forest interiors. Multi-temporal analyses of satellite imagery from two frontier areas reveal that fire frequency over 12-14-y periods was substantially elevated within at least 2400 m of forest margins. Application of these data with a mathematical core-area model suggests that even large forest remnants (up to several hundred thousand ha in area) could be vulnerable to edge-related fires. The synergistic interactions of forest fragmentation, logging and human-ignited fires pose critical threats to Amazonian forests, particularly in more seasonal areas of the basin. C1 Smithsonian Trop Res Inst, Balboa, Panama. Michigan State Univ, Basic Sci & Remote Sensing Initiat, E Lansing, MI 48823 USA. Natl Inst Amazonian Res, INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012 NR 51 TC 190 Z9 202 U1 11 U2 71 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAY PY 2002 VL 18 BP 311 EP 325 DI 10.1017/S0266467402002237 PN 3 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 540AZ UT WOS:000174907100001 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Christo and Jeanne-Claude: A biography. 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 MAY 1 PY 2002 VL 127 IS 8 BP 96 EP 97 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 547NJ UT WOS:000175338400042 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Christo and Jeanne-Claude in the vogel collection. 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 MAY 1 PY 2002 VL 127 IS 8 BP 96 EP 97 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 547NJ UT WOS:000175338400043 ER PT J AU Yuri, T Mindell, DP AF Yuri, T Mindell, DP TI Molecular phylogenetic analysis of Fringillidae, "New World nine-primaried oscines" (Aves : Passeriformes) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID INFERRING COMPLEX PHYLOGENIES; SEQUENCE DATA; MITOCHONDRIAL GENOME; AMERICAN SPARROWS; MTDNA SEQUENCES; EVOLUTION; CHARACTER; FINCHES; BIRDS; PARSIMONY AB Systematic studies of Fringillidae have long been problematic due to their apparent recent and explosive diversification. We present phylogenetic hypotheses of 44 fringillids that represent the overall diversity of the family, based on 3.2 kb of mitochondrial DNA sequences, and phylogenetic analyses for a subset of fringillids based on new and published mitochondrial cytochrome b sequences. Monophyly of Fringillidae and its two constituent subfamilies, Fringillinae and Emberizinae, was consistently supported with the exceptions of Peucedramus being placed outside of Fringillinae and Euphonia being placed within Fringillinae instead of within Emberizinae. Within Emberizinae, Thraupini (tanagers), Cardinalini (cardinals and grosbeaks), and Emberizini (New World sparrows) did not form separate monophyletic groups. Our results indicate that Emberizinae consists of three clades, each with a different overall geographical distribution. Several taxa traditionally considered members of Thraupini fall outside of the thraupine clade, including the only North American genus, Piranga. Consequently, the thraupine clade includes only Neotropical species. Increasing evidence suggests that Fringillidae, often called "New World nine-primaried oscines," does not in fact have a New World origin. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. Univ Michigan, Dept Ecol & Evolut Biol, Ann Arbor, MI 48109 USA. RP Yuri, T (reprint author), Smithsonian Inst, Labs Analyt Biol, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM tyuri@lab.si.edu NR 88 TC 95 Z9 103 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAY PY 2002 VL 23 IS 2 BP 229 EP 243 AR PII S1055-7903(02)00012-X DI 10.1016/S1055-7903(02)00012-X PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 569AA UT WOS:000176576100011 PM 12069553 ER PT J AU Churazov, E Sunyaev, R Forman, W Bohringer, H AF Churazov, E Sunyaev, R Forman, W Bohringer, H TI Cooling flows as a calorimeter of active galactic nucleus mechanical power SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; cooling flows; galaxies : jets; galaxies : nuclei ID INTERNAL GRAVITY-WAVES; RAY LUMINOUS CLUSTERS; HYDRA-A CLUSTER; X-RAY; BLACK-HOLE; DOMINATED ACCRETION; INTRACLUSTER MEDIUM; ELLIPTIC GALAXIES; M87; CHANDRA AB The assumption that radiative cooling of gas in the centres of galaxy clusters is approximately balanced by energy input from a central supermassive black hole implies that the observed X-ray luminosity of the cooling flow region sets a lower limit on active galactic nucleus (AGN) mechanical power. The conversion efficiency of the mechanical power of the AGN into gas heating is uncertain, but we argue that it can be high even in the absence of strong shocks. These arguments inevitably lead to the conclusion that the time-averaged mechanical power of AGNs in cooling flows is much higher than the bolometric luminosity of these objects observed currently. The energy balance between cooling losses and AGN mechanical power requires some feedback mechanism. We consider a toy model in which the accretion rate on to a black hole is set by the classic Bondi formula. Application of this model to the best studied case of M87 suggests that accretion proceeds at approximately the Bondi rate down to a few gravitational radii with most of the power (at the level of a few per cent of the rest mass) being carried away by an outflow. C1 Max Planck Inst Astrophys, D-85741 Garching, Germany. Moscow Space Res Inst, Moscow 117810, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Churazov, E (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. RI Churazov, Eugene/A-7783-2013 NR 55 TC 239 Z9 241 U1 0 U2 2 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2002 VL 332 IS 3 BP 729 EP 734 DI 10.1046/j.1365-8711.2002.05332.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 553FD UT WOS:000175664400020 ER PT J AU Bate, MR Bonnell, IA Bromm, V AF Bate, MR Bonnell, IA Bromm, V TI The formation mechanism of brown dwarfs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; hydrodynamics; binaries : general; circumstellar matter; stars : formation; stars : low-mass, brown dwarfs ID SMOOTHED PARTICLE HYDRODYNAMICS; ROTATING INTERSTELLAR CLOUDS; DISC-DISC ENCOUNTERS; PROTOSTELLAR ENCOUNTERS; NUMERICAL SIMULATIONS; MOLECULAR CLOUD; STAR-FORMATION; MULTIPLE SYSTEMS; BINARY-SYSTEMS; MASS FUNCTION AB We present results from the first hydrodynamical star formation calculation to demonstrate that brown dwarfs are a natural and frequent product of the collapse and fragmentation of a turbulent molecular cloud. The brown dwarfs form via the fragmentation of dense molecular gas in unstable multiple systems and are ejected from the dense gas before they have been able to accrete to stellar masses. Thus, they can be viewed as 'failed stars'. Approximately three-quarters of the brown dwarfs form in gravitationally unstable circumstellar discs while the remainder form in collapsing filaments of molecular gas. These formation mechanisms are very efficient, producing roughly the same number of brown dwarfs as stars, in agreement with recent observations. However, because close dynamical interactions are involved in their formation, we find a very low frequency of binary brown dwarf systems (less than or similar to5 per cent) and that those binary brown dwarf systems that do exist must be close, less than or similar to10 au. Similarly, we find that young brown dwarfs with large circumstellar discs (radii greater than or similar to10 au) are rare (approximate to5 per cent). C1 Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ St Andrews, Dept Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bate, MR (reprint author), Univ Exeter, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England. EM mbate@astro.ex.ac.uk NR 39 TC 162 Z9 162 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2002 VL 332 IS 3 BP L65 EP U1 DI 10.1046/j.1365-8711.2002.05539.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 553FD UT WOS:000175664400005 ER PT J AU Worrall, DM AF Worrall, DM TI The gaseous environments of radio galaxies SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Workshop on Life Cycles of Radio Galaxies CY JUL 15-17, 1999 CL SPACE TELESCOPE SCI INST, BALTIMORE, MARYLAND HO SPACE TELESCOPE SCI INST DE radio continuum : galaxies; X-rays : galaxies : clusters ID X-RAY OBSERVATIONS; CYGNUS-A; ROSAT OBSERVATIONS; COMPLETE SAMPLE; EMISSION; LOBES; CLUSTERS; ASCA; GAS; NGC-6251 AB X-ray emission traces the gaseous environments of radio sources. The medium must be present for jet confinement, but what are its influence on jet fueling, dynamics, propagation, and disruption? The observational situation is both complicated and enriched by radio sources being multi-component X-ray emitters, with several possible regions of non-thermal emission. Recent work, primarily based on sensitive ROSAT pointings, is used to contrast the X-ray emission and environments of radio sources with: (a) low power, (b) high power at high redshift, (c) high power at lower redshift, and (d) GHz peaked spectrum emission. The trends in external gas density and pressure near extended radio structures are reviewed. Imminently-avail able X-ray measurements with vastly improved resolution and sensitivity have great potential for resolving many open issues. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. RP Worrall, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 59 TC 4 Z9 4 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 MAY PY 2002 VL 46 IS 2-7 BP 121 EP 134 AR PII S1387-6473(01)00167-1 DI 10.1016/S1387-6473(01)00167-1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554CX UT WOS:000175717000013 ER PT J AU McNamara, BR AF McNamara, BR TI Radio triggered star formation in cooling flows SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Workshop on Life Cycles of Radio Galaxies CY JUL 15-17, 1999 CL SPACE TELESCOPE SCI INST, BALTIMORE, MD HO SPACE TELESCOPE SCI INST DE radio continuum : galaxies; stars : formation; X-rays : galaxies : clusters ID CENTRAL CLUSTER GALAXIES; U-BAND POLARIMETRY; ABELL 2597; LINE EMISSION; LIGHT; CONTINUUM AB The giant galaxies located at the centers of cluster cooling flows are frequently sites of vigorous star formation. In some instances, star formation appears to have been triggered by the galaxy's radio source. The colors and spectral indices of the young populations are generally consistent with short duration bursts or continuous star formation for durations much less than 1 Gyr, which is less than the presumed ages of cooling flows. The star formation properties are inconsistent with fueling by a continuously accreting cooling flow, although the prevalence of star formation is consistent with repeated bursts and periodic refueling. Star formation may be fueled, in some cases, by cold material stripped from neighboring cluster galaxies. (C) 2002 Published by Elsevier Science B.V. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McNamara, BR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM brm@cfa.harvard.edu NR 34 TC 7 Z9 7 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 MAY PY 2002 VL 46 IS 2-7 BP 141 EP 148 AR PII S1387-6473(01)00169-5 DI 10.1016/S1387-6473(01)00169-5 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554CX UT WOS:000175717000015 ER PT J AU Koekemoer, AM O'Dea, CP Sarazin, CL McNamara, BR Donahue, M Voit, M Baum, SA Gallimore, JF AF Koekemoer, AM O'Dea, CP Sarazin, CL McNamara, BR Donahue, M Voit, M Baum, SA Gallimore, JF TI Interactions between the Abell 2597 central radio source and dense gas in its host galaxy SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Workshop on Life Cycles of Radio Galaxies CY JUL 15-17, 1999 CL SPACE TELESCOPE SCI INST, BALTIMORE, MARYLAND HO SPACE TELESCOPE SCI INST DE cooling flows; galaxies : active; galaxies : clusters; individual (Abell 2597); radio continuum : galaxies ID COOLING FLOWS; CLUSTERS; EMISSION AB We present a detailed HST/WFPC2 study of the complex network of emission-line filaments and blue continuum emission associated with the lobes of the radio source at the center of the nearby strong cooling-flow cluster Abell 2597. This object is a prototypical "blue-lobed" cluster radio galaxy. We discuss ways in which the radio source is interacting with the cool dense gas around it, and derive detailed constraints on the physical properties of the gas. We also resolve the blue continuum emission, which is most likely due to young stars, and discuss possible relationships between the radio source, the supply of gas and the triggering mechanisms for the active nucleus and the star formation. (C) 2002 Elsevier Science B.V. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Space Telecope Sci Inst, Baltimore, MD 21218 USA. Univ Virginia, Astron Dept, Charlottesville, VA 22903 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NRAO, Charlottesville, VA 22903 USA. RP Koekemoer, AM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Donahue, Megan/B-5361-2012; OI Koekemoer, Anton/0000-0002-6610-2048 NR 15 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 MAY PY 2002 VL 46 IS 2-7 BP 149 EP 153 AR PII S1387-6473(01)00170-1 DI 10.1016/S1387-6473(01)00170-1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554CX UT WOS:000175717000016 ER PT J AU Birkinshaw, M AF Birkinshaw, M TI Radio source stability SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT International Workshop on Life Cycles of Radio Galaxies CY JUL 15-17, 1999 CL SPACE TELESCOPE SCI INST, BALTIMORE, MARYLAND HO SPACE TELESCOPE SCI INST DE galaxies : jets, hydrodynamics ID JETS AB This paper describes several modifications to the simplest model of a beam that might have the effect of suppressing the short-wavelength Kelvin-Helmholtz instabilities that can cause jet disruption while maintaining the long-wavelength modes that are popular as causes of distorted jet structure. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Birkinshaw, M (reprint author), Univ Bristol, Dept Phys, Tyndall Ave, Bristol BS8 1TL, Avon, England. NR 8 TC 1 Z9 1 U1 1 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 MAY PY 2002 VL 46 IS 2-7 BP 417 EP 420 AR PII S1387-6473(01)00153-7 DI 10.1016/S1387-6473(02)00153-7 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554CX UT WOS:000175717000063 ER PT J AU Newell, EA Mulkey, SS Wright, SJ AF Newell, EA Mulkey, SS Wright, SJ TI Seasonal patterns of carbohydrate storage in four tropical tree species SO OECOLOGIA LA English DT Article DE total non-structural carbohydrates; Anacardium excelsum; Cecropia longipes; Luehea seemannii; Urera caracasana ID FOREST; PLANTS; CANOPY; GROWTH; PHENOLOGY; NITROGEN; RESERVES; ECOLOGY; WATER AB We examined the seasonal variation in total non-structural carbohydrate (TNC) concentrations in branch, trunk, and root tissues of Anacardium excelsum, Luehea seemannii, Cecropia longipes, and Urera caracasana growing in a seasonally dry forest in Panama. Our main goals were: (1) to determine the main sites of carbohydrate storage, and (2) to determine if seasonal patterns of carbohydrate storage are related to seasonal asynchronies in carbon supply and demand. We expected asynchronies to be related to seasonal variation in water and light availability and to foliar and reproductive phenology. Cecropia and Urera are fully drought-deciduous and so we expected them to exhibit the most dramatic seasonal variation in TNC concentrations. We predicted that maximum carbon supply would occur when canopies were at their fullest and that maximum carbon demand would occur when leaves, flowers, and fruits were produced. The concentration of total non-structural carbohydrates was assessed monthly in wood tissue of roots and in wood and bark tissue of terminal branches. Trunk tissue was sampled bimonthly. All tissues sampled served as storage sites for carbohydrates. As predicted, TNC concentrations varied most dramatically in branches of Cecropia and Urera: a 4-fold difference was observed between dry season maxima and wet season minima in branch wood tissue. Peak concentrations exceeded 25% in Urera and 30% in Cecropia. Less dramatic but significant seasonal variation was observed in Anacardium and Luehea. In all species, minimum branch TNC concentrations were measured during canopy rebuilding. In Anacardium. maximum branch TNC concentrations occurred when canopies were at their fullest. In Cecropia, Urera, and Luehea, TNC concentrations continued to increase even as canopies thinned in the early dry season. The greater photosynthetic capacity of leaves produced at the beginning of the dry season and the potential for the export of carbohydrates from senescing leaves may explain this pattern. In all species, the phenology of carbon gain was more important than the phenology of reproduction in influencing seasonal carbohydrate patterns. The combination of high TNC concentrations and the large biomass of branches, trunks, and roots indicates these species are storing and moving large quantities of carbohydrates. C1 Hobart & William Smith Coll, Dept Biol, Geneva, NY 14456 USA. Univ Florida, Dept Bot, Gainesville, FL 32611 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Newell, EA (reprint author), Hobart & William Smith Coll, Dept Biol, Geneva, NY 14456 USA. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 29 TC 61 Z9 70 U1 5 U2 42 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAY PY 2002 VL 131 IS 3 BP 333 EP 342 DI 10.1007/s00442-002-0888-6 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 557YH UT WOS:000175936300002 ER PT J AU Bergenius, MAJ Meekan, MG Robertson, DR McCormick, MI AF Bergenius, MAJ Meekan, MG Robertson, DR McCormick, MI TI Larval growth predicts the recruitment success of a coral reef fish SO OECOLOGIA LA English DT Article DE critical period; growth; otolith; plankton; settlement ID ICHTHYOPLANKTON MORTALITY-RATES; LIFE-HISTORY TRAITS; PHYSICAL PROCESSES; MARINE FISHES; GADUS-MORHUA; SETTLEMENT; SIZE; PREDATION; OTOLITH; PANAMA AB While growth rates of pelagic larvae have been argued to be one of the principal determinants of the recruitment success of temperate marine fishes, it is not known if this is the case in the tropics. Here, we use larval growth histories derived from otoliths of a Caribbean reef fish to show that monthly variation in the intensity of settlement and recruitment of pelagic juveniles onto reefs is positively correlated with variation in growth rates 1-2 weeks after larvae begin feeding. Our results suggest that the processes thought to underlie recruitment of marine fishes in temperate regions may also operate in the tropics and contrasts with current research on the causes of recruitment variability in coral reef fishes, which emphasises the role of larval transport. C1 James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. No Terr Univ, Australian Inst Marine Sci Trop Fisheries, Darwin, NT 0909, Australia. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. EM mikaela.bergenius@jcu.edu.au RI McCormick, Mark/J-8301-2014 OI McCormick, Mark/0000-0001-9289-1645 NR 44 TC 112 Z9 114 U1 5 U2 28 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 MAY PY 2002 VL 131 IS 4 BP 521 EP 525 DI 10.1007/s00442-002-0918-4 PG 5 WC Ecology SC Environmental Sciences & Ecology GA 562UU UT WOS:000176218000006 ER PT J AU Langley, JA Drake, BG Hungate, BA AF Langley, JA Drake, BG Hungate, BA TI Extensive belowground carbon storage supports roots and mycorrhizae in regenerating scrub oaks SO OECOLOGIA LA English DT Article DE carbon remobilization; ectomycorrhizae; rhizomes; scrub oak; storage ID ELEVATED CO2; RESERVES; GROWTH; FUNGI; PLANTS; SHOOTS; PARTS; C-13 AB Portions of a regenerating scrub oak ecosystem were enclosed in open-top chambers and exposed to elevated CO, The distinct C-13 signal of the supplemental CO2 was used to trace the rate of C integration into various ecosystem components. Oak foliage, stems, roots and ectomycorrhizae were sampled over 3 years and were analyzed for C-13 composition. The aboveground tissue C-13 equilibrated to the novel C-13 signal in the first season, while the belowground components displayed extremely slow integration of the new C. Roots taken from ingrowth cores showed that 33% of the C in newly formed roots originated from a source other than recent photosynthesis inside the chamber. In this highly fire-prone system, the oaks re-establish primarily by resprouting from large rhizomes. Remobilization from belowground C stores may support fine roots and mycorrhizae for several years into stand re-establishment and, therefore, may explain why below-round tissues contain less of the new photosynthate than expected. Though it has been shown that long-term cycles of C storage are theoretically advantageous for plants in systems with frequent and severe disturbances, such patterns have not been previously examined in wild systems. C1 No Arizona Univ, Dept Sci Biol, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Langley, JA (reprint author), No Arizona Univ, Dept Sci Biol, Merriam Powell Ctr Environm Res, Box 5640, Flagstaff, AZ 86011 USA. RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 33 TC 50 Z9 56 U1 4 U2 18 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAY PY 2002 VL 131 IS 4 BP 542 EP 548 DI 10.1007/s00442-002-0932-6 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 562UU UT WOS:000176218000009 ER PT J AU Crooks, JA AF Crooks, JA TI Characterizing ecosystem-level consequences of biological invasions: the role of ecosystem engineers SO OIKOS LA English DT Review ID CARP CYPRINUS-CARPIO; BIVALVE MUSCULISTA-SENHOUSIA; GYPSY-MOTH DEFOLIATION; NEST-SITE SELECTION; NATIVE MUD SNAILS; SAN-FRANCISCO BAY; DUTCH ELM DISEASE; HABITAT COMPLEXITY; PLANT-COMMUNITIES; MACROINVERTEBRATE COMMUNITIES AB Invasions by exotic species represent both threats to ecosystems as well as opportunities to learn more about them. Among the invaders that will have the largest impacts are those that directly modify ecosystems and thus have cascading effects for resident biota. Exotics can affect ecosystems by altering system-level flows, availability, or quality of nutrients, food, and physical resources (e.g. living space, water, heat or light). The invader-mediated control of physical resources, typically achieved through the modification of habitats, has received limited attention in invasion biology. This reflects a general trend in ecology, and only recently has the concept of ecosystem engineering been developed to account for the role of species that shape habitats. Plants and animals in terrestrial and aquatic systems can both create and destroy structure. When introduced into ecosystems, these exotic engineers cause physical state changes with effects that ramify throughout the system. Although the consequences of these modifications are varied and complex, insight gained from general ecological principles offers an opportunity to predict what invaders will do upon their integration into systems. Examples from the literature suggest that introduced ecosystem engineers that increase habitat complexity or heterogeneity tend to cause abundances and/or species richness to rise, while those that decrease complexity tend to have the reverse effect. In assessing such patterns, however, it is critical to also consider spatial scales and the life habits of resident organisms. In addition to providing predictive power, recognition of engineering as a major means by which invasive species affect ecosystems provides a unifying theme for invasion biology and offers a chance to consider more fully the general role of species in ecosystems. C1 San Francisco State Univ, Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. RP Crooks, JA (reprint author), San Francisco State Univ, Smithsonian Environm Res Ctr, 3152 Paradise Dr, Tiburon, CA 94920 USA. RI Ross, Donald/F-7607-2012 OI Ross, Donald/0000-0002-8659-3833 NR 180 TC 584 Z9 610 U1 56 U2 415 PU BLACKWELL MUNKSGAARD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0030-1299 J9 OIKOS JI Oikos PD MAY PY 2002 VL 97 IS 2 BP 153 EP 166 DI 10.1034/j.1600-0706.2002.970201.x PG 14 WC Ecology SC Environmental Sciences & Ecology GA 570VF UT WOS:000176678800001 ER PT J AU Feller, IC AF Feller, IC TI The role of herbivory by wood-boring insects in mangrove ecosystems in Belize SO OIKOS LA English DT Article ID HYPSIPYLA-GRANDELLA ZELLER; MAHOGANY SHOOT BORER; FOREST DISTURBANCES; NUTRIENT ENRICHMENT; RHIZOPHORA MANGLE; AVICENNIA-MARINA; HONG-KONG; GROWTH; PLANT; PINE AB The roles wood-boring insects play in modifying mangrove ecosystems were examined on small, offshore mangrove islands in Belize. Several species of xylem- and phloem-feeding woodborers consume the wood of living mangrove trees. By girdling, pruning, and hollowing, woodborers killed over 50% of the Rhizophora mangle canopy in experimental plots arrayed across a tidal-elevation gradient. In contrast, leaf-feeding herbivores removed less than 6%,, of the canopy. In the plots, stem girdlers killed over three branches per tree. The patterns of herbivory by three functional feeding groups were heterogeneous and did not vary consistently with tidal elevation. Because R. mangle lacks viable axillary buds or the ability to produce epicormic shoots to replace pruned branches, the canopy architecture was significantly modified by this damage. The branches that were pruned by stem girdlers created numerous small holes or gaps in the mangrove canopy. Shoot growth and flowering increased in R. mangle trees with 50% of their branches experimentally girdled. Because branches and twigs attacked by woodborers lost their leaves prematurely as greenfall, the quantity and quality of leaf litter were altered when a leaf-bearing branch was girdled or hollowed. These changes suggest that wood-boring insects also significantly affect internal and external nutrient cycling processes in mangrove ecosystems. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Feller, IC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM feller@serc.si.edu OI Feller, Ilka/0000-0002-6391-1608 NR 72 TC 37 Z9 41 U1 4 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0030-1299 EI 1600-0706 J9 OIKOS JI Oikos PD MAY PY 2002 VL 97 IS 2 BP 167 EP 176 DI 10.1034/j.1600-0706.2002.970202.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 570VF UT WOS:000176678800002 ER PT J AU Andre, A Lukin, MD AF Andre, A Lukin, MD TI Atom correlations and spin squeezing near the Heisenberg limit: Finite-size effect and decoherence SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATE; SINGLE PHOTONS; GROUP-VELOCITY; ENTANGLEMENT; LIGHT; STATES; DYNAMICS; ENSEMBLE; STORAGE; CAVITY AB We analyze a model for spin squeezing based on the so-called countertwisting Hamiltonian, including the effects of dissipation and finite system size. We discuss the conditions under which the Heisenberg limit, i.e., phase sensitivity proportional to1/N, can be achieved. A specific implementation of this model based on atom-atom interactions via quantized photon exchange is presented in detail. The resulting excitation corresponds to the creation of spin-flipped atomic pairs and can be used for fast generation of entangled atomic ensembles, spin squeezing, and applications in quantum information processing. The conditions for achieving strong spin squeezing with this mechanism are also analyzed. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Andre, A (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. NR 51 TC 53 Z9 54 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAY PY 2002 VL 65 IS 5 AR 053819 DI 10.1103/PhysRevA.65.053819 PN B PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 554PH UT WOS:000175744300062 ER PT J AU Kannappan, SJ Fabricant, DG Hughes, CB AF Kannappan, SJ Fabricant, DG Hughes, CB TI Building a CCD spectrograph for educational or amateur astronomy SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB We discuss the design of an inexpensive, high-throughput CCD spectrograph for a small telescope. By using optical fibers to carry the light from the telescope focus to a tabletop spectrograph, one can minimize the weight carried by the telescope and simplify the spectrograph design. We recently employed this approach in the construction of IntroSpec, an instrument built for the 16 inch Knowles Telescope on the Harvard College campus. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kannappan, SJ (reprint author), Univ Texas, McDonald Observ, 2511 Speedway,RLM 15-308 C1400, Austin, TX 78712 USA. NR 5 TC 3 Z9 3 U1 1 U2 1 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 MAY PY 2002 VL 114 IS 795 BP 577 EP 585 DI 10.1086/341678 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546XB UT WOS:000175300700008 ER PT J AU DiMichele, WA Phillips, TL AF DiMichele, WA Phillips, TL TI The ecology of Paleozoic ferns SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY LA English DT Article; Proceedings Paper CT 6th International Organization of Palaeobotany Conference (IOPCVI) CY JUL 31-AUG 03, 2000 CL QINHUANGDAO, PEOPLES R CHINA DE ferns; Paleozoic; ecology; paleoecology; evolution ID COAL-SWAMP VEGETATION; SP-NOV; ILLINOIS BASIN; PALEOECOLOGY; PATTERNS; FLORAS; USA; GEN; PALEOBOTANY; TRANSITION AB Ferns or fern-like plants have been important elements of terrestrial vegetation since the Late Devonian. Rhacophyton, a fern-like plant of the Late Devonian, appears to have been a colonizer of wet substrates, often forming large, nearly monotypic stands in peat-accumulating swamps. The earliest true ferns have been found in environments with high levels of disturbance, often tire, which suggest opportunistic, colonizing life histories, consistent with small, scrambling body plans. During the Early Carboniferous all major body plans and life histories of ferns appear, including scrambling ground cover, tree habit, and lianas. These ecological roles are distributed across several major lineages, including the Zygopteridales, Filicales, and Marattiales, plus some fern-like groups of uncertain affinity, and disappear and reappear independently within these groups. Until the Stephanian, the later part of the Late Carboniferous, ferns largely were confined to secondary ecological roles: colonists, understory vegetation, small vines. Beginning in the latter part of the Westphalian and expanding dramatically in the Stephanian, marattialean tree ferns became the dominant trees of tropical lowland, wetland forests. This dominance continued locally into the Permian in wetter parts of the landscape. The Paleozoic ferns suffered major extinctions at several times, beginning in the Late Carboniferous. By the Permian, new lineages were appearing, some of which would persist into and become dominant vegetational components during the Mesozoic. Among these lineages virtually all of the life histories and body plans that characterized Paleozoic ferns would reappear independently, plus some new kinds of organization and ecology, emphasizing the great evolutionary flexibility and responsiveness of fern-like construction and reproductive biology. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP DiMichele, WA (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RI DiMichele, William/K-4301-2012 NR 102 TC 47 Z9 52 U1 2 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0034-6667 J9 REV PALAEOBOT PALYNO JI Rev. Palaeobot. Palynology PD MAY PY 2002 VL 119 IS 1-2 BP 143 EP 159 AR PII S0034-6667(01)00134-8 DI 10.1016/S0034-6667(01)00134-8 PG 17 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA 577KH UT WOS:000177059700009 ER PT J AU Lundrigan, BL Jansa, SA Tucker, PK AF Lundrigan, BL Jansa, SA Tucker, PK TI Phylogenetic relationships in the genus Mus, based on paternally, maternally, and biparentally inherited characters SO SYSTEMATIC BIOLOGY LA English DT Review DE Coelomys; molecular phylogeny; Muridae; Mus; Nannomys; Pyromys ID MITOCHONDRIAL-DNA EVOLUTION; SEX-DETERMINING REGION; HOUSE MICE; BIOCHEMICAL GENETICS; NUCLEOTIDE-SEQUENCES; MUSCULUS-DOMESTICUS; ZONA PELLUCIDA; COMBINING DATA; Y-CHROMOSOME; HYBRIDIZATION EXPERIMENTS AB Several species in the rodent genus Mus are used as model research organisms, but comparative studies of these mice have been hampered by the lack of a well-supported phylogeny. We used DNA sequences from six genes representing paternally, maternally, and biparentally inherited regions of the genome to infer phylogenetic relationships among 10 species of Mus commonly used in laboratory research. Our sample included seven species from the subgenus Mus; one species each from the subgenera Pyromys, Coelomys, and Nannomys; and representatives from three additional murine genera, which served as outgroups in the phylogenetic analyses. Although each of the six genes yielded a unique phylogeny, several clades were supported by four or more gene trees. Nodes that conflicted between trees were generally characterized by weak support for one or both of the alternative topologies, thus providing no compelling evidence that any individual gene, or part of the genome, was misleading with respect to the evolutionary history of these mice. Analysis of the combined data resulted in a fully resolved tree that strongly supports monophyly of the genus Mus, monophyly of the subgenus Mus, division of the subgenus Mus into Palearctic (M. musculus, M. macedonicus, M. spicilegus, and M. spretus) and Asian (M. cervicolor, M. cookii, and M. caroli) clades, monophyly of the house mice (M. m. musculus, "M. m. molossinus," M. m. castaneus, and M. m. domesticus), and a sister-group relationship between M. macedonicus and M. spicilegus. Other clades that were strongly supported by one or more gene partitions were not strongly supported by the combined data. This appears to reflect a localized homoplasy in one partition obscuring the phylogenetic signal from another, rather than differences in gene or genome histories. C1 Michigan State Univ Museum, E Lansing, MI 48824 USA. Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Div Mammal, Washington, DC 20560 USA. Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Lundrigan, BL (reprint author), Michigan State Univ Museum, E Lansing, MI 48824 USA. FU NCI NIH HHS [N01-CB-71085] NR 132 TC 84 Z9 91 U1 3 U2 13 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 MAY-JUN PY 2002 VL 51 IS 3 BP 410 EP 431 DI 10.1080/10635150290069878 PG 22 WC Evolutionary Biology SC Evolutionary Biology GA 562KY UT WOS:000176197000002 PM 12079642 ER PT J AU Schwartz, GT Samonds, KE Godfrey, LR Jungers, WL Simons, EL AF Schwartz, GT Samonds, KE Godfrey, LR Jungers, WL Simons, EL TI Dental microstructure and life history in subfossil Malagasy lemurs SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE body size; Palaeopropithecus; dental development; incremental markings; gestation length ID SOCIAL-ORGANIZATION; MADAGASCAR; ECOLOGY; PRIMATES; ISLAND; TEETH AB When compared with their recently extinct relatives, living lemurs represent a mere fraction of a broad radiation that occupied unique niches in the recent past. Among living lemurs, indrids exhibit the fastest rates of dental development. This dental precocity is tightly correlated with rapid pace of postnatal dental eruption, early replacement of the deciduous teeth, high dental endowment at weaning, and relatively slow somatic growth. This pattern is in stark contrast to that seen in extant lemurids, where somatic development is highly accelerated and dental development is relatively slow. We report on the pace of dental development in one species of palaeopropithecid, the sister group to extant indrids. Like much smaller modern indrids, the chimpanzee-sized Palaeopropithecus ingens was dentally precocious at birth as evidenced by the advanced state of molar crown formation. This finding implies a pattern characteristic of Propithecus and other indrids-rapid dental development despite relatively prolonged gestation. Gestation length in this one species of subfossil lemur was likely greater than 9 months. Our results demonstrate that large body size in primates does not preclude exceedingly rapid dental development. C1 George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. Duke Univ, Dept Biol Anthropol & Anat, Durham, NC 27705 USA. Duke Univ, Ctr Primate, Durham, NC 27705 USA. Univ Massachusetts, Dept Anthropol, Amherst, MA 01003 USA. SUNY Stony Brook, Dept Anat Sci, Stony Brook, NY 11794 USA. Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC USA. RP Schwartz, GT (reprint author), George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. RI Samonds, Karen/A-1493-2012 NR 33 TC 51 Z9 52 U1 0 U2 4 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 APR 30 PY 2002 VL 99 IS 9 BP 6124 EP 6129 DI 10.1073/pnas.092685099 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 548FK UT WOS:000175377800069 PM 11983905 ER PT J AU Novotny, V Basset, Y Miller, SE Weiblen, GD Bremer, B Cizek, L Drozd, P AF Novotny, V Basset, Y Miller, SE Weiblen, GD Bremer, B Cizek, L Drozd, P TI Low host specificity of herbivorous insects in a tropical forest SO NATURE LA English DT Article ID PHYLOGENETIC-RELATIONSHIPS; SEQUENCES; RBCL AB Two decades of research(1-4) have not established whether tropical insect herbivores are dominated by specialists or generalists. This impedes our understanding of species coexistence in diverse rainforest communities. Host specificity and species richness of tropical insects are also key parameters in mapping global patterns of biodiversity(1,4,5). Here we analyse data for over 900 herbivorous species feeding on 51 plant species in New Guinea and show that most herbivorous species feed on several closely related plant species. Because species-rich genera are dominant in tropical floras, monophagous herbivores are probably rare in tropical forests. Furthermore, even between phylogenetically distant hosts, herbivore communities typically shared a third of their species. These results do not support the classical view that the coexistence of herbivorous species in the tropics is a consequence of finely divided plant resources; non-equilibrium models of tropical diversity(6) should instead be considered. Low host specificity of tropical herbivores reduces global estimates of arthropod diversity from 31 million (ref. 1) to 4-6 million species. This finding agrees with estimates based on taxonomic collections, reconciling an order of magnitude discrepancy between extrapolations of global diversity based on ecological samples of tropical communities with those based on sampling regional faunas (7,8). C1 Acad Sci Czech Republ, 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. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Univ Minnesota, Dept Plant Biol, Ctr Biol Sci 220, St Paul, MN 55108 USA. Royal Swedish Acad Sci, Bergius Fdn, SE-10405 Stockholm, Sweden. Univ Ostrava, Dept Biol, Ostrava, Czech Republic. RP Novotny, V (reprint author), Acad Sci Czech Republ, Inst Entomol, Branisovska 31, CR-37005 Ceske Budejovice, Czech Republic. RI Drozd, Pavel/J-3943-2013; Basset, Yves/B-6642-2014; Cizek, Lukas/G-7905-2014; Novotny, Vojtech/G-9434-2014; Cizek, Lukas/K-7111-2015; OI Drozd, Pavel/0000-0002-4602-8856; Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 30 TC 356 Z9 377 U1 11 U2 162 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 25 PY 2002 VL 416 IS 6883 BP 841 EP 844 DI 10.1038/416841a PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 544MH UT WOS:000175163800049 PM 11976681 ER PT J AU Tosaki, T Hasegawa, T Shioya, Y Kuno, N Matsushita, S AF Tosaki, T Hasegawa, T Shioya, Y Kuno, N Matsushita, S TI Variation of molecular cloud properties across the spiral arm in M 51 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies : individual (M 5 1); galaxies : ISM; galaxies : spiral ID ACTIVE GALACTIC NUCLEUS; STAR-FORMATION; CARBON-MONOXIDE; HIGH-DENSITY; GALAXY M51; GAS; CO; EMISSION; DYNAMICS; ASSOCIATIONS AB We present the results of high-resolution (CO)-C-13 (J = 1-0) mapping observations with the NRO 45 in telescope of the area toward the southern bright arm region of M 51, including the galactic center, in order to study the physical conditions of the molecular clouds in the arm and the interarm. The obtained map shows the central depression of the (CO)-C-13 (J = 1-0) emission, the circumnuclear ring (radius similar to 10"-20"), and the spiral arm structure. The arm-to-interarm ratio of the (CO)-C-13 (J = 1-0) integrated intensity is 2-4. We also have found a feature different from that found in the (CO)-C-12 results. For example, the (CO)-C-13 distribution shows a depression in part of the spiral arm, The (CO)-C-12/(CO)-C-13 ratio spatially varies, and shows high values (similar to 20) for the interarm and the central region, but low values (similar to 10) for the arm. Their values indicate that there is a denser gas in the spiral arm than in the interarm. The distribution of the (CO)-C-13 shows a better correspondence with that of the Halpha emission than with the (CO)-C-12 in the disk region, except for the central region. We found that the (CO)-C-13 emission is located on the downstream side of the (CO)-C-12 arm, namely there is an offset between the (CO)-C-12 and the (CO)-C-13 as well as the Halpha emission. This suggests that there is a time delay between the accumulation of gas caused by the density wave and dense gas formation, accordingly star formation. This time delay is estimated to be similar to 10(7) yr based on the assumption of galactic rotation derived by the rotation curve and the pattern speed of the M 51 spiral pattern. It is similar to the growth timescale of a gravitational instability in the spiral arm of M 51, suggesting that the gravitational instability plays an important role for dense gas formation. C1 Gunma Astron Observ, Gunma 3770702, Japan. Tohoku Univ, Aoba Ku, Sendai, Miyagi 9808578, Japan. Nobeyama Radio Observ, Minamisa Ku, Nagano 3841805, Japan. Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96721 USA. RP Gunma Astron Observ, Gunma 3770702, Japan. EM tomoka@astron.pref.gunma.jp NR 49 TC 23 Z9 23 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD APR 25 PY 2002 VL 54 IS 2 BP 209 EP 221 DI 10.1093/pasj/54.2.209 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547UA UT WOS:000175349400012 ER PT J AU Moore, MG Vardi, A AF Moore, MG Vardi, A TI Bose-enhanced chemistry: Amplification of selectivity in the dissociation of molecular Bose-Einstein condensates SO PHYSICAL REVIEW LETTERS LA English DT Article ID SCATTERING AB We study the photodissociation chemistry of a quantum degenerate gas of bosonic triatomic ABC molecules, assuming two open rearrangement channels (AB + C or A + BC ). The equations of motion are equivalent to those of a parametric multimode laser, resulting in an exponential buildup of macroscopic mode populations. By exponentially amplifying a small differential in the single-particle rate coefficients, Bose stimulation leads to a nearly complete selectivity of the collective N -body process, indicating a novel type of ultraselective quantum degenerate chemistry. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Moore, MG (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Vardi, Amichay/D-8189-2011 OI Vardi, Amichay/0000-0002-8992-2129 NR 21 TC 39 Z9 40 U1 0 U2 2 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD APR 22 PY 2002 VL 88 IS 16 AR 160402 DI 10.1103/PhysRevLett.88.160402 PG 4 WC Physics, Multidisciplinary SC Physics GA 540AH UT WOS:000174905400002 PM 11955220 ER PT J AU Tafalla, M Myers, PC Caselli, P Walmsley, CM Comito, C AF Tafalla, M Myers, PC Caselli, P Walmsley, CM Comito, C TI Systematic molecular differentiation in starless cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : clouds; ISM : molecules; stars : formation ID INTER-STELLAR CLOUDS; DENSE CORES; DARK CLOUDS; ROTATIONAL-EXCITATION; FORMING REGIONS; INTERSTELLAR AMMONIA; PROTOSTELLAR CORES; NH3 OBSERVATIONS; CHEMICAL-MODELS; CS AB We present evidence that low-mass starless cores, the simplest units of star formation, are systematically differentiated in their chemical composition. Some molecules, including CO and CS, almost vanish near the core centers, where the abundance decreases by at least 1 or 2 orders of magnitude with respect to the value in the outer core. At the same time, the N2H+ molecule has a constant abundance, and the fraction of NH3 increases toward the core center. Our conclusions are based on a systematic study of five mostly round starless cores ( L1498, L1495, L1400K, L1517B, and L1544), which we have mapped in (CO)-O-18 (1-0), CS (2-1), N2H+ (1-0), NH3 (1, 1) and (2, 2), and the 1.2 mm continuum [ complemented with (CO)-O-17 (1-0) and (CS)-S-34 (2-1) data for some systems]. For each core we have built a spherically symmetric model in which the density is derived from the 1.2 mm continuum, the kinetic temperature is derived from NH3, and the abundance of each molecule is derived using a Monte Carlo radiative transfer code, which simultaneously fits the shape of the central spectrum and the radial pro le of integrated intensity. Regarding the cores for which we have (CO)-O-17 (1-0) and (CS)-S-34 (2-1) data, the model fits these observations automatically when the standard isotopomer ratio is assumed. As a result of this modeling, we also find that the gas kinetic temperature in each core is constant at approximately 10 K. In agreement with previous work, we find that if the dust temperature is also constant, then the density profiles are centrally flattened, and we can model them with a single analytic expression. We also find that for each core the turbulent line width seems constant in the inner 0.1 pc. The very strong abundance drop of CO and CS toward the center of each core is naturally explained by the depletion of these molecules onto dust grains at densities of (2-6) 10(4) cm(-3). N2H+ seems unaffected by this process up to densities of several times 10(5) cm(-3), or even 10(6) cm(-3), while the NH3 abundance may be enhanced by its lack of depletion and by reactions triggered by the disappearance of CO from the gas phase. With the help of the Monte Carlo modeling, we show that chemical differentiation automatically explains the discrepancy between the sizes of CS and NH3 maps, a problem that has remained unexplained for more than a decade. Our models, in addition, show that a combination of radiative transfer effects can give rise to the previously observed discrepancy in the line width of these two tracers. Although this discrepancy has been traditionally interpreted as resulting from a systematic increase of the turbulent line width with radius, our models show that it can arise in conditions of constant gas turbulence. C1 Observ Astron Nacl, E-28014 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Tafalla, M (reprint author), Observ Astron Nacl, Alfonso XII 3, E-28014 Madrid, Spain. NR 83 TC 338 Z9 338 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2002 VL 569 IS 2 BP 815 EP 835 DI 10.1086/339321 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 541ND UT WOS:000174989900023 ER PT J AU Gaensler, BM Arons, J Kaspi, VM Pivovaroff, MJ Kawai, N Tamura, K AF Gaensler, BM Arons, J Kaspi, VM Pivovaroff, MJ Kawai, N Tamura, K TI Chandra imaging of the X-ray nebula powered by pulsar B1509-58 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G320.4-1.2); ISM : jets and outflows; pulsars : individual (B1509-58); stars : neutron; supernova remnants; X-rays : ISM ID SUPER-NOVA REMNANT; HIGH-ENERGY EMISSION; SOUTHERN MILKY-WAY; CRAB-NEBULA; MSH 15-52; PSR B1509-58; GAMMA-RAY; WIND NEBULA; SYNCHROTRON NEBULA; RADIO OBSERVATIONS AB We present observations with the Chandra X-Ray Observatory of the pulsar wind nebula ( PWN) powered by the energetic young pulsar B1509-58. These data confirm the complicated morphology of the system indicated by previous observations, and in addition reveal several new components to the nebula. The overall PWN shows a clear symmetry axis oriented at a position angle 150degrees +/- 5degrees (north through east), which we argue corresponds to the pulsar spin axis. We show that a previously identified radio feature matches well with the overall extent of the X-ray PWN, and propose the former as the long-sought radio nebula powered by the pulsar. We further identify a bright collimated feature, at least 4' long, lying along the nebulas main symmetry axis; we interpret this feature as a physical outflow from the pulsar, and infer a velocity for this jet of greater than 0.2c. The lack of any observed counterjet implies that the pulsar spin axis is inclined at similar to30degrees to the line of sight, contrary to previous estimates made from lower resolution data. We also identify a variety of compact features close to the pulsar. A pair of semicircular X-ray arcs lie 17" and 30" to the north of the pulsar; the latter arc shows a highly polarized radio counterpart. We show that these features can be interpreted as ion-compression wisps in a particle-dominated equatorial flow, and use their properties to infer a ratio of electromagnetic to particle energy in pairs at the wind shock sigma similar to 005, similar to that seen in the Crab Nebula. We further identify several compact knots seen very close to the pulsar; we use these to infer sigma< 0.003 at a separation from the pulsar of 0.1 pc. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. McGill Univ, Dept Phys, Montreal, PQ, Canada. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. Nagoya Univ, Fac Sci, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. RP MIT, Ctr Space Res, 70 Vassar St, Cambridge, MA 02139 USA. EM bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; Pivovaroff, Michael/M-7998-2014; OI Pivovaroff, Michael/0000-0001-6780-6816; Gaensler, Bryan/0000-0002-3382-9558 NR 93 TC 144 Z9 146 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 APR 20 PY 2002 VL 569 IS 2 BP 878 EP 893 DI 10.1086/339354 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 541ND UT WOS:000174989900029 ER PT J AU Furlanetto, SR Loeb, A AF Furlanetto, SR Loeb, A TI Identifying gamma-ray burst remnants through positron annihilation radiation SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; supernova remnants; X-rays : ISM ID SNR RX J1713.7-3946; SUPERNOVA-REMNANTS; COSMIC FIREBALLS; SHELL; ACCELERATION; DISCOVERY; EMISSION; PLASMAS; SN-1006 AB We model the annihilation of relic positrons produced in a gamma-ray burst (GRB) after its afterglow has faded. We find that the annihilation signal from at least one GRB remnant in the Milky Way should be observable with future space missions such as the International Gamma-Ray Astrophysical Laboratory and the Energetic X-ray Imaging Survey Telescope, provided that the gas surrounding the GRB source has the typical density of the interstellar medium, less than or similar to1 cm(-3). Three fortunate circumstances conspire to make the signal observable. First, unlike positrons in a standard supernova, the GRB positrons initially travel at a relativistic speed and remain ahead of any nonrelativistic ejecta until the ejecta become rarefied and the annihilation time becomes long. Second, the GRB remnant remains sufficiently hot (Tgreater than or similar to5 x 10(5) K) for a strong annihilation line to form without significant smearing by three-photon decay of positronium. Third, the annihilation signal persists over a time longer than the average period between GRB events in the Milky Way. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 51 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 APR 20 PY 2002 VL 569 IS 2 BP L91 EP L94 DI 10.1086/340772 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 541NU UT WOS:000174991300008 ER PT J AU Wilner, DJ Holman, MJ Kuchner, MJ Ho, PTP AF Wilner, DJ Holman, MJ Kuchner, MJ Ho, PTP TI Structure in the dusty debris around Vega SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; circumstellar matter; planetary systems : protoplanetary disks; stars : individual (Lyrae) ID BETA-PICTORIS; SOLAR-SYSTEM; CIRCUMSTELLAR DISK; GIANT PLANETS; SIGNATURES; NEPTUNE; STARS AB We present images of the Vega system obtained with the IRAM Plateau de Bure interferometer at a 1. 3 mm wavelength with submillijansky sensitivity and similar to2."5 resolution (about 20 AU). These observations clearly detect the stellar photosphere and two dust emission peaks offset from the star by 9."5 and 8."0 to the northeast and southwest, respectively. These offset emission peaks are consistent with the barely resolved structure visible in previous submillimeter images, and they account for a large fraction of the dust emission. The presence of two dust concentrations at the observed locations is plausibly explained by the dynamical influence of an unseen planet of a few Jupiter masses in a highly eccentric orbit that traps dust in principal mean motion resonances. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Kuchner, Marc/E-2288-2012 NR 36 TC 131 Z9 132 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2002 VL 569 IS 2 BP L115 EP L119 DI 10.1086/340691 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 541NU UT WOS:000174991300014 ER PT J AU Jackman, TR Irschick, DJ De Queiroz, K Losos, JB Larson, A AF Jackman, TR Irschick, DJ De Queiroz, K Losos, JB Larson, A TI Molecular phylogenetic perspective on evolution of lizards of the Anolis grahami series SO JOURNAL OF EXPERIMENTAL ZOOLOGY LA English DT Article ID TRANSFER-RNA GENES; MITOCHONDRIAL GENOME; MICROGEOGRAPHIC VARIATION; LOCOMOTOR PERFORMANCE; SEQUENCE EVOLUTION; CONFIDENCE-LIMITS; ISLAND LIZARDS; SPECIES GROUP; WEST-INDIES; TREES AB We report the results of phylogenetic analyses of 1447 bases of mitochondrial DNA sequence for 21 populations representing seven species of the Anolis grahami series (A. conspersus, A. garmani, A. grahami, A. lineatopus, A. opalinus, A. redonditus, and A. valencienni), six of which occur on Jamaica. These data include 705 characters that are phylogenetically informative according to parsimony. A parsimony analysis of these data combined with previously published allozymic data yields a single most parsimonious tree with strong support for monophyly of the A. grahami series, the sister-group relationship between Anolis lineatopus and A. reconditus and a clade composed of Anolis garmani, A. grahami, and A. opalinus. Based on DNA data alone, A. conspersus is nested within A. grahami. Haplotypes sampled from geographic populations of A. grahami, A. lineatopus, and A. opalinus are highly divergent (approximate to12-15% sequence difference on average for each species) and show similar phylogeographic patterns, suggesting that each of these currently recognized species may be a complex of species. Anolis valencienni also shows high sequence divergence among haplotypes from different geographic populations (approximate to8% sequence difference) and may contain cryptic species. Divergence among haplotypes within A. garmani is substantially lower (approximate to3% sequence difference), and phylogeographic patterns are significantly different from those observed in A. grahami, A. lineatopus and A. opalinus. (C) 2002 Wiley-Liss, Inc. C1 Villanova Univ, Dept Biol, Villanova, PA 19085 USA. Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. Smithsonian Inst, Natl Museum Nat Hist, Div Amphibians & Reptiles, Washington, DC 20560 USA. Washington Univ, Dept Biol, St Louis, MO 63130 USA. RP Jackman, TR (reprint author), Villanova Univ, Dept Biol, Villanova, PA 19085 USA. OI Jackman, Todd/0000-0002-5391-8136 NR 78 TC 43 Z9 46 U1 3 U2 7 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0022-104X J9 J EXP ZOOL JI J. Exp. Zool. PD APR 15 PY 2002 VL 294 IS 1 BP 1 EP 16 DI 10.1002/jer.10073 PG 16 WC Zoology SC Zoology GA 537GX UT WOS:000174751500001 PM 11932945 ER PT J AU Kral, P Sadeghpour, HR AF Kral, P Sadeghpour, HR TI Laser spinning of nanotubes: A path to fast-rotating microdevices SO PHYSICAL REVIEW B LA English DT Article ID INDIVIDUAL CARBON NANOTUBES; OPTICAL CENTRIFUGE; PARTICLES; NANOMECHANICS; ACCELERATION; MICROSCOPY; MOLECULES; PHONONS; GAS AB We show that circularly polarized light can spin nanotubes with GHz frequencies. In this method, angular momenta of infrared photons are resonantly transferred to nanotube phonons and passed to the tube body by "Umklapp" scattering. We investigate experimental realization of this ultrafast rotation in carbon nanotubes, levitating in an optical trap and undergoing mechanical vibrations, and discuss possible applications to rotating microdevices. C1 Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Kral, P (reprint author), Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. NR 41 TC 31 Z9 31 U1 0 U2 5 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD APR 15 PY 2002 VL 65 IS 16 AR 161401 DI 10.1103/PhysRevB.65.161401 PG 4 WC Physics, Condensed Matter SC Physics GA 547GQ UT WOS:000175325000017 ER PT J AU Harry, GM Houser, JL Strain, KA AF Harry, GM Houser, JL Strain, KA TI Comparison of advanced gravitational-wave detectors SO PHYSICAL REVIEW D LA English DT Article ID ACOUSTIC QUALITY FACTOR; FUSED-SILICA FIBERS; NEUTRON-STAR; COMPACT BINARIES; MECHANICAL LOSS; THERMAL NOISE; STELLAR CORES; RADIATION; ANTENNAS; INTERFEROMETER AB We compare two advanced designs for gravitational-wave antennas in terms of their ability to detect two possible gravitational wave sources. Spherical, resonant mass antennas and interferometers incorporating resonant sideband extraction (RSE) were modeled using experimentally measurable parameters. The signal-to-noise ratio of each detector for a binary neutron star system and a rapidly rotating stellar core were calculated. For a range of plausible parameters we found that the advanced LIGO interferometer incorporating RSE gave higher signal-to-noise ratios than a spherical detector resonant at the same frequency for both sources. Spheres were found to be sensitive to these sources at distances beyond our galaxy. Interferometers were sensitive to these sources at far enough distances that several events per year would be expected. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA. Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. MIT, LIGO Lab, Cambridge, MA 02139 USA. RP MIT, LIGO Lab, Room NW17-161,175 Albany St, Cambridge, MA 02139 USA. RI Strain, Kenneth/D-5236-2011 OI Strain, Kenneth/0000-0002-2066-5355 NR 85 TC 14 Z9 14 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD APR 15 PY 2002 VL 65 IS 8 AR 082001 DI 10.1103/PhysRevD.65.082001 PN A PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 544FE UT WOS:000175146900004 ER PT J AU Li, LX AF Li, LX TI Toy model for the magnetic connection between a black hole and a disk SO PHYSICAL REVIEW D LA English DT Article ID EXTRACTING ENERGY; ACCRETION DISK AB A magnetic field connecting a Kerr black hole to a disk rotating around it can extract energy and angular momentum from the black hole and transfer them to the disk if the black hole rotates faster than the disk. The energy can be dissipated and radiated away by the disk, which makes the disk shine without the need of accretion. In this paper we present a toy model for the magnetic connection: A single electric current flowing around a Kerr black hole in the equatorial plane generates a poloidal magnetic field which connects the black hole to the disk. The rotation of the black hole relative to the disk generates an electromotive force which in turn generates a poloidal electric current flowing through the black hole and the disk and produces a power on the disk. We will consider two cases: (1) The toroidal current flows on the inner boundary of the disk, which generates a poloidal magnetic field connecting the horizon of the black hole to a region of the disk beyond the inner boundary; (2) the toroidal current flows on a circle inside the inner boundary of the disk but outside the horizon of the black hole, which generates a poloidal magnetic field connecting a portion of the horizon of the black hole to the whole disk. We will calculate the power produced by the magnetic connection and the resulting radiation flux of the disk in the absence of accretion, and compare them with that produced by accretion. C1 Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Li, LX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM lli@cfa.harvard.edu NR 20 TC 15 Z9 16 U1 2 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD APR 15 PY 2002 VL 65 IS 8 AR 084047 DI 10.1103/PhysRevD.65.084047 PN B PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 544FF UT WOS:000175147000011 ER PT J AU Marian, P Marian, TA Scutaru, H AF Marian, P Marian, TA Scutaru, H TI Quantifying nonclassicality of one-mode Gaussian states of the radiation field SO PHYSICAL REVIEW LETTERS LA English DT Article ID SQUEEZED THERMAL STATES; QUANTUM TELEPORTATION; NOISE; DISTANCE; FIDELITY; OPTICS; LIGHT; BURES AB We define the degree of nonclassicality of a one-mode Gaussian state of the quantum electromagnetic field in terms of the Bures distance between the state and the set of all classical one-mode Gaussian states. We find the closest classical Gaussian state and the degree of nonclassicality using a recently established expression for the Uhlmann fidelity of two single-mode Gaussian states. The decrease of nonclassicality under thermal mapping is carefully analyzed. Along the same lines, we finally present the evolution of nonclassicality during linear amplification. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Bucharest, Dept Chem, Phys Lab, R-70346 Bucharest, Romania. Univ Bucharest, Dept Phys, R-76900 Bucharest, Romania. Romanian Acad, Ctr Adv Studies, R-76117 Bucharest, Romania. RP Marian, P (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 31 TC 66 Z9 66 U1 0 U2 4 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 APR 15 PY 2002 VL 88 IS 15 AR 153601 DI 10.1103/PhysRevLett.88.153601 PG 4 WC Physics, Multidisciplinary SC Physics GA 537RM UT WOS:000174773400012 PM 11955195 ER PT J AU Muller, A Phaneuf, RA Aguilar, A Gharaibeh, MF Schlachter, AS Alvarez, I Cisneros, C Hinojosa, G McLaughlin, BM AF Muller, A Phaneuf, RA Aguilar, A Gharaibeh, MF Schlachter, AS Alvarez, I Cisneros, C Hinojosa, G McLaughlin, BM TI Photoionization of C2+ ions: time-reversed recombination of C3+ with electrons SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID CROSS-SECTIONS; THRESHOLD; ELEMENTS; CARBON AB We have investigated photoionization (PI) of the S-1 ground state and P-3(o) metastable states of C2+ ions in the photon energy range 40.8-56.9 eV at a resolution of 30 meV. Absolute PI cross sections have been measured using a photon-ion merged beam arrangement at the Advanced Light Source. Detailed calculations using the semi-relativistic Breit-Pauli R-matrix approach suggest a fraction of 40% of metastable ions in the primary beam of the experiment. The present results are discussed in the light of previous electron-C3+-ion photorecombination (PR) studies. As an example, the role of the intermediate C2+(2p4d P-1) resonance in both PI and PR is analysed. C1 Univ Giessen, Inst Kernphys, D-35392 Giessen, Germany. Univ Nevada, Dept Phys, Reno, NV 89557 USA. Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA. Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico. 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. RP Muller, A (reprint author), Univ Giessen, Inst Kernphys, D-35392 Giessen, Germany. RI Muller, Alfred/A-3548-2009 OI Muller, Alfred/0000-0002-0030-6929 NR 22 TC 42 Z9 42 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD APR 14 PY 2002 VL 35 IS 7 BP L137 EP L143 AR PII S0953-4075(02)31274-4 DI 10.1088/0953-4075/35/7/101 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 548AB UT WOS:000175364400001 ER PT J AU Cecchi-Pestellini, C Dalgarno, A AF Cecchi-Pestellini, C Dalgarno, A TI C-2 absorption-line diagnostics of diffuse interstellar clouds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE molecular processes; ISM : clouds; ISM : individual : Cygnus OB2No. 12; ISM : molecules ID ZETA-OPHIUCHI; H-3(+); ASSOCIATION; SPACE AB The excitation of the diatomic carbon molecule in diffuse interstellar clouds is discussed for a cloud with large density fluctuations of small linear filling factor along the line of sight. Possible implications for the chemistry of the diffuse cloud in front of Cygnus OB2 No. 12 are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. RP Cecchi-Pestellini, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cecchi Pestellini, Cesare/0000-0001-7480-0324 NR 20 TC 24 Z9 24 U1 0 U2 3 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2002 VL 331 IS 3 BP L31 EP L34 DI 10.1046/j.1365-8711.2002.05418.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546JG UT WOS:000175270500002 ER PT J AU Kraft, RP Forman, WR Jones, C Murray, SS Hardcastle, MJ Worrall, DM AF Kraft, RP Forman, WR Jones, C Murray, SS Hardcastle, MJ Worrall, DM TI Chandra observations of the X-ray jet in Centaurus A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Centaurus A, NGC 5128); galaxies : jets; X-rays : galaxies ID ROSAT-HRI OBSERVATIONS; M87 JET; RADIO; RESOLUTION; POLARIMETRY; EMISSION; NGC-5128; NUCLEUS AB We present high angular resolution X-ray images and spectra from two Chandra AXAF CCD Imaging Spectrometer (ACIS-I) observations of the X-ray jet in the nearby radio galaxy Cen A. We find that the X-ray emission from the jet is composed of a low surface brightness diffuse component extending continuously from within at least 60 pc of the active nucleus into the northeast radio lobe 4 kpc from the nucleus, along with 31 discrete compact knots, most of which are extended at the resolution of our observation. We find that there are small but significant differences between the X-ray and radio morphologies of the inner jet at the arcsecond level, making it unlikely that a single, spatially coincident population of ultrarelativistic electrons is responsible for the emission in both energy regimes. We suggest that the X-ray knots of the inner jet are indeed the sites of particle acceleration and shocks and that the X-ray and radio knot offsets are caused by a combination of particle diffusion and energy loss. These offsets may be a common feature of all jets in radio galaxies, or at least jets in FR I galaxies, and may be fundamental to the physics of such jets. They are best observed in Cen A because the source is so close. Even though the X-ray and radio knots are offset in position and there are variations of more than a factor of 3 in the ratio of X-ray to radio flux density in the inner jet, the radio to X-ray two-point spectral indices at the X-ray knots are not unusually at and are consistent with those observed in other X-ray jets seen in FR I galaxies such as M87 and 3C 66B. We find the width of the jet in the X-ray bandpass to be narrower than that measured in the radio along most of its length. The X-ray spectra of several regions of the jet are well fitted by absorbed power-law models with photon indices similar to2.2-2.5, although the spectrum of one bright knot located similar to1 kpc from the nucleus (knot B) is harder (photon index = 2.0). 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,MS-31, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012; OI Hardcastle, Martin/0000-0003-4223-1117; Forman, William/0000-0002-9478-1682 NR 43 TC 80 Z9 80 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2002 VL 569 IS 1 BP 54 EP 71 DI 10.1086/339062 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539NF UT WOS:000174876800007 ER PT J AU Eisner, JA Greenhill, LJ Herrnstein, JR Moran, JM Menten, KM AF Eisner, JA Greenhill, LJ Herrnstein, JR Moran, JM Menten, KM TI Outflow 20-2000 AU from a high-mass protostar in W51-IRS 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (W51); ISM : jets and outflows; ISM : kinematics and dynamics; ISM : molecules; masers; stars : pre-main sequence ID YOUNG STELLAR OBJECTS; H-II REGIONS; DYNAMICAL COLLAPSE; MOLECULAR OUTFLOW; PROPER MOTIONS; STAR-FORMATION; AMMONIA MASER; SIO MASERS; ORION-KL; W51 AB We present the results of the first high angular resolution observations of SiO maser emission toward the star-forming region W51-IRS 2 made with the Very Large Array (VLA) and Very Long Baseline Array (VLBA). Our images of the H2O maser emission in W51-IRS 2 reveal two maser complexes bracketing the SiO maser source. One of these H2O maser complexes appears to trace a bow shock whose opening angle is consistent with the opening angle observed in the distribution of SiO maser emission. A comparison of our H2O maser image with an image constructed from data acquired 19 years earlier clearly shows the persistence and motion of this bow shock. The proper motions correspond to an outflow velocity of 80 km s(-1), which is consistent with the data of 19 years ago ( that spanned 2 years). We have discovered a two-armed linear structure in the SiO maser emission on scales of similar to25 AU, and we find a velocity gradient on the order of 0.1 km s(-1) AU(-1) along the arms. We propose that the SiO maser source traces the limbs of an accelerating bipolar outflow close to an obscured protostar. We estimate that the outflow makes an angle of less than 20degrees with respect to the plane of the sky. Our measurement of the acceleration is consistent with a reported drift in the line-of-sight velocity of the W51 SiO maser source. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Eisner, JA (reprint author), CALTECH, Palomar Observ 105 24, Pasadena, CA 91125 USA. OI Moran, James/0000-0002-3882-4414 NR 39 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 APR 10 PY 2002 VL 569 IS 1 BP 334 EP 342 DI 10.1086/338968 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539NF UT WOS:000174876800028 ER PT J AU Torres, MAP Callanan, PJ Garcia, MR McClintock, JE Garnavich, P Balog, Z Berlind, P Brown, WR Calkins, M Mahdavi, A AF Torres, MAP Callanan, PJ Garcia, MR McClintock, JE Garnavich, P Balog, Z Berlind, P Brown, WR Calkins, M Mahdavi, A TI Optical spectral monitoring of XTE J1118+480 in outburst: Evidence for a precessing accretion disk? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; stars : individual (XTE J1118+480); X-rays : stars ID X-RAY TRANSIENT; MULTIWAVELENGTH OBSERVATIONS; OY CARINAE; H-I; SPECTROSCOPY; SUPERHUMPS; EMISSION; BINARIES; SUPEROUTBURST; STREAM AB We present spectroscopic observations of the X-ray transient XTE J1118+480 acquired during different epochs following the 2000 March outburst. We find that the emission line profiles show variations in their double-peak structure on timescales longer than the 4.1 hr orbital period. We suggest that these changes are due to a tidally driven precessing disk. Doppler imaging of the more intense Balmer lines and the He II lambda4686 line shows evidence of a persistent region of enhanced intensity superposed on the disk which is probably associated with the gas stream, the hot spot, or both. We discuss the possible origins of the optical flux in the system and conclude that it may be due to a viscously heated disk. C1 Univ Coll, Dept Phys, Cork, Ireland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. RP Univ Coll, Dept Phys, Cork, Ireland. EM mapt@phys.ucc.ie; paulc@ucc.ie; mgarcia@cfa.harvard.edu; jem@cfa.harvard.edu; pgarnavi@nd.edu; pzhao@cfa.harvard.edu; pberlind@cfa.harvard.edu; wbrown@cfa.harvard.edu; mcalkins@cfa.harvard.edu; amahdavi@cfa.harvard.edu NR 43 TC 15 Z9 15 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 APR 10 PY 2002 VL 569 IS 1 BP 423 EP 431 DI 10.1086/339282 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539NF UT WOS:000174876800036 ER PT J AU Dobrzycki, A Groot, PJ Macri, LM Stanek, KZ AF Dobrzycki, A Groot, PJ Macri, LM Stanek, KZ TI Discovery of four X-ray quasars behind the Large Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE Magellanic Clouds; quasars : individual (QSO J050736.52-684751.7,QSO J050833.29-685427.5,QSO J050924.05-672124.1,QSO J051853.19-690217.7); X-rays : general ID GRAVITATIONAL LENSING EXPERIMENT; LMC REGION; GALAXIES; CATALOG; DUST AB We present the discovery of four X-ray quasars (z(em) = 0.26, 0.53, 0.61, and 1.63) located behind the Large Magellanic Cloud; three of them are located behind the bar of the LMC. The quasars were identified via spectroscopy of optical counterparts to X-ray sources found serendipitously by the Chandra X-Ray Observatory satellite. All four quasars have archival VI photometry from the second phase of the Optical Gravitational Lensing Experiment (OGLE-II); one of them was found by OGLE to be variable. We present the properties of the quasars and discuss their possible applications. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dobrzycki, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Groot, Paul/K-4391-2016; OI Groot, Paul/0000-0002-4488-726X; Macri, Lucas/0000-0002-1775-4859 NR 24 TC 20 Z9 20 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2002 VL 569 IS 1 BP L15 EP L18 DI 10.1086/340539 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539PE UT WOS:000174879000004 ER PT J AU Mazzotta, P Fusco-Femiano, R Vikhlinin, A AF Mazzotta, P Fusco-Femiano, R Vikhlinin, A TI Chandra observation of a 300 kiloparsec hydrodynamic instability in the intergalactic medium of the merging cluster of galaxies A3667 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general galaxies : clusters : individual (Abell 3667); instabilities; turbulence; X-rays : galaxies : clusters AB We present results from the combination of two Chandra pointings of the central region of the cluster of galaxies A3667. From the data analysis of the first pointing, Vikhlinin, Markevitch, and Murray reported the discovery of a prominent cold front that is interpreted as the boundary of a cool gas cloud moving through the hotter ambient gas. They discussed the role of the magnetic fields in maintaining the apparent dynamical stability of the cold front over a wide sector at the forward edge of the moving cloud and in suppressing transport processes across the front. In this Letter, we identify two new features in the X-ray image of A3667: (1) a 300 kpc arclike filamentary X-ray excess extending from the cold gas cloud border into the hotter ambient gas and (2) a similar arclike filamentary X-ray depression that develops inside the gas cloud. Both features are located beyond the sector identified by the cold front and are oriented in a direction perpendicular to the direction of motion. The temperature map suggests that the temperature of the filamentary excess is consistent with that inside the gas cloud, while the temperature of the depression is consistent with that of the ambient gas. We suggest that the observed features represent the first evidence for the development of a large-scale hydrodynamic instability in the cluster atmosphere resulting from a major merger. This result confirms previous claims for the presence of a moving cold gas cloud in the hotter ambient gas. Moreover, it shows that, although the gas mixing is suppressed at the leading edge of the subcluster as a result its magnetic structure, strong turbulent mixing occurs at larger angles toward the direction of motion. We show that this mixing process may favor the deposition of a nonnegligible quantity of thermal energy right in the cluster center, affecting the development of the central cooling flow. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Durham, Dept Phys, Durham DH1 3LE, England. Ist Astrofis Spaziale, Area CNR Tor Vergata, I-00133 Rome, Italy. RP Mazzotta, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Mazzotta, Pasquale/B-1225-2016 OI Mazzotta, Pasquale/0000-0002-5411-1748 NR 10 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 APR 10 PY 2002 VL 569 IS 1 BP L31 EP L34 DI 10.1086/340481 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539PE UT WOS:000174879000008 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, MC Thaddeus, P TI Laboratory detection of a bent-chain carbene isomer of C6H2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; line : identification; molecular data; molecular processes; radio lines : ISM ID ASTRONOMICAL DETECTION; LINE SURVEY; H2CCC; TMC-1; C5H2 AB The rotational spectrum of a bent singlet isomer of the C6H2 carbene, a carbon chain that has been observed C H in the laboratory and in space, was detected in a supersonic molecular beam by Fourier transform microwave spectroscopy. The three rotational constants and the leading centrifugal distortion constants were determined to high accuracy, allowing the entire rotational spectrum of this molecule below 120 GHz to be calculated to a fraction of 1 km s(-1) in equivalent radio velocity. The spectroscopic constants agree well with those recently calculated from high-level ab initio methods by Sattelmeyer & Stanton. Although bent C6H2 is calculated to lie 54 kcal mol(-1) above the ground-state isomer triacetylene, it is comparable in polarity and stability to the previously observed cumulene carbene with a linear carbon backbone. Rotational lines of bent C6H2 can be detected in the laboratory with a signal-to-noise ratio of better than 20 in 1 minute of integration, implying that several six-membered ring isomers of C6H2 lying about 40 kcal mol(-1) above ground may also be found in the laboratory and in space. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 14 TC 6 Z9 6 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 APR 10 PY 2002 VL 569 IS 1 BP L55 EP L58 DI 10.1086/340422 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539PE UT WOS:000174879000014 ER PT J AU Schwartz, DA AF Schwartz, DA TI X-ray jets as cosmic beacons SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background galaxies : jets; quasars : general; X-rays : galaxies ID RADIO GALAXIES; LUMINOSITY FUNCTION; ROSAT HRI; PKS-0637-752; QUASARS AB The Chandra X-Ray Observatory has proved to have the unique capability to detect jets and hot spots in quasars and radio sources. If X-rays from any of the observed objects are due to inverse Compton scattering of relativistic electrons on the cosmic microwave background (CMB) radiation, then such an object will be detectable with the same surface brightness anywhere in the more distant universe. This is because the enhancement of the CMB energy density by a factor of (1 + z)(4) compensates for the (1 + z)(-4) decrease of surface brightness. These may already have been detected in X-ray surveys, and we point out the unique considerations that must be applied to correctly identify them, namely, that the jets could outshine the parent quasars, that a few arcsecond X-ray position circle will likely not include the quasar, and that the X-ray source will be resolved with telescopes that have 2" resolution. We predict that Chandra will detect many of these in the next observing cycle, for example, in a distant Sloan survey quasar or the ROSAT X-ray source PKS 2215+020. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02137 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02137 USA. NR 31 TC 59 Z9 59 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2002 VL 569 IS 1 BP L23 EP L26 DI 10.1086/340482 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539PE UT WOS:000174879000006 ER PT J AU Silverman, JD Green, PJ Kim, DW Wilkes, BJ Cameron, RA Morris, D Dosaj, A Smith, C Infante, L Smith, PS Jannuzi, BT Mathur, S AF Silverman, JD Green, PJ Kim, DW Wilkes, BJ Cameron, RA Morris, D Dosaj, A Smith, C Infante, L Smith, PS Jannuzi, BT Mathur, S TI Discovery of A z=4.93, X-ray-selected quasar by the Chandra multiwavelength project (chaMP) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei; quasars : general; quasars : individual (CXOMP J213945.0-234655); X-rays : general ID HIGH-REDSHIFT QUASARS; LUMINOSITY FUNCTION; SPACE DENSITY; ALPHA FOREST; SPECTROPHOTOMETRY; EVOLUTION; DECREASE AB We present X-ray and optical observations of CXOMP J213945.0-234655, a high-redshift (z = 4.93) quasar discovered through the Chandra Multiwavelength Project (ChaMP). This object is the most distant X-ray-selected quasar published, with a rest-frame X-ray luminosity of L-x = 5.9 x 10(44) ergs s(-1) (measured in the 0.3-2.5 keV band and corrected for Galactic absorption). CXOMP J213945.0-234655 is a g' dropout object (>26.2), with r' = 22.87 and i' = 21.36. The rest- frame X-ray-to-optical flux ratio is similar to quasars at lower redshifts and slightly X-ray bright relative to z > 4 optically selected quasars observed with Chandra. The ChaMP is beginning to acquire significant numbers of high-redshift quasars to investigate the X-ray luminosity function out to. z similar to 5. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Silverman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 29 TC 24 Z9 24 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2002 VL 569 IS 1 BP L1 EP L4 DI 10.1086/340458 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539PE UT WOS:000174879000001 ER PT J AU Butler, JP Mair, RW Hoffmann, D Hrovat, MI Rogers, RA Topulos, GP Walsworth, RL Patz, S AF Butler, JP Mair, RW Hoffmann, D Hrovat, MI Rogers, RA Topulos, GP Walsworth, RL Patz, S TI Measuring surface-area-to-volume ratios in soft porous materials using laser-polarized xenon interphase exchange nuclear magnetic resonance SO JOURNAL OF PHYSICS-CONDENSED MATTER LA English DT Letter ID TIME-DEPENDENT DIFFUSION; GAS-DIFFUSION; LIGHT-SCATTERING; MEDIA; LUNG; COEFFICIENT; PROBE; NMR AB We demonstrate a minimally invasive nuclear magnetic resonance (NMR) technique that enables determination of the surface-area-to-volume ratio (S/V) of soft porous materials from measurements of the diffusive exchange of laser-polarized Xe-129 between gas in the pore space and Xe-129 dissolved in the solid phase. We apply this NMR technique to porous polymer samples and find approximate agreement with destructive stereological measurements of S/V obtained with optical confocal microscopy. Potential applications of laser-polarized xenon interphase exchange NMR include measurements of in vivo lung function in humans and characterization of gas chromatography columns. C1 Harvard Univ, Sch Publ Hlth, Boston, MA 02115 USA. Harvard Univ, Sch Med, Boston, MA 02115 USA. Brigham & Womens Hosp, Boston, MA 02115 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Mirtech Inc, Brockton, MA 02301 USA. RP Butler, JP (reprint author), Harvard Univ, Sch Publ Hlth, 665 Huntington Ave, Boston, MA 02115 USA. RI Patz, Samuel/I-2879-2012 FU NCRR NIH HHS [R21 RR014297-02, R21 RR014297, R21 RR014297-01A1, R21 RR014297-01A18280, R21-RR/CA14297]; NHLBI NIH HHS [R01 HL-55569] NR 28 TC 47 Z9 47 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-8984 J9 J PHYS-CONDENS MAT JI J. Phys.-Condes. Matter PD APR 8 PY 2002 VL 14 IS 13 BP L297 EP L304 AR PII S0953-8984(02)32496-2 DI 10.1088/0953-8984/14/13/103 PG 8 WC Physics, Condensed Matter SC Physics GA 547ZH UT WOS:000175362700003 PM 12741395 ER PT J AU Tudge, CC Scheltinga, DM AF Tudge, CC Scheltinga, DM TI Spermatozoal morphology of the freshwater anomuran Aegla longirostri Bond-Buckup & Buckup, 1994 (Crustacea : Decapoda : Aeglidae) from South America SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID ULTRASTRUCTURE; PHYLOGENY AB Unique sperm morphology is described for Aegla longirostri Bond-Buckup & Buckup, 1994. a representative of the freshwater anomuran family Aeglidae from South America. Comparisons of the spermatozoal ultrastructure of this species with that described for other anomurans indicate that A. longirostri has a distinct suite of spermatozoal characters. Within the Anomura, the aeglids share more spermatozoal characters with the superfamily Lomoidea. represented by the monotypic Australian endemic genus, Lomis, than to any previously described representative from the Galatheoidea, Hippoidea. or Paguroidea. A more basal ancestry, with an independent evolutionary lineage. within the Anomura is Postulated for the Aeglidae. A Superficial resemblance of the spermatozoal ultrastructure of A. longirostri to that described for a palinurid lobster, Jasus, and a thalassinidean mud shrimp, Neaxius, is also noted. C1 American Univ, Dept Biol, Washington, DC 20016 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Univ Queensland, Dept Zool & Entomol, Brisbane, Qld 4072, Australia. RP Tudge, CC (reprint author), American Univ, Dept Biol, 4400 Massachusetts Ave NW, Washington, DC 20016 USA. NR 49 TC 18 Z9 19 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 3 PY 2002 VL 115 IS 1 BP 118 EP 128 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 541NJ UT WOS:000174990400009 ER PT J AU Kornicker, LS Yager, J AF Kornicker, LS Yager, J TI Description of Spelaeoecia saturno, a new species from an anchialine cave in Cuba, (Crustacea : Ostracoda : Myodocopa : Halocyprididae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new troglobitic halocyprid species of Ostracoda, Spelaeoecia saturno, is described from Cueva El Saturno, Holguin Province, northeast coast of Cuba. Also, Spelaeoecia cubensis Kornicker & Yager, 1996, is reported from two additional caves in southern Matanzas Province: Cueva El Brinco and Cueva 1900. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Antioch Coll, Environm & Biol Sci Dept, Yellow Springs, OH 45387 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 12 TC 1 Z9 1 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 APR 3 PY 2002 VL 115 IS 1 BP 153 EP 170 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 541NJ UT WOS:000174990400013 ER PT J AU Hershler, R Liu, HP Stockwell, CA AF Hershler, R Liu, HP Stockwell, CA TI A new genus and species of aquatic gastropods (Rissooidea : Hydrobiidae) from the North American Southwest : phylogenetic relationships and biogeography SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID WHITE SANDS PUPFISH; NEW-MEXICO; BASIN; TEXAS AB Juturnia, a new genus composed of three species from the Rio Grande region of southwestern North America, is described. Two of these species were previously placed in the genus Durangonella while the third, J. tularosae, is described herein. Juturnia is shown to be a monophyletic subunit of the gastropod subfamily Cochliopinae based on phylogenetic analysis of mitochondrial DNA sequences and an uniquely shared morphological character (within the subfamily), the presence of a single non-glandular lobe on the inner edge of the penis. Our phylogenetic hypothesis indicates that Juturnia is most closely related to North American brackish-coastal taxa, and we conjecture that progenitors of this genus penetrated inland along the Tertiary drainages which headed along eastern flanks of Laramide uplifts and flowed to the Gulf of Mexico. Subsequent vicariance of congeners in southeastern New Mexico is attributed to development of the Pecos depression, and inception of the drainage divide between the Rio Grande Rift and southern Great Plains. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. N Dakota State Univ, Dept Zool, Fargo, ND 58105 USA. RP Hershler, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 75 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 APR 3 PY 2002 VL 115 IS 1 BP 171 EP 188 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 541NJ UT WOS:000174990400014 ER PT J AU Thompson, FG Hershler, R AF Thompson, FG Hershler, R TI Tepalcatia, a new genus of hydrobiid snails (Prosobranchia : Rissooidea) from the Rio Balsas basin, central Mexico SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Tepalcatia, a new genus of cochliopine snail from the Rio Balsas basin of central Mexico, is composed of Tepalcatia tela, new species, described herein; and Tepalcatia polia (Thompson & Hershler, 199 1), previously assigned to Aroapyrgus. A third species, Tepalcatia bakeri (Pilsbry, 1891a), is tentatively referred to the genus. This snail, known only as a subfossil, most recently was assigned to Tryonia. Tepalcatia is placed in the informal "Cochliopa group" based on the absence of penial glands; division of penis into a folded base and smooth, tapered filament; and the very short female sperm duct. Tepalcatia is distinguished from other members of this group by its ovate-conic to turriform shell; long ducts of the female sperm pouches; and large circular-horizontal loop of the coiled oviduct. Tepalcatia tela differs from T polia by its smaller size, more elongate shell, longer and broader penial filament, and several additional anatomical features. Tepalcatia bakeri is a large, slender-shelled species with stronger spiral sculpture than its congeners. C1 Univ Florida, Florida Museum Nat Hist, Div Malacol, Gainesville, FL 32611 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Thompson, FG (reprint author), Univ Florida, Florida Museum Nat Hist, Div Malacol, Gainesville, FL 32611 USA. NR 20 TC 1 Z9 1 U1 0 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 3 PY 2002 VL 115 IS 1 BP 189 EP 204 PG 16 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 541NJ UT WOS:000174990400015 ER PT J AU Cairns, SD AF Cairns, SD TI A new species of Chrysogorgia (Anthozoa : Octocorallia) from the Antarctic SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new species of Chrysogorgia, C. antarctica, is described from the Ross Sea, Antarctica, representing the first chrysogorgiid described from south of 50degreesS. It is distinguished by having only scales in its body wall and tentacles (Group C), a dichotomously branching main stem with a 1/4R branching sequence, and uniquely shaped tentacular sclerites. Based on an extrapolation of the height (and thus age) of the colony and the number of concentric axial lamellae, it was determined that one lamella is secreted approximately every 43 days, not on an annual basis as in tropical species that have been examined. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Invertebrate Zool, Washington, DC 20560 USA. RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Invertebrate Zool, Washington, DC 20560 USA. NR 9 TC 4 Z9 5 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 3 PY 2002 VL 115 IS 1 BP 217 EP 222 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 541NJ UT WOS:000174990400017 ER PT J AU Dudley, R AF Dudley, R TI Fermenting fruit and the historical ecology of ethanol ingestion: is alcoholism in modern humans an evolutionary hangover? SO ADDICTION LA English DT Article DE alcoholism; ethanol; frugivory; fruit; primate ID DROSOPHILA; DEPENDENCE; REWARD; RISK; HORMESIS; DRINKING; GENES; POLYMORPHISM; POPULATIONS; SENSITIVITY AB In the field of addiction research, the possibility of ancestral exposure to psychoactive compounds has generally been excluded. A paleobiological approach to the human diet, however, illustrates the potential utility of historical data in interpreting modern-day addictive behaviors. Low-level dietary exposure to ethanol via ingestion of fermenting fruit has probably characterized the predominantly frugivorous anthropoid lineage for about 40 million years. Potentially adaptive primate behaviors associated with the natural occurrence of ethanol include the olfactory use of ethanol plumes to localize fruit crops, the use of ethanol as an appetitive stimulant to facilitate rapid consumption of transient nutritional resources, and the physiological exploitation of the caloric benefits of ethanol. Such behavioral and energetic advantages probably pertain to all animal taxa that consume fermenting fruit, and may have been retained in modern humans in spite of considerable dietary diversification over the last several million years. In contemporary human environments, excessive consumption of ethanol would then represent maladaptive cooption of ancestrally advantageous behaviors given essentially ad libitum access to a compound otherwise found only within scarce nutritional substrates. Epidemiologically demonstrated health benefits of low-level alcohol consumption are consistent with an ancient and potentially adaptive exposure of primate frugivores to this most common of the psychoactive substances. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Univ Texas, Waggoner Ctr Alcohol & Addict Res, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Dudley, R (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. NR 62 TC 60 Z9 61 U1 3 U2 25 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0965-2140 J9 ADDICTION JI Addiction PD APR PY 2002 VL 97 IS 4 BP 381 EP 388 DI 10.1046/j.1360-0443.2002.00002.x PG 8 WC Substance Abuse; Psychiatry SC Substance Abuse; Psychiatry GA 539BY UT WOS:000174850900003 PM 11964055 ER PT J AU Lellinger, DB AF Lellinger, DB TI Obituary: Warren H. Wagner, Jr. (1920-2000) SO AMERICAN FERN JOURNAL LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Lellinger, DB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 USA SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD APR-JUN PY 2002 VL 92 IS 2 BP 43 EP 44 PG 2 WC Plant Sciences SC Plant Sciences GA 584JR UT WOS:000177463900004 ER PT J AU Lellinger, DB AF Lellinger, DB TI Bibliography of Warren Herbert Wagner, Jr SO AMERICAN FERN JOURNAL LA English DT Biographical-Item AB This bibliography contains 395 entries, all the scientific publications of Warren H. Wagner, Jr. The bibliography is based on a list maintained by Prof. Wagner, with additional comments and entries by Dr. Florence S. Wagner and Dr. Richard Rabeler. It includes abstracts, ephemera, reports, and reviews. The bibliography is in rough chronological order of publication. Exact publication dates were found for most journal articles. However, month or estimated dates were used for other publications, especially books, which usually are not datable within a year. All the entries are contained in a searchable database now maintained by Florence S. Wagner, The database categorizes the publications according to their subject matter and includes the more or less exact publication dates that are the basis for the chronological list. C1 Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Lellinger, DB (reprint author), Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 USA SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD APR-JUN PY 2002 VL 92 IS 2 BP 50 EP 64 DI 10.1640/0002-8444(2002)092[0050:BOWHWJ]2.0.CO;2 PG 15 WC Plant Sciences SC Plant Sciences GA 584JR UT WOS:000177463900012 ER PT J AU Lellinger, DB AF Lellinger, DB TI Additions to the fern flora of Saba, Netherlands Antilles SO AMERICAN FERN JOURNAL LA English DT Article AB Recent fieldwork on Saba, Netherlands Antilles, has resulted in the discovery of nine fern species unrecorded for the island. All are known from other islands in the Antilles, as well as from other tropical areas. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Lellinger, DB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 USA SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD APR-JUN PY 2002 VL 92 IS 2 BP 93 EP 96 DI 10.1640/0002-8444(2002)092[0093:ATTFFO]2.0.CO;2 PG 4 WC Plant Sciences SC Plant Sciences GA 584JR UT WOS:000177463900015 ER PT J AU Skog, JE Zimmer, EA Mickel, JT AF Skog, JE Zimmer, EA Mickel, JT TI Additional support for two subgenera of Anemia (Schizaeaceae) from data for the chloroplast intergenic spacer region trnL-F and morphology SO AMERICAN FERN JOURNAL LA English DT Article ID PHYLOGENETIC-RELATIONSHIPS; EXTANT FERNS; SEQUENCES; RBCL; NUCLEAR; DNA AB An analysis of morphological data for 13 species with 33 characters and molecular data for 14 species from the chloroplast DNA intergenic spacer region trnL-F indicates that species of the genus Anemia fall into two well-supported subgenera, Anemiorrhiza and Anemia. In addition, one species of the genus Mohria appears to belong within Anemia. Although further study is required, these data support the relationships suggested by a previous study of fossil and extant representatives of the genus. C1 George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. Smithsonian Inst, Lab Mol Systemat, Washington, DC 20560 USA. New York Bot Garden, Bronx, NY 10458 USA. RP Skog, JE (reprint author), George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. RI Zimmer, Elizabeth/G-3890-2011 NR 28 TC 21 Z9 22 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 USA SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD APR-JUN PY 2002 VL 92 IS 2 BP 119 EP 130 DI 10.1640/0002-8444(2002)092[0119:ASFTSO]2.0.CO;2 PG 12 WC Plant Sciences SC Plant Sciences GA 584JR UT WOS:000177463900019 ER PT J AU McKeown, AH AF McKeown, AH TI Biological anthropology of the human skeleton. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP McKeown, AH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD APR PY 2002 VL 117 IS 4 BP 373 EP 374 DI 10.1002/ajpa.10068 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 533ZN UT WOS:000174560300011 ER PT J AU Henson, PM AF Henson, PM TI Invading Arcadia: Women scientists in the field in Latin America, 1900-1950 SO AMERICAS LA English DT Article ID SCIENCE C1 Smithsonian Inst Arch, Inst Hist Div, Washington, DC 20560 USA. RP Henson, PM (reprint author), Smithsonian Inst Arch, Inst Hist Div, Washington, DC 20560 USA. NR 74 TC 6 Z9 7 U1 0 U2 0 PU ACAD AMER FRANCISCAN HIST PI WEST BETHESDA PA BOX 34440, WEST BETHESDA, MD 20817 USA SN 0003-1615 J9 AMERICAS JI Americas PD APR PY 2002 VL 58 IS 4 BP 577 EP 600 DI 10.1353/tam.2002.0045 PG 24 WC History SC History GA 547YF UT WOS:000175360100004 ER PT J AU Crosthwaite, LP Turner, JL Buchholz, L Ho, PTP Martin, RN AF Crosthwaite, LP Turner, JL Buchholz, L Ho, PTP Martin, RN TI CO in the disk of the barred spiral galaxy M83: CO (1-0), CO (2-1), and neutral gas SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M83, NGC 5236); galaxies : ISM; galaxies : spiral; galaxies : structure; ISM : molecules ID RADIO-CONTINUUM EMISSION; PHOTON-DOMINATED REGIONS; MOLECULAR CLOUD COMPLEX; J=2-1 LINE OBSERVATIONS; CARBON-MONOXIDE; STAR-FORMATION; MILKY-WAY; PHOTODISSOCIATION REGIONS; PHYSICAL CONDITIONS; GALACTIC WARPS AB We present "on-the-fly" maps of CO (1-0) and CO (2-1) in the barred spiral galaxy M83. The entire optical disk is filled with CO emission in both lines, including interarm regions. For a "standard" conversion factor the total molecular mass is 2.5 x 10(9) M., 4% of the total dynamical mass. Molecular gas constitutes 80% of total gas mass within the inner 10' and 30% overall. CO (1-0) emission and 21 cm continuum emission are extremely well correlated spatially in regions where H-2 dominates the gas surface density. The spatial correlation between CO (1-0) and 100 mum emission is not as good. While the kinematics of the outer H I disk is severely nonaxisymmetrically perturbed, the kinematics of the CO disk and inner H I disk is well behaved and circular. The molecular disk appears to have a distinct hard edge at 5'. The hard edge is accompanied by a steep decline in the total gas surface density at that radius, although the H I does continue outward at a lower level. This edge is coincident with the onset of strong warping of the outer disk. The mean ratio of CO (2-1)/CO (1-0) emission is similar to1, high by Galactic standards. Peaks in this ratio in interarm regions suggest that the CO emission is optically thin there, among other possibilities. Thus, M83 is unusual in that it has a relatively axisymmetric, almost entirely molecular, inner 10' gas disk surrounded by a warped, entirely atomic, outer gas disk. A sharp discontinuity separates the inner and outer gas disks. This kind of gas distribution is not seen in other late-type, gas-rich spirals. C1 Univ Calif Los Angeles, Dept Phys & Astron, Div Astron & Astrophys, Los Angeles, CA 90095 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. RP Crosthwaite, LP (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Div Astron & Astrophys, Los Angeles, CA 90095 USA. NR 81 TC 50 Z9 50 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2002 VL 123 IS 4 BP 1892 EP 1912 DI 10.1086/339479 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 537JX UT WOS:000174756400007 ER PT J AU Barmby, P Holland, S Huchra, JP AF Barmby, P Holland, S Huchra, JP TI M31 globular clusters in the Hubble Space Telescope archive. II. Structural parameters SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M31); galaxies : star clusters ID STELLAR POPULATIONS; ELLIPTICAL GALAXIES; SURFACE PHOTOMETRY; LIGHT-DISTRIBUTION; FUNDAMENTAL PLANE; CORES; SYSTEM; RATIOS; RADII AB We analyze the structural parameters of the largest available sample of spatially resolved extragalactic globular clusters. The images of M31 GCs were found in a search of Hubble Space Telescope (HST) archival data, described in a companion paper. We measure the ellipticities and position angles of the clusters and conclude that the ellipticities are consistent with being caused by rotation. We find that most clusters surface brightness distributions are well fitted by two-dimensional single-mass Michie-King models. A few clusters show possible power-law distributions characteristic of core collapse, but the spatial resolution is not high enough to make definitive claims. As has been found for other galaxies, the metal-rich clusters are slightly smaller than the metal-poor clusters. There are strong correlations between structural properties of M31 GCs, as for Milky Way clusters, and the two populations are located close to the same fundamental plane in parameter space. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. RP Barmby, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 44 TC 81 Z9 81 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2002 VL 123 IS 4 BP 1937 EP 1952 DI 10.1086/339667 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 537JX UT WOS:000174756400010 ER PT J AU Georgantopoulos, I Panessa, F Akylas, A Zezas, A Cappi, M Comastri, A AF Georgantopoulos, I Panessa, F Akylas, A Zezas, A Cappi, M Comastri, A TI BeppoSAX observations of LINER-2 galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : starburst; X-rays : galaxies ID RAY ASTRONOMY SATELLITE; ASCA OBSERVATIONS; ON-BOARD; EMISSION; NUCLEI; SPECTRA; NGC-253; SEARCH AB We present BeppoSAX observations of 6 "type-2" LINER and "transition" galaxies (NGC 3379, NGC 3627, NGC 4125, NGC 4374, NGC 5195 and NGC 5879) from the Ho et al. (1997) spectroscopic sample of nearby galaxies. All objects are detected in the 2-10 keV band, having luminosities in the range L2-10 (keV) similar to 1 x 10(39)-1 x 10(40) erg s(-1). The PDS upper limits above 10 keV place constraints on the presence of a heavily obscured AGN in the case of NGC 3379 and NGC 4125. No significant variability is detected in any of the objects. The spectra are described in most cases by a simple power-law model with a spectral slope of Gamma similar to 1.7-2.5 while there is evidence neither for a significant absorption above the Galactic nor for an FeKalpha emission line. Therefore, based on the spectral properties alone, it is difficult to differentiate between a low-luminosity AGN or a star-forming galaxy scenario. However, imaging observations of NGC 3627 and NGC 5195 with Chandra ACIS-S reveal very weak nuclear sources while most of the X-ray flux originates either in off-nuclear point sources or in diffuse emission. The above clearly argue in favour of a star-forming origin for the bulk of the X-ray emission, at least in the above two sources. C1 Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. CNR, Ist Technol & Studio Radiaz Extraterr, I-40129 Bologna, Italy. Univ Athens, Dept Phys, Athens 15783, Greece. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Bologna, I-40127 Bologna, Italy. RP Georgantopoulos, I (reprint author), Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. RI Georgantopoulos, Ioannis/L-3687-2013; Akylas, Athanassios/K-4629-2013; Cappi, Massimo/F-4813-2015; Comastri, Andrea/O-9543-2015; Zezas, Andreas/C-7543-2011; OI Comastri, Andrea/0000-0003-3451-9970; Zezas, Andreas/0000-0001-8952-676X; Panessa, Francesca/0000-0003-0543-3617; Cappi, Massimo/0000-0001-6966-8920 NR 47 TC 16 Z9 16 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2002 VL 386 IS 1 BP 60 EP 68 DI 10.1051/0004-6361:20020078 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543YU UT WOS:000175132100009 ER PT J AU Dennerl, K Burwitz, V Englhauser, J Lisse, C Wolk, S AF Dennerl, K Burwitz, V Englhauser, J Lisse, C Wolk, S TI Discovery of X-rays from Venus with Chandra SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic processes; molecular processes; scattering; Sun : X-rays; gamma rays; planets and satellites : individual : Venus; X-rays : general ID SPECTRA; PHOTOABSORPTION; MOLECULES; ENERGIES; EMISSION; OXYGEN AB On January 10 and 13, 2001, Venus was observed for the first time with an X-ray astronomy satellite. The observation, performed with the ACIS-I and LETG/ACIS-S instruments on Chandra, yielded data of high spatial, spectral, and temporal resolution. Venus is clearly detected as a half-lit crescent, with considerable brightening on the sunward limb. The morphology agrees well with that expected from fluorescent scattering of solar X-rays in the planetary atmosphere. The radiation is observed at discrete energies, mainly at the O-K-alpha energy of 0.53 keV. Fluorescent radiation is also detected from C-K-alpha at 0.28 keV and, marginally, from N-K-alpha at 0.40 keV. An additional emission line is indicated at 0.29 keV, which might be the signature of the C 1s --> pi* transition in CO2 and CO. Evidence for temporal variability of the X-ray flux was found at the 2.6sigma level, with fluctuations by factors of a few times indicated on time scales of minutes. All these findings are fully consistent with fluorescent scattering of solar X-rays. No other source of X-ray emission was detected, in particular none from charge exchange interactions between highly charged heavy solar wind ions and atmospheric neutrals, the dominant process for the X-ray emission of comets. This is in agreement with the sensitivity of the observation. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, Cambridge, MA 02138 USA. RP Dennerl, K (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. RI Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Wolk, Scott/0000-0002-0826-9261 NR 33 TC 43 Z9 43 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 APR PY 2002 VL 386 IS 1 BP 319 EP 330 DI 10.1051/0004-6361:20020097 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543YU UT WOS:000175132100033 ER PT J AU Eichhorn, G AF Eichhorn, G TI Physics on ADS SO ASTRONOMY & GEOPHYSICS LA English DT News Item C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eichhorn, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 NR 0 TC 0 Z9 0 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1366-8781 J9 ASTRON GEOPHYS JI Astron. Geophys. PD APR PY 2002 VL 43 IS 2 BP 9 EP 9 PG 1 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA 538HR UT WOS:000174809900008 ER PT J AU Hamana, T Yoshida, N Suto, Y AF Hamana, T Yoshida, N Suto, Y TI Reliability of the dark matter clustering in cosmological N-body simulations on scales below the mean separation length of particles SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; dark matter; gravitation; large-scale structure of universe; methods : n-body simulations ID GALAXY FORMATION; ANALYTIC MODEL; FLUCTUATIONS; EVOLUTION; DENSITY; HALOS; BIAS; STATISTICS; PARAMETERS; UNIVERSE AB We critically examine the reliability of the dark matter clustering in high-resolution cosmological N-body simulations on scales below the mean separation length of particles. The particle discreteness effect imposes the two fundamental limitations on those scales: the lack of the initial fluctuation power and the finite mass resolution. We address this problem applying the dark halo approach and are able to discuss separately how those two limitations affect the dark matter clustering in N-body simulations at early epochs. We find that limitations of the dark matter clustering are primarily determined by the mass of particles. By a detailed comparison with three major cosmological simulations, we also find that in order to reproduce a proper amplitude of the dark matter clustering on small scales, halos with a characteristic nonlinear mass, M-NL(dz), defined by sigma(R)(M-NL; z) = 1, must be resolved in the simulation. This leads to a critical redshift z(crit) determined by M-NL(z(crit)) = halo m part, where n(halo) is the number of particles necessary to resolve the typical nonlinear mass halo (similar to10). We conclude that, at least as far as the two-point correlation functions are concerned, the dark matter clustering in high-resolution N-body simulations on scales below the mean particle separation is reliable down to the gravitational force resolution length only for z < z(crit), while it is strongly affected by the finite mass resolution for z > z(crit). C1 Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Max Planck Inst Astrophys, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. Univ Tokyo, Sch Sci, Res Ctr Early Universe RESCEU, Tokyo 1130033, Japan. RP Hamana, T (reprint author), Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. RI Yoshida, Naoki/A-4305-2011 NR 73 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 APR 1 PY 2002 VL 568 IS 2 BP 455 EP 462 DI 10.1086/338970 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 535BQ UT WOS:000174625700001 ER PT J AU Willner, SP Nelson-Patel, K AF Willner, SP Nelson-Patel, K TI Neon abundances in the HII regions of M33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : individual (M33); HII regions; infrared : galaxies ID H-II REGIONS; SPIRAL GALAXIES; THEORETICAL-MODELS; SOUTHERN GALAXIES; NEARBY GALAXIES; GRADIENTS; OXYGEN; EMISSION; NITROGEN; MORPHOLOGY AB We present neon abundances for 25 H II regions of M33, measured from line profiles of the mid-infrared transitions of [Ne II] and [Ne III] taken with the Infrared Space Observatory Short-Wavelength Spectrometer. The distribution of neon abundances as a function of galactocentric radius is best described as a step, -0.15 dex relative to the solar neon abundance from 0.7 to 4.0 kpc and -0.35 dex from 4.0 to 6.7 kpc, with estimated intrinsic scatter of 0.07 dex. The nearly at neon abundance distribution differs from the steep oxygen abundance gradient found by previous investigators. Unless the oxygen abundance determinations are wrong, the chemical evolution of the galaxy has been radially dependent. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Willner, SP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 59 TC 26 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 APR 1 PY 2002 VL 568 IS 2 BP 679 EP 688 DI 10.1086/339032 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 535BQ UT WOS:000174625700018 ER PT J AU Keto, E AF Keto, E TI An ionized accretion flow in the ultracompact HII region G10.6-0.4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; HII regions; stars : individual (G10.6-0.4) ID H-II REGIONS; MASSIVE STAR-FORMATION; LUMINOUS IRAS SOURCES; MOLECULAR CORES; DYNAMICAL COLLAPSE; DENSITY STRUCTURE; MAIN-SEQUENCE; B-STAR; EVOLUTION; DISKS AB Analysis of the H66alpha radio recombination line velocities in the ultracompact H II region G10.6-0.4 indicates inward motion of the ionized gas within the H II region. Comparison with the velocities of molecular lines from the surrounding neutral gas suggests that a molecular accretion flow passes through the ionization boundary of the H II region and continues inward as an ionized accretion flow. Interpreted in the context of a model for star formation in hot molecular cores, these observations indicate that G10.6-0.4 is at a stage of development just after the massive star or stars at the center of the accretion flow have first formed an ionized H II region within the hot molecular core. 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 73 TC 54 Z9 55 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2002 VL 568 IS 2 BP 754 EP 760 DI 10.1086/339056 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 535BQ UT WOS:000174625700024 ER PT J AU Orosz, JA Groot, PJ van der Klis, M McClintock, JE Garcia, MR Zhao, P Jain, RK Bailyn, CD Remillard, RA AF Orosz, JA Groot, PJ van der Klis, M McClintock, JE Garcia, MR Zhao, P Jain, RK Bailyn, CD Remillard, RA TI Dynamical evidence for a black hole in the microquasar XTE J1550-564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; black hole physics; stars : individual (XTE J1550-564); X-rays : binaries; X-rays : stars ID TRANSIENT GS 2023+338; X-RAY TRANSIENTS; GRO J1655-40; EVOLUTIONARY STATE; ORBITAL PARAMETERS; ACCRETION DISKS; MASS; SPECTROSCOPY; A0620-00; CYGNI AB Optical spectroscopic observations of the companion star ( type G8 IV to K4 III) in the microquasar system XTE J1550-564 reveal a radial velocity curve with a best-fitting spectroscopic period of P-sp = 1.552 +/- 0.010 days and a semiamplitude of K-2 = 349 +/- 12 km s(-1). The optical mass function is f(M) = 6.86 +/- 0.71 M-. (1sigma). We tentatively measure the rotational velocity of the companion star to be V-rot sin i = 90 +/- 10 km s(-1), which when taken at face value implies a mass ratio of Q = M-1/M-2 = 6.6(-1.6)(+2.5) (1 sigma),using the above value of K-2. We derive constraints on the binary parameters from simultaneous modeling of the ellipsoidal light and radial velocity curves. We find 1sigma ranges for the photometric period (1.5430 days less than or equal to P-ph less than or equal to 1.5440 days), K-velocity (350.2 less than or equal to K-2 less than or equal to 368.6 km s(-1)), inclination (67.degrees0 less than or equal to i less than or equal to 77.degrees4), mass ratio (Q greater than or equal to 12.0), and orbital separation (11.55 R-. less than or equal to a less than or equal to 12.50 R-.). Given these geometrical constraints, we find that the most likely value of the mass of the compact object is 9.41 M-. with a 1sigma range of 8.36 M-. less than or equal to M-1 less than or equal to 10.76 M-.. If we apply our tentative value of V-rot sin i = 90 +/- 10 km s(-1) as an additional constraint in the ellipsoidal modeling,we find 1sigma ranges of 1.5432 days less than or equal to P-ph less than or equal to 1.5441 days for the photometric period, 352.2 less than or equal to K-2 less than or equal to 370.1 km s(-1) for the K-velocity, 70.degrees8 less than or equal to i less than or equal to 75.degrees4 for the inclination, 6.7 less than or equal to Q less than or equal to 11.0 for the mass ratio, and 12.35 R-. less than or equal to a less than or equal to 13.22 R-. for the orbital separation. These geometrical constraints imply the most likely value of the mass of the compact object of 10.56 M-. with a 1sigma range of 9.68 M-. less than or equal to M-1 less than or equal to 11.58 M-.. In either case the mass of the compact object is well above the maximum mass of a stable neutron star, and we therefore conclude that XTE J1550-564 contains a black hole. C1 Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Natl Inst Nucl & High Energy Phys, Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Yale Univ, Dept Phys, New Haven, CT 06520 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Orosz, JA (reprint author), Univ Utrecht, Astron Inst, Postbus 80000, NL-3508 TA Utrecht, Netherlands. RI Groot, Paul/K-4391-2016 OI Groot, Paul/0000-0002-4488-726X NR 78 TC 164 Z9 165 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2002 VL 568 IS 2 BP 845 EP 861 DI 10.1086/338984 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 535BQ UT WOS:000174625700032 ER PT J AU Wachter, S Hoard, DW Bailyn, CD Corbel, S Kaaret, P AF Wachter, S Hoard, DW Bailyn, CD Corbel, S Kaaret, P TI A closer look at the soft X-ray transient X1608-52: Long-term optical and X-ray observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; stars : individual (QX Normae); stars : neutron; stars : variables : other; X-rays : binaries ID 4U-1608-52; EXTINCTION; BINARIES; NOVAE AB We report long-term simultaneous optical and (RXTE) X-ray observations of the soft X-ray transient and low-mass X-ray binary X1608-52 spanning from 1999 to 2001. In addition to the usual X-ray outburst and quiescent states, X1608-52 also exhibits an extended low-intensity state, during which the optical counterpart, QX Nor, is found to be about 2 mag brighter than during quiescence. We detect optical photometric variability on a possible period of 0.5370 days with a semiamplitude of similar to0.27 mag in the I band. The modulation could be orbital but is also consistent with a scenario invoking a superhump with decreasing period. We discuss the possibilities of distinguishing between the orbital- and superhump-period cases. Observations of QX Nor during quiescence indicate an F- to G-type main-sequence secondary, while theoretical considerations argue for an evolved mass donor. Only an evolved mass donor would satisfy the condition for the occurrence of superhumps. C1 Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Univ Paris 07, F-91191 Gif Sur Yvette, France. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wachter, S (reprint author), Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. OI Hoard, Donald W./0000-0002-6800-6519 NR 34 TC 32 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 APR 1 PY 2002 VL 568 IS 2 BP 901 EP 911 DI 10.1086/339034 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 535BQ UT WOS:000174625700035 ER PT J AU Reid, MJ Goldston, JE AF Reid, MJ Goldston, JE TI How Mira variables change visual light by a thousandfold SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular processes; stars : AGB and post-AGB; stars : atmospheres; stars : late-type; stars : variables : other ID CIRCUMSTELLAR DUST SHELLS; LONG-PERIOD VARIABLES; ATMOSPHERIC STRUCTURE; MODEL ATMOSPHERES; ANGULAR DIAMETER; R-LEONIS; STARS; PULSATION; MICRONS; TIO AB Mira variables change visual light by up to 8 mag over their roughly yearly cycle. Here we present a simple explanation for the extremely large amplitudes of light curves of oxygen-rich Mira variables. Metallic oxides, such as TiO, form throughout the stellar atmosphere as the star cools when approaching minimum light. When this happens, the visual light can be almost completely absorbed at large radii, extending the visual photosphere to nearly twice its nominal size. At these large radii, temperatures can fall to 1400 K and essentially all of the star's radiation emerges in the infrared. Since almost no optical light is emitted at these low temperatures, Mira variables can decrease their visual light by more than a thousandfold and almost disappear to the human eye. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 41 Z9 41 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2002 VL 568 IS 2 BP 931 EP 938 DI 10.1086/338947 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 535BQ UT WOS:000174625700037 ER PT J AU Calvet, N D'Alessio, P Hartmann, L Wilner, D Walsh, A Sitko, M AF Calvet, N D'Alessio, P Hartmann, L Wilner, D Walsh, A Sitko, M TI Evidence for a developing gap in a 10 Myr old protoplanetary disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars : formation; stars : pre main-sequence ID T-TAURI STARS; INTERSTELLAR SILICATE MINERALOGY; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; PROTOSTELLAR DISKS; HYDRAE ASSOCIATION; OPTICAL-CONSTANTS; GIANT PLANETS; SOLAR NEBULA AB We have developed a physically self-consistent model of the disk around the nearby 10 Myr old star TW Hya that matches the observed spectral energy distribution and 7 mm images of the disk. The model requires both significant dust-size evolution and a partially evacuated inner disk region, as predicted by theories of planet formation. The outer disk, which extends to at least 140 AU in radius, is very optically thick at infrared wavelengths and quite massive (similar to0.06 M-.) for the relatively advanced age of this T Tauri star. This implies long viscous and dust evolution timescales, although dust must have grown to sizes of the order of similar to1 cm to explain the submillimeter and millimeter spectral slopes. In contrast, the negligible near-infrared excess emission of this system requires that the disk be optically thin inside. 4 AU. This inner region cannot be completely evacuated; we need similar to0.5 lunar mass of similar to1 mum particles remaining to produce the observed 10 mum silicate emission. Our model requires a distinct transition in disk properties at 4 AU separating the inner and outer disks. The inner edge of the optically thick outer disk must be heated almost frontally by the star to account for the excess flux at mid-infrared wavelengths. We speculate that this truncation of the outer disk may be the signpost of a developing gap due to the effects of a growing protoplanet; the gap is still presumably evolving because material still resides in it, as indicated by the silicate emission, the molecular hydrogen emission, and the continued accretion onto the central star ( albeit at a much lower rate than typical of younger T Tauri stars). Thus, TW Hya may become the Rosetta stone for our understanding of the evolution and dissipation of protoplanetary disks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Autonomous Univ Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Amer Museum Nat Hist, New York, NY 10024 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. RP Calvet, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Walsh, Andrew/B-5627-2013 OI Walsh, Andrew/0000-0001-9506-0855 NR 65 TC 377 Z9 378 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 APR 1 PY 2002 VL 568 IS 2 BP 1008 EP 1016 DI 10.1086/339061 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 535BQ UT WOS:000174625700044 ER PT J AU Yusef-Zadeh, Y Law, C Wardle, M AF Yusef-Zadeh, Y Law, C Wardle, M TI The origin of X-ray emission from a Galactic center molecular cloud: Low-energy cosmic-ray electrons SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; Galaxy : center; ISM : abundances; X-rays : ISM ID CENTER ARC; CENTER REGION; RADIO; RIDGE; LINE AB The Galactic center region near l approximate to 0.degrees2 hosts a mixture of nonthermal linear filaments and thermal radio continuum features associated with the radio arc. Chandra observations of this region reveal an X- ray filament and diffuse emission with an extent of roughly 60" x 2" and 5' x 3', respectively. The X-ray filament lies at the edge of the nonthermal radio filaments and the dense molecular shell G0.13-0.13 that has an unusually high kinetic temperature greater than or equal to70 K. These observations demonstrate that the G0.13-0.13 molecular cloud and the nonthermal radio filaments of the arc are interacting. The diffuse X-ray emission is correlated with the molecular shell and is fitted either by two-temperature (1 and 10 keV) thermal emission or by power-law and 1 keV thermal gas. Fluorescent 6.4 keV line emission is also detected throughout the molecular shell. This cloud coincides within the error circle of a steady unidentified EGRET source, 3EG J1746-2851. We argue that low-energy cosmic-ray electrons produce the power-law continuum by bremsstrahlung and 6.4 keV line emission from the filament and the diffuse cloud with the implication on the origin of the Galactic ridge X-ray emission. The strong 6.4 keV Fe line emission seen from other Galactic center clouds could be produced in a similar fashion rather than via fluorescent emission induced by a transient hard X-ray source in the Galactic center. In addition, heating by ionization induced by low-energy cosmic-ray electrons are also responsible for the high temperature of G0.13-0.13. The gamma-ray source is a result of bremsstrahlung by the high-energy tail of the electron energy distribution. C1 Northwestern Univ, Dept Phys & Astron, Dearborn Observ, Evanston, IL 60208 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Special Res Ctr Theoret Astrophys, Sydney, NSW 2006, Australia. RP Yusef-Zadeh, Y (reprint author), Northwestern Univ, Dept Phys & Astron, Dearborn Observ, Room 9C,2145 Sheridan Rd, Evanston, IL 60208 USA. OI Wardle, Mark/0000-0002-1737-0871 NR 27 TC 59 Z9 59 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2002 VL 568 IS 2 BP L121 EP L125 DI 10.1086/340379 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 535BR UT WOS:000174625800013 ER PT J AU Giacconi, R Zirm, A Wang, JX Rosati, P Nonino, M Tozzi, P Gilli, R Mainieri, V Hasinger, G Kewley, L Bergeron, J Borgani, S Gilmozzi, R Grogin, N Koekemoer, A Schreier, E Zheng, W Norman, C AF Giacconi, R Zirm, A Wang, JX Rosati, P Nonino, M Tozzi, P Gilli, R Mainieri, V Hasinger, G Kewley, L Bergeron, J Borgani, S Gilmozzi, R Grogin, N Koekemoer, A Schreier, E Zheng, W Norman, C TI Chandra Deep Field South: The 1 Ms catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies : active; galaxies : high-redshift; X-rays : diffuse background; X-rays : galaxies ID X-RAY SOURCES; N-LOG S; LOCKMAN FIELD; SKY AB In this paper we present the source catalog obtained from a 942 ks exposure of the Chandra Deep Field South (CDFS), using the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-ray Observatory. Eleven individual pointings made between 1999 October and 2000 December were combined to generate the final image used for object detection. Catalog generation proceeded simultaneously using two different methods; a method of our own design using a modified version of the SExtractor algorithm, and a wavelet transform technique developed specifically for Chandra observations. The detection threshold has been set in order to have less than 10 spurious sources, as assessed by extensive simulations. We subdivided the catalog into four sections. The primary list consists of objects common to the two detection methods. Two secondary lists contain sources which were detected by ( 1) the SExtractor algorithm alone and ( 2) the wavelet technique alone. The fourth list consists of possible diffuse or extended sources. The flux limits at the aimpoint for the soft (0.5-2 keV) and hard (2-10 keV) bands are 5.5 x 10(-17) erg s(-1) cm(-2) and 4.5 x 10(-16) erg s(-1) cm(-2), respectively. The total number of sources is 346; out of them, 307 were detected in the 0.5-2 keV band, and 251 in the 2 10 keV band. We also present optical identifications for the cataloged sources. Our primary optical data are R band imaging from VLT/FORS1 to a depth of R similar to 26.5 (Vega). In regions of the field not covered by the VLT/ FORS1 deep imaging, we use R-band data obtained with the Wide Field Imager (WFI) on the ESO-MPI 2.2 m telescope, as part of the ESO Imaging Survey ( EIS), which cover the entire X-ray survey. We found that the FORS1/Chandra offsets are small, similar to1". Coordinate cross-correlation finds 85% of the Chandra sources covered by FORS1 R to have counterparts within the 3 error box (greater than or similar to1."5 depending on off-axis angle and Xray signal-to-noise). The unidentified fraction of sources, approximately similar to10%15%, is close to the limit expected from the observed X-ray flux to R-band ratio distribution for the identified sample. C1 Johns Hopkins Univ, Baltimore, MD 21218 USA. Associated Univ Inc, Washington, DC 20036 USA. European So Observ, D-85748 Garching, Germany. Osserv Astron Trieste, I-34131 Trieste, Italy. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Univ Studi Roma Tre, Dipartimento Fis E Amaldi, I-00146 Rome, Italy. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Trieste, Dipartimento Astron, Ist Nazl Fis Nucl, I-34131 Trieste, Italy. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Giacconi, R (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA. RI Gilli, Roberto/P-1110-2015; OI Gilli, Roberto/0000-0001-8121-6177; Nonino, Mario/0000-0001-6342-9662; Borgani, Stefano/0000-0001-6151-6439; Koekemoer, Anton/0000-0002-6610-2048 NR 30 TC 478 Z9 480 U1 0 U2 6 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 APR PY 2002 VL 139 IS 2 BP 369 EP 410 DI 10.1086/338927 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 533KB UT WOS:000174527600002 ER PT J AU Isler, ML Alonso, JA Isler, PR Valqui, T Begazo, A Whitney, BM AF Isler, ML Alonso, JA Isler, PR Valqui, T Begazo, A Whitney, BM TI Rediscovery of a cryptic species and description of a new subspecies in the Myrmeciza hemimelaena complex (Thamnophilidae) of the neotropics SO AUK LA English DT Article ID ANTBIRDS PASSERIFORMES; HERPSILOCHMUS; PERU; FORMICARIIDAE; BRAZIL; LIMITS; AVES AB The recording in 1992 of an unknown antbird loudsong initiated a journey of discovery that led to the resolution of the conflict between John Zimmer (1932) and Melvin Carriker (1934) regarding the taxonomic standing of the population of Myrmeciza hemimelaena, a widespread southern Amazonian antbird, that occurs in lower Andean elevations in San Martin, Peru. Zimmer had described a new subspecies, M. h. castanea, from the Moyobamba Valley, but Carriker, on the basis of specimens he collected at the same elevation in an adjoining valley, could not find morphological differences between his specimens and the widespread nominate form of M. hemimelaena. Both authors were correct. Two cryptic sister taxa coexist in the foothills of San Martin. Diagnostic vocal and morphological characters and syntopy confirm their status as distinct species. Myrmeciza hemimelaena castanea Zimmer is revived and raised to species status. Concurrently, analysis of the vocalizations and morphology of the lowland population north of the Rio Maranon in Peru, the loudsong recording of which initiated the project, revealed that this population was closely related to M. castanea of which it is described as a subspecies, M. c. centunculorum, under the biological species concept. The discovery that there are two cryptic species in the Myrmeciza hemimelaena complex exemplifies the continuing need to pursue field knowledge and analysis of avian species limits in the Neotropics required for the development of conservation strategies as well as phylogenetic understanding. Received 17 April 2001, accepted 7 December 2001. C1 Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. Inst Invest Amazonia Peruana, Iquitos, Peru. Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. RP Isler, ML (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. EM piantbird@ao.com NR 29 TC 16 Z9 17 U1 1 U2 5 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD APR PY 2002 VL 119 IS 2 BP 362 EP 378 DI 10.1642/0004-8038(2002)119[0362:ROACSA]2.0.CO;2 PG 17 WC Ornithology SC Zoology GA 553ZZ UT WOS:000175709400006 ER PT J AU McCartney, MA Lessios, HA AF McCartney, MA Lessios, HA TI Quantitative analysis of gametic incompatibility between closely related species of neotropical sea urchins SO BIOLOGICAL BULLETIN LA English DT Article ID REPRODUCTIVE ISOLATION; GENUS ECHINOMETRA; MONTASTRAEA-ANNULARIS; GENETIC-DIVERGENCE; MITOCHONDRIAL-DNA; MARINE SPECIATION; SEXUAL SELECTION; 2 SIDES; EVOLUTION; PANAMA AB Species of the sea urchin genus Echinometra found on the two coasts of Panama are recently diverged and only partially isolated by incomplete barriers to interspecific fertilization. This study confirms previous work that revealed incompatibility between the eggs of the Atlantic E. lucunter and the sperm of the other two neotropical species, whereas eggs of its sympatric congener E. viridis and allopatric E. vanbrunti are largely compatible with heterospecific sperm. Here we quantify fertilization using a range of sperm dilutions. We demonstrate a much stronger block to cross-species fertilization of E. lucunter eggs than was previously shown at fixed sperm concentrations, and mild incompatibility of the other two species' eggs where previous crosses between species were not distinguishable from within-species controls. Additionally, we present evidence for intraspecific variation in egg receptivity towards heterospecific sperm. Our findings here again discount the "reinforcement model" as a viable explanation for the pattern of prezygotic isolation. Gamete incompatibility in these Echinometra has appeared recently-within the last 1.5 million years-but is weaker in sympatry than in allopatry. Accidents of history may help explain why incompatibility of eggs emerged in one species and not in others. Compensatory sexual selection on sperm in this species could follow, and promote divergence of proteins mediating sperm-egg recognition. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP McCartney, MA (reprint author), Univ N Carolina, Dept Biol Sci, 5600 Marvin Moss Lane, Wilmington, NC 28409 USA. NR 64 TC 51 Z9 54 U1 2 U2 10 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 J9 BIOL BULL JI Biol. Bull. PD APR PY 2002 VL 202 IS 2 BP 166 EP 181 DI 10.2307/1543653 PG 16 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 547ZE UT WOS:000175362400008 PM 11971812 ER PT J AU Svenning, JC AF Svenning, JC TI A review of natural vegetation openness in north-western Europe SO BIOLOGICAL CONSERVATION LA English DT Review DE fire grazing; nature conservation; temperate forest; quaternary interglacials ID PLEISTOCENE INTERGLACIAL DEPOSITS; LAST 3000 YEARS; POLLEN DATA; VERTEBRATE FAUNA; EASTERN ENGLAND; LITTLE-OAKLEY; SUSERUP SKOV; ICE-AGE; HISTORY; FOREST AB Secondary succession is threatening many species of open habitats in north-western Europe. This problem has caused an intense debate over whether the present-natural vegetation in this region would be closed forest or more open vegetation. Native large herbivores have been proposed as the key agents creating such open vegetation. Here I address this question by reviewing the palaeoecological evidence regarding vegetation openness in past oceanic interglacials and the pre-agricultural Holocene, i.e. before the onset of strong human impact. I conclude that closed forest would predominate, but include localized longer-lasting openings. Further, open vegetation would be frequent on floodplains, infertile soils, chalklands, and in continental and submeditteranean areas. Large herbivores and fire emerge as likely potential key factors in creating open vegetation in north-western Europe. Fire would probably also be important in the maintenance of light-demanding or short-statured woody species within closed upland forests. (C) 2002 Elsevier Science Ltd. All rights reserved. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Svenning, JC (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. RI Svenning, Jens-Christian/C-8977-2012 OI Svenning, Jens-Christian/0000-0002-3415-0862 NR 165 TC 180 Z9 190 U1 5 U2 82 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD APR PY 2002 VL 104 IS 2 BP 133 EP 148 AR PII S0006-3207(01)00162-8 DI 10.1016/S0006-3207(01)00162-8 PG 16 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 533ZA UT WOS:000174559100001 ER PT J AU Acevedo-Rodriguez, P Ferrucci, MS AF Acevedo-Rodriguez, P Ferrucci, MS TI Averrhoidium dalyi (Sapindaceae): a new species from western Amazonia SO BRITTONIA LA English DT Article DE Sapindaceae; Averrhoidium; Acre; Brazil; Madre de dios; Peru AB The present paper describes and illustrates the new species Averrhoidium dalyi and provides a key to the species of Averrhoidium. The new species is known from lowland, terra firme forest in the Purus River basin, in Acre, Brazil, and from Manu National Park in Madre de Dios, Peru. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Bot, Washington, DC 20560 USA. RP Acevedo-Rodriguez, P (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Bot, MRC-166, Washington, DC 20560 USA. NR 3 TC 3 Z9 3 U1 1 U2 2 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD APR-JUN PY 2002 VL 54 IS 2 BP 112 EP 115 DI 10.1663/0007-196X(2002)054[0112:ADSANS]2.0.CO;2 PG 4 WC Plant Sciences SC Plant Sciences GA 578HU UT WOS:000177112000007 ER PT J AU Sioris, CE Evans, WFJ Gattinger, RL McDade, IC Degenstein, DA Llewellyn, EJ AF Sioris, CE Evans, WFJ Gattinger, RL McDade, IC Degenstein, DA Llewellyn, EJ TI Ground-based Ring-effect measurements with the OSIRIS development model SO CANADIAN JOURNAL OF PHYSICS LA English DT Article ID ROTATIONAL RAMAN-SCATTERING; RAYLEIGH-SCATTERING; SKY; SPECTRUM; IMPACT AB The Ring effect is measured using the UV-visible spectrometer (similar to1 nm spectral resolution) of OSIRIS, the optical spectrograph and infrared imaging system. The observed filling in of Ca(II) H and K (similar to395 nm), the two largest Fraunhofer lines in the solar spectrum, are compared with the filling in simulated with a new model that includes rotational Raman scattering (RRS) by N-2 and O-2. The filling in is (1.06 +/- 0.60)% at Ca(II) K and (1.40 +/- 0.50)%, at Ca(II) H for blue-sky observations at a solar zenith angle of 37degrees. The measured filling in agrees with the modelled filling in within the uncertainties. C1 York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 1P3, Canada. Trent Univ, Dept Phys, Peterborough, ON K9J 7B8, Canada. Canadian Space Agcy, Ottawa, ON K1A 0R6, Canada. York Univ, Dept Earth & Atmospher Sci, Toronto, ON M3J 1P3, Canada. Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK S7N 5E2, Canada. RP Sioris, CE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Sioris, Christopher/0000-0003-1168-8755 NR 19 TC 10 Z9 10 U1 0 U2 0 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD APR PY 2002 VL 80 IS 4 BP 483 EP 491 DI 10.1139/P01-155 PG 9 WC Physics, Multidisciplinary SC Physics GA 567TF UT WOS:000176500700013 ER PT J AU Taylor, SS Leonard, ML Boness, DJ Majluf, P AF Taylor, SS Leonard, ML Boness, DJ Majluf, P TI Foraging by Humboldt penguins (Spheniscus humboldti) during the chick-rearing period: general patterns, sex differences, and recommendations to reduce incidental catches in fishing nets SO CANADIAN JOURNAL OF ZOOLOGY LA English DT Article ID DIVING BEHAVIOR; PYGOSCELIS-PAPUA; MACQUARIE ISLAND; ADELIE PENGUINS; PELAGIC SEABIRD; GENTOO; LONG; SEAL; CONSERVATION; PERFORMANCE AB We studied the foraging behaviour of endangered Humboldt penguins (Spheniscus humboldti) to examine general foraging patterns, sex differences in foraging behaviour, and the reasons for incidental catches in fishing nets. Humboldt penguins foraged diurnally and typically made short, shallow dives within 30 m of the surface. Males and females made overnight (lasting 25.8 +/- 3.4 h; mean +/- SD) and day (10.4 +/- 2.0 h) trips when they departed the colony to forage. Overnight trips were more common (68.2% of all trips) and were associated with a significantly greater amount of foraging time. Males dived to greater maximum depths than females but did not differ in other diving parameters, including foraging time, foraging effort, and proportions of day and overnight trips made. Adults may maintain their body condition during chick rearing by making a mixture of overnight and day trips. The two foraging periods observed during overnight trips may function to feed both the adults and the chicks, whereas the single period observed during day trips may function to accommodate the rate of provisioning required by the chicks. We suggest that both males and females would be protected from incidental catches in fishing nets if commercial fisheries avoided setting surface nets at night and setting nets between 0 and 30 m depth during the day in areas where penguins forage and transit. C1 Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. Smithsonian Inst, Conservat & Resource Ctr, Washington, DC 20008 USA. Wildlife Conservat Soc Peru, Lima 17, Peru. RP Leonard, ML (reprint author), Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. EM mleonard@is.dal.ca NR 52 TC 16 Z9 17 U1 6 U2 13 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0008-4301 EI 1480-3283 J9 CAN J ZOOL JI Can. J. Zool. PD APR PY 2002 VL 80 IS 4 BP 700 EP 707 DI 10.1139/Z02-046 PG 8 WC Zoology SC Zoology GA 549DL UT WOS:000175429200010 ER PT J AU Kursar, TA Grauel, W AF Kursar, TA Grauel, W TI Logging from rivers may control human invasions SO CONSERVATION BIOLOGY LA English DT Letter ID TROPICAL FORESTS C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Panama City, Panama. Univ Florida, Coll Nat Resources & Environm, Gainesville, FL 32611 USA. RP Kursar, TA (reprint author), Univ Utah, Dept Biol, 257 S 1400 E, Salt Lake City, UT 84112 USA. NR 4 TC 2 Z9 3 U1 0 U2 0 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD APR PY 2002 VL 16 IS 2 BP 285 EP 285 DI 10.1046/j.1523-1739.2002.00204.x PG 1 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 537GP UT WOS:000174750800002 ER PT J AU Pandolfi, JM AF Pandolfi, JM TI Coral community dynamics at multiple scales SO CORAL REEFS LA English DT Article DE coral; pleistocene; ecological dynamics; community ecology ID PAPUA-NEW-GUINEA; PATCH REEFS; NETHERLANDS-ANTILLES; SPECIES RICHNESS; TEMPORAL VARIABILITY; DEATH ASSEMBLAGES; FISH COMMUNITIES; HIGH DIVERSITY; STABLE STATES; PHASE-SHIFTS AB Our understanding of ecosystem dynamics is directly linked to the scale at which we make our ecological observations. The ecological dynamics of Pleistocene coral communities varies with spatial and temporal scale of study. Reef coral communities studied over small spatial and temporal scales show ecological chaos where disturbance prevents ecological equilibrium, and those studied at the largest biogeographic scales show large differences due to history, chance, dispersion, and regional-scale processes. However, communities that are located within tens of kilometers of one another appear to show a large degree of order.. probably due to underlying principles of niche similarity. Similarly, temporal studies conducted over large temporal scales show persistence in coral community structure through tens of thousands of years. The history of Caribbean reef coral communities shows that this persistence has been recently interrupted by massive degradation of coral reef habitats. Whether such habitat reduction and change in species composition are unprecedented and due to the acceleration of human consumption and pollution, or whether they represent a short-term fluctuation in an otherwise predictable community structure, is one of the most important questions facing reef managers today. Investigations of coral community structure at different spatial scales illuminate the dependence of ecological dynamics on spatial scale, and at different temporal scales show that present trends are not predicted from history but may well be related to human-induced environmental modification. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC-121, Washington, DC 20560 USA. EM pandolfi.john@nmnh.si.edu RI Pandolfi, John/A-3121-2009 OI Pandolfi, John/0000-0003-3047-6694 NR 97 TC 75 Z9 83 U1 2 U2 27 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 APR PY 2002 VL 21 IS 1 BP 13 EP 23 DI 10.1007/s00338-001-0204-7 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 552FG UT WOS:000175608200004 ER PT J AU Harnal, VK Wildt, DE Bird, DM Monfort, SL Ballou, JD AF Harnal, VK Wildt, DE Bird, DM Monfort, SL Ballou, JD TI Computer simulations to determine the efficacy of different genome resource banking strategies for maintaining genetic diversity SO CRYOBIOLOGY LA English DT Article DE genome resource banks (GRBs); endangered species; genetic diversity; inbreeding; Przewalski's horse; Eld's deer; Sumatran tiger ID CONSERVATION AB Genome resource banks (GRBs) and assisted reproductive techniques are increasingly recognized as useful tools for the management and conservation of biodiversity, including endangered species. Cryotechnology permits long-term storage of valuable genetic material. Although the actual application to endangered species management requires technical knowledge about sperm freezing and thawing, a systematic understanding of the quantitative impacts of various germ plasm storage and use scenarios is also mandatory. In this study, various GRB strategies were analyzed using the historical data from three managed populations of endangered species with varied pedigrees (Eld's deer, Przewalski's horse, and Sumatran tiger). The following types of sperm banks were assessed: (1) a "Wild Bank" consisting of sperm (i.e., genes) from 5 to 10 males unrelated to the managed population and to each other; and (2) a "Best Male" bank containing sperm from only the most genetically valuable males alive in the ex situ population at the time the bank was established. These different bank types were then used to evaluate the effectiveness of different bank usage frequencies. The efficiency of each scenario was assessed by examining the level of inbreeding and gene diversity in the population. Overall, a sperm usage frequency of five times per year was determined to be the most efficient and "wild banks" were highly successful at enhancing genetic diversity. The value of a GRB established from the ex situ population depends on how closely related the banked males are to future generations. A GRB will have significantly less benefit when banked males also produce many successful offspring, or when donors are already genetically over-represented in the population at the time of establishing the GRB. (C) 2002 Elsevier Science (USA). All rights reserved. C1 Smithsonian Inst, Conservat & Res Ctr, Smithsonian Natl Zool Pk, Front Royal, VA 22630 USA. McGill Univ, Avian Sci & Conservat Ctr, Ste Anne De Bellevue, PQ H9W 3W3, Canada. RP Harnal, VK (reprint author), Smithsonian Inst, Conservat & Res Ctr, Smithsonian Natl Zool Pk, Front Royal, VA 22630 USA. NR 24 TC 19 Z9 20 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 J9 CRYOBIOLOGY JI Cryobiology PD APR PY 2002 VL 44 IS 2 BP 122 EP 131 AR PII S0011-2240(02)00013-5 DI 10.1016/S0011-2240(02)00013-5 PG 10 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 584KC UT WOS:000177464900004 PM 12151267 ER PT J AU Phillips, OL Malhi, Y Vinceti, B Baker, T Lewis, SL Higuchi, N Laurance, WF Vargas, PN Martinez, RV Laurance, S Ferreira, LV Stern, M Brown, S Grace, J AF Phillips, OL Malhi, Y Vinceti, B Baker, T Lewis, SL Higuchi, N Laurance, WF Vargas, PN Martinez, RV Laurance, S Ferreira, LV Stern, M Brown, S Grace, J TI Changes in growth of tropical forests: Evaluating potential biases SO ECOLOGICAL APPLICATIONS LA English DT Article DE Amazon rain forest; basal area; bias, evaluating; buttresses; carbon sink; climate change, global; forest plot data; forest-plot-based estimates of biomass; Neotropics; tree growth; tropical forests; changing dynamics ID RAIN-FOREST; SECONDARY FORESTS; SPECIES RICHNESS; CARBON-DIOXIDE; TREE; DYNAMICS; TURNOVER; CO2; AMAZONIA; CYCLE AB Over the past century almost every ecosystem on Earth has come under the influence of changes in atmospheric composition and climate caused by human activity, Tropical forests are among the most productive and extensive ecosystems, and it has been hypothesized that both the dynamics and biomass of apparently undisturbed, old-growth tropical forests have been changing in response to atmospheric changes. Long-term forest sample plots are a critical tool in detecting and monitoring such changes, and our recent analysis of pan-tropical-forest plot data has suggested that the biomass of tropical forests has been increaing. providing a modest negative feedback on the rate of accumulation of atmospheric CO2. However it has been argued that some of these old forest plot data sets have significant problems in interpretation because of the use of nonstandardized methodologies. In this paper we examine the extent to which potential field methodological errors may bias estimates of total biomass change by detailed examination of tree-by-tree records from up to 120 Neotropical plots to test prediction,; from theory. Potential positive biases on measurements of biomass change include a bias in site selection, tree deformities introduced by the measurement process. poor methodologies to deal with tree deformities or buttresses, and nonrecording of negative growth increments. We show that, while it is important to improve and standardize methodologies in current and future forest-plot work, any systematic errors introduced by currently identified biases in past studies are small and calculable. We conclude that most tropical-forest plot data are of useful quality, and that the evidence does still weigh conclusively in favor of a recent increase of biomass in old-growth tropical forests. C1 Univ Leeds, Sch Geog, Ctr Biodivers & Conservat, Leeds LS2 9JT, W Yorkshire, England. Univ Edinburgh, Inst Ecol & Resource Management, Edinburgh, Midlothian, Scotland. Inst Nacl Pesquisas, Dept Silvicultura Trop, Manaus, Amazonas, Brazil. Natl Inst Amazonian Res, INPA, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. Univ Nacl San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. Proyecto Flora Peru, Jardin Bot Missouri, Jaen, Cajamarca, Peru. New York Bot Garden, New York, NY USA. Winrock Int Livestock Res & Training Ctr, Corvallis, OR USA. RP Phillips, OL (reprint author), Univ Leeds, Sch Geog, Ctr Biodivers & Conservat, Leeds LS2 9JT, W Yorkshire, England. RI Laurance, William/B-2709-2012; Phillips, Oliver/A-1523-2011; Laurance, Susan/G-6021-2011; OI Phillips, Oliver/0000-0002-8993-6168; Laurance, Susan/0000-0002-2831-2933; Lewis, Simon/0000-0002-8066-6851 NR 49 TC 106 Z9 113 U1 3 U2 33 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 APR PY 2002 VL 12 IS 2 BP 576 EP 587 DI 10.1890/1051-0761(2002)012[0576:CIGOTF]2.0.CO;2 PG 12 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 532EC UT WOS:000174457800022 ER PT J AU McKee, KL Feller, IC Popp, M Wanek, W AF McKee, KL Feller, IC Popp, M Wanek, W TI Mangrove isotopic (delta N-15 and delta C-13) fractionation across a nitrogen vs. phosphorus limitation gradient SO ECOLOGY LA English DT Article DE carbon isotope discrimination; height forms; mangrove, red; nitrogen isotope discrimination; nutrient limitation; Rhizophora mangle; stress tolerance ID RHIZOPHORA-MANGLE L; RED MANGROVE; SPARTINA-ALTERNIFLORA; NUTRIENT ENRICHMENT; METROSIDEROS-POLYMORPHA; CARBON; GROWTH; SALINITY; FOREST; DISCRIMINATION AB Mangrove islands in Belize are characterized by a unique switching from nitrogen (N) to phosphorus (P) limitation to tree growth from shoreline to interior. Fertilization has previously shown that Rhizophora mangle (red mangrove) fringe trees (5-6 m tall) growing along the shoreline are N limited; dwarf trees (less than or equal to 1.5 m tall) in the forest interior are P limited; and transition trees (2-4 m tall) are co-limited by both N and P. Growth patterns paralleled a landward decrease in soil flushing by tides and an increase in bioavailable N, but P availability remained consistently low across the gradient. Stable isotopic composition was measured in R. mangle leaves to aid in explaining this nutrient switching pattern and growth variation. Along control transects, leaf delta(15)N decreased from +0.10parts per thousand (fringe) to -5.38parts per thousand (dwarf). The delta(15)N of N-fertilized trees also varied spatially, but the values were consistently more negative (by similar to3parts per thousand) compared to control trees. Spatial variation in 815 N values disappeared when the trees were fertilized with P and values averaged +0.12parts per thousand, similar to that in control fringe trees. Neither variation in source inputs nor microbial fractionation could fully account for the observed patterns in delta(15)N. The results instead suggest that the lower delta(15)N values in transition and dwarf control trees were due to plant fractionation as a consequence of slower growth and lower N demand. P fertilization increased N demand and decreased fractionation. Although leaf delta(13)C was unaffected by fertilization, values increased from fringe (-28.6parts per thousand) to transition (-27.9parts per thousand) to dwarf (-26.4parts per thousand) zones, indicating spatial variation in environmental stresses affecting stomatal conductance or carboxylation. The results thus suggest an interaction of external supply, internal demand, and plant ability to acquire nutrients under different hydro-edaphic conditions that vary across this tree-height gradient. The findings not only aid in understanding mangrove discrimination of nitrogen and carbon isotopes, but also have implications for identifying nutrient loading and other stress conditions in coastal systems dominated by mangroves. C1 US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Vienna, Inst Plant Physiol, Vienna, Austria. RP McKee, KL (reprint author), US Geol Survey, Natl Wetlands Res Ctr, 700 Cajundome Blvd, Lafayette, LA 70506 USA. RI Wanek, Wolfgang/E-7001-2012; Popp, Marianne/E-7559-2012; McKee, Karen/D-1365-2014 OI Wanek, Wolfgang/0000-0003-2178-8258; McKee, Karen/0000-0001-7042-670X NR 51 TC 141 Z9 149 U1 5 U2 45 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 APR PY 2002 VL 83 IS 4 BP 1065 EP 1075 DI 10.2307/3071914 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 533HP UT WOS:000174523800018 ER PT J AU Sorensen, LL Coddington, JA Scharff, N AF Sorensen, LL Coddington, JA Scharff, N TI Inventorying and estimating subcanopy spider diversity using semiquantitative sampling methods in an Afromontane forest SO ENVIRONMENTAL ENTOMOLOGY LA English DT Article DE montane forest spiders; sampling methods; sampling intensity; species richness estimation ID SPECIES RICHNESS; POPULATION-SIZE; EXTRAPOLATION; BIODIVERSITY; PERFORMANCE; COMMUNITIES AB We investigated the effect of plot-based and unrestricted (plot-less) sampling on an inventory of a megadiverse taxon, spiders, in an Afrotropical forest for the purpose of species richness estimates. We also investigated the efficiency of human-based sampling methods and the effect of allocation of sampling effort to different sampling methods to cover as many microhabitats as possible. In the 10-d sampling period in the montane forest of the Uzungwa Scarp Forest Reserve in Tanzania, eight collectors sampled spiders for 350 h and 800 pitfall "trap-days." Two hundred hours of sampling were restricted to a 1-ha plot and 150 It of sampling took place outside the plot. The sampling team included both experienced and inexperienced collectors using five different hand collecting methods during day and night sampling periods. Sampling yielded 9,096 adult spiders representing 170 species in total. Number of species and adult spiders per sample and overall species composition depended mainly on the sampling methods used and time of day. Whether the sampling took place within or at random outside the plot did not affect species composition or number of species per sample. Collector experience did affect the number of species collected per hour and thereby overall species composition of the sample but was less important than sampling methods used and time of day. C1 Univ Copenhagen, Museum Zool, DK-2100 Copenhagen, Denmark. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Sorensen, LL (reprint author), Univ Copenhagen, Museum Zool, Univ Pk 15, DK-2100 Copenhagen, Denmark. EM llsorensen@zmuc.ku.dk; coddington@jon.nmnh.si.edu; nscharff@zmuc.ku.dk RI Scharff, Nikolaj/A-4787-2013 OI Scharff, Nikolaj/0000-0001-6809-2878 NR 30 TC 85 Z9 94 U1 0 U2 19 PU ENTOMOLOGICAL SOC AMER PI LANHAM PA 10001 DEREKWOOD LANE, STE 100, LANHAM, MD 20706-4876 USA SN 0046-225X EI 1938-2936 J9 ENVIRON ENTOMOL JI Environ. Entomol. PD APR PY 2002 VL 31 IS 2 BP 319 EP 330 DI 10.1603/0046-225X-31.2.319 PG 12 WC Entomology SC Entomology GA 599GN UT WOS:000178325900017 ER PT J AU Neubauer, SC Anderson, IC Constantine, JA Kuehl, SA AF Neubauer, SC Anderson, IC Constantine, JA Kuehl, SA TI Sediment deposition and accretion in a mid-Atlantic (USA) tidal freshwater marsh SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE sedimentation; accretion; respiration; beryllium-7; cesium-137; carbon-14; tidal freshwater marsh; Virginia ID SEA-LEVEL RISE; WATER MARSH; SALT-MARSH; VERTICAL ACCRETION; TEMPORAL CHANGES; NORTH-CAROLINA; RATES; RIVER; ACCUMULATION; ESTUARINE AB Sediment deposition and accretion rates in a Virginia tidal freshwater marsh were measured to provide insight to the processes and time scales that are important for maintaining marsh surface elevation. Short-term sediment deposition rates (biweekly to monthly) measured using sediment collection tiles were spatially and temporally variable. Rates were greatest near a tidal creak and decreased along a transect extending toward the marsh interior. When integrated across the entire marsh, annual sediment deposition (as organic carbon) averaged 517 +/- 353 g C m(-2) y(-1) and was sufficient to balance the effects of existing relative sea level rise and marsh respiration rates. At the creekbank, the highest deposition rates were measured during summer although rates were relatively constant over time at the interior sites. Similar spatial and temporal patterns were obtained when deposition rates were calculated from Be-7 inventories (monthly time scale). Sediment inventories of Be-7 were greater than those supported atmospherically, indicating that the spatial patterns of sedimentation were not due to sediment erosion and redistribution within the marsh. Accretion rates calculated from Cs-137 (decadal scale) and C-14 dating (centuries to millennia) were substantially less than annual deposition rates, with a decrease in accretion rate with increasing time scale. Mineralization rates of recently deposited sediments (measured as O-2 consumption) indicated that sediment metabolism could potentially remove similar to30% of recently deposited carbon within one month of deposition. The metabolism of a labile sediment fraction could explain a portion of the observed decrease in accretion rate with increasing time scale, with the remainder due to periodic storm-induced erosion and historical variability in sediment deposition rates. (C) 2002 Elsevier Science Ltd. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. Coll William & Mary, Dept Geol, Williamsburg, VA 23187 USA. RP Neubauer, SC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Constantine, Jose/D-3479-2009; Neubauer, Scott/A-3443-2011 OI Neubauer, Scott/0000-0001-8948-2832 NR 56 TC 52 Z9 54 U1 1 U2 28 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0272-7714 J9 ESTUAR COAST SHELF S JI Estuar. Coast. Shelf Sci. PD APR PY 2002 VL 54 IS 4 BP 713 EP 727 DI 10.1006/ecss.2001.0854 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 575LL UT WOS:000176947700006 ER PT J AU Velez, MJ Jennions, MD Telford, SR AF Velez, MJ Jennions, MD Telford, SR TI The effect of an experimental brood reduction on male desertion in the Panamanian blue acara Cichlid Aequidens coeruleopunctatus SO ETHOLOGY LA English DT Article ID PARENTAL CARE; MATE DESERTION; FISH; EVOLUTION AB Investment in present vs. future reproduction is a life-history trade-off faced by many animals. Because males generally pay a higher cost from lost mating opportunities than females, males are expected to react more strongly to changes in brood value. We examined the effect of an experimental brood reduction on male desertion in the substrate-brooding biparental cichlid Aequidens coeruleo-punctatus under field conditions. We tested the prediction that brood reduction should decrease the duration of male care and examined the effect of brood reduction on the quality of male and female parental care. Our results show that males with reduced broods stopped providing parental care earlier than males with control broods. Males with reduced broods, however, also stayed longer with their broods as the season progressed. Brood reduction did not decrease daily investment in male or female parental care. We conclude that males trade off present and future reproduction by changing the duration but not the quality of parental care. The longer duration of male care in the experimental group later in the season suggests that the trade-off between present and future reproduction changes as the season progresses because the payoffs of desertion progressively decrease. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Florida, Dept Zool, Gainesville, FL 32611 USA. RP Velez, MJ (reprint author), Univ Florida, Dept Zool, POB 118525, Gainesville, FL 32611 USA. RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 20 TC 9 Z9 9 U1 0 U2 4 PU BLACKWELL VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0179-1613 J9 ETHOLOGY JI Ethology PD APR PY 2002 VL 108 IS 4 BP 331 EP 340 DI 10.1046/j.1439-0310.2002.00772.x PG 10 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 544FN UT WOS:000175147700004 ER PT J AU Dasmahapatra, KK Blum, MJ Aiello, A Hackwell, S Davies, N Bermingham, EP Mallett, T AF Dasmahapatra, KK Blum, MJ Aiello, A Hackwell, S Davies, N Bermingham, EP Mallett, T TI Inferences from a rapidly moving hybrid zone SO EVOLUTION LA English DT Article DE Anartia; concordant clines; cytonuclear disequilibrium; linkage disequilibrium; moving hybrid zones; shifting balance; speciation ID FIRE-BELLIED TOADS; MITOCHONDRIAL-DNA; GENE FLOW; LINKAGE DISEQUILIBRIUM; BOMBINA-BOMBINA; SPECIATION; SELECTION; HYBRIDIZATION; DIFFERENTIATION; POLYMORPHISM AB Anartia fatima and Anartia amathea (Lepidoptera: Nymphalidae) are sister taxa whose ranges abut in a narrow hybrid zone in eastern Panama. At the center of the zone, hybrids are abundant, although deviations from Hardy-Weinberg and linkage disequilibria are strong, due in part to assortative mating. We measured differences across the zone in four wing color-pattern characters, three allozyme loci, and mitochondrial haplotype. Wing pattern, allozyme, and mitochondrial clines were coincident (i.e., had the same positions) and concordant (i.e., all markers had similar cline shapes, about 28 km wide). Repeated samples demonstrated that the hybrid zone has been moving eastwards at an average rate of 2.5 km/year over the past 20 years, accompanied by an equivalent movement of the mtDNA cline. No introgression of mtDNA haplotypes were found in the "wake" of the moving cline, as might be expected for a neutral marker. The concordance of morphological and mtDNA clines between 1994 and 2000, in spite of hybrid zone movement, suggests strong epistasis between the mitochondrial genome and nuclear loci. Cline movement is achieved mainly by pure fatima immigrating into amathea populations; hybrids had little effect, and were presumably outcompeted by fitter pure fatima genotypes. This movement can be explained if random dispersal of 7-19 km.gen(-1/2) is coupled with a competitive advantage to A. fatima genomes of 2-5%. Hybrid zone motion is equivalent to Phase III of Wright's shifting balance. Hybrid zone movement has rarely been considered likely in the past, but our results show that it may be more important in biogeography and evolution than generally realized. C1 UCL, Dept Biol, Galton Lab, London NW1 2HE, England. Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. Duke Univ, Dept Biol, Durham, NC 27705 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Calif Berkeley, Gump Res Stn, Moorea, Fr Polynesia. RP Dasmahapatra, KK (reprint author), UCL, Dept Biol, Galton Lab, 4 Stephenson Way, London NW1 2HE, England. EM kkd22@cam.ac.uk; mjblum@duke.edu; aielloa@tivoli.si.edu; ndavies@nature.berkeley.edu; eb@naos.si.edu; j.mallet@ucl.ac.uk RI Davies, Neil/E-5863-2012; OI Davies, Neil/0000-0001-8085-5014; Mallet, James/0000-0002-3370-0367 NR 63 TC 81 Z9 88 U1 3 U2 18 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0014-3820 J9 EVOLUTION JI Evolution PD APR PY 2002 VL 56 IS 4 BP 741 EP 753 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 552HQ UT WOS:000175614400009 PM 12038532 ER PT J AU Zimbelman, JR Williams, SH AF Zimbelman, JR Williams, SH TI Geochemical indicators of separate sources for eolian sands in the eastern Mojave Desert, California, and western Arizona SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article DE deserts; eolian; geochemistry; sand; sand dunes; sediment ID NORTHEASTERN COLORADO; MARTIAN SURFACE; GEOMORPHOLOGY; DUNES; RAMPS; MARS AB Low, stabilized sand dunes cover much of the Cactus and La Posa Plains in western Arizona, near the town of Parker. The provenance of the dunes is not well defined, and it had been hypothesized that they were possibly related to extensive eolian sand deposits in the eastern Mojave Desert of California, on the other side of the Colorado River. Major oxide analyses of bulk sand samples collected from southeastern California and western Arizona show clear chemical differences. The Mojave sands all have SiO2 < 79 wt%, Al2O3 > 10 wt%, and Na2O + K2O > 5 wt%, whereas the Colorado River and Arizona sands have SiO2 > 81 wt%, Al2O3 < 6 wt%, and Na2O + K2O < 4 wt%. These results show that the stabilized dunes near Parker are chemically indistinguishable from Colorado River sands. The chemical differences between the southeastern California sands and the western Arizona sands are supported by X-ray diffraction results that indicate these two sand populations have significant differences in the relative abundance of quartz and feldspar. Our data also indicate a near-source origin for the Mojave sands, whereas the Colorado River and Arizona sands have undergone more prolonged chemical weathering. The major oxide results are consistent with published trace element studies by others that clearly distinguished between mature and immature sands in California and Colorado. The quartz/feldspar ratio may be amenable to measurement by some advanced remote-sensing instruments. C1 Natl Air & Space Museum, Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Biol Sci Curriculum Study, Colorado Springs, CO 80918 USA. RP Zimbelman, JR (reprint author), Natl Air & Space Museum, Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 46 TC 17 Z9 18 U1 1 U2 5 PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER PI COLLEGE STN PA TEXAS A & M UNIV, DEPT GEOLOGY & GEOPHYSICS, COLLEGE STN, TX 77843-3115 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD APR PY 2002 VL 114 IS 4 BP 490 EP 496 DI 10.1130/0016-7606(2002)114<0490:GIOSSF>2.0.CO;2 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 538YJ UT WOS:000174842500008 ER PT J AU Rougvie, JR Sorensen, SS AF Rougvie, JR Sorensen, SS TI Cathodoluminescence record of K-metasomatism in ash-flow tuffs: Grain-scale mechanisms and large-scale geochemical implications SO GEOLOGY LA English DT Article DE alteration; ash-flow tuff; cathodoluminescence; feldspar; Tertiary ID VOLCANIC-ROCKS; ARIZONA; CALIFORNIA; MOUNTAINS AB Near-surface., low-temperature, K-metasomatism of rhyolitic to dacitic ash-flow tuffs is a volumetrically and petrologically significant feature of the western United States and may be a primary alteration path in and lands. Cathodoluminescence (CL) petrography of K-metasomatized ash-flow tuffs quickly yields information about the mineralogical changes and reaction mechanisms that take place during alteration for large sample suites and links these properties to geochemical changes. Tertiary volcanic rocks from Creede (Colorado), Socorro (New Mexico), and the Harcuvar Mountains (Arizona), were altered in different geologic settings, yet have very similar CL textures and chemistry. Original igneous feldspars were replaced by adularia primarily by dissolution and crystallization that occurred preferentially along preexisting fractures, surfaces, compositional zoning features, and cleavages. Fluid flow was primarily along grain boundaries, but was in some cases inhomogeneous at the thin-section scale. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Rougvie, JR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. NR 19 TC 12 Z9 13 U1 1 U2 3 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD APR PY 2002 VL 30 IS 4 BP 307 EP 310 DI 10.1130/0091-7613(2002)030<0307:CROKMI>2.0.CO;2 PG 4 WC Geology SC Geology GA 539HV UT WOS:000174865200005 ER PT J AU Hymus, GJ Snead, TG Johnson, DP Hungate, BA Drake, BG AF Hymus, GJ Snead, TG Johnson, DP Hungate, BA Drake, BG TI Acclimation of photosynthesis and respiration to elevated atmospheric CO2 in two Scrub Oaks SO GLOBAL CHANGE BIOLOGY LA English DT Article DE elevated CO2; leaf nitrogen; leaf respiration; open-top chambers; photosynthetic acclimation; scrub oaks ID CARBON-DIOXIDE ENRICHMENT; CASTANEA-SATIVA MILL; LEAF RESPIRATION; DARK RESPIRATION; MITOCHONDRIAL RESPIRATION; MAINTENANCE RESPIRATION; PERENNIAL RYEGRASS; DIRECT INHIBITION; PARTIAL-PRESSURE; PINUS-RADIATA AB For two species of oak, we determined whether increasing atmospheric CO2 concentration (C-a) would decrease leaf mitochondrial respiration (R) directly, or indirectly owing to their growth in elevated C-a, or both. In particular, we tested whether acclimatory decreases in leaf-Rubisco content in elevated C-a would decrease R associated with its maintenance. This hypothesis was tested in summer 2000 on sun and shade leaves of Quercus myrtifolia Willd. and Quercus geminata Small. We also measured R on five occasions between summer 1999 and 2000 on leaves of Q. myrtifolia. The oaks were grown in the field for 4 years, in either current ambient or elevated (current ambient+350 mumol mol(-1)) C-a, in open-top chambers (OTCs). For Q. myrtifolia, an increase in C-a from 360 to 710 mumol mol(-1) had no direct effect on R at any time during the year. In April 1999, R in young Q. myrtifolia leaves was significantly higher in elevated C-a-the only evidence for an indirect effect of growth in elevated C-a. Leaf R was significantly correlated with leaf nitrogen (N) concentration for the sun and shade leaves of both the species of oak. Acclimation of photosynthesis in elevated C-a significantly reduced maximum RuBP-saturated carboxylation capacity (V-c max) for both the sun and shade leaves of only Q. geminata. However, we estimated that only 11-12% of total leaf N was invested in Rubisco; consequently, acclimation in this plant resulted in a small effect on N and an insignificant effect on R. In this study measurements of respiration and photosynthesis were made on material removed from the field; this procedure had no effect on gas exchange properties. The findings of this study were applicable to R expressed either per unit leaf area or unit dry weight, and did not support the hypothesis that elevated C-a decreases R directly, or indirectly owing to acclimatory decreases in Rubisco content. C1 Smithsonian Environm Res Ctr, Kennedy Space Ctr, FL 32899 USA. No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. RP Hymus, GJ (reprint author), Smithsonian Environm Res Ctr, Mailcode DYN-2, Kennedy Space Ctr, FL 32899 USA. RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 46 TC 15 Z9 18 U1 0 U2 6 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 APR PY 2002 VL 8 IS 4 BP 317 EP 328 DI 10.1046/j.1354-1013.2001.00472.x PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 551PN UT WOS:000175570200003 ER PT J AU Ostro, SJ Rosema, KD Campbell, DB Shapiro, II AF Ostro, SJ Rosema, KD Campbell, DB Shapiro, II TI Radar observations of asteroid 1862 Apollo SO ICARUS LA English DT Article DE asteroids; radar ID NEAR-EARTH ASTEROIDS AB Arecibo radar echo spectra show the Q-class asteroid 1862 Apollo to have an elongation within 10% of 1.27, a pole-on silhouette with an average dimension of about 1.7 km, and disc-integrated radar properties that are typical for radar-detected near-Earth asteroids. (C) 2002 Elsevier Science (USA). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Dept Astron, Ithaca, NY USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ostro, SJ (reprint author), CALTECH, Jet Prop Lab, 300-233, Pasadena, CA 91109 USA. NR 11 TC 6 Z9 6 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2002 VL 156 IS 2 BP 580 EP 583 DI 10.1006/icar.2001.6805 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 553ED UT WOS:000175662000020 ER PT J AU Garcia-Rubio, S Attygalle, AB Weldon, PJ Meinwald, J AF Garcia-Rubio, S Attygalle, AB Weldon, PJ Meinwald, J TI Reptilian chemistry: Volatile compounds from paracloacal glands of the American crocodile (Crocodylus acutus) SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE American crocodile; Crocodylus acutus; paracloacal glands; fatty; esters; formates; mass spectrometry; GC-FTIR ID MAMMALIAN EXOCRINE SECRETIONS; PREORBITAL SECRETION; DEFENSIVE SECRETION; CONSTITUENTS; LIPIDS; DIANEACKERONE; ESTERS AB The secretion of the paracloacal glands of the American crocodile (Crocodylus acutus) contains over 80 lipophilic compounds, including saturated and unsaturated long-chain alcohols along with their formic, acetic, and butyric acid esters, and several isoprenoids. Most of these compounds were identified on the basis of mass spectra, obtained by GC-MS. In addition, identification of the major components was supported by infrared spectra obtained by GC-FTIR. Major differences are indicated in the composition of the paracloacal gland secretion of C. acutus and that of another crocodylid, the African dwarf crocodile (Osteolaemus tetraspis). C1 Cornell Univ, Dept Chem & Chem Biol, Ithaca, NY 14853 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Meinwald, J (reprint author), Cornell Univ, Dept Chem & Chem Biol, Ithaca, NY 14853 USA. NR 30 TC 9 Z9 9 U1 0 U2 2 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD APR PY 2002 VL 28 IS 4 BP 769 EP 781 AR UNSP 0098-0331/02/0400-0769/0 DI 10.1023/A:1015288726605 PG 13 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 552PJ UT WOS:000175628500009 PM 12035925 ER PT J AU Belyaev, AK Dalgarno, A McCarroll, R AF Belyaev, AK Dalgarno, A McCarroll, R TI The dependence of nonadiabatic couplings on the origin of electron coordinates SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MULTIPLY CHARGED IONS; ATOMIC-COLLISIONS; ELEMENTS; ENERGIES; MODEL AB It is shown both analytically and numerically for a number of examples that both radial and rotational nonadiabatic couplings within the standard adiabatic approach depend on the origin of the light-particle coordinates and the ambiguity in the nonadiabatic couplings does not lead to ambiguity in the coupled channel equations. The examples considered are the nH, nD, npmu(-) quasimolecules, for which the nonadiabatic couplings can be calculated analytically, and the HeH molecule, for which ab initio calculations are carried out. Analytical formulas for couplings calculated with the shifted origin are derived. The coupled equations take their simplest form in Jacobi coordinates for which many nonadiabatic couplings are nonzero, even for such noninteracting systems as nH, nD, and npmu(-). These couplings are a fundamental feature of the adiabatic approach. (C) 2002 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. AI Herzen Univ Russia, Dept Theoret Phys, St Petersburg 191186, Russia. Univ Paris 06, Lab Dynam Ions Atom & Mol, CNRS, UMR 7066, F-75252 Paris, France. RP Belyaev, AK (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Belyaev, Andrey/B-6051-2011 OI Belyaev, Andrey/0000-0001-8834-1456 NR 24 TC 31 Z9 31 U1 0 U2 12 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 APR 1 PY 2002 VL 116 IS 13 BP 5395 EP 5400 DI 10.1063/1.1457443 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 532JH UT WOS:000174470700009 ER PT J AU Bobe, R Behrensmeyer, AK Chapman, RE AF Bobe, R Behrensmeyer, AK Chapman, RE TI Faunal change, environmental variability and late Pliocene hominin evolution SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE climate change; faunal change; Pliocene mammals; environmental variability; lower Omo valley; Shungura Formation; hominid evolution; Homo ID SHUNGURA FORMATION; TURKANA BASIN; ETHIOPIA; KENYA; CLIMATE; MEMBER; TOOLS; HOMO AB Global change during the late Pliocene was manifested in declining temperatures, increased amplitude of climate cycles, and shifts in the periodicity of orbital climate forcing. Linking these changes to the evolution of African continental faunas and to hominin evolution requires well-documented fossil evidence that can be examined through substantial periods of time. The Omo sequence of southern Ethiopia provides such a database, and we use it to analyze change in the abundances of mammal taxa at different levels of temporal and taxonomic resolution between 4 and 2 Ma. This study provides new evidence for shifts through time in the ecological dominance of suids, cercopithecids, and bovids, and for a trend from more forested to more open woodland habitats. Superimposed on these long-term trends are two episodes of faunal change, one involving a marked shift in the abundances of different taxa at about 2.8 +/- 0.1 Ma, and the second the transition at 2.5 Ma from a 200-ka interval of faunal stability to marked variability over intervals of about 100 ka. The first appearance of Homo, the earliest artefacts, and the extinction of non-robust Australopithecus in the Omo sequence coincide in time with the beginning of this period of high variability. We conclude that climate change caused significant shifts in vegetation in the Omo paleo-ecosystem and is a plausible explanation for the gradual ecological change from forest to open woodland between 3.4 and 2.0 Ma, the faunal shift at 2.8 +/- 0.1 Ma, and the change in the tempo of faunal variability of 2.5 Ma. Climate forcing in the late Pliocene is more clearly indicated by population shifts within the Omo mammal community than by marked turnover at the species level. C1 Smithsonian Inst, Evolut Terr Ecosyst Program, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. Smithsonian Inst, Appl Morphometr Lab, MRC 136, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Bobe, R (reprint author), Smithsonian Inst, Evolut Terr Ecosyst Program, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. EM bobe.rene@nmnh.si.edu; behrensmeyer.kay@nmnh.si.edu; chapman.ralph@nmnh.si.edu RI BOBE, Regis/F-4951-2016 OI Bobe, Rene/0000-0001-9059-2203; BOBE, Regis/0000-0002-8225-9117 NR 71 TC 129 Z9 137 U1 1 U2 27 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD APR PY 2002 VL 42 IS 4 BP 475 EP 497 DI 10.1006/jhev.2001.0535 PG 23 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 542QU UT WOS:000175056500006 PM 11908957 ER PT J AU Gonzalez, VH Brown, BV Ospina, M AF Gonzalez, VH Brown, BV Ospina, M TI A new species of Megaselia (Diptera : Phoridae) associated with brood provisions of nests of Neocorynura (Hymenoptera : Halictidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE Megaselia; taxonomy; Neocorynura; nest parasitism; kleptoparasite ID ARCHITECTURE; FLY AB Males and females of Megaselia neocorynurae n. sp. from the Eastern Andes of Colombia are described and illustrated. Females of this species can be recognized by the peculiar white color of the region of tergites 5 and 6 in the abdomen, and males by the combination of relatively large body size, dark color, presence of four supra-antennal setae and four large scutellar setae. and the unusual erect cerci of the terminalia. Larvae of M. neocorynurae n. sp. were found feeding on brood provision 11.4 and 14.9% of the cells of two as yet undescribed species of Neo-corynura. These associations represent the first halictid host for Megaselia as well as the first examples of this phorid fly genus as a kleptoparasite of halictid bees. Biological information of M. neocorynurae n. sp. is compared with that known for Phalacrotophora halictorum, the only previously known phorid fly associated with brood provisions of Halictidae. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Nat Hist Museum Los Angeles, Entomol Sect, Los Angeles, CA 90007 USA. Univ Nacl Colombia, Lab Invest Abejas, Bogota, Colombia. RP Gonzalez, VH (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. EM vhgonzales@rocketmail.com; bbrown@nhm.org; thygater@eudoramail.com RI Gonzalez Betancourt, Victor /B-9528-2011; Gonzalez, Victor/B-4072-2015 NR 18 TC 8 Z9 10 U1 0 U2 1 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 EI 1937-2353 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD APR PY 2002 VL 75 IS 2 BP 73 EP 79 PG 7 WC Entomology SC Entomology GA 589FW UT WOS:000177749000002 ER PT J AU Citino, SB Bush, M Grobler, D Lance, W AF Citino, SB Bush, M Grobler, D Lance, W TI Anesthesia of boma-captured Lichtenstein's hartebeest (Sigmoceros lichtensteinii) with a combination of thiafentanil, medetomidine, and ketamine SO JOURNAL OF WILDLIFE DISEASES LA English DT Article DE A3080; anesthesia; atipamezole; hartebeest; ketamine; medetomidine; naltrexone; Sigmoceros lichtensteinii; thiafentanil ID ORYX ORYX-LEUCORYX; IMMOBILIZATION AB A dose range was determined For anesthesia OF recently boma-captured Lichtenstein's hartebeest (Sigmoccros 13) with the synthetic opiate thiafentanil (THIA) (formerly called A3080) combined with medetomidine (MED) and ketamine (KET) in the Kasungu National Park, Malawi on 4 to 5 September 1999. The close range of 11-26 mug/kg THA (mean +/- SD = 21 +/- 4 mug/kg) combined with 5-10 mg/kg MED (8 +/- 1 mug/kg) plus 0.7-1.4 mg/kg KET (1.1 +/- 0.2 mg/kg) was found to be safe and effective For the field conditions associated with this study. The anesthesia produced by this drug combination vas very preditable and characterized by a short induction time (3:34 +/- 1:20 min : see), good muscle relaxation, and acceptable physiologic parameters for anesthesia periods ranging from 22:30-35:00 min : see (31:14 +/- 2:50). within the range of doses used in this study, times to onset of initial effects and recumbency were not dependent on THAI, MED, or KET doses. Anesthesia was rapidly and completely reversed by intravenous injections of naltrexone at 30 times the THAI dosage (0.69 +/- 0.19 mg/kg) and atipamezole at about four times the MED dosage (38 +/- 14 mug/kg). There was no residual effect from ketamine noted following reversal of THIA and MED and no mortality or morbidity was associated with this anesthetic regimen. C1 White Oak Conservat Ctr, Yulee, FL 32097 USA. Natl Zool Pk, Conservat & Res Ctr, Smithsonian Inst, Front Royal, VA 22630 USA. S African Natl Pk, Kruger Natl Pk, ZA-1350 Skukuza, South Africa. Wildlife Pharmaceut Inc, Ft Collins, CO 80524 USA. RP Citino, SB (reprint author), White Oak Conservat Ctr, 3823 Owens Rd, Yulee, FL 32097 USA. NR 19 TC 14 Z9 16 U1 0 U2 0 PU WILDLIFE DISEASE ASSN, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD APR PY 2002 VL 38 IS 2 BP 457 EP 462 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA 547YR UT WOS:000175361100029 PM 12038149 ER PT J AU Schroll, S AF Schroll, S TI Image duplicator: Roy Lichtenstein and the emergence of pop art. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Schroll, S (reprint author), Smithsonian Inst Libs, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 1 PY 2002 VL 127 IS 6 BP 102 EP 102 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 534ZJ UT WOS:000174619400063 ER PT J AU Lazendic, JS Wardle, M Burton, MG Yusef-Zadeh, F Whiteoak, JB Green, AJ Ashley, MCB AF Lazendic, JS Wardle, M Burton, MG Yusef-Zadeh, F Whiteoak, JB Green, AJ Ashley, MCB TI Shocked molecular gas towards the supernova remnant G359.1-0.5 and the Snake SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE masers; shock waves; ISM : clouds; ISM : individual : G359.1-0.5; ISM : individual : Snake; supernova remnants ID EXCITED MASER EMISSION; GALACTIC-CENTER; INTRINSIC COLORS; DARK CLOUDS; OH; WAVES; LINE; PHOTOMETRY; RADIO AB We have found a bar of shocked molecular hydrogen (H-2) towards the OH(1720 MHz) maser located at the projected intersection of supernova remnant (SNR) G359.1-0.5 and the nonthermal radio filament known as the Snake. The H-2 bar is well aligned with the SNR shell and almost perpendicular to the Snake. The OH(1720 MHz) maser is located inside the sharp western edge of the H-2 emission, which is consistent with the scenario in which the SNR drives a shock into a molecular cloud at that location. The spectral line profiles of (CO)-C-12, HCO+ and CS towards the maser show broad-line absorption, which is absent in the (CO)-C-13 spectra and most probably originates from the pre-shock gas. A density gradient is present across the region and is consistent with the passage of the SNR shock, while the H-2 filament is located at the boundary between the pre-shock and post-shock regions. C1 Univ Sydney, Sch Phys A28, Sydney, NSW 2006, Australia. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. Northwestern Univ, Dept Phys & Astron, Dearborn Observ, Evanston, IL 60201 USA. RP Lazendic, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Burton, Michael/0000-0001-7289-1998; Wardle, Mark/0000-0002-1737-0871 NR 40 TC 19 Z9 19 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 1 PY 2002 VL 331 IS 2 BP 537 EP 544 DI 10.1046/j.1365-8711.2002.05227.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 542FE UT WOS:000175032200028 ER PT J AU Jennions, MD Kelly, CD AF Jennions, MD Kelly, CD TI Geographical variation in male genitalia in Brachyphaphis episcopi (Poeciliidae): is it sexually or naturally selected? SO OIKOS LA English DT Article ID FEMALE MATE CHOICE; CONDITION-DEPENDENT TRAITS; LEK PARADOX; ENVIRONMENTAL GRADIENTS; TRINIDADIAN GUPPIES; ANIMAL GENITALIA; MALE COMPETITION; SIZE DIMORPHISM; MATING-BEHAVIOR; PREDATION RISK AB Male poeciliid fishes inseminate females using an intromittent organ called the gonopodium. Here we report on natural variation in gonopodium size both within and between 12 populations of the freshwater fish Brachyrhaphis episcopi (Poeciliidae) in Panama. We show that males from sites with more predatory fish species have, on average, a relatively longer gonopodium than males inhabiting sites with fewer predatory fish. Gonopodium length was not correlated with the site-specific adult sex ratio and the average sex ratio was more strongly female biased at sites with more predatory fish. The gonopodium. exhibited lower phenotypic variance than the average for sexually selected traits and it generally showed negative allometry. Our results are similar to those reported for the guppy Poecilia reticulata. Two alternative hypotheses for these findings are discussed. First, that population differences are sexually selected. Second, that they are an incidental consequence of environmental differences between sites. Specifically, that higher water flow rates select for enlarged fin size and stockier bodies in downstream sites where predatory fish are more common. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. ANU, Sch Bot & Zool, Canberra, ACT 0200, Australia. Univ Toronto, Biol Grp, Mississauga, ON L5L 1C6, Canada. RP Kelly, CD (reprint author), Univ Toronto, Biol Grp, Mississauga, ON L5L 1C6, Canada. RI Kelly, Clint/A-2311-2008; Jennions, Michael/C-7560-2009; OI Jennions, Michael/0000-0001-9221-2788; Kelly, Clint/0000-0002-0693-7211 NR 61 TC 52 Z9 54 U1 2 U2 16 PU BLACKWELL MUNKSGAARD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0030-1299 J9 OIKOS JI Oikos PD APR PY 2002 VL 97 IS 1 BP 79 EP 86 DI 10.1034/j.1600-0706.2002.970108.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 559JC UT WOS:000176022200008 ER PT J AU Deocampo, DM AF Deocampo, DM TI Sedimentary structures generated by Hippopotamus amphibius in a lake-margin wetland, Ngorongoro Crater, Tanzania SO PALAIOS LA English DT Article ID BOTSWANA; TRACKS AB Large mammals, especially Hippopotamus amphibius, have created a distinctive set of traces in a spring-fed freshwater wetland on the margin of the saline-alkaline Crater lake in the Ngorongoro Crater, Tanzania. It is comprised of a similar to30 m diameter zone of deep (<2m) bioturbation due to hippo wallowing, surrounded by dendritic to radial hippo trails 1-5 m wide and <0.5 m deep, infilled with organic-rich mud. These trails narrow and thin as they grade into trackways on the lake flat. Tracks and trackways of more terrestrial mammals, such as bovids and equids, are found in the lake flat muds surrounding the hippo-dominated area. Associations of sedimentary structures such as these are important indicators of paleoenvironmental conditions where they are preserved in the sedimentary record, due to the strong affinity of Hippopotamidae for freshwater environments. C1 Rutgers State Univ, Dept Geol Sci, Piscataway, NJ 08854 USA. RP Deocampo, DM (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, MRC 119, Washington, DC 20560 USA. RI Deocampo, Daniel/A-9830-2010 NR 21 TC 31 Z9 31 U1 0 U2 8 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD APR PY 2002 VL 17 IS 2 BP 212 EP 217 DI 10.1669/0883-1351(2002)017<0212:SSGBHA>2.0.CO;2 PG 6 WC Geology; Paleontology SC Geology; Paleontology GA 576FF UT WOS:000176991600008 ER PT J AU Jonsell, S Saenz, A Froelich, P Forrey, RC Cote, R Dalgarno, A AF Jonsell, S Saenz, A Froelich, P Forrey, RC Cote, R Dalgarno, A TI Long-range interactions between two 2s excited hydrogen atoms SO PHYSICAL REVIEW A LA English DT Article ID AUTOIONIZING STATES; BETA-DECAY; MOLECULE; H-2; ENERGIES AB The doubly excited (1)Sigma(g)(+) and (3)Sigma(u)(+) states of the H-2 molecule converging to the H(n=2)+H(n(')=2) limit have been calculated using explicitly correlated basis functions, giving accurate results out to a nuclear separation sufficiently large to apply asymptotic expansions for the potential energy. The autoionization widths have been obtained using the complex-scaling method. For nuclear separations larger than 22 a.u., asymptotic expressions for the interaction energies have been obtained from perturbation theory. C1 Max Planck Inst Quantum Opt, D-85748 Garching, Germany. Univ Uppsala, Dept Quantum Chem, S-75120 Uppsala, Sweden. NORDITA, DK-2100 Copenhagen, Denmark. Penn State Univ, Berks Lehigh Valley Coll, Reading, PA 19610 USA. Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Jonsell, S (reprint author), Max Planck Inst Quantum Opt, Hans Kopfermann Str 1, D-85748 Garching, Germany. RI Jonsell, Svante/J-2251-2016 OI Jonsell, Svante/0000-0003-4969-1714 NR 14 TC 16 Z9 16 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 APR PY 2002 VL 65 IS 4 AR 042501 DI 10.1103/PhysRevB.65.042501 PN A PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 541HF UT WOS:000174978600055 ER PT J AU Yurovsky, VA Ben-Reuven, A Julienne, PS AF Yurovsky, VA Ben-Reuven, A Julienne, PS TI Quantum effects on curve crossing in a Bose-Einstein condensate SO PHYSICAL REVIEW A LA English DT Article ID FESHBACH RESONANCE; ATOM LOSS; COLLISIONS AB Formation of atomic pairs by the dissociation of a molecular condensate or by inelastic collisions in an atomic condensate due to a time-dependent curve crossing process is studied beyond the mean-field approximation. The number of atoms formed by the spontaneous process is described by a Landau-Zener formula multiplied by an exponential amplification factor due to quantum many-body effects. Correlated atomic pairs are formed in squeezed states. The rate of stimulated processes depends on the relative phase of the two fields. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Tel Aviv Univ, Sch Chem, IL-69978 Tel Aviv, Israel. Natl Inst Stand & Technol, Atom Phys Div, Bethesda, MD 20889 USA. RP Yurovsky, VA (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. RI Julienne, Paul/E-9378-2012 OI Julienne, Paul/0000-0002-5494-1442 NR 20 TC 30 Z9 30 U1 0 U2 2 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD APR PY 2002 VL 65 IS 4 AR 043607 DI 10.1103/PhysRevA.65.043607 PN B PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 541HL UT WOS:000174979100026 ER PT J AU Svenning, JC AF Svenning, JC TI Crown illumination limits the population growth rate of a neotropical understorey palm (Geonoma macrostachys, Arecaceae) SO PLANT ECOLOGY LA English DT Article DE crown illumination index; demography; Ecuador; matrix modelling; shade; understorey plants ID RAIN-FOREST; ASTROCARYUM-MEXICANUM; CANOPY STRUCTURE; DENSITY-DEPENDENCE; FINITE RATE; TREE; LIGHT; REPRODUCTION; DEMOGRAPHY; PATTERNS AB The importance of light as a limiting factor for growth and reproduction in tropical understorey plants is well known, but the population-level consequences of light limitation remain little explored. Here, I use demographic modelling to examine if the effect of canopy gaps on individual-level performance in a tropical understorey palm translates into an effect on the population growth rate. The demographic effects of heterogeneity in crown illumination (index of hemispherical canopy openness), forest-phase, and other microenvironmental parameters were quantified using data on 2592 individuals of all sizes in permanent plots followed over a 1.5 year period. Supplementary experiments investigating the effects of canopy conditions on seedling recruitment were also conducted. Among the microenvironmental parameters only crown illumination and forest-phase had strong and consistent demographic effects. Growth and fecundity generally increased with increasing crown illumination. Under open forest-phase conditions growth tended to increase and survival to decrease (due to increased physical damage). Seedlings transplanted into gap centres were damaged by solarization. The population-level effect of heterogeneity in crown illumination and forest-phase was investigated using transition matrix models. The overall population growth rate was 0.999, and not significantly different from 1. Illumination-specific models showed that G. macrostachys would be unable to persist at permanently low illumination, but would increase in density under higher illumination. Forest-phase-specific models gave similar, but weaker results. Thus, in G. macrostachys effects of canopy openness on individual-level performance strongly limit the population growth rate. The present study thereby shows that fine-scale spatiotemporal variation in canopy openness in the tropical rain forest understorey can play a central role in the population ecology of shade-tolerant understorey plants. C1 Aarhus Univ, Dept Systemat Bot, DK-8000 Aarhus C, Denmark. RP Svenning, JC (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Svenning, Jens-Christian/C-8977-2012 OI Svenning, Jens-Christian/0000-0002-3415-0862 NR 63 TC 38 Z9 41 U1 1 U2 17 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD APR PY 2002 VL 159 IS 2 BP 185 EP 199 DI 10.1023/A:1015520116260 PG 15 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 552TV UT WOS:000175636900007 ER PT J AU Brown, JW Pena, J Vazquez, T Baixeras, J AF Brown, JW Pena, J Vazquez, T Baixeras, J TI Description of a new tortricid pest (Lepidoptera : Tortricidae : Olethreutinae) of litchi (Litchi chinensis) in Florida, with a review of tortricid pests of litchi worldwide SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Crocidosema; Litchi chinensis; pest species; new record; species introduction; Caribbean AB The adult, larva, and pupa of Crocidosema litchivora Baixeras, new species, are described and illustrated; details of the life history are presented. Since 1993, an increase in the abundance of C litchivora in southern Florida has resulted in significant damage to commercially grown litchi (Litchi chinensis Sonnerat; Sapindaceae). The larvae feed on the inflorescences and buds of the host plant, significantly reducing crop yield. Owing to the absence of records of C litchivora prior to 1992, it is likely that this Neotropical species is a relatively recent arrival in southern Florida. A list of tortricid pests of litchi worldwide is presented. C1 Natl Museum Nat Hist, Smithsonian Inst, Systemat Entomol Lab, PSI,Agr Res Serv,USDA, Washington, DC 20560 USA. RP Brown, JW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Systemat Entomol Lab, PSI,Agr Res Serv,USDA, Washington, DC 20560 USA. RI Baixeras, Joaquin/L-1734-2014 OI Baixeras, Joaquin/0000-0002-6092-0496 NR 26 TC 3 Z9 4 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2002 VL 104 IS 2 BP 318 EP 329 PG 12 WC Entomology SC Entomology GA 543EE UT WOS:000175087800005 ER PT J AU Perez-Gelabert, DE AF Perez-Gelabert, DE TI Further characterization of Paleomastacris ambarinus Perez et al. (Orthoptera : Eumastacidae) from Dominican amber SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE amber fossils; Dominican republic; Eumastacidae; grasshoppers AB Three new specimens of fossil Eumastacidae in Dominican amber are characterized and identified as the previously described Paleomastacris and7arinus Perez et al. 1997. The better preservation of these specimens allows examination of features of the head not visible in the holotype. Paleomastacris ambarinus lacks the protruding fastigium typical of extant Hispaniolan Eumastacidae and in this respect seems to resemble Central American Episactinae more closely than those of Hispaniola. This fossil species likely represents an early link between these two extant groups of eumastacids. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. RP Perez-Gelabert, DE (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. NR 13 TC 2 Z9 3 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2002 VL 104 IS 2 BP 330 EP 334 PG 5 WC Entomology SC Entomology GA 543EE UT WOS:000175087800006 ER PT J AU Hall, JPW AF Hall, JPW TI A review of Chalodeta Stichel with a revision of the Chelonis group (Lepidoptera : Riodinidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE Chalodeta; Charis; Neotropics; Riodinini; taxonomy AB An overview of the Neotropical riodinid genus Chalodeta Stichel is presented which defines the taxon, delineates its member species, and discusses its systematic position within the tribe Riodinini. A revision of the Chalodeta chelonis group includes notes on the taxonomy and biology of its species, and illustrations of the adults and male and female genitalia (where known) of all taxa. Four species are recognized, including two that are previously described, C. chelonis (Hewitson 1866) and C chaonitis (Hewitson 1866), and two that are described here, C. chitinosa, n. sp., and C. chlosine, n. sp. The taxon stilbos Stichel 1910, is synonymized with C theodora (C. and R. Felder 1862) (n. syn.). C1 Natl Museum Nat Hist, Dept Systemat Biol, Entomol Sect, Smithsonian Inst, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Natl Museum Nat Hist, Dept Systemat Biol, Entomol Sect, Smithsonian Inst, Washington, DC 20560 USA. NR 26 TC 2 Z9 2 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2002 VL 104 IS 2 BP 376 EP 389 PG 14 WC Entomology SC Entomology GA 543EE UT WOS:000175087800012 ER PT J AU Smith, DR Shinohara, A AF Smith, DR Shinohara, A TI The stem-boring sawfly genus Cephus Latreille (Hymenoptera : Cephidae) in Japan SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE stem-borers; Cephidae; Cephus; Japan AB Two species of Cephus occur in Japan, C. hyalinatus Konow from Hokkaido and C. brachycercus Thomson, newly recorded from Japan, from Honshu. Clarification of past records of Cephus in Japan are presented. A key, descriptions, and illustrations of the abdomen are given for both species. C1 Natl Museum Nat Hist, Smithsonian Inst, Systemat Entomol Lab, PSI,Agr Res Serv,USDA, Washington, DC 20560 USA. RP Smith, DR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Systemat Entomol Lab, PSI,Agr Res Serv,USDA, Washington, DC 20560 USA. NR 17 TC 4 Z9 5 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2002 VL 104 IS 2 BP 479 EP 484 PG 6 WC Entomology SC Entomology GA 543EE UT WOS:000175087800018 ER PT J AU Golub, L Deluca, E Hamilton, P Nystrom, G Windt, DL Schmidt, WKH Dannenberg, A AF Golub, L Deluca, E Hamilton, P Nystrom, G Windt, DL Schmidt, WKH Dannenberg, A TI A photometric imaging solar telescope, tunable in the extreme ultraviolet, utilizing multilayer x-ray optics SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID MISSION AB We present a new instrument for space-based observational solar physics, recently flown successfully on a sounding rocket, designed to provide high spatial resolution, time-resolved images of the solar corona at specific wavelengths in the extreme ultraviolet (XUV). The primary instrument employs multilayer x-ray mirrors in a novel geometry that affords quasi-monochromatic imaging at wavelengths tunable continuously over the spectral range from 17.1 to 21.1 nm. The secondary instrument also uses multilayer x-ray mirrors to provide high-resolution imaging at three fixed XUV wavelength bands. Both instruments use charge coupled device detectors and thin A1 filters for rejection of unwanted wavelengths. We describe the design, construction, and performance of the instrument and discuss prospects for the future. (C) 2002 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Astrophys Lab, New York, NY 10027 USA. Max Planck Inst Aeron, D-37191 Katlenburg Lindau, Germany. RP Golub, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Hamilton, Paul/E-7891-2015; DeLuca, Edward/L-7534-2013; OI Hamilton, Paul/0000-0001-6080-632X; DeLuca, Edward/0000-0001-7416-2895; Golub, Leon/0000-0001-9638-3082 NR 11 TC 3 Z9 3 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 APR PY 2002 VL 73 IS 4 BP 1908 EP 1913 DI 10.1063/1.1453506 PG 6 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 535FG UT WOS:000174634100036 ER PT J AU Anglada, G Rodriguez, LF AF Anglada, G Rodriguez, LF TI VLA detection of the exciting sources of the molecular outflows associated with L1448 IRS2, IRAS 05327+3404, L43, IRAS 22142+5206, L1211, and IRAS 23545+6508 SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE ISM : jets and outflows; stars : formation; stars : mass loss; radio continuum : stars ID PROTOPLANETARY NEBULA CANDIDATES; YOUNG STELLAR OBJECTS; AMMONIA OBSERVATIONS; BIPOLAR-OUTFLOW; DENSE CORES; CO OUTFLOW; STARS; JET; PROTOSTAR; REGIONS AB We present, sensitive very large array observations at 3.6 cm of nine fields containing molecular outflows. We detected candidates for the exciting sources of the molecular outflows in six of the fields: L1448 IRS2, IRAS 05327+3404, L43, IRAS 22142+5206, L1211, and IRAS 23545+6508. We discuss the parameters of these sources, as well as their relation with sources detected at other wavelengths. C1 CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. Univ Nacl Autonoma Mexico, Astron Inst, Morelia 58090, Michoacan, Mexico. RP Anglada, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM guillem@iaa.es; l.rodriguez@astrosmo.unam.mx NR 37 TC 11 Z9 11 U1 0 U2 1 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD APR PY 2002 VL 38 IS 1 BP 13 EP 21 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 555CV UT WOS:000175776500002 ER PT J AU Winfrey, S AF Winfrey, S TI Mail call (Anthrax, U.S. postal service) SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Winfrey, S (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD APR PY 2002 VL 33 IS 1 BP 11 EP 11 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 533NQ UT WOS:000174537000001 ER PT J AU Small, LM AF Small, LM TI Cartwheels at 50 (Smithsonian Institution Traveling Exhibition Service, SITE) SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD APR PY 2002 VL 33 IS 1 BP 12 EP 12 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 533NQ UT WOS:000174537000002 ER PT J AU Hall, JPW AF Hall, JPW TI Phylogeny of the riodinid butterfly subtribe Theopeina (Lepidoptera : Riodinidae : Nymphidiini) SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID TRIBE JOSIINI NOTODONTIDAE; CLADISTIC-ANALYSIS; PARSIMONIOUS TREES; ADULT MORPHOLOGY; DOMINICAN AMBER; DNA-SEQUENCES; CLASSIFICATION; EVOLUTION; LARVAL; ANTS AB The almost exclusively Neotropical butterfly family Riodinidae is poorly represented in both ecological and systematic studies of Lepidoptera. A comparative morphological study of all seventy-five species in subtribe Theopeina (tribe Nymphidiini) yielded 104 characters, predominantly from wing pattern, male and female genitalia, and abdominal structures. All morphological characters and adults representing the range of wing pattern variation are illustrated. Phylogenetic analysis of the data produced a large number of most parsimonious cladograms, but the strict consensus of these, both when using equal weights and after successive weighting, is well resolved and the majority of terminal clades have high character and branch support. Theopeina is found to consist of five monophyletic genera. Protonymphidia, Archaeonympha, Calicosama, Behemothia and Theope (= Parnes and Dinoplotis), with the largest genus Theope containing thirteen monophyletic species groups, which are delineated to facilitate a discussion of broad evolutionary patterns in this morphologically diverse subtribe. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Entomol, Washington, DC 20560 USA. EM jpwhall@hotmail.com NR 92 TC 16 Z9 16 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0307-6970 J9 SYST ENTOMOL JI Syst. Entomol. PD APR PY 2002 VL 27 IS 2 BP 139 EP 167 DI 10.1046/j.1365-3113.2002.00171.x PG 29 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 548JV UT WOS:000175385600001 ER PT J AU Chatterjee, P Hernquist, L Loeb, A AF Chatterjee, P Hernquist, L Loeb, A TI Brownian motion in gravitationally interacting systems SO PHYSICAL REVIEW LETTERS LA English DT Article ID MASSIVE BLACK-HOLE; GLOBULAR-CLUSTER AB wWe derive a model that describes the dynamics of a Brownian particle, such as a massive black hole, in a stellar system dominated by gravitational forces, and examine whether it achieves a state of equipartition of kinetic energy with the stars. This problem has been considered before only for stellar systems with an isothermal Maxwellian distribution of velocities; here we study other examples and confirm our calculations with N-body simulations. We show that in certain cases the black hole's steady state kinetic energy can be very far from equipartition. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chatterjee, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 14 Z9 14 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 25 PY 2002 VL 88 IS 12 AR 121103 DI 10.1103/PhysRevLett.88.121103 PG 4 WC Physics, Multidisciplinary SC Physics GA 533QP UT WOS:000174542000011 PM 11909441 ER PT J AU Heyl, JS Loeb, A AF Heyl, JS Loeb, A TI Vacuum decay constraints on a cosmological scalar field SO PHYSICAL REVIEW LETTERS LA English DT Article ID UNIVERSE; SUPERNOVAE AB If the potential of a scalar filed phi which currently provides the dark energy of the Universe has a minimum at phi = -M-0(4) < 0, then quantum-mechanical fluctuations could nucleate a bubble of φ at a negative value of the potential. This bubble would then expand at the speed of light. Given that no such bubble enveloped us in the past, we find that any minimum in V(φ) must be separated from the current φ value by more than min{1.5M(&ODOT;), 0.21M(P1)} where M-P1 is the Planck mass. We also show that vacuum decay renders a cyclic or ekpyrotic universe with M-0(4) greater than or similar to 10(-10) M-P1(4) untenable. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heyl, JS (reprint author), Harvard Smithsonian Ctr Astrophys, MS 51,60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 4 Z9 4 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 25 PY 2002 VL 88 IS 12 AR 121302 DI 10.1103/PhysRevLett.88.121302 PG 3 WC Physics, Multidisciplinary SC Physics GA 533QP UT WOS:000174542000013 PM 11909443 ER PT J AU Todd, JA Jackson, JBC Johnson, KG Fortunato, HM Heitz, A Alvarez, M Jung, P AF Todd, JA Jackson, JBC Johnson, KG Fortunato, HM Heitz, A Alvarez, M Jung, P TI The ecology of extinction: molluscan feeding and faunal turnover in the Caribbean Neogene SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE faunal turnover; primary productivity; Caribbean; Neogene; macroecology ID TROPICAL AMERICAN MOLLUSKS; MASS EXTINCTION; COSTA-RICA; DIVERSITY; PANAMA; EMERGENCE; ISTHMUS; PACIFIC; RECORD AB Molluscan faunal turnover in the Plio-Pleistocene of the tropical western Atlantic has been attributed to drops in temperature or primary productivity, but these competing hypotheses have not been assessed ecologically. To test these alternatives, we compiled data on changing molluscan life habits and trophic composition over 12 million years derived from 463 newly made collections from the southwestern Caribbean. Shelf ecosystems have altered markedly in trophic structure since the Late Pliocene. Predatory gastropods and suspension-feeding bivalves declined significantly in abundance, but not in diversity, and reef-dwellers became common. By contrast, all other ecological life habits remained remarkably stable. Food-web changes strongly support the hypothesis that declining regional nutrient supply had an increasing impact on regional macroecology, culminating in a faunal turnover. C1 Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. Nat Hist Museum, CH-4001 Basel, Switzerland. RP Todd, JA (reprint author), Nat Hist Museum, Dept Palaeontol, Cromwell Rd, London SW7 5BD, England. EM j.todd@nhm.ac.uk OI Todd, Jonathan/0000-0002-0433-1611 NR 39 TC 68 Z9 72 U1 0 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 MAR 22 PY 2002 VL 269 IS 1491 BP 571 EP 577 DI 10.1098/rspb.2001.1923 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 538WC UT WOS:000174837200004 PM 11916472 ER PT J AU Gaztanaga, E Fosalba, P Croft, RAC AF Gaztanaga, E Fosalba, P Croft, RAC TI Two-point moments in cosmological large-scale structure - I. Theory and comparison with simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmology : theory; dark matter; large-scale structure of Universe ID PERTURBATION-THEORY; NONLINEAR EVOLUTION; INITIAL CONDITIONS; STATISTICS; CATALOGS; 2-POINT; BIAS AB We present new perturbation theory (PT) predictions in the spherical collapse (SC) model for the two-point moments of the large-scale distribution of dark matter density in the Universe. We assume that these fluctuations grow under gravity from small Gaussian initial conditions. These predictions are compared with numerical simulations and with previous PT results to assess their domain of validity. We find that the SC model provides in practice a more accurate description of two-point moments than previous tree-level PT calculations. The agreement with simulations is excellent for a wide range of scales (5-50 h(-1) Mpc) and fluctuation amplitudes (sigma(2) similar or equal to 0.02-2). When normalized to unit variance these results are independent of the cosmological parameters and of the initial amplitude of fluctuations. The two-point moments provide a convenient tool for studying the statistical properties of gravitational clustering for fairly non-linear scales and complicated survey geometries, such as those probing the clustering of the Lyalpha forest. In this context, the perturbative SC predictions presented here provide a simple and novel way of testing the gravitational instability paradigm. C1 INAOE, Puebla 7200, Mexico. CSIC, IEEC, ES-08034 Barcelona, Spain. Univ Barcelona, Dept Fis Fonamental, E-08028 Barcelona, Spain. European Space Agcy, ESTEC, Dept Space Sci, NL-2200 AG Noordwijk, Netherlands. Inst Astrophys, F-75014 Paris, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaztanaga, E (reprint author), INAOE, Apdo Postal 216 & 51, Puebla 7200, Mexico. RI Fosalba Vela, Pablo/I-5515-2016; Croft, Rupert/N-8707-2014; Gaztanaga, Enrique/L-4894-2014 OI Croft, Rupert/0000-0003-0697-2583; Gaztanaga, Enrique/0000-0001-9632-0815 NR 25 TC 8 Z9 8 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2002 VL 331 IS 1 BP 13 EP 22 DI 10.1046/j.1365-8711.2002.05110.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539BZ UT WOS:000174851000005 ER PT J AU Nulsen, PEJ David, LP McNamara, BR Jones, C Forman, WR Wise, M AF Nulsen, PEJ David, LP McNamara, BR Jones, C Forman, WR Wise, M TI Interaction of radio lobes with the hot intracluster medium: Driving convective outflow in Hydra A SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : individual (Hydra A); intergalactic medium ID RAY-EMITTING GAS; MAGNETIC-FIELDS; CLUSTER GAS; A CLUSTER; CYGNUS-A; GALAXIES; NGC-1275; M87 AB The radio lobes of Hydra A lie within cavities surrounded by a rim of enhanced X-ray emission in the intra-cluster gas. Although the bright rim appears cooler than the surrounding gas, existing Chandra data do not exclude the possibility that the rim is produced by a weak shock. A temperature map shows that cool gas extends out along the radio axis of Hydra A. The age of the radio source and equipartition pressure of the radio lobe argue against a shock, and comparison with similar structure in the Perseus Cluster also suggests that the rim is cool. We show that the cool bright rim cannot be the result of shock-induced cooling or due to the effect of magnetic fields in shocks. The most likely source of low-entropy ( cool) gas is entrainment by the rising cavity. This requires some means of communicating the bouyant force on the cavity to the surrounding gas. The magnetic field required to produce the Faraday rotation in Hydra A has the appropriate properties for this if the Faraday screen is mainly in this bright rim. In Hydra A, the mass out flow due to the rising cavities could be sufficient to balance cooling-driven inflow, so preventing the build up of low-entropy gas in the cluster core. C1 Univ Wollongong, Wollongong, NSW 2522, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Nulsen, PEJ (reprint author), Univ Wollongong, Wollongong, NSW 2522, Australia. OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 NR 32 TC 112 Z9 113 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 MAR 20 PY 2002 VL 568 IS 1 BP 163 EP 173 DI 10.1086/338494 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 531VN UT WOS:000174438100015 ER PT J AU Murray, SS Slane, PO Seward, FD Ransom, SM Gaensler, BM AF Murray, SS Slane, PO Seward, FD Ransom, SM Gaensler, BM TI Discovery of X-ray pulsations from the compact central source in the supernova remnant 3C 58 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (3C 58); pulsars : individual (PSR J0205+6449); stars : neutron; supernova remnants; X-rays : stars ID CALIBRATION; NEBULAE; PULSARS; STARS; 3C-58 AB We report on high time and spatial resolution observations of the supernova remnant (SNR) 3C 58 using the High Resolution Camera (HRC) on the Chandra X-Ray Observatory. These data show a pointlike central source from which we detect 65.68 ms pulsations at 6.7 sigma significance. We interpret these pulsations as corresponding to a young rotation-powered pulsar, PSR J0205+ 6449, that is associated with and powers SNR 3C 58. Analysis of archival Rossi X-Ray Timing Explorer ( RXTE) data from 3 years earlier confirms these pulsations and allows us to determine a spin-down rate of (P) over dot = 1.93 x 10(-13) s s(-1). Assuming a magnetic dipole model for PSR J0205+ 6449, we infer a surface magnetic field of 3.6 x 10(12) G. The historical age for the pulsar (based on its identification with SN 1181) is 820 yr. Taken with the observed period and spin-down rate, we derive an initial spin period of similar to60 ms. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Murray, SS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; OI Ransom, Scott/0000-0001-5799-9714; Gaensler, Bryan/0000-0002-3382-9558 NR 18 TC 85 Z9 86 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2002 VL 568 IS 1 BP 226 EP 231 DI 10.1086/338766 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 531VN UT WOS:000174438100022 ER PT J AU Zucker, S Naef, D Latham, DW Mayor, M Mazeh, T Beuzit, JL Drukier, G Perrier-Bellet, C Queloz, D Sivan, JP Torres, G Udry, S AF Zucker, S Naef, D Latham, DW Mayor, M Mazeh, T Beuzit, JL Drukier, G Perrier-Bellet, C Queloz, D Sivan, JP Torres, G Udry, S TI A planet candidate in the stellar triple system HD 178911 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; planetary systems; stars : abundances; stars : individual (HD 178911, 16 Cygni); techniques : radial velocities ID BINARY STARS; ORBITAL CIRCULARIZATION; RADIAL-VELOCITIES; ORION-NEBULA; PARENT STARS; SOLAR TWINS; ABUNDANCES; EVOLUTION; 16-CYGNI-B; TELESCOPE AB We report the detection of a low-mass companion orbiting the solar-type star HD 178911B, the distant component of the stellar triple system HD 178911. The variability of HD 178911B was first detected using radial velocity measurements obtained with the High Resolution Echelle Spectrometer mounted on the 10 m Keck 1 telescope at the W. M. Keck Observatory (Hawaii). We then started an intense radial velocity follow-up of the star with the ELODIE echelle spectrograph mounted on the 1.93 m telescope at the Observatoire de Haute-Provence (France) in order to derive its orbital solution. The detected planet candidate has an orbital period of 71.5 days and a minimum mass of 6.3 M-J. We performed a spectral analysis of the star that shows that the lithium abundances in the system are similar to those in another known planet-hosting wide binary stellar system, 16 Cyg. In both systems the lithium is undetected in the atmosphere of the visual secondary harboring the planetary companion but is easily detected in the spectrum of the visual primary. We discuss this similarity and its ramifications. C1 Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Observ Geneva, CH-1290 Sauverny, Switzerland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Grenoble 1, Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. Observ Haute Provence, F-04870 St Michel lObserv, France. RP Zucker, S (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. NR 42 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 MAR 20 PY 2002 VL 568 IS 1 BP 363 EP 368 DI 10.1086/338892 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 531VN UT WOS:000174438100036 ER PT J AU Charbonneau, D Brown, TM Noyes, RW Gilliland, RL AF Charbonneau, D Brown, TM Noyes, RW Gilliland, RL TI Detection of an extrasolar planet atmosphere SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; planetary systems; stars : atmospheres; stars : individual (HD 209458); techniques : photometric ID DWARF GLIESE 229B; ALL-SKY SURVEY; GIANT PLANETS; TAU-BOOTIS; SPECTRA; TRANSIT; SEARCH; HD-209458; 51-PEG-B; LIGHT AB We report high-precision spectrophotometric observations of four planetary transits of HD 209458, in the region of the sodium resonance doublet at 589.3 nm. We find that the photometric dimming during transit in a bandpass centered on the sodium feature is deeper by (2.32 +/- 0.57) x 10(-4) relative to simultaneous observations of the transit in adjacent bands. We interpret this additional dimming as absorption from sodium in the planetary atmosphere, as recently predicted from several theoretical modeling efforts. Our model for a cloudless planetary atmosphere with a solar abundance of sodium in atomic form predicts more sodium absorption than we observe. There are several possibilities that may account for this reduced amplitude, including reaction of atomic sodium into molecular gases and/or condensates, photoionization of sodium by the stellar flux, a low primordial abundance of sodium, and the presence of clouds high in the atmosphere. C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP CALTECH, Dept Astron, 105-24,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM dc@astro.caltech.edu; timbrown@hao.ucar.edu; rnoyes@cfa.harvard.edu; gillil@stsci.edu OI Charbonneau, David/0000-0002-9003-484X NR 45 TC 673 Z9 674 U1 9 U2 36 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2002 VL 568 IS 1 BP 377 EP 384 DI 10.1086/338770 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 531VN UT WOS:000174438100038 ER PT J AU Michels, JG Raymond, JC Bertaux, JL Quemerais, E Lallement, R Ko, YK Spadaro, D Gardner, LD Giordano, S O'Neal, R Fineschi, S Kohl, JL Benna, C Ciaravella, A Romoli, M Judge, D AF Michels, JG Raymond, JC Bertaux, JL Quemerais, E Lallement, R Ko, YK Spadaro, D Gardner, LD Giordano, S O'Neal, R Fineschi, S Kohl, JL Benna, C Ciaravella, A Romoli, M Judge, D TI The helium focusing cone of the local interstellar medium close to the Sun SO ASTROPHYSICAL JOURNAL LA English DT Article DE interplanetary medium; solar wind; ultraviolet : solar system ID PICKUP IONS; SOLAR-WIND; HELIOSPHERE; PARAMETERS; SOHO; IONIZATION; HYDROGEN; EMISSION; ULYSSES; GAS AB The Solar and Heliospheric Observatory (SOHO) Ultraviolet Coronagraph Spectrometer is used to observe the interplanetary He focusing cone within 1 AU. Taken over 2 yr and from differing orbit positions, the series of observations includes measurements of He I 584 Angstrom and Lybeta intensities. The cone itself is spatially well defined, and the He I intensity within the cone was 45 R in 1996 December, compared with similar to1 R for lines of sight outward from 1 AU. Between 1996 December and 1998 June, the focusing cone dimmed by a factor of 3.3 as the level of solar activity rose. This is the first time that interstellar helium is observed so near the Sun. Measured intensities are compared to a detailed temperature and density model of interstellar helium in the solar system. The model includes EUV ionization but does not include ionization by electron impact from solar wind electrons. There are several features in the data model comparison that we attribute to the absence of electron impact ionization in the model. The absolute maximum intensity of 45 R first measured in 1996 December calls for an ionization 45% more intense than the EUV photoionization alone as measured by the Solar EUV Monitor/Charge, Element, and Isotope Analysis System (SEM/CELIAS) on SOHO. Important day-to-day variations of the intensity are observed, as well as a general decrease as the solar activity rises ( both absolute and divided by a model with a constant ionization). This general decrease is even larger than predicted by a model run with the SEM/CELIAS photoionization rate alone, in spite of a factor of 1.5 increase of this rate from 1996 December to 1998 June. At this time, an additional ionization rate of 0.56 x 10(-7) s(-1) (compared with 1.00 x 10(-7) s(-1) from solar EUV) is required to fit the measured low intensity. We attribute this additional rate to solar wind electron impact ionization of the atoms. This shows that the helium intensity pattern is a very sensitive indicator of the electron density and temperature near the Sun. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ, Princeton Mat Inst, Princeton, NJ 08540 USA. CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. Osserv Astrofis Catania, I-95125 Catania, Italy. Osserv Astron Torino, I-10025 Pino Torinese, Italy. Univ Florence, I-50125 Florence, Italy. Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA. RP Michels, JG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Romoli, Marco/H-6859-2012; OI Spadaro, Daniele/0000-0003-3517-8688; Ciaravella, Angela/0000-0002-3127-8078; Benna, Carlo/0000-0003-1688-2434; Giordano, Silvio/0000-0002-3468-8566 NR 27 TC 22 Z9 22 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2002 VL 568 IS 1 BP 385 EP 395 DI 10.1086/338764 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 531VN UT WOS:000174438100039 ER PT J AU Balakrishnan, N Yan, M Dalgarno, A AF Balakrishnan, N Yan, M Dalgarno, A TI Quantum-mechanical study of rotational and vibrational transitions in CO induced by H atoms SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; molecular data; molecular processes ID HOT HYDROGEN-ATOMS; UNIMOLECULAR DISSOCIATION; RESONANCE ENERGIES; FUNDAMENTAL BANDS; CARBON-MONOXIDE; EMISSION-LINES; SN 1987A; HCO; EXCITATION; SPECTRUM AB We report rate coefficients for rotational and vibrational transitions in CO induced by H atoms using quantum-mechanical scattering calculations and the H-CO interaction potential of Keller et al. We use the infinite-order sudden approximation for vibrational transitions and the close-coupling method for rotational transitions. Rate coefficients are presented for temperatures 5 K < T < 3000 K. Differences of a factor of 30 are found for rate coefficients for low temperatures below 100 K compared to earlier results of Green and Thaddeus. The discrepancies are attributed to the differences in the details of the interaction potentials, especially the long-range part to which the low-temperature rate coefficients are most sensitive. There is good spectroscopic evidence that the potential-energy surface employed here reproduces the resonance energies and widths of the HCO system better than any previously available HCO interaction potentials. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Balakrishnan, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 42 Z9 42 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2002 VL 568 IS 1 BP 443 EP 447 DI 10.1086/321434 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 531VN UT WOS:000174438100046 ER PT J AU Krems, RV AF Krems, RV TI Vibrational relaxation of vibrationally and rotationally excited CO molecules by He atoms SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID POTENTIAL-ENERGY SURFACE; INELASTIC-COLLISIONS; INFRARED-SPECTRUM; COORDINATE DEPENDENCE; STATES APPROXIMATION; SCATTERING THEORY; CROSS-SECTIONS; QUANTUM; HE+CO; DEACTIVATION AB This work presents a detailed quantum mechanical study of rovibrationally inelastic He+CO collisions in a wide range of translational and internal energies of the collision partners. Fully converged coupled states calculations of rate constants for vibrational relaxation of CO(v=1) by He are found to be in excellent agreement with experimental measurements at temperatures between 35 and 1500 K. The role of rotational energy for vibrational relaxation of CO is investigated and it is illustrated that the CO molecules in the first excited vibrational state can exhibit near-resonant vibrational relaxation when they are initially in high rotational excitation and the collision energy is small. A reduced channel coupled states approach neglecting low vibrational states in the basis set is implemented for calculations of rate constants for vibrational and rotational energy transfer in collisions of vibrationally excited CO molecules with He atoms. It is shown that initial vibrational excitation significantly increases rate constants for vibrationally inelastic collisions but does not affect purely rotational energy transfer. (C) 2002 American Institute of Physics. C1 Univ Gothenburg, Dept Chem, SE-41296 Gothenburg, Sweden. RP Krems, RV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 57 TC 24 Z9 24 U1 1 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 15 PY 2002 VL 116 IS 11 BP 4517 EP 4524 DI 10.1063/1.1451061 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 527WC UT WOS:000174210100016 ER PT J AU Krems, RV AF Krems, RV TI Vibrational relaxation in CO plus He collisions: Sensitivity to interaction potential and details of quantum calculations SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MOLECULAR-SCATTERING THEORY; INTERACTION ENERGY SURFACE; COORDINATE DEPENDENCE; STATES APPROXIMATION; INELASTIC-COLLISIONS; HE+CO AB The present work investigates the sensitivity of cross sections for vibrational relaxation in He+CO collisions to details of quantum coupled-states calculations and the choice of vibrational wave functions used for evaluation of the coupling matrix elements. It is illustrated that the J-labeled coupled-states (CS) approach provides results in close agreement with accurate close coupling calculations and experimental measurements while the l-labeled approximation leads to cross sections underestimating the accurate data by a large factor. It is shown that centrifugal distortion of vibrational wave functions enhances cross sections for vibrational relaxation by approximately an energy independent factor. It is found that vibrationally inelastic cross sections are more sensitive to high-order terms in the Legendre expansion of the interaction potential when the J-labeled CS approach and the accurate vibrational wave functions with centrifugal distortion are used for the calculations. (C) 2002 American Institute of Physics. C1 Univ Gothenburg, Dept Chem, SE-41296 Gothenburg, Sweden. RP Krems, RV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 20 Z9 20 U1 1 U2 5 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 MAR 15 PY 2002 VL 116 IS 11 BP 4525 EP 4529 DI 10.1063/1.1451062 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 527WC UT WOS:000174210100017 ER PT J AU Baer, M Mebel, AM Englman, R AF Baer, M Mebel, AM Englman, R TI Conical intersection revisited: extension to an elliptic form SO CHEMICAL PHYSICS LETTERS LA English DT Article ID BORN-OPPENHEIMER APPROXIMATION; SINGLE-SURFACE APPROXIMATIONS; SCATTERING PROCESSES; MOLECULAR-SYSTEMS; GEOMETRIC PHASE; EQUATION AB In this Letter we relate to a general 2 x 2 diabatic potential matrix for which is derived an analytic expression for the various non-adiabatic coupling terms. Its main advantage is in leading to a simple algorithm to determine the number and the kind of conical intersections one encounters in a (planar) region defined by a closed contour. This approach was tested with respect to two models, one of them is the elliptical linear model. This model was then, further, applied to simulate ab initio results obtained for the C2H molecule, (C) 2002 Elsevier Science B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Soreq NRC, Dept Phys & Appl Math, IL-81800 Yavne, Israel. Acad Sinica, Inst Atom & Mol Sci, Taipei 10764, Taiwan. RP Baer, M (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Mebel, Alexander/A-5234-2009 NR 35 TC 26 Z9 26 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD MAR 12 PY 2002 VL 354 IS 3-4 BP 243 EP 250 AR PII S0009-2614(02)00094-5 DI 10.1016/S0009-2614(02)00094-5 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 536FU UT WOS:000174690700009 ER PT J AU Carilli, CL Harris, DE Pentericci, L Rottgering, HJA Miley, GK Kurk, JD van Breugel, W AF Carilli, CL Harris, DE Pentericci, L Rottgering, HJA Miley, GK Kurk, JD van Breugel, W TI The X-ray-radio alignment in the z=2.2 radio galaxy PKS 1138-262 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : high-redshift; radio continuum : galaxies; X-rays : galaxies : clusters ID CYGNUS-A; PROTO-CLUSTER; REDSHIFT; EMISSION; HOTSPOTS AB We present high-resolution X-ray observations of the narrow-line radio galaxy PKS 1138-262 at z = 2.156 with the ACIS-S detector on the Chandra X-Ray Observatory. These observations show that the X-ray emission from 1138-262 is dominated by emission from the active galactic nucleus (AGN) with a 2-10 keV luminosity of 4 x 10(45) ergs s(-1). The relative X-ray and radio properties of the AGN in 1138-262 are similar to those seen for the AGN in the archetype powerful radio galaxy Cygnus A. Between 10% and 25% (depending on energy) of the X-ray emission from 1138-262 is spatially extended on scales of 10"-20". The extended X-ray emission is elongated, with a major axis aligned with that of the radio source. While the X-ray and radio emissions are elongated on similar scales and position angles, there is no one-to-one correspondence between the radio and X-ray features in the source. The most likely origin for the extended X-ray emission in 1138-262 is thermal emission from shocked gas, although we cannot rule out a contribution from inverse Compton emission. If the emission is from hot gas, then the gas density is 0.05 cm(-3) and the gas mass is 2.5 x 10(12) M.. The pressure in this hot gas is adequate to confine the radio-emitting plasma and the optical line-emitting gas. We set an upper limit of 1.5 x 10(44) ergs s(-1) to the (rest frame) 2-10 keV luminosity of any normal cluster atmosphere associated with 1138-262. No emission was detected from any of the Lyalpha-emitting galaxies in the (proto-) cluster around 1138-262, outside of the Lyalpha halo of 1138-262 itself, to a (rest frame) 2-10 keV luminosity limit of 1.2-10(43) ergs s(-1). Emission was detected from a z = 2.183 QSO located 2' west of 1138-262 with a luminosity of 1.8 x 10(44) ergs s(-1). C1 Natl Radio Astron Observ, New Mexico Array Oeprat Ctr, VLA, VLBA, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astron Observ, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Leiden Univ, Dept Astron, Leiden Observ, NL-2300 RA Leiden, Netherlands. Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. RP Carilli, CL (reprint author), Natl Radio Astron Observ, New Mexico Array Oeprat Ctr, VLA, VLBA, POB O,1003 Lopezville Rd, Socorro, NM 87801 USA. NR 38 TC 69 Z9 69 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 MAR 10 PY 2002 VL 567 IS 2 BP 781 EP 789 DI 10.1086/338669 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WF UT WOS:000174210400009 ER PT J AU Garay, G Mardones, D Rodriguez, LF Caselli, P Bourke, TL AF Garay, G Mardones, D Rodriguez, LF Caselli, P Bourke, TL TI Methanol and silicon monoxide observations toward bipolar outflows associated with Class 0 objects SO ASTROPHYSICAL JOURNAL LA English DT Review DE ISM : abundances; ISM : individual (IRAS 16293-2422, NGC 2264G, Serpens); ISM : jets and outflows; ISM : molecules; stars : formation ID YOUNG STELLAR OBJECTS; OB1 MOLECULAR CLOUD; RHO-OPHIUCHI CLOUD; GRAIN-GRAIN COLLISIONS; SMALL DARK CLOUDS; INTERSTELLAR SHOCKS; IRAS 16293-2422; STAR-FORMATION; NGC 2264G; SUBMILLIMETER CONTINUUM AB We report Swedish-ESO Submillimetre Telescope observations of seven bipolar outflows thought to be associated with Class 0 objects in the upsilon=0 J=3-->2 and J=2-->1 transitions of SiO and J(k)= 3(k)-->2(k) and J(k)=2(k)-->1k transitions of CH(3)OH. Methanol and silicon monoxide emission from outflowing gas were detected toward the lobes of four objects (NGC 2264G, IRAS 16293-2422, Serpens S68N, and Serpens SMM 4). The SiO line profiles are characteristics of C-type bow shocks, showing a peak at a radial velocity close to but displaced from the ambient cloud velocity and a gradual decrease in intensity from the peak toward higher flow velocities. There is a significant correlation between the column density of SiO and the terminal SiO flow velocity, which suggests a velocity-selective enhancement in the production of SiO molecules. We find that the SiO abundance in the lobes is enhanced with respect to that of the ambient cloud by a factor of at least 330 in IRAS 16293-2422 and SMM 4, 170 in NGC 2264G, and 80 in S68N. The abundance is enhanced by a factor of 500 in CH 3 OH IRAS 16293-2422, 330 in SMM 4, 80 in S68N, and 23 in NGC 2264G. In addition, we find that the dependence of the SiO/CO and CH(3)OH/CO abundance ratios with radial flow velocity shows a steep increase in the range from similar to0 to similar to4-5 km s(-1) and a gradual decline toward higher flow velocities. In the remaining three sources (CG 30, IRAS 13036-7644, and VLA 1623-243), emission in methanol was detected from a narrow line at the velocity of the ambient cloud, and no emission was detected in silicon monoxide. Weak methanol emission from a low-velocity outflow component was detected toward CG 30. C1 Univ Chile, Dept Astron, Santiago, Chile. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Garay, G (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. EM guido@das.uchile.cl; mardones@das.uchile.cl RI Garay, Guido/H-8840-2013; Mardones, Diego/I-5719-2016 OI Garay, Guido/0000-0003-1649-7958; NR 101 TC 38 Z9 39 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2002 VL 567 IS 2 BP 980 EP 998 DI 10.1086/338668 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WF UT WOS:000174210400027 ER PT J AU Piraino, S Santangelo, A Kaaret, P AF Piraino, S Santangelo, A Kaaret, P TI X-ray spectral and timing observations of Cygnus X-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : individual (Cygnus X-2); stars : neutron; X-rays : binaries; X-rays : general; X-rays : stars ID QUASI-PERIODIC OSCILLATIONS; MASS; BINARIES; COMPTONIZATION AB We report on a joint BeppoSAX/RXTE observation of the Z-type low-mass X-ray binary Cyg X-2. The source was in the so-called high overall intensity state and in less than 24 hr went through all three branches of the Z track. The continuum X-ray spectrum could be described by the absorbed sum of a soft thermal component, modeled as either a blackbody or a multicolor disk blackbody, and a Comptonized component. The timing power spectrum showed several components, including quasi-periodic oscillations in the range 28-50 Hz while the source was on the horizontal branch (horizontal branch oscillation; HBO). We found that the HBO frequency was well correlated with the parameters of the soft thermal component in the X-ray spectrum. We discuss implications of this correlation for models of the HBO. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist Fis Cosm Applicaz Informat, I-90146 Palermo, Italy. RP Piraino, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM piraino@ifcai.pa.cnr.it; pkaaret@cfa.harvard.edu OI Piraino, Santina/0000-0003-0122-6899 NR 31 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2002 VL 567 IS 2 BP 1091 EP 1101 DI 10.1086/338037 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WF UT WOS:000174210400036 ER PT J AU Evans, NR Sasselov, DD Short, CI AF Evans, NR Sasselov, DD Short, CI TI Polaris: Amplitude, period change, and companions SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : visual; Cepheids; stars : atmospheres; stars : individual (Polaris, alpha Ursae Minoris); stars : oscillations ID LATE-TYPE GIANTS; NONVARIABLE SUPERGIANTS; CEPHEID VARIABLES; RADIAL-VELOCITY; ALPHA-PERSEI; STARS; LUMINOSITY; DISTRIBUTIONS; CLUSTER; MASSES AB Polaris has presented us with the rare phenomenon of a Cepheid with a pulsation amplitude that has decreased over the last 50 yr. In this study we have used this property to see whether the amplitude decrease during the last 15 yr has had any effect on upper atmosphere heating. We obtained IUE high- and low-resolution spectra but found no change in either the Mg II chromospheric emission or the flux at 1800 Angstrom between 1978 and 1993 when the pulsation amplitude dropped by 50% (from 2.8 to 1.6 km s(-1)). The energy distribution from 1700 Angstrom through V, B, R(KC), and I(KC) is like that of a nonvariable supergiant of the same color rather than a full amplitude Cepheid in that it has more flux at 1800 Angstrom than the full amplitude Cepheid delta Cep. Polaris also has a rapidly changing period (3.2 s yr(-1)), in common with other overtone pulsators. We argue that this is a natural consequence of the different envelope locations that dominate pulsation growth rates in fundamental and overtone pulsation. In fundamental mode pulsators, the deeper envelope is more important in determining growth rates than for overtone pulsators. For fundamental mode pulsators, evolutionary changes in the radius produce approximately linear changes in period. In overtone pulsators, pulsation reacts to small evolutionary changes in a more unstable way because the modes are more sensitive to high envelope features such as opacity bumps, and the growth rates for the many closely spaced overtone modes change easily. Finally, the upper limit to the X-ray flux from an Einstein observation implies that the companion in the astrometric orbit is earlier than F4 V. The combination of upper and lower limits on the companion from IUE and Einstein respectively catch the companion mass between 1.7 and 1.4 M-circle dot. The X-ray limit is consistent with the more distant companion alpha UMi B being a physical companion in a hierarchal triple system. However the X-ray limits require that the even more distant companions a UMi C and D are too old to be physically associated with Polaris. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Florida Atlantic Univ, Dept Phys, Boca Raton, FL 33431 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 54 TC 24 Z9 24 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2002 VL 567 IS 2 BP 1121 EP 1130 DI 10.1086/338583 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WF UT WOS:000174210400039 ER PT J AU Marengo, M Sasselov, DD Karovska, M Papaliolios, C Armstrong, JT AF Marengo, M Sasselov, DD Karovska, M Papaliolios, C Armstrong, JT TI Theoretical limb darkening for pulsating Cepheids SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; stars : atmospheres; stars : oscillations; techniques : interferometric ID FUNDAMENTAL PARAMETERS; MODEL ATMOSPHERES; COEFFICIENTS; STAR AB Ground-based interferometry has finally reached a stage in which accurate determination of Cepheid diameters using the Baade-Wesselink method is feasible. Determining these diameters is the basis for calibrating the period-luminosity relation for classical Cepheids, and thus the extragalactic distance scale, but requires accurate limb-darkened models. This work presents a new method to compute time- and wavelength-dependent center-to-limb brightness distributions for classical Cepheids. Our model atmospheres are based on second-order accurate one-dimensional hydrodynamic calculations performed in spherical geometry. The brightness intensity distributions and the resulting limb darkening are computed through the dynamic atmospheres by using a full set of atomic and molecular opacities. Our results confirm important differences with respect to equivalent hydrostatic models. The amount of limb darkening and the shape of the limb profiles show a strong dependence on the pulsational phase of the Cepheid, which cannot be reproduced by static models. Nonlinear effects in our hydrodynamic equations add a new level of complexity in the wavelength dependence of our limb profiles, which are affected by the presence of shock waves traveling through the atmosphere. These effects, already detectable by present-day interferometers, should be taken into consideration when deriving limb-darkened diameters for nearby Cepheids with the accuracy required to measure their radial pulsations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 33 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 MAR 10 PY 2002 VL 567 IS 2 BP 1131 EP 1139 DI 10.1086/338684 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WF UT WOS:000174210400040 ER PT J AU Torres, G Ribas, I AF Torres, G Ribas, I TI Absolute dimensions of the M-type eclipsing binary YY Geminorum (Castor C): A challenge to evolutionary models in the lower main sequence SO ASTROPHYSICAL JOURNAL LA English DT Review DE binaries : eclipsing; binaries : spectroscopic; stars : fundamental parameters; stars : individual (YY Geminorum); stars : low-mass, brown dwarfs ID LOW-MASS STARS; M-CIRCLE-DOT; HERTZSPRUNG-RUSSELL DIAGRAMS; COLOR-MAGNITUDE DIAGRAMS; STELLAR MODELS; LATE-F; SPECTROSCOPIC BINARIES; BOLOMETRIC CORRECTIONS; EFFECTIVE TEMPERATURE; OPEN CLUSTERS AB We present new spectroscopic observations of the detached late-type double-lined eclipsing binary YY Geminorum (P=0.814 day), a member of the Castor sextuple system and one of the benchmarks for the comparison between observations and stellar evolution theory in the lower main sequence. In addition, we have reanalyzed existing light curves in several passbands using modern techniques that account for the conspicuous presence of spots. This, combined with the spectroscopy, has yielded a very precise determination of the absolute dimensions of the components, which are virtually identical to each other. We obtain for the mean mass, radius, and effective temperature the values M=0.5992+/-0.0047 M-circle dot, R=0.6191+/-0.0057 R-circle dot, and T-eff = 3820+/-100 K, respectively. Both the mass and the radius determinations are good to better than 1%, which in the case of the radius represents a fourfold improvement over previous results and signifintly enhances the value of this quantity for testing the models. We discuss the importance of systematic effects in these measurements by comparison with another high-precision determination of the mass by Segransan and coworkers. A reanalysis of the Hipparcos transit data for Castor AB that accounts for the relative motion of the pair in its 467 yr period orbit has yielded an improved parallax for the system of 66.90+/-0.63 mas. With this, we have estimated the age (similar to370 Myr) and metal abundance ([Fe/H]similar to0.0) of YY Gem from isochrone fits to Castor A and B under the assumption of a common origin. This, along with the other physical properties, allow for an unusually stringent test of the models for low-mass stars. We have compared the observations of YY Gem with a large number of recent theoretical calculations, and we show that all models underestimate the radius by up to 20% and that most overestimate the effective temperature by 150 K or more. Both of these trends are confirmed by observations of another similar system in the Hyades (V818 Tau). Consequently, theoretical ages for relatively low mass objects such as T Tauri stars derived by placing them on the H-R diagram may be considerably biased. If the radius is used directly as a measure of evolution, ages could be underestimated by as much as a factor of 10 in this mass regime. In view of these discrepancies, absolute ages from essentially all current models for the lower main sequence must be viewed with at least some measure of skepticism. Finally, we derive a new and very accurate ephemeris based on all available times of eclipse, and we lay to rest previous claims of sudden changes in the orbital period of the binary, which we show to be spurious. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Ribas, Ignasi/M-2134-2014 OI Ribas, Ignasi/0000-0002-6689-0312 NR 143 TC 191 Z9 194 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2002 VL 567 IS 2 BP 1140 EP 1165 DI 10.1086/338587 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WF UT WOS:000174210400041 ER PT J AU Wood, K Lada, CJ Bjorkman, JE Kenyon, SJ Whitney, B Wolff, MJ AF Wood, K Lada, CJ Bjorkman, JE Kenyon, SJ Whitney, B Wolff, MJ TI Infrared signatures of protoplanetary disk evolution SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; dust, extinction; radiative transfer; scattering; stars : pre-main-sequence ID T-TAURI-STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; ROTATING PROTOSTARS; RADIATIVE-TRANSFER; IRAS OBSERVATIONS; DUST; SYSTEMS AB We investigate the observational signatures of a straightforward evolutionary scenario for protoplanetary disks, in which the disk mass of small (less than or similar to50 mum) particles decreases homologously with time, but the disk structure and stellar parameters do not change. Our goal is to identify optimal infrared spectral indicators of the existence of disks, their structure, and mass evolution that may be tested with the upcoming SIRTF mission. We present simulated spectral energy distributions (SEDs) and colors over a wide range of masses, 10(-8) M-circle dot less than or equal to M-disk less than or equal to 10(-1) M-circle dot. Our Monte Carlo radiative equilibrium techniques enable us to explore the wide range of optical depths of these disks and incorporate multiple, anisotropic dust scattering. The SED is most sensitive to disk mass in the far-IR and longer wavelengths, as is already known from millimeter and radio observations. As the disk mass decreases, the excess emission of the disk over the stellar photosphere diminishes more rapidly at the longest than at short wavelengths. At near-infrared wavelengths, the disk remains optically thick to stellar radiation over a wide range of disk masses, resulting in a slower decline in the SED in this spectral regime. Therefore, near-IR excesses (K-L) provide a robust means of detecting disks in star clusters down to M(disk)similar to10(-7) M-circle dot, while the far-IR excess probes the disk mass, the caveat being that large inner-disk holes can decrease the near-IR disk emission. Various other disk parameters (outer radius, flaring, and dust size distribution) alter the SED quantitatively, but do not change our general conclusions on the evolution of SEDs and colors with the mass of small particles in the disk. Reducing the disk mass results in a clear progression in color-color diagrams, with low-mass disks displaying the bluest colors. We interpret color-color diagrams for Taurus-Auriga sources in the context of decreasing disk mass. Different viewing angles yield degeneracies in the color-mass relationship, but highly inclined disks are very faint and red and are readily identified in color-magnitude diagrams. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toledo, Ritter Observ, Dept Phys & Astron, Toledo, OH 43606 USA. Space Sci Inst, Boulder, CO 80303 USA. RP Wood, K (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. OI Kenyon, Scott/0000-0003-0214-609X NR 68 TC 76 Z9 76 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2002 VL 567 IS 2 BP 1183 EP 1191 DI 10.1086/338662 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WF UT WOS:000174210400043 ER PT J AU Elvis, M Marengo, M Karovska, M AF Elvis, M Marengo, M Karovska, M TI Smoking quasars: A new source for cosmic dust SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust extinction; galaxies : abundances; intergalactic medium; quasars : general ID CIRCUMSTELLAR DUST; INFRARED-EMISSION; INTERGALACTIC DUST; HOT GAS; STARS; GALAXIES; VARIABLES; RADIATION; ENVELOPES; GRAINS AB Although dust is widely found in astrophysics, forming dust is surprisingly difficult. The proper combination of low temperature (<2000 K) and high density is mainly found in the winds of late-type giant and supergiant stars that, as a result, are the most efficient sources of dust known. Dust ejected from these stars into the interstellar medium has multiple important effects, including obscuring background objects and enhancing star formation. We show here that quasars are also naturally copious producers of dust, if the gas clouds producing their characteristic broad lines are part of an outflowing wind. This offers an explanation for the strong link between quasars and dust and for the heavy nuclear obscuration around many quasars and introduces a new means of forming dust at early cosmological times. 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 36 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 MAR 10 PY 2002 VL 567 IS 2 BP L107 EP L110 DI 10.1086/340006 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WG UT WOS:000174210500002 ER PT J AU Jones, C Forman, W Vikhlinin, A Markevitch, M David, L Warmflash, A Murray, S Nulsen, PEJ AF Jones, C Forman, W Vikhlinin, A Markevitch, M David, L Warmflash, A Murray, S Nulsen, PEJ TI Chandra observations of NGC 4636 - An elliptical galaxy in turmoil SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4636); X-rays : galaxies ID RAY-EMITTING GAS; RESOLUTION X-RAY; COOLING FLOWS; ROSAT; NGC-4636; CLUSTER AB Chandra images show symmetric, 8 kpc long, armlike features in the X-ray halo surrounding NGC 4636. The leading edges of these features are sharp and are accompanied by temperature increases of similar to30%. These properties suggest that the armlike structures are produced by shocks, driven by symmetric off-center outbursts. We interpret these observations as part of a cycle in which the cooling gas originally fueled a nuclear outburst about 3 x 10(6) yr ago that led to shocks reheating the cooling gas and thus preventing the accumulation of significant amounts of cooled gas in the galaxy center and temporarily starving the central active galactic nucleus. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Wollongong, Dept Engn Phys, Wollongong, NSW 2522, Australia. RP Jones, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-31, Cambridge, MA 02138 USA. OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 NR 26 TC 127 Z9 127 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 MAR 10 PY 2002 VL 567 IS 2 BP L115 EP L118 DI 10.1086/340114 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WG UT WOS:000174210500004 ER PT J AU Migliazzo, JM Gaensler, BM Backer, DC Stappers, BW van der Swaluw, E Strom, RG AF Migliazzo, JM Gaensler, BM Backer, DC Stappers, BW van der Swaluw, E Strom, RG TI Proper-motion measurements of pulsar B1951+32 in the supernova remnant CTB 80 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (CTB 80); pulsars : individual (PSR B1951+32); radio continuum : ISM; stars : neutron; supernova remnants ID X-RAY PULSAR; EMISSION; EVOLUTION; SHELL AB Using the Very Large Array and the Pie Town antenna, we have measured the position of the radio pulsar B1951+32 relative to nearby background radio sources at four epochs between 1989 and 2000. These data show a clear motion for the pulsar of 25+/-4 mas yr(-1) at a position angle 252degrees+/-7degrees (north through east), corresponding to a transverse velocity 240+/-40 km s(-1) for a distance to the source of 2 kpc. The measured direction of motion confirms that the pulsar is moving away from the center of its associated supernova remnant, the first time that such a result has been demonstrated. Independent of assumptions made about the pulsar birthplace, we show that the measured proper motion implies an age for the pulsar of 64+/-18 kyr, somewhat less than its characteristic age of 107 kyr. This discrepancy can be explained if the initial spin period of the pulsar was P-0 = 27+/-6 ms. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. ASTRON, NL-7990 AA Dwingeloo, Netherlands. Dublin Inst Adv Studies, Dublin 2, Ireland. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Migliazzo, JM (reprint author), MIT, Ctr Space Res, 70 Vassar St, Cambridge, MA 02139 USA. RI Gaensler, Bryan/F-8655-2010 NR 30 TC 58 Z9 59 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2002 VL 567 IS 2 BP L141 EP L144 DI 10.1086/340002 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WG UT WOS:000174210500010 ER PT J AU Monnier, JD Tuthill, PG Danchi, WC AF Monnier, JD Tuthill, PG Danchi, WC TI Proper motions of new dust in the colliding wind binary WR 140 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; circumstellar matter; stars : individual (WR 98a, WR 104, WR 137, WR 140); stars : winds, outflows; stars : Wolf-Rayet ID MULTIFREQUENCY VARIATIONS; PINWHEEL NEBULA; RADIO-EMISSION; HD-193793; TELESCOPE; ASTRONOMY; SHELL; STARS; PHASE AB The eccentric W-R + O binary system WR 140 produces dust for a few months at intervals of 7.94 yr coincident with periastron passage. We present the first resolved images of this dust shell, at binary phases phi similar to 0.039 and similar to 0.055, using aperture masking techniques on the Keck I telescope to achieve diffraction-limited resolution. Proper motions of approximately 1.1 mas per day were detected, implying a distance less than or similar to1.5 kpc from the known wind speed. The dust plume observed is not as simple as the "pinwheel" nebulae seen around other W-R colliding wind binaries, indicating the orbital plane is highly inclined to our line of sight and/or the dust formation is very clumpy. Follow-up imaging in the mid-infrared and with adaptive optics is urgently required to track the dust motion further, necessary for unambiguously determining the orbital geometry, which we only partially constrain here. With full knowledge of the orbital elements, these infrared images can be used to reconstruct the dust distribution along the colliding wind interface, providing a unique tool for probing the postshock physical conditions of violent astrophysical flows. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Monnier, JD (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42,60 Garden St, Cambridge, MA 02138 USA. EM jmonnier@cfa.harvard.edu; gekko@physics.usyd.edu.au; wcd@iri1.gsfc.nasa.gov OI Monnier, John D/0000-0002-3380-3307 NR 25 TC 42 Z9 42 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 MAR 10 PY 2002 VL 567 IS 2 BP L137 EP L140 DI 10.1086/340005 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WG UT WOS:000174210500009 ER PT J AU Krebs, E AF Krebs, E TI Pierre Verger: Parisian trickster SO AMERICAN ANTHROPOLOGIST LA English DT Review C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Krebs, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 4 TC 3 Z9 3 U1 0 U2 2 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 USA SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD MAR PY 2002 VL 104 IS 1 BP 307 EP 310 DI 10.1525/aa.2002.104.1.307 PG 4 WC Anthropology SC Anthropology GA 536YR UT WOS:000174729900034 ER PT J AU Linares, OF AF Linares, OF TI Commodities and globalization: Anthropological perspectives. SO AMERICAN ANTHROPOLOGIST LA English DT Book Review C1 Smithsonian Trop Res Inst, Washington, DC 20560 USA. RP Linares, OF (reprint author), Smithsonian Trop Res Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 USA SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD MAR PY 2002 VL 104 IS 1 BP 358 EP 359 DI 10.1525/aa.2002.104.1.358 PG 2 WC Anthropology SC Anthropology GA 536YR UT WOS:000174729900057 ER PT J AU Meggers, BJ AF Meggers, BJ TI Consequences of cultivar diffusion. SO AMERICAN ANTHROPOLOGIST LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Meggers, BJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 USA SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD MAR PY 2002 VL 104 IS 1 BP 372 EP 373 DI 10.1525/aa.2002.104.1.372 PG 2 WC Anthropology SC Anthropology GA 536YR UT WOS:000174729900069 ER PT J AU Bilby, K AF Bilby, K TI The Gullah people and their African heritage. SO AMERICAN ANTHROPOLOGIST LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Bilby, K (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 USA SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD MAR PY 2002 VL 104 IS 1 BP 373 EP 374 DI 10.1525/aa.2002.104.1.373 PG 2 WC Anthropology SC Anthropology GA 536YR UT WOS:000174729900070 ER PT J AU Sakai, S AF Sakai, S TI Aristolochia spp. (Aristolochiaceae) pollinated by flies breeding on decomposing flowers in Panama SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Diptera; Drosophilidae; flower-breeding pollinator; Panama; Phoridae; tropical forest ID GALL MIDGE POLLINATION; THRIPS POLLINATION; DIPTERA; EVOLUTION; MUTUALISM; FOREST; ANGIOSPERMS; PHORIDAE; MORACEAE; CYCAD AB This study presents breeding and pollination systems of Aristolochia maxima and A. inflata in a seasonal tropical forest of Panama. Aristolochia is the most diverse genus of Aristolochiaceae, with similar to120 species distributed throughout the tropics and subtropics. All the Aristolochia species studied so far are pollinated by saprophagous flies of different families, which are presumably deceived by floral odor Flowers of many species have trap-and-release mechanisms. The flowers attract and imprison pollinators during the female stage first day of flowering and release them after anther dehiscence Pollination systems of A. maxima and A. inflata are different from those of other Aristolochia in lacking trap mechanisms. Furthermore, the pollinators oviposit in the flowers, and their larvae brow on the fallen, decaying flowers on the ground. Therefore, the plants have a mutualistic relationship with their pollinators. Self-compatible A. inflata is pollinated by Megaselia sakaiae (Phoridae, Diptera). The pollinator may be specialized to Aristolochia flowers, which is the only substrate for larval development. On the other hand, self-incompatible A. maxima is pollinated by Drosophila spp. (Drosophilidae, Diptera), which utilize Aristolochia flowers as a breeding site only occasionally This pollination mutualism might have evolved from deceit pollination. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Sakai, S (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. NR 66 TC 42 Z9 46 U1 4 U2 15 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 MAR PY 2002 VL 89 IS 3 BP 527 EP 534 DI 10.3732/ajb.89.3.527 PG 8 WC Plant Sciences SC Plant Sciences GA 595FT UT WOS:000178098300021 PM 21665652 ER PT J AU Rose, JA Gaba, AE Christiansen, WA Davis, DS Caldwell, N Hunstead, RW Hollitt, MJ AF Rose, JA Gaba, AE Christiansen, WA Davis, DS Caldwell, N Hunstead, RW Hollitt, MJ TI Multiple merging events in the double cluster A3128/A3125 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD galaxies : evolution ID X-RAY-CLUSTERS; SHAPLEY SUPERCLUSTER; GALAXY CLUSTERS; UNIVERSE; EMISSION; SUBSTRUCTURE; CATALOG; PLASMAS; SAMPLE; MERGER AB Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20 ks Chandra ACIS-I image of the central 16' x 16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM). The most striking large-scale feature in the galaxy distribution is a relatively underpopulated redshift zone similar to4000 km s(-1) on either side of the mean cluster velocity at similar to17,500 km s(-1). We attribute this depletion zone to the effect of the extensive Horologium-Reticulum (H-R) supercluster, within which A3128/A3125 is embedded. In addition to this large-scale feature, numerous smaller groups of galaxies can be identified, particularly within the underpopulated region within +/-4000 km s(-1) of the mean cluster redshift. Because of the large gravitational influence of the H-R supercluster, these groups arrive at A3128 with a high infall velocity, well in excess of the local sound speed. Two of these groups appear as elongated laments in position-velocity diagrams, indicating that they are tidally distended groups that have been disrupted after a close passage through A3128. In fact, A3125 itself appears to be in such a postpassage condition. We have identified a primary northeast-southwest merger axis connecting A3128 with A3125, along which the laments are also oriented. In addition, the Chandra image reveals that the X-ray emission is split into two components, each with very small core radii, that are separated by similar to1 Mpc along the northeast-southwest axis. We have combined the redshift, X-ray, and radio data to propose that the complex X-ray morphology revealed in the Chandra image is likely the result of a hypersonic infall of a relatively small group into A3128. The group produces a major disruption in the ICM as a result of its high infall velocity. C1 Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys A29, Sydney, NSW 2006, Australia. Univ Adelaide, Dept Phys & Math Phys, Adelaide, SA 5005, Australia. Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Rose, JA (reprint author), Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. RI Johnston-Hollitt, Melanie/B-1803-2013 NR 62 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 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2002 VL 123 IS 3 BP 1216 EP 1246 DI 10.1086/339183 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 534KN UT WOS:000174585700007 ER PT J AU Wilner, DJ Wright, MCH Di Francesco, J AF Wilner, DJ Wright, MCH Di Francesco, J TI Search for molecular gas in the quasar SDSS 1044-0125 at z=5.73 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : ISM; quasars : individual (SDSSp J104433.04-012502.2); radio emission lines ID INFRARED GALAXIES; DUST AB We report upper limits on CO J = 2-1 and J = 5-4 emission from the quasar SDSSp J104433.04-012502.2, at z = 5.73, from observations made with the Berkeley-Illinois-Maryland Association array. Previously reported limits on CO J = 6 5 emission were obtained at z = 5. 80, which is now thought to be off by 1%, and the observations likely missed the relevant redshifts for molecular gas. The new 3 sigma upper limits on the line luminosities are L-CO'(2-1) < 5.1 x 10(10) K km s(-1) pc(2) and L-CO'(5-4) < 3.0 x 10(10) K km s(-1) pc(2), assuming 200 km s(-1) line width. The CO J = 5-4 observations place an upper limit on warm, dense molecular gas mass comparable to amounts derived for some other high-redshift quasar systems from detections of this line. The limit on CO J = 2 1 emission suggests that excitation bias does not affect this conclusion. In addition, no companion galaxies rich in molecular gas are found in a similar to1.4 Mpc field surrounding the quasar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 0 Z9 0 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2002 VL 123 IS 3 BP 1288 EP 1291 DI 10.1086/338854 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 534KN UT WOS:000174585700010 ER PT J AU Rebull, LM Makidon, RB Strom, SE Hillenbrand, LA Birmingham, A Patten, BM Jones, BF Yagi, H Adams, MT AF Rebull, LM Makidon, RB Strom, SE Hillenbrand, LA Birmingham, A Patten, BM Jones, BF Yagi, H Adams, MT TI Circumstellar disk candidates identified in NGC 2264 SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 2264); stars : pre-main-sequence ID ORION-NEBULA-CLUSTER; INITIAL MASS FUNCTION; STAR-FORMING HISTORY; MAIN-SEQUENCE TRACKS; STELLAR POPULATION; MONOCEROS OB1; DARK CLOUD; NGC-2264; PHOTOMETRY; ULTRAVIOLET AB We present an optical and near-infrared study of a 45' x 45' field in NGC 2264, which includes both S Mon and the Cone Nebula. We report photometry at optical (UBVRCIC) and near-infrared (JHK) wavelengths for similar to5600 stars and spectroscopic classifications for similar to400 of these stars. We identify circumstellar disk candidates using three techniques: excess ultraviolet ( U V) emission, excess near-IR (I-K and H-K) emission, and Halpha emission-line equivalent widths for those stars with spectra. We find generally good correlation between disk indicators thought to originate from different physical processes. We find little if any evolution of disk fraction with stellar age or mass. However, when we derive mass accretion rates ((M)over dot) from the excess emission at U, we find that (M)over dot decreases with age over the age range spanned by our data, similar to0.1-5 Myr, and increases with mass over the range similar to0.25-1 M-circle dot. These findings are comparable to results found previously by us in the Orion Nebula cluster flanking fields. C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Natl Opt Astron Observ, Tucson, AZ USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Amherst Coll, Five Coll Astron Dept, Amherst, MA 01002 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Univ Massachusetts, Five Coll Dept Astron, Amherst, MA 01003 USA. Univ Texas, McDonald Observ, Ft Davis, TX 79734 USA. RP Rebull, LM (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr,Mail Stop 169-506, Pasadena, CA 91109 USA. OI Rebull, Luisa/0000-0001-6381-515X NR 40 TC 87 Z9 87 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 MAR PY 2002 VL 123 IS 3 BP 1528 EP 1547 DI 10.1086/338904 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 534KN UT WOS:000174585700028 ER PT J AU Koo, BC Lee, JJ Seward, FD AF Koo, BC Lee, JJ Seward, FD TI An ASCA study of the W51 complex SO ASTRONOMICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (W51); stars : formation; supernova remnants; X-rays : ISM ID X-RAY-EMISSION; SUPERNOVA REMNANT; MOLECULAR CLOUD; H-I; STARS; MODELS; GALAXY; LINE; CO AB We present the analysis of ASCA archival data from the Galactic source W51. The ASCA spectra show that the soft (kT less than or similar to 2.5 keV) X-rays are of thermal origin and are compatible with W51C being a single isothermal (kT similar or equal to 0.3 keV) supernova remnant at the far side of the Sagittarius arm. The ASCA images reveal hard (kT greater than or similar to 2.5 keV) X-ray sources that were not seen in previous X-ray observations. Some of these sources are coincident with massive star-forming regions, and the spectra are used to derive X-ray parameters. By comparing the X-ray absorbing column density with atomic hydrogen column density, we infer the location of star-forming regions relative to molecular clouds. There are unidentified hard X-ray sources superposed on the supernova remnant, and we discuss the possibility of their association. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Seoul Natl Univ, Astron Program, SEES, Seoul 151742, South Korea. RP Koo, BC (reprint author), Seoul Natl Univ, Astron Program, SEES, Seoul 151742, South Korea. 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 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2002 VL 123 IS 3 BP 1629 EP 1638 DI 10.1086/339179 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 534KN UT WOS:000174585700034 ER PT J AU Torres, G Neuhauser, R Guenther, EW AF Torres, G Neuhauser, R Guenther, EW TI Spectroscopic binaries in a sample of ROSAT X-ray sources south of the taurus molecular clouds SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; stars : activity; stars : evolution; stars : pre-main-sequence; X-rays ID ALL-SKY SURVEY; HIGH-RESOLUTION SPECTROSCOPY; SOLAR-TYPE STARS; CHROMOSPHERICALLY ACTIVE STARS; RS-CANUM-VENATICORUM; OPEN CLUSTER M-67; LOW-MASS; RADIAL-VELOCITIES; FORMING REGION; AURIGA AB We report the results of our radial velocity monitoring of spectroscopic binary systems in a sample of X-ray sources from the ROSAT All Sky Survey south of the Taurus-Auriga star-forming region. The original sample of similar to120 sources by Neuhauser et al. was selected on the basis of their X-ray properties and the visual magnitude of the nearest optical counterpart, in such a way as to promote the inclusion of young objects. Roughly 20% of those sources have previously been confirmed to be very young. We focus here on the subset of the original sample that shows variable radial velocities ( 43 objects), a few of which have also been flagged previously as being young. New spectroscopic orbits are presented for 42 of those systems. Two of the binaries, RX J0528.9+1046 and RX J0529.3+1210, are indeed weak-lined T Tauri stars likely to be associated with the lambda Ori region. Most of the other binaries are active objects of the RS Canum Venaticorum type, including several W Ursae Majoris and Algol systems. We detect a strong excess of short-period binaries compared with the field and an unusually large fraction of double-lined systems. This, along with the overall high frequency of binaries out of the original sample of similar to120 sources, can be understood as a selection effect, since all these properties tend to favor the inclusion of the objects in a flux-limited X-ray survey such as this by making them brighter in X-rays. A short description of the physical properties of each binary is provided, and a comparison with evolutionary tracks is made using the stellar density as a distance-independent measure of evolution. We rely for this on our new determinations of the effective temperature and projected rotational velocities of all visible components of the binaries. A number of the systems merit follow-up observations, including at least four confirmed or probable eclipsing binaries. One of these, RX J0239.1-1028, consists of a pair of detached K dwarfs and may provide for a potentially important test of stellar evolution models once the absolute dimensions of the components are determined. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Karl Schwarzschild Observ, Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 52 TC 60 Z9 60 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2002 VL 123 IS 3 BP 1701 EP 1722 DI 10.1086/339178 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 534KN UT WOS:000174585700037 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, SJ Bromley, BC TI Collisional cascades in planetesimal disks. I. Stellar flybys SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : formation; solar system : formation; stars : formation ID EDGEWORTH-KUIPER BELT; MAIN-SEQUENCE STARS; PICTORIS CIRCUMSTELLAR DISK; N-BODY SIMULATION; SOLAR-TYPE STARS; VEGA-LIKE STARS; BETA-PICTORIS; PLANETARY ACCRETION; DUST DISK; HR 4796A AB We use a new multiannulus planetesimal accretion code to investigate the evolution of a planetesimal disk following a moderately close encounter with a passing star. The calculations include fragmentation, gas and Poynting-Robertson drag, and velocity evolution from dynamical friction and viscous stirring. We assume that the stellar encounter increases planetesimal velocities to the shattering velocity, initiating a collisional cascade in the disk. During the early stages of our calculations, erosive collisions damp particle velocities and produce substantial amounts of dust. For a wide range of initial conditions and input parameters, the time evolution of the dust luminosity follows a simple relation, L(d)/L(*) = L(0)/[alpha+(t/t(d))(beta)]. The maximum dust luminosity L(0) and the damping time t(d) depend on the disk mass, with L(0) proportional to M(d) and t(d) proportional to M(d)(-1). For disks with dust masses of 1%-100% of the minimum-mass solar nebula (1-100 M(circle plus) at 30-150 AU), our calculations yield t(d) similar to 1-10 Myr, alpha approximate to 1-2, beta = 1, and dust luminosities similar to the range observed in known debris disk systems, L(0) similar to 10(-3) to 10(-5). Less massive disks produce smaller dust luminosities and damp on longer timescales. Because encounters with field stars are rare, these results imply that moderately close stellar flybys cannot explain collisional cascades in debris disk systems with stellar ages of 100 Myr or longer. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X NR 95 TC 61 Z9 61 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2002 VL 123 IS 3 BP 1757 EP 1775 DI 10.1086/338850 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 534KN UT WOS:000174585700041 ER PT J AU Andrievsky, SM Bersier, D Kovtyukh, VV Luck, RE Maciel, WJ Lepine, JRD Beletsky, AV AF Andrievsky, SM Bersier, D Kovtyukh, VV Luck, RE Maciel, WJ Lepine, JRD Beletsky, AV TI Using Cepheids to determine the galactic abundance gradient - II. Towards the galactic center SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : abundances; stars : Cepheids; Galaxy : abundances; Galaxy : evolution ID MOLECULAR CLOUDS; OPEN CLUSTERS; KINEMATICS; EVOLUTION; DISK; BAR AB Based on spectra obtained at the Anglo-Australian Observatory, we present a discussion of the metallicity of the galactic disc derived using Cepheids at galactocentric distances of 4-6 kpc. Our new results together with previous gradient determination (Paper I) show that the overall abundance distribution within the galactocentric distances 4-11 kpc cannot be represented by a single gradient value. The distribution is more likely bimodal: it is flatter in the solar neighbourhood with a small gradient, and steepens towards the galactic center. The steepening begins at a distance of about 6.6 kpc. C1 Univ Sao Paulo, Inst Astron & Geofis, BR-4200 Sao Paulo, Brazil. Odessa II Mechnikov State Univ, Dept Astron, UA-65014 Odessa, Ukraine. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Odessa Astron Observ, Odessa, Ukraine. Isaac Newton Inst Chile, Odessa Branch, Odessa, Ukraine. Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. RP Andrievsky, SM (reprint author), Univ Sao Paulo, Inst Astron & Geofis, Avv Miguel Stefano, BR-4200 Sao Paulo, Brazil. NR 18 TC 107 Z9 110 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2002 VL 384 IS 1 BP 140 EP 144 DI 10.1051/0004-6361:20020016 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527KP UT WOS:000174185500013 ER PT J AU Beuther, H Schilke, P Sridharan, TK Menten, KM Walmsley, CM Wyrowski, F AF Beuther, H Schilke, P Sridharan, TK Menten, KM Walmsley, CM Wyrowski, F TI Massive molecular outflows SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE molecular data; turbulence; stars : early type; stars : formation; ISM : jets and outflows ID YOUNG STELLAR OBJECTS; STAR-FORMATION REGIONS; CO LINE FORMATION; BIPOLAR FLOWS; EVOLUTION; COLLAPSE AB With the aim of understanding the role of massive outflows in high-mass star formation, we mapped in the (CO)-C-12 J = 2 - 1 transition 26 high-mass star-forming regions at very early stages of their evolution. At a spatial resolution of 11" bipolar molecular outflows were found in 21 of them. The other five sources show confusing morphology but strong line wings. This high detection rate of bipolar structure proves that outflows common in low-mass sources are also ubiquitous phenomena in the formation process of massive stars. The flows are large, very massive and energetic, and the data indicate stronger collimation than previously thought. The dynamical timescales of the flows correspond well to the free-fall timescales of the associated cores. Comparing with correlations known for low-mass flows, we find continuity up to the high-mass regime suggesting similar flow-formation scenarios for all masses and luminosities. Accretion rate estimates in the 10(4) L. range are around 10(4) M. yr(-1), higher than required for low-mass star formation, but consistent with high-mass star formation scenarios. Additionally, we find a tight correlation between the outflow mass and the core mass over many orders of magnitude. The strong correlation between those two quantities implies that the product of the accretion efficiency f(acc) = (M) over dot (acc)/(M-core/t(ff)) and f(r) (the ratio between jet mass loss rate and accretion rate), which equals the ratio between jet and core mass (f(acc)f(r) = M-jet/M-core), is roughly constant for all core masses. This again indicates that the flow-formation processes are similar over a large range of masses. Additionally, we estimate median f(r) and f(acc) values of approximately 0.2 and 0.01, respectively, which is consistent with current jet-entrainment models. To summarize, the analysis of the bipolar outflow data strongly supports theories which explain massive star formation by scaled up, but otherwise similar physical processes - mainly accretion - to their low-mass counterparts. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Beuther, H (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. NR 46 TC 307 Z9 310 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 MAR PY 2002 VL 383 IS 3 BP 892 EP 904 DI 10.1051/0004-6361:20011808 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527KN UT WOS:000174185400019 ER PT J AU Ventura, R Spadaro, D Uzzo, M Suleiman, R AF Ventura, R Spadaro, D Uzzo, M Suleiman, R TI UV line intensity and flow velocity distributions in two coronal mass ejections as deduced by UVCS-SOHO observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : corona; Sun : UV radiation ID SOLAR CORONA; SPECTROMETER; SIGNATURES; UVCS/SOHO; ERUPTION; EMISSION; FLARES AB The Ultraviolet Coronagraph Spectrometer (UVCS) instrument onboard the SOHO satellite observed two coronal mass ejections on November 2 and 3, 2000, related to the eruptions of a large filament structure in an active region close to the West limb of the Sun, and of a prominence near the South Pole, respectively. Intensity and profile of the O VI resonance doublet lines at 1032 and 1037 Angstrom and of Lybeta (1026 Angstrom) line, together with the intensity of some other minor ions, were observed using the O VI channel of UVCS. We analysed these spectroscopic observations in order to get information about the distributions of ionic densities and flow velocities in the solar coronal plasma ejected during these transient events. Emission in ions ranging from C II to O VI indicates a temperature range between 10(4.5) and 10(5.5) K. The morphology of the bright emission regions suggests the development of several strands of plasma irregularly distributed inside the CME structures, whose temporal evolution is significantly different from each other. The velocities determined for each bright element also give a complex picture of the plasma kinematics characterizing these coronal mass ejections. C1 Osserv Astrofis Catania, I-95125 Catania, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ventura, R (reprint author), Osserv Astrofis Catania, Citta Univ,Via S Sofia 78, I-95125 Catania, Italy. RI Ventura, Rita/B-7524-2016; OI Ventura, Rita/0000-0002-5152-0482; Spadaro, Daniele/0000-0003-3517-8688 NR 27 TC 5 Z9 5 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2002 VL 383 IS 3 BP 1032 EP 1048 DI 10.1051/0004-6361:20011802 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527KN UT WOS:000174185400031 ER PT J AU Nelson, AE Simard, L Zaritsky, D Dalcanton, JJ Gonzalez, AH AF Nelson, AE Simard, L Zaritsky, D Dalcanton, JJ Gonzalez, AH TI Constraints on the size evolution of brightest cluster galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : formation ID VELOCITY DISPERSIONS; ELLIPTICAL GALAXIES; ABSOLUTE MAGNITUDES; SURFACE PHOTOMETRY; FUNDAMENTAL PLANE; DISTANT CLUSTERS; LUMINOSITY; PARAMETERS; DYNAMICS; MEMBERS AB We measure the luminosity profiles of 16 brightest cluster galaxies (BCGs) at 0.4 < z < 0.8 using high-resolution F160W NICMOS and F814W WFPC2 Hubble Space Telescope imaging. The heterogeneous sample is drawn from a variety of surveys : seven from clusters in the Einstein Medium Sensitivity Survey, five from the Las Campanas Distant Cluster Survey and its Northern Hemisphere precursor, and the remaining four from traditional optical surveys. We find that the surface brightness profiles of all but three of these BCGs are well described by a standard de Vaucouleurs (r(1/4)) profile out to at least similar to2r(e) and that the biweight-estimated NICMOS effective radius of our high-redshift BCGs (r(e) = 8.3 +/- 1.4 kpc for H-0 = 80 km s(-1) Mpc(-1), Omega(m) = 0.2, Omega(Lambda) = 0.0) is similar to2 times smaller than that measured for a local BCG sample. If high-redshift BCGs are in dynamical equilibrium and satisfy the same scaling relations as low-redshift ones, this change in size would correspond to a mass growth of a factor of 2 since z similar to 0.5. However, the biweight-estimated WFPC2 effective radius of our sample is 18 +/- 5.1 kpc, which is fully consistent with the local sample. While we can rule out mass accretion rates higher than a factor of 2 in our sample, the discrepancy between our NICMOS and WFPC2 results, which after various tests we describe appears to be physical, does not yet allow us to place strong constraints on accretion rates below that level. C1 Univ Calif Santa Cruz, Board Astron & Astrophys, Santa Cruz, CA 95064 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Washington, Seattle, WA 98195 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nelson, AE (reprint author), Univ Calif Santa Cruz, Board Astron & Astrophys, Santa Cruz, CA 95064 USA. NR 47 TC 17 Z9 17 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2002 VL 567 IS 1 BP 144 EP 154 DI 10.1086/338221 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BQ UT WOS:000174047700015 ER PT J AU Sarzi, M Rix, HW Shields, JC McIntosh, DH Ho, LC Rudnick, G Filippenko, AV Sargent, WLW Barth, AJ AF Sarzi, M Rix, HW Shields, JC McIntosh, DH Ho, LC Rudnick, G Filippenko, AV Sargent, WLW Barth, AJ TI Limits on the mass of the central black hole in 16 nearby bulges SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : bulges; galaxies : kinematics and dynamics; galaxies : nuclei; galaxies : spiral ID TELESCOPE SPECTROSCOPIC EVIDENCE; ACTIVE GALACTIC NUCLEI; IONIZED-GAS; SPIRAL GALAXIES; VELOCITY DISPERSION; CENTRAL REGION; HOST GALAXIES; STELLAR; DISK; SEARCH AB We report upper limits on the masses of black holes that can be present in the centers of 16 nearby galaxy bulges. These limits M-BH(lim) for our statistically complete sample were derived from the modeling of the central emission-line widths ([N II] or [S II]), observed over a 0."25 x 0."2 (R less than or similar to 9 pc) aperture. The experiment has a mean detection sensitivity of similar to3.9 x 10(6) M.. For three sample members with direct determinations of M-BH our upper limits agree within the uncertainties, while in general our upper limits are found to be close to the masses measured in other bulges with global properties similar to ours. Remarkably, our limits are quite close to the recently derived M-BH-sigma(*) relation. These results support a picture wherein the black hole mass and overall galaxy structure are closely linked, as galaxies with exceptionally high M-BH at a given sigma(*) apparently are rare. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. CALTECH, Palomar Observ, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM sarzi@mpia-hd.mpg.de; rix@mpia-hd.mpg.de; shields@phy.ohiou.edu; dmac@hamerkop.astro.umass.edu; lho@ociw.edu; grudnick@as.arizona.edu; alex@astro.berkeley.edu; wws@astro.caltech.edu; abarth@cfa.harvard.edu OI Barth, Aaron/0000-0002-3026-0562 NR 61 TC 33 Z9 33 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 MAR 1 PY 2002 VL 567 IS 1 BP 237 EP 246 DI 10.1086/338351 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BQ UT WOS:000174047700022 ER PT J AU Lou, YQ Walsh, WM Han, JL Fan, ZH AF Lou, YQ Walsh, WM Han, JL Fan, ZH TI Multiwavelength structural manifestations of fast magnetohydrodynamic density waves in spiral galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 2997, NGC 1097); galaxies : magnetic fields; galaxies : spiral; galaxies : structure; ISM : magnetic fields; MHD ID STAR-FORMING RINGS; MAGNETIC-FIELDS; NUMERICAL EXPERIMENTS; DISK GALAXIES; GASEOUS DISCS; NGC-6946; STELLAR; ARMS; GAS; INSTABILITY AB In a spiral galaxy, disks of stars and of magnetized interstellar medium (ISM) are dynamically coupled by gravity. The theory of magnetohydrodynamic (MHD) density waves in such a composite rotating disk system provides a basic framework for studying large-scale dynamics and multiwavelength diagnostics of galactic structures. As swirllike, trailing spiral structures with broad, fuzzy arms (regular or irregular) manifest in neutral hydrogen H I disks that are usually larger than optical spiral patterns in disk galaxies, spiral MHD density waves in H I gas disks should persist within and beyond optical patterns. Sporadic diffusions of relativistic cosmic-ray electrons beyond optical patterns may cause radio continuum arms to occasionally extend across optical spiral patterns and correlate with H I spiral arms at larger radii. We here report the first H I observations of the southern spiral galaxy NGC 2997 to support the fast MHD density wave (FMDW) scenario and to confirm the prior prediction that the isolated, polarized radio continuum arm discovered in the southeast quadrant is indeed associated with a broad segment of the H I arm. For multiwavelength observations of spiral galaxies, we emphasize the important perspective that large-scale magnetic fields of MHD density waves play the key role in organizing correlated spiral structures of the various underlying ISM components. Meanwhile, we briefly discuss the nature of circum-nuclear structures of NGC 2997 in reference to those of NGC 1097. C1 Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CAS PKU, Beijing Astrophys Ctr, Beijing 100871, Peoples R China. RP Lou, YQ (reprint author), Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China. NR 47 TC 9 Z9 9 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2002 VL 567 IS 1 BP 289 EP 293 DI 10.1086/338244 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BQ UT WOS:000174047700026 ER PT J AU Li, LX AF Li, LX TI Accretion disk torqued by a black hole SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; magnetic fields ID MAGNETIC NEUTRON STARS; BLANDFORD-ZNAJEK MECHANISM; MARGINALLY STABLE ORBIT; X-RAY SOURCES; EXTRACTING ENERGY; INSTABILITY; EVOLUTION AB If a Kerr black hole is connected to a disk rotating around it by a magnetic field, the rotational energy of the Kerr black hole provides an energy source for the radiation of the disk in addition to disk accretion. The black hole exerts a torque on the disk, which transfers energy and angular momentum between the black hole and the disk. If the black hole rotates faster than the disk, energy and angular momentum are extracted from the black hole and transferred to the disk. The energy deposited into the disk is eventually radiated away by the disk, which will increase the efficiency of the disk. If the black hole rotates slower than the disk, energy and angular momentum are transferred from the disk to the black hole, which will lower the efficiency of the disk. With suitable boundary conditions, quasi-steady state solutions are obtained for a thin Keplerian disk magnetically coupled to a Kerr black hole. By "quasi-steady state" we mean that any macroscopic quantity at a given radius in the disk slowly changes with time: the integrated change within one rotation period of the disk is much smaller than the quantity itself. We find that the torque produced by magnetic coupling propagates outward only in the disk, and the total radiation flux of the disk is a superposition of the radiation flux produced by magnetic coupling and that produced by accretion. Interestingly, a disk magnetically coupled to a rapidly rotating black hole can radiate without accretion : the total power of the disk comes from the rotational energy of the black hole. With a simple example that the magnetic field touches the disk at a single radius, we show that the radial radiation profile produced by magnetic coupling can be very different from that of a standard accretion disk : the emissivity index is significantly larger, and most radiation can come from a region that is closer to the center of the disk. While the shape of the radiation flux curve sensitively depends on the extension of the magnetic field in the disk, the spectral signature of magnetic coupling can be robust. The limitations of our model are briefly discussed, which include the assumption of a weak magnetic field, the ignorance of the instabilities of the disk and the magnetic field, and the ignorance of the radiation captured by the black hole and the radiation returning to the disk. C1 Princeton Univ Observ, Princeton, NJ 08544 USA. RP Li, LX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. NR 57 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 MAR 1 PY 2002 VL 567 IS 1 BP 463 EP 476 DI 10.1086/338486 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BQ UT WOS:000174047700044 ER PT J AU Heyl, JS Hernquist, L AF Heyl, JS Hernquist, L TI Hot spot emission from a freely precessing neutron star SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : neutron; stars : oscillations; X-rays : stars ID PULSARS AB Recent observations of 1E 161348-5055, the neutron star candidate at the center of the supernova remnant RCW 103, show that a component of its emission varies sinusoidally with a period of approximately 6 hours. We argue that this period is what one would expect for a freely precessing neutron star with a spin period of about 1 s. We produce light curves for a freely precessing neutron star with a hot spot. By a suitable choice of parameters, we obtain light curves which are constant with rotational phase when the flux from the star reaches a maximum. At other phases of the precession, the flux varies as the star rotates, but the total flux decreases by a factor of several. These models can explain the behavior observed from 1E 161348-5055 and predict that the spin period should be detectable at minimum flux from sufficiently sensitive measurements. C1 CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heyl, JS (reprint author), CALTECH, Mail Code 130-33, Pasadena, CA 91125 USA. NR 30 TC 7 Z9 7 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 MAR 1 PY 2002 VL 567 IS 1 BP 510 EP 514 DI 10.1086/338547 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BQ UT WOS:000174047700048 ER PT J AU Camilo, F Manchester, RN Gaensler, BM Lorimer, DR Sarkissian, J AF Camilo, F Manchester, RN Gaensler, BM Lorimer, DR Sarkissian, J TI PSR J1124-5916: Discovery of a young energetic pulsar in the supernova remnant G292.0+1.8 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G292.0+1.8); pulsars : individual (PSR J1124-5916); supernova remnants ID RADIO PULSARS; EVOLUTION; NEBULAE; LUMINOSITY; DISTANCES; SEARCH AB We report the discovery with the Parkes radio telescope of a pulsar associated with the similar to1700 yr old oxygen-rich composite supernova remnant G292.0+1.8. The pulsar PSR J1124-5916 has a period of 135 ms and a period derivative of 7.4 x 10(-13), implying a characteristic age of 2900 yr, a spin-down luminosity of 1.2 x 10(37) ergs s(-1), and a surface magnetic field strength of 1.0 x 10(13) G. Association between the pulsar and the synchrotron nebula previously identified with Chandra within this supernova remnant is confirmed by the subsequent detection of X-ray pulsations by Hughes et al. The pulsar's flux density at 1400 MHz is very small, S approximate to 80 muJy, but the radio luminosity of Sd(2) similar to 2 mJy kpc(2) is not especially small, although it is 1 order of magnitude smaller than that of the least luminous young pulsar previously known. This discovery suggests that very deep radio searches should be done for pulsations from pulsar wind nebulae in which the central pulsed source is yet to be detected and possibly from other more exotic neutron stars. C1 Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Manchester, Jodrell Bank, Macclesfield SK11 9DL, Cheshire, England. CSIRO, Australia Telescope Natl Facil, Parkes, NSW 2870, Australia. RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 550 W 120th St, New York, NY 10027 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 37 TC 94 Z9 95 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 MAR 1 PY 2002 VL 567 IS 1 BP L71 EP L75 DI 10.1086/339799 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BT UT WOS:000174047900017 ER PT J AU Markevitch, M Gonzalez, AH David, L Vikhlinin, A Murray, S Forman, W Jones, C Tucker, W AF Markevitch, M Gonzalez, AH David, L Vikhlinin, A Murray, S Forman, W Jones, C Tucker, W TI A textbook example of a bow shock in the merging galaxy cluster 1E 0657-56 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (1E 0657-56); intergalactic medium; X-rays : galaxies ID TEMPERATURE; 1E-0657-56; MERGER AB The Chandra image of the merging, hot galaxy cluster 1E 0657-56 reveals a bow shock propagating in front of a bullet-like gas cloud just exiting the disrupted cluster core. This is the first clear example of a shock front in a cluster. From the jumps in the gas density and temperature at the shock, the Mach number of the bulletlike cloud is 2-3. This corresponds to a velocity of 3000-4000 km s(-1) relative to the main cluster, which means that the cloud traversed the core just 0.1- 0.2 Gyr ago. The 6-7 keV "bullet" appears to be a remnant of a dense cooling flow region once located at the center of a merging subcluster whose outer gas has been stripped by ram pressure. The bullet's shape indicates that it is near the final stage of being destroyed by ram pressure and gasdynamic instabilities, as the subcluster galaxies move well ahead of the cool gas. The unique simplicity of the shock front and bullet geometry in 1E 0657-56 may allow a number of interesting future measurements. The cluster's average temperature is 14-15 keV but shows large spatial variations. The hottest gas (T > 20 keV) lies in the region of the radio halo enhancement and extensive merging activity involving subclusters other than the bullet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif San Diego, San Diego, CA 92103 USA. RP Markevitch, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 258 Z9 258 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 MAR 1 PY 2002 VL 567 IS 1 BP L27 EP L31 DI 10.1086/339619 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BT UT WOS:000174047900007 ER PT J AU Mazzotta, P Kaastra, JS Paerels, FB Ferrigno, C Colafrancesco, S Mewe, R Forman, WR AF Mazzotta, P Kaastra, JS Paerels, FB Ferrigno, C Colafrancesco, S Mewe, R Forman, WR TI Evidence for a heated gas bubble inside the "cooling flow" region of MKW 3s SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; galaxies : clusters : individual (MKW 3s); X-rays : galaxies ID RADIO-SOURCES; CLUSTERS; GALAXIES; SAMPLE; TEMPERATURE; ROSAT AB We report on the deep Chandra observation of the central r = 200 kpc region of the cluster of galaxies MKW 3s, which was previously identified as a moderate cooling flow cluster. The Chandra image reveals two striking features-a 100 kpc long and 21 kpc wide filament, extending from the center to the southwest, and a nearly circular, 50 kpc diameter depression 90 kpc south of the X-ray peak. The temperature map shows that the filamentary structure is colder while the surface brightness depression is hotter than the average cluster temperature at any radius. The hot and the cold regions indicate that both cooling and heating processes are taking place in the center of MKW 3s. We argue that the surface brightness depression is produced by a heated, low-density gas bubble along the line of sight. We suggest that the heated bubble is produced by short-lived nuclear outbursts from the central galaxy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SRON, Space Res Lab, NL-3584 CA Utrecht, Netherlands. Columbia Univ, Astrophys Lab, New York, NY 10027 USA. Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. RP Mazzotta, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Ferrigno, Carlo/H-4139-2012; Mazzotta, Pasquale/B-1225-2016 OI Mazzotta, Pasquale/0000-0002-5411-1748 NR 20 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 MAR 1 PY 2002 VL 567 IS 1 BP L37 EP L40 DI 10.1086/323512 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BT UT WOS:000174047900009 ER PT J AU Smith, N Gehrz, RD Hinz, PM Hoffmann, WF Mamajek, EE Meyer, MR Hora, JL AF Smith, N Gehrz, RD Hinz, PM Hoffmann, WF Mamajek, EE Meyer, MR Hora, JL TI A disrupted circumstellar torus inside eta Carinae's Homunculus Nebula SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : individual (Homunculus Nebula); stars : individual (eta Carinae) ID MIDINFRARED ARRAY CAMERA; SPECTROSCOPY; ASTRONOMY; RING AB We present thermal infrared images of the bipolar nebula surrounding eta Carinae at six wavelengths from 4.8 to 24.5 mum. These were obtained with the MIRAC3 camera system at the Magellan Observatory. Our images reveal new intricate structure in the bright core of the nebula, allowing us to reevaluate interpretations of morphology seen in images with lower resolution. Complex structures in the core might not arise from a pair of overlapping rings or a cool (110 K) and very massive dust torus, as has been suggested recently. Instead, it seems more likely that the arcs and compact knots comprise a warm (200-350 K) disrupted torus at the intersection of the larger polar lobes. Some of the arcs appear to break out of the inner core region and may be associated with equatorial features seen in optical images. The torus could have been disrupted by a posteruption stellar wind or by ejecta from the Great Eruption itself if the torus existed before that event. Kinematic data are required to rule out either possibility. C1 Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, N (reprint author), Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 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 MAR 1 PY 2002 VL 567 IS 1 BP L77 EP L80 DI 10.1086/339897 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BT UT WOS:000174047900018 ER PT J AU Winebarger, AR Warren, H van Ballegooijen, A DeLuca, EE Golub, L AF Winebarger, AR Warren, H van Ballegooijen, A DeLuca, EE Golub, L TI Steady flows detected in extreme-ultraviolet loops SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona ID TRANSITION-REGION; CORONAL EXPLORER; SUMER TELESCOPE; SOLAR CORONA; PROFILES; TRACE; SOHO; SPECTROMETER; TEMPERATURE; DYNAMICS AB Recent Transition Region and Coronal Explorer (TRACE) observations have detected a class of active region loops whose physical properties are inconsistent with previous hydrostatic loop models. In this Letter we present the first co-aligned TRACE and the Solar Ultraviolet Measurement of Emitted Radiation (SUMER) observations of these loops. Although these loops appear static in the TRACE images, SUMER detects line-of-sight flows along the loops of up to 40 km s(-1). The presence of flows could imply an asymmetric heating function; such a heating function would be expected for heating that is proportional to (often asymmetric) footpoint field strength. We compare a steady flow solution resulting from an asymmetric heating function to a static solution resulting from a uniform heating function in a hypothetical coronal loop. We find that the characteristics associated with the asymmetrically heated loop better compare with the characteristics of the loops observed in the TRACE data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP USN, Res Lab, Code 7673W, Washington, DC 20375 USA. EM awinebarger@cfa.harvard.edu; hwarren@cfa.harvard.edu; avanballegooijen@cfa.harvard.edu; edeluca@cfa.harvard.edu; lgolub@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen, Adriaan/0000-0002-5622-3540; Golub, Leon/0000-0001-9638-3082 NR 20 TC 97 Z9 97 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 MAR 1 PY 2002 VL 567 IS 1 BP L89 EP L92 DI 10.1086/339796 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525BT UT WOS:000174047900021 ER PT J AU Bird, WL AF Bird, WL TI Advertising progress: American business and the rise of consumer marketing. SO BUSINESS HISTORY REVIEW LA English DT Book Review C1 Smithsonian Natl Museum Amer Hist, Polit Campaign Collect, Washington, DC USA. RP Bird, WL (reprint author), Smithsonian Natl Museum Amer Hist, Polit Campaign Collect, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 3 PU HARVARD BUSINESS SCHOOL PI BOSTON PA BUSINESS HISTORY REVIEW, 60 HARVARD WAY, BOSTON, MA 02163 USA SN 0007-6805 J9 BUS HIST REV JI Bus. Hist. Rev. PD SPR PY 2002 VL 76 IS 1 BP 139 EP 141 PG 3 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA 550LC UT WOS:000175503700007 ER PT J AU Lagarde, F Bonnet, X Nagy, K Henen, B Corbin, J Naulleau, G AF Lagarde, F Bonnet, X Nagy, K Henen, B Corbin, J Naulleau, G TI A short spring before a long jump: the ecological challenge to the steppe tortoise (Testudo horsfieldi) SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID DESERT TORTOISES; GOPHERUS-AGASSIZII; POPULATION; HERMANNI; BUDGETS AB The steppe tortoise (Testudo horsfieldi) is probably the most widespread and abundant of all living terrestrial tortoises, but paradoxically, this chelonian as been studied only superficially. Steppe tortoise populations are declining rapidly as a result of massive harvesting for the pet trade and extensive disruption of their habitat by intensive agriculture. Thus, it is urgent to acquire accurate information on major life-history traits. Our 5-year field study at the Djeiron Ecocenter in the Republic of Uzbekistan indicates that steppe tortoises usually remain buried in one place for over 9 months, which helps them cope with the extreme environmental conditions that occur in summer, fall, and winter. After emerging in late winter, steppe tortoises have less than 3 months in spring to forage to obtain the fuel needed for growth and reproduction, and replenish the body reserves necessary for the subsequent 9 months of total starvation. The mating period occurred between the end of March and mid-April and the egg-laying period from the end of April to mid-June. Using radio-tracking and focal sampling, we measured the time devoted to different activities by males and females. During the mating period, males allocated a large proportion of their daily activity to sexual behaviours, whereas females' sexual activity tended to be cryptic. However, males devoted less time to feeding and resting than did females. During the postmating period, both males and females spent much time foraging. The strong sexual divergences indicate that each sex copes differently with the extreme continental climate. The seasonal and interannual changes in body mass indicate complex interactions between climatic conditions, activity budget, and body reserves. C1 CNRS, Ctr Etud Biol Chize, F-79360 Villiers En Bois, France. Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, Los Angeles, CA 90095 USA. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. RP Lagarde, F (reprint author), CNRS, Ctr Etud Biol Chize, F-79360 Villiers En Bois, France. RI Henen, Brian/S-6552-2016 OI Henen, Brian/0000-0003-3412-4944 NR 42 TC 32 Z9 34 U1 1 U2 6 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD MAR PY 2002 VL 80 IS 3 BP 493 EP 502 DI 10.1139/Z02-032 PG 10 WC Zoology SC Zoology GA 541XG UT WOS:000175011400012 ER PT J AU Komai, T Lemaitre, R AF Komai, T Lemaitre, R TI A new species of Bathypaguropsis McLaughlin, 1994 from Japan, and redescription of B-kuroshioensis (Miyake, 1978) (Decapoda, Anomura, Paguridae) SO CRUSTACEANA LA English DT Article ID HERMIT-CRABS; GENUS AB A new species of the genus Bathypaguropsis McLaughlin, 1994, B. foresti, is described from off Boso Peninsula, central Japan. The assignment of Pagurus kuroshioensis Miyake, 1978 to Bathypaguropsis is confirmed based on examination of the holotype and supplemental material. Bathypaguropsis rahayuae McLaughlin, 1997 is found to be a junior subjective synonym of B. kuroshioensis, which is redescribed and illustrated in detail. Morphological similarities of B. foresti and B. kuroshioensis are discussed. A key to aid in the identification of the species of the genus Bathypaguropsis is presented. C1 Nat Hist Museum, Chuo Ku, Chiba 2608682, Japan. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Komai, T (reprint author), Nat Hist Museum, Chuo Ku, 955-2 Aoba Cho, Chiba 2608682, Japan. NR 11 TC 4 Z9 5 U1 0 U2 1 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD MAR-APR PY 2002 VL 75 BP 423 EP 441 DI 10.1163/156854002760095499 PN 3-4 PG 19 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 587ET UT WOS:000177628100017 ER PT J AU Longino, JT Coddington, J Colwell, RK AF Longino, JT Coddington, J Colwell, RK TI The ant fauna of a tropical rain forest: Estimating species richness three different ways SO ECOLOGY LA English DT Article DE abundance distribution; ants; biodiversity; Costa Rica; Formicidae; incidence-based coverage estimator; inventories, species; La Selva; lognormal; Michaelis-Menten; richness estimation; species accumulation curves; tropical rain forest ID LOGNORMAL DISTRIBUTIONS; AMAZONIAN FOREST; SAMPLE COVERAGE; POPULATION-SIZE; COSTA-RICA; DIVERSITY; BIODIVERSITY; CONSERVATION; HYMENOPTERA; FORMICIDAE AB Species richness is an important characteristic of ecological communities, but it is difficult to quantify. We report here a thorough inventory of a tropical rain forest ant fauna and use it to evaluate species richness estimators. The study was carried out in similar to1500 ha of lowland rain forest at La Selva Biological Station, Costa Rica. Diverse methods were used, including canopy fogging, Malaise traps, Berlese samples, Winkler samples, baiting, and manual search. Workers of 437 ant species were encountered. The abundance distribution was clearly lognormal, and the distribution emerged from a veil line with each doubling of sampling effort. Three richness estimates were calculated: the area under the fitted lognormal distribution, the asymptote of the Michaelis-Menten equation fit to the species accumulation curve, and the Incidence-based Coverage Estimator (ICE). The performance of the estimators was evaluated with sample-based rarefaction plots. The inventory was nearly complete because the species accumulation curve approached an asymptote, the richness estimates were very close to the observed species richness, and the uniques and duplicates curves were both declining. None of the richness estimators was stable in sample-based rarefaction plots, but regions of stability of estimators occurred. The explanation of rarity is one key to understanding why richness estimates fail. Fifty-one species (12% of the total) were still uniques (known from only one sample) at the end of the inventory. The rarity of 20 of these species was explained by "edge effects": "methodological edge species" (possibly abundant at the site but difficult to sample because of their microhabitat), and "geographic edge species," known to be common in habitats or regions outside of La Selva. Rarity of 31 species remained unexplained. Most of the 51 rare species were known from additional collections outside of La Selva, either in other parts of Costa Rica or in other countries. Only six species were "global uniques," known to date from only one sample on Earth. The study demonstrates that patterns of species occurrence early in an inventory may be inadequate to estimate species richness, but that relatively complete inventories of species-rich arthropod communities are possible if multiple sampling methods and extensive effort are applied. C1 Evergreen State Coll, Olympia, WA 98505 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Entomol, Washington, DC 20560 USA. Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. RP Longino, JT (reprint author), Evergreen State Coll, Olympia, WA 98505 USA. EM longinoj@evergreen.edu RI Colwell, Robert/C-7276-2015 NR 83 TC 340 Z9 367 U1 7 U2 113 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD MAR PY 2002 VL 83 IS 3 BP 689 EP 702 DI 10.1890/0012-9658(2002)083[0689:TAFOAT]2.0.CO;2 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 523QY UT WOS:000173967500011 ER PT J AU Lovelock, CE Miller, R AF Lovelock, CE Miller, R TI Heterogeneity in inoculum potential and effectiveness of arbuscular mycorrhizal fungi SO ECOLOGY LA English DT Article DE Acer rubrum; arbuscular mycorrhizae; inoculum potential; Maryland, USA; Quercus falcata; temperate forest; treefall gaps ID PLANT COMMUNITY STRUCTURE; TREE SOIL INTERACTIONS; SPATIAL PATTERNS; TROPICAL AUSTRALIA; FLOODPLAIN FORESTS; TEMPERATE FORESTS; SEEDLING GROWTH; USE EFFICIENCY; KAKADU REGION; JARRAH FOREST AB Arbuscular mycorrhizae are symbiotic associations among glomalean fungi and plant roots that often lead to enhanced water and nutrient uptake and plant growth. We describe experiments to test whether inoculum potential of arbuscular mycorrhizal (AM) fungal communities varies spatially within a broadleaf temperate forest, and also whether there is variability in the effectiveness of AM fungal communities in enhancing seedling growth. Inoculum potential of arbuscular mycorrhizal fungi in a temperate broad-leaved forest did not vary significantly among sites. Inoculum potential, measured as the extent to which the roots of red maple seedlings that had been germinated on sterile sand and then transplanted into the forest, were colonized by AM fungi, was similar in floodplain and higher elevation sites. It was as similar under ectomycorrhizal oaks as it was under red maples and other AM tree species. It was also similar among sites with deciduous understory shrubs with arbuscular mycorrhizae (spicebush, Lindera benzoin) and those with evergreen vegetation with ericoid mycorrhizae (mountain laurel, Kalmia latifolia). Where spicebush was the dominant understory shrub, inoculum potential was greater under gaps in the canopy than within the understory. Survivorship of transplanted red maple seedlings varied significantly over sites but was not strongly correlated with measures of inoculum potential. In a greenhouse growth experiment, arbuscular mycorrhizal fungal communities obtained from tree roots from the forest had different effects on plant growth. Seedlings inoculated with roots of red maple had twice the leaf area after 10 wk of growth compared to the AM community obtained from roots of southern red oaks. Thus, although there appears to be little heterogeneity in inoculum potential in the forest, there are differences in the effectiveness of different inocula. These effects have the potential to affect tree species diversity in forests by modifying patterns of seedling recruitment. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Melbourne, Sch Bot, Melbourne, Vic, Australia. RP Lovelock, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; MILLER, REBECCA/0000-0003-2785-0024 NR 71 TC 16 Z9 20 U1 2 U2 19 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD MAR PY 2002 VL 83 IS 3 BP 823 EP 832 DI 10.2307/3071884 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 523QY UT WOS:000173967500021 ER PT J AU Miller, AW Hewitt, CL Ruiz, GM AF Miller, AW Hewitt, CL Ruiz, GM TI Invasion success: does size really matter? SO ECOLOGY LETTERS LA English DT Article DE body size; marine bivalves; invasion success; non-indigenous species; oyster transport ID BIOLOGICAL INVASIONS; MARINE AB The recent paper by Roy et al. (2001) presents a compelling relationship between range Emit shafts, climatic fluctuations, and body size for marine bivalves in the fossil record. However, their extension of body size as a correlate for contemporary, marine bivalve introductions is problematic and requires further scrutiny. Unlike their analysis of the fossil assemblage, the approach used for contemporary invasions does not adequately control for dispersal mechanism (vector) or source region. First, their analysis included mariculture species, intentionally introduced because of their large size, creating a vector-specific bias. Second, successful invaders from multiple source regions (Northern Hemisphere) were compared with potential invaders from a single source region (northeastern Pacific), leaving both source and vector as uncontrolled variables. We present an analysis of body size for bivalve introductions from a single vector and source region, indicating no correlation between body size and invasion success when eliminating intentional introduction, source region and transport vector as confounding factors. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Calif Los Angeles, Environm Sci & Engn Program, Los Angeles, CA USA. CSIRO Marine Res, Ctr Res Introduced Marine Pests, Marmion, WA 6020, Australia. RP Miller, AW (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Hewitt, Chad/C-4460-2008; Ross, Donald/F-7607-2012; OI Hewitt, Chad/0000-0002-6859-6512; Ross, Donald/0000-0002-8659-3833; Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X NR 21 TC 20 Z9 21 U1 0 U2 6 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD MAR PY 2002 VL 5 IS 2 BP 159 EP 162 DI 10.1046/j.1461-0248.2002.00306.x PG 4 WC Ecology SC Environmental Sciences & Ecology GA 543UF UT WOS:000175119000001 ER PT J AU Briceno, RD Eberhard, WG AF Briceno, RD Eberhard, WG TI Courtship in the medfly, Ceratitis capitata, includes tactile stimulation with the male's aristae SO ENTOMOLOGIA EXPERIMENTALIS ET APPLICATA LA English DT Article DE medfly; courtship stimuli; female choice; Diptera; Tephritidae ID TEPHRITIDAE; DIPTERA; BEHAVIOR; WILD AB Male Ceratitis capitata (Wiedemann) (Diptera: Tephritidae) used their aristae to repeatedly tap the female, usually on her aristae, during the second stage of head rocking courtship. The male's antennae moved in an apparently exploratory manner earlier in head rocking. Reduced rates of copulation followed removal of male and female aristae, supporting the idea that tapping with the aristae is an important part of medfly courtship. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. NR 14 TC 10 Z9 12 U1 0 U2 4 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0013-8703 J9 ENTOMOL EXP APPL JI Entomol. Exp. Appl. PD MAR PY 2002 VL 102 IS 3 BP 221 EP 228 DI 10.1046/j.1570-7458.2002.00943.x PG 8 WC Entomology SC Entomology GA 579GH UT WOS:000177169900002 ER PT J AU Froeschner, RC Miller, LT AF Froeschner, RC Miller, LT TI Corythucha melissae, a new species of lace bug (Heteroptera : Tingidae) from Manzanita in California SO ENTOMOLOGICAL NEWS LA English DT Article AB Description and illustrations for a new species, Corythucha melissae, collected on manzanita, the ericaceous plant Arctostaphylos regismontana Eastwood in California. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Froeschner, RC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. NR 3 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 0013-872X J9 ENTOMOL NEWS JI Entomol. News PD MAR-APR PY 2002 VL 113 IS 2 BP 94 EP 96 PG 3 WC Entomology SC Entomology GA 567EQ UT WOS:000176472800004 ER PT J AU Pandolfi, JM Lovelock, CE Budd, AF AF Pandolfi, JM Lovelock, CE Budd, AF TI Character release following extinction in a Caribbean reef coral species complex SO EVOLUTION LA English DT Review DE biological interaction; character release; coral reefs; corals; evolution; Pleistocene; species complex ID MONTASTRAEA-ANNULARIS COMPLEX; BUILDING CORAL; WEST-INDIES; SCLERACTINIAN CORALS; COMMUNITY STRUCTURE; REPRODUCTIVE CHARACTERISTICS; PLEISTOCENE CARBONATES; ENVIRONMENTAL-CHANGE; CHEILOSTOME BRYOZOA; MASS EXTINCTIONS AB The Pleistocene extinction of the widespread organ-pipe Montastraea coral had measurable morphological and ecological effects on surviving lineages of the Montastraea ''annularis" species complex. Extinction of the organ-pipe Montastraea occurred after more than 500,000 years of dominance in the shallow-water reef habitat of Barbados. Extinction resulted in a morphological shift of the columnar Montastraea lineage from thick to thin columns in modern reef environments, Pleistocene colonies of the columnar morphotype sympatric with organ-pipe Montastraea showed greater column widths than those in allopatry. We subjected our data to a number of criteria for interpreting the morphological shift as character release following lifting of competitive pressure after extinction. The morphological differences do not appear to be due either to chance or to physical properties of the marine environment. Differential local extinction and recolonization of four members of the species complex did not occur on Barbados, so that the species coexisted and appear to have coevolved between more than 600,000 and 82,000 years ago. The morphological shift is related to coral growth form and growth rate, and thus reflects the acquisition of a primary resource in corals-lights. Character release occurred at the same oceanic Caribbean island (Barbados) where environments have fluctuated with similar variance throughout the period of coexistence. Not only has competition among living members of the Montastraea "annularis" species complex been convincingly demonstrated, but trends in relative abundance among fossil members of the species complex strongly suggest that a competitive hierarchy was operating during their Pleistocene coexistence on Barbados. We also observed an ecological analogue to character release on another Caribbean island, Curacao, The distribution and abundance of living columnar M. annularis s.s. and massive M. faveolata from the leeward reef crest in Curacao is greater now than in the Pleistocene, when organ-pipe Montastraea dominated this shallow-water reef habitat. Extinction of the faster growing, shallow-water organ-pipe Montastraea resulted in higher abundance of the columnar Montastraea lineage in shallow-water habitats, where it shifted its morphology to one adapted to high light levels. The species extinction released surviving lineages from a competitive network that had resulted in lower rank abundance in the Pleistocene community and enhanced abundance of both columnar M. annularis s.s. and AT faveolata in modern communities. Full validation of our interpretation of character release must await experiments that demonstrate whether phenotypic differences between populations have a genetic basis. However, we believe the results of this study point to the important, yet heretofore neglected, role that biological interactions have played in the evolution of closely related reef coral species. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. RP Pandolfi, JM (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. EM pandolfi.john@nmnh.si.edu; lovelock@serc.si.edu; ann-budd@uiowa.edu RI Pandolfi, John/A-3121-2009; Lovelock, Catherine/G-7370-2012 OI Pandolfi, John/0000-0003-3047-6694; Lovelock, Catherine/0000-0002-2219-6855 NR 116 TC 31 Z9 36 U1 2 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD MAR PY 2002 VL 56 IS 3 BP 479 EP 501 PG 23 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 542JV UT WOS:000175040500005 PM 11989679 ER PT J AU Davies, N Bermingham, E AF Davies, N Bermingham, E TI The historical biogeography of two Caribbean butterflies (Lepidoptera : Heliconiidae) as inferred from genetic variation at multiple loci SO EVOLUTION LA English DT Article DE allozymes; island; mitochondrial DNA; phylogeography; population genetics; West Indies ID WEST-INDIES; DNA; PHYLOGEOGRAPHY; SEQUENCE AB Mitochondrial DNA and allozyme variation was examined in populations of two Neotropical butterflies, Heliconius charithonia and Dryas iulia. On the mainland, both species showed evidence of considerable gene flow over huge distances, The island populations, however, revealed significant genetic divergence across some, but not all, ocean passages. Despite the phylogenetic relatedness and broadly similar ecologies of these two butterflies, their intraspecific biogeography clearly differed. Phylogenetic analyses of mitochondrial DNA sequences revealed that populations of D iulia north of St. Vincent are monophyletic and were probably derived from South America. By contrast, the Jamaican subspecies of H. charithonia rendered West Indian H. charithonia polyphyletic with respect to the mainland populations thus, H. charithonia seems to have colonized the Greater Antilles on at least two separate occasions from Central America. Colonization velocity does not correlate with subsequent levels of gene flow in either species. Even where range expansion seems to have been instantaneous on a geological timescale, significant allele frequency differences at allozyme loci demonstrate that gene flow is severely curtailed across narrow ocean passages. Stochastic extinction, rapid (re)colonization, but low gene flow probably explain why, in the same species, some islands support genetically distinct and nonexpanding populations, while nearby a single lineage is distributed across several islands. Despite the differences, some common biogeographic patterns were evident between these butterflies and other West Indian taxa; such congruence suggests that intraspecific evolution in the West Indies has been somewhat constrained by earth history events, such as changes in sea level. C1 Smithsonian Trop Res Inst, Balbao, Ancon, Panama. RP Davies, N (reprint author), Univ Calif Berkeley, Richard B Gump S Pacific Res Stn, 101 Giannini Hall, Berkeley, CA 94720 USA. RI Davies, Neil/E-5863-2012 OI Davies, Neil/0000-0001-8085-5014 NR 39 TC 27 Z9 28 U1 0 U2 2 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD MAR PY 2002 VL 56 IS 3 BP 573 EP 589 PG 17 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 542JV UT WOS:000175040500013 PM 11989687 ER PT J AU Briceno, RD Eberhard, WG AF Briceno, RD Eberhard, WG TI Decisions during courtship by male and female medflies (diptera, tephritidae): Correlated changes in male behavior and female acceptance criteria in mass-reared flies SO FLORIDA ENTOMOLOGIST LA English DT Article DE medfly; sexual selection; courtship behavior; mass-rearing; female choice ID CERATITIS-CAPITATA DIPTERA; MEDITERRANEAN FRUIT-FLY; TRICHOPLUSIA-NI; MATING-BEHAVIOR; STERILE; CHOICE; PHEROMONE; SUCCESS; WILD AB Analyses of more than 300 videotaped courtships of wild and mass-reared medflies from Costa Rica showed that the tendency for male and female to align themselves facing directly toward each other increased, and that the distance between them decreased as courtship proceeded. More direct alignments and shorter distances between the flies at the moment the male jumped onto the female were correlated with greater female acceptance of copulation. There were no consistent differences in durations of components of intermittent buzzing songs or male size between successful and unsuccessful courtship in either strain, Several possible cues may release different courtship responses: males of both strains tend to initiate both continuous vibration and intermittent buzzing after reduction of the distance to the female; slow creeping toward the female was associated with longer courtships that had failed to lure the female close; and females tended to turn to face more directly toward the male soon after the male began continuous vibration, and especially after he began intermittent buzzing. Females became progressively more immobile as courtship progressed, especially soon after intermittent buzzing began. There were numerous differences between strains. Mass-reared males were more likely to mount females without previous courtship than were wild males. Wild males initiated continuous wing vibration when farther from the female and when the female was looking less directly toward them, but the two strains did not differ in the distances and angles at which males initiated intermittent buzzing and jumped. Wild males were more likely to creep toward the female during intermittent buzzing. Mass-reared females but not wild females were more likely to copulate when the proportion of time the male had spent in intermittent buzzing was low, and if the courtship began when the flies were nearer each other. Wild but not mass-reared females were less likely to copulate if courtship was shorter. Possible coevolution of female responses with the five different male courtship traits that differ between mass-reared and wild flies are discussed. C1 Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Smithsonian Trop Res Inst, Balboa, Panama. RP Briceno, RD (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica. NR 30 TC 39 Z9 40 U1 1 U2 3 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD MAR PY 2002 VL 85 IS 1 BP 14 EP 31 DI 10.1653/0015-4040(2002)085[0014:DDCBMA]2.0.CO;2 PG 18 WC Entomology SC Entomology GA 545DD UT WOS:000175200200002 ER PT J AU Briceno, RD Eberhard, WG Vilardi, JC Liedo, P Shelly, TE AF Briceno, RD Eberhard, WG Vilardi, JC Liedo, P Shelly, TE TI Variation in the intermittent buzzing songs of male medflies (Diptera : Tephritidae) associated with geography, mass-rearing, and courtship success SO FLORIDA ENTOMOLOGIST LA English DT Article DE courtship sounds; medfly; geographic differences ID FRUIT-FLY; DROSOPHILA; CHARACTERS AB Many aspects of the temporal pattern of sounds produced during the intermittent buzzing displays of pre-copulatory courtship by male medflies varied between wild flies from Costa Rica, Argentina, and Hawaii, and between mass-reared flies from Costa Rica, Argentina, Mexico, and Hawaii. There were no consistent differences when mass-reared strains were compared with the wild strains from the area where they originated in Costa Rica, Argentina and Hawaii. Buzzing sounds produced prior to successful mounting attempts did not differ consistently from those preceding unsuccessful mounts in flies from Costa Rica and Argentina. In strains from all sites, however, courtships in which buzzes were interrupted were more likely not to result in mounting of the female. There was a weak tendency for interruptions to be more common in mass-reared strains. C1 Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Smithsonian Trop Res Inst, Balboa, Panama. Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Ciencias Biol, Lab Genet Poblac, RA-1428 Buenos Aires, DF, Argentina. Colegio Frontera Sur, Tapachula, Chiapas, Mexico. USDA ARS, Honolulu, HI 96804 USA. RP Briceno, RD (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica. RI Liedo, Pablo/E-9313-2010 OI Liedo, Pablo/0000-0002-0004-1721 NR 21 TC 20 Z9 21 U1 0 U2 3 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD MAR PY 2002 VL 85 IS 1 BP 32 EP 40 DI 10.1653/0015-4040(2002)085[0032:VITIBS]2.0.CO;2 PG 9 WC Entomology SC Entomology GA 545DD UT WOS:000175200200003 ER PT J AU Ruiz-Miranda, CR Archer, CA Kleiman, DG AF Ruiz-Miranda, CR Archer, CA Kleiman, DG TI Acoustic differences between spontaneous and induced long calls of golden lion tamarins, Leontopithecus rosalia SO FOLIA PRIMATOLOGICA LA English DT Review DE vocalizations; playbacks; primates; bioacoustics; communication; tamarins ID LOUD CALLS; MONKEYS; TRANSMISSION; ADAPTATION; RESPONSES; PLAYBACK; PRIMATE; SONGS AB Long calls are emitted by several primate taxa and appear to have multiple functions related to spacing mechanisms and reproduction. Yet, in some species the spontaneous rate of emission of these calls is low, and playbacks are used to elicit long calls to augment the sample size of studies. The objective of this study was to compare the acoustic structure of spontaneously emitted and experimentally induced long calls of golden lion tamarins. Results from 6 adult tamarins show that spontaneously emitted long calls differ acoustically from experimentally induced long calls in several frequency measures. Several explanations for these differences are discussed. We conclude that regardless of the underlying mechanisms, playbacks elicit responses that may be different from naturally occurring calls. Copyright (C) 2002 S. Karger AG, Basel. C1 Univ Estadual Norte Fluminense, Lab Ciencias Ambietais, CBB, BR-28015620 Campos Dos Goytacazes, RJ, Brazil. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. RP Ruiz-Miranda, CR (reprint author), Univ Estadual Norte Fluminense, Lab Ciencias Ambietais, CBB, BR-28015620 Campos Dos Goytacazes, RJ, Brazil. EM cruiz@uenf.br RI Ruiz-Miranda, Carlos/A-4719-2008; Ruiz-Miranda, Carlos/H-7308-2015; Ruiz, Carlos/I-4446-2016 OI Ruiz-Miranda, Carlos/0000-0001-9786-5315; Ruiz-Miranda, Carlos/0000-0001-7360-0304; NR 34 TC 4 Z9 4 U1 1 U2 7 PU KARGER PI BASEL PA ALLSCHWILERSTRASSE 10, CH-4009 BASEL, SWITZERLAND SN 0015-5713 EI 1421-9980 J9 FOLIA PRIMATOL JI Folia Primatol. PD MAR-JUN PY 2002 VL 73 IS 2-3 BP 124 EP 131 DI 10.1159/000064791 PG 8 WC Zoology SC Zoology GA 593RY UT WOS:000178007100006 PM 12207059 ER PT J AU Hungate, BA Reichstein, M Dijkstra, P Johnson, D Hymus, G Tenhunen, JD Hinkle, CR Drake, BG AF Hungate, BA Reichstein, M Dijkstra, P Johnson, D Hymus, G Tenhunen, JD Hinkle, CR Drake, BG TI Evapotranspiration and soil water content in a scrub-oak woodland under carbon dioxide enrichment SO GLOBAL CHANGE BIOLOGY LA English DT Article DE elevated CO2; evapotranspiration; hydrology; soil water content ID ELEVATED ATMOSPHERIC CO2; CALCAREOUS GRASSLAND; REGIONAL TRANSPIRATION; TALLGRASS PRAIRIE; GAS-EXCHANGE; RESPONSES; ECOSYSTEM; PLANT; VEGETATION; NITROGEN AB Leaf conductance often decreases in response to elevated atmospheric CO2 concentration (C-a) potentially leading to changes in hydrology. We describe the hydrological responses of Florida scrub oak to elevated C-a during an eight-month period two years after C-a manipulation began. Whole-chamber gas exchange measurements revealed a consistent reduction in evapotranspiration in response to elevated C-a , despite an increase in leaf area index (LAI). Elevated C-a also increased surface soil water content, but xylem water deuterium measurements show that the dominant oaks in this system take up most of their water from the water table (which occurs at a depth of 1.5-3 m), suggesting that the water savings in elevated C-a in this system are primarily manifested as reduced water uptake at depth. Extrapolating these results to larger areas requires considering a number of processes that operate on scales beyond these accessible in this field experiment. Nevertheless, these results demonstrate the potential for reduced evapotranspiration and associated changes in hydrology in ecosystems dominated by woody vegetation in response to elevated C-a . C1 No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86001 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86001 USA. Univ Bayreuth, Dept Plant Ecol, D-95440 Bayreuth, Germany. Dynamac Corp, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Hungate, BA (reprint author), No Arizona Univ, Dept Biol Sci, Box 5640, Flagstaff, AZ 86001 USA. RI Reichstein, Markus/A-7494-2011; Hungate, Bruce/F-8991-2011 OI Reichstein, Markus/0000-0001-5736-1112; Hungate, Bruce/0000-0002-7337-1887 NR 52 TC 63 Z9 67 U1 2 U2 23 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 MAR PY 2002 VL 8 IS 3 BP 289 EP 298 DI 10.1046/j.1365-2486.2002.00468.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 541WL UT WOS:000175008800007 ER PT J AU Mawdsley, JR AF Mawdsley, JR TI Ecological notes on species of Cleridae (Insecta : Coleoptera) associated with the prairie flora of Central North America SO GREAT LAKES ENTOMOLOGIST LA English DT Article AB The association of eighteen species of Cleridae (Coleoptera) with tallgrass and shortgrass prairie ecosystems in central North America is reported for the first time. New flower visitation, habitat association, distribution, and/or rearing records are reported for Enoclerus analis (LeConte), E. coccineus coccineus (Schenkling), E. cordifer (LeConte), E. rosmarus (Say), E. zonatus (King), Placopterus thoracicus pallipes (Wolcott), Trichodes bibalteatus LeConte, T. bicinctus Green, T. nutalli (Kirby), Phyllobaenus dubius (Wolcott), P. knausii (Wickham), P. pubescens (LeConte), P. subfasciatus (LeConte), Isohydnocera albocincta (Horn), L brunnea (Horn), L curtipennis (Newman), L tricondylae (LeConte) and Wolcottia pedalis (LeConte). Diagnostic characters are presented to separate adults of P. dubius, a species endemic to the northern shortgrass prairie region, from the common and widespread P. pubescens. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Div Entomol, Washington, DC 20560 USA. RP Mawdsley, JR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Div Entomol, Washington, DC 20560 USA. NR 25 TC 3 Z9 5 U1 2 U2 5 PU MICH ENTOMOL SOC PI E LANSING PA MICH STATE UNIV DEPT ENTOMOL, E LANSING, MI 48823 USA SN 0090-0222 J9 GREAT LAKES ENTOMOL JI Gt. Lakes Entomol. PD SPR-SUM PY 2002 VL 35 IS 1 BP 15 EP 22 PG 8 WC Entomology SC Entomology GA 699PY UT WOS:000184066200003 ER PT J AU Bosch, J Rand, AS Ryan, MJ AF Bosch, J Rand, AS Ryan, MJ TI Response to variation in chuck frequency by male and female tungara frogs SO HERPETOLOGICA LA English DT Article DE communication; Physalaemus pustulosus; sexual selection; Tungara frogs ID PHYSALAEMUS-PUSTULOSUS; ACOUSTIC COMPETITION; SEXUAL SELECTION; NEOTROPICAL FROG; SIZE; CHOICE; RECOGNITION; CALL AB We examined how male and female tungara frogs, Physalaemus pustulosus, respond to variation in the frequency spectrum of the chuck component of the advertisement call. We varied chuck frequency in two different ways. In the fixed frequeucy series, the sequeuce of calls within each series had chucks of the same dominant frequency. Different fixed-frequency series had chucks of different dominant frequencies designated as high, high-medium, medium, medium-low, or low frequency relative to variation in the test population. In the second varying frequency series, the sequence of calls varied in the chuck's dominant frequency such that the individual series had the same average frequencies as the high, high-medium, medium, medium-low, and low fixed-frequency experiments. Both males and females tended to respond more to lower-frequeucy chucks. The responses of both sexes to the same mean chuck frequency was similar to the fixed- and varying frequency series of chucks. C1 CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sect Integrat Biol C0930, Austin, TX 78712 USA. RP Bosch, J (reprint author), CSIC, Museo Nacl Ciencias Nat, Jose Gutierrez Abascal 2, E-28006 Madrid, Spain. RI Bosch, Jaime/H-3042-2011; OI Bosch, Jaime/0000-0002-0099-7934 NR 31 TC 13 Z9 13 U1 0 U2 2 PU HERPETOLOGISTS LEAGUE PI EMPORIA PA EMPORIA STATE UNIV, DIVISION BIOLOGICAL SCIENCES, 1200 COMMERCIAL ST, EMPORIA, KS 66801-5087 USA SN 0018-0831 J9 HERPETOLOGICA JI Herpetologica PD MAR PY 2002 VL 58 IS 1 BP 95 EP 103 DI 10.1655/0018-0831(2002)058[0095:RTVICF]2.0.CO;2 PG 9 WC Zoology SC Zoology GA 527EB UT WOS:000174172700008 ER PT J AU Matsunaga, T Tong, CE Blundell, R Noguchi, T AF Matsunaga, T Tong, CE Blundell, R Noguchi, T TI A 600-700 GHz resonant distributed junction for a fixed-tuned waveguide receiver SO IEICE TRANSACTIONS ON ELECTRONICS LA English DT Article; Proceedings Paper CT 8th International Superconductive Electronics Conference (ISEC 01) CY JUN 19-22, 2001 CL OSAKA, JAPAN SP IEICE Electr Soc DE SIS transmission line; resonator; optical lithography; stress; receiver noise temperature ID TUNNEL-JUNCTIONS; LINE AB The non-linear quasiparticle tunnel current flowing in a distributed superconductor-insulator-superconductor (SIS) transmission line resonator has been exploited in a low-noise heterodyne fixed-tuned waveguide receiver in the 600-700GHz band. The mixer employs two half-wave or full-wave distributed SIS long junctions connected in series, These devices have been fabricated with optical lithography. At 654 GHz, a V-factor of 1.79 has been recorded, corresponding to a double-side-band (DSB) receiver noise temperature of 198 K at an IF of 3 GHz. C1 Grad Univ Adv Studies, Dept Astron Sci, Nagano 3841305, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. RP Matsunaga, T (reprint author), Grad Univ Adv Studies, Dept Astron Sci, Nagano 3841305, Japan. EM teru@nro.nao.ac.jp OI Tong, Edward/0000-0002-7736-4203 NR 12 TC 6 Z9 6 U1 0 U2 1 PU IEICE-INST ELECTRONICS INFORMATION COMMUNICATIONS ENG PI TOKYO PA KIKAI-SHINKO-KAIKAN BLDG, 3-5-8, SHIBA-KOEN, MINATO-KU, TOKYO, 105-0011, JAPAN SN 0916-8524 EI 1745-1353 J9 IEICE T ELECTRON JI IEICE Trans. Electron. PD MAR PY 2002 VL E85C IS 3 BP 738 EP 741 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA 528TB UT WOS:000174258200056 ER PT J AU Gingerich, O AF Gingerich, O TI The trouble with ptolemy SO ISIS LA English DT Article AB Ptolemy's Almagest, a brilliant treatise on theoretical astronomy combined with a practical handbook for computation, includes many compromises to reconcile discordant observations. This defense of Ptolemy examines in some detail a critical case concerning the model for Venus, which has sometimes been used as evidence for Ptolemy's perfidy. There the Alexandrian astronomer demonstrated his ingenuity when orbital constraints made it impossible to obtain directly the observed configurations he might have preferred. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 0 Z9 0 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD MAR PY 2002 VL 93 IS 1 BP 70 EP 74 DI 10.1086/343243 PG 5 WC History & Philosophy Of Science SC History & Philosophy of Science GA 562RV UT WOS:000176213500005 ER PT J AU Sillett, TS Holmes, RT AF Sillett, TS Holmes, RT TI Variation in survivorship of a migratory songbird throughout its annual cycle SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE avian demography; capture-recapture models; Dendroica caerulescens; Nearctic-Neotropical migrant birds; population ecology; seasonal and annual survival ID LIFE-HISTORY EVOLUTION; CAPTURE-RECAPTURE DATA; SURVIVAL RATES; POPULATION LIMITATION; DENDROICA-CAERULESCENS; POSTFLEDGING SURVIVAL; NEOTROPICAL MIGRANT; OVERWINTER SURVIVAL; HABITAT QUALITY; MARKED ANIMALS AB 1. Demographic data from both breeding and non-breeding periods are needed to manage populations of migratory birds, many of which are declining in abundance and are of conservation concern. Although habitat associations. and to a lesser extent, reproductive biology, are known for many migratory species. few studies have measured survival rates of these birds at different parts of their annual cycle. 2. Cormack-Jolly-Seber models and Akaike's information criterion model selection were used to investigate seasonal variation in survival of a Nearctic - Neotropical migrant songbird, the black-throated blue warbler, Dendroica caerulescens. Seasonal and annual survival,were estimated from resightings of colour-ringed individuals on breeding grounds in New Hampshire, USA from 1986 to 2000 and on winter quarters in Jamaica, West Indies from 1986 to 1999. Warblers were studied each year during the May-August breeding period in New Hampshire and during the October-March overwinter period in Jamaica. 3. In New Hampshire, males had higher annual survival (0.51 +/- 0.03) and recapture probabilities (0.93 +/- 0.03) than did females (survival: 0.40 +/- 0.04 recapture: 0.87 +/- 0.06). In Jamaica, annual survival (0.43 +/- 0.03) and recapture (0.95 +/- 0.04) probabilities did not differ between sexes. Annual survival and recapture probabilities of young birds (i.e. yearlings in New Hampshire and hatch-year birds in Jamaica) did not differ from adults. indicating that from the time hatch-year individuals acquire territories on winter quarters in mid-October, they survive as well as adults within the same habitat. 4. Monthly survival probabilities during the summer (May-August) and winter (October-March) stationary periods were high: 1.0 for males in New Hampshire, and 0.99 +/- 0.01 for males in Jamaica and for females in both locations. 5. These annual and seasonal survival estimates were used to calculate warbler survival for the migratory periods. Monthly survival probability during migration ranged from 0.77 to 0.81 +/- 0.02. Thus, apparent mortality rates were at least 15 times higher during migration compared to that in the stationary periods, and more than 85% of apparent annual mortality of D. caerulescens occurred during migration. 6. Additional data from multiple species, especially measures of habitat-specific demography and dispersal, will improve our understanding of the relative impacts of the breeding, migratory, and winter periods on population dynamics of migratory birds and thus enhance future conservation efforts. C1 Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. RP Sillett, TS (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. EM silletts@nzp.si.edu NR 97 TC 421 Z9 432 U1 21 U2 155 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8790 EI 1365-2656 J9 J ANIM ECOL JI J. Anim. Ecol. PD MAR PY 2002 VL 71 IS 2 BP 296 EP 308 DI 10.1046/j.1365-2656.2002.00599.x PG 13 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 541LU UT WOS:000174986700013 ER PT J AU Melson, WG Potts, R AF Melson, WG Potts, R TI Origin of reddened and melted zones in Pleistocene sediments of the Olorgesailie Basin, southern Kenya Rift SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE combustion metamorphism; melt rocks; Pleistocene; Olorgesailie; Homo erectus; drought; Kenya AB Hardened red zones and rare melt rocks are puzzling and rare features in the Middle Pleistocene sediments of the Olorgesailie Formation of the southern Kenya Rift. We propose that combustion metamorphism and melting produced these zones. This is evidenced by field observations, chemical composition, X-ray diffraction and melting experiments. Plant-rich beds and disbursed plant matter served as fuel. Probably lightning generated surface fires that ignited carbonaceous beds exposed in gullies. The burning then proceeded underground. Melt rocks and red thermally metamorphosed zones within beds distinguish combustion metamorphism from reddening of paleosols by surface vegetation fires. Diagenetic oxidation has removed much of the carbonaceous material from the paleosols and marsh deposits, except where they are included in dense metasediments. Extraordinarily high temperatures of about 1200(o)C, which are essential to producing the melt rocks, required plant matter buildup, burial of the plant fuel under at most a few metres of sediment, and then rapid burning under dry conditions. This sequence of events points to one or more extreme droughts between 601,000 and 493,000 years ago, the period represented by upper Member 12 and Member 13 of the Olorgesailie Formation. Combustion metamorphism was not recognized in early studies at Olorgesailie, partly because it is not a widely taught nor published subject. Other Pleistocene East African basins and similar sites may contain as yet unrecognized products of combustion metamorphism that may prove of paleoclimatological importance. C1 Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. RP Melson, WG (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. NR 18 TC 6 Z9 6 U1 1 U2 6 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD MAR PY 2002 VL 29 IS 3 BP 307 EP 316 DI 10.1006/jasc.2001.0695 PG 10 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 554ZJ UT WOS:000175767000008 ER PT J AU Slikas, B Olson, SL Fleischer, RC AF Slikas, B Olson, SL Fleischer, RC TI Rapid, independent evolution of flightlessness in four species of Pacific Island rails (Rallidae): an analysis based on mitochondrial sequence data SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID HENDERSON ISLAND; CYTOCHROME-B; PHYLOGENY; DNA; HISTORY; AVES; INCONGRUENCE; BIRDS AB Flightless rails were once ubiquitous in the avifauna of Pacific oceanic islands. Most species have become extinct since human colonization of islands began about 2000 years ago. In this study, we use mitochondrial sequence data to estimate the phylogenetic relationships and ages of four species of flightless insular rails in the genus Porzana: palmeri, from Laysan Island in the Hawaiian archipelago; sandwichensis, from the island of Hawaii; monasa, from Kosrae Island in Micronesia; and atra, from Henderson Island in the Pitcairn group. Although all four species survived into historic times, all but atra are now extinct. The optimal trees show that palmeri is descended from Porzana pusilla, a volant crake distributed widely throughout the Old World. Porzana sandwichensis, P. monasa, and P. atra are each descended from the lineage leading to P. tabuensis, a volant rail widespread in northern and eastern Australia and on islands north to Micronesia and the Philippines and east through Polynesia. Loss of flight appears to have evolved rapidly in these insular rails, based on both sequence divergence values and data on the ages of the islands. In the case of the Laysan Rail (palmeri), divergences including loss of flight probably evolved in less than 125,000 years. C1 Smithsonian Inst, Genet Mol Lab, Washington, DC 20008 USA. Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Slikas, B (reprint author), Smithsonian Inst, Genet Mol Lab, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Slikas, Beth/E-7275-2013 NR 41 TC 45 Z9 46 U1 8 U2 40 PU BLACKWELL MUNKSGAARD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD MAR PY 2002 VL 33 IS 1 BP 5 EP 14 DI 10.1034/j.1600-048X.2002.330103.x PG 10 WC Ornithology SC Zoology GA 540MG UT WOS:000174932300002 ER PT J AU Gray, HM Ouellet, M Green, DM Rand, AS AF Gray, HM Ouellet, M Green, DM Rand, AS TI Traumatic injuries in two neotropical frogs, Dendrobates auratus and Physalaemus pustulosus SO JOURNAL OF HERPETOLOGY LA English DT Article ID SKIN ALKALOIDS; POISON; CLASSIFICATION C1 McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Gray, HM (reprint author), McGill Univ, Redpath Museum, 859 Sherbrooke St W, Montreal, PQ H3A 2K6, Canada. NR 22 TC 14 Z9 15 U1 1 U2 4 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 MAR PY 2002 VL 36 IS 1 BP 117 EP 121 PG 5 WC Zoology SC Zoology GA 530HJ UT WOS:000174352000022 ER PT J AU Noll, M AF Noll, M TI Interpreting Acheulean stone tool variability at Olorgesailie, Kenya SO JOURNAL OF HUMAN EVOLUTION LA English DT Meeting Abstract C1 Smithsonian Inst, Museum Natl Hist Nat, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 4 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD MAR PY 2002 VL 42 IS 3 BP A25 EP A25 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 543QA UT WOS:000175111600042 ER PT J AU Smith, M AF Smith, M TI Islamic paper: A study of the ancient craft SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Book Review C1 Smithsonian Inst, Freer Gallery Art & AM Sackler Gallery, Washington, DC 20560 USA. RP Smith, M (reprint author), Smithsonian Inst, Freer Gallery Art & AM Sackler Gallery, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SPR PY 2002 VL 41 IS 1 BP 97 EP 98 DI 10.2307/3179901 PG 2 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 592EK UT WOS:000177923600009 ER PT J AU Reinert, JF AF Reinert, JF TI A comparative analysis of the ventral brush and its attachment to segment X of fourth-stage larvae in tribe Aedini (Diptera : Culicidae) SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Article DE fourth-stage larva; seta 4-X; ventral brush; grid; boss; Aedini; Culicidae ID CLASSIFICATION AB A comparative anatomical analysis of the ventral brush and its attachment to segment X of 4th-stage larvae was conducted for the genera and subgenera in tribe Aedini. Four types and 18 subtypes are recognized and examples of each are described and illustrated. A key distinguishing the types and subtypes is included. Some comments concerning the phylogenetic utility of the ventral brush are provided. C1 Smithsonian Inst, Natl Museum Nat Hist, Walter Reed Biosyst Unit, Washington, DC 20560 USA. RP Reinert, JF (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Walter Reed Biosyst Unit, Washington, DC 20560 USA. NR 8 TC 6 Z9 6 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 MAR PY 2002 VL 18 IS 1 BP 16 EP 25 PG 10 WC Entomology SC Entomology GA 543UB UT WOS:000175118600003 PM 11998925 ER PT J AU Harris, SC Flint, OS Holzenthal, RW AF Harris, SC Flint, OS Holzenthal, RW TI Two new genera of Hydroptilidae from the Neotropics (Trichoptera : Hydroptilidae : Stactobiini) SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Trichoptera; Hydroptilidae; microcaddisflies; new genera; Neotropics; Venezuela; Costa Rica; key AB Two new monotypic genera of stactobine microcaddisflies (Trichoptera: Hydroptilidae), Orinocotrichia, and Tizatetrichia, are described and illustrated from Venezuela and Costa Rica, respectively. Keys are provided for males and females of the New World genera comprising the tribe Stactobiini. C1 Clarion Univ Pennsylvania, Dept Biol, Clarion, PA 16214 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. RP Harris, SC (reprint author), Clarion Univ Pennsylvania, Dept Biol, Clarion, PA 16214 USA. NR 7 TC 6 Z9 10 U1 0 U2 0 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SPR PY 2002 VL 110 IS 1 BP 49 EP 64 DI 10.1664/0028-7199(2002)110[0049:TNGOHF]2.0.CO;2 PG 16 WC Entomology SC Entomology GA 592AP UT WOS:000177914800002 ER PT J AU Harris, SC Flint, OS Holzenthal, RW AF Harris, SC Flint, OS Holzenthal, RW TI Review of the Neotropical genus Flintiella (Trichoptera : Hydroptilidae : Stactobiini) SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Trichoptera; Hydroptilidae; microcaddisflies; Flintiella; new species; Neotropics; key AB The Neotropical genus Flintiella is reviewed and eight new species are described and illustrated: F. alajuela from Costa Rica, F. boraceia from Brazil, F. panamensis from Panama, F. tamaulipasa from Mexico, F. yanamona from Peru, F. heredia from Costa Rica, Ecuador, and Peru, F. astilla from Brazil, Costa Rica, Ecuador, Paraguay, Peru, and Venezuela, and F. pizotensis from Columbia, Costa Rica, Ecuador, Mexico, Panama, and Peru. New illustrations are provided for F. andreae Angrisano. Keys are provided to separate the males and the associated females of the nine known species in the genus. C1 Clarion Univ Pennsylvania, Dept Biol, Clarion, PA 16214 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. RP Harris, SC (reprint author), Clarion Univ Pennsylvania, Dept Biol, Clarion, PA 16214 USA. NR 5 TC 6 Z9 9 U1 0 U2 1 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SPR PY 2002 VL 110 IS 1 BP 65 EP 90 DI 10.1664/0028-7199(2002)110[0065:ROTNGF]2.0.CO;2 PG 26 WC Entomology SC Entomology GA 592AP UT WOS:000177914800003 ER PT J AU King, RS Richardson, CJ AF King, RS Richardson, CJ TI Evaluating subsampling approaches and macro invertebrate taxonomic resolution for wetland bioassessment SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article DE biological assessment; biological monitoring; fixed-count subsampling; fixed-area subsampling; taxonomic sufficiency; large-rare search; multivariate approach; Chironomidae; Everglades ID AQUATIC COMMUNITY ECOLOGY; FIXED-COUNT METHOD; BENTHIC MACROINVERTEBRATES; RAPID ASSESSMENT; BIOTIC INDEX; STREAMS; EVERGLADES; RIVERS; IMPACT; SCALE AB Methods for wetland bioassessment using macroinvertebrates are not well developed. Two of the most controversial issues in stream bioassessment, subsampling and taxonomic resolution, have vet to be quantitatively addressed for wetlands. Using a multivariate approach, we evaluated the efficacy of family-, genus-, and species-level assemblage data in reflecting the environment and distinguishing impaired sites from the reference condition. We used 5 basic levels of subsampling (100, 200-, and 300-organism fixed counts; 10% and 25% fixed areas), an integrated subsample requiring a minimum fixed count and fixed area (100&10%), and 100-count and 10%-area subsamples coupled with a supplementary large-rare (LR) search. Data were obtained from 1.5-m(2) composite samples collected from 126 plots along a 10-km-long eutrophication gradient in the Florida Everglades. Our results suggest that effectiveness of subsampling depended more upon the minimum number of individuals retained than minimum area or proportion of the sample picked. Fixed-area subsamples were generally less efficient than fixed counts, with 200- and 300-individual fixed counts resulting in significantly greater assemblage-environment relationships and Much higher accuracy in detecting impairment than 10% fixed area, despite averaging similar numbers of individuals. The greatest improvement with increasing subsample size was observed between fixed counts of 100 and 200 individuals; detecting impairment, in particular, was not markedly improved with subsample sizes >200 individuals. Supplementing subsamples with a LR search resulted in only very sleight improvements in assemblage-environment relationships, but was effective in improving prediction accuracy, particularly for fan-Lily-level data. However, family-level assemblage-environment relationships and abilities to detect impairment were inferior to genus- and species-level data, regardless of subsample size. Species-level data performed best, primarily because of the large proportion (>20%) of total species belonging to Chironomidae. The potential importance of Chironomidae to wetland bioassessment was further revealed through an evaluation of a tiered-taxonomic approach, which showed that non-Chironomidae family-level data tiered with species-level Chironomidae data produced results very similar to those obtained using genus- or species-level data exclusively. Our results suggest that fixed counts greater than or equal to200 or integrated fixed-area/fixed-count approaches that consistently obtain a minimum of 200 individuals should be considered as minimum subsample sizes for wetlands. We additionally advocate LR searches and recommend genus- or species-level taxonomy, particularly for the Chironomidae. C1 Duke Univ, Wetland Ctr, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA. RP King, RS (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 90 TC 101 Z9 104 U1 3 U2 21 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD MAR PY 2002 VL 21 IS 1 BP 150 EP 171 DI 10.2307/1468306 PG 22 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 526MQ UT WOS:000174134600013 ER PT J AU Mills, C AF Mills, C TI Richmond's Monument Avenue SO JOURNAL OF THE SOCIETY OF ARCHITECTURAL HISTORIANS LA English DT Book Review C1 Smithsonian Inst, Museum Amer Art, Washington, DC 20560 USA. RP Mills, C (reprint author), Smithsonian Inst, Museum Amer Art, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC ARCHITECTURAL HISTORIANS PI CHICAGO PA 1365 NORTH ASTOR ST, CHICAGO, IL 60610-2144 USA SN 0037-9808 J9 J SOC ARCHIT HIST JI J. Soc. Archit. Hist. PD MAR PY 2002 VL 61 IS 1 BP 108 EP 110 DI 10.2307/991824 PG 3 WC Architecture SC Architecture GA 665JP UT WOS:000182117000019 ER PT J AU Stuntz, S Ziegler, C Simon, U Zotz, G AF Stuntz, S Ziegler, C Simon, U Zotz, G TI Diversity and structure of the arthropod fauna within three canopy epiphyte species in central Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Barro Colorado Island; bromeliads; guild structure; leaf litter; microclimate; orchids; plant size; spiders ID RAIN-FOREST TREES; COMMUNITY ORGANIZATION; PREY AVAILABILITY; VEGETATION; SPIDERS; DETERMINANTS; ARCHITECTURE; MICROCLIMATE; ABUNDANCE; LITTER AB The arthropod fauna inhabiting 90 individuals of three different species of epiphyte was investigated in the moist lowland forest of the Barro Colorado National Monument in Panama. In total, 3694 arthropods belonging to 89 morphospecies and 19 orders were collected. While arthropod abundance was primarily a function of host plant biomass irrespective of epiphyte species, there were pronounced differences in species richness, species composition and guild structure of the arthropod faunas of the three epiphyte species. Although all study plants were growing in close proximity on the same host tree species, there was remarkably little overlap in the species assemblages across epiphyte taxa. The inhabitant species also differed dramatically in their ecological functions, as feeding guild and hunting guild analyses indicated. The influence of plant size, structure and impounded leaf litter on arthropod diversity is discussed. We conclude that epiphytes are microhabitats for a diverse and numerous fauna, and that different species of epiphytes foster both taxonomically and ecologically very distinct arthropod assemblages. C1 Univ Wurzburg, Lehrstuhl Bot 2, D-97082 Wurzburg, Germany. Tech Univ Munich, Forstwissensch Fak, D-85354 Freising Weihenstephan, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. NR 52 TC 40 Z9 46 U1 3 U2 16 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2002 VL 18 BP 161 EP 176 DI 10.1017/S0266467402002110 PN 2 PG 16 WC Ecology SC Environmental Sciences & Ecology GA 527QA UT WOS:000174196500001 ER PT J AU Blanco, JM Gee, GF Wildt, DE Donoghue, AM AF Blanco, JM Gee, GF Wildt, DE Donoghue, AM TI Producing progeny from endangered birds of prey: Treatment of urine-contaminated semen and a novel intramagnal insemination approach SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE spermatozoa; artificial insemination; avian; raptor; captive breeding; genetic management ID ARTIFICIAL-INSEMINATION; SPERMATOZOA; POULTRY AB Wild raptors brought into an ex situ environment often have poor semen quality that is further compromised by urine contamination. Generally, it is believed that in birds, artificial insemination into the cloaca or caudal vagina of females requires large doses of high-quality spermatozoa to maximize fertility. In an effort to define and overcome some of the challenges associated with reproduction in wild raptors, the objectives of this study were to 1) evaluate the frequency, impact, and remediation of urine contamination in fresh ejaculates for the purpose of maintaining sperm motility and viability in vitro, and 2) develop a deep insemination method that allows low numbers of washed sperm to be placed directly into the magnum to increase the probability of producing fertilized eggs. The species evaluated include golden eagle (Aquila chrysoetos), imperial eagle (A. adalberti), Bonelli's eagle (Hiernaetus fasciatus), and peregrine, falcon (Falco peregrinus). Semen samples were collected and pooled by species, and a minimum of 25 pooled ejaculates per species were evaluated for urine contamination, pH, sperm viability, and sperm motility; the samples were either unwashed or washed in neutral (pH 7.0) or alkaline (pH 8.0) modified Lake's diluent. Female golden eagles and peregrine falcons were inseminated via transjunctional, intramagnal insemination with washed spermatozoa from urine-contaminated samples. Urine contamination occurred in 36.8 +/- 12.8% (mean +/- SEM) golden eagle, 43.1 +/- 9.1% imperial eagle, 28.7 +/- 16.1% Bonelli's eagle, and 48.2 +/- 17.3% peregrine falcon ejaculates. The pH in urine-contaminated semen samples ranged from 6.48 +/- 0.3 to 6.86 +/- 0.2, and in noncontaminated samples it ranged from from 7.17 +/- 0.1 to 7.56 +/- 0.1. Sperm viability and motility were reduced (P < 0.05) in all species for unwashed vs. washed sperm after 30 min incubation at room temperature. Two peregrine falcon chicks and one golden eagle chick hatched after intramagnal insemination. This study demonstrates that urine contamination, a common and lethal acidifier in manually collected raptor ejaculates, can be circumvented by immediate, gentle seminal washing. Furthermore, these processed sperm, when deposited by transjunctional intramagnal insemination, can produce live young. C1 Univ Arkansas, USDA ARS, Poultry Prod & Product Safety Res Unit, Poultry Sci Ctr, Fayetteville, AR 72701 USA. US Fish & Wildlife Serv, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Ctr Studies Iberian Raptors, Toledo 45671, Spain. RP Blanco, JM (reprint author), Univ Arkansas, USDA ARS, Poultry Prod & Product Safety Res Unit, Poultry Sci Ctr, Fayetteville, AR 72701 USA. NR 27 TC 19 Z9 20 U1 1 U2 5 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 MAR PY 2002 VL 33 IS 1 BP 1 EP 7 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA 589QH UT WOS:000177771200001 PM 12216788 ER PT J AU Schroll, SR AF Schroll, SR TI Friedl Dicker-Brandeis: Vienna 1898-Auschwitz 1944. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Schroll, SR (reprint author), Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 1 PY 2002 VL 127 IS 4 BP 96 EP 96 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 526LA UT WOS:000174130900042 ER PT J AU Fagan, TJ Taylor, GJ Keil, K Bunch, TE Wittke, JH Korotev, RL Jolliff, BL Gillis, JJ Haskin, LA Jarosewich, E Clayton, RN Mayeda, TK Fernandes, VA Burgess, R Turner, G Eugster, O Lorenzetti, S AF Fagan, TJ Taylor, GJ Keil, K Bunch, TE Wittke, JH Korotev, RL Jolliff, BL Gillis, JJ Haskin, LA Jarosewich, E Clayton, RN Mayeda, TK Fernandes, VA Burgess, R Turner, G Eugster, O Lorenzetti, S TI Northwest Africa 032: product of lunar volcanism SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID LASER ARGON-40-ARGON-39 AGE; APOLLO 12 SITE; MARE BASALTS; CENTRAL HIGHLANDS; CRYSTAL-GROWTH; NOBLE-GASES; METEORITE; CRYSTALLIZATION; OLIVINE; HISTORY AB Mineralogy, major element compositions of minerals, and elemental and oxygen isotopic compositions of the whole rock attest to a lunar origin of the meteorite Northwest Africa (NWA) 032, an unbrecciated basalt found in October 1999. The rock consists predominantly of olivine, pyroxene and chromite phenocrysts, set in a crystalline groundmass of feldspar, pyroxene, ilmenite, troilite and trace metal. Whole-rock shock veins comprise a minor, but ubiquitous portion of the rock. Undulatory to mosaic extinction in olivine and pyroxene phenocrysts and micro-faults in groundmass and phenocrysts also are attributed to shock. Several geochemical signatures taken together indicate unambiguously that NWA 032 originated from the Moon. The most diagnostic criteria include whole-rock oxygen isotopic composition and ratios of Fe/Mn in the whole rock, olivine, and pyroxene. A lunar origin is documented further by the presence of Fe-metal, troilite, and ilmenite; zoning to extremely Fe-rich compositions in pyroxene; the ferrous oxidation state of all Fe in pyroxene; and the rare earth element (REE) pattern with a well-defined negative europium anomaly. This rock is similar in major element chemistry to basalts from Apollo 12 and 15, but is enriched in light REE and has an unusually high Th/Sm ratio. Some Apollo 14 basalts yield a closer match to NWA 032 in REE patterns, but have higher concentrations of Al(2)O(3). Ar-Ar step release results are complex, but yield a whole-rock age of similar to2.8 Ga, suggesting that NWA 032 was extruded at 2.8 Ga or earlier. This rock may be the youngest sample of mare basalt collected to date. Noble gas concentrations combined with previously collected radionuclide data indicate that the meteorite exposure history is distinct from currently recognized lunar meteorites. In short, the geochemical and petrographic features of NWA 032 are not matched by Apollo or Luna samples, nor by previously identified lunar meteorites, indicating that it originates from a previously unsampled mare deposit. Detailed assessment of petrographic features, olivine zoning, and thermodynamic modelling indicate a relatively simple cooling and crystallization history for NWA 032. Chromite-spinel, olivine, and pyroxene crystallized as phenocrysts while the magma cooled no faster than 2 degreesC/h based on the polyhedral morphology of olivine. Comparison of olivine size with crystal growth rates and preserved Fe-Mg diffusion profiles in olivine phenocrysts suggest that olivine was immersed in the melt for no more than 40 days. Plumose textures in groundmass pyroxene, feldspar, and ilmenite, and Fe-rich rims on the phenocrysts formed during rapid crystallization (cooling rates similar to20 to 60 degreesC/h) after eruption. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. No Arizona Univ, Dept Geol, Flagstaff, AZ USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Manchester, Dept Earth Sci, Manchester M13 9PL, Lancs, England. Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. RP Fagan, TJ (reprint author), Tokyo Inst Technol, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan. EM fagan@geo.titech.ac.jp RI Burgess, Ray/A-5767-2009; Fernandes, Vera/B-4653-2013; Lorenzetti, Silvio/B-1188-2009 OI Burgess, Ray/0000-0001-7674-8718; Fernandes, Vera/0000-0003-0848-9229; Lorenzetti, Silvio/0000-0002-8339-8960 NR 78 TC 55 Z9 59 U1 2 U2 6 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD MAR PY 2002 VL 37 IS 3 BP 371 EP 394 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 538BW UT WOS:000174795000004 ER PT J AU Whittingham, LA Slikas, B Winkler, DW Sheldon, FH AF Whittingham, LA Slikas, B Winkler, DW Sheldon, FH TI Phylogeny of the tree swallow genus, Tachycineta (Aves : Hirundinidae), by Bayesian analysis of mitochondrial DNA sequences SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE swallow phylogeny; Hirundinidae; Tachycineta; Bayesian; mitochondrial genes; DNA sequencing ID CYTOCHROME-B GENE; HYBRIDIZATION; VERTEBRATES; CONFIDENCE; EVOLUTION AB To set the stage for historical analyses of the ecology and behavior of tree swallows and their allies (genus Tachycineta), we reconstructed the phylogeny of the nine Tachycineta species by comparing DNA sequences of six mitochondrial genes: Cytochrome b (990 base pairs), the second subunit of nicotinamide adenine dinucleotide dehydrogenase (839 base pairs), cytochrome oxidase II (85 base pairs), ATPase 8 (158 base pairs), tRNA-lysine (73 base pairs), and tRNA-methionine (25 base pairs). The phylogeny consisted of two main clades: South and Central American species ((T. stolzmanni, T. albilinea, T. albiventris), (T. leucorrhoa, T. meyeni)), and North American and Caribbean species (T. bicolor, (T. thalassina, T. euchrysea, T. cyaneoviridis)). The genetic distances among the species suggested that Tachycineta is a relatively old group compared to other New World swallow genera. One interesting biogeographic discovery was the close relationship between Caribbean and western North American taxa. This historical connection occurs in other groups of swallows and swifts as well. To reconstruct the phylogeny, we employed Bayesian as well as traditional maximum-likelihood methods. The Bayesian approach provided probability values for trees produced from the different genes and gene combinations, as well as probabilities of branches within those trees. We compared Bayesian and maximum-likelihood bootstrap branch support and found that all branches with Bayesian probabilities greater than or equal to95% received bootstrap support >70%. (C) 2002 Elsevier Science (USA). C1 Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Sheldon, FH (reprint author), Louisiana State Univ, Museum Nat Sci, 119 Foster Hall, Baton Rouge, LA 70803 USA. RI Slikas, Beth/E-7275-2013 NR 40 TC 59 Z9 62 U1 1 U2 7 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 MAR PY 2002 VL 22 IS 3 BP 430 EP 441 DI 10.1006/mpev.2001.1073 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 530KX UT WOS:000174357800011 PM 11884168 ER PT J AU Fairley, BW Jones, LR Wake, DA Collins, CA Burke, DJ Nichol, RC Romer, AK AF Fairley, BW Jones, LR Wake, DA Collins, CA Burke, DJ Nichol, RC Romer, AK TI Galaxy colours in high-redshift, X-ray-selected clusters - I. Blue galaxy fractions in eight clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : fundamental parameters; galaxies : spiral ID BUTCHER-OEMLER CLUSTERS; NUMBER COUNTS; DISTANT CLUSTERS; CCD OBSERVATIONS; FIELD GALAXIES; EVOLUTION; SPECTROSCOPY; POPULATIONS; MAG; MORPHOLOGY AB We present initial results from a wide-field, multicolour imaging project, designed to study C galaxy evolution in X-ray-selected clusters at intermediate (z similar to 0.25) and high redshifts (z similar to 0.5). We give blue galaxy fractions from eight X-ray-selected clusters, drawn from a combined sample of three X-ray surveys. We find that all the clusters exhibit excess blue galaxy populations over the numbers observed in local systems, although a large scatter is present in the results. We find no significant correlation of blue fraction with redshift at z > 0.2, although the large scatter could mask a positive trend. We also find no systematic trend of blue fraction with X-ray luminosity. We show that the blue fraction is a function of (a) radius within a cluster, (b) absolute magnitude and (c) the passbands used to measure the colour. We find that our blue fractions (f(b)) from galaxy colours close to rest frame (U - B)(0). f(b) similar to 0.4, are systematically higher than those from rest frame (B - V)(0) colours, f(b) similar to 0.2. We conclude this effect is real, may offer a partial explanation of the widely differing levels of blue fraction found in previous studies, and may have implications for biases in optical samples selected in different bands. While the increasing blue fraction with radius can be interpreted as evidence of cluster infall of field galaxies, the exact physical processes which these galaxies undergo is unclear. We estimate that, in the cores of the more massive clusters, galaxies should be experiencing ram-pressure stripping of galactic gas by the intracluster medium. The fact that our low X-ray luminosity systems show a similar blue fraction as the high-luminosity systems, as well as a significant blue fraction gradient with radius, implies other physical effects are also important. C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead L41 1LD, Merseyside, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. RP Fairley, BW (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. NR 65 TC 43 Z9 43 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 MAR 1 PY 2002 VL 330 IS 3 BP 755 EP 767 DI 10.1046/j.1365-8711.2002.05121.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 530NQ UT WOS:000174365200028 ER PT J AU Abel, T Wandelt, BD AF Abel, T Wandelt, BD TI Adaptive ray tracing for radiative transfer around point sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; radiative transfer; methods : N-body simulations; methods : numerical; ISM : evolution; cosmology : theory ID IONIZING-RADIATION; GALAXY FORMATION; ABSORPTION AB We describe a novel adaptive ray tracing scheme to solve the equation of radiative transfer around point sources in hydrodynamical simulations. The angular resolution adapts to the local hydrodynamical resolution and hence is of use for adaptive meshes as well as adaptive smooth particle hydrodynamical simulations, Recursive creation of rays ensures ease of implementation. The multiple radial integrations needed to solve the time-dependent radiative transfer are speeded up significantly using a quad-tree once the rays are cast. Simplifications advantageous for methods with one radiation source are briefly discussed. The suggested method is easily generalized to speed up Monte Carlo radiative transfer techniques. In summary, a nearly optimal use of long characteristics is presented and aspects of its implementation and comparison with other methods are given. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Abel, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 66 Z9 66 U1 0 U2 2 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2002 VL 330 IS 3 BP L53 EP L56 DI 10.1046/j.1365-8711.2002.05206.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 530NQ UT WOS:000174365200001 ER PT J AU Gardner, JB AF Gardner, JB TI Collecting a national tragedy (What role should a cultural institution like the National Museum of American History play in a time of crisis) SO MUSEUM NEWS LA English DT Article C1 Smithsonian Inst, Amer Museum Nat Hist, Behring Ctr, Washington, DC 20560 USA. RP Gardner, JB (reprint author), Smithsonian Inst, Amer Museum Nat Hist, Behring Ctr, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 2002 VL 81 IS 2 BP 42 EP + PG 0 WC Art SC Art GA 593MN UT WOS:000177995400035 ER PT J AU Levin, RA AF Levin, RA TI Taxonomic status of Acleisanthes, Selinocarpus, and Ammocodon (Nyctaginaceae) SO NOVON LA English DT Article DE Acleisanthes; Ammocodon; Chihuahuan Desert; four o'clock; Nyctaginaceae; Selinocarpus AB Recent molecular arid morphological studies suggest that neither Acleisanthes nor Selinocarpus (Nyctaginaceae) are monophyletic as currently circumscribed. Further, these data provide no basis for Continued recognition of the monotypic genus Ammocodon as separate from these other two genera. Therefore, all 8 Selinocarpus species and the monospecific Ammocodon are transferred to Acleisanthes: 3 additional Selinocarpus species are reduced to The genus Acleisanthes is rime composed of 16 species. distributed primarily in the Chihuahuan Desert of North America. Diagnostic features of Acleisanthes include an herbaceous or woody pereniial habit in arid environments, and the presence of both cleistogamous and chasmogamous flowers often simultaneously on an individual plant. Further, flowers are usually axillary and subtended by 1 to 4 subulate braets, with chasmogamous flowers frequently white or yellow and funnelform to salverform. C1 Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. RP Levin, RA (reprint author), Natl Museum Nat Hist, Smithsonian Museum Support Ctr, Lab Mol Systemat, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 13 TC 9 Z9 9 U1 1 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 SPR PY 2002 VL 12 IS 1 BP 58 EP 63 DI 10.2307/3393240 PG 6 WC Plant Sciences SC Plant Sciences GA 541FT UT WOS:000174975100013 ER PT J AU Barry, JC Morgan, MLE Flynn, LJ Pilbeam, D Behrensmeyer, AK Raza, SM Khan, IA Badgley, C Hicks, J Kelley, J AF Barry, JC Morgan, MLE Flynn, LJ Pilbeam, D Behrensmeyer, AK Raza, SM Khan, IA Badgley, C Hicks, J Kelley, J TI Faunal and environmental change in the late Miocene Siwaliks of northern Pakistan SO PALEOBIOLOGY LA English DT Article ID MAGNETIC POLARITY STRATIGRAPHY; CONFIDENCE-INTERVALS; HIMALAYAN FOREDEEP; ISOTOPIC EVIDENCE; FLUVIAL SYSTEMS; TIBETAN PLATEAU; FOSSIL HORIZONS; POTWAR PLATEAU; CHINJI VILLAGE; INDIAN MONSOON AB The Siwalik formations of northern Pakistan consist of deposits of ancient rivers that existed throughout the early Miocene through the late Pliocene. The formations are highly fossiliferous with a diverse array of terrestrial and freshwater vertebrates, which in combination with exceptional lateral exposure and good chronostratigraphic control allows a more detailed and temporally resolved study of the sediments and faunas than is typical in terrestrial deposits. Consequently the Siwaliks provide an opportunity to document temporal differences in species richness, turnover, and ecological structure in a terrestrial setting, and to investigate how such differences are related to changes in the fluvial system, vegetation, and climate. Here we focus on the interval between 10.7 and 5.7 Ma, a time of significant local tectonic and global climatic change. It is also the interval with the best temporal calibration of Siwalik faunas and most comprehensive data on species occurrences. A methodological focus of this paper is on controlling sampling biases that confound biological and ecological signals. Such biases include uneven sampling through time, differential preservation of larger animals and more durable skeletal elements, errors in age-dating imposed by uncertainties in correlation and paleomagnetic timescale calibrations, and uneven taxonomic treatment across groups. We attempt to control for them primarily by using a relative-abundance model to estimate limits for the first and last appearances from the occurrence data. This model also incorporates uncertainties in a e estimates. Because of sampling limitations inherent in the terrestrial fossil record, our 100-Kyr temporal resolution may approach the finest possible level of resolution for studies of vertebrate faunal changes over periods of millions of years. Approximately 40,000 specimens from surface and screenwash collections made at 555 localities form the basis of our study. Sixty percent of the localities have maximum and minimum age estimates differing by 100 Kyr or less, 82% by 200 Kyr or less. The fossils represent 115 mammalian species or lineages of ten orders: Insectivora, Scandentia, Primates, Tubulidentata, Proboscidea, Pholidota, Lagomorpha, Perissodactyla, Artiodactyla, and Rodentia. Important taxa omitted from this study include Carnivora, Elephantoidea, and Rhinocerotidae. Because different collecting methods were used for large and small species, they are treated separately in analyses. Small species include insectivores, tree shrews, rodents, lagomorphs, and small primates. They generally weigh less than 5 kg. The sediments of the study interval were deposited by coexisting fluvial systems, with the larger emergent Nagri system being displaced between 10.1 and 9.0 Ma by an interfan Dhok Pathan system. In comparison to Nagri floodplains, Dhok Pathan floodplains were less well drained, with smaller rivers having more seasonally variable flow and more frequent avulsions. Paleosol sequences indicate reorganization of topography and drainage accompanying a transition to a more seasonal climate. A few paleosols may have formed under waterlogged, grassy woodlands, but most formed under drier conditions and more closed vegetation. The oxygen isotopic record also indicates significant change in the patterns of precipitation beginning at 9.2 Ma, in what may have been a shift to a drier and more seasonal climate. The carbon isotope record demonstrates that after 8.1 Ma significant amounts of C-4 grasses began to appear and that by 6.8 Ma floodplain habitats included extensive C-4 grasslands. Plant communities with predominantly C-4 plants were greatly diminished after 7.0 Ma, and those with predominantly C-4 plants, which would have been open woodlands or grassy woodlands, appeared as early as 7.4 Ma. Inferred first and last appearances show a constant, low level of faunal turnover throughout the interval 10.7-5.7-Ma, with three short periods of elevated turnover at 10.3, 7.8, and 7.3-7.0 Ma. The three pulses account for nearly 44% of all turnover. Throughout the late Miocene, species richness declined steadily, and diversity and richness indices together with data on body size imply that community ecological structure changed abruptly just after 10 Ma, and then again at 7.8 Ma. Between 10 and 7.8 Ma the large-mammal assemblages were strongly dominated by equids, with more balanced faunas before and after. The pattern of appearance and disappearance is selective with respect to inferred habits of the animals. Species appearing after 9.0 Ma are grazers or typical of more open habitats, whereas many species that disappear can be linked to more closed vegetation. We presume exceptions to this pattern were animals of the mixed C-3/C-4 communities or the wetter parts of the floodplain that did not persist into the latest Miocene. The pace of extinction accelerates once there is C-4 vegetation on the floodplain. The 10.3 Ma event primarily comprises disappearance of taxa that were both common and of long duration. The event does not correlate to any obvious local environmental or climatic event, and the pattern of species disappearance and appearance suggests that biotic interactions may have been more important than environmental change. The 7.8 Ma event is characterized solely by appearances, and that at 7.3 Ma by a combination of appearances and disappearances. These two latest Miocene events include more taxa that were shorter ranging and less common, a difference of mode that developed between approximately 9.0 and 8.5 Ma when many short-ranging and rare species began to make appearances. Both events also show a close temporal correlation to changes in floodplain deposition and vegetation. The 7.8 Ma event follows the widespread appearance of C-4 vegetation and is coincident with the shift from equid-dominated to more evenly balanced large-mammal assemblages, The 7.3 to 7.0 Ma event starts with the first occurrence of C-4-dominated floras and ends with the last occurrence of C dominated vegetation. Absence of a consistent relationship between depositional facies and the composition of faunal assemblages leads us to reject fluvial system dynamics as a major cause of faunal change. The close correlation of latest Miocene species turnover and ecological change to expansion of C-4 plants on the floodplain, in association with oxygen isotopic and sedimentological evidence for increasingly drier and more seasonal climates, causes us to favor explanations based on climatic change for both latest Miocene pulses. The Siwalik record supports neither "coordinated stasis" nor "turnover pulse" evolutionary models. The brief, irregularly spaced pulses of high turnover are characteristic of both the Stasis and pulse models, but the high level of background turnover that eliminates 65-70% of the initial species shows there is no stasis in the Siwalik record. In addition, the steadily declining species richness and abrupt, uncoordinated changes in diversity do not fit either model. C1 Harvard Univ, Dept Anthropol, Cambridge, MA 02138 USA. Harvard Univ, Peabody Museum, Cambridge, MA 02138 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Geol Survey Pakistan, Quetta, Pakistan. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. Denver Museum Nat Hist, Denver, CO 80205 USA. Univ Illinois, Coll Dent, Dept Oral Biol, Chicago, IL 60612 USA. RP Barry, JC (reprint author), Harvard Univ, Dept Anthropol, Cambridge, MA 02138 USA. NR 94 TC 207 Z9 222 U1 5 U2 44 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2002 VL 28 IS 2 SU S BP 1 EP 71 DI 10.1666/0094-8373(2002)28[1:FAECIT]2.0.CO;2 PG 71 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 565PE UT WOS:000176378000001 ER PT J AU Jaramillo, CA AF Jaramillo, CA TI Response of tropical vegetation to Paleogene warming SO PALEOBIOLOGY LA English DT Article ID PALEOCENE THERMAL MAXIMUM; LATE QUATERNARY VEGETATION; NORTHERN SOUTH-AMERICA; EARLY EOCENE CLIMATE; LOWLAND AMAZONIA; STABLE ISOTOPES; PLANT DIVERSITY; BIGHORN BASIN; POLLEN RECORD; HISTORY AB The late Paleocene-early Eocene transition was characterized by along period of global warming that culminated with the highest temperatures of the Cenozoic. This interval is associated with a significant increase in plant diversity in temperate latitudes. However, data from tropical regions remain largely unknown. The record of pollen and spore diversity across the late Paleocene to the early middle Eocene of eight sections in central and eastern Colombia was analyzed. Several techniques, including range-through method, rarefaction, bootstrap, detrended correspondence analysis, and Shannon index, were used to assess the significance of the observed diversity pattern. The palynofloral record indicates that the lower to middle Eocene contains a significantly higher palynofloral diversity than the underlying upper Paleocene strata. This pattern is maintained after accounting for sample size, number of samples/time unit, lithofacies, and depositional systems. Eocene palynofloras have higher alpha and beta diversities and a higher equitability than Paleocene palynofloras. This increase in diversity is the product of a gradual increase in the rate of first appearances and a gradual decrease in the rate of last appearances. The early to middle Eocene increase in diversity, as well as the increase in spore abundance and diversity, suggests that tropical (equatorial) climate became wetter during the early to middle Eocene. This interpretation favors causes for early Eocene warming that do not involve significant increases in greenhouse gases. Samples from strata associated with the Paleocene/Eocene thermal maximum were barren for palynomorphs, and the effects of this climatic event on tropical vegetation remains uncertain. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Jaramillo, CA (reprint author), Inst Colombiano Petr, AA-4185, Bucaramanga, Colombia. NR 87 TC 39 Z9 43 U1 0 U2 6 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2002 VL 28 IS 2 BP 222 EP 243 DI 10.1666/0094-8373(2002)028<0222:ROTVTP>2.0.CO;2 PG 22 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 563BE UT WOS:000176232900004 ER PT J AU Dondera, M Muller, HG Gavrila, M AF Dondera, M Muller, HG Gavrila, M TI Observability of the dynamic stabilization of ground-state hydrogen with superintense femtosecond laser pulses SO PHYSICAL REVIEW A LA English DT Article ID HIGH-FREQUENCY; ADIABATIC STABILIZATION; HIGH-INTENSITY; FIELDS; SUPPRESSION; IONIZATION; REGIME; ATOMS; MODEL AB Theoretical information on dynamic stabilization (DS) of the ground state of H is still fragmentary, while its detection has remained open because of a lack of lasers with the required characteristics. The problem has been reactivated by the new light sources that are being developed, such as VUV-FEL's or attosecond pulses from high-harmonic generation, which will offer adequate frequencies, intensities, and pulse durations. We are now presenting a mapping out of DS over an extended range of high frequencies, for pulses with various envelopes, peak intensities, and durations. We find prominent DS under conditions where our nonrelativistic, dipole approximation, and calculation should be valid. There is a marked dependence of DS on the pulse shape. The effect of quasistationary stabilization (of the rates) on DS is analyzed. We comment on the impact of our results on the detection possibility. We conclude that ground-state DS for H should be observable with the new light sources in a state-of-the-art experiment. C1 Univ Bucharest, Dept Phys, Bucharest 76900, Romania. FOM, Inst Atom & Mol Phys, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Dondera, M (reprint author), Univ Bucharest, Dept Phys, Bucharest 76900, Romania. RI Dondera, Mihai/O-4695-2014 NR 24 TC 17 Z9 17 U1 1 U2 7 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 2002 VL 65 IS 3 AR 031405 DI 10.1103/PhysRevA.65.031405 PN A PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 533UJ UT WOS:000174548500013 ER PT J AU Mair, A Hager, J Phillips, DF Walsworth, RL Lukin, MD AF Mair, A Hager, J Phillips, DF Walsworth, RL Lukin, MD TI Phase coherence and control of stored photonic information SO PHYSICAL REVIEW A LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; GROUP-VELOCITY; ATOMIC GAS; LIGHT; ENTANGLEMENT; ENSEMBLE; CAVITY AB We report the demonstration of phase coherence and control for the recently developed "light-storage'' technique. Specifically, we employ a dynamic form of electromagnetically induced transparency to bring the group velocity of a light pulse to zero, thereby mapping the photonic information into an ensemble spin coherence in warm Rb vapor. We then apply a pulsed magnetic field to vary the phase of the atomic spin excitations and map the altered information back into light. We detect the resultant phase shift in an optical interferometric measurement, thus confirming that the storage process preserves phase coherence. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, ITAMP, Cambridge, MA 02138 USA. RP Mair, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 103 Z9 106 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 MAR PY 2002 VL 65 IS 3 AR 031802 DI 10.1103/PhysRevA.65.031802 PN A PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 533UJ UT WOS:000174548500018 ER PT J AU Yurovsky, VA AF Yurovsky, VA TI Quantum effects on dynamics of instabilities in Bose-Einstein condensates SO PHYSICAL REVIEW A LA English DT Article ID MEAN-FIELD THEORY; ATTRACTIVE INTERACTIONS; TRAPPED GASES; MATTER WAVES; COLLAPSE; STATES AB Dynamics of fluctuations in unstable Bose-Einstein condensates is analyzed by the solution of approximate operator equations. In the case of a condensate with a negative scattering length the present treatment describes a delay of collapse, in agreement with recent experiments. In the case of a collision of two condensate wave packets it is shown that quantum effects lead to a Bose enhancement of elastic-scattering losses. In both cases the noncondensate atoms are formed as entangled pairs in squeezed states. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Natl Inst Stand & Technol, Atom Phys Div, Gaithersburg, MD 20899 USA. Tel Aviv Univ, Sch Chem, IL-69978 Tel Aviv, Israel. RP Yurovsky, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 38 TC 43 Z9 43 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 MAR PY 2002 VL 65 IS 3 AR 033605 DI 10.1103/PhysRevA.65.033605 PN B PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 533UK UT WOS:000174548600033 ER PT J AU Zhu, C Dalgarno, A Derevianko, A AF Zhu, C Dalgarno, A Derevianko, A TI van der Waals interactions between molecular hydrogen and alkali-metal atoms SO PHYSICAL REVIEW A LA English DT Article ID COEFFICIENTS; POLARIZABILITY; CONSTANTS AB In this paper, we have calculated the values of the C-6 coefficients and the anisotropy parameters g of the leading term of the van der Waals interactions between molecular hydrogen and alkali-metal atoms from Li to Fr. The uncertainties in our results are less than 2%. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Nevada, Dept Phys, Reno, NV 89557 USA. RP Zhu, C (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. RI Derevianko, Andrei/G-8356-2011 NR 9 TC 0 Z9 0 U1 0 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 2002 VL 65 IS 3 AR 034708 DI 10.1103/PhysRevA.65.034708 PN B PG 2 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 533UK UT WOS:000174548600107 ER PT J AU Kirby, K Czujko, R Mulvey, P AF Kirby, K Czujko, R Mulvey, P TI 'Pipeline' provides physicists with flexibility - Reply SO PHYSICS TODAY LA English DT Letter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Amer Inst Phys, College Pk, MD USA. RP Kirby, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD MAR PY 2002 VL 55 IS 3 BP 12 EP 13 PG 2 WC Physics, Multidisciplinary SC Physics GA 525PC UT WOS:000174079300006 ER PT J AU Warkentin, KM AF Warkentin, KM TI Hatching timing, oxygen availability, and external gill regression in the tree frog, Agalychnis callidryas SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID RED-EYED TREEFROG; XENOPUS-LAEVIS; PREDATION RISK; EGG MASSES; EMBRYOS; RESPIRATION; AMBYSTOMA; LARVAE; CONSUMPTION; INCUBATION AB The physiological role of the embryonic external gills in anurans is equivocal. In some species, diffusion alone is clearly sufficient to supply oxygen throughout the embryonic period. In others, morphological elaboration and environmental regulation of the external gills suggest functional importance. Since oxygen stress is a common trigger of hatching, I examined the relationships among hatching timing, oxygen stress, and external gill loss. I worked with the red-eyed tree frog, Agalychnis callidryas, a species with arboreal eggs and aquatic tadpoles in which gill regression is associated with hatching, and hatching timing affects posthatching survival with aquatic predators. Both exposure to a hypoxic gas mixture and submergence in water, a natural context in which hypoxic stress can occur, induced early hatching. Exposure to hyperoxic gas mixtures induced regression of external gills, and subsequent exposure to air induced early hatching. Prostaglandin-induced external gill regression also induced hatching, and this effect was partially ameliorated by exposure to hyperoxic gas. Together, these results suggest that external gills enhance the oxygen uptake of embryos and are necessary to extend embryonic development past the onset of hatching competence. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Warkentin, KM (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. NR 38 TC 34 Z9 34 U1 1 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD MAR-APR PY 2002 VL 75 IS 2 BP 155 EP 164 DI 10.1086/339214 PG 10 WC Physiology; Zoology SC Physiology; Zoology GA 615AC UT WOS:000179222800005 PM 12024291 ER PT J AU Mahapatra, PR Benner, LAM Ostro, SJ Jurgens, RF Giorgini, JD Yeomans, DK Chandler, JF Shapiro, II AF Mahapatra, PR Benner, LAM Ostro, SJ Jurgens, RF Giorgini, JD Yeomans, DK Chandler, JF Shapiro, II TI Radar observations of asteroid 7335 (1989 JA) SO PLANETARY AND SPACE SCIENCE LA English DT Article DE asteroids; radar AB Radar observations of 1989 JA during its discovery apparition yielded dual-polarization echo spectra on two dates at Arecibo and three dates at Goldstone. The echoes indicate that this object has an effective diameter within a factor of two of 1 km, a rotation period less than half a day, and a surface that is fairly smooth at centimeter-to-meter scales. (C) 2002 Elsevier Science Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Indian Inst Sci, Bangalore 560012, Karnataka, India. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ostro, SJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 2 Z9 2 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD MAR PY 2002 VL 50 IS 3 BP 257 EP 260 AR PII S0032-0633(02)00002-8 DI 10.1016/S0032-0633(02)00002-8 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 547UD UT WOS:000175349800002 ER PT J AU Kenyon, SJ AF Kenyon, SJ TI Planet formation in the outer solar system SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Editorial Material ID EDGEWORTH-KUIPER BELT; SHORT-PERIOD COMETS; TRANS-NEPTUNIAN OBJECTS; JUPITER-FAMILY COMETS; COMPACT RADIO GALAXY; SLOW-MOVING OBJECTS; N-BODY SIMULATIONS; GIANT PLANETS; COLLISIONAL EVOLUTION; CIRCUMSTELLAR DISK AB This paper reviews coagulation models for planet formation in the Kuiper belt, emphasizing links to recent observations of our and other solar systems. At heliocentric distances of 35-50 AU, single-annulus and multiannulus planetesimal accretion calculations produce several 1000 km or larger planets and many 50-500 km objects on timescales of 10-30 Myr in a minimum-mass solar nebula. Planets form more rapidly in more massive nebulae. All models yield two power-law cumulative size distributions, N-C proportional to r(-q) with q = 3.0-3.5 for radii r greater than or similar to 10 km and N-C proportional to r(-2.5) for radii r less than or similar to 1 km. These size distributions are consistent with observations of Kuiper belt objects acquired during the past decade. Once large objects form at 35-50 AU, gravitational stirring leads to a collisional cascade where 0.1-10 km objects are ground to dust. The collisional cascade removes 80%-90% of the initial mass in the nebula in similar to1 Gyr. This dust production rate is comparable to rates inferred for alpha Lyr, beta Pic, and other extrasolar debris disk systems. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X NR 185 TC 69 Z9 69 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR PY 2002 VL 114 IS 793 BP 265 EP 283 DI 10.1086/339188 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525LU UT WOS:000174073900001 ER PT J AU Preciado, ME Boroson, B Vrtilek, SD AF Preciado, ME Boroson, B Vrtilek, SD TI The ultraviolet light curve of LMC X-4: X-ray heating of the O star and accretion disk SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID HUBBLE-SPACE-TELESCOPE; EXPLORER IUE; MULTIWAVELENGTH CAMPAIGN; PHOTOMETRIC CALIBRATION; LOW-DISPERSION; PERIOD CHANGES; FINAL ARCHIVE; ORBITAL DECAY; STELLAR WIND; NEUTRON-STAR AB We present an archival study of ultraviolet spectra of the X-ray binary LMC X-4 obtained with the IUE satellite. We fit these spectra with models that incorporate the X-ray heating of the O star and accretion disk. A systematic analysis of the UV continuum confirms the general picture of an O star that fills its Roche lobe and is heated by X-rays from the neutron star. About 5% of the UV emission arises in an accretion disk, which may precess with a approximate to30 day period. We measure the mass transfer through the accretion disk and attempt to relate this quantity to changes in the pulse period and disk precession. The principal source of uncertainty in our model results from the choice of the 30 day disk precession ephemeris. We examine the RXTE All-Sky Monitor data for LMC X-4 to attempt to clarify the variability of the 30 day period. We find no evidence for additional heating of the O star or disk as the result of an X-ray flare observed with IUE and EXOSAT in 1983. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Claremont Coll, Joint Sci Dept, Claremont, CA 91711 USA. RP Preciado, ME (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 43 TC 2 Z9 2 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR PY 2002 VL 114 IS 793 BP 340 EP 349 DI 10.1086/339254 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525LU UT WOS:000174073900006 ER PT J AU Leverington, DW Mann, JD Teller, JT AF Leverington, DW Mann, JD Teller, JT TI Changes in the bathymetry and volume of glacial Lake Agassiz between 9200 and 7700 C-14 yr BP SO QUATERNARY RESEARCH LA English DT Article DE Lake Agassiz; Lake Ojibway; bathymetry; volume ID LAURENTIDE ICE-SHEET; YOUNGER DRYAS; MELTWATER; OUTLET AB Computer reconstructions of the bathymetry of the lake were used to quantify variations in the size and form of Lake Agassiz during its final two phases (the Nipigon and Ojibway phases), between about 9200 and 7700 C-14 yr B.P. (ca. 10,300-8400 cal yr B.P.). New bathymetric models for four Nipigon Phase stages (corresponding to the McCauleyville, Hillsboro, Burnside, and The Pas strandlines) indicate that Lake Agassiz ranged between about 19,200 and 4600 km(3) in volume and 254,000 and 151,000 km(2) in areal extent at those times. A bathymetric model of the last (Ponton) stage of the lake, corresponding to the period in which Lake Agassiz was combined with glacial Lake Ojbway to the east, shows that Lake Agassiz-Ojibway was about 163,000 km(3) in volume and 841,000 km(2) in areal extent prior to the final release of lake waters into the Tyrrell Sea. During the Nipigon Phase, a number of catastrophic releases of water from Lake Agassiz occurred as more northerly (lower) outlets were made available by the retreating southern margin of the Laurentide Ice Sheet; we estimate that each of the four newly investigated Nipigon Phase releases involved water volumes of between 1600 and 2300 km(3). The final release of Lake Agassiz waters into the Tyrrell Sea at about 7700 C-14 yr B.P. is estimated to have been about 163,000 km(3) in volume. (C) 2002 University of Washington. C1 Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. RP Leverington, DW (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 41 TC 53 Z9 55 U1 2 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD MAR PY 2002 VL 57 IS 2 BP 244 EP 252 DI 10.1006/qres.2001.2311 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 532MZ UT WOS:000174480200007 ER PT J AU Deocampo, DM Blumenschine, RJ Ashley, GM AF Deocampo, DM Blumenschine, RJ Ashley, GM TI Wetland diagenesis and traces of early hominids, Olduvai Gorge, Tanzania SO QUATERNARY RESEARCH LA English DT Article DE Olduvai; diagenesis; clay minerals; early hominids; landscape paleoanthropology ID LAND-USE; BASIN; LAKE; KEROLITE; PATTERNS; NEVADA; KENYA AB Lateral variations in whole-rock and clay geochemistry of basal Bed II claystones in Olduvai Gorge, Tanzania, reflect water quality differences across the Eastern Lacustrine Plain similar to1.75 myr ago. Bulk Ba/Sr and (Na2O + K2O + MgO)/Al2O3 range from 1.4 to 4.2 and from 0.7 to 1.4, respectively, and indicate leaching of lacustrine claystones beneath freshwater wetlands at times following lake retreat. Bulk MgO/Al2O3 (0.3-1.0) and molar Mg/Al (0.5-3.9) ratios of <0.2-mum clays reflect alteration of Mg-rich lacustrine clays. These indicators point to freshest conditions near Locality 43 of Hay (1976; HWK-East; Leakey, 1971), moderate conditions to the east (Locality 40-MCK), and high salinity and alkalinity to the west (Localities 85-VEK, 45-FLK). Clay geochemistry and artifact abundances are well correlated (r = -0.67, p < 0.005), suggesting a relationship between paleowater quality and hominid paleoecology. This pattern is consistent with predictions of greatest artifact discard/loss around freshwater sources where scavanging opportunities were greatest for hominids. This quantifies a relationship between artifact density distribution and a paleoecological proxy over landscape scales for the first time in Early Stone Age archaeology. In contrast, fossil bone abundance is uncorrelated (r = 0.14, p = 0.6), reflecting more complex taphonomic processes. Quantitative tests of landscape-scale land-use models are important for understanding early hominid behavior and its evolution. (C) 2002 University of Washington. C1 Rutgers State Univ, Dept Geol Sci, Piscataway, NJ 08854 USA. Rutgers State Univ, Dept Anthropol, New Brunswick, NJ 08901 USA. Rutgers State Univ, Dept Geol Sci, Piscataway, NJ 08854 USA. RP Deocampo, DM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, MRC 119, Washington, DC 20560 USA. RI Deocampo, Daniel/A-9830-2010 NR 39 TC 37 Z9 38 U1 0 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD MAR PY 2002 VL 57 IS 2 BP 271 EP 281 DI 10.1006/qres.2001.2317 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 532MZ UT WOS:000174480200010 ER PT J AU Laurence, WF Fearnside, PM AF Laurence, WF Fearnside, PM TI Issues in Amazonian development SO SCIENCE LA English DT Letter C1 Smithsonian Trop Res Inst, Balboa, Panama. Natl Inst Amazonian Res, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Natl Inst Amazonian Res, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. RP Laurence, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. RI Fearnside, Philip/D-6559-2011 OI Fearnside, Philip/0000-0003-3672-9082 NR 7 TC 12 Z9 13 U1 0 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 1 PY 2002 VL 295 IS 5560 BP 1643 EP 1643 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 527XH UT WOS:000174212900019 PM 11881632 ER PT J AU Small, LM AF Small, LM TI Dust-free art (Hirshhorn Museum collection) SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAR PY 2002 VL 32 IS 12 BP 16 EP 16 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 527XB UT WOS:000174212300002 ER PT J AU Funk, VA Sakai, AK Richardson, K AF Funk, VA Sakai, AK Richardson, K TI Biodiversity: The interface between systematics and conservation SO SYSTEMATIC BIOLOGY LA English DT Editorial Material C1 Smithsonian Inst, US Natl Herbarium, Washington, DC 20560 USA. Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada. RP Funk, VA (reprint author), Smithsonian Inst, US Natl Herbarium, Washington, DC 20560 USA. NR 2 TC 13 Z9 14 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD MAR-APR PY 2002 VL 51 IS 2 BP 235 EP 237 DI 10.1080/10635150252899743 PG 3 WC Evolutionary Biology SC Evolutionary Biology GA 545NA UT WOS:000175222800003 PM 12028730 ER PT J AU Sakai, AK Wagner, WL Mehrhoff, LA AF Sakai, AK Wagner, WL Mehrhoff, LA TI Patterns of endangerment in the Hawaiian flora SO SYSTEMATIC BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Biodiversity, Systematics, and Conservation CY JUN, 2000 CL INDIANA UNIV, BLOOMINGTON, INDIANA SP Soc Systemat Biologists, Assoc Trop Biologists, Natl Museum Nat Hist, Smithsonian Inst HO INDIANA UNIV DE angiosperms; biogeography; conservation planning; endangered plants; endemism; extinction; Hawaiian Islands; rarity ID RARE; RARITY; BIODIVERSITY; CONSERVATION; EVOLUTION; PLANTS; DIOECY; DIVERSIFICATION; CARYOPHYLLACEAE; ALSINOIDEAE AB The Hawaiian flora, because of its great isolation, high levels of endemism, known lineages, and high rates of endangerment, offers unique opportunities to explore patterns of endangerment related to phylogeny, ecological and life history traits, and geographic patterns. Nine percent of the native flora of 1159 taxa are already extinct, and 52.5% are at risk (extinct, endangered, vulnerable, or rare). Risk is strongly associated with limited geographic distribution at several scales: endemic taxa (native only to the Hawaiian Islands) are at far greater risk than indigenous taxa (with both Hawaiian and extra-Hawaiian ranges); single-island endemics are more at risk than multi-island endemics; small islands have the highest proportion of endemic taxa at risk; and endemics with more limited habitat distributions (elevation, community type) are more at risk. Historic population density is a strong predictor of risk, and taxa with low historic population densities are at greatest risk with rapid anthropogenic changes. Among the major islands, Maui Nui has the highest percent of taxa that are extinct. Kaua'i has the lowest percent of extinct taxa and the highest proportion of single-island endemic taxa that are rare. Endemic taxa at risk are associated with distributions in shrublands, forests, bogs, and cliff habitats. Endemic taxa with distributions in low elevation dry habitats have the highest proportion of taxa at risk, but the greatest absolute numbers of taxa at risk have distributions in mesic lowland and montane forests, and in wet montane forests. The life history patterns associated with risk are complicated, and inclusion of the effects of evolutionary relationships (lineages) changes some of these patterns. Species level analyses without respect to lineage shows risk associated with monomorphic (hermaphroditic) breeding systems and bird pollination because of the large number of hermaphroditic, bird-pollinated species in the Campanulaceae. Analyses incorporating the effect of lineage greatly reduce the impact of large lineages and result in an association of risk with insect pollination, and no effect of breeding system. There is no association of lineage size and the percent of taxa at risk within the lineage; endemic taxa from lineages with large radiations are at no greater risk than endemic single-taxon lineages. The percentages of taxa at risk at the family level in the Hawaiian Islands and worldwide (excluding Hawaiian taxa) are positively correlated, although flowering plant families in the Hawaiian Islands have a much greater proportion of taxa at risk. Some of the approaches described here may be useful to predict geographical and biological patterns of endangerment in island and island-like ecosystems under increasing pressures of endangerment and extinction. C1 Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Natl Pk Serv, Endangered Species Program, Ft Collins, CO 80525 USA. RP Sakai, AK (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. NR 68 TC 49 Z9 58 U1 8 U2 24 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 MAR-APR PY 2002 VL 51 IS 2 BP 276 EP 302 DI 10.1080/10635150252899770 PG 27 WC Evolutionary Biology SC Evolutionary Biology GA 545NA UT WOS:000175222800006 PM 12028733 ER PT J AU Funk, VA Richardson, KS AF Funk, VA Richardson, KS TI Systematic data in biodiversity studies: Use it or lose it SO SYSTEMATIC BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Biodiversity, Systematics, and Conservation CY JUN, 2000 CL INDIANA UNIV, BLOOMINGTON, IN SP Soc Systemat Biologists, Assoc Trop Biologists, Natl Museum Nat Hist, Smithsonian Inst HO INDIANA UNIV DE biodiversity; collections data; conservation planning; Guyana; irreplaceability ID PROTECTED AREA STRATEGY; RESERVE SELECTION; CONSERVATION STRATEGIES; SOUTH-AFRICA; DIVERSITY; HOTSPOTS; GUYANA; REPRESENTATIVENESS; IRREPLACEABILITY; INDICATORS AB Systematic data in the form of collections data are useful in biodiversity studies in many ways, most importantly because they serve as the only direct evidence of species distributions. However, collecting bias has been demonstrated for most areas of the world and has led some to propose methods that circumvent the need for collections data. New methods that model collections data in combination with abiotic data and predict potential total species distribution are examined using 25,111 records representing 5, 123 species of plants and animals from Guyana; some methods use the reduced number of 320 species. These modeled species distributions are evaluated and potential high-priority biodiversity sites are selected based on the concept of irreplaceability, a measure of uniqueness. The major impediments to using collections data are the lack of data that are available in a useful format and the reluctance of most systematists to become involved in biodiversity and conservation research. C1 Smithsonian Inst, US Natl Herbarium, Washington, DC 20560 USA. McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada. RP Funk, VA (reprint author), Smithsonian Inst, US Natl Herbarium, Washington, DC 20560 USA. EM funkv@nmnh.si.edu NR 59 TC 88 Z9 101 U1 1 U2 14 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD MAR-APR PY 2002 VL 51 IS 2 BP 303 EP 316 DI 10.1080/10635150252899789 PG 14 WC Evolutionary Biology SC Evolutionary Biology GA 545NA UT WOS:000175222800007 PM 12028734 ER PT J AU Harris, SC Holzenthal, RW Flint, OS AF Harris, SC Holzenthal, RW Flint, OS TI Review of the Neotropical genus Bredinia (Trichoptera : Hydroptilidae : Stactobiini) SO ANNALS OF CARNEGIE MUSEUM LA English DT Review DE Trichoptera; Hydroptilidae; Neotropics; Bredinia; new species; key; systematics AB The Neotropical genus Bredinia is reviewed, with descriptions and figures provided for the 16 species presently known, including 13 new species: B. guanacasteca n.sp., B. emarginata n.sp., and B. selva n.sp. from Costa Rica; B. davenporti n.sp. and B. pilcopata n.sp. from Peru; B. manabiensis n.sp. and B. spangleri n.sp. from Ecuador; B. alza n.sp. from Paraguay; B. mexicana n.sp. from Mexico; B. sucrensis n.sp. and B. zulia n.sp. from Venezuela; B. espinosa n.sp. from Brazil, Ecuador, and Venezuela, and B. venezuelensis n.sp. from Venezuela, Peru, and Ecuador. New records and illustrations are provided for B. costaricensis (Flint), B. dominicensis Flint, and B. appendiculata Flint and Sykora. A key is provided to separate the males and the associated females. C1 Clarion Univ Pennsylvania, Dept Biol, Sect Invertebrate Zool, Clarion, PA 16214 USA. Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. Smithsonian Inst, Dept Entomol, Museum Natl Hist Nat, Washington, DC 20560 USA. RP Harris, SC (reprint author), Clarion Univ Pennsylvania, Dept Biol, Sect Invertebrate Zool, Clarion, PA 16214 USA. NR 8 TC 4 Z9 7 U1 0 U2 1 PU CARNEGIE MUSEUM NATURAL HISTORY PI PITTSBURGH PA 4400 FORBES AVE, PITTSBURGH, PA 15213 USA SN 0097-4463 J9 ANN CARNEGIE MUS JI Ann. Carnegie Mus. PD FEB 26 PY 2002 VL 71 IS 1 BP 13 EP 45 PG 33 WC Paleontology; Zoology SC Paleontology; Zoology GA 609NK UT WOS:000178911700002 ER PT J AU Towe, KM AF Towe, KM TI The problematic rise of Archean oxygen SO SCIENCE LA English DT Editorial Material ID EVOLUTION; IRON C1 Smithsonian Inst, Washington, DC 20560 USA. RP Towe, KM (reprint author), 230 W Adams St, Tennille, GA 31089 USA. NR 11 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 22 PY 2002 VL 295 IS 5559 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 523WV UT WOS:000173981300001 ER PT J AU Lira, P Ward, M Zezas, A Alonso-Herrero, A Ueno, S AF Lira, P Ward, M Zezas, A Alonso-Herrero, A Ueno, S TI Chandra observations of the luminous infrared galaxy NGC 3256 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : general; galaxies : individual : NGC 3256; galaxies : nuclei; X-rays : galaxies ID X-RAY-SPECTRA; STAR-FORMATION; GALACTIC SUPERWINDS; ROSAT OBSERVATIONS; STARBURST; EMISSION; NGC-3256; NUCLEUS; MERGER; NGC-253 AB We present a detailed analysis of high-resolution Chandra observations of the merger system NGC 3256, the most infrared-luminous galaxy in the nearby universe. The X-ray data show that several discrete sources embedded in complex diffuse emission contribute 20 per cent of the total emission (L-X(tot) similar to 8 x 10(41) erg s(-1) in the 0.5-10 keV energy range). The compact sources are hard and extremely bright and their emission is probably dominated by accretion-driven processes. Both galaxy nuclei are detected with L-X similar to 3-10 x 10(40) erg s(-1). No evidence is found for the presence of an active nucleus in the southern nucleus, contrary to previous speculation. Once the discrete sources are removed, the diffuse component has a soft spectrum that can be modelled by the superposition of three thermal plasma components with temperatures kT = 0.6, 0.9 and 3.9 keV. Alternatively, the latter component can be described as a power law with index Gamma similar to 3. Some evidence is found for a radial gradient of the amount of absorption and temperature of the diffuse component. We compare the X-ray emission with optical, Ha and NICMOS images of NGC 3256 and find a good correlation between the inferred optical/near-infrared and X-ray extinctions. Although inverse Compton scattering could be important in explaining the hard X-rays seen in the compact sources associated with the nuclei, the observed diffuse emission is probably of thermal origin. The observed X-ray characteristics support a scenario in which the powerful X-ray emission is driven solely by the current episode of star formation. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Chile, Dept Astron, Santiago, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hertfordshire, Dept Phys Sci, Hatfield AL10 9AB, Herts, England. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Natl Space Dev Agcy Japan, Tsukuba Space Ctr, Space Utilizat Res Program, Tsukuba, Ibaraki 305, Japan. RP Lira, P (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RI Lira, Paulina/G-8536-2016; Alonso-Herrero, Almudena/H-1426-2015; Zezas, Andreas/C-7543-2011 OI Alonso-Herrero, Almudena/0000-0001-6794-2519; Zezas, Andreas/0000-0001-8952-676X NR 61 TC 106 Z9 106 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2002 VL 330 IS 2 BP 259 EP 278 DI 10.1046/j.1365-8711.2002.05014.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 526XL UT WOS:000174155100007 ER PT J AU Lazzati, D Perna, R AF Lazzati, D Perna, R TI Determining the location of gamma-ray bursts through the evolution of their soft X-ray absorption SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-rays : bursts; X-rays : general; X-rays : ISM ID PHOTOELECTRIC ABSORPTION; AFTERGLOW; LINE; PROGENITORS; SUPERNOVAE; SIGNATURES; EMISSION; REDSHIFT; CLOUD; CORES AB We investigate through dedicated numerical simulations the evolution of the soft X-ray absorption properties of a cloud surrounding a gamma-ray burst source. We show that the absorption properties of the material are strongly modified by the ionization induced by the intense burst flux. We derive the temporal evolution of the measured column density as a function of the density and size of the absorbing medium. Even if their statistical significance is not extremely compelling, we find that the detection in several bursts of variable absorption during the gamma-ray phase can be accounted for if these bursts are associated to overdense regions in molecular clouds with properties similar to those of star formation globules. We fit our model variable column density to the data of GRB 980329 and GRB 780506, showing that with this method the size, density and density distribution of the material surrounding a burst can be measured. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lazzati, D (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. NR 45 TC 46 Z9 46 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2002 VL 330 IS 2 BP 383 EP 389 DI 10.1046/j.1365-8711.2002.05064.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 526XL UT WOS:000174155100016 ER PT J AU Lamers, HJGLM Panagia, N Scuderi, S Romaniello, M Spaans, M de Wit, WJ Kirshner, R AF Lamers, HJGLM Panagia, N Scuderi, S Romaniello, M Spaans, M de Wit, WJ Kirshner, R TI Ongoing massive star formation in the bulge of M51 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : bulges; galaxies : individual (M51, NGC 5194); galaxies : spiral; galaxies : stellar content; stars : evolution; stars : formation ID HUBBLE-SPACE-TELESCOPE; LARGE MAGELLANIC CLOUD; ANTENNAE GALAXIES; STELLAR CLUSTERS; NEARBY GALAXIES; EVOLUTION; COLORS; FIELD AB We present a study of Hubble Space Telescope Wide Field Planetary Camera 2 observations of the inner kiloparsec of the interacting galaxy M51 in six bands from 2550 to 8140 Angstrom. The images show an oval-shaped area (which we call the "bulge") of about 11" x 16", or 450 x 650 pc, around the nucleus that is dominated by a smooth "yellow/reddish" background population with overimposed dust lanes. These dust lanes are the inner extensions of the spiral arms. The extinction properties, derived in four fields in and outside dust lanes, are similar to the Galactic extinction law. The reddish stellar population has an intrinsic color of (B-V)(0) similar or equal to 1.0, suggesting an age in excess of 5 Gyr. We found 30 bright pointlike sources in the bulge of M51, i.e., within 110-350 pc from the nucleus. The point sources have 21.4 < V < 24.3, many of which are blue with B-V < 0 and are bright in the UV with 19.8 < m(2550) < 22.0. These objects appear to be located in elongated "strings" that follow the general pattern of the dust lanes around the nucleus. The spectral energy distributions of the pointlike sources are compared with those predicted for models of clusters or single stars. There are three reasons to conclude that most of these point sources are isolated massive stars (or very small groups of a few isolated massive stars) rather than clusters : 1. The energy distributions of most objects are best fitted with models of single stars of M-V between -6.1 and -9.1, temperatures between 4000 and 50,000 K, and with 4.2 < log (L/L.) < 7.2 and 12 M. < M-* < 200 M.. 2. In the Hertzsprung-Russel diagram the sources follow the Humphreys-Davidson luminosity upper limit for massive stars. 3. The distribution of the sources in the Hertzsprung-Russel diagram shows a gap in the range of 20,000K < T-eff < 10,000 K, which agrees with the rapid crossing of the Hertzsprung-Russel diagram by stars, but not of clusters. We have derived upper limits to the total mass of lower mass stars (M-* < 10 M.) that could be "hiding" within the point sources. For the "bluest" sources, the upper limit is only a few hundred M.. We conclude that the formation of massive stars outside clusters (or in very low mass clusters) is occurring in the bulge of M51. The estimated star formation rate in the bulge of M51 is (1-2) x 10(-3) M. yr(-1), depending on the adopted initial mass function. With the observed total amount of gas in the bulge, similar to4 x 10(5) M., and the observed normal gas-to-dust ratio of similar to150, this star formation rate could be sustained for about (2-4) x 10(8) yr. This suggests that the ongoing massive star formation in the bulge of M51 is fed/triggered by the interaction with its companion about 4 x 10(8) yr ago. The star formation in the bulge of M51 is compared with that in bulges of other spirals. Theoretical predictions of star formation suggest that isolated massive stars might be formed in clouds in which H-2, [O I] 63 mum and [C II] 158 mum are the dominant coolants. This is expected to occur in regions of rather low optical depth, A(V) less than or equal to 1 with a hot source that can dissociate the CO molecules. These conditions are met in the bulge of M51, where the extinction is low and where CO can be destroyed by the radiation from the bright nuclear starburst cluster in the center. The mode of formation of massive stars in the bulge of M51 may resemble the star formation in the early universe, when the CO and dust contents were low because of the low metallicity. C1 Astron Inst, NL-3584 CC Utrecht, Netherlands. SRON, Space Res Lab, NL-3584 CA Utrecht, Netherlands. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Osserv Astrofis Catania, I-95125 Catania, Italy. European So Observ, D-85748 Garching, Germany. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lamers, HJGLM (reprint author), Astron Inst, Princetonpl 5, NL-3584 CC Utrecht, Netherlands. OI Scuderi, Salvatore/0000-0002-8637-2109 NR 40 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 FEB 20 PY 2002 VL 566 IS 2 BP 818 EP 832 DI 10.1086/338273 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WE UT WOS:000173804900020 ER PT J AU Sridharan, TK Beuther, H Schilke, P Menten, KM Wyrowski, F AF Sridharan, TK Beuther, H Schilke, P Menten, KM Wyrowski, F TI High-mass protostellar candidates. I. The sample and initial results SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : ISM; ISM : clouds; ISM : molecules; radio lines : ISM; stars : formation; stars : mass loss ID ULTRACOMPACT HII-REGIONS; STAR-FORMATION REGIONS; LUMINOUS IRAS SOURCES; NRAO PMN SURVEYS; VLA OBSERVATIONS; MOLECULAR CLOUDS; GALACTIC-PLANE; SOURCE CATALOG; MAIN-SEQUENCE; DENSE CORES AB We describe a systematic program aimed at identifying and characterizing candidate high-mass protostellar objects (HMPOs). Our candidate sample consists of 69 objects selected by criteria based on those established by Ramesh & Sridharan using far-infrared, radio continuum, and molecular line data. IRAS and Midcourse Space Experiment data were used to study the larger scale environments of the candidate sources and determine their total luminosities and dust temperatures. To derive the physical and chemical properties of our target regions, we observed continuum and spectral line radiation at millimeter and radio wavelengths. We imaged the free-free and dust continuum emission at wavelengths of 3.6 cm and 1.2 mm, respectively, searched for H2O and CH3OH maser emission, and observed the CO J = 2 --> 1 line and several NH3 lines toward all sources in our sample. Other molecular tracers were observed in a subsample. While dust continuum emission was detected in all sources, most of them show only weak or no emission at 3.6 cm. Where detected, the centimeter emission is frequently found to be offset from the millimeter emission, indicating that the free-free and dust emissions arise from different subsources possibly belonging to the same (proto)cluster. A comparison of the luminosities derived from the centimeter emission with bolometric luminosities calculated from the IRAS far-infrared fluxes shows that the centimeter emission very likely traces the most massive source, whereas the whole cluster contributes to the far-infrared luminosity. Estimates of the accretion luminosity indicate that a significant fraction of the bolometric luminosity is still due to accretion processes. The earliest stages of HMPO evolution we seek to identify are represented by dust cores without radio emission. Line wings due to outflow activity are nearly omnipresent in the CO observations, and the molecular line data indicate the presence of hot cores for several sources, where the abundances of various molecular species are elevated because of evaporation of icy grain mantles. Kinetic gas temperatures of 40 sources are derived from NH3 (1, 1) and (2, 2) data, and we compare the results with the dust temperatures obtained from the IRAS data. Comparing the amount of dust, and hence the gas, associated with the HMPOs and with ultracompact H II (UCH II) regions, we find that the two types of sources are clearly separated in mass-luminosity diagrams: for the same dust masses, the UCH II regions have higher bolometric luminosities than HMPOs. We suggest that this is an evolutionary trend, with the HMPOs being younger and reprocessing less (stellar) radiation in the IR than the more evolved UCH II regions. These results indicate that a substantial fraction of our sample harbors HMPOs in a pre-UCH II region phase, the earliest known stage in the high-mass star formation process. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Sridharan, TK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. NR 75 TC 298 Z9 299 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2002 VL 566 IS 2 BP 931 EP 944 DI 10.1086/338332 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WE UT WOS:000173804900030 ER PT J AU Beuther, H Schilke, P Menten, KM Motte, F Sridharan, TK Wyrowski, F AF Beuther, H Schilke, P Menten, KM Motte, F Sridharan, TK Wyrowski, F TI High-mass protostellar candidates. II. Density structure from dust continuum and CS emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : molecules; radio continuum : ISM; radio lines : ISM; stars : formation ID ULTRACOMPACT HII-REGIONS; STAR-FORMATION REGIONS; LUMINOUS IRAS SOURCES; MOLECULAR CLOUDS; VLA OBSERVATIONS; CORES; AMMONIA; PROTOSTARS; PRECURSORS; G34.3+0.2 AB We present a detailed 1.2 mm continuum and CS spectral line study of a large sample of 69 massive star forming regions in very early stages of evolution, most of them prior to building up an ultracompact H II region. The continuum data show a zoo of different morphologies and give detailed information on the spatial distributions, masses, column densities, and average densities of the whole sample. Fitting the radial intensity profiles shows that three parameters are needed to describe the spatial distribution of the sources : constant emission from the center out to a few arcseconds radius followed by a first power-law intensity distribution, which steepens farther outside into a second power-law distribution. The inner flat region is possibly caused by fragmentation of the large-scale cores into smaller subsources, whereas the steeper outer power-law distributions indicate finite sizes of the cores. Separating the sources into subsamples suggests that in the earliest stages prior to the onset of massive star formation, the intensity radial distributions are rather flat, resembling the structure of intensity peaks in more quiescent molecular clouds. Then in the subsequent collapse and accretion phase the intensity distributions become centrally peaked, with steep power-law indices. In this evolutionary stage the sources show also the broadest (CS)-S-34 line width. During the following phase, when ultracompact H II regions evolve, the intensity power-law radial distributions flatten out again. This is probably caused by the ignited massive stars in the center which disrupt the surrounding cores. The mean inner power-law intensity index is 1.2, corresponding to density indices p (n similar to r(-p)) of 1.6. In total, the density distributions of our massive star formation sites seem to be not too different from their low-mass counterparts, but we show that setting tight constrains on the density indices is very difficult and subject to many possible errors. The local densities we derive from CS calculations are higher (up to 1 order of magnitude) than the mean densities we find via the millimeter continuum. Such inhomogeneous density distribution reflects most likely the ubiquitous phenomenon of clumping and fragmentation in molecular clouds. Line width-mass relations show a departure from virial equilibrium in the stages of strongly collapsing cores. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Beuther, H (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. NR 51 TC 315 Z9 318 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2002 VL 566 IS 2 BP 945 EP 965 DI 10.1086/338334 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WE UT WOS:000173804900031 ER PT J AU Zhang, QZ Hunter, TR Sridharan, TK Ho, PTP AF Zhang, QZ Hunter, TR Sridharan, TK Ho, PTP TI A disk/jet system toward the high-mass young star in AFGL 5142 SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : clouds; ISM : individual (AFGL 5142); ISM : kinematics and dynamics; masers; stars : formation; stars : pre-main-sequence ID MOLECULAR OUTFLOWS; HOT AMMONIA; CH3CN OBSERVATIONS; BIPOLAR OUTFLOWS; INFRARED SOURCES; STELLAR OBJECTS; IRAS 20126+4104; FORMING REGION; ROTATING-DISK; SIO EMISSION AB We present observational studies of a high-mass star-forming region AFGL 5142 in the NH(3) (J, K) = (1, 1), (2, 2), (3, 3), and (4, 4) inversion transitions. We discover a compact structure of 1" (or 1800 AU) in NH(3) emission toward the position of a high-mass young star. The star, with a spectral type of B2 if it is at the zero-age main sequence, excites a weak centimeter continuum source and drives a well-collimated SiO jet. The compact NH(3) structure, with a temperature of 70 K, gives rise to a broad NH(3) line emission of 6.4 km s(-1) (FWHM). The small size of the NH(3) feature, broad line emission, and the association with a SiO jet indicate that the object is most likely an unresolved rotating disk. The compact disk is embedded in a flattened core of gas temperatures of about 20 K. The extended core delineates an X shape with the SiO jet located in the void of the dense and cold NH(3) gas. A faint component of NH(3) emission can be identified, especially in the highly excited NH(3) (3, 3) and (4, 4) lines, tracing the SiO jet. This component, arising from hot gas of about 170 K, is likely heated by shocks in the outflow. The coincidence of a disk and a jet with the radio continuum source toward AFGL 5142 indicates that this high-mass star may have formed via a disk-mediated accretion process. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, QZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 NR 51 TC 57 Z9 57 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2002 VL 566 IS 2 BP 982 EP 992 DI 10.1086/338278 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WE UT WOS:000173804900034 ER PT J AU Allen, LE Myers, PC Di Francesco, J Mathieu, R Chen, H Young, E AF Allen, LE Myers, PC Di Francesco, J Mathieu, R Chen, H Young, E TI Hubble Space Telescope/NICMOS imaging survey of the Ophiuchus (Lynds 1688) cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; ISM : individual (rho Ophiuchi); stars : formation; stars : pre-main-sequence ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; INITIAL MASS FUNCTION; MAIN-SEQUENCE STARS; RHO-OPHIUCHI; DARK-CLOUD; INFRARED OBSERVATIONS; GSS-30; CORE; IMAGES AB We present a catalog of near-infrared photometry of young stars associated with the Ophiuchus molecular cloud based on observations made with the Hubble Space Telescope NICMOS3 camera at 1.1 and 1.6 mum. Our survey covers 0.02 deg(2) centered on the dense molecular cores in Lynds 1688. We detect 165 sources at 1.6 mum and 65 sources at 1.1 mum within our estimated completeness limits of 21.0 and 21.5 mag, respectively. An analysis of the cloud extinction, based on existing molecular line maps, suggests that most of the sources lying within the 40 extinction contour of the cloud are probable A V cloud members. Approximately half (58/108) of these sources are previously unpublished. The faint embedded sources revealed by these observations are spatially concentrated in three regions of high stellar space density (N > 10(4) stars pc(-3)). While the spatial distribution of these sources reflects that of the brighter, well-known population of young stars in Ophiuchus, it is distinctly different from the distribution of cool concentrations seen in the submillimeter. Seven new brown dwarf candidates are identified based on their infrared colors and their projected locations on high column density regions of the molecular cloud. Eight new candidate binary and five new candidate triple systems, having separations between 0."2 and 10" (29-1450 AU) are reported. The spatial resolution and sensitivity of these observations reveal five apparent disk/envelope systems seen via scattered light and four nebulous objects with complex morphologies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Allen, LE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS42, Cambridge, MA 02138 USA. NR 50 TC 57 Z9 57 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2002 VL 566 IS 2 BP 993 EP 1004 DI 10.1086/338128 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WE UT WOS:000173804900035 ER PT J AU Branch, D Benetti, S Kasen, D Baron, E Jeffery, DJ Hatano, K Stathakis, RA Filippenko, AV Matheson, T Pastorello, A Altavilla, G Cappellaro, E Rizzi, L Turatto, M Li, WD Leonard, DC Shields, JC AF Branch, D Benetti, S Kasen, D Baron, E Jeffery, DJ Hatano, K Stathakis, RA Filippenko, AV Matheson, T Pastorello, A Altavilla, G Cappellaro, E Rizzi, L Turatto, M Li, WD Leonard, DC Shields, JC TI Direct analysis of spectra of Type Ib supernovae SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; supernovae : general ID NGC 4214; OPTICAL-SPECTRA; IIB SUPERNOVA; SN 1993J; H-ALPHA; HELIUM; SPECTROSCOPY; EXCITATION; EVOLUTION; BINARIES AB Synthetic spectra generated with the parameterized supernova synthetic-spectrum code SYNOW are compared to photospheric-phase spectra of Type Ib supernovae (SNe Ib). Although the synthetic spectra are based on simplifying approximations, including spherical symmetry, they account well for the observed spectra. Our sample of SNe Ib obeys a tight relation between the velocity at the photosphere, as determined from the Fe II features, and the time relative to that of maximum light. From this we infer that the masses and the kinetic energies of the events in this sample were similar. After maximum light the minimum velocity at which the He I features form usually is higher than the velocity at the photosphere, but the minimum velocity of the ejected helium is at least as low as 7000 km s(-1). Spectra of SN 2000H reveal the presence of hydrogen absorption features, and we conclude that hydrogen lines also were present in SNe 1999di and 1954A. Hydrogen appears to be present in SNe Ib in general, although in most events it becomes too weak to identify soon after maximum light. The hydrogen-line optical depths that we use to fit the spectra of SNe 2000H, 1999di, and 1954A are not high, so only a mild reduction in the hydrogen optical depths would be required to make these events look like typical SNe Ib. Similarly, the He I line optical depths are not very high, so a moderate reduction would make SNe Ib look like SNe Ic. C1 Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Osserv Astron Padova, I-35122 Padua, Italy. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. New Mexico Inst Min & Technol, Dept Phys, Astrophys Res Ctr, Socorro, NM 87801 USA. Res Ctr Early Universe, Tokyo, Japan. Anglo Australian Observ, Epping, NSW 1710, Australia. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Univ Massachusetts, Five Coll Astron Dept, Amherst, MA 01003 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. RP Branch, D (reprint author), Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. RI Baron, Edward/A-9041-2009; Altavilla, Giuseppe/O-9454-2015; OI Baron, Edward/0000-0001-5393-1608; Altavilla, Giuseppe/0000-0002-9934-1352; Cappellaro, Enrico/0000-0001-5008-8619; Benetti, Stefano/0000-0002-3256-0016; Turatto, Massimo/0000-0002-9719-3157 NR 41 TC 105 Z9 108 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2002 VL 566 IS 2 BP 1005 EP 1017 DI 10.1086/338127 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WE UT WOS:000173804900036 ER PT J AU Murray, SS Ransom, SM Juda, M Hwang, U Holt, SS AF Murray, SS Ransom, SM Juda, M Hwang, U Holt, SS TI Is the compact source at the center of Cassiopeia A pulsed? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Cassiopeia A); pulsars : general; stars : neutron; supernova remnants; X-rays : stars ID RESOLUTION CAMERA HRC; RAY; STARS; MASS; AXAF AB A 50 ks observation of the supernova remnant Cas A was taken, using the Chandra X-Ray Observatory High-Resolution Camera (HRC) to search for periodic signals from the compact source located near the center. Using the HRC-S in imaging mode, problems with correctly assigning times to events were overcome, allowing the period search to be extended to higher frequencies than possible with previous observations. In an extensive analysis of the HRC data, several possible candidate signals are found using various algorithms, including advanced techniques recently developed by Ransom to search for low-significance periodic signals. Of these possible periods, none is at a high enough confidence level to be particularly favored over the rest. When combined with other information, however (e.g., spectra, total energetics, and the historical age of the remnant), a 12 ms period seems to be more physically plausible than the others, and we use it for illustrative purposes in discussing the possible properties of a putative neutron star in the remnant. We emphasize that this is not necessarily the true period, and that a follow-up observation, scheduled for the fall of 2001, is required. A 50 ks Advanced CCD Imaging Spectrometer (ACIS) observation was taken, and analysis of these data for the central object shows that the spectrum is consistent with several forms and that the emitted X-ray luminosity in the 0.1-10 keV band is 10(33)-10(35) ergs cm(-2) s(-1), depending on the spectral model and the interstellar absorption along the line of sight to the source. The spectral results are consistent with those of Pavlov et al. and Chakrabarty et al. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Olin Coll Engn, Needham, MA 02492 USA. RP Murray, SS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Juda, Michael/0000-0002-4375-9688; Ransom, Scott/0000-0001-5799-9714 NR 25 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 FEB 20 PY 2002 VL 566 IS 2 BP 1039 EP 1044 DI 10.1086/338224 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WE UT WOS:000173804900038 ER PT J AU Luhman, KL Jayawardhana, R AF Luhman, KL Jayawardhana, R TI An adaptive optics search for companions to stars with planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; planetary systems; stars : low-mass, brown dwarfs; techniques : high angular resolution ID EXTRASOLAR GIANT PLANETS; SOLAR-TYPE STARS; LOW-MASS STARS; UPSILON-ANDROMEDAE; BROWN DWARF; NEARBY STARS; FIRST LIGHT; DISCOVERY; SYSTEM; EVOLUTIONARY AB We have performed a Keck adaptive optics (AO) imaging survey of 25 extrasolar planetary systems discovered by the radial velocity programs. Typically, the high-resolution (FWHM similar to 0."04) near-infrared images are able to detect point sources at DeltaH = 10 at 1", L and T dwarfs at 0."5-2", and stars and brown dwarfs at 3-10 and 10-100 AU from the targets. The AO images reveal 15 faint sources (H = 14- 20) near the stars HD 37124, HD 168443, HD 187123, and HD 190228 out to a search radius of 3."3. We have obtained AO images at a second epoch for five of the candidate companions at Keck and Gemini Observatories. The resulting measurements of proper motions relative to the primary stars indicate that these five sources are background stars. Given that the four primaries are near the Galactic plane (\b\ < 6&DEG;), the remaining faint sources are also likely to be background stars rather than substellar companions. We present the companion detection limits for each target as a function of separation and compare them to the sensitivities of radial velocity surveys, demonstrating the complementary nature of the two techniques. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 74 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 FEB 20 PY 2002 VL 566 IS 2 BP 1132 EP 1146 DI 10.1086/338338 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WE UT WOS:000173804900047 ER PT J AU Risaliti, G Elvis, M Gilli, R AF Risaliti, G Elvis, M Gilli, R TI The contribution of quasars to the far-infrared background SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; infrared : galaxies; X-rays : diffuse background ID ACTIVE GALACTIC NUCLEI; X-RAY; EMISSION AB Recent observational results obtained with the Submillimeter Common-User Bolometric Array, COBE, and the Infrared Space Observatory have greatly improved our knowledge of the infrared and submillimeter background radiation. These limits become constraining given the realization that most active galactic nuclei (AGNs) are heavily obscured and must reradiate strongly in the IR/submillimeter wavelengths. Here we predict the contribution of AGNs to the IR/submillimeter background, starting from measurements of the hard X-ray background. We show that an application of what we know of AGN spectral energy distributions and the IR background requires that a significant fraction of the 10-150 mum background comes from AGNs. This conclusion can be avoided only if obscured AGNs are intrinsically brighter in the X-rays (with respect to the optical-UV) than unobscured AGNs, which is contrary to "unified schemes" for AGNs, or if they have a dust-to-gas ratio much lower (less than or equal to0.1) than Galactic. We show that these results are rather robust and not strongly dependent on the details of the modeling. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gilli, Roberto/P-1110-2015; OI Gilli, Roberto/0000-0001-8121-6177; Risaliti, Guido/0000-0002-3556-977X NR 37 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 FEB 20 PY 2002 VL 566 IS 2 BP L67 EP L70 DI 10.1086/339593 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520WF UT WOS:000173805100002 ER PT J AU Labandeira, CC Johnson, KR Wilf, P AF Labandeira, CC Johnson, KR Wilf, P TI Impact of the terminal Cretaceous event on plant-insect associations SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID TERTIARY BOUNDARY; FOSSIL RECORD; CONFIDENCE-INTERVALS; EARLY EVOLUTION; NORTH-DAKOTA; LEAF BEETLES; DEAD-END; EXTINCTION; SPECIALIZATION; HYMENOPTERA AB Evidence for a major extinction of insect herbivores is provided by presence-absence data for 51 plant-insect associations on 13,441 fossil plant specimens, spanning the Cretaceous/Paleogene boundary in southwestern North Dakota. The most specialized associations, which were diverse and abundant during the latest Cretaceous, almost disappeared at the boundary and failed to recover in younger strata even while generalized associations regained their Cretaceous abundances. These results are consistent with a sudden ecological perturbation that precipitated a diversity bottleneck for insects and plants. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. Denver Museum Nat & Sci, Dept Earth Sci, Denver, CO 80205 USA. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. Univ Michigan, Dept Geol Sci, Ann Arbor, MI 48109 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM labandeira.conrad@nmnh.si.edu NR 54 TC 137 Z9 142 U1 4 U2 33 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 19 PY 2002 VL 99 IS 4 BP 2061 EP 2066 DI 10.1073/pnas.042492999 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 524UK UT WOS:000174031100057 PM 11854501 ER PT J AU Bodo, E Gianturco, FA Dalgarno, A AF Bodo, E Gianturco, FA Dalgarno, A TI Quenching of vibrationally excited CO(nu=2) molecules by ultra-cold collisions with He-4 atoms SO CHEMICAL PHYSICS LETTERS LA English DT Article AB The quenching of vibrational excited CO(nu = 2) molecules by He atoms at ultra-low temperature is examined to determine the relative efficiency of the processes that involve the exchange of a double or a single quantum of vibrational energy. We find that at low temperature the double quantum exchange cross-section is orders of magnitude smaller than for the single quantum process. This result is valid for different initial rotational states of the CO molecule. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Univ Roma La Sapienza, Dept Chem, I-00185 Rome, Italy. Univ Roma La Sapienza, INFM, I-00185 Rome, Italy. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Bodo, E (reprint author), Univ Roma La Sapienza, Dept Chem, P Aldo Moro 5, I-00185 Rome, Italy. RI Bodo, Enrico/F-4375-2012 NR 20 TC 19 Z9 19 U1 1 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD FEB 13 PY 2002 VL 353 IS 1-2 BP 127 EP 130 AR PII S0009-2614(01)01501-9 DI 10.1016/S0009-2614(01)01501-9 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 522VV UT WOS:000173918400019 ER PT J AU Rusin, D Norbury, M Biggs, AD Marlow, DR Jackson, NJ Browne, IWA Wilkinson, PN Myers, ST AF Rusin, D Norbury, M Biggs, AD Marlow, DR Jackson, NJ Browne, IWA Wilkinson, PN Myers, ST TI High-resolution observations and mass modelling of the CLASS gravitational lens B1152+199 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; galaxies : structure ID TIME-DELAY; GALAXY STRUCTURE; HUBBLE-CONSTANT; B1608+656; H-0; VLA AB We present a series of high-resolution radio and optical observations of the CLASS gravitational lens system B1152+199 obtained with the Multi-Element Radio-Linked Interferometer Network, Very Long Baseline Array and Hubble Space Telescope. Based on the milliarcsecond-scale substructure of the lensed radio components and precise optical astrometry for the lensing galaxy, we construct models for the system and place constraints on the galaxy mass profile. For a single galaxy model with surface mass density Sigma(r) proportional to r(-beta), we find that 0.95 less than or equal to beta less than or equal to 1.21 at 2sigma confidence. Including a second deflector to represent a possible satellite galaxy of the primary lens leads to slightly steeper mass profiles. C1 Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Rusin, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. NR 32 TC 45 Z9 45 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2002 VL 330 IS 1 BP 205 EP 211 DI 10.1046/j.1365-8711.2002.05043.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 525FG UT WOS:000174057700025 ER PT J AU Nelson, AE Gonzalez, AH Zaritsky, D Dalcanton, JJ AF Nelson, AE Gonzalez, AH Zaritsky, D Dalcanton, JJ TI Revisiting brightest cluster galaxy evolution with the Las Campanas Distant Cluster Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : formation; galaxies : high-redshift; surveys ID PHOTOMETRIC STANDARD STARS; COLOR-MAGNITUDE RELATION; BAND HUBBLE DIAGRAM; SURFACE PHOTOMETRY; CELESTIAL EQUATOR; RICH CLUSTERS; REDSHIFT; RADIATION; TELESCOPE; EMISSION AB We investigate the influence of environment on brightest cluster galaxy (BCG) evolution using a sample of 63 clusters at 0.3 less than or equal to z less than or equal to 0.9 drawn primarily from the Las Campanas Distant Cluster Survey and follow-up V, I, and K' photometry. The luminosity evolution of the entire BCG sample is not adequately described by a single evolutionary model. Using the integrated light from the cluster detection as a proxy for cluster L-X and the suggestion by Burke, Collins, & Mann, we set L-X = 2 x 10(44) ergs s(-1) to be the division between high- and low-luminosity clusters. At high redshift (z > 0.6) BCGs from low-L-X clusters are fainter, on average, than those from high-L-X clusters and are best modeled as having constant luminosity with redshift. The BCGs from clusters are best modeled as having a stellar population that formed at large redshift (z(form) > 5) and is passively evolving. However, for the entire BCG population, the observed V - I and I - K' colors are well described by a single evolutionary model in which the stellar populations have zform > 5 and subsequently passively evolve. We conclude that accretion is proportionally more significant for BCGs in lower mass clusters at these redshifts (a factor of 2-4 increase in mass since z similar to 1 for the low-L-X systems; Aragon-Salamanca and coworkers) and that the accreted matter is in the form of systems with evolved stellar populations. C1 Univ Calif Santa Cruz, Board Astron & Astrophys, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Nelson, AE (reprint author), Univ Calif Santa Cruz, Board Astron & Astrophys, Santa Cruz, CA 95064 USA. NR 53 TC 21 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2002 VL 566 IS 1 BP 103 EP 122 DI 10.1086/338054 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EB UT WOS:000173766700009 ER PT J AU Igumenshchev, IV Narayan, R AF Igumenshchev, IV Narayan, R TI Three-dimensional magnetohydrodynamic simulations of spherical accretion SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; convection; galaxies : nuclei; MHD; supernovae : general; turbulence ID EMERGENT RADIATION SPECTRUM; ISOLATED NEUTRON-STARS; BLACK-HOLE MODEL; MAGNETIC-FIELD; SAGITTARIUS-A; FLOWS; CONVECTION; SUPERNOVA; EMISSION; MATTER AB We present three-dimensional numerical magnetohydrodynamic simulations of radiatively inefficient spherical accretion onto a black hole. The simulations are initialized with a Bondi flow and with a weak, dynamically unimportant, large-scale magnetic field. As the gas flows in, the magnetic field is amplified. When the magnetic pressure approaches equipartition with the gas pressure, the field begins to reconnect and the gas is heated up. The heated gas is buoyant and moves outward, causing line stretching of the frozen-in magnetic field. This leads to further reconnection and more heating and buoyancy-induced motions, so that the flow makes a transition to a state of self-sustained convection. The radial structure of the flow changes dramatically from its initial Bondi profile, and the mass accretion rate onto the black hole decreases significantly. Motivated by the numerical results, we develop a simplified analytical model of a radiatively inefficient spherical flow in which convective transport of energy to large radii plays an important role. In this "convection-dominated Bondi flow," the accretion velocity is highly subsonic, and the density varies with radius as rho proportional to R-1/2 rather than the standard Bondi scaling rho proportional to R-3/2. We estimate that the mass accretion rate onto the black hole correspondingly scales as (M) over dot similar to (R-in/R-a)(M) over dot(Bondi), where R-in is a small multiple of the Schwarzschild radius of the black hole and R-a is the "accretion radius" at which the ambient gas in the surrounding medium is gravitationally captured by the black hole. Since the factor R-in/R-a is typically very small, (M) over dot is significantly less than the Bondi accretion rate. Convection-dominated Bondi flows may be relevant for understanding many astrophysical phenomena, e.g., post-supernova fallback and radiatively inefficient accretion onto supermassive black holes, stellar-mass black holes, and neutron stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Igumenshchev, IV (reprint author), Univ Rochester, Laser Energet Lab, 250 E River Rd, Rochester, NY 14623 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 65 TC 62 Z9 63 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2002 VL 566 IS 1 BP 137 EP 147 DI 10.1086/338077 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EB UT WOS:000173766700011 ER PT J AU Monnier, JD Greenhill, LJ Tuthill, PG Danchi, WC AF Monnier, JD Greenhill, LJ Tuthill, PG Danchi, WC TI Radio properties of pinwheel nebulae SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; circumstellar matter; radio continuum : stars; stars : winds, outflows; stars : Wolf-Rayet ID WOLF-RAYET STARS; MASS-LOSS; X-RAY; MULTIFREQUENCY VARIATIONS; PARTICLE-ACCELERATION; SYSTEM HD-193793; EMISSION; WINDS; OBJECTS; WR-147 AB A small number of dusty Wolf-Rayet stars have been resolved into pinwheel nebulae, defined by their "rotating" spiral dust shells observed in the infrared. This morphology is naturally explained by dust formation associated with colliding winds in a binary system. In order to confirm and further explore this hypothesis, we have observed the known pinwheel nebulae (WR 104 and WR 98a) as well as the suspected binary WR 112 at multiple radio wavelengths with the Very Large Array to search for nonthermal radio emission from colliding winds. The spectrum of each target is nearly flat between 5 and 22 GHz, consistent with the presence of nonthermal emission that is reduced at low frequencies by free-free absorption. This emission must lie outside the radio "photosphere," leading us to estimate a lower limit to the physical size of the nonthermal emitting region that is larger than expected from current theory. Based on a radio and infrared comparison to WR 104 and WR 98a, we conclude that WR 112 is a likely candidate pinwheel nebula, but its temporal variability indicates an eccentric binary orbit or a pinwheel viewed nearly edge-on. A sensitive radio survey of IR-bright WRs would stringently test the hypothesis that colliding winds lie at the heart of all dusty WR systems. We also discuss the effects of dust obscuration in the ultraviolet and how radio-determined mass-loss rates of pinwheel nebulae (and dusty WR stars in general) may be underestimated due to shadowing effects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Monnier, JD (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42,60 Garden St, Cambridge, MA 02138 USA. OI Monnier, John D/0000-0002-3380-3307 NR 43 TC 22 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 FEB 10 PY 2002 VL 566 IS 1 BP 399 EP 408 DI 10.1086/337961 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EB UT WOS:000173766700038 ER PT J AU Bromm, V Clarke, CJ AF Bromm, V Clarke, CJ TI The formation of the first globular clusters in dwarf galaxies before the epoch of reionization SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; early universe; galaxies : formation; globular clusters : general; hydrodynamics; stars : formation ID COLD DARK MATTER; STAR-CLUSTERS; ORIGIN; SYSTEMS AB We explore a mechanism for the formation of the first globular clusters, operating during the assembly of dwarf galaxies at high redshifts, z greater than or similar to 10. The substructure in the dark matter and the corresponding potential wells are responsible for setting the cluster scale of 10 5 M. The second mass scale in the formation problem, the stellar scale of similar to1 M., is determined in turn by the processes that cool the gas. We address the origin of the first, cluster mass scale by means of three-dimensional numerical simulations of the collapsing dark matter and gaseous components. We find that the gas falls into the deepest dark subhalos, resulting in a system of approximately five protoglobular clouds. The incipient globular clusters lose their individual dark halos in the process of violent relaxation, leading to the buildup of the general dark halo around the dwarf galaxy. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Bromm, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 29 TC 75 Z9 75 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2002 VL 566 IS 1 BP L1 EP L4 DI 10.1086/339440 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EG UT WOS:000173767200001 ER PT J AU Hartmann, L AF Hartmann, L TI On disk braking of T Tauri rotation SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars : formation; stars : pre-main-sequence ID ORION-NEBULA-CLUSTER; ACCRETION DISKS; MAGNETOSPHERIC ACCRETION; YOUNG STARS; SPIN-DOWN; EVOLUTION; PERIODS; FIELD; FLOWS; MODEL AB The rotation of T Tauri stars is thought to be slowed by coupling between the stellar magnetosphere and the circumstellar disk. Stassun and collaborators have recently questioned this picture, based on their observations of young stars in and near the Orion Nebula Cluster (ONC) that indicate little evidence for disk-mediated spin-down. However, stellar spin-down can occur no faster than the rate at which angular momentum is removed from the inner disk, either through viscous processes associated with accretion or by a wind. Observational estimates of these processes suggest that the timescales for angular momentum loss may be comparable to the ages of the ONC stars, so that disk braking may not be completely effective, at least among the lowest mass stars. Testing this hypothesis will require further measurements of mass accretion and mass-loss rates as well as determinations of rotational periods as a function of age. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 43 TC 40 Z9 40 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2002 VL 566 IS 1 BP L29 EP L32 DI 10.1086/339455 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EG UT WOS:000173767200008 ER PT J AU Burns, JR Meisner, AD Weitzman, SH Malabarba, LR AF Burns, JR Meisner, AD Weitzman, SH Malabarba, LR TI Sperm and spermatozeugma ultrastructure in the inseminating catfish, Trachelyopterus lucenai (Ostariophysi : Siluriformes : Auchenipteridae) SO COPEIA LA English DT Article ID LEPIDOGALAXIAS-SALAMANDROIDES; INTERNAL FERTILIZATION; FISHES TELEOSTEI; CHARACIDAE; MORPHOLOGY; SPERMATOGENESIS; HISTOLOGY; TESTIS; PISCES AB This study presents details of the ultrastructure of the spermatozeugmata and spermatozoa of the South American catfish, Trachelyopterus lucenai, an inseminating species. Spermatozoa are tightly packaged into unencapsulated bundles, spermatozeugmata, with as many as 130 cells comprising a single packet. Within an individual spermatozeugma, cells are aligned side by side such that the anterior region of the bundle is comprised of nuclei, the middle region midpieces, and the posterior region flagella. Integrity of the packet appears to be maintained by specialized junctions between adjacent cells along their entire lengths. Each spermatozoon is characterized by an elongate nucleus containing condensed chromatin and a fossa at the posterior end. The elongate midpiece contains multiple mitochondria, abundant glycogen deposits, and accessory microtubules that run along the length of the midpiece. The ultrastructural modifications of the spermatozoa are discussed as possible adaptations associated with the reproductive mode of insemination. C1 George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. Amer Museum Nat Hist, Dept Ichthyol, New York, NY 10024 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Pontificia Univ Catolica Rio Grande Sul, Museu Ciencias & Tecnol, Porto Alegre, RS, Brazil. Univ Fed Rio Grande Sul, Dept Zool, Porto Alegre, RS, Brazil. RP Burns, JR (reprint author), George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RI Malabarba, Luiz/I-3225-2012 NR 37 TC 23 Z9 26 U1 0 U2 3 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 FEB 8 PY 2002 IS 1 BP 173 EP 179 PG 7 WC Zoology SC Zoology GA 520ZJ UT WOS:000173813400021 ER PT J AU Anderson, WD Baldwin, CC AF Anderson, WD Baldwin, CC TI Plectranthias lamillai Rojas and Pequeno, 1998: A junior synonym of Plectranthias exsul Heemstra and Anderson, 1983 SO COPEIA LA English DT Article ID EASTERN SOUTH-PACIFIC; SERRANIDAE; PISCES; ATLANTIC; ANTHIAS; GENUS AB Comparisons of the holotype of Plectranthias lamillai Rojas and Pequeno, 1998, collected off the Juan Fernandez Islands off the coast of Chile, with type and non-type material of another eastern South Pacific species, Plectranthias exsul Heemstra and Anderson, 1983, show that the differences between the two nominal taxa reported by Rojas and Pequeno are not great enough to warrant recognition of two distinct species. Accordingly, we consider P. lamillai to be a junior synonym of P. exsul. C1 Coll Charleston, Grice Marine Biol Lab, Charleston, SC 29412 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Anderson, WD (reprint author), Coll Charleston, Grice Marine Biol Lab, 205 Ft Johnson, Charleston, SC 29412 USA. EM andersonwd@cofc.edu; baldwin.carole@nmnh.si.edu NR 11 TC 3 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 FEB 8 PY 2002 IS 1 BP 233 EP 238 PG 6 WC Zoology SC Zoology GA 520ZJ UT WOS:000173813400032 ER PT J AU Krot, AN McKeegan, KD Leshin, LA MacPherson, GJ Scott, ERD AF Krot, AN McKeegan, KD Leshin, LA MacPherson, GJ Scott, ERD TI Existence of an O-16-rich gaseous reservoir in the solar nebula SO SCIENCE LA English DT Article ID REFRACTORY INCLUSION; ORDINARY CHONDRITES; CHONDRULE FORMATION; CONSTRAINTS; SYSTEM; AL-26; CONDENSATION; METEORITES; ALLENDE; MODELS AB Carbonaceous chondrite condensate olivine grains from two distinct petrographic settings, calcium-aluminum-rich inclusion (CAI) accretionary rims and amoeboid olivine aggregates (AOAs), are oxygen-16 (O-16) enriched at the level, previously observed inside CAIs. This requires that the gas in the nebular region where these grains condensed was O-16-rich. This contrasts with an O-16-poor gas present during the formation of chondrules, suggesting that CAIs and AOAs formed in a spatially restricted region of the solar nebula containing O-16-rich gas. The O-16-rich gas composition may have resulted either from mass-independent isotopic chemistry or from evaporation of regions with enhanced dust/gas ratios, possibly in an X-wind environment near the young Sun. C1 Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Smithsonian Inst, US Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Krot, AN (reprint author), Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011 OI McKeegan, Kevin/0000-0002-1827-729X; NR 33 TC 75 Z9 76 U1 1 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 8 PY 2002 VL 295 IS 5557 BP 1051 EP 1054 DI 10.1126/science.1068200 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 520QR UT WOS:000173793000060 PM 11834830 ER PT J AU Rubenstein, DR Chamberlain, CP Holmes, RT Ayres, MP Waldbauer, JR Graves, GR Tuross, NC AF Rubenstein, DR Chamberlain, CP Holmes, RT Ayres, MP Waldbauer, JR Graves, GR Tuross, NC TI Linking breeding and wintering ranges of a migratory songbird using stable isotopes SO SCIENCE LA English DT Article ID CARBON; TRENDS; BEHAVIOR; FEATHERS; GROUNDS; PLANTS; RATIOS; BIRDS AB We used the natural abundance of stable isotopes (carbon and hydrogen) in the feathers of a neotropical migrant songbird to determine where birds from particular breeding areas spend the winter and the extent to which breeding populations mix in winter quarters. We show that most birds wintering on western Caribbean islands come from the northern portion of the species' North American breeding range, whereas those on more easterly islands are primarily from southern breeding areas. Although segregated by breeding latitude, birds within local wintering areas derive from a wide range of breeding longitudes, indicating considerable population mixing with respect to breeding Longitude. These results are useful for assessing the effects of wintering habitat Loss on breeding population abundances and for predicting whether the demographic consequences will be concentrated or diffuse. C1 Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. Dartmouth Coll, Dept Earth Sci, Hanover, NH 03755 USA. Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Rubenstein, DR (reprint author), Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. RI Rubenstein, Dustin/A-3451-2015 OI Rubenstein, Dustin/0000-0002-4999-3723 NR 25 TC 166 Z9 171 U1 4 U2 50 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 8 PY 2002 VL 295 IS 5557 BP 1062 EP 1065 DI 10.1126/science.1067124 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 520QR UT WOS:000173793000063 PM 11834833 ER PT J AU Paxinos, EE James, HF Olson, SL Sorenson, MD Jackson, J Fleischer, RC AF Paxinos, EE James, HF Olson, SL Sorenson, MD Jackson, J Fleischer, RC TI mtDNA from fossils reveals a radiation of Hawaiian geese recently derived from the Canada goose (Branta canadensis) SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID MITOCHONDRIAL-DNA EVOLUTION; PHYLOGENETIC ANALYSIS; ANCIENT DNA; SEQUENCE; WATERFOWL; ISLANDS; LIMITS; AGES AB Phylogenetic analysis of 1.35 kb of mtDNA sequence from fossils revealed a previously unknown radiation of Hawaiian geese, of which only one representative remains alive (the endangered Hawaiian goose or nene, Branta sandivicensis). This radiation is nested phylogenetically within a living species, the Canada goose (Branta canadensis) and is related most closely to the large-bodied lineage within that species. The barnacle goose (Branta leucopsis) is also nested within the Canada goose species and is related most closely to the small-bodied lineage of Canada geese. The peripheral isolation of the barnacle goose in the Palearctic apparently allowed the evolution of its distinctive plumage pattern, whereas the two Nearctic lineages of Canada geese share a primitive plumage pattern. The Hawaiian lineage of Canada geese diverged more dramatically, splitting into at least three species that differ in body size, body proportions, and flight ability. One fossil species, limited to the island of Hawaii, was related closely to the nene but was over four times larger, flightless, heavy-bodied and had a much more robust cranium. Application of a rate calibration to levels of DNA divergence suggests that this species evolved on the island of Hawaii in less than 500,000 years. This date is consistent with the potassium/argon-based age of the island of Hawaii of 430,000-500,000 years. The giant Hawaii goose resembles the moa-nalos, a group of massive, extinct, flightless ducks that lived on older Hawaiian Islands and thus is an example of convergent evolution of similar morphologies in island ecosystems. C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. ViroLog Inc, San Francisco, CA 94080 USA. Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. Boston Univ, Dept Biol, Boston, MA 02215 USA. Univ Oxford, Dept Zool & Biol Anthropol, Oxford OX2 6QS, England. RP Fleischer, RC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Sorenson, Michael/D-8065-2011; Jackson, Jennifer/E-7997-2013 OI Sorenson, Michael/0000-0001-5375-2917; NR 35 TC 68 Z9 78 U1 1 U2 16 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 5 PY 2002 VL 99 IS 3 BP 1399 EP 1404 DI 10.1073/pnas.032166399 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 519YF UT WOS:000173752500056 PM 11818543 ER PT J AU Zimmer, EA Roalson, EH Skog, LE Boggan, JK Idnurm, A AF Zimmer, EA Roalson, EH Skog, LE Boggan, JK Idnurm, A TI Phylogenetic relationships in the Gesnerioideae (Gesneriaceae) based on nrDNA ITS and cpDNA trnL-F and trnE-T spacer region sequences SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Gesneriaceae; Gesnerioideae; ITS; molecular phylogenetics; trnE-T; trnL-F ID INTERNAL TRANSCRIBED SPACER; MAXIMUM-LIKELIHOOD ANALYSES; NUCLEAR RIBOSOMAL DNA; SANANGO-RACEMOSUM; NDHF SEQUENCES; EPISCIEAE GESNERIACEAE; TRIBAL RELATIONSHIPS; CLADISTIC-ANALYSIS; CHLOROPLAST NDHF; PARSIMONY AB The Gesnerioideae includes most of the New World members of the Gesneriaceae family and is currently considered to include five tribes Beslerieae, Episcieae, Gesnerieae, Gloximeae, and Napeantheae This study presents maximum parsimony and maximum likelihood phylogenetic analyses of nuclear ribosomal DNA internal transcribed spacer regions (ITS), and the chloroplast DNA trnL intron, trnL-trnF intergenic spacer region, and trnE-trnT intergenic spacer region sequences The ITS and cpDNA data sets strongly support the monophyly of a Beslerieae/Napeantheae clade. an Episcieae clade, a Gesnerieae clade: a Gloximeae clade minus Sinningia, Sinningia relatives, and Gloxinia sarmentiana, and a Sinningia/Pahavana/Vanhouttea clade. This is the first study to provide strong statistical support for these tribes/clades These analyses suggest that Sinningia and relatives should be considered as a separate tribe Additionally, generic relationships are explored, including the apparent polyphyly of Gloxama Chromosome number changes are minimized on the proposed phylogeny, with the exception of the n = 11 taxa of the Gloximeae. Scaly rhizomes appear to have been derived once in the Gloximeae sensu stricto The number of derivations of the inferior ovary is unclear either there was one derivation with a reversal to a superior ovary in the Episcieae. or there were multiple independent derivations of the inferior ovary. C1 Smithsonian Inst, Lab Mol Systemat, Natl Museum Nat Hist, Washington, DC 20560 USA. Smithsonian Inst, Dept Systemat Biol Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Zimmer, EA (reprint author), Smithsonian Inst, Lab Mol Systemat, Natl Museum Nat Hist, Washington, DC 20560 USA. RI Zimmer, Elizabeth/G-3890-2011; Idnurm, Alexander/K-8558-2013 OI Idnurm, Alexander/0000-0001-5995-7040 NR 61 TC 60 Z9 71 U1 0 U2 4 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 FEB PY 2002 VL 89 IS 2 BP 296 EP 311 DI 10.3732/ajb.89.2.296 PG 16 WC Plant Sciences SC Plant Sciences GA 595FQ UT WOS:000178098100014 PM 21669739 ER PT J AU Power, ML Oftedal, OT Tardif, SD AF Power, ML Oftedal, OT Tardif, SD TI Does the milk of callitrichid monkeys differ from that of larger anthropoids? SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article ID PRIMATES; CARE; JACCHUS; GROWTH AB The generalization that anthropoid primates produce dilute milks that are low in protein and energy is based primarily on data from large monkeys of the families Cebidae and Cercopithecidae, as well as humans. The marmosets and tamarins (Callitrichidae) are not only much smaller in body size, but also typically raise multiple offspring during a relatively brief lactation. We hypothesized that selection for small body size and high reproductive rate might favor secretion of milk of higher energy and protein concentrations. To test this hypothesis, 46 milk samples collected from 10 common marmosets (Callithrix jacchus, ca. 350 g) were assayed for dry matter (DM), crude protein (CP), fat, and sugar; and gross energy (GE) was calculated from these constituents. We also assayed five samples collected from three golden lion tamarins (Leontopithecus rosalia, ca. 700 g) and six samples collected from a single pygmy marmoset (Cebuella pygmaea, ca. 150 g) over two lactation periods. All samples were collected between days 10 and 57 post partum, representing mid lactation for these species. The milks of these three species were similar, containing 14.0%, 16.1%, and 13.7% DM; 2.7%, 2.6%, and 2.9% CP; 3.6%, 5.2%, and 3.7% fat; 7.4%, 7.2%, and 7.8% sugar; and 0.76, 0.90, and 0.82 kcal/g for common marmosets, golden lion tamarins, and the pygmy marmoset, respectively. These species produced milks with energy values that were within the range reported for large anthropoids, albeit with slightly higher protein concentration. However, milk composition did vary substantially among individual common marmoset females, especially in the proportion of milk energy derived from fat. In contrast, CP as expressed as a percent of GE was remarkably constant among common marmoset females. Callitrichid milk appeared to be similar to that of larger anthropoid primates in GE, but was higher in CP and in the proportion of GE from CP However, the small sample sizes for the golden lion tamarin and the pygmy marmoset, and the wide variation in milk composition found among common marmoset females cautions against definitively characterizing the milks of callitrichids from these data. (C) 2002 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Nutr Lab, Dept Conservat Biol, Washington, DC 20008 USA. SW Reg Primate Res Ctr, San Antonio, TX USA. RP Power, ML (reprint author), Smithsonian Inst, Natl Zool Pk, Nutr Lab, Dept Conservat Biol, Washington, DC 20008 USA. FU NCRR NIH HHS [RR 02022] NR 43 TC 38 Z9 38 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 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD FEB PY 2002 VL 56 IS 2 BP 117 EP 127 DI 10.1002/ajp.1068 PG 11 WC Zoology SC Zoology GA 514RE UT WOS:000173454200004 PM 11793418 ER PT J AU Borda-de-Agua, L Hubbell, SP McAllister, M AF Borda-de-Agua, L Hubbell, SP McAllister, M TI Species-area curves, diversity indices, and species abundance distributions: A multifractal analysis SO AMERICAN NATURALIST LA English DT Article DE species-area relationship; species diversity indices; species abundance distribution; multifractals; method of moments; method of histograms ID SELF-SIMILARITY; CRITICAL-STATE; RAIN-FORESTS; PATTERNS; EXTRAPOLATION; BIODIVERSITY; RICHNESS; DYNAMICS; RANGE AB Although fractals have been applied in ecology for some time, multifractals have, in contrast, received little attention. In this article, we apply multifractals to the species-area relationship and species abundance distributions. We highlight two results: first, species abundance distributions collected at different spatial scales may collapse into a single curve after appropriate renormalization, and second, the power-law form of the species-area relationship and the Shannon, Simpson, and Berger-Parker diversity indices belong to a family of equations relating the species number, species abundance, and area through the moments of the species abundance-probability density function. Explicit formulas for these diversity indices, as a function of area, are derived. Methods to obtain the multifractal spectra from a data set are discussed, and an example is shown with data on tree and shrub species collected in a 50-ha plot on Barro Colorado Island, Panama. Finally, we discuss the implications of the multifractal formalism to the relationship between species range and abundance and the relation between the shape of the species abundance distribution and area. C1 Columbia Univ, Ctr Environm Res & Conservat, New York, NY 10027 USA. Univ Georgia, Dept Bot, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ London Imperial Coll Sci Technol & Med, Royal Sch Mines, Dept Environm Sci & Technol, London SW7 2BP, England. RP Borda-de-Agua, L (reprint author), Columbia Univ, Ctr Environm Res & Conservat, New York, NY 10027 USA. RI Borda-de-Agua, Luis/D-6063-2011 OI Borda-de-Agua, Luis/0000-0002-0802-6235 NR 52 TC 52 Z9 56 U1 1 U2 27 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 FEB PY 2002 VL 159 IS 2 BP 138 EP 155 PG 18 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 522CZ UT WOS:000173879300003 PM 18707410 ER PT J AU Oosterloo, TA Morganti, R Sadler, EM Vergani, D Caldwell, N AF Oosterloo, TA Morganti, R Sadler, EM Vergani, D Caldwell, N TI Extended H I disks in dust lane elliptical galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 1947, NGC 3108, NGC 7049, NGC 7070A, ESO 263-G48); galaxies : ISM; galaxies : kinematics and dynamics ID INTERSTELLAR MATTER; MOLECULAR GAS; IONIZED-GAS; CONTINUUM SUBTRACTION; DARK-MATTER; CENTAURUS-A; RADIO; KINEMATICS; NGC-1052; PHOTOIONIZATION AB We present the results of H I observations of five dust lane elliptical galaxies with the Australia Telescope Compact Array. Two galaxies (NGC 3108 and NGC 1947) are detected, and sensitive upper limits are obtained for the other three. In the two detected galaxies, the H I is distributed in a regular, extended, and warped disklike structure of low surface brightness. Adding data from the literature, we find that several more dust lane elliptical galaxies have regular H I structures. This H I is likely to be a remnant of accretions and/or mergers that took place a considerable time ago and in which a significant fraction of the gas survived to form a disk. The presence of regular H I structures suggests that some mergers lead to galaxies with extended low surface brightness density gas disks. These gas disks will evolve very slowly, and these elliptical galaxies will remain gas-rich for a long period of time. One of the galaxies we observed ( NGC 3108) has a very large amount of neutral hydrogen (M-H I = 4.5x10(9) M-circle dot; M-H I/L-B similar to 0.09), which is very regularly distributed in an annulus extending to a radius of similar to6 R-eff. The kinematics of the H I distribution suggest that the rotation curve of NGC 3108 is at out to at least the last observed point. We estimate a mass-to-light ratio of M/L-B similar to 18 M-circle dot/L-B,(circle dot) at a radius of similar to6 R-eff from the center. Several of the galaxies we observed have an unusually low gas-to-dust ratio M-H I/M-dust, suggesting that their cold interstellar medium, if present as expected from the presence of dust, may be mainly in molecular rather than atomic form. C1 ASTRON, NL-7990 AA Dwingeloo, Netherlands. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Univ Bologna, Dipartimento Astron, I-40126 Bologna, Italy. Smithsonian Astrophys Observ, Tucson, AZ 85719 USA. Steward Observ, Tucson, AZ 85719 USA. RP Oosterloo, TA (reprint author), ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. OI Sadler, Elaine/0000-0002-1136-2555; Vergani, Daniela/0000-0003-0898-2216 NR 63 TC 58 Z9 58 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2002 VL 123 IS 2 BP 729 EP 744 DI 10.1086/338312 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WK UT WOS:000174210800011 ER PT J AU Bersier, D Wood, PR AF Bersier, D Wood, PR TI Variable stars in the Fornax dwarf galaxy SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; galaxies : individual (Fornax); RR Lyrae variable; stars : variables : general ID RR LYRAE STARS; BLUE FUNDAMENTAL EDGE; SPHEROIDAL GALAXY; METALLICITY; PHOTOMETRY; CLUSTERS; CALIBRATION; MAGNITUDES; LUMINOSITY; DISTANCES AB We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have similar to30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]similar or equal to-1.6 dex. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Bersier, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 54 Z9 54 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2002 VL 123 IS 2 BP 840 EP 847 DI 10.1086/338315 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WK UT WOS:000174210800019 ER PT J AU Romaniello, M Panagia, N Scuderi, S Kirshner, RP AF Romaniello, M Panagia, N Scuderi, S Kirshner, RP TI Accurate stellar population studies from multiband photometric observations SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : individual (Large Magellanic Cloud); stars : fundamental parameters; supernovae : individual (SN 1987A) ID LARGE-MAGELLANIC-CLOUD; MODEL ATMOSPHERES; DUST; SN-1987A; STARS; EXTINCTION; CLUSTERS; DISTANCE; COLORS AB We present a new technique based on multiband near-ultraviolet and optical photometry to measure both the stellar intrinsic properties, i.e., luminosity and effective temperature, and the interstellar dust extinction along the line of sight to hundreds of stars per square arcminute. The yield is twofold. On the one hand, the resulting reddening map has a very high spatial resolution, of the order of a few arcseconds, and can be quite effectively used in regions where the interstellar material is patchy, thus producing considerable differential extinction on small angular scales. On the other hand, combining the photometric information over a wide baseline in wavelength provides an accurate determination of temperature and luminosity for thousands of stars. As a test case, we present the results for the region around SN 1987A in the Large Magellanic Cloud imaged with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope. C1 European So Observ, D-85748 Garching, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Osserv Astrofis Catania, I-95125 Catania, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romaniello, M (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. OI Scuderi, Salvatore/0000-0002-8637-2109 NR 33 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 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2002 VL 123 IS 2 BP 915 EP 940 DI 10.1086/338430 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WK UT WOS:000174210800025 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 WW Camelopardalis SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : evolution; stars : fundamental parameters; stars : individual (WW Camelopardalis) ID LIMB-DARKENING COEFFICIENTS; LIGHT CURVES; STELLAR MODELS; SYNCHRONIZATION; DIMENSIONS; PHOTOMETRY; ABUNDANCE; SYSTEMS; MASSES AB We present absolute photometric observations in uvbybeta and 5759 differential observations in the V filter (the most complete light curve ever obtained) measured by a robotic telescope, as well as radial velocities from spectroscopic observations of the detached, eccentric, 2.3 day, double-lined, eclipsing binary star WW Camelopardalis. 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 1.920 +/- 0.013 M. and 1.911 +/- 0.016 R. for the primary, and 1.873 +/- 0.018 M. and 1.808 +/- 0.014 R. for the secondary. The effective temperatures and interstellar reddening of the stars are accurately determined from new uvbybeta photometry: 8350 135 K for the primary and 8240 +/- 135 K for the secondary, corresponding to a spectral type of A4m for both, and 0.294 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 in a slightly eccentric orbit (e = 0.0098). The components of WW Cam are main-sequence stars with an age of about 490 Myr 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. RP Lacy, CHS (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. NR 51 TC 26 Z9 27 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 FEB PY 2002 VL 123 IS 2 BP 1013 EP 1022 DI 10.1086/338691 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527WK UT WOS:000174210800032 ER PT J AU Pellegrini, S Fabbiano, G Fiore, F Trinchieri, G Antonelli, A AF Pellegrini, S Fabbiano, G Fiore, F Trinchieri, G Antonelli, A TI Nuclear and global x-ray properties of LINER galaxies: Chandra and BeppoSAX results for Sombrero and NGC 4736 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : spiral; galaxies : individual : NGC 4594, NGC 4736; galaxies : active; galaxies : nuclei; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; NEARBY SPIRAL GALAXIES; ASTRONOMY SATELLITE; SEYFERT-GALAXIES; ALPHA EMISSION; STAR-FORMATION; IONIZED-GAS; ON-BOARD; NGC-4736; REGION AB We report on the 0.1-100 keV BeppoSAX observations of two nearby LINER galaxies, Sombrero and NGC4736. Chandra ACIS-S observations supplement this broad-beam spectral study with a high resolution look into the nuclear region, and show a dominating central point source in Sombrero and a complex X-ray binary dominated/starburst region in NGC4736. A compact non-thermal radio source, present in the nucleus of both galaxies, coincides with the central source in Sombrero, while in NGC 4736 its X-ray counterpart is a much fainter point source, not the brightest of the central region. On the basis of these and other results, we conclude that the LINER activity is linked to the presence of a low luminosity AGN in Sombrero and to a recent starburst in NGC4736, and that Chandra's spectroscopic capabilities coupled to high resolution imaging are essential to establish the origin of the nuclear activity. C1 Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Roma, I-00044 Monteporzio Catone, Italy. Osserv Astron Brera, I-20121 Milan, Italy. RP Pellegrini, S (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy. OI Trinchieri, Ginevra/0000-0002-0227-502X; Fiore, Fabrizio/0000-0002-4031-4157 NR 59 TC 20 Z9 20 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2002 VL 383 IS 1 BP 1 EP 13 DI 10.1051/0004-6361:20011482 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527JT UT WOS:000174183500004 ER PT J AU Mancuso, S Raymond, JC Kohl, J Ko, YK Uzzo, M Wu, R AF Mancuso, S Raymond, JC Kohl, J Ko, YK Uzzo, M Wu, R TI UVCS/SOHO observations of a CME-driven shock: Consequences on ion heating mechanisms behind a coronal shock SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : corona, UV radiation, radio radiation; shock waves; magnetohydrodynamics (MHD) ID KINETIC TEMPERATURE; COLLISIONLESS SHOCK; SOLAR CORONA; SPECTROMETER; RADIO; SOHO; ACCELERATION; INCREASE; WAVE AB We report the observation of a 1100 km s(-1) CME-driven shock with the UltraViolet Coronagraph Spectrometer (UVCS) telescope operating on board SOHO on March 3, 2000. The shock speed was derived from the type II radio burst drift rate and from UVCS observations that can yield the density profile just before the passage of the shock. A CME projected speed of 920 km s(-1) was deduced from the Large Angle Spectrometric Coronagraph (LASCO) white light images, indicating that the CME leading edge was lagging behind at about 20% of the shock speed. The spectral profiles of both the O VI and Lyalpha lines were Doppler dimmed and broadened at the passage of the shock by the emission from shocked material along the line of sight. The observed line broadening for both protons and oxygen ions was modeled by adopting a mechanism in which the heating is due to the nondeflection of the ions at the shock ramp in a quasi-perpendicular shock wave. This specific ion heating model was able to reproduce the observed spectroscopic properties of the shocked plasma. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mancuso, S (reprint author), Osserv Astron Torino, Strada Osservatorio 20, I-10025 Pino Torinese, Italy. NR 30 TC 71 Z9 72 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 FEB PY 2002 VL 383 IS 1 BP 267 EP 274 DI 10.1051/0004-6361:20011721 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527JT UT WOS:000174183500031 ER PT J AU Heithausen, A Bertoldi, F Bensch, F AF Heithausen, A Bertoldi, F Bensch, F TI Gravitationally bound cores in a molecular cirrus cloud SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; ISM : abundances; ISM : clouds; ISM : individual objects : MCLD 123.5+24.9; ISM : molecules; ISM : dust ID HIGH-LATITUDE CLOUD; STAR-FORMING REGIONS; GALACTIC CIRRUS; MCLD-123.5+24.9; EMISSION; DUST; CO AB Using MAMBO at the IRAM 30 m telescope we have observed a dense core in the cirrus cloud MCLD 123.5+24.9 in the dust continuum emission at 250 GHz. The core is detected as an elongated filament with an extent of 4.'2 x 0.'7, corresponding to 0.18 pc x 0.03 pc at an adopted distance of 150 pc. We find a close correlation between the continuum emission and previously observed (CO)-O-18 (1-->0) line emission. Using standard dust models we derive hydrogen column densities of up to 10(22) cm(-2). The total mass for the filament is about 0.66 M-circle dot. We also present observations of the HCN (3-->2), (4-->3), and (10-->9) emission lines obtained with the MPIfR 100 m and the IRAM 30 m telescopes. The distribution is very different from the dust continuum and the (CO)-O-18 (1-->0) line emission. HC3N is concentrated in two distinct clumps located at the ends of the filament seen in the other tracers. Based on a LVG analysis of the HC3N transitions we derive column densities of N(HC3N)/Deltav approximate to 10(13) cm(-2) /km s(-1) and volume densities of n(H-2) approximate to 10(5) cm(-3). We find that the HC3N clumps have masses of 0.13 and 0.19 M-circle dot. Our data demonstrate that the cirrus cloud cores are gravitationally bound, and that they show chemical structure indicating different evolutionary stages within the cloud. C1 Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heithausen, A (reprint author), Univ Bonn, Inst Radioastron, Hugel 71, D-53121 Bonn, Germany. NR 29 TC 22 Z9 22 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2002 VL 383 IS 2 BP 591 EP 597 DI 10.1051/0004-6361:20011806 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 527KC UT WOS:000174184400021 ER PT J AU El-Ad, H Martel, H Lecar, M Piran, T AF El-Ad, H Martel, H Lecar, M Piran, T TI The cluster mass function in COBE- and cluster-normalized cold dark matter simulations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : clusters : general; large-scale structure of universe; methods : numerical ID ANGULAR POWER SPECTRUM; CFA REDSHIFT SURVEY; COSMOLOGICAL MODELS; SCALE STRUCTURE; EVOLUTION; SUPERNOVAE; UNIVERSE; GALAXIES; OMEGA; VOIDS AB We introduce a set of four new publicly available N-body simulations, the most recent additions to the ever expanding Texas (PM)-M-3 Database. Our models probe the less studied parameter space region of moderate volume (100 h(-1) Mpc box) combined with fine mass resolution (proportional to10(12) M-circle dot, roughly comparable to an L-* galaxy; 140(3) particles with M-particle = 10(11)Omega(0) h(-1) M-circle dot), making these simulations especially suitable for study of major large-scale structure features, such as voids and walls, and for comparison with the largest three-dimensional redshift surveys currently available (CfA2, SSRS2, IRAS PSCz). We match the above quartet with a set of smaller (40 h(-1) Mpc), higher resolution simulations (M-particle = 10(10)Omega(0) h(-1) M-circle dot), to verify the reliability of the derived dark matter halo mass function at the small mass end. Our cosmological models (LCDM, TOCDM, OCDM, TCDM) are all COBE-normalized and, when possible (LCDM and TOCDM), also cluster-normalized, based on the X-ray cluster M-T relation. The COBE- and cluster-normalized LCDM model reiterates the attractiveness of this currently favored model, which does not require the introduction of tilt in order to snugly fit the ever narrowing constraints imposed by observational estimates of other cosmological parameters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP El-Ad, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 34 TC 1 Z9 1 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2002 VL 565 IS 2 BP 649 EP 654 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600001 ER PT J AU Greenhill, LJ Ellingsen, SP Norris, RP McGregor, PJ Gough, RG Sinclair, MW Rayner, DP Phillips, CJ Herrnstein, JR Moran, JM AF Greenhill, LJ Ellingsen, SP Norris, RP McGregor, PJ Gough, RG Sinclair, MW Rayner, DP Phillips, CJ Herrnstein, JR Moran, JM TI Search for H2O maser emission in southern active galactic nuclei and star-forming galaxies: Discovery of a maser in the edge-on galaxy IRAS F01063-8034 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (IRAS F01063-8034); galaxies : Seyfert; ISM : molecules; masers ID WATER-VAPOR MASER; LARGE MAGELLANIC CLOUD; POINT-SOURCE CATALOG; OPTICAL SPECTROSCOPY; RADIO; DISTANCE; NGC4258; GAS; OH; VELOCITIES AB We report the cumulative results of five surveys for H2O maser emission at 1.35 cm wavelength in 131 active galactic nuclei (AGNs) and star-forming galaxies, conducted at the Parkes Observatory between 1993 and 1998. We detected one new maser, in the edge-on galaxy IRAS F01063-8034, which exhibits a single similar to0.1 Jy spectral feature at 4282+/-6 km s(-1) (heliocentric) with an unusually large 54+/-16 km s(-1) half-power full width. The centroid velocity of the emission increased to 4319.6+/-0.6 km s(-1) (38+/-2 km s(-1) width) over the 13 days between discovery and confirmation of the detection. A similarly broad-line width and large change in velocity has been noted for the maser in NGC 1052, wherein jet activity excites the emission. Neither optical spectroscopy, radio-infrared correlations, nor infrared colors provide compelling evidence of unusual activity in the nucleus of IRAS F01063-8034. Since the galaxy appears to be outwardly normal at optical and infrared wavelengths, detection of an H2O maser therein is unique. The maser emission is evidence that the galaxy harbors an AGN that is probably obscured by the edge-on galactic disk. The detection highlights the possibility that undetected AGNs could be hidden in other relatively nearby galaxies. No other maser emission features have been identified at velocities between 3084 and 6181 km s(-1). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. Australian Natl Univ, Inst Adv Studies, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Rayner, David/A-6414-2011; Ellingsen, Simon/J-7754-2014; Norris, Ray/A-1316-2008 OI Rayner, David/0000-0003-0545-3634; Ellingsen, Simon/0000-0002-1363-5457; Norris, Ray/0000-0002-4597-1906 NR 62 TC 21 Z9 22 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2002 VL 565 IS 2 BP 836 EP 848 DI 10.1086/324383 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600015 ER PT J AU Furlanetto, SR Loeb, A AF Furlanetto, SR Loeb, A TI Constraining the collisional nature of the dark matter through observations of gravitational wakes SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies : clusters : general; hydrodynamics; X-rays : galaxies : clusters ID DYNAMICAL FRICTION; PLANETARY-NEBULAE; COMA CLUSTER; RADIAL-VELOCITIES; GASEOUS MEDIUM; GALAXIES; HALOS; MASS; ABELL-2142 AB We propose to use gravitational wakes as a direct observational probe of the collisional nature of the dark matter. We calculate analytically the structure of a wake generated by the motion of a galaxy in the core of an X-ray cluster for dark matter in the highly collisional and collisionless limits. Although the difference between these limits is most likely too subtle to be detected with weak lensing observations, we show that the two cases can be distinguished through detailed X-ray observations. We also discuss the sizes of subhalos in these limits. Preliminary X-ray data on the motion of NGC 1404 through the Fornax group disfavors fluidlike dark matter but does not exclude scenarios in which the dark matter is weakly collisional. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 65 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 FEB 1 PY 2002 VL 565 IS 2 BP 854 EP 866 DI 10.1086/324693 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600017 ER PT J AU Sun, M Murray, SS Markevitch, M Vikhlinin, A AF Sun, M Murray, SS Markevitch, M Vikhlinin, A TI Chandra observation of A2256: A cluster at the early stage of merging SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (A2256); X-rays : galaxies : clusters ID X-RAY; INTRACLUSTER MEDIUM; GALAXY CLUSTERS; RADIO-EMISSION; ABELL-2256; ASCA; MERGERS; TEMPERATURE; AWM-7; SUBSTRUCTURE AB We present Chandra observations of the rich cluster of galaxies A2256. In addition to the known cool subcluster, a new structure (we call it the "shoulder" in this paper, based on its morphology) was resolved 2' east of the peak of the main cluster. It is shown as a localized feature embedded in the main cluster. Its position is roughly at the center of a low-brightness radio relic. Spectral analysis shows that the shoulder has a high iron abundance, similar to1 (after the decomposition). The gas mass within it is around 2x10(11) M-circle dot. We suggest that this structure is either another merging component or an internal structure of the main cluster. The previously known subcluster has a low temperature (similar to4.5 keV) and high iron abundance (similar to0.6) in the central 150 kpc. The main cluster has a temperature of 7-8 keV and an iron abundance of 0.2-0.3 around the center. The Chandra image shows a relatively sharp brightness gradient at the south of the subcluster peak running south-southeast. A temperature jump was found across the edge, with lower temperature inside the subcluster. This phenomenon is qualitatively similar to the "cold fronts" found in A2142 and A3667. While a simple interpretation is not possible because of the projection, the edge indicates relative motion and contact of the two gas clouds. The Chandra temperature map shows only moderate temperature variations across the cluster, but not as strong as those expected in a major merger. If the shoulder is ignored, the temperature map resembles simulations at the early stage of merging while the subcluster approached the main cluster from somewhere west. The observed temperature map and the edgelike feature near the south of the subcluster imply that the ongoing merger is still at the early stage. The X-ray redshifts of several regions were measured. The results are consistent with a single value and all agree with the optical value. At least three member galaxies, including a radio head-tail galaxy, were found to have corresponding X-ray emission, with X-ray luminosity from several times 10(40) to 10(41) ergs s(-1). We find that the observed characteristics (temperature and iron abundance gradient) of the subcluster are similar to those of some poor clusters. The absence of galaxies around the peak of the subcluster is proposed to be the result of different falling velocities of the galaxies and the core gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Res Inst, Moscow, Russia. RP Sun, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 42 TC 73 Z9 73 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2002 VL 565 IS 2 BP 867 EP 876 DI 10.1086/324721 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600018 ER PT J AU Paolillo, M Fabbiano, G Peres, G Kim, DW AF Paolillo, M Fabbiano, G Peres, G Kim, DW TI Deep ROSAT HRI observations of the NGC 1399/NGC 1404 region: Morphology and structure of the X-ray halo SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (Fornax); galaxies : halos; galaxies : jets; radio continuum : galaxies; X-rays : galaxies; X-rays : individual (NGC 1399, NGC 1404) ID EARLY-TYPE GALAXIES; COUNTING DETECTOR IMAGES; ELLIPTIC GALAXIES; FORNAX CLUSTER; SURFACE PHOTOMETRY; RADIO LOBES; WAVELET TRANSFORMS; DOMINANT GALAXIES; PSPC OBSERVATIONS; POOR CLUSTERS AB We present the analysis of a deep (167 ks) ROSAT HRI observation of the cD galaxy NGC 1399 in the Fornax Cluster, comparing it with previous work on this galaxy and with recent Chandra data. We find, in agreement with previous observations, an extended and asymmetric gaseous halo with a luminosity (in the 0.1-2.4 keV energy band) L-X = (5.50+/-0.04) x 10(41) of ergs s(-1) within 46 kpc (assuming a distance of D=19 Mpc). Using both HRI and, at larger radii, archival PSPC data, we find that the radial behavior of the X-ray surface brightness profile is not consistent with a simple beta-model and suggests instead three distinct components. We use a multicomponent bidimensional model to study in detail these three components, which we identify respectively with the cooling flow region, the galactic halo, and the cluster halo. From these data we derive a binding mass distribution in agreement with that suggested by optical dynamical indicators, with an inner core dominated by luminous matter and an extended dark halo differently distributed on galactic and cluster scales. The HRI data and a preliminary analysis of Chandra public data allow us to detect significant density fluctuations in the halo. We discuss possible nonequilibrium scenarios to explain the hot halo structure, including tidal interactions with neighboring galaxies, ram stripping from the intracluster medium, and merging events. In the innermost region of NGC 1399, the comparison between the X-ray and radio emission suggests that the radio-emitting plasma is displacing and producing shocks in the hot X-ray-emitting gas. We do not detect the nuclear source in X-rays, and we pose an upper limit of similar to4x10(39) ergs s(-1) (0.1-2.4 keV) to its X-ray luminosity. We found that the NGC 1404 halo is well represented by a single symmetric b-model and follows the stellar light profile within the inner 8 kpc. The mass distribution is similar to the "central" component of the NGC 1399 halo. At larger radii, ram pressure stripping from the intracluster gas produces strong asymmetries in the galactic halo. Finally, we discuss the properties of the point-source population, finding evidence of correlation between the source excess and NGC 1399. C1 Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, I-90134 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, High Energy Div, Cambridge, MA 02138 USA. RP Paolillo, M (reprint author), Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, Piazza Parlamento 1, I-90134 Palermo, Italy. RI Paolillo, Maurizio/J-1733-2012; OI Paolillo, Maurizio/0000-0003-4210-7693; PERES, Giovanni/0000-0002-6033-8180 NR 75 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 FEB 1 PY 2002 VL 565 IS 2 BP 883 EP 907 DI 10.1086/337919 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600020 ER PT J AU Fabbiano, G Shapley, A AF Fabbiano, G Shapley, A TI A multivariate statistical analysis of spiral galaxy luminosities. II. Morphology-dependent multiwavelength emission properties SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : fundamental parameters; galaxies : spiral; galaxies : statistics; X-rays : galaxies ID X-RAY-PROPERTIES; FAR-INFRARED EMISSION; RADIO-CONTINUUM; STAR-FORMATION; ANTENNAE GALAXIES; S0 GALAXIES; NGC 4736; SAMPLE; NUCLEI; NEARBY AB This is the second of two papers based on a systematic multiwavelength (X, B, H, 12 mum, FIR, and 6 cm) statistical analysis of the Einstein Observatory Galaxy Catalog sample of 234 "normal" S0/a-Irr galaxies. This sample is representative of spiral galaxies, and its wide wavelength coverage provides a unique opportunity for a systematic exploration of the relations among different emission bands, which can give novel insight on the different emission processes and their relation to galaxian components, as a function of galaxy morphology. We find clear morphological differences in the overall relationships among different emission bands: while all wave bands tend to be well correlated in late-type Sc-Irr galaxies, in agreement with a general connection of all emission bands with the stellar component, in bulge-dominant early-type S0/a-Sab galaxies instead our results point to unrelated emission mechanisms for the two groups of wave bands: (12 mum, FIR, 6 cm) and (X, B, H). A dependence on galaxy morphology is also found in the 12 mum-FIR link, which was shown by the multivariate analysis of our first paper to be one the two strongest fundamental correlations in spiral galaxies, together with the well-known B-H correlation. We find that blue late-type dwarf galaxies appear to lack 12 mum emission, suggesting a lack of small-size dust grains in their interstellar medium (ISM), perhaps resulting from a particularly intense UV photon field. Also, the IR-B color-color plot of S0/a-Sab galaxies presents more scatter than those of later type galaxies, suggesting both significant red giant circumstellar dust emission and nuclear emission. Examining the well-known IR-radio-continuum link of spiral galaxies, we find surprising morphological differences : the "fundamental" radio-IR correlation flips from the mid-IR (12 mum) emission in S0/a-Sab galaxies to the FIR in Sc-Irr. These correlations also have different slopes : the 6 cm-12 mum correlation of S0/a-Sab galaxies is steep and follows the same trend as that of the bright active galactic nuclei (AGNs) in the sample, suggesting that low-luminosity AGNs embedded in these normal galaxies may be responsible for the bulk of their mid-IR and radio emission; the 6 cm-FIR correlation of Sc-Irr galaxies is linear, consistent with the well-known star formation link. The X-ray emission is not strongly correlated with any of the other variables, with the exception of the FIR in Sc-Irr, consistent with a general link with the young stellar population in these systems. Contrary to preliminary reports, we find that the X-ray-B correlation is similarly nonlinear (slope similar to 1.5) in early- and late-type spirals. We suggest that this apparent similarity stems from different processes in the two samples. In S0/a-Sab galaxies the steep slope may be due to the presence of some hot ISM in the more X-ray-luminous systems, as observed in E and S0 galaxies. In Sc-Irr galaxies instead it may be related to a luminosity dependence of intrinsically absorbed X-ray emission regions, connected with star formation activity. Obscured star-forming regions in higher luminosity galaxies can also explain other functional relations of the correlations found in the Sc-Irr sample. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 58 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2002 VL 565 IS 2 BP 908 EP 920 DI 10.1086/324780 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600021 ER PT J AU Beltran, MT Estalella, R Ho, PTP Calvet, N Anglada, G Sepulveda, I AF Beltran, MT Estalella, R Ho, PTP Calvet, N Anglada, G Sepulveda, I TI Multiwavelength study of the powering sources of the double H-2 bipolar jet in L1634 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; ISM : individual (L1634, HH 240/241); radio continuum : ISM; stars : formation ID YOUNG STELLAR OBJECTS; SUBMILLIMETER CONTINUUM IMAGES; AURIGA MOLECULAR CLOUD; HARO ENERGY-SOURCES; PROTOSTELLAR CORES; STAR-FORMATION; CIRCUMSTELLAR DISKS; COLD DUST; EVOLUTION; EMISSION AB We present observations of the centimeter, millimeter, and submillimeter continuum emission toward the core of L1634, a region with two embedded young stellar objects, IRAS 05173-0555 and IRS 7, which are powering two outflows. The submillimeter dust emission around IRAS 05173-0555 is resolved and shows two components, a centrally peaked source plus a considerably extended envelope, while the emission around IRS 7 appears unresolved with an angular resolution of similar to8". The dust emissivity index, derived from the submillimeter spectral index, is beta similar to 1.8 for both embedded sources, implying that the properties of the dust are similar around both objects. The submillimeter spectral index varies throughout the region, with lower values found toward the compact embedded sources, likely indicating grain growth on small scales. The high quality of the 850 and 450 mum continuum maps allows us to fit the radial intensity profiles of the extended emission around IRAS 05173-0555 with a power-law model that constrains the density distribution. The best fit to the data is a model with a multiple power-law density distribution, with slopes consistent with the predictions of the inside-out protostellar collapse model. We derive an infall rate of (2.6-8.0) x 10(-5) yr(-1) for the free-falling inner region of the envelope. The submillimeter luminosity, the total circumstellar mass derived, and the infall rate estimate are consistent with IRAS 05173-0555 being a Class 0 object. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. RP Beltran, MT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626 NR 53 TC 10 Z9 10 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2002 VL 565 IS 2 BP 1069 EP 1083 DI 10.1086/324683 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600036 ER PT J AU Abramowicz, MA Igumenshchev, IV Quataert, E Narayan, R AF Abramowicz, MA Igumenshchev, IV Quataert, E Narayan, R TI On the radial structure of radiatively inefficient accretion flows with convection SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; convection ID ADVECTION-DOMINATED ACCRETION; BLACK-HOLES; MODELS; OUTFLOWS; DISKS AB We consider the radial structure of radiatively inefficient hydrodynamic accretion flows around black holes. We show that low-viscosity flows consist of two zones: an outer convection-dominated zone and an inner advection-dominated zone. The transition between these two zones occurs at similar to50 Schwarzschild radii. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Abramowicz, MA (reprint author), Chalmers Univ Technol, Univ Gothenburg, Dept Astron & Astrophys, S-41296 Gothenburg, Sweden. OI Narayan, Ramesh/0000-0002-1919-2730 NR 31 TC 42 Z9 42 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2002 VL 565 IS 2 BP 1101 EP 1106 DI 10.1086/324717 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600039 ER PT J AU Winebarger, AR Emslie, AG Mariska, JT Warren, HP AF Winebarger, AR Emslie, AG Mariska, JT Warren, HP TI Energetics of explosive events observed with SUMER SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : transition region; Sun : UV radiation ID SOLAR TRANSITION ZONE; QUIET SUN; PHYSICAL PARAMETERS; ENERGY-DISTRIBUTION; MAGNETIC NETWORK; NANOFLARES; CORONA; ULTRAVIOLET; MICROFLARES; TELESCOPE AB Observations of solar chromosphere-corona transition region plasma show evidence of small-scale, short-lived dynamic phenomena characterized by significant nonthermal broadening and asymmetry in the wings of spectral line profiles. These impulsive mass motions (explosive events) are thought to be the product of magnetic reconnection and to be similar in driving mechanism (though larger in size) to nanoflares, the small-scale events proposed to heat the corona. In this paper, we present a statistical analysis of the energetics of explosive events to address the viability of the nanoflare heating theory. We consider high spectral, spatial, and temporal resolution spectra of the C III lambda977, N IV lambda765, O VI lambda1032, and Ne VIII lambda770 lines observed with the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) telescope and spectrometer. Each line profile exhibiting explosive event characteristics was analyzed using the velocity differential emission measure (VDEM) technique. A VDEM is a measure of the emitting power of the plasma as a function of its line-of-sight velocity and hence provides a method of accurately measuring the energy flux associated with an explosive event. We find that these events globally release similar to4 x 10(4) ergs cm(-2) s(-1) toward both the corona and chromosphere. This implies that explosive events themselves are not energetically significant to the solar atmosphere. However, the distribution of these explosive events as a function of their energy has a power-law spectral index of alpha = 2.9 +/- 0.1 for the energy range 10(22.7)-10(25.1) ergs. Since alpha is greater than 2, the energy content is dominated by the smallest events. Hence, if this distribution is representative of the size distribution down to lower energy ranges (similar to10(22) ergs), such small and (currently) undetectable events would release enough energy to heat the solar atmosphere. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. USN, EO Hulburt Ctr Space Res, Res Lab, Washington, DC 20375 USA. RP Winebarger, AR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. NR 33 TC 31 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 FEB 1 PY 2002 VL 565 IS 2 BP 1298 EP 1311 DI 10.1086/324714 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520DP UT WOS:000173765600056 ER PT J AU Elvis, M Risaliti, G Zamorani, G AF Elvis, M Risaliti, G Zamorani, G TI Most supermassive black holes must be rapidly rotating SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; X-rays : diffuse background ID ACTIVE GALACTIC NUCLEI; X-RAY; QUASARS; BEPPOSAX; EVOLUTION; LUMINOSITY; SPECTRUM; SAMPLE; ASCA AB We use the integrated spectrum of the X-ray background and quasars' spectral energy distribution to derive the contribution of quasars to the energy output of the universe. We find a lower limit for the energy from accretion onto black holes of 7% of the total luminosity of the universe and probably more, with 15% quite possible. Comparing these values with the masses of black holes in the center of nearby galaxies, we show that the accretion process must be, on average, very efficient: at least 15% of the accreted mass must be transformed into radiated energy. This further implies that most supermassive black holes are rotating rapidly. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astrofis Arcetri Firenze, I-50125 Florence, Italy. Osservatorio Astron Bologna, I-40127 Bologna, Italy. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Risaliti, Guido/0000-0002-3556-977X; Zamorani, Giovanni/0000-0002-2318-301X NR 31 TC 154 Z9 159 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2002 VL 565 IS 2 BP L75 EP L77 DI 10.1086/339197 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EA UT WOS:000173766600003 ER PT J AU Harwit, M Bergin, EA AF Harwit, M Bergin, EA TI 557 Ghz observations of water vapor outflow from VY Canis Majoris and W Hydrae SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; stars : individual (VY Canis Majoris, W Hydrae); stars : mass loss; stars : winds, outflows ID INFRARED-EMISSION; LINES; DUST AB We report the first detection of thermal water vapor emission in the 557 GHz, 1(10)-1(01) ground-state transition of ortho-H2O toward VY Canis Majoris. In observations obtained with the Submillimeter Wave Astronomy Satellite, we measured a flux of similar to450 Jy, in a spectrally resolved line centered on a velocity v(LSR) = 25 km s(-1) with an FWHM of similar to35 km s, somewhat dependent on the assumed line shape. We analyze the line shape in the context of three different radial outflow models for which we provide analytical expressions. We also detected a weaker 557 GHz emission line from W Hydrae. We find that these and other H2O emission-line strengths scale as suggested by Zubko and Elitzur. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Cornell Univ, Ithaca, NY 14853 USA. RP Harwit, M (reprint author), 511 H St SW, Washington, DC 20024 USA. NR 17 TC 13 Z9 13 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2002 VL 565 IS 2 BP L105 EP L108 DI 10.1086/339365 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EA UT WOS:000173766600010 ER PT J AU Johnson, O Drake, JJ Kashyap, V Brickhouse, NS Dupree, AK Freeman, P Young, PR Kriss, GA AF Johnson, O Drake, JJ Kashyap, V Brickhouse, NS Dupree, AK Freeman, P Young, PR Kriss, GA TI The Capella giants and coronal evolution across the Hertzsprung gap SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : coronae; stars : evolution; stars : individual (Capella); stars : late type; ultraviolet : stars ID X-RAY VARIABILITY; HE-I LAMBDA-10830; LATE-TYPE STARS; CHROMOSPHERIC ACTIVITY; COOL GIANT; LINE; MODULATION; EMISSION; SPECTRA; ORBIT AB We present an analysis of the coronal line Fe XXI lambda1354 observed in medium-resolution Hubble Space Telescope/Space Telescope Imaging Spectrograph echelle spectra of Capella obtained on 1999 September 12. These data were collected in support of a multiwavelength spectroscopic campaign designed to provide detailed temperature and density diagnostics over a wide range of temperatures, and they are accompanied by simultaneous Chandra, Extreme Ultraviolet Explorer, BeppoSAX, and Very Large Array observations. The line Fe XXI lambda1354 formed at 10(7) K is crucial to the interpretation of these data sets since it allows the deconvolution of the coronal flux of the two binary components. While earlier observations implied comparable coronal emission from both stars, our data indicate that nearly all the Fe XXI flux in the C I/Fe XXI blend at 1354 Angstrom arises from the rapidly rotating G1 III secondary. This suggests a significant decline in the hottest part of the corona of the G8 III primary over the past 5 years. For the first time, we can assign the variability of the high-temperature X-rays to the cooler He core burning star in the system. This result suggests that nascent coronae in the early Hertzsprung gap phase apparently do not vary and that cyclic activity and strong variability are seen only in later evolutionary stages when dynamos are more developed in deeper convective envelopes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Johnson, O (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. OI Brickhouse, Nancy/0000-0002-8704-4473 NR 36 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 FEB 1 PY 2002 VL 565 IS 2 BP L97 EP L100 DI 10.1086/339364 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EA UT WOS:000173766600008 ER PT J AU Gordon, VD McCarthy, MC Apponi, AJ Thaddeus, P AF Gordon, VD McCarthy, MC Apponi, AJ Thaddeus, P TI Rotational spectra of sulfur-carbon chains. II. HC5S, HC6S, HC7S, and HC8S, and H2C4S, H2C5S, H2C6S, and H2C7S SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : molecules; line : identification; molecular data; molecular processes; radio lines : ISM ID DENSE INTERSTELLAR CLOUDS; AB-INITIO; MILLIMETER-WAVE; MOLECULES; SPECTROSCOPY; CHEMISTRY; RADICALS; TMC-1 AB The linear carbon chain radicals HC5S, HC6S, HC7S, and HC8S and the asymmetric top chains H2C4S, H2C5S, H2C6S, and H2C7S have been detected in a supersonic molecular beam by Fourier transform microwave spectroscopy. Like the shorter HCnS chains, the electronic ground states of the four longer chains here alternate with even and odd number of carbon atoms: HC5S and HC7S have (2)Pi(1/2) ground states, while HC6S and HC8S have (2)Pi(3/2) ground states. Each of the four new thiocumulene chains possesses a rotational spectrum characteristic of a molecule with C-2v symmetry, in agreement with that observed for the two shorter chains H2C2S and H2C3S. The microwave spectra of all eight chains have been fully characterized, and spectroscopic constants, including fine and hyperfine structure constants where applicable, have been determined to high precision. The eight new chains are probably all highly polar and all are plausible candidates for astronomical detection. For the radical chains, the spectroscopic constants determined from the present work allow the astronomically most relevant lines to be calculated with an uncertainty of less than 1 km s(-1) up to 40 GHz; for the asymmetric top chains, the same transitions can be calculated with an uncertainty of less than 0.5 km s(-1) up to 55 GHz. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Gordon, VD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 27 TC 23 Z9 24 U1 2 U2 7 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 FEB PY 2002 VL 138 IS 2 BP 297 EP 303 DI 10.1086/324264 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 523NC UT WOS:000173959700005 ER PT J AU Stark, G Smith, PL Yoshino, K Esmond, JR Matsui, T Ito, K AF Stark, G Smith, PL Yoshino, K Esmond, JR Matsui, T Ito, K TI Line oscillator strength measurements in the d(7)-X(0) and e(4)-x(0) bands of CO SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM : molecules; methods : laboratory; molecular data; ultraviolet : general ID PICTORIS CIRCUMSTELLAR DISK; VUV SPECTROSCOPIC FACILITY; DIPOLE TRANSITION-MOMENT; X-PERSEI HD-24534; CARBON-MONOXIDE; CROSS-SECTIONS; INTERSYSTEM TRANSITIONS; RADIATIVE LIFETIMES; INTERSTELLAR CO; GROUND-STATE AB Laboratory measurements of line oscillator strengths in the "intersystem" bands of carbon monoxide currently provide an incomplete data set for the interpretation of astronomical observations in the vacuum ultraviolet region. We report line f-values in two intersystem bands, d(3)Delta(v = 7)-X E-1(+) (v = 0) at 146.4 nm and e(3)Sigma(-)(4)-X(0) at 147.1 nm, from photoabsorption spectra recorded with an instrumental resolution of 7.6 x 10(-4) nm (resolving power similar to190,000). The high-resolution measurements (1) minimize line saturation effects in the determination off-values and (2) allow for the direct experimental determination of the f-values of low-J lines that contribute to interstellar absorption features. We compare our measured line f-values with those generated from the intersystem band model of Rostas and coworkers. We find the predictions of relative line f-values within each band to be in agreement with the measurements, but there are discrepancies in the absolute scale. Based on this comparison, we present recommended f-values for low-J rotational lines within each band. C1 Wellesley Coll, Dept Phys, Wellesley, MA 02481 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tsukuba, Venture Business Lab, Tsukuba, Ibaraki 3058573, Japan. High Energy Accelerator Res Org, Inst Mat Struct Sci, Photon Factory, Tsukuba, Ibaraki 3050801, Japan. RP Stark, G (reprint author), Wellesley Coll, Dept Phys, 60 Garden St, Wellesley, MA 02481 USA. NR 31 TC 3 Z9 3 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 FEB PY 2002 VL 138 IS 2 BP 305 EP 313 DI 10.1086/324643 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 523NC UT WOS:000173959700006 ER PT J AU Sakai, S AF Sakai, S TI General flowering in lowland mixed dipterocarp forests of South-east Asia SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE Dipterocarpaceae; environmental prediction; masting; plant reproductive phenology; predator satiation; promotion of pollination; tropical forest ID MAST-FRUITING DIPTEROCARPACEAE; TROPICAL RAIN-FOREST; SEED PRODUCTION; REPRODUCTIVE SYNCHRONY; BEETLE POLLINATION; EL-NINO; PREDATOR SATIATION; ASEASONAL TROPICS; WIND POLLINATION; COSTA-RICA AB The general flowering (GF) events of forests in south-east Asia are perhaps the most spectacular phenomena in tropical biology. GF events occur at multiyear intervals. In GF, most dipterocarp species and many plants of other families come into flower and set fruit massively; these species and plants rarely flower except during GF events. GF is unique, because it can occur over thousands of kilometers and involve hundreds of plant species representing diverse families and lifeforms. It also involves strict mast fruiting. Satiation of generalist seed predators has been considered a primary force for GF. However, recent observations indicate that several selective agents rather than a single major factor may shape GF. In addition to the satiation of generalist predators, promotion of pollination could be one of the selective factors for GF, since synchronized flowering of many species causes an increase in pollinator activity through immigration and population growth. Although environmental prediction for better establishment of seedlings may also be involved in GF, no field data have been reported to support this idea. Longterm monitoring and further understanding of GF are essential for the conservation of this unique and diverse tropical forest in south-east Asia, especially in a period of global climatic change. (C) 2002 The Linnean Society of London. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Sakai, S (reprint author), Kyoto Univ, Grad Sch Human & Environm Studies, Kyoto 606850, Japan. NR 102 TC 98 Z9 106 U1 4 U2 41 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD FEB PY 2002 VL 75 IS 2 BP 233 EP 247 DI 10.1111/j.1095-8312.2002.tb01424.x PG 15 WC Evolutionary Biology SC Evolutionary Biology GA 527DZ UT WOS:000174172500007 ER PT J AU Huber, BT Norris, RD MacLeod, KG AF Huber, BT Norris, RD MacLeod, KG TI Deep-sea paleotemperature record of extreme warmth during the Cretaceous SO GEOLOGY LA English DT Article DE Cretaceous climate; greenhouse effect; oxygen isotopes; ocean circulation; polar regions ID MARINE TEMPERATURES; EVOLUTION; SURFACE; OCEANS AB Oxygen isotope analyses of well-preserved foraminifera from Blake Nose (30degreesN paleolatitude, North Atlantic) and globally distributed deep-sea sites provide a long-term paleotemperature record for the late Albian-Maastrichtian interval that is difficult to reconcile with the existence of significant Cretaceous ice sheets. Given reasonable assumptions about the isotopic composition of Cretaceous seawater, our results suggest that middle bathyal water temperatures at Blake Nose increased from similar to12 degreesC in the late Albian through middle Cenomanian to a maximum of 20 degreesC during the latest Cenomanian and earliest Turonian. Bottom waters were again similar to12 degreesC during the middle Campanian and cooled to a minimum of 9 T during the Maastrichtian. Correlative middle bathyal foraminifera from other ocean basins yield paleotemperature estimates that are very similar to those from Blake Nose. Comparison of global bottom-water temperatures and latitudinal thermal gradients suggests that global climate changed from a warm greenhouse state during the late Albian through late Cenomanian to a hot greenhouse phase during the latest Cenomanian through early Campanian, then to cool greenhouse conditions during the mid-Campanian through Maastrichtian. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Woods Hole Oceanog Inst, Dept Geol & Geophys, Woods Hole, MA 02543 USA. Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. RP Huber, BT (reprint author), Smithsonian Inst, Dept Paleobiol, NHB-121, Washington, DC 20560 USA. RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 NR 33 TC 345 Z9 374 U1 8 U2 66 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD FEB PY 2002 VL 30 IS 2 BP 123 EP 126 DI 10.1130/0091-7613(2002)030<0123:DSPROE>2.0.CO;2 PG 4 WC Geology SC Geology GA 521NF UT WOS:000173846400007 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI Wernher von Braun, the SS, and concentration camp labor: Questions of moral, political, and criminal responsibility SO GERMAN STUDIES REVIEW LA English DT Article C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 41 TC 8 Z9 8 U1 0 U2 2 PU ARIZ STATE UNIV PI TEMPE PA ARIZONA STATE UNIV, BOX 873204, TEMPE, AZ 85287-3204 USA SN 0149-7952 J9 GER STUD REV JI Ger. Stud. Rev. PD FEB PY 2002 VL 25 IS 1 BP 57 EP 78 DI 10.2307/1433245 PG 22 WC Area Studies; Humanities, Multidisciplinary SC Area Studies; Arts & Humanities - Other Topics GA 528LE UT WOS:000174244600004 ER PT J AU Dudley, R AF Dudley, R TI Mechanisms and implications of animal flight maneuverability SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2001 CL CHICAGO, IL SP Soc Integrat & Comparat Biol ID HOVERING INSECT FLIGHT; SEXUAL SELECTION; MUSCA-DOMESTICA; TAIL STREAMER; BARN SWALLOW; LEADING-EDGE; FLYING FROGS; WING BEAT; PERFORMANCE; AERODYNAMICS AB Accelerations and directional changes of flying animals derive from interactions between aerodynamic force production and the inertial resistance of the body to translation and rotation. Anatomical and allometric features of body design thus mediate the rapidity of aerial maneuvers. Both translational and rotational responsiveness of the body to applied force decrease with increased total mass. For flying vertebrates, contributions of the relatively heavy wings to whole-body rotational inertia are substantial, whereas the relatively light wings of many insect taxa suggest that rotational inertia is dominated by the contributions of body segments. In some circumstances, inertial features of wing design may be as significant as are their aerodynamic properties in influencing the rapidity of body rotations. Stability in flight requires force and moment balances that are usually attained via bilateral symmetry in wingbeat kinematics, whereas body roll and yaw derive from bilaterally asymmetric movements of both axial and appendicular structures. In many flying vertebrates, use of the tail facilitates the generation of aerodynamic torques and substantially enhances quickness of body rotation. Geometrical constraints on wingbeat kinematics may limit total force production and thus accelerational capacity in certain behavioral circumstances. Unitary limits to animal flight performance and maneuverability are unlikely, however, given varied and context-specific interactions among anatomical, biomechanical, and energetic features of design. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Dudley, R (reprint author), Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. EM r_dudley@utxvms.cc.utexas.edu NR 60 TC 54 Z9 58 U1 1 U2 16 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2002 VL 42 IS 1 BP 135 EP 140 DI 10.1093/icb/42.1.135 PG 6 WC Zoology SC Zoology GA 597TT UT WOS:000178237400015 PM 21708702 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, MC Thaddeus, P TI The rotational spectra of H2CCSi and H2C4Si SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID LINEAR SILICON CARBIDES; MICROWAVE-SPECTRUM; ASTRONOMICAL DETECTION; LABORATORY DETECTION; CARBON CHAINS; ISOTOPIC-SUBSTITUTION; SILACYCLOPROPENYLIDENE; SPECTROSCOPY; CONSTANTS; RADICALS AB The microwave rotational spectra of two singlet chains H2CCSi and H2C4Si, have been observed in a pulsed supersonic molecular beam by Fourier transform microwave spectroscopy. Following detection of the singly substituted rare isotopic species and D2CCSi, an experimental structure (r(0)) has been determined to high accuracy for H2CCSi by isotopic substitution. In addition, the rotational transitions of the Si-29 and the two C-13 isotopic species of H2CCSi exhibit nuclear spin-rotation hyperfine structure. The component of the spin-rotation tensor along the a-inertial axis is abnormally large for each of these isotopic species, especially for that with Si-29. where the magnitude of C-aa is in excess of 700 kHz. (C) 2002 Elsevier Science (USA). 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. OI McCarthy, Michael/0000-0001-9142-0008 NR 36 TC 11 Z9 11 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD FEB PY 2002 VL 211 IS 2 BP 228 EP 234 DI 10.1006/jmsp.2001.8467 PG 7 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 547WF UT WOS:000175355100007 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, MC Thaddeus, P TI Carbon-13 isotopic species of H2C3, H2C4, and H2C5: High-resolution rotational spectra SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID ASTRONOMICAL DETECTION; CUMULENE CARBENES; LINE SURVEY; H2CCCC; TMC-1 AB The microwave rotational spectra of the carbon-13 isotopic species of H2C3, H2C4, and H2C5 have been observed in a pulsed supersonic molecular beam by Fourier transform microwave spectroscopy. At high resolution all of the rotational lines exhibit hyperfine structure produced by the magnetic interaction between the nuclear spin of C-13 and the overall rotation of the molecule. The component of the nuclear spin-rotation tensor along the a-inertial axis is large for most isotopic species, especially at the carbene carbon; at this position C-aa is two to three times larger than at other substituted positions along the chain. In contrast to both H2C3 and H2C3, in H2C4 C-aa exhibits a pronounced alternation along the carbon chain backbone. Following detection of the five carbon-13 isotopic species and D2C5, an experimental structure (r(0)) has been determined to high accuracy for H2C5. (C) 2002 Elsevier Science (USA). 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. OI McCarthy, Michael/0000-0001-9142-0008 NR 23 TC 6 Z9 6 U1 1 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD FEB PY 2002 VL 211 IS 2 BP 235 EP 240 DI 10.1006/jmsp.2001.8468 PG 6 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 547WF UT WOS:000175355100008 ER PT J AU Hershler, R Liu, HP Landye, JJ AF Hershler, R Liu, HP Landye, JJ TI A new species of Eremopyrgus (Hydrobiidae : Cochliopinae) from the Chihuahuan Desert, Mexico: Phylogenetic relationships and biogeography SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID ANCESTRAL COLORADO RIVER; WESTERN UNITED-STATES; SOUTHERN CALIFORNIA; SNAILS GASTROPODA; GREAT-BASIN; RISSOOIDEA; GENUS AB A new species of hydrobiid gastropod, Eremopyrgus elegans, is described from northwestern Chihuahua state, Mexico. This new species inhabits a single spring more than 1000 kin south-southeast of waters occupied by its sole congener (E. eganensis), which lives in cast-central Nevada. Eremapygus elegans differs from its congener in its narrower shell, larger number of shell whorls, tilted shell apex, location of glandular lobe on the outer edge of the penis, presence of a terminal penial papilla, and 12 additional anatomical features. Although well differentiated, these two species share an unique type of glandular penial lobe and distinctive female genitalic organs, and their monophyly within the Cochliopinae is supported by a phylogenetic analysis based on a partial sequence of the mitochondrial COI gene. Our phylogenetic analysis depicts Eremopyrgus as sister to Zetekina, which is distributed along the Pacific Coast of southern Central America. We conjecture that the broadly disjunct distribution of Eremopyrgus. which cute. across the structural grain of western North America, may reflect the trace of a prior inland 'invasion' by coastal progenitors. C1 Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. US Fish & Wildlife Serv, New Mexico Fishery Res Off, Albuquerque, NM 87113 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 40 TC 5 Z9 6 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 J9 J MOLLUS STUD JI J. Molluscan Stud. PD FEB PY 2002 VL 68 BP 7 EP 15 DI 10.1093/mollus/68.1.7 PN 1 PG 9 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 535LJ UT WOS:000174645700002 ER PT J AU Harasewych, MG Kantor, YI AF Harasewych, MG Kantor, YI TI Buccinum thermophilum (Gastropoda : Neogastropoda : Buccinidae), a new species from the Endeavour vent field of the Juan de Fuca Ridge SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID HYDROTHERMAL VENTS; FAMILY AB Buccinum thermophilum new species, is described from abyssal depths of the Endeavour Vent Field, a portion of the Juan de Fuca Ridge in the northeastern Pacific. The new species is provisionally assigned to the subgenus Viridibuccinum Golikov and Sirenko, 1988, primarily on the basis of its conchological similarities with some of the species included in this subgenus, especially its type species B. (V) viridum Dail, 1890. The anatomy of this new species is similar in most respects to that of the few species of Buccininae for which the anatomy is known. Buccinum thermophilum most closely resembles B. viridum, B. rondinum Dail, 1919, and, to a much lesser extent, Buccinum diplodetum Dail, 1907, which has a similar geographic and bathymetric range. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Russian Acad Sci, AN Severtzov Inst Problems Evolut, Moscow 117071, Russia. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RI Kantor, Yuri/D-5259-2014 OI Kantor, Yuri/0000-0002-3209-4940 NR 14 TC 6 Z9 6 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 J9 J MOLLUS STUD JI J. Molluscan Stud. PD FEB PY 2002 VL 68 BP 39 EP 44 DI 10.1093/mollus/68.1.39 PN 1 PG 6 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 535LJ UT WOS:000174645700006 ER PT J AU Dondera, M Muller, HG Gavrila, M AF Dondera, M Muller, HG Gavrila, M TI Dynamic stabilization of ground-state hydrogen in superintense laser pulses of finite duration SO LASER PHYSICS LA English DT Article; Proceedings Paper CT 10th International Laser Physics Workshop CY JUL 03-07, 2001 CL MOSCOW, RUSSIA ID HIGH-FREQUENCY; ADIABATIC STABILIZATION; ATOMIC-HYDROGEN; HIGH-INTENSITY; FIELD; IONIZATION; SUPPRESSION; MODEL AB We present a comprehensive calculation of 3D dynamic stabilization (DS) of ground-state hydrogen in superintense laser pulses of finite duration, with cos 2 envelope. The ionization probability at the end of the pulse was calculated for a range of frequencies omega from 0.8 to 8 a.u., for peak fields ranging, up to 80 a.u. (depending on omega), and for pulse lengths tau extending from 1 to 400 cycles (depending on omega). We find prominent DS and substantial atomic survival under conditions where our nonrelativistic, dipole approximation calculation is expected to be valid. The connection of our results with other theories is analyzed. Thus, we find that the evolution of the atom is adiabatic and amenable to single-state Floquet theory, up to very large peak fields of several atomic units, and down to very short femtosecond pulses. In the general case, however, a unitary description of the ionization process, and DS in particular, requires "multistate Floquet theory." Our results favor the possibility of observing DS experimentally with the new VUV-FEL light sources that are now in test operation or construction, or with the attosecond pulses that have been obtained from hi h harmonic generation. C1 Univ Bucharest, Dept Phys, Bucharest 76900, Romania. FOM, Inst Atom & Mol Phys, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Dondera, M (reprint author), Univ Bucharest, Dept Phys, MG11, Bucharest 76900, Romania. NR 29 TC 2 Z9 2 U1 0 U2 2 PU INTERPERIODICA PI BIRMINGHAM PA PO BOX 1831, BIRMINGHAM, AL 35201-1831 USA SN 1054-660X J9 LASER PHYS JI Laser Phys. PD FEB PY 2002 VL 12 IS 2 BP 415 EP 423 PG 9 WC Optics; Physics, Applied SC Optics; Physics GA 527DG UT WOS:000174170400028 ER PT J AU Matocq, MD AF Matocq, MD TI Phylogeographical structure and regional history of the dusky-footed woodrat, Neotoma fuscipes SO MOLECULAR ECOLOGY LA English DT Article DE California; control region; cytochrome b; mitochondrial DNA; Neotoma; phylogeography ID MITOCHONDRIAL-DNA; NUCLEOTIDE SUBSTITUTIONS; POPULATION-GROWTH; UNITED-STATES; EVOLUTIONARY; CALIFORNIA; SEQUENCE; ENSATINA; POLYMORPHISM; SPECIATION AB The dusky-footed woodrat, Neotoma fuscipes, is a medium-sized rodent that inhabits low elevation woodland habitats along the Pacific coast of North America from Oregon, throughout California and into Baja California. Analyses of mitochondrial sequence variation throughout the distribution reveal substantial phylogeographical structure within N. fuscipes. The major mitochondrial lineages are largely concordant with previously identified morphological subdivisions within the taxon. The geographical distribution of distinct clades suggests that a combination of topographic barriers and the expansion and contraction of suitable habitat during the past 2 million years, especially along particular mountain ranges, have played a major role in the diversification of N. fuscipes. Furthermore, relatively low levels of genetic variation across the northern half of the distribution suggest that dusky-footed woodrats may have only recently expanded into this region. C1 Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. RP Matocq, MD (reprint author), Smithsonian Inst, Natl Zool Pk, Mol Genet Lab, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 60 TC 53 Z9 54 U1 1 U2 16 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD FEB PY 2002 VL 11 IS 2 BP 229 EP 242 DI 10.1046/j.0962-1083.2001.01430.x PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 519KV UT WOS:000173726200007 PM 11856424 ER PT J AU Rocha, LA Bass, AL Robertson, DR Bowen, BW AF Rocha, LA Bass, AL Robertson, DR Bowen, BW TI Adult habitat preferences, larval dispersal, and the comparative phylogeography of three Atlantic surgeonfishes (Teleostei : Acanthuridae) SO MOLECULAR ECOLOGY LA English DT Article DE Acanthurus; biogeography; Brazil; Caribbean; central Atlantic islands; dispersal; reef fishes ID CORAL-REEF FISHES; MITOCHONDRIAL-DNA; PATTERNS AB Although many reef fishes of the tropical Atlantic are widely distributed, there are large discontinuities that may strongly influence phylogeographical patterns. The freshwater outflow of the Amazon basin is recognized as a major barrier that produces a break between Brazilian and Caribbean faunas. The vast oceanic distances between Brazil and the mid-Atlantic ridge islands represent another formidable barrier. To assess the relative importance of these barriers, we compared a fragment of the mitochondrial DNA (mtDNA) cytochrome b gene among populations of three species of Atlantic surgeonfishes:Acanthurus bahianus, A. chirurgus and A. coeruleus. These species have similar life histories but different adult habitat preferences. The mtDNA data show no population structure between Brazil and the mid-Atlantic islands, indicating that this oceanic barrier is readily traversed by the pelagic larval stage of all three surgeonfishes, which spend similar to45-70 days in the pelagic environment. The Amazon is a strong barrier to dispersal of A. bahianus (d = 0.024, Phi(ST) = 0.724), a modest barrier for A. coeruleus (Phi(ST) = 0.356), and has no discernible effect as a barrier for A. chirurgus. The later species has been collected on soft bottoms with sponge habitats under the Amazon outflow, indicating that relaxed adult habitat requirements enable it to readily cross that barrier. A limited ability to use soft bottom habitats may also explain the low (but significant) population structure in A. coeruleus. In contrast, A. bahianus has not been collected over deep sponge bottoms, and rarely settles outside shallow reefs. Overall, adult habitat preferences seem to be the factor that differentiates phylogeographical patterns in these reef-associated species. C1 Univ Florida, Dept Fisheries & Aquat Sci, Gainesville, FL 32653 USA. Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Smithsonian Trop Res Inst Panama, Unit 0948, APO, AA 34002 USA. RP Univ Florida, Dept Fisheries & Aquat Sci, 7922 NW 71st St, Gainesville, FL 32653 USA. EM rocha@gnv.ifas.ufl.edu RI Rocha, Luiz/C-5107-2011 NR 45 TC 150 Z9 161 U1 3 U2 36 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 FEB PY 2002 VL 11 IS 2 BP 243 EP 252 DI 10.1046/j.0962-1083.2001.01431.x PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 519KV UT WOS:000173726200008 PM 11856425 ER PT J AU Labandeira, CC Phillips, TL AF Labandeira, CC Phillips, TL TI Stem borings and petiole galls from Pennsylvanian tree ferns of Illinois, USA: Implications for the origin of the borer and galler functional-feeding-groups and holometabolous insects SO PALAEONTOGRAPHICA ABTEILUNG A-PALAOZOOLOGIE-STRATIGRAPHIE LA English DT Review DE carboniferous; insects; Blattopteriformia; Holometabola; herbivores; pteridophytes ID CRYPTOCERCUS-PUNCTULATUS SCUDDER; PANESTHIA-CRIBRATA SAUSSURE; PLANT ANIMAL INTERACTIONS; UROPHORA-CARDUI DIPTERA; COAL-SWAMP VEGETATION; AQUILINUM L KUHN; PTERIDIUM-AQUILINUM; CELLULOSE DIGESTION; FOSSIL EVIDENCE; LIFE-HISTORY AB Latest Middle Pennsylvanian, lowland, equatorial communities of Euramerica occurred in equable, wetland habitats with peat substrates dominated by pole-like lycopod trees amid subdominant tree ferns and seed ferns, along with sphenopsids and rare cordaites. In these taxonomically diverse and physiognomically varied communities detritivores overwhelmingly channeled plant biomass from primary production to reduced organic matter. However, by the Late Pennsylvanian, when Psaronius tree ferns replaced lycopods as dominant floral elements, there was a dramatic increase in the spectrum and intensity of herbivore functional-feeding-groups. This shift toward the importance of herbivores is supported by a significant increase of arthropod coprolites in peat litter whose origin is most parsimoniously explained by herbivory. Equally important are the earliest documented occurrences of highly stereotyped and host specific plant damage caused by herbivorous insects. We describe two of these distinctive interactions as the newly established ichnogenera Pteridiscaphichnos, a detritivore-created, tunnel-and-gallery network in Middle- and Late Pennsylvanian Psaronius stems; and Pteriditorichnos, an elongate petiole gall from the frond of the Late Pennsylvanian Psaronius chasei, caused by an herbivorous and endophytic larval holometabolan. The Psaronius stem-boring, Pteridiscaphichnos, occurs in the late Middle Pennsylvanian form "layered cells morphotype" and the Late Pennsylvanian species Psaronius magnificus and R chasei. This distinctive stem boring is characterized by evacuated ground parenchyma replaced by frass of ellipsoidal coprolites 1.0 mm. X 3.0 min in average size and macerated fragments of processed but unconsurned parenchyma. All known specimens occur among linear to arcuate vascular strands interior to the outer sclerenchyma cylinder. The lack of reaction tissue indicates postmortem consumption of relatively soft, nutrient-rich parenchyma, although construction of the tunnel-and-gallery network preceded significant decomposition of the trunk since lignified tissues, such as sclerenchyma, vascular tissue and part of the root mantle, were still structurally sound and were avoided by the detritivores. Based on the geometry of the boring, coprolite structure, and the life-habits of modern ecologic analogs inhabiting tree fern trunks, the culprit of Pteridiscaphichnos is attributed to a roach or roach-like insect. The Late Pennsylvanian gall, Pteriditorichnos, is known only on Psaronius chasei hosts, and occurs in basal frond petioles. The structure of this gall consists of a lumen formed by removal of ground parenchyma through the petiolar axis, and its partial replacement by files of hypertrophied cells organized into radiating, impinging tufts that define a differentiated zone of callus. The lumen, encapsulated by callus, contains regions with frass consisting of coprolites and macerated parenchyma fragments. Barrel-shaped coprolites average 1.5 min X 2.5 mm in size, have smooth longitudinal surfaces but ragged ends, and contain recognizable cell types found in the surrounding callus and unmodified parenchyma. All fines of evidence indicate that an endophytic insect tunneled through medullary petiolar parenchyma, which induced plant response by production of callus, and was followed by insect consumption of the callus. Based on the three-dimensional structure of this gall, the particulate nature of the coprolites, and an extensive literature documenting known gall-making arthropods, we identify the culprit as a holometabolous larva. Although this earliest known gall resembles those made by extant tenthredinoid Hymenoptera, it is unassignable to any modern lineage of Holometabola. Although possible body fossils of the Holometabola have been mentioned in Pennsylvanian strata, Pteriditorichnos provides the first high-resolution, trace-fossil documentation of the life-habits of any Paleozoic larval holometabolan. Because of its exceptional anatomical preservation and Late Pennsylvanian age, this larval-induced gall is important in assessing existing hypotheses regarding the ancestral life-habits of the earliest larval Holometabola. Evidence indicates: 1. That the larval holometabolan galler occurred in a climatically equable, tropical, and humid swamp forest with a peat substrate. 2. That endophytic petiole galling is the earliest known life-habit for the Holometabola, and that stem galling or a related endophytic guild was an ancestral/behavior for this clade. 3. The prediction of LAMEERF, later elaborated by MALYSHFV, is vindicated: the endophytic penetration of tissues in primitive vascular plants (especially pteridophytes) was integrally associated with the holometabolous condition. These data indicate not only the occurrence of a stem borer and a herbivore galler during the Paleozoic, but also document the presence of an intimate interaction between a herbivore and its responding plant host as early as the Late Pennsylvanian. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Palaeontol, Washington, DC 20560 USA. Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Palaeontol, Washington, DC 20560 USA. NR 728 TC 41 Z9 43 U1 1 U2 7 PU E SCHWEIZERBARTSCHE VERLAGS PI STUTTGART PA NAEGELE U OBERMILLER, SCIENCE PUBLISHERS, JOHANNESSTRASSE 3A, D 70176 STUTTGART, GERMANY SN 0375-0442 J9 PALAEONTOGR ABT A JI Palaeontogr. Abt. A PD FEB PY 2002 VL 264 IS 1-4 BP 1 EP + PG 100 WC Paleontology SC Paleontology GA 673UZ UT WOS:000182599800001 ER PT J AU Vardi, A Shapiro, M Anglin, JR AF Vardi, A Shapiro, M Anglin, JR TI Comment on "quasicontinuum modeling of photoassociation" SO PHYSICAL REVIEW A LA English DT Letter AB We maintain that the reservations against the use of stimulated Raman adiabatic photoassociation in a nondegenerate gas, expressed by Mackie and Javanainen in a recent manuscript [Phys. Rev. A 60, 3174 (1999)], do not account for the coherence induced by the photoassociating laser. The authors treat the problem of two-color stimulated photoassociation using a set of decoupled three-mode problems, each containing a box eigenstate and the two bound states. We argue that such decomposition is not justified, since in the limit of a very large box all three-mode problems are, in fact, coherently coupled. The three-mode condition can only be met with a set of wave packets whose bandwidth matches the spectral width of the photoassociating pulse. Using this basis set, we show that by the authors' own formalism; stimulated Raman photoassociation is a viable process in the thermal ensemble. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. RP Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St,MS14, Cambridge, MA 02138 USA. RI Vardi, Amichay/D-8189-2011 OI Vardi, Amichay/0000-0002-8992-2129 NR 5 TC 15 Z9 15 U1 0 U2 1 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 FEB PY 2002 VL 65 IS 2 AR 027401 DI 10.1103/PhysRevA.65.027401 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 522DB UT WOS:000173879500130 ER PT J AU Ho, LC Sarzi, M Rix, HW Shields, JC Rudnick, G Filippenko, AV Barth, AJ AF Ho, LC Sarzi, M Rix, HW Shields, JC Rudnick, G Filippenko, AV Barth, AJ TI An efficient strategy to select targets for gasdynamical measurements of black hole masses using the Hubble Space Telescope SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID EARLY-TYPE GALAXIES; HOST GALAXIES; IONIZED-GAS; DISK; DUST; SPECTRA; IMAGES; MODELS; NUCLEI; WFPC2 AB Gasdynamical studies using the Hubble Space Telescope are an integral component for future progress in the search for massive black holes in galactic nuclei. Here we present an extensive set of gas rotation curves obtained with the Space Telescope Imaging Spectrograph for the central regions of 23 disk galaxies. We find that the bulges of randomly selected, nearby spiral and S0 galaxies generally do not contain well-defined gaseous disks. Only 15%-20% of disk galaxies have regular, symmetric velocity fields useful for dynamical analysis. Through comparison of the kinematics with Hubble Space Telescope images of the nuclear regions, we show that the probability of success can be significantly boosted by preselecting objects whose central dust lanes follow a well-ordered, circularly symmetric pattern. The dust morphology can be ascertained efficiently by visual inspection of unsharp-masked images. C1 Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Ho, LC (reprint author), Carnegie Inst Washington Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. OI Barth, Aaron/0000-0002-3026-0562 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 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD FEB PY 2002 VL 114 IS 792 BP 137 EP 143 DI 10.1086/338546 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 517EJ UT WOS:000173597900003 ER PT J AU Towe, KM AF Towe, KM TI Evolution of nitrogen fixation SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Tennille, GA 31089 USA. RP Towe, KM (reprint author), Smithsonian Inst, 230 W Adams St, Tennille, GA 31089 USA. NR 3 TC 7 Z9 8 U1 1 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 1 PY 2002 VL 295 IS 5556 BP 798 EP 799 DI 10.1126/science.295.5556.798 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 519NU UT WOS:000173733000020 PM 11824449 ER PT J AU Kress, WJ DePriest, PT AF Kress, WJ DePriest, PT TI Linnaeus visits the 21(st) century SO TAXON LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Nat Hist, United States Natl Herbarium, Bot Sect, Washington, DC 20560 USA. RP Kress, WJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, United States Natl Herbarium, Bot Sect, MRC 166, Washington, DC 20560 USA. RI DePriest, Paula/K-6633-2015 NR 2 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 FEB PY 2002 VL 51 IS 1 BP 5 EP 6 PG 2 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 550MT UT WOS:000175507400002 ER PT J AU Nicolson, DH AF Nicolson, DH TI Stone, plant, or animal SO TAXON LA English DT Article DE history; Linnaeus; nomenclature; scala naturae AB Linnaeus organised almost everything to which he put his mind and was the first to systematically apply a binomial system to all of nature. The philosophy underlying his system of nature is that of a ladder (pyramid) leading from stones, the lowest (furthest from Man), to animals, with Man, created in the image of God, being the highest, The classification functioned like a two-dimensional map, characters of taxa being like latitude and longitude with a hierarchy of precision. It was of value in an age of discovery, although his classifications of stones and plants had short lives. The binomial system of naming, although not considered important by Linnaeus, was important in separating diagnoses/descriptions of taxa from the names of taxa. It is hoped that new philosophies will maintain the distinction between things named and their names. C1 Natl Museum Nat Hist, Smithsonian Inst, United Stated Natl Herbarium, Bot Sect, Washington, DC 20560 USA. RP Nicolson, DH (reprint author), Natl Museum Nat Hist, Smithsonian Inst, United Stated Natl Herbarium, Bot Sect, Washington, DC 20560 USA. NR 8 TC 1 Z9 1 U1 1 U2 5 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 FEB PY 2002 VL 51 IS 1 BP 7 EP 10 DI 10.2307/1554958 PG 4 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 550MT UT WOS:000175507400003 ER PT J AU Krebs, E AF Krebs, E TI The compadrito. His fate, his neighborhoods, his music SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Book Review C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Krebs, E (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TIMES SUPPLEMENTS LIMITED PI MARKET HARBOROUGH PA TOWER HOUSE, SOVEREIGN PARK, MARKET HARBOROUGH LE87 4JJ, ENGLAND SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD FEB 1 PY 2002 IS 5157 BP 26 EP 26 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 518FE UT WOS:000173655300052 ER PT J AU Parker, GG Davis, MM Chapotin, SM AF Parker, GG Davis, MM Chapotin, SM TI Canopy light transmittance in Douglas-fir-western hemlock stands SO TREE PHYSIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Aging in Pacific Northwest Forests CY OCT 19, 2000 CL OREGON STATE UNIV, CORVALLIS, OREGON SP Western Regional Ctr, Nat Inst Global Environm Change HO OREGON STATE UNIV DE attenuation; canopy structure; LAI; old-growth; PAR; spatial variation ID LEAF-AREA INDEX; TROPICAL RAIN-FOREST; PHOTOSYNTHETICALLY ACTIVE RADIATION; SOLAR-RADIATION; HEMISPHERICAL PHOTOGRAPHS; EXTINCTION COEFFICIENTS; DECIDUOUS FORESTS; CONIFEROUS FOREST; PLANT CANOPIES; MOIST FOREST AB We measured vertical and horizontal variation in canopy transmittance of photosynthetically active radiation in five Pseudotsuga menziesii (Mirb.) Franco-Tsuga heterophylla (Raf.) Sarg. (Douglas-fir-western hemlock) stands in the central Cascades of southern Washington to determine how stand structure and age affect the forest light environment. The shape of the mean transmittance profile was related to stand height, but height of mean maximum transmittance was progressively lower than maximum tree height in older stands. The vertical rate of attenuation declined with stand age in both the overstory and understory. A classification of vertical light zones based on the mean and variance of transmittance showed a progressive widening of the bright (low variance and high mean) and transition (high variance and rapid vertical change) zones in older stands, whereas the dim zone (low variance and mean) narrowed. The zone of maximum canopy surface area in height profiles, estimated by inversion of transmittance profiles, changed from relatively high in the canopy in most young stands ("top-heavy") to lower in the canopy in older stands ("bottom-heavy"). In the understory, all stands had similar mean transmittances, but the spatial scale of variation increased with stand age and increasing crown size. The angular distribution of openness was similar in all stands, though the older stands were less open at all angles than the younger stands. Understory openness was generally unrelated to transmittance in the canopy above. Whole-canopy leaf area indices, estimated using three methods of inverting light measurements, showed little correspondence across methods. The observed patterns in light environment are consistent with structural changes occurring during stand development, particularly the diversification of crowns, the creation of openings of various sizes and the elaboration of the outer canopy surface. The ensemble of measurements has potential use in distinguishing forests of differing ages that have similar stature. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Whitman Coll, Walla Walla, WA 99362 USA. Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. RP Parker, GG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. OI Parker, Geoffrey/0000-0001-7055-6491 NR 55 TC 61 Z9 64 U1 1 U2 18 PU HERON PUBLISHING PI VICTORIA PA 202, 3994 SHELBOURNE ST, VICTORIA, BC V8N 3E2, CANADA SN 0829-318X J9 TREE PHYSIOL JI Tree Physiol. PD FEB PY 2002 VL 22 IS 2-3 BP 147 EP 157 PG 11 WC Forestry SC Forestry GA 522TN UT WOS:000173913200009 PM 11830411 ER PT J AU West-Eberhard, MJ AF West-Eberhard, MJ TI Development and selection in adaptive evolution SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter C1 Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. RP West-Eberhard, MJ (reprint author), Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. NR 8 TC 3 Z9 3 U1 2 U2 28 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD FEB PY 2002 VL 17 IS 2 BP 65 EP 65 DI 10.1016/S0169-5347(01)02413-2 PG 1 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 514VU UT WOS:000173462400009 ER PT J AU Webster, MS Marra, PP Haig, SM Bensch, S Holmes, RT AF Webster, MS Marra, PP Haig, SM Bensch, S Holmes, RT TI Links between worlds: unraveling migratory connectivity SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID FALCONS FALCO-PEREGRINUS; POPULATION-STRUCTURE; WESTERN-HEMISPHERE; SATELLITE TRACKING; CARBON ISOTOPES; SWAINSON HAWKS; BIRDS; WARBLERS; WILDLIFE; SEA AB Migration is the regular seasonal movement of animals from one place to another, often from a breeding site to a nonbreeding site and back. Because the act of migration makes it difficult to follow individuals and populations year round, our understanding of the ecology and evolution of migrating organisms, particularly binds, has been severely impeded. Exciting new advances in satellite telemetry, genetic analyses and stable isotope chemistry are now making it possible to determine the population and geographical origin of individual birds. Here, we review these new approaches and consider the relevance of understanding migratory connectivity to ecological, evolutionary and conservation issues. C1 Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. USGS Forest & Rangeland Ecosyst Sci Ctr, Corvallis, OR 97331 USA. Lund Univ, Dept Anim Ecol, S-22362 Lund, Sweden. Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. RP Webster, MS (reprint author), Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. NR 60 TC 557 Z9 596 U1 30 U2 236 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD FEB PY 2002 VL 17 IS 2 BP 76 EP 83 DI 10.1016/S0169-5347(01)02380-1 PG 8 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 514VU UT WOS:000173462400012 ER PT J AU McLaughlin, BM Daw, A Bell, KL AF McLaughlin, BM Daw, A Bell, KL TI Electron impact excitation of the 2s(2)2p3[S-4 degrees O]3s S-5 degrees(2)-2S(2) 2p(4) P-3(2,1,0) intercombination lines and of other observationally important extreme-ultraviolet lines in NeIII SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID STRUCTURE CROSS-SECTIONS; COLLISIONAL EXCITATION; REACTANCE MATRICES; ATOMIC DATA; TRANSITIONS; SPECTRUM; IONS AB Electron impact excitation collision strengths of doubly ionized atomic neon (Ne III) are calculated in the close-coupling approximation using the state-of-the-art R-matrix method. Twenty-eight 2s(2)2p(4), 2s2p(5), 2S(2)2p(3)3l (l = s, p, d), and 2s(2)2p(3)4s LS target terms, which comprise 56 fine-structure levels, are retained in the present calculations. The effective collision strengths for astrophysically important lines in the Ne in spectra are obtained by averaging the electron collision strengths, for a wide range of incident electron energies, over a Maxwellian distribution of velocities. Results are presented for electron temperatures (T-e in kelvins) in the range 3.0 less than or equal to log T-e less than or equal to 6.0, applicable to many laboratory and astrophysical plasmas. The present results provide information on several important astrophysically observed lines in the Ne III spectrum necessary in order to quantitatively analyse existing extreme-ultraviolet solar spectra. C1 Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McLaughlin, BM (reprint author), Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. RI daw, adrian/D-2297-2012 NR 21 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD JAN 28 PY 2002 VL 35 IS 2 BP 283 EP 292 DI 10.1088/0953-4075/35/2/307 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 520GM UT WOS:000173772700009 ER PT J AU Yang, XY Huan, C Candela, D Mair, RW Walsworth, RL AF Yang, XY Huan, C Candela, D Mair, RW Walsworth, RL TI Measurements of grain motion in a dense, three-dimensional granular fluid SO PHYSICAL REVIEW LETTERS LA English DT Article ID HYDRODYNAMIC EQUATIONS; DIFFUSION; FLOWS; GAS; FLUIDIZATION; SPHERES; SMOOTH; ENERGY; SYSTEM; BED AB We have used an NMR technique to measure the short-time, three-dimensional displacement of grains in a system of mustard seeds vibrated vertically at 15g. The technique averages over a time interval in which the grains move ballistically, giving a direct measurement of the granular temperature profile. The dense, lower portion of the sample is well described by a recent hydrodynamic theory for inelastic hard spheres. Near the free upper surface the mean free path is longer than the particle diameter and the hydrodynamic description fails. C1 Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yang, XY (reprint author), Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. RI Huan, Chao/F-4735-2014 OI Huan, Chao/0000-0002-0696-4412 NR 25 TC 62 Z9 62 U1 0 U2 12 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 JAN 28 PY 2002 VL 88 IS 4 AR 044301 DI 10.1103/PhysRevLett.88.044301 PG 4 WC Physics, Multidisciplinary SC Physics GA 522QB UT WOS:000173907500030 PM 11801123 ER PT J AU Duivenvoorden, JF Svenning, JC Wright, SJ AF Duivenvoorden, JF Svenning, JC Wright, SJ TI Ecology - Beta diversity in tropical forests SO SCIENCE LA English DT Editorial Material ID TREE C1 Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1090 GT Amsterdam, Netherlands. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Duivenvoorden, JF (reprint author), Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, POB 94766, NL-1090 GT Amsterdam, Netherlands. RI Svenning, Jens-Christian/C-8977-2012; Wright, Stuart/M-3311-2013 OI Svenning, Jens-Christian/0000-0002-3415-0862; Wright, Stuart/0000-0003-4260-5676 NR 15 TC 101 Z9 110 U1 5 U2 41 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 25 PY 2002 VL 295 IS 5555 BP 636 EP 637 DI 10.1126/science.295.5555.636 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 516PD UT WOS:000173560900029 PM 11809957 ER PT J AU Condit, R Pitman, N Leigh, EG Chave, J Terborgh, J Foster, RB Nunez, P Aguilar, S Valencia, R Villa, G Muller-Landau, HC Losos, E Hubbell, SP AF Condit, R Pitman, N Leigh, EG Chave, J Terborgh, J Foster, RB Nunez, P Aguilar, S Valencia, R Villa, G Muller-Landau, HC Losos, E Hubbell, SP TI Beta-diversity in tropical forest trees SO SCIENCE LA English DT Article ID PATTERNS; SIMILARITY; DISPERSAL; DECAY AB The high alpha-diversity of tropical forests has been amply documented, but beta-diversity-how species composition changes with distance has seldom been studied. We present quantitative estimates of beta-diversity for tropical trees by comparing species composition of plots in lowland terra firme forest in Panama, Ecuador, and Peru. We compare observations with predictions derived from a neutral model in which habitat is uniform and only dispersal and speciation influence species turnover. We find that beta-diversity is higher in Panama than in western Amazonia and that patterns in both areas are inconsistent with the neutral model. In Panama, habitat variation appears to increase species turnover relative to Amazonia, where unexpectedly tow turnover over great distances suggests that population densities of some species are bounded by as yet unidentified processes. At intermediate scales in both regions, observations can be matched by theory, suggesting that dispersal limitation, with speciation, influences species turnover. C1 Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. Duke Univ, Ctr Trop Conservat, Durham, NC 27708 USA. Univ Toulouse 2, CNRS, UMR 5552, Lab Ecol Terr, F-31029 Toulouse, France. Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. Univ Nacl San Antonio de Abad, Herbario Vargas, Cuzco, Peru. Pontificia Univ Catolica del Ecuador, Dept Biol Sci, Quito, Ecuador. Princeton Univ, Dept Ecol & Evolut Biol, Princeton, NJ 08544 USA. Smithsonian Inst, Ctr Trop Forest Sci, Washington, DC 20560 USA. Univ Georgia, Dept Bot, Athens, GA 30602 USA. RP Condit, R (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. RI Pitman, Nigel/A-7681-2008 OI Pitman, Nigel/0000-0002-9211-2880 NR 17 TC 699 Z9 754 U1 21 U2 262 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 25 PY 2002 VL 295 IS 5555 BP 666 EP 669 DI 10.1126/science.1066854 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 516PD UT WOS:000173560900041 PM 11809969 ER PT J AU Krems, RV Buchachenko, AA Szczesniak, MM Klos, J Chalasinski, G AF Krems, RV Buchachenko, AA Szczesniak, MM Klos, J Chalasinski, G TI Dynamics of O(P-3(j))+Rg collisions on ab initio and scattering potentials SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; RARE-GAS OXIDES; FINE-STRUCTURE TRANSITIONS; QUANTUM-MECHANICAL TREATMENT; LYING ELECTRONIC STATES; INTRAMULTIPLET TRANSITIONS; ATOMIC-COLLISIONS; CROSS-SECTIONS; HE AB Interaction potentials of the (3)Pi and (3)Sigma(-) electronic states of the Rg-O(P-3) systems (Rg=He-Kr) are computed at the coupled cluster single, double (triple) level of ab initio theory using extended basis sets augmented by bond functions. The ab initio potentials agree well with the scattering potentials determined from experiments in molecular beams [Aquilanti et al., J. Chem. Phys. 89, 6157 (1988)]. Both sets of the interaction potentials are employed for accurate close-coupling calculations of cross sections and rate constants for intramultiplet transitions in collisions of O(P-3(j)) with Rg atoms and analytical approximations for temperature dependencies of rate constants over temperature interval 50-3500 K are proposed. The sensitivity of the dynamical results to the nature of Rg atoms and interaction potentials is analyzed and the dynamics of intramultiplet mixing in O(P-3(j)) is investigated in both high- and low-energy limits. (C) 2002 American Institute of Physics. C1 Univ Gothenburg, Dept Chem, SE-41296 Gothenburg, Sweden. Moscow MV Lomonosov State Univ, Dept Chem, Moscow 119899, Russia. Oakland Univ, Dept Chem, Rochester, MI 48309 USA. Warsaw Univ, Fac Chem, PL-02093 Warsaw, Poland. CSIC, IMAFF, Madrid, Spain. RP Krems, RV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM chalbie@chem.uw.edu.pl RI Buchachenko, Alexei/C-8452-2012; Klos, Jacek/A-6457-2008 OI Buchachenko, Alexei/0000-0003-0701-5531; Klos, Jacek/0000-0002-7407-303X NR 48 TC 19 Z9 19 U1 1 U2 6 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JAN 22 PY 2002 VL 116 IS 4 BP 1457 EP 1467 DI 10.1063/1.1425409 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 513NG UT WOS:000173384200029 ER PT J AU Kong, AKH Charles, PA Kuulkers, E Kitamoto, S AF Kong, AKH Charles, PA Kuulkers, E Kitamoto, S TI Long-term X-ray variability and state transition of GX 339-4 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; binaries : close; stars : individual : GX 339-4; X-rays : stars ID BLACK-HOLE CANDIDATE; ASTRONOMY SATELLITE; TIMING EXPLORER; SOURCE GX-339-4; SKY MONITOR; SPACED DATA; CYGNUS X-1; ON-BOARD; LMC X-3; INSTABILITY AB With extensive monitoring data spanning over 30 years from Vela 5B, Ariel 5, Ginga, Compton Gamma Ray Observatory, Rossi X-ray Timing Explorer and BeppoSAX, we find evidence for long-term X-ray variability on time-scales similar to 190-240d from the black hole low-mass X-ray binary system GX339-4. Such variability resembles the outburst cycle of Z Cam-type dwarf novae, in which the standard disc instability model plays a crucial role. If such a model is applicable to GX 339-4, then the observed variability might be due to the irradiation of an unstable accretion disc. We show that within the framework of the X-ray irradiation model, when the accretion rate exceeds a critical value, GX 339-4 enters a 'flat-topped' high/soft state, such as seen in 1998, which we suggest corresponds to the 'standstill' state of Z Cam systems. C1 Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Space Res Org Netherlands, NL-3584 CA Utrecht, Netherlands. Univ Utrecht, Astron Inst, NL-3507 TA Utrecht, Netherlands. Rikkyo Univ, Dept Phys, Coll Sci, Toshima Ku, Tokyo 1718501, Japan. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 71 TC 17 Z9 17 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 JAN 21 PY 2002 VL 329 IS 3 BP 588 EP 596 DI 10.1046/j.1365-8711.2002.05022.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 518DV UT WOS:000173652100011 ER PT J AU Chartas, G Gupta, V Garmire, G Jones, C Falco, EE Shapiro, II Tavecchio, F AF Chartas, G Gupta, V Garmire, G Jones, C Falco, EE Shapiro, II Tavecchio, F TI Constraining H-o from Chandra observations of Q0957+561 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; distance scale; galaxies : clusters : individual (Q0957+561); gravitational lensing; X-rays : galaxies ID GRAVITATIONAL LENS SYSTEM; MASS-DISTRIBUTION; DARK-MATTER; CLUSTERS; GALAXIES; LENS-0957+561; PKS-0637-752; MODELS; JET AB We report the detection of the lens cluster of the gravitational lens (GL) system Q0957+561 from a deep observation with the Advanced CCD Imaging Spectrometer on board the Chandra X-Ray Observatory. Intracluster X-ray emission is found to be centered 4".3+/-1"3 east and 3".5(-0".6)(+1".2) north of image B, nearer than previous estimates. Its spectrum can be modeled well with a thermal plasma model consistent with the emission's originating from a cluster at a redshift of 0.36. Our best-fit estimates of the cluster temperature, T-e = 2.09(-0.54)(+0.83) keV (90% confidence), and of the mass distribution of the cluster are used to derive the convergence parameter kappa, the ratio of the cluster surface mass density to the critical density required for lensing. We estimate the convergence parameter at the location of the lensed images A and B to be kappa(A) = 0.22(-0.07)(+0.14) and kappa(B) = 0.21(-0.07)(+0.12) respectively (90% confidence levels). The observed cluster center, mass distribution, and convergence parameter kappa provide additional constraints to lens models of this system. Our new results break a mass-sheet degeneracy in GL models of this system and provide better constraints of similar to29% (90% confidence levels) on the Hubble constant. We also present results from the detection of the most distant X-ray jet (z=1.41) detected to date. The jet extends approximately 8" northeast of image A, and three knots are resolved along the X-ray jet, with flux densities decreasing with distance from the core. The observed radio and optical flux densities of the knots are fitted well with a synchrotron model, and the X-ray emission is modeled well with inverse Compton scattering of cosmic microwave background photons by synchrotron-emitting electrons in the jet. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. Osserv Astron Brera, I-20121 Milan, Italy. RP Chartas, G (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. NR 41 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 JAN 20 PY 2002 VL 565 IS 1 BP 96 EP 104 DI 10.1086/324485 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200008 ER PT J AU Colley, WN Schild, RE Abajas, C Alcalde, D Aslan, Z Barrena, R Dudinov, V Khamitov, I Kjernsmo, K Lee, HJ Lee, J Lee, MG Licandro, J Maoz, D Mediavilla, E Motta, V Munoz, J Oscoz, A Serra-Ricart, M Sinelnikov, I Stabell, R Teuber, J Zheleznyak, A AF Colley, WN Schild, RE Abajas, C Alcalde, D Aslan, Z Barrena, R Dudinov, V Khamitov, I Kjernsmo, K Lee, HJ Lee, J Lee, MG Licandro, J Maoz, D Mediavilla, E Motta, V Munoz, J Oscoz, A Serra-Ricart, M Sinelnikov, I Stabell, R Teuber, J Zheleznyak, A TI Around the clock observations of the Q0957+561A,B gravitationally lensed quasar SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (Q0957+561A,B) ID VARIABILITY; PHOTOMETRY AB An observing campaign with 10 participating observatories has undertaken to monitor the optical brightness of the Q0957 gravitationally lensed quasar for 10 consecutive nights in 2000 January. The resulting A image brightness curve has significant brightness fluctuations and makes a photometric prediction for the B image light curve for a second campaign planned for 2001 March 12-21. The ultimate purpose is to determine the gravitational lens time delay to a fraction of an hour and to seek evidence of rapid microlensing. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, E-38200 La Laguna, Tenerife, Spain. Akdeniz Univ, Dept Phys, TR-07058 Antalya, Turkey. Tubitak Natl Observ, TR-07058 Antalya, Turkey. Univ La Laguna, Dept Astrofiis, Tenerife 38200, Spain. Kharkov Natl Univ, Astron Observ, UA-61022 Kharkov, Ukraine. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Seoul Natl Univ, Astron Program, SEES, Seoul 151742, South Korea. DACOM Corp, Internet Technol Div, Seoul 135610, South Korea. Telescopio Nazl Galileo, Tenerife 38700, Spain. Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Columbia Univ, Dept Astron, New York, NY 10027 USA. Univ Republica, Fac Ciencias, Dept Astron, Montevideo 11400, Uruguay. Danish Lib Nat & Med Sci, Copenhagen, Denmark. RP Colley, WN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA 02138 USA. NR 9 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2002 VL 565 IS 1 BP 105 EP 107 DI 10.1086/338135 PN 1 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200009 ER PT J AU Harris, DE Krawczynski, H AF Harris, DE Krawczynski, H TI X-ray emission processes in radio jets SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; magnetic fields; radiation mechanisms : nonthermal ID CYGNUS-A; PKS-0637-752; RADIATION; NUCLEUS; GALAXY; M87 AB The emission processes responsible for the observed X-rays from radio jets are commonly believed to be nonthermal, but in any particular case, it is unclear if synchrotron emission or one or more varieties of inverse Compton emission predominates. We present a formulation of inverse Compton emission from a relativistically moving jet ("IC/beaming") that relies on radio-emitting synchrotron sources for which the energy densities in particles and fields are comparable. We include the nonisotropic nature of inverse Compton scattering of the relativistic electrons on photons of the cosmic microwave background (CMB) and provide beaming parameters for a number of jets. A list of X-ray-emitting jets is given and the jets are classified on the basis of their morphology and spectral energy distribution to determine their likely emission process. We conclude that these jets have significant bulk relativistic velocities on kiloparsec scales, that higher redshift sources require less beaming because the energy density of the CMB is significantly greater than locally, and that for some nearby sources synchrotron X-ray emission predominates because the jet makes a large angle to the line of sight. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Yale Univ, New Haven, CT 06520 USA. RP Harris, DE (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 35 TC 144 Z9 146 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2002 VL 565 IS 1 BP 244 EP 255 DI 10.1086/324544 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200022 ER PT J AU Caselli, P Walmsley, CM Zucconi, A Tafalla, M Dore, L Myers, PC AF Caselli, P Walmsley, CM Zucconi, A Tafalla, M Dore, L Myers, PC TI Molecular ions in L1544. I. Kinematics SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : clouds; ISM : individual (L1544); ISM : magnetic fields; ISM : molecules ID STARLESS CORE L1544; HYPERFINE-STRUCTURE; PRESTELLAR CORES; DENSE CORES; CLOUD; INFALL; PREPROTOSTELLAR; TRANSITION AB We have mapped the dense dark core L1544 in (HCO+)-C-13 (1-0), DCO+ (2-1), DCO+ (3-2), N2H+ (1-0), N2H+ (3-2), N2D+ (2-1), N2D+ (3-2), (CO)-O-18 (1-0), and (CO)-O-17 (1-0) using the IRAM 30 m tele-scope. We have obtained supplementary observations of (HCO+)-O-18 (1-0), (HCO+)-O-17 (1-0), and (DCO+)-C-13 (2-1). Many of the observed maps show a general correlation with the distribution of dust continuum emission, in contrast to (CO)-O-18 (1-0) and (CO)-O-17 (1-0), which give clear evidence for depletion of CO at positions close to the continuum peak. In particular, N2D+ (2-1) and (3-2) and to a lesser extent N2H+ (1-0) appear to be excellent tracers of the dust continuum. Our DCO+ maps have the same general morphology as the continuum while (HCO+)-C-13 (1-0) is more extended. We find also that many apparently optically thin spectral lines such as (HCO+)-O-18 and (DCO+)-C-13 have double or highly asymmetric profiles toward the dust continuum peak. We have studied the velocity field in the high-density nucleus of L1544, putting particular stress on tracers such as N2H+ and N2D+ which trace the dust emission and which we therefore believe trace the gas with density of order 10(5) cm(-3). We find that the tracers of high-density gas (in particular, N2D+) show a velocity gradient along the minor axis of the L1544 core and that there is evidence for larger line widths close to the dust emission peak. We interpret this using the model of the L1544 proposed by Ciolek and Basu and by comparing the observed velocities with those expected on the basis of their model. The results show reasonable agreement between observations and model in that the velocity gradient along the minor axis and the line broadening toward the center of L1544 are predicted by the model. This is evidence in favor of the idea that ambipolar diffusion across field lines is one of the basic processes leading to gravitational collapse. However, the double-peaked nature of the profiles is reproduced only at the core center and if a "hole" in the molecular emission, due to depletion, is present. Moreover, line widths are significantly narrower than observed and are better reproduced by the Myers & Zweibel model, which considers the quasi-static vertical contraction of a layer due to dissipation of its Alfvenic turbulence, indicating the importance of this process for cores on the verge of forming a star. C1 Osserv Astrofis Arcetri, I-50125 Florence, Italy. Observ Astron Nacl IGN, E-28800 Alcala De Henares, Spain. Univ Bologna, Dipartimento Chim G Ciamician, I-40126 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Osserv Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. EM caselli@arcetri.astro.it; walmsley@arcetri.astro.it; zucconi@arcetri.astro.it; tafalla@oan.es; dore@ciam.unibo.it; pmyers@cfa.harvard.edu OI DORE, LUCA/0000-0002-1009-7286 NR 33 TC 123 Z9 123 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2002 VL 565 IS 1 BP 331 EP 343 DI 10.1086/324301 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200029 ER PT J AU Caselli, P Walmsley, CM Zucconi, A Tafalla, M Dore, L Myers, PC AF Caselli, P Walmsley, CM Zucconi, A Tafalla, M Dore, L Myers, PC TI Molecular ions in L1544. II. The ionization degree SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : clouds; ISM : individual (L1544); ISM : molecules ID DENSE INTERSTELLAR CLOUDS; INTER-STELLAR CLOUDS; DEUTERIUM FRACTIONATION; ROTATIONAL-EXCITATION; DARK CLOUDS; STAR FORMATION; CORES; CHEMISTRY; H-2; GAS AB The maps presented in Paper I are here used to infer the variation of the column densities of HCO+, DCO+, N2H+, and N2D+ as a function of distance from the dust peak. These results are interpreted with the aid of a crude chemical model that predicts the abundances of these species as a function of radius in a spherically symmetric model with radial density distribution inferred from the observations of dust emission at millimeter wavelengths and dust absorption in the infrared. Our main observational finding is that the N(N2D+)/N(N2H+) column density ratio is of order 0.2 toward the L1544 dust peak as compared to N(DCO+)/N(HCO+) = 0.04. We conclude that this result, as well as the general finding that N2H+ and N2D+ correlate well with the dust, is caused by CO being depleted to a much higher degree than molecular nitrogen in the high-density core of L1544. Depletion also favors deuterium enhancement, and thus N2D+, which traces the dense and highly CO-depleted core nucleus, is much more enhanced than DCO+. Our models do not uniquely define the chemistry in the high-density depleted nucleus of L1544, but they do suggest that the ionization degree is a few times 10(-9) and that the ambipolar diffusion timescale is locally similar to the free-fall time. It seems likely that the lower limit, which one obtains to ionization degree by summing all observable molecular ions, is not a great underestimate of the true ionization degree. We predict that atomic oxygen is abundant in the dense core and, if so, H3O+ may be the main ion in the central highly depleted region of the core. C1 Osserv Astrofis Arcetri, I-50125 Florence, Italy. Observ Astron Nacl IGN, E-28800 Alcala De Henares, Spain. Univ Bologna, Dipartimento Chim G Ciamician, I-40126 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Caselli, P (reprint author), Osserv Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. OI DORE, LUCA/0000-0002-1009-7286 NR 74 TC 206 Z9 207 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2002 VL 565 IS 1 BP 344 EP 358 DI 10.1086/324302 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200030 ER PT J AU Slavin, JD Frisch, PC AF Slavin, JD Frisch, PC TI The ionization of nearby interstellar gas SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmic rays; ISM : abundances; ISM : clouds; solar system : general; ultraviolet : ISM; X-rays : diffuse background ID EXTREME-ULTRAVIOLET EXPLORER; LINE-OF-SIGHT; PICKUP ION OBSERVATIONS; EPSILON-CANIS-MAJORIS; GHRS OBSERVATIONS; ALPHA-CENTAURI; LYMAN-ALPHA; HELIOSPHERIC INTERFACE; RADIATION-FIELD; WHITE-DWARFS AB We present new calculations of the photoionization of interstellar matter within similar to5 pc of the Sun (which we refer to as the "complex of local interstellar clouds," or CLIC) by directly observed radiation sources, including nearby hot stars and the diffuse emission of the soft X-ray background (SXRB). In addition, we model the important, unobserved extreme-ultraviolet (EUV) emission both from the hot gas responsible for the SXRB and from a possible evaporative boundary between the CLIC and the hot gas. We carry out radiative transfer calculations and show that these radiation sources can provide the ionization and heating of the cloud required to match a variety of observations. The ionization predicted in our models shows good agreement with pickup ion results, interstellar absorption-line data toward epsilon CMa, and EUV opacity measurements of nearby white dwarf stars. Including the radiation from the conductive boundary improves agreement with data on the temperature and electron density in the cloud. The presence of dust in the cloud, or at least depleted abundances, is necessary to maintain the heating/cooling balance and reach the observed temperature. Using the column density observations as inputs, we derive the gas-phase abundances of C, N, O, Mg, Si, S, and Fe. Based on these inferred depletions, it appears that silicate and iron dust exists in the CLIC, while carbonaceous dust has been destroyed. In addition, we find evidence that the Ne abundance in the CLIC is larger than solar. C1 Eureka Sci Inc, Oakland, CA 94602 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Eureka Sci Inc, 2452 Delmer St,Suite 100, Oakland, CA 94602 USA. NR 101 TC 113 Z9 113 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2002 VL 565 IS 1 BP 364 EP 379 DI 10.1086/324495 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200032 ER PT J AU Young, PR Dupree, AK AF Young, PR Dupree, AK TI Capella: Separating the giants SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : chromospheres; stars : coronae; stars : individual (alpha Aurigae); stars : late-type; ultraviolet : stars ID TRANSITION REGION; EMISSION; STARS; LINE; CORONAE; SPECTRA; HYADES; ORBIT AB Images from the Faint Object Camera (FOC) on the Hubble Space Telescope (HST) are used to spatially separate the two giants of Capella (alpha Aurigae; HD 34029) for the first time at ultraviolet wavelengths. The images were obtained with broadband filters that isolate the wavelength regions 2500-3000 Angstrom and 1300-1500 Angstrom. The cool G8 giant is found to be weaker than the hot G1 giant by factors of around 4 and 17, respectively, in these bands. The latter factor is largely due to the much stronger G1 continuum at short wavelengths. No evidence is found for material lying between the two stars in the images. In addition, the objective prisms of the FOC were used to obtain low-resolution spectra from 1200 to 3000 Angstrom, allowing individual emission lines from each star to be spatially separated. Cool-to-hot star ratios for the emission lines H I Lyalpha, O I lambda1305, Si II lambda1816, C II lambda1335, He II lambda1640, and Si IV lambda1393 are presented, showing that the cool giant is weaker than the hot giant by factors of 5-10 in these lines. The O I emission is only a factor of 2.5 weaker in the cool giant, most probably resulting from fluorescence in the extended atmosphere of the cool giant. The line ratios are compared with values derived from International Ultraviolet Explorer and HST/Goddard High Resolution Spectrograph spectra, which could separate the stars spectrally but not spatially. Reasonable agreement is found although the FOC ratios generally imply lower contributions from the cool giant. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Young, PR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2002 VL 565 IS 1 BP 598 EP 607 DI 10.1086/324481 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200050 ER PT J AU Murray, N Paskowitz, M Holman, M AF Murray, N Paskowitz, M Holman, M TI Eccentricity evolution of migrating planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation ID LOCAL SHEAR INSTABILITY; WEAKLY MAGNETIZED DISKS; PRIMORDIAL SOLAR NEBULA; N-BODY PROBLEM; ORBITAL MIGRATION; TIDAL INTERACTION; SYMPLECTIC MAPS; PROTOPLANETS; SYSTEMS AB We examine the eccentricity evolution of a system of two planets locked in a mean motion resonance, in which either the outer or both planets lose energy and angular momentum. The sink of energy and angular momentum could be a gas or planetesimal disk. We analytically calculate the eccentricity damping rate in the case of a single planet migrating through a planetesimal disk. When the planetesimal disk is cold (the average eccentricity is much less than 1), the circularization time tau(c) is comparable to the inward migration time tau(m) as previous calculations have found for the case of a gas disk. If the planetesimal disk is hot, tau(c) can be an order of magnitude shorter than tau(m). We show that the eccentricity of both planetary bodies can grow to large values, particularly if the inner body does not directly exchange energy or angular momentum with the disk. We present the results of numerical integrations of two migrating resonant planets showing rapid growth of eccentricity. We also present integrations in which a Jupiter-mass planet is forced to migrate inward through a system of 5-10 roughly Earth-mass planets. The migrating planet can eject or accrete the smaller bodies; roughly 5% of the mass (averaged over all the integrations) accretes onto the central star. The results are discussed in the context of the currently known extrasolar planetary systems. C1 Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Murray, N (reprint author), Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. NR 33 TC 41 Z9 41 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2002 VL 565 IS 1 BP 608 EP 620 DI 10.1086/324536 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200051 ER PT J AU Dobrzycka, D Cranmer, SR Raymond, JC Biesecker, DA Gurman, JB AF Dobrzycka, D Cranmer, SR Raymond, JC Biesecker, DA Gurman, JB TI Polar coronal jets at solar minimum SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : activity; Sun : corona; Sun : UV radiation ID ANGLE SPECTROMETRIC CORONAGRAPH; DENSITY STRUCTURE; SOHO MISSION; WHITE-LIGHT; HOLES; PLUMES; TELESCOPE; UVCS/SOHO; MODEL; EIT AB We present an analysis of six polar coronal jets observed by the Ultraviolet Coronagraph Spectrometer (UVCS) at solar minimum (1996). Four of the events were also recorded by the Extreme-Ultraviolet Imaging Telescope (EIT) and/or the Large Angle Spectrometric Coronagraph (LASCO) C2 coronagraph. We compared the jets with others recorded in 1997. We modeled the observable properties of the jet from 1996 June 11, detected at 1.5 R-circle dot. It represents a type of polar jet in which H I Lyalpha and O VI get brighter at the same time. The model reproduced the line properties with an electron density enhancement of a factor of 2 (with a resulting density of 4.8 x 10(6) cm(-3)), an outflow velocity enhancement of a factor of 3 (yielding a velocity of 200 km s(-1)), and an electron temperature decrease of a factor of 0.36 (with a resulting temperature of 5.3 x 10(5) K). We derived the jet's electron densities from the LASCO C2 white-light observations. They are a factor of 1.5 higher than in the interplume corona and comparable to those in plume regions within the C2 field of view. We developed a model for the origin of polar jets based on Wang's model for plumes. We envisioned that jets may be the result of short-lived bursts of base heating, while plumes may be the result of base-heating events that last longer than several hours. Models with the base heat flux near 3 x 10(5) ergs cm(-2) s(-1) come closest to matching the observations, though they are not entirely consistent. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Emergent Informat Technol Inc, Vienna, VA 22180 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Dobrzycka, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 33 TC 17 Z9 17 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2002 VL 565 IS 1 BP 621 EP 629 DI 10.1086/324431 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QP UT WOS:000173507200052 ER PT J AU Barmby, P Perrett, KM Bridges, TJ AF Barmby, P Perrett, KM Bridges, TJ TI The 'remarkable' M31 globular cluster 037-B327 revisited SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE globular clusters : general; galaxies : individual : M31; galaxies : star clusters ID HUBBLE-SPACE-TELESCOPE; SYSTEM; DISTANCE AB The M31 globular cluster candidate 037-B327 has long been known to be an extremely red, non-stellar object. The first published spectrum of this object is used to confirm that it is a globular cluster belonging to M31, with rather typical values of upsilon(r) = -338 +/- 12 km s(-1) and [Fe/H] = -1.07 +/- 0.20 dex. Using the spectroscopic metallicity to predict the intrinsic colours, we derive a reddening value of E(B - V) = 1.30 +/- 0.04, in good agreement with the value obtained using reddening-free parameters. The extinction-corrected magnitude of 037-B327 is V-0 = 12.73 (absolute magnitude M-V = -11.74), which makes it the most luminous globular cluster in M31. We examine van den Bergh's argument regarding the brightest and most-reddened globular cluster in M31; we find that the brightest clusters are more heavily reddened than average, but this can be explained by selection effects rather than a different R-V in M31. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Queens Univ, Dept Phys, Kingston, ON K7L 3N6, Canada. Anglo Australian Observ, Epping, NSW 1710, Australia. RP Barmby, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 29 TC 18 Z9 18 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 JAN 11 PY 2002 VL 329 IS 2 BP 461 EP 464 DI 10.1046/j.1365-8711.2002.04993.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 516ZV UT WOS:000173587400026 ER PT J AU Walsh, AJ Lee, JK Burton, MG AF Walsh, AJ Lee, JK Burton, MG TI The massive star-forming region G323.74-0.26 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE masers; stars : formation; HII regions; ISM : individual : G323.74-0.26; ISM : jets and outflows ID METHANOL MASERS; GHZ; EMISSION; LINE; SPECTROMETER; TELESCOPE; POSITIONS; OH AB We report near-infrared molecular hydrogen and Brackett gamma observations towards the massive star formation site G323.74-0.26. The region contains an H II region, similar to 30 arcsec across, and two Class II methanol maser sites, which are separate from the H II region. We show that the spectral type of the star powering the H II region is B0. We also show that at least one of the maser sites is powered by an infrared source that appears to be at least as luminous as the star responsible for the H II region. However, neither of the two stars associated with the methanol maser sites shows any signs of radio continuum emission above 0.2 mJy. For at least one of these maser sites, this shows a real deficiency in the radio continuum flux, which we suggest is an indication that the star is in an early stage of development, before its H II region becomes visible, or it is a multiple intermediate mass star system. A shocked molecular hydrogen outflow is seen extending from one of the maser sites towards the west and possibly in a fan shape, suggesting that the stars, associated with the maser sites are indeed at a very early stage of evolution. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ New S Wales, Dept Astrophys & Opt, Sch Phys, Sydney, NSW 2052, Australia. RP Walsh, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 42,60 Garden St, Cambridge, MA 02138 USA. RI Walsh, Andrew/B-5627-2013; OI Walsh, Andrew/0000-0001-9506-0855; Burton, Michael/0000-0001-7289-1998 NR 28 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 JAN 11 PY 2002 VL 329 IS 2 BP 475 EP 480 DI 10.1046/j.1365-8711.2002.05006.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 516ZV UT WOS:000173587400028 ER PT J AU Brough, S Collins, CA Burke, DJ Mann, RG Lynam, PD AF Brough, S Collins, CA Burke, DJ Mann, RG Lynam, PD TI Evolution of brightest cluster galaxies in X-ray clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : formation ID BAND HUBBLE DIAGRAM AB A recent paper presents the analysis of the K-band Hubble diagram of 76 brightest cluster galaxies (BCGs) in X-ray clusters and shows that the properties of BCGs depend on the X-ray luminosity (L-X) of their host clusters. Unfortunately, the low numbers of nearby clusters in this sample makes it difficult to constrain evolutionary trends. In this letter we extend the Hubble diagram of Burke, Collins & Mann to a total of 155 clusters using new data on 79 BCGs at z less than or equal to 0.1 from the 2MASS extended source catalogue. We show that the major division between BCGs in high- and low-L-X clusters disappears at z less than or equal to 0.1, with BCGs having similar absolute magnitudes independent of the X-ray luminosity of their host clusters. At larger redshifts, the K-band light of BCGs in high-L-X systems is consistent with little or no merging back to z similar to 0.8, whereas BCGs in the low-L-X systems have a different evolutionary history, with many increasing their mass by a factor greater than or equal to4 since z similar or equal to 1. This provides direct evidence of hierarchical merging in a galaxy population. C1 Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Edinburgh, Inst Astron, Edinburgh EH9 3NJ, Midlothian, Scotland. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Brough, S (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, Egerton Wharf, Birkenhead CH41 1LD, Merseyside, England. NR 25 TC 30 Z9 30 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 JAN 11 PY 2002 VL 329 IS 2 BP L53 EP L56 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 516ZV UT WOS:000173587400006 ER PT J AU Di Matteo, T Perna, R Abel, T Rees, MJ AF Di Matteo, T Perna, R Abel, T Rees, MJ TI Radio foregrounds for the 21 centimeter tomography of the neutral intergalactic medium at high redshifts SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; galaxies : general ID RADIATIVE-TRANSFER; SOURCE COUNTS; REIONIZATION; GALAXIES; SIGNATURES; OBJECTS AB Absorption or emission against the cosmic microwave background (CMB) radiation may be observed in the redshifted 21 cm line if the spin temperature of the neutral intergalactic medium (IGM) prior to reionization differs from the CMB temperature. This so-called 21 cm tomography should reveal important information on the physical state of the IGM at high redshifts. The fluctuations in the redshifted 21 cm line, due to gas density inhomogeneities at early times, should be observed at meter wavelengths by the next-generation radio telescopes such as the proposed Square Kilometer Array (SKA). Here we show that the extragalactic radio sources provide a serious contamination to the brightness temperature fluctuations expected in the redshifted 21 cm emission from the IGM at high redshifts. Unless the radio source population cuts off at flux levels above the planned sensitivity of SKA, its clustering noise component will dominate the angular fluctuations in the 21 cm signal. The integrated foreground signal is smooth in frequency space, and it should nonetheless be possible to identify the sharp spectral feature arising from the nonuniformities in the neutral hydrogen density during the epoch when the first UV sources reionize the IGM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astron, Cambridge CB03 0HA, England. RP Di Matteo, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 33 TC 139 Z9 139 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 JAN 10 PY 2002 VL 564 IS 2 BP 576 EP 580 DI 10.1086/324293 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509TZ UT WOS:000173166900006 ER PT J AU Corbett, EA Norris, RP Heisler, CA Dopita, MA Appleton, P Struck, C Murphy, T Marston, A Charmandaris, V Kewley, L Zezas, AL AF Corbett, EA Norris, RP Heisler, CA Dopita, MA Appleton, P Struck, C Murphy, T Marston, A Charmandaris, V Kewley, L Zezas, AL TI First results from the COLA project: The radio-far-infrared correlation and compact radio cores in southern COLA galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : starburst; infrared : galaxies; radio continuum : galaxies ID ACTIVE GALACTIC NUCLEI; STARBURST-AGN CONNECTION; BROAD-LINE REGION; SEYFERT-GALAXIES; IRAS OBSERVATIONS; SPIRAL GALAXIES; STAR-FORMATION; HOT DUST; EMISSION; LUMINOSITY AB We present the first results from the COLA (compact objects in low-power AGNs) project, which aims to determine the relationship between one facet of AGN activity, the compact radio core, and star formation in the circumnuclear region of the host galaxy. This will be accomplished by the comparison of the multiwavelength properties of a sample of AGNs with compact radio cores to those of a sample of AGNs without compact cores and a matched sample of galaxies without AGNs. In this paper we discuss the selection criteria for our galaxy samples and present the initial radio observations of the 107 southern (delta < 0&DEG;) galaxies in our sample. Low-resolution ATCA observations at 4.8, 2.5, and 1.4 GHz and high-resolution, single-baseline snapshots at 2.3 GHz with the Australian Long Baseline Array (LBA) are presented. We find that for the majority of the galaxies in our sample, the radio luminosity is correlated with the far-infrared (FIR) luminosity. However, a small number of galaxies exhibit a radio excess causing them to depart from the FIR-radio correlation. Compact radio cores are detected at fluxes greater than 1.5 mJy in nine of the 105 galaxies observed with the LBA. The majority (8/9) of these galaxies exhibit a radio excess, and 50% (7/14) of the galaxies that lie above the radio-FIR correlation by more than 1 p have compact radio cores. The emission from the compact cores is too weak to account for this radio excess, implying that there are radio structures associated with the compact cores that extend farther than the 0."05 resolution (corresponding to a linear scale 11-22 pc) of the LBA. There is no evidence that the radio luminosity of the compact cores is correlated with the FIR galaxy luminosity, indicating that the core contributes little to the overall FIR emission of the galaxy. The galaxies with compact cores tend to be classified optically as AGNs, with two-thirds (6/9) exhibiting Seyfert-like optical emission line ratios, and the remaining galaxies classified either as composite objects (2/9) or starburst (1/9). The galaxies classified optically as AGNs also exhibit the largest radio excesses, and we therefore conclude that a large radio excess on the radio-FIR correlation is a strong indication of an AGN with a compact radio core. C1 Anglo Australian Observ, Epping, NSW 1710, Australia. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Iowa State Univ, Erwin W Fick Observ, Ames, IA 50011 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Corbett, EA (reprint author), Anglo Australian Observ, POB 296, Epping, NSW 1710, Australia. RI Charmandaris, Vassilis/A-7196-2008; Norris, Ray/A-1316-2008; Dopita, Michael/P-5413-2014; Zezas, Andreas/C-7543-2011; OI Charmandaris, Vassilis/0000-0002-2688-1956; Norris, Ray/0000-0002-4597-1906; Dopita, Michael/0000-0003-0922-4986; Zezas, Andreas/0000-0001-8952-676X; Struck, Curtis/0000-0002-6490-2156; Appleton, Philip/0000-0002-7607-8766; Murphy, Tara/0000-0002-2686-438X NR 80 TC 20 Z9 20 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2002 VL 564 IS 2 BP 650 EP 668 DI 10.1086/324281 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509TZ UT WOS:000173166900012 ER PT J AU Marshall, HL Miller, BP Davis, DS Perlman, ES Wise, M Canizares, CR Harris, DE AF Marshall, HL Miller, BP Davis, DS Perlman, ES Wise, M Canizares, CR Harris, DE TI A high-resolution X-ray image of the jet in M87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M87); galaxies : jets; X-rays : galaxies ID RADIO; SPECTRUM; NUCLEUS; M-87 AB We present the first high-resolution X-ray image of the jet in M87 using the Chandra X-Ray Observatory. There is clear structure in the jet and almost all of the optically bright knots are detected individually. The unresolved core is the brightest X-ray feature but is only 2-3 times brighter than knot A (12."3 from the core) and the inner knot HST-1 (1."0 from the core). The X-ray and optical positions of the knots are consistent at the 0."1 level, but the X-ray emission from the brightest knot (A) is marginally upstream of the optical emission peak. Detailed Gaussian fits to the X-ray jet one-dimensional profile show distinct X-ray emission that is not associated with specific optical features. The X-ray/optical flux ratio decreases systematically from the core, and X-ray emission is not clearly detected beyond 20" from the core. The X-ray spectra of the core and the two brightest knots, HST-1 and A, are consistent with a simple power law (S-nu proportional to nu(-alpha)) with alpha = 1.46 +/- 0.05, practically ruling out inverse Compton models as the dominant X-ray emission mechanism. The core flux is significantly larger than expected from an advective accretion flow, and the spectrum is much steeper, indicating that the core emission may be due to synchrotron emission from a small-scale jet. The spectral energy distributions of the knots are well fitted by synchrotron models. The spectral indices in the X-ray band, however, are comparable to that expected in the Kardashev-Pacholczyk synchrotron model but are much flatter than expected in the pitch-angle isotropization model of Jaffe and Perola. The break frequencies derived from both models drop by factors of 10-100 with distance from the core. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marshall, HL (reprint author), MIT, Ctr Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 29 TC 134 Z9 136 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 JAN 10 PY 2002 VL 564 IS 2 BP 683 EP 687 DI 10.1086/324396 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509TZ UT WOS:000173166900014 ER PT J AU Moscadelli, L Menten, KM Walmsley, CM Reid, MJ AF Moscadelli, L Menten, KM Walmsley, CM Reid, MJ TI Kinematics of the 12 GHz methanol masers toward W3(OH) SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (W3); ISM : molecules; masers; radio lines : ISM; stars : formation ID VLBI OBSERVATIONS; PROPER MOTIONS; OH MASERS; REGIONS; DISKS AB In this paper, two epochs (1994 February and 1998 December) of Very Long Baseline Array observations of the 12 GHz CH3OH masers toward the ultracompact (UC) H II region W3(OH) are compared. The 12 GHz maser emission is observed in three separated clumps (<500 AU in size), located north, south, and at the center of the UC H II region. The general structure of the 12 GHz maser emission has remained remarkably constant, with the maser spots identified in the 1994 epoch maps having similar relative positions (within a few milliarcseconds), shapes, and line-of-sight velocities (within a few tenths of a kilometer per second) as in the 1998 epoch maps. Cross-correlating the intensity distribution of the corresponding spots between the two epochs, we measure relative proper motions of amplitude in the range 1-7 km s(-1). The spots of the southern clump move relative to the reference feature (located in the northern clump) with high velocities (&AP;4 km s(-1)) and have similar directions of motion. This suggests that the whole southern clump moves relative to the northern clump. The amplitude of the proper motions of the 12 GHz masers agrees well with the values measured for the 1.665 GHz OH masers in W3(OH). The different spatial distribution of the 1.665 and 12 GHz maser spots prevents one from performing a detailed comparison of the gas motion traced by the two maser transitions. The 12 GHz CH3OH masers of the northern clump are clearly associated with both the 6.035 GHz OH and 6.7 GHz CH3OH masers. In particular, the same "linear structure" (&AP;200 mas in size at P.A. = 141&DEG;) is traced by the most intense spots of the three maser species, and they all show a common regular variation of the line-of-sight velocities along it. We fit the measured three-dimensional velocities and the sky-projected positions of the 12 GHz maser spots of the northern clump with an "expanding conical model," in which the spots lie on the surface of a bipolar cone and are accelerated radially outward, spiraling with a constant angular velocity around the cone axis. The model suggests that geometrical conditions may play an important selective role in the observation of the strong 12 GHz masers since the strongest spots are predicted at positions on the conical surface where the cone generators are approximately parallel (within a few degrees) to the line of sight. C1 Stn Astron Cagliari, I-09012 Capoterra, CA, Italy. Max Planck Inst Radioastron, D-5300 Bonn, Germany. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moscadelli, L (reprint author), Stn Astron Cagliari, Loc Poggio Pina,Str 54, I-09012 Capoterra, CA, Italy. OI Moscadelli, Luca/0000-0002-8517-8881 NR 20 TC 36 Z9 36 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2002 VL 564 IS 2 BP 813 EP 826 DI 10.1086/324304 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509TZ UT WOS:000173166900026 ER PT J AU Shang, H Glassgold, AE Shu, FH Lizano, S AF Shang, H Glassgold, AE Shu, FH Lizano, S TI Heating and ionization of X-winds SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : formation; stars : winds, outflows; X-rays : stars ID MAGNETOCENTRIFUGALLY DRIVEN FLOWS; YOUNG STELLAR OBJECTS; T-TAURI STARS; MUTUAL NEUTRALIZATION; RAY IONIZATION; EXTINCT RADIOACTIVITIES; AMBIPOLAR DIFFUSION; PROTON COLLISIONS; PROTOSTELLAR JETS; THERMAL STRUCTURE AB In order to compare the X-wind with observations, one needs to be able to calculate its thermal and ionization properties. We formulate the physical basis for the streamline-by-streamline integration of the ionization and heat equations of the steady X-wind. In addition to the well-known processes associated with the interaction of stellar and accretion funnel hot spot radiation with the wind, we include X-ray heating and ionization, mechanical heating, and a revised calculation of ambipolar diffusion heating. The mechanical heating arises from fluctuations produced by star-disk interactions of the time-dependent X-wind that are carried by the wind to large distances where they are dissipated in shocks, MHD waves, and turbulent cascades. We model the time-averaged heating by the scale-free volumetric heating rate, Gamma(mech) = alpharhonu(3)s(-1), where rho and v are the local mass density and wind speed, respectively, s is the distance from the origin, and alpha is a phenomenological constant. When we consider a partially revealed but active young stellar object, we find that choosing alpha similar to 10(-3) in our numerical calculations produces temperatures and electron fractions that are high enough for the X-wind jet to radiate in the optical forbidden lines at the level and on the spatial scales that are observed. We also discuss a variety of applications of our thermal-chemical calculations that can lead to further observational checks of X-wind theory. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58090, Michoacan, Mexico. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hshang@cfa.harvard.edu; aeg@astro.berkeley.edu; fshu@astro.berkeley.edu; lizano@astrosmo.unam.mx NR 97 TC 122 Z9 122 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2002 VL 564 IS 2 BP 853 EP 876 DI 10.1086/324197 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509TZ UT WOS:000173166900030 ER PT J AU Wood, K Wolff, MJ Bjorkman, JE Whitney, B AF Wood, K Wolff, MJ Bjorkman, JE Whitney, B TI The spectral energy distribution of HH30IRS: Constraining the circumstellar dust size distribution SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; dust, extinction; radiative transfer; scattering; stars : individual (HH 30 IRS); stars : pre-main-sequence ID YOUNG STELLAR OBJECTS; HL TAURI REGION; RADIATION TRANSFER; LIGHT-SCATTERING; ACCRETION DISKS; JET; HH-30; STARS; EXTINCTION; PARTICLES AB We present spectral energy distribution (SED) models for the edge-on classical T Tauri star HH 30 IRS that indicate that dust grains have grown to larger than 50 mum within its circumstellar disk. The disk geometry and inclination are known from previous modeling of multiwavelength Hubble Space Telescope images, and we use the SED (0.5 mum less than or equal to lambda less than or equal to 3 mm) to constrain the dust size distribution. Model spectra are shown for different circumstellar dust models: a standard interstellar medium (ISM) mixture and larger grain models. As compared to ISM grains, the larger dust grain models have a shallower wavelength-dependent opacity : smaller at short wavelengths and larger at long wavelengths. Models with the larger dust grains provide a good match to the observed SED of HH 30 IRS. Although the currently available SED is poorly sampled, we estimate and a L-* approximate to 0.2 L-., M-disk approximate to 1.5 x 10(-3) M-., power law with exponential cutoff dust grain size distribution. This model provides a good fit to the currently available data, but mid- and far-IR observations are required to more tightly constrain the size distribution. The accretion luminosity in our models is L-acc less than or similar to 0.2L(*), corresponding to an accretion rate (M) over dot less than or similar to 4 x 10(-9) M-. yr(-1). Dust size distributions that are simple power-law extensions (i.e., no exponential cutoff) yield acceptable fits to the optical/near-IR but too much emission at millimeter wavelengths, and require larger disk masses up to M-disk similar to 0.5 M-.. Such a simple size distribution would not be expected in an environment such as the disk of HH 30 IRS (i.e., where coagulation and accretion processes are occurring in addition to grain shattering), particularly over such a large range in grain sizes. Its ability to adequately characterize the grain populations, however, may be determined from more complete observational sampling of the SED in the mid- to far-IR. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9AD, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Sci Inst, Boulder, CO 80303 USA. Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. RP Wood, K (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9AD, Fife, Scotland. NR 48 TC 114 Z9 114 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2002 VL 564 IS 2 BP 887 EP 895 DI 10.1086/324285 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509TZ UT WOS:000173166900032 ER PT J AU Remillard, RA Sobczak, GJ Muno, MP McClintock, JE AF Remillard, RA Sobczak, GJ Muno, MP McClintock, JE TI Characterizing the quasi-periodic oscillation behavior of the X-ray nova XTE J1550-564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (XTE J1550-564); X-rays : stars ID PHASE-LAG VARIABILITY; MICROQUASAR GRS-1915+105; RXTE OBSERVATIONS; GRO J1655-40; CYGNUS X-1; BINARIES; MODEL AB For all 209 Rossi X-Ray T iming Explorer observations of the X-ray nova XTE J1550-564 during its major outburst of 1998-1999, we have analyzed the X-ray power spectra, phase lags, and coherence functions. These observations constitute one of the richest and most complete data sets obtained for any black hole X-ray nova. The phase lags and coherence measures of low-frequency quasi-periodic oscillations (QPOs; nu<20 Hz) are used to distinguish three types (one more than those reported by Wijnands, Homan, & van der Klis). For the most common type ("C"), the phase lag is correlated with both the QPO frequency and the amplitude. The physical significance of the QPO types is evident in the relationships between QPO properties and the apparent temperature and flux from the accretion disk. There is also a clear pattern in how the QPO types relate to the presence of high-frequency QPOs (ν>100 Hz). In general, the amplitude of low-frequency QPOs decreases when high-frequency oscillations appear, and when both low-frequency and high-frequency QPOs are present, their Q-values (nu/FWHM) are anticorrelated. We speculate that this opposition between low-frequency and high-frequency QPOs arises from competing structures in a perturbed accretion disk. However, we find that the frequencies of slow and fast QPOs are not correlated. In addition, we encounter systematic problems in attempting to reliably compare the QPO frequencies with broad features in the power continuum, since there are a variable number of features or spectral breaks in the power spectra. These results cast some doubt on the reported global relationship between QPOs from neutron stars and those from black hole systems. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Remillard, RA (reprint author), MIT, Ctr Space Res, Cambridge, MA 02139 USA. NR 38 TC 112 Z9 114 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2002 VL 564 IS 2 BP 962 EP 973 DI 10.1086/324276 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509TZ UT WOS:000173166900040 ER PT J AU Raymond, JC Uzzo, M Ko, YK Mancuso, S Wu, R Gardner, L Kohl, JL Marsden, B Smith, PL AF Raymond, JC Uzzo, M Ko, YK Mancuso, S Wu, R Gardner, L Kohl, JL Marsden, B Smith, PL TI Far-ultraviolet observations of Comet 2P/Encke at perihelion SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : individual (2P/Encke); ultraviolet : solar system ID LYMAN-ALPHA OBSERVATIONS; CORONAGRAPH SPECTROMETER; X-RAY; SOLAR; ENCKE; SPECTRA; NUCLEUS; SOHO; IONS; ATMOSPHERES AB Comet 2P/Encke was observed with UVCS/SOHO near perihelion (2000 September 9 and 11) in the Lyman lines of hydrogen. We present a Lyalpha image reconstructed from a series of long-slit spectra, along with the intensity ratios of Lyalpha, Lybeta, and Lygamma. The narrow Lyalpha profile indicates that the observed photons are scattered from hydrogen atoms produced by dissociation of H(2)O and OH, though a broader profile far from the coma suggests a contribution from hydrogen atoms produced by charge transfer with solar wind protons. The outgassing rate derived from the Lyalpha intensity distribution is in excellent agreement with Sekanina's model of two active vents. We also present upper limits for the outgassing rates of the noble gases helium, neon, and argon. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu; muzzo@cfa.harvard.edu; yko@cfa.harvard.edu; mancuso@to.astro.it; rwu@cfa.harvard.edu; lgardner@cfa.harvard.edu; jkohl@cfa.harvard.edu; bmarsden@cfa.harvard.edu; plsmith@cfa.harvard.edu NR 50 TC 10 Z9 10 U1 0 U2 5 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 JAN 10 PY 2002 VL 564 IS 2 BP 1054 EP 1060 DI 10.1086/324545 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509TZ UT WOS:000173166900051 ER PT J AU Menou, K Perna, R Hernquist, L AF Menou, K Perna, R Hernquist, L TI Hydrogen-poor disks in compact X-ray binaries SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; MHD; turbulence; X-rays : stars ID DWARF NOVA OUTBURSTS; ACCRETION DISKS; INSTABILITY MODEL; 4U 1820-30; PARAMETER; DISCOVERY; SYSTEMS; FRONTS; PERIOD; STARS AB We show that accretion disks in several compact X-ray binaries with hydrogen-depleted donors are likely subject to a thermal ionization instability, unless they are strongly irradiated. These disks are particularly interesting in that their MHD-turbulent properties in the neutral phase may be quite different from those of standard, hydrogen-rich disks. C1 Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist Astrofis Spaziale, I-00133 Rome, Italy. RP Menou, K (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA. NR 37 TC 36 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 JAN 10 PY 2002 VL 564 IS 2 BP L81 EP L84 DI 10.1086/338909 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509UD UT WOS:000173167300006 ER PT J AU Wilkes, BJ Schmidt, GD Cutri, RM Ghosh, H Hines, DC Nelson, B Smith, PS AF Wilkes, BJ Schmidt, GD Cutri, RM Ghosh, H Hines, DC Nelson, B Smith, PS TI The X-ray properties of 2MASS red active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars : general; surveys; X-rays : galaxies ID BROAD ABSORPTION-LINE; LUMINOUS INFRARED GALAXIES; SEYFERT 2 GALAXIES; AREA SURVEY HELLAS; SPECTRAL PROPERTIES; SYNTHESIS MODELS; QUASARS; CHANDRA; EMISSION; BEPPOSAX AB The Two Micron All Sky Survey is finding previously unidentified, luminous, red, active galactic nuclei (AGNs). This new sample has a space density similar to, or greater than, previously known AGNs, suggesting that a large fraction of the overall population has been missed. Chandra observations of a well-defined subset of these objects reveal that all are X-ray-faint, with the reddest sources being the faintest in X-rays. The X-ray hardness ratios cover a wide range, generally indicating N(H)similar to10(21)cm(-2), but the softest sources show no spectral evidence for intrinsic absorption. These characteristics suggest that a mix of absorbed, direct emission and unabsorbed, scattered, and/or extended emission contributes to the X-ray flux, although we cannot rule out the possibility that they are intrinsically X-ray-weak. This population of X-ray-faint, predominantly broad-line objects could provide the missing population of X-ray-absorbed AGNs required by current models of the cosmic X-ray background. The existence of AGNs that display both broad emission lines and absorbed X-rays has important implications for unification schemes and emphasizes the need for care in assigning classifications to individual AGNs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bwilkes@cfa.harvard.edu; gschmidt@as.arizona.edu; roc@ipac.caltedh.edu; hghosh@cfa.harvard.edu; dhines@as.arizona.edu; nelson@ipac.caltech.edu; psmith@as.arizona.edu OI Wilkes, Belinda/0000-0003-1809-2364 NR 44 TC 43 Z9 43 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2002 VL 564 IS 2 BP L65 EP L68 DI 10.1086/338908 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509UD UT WOS:000173167300002 ER PT J AU Sanjur, OI Piperno, DR Andres, TC Wessel-Beaver, L AF Sanjur, OI Piperno, DR Andres, TC Wessel-Beaver, L TI Phylogenetic relationships among domesticated and wild species of Cucurbita (Cucurbitaceae) inferred from a mitochondrial gene: Implications for crop plant evolution and areas of origin SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID CHLOROPLAST DNA; AMPLIFICATION; SUBSTITUTION; SYSTEMATICS; CULTIVATION; AMERICA; PEPO AB We have investigated the phylogenetic relationships among six wild and six domesticated taxa of Cucurbita using as a marker an intron region from the mitochondrial nad1 gene. Our study represents one of the first successful uses of a mtDNA gene in resolving inter- and intraspecific taxonomic relationships in Angiosperms and yields several important insights into the origins of domesticated Cucurbita. First, our data suggest at least six independent domestication events from distinct wild ancestors. Second, Cucurbita argyrosperma likely was domesticated from a wild Mexican gourd, Cucurbita sororia, probably in the same region of southwest Mexico that gave rise to maize. Third, the wild ancestor of Cucurbita moschata is still unknown, but mtDNA data combined with other sources of information suggest that it will probably be found in lowland northern South America. Fourth, Cucurbita andreana is supported as the wild progenitor of Cucurbita maxima, but humid lowland regions of Bolivia in addition to warmer temperate zones in South America from where C andreana was originally described should possibly be considered as an area of origin for C maxima. Fifth, our data support other molecular results that indicate two separate domestications in the Cucurbita pepo complex. The potential zone of domestication for one of the domesticated subspecies, C pepo subsp. ovifera, includes eastern North America and should be extended to northeastern Mexico. The wild ancestor of the other domesticated subspecies, C. pepo subsp. pepo, is undiscovered but is closely related to C. pepo subsp. fraterna and possibly will be found in southern Mexico. C1 Smithsonian Trop Res Inst, Mol Evolut Labs, Balboa, Panama. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. Curcurbit Network, Bronx, NY 10471 USA. Univ Puerto Rico, Dept Agron & Soils, Mayaguez, PR 00681 USA. RP Sanjur, OI (reprint author), Smithsonian Trop Res Inst, Mol Evolut Labs, Box 2072, Balboa, Panama. NR 32 TC 123 Z9 142 U1 3 U2 46 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 8 PY 2002 VL 99 IS 1 BP 535 EP 540 DI 10.1073/pnas.012577299 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 510XV UT WOS:000173233300095 PM 11782554 ER PT J AU Termonia, A Pasteels, JM Windsor, DM Milinkovitch, MC AF Termonia, A Pasteels, JM Windsor, DM Milinkovitch, MC TI Dual chemical sequestration: a key mechanism in transitions among ecological specialization SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE chemical defence; toxin sequestration; ecological specialization; molecular phylogeny ID TREE TOPOLOGIES; EVOLUTION; ALKALOIDS; PLANT AB Platyphora leaf beetles form a vast group of tropical species each feeding on a restricted set of host plants and exhibiting bright coloration warning predators against their chemical protection. These beetles offer an exceptional opportunity for understanding the evolution of phytochemical sequestration. Indeed, qualitative studies of defensive secretions indicate that Platyphora species acquire toxicity via sequestration of plant secondary metabolites. All produce pentacyclic triterpene saponins from sequestered plant amyrins, but our analyses also indicate that many Platyphora species produce a dual chemical defence, that is, they are additionally protected by lycopsamine-type pyrolyzidine alkaloids that they also sequester from their host. This paper reports on the evolution of chemical defence and host affiliation in Platyphora leaf beetles as reconstructed on a molecular phylogeny of mitochondrial and nuclear DNA sequences. The analyses indicate that dual sequestration could be the key mechanistic means by which transitions among ecological specializations (i.e. restricted host-plant affiliations) are made possible. C1 Free Univ Brussels, Unit Evolutionary Genet, Inst Mol Biol & Med, B-6041 Gosselies, Belgium. ULB, Lab Biol Anim & Cellulaire, B-1050 Brussels, Belgium. Smithsonian Trop Res Inst, Balboa, Panama. RP Milinkovitch, MC (reprint author), Free Univ Brussels, Unit Evolutionary Genet, Inst Mol Biol & Med, CP 300,Rue Jeener & Brachet 12, B-6041 Gosselies, Belgium. EM mcmilink@ulb.ac.be NR 31 TC 40 Z9 40 U1 1 U2 9 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JAN 7 PY 2002 VL 269 IS 1486 BP 1 EP 6 DI 10.1098/rspb.2001.1859 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 515AP UT WOS:000173473500001 PM 11788029 ER PT J AU Lovette, IJ Bermingham, E Ricklefs, RE AF Lovette, IJ Bermingham, E Ricklefs, RE TI Clade-specific morphological diversification and adaptive radiation in Hawaiian songbirds SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE speciation; adaptive radiation; colonization; morphology; Drepaniidae; Myadestes ID BILL SIZE POLYMORPHISM; AFRICAN FINCH; EVOLUTION; FRINGILLIDAE; SELECTION AB The Hawaiian honeycreepers are a dramatic example of adaptive radiation but contrast with the four other songbird lineages that successfully colonized the Hawaiian archipelago and failed to undergo similar diversification. To explore the processes that produced the diversity dichotomy in this insular fauna, we compared clade age and morphological diversity between the speciose honeycreepers and the comparatively depauperate Hawaiian thrushes. Mitochondrial-DNA-based genetic distances between these Hawaiian clades and their continental sister taxa indicate that the ancestral thrush colonized the Hawaiian Islands as early as the common ancestor of the honeycreepers. This similar timing of colonization indicates that the marked difference in diversity between the Hawaiian honeycreeper and thrush clades is unlikely to result from differences in these clades' tenures within the archipelago. If time cannot explain the contrasting diversities of these taxa, then an intrinsic, clade-specific trait may have fostered the honeycreeper radiation. As the honeycreepers have diversified most dramatically in morphological characters related to resource utilization, we used principal components analyses of bill characters to compare the magnitudes of morphological variation in the ancestral clades from which the Hawaiian honeycreeper and thrush lineages are derived, the Carduelini and Turdinae respectively. Although the Carduelini share a more recent common ancestor and have a lower species diversity than the Turdinae, these finch-like relatives of the honeycreepers exhibit significantly greater variation in bill morphology than do the continental relatives of the Hawaiian thrushes. The higher magnitude of morphological variation in the non-Hawaiian Carduelini suggests that the honeycreepers fall within a clade exhibiting a generally high evolutionary flexibility in bill morphology. Accordingly, although the magnitude of bill variation among the honeycreepers is similar to that of the entire passerine radiation, this dramatic morphological radiation represents an extreme manifestation of a general clade-specific ability to evolve novel morphologies. C1 Cornell Univ, Cornell Lab Ornithol, Ithaca, NY 14850 USA. Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14850 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Missouri, Dept Biol, St Louis, MO 63121 USA. RP Lovette, IJ (reprint author), Cornell Univ, Cornell Lab Ornithol, 159 Sapsucker Woods Rd, Ithaca, NY 14850 USA. EM ijl2@cornell.edu RI Lovette, Irby/P-3477-2014 NR 39 TC 102 Z9 104 U1 7 U2 53 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 JAN 7 PY 2002 VL 269 IS 1486 BP 37 EP 42 DI 10.1098/rspb.2001.1789 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 515AP UT WOS:000173473500006 PM 11788034 ER PT J AU Jennions, MD Moller, AP AF Jennions, MD Moller, AP TI Relationships fade with time: a meta-analysis of temporal trends in publication in ecology and evolution SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE ecology; evolution; meta-analysis; paradigms; publication bias ID SEXUAL SELECTION; FLUCTUATING ASYMMETRY; METAANALYSIS; PARADIGM; BIAS AB Both significant positive and negative relationships between the magnitude of research findings (their 'effect size') and their year of publication have been reported in a few areas of biology. These trends have been attributed to Kuhnian paradigm shifts, scientific fads and bias in the choice of study systems. Here we test whether or not these isolated cases reflect a more general trend. We examined the relationship using effect sizes extracted from 44 peer-reviewed meta-analyses covering a wide range of topics in ecological and evolutionary biology. On average, there was a small but significant decline in effect size with year of publication. For the original empirical studies there was also a significant decrease in effect size as sample size increased. However, the effect of year of publication remained even after we controlled for sampling effort. Although these results have several possible explanations, it is suggested that a publication bias against non-significant or weaker findings offers the most parsimonious explanation. As in the medical sciences, non-significant results may take longer to publish and studies with both small sample sizes and non-significant results may be less likely to be published. C1 Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Paris 06, Lab Ecol Evolut Parasitaire, CNRS FRE 2365, F-75252 Paris 5, France. RP Jennions, MD (reprint author), Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. EM michael.jennions@anu.edu.au RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 33 TC 93 Z9 95 U1 0 U2 32 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 JAN 7 PY 2002 VL 269 IS 1486 BP 43 EP 48 DI 10.1098/rspb.2001.1832 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 515AP UT WOS:000173473500007 PM 11788035 ER PT J AU Balakrishnan, N Dalgarno, A AF Balakrishnan, N Dalgarno, A TI Chemistry at ultracold temperatures (vol 341, pg 652, 2001) SO CHEMICAL PHYSICS LETTERS LA English DT Correction C1 Harvard Univ, Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Balakrishnan, N (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 6 Z9 6 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD JAN 4 PY 2002 VL 351 IS 1-2 BP 159 EP 160 DI 10.1016/S0009-2614(01)01363-X PG 2 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 511RX UT WOS:000173280300024 ER PT J AU Abel, T Bryan, GL Norman, ML AF Abel, T Bryan, GL Norman, ML TI The formation of the first star in the universe SO SCIENCE LA English DT Article ID X-RAY-CLUSTERS; GALAXY FORMATION; PRIMORDIAL GAS; FRAGMENTATION; HYDRODYNAMICS; RESOLUTION; SIMULATION; PROTOSTARS; ENRICHMENT; CHEMISTRY AB We describe results from a fully self-consistent three-dimensional hydrodynamical simulation of the formation of one of the first stars in the Universe. In current models of structure formation, dark matter initially dominates, and pregalactic objects form because of gravitational instability from small initial density perturbations. As they assemble via hierarchical merging, primordial gas coots through ro-vibrational lines of hydrogen molecules and sinks to the center of the dark matter potential well. The high-redshift analog of a molecular cloud is formed. As the dense, central parts of the cold gas cloud become self-gravitating, a dense core of similar to 100 M-. (where M-. is the mass of the Sun) undergoes rapid contraction. At particle number densities greater than 10(9) per cubic centimeter, a 1 M-. protostellar core becomes fully molecular as a result of three-body H-2 formation. Contrary to analytical expectations, this process does not lead to renewed fragmentation and only one star is formed. The calculation is stopped when optical depth effects become important, leaving the final mass of the fully formed star somewhat uncertain. At this stage the protostar is accreting material very rapidly (similar to 10(-2) M-. year(-1)). Radiative feedback from the star will not only halt its growth but also inhibit the formation of other stars in the same pregalactic object (at [east until the first star ends its life, presumably as a supernova). We conclude that at most one massive (M >> 1 M-.) metal-free star forms per pregalactic halo, consistent with recent abundance measurements of metal-poor galactic halo stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. MIT, Dept Phys, Div Astrophys, Cambridge, MA 02139 USA. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Abel, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 42 TC 963 Z9 966 U1 5 U2 33 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 4 PY 2002 VL 295 IS 5552 BP 93 EP 98 DI 10.1126/science.1063991 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 509HV UT WOS:000173143100039 PM 11711636 ER PT J AU Flint, OS AF Flint, OS TI List of the name-bearing Neuropterida types in the collection of the National Museum of Natural History, Smithsonian Institution, USA SO ACTA ZOOLOGICA ACADEMIAE SCIENTIARUM HUNGARICAE LA English DT Article; Proceedings Paper CT 7th International Symposium on Neuropterology CY AUG 06-09, 2000 CL BUDAPEST, HUNGARY DE Neuroptera; Megaloptera; Raphidioptera; name-bearing types; Smithsonian Institution AB The collection of Neuropterida at the National Museum of Natural History, Smithsonian Institution, is housed in 221 insect drawers and 311 bottles of vials. It is estimated to contain 132 species of Megaloptera. 1192 species of Neuroptera and 33 species of Raphidioptera. The 163 name-bearing types are divided among the Megaloptera (26), Neuroptera (134), and Raphidioptera (3). A list of all the name-bearing, types including author, year of publication, country of origin. and current placement is given it is also noted if it is a lectotype or neotype. C1 Smithsonian Inst, Dept Entomol, Museum Natl Hist Nat, Washington, DC 20560 USA. RP Flint, OS (reprint author), Smithsonian Inst, Dept Entomol, Museum Natl Hist Nat, NHB 169, Washington, DC 20560 USA. NR 5 TC 3 Z9 3 U1 0 U2 0 PU HUNGARIAN NATURAL HISTORY MUSEUM PI BUDAPEST PA BAROSS U 13, H-1088 BUDAPEST, HUNGARY SN 1217-8837 J9 ACTA ZOOL ACAD SCI H JI Acta Zool. Acad. Sci. Hung. PY 2002 VL 48 SU 2 BP 89 EP 98 PG 10 WC Zoology SC Zoology GA 625DN UT WOS:000179801800009 ER PT S AU Hunter, TR Wilson, RW Kimberk, R Leiker, PS Christensen, R AF Hunter, TR Wilson, RW Kimberk, R Leiker, PS Christensen, R BE Lewis, H TI Receiver control for the Submillimeter Array SO ADVANCED TELESCOPE AND INSTRUMENTATION CONTROL SOFTWARE II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced Telescope and Instrumentation Control Software II CY AUG 27-28, 2002 CL WAIKOLOA, HI SP SPIE, Int Commiss Opt, Amer Astron Soc, European SO Observ, Int Astron Union DE Submillimeter receiver; microcontroller; interferometry; Gunn oscillator; multiplier; DC servo motor; digital PLL ID MILLIMETER ARRAY AB Efficient operation of a submillimeter interferometer requires remote (preferably automated) control of mechanically tuned local oscillators, phase-lock loops, mixers, optics, calibration vanes and cryostats. The present control system for these aspects of the Submillimeter Array (SMA) will be described. Distributed processing forms the underlying architecture. In each antenna cabin, a serial network of up to ten independent 80C196 microcontroller boards attaches to the real-time PowerPC computer (running LynxOS). A multi-threaded, gcc-compiled program on the PowerPC accepts top-level requests via remote procedure calls (RPC), subsequently dispatches tuning commands to the relevant microcontrollers, and regularly reports the system status to optical-fiber-based reflective memory for common access by the telescope monitor and error reporting system. All serial communication occurs asynchronously via encoded, variable-length packets. The microcontrollers respond to the requested commands and queries by accessing non-volatile, rewriteable lookup-tables (when appropriate) and executing embedded software that operates additional electronic devices (DACs, ADCs, etc.). Since various receiver hardware components require linear or rotary motion, each microcontroller also implements a position servo via a one-millisecond interrupt service routine which drives a DC-motor/encoder combination that remains standard across each subsystem. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hunter, TR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA. OI Wilson, Robert/0000-0001-5694-6725; Hunter, Todd/0000-0001-6492-0090 NR 17 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4627-0 J9 P SOC PHOTO-OPT INS PY 2002 VL 4848 BP 206 EP 217 DI 10.1117/12.461362 PG 12 WC Automation & Control Systems; Computer Science, Software Engineering; Instruments & Instrumentation SC Automation & Control Systems; Computer Science; Instruments & Instrumentation GA BV91S UT WOS:000180380600021 ER PT S AU Harasewych, MG AF Harasewych, MG BE Southward, AJ Tyler, PA Young, CM Fuiman, LA TI Pleurotomarioidean gastropods SO ADVANCES IN MARINE BIOLOGY, VOL 42: MOLLUSCAN RADIATION - LESSER-KNOWN BRANCHES SE Advances in Marine Biology LA English DT Review ID PROSOBRANCH GASTROPODS; PHYLOGENY; MOLLUSCA; VETIGASTROPODA; BIOGEOGRAPHY; PEROTROCHUS; SYSTEMATICS; EVOLUTION; PACIFIC; ECOLOGY C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. RP Harasewych, MG (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. EM Harasewych@nmnh.si.edu NR 137 TC 30 Z9 32 U1 2 U2 6 PU ACADEMIC PRESS LTD-ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL ROAD, LONDON NW1 7DX, ENGLAND SN 0065-2881 BN 0-12-026142-1 J9 ADV MAR BIOL JI Adv. Mar. Biol. PY 2002 VL 42 BP 237 EP 294 PG 66 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BU73W UT WOS:000176862800004 PM 12094724 ER PT J AU Ecker, HL AF Ecker, HL TI 'Arab Stones'. Rodrigo Caro's translations of Arabic inscriptions in Seville (1634), revisited SO AL-QANTARA LA English DT Article AB This article seeks to illuminate the problem of baroque translations of medieval Arabic inscriptions, in particular those provided by Rodrigo Caro in 1634 of inscriptions from Seville. The Sevillian inscriptions have been ignored by scholars since the nineteenth century when they were recognized as fraudulent. This paper argues that the content of these false translations was subservient to the context of their production -namely that of the translations of the Grenadine lead books, the baroque perceived ideal of a 'sacred antiquity' and the counter-reformation promotion and elevation of false martyrs and their relics. These were all elements of a conscious programme of a fictitious but significant Christian past in Andalucia. The main protagonists in the Seville translations--Rodrigo Caro, Pedro de Castro and Adan Centurion--were implicated in all of these processes as well as belonging to a Peninsula-wide network of antiquarian enthusiasts and forgers. Their critical judgement, when faced with evident frauds, was consumed by their will to promote specific religious and political agendas. Consequently, their shared translators, with their own agendas, obliged their patrons with capricious ammunition. C1 Smithsonian Inst, Washington, DC 20560 USA. RP Ecker, HL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 88 TC 0 Z9 0 U1 0 U2 0 PU CONSEJO SUPERIOR DE INVESTIGACINVESTIGACIONES CIENTIFICAS PI MADRID PA INSTITUTO DE FILOLOGIA, DUQUE MEDINACELI, 6, 28014 MADRID, SPAIN SN 0211-3589 J9 AL-QANTARA JI Al-Qantara PY 2002 VL 23 IS 2 BP 347 EP 402 PG 56 WC History; Religion SC History; Religion GA 637LF UT WOS:000180512000006 ER PT J AU Barker, AW Skinner, CE Shackley, MS Glascock, MD Rogers, JD AF Barker, AW Skinner, CE Shackley, MS Glascock, MD Rogers, JD TI Mesoamerican origin for an obsidian scraper from the Precolumbian southeastern United States SO AMERICAN ANTIQUITY LA English DT Article AB EDXRF analysis of an obsidian scraper from the Spiro Mounds, Oklahoma, shows that the,source material was from Pachuca. Hidalgo. Mexico. Given the distinctive peralkaline character of the obsidian, the source assignment is considered extremely secure. The artifact wets recovered from the east tunnel of Craig Mound, Spiro, immediately after the cessation of commercial digging in 1935, and has been in the Smithsonian's collections since 1937. Despite more than 150 years of speculation regarding supposed contact with and influence from the region, this represents the first documented example of Mesoamerican material from any Mississippian archaeological context in the Precolumbian southeastern United States. C1 Milwaukee Publ Museum, Dept Anthropol, Milwaukee, WI 53233 USA. NW Res Obsidian Studies Lab, Corvallis, OR 97330 USA. Univ Calif Berkeley, Archaeol XRF Lab, Phoebe Hearst Museum, Berkeley, CA 94720 USA. Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA. Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. RP Barker, AW (reprint author), Milwaukee Publ Museum, Dept Anthropol, 800 W Wells St, Milwaukee, WI 53233 USA. RI Barker, Alex W./L-6496-2014; OI Barker, Alex W./0000-0001-6255-0647; Glascock, Michael D./0000-0003-0686-7556 NR 22 TC 15 Z9 16 U1 0 U2 8 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 0002-7316 J9 AM ANTIQUITY JI Am. Antiq. PD JAN PY 2002 VL 67 IS 1 BP 103 EP 108 DI 10.2307/2694879 PG 6 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 518LF UT WOS:000173669300006 ER PT J AU Prado, J Lellinger, DB AF Prado, J Lellinger, DB TI Adiantum argutum, an unrecognized species of the A-latifolium group SO AMERICAN FERN JOURNAL LA English DT Article AB The present paper distinguishes A. argutum, an unrecognized but widespread species from South America, from the related A. latifolium, and designates a lectotype for A. argutum. C1 Inst Bot, Secao Briol & Pteridol, BR-01061970 Sao Paulo, Brazil. Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, Washington, DC 20560 USA. RP Prado, J (reprint author), Inst Bot, Secao Briol & Pteridol, Caixa Postal 4005, BR-01061970 Sao Paulo, Brazil. RI Prado, Jefferson/C-4766-2012 OI Prado, Jefferson/0000-0003-4783-3125 NR 8 TC 3 Z9 4 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 USA SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD JAN-MAR PY 2002 VL 92 IS 1 BP 23 EP 29 DI 10.1640/0002-8444(2002)092[0023:AAAUSO]2.0.CO;2 PG 7 WC Plant Sciences SC Plant Sciences GA 550KV UT WOS:000175503000004 ER PT J AU McMullen, A AF McMullen, A TI More than curiosities: A grassroots history of the Indian Arts and Crafts Board and its precursors, 1920-1942 SO AMERICAN INDIAN CULTURE AND RESEARCH JOURNAL LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. RP McMullen, A (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU U C L A, AMER INDIAN STUDIES CENTER PI LOS ANGELES PA 3220 CAMPBELL HALL, BOX 951548, LOS ANGELES, CA 90095-1548 USA SN 0161-6463 J9 AM INDIAN CULT RES J JI Am. Indian Cult. Res. J. PY 2002 VL 26 IS 3 BP 152 EP 155 PG 4 WC History SC History GA 655VH UT WOS:000181573000017 ER PT J AU Bobe, R Eck, G AF Bobe, R Eck, G TI Patterns of faunal and environmental change in the Hadar Formation, Ethiopia SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2002 SU 34 BP 45 EP 46 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534VG UT WOS:000174609700047 ER PT J AU Hunt, D Williams, H AF Hunt, D Williams, H TI Asymmetrical angular rotation of the femur; divergence between prehistoric and modern American populations. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Natl Museum Nat Hist, Dept Anthropol, MRC112, Smithsonian Inst, Washington, DC 20560 USA. George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2002 SU 34 BP 87 EP 87 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534VG UT WOS:000174609700220 ER PT J AU Miller, G Hunt, D Lofton, S Mullins, J AF Miller, G Hunt, D Lofton, S Mullins, J TI Evaluation of computer enhanced facial reproduction at the National Center for Missing and Exploited Children using Terry Collection death masks and photographs. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Natl Ctr Missing & Exploited Children, Alexandria, VA USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2002 SU 34 BP 113 EP 113 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534VG UT WOS:000174609700330 ER PT J AU Mulhern, D Ubelaker, D AF Mulhern, D Ubelaker, D TI Histologic examination of age in chimpanzees. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2002 SU 34 BP 116 EP 116 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534VG UT WOS:000174609700343 ER PT J AU Ousley, S Jantz, RL AF Ousley, S Jantz, RL TI Social races and human populations: why forensic anthropologists are good at identifying races. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA. NR 0 TC 0 Z9 0 U1 3 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. PY 2002 SU 34 BP 121 EP 121 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534VG UT WOS:000174609700362 ER PT J AU Potts, R AF Potts, R TI Paleoenvironmental basis of cognitive evolution in great apes. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2002 SU 34 BP 127 EP 127 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534VG UT WOS:000174609700388 ER PT J AU Tuross, N AF Tuross, N TI Human migration in the archaic. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol MSC, Suitland, MD 20746 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2002 SU 34 BP 157 EP 158 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534VG UT WOS:000174609700515 ER PT B AU Mazzotta, P Markevitch, M Vikhlinin, A Forman, WR AF Mazzotta, P Markevitch, M Vikhlinin, A Forman, WR BE Chen, LW Ma, CP Ng, KW Pen, UL TI Chandra observations of cold fronts in clusters of galaxies SO AMIBA 2001: HIGH-Z CLUSTERS, MISSING BARYONS, AND CMB POLARIZATION, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 8th Taipei Astrophysics Workshop on the AMiBA 2001 - High-z Clusters, Missing Baryons, and CMB Polarization CY JUN 11-15, 2001 CL TAIPEI, TAIWAN SP Natl Taiwan Univ, Phys Dept, Acad Sinica, Inst Astron & Astrophys ID RAY-EMITTING GAS AB High-resolution Chandra images of several clusters of galaxies reveal sharp, edge-like discontinuities in their gas density. The gas temperature is higher in front of the edge where the density is low, corresponding to approximately continuous pressure across the edge. This new phenomenon was called "cold fronts", to contrast it to shock fronts that should look similar in X-ray images but where the temperature should jump in the opposite direction. The first cold fronts were discovered in merging clusters, where they appear to delineate the boundaries of dense cool subcluster remnants moving through and being stripped by the surrounding shock-heated gas. Later, Chandra revealed cold fronts in the central regions of several apparently relaxed clusters. To explain the gas bulk motion in these clusters, we propose either a peculiar cluster formation history that resulted in an oscillating core, or gas sloshing (without the involvement of the underlying dark matter peak) caused by past subcluster infall or central AGN activity. We review these observations and discuss their implications for the X-ray cluster mass estimates. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mazzotta, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Forman, William/0000-0002-9478-1682 NR 15 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-097-8 J9 ASTR SOC P PY 2002 VL 257 BP 173 EP 179 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV22W UT WOS:000178268900019 ER PT J AU Day, TA Neale, PJ AF Day, TA Neale, PJ TI Effects of UV-B radiation on terrestrial and aquatic primary producers SO ANNUAL REVIEW OF ECOLOGY AND SYSTEMATICS LA English DT Review DE biological weighting functions; ozone depletion; photosynthesis; phytoplankton; UV screening ID STRATOSPHERIC OZONE DEPLETION; ALPINE LIFE ZONE; SUB-ARCTIC HEATH; CHONDRUS-CRISPUS FLORIDEOPHYCEAE; LEAF EPIDERMAL TRANSMITTANCE; SPECTRAL WEIGHTING FUNCTIONS; SOLAR ULTRAVIOLET-RADIATION; FUEGO SOUTHERN ARGENTINA; MARINE TROPHIC LEVELS; AMINO-ACIDS AB Ozone depletion by anthropogenic gases has increased the atmospheric transmission of solar ultraviolet-B radiation (UV-B, 280-315 nm). Our understanding of the consequencences of enhanced UV-B levels on primary producers has grown dramatically over the past 20 years, but it has been hampered by how realistically experimental U-V-B exposures mimic ozone-depletion scenarios. Overcoming these shortcomings will require sophisticated and creative approaches. Biological weighting functions and solar spectral irradiance estimates are critical in evaluating effects and require more attention. Whereas UV screening compounds in terrestrial and aquatic producers commonly increase with UV-B exposure, the implications, while potentially far reaching, are unclear. Photosynthesis is more sensitive to UV-B in phytoplankton than in terrestrial plants, probably owing to less effective screening in phytoplankton. Productivity of terrestrial plants is usually unaffected by enhanced UV-B, although reduced growth has been observed and may increase in magnitude over successive years. Aquatic productivity is often compromised by short-term exposures to enhanced UV-B, and long-term assessments are complicated by the dynamic nature of aquatic systems and by nonlinear responses. Recent work examining UV-B effects on multiple trophic levels suggests that outcomes will be diverse and difficult to predict. Such effects may lead to feedbacks on primary producers. C1 Arizona State Univ, Dept Plant Biol, Tempe, AZ 85287 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Day, TA (reprint author), Arizona State Univ, Dept Plant Biol, Tempe, AZ 85287 USA. RI Neale, Patrick/A-3683-2012 NR 177 TC 106 Z9 119 U1 5 U2 25 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4162 J9 ANNU REV ECOL SYST JI Annu. Rev. Ecol. Syst. PY 2002 VL 33 BP 371 EP 396 DI 10.1146/annurev.ecolysis.33.010802.150434 PG 26 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 628QE UT WOS:000180007000014 ER PT J AU Mair, RW Walsworth, RL AF Mair, RW Walsworth, RL TI Novel MRI applications of laser-polarized noble gases SO APPLIED MAGNETIC RESONANCE LA English DT Article; Proceedings Paper CT 6th International Conference on Magnetic Resonance Microscopy CY SEP, 2001 CL NOTTINGHAM, ENGLAND ID NUCLEAR-MAGNETIC-RESONANCE; DEPENDENT DIFFUSION-COEFFICIENT; HYPERPOLARIZED XE-129 NMR; TO-VOLUME RATIO; POROUS-MEDIA; CROSS-POLARIZATION; FIELD-GRADIENT; LIQUID XENON; SPIN-ECHO; LONGITUDINAL RELAXATION AB Gas-phase nuclear magnetic resonance (NMR) has great potential as a probe for a variety of interesting physical and biomedical problems that are not amenable to study by water or similar liquid. However, NMR of gases was largely neglected due to the low signal obtained from the thermally polarized gases with very low sample density. The advent of optical pumping techniques for enhancing the polarization of the noble gases He-3 and Xe-129 has bought new life to this field, especially in medical imaging where He-3 lung inhalation imaging is approaching a clinical application. However, there are numerous applications in materials science that also benefit from the use of these gases. We review primarily nonmedical applications of laser-polarized noble gases for both NMR imaging and spectroscopy and highlight progress with examples from our laboratory including high-resolution imaging at millitesla applied field strength and velocity imaging of convective flow. Porous media microstucture has been probed with both thermal and laser-polarized xenon, as xenon is an ideal probe due to low surface interaction with the grains of the porous media. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mair, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 59, Cambridge, MA 02138 USA. NR 83 TC 12 Z9 12 U1 2 U2 9 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0937-9347 EI 1613-7507 J9 APPL MAGN RESON JI Appl. Magn. Reson. PY 2002 VL 22 IS 2 BP 159 EP 173 DI 10.1007/BF03166100 PG 15 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 562QU UT WOS:000176211100004 ER PT S AU Lambert, JB Wu, YY Santiago-Blay, JA AF Lambert, JB Wu, YY Santiago-Blay, JA BE Jakes, KA TI Modern and ancient resins from Africa and the Americas SO ARCHAEOLOGICAL CHEMISTRY: MATERIALS, METHODS, AND MEANING SE ACS SYMPOSIUM SERIES LA English DT Article; Proceedings Paper CT 10th Archaeological Chemistry Symposium held at the 222nd National Meeting of the American-Chemical-Society CY AUG 26-30, 2001 CL CHICAGO, ILLINOIS SP Amer Chem Soc, Div Hist Chem ID MAGNETIC-RESONANCE SPECTROSCOPY; AMBER; CLASSIFICATION AB New samples of resinous materials from Africa and the Americas, both modern and fossilized, have been characterized by solid state carbon-13 nuclear magnetic resonance spectroscopy. The large Hymenaea-related grouping has been expanded to include sites in North Africa (Morocco), West Africa (Mauritania), and several countries in South America (Guyana, Brazil, and Uruguay). The worldwide Agathis-related grouping has been slightly expanded to include locations in North Dakota, North Carolina, and Spain. The other worldwide group, possibly associated with Dipterocarpaceae, has been found to occur also in North Carolina, the second American site to be represented. We have found that Dacryodes excelsa (Burseraceae) from Puerto Rico exhibits the same spectra as materials from the Burseraceae family from Mexico and that Guiacum officinale (Zygophyllaceae) exhibits a unique new spectral pattern. C1 Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Lambert, JB (reprint author), Northwestern Univ, Dept Chem, 2145 Sheridan Rd, Evanston, IL 60208 USA. NR 24 TC 4 Z9 6 U1 1 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 SIXTEENTH ST NW, WASHINGTON, DC 20036 USA SN 0097-6156 BN 0-8412-3810-3 J9 ACS SYM SER PY 2002 VL 831 BP 64 EP 83 DI 10.1021/bk-2002-0831.ch006 PG 20 WC Archaeology; Chemistry, Multidisciplinary; Materials Science, Characterization & Testing SC Archaeology; Chemistry; Materials Science GA BW17G UT WOS:000181072600006 ER PT J AU Mann, T AF Mann, T TI Thomas Eakins SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Mann, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 2002 VL 42 IS 1-2 BP 34 EP 37 PG 4 WC Art SC Art GA 753LR UT WOS:000187233300005 ER PT J AU Mann, T AF Mann, T TI Secret knowledge: Rediscovering the techniques of the old masters SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Mann, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 2002 VL 42 IS 1-2 BP 34 EP 37 PG 4 WC Art SC Art GA 753LR UT WOS:000187233300004 ER PT J AU Rappole, JH Jones, P AF Rappole, JH Jones, P TI Evolution of old and new world migration systems SO ARDEA LA English DT Article; Proceedings Paper CT 3rd Conference of the European-Ornithologists-Union CY AUG 22-26, 2001 CL UNIV GRONINGEN, GRONINGEN, NETHERLANDS SP European Ornithologists Union HO UNIV GRONINGEN DE migratory bird evolution; Old World migration systems; New World migration systems ID BIRD MIGRATION; MIGRANTS; WARBLERS; AFRICA; PASSERINES; STRATEGIES; TEMPERATE; HABITS; PANAMA; FOREST AB The apparent nomadism of Palearctic migrant birds during the wintering period in Afrotropical savannah resulted in their characterisation as wandering interlopers, subordinate to Tropical residents, forced to subsist on temporary resource concentrations in marginal habitats. These ideas persist, and, indeed, provide the theoretical basis for many modern studies of migrant evolution. However, recent studies have established that migrant ecology is more complex, with many migrants using stable resources and demonstrating site fidelity to a broad range of Tropical habitats, both within and between wintering seasons. Furthermore, intra-Tropical movements are now known to occur in a number of Tropical resident species as well as migrants, and appear related to resource and habitat seasonality. These findings, plus extensive taxonomic evidence, indicate that most long-distance migrants to temperate and boreal breeding sites are derived from Tropical-breeding resident birds, emphasising the critical importance of taking into account selective factors and evolution occurring during the non-breeding portion of the life cycle. The three principal Holarctic migration systems are similar in these and many other aspects, but differ in that, while roughly one third of the Nearctic/Neotropical and eastern Palearctic/Asian Tropical migrants winter in forest, almost none of European/Afrotropical migrants do so. We propose that habitats connecting Holarctic and Tropical regions serve as a filter for potential migrants to the Holarctic, and that absence of forest from northern Africa has limited exploitation of European forests by Afrotropical species. C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Edinburgh, Inst Cell Anim & Populat Biol, Edinburgh EH9 3JT, Midlothian, Scotland. RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM jrappole@crc.si.edu NR 74 TC 28 Z9 29 U1 3 U2 22 PU NEDERLANDSE ORNITHOLOGISCHE UNIE PI ZEIST PA C/O PAUL STARMANS, OUDE ARNHEMSEWEG 261, 3705 BD ZEIST, NETHERLANDS SN 0373-2266 EI 2213-1175 J9 ARDEA JI Ardea PY 2002 VL 90 IS 3 SI SI BP 525 EP 537 PG 13 WC Ornithology SC Zoology GA 699UA UT WOS:000184073300016 ER PT S AU Kurtz, MJ Eichhorn, G Accomazzi, A Grant, CS Murray, SS AF Kurtz, MJ Eichhorn, G Accomazzi, A Grant, CS Murray, SS BE Starck, JL Murtagh, FD TI Second order bibliometric operators in the astrophysics data system SO ASTRONOMICAL DATA ANALYSIS II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Astronomical Data Analysis II CY AUG 27-28, 2002 CL WAIKOLOA, HI SP SPIE, Int Commiss Opt, Amer Astron Soc, European SO Observ, Int Astron Union DE NASA ADS; information retrieval; bibliometrics; data analysis AB Second order relational operators are functions which take lists which have been generated by a database query, and from those lists form sets of other lists, which can then be merged and sorted on the basis of one or more of the attributes of the items in the lists. The NASA Astrophysics Data System is unique among bibliometric information retrieval systems in the degree to which users are permitted to make use of these concepts. Given a knowledge of how the second order operators work, ADS users can create complex logical algebras which facilitate the discovery of very highly specific information. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurtz, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009; OI Eichhorn, Guenther/0000-0002-3032-1978; Kurtz, Michael/0000-0002-6949-0090; Accomazzi, Alberto/0000-0002-4110-3511 NR 6 TC 7 Z9 7 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4626-2 J9 P SOC PHOTO-OPT INS PY 2002 VL 4847 BP 238 EP 245 DI 10.1117/12.460438 PG 8 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications; Optics; Imaging Science & Photographic Technology; Spectroscopy SC Astronomy & Astrophysics; Computer Science; Optics; Imaging Science & Photographic Technology; Spectroscopy GA BW03E UT WOS:000180673000022 ER PT B AU Rots, AH AF Rots, AH BE Bohlender, DA Durand, D Handley, TH TI TEBC: A multi-mission time, ephemeris, and Barycenter correction package SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB TEBC is provided as a, service to missions and observatories that all have to deal with issues of time and space. Written in ANSI C, TEBC has five main components/tools to: perform conversions between various time scales (TT, TAI, ET, UTC, TDB), generate solar system ephemerides in FITS format; compute barycenter corrections; perform phase-binning of pulsar observations; calculate absolute phase for pulsars. In addition, there is a related, though separate, C++ library that provides time-related classes with an extensive repertoire of time transformation methods. The TEBC package is based on a FITS-ified version of the JPL DE200 and DE405 solar system ephemerides and includes the code to convert the original JPL files to this format. It was originally written to provide a high-precision barycenter tool for the RXTE mission, but support for Chandra has been included, other missions can easily be added, and the functionality of the package has been extended. C1 Harvard Smithsonian Ctr Astrophys, CXC, Cambridge, MA 02138 USA. RP Rots, AH (reprint author), Harvard Smithsonian Ctr Astrophys, CXC, 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 BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 54 EP 57 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700010 ER PT B AU Cameron, RA Morris, DC Virani, SN Wolk, SJ Blackwell, WC Minow, JI O'Dell, SL AF Cameron, RA Morris, DC Virani, SN Wolk, SJ Blackwell, WC Minow, JI O'Dell, SL BE Bohlender, DA Durand, D Handley, TH TI Shelter from the storm: Protecting the Chandra X-ray Observatory from radiation SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB NASA's Chandra X-ray Observatory was launched in July 1999, and the first images were recorded by the ACTS x-ray detector in August 1999. Shortly after first light, degradation of the energy resolution and charge transfer efficiency in the ACTS CCD detectors was observed., and this was quickly attributed to cumulative particle radiation damage in the CCD's, in particular from 100 keV to 200 keV protons. Since the onset of this radiation damage to ACTS, several improvements have been made to autonomous Chandra operation and ground-based operations and mission planning, to limit the effects of radiation while preserving optimum observing efficiency for the Observatory. These changes include implementing an automatic science instrument radiation protection system on Chandra, implementing a real-time radiation monitoring and alert system by the Science Operations Team, and improving the radiation prediction models used in mission planning for the Observatory. These satellite- and ground-based systems provide protection for Chandra from passages through the Earth's trapped radiation belts and outer magnetosphere and from flares and coronal mass ejections from the Sun. We describe the design and performance of the automatic on-board radiation protection system on Chandra, and the ground-based software systems and data products for real-time radiation monitoring. We also describe the development and characterize the performance of the Chandra Radiation Model (CRM), which provides predictions of the solar wind and magnetospheric proton fluxes along Chandra's orbit, indexed by the geomagnetic activity index, Kp. We compare the observed and predicted damage rates to ACTS based on net mission proton fluence, and outline planned enhancements to the CRM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cameron, RA (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 BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 132 EP 135 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700027 ER PT B AU Mink, DJ AF Mink, DJ BE Bohlender, DA Durand, D Handley, TH TI WCSTools 3.0: More tools for image astrometry and catalog searching SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB For five years, WCSTools has provided image astrometry for astronomers who need accurate positions for objects they wish to observe. Other functions have been added and improved since the package was first released. Support has been added for new catalogs, such as the GSC-ACT, 2MASS Point Source Catalog, and GSC II, as they have been published. A simple command line interface can search any supported catalog, returning information in several standard formats, whether the catalog is on a local disk or searchable over the World Wide Web. The catalog searching routine can be located on either end (or both ends!) of such a web connection, and the output from one catalog search can be used as the input to another search. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mink, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 48 Z9 49 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 169 EP 172 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700036 ER PT B AU Wolk, NRA Noble, MS Doe, SM AF Wolk, NRA Noble, MS Doe, SM BE Bohlender, DA Durand, D Handley, TH TI Advances in Chandra Data Analysis SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB With the December 2000 release of the Chandra Data Analysis System (CIAO), the interpreted programming language S-Lang was embedded into the system. This change ushered in a, new phase of analysis within CIAO. S-Lang has increased the data reduction capability of CIAO applications and has provided a method for scientists and developers to quickly create new packages for specific analysis problems. In this paper, we present a brief review of the CIAO applications ChIPS and Sherpa, and then discuss the recent advances in interactive analysis. The focus is on the S-Lang language and the benefits of this integration. We present a series of examples that demonstrate the power and flexibility of CIAO. Finally, we discuss plan for future enhancements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolk, NRA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 282 EP 285 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700059 ER PT B AU Wolk, SJ Cresitello-Dittmar, M Estes, A Overbeck, R Petreshock, J Rots, A Spitzbart, B Zografou, P AF Wolk, SJ Cresitello-Dittmar, M Estes, A Overbeck, R Petreshock, J Rots, A Spitzbart, B Zografou, P BE Bohlender, DA Durand, D Handley, TH TI The monitoring and trends databases for the Chandra X-ray observatory SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB One of the requirements of the Chandra mission is to be able to quickly examine spacecraft data which span the full ten year planned mission lifetime. It was clear from the outset that warehoused FITS files would not meet this requirement. We opted to create a set of databases which resample all engineering telemetry into a fixed five minute time grid. This allows a year's worth of data to be compressed to the scale of about 10 GB. Bi-level data were written into special databases which only report when bi-levels change. This not only results in space savings, but allows for very rapid responses to queries which are concerned with system settings. Currently we can access one year's worth of data across several tables in under 15 minutes. We discuss the design of the databases, the status of testing and implementation. Finally, we discuss ongoing database development and plans for handling image and source data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 341 EP 345 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700073 ER PT B AU Wang, Z Patten, BM Ashby, MLN Zhang, YF Plume, R AF Wang, Z Patten, BM Ashby, MLN Zhang, YF Plume, R BE Bohlender, DA Durand, D Handley, TH TI Real-mission operations of the SWAS science data pipeline SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB SWAS, the Submillimeter Wave Astronomy Satellite mission, has been in successful flight operations with a high observing efficiency (> 80%) since January 1999. Its daily data reduction pipeline, created by integrating parts of existing software tools and building from scratch a set of special-purpose codes, systematically monitors, calibrates, and archives the continuous data stream from the satellite. It, has proven to be a reliable, flexible, and efficient system in support of the mission's active scientific programs. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Wang, Z (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 359 EP 362 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700077 ER PT B AU Eichhorn, G Kurtz, MJ AF Eichhorn, G Kurtz, MJ BE Bohlender, DA Durand, D Handley, TH TI From Urania to the Astronomical Virtual Observatory (AVO) SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB The astronomical community in the last decade has built a system of interlinked data centers that is unique among the sciences. This system has been called Urania. It is composed of the closely integrated operations of the ADS, CDS, NED, the Data and Archive Centers, and the Journals. It began functioning in 1993 with the ability to make joint queries to the ADS and the SIMBAD database at the CDS. It now provides the user with a tightly integrated web of information links. We believe that the continuous expansion and strengthening of the indexing centers in Urania (ADS, CDS, NED) along with similar indexing efforts at the data and archive centers will be a key requirement for the success of the transition from the current system to a fully integrated AVO. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eichhorn, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-83, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 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 BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 441 EP 444 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700093 ER PT B AU Overbeck, RS Wolk, SJ Cresitello-Dittmar, M Petreshock, JG Spitzbart, B AF Overbeck, RS Wolk, SJ Cresitello-Dittmar, M Petreshock, JG Spitzbart, B BE Bohlender, DA Durand, D Handley, TH TI DataSeeker: A Web interface to Chandra M&TA data SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB Chandra's Monitoring and Trends Analysis (M&TA) team utilizes a series of database tables to store binned information about spacecraft configuration and condition over the life of the mission. The DATASEEKER was developed as an efficient means to specify a particular set of this data and have it conveniently downloaded in a usable format. In Chandra's brief operational life of a little over two years in orbit, there are already well over 10 GB of data stored in approximately 50 relational database tables for the Science Operation Team to sift through. DATASEEKER has made it possible to discriminately pull out small subsets of these data in a matter of minutes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Overbeck, RS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 449 EP 452 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700095 ER PT B AU Rey-Bakaikoa, V Accomazzi, A Eichhorn, G Grant, CS AF Rey-Bakaikoa, V Accomazzi, A Eichhorn, G Grant, CS BE Bohlender, DA Durand, D Handley, TH TI Managing the ADS citation database SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Annual Conference for Astronomical Data Analysis Software and Systems CY SEP 30-OCT 03, 2001 CL VICTORIA, CANADA SP Natl Res Council Canada, CADC, NCSA, Natl Radio Astron Observ, Canadian France Hawaii Telescope Corp, Natl Sci Fdn, NASA, Natl Opt Astron Observ, IPAC, Space Telescope Sci Inst AB The NASA Astrophysics Data System (ADS) has become the standard tool for searching the literature in the astronomy and astrophysics community. Within the ADS we are now consolidating the article reference catalog. Reference sources come in a variety of data formats. OCR'ed scanned articles (HTML, LATEX, XML...) from a large number of different publications. We present in this paper new developments allowing the automation of the reference digester through a set of highly configurable, object-oriented, Python/XML applications and tools. We expect the use of these tools to ease the burden of incorporating new publications to the reference databases. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rey-Bakaikoa, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-124-9 J9 ASTR SOC P PY 2002 VL 281 BP 471 EP 474 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW17P UT WOS:000181074700100 ER PT J AU Winn, JN Morgan, ND Hewitt, JN Kochanek, CS Lovell, JEJ Patnaik, AR Pindor, B Schechter, PL Schommer, RA AF Winn, JN Morgan, ND Hewitt, JN Kochanek, CS Lovell, JEJ Patnaik, AR Pindor, B Schechter, PL Schommer, RA TI PMN J1632-0033: A new gravitationally lensed quasar SO ASTRONOMICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (J1632-0033) ID EARLY-TYPE GALAXIES; MODELS; IMAGE AB We report the discovery of a gravitationally lensed quasar resulting from our survey for lenses in the southern sky. Radio images of J1632-0033 with the Very Large Array and the Australia Telescope Compact Array exhibit two compact, flat-spectrum components with separation 1."47 and flux density ratio 13.2. Images with the Hubble Space Telescope reveal the optical counterparts to the radio components and also the lens galaxy. An optical spectrum of the bright component obtained with the first Magellan telescope reveals quasar emission lines at redshift 3.42. Deeper radio images with the Multi-Element Radio Linked Interferometry Network and the Very Long Baseline Array reveal a faint third radio component located near the center of the lens galaxy, which is either a third image of the background quasar or faint emission from the lens galaxy. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Princeton Univ Observ, Princeton, NJ 08544 USA. Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile. RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. NR 34 TC 35 Z9 35 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 JAN PY 2002 VL 123 IS 1 BP 10 EP 19 DI 10.1086/338094 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EJ UT WOS:000173767400002 ER PT J AU Koranyi, DM Geller, MJ AF Koranyi, DM Geller, MJ TI Kinematics of AWM and MKW poor clusters SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : distances and redshifts; galaxies : kinematics and dynamics ID X-RAY-EMISSION; CD GALAXIES; VELOCITY DISPERSIONS; BOUND POPULATIONS; RICH CLUSTERS; INTRACLUSTER MEDIUM; DOMINANT GALAXIES; COMPLETE SAMPLE; MASS PROFILE; REDSHIFTS AB We have measured 1365 redshifts to a limiting magnitude of R similar to 15.5 in 15 AWM/MKW clusters and have collected another 203 from the literature in MKW 4s, MKW 2, and MKW 2s. In AWM 7 we have extended the redshift sample to R similar to 18 in the cluster center. We have identified 704 cluster members in 17 clusters; 201 are newly identified. We summarize the kinematics and distributions of the cluster galaxies and provide an initial discussion of substructure, mass and luminosity segregation, spectral segregation, velocity-dispersion proles, and the relation of the central galaxy to global cluster properties. We compute optical mass estimates, which we compare with X-ray mass determinations from the literature. The clusters are in a variety of dynamical states, reflected in the three classes of behavior of the velocity-dispersion pro le in the core: rising, falling, or flat/ambiguous. The velocity dispersion of the emission-line galaxy population significantly exceeds that of the absorption-line galaxies in almost all of the clusters, and the presence of emission-line galaxies at small projected radii suggests continuing infall of galaxies onto the clusters. The presence of a cD galaxy does not constrain the global cluster properties; these clusters are similar to other poor clusters that contain no cD. We use the similarity of the velocity-dispersion profiles at small radii and the cD-like galaxies internal velocity dispersions to argue that cD formation is a local phenomenon. Our sample establishes an empirical observational baseline of poor clusters for comparison with simulations of similar systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Koranyi, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkoranyi@cfa.harvard.edu; mgeller@cfa.harvard.edu NR 69 TC 24 Z9 25 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 JAN PY 2002 VL 123 IS 1 BP 100 EP 124 DI 10.1086/338096 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 520EJ UT WOS:000173767400008 ER PT B AU Matsushita, S Matsuo, H AF Matsushita, S Matsuo, H BE Vernin, J Benkhaldoun, Z MunozTunon, C TI Relation between 183 GHz water vapor line and water continuum absorption measured with FTS SO ASTRONOMICAL SITE EVALUATION IN THE VISIBLE AND RADIO RANGE SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Astronomical Site Evaluation in the Visible and Radio Range Workshop CY NOV 13-17, 2000 CL MARRAKECH, MOROCCO SP Int Astron Union, Int Radio Sci Union ID PAMPA-LA-BOLA; WAVE ATMOSPHERIC OPACITY; MAUNA-KEA; SUBMILLIMETER; TRANSMISSION; MODEL AB We have carried out Fourier Transform Spectrometer (FTS) measurements of the millimeter and submillimeter-wave (100-1500 GHz or 3 mm - 200 mum) atmospheric opacity at Pampa la Bola, 4800 m above sea level in northern Chile on September 1997 and June 1998. Correlations between 220 GHz opacities and those of the center of submillimeter-wave windows were obtained using the entire data set, and good correlations were obtained except for the periods affected by the liquid water opacity component. We succeeded to separate the total opacity to water vapor and liquid water opacity components. The separated water vapor opacity component shows good correlation with the 183 GHz pure water vapor line opacity, which is also covered in the measured spectra, but the liquid water opacity component shows no correlation. Since the submillimeter-wave opacity is merely affected by the liquid water component, it may be better to use the submillimeter-wave opacity for the phase correction. C1 Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96721 USA. RP Matsushita, S (reprint author), Harvard Smithsonian Ctr Astrophys, Submillimeter Array, POB 824, Hilo, HI 96721 USA. NR 16 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-106-0 J9 ASTR SOC P PY 2002 VL 266 BP 180 EP 187 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV22Y UT WOS:000178271800022 ER PT B AU Wiedner, M Hills, R Pardo-Carrion, J AF Wiedner, M Hills, R Pardo-Carrion, J BE Vernin, J Benkhaldoun, Z MunozTunon, C TI 183 GHz water vapor monitors SO ASTRONOMICAL SITE EVALUATION IN THE VISIBLE AND RADIO RANGE SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Astronomical Site Evaluation in the Visible and Radio Range Workshop CY NOV 13-17, 2000 CL MARRAKECH, MOROCCO SP Int Astron Union, Int Radio Sci Union AB Water vapor monitors (WVM) operating at 183 GHz have been built and used for phase correction of observations taken at 0.85 mm. We present Allan variances, find the optimal smoothing method and compare the WVM data to Fourier Transform Spectrometer data. Phase correction with these radiometers reduces the phase fluctuations significantly to about 140 mum rms. Phase correction using a theoretical conversion factor from brightness temperature to phase is as successful as choosing the optimal conversion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wiedner, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Ms78, Cambridge, MA 02138 USA. NR 6 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-106-0 J9 ASTR SOC P PY 2002 VL 266 BP 278 EP 286 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV22Y UT WOS:000178271800034 ER PT J AU Hussain, GAJ AF Hussain, GAJ TI Starspot lifetimes SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE stars : activity; stars : spots; techniques : spectroscopic; techniques : photometric ID ACTIVE LONGITUDES; ACTIVITY CYCLE; MAIN-SEQUENCE; BINARY STARS; HK LACERTAE; COOL STARS; PHOTOMETRY; SPOT; V471-TAU; TAURI AB Photometry and Doppler imaging are both powerful techniques that can be used to evaluate the timescales of surface activity phenomena on active rapidly rotating objects. Active longitudes are most easily detected through photometry. These are found to have lifetimes of between 4-8 years. Many RSCVn binary systems and single stars show the "flip-flop" effect, where dominant spotted regions switch back and forth by 180degrees longitude over a set number of years. Doppler imaging is most effective at evaluating the presence of polar spots and smaller scale spots in the mid to low latitude regions (up to 3degrees resolution at the equator), This technique enables the monitoring of spot group lifetimes with greater accuracy than with photometry alone. Polar spots are found to have lifetimes of over a decade in RSCVn binary systems (V711 Tau & El Eri) and in single MS stars, (AB Dor), In AB Dor, long-term photometry and Doppler imaging show that when the star was at its most spotted, there was no polar spot. Recent results indicate that surface shear was also suppressed in AB Dor at the same epoch, This implies that spot lifetimes can also be affected by changing surface shear rates over the course of an activity cycle. Mid to low latitude spots on single MS stars are found to have lifetimes of under 1 month. Spots in active components of RSCVn binaries show less modulation over a month compared to single MS rapid rotators. This indicates that either less flux is injected into the stellar surface over one month, or else that flux emergence is confined to small preferred regions in tidally locked systems. More long-term monitoring of these and other rapidly rotating systems using Doppler imaging, photometry and molecular band mapping using TiO and OH will enable us to evaluate whether or not these initial trends are representative of active cool stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, MS-16,60 Garden St, Cambridge, MA 02138 USA. EM ghussain@cfa.harvard.edu NR 37 TC 35 Z9 36 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PY 2002 VL 323 IS 3-4 BP 349 EP 356 DI 10.1002/1521-3994(200208)323:3/4<349::AID-ASNA349>3.0.CO;2-E PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 591DU UT WOS:000177865100033 ER PT J AU Saar, SH Brandenburg, A AF Saar, SH Brandenburg, A TI A new look at dynamo cycle amplitudes SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE stars : magnetic fields; stars : activity; stars : chromospheres ID MAIN-SEQUENCE STARS; SUN-LIKE STARS; MAGNETIC ACTIVITY; TIME EVOLUTION; ROTATION; PERIOD AB We explore the dependence of the amplitude of stellar dynamo cycle variability (as seen in the Mount Wilson Ca II HK timeseries data) on other stellar parameters. We find that the fractional cycle amplitude A(cyc) (i.e. the ratio of the peak-to-peak variation to the average) decreases somewhat with mean activity, increases with decreasing effective temperature, but is not correlated with inverse Rossby number Ro(-1). We find that A(cyc) increases with the ratio of cycle and rotational frequencies omega(cyc)/Omega along two, nearly parallel branches. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NORDITA, DK-2100 Copenhagen O, Denmark. RP Saar, SH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Brandenburg, Axel/I-6668-2013 OI Brandenburg, Axel/0000-0002-7304-021X NR 16 TC 18 Z9 18 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2002 VL 323 IS 3-4 BP 357 EP 360 DI 10.1002/1521-3994(200208)323:3/4<357::AID-ASNA357>3.0.CO;2-I PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 591DU UT WOS:000177865100034 ER PT J AU Andrievsky, SM Kovtyukh, VV Luck, RE Lepine, JRD Bersier, D Maciel, WJ Barbuy, B Klochkova, VG Panchuk, VE Karpischek, RU AF Andrievsky, SM Kovtyukh, VV Luck, RE Lepine, JRD Bersier, D Maciel, WJ Barbuy, B Klochkova, VG Panchuk, VE Karpischek, RU TI Using Cepheids to determine the galactic abundance gradient - I. The solar neighbourhood SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : abundances; stars : supergiants; galaxy : abundances; galaxy : evolution ID B-TYPE STARS; OLD OPEN CLUSTERS; LARGE-MAGELLANIC-CLOUD; BODY BARRED MODELS; RADIAL GAS-FLOWS; CHEMICAL EVOLUTION; MILKY-WAY; PLANETARY-NEBULAE; CLASSICAL CEPHEIDS; SPIRAL STRUCTURE AB A number of studies of abundance gradients in the galactic disk have been performed in recent years. The results obtained are rather disparate: from no detectable gradient to a rather significant slope of about -0.1 dex kpc(-1). The present study concerns the abundance gradient based on the spectroscopic analysis of a sample of classical Cepheids. These stars enable one to obtain reliable abundances of a variety of chemical elements. Additionally, they have well determined distances which allow an accurate determination of abundance distributions in the galactic disc. Using 236 high resolution spectra of 77 galactic Cepheids, the radial elemental distribution in the galactic disc between galactocentric distances in the range 6-11 kpc has been investigated. Gradients for 25 chemical elements (from carbon to gadolinium) are derived. The following results were obtained in this study. Almost all investigated elements show rather at abundance distributions in the middle part of galactic disc. Typical values for iron-group elements lie within an interval from approximate to -0.02 to approximate to -0.04 dex kpc(-1) (in particular, for iron we obtained d[Fe/H]/dR(G) = 0.029 dex kpc(-1)). Similar gradients were also obtained for O, Mg, Al, Si, and Ca. For sulphur we have found a steeper gradient (-0.05 dex kpc(-1)). For elements from Zr to Gd we obtained (within the error bars) a near to zero gradient value. This result is reported for the first time. Those elements whose abundance is not expected to be altered during the early stellar evolution (e.g. the iron-group elements) show at the solar galactocentric distance [El/H] values which are essentially solar. Therefore, there is no apparent reason to consider our Sun as a metal-rich star. The gradient values obtained in the present study indicate that the radial abundance distribution within 6-11 kpc is quite homogeneous, and this result favors a galactic model including a bar structure which may induce radial flows in the disc, and thus may be responsible for abundance homogenization. C1 Univ Sao Paulo, Inst Astron & Geofis, BR-4200 Sao Paulo, Brazil. Odessa II Mechnikov State Univ, Dept Astron, UA-65014 Odessa, Ukraine. Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. Odessa Astron Observ, Odessa, Ukraine. Isaac Newton Inst Chile, Odessa Branch, Odessa, Ukraine. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Stavropol Terri, Russia. Isaac Newton Inst Chile, SAO RAS Branch, Nizhnii Arkhyz, Russia. Univ Sao Paulo, EdIC Grp, Sao Paulo, Brazil. RP Andrievsky, SM (reprint author), Univ Sao Paulo, Inst Astron & Geofis, Av Miguel Stefano, BR-4200 Sao Paulo, Brazil. NR 92 TC 141 Z9 145 U1 0 U2 4 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2002 VL 381 IS 1 BP 32 EP 50 DI 10.1051/0004-6361:20011488 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 503GQ UT WOS:000172791100014 ER PT J AU Li, LX AF Li, LX TI Jet collimation by small-scale magnetic fields SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; magnetic fields; MHD; stars : winds, outflows ID ACCRETION-EJECTION STRUCTURES; DOUBLE RADIO-SOURCES; MASSIVE BLACK-HOLE; EXTRAGALACTIC JETS; DRIVEN JETS; IONIZED-GAS; DISKS; MODEL; INSTABILITY; ELECTRODYNAMICS AB A popular model for jet collimation is associated with the presence of a large-scale and predominantly toroidal magnetic field originating from the central engine (a star, a black hole, or an accretion disk). Besides the problem of how such a large-scale magnetic field is generated, in this model the jet suffers from the fatal long-wave mode kink magnetohydrodynamic instability. In this paper we explore an alternative model: jet collimation by small-scale magnetic fields. These magnetic fields are assumed to be local, chaotic, and tangled, but are dominated by toroidal components. Just as in the case of a large-scale toroidal magnetic field, we show that the "hoop stress" of the tangled toroidal magnetic fields exerts an inward force which confines and collimates the jet. The magnetic "hoop stress" is balanced either by the gas pressure of the jet or by centrifugal force if the jet is spinning. Since the length scale of the magnetic field is small (< the cross-sectional radius of the jet << the length of the jet), in this model the jet does not suffer from the long-wave mode kink instability. Many other problems associated with the large-scale magnetic field are also eliminated or alleviated for small-scale magnetic fields. Though it remains an open question how to generate and maintain the required small-scale magnetic fields in a jet, the scenario of jet collimation by small-scale magnetic fields is favored by the current study on disk dynamo which indicates that small-scale magnetic fields are much easier to generate than large-scale magnetic fields. C1 Princeton Univ Observ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Princeton Univ Observ, Peyton Hall, Princeton, NJ 08544 USA. EM lli@cfa.harvard.edu NR 61 TC 15 Z9 15 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2002 VL 564 IS 1 BP 108 EP 112 DI 10.1086/324135 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509NR UT WOS:000173154300012 ER PT J AU Slane, P Smith, RK Hughes, JP Petre, R AF Slane, P Smith, RK Hughes, JP Petre, R TI An X-ray study of the supernova remnant G290.1-0.8 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G290.1-0.8, MSH 11-61A); supernova remnants; X-rays : ISM ID FORMED DENSE SHELL; INTERSTELLAR-MEDIUM; THERMAL CONDUCTION; MODELING W44; HOT INTERIOR; EMISSION; CLOUDS; GRADIENT; YOUNG; RADIO AB G290.1-0.8 (MSH 11-61A) is a supernova remnant (SNR) whose X-ray morphology is centrally bright. However, unlike the class of X-ray composite SNRs whose centers are dominated by nonthermal emission presumably driven by a central pulsar, we show that the X-ray emission from G290.1-0.8 is thermal in nature, placing the remnant in an emerging class which includes such remnants as W44, W28, 3C391, and others. The evolutionary sequence which leads to such X-ray properties is not well understood. Here we investigate two scenarios for such emission : evolution in a cloudy interstellar medium, and early-stage evolution of a remnant into the radiative phase, including the effects of thermal conduction. We construct models for these scenarios in an attempt to reproduce the observed center-filled X-ray properties of G290.1-0.8, and we derive the associated age, energy, and ambient density conditions implied by the models. We find that for reasonable values of the explosion energy, the remnant age is of order (1-2) x 10(4) yr. This places a fairly strong constraint on any association between G290.1-0.8 and PSR J1105-610, which would require an anomalously large velocity for the pulsar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. NASA, GSFC, Greenbelt, MD USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 36 TC 30 Z9 30 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2002 VL 564 IS 1 BP 284 EP 290 DI 10.1086/324155 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509NR UT WOS:000173154300028 ER PT J AU Curiel, S Trinidad, MA Canto, J Rodriguez, LF Torrelles, JM Ho, PTP Patel, NA Greenhill, L Gomez, JF Garay, G Hernandez, L Contreras, ME Anglada, G AF Curiel, S Trinidad, MA Canto, J Rodriguez, LF Torrelles, JM Ho, PTP Patel, NA Greenhill, L Gomez, JF Garay, G Hernandez, L Contreras, ME Anglada, G TI Detection of a candidate for the exciting source of the expanding water maser bubble in Cepheus A SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Cepheus A); ISM : jets and outflows; radio continuum : ISM; stars : formation ID THERMAL RADIO JET; A HW2 AB We report sensitive, high angular resolution VLA 3.6 cm and 7 mm continuum observations toward the star-forming region Cepheus A. Three embedded young stellar objects (YSOs) were found within a projected area of similar or equal to 0".6 x 0".6 (400x400 AU(2)). One of the sources is the already known radio continuum jet HW2 (detected at 3.6 cm and 7 mm), while the other two weak sources were not previously known. One of these two new sources is detected only at 7 mm and is located similar or equal to0".15 south from HW2. The other source, detected only at 3.6 cm, is located 0".6 south from HW2 and nearly coincides with the center of the enigmatic expanding bubble of water masers recently detected with the Very Long Baseline Array. We suggest that this radio continuum source is the embedded YSO powering the water maser structure, but its nature is still unknown at present. We also discuss possible scenarios that could explain the surprisingly precise spherical geometry of the water maser bubble. C1 Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. CSIC, Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain. CSIC, Inst Ciencias Espacio, E-08034 Barcelona, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lab Astrofis Espacial & Fis Fundamental INTA, E-28080 Madrid, Spain. Univ Chile, Dept Astron, Santiago, Chile. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. RP Curiel, S (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. RI Garay, Guido/H-8840-2013; Gomez, Jose Francisco/D-8392-2016; OI Garay, Guido/0000-0003-1649-7958; Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 12 TC 25 Z9 25 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2002 VL 564 IS 1 BP L35 EP L38 DI 10.1086/338844 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509NT UT WOS:000173154400009 ER PT J AU Edmonds, PD Heinke, CO Grindlay, JE Gilliland, RL AF Edmonds, PD Heinke, CO Grindlay, JE Gilliland, RL TI Hubble Space Telescope detection of a quiescent low-mass X-ray binary companion in 47 Tucanae SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; globular clusters : individual (47 Tucanae); techniques : photometric; X-rays : binaries ID GLOBULAR-CLUSTERS; CALIBRATION; 47-TUCANAE; MODELS AB We present the results of a search for optical counterparts to the two quiescent low-mass X-ray binaries (X5 and X7) in the globular cluster 47 Tucanae, using high-quality Chandra and Hubble Space Telescope images. A faint blue (V=21.7; U-V=0.9) star within 0".03 of the eclipsing system X5 shows variability on both short and long timescales and is the counterpart of the X-ray source. The colors and variability of this object are consistent with the combination of light from an accretion disk and a red main-sequence star (possibly somewhat larger than a normal main-sequence star with similar luminosity). No evidence is found for a star showing either variability or unusual colors near the position of X7, but a probable chance superposition of a star with V=20.25 limits the depth of our search. 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 23 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 JAN 1 PY 2002 VL 564 IS 1 BP L17 EP L20 DI 10.1086/338776 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509NT UT WOS:000173154400005 ER PT J AU Park, S Roming, PWA Hughes, JP Slane, PO Burrows, DN Garmire, GP Nousek, JA AF Park, S Roming, PWA Hughes, JP Slane, PO Burrows, DN Garmire, GP Nousek, JA TI The structure of the oxygen-rich supernova remnant G292.0+1.8 from Chandra X-ray images: Shocked ejecta and circumstellar medium SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : individual (G292.0+1.8); supernova remnants; X-rays : ISM ID NOVA REMNANT; VRO 42.05.01; EVOLUTION; YOUNG AB We present results from the observation of the young Galactic supernova remnant (SNR) G292.0+1.8 with the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. In the 0.3-8 keV band, the high-resolution ACIS images reveal a complex morphology consisting of knots and filaments as well as the blast wave around the periphery of the SNR. We present equivalent width (EW) maps for the elemental species O, Ne, Mg, and Si, which allow us to identify regions of enhanced metallicity in the SNR. G292.0+1.8 is bright in O, Ne, and Si and weaker in S and Ar, with little Fe. The EW and broadband images indicate that the metal-rich ejecta are distributed primarily around the periphery of the SNR. The central beltlike structure has a normal solar-type composition, strongly suggesting that it is primarily emission from a shocked circumstellar medium rather than metal-rich ejecta. We propose that the belt traces its origin to enhanced mass loss in the star's equatorial plane during the slow, red supergiant phase. We also identify thin filaments with normal composition, centered on and extending nearly continuously around the outer boundary of the SNR. These may originate in a shell caused by the stellar winds from the massive progenitor in the red/blue supergiant phases, overrun by the blast wave. C1 Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Park, S (reprint author), Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. NR 28 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 JAN 1 PY 2002 VL 564 IS 1 BP L39 EP L43 DI 10.1086/338861 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 509NT UT WOS:000173154400010 ER PT J AU Hanson, MM Luhman, KL Rieke, GH AF Hanson, MM Luhman, KL Rieke, GH TI A near-infrared survey of radio-selected ultracompact HII regions SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE HII regions; infrared : ISM; ISM : lines and bands; ISM : molecules; stars : evolution; stars : formation ID H-II-REGIONS; HIGH-SPATIAL-RESOLUTION; YOUNG STELLAR OBJECTS; STAR-FORMING REGION; MOLECULAR CLOUD; CONTINUUM EMISSION; REFLECTION NEBULA; UBVRI-PHOTOMETRY; GASEOUS NEBULAE; HYDROGENIC IONS AB A near-infrared (NIR) survey of 63 radio-selected, ultracompact (UC) H II regions representing 47 different star-forming sites has been completed. The survey was obtained using H-band imaging and moderate-resolution, R = 1200, K-band spectroscopy, centered on the radio emission peak of the UC H II regions. The goal of this survey was to determine the fraction of radio-selected UC H II regions that can be studied with NIR observations and analysis. Approximately 50% of the 63 radio-selected UC H II regions appear to be detected at NIR wavelengths in Brgamma emission (10(7) ergs s(-1) cm(-2) sr(-1)). Typical line-of-sight extinction toward the detected UC H II regions ranged from A(V) = 30 to 50, though one source was measured to have A(V) = 80. For a few of these UC H II regions, the central ionizing sources are detected through high signal-to-noise ratio NIR spectra of photospheric transitions. This preliminary survey suggests that perhaps 5%-10% of UC H II regions showing NIR counterparts will have directly detectable central ionizing sources. Using the ratio of He I 2.11 to Brgamma, the effective temperatures of the central ionizing stars in 25 UC H II regions have been estimated. While He I is not always detected in UC H II regions, when it was found or a meaningful upper limit determined, the spectral type implied by the ratio of He I 2.11 to Brgamma closely matched similar estimates of spectral type derived from radio. Model predictions based on mid-infrared measurements appear to underestimate the temperature of the central ionizing stars for which we have directly detected spectral types. The line ratios of H(2) 2-1 S(1) and 1-0 S(0) relative to the 1-0 S(1) line in our sample of UC H II regions are generally indicative of dense photodissociation regions rather than shocks, similar to what is seen in the Orion Bar. This was true even for UC H II regions showing very weak Brgamma emission. While Brgamma was generally found to be spatially correlated with the radio emission, showed little correlation with the UC H II regions, typically lying H 2 greater than or similar to10" from the central radio emission. A discussion of each UC H II region studied is included in an extensive appendix. C1 Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Hanson, MM (reprint author), Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. EM hanson@physics.uc.edu; kluhman@cfa.harvard.edu; grieke@as.arizona.edu NR 98 TC 64 Z9 65 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 JAN PY 2002 VL 138 IS 1 BP 35 EP 61 DI 10.1086/324073 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QT UT WOS:000173507500003 ER PT J AU Freeman, PE Kashyap, V Rosner, R Lamb, DQ AF Freeman, PE Kashyap, V Rosner, R Lamb, DQ TI A wavelet-based algorithm for the spatial analysis of Poisson data SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE methods : data analysis; techniques : image processing; X-rays : general ID X-RAY SOURCES; COUNTING DETECTOR IMAGES; ROSAT DEEP SURVEY; LOCKMAN FIELD; COMA CLUSTER; GALAXY; TRANSFORMS; PLEIADES; IDENTIFICATION; SEARCH AB Wavelets are scalable, oscillatory functions that deviate from zero only within a limited spatial regime and have average value zero, and thus may be used to simultaneously characterize the shape, location, and strength of astronomical sources. But in addition to their use as source characterizers, wavelet functions are rapidly gaining currency within the source detection field. Wavelet-based source detection involves the correlation of scaled wavelet functions with binned, two-dimensional image data. If the chosen wavelet function exhibits the property of vanishing moments, significantly nonzero correlation coefficients will be observed only where there are high-order variations in the data; e.g., they will be observed in the vicinity of sources. Source pixels are identified by comparing each correlation coefficient with its probability sampling distribution, which is a function of the (estimated or a priori known) background amplitude. In this paper, we describe the mission-independent, wavelet-based source detection algorithm "WAVDETECT," part of the freely available Chandra Interactive Analysis of Observations (CIAO) software package. Our algorithm uses the Marr, or "Mexican Hat" wavelet function, but may be adapted for use with other wavelet functions. Aspects of our algorithm include : (1) the computation of local, exposure-corrected normalized (i.e., flat-fielded) background maps; (2) the correction for exposure variations within the field of view (due to, e.g., telescope support ribs or the edge of the field); (3) its applicability within the low-counts regime, as it does not require a minimum number of background counts per pixel for the accurate computation of source detection thresholds; (4) the generation of a source list in a manner that does not depend upon a detailed knowledge of the point spread function (PSF) shape; and (5) error analysis. These features make our algorithm considerably more general than previous methods developed for the analysis of X-ray image data, especially in the low count regime. We demonstrate the robustness of WAVDETECT by applying it to an image from an idealized detector with a spatially invariant Gaussian PSF and an exposure map similar to that of the Einstein IPC; to Pleiades Cluster data collected by the ROSAT PSPC; and to simulated Chandra ACIS-I image of the Lockman Hole region. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Freeman, PE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 46 TC 389 Z9 390 U1 1 U2 12 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 JAN PY 2002 VL 138 IS 1 BP 185 EP 218 DI 10.1086/324017 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 515QT UT WOS:000173507500009 ER PT S AU Gaensler, BM Dickey, JM McClure-Griffiths, NM Bizunok, NS Green, AJ AF Gaensler, BM Dickey, JM McClure-Griffiths, NM Bizunok, NS Green, AJ BE Cecchini, S Cortiglioni, S Sault, R Sbarra, C TI High resolution polarimetry of the inner Galaxy SO ASTROPHYSICAL POLARIZED BACKGROUNDS SE AIP Conference Proceedings LA English DT Proceedings Paper CT Workshop on Astrophysical Polarized Backgrounds CY OCT 09-12, 2001 CL BOLOGNA, ITALY ID SOUTHERN GALACTIC PLANE; POLARIZATION; EMISSION; ABSORPTION; SCALE; GHZ AB We resent our results from the South Galactic Plane Survey, an effort to map the fourth quadrant of the Milky Way in linear polarization at a frequency of 1.4 GHz and at a resolution of 1-2 arcmin. These data scale structure of magneto-ionic gas, and have revealed a are a powerful probe of both the turbulence and large-scale structure of magneto-ionic gas, and have revealed a variety of new features in the interstellar medium. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013 NR 16 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0055-5 J9 AIP CONF PROC PY 2002 VL 609 BP 20 EP 25 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25W UT WOS:000175483200004 ER PT S AU Shinnaga, H Tsuboi, M Kasuga, T AF Shinnaga, H Tsuboi, M Kasuga, T BE Cecchini, S Cortiglioni, S Sault, R Sbarra, C TI A millimeter polarimeter for the 45m telescope at Nobeyama SO ASTROPHYSICAL POLARIZED BACKGROUNDS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Workshop on Astrophysical Polarized Backgrounds CY OCT 09-12, 2001 CL BOLOGNA, ITALY ID MASER AB We have designed and constructed a tunable polarimeter system to cover frequencies from 35 GHz to 250 GHz, (8.6 mm and 1.2 mm in wavelength) for the 45m telescope at Nobeyama Radio Observatory (NRO). Both circular and linear polarizations can be measured by the polarimeter. The performance of the polarimeter in astronomical observations was tested by simultaneously measuring the linear polarization of the J = 2 - 1 transition of SiO in the nu=0 and 1 states at 86 GHz toward VY CMa. The design, construction, and tests are presented briefly. C1 Harvard Smithsonian Ctr Astrophys, SAO SMA Project, Hilo, HI 96720 USA. RP Shinnaga, H (reprint author), Harvard Smithsonian Ctr Astrophys, SAO SMA Project, 82 Puuhonu Pl, Hilo, HI 96720 USA. NR 10 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 0-7354-0055-5 J9 AIP CONF PROC PY 2002 VL 609 BP 283 EP 286 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25W UT WOS:000175483200049 ER PT J AU Eichhorn, G Accomazzi, A Grant, CS Kurtz, MJ Murray, SS AF Eichhorn, G Accomazzi, A Grant, CS Kurtz, MJ Murray, SS TI The NASA Astrophysics Data System: Free access to the astronomical literature on-line and through email SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 10th UN/ESA Workshop on Basic Space Science CY JUN 18-21, 2001 CL UNIV MAURITIUS, MAURITIUS SP UN, ESA HO UNIV MAURITIUS ID VOIDS AB The Astrophysics Data System (ADS) provides access to the astronomical literature through the World Wide Web. It is a NASA funded project and access to all the ADS services is free to everybody world-wide. The ADS Abstract Service allows the searching of four databases with abstracts in Astronomy, Instrumentation, Physics/Geophysics, and the LANL Preprints with a total of over 2.2 million references. The system also provides access to reference and citation information, links to on-line data, electronic journal articles, and other on-line information. The ADS Article Service contains the full articles for most of the astronomical literature back to volume 1. It contains the scanned pages of all the major journals (Astrophysical Journal, Astronomical Journal, Astronomy & Astrophysics, Monthly Notices of the Royal Astronomical Society, and Solar Physics), as well as most smaller journals back to volume 1. The ADS can be accessed through any web browser without signup or login. Alternatively an email interface is available that allows our users to execute queries via email and to retrieve scanned articles via email. This might be interesting for users on slow or unreliable links, since the email system will retry sending information automatically until the transfer is complete. There are now 9 mirror sites of the ADS available in different parts of the world to improve access. The ADS is available at: http://ads.harvard.edu. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eichhorn, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009; KURTZ, Michael /B-3890-2009; OI Eichhorn, Guenther/0000-0002-3032-1978; Kurtz, Michael/0000-0002-6949-0090 NR 46 TC 2 Z9 2 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2002 VL 282 IS 1 BP 299 EP 340 DI 10.1023/A:1021179209872 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 617BW UT WOS:000179341200026 ER PT J AU Maraston, C Kissler-Patig, M Brodie, J Barmby, P Huchra, J AF Maraston, C Kissler-Patig, M Brodie, J Barmby, P Huchra, J TI AGB phase transition in globular clusters: A tool for dating starbursts SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 2nd Euroconference on Relevant Basic Building Blocks and Small-scale Processes in Galaxy Evolution CY OCT 16-21, 2001 CL ST DENIS REUNION, FRANCE SP European Commiss, Res DG, Dept Reunion, Conseil Reg Reunion, CNRS, Ctr Natl Etudes Spatiales, Observ Paris Meudon, Dept Astrophys Extragalact & Cosmologie, Comite Tourisme Reunion, France Telecom, Europcar DE AGB stars; star clusters; merger remnants ID NGC-7252 AB A new method to detect and study young star clusters is presented. This is based on the knowledge that the light of stellar populations with ages between similar to 200 Myr and similar to 1/2 Gyr is dominated by very red, bright AGB stars. Star clusters undergoing this so-called `AGB phase transition' are featured by very red V-K colours, like those of Magellanic Clouds clusters, while optical colours like B-V remain blue typical for young populations. The best channel for detecting star clusters in this age range is therefore the near IR. From the theoretical side, SSP models including properly the contribution of the bright AGB are required (Maraston, 1998). Using this strategy, we succesfully detected the AGB phase transition among the clusters of the merger remnant galaxy NGC 7252 (see Maraston et al., 2001). C1 Univ Sternwarte Munchen, Munich, Germany. European So Observ, D-8046 Garching, Germany. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Maraston, C (reprint author), Univ Sternwarte Munchen, Munich, Germany. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 3 TC 1 Z9 1 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2002 VL 281 IS 1-2 BP 137 EP 138 DI 10.1023/A:1019512014958 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 557RG UT WOS:000175921200025 ER PT J AU Abel, T AF Abel, T TI The basic building blocks of galaxies SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 2nd Euroconference on Relevant Basic Building Blocks and Small-scale Processes in Galaxy Evolution CY OCT 16-21, 2001 CL ST DENIS REUNION, FRANCE SP European Commiss, Res DG, Dept Reunion, Conseil Reg Reunion, CNRS, Ctr Natl Etudes Spatiales, Observ Paris Meudon, Dept Astrophys Extragalact & Cosmologie, Comite Tourisme Reunion, France Telecom, Europcar AB Current cold dark matter models of structure formation make a clear prediction for cosmic structures in the Dark Ages. We discuss the formation and nature of the first collapsed and first luminous objects in the universe arising in these theories. The first virialized objects are dark matter halos at the free streaming length which depends on the mass and nature of the assumed weakly interacting massive particle. The first objects that also contain significant fractions of gas have masses of the cosmological Jeans scale similar to 10(4)M(.) at the redshifts of interest (z similar to 30). The first pre-galactic objects that host stars have masses of 10(6) M-.. This mass scale is given by the requirement of a sufficiently high virial temperature to enable the chemical reactions necessary to form molecular hydrogen which subsequently allows the gas to dissipate its gravitational energy and to collapse to form a star. An individual massive star is formed per such object and explodes in a supernova within a few Myrs. All these stages of the formation of the first objects are illustrated by fully resolved three dimensional cosmological hydrodynamic simulations. C1 Penn State Univ, University Pk, PA 16802 USA. RP Abel, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2002 VL 281 IS 1-2 BP 471 EP 473 DI 10.1023/A:1019509211972 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 557RG UT WOS:000175921200111 ER PT S AU Traub, NA Jucks, KW AF Traub, NA Jucks, KW BE Mendillo, M Nagy, A Waite, JH TI A possible aeronomy of extrasolar terrestrial planets SO ATMOSPHERES IN THE SOLAR SYSTEM: COMPARATIVE AERONOMY SE GEOPHYSICAL MONOGRAPH SERIES LA English DT Proceedings Paper CT Yosemite Conference on Comparative Aeronomy in the Solar System CY FEB 08-11, 2000 CL YOSEMITE, CA SP NASA, NSF, SW Res Inst ID NEOPROTEROZOIC SNOWBALL EARTH; EVOLUTION; TRANSMISSION; SIMULATIONS; EMISSION; SEARCHES; CLIMATE; SYSTEM; LIFE AB Terrestrial planetary systems may exist around nearby stars as the Earth-sized counterparts to the many giant planets already discovered within the solar neighborhood. In this chapter we first discuss the numerous techniques which have been suggested to search for extrasolar terrestrial planets. We then focus on the expected results from that technique in which an orbiting telescope or interferometer is used to obtain a visible or infrared spectrum of a planet, without contamination from the parent star. We show examples of such spectra for selected cases: the present Earth. the Neoproterozoic (snowball) Earth, a methane-rich Earth, and the present Mars and Venus. We conclude by discussing the implications of such spectra for the detection of life on an extrasolar terrestrial planet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Traub, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 48 TC 2 Z9 2 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0065-8448 BN 0-87590-989-2 J9 GEOPH MONOG SERIES PY 2002 VL 130 BP 369 EP 380 DI 10.1029/130GM25 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU78Y UT WOS:000177015100025 ER PT S AU Kurucz, RL AF Kurucz, RL BE Schultz, DR Krstic, PS Ownby, F TI Atomic and molecular data needs for astrophysics SO ATOMIC AND MOLECULAR DATA AND THEIR APPLICATIONS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Atomic and Molecular Data and Their Applications CY APR 24-27, 2002 CL GATLINBURG, TN SP US DOE Off Fus Energy Sci, ORNL Controlled Fus Atom Data Ctr, ORNL Phys Div, ORNL Phys Sci Directorate, Int Union Pure & Appl Phys, Natl Inst Stand & Technol, U/Battelle ID TERM SYSTEM; CO-I; SPECTRUM; IODINE C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurucz, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 25 Z9 25 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 0-7354-0091-1 J9 AIP CONF PROC PY 2002 VL 636 BP 134 EP 143 PG 10 WC Astronomy & Astrophysics; Physics, Atomic, Molecular & Chemical SC Astronomy & Astrophysics; Physics GA BV50H UT WOS:000179183500012 ER PT J AU Paredes, R Zavalaga, CB Boness, DJ AF Paredes, R Zavalaga, CB Boness, DJ TI Patterns of egg laying and breeding success in Humboldt Penguins (Spheniscus humboldti) at Punta San Juan, Peru SO AUK LA English DT Article ID 1982-83 EL-NINO; KING PENGUIN; CYCLE AB We analyzed patterns of egg laying and breeding frequency of Humboldt Penguins (Spheniscus hunboldti) between 1993 and 1997 at Punta San Juan, Peru. Egg-laying extended from mid-March to the first week of December, showing two well-defined peaks in April and August-September. The extended breeding period of these birds was the result of individuals having a second clutch. About half of the females (n = 189) had two clutches per year, most of which were double broods (73%). The date of completion and outcome of reproduction, or whether a change of mates occurred from the previous year, did not affect timing of egg laying. The majority of first clutches (62%) were laid in April each year. Two-clutch breeders that started laying eggs early in April had a higher breeding success than those starting in late April, and double brooders had greater success than single brooders. Two-clutch breeders started to lay eggs earlier than single-clutch breeders. Taking into account that a penguin breeding cycle (from egg laying to fledging) lasts similar to4 months, laying eggs early in April increases the chance of rearing two successful broods per year. During three consecutive years, females tended to have two clutches instead of only one clutch and an average breeding success of 4.54 fledglings over 3 years. Having as many clutches as possible when conditions are favorable appears to be a strategy used by Humboldt Penguins to maximize their lifetime reproductive success within a productive but unpredictable environment. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Wildlife Conservat Soc Peru, Lima 17, Peru. RP Boness, DJ (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. NR 37 TC 19 Z9 20 U1 1 U2 9 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JAN PY 2002 VL 119 IS 1 BP 244 EP 250 DI 10.1642/0004-8038(2002)119[0244:POELAB]2.0.CO;2 PG 7 WC Ornithology SC Zoology GA 528ZH UT WOS:000174275200025 ER PT J AU Yavitt, JB Wright, SJ AF Yavitt, JB Wright, SJ TI Charge characteristics of soil in a lowland tropical moist forest in Panama in response to dry-season irrigation SO AUSTRALIAN JOURNAL OF SOIL RESEARCH LA English DT Article DE permanent charge; soil pH; tropical forest soil; variable charge; water regime ID BARRO-COLORADO ISLAND; SATURATED HYDRAULIC CONDUCTIVITY; NINO SOUTHERN-OSCILLATION; VARIABLE-CHARGE; SULFATE ADSORPTION; NUTRIENT DYNAMICS; SURFACE-CHARGE; PH; PRECIPITATION; ALFISOLS AB Although the hot, moist tropics in the Republic of Panama receive more than 2000 mm of rain per year, soils dry considerably during the 4-month dry season. We examined the effect of seasonal drought by irrigating two 2.25-ha plots of lowland tropical moist forest on Barro Colorado Island (BCI) for 5 consecutive dry seasons. Irrigation decreased soil permeability and improved soil nutrient status, which prompted this study of soil charge characteristics in the irrigated and control plots. Soil was an Alfisol, and thus it was not clear a priori whether variable-charge or permanent-charge components dominated. Surface soil (0-15 cm) had a pH( H2O) of 5.5 and pH(KCl) of 4.8. Subsurface soil (30-45 cm) had a pH(H2O) of 4.8 and a pH(KCl) of 3.5. The point of zero salt effect (PZSE), measured by titration, varied from 3.7 to 5.0 in surface soil and from 3.5 to 4.2 in subsurface soil. Variable charge of surface soil was 2.6 cmol(c)/kg.pH unit after the dry season in April versus 3.2 cmol(c)/kg. pH unit after the wet season in December in both control and dry-season irrigated plots, reflecting seasonal differences in pH and PZSE. The point of zero net charge (PZNC), measured by ion retention, was at pH <2.0, indicating that permanent-charge components dominated the soil surface charge. Five years of dry-season irrigation resulted in pH(H2O) increasing by 0.6 units and pH(KCl) increasing by 0.2 units. As well, irrigation increased the amount of permanent charge and cation retention, leading to less sorption of phosphate and sulfate. The results have important ecological implications, showing mechanistically how wetter conditions affected soil surface charge leading to improved soil nutrient status. C1 Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Yavitt, JB (reprint author), Cornell Univ, Dept Nat Resources, Fernow Hall, Ithaca, NY 14853 USA. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 46 TC 7 Z9 8 U1 0 U2 3 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0004-9573 J9 AUST J SOIL RES JI Aust. J. Soil Res. PY 2002 VL 40 IS 2 BP 269 EP 281 AR UNSP 0004-9573/02/020269 DI 10.1071/SR00061 PG 13 WC Soil Science SC Agriculture GA 529YN UT WOS:000174329000006 ER PT J AU Rothstein, SI Patten, MA Fleischer, RC AF Rothstein, SI Patten, MA Fleischer, RC TI Phylogeny, specialization, and brood parasite-host coevolution: some possible pitfalls of parsimony SO BEHAVIORAL ECOLOGY LA English DT Review DE brood parasitism; coevolution; cowbirds; cuckoos; generalist; parsimony; phylogenetic reconstruction; specialist ID COWBIRD MOLOTHRUS-RUFOAXILLARIS; GREAT SPOTTED CUCKOO; CUCULUS-CANORUS; SHINY COWBIRD; EVOLUTIONARY RATES; SCREAMING COWBIRD; EGG RECOGNITION; COMMON CUCKOO; MOLECULAR PHYLOGENY; REED WARBLERS AB Coevolutionary hypotheses (COEV) predict that parasitic birds become more specialized in host selection over time as more host species evolve defenses. A contrasting model, PHYLO, suggests that brood parasites exhibit a phylogenetic trajectory toward increasing generalization because there is a positive correlation between present-day numbers of host species and the branching order of parasitic cowbird species in a DNA-based phylogeny. However, this apparent phylogenetic pattern does not conflict with COEV, as some have concluded. Assuming allopatric speciation, which is supported by an area cladogram, COEV predicts a correlation between branching order and host number because the potential hosts of the earliest cowbirds to branch off have had the greatest amount of time to evolve defenses. Although PHYLO is more parsimonious than COEV, the difference is trivial, with the latter requiring only one more evolutionary change in the entire cowbird clade to produce the pattern that exists today. Support for COEV over PHYLO comes from brood parasitic cuckoos, which are much more specialized than parasitic cowbirds and represent an older clade, as shown by new DNA data. Cuckoos also have lower interspecific variance in host numbers than do cowbirds, which conflicts with PHYLO. Unlike COEV, which assumes that the number of hosts a parasite uses is related at least as much to present ecological conditions as to phylogenetic history, PHYLO assumes that current host numbers reflect historical character states. However, host number is labile, with as much variation within as between species. Nor are published host numbers reliable measures of parasite host selectivity, as they are due in part to researcher effort and range size. Although the comparative approach can provide insights into evolutionary history, some coevolved features may be too dynamic to retain a phylogenetic signature, and, in the case of parasitic birds, neither PHYLO nor COEV can be invalidated, although the latter is more consistent with available evidence. Strict adherence to parsimony may often be inappropriate when assessing coevolved characters. C1 Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Rothstein, SI (reprint author), Dartmouth Coll, Environm Studies Program, Hanover, NH 03755 USA. EM rothstei@lifesci.ucsb.edu NR 110 TC 42 Z9 45 U1 4 U2 21 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 EI 1465-7279 J9 BEHAV ECOL JI Behav. Ecol. PD JAN PY 2002 VL 13 IS 1 BP 1 EP 10 DI 10.1093/beheco/13.1.1 PG 10 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 513QW UT WOS:000173390700001 ER PT J AU Spindler, RE Wildt, DE AF Spindler, RE Wildt, DE TI Quality and age of companion felid embryos modulate enhanced development by group culture SO BIOLOGY OF REPRODUCTION LA English DT Article DE early development; embryo; gamete biology; in vitro fertilization; reproductive technology ID LAPAROSCOPIC ARTIFICIAL-INSEMINATION; IN-VITRO FERTILIZATION; CAT FOLLICULAR OOCYTES; DOMESTIC CAT; INVITRO FERTILIZATION; EXOGENOUS GONADOTROPINS; MOUSE EMBRYOS; PROTEIN SUPPLEMENTATION; PANTHERA-TIGRIS; BOVINE EMBRYOS AB For some species, embryos cultured with conspecific companions may have enhanced in vitro development compared with singletons. The objective of this study was to determine the effect of quality and age of companion embryos on single felid embryos produced by in vitro maturation or in vitro fertilization. Test oocytes (intermediate quality) were inseminated and incubated alone or with 10 embryos derived from oocytes with a high, intermediate, or low glucose uptake. The effect of relative age of companion embryos on test embryo development was also examined by insemination and incubation of test oocytes alone or with 10 conspecific embryos that were older, younger, or the same age. Test embryos coincubated with better- or equal-quality companions had better development and more cells per embryo (mean +/- SEM number, 74.9 +/- 16.9 and 40.6 +/- 8.8, respectively, Day 7; P < 0.05) than test embryos coincubated with lesser-quality companions (5.1 +/- 1.4) or alone (8.4 +/- 3.7). Intermediate-quality embryos incubated with older companions had more cells per embryo (88.3 +/- 17.0; P < 0.01) than those incubated with synchronous (49.3 +/- 12.1) or younger (29.4 +/- 6.1) embryos. The cell number of solitary embryos (9.8 +/- 3.1) was less (P < 0.05) than that of every group of test embryos incubated with companions, regardless of age. In vitro development of solitary cat embryos is improved by culture with excellent-quality conspecific companions, particularly companions of an advanced age. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Spindler, RE (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM rspindler@crc.si.edu FU NICHD NIH HHS [R03 HD39430-01A1] NR 63 TC 24 Z9 27 U1 1 U2 5 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 JAN PY 2002 VL 66 IS 1 BP 167 EP 173 DI 10.1095/biolreprod66.1.167 PG 7 WC Reproductive Biology SC Reproductive Biology GA 505KW UT WOS:000172912800023 PM 11751278 ER PT J AU Aitken-Palmer, C Wildt, DE Carpenter, JW Spindler, RE AF Aitken-Palmer, C Wildt, DE Carpenter, JW Spindler, RE TI Influence of bicarbonate, hepes, and mops buffers on cat sperm metabolism. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Kansas State Univ, Coll Vet Med, Manhattan, KS 66506 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2002 VL 66 SU 1 MA 190 BP 174 EP 175 PG 2 WC Reproductive Biology SC Reproductive Biology GA 568UD UT WOS:000176561900249 ER PT J AU Pukazhenthi, B Penfold, L Wildt, D Howard, JG AF Pukazhenthi, B Penfold, L Wildt, D Howard, JG TI Direct assessment of cooling-induced changes in cheetah spermatozoa. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. White Oak Conservat Ctr, Yulee, FL USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2002 VL 66 SU 1 MA 351 BP 240 EP 240 PG 1 WC Reproductive Biology SC Reproductive Biology GA 568UD UT WOS:000176561900410 ER PT J AU Siriaroonrat, B Spindler, R Monfort, S Pukazhenthi, B AF Siriaroonrat, B Spindler, R Monfort, S Pukazhenthi, B TI Influence of oocyte selection and estradiol on in vitro maturation of whitetailed deer oocytes. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2002 VL 66 SU 1 MA 353 BP 241 EP 241 PG 1 WC Reproductive Biology SC Reproductive Biology GA 568UD UT WOS:000176561900412 ER PT J AU Brown, JL Goeritz, F Hermes, R Pratt-Hawkes, N Galloway, M Hildebrandt, TB AF Brown, JL Goeritz, F Hermes, R Pratt-Hawkes, N Galloway, M Hildebrandt, TB TI Artificial insemination in the Asian elephant. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Inst Zoo Biol & Wildlife Res, Berlin, Germany. Disneys Anim Kingdom, Lake Buena Vista, FL USA. Smithsonian Natl Zool Pk, Washington, DC USA. NR 0 TC 1 Z9 1 U1 0 U2 2 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2002 VL 66 SU 1 MA 399 BP 259 EP 260 PG 2 WC Reproductive Biology SC Reproductive Biology GA 568UD UT WOS:000176561900458 ER PT J AU Freeman, EW Weiss, E Brown, JL AF Freeman, EW Weiss, E Brown, JL TI Reproductive survey of the African elephant population in North America. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Sedgwick Cty Zoo, Wichita, KS USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2002 VL 66 SU 1 MA 398 BP 259 EP 259 PG 1 WC Reproductive Biology SC Reproductive Biology GA 568UD UT WOS:000176561900457 ER PT J AU Moreland, RB Brown, J Wildt, DE Howard, J AF Moreland, RB Brown, J Wildt, DE Howard, J TI Basic reproductive biology of the fishing cat (Prionailurus viverrinus). SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonians Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. NR 0 TC 10 Z9 11 U1 0 U2 9 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2002 VL 66 SU 1 MA 567 BP 328 EP 328 PG 1 WC Reproductive Biology SC Reproductive Biology GA 568UD UT WOS:000176561900626 ER PT J AU Coddington, JA Chanzy, HD Jackson, CL Raty, G Gardner, KH AF Coddington, JA Chanzy, HD Jackson, CL Raty, G Gardner, KH TI The unique ribbon morphology of the major ampullate silk of spiders from the genus Loxosceles (Recluse spiders) SO BIOMACROMOLECULES LA English DT Article ID MECHANICAL-PROPERTIES; CAPTURE THREADS; STICKINESS; DRAGLINE AB The morphology of silk produced by recluse spiders (Loxosceles arizonica) was investigated by scanning electron microscopy, atomic force microscopy, and transmission electron microscopy. This silk consisted entirely of very long, thin ribbons of width 2-4 mum and thicknesses of no more than 40 nm. The correspondence in shape and dimension between the silk ribbons and the elongated aperture of the major ampullate spigot indicated that these ribbons were major ampullate silk. Selected area electron diffraction patterns from single ribbons were indexed with an orthorhombic unit cell (a = 9.43(2) Angstrom, b = 8.96(3) Angstrom, c = 6.96(1) Angstrom). This unit cell is in good agreement with that previously reported for synthetic poly(L-alanylglycine). Thus it is likely that the crystalline regions of the major ampullate silk of L. arizonica consist of an alternating glycine-L-alanine motif that has adopted a beta-sheet structure. The amino acid composition achieved with the silk of L. arizonica as well as that of L. laeta confirmed that the major amino acid constituents of this silk were glycine and L-alanine in nearly equal amounts. As it was noticed that the dry ribbons were highly electrostatic, it is suggested that the electrostatic interaction plays an important role in prey capture for Loxoseles. C1 Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Univ Grenoble 1, CERMAV, CNRS, Ctr Rech Macromol Vegetales, F-38041 Grenoble 9, France. Dupont Co Inc, Cent Res & Dev, Expt Stn, Wilmington, DE 19880 USA. RP Jackson, CL (reprint author), Natl Inst Stand & Technol, 100 Bur Dr,Stop 8541, Gaithersburg, MD 20899 USA. EM catheryn.jackson@att.net OI Jackson, Catheryn/0000-0003-1611-3926 NR 18 TC 6 Z9 6 U1 0 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1525-7797 J9 BIOMACROMOLECULES JI Biomacromolecules PD JAN-FEB PY 2002 VL 3 IS 1 BP 5 EP 8 DI 10.1021/bm010108m PG 4 WC Biochemistry & Molecular Biology; Chemistry, Organic; Polymer Science SC Biochemistry & Molecular Biology; Chemistry; Polymer Science GA 528RJ UT WOS:000174256500002 PM 11866550 ER PT J AU Lefsky, MA Cohen, WB Parker, GG Harding, DJ AF Lefsky, MA Cohen, WB Parker, GG Harding, DJ TI Lidar remote sensing for ecosystem studies SO BIOSCIENCE LA English DT Article ID LASER SCANNER DATA; LEAF-AREA INDEX; AIRBORNE LIDAR; ALTIMETER MEASUREMENTS; LIGHT TRANSMITTANCE; DECIDUOUS FORESTS; CANOPY STRUCTURE; HEIGHT PROFILES; BASAL AREA; VEGETATION C1 Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. Lab Applicat Remote Sensing Ecol, Corvallis, OR 97331 USA. USDA, Forest Serv, Forestry Sci Lab,Pacific NW Res Stn, Lab Applicat Remote Sensing Ecol, Corvallis, OR 97331 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. RP Lefsky, MA (reprint author), Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. EM lefsky@fsl.orst.edu RI Lefsky, Michael/A-7224-2009; Harding, David/F-5913-2012; OI Parker, Geoffrey/0000-0001-7055-6491 NR 68 TC 746 Z9 780 U1 49 U2 320 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD JAN PY 2002 VL 52 IS 1 BP 19 EP 30 DI 10.1641/0006-3568(2002)052[0019:LRSFES]2.0.CO;2 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 514TG UT WOS:000173456700009 ER PT J AU Farris, HE Rand, AS Ryan, MJ AF Farris, HE Rand, AS Ryan, MJ TI The effects of spatially separated call components on phonotaxis in tungara frogs: Evidence for auditory grouping SO BRAIN BEHAVIOR AND EVOLUTION LA English DT Article DE auditory stream analysis; cocktail party effect; spatial masking; calling song; mate choice; phonotaxis; chorus; amphibian; frog; tungara ID SPARROW SPIZELLA-PUSILLA; TREEFROG HYLA-CINEREA; PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; NEOTROPICAL FROG; MULTICOMPONENT SIGNALS; ACOUSTIC INTERFERENCE; SENSORY EXPLOITATION; EUROPEAN STARLINGS; MECHANICAL MODEL AB Numerous animals across disparate taxa must identify and locate complex acoustic signals imbedded in multiple overlapping signals and ambient noise. A requirement of this task is the ability to group sounds into auditory streams in which sounds are perceived as emanating from the same source. Although numerous studies over the past 50 years have examined aspects of auditory grouping in humans, surprisingly few assays have demonstrated auditory stream formation or the assignment of multicomponent signals to a single source in non-human animals. In our study, we present evidence for auditory grouping in female tungara frogs. In contrast to humans, in which auditory grouping may be facilitated by the cues produced when sounds arrive from the same location, we show that spatial cues play a limited role in grouping, as females group discrete components of the species' complex call over wide angular separations. Furthermore, we show that once grouped the separate call components are weighted differently in recognizing and locating the call, so called 'what' and 'where' decisions, respectively. Copyright (C) 2002 S. Karger AG, Basel. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. RP Farris, HE (reprint author), Louisiana State Univ, Hlth Sci Ctr, Ctr Neurosci, 2020 Gravier St, New Orleans, LA 70112 USA. NR 46 TC 28 Z9 30 U1 0 U2 4 PU KARGER PI BASEL PA ALLSCHWILERSTRASSE 10, CH-4009 BASEL, SWITZERLAND SN 0006-8977 J9 BRAIN BEHAV EVOLUT JI Brain Behav. Evol. PY 2002 VL 60 IS 3 BP 181 EP 188 DI 10.1159/000065937 PG 8 WC Behavioral Sciences; Neurosciences; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Zoology GA 619EX UT WOS:000179463300004 PM 12417822 ER PT J AU Feuillet, C AF Feuillet, C TI A new series and three new species of Passiflora subgenus Astrophea from the Guianas SO BRITTONIA LA English DT Article DE Passifloraceae; Passiflora subg. Astrophea; Brazil; French Guiana; Guyana; Suriname; Venezuela AB A new series, Passiflora ser. Carneae, and three new species are described in Passiflora subg. Astrophea: P. ascidia from Guyana and Venezuelan Guayana; P. balbis from Guyana, Venezuelan Guayana, and Amazonian Brazil; and P. saulensis from central French Guiana. A key to the 19 Guianan species of Passiflora subg. Astrophea is provided. C1 Smithsonian Inst, Dept Systemat Biol Bot, Washington, DC 20560 USA. RP Feuillet, C (reprint author), Smithsonian Inst, Dept Systemat Biol Bot, MRC-166, Washington, DC 20560 USA. NR 5 TC 2 Z9 5 U1 0 U2 2 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD JAN-MAR PY 2002 VL 54 IS 1 BP 18 EP 29 DI 10.1663/0007-196X(2002)054[0018:ANSATN]2.0.CO;2 PG 12 WC Plant Sciences SC Plant Sciences GA 558NA UT WOS:000175972500004 ER PT J AU Collin, R AF Collin, R TI Another last word on Crepidula convexa with a description of C-ustulatulina n. sp (Gastropoda : Calyptraeidae) from the Gulf of Mexico and southern Florida SO BULLETIN OF MARINE SCIENCE LA English DT Article ID PROSOBRANCHIA AB The taxonomy of Crepidula has a history of instability due to the low number of informative shell characters and their phenotypic plasticity. Molecular and developmental data show that Crepidula convexa sensu Hoagland 1977 is composed of two distinct species. Animals of the northern species are relatively larger, and have darker shells and direct development, while animals from the Gulf of Mexico and southeastern Florida have smaller, pale spotted shells and produce pediveligers. C. convexa Say, 1822 is redescribed and a single neotype is designated for C. convexa and C. glauca Say, 1822 to represent the northern species and to formalize the synonymy of these two names. The southern species, which is distributed throughout the Gulf of Mexico, is described as a new species, C. ustulatulina. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. RI Collin, Rachel/G-2001-2010 NR 29 TC 21 Z9 21 U1 1 U2 4 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 2002 VL 70 IS 1 BP 177 EP 184 PG 8 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 563RB UT WOS:000176268400014 ER PT J AU Swearer, SE Shima, JS Hellberg, ME Thorrold, SR Jones, GP Robertson, DR Morgan, SG Selkoe, KA Ruiz, GM Warner, RR AF Swearer, SE Shima, JS Hellberg, ME Thorrold, SR Jones, GP Robertson, DR Morgan, SG Selkoe, KA Ruiz, GM Warner, RR TI Evidence of self-recruitment in demersal marine populations SO BULLETIN OF MARINE SCIENCE LA English DT Review ID GREAT-BARRIER-REEF; SPECIES MYTILUS-GALLOPROVINCIALIS; DIFFERENT SPATIAL SCALES; LONG-DISTANCE DISPERSAL; EASTERN PACIFIC-OCEAN; SUPPLY-SIDE ECOLOGY; OF-THORNS STARFISH; GENE FLOW; PLANKTONIC LARVAE; CORAL-REEFS AB The majority of shallow-water marine species have a two-phase life cycle in which relatively sedentary, demersal adults produce pelagic larvae. Because these larval stages are potentially subject to dispersal by ocean cur-rents, it has been widely accepted that local populations are open. with recruitment resulting from the arrival of larvae from non-local sources. However, a growing number of studies indicate that larvae are capable of recruiting back to their source population. Here, we review the evidence for self-recruitment in demersal marine populations, drawing from studies of endemism, introduced species, population genetics, stock-recruitment relationships, larval distributions, populations at the limit of a species' range, and applications of environmental and chemical markers. These studies indicate that self-recruitment can and does occur across species representative of most life history traits and geographical localities. Thus, the ability of larvae to recruit back to their natal population may be a pervasive phenomenon among marine species, The mounting evidence in support of self-recruitment dynamics indicates a pressing need for a reevaluation of the appropriateness of demographically-open population models and their applicability to the management and conservation of marine ecosystems. C1 Univ Melbourne, Dept Zool, Melbourne, Vic 3010, Australia. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Calif Bodega, Marine Lab, Bodega Bay, CA 94923 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Swearer, SE (reprint author), Univ Melbourne, Dept Zool, Melbourne, Vic 3010, Australia. RI 平山, 幸恵/G-9307-2012; Thorrold, Simon/B-7565-2012; jones, geoffrey/E-9306-2010; Warner, Robert/M-5342-2013; OI Thorrold, Simon/0000-0002-1533-7517; jones, geoffrey/0000-0002-6244-1245; Warner, Robert/0000-0002-3299-5685; Shima, Jeffrey/0000-0001-5770-4859; SWEARER, STEPHEN/0000-0001-6381-9943; Ruiz, Gregory/0000-0003-2499-441X NR 130 TC 265 Z9 270 U1 2 U2 52 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 2002 VL 70 IS 1 SU S BP 251 EP 271 PG 21 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 565NZ UT WOS:000176377500002 ER PT J AU Strathmann, RR Hughes, TP Kuris, AM Lindeman, KC Morgan, SG Pandolfi, JM Warner, RR AF Strathmann, RR Hughes, TP Kuris, AM Lindeman, KC Morgan, SG Pandolfi, JM Warner, RR TI Evolution of local recruitment and its consequences for marine populations SO BULLETIN OF MARINE SCIENCE LA English DT Review ID CORAL-REEF FISH; ROCKY INTERTIDAL COMMUNITIES; BENTHIC INVERTEBRATES; LARVAL DEVELOPMENT; POSTSETTLEMENT MORTALITY; VARYING ENVIRONMENTS; SUSPENSION-FEEDER; SPECIES LONGEVITY; PLANKTONIC LARVAE; GENETIC-STRUCTURE AB Advantages of dispersal on the scales that are possible in a long pelagic larval period are not apparent, even for benthic species. An alternative hypothesis is that wide dispersal may be an incidental byproduct of an ontogenetic migration from and then back to the parental habitat. Under this hypothesis, the water column is a better habitat than the bottom for early development. Because the parental area is often an especially favorable habitat for juveniles and adults, selection may even favor larval retention or larval return rather than dispersal. Where larval capabilities and currents permit, a high percentage of recruits may then be produced from local adults. Expected consequences of a high proportion of local recruitment are stronger links between stock and recruitment, greater vulnerability to recruitment overfishing and local modifications of habitat, greater local benefits from fishery reserves, and possibly more localized adaptation within populations. Export of some larvae is consistent with a high proportion of retained or returning larvae, could stabilize populations linked by larval exchange, and provide connectivity between marine reserves. Even a small amount of larval export could account for the greater gene flow, large ranges, and long evolutionary durations seen in species with long pelagic larval stages. C1 Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. Univ Washington, Dept Zool, Friday Harbor, WA 98250 USA. James Cook Univ N Queensland, Dept Marine Sci, Townsville, Qld 4811, Australia. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Environm Def, Miami Field Off, Miami, FL 33186 USA. Univ Calif Bodega, Marine Lab, Bodega Bay, CA 94923 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Strathmann, RR (reprint author), Univ Washington, Friday Harbor Labs, 620 Univ Rd, Friday Harbor, WA 98250 USA. EM rrstrath@u.washington.edu; terry.hughes@jcu.edu.au; kuris@lifesci.ucsb.edu; klindeman@environmentaldefense.org; sgmorgan@ucdavis.edu; pandolfi.john@nmnh.si.edu; warner@lifesci.ucsb.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 NR 130 TC 146 Z9 154 U1 4 U2 62 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 2002 VL 70 IS 1 SU S BP 377 EP 396 PG 20 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 565NZ UT WOS:000176377500007 ER PT J AU Asher, RJ McKenna, MC Emry, RJ Tabrum, AR Kron, DG AF Asher, RJ McKenna, MC Emry, RJ Tabrum, AR Kron, DG TI Morphology and relationships of Apternodus and other extinct, zalambdodont, placental mammals SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Review ID EUTHERIAN MAMMALS; NORTH-AMERICA; EOCENE; CHARACTERS; INSECTIVORE; PHYLOGENY; HOMOLOGY; MONTANA; ORDER; FAUNA AB We describe and illustrate new, middle Cenozoic fossils of dentally zalambdodont, North American placentals, including six relatively complete crania of Apternodus and two of Oligoryctes, as well as many partial skulls, mandibles, and teeth of these and other taxa. Several of the new Apternodus specimens are also associated with postcrania. We recognize seven species of Apternodus, three of which are new, formally propose the combination Oligoryctes altitalonidus, and recognize two other genera of small, North American, anatomically zalambdodont placentals, Parapternodus and Koniaryctes. We regard two other taxa previously associated with North American fossil zalambdodonts, one Bridgerian and the other Tiffanian, as valid but do not name them in this paper. In addition, we argue that dental zalambdodonty entails a primary occlusal relationship between the paracone and the ectoflexid, and the reduction or absence of the metacone and talonid basin. A phylogenetic analysis of cranial, dental, and postcranial characters of 30 fossil and Recent taxa leads us to conclude that (1) the Apternodontidae as defined in previous literature is not monophyletic and should be restricted to seven species of Apternodus, (2) the genus Oligoryctes contains at least two species and has a considerably longer geologic record than Apternodus, (3) neither Micropternodus nor currently known Paleocene taxa are closely related to Apternodus or Oligoryctes, and (4) a case can be made for a close relationship among modern soricids, Parapternodus, Koniaryctes, Oligoryctes, and Apternodus to the exclusion of other insectivoran-grade taxa. With the use of ordered, multistate character transformations, Solenodon comprises the sister taxon to a soricid-fossil zalambdodont clade. C1 Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. Univ Wyoming, Laramie, WY 82071 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Paleobiol, Washington, DC 20560 USA. Carnegie Museum Nat Hist, Sect Vertebrate Paleontol, Pittsburgh, PA 15213 USA. Univ Colorado Museum, Sect Geol, Boulder, CO 80309 USA. EM asher@amnh.org; m4pmck@indra.com; emry.robert@nmnh.si.edu; tabrum@carnegiemuseums.org NR 173 TC 35 Z9 38 U1 2 U2 4 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 0003-0090 EI 1937-3546 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 2002 IS 273 BP 1 EP 117 PG 117 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 621AZ UT WOS:000179567500001 ER PT J AU Wunderman, R AF Wunderman, R TI Smithsonian Institution's global volcanism network SO BULLETIN OF VOLCANOLOGY LA English DT Article C1 Smithsonian Inst, Natl Museum Nat Hist, Global Volcanism Network, Washington, DC 20560 USA. RP Wunderman, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Global Volcanism Network, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0258-8900 J9 B VOLCANOL JI Bull. Volcanol. PD JAN PY 2002 VL 63 IS 8 BP 572 EP 573 DI 10.1007/s004450100169 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 521KM UT WOS:000173839200007 ER PT J AU Schulze, A AF Schulze, A TI Histological and ultrastructural characterization of the intravasal body in Vestimentifera (Siboglinidae, Polychaeta, Annelida) SO CAHIERS DE BIOLOGIE MARINE LA English DT Article; Proceedings Paper CT 2nd International Symposium on Deep-Sea Hydrothermal Vent Biology CY OCT 08-12, 2001 CL BREST, FRANCE SP 5th Framework Program European Commiss, CNRS, IFREMER, Univ Bretagne Occidentale, Inst Univ Europeen Mer, Reg Bretagne, Counseil Gen Finistere & Communaute Urbaine Brest, Total Fina Elf, Banque Populaire Ouest, Casden Banque Populaire, FEI Co, Proteus, Air France, Dorsales, InterRidge, Ridge USA, Mineral Management Serv, USA ID HEMOGLOBIN; SYSTEM C1 Smithsonian Inst, NMNH, Washington, DC 20560 USA. RP Schulze, A (reprint author), Smithsonian Inst, NMNH, MRC 163, Washington, DC 20560 USA. RI Schulze, Anja/I-4215-2012 NR 13 TC 7 Z9 9 U1 0 U2 1 PU CAHIERS DE BIOLOGIE MARINE PI ROSCOFF PA STATION BIOLOGIQUE PLACE GEORGES TEISSIER, 29680 ROSCOFF, FRANCE SN 0007-9723 J9 CAH BIOL MAR JI Cah. Biol. Mar. PY 2002 VL 43 IS 3-4 BP 355 EP 358 PG 4 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 627NB UT WOS:000179938200031 ER PT J AU Guzman, HM Guevara, CA AF Guzman, HM Guevara, CA TI Population structure, distribution and abundance of three commercial species of sea cucumber (Echinodermata) in Panama SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article ID HOLOTHUROIDEA; REPRODUCTION AB Overfishing due to high demand in Asian markets, have encouraged illegal fisheries of sea cucumbers in non-traditional areas of the tropical Caribbean. This work assesses the population structure, distribution, and abundance of three commercially important Caribbean species (Isostichopus badionotus, Holothuria mexicana, and Astichopus multifidus) in 47 158 hectares of shallow habitats in Bocas del Toro (Panama), from May to October 2000. Mean size class distribution was unimodal; 26.5 cm in I. badionotus and 16 cm in H. mexicana, and dominated by adult individuals of 25-30 cm for both species. Body wall wet weight (gutted) showed a similar distribution, with a higher number of individuals between 200-300 g, but with a lower mean in L badionotus (214 g) than in H. mexicana (258g). A total of 6017 individuals of H. mexicana, 4431 L badionotus and 208 A. multifidus were quantified, with mean densities of 161.8 ind./ha, 117.4 ind./ha., and 4.9 ind./ha, respectively. Based on these results and the total area of the archipelago, we estimated a stock of 7 630 164 individuals for H. mexicana, 5 536 349 for I. badionotus, and 231 074 for A. multifidus. This assessment is discouraging because during the 1997 30-day legal fishing period, a catch of ca. 750 000 holothuroids was estimated for the archipelago. 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 15 Z9 16 U1 5 U2 14 PU UNIV PUERTO RICO, PI MAYAGUEZ PA COLLEGE ARTS SCIENCES, MAYAGUEZ, PUERTO RICO 00680 USA SN 0008-6452 J9 CARIBB J SCI JI Caribb. J. Sci. PY 2002 VL 38 IS 3-4 BP 230 EP 238 PG 9 WC Biodiversity Conservation SC Biodiversity & Conservation GA 623BT UT WOS:000179683900006 ER PT J AU Woodman, N Schneider, E Grant, P Same, D Schmall, KE Curtis, JT AF Woodman, N Schneider, E Grant, P Same, D Schmall, KE Curtis, JT TI A new southern distributional limit for the Central American rodent Peromyscus stirtoni SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article ID MAMMALS C1 Smithsonian Inst, Natl Museum Nat Hist, USGS, Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. Peace Corps, Lilongwe, Malawi. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS, Patuxent Wildlife Res Ctr, POB 37012,NHB 378,MRC-111, Washington, DC 20013 USA. NR 11 TC 1 Z9 2 U1 0 U2 1 PU UNIV PUERTO RICO, PI MAYAGUEZ PA COLLEGE ARTS SCIENCES, MAYAGUEZ, PUERTO RICO 00680 USA SN 0008-6452 J9 CARIBB J SCI JI Caribb. J. Sci. PY 2002 VL 38 IS 3-4 BP 281 EP 284 PG 4 WC Biodiversity Conservation SC Biodiversity & Conservation GA 623BT UT WOS:000179683900018 ER PT S AU Huber, BT MacLeod, KG Norris, RD AF Huber, BT MacLeod, KG Norris, RD BE Koeberl, C MacLeod, KG TI Abrupt extinction and subsequent reworking of Cretaceous planktonic foraminifera across the Cretaceous-Tertiary boundary: Evidence from the subtropical North Atlantic SO CATASTROPHIC EVENTS AND MASS EXTINCTIONS: IMPACTS AND BEYOND SE Geological Society of America Special Papers LA English DT Proceedings Paper CT International Interdisciplinary Conference on Catastrophic Events and Mass Extinctions - Impacts and Beyond CY JUL 09-12, 2000 CL UNIV VIENNA, VIENNA, AUSTRIA SP Lunar & Planetary Inst, Barringer Crater Co, European Sci Fdn Impact, Fed Minist Educ, Sci, and Culture, Geolog Survey Austria, Vienna Convent Bureau, Int Assoc Geochem & Cosmochem, Finnegan, Micromass, & Cameca Instruments HO UNIV VIENNA ID K-T BOUNDARY; BLAKE NOSE; MASS EXTINCTION; IMPACT; CHICXULUB; PRODUCTIVITY; SURVIVORSHIP; SEDIMENTS AB An impact ejecta bed containing shocked quartz and diagenetically altered tektite spherules coincides exactly with biostratigraphic placement of the Cretaceous-Tertiary (K-T) boundary in three drill cores recovered from Ocean Drilling Program Site 1049 (located in the subtropical North Atlantic Ocean). Both the bracketing pelagic ooze and the ejecta bed are undisturbed at Site 1049, allowing detailed examination of the expression of the boundary event in an open ocean setting. The youngest Cretaceous sediments contain a diverse assemblage of well-preserved upper Maastrichtian Tethyan microfossils. The overlying ejecta bed varies laterally in thickness, has sharp lower and upper contacts, and contains features (e.g., presence of a foraminiferal grainstone layer at its base and large chalk clasts in its middle, and dominance of poorly sorted coarse grains throughout) that suggest it was deposited by one or several mass-flow events. The oldest Danian ooze contains abundant, tiny planktonic foraminifera characteristic of the early Danian Palpha Zone as well as common, large Cretaceous individuals. The lowermost Danian P0 Zone (assemblage dominated by Guembelitria cretacea) is apparently absent. This absence could reflect restriction of the P0 assemblage to shallower settings, slow sedimentation rates coupled with bioturbation mixing Tertiary forms into (and thus obscuring) the P0 Zone, or an interval of erosion or nondeposition. Cretaceous species decline and last occur in the first several meters of section above the ejecta bed. This pattern could be interpreted as evidence for gradual extinction above the impact bed, but thin-section observations, relative abundance counts, size-distribution analyses, and comparison with species extinctions at other K-T sections demonstrate sudden extinction, nearly all post-K-T occurrences of Cretaceous planktonic foraminiferal species being explained as the result of sediment reworking. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Huber, BT (reprint author), Smithsonian Inst, Dept Paleobiol, MRC NHB-121, Washington, DC 20560 USA. EM huber.brian@nmnh.si.edu; macleodk@missouri.edu; rnorris@whoi.edu RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 NR 31 TC 18 Z9 18 U1 0 U2 2 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 0-8137-2356-6 J9 GEOL SOC AM SPEC PAP PY 2002 VL 356 BP 277 EP 289 PG 13 WC Geochemistry & Geophysics; Geology SC Geochemistry & Geophysics; Geology GA BV31N UT WOS:000178575200020 ER PT B AU Fabbiano, G AF Fabbiano, G BE FuscoFemiano, R Matteucci, F TI Observations of galaxies with Chandra SO CHEMICAL ENRICHMENT OF INTRACLUSTER AND INTERGALACTIC MEDIUM SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Chemical Enrichment of Intracluster and Intergalactic Medium CY MAY 14-18, 2001 CL VULCANO, ITALY SP Univ Trieste, Dept Atronom, CNR, Ist Astrofis Spaziale ID X-RAY-EMISSION; SAMPLE; M81 AB This talk discusses the growing impact of Chandra observations on the study of galaxies. In particular, we address progress in the study of X-ray source populations in diverse galaxies and in the study of the hot ISM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-093-5 J9 ASTR SOC P PY 2002 VL 253 BP 93 EP 102 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU69P UT WOS:000176731700010 ER PT S AU Brown, DS Parnell, CE DeLuca, EE McMullen, RA Golub, L Priest, ER AF Brown, DS Parnell, CE DeLuca, EE McMullen, RA Golub, L Priest, ER BE Buchner, J TI Magnetic structure and reconnection of X-ray bright points in the solar corona SO COMPARATIVE RECONNECTION STUDIES AT THE SUN AND IN PLANETARY MAGNETOSPHERES SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT D0 1-E3 1 Symposium of COSPAR Scientific Commission D held at the 33rd COSPAR Scientific Assmbly CY JUL, 2000 CL WARSAW, POLAND SP Comm Space Res ID FIELDS; MODEL AB The three-dimensional magnetic topology of the solar corona is incredibly complex and its effect on the nature of 3D reconnection is profound. We study the supposedly simple topology of a small scale X-ray bright point observed by TRACE and SOHO/MDl, and how it is driven by reconnection when it forms and during the early stages of its lifetime. (C) 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved. C1 Univ St Andrews, Inst Math, St Andrews KY16 9SS, Fife, Scotland. Smithsonian Astrophys Observ, Cambridge, MA 02188 USA. Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Brown, DS (reprint author), Univ St Andrews, Inst Math, St Andrews KY16 9SS, Fife, Scotland. RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Brown, Daniel/0000-0002-1618-8816; Golub, Leon/0000-0001-9638-3082 NR 16 TC 2 Z9 2 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2002 VL 29 IS 7 BP 1093 EP 1099 AR PII S0273-1177(02)00026-1 DI 10.1016/S0273-1177(02)00026-1 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BU54U UT WOS:000176290600010 ER PT J AU van den Biggelaar, JAM Edsinger-Gonzales, E Schram, FR AF van den Biggelaar, JAM Edsinger-Gonzales, E Schram, FR TI The improbability of dorso-ventral axis inversion during animal evolution, as presumed by Geoffroy Saint Hilaire SO CONTRIBUTIONS TO ZOOLOGY LA English DT Article DE amphistomy; axis inversion; deuterostomes; spiral cleavage; protostomes; gastrulation AB Recent discoveries in the field of developmental genetics have lead to the resurrection of the old idea, first proposed in the early 1911 century, that the dorso-ventral axis of deuterostomes, such as vertebrates, has been inverted during the course of evolution from that noted in protostomes, i.e., what in deuterostomes is dorsal, is in protostomes ventral. However, while attractive in its simplicity, such a suggestion ignores the real events of embryogenesis. During the onset of gastrulation in deuterostomes as well as in protostomes a blastopore is formed with exactly the same embryonic, antero-posterior/dorso-ventral polarity. Subsequent differences in the patterns or morphogenetic movement in gastrulation result in a spatial inversion of this developniental architecture in the adult body plans of protostomes versus deuterostomes. In deuterostomes, the initial anterior-posterior axis is extended more or less evenly while the blastopore remains located posteriorly. In protostomes, such as annelids and gastropods, the growth of the original antero-posterior or animal-vegetal axis is extremely uneven and almost exclusively limited to cells of the embryonic dorsal side. This is coupled with the cells of the original ventral side of the embryo in part moving into the inside of the embryo, and in part moving into what had spatially been the embryonic lateral and more dorsal position. Because of this uneven migration, the embryonic ventral side of the developing larva is not extended and the initial anteroposterior axis is bent, with the blastopore moving into an animal-vegetal position. What were originally dorsal cells move to a ventral position. This fully explains the conservation of developmental gene expression patterns as resulting from a shift of initially dorsally specified cells to a secondarily ventral position. C1 Univ Utrecht, Fac Biol, Dept Expt Zool, NL-3584 CH Utrecht, Netherlands. Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1092 AD Amsterdam, Netherlands. RP van den Biggelaar, JAM (reprint author), Univ Utrecht, Fac Biol, Dept Expt Zool, Padualaan 8, NL-3584 CH Utrecht, Netherlands. NR 32 TC 11 Z9 11 U1 0 U2 5 PU S P B ACADEMIC PUBLISHING BV PI LELYSTAD PA PLATINASTRAAT 33, 8211 AR LELYSTAD, NETHERLANDS SN 0067-8546 J9 CONTRIB ZOOL JI Contrib. Zool. PY 2002 VL 71 IS 1-3 BP 29 EP 36 PG 8 WC Zoology SC Zoology GA 636NZ UT WOS:000180463800003 ER PT J AU Alvarez, B van Soest, RWM Rutzler, K AF Alvarez, B van Soest, RWM Rutzler, K TI Svenzea, a new genus of Dictyonellidae (Porifera : Demospongiae) from tropical reef environments, with description of two new species SO CONTRIBUTIONS TO ZOOLOGY LA English DT Article DE Porifera; Demospongiae; Dictyonellidae; new genus; new species; Svenzea cristinae; Svenzea devoogdae ID SPONGE CALYX-PODATYPA AB The new genus Svenzea is created to group three sponge species from tropical reef environments of the Caribbean Sea and Indonesia: Pseudaxinella (?) zeai Alvarez, Van Soest & Rutzler, Svenzea cristinae n. sp. and S. devoogdae n. sp. The genus shows affinities with members of both Halichondrida and Haplosclerida but it is assigned to the family Dictyonellidae based on shared microanatomical and developmental features. The higher taxonomic position of Svenzea is a subject for future investigations. C1 Museum & Art Gallery No Terr, Darwin, NT 0801, Australia. Univ Amsterdam, Fac Sci, Zool Museum, NL-1090 GT Amsterdam, Netherlands. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Alvarez, B (reprint author), Museum & Art Gallery No Terr, POB 4646, Darwin, NT 0801, Australia. NR 19 TC 11 Z9 13 U1 0 U2 4 PU S P B ACADEMIC PUBLISHING BV PI LELYSTAD PA PLATINASTRAAT 33, 8211 AR LELYSTAD, NETHERLANDS SN 0067-8546 J9 CONTRIB ZOOL JI Contrib. Zool. PY 2002 VL 71 IS 4 BP 171 EP 176 PG 6 WC Zoology SC Zoology GA 642ER UT WOS:000180791700007 ER PT S AU Rodriguez, LF Anglada, G Torrelles, JM Mendoza-Torres, JE Haschick, AD Ho, PTP AF Rodriguez, LF Anglada, G Torrelles, JM Mendoza-Torres, JE Haschick, AD Ho, PTP BE Migenes, V Reid, MJ TI VLA Observations of water maser emission associated with SVS 13 SO COSMIC MASERS: FROM PROTOSTARS TO BLACKHOLES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Cosmic Masers - From Protostars to Blackholes CY MAR 05-10, 2001 CL ANGRA REIS, BRAZIL SP Int Astron Union ID HERBIG-HARO OBJECTS; HH 7-11; EXCITING SOURCE; NGC-1333; REGION; STAR AB The young stellar object SVS 13 has been proposed as the powering source of the HH 7-11 objects. Recent observations have revealed that in the radio continuum (3.6-cm) the source is a binary separated by about 0."3 in the east-west direction. We present Very Large Array observations, made in the highest angular resolution A configuration, of H(2)O maser emission toward this source. Our data show that the H(2)O spots appear to be segregated in two velocity groups: a group with radial velocity similar to that of the ambient cloud (V(LSR) similar or equal to 8 km s(-1)) that is associated with the western radio source, and a blueshifted (by similar to20 km s(-1)) velocity group that is associated with the eastern radio source. We discuss the possible implications of this observation. C1 Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, IEEC, E-08034 Barcelona, Spain. CSIC, Inst Ciencias Espacio, E-08034 Barcelona, Spain. Inst Nacl Astrofis Opt & Electr, Tonantzintla 72840, Puebla, Mexico. MIT, Haystack Observ, Westford, MA 01886 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rodriguez, LF (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Campus Morelia,Apdo Postal 3-72, Morelia 58089, Michoacan, Mexico. EM l.rodriguez@astrosmo.unam.mx; torrelle@ieec.fcr.es NR 14 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 1-58381-112-5 J9 IAU SYMP PY 2002 IS 206 BP 59 EP 62 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW16P UT WOS:000181054300011 ER PT S AU Trinidad, MA Curiel, S Canto, J Torrelles, JM Rodriguez, LF Gomez, JF Ho, PTP AF Trinidad, MA Curiel, S Canto, J Torrelles, JM Rodriguez, LF Gomez, JF Ho, PTP BE Migenes, V Reid, MJ TI Observations of H2O maser and continuum emission in AFGL 2591 SO COSMIC MASERS: FROM PROTOSTARS TO BLACKHOLES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Cosmic Masers - From Protostars to Blackholes CY MAR 05-10, 2001 CL ANGRA REIS, BRAZIL SP Int Astron Union ID MOLECULAR OUTFLOWS; STAR; REGIONS AB We report results of radio continuum (1.3 and 3.6 cm) and H2O maser line observations, made with the Very Large Array (A configuration), toward the star-forming region AFGL 2591. We detected 85 maser spots toward this region, which are distributed in three main groups. Two of these groups spatially coincide with the radio continuum sources VLA 2 and VLA 3. The maser spots associated with VLA 3 are distributed along a shell-like structure of 0."01 and nearly perpendicular to the CO bipolar outflow. We propose that VLA 3 is the center of the observed molecular flow in this region. Finally, we confirm that AFGL 2591 region is a cluster of B type stars, each one with its own optically thin H II region. C1 Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. CSIC, IEEC, E-08034 Barcelona, Spain. CSIC, Inst Ciencias Espacio, E-08034 Barcelona, Spain. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. INTA, Lab Astrofis Espacial & Fis Fundamental, E-28080 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Trinidad, MA (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 70-264, Mexico City 04510, DF, Mexico. EM trinidad@gastroscu.unam.mx; scuriel@astroscu.unam.mx; torrelle@ieec.fcr.es; l.rodriguez@astrosmo.unam.mx OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 9 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 1-58381-112-5 J9 IAU SYMP PY 2002 IS 206 BP 68 EP 71 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW16P UT WOS:000181054300013 ER PT S AU Torrelles, JM Patel, NA Gomez, JF Ho, PTP Rodriguez, LF Anglada, G Garay, G Greenhill, L Curiel, S Canto, J AF Torrelles, JM Patel, NA Gomez, JF Ho, PTP Rodriguez, LF Anglada, G Garay, G Greenhill, L Curiel, S Canto, J BE Migenes, V Reid, MJ TI VLBA multi-epoch water maser observations towards Cepheus A SO COSMIC MASERS: FROM PROTOSTARS TO BLACKHOLES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Cosmic Masers - From Protostars to Blackholes CY MAR 05-10, 2001 CL ANGRA REIS, BRAZIL SP Int Astron Union ID THERMAL RADIO JET; EMISSION; HW2 AB We have carried out and recently reported VLBA multi-epoch water maser observations toward Cepheus A with an angular and velocity resolution of 0.5 mas and 0.2 km s(-1), respectively. Some of the masers detected previously with the VLA (observations made with angular and velocity resolutions of 80 mas and 1.3 km s(-1) respectively) are resolved now into linear/arcuate coherent "microstructures". These structures, while smaller than the VLA beam, are 6-200 times the size of the VLBA synthesized beam. The morphology and the observed proper motions found in these structures imply three different centers of star formation activity in a region of similar or equal to 0."3 radius (similar or equal to 200 AU). The most remarkable result from these observations is the discovery of an arc of water masers which is perfectly fitted by a circle to one part in a thousand. This arc is expanding and suggests a spherical "puff" of ejected material ejected 33 years ago from a protostar located 600 mas south of the radio jet HW2. This spherical ejection represents a very strong challenge for theoretical studies of star formation. C1 CSIC, IEEC, E-08034 Barcelona, Spain. CSIC, Inst Ciencias Espacio, E-08034 Barcelona, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INTA, Lab Astrofis Espacial & Fis Fundamental, E-28080 Madrid, Spain. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Univ Chile, Dept Astron, Santiago, Chile. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Torrelles, JM (reprint author), CSIC, IEEC, Edifici Nexus,C Gran Capita,2-4, E-08034 Barcelona, Spain. EM torrelle@ieec.fcr.es; l.rodriguez@astrosmo.unam.mx; garay@das.uchile.cl; lincoln@cfa.harvard.edu; scuriel@astroscu.unam.mx RI Garay, Guido/H-8840-2013; OI Garay, Guido/0000-0003-1649-7958; Torrelles, Jose Maria/0000-0002-6896-6085 NR 12 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-112-5 J9 IAU SYMP PY 2002 IS 206 BP 84 EP 87 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW16P UT WOS:000181054300017 ER PT S AU Argon, AL Reid, MJ Menten, KM AF Argon, AL Reid, MJ Menten, KM BE Migenes, V Reid, MJ TI Full-polarization maps of OH main-line masers in the W51 and G351.78-0.54 star-forming regions SO COSMIC MASERS: FROM PROTOSTARS TO BLACKHOLES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Cosmic Masers - From Protostars to Blackholes CY MAR 05-10, 2001 CL ANGRA REIS, BRAZIL SP Int Astron Union ID MAGNETIC-FIELD STRENGTHS; INTERSTELLAR AB Full-polarization spectral-line VLBA observations were made of the ground state, main-line, (2)Pi(3/2) J = 3/2 OH masers in two Galactic star-forming regions: the "el"/"e2" region of W51 and G351.78-0.54. Two especially interesting results are presented. (1) Two of the 27 Zeeman pairs in W51 were found to be associated with unusually strong magnetic fields (approximate to 20 mG), more than twice as strong as for any previously reported OH maser. (2) C351.78-0.54 was found to exhibit a high degree of linear polarization (up to 61%), which constrains the three dimensional structure of its magnetic field. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-5300 Bonn, Germany. RP Argon, AL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-112-5 J9 IAU SYMP PY 2002 IS 206 BP 367 EP 370 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW16P UT WOS:000181054300077 ER PT S AU Fish, VL Reid, MJ Argon, AL Menten, KM AF Fish, VL Reid, MJ Argon, AL Menten, KM BE Migenes, V Reid, MJ TI Zeeman splitting of OH masers and the galactic magnetic field SO COSMIC MASERS: FROM PROTOSTARS TO BLACKHOLES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Cosmic Masers - From Protostars to Blackholes CY MAR 05-10, 2001 CL ANGRA REIS, BRAZIL SP Int Astron Union ID HYDROXYL MASERS; GALAXY AB Zeeman measurements of OH masers are used to probe the magnetic field around regions of massive star formation. Previous observations suggested that OH maser field directions were aligned in a clockwise sense in the Milky Way, but recent data from a large-scale VLA survey do not support this hypothesis. However, these observations suggest that the magnetic field of the Milky Way is correlated on kiloparsec scales. 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 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 1-58381-112-5 J9 IAU SYMP PY 2002 IS 206 BP 371 EP 374 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW16P UT WOS:000181054300078 ER PT S AU Greenhill, LJ AF Greenhill, LJ BE Migenes, V Reid, MJ TI Extragalactic H2O masers SO COSMIC MASERS: FROM PROTOSTARS TO BLACKHOLES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Cosmic Masers - From Protostars to Blackholes CY MAR 05-10, 2001 CL ANGRA REIS, BRAZIL SP Int Astron Union ID WATER-VAPOR MASERS; LARGE MAGELLANIC CLOUD; GALAXY NGC4258; EMISSION; NGC-4258; DISK; NGC-1068; CIRCINUS; DISCOVERY; MEGAMASER AB Study of extragalactic H2O masers has progressed significantly in the 25 years since their discovery. Existing in star forming regions and in the accretion disks supermassive black holes, they are familiar and unfamiliar at the same time. A review of how our understanding has grown, up to the present day, is followed by comments on future prospects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. NR 59 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 1-58381-112-5 J9 IAU SYMP PY 2002 IS 206 BP 381 EP 391 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW16P UT WOS:000181054300080 ER PT S AU Reid, MJ AF Reid, MJ BE Migenes, V Reid, MJ TI Masers, from protostars to black holes: Conference summary SO COSMIC MASERS: FROM PROTOSTARS TO BLACKHOLES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Cosmic Masers - From Protostars to Blackholes CY MAR 05-10, 2001 CL ANGRA REIS, BRAZIL SP Int Astron Union AB Astronomical sources of maser emission have now been studied for more than 30 years, and research related to masers spans a very wide range of topics in astrophysics. Over this period great progress has been made in many areas of maser research. This summary will put maser research into an historical perspective and focus on highlights from this conference. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-112-5 J9 IAU SYMP PY 2002 IS 206 BP 506 EP 519 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW16P UT WOS:000181054300100 ER PT J AU Randall, JE Earle, JL Robertson, DR AF Randall, JE Earle, JL Robertson, DR TI Iniistius auropunctatus, a new razorfish (Perciformes : Labridae) from the Marquesas Islands SO CYBIUM LA English DT Article DE Labridae; Iniistius auropunctatus; ISEW; Marquesas Islands; new species AB The labrid fish Iniitstius auropunctatus is described from 13 specimens, 95.5-129 mm SL, collected in 15-17 in at Ua Pou, Marquesas Islands. It is one of a complex of species characterized by the first two dorsal spines not being fully separated from the rest of fin and by a broad column of small scales extending from below the eye to behind the corner of the mouth. It is closely related to the wide-ranging, allopatric, Indo-Pacific species L pentadactylus, having nearly the same female color pattern. It differs from L pentadactylus chiefly in the color of the male, with blackish lines under edges of anterior lateral-line scales instead of three to six large deep red spots in a row behind the eye. Also it is a smaller species, the largest specimen 129 mm SL (I. pentadactylus reaches 200 mm SL). C1 Bernice P Bishop Museum, Honolulu, HI 96817 USA. Smithsonian Trop Res Inst, Unit 0948, Balboa 34002, Panama. RP Randall, JE (reprint author), Bernice P Bishop Museum, 1525 Bernice St, Honolulu, HI 96817 USA. NR 4 TC 1 Z9 4 U1 0 U2 0 PU SOC FRANCAISE D ICHTYOLOGIE PI PARIS PA MUSEUM NATL D HISTOIRE NATURELLE, 43 RUE CUVIER, 75231 PARIS, FRANCE SN 0399-0974 J9 CYBIUM JI Cybium PY 2002 VL 26 IS 2 BP 93 EP 98 PG 6 WC Zoology SC Zoology GA 586VP UT WOS:000177607100003 ER PT S AU Marvin, UB AF Marvin, UB BE Oldroyd, DR TI Geology: From an Earth to a planetary science in the twentieth century SO EARTH INSIDE AND OUT: SOME MAJOR CONTRIBUTIONS TO GEOLOGY IN THE TWENTIETH CENTURY SE Geological Society Special Publication LA English DT Proceedings Paper CT 31st International Geological Congress CY AUG 16-18, 2000 CL RIO DE JANEIRO, BRAZIL SP Int Commiss Hist Geol Sci, IGCP 404, INQUA ID PRIMITIVE METEORITES; LUNAR PROSPECTOR; SILICON-CARBIDE; IMPACT CRATER; CATACLYSM; DIAMOND; HISTORY; GRAINS; MOON; ROCK AB Since the opening of the Space Age, images from spacecraft have enabled us to map the surfaces of all the rocky planets and satellites in the Solar System, thus transforming them from astronomical to geological objects. This progression of geology from being a strictly Earth-centred science to one that is planetary-wide has provided us with a wealth of information on the evolutionary histories of other bodies and has supplied valuable new insights on the Earth itself. We have learned, for example, that the Earth-Moon system most likely formed as a result of a collision in space between the protoearth and a large impactor, and that the Moon subsequently accreted largely from debris of Earth's mantle. The airless, waterless Moon still preserves a record of the impact events that have scarred its surface from the time its crust first formed. The much larger, volcanic Earth underwent a similar bombardment but most of the evidence was lost during the earliest 550 million years or so that elapsed before its first surviving systems of crustal rocks formed. Therefore, we decipher Earth's earliest history by investigating the record on the Moon. Lunar samples collected by the Apollo astronauts of the USA and the robotic Luna missions of the former USSR linked the Earth and Moon by their oxygen isotopic compositions and enabled us to construct a timescale of lunar events keyed to dated samples. They also permitted us to identify certain meteorites as fragments of the lunar crust that were projected to the Earth by impacts on the Moon. Similarly, analyses of the Martian surface soils and atmosphere by the Viking and Pathfinder missions led to the identification of meteorite fragments ejected by hypervelocity impacts on Mars. Images of Mars displayed landforms wrought in the past by voluminous floodwaters, similar to those of the long-controversial Channeled Scablands of Washington State, USA. The record on Mars confirmed catastrophic flooding as a significant geomorphic process on at least one other planet. The first views of the Earth photographed by the crew of Apollo 8 gave us the concept of 'Spaceship Earth' and heightened international concern for protection of the global environment. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marvin, UB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 116 TC 3 Z9 3 U1 3 U2 4 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0305-8719 BN 1-86239-096-7 J9 GEOL SOC SPEC PUBL PY 2002 VL 192 BP 17 EP 57 DI 10.1144/GSL.SP.2002.192.01.03 PG 41 WC Geology SC Geology GA BU36N UT WOS:000175779100002 ER PT J AU Cochran, A Veverka, J Bell, J Belton, M Benkhoff, J Cheng, A Clark, B Feldman, P Kissel, J Mahaffy, P Malin, M Murchie, S Neimann, H Owen, T Robinson, M Schwehm, G Squyres, S Thomas, P Whipple, F Yeomans, D AF Cochran, A Veverka, J Bell, J Belton, M Benkhoff, J Cheng, A Clark, B Feldman, P Kissel, J Mahaffy, P Malin, M Murchie, S Neimann, H Owen, T Robinson, M Schwehm, G Squyres, S Thomas, P Whipple, F Yeomans, D TI The COmet Nucleus TOUR (CONTOUR) - A NASA discovery mission SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT IAU Colloquium No 186 on Cometary Science after Hale-Bopp CY JAN 21-25, 2002 CL CANARY ISL, SPAIN SP Int Astronom Union DE comets; missions AB In 1997, the COmet Nucleus TOUR ( CONTOUR) was selected by NASA for a new start as part of the Discovery line. In this paper, we review the status of the mission, the mission timeline and the instruments to be flown. Detail is given of the science goals and how they are to be accomplished. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Cornell Univ, Ithaca, NY 14853 USA. Belton Space Explorat Initiat LLC, Tucson, AZ 85716 USA. Inst Space Sensor & Planetary Explorat, D-12489 Berlin, Germany. Johns Hopkins APL, Laurel, MD 20723 USA. Lockheed Martin, Denver, CO 80201 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. MPI Astrophys, D-85741 Garching, Germany. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. Malin Space Sci, San Diego, CA 92191 USA. Astron Inst, Honolulu, HI 96822 USA. Northwestern Univ Geol Sco, Evanston, IL 60208 USA. European Space Agcy, Dept Space Sci, SO Div, Estec, NL-2200 AG Noordwijk, Netherlands. Cornell Univ, Ithaca, NY 14853 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cochran, A (reprint author), Univ Texas, Dept Astron, RLM 15308, Austin, TX 78712 USA. RI Mahaffy, Paul/E-4609-2012; Murchie, Scott/E-8030-2015 OI Murchie, Scott/0000-0002-1616-8751 NR 0 TC 1 Z9 1 U1 0 U2 1 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 PY 2002 VL 89 IS 1-4 BP 289 EP 300 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 622RG UT WOS:000179660300014 ER PT J AU Brown, ED Hopkins, MJG AF Brown, ED Hopkins, MJG TI Tests of disperser specificity between frugivorous birds and rainforest fruits in New Guinea SO EMU LA English DT Article ID SUBTROPICAL RAIN-FORESTS; SEED DISPERSAL; FEEDING ECOLOGY; SIZE; COEVOLUTION; QUEENSLAND; COMMUNITY; AUSTRALIA; EXAMPLES; PARADISE AB Interactions between frugivorous birds and their food plants were studied in tropical lowland hill forest in Papua New Guinea. Over a 2-year period we made intensive observations at 20 fruiting tree species in order to determine avian feeding assemblages at each species. In all, 38 bird species took fruit during observations, mainly in the families Paradisaeidae, Columbidae, Meliphagidae, Campephagidae, Dicaeidae, Zosteropidae, and Pachycephalidae. We tested specificity of bird-plant interactions by examining various statistical associations between bird and plant characteristics to identify key factors in consistent patterns of fruit consumption, if any. Bird families were significantly associated with different types of fruits: cuckoo-shrikes, thickheads and honeyeaters visited figs more often than expected, and birds of paradise and white-eyes visited arillate fruits more often than expected. In other tests, number of visits to very small fruits 5-6.5 mm in diameter (which included several fig species) was correlated with birds ranked by size, especially for berrypeckers, flowerpeckers and white-eyes. However, for both smaller and larger fruits, or for fruits of different structure or accessibility, there was no correlation with bird size. Fruit size showed no correlation with avian food-handling behaviour, or with avian taxonomic affinity. Size of fruiting display was not correlated with either avian residency or nomadism. Our study provided an overview of most of the avian frugivore species at the study site, which fed at a wide array of fruiting plants, and thus our results give an indication of whether patterns in bird-plant relationships are discernible at the level of species, family or guild, or other ecological subset, and whether determining factors might be morphology, size, bird behaviour, etc. These results also provide a broader context within which other regional studies of bird-plant relationships can be interpreted, and were consistent with some, but not all, of the conclusions of previous studies that suggested specialised relationships between Australo-Papuan birds and fruiting plants. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. Univ Papua New Guinea, Dept Biol, Waigani, Papua N Guinea. RP Brown, ED (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. NR 36 TC 8 Z9 9 U1 4 U2 15 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0158-4197 J9 EMU JI Emu PY 2002 VL 102 IS 2 BP 137 EP 146 DI 10.1071/MU00082 PG 10 WC Ornithology SC Zoology GA 571XG UT WOS:000176744000002 ER PT J AU Vann, CD Megonigal, JP AF Vann, CD Megonigal, JP TI Productivity responses of Acer rubrum and Taxodium distichum seedlings to elevated CO2 and flooding SO ENVIRONMENTAL POLLUTION LA English DT Article; Proceedings Paper CT Advances in Terrestrial Ecosystem: Carbon Inventory Measurements and Monitoring Conference CY OCT 03-05, 2000 CL RALEIGH, NORTH CAROLINA DE elevated CO2; wetlands; tree seedlings; productivity; Taxodium distichum; Acer rubrum ID BALD CYPRESS; FOREST; ENRICHMENT; GROWTH AB Elevated levels of atmospheric CO2 are expected to increase photosynthetic rates Of C-3 tree species, but it is uncertain whether this will result in an increase in wetland seedling productivity. Separate short-term experiments (12 and 17 weeks) were performed on two wetland tree species, Taxodium distichum and Acer rubrum, to determine if elevated CO2 would influence the biomass responses of seedlings to flooding. T. distichum were grown in replicate glasshouses (n = 2) at CO2 concentrations of 350 or 700 ppm, and A. rubrum were grown in growth chambers at CO2 concentrations of 422 or 722 ppm. Both species were grown from seed. The elevated CO2 treatment was crossed with two water table treatments, flooded and non-flooded. Elevated CO2 increased leaf-level photosynthesis, whole-plant photosynthesis, and trunk diameter of T. distichum in both flooding treatments, but did not increase biomass of T. distichum or A. rubrum. Flooding severely reduced biomass, height, and leaf area of both T. distichum and A. rubrum. Our results suggest that the absence of a CO2-induced increase in growth may have been due to an 02 limitation on root production even though there was a relatively deep (similar to10 cm) aerobic soil surface in the non-flooded treatment. (C) 2001 Elsevier Science Ltd. All rights reserved. C1 US Dept Interior, US Geol Survey, Reston, VA 20192 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. George Mason Univ, Fairfax, VA 22030 USA. RP Vann, CD (reprint author), US Dept Interior, US Geol Survey, MS 926A, Reston, VA 20192 USA. NR 22 TC 11 Z9 11 U1 1 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0269-7491 J9 ENVIRON POLLUT JI Environ. Pollut. PY 2002 VL 116 SU 1 BP S31 EP S36 DI 10.1016/S0269-7491(01)00244-5 PG 6 WC Environmental Sciences SC Environmental Sciences & Ecology GA 511XU UT WOS:000173291500005 PM 11833915 ER PT J AU Panger, MA Brooks, AS Richmond, BG Wood, B AF Panger, MA Brooks, AS Richmond, BG Wood, B TI Older than the oldowan? Rethinking the emergence of hominin tool use SO EVOLUTIONARY ANTHROPOLOGY LA English DT Review DE stone tools; primate tool use; hominid evolution ID BONOBO PAN-PANISCUS; HUMAN-EVOLUTION; OLDUVAI-GORGE; CEBUS MONKEYS; STONE TOOLS; AUSTRALOPITHECUS-AFARENSIS; MECHANICAL FORCES; WILD CHIMPANZEES; HAND PREFERENCE; GREAT APES AB Intentionally modified stone tools first appear in the hominin archeological record about 2.5 mya. Their appearance has been variously interpreted as marking the onset of tool use by hominins or, less restrictively, the origin of hominin lithic technology.(1,2) Although the 2.5 mya date has persisted for two decades, several related but distinct questions about the origin and evolution of hominin tool use remain to be answered: Did hominins use tools before 2.5 mya? Did hominins use unmodified stones as tools before 2.5 mya? Does the earliest appearance of stone tools in the archeological record represent the earliest use of intentionally modified stones as tools?. C1 George Washington Univ, Dept Anthropol, Washington, DC USA. George Washington Univ, Ctr Adv Study Human Paleobiol, Washington, DC USA. Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 104 TC 100 Z9 104 U1 6 U2 62 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 1060-1538 J9 EVOL ANTHROPOL JI Evol. Anthropol. PY 2002 VL 11 IS 6 BP 235 EP 245 DI 10.1002/evan.10094 PG 11 WC Anthropology SC Anthropology GA 632WU UT WOS:000180247500006 ER PT S AU Stark, AA AF Stark, AA BE DePetris, M Gervasi, M TI Millimeter and submillimeter observations from the South Pole SO EXPERIMENTAL COSMOLOGY AT MILLIMETRE WAVELENGTHS SE AIP Conference Proceedings LA English DT Proceedings Paper CT Breuil-Cervinia Workshop on Experimental Cosmology at Millimetre Wavelengths CY JUL 09-13, 2001 CL BRUIL-CERVINIA, ITALY SP Rivoira, Agilent Technol, Tektronix, QMC Instruments Ltd, Superelect, Ist San Paolo Torino ID MICROWAVE BACKGROUND ANISOTROPY; INTEGRATED GALACTIC EMISSION; ANGULAR SCALES; ATMOSPHERIC OPACITY; 90 GHZ; SKY; RECEIVER; SEARCH; DESIGN; MIXERS AB During the past decade, a year-round observatory has been established at the geographic South Pole by the Center for Astrophysical Research in Antarctica (CARA). CARA has fielded several millimeter- and submillimeter-wave instruments: AST/RO (the Antarctic Submillimeter Telescope and Remote Observatory, a 1.7-m telescope outfitted with a variety of receivers at frequencies from 230 GHz to 810 GHz, including PoleSTAR, a heterodyne spectrometer array), Python (a degree-scale CMB telescope), Viper (a 2-m telescope which has been outfitted with SPARO, a submillimeter-wave bolometric array polarimeter, ACBAR, a multi-channel CMB instrument, and Dos Equis, a HEMT polarimeter), and DASI (the Degree-Angular Scale Interferometer). These instruments have obtained significant results in studies of the interstellar medium and observational cosmology, including detections of the 1degrees acoustic peak in the CMB and the Sunyaev-Zel'dovich effect. The South Pole environment is unique among observatory sites for unusually low wind speeds, low absolute humidity, and the consistent clarity of the submillimeter sky. The atmosphere is dessicated by cold: at the South Pole's average annual temperature of -49 C, the partial pressure of saturated water vapor is only 1.2% of what it is at 0 C. The low water vapor levels result in exceptionally low values of sky noise. This is crucial for large-scale observations of faint cosmological sources-for such observations the South Pole is unsurpassed. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Stark, AA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 66 TC 3 Z9 3 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 0-7354-0062-8 J9 AIP CONF PROC PY 2002 VL 616 BP 83 EP 91 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU75M UT WOS:000176917100014 ER PT S AU Perrett, K Bridges, T Hanes, D Irwin, M Carter, D Brodie, J Huchra, J Watson, F AF Perrett, K Bridges, T Hanes, D Irwin, M Carter, D Brodie, J Huchra, J Watson, F BE Geisler, D Grebel, EK Minniti, D TI The globular clusters of M31: Keys to its formation history SO EXTRAGALACTIC STAR CLUSTERS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Extragalactic Star Clusters CY MAR 12-16, 2001 CL PUCON, CHILE SP Int Astronom Union ID GALAXIES; MASS; HALO; SYSTEM AB With the ultimate goal of distinguishing between various models describing the formation of galaxy halos (e.g., radial collapse, chaotic mergers), we present the results of a spectroscopic study of the globular cluster system of M31. We have obtained deep, intermediate-resolution spectra for several hundred of the M31 globular clusters using the WYFFOS fibre-fed spectrograph at the William Herschel Telescope. These observations have yielded precise radial velocities and metallicities for over 200 members of the M31 globular cluster population, the vast majority of which represent new data or significant improvements over pre-existing data. C1 Queens Univ, Dept Phys, Kingston, ON K7L 3N6, Canada. Anglo Australian Observ, Epping, NSW 1710, Australia. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Liverpool JMU, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Anglo Australian Observ, Coonabarabran, NSW 2357, Australia. RP Perrett, K (reprint author), Queens Univ, Dept Phys, Kingston, ON K7L 3N6, Canada. NR 19 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 1-58381-115-X J9 IAU SYMP PY 2002 VL 207 BP 52 EP 57 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV57N UT WOS:000179397100006 ER PT S AU Barmby, P AF Barmby, P BE Geisler, D Grebel, EK Minniti, D TI M31 globular cluster metallicities and ages SO EXTRAGALACTIC STAR CLUSTERS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Extragalactic Star Clusters CY MAR 12-16, 2001 CL PUCON, CHILE SP Int Astronom Union ID LUMINOSITY FUNCTION; COLORS AB Globular cluster ages are more than just lower limits to the age of the universe; the distribution of ages constraints the timescales for galaxy formation and chemical evolution. Globular cluster populations with different metallicities have now been detected in many galaxies, and understanding how these populations formed requires knowing their relative ages. We examined the relative ages of the two M31 globular cluster populations using their color and luminosity distributions and found that the metal-rich clusters could be up to 50% younger than the metal-poor clusters. While a small delay in the formation of metal-rich clusters might be imposed by chemical enrichment timescales, a large age gap demands a more detailed explanation. I outline several possibilities and their promises and problems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barmby, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mailstop 10, Cambridge, MA 02138 USA. NR 14 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-115-X J9 IAU SYMP PY 2002 VL 207 BP 58 EP 61 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV57N UT WOS:000179397100007 ER PT S AU Olsen, K Miller, B Schommer, R Suntzeff, N Bright, J AF Olsen, K Miller, B Schommer, R Suntzeff, N Bright, J BE Geisler, D Grebel, EK Minniti, D TI The globular cluster systems of the Sculptor Group SO EXTRAGALACTIC STAR CLUSTERS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT Symposium on Extragalactic Star Clusters CY MAR 12-16, 2001 CL PUCON, CHILE SP Int Astronom Union ID LARGE-MAGELLANIC-CLOUD; STAR-CLUSTERS; LMC CLUSTERS; SPECTROSCOPY; KINEMATICS; GALAXIES; NGC-55; SEARCH; GIANTS AB We present results from a study to identify the globular cluster systems of six of the brightest galaxies of the Sculptor Group. From Mosaic II CMR images of the area surrounding the galaxies NGC 45, NGC 55, NGC 247, NGC 253, NGC 300, and NGC 7793, we identify cluster candidates through their morphology, luminosity, and color. We show that many of the Milky Way's globular clusters would appear extended in our images if placed in the Sculptor Group; only in the two most distant galaxies, NGC 45 and NGC 7793, is the discrimination difficult. We find 50-100 candidates per galaxy with integrated properties similar to Milky Way clusters. Published spectroscopic identifications of candidates in NGC 253 lead us to expect that similar to50% of the candidates are true clusters, while the remainder are background galaxies. Study of the Sculptor Group galaxies increases the sample of late-type spiral and Magellanic-type galaxies with known globular cluster systems from 2 to similar to10. C1 Cerro Tololo Interamer Observ, La Serena, Chile. AURA, Gemini Observ, La Serena, Chile. AURA, US Gemini Project Off, La Serena, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Olsen, K (reprint author), Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. NR 15 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 1-58381-115-X J9 IAU SYMP PY 2002 VL 207 BP 275 EP 280 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV57N UT WOS:000179397100055 ER PT S AU Sternberg, RV AF Sternberg, RV BE VanSpeybroeck, L VandeVijver, G DeWaele, D TI On the roles of repetitive DNA elements in the context of a unified genomic-epigenetic system SO FROM EPIGENESIS TO EPIGENETICS: THE GENOME IN CONTEXT SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Contextualizing the Genome - The Role of Epigenetics in Genetics, Development and Evolution CY NOV 25-28, 2001 CL GHENT, BELGIUM SP Res Community Evolut & Complex (FWO Flanders) DE repetitive DNA; selfish DNA; genomes; neo-Darwinism; epigenetics; theoretical biology ID DROSOPHILA-MELANOGASTER; TRANSPOSABLE ELEMENTS; GENE-REGULATION; I-FACTOR; HYBRID DYSGENESIS; STRESS INDUCTION; READING FRAMES; NONCODING RNAS; CONTROL REGION; L1 ELEMENTS AB Repetitive DNA sequences comprise a substantial portion of most eukaryotic and some prokaryotic chromosomes. Despite nearly forty years of research, the functions of various sequence families as a whole and their monomer units remain largely unknown. The inability to map specific functional roles onto many repetitive DNA elements (RIES), coupled with the taxon-specificity of sequence families, have led many to speculate that these genomic components are "selfish" replicators generating genomic "junk." The purpose of this paper is to critically examine the selfishness, evolutionary effects, and functionality of REs. First, a brief overview of the range of ideas pertaining to RE function is presented. Second, the argument is presented that the selfish DNA "hypothesis" is actually a narrative scheme, that it serves to protect neo-Darwinian assumptions from criticism, and that this story is untestable and therefore not a hypothesis. Third, attempts to synthesize the selfish DNA concept with complex systems models of the genome and RE functionality are critiqued. Fourth, the supposed connection between RE-induced mutations and macro-evolutionary events are stated to be at variance with empirical evidence and theoretical considerations. Hypotheses that base phylogenetic transitions in repetitive sequence changes thus remain speculative. Fifth and finally, the case is made for viewing RIES as integrally functional components of chromosomes, genomes, and cells. It is argued throughout that a new conceptual framework is needed for understanding the roles of repetitive DNA in genomic/epigenetic systems, and that neo-Darwinian "narratives" have been the primary obstacle to elucidating the effects of these enigmatic components of chromosomes. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Syst Biol, Washington, DC 20560 USA. RP Sternberg, RV (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Syst Biol, NHB 163, Washington, DC 20560 USA. NR 138 TC 15 Z9 17 U1 2 U2 4 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-424-2 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2002 VL 981 BP 154 EP 188 PG 35 WC Biochemistry & Molecular Biology; Evolutionary Biology; Multidisciplinary Sciences SC Biochemistry & Molecular Biology; Evolutionary Biology; Science & Technology - Other Topics GA BW05H UT WOS:000180751600009 ER PT J AU Krom, MD Stanley, JD Cliff, RA Woodward, JC AF Krom, MD Stanley, JD Cliff, RA Woodward, JC TI Nile River sediment fluctuations over the past 7000 yr and their key role in sapropel development SO GEOLOGY LA English DT Article DE paleoclimate; Nile catchment; Sr-87/Sr-86; sediment provenance; sapropels; primary productivity ID SURFACE SEDIMENTS; LEVANTINE BASIN; EASTERN; PRODUCTIVITY; PHOSPHORUS; SUBSIDENCE; SEA AB The provenance pattern of Nile River sediments can be used as a proxy for paleoclimatic changes in East Africa. The Sr-87/Sr-86 ratios are particularly appropriate for such provenance investigations, because the White Nile drains predominantly crystalline basement rocks, whereas the Blue Nile and Atbara flow off the Ethiopian Highlands, which consist of Tertiary volcanic rocks. A high-resolution profile of Sr-87/Sr-86 and Ti/Al ratios from a well-dated core in the Nile Delta shows a close correspondence with known changes in Nile flow over the past 7000 yr. At times of higher river flow there was markedly decreased input of Blue Nile-derived and total sediment. This change was caused by northward movement of the Inter Tropical Convergence Zone, resulting in increased vegetative cover in the Ethiopian Highlands due to higher rainfall and a longer wet season. This inverse relationship between Nile River flow and sediment flux may have had important implications in the development of agricultural technology in ancient Egypt. The marked minimum in Sr-87/Sr-86 at 4200-4500 yr B.P. is coincident with the end of the Old Kingdom in Egypt and provides independent evidence that demise of the Old Kingdom might have been associated with an extended period of catastrophic low floods. During the Quaternary and late Neogene, there was periodic deposition of organic-rich sediments (sapropels) in the eastern Mediterranean that represent important indicators of major environmental change. Evidence from the Ti/Al ratio suggests that the pattern of erosion and sediment supply from the Nile catchment observed in this study also occurred throughout much of the Neogene and Quaternary. The reduced inputs of Blue Nile sediment during times of sapropel formation contributed to the increased primary productivity by reducing the amount of phosphate removed on particles and to the observed change to N limitation in the eastern Mediterranean, which are important characteristics of sapropel deposition. C1 Univ Leeds, Sch Earth Sci, Leeds LS2 9JT, W Yorkshire, England. Smithsonian Inst, Deltas Global Change Program, Washington, DC 20560 USA. Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. RP Krom, MD (reprint author), Univ Leeds, Sch Earth Sci, Leeds LS2 9JT, W Yorkshire, England. NR 30 TC 89 Z9 91 U1 4 U2 30 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD JAN PY 2002 VL 30 IS 1 BP 71 EP 74 DI 10.1130/0091-7613(2002)030<0071:NRSFOT>2.0.CO;2 PG 4 WC Geology SC Geology GA 515KR UT WOS:000173495200018 ER PT J AU Dijkstra, P Hymus, G Colavito, D Vieglais, DA Cundari, CM Johnson, DP Hungate, BA Hinkle, CR Drake, BG AF Dijkstra, P Hymus, G Colavito, D Vieglais, DA Cundari, CM Johnson, DP Hungate, BA Hinkle, CR Drake, BG TI Elevated atmospheric CO2 stimulates aboveground biomass in a fire-regenerated scrub-oak ecosystem SO GLOBAL CHANGE BIOLOGY LA English DT Article DE elevated CO2; biomass; Florida scrub; Quercus myrtifolia; Q. chapmanii; Q. geminata; natural forest ID RESPONSES; FOREST; ENRICHMENT; GROWTH; COMMUNITY; GRASSLAND; EXPOSURE; PLANTS; MARSH; TREE AB The effect of elevated atmospheric CO2 concentration (C-a) on the aboveground biomass of three oak species, Quercus myrtifolia, Q. geminata, and Q. chapmanii, was estimated nondestructively using allometric relationships between stem diameter and aboveground biomass after four years of experimental treatment in a naturally fire-regenerated scrub-oak ecosystem. After burning a stand of scrub-oak vegetation, re-growing plants were exposed to either current ambient (379 muL L-1 CO2) or elevated (704 muL L-1 CO2) C-a in 16 open-top chambers over a four-year period, and measurements of stem diameter were carried out annually on all oak shoots within each chamber. Elevated C,, significantly increased aboveground biomass, expressed either per unit ground area or per shoot; elevated C. had no effect on shoot density. The relative effect of elevated Ca on aboveground biomass increased each year of the study from 44% (May 96-Jan 97), to 55% (Jan 97-Jan 98), 66% (Jan 98-Jan 99), and 75% (Jan 99-Jan 00). The effect of elevated C-a was species specific: elevated C-a significantly increased aboveground biomass of the dominant species, Q. myrtifolia, and tended to increase aboveground biomass of Q. chapmanii, but had no effect on aboveground biomass of the subdominant, Q. geminata. These results show that rising atmospheric CO2 has the potential to stimulate aboveground biomass production in ecosystems dominated by woody species, and that species-specific growth responses could, in the long term, alter the composition of the scrub-oak community. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Dynam Corp, Kennedy Space Ctr, FL 32899 USA. Natl Acad Sci, Washington, DC 20418 USA. No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. RP Drake, BG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Hungate, Bruce/F-8991-2011; Vieglais, Dave/C-7356-2009 OI Hungate, Bruce/0000-0002-7337-1887; Vieglais, Dave/0000-0002-6513-4996 NR 40 TC 64 Z9 73 U1 0 U2 11 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 JAN PY 2002 VL 8 IS 1 BP 90 EP 103 DI 10.1046/j.1354-1013.2001.00458.x PG 14 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 515WA UT WOS:000173518600006 ER PT S AU Esser, R Edgar, RJ AF Esser, R Edgar, RJ BE BelyDubau, F TI Constraints on ion outflow speeds and electron distribution function in the corona derived from SUMER electron temperatures and SWICS ion fractions SO HEATING AND ENERGETICS OF THE SOLAR CORONA AND SOLAR WIND SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT E2 1-D2 3 Symposium of COSPAR Scientific Commission E held at the 33rd COSPAR Scientific Assembly CY JUL, 2000 CL WARSAW, MASSACHUSETTS SP CNES, European Space Agcy, Inst Space & Astronaut Sci, Comm Space Res ID SOLAR-WIND; PHYSICAL-PROPERTIES; INNER CORONA; HOLE; ULYSSES; COEFFICIENTS; IONIZATION; ATOMS; SOHO AB It has been a puzzle for quite some time that spectroscopic measurements in the inner corona indicate electron temperatures far too low to produce the ion fractions observed in the in situ solar wind. In the present paper we show that in order to reconcile the two sets of measurements, a number of conditions have to exist in the inner corona: 1) the electron distribution function has to be Maxwellian or close to Maxwellian close to the coronal base; 2) the non-Maxwellian character of the distribution has to develop rapidly as a function of height and has to reach close to interplanetary properties inside of a few solar radii; 3) ions of different elements have to flow with significantly different speeds to separate their "freezing-in" distances sufficiently so they can encounter different distribution functions. We chose a set of observationally constrained coronal plasma parameters to demonstrate that these conditions are general requirements if both coronal electron temperatures and in situ ion fractions axe correct. However, the details of the required distribution functions are very sensitive to the exact electron temperature, density and ion flow speed profiles in the region of the corona where the ions predominantly form. (C) 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Esser, R (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 32 TC 4 Z9 4 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2002 VL 30 IS 3 BP 481 EP 486 AR PII S0273-1177(02)00321-6 DI 10.1016/S0273-1177(02)00321-6 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BV25S UT WOS:000178339400009 ER PT S AU Marsden, BG AF Marsden, BG BE Rickman, H TI The exploration of the transneptunian population SO HIGHLIGHTS OF ASTRONOMY, VOL 12 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID OUTER SOLAR-SYSTEM AB The recognition of the extensive population of bodies in the outer Solar System has been arguably the most significant discovery about the Solar System from groundbased observations during the twentieth century. Our understanding of the transneptunian population is still quite flawed in its details, although a plausible picture has been emerging. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marsden, BG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-086-2 J9 IAU SYMP PY 2002 VL 12 BP 189 EP 192 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV30K UT WOS:000178493500051 ER PT S AU Wilner, DJ AF Wilner, DJ BE Rickman, H TI A joint discussion on the topic of cold gas and dust at high redshift SO HIGHLIGHTS OF ASTRONOMY, VOL 12 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilner, DJ (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 1-58381-086-2 J9 IAU SYMP PY 2002 VL 12 BP 455 EP 455 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV30K UT WOS:000178493500129 ER PT S AU Forman, W Donnelly, H Markevitch, M Kraft, R Murray, S Vikhlinin, A Churazov, E David, L Jones, C AF Forman, W Donnelly, H Markevitch, M Kraft, R Murray, S Vikhlinin, A Churazov, E David, L Jones, C BE Rickman, H TI Chandra observations of clusters of galaxies SO HIGHLIGHTS OF ASTRONOMY, VOL 12 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union AB We discuss two themes from Chandra cluster observations. First, we describe the interaction of buoyant, radio emitting plasma bubbles with the hot intracluster gas. Second we summarize the Chandra observations of "cold" fronts (sharp discontinuities in gas density and temperature) separating cool, denser gas clouds from the hotter intracluster medium. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow Space Res Inst, Moscow 117810, Russia. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Forman, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Churazov, Eugene/A-7783-2013; OI Forman, William/0000-0002-9478-1682 NR 16 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 1-58381-086-2 J9 IAU SYMP PY 2002 VL 12 BP 504 EP 506 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV30K UT WOS:000178493500142 ER PT S AU Reid, MJ AF Reid, MJ BE Rickman, H TI The magnetic field of the Milky Way SO HIGHLIGHTS OF ASTRONOMY, VOL 12 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID PULSAR ROTATION MEASURES; GALAXY; MASERS AB Models of the magnetic field configuration of the Milky Way are reviewed. Current analyses of rotation measure data suggest that the Milky Way possesses a bisymmetric-like spiral magnetic field, that field reversals among spiral arms exist, and that the magnetic spiral may not closely match the mass spiral structure. Zeeman measurements of OH masers may provide alternative magnetic field information. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-086-2 J9 IAU SYMP PY 2002 VL 12 BP 716 EP 718 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV30K UT WOS:000178493500193 ER PT S AU Blackman, EG Field, GB AF Blackman, EG Field, GB BE Rickman, H TI Mean field dynamo saturation: Toward understanding conflicting results SO HIGHLIGHTS OF ASTRONOMY, VOL 12 SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID ALPHA AB Mean field dynamos may explain the origin of large scale magnetic fields of galaxies, but controversy arises over the extent of dynamo quenching by the growing field. Here we explain how apparently conflicting results may be mutually consistent, by showing the role of magnetic helicity conservation and boundary terms usually neglected. We estimate the associated magnetic energy flowing out of the Galaxy but emphasize that the mechanism of field escape needs to be addressed. C1 Univ Rochester, Dept Phys & Astron, 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 16 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 1-58381-086-2 J9 IAU SYMP PY 2002 VL 12 BP 736 EP 738 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BV30K UT WOS:000178493500201 ER PT J AU Olin, JS Blackman, MJ Mitchern, JE Waselkov, GA AF Olin, JS Blackman, MJ Mitchern, JE Waselkov, GA TI Compositional analysis of glazed earthenwares from eighteenth-century sties on the northern Gulf Coast SO HISTORICAL ARCHAEOLOGY LA English DT Article ID CERAMICS AB Compositional classification of colonial-era ceramics using neutron activation analysis has heretofore focused primarily on majolicas from Spain and Mexico. In order to expand the chemical database to include 18th-century French ceramics, 186 sherds from Old Mobile and nearby sites on the north-central Gulf Coast have been analyzed, including faience blanche, faience brune, Mexican majolicas, and several types of coarse earthenware. Quantitative analysis of 23 elements provides a basis for distinguishing French and Spanish-colonial earthenwares, as well as suggesting some preliminary chemical groupings of French faience. C1 Smithsonian Ctr Materials Res & Educ, Sutland, MD 20746 USA. Univ S Alabama, Ctr Archaeol Studies, Mobile, AL 36688 USA. RP Blackman, MJ (reprint author), Smithsonian Ctr Materials Res & Educ, Sutland, MD 20746 USA. NR 40 TC 1 Z9 1 U1 0 U2 1 PU SOC HISTORICAL ARCHAEOLOGY PI TUCSON PA PO BOX 30446, TUCSON, AZ 85751-0446 USA SN 0440-9213 J9 HIST ARCHAEOL JI Hist. Archaeol. PY 2002 VL 36 IS 1 BP 79 EP 96 PG 18 WC Archaeology SC Archaeology GA 532AZ UT WOS:000174450600008 ER PT J AU Billeck, WT AF Billeck, WT TI Trade beads from archeological excavations at Fort Union Trading Post National Historic Sites SO HISTORICAL ARCHAEOLOGY LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Billeck, WT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC HISTORICAL ARCHAEOLOGY PI TUCSON PA PO BOX 30446, TUCSON, AZ 85751-0446 USA SN 0440-9213 J9 HIST ARCHAEOL JI Hist. Archaeol. PY 2002 VL 36 IS 2 BP 133 EP 133 PG 1 WC Archaeology SC Archaeology GA 568BQ UT WOS:000176522900014 ER PT B AU Allison, DK AF Allison, DK BE Hashagen, U KeilSlawik, R Norberg, AL TI Preserving software in history museums: A material culture approach SO HISTORY OF COMPUTING: SOFTWARE ISSUES LA English DT Proceedings Paper CT International Conference on the History of Computing (ICHC 2000) CY APR 05-07, 2000 CL PADERBORN, GERMANY SP Heinz Nixdorf MuseumsForum, Charles Babbage Inst, Univ Paderborn, Heinz Nixdorf Inst C1 Natl Museum Amer Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Allison, DK (reprint author), Natl Museum Amer Hist, Smithsonian Inst, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-42664-7 PY 2002 BP 263 EP 272 PG 10 WC Computer Science, Software Engineering; History & Philosophy Of Science SC Computer Science; History & Philosophy of Science GA BV02S UT WOS:000177648100028 ER PT B AU DeVorkin, D AF DeVorkin, D BE Ansari, SMR TI Toshio Takamine's contact with western astrophysics SO HISTORY OF ORIENTAL ASTRONOMY SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT 23rd General Assembly of the International-Astronomical-Union CY AUG 22-23, 1997 CL KYOTO, JAPAN SP Int Astron Union C1 Smithsonian Inst, Washington, DC 20560 USA. NR 47 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-0657-8 J9 ASTROPHYS SPACE SC L PY 2002 VL 274 BP 145 EP 157 PG 13 WC History & Philosophy Of Science SC History & Philosophy of Science GA BW42C UT WOS:000181949900012 ER PT B AU Fitzhugh, WW Loring, S AF Fitzhugh, WW Loring, S BE Fitzhugh, WW Loring, S Odess, D TI Honouring our elders - A history of Eastern Artic archeology - Introduction SO HONORING OUR ELDERS: A HISTORY OF EASTERN ARCTIC ARCHAEOLOGY SE CONTRIBUTIONS TO CIRCUMPOLAR ANTHROPOLOGY LA English DT Proceedings Paper CT Eastern Arctic Archaeology Elders Conference held in Honor of Elmer Harp CY APR 22-24, 1993 CL Dartmouth Coll, Hannover, NH HO Dartmouth Coll ID CENTRAL LABRADOR COAST; RADIOCARBON TIME SCALE; NORTHERN LABRADOR; SOCIAL-ORGANIZATION; POLLEN DIAGRAMS; HAMILTON INLET; ARCTIC CANADA; ARCHEOLOGICAL INVESTIGATIONS; ESKIMO OCCUPATIONS; ELLESMERE-ISLAND C1 Smithsonian Inst, Natl Museum Nat Hist, Arct Studies Ctr, Washington, DC USA. NR 1136 TC 4 Z9 4 U1 1 U2 5 PU ARCTIC STUDIES CENTER PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY, DEPT ANTHROPOLOGY, 10TH CONSTITUTION AVE., NW, WASHINGTON, DC 20013-7012 USA BN 0-9673429-2-9 J9 CONTRIB CIRCUMPOL AN PY 2002 VL 2 BP 1 EP + PG 68 WC Archaeology; History Of Social Sciences SC Archaeology; Social Sciences - Other Topics GA BAJ47 UT WOS:000222550400001 ER PT B AU Fitzhugh, WW AF Fitzhugh, WW BE Fitzhugh, WW Loring, S Odess, D TI Nukasusutok 2 and the paleoskimo tradition in Labrador SO HONORING OUR ELDERS: A HISTORY OF EASTERN ARCTIC ARCHAEOLOGY SE CONTRIBUTIONS TO CIRCUMPOLAR ANTHROPOLOGY LA English DT Proceedings Paper CT Eastern Arctic Archaeology Elders Conference held in Honor of Elmer Harp CY APR 22-24, 1993 CL Dartmouth Coll, Hannover, NH HO Dartmouth Coll C1 Smithsonian Inst, Natl Museum Nat Hist, Arct Studies Ctr, Washington, DC USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ARCTIC STUDIES CENTER PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY, DEPT ANTHROPOLOGY, 10TH CONSTITUTION AVE., NW, WASHINGTON, DC 20013-7012 USA BN 0-9673429-2-9 J9 CONTRIB CIRCUMPOL AN PY 2002 VL 2 BP 133 EP 162 PG 30 WC Archaeology; History Of Social Sciences SC Archaeology; Social Sciences - Other Topics GA BAJ47 UT WOS:000222550400013 ER PT B AU Loring, S AF Loring, S BE Fitzhugh, WW Loring, S Odess, D TI "And they took away the stones from Ramah": Lithic raw material sourcing and eastern artic archaeology SO HONORING OUR ELDERS: A HISTORY OF EASTERN ARCTIC ARCHAEOLOGY SE CONTRIBUTIONS TO CIRCUMPOLAR ANTHROPOLOGY LA English DT Proceedings Paper CT Eastern Arctic Archaeology Elders Conference held in Honor of Elmer Harp CY APR 22-24, 1993 CL Dartmouth Coll, Hannover, NH HO Dartmouth Coll C1 Smithsonian Inst, Natl Museum Nat Hist, Arct Studies Ctr, Washington, DC USA. NR 2 TC 6 Z9 6 U1 0 U2 0 PU ARCTIC STUDIES CENTER PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY, DEPT ANTHROPOLOGY, 10TH CONSTITUTION AVE., NW, WASHINGTON, DC 20013-7012 USA BN 0-9673429-2-9 J9 CONTRIB CIRCUMPOL AN PY 2002 VL 2 BP 163 EP 185 PG 23 WC Archaeology; History Of Social Sciences SC Archaeology; Social Sciences - Other Topics GA BAJ47 UT WOS:000222550400014 ER PT J AU Wilkison, SL Robinson, MS Thomas, PC Veverka, J McCoy, TJ Murchie, SL Prockter, LM Yeomans, DK AF Wilkison, SL Robinson, MS Thomas, PC Veverka, J McCoy, TJ Murchie, SL Prockter, LM Yeomans, DK TI An estimate of Eros's porosity and implications for internal structure SO ICARUS LA English DT Article DE Eros; meteorites; surfaces; asteroids; interiors ID CHONDRITE PARENT BODIES; ASTEROIDS; METEORITES; DISRUPTION; EVOLUTION; HISTORY; IMPACT; PHOBOS; GASPRA; SHAPE AB Earth-based spectral measurements and NEAR Shoemaker magnetometer, X-ray, and near-infrared spectrometer data are all consistent with Eros having a bulk composition and mineralogy similar to ordinary chondrite meteorites (OC). By comparing the bulk density of 433 Eros (2.67 +/- 0.03 g/cm(3)) with that of OCs (3.40 g/cm(3)), We estimate the total porosity of the asteroid to be 21-33%. Macro (or structural) porosity, best estimated to be similar to20%, is constrained to be between 6 and 33%. We conclude that Eros is a heavily fractured body, but we find no evidence that it was ever catastrophically disrupted and reaccumulated into a rubble pile. (C) 2002 Elsevier Science (USA). C1 Northwestern Univ, Dept Geol Sci, Evanston, IL 60208 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Appl Phys Lab, Laurel, MD 20723 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Northwestern Univ, Dept Geol Sci, Evanston, IL 60208 USA. EM sarah@earth.nwu.edu RI Murchie, Scott/E-8030-2015 OI Murchie, Scott/0000-0002-1616-8751 NR 82 TC 41 Z9 42 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JAN PY 2002 VL 155 IS 1 BP 94 EP 103 DI 10.1006/icar.2001.6751 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544ML UT WOS:000175164100007 ER PT B AU Leverington, DW Moon, WM AF Leverington, DW Moon, WM GP IEEE IEEE IEEE TI An evaluation of consensus neural networks and evidential reasoning algorithms for image classification SO IGARSS 2002: IEEE INTERNATIONAL GEOSCIENCE AND REMOTE SENSING SYMPOSIUM AND 24TH CANADIAN SYMPOSIUM ON REMOTE SENSING, VOLS I-VI, PROCEEDINGS: REMOTE SENSING: INTEGRATING OUR VIEW OF THE PLANET SE IEEE International Symposium on Geoscience and Remote Sensing (IGARSS) LA English DT Proceedings Paper CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS 2002)/24th Canadian Symposium on Remote Sensing CY JUN 24-28, 2002 CL TORONTO, CANADA SP IEEE, IEEE, Geosci & Remote Sensing Soc, Canadian Remote Sensing Soc, Univ Waterloo, Natl Resouces Candad, Canadian Space Agcy, Environm Canada, Natl Aeronaut & Space Adm, Natl Ocean & Atmospher Adm, Off Naval Res, Natl Space Dev Agcy Japan, Natl Polar-Orbit Environm Satellite Syst, Ball Aerosp & Technol, Int Union Radio Sci AB Empirical investigations of classification algorithms for lithological discrimination were performed in this research using two study areas in northern Canada: Melville Island, Nunavut, and the Cape Smith Belt of northern Quebec. These investigations suggest that a consensus neural network classifier (a majority-vote algorithm that combines the classification results of ten feedforward backpropagation neural networks) is capable of consistently producing results that approximate those produced by the best individual neural network execution, and that are superior to those generated by the maximum likelihood and evidential reasoning classifiers. The majority-vote consensus routine serves to eliminate the effect of the natural variability among individual neural network classification results, by producing strong results without necessitating the manual evaluation and ranking of all individual neural network classifications. Image classifications produced using the evidential reasoning classification algorithm were generally very poor when measures of initial evidence were derived from the proportions of training data that contained the image values being classified. Evidential reasoning classifications that derived measures of initial evidence from output activations generated by multiple neural network classifications were typically comparable to those of the neural network consensus algorithm. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Leverington, DW (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-7536-X J9 INT GEOSCI REMOTE SE PY 2002 BP 3474 EP 3476 PG 3 WC Computer Science, Artificial Intelligence; Geosciences, Multidisciplinary; Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Computer Science; Geology; Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BV48S UT WOS:000179116801130 ER EF