FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Stauffer, JR Jones, BF Backman, D Hartmann, LW Navascues, DBY Pinsonneault, MH Terndrup, DM Muench, AA AF Stauffer, JR Jones, BF Backman, D Hartmann, LW Navascues, DBY Pinsonneault, MH Terndrup, DM Muench, AA TI Why are the K dwarfs in the Pleiades so blue? SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (Pleiades); stars : low mass, brown dwarfs ID LOW-MASS STARS; PRE-MAIN-SEQUENCE; OPEN CLUSTER NGC-2516; H-BETA-PHOTOMETRY; COLOR-MAGNITUDE DIAGRAMS; ALPHA-PERSEI CLUSTERS; T-TAURI STARS; ROTATIONAL VELOCITIES; CHEMICAL-COMPOSITION; GALACTIC CLUSTERS AB The K dwarfs in the Pleiades fall nearly 1/2 mag below a main-sequence isochrone when plotted in a color-magnitude diagram utilizing V magnitude as the luminosity index and B-V as the color index. This peculiarity has been known for 40 years but has gone unexplained and mostly ignored. When compared to Praesepe members, the Pleiades K dwarfs again are subluminous (or blue) in a color-magnitude diagram using B-V as the color index. However, using V-I as the color index, stars in the two clusters are coincident to M(V) similar to 10; using V-K as the color index, Pleiades late K and M stars fall above the main-sequence locus defined by Praesepe members. We believe that the anomalous spectral energy distributions for the Pleiades K dwarfs, as compared to older clusters, are a consequence of rapid stellar rotation and may be primarily due to spottedness. If so, the required areal filling factor for the cool component has to be very large (greater than or equal to50%). Weak-lined T Tauri stars have similar color anomalies, and we suspect that this is a common feature of all very young K dwarfs (spectral type >K3). The peculiar spectral energy distribution needs to be considered in deriving accurate pre-main-sequence isochrone-fitting ages for clusters like the Pleiades, since the age derived will depend on the temperature index used. C1 CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Lab Astrofis Espacial & Fis Fundamental, Madrid 28080, Spain. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Stauffer, JR (reprint author), CALTECH, SIRTF Sci Ctr, Mail Code 314-6,1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 85 TC 73 Z9 73 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2003 VL 126 IS 2 BP 833 EP 847 DI 10.1086/376739 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706GU UT WOS:000184446600019 ER PT J AU Cohen, M Wheaton, WA Megeath, ST AF Cohen, M Wheaton, WA Megeath, ST TI Spectral irradiance calibration in the infrared. XIV. The absolute calibration of 2MASS SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared radiation; surveys ID STARS AB Element by element, we have combined the optical components in the three cameras of the Two Micron All Sky Survey (2MASS), and incorporated detector quantum efficiency curves and site-specific atmospheric transmissions, to create three relative spectral response curves (RSRs). We provide the absolute 2MASS attributes associated with "zero magnitude'' in the JHKs bands so that these RSRs may be used for synthetic photometry. The RSRs tie 2MASS to the "Cohen-Walker-Witteborn'' framework of absolute photometry and stellar spectra for the purpose of using 2MASS data to support the development of absolute calibrators for the Infrared Array Camera and pairwise cross-calibrators between all three SIRTF instruments. We examine the robustness of these RSRs to changes in water vapor within a night. We compare the observed 2MASS magnitudes of 33 stars ( converted from the precision optical calibrators of Landolt and Carter-Meadows into absolute infrared calibrators from 1.2 to 35 mum) with our predictions, thereby deriving 2MASS "zero-point offsets'' from the ensemble. These offsets are the final ingredients essential to merge 2MASS JHKs data with our other absolutely calibrated bands and stellar spectra, and to support the creation of faint calibration stars for SIRTF. C1 Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cohen, M (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA. NR 11 TC 433 Z9 435 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2003 VL 126 IS 2 BP 1090 EP 1096 DI 10.1086/376474 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 706GU UT WOS:000184446600038 ER PT J AU Rodriguez, J Tomsick, JA Foschini, L Walter, R Goldwurm, A Corbel, S Kaaret, P AF Rodriguez, J Tomsick, JA Foschini, L Walter, R Goldwurm, A Corbel, S Kaaret, P TI An XMM-Newton observation of IGR J16320-4751 = AX J1631.9-4752 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disk; stars : individual : IGR J16320-4751; X-rays : binaries; X-rays : general ID PHOTON IMAGING CAMERA; X-RAY-SPECTRA; NEUTRON-STARS; NOVAE AB The hard X-ray sensitivity and arcminute position accuracy of the recently launched International Gamma-Ray Laboratory (INTEGRAL) has lead to the (re-)discovery of a class of heavily absorbed hard X-ray sources lying in the Galactic plane. We report on the analysis of an XMM observation of such a source IGR J16320-4751 = AX J1631.9-4752. Our analysis allowed us to obtain the most accurate X-ray position to date (Rodriguez et al. 2003), and to identify a likely infrared counterpart (Tomsick et al. 2003). We present the detailed analysis of the IGR J16320-4751 XMM spectra. The PN spectrum can be well represented by a single powerlaw or a comptonized spectrum with a high equivalent absorption column density of similar to2 x 10(23) cm(-2). The current analysis and the comparison with the properties of other sources favor the possibility that the source is a Galactic X-Ray Binary (XRB). The identification of two candidate IR counterparts is in good agreement with this identification. The hard spectrum previously seen with ASCA, and the brightness of the candidate counterparts indicate that IGR J16320-4751 is most probably a highly absorbed High Mass X-ray Binary, hosting a neutron star. C1 CEA Saclay, DSM DAPNIA SAp, CNRS, FRE 2591, F-91191 Gif Sur Yvette, France. Integral Sci Data Ctr, CH-1290 Versoix, Switzerland. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. IASF CNR, Sez Bologna, I-40129 Bologna, Italy. Univ Paris 07, Federat APC, F-75251 Paris 05, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rodriguez, J (reprint author), CEA Saclay, DSM DAPNIA SAp, CNRS, FRE 2591, F-91191 Gif Sur Yvette, France. RI Foschini, Luigi/H-3833-2012 OI Foschini, Luigi/0000-0001-8678-0324 NR 25 TC 45 Z9 45 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 AUG PY 2003 VL 407 IS 2 BP L41 EP L45 DI 10.1051/0004-6361:20031093 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 708CV UT WOS:000184550300006 ER PT J AU Boonman, AMS Doty, SD van Dishoeck, EF Bergin, EA Melnick, GJ Wright, CM Stark, R AF Boonman, AMS Doty, SD van Dishoeck, EF Bergin, EA Melnick, GJ Wright, CM Stark, R TI Modeling gas-phase H2O between 5 mu m and 540 mu m toward massive protostars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : abundances; ISM : molecules; infrared : ISM; ISM : lines and bands; molecular processes ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; MAGNETOHYDRODYNAMIC SHOCK-WAVES; MOLECULAR CLOUD CORES; ISO-SWS OBSERVATIONS; WATER-VAPOR; ABSORPTION FEATURES; ASTRONOMY-SATELLITE; INTERSTELLAR WATER; RADIATIVE-TRANSFER AB We present models and observations of gas-phase H2O lines between 5 and 540 mum toward deeply embedded massive protostars, involving both pure rotational and ro-vibrational transitions. The data have been obtained for 6 sources with both the Short and Long Wavelength Spectrometers (SWS and LWS) on board the Infrared Space Observatory (ISO) and with the Submillimeter Wave Astronomy Satellite (SWAS). For comparison, CO J = 7-6 spectra have been observed with the MPIfR/SRON 800 GHz heterodyne spectrometer at the James Clerk Maxwell Telescope (JCMT). A radiative transfer model in combination with different physical/chemical scenarios has been used to model these H2O lines for 4 sources to probe the chemical structure of these massive protostars. The results indicate that pure gas-phase production of H2O cannot explain the observed spectra. Ice evaporation in the warm inner envelope and freeze-out in the cold outer part are important for most of our sources and occur at T similar to 90-110 K. The ISO-SWS data are particularly sensitive to ice evaporation in the inner part whereas the ISO-LWS data are good diagnostics of freeze-out in the outer region. The modeling suggests that the 557 GHz SWAS line includes contributions from both the cold and the warm H2O gas. The SWAS line profiles indicate that for some of the sources a fraction of up to 50% of the total flux may originate in the outflow. Shocks do not seem to contribute significantly to the observed emission in other H2O lines, however, in contrast with the case for Orion. The results show that three of the observed and modeled H2O lines, the 3(03)-2(12), 2(12)-1(01), and 1(10)-1(01) lines, are good candidates to observe with the Herschel Space Observatory in order to further investigate the physical and chemical conditions in massive star-forming regions. C1 Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Boonman, AMS (reprint author), Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands. NR 58 TC 47 Z9 47 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 AUG PY 2003 VL 406 IS 3 BP 937 EP 955 DI 10.1051/0004-6361:20030765 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 704BL UT WOS:000184317800018 ER PT J AU Hempelmann, A Schmitt, JHMM Baliunas, SL Donahue, RA AF Hempelmann, A Schmitt, JHMM Baliunas, SL Donahue, RA TI Evidence for coronal activity cycles on 61 Cygni A and B SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : late-type; stars : activity; stars : coronae; stars : chromospheres ID X-RAY-EMISSION; MAIN-SEQUENCE STARS; CHROMOSPHERIC VARIATIONS AB We investigate a four-and-one-half year time-series of ROSAT HRI pointed observations of 61 Cyg A and B and compare the X-ray light curves with the chromospheric Ca HK variability. The ROSAT sampling rate was two pointings per year and typical errors lie in the range of 5-10%. The chromospheric cycles are well-known for both stars from the Mt. Wilson Ca HK survey. Although the time basis of our ROSAT observations is shorter than the 7-and 12-year cycles of components A and B, respectively, we find the long-term trend of coronal activity in close correlation with the chromospheric activity during the observation period, between 1993 and 1998. The chromospheric activity increased through maximum activity down to a minimum for component A, and from maximum to minimum activity for component B. The same behaviour is observed for the X-ray light curves but with much higher amplitudes by factors 2.5-3. The remaining scatter observed around low-order regression curves of coronal activity is small. We conclude that both stars do show coronal cycles and that coronal cycles are the dominant source of variability for 61 Cygni. C1 Univ Hamburg, D-21029 Hamburg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hempelmann, A (reprint author), Univ Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany. NR 12 TC 13 Z9 14 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2003 VL 406 IS 2 BP L39 EP L42 DI 10.1051/0004-6361:20030882 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 702KC UT WOS:000184222200003 ER PT J AU Yoshida, N Abel, T Hernquist, L Sugiyama, N AF Yoshida, N Abel, T Hernquist, L Sugiyama, N TI Simulations of early structure formation: Primordial gas clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; early universe; galaxies : formation; stars : formation ID COLD DARK-MATTER; POPULATION-III STARS; PARTICLE HYDRODYNAMICS SIMULATIONS; FIRST COSMOLOGICAL OBJECTS; 1ST STARS; RADIATIVE FEEDBACK; ANGULAR-MOMENTUM; GALAXY FORMATION; HIGH-REDSHIFT; MASS FUNCTION AB We use cosmological simulations to study the origin of primordial star-forming clouds in a LambdaCDM universe, by following the formation of dark matter halos and the cooling of gas within them. To model the physics of chemically pristine gas, we employ a nonequilibrium treatment of the chemistry of nine species (e(-), H, H(+), He, He(+), He(++), H(2), H(2)(+), H(-)) and include cooling by molecular hydrogen. By considering cosmological volumes, we are able to study the statistical properties of primordial halos, and the high resolution of our simulations enables us to examine these objects in detail. In particular, we explore the hierarchical growth of bound structures forming at redshifts z approximate to 25-30 with total masses in the range approximate to10(5)-10(6) M(.). We find that when the amount of molecular hydrogen in these objects reaches a critical level, cooling by rotational line emission is efficient, and dense clumps of cold gas form. We identify these "gas clouds'' as sites for primordial star formation. In our simulations, the threshold for gas cloud formation by molecular cooling corresponds to a critical halo mass of approximate to5 x 10(5) h(-1) M(.), in agreement with earlier estimates, but with a weak dependence on redshift in the range z > 16. The complex interplay between the gravitational formation of dark halos and the thermodynamic and chemical evolution of the gas clouds compromises analytic estimates of the critical H(2) fraction. Dynamical heating from mass accretion and mergers opposes relatively inefficient cooling by molecular hydrogen, delaying the production of star-forming clouds in rapidly growing halos. We also investigate the effect of photodissociating ultraviolet radiation on the formation of primordial gas clouds. We consider two extreme cases, first by including a uniform radiation field in the optically thin limit and second by accounting for the maximum effect of gas self-shielding in virialized regions. For radiation with Lyman-Werner band flux J > 10(-23) ergs s(-1) cm(-2) Hz(-1) sr(-1), hydrogen molecules are rapidly dissociated, rendering gas cooling inefficient. In both the cases we consider, the overall effect can be described by computing an equilibrium H(2) abundance for the radiation flux and defining an effective shielding factor. Based on our numerical results, we develop a semianalytic model of the formation of the first stars and demonstrate how it can be coupled with large N-body simulations to predict the star formation rate in the early universe. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Natl Astron Observ Japan, Tokyo 1818588, Japan. RP Yoshida, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Yoshida, Naoki/A-4305-2011 NR 66 TC 337 Z9 338 U1 3 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2003 VL 592 IS 2 BP 645 EP 663 DI 10.1086/375810 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RG UT WOS:000184408100001 ER PT J AU Aldcroft, TL Green, PJ AF Aldcroft, TL Green, PJ TI Lens or binary? Chandra observations of the wide-separation broad absorption line quasar pair UM 425 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : absorption lines; quasars : individual (UM Q2345, 425+007); X-rays : general ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; EARLY DATA RELEASE; X-RAY-EMISSION; STELLAR OBJECTS; ULTRAVIOLET-ABSORPTION; INTRACLUSTER MEDIUM; OPTICAL-PROPERTIES; CANDIDATE UM-425; TIME-DELAY AB We have obtained a 110 ks Chandra ACIS-S exposure of UM 425, a pair of QSOs at z = 1.47 separated by 6."5, which show remarkably similar emission and broad absorption line (BAL) profiles in the optical/UV. Our 5000 count X-ray spectrum of UM 425A ( the brighter component) is well fitted with a power law (photon spectral index Gamma = 2.0) partially covered by a hydrogen column of 3.8 x 10(22) cm(-2). The underlying power-law slope for this object and for other recent samples of BALQSOs is typical of radio-quiet quasars, lending credence to the hypothesis that BALs exist in every quasar. Assuming the same Gamma for the much fainter image of UM 425B, we detect an obscuring column 5 times larger. We search for evidence of an appropriately large lensing mass in our Chandra image and find weak diffuse emission near the quasar pair, with an X-ray flux typical of a group of galaxies at redshift z similar to 0.6. From our analysis of archival HST WFPC2 and NICMOS images, we find no evidence for a luminous lensing galaxy, but note a 3 sigma excess of galaxies in the UM 425 field with plausible magnitudes for a z = 0.6 galaxy group. However, the associated X-ray emission does not imply sufficient mass to produce the observed image splitting. The lens scenario thus requires a dark (high M/L ratio) lens or a fortuitous configuration of masses along the line of sight. UM425 may instead be a close binary pair of BALQSOs, which would boost arguments that interactions and mergers increase nuclear activity and outflows. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Aldcroft, TL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 72 TC 13 Z9 13 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2003 VL 592 IS 2 BP 710 EP 720 DI 10.1086/375863 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RG UT WOS:000184408100006 ER PT J AU Gilli, R Cimatti, A Daddi, E Hasinger, G Rosati, P Szokoly, G Tozzi, P Bergeron, J Borgani, S Giacconi, R Kewley, L Mainieri, V Mignoli, M Nonino, M Norman, C Wang, J Zamorani, G Zheng, W Zirm, A AF Gilli, R Cimatti, A Daddi, E Hasinger, G Rosati, P Szokoly, G Tozzi, P Bergeron, J Borgani, S Giacconi, R Kewley, L Mainieri, V Mignoli, M Nonino, M Norman, C Wang, J Zamorani, G Zheng, W Zirm, A TI Tracing the large-scale structure in the Chandra Deep Field South SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : high-redshift; large-scale structure of universe; X-rays : general ID ACTIVE GALACTIC NUCLEI; ESO IMAGING SURVEY; X-RAY; REDSHIFT SURVEY; ANGULAR-CORRELATION; SOURCE CATALOG; OPTICAL SURVEY; QSOS; GALAXIES; EVOLUTION AB We report the discovery of large-scale structures of X-ray sources in the 1 Ms observation of the Chandra Deep Field South. Two main structures appear as narrow (Deltaz less than or similar to 0.02) spikes in the source redshift distribution at z = 0.67 and 0.73, respectively. Their angular distribution spans a region at least similar to17' wide, corresponding to a physical size of 7.3 h(70)(-1) Mpc at a redshift of z 0.7 (Omega(m) = 0.3, Omega(Lambda) = 0.7). These spikes are populated by 19 sources each, which are mainly identified as active galactic nuclei (AGNs). Two sources in each spike are extended in X-rays, corresponding to galaxy groups/clusters embedded in larger structures. The X-ray source redshift distribution shows other spikes, the most remarkable at z = 1.04, 1.62, and 2.57. This is one of the first evidences for large-scale structure traced by X-ray sources and for spatial clustering of X-ray-selected AGNs. The X-ray data have been complemented with the spectroscopic data from the K20 near-infrared survey (Cimatti et al.), which covers similar to1/10 of the X-ray field. In this survey, too, the source redshift distribution shows several spikes. Two narrow structures at z = 0.67 and 0.73 (again with Deltaz similar to 0.02) are the most significant features, containing 24 and 47 galaxies, respectively. While the K20 structure at z = 0.73 is dominated by a standard galaxy cluster with a significant concentration around a central cD galaxy and morphological segregation, the galaxies at z = 0.67 constitute a loose structure rather uniformly distributed along the K20 field. Moreover, we find a very good correlation (almost one-to-one) between less prominent peaks detected in the redshift distributions of X-ray and K20 sources. In particular, at z < 1.3 we find that five out of the six more significant K20 peaks have a corresponding peak in the X-ray-selected sources and, similarly, all five X-ray peaks below that redshift have a corresponding K20 peak. Since the K20 survey sensitivity drops beyond z &SIM; 1.3, structures at higher redshift are traced only by the X-ray sources. This correlation suggests that AGNs ( from the X-ray data) and (early-type) galaxies ( from the K20 survey) are tracing the same underlying structures. We also compared the X-ray and K-band catalogs to search for enhanced X-ray activity in the sources in the two main redshift spikes. While in the structure at z = 0.73 the fraction of X-ray sources is the same as in the field, in the structure at z = 0.67 it is higher by a factor of &SIM;2, suggesting that X-ray activity may be triggered preferentially in the structure at z = 0.67. Given the limited statistics, this result is significant only at the &SIM;2σ level. C1 INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. Johns Hopkins Univ, Baltimore, MD 21218 USA. European So Observ, D-85748 Garching, Germany. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. INAF, Osservatorio Astron Trieste, I-34131 Trieste, Italy. CNRS, Inst Astrophys Paris, F-75014 Paris, France. Univ Trieste, Dipartimento Astron, Ist Nazl Fis Nucl, I-34131 Trieste, Italy. Associated Univ Inc, Washington, DC 20036 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Gilli, R (reprint author), INAF, Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. RI Daddi, Emanuele/D-1649-2012; Mignoli, Marco/O-9426-2015; Gilli, Roberto/P-1110-2015; OI Daddi, Emanuele/0000-0002-3331-9590; Mignoli, Marco/0000-0002-9087-2835; Gilli, Roberto/0000-0001-8121-6177; Nonino, Mario/0000-0001-6342-9662; Borgani, Stefano/0000-0001-6151-6439; Zamorani, Giovanni/0000-0002-2318-301X NR 29 TC 124 Z9 124 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2003 VL 592 IS 2 BP 721 EP 727 DI 10.1086/375777 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RG UT WOS:000184408100007 ER PT J AU Steidel, CC Adelberger, KL Shapley, AE Pettini, M Dickinson, M Giavalisco, M AF Steidel, CC Adelberger, KL Shapley, AE Pettini, M Dickinson, M Giavalisco, M TI Lyman break galaxies at redshift z similar to 3: Survey description and full data set SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies : evolution; galaxies : high-redshift ID HUBBLE DEEP FIELD; RESOLUTION IMAGING SPECTROMETER; RADIO-QUIET GALAXY; C-IV ABSORPTION; STAR-FORMATION; PRIMEVAL GALAXIES; QSO FIELDS; ULTRAVIOLET LUMINOSITY; KECK SPECTROSCOPY; MS 1512-CB58 AB We present the basic data for a large ground-based spectroscopic survey for z similar to 3 Lyman break galaxies (LBGs), photometrically selected using rest-UV colors from very deep images in 17 high Galactic latitude fields. The total survey covers an area of 0.38 deg(2) and includes 2347 photometrically selected candidate LBGs to an apparent R-AB magnitude limit of 25.5. Approximately half of these objects have been observed spectroscopically using the Keck telescopes, yielding 940 redshifts with (z) = 2.96 +/- 0.29. We discuss the images, photometry, target selection, and spectroscopic program in some detail and present catalogs of the photometric and spectroscopic data, made available in electronic form. We discuss the general utility of conducting nearly volume-limited redshift surveys in prescribed redshift intervals using judicious application of photometric preselection. C1 CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP CALTECH, MS 105-24, Pasadena, CA 91125 USA. NR 73 TC 526 Z9 527 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2003 VL 592 IS 2 BP 728 EP 754 DI 10.1086/375772 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RG UT WOS:000184408100008 ER PT J AU Di Stefano, R Kong, AKH AF Di Stefano, R Kong, AKH TI Luminous supersoft X-ray sources in external galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M51, M83, M101, NGC 4697); methods : data analysis; supernova remnants; white dwarfs; X-rays : binaries; X-rays : galaxies ID CHANDRA; DISCOVERY; EMISSION; NUCLEUS; M101; POPULATION; DISTANCES; M-83; MASS AB We use a set of conservative criteria to identify luminous supersoft X-ray sources (SSSs) in external galaxies. We test this approach on blackbody models and then apply it to Chandra data from four galaxies: an elliptical galaxy (NGC 4967), two face-on spiral galaxies (M101 and M83), and an interacting galaxy (M51). We find SSSs in every galaxy and estimate that the total SSS population of sources with L > 10(37) ergs s(-1) in each galaxy is at least several hundred and could be significantly larger. In addition, we discover two intriguing features of galactic populations of SSSs. First, there are significant subpopulations of high-luminosity sources; the bolometric luminosities can exceed 10(39) ergs s(-1). Second, in the spiral galaxies M101, M83, and M51, SSSs appear to be associated with the spiral arms. This may indicate that some SSSs are young systems, possibly younger than 10(8) yr. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 29 TC 64 Z9 64 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 AUG 1 PY 2003 VL 592 IS 2 BP 884 EP 899 DI 10.1086/375858 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RG UT WOS:000184408100017 ER PT J AU De Pasquale, M Piro, L Perna, R Costa, E Feroci, M Gandolfi, G In't Zand, J Nicastro, L Frontera, F Antonelli, LA Fiore, F Stratta, G AF De Pasquale, M Piro, L Perna, R Costa, E Feroci, M Gandolfi, G In't Zand, J Nicastro, L Frontera, F Antonelli, LA Fiore, F Stratta, G TI A comparative study of the X-ray afterglow properties of optically bright and dark gamma-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID HOST GALAXY; UNIVERSE; DUST; REIONIZATION; DESTRUCTION; COUNTERPART; GRB-970828; EMISSION; LINE AB We have examined the complete set of X-ray afterglow observations of dark and optically bright gamma-ray bursts (GRBs) performed by BeppoSAX through 2001 February. X-ray afterglows are detected in similar to90% of the cases. We do not find significant differences in the X-ray spectral shape, in particular no increased X-ray absorption in GRBs without optical transient (dark GRBs) compared to GRBs with optical transient (OTGRBs). Rather, we find that the 1.6-10 keV flux of OTGRBs is on average about 5 times larger than that of the dark GRBs. A Kolmogorov-Smirnov test shows that this difference is significant at 99.8% probability. Under the assumption that dark and OTGRBs have similar spectra, this could suggest that the first are uncaught in the optical band because they are just faint sources. In order to test this hypothesis, we have determined the optical-to-X-ray flux ratios of the sample. OTGRBs show a remarkably narrow distribution of flux ratios, which corresponds to an average optical-to-X-ray spectral index (α) over bar (OT)(ox) = 0.794 +/- 0.054. We find that, while 75% of dark GRBs have flux ratio upper limits still consistent with those of OT GRBs, the remaining 25% are 4-10 times weaker in optical than in X-rays. The significance of this result is greater than or equal to2.6 sigma. If this subpopulation of dark GRBs were constituted by objects assimilable to OTGRBs, they should have shown optical fluxes higher than upper limits actually found. We discuss the possible causes of their behavior, including a possible occurrence in high-density clouds or origin at very high redshift and a connection with ancient, Population III stars. C1 CNR, IASF, I-00133 Rome, Italy. Univ Roma La Sapienza, I-00185 Rome, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Res Org Netherlands, NL-3584 CA Utrecht, Netherlands. CNR, IASF, I-90146 Palermo, Italy. CNR, IASF, I-40129 Bologna, Italy. Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy. Rome Astron Observ, I-00044 Frascati, Italy. RP De Pasquale, M (reprint author), CNR, IASF, Via Fosso Del Cavaliere 100, I-00133 Rome, Italy. RI PIRO, LUIGI/E-4954-2013; Nicastro, Luciano/F-5866-2015; Stratta, Maria Giuliana/L-3045-2016; OI PIRO, LUIGI/0000-0003-4159-3984; Nicastro, Luciano/0000-0001-8534-6788; Stratta, Maria Giuliana/0000-0003-1055-7980; Costa, Enrico/0000-0003-4925-8523; Feroci, Marco/0000-0002-7617-3421; Fiore, Fabrizio/0000-0002-4031-4157 NR 47 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 AUG 1 PY 2003 VL 592 IS 2 BP 1018 EP 1024 DI 10.1086/375854 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RG UT WOS:000184408100028 ER PT J AU Igumenshchev, IV Narayan, R Abramowicz, MA AF Igumenshchev, IV Narayan, R Abramowicz, MA TI Three-dimensional magnetohydrodynamic simulations of radiatively inefficient accretion flows SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; convection; MHD; turbulence ID ADVECTION-DOMINATED ACCRETION; ANGULAR-MOMENTUM TRANSPORT; BLACK-HOLES; 3 DIMENSIONS; RADIO JETS; DISKS; CONVECTION; TRANSITIONS; MODELS; STARS AB We present three-dimensional MHD simulations of rotating radiatively inefficient accretion flows onto black holes. We continuously inject magnetized matter into the computational domain near the outer boundary and run the calculations long enough for the resulting accretion flow to reach a quasi-steady state. We have studied two limiting cases for the geometry of the injected magnetic field: pure toroidal field and pure poloidal field. In the case of toroidal field injection, the accreting matter forms a nearly axisymmetric, geometrically thick, turbulent accretion disk. The disk resembles in many respects the convection-dominated accretion flows found in previous numerical and analytical investigations of viscous hydrodynamic flows. Models with poloidal field injection evolve through two distinct phases. In an initial transient phase, the flow forms a relatively flattened, quasi-Keplerian disk with a hot corona and a bipolar outflow. However, when the flow later achieves steady state, it changes in character completely. The magnetized accreting gas becomes two-phase, with most of the volume being dominated by a strong dipolar magnetic field from which a thermal low-density wind flows out. Accretion occurs mainly via narrow slowly rotating radial streams that "diffuse'' through the magnetic field with the help of magnetic reconnection events. C1 Univ Rochester, Laser Energet Lab, Rochester, NY 14623 USA. Harvard Smithsonian Ctr Astrophys, Dept Astron, Cambridge, MA 02138 USA. Gothenburg Univ, Dept Astron & Astrophys, S-41296 Gothenburg, Sweden. Chalmers Univ Technol, S-41296 Gothenburg, Sweden. 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 56 TC 206 Z9 206 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2003 VL 592 IS 2 BP 1042 EP 1059 DI 10.1086/375769 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RG UT WOS:000184408100031 ER PT J AU Tomsick, JA Kalemci, E Corbel, S Kaaret, P AF Tomsick, JA Kalemci, E Corbel, S Kaaret, P TI X-ray flares and oscillations from the black hole candidate X-ray transient XTE J1650-500 at low luminosity SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars : individual (XTE J1650-500); X-rays : stars ID ADVECTION-DOMINATED ACCRETION; SAGITTARIUS-A-ASTERISK; SYNCHROTRON EMISSION; TIMING EXPLORER; GALACTIC-CENTER; XTE J1650-500; GRO J0422+32; ENERGY; OUTBURST; STATES AB We report on X-ray observations made with the Rossi X-Ray Timing Explorer of the black hole candidate (BHC) transient XTE J1650-500 at the end of its first, and currently only, outburst. By monitoring the source at low luminosities over several months, we found six bright similar to100 s X-ray flares and long timescale oscillations of the X-ray flux. The oscillations are aperiodic with a characteristic timescale of 14.2 days and an order of magnitude variation in the 2.8-20 keV flux. The oscillations may be related to optical "mini-outbursts'' that have been observed at the ends of outbursts for other short orbital period BHC transients. The X-ray flares have durations between 62 and 215 s and peak fluxes that are 5-24 times higher than the persistent flux. The. ares have nonthermal energy spectra and occur when the persistent luminosity is near 3 x 10(34) (d/4 kpc)(2) ergs s(-1) (2.8-20 keV). The rise time for the brightest. are demonstrates that physical models for BHC systems must be able to account for the situation where the X-ray flux increases by a factor of up to 24 on a timescale of seconds. We discuss the. ares in the context of observations and theory of Galactic BHCs and compare the. ares to those detected from Sgr A*, the supermassive black hole at the Galactic center. We also compare the. ares to X-ray bursts that are seen in neutron star systems. While some of the. are light curves are similar to those of neutron star bursts, the. ares have nonthermal energy spectra in contrast to the blackbody spectra exhibited in bursts. This indicates that X-ray bursts should not be taken as evidence that a given system contains a neutron star unless the presence of a blackbody component in the burst spectrum can be demonstrated. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA. CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Paris 07, F-91191 Gif Sur Yvette, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tomsick, JA (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, Code 0424, La Jolla, CA 92093 USA. NR 63 TC 25 Z9 25 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2003 VL 592 IS 2 BP 1100 EP 1109 DI 10.1086/375811 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RG UT WOS:000184408100035 ER PT J AU Habbal, SR Arndt, MB Nayfeh, MH Arnaud, J Johnson, J Hegwer, S Woo, R Ene, A Habbal, F AF Habbal, SR Arndt, MB Nayfeh, MH Arnaud, J Johnson, J Hegwer, S Woo, R Ene, A Habbal, F TI On the detection of the signature of silicon nanoparticle dust grains in coronal holes SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; eclipses; polarization; Sun : corona; Sun : infrared; Sun : magnetic fields ID 1991 SOLAR ECLIPSE; INTERPLANETARY DUST; INFRARED OBSERVATIONS; THERMAL RADIATION; CIRCUMSOLAR DUST; MAGNETIC-FIELD; EMISSION-LINE; POLARIZATION AB We report on polarization measurements in the Fe XIII line at 1074.7 nm made during the total solar eclipse of 2001 June 21, which yielded the first signature of interplanetary dust in the inner corona. In the first-ever images at this wavelength, the signature of dust appears as a tangentially polarized emission in the radial extension of the low-temperature and low-density coronal holes as opposed to a predominantly radial polarization direction in the rest of the corona. The observed emission and polarization are attributed to fluorescence from silicon nanoparticle dust grains in the inner corona. C1 Univ Coll Wales, Dept Phys, Aberystwyth SY23 3BZ, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Bridgewater State Coll, Dept Phys, Bridgewater, MA 02325 USA. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Observ Midi Pyrenees, F-31400 Toulouse, France. Electricon, Boulder, CO 80304 USA. Natl Solar Observ, Sunspot, NM 88349 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Stanford Univ, Dept Phys, Stanford, CA 94305 USA. Univ Texas, Dept Mech Engn, Austin, TX 78712 USA. RP Habbal, SR (reprint author), Univ Coll Wales, Dept Phys, Aberystwyth SY23 3BZ, Dyfed, Wales. NR 21 TC 17 Z9 17 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2003 VL 592 IS 2 BP L87 EP L90 DI 10.1086/377678 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RJ UT WOS:000184408300009 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, MC Thaddeus, P TI The radio spectrum of Si-3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; line : identification; molecular data; molecular processes; radio lines : ISM ID GROUND-STATE; CLUSTERS AB The silicon trimer Si-3 and several of its rare isotopic species have been detected in the laboratory, and the frequencies of 66 rotational transitions in the range 5 - 42 GHz have been measured to a few parts in 10(7). The most intense radio lines can be calculated from the derived spectroscopic constants to better than 3 km s(-1) in equivalent radial velocity up to frequencies of 50 GHz, adequate for a deep search in the best astronomical sources; above that frequency the uncertainties increase to of the order of 20 km s(-1) at 160 GHz, which is still sufficient for a deep search in a wide-line source such as IRC + 10216. 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. NR 12 TC 3 Z9 3 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2003 VL 592 IS 2 BP L91 EP L93 DI 10.1086/375728 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 705RJ UT WOS:000184408300010 ER PT J AU Liu, X Newchurch, MJ Kim, JH AF Liu, X Newchurch, MJ Kim, JH TI Occurrence of ozone anomalies over cloudy areas in TOMS version-7 level-2 data SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPICAL TROPOSPHERIC OZONE; MAPPING SPECTROMETER; COLUMN OZONE; STRATOSPHERIC AEROSOL; SOUTH-AMERICA; TRACE-A; CLIMATOLOGY; REFLECTIVITY; ABSORPTION; RADIATION AB This study investigates anomalous ozone distributions over cloudy areas in Nimbus-7 (N7) and Earth-Probe (EP) TOMS version-7 data and analyzes the causes for ozone anomaly formation. A 5degrees-longitude by 5degrees-latitude region is defined to contain a Positive Ozone Anomaly (POA) or Negative Ozone Anomaly (NOA) if the correlation coefficient between total ozone and reflectivity is greater than or equal to0.5 or less than or equal to0.5. The average fractions of ozone anomalies among all cloud fields are 31.8+/-7.7% and 35.8+/-7.7% in the N7 and EP TOMS data, respectively. Some ozone anomalies are caused by ozone retrieval errors, and others are caused by actual geophysical phenomena. Large cloud-height errors are found in the TOMS version-7 algorithm in comparison to the Temperature Humidity Infrared Radiometer (THIR) cloud data. On average, cloud-top pressures are overestimated by similar to200 hPa (THIR cloud-top pressure less than or equal to200 hPa) for high-altitude clouds and underestimated by similar to150 hPa for low-altitude clouds ( THIR cloud-top pressure greater than or equal to750 hPa). Most tropical NOAs result from negative errors induced by large cloud-height errors, and most tropical POAs are caused by positive errors due to intra-cloud ozone absorption enhancement. However, positive and negative errors offset each other, reducing the ozone anomaly occurrence in TOMS data. Large ozone/reflectivity slopes for mid-latitude POAs show seasonal variation consistent with total ozone fluctuation, indicating that they result mainly from synoptic and planetary wave disturbances. POAs with an occurrence fraction of 30-60% occur in regions of marine stratocumulus off the west coast of South Africa and off the west coast of South America. Both fractions and ozone/reflectivity slopes of these POAs show seasonal variations consistent with that in the tropospheric ozone. About half the ozone/reflectivity slope can be explained by ozone retrieval errors over clear and cloudy areas. The remaining slope may result from there being more ozone production because of rich ozone precursors and higher photolysis rates over high-frequency, low-altitude clouds than in clear areas. Ozone anomalies due to ozone retrieval errors have important implications in TOMS applications such as tropospheric ozone derivation and analysis of ozone seasonal variation. C1 Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. Pusan Natl Univ, Dept Atmospher Sci, Pusan, South Korea. RP Liu, X (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X NR 50 TC 10 Z9 11 U1 0 U2 1 PU EUROPEAN GEOPHYSICAL SOC PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 01 PY 2003 VL 3 BP 1113 EP 1129 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 707KD UT WOS:000184509100002 ER PT J AU Sumner, S Hughes, WOH Boomsma, JJ AF Sumner, S Hughes, WOH Boomsma, JJ TI Evidence for differential selection and potential adaptive evolution in the worker caste of an inquiline social parasite SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE inquilinism; metapleural gland; disease resistance; Metarhizium; leaf-cutting ant ID LEAF-CUTTING ANTS; METAPLEURAL GLANDS; ACROMYRMEX-OCTOSPINOSUS; SYMPATRIC SPECIATION; ATTA-SEXDENS; HYMENOPTERA; FORMICIDAE; INSINUATOR; SECRETION; SIZE AB Social parasites exploit the socially managed resources of social insect colonies in order to maximise their own fitness. The inquilines are among the most specialised social parasites, because they are dependent on being fully integrated into their host's colony throughout their lives. They are usually relatives of their host and so share ancestral characteristics (Emery's rule). Closely related inquiline-host combinations offer a rare opportunity to study trade-offs in natural selection. This is because ancestral adaptations to a free-living state (e.g. the production of a worker caste) become redundant and may be replaced by novel, parasitic traits as the inquiline becomes more specialised. The dynamics of such processes are, however, unknown as virtually all extant inquiline social parasites have completely lost their worker caste. An exception is Acromyrmex insinuator, an incipient permanent social parasite of the leaf-cutting ant Acromyrmex echinatior. In the present study, we document the size distribution of parasite and host workers and infer how selection has acted on A. insinuator to reduce, but not eliminate, its investment in a worker caste. We show that the antibiotic producing metapleural glands of these parasite workers are significantly smaller than in their host counterparts and we deduce that the metapleural gland size in the host represents the ancestral state. We further show experimentally that social parasite workers are more vulnerable to the general insect pathogenic fungus Metarhizium than are host workers. Our findings suggest that costly disease resistance mechanisms are likely to have been lost early in inquiline evolution, possibly because active selection for maintaining these traits became less when parasite workers had evolved the ability to exploit the collective immune system of their host societies. C1 Univ Copenhagen, Inst Zool, Dept Populat Ecol, DK-2100 Copenhagen, Denmark. RP Sumner, S (reprint author), Smithsonian Trop Res Inst, Gamboa POB 2072, Balboa, Panama. EM sumners@naos.si.edu RI Sumner, Seirian/E-6611-2011; Hughes, William/A-6957-2014; Boomsma, Jacobus/M-2785-2014 OI Hughes, William/0000-0003-0951-9768; Boomsma, Jacobus/0000-0002-3598-1609 NR 41 TC 23 Z9 23 U1 1 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD AUG PY 2003 VL 54 IS 3 BP 256 EP 263 DI 10.1007/s00265-003-0633-0 PG 8 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 711RM UT WOS:000184754900008 ER PT J AU Kursar, TA Coley, PD AF Kursar, TA Coley, PD TI Convergence in defense syndromes of young leaves in tropical rainforests SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Article; Proceedings Paper CT 4th International Legume Conference CY JUL 02-06, 2001 CL CANBERRA, AUSTRALIA DE herbivory; rainforest; Barro Colorado Island; young leaves; phenolics; leaf expansion; pathogens; bioassays; toughness; delayed greening; Inga ID LEAF DEVELOPMENT; HERBIVORY; TREE; COEVOLUTION; CONSEQUENCES; EXPANSION; TOXICITY; INSECTS AB In tropical forests, the majority of damage by herbivores or pathogens occurs on young leaves, yet the patterns of damage and the factors that influence them are poorly known. By measuring damage throughout leaf development and maturation for five. species in a Panamanian forest, we showed that leaf toughening, which only occurs over a few days once the leaf is fully expanded, is the main factor decreasing damage in mature leaves. Although rates of damage to young leaves are, on average, orders of magnitude greater than on mature leaves, there is significant interspecific variation in young leaf defenses and in damage rates. In a survey of 55 species of shade-tolerant plants, we found that each species only invested in a subset of the,potential defensive mechanisms for young leaves. We measured rates of young leaf expansion, nitrogen content, delayed chloroplast development, synchrony of leaf production and rates of damage in the field. On a subset of 24 species, we also measured phenolic compounds, checked for the presence of saponins and alkaloids, and conducted bioassays using lepidopteran, coleopteran and orthopteran herbivores and. four fungal pathogens to test for toxicity of young leaf extracts. Certain combinations,of traits repeatedly co-occurred across unrelated species suggesting convergent evolution. We argue that selection has repeatedly led to tradeoffs among defenses such that species fall along an escape/defense continuum. At one extreme are species with a 'defense' strategy, which includes effective chemical defense, slow leaf expansion, normal greening and low rates of damage (less than 20% of the leaf area lost). At the other extreme are 'escape' species which have ineffective chemical defenses and, as a consequence, have high rates of leaf damage, >60% of leaf area lost during expansion. In partial compensation for ineffective chemical defense, these species have very rapid leaf expansion (doubling in area every day) which minimizes the window of vulnerability, delayed chloroplast development (white young leaves) which contain fewer resources, and synchronous leaf production to satiate herbivores. Thus, interspecific variation in young leaf damage rates is explained by differences in defense combinations along this escape/defense continuum. Because apparently beneficial traits such as effective chemical defense and rapid leaf expansion do not occur in the same species, we suggest that physiological constraints limit the defense combinations of any one species to a restricted subset of those observed. However, the defense and escape strategies do not represent different tradeoffs that have equal fitness, as species with the escape syndrome suffer much higher rates of damage. We hypothesize that the escape syndrome arose over evolutionary time among plants that failed to evolve effective secondary metabolites while herbivores succeeded in evolving adaptations to the chemistry of their host plant. Hence the defense syndrome should provide the greatest fitness, whereas the escape syndrome minimizes damage given the failure of the plant's secondary metabolites to provide protection. (C) 2003 Elsevier Science Ltd. All rights reserved. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Kursar, TA (reprint author), Univ Utah, Dept Biol, 257 South 1400 East, Salt Lake City, UT 84112 USA. NR 52 TC 146 Z9 159 U1 5 U2 72 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0305-1978 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD AUG PY 2003 VL 31 IS 8 BP 929 EP 949 DI 10.1016/S0305-1978(03)00087-5 PG 21 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 696TH UT WOS:000183903000008 ER PT J AU Zigler, KS Lessios, HA AF Zigler, KS Lessios, HA TI 250 million years of bindin evolution SO BIOLOGICAL BULLETIN LA English DT Article ID POSITIVE DARWINIAN SELECTION; ABALONE SPERM LYSIN; SEA-URCHIN EGGS; STRONGYLOCENTROTUS-FRANCISCANUS; MOLECULAR EVOLUTION; MITOCHONDRIAL-DNA; MEMBRANE-FUSION; RAPID EVOLUTION; PROTEIN BINDIN; SEQUENCE AB Bindin plays a central role in sperm-egg attachment and fusion in sea urchins (echinoids). Previous studies determined the DNA sequence of bindin in two orders of the class Echinoidea, representing 10% of all echinoid species. We report sequences of mature bindin from five additional genera, representing four new orders, including the distantly related sand dollars, heart urchins, and pencil urchins. The six orders in which bindin is now known include 70% of all echinoids, and indicate that bindin was present in the common ancestor of all extant sea urchins more than 250 million years ago. Over this span of evolutionary time there has been (1) remarkable conservation in the core region of bindin, particularly in a stretch of 29 amino acids that has not changed at all; (2) conservation of a motif of basic amino acids at the cleavage site between preprobindin and mature bindin; (3) more than a twofold change in length of mature bindin; and (4) emergence of high variation in the sequences outside the core, including the insertion of glycine-rich repeats in the bindins of some orders, but not others. C1 Smithsonian Trop Res Inst, Balboa, Panama. Duke Univ, Dept Biol, Durham, NC USA. RP Zigler, KS (reprint author), Univ Washington, Friday Harbor Labs, 620 Univ Rd, Friday Harbor, WA 98250 USA. NR 45 TC 37 Z9 38 U1 2 U2 7 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 J9 BIOL BULL-US JI Biol. Bull. PD AUG PY 2003 VL 205 IS 1 BP 8 EP 15 DI 10.2307/1543440 PG 8 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 714ZJ UT WOS:000184945300002 PM 12917217 ER PT J AU Larson, SR Jones, TA McCracken, CL Jensen, KB AF Larson, SR Jones, TA McCracken, CL Jensen, KB TI Amplified fragment length polymorphism in Elymus elymoides, Elymus multisetus, and other Elymus taxa SO CANADIAN JOURNAL OF BOTANY-REVUE CANADIENNE DE BOTANIQUE LA English DT Article DE AFLP; Elymus; nucleotide diversity; squirreltail ID NEEDLEGRASS NASSELLA-PULCHRA; NORTH-AMERICAN ELYMUS; PERENNIAL TRITICEAE; SYNTHETIC HYBRIDS; GENETIC-VARIATION; SITANION HYSTRIX; AFLP; GENERA; REGRESSION; CANADENSIS AB The geographic and phylogenetic significance of amplified fragment length polymorphism within and among 22 Elymus elymoides (Raf.) Swezey subsp. elymoides, 24 E. elymoides subsp. brevifolius (J.G. Sm.) Barkworth, and 13 Elymus multisetus (J.G. Sm.) Burtt-Davy squirreltail accessions was assessed relative to six other North American and three Eurasian Elymus taxa. Elymus elymoides and E. multisetus, comprising Elymus sect. Sitanion (Raf.) A. Love, were both monophyletic and closely related compared with other congeners. The monophyly of subsp. elymoides was also supported; subsp. brevifolius, however, was paraphyletic and separated into four genetically distinct groups. Estimates of nucleotide divergence among the five E. elymoides groups range from 0.0194 to 0.0288, with approximately 0.0329 differences per site between E. elymoides and E. multisetus. Corresponding estimates of nucleotide divergence range from 0.0243 to 0.0387 among North American taxa and from 0.0337 to 0.0455 between North American and Eurasian taxa. DNA polymorphism among E. elymoides accessions was correlated with geographic provenance and previously reported quantitative traits. Distinct genetic groups of E. elymoides generally correspond to different geographic regions, whereas divergent E. multisetus and E. elymoides accessions are sympatric. Thus, taxonomic ranks of E. multisetus and E. elymoides were supported and geographic groups within E. elymoides were distinguished. C1 Utah State Univ, USDA ARS, Forage & Range Res Lab, Logan, UT 84341 USA. Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA. RP Larson, SR (reprint author), Utah State Univ, USDA ARS, Forage & Range Res Lab, Logan, UT 84341 USA. OI McCracken, Carrie/0000-0002-8038-9727 NR 49 TC 21 Z9 23 U1 1 U2 3 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4026 J9 CAN J BOT JI Can. J. Bot.-Rev. Can. Bot. PD AUG PY 2003 VL 81 IS 8 BP 789 EP 804 DI 10.1139/B03-077 PG 16 WC Plant Sciences SC Plant Sciences GA 727DJ UT WOS:000185641100004 ER PT J AU Grosholz, ED Ruiz, GM AF Grosholz, ED Ruiz, GM TI Biological invasions drive size increases in marine and estuarine invertebrates SO ECOLOGY LETTERS LA English DT Article DE biological invasions; body size; climate change; extinction; fossil record; introduced species; marine invertebrates; range expansion ID CHARACTER DISPLACEMENT; SEXUAL DIMORPHISM; ANOLIS LIZARDS; BODY-SIZE; EVOLUTION; ISLANDS; PLANTS; DIFFERENTIATION; CONSEQUENCES; BIODIVERSITY AB Ecologists have long been fascinated by the morphological changes that species frequently undergo when introduced into new regions. In this study an unusual pattern of size change associated with the invasion of 19 species of marine and estuarine invertebrates is reported. The results show that the majority of species are significantly larger in the introduced range compared with the native range with little evidence for any decrease in size following invasion. This invasion-driven increase in body size sharply contrasts with the pattern observed in many other taxa including plants, mammals and lizards, where invaders frequently exhibit post-invasion decreases and increases in size. These size changes were not influenced by differences in latitude, sample size or length of time since invasion. Although several mechanisms, may explain the results, none have been demonstrated. C1 Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Grosholz, ED (reprint author), Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. RI Ross, Donald/F-7607-2012; OI Ross, Donald/0000-0002-8659-3833; Ruiz, Gregory/0000-0003-2499-441X NR 36 TC 49 Z9 53 U1 3 U2 30 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD AUG PY 2003 VL 6 IS 8 BP 700 EP 705 DI 10.1046/j.1461-0248.2003.00495.x PG 6 WC Ecology SC Environmental Sciences & Ecology GA 710QA UT WOS:000184689900005 ER PT J AU Langley, JA Dijkstra, P Drake, BG Hungate, BA AF Langley, JA Dijkstra, P Drake, BG Hungate, BA TI Ectomycorrhizal colonization, biomass, and production in a regenerating scrub oak forest in response to elevated CO2 SO ECOSYSTEMS LA English DT Article DE ectomycorrhizae; fine roots; ingrowth bags; production; turnover; Quercus ID ATMOSPHERIC CARBON-DIOXIDE; MYCORRHIZAL COLONIZATION; ROOT PRODUCTION; QUERCUS-ALBA; ECOSYSTEM; GROWTH; SOIL; DECOMPOSITION; GRASSLANDS; FUNGI AB The effects of CO2 elevation on the dynamics of fine root (FR) mass and ectomycorrhizal (EM) mass and colonization were studied in situ in a Florida scrub oak system over four years of postfire regeneration. Soil cores were taken at five dates and sorted to assess the standing crop of ectomycorrhizal and fine roots. We used ingrowth bags to estimate the effects of elevated CO2 on production of EM roots and fine roots. Elevated CO2 tended to increase EM colonization frequency but did not affect EM mass nor FR mass in soil cores (standing mass). However, elevated CO2 strongly increased EM mass and FR mass in ingrowth bags (production), but it did not affect the EM colonization frequency therein. An increase in belowground production with unchanged biomass indicates that elevated CO2 may stimulate root turnover. The CO2-stimulated increase of belowground production was initially larger than that of aboveground production. The oaks may allocate a larger portion of resources to root/mycorrhizal production in this system in elevated rather than ambient CO2. C1 No Arizona Univ, Dept Biol Sci, 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 Biol Sci, 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 36 TC 11 Z9 12 U1 2 U2 17 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 1432-9840 J9 ECOSYSTEMS JI Ecosystems PD AUG PY 2003 VL 6 IS 5 BP 424 EP 430 DI 10.1007/s10021-002-0194-5 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 720HU UT WOS:000185256000002 ER PT J AU Meyerson, LA Reaser, JK AF Meyerson, LA Reaser, JK TI Bioinvasions, bioterrorism, and biosecurity SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Review ID INFECTIOUS-DISEASES; UNITED-STATES; BIODIVERSITY; AGRICULTURE; THREATS; IMPACT; MEXICO; HEALTH; TRENDS AB Despite their high profile and potentially devastating consequences, bioterrorist acts are relatively unpredictable, rare, and thus far small-scale events. In contrast, biological invasions are occurring daily in the US and have significant impacts on human health, agriculture, infrastructure, and the environment, yet they receive far less attention and fewer resources. Scientists and the US government must work together to implement a comprehensive approach to biosecurity that addresses not only bioterrorism, but also the more common incursions of invasive alien species. This approach should also address the potential for the deliberate use of invasive alien species as agents of bioterrorism. To achieve these goals, it will be necessary for the relevant government institutions to acknowledge and include prevention, early detection, and rapid response to species incursions as central mission themes. In addition, the scientific community, industry, and the public must work together to ensure that the necessary technology and information systems are readily available. C1 US EPA, Amer Assoc Adv Sci Fellow, Natl Ctr Environm Assessment, Washington, DC 20460 USA. Ecos Syst Inst, Springfield, VA 22150 USA. Museum Natl Hist Nat, Smithsonian Inst, Washington, DC 20560 USA. RP Meyerson, LA (reprint author), US EPA, Amer Assoc Adv Sci Fellow, Natl Ctr Environm Assessment, Washington, DC 20460 USA. EM meyerson.laura@nmnh.si.edu RI Meyerson, Laura/K-9013-2012; Meyerson, Laura/D-4487-2013 NR 50 TC 32 Z9 34 U1 2 U2 14 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD AUG PY 2003 VL 1 IS 6 BP 307 EP 314 DI 10.2307/3868091 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 825WZ UT WOS:000221790800019 ER PT J AU Wehncke, EV Hubbell, SP Foster, RB Dalling, JW AF Wehncke, EV Hubbell, SP Foster, RB Dalling, JW TI Seed dispersal patterns produced by white-faced monkeys: implications for the dispersal limitation of neotropical tree species SO JOURNAL OF ECOLOGY LA English DT Article DE Cebus capucinus; dispersal effectiveness; primate dispersal; recruitment limitation; seed dispersal ID TROPICAL RAIN-FOREST; BROWN CAPUCHIN MONKEYS; INDIVIDUAL SPATIAL CHOICE; CEBUS-APELLA; RECRUITMENT LIMITATION; FORAGING GROUPS; FRENCH-GUIANA; HOME-RANGE; DIVERSITY; CONSEQUENCES AB 1 Primate frugivores are important seed dispersers for a large fraction of tree species in many tropical forests. The movement, diet preferences and defecation patterns produced by primates may therefore strongly influence seed dispersion patterns and seedling recruitment success. Here we examine the pattern of seed dispersal generated by white-faced monkeys (Cebus capucinus ) in relation to adult tree distribution in the 50-ha plot on Barro Colorado Island (BCI), Panama. 2 Diet breadth of Cebus was remarkably wide. Over four months they consumed fruits of 95 out of an estimated 240 species available. Seeds of 67 species passed intact through the gut and 28 were spat out. 3 Dispersal effectiveness of Cebus was also high. Two Cebus groups on average spent < 10 min feeding in individual trees, had large home ranges (> 150 ha), travelled 1-3 km day(-1) and defecated seeds in small clumps throughout the day. 4 Mean dispersal distance of ingested seeds was 216 m (range 20-844 m), with the highest probability of dispersal 100-200 m from the parent plant. For six of nine species studied, the distance between defecation sites and nearest conspecific adults of seeds in faeces was not significantly different from random expectations. 5 The scattered dispersal pattern produced by Cebus suggests that this species contributes relatively little to dispersal limitation (sensu Nathan & Muller-Landau 2000) compared to other dispersers in the community. Long-distance dispersal by Cebus resulted in substantial movement of seeds in and out of the 50 ha plot, and suggests that inverse modelling procedures to estimate dispersal functions from trap data may not adequately describe dispersal patterns generated by this primate. C1 Univ Nacl Autonoma Mexico, Lab Interac Planta Anim, Dept Ecol Evolut, Mexico City 04510, DF, Mexico. Smithsonian Trop Res Inst, Balboa, Panama. Univ Georgia, Dept Bot, Athens, GA 30602 USA. Field Museum, Dept Bot, Chicago, IL 60605 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Wehncke, EV (reprint author), Univ Nacl Autonoma Mexico, Lab Interac Planta Anim, Dept Ecol Evolut, Apartado 70-275,Ciudad Univ,Circuito Rxterior, Mexico City 04510, DF, Mexico. NR 79 TC 75 Z9 81 U1 2 U2 38 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD AUG PY 2003 VL 91 IS 4 BP 677 EP 685 DI 10.1046/j.1365-2745.2003.00798.x PG 9 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 703FA UT WOS:000184268300015 ER PT J AU Woodman, N Cuartas-Calle, CA Delgado, CA AF Woodman, N Cuartas-Calle, CA Delgado, CA TI The humerus of Cryptotis colombiana and its bearing on the species' phylogenetic relationships (Soricomorpha : Soricidae) SO JOURNAL OF MAMMALOGY LA English DT Article DE anatomy; Cryptotis; Insectivora; morphology; osteology ID SMALL-EARED SHREW; MAMMALIA; INSECTIVORA AB The Colombian small-eared shrew, Cryptotis colombiana Woodman and Timm, was described from the Colombian Andes in 1993. Its original allocation to the C. nigrescens group recently was questioned based on several cranial characters the species appeared to share with some members of the C. thomasi group. We review characteristics of the C. nigrescens and C. thomasi groups, and we describe the humerus of C. colombiana and the humerus and manus of C. medellinia. The morphology of the humerus joins the suite of characters that supports the hypotheses that C. colombiana is not a member of the C. thomasi group and that all remaining South American species form a cohesive, definable set that is probably monophyletic. C1 Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, MRC 111, Washington, DC 20013 USA. Univ Antioquia, Inst Biol, Medellin 1226, Colombia. RP Woodman, N (reprint author), Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, MRC 111, POB 37012, Washington, DC 20013 USA. EM woodman.neal@nmnh.si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 12 TC 9 Z9 13 U1 0 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD AUG PY 2003 VL 84 IS 3 BP 832 EP 839 DI 10.1644/BME-007 PG 8 WC Zoology SC Zoology GA 718MC UT WOS:000185149300004 ER PT J AU Jakab, PL AF Jakab, PL TI First to fly: North Carolina and the beginnings of aviation. SO JOURNAL OF SOUTHERN HISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Jakab, PL (reprint author), Smithsonian Inst, Natl Air & Space Museum, 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 AUG PY 2003 VL 69 IS 3 BP 729 EP 730 PG 2 WC History SC History GA 708YG UT WOS:000184597500065 ER PT J AU Kensley, B Cartes, JE AF Kensley, B Cartes, JE TI Records and distribution of Syscenus infelix in the deep Mediterranean (Crustacea : Isopoda : Aegidae) SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article ID FISHES AB The parasitic isopod Syscenus infelix is recorded from the Mediterranean, based on 19 specimens from a depth range of 375-2071 m. The first ovigerous female of the species is also recorded. Patterns of possible parasitism were suggested based on the depth distribution of S. infelix, and their possible host macrourid fish below 900 m depth in the Catalano-Balearic basin. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. CSIC, Inst Ciencies Mar Barcelona, Barcelona 080003, Spain. RP Kensley, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 8 TC 3 Z9 4 U1 1 U2 4 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD AUG PY 2003 VL 83 IS 4 BP 775 EP 777 DI 10.1017/S002531540300777Xh PG 3 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 719KM UT WOS:000185202300015 ER PT J AU Endo, H Sasaki, M Narushima, E Komiya, T Hayashida, A Hayashi, Y Stafford, BJ AF Endo, H Sasaki, M Narushima, E Komiya, T Hayashida, A Hayashi, Y Stafford, BJ TI Macroscopic study of the functional significance of the forearm muscles in the giant panda SO JOURNAL OF VETERINARY MEDICAL SCIENCE LA English DT Article DE accessory carpal bone; forearm; giant panda; radial sesamoid bone ID RADIAL SESAMOID BONE; AILUROPODA-MELANOLEUCA; ANATOMY AB The extensor and flexor group muscles and their related muscles were functional-morphologically observed in the dead body of the giant panda to clarify the action of the forearm and the palm in the manipulation of the species. The Musculus flexor carpi ulnaris had two developed heads, however, we can conclude that the contraction of this muscle slightly changes the angle of the accessory carpal bone to the ulna. The data pointed out that the accessory carpal bone acts as a supporting post, when the giant panda seizes the object. The M. abductor digiti I longus possessed the well-developed origin in both ulna and radius. These findings suggest that this muscle may function as a supinator of the forearm. We also suggest that the well-developed M. pronator quadratus and M. pronator teres, and the proximal part of the M. abductor digiti I longus and the M. supinator may efficiently contribute to the pronator-spinator action of the forearm, when the giant panda brings the food to its mouth using the manipulation system equipped in the palm region. C1 Natl Sci Museum, Dept Zool, Shinjuku Ku, Tokyo 1690073, Japan. Obihiro Univ Agr & Vet Med, Dept Vet Anat, Obihiro, Hokkaido 0108666, Japan. Ueno Zool Gardens, Tokyo 1108701, Japan. Rakuno Gakuen Univ, Fac Med Vet, Dept Toxicol, Ebetsu, Hokkaido 0698501, Japan. Univ Tokyo, Grad Sch Agr & Life Sci, Dept Vet Anat, Tokyo 1138567, Japan. Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA. RP Endo, H (reprint author), Natl Sci Museum, Dept Zool, Shinjuku Ku, 3-23-1 Hyakunin Cho, Tokyo 1690073, Japan. NR 17 TC 2 Z9 3 U1 0 U2 3 PU JAPAN SOC VET SCI PI TOKYO PA UNIV TOKYO, 1-1-1 YAYOI, BUNKYO-KU, TOKYO, 103, JAPAN SN 0916-7250 J9 J VET MED SCI JI J. Vet. Med. Sci. PD AUG PY 2003 VL 65 IS 8 BP 839 EP 843 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA 719PR UT WOS:000185212700003 PM 12951414 ER PT J AU Endo, H Hikida, T Motokawa, M Chou, LM Fukuta, K Stafford, BJ AF Endo, H Hikida, T Motokawa, M Chou, LM Fukuta, K Stafford, BJ TI Morphological adaptation of the skull for various behaviors in the tree shrews SO JOURNAL OF VETERINARY MEDICAL SCIENCE LA English DT Article DE adaptation; behavior; osteometry; skull; Tupaiidae ID TUPAIA-GLIS; THAILAND AB Skull size and shape were examined among 14 species of the tree shrews (Tupaia montana, T. picta, T. splendidula, T. mulleri, T. longipes, T. glis, T. javanica, T. minor, T. gracilis, T. dorsalis, T. tana, Dendrogale melanura, D. murina, and Ptilocercus lowii). The bones of face were rostro-caudally longer in T. tana and T. dorsalis, contrasting with T. minor and T. gracilis, D. melanura, D. murina and P. lowii which have smaller facial length ratios. The arbo-terrestrial species (T. longipes and T. glis) were similar to terrestrial species in length ratios of bones of face unlike the other arbo-terrestrial species (T. montana., T. picta, T. splendidula, and T. mulleri). We propose that T. longipes and T. glis have adapted to foraging for termites and ants as have T. tana and T dorsalis. Additionally small body size in T. javanica may be the result of being isolated in Java. We separated the species into 5 groups from the measurment values of skulls: 1) Terrestrial species; T. tana and T dorsalis, 2) Arboreal species; T. minor and T. gracilis, 3) Arbo-terrestrial species group 1: T. montana. T. splendidula, T. picta and T. mulleri, and T. javanica, 4) Arbo-terrestrial species group 2: T. glis and T longipes, 5) Arboreal species of Dendrogale and Ptilocercus. Principal component analysis separated species into 8 clusters as follows: 1) T. tana, 2) T. dorsalis, 3) T. montana, T. splendidula, T. picta and T. mulleri, 4) T. glis and T. longipes, 5) T. javanica, 6) T. minor and T. gracilis, 7) D. melanura and D. murina, and 8) P. lowii. We suggest that these clusters correspond to behavioral strategies and peculiarities observed in foraging, feeding and locomotion in each species. C1 Natl Sci Museum, Dept Zool, Shinjuku Ku, Tokyo 1690073, Japan. Kyoto Univ, Fac Sci, Dept Zool, Kyoto 6068501, Japan. Kyoto Univ, Univ Museum, Kyoto 6068501, Japan. Natl Univ Singapore, Raffles Museum Biodivers Res, Singapore 117548, Singapore. Nagoya Univ, Grad Sch Bioagr Sci, Lab Anim Morphol & Funct, Nagoya, Aichi 4648601, Japan. Smithsonian Inst, Natl Museum Nat Hist, Div Mammal, Washington, DC 20560 USA. Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA. RP Endo, H (reprint author), Natl Sci Museum, Dept Zool, Shinjuku Ku, 3-23-1 Hyakunin Cho, Tokyo 1690073, Japan. RI Chou, Loke Ming/I-2951-2012 NR 25 TC 4 Z9 5 U1 0 U2 8 PU JAPAN SOC VET SCI PI TOKYO PA UNIV TOKYO, 1-1-1 YAYOI, BUNKYO-KU, TOKYO, 103, JAPAN SN 0916-7250 J9 J VET MED SCI JI J. Vet. Med. Sci. PD AUG PY 2003 VL 65 IS 8 BP 873 EP 879 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA 719PR UT WOS:000185212700008 PM 12951419 ER PT J AU Hutchinson, A AF Hutchinson, A TI Bear in mind: The California grizzly. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Hutchinson, A (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 2003 VL 128 IS 13 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 710VG UT WOS:000184703100284 ER PT J AU Riley, S AF Riley, S TI Present value. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 2003 VL 128 IS 13 BP 137 EP 137 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 710VG UT WOS:000184703100367 ER PT J AU Grapes, RH Wysoczanski, RJ Hoskin, PWO AF Grapes, RH Wysoczanski, RJ Hoskin, PWO TI Rhonite paragenesis in pyroxenite xenoliths, Mount Sidley volcano, Marie Byrd Land, West Antarctica SO MINERALOGICAL MAGAZINE LA English DT Article DE rhonote; pyroxenite xenoliths; Mount Sidney; volcano; Antarctica; kaersutite ID AMPHIBOLE; OCCURRENCES; PETROLOGY; LAVAS AB Rhonite occurs in lower crustal pyroxenite xenoliths erupted in phonolite from the Mount Sidley composite volcano, Marie Byrd Land, Antarctica, as a localized breakdown product, with plagioclase, clinopyroxene, +/- olivine +/- Ti-magnetite + melt, of kaersutite, and as rnicrophenocrysts (with olivine, plagioclase, clinopyroxene) in pockets of basanitic melt. Rhonite after kaersutite has a more NaSi-rich/ CaAl-poor composition, lower Ti, and formed at higher oxidation (similar toNNO) conditions than rhonite Occurring as microphenocrysts in basanite. Comparison with experimentally deterinined rhonite stability in understaturated alkali basalt and as a reaction product after Ti-amphibole indicates that the Mount Sidley rhonite (and associated minerals) formed between 1090 and 1190 degreesC at <0.5 kbar, presumably during temporary residence of the xenoliths in a shallow magma chamber below the volcanic edifice. C1 Univ Freiburg, Inst Mineral Petr & Geochem, D-79104 Freiburg, Germany. Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Grapes, RH (reprint author), Univ Freiburg, Inst Mineral Petr & Geochem, Hugstetter Str 55, D-79104 Freiburg, Germany. RI Wysoczanski, Richard/C-2930-2009; Wysoczanski, Richard/I-7730-2012 NR 31 TC 11 Z9 14 U1 0 U2 1 PU MINERALOGICAL SOCIETY PI LONDON PA 41 QUEENS GATE, LONDON SW7 5HR, ENGLAND SN 0026-461X J9 MINERAL MAG JI Mineral. Mag. PD AUG PY 2003 VL 67 IS 4 BP 639 EP 651 DI 10.1180/0026461036740123 PG 13 WC Mineralogy SC Mineralogy GA 722GB UT WOS:000185366100006 ER PT J AU Songsasen, N Yu, I Gomez, M Leibo, SP AF Songsasen, N Yu, I Gomez, M Leibo, SP TI Effects of meiosis-inhibiting agents and equine chorionic gonadotropin on nuclear maturation of canine oocytes SO MOLECULAR REPRODUCTION AND DEVELOPMENT LA English DT Article DE canine oocytes; nuclear maturation; dbcAMP; roscovitine; equine chorionic gonadotropin ID IN-VITRO MATURATION; HIGH DEVELOPMENTAL COMPETENCE; PREPUBERTAL GOAT OOCYTES; MEIOTIC COMPETENCE; BOVINE OOCYTES; BUTYROLACTONE-I; PIG OOCYTES; GERMINAL VESICLE; ANTRAL FOLLICLES; BITCH OOCYTES AB Experiments were conducted to determine the effects of meiosis-inhibiting-agents and gonadotropins on nuclear maturation of canine oocytes. The culture medium was TCM199 + 10 ng/ml epidermal growth factor supplemented with 25 muM beta-mercapto-ethanol, 0.25 mM pyruvate, and 1.0 mM L-glutamine (Basal TCM). Initially, oocytes were cultured in Basal TCM alone or in Basal TCM + dibutylryl cyclic adenosine monophosphate (0.5, 1, 5, or 10 mM dbcAMP) for 24 hr. Dibutylryl cAMP inhibited resumption of meiosis in a dose-dependent manner; 60% of oocytes remained at the germinal vesicle (GV) stage after being cultured for 24 hr in 5 mM dbcAMP. The meiosis-inhibitory effect of dbcAMP appeared to be reversible, as the oocytes resumed meiosis and completed nuclear maturation after being cultured for an additional 48 hr in its absence. Oocytes were then cultured in Basal TCM alone or in Basal TCM + roscovitine (12.5, 25, or 50 muM) for 24 hr. Although similar to60% of oocytes cultured in 25 muM roscovitine remained at the GV stage, this percentage was not significantly different from the 48% that also remained at the GV stage when cultured in its absence. Oocytes were cultured in Basal TCM + 25 1.0 roscovitine for 17 hr, exposed briefly to equine chorionic gonadotropin (eCG), and then cultured in Basal TCM for 48 hr. Short exposure of oocytes to eCG was beneficial, as it significantly increased the proportion of oocytes developing beyond germinal vesicle breakdown (P < 0.05) with similar to20-30% of these were metaphase I (MI) oocytes. Study of the kinetics of nuclear maturation demonstrated that large numbers of oocytes remained at MI even after being cultured for 52 hr following brief exposure to eCG. This study showed that in vitro maturation of canine oocytes can be somewhat improved by short exposure of oocytes to eCG. However, further studies are still required to derive effective methods to mature canine oocytes in vitro. (C) 2003 Wiley-Liss, Inc. C1 Univ New Orleans, Dept Sci Biol, New Orleans, LA USA. Audubon Ctr Res Endangered Species, New Orleans, LA USA. Louisiana State Univ, Ctr Agr, Baton Rouge, LA 70803 USA. RP Songsasen, N (reprint author), Smithsonian Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 73 TC 19 Z9 24 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 1040-452X J9 MOL REPROD DEV JI Mol. Reprod. Dev. PD AUG PY 2003 VL 65 IS 4 BP 435 EP 445 DI 10.1002/mrd.10321 PG 11 WC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology SC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology GA 700QK UT WOS:000184122500011 PM 12840817 ER PT J AU Jones, LR Ponman, TJ Horton, A Babul, A Ebeling, H Burke, DJ AF Jones, LR Ponman, TJ Horton, A Babul, A Ebeling, H Burke, DJ TI The nature and space density of fossil groups of galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : general; X-rays : galaxies : clusters ID BRIGHTEST CLUSTER GALAXIES; X-RAY-CLUSTERS; N-BODY SIMULATIONS; POOR CLUSTERS; WARPS SURVEY; HIERARCHICAL-MODELS; LUMINOSITY FUNCTION; MERGER RATES; CD GALAXIES; EVOLUTION AB We describe the properties of a sample of galaxy groups with very unusual distributions of galaxy luminosities. The most extreme example has an X-ray luminosity similar to that of the Virgo cluster but has a very low richness, with only one galaxy brighter than L *, compared with six in Virgo. That one galaxy, however, is optically more luminous than any galaxy in Virgo and has an optical luminosity as bright as many of the central cD galaxies in rich Abell clusters. The characteristic feature of the fossil groups we study is that most of the light arises from one dominant, central galaxy. We define a fossil system and, based on this definition, construct a small X-ray-selected, flux-limited sample of fossil groups with well-known selection criteria. We confirm that these systems are indeed groups of galaxies, but dominated by one central luminous giant elliptical galaxy and with few, or no, L * galaxies. We find that fossil systems represent 8-20 per cent of all systems of the same X-ray luminosity. Fossil groups are at least as numerous as all poor and rich clusters combined, and are thus a possible site for the formation of luminous central cluster galaxies before infall into clusters occurs. The fossil systems in our sample have significantly higher X-ray luminosities than normal groups of similar total optical luminosities (or similar X-ray temperature, where the latter can be measured). These enhanced X-ray luminosities may be due to relatively cool gas in the innermost regions or due to a low central gas entropy. We interpret fossil groups as old, undisturbed systems which have avoided infall into clusters, but where galaxy merging of most of the L * galaxies has occurred. An early formation epoch, before that of most groups, could explain low central gas entropies and high X-ray luminosities. C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jones, LR (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. NR 76 TC 187 Z9 188 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 AUG 1 PY 2003 VL 343 IS 2 BP 627 EP 638 DI 10.1046/j.1365-8711.2003.06702.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 704HT UT WOS:000184334600031 ER PT J AU Erhardt, D AF Erhardt, D TI Not-so-new technology SO NATURE MATERIALS LA English DT News Item C1 Smithsonian Inst, Museum Support Ctr, Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. RP Erhardt, D (reprint author), Smithsonian Inst, Museum Support Ctr, Smithsonian Ctr Mat Res & Educ, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 0 TC 7 Z9 8 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1476-1122 J9 NAT MATER JI Nat. Mater. PD AUG PY 2003 VL 2 IS 8 BP 509 EP 510 DI 10.1038/nmat951 PG 2 WC Chemistry, Physical; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 710NW UT WOS:000184687200006 PM 12894257 ER PT J AU Engelbrecht, BMJ Kursar, TA AF Engelbrecht, BMJ Kursar, TA TI Comparative drought-resistance of seedlings of 28 species of co-occurring tropical woody plants SO OECOLOGIA LA English DT Article DE growth; irrigation; soil moisture; survival; tropical moist forest ID EL-NINO DROUGHT; RAIN-FOREST; TREE SEEDLINGS; MOIST FOREST; HABITAT ASSOCIATIONS; VIROLA-SURINAMENSIS; WATER RELATIONS; GROWTH; SURVIVAL; TOLERANCE AB Quantifying plant drought resistance is important for understanding plant species' association to microhabitats with different soil moisture availability and their distribution along rainfall gradients, as well as for understanding the role of underlying morphological and physiological mechanisms. The effect of dry season drought on survival and leaf-area change of first year seedlings of 28 species of co-occurring woody tropical plants was experimentally quantified in the understory of a tropical moist forest. The seedlings were subjected to a drought or an irrigation treatment in the forest for 22 weeks during the dry season. Drought decreased survival and growth (assessed as leaf-area change) in almost all of the species. Both survival and leaf-area change in the dry treatment ranged fairly evenly from 0% to about 100% of that in the irrigated treatment. In 43% of the species the difference between treatments in survival was not significant even after 22 weeks. In contrast, only three species showed no significant effect of drought on leaf-area change. The effects of drought on species' survival and growth were not correlated with each other, reflecting different strategies in response to drought. Seedling size at the onset of the dry season had no significant effect on species' drought response. Our study is the first to comparatively assess seedling drought resistance in the habitat for a large number of tropical species, and underlines the importance of drought for plant population dynamics in tropical forests. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Engelbrecht, BMJ (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. RI Engelbrecht, Bettina/E-9914-2012 NR 64 TC 126 Z9 137 U1 5 U2 54 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD AUG PY 2003 VL 136 IS 3 BP 383 EP 393 DI 10.1007/s00442-003-1290-8 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 711RZ UT WOS:000184756000007 PM 12811534 ER PT J AU Torres, DF Romero, GE Dame, TM Combi, JA Butt, YM AF Torres, DF Romero, GE Dame, TM Combi, JA Butt, YM TI Supernova remnants and gamma-ray sources SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS LA English DT Review DE gamma-rays; observations; gamma-rays; theory; ISM; supernova remnants; ISM; clouds; cosmic rays ID UNIDENTIFIED EGRET SOURCES; GALACTIC PLANE SURVEY; HIGH-ENERGY EMISSION; ACCELERATED COSMIC-RAYS; RADIO-CONTINUUM SURVEY; PULSAR SAX J0635+0533; ACCRETING BLACK-HOLE; AIR-SHOWER ARRAY; EARLY-TYPE STARS; X-RAY AB A review of the possible relationship between x-ray sources and supernova remnants (SNRs) is presented. Particular emphasis is given to the analysis of the observational status of the problem of cosmic ray acceleration at SNR shock fronts. All positional coincidences between SNRs and unidentified gamma-ray sources listed in the Third EGRET Catalog at low Galactic latitudes are discussed on a case by case basis. For several coincidences of particular interest, new CO(J = 1 - 0) and radio continuum maps are shown, and the mass content of the SNR surroundings is determined. The contribution to the T-ray flux observed that might come from cosmic ray particles (particularly nuclei) locally accelerated at the SNR shock fronts is evaluated. We discuss the prospects for future research in this field and remark on the possibilities for observations with forthcoming gamma-ray instruments. (C) 2003 Published by Elsevier B.V. C1 Lawrence Livermore Lab, Livermore, CA 94550 USA. Inst Argentino Radioastron, Buenos Aires, DF, Argentina. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lawrence Livermore Lab, 7000 E Ave,L-413, Livermore, CA 94550 USA. EM dtorres@igpp.uclln1.org RI Torres, Diego/O-9422-2016 OI Torres, Diego/0000-0002-1522-9065 NR 293 TC 104 Z9 104 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-1573 EI 1873-6270 J9 PHYS REP JI Phys. Rep.-Rev. Sec. Phys. Lett. PD AUG PY 2003 VL 382 IS 6 BP 303 EP 380 DI 10.1016/S0370-1573(03)00201-1 PG 78 WC Physics, Multidisciplinary SC Physics GA 703RG UT WOS:000184294300001 ER PT J AU Hanson, DT Franklin, LA Samuelsson, G Badger, MR AF Hanson, DT Franklin, LA Samuelsson, G Badger, MR TI The Chlamydomonas reinhardtii cia3 mutant lacking a thylakoid lumen-localized carbonic anhydrase is limited by CO2 supply to rubisco and not photosystem II function in vivo SO PLANT PHYSIOLOGY LA English DT Article ID INORGANIC CARBON; CONCENTRATING MECHANISM; CO2-CONCENTRATING MECHANISMS; DEFICIENT MUTANTS; QUANTUM YIELD; PHOTOSYNTHESIS; EXCHANGE; OXYGEN; ALGAE; TRANSPORT AB The Chlamydomonas reinhardtii cia3 mutant has a phenotype indicating that it requires high-CO2 levels for effective photosynthesis and growth. It was initially proposed that this mutant was defective in a carbonic anhydrase (CA) that was a key component of the photosynthetic CO2-concentrating mechanism (CCM). However, more recent identification of the genetic lesion as a defect in a lumenal CA associated with photosystem II (PSII) has raised questions about the role of this CA in either the CCM or PSII function. To resolve the role of this lumenal CA, we re-examined the physiology of the cia3 mutant. We confirmed and extended previous gas exchange analyses by using membrane-inlet mass spectrometry to monitor O-16(2), O-18(2), and CO2 fluxes in vivo. The results demonstrate that PSII electron transport is not limited in the cia3 mutant at low inorganic carbon (Ci). We also measured metabolite pools sizes and showed that the RuBP pool does not fall to abnormally low levels at low Ci as might be expected by a photosynthetic electron transport or ATP generation limitation. Overall, the results demonstrate that under low Ci conditions, the mutant lacks the ability to supply Rubisco with adequate CO2 for effective CO2 fixation and is not limited directly by any aspect of PSII function. We conclude that the thylakoid CA is primarily required for the proper functioning of the CCM at low Ci by providing an ample supply of CO2 for Rubisco. C1 Australian Natl Univ, Res Sch Biol Sci, Mol Plant Physiol Grp, Canberra, ACT 2601, Australia. Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Umea Univ, Dept Plant Physiol, Umea Plant Sci Ctr, S-90187 Umea, Sweden. RP Badger, MR (reprint author), Australian Natl Univ, Res Sch Biol Sci, Mol Plant Physiol Grp, GPO Box 475, Canberra, ACT 2601, Australia. RI Hanson, David/J-8034-2012; Samuelsson, Goran/E-1824-2015; Badger, Murray/C-8153-2009 NR 43 TC 44 Z9 47 U1 0 U2 7 PU AMER SOC PLANT BIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD AUG PY 2003 VL 132 IS 4 BP 2267 EP 2275 DI 10.1104/pp.103.023481 PG 9 WC Plant Sciences SC Plant Sciences GA 710ZV UT WOS:000184713400053 PM 12913181 ER PT J AU Kim, HG Funk, VA Vlasak, A Zimmer, EA AF Kim, HG Funk, VA Vlasak, A Zimmer, EA TI A phylogeny of the Munnoziinae (Asteraceae, Liabeae): circumscription of Munnozia and a new placement of M-perfoliata SO PLANT SYSTEMATICS AND EVOLUTION LA English DT Article DE Asteraceae; Cichorioideae; Liabeae; Munnoziinae; Liabinae; Paranepheliinae; Phylogeny; internal transcribed spacer (ITS); parsimony and maximum likelihood analyses; monophyly; paraphyly; biogeography ID NUCLEAR RIBOSOMAL DNA; TRANSCRIBED SPACER SEQUENCES; MOLECULAR EVIDENCE; DATA SETS; EVOLUTION; GENUS; BIOGEOGRAPHY; CONFIDENCE; COMPOSITAE; ORIGIN AB The tribe Liabeae (Compositae, Cichorioideae) comprises three subtribes, Liabinae, Munnoziinae, and Paranepheliinae. For one of these, the Munnoziinae, which contains the genera Munnozia, Chrysactinium, Erato, and Philoglossa, the nuclear ITS (internal transcribed spacer) region was sequenced to examine the monophyly of the subtribe and the core genus Munnozia within it. Thirty-six samples representing four currently recognized genera of Munnoziinae and two outgroups were included in this study. Molecular phylogenetic analyses confirm the close relationship of Munnozia with Chrysactinium, and Erato with Philoglossa. However, the monophyly of the Munnoziinae and Munnozia is not supported, in disagreement with the current morphological findings. The discrepancies were attributed to the placements of Munnozia perfoliata outside the Munnoziinae and Munnozia, and Chrysactinium within Munnozia. The resulting tree indicates that first, M. perfoliata needs to be moved out of the munnoziinae and second, Chrysactinium originated from within Munnozia. For the first finding, morphological and palynological reevaluation of this species with allegedly related species reveals additional support in agreement with molecular data. Therefore we propose that the genus Munnozia be re-delimited to the members having black or dark brown anther theca and sordid or reddish pappus and re-organized. C1 Smithsonian Inst, Museum Support Ctr, Labs Analyt Biol, Suitland, MD 20746 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Div Bot, Washington, DC 20560 USA. RP Kim, HG (reprint author), Univ Texas, Dept Biol Sci, Sect Integrat Biol, Austin, TX 78713 USA. RI Zimmer, Elizabeth/G-3890-2011 NR 51 TC 8 Z9 10 U1 0 U2 1 PU SPRINGER-VERLAG WIEN PI VIENNA PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 VIENNA, AUSTRIA SN 0378-2697 J9 PLANT SYST EVOL JI Plant Syst. Evol. PD AUG PY 2003 VL 239 IS 3-4 BP 171 EP 185 DI 10.1007/s00606-003-0003-4 PG 15 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 719KE UT WOS:000185201600001 ER PT J AU Kennicutt, RC Armus, L Bendo, G Calzetti, D Dale, DA Draine, BT Engelbracht, CW Gordon, KD Grauer, AD Helou, G Hollenbach, DJ Jarrett, TH Kewley, LJ Leitherer, C Li, A Malhotra, S Regan, MW Rieke, GH Rieke, MJ Roussel, H Smith, JDT Thornley, MD Walter, F AF Kennicutt, RC Armus, L Bendo, G Calzetti, D Dale, DA Draine, BT Engelbracht, CW Gordon, KD Grauer, AD Helou, G Hollenbach, DJ Jarrett, TH Kewley, LJ Leitherer, C Li, A Malhotra, S Regan, MW Rieke, GH Rieke, MJ Roussel, H Smith, JDT Thornley, MD Walter, F TI SINGS: The SIRTF nearby galaxies survey SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Review ID STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; SPACE-OBSERVATORY ATLAS; VIRGO CLUSTER GALAXIES; BRIGHT SPIRAL GALAXIES; SHORT-WAVELENGTH SPECTROMETER; FABRY-PEROT OBSERVATIONS; CLERK-MAXWELL-TELESCOPE; WESTERBORK HI SURVEY; INTERSTELLAR-MEDIUM AB The SIRTF Nearby Galaxy Survey is a comprehensive infrared imaging and spectroscopic survey of 75 nearby galaxies. Its primary goal is to characterize the infrared emission of galaxies and their principal infrared-emitting components, across a broad range of galaxy properties and star formation environments. SINGS will provide new insights into the physical processes connecting star formation to the interstellar medium properties of galaxies and provide a vital foundation for understanding infrared observations of the distant universe and ultraluminous and active galaxies. The galaxy sample and observing strategy have been designed to maximize the scientific and archival value of the data set for the SIRTF user community at large. The SIRTF images and spectra will be supplemented by a comprehensive multiwavelength library of ancillary and complementary observations, including radio continuum, H I, CO, submillimeter, BVRIJHK, Halpha, Paalpha, ultraviolet, and X-ray data. This paper describes the main astrophysical issues to be addressed by SINGS, the galaxy sample and the observing strategy, and the SIRTF and other ancillary data products. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. CALTECH, Pasadena, CA 91101 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Bucknell Univ, Dept Phys, Lewisburg, PA 17837 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Kennicutt, RC (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. OI Draine, Bruce/0000-0002-0846-936X NR 106 TC 776 Z9 779 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 2003 VL 115 IS 810 BP 928 EP 952 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 704DK UT WOS:000184322400002 ER PT J AU Evans, NJ Allen, LE Blake, GA Boogert, ACA Bourke, T Harvey, PM Kessler, JE Koerner, DW Lee, CW Mundy, LG Myers, PC Padgett, DL Pontoppidan, K Sargent, AI Stapelfeldt, KR van Dishoeck, EF Young, CH Young, KE AF Evans, NJ Allen, LE Blake, GA Boogert, ACA Bourke, T Harvey, PM Kessler, JE Koerner, DW Lee, CW Mundy, LG Myers, PC Padgett, DL Pontoppidan, K Sargent, AI Stapelfeldt, KR van Dishoeck, EF Young, CH Young, KE TI From molecular cores to planet-forming disks: An SIRTF legacy program SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID TELESCOPE-FACILITY SIRTF; INTERMEDIATE-MASS STARS; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISKS; ISO SPECTROSCOPY; BROWN DWARFS; SPECTRAL ENERGY; TAURUS-AURIGA; DENSE CORES; DARK CLOUD AB Crucial steps in the formation of stars and planets can be studied only at mid- to far-infrared wavelengths, where the Space Infrared Telescope (SIRTF) provides an unprecedented improvement in sensitivity. We will use all three SIRTF instruments ( Infrared Array Camera [IRAC], Multiband Imaging Photometer for SIRTF [MIPS], and Infrared Spectrograph [IRS]) to observe sources that span the evolutionary sequence from molecular cores to protoplanetary disks, encompassing a wide range of cloud masses, stellar masses, and star-forming environments. In addition to targeting about 150 known compact cores, we will survey with IRAC and MIPS (3.6 - 70 mum) the entire areas of five of the nearest large molecular clouds for new candidate protostars and substellar objects as faint as 0.001 solar luminosities. We will also observe with IRAC and MIPS about 190 systems likely to be in the early stages of planetary system formation ( ages up to about 10 Myr), probing the evolution of the circumstellar dust, the raw material for planetary cores. Candidate planet-forming disks as small as 0.1 lunar masses will be detectable. Spectroscopy with IRS of new objects found in the surveys and of a select group of known objects will add vital information on the changing chemical and physical conditions in the disks and envelopes. The resulting data products will include catalogs of thousands of previously unknown sources, multiwavelength maps of about 20 deg(2) of molecular clouds, photometry of about 190 known young stars, spectra of at least 170 sources, ancillary data from ground-based telescopes, and new tools for analysis and modeling. These products will constitute the foundations for many follow-up studies with ground-based telescopes, as well as with SIRTF itself and other space missions such as SIM, JWST, Herschel, and TPF/ Darwin. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. Korea Astron Observ, Taeduk Radio Astron Observ, Taejon 305348, South Korea. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. SIRTF Sci Ctr, Pasadena, CA 91125 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Evans, NJ (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. RI Stapelfeldt, Karl/D-2721-2012 NR 58 TC 354 Z9 355 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 2003 VL 115 IS 810 BP 965 EP 980 DI 10.1086/376697 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 704DK UT WOS:000184322400004 ER PT J AU Maness, H Vrtilek, SD AF Maness, H Vrtilek, SD TI Nebular versus stellar wind abundances in NGC 6543 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ABSORPTION CROSS-SECTIONS; PLANETARY-NEBULAE AB An early analysis of Chandra observations of the planetary nebula NGC 6543 suggested that the location and the derived temperature for the X-ray-emitting region are inconsistent with the abundances measured for this object. We revisit Chandra observations of this source ( following significant updates to both the reprocessing and extraction software) in order to propose a resolution to this apparent anomaly. Our reanalysis using abundances found from observations in the infrared, optical, and ultraviolet suggests that the location and temperature of the X-ray emission from NGC 6543 is consistent with nebular abundances expected for the source. C1 Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Maness, H (reprint author), Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. NR 12 TC 5 Z9 5 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 2003 VL 115 IS 810 BP 1002 EP 1005 DI 10.1086/376573 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 704DK UT WOS:000184322400007 ER PT J AU Launius, RD AF Launius, RD TI Public opinion polls and perceptions of US human spaceflight SO SPACE POLICY LA English DT Article; Proceedings Paper CT World Space Congress CY OCT 10-19, 2002 CL HOUSTON, TEXAS SP Comm Space Res DE spaceflight; public opinion; human exploration of space; project Apollo ID SPACE AB A belief exists in the United States about public support for NASA's human spaceflight activities. Many hold that NASA and the cause of the human exploration of space enjoyed outstanding public support and confidence in the 1960s during the era of Apollo and that public support waned in the post-Apollo era, only to sink to quite low depths in the decade of the 1990s. These beliefs are predicated on anecdotal evidence that should not be discounted, but empirical evidence gleaned from public opinion polling data suggests that some of these conceptions are totally incorrect and others are either incomplete or more nuanced than previously believed. This article explores the evolution of public support for space exploration since the 1960s. Using polling data from a variety of sources it presents trends over time and offers comments on the meaning of public perceptions for the evolution of space policy and the development of space exploration in the United States. Published by Elsevier Ltd. C1 Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, POB 37012,NASM Room 3550,MRC 311, Washington, DC 20013 USA. OI Launius, Roger/0000-0003-1633-1253 NR 30 TC 19 Z9 19 U1 0 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 J9 SPACE POLICY JI Space Policy PD AUG PY 2003 VL 19 IS 3 BP 163 EP 175 DI 10.1016/S0265-9646(03)00039-0 PG 13 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 714AD UT WOS:000184889400002 ER PT J AU Fiore, AM Jacob, DJ Mathur, R Martin, RV AF Fiore, AM Jacob, DJ Mathur, R Martin, RV TI Application of empirical orthogonal functions to evaluate ozone simulations with regional and global models SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE empirical orthogonal functions; principal components; air pollution; ozone; regional modeling; global modeling ID EASTERN UNITED-STATES; SURFACE OZONE; NORTH-AMERICA; TRANSPORT; POLLUTION; SYSTEMS; PREDICTIONS/; PERFORMANCE; CHEMISTRY; MECHANISM AB Empirical orthogonal functions are used together with standard statistical metrics to evaluate the ability of models with different spatial resolutions to reproduce observed patterns of surface ozone (O-3) in the eastern United States in the summer of 1995. We examine simulations with the regional Multiscale Air Quality Simulation Platform model (horizontal resolution of 36 km(2)) and the global GEOS-CHEM model (2degrees x 2.5degrees and 4degrees x 5degrees). As the model resolution coarsens, the ability to resolve local O-3 maxima (O-3 greater than or equal to 90 ppbv) is compromised, but the spatial correlation improves. This result shows that synoptic-scale processes modulating O-3 concentrations are easier to capture in models than processes occurring on smaller scales. Empirical orthogonal functions (EOFs) derived from the observed O-3 fields reveal similar modes of variability when averaged onto the three model horizontal resolutions. The EOFs appear to represent (1) an east-west pattern associated with frontal passages, (2) a midwest-northeast pattern associated with migratory high-pressure systems, and (3) a southeast stagnation pattern linked to westward extension of the Bermuda High. All models capture the east-west and southeast EOFs, but the midwest-northeast EOF is misplaced in GEOS-CHEM. GEOS-CHEM captures the principal components of the observational EOFs when the model fields are projected onto these EOFs, implying that it can resolve the contribution of the EOFs to the observed variance. We conclude that coarse-resolution global models can successfully simulate the synoptic conditions leading to high-O-3 episodes in the eastern United States. C1 Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. MCNC, Environm Modeling Ctr, Res Triangle Pk, NC 27709 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fiore, AM (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 12 Oxford St, Cambridge, MA 02138 USA. EM afiore@post.harvard.edu RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; NR 39 TC 43 Z9 43 U1 0 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 31 PY 2003 VL 108 IS D19 AR 4431 DI 10.1029/2002JD003151 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 710WZ UT WOS:000184707000007 ER PT J AU Losos, JB Leal, M Glor, RE de Queiroz, K Hertz, PE Schettino, LR Lara, AC Jackman, TR Larson, A AF Losos, JB Leal, M Glor, RE de Queiroz, K Hertz, PE Schettino, LR Lara, AC Jackman, TR Larson, A TI Niche lability in the evolution of a Caribbean lizard community SO NATURE LA English DT Article ID ANOLIS LIZARDS; PHYLOGENETIC-RELATIONSHIPS; ECOLOGY; SYSTEMS; MODEL AB Niche conservatism-the tendency for closely related species to be ecologically similar - is widespread(1-3). However, most studies compare closely related taxa that occur in allopatry(3); in sympatry, the stabilizing forces that promote niche conservatism(4,5), and thus inhibit niche shifts, may be countered by natural selection favouring ecological divergence to minimize the intensity of interspecific interactions(6,7). Consequently, the relative importance of niche conservatism versus niche divergence in determining community structure has received little attention(7). Here, we examine a tropical lizard community in which species have a long evolutionary history of ecological interaction. We find that evolutionary divergence overcomes niche conservatism: closely related species are no more ecologically similar than expected by random divergence and some distantly related species are ecologically similar, leading to a community in which the relationship between ecological similarity and phylogenetic relatedness is very weak. Despite this lack of niche conservatism, the ecological structuring of the community has a phylogenetic component: niche complementarity only occurs among distantly related species, which suggests that the strength of ecological interactions among species may be related to phylogeny, but it is not necessarily the most closely related species that interact most strongly. C1 Washington Univ, Dept Biol, St Louis, MO 63130 USA. Union Coll, Dept Biol Sci, Schenectady, NY 12308 USA. Smithsonian Inst, Natl Museum Amer Hist, Div Amphibians & Reptiles, Washington, DC 20560 USA. Columbia Univ Barnard Coll, Dept Biol, New York, NY 10027 USA. CITGMA, Inst Ecol & Sistemat, Havana 10800, Cuba. Villanova Univ, Dept Biol, Villanova, PA 19085 USA. RP Losos, JB (reprint author), Washington Univ, Dept Biol, Campus Box 1137, St Louis, MO 63130 USA. RI Leal, Manuel/A-7220-2010; Glor, Richard/N-4656-2013; OI Glor, Richard/0000-0002-3359-1631; Jackman, Todd/0000-0002-5391-8136 NR 30 TC 181 Z9 188 U1 2 U2 73 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 31 PY 2003 VL 424 IS 6948 BP 542 EP 545 DI 10.1038/nature01814 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 706LG UT WOS:000184454700040 PM 12891355 ER PT J AU Olshanii, M Dunjko, V AF Olshanii, M Dunjko, V TI The short-distance first-order correlation function of the interacting one-dimensional Bose gas SO NEW JOURNAL OF PHYSICS LA English DT Article ID IMPENETRABLE BOSONS; QUANTUM FLUIDS; DENSITY-MATRIX; GROUND STATE; TEMPERATURE; CONFINEMENT; MODELS; TIME AB We derive exact closed-form expressions for the first few terms of the short-distance Taylor expansion of the one-body correlation function of the Lieb-Liniger gas. C1 Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Olshanii, M (reprint author), Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. RI Olshanii, Maxim/M-2830-2013 OI Olshanii, Maxim/0000-0003-3629-6002 NR 19 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD JUL 28 PY 2003 VL 5 AR 98 DI 10.1088/1367-2630/5/1/398 PG 5 WC Physics, Multidisciplinary SC Physics GA 706RG UT WOS:000184466900002 ER PT J AU Chatterjee, P Hernquist, L Loeb, A AF Chatterjee, P Hernquist, L Loeb, A TI Effects of wandering on the coalescence of black hole binaries in galactic centers SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : kinematics and dynamics; galaxies : nuclei; methods : n-body simulations; stellar dynamics ID EARLY-TYPE GALAXIES; DYNAMICAL EVOLUTION; ELLIPTIC GALAXIES; MASSIVE BINARY; HST; SYSTEM; MOTION; NUCLEI AB We examine whether massive binary black holes in spherically symmetric bulges of galaxies can achieve coalescence through the emission of gravitational radiation under the action of stellar dynamical processes alone. In particular, we address the importance of the Brownian motion of a binary's center of mass to its continued interaction with stellar orbits that allows it to keep hardening. We use an analytical model and N-body simulations to calculate the time required to reach the gravitational radiation-dominated stage. We find that a substantial fraction of all massive binaries in galaxies can coalesce within a Hubble time. 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 31 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2003 VL 592 IS 1 BP 32 EP 41 DI 10.1086/375552 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700EA UT WOS:000184098600004 ER PT J AU Kraft, RP Vazquez, SE Forman, WR Jones, C Murray, SS Hardcastle, MJ Worrall, DM Churazov, E AF Kraft, RP Vazquez, SE Forman, WR Jones, C Murray, SS Hardcastle, MJ Worrall, DM Churazov, E TI X-ray emission from the hot interstellar medium and southwest radio lobe of the nearby radio galaxy Centaurus A SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : active; galaxies : individual (Centaurus A, NGC 5128); galaxies : ISM; galaxies : jets; radio continuum : galaxies; X-rays : galaxies ID MAGNETIC-FIELD STRENGTHS; ACTIVE GALACTIC NUCLEI; COOLING FLOWS; CHANDRA OBSERVATIONS; ELLIPTIC GALAXY; EMITTING GAS; HYDRA-A; INTRACLUSTER MEDIUM; HIGH-RESOLUTION; INTERGALACTIC MEDIUM AB We present results from two Chandra/ACIS-I observations and one XMM-Newton observation of X-ray emission from the interstellar medium (ISM) and the inner radio lobes of the nearby radio galaxy Centaurus A. The ISM has an average radial surface brightness pro. le that is well described by a beta-model pro. le with index beta = 0.40 +/- 0.04 and a temperature of k(B)T(ISM) similar to 0.29 keV beyond 2 kpc from the nucleus. We. nd that diffuse X-ray emission is coincident with the outer half of the southwest radio lobe, and a bright X-ray enhancement is detected along the edge of the lobe. On the basis of energetic and lifetime arguments, we reject a nonthermal explanation for this emission. We model this emission as a thin, hot shell or cap of X-ray emitting plasma surrounding the radio lobe that was created by the supersonic inflation of the lobe. This plasma shell is both hotter than (k(B)T(SH) similar to 2.9 keV) and greatly overpressurized relative to the ambient ISM, indicating supersonic expansion. We estimate that the lobe is expanding into the ISM at approximately Mach 8.5, or 2400 km s(-1). We are not directly observing the bow shock, but rather the cooler, denser material that is accumulating ahead of the contact discontinuity. The thermal energy in the shell is a significant fraction of the thermal energy of the hot ISM, demonstrating the possibility that the hot ISM of early galaxies can be reenergized by outflows from nuclear activity. Interestingly, no similarly bright X-ray emission is detected in or along the edge of the northeast lobe, implying that there are differences in the dynamics and evolution of the kiloparsec-scale radio components. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Moscow Space Res Inst, Moscow 117810, Russia. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-31, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012; Churazov, Eugene/A-7783-2013 OI Hardcastle, Martin/0000-0003-4223-1117; NR 112 TC 118 Z9 118 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2003 VL 592 IS 1 BP 129 EP 146 DI 10.1086/375533 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700EA UT WOS:000184098600010 ER PT J AU Muzerolle, J Hillenbrand, L Calvet, N Briceno, C Hartmann, L AF Muzerolle, J Hillenbrand, L Calvet, N Briceno, C Hartmann, L TI Accretion in young stellar/substellar objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars : emission-line, Be; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID T-TAURI STARS; LOW-MASS STARS; ORION-NEBULA-CLUSTER; EMISSION-LINE DIAGNOSTICS; MAIN-SEQUENCE EVOLUTION; AURIGA MOLECULAR CLOUD; X-RAY IONIZATION; DISK ACCRETION; BROWN DWARFS; MAGNETOSPHERIC ACCRETION AB We present a study of accretion in a sample of 45 young, low-mass objects in a variety of star-forming regions and young associations, about half of which are likely substellar. Based primarily on the presence of broad, asymmetric Halpha emission, we have identified 13 objects (similar to30% of our sample) that are strong candidates for ongoing accretion. At least three of these are substellar. We do not detect significant continuum veiling in most of the accretors with late spectral types (M5-M7). Accretion shock models show that lack of measurable veiling allows us to place an upper limit to the mass accretion rates of less than or similar to10(-10) M-circle dot yr(-1). Using magnetospheric accretion models with appropriate ( sub) stellar parameters, we can successfully explain the accretor Halpha emission-line profiles and derive quantitative estimates of accretion rates in the range 10(-12) M-circle dot yr(-1) < (M)over dot < 10(-9) M-circle dot yr(-1). There is a clear trend of decreasing accretion rate with stellar mass, with mean accretion rates declining by 3-4 orders of magnitude over similar to1-0.05 M-circle dot. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Invest Astron, Merida 5010A, Venezuela. RP Muzerolle, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 78 TC 258 Z9 259 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2003 VL 592 IS 1 BP 266 EP 281 DI 10.1086/375704 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700EA UT WOS:000184098600021 ER PT J AU Jayawardhana, R Mohanty, S Basri, G AF Jayawardhana, R Mohanty, S Basri, G TI Evidence for a T Tauri phase in young brown dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence; techniques : spectroscopic ID LOW-MASS STARS; EMISSION-LINE DIAGNOSTICS; MAGNETOSPHERIC ACCRETION; CIRCUMSTELLAR DISKS; FORMING REGION; ASSOCIATION; ROTATION; CLUSTER; MEMBERS; MODELS AB As part of a multifaceted program to investigate the origin and early evolution of substellar objects, we present high-resolution Keck optical spectra of 14 very low mass sources in the IC 348 young cluster and the Taurus star-forming cloud. All of our targets, which span a range of spectral types from M5 to M8, exhibit moderate to very strong Halpha emission. In half of the IC 348 objects, the Halpha profiles are broad and asymmetric, indicative of ongoing accretion. Of these, IC 348-355 ( M8) is the lowest mass object to date to show accretion-like Halpha. Three of our similar toM6IC 348 targets with broad Halpha also harbor broad O I (8446 Angstrom) and Ca II (8662 Angstrom) emission, and one shows broad He I (6678 Angstrom) emission; these features are usually seen in strongly accreting classical T Tauri stars. We find that in very low mass accretors, the Halpha profile may be somewhat narrower than that in higher mass stars. We propose that low accretion rates combined with small infall velocities at very low masses can conspire to produce this effect. In the nonaccretors in our sample, Halpha emission is commensurate with, or higher than, saturated levels in field M dwarfs of similar spectral type. Our results constitute the most compelling evidence to date that young brown dwarfs undergo a T Tauri-like accretion phase similar to that in stars. This is consistent with a common origin for most low-mass stars, brown dwarfs, and isolated planetary mass objects. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Jayawardhana, R (reprint author), Univ Michigan, Dept Astron, 830 Dennison, Ann Arbor, MI 48109 USA. NR 31 TC 126 Z9 126 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2003 VL 592 IS 1 BP 282 EP 287 DI 10.1086/375573 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700EA UT WOS:000184098600022 ER PT J AU Rho, JH Reynolds, SP Reach, WT Jarrett, TH Allen, GE AF Rho, JH Reynolds, SP Reach, WT Jarrett, TH Allen, GE TI Near-infrared synchrotron emission from Cassiopeia A SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; ISM : individual (Cassiopeia A); supernova remnants ID SHOCK-ACCELERATED ELECTRONS; KEPLER SUPERNOVA-REMNANTS; GAMMA-RAY EMISSION; NONTHERMAL X-RAYS; MAXIMUM ENERGIES; RICH EJECTA; SHELL; DISCOVERY; RADIO; DUST AB Recent high-energy observations of Cassiopeia A suggest the presence of synchrotron radiation, implying acceleration of cosmic rays by young supernova remnants. We detect synchrotron emission from Cas A in the near-infrared using Two Micron All-Sky Survey (2MASS) and Palomar 200 inch (5.1 m) PFIRCAM observations. The remnant is detected in the J, H, and K(s) bands using 2MASS: the K(s) band is the brightest, H is moderate, and J is faint. In the J and H bands, bright [Fe II] lines (1.24 and 1.64 mum) are detected spectroscopically. The Palomar observations include K(s)-continuum, narrowband 1.64 mum (centered on [Fe II]) and 2.12 mum [centered on H(2) (1-0)] images. While the narrowband 1.64 mum image shows filamentary and knotty structures, similar to the optical image, the K(s) image shows a relatively smooth, diffuse shell, remarkably similar to the radio image. The H(2) image is identical to the K(s)-continuum image, with surface brightness reduced as expected for the ratio of filter bandwidths, showing no contribution of H(2) lines to the K(s)-band image. The broadband near-infrared fluxes of Cas A are generally consistent with, but a few tens of percent higher than, an extrapolation of the radio fluxes. The hardening to higher frequencies is possibly due to nonlinear shock acceleration and/or spectral index variation across the remnant. We show evidence of spectral index variation across Cas A using the "spectral tomography" technique. The presence of near-infrared synchrotron radiation requires the rolloff frequency to be higher than 1.5 x 10(14) Hz, implying that electrons are accelerated to energies of at least E = 0.3B(mG)(-1/2) ergs, or 0.2 TeV. The morphological similarity in diffuse emission between the radio and K(s)-band images implies that synchrotron losses are not dominant, or we would expect to see a greater concentration in knots. We also show that dust continuum is not significant in the near-infrared emission of Cas A. Our observations show unambiguous evidence that the near-infrared K(s)-band emission of Cas A is from synchrotron emission by accelerated cosmic-ray electrons. C1 CALTECH, SIRTF Sci Ctr, IPAC, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Cornell Univ, Ithaca, NY 14853 USA. N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. RP Rho, JH (reprint author), CALTECH, SIRTF Sci Ctr, IPAC, MS 220-6, Pasadena, CA 91125 USA. EM rho@ipac.caltech.edu OI Reach, William/0000-0001-8362-4094 NR 52 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2003 VL 592 IS 1 BP 299 EP 310 DI 10.1086/375564 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700EA UT WOS:000184098600024 ER PT J AU Heyl, JS AF Heyl, JS TI The synoptic swift synergy - Catching gamma-ray bursts before they fly SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID OPTICAL AFTERGLOW; SUPERNOVA; GRB-021004 AB The advent of large panoramic photometric surveys of the sky offers the possibly of exploring the association of gamma-ray bursts (GRBs) with supernovae. To date, a few GRBs have been connected possibly with supernovae: GRB 980425-SN 1998bw, GRB 011121-SN 2001ke, GRB 970228, and GRB 980326. A combination of a large detection rate of GRBs and rapid coverage of a large portion of the sky to faint magnitude limits offers the possibility of detecting a supernova preceding an associated GRB or at least placing limits on the rate of association between these two phenomena and the time delay between them. This would provide important constraints on theoretical models for GRBs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heyl, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 3 Z9 3 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2003 VL 592 IS 1 BP 401 EP 403 DI 10.1086/375699 PN 1 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700EA UT WOS:000184098600033 ER PT J AU Boroson, B Vrtilek, SD Kallman, T Corcoran, M AF Boroson, B Vrtilek, SD Kallman, T Corcoran, M TI Chandra grating spectroscopy of the X-ray binary 4U 1700-37 in a flaring state SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; stars : individual (4U 1700-37); X-rays : binaries; X-rays : individual ( 4U 1700-37) ID QUASI-PERIODIC OSCILLATIONS; STELLAR WIND; VELA X-1; APERIODIC VARIABILITY; LMC X-4; 4U-1700-37; SPECTRUM; LINES; COMPTONIZATION; HERCULES-X-1 AB Chandra X-Ray Observatory grating spectra of the supergiant X-ray binary 4U 1700-37 reveal emission lines from hydrogen- and helium-like S, Si, Mg, and Ne in the 4 - 13 Angstrom range. The spectrum also shows fluorescent lines from S and Si and a prominent Fe Kalpha line at 1.94 Angstrom. The lines contribute to the previously unaccounted "soft excess'' in the flux in this range at orbital phi approximate to 0.7. The X-ray source was observed during intermittent flaring, and the strengths of the lines vary with the source state. The widths of the lines (FWHM approximate to 1000 2000 km s(-1)) can result from either Compton scattering or Doppler shifts. Power spectra of the hard X- rays show red noise, and the soft X- rays and lines show in addition quasi-periodic oscillations and a power spectral break. Helium-like triplets of Si and Mg suggest that the gas is not in a pure photoionization equilibrium. We discuss whether resonant scattering could affect the line ratios or whether a portion of the wind may be heated to temperatures T similar to 10(6) K. C1 MIT, Space Res Ctr, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Boroson, B (reprint author), MIT, Space Res Ctr, Cambridge, MA 02138 USA. NR 61 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 JUL 20 PY 2003 VL 592 IS 1 BP 516 EP 531 DI 10.1086/375636 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700EA UT WOS:000184098600042 ER PT J AU Park, S Hughes, JP Slane, PO Burrows, DN Warren, JS Garmire, GP Nousek, JA AF Park, S Hughes, JP Slane, PO Burrows, DN Warren, JS Garmire, GP Nousek, JA TI Detection of magnesium-rich ejecta in the middle-aged supernova remnant N49B SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (N49B); supernova remnants; X-rays : ISM ID LARGE-MAGELLANIC-CLOUD; CCD IMAGING SPECTROMETER; CHARGE-TRANSFER INEFFICIENCY; X-RAY-EMISSION; ABUNDANCES; SPECTROSCOPY; ELEMENTS AB The middle-aged supernova remnant (SNR) N49B in the Large Magellanic Cloud has been observed with the Chandra X-Ray Observatory. The superb angular resolution of Chandra resolves the complex structure of X-ray-emitting filaments across the SNR. All observed features are soft (E < 3 keV), and we find no evidence of either pointlike or extended hard emission within the SNR. Spectral lines from O, Ne, Mg, Si, S, and Fe are present. Equivalent width images for the detected elemental species and spatially resolved spectral analysis reveal the presence of Mg-rich ejecta within the SNR. We find no such enrichment in O or Ne, which may reflect details of the nucleosynthesis process or the heating and cooling of the ejecta as it evolved. The bright circumferential filaments are emission from the shocked dense interstellar medium (ISM). We detect faint diffuse X-ray emission that extends beyond the X-ray-bright filaments toward the west and southeast. These features appear to be the blast wave shock front expanding into lower density portions of the ISM seen in projection. We set an upper limit of &SIM;2 x 10(33) ergs s(-1) on the 0.5-5 keV band X-ray luminosity of any embedded compact object. 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 22 TC 26 Z9 26 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2003 VL 592 IS 1 BP L41 EP L44 DI 10.1086/377507 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700ED UT WOS:000184098900011 ER PT J AU Li, LX AF Li, LX TI Disk accretion flow driven by large-scale magnetic fields: Solutions with constant specific energy SO PHYSICAL REVIEW D LA English DT Article ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; BLACK-HOLE MAGNETOSPHERE; ACTIVE GALACTIC NUCLEI; DOMINATED ACCRETION; ANGULAR-MOMENTUM; DYNAMO ACTION; MHD; INSTABILITY; EXTRACTION; CONVECTION AB We study the dynamical evolution of a stationary, axisymmetric, and perfectly conducting cold accretion disk containing a large-scale magnetic field around a Kerr black hole, trying to understand the relation between accretion and the transportation of angular momentum and energy. A one-dimensional radial momentum equation is derived near the equatorial plane, which has one intrinsic singularity at the fast critical point. We solve the radial momentum equation for solutions corresponding to an accretion flow that starts from a subsonic state at infinity, smoothly passes the fast critical point, then supersonically falls into the horizon of the black hole. The solutions always have the following features: (1) The specific energy of fluid particles remains constant but the specific angular momentum is effectively removed by the magnetic field. (2) At large radii, where the disk motion is dominantly rotational, the energy density of the magnetic field is equipartitioned with the rotational energy density of the disk. (3) Inside the fast critical point, where radial motion becomes important, the ratio of the electromagnetic energy density to the kinetic energy density drops quickly. The results indicate that: (1) disk accretion does not necessarily imply energy dissipation since magnetic fields do not have to transport or dissipate a lot of energy as they effectively transport angular momentum and (2) when resistivity is small, the large-scale magnetic field is amplified by the shearing rotation of the disk until the magnetic energy density is equipartitioned with the rotational energy density, ending up with a geometrically thick disk. This is in contrast to the evolution of small-scale magnetic fields where if the resistivity is nonzero the magnetic energy density is likely to be equipartitioned with the kinetic energy density associated with local random motions (e.g., turbulence), making a thin Keplerian disk possible. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 54 TC 3 Z9 3 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUL 15 PY 2003 VL 68 IS 2 AR 024022 DI 10.1103/PhysRevD.68.024022 PG 23 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 719XA UT WOS:000185229300055 ER PT J AU Ozanne, CMP Anhuf, D Boulter, SL Keller, M Kitching, RL Korner, C Meinzer, FC Mitchell, AW Nakashizuka, T Dias, PLS Stork, NE Wright, SJ Yoshimura, M AF Ozanne, CMP Anhuf, D Boulter, SL Keller, M Kitching, RL Korner, C Meinzer, FC Mitchell, AW Nakashizuka, T Dias, PLS Stork, NE Wright, SJ Yoshimura, M TI Biodiversity meets the atmosphere: A global view of forest canopies SO SCIENCE LA English DT Review ID TROPICAL FOREST; ELEVATED CO2; HERBIVOROUS INSECTS; TREES; PLANTS; DIVERSITY; RESPONSES; PATTERNS; ECOLOGY; GROWTH AB The forest canopy is the functional interface between 90% of Earth's terrestrial biomass and the atmosphere. Multidisciplinary research in the canopy has expanded concepts of global species richness, physiological processes, and the provision of ecosystem services. Trees respond in a species-specific manner to elevated carbon dioxide levels, while climate change threatens plant-animal interactions in the canopy and will likely alter the production of biogenic aerosols that affect cloud formation and atmospheric chemistry. C1 Univ Surrey Roehampton, Sch Life & Sport Sci, Ctr Res Ecol & Environm, London SW15 3SN, England. Univ Sao Paulo, Inst Estudos Avancados, BR-05508900 Sao Paulo, Brazil. Griffith Univ, Environm Sci & Rainforest Cooperat Res Ctr, Nathan, Qld 4111, Australia. US Forest Serv, Int Inst Trop Forestry, USDA, San Juan, PR 00926 USA. Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. US Forest Serv, USDA, Pacific NW Res Stn, Corvallis, OR 97331 USA. Univ Oxford, Global Canopy Programme, Oxford OX1 3UB, England. Res Inst Human & Nat, Kamigyo Ku, Kyoto 6020878, Japan. Japan Sci & Technol Corp, Core Res Evolut Sci & Technol, Osaka, Japan. Univ Sao Paulo, Inst Astron & Geofis, BR-05508900 Sao Paulo, Brazil. James Cook Univ N Queensland, Rainforest Cooperat Res Ctr, Cairns, Qld 4870, Australia. Smithsonian Trop Res Inst, Balboa, Panama. RP Ozanne, CMP (reprint author), Univ Surrey Roehampton, Sch Life & Sport Sci, Ctr Res Ecol & Environm, West Hill, London SW15 3SN, England. RI Kitching, Roger/C-5102-2009; Keller, Michael/A-8976-2012; Korner, Christian/B-6592-2014; Meinzer, Frederick/C-3496-2012; Wright, Stuart/M-3311-2013; Leite da Silva Dias, Pedro/H-1183-2016 OI Keller, Michael/0000-0002-0253-3359; Wright, Stuart/0000-0003-4260-5676; Leite da Silva Dias, Pedro/0000-0002-4051-2962 NR 71 TC 139 Z9 165 U1 7 U2 88 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 11 PY 2003 VL 301 IS 5630 BP 183 EP 186 DI 10.1126/science.1084507 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 699KN UT WOS:000184056200032 PM 12855799 ER PT J AU Fabbiano, G King, AR Zezas, A Ponman, TJ Rots, A Schweizer, F AF Fabbiano, G King, AR Zezas, A Ponman, TJ Rots, A Schweizer, F TI A variable ultraluminous supersoft X-ray source in ''the antennae'': Stellar-mass black hole or white dwarf? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038/4039); galaxies : interactions; galaxies : peculiar; X-rays : binaries; X-rays : galaxies ID CHANDRA OBSERVATIONS; GALAXIES NGC-4038/4039; DISCOVERY; BINARIES; M101; M81 AB The Chandra monitoring observations of "The Antennae'' (NGC 4038/4039) have led to the discovery of a variable, luminous, supersoft source (SSS). This source is detected only at energies below 2 keV and, in 2002 May, reached count rates comparable to those of the nine ultraluminous X-ray sources (ULXs) detected in these galaxies. Spectral fits of the SSS data give acceptable results only for a similar to90 - 100 eV blackbody spectrum with an intrinsic absorption column of N-H similar to (2-3) x 10(21) cm(-2). For a distance of 19 Mpc, the best-fit observed luminosity increases from 1.7 x 10(38) ergs s(-1) in 1999 December to 8.0 x 10(38) ergs s(-1) in 2002 May. The intrinsic, absorption-corrected, best-fit luminosity reaches 1.4 x 10(40) ergs s(-1) in 2002 May. The assumption of unbeamed emission would suggest a black hole of greater than or similar to 100M(.). However, if the emission is blackbody at all times, as suggested by the steep soft spectrum, the radiating area would have to vary by a factor of similar to10(3), inconsistent with gravitational energy release from within a few Schwarzschild radii of a black hole. Viable explanations for the observed properties of the SSS are provided by anisotropic emission from either an accreting nuclear-burning white dwarf or an accreting stellar-mass black hole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Rots, Arnold/0000-0003-2377-2356 NR 25 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 JUL 10 PY 2003 VL 591 IS 2 BP 843 EP 849 DI 10.1086/375441 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698UF UT WOS:000184016700024 ER PT J AU Bensch, F Leuenhagen, U Stutzki, J Schieder, R AF Bensch, F Leuenhagen, U Stutzki, J Schieder, R TI [C I] 492 GHz mapping observations of the high-latitude translucent cloud MCLD 123.5+24.9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : abundances; ISM : clouds; ISM : individual (MCLD 123.5+24.9); radio lines : ISM ID A MOLECULAR CLOUD; ATOMIC CARBON; PHOTODISSOCIATION REGIONS; INTERSTELLAR CLOUDS; ORION-A; NEUTRAL CARBON; CIRRUS CLOUD; DARK CLOUD; EMISSION; SUBMILLIMETER AB We present the first map of the [C I] P-3(1) --> P-3(0) fine-structure transition of neutral carbon made toward a translucent molecular cloud (MCLD 123.5+ 24.9, located in the Polaris Flare). The [C I] observations were made with the Submillimeter Wave Astronomy Satellite and are supplemented by ground-based observations of (CO)-C-12 and (CO)-C-13 rotational transitions. We find that the [C I] emission is spatially extended following the region bright in (CO)-C-12. The [C I] to CO line ratios observed throughout the MCLD 123.5+ 24.9 cloud are relatively low, and the [C I] line flux density is only similar to50% of the emission by the three lowest CO rotational transitions. However, the ratios are still within the range observed along selected lines of sight toward other diffuse and translucent molecular clouds. Assuming LTE conditions for the neutral atomic carbon with an excitation temperature of 8 K derived from the (CO)-C-12 spectra, we derive a total carbon column density of (0.25-1) x 10(17) cm(-2) and a C to CO column density ratio between 0.2 and 1.1. Comparison with a photon-dominated region model shows that the model consistently would require uncomfortably high values for the gas volume density in order to reproduce the low [C I] to CO line ratios observed (n > 10(5) cm(-3)), unless we assume that the line-emitting clumps are embedded in an interclump medium with a density of n < 10(3) cm(-3). The low-density interclump medium does not significantly contribute to the observed [C I] and CO line emission, but the molecular hydrogen in the gas provides an effective shielding for the CO in the embedded clumps by blocking the FUV photons at the frequencies of CO line transition to the predissociation states. This reduces the photodissociation of CO and, thus, the abundance of neutral and ionized carbon in the denser clumps. C1 Univ Cologne, Inst Phys, D-50937 Cologne, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. LB Kiel, D-24103 Kiel, Germany. RP Bensch, F (reprint author), Univ Cologne, Inst Phys, Zulpicher Str 77, D-50937 Cologne, Germany. NR 48 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 JUL 10 PY 2003 VL 591 IS 2 BP 1013 EP 1024 DI 10.1086/375393 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698UF UT WOS:000184016700036 ER PT J AU Bergin, E Calvet, N D'Alessio, P Herczeg, GJ AF Bergin, E Calvet, N D'Alessio, P Herczeg, GJ TI The effects of UV continuum and Ly alpha radiation on the chemical equilibrium of T Tauri disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; astrobiology; astrochemistry; circumstellar matter; stars : pre-main-sequence; ultraviolet : stars ID AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE STARS; PROTOPLANETARY DISKS; ACCRETION DISKS; 2-DIMENSIONAL DISTRIBUTIONS; OSCILLATOR-STRENGTHS; GASEOUS MOLECULES; COLUMN DENSITIES; YOUNG OBJECTS; X-RAY AB We show in this Letter that the spectral details of the far-ultraviolet (FUV) radiation fields have a large impact on the chemistry of protoplanetary disks surrounding T Tauri stars. We show that the strength of a realistic stellar FUV field is significantly lower than typically assumed in chemical calculations and that the radiation field is dominated by strong line emission, most notably Lyalpha radiation. The effects of the strong Lyalpha emission on the chemical equilibrium in protoplanetary disks have previously been unrecognized. We discuss the impact of this radiation on molecular observations in the context of a radiative transfer model that includes both direct attenuation and scattering. In particular, Lya radiation will directly dissociate water vapor and may contribute to the observed enhancements of CN/HCN in disks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. Univ Colorado, Joint Inst Lab Astrophys, UCB 440, Boulder, CO 80309 USA. RP Bergin, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 42 TC 90 Z9 90 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2003 VL 591 IS 2 BP L159 EP L162 DI 10.1086/377148 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698UJ UT WOS:000184017100022 ER PT J AU Bonanos, AZ Stanek, KZ AF Bonanos, AZ Stanek, KZ TI Reanalysis of Very Large Telescope data for M83 with image subtraction - Ninefold increase in number of cepheids SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; distance scale; galaxies : individual (M83) ID DETACHED ECLIPSING BINARIES; DIRECT DISTANCES; ADDITIONAL VARIABLES; M31 AB We apply the image-subtraction method in order to reanalyze the ESO Very Large Telescope data on M83 (NGC 5236), obtained and analyzed by Thim et al. Whereas Thim et al. found 12 Cepheids with periods between 12 and 55 days, we find 112 Cepheids with periods ranging from 7 to 91 days as well as similar to60 other variables. These include two candidate eclipsing binaries, which, if confirmed, would be the first optically discovered outside the Local Group. We thus demonstrate that the image-subtraction method is much more powerful for detecting variability, especially in crowded fields. However, Hubble Space Telescope observations are necessary to obtain a Cepheid period-luminosity distance not dominated by blending and crowding. We propose a "hybrid" approach, in which numerous Cepheids are discovered and characterized using large ground-based telescopes and then followed up with the Hubble Space Telescope to obtain precise distances. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bonanos, AZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Bonanos, Alceste/K-5392-2013 OI Bonanos, Alceste/0000-0003-2851-1905 NR 14 TC 9 Z9 9 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 JUL 10 PY 2003 VL 591 IS 2 BP L111 EP L114 DI 10.1086/377073 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698UJ UT WOS:000184017100010 ER PT J AU Hughes, JP Slane, PO Park, S Roming, PWA Burrows, DN AF Hughes, JP Slane, PO Park, S Roming, PWA Burrows, DN TI An X-ray pulsar in the oxygen-rich supernova remnant G292.0+1.8 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G292.0+1.8, MSH 11-54); pulsars : individual (PSR J1124-5916) stars : neutron; supernova remnants; X-rays : individual (CXOU J112439.1-591620) ID CASSIOPEIA-A; WIND AB We report the discovery of pulsed X-ray emission from the compact object CXOU J112439.1-591620 within the supernova remnant G292.0+1.8 using the High Resolution Camera on the Chandra X-Ray Observatory. The X-ray period (P = 0.13530915 s) is consistent with the extrapolation of the radio pulse period of PSR J1124-5916 for a spin-down rate of (P) over dot = 7.6 x 10(-13) s s(-1). The X-ray pulse is single-peaked and broad, with an FWHM width of 0.23P (83degrees). The pulse-averaged X-ray spectral properties of the pulsar are well described by a featureless power-law model with an absorbing column density N(H) = 3.1 x 10(21) cm(-2), a photon index Gamma = 1.6, and an unabsorbed 0.3-10 keV band luminosity L(x) = 7.2 x 10(32) ergs s(-1). We plausibly identify the location of the pulsar's termination shock. Pressure balance between the pulsar wind nebula and the larger synchrotron nebula, as well as lifetime issues for the X-ray-emitting electrons, argue for a particle-dominated pulsar wind nebula that is far from the minimum-energy condition. Upper limits on the surface temperature of the neutron star are at, or slightly below, values expected from "standard" cooling curves. There is no optical counterpart to the new pulsar; its optical luminosity is at least a factor of 5 below that of the Crab pulsar. C1 Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RP Hughes, JP (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. EM jph@physics.rutgers.edu; slane@head-cfa.harvard.edu NR 19 TC 42 Z9 43 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2003 VL 591 IS 2 BP L139 EP L142 DI 10.1086/377072 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698UJ UT WOS:000184017100017 ER PT J AU Pooley, D Lewin, WHG Anderson, SF Baumgardt, H Filippenko, AV Gaensler, BM Homer, L Hut, P Kaspi, VM Makino, J Margon, B McMillan, S Portegies Zwart, S van der Klis, M Verbunt, F AF Pooley, D Lewin, WHG Anderson, SF Baumgardt, H Filippenko, AV Gaensler, BM Homer, L Hut, P Kaspi, VM Makino, J Margon, B McMillan, S Portegies Zwart, S van der Klis, M Verbunt, F TI Dynamical formation of close binary systems in globular clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; globular clusters : general; X-rays : binaries ID X-RAY SOURCES; NEUTRON-STAR; LUMINOSITY FUNCTIONS; STELLAR DYNAMICS; EVOLUTION; DISCOVERY; CATALOG; CORE; M15 AB We know from observations that globular clusters are very efficient catalysts in forming unusual short-period binary systems or their offspring, such as low-mass X-ray binaries (LMXBs; neutron stars accreting matter from low-mass stellar companions), cataclysmic variables ( white dwarfs accreting matter from stellar companions), and millisecond pulsars ( rotating neutron stars with spin periods of a few milliseconds). Although there has been little direct evidence, the overabundance of these objects in globular clusters has been attributed by numerous authors to the high densities in the cores, which leads to an increase in the formation rate of exotic binary systems through close stellar encounters. Many such close binary systems emit X-radiation at low luminosities (L-x less than or similar to 10(34) ergs s(-1)) and are being found in large numbers through observations with the Chandra X-Ray Observatory. Here we present conclusive observational evidence of a link between the number of close binaries observed in X-rays in a globular cluster and the stellar encounter rate of the cluster. We also make an estimate of the total number of LMXBs in globular clusters in our Galaxy. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Adv Study, Princeton, NJ 08540 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. RP Pooley, D (reprint author), MIT, Ctr Space Res, 70 Vassar St, Cambridge, MA 02139 USA. EM dave@mit.edu; lewin@space.mit.edu; anderson@astro.washington.edu; holger@astron.s.u-tokyo.ac.jp; alex@astron.berkeley.edu; bgaensler@cfa.harvard.edu; homer@astro.washington.edu; piet@ias.edu; vkaspi@hep.physics.mcgill.ca; makino@astron.s.u-tokyo.ac.jp; margon@stsci.edu; steve@kepler.physics.drexel.edu; spz@science.uva.nl; michiel@astro.uva.nl; f.w.m.verbunt@astro.uu.nl RI Gaensler, Bryan/F-8655-2010; Baumgardt, Holger/A-5444-2012; Margon, Bruce/B-5913-2012; Makino, Junichiro/A-9525-2014; OI Gaensler, Bryan/0000-0002-3382-9558 NR 37 TC 134 Z9 134 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2003 VL 591 IS 2 BP L131 EP L134 DI 10.1086/377074 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698UJ UT WOS:000184017100015 ER PT J AU Van Bael, SA Brawn, JD Robinson, SK AF Van Bael, SA Brawn, JD Robinson, SK TI Birds defend trees from herbivores in a Neotropical forest canopy SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID TROPHIC CASCADES; FOOD-WEB; IMPACT; DAMAGE; INSECTS; TOP AB Most forest birds include arthropods in their diet, sometimes specializing on arthropods that consume plant foliage. Experimental tests of whether bird predation on arthropods can reduce plant damage, however, are few and restricted to relatively low-diversity systems. Here, we describe an experimental test in a diverse tropical forest of whether birds indirectly defend foliage from arthropod herbivores. We also compare how the indirect effects of bird predation vary with different levels of foliage productivity in the canopy vs. the understory. For three Neotropical tree species, we observed that birds decreased local arthropod densities on canopy branches and reduced consequent damage to leaves. In contrast, we observed no evidence of bird-arthropod limitation on conspecific saplings in the less productive understory of the same forest. Our results support theory that predicts trophic cascades where productivity is high and suggest that birds play an important role in Neotropical communities by means of their indirect defense of some canopy tree species. C1 Univ Illinois, Dept Anim Biol, Champaign, IL 61820 USA. Univ Illinois, Dept Nat Resources & Environm Sci, Champaign, IL 61820 USA. RP Van Bael, SA (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. NR 32 TC 107 Z9 111 U1 1 U2 24 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 JUL 8 PY 2003 VL 100 IS 14 BP 8304 EP 8307 DI 10.1073/pnas.1431621100 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 702KF UT WOS:000184222500049 PM 12832618 ER PT J AU Simkin, T Fiske, RS AF Simkin, T Fiske, RS TI Krakatoa - The day the world exploded: August 27, 1883 SO SCIENCE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Simkin, T (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 6 TC 0 Z9 1 U1 3 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 4 PY 2003 VL 301 IS 5629 BP 50 EP 51 DI 10.1126/science.1086522 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 696YG UT WOS:000183914700022 ER PT J AU Ewe, SML Sternberg, LD AF Ewe, SML Sternberg, LD TI Seasonal gas exchange characteristics of Schinus terebinthifolius in a native and disturbed upland community in Everglades National Park, Florida SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE invasive exotic; everglades; photosynthesis ID NITROGEN-USE EFFICIENCY; WATER-USE EFFICIENCY; CARBON ISOTOPE DISCRIMINATION; PHOTOSYNTHETIC CAPACITY; GROWTH; HAWAII; ALLOCATION; INCREASE; PATTERNS; DECLINE AB Schinus terebinthifolius Raddi (Schinus) is an invasive exotic plant widely found in Florida and Hawaii. This species is found from the upland pinelands to the mangrove forests of Florida. Dense Schinus infestations have the capacity to displace native species, reduce species diversity and been shown to reduce faunal use of the community. The purpose of this study was to determine if gas exchange patterns of Schinus were significantly different from native species. This work was part of a larger study to determine if the exotic's physiology contributed to its presence in two upland communities of South Florida. The first was an endemic rock pineland community and the second, a disturbed previously farmed area where Schinus was the canopy dominant. Schinus gas exchange, leaf nitrogen and carbon stable isotope contents were contrasted with four native species for one wet and dry season. Schinus tended to have higher assimilation (A), mesophyll conductance (g(m)), intrinsic water-use efficiency (WUE) and photosynthetic nitrogen-use efficiency (PNUE) than native species in the pineland site during the wet season but these differences were not statistically significant. There were also no significant differences in conspecific plant responses between the two communities. Seasonal differences were, however, significant for most of the gas exchange parameters at either one or both of the study sites. Wet season A, g(m), nitrogen concentration ([N]), intrinsic WUE, PNUE and carbon stable isotope signatures (delta(13)C) were higher than the dry season, most likely a consequence of greater water availability within the substrate. Although differences in gas exchange could contribute to the invasiveness of Schinus into native pineland and disturbed upland areas, other aspects of its autoecology also play an important role. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. Smithsonian Marine Stn, Ft Pierce, FL USA. RP Ewe, SML (reprint author), Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. NR 45 TC 27 Z9 33 U1 2 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD JUL 3 PY 2003 VL 179 IS 1-3 BP 27 EP 36 AR PII S0378-1127(02)00531-5 DI 10.1016/S0378-1127(02)00531-5 PG 10 WC Forestry SC Forestry GA 695ND UT WOS:000183836300003 ER PT J AU Ott, JD Oran, ES Anderson, JD AF Ott, JD Oran, ES Anderson, JD TI A mechanism for flame acceleration in narrow tubes SO AIAA JOURNAL LA English DT Article ID TO-DETONATION TRANSITION; NUMERICAL-SIMULATION; BOUNDARY-CONDITIONS; SHOCK; PROPAGATION C1 Combust Res & Flow Technol, Dublin, PA 18917 USA. USN, Res Lab, Computat Phys & Fluid Dynam Lab, Washington, DC 20375 USA. Smithsonian Inst, Natl Air & Space Museum, Aeronaut Div, Washington, DC 20560 USA. RP Ott, JD (reprint author), Combust Res & Flow Technol, 174 N Main St,Bldg 3,POB 1150, Dublin, PA 18917 USA. NR 22 TC 36 Z9 40 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD JUL PY 2003 VL 41 IS 7 BP 1391 EP 1396 DI 10.2514/2.2088 PG 6 WC Engineering, Aerospace SC Engineering GA 698GR UT WOS:000183990800022 ER PT J AU Lellinger, DB AF Lellinger, DB TI Nomenclatural and taxonomic notes on the pteridophytes of Costa Rica, Panama, and Colombia, III SO AMERICAN FERN JOURNAL LA English DT Article AB The new species Hypolepis rubginopilosula and Polypodium chirripoense are described, the new combinations Blechnum loxense var. stenophyllum, B. l'herminieri subsp. lehmannii, Diplazium ribae, Lastreopsis squamifera, Lomariopsis salicifolia, Pteridium caudatum subsp. arachnoideum, and Tectaria xmicheleriana are made, and three lectotypes are chosen for tropical American ferns. C1 Natl Museum Nat Hist, Smithsonian Inst, Bot Sect, Washington, DC 20560 USA. RP Lellinger, DB (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Bot Sect, Washington, DC 20560 USA. NR 5 TC 5 Z9 8 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 JUL-SEP PY 2003 VL 93 IS 3 BP 146 EP 151 DI 10.1640/0002-8444(2003)093[0146:NATNOT]2.0.CO;2 PG 6 WC Plant Sciences SC Plant Sciences GA 726CK UT WOS:000185580400005 ER PT J AU Herken, G AF Herken, G TI Comment on book review of "brotherhood of the bomb: The tangled lives and loyalties of Robert Oppenheimer, Ernest Lawrence, and Edward Teller," by Gregg Herken [Am. J. Phys. 71(4),411-415 (2003)] SO AMERICAN JOURNAL OF PHYSICS LA English DT Letter C1 Smithsonian Inst, Washington, DC 20560 USA. RP Herken, G (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC PHYSICS TEACHERS AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0002-9505 J9 AM J PHYS JI Am. J. Phys. PD JUL PY 2003 VL 71 IS 7 BP 647 EP 648 DI 10.1119/1.1579499 PG 2 WC Education, Scientific Disciplines; Physics, Multidisciplinary SC Education & Educational Research; Physics GA 692KR UT WOS:000183660700001 ER PT J AU Christy, JH Baum, JK Backwell, PRY AF Christy, JH Baum, JK Backwell, PRY TI Attractiveness of sand hoods built by courting male fiddler crabs, Uca musica: test of a sensory trap hypothesis SO ANIMAL BEHAVIOUR LA English DT Article ID SEXUAL SELECTION; CHOICE AB Courting male fiddler crabs, Uca musica, sometimes build sand hoods at the entrances of their burrows to which they attract females for mating. On average, females visit 17 males in as many minutes before they choose a mate, and they preferentially visit males with hoods. When moving between burrows, fiddler crabs of both sexes sometimes approach and temporarily hide against objects on the surface. Hence, mate-searching females may approach hoods because they resemble (mimic) other objects that crabs approach to reduce their predation risk. We conducted two experiments to test this sensory trap hypothesis. First, we determined whether sexually receptive and nonreceptive female U. musica and nonreceptive female U. stenodactylus, a species that does not build structures, spontaneously approach hoods (replicas), stones, pieces of wood and shells. As predicted by the sensory trap hypothesis, both species, irrespective of sexual receptivity, approached these objects and neither preferred hoods. Second, to determine whether female U. musica show a preference for hoods when they search for a mate, we recorded the frequency with which females approached males with natural hoods, hood replicas, wood, stones and shells. Again as expected, females approached males with these different structures at the same rates. We conclude that hoods are effective mimics of objects that females approach for safety whether they are searching for a mate or not. Males benefit by using this sensory trap because hoods make them more attractive, and receptive females may benefit when they approach hoods because they reduce their mate-search risk. (C) 2003 Published by Elsevier Ltd on behalf of The Association for the Study of Animal Behaviour. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. RI Baum, Julia/A-4693-2008; Backwell, Patricia/C-8883-2009 NR 21 TC 48 Z9 50 U1 2 U2 10 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUL PY 2003 VL 66 BP 89 EP 94 DI 10.1006/anbe.2003.2196 PN 1 PG 6 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 707CN UT WOS:000184492000008 ER PT J AU Endo, H Watanabe, K Hayashi, Y Matsuzaki, M Sakai, T Itoh, T Koie, H Kimura, J Stafford, BL AF Endo, H Watanabe, K Hayashi, Y Matsuzaki, M Sakai, T Itoh, T Koie, H Kimura, J Stafford, BL TI Three-dimensional CT image analysis of the digging system in the aardvark SO ANNALS OF ANATOMY-ANATOMISCHER ANZEIGER LA English DT Article DE aardvark; CT; digging; metacarpal; metatarsal ID PANDA AILUROPODA-MELANOLEUCA AB We examined the bone movement in the forepaw and hind paw in the aardvark (Orycteropus afer) by using three-dimensional (3D)-computed tomography (CT) techniques and osteometrical methods to confirm the functional adaptation of the extremities as a digging system. The four metacarpal bones could be strongly bent from the distal carpal bones. The distal end of the second and third metacarpal bones possessed enlarged smooth articulation surfaces that allowed the proximal phalanx to bend at a sharp angle. However, the articulation surface was not well-developed in the distal end of the fourth and fifth metacarpal bones and the proximal phalanx could bend at smaller angle in these two lateral digits. The proximal phalanges sharply crook from the metatarsal in the first, second, third and fourth digits in the hind paw. We suggest that the medial two digits in the forepaw directly contribute to the crushing, when these proximal phalanges crook in the phase of power stroke. In contrast the lateral third and fourth digits may act as sweeper of the crushed soil. These suggestions regarding the different functional adaptation between medial two digits and lateral two digits are consistent with the anatomical data of the forearm musculature. In the hind paw, we suggest that the second, third and fourth digits are functionally similar and that the hind paw may not act as a crushing apparatus but as a running motor or soil-sweeper similarly using these main three digits. C1 Museum Nat Sci, Dept Zool, Tokyo 1690073, Japan. Univ Tokyo, Fac Agr, Dept Vet Anat, Tokyo 113, Japan. Nihon Univ, Coll Bioresources Sci, Dept Prevent Vet Med & Anim Hlth, Kanagawa, Japan. Nihon Univ, Coll Bioresources Sci, Lab Comprehens Vet Clin Studies, Kanagawa, Japan. Nihon Univ, Coll Bioresources Sci, Dept Vet Anat, Kanagawa, Japan. Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA. RP Endo, H (reprint author), Museum Nat Sci, Dept Zool, Tokyo 1690073, Japan. RI Itou, Takuya/H-7406-2013 NR 10 TC 4 Z9 4 U1 3 U2 13 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0940-9602 J9 ANN ANAT JI Ann. Anat.-Anat. Anz. PD JUL PY 2003 VL 185 IS 4 BP 367 EP 372 DI 10.1016/S0940-9602(03)80063-8 PG 6 WC Anatomy & Morphology SC Anatomy & Morphology GA 709TL UT WOS:000184640400012 PM 12924475 ER PT J AU Bonanos, AZ Stanek, KZ Sasselov, DD Mochejska, BJ Macri, LM Kaluzny, J AF Bonanos, AZ Stanek, KZ Sasselov, DD Mochejska, BJ Macri, LM Kaluzny, J TI Direct distances to nearby galaxies using detached eclipsing binaries and Cepheids. IX. Variables in the field M31Y discovered with image subtraction SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; Cepheids; distance scale; galaxies : individual (M31); stars : variables : other ID ANDROMEDA GALAXY; MAGELLANIC-CLOUD; STARS; RADII; M-31; IV AB The DIRECT Project aims to obtain direct distances to two Local Group galaxies, M31 and M33, which occupy a crucial position near the base of the cosmological distance ladder. The first step is to search for detached eclipsing binaries (DEBs) and Cepheids using 1 m class telescopes to select good candidates, which will be followed up spectroscopically on 6.5-10 m class telescopes. In this ninth paper, we present a catalog of variable stars discovered with image subtraction in field M31Y (alpha = 10.degrees97, delta = 41.degrees69; J2000.0). The data were obtained with the Fred Lawrence Whipple Observatory 1.2 m telescope on 25 nights, over a period of 6 months. In our search covering 22' x 22', we discovered 41 eclipsing binaries, 126 Cepheids, and 97 other periodic or nonperiodic variables, including a luminous blue variable candidate, a nova, and a Galactic cataclysmic variable. The catalog of variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Bonanos, AZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Bonanos, Alceste/K-5392-2013; OI Bonanos, Alceste/0000-0003-2851-1905; Macri, Lucas/0000-0002-1775-4859 NR 28 TC 39 Z9 39 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2003 VL 126 IS 1 BP 175 EP 186 DI 10.1086/375762 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696UG UT WOS:000183905500017 ER PT J AU Ridge, NA Wilson, TL Megeath, ST Allen, LE Myers, PC AF Ridge, NA Wilson, TL Megeath, ST Allen, LE Myers, PC TI A (CO)-C-13 and (CO)-O-18 survey of the molecular gas around young stellar clusters within 1 kiloparsec of the Sun SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : clouds; radio emission lines; stars : formation ID HERBIG-AE/BE STARS; RADIATION-DRIVEN IMPLOSION; BRIGHT-RIMMED CLOUDS; IR IMAGING PHOTOMETRY; H-II REGIONS; DENSE CORES; FORMING REGIONS; UNBIASED SURVEY; HARO OBJECTS; CEPHEUS-A AB As the first step of a multiwavelength investigation into the relationship between young stellar clusters and their environment, we present fully sampled maps in the J = 1 - 0 lines of (CO)-C-13 and (CO)-O-18 and the J = 2 - 1 line of (CO)-O-18 for a selected group of 30 young stellar groups and clusters within 1 kpc of the Sun. This is the first systematic survey of these regions to date. The clusters range in size from several stars to a few hundred stars. Thirty fields ranging in size from 8' x 8' to 30' x 60' were mapped with 47" resolution simultaneously in the two J = 1 - 0 lines at the Five College Radio Astronomy Observatory. Seventeen sources were mapped over fields ranging in size from 3' x 3' to 13' x 13' in the J = 2 - 1 line with 35" resolution at the Submillimeter Telescope Observatory. We compare the cloud properties derived from each of the three tracers in order to better understand systematic uncertainties in determining masses and line widths. Cloud masses are determined independently using the (CO)-C-13 and (CO)-O-18 transitions; these masses range from 30 to 4000 M-.. Finally, we present a simple morphological classification scheme, which may serve as a rough indicator of cloud evolution. C1 Univ Massachusetts, Five Coll Radio Astron Observ, Dept Astron, Amherst, MA 01003 USA. Univ Arizona, Submillimeter Telescope Observ, Tucson, AZ 85721 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ridge, NA (reprint author), Univ Massachusetts, Five Coll Radio Astron Observ, Dept Astron, Amherst, MA 01003 USA. NR 95 TC 64 Z9 64 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2003 VL 126 IS 1 BP 286 EP 310 DI 10.1086/375455 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696UG UT WOS:000183905500026 ER PT J AU Malizia, A Bassani, L Capalbi, M Fabian, AC Fiore, F Nicastro, F AF Malizia, A Bassani, L Capalbi, M Fabian, AC Fiore, F Nicastro, F TI A BeppoSAX observation of MKN6 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : galaxies; galaxies : Seyfert; galaxies : individual : MKN6 ID X-RAY ABSORPTION; GALAXIES; REGIONS; NUCLEUS AB We have used the BeppoSAX satellite to study the broad band (0.5-100 keV) X-ray spectrum of the Seyfert 1.5 galaxy MKN6. The source is characterized by a power law of Gamma = 1.7(-0.07)(+0.08) and there is no strong evidence for either a reflection bump or a high energy cut-off. We have detected a narrow iron line at 6.4 keV ( rest frame) with an equivalent width of 98(-35+33) eV. MKN6 also exhibits strong and complex absorption. At least two components (N-H1 = 1.34(-0.4)(+0.4) x 10(22) cm(-2) and N-H2 = 4.18(-1.3)(+2.2) x 10(22) cm(-2)) are present and they both partially cover the source with covering fractions of similar to90% and similar to50% respectively. Comparison with a previous ASCA observation indicates that in both absorbing columns the N-H is variable over a 2 year timescale, while the covering fractions are constant over the same amount of time. The state of each absorber is cold or mildly photoionized. The Broad Line Region (BLR) is suggested as the possible location for this complex absorption. C1 CNR, IASF, I-40129 Bologna, Italy. ESA, ESRIN, ASI Sci Data Ctr, I-00044 Frascati, Italy. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Osserv Astron Roma, INAF, I-00044 Monte Porzio Catone, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Malizia, A (reprint author), CNR, IASF, Via Piero Gobetti 101, I-40129 Bologna, Italy. OI Fiore, Fabrizio/0000-0002-4031-4157; Malizia, Angela/0000-0002-6558-1163; Nicastro, Fabrizio/0000-0002-6896-1364; Bassani, Loredana/0000-0003-4858-6963 NR 14 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 JUL PY 2003 VL 406 IS 1 BP 105 EP 109 DI 10.1051/0004-6361:20030743 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700EJ UT WOS:000184099400018 ER PT J AU Morales-Rueda, L Marsh, TR Steeghs, D Unda-Sanzana, E Wood, JH North, RC AF Morales-Rueda, L Marsh, TR Steeghs, D Unda-Sanzana, E Wood, JH North, RC TI New results on GP Com SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion discs; binaries : spectroscopic; line : profiles; stars : mass-loss; stars : novae, cataclysmic variables; stars : individual : GP Com ID DB-WHITE-DWARFS; CATACLYSMIC VARIABLES; FORBIDDEN COMPONENTS; NEUTRAL HELIUM; STARS; SECONDARIES; SPECTRUM; BINARIES; G61-29; SEARCH AB We present high resolution optical and UV spectra of the 46 min orbital period, helium binary, GP Com. Our data contains simultaneous photometric correction which confirms the flaring behaviour observed in previous optical and UV data. In this system all lines show a triple peaked structure where the outer two peaks are associated with the accretion disc around the compact object. The main aim of this paper is to constrain the origin of the central peak, also called "central spike". We find that the central spike contributes to the flare spectra indicating that its origin is probably the compact object. We also detect that the central spike moves with orbital phase following an S-wave pattern. The radial velocity semiamplitude of the S-wave is similar to10 km s(-1) indicating that its origin is near the centre of mass of the system, which in this case lies very close to the white dwarf. Our resolution is higher than that of previous data which allows us to resolve structure in the central peak of the line. The central spike in three of the He. lines shows another peak blueshifted with respect to the main peak. We propose that one of the peaks is a neutral helium forbidden transition excited in a high electron density region. This forbidden transition is associated with the permitted one ( the stronger peak in two of the lines). The presence of a high electron density region again favours the white dwarf as their origin. We compute Doppler maps for the emission lines which show three emission regions: an accretion disc, a bright spot and an unidentified low velocity emission region associated with the central spike. We obtain modulation Doppler tomograms for some of the emission lines that map the anisotropic emission from the bright spot region. The HST UV spectra also show a strong flare component and confirm the under abundance of silicon in GP Com. C1 Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02318 USA. Univ Keele, Sch Chem & Phys, Astrophys Grp, Keele ST5 5BG, Staffs, England. Met Off, Bracknell RG12 2SZ, Berks, England. RP Morales-Rueda, L (reprint author), Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. RI Unda-Sanzana, Eduardo/K-3592-2012; Steeghs, Danny/C-5468-2009 OI Unda-Sanzana, Eduardo/0000-0002-7514-8312; Steeghs, Danny/0000-0003-0771-4746 NR 29 TC 32 Z9 32 U1 0 U2 2 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2003 VL 405 IS 1 BP 249 EP 261 DI 10.1051/0004-6361:20030552 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 689RV UT WOS:000183507500027 ER PT J AU Pirogov, L Zinchenko, I Caselli, P Johansson, LEB Myers, PC AF Pirogov, L Zinchenko, I Caselli, P Johansson, LEB Myers, PC TI N2H+(1-0) survey of massive molecular cloud cores SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; ISM : clouds; ISM : molecules; radio lines : ISM ID H-II REGIONS; YOUNG STELLAR OBJECTS; FAR-INFRARED SOURCES; SOUTHERN H2O MASERS; STAR-FORMATION; DENSE CORES; DUST CONTINUUM; OUTER GALAXY; HYPERFINE-STRUCTURE; DARK CLOUDS AB We present the results of N2H+(1-0) observations of 35 dense molecular cloud cores from the northern and southern hemispheres where massive stars and star clusters are formed. Line emission has been detected in 33 sources, for 28 sources detailed maps have been obtained. Peak N2H+ column densities lie in the range: 3.6 x 10(12)-1.5 x 10(14) cm(-2). Intensity ratios of (01-12) to (23-12) hyperfine components are slightly higher than the LTE value. The optical depth of (23-12) component toward peak intensity positions of 10 sources is similar to0.2-1. In many cases the cores have elongated or more complex structures with several emission peaks. In total, 47 clumps have been revealed in 26 sources. Their sizes lie in the range 0.3-2.1 pc, the range of virial masses is similar to30-3000 M-circle dot. Mean N2H+ abundance for 36 clumps is 5 x 10-10. Integrated intensity maps with axial ratios <2 have been fitted with a power-law radial distribution &SIM;r(-p) convolved with the telescope beam. Mean power-law index for 25 clumps is close to 1.3. For reduced maps where positions of low intensity are rejected mean power-law index is close to unity corresponding to the &SIM;r(-2) density profile provided N2H+ excitation conditions do not vary inside these regions. In those cases where we have relatively extensive and high quality maps, line widths of the cores either decrease or stay constant with distance from the center, implying an enhanced dynamical activity in the center. There is a correlation between total velocity gradient direction and elongation angle of the cores. However, the ratio of rotational to gravitational energy is too low (4 x 10(-4)-7.1 x 10(-2)) for rotation to play a significant role in the dynamics of the cores. A correlation between mean line widths and sizes of clumps has been found. A comparison with physical parameters of low-mass cores is given. C1 Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603950, Russia. Nizhny Novgorod Univ, Nizhnii Novgorod 603950, Russia. Univ Helsinki, Helsinki Univ Observ, FIN-00014 Helsinki, Finland. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Onsala Space Observ, S-43992 Onsala, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pirogov, L (reprint author), Russian Acad Sci, Inst Appl Phys, Ulyanova 46, Nizhnii Novgorod 603950, Russia. OI Zinchenko, Igor/0000-0003-2793-8229 NR 52 TC 62 Z9 63 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2003 VL 405 IS 2 BP 639 EP 654 DI 10.1051/0004-6361:20030659 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691PY UT WOS:000183615700028 ER PT J AU Krivonos, RA Vikhlinin, AA Markevitch, ML Pavlinsky, MN AF Krivonos, RA Vikhlinin, AA Markevitch, ML Pavlinsky, MN TI A possible shock wave in the intergalactic medium of the cluster of galaxies A754 SO ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS LA English DT Article DE clusters of galaxies; shock waves ID PHYSICS; A3667 AB observations show the nonequilibrium state of the central part of the cluster, in which a cloud of cold plasma similar to500 kpc in size was identified amid the hotter cluster gas. The X-ray image of A754 exhibits a brightness discontinuity, which can be interpreted as a shock wave in front of a moving cloud of dense gas. The shock parameters are determined from the jump in intergalactic gas density using the ROSAT image. The estimated Mach number is M-1 = 1.71(-0.24)(+0.45) at a 68% confidence level. (C) 2003 MAIK "Nauka/Interperiodica". kalInterperiodica". C1 Russian Acad Sci, Space Res Inst, Moscow 117810, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krivonos, RA (reprint author), Russian Acad Sci, Space Res Inst, Profsoyuznaya Ul 84-32, Moscow 117810, Russia. NR 12 TC 15 Z9 15 U1 0 U2 1 PU MAIK NAUKA/INTERPERIODICA PUBL PI MELVILLE PA C/O AMERICAN INST PHYSICS, 2 HUNTINGTON QUANDRANGLE, STE 1NO1, MELVILLE, NY 11747-4502 USA SN 1063-7737 J9 ASTRON LETT+ JI Astron. Lett.-J. Astron. Space Astrophys. PD JUL PY 2003 VL 29 IS 7 BP 425 EP 428 DI 10.1134/1.1589859 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 704VF UT WOS:000184360800001 ER PT J AU Erb, DK Shapley, AE Steidel, CC Pettini, M Adelberger, KL Hunt, MP Moorwood, AFM Cuby, JG AF Erb, DK Shapley, AE Steidel, CC Pettini, M Adelberger, KL Hunt, MP Moorwood, AFM Cuby, JG TI H alpha spectroscopy of galaxies at z > 2: Kinematics and star formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : high-redshift; galaxies : kinematics and dynamics stars : formation ID LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; LUMINOSITY FUNCTION; STARBURST GALAXIES; FORMING GALAXIES; FIELD GALAXIES; ULTRAVIOLET LUMINOSITY; STELLAR POPULATIONS; BRIGHT STARBURST; QSO FIELDS AB We present near-infrared spectroscopy of Halpha emission lines in a sample of 16 star-forming galaxies at redshifts 2.0 < z < 2.6. Our targets are drawn from a large sample of galaxies photometrically selected and spectroscopically confirmed to lie in this redshift range. We have obtained this large sample with an extension of the broadband U(n)GR color criteria used to identify Lyman break galaxies at z similar to 3. The primary selection criterion for IR spectroscopic observation was proximity to a QSO sight line; we therefore expect the galaxies presented here to be representative of the sample as a whole. Six of the galaxies exhibit spatially extended, tilted Halpha emission lines; rotation curves for these objects reach mean velocities of similar to150 km s(-1) at radii of similar to6 kpc, without corrections for inclination or any other observational effect. The velocities and radii give a mean dynamical mass of (M) greater than or equal to 4 x 10(10) M(circle dot). We have obtained archival Hubble Space Telescope images for two of these galaxies; they are morphologically irregular. One-dimensional velocity dispersions for the 16 galaxies range from similar to50 to similar to260 km s(-1), and in cases in which we have both virial masses implied by the velocity dispersions and dynamical masses derived from the spatially extended emission lines, they are in rough agreement. We compare our kinematic results with similar measurements made at z similar to 3 and find that both the observed rotational velocities and velocity dispersions tend to be larger at z similar to 2 than at z similar to 3. We also calculate star formation rates (SFRs) from the Halpha luminosities and compare them with SFRs calculated from the UV continuum luminosity. We find a mean SFR(Halpha) of 16 M(circle dot) yr(-1) and an average SFR(Halpha)/SFR(UV) ratio of 2.4, without correcting for extinction. We see moderate evidence for an inverse correlation between the UV continuum luminosity and the ratio SFR(Halpha)/SFR(UV), such as might be observed if the UV-faint galaxies suffered greater extinction. We discuss the effects of dust and star formation history on the SFRs and conclude that extinction is the most likely explanation for the discrepancy between the two SFRs. C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. European So Observ, Santiago 19, Chile. RP Erb, DK (reprint author), CALTECH, Dept Astron, MS 105-24, Pasadena, CA 91125 USA. EM dke@astro.caltech.edu NR 59 TC 164 Z9 164 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2003 VL 591 IS 1 BP 101 EP 118 DI 10.1086/375316 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QR UT WOS:000183617400007 ER PT J AU McDowell, JC Clements, DL Lamb, SA Shaked, S Hearn, NC Colina, L Mundell, C Borne, K Baker, AC Arribas, S AF McDowell, JC Clements, DL Lamb, SA Shaked, S Hearn, NC Colina, L Mundell, C Borne, K Baker, AC Arribas, S TI Chandra observations of extended X-ray emission in Arp 220 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (Arp 220); galaxies : interactions; galaxies : starburst; X-rays : galaxies ID ULTRALUMINOUS IRAS GALAXIES; ARP 220; INFRARED GALAXIES; STARBURST GALAXY; STAR-FORMATION; RING GALAXIES; IC 4553; H-I; MARKARIAN-231; MORPHOLOGIES AB We resolve the extended X-ray emission from the prototypical ultraluminous infrared galaxy Arp 220. Extended, faint, edge-brightened, soft X-ray lobes outside the optical galaxy are observed to a distance of 10-15 kpc on each side of the nuclear region. Bright plumes inside the optical isophotes coincide with the optical line emission and extend 11 kpc from end to end across the nucleus. The data for the plumes cannot be fitted by a single-temperature plasma and display a range of temperatures from 0.2 to 1 keV. The plumes emerge from bright, diffuse circumnuclear emission in the inner 3 kpc centered on the Halpha peak, which is displaced from the radio nuclei. There is a close morphological correspondence between the Halpha and soft X-ray emission on all spatial scales. We interpret the plumes as a starburst-driven superwind and discuss two interpretations of the emission from the lobes in the context of simulations of the merger dynamics of Arp 220. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2BW, England. Univ Illinois, Ctr Theoret Astrophys, Dept Phys, Loomis Lab Phys, Urbana, IL 61801 USA. Univ Illinois, Ctr Theoret Astrophys, Dept Astron, Loomis Lab Phys, Urbana, IL 61801 USA. Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. CSIC, Inst Estructura Mat, E-28006 Madrid, Spain. Liverpool John Moores Univ, ARI, Wirral CH41 1LD, Cheshire, England. NASA, Goddard Space Flight Ctr, Raytheon Informat Technol Serv, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Raytheon Sci Serv, Greenbelt, MD 20771 USA. Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. Space Telescope Sci Inst, ESA Space Telescope Div, Baltimore, MD 21218 USA. RP McDowell, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 45 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 JUL 1 PY 2003 VL 591 IS 1 BP 154 EP 166 DI 10.1086/375289 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QR UT WOS:000183617400011 ER PT J AU Saucedo, J Calvet, N Hartmann, L Raymond, J AF Saucedo, J Calvet, N Hartmann, L Raymond, J TI The spatial distribution of fluorescent H-2 emission near T Tauri SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : formation; stars : individual (T Tauri); stars : pre-main-sequence; stars : winds, outflows; ultraviolet : stars ID HUBBLE-SPACE-TELESCOPE; HERBIG-HARO OBJECTS; BINARY-SYSTEM; MOLECULAR-HYDROGEN; BURNHAMS NEBULA; YOUNG STARS; SPECTRA; CLOUD; JETS; SPECTROSCOPY AB New subarcsecond far-UV observations of T Tau with Hubble Space Telescope STIS show spatially resolved structures in the 2" x 2" area around the star. The structures are apparent in multiline emission of fluorescent H-2 pumped by Lyalpha. One emission structure follows the cavity walls observed around T Tau N in scattered light in the optical. A temperature of greater than or equal to1000 K is required to have a high enough population in the H-2 to produce the observed fluorescent lines; in the cool environment of the T Tau system, shock heating is required to achieve this temperature at distances of a few tens of AU. Fluorescent H-2 along the cavity wall represents the best evidence to date for the action of low-density, wide opening angle outflows driving cavities into the molecular medium at scales less than or equal to100 AU. A southern region of emission consists of two arcs, with shape and orientation similar to the arcs of H-2 2.12 mum and forbidden-line emission crossing the outflow associated with the embedded system T Tau S. This region is located near the centroid of forbidden-line emission at the blueshifted lobe of the north-south outflow. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Saucedo, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 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 JUL 1 PY 2003 VL 591 IS 1 BP 275 EP 282 DI 10.1086/374885 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QR UT WOS:000183617400019 ER PT J AU Garcia, MR Miller, JM McClintock, JE King, AR Orosz, J AF Garcia, MR Miller, JM McClintock, JE King, AR Orosz, J TI Resolved jets and long-period black hole X-ray novae SO ASTROPHYSICAL JOURNAL LA English DT Review DE novae, cataclysmic variables; X-rays : binaries ID RXTE SPECTRAL OBSERVATIONS; MICROQUASAR XTE J1550-564; TRANSIENT GRO J1655-40; RADIO-EMISSION; SUPERLUMINAL SOURCE; RELATIVISTIC JETS; SOURCE A0620-00; ENERGY-SPECTRA; NEUTRON-STAR; LIGHT CURVES AB In this brief note we point out that the four spatially resolved relativistic jets among the 14 dynamically confirmed black hole X-ray novae are all in systems with long orbital periods. Many shorter period systems show transient radio outbursts that are attributed to jets, but these jets have not been spatially resolved. Super-Eddington accretion has been suggested as a requirement for jet formation and may be consistent with our compilation of luminosities, but some super-Eddington outbursts did not form spatially resolved jets. We speculate that some as yet unknown process (or combination of processes) favors formation of substantially larger jets in long-period systems. Two short-period systems show evidence of being extended, but have not been resolved into multiple components, as the long-period systems have. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Garcia, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM garcia@cfa.harvard.edu; jmmiller@cfa.harvard.edu; jem@cfa.harvard.edu; ark@astro.le.ac.uk; orosz@zwartgat.sdsu.edu NR 107 TC 27 Z9 27 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2003 VL 591 IS 1 BP 388 EP 396 DI 10.1086/375218 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QR UT WOS:000183617400029 ER PT J AU Goldberg, D Mazeh, T Latham, DW AF Goldberg, D Mazeh, T Latham, DW TI On the mass-ratio distribution of spectroscopic binaries SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; Galaxy : halo; methods : statistical; stars : formation; stars : fundamental parameters ID PROPER-MOTION STARS; DA WHITE-DWARFS; SOLAR-TYPE STARS; ORBITAL SOLUTIONS; SAMPLE; EVOLUTION; FRAGMENTATION; MULTIPLICITY; SECONDARIES; PHOTOMETRY AB In this paper we derive the mass-ratio and secondary-mass distributions of a large, well-defined, complete sample of 129 spectroscopic binaries with periods between 1 and 2500 days. The binaries, whose orbits were published recently, were detected by a systematic radial-velocity survey of a sample of more than 1400 large proper motion stars. Three features stand out in the mass-ratio distribution: a rise as the mass ratio goes down to q similar to 0.2, a sharp drop below q similar to 0.2, and a smaller peak at q similar to 0.8. Another way to characterize the results is to state that the distribution includes two "populations," one with a high asymmetric peak at q similar to 0.2 and another with a smaller peak at q similar to 0.8, while the minimum between the two populations is centered at q similar to 0.55. The size of the binary sample allows us to divide it into two subsamples and look for differences in the mass-ratio distributions of the two subsamples. We performed two different divisions: one into Galactic halo versus disk populations, and the other into high- and low-mass primary stars ( above and below 0.67 M-circle dot). The former division yields differences with moderate statistical significance of 88%, while the latter is more significant at a level of 97%. Our analysis suggests that the rise toward low mass ratios does not appear in the mass-ratio distribution of the halo binaries. The other separation shows a broad peak at mass ratio of q similar to 0.8-1 for the subsample of binaries with low-mass primaries but no corresponding peak in the subsample with high- mass primaries. We discuss our findings and their application to theories of binary formation. C1 Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Goldberg, D (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. NR 67 TC 41 Z9 41 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2003 VL 591 IS 1 BP 397 EP 405 DI 10.1086/345990 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QR UT WOS:000183617400030 ER PT J AU Grav, T Holman, MJ Kavelaars, JJ AF Grav, T Holman, MJ Kavelaars, JJ TI The short rotation period of Nereid SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites : individual (Nereid) ID CHAOTIC ROTATION; HYPERION; NEPTUNE; SATELLITES; PHOTOMETRY; DYNAMICS AB We determine the period, p = 11.52 +/- 0.14 hr, and a light-curve peak-to-peak amplitude, a = 0.029 +/- 0.003 mag, of the Neptunian irregular satellite Nereid. If the light-curve variation is due to albedo variations across the surface, rather than solely to the shape of Nereid variations, the rotation period would be a factor of 2 shorter. In either case, such a rotation period and light-curve amplitude, together with Nereid's orbital period, p = 360.14 days, imply that Nereid is almost certainly in a regular rotation state, rather than the chaotic rotation state suggested in work of Schaefer & Schaefer and of Dobrovolskis. Assuming that Nereid is perfectly spherical, the albedo variation is 3% across the observed surface. Assuming a uniform geometric albedo, the observed cross-sectional area varies by 3%. We caution that the light curve found in this Letter only sets limits on the combination of albedo and physical irregularity and that we cannot determine the orientation of Nereid's spin axis from our data. C1 Univ Oslo, Inst Theoret Astrophys, N-0359 Oslo, Norway. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. RP Grav, T (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0359 Oslo, Norway. EM tommy.grav@astro.uio.no; mholman@cfa.harvard.edu; jj.kavelaars@nrc-cnrc.gc.ca NR 24 TC 14 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 JUL 1 PY 2003 VL 591 IS 1 BP L71 EP L74 DI 10.1086/377067 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QZ UT WOS:000183618100018 ER PT J AU Kastner, JH Balick, B Blackman, EG Frank, A Soker, N Vrtilek, SD Li, JQ AF Kastner, JH Balick, B Blackman, EG Frank, A Soker, N Vrtilek, SD Li, JQ TI A compact X-ray source and possible X-ray jets within the planetary nebula Menzel 3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : jets and outflows; planetary nebulae : individual (Menzel 3); stars : AGB and post-AGB; stars : mass loss; stars : winds, outflows ID PREPLANETARY NEBULAE; BINARY-SYSTEMS; R-AQUARII; EMISSION; STARS; MZ-3; DISCOVERY; NGC-7027; OUTFLOW; WINDS AB We report the discovery, by the Chandra X-Ray Observatory, of X-ray emission from the bipolar planetary nebula Menzel 3. In Chandra CCD imaging, Mz 3 displays hot [similar to(3-6) x 10(6) K] gas within its twin, coaxial bubbles of optical nebulosity as well as a compact X-ray source at the position of its central star(s). The brightest diffuse X-ray emission lies along the polar axis of the optical nebula, suggesting a jetlike configuration. The observed combination of an X-ray-emitting point source and possible X-ray jet(s) is consistent with models in which accretion disks and, potentially, magnetic fields shape bipolar planetary nebulae via the generation of fast, collimated outflows. C1 Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Dept Phys, IL-36006 Oranim, Tivon, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kastner, JH (reprint author), Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. NR 37 TC 51 Z9 51 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2003 VL 591 IS 1 BP L37 EP L40 DI 10.1086/376979 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QZ UT WOS:000183618100010 ER PT J AU Stanek, KZ Matheson, T Garnavich, PM Martini, P Berlind, P Caldwell, N Challis, P Brown, WR Schild, R Krisciunas, K Calkins, ML Lee, JC Hathi, N Jansen, RA Windhorst, R Echevarria, L Eisenstein, DJ Pindor, B Olszewski, EW Harding, P Holland, ST Bersier, D AF Stanek, KZ Matheson, T Garnavich, PM Martini, P Berlind, P Caldwell, N Challis, P Brown, WR Schild, R Krisciunas, K Calkins, ML Lee, JC Hathi, N Jansen, RA Windhorst, R Echevarria, L Eisenstein, DJ Pindor, B Olszewski, EW Harding, P Holland, ST Bersier, D TI Spectroscopic discovery of the supernova 2003dh associated with GRB 030329 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : distances and redshifts; gamma rays : bursts; supernovae : general; supernovae : individual (SN 2003dh) ID GAMMA-RAY BURST; OPTICAL AFTERGLOW; STANDARD STARS; SN 1998BW; FOLLOW-UP; SPECTROPHOTOMETRY; SPECTROGRAPH; GRB-011121; HYPERNOVA; TELESCOPE AB We present early observations of the afterglow of GRB 030329 and the spectroscopic discovery of its associated supernova SN 2003dh. We obtained spectra of the afterglow of GRB 030329 each night from March 30.12 (0.6 days after the burst) to April 8.13 (UT) (9.6 days after the burst). The spectra cover a wavelength range of 350-850 nm. The early spectra consist of a power-law continuum (F-v proportional to v(-0.9)) with narrow emission lines originating from H II regions in the host galaxy, indicating a low redshift of. However, our spectra taken z = 0.1687 after 2003 April 5 show broad peaks in flux characteristic of a supernova. Correcting for the afterglow emission, we find that the spectrum of the supernova is remarkably similar to the Type Ic "hypernova" SN 1998bw. While the presence of supernovae has been inferred from the light curves and colors of gamma-ray burst afterglows in the past, this is the first direct, spectroscopic confirmation that a subset of classical gamma-ray bursts originate from supernovae. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Smithsonian Inst, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Campanas Observ, La Serena, Chile. Cerro Tololo Interamer Observ, La Serena, Chile. Univ Arizona, Steward Observ, Tucson, AZ 85718 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. RP Stanek, KZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Hathi, Nimish/J-7092-2014 OI Hathi, Nimish/0000-0001-6145-5090 NR 45 TC 842 Z9 850 U1 2 U2 10 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2003 VL 591 IS 1 BP L17 EP L20 DI 10.1086/376976 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QZ UT WOS:000183618100005 ER PT J AU Yoshida, N Sokasian, A Hernquist, L Springel, V AF Yoshida, N Sokasian, A Hernquist, L Springel, V TI Early structure formation and reionization in a warm dark matter cosmology SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; dark matter; early universe; stars : formation ID NUMERICAL COSMOLOGY; 1ST STARS; UNIVERSE; CONSTRAINTS AB We study the first structure formations in Lambda-dominated universes using large cosmological N-body/smoothed particle hydrodynamics simulations. We consider a standard Lambda cold dark matter (CDM) model and a Lambda warm dark matter (WDM) model in which the mass of the dark matter particles is taken to be m(X) = 10 keV. The linear power spectrum for the LambdaWDM model has a characteristic cutoff at a wavenumber k = 200 Mpc(-1), suppressing the formation of low- mass (<10(6) M-circle dot) nonlinear objects early on. The absence of low- mass halos in the WDM model makes the formation of primordial gas clouds with molecular hydrogen very inefficient at high redshifts. The first star-forming gas clouds form at z approximate to 21 in the WDM model, considerably later than in the CDM counterpart, and the abundance of these gas clouds differs by an order of magnitude between the two models. We carry out radiative transfer calculations by embedding massive Population III stars in the gas clouds. We show that the volume fraction of ionized gas rises up close to 100% by z = 18 in the CDM case, whereas that of the WDM model remains extremely small at a level of a few percent. Thus, the WDM model with m(X) = 10 keV is strongly inconsistent with the high optical depth observed by the Wilkinson Microwave Anisotropy Probe satellite. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Yoshida, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Yoshida, Naoki/A-4305-2011 NR 25 TC 92 Z9 92 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 JUL 1 PY 2003 VL 591 IS 1 BP L1 EP L4 DI 10.1086/376963 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QZ UT WOS:000183618100001 ER PT J AU Beadell, JS Schreiber, EA Schreiber, RW Schenk, GA Doherty, PF AF Beadell, JS Schreiber, EA Schreiber, RW Schenk, GA Doherty, PF TI Survival of Brown Boobies (Sula leucogaster) at Johnston Atoll: A long-term study SO AUK LA English DT Article ID NINO-SOUTHERN OSCILLATION; EL-NINO; MARKED ANIMALS; BREEDING PROBABILITIES; POPULATIONS; VARIABILITY; SEABIRDS; PACIFIC AB Survival of Brown Boobies (Sula leucogaster) at Johnston Atoll was examined over a 17-year period using capture-mark-recapture analysis. Annual adult survival was estimated to be 0.90 +/- 0.01 (SE). Variation in survival did not correspond to either local environmental fluctuation or more widespread disturbances associated with El Nino-Southern Oscillation events, and a time-invariant model of survival was best supported by our data. Absence of major oceanographic anomalies in the immediate vicinity of Johnston Atoll may contribute to relatively high and invariant survival in Brown Boobies. C1 Natl Museum Nat Hist, Bird Dept, Washington, DC 20560 USA. Smithsonian Inst, Genet Program, Washington, DC 20008 USA. Museum Hist Nat, Los Angeles, CA 90007 USA. Colorado State Univ, Dept Fishery & Wildlife Biol, Ft Collins, CO 80512 USA. RP Schreiber, EA (reprint author), Natl Museum Nat Hist, Bird Dept, E 607 MRC 116, Washington, DC 20560 USA. NR 41 TC 11 Z9 11 U1 1 U2 7 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JUL PY 2003 VL 120 IS 3 BP 811 EP 817 DI 10.1642/0004-8038(2003)120[0811:SOBBSL]2.0.CO;2 PG 7 WC Ornithology SC Zoology GA 713AB UT WOS:000184830800022 ER PT J AU Meese, RJ Neronov, VM Alestchenko, GM Ruggiero, M AF Meese, RJ Neronov, VM Alestchenko, GM Ruggiero, M TI Rapid acquisition and dissemination of standardized biological inventories from Russian Biosphere Reserves SO BIODIVERSITY AND CONSERVATION LA English DT Article DE biodiversity; biological inventory; biosphere reserve; nomenclature; Russia; systematics; zapovednik ID WESTERN AB We accumulate, standardize, and disseminate the results of biological inventories of 21 protected areas in the Russian Federation; each of these areas has been recognized by UNESCO's Man and the Biosphere (MAB) program as a Biosphere Reserve. These inventories, comprising 4702 species of plants and 1094 species of vertebrate animals of the breadth of Russia, represent 20% of the vascular flora and 73% of the vertebrate fauna of Russia and are made widely available for the first time. We describe an approach to the development and Internet availability of large databases of species inventories which were produced through the provision of custom biological inventory software supported by training, cost-free distribution, and a modest amount of taxonomic support. Our experiences also highlight the essential role of an active national office in a system of protected areas. Our approach overcomes many of the obstacles inherent in previous and existing attempts to assemble the results of biological inventories derived from a variety of sources. We suggest a similar application of biological inventory software, supported by national coordination, as an effective means to provide access to species inventories of a system of protected areas. Standardized, taxonomically current species inventories are essential components of regional and global conservation efforts. C1 Univ Calif Davis, Informat Ctr Environm, Dept Environm Sci & Policy, Davis, CA 95616 USA. Russian MAB Comm, Moscow, Russia. Natl Museum Nat Hist, Smithsonian Inst, Biodivers Programs ITIS, Washington, DC 20560 USA. RP Meese, RJ (reprint author), Univ Calif Davis, Informat Ctr Environm, Dept Environm Sci & Policy, Davis, CA 95616 USA. RI Neronov, Valery/C-3959-2014 NR 17 TC 0 Z9 0 U1 1 U2 3 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD JUL PY 2003 VL 12 IS 7 BP 1421 EP 1429 DI 10.1023/A:1023685928666 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 675WZ UT WOS:000182721700007 ER PT J AU Rehse, T Kress, WJ AF Rehse, T Kress, WJ TI Distichochlamys rubrostriata (Zingiberaceae), a new species from northern Vietnam SO BRITTONIA LA English DT Article DE Distichochlamys; Zingiberaceae; Zingibereae; Scaphochlamys; Vietnam; southeast Asia AB A third species of the until recently monotypic genus Distichochlamys (Zingiberaceae) is described from living and preserved material collected in northern Vietnam. Distichochlamys rubrostriata is distinguished from the original species, D. citrea, and the recently described D. orlowii, on the basis of leaf, inflorescence bract, lateral staminode, and labellum characters. C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Natl Museum Nat Hist, Smithsonian Inst, US Natl Herbarium, Washington, DC 20560 USA. RP Rehse, T (reprint author), Duke Univ, Dept Biol, Box 90338, Durham, NC 27708 USA. NR 9 TC 1 Z9 2 U1 0 U2 0 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD JUL-AUG PY 2003 VL 55 IS 3 BP 205 EP 208 DI 10.1663/0007-196X(2003)055[0205:DRZANS]2.0.CO;2 PG 4 WC Plant Sciences SC Plant Sciences GA 703YD UT WOS:000184309800001 ER PT J AU Eberhard, WG AF Eberhard, WG TI Sexual behavior and morphology of Themira minor (Diptera : Sepsidae) males and the evolution of male sternal lobes and genitalic surstyli SO CANADIAN ENTOMOLOGIST LA English DT Article ID FUNCTIONAL-MORPHOLOGY; FLIES DIPTERA; COURTSHIP; MICROSEPSIS; COPULATION; CYNIPSEA AB Probable ancestral types of courtship behavior for most sepsid flies were deduced from the behavior and morphology of a species in the relatively basal genus Themira. At least three of the five behavior patterns used by Themira minor (Haliday) males to court females prior to and during copulation are shared with other, more derived groups. During copulation the male's sternal lobes were rotated so that their brushes of long setae were fanned apart and may tap the female. The morphology of the tips of the male's genitalic surstyli and the muscles attached to them indicate that they are also moveable. This trait, which occurs in several other distantly related species, probably serves to squeeze the female during copulation. Thus, contrary to the impression from previous studies, elaborate courtship before and during copulation may be widespread among sepsids. C1 Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad, Costa Rica. Ciudad Sanitaria & Univ Vall Hebron, Escuela Biol, Ciudad, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad, Costa Rica. NR 22 TC 15 Z9 15 U1 1 U2 9 PU ENTOMOL SOC CANADA PI OTTAWA PA 393 WINSTON AVE, OTTAWA, ONTARIO K2A 1Y8, CANADA SN 0008-347X J9 CAN ENTOMOL JI Can. Entomol. PD JUL-AUG PY 2003 VL 135 IS 4 BP 569 EP 581 PG 13 WC Entomology SC Entomology GA 700YU UT WOS:000184139400005 ER PT J AU Klemm, DJ Daniels, BA Moser, WE Lester, RJG AF Klemm, DJ Daniels, BA Moser, WE Lester, RJG TI Biology of the leech Actinobdella inequiannulata Moore, 1901 (Annelida : Hirudinea : Rhynchobdellida : Glossiphoniidae), parasitic on the white sucker, Catostomus commersoni Lacepede, 1803, and the longnose sucker, Catostomus catostomus Forster, 1773, in Algonquin Provincial Park, Ontario, Canada SO COMPARATIVE PARASITOLOGY LA English DT Article DE benthic invertebrate; freshwater annelid; feeding behavior; fish parasite; leech; parasitism; Actinobdella annectens; Actinobdella inequiannulata; Actinobdella pediculata; Actinobdella triannulata; Myzobdella lugubris; white sucker; Catostomus commersoni; longnose sucker; Catostomus catostomus; Algonquin Provincial Park; Ontario; Canada ID HELOBDELLA-STAGNALIS L; FRESH-WATER LEECHES; LIFE-HISTORY; SOUTH-WALES; POPULATION; RECORDS; RIVER; CYCLE; LAKE AB Actinobdella inequiannulata was found on the white sucker. Catostomus commersoni, and less frequently on the longnose sucker, Catostomus catostomus, in Algonquin Provincial Park, Ontario, Canada. Catostomus commersoni parasitized with Act. inequiannulata was collected from July to October 1973 and May to October 1974. In May and October, less than 3% of the fish carried leeches. In July, 80% of the fish were parasitized with an average of 1.5 leeches/fish. Observations on leech weight suggest that young leeches attach to fish from May to September, some mature in July, and a second generation of leeches reparasitize the fish in August and September. The mean size of leeches on suckers increased from May until July, after which the size remained relatively constant. Leeches produced characteristic lesions on the opercula of suckers. Fully developed lesions on fish opercula produced by aggregated leeches had varying amounts of central erosion, extravasation, dermal and epidermal hyperplasia, and necrosis. C1 US EPA, Off Res & Dev, Natl Exposure Res Lab, Ecosyst Res Branch,Ecol Exposure Res Div, Cincinnati, OH 45268 USA. Smithsonian Inst, Natl Museum Nat Hist, ADP Off, Washington, DC 20560 USA. Univ Queensland, Dept Microbiol & Parasitol, Brisbane, Qld 4072, Australia. RP Klemm, DJ (reprint author), US EPA, Off Res & Dev, Natl Exposure Res Lab, Ecosyst Res Branch,Ecol Exposure Res Div, Cincinnati, OH 45268 USA. EM klemm.Donald@epa.gov; daniels.bruce@nmnh.si.edu; moser.William@nmnh.si.edu; r.lester@mail.box.uq NR 40 TC 4 Z9 4 U1 3 U2 7 PU HELMINTHOLOGICAL SOC WASHINGTON PI LAWRENCE PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS 66044 USA SN 1525-2647 EI 1938-2952 J9 COMP PARASITOL JI Comp. Parasitol. PD JUL PY 2003 VL 70 IS 2 BP 120 EP 127 DI 10.1654/4064 PG 8 WC Parasitology; Zoology SC Parasitology; Zoology GA 701XH UT WOS:000184193900003 ER PT J AU Dupuis, AP Marra, PP Kramer, LD AF Dupuis, AP Marra, PP Kramer, LD TI Serologic evidence of West Nile virus transmission, Jamaica, West Indies SO EMERGING INFECTIOUS DISEASES LA English DT Article ID CROSS-NEUTRALIZATION; BIRDS; ARBOVIRUSES; FLAVIVIRUSES; INFECTION AB In spring 2002, an intensive avian serosurvey was initiated in Jamaica, Puerto Rico, and Mexico. We collected >1,600 specimens from resident and nonresident neotropical migratory birds before their northerly migrations. Plaque reduction neutralization test results indicated specific neutralizing antibodies to West Nile virus in 11 resident species from Jamaica. C1 New York State Dept Hlth, Slingerlands, NY USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Dupuis, AP (reprint author), Griffin Lab, 5668 State Farm Rd, Slingerlands, NY 12159 USA. FU ODCDC CDC HHS [U50/CCU320544-01] NR 18 TC 90 Z9 102 U1 0 U2 5 PU CENTER DISEASE CONTROL PI ATLANTA PA ATLANTA, GA 30333 USA SN 1080-6040 J9 EMERG INFECT DIS JI Emerg. Infect. Dis PD JUL PY 2003 VL 9 IS 7 BP 860 EP 863 PG 4 WC Immunology; Infectious Diseases SC Immunology; Infectious Diseases GA 698WL UT WOS:000184022300017 PM 12890329 ER PT J AU de Oliveira, CR Ruiz-Miranda, CR Kleiman, DG Beck, BB AF de Oliveira, CR Ruiz-Miranda, CR Kleiman, DG Beck, BB TI Play behavior in juvenile golden lion tamarins (Callitrichidae : Primates): Organization in relation to costs SO ETHOLOGY LA English DT Article ID COTTON-TOP TAMARINS; SOCIAL PLAY; LEONTOPITHECUS-ROSALIA; SQUIRREL-MONKEYS; HABITAT QUALITY; GELADA BABOONS; MACACA-MULATTA; VIGILANCE; ECOLOGY; VOCALIZATIONS AB Play is a complex behavior that is widespread among vertebrates. Despite the potential benefits for the development of social, cognitive and motor skills, play behavior has costs: energy expenditure, and the risks of injury and predation. As the fitness benefits of play are presumably to be gained as adults, we expect young animals to minimize its immediate costs. Here, we describe play behavior in golden lion tamarins (GLTs) (Leontopithecus rosalia ) and test cost-minimizing hypotheses. We collected data on play behavior and adult vigilance in nine groups (four wild and five supplemented, the latter deriving from a reintroduction) of wild-living lion tamarins (16 infants) in Brazil. Results showed that play occupied 3.8% of the activity budget, occurred during the hottest times of the day, and was characterized by being mainly social, involving partners of different ages, and sometimes different species. We found no differences in playing time between wild and supplemented groups. The lion tamarins played less in 'dangerous' substrates (canopy branches and forest floor), and more in 'safe' substrates (large branches and vine tangles), and favored playing in the center of the group over the periphery. The reproductive animals were vigilant during 78% of the time the infants were playing, and were mostly oriented away from the playing animals. The observed organization of play behavior suggests that juvenile GLTs minimize the risk of predation and accidental injuries, but do not seem to minimize energy expenditure and the risks of social injuries. The social-cognitive benefits acquired from experience of older partners during play may overcome the costs of the latter behavior, and because little time was spent in play, the energetic costs may be inconsequential. C1 Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, CBB, BR-28015620 Campos Dos Goytacazes, RJ, Brazil. Univ Sao Paulo, Dept Psicobiol, BR-14049 Ribeirao Preto, Brazil. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Ruiz-Miranda, CR (reprint author), Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, CBB, Av Alberto Lamego 2000, BR-28015620 Campos Dos Goytacazes, RJ, Brazil. 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 85 TC 17 Z9 17 U1 6 U2 49 PU BLACKWELL VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0179-1613 J9 ETHOLOGY JI Ethology PD JUL PY 2003 VL 109 IS 7 BP 593 EP 612 DI 10.1046/j.1439-0310.2003.00901.x PG 20 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 697TK UT WOS:000183959200005 ER PT J AU Dudar, JC Waye, JS Saunders, SR AF Dudar, JC Waye, JS Saunders, SR TI Determination of a kinship system using ancient DNA, mortuary practice, and historic records in an Upper Canadian pioneer cemetery SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE ancient DNA; kinship system; mortuary practice; historic cemetery; Upper Canadian history ID TANDEM REPEAT LOCI; 19TH-CENTURY CANADA; SKELETAL REMAINS; STR LOCI; POPULATION; IDENTIFICATION; AMPLIFICATION; PATTERNS; FAMILY; BONE AB Recovered and amplified ancient DNA (aDNA), from a historically documented 19th century Upper Canadian pioneer cemetery produced genotypes that were used to infer a past societal kinship system. While the results from multiplex short tandem repeat (STR) amplifications showed an unreliable polymerase chain reaction (PCR) product, a single locus HUMTH01 analysis yielded reproducible data and an allelic frequency pattern not statistically different from modern populations. Mitochondrial (mt) DNA HVR II data showed that a combined cemetery database exhibited reduced haplotype diversity indicators, as well as clusters of probable maternally related burials, The chronological persistence and replacement of mtDNA clusters approximately every two generations suggests a patrilineal/patrilocal kinship structure from a virilocal burial program for the Harmony Road cemetery. Through the integration of the aDNA analysis with archaeological material culture, historic records, and other ethnohistoric sources of information, this conclusion is supported. In this study persisting patrilineally inherited surnames act as a surrogate for aDNA Y-chromosome haplotype analysis. These results suggest that aDNA applications on aggregate skeletal collections where sparse, or no ethnological or historical documentation exists, may result in incorrect population history inferences if the presence of a kinship interment bias is not considered. Copyright (C) 2003 John Wiley Sons, Ltd. C1 Natl Museum Nat Hist, Smithsonian Inst, Repatriat Off, Washington, DC USA. McMaster Univ, Dept Pathol & Mol Med, Hamilton, ON, Canada. McMaster Univ, Dept Anthropol, Hamilton, ON, Canada. RP Dudar, JC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Repatriat Off, POB 37012,MRC 138, Washington, DC USA. NR 68 TC 15 Z9 16 U1 0 U2 10 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD JUL-AUG PY 2003 VL 13 IS 4 BP 232 EP 246 DI 10.1002/oa.680 PG 15 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 713BT UT WOS:000184836100006 ER PT J AU Cabrera-Asencio, I Santiago-Blay, JA Velez, AL AF Cabrera-Asencio, I Santiago-Blay, JA Velez, AL TI Epitragus aurulentus (Kirsch) (Coleoptera : Tenebrionidae): A new record and report for Puerto Rico SO JOURNAL OF AGRICULTURE OF THE UNIVERSITY OF PUERTO RICO LA English DT Article C1 Dept Crop Protect, Juana Diaz, PR 00795 USA. Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA. Natl Museum Nat Hist, Dept Systemat Biol Entomol, Smithsonian Inst, Washington, DC 20013 USA. Univ Puerto Rico, Coll Agr Sci, Agr Expt Stn, Rio Piedras, PR 00928 USA. RP Cabrera-Asencio, I (reprint author), Dept Crop Protect, HC-04,Box 7115, Juana Diaz, PR 00795 USA. NR 15 TC 0 Z9 0 U1 1 U2 1 PU COLL AGRICULTURAL SCI, AGRICULTURAL EXPERIMENT STN PI RIO PIEDRAS PA UNIV PUERTO RICO, MAYAGUEZ CAMPUS, RIO PIEDRAS, PR 00928 USA SN 0041-994X J9 J AGR U PUERTO RICO JI J. Agric. Univ. P. R. PD JUL-OCT PY 2003 VL 87 IS 3-4 BP 161 EP 164 PG 4 WC Agriculture, Multidisciplinary SC Agriculture GA 875UB UT WOS:000225446200008 ER PT J AU Piperno, DR AF Piperno, DR TI A few kernels short of a cob: on the Staller and Thompson late entry scenario for the introduction of maize into northern South America SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Zea mays; Ecuador; phytolith analysis; multiproxy data collection ID ARCHAEOLOGICAL SITE; TROPICAL FOREST; COASTAL ECUADOR; AGRICULTURE; ANCIENT; EVOLUTION; AMAZON; DOMESTICATION; PHYTOLITHS; LOWLANDS AB In recent JAS articles, Staller and Thompson (J. Archaeol. Sci. 29 (2002) 33) and Staller (2002) claim that phytoliths recovered in food residues from the Late Valdivia site of La Emerenciana represent the earliest remains of maize in Ecuador. These authors also dispute the utility of a technique developed by Pearsall and this author which identifies the remains of vegetative structures of maize retrieved from archaeological and paleoecological sediments. Staller and Thompson, in arguing that maize phytoliths occur only in the latest sherds recovered from La Emerenciana, ignore evidence strongly suggesting that maize is also present in the earliest ceramics at the site, despite the very small sample of pottery sherds from this time period that was analyzed. Their criticisms of the corpus of evidence identifying maize use during the late preceramic and early ceramic periods in northern South America, remains of which age they did not study, are based on inaccurate depictions of the methodology and interpretations relating to these accumulated data, and on unsupported assumptions concerning the integrity of this well-dated, multiproxy collection of information. (C) 2003 Elsevier Science Ltd. All rights reserved. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Smithsonian Trop Res Inst, Unit 0948, Balboa, Panama. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 41 TC 12 Z9 13 U1 0 U2 5 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 JUL PY 2003 VL 30 IS 7 BP 831 EP 836 DI 10.1016/S0305-4403(02)00255-8 PG 6 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 682LB UT WOS:000183092200004 ER PT J AU Puyravaud, JP Dufour, C Aravajy, S AF Puyravaud, JP Dufour, C Aravajy, S TI Rain forest expansion mediated by successional processes in vegetation thickets in the Western Ghats of India SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE rainforest; disturbance; succession; India; thickets; nestedness ID SOUTHERN INDIA; SAVANNA; REGENERATION; MANAGEMENT; DISPERSAL; DYNAMICS; PATTERNS; SUBSETS; HABITAT; MATTER AB Aim The objective of this study was to document succession from grassland thickets to rain forest, and to provide evidence for their potential as restoration tools. Location The Linganamakki region (State of Karnataka) of the Central Western Ghats of India. Method We selected thirty vegetation thickets ranging from 4 to 439 m(2) in area in the vicinity of rain forest. The area of each small thicket was estimated as an oval using its maximum length and its maximum width. When the shape was irregular (mostly in large thickets) the limits of the thicket were mapped and the area calculated from the map. Plant species were identified, the number of individuals was estimated and their heights measured. Results There was a progression in the thickets from early to late successional species. Small thickets were characterized by ecotone species and savanna trees such as Catunaregam dumetorum . Savanna trees served as a nucleus for thicket formation. Colonizing species were mostly bird-dispersed. As succession proceeded in larger thickets, the proportion of evergreen, late-successional rain forest trees increased. The species composition of the large thickets differed depending on the species composition of reproductive adults in the nearby forested areas. The species within small thickets were also found in the large thickets. The nestedness in species composition suggested that species turnover was deterministic based on thicket size. Human disturbance (leaf and wood collection by the local populations) affected the species composition and the species-area relationship of thickets. Main conclusions Vegetation thickets are nodal centres for rain forest colonization within grasslands. They expand and replace savanna. Early successional bird-dispersed species established around savanna trees followed by late-successional rain forest trees dispersed from the nearby forest by birds. Restoration programmes that reproduce natural successional processes such as those observed in thickets will be more successful and less expensive than the methods currently being employed, where trees are individually planted in grassland. Wood harvesting is the only factor that prevents thicket growth and coalescence and hampers forest expansion. C1 French Inst Pondicherry, Pondicherry, India. RP Puyravaud, JP (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. EM puyravaudj@tivoli.si.edu NR 59 TC 32 Z9 32 U1 2 U2 9 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD JUL PY 2003 VL 30 IS 7 BP 1067 EP 1080 PG 14 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 694DT UT WOS:000183759100009 ER PT J AU Swider, JR Hackley, VA Winter, J AF Swider, JR Hackley, VA Winter, J TI Characterization of Chinese ink in size and surface SO JOURNAL OF CULTURAL HERITAGE LA English DT Article DE soot; animal glue; sol; electrophoresis; scanning electron microscopy (SEM); photon correlation spectroscopy (PCS); laser Doppler electrophoresis (LDE); isoelectric point (IEP) ID CARBON; SOOT AB Chinese ink, a mixture of soot and animal glue, has been used in East Asia for centuries as the sole black paint of choice. The combination of animal glue and soot particles create a distinctive dispersion system giving Chinese ink its unique properties among paints and inks. Photon correlation spectroscopy (PCS) size measurements and scanning electron microscopy (SEM) imaging revealed subtle differences in particle size and aggregation among inks of different soot origin. Surface chemistry of the particles was examined using laser Doppler electrophoresis (LDE) for determination of the isoelectric point (IEP). The IEPs of different inks were not distinct, but reflected the presence of the collagen-based glue on the particles' surface. The IEP and size dropped significantly when inks were treated with collagenase and when soot and carbon blacks alone were measured, pointing to the important role of animal glue in this dispersion system. (C) 2003 Editions scientifiques et medicales Elsevier SAS. All rights reserved. C1 Smithsonian Inst, Freer Gallery Art, Dept Conservat & Sci Res, Washington, DC 20560 USA. Smithsonian Inst, Arthur M Sackler Gallery, Dept Conservat & Sci Res, Washington, DC 20560 USA. NIST, Mat Sci & Engn Lab, Gaithersburg, MD 20899 USA. RP Swider, JR (reprint author), Smithsonian Inst, Freer Gallery Art, Dept Conservat & Sci Res, Washington, DC 20560 USA. EM joseph.swider@asia.si.edu OI Hackley, Vincent/0000-0003-4166-2724 NR 33 TC 15 Z9 15 U1 5 U2 22 PU EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1296-2074 J9 J CULT HERIT JI J. Cult. Herit. PD JUL-SEP PY 2003 VL 4 IS 3 BP 175 EP 186 DI 10.1016/S1296-2074(03)00044-X PG 12 WC Archaeology; Art; Chemistry, Analytical; Geosciences, Multidisciplinary; Materials Science, Multidisciplinary; Spectroscopy SC Archaeology; Art; Chemistry; Geology; Materials Science; Spectroscopy GA 738NF UT WOS:000186294200003 ER PT J AU Jordan, TE Whigham, DF Hofmockel, KH Pittek, MA AF Jordan, TE Whigham, DF Hofmockel, KH Pittek, MA TI Nutrient and sediment removal by a restored wetland receiving agricultural runoff SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article ID PARTIALLY STRATIFIED ESTUARY; SMALL CONSTRUCTED WETLANDS; NONPOINT-SOURCE POLLUTION; CHESAPEAKE BAY; COASTAL-PLAIN; PHOSPHORUS RETENTION; REDUCING NITROGEN; TILE DRAINAGE; WATER-QUALITY; PHYTOPLANKTON AB Few studies have measured removal of pollutants by restored wetlands that receive highly variable inflows. We used automated flow-proportional sampling to monitor the removal of nutrients and sus? ended solids by a 1.3-ha restored wetland receiving unregulated inflows from a 14-ha agricultural watershed in Maryland, USA. Water entered the wetland mainly in brief pulses of runoff, which sometimes exceeded the 2500-m(3) water holding capacity of the wetland. Half of the total water inflow occurred in only 24 days scattered throughout the two-year study. Measured annual water gains were within 5% of balancing water losses. Annual removal of nutrients differed greatly between the two years of the study. The most removal occurred in the first year, which included a three-month period of decreasing water level in the wetland. In that year, the wetland removed 59% of the total P, 38% of the total N, and 41% of the total organic C it received. However, in the second year, which lacked a drying period, there was no significant (p > 0.05) net removal of total N or P, although 30% of the total organic C input was removed. For the entire two-year period, the wetland removed 25% of the ammonium, 52% of the nitrate, and 34% of the organic C it received, but there was no significant net removal of total suspended solids (TSS) or other forms of N and P. Although the variability of inflow may have decreased the capacity of the wetland to remove materials, the wetland still reduced nonpoint-source pollution. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Duke Univ, Dept Biol, Durham, NC 27708 USA. Univ Maryland, Dept Biol Resources Engn, College Pk, MD 20742 USA. RP Jordan, TE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM jordanth@si.edu OI Whigham, Dennis/0000-0003-1488-820X NR 62 TC 104 Z9 115 U1 5 U2 66 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 USA SN 0047-2425 J9 J ENVIRON QUAL JI J. Environ. Qual. PD JUL-AUG PY 2003 VL 32 IS 4 BP 1534 EP 1547 PG 14 WC Environmental Sciences SC Environmental Sciences & Ecology GA 700EN UT WOS:000184099800042 PM 12931911 ER PT J AU Coxall, HK Huber, BT Pearson, PN AF Coxall, HK Huber, BT Pearson, PN TI Origin and morphology of the Eocene planktonic foraminifer Hantkenina SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID MOLECULAR EVIDENCE; EVOLUTION; STRATIGRAPHY; SPECIATION; TRENDS; OCEAN AB Study of the origin and early evolution of the tubulospine-bearing planktonic foraminiferal genus Hantkenina reveals that it evolved gradually from the clavate species Clavigerinella eocanica in the earliest middle Eocene and is unrelated to the genus Pseudohastigerina. Clavigerinella eocanica and the lower middle Eocene species Hantkenina nuttalli share many morphologic features and show similar developmental patterns but differ significantly in these aspects from P. micra. Rare, transitional Clavigerinella-Hantkenina forms from the Helvetikum section of Austria bridge the gap between clavate and tubulospinose morphologies, providing direct, stratigraphically-ordered evidence of the evolutionary transition between Hantkenina and Clavigerinella. Clavigerinellid ancestry is traced to a previously undescribed low-trochospiral species, Parasubbotina eoclava sp. nov., at Ocean Drilling Program Site 865. We speculate that Hantkenina originated through competition for limited food resources in a deep, oxygen-deficient habitat below the thermocline. The tubulospines may represent a structural adaptation to this new trophic strategy, allowing the organism to harvest a greater volume of water at minimal metabolic cost. The abrupt occurrence of Hantkenina in pelagic sediment cores from the central Pacific and other regions of the world ocean may represent immigration into these areas following speciation within the hydrographically evolving Tethys Seaway. Alternatively, cladogenesis may have occurred over a wider area, but due to a contemporaneous global hiatus the fossil record of this bioevent is poorly preserved. C1 Sch Ocean & Earth Sci, Southampton Oceanog Ctr, Southampton SO14 3ZH, Hants, England. Smithsonian Inst, Natl Museum Nat Hist, MRC 121, Dept Paleobiol, Washington, DC 20560 USA. Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. RP Coxall, HK (reprint author), Sch Ocean & Earth Sci, Southampton Oceanog Ctr, European Way, Southampton SO14 3ZH, Hants, England. RI Pearson, Paul/B-2276-2009 OI Pearson, Paul/0000-0003-4628-9818 NR 88 TC 13 Z9 15 U1 0 U2 3 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD JUL PY 2003 VL 33 IS 3 BP 237 EP 261 DI 10.2113/33.3.237 PG 25 WC Paleontology SC Paleontology GA 723GH UT WOS:000185424000005 ER PT J AU Ceruzzi, PE AF Ceruzzi, PE TI Strategic computing: DARPA and the quest for machine intelligence, 1983-1993. SO JOURNAL OF MILITARY HISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Ceruzzi, PE (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC MILITARY HISTORY PI LEXINGTON PA C/O VIRGINIA MILITARY INST, GEORGE C MARSHALL LIBRARY, LEXINGTON, VA 24450-1600 USA SN 0899-3718 J9 J MILITARY HIST JI J. Mil. Hist. PD JUL PY 2003 VL 67 IS 3 BP 994 EP 996 DI 10.1353/jmh.2003.0207 PG 3 WC History SC History GA 697CU UT WOS:000183925300065 ER PT J AU Zu, L Hamilton, PA Chance, KV Davies, PB AF Zu, L Hamilton, PA Chance, KV Davies, PB TI Pressure broadening of the lowest rotational transition of (HCl)-Cl-35 by N-2 and O-2 SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID HCL; SPECTRUM; LINE AB The nitrogen and oxygen pressure broadening coefficients of the J = 1 <-- 0 transition of (HCl)-Cl-35 at 626 GHz (21 cm(-1)) have been measured using a high resolution tunable far infrared sideband spectrometer. The profiles of the three Cl-35 hyperfine components of the transition were separately fitted to Voigt line shapes and the Lorentzian widths determined over a range of broadening gas pressures up to 1.1 Torr for nitrogen and 1 Torr for oxygen. The room temperature pressure broadening coefficient for nitrogen was derived as 3.46(6) MHz/Torr and for oxygen as 2.70(5) MHz/Torr. (C) 2003 Elsevier Science (USA). All rights reserved. C1 Univ Cambridge, Dept Chem, Cambridge CB2 1EW, England. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Ohio State Univ, Dept Chem, 100 W 8th Av, Columbus, OH 43210 USA. EM pbd2@cus.cam.ac.uk OI Chance, Kelly/0000-0002-7339-7577 NR 14 TC 3 Z9 3 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD JUL PY 2003 VL 220 IS 1 BP 107 EP 112 DI 10.1016/S0022-2852(03)00096-1 PG 6 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 699VM UT WOS:000184076700011 ER PT J AU Mendoza, DT Gonzalez, LDU Ortega-Barria, E Capson, TL Rios, LC AF Mendoza, DT Gonzalez, LDU Ortega-Barria, E Capson, TL Rios, LC TI Five new cassane diterpenes from Myrospermum frutescens with activity against Trypanosoma cruzi SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID DERIVATIVES; ACID AB Five novel cassane diterpenes (1-5) with activity against Trypanosoma cruzi were isolated from leaves of Myrospermum frutescens. The structures were determined as 18-hydroxycassan-13,15-diene (1), 6beta,18-dihydroxycassan-13,15-diene (2), 6beta-hydroxy-18-acetoxycassan-13,15-diene (3),18-acetoxy-13,15-diene-19-cassanoic acid (4), and 6beta,13beta-dihydroxy-18-acetoxycassan-14(17),15-diene (5). Structures were elucidated by spectroscopic analysis (NMR and HRCIMS) and by the synthesis of derivatives 2a and 2b. Compounds 3 and 5 were more active against the extracellular form of the parasite (11 and 16 muM, respectively) than the intracellular forms, while compounds 1 and 2 were more active against the more clinically relevant intracellular forms of the parasite (17 muM). Compounds 1 and 2 were approximately 9-fold more toxic toward T. cruzi than toward human fibroblasts, the cell type that serves as the parasite's mammalian host cell. C1 Univ Panama, Fac Nat & Exact Sci & Technol, Lab Nat Prod, Panama City, Panama. Florida State Univ, Inst Trop Med & Hlth Sci, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. RP Rios, LC (reprint author), Univ Panama, Fac Nat & Exact Sci & Technol, Lab Nat Prod, Apartado 0824, Panama City, Panama. EM lucr@ancon.up.ac.pa OI Torres-Mendoza, Daniel/0000-0002-3540-4238 NR 15 TC 18 Z9 19 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD JUL PY 2003 VL 66 IS 7 BP 928 EP 932 DI 10.1021/np030010o PG 5 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 705UE UT WOS:000184412800005 PM 12880308 ER PT J AU Pojeta, J Eernisse, DJ Hoare, RD Henderson, MD AF Pojeta, J Eernisse, DJ Hoare, RD Henderson, MD TI Echinochiton dufoei: A new spiny Ordovician chiton SO JOURNAL OF PALEONTOLOGY LA English DT Article ID WIWAXIA-CORRUGATA MATTHEW; BURGESS SHALE; MOLLUSK; FOSSIL AB Echinochiton dufoei new genus and species is described from the Ordovician age Forreston Member, Grand Detour Formation (Blackriveran) near Beloit, Wisconsin. For a variety of reasons, we regard E. dufoei as a chiton; the species is known from four articulated or partially articulated specimens, one of which has eight plates and two of which have a mucro on the tail plate. Echinochiton dufoei differs from other chitons in having large hollow spines that project from each of the known plates. In plate shape and position, E. dufoei is much like the Upper Cambrian species Matthevia variabilis Walcott, 1885, and the Lower Ordovician species Chelodes whitehousei Runnegar, Pojeta, Taylor, and Collins (1979). C1 Smithsonian Inst, Museum Hist Nat, US Geol Survey, Washington, DC 20560 USA. Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92834 USA. Bowling Green State Univ, Dept Geol, Bowling Green, OH 43403 USA. Burpee Museum Nat Hist, Rockford, IL 61103 USA. RP Pojeta, J (reprint author), Smithsonian Inst, Museum Hist Nat, US Geol Survey, Washington, DC 20560 USA. RI Eernisse, Douglas/B-5016-2011 NR 20 TC 21 Z9 24 U1 0 U2 1 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 2003 VL 77 IS 4 BP 646 EP 654 DI 10.1666/0022-3360(2003)077<0646:EDANSO>2.0.CO;2 PG 9 WC Paleontology SC Paleontology GA 704RZ UT WOS:000184354900003 ER PT J AU Rogalla, NS Carter, JG Pojeta, J AF Rogalla, NS Carter, JG Pojeta, J TI Shell microstructure of the Late Carboniferous rostroconch mollusc Apotocardium lanterna (Branson, 1965) SO JOURNAL OF PALEONTOLOGY LA English DT Article ID CAMBRIAN MOLLUSKS; BIVALVIA; ORIGIN; WATSONELLA; EVOLUTION AB The Late Carboniferous bransoniid conocardioidean Apotocardium lanterna (Branson, 1965) had an entirely aragonitic shell with a finely prismatic outer shell layer, a predominantly crossed lamellar to complex crossed lamellar middle shell layer, and an "inner" shell layer of finely textured porcelaneous and/or matted structure. This "inner" layer is probably homologous with the inner part of the middle shell layer and the inner layer sensu stricto of bivalved molluscs. Shell morphological and microstructural convergences between conocardioids and living heart cockles suggest that at least some conocardioids may have farmed algal endosymbionts in their posterior mantle margins. This symbiosis may have helped conocardioids compete with the biomechanically more efficient bivalves during the latter part of the Paleozoic. C1 Univ Marburg, Inst Geol & Palaeontol, D-35032 Marburg, Germany. Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA. Smithsonian Inst, Natl Museum Nat Hist, US Geol Survey, Washington, DC 20013 USA. RP Rogalla, NS (reprint author), Univ Marburg, Inst Geol & Palaeontol, Hans Meerwein Str, D-35032 Marburg, Germany. NR 52 TC 8 Z9 8 U1 0 U2 4 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 2003 VL 77 IS 4 BP 655 EP 673 DI 10.1666/0022-3360(2003)077<0655:SMOTLC>2.0.CO;2 PG 19 WC Paleontology SC Paleontology GA 704RZ UT WOS:000184354900004 ER PT J AU Emmons, LH Dubois, MA AF Emmons, LH Dubois, MA TI Leaf-area index change across river-beach successional transects in south-eastern Peru SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE ecotone; Leaf Area Index; Peru; plant succession; rain forest ID FOREST/ C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. CEA Saclay, Serv Phys Etat Condense, F-91191 Gif Sur Yvette, France. RP Emmons, LH (reprint author), Smithsonian Inst, Dept Systemat Biol, NHB 390,MRC 108,POB 37012, Washington, DC 20013 USA. NR 12 TC 5 Z9 6 U1 0 U2 3 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JUL PY 2003 VL 19 BP 473 EP 477 DI 10.1017/S0266467403003523 PN 4 PG 5 WC Ecology SC Environmental Sciences & Ecology GA 709WZ UT WOS:000184650700013 ER PT J AU Way, T AF Way, T TI Grounds for pleasure: Four centuries of the American garden SO LANDSCAPE ARCHITECTURE LA English DT Book Review C1 Cornell Univ, Ithaca, NY 14853 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Way, T (reprint author), Cornell Univ, Ithaca, NY 14853 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC LANDSCAPE ARCHITECTS PI WASHINGTON PA 636 EYE ST, NW, WASHINGTON, DC 20001-3736 USA SN 0023-8031 J9 LANDSCAPE ARCHIT JI Landsc. Archit. PD JUL PY 2003 VL 93 IS 7 BP 96 EP 96 PG 1 WC Architecture SC Architecture GA 692JX UT WOS:000183658900019 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Il Gigante: Michelangelo, Florence, and the David, 1492-1504. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUL PY 2003 VL 128 IS 12 BP 75 EP 76 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 696VL UT WOS:000183908200051 ER PT J AU Schroll, S AF Schroll, S TI John Currin. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUL PY 2003 VL 128 IS 12 BP 75 EP 75 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 696VL UT WOS:000183908200049 ER PT J AU Reimold, WU Koeberl, C Hough, RM McDonald, I Bevan, A Amare, K French, BM AF Reimold, WU Koeberl, C Hough, RM McDonald, I Bevan, A Amare, K French, BM TI Woodleigh impact structure, Australia: Shock petrography and geochemical studies SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID PLATINUM-GROUP ELEMENTS; SOUTHERN CARNARVON BASIN; SMALL SAMPLE ANALYSIS; LATE DEVONIAN AGE; MORY,A.J. ET-AL.; K-AR EVIDENCE; WESTERN-AUSTRALIA; SUEVITE BRECCIA; ILLITIC CLAYS; CRATER AB The large, complex Woodleigh structure in the Carnarvon basin of Western Australia has recently been added to the terrestrial impact crater record. Many aspects of this structure are, however, still uncertain. This work provides a detailed petrographic assessment of a suite of representative drill core samples from the borehole Woodleigh I that penetrated uplifted basement rocks of the central part of this structure. Fundamental rock and mineral deformation data and high-precision chemical data, including results of PGE and oxygen isotopic analysis, are presented. The sampled interval displays likely impact-produced macrodeformation in the form of fracturing and breccia veining at the microscopic scale. Contrary to earlier reports that these breccias represent pseudotachylite (friction melt) or even shock/shear-produced pseudotachylitic melt breccia cannot be confirmed due to pervasive post-impact alteration. Abundant planar deformation features (PDFs) in quartz, in addition to diaplectic glass and partial isotropization, are the main shock deformation effects observed, confirming that Woodleigh is of impact origin. Over the investigated depth interval, the statistics of quartz grains with a variable number of sets of PDFs does not change significantly, and the patterns of crystallographic orientations of PDFs in randomly selected quartz grains does not indicate a change in absolute shock pressure with depth either. The value of oxygen isotopes for the recognition of meteoritic contamination, as proposed by earlier Woodleigh workers, is critically assessed. Neither INA nor PGE analyses of our samples support the presence of a meteoritic component within this basement section, as had been claimed in earlier work. C1 Univ Witwatersrand, Sch Geosci, Impact Cratering Res Grp, Johannesburg, South Africa. Univ Vienna, Dept Geosci, A-1090 Vienna, Austria. Western Australian Museum, Dept Earth & Planetary Sci, Perth, WA, Australia. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. Cardiff Univ, Dept Earth Sci, Cardiff CF10 3YE, S Glam, Wales. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Reimold, WU (reprint author), Univ Witwatersrand, Sch Geosci, Impact Cratering Res Grp, POB 2050, Johannesburg, South Africa. OI McDonald, Iain/0000-0001-9066-7244 NR 53 TC 15 Z9 16 U1 1 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2003 VL 38 IS 7 BP 1109 EP 1130 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 738UJ UT WOS:000186306000011 ER PT J AU Weldon, PJ Aldrich, JR Klun, JA Oliver, JE Debboun, M AF Weldon, PJ Aldrich, JR Klun, JA Oliver, JE Debboun, M TI Benzoquinones from millipedes deter mosquitoes and elicit self-anointing in capuchin monkeys (Cebus spp.) SO NATURWISSENSCHAFTEN LA English DT Article ID INSECTS AB Neotropical monkeys of the genus Cebus anoint themselves by rubbing arthropods and plants against their pelage. A recent study has shown that free-ranging wedge-capped capuchin monkeys (C. olivaceus) in Venezuela self-anoint with a benzoquinone-secreting millipede, an activity by which they are hypothesized to appropriate chemical deterrents of mosquitoes. To evaluate the plausibility of this hypothesis, female yellow fever mosquitoes (Aedes aegypti) were presented with two millipede secretory compounds, 2-methyl-1,4-benzoquinone and 2-methoxy-3-methyl-1,4-benzoquinone, on nylon-reinforced silicone membranes placed over wells filled with human blood, a highly preferred food. Mosquitoes exhibited fewer landings, fed less frequently, and flew more frequently (a possible indication of repellency) in the presence of membranes treated with benzoquinones than with controls. These compounds also elicit self-anointing in captive male and female tufted (C. apella) and white-faced (C. capucinus) capuchin monkeys. C1 ARS, Chem Affecting Insect Behav Lab, USDA, Beltsville, MD 20705 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. Walter Reed Army Med Ctr, Walter Reed Army Inst Res, Dept Entomol, Div Communicable Dis & Immunol, Washington, DC 20307 USA. RP Aldrich, JR (reprint author), ARS, Chem Affecting Insect Behav Lab, USDA, Beltsville, MD 20705 USA. NR 25 TC 39 Z9 41 U1 0 U2 14 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD JUL PY 2003 VL 90 IS 7 BP 301 EP 304 DI 10.1007/s00114-003-0427-2 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 703UC UT WOS:000184298500002 PM 12883771 ER PT J AU Nagamine, K Loeb, A AF Nagamine, K Loeb, A TI Future evolution of nearby large-scale structures in a universe dominated by a cosmological constant SO NEW ASTRONOMY LA English DT Article DE cosmology : theory; large-scale structure of Universe; Local Group; methods : numerical ID PECULIAR VELOCITY ANALYSIS; GALAXY REDSHIFT SURVEY; DISTANCE DATA; LOCAL GROUP; MASS; HALO; SPECTROSCOPY; CALIBRATION; SIMULATIONS; ANISOTROPY AB We simulate the future evolution of the observed inhomogeneities in the local universe assuming that the global expansion rate is dominated by a cosmological constant. We find that within two Hubble times (similar to30 billion years) from the present epoch, large-scale structures will freeze in co-moving coordinates and the mass distribution of bound objects will stop evolving. The Local Group will get somewhat closer to the Virgo cluster in co-moving coordinates, but will be pulled away from the Virgo in physical coordinates due to the accelerated expansion of the Universe. In the distant future there will only be one massive galaxy within our event horizon, namely the merger product of the Andromeda and the Milky Way galaxies. All galaxies that are not gravitationally bound to the Local Group will recede away from us and eventually exit from our event horizon. More generally, we identify the critical interior overdensity above which a shell of matter around an object will remain bound to it at late times. (C) 2003 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nagamine, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM knagamin@cfa.harvard.edu; aloeb@cfa.harvard.edu NR 36 TC 50 Z9 50 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1076 EI 1384-1092 J9 NEW ASTRON JI New Astron. PD JUL PY 2003 VL 8 IS 5 BP 439 EP 448 DI 10.1016/S1384-1076(02)00234-8 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710CD UT WOS:000184662500006 ER PT J AU Dalal, N Kochanek, CS AF Dalal, N Kochanek, CS TI Detection of CDM substructure SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Article; Proceedings Paper CT 5th International UCLA Symposium on Sources and Detection of Dark Matter and Dark Energy in the Universe CY FEB 20-22, 2002 CL MARINA DEL REY, CALIFORNIA ID DARK-MATTER SUBSTRUCTURE; GALACTIC SATELLITES; GALAXIES; MODELS; POWER; LENS AB The properties of multiple image gravitational lenses require a fractional surface mass density in satellites of f(sat) = 0.02 (0.006 less than or similar to f(sat) less than or similar to 0.07 at 90% confidence) that is consistent with the expectations for CDM. The characteristic satellite mass scale, 10(6)-10(9) M-circle dot, is also consistent with the expectations for CDM. The agreement between the observed and expected density of CDM substructure supports the basic CDM paradigm, and disfavors modifications to the CDM theory such as self-interacting dark matter or a warm dark matter component. C1 Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA. RP Dalal, N (reprint author), Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD JUL PY 2003 VL 124 BP 144 EP 147 DI 10.1016/S0920-5632(03)02094-2 PG 4 WC Physics, Particles & Fields SC Physics GA 703UE UT WOS:000184298700025 ER PT J AU Lopez, OR Kursar, TA AF Lopez, OR Kursar, TA TI Does flood tolerance explain tree species distribution in tropical seasonally flooded habitats? SO OECOLOGIA LA English DT Article DE Panama; root growth; seasonality; stomatal conductance; swamps ID NEOTROPICAL FOREST; CENTRAL AMAZONIA; VARZEA FORESTS; RAIN-FORESTS; GROWTH; DROUGHT; RESPONSES; SEEDLINGS; PATTERNS; STRESS AB In the tropics, seasonally flooded forests (SFF) harbor fewer tree species than terra firme (i.e. non-flooded) forests. The low species diversity of tropical flooded forests has been ascribed to the paucity of species with adaptations to tolerate flooding. To test the hypothesis that flooding is the only factor restricting most species from SFF, we compared plant morphological and physiological responses to flooding in 2-month old seedlings of 6 species common to SFF and 12 species common to terra firme forests. Although flooding impaired growth, total biomass, maximum root length and stomatal conductance in most species, responses varied greatly and were species-specific. For example, after 90 days, flooding reduced leaf area growth by 10-50% in all species, except in Tabebuia, a common species from non-flooded habitats. Similarly, flooding had a 5-45% negative effect on total biomass for all species, except in 1 SFF and 1 terra firme species both of which had more biomass under flooding. A principal component analysis, using the above responses to flooding, provided no evidence that SFF and terra firme species differed in their responses to flooding. Flooding also caused reductions in root growth for most species. Rooting depth and root: shoot ratios were significantly less affected by flooding in SFF than in terra firme species. Although flood tolerance is critical for survival in flooded habitats, we hypothesize that responses to post-flooding events such as drought might be equally important in seasonal habitats. Therefore, we suggest that the ability to grow roots under anoxia might be critical in predicting success in inundated habitats that also experience a strong dry season. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Lopez, OR (reprint author), Univ Wisconsin, Dept Bot, 430 Lincoln Dr, Madison, WI 53706 USA. NR 57 TC 35 Z9 37 U1 0 U2 19 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUL PY 2003 VL 136 IS 2 BP 193 EP 204 DI 10.1007/s00442-003-1259-7 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 700BJ UT WOS:000184092500004 PM 12743794 ER PT J AU Harrington, GJ AF Harrington, GJ TI Wasatchian (Early Eocene) pollen floras from the Red Hot Truck Stop, Mississippi, USA SO PALAEONTOLOGY LA English DT Article DE Red Hot Truck Stop; US Gulf Coast; palynology; Palaeocene; Eocene ID PALEOCENE THERMAL MAXIMUM; NORTH-AMERICA; BIGHORN BASIN; MARINE; DIVERSITY; EVOLUTION; TERRESTRIAL; BOUNDARY; TURNOVER; RECORDS AB Sediments at the Red Hot Truck Stop (RUTS), Mississippi, USA are important because they contain the lowest latitude record of both the earliest known Eocene plant and mammal fossils in North America. The RHTS contains the uppermost Tuscahoma Formation and the lowermost part of the basal Bashi and Hatchetigbee formations. The Tuscahoma Formation is composed of glauconitic sands and silts that represent estuarine to shallow marine sediments. Faunal remains indicate that the RHTS section belongs to the Wasatchian North American land mammal age and specifically to the lower Graybullian subdivision. Pollen and spore floras from the RHTS are moderately diverse (113 taxa) and contain families that today are associated with warm-adapted vegetation types such as Annonaceae, Bombacaceae, Burseraceae and palms. Eocene first occurrences are represented by Brosipollis sp., Celtispollenites sp., Interpollis microsupplingensis, cf. Nuxpollenites psilatus, Platycarya spp., Retistephanocolporites sp. and Symplocos? contracta and by one genus of pteridophyte spore (Granulatisporites sp.). The overall composition and within-sample diversity of the sporomorph flora is more similar to the Hatchetigbee Formation (early Eocene) than to the middle Tuscahoma Formation (late Palaeocene) but among-sample diversity remains unchanged across the Palaeocene/Eocene boundary. The distinct composition of the RUTS demonstrates that floral change across the Palaeocene/Eocene boundary is complex and composed of several phases of floral change. C1 Univ Coll Cork, Dept Geol, Cork, Ireland. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Harrington, GJ (reprint author), Univ Coll Cork, Dept Geol, Cork, Ireland. NR 60 TC 21 Z9 21 U1 0 U2 3 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0031-0239 J9 PALAEONTOLOGY JI Paleontology PD JUL PY 2003 VL 46 BP 725 EP 738 DI 10.1111/1475-4983.00318 PN 4 PG 14 WC Paleontology SC Paleontology GA 705NK UT WOS:000184401000006 ER PT J AU Krems, RV Dalgarno, A AF Krems, RV Dalgarno, A TI Disalignment transitions in cold collisions of P-3 atoms with structureless targets in a magnetic field SO PHYSICAL REVIEW A LA English DT Article ID FINE-STRUCTURE TRANSITIONS; LOWEST EXCITED-STATES; LOG-DERIVATIVE METHOD; EXCITATION TRANSFER; CROSS-SECTIONS; NE-ASTERISK(2P(5)3P)+HE COLLISIONS; INTRAMULTIPLET TRANSITIONS; SCATTERING; HE; RELAXATION AB A method for quantum-mechanical calculations of cross sections for the Zeeman transitions in collisions of P-3 atoms with structureless targets in a magnetic field is presented and applied to the study of magnetic and electronic relaxation in oxygen-helium and carbon-helium collisions at cold and ultracold temperatures. The rate constants for collisionally induced transitions between Zeeman levels in ground-state oxygen have large magnitudes in a 1 T field. It is shown that magnetic fields induce the forbidden P-3(1) --> P-3(0) transition in ultracold collisions of carbon with helium. The cross section vanishes at zero energy for field-free collisions, but becomes infinitely large in a finite magnetic field, varying with velocity v and magnetic field B as B-2/v. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Inst Theoret Atom & Mol & Opt Phys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, ITAMP, Inst Theoret Atom & Mol & Opt Phys, 60 Garden St, Cambridge, MA 02138 USA. EM rkrems@cfa.harvard.edu NR 50 TC 35 Z9 35 U1 1 U2 3 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 JUL PY 2003 VL 68 IS 1 AR 013406 DI 10.1103/PhysRevA.68.013406 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 708MP UT WOS:000184571600092 ER PT J AU Geller, MJ AF Geller, MJ TI Cloaks and kudos for PHYSICS TODAY'S portrayal of women SO PHYSICS TODAY LA English DT Letter C1 Smithsonian Astrophys Observ, Cambridge, MA USA. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 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 JUL PY 2003 VL 56 IS 7 BP 16 EP 17 DI 10.1063/1.1603062 PG 2 WC Physics, Multidisciplinary SC Physics GA 696WN UT WOS:000183910700012 ER PT J AU Tyree, MT Engelbrecht, BMJ Vargas, G Kursar, TA AF Tyree, MT Engelbrecht, BMJ Vargas, G Kursar, TA TI Desiccation tolerance of five tropical seedlings in Panama. Relationship to a field assessment of drought performance SO PLANT PHYSIOLOGY LA English DT Article ID 2 DESERT SUCCULENTS; HYDRAULIC CONDUCTANCE; MOIST FOREST; NEOTROPICAL TREE; WATER RELATIONS; RAIN-FOREST; ROOT; VULNERABILITY; ADAPTATION; SARAWAK AB Studies of the desiccation tolerance of the seedlings of five tropical trees were made on potted plants growing in a greenhouse. Pots were watered to field capacity and then dehydrated for 3 to 9 weeks to reach various visual wilting stages, from slightly wilted to dead. Saturated root hydraulic conductance was measured with a high-pressure flowmeter, and whole-stem hydraulic conductance was measured by a vacuum chamber method. Leaf punches (5.6-mm diameter) were harvested for measurement of leaf water potential by a thermocouple psychrometer method and for measurement of fresh and dry weight. In a parallel study, the same five species were studied in a field experiment in the understory of a tropical forest, where these species frequently germinate. Control seedlings were maintained in irrigated plots during a dry season, and experimental plants were grown in similar plots with rain exclusion shelters. Every 2 to 4 weeks, the seedlings were scored for wilt state and survivorship. After a 22-week drought, the dry plots were irrigated for several weeks to verify visual symptoms of death. The field trials were used to rank drought performance of species, and the greenhouse desiccation studies were used to determine the conditions of moribund plants. Our conclusion is that the desiccation tolerance of moribund plants correlated with field assessment of drought-performance for the five species (r(2) > 0.94). C1 ARS, USDA, Burlington, VT 05402 USA. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Tyree, MT (reprint author), ARS, USDA, POB 968, Burlington, VT 05402 USA. RI Engelbrecht, Bettina/E-9914-2012 NR 33 TC 65 Z9 76 U1 2 U2 38 PU AMER SOC PLANT BIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD JUL PY 2003 VL 132 IS 3 BP 1439 EP 1447 DI 10.1104/pp.102.018937 PG 9 WC Plant Sciences SC Plant Sciences GA 717FU UT WOS:000185076800035 PM 12857825 ER PT J AU Montenegro, H Guterrez, M Romero, LI Ortega-Barria, E Capson, TL Rios, LC AF Montenegro, H Guterrez, M Romero, LI Ortega-Barria, E Capson, TL Rios, LC TI Aporphine alkaloids from Guatteria spp. with leischmanicidal activity SO PLANTA MEDICA LA English DT Article ID IN-VITRO; ANNONACEAE AB Fractionation of Guatteria amplifolia yielded the alkaloids xylopine (1), nornuciferine (4), lysicamine (6), and laudanosine (5). Fractionation of Guatteria dumetorum yielded the alkaloids cryptodorine (2) and nornantenine (3). Compounds 1-4 demonstrated significant activity against Leishmania mexicana and L. panamensis. Xylopine (1) was among the most active compounds (LD50 = 3muM) and showed a 37-fold higher toxicity towards L. mexicana than macrophages, the regular host cells of Leishmania spp. C1 Univ Panama, Dept Quim Organ, Panama City, Panama. Florida State Univ, Inst Trop Med & Hlth Sci, Panama City, Panama. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Rios, LC (reprint author), Univ Panama, Dept Quim Organ, Apdo 0824-10835, Panama City, Panama. FU FIC NIH HHS [1U10 TW01021-01] NR 15 TC 45 Z9 51 U1 3 U2 15 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 J9 PLANTA MED JI Planta Med. PD JUL PY 2003 VL 69 IS 7 BP 677 EP 679 PG 3 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA 714AK UT WOS:000184890000018 PM 12898429 ER PT J AU Smith, DR Saini, MS AF Smith, DR Saini, MS TI A new species of Conaspidia Konow (Hymenoptera : Tenthredinidae) from India and review of the Indian species SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE India; Conaspidia; sawfly; Tenthredininae AB Conaspidia maculosa, new species, is described from Sikkim, India. It is the fourth species of this Asian genus known from India, the other species being C. dubiosa Forsius, C. fasciatipennis Turner, and C. sikkimensis Konow. The new species belongs in the scutellaris group of Conaspidia and is separated from related species in that group and the other Indian species. C1 ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. NR 5 TC 1 Z9 3 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2003 VL 105 IS 3 BP 555 EP 558 PG 4 WC Entomology SC Entomology GA 694CK UT WOS:000183756100005 ER PT J AU Brown, JW AF Brown, JW TI Three new genera, two new species, and some rectifications in neotropical Euliini (Lepidoptera : Tortricidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE genitalia; biodiversity; synonymy; new combinations; classification; Euryeulia; Pseudapina; Circapina; Pycnospina; Lobogenesis; Osmaria; Anopina; Chirotes; Prochirotes; Strophotina AB Three new genera in the tortricid tribe Euliini are described and illustrated: Euryeulia, with type species E. biocellata (Walsingham 1914), new combination, from Mexico; Pseudapina, with type species P. lanceovalva, new species, from Venezuela; and Circapina, with type species C flexalana, new species, from Costa Rica. Three new generic synonymies are proposed: Pycnospina Razowski 1997 is a junior synonym of Lobogenesis Razowski 1990, with the new combination L. centrota (Razowski 1997); Osmaria Razowski 1991 is a junior synonym of Anopina Obraztsov 1962, with the new combination A. psaeroptera (Razowski and Becker 1991); and Chirotes Razowski and Becker 1999, along with its replacement name, Prochirotes Razowski 2001, are junior synonyms of Strophotina Brown 1998, with the new combinations S. chorestis (Razowski and Becker 1999) and S. niphochondra (Razowski and Becker 1999). C1 ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Brown, JW (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM jbrown@sel.barc.usda.gov NR 19 TC 1 Z9 2 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2003 VL 105 IS 3 BP 630 EP 640 PG 11 WC Entomology SC Entomology GA 694CK UT WOS:000183756100012 ER PT J AU Saini, MS Smith, DR Saini, TP AF Saini, MS Smith, DR Saini, TP TI Review of the southeastern Asian sawfly genus Anapeptamena Konow (Hymenoptera : Tenthredinidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE India; Myanmar; Selandriinae AB Anapeptamena Konow (Tenthredinidae: Selandriinae) has been known only by its type species, A. albipes Konow, from India and Myanmar. Two new species have been discovered from India and are described: Anapeptamena darjeelingensis, n. sp., and A. dhanoultiensis, n. sp. A male of the genus, that of A. dhanoultiensis, is described for the first time. Descriptions, illustrations, and a key are provided for identification of the species. C1 Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India. ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. RP Smith, DR (reprint author), Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India. NR 5 TC 2 Z9 3 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2003 VL 105 IS 3 BP 641 EP 646 PG 6 WC Entomology SC Entomology GA 694CK UT WOS:000183756100013 ER PT J AU Gordon, RD McCleve, S AF Gordon, RD McCleve, S TI Five new species of Euparixia brown (Coleoptera : Aphodiidae : Eupariinae), with a revised key to species SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE taxonomy; new species; ant nests AB Five previously undescribed species of Euparixia Brown, E. boliviana from Bolivia, E. campbelli from Costa Rica, E. isthmia and E. panamaensis from Panama, and E. mexicana from Mexico are described and integrated into the existing classification. A revised key to all known species is presented. C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entom Lab, Washington, DC 20560 USA. RP Gordon, RD (reprint author), No Plains Entomol, POB 65, Willow City, ND 58384 USA. NR 2 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 JUL PY 2003 VL 105 IS 3 BP 685 EP 697 PG 13 WC Entomology SC Entomology GA 694CK UT WOS:000183756100018 ER PT J AU Marsh, PM Shaw, SR AF Marsh, PM Shaw, SR TI Revision of North American Aleiodes Wesmael (Part 7): The compressor Herrich-Schaeffer, ufei (Walley), gressitti (Muesebeck), and procerus Wesmael species-groups (Hymenoptera : Braconidae : Rogadinae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Hymenoptera; Braconidae; parasitoids AB Six North American species in four species-groups of the genus Aleiodes are treated. The compressor (Herrich-Schaeffer) species-group includes A. palmatus (Walley), new combination and A. palmatoides, new species; the ufei (Walley) species-group includes only A. ufei (Walley), new combination; the gressitti (Muesebeck) species-group includes A. lissos, new species; and the procerus species-group includes A. granulatus (DeGant), new combination, and A. angustipennis, new species. Other new combinations proposed are: A. aligharensis (Quadri), new combination; A. compressor (Herrich-Schaeffer), new combination; A. gressitti (Muesebeck), new combination; and A. narangae (Rohwer), new combination. C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. Univ Wyoming, Dept Renewable Resources, Insect Museum, Laramie, WY 82071 USA. RP Marsh, PM (reprint author), POB 384, N Newton, KS 67117 USA. NR 20 TC 7 Z9 7 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2003 VL 105 IS 3 BP 698 EP 707 PG 10 WC Entomology SC Entomology GA 694CK UT WOS:000183756100019 ER PT J AU Braud, R Smith, DR Strazanac, JS Butler, L AF Braud, R Smith, DR Strazanac, JS Butler, L TI Diversity, abundance, and seasonality of adult and larval Symphyta (Hymenoptera) in the George Washington National Forest, Virginia, and the Monongahela National Forest, West Virginia SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Symphyta; richness; abundance; diversity; Acordulecera dorsalis ID FOOD; TRAP AB Adult Symphyta richness and abundance were studied using data collected from 36 Malaise traps in the Monongahela National Forest, Pocahontas County, West Virginia, and in the George Washington National Forest, Augusta County, Virginia. A total of 8,884 adults representing 155 species in 49 genera and 8 families were collected. Diversity estimators suggest that approximately 81% of the actual species present on the two forests were sampled over five years (1995-1999). Fifty percent of all adults (4,48 1) were Acordulecera dorsalis Say ((Pergidae). The next most :abundant species were Pristphora banksi Marlatt (Tenthredinidae) (12.8%), Pachynematus corniger,(Norton) (Tenthredinidae) (4%), Pracharactus rudis (Norton) (Tenthredinidae) (3%), and Taxonus palipes (Say) (Tenthredinidae) (2%). Larval symphytan richness and abundance were determined by foliage collections from Quercus spp., Carya spp., and Acer spp. Symphytan larvae from foliage numbered 11,621 specimens representing eight genera. Sixty-three percent of all larvae (7,373) were Acordulecera spp. The next most abundant genus was Periclista (2,328) which accounted for 20% of the total larvae. Differences in species,richness and abundance of both adults and larvae occurred between forests and between years. C1 W Virginia Univ, Div Plant & Soil Sci, Morgantown, WV 26506 USA. Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. RP Braud, R (reprint author), W Virginia Univ, Div Plant & Soil Sci, Morgantown, WV 26506 USA. NR 15 TC 6 Z9 8 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2003 VL 105 IS 3 BP 756 EP 768 PG 13 WC Entomology SC Entomology GA 694CK UT WOS:000183756100023 ER PT J AU Poinar, G Smith, DR AF Poinar, G Smith, DR TI Food plant, life history notes, and distribution of Nematus atriceps (Marlatt) - (Hymenoptera : Tenthredinidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID ZIGADENUS LILIACEAE C1 Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA. Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. RP Poinar, G (reprint author), Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA. NR 6 TC 1 Z9 2 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2003 VL 105 IS 3 BP 778 EP 780 PG 3 WC Entomology SC Entomology GA 694CK UT WOS:000183756100026 ER PT J AU Smith, DR Marshall, SA AF Smith, DR Marshall, SA TI First report of nuptial feeding in sawflies, Aneugmenus flavipes (Norton) (Hymenoptera : Tenthredinidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article C1 Smithsonian Inst, Natl Museum Nat Hist, Agr Res Serv, PSI,Systemat Entomol Lab, Washington, DC 20560 USA. Univ Guelph, Dept Environm Biol, Guelph, ON N1G 2W1, Canada. RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Agr Res Serv, PSI,Systemat Entomol Lab, Washington, DC 20560 USA. NR 8 TC 2 Z9 4 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2003 VL 105 IS 3 BP 789 EP 791 PG 3 WC Entomology SC Entomology GA 694CK UT WOS:000183756100030 ER PT J AU Roalson, EH Skog, LE Zimmer, EA AF Roalson, EH Skog, LE Zimmer, EA TI Phylogenetic relationships and the diversification of floral form in Achimenes (Gesneriaceae) SO SYSTEMATIC BOTANY LA English DT Article ID MAXIMUM-LIKELIHOOD ANALYSES; NDHF SEQUENCES; CLADISTIC-ANALYSIS; SAINTPAULIA GESNERIACEAE; EPISCIEAE GESNERIACEAE; TRIBAL RELATIONSHIPS; POLLINATION SYSTEMS; CHLOROPLAST DNA; EVOLUTION; ORCHIDACEAE AB Achimenes is a genus in the Gesneriaceae, subfamily Gesnerioideae, tribe Gloxinieae that shows remarkable variation in floral form and possibly floral pollination syndrome. This includes flowers that are salverform, tubular, or infundibuliform, white, yellow, pink, purple, and red, and with or without corolla spurs. Previous classifications of Achimenes have relied heavily on floral form as a measure of relationship. This study explores phylogenetic relationships in Achimenes and addresses questions of proper supraspecific classification, evolution of floral forms and pollination syndromes, the origins of floral spurs, chromosome evolution, and biogeographic patterns using nrDNA ITS and cpDNA trnL-F spacer sequences analyzed using maximum parsimony and maximum likelihood methodologies. Phylogenetic hypotheses support the non-monophyly of most of the supraspecific classification units currently recognized in Achimenes, multiple origins of each of the pollination syndromes and the major morphological characteristics used to define these syndromes, multiple origins of floral spurs, multiple tetraploid events, and sympatric distributions of many closely related species. C1 Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. Natl Museum Nat Hist, Labs Analyt Biol, Smithsonian Inst, Suitland, MD 20746 USA. Smithsonian Inst, Dept Systemat Biol Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Roalson, EH (reprint author), Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. EM roalson@mail.wsu.edu RI Zimmer, Elizabeth/G-3890-2011 NR 77 TC 18 Z9 19 U1 0 U2 7 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 2003 VL 28 IS 3 BP 593 EP 608 PG 16 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 713FF UT WOS:000184845900013 ER PT J AU Warner, DJ AF Warner, DJ TI The art of teaching physics: Instrumentation of Jean-Antoine Nollet 1700-1770 SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Warner, DJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2003 VL 44 IS 3 BP 603 EP 604 DI 10.1353/tech.2003.0141 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 715TG UT WOS:000184987900014 ER PT J AU Langley, HD AF Langley, HD TI Medicine under sail. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Langley, HD (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2003 VL 44 IS 3 BP 609 EP 610 DI 10.1353/tech.2003.0118 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 715TG UT WOS:000184987900018 ER PT J AU Molella, A AF Molella, A TI Technomanifestos: Visions from the information revolutionaries. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA. RP Molella, A (reprint author), Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2003 VL 44 IS 3 BP 639 EP 640 DI 10.1353/tech.2003.0123 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 715TG UT WOS:000184987900038 ER PT J AU McNair, DB Dean, JP AF McNair, DB Dean, JP TI Distributional information on birds from egg sets collected by Henry Rogers Durkee in 1870 in Southwestern Wyoming SO WESTERN NORTH AMERICAN NATURALIST LA English DT Article DE eggs; museum collections; Wyoming; distribution; history; Ammodramus savannarum; Grasshopper Sparrow; Calamospiza melanocorys; Lark Bunting; Passerella iliaca schistacea; Fox Sparrow; Grus canadensis; Sandhill Crane ID SPARROW AB Henry Rogers Durkee collected 74 egg sets of 27 avian species in 1870 at Gilmer, Uinta County, in southwestern Wyoming. Despite the paucity of documented breeding evidence from this region during the late 19th and early 20th centuries, his material at the Smithsonian Institution was generally overlooked and has never been critically examined. Durkee's egg sets included 5 species (Sandhill Crane, Grus canadensis; Northern Rough-winged Swallow, Stelgidopteryx serripennis; Grasshopper Sparrow, Ammodramus savannarum; Fox Sparrow, Passerella iliaca; Cassin's Finch, Carpodacus cassinii) whose breeding distribution was then poorly known, 25 to more than 70 years before nests and eggs were otherwise documented in Wyoming. Durkee also collected complete egg sets of Lark Bunting (Calamospiza melanocorys) over 70 years before breeding was confirmed at other peripheral locations in Wyoming. In addition, Durkee's incomplete egg sets of Grasshopper Sparrow were the 1st for the western subspecies (A. s. perpallidus); his incomplete egg set and nest of the Fox Sparrow collected at Gilmer constituted the 2nd locality for the species or species group (P. i. schistacea). Although the number of egg sets Durkee collected is modest, he made a meaningful contribution to the early history of avifaunal exploration in Wyoming. C1 Tall Timbers Res Stn, Tallahassee, FL 32312 USA. Smithsonian Inst, Dept Systemat Biol, Div Birds, Washington, DC 20013 USA. RP McNair, DB (reprint author), Dept Planning & Nat Resources, Div Game & Fish, 45 Mars Hill, Frederiksted, VI 00840 USA. NR 93 TC 1 Z9 1 U1 0 U2 3 PU BRIGHAM YOUNG UNIV PI PROVO PA 290 LIFE SCIENCE MUSEUM, PROVO, UT 84602 USA SN 1527-0904 J9 WEST N AM NATURALIST JI West. North Am. Naturalist PD JUL PY 2003 VL 63 IS 3 BP 320 EP 332 PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 712HG UT WOS:000184791800005 ER PT J AU Hershler, R Liu, HP Thompson, FG AF Hershler, R Liu, HP Thompson, FG TI Phylogenetic relationships of North American nymphophiline gastropods based on mitochondrial DNA sequences SO ZOOLOGICA SCRIPTA LA English DT Article ID HYDROBIIDAE MOLLUSCA; GENUS PYRGULOPSIS; RISSOOIDEA; SYSTEMATICS; SNAIL; PROSOBRANCHIA; SUBSTITUTION; SUBUNIT; GENERA; MODEL AB Phylogenetic relationships of 36 nymphophiline species representing 10 genera were inferred from mtCOI sequence data and compared to recent morphology-based classifications of this group. Parsimony and maximum likelihood analyses of the molecular data set suggested monophyly of the North American nymphophilines and a sister or otherwise close relationship between this fauna and a European species assigned to the subfamily. Results also supported a previously hypothesized close relationship between the predominantly freshwater nymphophilines and the brackish-water genus Hydrobia . Our analyses resolved a North American nymphophiline subclade composed of Floridobia , Nymphophilus , and Pyrgulopsis , and depicted the remaining North American genera (Cincinnatia , Marstonia , Notogillia , Rhapinema , Spilochlamys , Stiobia ) as either a monophyletic or paraphyletic group. Two of the large North American genera (Floridobia , Marstonia ) were supported as monophyletic groups while monophyly of Pyrgulopsis , a western North American group containing > 100 species, was equivocal. North American nymphophiline phylogeny implies that vicariance of eastern and western North American groups was followed by a secondary invasion of eastern coastal areas from the west. We attribute this to dispersal of salt-tolerant progenitors along the Gulf of Mexico coast. C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. Univ Florida, Florida Museum Nat Hist, Div Malacol, Gainesville, FL 32611 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Systemat Biol, POB 37012,NHB W-305,MRC 118, Washington, DC 20013 USA. NR 50 TC 36 Z9 36 U1 0 U2 3 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD JUL PY 2003 VL 32 IS 4 BP 357 EP 366 DI 10.1046/j.1463-6409.2003.00115.x PG 10 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 688NZ UT WOS:000183443300004 ER PT J AU Randall, JE Allen, GR Robertson, DR AF Randall, JE Allen, GR Robertson, DR TI Myripristis earlei, a new soldierfish (Beryciformes : Holocentridae) from the Marquesas and Phoenix Islands SO ZOOLOGICAL STUDIES LA English DT Article DE fish taxonomy; Holocentridae; new soldierfish; oceania AB The common holocentrid fish in the Marquesas Islands, previously regarded as an insular variant of the wide-ranging Myripristis berndti, is described as a new species, M. earlei, after discovering a typical M. berndti in the islands and also finding the species in the Phoenix Islands with M. berndti. No meristic or proportional measurement differences were found to separate the 2 species, and no mtDNA differences were detected. Myripristis earlei differs from M. berndti by lacking or having only a few small scales on the lower 1/2 of the pectoral-fin axil; the lower jaw of adults not as strongly projecting; the leading edges of the soft dorsal, anal, and caudal fins not white; and the spinous portion of the dorsal fin red instead of being orange-yellow on the outer part as in M. berndti. C1 Bernice P Bishop Museum, Honolulu, HI 96817 USA. Conservat Int, Roleystone, Australia. Western Australian Museum, Perth, WA, Australia. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Randall, JE (reprint author), Bernice P Bishop Museum, 1525 Bernice St, Honolulu, HI 96817 USA. NR 5 TC 3 Z9 5 U1 2 U2 3 PU ACAD SINICA INST ZOOLOGY PI TAIPEI PA EDITORIAL OFFICE, TAIPEI 115, TAIWAN SN 1021-5506 J9 ZOOL STUD JI Zool. Stud. PD JUL PY 2003 VL 42 IS 3 BP 405 EP 410 PG 6 WC Zoology SC Zoology GA 705PD UT WOS:000184402700002 ER PT J AU Pawson, DL Gage, JD Belyaev, GM Mironov, AN Smirnov, AV AF Pawson, DL Gage, JD Belyaev, GM Mironov, AN Smirnov, AV TI The deep sea synaptid Protankyra brychia (Echinodermata : Holothuroidea) and its near-surface dwelling planktotrophic larva, Auricularia nudibranchiata SO SARSIA LA English DT Article DE Holothurians; synaptids; auricularia; bathyal; abyssal ID NORTHEAST ATLANTIC-OCEAN; ROCKALL TROUGH; ABYSSAL-PLAIN; REPRODUCTION AB Pacific and Atlantic Ocean material of the bathyal to abyssal synaptid holothurian genus Protankyra confirm that P. abyssicola (Theel) and P. pacifica (Ludwig) are subjective synonyms of P. brychia (Verrill 1885). This species is probably cosmopolitan in distribution at 869-4990 m. Post-larval juveniles from several localities in the Atlantic and Pacific Oceans retain wheel ossicles from pelagic planktotrophic larvae; the wheels are identical to those of the giant pelagic larva Auricularia nudibranchiata Chun 1896. We believe that Auricularia nudibranchiata is the larva of P. brychia. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Scottish Marine Biol Assoc, Oban PA34 4AD, Argyll, Scotland. USSR Acad Sci, Inst Oceanol, Moscow, Russia. Russian Acad Sci, Inst Oceanol, Moscow 117218, Russia. Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. RP Pawson, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Mail Stop MRC163, Washington, DC 20560 USA. NR 54 TC 5 Z9 6 U1 4 U2 4 PU TAYLOR & FRANCIS AS PI OSLO PA CORT ADELERSGT 17, PO BOX 2562, SOLLI, 0202 OSLO, NORWAY SN 0036-4827 J9 SARSIA JI Sarsia PD JUN 30 PY 2003 VL 88 IS 3 BP 159 EP 174 DI 10.1080/00364820310001165 PG 16 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 700AM UT WOS:000184090500001 ER PT J AU Clarke, RD Tyler, JC AF Clarke, RD Tyler, JC TI Differential space utilization by male and female spinyhead blennies, Acanthemblemaria spinosa (Teleostei : Chaenopsidae) SO COPEIA LA English DT Article ID MALE REPRODUCTIVE SUCCESS; CORAL-REEF; GENUS ACANTHEMBLEMARIA; TUBE BLENNIES; HABITAT USE; FISHES; MICROHABITAT; COMPETITION; CHOICE AB To assess the ways in which different selection pressures on male and female spinyhead blennies (Acanthemblemaria spinosa) influence their use of space, we measured a number of features of their shelter sites. Both sexes occurred primarily on dead surfaces of elkhorn coral (Acropora palmata), but significantly more males than females were found on live coral surfaces. Males occurred twice. as frequently as females in the vacated constructed tubes of serpulid worms or vermetid molluscs, which provide greater surface for egg deposition than the shorter cavities excavated by other organisms. There was no difference between the sexes in shelter height above the reef surface. Fish size was positively correlated with shelter height above the reef surface for both sexes. Number of eggs being guarded by males was positively correlated with both fish size and shelter height above the reef surface; in concert they account for 44% of the variance in egg number. To assess the effects of competition, we removed spinybeads from corals and documented recolonization along with shelter site parameters. Corals originally harboring larger fish were recolonized at a higher rate, and in all cases the mean size of recolonists was smaller than originals; the original correlation of fish size with height above the reef surface collapsed for recolonists. These observations are consistent with others that indicate that spinyhead blennies compete for quality shelters. C1 Sarah Lawrence Coll, Dept Biol, Bronxville, NY 10708 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Clarke, RD (reprint author), Sarah Lawrence Coll, Dept Biol, Bronxville, NY 10708 USA. EM rclarke@mail.slc.edu NR 28 TC 7 Z9 7 U1 0 U2 3 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD JUN 23 PY 2003 IS 2 BP 241 EP 247 PG 7 WC Zoology SC Zoology GA 695EG UT WOS:000183817700002 ER PT J AU Sumner, S Nash, DR Boomsma, JJ AF Sumner, S Nash, DR Boomsma, JJ TI The adaptive significance of inquiline parasite workers SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE reproductive suppression; social parasitism; Acromyrmex insinuator; adaptation ID SOCIAL PARASITISM; ACROMYRMEX INSINUATOR; CUCULUS-CANORUS; ANTS; HYMENOPTERA; FORMICIDAE; BEHAVIOR; CASTE; EVOLUTION; CUCKOOS AB Social parasites exploit the socially managed resources of their host's society. Inquiline social parasites are dependent on their host throughout their life cycle, and so many of the traits inherited from their free-living ancestor are removed by natural selection. One trait that is commonly lost is the worker caste, the functions of which are adequately fulfilled by host workers. The few inquiline parasites that have retained a worker caste are thought to be at a transitional stage in the evolution of social parasitism, and their worker castes are considered vestigial and non-adaptive. However, this idea has not been tested. Furthermore, whether inquiline workers have an adaptive role outside the usual worker repertoire of foraging, brood care and colony maintenance has not been examined. In this paper, we present data that suggest that workers of the inquiline ant Acromyrmex insinuator play a vital role in ensuring the parasite's fitness. We show that the presence of these parasite workers has a positive effect on the production of parasite sexuals and a negative effect on the production of host sexuals. This suggests that inquiline workers play a vital role in suppressing host queen reproduction, thus promoting the rearing of parasite sexuals. To our knowledge, these are the first experiments on inquiline workers and the first to provide evidence that inquiline workers have an adaptive role. C1 Univ Copenhagen, Inst Zool, Dept Populat Ecol, DK-2100 Copenhagen, Denmark. RP Sumner, S (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM sumners@naos.si.edu RI Nash, David/B-2916-2009; Sumner, Seirian/E-6611-2011; Nash, David/H-4433-2012; Boomsma, Jacobus/M-2785-2014 OI Nash, David/0000-0002-0462-6794; Nash, David/0000-0002-0462-6794; Boomsma, Jacobus/0000-0002-3598-1609 NR 27 TC 16 Z9 16 U1 0 U2 9 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUN 22 PY 2003 VL 270 IS 1521 BP 1315 EP 1322 DI 10.1098/rspb.2003.2362 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 693BV UT WOS:000183695500013 PM 12816646 ER PT J AU Neufeld, DA Bergin, EA Melnick, GJ Goldsmith, PF AF Neufeld, DA Bergin, EA Melnick, GJ Goldsmith, PF TI Submillimeter Wave Astronomy Satellite mapping observations of water vapor around Sagittarius B2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : clouds; ISM : individual (Sagittarius B2); ISM : molecules; molecular processes; submillimeter ID MOLECULAR LINE SURVEY; GALACTIC-CENTER; ORION-KL; 263 GHZ; SGR B2; CLOUDS; ABSORPTION; EMISSION; AMMONIA; CO AB Observations of the 1(10)-1(01) 556.936 GHz transition of ortho-water with the Submillimeter Wave Astronomy Satellite have revealed the presence of widespread emission and absorption by water vapor around the strong submillimeter continuum source Sagittarius B2. An incompletely sampled spectral line map of a region of size 26' x 19' around Sgr B2 reveals three noteworthy features. First, absorption by foreground water vapor is detectable at local standard of rest (LSR) velocities in the range -100 to 0 km s(-1) at almost every observed position. Second, spatially extended emission by water is detectable at LSR velocities in the range 80-120 km s(-1) at almost every observed position. This emission is attributable to the 180 pc molecular ring identified from previous observations of CO. The typical peak antenna temperature of 0.075 K for this component implies a typical water abundance of (1.2-8) x 10(-6) relative to H-2. Third, strong absorption by water is observed within 50 of Sgr B2 at LSR velocities in the range 60-82 km s(-1). An analysis of this absorption yields a (H2O)-O-16 abundance similar to(2-4) x 10(-7) relative to H-2 if the absorbing water vapor is located within the core of Sgr B2 itself, or, alternatively, a water column density of similar to(2.5-4) x 10(16) cm(-2) if the water absorption originates in the warm, foreground layer of gas proposed previously as the origin of ammonia absorption observed toward Sgr B2. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Cornell Univ, Dept Astron, NAIC, Ithaca, NY 14853 USA. RP Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RI Goldsmith, Paul/H-3159-2016 NR 30 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2003 VL 590 IS 2 BP 882 EP 894 DI 10.1086/375024 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 688WA UT WOS:000183459200024 ER PT J AU Takakuwa, S Ohashi, N Hirano, N AF Takakuwa, S Ohashi, N Hirano, N TI Interaction between the outflow and the core in IRAM 04191+1522 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : individual (IRAM 04191+1522); ISM : jets and outflows; ISM : molecules; stars : formation; stars : mass loss ID MASS STAR-FORMATION; MAGNETOHYDRODYNAMIC SHOCK-WAVES; YOUNG STELLAR OBJECTS; L1157 DARK CLOUD; DENSE CORES; MOLECULAR CLOUD; SIO EMISSION; PROTOSTELLAR OUTFLOWS; METHANOL ENHANCEMENT; CH3OH AB We have carried out mapping observations of the molecular core associated with the young Class 0 protostar, IRAM 04191+ 1522, in the CH3OH (J(K) = 2(K)-1(K)) and (CS)-S-34 (J = 2-1) lines, using the 45 m telescope at Nobeyama Radio Observatory. Our observations have revealed that there is a condensation associated with the protostar, elongated in the east-west direction mostly perpendicular to the axis of the associated CO out. flow. Its size and mass are estimated to be 0.07 x 0.04 pc and 2.3M(.), respectively, from the CH3OH data. In addition to the elongated envelope, two compact (similar to0.03 pc) condensations were found in the CH3OH line at the southern edge of the elongated envelope, where the blueshifted CO outflow emerging from the protostar is located. In contrast to the elongated envelope, those compact CH3OH condensations show much larger line width (up to 2.0 km s(-1)), with centroid velocities blueshifted by similar to0.8 km s(-1). The compact condensations have momenta (similar to0.06 M-. km s(-1)) comparable to that of the blueshifted molecular outflow. In addition, they are gravitationally unbound, and most probably will dissipate eventually. These results suggest that the compact condensations are probably formed in the course of interaction between the outflow and the ambient gas surrounding the protostar and that such interaction may cause dissipation of a part of the ambient gas. No drastic, localized enhancement of the CH3OH abundance is, however, observed toward the compact condensations, implying that there seems to be no significant shock heating at the compact condensations, in spite of the interaction with the outflow. This may be because the CO outflow velocity (< 10 km s(-1)) is too low to cause effective heating to release CH3OH on dust grains into the gas phase. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Takakuwa, S (reprint author), Harvard Smithsonian Ctr Astrophys, 82 Puuhonu Pl,Suite 210, Hilo, HI 96720 USA. NR 68 TC 16 Z9 16 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2003 VL 590 IS 2 BP 932 EP 943 DI 10.1086/375190 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 688WA UT WOS:000183459200028 ER PT J AU Casares, J Steeghs, D Hynes, RI Charles, PA O'Brien, K AF Casares, J Steeghs, D Hynes, RI Charles, PA O'Brien, K TI Bowen fluorescence from the companion star in X1822-371 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; stars : individual (X1822-371); X-rays : binaries; X-rays : stars ID X-1822-371; SPECTROSCOPY AB We present clear evidence for the motion of the companion star in the low-mass X-ray binary (LMXB) X1822 - 371. We detect NIII lambda4640 emission moving in antiphase with the radial velocity curve of the neutron star and produced on the X-ray - heated hemisphere of the donor star. From the motion of this feature we derive a lower limit to the radial velocity semiamplitude of the companion star, K-2 greater than or equal to 300 +/- 8 km s(-1), which, combined with a previous determination of the inclination angle and the pulsar's radial velocity curve, yields M-2 greater than or equal to 0.36(2) M-. and M-1 greater than or equal to 1.14(6)M-.. The He I lambda4471 absorption line moves at lower velocities (similar or equal to225 km s(-1)) and with a -0.05 phase shift, suggesting a likely origin on the gas stream near the L1 point. In addition, we detect an S-wave emission of O vi lambda3811 produced by illumination of the hot spot bulge by the central source. The Balmer lines are dominated by broad absorptions probably due to obscuration of the accretion disk by vertically extended cool material from the splash region and over. owing stream. We also derive a more accurate, and significantly different ( compared to earlier work), systemic velocity of gamma = -44 +/- 5 km s(-1), based on the motion of the He II lambda4686 wings and Doppler tomography. This work confirms the power of imaging the companion stars in LMXBs and outbursting transients using the Bowen fluorescence transitions. C1 Inst Astrofis Canarias, Tenerife 38200, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Southampton, Dept Phys & Astron, Southampton S017 1BJ, Hants, England. European So Observ, Santiago 19, Chile. RP Casares, J (reprint author), Inst Astrofis Canarias, Tenerife 38200, Spain. RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 25 TC 40 Z9 40 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 JUN 20 PY 2003 VL 590 IS 2 BP 1041 EP 1048 DI 10.1086/375055 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 688WA UT WOS:000183459200037 ER PT J AU Wang, J Yaqoob, T Szokoly, G Gilli, R Kewley, L Mainieri, V Nonino, M Rosati, P Tozzi, P Zheng, W Zirm, A Norman, C AF Wang, J Yaqoob, T Szokoly, G Gilli, R Kewley, L Mainieri, V Nonino, M Rosati, P Tozzi, P Zheng, W Zirm, A Norman, C TI A puzzling X-ray source found in the Chandra Deep Field-South SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (CXOCDFS J033225.3-274219) galaxies : peculiar; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; EMISSION-LINE; AFTERGLOW; NGC-6240; GALAXY; BURST AB In this Letter, we report the detection of an extremely strong X-ray emission line in the 940 ks Chandra ACIS-I spectrum of CXOCDFS J033225.3-274219. The source was identified as a type 1 active galactic nucleus at a redshift of z = 1.617, with a 2.0-10.0 keV rest-frame X-ray luminosity of similar to10(44) ergs s(-1). The emission line was detected at 6.2(-0.1)(+0.2) keV, with an equivalent width ( EW) of 4.4(-1.4)(+3.2) keV; both quantities refer to the observed frame. In the rest frame, the line is at 16.2(-0.3)(+0.4) keV with an EW of 11.5(-3.7)(+8.3) keV. An X-ray emission line at a similar energy(similar to17 keV, in the rest frame) in PKS 2149-306 was discovered before using ASCA data. We reject the possibility that the line is due to a statistical or instrumental artifact. The line is most likely due to blueshifted Fe K emission from an relativistic outflow, probably an inner X-ray jet, with velocities of the order of similar to0.6c-0.7c. Other possible explanations are also discussed. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. Ist Nazl Astrofis, Osservatorio Astron, I-34131 Trieste, Italy. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Wang, J (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RI Gilli, Roberto/P-1110-2015 OI Gilli, Roberto/0000-0001-8121-6177 NR 20 TC 12 Z9 12 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2003 VL 590 IS 2 BP L87 EP L90 DI 10.1086/376821 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 688WE UT WOS:000183459600006 ER PT J AU Kirshner, RP AF Kirshner, RP TI Throwing light on dark energy SO SCIENCE LA English DT Review ID HIGH-REDSHIFT SUPERNOVAE; HUBBLE DEEP FIELD; IA SUPERNOVAE; COSMOLOGICAL CONSTANT; ACCELERATING UNIVERSE; ELEMENTARY PARTICLES; LAMBDA; CONSEQUENCES; DECELERATION; PARAMETERS AB Supernova observations show that the expansion of the universe has been speeding up. This unexpected acceleration is ascribed to a dark energy that pervades space. Supernova data, combined with other observations, indicate that the universe is about 14 billion years old and is composed of about 30% matter and 70% dark energy. New observational programs can trace the history of cosmic expansion more precisely and over a larger span of time than has been done to date to learn whether the dark energy is a modern version of Einstein's cosmological constant or another form of dark energy that changes with time. Either conclusion is an enigma that points to gaps in our fundamental understanding of gravity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Kirshner, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA. EM kirshner@cfa.harvard.edu NR 54 TC 29 Z9 29 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 JUN 20 PY 2003 VL 300 IS 5627 BP 1914 EP 1918 DI 10.1126/science.1086879 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 691RN UT WOS:000183619400036 PM 12817141 ER PT J AU Riley, S AF Riley, S TI The difference between you and me. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Riley, S (reprint author), Smithsonian Inst Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 15 PY 2003 VL 128 IS 11 BP 99 EP 99 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 688XZ UT WOS:000183463700200 ER PT J AU Watters, TR AF Watters, TR TI Thrust faults along the dichotomy boundary in the eastern hemisphere of Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE thrust faults; dichotomy boundary; lobate scarps; Mars; lithospheric flexure ID ORBITER LASER ALTIMETER; CRUSTAL DICHOTOMY; LOBATE SCARPS; TERRESTRIAL PLANETS; GIANT IMPACT; DISPLACEMENT; TOPOGRAPHY; MERCURY; EVOLUTION; LINKAGE AB Mars Orbiter Laser Altimetry (MOLA) data have been used to characterize lobate scarps along the dichotomy boundary in the eastern hemisphere of Mars. These structures are the surface expression of thrust faulting of the southern highlands. Displacement on the thrust faults is generally less than 1 km except in the case of the Amenthes Rupes thrust fault, where the maximum displacement is on the order of 3 km. The ratio of maximum displacement to fault length g of the population of thrust faults is similar to6.2 x 10(-3) (n = 26), consistent with previous estimates for Martian thrust faults based on photoclinometrically derived topography, and other planetary thrust fault populations. Thrust faulting is roughly coincident with Late Noachian to Early Hesperian fracturing and normal faulting along the dichotomy boundary. This suggests that the formation of the present-day dichotomy boundary involved compressional and extensional deformation. The long-wavelength topography suggests that the dichotomy boundary in the eastern hemisphere may have been formed by flexure of the southern highlands lithosphere. Lithospheric flexure alone cannot account for the thrust faulting of the highlands along the dichotomy boundary. A combination of stresses due to bending, erosion, and global contraction may have formed the lobate scarp thrust faults. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 67 TC 34 Z9 34 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 14 PY 2003 VL 108 IS E6 AR 5054 DI 10.1029/2002JE001934 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 691XJ UT WOS:000183631000002 ER PT J AU Vikhlinin, A Voevodkin, A Mullis, CR VanSpeybroeck, L Quintana, H McNamara, BR Gioia, I Hornstrup, A Henry, JP Forman, WR Jones, C AF Vikhlinin, A Voevodkin, A Mullis, CR VanSpeybroeck, L Quintana, H McNamara, BR Gioia, I Hornstrup, A Henry, JP Forman, WR Jones, C TI Cosmological constraints from the evolution of the cluster baryon mass function at z similar to 0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; galaxies : clusters : general; surveys; X-rays : galaxies : clusters ID MEDIUM-SENSITIVITY SURVEY; NEARBY GALAXY CLUSTERS; RAY SCALING RELATIONS; TEMPERATURE RELATION; INTRACLUSTER MEDIUM; HIGH-REDSHIFT; DARK-MATTER; FRACTION; OMEGA(M); CONSTANT AB We present a new method for deriving cosmological constraints based on the evolution of the baryon mass function of galaxy clusters and implement it using 17 distant clusters from our 160 deg(2) ROSAT survey. The method uses the cluster baryon mass as a proxy for the total mass, thereby avoiding the large uncertainties of the M-tot-T or M-tot-L-X relations used in all previous studies. Instead, we rely on a well-founded assumption that the M-b/M-tot ratio is a universal quantity, which should result in a much smaller systematic uncertainty. Taking advantage of direct and accurate Chandra measurements of the gas masses for distant clusters, we find strong evolution of the baryon mass function between z > 0.4 and the present. The observed evolution defines a narrow band in the Omega(m)-Lambda plane, Omega(m) + 0.23Lambda = 0.41 +/- 0.10 at 68% confidence, which intersects with constraints from the cosmic microwave background and Type Ia supernovae near Omega(m) = 0.3 and Lambda = 0.7. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. European So Observ, D-85748 Garching, Germany. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. CNR, Ist Radioastron, I-40129 Bologna, Italy. Danish Space Res Inst, DK-2100 Copenhagen O, Denmark. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gioia, Isabella/B-6982-2012 OI Gioia, Isabella/0000-0003-3127-498X NR 57 TC 65 Z9 65 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP 15 EP 25 DI 10.1086/374863 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700003 ER PT J AU Winn, JN Kochanek, CS Keeton, CR Lovell, JEJ AF Winn, JN Kochanek, CS Keeton, CR Lovell, JEJ TI The quintuple quasar: Radio and optical observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (PMN J0134-0931) ID GALACTIC-CENTER; A-ASTERISK; LENS; PKS-1830-211; GALAXY; GHZ AB We present results from high-resolution radio and optical observations of PMN J0134-0931, a gravitational lens with a unique radio morphology and an extremely red optical counterpart. Our data support the theory of Keeton & Winn: five of the six observed radio components are multiple images of a single quasar, produced by a pair of lens galaxies. Multifrequency Very Long Baseline Array maps show that the sixth and faintest component has a different radio spectrum than the others, confirming that it represents a second component of the background source rather than a sixth image. The lens models predict that there should be additional faint images of this second source component, and we find evidence for one of the predicted images. The previously observed large angular sizes of two of the five bright components are not intrinsic (which would have excluded the possibility that they are lensed images) but are instead due to scatter broadening. Both the extended radio emission observed at low frequencies and the intrinsic image shapes observed at high frequencies can be explained by the lens models. The pair of lens galaxies is marginally detected in Hubble Space Telescope images. The differential extinction of the quasar images suggests that the extreme red color of the quasar is at least partly due to dust in the lens galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 16 Z9 16 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP 26 EP 38 DI 10.1086/374832 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700004 ER PT J AU Keeton, CR Winn, JN AF Keeton, CR Winn, JN TI The quintuple quasar: Mass models and interpretation SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (PMN J0134-0931) ID GRAVITATIONALLY LENSED QUASAR; EARLY-TYPE GALAXIES; SUBSTRUCTURE; POTENTIALS; STATISTICS; B1359+154; SYSTEMS; HALOS AB The strange morphology of the six-component gravitational lens PMN J0134-0931 has resisted explanation. We present the first successful quantitative models for the system, based on the idea that there are two lens galaxies and two components of the background source. One source is quintuply imaged and corresponds to the five brightest observed radio components. The other source is triply imaged and corresponds to the sixth component, along with two others too faint to have been detected. The models reproduce the observed image positions and fluxes and make falsi. able predictions about other properties of the system. Some of these predictions have been confirmed by high-resolution radio and optical observations, as described in the companion paper by Winn and coworkers. Although we cannot determine the lens model uniquely with current data, we predict that the lens galaxies are spiral galaxies with roughly equal velocity dispersions sigma similar to 120 km s(-1) and a projected separation of only 0."4 (2 h(-1) kpc at z(l) = 0.76). This system is the first known lens with five images of a single quasar and the second with more than four images. C1 Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keeton, CR (reprint author), Univ Chicago, Ctr Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. NR 40 TC 22 Z9 22 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP 39 EP 51 DI 10.1086/374833 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700005 ER PT J AU Kuraszkiewicz, JK Wilkes, BJ Hooper, EJ McLeod, KK Wood, K Bjorkman, J Delain, KM Hughes, DH Elvis, MS Impey, CD Lonsdale, CJ Malkan, MA McDowell, JC Whitney, B AF Kuraszkiewicz, JK Wilkes, BJ Hooper, EJ McLeod, KK Wood, K Bjorkman, J Delain, KM Hughes, DH Elvis, MS Impey, CD Lonsdale, CJ Malkan, MA McDowell, JC Whitney, B TI The far-infrared spectral energy distributions of X-ray - Selected active galaxies SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : active; galaxies : nuclei; infrared : galaxies; X-rays : galaxies ID RADIO-QUIET QUASARS; GALACTIC NUCLEI; SEYFERT-GALAXIES; HOST GALAXIES; DUST EMISSION; STATISTICAL-METHODS; IONIZING CONTINUUM; ASTRONOMICAL DATA; STEEP-SPECTRUM; OBSCURING TORI AB Hard X-ray selection is, arguably, the optimal method for de. ning a representative sample of active galactic nuclei (AGNs). Hard X-rays are unbiased by the effects of obscuration and reprocessing along the line of sight intrinsic/external to the AGN, which result in unknown fractions of the population being missed from traditional optical/soft X-ray samples. We present the far-infrared (far-IR) observations of 21 hard X-ray-selected AGNs from the HEAO 1 A2 sample observed with Infrared Space Observatory (ISO). We characterize the far-IR continua of these X-ray-selected AGNs and compare them with those of various radio and optically selected AGN samples and with models for an AGN-heated, dusty disk. The X-ray selected AGNs show broad, warm IR continua covering a wide temperature range (similar to20-1000 K in a thermal emission scenario). Where a far-IR turnover is clearly observed, the slopes are less than 2.5 in all but three cases so that nonthermal emission remains a possibility, although the presence of cooler dust resulting in a turnover at wavelengths longward of the ISO range is considered more likely. The sample also shows a wider range of optical/UV shapes than the optical/radio-selected samples, extending to redder near-IR colors. The bluer objects are type 1 Seyfert galaxies, while the redder AGNs are mostly intermediate or type 2 Seyfert galaxies. This is consistent with a modified unification model in which obscuration increases as we move from a face-on toward a more edge-on line of sight. However, this relation does not extend to the mid-infrared as the 25/60 mum ratios are similar in Seyfert galaxies with differing type and optical/UV reddening. The resulting limits on the column density of obscuring material through which we are viewing the redder AGNs (N-H similar to 10(22) cm(-2)) are inconsistent with standard optically thick torus models (NH similar to 1024 cm(-2)) and simple unification models. Instead our results support more complex models in which the amount of obscuring material increases with viewing angle and may be clumpy. Such a scenario, already suggested by differing optical/near-IR spectroscopic and X-ray AGN classifications, allows for different amounts of obscuration of the continuum emission in different wave bands and of the broad emission line region, which, in turn, results in a mixture of behaviors for AGNs with similar optical emission-line classifications. The resulting decrease in the optical depth of the obscuring material also allows the AGN to heat more dust at larger radial distances. We show that an AGN-heated, flared, dusty disk with mass of similar to10(9) M. and size of approximately a few hundred parsecs is able to generate optical-far-IR spectral energy distributions (SEDs) that reproduce the wide range of SEDs present in our sample with no need for an additional starburst component to generate the long-wavelength, cooler part of the IR continuum. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA. Univ St Andrews, Dept Phys & Astron, St Andrews, Fife, Scotland. Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Inst Natl Astrofis Opt & Elect, Mexico City, DF, Mexico. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, IPAC, Pasadena, CA 91125 USA. Univ Calif Los Angeles, Dept Astron, Los Angeles, CA 90095 USA. Space Sci Inst, Boulder, CO 80303 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jkuraszkiewicz@cfa.harvard.edu; bwilkes@cfa.harvard.edu; ehooper@astro.as.utexas.edu; kmcleod@wellesley.edu; kw25@st-andrews.ac.uk; jon@astro.utoledo.edu; kdelain@astro.umn.edu; dhughes@inaoep.mx; melvis@cfa.harvard.edu; impey@as.arizona.edu; cjl@ipac.caltech.edu; malkan@bonnie.astro.ucla.edu; jmcdowell@cfa.harvard.edu; bwhitney@colorado.edu OI Wilkes, Belinda/0000-0003-1809-2364 NR 114 TC 50 Z9 50 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP 128 EP 148 DI 10.1086/374919 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700014 ER PT J AU Peck, AB Henkel, C Ulvestad, JS Brunthaler, A Falcke, H Elitzur, M Menten, KM Gallimore, JF AF Peck, AB Henkel, C Ulvestad, JS Brunthaler, A Falcke, H Elitzur, M Menten, KM Gallimore, JF TI The flaring H2O megamaser and compact radio source in Markarian 348 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Markarian 348, NGC 262); galaxies : jets; galaxies : Seyfert; masers; radio lines : galaxies ID STAR-FORMING REGIONS; ACTIVE GALACTIC NUCLEI; FREE-FREE ABSORPTION; NARROW-LINE REGION; X-RAY-EMISSION; III ZW 2; SEYFERT-GALAXIES; WATER-VAPOR; NEUTRAL HYDROGEN; OBSCURING TORUS AB We report on single-dish monitoring and extremely high angular resolution observations of the flaring H2O megamaser in the Seyfert 2 galaxy Mrk 348. The H2O line is redshifted by similar to130 km s(-1) with respect to the systemic velocity, is very broad, with an FWHM of 130 km s(-1), and has no detectable high-velocity components within 1500 km s(-1) on either side of the strong line. Monitoring observations made with the Effelsberg 100 m telescope show that the maser varies significantly on timescales as short as 1 day and that the integrated line flux is loosely correlated with the continuum flux. Very Long Baseline Array (VLBA) observations indicate that the maser emission arises entirely from a region less than 0.25 pc in extent, located toward a continuum component thought to be associated with the receding jet. We also report on integrated flux monitoring with the VLA between 1.4 and 43 GHz, and VLBA continuum observations of the milliarcsecond scale jets at 1.7, 8, 15, and 22 GHz. These observations have allowed us to tentatively pinpoint the location of the core, and also show the ejection of a new jet component during the current radio "flare''. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. Bucknell Univ, Dept Phys, Lewisburg, PA 17837 USA. RP Peck, AB (reprint author), Harvard Smithsonian Ctr Astrophys, SAO SMA Project, POB 824, Hilo, HI 96721 USA. EM apeck@cfa.harvard.edu RI Falcke, Heino/H-5262-2012 OI Falcke, Heino/0000-0002-2526-6724 NR 71 TC 52 Z9 53 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP 149 EP 161 DI 10.1086/374924 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700015 ER PT J AU Greenhill, LJ Booth, RS Ellingsen, SP Herrnstein, JR Jauncey, DL McCulloch, PM Moran, JM Norris, RP Reynolds, JE Tzioumis, AK AF Greenhill, LJ Booth, RS Ellingsen, SP Herrnstein, JR Jauncey, DL McCulloch, PM Moran, JM Norris, RP Reynolds, JE Tzioumis, AK TI A warped accretion disk and wide-angle outflow in the inner parsec of the Circinus galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Circinus); galaxies : Seyfert; ISM : jets and outflows; ISM : molecules; masers ID ACTIVE GALACTIC NUCLEI; WATER MASER EMISSION; STAR-FORMING REGIONS; SEYFERT-GALAXIES; MOLECULAR DISK; LINE REGION; H2O MASERS; NGC-4258; NGC-5548; SPECTROPOLARIMETRY AB We present the first VLBI maps of H2O maser emission (lambda1.3 cm) in the nucleus of the Circinus galaxy, constructed from data obtained with the Australia Telescope Long Baseline Array. The maser emission traces a warped, edge-on accretion disk between radii of 0.11 +/- 0.02 and similar to0.40 pc, as well as a wide-angle outflow that extends up to similar to1 pc from the estimated disk center. The disk rotation is close to Keplerian ( v proportional to r(-0).5), the maximum detected rotation speed is 260 km s(-1), and the inferred central mass is (1.7 +/- 0.3) x 106 M.. The out. owing masers are irregularly distributed above and below the disk, with relative outflow velocities up to similar to+/-160 km s(-1), projected along the line of sight. The flow probably originates closer than 0.1 pc to the central engine, possibly in an inward extension of the accretion disk, although there is only weak evidence of rotation in the outward-moving material. We observe that the warp of the disk appears to collimate the outflow and to. x the extent of the ionization cone observed on larger angular scales. This study provides the first direct evidence (i.e., through imaging) of dusty, high-density, molecular material in a nuclear outflow less than 1 pc from the central engine of a Seyfert galaxy, as well as the first graphic evidence that warped accretion disks can channel outflows and illumination patterns in active galactic nuclei. We speculate that the same arrangement, which in some ways obviates the need for a geometrically thick, dusty torus, may apply to other type 2 active galactic nuclei. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chalmers Inst Technol, Onsala Space Observ, S-43992 Onsala, Sweden. Univ Tasmania, Sch Phys, Hobart, Tas 7001, Australia. Australia Telescope Natl Facil, Epping, NSW 2121, Australia. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Ellingsen, Simon/J-7754-2014; Norris, Ray/A-1316-2008; OI Ellingsen, Simon/0000-0002-1363-5457; Norris, Ray/0000-0002-4597-1906; Moran, James/0000-0002-3882-4414 NR 50 TC 178 Z9 180 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP 162 EP 173 DI 10.1086/374862 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700016 ER PT J AU Churazov, E Forman, W Jones, C Bohringer, H AF Churazov, E Forman, W Jones, C Bohringer, H TI XMM-Newton observations of the Perseus Cluster. I. The temperature and surface brightness structure SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : active; galaxies : clusters : individual (Perseus); galaxies : individual (NGC 1275); X-rays : galaxies; X-rays : galaxies : clusters ID RAY-EMITTING GAS; GALAXY CLUSTERS; NGC-1275; ROSAT; RADIO; CORE; IMAGES; FLOWS; ASCA AB We present preliminary results of a XMM-Newton 50 ks observation of the Perseus Cluster that provides an unprecedented view of the central 0.5 Mpc region. The projected gas temperature declines smoothly by a factor of 2 from a maximum value of similar to 7 keV in the outer regions to just above 3 keV at the cluster center. Over this same range, the heavy-element abundance rises slowly from 0.4 to 0.5 solar as the radius decreases from 140 to 50, and then it rises to a peak of almost 0.7 solar at 1.'25 before declining to 0.4 at the center. The global east-west asymmetry of the gas temperature and surface brightness distributions, approximately aligned with the chain of bright galaxies, suggests an ongoing merger, although the modest degree of the observed asymmetry certainly excludes a major merger interpretation. The chain of galaxies probably traces the. lament along which accretion started some time ago and is continuing at the present time. A cold and dense (low-entropy) cluster core like Perseus is probably well "protected'' against the penetration of the gas of infalling groups and poor clusters, whereas in noncooling core clusters such as Coma and A1367, infalling subclusters can penetrate deeply into the core region. In Perseus, gas associated with infalling groups may be stripped completely at the outskirts of the main cluster and only compression waves (shocks) may reach the central regions. We argue, and show supporting simulations, that the passage of such a wave(s) can qualitatively explain the overall horseshoe shaped appearance of the gas temperature map (the hot horseshoe surrounds the colder, low-entropy core) as well as other features of the Perseus Cluster core. These simulations also show that as compression waves traverse the cluster core, they can induce oscillatory motion of the cluster gas that can generate multiple sharp "edges'' on opposite sides of the central galaxy. Gas motions induced by mergers may be a natural way to explain the high frequency of "edges'' seen in clusters with cooling cores. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Space Res Inst IKI, 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-85740 Garching, Germany. RI Churazov, Eugene/A-7783-2013 NR 50 TC 186 Z9 187 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP 225 EP 237 DI 10.1086/374923 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700022 ER PT J AU Luhman, KL Briceno, C Stauffer, JR Hartmann, L Navascues, DBY Caldwell, N AF Luhman, KL Briceno, C Stauffer, JR Hartmann, L Navascues, DBY Caldwell, N TI New low-mass members of the Taurus star-forming region SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : luminosity function, mass function; stars : pre-main-sequence ID BROWN DWARFS; MAIN-SEQUENCE; EMISSION; SPECTROSCOPY; ACCRETION; OBJECT; IC-348; L1495E; LIMIT AB Briceno et al. recently used optical imaging, data from the Two-Micron All-Sky Survey (2MASS), and follow-up spectroscopy to search for young low-mass stars and brown dwarfs in 8 deg(2) of the Taurus star-forming region. By the end of that study, there remained candidate members of Taurus that lacked the spectroscopic observations needed to measure spectral types and determine membership. In this work, we have obtained spectroscopy of the 22 candidates that have A(V) less than or equal to 8, from which we find six new Taurus members with spectral types of M2.75 through M9. The new M9 source has the second latest spectral type of the known members of Taurus (similar to0.02 M-.). Its spectrum contains extremely strong emission in Halpha (W-lambda similar to 950 Angstrom), as well as emission in He I 6678 Angstrom and the Ca II IR triplet. This is the least massive object known to exhibit emission in He I and Ca II, which together with the strong Halpha are suggestive of intense accretion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Invest Astron, Merida 5101 A, Venezuela. CALTECH, SIRTF Sci Ctr, MS 314 6, Pasadena, CA 91125 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 30 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 JUN 10 PY 2003 VL 590 IS 1 BP 348 EP 356 DI 10.1086/374983 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700033 ER PT J AU Antiochos, SK Karpen, JT DeLuca, EE Golub, L Hamilton, P AF Antiochos, SK Karpen, JT DeLuca, EE Golub, L Hamilton, P TI Constraints on active region coronal heating SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : transition region; Sun : UV radiation ID TRANSITION REGION; SOLAR CORONA; LOOPS; EXPLORER; TRACE; TEMPERATURE; DIAGNOSTICS; NANOFLARES; PLASMA; MODELS AB We derive constraints on the time variability of coronal heating from observations of the so-called active region moss by the Transition Region and Coronal Explorer ( TRACE). The moss is believed to be due to million-degree emission from the transition regions at the footpoints of coronal loops whose maximum temperatures are several million degrees. The two key results from the TRACE observations discussed in this paper are that in the moss regions one generally sees only moss, not million-degree loops, and that the moss emission exhibits only weak intensity variations, similar to10% over periods of hours. TRACE movies showing these results are presented. We demonstrate, using both analytic and numerical calculations, that the lack of observable million-degree loops in the moss regions places severe constraints on the possible time variability of coronal heating in the loops overlying the moss. In particular, the heating in the hot moss loops cannot be truly flarelike with a sharp cutoff, but instead must be quasi-steady to an excellent approximation. Furthermore, the lack of significant variations in the moss intensity implies that the heating magnitude is only weakly varying. The implications of these conclusions for coronal heating models will be discussed. C1 USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. EM antiochos@nrl.navy.mil RI Karpen, Judith/E-1484-2012; Antiochos, Spiro/D-4668-2012; Hamilton, Paul/E-7891-2015; DeLuca, Edward/L-7534-2013 OI Antiochos, Spiro/0000-0003-0176-4312; Hamilton, Paul/0000-0001-6080-632X; DeLuca, Edward/0000-0001-7416-2895 NR 30 TC 58 Z9 58 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP 547 EP 553 DI 10.1086/375003 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TE UT WOS:000183278700049 ER PT J AU Kong, AKH Sjouwerman, LO Williams, BF Garcia, MR Dickel, JR AF Kong, AKH Sjouwerman, LO Williams, BF Garcia, MR Dickel, JR TI Discovery of radio/X-ray/optical-resolved supernova remnants in the center of the Andromeda galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); supernova remnants; X-rays : ISM ID LARGE-MAGELLANIC-CLOUD; RAY POINT SOURCES; X-RAY; NOVA REMNANTS; CASSIOPEIA-A; M31; CHANDRA; EMISSION; CANDIDATES; RCW-103 AB We have detected a spatially resolved supernova remnant (SNR) in the center of the Andromeda galaxy, in radio, X-ray, and optical wavelengths. These observations provide the highest spatial resolution imaging of a radio/X-ray/optical SNR in that galaxy to date. The multiwavelength morphology, radio spectral index, X-ray colors, and narrowband optical imaging are consistent with a shell-type SNR. A second SNR is also seen resolved in both radio and X-ray. By comparing the morphological structure of the SNRs in different wavelengths and with that in our own Galaxy, we can study the shock morphologies of SNRs in the Andromeda galaxy. The proximity of the SNRs to the core suggests a high interstellar medium density in the vicinity of the SNRs in the center of the Andromeda galaxy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 39 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 JUN 10 PY 2003 VL 590 IS 1 BP L21 EP L24 DI 10.1086/376687 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TF UT WOS:000183278800006 ER PT J AU Kong, AKH Di Stefano, R AF Kong, AKH Di Stefano, R TI A luminous recurrent supersoft X-ray source in NGC 300 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 300); X-rays : binaries; X-rays : galaxies ID GALAXY NGC-300; SPACED DATA; CHANDRA; CATALOG AB We report the results of XMM-Newton observations for an especially luminous supersoft X-ray source (SSS) with a bolometric luminosity of 10(39) ergs s(-1) in the spiral galaxy NGC 300. The source was detected as an SSS in 1992 and disappeared in subsequent X-ray observations. The source was active again during recent XMM-Newton observations. It appeared to be very soft (kT similar to 60 eV) and very luminous (similar to10(38)-10(39) ergs s(-1)). The two XMM-Newton observations also reveal that the source went from a "high" state to a "low" state in 6 days. We also found a 5.4 hr periodicity during the low state. We consider white dwarf, black hole, and neutron star models in order to explain the nature of the source. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 25 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP L13 EP L16 DI 10.1086/376552 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TF UT WOS:000183278800004 ER PT J AU McMahon, RJ McCarthy, MC Gottlieb, CA Dudek, JB Stanton, JF Thaddeus, P AF McMahon, RJ McCarthy, MC Gottlieb, CA Dudek, JB Stanton, JF Thaddeus, P TI The radio spectrum of the phenyl radical SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; line : identification; molecular data; molecular processes; radio lines : ISM ID MOLECULAR LINE SURVEY; BENZENE; CRL-618; ORION; BEAM; GHZ AB The phenyl radical, C6H5, derived from benzene by removal of one hydrogen atom, was detected at centimeter wavelengths in a pulsed supersonic molecular beam and subsequently at millimeter wavelengths in a low-pressure direct current glow discharge. Fourteen rotational transitions between 9 and 40 GHz and over 50 transitions between 150 and 330 GHz, each split by spin doubling, have been measured for the normal isotopic species, and a comparable number have been measured for the fully deuterated species. The spectrum of both isotopic species at millimeter wavelengths is reproduced to an uncertainty of 0.5 km s(-1) or better with seven spectroscopic constants. Rotational constants predicted from high-level molecular structure calculations are in excellent agreement with the measurements. Phenyl is a prime candidate for astronomical detection, because it is the prototypical aromatic hydrocarbon radical and a possible progenitor of other aromatic species. C1 Univ Wisconsin, Dept Chem, Madison, WI 53706 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Texas, Dept Chem & Biochem, Inst Theoret Chem, Austin, TX 78712 USA. RP McMahon, RJ (reprint author), Univ Wisconsin, Dept Chem, 1101 Univ Ave, Madison, WI 53706 USA. NR 24 TC 28 Z9 28 U1 1 U2 10 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2003 VL 590 IS 1 BP L61 EP L64 DI 10.1086/376587 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685TF UT WOS:000183278800016 ER PT J AU Soon, W Baliunas, S Idso, SB Kondratyev, KY Posmentier, ES AF Soon, W Baliunas, S Idso, SB Kondratyev, KY Posmentier, ES TI Modeling climatic effects of anthropogenic carbon dioxide emissions: unknowns and uncertainties. Reply to Karoly et al. (2003) SO CLIMATE RESEARCH LA English DT Editorial Material C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Mt Wilson Observ, Mt Wilson, CA 91023 USA. US Water Conservat Lab, Phoenix, AZ 85040 USA. Russian Acad Sci, Res Ctr Ecol Safety, St Petersburg 197110, Russia. Long Isl Univ, Brooklyn, NY 11201 USA. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 0 Z9 0 U1 1 U2 4 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0936-577X J9 CLIMATE RES JI Clim. Res. PD JUN 10 PY 2003 VL 24 IS 1 BP 93 EP 94 DI 10.3354/cr024093 PG 2 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 741FQ UT WOS:000186448400010 ER PT J AU Weck, PF Stancil, PC Kirby, K AF Weck, PF Stancil, PC Kirby, K TI Theoretical study of the rovibrationally resolved transitions of CaH SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ELECTRONIC STATES; SPECTRA; COEFFICIENTS; MOLECULES AB Comprehensive absorption line lists for (CaH)-Ca-40 have been calculated for electronic transitions from the X(2)Sigma(+) ground state to the A (2)Pi, B/B' (2)Sigma(+), and E (2)Pi low-lying excited states. The lists include transition energies and oscillator strengths for all possible allowed transitions and were computed using the most recent set of theoretical potential energy curves and dipole transition moment functions, with adjustments to account for experimental dissociation energies and asymptotic limits. Good agreement with previous calculations and available experimental data has been obtained. Oscillator strengths for the transition from the X (2)Sigma(+) state to the D (2)Sigma(+) state are also given, but due to the large uncertainty of the available dipole transition moment function the line list is highly uncertain. For the C (2)Sigma(+) <-- X (2)&USigma;(+) transition, a Franck-Condon approximation has been used. (C) 2003 American Institute of Physics. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Weck, PF (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. OI , Philippe/0000-0002-7610-2893 NR 26 TC 26 Z9 26 U1 0 U2 7 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUN 8 PY 2003 VL 118 IS 22 BP 9997 EP 10005 DI 10.1063/1.1573181 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 680TC UT WOS:000182993800012 ER PT J AU Kreamer, CM AF Kreamer, CM TI A tribute to Roy Sieber Part 2 (His contributions as the consummate connoisseur of tradition-based African arts) SO AFRICAN ARTS LA English DT Article C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. RP Kreamer, CM (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. NR 30 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SUM PY 2003 VL 36 IS 2 BP 10 EP + PG 0 WC Art SC Art GA 751XQ UT WOS:000187115900004 ER PT J AU Moffett, D Mellor, S AF Moffett, D Mellor, S TI The curator-conservator collaboration - Remembering Roy Sieber (African art connoisseurship and the contribution of science) SO AFRICAN ARTS LA English DT Article C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. RP Moffett, D (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SUM PY 2003 VL 36 IS 2 BP 44 EP + PG 0 WC Art SC Art GA 751XQ UT WOS:000187115900006 ER PT J AU Arnoldi, MJ AF Arnoldi, MJ TI Symbolically inscribing the city - Public monuments in Mali, 1995-2002 SO AFRICAN ARTS LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Arnoldi, MJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 5 TC 5 Z9 5 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SUM PY 2003 VL 36 IS 2 BP 56 EP + PG 0 WC Art SC Art GA 751XQ UT WOS:000187115900007 ER PT J AU Hacker, BC AF Hacker, BC TI Amchitka and the bomb: Nuclear testing in Alaska. SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER HISTORICAL REVIEW PI WASHINGTON PA 400 A ST SE, WASHINGTON, DC 20003 USA SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD JUN PY 2003 VL 108 IS 3 BP 873 EP 874 DI 10.1086/529686 PG 2 WC History SC History GA 692CU UT WOS:000183643400095 ER PT J AU Jantz, RL Owsley, DW AF Jantz, RL Owsley, DW TI Reply to Van Vark et al.: Is European Upper Paleolithic cranial morphology a useful analogy for early Americans? SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Editorial Material DE cranial morphology; Paleoamericans; population history ID CRANIOMETRIC VARIATION; PLEISTOCENE; ORIGINS; SHAPE C1 Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Jantz, RL (reprint author), Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA. NR 33 TC 18 Z9 18 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JUN PY 2003 VL 121 IS 2 BP 185 EP 188 DI 10.1002/ajpa.10188 PG 4 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 682HB UT WOS:000183084700011 ER PT J AU Power, ML Tardif, SD Power, RA Layne, DG AF Power, ML Tardif, SD Power, RA Layne, DG TI Resting energy metabolism of Goeldi's monkey (Callimico goeldii) is similar to that of other callitrichids SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE metabolic rate; Callitrichidae; circadian phase; primates ID THERMOREGULATION; PRIMATES AB The resting metabolic rates (RMRs) of six adult Goeldi's monkeys (Callimico, goeldii) were measured using standard methods of open circuit respirometry during both the active (daytime) and inactive (nighttime) circadian phases for this species. One subject was measured both while she was pregnant and after she delivered a full-term, stillborn infant. Inactive-phase RMR within thermal neutrality (above 27.5degreesC) averaged 288.5 +/- 30.8 ml O-2/hr; active-phase RMR within thermal neutrality averaged 416.3 +/- 60.9 ml O-2/hr. These values are 74.6% and 107.6%, respectively, of the mammalian expected for animals of this body mass. During the inactive phase, metabolic rate increased an estimated 4.3% for every degree decline in temperature below 27.5degreesC. The RMR in Goeldi's monkey is similar quantitatively and qualitatively to those of other captive callitrichids that have been studied, with active-phase RMR being at or slightly above the mammalian expected, and inactive-phase RMR being significantly reduced. We propose that this circadian pattern of RMR is a consequence of small body size, and is not a specific metabolic adaptation within the Callitrichidae. Thus we predict that metabolic studies measuring both circadian phases in other small primates will also find this pattern of reduced RMR during the inactive phase. The inactive-phase RMR within thermal neutrality of the pregnant female was not different from that measured after the stillbirth, despite an almost 15% difference in body mass. During pregnancy, however, the female was more metabolically responsive to temperature below thermal neutrality, and had a lower upper critical temperature (i.e., was less tolerant of heat). (C) 2003 Wiley-Liss, Inc. C1 Smithsonian Natl Zool Pk, Dept Conservat Biol, Nutr Lab, Washington, DC 20008 USA. SW Reg Primate Res Ctr, San Antonio, TX USA. Univ Florida, Coll Vet Med, Dept Physiol Sci, Gainesville, FL 32610 USA. RP Power, ML (reprint author), Smithsonian Natl Zool Pk, Dept Conservat Biol, Nutr Lab, Washington, DC 20008 USA. EM powerm@nzp.si.edu OI Power, Michael/0000-0002-6120-3528 FU NCRR NIH HHS [RR2022] NR 31 TC 4 Z9 4 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD JUN PY 2003 VL 60 IS 2 BP 57 EP 67 DI 10.1002/ajp.10078 PG 11 WC Zoology SC Zoology GA 697TN UT WOS:000183959500003 PM 12784286 ER PT J AU Bloom, JS AF Bloom, JS TI Is the redshift clustering of long-duration gamma-ray bursts significant? SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology : miscellaneous; cosmology : observations; gamma rays ID HOST GALAXY; OPTICAL AFTERGLOW; SPACE DENSITIES; MS 1054-03; DISCOVERY; LUMINOSITIES; SPECTROSCOPY; SUPERNOVA; FAINT; IDENTIFICATION AB The 26 long-duration gamma-ray bursts (GRBs) with known redshifts form a distinct cosmological set, selected differently than other cosmological probes such as quasars and galaxies. Since the progenitors are now believed to be connected with active star formation and since burst emission penetrates dust, one hope is that with a uniformly selected sample, the large-scale redshift distribution of GRBs can help constrain the star formation history of the universe. However, we show that strong observational biases in ground-based redshift discovery hamper a clean determination of the large-scale GRB rate and hence the connection of GRBs to the star formation history. We then focus on the properties of the small-scale (clustering) distribution of GRB redshifts. When corrected for heliocentric motion relative to the local Hubble flow, the observed redshifts appear to show a propensity for clustering: eight of 26 GRBs occurred within a recession velocity difference of 1000 km s(-1) of another GRB. That is, four pairs of GRBs occurred within 30 h(65)(-1) Myr in cosmic time, despite being causally separated on the sky. We investigate the significance of this clustering using a simulation that accounts for at least some of the strong observational and intrinsic biases in redshift discovery. Comparison of the numbers of close redshift pairs expected from the simulation with that observed shows no significant small-scale clustering excess in the present sample; however, the four close pairs occur in only about 20% of the simulated data sets (the precise significance of the clustering is dependent on the modeled biases). We conclude with some impetuses and suggestions for future precise GRB redshift measurements. C1 Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Soc Fellows, 78 Mt Auburn St, Cambridge, MA 02138 USA. NR 68 TC 36 Z9 36 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 JUN PY 2003 VL 125 IS 6 BP 2865 EP 2875 DI 10.1086/374945 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684YM UT WOS:000183234100008 ER PT J AU Caldwell, N Rose, JA Concannon, KD AF Caldwell, N Rose, JA Concannon, KD TI Star formation histories of early-type galaxies. I. Higher order Balmer lines as age indicators SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : stellar content ID OLD STELLAR POPULATIONS; COLOR-MAGNITUDE RELATION; DWARF ELLIPTIC GALAXIES; M31 GLOBULAR-CLUSTERS; VIRGO CLUSTER; 47 TUCANAE; SPECTRAL-RESOLUTION; EVOLUTIONARY TRACKS; INTEGRATED SPECTRA; SPECTROSCOPIC AGE AB We have obtained blue integrated spectra of 175 nearby early-type galaxies, covering a wide range in galaxy velocity dispersion and emphasizing those with sigma<100 km s(-1). Galaxies have been observed both in the Virgo Cluster and in lower density environments. The main goals are the evaluation of higher order Balmer lines as age indicators and differences in stellar populations as a function of mass, environment, and morphology. In this first paper, our emphasis is on presenting the methods used to characterize the behavior of the Balmer lines through evolutionary population synthesis models. Lower σ galaxies exhibit a substantially greater intrinsic scatter, in a variety of line-strength indicators, than do higher σ galaxies, with the large intrinsic scatter setting in below a σ of 100 km s(-1). Moreover, a greater contrast in scatter is present in the Balmer lines than in the lines of metal features. Evolutionary synthesis modeling of the observed spectral indexes indicates that the strong Balmer lines found primarily among the low-σ galaxies are caused by young age, rather than by low metallicity. Thus we find a trend between the population age and the central velocity dispersion, such that low-σ galaxies have younger luminosity-weighted mean ages. We have repeated this analysis using several different Balmer lines and find consistent results from one spectral indicator to another. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. RP Caldwell, N (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 79 TC 145 Z9 146 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2003 VL 125 IS 6 BP 2891 EP 2926 DI 10.1086/375308 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684YM UT WOS:000183234100010 ER PT J AU Schlegel, EM Pannuti, TG AF Schlegel, EM Pannuti, TG TI Chandra-detected X-ray sources in the nearby spiral Scd galaxy NGC 2403 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 2403); galaxies : spiral; X-rays ID SUPERNOVA-REMNANTS; STAR-FORMATION; RADIO SEARCH; ETA-CARINAE; NGC-2403; ROSAT; NGC-6946; EMISSION; LUMINOSITY; STARBURST AB We present an analysis of a 35.6 ks observation made with the Chandra X-Ray Observatory of the nearby spiral Scd galaxy NGC 2403. Forty-one discrete sources are detected at a significance of 3 sigma or greater within the portion of the galaxy sampled by the Chandra detectors. The luminosities of the discrete sources range from similar to10(36) through similar to10(39) ergs s(-1) over the energy range of 0.5-10 keV. We have also analyzed Einstein, ROSAT, and ASCA observations of this galaxy to search for time variability from the detected sources. One luminous X-ray source seen in an Einstein observation of this galaxy is not detected by Chandra or in a separate observation made with ASCA, while a luminous source observed by Chandra was not detected by Einstein or ASCA. For the four most luminous X-ray sources detected by the Chandra observation including one previously identified as an ultraluminous X-ray source-spectral fits to these sources provide the best broadband CCD spectra to date. We have searched for counterparts at optical and radio wavelengths. Only one of the 35 optically identified supernova remnants (SNRs) in this galaxy, MFBL 31, is clearly associated with an X-ray source in our sample. Three other optically identified SNRs-MFBL 15, MFBL 17, and MFBL 29-may also have X-ray counterparts, but the associations are far less robust. A similar search for X-ray counterparts to known discrete radio sources seen toward NGC 2403 yields a single coincidence between an X-ray source and a candidate radio SNR, TH-2. None of the detected X-ray sources are coincident with either candidate globular clusters or massive star clusters associated with NGC 2403. The only historical supernova in NGC 2403, SN 1954J, is not detected; neither is an X-ray counterpart to the galaxy's optical nucleus detected. Finally, we confirm the diffuse emission results of Fraternali et al. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Schlegel, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 56 TC 21 Z9 21 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2003 VL 125 IS 6 BP 3025 EP 3036 DI 10.1086/374990 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684YM UT WOS:000183234100018 ER PT J AU Mochejska, BJ Stanek, KZ Kaluzny, J AF Mochejska, BJ Stanek, KZ Kaluzny, J TI Long-term variability survey of the old open cluster NGC 6791 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; color-magnitude diagrams; novae, cataclysmic variables; open clusters and associations : individual (NGC 6791); stars : variables : other ID IMAGE SUBTRACTION; CCD PHOTOMETRY; VARIABLE-STARS; BINARY STARS; NGC-6791; SEARCH; FIELD; DISCOVERY; SYSTEMS AB We present the results of a long-term variability survey of the old open cluster NGC 6791. The BVI observations, collected over a time span of 6 years, were analyzed using the ISIS image subtraction package. The main target of our observations were two cataclysmic variables, B7 and B8. We have identified possible cycle lengths of about 25 and 18 days for B7 and B8, respectively. We tentatively classify B7 as a VY Sculptoris type nova-like variable or a Z Camelopardalis type dwarf nova. B8 is most likely an SS Cygni type dwarf nova. We have also extracted the light curves of 42 other previously reported variable stars and discovered seven new ones. The new variables show long-period or nonperiodic variability. The long baseline of our observations has also allowed us to derive more precise periods for the variables, especially for the short-period eclipsing binaries. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Mochejska, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 16 Z9 16 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2003 VL 125 IS 6 BP 3175 EP 3184 DI 10.1086/374993 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684YM UT WOS:000183234100028 ER PT J AU Torres, G Mader, JA Marschall, LA Neuhauser, R Duffy, AS AF Torres, G Mader, JA Marschall, LA Neuhauser, R Duffy, AS TI Optical photometry and X-ray monitoring of the "cool Algol" BD +05 degrees 706: Determination of the physical properties SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : activity; stars : fundamental parameters; stars : individual (BD+05 degrees 706) ID BINARY STAR LIGHT; ECLIPSING BINARIES; SPECTROSCOPIC BINARIES; DIFFERENTIAL ROTATION; ABSOLUTE DIMENSIONS; MAIN-SEQUENCE; SPOT; MONOCEROTIS; STARSPOTS; SYSTEMS AB We present new photometric observations in the BVRI bands of the double-lined eclipsing binary BD + 05degrees706 conducted over three observing seasons, as well as new X-ray observations obtained with ROSAT covering a full orbital cycle ( P = 18.9 days). A detailed light-curve analysis of the optical data shows the system to be semidetached, confirming indications from an earlier analysis by Torres et al. (published in 1998), with the less massive and cooler star filling its Roche lobe. The system is a member of the rare class of cool Algol systems, which are different from the "classical'' Algol systems in that the mass-gaining component is also a late-type star rather than a B- or A-type star. By combining the new photometry with a reanalysis of the spectroscopic observations reported by Torres et al., we derive accurate absolute masses for the components of M-1 = 2.633 +/- 0.028 M-. and M-2 = 0.5412 +/- 0.0093 M-., radii of R-1 = 7.55 +/- 0.20 R-. and R-2 = 11.02 +/- 0.21 R-., as well as effective temperatures of 5000 +/- 100 and 4640 +/- 150 K, for the primary and secondary, respectively. There are obvious signs of activity (spottedness) in the optical light curve of the binary. Our X-ray light curve clearly shows the primary eclipse but not the secondary eclipse, suggesting that the primary star is the dominant source of the activity in the system. The depth and duration of the eclipse allow us to infer some of the properties of the X-ray-emitting region around that star. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, McDonald Observ, Hobby Eberly Telescope, Ft Davis, TX 79734 USA. Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Univ Jena, Inst Astrophys, D-07445 Jena, Germany. Univ Jena, Univ Sternwarte, D-07445 Jena, Germany. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 51 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 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2003 VL 125 IS 6 BP 3237 EP 3251 DI 10.1086/375203 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684YM UT WOS:000183234100034 ER PT J AU Haverkorn, M Katgert, P de Bruyn, AG AF Haverkorn, M Katgert, P de Bruyn, AG TI Multi-frequency polarimetry of the Galactic radio background around 350 MHz - II. A region in Horologium around l=137 degrees, b=7 degrees SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; polarization; techniques : polarimetric; ISM : magnetic fields; ISM : structure; radio continuum : ISM ID GALAXY; POLARIZATION; SCALE AB We study a conspicuous ring-like structure with a radius of about 1.4degrees which was observed with the Westerbork Synthesis Radio Telescope (WSRT) at 5 frequencies around 350 MHz. This ring is very prominent in Stokes Q and U, and less so in polarized intensity P. No corresponding structure is visible in total intensity Stokes I, which indicates that the ring is created by Faraday rotation and depolarization processes. The polarization angle changes from the center of the ring outwards to a radius greater than or similar to1.7degrees. Thus, the structure in polarization angle is not ring-like but resembles a disk, and it is larger than the ring in P. The rotation measure RM decreases almost continuously over the disk, from RM approximate to 0 rad m(-2) at the edge, to -8 rad m(-2) in the center, while outside the ring the RM is slightly positive. This radial variation of RM yields stringent constraints on the nature of the ring-like structure, because it rules out any spherically symmetrical magnetic field configuration, such as might be expected from supernova remnants or wind-blown bubbles. We discuss several possible connections between the ring and known objects in the ISM, and conclude that the ring is a predominantly magnetic funnel-like structure. This description can explain both the field reversal from outside to inside the ring, and the increase in magnetic field, probably combined with an electron density increase, towards the center of the ring. The ring-structure in P is most likely caused by a lack of depolarization due to a very uniform RM distribution at that radius. Beyond the ring, the RM gradient increases, depolarizing the polarized emission, so that the polarized intensity decreases. In the southwestern corner of the field a pattern of narrow filaments of low polarization, aligned with Galactic longitude, is observed, indicative of beam depolarization due to abrupt changes in RM. This explanation is supported by the observed RM. C1 ASTRON, NL-7990 AA Dwingeloo, Netherlands. Kapteyn Inst, NL-9700 AV Groningen, Netherlands. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. EM mhaverkorn@cfa.harvard.edu; katgert@strw.leidenuniv.nl; ger@astron.nl NR 40 TC 37 Z9 37 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2003 VL 404 IS 1 BP 233 EP 247 DI 10.1051/0004-6361:20030530 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FP UT WOS:000183081300025 ER PT J AU Menard, B Hamana, T Bartelmann, M Yoshida, N AF Menard, B Hamana, T Bartelmann, M Yoshida, N TI Improving the accuracy of cosmic magnification statistics SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : gravitational lensing; cosmology : large-scale structure of Universe ID LARGE-SCALE STRUCTURE; QUASAR-GALAXY CORRELATIONS; ANGULAR-CORRELATIONS; DARK-MATTER; SHEAR; SIMULATIONS; FIELDS; HYDRA; BIAS; QSO AB The systematic magnification of background sources by the weak gravitational-lensing effects of foreground matter, also called cosmic magnification, is becoming an efficient tool both for measuring cosmological parameters and for exploring the distribution of galaxies relative to the dark matter. We extend here the formalism of magnification statistics by estimating the contribution of second-order terms in the Taylor expansion of the magnification and show that the effect of these terms was previously underestimated. We test our analytical predictions against numerical simulations and demonstrate that including second-order terms allows the accuracy of magnification-related statistics to be substantially improved. We also show, however, that both numerical and analytical estimates can provide only lower bounds to real correlation functions, even in the weak lensing regime. We propose to use count-in-cells estimators rather than correlation functions for measuring cosmic magnification since they can more easily be related to correlations measured in numerical simulations. C1 Max Planck Inst Astrophys, D-85741 Garching, Germany. Inst Astrophys Paris, F-75014 Paris, France. Natl Astron Observ Japan, Tokyo 1818588, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Menard, B (reprint author), Max Planck Inst Astrophys, POB 1317, D-85741 Garching, Germany. RI Yoshida, Naoki/A-4305-2011; Bartelmann, Matthias/A-5336-2014 NR 39 TC 34 Z9 34 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2003 VL 403 IS 3 BP 817 EP 828 DI 10.1051/0004-6361:20030406 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FE UT WOS:000183080400008 ER PT J AU Sasaki, M Pietsch, W Haberl, F AF Sasaki, M Pietsch, W Haberl, F TI XMM-Newton observations of high Mass X-ray binaries in the SMC SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : galaxies; X-rays : binaries; stars : neutron; Magellanic Clouds ID SMALL MAGELLANIC CLOUD; ROSAT OBSERVATIONS; SPECTRUM; CATALOG; PULSAR; SPECTROSCOPY; HERCULES-X-1; EMISSION; SMC-X-1; LMC-X-4 AB Based on XMM-Newton EPIC data of four pointings towards the Small Magellanic Cloud (SMC), results on timing and spectral analyses of 16 known high mass X-ray binaries (HMXBs) and HMXB candidates in the SMC are presented. We confirm the pulse periods of four sources which were known to show pulsations. In addition, two new X-ray pulsars are discovered: XMMU J005605.2-722200 with P-pulse = 140.1 +/- 0.3 s and RX J0057.8-7207 with P-pulse = 152.34 +/- 0.05 s. Due to the low Galactic foreground absorption, X-ray binary systems in the Magellanic Clouds are well suited for studies of the soft component in their X-ray spectrum. Spectral analysis reveals soft emission besides a power law component in the spectra of three sources. The existence of emission lines in at least one of them corroborates the thermal nature of this emission with temperatures of 0.2-0.3 keV and heavy element abundances lower than solar. For the HMXB SMCX-2 which was in a low luminosity state, we determine a flux upper limit of 1.5 x 10(-14) erg cm(-2) s(-1) (0.3-10.0 keV). Furthermore, two new sources (XMMU J005735.7-721932 and XMMU J010030.2-722035) with hard spectrum and emission line objects as likely optical counterparts are proposed as new X-ray binary candidates. C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msasaki@cfa.harvard.edu RI Sasaki, Manami/P-3045-2016 OI Sasaki, Manami/0000-0001-5302-1866 NR 53 TC 38 Z9 38 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2003 VL 403 IS 3 BP 901 EP 916 DI 10.1051/0004-6361:20030420 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FE UT WOS:000183080400015 ER PT J AU Haverkorn, M Katgert, P de Bruyn, AG AF Haverkorn, M Katgert, P de Bruyn, AG TI Multi-frequency polarimetry of the Galactic radio background around 350 MHz - I. A region in Auriga around l=161 degrees, b=16 degrees SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; polarization; techniques : polarimetric; ISM : magnetic fields; ISM : structure; radio continuum : ISM ID MAGNETIC-FIELD; ROTATION MEASURES; FARADAY-ROTATION; LINEAR-POLARIZATION; INTERSTELLAR-MEDIUM; INNER GALAXY; SPIRAL ARMS; SCALE; EMISSION; DENSITY AB With the Westerbork Synthesis Radio Telescope (WSRT), multi-frequency polarimetric images were taken of the diffuse radio synchrotron background in a similar to5degrees x 7degrees region centered on (l,b) = (161degrees,16degrees) in the constellation of Auriga. The observations were done simultaneously in 5 frequency bands, from 341 MHz to 375 MHz, and have a resolution of similar to5.0' x 5.0' cosec delta. The polarized intensity P and polarization angle phi show ubiquitous structure on arcminute and degree scales, with polarized brightness temperatures up to about 13 K. On the other hand, no structure at all is observed in total intensity I to an rms limit of 1.3 K, indicating that the structure in the polarized radiation must be due to Faraday rotation and depolarization mostly in the warm component of the nearby Galactic interstellar medium ( ISM). Different depolarization processes create structure in polarized intensity P. Beam depolarization creates "depolarization canals" of one beam wide, while depth depolarization is thought to be responsible for creating most of the structure on scales larger than a beam width. Rotation measures (RM) can be reliably determined, and are in the range -17 less than or similar to RM less than or similar to 10 rad m(-2) with a non-zero average RM0 approximate to -3/4 rad m(-2). The distribution of RMs on the sky shows both abrupt changes on the scales of the beam and a gradient in the direction of positive Galactic longitude of similar to1 rad m(-2) per degree. The gradient and average RM are consistent with a regular magnetic field of similar to1 muG which has a pitch angle of p = -14degrees. There are 13 extragalactic sources in the field for which RMs could be derived, and those have \RM\ less than or similar to 13 rad m(-2), with an estimated intrinsic source contribution of similar to3.6 rad m(-2). The RMs of the extragalactic sources show a gradient that is about 3 times larger than the gradient in the RMs of the diffuse emission and that is approximately in Galactic latitude. This difference is ascribed to a vastly different effective length of the line of sight. The RMs of the extragalactic sources also show a sign reversal which implies a reversal of the magnetic field across the region on scales larger than about ten degrees. The observations are interpreted in terms of a simple single-cell-size model of the warm ISM which contains gas and magnetic fields, with a polarized background. The observations are best fitted with a cell size of 10 to 20 pc and a ratio of random to regular magnetic fields B-ran/B-reg approximate to 0.7 +/- 0.5. The polarization horizon, beyond which most diffuse polarized emission is depolarized, is estimated to be at a distance of about 600 pc. C1 ASTRON, NL-7990 AA Dwingeloo, Netherlands. Univ Groningen, Kapteyn Inst, NL-9700 AV Groningen, Netherlands. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. EM mhaverkorn@cfa.harvard.edu; katgert@strw.leidenuniv.nl; ger@astron.nl NR 60 TC 48 Z9 48 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2003 VL 403 IS 3 BP 1031 EP 1044 DI 10.1051/0004-6361:20030432 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FE UT WOS:000183080400026 ER PT J AU Haverkorn, M Katgert, P de Bruyn, AG AF Haverkorn, M Katgert, P de Bruyn, AG TI Characteristics of the structure in the Galactic polarized radio background at 350 MHz SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; polarization; techniques : polarimetric; ISM : magnetic fields; ISM : structure; radio continuum : ISM ID MAGNETIC-FIELD; ROTATION MEASURES; LINEAR-POLARIZATION; INTERSTELLAR-MEDIUM; POWER SPECTRUM; INNER GALAXY; EMISSION; SYNCHROTRON; DENSITY; SCALE AB Angular power spectra and structure functions of the Stokes parameters Q and U and polarized intensity P are derived from three sets of radio polarimetric observations. Two of the observed fields have been studied at multiple frequencies, allowing determination of power spectra and structure functions of rotation measure RM as well. The third field extends over a large part of the northern sky, so that the variation of the power spectra over Galactic latitude and longitude can be studied. The power spectra of Q and U are steeper than those of P, probably because a foreground Faraday screen creates extra structure in Q and U, but not in P. The extra structure in Q and U occurs on large scales, and therefore causes a steeper spectrum. The derived slope of the power spectrum of P is the multipole spectral index alpha(P), and is consistent with earlier estimates. The multipole spectral index alpha(P) decreases with Galactic latitude (i.e. the spectrum becomes flatter), but is consistent with a constant value over Galactic longitude. Power spectra of the rotation measure RM show a spectral index alpha(RM) approximate to 1, while the structure function of RM is approximately flat. The structure function is flatter than earlier estimates from polarized extragalactic sources, which could be due to the fact that extragalactic source RM probes the complete line of sight through the Galaxy, whereas as a result of depolarization diffuse radio polarization only probes the nearby ISM. C1 ASTRON, NL-7990 AA Dwingeloo, Netherlands. Univ Groningen, Kapteyn Inst, NL-9700 AV Groningen, Netherlands. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. EM mhaverkorn@cfa.harvard.edu; ger@astron.nl NR 40 TC 38 Z9 38 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2003 VL 403 IS 3 BP 1045 EP 1057 DI 10.1051/0004-6361:20030464 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FE UT WOS:000183080400027 ER PT J AU Kurster, M Endl, M Rouesnel, F Els, S Kaufer, A Brillant, S Hatzes, AP Saar, SH Cochran, WD AF Kurster, M Endl, M Rouesnel, F Els, S Kaufer, A Brillant, S Hatzes, AP Saar, SH Cochran, WD TI The low-level radial velocity variability in Barnard's star (= GJ 699) - Secular acceleration, indications for convective redshift, and planet mass limits SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : radial velocities; stars : kinematics; stars : planetary systems; stars : activity ID SURFACE CONVECTION; MAGNETIC ACTIVITY; PROXIMA CENTAURI; LINE ASYMMETRIES; SEARCH; GRANULATION; SHIFTS; SYSTEM; ROSAT AB We report results from 2 1/2 yr of high precision radial velocity ( RV) monitoring of Barnard's star. The high RV measurement precision of the VLT-UT2+UVES of 2.65 m s(-1) made the following findings possible. ( 1) The first detection of the change in the RV of a star caused by its space motion ( RV secular acceleration). ( 2) An anti-correlation of the measured RV with the strength of the filling-in of the H-alpha line by emission. ( 3) Very stringent mass upper limits to planetary companions. Using only data from the first 2 years, we obtain a best-fit value for the RV secular acceleration of 5.15 +/- 0.89 m s(-1) yr(-1). This agrees within 0.95sigma with the predicted value of 4.50 m s(-1) yr(-1) based on the Hipparcos proper motion and parallax combined with the known absolute radial velocity of the star. When the RV data of the last half-year are added the best-fit slope is strongly reduced to 2.97 +/- 0.51 m s(-1) yr(-1) (3.0sigma away from the predicted value), clearly suggesting the presence of additional RV variability in the star. Part of it can be attributed to stellar activity as we demonstrate by correlating the residual RVs with an index that describes the filling-in of the H-alpha line by emission. A correlation coefficient of -0.50 indicates that the appearance of active regions causes a blueshift of photospheric absorption lines. Assuming that active regions basically inhibit convection we discuss the possibility that the fundamental ( inactive) convection pattern in this M4V star produces a convective redshift which would indicate that the majority of the absorption lines relevant for our RV measurements is formed in a region of convective overshoot. This interpretation could possibly extend a trend indicated in the behaviour of earlier spectral types that exhibit convective blueshift, but with decreasing line asymmetries and blueshifts as one goes from G to K dwarfs. Based on this assumption, we estimate that the variation of the visible plage coverage is about 20%. We also determine upper limits to the projected mass m sin i and to the true mass m of hypothetical planetary companions in circular orbits. For the separation range 0.017-0.98 AU we exclude any planet with m sin i > 0.12 M-Jupiter and m > 0.86 M-Jupiter. Throughout the habitable zone around Barnard's star, i.e. 0.034-0.082 AU, we exclude planets with m sin i > 7.5 M-Earth and m > 3.1 M-Neptune. C1 Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Paris 11, F-91405 Orsay, France. Isaac Newton Grp Telescopes, Santa Cruz De La Palma 38700, Canary Islands, Spain. European So Observ, Santiago 19, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurster, M (reprint author), Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. NR 47 TC 76 Z9 77 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2003 VL 403 IS 3 BP 1077 EP 1087 DI 10.1051/0004-6361:20030396 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FE UT WOS:000183080400030 ER PT J AU Soker, N David, LP AF Soker, N David, LP TI Observed non-steady state cooling and the moderate cluster cooling flow model SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; intergalactic medium; X-rays : galaxies : clusters ID HYDRA-A CLUSTER; CHANDRA X-RAY; FEEDBACK; GALAXIES; CORES; GAS AB We examine recent developments in the cluster cooling flow scenario following recent observations by Chandra and XMM-Newton. We show that the distribution of gas emissivity versus temperature determined by XMM-Newton gratings observations demonstrates that the central gas, when the cooling time is less than the age of the cluster, in cooling flow clusters cannot be in simple steady state; i.e., (M)over dot is not a constant at all temperatures. On the basis of the measured gas emissivity, the gas can be in steady state only if there exists a steady heating mechanism that scales as H(T) proportional to T-alpha, where alpha = 1-2. A heating mechanism that preferentially targets the hottest and highest entropy gas seems very unlikely. Combining this result with the lack of spectroscopic evidence for gas below one-third of the ambient cluster temperature is strong evidence that the gas is heated intermittently. While the old steady state isobaric cooling flow model is incompatible with recent observations, a moderate cooling flow model in which the gas undergoes intermittent heating that effectively reduces the age of a cooling flow is consistent with observations. Most of the gas within cooling flows resides in the hottest gas, which is prevented from cooling continuously and attaining a steady state configuration. This results in a mass cooling rate that decreases with decreasing temperature, with a much lower mass cooling rate at the lowest temperatures. Such a temperature-dependent (M)over dot is required by the XMM-Newton RGS data and will produce an increasing amount of intermediate-temperature gas that will then be reheated during the next heating cycle. We show the compatibility of this model with the cooling flow cluster A2052. This paper strengthens the moderate cooling flow model, which can accommodate the unique activities observed in cooling flow clusters. C1 Oranim, Dept Phys, IL-36006 Tivon, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Soker, N (reprint author), Oranim, Dept Phys, IL-36006 Tivon, Israel. NR 25 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 JUN 1 PY 2003 VL 589 IS 2 BP 770 EP 773 DI 10.1086/374815 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 681NX UT WOS:000183043200009 ER PT J AU Marengo, M Karovska, M Sasselov, DD Papaliolios, C Armstrong, JT Nordgren, TE AF Marengo, M Karovska, M Sasselov, DD Papaliolios, C Armstrong, JT Nordgren, TE TI Theoretical limb darkening for classical Cepheids. II. Corrections for the geometric Baade-Wesselink method SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; stars : atmospheres; stars : individual (zeta Geminorum) stars : oscillations; techniques : interferometric ID FUNDAMENTAL PARAMETERS; LINE; STAR AB The geometric Baade-Wesselink method is one of the most promising techniques for obtaining a better calibration of the Cepheid period-luminosity relation by means of interferometric measurements of accurate diameters. In this paper we present new wavelength- and phase-dependent limb-darkening (LD) corrections based on our time-dependent hydrodynamic models of the classical Cepheid zeta Gem. We show that a model simulation of a Cepheid atmosphere, taking into account the hydrodynamic effects associated with the pulsation, shows strong departures from the LD otherwise predicted by a static model. For most of its pulsational cycle the hydrodynamic model predicts a larger LD than the equivalent static model. The hydrodynamics affects the LD mainly at UV and optical wavelengths. Most of these effects evolve slowly as the star pulsates, but there are phases, associated with shocks propagating into the photosphere, in which significant changes in the LD take place on timescales of the order of less than a day. We assess the implication of our model LD corrections fitting the geometric Baade-Wesselink distance of zeta Gem for the available near-IR PTI data. We discuss the effects of our model LD on the best-fit result and analyze the requirements needed to test the time dependence of the LD with future interferometric measurements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. Univ Redlands, Dept Phys, Redlands, CA 92373 USA. RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2003 VL 589 IS 2 BP 968 EP 975 DI 10.1086/374736 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 681NX UT WOS:000183043200028 ER PT J AU Israel, GL Covino, S Perna, R Mignani, R Stella, L Campana, S Marconi, G Bono, G Mereghetti, S Motch, C Negueruela, I Oosterbroek, T Angelini, L AF Israel, GL Covino, S Perna, R Mignani, R Stella, L Campana, S Marconi, G Bono, G Mereghetti, S Motch, C Negueruela, I Oosterbroek, T Angelini, L TI The infrared counterpart to the anomalous X-ray pulsar 1RXS J170849-400910 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; pulsars : general; pulsars : individual (1RXS J170849-400910); stars : neutron; X-rays : stars ID MAGNETIZED NEUTRON-STARS; FALLBACK DISKS; EXTINCTION; REPEATERS; EMISSION; BURSTS; MODEL; MASS AB We report the discovery of the likely IR counterpart to the anomalous X-ray pulsar (AXP) 1RXS J170849-400910 based on the Chandra High Resolution Camera (imaging detector) X-ray position and the deep optical/IR observations carried out from ESO telescopes and the Canada-France-Hawaii Telescope during 1999-2002. Within the narrow uncertainty region, we found two relatively faint (K' = 20.0 and K' = 17.53) IR objects. Based on their color and position in the J-K' versus J-H diagram, only the brighter object is consistent with the known IR properties of the counterparts to other AXPs. No variability was detected for this source, which is similar to what is observed in the case of 4U 0142+614. Like in other AXPs, we found that the IR flux of 1RXS J170849-400910 is higher than expected for a simple blackbody component extrapolated from the X-ray data. If confirmed, this object would be the fourth IR counterpart to a source of the AXP class and would make the IR excess a likely new characteristic of AXPs. C1 Osserv Astron Roma, INAF, I-00040 Rome, Italy. Osserv Astron Brera, INAF, I-23807 Merate, Lc, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. European So Observ, Santiago 19, Chile. CNR, IASF, Sez Milano G Occhialini, I-20133 Milan, Italy. Observ Strasbourg, F-67000 Strasbourg, France. Univ Alicante, Dept Fis Ingn Sistemas & Teor Senales, E-03080 Alicante, Spain. European Space Agcy, European Space Res & Technol Ctr, Dept Astrophys, NL-2200 AG Noordwijk, Netherlands. NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Israel, GL (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Rome, Italy. RI Negueruela, Ignacio/L-5483-2014; OI Negueruela, Ignacio/0000-0003-1952-3680; MEREGHETTI, SANDRO/0000-0003-3259-7801; Israel, GianLuca/0000-0001-5480-6438; Covino, Stefano/0000-0001-9078-5507 NR 36 TC 44 Z9 44 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2003 VL 589 IS 2 BP L93 EP L96 DI 10.1086/375832 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 681NZ UT WOS:000183043400009 ER PT J AU Aguilar, A Covington, AM Hinojosa, G Phaneuf, RA Alvarez, I Cisneros, C Bozek, JD Dominguez, I Sant'Anna, MM Schlachter, AS Nahar, SN McLaughlin, BM AF Aguilar, A Covington, AM Hinojosa, G Phaneuf, RA Alvarez, I Cisneros, C Bozek, JD Dominguez, I Sant'Anna, MM Schlachter, AS Nahar, SN McLaughlin, BM TI Absolute photoionization cross section measurements of O II ions from 29.7 to 46.2 eV SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic data; atomic processes; methods : laboratory ID OSCILLATOR-STRENGTHS; ATOMIC DATA; K+ IONS; ULTRAVIOLET; THRESHOLD; OXYGEN; STATE; RECOMBINATION; NITROGEN AB Absolute photoionization cross sections have been measured for a mixture of ground-state and metastable O II (O+) ions at photon energies ranging from 29.9 to 46.0 eV (414.7 to 269.5 Angstrom). All measurements were performed by merging an O+ beam with synchrotron radiation from an undulator beam line at the Advanced Light Source (ALS). At a resolution of 17 meV, more than 70 spectral features have been resolved, most of them identified and characterized. These measurements are compared with two independent R-matrix calculations and the data in TOPbase. All three calculations agree within 25% on the direct photoionization cross section, and with the absolute measurements within 40%. Some differences are noted in the predicted resonance positions among the three close-coupling R-matrix calculations, the TOPbase data being the least accurate. The estimated total experimental uncertainty varies from 15% to 20%. Such measurements benchmark theoretical photoionization cross section calculations performed within the framework of the Opacity Project and the Iron Project. C1 Univ Nevada, Dept Phys, Reno, NV 89557 USA. Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico. Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Aguilar, A (reprint author), Univ Nevada, Dept Phys, Reno, NV 89557 USA. RI Bozek, John/E-4689-2010; Sant'Anna, Marcelo/B-9355-2013; Bozek, John/E-9260-2010; Dominguez-Lopez, Ivan/B-6072-2016 OI Sant'Anna, Marcelo/0000-0001-5342-5799; Bozek, John/0000-0001-7486-7238; Dominguez-Lopez, Ivan/0000-0001-8084-8711 NR 34 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2003 VL 146 IS 2 BP 467 EP 477 DI 10.1086/368077 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 680ZP UT WOS:000183010200010 ER PT J AU Smith, AR Weislo, WT O'Donnell, S AF Smith, AR Weislo, WT O'Donnell, S TI Assured fitness returns favor sociality in a mass-provisioning sweat bee, Megalopta genalis (Hymenoptera : Halictidae) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE assured fitness returns; social evolution; ant predation; brood defense ID RUBICUNDUS HYMENOPTERA; LATITUDINAL GRADIENT; ALLODAPINE BEE; EVOLUTION; EUSOCIALITY; SOLITARY; ABUNDANCE; INSURANCE; PREDATION; ADVANTAGE AB Assured fitness returns models for the evolution of sociality emphasize the selective value of ensuring that offspring receive adequate parental care to reach maturity. If a member of a social group dies, it can accrue returns on investment in offspring through the efforts of surviving social partners. We provide evidence that in the mass-provisioning, facultatively social sweat bee Megalopta genalis, adult presence in the nest throughout brood development provides protection from ant predation. Nests with adults present were well protected, and brood in nests with adults removed suffered higher predation. Females in observation nests showed effective defensive behavior against experimentally introduced ants, and bees in natural nests repulsed naturally occurring ant raids. Megalopta nest architecture and behavior are such that the brood of several cooperating females can be defended with little additional cost relative to solitary nesting. The benefits of cooperative defense may favor group living in mass provisioning bees. Our observations and experiments suggest that parental care throughout brood development can be adaptive in mass provisioning species, supporting the predictions of assured fitness returns models. C1 Smithsonian Trop Res Inst, Unit 0948, APO AA, Panama City, FL 34002 USA. RP Smith, AR (reprint author), Univ Washington, Dept Psychol, Anim Behav Area, Seattle, WA 98195 USA. NR 52 TC 41 Z9 41 U1 0 U2 12 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD JUN PY 2003 VL 54 IS 1 BP 14 EP 21 DI 10.1007/s00265-003-0589-0 PG 8 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 698BU UT WOS:000183978400003 ER PT J AU Weiss, JV Emerson, D Backer, SM Megonigal, JP AF Weiss, JV Emerson, D Backer, SM Megonigal, JP TI Enumeration of Fe(II)-oxidizing and Fe(III)-reducing bacteria in the root zone of wetland plants: Implications for a rhizosphere iron cycle SO BIOGEOCHEMISTRY LA English DT Article DE Fe(II)-oxidizing bacteria; Fe(III)-reducing bacteria; rhizosphere; wetland ID FE(III) OXIDE REDUCTION; FERRIC HYDROXIDE PLAQUE; TYPHA-LATIFOLIA L; RICE ROOTS; OXIDIZING BACTERIA; METHANE OXIDATION; DENITRIFYING BACTERIA; PHRAGMITES-AUSTRALIS; AQUATIC SEDIMENTS; REDUCING BACTERIA AB Iron plaque occurs on the roots of most wetland and submersed aquatic plant species and is a large pool of oxidized Fe(III) in some environments. Because plaque formation in wetlands with circumneutral pH has been largely assumed to be an abiotic process, no systematic effort has been made to describe plaque-associated microbial communities or their role in plaque deposition. We hypothesized that Fe(II)-oxidizing bacteria (FeOB) and Fe(III)-reducing bacteria (FeRB) are abundant in the rhizosphere of wetland plants across a wide range of biogeochemical environments. In a survey of 13 wetland and aquatic habitats in the Mid-Atlantic region, FeOB were present in the rhizosphere of 92% of the plant specimens collected (n = 37), representing 25 plant species. In a subsequent study at six of these sites, bacterial abundances were determined in the rhizosphere and bulk soil using the most probable number technique. The soil had significantly more total bacteria than the roots on a dry mass basis (1.4 x 10(9) cells/g soil vs. 8.6 x 10(7) cells/g root; p < 0.05). The absolute abundance of aerobic, lithotrophic FeOB was higher in the soil than in the rhizosphere (3.7 x 10(6)/g soil vs. 5.9 x 10(5)/g root; p < 0.05), but there was no statistical difference between these habitats in terms of relative abundance (similar to1% of the total cell number). In the rhizosphere, FeRB accounted for an average of 12% of all bacterial cells while in the soil they accounted for <1% of the total bacteria. We concluded that FeOB are ubiquitous and abundant in wetland ecosystems, and that FeRB are dominant members of the rhizosphere microbial community. These observations provide a strong rationale for quantifying the contribution of FeOB to rhizosphere Fe(II) oxidation rates, and investigating the combined role of FeOB and FeRB in a rhizosphere iron cycle. C1 George Mason Univ, Environm Sci & Policy Dept, Fairfax, VA 22030 USA. Amer Type Culture Collect, Manassas, VA 22010 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. NR 63 TC 95 Z9 109 U1 9 U2 66 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD JUN PY 2003 VL 64 IS 1 BP 77 EP 96 DI 10.1023/A:1024953027726 PG 20 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 705UJ UT WOS:000184413200004 ER PT J AU Heyer, WR AF Heyer, WR TI Ultraviolet-B and amphibia SO BIOSCIENCE LA English DT Editorial Material C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20012 USA. RP Heyer, WR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, MRC 162,POB 37012, Washington, DC 20012 USA. NR 4 TC 6 Z9 6 U1 0 U2 1 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 JUN PY 2003 VL 53 IS 6 BP 540 EP 541 DI 10.1641/0006-3568(2003)053[0540:UAA]2.0.CO;2 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 687BA UT WOS:000183354900002 ER PT J AU Elias, M Potvin, C AF Elias, M Potvin, C TI Assessing inter- and intra-specific variation in trunk carbon concentration for 32 neotropical tree species SO CANADIAN JOURNAL OF FOREST RESEARCH-REVUE CANADIENNE DE RECHERCHE FORESTIERE LA English DT Article ID WOOD SPECIFIC-GRAVITY; TROPICAL FORESTS; BIOMASS; STORAGE; GROWTH; PLANTATIONS; CYCLE; SINKS AB Trunk carbon (C) concentrations were assessed for 32 species of tropical trees to understand sources of variation. The main effect of species accounted for 38% of the total variance in C concentration (p < 0.0001). Tectona grandis demonstrated the greatest C concentration (49.4%), while Ormosia macrocalyx displayed the lowest C concentration (44.4%). We also observed significant differences among the sampling sites (F = 2.2, p < 0.02). For three of the species sampled in both plantations and natural forests, the natural forest individuals had significantly higher C concentrations (Dipteryx panamensis: F = 6.10, p = 0.06; Hura crepitans: F = 5.53, p = 0.06; and Miconia argentea: F = 8.92, p = 0.02). C concentration was highly correlated with wood specific gravity (r(2) = 0.86). A canonical correspondence analysis was performed to identify the environmental and (or) growth factors explaining variation in trunk C concentration. The two factors with the highest loading values on the first canonical axis are site and diameter at breast height (DBH), while DBH and density load on axis 2. The biplot shows that species respond differently to environmental factors. Our results suggest that a better consideration of interspecific variation in C concentration could reduce the error associated with estimates of C sequestration by up to 10%. C1 McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Potvin, C (reprint author), McGill Univ, Dept Biol, 1205 Ave Dr Penfield, Montreal, PQ H3A 1B1, Canada. NR 35 TC 54 Z9 65 U1 0 U2 16 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0045-5067 J9 CAN J FOREST RES JI Can. J. For. Res.-Rev. Can. Rech. For. PD JUN PY 2003 VL 33 IS 6 BP 1039 EP 1045 DI 10.1139/X03-018 PG 7 WC Forestry SC Forestry GA 685JQ UT WOS:000183259800008 ER PT J AU Pontailler, JY Hymus, GJ Drake, BG AF Pontailler, JY Hymus, GJ Drake, BG TI Estimation of leaf area index using ground-based remote sensed NDVI measurements: validation and comparison with two indirect techniques SO CANADIAN JOURNAL OF REMOTE SENSING LA English DT Article ID VEGETATION; RED; FOREST; REFLECTANCE; INSTRUMENT AB This study took place in an evergreen scrub oak ecosystem in Florida. Vegetation reflectance was measured in situ with a laboratory-made sensor in the red (640-665 nm) and near-infrared (750-950 nm) bands to calculate the normalized difference vegetation index (NDVI) and derive the leaf area index (LAI). LAI estimates from this technique were compared with two other nondestructive techniques, intercepted photosynthetically active radiation (PAR) and hemispherical photographs, in four contrasting 4 m(2) plots in February 2000 and two 4 m(2) plots in June 2000. We used Beer's law to derive LAI from PAR interception and gap fraction distribution to derive LAI from photographs. The plots were harvested manually after the measurements to determine a "true" LAI value and to calculate a light extinction coefficient (k). The technique based on Beer's law was affected by a large variation of the extinction coefficient, owing to the larger impact of branches in winter when LAI was low. Hemispherical photographs provided satisfactory estimates, slightly overestimated in winter because of the impact of branches or underestimated in summer because of foliage clumping. NDVI provided the best fit, showing only saturation in the densest plot (LAI = 3.5). We conclude that in situ measurement of NDVI is an accurate and simple technique to nondestructively assess LAI in experimental plots or in crops if saturation remains acceptable. C1 Univ Paris Sud 11, CNRS, UMR 8079, Syst & Evolut ESE,Lab Ecol,Dept Ecophysiol Vegeta, F-91405 Orsay, France. Smithsonian Environm Res Ctr, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. RP Pontailler, JY (reprint author), Univ Paris Sud 11, CNRS, UMR 8079, Syst & Evolut ESE,Lab Ecol,Dept Ecophysiol Vegeta, Bat 362, F-91405 Orsay, France. NR 24 TC 22 Z9 22 U1 0 U2 9 PU CANADIAN AERONAUTICS SPACE INST PI OTTAWA PA 1685 RUSSELL RD, UNIT 1-R, OTTAWA, ON K1G 0N1, CANADA SN 0703-8992 J9 CAN J REMOTE SENS JI Can. J. Remote Sens. PD JUN PY 2003 VL 29 IS 3 BP 381 EP 387 PG 7 WC Remote Sensing SC Remote Sensing GA 686YZ UT WOS:000183349700009 ER PT J AU Lidgard, DC Boness, DJ Bowen, WD McMillan, JI AF Lidgard, DC Boness, DJ Bowen, WD McMillan, JI TI Diving behaviour during the breeding season in the terrestrially breeding male grey seal: implications for alternative mating tactics SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID LAND-FAST ICE; HALICHOERUS-GRYPUS; GRAY SEALS; REPRODUCTIVE-BEHAVIOR; HARBOR SEAL; FORAGING BEHAVIOR; PHOCA-VITULINA; SABLE ISLAND; NORTH RONA; SUCCESS AB We examined the diving behaviour of breeding male grey seals (Halichoerus grypus) at Sable Island, Nova Scotia, from 1997 to 2001. The proportion of time spent at sea varied between 0 and 78% (N=30). Males engaged in deep (43.4+/-3.3 m (mean+/-SE), N=27) diving, and these dives were clustered into bouts, which mostly occurred during long trips (62.2+/-14.7 h). We suggest that males spent time foraging during deep dives. Shallow diving (5.9+/-0.1 m, N=27) accounted for 40.8% of dives, which were also clustered into bouts that mostly occurred during short trips (2.1+/-0.37 h). We suggest that shallow diving comprised a suite of behaviours, but included little foraging behaviour. Phenotypic traits had little influence on diving behaviour. Further work is required to understand the extent to which foraging behaviour enhances reproductive success, and whether shallow diving is a component of the mating tactics of male grey seals at Sable Island. C1 Univ La Rochelle, Lab Biol & Environm Marins, F-17000 La Rochelle, France. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Fisheries & Oceans Canada, Bedford Inst Oceanog, Marine Fish Div, Dartmouth, NS B2Y 4A2, Canada. RP Lidgard, DC (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Bowen, William/D-2758-2012 NR 45 TC 5 Z9 5 U1 3 U2 10 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 JUN PY 2003 VL 81 IS 6 BP 1025 EP 1033 DI 10.1139/Z03-085 PG 9 WC Zoology SC Zoology GA 711AG UT WOS:000184714500010 ER PT J AU Mawdsley, JR AF Mawdsley, JR TI The importance of species of Dasytinae (Coleoptera : Melyridae) as pollinators in western North America SO COLEOPTERISTS BULLETIN LA English DT Article ID BEETLE POLLINATION; FRENCH-GUIANA; SCARABAEIDAE; MALAYSIA; SARAWAK; FLOWERS; ARACEAE; AFRICA AB Species of 11 families of Coleoptera are known to pollinate flowering plants. In western North America, the 300+ species of the beetle subfamily Dasytinae (Coleoptera: Melyridae) are commonly found on flowers, where adults feed on both nectar and pollen. The dense setae and pubescence of adult dasytines often trap pollen grains, which are transported to other flowers during the course of normal adult feeding. Adults of many dasytine species are abundant, and may form large feeding aggregations. A preliminary list is presented of plant species on whose flowers or pollen cones adult dasytines have been collected, based on literature records and museum specimen labels. These plant species represent 68 genera in 26 families, and include species grown as food crops and species that are important browse or forage plants for livestock and wildlife. At least two plant species, both in the family Polemoniaceae, rely predominantly on species of Dasytinae for pollination. C1 Smithsonian Inst, Sect Entomol, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Mawdsley, JR (reprint author), Smithsonian Inst, Sect Entomol, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 31 TC 7 Z9 10 U1 1 U2 9 PU COLEOPTERISTS SOC PI NATCHEZ PA PO BOX 767, NATCHEZ, MS 39121 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD JUN PY 2003 VL 57 IS 2 BP 154 EP 160 DI 10.1649/541 PG 7 WC Entomology SC Entomology GA 693UL UT WOS:000183736700010 ER PT J AU Petit, LJ Petit, DR AF Petit, LJ Petit, DR TI Evaluating the importance of human-modified lands for neotropical bird conservation SO CONSERVATION BIOLOGY LA English DT Article ID SHADE COFFEE; BIODIVERSITY; COMMUNITIES; CHIAPAS; FOREST; PANAMA; MEXICO AB Development of effective conservation plans for terrestrial animals will require some assessment of which human-modified and natural habitats can support populations of priority species. We examined bird communities associated with 11 natural and human-modified habitats in Panama and assessed the importance of those habitats for species of different vulnerability to disturbance. We calculated habitat importance scores using both relative habitat preferences and vulnerability scores for all species present. Species of moderate and high vulnerability were primarily those categorized as forest specialists or forest generalists. As expected, even species-rich nonforest habitats provided little conservation value for the most vulnerable species. However, shaded coffee plantations and gallery forest corridors were modified habitats with relatively high conservation value. Sugar cane fields and Caribbean pine plantations offered virtually no conservation value for birds. Our method of assessing the conservation importance of different habitats is useful because it considers the types of species present and the potential role of the habitat in the conservation of those species (i.e., habitat preference). This method of habitat evaluation could be tailored to other conservation contexts with any measure of species vulnerability desired. C1 Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. US Geol Survey, Biol Resources Div, Reston, VA 20192 USA. RP Petit, LJ (reprint author), Cuyahoga Valley Natl Pk, Natl Pk Serv, 15610 Vaughn Rd, Brecksville, OH 44141 USA. NR 35 TC 74 Z9 79 U1 2 U2 34 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD JUN PY 2003 VL 17 IS 3 BP 687 EP 694 DI 10.1046/j.1523-1739.2003.00124.x PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 682EF UT WOS:000183077800012 ER PT J AU Kuchner, MJ AF Kuchner, MJ TI Planetary perturbers in debris disks SO EARTH MOON AND PLANETS LA English DT Article ID EDGEWORTH-KUIPER BELT; CIRCUMSTELLAR DUST DISK; SOLAR-SYSTEM DUST; BETA-PICTORIS; GIANT PLANETS; RING; SIGNATURES; RESONANCE; JUPITER; PERTURBATIONS AB Neptune dominates the dynamics of the Kuiper Belt. By examining images of debris disks around other stars, we may be able to infer what kinds of planets shape the outer edges of other planetary systems. The last few years have seen a burst of progress in the modeling of azimuthal structures in debris disks created by planetary perturbers; new models incorporate planets on substantially eccentric orbits. I review this recent progress in debris disk dynamics and discuss the Kuiper Belt as a key example. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kuchner, MJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Kuchner, Marc/E-2288-2012 NR 47 TC 1 Z9 1 U1 1 U2 3 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD JUN PY 2003 VL 92 IS 1-4 BP 435 EP 445 DI 10.1023/B:MOON.0000031957.71828.d3 PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 829OD UT WOS:000222057600037 ER PT J AU Zhu, RX An, ZS Potts, R Hoffman, KA AF Zhu, RX An, ZS Potts, R Hoffman, KA TI Magnetostratigraphic dating of early humans in China SO EARTH-SCIENCE REVIEWS LA English DT Article DE magnetic stratigraphy; China; human fossil remains; stone artifacts; early Pleistocene; paleolithic ID PALEOMAGNETIC DATES; EARLY HOMO; HOMINID; AGE; DMANISI; GEORGIA; BASIN; SITES; ASIA; INDONESIA AB China is a key area for research into human occupation in the Old World after the initial expansion of early humans out of Africa. Reliable age determinations are pivotal for assessing the patterns of human evolution and dispersal in this region. This paper reviews magnetostratigraphic studies of some early Pleistocene strata bearing hominin remains and/or artifact stone tools from northern to southern China. The quality and reliability of the paleomagnetic dates are also evaluated. New magnetostratigraphic results for the Xihoudu Paleolithic site in north-central China are also presented. Among the few hominin or Paleolithic sites in China from the early Pleistocene, five have been well investigated. Three of these are in northern China at Xiaochangliang, Donggutuo and Gongwangling; the remaining two in southern China at Longgupo and Yuanmou. Considerable progress has been made during the past three decades towards paleomagnetically dating these sites. Indeed, the age estimates at Xiaochangliang and Gongwangling have been widely accepted. Magnetostratigraphic consensus about the age of the Donggutuo site has also been reached. However, the age determination for the two sites in southern China is still contested. The integration of rock-magnetic stratigraphy with magnetic polarity stratigraphy has resulted in a determined age of 1.36 Ma for a stone tool-containing layer of lacustrine sediments at the Xiaochangliang site in the Nihewan Basin. Lithostratigraphic constraints have significantly contributed to determining the age of Lantian Homo erectus at Gongwangling, which occurred in a loess-paleosol sequence of the southern Loess Plateau. Its age, paleomagnetically derived, is about 1.15 Ma. These two paleomagnetic ages suggest an expansion and flourishing of human groups from northern to north-central China during the early Pleistocene. This suggestion has been reinforced by our new magnetostratigraphic age estimate of about 1.27 Ma for the Xihoudu site as will be presented in this paper. However, more work is needed for the age determinations of the hominin-bearing strata at the Longgupo and Yuanmou sites in southern China. Finally, we stress that it is necessary to combine biostratigraphy, lithostratigraphy and rock-magnetic stratigraphy with the traditional magnetic polarity stratigraphy in order to obtain reliable age determinations for strata bearing hominin remains or stone artifacts. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Chinese Acad Sci, Inst Geol & Geophys, Paleomagnetism Lab, Beijing 100029, Peoples R China. Chinese Acad Sci, Inst Earth Environm, Xian 710054, Peoples R China. Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. California Polytech STate Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93410 USA. RP Zhu, RX (reprint author), Chinese Acad Sci, Inst Geol & Geophys, Paleomagnetism Lab, POB 9825, Beijing 100029, Peoples R China. RI AN, Zhisheng/F-8834-2012 NR 80 TC 91 Z9 125 U1 5 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-8252 J9 EARTH-SCI REV JI Earth-Sci. Rev. PD JUN PY 2003 VL 61 IS 3-4 BP 341 EP 359 DI 10.1016/S0012-8252(02)00132-0 PG 19 WC Geosciences, Multidisciplinary SC Geology GA 687UB UT WOS:000183394400004 ER PT J AU Rappole, JH King, DI Diez, J AF Rappole, JH King, DI Diez, J TI Winter- vs. breeding-habitat limitation for an endangered avian migrant SO ECOLOGICAL APPLICATIONS LA English DT Article DE avian migrant; breeding habitat; Dendroica chrysoparia; endangered species; Golden-cheeked Warbler; habitat limitation; population limitation; remote sensing; winter habitat ID WARBLERS; BIRDS AB Migratory species have critical habitat needs during both breeding and wintering portions of the life cycle. Recent advances have made it possible to use satellite imagery and computer-assisted spatial analysis technology along with fieldwork to determine estimates for these critical habitat needs for the endangered Golden-cheeked Warbler, Dendroica chrysoparia. Using these procedures, we estimate that the Ashe juniper-oak breeding habitat for this species covers 6430 km(2) of central Texas, USA, whereas appropriate habitat in the known winter range covers 6750 km(2) of the Middle American cordillera. When combined with information on warbler breeding and wintering ecology, these figures indicate that the amount of available winter habitat (pine-oak above 1219 m [4000'] in elevation) supports only a fraction (15%) of the population that could be supported by the amount of estimated available breeding habitat, suggesting that Golden-cheeked Warbler populations could be limited by winter habitat availability. C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Massachusetts, Holdsworth Nat Resources Ctr 203, US Forest Serv, NE Expt Stn, Amherst, MA 01003 USA. Univ Georgia, Inst Ecol, Athens, GA 30602 USA. RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 26 TC 30 Z9 33 U1 0 U2 17 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 JUN PY 2003 VL 13 IS 3 BP 735 EP 742 DI 10.1890/1051-0761(2003)013[0735:WVBLFA]2.0.CO;2 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 707TA UT WOS:000184524900013 ER PT J AU Liu, AZ Kress, WJ Long, CL AF Liu, AZ Kress, WJ Long, CL TI The ethnobotany of Musella lasiocarpa (Musaceae), an endemic plant of southwest China. SO ECONOMIC BOTANY LA English DT Article C1 Chinese Acad Sci, Kunming Inst Bot, Kunming 650204, Peoples R China. Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, MRC 166, Washington, DC 20013 USA. RP Liu, AZ (reprint author), Chinese Acad Sci, Kunming Inst Bot, Kunming 650204, Peoples R China. RI Liu, aizhong/F-1770-2010; OI Long, Chunlin/0000-0002-6573-6049 NR 10 TC 8 Z9 11 U1 0 U2 3 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0013-0001 J9 ECON BOT JI Econ. Bot. PD SUM PY 2003 VL 57 IS 2 BP 279 EP 281 DI 10.1663/0013-0001(2003)057[0279:TEOMLM]2.0.CO;2 PG 3 WC Plant Sciences SC Plant Sciences GA 710EA UT WOS:000184666800010 ER PT J AU King, RS Richardson, CJ AF King, RS Richardson, CJ TI Integrating bioassessment and ecological risk assessment: An approach to developing numerical water-quality criteria SO ENVIRONMENTAL MANAGEMENT LA English DT Article DE biological assessment; ecological thresholds; everglades; Index of Biological integrity; macroinvertebrates; nutrients; phosphorus; risk assessment; wetlands ID BIOTIC INTEGRITY; STREAMS; EVERGLADES; LIMITATION; ENRICHMENT; PERIPHYTON; COMMUNITY; NUTRIENTS; GRADIENT; WETLANDS AB ioassessment is used worldwide to monitor aquatic health but is infrequently used with risk-assessment objectives, such as supporting the development of defensible, numerical water-quality criteria, To this end, we present a generalized approach for detecting potential ecological thresholds using assemblage-level attributes and a multimetric index (Index of Biological Integrity-IBI) as endpoints in response to numerical changes in water quality. To illustrate the approach, we used existing macroinvertebrate and surface-water total phosphorus (TP) datasets from an observed P gradient and a P-dosing experiment in wetlands of the south Florida coastal plain nutrient ecoregion. Ten assemblage attributes were identified as potential metrics using the observational data, and five were validated in the experiment. These five core metrics were subjected individually and as an aggregated Nutrient-IBI to nonparametric changepoint analysis (nCPA) to estimate cumulative probabilities of a threshold response to TP. Threshold responses were evident for all metrics and the IBI, and were repeatable through time. Results from the observed gradient indicated that a threshold was greater than or equal to50% probable between 12.6 and 19.4 mug/L TP for individual metrics and 14.8 mug/L TP for the IBI. Results from the P-dosing experiment revealed greater than or equal to50% probability of a response between 11.2 and 13.0 mug/L TP for the metrics and 12.3 mug/L TIP for the IBI. Uncertainty analysis indicated a low (typically greater than or equal to5%) probability that an IBI threshold occurred at less than or equal to 10 mug/L TP, while there was greater than or equal to95% certainty that the threshold was less than or equal to 17 mug/L TP. The weight-of-evidence produced from these analyses implies that a TP concentration > 12-15 mug/L is likely to cause degradation of macroinvertebrate assemblage structure and function, a reflection of biological integrity, in the study area. This finding may assist in the development of a numerical water-quality criterion for TP in this ecoregion, and illustrates the utility of bioassessment to environmental decision-making. C1 Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA. RP King, RS (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,Box 28, Edgewater, MD 21037 USA. NR 62 TC 74 Z9 80 U1 6 U2 42 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0364-152X J9 ENVIRON MANAGE JI Environ. Manage. PD JUN PY 2003 VL 31 IS 6 BP 795 EP 809 DI 10.1007/s00267-002-0036-4 PG 15 WC Environmental Sciences SC Environmental Sciences & Ecology GA 711AK UT WOS:000184714800010 PM 14565699 ER PT J AU Castro, MS Driscoll, CT Jordan, TE Reay, WG Boynton, WR AF Castro, MS Driscoll, CT Jordan, TE Reay, WG Boynton, WR TI Sources of nitrogen to estuaries in the United States SO ESTUARIES LA English DT Article ID COASTAL EUTROPHICATION; CHESAPEAKE BAY; ATMOSPHERIC DEPOSITION; NUTRIENTS; DENITRIFICATION; GROUNDWATER; TEMPERATURE; TRANSPORT; BUDGETS; BLOOMS AB The purpose of this study was to quantify the nitrogen (N) inputs to 34 estuaries on the Atlantic and Gulf Coasts of the United States. Total nitrogen (TN) inputs ranged from 1 kg N ha(-1) yr(-1) for Upper Laguna Madre, Texas, to 49 kg N ha(-1) yr(-1) for Massachusetts Bay, Massachusetts. TN inputs to 11 of the 34 estuaries were dominated by urban N sources (point sources and septic systems) and nonpoint source N runoff (5% of total); point sources accounted for 36-86% of the TN inputs to these 11 urban-dominated estuaries. TN inputs to 20 of the 34 estuaries were dominated by agricultural N sources; N fertilization was the dominant source (46% of the total), followed by manure (32% of the total) and N fixation by crops (16% of the total). Atmospheric deposition (runoff from watershed plus direct deposition to the surface of the estuary) was the dominant N source for three estuaries (Barnegat Bay, New Jersey: 64%; St. Catherines-Sapelo, Georgia: 72%; and Barataria Bay, Louisiana: 53%). Six estuaries had atmospheric contributions 30% of the TN inputs (Casco Bay, Maine: 43%; Buzzards Bay, Massachusetts: 30%; Great Bay, New Jersey: 40%; Chesapeake Bay: 30%; Terrebonne-Timbalier Bay, Louisiana: 59%; and Upper Laguna Madre: 41%). Results from our study suggest that reductions in N loadings to estuaries should be accomplished by implementing watershed specific programs that target the dominant N sources. C1 Appalachian Lab, Frostburg, MD 21532 USA. Syracuse Univ, Dept Civil & Environm Engn, Syracuse, NY 13244 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. RP Castro, MS (reprint author), Appalachian Lab, 301 Braddock Rd, Frostburg, MD 21532 USA. RI Boynton, Walter/C-3035-2012; Driscoll, Charles/F-9832-2014; Castro, Mark/J-6529-2015; OI Castro, Mark/0000-0002-4279-8204; Driscoll, Charles/0000-0003-2692-2890 NR 24 TC 54 Z9 55 U1 5 U2 39 PU ESTUARINE RES FEDERATION PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0160-8347 J9 ESTUARIES JI Estuaries PD JUN PY 2003 VL 26 IS 3 BP 803 EP 814 DI 10.1007/BF02711991 PG 12 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 712NN UT WOS:000184803900017 ER PT J AU Weems, HV Thompson, FC Rotheray, G Deyrup, MA AF Weems, HV Thompson, FC Rotheray, G Deyrup, MA TI The genus Rhopalosyrphus (Diptera : Syrphidae) SO FLORIDA ENTOMOLOGIST LA English DT Article DE taxonomy; identification key; neotropics; nearctic AB The flower fly genus Rhopalosyrphus Giglio-Tos (Diptera: Syrphidae) is revised. The genus is redescribed; a key to species is presented; the phylogenetic relationships of the genus and species are hypothesized; the included species are described; with new species, R. ramulorum Weems & Deyrup, described from Florida (type) and Mexico; R. australis Thompson from Brazil and Paraguay (type); and the critical characters are illustrated. C1 USDA, Systemat Entomol Lab, Smithsonian Inst NHB168, Washington, DC 20560 USA. Royal Museum Scotland, Dept Nat Hist, Edinburgh EH1 1JF, Midlothian, Scotland. Archbold Biol Stn, Lake Placid, FL 33862 USA. RP Weems, HV (reprint author), USDA, Systemat Entomol Lab, Smithsonian Inst NHB168, Washington, DC 20560 USA. NR 27 TC 4 Z9 4 U1 0 U2 0 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 JUN PY 2003 VL 86 IS 2 BP 186 EP 193 DI 10.1653/0015-4040(2003)086[0186:TGRDS]2.0.CO;2 PG 8 WC Entomology SC Entomology GA 697ZJ UT WOS:000183972900013 ER PT J AU Pearson, TRH Burslem, DFRP Mullins, CE Dalling, JW AF Pearson, TRH Burslem, DFRP Mullins, CE Dalling, JW TI Functional significance of photoblastic germination in neotropical pioneer trees: a seed's eye view SO FUNCTIONAL ECOLOGY LA English DT Article DE Gap size; litter; r : fr; seed size; tropical forest ID TROPICAL RAIN-FOREST; ECOLOGICAL SIGNIFICANCE; PIPER-AURITUM; LIGHT; SOIL; PENETRATION; PHYTOCHROME; LITTER; PERCEPTION; DYNAMICS AB 1. We investigated the relationship between seed mass and the suitability of microsites for germination for five small-seeded (<2.4 mg fresh mass) photoblastic neotropical pioneer trees. We determined the germination response of these species to the ratio of red to far-red irradiance (r:fr) and compared it to r:fr measured under varying conditions of canopy openness, litter and soil thickness. 2. At a constant temperature the germination percentage of each of the species increased sharply with increasing r:fr above a species-specific threshold r:fr. The smallest-seeded species, Miconia argentea , had the lowest r:fr threshold for germination (0.12) while the larger-seeded Cecropia species and Solanum hayesii possessed higher values (0.21-0.27). The largest seeded species, Solanum hayesii , also showed a positive germination response to a 10degreesC temperature fluctuation, which was independent of the response to r:fr. 3. The mean r:fr at ground level declined with decreasing gap size but not sufficiently to suppress the germination of these five species. However, a covering of one litter leaf in direct sunlight reduced the r:fr to between 0.18 and 0.83 depending on the species and leaf wetness. The top-soil at our study site was aggregated and irradiance was transmitted or reflected between soil aggregates with little change in r:fr. Light did not penetrate the aggregates. 4. We suggest that photoblastic germination in neotropical pioneers has evolved to inhibit germination in response to conditions most likely to alter within the life of an individual seed (i.e. superficial burial by leaf litter or incorporation into the surface soil), rather than to fine scale variation in canopy openness. Among photoblastic species, the pattern of response to r:fr suggests that smaller-seeded species would germinate in a broader range of microsites than larger-seeded species. This lower degree of discrimination may be associated with their higher risk of mortality and therefore more limited persistence in the soil seed bank. C1 Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Smithsonian Trop Res Inst, UNIT 0948, APO, AA 34002 USA. RP Pearson, TRH (reprint author), Univ Aberdeen, Sch Biol Sci, Cruickshank Bldg,St Machar Dr, Aberdeen AB24 3UU, Scotland. OI Burslem, David/0000-0001-6033-0990 NR 33 TC 49 Z9 63 U1 1 U2 22 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD JUN PY 2003 VL 17 IS 3 BP 394 EP 402 DI 10.1046/j.1365-2435.2003.00747.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 687FA UT WOS:000183364400013 ER PT J AU Ferrari, FD Fornshell, JA Ong, L Ambler, JW AF Ferrari, FD Fornshell, JA Ong, L Ambler, JW TI Diel distribution of copepods across a channel of an overwash mangrove island SO HYDROBIOLOGIA LA English DT Article DE planktonic copepods; swarms; age structure; diel changes ID DIOITHONA-OCULATA; ZOOPLANKTON AB The distribution of copepod species and their nauplii was studied in a narrow, blind channel on an overwash mangrove island offshore of Belize. Copepodids were sampled with a pump at five stations across the channel during a diel cycle. Diel changes of copepodid stages II - VI were marked by horizontal dispersal of Dioithona oculata, the dominant species, from swarms in the prop roots along the shore during the day to the edge of the prop root habitat at night. Migration of copepodids back to the prop roots appeared to be controlled endogenously because change from a night to a daytime age structure began before first light. Mean copepodid stage at subsurface depths in the channel and prop root edge decreased from 4.2 ( with 6.0 = all adults) to 2.9 at predawn to 1.1 during day. The oceanic Oithona nana and O. simplex, and the coastal zone O. fonsecae were evenly distributed with depth and distance from shore during day and night, with avoidance of prop root shoreline during day. These species were much less abundant than Dioithona oculata in the prop roots, but of comparable or greater abundance in the channel. Coastal zone Acartia spinata exhibited evidence of swarming. Nauplii, sampled with a 25 mum plankton net, were dominated by harpacticoid (50%) and cyclopoid (34%) nauplii, which generally were more abundant at 1m than at the surface and more abundant at night than the day. Lagrangian current measurements indicated velocities at ebb tide twice those of flood tide (1.9 vs. 0.8 cm s(-1)) and a minimal residence time of 5 days, which could result in advection of D. oculata nauplii out of the Lair Channel before their recruitment into swarms as copepodid stage II. Previously reported maximum swimming speeds of swarming D. oculata copepodid stages (2.0 cm s(-1)) and greater densities in prop roots and near the benthos may help copepodids avoid advection. The swarming behavior and diel horizontal migration ( or dispersal) reported for D. oculata appears analogous to that of limnetic zooplankton, which may swarm among macrophytes along shorelines during the day to avoid visual predators and disperse or migrate away from the shoreline at night. C1 Smithsonian Inst, Dept Invertebrate Zool, MSC, Washington, DC 20013 USA. Millersville Univ Pennsylvania, Dept Biol, Millersville, PA 17551 USA. RP Ferrari, FD (reprint author), Smithsonian Inst, Dept Invertebrate Zool, MSC, POB 37012,MRC 534, Washington, DC 20013 USA. NR 24 TC 2 Z9 3 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD JUN PY 2003 VL 499 IS 1-3 BP 147 EP 159 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 737LY UT WOS:000186235100011 ER PT J AU Tong, CYE Meledin, DV Marrone, DP Paine, SN Gibson, H Blundell, R AF Tong, CYE Meledin, DV Marrone, DP Paine, SN Gibson, H Blundell, R TI Near field vector beam measurements at 1 THz SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE antenna pattern; Gaussian beam; submillimeter wave; vector measurements AB We have performed near-field vector beam measurements at 1.03 THz to characterize and align the receiver optics of a superconducting receiver. The signal source is a harmonic generator mounted on an X-Y translation stage. We model the measured two-dimensional complex beam pattern by a fundamental. Gaussian mode, from which we derive the position of the beam center, the beam radius and the direction of propagation. By performing scans in the planes separated by 400 mm, we have confirmed that our beam pattern measurements are highly reliable. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Tong, Edward/0000-0002-7736-4203 NR 6 TC 11 Z9 11 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD JUN PY 2003 VL 13 IS 6 BP 235 EP 237 DI 10.1109/LMWC.2003.814602 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 697KH UT WOS:000183941400015 ER PT J AU Meledin, D Tong, CYE Blundell, R Kaurova, N Smirnov, K Voronov, B Goltsman, G AF Meledin, D Tong, CYE Blundell, R Kaurova, N Smirnov, K Voronov, B Goltsman, G TI Study of the IF bandwidth of NbNHEB mixers based on crystalline quartz substrate with an MgO buffer layer SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 04-09, 2002 CL HOUSTON, TEXAS SP Apple, Argonne Natl Lab, Florida State Univ, Ctr Adv Power Syst, Cingular Wireless, Council SuperCond Amer Competit, Hewlett Packard Co, Houston Adv Res Ctr, IEEE CSC Council Supercond, IISSC, Marimon, Naval Res Lab, Oak Ridge Natl Lab, Univ Houston, Texas Ctr Supercond & Adv Mat, US DOE, Div High Energy Phys, Univ Houston, Cullen Coll Engn, Univ Houston, Coll Nat Sci & Math, Univ Houston, Div Res, Wah Chang DE electron temperature; hot-electron bolometer; self-heating parameter ID ELECTRON BOLOMETER MIXER AB In this paper, we present the results of IF bandwidth measurements on 3-4 mn thick NbN hot electron bolometer waveguide mixers, which have been fabricated on a 200-nm thick MgO buffer layer deposited on a crystalline quartz substrate. The 3-dB IF bandwidth, measured at an LO frequency of 0.81 THz, is 3.7 GHz at the optimal bias point for low noise receiver operation. We have-also made measurements of the IF dynamic impedance, which allow us to evaluate the intrinsic electron temperature relaxation time and self-heating parameters at different bias conditions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Moscow State Pedag Univ, Moscow 119435, Russia. RP Meledin, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Tong, Edward/0000-0002-7736-4203 NR 15 TC 20 Z9 20 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2003 VL 13 IS 2 BP 164 EP 167 DI 10.1109/TASC.2003.813671 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 702UB UT WOS:000184241700022 ER PT J AU Maezawa, H Tong, CYE Noguchi, T Matsunaga, T Blundell, R Pan, SK AF Maezawa, H Tong, CYE Noguchi, T Matsunaga, T Blundell, R Pan, SK TI An Nb-based waveguide SIS distributed mixer employing coplanar inductor loaded microstrip transformer for the 800 GHz frequency band SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 04-09, 2002 CL HOUSTON, TEXAS SP Apple, Argonne Natl Lab, Florida State Univ, Ctr Adv Power Syst, Cingular Wireless, Council SuperCond Amer Competit, Hewlett Packard Co, Houston Adv Res Ctr, IEEE CSC Council Supercond, IISSC, Marimon, Naval Res Lab, Oak Ridge Natl Lab, Univ Houston, Texas Ctr Supercond & Adv Mat, US DOE, Div High Energy Phys, Univ Houston, Cullen Coll Engn, Univ Houston, Coll Nat Sci & Math, Univ Houston, Div Res, Wah Chang ID RECEIVER; LINE AB We present a novel superconducting waveguide mixer for 800 GHz. In this mixer, a half-wave Nb/Al-AlOx/Nb superconducting-insulator-superconductor (SIS) resonator is integrated with a microstrip superconducting transmission line loaded with coplanar inductors. This hybrid coplanar/microstrip transmission line acts as an impedance matching section between the distributed junction and the waveguide feed point of the mixer mount. We have designed mixers with a simple model which predicts that the insertion loss of the matching network is less than 10 percent up to 840 GHz. Preliminary experimental results show that the resonator can work up to 800 GHz but the parameters of the coplanar inductor loaded microstrip line need to be refined to improve power coupling to the resonator. C1 Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Maezawa, H (reprint author), Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. OI Tong, Edward/0000-0002-7736-4203 NR 11 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2003 VL 13 IS 2 BP 668 EP 671 DI 10.1109/TASC.2003.813991 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 702UB UT WOS:000184241700146 ER PT J AU Tong, CYE Blundell, R Megerian, KG Stern, JA LeDuc, HG AF Tong, CYE Blundell, R Megerian, KG Stern, JA LeDuc, HG TI A 650 GHz fixed-tuned waveguide SIS distributed mixer with no integrated tuning circuit SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 04-09, 2002 CL HOUSTON, TEXAS SP Apple, Argonne Natl Lab, Florida State Univ, Ctr Adv Power Syst, Cingular Wireless, Council SuperCond Amer Competit, Hewlett Packard Co, Houston Adv Res Ctr, IEEE CSC Council Supercond, IISSC, Marimon, Naval Res Lab, Oak Ridge Natl Lab, Univ Houston, Texas Ctr Supercond & Adv Mat, US DOE, Div High Energy Phys, Univ Houston, Cullen Coll Engn, Univ Houston, Coll Nat Sci & Math, Univ Houston, Div Res, Wah Chang DE distributed mixing; integrated tuning network; resonant mixer; SIS devices ID LINE AB A Superconductor-Insulator-Superconductor (SIS) distributed mixer with no integrated tuning circuit has been designed for use in a fixed-tuned waveguide mixer block. This mixer employs two half-wave SIS resonators connected in series across the feed point of the waveguide circuit. By selecting appropriate dimensions for the resonators, we can obtain proper impedance matching over a reasonable input bandwidth. Since there is no lossy thin film microstrip line in front of the SIS junction, efficient power transfer from the waveguide feed to the mixer element can be achieved. A receiver noise temperature of 185 K at 650 GHz has been measured with a dual 0.33 x 16.8 mum SIS resonator. The noise temperature remains below 300 K over an input bandwidth of about 10%. This design can be used at much higher frequency where the loss of tuning circuit becomes significant. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Tong, Edward/0000-0002-7736-4203 NR 6 TC 5 Z9 5 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2003 VL 13 IS 2 BP 680 EP 683 DI 10.1109/TASC.2003.813996 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 702UB UT WOS:000184241700149 ER PT J AU McGovern, CF AF McGovern, CF TI The politics of consumption: Material culture and citizenship in Europe and America. SO JOURNAL OF INTERDISCIPLINARY HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP McGovern, CF (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 3 TC 0 Z9 0 U1 0 U2 1 PU M I T PRESS PI CAMBRIDGE PA FIVE CAMBRIDGE CENTER, CAMBRIDGE, MA 02142 USA SN 0022-1953 J9 J INTERDISCIPL HIST JI J. Interdiscip. Hist. PD SUM PY 2003 VL 34 IS 1 BP 69 EP 71 DI 10.1162/002219503322645510 PG 4 WC History SC History GA 756FU UT WOS:000187455800009 ER PT J AU Hussein, AA Bozzi, B Correa, M Capson, TL Kursar, TA Coley, PD Solis, PN Gupta, MP AF Hussein, AA Bozzi, B Correa, M Capson, TL Kursar, TA Coley, PD Solis, PN Gupta, MP TI Bioactive constituents from three Vismia species SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID PRENYLATED ANTHRANOIDS; GENUS VISMIA; CHEMISTRY; XANTHONES; GUINEENSIS AB Bioassay-guided fractionation of the methanolic extracts of Vismia baccifera, V. jefensis, and V. macrophylla against human breast, CNS, and lung cancer cell lines resulted in the isolation of a new compound, ferruginin C (1), and seven known compounds, ferruginins A (2) and B (3), vismin (4), harunganin (5), vismione B (6), deacetylvismione H (7), and deacetylvismione A (8), as active constituents. In addition, bivismiaquinone (9) and vismiaquinone (10) were obtained as inactive constituents. The structure of ferruginin C was elucidated by spectroscopic means. Compounds 6-8 were the most active, and the cytotoxic activity of compounds 2-5 and 7 is reported for the first time. C1 Univ Panama, CIFLORPAN, Fac Farm, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Gupta, MP (reprint author), Univ Panama, CIFLORPAN, Fac Farm, Apartado 10767,Estafeta Univ, Panama City, Panama. EM cytedqff@ancon.up.ac.pa OI Gupta, Mahabir/0000-0002-9302-7864; Hussein, Ahmed/0000-0002-3877-9959 FU FIC NIH HHS [1U01 TW 01021-01] NR 25 TC 41 Z9 43 U1 0 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD JUN PY 2003 VL 66 IS 6 BP 858 EP 860 DI 10.1021/np020566w PG 3 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 695CY UT WOS:000183814600023 PM 12828475 ER PT J AU Rubio-Palis, Y Wilkerson, R Guzman, H AF Rubio-Palis, Y Wilkerson, R Guzman, H TI Morphological characters of adult Anopheles (Nyssorhynchus) marajoara in Venezuela SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Article DE Anopheles marajoara; malaria vectors; morphology; random amplified polymorphic DNA-polymerase; chain reaction ID AMPLIFIED POLYMORPHIC DNA; POLYMERASE CHAIN-REACTION; ALBITARSIS COMPLEX; WESTERN VENEZUELA; MALARIA VECTOR; CULICIDAE; DIPTERA; BRAZIL; ARGENTINA AB A morphometric study was carried out to find diagnostic characters with which to update taxonomic keys for field identification of Anopheles (Nyssorhynchus) marajoara and the 3 other sympatric Anopheles (Nyssorhynchus) species (An. darlingi, An. argyritarsis, and An. braziliensis) that occur in Venezuela. Diagnostic random amplified polymorphic DNA-polymerase chain reaction markers from wild-caught specimens showed that An. marajoara was the only species in the Anopheles albitarsis complex collected in Venezuela. C1 Inst Altos Estudios Dr Arnoldo Gabaldon, Maracay 2101A, Venezuela. Univ Carabobo, BIOMED, Bioanalisis, Maracay, Venezuela. Smithsonian Inst, Walter Reed Biosystemat Unit, Washington, DC 20560 USA. RP Rubio-Palis, Y (reprint author), Inst Altos Estudios Dr Arnoldo Gabaldon, Apartado 2073, Maracay 2101A, Venezuela. NR 30 TC 12 Z9 15 U1 0 U2 0 PU AMER MOSQUITO CONTROL ASSOC PI EATONTOWN PA P O BOX 234, EATONTOWN, NJ 07724-0234 USA SN 8756-971X J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD JUN PY 2003 VL 19 IS 2 BP 107 EP 114 PG 8 WC Entomology SC Entomology GA 693LZ UT WOS:000183720200001 PM 12825659 ER PT J AU Verling, E Crook, AC Barnes, DKA Harrison, SSC AF Verling, E Crook, AC Barnes, DKA Harrison, SSC TI Structural dynamics of a sea-star (Marthasterias glacialis) population SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article ID PARACENTROTUS-LIVIDUS LAMARCK; ASTERIAS-VULGARIS; FEEDING ECOLOGY; LOUGH INE; PREY; BEHAVIOR; RECRUITMENT; SELECTION; SEASTARS; PREDATOR AB The dynamics and feeding biology of a population of Marthasterias glacialis (Echinodermata: Asteroidea) was examined over a two-year period from 2000-2002 at Lough Hyne Marine Nature Reserve, Co. Cork, Ireland. A multivariate approach was used and both multiple factors and multiple interactions between factors were found to influence population structure. These included time of year, site, individual sea-star size, depth, and predator density. Individuals belonging to the smallest size-classes (0-50 mm and 51-100 mm) were most abundant amongst boulders in shallow water (0-1 m), while larger individuals were primarily found in water below 1 m in depth on finer grade substratum and shell debris. Dietary composition was also found to differ with depth; sea-stars in the immediate subtidal had an opportunistic diet, and fed on a variety of taxa, whilst those M. glacialis from 1-6 m were more selective and restrictive, feeding chiefly on bivalve prey. We propose that spatial partitioning of different size-classes and a generalist feeding strategy may account for the success of M. glacialis at Lough Hyne. C1 Natl Univ Ireland Univ Coll Cork, Dept Zool & Anim Ecol, Cork, Ireland. British Antarctic Survey, Div Biol Sci, Cambridge CB3 0ET, England. RP Verling, E (reprint author), Smithsonian Environm Res Ctr, Marine Invas Res Lab, POB 28, Edgewater, MD 21037 USA. NR 31 TC 23 Z9 25 U1 1 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD JUN PY 2003 VL 83 IS 3 BP 583 EP 592 DI 10.1017/S0025315403007513h PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 679HR UT WOS:000182915100023 ER PT J AU Stevens, MA Boness, DJ AF Stevens, MA Boness, DJ TI Influences of habitat features and human disturbance on use of breeding sites by a declining population of southern fur seals (Arctocephalus australis) SO JOURNAL OF ZOOLOGY LA English DT Article DE fur seals; Arctocephalus australis; breeding habitat; El Nino; population decline; Allee effect ID MONK SEAL; DISCRIMINANT-ANALYSIS; GREY SEALS; BEHAVIOR; SELECTION; VARIABLES; POLYGYNY; PERU AB Southern fur seals Arctocephalus australis in Peru have declined gradually over the past decade, and declined dramatically (72%) as a result of low food availability during the severe El Nino in 1997-98. In 1999, seals abandoned some historically important breeding sites. This is particularly alarming because new sites were not colonized. Our objective was to examine how habitat features and human disturbance influenced whether sites were currently used, abandoned or apparently not used in the past by fur seals for breeding. Data were collected on 14 variables at 70 potential breeding sites at three guano reserves in Peru. Discriminant analysis revealed significant multivariate differences among sites currently used for breeding, abandoned sites and unused sites (F = 5.97, P < 0.00001), and the model classified 74% of sites correctly. Currently used sites were less likely to have human disturbance and more likely to have offshore islands, stacked rocks, tide pools and abundant shade. Separate discriminant analyses for each reserve produced similar results. Habitat associated with thermoregulation (e.g. shade or pools) may be more important to fur seals in Peru, which breed at lower latitudes and are at greater risk of overheating on land than other populations. Habitat with minimized human access may be especially important to seals in small populations in which individuals may perceive themselves as more vulnerable because of decreased vigilance and dilution effects. Seals in our study selected breeding habitat with stacked rocks, which create shade and tide pools for thermoregulation and make human access difficult; but pups might suffer higher mortality in this habitat. We hypothesize that fur seals in Peru may exhibit an Allee effect, whereby suitability of habitat varies with population abundance. C1 Univ New Hampshire, Dept Zool, Durham, NH 03824 USA. Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA. RP Stevens, MA (reprint author), Univ New Hampshire, Dept Zool, 46 Coll Rd, Durham, NH 03824 USA. NR 51 TC 34 Z9 37 U1 3 U2 21 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA SN 0952-8369 J9 J ZOOL JI J. Zool. PD JUN PY 2003 VL 260 BP 145 EP 152 DI 10.1017/S0952836903003583 PN 2 PG 8 WC Zoology SC Zoology GA 695CK UT WOS:000183813400007 ER PT J AU Smith, HA AF Smith, HA TI Designer filters rely on metal mesh SO LASER FOCUS WORLD LA English DT Article AB Infrared filters fabricated from metal grids allow easy tailoring of the filters' optical properties. C1 Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, Cambridge, MA 02138 USA. RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 0 Z9 0 U1 2 U2 2 PU PENNWELL PUBL CO PI NASHUA PA 98 SPIT BROOK RD, NASHUA, NH 03062-2801 USA SN 0740-2511 J9 LASER FOCUS WORLD JI Laser Focus World PD JUN PY 2003 VL 39 IS 6 BP 123 EP 125 PG 3 WC Optics SC Optics GA 696GF UT WOS:000183878700038 ER PT J AU Schroll, S AF Schroll, S TI American expressionism: Art and social change 1920-1950. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Schroll, S (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2003 VL 128 IS 10 BP 112 EP + PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 685WX UT WOS:000183288100044 ER PT J AU Aiello, A AF Aiello, A TI An obsession with butterflies: Our long love affair with a singular insect. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Trop Res Inst, Ancon, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Ancon, Panama. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2003 VL 128 IS 10 BP 160 EP 160 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 685WX UT WOS:000183288100178 ER PT J AU Dick, MH Herrera-Cubilla, A Jackson, JBC AF Dick, MH Herrera-Cubilla, A Jackson, JBC TI Molecular phylogeny and phylogeography of free-living Bryozoa (Cupuladriidae) from both sides of the Isthmus of Panama SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID TROPICAL AMERICAN MOLLUSKS; MITOCHONDRIAL-DNA; EVOLUTIONARY RELATIONSHIPS; MORPHOLOGICAL DIVERGENCE; EASTERN PACIFIC; 16S RDNA; CRABS; SEA; SUBSTITUTION; SPECIATION AB Genetic data were used to identify Recent species of free-living bryozoans (Cupuladriidae) from both sides of the Isthmus of Panama, and to examine their phylogenetic relationships, species richness, and population structures. An approximately 480 bp fragment of the 16S mitochondrial rRNA gene was sequenced from 182 individuals from Panama, the Gulf of Mexico, and El Salvador. Ten haplotype groups (Cupuladria 4, 5, and 6; Discoporella 1, 2, 3A, 3B, 3C, 7, and 8) were identified. Genetic distances between haplotype groups (3.2-26.5%; K2P + Gamma) were 1-2 orders of magnitude greater than within groups (0.1-1.4%). Seven of the haplotype groups represent morphologically distinct species; Discoporellas 3A-C appear to be cryptic species. Phylogenetic analyses identified two pairs of transisthmian sister clades. An average divergence rate derived from other taxa suggests that Cupuladrias 4 and 5 diverged approximate to7 Ma, a Discoporella 7 clade diverged from a 3A-C clade approximate to11 Ma, and the 3A-C clade radiated approximate to6-4 Ma; these events all predated final closure of the isthmus? 3 Ma. The Caribbean side of the isthmus, with 5 species, is only marginally richer in cupuladriids than the Pacific side, with 4, but has greater phylogenetic depth. The Caribbean retains lineages stemming from a New World Miocene radiation that are not represented in the eastern Pacific; extant eastern Pacific cupuladriids share most recent common ancestry with only two of the Caribbean lineages. Species in the eastern Pacific tend to show shallow population structures, with high levels of gene flow between geographically separate populations, whereas Caribbean species tend to show deeper populations structures, with indications of restricted gene flow between Bocas del Toro/Gulf of Mosquitos and Costa Arriba/San Blas. The population structures derive from Pleistocene histories and may be of limited value in interpreting the macroevolutionary pattern, as our results provide no evidence of speciation on either side of the isthmus following closure in the late Pliocene. (C) 2003 Elsevier Science (USA). All rights reserved. C1 Middlebury Coll, Dept Biol, Middlebury, VT 05753 USA. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Panama. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Dick, MH (reprint author), Middlebury Coll, Dept Biol, Middlebury, VT 05753 USA. EM dick@middlebury.edu RI Dick, Matthew/E-1327-2012 NR 79 TC 32 Z9 35 U1 1 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD JUN PY 2003 VL 27 IS 3 BP 355 EP 371 DI 10.1016/S1055-7903(03)00025-3 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 680VG UT WOS:000182999200001 PM 12742742 ER PT J AU Burke, DJ Collins, CA Sharples, RM Romer, AK Nichol, RC AF Burke, DJ Collins, CA Sharples, RM Romer, AK Nichol, RC TI The Southern SHARC catalogue: a ROSAT survey for distant galaxy clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; surveys; galaxies : clusters : general; X-rays : galaxies : clusters ID SPATIAL CORRELATION-FUNCTION; X-RAY-CLUSTERS; N-LOG-S; MEDIUM-SENSITIVITY SURVEY; FLUX-LIMITED SAMPLE; ALL-SKY SURVEY; LUMINOSITY FUNCTION; RICH CLUSTERS; WARPS SURVEY; PSPC OBSERVATIONS AB X-ray selection provides a way of creating well-defined samples of distant clusters free from projection effects and with a well-understood selection function. This paper describes the creation of one such catalogue - the Southern Serendipitous High-redshift Archival ROSAT Cluster (SHARC) survey - which covers an area of 17.7 deg(2) and consists of 32 clusters with redshifts between 0.05 and 0.7 and X-ray luminosities between 7 x 10(42) and 4 x 10(44) erg s(-1): the high-redshift subsample contains 16 clusters with z greater than or equal to 0.3 and X-ray luminosities greater than 2 x 10(43) erg s(-1) (luminosities are quoted for the 0.5-2.0 keV energy band). The catalogue is in good agreement with those of other ROSAT cluster surveys for those fields in common. The high-redshift sample is consistent with there being no evolution in the cluster X-ray luminosity function at luminosities similar to10(44) erg s(-1): the implications of this work have been described elsewhere. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Univ Durham, Dept Phys, Durham DH1 3LE, England. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dburke@cfa.harvard.edu RI Sharples, Ray/N-7309-2013; OI Sharples, Ray/0000-0003-3449-8583; Burke, Douglas/0000-0003-4428-7835 NR 92 TC 24 Z9 24 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2003 VL 341 IS 4 BP 1093 EP 1108 DI 10.1046/j.1365-8711.2003.06378.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FD UT WOS:000183080200012 ER PT J AU Torres, MAP Callanan, PJ Garcia, MR AF Torres, MAP Callanan, PJ Garcia, MR TI Time-resolved spectroscopy of the M15 X-ray binary AC211/X2127+119 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : close; stars : individual : AC211; stars : individual : X2127+119; X-rays : binaries ID ACCRETION DISK CORONAE; GLOBULAR-CLUSTERS; OPTICAL COUNTERPART; X2127+119; PERIOD; EVOLUTION; EMISSION; BURST; DISCOVERY; OUTFLOW AB We present time-resolved spectroscopy acquired during two epochs (spaced apart by similar to15 d) of the eclipsing low-mass X-ray binary AC211/X2127+119 in the globular cluster M15. The spectra show variations in the He iilambda4686 emission line not only modulated on the orbital period, but also on time-scales of a few days. During the first epoch of observation, the emission line shows a strong S -wave superimposed on the average double-peaked profile. The line exhibits no evidence of rotational disturbance at the orbital phases when the eclipse is observed in the optical continuum. During the second epoch, no double-peak or S -wave component is present. The He i absorption lines detected by other authors are not present in our spectra. A Doppler image of He iilambda4686 for the first epoch supports the presence of the accretion disc. No hotspot is detected, although enhanced emission at V-X = 30 km s(-1) , V-Y = 160 km s(-1) is observed. We discuss the implications of this emission in the context of an X-ray heated donor star, in which case a high mass ratio and neutron star primary are implied. Finally, we speculate on the possibility of a misaligned secondary star in AC211. C1 Univ Coll, Dept Phys, Cork, Ireland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, MAP (reprint author), Univ Coll, Dept Phys, Cork, Ireland. NR 46 TC 3 Z9 3 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2003 VL 341 IS 4 BP 1231 EP 1238 DI 10.1046/j.1365-8711.2003.06486.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FD UT WOS:000183080200024 ER PT J AU Saija, R Iati, MA Giusto, A Borghese, F Denti, P Aiello, S Cecchi-Pestellini, C AF Saija, R Iati, MA Giusto, A Borghese, F Denti, P Aiello, S Cecchi-Pestellini, C TI Radiation pressure cross-sections of fluffy interstellar grains SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms : general; dust, extinction ID OPTICAL-PROPERTIES; ELECTROMAGNETIC SCATTERING; DUST GRAINS; GALAXIES; PARTICLES; EMISSION; SPHERES; EFFLUX AB We computed, through the transition matrix method, the radiation pressure cross-sections of cosmic dust grains modelled as aggregates (clusters) of spheres of appropriate geometry. The calculation is performed without resorting to any approximation and with a computational effort that is noticeably lighter than the one required by other methods. Our results show that radiation pressure cross-sections decrease with increasing particle fluffiness in the near-ultraviolet and visible range of the spectrum. This is due to the decrease of the corresponding strength of the multiple scattering processes that couple the aggregated spheres to each other. As a result, the inertial response to radiation forces of highly porous aggregates tends to become similar to that of the constituent particles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Messina, Dipartimento Fis Mat & Tecnol Fis Avanzate, I-98166 Messina, Italy. Ist Nazl Fis Mat, Unita Messina, Messina, Italy. Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. RP Saija, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cecchi Pestellini, Cesare/0000-0001-7480-0324; IATI', MARIA ANTONIA/0000-0002-3576-8656; IATI', MARIA ANTONIA/0000-0003-0467-8049 NR 34 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 JUN 1 PY 2003 VL 341 IS 4 BP 1239 EP 1245 DI 10.1046/j.1365-8711.2003.06490.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FD UT WOS:000183080200025 ER PT J AU Hernquist, L Springel, V AF Hernquist, L Springel, V TI An analytical model for the history of cosmic star formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : analytical; galaxies : formation; cosmology : theory ID ULTRAVIOLET LUMINOSITY DENSITY; GALAXY REDSHIFT SURVEY; HUBBLE DEEP FIELD; SIMULATIONS; POPULATION; EVOLUTION; UNIVERSE; LAW AB We use simple analytic reasoning to identify physical processes that drive the evolution of the cosmic star formation rate, (rho) over dot(*), in cold dark matter universes. Based on our analysis, we formulate a model to characterize the redshift dependence of (rho) over dot(*) and compare it with results obtained from a set of hydrodynamic simulations that include star formation and feedback. We find that the cosmic star formation rate is described by two regimes. At early times, densities are sufficiently high and cooling times sufficiently short that abundant quantities of star-forming gas are present in all dark matter haloes that can cool by atomic processes. Consequently, (rho) over dot(*) generically rises exponentially as z decreases, independent of the details of the physical model for star formation, but dependent on the normalization and shape of the cosmological power spectrum. This part of the evolution is dominated by gravitationally driven growth of the halo mass function. At low redshifts, densities decline as the universe expands to the point that cooling is inhibited, limiting the amount of star-forming gas available. We find that in this regime the star formation rate scales approximately as (rho) over dot(*) proportional to H(z)(4/3), in proportion to the cooling rate within haloes. We demonstrate that the existence of these two regimes leads to a peak in the star formation rate at an intermediate redshift z =z (peak). We discuss how the location of this peak depends on our model parameters, and show that the peak cannot occur above a limiting redshift of z approximate to 8.7. For the star formation efficiency adopted in our numerical simulations, z (peak) approximate to 5-6, with half of all stars forming at redshifts larger than z similar or equal to 2.2. We derive analytic expressions for the full star formation history and show that they match our simulation results to better than similar or equal to10 per cent. Using various approximations, we reduce the expressions to a simple analytic fitting function for (rho) over dot(*) that can be used to compute global cosmological quantities that are directly related to the star formation history. As examples, we consider the integrated stellar density, the supernova and gamma-ray burst rates observable on Earth, the metal enrichment history of the Universe, and the density of compact objects. We also briefly discuss the expected dependence of the star formation history on cosmological parameters and the physics of the gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Hernquist, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 55 TC 164 Z9 164 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2003 VL 341 IS 4 BP 1253 EP 1267 DI 10.1046/j.1365-8711.2003.06499.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 682FD UT WOS:000183080200027 ER PT J AU Elander, N Levin, S Yarevsky, E AF Elander, N Levin, S Yarevsky, E TI Smooth exterior complex-scaling, full-angular-momentum, and three-dimensional finite-element method applied to doubly excited states of helium SO PHYSICAL REVIEW A LA English DT Article ID RESONANCE; HE; TRANSITIONS; THRESHOLDS; ENERGIES; SYSTEMS; ATOM AB A technique based on the total-angular-momentum representation the smooth exterior complex-scaling procedure, and the three-dimensional finite-element method, is applied to calculations of S, P, and D resonant, so-called doubly excited, states of the helium atom. The resonances are calculated with an accuracy better than 10(-5) a.u. The applicability of an extrapolation procedure to complex energies is analyzed. C1 Stockholm Univ, Alba Nova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. St Petersburg State Univ, Inst Phys, St Petersburg 198904, Russia. Harvard Univ, Cambridge, MA 02138 USA. Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Int Solvay Inst Phys & Chem, B-1050 Brussels, Belgium. RP Elander, N (reprint author), Stockholm Univ, Alba Nova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. RI Yarevsky, Evgeny/J-4447-2013 OI Yarevsky, Evgeny/0000-0002-0921-6196 NR 34 TC 13 Z9 13 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 2003 VL 67 IS 6 AR 062508 DI 10.1103/PhysRevA.67.062508 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 696YM UT WOS:000183915200058 ER PT J AU Krems, RV Dalgarno, A Balakrishnan, N Groenenboom, GC AF Krems, RV Dalgarno, A Balakrishnan, N Groenenboom, GC TI Spin-flipping transitions in (2)Sigma molecules induced by collisions with structureless atoms SO PHYSICAL REVIEW A LA English DT Article ID ULTRACOLD MOLECULES; COLD; TEMPERATURES; SCATTERING AB It is shown that spin-flipping transitions in low energy collisions of (2)Sigma diatomic molecules in the lowest rotational N=0 level with structureless atoms proceed through coupling to the rotationally excited N>0 levels, and are determined by the spin-rotation interaction in the rotationally excited molecule. We carry out calculations for collisions of CaH and He-3. For the spin-flip rate coefficient corresponding to an interaction potential that does not generate a shape resonance, we obtain 1.20x10(-17) cm(3) s(-1) at a temperature of 0.4 K consistent with the measured value of 10(-17+/-1) cm(3) s(-1). We make predictions as to which molecules should have the least probability of spin-flipping in collisions with atoms. C1 Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. Univ Nijmegen, Inst Theoret Chem, NSRIM, NL-6525 ED Nijmegen, Netherlands. RP Krems, RV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. RI Groenenboom, Gerrit/F-9692-2015 NR 16 TC 50 Z9 50 U1 1 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 JUN PY 2003 VL 67 IS 6 AR 060703 DI 10.1103/PhysRevA.67.060703 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 696YM UT WOS:000183915200007 ER PT J AU Wright, HE AF Wright, HE TI A quiz for our readers (Johannes de Mare, 1806-89) SO PRINT QUARTERLY LA English DT Article C1 Smithsonian Inst, Amer Museum Nat Hist, Washington, DC 20013 USA. RP Wright, HE (reprint author), Smithsonian Inst, Amer Museum Nat Hist, PO Box 37012, Washington, DC 20013 USA. EM wrighth@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU PRINT QUART LTD PI LONDON PA 80 CARLTON HILL, LONDON NW8 0ER, ENGLAND SN 0265-8305 J9 PRINT Q JI Print Q. PD JUN PY 2003 VL 20 IS 2 BP 162 EP 163 PG 2 WC Art SC Art GA 712EL UT WOS:000184784200005 ER PT J AU Katz, CA Hewitt, JN Corey, BE Moore, CB AF Katz, CA Hewitt, JN Corey, BE Moore, CB TI A survey for transient astronomical radio emission at 611 MHz SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GAMMA-RAY BURST; BLACK-HOLE EXPLOSIONS; PULSES; SEARCH; AFTERGLOWS; SUPERNOVAE; RADIATION; PULSARS; EVENTS; STARS AB We have constructed and operated the Survey for Transient Astronomical Radio Emission ( STARE) to detect transient astronomical radio emission at 611 MHz originating from the sky over the northeastern United States. The system is sensitive to transient events on timescales of 0.125 s to a few minutes, with a typical zenith flux density detection threshold of approximately 27 kJy. During 18 months of around-the-clock observing with three geographically separated instruments, we detected a total of 4,318,486 radio bursts. Of these events, 99.9% were rejected as locally generated interference, determined by requiring the simultaneous observation of an event at all three sites for it to be identified as having an astronomical origin. The remaining 3898 events have been found to be associated with 99 solar radio bursts. These results demonstrate the remarkably effective radio frequency interference rejection achieved by a coincidence technique using precision timing (such as GPS clocks) at geographically separated sites. The nondetection of extrasolar bursting or flaring radio sources has improved the flux density sensitivity and timescale sensitivity limits set by several similar experiments in the 1970s. We discuss the consequences of these limits for the immediate solar neighborhood and the discovery of previously unknown classes of sources. We also discuss other possible uses for the large collection of 611 MHz monitoring data assembled by STARE. C1 MIT, Elect Res Lab, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Haystack Observ, Westford, MA 01886 USA. TransForm Pharmaceut, Lexington, MA 02421 USA. RP Katz, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM ckatz@cfa.harvard.edu; jhewitt@mit.edu; bcorey@haystack.mit.edu; cmoore@alum.mit.edu NR 51 TC 16 Z9 16 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2003 VL 115 IS 808 BP 675 EP 687 DI 10.1086/375568 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679WF UT WOS:000182944400005 ER PT J AU Gonsalves, R Nisenson, P AF Gonsalves, R Nisenson, P TI Calculation of optimized apodizers for a Terrestrial Planet Finder coronagraphic telescope SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID RECTANGULAR APERTURES AB One of two approaches to implementing NASA's Terrestrial Planet Finder is to build a space telescope that utilizes the techniques of coronagraphy and apodization to suppress diffraction and image exoplanets. We present a method for calculation of a telescope's apodizer that suppresses the sidelobes of the image of a star so as to optimally detect an Earth-like planet. Given the shape of a telescope's aperture and given a search region for a detector, we solve an integral equation to determine an amplitude modulation ( an apodizer) that suppresses the star's energy in the focal plane search region. The method is quite general and yields as special cases the product apodizer reported by Nisenson & Papaliolios and the prolate spheroidal apodizer of Kasdin et al. and Aime et al. We show computer simulations of the apodizers and the corresponding point-spread functions for various aperture-detector configurations. C1 Tufts Univ, Dept Elect Engn & Comp Sci, Medford, MA 02155 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01803 USA. RP Gonsalves, R (reprint author), Tufts Univ, Dept Elect Engn & Comp Sci, Medford, MA 02155 USA. NR 12 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 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2003 VL 115 IS 808 BP 706 EP 711 DI 10.1086/374914 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679WF UT WOS:000182944400008 ER PT J AU Christy, JH AF Christy, JH TI Reproductive timing and larval dispersal of intertidal crabs: the predator avoidance hypothesis SO REVISTA CHILENA DE HISTORIA NATURAL LA English DT Article; Proceedings Paper CT Symposium on Behavioral Ecology of Crustaceans CY MAY, 2002 CL VALDIVIA, CHILE DE larval release; larval dispersal; crabs; reproductive timing; plankton; predation ID MALE FIDDLER-CRABS; ADAPTIVE SIGNIFICANCE; UCA-PUGILATOR; PLANKTIVOROUS FISHES; HATCHING RHYTHMS; GENUS UCA; RELEASE; MECHANISMS; SYNCHRONY; CYCLES AB Many intertidal and shallow water crabs have strong reproductive cycles and migratory larvae. Females release larvae near the time of high water of the larger amplitude nocturnal tides during the semilunar or lunar cycles. Newly hatched larvae move quickly at night toward and into the sea where, weeks later, they develop to megalopae that then ride nocturnal flood tides inshore and up estuaries to settle in adult habitats. It was first thought that crabs might time larval release so that larvae will become megalopae when they can ride the larger amplitude spring flood tides to adult habitats. This idea was rejected when it was found that were was no change in the timing of hatching during the breeding season by several estuarine species that would compensate for the decrease in the larval development period as the water temperature increased. In addition, megalopae moved up-stream at night but not on the largest spring flood tides. Attention shifted to the possible value to larvae of leaving the estuary quickly to avoid high temperatures, low salinities or stranding. This idea was not supported when it was found that species on open coasts exhibit the same reproductive patterns as do estuarine species. Alternatively, by moving quickly to the ocean at night larvae may best escape visual planktivorous fishes that are especially abundant in shallow areas. This predator avoidance hypothesis has been broadly supported: species with larvae that are cryptic, spiny and better protected from predation lack both strong reproductive cycles and larval migration. The mechanisms that promote precise reproductive timing have been little studied. evidence is presented that female fiddler crabs may adjust the timing of fertilization to compensate for variation in incubation temperatures that would otherwise induce timing errors. However, crabs on colder coasts, as in Chile, apparently do not exhibit biweekly or monthly cycles of larval release. The consequences of this for adults and larvae have vet to be explored. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. NR 50 TC 35 Z9 35 U1 0 U2 4 PU SOCIEDAD BIOLGIA CHILE PI SANTIAGO PA CASILLA 16164, SANTIAGO 9, CHILE SN 0716-078X J9 REV CHIL HIST NAT JI Rev. Chil. Hist. Nat. PD JUN PY 2003 VL 76 IS 2 BP 177 EP 185 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 689TN UT WOS:000183509200005 ER PT J AU Corrales, JF Epstein, ME AF Corrales, JF Epstein, ME TI Revision of the Natada fusca complex and description of six new Neotropical species (Lepidoptera : Limacodidae) SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE Limacodidae; Natada fusca complex; Natada; Costa Rica; larval host plants; defoliation AB Six new species in the genus Natada, which have been hidden under Natada fusca Druce, are described and defined primarily by genitalia. New species include N. burnsi, N. truncata, N. singulara, N. chaconi, N. covelli, and N. confusa. Five of eight species in the Natada fusca complex, which also includes N.fuscodivisa Dognin, occur in Costa Rica. Distribution of the complex ranges from Mexico to the upper Amazon Basin and Guianas. Detailed geographic information and multiple genitalic drawings of males of one species, N. confusa, are provided to help define and separate species. The lectotype and paralectotype of N. fusca are designated. C1 Inst Nacl Biodiversidad, INBio, Heredia, Costa Rica. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Corrales, JF (reprint author), Inst Nacl Biodiversidad, INBio, 22-3100 Sto Domingo, Heredia, Costa Rica. EM epstein.marc@nmnh.si.edu NR 9 TC 1 Z9 1 U1 0 U2 2 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD JUN PY 2003 VL 51 IS 2 BP 445 EP 462 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 764TY UT WOS:000188223200017 PM 15162738 ER PT J AU De Queiroz, K Poe, S AF De Queiroz, K Poe, S TI Failed refutations: Further comments on parsimony and likelihood methods and their relationship to Popper's degree of corroboration SO SYSTEMATIC BIOLOGY LA English DT Article DE assumptions; corroboration; Karl Popper; likelihood; parsimony; philosophy; phylogenetics; probability ID MAXIMUM-LIKELIHOOD; PHYLOGENETIC INFERENCE; EVOLUTIONARY TREES; SUBSTITUTION; MODELS; SYSTEMATICS; CONSEQUENCES; CONJECTURES; HYPOTHESES; PHILOSOPHY AB Kluge's (2001, Syst. Biol. 50: 322 - 330) continued arguments that phylogenetic methods based on the statistical principle of likelihood are incompatible with the philosophy of science described by Karl Popper are based on false premises related to Kluge's misrepresentations of Popper's philosophy. Contrary to Kluge's conjectures, likelihood methods are not inherently verificationist; they do not treat every instance of a hypothesis as confirmation of that hypothesis. The historical nature of phylogeny does not preclude phylogenetic hypotheses from being evaluated using the probability of evidence. The low absolute probabilities of hypotheses are irrelevant to the correct interpretation of Popper's concept termed degree of corroboration, which is defined entirely in terms of relative probabilities. Popper did not advocate minimizing background knowledge; in any case, the background knowledge of both parsimony and likelihood methods consists of the general assumption of descent with modification and additional assumptions that are deterministic, concerning which tree is considered most highly corroborated. Although parsimony methods do not assume ( in the sense of entailing) that homoplasy is rare, they do assume ( in the sense of requiring to obtain a correct phylogenetic inference) certain things about patterns of homoplasy. Both parsimony and likelihood methods assume ( in the sense of implying by the manner in which they operate) various things about evolutionary processes, although violation of those assumptions does not always cause the methods to yield incorrect phylogenetic inferences. Test severity is increased by sampling additional relevant characters rather than by character reanalysis, although either interpretation is compatible with the use of phylogenetic likelihood methods. Neither parsimony nor likelihood methods assess test severity ( critical evidence) when used to identify a most highly corroborated tree(s) based on a single method or model and a single body of data; however, both classes of methods can be used to perform severe tests. The assumption of descent with modification is insufficient background knowledge to justify cladistic parsimony as a method for assessing degree of corroboration. Invoking equivalency between parsimony methods and likelihood models that assume no common mechanism emphasizes the necessity of additional assumptions, at least some of which are probabilistic in nature. Incongruent characters do not qualify as falsifiers of phylogenetic hypotheses except under extremely unrealistic evolutionary models; therefore, justifications of parsimony methods as falsificationist based on the idea that they minimize the ad hoc dismissal of falsifiers are questionable. Probabilistic concepts such as degree of corroboration and likelihood provide a more appropriate framework for understanding how phylogenetics conforms with Popper's philosophy of science. Likelihood ratio tests do not assume what is at issue but instead are methods for testing hypotheses according to an accepted standard of statistical significance and for incorporating considerations about test severity. These tests are fundamentally similar to Popper's degree of corroboration in being based on the relationship between the probability of the evidence e in the presence versus absence of the hypothesis h, i.e., between p(e\hb) and p(e\b), where b is the background knowledge. Both parsimony and likelihood methods are inductive in that their inferences ( particular trees) contain more information than ( and therefore do not follow necessarily from) the observations upon which they are based; however, both are deductive in that their conclusions ( tree lengths and likelihoods) follow necessarily from their premises ( particular trees, observed character state distributions, and evolutionary models). For these and other reasons, phylogenetic likelihood methods are highly compatible with Karl Popper's philosophy of science and offer several advantages over parsimony methods in this context. C1 Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. RP De Queiroz, K (reprint author), Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM dequeiroz.kevin@nmnh.si.edu NR 41 TC 20 Z9 20 U1 1 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD JUN PY 2003 VL 52 IS 3 BP 352 EP 367 DI 10.1080/10635150390196984 PG 16 WC Evolutionary Biology SC Evolutionary Biology GA 680VL UT WOS:000182999600005 PM 12775524 ER PT J AU Harshman, J Huddleston, CJ Bollback, JP Parsons, TJ Braun, MJ AF Harshman, J Huddleston, CJ Bollback, JP Parsons, TJ Braun, MJ TI True and false gharials: A nuclear gene phylogeny of Crocodylia SO SYSTEMATIC BIOLOGY LA English DT Article DE c-myc; crocodylia; data conflict; data partitions; partitioned likelihood analysis; phylogeny; rooting ID DATA SET INCONGRUENCE; DNA-SEQUENCE DATA; C-MYC; NUCLEOTIDE-SEQUENCE; EVOLUTIONARY TREES; BAYESIAN-INFERENCE; MITOCHONDRIAL-DNA; SYSTEMATICS; FAMILY; BIOGEOGRAPHY AB The phylogeny of Crocodylia offers an unusual twist on the usual molecules versus morphology story. The true gharial (Gavialis gangeticus) and the false gharial (Tomistoma schlegelii), as their common names imply, have appeared in all cladistic morphological analyses as distantly related species, convergent upon a similar morphology. In contrast, all previous molecular studies have shown them to be sister taxa. We present the first phylogenetic study of Crocodylia using a nuclear gene. We cloned and sequenced the c-myc proto-oncogene from Alligator mississippiensis to facilitate primer design and then sequenced an 1,100-base pair fragment that includes both coding and noncoding regions and informative indels for one species in each extant crocodylian genus and six avian outgroups. Phylogenetic analyses using parsimony, maximum likelihood, and Bayesian inference all strongly agreed on the same tree, which is identical to the tree found in previous molecular analyses: Gavialis and Tomistoma are sister taxa and together are the sister group of Crocodylidae. Kishino-Hasegawa tests rejected the morphological tree in favor of the molecular tree. We excluded long-branch attraction and variation in base composition among taxa as explanations for this topology. To explore the causes of discrepancy between molecular and morphological estimates of crocodylian phylogeny, we examined puzzling features of the morphological data using a priori partitions of the data based on anatomical regions and investigated the effects of different coding schemes for two obvious morphological similarities of the two gharials. C1 Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Suitland, MD 20746 USA. Univ Rochester, Dept Biol, Rochester, NY 14627 USA. Univ Calif San Diego, Sect Ecol Behav & Evolut, Div Biol Sci, La Jolla, CA 92093 USA. Armed Forces Inst Pathol, US Armed Forces DNA Identificat Lab, Rockville, MD 20850 USA. RP Harshman, J (reprint author), Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Suitland, MD 20746 USA. EM jharshman@pacbell.net; braun@lab.si.edu NR 64 TC 61 Z9 64 U1 0 U2 14 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 EI 1076-836X J9 SYST BIOL JI Syst. Biol. PD JUN PY 2003 VL 52 IS 3 BP 386 EP 402 DI 10.1080/10635150390197028 PG 17 WC Evolutionary Biology SC Evolutionary Biology GA 680VL UT WOS:000182999600008 PM 12775527 ER PT J AU Langley, HD AF Langley, HD TI From the collection: Warren Opie's sailor's uniform at Winterthur SO WINTERTHUR PORTFOLIO-A JOURNAL OF AMERICAN MATERIAL CULTURE LA English DT Article AB A visitor's curiosity about the garb of a sailor in a Winterthur exhibit led him to investigate the uniform and the person who wore it. The result is a brief sketch of the life of Warren Opie of Burlington, New Jersey, and his participation in the expedition of Commo. Matthew C. Perry to open Japan to American commerce. Also discussed are the decorations on Opie's uniform and sea bag and thier significance to his life and service. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0084-0416 J9 WINTERTHUR PORTFOLIO JI Winterthur Portfol.-J. Amer. Mater. Cult. PD SUM-FAL PY 2003 VL 38 IS 2-3 BP 131 EP 141 DI 10.1086/421424 PG 11 WC Art SC Art GA 812TI UT WOS:000220861400003 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, MC Thaddeus, P TI Rotational spectrum and structure of Si-3 SO PHYSICAL REVIEW LETTERS LA English DT Article ID SMALL SILICON CLUSTERS; LABORATORY MEASUREMENT; GROUND-STATE; LINE SURVEY; SIC2; IRC+10216; IONS AB The rotational spectrum of a pure silicon cluster, the Si-3 trimer, has been observed for the first time. From the rotational constants of the normal and the Si-29 and Si-30 isotopic species, a precise geometrical structure has been derived: the trimer is an isosceles triangle with a bond to the apex Si of length 2.177(1) Angstrom and an apex angle of 78.10(3)degrees. The substantial inertial defect and fairly large centrifugal distortion suggest that the molecule possesses a shallow bending potential. Si-3 is a good candidate for astronomical detection because radio lines of comparably massive silicon molecules (e.g., SiC2, SiC4, and SiS) are readily observed in at least one astronomical source. The rotational spectra of Si-6, Si-9, and even larger polar silicon clusters may be detectable with the present technique, as well as similar germanium clusters. 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. NR 36 TC 34 Z9 34 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 MAY 30 PY 2003 VL 90 IS 21 AR 213003 DI 10.1103/PhysRevLett.90.213003 PG 4 WC Physics, Multidisciplinary SC Physics GA 684TV UT WOS:000183223400015 PM 12786553 ER PT J AU Towe, KM AF Towe, KM TI Evolution of protein amino acids 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 4 Z9 4 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 30 PY 2003 VL 300 IS 5624 BP 1370 EP 1371 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 683ZW UT WOS:000183181800019 PM 12775820 ER PT J AU Smith, HA Rebbert, M Sternberg, O AF Smith, HA Rebbert, M Sternberg, O TI Designer infrared filters using stacked metal lattices SO APPLIED PHYSICS LETTERS LA English DT Article ID BAND-GAP STRUCTURES AB We have designed and fabricated infrared filters for use at wavelengths greater than or similar to 15 microns. Unlike conventional dielectric filters used at the short wavelengths, ours are made from stacked metal grids, spaced at a very small fraction of the performance wavelengths. The individual lattice layers are gold, the spacers are polyimide, and they are assembled using integrated circuit processing techniques; they resemble some metallic photonic band-gap structures. We simulate the filter performance accurately, including the coupling of the propagating, near-field electromagnetic modes, using computer aided design codes. We find no anomalous absorption. The geometrical parameters of the grids are easily altered in practice, allowing for the production of tuned filters with predictable useful transmission characteristics. Although developed for astronomical instrumentation, the filters are broadly applicable in systems across infrared and terahertz bands. (C) 2003 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Washington, DC 20375 USA. RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 18 Z9 18 U1 0 U2 7 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAY 26 PY 2003 VL 82 IS 21 BP 3605 EP 3607 DI 10.1063/1.1579115 PG 3 WC Physics, Applied SC Physics GA 680TB UT WOS:000182993700007 ER PT J AU Mege, D Cook, AC Garel, E Lagabrielle, Y Cormier, MH AF Mege, D Cook, AC Garel, E Lagabrielle, Y Cormier, MH TI Volcanic rifting at Martian grabens SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review DE rifting; graben; pit crater; magma chamber; dyke ID EAST PACIFIC RISE; ORBITER LASER ALTIMETER; FAST SPREADING RIDGES; GIANT DIKE SWARMS; VALLES-MARINERIS; SURFACE DEFORMATION; INTERNAL STRUCTURE; MIDOCEAN RIDGE; MAGMA CHAMBERS; PLATE BOUNDARY AB [1] A large fraction of surface extension on Mars occurred at segmented grabens having width/length ratios akin to oceanic rifts on Earth. Association with volcanic landforms such as pit craters clearly suggests interconnection between tectonic and magmatic processes. A Martian rift evolution model is proposed on the basis of new geomorphological and structural interpretations of imagery, high-resolution digital elevation models (DEMs), scaled experimental modeling and three-dimensional boundary element modeling of magmatic and tectonic processes, and a comparison with terrestrial rifts. The DEMs were obtained from Mars Observer Laser Altimeter, Viking Orbiter stereo images, or a combination of both. Comparison of terrestrial rifts included Afar, Iceland, and the East Pacific Rise. The ambient extensional stress field induced by regional body forces is combined at depth with decompression melting and mantle plume thermal anomaly, resulting in emplacement of elongated magma reservoirs along the grabens. Injection of dikes above the reservoirs and flood basalt eruption result in a reservoir underpressurization of up to hundreds of MPa and induces surface collapse. Each collapse event is associated with an eruption of volcanic volumes akin to those of individual flow eruptions in large terrestrial igneous provinces. The geometry and mechanisms of graben formation and surface collapse are described and used to infer reservoir depth and width. We conclude from this study that giant dike swarms akin to typical giant terrestrial dike swarms are unlikely to underlie the volcanic Martian grabens on the basis one graben-one dike. Rather, every volcanic graben segment appears to own a local dike swarm perhaps analogous to the dike swarms in the Icelandic fissure zones. C1 Univ Paris 06, Lab Tecton, CNRS, UMR 7072, F-75252 Paris 05, France. Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Maine, Lab Geodynam Rifts & Marges Pass, F-72085 Le Mans 9, France. Univ Bretagne Occidentale, Inst Rech Dev, CNRS, UMR 6538, F-29280 Plouzane, France. Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Mege, D (reprint author), Univ Paris 06, Lab Tecton, CNRS, UMR 7072, Boite 129,4 Pl Jussieu, F-75252 Paris 05, France. EM dmege@lgs.jussieu.fr; acc@cs.nott.ac.uk; Erwan.Garel@univ-lemans.fr; yvesla@univ-brest.fr; cormier@ldeo.columbia.edu RI Mege, Daniel/A-2331-2009; OI Mege, Daniel/0000-0003-4304-9878 NR 149 TC 44 Z9 44 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY 22 PY 2003 VL 108 IS E5 AR 5044 DI 10.1029/2002JE001852 PG 33 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 683YY UT WOS:000183179700001 ER PT J AU Zimbelman, JR AF Zimbelman, JR TI Flow field stratigraphy surrounding Sekmet Mons Volcano, Kawelu Planitia, Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE fracture zones; pahoehoe; Strenia Fluctus; effusion rate; Carrizozo; northern lowlands ID GLOBAL DISTRIBUTION; IMPACT CRATERS; LAVA FLOWS; RADAR DATA; EMPLACEMENT; MAGELLAN; BASALT; ASSOCIATIONS; EVOLUTION; FEATURES AB [1] Detailed mapping has revealed several stratigraphic components among lobate plains in the vicinity of Sekmet Mons volcano (44.5degreesN. lat., 240.5degrees long.), located on the northern lowland plains of Kawelu Planitia on Venus. Volcanic effusion events produced discrete lobate plains throughout the area. Superposition of flow margins between adjacent lobate plains components indicate that the effusive activity generally progressed from southwest to northeast across the Sekmet Mons area, leading to a cumulative total of 1.5 million km(2) covered by adjacent lobate plains components. Source areas for the effusion responsible for the lobate plains components occur primarily along fracture zones or from concentrations of low volcanic domes ("shield fields'') instead of from single constructs. Magellan radar backscatter values from a mixture of both radar bright and radar dark flow components within the flow fields are well below values typical of clinkery a a lava flows on Earth, but they are consistent with values from terrestrial pahoehoe flows. Detailed mapping of Strenia Fluctus (centered on 41.5degrees N. lat., 251.0degrees long.), one of the latest lobate plains units in the area, does not show a systematic trend among effusive centers that contributed to the generation of this flow field. Instead, the Strenia Fluctus flow field is a complex mixture of flows that emanated from a shield field along Mist Chasma and that flowed down a very gentle (>0.1degrees) regional slope to the east. A 4-km-diameter cone north of Strenia Fluctus was the source of a flow complex traceable for more than 200 km over a slope of only 0.03degrees. Individual flows within Strenia Fluctus are composed of intermixed lobes, similar to relationships observed on the distal portion of the 75-km-long Carrizozo basalt flow in New Mexico, which also displays abundant inflation features and a predominant pahoehoe surface texture. If the Venusian lobate plains consist of pahoehoe flows comparable to the Carrizozo flow, they were most likely emplaced at modest effusion rates (similar to50 to 500 m(3)/s), and even with inflation the flows are likely less than or equal to15 m in thickness. Under these conditions all of the lobate plains surrounding Sekmet Mons could have been emplaced in similar to14,000 to 1400 Earth years, assuming continuous effusion with only one source vent active at a time. At similar rates all of the lowland plains in the northern hemisphere of Venus could have been resurfaced by 15-m-thick flows through continuous single-vent effusion in similar to1.4 million to similar to140 thousand Earth years. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Zimbelman, JR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 59 TC 1 Z9 1 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY 21 PY 2003 VL 108 IS E5 AR 5043 DI 10.1029/2002JE001965 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 683YX UT WOS:000183179600001 ER PT J AU Sankrit, R Blair, WP Raymond, JC AF Sankrit, R Blair, WP Raymond, JC TI Optical and far-ultraviolet spectroscopy of knot D in the Vela supernova remnant SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Vela Supernova Remnant); shock waves; supernova remnants; ultraviolet : ISM ID X-RAY; CYGNUS-LOOP; RADIATIVE SHOCKS; ABSORPTION LINES; RX J0852.0-4622; HIGH-VELOCITY; EMITTING GAS; TELESCOPE; PERFORMANCE; CALIBRATION AB We present spectra of optical. laments associated with the X-ray knot D in the Vela supernova remnant. It has been suggested that knot D is formed by a bullet of supernova ejecta, that it is a breakout of the shock front of the Vela supernova remnant, and also that it is an outflow from the recently discovered remnant RX J0852.0-4622. We find that knot D is a bow shock propagating into an interstellar cloud with normal abundances and typical cloud densities (n(H) similar to 4-11 cm(-3)). Optical long-slit spectra show that the [S II] lambdalambda6716, 6731 to Halpha line ratio is greater than unity, proving that the optical. laments are shock excited. The analysis of far-ultraviolet spectra obtained with the Hopkins Ultraviolet Telescope and with the Far Ultraviolet Spectroscopic Explorer ( FUSE) LWRS aperture show that slower shocks (similar to100 km s(-1)) produce most of the low-ionization lines such as O III] lambda1662, while faster shocks (similar to180 km s(-1)) produce the O VI lambdalambda1032, 1038 and other high-ionization lines. C III and O vi lines are also detected in the FUSE MDRS aperture, which was located on an X-ray-bright region away from the optical. laments. The lines have two velocity components consistent with similar to 150 km s(-1) shocks on the near and far sides of the knot. The driving pressure in the X-ray knot, P/k(B) similar to 1.8 x 10(7) cm(-3) K, is derived from the shock properties. This is over an order of magnitude larger than the characteristic X-ray pressure in the Vela supernova remnant. The velocity distribution of the emission and the overpressure support the idea that knot D is a bow shock around a bullet or cloud that originated near the center of the Vela remnant. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sankrit, R (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM ravi@pha.jhu.edu; wpb@pha.jhu.edu; jraymond@cfa.harvard.edu NR 42 TC 19 Z9 19 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 2003 VL 589 IS 1 BP 242 EP 252 DI 10.1086/374591 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679VW UT WOS:000182943500019 ER PT J AU Trinidad, MA Curiel, S Canto, J D'Alessio, P Rodriguez, LF Torrelles, JM Gomez, JF Patel, N Ho, PTP AF Trinidad, MA Curiel, S Canto, J D'Alessio, P Rodriguez, LF Torrelles, JM Gomez, JF Patel, N Ho, PTP TI Observations of water masers and radio continuum emission in AFGL 2591 SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (AFGL 2591); ISM : jets and outflows; masers; stars : formation ID YOUNG STELLAR OBJECTS; ACCRETION DISKS; MOLECULAR OUTFLOWS; VLA OBSERVATIONS; H2O MASERS; CEPHEUS-A; STAR; SYSTEM; GL-2591; JET AB We report results of continuum (1.3 and 3.6 cm) and H2O maser line high angular resolution observations, made with the Very Large Array (VLA) in the A configuration, toward the star-forming region AFGL 2591. Three radio continuum sources (VLA 1, VLA 2, and VLA 3) were detected in the region at 3.6 cm, and one source (VLA 3) at 1.3 cm. VLA 1 and VLA 2 appear resolved and their spectral indices suggest free-free emission from optically thin H II regions. VLA 3 is elongated in the east-west direction, along the axis of the bipolar molecular outflow observed in the region. Its spectral energy distribution is consistent with it being a similar to200 AU optically thick disk plus a photoionized wind. In addition, we detected 85 water maser spots toward the AFGL 2591 region, which are distributed in three main clusters. Two of these clusters are spatially associated with VLA 2 and VLA 3, respectively. The third cluster of masers, including the strongest water maser of the region, does not coincide with any known continuum source. We suggest that this third cluster of masers is excited by an undetected protostar that we predict to be located similar or equal to0."5 (500 AU) north from VLA 3. The maser spots associated with VLA 3 are distributed along a shell-like structure of 0."01 size, showing a peculiar velocity-position helical distribution. We propose that VLA 3 is the powering source of the observed molecular outflow in this region. Finally, we support the notion that the AFGL 2591 region is a cluster of B0-B3 type stars. C1 Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico. Univ Nacl Autonoma Mexico, Astron Inst, Morelia 58089, Michoacan, Mexico. CSIC, Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain. 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, Astron Inst, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 50 TC 39 Z9 39 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2003 VL 589 IS 1 BP 386 EP 396 DI 10.1086/374618 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679VW UT WOS:000182943500030 ER PT J AU Ford, KES Neufeld, DA Goldsmith, PF Melnick, GJ AF Ford, KES Neufeld, DA Goldsmith, PF Melnick, GJ TI Detection of OH toward the extreme carbon star IRC+10216 SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : general; Kuiper Belt; planetary systems; radio lines : stars; stars : AGB and post-AGB; stars : individual (IRC+10216) ID CIRCUMSTELLAR DUST SHELLS; GIANT BRANCH STARS; MULTIPLE SHELLS; WATER-VAPOR; ENVELOPE; MASER; GAS; IRC; EVOLUTION; DISCOVERY AB We report the detection of the 1665 and 1667 MHz main lines of OH ( hydroxyl) and upper limits on the 1612 MHz satellite line of OH toward the carbon-rich AGB star IRC + 10216. We find a beam-averaged fractional abundance x(OH) similar to4 x 10(-8). This detection supports the identification by Melnick et al. of the 1(10)-1(01) transition of water vapor with a 556.936 GHz rest-frequency emission feature detected toward IRC + 10216, since OH is the expected photodissociation product of water vapor. The shape of the OH lines, however, differs significantly from the shape expected on the basis of the observations of Melnick et al. Possible explanations for the anomalous shapes of the 1665 and 1667 MHz lines are discussed. The most likely explanations for the unexpected OH line shapes are either masing or an asymmetric distribution of OH molecules around IRC + 10216. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Dept Astron, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ford, KES (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RI Goldsmith, Paul/H-3159-2016 NR 29 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 MAY 20 PY 2003 VL 589 IS 1 BP 430 EP 438 DI 10.1086/374552 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679VW UT WOS:000182943500034 ER PT J AU Maness, HL Vrtilek, SD Kastner, JH Soker, N AF Maness, HL Vrtilek, SD Kastner, JH Soker, N TI Abundance anomalies in the X-ray spectra of planetary nebulae NGC 7027 and BD +30 degrees 3639 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary nebulae : general; planetary nebulae : individual; (BD+30 degrees 3639, NGC 7027); stars : winds, outflows; X-rays : ISM ID NGC-7027; EMISSION; BD+30-DEGREES-3639; MODEL; DUST; STARS; PLASMAS; NOVA AB We revisit Chandra observations of planetary nebulae NGC 7027 and BD + 30degrees3639 in order to address the question of abundance anomalies in the X-ray-emitting gas. Enhanced abundances relative to solar of magnesium (Mg) for NGC 7027 and neon (Ne) for BD + 30degrees3639 are required to fit their X-ray spectra, whereas observations at optical and infrared wavelengths show depleted Mg and Ne in these systems. We attribute the enhancement of Mg in NGC 7027 in the X-ray, relative to the optical, to the depletion of Mg onto dust grains within the optical nebula. For BD + 30degrees3639, we speculate that the highly enhanced Ne comes from a white dwarf companion, which accreted a fraction of the wind blown by the asymptotic giant branch progenitor and went through a novalike outburst that enriched the X-ray-emitting gas with Ne. C1 Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. Dept Phys, IL-36006 Oranim, Tivon, Israel. RP Maness, HL (reprint author), Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. NR 34 TC 16 Z9 16 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2003 VL 589 IS 1 BP 439 EP 443 DI 10.1086/374414 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679VW UT WOS:000182943500035 ER PT J AU Evans, NR Seward, FD Krauss, MI Isobe, T Nichols, J Schlegel, EM Wolk, SJ AF Evans, NR Seward, FD Krauss, MI Isobe, T Nichols, J Schlegel, EM Wolk, SJ TI Chandra observations of associates of eta Carinae. I. Luminosities SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (Trumpler 14, Trumpler 16); X-rays : stars ID WOLF-RAYET STARS; X-MEGA TARGETS; O-TYPE STARS; OPEN CLUSTER TRUMPLER-14; OPTICAL SPECTROSCOPY; ORION-NEBULA; FUNDAMENTAL PARAMETERS; PROGENITOR MASSES; MULTIPLE SYSTEM; STELLAR CONTENT AB The region around the eta Carinae Nebula has three OB associations, which contain a Wolf-Rayet star and several massive O3 stars. An early Chandra ACIS-I image was centered on eta Car and includes Trumpler 16 and part of Trumpler 14. The Chandra image confirms the well-known result that O and very early B stars are X-ray sources with L-X similar or equal to 10(-7) L-bol over an X-ray luminosity range of about 100. Two new, anomalously strong X-ray sources have been found among the hot star population: Tr 16-244, a heavily reddened O3 I star, and Tr 16-22, a heavily reddened O8.5 V star. Two stars have an unusually large L-X/L-bol: HD 93162, a Wolf-Rayet star ( and possible binary), and Tr 16-22, a possible colliding-wind binary. In addition, a population of sources associated with cool stars is detected. In the color-magnitude diagram, these X-ray sources sit above the sequence of field stars in the Carina arm. The OB stars are on average more X-ray-luminous than the cool star X-ray sources. X-ray sources among A stars have X-ray luminosities similar to those of cooler stars and may be due to cooler companions. Upper limits are presented for B stars that are not detected in X-rays. These upper limits are also the upper limits for any cool companions that the hot stars may have. Hardness ratios are presented for the most luminous sources in bands 0.5-0.9, 0.9-1.5, and 1.5-2.04 keV. The available information on the binary nature of the hot stars is discussed, but binarity does not correlate with X-ray strength in a simple way. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. NR 45 TC 33 Z9 33 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2003 VL 589 IS 1 BP 509 EP 525 DI 10.1086/374355 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679VW UT WOS:000182943500042 ER PT J AU Nicastro, F Martocchia, A Matt, G AF Nicastro, F Martocchia, A Matt, G TI The lack of broad-line regions in low accretion rate active galactic nuclei as evidence of their origin in the accretion disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies : active; quasars : emission lines ID SEYFERT-2 GALAXIES; EMISSION AB In this Letter, we present evidence suggesting that the absence or presence of hidden broad-line regions (HBLRs) in Seyfert 2 galaxies is regulated by the rate at which matter accretes onto a central supermassive black hole, in units of the Eddington rate. Evidence is based on data from a subsample of type 2 active galactic nuclei extracted from the Tran spectropolarimetric sample and made up of all those sources that also have good-quality X-ray spectra available and for which a bulge luminosity can be estimated. We use the intrinsic (i.e., unabsorbed) Xray luminosities of these sources and their black hole masses ( estimated by using the well-known relationship between nuclear mass and bulge luminosity in galaxies) to derive the nuclear accretion rate in Eddington units. We find that virtually all HBLR sources have accretion rates larger than a threshold value of (m) over dot(thres) similar or equal to 10(-3) (in Eddington units), while non-HBLR sources lie at (m) over dot less than or similar to (m) over dot(thres). These data nicely fit predictions from a model proposed by Nicastro in which the broad- line regions ( BLRs) are formed by accretion disk instabilities occurring in proximity of the critical radius at which the disk changes from gas pressure dominated to radiation pressure dominated. This radius diminishes with decreasing (m) over dot; for low enough accretion rates ( and therefore luminosities),. the critical radius becomes smaller than the innermost stable orbit and BLRs cannot form. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. Astron Observ, F-67000 Strasbourg, France. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 21 TC 78 Z9 78 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2003 VL 589 IS 1 BP L13 EP L16 DI 10.1086/375715 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679WA UT WOS:000182943900004 ER PT J AU Handler, MR Wysoczanski, RJ Gamble, JA AF Handler, MR Wysoczanski, RJ Gamble, JA TI Proterozoic lithosphere in Marie Byrd Land, West Antarctica: Re-Os systematics of spinel peridotite xenoliths SO CHEMICAL GEOLOGY LA English DT Article DE Re-Os isotopes; continental lithospheric mantle; xenoliths; Marie Byrd Land; West Antarctica ID IONIZATION MASS-SPECTROMETRY; OSMIUM ISOTOPIC COMPOSITION; OCEANIC ISLAND BASALTS; MANTLE-PLUME ACTIVITY; NEW-ZEALAND; SOUTHEASTERN AUSTRALIA; SUBCONTINENTAL MANTLE; SUBDUCTION ZONES; PACIFIC MARGIN; UNITED-STATES AB Marie Byrd Land, which forms part of the composite West Antarctica microplate, experienced a long history of subduction during Paleozoic and Mesozoic times, and has been argued to have been affected by at least one mantle plume. The age of the Marie Byrd Land lithosphere is not known, as the only lower crustal samples (granulite and pyroxenite xenoliths) have proven resistant to conventional radiogenic dating methods. The oldest exposed magmatic rocks are Cambrian, and any Precambrian history for Marie Byrd Land, while speculated upon, is unknown. Here we present the first geochemical data for a peridotite xenolith suite from Marie Byrd Land, including Re-Os isotope measurements for 17 samples. The 17 spinel peridotites are from three volcanic centers: Mt Hampton and Mt Cumming, in the Executive Committee Range, and Mt Aldaz, in the USAS Escarpment. The xenoliths are residual lherzolites and harzburgites, ranging from fertile to depleted (e.g. 0.39-3.38 wt.% CaO) compositions. Re-Os isotopic systematics indicate a complex evolution for the Marie Byrd Land lithosphere. One sample records Re + Cu +/- Os enrichment and two samples document localized Os enrichment, which is most likely related to supra-subduction zone processing, although enrichment due to plume interaction cannot be ruled out. Proterozoic lithosphere stabilization model ages of ca. 1.1 and > 1.3 Ga are recorded in xenoliths from the Executive Committee Range. The Proterozoic ages are significantly older than outcropping mid-crustal rocks, marking Marie Byrd Land as a third circum-Pacific Phanerozoic mobile belt with preserved Proterozoic lithospheric mantle. The Mesoproterozoic Os model ages are consistent with Proterozoic Nd model ages in Marie Byrd Land granites and orthogneisses, and with a significant detrital zircon age component (ca. 1.0-1.2 Ga) in the thick Swanson Formation sediments that are exposed along the coast. The simplest interpretation of the available mantle and crustal age data is that the lower crust beneath Marie Byrd Land is also Proterozoic in age. Alternatively, if the mantle and lower crust in Marie Byrd Land are not temporally coupled, possible origins for the Proterozoic mantle include older lithosphere impinging from the adjacent East Antarctic craton, or lithospheric mantle that was incorporated into younger oceanic lithosphere during "messy" continental breakup (e.g. within an oceanic plateau) and subsequently accreted to the Antarctic margin. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Carnegie Inst Washington, DTM, Washington, DC 20015 USA. Smithsonian Inst, NMNH, Dept Mineral Sci, Washington, DC 20560 USA. Victoria Univ Wellington, Dept Geol, Wellington, New Zealand. RP Handler, MR (reprint author), JAMSTEC, IFREE, 2-15 Natsushima Cho, Kanagawa 2370061, Japan. EM monica@jamstec.go.jp RI Wysoczanski, Richard/C-2930-2009; Handler`, Monica/E-9460-2011; Wysoczanski, Richard/I-7730-2012 OI Handler`, Monica/0000-0001-7095-0835; NR 80 TC 31 Z9 33 U1 2 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 J9 CHEM GEOL JI Chem. Geol. PD MAY 15 PY 2003 VL 196 IS 1-4 BP 131 EP 145 DI 10.1016/S0009-2541(02)00410-2 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 671HA UT WOS:000182458200008 ER PT J AU Parkinson, WH Rufus, J Yoshino, K AF Parkinson, WH Rufus, J Yoshino, K TI Absolute absorption cross section measurements of CO2 in the wavelength region 163-200 nm and the temperature dependence SO CHEMICAL PHYSICS LA English DT Article DE carbon dioxide; cross sections ID CARBON-DIOXIDE; HIGH-RESOLUTION; SPECTRUM; PHOTODISSOCIATION; ATMOSPHERE; TRANSITION; MARS AB Laboratory measurements of the absorption cross section Of CO2 at the temperatures 195 and 295 K have been made throughout the wavelength region 163-200 nm by using a high resolution grating spectrometer. Cross sections at 195 K are smaller than those at 295 K, and the band structures are more emphasized as expected. In combining with our previous measurements [J. Quant. Spectrosc. Radiat. Transfer, 55 (1996) 53], the absorption cross sections Of CO2 are available in the wavelength region 117.8-200.0 nm at 295 K and 117.8-192.5 nm at 195 K. (C) 2003 Elsevier Science B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoshino, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-50, Cambridge, MA 02138 USA. NR 18 TC 38 Z9 38 U1 1 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD MAY 15 PY 2003 VL 290 IS 2-3 BP 251 EP 256 DI 10.1016/S0301-0104(03)00146-0 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 679ZA UT WOS:000182950800012 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Ceanne and Provence: The painter in his culture. 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 15 PY 2003 VL 128 IS 9 BP 84 EP 84 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 678RN UT WOS:000182880400042 ER PT J AU Riley, S AF Riley, S TI Brilliant. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 15 PY 2003 VL 128 IS 9 BP 125 EP 125 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 678RN UT WOS:000182880400230 ER PT J AU Chandra, S Ziemke, JR Martin, RV AF Chandra, S Ziemke, JR Martin, RV TI Tropospheric ozone at tropical and middle latitudes derived from TOMS/MLS residual: Comparison with a global model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE biomass burning; tropospheric ozone; stratospheric ozone; El Nino; global circulation model; tropopause ID SOUTH-ATLANTIC-OCEAN; 1997-1998 EL-NINO; STRATOSPHERIC OZONE; UNITED-STATES; COLUMN OZONE; WATER-VAPOR; 3-D MODELS; PACIFIC; CHEMISTRY; POLLUTION AB The tropospheric ozone residual method is used to derive zonal maps of tropospheric column ozone using concurrent measurements of total column ozone from Nimbus 7 and Earth Probe (EP) Total Ozone Mapping Spectrometer (TOMS) and stratospheric column ozone from the Microwave Limb Sounder (MLS) instrument on the Upper Atmosphere Research Satellite (UARS). Our study shows that the zonal variability in TOMS total column ozone at tropical and subtropical latitudes is mostly of tropospheric origin. The seasonal and zonal variability in tropospheric column ozone (TCO), derived from the TOMS/MLS residual, is consistent with that derived from the convective cloud differential method and ozonesonde measurements in regions where these data overlap. A comparison of TCO derived from the TOMS/MLS residual and a global three-dimensional model of tropospheric chemistry (GEOS-CHEM) for 1996-1997 shows good agreement in the tropics south of the equator. Both the model and observations show similar zonal and seasonal characteristics including an enhancement of TCO in the Indonesian region associated with the 1997 El Nino. Both show the decline of the wave-1 pattern from the tropics to the extratropics as lightning activity and the Walker circulation decline. Both show enhanced ozone in the downwelling branches of the Hadley Circulation near +/-30degrees. Model and observational differences increase with latitude during winter and spring. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Div Engn & Appl Sci, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP NASA, Goddard Space Flight Ctr, Code 916, Greenbelt, MD 20771 USA. EM chandra@chapman.gsfc.nasa.gov; ziemke@jwocky.gsfc.nasa.gov; rvmartin@fas.harvard.edu RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; NR 57 TC 34 Z9 34 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 13 PY 2003 VL 108 IS D9 AR 4291 DI 10.1029/2002JD002912 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 682QN UT WOS:000183103300009 ER PT J AU Molbo, D Machado, CA Sevenster, JG Keller, L Herre, EA AF Molbo, D Machado, CA Sevenster, JG Keller, L Herre, EA TI Cryptic species of fig-pollinating wasps: Implications for the evolution of the fig-wasp mutualism, sex allocation, and precision of adaptation SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE coevolution; symbiosis; fig wasp; ficus; local mate competition ID MITOCHONDRIAL-DNA SEQUENCES; PHYLOGENETIC-RELATIONSHIPS; RATIOS; FICUS; COOPERATION; AGAONIDAE; CONFLICT; BIOGEOGRAPHY; SPECIFICITY; COEVOLUTION AB Fig-pollinating wasps have provided model systems for developing and testing theories of the evolution of mutualism, sex allocation, and precision of adaptation. With few exceptions, previous studies have assumed one species of pollinator wasp per host fig species. Here we report genetic data demonstrating the coexistence of previously undetected cryptic fig wasp species in at least half of the host fig species surveyed. The substantial mitochondrial sequence differences (4.2-6.1%) imply old divergences ( approximate to 1.5-5.1 million years ago) among these species. Furthermore, some cryptic species pairs seem to be sister taxa, whereas others clearly are not, indicating both long-term coexistence on shared hosts and the colonization of novel fig species. These findings undermine the prevalent notion of strict one-to-one specificity between cospeciating figs and their pollinators, thereby challenging existing theory concerning the evolution and stability of mutualisms. Moreover, the incorporation of the genetic information significantly improves the fit of the observed sex ratios to predictions of local mate-competition theory, further strengthening support for sex allocation theory and the precision of adaptation. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Lausanne, Inst Ecol, CH-1015 Lausanne, Switzerland. Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. Leiden Univ, Sect Anim Ecol, Inst Biol, NL-2300 RA Leiden, Netherlands. RP Herre, EA (reprint author), Smithsonian Trop Res Inst, Apartado 22072, Balboa, Panama. EM herrea@gamboa.si.edu RI Machado, Carlos/B-8855-2009; OI Machado, Carlos/0000-0003-1546-7415; keller, laurent/0000-0002-5046-9953; Molbo, Drude/0000-0003-3372-8711 NR 56 TC 187 Z9 205 U1 7 U2 64 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 MAY 13 PY 2003 VL 100 IS 10 BP 5867 EP 5872 DI 10.1073/pnas.0930903100 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 679UB UT WOS:000182939400056 PM 12714682 ER PT J AU Lee, S Pak, S Davis, CJ Herrnstein, RM Geballe, TR Ho, PTP Wheeler, JC AF Lee, S Pak, S Davis, CJ Herrnstein, RM Geballe, TR Ho, PTP Wheeler, JC TI Interaction between the north-eastern boundary of Sgr A East and giant molecular clouds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM : individual : Sgr A East; ISM : individual : M-0.02-0.07; ISM : lines and bands; ISM : molecules; Galaxy : centre; infrared : ISM ID SAGITTARIUS-A EAST; GALACTIC-CENTER; ORION NEBULA; PHOTODISSOCIATION REGIONS; RESOLUTION OBSERVATIONS; INTERSTELLAR SHOCKS; HYDROGEN EMISSION; GALAXY; MASERS; H-2 AB We have detected the v = 1 --> 0 S(1) (lambda= 2.1218 mum) and v = 2 --> 1 S(1) (lambda= 2.2477 mum) lines of H-2 in the Galactic Centre, in a 90 x 27 arcsec(2) region between the north-eastern boundary of the non-thermal source Sgr A East, and the giant molecular cloud (GMC) M-0.02 - 0.07. The detected H-2 v = 1 --> 0 S(1) emission has an intensity of 1.6-21 x 10(-18) W m(-2) arcsec(-2) and is present over most of the region. Along with the high intensity, the large linewidths (FWHM = 40-70 km s(-1) ) and the H-2 v = 2 --> 1 S(1) to v = 1 --> 0 S(1) line ratios (0.3-0.5) can be best explained by a combination of C-type shocks and fluorescence. The detection of shocked H-2 is clear evidence that Sgr A East is driving material into the surrounding adjacent cool molecular gas. The H-2 emission lines have two velocity components at similar to+50 and similar to0 km s(-1) , which are also present in the NH3 (3, 3) emission mapped by McGary, Coil & Ho. This two-velocity structure can be explained if Sgr A East is driving C-type shocks into both the GMC M-0.02 - 0.07 and the northern ridge of McGary et al. C1 Seoul Natl Univ, Astron Programme SEES, Seoul 151742, South Korea. Korea Astron Observ, Taejon 305348, South Korea. Joint Astron Ctr, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Gemini Observ, Hilo, HI 96720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Lee, S (reprint author), Seoul Natl Univ, Astron Programme SEES, Seoul 151742, South Korea. RI Pak, Soojong/E-2360-2013; OI Pak, Soojong/0000-0002-2548-238X NR 44 TC 11 Z9 11 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2003 VL 341 IS 2 BP 509 EP 516 DI 10.1046/j.1365-8711.2003.06425.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 674TE UT WOS:000182651400011 ER PT J AU Scappini, F Cecchi-Pestellini, C Smith, H Klemperer, W Dalgarno, A AF Scappini, F Cecchi-Pestellini, C Smith, H Klemperer, W Dalgarno, A TI Hydrated sulphuric acid in dense molecular clouds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM : clouds; dust, extinction; ISM : lines and bands; ISM : molecules; infrared : ISM ID HOT CORES; CHEMISTRY; WATER; SULFIDE; MODELS; ABUNDANCES; INVENTORY; EMISSIONS; DEPLETION; FEATURES AB We consider sulphur depletion in dense molecular clouds, and suggest hydrated sulphuric acid, H(2) SO(4) . n H(2) O, as a component of interstellar dust in icy mantles. We discuss the formation of hydrated sulphuric acid in collapsing clouds and its instability in heated regions in terms of the existing hot core models and observations. We also show that some features of the infrared spectrum of hydrated sulphuric acid have correspondence in the observed spectra of young stellar objects. C1 CNR, Ist Studio Mat Nanostrutturati, I-40129 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Chem, Cambridge, MA 02138 USA. RP Scappini, F (reprint author), CNR, Ist Studio Mat Nanostrutturati, Via P Gobetti 101, I-40129 Bologna, Italy. EM ccecchi-pestellini@cfa.harvard.edu OI Cecchi Pestellini, Cesare/0000-0001-7480-0324 NR 37 TC 15 Z9 15 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2003 VL 341 IS 2 BP 657 EP 661 DI 10.1046/j.1365-8711.2003.06443.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 674TE UT WOS:000182651400024 ER PT J AU Colley, WN Shapiro, II Pegg, J Turner, EL Kundic, T Loomis, K Hastings, NC McMillan, R AF Colley, WN Shapiro, II Pegg, J Turner, EL Kundic, T Loomis, K Hastings, NC McMillan, R TI Rapid brightness fluctuations in Q0957+561A,B: Microlensing or seeing? SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies : halos; gravitational lensing; methods : data analysis; quasars : individual (0957+561); techniques : photometric ID TIME-DELAY; PHOTOMETRY; 0957+561A AB We address the following question: How does one reliably distinguish rapid microlensing events from atmospheric or instrumental effects on observed brightness fluctuations of distant objects? Our approach was to do a controlled, albeit limited, experiment, the first of its kind: observe Q0957+561A,B simultaneously through filters of the same characteristics with two telescopes with comparable fields of view but separated sufficiently for atmospheric fluctuations to be independent. Over the 1998-1999 viewing season, we succeeded in obtaining simultaneous data on 14 of the 55 nights scheduled. Analysis of these data led to the following: (1) after correction for "blending'' of the A and B images, most rapid microlensing candidate outliers disappeared, and the agreement of the photometry from the two telescopes improved to an rms difference of about 15 mmag; (2) no microlensing events of amplitude greater than 0.1 mag were observed in either data set over the entire run, nearly ruling out similar to10(-5) M-circle dot MACHOs as composing more than about half the dark matter in the lens galaxy, if the source size is less than or similar to3x10(14) cm. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Renaissance Technol, E Setauket, NY 11733 USA. Apache Point Observ, Sunspot, NM 88349 USA. RP Colley, WN (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. RI Turner, Edwin/A-4295-2011 NR 9 TC 3 Z9 3 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2003 VL 588 IS 2 BP 711 EP 715 DI 10.1086/374308 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 680RV UT WOS:000182991900006 ER PT J AU Stepanian, JA Benitez, E Krongold, Y Cruz-Gonzalez, I de Diego, JA Chavushyan, V Mujica, R Dultzin-Hacyan, D Verdugo, T AF Stepanian, JA Benitez, E Krongold, Y Cruz-Gonzalez, I de Diego, JA Chavushyan, V Mujica, R Dultzin-Hacyan, D Verdugo, T TI A multiwavelength study of narrow-line Seyfert 1 galaxies from the Second Byurakan Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : Seyfert; quasars : general ID X-RAY PROPERTIES; ALL-SKY SURVEY; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; OPTICALLY SELECTED QUASARS; POINT-SOURCE CATALOG; WARM IRAS SOURCES; FE-II-EMISSION; COMPLETE SAMPLE; MARKARIAN GALAXIES AB In this work we present a multiwavelength study of narrow-line Seyfert 1 galaxies (NLS1s) discovered in the Second Byurakan Survey (SBS). The sample consists of 26 objects, which have M-B greater than or equal to -23.0, or -19.9>M-B>-23.0, 0.02431). The traditional linear correlation L-X and L-op, which seems to hold for active galactic nuclei in general, is found for SBS NLS1s. An anticorrelation between the FWHM of Hbeta and the ratio of Fe II lambda4570/Hbeta is also observed. A weak correlation is found between alpha(ox) slope and L-op. One of our main findings is that almost all SBS NLS1s may not have an FIR bump. Their spectral energy distribution suggests that they may also possess a big blue bump. The absence of an IR bump in most SBS NLS1s and the weakness of X-ray radiation in some of them may argue against the presence of a broad-line region. The surface density of SBS NLS1s is less than 0.015 deg(-2) (B<17.5; z<0.16). C1 Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Nacl Astrofis Opt & Elect, Puebla 7200, Mexico. RP Stepanian, JA (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. OI Verdugo, Tomas/0000-0003-4062-6123; Jose A., de Diego/0000-0001-7040-069X NR 75 TC 15 Z9 16 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2003 VL 588 IS 2 BP 746 EP 762 DI 10.1086/374215 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 680RV UT WOS:000182991900010 ER PT J AU Done, C Madejski, GM Zycki, PT Greenhill, LJ AF Done, C Madejski, GM Zycki, PT Greenhill, LJ TI Simultaneous Chandra and Rossi X-Ray Timing Explorer observations of the nearby bright Seyfert 2 galaxy NGC 4945 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4945); galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; MASER EMISSION; COLD MATTER; XMM-NEWTON; NGC-4945; SPECTROSCOPY; NGC-3079; DISK; GAS; REFLECTION AB We analyze recent simultaneous Chandra/RXTE observations of the Seyfert 2 galaxy NGC 4945. The unprecedented spatial resolution of Chandra means we are able to separate the spectra of the nucleus, starburst, and superwind regions, while the RXTE data extend the spectrum to higher energies. The extreme absorbing column of NHsimilar to4x10(24) cm(-2) means that the nucleus is only directly seen above 8-10 keV, while the lower energy spectrum from the nuclear region in Chandra is dominated by reflection. By contrast, the superwind is dominated by emission from hot plasma, but the starburst region contains both hot plasma and reflection signatures. Forming a reflected spectrum requires that the starburst region contain clumps of cool, optically thick material, perhaps star-forming cores, which are irradiated by 7-10 keV photons from the nucleus. Since photons of this energy are obscured along the line of sight, this confirms the result of Madejski et al. that the extreme absorption material is disklike rather than toroidal. However, the IR/optical limits on the lack of high-excitation emission lines show that, by contrast, the lower energy photons from the nucleus are obscured in all directions. We discuss the complex absorption structure revealed by these observations and propose an overall source geometry in which the nucleus is completely embedded in material with NHsimilar to10(23) cm(-2). C1 Univ Durham, Dept Phys, Durham DH1 3LE, England. Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Done, C (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. RI done, chris/D-4605-2016 OI done, chris/0000-0002-1065-7239 NR 39 TC 35 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2003 VL 588 IS 2 BP 763 EP 770 DI 10.1086/374332 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 680RV UT WOS:000182991900011 ER PT J AU Holt, SS Schlegel, EM Hwang, U Petre, R AF Holt, SS Schlegel, EM Hwang, U Petre, R TI Chandra observation of the X-ray source population of NGC 6946 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 6946); X-rays : binaries; X-rays : galaxies; X-rays : general ID SPIRAL GALAXY NGC-6946; ULTRALUMINOUS SUPERNOVA REMNANT; POINT SOURCES; LUMINOSITY; COMPLEX; STARBURST; M101; BAR; M31 AB We present the results of a study of discrete X-ray sources in NGC 6946 using a deep Chandra ACIS observation. Based on the slope of the log N-log S distribution and the general correlation of sources with the spiral arms, we infer that the overall discrete source sample in NGC 6946 is dominated by high-mass X-ray binaries, in contrast to the source distributions in M31 and the Milky Way. This is consistent with the higher star formation rate in NGC 6946 than in those galaxies. We find that the strong X-ray sources in the region of the galactic center do not correlate in detail with images of the region in the near-IR, although one of them may be coincident with the galactic center. The noncentral ultraluminous X-ray source in NGC 6946, previously identified with a supernova remnant, has an X-ray spectrum and luminosity that is inconsistent with either a traditional pulsar wind nebula or a blast wave remnant. C1 Franklin W Olin Coll Engn, Needham, MA 02492 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Harvard Coll Observ, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Holt, SS (reprint author), Franklin W Olin Coll Engn, 1735 Great Plain Ave, Needham, MA 02492 USA. NR 33 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 MAY 10 PY 2003 VL 588 IS 2 BP 792 EP 800 DI 10.1086/374311 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 680RV UT WOS:000182991900013 ER PT J AU Kraemer, KE Jackson, JM Kassis, M Deutsch, LK Hora, JL Simon, R Hoffmann, WF Fazio, GG Dayal, A Bania, TM Clemens, DP Heyer, MH AF Kraemer, KE Jackson, JM Kassis, M Deutsch, LK Hora, JL Simon, R Hoffmann, WF Fazio, GG Dayal, A Bania, TM Clemens, DP Heyer, MH TI Five star-forming cores in the Galactic Ring Survey: A mid-infrared study SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : ISM; stars : formation ID H-II REGIONS; YOUNG MASSIVE STARS; VLA OBSERVATIONS; ISOGAL SURVEY; ARRAY CAMERA; NGC 6334; DUST; ABSORPTION; EMISSION; CLUSTER AB We have imaged five dense molecular cores, selected from the Galactic Ring Survey (GRS), in the mid-infrared with the MIRAC3 instrument. We obtained high spatial resolution (similar to1") images through narrow-band filters at 12.5 and 20.6 mum. Four of the five cores show multiple compact sources, extended structure, or both. Lower resolution observations by the Infrared Space Observatory (ISO) and the Midcourse Space Experiment (MSX) suggest that the fifth core is also surrounded by extended emission on large scales (greater than or similar to2'). The extended mid-infrared structure is well-correlated with the radio continuum morphology in each of the five cores. This similarity suggests that the hot dust traced by the mid-infrared is located within the H II region, traced by the radio continuum, and not merely in a surrounding photodissociation region or molecular cloud. If a single exciting source is assumed for each core, estimates of the zero-age main-sequence spectral types based on the infrared luminosities are typically 1-2 spectral types earlier than those based on the radio free-free emission. However, allowing for multiple exciting sources and apportioning the far-infrared and radio fluxes to the component sources according to the mid-infrared flux distribution produces better agreement between the derived spectral types, with an average difference of less than half a spectral type. C1 USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. IPAC JPL, Pasadena, CA 91125 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP USAF, Res Lab, Space Vehicles Directorate, 29 Randolph Rd, Hanscom AFB, MA 01731 USA. EM kathleen.kraemer@hanscom.af.mil; jackson@bu.edu; mkassis@bu.edu; deutschl@bu.edu; jhora@cfa.harvard.edu; simonr@chub.bu.edu; whoffmann@as.arizona.edu; gfazio@cfa.harvard.edu; adayal@ipac.caltech.edu; bania@bu.edu; clemens@bu.edu; heyer@astro.umass.edu RI Bania, Thomas/H-2318-2014; OI Hora, Joseph/0000-0002-5599-4650; Kraemer, Kathleen/0000-0002-2626-7155 NR 48 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2003 VL 588 IS 2 BP 918 EP 930 DI 10.1086/374264 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 680RV UT WOS:000182991900024 ER PT J AU Damiani, F Flaccomio, E Micela, G Sciortino, S Harnden, FR Murray, SS Wolk, SJ Jeffries, RD AF Damiani, F Flaccomio, E Micela, G Sciortino, S Harnden, FR Murray, SS Wolk, SJ Jeffries, RD TI Chandra X-ray observations of the young open cluster NGC 2516 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 2516); stars : coronae; X-rays : stars ID COUNTING DETECTOR IMAGES; ROSAT HRI OBSERVATIONS; DEEP FIELD-SOUTH; WAVELET TRANSFORMS; OPTICAL SURVEY; NGC-2516; STARS; LUMINOSITY; EMISSION; PLEIADES AB We present a comprehensive study of the Chandra X-ray observations of the young open cluster NGC 2516. We have analyzed eight individual Chandra observations. We have combined the data to achieve the greatest sensitivity, reaching down to logf(X) = -14.56 (ergs s(-1) cm(-2)), or log L-X = 28.69 (ergs s(-1)) at the distance of NGC 2516. Out of 284 X-ray sources detected, 155 are identified with photometric cluster members, with very little ambiguity. We have studied the X-ray luminosity functions for the various spectral types, correcting for nonmember contamination those for later type stars. We find strong X-ray emission from a couple of B stars that cannot be due to companions. Among A stars, chemically peculiar stars show a detection fraction much larger than normal A stars. The luminosity functions decrease monotonically from F to M stars, and those for K stars are significantly lower than similar stars in the Pleiades, a cluster only slightly younger than NGC 2516. We discuss possible causes of this discrepancy, including differences in age and stellar rotation. C1 Osservatorio Astron Palermo GS Vaiana, INAF, I-90134 Palermo, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Keele, Dept Phys, Keele ST5 5BG, Staffs, England. RP Damiani, F (reprint author), Osservatorio Astron Palermo GS Vaiana, INAF, Piazza Parlamento 1, I-90134 Palermo, Italy. OI Flaccomio, Ettore/0000-0002-3638-5788; Wolk, Scott/0000-0002-0826-9261; Damiani, Francesco/0000-0002-7065-3061 NR 27 TC 21 Z9 21 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 MAY 10 PY 2003 VL 588 IS 2 BP 1009 EP 1024 DI 10.1086/374214 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 680RV UT WOS:000182991900032 ER PT J AU Kuchner, MJ Holman, MJ AF Kuchner, MJ Holman, MJ TI The geometry of resonant signatures in debris disks with planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; circumstellar matter; interplanetary medium; planetary systems; stars : individual (alpha Lyrae, epsilon Eridani, Fomalhaut) ID CIRCUMSTELLAR DUST DISK; MEAN-MOTION RESONANCES; POYNTING-ROBERTSON DRAG; BETA-PICTORIS; SOLAR-SYSTEM; ZODIACAL EMISSION; EVOLUTION; RING; PERTURBATIONS; ASYMMETRIES AB Using simple geometrical arguments, we paint an overview of the variety of resonant structures a single planet with moderate eccentricity (e less than or similar to 0.6) can create in a dynamically cold, optically thin dust disk. This overview may serve as a key for interpreting images of perturbed debris disks and inferring the dynamical properties of the planets responsible for the perturbations. We compare the resonant geometries found in the solar system dust cloud with observations of dust clouds around Vega, epsilon Eridani, and Fomalhaut. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kuchner, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Kuchner, Marc/E-2288-2012 NR 43 TC 105 Z9 106 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2003 VL 588 IS 2 BP 1110 EP 1120 DI 10.1086/374213 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 680RV UT WOS:000182991900039 ER PT J AU Kazmi, QB Manning, RB AF Kazmi, QB Manning, RB TI A new genus and species of pinnotherid crab from Karachi, northern Arabian Sea (Crustacea, Decapoda, Brachyura) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Decapoda; Pinnotheridae; commensal; Gastrochaena; Sindheres; Pakistan; new genus; new species AB A new monotypic genus, Sindheres, is established to accommodate a new species, S. karachiensis, of pinnotherid crab from the northern Arabian Sea. The new genus resembles Nepinnotheres Manning, 1993 in having the dactylus of the third maxilliped inserted near the mid-length of the ventral margin of the propodus but it differs in having a sub-hexagonal carapace. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA. Univ Karachi, Marine Reference Collect & Resource Ctr, Karachi 75270, Pakistan. RP Manning, RB (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 8 TC 3 Z9 4 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD MAY 10 PY 2003 VL 37 IS 9 BP 1085 EP 1089 DI 10.1080/00222930110108353 PG 5 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 676MV UT WOS:000182756600003 ER PT J AU Ashworth, AC Thompson, FC AF Ashworth, AC Thompson, FC TI A fly in the biogeographic ointment SO NATURE LA English DT Article ID TRANSANTARCTIC MOUNTAINS; SIRIUS GROUP; ANTARCTICA C1 N Dakota State Univ, Dept Geosci, Fargo, ND 58105 USA. Smithsonian Inst, USDA, Systemat Entomol Lab, Washington, DC 20560 USA. RP Ashworth, AC (reprint author), N Dakota State Univ, Dept Geosci, Fargo, ND 58105 USA. NR 11 TC 19 Z9 19 U1 0 U2 7 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 8 PY 2003 VL 423 IS 6936 BP 135 EP 136 DI 10.1038/423135a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 675MR UT WOS:000182699600033 PM 12736672 ER PT J AU Bice, KL Huber, BT Norris, RD AF Bice, KL Huber, BT Norris, RD TI Extreme polar warmth during the Cretaceous greenhouse? Paradox of the late Turonian delta O-18 record at Deep Sea Drilling Project Site 511 SO PALEOCEANOGRAPHY LA English DT Article DE carbon dioxide; Cretaceous; Turonian; oxygen isotopes; modeling; salinity ID STRONTIUM-ISOTOPE STRATIGRAPHY; SOUTHWEST ATLANTIC; OXYGEN-ISOTOPE; PLANKTONIC-FORAMINIFERA; FALKLAND PLATEAU; OCEAN; ANTARCTICA; LEG-71; PRECIPITATION; EVOLUTION AB [1] Oxygen isotope data for upper Turonian planktonic foraminifera at Deep Sea Drilling Project Site 511 (Falkland Plateau, 60degreesS paleolatitude) exhibit an similar to2parts per thousand excursion to values as low as -4.66parts per thousand (Vienna Peedee belemnite standard; PDB) coincident with the warmest tropical temperature estimates yet obtained for the open ocean. The lowest planktonic foraminifer delta(18)O values suggest that the upper ocean was as warm as 30-32degreesC. This is an extraordinary temperature for 60degreesS latitude but is consistent with temperatures estimated from apparently coeval mollusc delta(18)O from nearby James Ross Island (65 p S paleolatitude). Glassy textural preservation, a well-defined depth distribution in Site 511 planktonics, low sediment burial temperature (similar to32degreesC), and lack of evidence of highly depleted pore waters argue against diagenesis (even solid state diffusion) as the cause of the very depleted planktonic values. The lack of change in benthic foraminifer delta(18)O suggests brackish water capping as the mechanism for the low planktonic delta(18)O values. However, mixing ratio calculations show that the amount of freshwater required to produce a 2% shift in ambient water would drive a 7 psu decrease in salinity. The abundance and diversity of planktonic foraminifera and nannofossils, high planktonic: benthic ratios, and the appearance of keeled foraminifera argue against lower-than-normal marine salinities. Isotope calculations and climate models indicate that we cannot call upon more depleted freshwater delta(18)O to explain this record. Without more late Turonian data, especially from outside the South Atlantic basin, we can currently only speculate on possible causes of this paradoxical record from the core of the Cretaceous greenhouse. C1 Woods Hole Oceanog Inst, Dept Geol & Geophys, Woods Hole, MA 02543 USA. Smithsonian Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Bice, KL (reprint author), Woods Hole Oceanog Inst, Dept Geol & Geophys, Mail Stop 23, Woods Hole, MA 02543 USA. NR 45 TC 44 Z9 46 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0883-8305 J9 PALEOCEANOGRAPHY JI Paleoceanography PD MAY 7 PY 2003 VL 18 IS 2 AR 1031 DI 10.1029/2002PA000848 PG 13 WC Geosciences, Multidisciplinary; Oceanography; Paleontology SC Geology; Oceanography; Paleontology GA 678QN UT WOS:000182878100001 ER PT J AU Drake, JJ Marshall, HL AF Drake, JJ Marshall, HL TI Is RXJ1856.5-3754 a strange quark star? SO NUCLEAR PHYSICS A LA English DT Article; Proceedings Paper CT 7th International Symposium on Nuclei in the Cosmos (NIC7) CY JUL 08-12, 2002 CL FUJI, JAPAN SP Todai Int Symp, Univ Tokyo, Int Symp Minist Educ, Culture, Spoets, Sci & Technol, Commemorat Assoc Japan World Exposit 1970, Japan Soc Promot Sci, Inoue Fdn Sci, Kajima Fdn, Natl Astronom Observ Japan ID ISOLATED NEUTRON-STAR; X-RAY-SPECTRUM; RX J1856.5-3754; RADIO PULSARS; RX-J1856.5-3754; J185635-3754; EQUATION AB Deep Chandra LETGS observations Of the isolated neutron star candidate RXJ1856.5-3754 have demonstrated that, to within the accuracy of the observations, the X-ray spectrum is consistent with a blackbody with a temperature of 7 x 10(5) K and a radiation radius R-infinity similar to 5 km-much too small for current neutron star equations of state. The small apparent radius, lack of X-ray pulsations down to a level of 3%, and failure to explain the observations in terms of current neutron star models, lead to the suggestion that R-XJ1856.5-3754 might be a strange quark star. We discuss some issues associated with this interpretation and look briefly at RX J1856.5-3754 in the context of other strange star candidates and recent Chandra observations of neutron stars that appear to have smooth featureless spectra. Both X-ray and optical spectra of some of these objects might be explained by "naked" crusted neutron stars or strange quark stars with thin coronae. RX J1856.5-3754 remains an interesting strange quark star candidate. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA. NR 39 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0375-9474 J9 NUCL PHYS A JI Nucl. Phys. A PD MAY 5 PY 2003 VL 718 BP 351C EP 358C DI 10.1016/S0375-9474(03)00738-3 PG 8 WC Physics, Nuclear SC Physics GA 668VR UT WOS:000182314300053 ER PT J AU Post, JE Heaney, PJ Von Dreele, RB Hanson, JC AF Post, JE Heaney, PJ Von Dreele, RB Hanson, JC TI Neutron and temperature-resolved synchrotron X-ray powder diffraction study of akaganeite SO AMERICAN MINERALOGIST LA English DT Article ID BETA-FEOOH; RIETVELD REFINEMENT; THERMAL-DECOMPOSITION AB Rietveld refinements using neutron powder diffraction data were used to locate H atom positions and obtain a more precise crystal structure refinement for akaganeite [Fe7.63+Ni0.42+O6.35 (OH)(9.65)Cl(1.25)(.)nH(2)O]. Difference Fourier maps clearly showed H atoms positions near those O atoms at the midpoints of the tunnel edges. The O-H vectors point toward the Cl sites at the center of the tunnel, and weak hydrogen bonds likely form between the framework 0 atoms and Cl. The Cl position is near the center of a prism defined by the eight hydroxyl H atoms. The Cl atoms fill similar to2/3 of the tunnel sites, suggesting an ordering scheme in a given tunnel with every third tunnel site vacant. Such an arrangement allows the Cl anions to increase their separation distance along a tunnel by displacing away from one another toward their respective adjacent vacancies. The Fe-O octahedra in akaganeite are distorted with Fe-(O, OH) distances ranging from 1.94 to 2.13 Angstrom and show three longer and three shorter Fe-O distances; as expected the longer distances are associated with the OH- anions. Temperature-resolved synchrotron X-ray powder diffraction data and Rietveld refinements were used to investigate changes in the akagandite structure and its transformation into hematite as it was heated from 26 to 800 degreesC. Rietveld refinements revealed surprising consistency in all unit-cell parameters between room temperature and similar to225 degreesC, resulting in nearly zero thermal expansion of the akaganeite structure over a 200 degreesC interval. Above similar to225 degreesC, the unit-cell volume gradually decreased, primarily in response to decreases in c and b, and an increase in the P angle. The a parameter remained nearly constant until similar to225 degreesC and increased thereafter. Akaganeite started to transform to hematite in the temperature range 290 to 310 degreesC with no evidence for maghemite as an intermediate phase. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Los Alamos Natl Lab, LANSCE 12, Los Alamos, NM 87545 USA. Brookhaven Natl Lab, Dept Chem, Upton, NY 11793 USA. RP Post, JE (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RI Hanson, jonathan/E-3517-2010 NR 26 TC 66 Z9 66 U1 3 U2 13 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 2003 VL 88 IS 5-6 BP 782 EP 788 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 677XY UT WOS:000182835600007 ER PT J AU Reed, DH O'Grady, JJ Ballou, JD Frankham, R AF Reed, DH O'Grady, JJ Ballou, JD Frankham, R TI The frequency and severity of catastrophic die-offs in vertebrates SO ANIMAL CONSERVATION LA English DT Article ID DYNAMICS; STOCHASTICITY; CONSERVATION; VARIABILITY; HURRICANE; ECOLOGY; MAMMALS; TERM AB Rare bouts of extreme environmental perturbations (catastrophes) have been predicted to have a major influence on the probability of extinction. Yet very little information is available on the frequency and severity of catastrophes. Improving the available information concerning catastrophe parameters would allow for an evaluation of their effect and a start towards understanding their causes. We used the Global Population Dynamics Database to determine the frequency and severity of die-offs in 88 species of vertebrates. We define a catastrophe as any 1-year decrease in population size of 50% or greater. The data yielded three findings. (1) The frequency of severe die-offs in vertebrate populations is strongly related to the generation length of the organism. (2) The probability of a severe die-off for a particular population is approximately 14% per generation. (3) The frequency of die-off severity can be modelled as a modified power function with the frequency of die-offs decreasing with increasing magnitude of effect. The distribution is not consistent with catastrophes stemming from environmental sources different than those responsible for smaller fluctuations, but seems to represent the tail of a continuous distribution of environmental perturbations. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Conservat Biol, Washington, DC 20008 USA. RP Reed, DH (reprint author), Univ Mississippi, Dept Biol, POB 1848, University, MS 38677 USA. NR 23 TC 63 Z9 64 U1 4 U2 28 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 2003 VL 6 BP 109 EP 114 DI 10.1017/S1367943003147 PN 2 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 688XB UT WOS:000183461600003 ER PT J AU Karanth, KU Nichols, JD Seidensticker, J Dinerstein, E Smith, JLD McDougal, C Johnsingh, AJT Chundawat, RS Thapar, V AF Karanth, KU Nichols, JD Seidensticker, J Dinerstein, E Smith, JLD McDougal, C Johnsingh, AJT Chundawat, RS Thapar, V TI Science deficiency in conservation practice: the monitoring of tiger populations in India SO ANIMAL CONSERVATION LA English DT Article ID LEOPARD; DHOLE AB Conservation practices are supposed to get refined by advancing scientific knowledge. We study this phenomenon in the context of monitoring tiger populations in India, by evaluating the 'pugmark census method' employed by wildlife managers for three decades. We use an analytical framework of modern animal population sampling to test the efficacy of the pugmark censuses using scientific data on tigers and our field observations. We identify three critical goals for monitoring tiger populations, in order of increasing sophistication: (1) distribution mapping, (2) tracking relative abundance, (3) estimation of absolute abundance. We demonstrate that the present census-based paradigm does not work because it ignores the first two simpler goals, and targets, but fails to achieve, the most difficult third goal. We point out the utility and ready availability of alternative monitoring paradigms that deal with the central problems of spatial sampling and observability. We propose an alternative sampling-based approach that can be tailored to meet practical needs of tiger monitoring at different levels of refinement. C1 Wildlife Conservat Soc, Int Program, Bronx, NY 10460 USA. US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. World Wildlife Fund, Washington, DC 20037 USA. Univ Minnesota, Dept Fisheries & Wildlife, St Paul, MN 55108 USA. Tiger Tops, Kathmandu, Nepal. Wildlife Inst India, Dehra Dun 248001, Uttar Pradesh, India. RP Karanth, KU (reprint author), 26-2,Aga Abbas Ali Rd,Apt 403, Bangalore 560042, Karnataka, India. NR 40 TC 66 Z9 72 U1 3 U2 26 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 2003 VL 6 BP 141 EP 146 DI 10.1017/S1367943003003184 PN 2 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 688XB UT WOS:000183461600007 ER PT J AU Uson, JM Matthews, LD AF Uson, JM Matthews, LD TI HI imaging observations of superthin galaxies. I. UGC 7321 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (UGC 7321); galaxies : ISM; galaxies : kinematics and dynamics; galaxies : spiral; ISM : HI ID SURFACE BRIGHTNESS GALAXIES; DARK-MATTER HALOS; EDGE-ON GALAXIES; NEUTRAL HYDROGEN OBSERVATIONS; TIDAL DWARF GALAXY; SPIRAL GALAXIES; ROTATION CURVES; GALACTIC DISKS; STAR-FORMATION; INTERSTELLAR-MEDIUM AB We have used the Very Large Array to image the isolated "superthin'' galaxy UGC 7321 in the H I line with a spatial resolution of 16" and a spectral resolution of 24 kHz (5.2 km s(-1)). We have reached a sensitivity of (0.36-0.40) mJy beam(-1) channel(-1), which correspond to a column density of (8-9) x 10(18) atoms cm(-2) (1 sigma). UGC 7321 has a gas-rich disk, with M-HI = (1.06 +/- 0.01) x 10(9) d(10)(2) M-. and M-H I/ L-B = 1.0 (d(10) is the distance to UGC 7321 in units of 10 Mpc, the value adopted in this paper), and no detectable radio continuum emission (F-CONT = 0.41 +/- 0.25 mJy). The global H I distribution of UGC 7321 is rather symmetric and extends to similar to1.5 times the optical radius (D-H I = 8.'65 +/- 0.'15 at n(HI) = 3 x 10(19) atoms cm(-2)). An "integral sign'' warp is observed in the H I disk, commencing near the edge of the stellar distribution and twisting back toward the equatorial plane in the outermost regions. In addition, the position-velocity diagram suggests the presence of a bar or inner arm within similar to40" from the center. The rotation curve of UGC 7321 is slowly rising; it reaches its asymptotic velocity of similar to110 km s(-1) at similar to2.'5 from the center ( about 0.9 optical radii) and declines near the edge of the H I disk. The ratio of the inferred dynamical mass to the mass in gas and stars is similar to12d(10)(-1) implying that UGC 7321 is a highly dark-matter-dominated galaxy. C1 Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Uson, JM (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. NR 78 TC 38 Z9 40 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 2003 VL 125 IS 5 BP 2455 EP 2472 DI 10.1086/374627 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 669VU UT WOS:000182371800013 ER PT J AU Cohen, M Megeath, ST Hammersley, PL Martin-Luis, F Stauffer, J AF Cohen, M Megeath, ST Hammersley, PL Martin-Luis, F Stauffer, J TI Spectral irradiance calibration in the infrared. XIII. "Supertemplates'' and on-orbit calibrators for the SIRTF Infrared Array Camera SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared radiation; methods : analytical; stars : late-type; techniques : spectroscopic ID MIDCOURSE SPACE EXPERIMENT; PHOTOMETRIC STANDARD STARS; MU-M SPECTRA; INTERSTELLAR EXTINCTION; ULTRAVIOLET EXTINCTION; MODEL ATMOSPHERES; CELESTIAL EQUATOR; STELLAR SPECTRA; TEMPERATURE; PASSBANDS AB We describe the technique that will be used to develop a set of on-orbit calibrators for the Infrared Array Camera (IRAC) and demonstrate the validity of the method for stars with spectral types either K0-M0 III or A0-A5 V. For application to SIRTF, the approach is intended to operate with all available optical, near-infrared (NIR), and mid-infrared (MIR) photometry and to yield complete absolute spectra from UV to MIR. One set of stars is picked from Landolt's extensive network of optical (UBVRI) calibrators, the other from the Carter-Meadows set of faint IR standards. Traceability to the "Cohen-Walker-Witteborn'' framework of absolute photometry and stellar spectra is assured. The method is based on the use of either "supertemplates,'' which represent the intrinsic shapes of the spectra of K0-M0 III stars from far-UV (1150 Angstrom) to MIR (35 mum) wavelengths, or Kurucz synthetic spectra for A0-A5 V stars. Each supertemplate or Kurucz model is reddened according to the individual star's extinction and is normalized using available characterized optical photometry. This paper tests our capability to predict NIR (JHK) magnitudes using supertemplates or models constrained by Hipparcos/Tycho or precision ground-based optical data. We provide absolutely calibrated 0.275-35.00 mum spectra of 33 Landolt and Carter-Meadows optical standard stars to demonstrate the viability of this technique, and to offer a set of IR calibrators 100-1000 times fainter than those we have previously published. As an indication of what we can expect for actual IRAC calibration stars, we have calculated the absolute uncertainties associated with predicting the IRAC magnitudes for the faintest cool giant and hot dwarf in this new set of calibration stars. C1 Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, E-38200 Tenerife, Spain. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. RP Cohen, M (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA. NR 54 TC 152 Z9 152 U1 0 U2 4 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 2003 VL 125 IS 5 BP 2645 EP 2663 DI 10.1086/374362 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 669VU UT WOS:000182371800028 ER PT J AU Franklin, FA Soper, PR AF Franklin, FA Soper, PR TI Some effects of mean motion resonance passage on the relative migration of Jupiter and Saturn SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids; planets and satellites : general; planets and satellites : individual (Jupiter, Saturn); solar system : formation; solar system : general ID PLANETS; SYSTEM AB We look for clues to the amount and direction of Saturn's migration relative to Jupiter in their current orbits, specifically, from the fact that the former lies barely sunward of their 5 : 2 mean motion resonance. Numerical simulations suggest that Saturn has moved in the same direction (presumably inward) as has Jupiter but that the pair has never passed through their more distant 3 : 1 resonance. Thus, their relative migration has been less than about 1.5 AU. Passage through 5 : 2 is consistent with their current orbits and could have contributed to their present eccentricities, e (and especially to their large periodic variations), but it probably cannot generate their e's if both, and particularly Jupiter's, were initially less than about 0.03. In fact, it is most likely that their initial e's were both close to the current values. Very long term capture into 5 : 2 for the Sun-Jupiter-Saturn case occurs with a remarkably high frequency. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts Lowell, Lowell, MA 01854 USA. RP Franklin, FA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 5 Z9 5 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2003 VL 125 IS 5 BP 2678 EP 2691 DI 10.1086/374228 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 669VU UT WOS:000182371800030 ER PT J AU Testi, L Natta, A Shepherd, DS Wilner, DJ AF Testi, L Natta, A Shepherd, DS Wilner, DJ TI Large grains in the disk of CQ Tau SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : planetary systems : protoplanetary disks; stars : planetary systems : formation; stars : formation; stars : individual : CQ Tauri ID SPECTRAL ENERGY-DISTRIBUTIONS; INTERMEDIATE-MASS STARS; HERBIG AE SYSTEMS; T-TAURI; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISKS; ACCRETION DISKS; HIGH-RESOLUTION; DUST; MODEL AB We present 7 mm observations of the dusty disk surrounding the 10 Myr old 1.5 M(.) pre-main-sequence star CQ Tauri obtained at the Very Large Array with 0.8 arcsec resolution and 0.1 mJy rms sensitivity. These observations resolve the 7 mm emission in approximately the north-south direction, confirming previous results obtained with lower resolution. We use a two-layer flared disk model to interpret the observed fluxes from 7 mm to 1.3 mm together with the resolved 7 mm structure. We find that the disk radius is constrained to the range 100 to 300 AU, depending on the steepness of the disk surface density distribution. The power law index of the dust opacity coefficient, beta, is constrained to be 0.5 to 0.7. Since the models indicate that the disk is optically thin at millimeter wavelengths for radii greater than 8 AU, the contribution of an optically thick region to the emission is less than 10%. This implies that high optical depth or complex disk geometry cannot be the cause of the observed shallow millimeter spectral index. Instead, the new analysis supports the earlier suggestion that dust particles in the disk have grown to sizes as large as a few centimeters. The dust in the CQ Tauri system appears to be evolved much like that in the TW Hydra system, a well-studied pre-main-sequence star of similar age and lower mass. The survival of gas-rich disks with incomplete grain evolution at such old ages deserves further investigations. C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Testi, L (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM lt@arcetri.astro.it NR 31 TC 122 Z9 123 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2003 VL 403 IS 1 BP 323 EP 328 DI 10.1051/0004-6361:20030362 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 673CC UT WOS:000182561100034 ER PT J AU Moy, E Barmby, P Rigopoulou, D Huang, JS Willner, SP Fazio, GG AF Moy, E Barmby, P Rigopoulou, D Huang, JS Willner, SP Fazio, GG TI H-band observations of the Chandra Deep Field South SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE catalogs; surveys; infrared : general; galaxies : general; stars : general; cosmology : observations ID CAMPANAS INFRARED SURVEY; HIGH-REDSHIFT GALAXIES; ESO IMAGING SURVEY; PHOTOMETRIC REDSHIFTS; NUMBER COUNTS; SELECTION; EVOLUTION; CATALOG AB We report results of our H-band survey of the Chandra Deep Field South (CDFS). The observations, made with SofI on the NTT, cover 0.027 square degrees to H < 20.5 and 0.17 square degrees to H < 19.8 ( 50% completeness limits). In total, 4819 objects were detected, of which 80% are galaxies based on the SExtractor parameter "stellarity index" having a value less than 0.5. Our astrometric solutions are in good agreement with those of the Las Campanas Infrared Survey (LCIRS), the COMBO-17, and the ESO-EIS surveys. Our photometry compares satisfactorily with the LCIRS results as well as with GOODS data. Galaxy number counts are similar to50 000 galaxies per square degree at H < 20.75, in good agreement with those of LCIRS. The object catalog is published electronically at the CDS**. C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moy, E (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany. EM moy@discovery.saclay.cea.fr RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 30 TC 22 Z9 22 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 2003 VL 403 IS 2 BP 493 EP 499 DI 10.1051/0004-6361:20030245 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 675DY UT WOS:000182678800015 ER PT J AU Durret, F Neto, GBL Forman, W Churazov, E AF Durret, F Neto, GBL Forman, W Churazov, E TI An XMM-Newton view of the extended "filament" near the cluster of galaxies Abell 85 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : clusters : individual : Abell 85; X-rays : galaxies : clusters ID RAY; EVOLUTION AB We have observed with XMM-Newton the extended 4 Mpc filament detected by the ROSAT PSPC in the neighbourhood of the cluster of galaxies Abell 85. We confirm that there is an extended feature, aligned at the same position angle as the major axis of the central cD, the bright cluster galaxies, and nearby groups and clusters. We find that the X-ray emission from the filament is best described by thermal emission with a temperature of similar to2 keV, which is significantly lower than the ambient cluster medium, but is significantly higher than anticipated for a gas in a weakly bound extended filament. It is not clear whether this is a filament of diffuse emission, a chain of several groups of galaxies, or stripped gas from the infalling south blob. C1 CNRS, Inst Astrophys Paris, F-75014 Paris, France. Univ Sao Paulo, Inst Astron Geofis & C Atmosf, BR-05508090 Sao Paulo, Brazil. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP CNRS, Inst Astrophys Paris, 98 Bis Bd Arago, F-75014 Paris, France. EM durret@iap.fr RI Churazov, Eugene/A-7783-2013; Lima Neto, Gastao/J-6117-2014; OI Forman, William/0000-0002-9478-1682 NR 20 TC 32 Z9 32 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2003 VL 403 IS 2 BP L29 EP L32 DI 10.1051/0004-6361:20030424 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 675DY UT WOS:000182678800002 ER PT J AU Ovaldsen, JE Teuber, J Schild, RE Stabell, R AF Ovaldsen, JE Teuber, J Schild, RE Stabell, R TI New aperture photometry of QSO 0957+561; application to time delay and microlensing SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing; quasars : individual : QSO 0957+561; techniques : photometric; methods : data analysis ID QUASAR Q0957+561; LIGHT CURVES; OPTICAL-DATA; QSO-0957+561; VARIABILITY; LIGHTCURVES; PARAMETERS; FEATURES; IMAGES; LENS AB We present a re-reduction of archival CCD frames of the doubly imaged quasar 0957 + 561 using a new photometry code. Aperture photometry with corrections for both cross contamination between the quasar images and galaxy contamination is performed on about 2650 R-band images from a five year period (1992-1997). From the brightness data a time delay of 424.9 +/- 1.2 days is derived using two different statistical techniques. The amount of gravitational microlensing in the quasar light curves is briefly investigated, and we find unambiguous evidence of both long term and short term microlensing. We also note the unusual circumstance regarding time delay estimates for this gravitational lens. Estimates by different observers from different data sets or even with the same data sets give lag estimates differing by typically 8 days, and error bars of only a day or two. This probably indicates several complexities where the result of each estimate depends upon the details of the calculation. C1 Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Ctr Adv Signal Proc, Copenhagen, Denmark. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ovaldsen, JE (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway. NR 35 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 MAY PY 2003 VL 402 IS 3 BP 891 EP 904 DI 10.1051/0004-6361:20030145 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EH UT WOS:000182452000019 ER PT J AU Furlanetto, SR Loeb, A AF Furlanetto, SR Loeb, A TI Metal absorption lines as probes of the intergalactic medium prior to the reionization epoch SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : high-redshift; intergalactic medium; quasars : absorption lines ID LY-ALPHA FOREST; GAMMA-RAY BURSTS; GALACTIC WINDS; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; DWARF GALAXIES; STAR-FORMATION; DRIVEN SUPERWINDS; ENRICHMENT; UNIVERSE AB Winds from star-forming galaxies provide the most promising explanation for the enrichment of the inter-galactic medium with heavy elements. Theoretical and observational arguments indicate that the pollution may have occurred at z greater than or similar to 6; however, direct observational tests of such a scenario are needed. We model star-burst winds in the high-redshift universe and find that the fraction of space filled by enriched material varies strongly with the assumed star formation efficiency f(*) and the fraction of supernova energy powering each wind f(esc). We show that metals carried by these winds can be seen in absorption against bright background sources, such as quasars or gamma-ray bursts, in narrow lines with characteristic equivalent widths similar to0.5 Angstrom less than or similar to W less than or similar to 5 Angstrom. We argue that a substantial fraction of the metals in high-redshift winds are likely to reside in low-ionization states (C II, O I, Si II, and Fe II), but higher ionization states (C IV and Si IV) could also provide useful probes of the winds. The number of such lines can constrain both f(*) and f(esc). Statistics of metal absorption lines can also be used to identify whether H-2 is an efficient coolant in the early universe and to study the initial mass function of stars at high redshifts. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Adv Study, Princeton, NJ 08540 USA. RP Furlanetto, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 91 TC 89 Z9 89 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2003 VL 588 IS 1 BP 18 EP 34 DI 10.1086/374045 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EF UT WOS:000182451800003 ER PT J AU Shapley, AE Steidel, CC Pettini, M Adelberger, KL AF Shapley, AE Steidel, CC Pettini, M Adelberger, KL TI Rest-frame ultraviolet spectra of z similar to 3 Lyman break galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article ID STAR-FORMING GALAXIES; HUBBLE DEEP FIELD; RESOLUTION IMAGING SPECTROMETER; SPACE-TELESCOPE SPECTROSCOPY; LY-ALPHA; REDSHIFT Z-SIMILAR-TO-3; STARBURST GALAXIES; CONTINUUM EMISSION; LUMINOSITY DENSITY; STELLAR YIELDS AB We present the results of a systematic study of the rest-frame UV spectroscopic properties of Lyman break galaxies (LBGs). The database of almost 1000 LBG spectra proves useful for constructing high signal-to-noise composite spectra. The composite spectrum of the entire sample reveals a wealth of features attributable to hot stars, H II regions, dust, and out. owing neutral and ionized gas. By grouping the database according to galaxy parameters such as Lyalpha equivalent width, UV spectral slope, and interstellar kinematics, we isolate some of the major trends in LBG spectra that are least compromised by selection effects. We find that LBGs with stronger Lyalpha emission have bluer UV continua, weaker low-ionization interstellar absorption lines, smaller kinematic offsets between Lyalpha and the interstellar absorption lines, and lower star formation rates. There is a decoupling between the dependence of low- and high-ionization outflow features on other spectral properties. Additionally, galaxies with rest-frame W-Lyalpha greater than or equal to 20 Angstrom in emission have weaker than average high-ionization lines and nebular emission lines that are significantly stronger than in the sample as a whole. Most of the above trends can be explained in terms of the properties of the large-scale outflows seen in LBGs. According to this scenario, the appearance of LBG spectra is determined by a combination of the covering fraction of out. owing neutral gas, which contains dust and the range of velocities over which this gas is absorbing. In contrast, the strengths of collisionally excited nebular emission lines should not be affected by the nature of the outflow, and variations in these lines may indicate differences in the temperatures and metallicities in H II regions of galaxies with very strong Lyalpha emission. Higher sensitivity and spectral resolution observations are still required for a full understanding of the covering fraction and velocity dispersion of the out. owing neutral gas in LBGs and its relationship to the escape fraction of Lyman continuum radiation in galaxies at z similar to 3. C1 CALTECH, Pasadena, CA 91125 USA. Inst Astron, Cambridge CB3 0HE, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. RP Shapley, AE (reprint author), CALTECH, MS 105-24, Pasadena, CA 91125 USA. NR 81 TC 843 Z9 843 U1 2 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 1 PY 2003 VL 588 IS 1 BP 65 EP 89 DI 10.1086/373922 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EF UT WOS:000182451800006 ER PT J AU Bechtold, J Siemiginowska, A Shields, J Czerny, B Janiuk, A Hamann, F Aldcroft, TL Elvis, M Dobrzycki, A AF Bechtold, J Siemiginowska, A Shields, J Czerny, B Janiuk, A Hamann, F Aldcroft, TL Elvis, M Dobrzycki, A TI Chandra survey of radio-quiet, high-redshift quasars SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; intergalactic medium; quasars : general; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-PROPERTIES; DOMINATED ACCRETION FLOWS; BAND ENERGY-DISTRIBUTION; OPTICALLY SELECTED QSOS; ROSAT DETECTED QUASARS; PALOMAR SKY SURVEY; BLACK-HOLES; Z-GREATER-THAN-4 QUASARS; ABSORPTION SYSTEMS AB We observed 17 optically selected, radio-quiet, high-redshift quasars with the Chandra ACIS and detected 16 of them. The quasars have redshifts between 3.70 and 6.28 and include the highest-redshift quasars known. When compared with low-redshift quasars observed with ROSAT, these high-redshift quasars are significantly more X-ray-quiet. We also find that the X-ray spectral index of the high-redshift objects is flatter than the average at lower redshift. These trends confirm the predictions of models in which the accretion flow is described by a cold, optically thick accretion disk surrounded by a hot, optically thin corona, provided the viscosity parameter alpha greater than or equal to 0.02. The high-redshift quasars have supermassive black holes, with masses of similar to10(10) M-circle dot, and are accreting material at similar to0.1 times the Eddington limit. We detect 10 X-ray photons from the z = 6.28 quasar SDSS 1030+0524, which might have a Gunn-Peterson trough and be near the redshift of reionization of the intergalactic medium. The X-ray data place an upper limit on the optical depth of the intergalactic medium, tau(IGM) < 10(6), compared to the lower limit from the spectrum of Lyα and Lyβ, which implies τ(IGM) > 20. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Nicholaus Copernicus Astron Ctr, Warsaw, Poland. Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. RP Bechtold, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Czerny, Bozena/A-2363-2015 OI Czerny, Bozena/0000-0001-5848-4333 NR 101 TC 69 Z9 70 U1 0 U2 1 PU UNIV 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 2003 VL 588 IS 1 BP 119 EP 127 DI 10.1086/378724 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EF UT WOS:000182451800010 ER PT J AU Fabbiano, G Elvis, M Markoff, S Siemiginowska, A Pellegrini, S Zezas, A Nicastro, F Trinchieri, G McDowell, J AF Fabbiano, G Elvis, M Markoff, S Siemiginowska, A Pellegrini, S Zezas, A Nicastro, F Trinchieri, G McDowell, J TI The X-ray-faint emission of the supermassive nuclear black hole of IC 1459 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : individual (IC 1459); galaxies : nuclei ID EARLY-TYPE GALAXIES; ACTIVE GALACTIC NUCLEI; ADVECTION-DOMINATED ACCRETION; IONIZED-GAS; RADIO GALAXIES; COUNTERROTATING CORE; SEYFERT-GALAXIES; SPECTRAL MODELS; FLOWS; DISK AB Chandra observations of the supermassive black hole in the nucleus of IC 1459 show a weak (L-X = 8 x 10(40) ergs s(-1), 0.3-8 keV), unabsorbed nuclear X-ray source, with a slope Gamma = 1.88 +/- 0.09, and no strong Fe K line at 6.4 keV (EW < 382 eV). This describes a normal active galactic nucleus (AGN) X-ray spectrum but lies at 3 x 10(-7) below the Eddington limit. The spectral energy distribution of the IC 1459 nucleus is extremely radio-loud compared to normal radio-loud quasars. The nucleus is surrounded by a hot interstellar medium (kT &SIM; 0.5-0.6 keV) with an average density of 0.3 cm(-3), within the central &SIM;180 pc radius, which is comparable to the gravitational capture radius, r(A) &SIM; 140 pc. We estimate that for a standard AGN efficiency of 10%, the Bondi accretion would correspond to a luminosity of &SIM;6 x 10(44) ergs s(-1), nearly 4 orders of magnitude higher than L-X. ADAF solutions can explain the X-ray spectrum, but not the high radio/X-ray ratio. A jet model fits the radio-100 μm and X-ray spectra well. The total power in this jet is &SIM;10% of L-Bondi, implying that accretion close to the Bondi rate is needed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Bologna, Dipartimento Astron, I-40126 Bologna, Italy. Osserv Astron Brera, I-20121 Milan, Italy. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Nicastro, Fabrizio/0000-0002-6896-1364 NR 87 TC 49 Z9 49 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2003 VL 588 IS 1 BP 175 EP 185 DI 10.1086/374040 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EF UT WOS:000182451800015 ER PT J AU Gaensler, BM Schulz, NS Kaspi, VM Pivovaroff, MJ Becker, WE AF Gaensler, BM Schulz, NS Kaspi, VM Pivovaroff, MJ Becker, WE TI XMM-Newton observations of PSR B1823-13: An asymmetric synchrotron nebula around a Vela-like pulsar SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G18.0-0.7); pulsars : individual (PSR B1823-13) stars : neutron; supernova remnants; X-rays : ISM ID X-RAY OBSERVATIONS; WIND-DRIVEN BUBBLES; SUPERNOVA REMNANT; NEUTRON-STARS; YOUNG PULSARS; BOW-SHOCK; EMISSION; SHELL; EVOLUTION; CRAB AB We present a deep observation with the X-Ray Multimirror Mission of PSR B1823-13, a young pulsar with similar properties to the Vela pulsar. We detect two components to the X-ray emission associated with PSR B1823-13: an elongated core of extent 3000 immediately surrounding the pulsar embedded in a fainter, diffuse component of emission 50 in extent, seen only on the southern side of the pulsar. The pulsar itself is not detected, either as a point source or through its pulsations. Both components of the X-ray emission are well fitted by a power-law spectrum, with photon index Gamma approximate to 1.6 and X-ray luminosity (0.5-10 keV) L-X approximate to 9 x 10(32) ergs s(-1) for the core and Gamma approximate to 2.3 and L-X approximate to 3 x 10(33) ergs s(-1) for the diffuse emission, for a distance of 4 kpc. We interpret both components of emission as corresponding to a pulsar wind nebula, which we designate G18.0-0.7. We argue that the core region represents the wind termination shock of this nebula, while the diffuse component indicates the shocked downstream wind. We propose that the asymmetric morphology of the diffuse emission with respect to the pulsar is the result of a reverse shock from an associated supernova remnant, which has compressed and distorted the pulsar-powered nebula. Such an interaction might be typical for pulsars at this stage in their evolution. The associated supernova remnant is not detected directly, most likely being too faint to be seen in existing X-ray and radio observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. 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 54 TC 71 Z9 72 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 MAY 1 PY 2003 VL 588 IS 1 BP 441 EP 451 DI 10.1086/368356 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EF UT WOS:000182451800037 ER PT J AU Heinke, CO Grindlay, JE Lloyd, DA Edmonds, PD AF Heinke, CO Grindlay, JE Lloyd, DA Edmonds, PD TI X-ray studies of two neutron stars in 47 tucanae: Toward constraints on the equation of state SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; binaries : eclipsing; globular clusters : individual (NGC 104); stars : neutron; X-rays : binaries ID GLOBULAR-CLUSTER 47-TUCANAE; THERMAL EMISSION; CENTAURUS X-4; BLACK-HOLE; AQUILA X-1; ROSAT OBSERVATIONS; MODEL ATMOSPHERES; XMM-NEWTON; QUIESCENCE; MASS AB We report spectral and variability analysis of two quiescent low-mass X-ray binaries (X5 and X7, previously detected with the ROSAT HRI) in a Chandra ACIS-I observation of the globular cluster 47 Tuc. X5 demonstrates sharp eclipses with an 8.666 +/- 0.01 hr period, as well as dips showing an increased N-H column. The thermal spectra of X5 and X7 are well modeled by unmagnetized hydrogen atmospheres of hot neutron stars. No hard power-law component is required. A possible edge or absorption feature is identified near 0.64 keV, perhaps an O V edge from a hot wind. Spectral fits imply that X7 is significantly more massive than the canonical 1.4 M-circle dot neutron star mass, with M > 1: 8 M-circle dot for a radius range of 9-14 km, while X5's spectrum is consistent with a neutron star of mass 1.4 M-circle dot for the same radius range. Alternatively, if much of the X-ray luminosity is due to continuing accretion onto the neutron star surface, the feature may be the 0.87 keV rest-frame absorption complex (O VIII and other metal lines) intrinsic to the neutron star atmosphere, and a mass of 1.4 M-circle dot for X7 may be allowed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cheinke@cfa.harvard.edu OI Heinke, Craig/0000-0003-3944-6109 NR 71 TC 51 Z9 51 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2003 VL 588 IS 1 BP 452 EP 463 DI 10.1086/374039 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EF UT WOS:000182451800038 ER PT J AU Dobrzycka, D Raymond, JC Biesecker, DA Li, J Ciaravella, A AF Dobrzycka, D Raymond, JC Biesecker, DA Li, J Ciaravella, A TI Ultraviolet spectroscopy of narrow coronal mass ejections SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : coronal mass ejections (CMEs); Sun : UV radiation ID ANGLE SPECTROMETRIC CORONAGRAPH; X-RAY TELESCOPE; WHITE-LIGHT; SOLAR MINIMUM; JETS; MODEL; SOHO; TRANSIENTS; DENSITY; HOLES AB We present Ultraviolet Coronagraph Spectrometer (UVCS) observations of five narrow coronal mass ejections (CMEs) that were among 15 narrow CMEs originally selected by Gilbert and coworkers. Two events (1999 March 27, April 15) were "structured," i.e., in white-light data they exhibited well-defined interior features, and three (1999 May 9, May 21, June 3) were "unstructured," i.e., appeared featureless. In UVCS data the events were seen as 4degrees-13degrees wide enhancements of the strongest coronal lines H I Lyalpha and O VI lambdalambda1032, 1037. We derived electron densities for several of the events from the Large Angle and Spectrometric Coronagraph Experiment (LASCO) C2 white-light observations. They are comparable to or smaller than densities inferred for other CMEs. We modeled the observable properties of examples of the structured (1999 April 15) and unstructured (1999 May 9) narrow CMEs at different heights in the corona between 1.5 and 2 R-circle dot. The derived electron temperatures, densities, and outflow speeds are similar for those two types of ejections. They were compared with properties of polar coronal jets and other CMEs. We discuss different scenarios of narrow CME formation as either a jet formed by reconnection onto open field lines or a CME ejected by expansion of closed field structures. Overall, we conclude that the existing observations do not definitively place the narrow CMEs into the jet or the CME picture, but the acceleration of the 1999 April 15 event resembles acceleration seen in many CMEs, rather than constant speeds or deceleration observed in jets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Ocean & Atmospher Adm, Space Environm Ctr, Boulder, CO 80305 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Osservatorio Astron Palermo Giuseppe S Vaina, I-90134 Palermo, Italy. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ddobrzycka@cfa.harvard.edu; jraymond@cfa.harvard.edu; doug.biesecker@noaa.gov; jing@ifa.hawaii.edu; ciarave@astropa.unipa.it NR 40 TC 20 Z9 20 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2003 VL 588 IS 1 BP 586 EP 595 DI 10.1086/374047 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EF UT WOS:000182451800049 ER PT J AU Gottlieb, CA Myers, PC Thaddeus, P AF Gottlieb, CA Myers, PC Thaddeus, P TI Precise millimeter-wave laboratory frequencies for CS and (CS)-S-34 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; methods : laboratory; molecular data; molecular processes; radio lines : ISM; stars : formation ID SUB-DOPPLER MEASUREMENTS; ROTATIONAL TRANSITIONS; HYPERFINE-STRUCTURE; CARBON-MONOXIDE; INFALL MOTIONS; STARLESS CORES; N2H+; SPECTRUM; CLOUDS AB Nine successive rotational lines in the ground vibrational state of CS and (CS)-S-34 between 96 GHz ( J = 2-1) and 500 GHz (10-9) were measured in the laboratory to an accuracy of a few kHz. When our measurements are combined with the submillimeter-wave measurements of Ahrens & Winnewisser, the entire rotational spectrum of both isotopic species is predicted to an accuracy of about 1 part in 10(8) up to 500 GHz and 5 parts in 10(8) near 1000 GHz. These frequencies should be useful for quantitative studies of cloud core collapse and star formation in the millimeter- and submillimeter-wave bands. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP Gottlieb, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 36 Z9 36 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 MAY 1 PY 2003 VL 588 IS 1 BP 655 EP 661 DI 10.1086/368378 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 671EF UT WOS:000182451800055 ER PT J AU Jennions, MD Moller, AP AF Jennions, MD Moller, AP TI A survey of the statistical power of research in behavioral ecology and animal behavior SO BEHAVIORAL ECOLOGY LA English DT Article DE effect size; meta-analysis; publication bias; sample sizes; statistical power ID RANDOMIZED CONTROLLED TRIALS; FILE DRAWER PROBLEM; PUBLICATION BIAS; FLUCTUATING ASYMMETRY; BIOLOGICAL-RESEARCH; METAANALYSIS; EVOLUTION; SIZE AB We estimated the statistical power of the first and last statistical test presented in 697 papers from 10 behavioral journals. First tests had significantly greater statistical power and reported more significant results (smaller p values) than did last tests. This trend was consistent across journals, taxa, and the type of statistical test used. On average, statistical power was 13-16% to detect a small effect and 40-47% to detect a medium effect. This is far lower than the general recommendation of a power of 80%. By this criterion, only 2-3%, 13-21%, and 37-50% of the tests examined had the requisite power to detect a small, medium, or large effect, respectively. Neither p values nor statistical power varied significantly across the 10 journals or 11 taxa. However, mean p values of first and last tests were significantly correlated across journals (r =.67, n = 10, p =.034), with a similar trend for mean power (r =.63, n = 10, p =.051). There is therefore some evidence that power and p values are repeatable among journals. Mean p values or power of first and last tests were, however, uncorrelated across taxa. Finally, there was a significant correlation between power and reported p value for both first (r =.13, n = 684, p =.001) and last tests (r =.16, n = 654, p <.0001). If true effect sizes are unrelated to study sample sizes, the average true effect size must be nonzero for this pattern to emerge. This suggests that failure to observe significant relationships is partly owing to small sample sizes, as power increases with sample size. Key words: effect size, meta-analysis, publication bias, sample sizes, statistical power. C1 Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. Smithsonian Trop Res Inst, Balboa, Panama. Univ Paris 06, CNRS, Lab Ecol Evolut Parasitaire, FRE 2365, F-75252 Paris 5, France. RP Jennions, MD (reprint author), Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. RI Rohlf, F/A-8710-2008; Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 40 TC 87 Z9 92 U1 0 U2 26 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 2003 VL 14 IS 3 BP 438 EP 445 DI 10.1093/beheco/14.3.438 PG 8 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 680CC UT WOS:000182957900020 ER PT J AU Baldwin, CC Smith, DG AF Baldwin, CC Smith, DG TI Larval gobiidae (teleostei : perciformes) of Carrie Bow Cay, Belize, central America SO BULLETIN OF MARINE SCIENCE LA English DT Article ID EARLY-LIFE-HISTORY; WESTERN ATLANTIC; STAGE LARVAE; GOBIOIDEI; MICRODESMIDAE; SYSTEMATICS; GOBIES; FISHES; PISCES; GOBY AB Little descriptive and specific taxonomic information is available regarding the early life history stages of Caribbean coral-reef fishes. Ongoing studies at the Smithsonian Institution's research station at Carrie Bow Cay, Belize, involving the rearing of net-collected larval fishes is allowing specific identifications of numerous larval types. Field protocol includes preserving larval types in ethanol plus butylated hydroxytoluene to enhance the retention of orange and yellow pigments. Studies of fish larvae at Carrie Bow during the summer months of several years between 1993-1997 have yielded generic or specific identifications of 21 goby larvae belonging to ten genera. Separating closely related larval types in the field was facilitated by microscopic observations of combined patterns of melanophores and chromatophores. Identification of morphological types was aided by comparing countable features of larvae and reared juveniles with those of adult Caribbean gobies from USNM collections. Continued implementation of the methods outlined herein should prove valuable in identifying much more of the ichthyoplankton fauna of the Caribbean. Species-level identifications of larvae of coral reef fishes will render these life history stages useful in a variety of studies including those of phylogenetic relationships, ecology, as well as reproductive and fisheries biology. Including information from larval morphology in systematic studies of the Gobioidei may help clarify poorly understood relationships within the Suborder. Supraspecific patterns of chromatophores warrant further investigation as a novel suite of phylogenetically informative ontogenetic features. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. RP Baldwin, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. NR 29 TC 11 Z9 14 U1 0 U2 3 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 MAY PY 2003 VL 72 IS 3 BP 639 EP 674 PG 36 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 750YR UT WOS:000187026500004 ER PT J AU Saavedra-Diaz, LM Munroe, TA Acero, A AF Saavedra-Diaz, LM Munroe, TA Acero, A TI Symphurus hernandezi (Pleuronectiformes : Cynoglossidae), a new deep-water tonguefish from the southern Caribbean sea off Colombia SO BULLETIN OF MARINE SCIENCE LA English DT Article ID REDESCRIPTION; BRACHYURA; DECAPODA; COAST AB A new cynoglossid species, Symphurus hernandezi, is described from 83 specimens (50.9-126.9 min SL) taken on the outer continental shelf (82 specimens collected between 148 and 301 in) off Caribbean Colombia. This species is distinguished from all congeners by its unique purplish pigmentation and pepperdot pattern of melanophores on the blind side of the body. Symphurus hernandezi has a 1-3-2 pattern of interdigitation of dorsal-fin pterygiophores and neural spines, 12 caudal-fin rays and a black peritoneum. Among congeners, S. hernandezi is most similar to the sympatrically occurring S. marginatus, but is easily distinguished from that species by differences in ocular- and blind-side pigmentation patterns, fewer longitudinal and head scales (77-86 and 13-16 in S. hernandezi vs 86-99 and 16-20 in S. marginatus, respectively), and by several morphometric features including shorter dorsal- and anal-fin rays, deeper body depth in the caudal region, longer head and postorbital lengths, and a smaller pupil diameter. Symphurus hernandezi has a restricted distribution on the outer continental shelf off Caribbean Colombia. C1 INVEMAR, Inst Invest Marinas & Costeras, AA-1016 Santa Marta, Colombia. Natl Museum Nat Hist, Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA. Univ Nacl Colombia, Inst Ciencias Nat, Santa Marta, Colombia. RP Saavedra-Diaz, LM (reprint author), INVEMAR, Inst Invest Marinas & Costeras, AA-1016 Santa Marta, Colombia. NR 29 TC 2 Z9 4 U1 0 U2 2 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 MAY PY 2003 VL 72 IS 3 BP 955 EP 970 PG 16 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 750YR UT WOS:000187026500021 ER PT J AU Haug, JD AF Haug, JD TI The fate of knowledge. SO COLLEGE & RESEARCH LIBRARIES LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Haug, JD (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASSOC COLL RESEARCH LIBRARIES PI CHICAGO PA 50 E HURON ST, CHICAGO, IL 60611 USA SN 0010-0870 J9 COLL RES LIBR JI Coll. Res. Libr. PD MAY PY 2003 VL 64 IS 3 BP 243 EP 246 PG 4 WC Information Science & Library Science SC Information Science & Library Science GA 681AX UT WOS:000183015200007 ER PT J AU Gonzalez, MA Eberhard, JR Lovette, IJ Olson, SL Bermingham, E AF Gonzalez, MA Eberhard, JR Lovette, IJ Olson, SL Bermingham, E TI Mitochondrial DNA phylogeography of the Bay Wren (Troglodytidae : Thryothorus nigricapillus) complex SO CONDOR LA English DT Article DE Bay Wren; Panama isthmus; phylogeny; phylogeography; plumage; speciation; Thryothorus nigricapillus ID REPRODUCTIVE STRATEGIES; GENETIC-DIVERGENCE; CENTRAL-AMERICA; SONG BEHAVIOR; DUETTING WREN; HYBRID ZONE; EVOLUTIONARY; DIFFERENTIATION; BIOGEOGRAPHY; POPULATIONS AB The Bay Wren (Thryothorus nigricapillus) is distributed from Costa Rica to Ecuador and includes seven described subspecies, five of which occur in the Caribbean lowlands of Panama. The subspecies vary in plumage characters, with particularly striking differences between Bay Wrens from western Panama (to the north), and eastern Panama (to the south). We surveyed mitochondrial DNA (mtDNA) sequence variation from a geographically broad sample of Bay Wrens and compared the phylogeographic structure of mtDNA diversity with previously described patterns of morphological variation. The mtDNA-based phylogeographic reconstructions revealed a basal split separating populations in far eastern Panama and South America from those in central Panama through Costa Rica. These two clades are concordant with previous morphology-based groupings of T. nigricapillus subspecies into the "castaneus group" (costaricensis, odicus, castaneus, and reditus) and the "nigricapillus group" (schottii, connectens, and nigricapillus). Morphological intergradation between the two groups takes place in central Panama, but all intergrades possess the mtDNA haplotype of the castaneus group, suggesting that mitochondrial gene flow is introgressing from west to east. In spite of the marked body size and plumage variation present among subspecies of the castaneus group, mtDNA variation within this group was low. At a deeper phylogenetic level, the mtDNA data support recognition of the Riverside Wren, T. semibadius, as a full species. This taxon has sometimes been considered conspecific with T nigricapillus, but the high mtDNA divergence between these species is consistent with previous suggestions that the morphological similarity results from convergence in plumage traits. C1 Smithsonian Trop Res Inst, Naos Labs, Balboa, Panama. Louisiana State Univ, Dept Sci Biol, Baton Rouge, LA 70803 USA. Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. Cornell Lab Ornithol, Ithaca, NY 14850 USA. Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. RP Bermingham, E (reprint author), Smithsonian Trop Res Inst, Naos Labs, Apartado 2072, Balboa, Panama. RI Lovette, Irby/P-3477-2014 NR 39 TC 16 Z9 17 U1 0 U2 5 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 2003 VL 105 IS 2 BP 228 EP 238 DI 10.1650/0010-5422(2003)105[0228:MDPOTB]2.0.CO;2 PG 11 WC Ornithology SC Zoology GA 674YF UT WOS:000182664700005 ER PT J AU Darke, AK Megonigal, JP AF Darke, AK Megonigal, JP TI Control of sediment deposition rates in two mid-Atlantic Coast tidal freshwater wetlands SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE sediment deposition; tidal freshwater wetland; sea level rise; flood depth; plant density; turbidity maximum; Mattapom River; VA; mid-Atlantic Coast ID SUSPENDED PARTICULATE MATTER; CHESAPEAKE BAY; CLIMATE-CHANGE; SALT MARSHES; TURBIDITY MAXIMUM; POTENTIAL IMPACTS; UNITED-STATES; ESTUARY; RIVER; TRANSPORT AB Eustatic sea level rise and rapidly increasing coastal development threaten tidal freshwater wetlands. Sediment deposition is one process that affects their ability to maintain surface elevations relative to adjacent rivers. Sediment dynamics in salt marshes have been studied extensively, but little is known about the factors that control sediment deposition rates in tidal freshwater wetlands. We examined geomorphic, hydrological, and biotic factors that may influence sedimentation in two tidal freshwater wetlands that fell at opposite ends of the riverine-estuarine continuum. Our data demonstrate that sediment dynamics are highly variable among tidal freshwater wetlands, and are influenced by the location of the wetland on the continuum. Sediment deposition was up to 10 times higher during the growing season at the downstream site than the upstream site. Plant density and height were highly correlated with sediment deposition rates at the downstream site (r greater than or equal to 0.92, p less than or equal to 0.009) but not at the upstream site. Elevation, flood depth, and flood duration were correlated with deposition rates only when each site/season combination was considered separately. River suspended sediment and surficial floodwater suspended sediment concentrations were significantly higher at the downstream site (p = 0.02 and p = 0.04, respectively). These data suggest that vegetation is important in determining sediment deposition rates when river suspended sediment is not limiting. which is not always the case. Longer flood duration increased sediment deposition, but was of secondary importance. Land use and proximity to the turbidity maximum (near the forward extent of the salt water intrusion) appear to be critically important in determining river suspended sediment availability in the tidal freshwater zone of the Mattaponi River, VA. (C) 2003 Elsevier Science B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. George Mason Univ, Environm Sci & Publ Program, Fairfax, VA 22030 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 59 TC 30 Z9 30 U1 3 U2 21 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 MAY PY 2003 VL 57 IS 1-2 BP 255 EP 268 DI 10.1016/S0272-7714(02)00353-0 PG 14 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 707FR UT WOS:000184500300022 ER PT J AU Naisbit, RE Jiggins, CD Mallet, J AF Naisbit, RE Jiggins, CD Mallet, J TI Mimicry: developmental genes that contribute to speciation SO EVOLUTION & DEVELOPMENT LA English DT Article ID WARNING-COLOR; HELICONIUS BUTTERFLIES; REPRODUCTIVE ISOLATION; NATURAL-SELECTION; EVOLUTIONARY GENETICS; POSTZYGOTIC ISOLATION; ADAPTIVE RADIATION; MULLERIAN MIMICRY; PATTERN-FORMATION; HYBRID ZONES AB Despite renewed interest in the role of natural selection as a catalyst for the origin of species, the developmental and genetic basis of speciation remains poorly understood. Here we describe the genetics of Mullerian mimicry in Heliconius cydno and H. melpomene (Lepidoptera: Nymphalidae), sister species that recently diverged to mimic other Heliconius. This mimetic shift was a key step in their speciation, leading to pre- and postmating isolation. We identify 10 autosomal loci, half of which have major effects. At least eight appear to be homologous with genes known to control pattern differences within each species. Dominance has evolved under the influence of identifiable "modifier" loci rather than being a fixed characteristic of each locus. Epistasis is found at many levels: phenotypic interaction between specific pairs of genes, developmental canalization due to polygenic modifiers so that patterns are less sharply defined in hybrids, and overall fitness through ecological selection against nonmimetic hybrid genotypes. Most of the loci are clustered into two genomic regions or "supergenes," suggesting color pattern evolution is constrained by preexisting linked elements that may have arisen via tandem duplication rather than having been assembled by natural selection. Linkage, modifiers, and epistasis affect the strength of mimicry as a barrier to gene flow between these naturally hybridizing species and may permit introgression in genomic regions unlinked to those under disruptive selection. Mullerian mimics in Heliconius use different genetic architectures to achieve the same mimetic patterns, implying few developmental constraints. Therefore, although developmental and genomic constraints undoubtedly influence the evolutionary process, their effects are probably not strong in comparison with natural selection. C1 UCL, Galton Lab, Dept Biol, London NW1 2HE, England. Smithsonian Trop Res Inst, Balboa, Panama. RP Naisbit, RE (reprint author), Univ Neuchatel, Inst Zool, Lab Ecol Anim & Entomol, CH-2007 Neuchatel, Switzerland. EM russell.naisbit@unine.ch RI Jiggins, Chris/B-9960-2008; Naisbit, Russell/B-9658-2011; mallet, james/B-5114-2008; OI Jiggins, Chris/0000-0002-7809-062X; Naisbit, Russell/0000-0003-0190-9323; Mallet, James/0000-0002-3370-0367 NR 82 TC 78 Z9 81 U1 1 U2 25 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1520-541X J9 EVOL DEV JI Evol. Dev. PD MAY-JUN PY 2003 VL 5 IS 3 BP 269 EP 280 DI 10.1046/j.1525-142X.2003.03034.x PG 12 WC Evolutionary Biology; Developmental Biology; Genetics & Heredity SC Evolutionary Biology; Developmental Biology; Genetics & Heredity GA 672TT UT WOS:000182539500006 PM 12752766 ER PT J AU Vila, R Mundina, M Tomi, F Ciccio, JF Gupta, MP Iglesias, J Casanova, J Canigueral, S AF Vila, R Mundina, M Tomi, F Ciccio, JF Gupta, MP Iglesias, J Casanova, J Canigueral, S TI Constituents of the essential oils from Piper friedrichsthalii C.DC. and P-pseudolindenii C.DC. from Central America SO FLAVOUR AND FRAGRANCE JOURNAL LA English DT Article DE Piper friedrichsthalii; Piper pseudolindenii; Piperaceae; essential oil; GC-MS; C-13-NMR; alpha-apinene; alpha-selinene; 11-selinen-4 alpha-ol; beta-elemene; beta-caryophyllene ID C-13 NMR; COMPLEX AB Essential oils obtained by hydrodistillation from the leaves and flower spikes of Piper friedrichsthalii from Costa Rica and Panama, and leaves of P. pseudolindenii from Costa Rica were analysed by GC-FID, GC-MS and C-13-NMR. Monoterpenoids constituted the main fraction of the oils of P. friedrichsthalii from Costa Rica, particularly a-pinene, camphene, beta-phellandrene, limonene and menthane derivatives, whereas the oils from leaves of P. friedrichsthalii from Panama and of P. pseudolindenii from Costa Rica were characterized by a high sesquiterpene content, especially 11-selinen-4alpha-ol, alpha-selinene, germacrene D and beta-selinene in the former, and beta-elemene, beta-caryophyllene, germacrene D and alpha-humulene in the latter. Copyright (C) 2003 John Wiley Sons, Ltd. C1 Univ Barcelona, Fac Farm, Unitat Farmacol & Farmacognisa, E-08028 Barcelona, Spain. Univ Corse, CNRS, UMR 6134, F-75700 Paris, France. Univ Costa Rica, Escuela Quim, CIPRONA, San Jose 2060, Costa Rica. Univ Panama, Estafeta Univ, Fac Farm, CIFLORPAN, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. RP Canigueral, S (reprint author), Univ Barcelona, Fac Farm, Unitat Farmacol & Farmacognisa, Avda Diagonal 643, E-08028 Barcelona, Spain. RI Canigueral, Salvador/O-2767-2013 OI Canigueral, Salvador/0000-0001-5056-489X NR 9 TC 7 Z9 8 U1 0 U2 2 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX PO19 1UD, ENGLAND SN 0882-5734 J9 FLAVOUR FRAG J JI Flavour Frag. J. PD MAY-JUN PY 2003 VL 18 IS 3 BP 198 EP 201 DI 10.1002/ffj.1181 PG 4 WC Chemistry, Applied; Food Science & Technology SC Chemistry; Food Science & Technology GA 675UD UT WOS:000182713600004 ER PT J AU Zito, M Evans, S Weldon, PJ AF Zito, M Evans, S Weldon, PJ TI Owl monkeys (Aotus spp.) self-anoint with plants and millipedes SO FOLIA PRIMATOLOGICA LA English DT Article DE owl monkeys; Aotus; self-anointing; millipedes C1 Primate Conservancy, Land OLakes, FL 34639 USA. DuMond Conservancy, Miami, FL USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA USA. RP Zito, M (reprint author), Primate Conservancy, POB 1551, Land OLakes, FL 34639 USA. NR 12 TC 22 Z9 26 U1 1 U2 8 PU KARGER PI BASEL PA ALLSCHWILERSTRASSE 10, CH-4009 BASEL, SWITZERLAND SN 0015-5713 J9 FOLIA PRIMATOL JI Folia Primatol. PD MAY-JUN PY 2003 VL 74 IS 3 BP 159 EP 161 DI 10.1159/000070649 PG 3 WC Zoology SC Zoology GA 698DV UT WOS:000183983100005 PM 12826735 ER PT J AU Petaev, MI Wood, JA Meibom, A Krot, AN Keil, K AF Petaev, MI Wood, JA Meibom, A Krot, AN Keil, K TI The ZONMET thermodynamic and kinetic model of metal condensation SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID CH CARBONACEOUS CHONDRITES; SOLAR NEBULA; OXIDIZING CONDITIONS; NUCLEATION PROCESS; MIXING PROPERTIES; HIGH-TEMPERATURE; GRAIN FORMATION; SYSTEM; ELEMENTS; ORIGIN AB The ZONMET model of metal condensation is a FORTRAN computer code that calculates condensation with partial isolation-type equilibrium partitioning of the 19 most abundant elements among 203 gaseous and 488 condensed phases and growth in the nebula of a zoned metal grain by condensation from the nebular gas accompanied by diffusional redistribution of Ni, Co, and Cr. Of five input parameters of the ZONMET model (chemical composition of the system expressed as the dust/gas [D/G] ratio, nebular pressure [P-tot], isolation degree [xi], cooling rate (CR), and seed size), only two-the D/G ratio and the CR of the nebular source region of a zoned Fe,Ni grain-are important in determining the grain radius and Ni, Co, and Cr zoning profiles. We found no evidence for the supercooling during condensation of Fe,Ni metal that is predicted by the homogeneous nucleation theory. The model allows estimates to be made of physicochemical parameters in the CH chondrite nebular source regions. Modeling growth and simultaneous diffusional redistribution of Ni, Co, and Cr in the zoned metal grains of CH chondrites reveals that the condensation zoning profiles were substantially modified by diffusion while the grains were growing in the nebula. This means that previous estimates of the physicochemical conditions in the nebular source regions of CH and CB chondrites, based on measured zoning profiles of Ni, Co, Cr, and platinum group elements in Fe,Ni metal grains, need to be corrected. The two zoned metal grains in the PAT 91456 and NWA 470 CH chondrites studied so far require nebular source regions with different chemical compositions (D/G = 1 and D/G = 4, respectively) and thermal histories characterized by variable cooling rates (CR = 0.011 + 0.0022 X DeltaT K/h and CR = 0.05 + 0.0035 X DeltaT K/h, respectively). It appears that the metal grains of the CH chondrites were formed in multiple nebular source regions or in different events within the same source region as the CB chondrite metal grains were formed. Copyright (C) 2003 Elsevier Science Ltd. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02128 USA. Stanford Univ, Stanford, CA 94305 USA. Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP Petaev, MI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 67 TC 21 Z9 21 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 2003 VL 67 IS 9 BP 1737 EP 1751 AR PII S0016-7037(02)00956-0 DI 10.1016/S0016-7037(02)00956-0 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 673PT UT WOS:000182589900012 ER PT J AU Golombek, MP Grant, JA Parker, TJ Crisp, JA Squyres, SW AF Golombek, MP Grant, JA Parker, TJ Crisp, JA Squyres, SW TI Landing the Mars Exploration Rovers SO GEOTIMES LA English DT Article C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Natl Air Space Museum Washington, Ctr Earth & Planetary Studies, Smithsonian Inst, Washington, DC USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Golombek, MP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RI Crisp, Joy/H-8287-2016 OI Crisp, Joy/0000-0002-3202-4416 NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 USA SN 0016-8556 J9 GEOTIMES JI Geotimes PD MAY PY 2003 VL 48 IS 5 BP 18 EP 23 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 779WY UT WOS:000189326000015 ER PT J AU Baliunas, S Donahue, R Rampino, MR Gaffey, MJ Shelton, JC Mohanty, S AF Baliunas, S Donahue, R Rampino, MR Gaffey, MJ Shelton, JC Mohanty, S TI Multispectral analysis of Asteroid 3 Juno taken with the 100-inch telescope at Mount Wilson Observatory SO ICARUS LA English DT Article AB High-resolution multispectral images of main-belt asteroid 3 Juno were taken at visible and near-IR wavelengths with the 100-inch telescope at Mount Wilson Observatory equipped with an adaptive optics system. The images show spectral features that may represent a large relatively recent impact that deeply excavated the coarse-grained olivine-pyroxene-rich crust of the asteroid. (C) 2003 Elsevier Science (USA). All rights reserved. C1 NYU, Earth & Environm Sci Program, New York, NY 10003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. Mt Wilson Inst, Pasadena, CA 91106 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Rampino, MR (reprint author), NYU, Earth & Environm Sci Program, 100 Washington Sq E Room 1009, New York, NY 10003 USA. NR 18 TC 8 Z9 8 U1 3 U2 4 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 MAY PY 2003 VL 163 IS 1 BP 135 EP 141 DI 10.1016/S0019-1035(03)00049-6 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 681VN UT WOS:000183056400009 ER PT J AU Ortner, DJ AF Ortner, DJ TI Human remains: Conservation, retrieval and analysis SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Bradford, Bradford BD7 1DP, W Yorkshire, England. RP Ortner, DJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD MAY-JUN PY 2003 VL 13 IS 3 BP 173 EP 174 DI 10.1002/oa.632 PG 2 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 691RE UT WOS:000183618600009 ER PT J AU Reich, PB Wright, IJ Cavender-Bares, J Craine, JM Oleksyn, J Westoby, M Walters, MB AF Reich, PB Wright, IJ Cavender-Bares, J Craine, JM Oleksyn, J Westoby, M Walters, MB TI The evolution of plant functional variation: Traits, spectra, and strategies SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Review DE plant traits; adaptation; fitness; functional groups; selection ID CARBON-ISOTOPE DISCRIMINATION; LEAF LIFE-SPAN; PINUS-SYLVESTRIS POPULATIONS; RELATIVE GROWTH-RATE; SHADE TOLERANCE; RAIN-FOREST; SCOTS PINE; LOW-LIGHT; PHOTOSYNTHETIC CAPACITY; COMMON-GARDEN AB Variation in plant functional traits results from evolutionary and environmental drivers that operate at a variety of different scales, which makes it a challenge to differentiate among them. In this article we describe patterns of functional trait variation and trait correlations within and among habitats in relation to several environmental and trade-off axes. We then ask whether such patterns reflect natural selection and can be considered plant strategies. In so doing we highlight evidence that demonstrates that (1) patterns of trait variation across resource and environmental gradients (light, water, nutrients, and temperature) probably reflect adaptation, (2) plant trait variation typically involves multiple-correlated traits that arise because of inevitable trade-offs among traits and across levels of whole-plant integration and that must be understood from a whole-plant perspective, and (3) such adaptation may be globally generalizable for like conditions; i. e., the set of traits (collections of traits in syndromes) of taxa can be considered as "plant strategies." C1 Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Landcare Res, Dunedin, New Zealand. Polish Acad Sci, Inst Dendrol, PL-62035 Kornik, Poland. Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. RP Reich, PB (reprint author), Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. RI Craine, Joseph/D-4569-2009; Wright, Ian/G-4979-2012; Oleksyn, Jacek/I-4539-2012; Cavender-Bares, Jeannine/K-5716-2013 OI Craine, Joseph/0000-0001-6561-3244; Wright, Ian/0000-0001-8338-9143; NR 166 TC 430 Z9 458 U1 41 U2 337 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD MAY PY 2003 VL 164 IS 3 SU S BP S143 EP S164 DI 10.1086/374368 PG 22 WC Plant Sciences SC Plant Sciences GA 698UW UT WOS:000184018500011 ER PT J AU Fogel, ML Tuross, N AF Fogel, ML Tuross, N TI Extending the limits of paleodietary studies of humans with compound specific carbon isotope analysis of amino acids SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE paleodiet; humans; stable carbon isotopes; plants ID DIETARY-PROTEIN INTAKE; STABLE CARBON; PLASMA-CONCENTRATIONS; DIURNAL-VARIATIONS; NITROGEN; COLLAGEN; ECOLOGY; RATIOS; C-13 AB Stable carbon isotopes in the bone collagen of prehistoric humans are valuable tools for determining human diet. We studied carbon isotopes in individual amino acids (IAA) in plants and collagen from herbivores and humans from North American prehistoric sites in order to determine whether more specific dietary information about Indians could be predicted. The VC of plant amino acids ranged extensively, whereas delta(13)C values of each amino acid from the C-3 (n = 3) and C-4 (n = 3) plant species were linearly related with a slope of 0.8. Essential amino acids from herbivores had delta(13)C values that were completely different from those measured in either C-3 or C-4 plants, suggesting metabolic resynthesis in the gut by microflora. The delta(13)C of essential amino acids from prehistoric North Americans, who had diets ranging from primarily maize-based (C-4) to hunter-gathers (C-3) subsistence, were highly correlated with delta(13)C values of herbivore essential amino acids. There was no significant correlation of delta(13)C in IAA from humans with those of plants. The delta(13)C of nonessential amino acids in human bone collagen can distinguish the presence of maize in the diet, whereas the delta(13)C of essential amino acids were transparent to a maize-derived carbon signal. Compound specific isotopic data on IAA distinguish between total carbon intake versus total protein intake and are useful for discerning the extent and nature of omnivory. (C) 2003 Elsevier Science Ltd. All rights reserved. C1 Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. Natl Museum Nat Hist, Smithsonian Inst, Ctr Mat Res & Educ, Suitland, MD 20746 USA. Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA. RP Fogel, ML (reprint author), Carnegie Inst Washington, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. RI Fogel, Marilyn/M-2395-2015 OI Fogel, Marilyn/0000-0002-1176-3818 NR 30 TC 64 Z9 65 U1 2 U2 22 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 MAY PY 2003 VL 30 IS 5 BP 535 EP 545 DI 10.1016/S0305-4403(02)00199-1 PG 11 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 663HZ UT WOS:000182001300003 ER PT J AU Andersson, M Wallander, J Oring, L Akst, E Reed, JM Fleischer, RC AF Andersson, M Wallander, J Oring, L Akst, E Reed, JM Fleischer, RC TI Adaptive seasonal trend in brood sex ratio: test in two sister species with contrasting breeding systems SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE brood sex ratio trend; molecular sexing; monogamy; Monte Carlo test; polyandry; sex role reversal ID REPRODUCTIVE SUCCESS; SPOTTED SANDPIPERS; ACTITIS-MACULARIA; KESTREL BROODS; LEK PARADOX; BIRDS; ALLOCATION; HYPOTHESIS; ADJUSTMENT; EVOLUTION AB Evolutionary theory predicts adaptive adjustment in offspring sex ratio by females. Seasonal change in sex ratio is one possibility, tested here in two sister species, the Common sandpiper and the Spotted sandpiper Actitis hypoleucos and A. macularia. In the monogamous Common sandpiper, males are the most competitive sex. In each of 3 years, there was a change from mainly sons in early clutches to mainly daughters in late clutches. This seasonal adjustment of clutch sex ratio took place within the female before the eggs were laid, not by differential egg or chick survival. The sex of all eggs laid in the clutches used here was determined molecularly from chick blood taken at the time of hatching. The Spotted sandpiper in contrast is polyandrous, with partly reversed sex roles. There was no seasonal trend from sons to daughters in this species. When tested together, the two species differed significantly as predicted by the hypothesis of adaptive sex ratio adjustment by females. C1 Univ Gothenburg, Dept Zool, SE-40530 Gothenburg, Sweden. Univ Nevada, Dept Environm & Resource Sci, Reno, NV 89557 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Genet Program, Washington, DC 20560 USA. RP Andersson, M (reprint author), Univ Gothenburg, Dept Zool, Box 463, SE-40530 Gothenburg, Sweden. NR 46 TC 40 Z9 40 U1 1 U2 8 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD MAY PY 2003 VL 16 IS 3 BP 510 EP 515 DI 10.1046/j.1420-9101.2003.00533.x PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 668XV UT WOS:000182322200015 PM 14635851 ER PT J AU Scherneck, HG Johansson, JM Koivula, H van Dam, T Davis, JL AF Scherneck, HG Johansson, JM Koivula, H van Dam, T Davis, JL TI Vertical crustal motion observed in the BIFROST project SO JOURNAL OF GEODYNAMICS LA English DT Article; Proceedings Paper CT 10th International Symposium on Recent Crustal Movement CY AUG 27-31, 2001 CL HELSINKI, FINLAND ID PERMANENT GPS NETWORK; SIGNAL SCATTERING; ENERGY BALANCES; SITE POSITIONS; SURFACE LOADS; LAND WATER; FENNOSCANDIA; DISPLACEMENTS; DEFORMATION; RATES AB This paper reports from investigations on the robustness of estimated rates of intraplate motion from the continuous GPS project BIFROST (Baseline Inferences from Fennoscandian Rebound Observations, Sealevel and Tectonics). We study loading effects due to ocean, atmosphere and hydrology and their impact on estimated rate parameters. We regularly find the admittance of a modelled perturbation at less than fifty percent of the full effect. We think that the finding relates to a difficult noise situation at all periods, and that a satisfying model for the dominating noise source has not been found yet. An additional reason for low admittance is found in the mapping process of the no-fiducial network solution into a conventional reference frame. (C) 2003 Elsevier Science Ltd. All rights reserved. C1 Chalmers Univ Technol, Onsala Space Observ, SE-43992 Onsala, Sweden. Finnish Geodet Inst, FI-02431 Masala, Finland. European Ctr Geodynam & Seismol, L-7256 Walferdange, Luxembourg. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Scherneck, HG (reprint author), Chalmers Univ Technol, Onsala Space Observ, SE-43992 Onsala, Sweden. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 21 TC 32 Z9 33 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0264-3707 J9 J GEODYN JI J. Geodyn. PD MAY-JUL PY 2003 VL 35 IS 4-5 BP 425 EP 441 DI 10.1016/S0264-3707(03)00005-X PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 678ZQ UT WOS:000182896900004 ER PT J AU Franz, NM Wcislo, WT AF Franz, NM Wcislo, WT TI Foraging behavior in two species of Ectatomma (Formicidae : Ponerinae): Individual learning of orientation and timing SO JOURNAL OF INSECT BEHAVIOR LA English DT Article DE cognitive ecology; Ectatomma; foraging behavior; individual learning; Ponerinae ID RUIDUM ROGER HYMENOPTERA; GIANT TROPICAL ANT; NESTMATE RECOGNITION; PARAPONERA-CLAVATA; COGNITIVE ECOLOGY; TUBERCULATUM; ENVIRONMENTS; POLYETHISM; EFFICIENCY; PREDATION AB The foraging behavior of marked individuals of Ectatomma ruidum and E. tuberculatum (Formicidae: Ponerinae) was observed on Barro Colorado Island, Panama, in order to determine whether learning of orientation and timing is involved when foraging on patchy resources on the forest floor. Foraging experiments under seminatural conditions were designed to control for the spatiotemporal distribution of resources at one or two preying sites. Using both single- and multi-event past experience, individual foragers of E. ruidum and (although less significantly) E. tuberculatum made directional and temporal adjustments to their behavior in response to previous differential foraging success. In spite of considerable individual variation in foraging efficiency, it is hypothesized that the observed differences in cognitive abilities can be invoked to explain ecological differences among both species. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Ancon, Panama. NR 45 TC 9 Z9 10 U1 1 U2 15 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0892-7553 J9 J INSECT BEHAV JI J. Insect Behav. PD MAY PY 2003 VL 16 IS 3 BP 381 EP 410 DI 10.1023/A:1024880110189 PG 30 WC Entomology SC Entomology GA 702ZA UT WOS:000184253900006 ER PT J AU McShea, WJ Pagels, J Orrock, J Harper, E Koy, K AF McShea, WJ Pagels, J Orrock, J Harper, E Koy, K TI Mesic deciduous forest as patches of small-mammal richness within an Appalachian Mountain Forest SO JOURNAL OF MAMMALOGY LA English DT Article DE biodiversity; Clethrionomys; forest ecology; landscape ecology; metapopulation theory; Napaeozapus; Peromyscus; Sorex ID MICE PEROMYSCUS-LEUCOPUS; SOUTHERN APPALACHIANS; MANAGED FOREST; NORTH-AMERICA; LANDSCAPE; ABUNDANCE; POPULATION; MANICULATUS; DYNAMICS; SCALE AB Forests of Southern Appalachia are critical habitats with respect to biodiversity, with a large portion of these forests residing on public multiuse lands. With pressure to extract timber from maturing forests, there is a need to identify the relative importance of forest types within the larger forest matrix. We examined small-mammal populations at 350 sample points across 157 km(2) of forested habitat in the George Washington and Jefferson National Forests, Virginia, to determine landscape and habitat correlates of species abundance and richness. A total of 3,955 individuals representing 20 species were captured using live trap and pitfall sampling at each point during 1996 and 1997. Nine species were sufficiently common to examine their abundance relative to landscape and habitat features. We found species abundance and richness to be highest in mesic deciduous forest types, with the exception of Peromyscus leucopus. Soil moisture capacity and the proportion of mesic habitat within 100 m of the sample point were also important for several species. If mesic deciduous forest can be considered patches within a matrix of xeric forest, then the abundance of 4 species and species richness could be predicted based on the distance of the sample point to the nearest mesic patch and the abundance of 3 species inside mesic patches was related to patch size. At least 73% of mesic patches within this forest were <25 ha and separated from other patches by >100 m. Our results indicate that mesic forest patches contain the bulk of the species richness for small mammals in the Southern Appalachian ecotype. Designing timber harvests that minimize use of mesic deciduous forest type and that does not decrease patch numbers would achieve the largest benefits to small mammals within the region. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. Iowa State Univ Sci & Technol, Ecol & Evolutionary Biol Program, Ames, IA 50011 USA. Univ Minnesota, Dept Fisheries & Wildlife, St Paul, MN 55108 USA. RP McShea, WJ (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM wmcshea@crc.si.edu NR 66 TC 17 Z9 18 U1 3 U2 17 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD MAY PY 2003 VL 84 IS 2 BP 627 EP 643 DI 10.1644/1545-1542(2003)084<0627:MDFAPO>2.0.CO;2 PG 17 WC Zoology SC Zoology GA 685VN UT WOS:000183284500027 ER PT J AU Matsui, T Cheung, ASC Leung, KWS Yoshino, K Parkinson, WH Thorne, AP Murray, JE Ito, K Imajo, T AF Matsui, T Cheung, ASC Leung, KWS Yoshino, K Parkinson, WH Thorne, AP Murray, JE Ito, K Imajo, T TI High resolution absorption cross-section measurements of the Schumann-Runge bands of O-2 by VUV Fourier transform spectroscopy SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID HERZBERG-I BANDS; OSCILLATOR-STRENGTHS; PREDISSOCIATION LINEWIDTHS; REGION; STATE; SPECTROMETER; OXYGEN AB The photoabsorption spectrum of the O-2 Schumann-Runge bands was measured with resolution comparable to the Doppler widths by using the VUV Fourier transform spectrometer from Imperial College, London, combined with synchrotron radiation as a continuum light source at the Photon Factory, KEK, Japan. The analysis of the (12,0)-(17,0) bands of the Schumann-Runge system provides accurate rotational line positions as well as the line intensities from 185 to 175nm. Molecular constants of the v' = 12 to 17 levels of the B(3)Sigma(u)(-) state have been determined. The (v', 0) band oscillator strengths were determined as 2.38, 2.62, 2.70, 2.66, 2.40, and 2.12 x 10(-5) for the bands from v' = 12 to 17, respectively. (C) 2003 Elsevier Science (USA). All rights reserved. C1 Univ Tsukuba, Tsukuba, Ibaraki 3058573, Japan. Univ Hong Kong, Hong Kong, Hong Kong, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. KEK, Photon Factory, Tsukuba, Ibaraki 3050801, Japan. Japan Womens Univ, Tokyo 1128681, Japan. RP Yoshino, K (reprint author), Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki 3058565, Japan. RI Cheung, Allan/D-3059-2009 NR 36 TC 10 Z9 10 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD MAY PY 2003 VL 219 IS 1 BP 45 EP 57 DI 10.1016/S0022-2852(03)00009-2 PG 13 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 684RW UT WOS:000183221200005 ER PT J AU Laurance, WF Merona, JMRD Andrade, A Laurance, SG D'Angelo, S Lovejoy, TE Vasconcelos, HL AF Laurance, WF Merona, JMRD Andrade, A Laurance, SG D'Angelo, S Lovejoy, TE Vasconcelos, HL TI Rain-forest fragmentation and the phenology of Amazonian tree communities SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Amazon; edge effects; flowering; fruiting; habitat fragmentation; leaf production; plant reproduction; rain forest; trees ID REPRODUCTIVE PHENOLOGY; POPULATION; RESPONSES; DYNAMICS; BEES C1 Smithsonian Trop Res Inst, Balboa, Panama. 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. RI Laurance, William/B-2709-2012; Vasconcelos, Heraldo/C-3353-2013; Laurance, Susan/G-6021-2011 OI Vasconcelos, Heraldo/0000-0001-6969-7131; Laurance, Susan/0000-0002-2831-2933 NR 29 TC 21 Z9 22 U1 4 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 MAY PY 2003 VL 19 BP 343 EP 347 DI 10.1017/S0266467403003389 PN 3 PG 5 WC Ecology SC Environmental Sciences & Ecology GA 692JU UT WOS:000183658600014 ER PT J AU Schroll, S AF Schroll, S TI Critical terms for art history, 2nd edition. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Schroll, S (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 1 PY 2003 VL 128 IS 8 BP 109 EP 109 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 672TA UT WOS:000182536600053 ER PT J AU Thresher, R Proctor, C Ruiz, G Gurney, R MacKinnon, C Walton, W Rodriguez, L Bax, N AF Thresher, R Proctor, C Ruiz, G Gurney, R MacKinnon, C Walton, W Rodriguez, L Bax, N TI Invasion dynamics of the European shore crab, Carcinus maenas, in Australia SO MARINE BIOLOGY LA English DT Article ID GREEN CRAB; DECAPODA; RECRUITMENT; DISPERSAL; LARVAE; CALIFORNIA; IMPACT; SPREAD; SHELF; COAST AB In Australia and most other invaded locations, rates of range expansion by the European shore crab, Carcinus maenas, are-typically only a few kilometres per year, despite a planktonic duration upwards of 50 days and off-shore larval development. This relatively static A distribution is punctuated by rare episodes of long-distance and large-scale spread, some of which appear to be related to unusual oceanographic conditions and some of which are likely to be human assisted. These observations suggest, first, that long planktonic duration and off-shore development in a marine invertebrate does not preclude very localised recruitment, and, second, that this recruitment norm may be punctuated by brief episodes of wide scale mixing of propagules. Punctuated dispersal has previously been suggested to account for large-scale biogeographic patterns of distribution and speciation, but may also have implications for the processes that stabilise structured spatial metapopulations. C1 CSIRO, Ctr Res Introduced Marine Pests, Hobart, Tas 7001, Australia. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Tasmania, Dept Zool, Taroona, Tas, Australia. RP Thresher, R (reprint author), CSIRO, Ctr Res Introduced Marine Pests, GPO Box 1538, Hobart, Tas 7001, Australia. EM Ron.Thresher@csiro.au RI Thresher, Ronald/C-7442-2009; Bax, Nicholas/A-2321-2012; Proctor, Craig/I-3710-2016; OI Bax, Nicholas/0000-0002-9697-4963; Ruiz, Gregory/0000-0003-2499-441X NR 46 TC 58 Z9 61 U1 2 U2 30 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD MAY PY 2003 VL 142 IS 5 BP 867 EP 876 DI 10.1007/s00227-003-1011-1 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 693NQ UT WOS:000183724000005 ER PT J AU Sanchez, JA McFadden, CS France, SC Lasker, HR AF Sanchez, JA McFadden, CS France, SC Lasker, HR TI Molecular phylogenetic analyses of shallow-water Caribbean octocorals SO MARINE BIOLOGY LA English DT Article ID GORGONACEAN OCTOCORALS; SARCOPHYTON GLAUCUM; MITOCHONDRIAL-DNA; MISMATCH REPAIR; COELENTERATA; CORAL; ANTHOZOA; CNIDARIA; GENE; SUBSTITUTION AB Octocorals, especially gorgonians, are conspicuous on Caribbean coral reefs, but there is no consensus regarding species relationships. Mitochondrial protein-coding genes [NADH-dehydrogenase subunits 2 (ND2) and 6 (ND6), and mutS homolog (msh1), 1633 bp] from 28 shallow-water species were sequenced to develop the first molecular phylogeny for Caribbean octocorals. The specimens were collected primarily in the Caribbean or off Brazil in 1999-2001. Morphological characters (sclerites and axial ultrastructure) were also examined in order to map them onto the molecular phylogeny. Analyses of both nucleotide and amino acid substitutions using maximum parsimony and likelihood (including maximum-likelihood and Bayesian analysis) generated very similar results, with most nodes having high levels of support. These molecular results were significantly different from the generally accepted classification. Neither Plexauridae nor Gorgoniidae were monophyletic. Plexaurella spp., nominal plexaurids, were basal to the gorgoniids, sharing many morphological characters with them. This corroborates previous findings using secondary metabolites and biosynthetic pathways. The sea fans, Gorgonia spp. and Pacifigorgia spp., as well as the pinnate gorgonians, Muriceopsis flavida and Pseudopterogorgia spp., did not have sea fan or pinnate relatives, suggesting there has been convergent evolution of colony form. Caribbean plexaurids appeared more derived and/or recently evolved according to both morphological and molecular data (e.g. Eunicea spp. and Plexaura spp.). Molecular phylogenetics is a promising approach for reconstructing phylogenetic relationships among octocorals as well as to understand their complex morphology. C1 SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA. Harvey Mudd Coll, Dept Biol, Claremont, CA 91711 USA. Coll Charleston, Dept Biol, Grice Marine Lab, Charleston, SC 29412 USA. RP Sanchez, JA (reprint author), Smithsonian Inst, Dept Systemat Biol, POB 37012,NMNH W 329,MRC-0163, Washington, DC 20013 USA. RI Johnson, Selena/K-3541-2013 NR 60 TC 75 Z9 81 U1 1 U2 13 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAY PY 2003 VL 142 IS 5 BP 975 EP 987 DI 10.1007/s00227-003-1018-7 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 693NQ UT WOS:000183724000015 ER PT J AU Myers, ST Jackson, NJ Browne, IWA de Bruyn, AG Pearson, TJ Readhead, ACS Wilkinson, PN Biggs, AD Blandford, RD Fassnacht, CD Koopmans, LVE Marlow, DR McKean, JP Norbury, MA Phillips, PM Rusin, D Shepherd, MC Sykes, CM AF Myers, ST Jackson, NJ Browne, IWA de Bruyn, AG Pearson, TJ Readhead, ACS Wilkinson, PN Biggs, AD Blandford, RD Fassnacht, CD Koopmans, LVE Marlow, DR McKean, JP Norbury, MA Phillips, PM Rusin, D Shepherd, MC Sykes, CM TI The Cosmic Lens All-Sky Survey - I. Source selection and observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; cosmology : observations ID 4-IMAGE GRAVITATIONAL LENS; PHASE CALIBRATION SOURCES; RADIO-SOURCES; SYSTEM; GALAXY; SPECTRUM; B2114+022; B1608+656; REDSHIFTS; B1152+199 AB The Cosmic Lens All-Sky Survey (CLASS) is an international collaborative programme which has obtained high-resolution radio images of over 10 000 flat-spectrum radio sources in order to create the largest and best-studied statistical sample of radio-loud gravitationally lensed systems. With this survey, combined with detailed studies of the lenses found therein, constraints can be placed on the expansion rate, matter density and dark energy (e.g. cosmological constant, quintessence) content of the Universe that are complementary to and independent of those obtained through other methods. CLASS is aimed at identifying lenses where multiple images are formed from compact flat-spectrum radio sources, which should be easily identifiable in the radio maps. Because CLASS is radio-based, dust obscuration in lensing galaxies is not a factor, and the relative insensitivity of the instrument to environmental conditions (e.g. weather, 'seeing') leads to nearly uniform sensitivity and resolution over the entire survey. In four observing 'seasons' from 1994 to 1999, CLASS has observed 13 783 radio sources with the Very Large Array (VLA) at 8.4 GHz in its largest 'A'-configuration (0.2-arcsec resolution). When combined with the Jodrell Bank VLA Astrometric Survey (JVAS), the CLASS sample contains over 16 000 images. A complete sample of 11 685 sources was observed, selected to have a flux density of at least 30 mJy in the Green Bank Survey (GB6) catalogue at 4.85 GHz (spanning the declination range 0degrees less than or equal to delta less than or equal to 75degrees and \b\ greater than or equal to 10degrees, excluding the Galactic plane) and a spectral index alpha greater than or equal to -0.5 between the NRAO-VLA Sky Survey (NVSS) at 1.4 GHz and the GB6. A typical 30-s CLASS snapshot reached an rms noise level of 0.4 mJy. So far, CLASS has found 16 new gravitational lens systems, and the JVAS/CLASS survey contains a total of 22 lenses. The follow-up of a small number of candidates using the VLA, MERLIN, the Very Long Baseline Array (VLBA) and optical telescopes is still underway. In this paper, we present a summary of the CLASS observations, the JVAS/CLASS sample, and statistics on sub-samples of the survey. An accompanying paper presents the lens candidate selection, and in a third paper the implications for cosmology are discussed. C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Univ Groningen, Kapteyn Astron Inst, NL-9700 AA Groningen, Netherlands. Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands. CALTECH, Pasadena, CA 91125 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Myers, ST (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA. EM smyers@nrao.edu RI Pearson, Timothy/N-2376-2015 OI Pearson, Timothy/0000-0001-5213-6231 NR 63 TC 212 Z9 213 U1 1 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 MAY 1 PY 2003 VL 341 IS 1 BP 1 EP 12 DI 10.1046/j.1365-8711.2003.06256.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 673JN UT WOS:000182577300002 ER PT J AU Browne, IWA Wilkinson, PN Jackson, NJF Myers, ST Fassnacht, CD Koopmans, LVE Marlow, DR Norbury, M Rusin, D Sykes, CM Biggs, AD Blandford, RD de Bruyn, AG Chae, KH Helbig, P King, LJ McKean, JP Pearson, TJ Phillips, PM Readhead, ACS Xanthopoulos, E York, T AF Browne, IWA Wilkinson, PN Jackson, NJF Myers, ST Fassnacht, CD Koopmans, LVE Marlow, DR Norbury, M Rusin, D Sykes, CM Biggs, AD Blandford, RD de Bruyn, AG Chae, KH Helbig, P King, LJ McKean, JP Pearson, TJ Phillips, PM Readhead, ACS Xanthopoulos, E York, T TI The Cosmic Lens All-Sky Survey - II. Gravitational lens candidate selection and follow-up SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE gravitation; gravitational lensing; radio continuum : galaxies ID PHASE CALIBRATION SOURCES; TIME-DELAY MEASUREMENTS; HUBBLE SPACE TELESCOPE; VLA ASTROMETRIC SURVEY; COMPACT RADIO-SOURCES; COSMOLOGICAL CONSTANT; EXTRAGALACTIC SURVEYS; VLBI OBSERVATIONS; SYSTEM B1933+503; CLASS B2319+051 AB We report the final results of the search for gravitationally lensed flat-spectrum radio sources found in the combination of CLASS (Cosmic Lens All-Sky Survey) and JVAS (Jodrell Bank VLA Astrometric Survey). VLA (Very Large Array) observations of 16 503 sources have been made, resulting in the largest sample of arcsec-scale lens systems available. Contained within the 16 503 sources is a complete sample of 11 685 sources which have two-point spectral indices between 1.4 and 5 GHz flatter than -0.5, and 5-GHz flux densities greater than or equal to30 mJy. A subset of 8958 sources form a well-defined statistical sample suitable for analysis of the lens statistics. We describe the systematic process by which 149 candidate lensed sources were picked from the statistical sample on the basis of possessing multiple compact components in the 0.2-arcsec resolution VLA maps. Candidates were followed up with 0.05-arcsec resolution MERLIN and 0.003-arcsec VLBA observations at 5 GHz and rejected as lens systems if they failed well-defined surface brightness and/or morphological tests. To illustrate the candidate elimination process, we show examples of sources representative of particular morphologies that have been ruled out by the follow-up observations. 194 additional candidates, not in the well-defined sample, were also followed up. Maps for all the candidates can be found on the World Wide Web at http://www.jb.man.ac.uk/research/gravlens/index.html. We summarize the properties of each of the 22 gravitational lens systems in JVAS/CLASS. 12 are double-image systems, nine are four-image systems and one is a six-image system. 13 constitute a statistically well-defined sample giving a point-source lensing rate of 1:690 +/- 190. The interpretation of the results in terms of the properties of the lensing galaxy population and cosmological parameters will be published elsewhere. C1 Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Natl Radio Astron Observ, Socorro, NM 87801 USA. Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands. CALTECH, Pasadena, CA 91125 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Univ Groningen, Kapteyn Astron Inst, NL-9700 AA Groningen, Netherlands. Univ Bonn, D-53121 Bonn, Germany. STScI, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Browne, IWA (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. EM iwb@jb.man.ac.uk RI Pearson, Timothy/N-2376-2015 OI Pearson, Timothy/0000-0001-5213-6231 NR 115 TC 203 Z9 204 U1 1 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2003 VL 341 IS 1 BP 13 EP 32 DI 10.1046/j.1365-8711.2003.06257.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 673JN UT WOS:000182577300003 ER PT J AU Arnold, AE Herre, EA AF Arnold, AE Herre, EA TI Canopy cover and leaf age affect colonization by tropical fungal endophytes: Ecological pattern and process in Theobroma cacao (Malvaceae) SO MYCOLOGIA LA English DT Article DE Barro Colorado Island; ecology; endophytic fungi; leaf chemistry; leaf toughness; Panama; sporefall; tropical forest ID PAECILOMYCES-FUMOSOROSEUS DEUTEROMYCOTINA; ENTOMOPATHOGENIC FUNGUS; WATER-STRESS; MONILINIA-FRUCTICOLA; MYCELIAL GROWTH; PECAN SCAB; DIVERSITY; LEAVES; GERMINATION; INFECTION AB Fungal endophytes inhabit healthy tissues of all terrestrial plant taxa studied to date and arc diverse and abundant in leaves of tropical woody angiosperms. Studies have demonstrated that plant location and leaf age influence density of endophyte infection in leaves of tropical forest trees. However, ecological factors underlying these observations have not been explored in detail. Here, we establish that foliar endophytes of a tropical tree (Theobroma cacao, Malvaceae) are transmitted horizontally and that endophyte-free seedlings can be produced for experimental manipulation by protecting aerial tissues from surface wetting. At Barro Colorado Island, Panama, we used transects of endophyte-free seedlings to determine the importance of several factors (canopy cover, abundance of aerial and epiphytic propagules, leaf age, leaf chemistry, leaf toughness and duration of exposure to viable air spora) in shaping colonization by endophytic fungi. Endophytes colonized leaves of T cacao more rapidly beneath the forest canopy than in cleared sites, reflecting local abundance of aerial and epiphytic propagules. The duration of exposure, rather than absolute leaf age, influenced endophyte infection, whereas leaf toughness and chemistry had no observed effect. Endophytes isolated from mature T cacao grew more rapidly on media containing leaf extracts of T cacao than on media containing extracts from other co-occurring tree species, suggesting that interspecific differences in leaf chemistry influence endophyte assemblages. Together, these data allow us to identify factors underlying patterns of endophyte colonization within healthy leaves of this tropical tree. C1 Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Arnold, AE (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. NR 76 TC 125 Z9 139 U1 4 U2 54 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0027-5514 J9 MYCOLOGIA JI Mycologia PD MAY-JUN PY 2003 VL 95 IS 3 BP 388 EP 398 DI 10.2307/3761880 PG 11 WC Mycology SC Mycology GA 705KG UT WOS:000184393800002 PM 21156627 ER PT J AU Sweeney, A Jiggins, C Johnsen, S AF Sweeney, A Jiggins, C Johnsen, S TI Insect communication: Polarized light as a butterfly mating signal SO NATURE LA English DT Article ID COLOR C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Edinburgh, Inst Cell Anim & Populat Biol, Edinburgh EH9 3JT, Midlothian, Scotland. RP Sweeney, A (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA. RI Jiggins, Chris/B-9960-2008 OI Jiggins, Chris/0000-0002-7809-062X NR 12 TC 125 Z9 131 U1 2 U2 42 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 1 PY 2003 VL 423 IS 6935 BP 31 EP 32 DI 10.1038/423031a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 673CG UT WOS:000182561600030 PM 12721616 ER PT J AU Takacs, E Silver, E Laming, JM Gillaspy, JD Schnopper, H Brickhouse, N Barbera, M Mantraga, M Ratliff, LP Tawara, H Makonyi, K Madden, N Landis, D Beeman, J Haller, EE AF Takacs, E Silver, E Laming, JM Gillaspy, JD Schnopper, H Brickhouse, N Barbera, M Mantraga, M Ratliff, LP Tawara, H Makonyi, K Madden, N Landis, D Beeman, J Haller, EE TI Astrophysics and spectroscopy with microcalorimeters on an electron beam ion trap SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 11th International Conference on the Physics of Highly Charged Ions (HCI 2002) CY SEP 01-06, 2002 CL CAEN, FRANCE DE electron beam ion trap; X-ray; microcalorimeter; highly charged ion; laboratory astrophysics ID X-RAY SPECTROSCOPY; TRANSMISSION GRATING SPECTROMETER; FE-XVII; LABORATORY ASTROPHYSICS; EMISSION; SPECTRA; CAPELLA; TEMPERATURE; INTENSITY; PROGRESS AB Electron beam ion traps combined with X-ray microcalorimeters provide an indispensable tool for laboratory astrophysics supporting recent and future X-ray missions. The program at the National Institute of Standards and Technology uses spectroscopic methods to study highly ionized plasmas and atomic physics related to astrophysics problems (C) 2003 Elsevier Science B.V. All rights reserved. C1 Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. MIT, Cambridge, MA USA. Debrecen Univ, H-4026 Debrecen, Hungary. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. INAF, Osserv Astron Palermo GS Vaiana, Palermo, Italy. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RP Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. EM endre.takacs@nist.gov OI Brickhouse, Nancy/0000-0002-8704-4473; Barbera, Marco/0000-0002-3188-7420 NR 36 TC 6 Z9 6 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X EI 1872-9584 J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD MAY PY 2003 VL 205 BP 144 EP 155 DI 10.1016/S0168-583X(03)00937-6 PG 12 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 684MM UT WOS:000183211200028 ER PT J AU Beiersdorfer, P Behar, E Boyce, KR Brown, GV Chen, H Gendreau, KC Graf, A Gu, MF Harris, CL Kahn, SM Kelley, RL Lepson, JK May, MJ Neill, PA Pinnington, EH Porter, FS Smith, AJ Stahle, CK Szymkowiak, AE Tillotson, A Thorn, DB Trabert, E Wargelin, BJ AF Beiersdorfer, P Behar, E Boyce, KR Brown, GV Chen, H Gendreau, KC Graf, A Gu, MF Harris, CL Kahn, SM Kelley, RL Lepson, JK May, MJ Neill, PA Pinnington, EH Porter, FS Smith, AJ Stahle, CK Szymkowiak, AE Tillotson, A Thorn, DB Trabert, E Wargelin, BJ TI Overview of the Livermore electron beam ion trap project SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 11th International Conference on the Physics of Highly Charged Ions (HCI 2002) CY SEP 01-06, 2002 CL CAEN, FRANCE DE electron beam ion trap; SuperEBIT; microcalorimeter; spectroscopy (X-ray and optical) ID M1 TRANSITION RATES; HIGH-RESOLUTION; FE-XVII; LINES; MICROCALORIMETER; SPECTROMETER; INTENSITY AB The Livermore electron beam ion trap facility has recently been moved to a new location within LLNL, and new instrumentation was added, including a 32-pixel microcalorimeter. The move was accompanied by a shift of focus toward in situ measurements of highly charged ions, which continue with increased vigor. Overviews of the facility, which includes EBIT-I and SuperEBIT, and the research projects are given, including results from optical spectroscopy, QED, and X-ray line excitation measurements. (C) 2003 Elsevier Science B.V. All rights reserved. C1 Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Columbia Univ, New York, NY 10027 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Davis, Davis, CA 95616 USA. MIT, Cambridge, MA 02139 USA. Univ Nevada, Reno, NV 89557 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. Univ Alberta, Edmonton, AB T6G 2J1, Canada. Morehouse Coll, Atlanta, GA 30314 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Beiersdorfer, P (reprint author), Lawrence Livermore Natl Lab, L-260, Livermore, CA 94550 USA. RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Porter, Frederick/0000-0002-6374-1119; NR 31 TC 11 Z9 11 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD MAY PY 2003 VL 205 BP 173 EP 177 DI 10.1016/S0168-583X(03)00941-8 PG 5 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 684MM UT WOS:000183211200032 ER PT J AU Matranga, M Barbera, M Maggio, A Peres, G Serio, S Takacs, E Silver, E Gillaspy, J Schnopper, H Laming, M Beeman, J Haller, E Madden, N AF Matranga, M Barbera, M Maggio, A Peres, G Serio, S Takacs, E Silver, E Gillaspy, J Schnopper, H Laming, M Beeman, J Haller, E Madden, N TI EBIT diagnostics using X-ray spectra of highly ionized Ne SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 11th International Conference on the Physics of Highly Charged Ions (HCI 2002) CY SEP 01-06, 2002 CL CAEN, FRANCE DE X-ray spectra; EBIT; excitation; ionization of atoms ID BEAM ION-TRAP; LABORATORY ASTROPHYSICS AB We have carried out a detailed analysis of highly ionized neon spectra collected at the NIST EBIT using an NTD germanium X-ray microcalorimeter developed at the Harvard-Smithsonian Center for Astrophysics [Nucl. Instr. and Meth. A 444 (2000) 156]. Our attention was focused especially on the Ne IX He-like triplet to check electron density diagnostics through the intercombination/forbidden line ratio. We have investigated possible effects of the ion dynamics on the plasma emission line intensities, looking at the dependence of the count-rate and the charge state distribution on the electron beam energy and current. The temperature and spatial distribution of the neon ions, and hence the overlap between the electron beam and the ion cloud, depend on the electron beam operating parameters. The overlap affects the average electron density seen by the ions, and in turn the measured line ratio. These results underscore the value of future improved studies of the trapped ion dynamics, both for understanding the EBIT performance and for allowing experimenters to take full advantage of its potential for astrophysical plasma diagnostics. (C) 2003 Elsevier Science B.V. All rights reserved. C1 INAF, Osserv Astron Palermo, I-90134 Palermo, Italy. Univ Palermo, Dipartimento Sci Fis & Astron, I-90134 Palermo, Italy. MIT, Cambridge, MA 02139 USA. Univ Debrecen, H-4026 Debrecen, Hungary. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. USN, Res Lab, Washington, DC 20375 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RP INAF, Osserv Astron Palermo, I-90134 Palermo, Italy. EM barbera@astropa.unipa.it RI Maggio, Antonio/P-5700-2015; OI Maggio, Antonio/0000-0001-5154-6108; Barbera, Marco/0000-0002-3188-7420; PERES, Giovanni/0000-0002-6033-8180 NR 11 TC 6 Z9 6 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X EI 1872-9584 J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD MAY PY 2003 VL 205 BP 244 EP 249 DI 10.1016/S0168-583X(03)00943-1 PG 6 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 684MM UT WOS:000183211200047 ER PT J AU Merabet, H Bruch, R Fulling, S Bailey, M Godunov, AL McGuire, JH Grum-Grzhimailo, AN Bartschat, K AF Merabet, H Bruch, R Fulling, S Bailey, M Godunov, AL McGuire, JH Grum-Grzhimailo, AN Bartschat, K TI Ionization-excitation magnetic sublevel cross sections for He+ (2p)P-2(0) states following fast electron and proton impact SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 11th International Conference on the Physics of Highly Charged Ions (HCI 2002) CY SEP 01-06, 2002 CL CAEN, FRANCE DE ionization-excitation; sublevel cross sections; electron impact; proton impact; helium ID HELIUM; EMISSION; SYSTEMS; ATOMS AB The first experimental magnetic substate scattering-angle-integrated cross sections following ionization-excitation of He(1s(2))S-1 to He-(2p) P-2(0) in the e(-) + He collision system have been determined using a combination of total cross sections and polarization fraction measurements in the extreme ultraviolet range. The derived magnetic sublevel cross sections, sigma(0) and sigma(1), for M-L = 0, +/-1 have been studied over a wide range of electron velocities (2-8.5 a.u.). These results are compared with previous cross sections for equi-velocity proton impact. In addition, our experimental data are compared with earlier theoretical predictions, our recent second-Born calculations fully including off-energy shell terms, and new R-matrix results. We have extended our polarization measurements for H+ + He collisions and found excellent agreement between theory and experiment at nearly all impact energies. However, the present second-Born and R-matrix results deviate slightly from the experimental electron data. (C) 2003 Elsevier Science B.V. All rights reserved. C1 Univ Nevada, Dept Phys, Reno, NV 89557 USA. Tulane Univ, Dept Phys, New Orleans, LA 70118 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Moscow MV Lomonosov State Univ, Inst Nucl Phys, Moscow 119992, Russia. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Univ Nevada, Dept Phys, Reno, NV 89557 USA. EM hocine@physics.unr.edu RI Godunov, Alexander/G-4266-2011; Grum-Grzhimailo, Alexei/D-6274-2012; Bartschat, Klaus/I-2527-2012 NR 21 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X EI 1872-9584 J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD MAY PY 2003 VL 205 BP 399 EP 404 DI 10.1016/S0168-583X(02)02047-5 PG 6 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 684MM UT WOS:000183211200078 ER PT J AU Janzen, PH Gardner, LD Reisenfeld, DB Kohl, JL AF Janzen, PH Gardner, LD Reisenfeld, DB Kohl, JL TI Absolute cross section for Si2+(3s3p P-3(o)-> 3s3p P-1(o)) electron-impact excitation SO PHYSICAL REVIEW A LA English DT Article ID SOLAR TRANSITION REGION; 3S(2) S-1->3S3P P-3; RESONANCE STRUCTURE; LINE RATIOS; IONS; INTERFERENCE AB We have measured the absolute energy-averaged cross section for electron-impact excitation of Si2+(3s3p P-3(o)-->3s3p P-1(o)) from energies below threshold to the turn-on of the 3s3p P-3(o)-->3p(2) P-3 transition. A beams modulation technique with inclined electron and ion beams was used. Radiation at 120.65 nm from the decay of the excited ions to the 3s(2) S-1 ground state was detected using an absolutely calibrated optical system. The fractional population of metastable Si2+(3s3p P-3(o)) in the incident ion beam was determined to be 0.256+/-0.035(1.65sigma). The experimental energy spread ranged from 0.85 eV (full width at half maximum) at the lowest energies to 0.56 eV at the highest. Resonance features consistent with 12-state close-coupling R-matrix calculations are seen. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Janzen, PH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Reisenfeld, Daniel/F-7614-2015 NR 28 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 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAY PY 2003 VL 67 IS 5 AR 052702 DI 10.1103/PhysRevA.67.052702 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 686AU UT WOS:000183298800054 ER PT J AU Krems, RV Dalgarno, A AF Krems, RV Dalgarno, A TI Threshold laws for collisional reorientation of electronic angular momentum SO PHYSICAL REVIEW A LA English DT Article ID ULTRACOLD MOLECULES; COLD; TEMPERATURES AB It is shown that the velocity dependence of cross sections for projection-changing transitions in collisions of paramagnetic atoms or molecules with structureless targets near threshold has the form v(2Deltam) when Deltam is even and v(2(Deltam+1)) when Deltam is odd, where Deltam is the change in the projection quantum number and v is the relative velocity. C1 Harvard Smithsonian Ctr Astrophys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. EM rkrems@cfa.harvard.edu NR 15 TC 26 Z9 26 U1 1 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD MAY PY 2003 VL 67 IS 5 AR 050704 DI 10.1103/PhysRevA.67.050704 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 686AU UT WOS:000183298800008 ER PT J AU Laurance, WF AF Laurance, WF TI Slow burn: the insidious effects of surface fires on tropical forests SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID EL-NINO; AMAZONIAN FORESTS; EASTERN AMAZON; CLIMATE-CHANGE; GROUND FIRES; RAIN-FOREST; RESPONSES; ECOLOGY; IMPACT; EVENT AB Accidental surface fires are emerging as one of the most pervasive threats to tropical forests. Although unimpressive in appearance, these fires can have surprisingly potent impacts on rainforest plant and animal communities, as demonstrated by recent studies led by Jos Barlow and Carlos Peres in central Amazonia. Even worse, surface fires greatly increase the likelihood of far larger conflagrations that can lead to complete forest destruction. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. RI Laurance, William/B-2709-2012 NR 25 TC 37 Z9 39 U1 2 U2 14 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 MAY PY 2003 VL 18 IS 5 BP 209 EP 212 DI 10.1016/S0169-5347(03)00064-8 PG 4 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 682XF UT WOS:000183117100002 ER PT J AU Temeles, EJ Kress, WJ AF Temeles, EJ Kress, WJ TI Adaptation in a plant-hummingbird association SO SCIENCE LA English DT Article ID AGE-SEX CLASSES; RUFOUS HUMMINGBIRDS; DIMORPHISM; BEHAVIOR AB Sexual dimorphism in bill morphology and body size of the Caribbean purple-throated carib hummingbird is associated with a reversal in. oral dimorphism of its Heliconia food plants. This hummingbird is the sole pollinator of H. caribaea and H. bihai, with flowers of the former corresponding to the short, straight bills of males, the larger sex, and flowers of the latter corresponding to the long, curved bills of females. On St. Lucia, H. bihai compensates for the rarity of H. caribaea by evolving a second color morph with flowers that match the bills of males, whereas on Dominica, H. caribaea evolves a second color morph with flowers that match the bills of females. The nectar rewards of all Heliconia morphs are consistent with each sex's choice of the morph that corresponds to its bill morphology and energy requirements, supporting the hypothesis that feeding preferences have driven their coadaptation. C1 Amherst Coll, Dept Biol, Amherst, MA 01002 USA. Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, MRC166, Washington, DC 20013 USA. RP Temeles, EJ (reprint author), Amherst Coll, Dept Biol, Amherst, MA 01002 USA. NR 16 TC 96 Z9 97 U1 3 U2 63 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD APR 25 PY 2003 VL 300 IS 5619 BP 630 EP 633 DI 10.1126/science.1080003 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 671FB UT WOS:000182453700039 PM 12714743 ER PT J AU Schneider, R Ferrara, A Salvaterra, R Omukai, K Bromm, V AF Schneider, R Ferrara, A Salvaterra, R Omukai, K Bromm, V TI Low-mass relics of early star formation SO NATURE LA English DT Article ID NUCLEOSYNTHESIS AB The earliest stars to form in the Universe were the first sources of light, heat and metals after the Big Bang. The products of their evolution will have had a profound impact on subsequent generations of stars. Recent studies(1-7) of primordial star formation have shown that, in the absence of metals (elements heavier than helium), the formation of stars with masses 100 times that of the Sun would have been strongly favoured, and that low-mass stars could not have formed before a minimum level of metal enrichment had been reached. The value of this minimum level is very uncertain, but is likely to be between 10(-6) and 10(-4) that of the Sun(6,8). Here we show that the recent discovery(9) of the most iron-poor star known indicates the presence of dust in extremely low-metallicity gas, and that this dust is crucial for the formation of lower-mass second-generation stars that could survive until today. The dust provides a pathway for cooling the gas that leads to fragmentation of the precursor molecular cloud into smaller clumps, which become the lower-mass stars. C1 Osserv Astrofis Arcetri, I-50125 Florence, Italy. Enrico Fermi Ctr, I-00184 Rome, Italy. Scuola Int Super Studi Avanzati, SSISA, I-34100 Trieste, Italy. Natl Astron Observ, Div Theoret Astrophys, Tokyo 1818588, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schneider, R (reprint author), Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy. RI Ferrara, Andrea/A-4357-2011; Schneider, Raffaella/E-4216-2017; OI Schneider, Raffaella/0000-0001-9317-2888; Salvaterra, Ruben/0000-0002-9393-8078 NR 14 TC 155 Z9 155 U1 2 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 24 PY 2003 VL 422 IS 6934 BP 869 EP 871 DI 10.1038/nature01579 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 670WR UT WOS:000182432600047 PM 12712198 ER PT J AU Dickerson, PW AF Dickerson, PW TI Intraplate mountain building in response to continent-continent collision - the Ancestral Rocky Mountains (North America) and inferences drawn from the Tien Shan (Central Asia) SO TECTONOPHYSICS LA English DT Article; Proceedings Paper CT Annual Conference on Collisional Orogenesis in the Geological Record and Modern Analogues CY 2001 CL SION, SWITZERLAND DE Tien Shan; Ancestral Rocky Mountains; tectonics; neotectonics; intraplate deformation; late Paleozoic; India; Eurasia; Laurentia; Gondwana; lithosphere ID LATE PALEOZOIC DEFORMATION; UNITED-STATES; MEXICO; EVOLUTION; TEXAS; LITHOSPHERE; CHIHUAHUA; EXAMPLES; MARGIN; BASIN AB The intraplate Ancestral Rocky Mountains of western North America extend from British Columbia, Canada, to Chihuahua, Mexico, and formed during Early Carboniferous through Early Permian time in response to continent-continent collision of Laurentia with Gondwana-the conjoined masses of Africa and South America, including Yucatan and Florida. Uplifts and flanking basins also formed within the Laurentian Midcontinent. On the Gondwanan continent, well inboard from the marginal fold belts, a counterpart structural array developed during the same period. Intraplate deformation began when full collisional plate coupling had been achieved along the continental margin; the intervening ocean had been closed and subduction had ceased-that is, the distinction between upper versus lower plates became moot. Ancestral Rockies deformation was not accompanied by volcanism. Basement shear zones that formed during Mesoproterozoic rifting of Laurentia were reactivated and exerted significant control on the locations, orientations, and modes of displacement on late Paleozoic faults. Ancestral Rocky Mountain uplifts extend as far south as Chihuahua and west Texas (28degrees to 33degreesN, 102degrees to 109degreesW) and include the Florida-Moyotes, Placer de Guadalupe-Carrizalillo, Ojinaga-Tascotal and Hueco Mountain blocks, as well as the Diablo and Central Basin Platforms. All are cored with Laurentian Proterozoic crystalline basement rocks and host correlative Paleozoic stratigraphic successions. Pre-late Paleozoic deformational, thermal, and metamorphic histories are similar as well. Southern Ancestral Rocky Mountain structures terminate along a line that trends approximately N 40degreesE (present coordinates), a common orientation for Mesoproterozoic extensional structures throughout southern to central North America. Continuing Tien Shan intraplate deformation (Central Asia) has created an analogous array of uplifts and basins in response to the collision of India with Eurasia, beginning in late Miocene time when full coupling of the colliding plates had occurred. As in the Laurentia-Gondwana case, structures of similar magnitude and spacing to those in Eurasia have developed in the Indian plate. Within the present orogen two ancient suture zones have been reactivated-the early Paleozoic Terskey zone and the late Paleozoic Turkestan suture between the Siberian and East Gondwanan cratons. Inverted Proterozoic to early Paleozoic rift structures and passive-margin deposits are exposed north of the Terskey zone. In the Alay and Tarim complexes, Vendian to mid-Carboniferous passive-margin strata and the subjacent Proterozoic crystalline basement have been uplifted. Data on Tien Shan uplifts, basins, structural arrays, and deformation rates guide paleotectonic interpretations of ancient intraplate mountain belts. Similarly,. exhumed deep crustal shear zones in the Ancestral Rockies offer insight into partitioning and reorientation of strain, during contemporary intraplate deformation. (C) 2003 Elsevier Science B.V. All rights reserved. C1 NASA, Lyndon B Johnson Space Ctr, Lockheed Martin, Houston, TX 77058 USA. RP Dickerson, PW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 66 TC 9 Z9 10 U1 0 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0040-1951 J9 TECTONOPHYSICS JI Tectonophysics PD APR 24 PY 2003 VL 365 IS 1-4 SI SI BP 129 EP 142 DI 10.1016/S0040-1951(03)00019-2 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 674ND UT WOS:000182642100007 ER PT J AU Nizinski, MS AF Nizinski, MS TI Annotated checklist of decapod crustaceans of Atlantic coastal and continental shelf waters of the United States SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Review ID LOBSTER PANULIRUS-ARGUS; GULF-OF-MEXICO; CRAB CARCINUS-MAENAS; WESTERN ATLANTIC; HEMIGRAPSUS-SANGUINEUS; NORTHWESTERN ATLANTIC; MOLECULAR PHYLOGENY; HERMIT-CRABS; CALLIANASSIDAE CRUSTACEA; TOMOPAGURUS CRUSTACEA AB The decapod crustacean assemblage inhabiting estuarine, neritic and continental shelf waters (to 190 m) of the temperate eastern United States is diverse, with 391 species reported from Maine to Cape Canaveral, Florida. Three recognized biogeographic provinces (Boreal in part, Virginian and Carolinian) are included in this region. The assemblage contains 122 shrimp species (28 penaeids, 2 stenopodids, and 92 carideans), 10 thalassinideans, 8 lobsters, 61 anomurans and 190 brachyurans. Since previous compilation of this fauna, 12 additional species have been described, including four carideans, one callianassid, four anomurans, and three brachyurans. Range extensions into the region have been reported for another five species (Parapenaeus americanus, Scyllarides aequinoctialis, Petrolisthes armatus, Dromia erythropus, Clythrocerus nitidus). One species, Hemigrapsus sanguineus, has been introduced and become established throughout intertidal environments from southern Maine to northern North Carolina. Six species previously recorded from this region are no longer considered to occur there. Two of these species occur south of the Carolinian biogeographic province, three others are now known to occur only in the Pacific Ocean, and one species previously considered as likely to occur in the region has never actually been recorded there. Scientific nomenclature for all species recorded from the region is updated and referenced. Geographic distributions are summarized for each species incorporating recent published information where available. C1 Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA. RP Nizinski, MS (reprint author), Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, POB 37012,NHB,MRC-0153, Washington, DC 20013 USA. NR 176 TC 35 Z9 40 U1 1 U2 7 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 23 PY 2003 VL 116 IS 1 BP 96 EP 157 PG 62 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 672PH UT WOS:000182529200010 ER PT J AU Blow, WC AF Blow, WC TI New brachyuran crabs (Crustacea : Decapoda) from the Upper Pliocene Yorktown Formation of southeastern Virginia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Six new species of crabs, representing three families and one new genus, are described and illustrated from the Upper Pliocene Yorktown Formation of southeastern Virginia. They are remarkable for their state of preservation and represent the first fossil record for three of these living genera in Virginia's rich Neogene marine deposits. The presence of Stenocionops along with the common occurrence of Persephona in these deposits suggests that warm temperate waters covered southeastern Virginia during the deposition of late Yorktown sediments. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Blow, WC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. NR 42 TC 4 Z9 7 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 23 PY 2003 VL 116 IS 1 BP 168 EP 189 PG 22 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 672PH UT WOS:000182529200012 ER PT J AU Bayer, FM Cairns, SD AF Bayer, FM Cairns, SD TI A new genus of the scleraxonian family Coralliidae (Octocorallia : Gorgonacea) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new genus of the family Coralliidae is established for seven species having longitudinally grooved axes and autozooids seated in distinctive axial pits with beaded margins. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. RP Bayer, FM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, POB 37012, Washington, DC 20013 USA. NR 28 TC 23 Z9 25 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 23 PY 2003 VL 116 IS 1 BP 222 EP 228 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 672PH UT WOS:000182529200017 ER PT J AU Robinson, H AF Robinson, H TI New taxa and combinations of Ageratina from Ecuador, Colombia, and Venezuela (Eupatorieae : Oxylobinae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Thirteen new species, one new combination, and one new forma of Ageratina are validated, mostly from from Ecuador, some from Colombia and Venezuela. The new taxa in subg. Ageratina are Ageratina adenophoroides, A. campii, A. cumbensis, A. cumbensis f. glandulifera, A. ewanii, A. parviceps, A. pseudogracilis, A. rosei, A. serrulata, A. villonacoensis, and A. websteri, with a new combination for A. rhodopappa f. glandularis. New species in subg. Andinia are A. harlingii, A. maranonii, and A. regalis. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Robinson, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 23 PY 2003 VL 116 IS 1 BP 229 EP 255 PG 27 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 672PH UT WOS:000182529200018 ER PT J AU Balakrishnan, N Groenenboom, GC Krems, RV Dalgarno, A AF Balakrishnan, N Groenenboom, GC Krems, RV Dalgarno, A TI The He-CaH((2)Sigma(+)) interaction. II. Collisions at cold and ultracold temperatures SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID VIBRATIONAL-RELAXATION; INELASTIC-COLLISIONS; DIATOMIC MOLECULE; NEUTRAL MOLECULES; CHEMICAL PHYSICS; ENERGY-TRANSFER; SCATTERING; AR; SUPERCHEMISTRY; RESONANCE AB We present cross sections for rotational, vibrational, and fine-structure transitions in He-CaH((2)Sigma) collisions at cold and ultracold temperatures calculated using the ab initio potential energy surface reported in the preceding paper. Rotational quenching is fast, vibrational quenching is slow. The spin-rotational interaction, although small and having no influence at temperatures above 10 K, changes significantly the rate coefficients for rotational quenching at lower temperatures. The theoretical rotational, vibrational, and elastic cross sections are compared with the results of a buffer gas cooling experiment carried out at a temperature of about 0.4 K. The theoretical predictions for the vibrational and elastic cross sections are larger than the measured values. The sensitivity to the potential energy surface is explored. A modified surface diminishes but does not remove the differences between theory and experiment. (C) 2003 American Institute of Physics. C1 Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. Univ Nijmegen, Inst Theoret Chem, NSRIM, NL-6525 ED Nijmegen, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Balakrishnan, N (reprint author), Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. EM naduvala@unlv.edu; gerritg@theochem.kun.nl; rkrems@cfa.harvard.edu; adalgarno@cfa.harvard.edu RI Groenenboom, Gerrit/F-9692-2015 NR 55 TC 63 Z9 64 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD APR 22 PY 2003 VL 118 IS 16 BP 7386 EP 7393 DI 10.1063/1.1562947 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 666CH UT WOS:000182157700027 ER PT J AU O'Sullivan, E Ponman, TJ Collins, RS AF O'Sullivan, E Ponman, TJ Collins, RS TI X-ray scaling properties of early-type galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : haloes; X-rays : galaxies ID ELLIPTIC GALAXIES; DARK-MATTER; PSPC OBSERVATIONS; POOR CLUSTERS; HOT PLASMA; ROSAT; GAS; EMISSION; LUMINOSITIES; CATALOG AB We present an analysis of 39 X-ray luminous early-type galaxies observed with the ROSAT PSPC. Using multicomponent spectral and spatial fits to these data, we have measured halo abundance, temperature, luminosity and surface brightness profile. We compare these measurements to similar results from galaxy groups and clusters, fitting a number of relations commonly used in the study of these larger objects. In particular, we find that the sigma-T-X relation for our sample is similar to that reported for clusters, consistent with beta(spec)=1, and that the L-X-T-X relation has a steep slope (gradient 4.8+/-0.7) comparable with that found for galaxy groups. Assuming isothermality, we construct three-dimensional models of our galaxies, allowing us to measure gas entropy. We find no correlation between gas entropy and system mass, but do find a trend for low-temperature systems to have reduced gas fractions. We conclude that the galaxies in our sample are likely to have developed their haloes through galaxy winds, influenced by their surrounding environment. C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Collins, Ross/G-1450-2010 NR 79 TC 91 Z9 91 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2003 VL 340 IS 4 BP 1375 EP 1399 DI 10.1046/j.1365-8711.2003.06396.x PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665KC UT WOS:000182118200030 ER PT J AU Sun, M Jones, C Murray, SS Allen, SW Fabian, AC Edge, AC AF Sun, M Jones, C Murray, SS Allen, SW Fabian, AC Edge, AC TI Chandra observations of the galaxy cluster A478: The interaction of hot gas and radio plasma in the core, and an improved determination of the compton y-parameter SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; galaxies : clusters : individual (A478); radio continuum : galaxies; X-rays : galaxies : clusters ID HYDRA-A CLUSTER; COOLING FLOW; HUBBLE CONSTANT; RAY; ABELL-2052; ABELL-478; REDSHIFT; BUBBLES AB We present the results from a 42 ks Chandra ACIS observation of the galaxy cluster A478. This cluster is generally considered to be highly relaxed. The Chandra image reveals, for the first time, X-ray cavities in the hot gas within the central 15 kpc radius of A478. Two weak and small (similar to4 kpc) radio lobes that extend from the central nucleus are detected in a 1.4 GHz VLA observation. The radio lobes are roughly along the direction of the X-ray cavities, but are much smaller than the X-ray cavities. We propose a "doughnut" configuration for the hot gas within the central 15 kpc, created by the interaction of the gas with the radio plasma that originated from the nucleus. The current radio activity of the central radio source is weak (similar to0.2% of Hydra A) and the total radio power is at least 10 times smaller than the minimum power needed to create the cavities. We compare A478 with other galaxy clusters in which similar X-ray cavities were found. A478 and A4059 host much weaker central radio sources than do others with similarly sized X-ray cavities. On larger scales, deprojected temperature and density profiles are obtained for A478. We used these to derive the Compton y-parameter, for the first time, through direct integration. The result has a much smaller statistical uncertainty than previous ones. This serves as an example of how high-quality X-ray data can help constrain H-0. The corresponding H-0 also was derived combining the available Sunyaev-Zeldovich effect measurement. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Sun, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 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 APR 20 PY 2003 VL 587 IS 2 BP 619 EP 624 DI 10.1086/368300 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 666CR UT WOS:000182159400014 ER PT J AU Fish, VL Reid, MJ Wilner, DJ Churchwell, E AF Fish, VL Reid, MJ Wilner, DJ Churchwell, E TI HI absorption toward ultracompact HII regions: Distances and Galactic structure SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : disk; Galaxy : structure; HII regions; radio lines : ISM ID II-REGIONS; KINEMATIC DISTANCES; SPIRAL STRUCTURE; STAR-FORMATION; GALAXY; PLANE; RECOMBINATION; LINES; MILKY; DUST AB The Very Large Array was used to observe H I absorption against 20 compact and ultracompact H II (UC H II) regions, thereby resolving the kinematic distance ambiguity to these sources. Combining these results with other sources whose distances were resolved through H I absorption, the half-width at half-maximum of the distribution of source height above and below the Galactic plane is found to be 35 +/- 2 pc within the solar circle. The vertical height distribution is used to investigate the predictive accuracy of the Galactic latitude in resolving the kinematic distance ambiguity to UC H II regions without the need for H I observations. For a large difference between far and near kinematic distances, high accuracy can be achieved by choosing the kinematic distance closer to 1.84\b\(-1) kpc, where b is the Galactic latitude in degrees. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Fish, VL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 30 TC 95 Z9 96 U1 0 U2 1 PU UNIV 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 2003 VL 587 IS 2 BP 701 EP 713 DI 10.1086/368284 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 666CR UT WOS:000182159400022 ER PT J AU Butt, YM Maccarone, TJ Prantzos, N AF Butt, YM Maccarone, TJ Prantzos, N TI Jet-induced nucleosynthesis in misaligned microquasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; ISM : jets and outflows; novae, cataclysmic variables; nuclear reactions, nucleosynthesis, abundances; X-rays : binaries ID X-RAY BINARIES; BLACK-HOLE; RELATIVISTIC JETS; EMISSION-LINE; NEUTRON-CAPTURE; LITHIUM; ANNIHILATION; SPECTRUM; SYSTEMS; NOVA AB The jet axes and the orbital planes of microquasar systems are usually assumed to be approximately perpendicular, even though this is not currently an observational requirement. On the contrary, in one of the few systems where the relative orientations are well constrained, V4641 Sgr, the jet axis is known to lie not more than similar to36degrees from the binary plane. Such a jet, lying close to the binary plane, and traveling at a significant fraction of the speed of light, may periodically impact the secondary star, initiating nuclear reactions on its surface. The integrated yield of such nuclear reactions over the age of the binary system (less the radiative mass loss) will detectably alter the elemental abundances of the companion star. This scenario may explain the anomalously high Li enhancements (roughly similar to20-200 times the Sun's photospheric value) seen in the companions of some black hole/X-ray binary systems. (Such enhancements are puzzling, since Li nuclei are exceedingly fragile, being easily destroyed in the interiors of stars, and Li would be expected to be depleted rather than enhanced there.) Gamma-ray line signatures of the proposed process could include the 2.22 MeV neutron-capture line as well as the 0.478 MeV Li-7* deexcitation line, both of which may be discernible with the INTEGRAL satellite if produced in an optically thin region during a large outburst. For very energetic jets, a relatively narrow neutral pion gamma-decay signature at 67.5 MeV could also be measurable with the GLAST satellite. We argue that about 10%-20% of all microquasar systems ought to be sufficiently misaligned to be undergoing the proposed jet-secondary impacts. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Scuola Int Super Studi Avanzati, Trieste, Italy. Inst Astrophys, F-75014 Paris, France. RP Butt, YM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 16 Z9 16 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 20 PY 2003 VL 587 IS 2 BP 748 EP 753 DI 10.1086/368301 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 666CR UT WOS:000182159400025 ER PT J AU Friedrich, AM Wernicke, BP Niemi, NA Bennett, RA Davis, JL AF Friedrich, AM Wernicke, BP Niemi, NA Bennett, RA Davis, JL TI Comparison of geodetic and geologic data from the Wasatch region, Utah, and implications for the spectral character of Earth deformation at periods of 10 to 10 million years SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Review DE geodetic; geologic; fault slip rate; normal fault; timescale; earthquake cycle ID WESTERN UNITED-STATES; SAN-ANDREAS FAULT; SEISMIC-REFLECTION DATA; GREAT-BASIN PROVINCE; RANGE PROVINCE; SLIP RATES; EXTENSIONAL TECTONICS; STRAIN ACCUMULATION; GPS MEASUREMENTS; ROCKY-MOUNTAINS AB [1] The Wasatch fault and adjacent fault zones provide an opportunity to compare present-day deformation rate estimates obtained from space geodesy with geologic displacement rates over at least four temporal windows, ranging from the last millennium up to 10 Myr. The three easternmost GPS sites of the Basin and Range Geodetic Network (BARGEN) at this latitude define a similar to130-km-wide region spanning three major normal faults extending east-west at a total rate of 2.7 +/- 0.4 mm/yr, with an average regional strain rate estimated to be 21 +/- 4 nstrain/yr, about twice the Basin and Range average. On the Wasatch fault, the vertical component of the geologic displacement rate is 1.7 +/- 0.5 mm/yr since 6 ka, < 0.6 mm/yr since 130 ka, and 0.5 - 0.7 mm/yr since 10 Ma. However, it appears likely that at the longest timescale, rates slowed over time, from 1.0 to 1.4 mm/yr between 10 and 6 Ma to 0.2 to 0.3 mm/yr since 6 Ma. The cumulative vertical displacement record across all three faults also shows time-variable strain release ranging from 2 to 4 mm/yr since 10 ka to < 1 mm/yr averaged over the past 130 kyr. Conventional earthquake recurrence models ("Reid-type'' behavior) would require an accordingly large variation in strain accumulation or loading rate on a 10-kyr timescale, for which there appears to be no obvious geophysical explanation. Alternatively, seismic strain release, given a wide range of plausible constitutive behaviors for frictional sliding, may be clustered on the 10-kyr timescale, resulting in the high Holocene rates, with comparatively low, uniform strain accumulation rates on the 100-kyr timescale ("Wallace-type'' behavior). The latter alternative, combined with observations at the million-year timescale and the likelihood of a significant contribution of postseismic transients, implies maxima of spectral amplitude in the velocity field at periods of similar to10 Myr ( variations in tectonic loading), similar to10 kyr ( clustered strain release), and of 100 years ( postseismic transients). If so, measurements of strain accumulation and strain release may be strongly timescale-dependent for any given fault system. C1 CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. Harvard Univ, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Friedrich, AM (reprint author), Univ Potsdam, Inst Geosci, Karl Liebknechtstr 24,Haus 25, D-14476 Golm, Germany. EM anke@alum.mit.edu; brian@gps.caltech.edu; niemi@crustal.ucsb.edu; rbennett@cfa.harvard.edu; jdavis@cfa.harvard.edu RI Niemi, Nathan/A-9996-2011; Friedrich, Anke/G-2921-2011; Davis, James/D-8766-2013 OI Friedrich, Anke/0000-0002-6938-8563; Davis, James/0000-0003-3057-477X NR 106 TC 127 Z9 128 U1 3 U2 29 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD APR 15 PY 2003 VL 108 IS B4 AR 2199 DI 10.1029/2001JB000682 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 673RW UT WOS:000182594800001 ER PT J AU Schroll, S AF Schroll, S TI Transgressions: The offenses of art. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Schroll, S (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 15 PY 2003 VL 128 IS 7 BP 81 EP 81 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 672MA UT WOS:000182523400034 ER PT J AU Flambaum, VV Shuryak, EV AF Flambaum, VV Shuryak, EV TI Dependence of hadronic properties on quark masses and constraints on their cosmological variation SO PHYSICAL REVIEW D LA English DT Article ID FINE-STRUCTURE CONSTANT; QSO ABSORPTION-LINES; TIME-VARIATION AB We follow our previous paper on the possible cosmological variation of the weak scale (quark masses) and the strong scale, inspired by data on the cosmological variation of the electromagnetic fine structure constant from distant quasar absorption spectra. In this work we identify the strange quark mass m(s) as the most important quantity, and the sigma meson mass as the ingredient of the nuclear forces most sensitive to it. As a result, we claim significantly stronger limits on the ratio of weak/strong scale (W=m(s)/Lambda(QCD)) variation following from our previous discussion on primordial big-bang nucleosynthesis (\deltaW/W\<0.006) and the Oklo natural nuclear reactor [\deltaW/W\<1.2x10(-10); there is also a nonzero solution deltaW/W=(-0.56+/-0.05)x10(-9)]. C1 Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. Harvard Smithsonian Ctr Astrophys, Inst Atom & Mol Theory, Cambridge, MA 02138 USA. SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. RP Flambaum, VV (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. NR 20 TC 54 Z9 54 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD APR 15 PY 2003 VL 67 IS 8 AR 083507 DI 10.1103/PhysRevD.67.083507 PG 7 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 675ZV UT WOS:000182728200021 ER PT J AU Davis, JL Bennett, RA Wernicke, BP AF Davis, JL Bennett, RA Wernicke, BP TI Assessment of GPS velocity accuracy for the Basin and Range Geodetic Network (BARGEN) SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID STRAIN ACCUMULATION; YUCCA MOUNTAIN; DEFORMATION; NEVADA AB [1] We assess the accuracy of horizontal velocity estimates from the Basin and Range Geodetic Network (BARGEN), a continuous GPS network that has been in operation since 1996. To make this quantitative assessment, we use a procedure that we term the "whole-error'' method. In this method, the measure of the velocity errors is the root-mean-square (RMS) residual velocity relative to a simple geophysical model. This method produces a conservative estimate of the uncertainties, since errors in the geophysical models also contribute to the RMS residual. Using estimates from two different BARGEN subnetworks, the Northern Basin and Range and the Yucca Mountain Cluster, we determine velocity uncertainties of 0.1-0.2 mm yr(-1). Since BARGEN covers a significant fraction of area of the proposed Plate Boundary Observatory component of EarthScope, our results indicate a good ability of this project to determine highly accurate long-term horizontal crustal velocities and deformation rates in this region. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM jdavis@cfa.harvard.edu; rbennett@cfa.harvard.edu; brian@gps.caltech.edu RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 16 TC 26 Z9 27 U1 0 U2 1 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 APR 11 PY 2003 VL 30 IS 7 AR 1411 DI 10.1029/2003GL016961 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 669JP UT WOS:000182348400008 ER PT J AU Lucas, SG Holbrook, LT Emry, RJ AF Lucas, SG Holbrook, LT Emry, RJ TI Isectolophus (Mammalia, Perissodactyla) from the Eocene of the Zaysan Basin, Kazakstan and its biochronological significance SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article AB We describe a skull and fragments of lower jaws of a ceratomorph perissodactyl from the Arshantan (Eocene) strata of the Zaysan Basin, eastern Kazakstan, and refer these specimens to Isectolophus latidens (Osborn, Scott, and Speir, 1878). The material from the Zaysan Basin is indistinguishable from the holotypes of Isectolophus bogdulensis Reshetov from Mongolia and Homogalax reliquius Qi from China. These two species are junior subjective synonyms of L latidens. The presence of L latidens, known also from Bridgerian strata of North America, in Asian deposits of Arshantan age provides further support for a correlation between the Arshantan and the Bridgerian land-mammal "ages.". C1 New Mexico Museum Nat Hist, Albuquerque, NM 87104 USA. Rowan Univ, Dept Biol Sci, Glassboro, NJ 08028 USA. Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. RP Lucas, SG (reprint author), New Mexico Museum Nat Hist, 1801 Mt Rd NW, Albuquerque, NM 87104 USA. NR 26 TC 4 Z9 5 U1 2 U2 2 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD APR 11 PY 2003 VL 23 IS 1 BP 238 EP 243 DI 10.1671/0272-4634(2003)23[238:IMPFTE]2.0.CO;2 PG 6 WC Paleontology SC Paleontology GA 666MG UT WOS:000182180600019 ER PT J AU Sanderson, AJR Ponman, TJ Finoguenov, A Lloyd-Davies, EJ Markevitch, M AF Sanderson, AJR Ponman, TJ Finoguenov, A Lloyd-Davies, EJ Markevitch, M TI The Birmingham-CfA cluster scaling project - I. Gas fraction and the M-T-X relation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : general; galaxies : haloes; intergalactic medium; X-rays : galaxies; X-rays : galaxies : clusters ID MASS-TEMPERATURE RELATION; HYDRA-A CLUSTER; GALAXY CLUSTERS; ELLIPTIC GALAXIES; RAY-CLUSTERS; INTRACLUSTER MEDIUM; HOT GAS; INTERGALACTIC MEDIUM; COOLING FLOWS; DARK MATTER AB We have assembled a large sample of virialized systems, comprising 66 galaxy clusters, groups and elliptical galaxies with high-quality X-ray data. To each system we have fitted analytical profiles describing the gas density and temperature variation with radius, corrected for the effects of central gas cooling. We present an analysis of the scaling properties of these systems and focus in this paper on the gas distribution and M-T-X relation. In addition to clusters and groups, our sample includes two early-type galaxies, carefully selected to avoid contamination from group or cluster X-ray emission. We compare the properties of these objects with those of more massive systems and find evidence for a systematic difference between galaxy-sized haloes and groups of a similar temperature. We derive a mean logarithmic slope of the M-T-X relation within R-200 of 1.84 +/- 0.06, although there is some evidence of a gradual steepening in the M-T-X relation, with decreasing mass. We recover a similar slope using two additional methods of calculating the mean temperature. Repeating the analysis with the assumption of isothermality, we find the slope changes only slightly, to 1.89 +/- 0.04, but the normalization is increased by 30 per cent. Correspondingly, the mean gas fraction within R-200 changes from (0.13 +/- 0.01) h(70)(-3/2) to (0.11 +/- 0.01) h(70)(-3/2), for the isothermal case, with the smaller fractional change reflecting different behaviour between hot and cool systems. There is a strong correlation between the gas fraction within 0.3R(200) and temperature. This reflects the strong (5.8sigma) trend between the gas density slope parameter, beta, and temperature, which has been found in previous work. These findings are interpreted as evidence for self-similarity breaking from galaxy feedback processes, active galactic nuclei heating or possibly gas cooling. We discuss the implications of our results in the context of a hierarchical structure formation scenario. C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Sanderson, AJR (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. NR 91 TC 156 Z9 157 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 11 PY 2003 VL 340 IS 3 BP 989 EP 1010 DI 10.1046/j.1365-8711.2003.06401.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 664AN UT WOS:000182039700033 ER PT J AU Handler, G O'Donoghue, D Muller, M Solheim, JE Gonzalez-Perez, JM Johannessen, F Paparo, M Szeidl, B Viraghalmy, G Silvotti, R Vauclair, G Dolez, N Pallier, E Chevreton, M Kurtz, DW Bromage, GE Cunha, MS Ostensen, R Fraga, L Kanaan, A Amorim, A Giovannini, O Kepler, SO da Costa, AFM Anderson, RF Wood, MA Silvestri, N Klumpe, EW Carlton, RF Miller, RH McFarland, JP Grauer, AD Kawaler, SD Riddle, RL Reed, MD Nather, RE Winget, DE Hill, JA Metcalfe, TS Mukadam, AS Kilic, M Watson, TK Kleinman, SJ Nitta, A Guzik, JA Bradley, PA Sekiguchi, K Sullivan, DJ Sullivan, T Shobbrook, RR Jiang, X Birch, PV Ashoka, BN Seetha, S Girish, V Joshi, S Dorokhova, TN Dorokhov, NI Akan, MC Meistas, EG Janulis, R Kalytis, R Alisauskas, D Anguma, SK Kalebwe, PC Moskalik, P Ogloza, W Stachowski, G Pajdosz, G Zola, S AF Handler, G O'Donoghue, D Muller, M Solheim, JE Gonzalez-Perez, JM Johannessen, F Paparo, M Szeidl, B Viraghalmy, G Silvotti, R Vauclair, G Dolez, N Pallier, E Chevreton, M Kurtz, DW Bromage, GE Cunha, MS Ostensen, R Fraga, L Kanaan, A Amorim, A Giovannini, O Kepler, SO da Costa, AFM Anderson, RF Wood, MA Silvestri, N Klumpe, EW Carlton, RF Miller, RH McFarland, JP Grauer, AD Kawaler, SD Riddle, RL Reed, MD Nather, RE Winget, DE Hill, JA Metcalfe, TS Mukadam, AS Kilic, M Watson, TK Kleinman, SJ Nitta, A Guzik, JA Bradley, PA Sekiguchi, K Sullivan, DJ Sullivan, T Shobbrook, RR Jiang, X Birch, PV Ashoka, BN Seetha, S Girish, V Joshi, S Dorokhova, TN Dorokhov, NI Akan, MC Meistas, EG Janulis, R Kalytis, R Alisauskas, D Anguma, SK Kalebwe, PC Moskalik, P Ogloza, W Stachowski, G Pajdosz, G Zola, S TI Amplitude and frequency variability of the pulsating DB white dwarf stars KUV 05134+2605 and PG 1654+160 observed with the Whole Earth Telescope SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : individual : KUV 05134+2605; stars : individual : PG 1654+160; stars : oscillations; stars : variables : other ID XX-PYX; MODES; ASTEROSEISMOLOGY; DISCOVERY AB We have acquired new time series photometry of the two pulsating DB white dwarf stars KUV 05134+2605 and PG 1654+160 with the Whole Earth Telescope. Additional single-site photometry is also presented. We use all these data plus all available archival measurements to study the temporal behaviour of the pulsational amplitudes and frequencies of these stars for the first time. We demonstrate that both KUV 05134+2605 and PG 1654+160 pulsate in many modes, the amplitudes of which are variable in time; some frequency variability of PG 1654+160 is also indicated. Beating of multiple pulsation modes cannot explain our observations; the amplitude variability must therefore be intrinsic. We cannot find stable modes to be used for determinations of the evolutionary period changes of the stars. Some of the modes of PG 1654+160 appear at the same periods whenever detected. The mean spacing of these periods (approximate to40 s) suggests that they are probably caused by non-radial gravity-mode pulsations of spherical degree l = 1. If so, PG 1654+160 has a mass around 0.6 M.. The time-scales of the amplitude variability of both stars (down to two weeks) are consistent with theoretical predictions of resonant mode coupling, a conclusion which might however be affected by the temporal distribution of our data. C1 S African Astron Observ, ZA-7935 Cape Town, South Africa. Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa. Univ Tromso, Inst Matemat Realfag, N-9000 Tromso, Norway. Konkoly Observ Budapest, H-1525 Budapest, Hungary. Osserv Astron Capodimonte, I-80131 Naples, Italy. Observ Midi Pyrenees, CNRS, UMR5572, F-31400 Toulouse, France. Observ Paris, LESIA, F-92195 Meudon, France. Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. Inst Super Maia, P-4470 Castelo Da Maia, Portugal. Isaac Newton Grp Telescopes, Santa Cruz De La Palma 37800, Canary Isl, Spain. Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. Univ Caixas do Sul, Dept Quim & Fis, BR-95001970 Caxias Do Sul, RS, Brazil. Univ Fed Rio Grande do Sul, Inst Fis, BR-15051 Porto Alegre, RS, Brazil. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. Florida Inst Technol, SARA Observ, Melbourne, FL 32901 USA. Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37132 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. SW Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65804 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Southwestern Univ, Informat Technol Serv Dept, Georgetown, TX 78626 USA. Apache Pt Observ, Sloan Digital Sky Survey, Sunspot, NM 88349 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Chinese Acad Sci, Joint Inst Opt Astron, Beijing 100012, Peoples R China. Perth Observ, Bickley, WA 6076, Australia. Indian Space Res Org, Bangalore 560017, Karnataka, India. Uttar Pradesh State Observ, Naini Tal 263129, India. Odessa II Mechnikov State Univ, Astron Observ, UA-270014 Odessa, Ukraine. Ege Univ, Fac Sci, Dept Astron & Space Sci, TR-35100 Izmir, Turkey. Inst Theoret Phys & Astrophys, LT-2600 Vilnius, Lithuania. Vilnius State Univ, Astron Observ, LT-2009 Vilnius, Lithuania. Mbarara Univ Sci & Technol, Dept Phys, Mbarara, Uganda. Univ Zambia, Dept Phys, Lusaka, Zambia. Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Krakow Pedag Univ, Mt Suhora Observ, PL-30084 Krakow, Poland. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. RP Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM handler@astro.univie.ac.at RI Metcalfe, Travis/A-9388-2008; Kepler, S. O. /H-5901-2012; Fraga, Luciano/K-9075-2013; de Amorim, Andre/H-5143-2016; OI Metcalfe, Travis/0000-0003-4034-0416; Silvotti, Roberto/0000-0002-1295-8174; Kepler, S. O. /0000-0002-7470-5703; Cunha, Margarida/0000-0001-8237-7343; Stachowski, Greg/0000-0003-1560-1039; Kawaler, Steven/0000-0002-6536-6367 NR 26 TC 9 Z9 9 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2003 VL 340 IS 3 BP 1031 EP 1038 DI 10.1046/j.1365-8711.2003.06373.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 664AN UT WOS:000182039700036 ER PT J AU Colley, WN Schild, RE Abajas, C Alcalde, D Aslan, Z Bikmaev, I Chavushyan, V Chinarro, L Cournoyer, JP Crowe, R Dudinov, V Evans, AKD Jeon, YB Goicoechea, LJ Golbasi, O Khamitov, I Kjernsmo, K Lee, HJ Lee, J Lee, KW Lee, MG Lopez-Cruz, O Mediavilla, E Moffat, AFJ Mujica, R Ullan, A Munoz, J Oscoz, A Park, MG Purves, N Saanum, O Sakhibullin, N Serra-Ricart, M Sinelnikov, I Stabell, R Stockton, A Teuber, J Thompson, R Woo, HS Zheleznyak, A AF Colley, WN Schild, RE Abajas, C Alcalde, D Aslan, Z Bikmaev, I Chavushyan, V Chinarro, L Cournoyer, JP Crowe, R Dudinov, V Evans, AKD Jeon, YB Goicoechea, LJ Golbasi, O Khamitov, I Kjernsmo, K Lee, HJ Lee, J Lee, KW Lee, MG Lopez-Cruz, O Mediavilla, E Moffat, AFJ Mujica, R Ullan, A Munoz, J Oscoz, A Park, MG Purves, N Saanum, O Sakhibullin, N Serra-Ricart, M Sinelnikov, I Stabell, R Stockton, A Teuber, J Thompson, R Woo, HS Zheleznyak, A TI Around-the-clock observations of the Q0957+561A,B gravitationally lensed quasar. II. Results for the second observing season SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (Q0957+561A,B) ID QSO 0957+561 A,B; TIME-DELAY; MICROLENSING VARIABILITY; LIGHT-CURVE; PARAMETERS AB We report on an observing campaign in 2001 March to monitor the brightness of the later arriving Q0957+ 561B image in order to compare with the previously published brightness observations of the (first-arriving) A image. The 12 participating observatories provided 3543 image frames, which we have analyzed for brightness fluctuations. From our classical methods for time-delay determination, we find a 417.09 +/- 0.07 day time delay, which should be free of effects due to incomplete sampling. During the campaign period, the quasar brightness was relatively constant and only small fluctuations were found; we compare the structure function for the new data with structure function estimates for the 1995-1996 epoch and show that the structure function during our observing interval is unusually depressed. We also examine the data for any evidence of correlated fluctuations at zero lag. We discuss the limits of our ability to measure the cosmological time delay if the quasar's emitting surface is time resolved, as seems likely. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, E-38200 Tenerife, Canary Isl, Spain. Akdeniz Univ, Dept Phys, TR-07058 Antalya, Turkey. Tubitak Natl Observ, TR-07058 Antalya, Turkey. Kazan VI Lenin State Univ, Kazan 420008, Russia. Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Observ Mont Megant, Montreal, PQ, Canada. Univ Hawaii, Hilo, HI 96720 USA. 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. Univ Cantabria, Dept Fis Moderna, E-39005 Santander, Spain. DACOM Corp, Internet Technol Div, Seoul 135610, South Korea. UCL, London WC1E 6BT, England. Univ Guanajuato, Dept Astron, Guanajuato 36000, Mexico. Observ Carnegie Inst Washington, Washington, DC 20005 USA. Kyungpook Natl Univ, Taegu 702701, South Korea. Danish Lib Nat & Med Sci, DK-2200 Copenhagen, Denmark. RP Colley, WN (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. NR 24 TC 22 Z9 22 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2003 VL 587 IS 1 BP 71 EP 79 DI 10.1086/368076 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EA UT WOS:000182105600006 ER PT J AU Winn, JN Rusin, D Kochanek, CS AF Winn, JN Rusin, D Kochanek, CS TI Investigation of the possible third image and mass models of the gravitational lens PMN J1632-0033 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : nuclei; galaxies : structure; gravitational lensing ID FREE-FREE ABSORPTION; DARK-MATTER HALOES; SCALING RELATIONS; GALAXY; CONSTRAINTS; RESOLUTION; PARSEC; MG-1131+0456; PROFILES; CURVES AB We present multifrequency VLBA(2) observations of PMN J1632-0033, one of the few gravitationally lensed quasars suspected of having a central "odd'' image. The central component has a different spectral index than the two bright quasar images. Therefore, either the central component is not a third image, and is instead the active nucleus of the lens galaxy, or else it is a third image whose spectrum is inverted by free-free absorption in the lens galaxy. In either case, we have more constraints on mass models than are usually available for a two-image lens, especially when combined with the observed orientations of the radio jets of the two bright quasars. If there is no third quasar image, the simplest permitted model is a singular isothermal sphere in an external shear field: beta = 2.05(-0.10)(+0.23) (2 sigma), where rho(r) proportional to r(-beta). If the central component is a third image, a hypothesis that can be tested with future high-frequency observations, then the density distribution is only slightly shallower than isothermal: beta = 1.91 +/- 0.02 (2 sigma). We also derive limits on the size of a constant-density core, and the break radius and exponent of an inner density cusp. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 57 TC 31 Z9 31 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 2003 VL 587 IS 1 BP 80 EP 89 DI 10.1086/368150 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EA UT WOS:000182105600007 ER PT J AU Rusin, D Kochanek, CS Falco, EE Keeton, CR McLeod, BA Impey, CD Lehar, J Munoz, JA Peng, CY Rix, HW AF Rusin, D Kochanek, CS Falco, EE Keeton, CR McLeod, BA Impey, CD Lehar, J Munoz, JA Peng, CY Rix, HW TI The evolution of a mass-selected sample of early-type field galaxies SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : elliptical and lenticular, cD; galaxies : evolution; gravitational lensing ID HUBBLE-SPACE-TELESCOPE; COLOR-MAGNITUDE RELATION; GRAVITATIONAL LENS GALAXIES; DIGITAL SKY SURVEY; CLUSTER CL 1358+62; FUNDAMENTAL PLANE; ELLIPTIC GALAXIES; LUMINOSITY FUNCTION; DISTANT CLUSTERS; DARK-MATTER AB We investigate the evolution of mass-selected early-type field galaxies using a sample of 28 gravitational lenses spanning the redshift range 0 less than or similar to z less than or similar to 1. Based on the redshift-dependent intercept of the fundamental plane in the rest-frame B band, we measure an evolution rate of d log (M/L)(B)/dz = -0.56 +/- 0.04 (all errors are 1 sigma unless noted) if we directly compare to the local intercept measured from the Coma Cluster. Refitting the local intercept helps minimize potential systematic errors and yields an evolution rate of d log (M/L)(B)/dz = -0.54 +/- 0.09. An evolution analysis of properly corrected aperture mass-to-light ratios (defined by the lensed image separations) is closely related to the Faber-Jackson relation. In the rest-frame B band, we find an evolution rate of d log(M/L)(B)/dz = -0.41 +/- 0.21, a present-day characteristic magnitude of M*0 = -19.70 + 5 log h +/- 0.29 (assuming a characteristic velocity dispersion of sigma(DM*) = 225 km s(-1)), and a Faber-Jackson slope of gamma(FJ) = 3.29 +/- 0.58. The measured evolution rates favor old stellar populations ( mean formation redshift [z(f)] > 1.8 at 2 sigma confidence for a Salpeter initial mass function and a. at Omega(m) = 0.3 cosmology) among early-type field galaxies and argue against significant episodes of star formation at z < 1. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Inst Astrofis Canarias, E-38200 Tenerife, Spain. Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Rusin, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 110 TC 115 Z9 115 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 APR 10 PY 2003 VL 587 IS 1 BP 143 EP 159 DI 10.1086/346206 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EA UT WOS:000182105600013 ER PT J AU Reid, MJ Menten, KM Genzel, R Ott, T Schodel, R Eckart, A AF Reid, MJ Menten, KM Genzel, R Ott, T Schodel, R Eckart, A TI The position of Sagittarius A*. II. Accurate positions and proper motions of stellar SiO masers near the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy : center; masers; stars : AGB and post-AGB; stars : variables : other ID SUPERMASSIVE BLACK-HOLE; MILKY-WAY; GALAXY; SYSTEM; RADIO; STARS; VLT AB In 1979, Menten and coworkers accurately determined the position of Sgr A* on an infrared image by aligning the infrared image with positions measured for SiO masers, associated with infrared-bright evolved stars, at radio wavelengths. We now report greatly improved radio positions and, for the first time, proper motions of many stellar SiO masers at the Galactic center. These positions and motions, coupled with better infrared imaging, allow a much improved location of Sgr A* on infrared images. With current data, infrared stars can be placed in a reference frame tied to Sgr A*, to an accuracy of approximate to10 mas in position and approximate to1 mas yr(-1) in motion. The position of Sgr A* is, within uncertainties, consistent with stellar accelerations and the measured orbital focus of the star S2. The star S2 was observed within 16 mas (approximate to130 AU in projection) of Sgr A* on 2002 May 2. Finally, we find that the central stellar cluster moves with Sgr A* to within approximate to70 km s(-1). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Schoedel, Rainer/D-4751-2014 OI Schoedel, Rainer/0000-0001-5404-797X NR 21 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 APR 10 PY 2003 VL 587 IS 1 BP 208 EP 220 DI 10.1086/368074 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EA UT WOS:000182105600017 ER PT J AU Li, D Goldsmith, PF Menten, K AF Li, D Goldsmith, PF Menten, K TI Massive quiescent cores in Orion. I. Temperature structure SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : individual (Orion); radio lines : ISM ID GIANT MOLECULAR CLOUDS; STAR-FORMATION; DENSE CORES; INTERSTELLAR AMMONIA; DARK CLOUDS; AMBIPOLAR DIFFUSION; CARBON-MONOXIDE; PROPER MOTIONS; MULTITRANSITION; THERMOMETER AB We have mapped four massive cores in Orion using the NH3 (J, K) = (1, 1) and (J, K) = (2, 2) inversion transitions as part of our effort to study the pre-protostellar phase of massive star formation. These cores were selected to be quiescent; i.e., they contain no apparent IR sources and are not associated with any molecular outflows. These cores are 1 order of magnitude more massive than dark cloud cores and have about twice the line width. This paper focuses on their temperature structure. We find a statistically significant correlation between the gas kinetic temperature and the gas column density. The general trend is for the gas to be colder where the column density is higher, which we interpret to mean that the interiors of these cores are colder than the regions surrounding them. This is in contrast with dark cloud cores, which exhibit relatively. at temperature profiles. The temperature gradient within the massive quiescent Orion cores is consistent with an external radiation source heating the dust and dust-gas collisions providing relatively close coupling between dust and gas temperatures. Thus, we suggest that the initial stage of massive pre-protostellar cloud cores is relatively quiescent condensations that are cooler than their surroundings. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Cornell Univ, Dept Astron, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Li, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Goldsmith, Paul/H-3159-2016 NR 51 TC 34 Z9 35 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 2003 VL 587 IS 1 BP 262 EP 277 DI 10.1086/368078 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EA UT WOS:000182105600022 ER PT J AU Ransom, RR Bartel, N Bietenholz, MF Ratner, MI Lebach, DE Shapiro, II Lestrade, JF AF Ransom, RR Bartel, N Bietenholz, MF Ratner, MI Lebach, DE Shapiro, II Lestrade, JF TI Very long baseline interferometry imaging of the RS Canum Venaticorum binary star system HR 5110 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; radio continuum : stars; stars : activity; stars : imaging; stars : individual (BH Canum Venaticorum); techniques : interferometric ID RADIO-EMISSION; MICROWAVE OBSERVATIONS; CLOSE BINARY; HR-5110; ALGOL; POLARIZATION; ASTROMETRY; HR-1099; REGION; GHZ AB We present VLBI images of the RS CVn binary star HR 5110 (= BH CVn; HD 118216), obtained from observations made at 8.4 GHz on 1994 May 29/30 in support of the NASA/Stanford Gravity Probe B project. Our images show an emission region with a core-halo morphology. The core was 0.39 +/- 0.09 mas (FWHM) in size, or 66% +/- 20% of the 0.6 +/- 0.1 mas diameter of the chromospherically active K subgiant star in the binary system. The halo was 1.95 +/- 0.22 mas (FWHM) in size, or 1.8 +/- 0.2 times the 1.1 +/- 0.1 mas separation of the centers of the K and F stars. (The uncertainties given for the diameter of the K star and its separation from the F star each reflect the level of agreement of the two most recent published determinations.) The core increased significantly in brightness over the course of the observations and seems to have been the site of. are activity that generated an increase in the total flux density of similar to200% in 12 hr. The fractional circular polarization simultaneously decreased from similar to10% to 2.5%. C1 York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, Dept Millimetr Radio Astron, F-75014 Paris, France. RP Ransom, RR (reprint author), York Univ, Dept Phys & Astron, 4700 Keele St, Toronto, ON M3J 1P3, Canada. NR 28 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2003 VL 587 IS 1 BP 390 EP 397 DI 10.1086/368070 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EA UT WOS:000182105600032 ER PT J AU Nisenson, P van Ballegooijen, AA de Wijn, AG Sutterlin, P AF Nisenson, P van Ballegooijen, AA de Wijn, AG Sutterlin, P TI Motions of isolated G-band bright points in the solar photosphere SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : atmospheric motions; Sun : faculae, plages; Sun : magnetic fields; techniques : high angular resolution ID MAGNETIC-FLUX TUBES; QUIET PHOTOSPHERE; FACULAR POINTS; NETWORK; SUN; GRANULATION; RESOLUTION; FIELDS; SIMULATIONS; DYNAMICS AB Magnetic elements on the quiet Sun are buffeted by convective flows that cause lateral motions on time-scales of minutes. The magnetic elements can be observed as bright points (BPs) in the G band at 4305 Angstrom. We present observations of BPs based on a long sequence of G-band images recorded with the Dutch Open Telescope and postprocessed using speckle-masking techniques. From these images we measured the proper motions of isolated BPs and derived the autocorrelation function of their velocity relative to the solar granulation pattern. The accuracy of BP position measurements is estimated to be less than 23 km on the Sun. The rms velocity of BPs (corrected for measurement errors) is about 0.89 km s(-1), and the correlation time of BP motions is about 60 s. This rms velocity is about 3 times the velocity measured using cork tracking, almost certainly due to the fact that isolated BPs move more rapidly than clusters of BPs. We also searched for evidence of vorticity in the motions of G-band BPs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Sterrekundig Inst, NL-3508 TA Utrecht, Netherlands. RP Nisenson, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 15, Cambridge, MA 02138 USA. EM pnisenson@cfa.harvard.edu; vanballe@cfa.harvard.edu; a.g.dewijn@astro.uu.nl; p.suetterlin@astro.uu.nl OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 36 TC 48 Z9 51 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 APR 10 PY 2003 VL 587 IS 1 BP 458 EP 463 DI 10.1086/368067 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EA UT WOS:000182105600039 ER PT J AU Metcalfe, TS AF Metcalfe, TS TI White dwarf asteroseismology and the C-12(alpha, gamma) O-16 rate SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : numerical; nuclear reactions, nucleosynthesis, abundances stars : individual (CBS 114, GD 358); stars : interiors; stars : oscillations; white dwarfs ID WHOLE EARTH TELESCOPE; GD-358; STARS; C-12(ALPHA,GAMMA)O-16 AB Due to a new global analysis method, it is now possible to measure the internal composition of pulsating white dwarf stars, even with relatively simple theoretical models. The precise internal mixture of carbon and oxygen is the largest single source of uncertainty in ages derived from white dwarf cosmochronometry, and it contains information about the rate of the astrophysically important, but experimentally uncertain, C-12(alpha, gamma)O-16 nuclear reaction. Recent determinations of the internal composition and structure of two helium-atmosphere variable (DBV) white dwarf stars, GD 358 and CBS 114, initially led to conflicting implied rates for the C-12(alpha, gamma)O-16 reaction. If both stars were formed through single-star evolution, then the initial analyses of their pulsation frequencies must have differed in some systematic way. I present improved fits to the two sets of pulsation data, resolving the tension between the initial results and leading to a value for the C-12(alpha, gamma)O-16 reaction rate that is consistent with recent laboratory measurements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Metcalfe, TS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Metcalfe, Travis/A-9388-2008 OI Metcalfe, Travis/0000-0003-4034-0416 NR 19 TC 40 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 10 PY 2003 VL 587 IS 1 BP L43 EP L46 DI 10.1086/375044 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EB UT WOS:000182105700011 ER PT J AU Risaliti, G Elvis, M Gilli, R Salvati, M AF Risaliti, G Elvis, M Gilli, R Salvati, M TI A Chandra minisurvey of X-ray-weak quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; X-rays : diffuse background ID BLACK-HOLES; PERFORMANCE; POPULATION; OBJECTS; SAMPLE; 2MASS AB We present Chandra observations of 18 spectroscopically selected quasars, which are already known to be X-ray weak from previous ROSAT observations. All the sources but one are detected by Chandra, and spectral analysis suggests that most of them are intrinsically underluminous in the X-rays (by a factor from 3 to >100). These objects could represent a large population of quasars with a spectral energy distribution different from that of standard blue quasars. We discuss the possibility that a significant fraction of the obscured active galactic nuclei needed in synthesis models of the X-ray background could instead be optical, broad-line, X-ray-weak quasars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM grisaliti@cfa.harvard.edu RI Gilli, Roberto/P-1110-2015; OI Gilli, Roberto/0000-0001-8121-6177; Risaliti, Guido/0000-0002-3556-977X NR 24 TC 17 Z9 17 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 APR 10 PY 2003 VL 587 IS 1 BP L9 EP L13 DI 10.1086/375048 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665EB UT WOS:000182105700003 ER PT J AU Hall, JPW Callaghan, CJ AF Hall, JPW Callaghan, CJ TI A revision of the new riodinid butterfly genus Pseudotinea (Lepidoptera : Riodinidae) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE biogeography; Calydna; conservation; morphology AB A revision of the new South American riodinid genus Pseudotinea is presented that includes taxonomic and ecological notes, distributional data and illustrations of adults and genital structures for all species. The systematic position of Pseudotinea within the Riodinidae, its ecology and biogeography are discussed. Five species are recognized: volcanicus Callaghan and Salazar, hemis Schaus and caprina Hewitson are transferred from Calydna (comb. n.) and two new species, P. eiselei and P. gagarini, are described here. The genus is confined to the Andes and south-east Brazil where all species are very rare and many endangered. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. EM jpwhall@hotmail.com NR 48 TC 6 Z9 8 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD APR 10 PY 2003 VL 37 IS 7 BP 821 EP 837 DI 10.1080/00222930110096771 PG 17 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 674WH UT WOS:000182659800003 ER PT J AU Sioris, CE Haley, CS McLinden, CA von Savigny, C McDade, IC McConnell, JC Evans, WFJ Lloyd, ND Llewellyn, EJ Chance, KV Kurosu, TP Murtagh, D Frisk, U Pfeilsticker, K Bosch, H Weidner, F Strong, K Stegman, J Megie, G AF Sioris, CE Haley, CS McLinden, CA von Savigny, C McDade, IC McConnell, JC Evans, WFJ Lloyd, ND Llewellyn, EJ Chance, KV Kurosu, TP Murtagh, D Frisk, U Pfeilsticker, K Bosch, H Weidner, F Strong, K Stegman, J Megie, G TI Stratospheric profiles of nitrogen dioxide observed by Optical Spectrograph and Infrared Imager System on the Odin satellite SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE optical; Sun-synchronous; polar-orbiting; Fraunhofer; Ring effect; iterative onion peel ID OZONE MONITORING EXPERIMENT; LIMB SCATTER MEASUREMENTS; ABSORPTION SPECTROSCOPY; RADIATIVE-TRANSFER; MIDDLE ATMOSPHERE; O-3 PROFILES; TRACE-GAS; MODEL; RETRIEVAL; MISSION AB [1] Vertical profiles of nitrogen dioxide in the 19-40 km altitude range are successfully retrieved over the globe from Optical Spectrograph and Infrared Imager System (OSIRIS) limb scatter observations in late 2001 and early 2002. The inclusion of multiple scattering in the radiative transfer model used in the inversion algorithm allows for the retrieval of NO2 down to 19 km. The slant column densities, which represent the observations in the inversion, are obtained by fitting the fine structure in normalized radiance spectra over the 435-449 nm range, where NO2 electronic absorption is readily observable because of long light paths through stratospheric layers rich in this constituent. Details of the spectral fitting and inversion algorithm are discussed, including the discovery of a pseudo-absorber associated with pixelated detectors and a new method to verify altitude registration. Comparisons are made with spatially and temporally coincident profile measurements of this photochemically active trace gas. Better than 20% agreement is obtained with all correlative measurements over the common retrieval altitude range, confirming the validity of OSIRIS NO2 profiles. Systematic biases in the number densities are not observed at any altitude. A "snapshot'' meridional cross section between 40degreesN and 70degreesS is shown from observations during a fraction of an orbit. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Heidelberg, Inst Environm Phys, D-69120 Heidelberg, Germany. Trent Univ, Dept Phys, Peterborough, ON K9J 7B8, Canada. Swedish Space Corp, SE-17104 Solna, Sweden. York Univ, Ctr Earth & Space Sci, Toronto, ON M3J 2R7, Canada. Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK S7N 5E2, Canada. Environm Canada, Meteorol Serv Canada, Toronto, ON, Canada. Univ Paris 06, IPSL, CNRS, Serv Aeron, F-75252 Paris 05, France. Chalmers Univ, Dept Radio & Space Sci, SE-41296 Gothenburg, Sweden. Stockholm Univ, Dept Meteorol, SE-10691 Stockholm, Sweden. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. RP Sioris, CE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM csioris@cfa.harvard.edu; chris.mclinden@ec.gc.ca; csavigny@iup.physik.uni-bremen.de; mcdade@yorku.ca; jack@nimbus.yorku.ca; wevans@trentu.ca; llewellyn@skisas.usask.ca; kchance@cfa.harvard.edu; tkurosu@cfa.harvard.edu; donal@rss.chalmers.se; pf@iup.uni-heidelberg.de; strong@atmosp.physics.utoronto.ca; jacek@misu.su.se RI McLinden, Chris/A-7710-2010; The Odin satellite, aeronomy mission/F-1671-2011; Strong, Kimberly/D-2563-2012; von Savigny, Christian/B-3910-2014; Boesch, Hartmut/G-6021-2012; Murtagh, Donal/F-8694-2011 OI McLinden, Chris/0000-0001-5054-1380; Murtagh, Donal/0000-0003-1539-3559 NR 52 TC 43 Z9 44 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 9 PY 2003 VL 108 IS D7 AR 4215 DI 10.1029/2002JD002672 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 669KB UT WOS:000182349500002 ER PT J AU Puyravaud, JP AF Puyravaud, JP TI Standardizing the calculation of the annual rate of deforestation SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE annual rate of deforestation; compound interest law; exponential decay model ID WESTERN GHATS; CONSERVATION AB Different authors utilize different formulae to calculate the annual rate of change of forest cover (or its opposite, the annual rate of deforestation) and use different terms to describe it. This generates confusion. I suggest that the annual rate of change of forest cover should be calculated as: r = (1/(t(2) - t(1))) x ln(A(2)/A(1)). This formula is derived from the Compound Interest Law. It is also derived from the mean annual rate of change and for this reason, is more intuitive than the formula used by FAO [q = ((A(2)/A(1))(1/(t2-t1))) - 1]. The rate r is always higher than q, but in most cases, the difference between the two quantities is lower than the sampling error. The rate r is significantly higher than q only when deforestation is extremely high. To ease comparisons between sites of annual rates of forest change, the forest area, time of measurements and formulae used should be clearly indicated. (C) 2002 Elsevier Science B.V All rights reserved. C1 ECOS 50, Pondicherry 605001, India. RP Puyravaud, JP (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. NR 14 TC 164 Z9 175 U1 4 U2 27 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD APR 7 PY 2003 VL 177 IS 1-3 BP 593 EP 596 AR PII S0378-1127(02)00335-3 DI 10.1016/S0378-1127(02)00335-3 PG 4 WC Forestry SC Forestry GA 664BL UT WOS:000182041800044 ER PT J AU Schultz, TR AF Schultz, TR TI Pheidole in the New World - A dominant, hyperdiverse ant genus SO SCIENCE LA English DT Book Review C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. RP Schultz, TR (reprint author), Smithsonian Inst, Dept Systemat Biol, POB 37012,NHB,CE516,MRC 188, Washington, DC 20013 USA. EM schultz@lab.si.edu NR 1 TC 0 Z9 0 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 APR 4 PY 2003 VL 300 IS 5616 BP 57 EP 58 DI 10.1126/science.1084090 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 663CP UT WOS:000181988900022 ER PT J AU Wilf, P Cuneo, NR Johnson, KR Hicks, JF Wing, SL Obradovich, JD AF Wilf, P Cuneo, NR Johnson, KR Hicks, JF Wing, SL Obradovich, JD TI High plant diversity in Eocene South America: Evidence from Patagonia SO SCIENCE LA English DT Article ID AMAZONIAN SPECIATION; CLIMATE-CHANGE; RAIN-FOREST; VEGETATION; HISTORY; HYPOTHESIS; TAPHONOMY; EVOLUTION; TERTIARY; COLORADO AB Tropical South America has the highest plant diversity of any region today, but this richness is usually characterized as a geologically recent development (Neogene or Pleistocene). From caldera-lake beds exposed at Laguna del Hunco in Patagonia, Argentina, paleolatitude similar to47degreesS, we report 102 leaf species. Radioisotopic and paleomagnetic analyses indicate that the. ora was deposited 52 million years ago, the time of the early Eocene climatic optimum, when tropical plant taxa and warm, equable climates reached middle latitudes of both hemispheres. Adjusted for sample size, observed richness exceeds that of any other Eocene leaf. ora, supporting an ancient history of high plant diversity in warm areas of South America. C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. Museo Paleontol Egidio Feruglio, RA-9100 Trelew, Chubut, Argentina. Denver Museum Nat & Sci, Dept Earth Sci, Denver, CO 80205 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. US Geol Survey, Lakewood, CO 80225 USA. RP Wilf, P (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM pwilf@geosc.psu.edu OI Wing, Scott/0000-0002-2954-8905 NR 68 TC 148 Z9 157 U1 2 U2 16 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD APR 4 PY 2003 VL 300 IS 5616 BP 122 EP 125 DI 10.1126/science.1080475 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 663CP UT WOS:000181988900046 PM 12677065 ER PT J AU Wood, JA AF Wood, JA TI Planetary science - Of asteroids and onions SO NATURE LA English DT Editorial Material ID PARENT BODIES C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wood, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jwood@cfa.harvard.edu NR 10 TC 8 Z9 8 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 3 PY 2003 VL 422 IS 6931 BP 479 EP 481 DI 10.1038/422479a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 662TW UT WOS:000181965400023 PM 12673234 ER PT J AU Muench, AA Lada, EA Lada, CJ Elston, RJ Alves, JF Horrobin, M Huard, TH Levine, JL Raines, SN Roman-Zuniga, C AF Muench, AA Lada, EA Lada, CJ Elston, RJ Alves, JF Horrobin, M Huard, TH Levine, JL Raines, SN Roman-Zuniga, C TI A study of the luminosity and mass functions of the young IC 348 cluster using FLAMINGOS wide-field near-infrared images SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared radiation; open clusters and associations : individual (IC 348); stars : formation; stars : luminosity function, mass function; stars : low-mass, brown dwarfs ID ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; T-TAURI STARS; BROWN DWARFS; MOLECULAR CLOUD; EVOLUTIONARY MODELS; DUST EXTINCTION; IC-348; ASSOCIATIONS; VARIABILITY AB We present wide-field near-infrared (JHK) images of the young, tau = 2 Myr IC 348 cluster taken with FLAMINGOS. We use these new data to construct an infrared census of sources, which is sensitive enough to detect a 10 M-Jup brown dwarf seen through an extinction of A(V)similar to7. We examine the cluster's structure and relationship to the molecular cloud and to construct the cluster's K-band luminosity function. Using our model luminosity function algorithm, we derive the cluster's initial mass function ( IMF) throughout the stellar and substellar regimes and find that the IC 348 IMF is very similar to that found for the Trapezium cluster, with both cluster IMFs having a mode between 0.2-0.08 M-.. In particular, we find that, similar to our results for the Trapezium, brown dwarfs constitute only one in four of the sources in the IC 348 cluster. We show that a modest secondary peak forms in the substellar IC 348 K-band luminosity function (KLF), corresponding to the same mass range responsible for a similar KLF peak found in the Trapezium. We interpret this KLF peak as either evidence for a corresponding secondary IMF peak at the deuterium burning limit or as arising from a feature in the substellar mass-luminosity relation that is not predicted by current theoretical models. Finally, we find that IC 348 displays radial variations of its subsolar (0.5-0.08 M-.) IMF on a parsec scale. Whatever mechanism that is breaking the universality of the IMF on small spatial scales in IC 348 does not appear to be acting on the brown dwarf population, whose relative size does not vary with distance from the cluster center. C1 Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-8574 Garching, Germany. RP Muench, AA (reprint author), CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. RI Roman-Zuniga, Carlos/F-6602-2016; OI Roman-Zuniga, Carlos/0000-0001-8600-4798; Muench, August/0000-0003-0666-6367; Alves, Joao/0000-0002-4355-0921 NR 59 TC 103 Z9 103 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2003 VL 125 IS 4 BP 2029 EP 2049 DI 10.1086/373925 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GK UT WOS:000181713100027 ER PT J AU Walter, FM Beck, TL Morse, JA Wolk, SJ AF Walter, FM Beck, TL Morse, JA Wolk, SJ TI Deconstructing HD 28867 SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (Taurus-Auriga); stars : individual (HD 28867) ID X-RAY-EMISSION; T-TAURI STARS; LATE B-TYPE; OPEN CLUSTER; EINSTEIN OBSERVATIONS; ORION NEBULA; ROSAT SURVEY; AURIGA; PLEIADES; CATALOG AB The 3" pair of B9 stars HD 28867 is one of the brightest X-ray sources in the Taurus-Auriga star-forming region. In this multiwavelength study, we attempt to deduce the source of the X-ray emission. We show that the east component is the X-ray source. The east component has a near-IR excess and displays narrow absorption lines in the optical, both of which are consistent with a cool stellar companion. This companion is one of the brightest low-mass pre-main-sequence stars in Tau-Aur; at 2 mum, it and the B9 star are equally bright. We see evidence of radial velocity variability in the cool component of over 34 km s(-1). It is not visible in K-band speckle imaging, which constrains the companion to lie within 14 AU of the B star. We also report on a possible fourth member of the group, an M1 star 18" south of HD 28867. C1 SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. Gemini Observ, Hilo, HI 96720 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Walter, FM (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. EM fwalter@astro.sunysb.edu; tbeck@gemini.edu; morsey@casa.colorado.edu; swolk@cfa.harvard.edu OI Wolk, Scott/0000-0002-0826-9261 NR 53 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2003 VL 125 IS 4 BP 2123 EP 2133 DI 10.1086/368245 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GK UT WOS:000181713100033 ER PT J AU Haas, M Klaas, U Muller, SAH Bertoldi, F Camenzind, M Chini, R Krause, O Lemke, D Meisenheimer, K Richards, PJ Wilkes, BJ AF Haas, M Klaas, U Muller, SAH Bertoldi, F Camenzind, M Chini, R Krause, O Lemke, D Meisenheimer, K Richards, PJ Wilkes, BJ TI The ISO view of Palomar-Green quasars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : fundamental parameters; galaxies : photometry; galaxies : quasars : general; infrared : galaxies ID ACTIVE GALACTIC NUCLEI; HYPERLUMINOUS INFRARED GALAXIES; CONTINUUM ENERGY-DISTRIBUTIONS; HIGH-REDSHIFT QUASARS; RADIO-QUIET QUASARS; OBSCURING DUST TORI; SKY SURVEY; EMISSION; ULTRAVIOLET; PHOTOMETRY AB Mining the ISO data archive we provide the complete ISO view of PG quasars containing 64 infrared spectral energy distributions between 5 and 200 mum. About half of the sample was supplemented by MAMBO and SCUBA (sub-) millimetre data. Since the PG quasars were selected optically, the high infrared detection rate of more than 80% suggests that every quasar possesses luminous to hyperluminous dust emission with dust masses comparable to Seyferts and ultraluminous IR galaxies (ULIRGs). The gas-to-dust mass ratio (of those sources where CO measurements are available in the literature) is consistent with the galactic value providing further evidence for the thermal nature of the IR emission of radio quiet quasars. The SEDs represent templates of unprecedented detail and sensitivity. The power-law like near- to mid-IR SEDs (F-v proportional to v(alpha)) are smooth up to far-infrared wavelengths, favouring dust heating by the central AGN, and we conclude that, in particular for our hyperluminous quasars at z=1, starbursts play only a minor role for powering the dust emission, even in the FIR. The IR spectral slopes alpha(1-10) mum range from -0.9 to -2.2 with a mean of -1.3+/-0.3. They neither correlate with the optical spectral slope alpha(0.3-1) mum, nor with the IR luminosity, nor with the FIR/MIR luminosity ratio, nor with inclination-dependent extinction effects in the picture of a dusty torus. We suggest that the diversity of the SEDs reflects largely the evolution of the dust distribution, and we propose a classification of the SED shapes as well as an evolutionary scheme in which this variety can be understood. During the evolution the surrounding dust redistributes, settling more and more into a torus/disk like configuration, while the SEDs show an initial FIR bump, then an increasing MIR emission and a steeper near- to mid-infrared slope, both of which finally also decrease. Strikingly, based on the sensitive ISO data now we do not only see the coarse IR differences between ULIRGs and quasars, but also the details and a possible evolution of the dust distribution and emission even among the optically selected PG sample. Regarding cosmic evolution, our hyperluminous quasars in the "local" universe at z=1 do not show the hyperluminous (L(FIR)greater than or similar to10(13) L-circle dot) starburst activity inferred for z=4 quasars detected in several (sub-) millimetre surveys. In view of several caveats this difference should be established further, but it already suggests that in the early dense universe stronger merger events led to more powerful starbursts accompanying the quasar phenomenon, while at later cosmic epochs any coeval starbursts obviously do not reach that high power and are outshone by the AGN. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Landessternwarte Heidelberg, D-69117 Heidelberg, Germany. Rutherford Appleton Lab, CLRC, Didcot OX11 0QX, Oxon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Haas, M (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. OI Wilkes, Belinda/0000-0003-1809-2364 NR 86 TC 144 Z9 144 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 APR PY 2003 VL 402 IS 1 BP 87 EP 111 DI 10.1051/0004-6361:20030110 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665NU UT WOS:000182128200012 ER PT J AU Kepler, SO Nather, RE Winget, DE Nitta, A Kleinman, SJ Metcalfe, T Sekiguchi, K Jiang, XJ Sullivan, D Sullivan, T Janulis, R Meistas, E Kalytis, R Krzesinski, J Ogloza, W Zola, S O'Donoghue, D Romero-Colmenero, E Martinez, P Dreizler, S Deetjen, J Nagel, T Schuh, SL Vauclair, G Ning, FJ Chevreton, M Solheim, JE Perez, JMG Johannessen, F Kanaan, A Costa, JE Costa, AFM Wood, MA Silvestri, N Ahrens, TJ Jones, AK Collins, AE Boyer, M Shaw, JS Mukadam, A Klumpe, EW Larrison, J Kawaler, S Riddle, R Ulla, A Bradley, P AF Kepler, SO Nather, RE Winget, DE Nitta, A Kleinman, SJ Metcalfe, T Sekiguchi, K Jiang, XJ Sullivan, D Sullivan, T Janulis, R Meistas, E Kalytis, R Krzesinski, J Ogloza, W Zola, S O'Donoghue, D Romero-Colmenero, E Martinez, P Dreizler, S Deetjen, J Nagel, T Schuh, SL Vauclair, G Ning, FJ Chevreton, M Solheim, JE Perez, JMG Johannessen, F Kanaan, A Costa, JE Costa, AFM Wood, MA Silvestri, N Ahrens, TJ Jones, AK Collins, AE Boyer, M Shaw, JS Mukadam, A Klumpe, EW Larrison, J Kawaler, S Riddle, R Ulla, A Bradley, P TI The everchanging pulsating white dwarf GD358 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : white dwarfs; stars : variables : general; stars : oscillations; stars : individual : GD 358; stars : evolution ID ZZ-CETI STARS; WHOLE EARTH TELESCOPE; GRAVITY MODES; TURBULENT CONVECTION; GD-358; SPECTRA; PERIOD; G29-38; ASTEROSEISMOLOGY; INSTABILITY AB We report 323 hours of nearly uninterrupted time series photometric observations of the DBV star GD 358 acquired with the Whole Earth Telescope ( WET) during May 23rd to June 8th, 2000. We acquired more than 232 000 independent measurements. We also report on 48 hours of time-series photometric observations in Aug 1996. We detected the non-radial g-modes consistent with degree l = 1 and radial order 8 to 20 and their linear combinations up to 6th order. We also detect, for the first time, a high amplitude l = 2 mode, with a period of 796 s. In the 2000 WET data, the largest amplitude modes are similar to those detected with the WET observations of 1990 and 1994, but the highest combination order previously detected was 4th order. At one point during the 1996 observations, most of the pulsation energy was transferred into the radial order k = 8 mode, which displayed a sinusoidal pulse shape in spite of the large amplitude. The multiplet structure of the individual modes changes from year to year, and during the 2000 observations only the k = 9 mode displays clear normal triplet structure. Even though the pulsation amplitudes change on timescales of days and years, the eigenfrequencies remain essentially the same, showing the stellar structure is not changing on any dynamical timescale. C1 UFRGS, Inst Fis, Porto Alegre, RS, Brazil. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Apache Pt Observ, Sloan Digital Sky Survey, Sunspot, NM 88349 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Beijing Astron Observ, Beijing 100080, Peoples R China. Victoria Univ Wellington, Wellington, New Zealand. Inst Theoret Phys & Astron, LT-2600 Vilnius, Lithuania. Cracow Pedag Univ, Mt Suhora Observ, PL-30084 Krakow, Poland. Jagiellonian Univ, Krakow, Poland. S African Astron Observ, ZA-7935 Cape Town, South Africa. Univ Tubingen, D-72074 Tubingen, Germany. Univ Toulouse 3, Observ Midi Pyrenees, CNRS, UMR5572, F-31400 Toulouse, France. Observ Paris, DAEC, F-92195 Meudon, France. Inst Fys, N-9037 Tromso, Norway. Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. Florida Inst Technol, SARA Observ, Melbourne, FL 32901 USA. Univ Florida, Nucl Sci Ctr 202, Gainesville, FL 32611 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37132 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Vigo, Dept Fis Aplicada, Fac Ciencias, Vigo 36200, Pontevedra, Spain. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Kepler, SO (reprint author), UFRGS, Inst Fis, Porto Alegre, RS, Brazil. EM kepler@if.ufrgs.br; travis@whitedwarf.org; kaz@subaru.naoj.org; jiang@astro.as.utexas.edu; zola@ao.uj.edu.pl; chevreton@obspm.fr; kanaan@fsc.ufsc.br; ulla@uvigo.es RI Metcalfe, Travis/A-9388-2008; Kepler, S. O. /H-5901-2012; Ulla Miguel, Ana Maria/M-2860-2014; OI Metcalfe, Travis/0000-0003-4034-0416; Kepler, S. O. /0000-0002-7470-5703; Kawaler, Steven/0000-0002-6536-6367 NR 45 TC 48 Z9 48 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2003 VL 401 IS 2 BP 639 EP 654 DI 10.1051/0004-6361:20030105 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658EN UT WOS:000181708800026 ER PT J AU Risaliti, G Woltjer, L Salvati, M AF Risaliti, G Woltjer, L Salvati, M TI The nature of the absorbing torus in compact radio galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; X-rays : galaxies ID PARSEC-SCALE JETS; OBSCURING TORUS; SPECTRUM; OBSCURATION; ABSORPTION; NUCLEUS; HYDRA; ASCA; GAS AB We present BeppoSAX observations of the two radio galaxies PKS 1934-63 and S5 1946 + 708. Strong Iron Kalpha lines are detected in both objects indicating that the two sources are absorbed by column densities higher than 1024 cm(-2). Combining radio continuum, HI absorption and X-ray data we can constrain the physical state and the dimensions of the absorber. We find that the putative obscuring torus is molecular and located at a distance higher than 20 pc from the center in S5 1946 + 70. In PKS 1934-63 no radio nucleus has been observed. If this is due to free-free absorption a radius of only a few pc is inferred. Since the Kalpha lines have been detected only at 90% confidence, we also discuss the implications if they would be not as strong as found from our data. From our results it appears that the combination of hard X-ray data and spatially resolved HI absorption measurements provides a powerful diagnostic for conditions in the absorbing "torus". C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Haute Provence, CNRS, F-04870 St Michel, France. 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 20 TC 7 Z9 7 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2003 VL 401 IS 3 BP 895 EP 901 DI 10.1051/0004-6361:20030124 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 662DA UT WOS:000181929900009 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, JSB Loeb, A TI Reionization of hydrogen and helium by early stars and quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; early universe; intergalactic medium; stars : formation ID MICROWAVE BACKGROUND ANISOTROPIES; DIGITAL SKY SURVEY; INTERGALACTIC MEDIUM; LUMINOSITY FUNCTION; IONIZING-RADIATION; GALAXY FORMATION; HE 2347-4342; UNIVERSE; Z-SIMILAR-TO-6; FRAGMENTATION AB We compute the reionization histories of hydrogen and helium caused by the ionizing radiation fields produced by stars and quasars. For the quasars we use a model based on halo-merger rates that reproduces all known properties of the quasar luminosity function at high redshifts. The less constrained properties of the ionizing radiation produced by stars are modeled with two free parameters: ( i) a transition redshift, z(tran), above which the stellar population is dominated by massive, zero-metallicity stars and below which it is dominated by a Scalo mass function; and (ii) the product of the escape fraction of stellar ionizing photons from their host galaxies and the star formation efficiency, f(esc) f*. We constrain the allowed range of these free parameters at high redshifts on the basis of the lack of the H I Gunn-Peterson trough at z less than or similar to 6 and the upper limit on the total intergalactic optical depth for electron scattering, tau(es) < 0.18, from recent cosmic microwave background (CMB) experiments. We find that quasars ionize helium by a redshift z similar to 4, but cannot reionize hydrogen by themselves before z similar to 6. A major fraction of the allowed combinations of f(esc) f* and z(tran) leads to an early peak in the ionized fraction because of the presence of metal-free stars at high redshifts. This sometimes results in two reionization epochs, namely, an early H ii or He III overlap phase followed by recombination and a second overlap phase. Even if early overlap is not achieved, the peak in the visibility function for scattering of the CMB often coincides with the early ionization phase rather than with the actual reionization epoch. Consequently, tau(es) does not correspond directly to the reionization redshift. We generically find values of tau(es) greater than or similar to 7%, which should be detectable by the MAP satellite. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Adv Study, Princeton, NJ 08540 USA. RP Wyithe, JSB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM swyithe@cfa.harvard.edu; loeb@sns.ias.edu OI Wyithe, Stuart/0000-0001-7956-9758 NR 53 TC 182 Z9 183 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 APR 1 PY 2003 VL 586 IS 2 BP 693 EP 708 DI 10.1086/367721 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500001 ER PT J AU Kim, DW Fabbiano, G AF Kim, DW Fabbiano, G TI Chandra X-ray observations of NGC 1316 (Fornax A) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : individual (NGC 1316, NGC 1317) galaxies : ISM; X-rays : galaxies ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; ROSAT PSPC OBSERVATIONS; ELLIPTIC GALAXIES; MULTIPARAMETRIC ANALYSIS; EMISSION MECHANISMS; INTERSTELLAR-MEDIUM; SPECTRAL PROPERTIES; METAL ABUNDANCES; EINSTEIN SAMPLE AB We report the results of the Chandra ACIS subarcsecond resolution X-ray observation of the archetypal merger radio galaxy NGC 1316 (Fornax A). We confirm the presence of. ne substructures in the hot interstellar medium (ISM). Some of these are likely to result from interaction with the radio jets, while others may be related to a complex intermingling of different phases of the ISM. We detect a low-luminosity X-ray active galactic nucleus (AGN) with L-X = 5 x 10(39) ergs s(-1) (in 0.3-8 keV) and a Gamma = 1.7 power-law energy spectrum. We also detect 81 point sources within the 25th magnitude isophotal ellipse of NGC 1316 (LX in the range of 2 x 10(37) to 2 x 10(39) ergs s(-1)), with hard (kT similar to 5 keV) X-ray spectra, typical of X-ray binaries, and a spatial radial distribution consistent with that of the optical (i.e., stellar) surface brightness. We derive the X-ray luminosity function (XLF) of these sources, correcting for the incompleteness at the faint end caused by the presence of the diffuse emission from the hot ISM in the central regions of NGC 1316 and by the widening of the Chandra point-spread functions at increasing distance from the aim point. With these corrections, the XLF is well reproduced by a single-unbroken-power law with a slope of -1.3 down to our threshold luminosity of similar to3 x 10(37) ergs s(-1). The hot ISM has temperatures in the 0.5-0.6 keV range, its surface brightness distribution is more centrally concentrated than that of the point sources, and its temperature appears to decrease at larger radii. These properties suggest that the ISM may be subject to partial winds. Taking into account the spectral complexity of the ISM, and the presence of unresolved low luminosity X-ray sources ( which can be inferred from the spectra), we constrain the metal abundance of the hot ISM to be Z = 0.25-1.3 Z. (90% confidence). C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kim, DW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 87 TC 110 Z9 110 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 2003 VL 586 IS 2 BP 826 EP 849 DI 10.1086/367930 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500012 ER PT J AU Paolillo, M Fabbiano, G Peres, G Kim, DW AF Paolillo, M Fabbiano, G Peres, G Kim, DW TI ROSAT HRI investigation of the NGC 507 X-ray halo SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies : clusters : individual (Perseus-Pisces); galaxies : halos; galaxies : jets; radio continuum : galaxies; X-rays : individual (NGC 507) ID EARLY-TYPE GALAXIES; LUMINOSITY RADIO GALAXIES; COUNTING DETECTOR IMAGES; COOLING FLOW GALAXIES; ELLIPTIC GALAXIES; XMM-NEWTON; INTRACLUSTER MEDIUM; WAVELET TRANSFORMS; PSPC OBSERVATIONS; VLA OBSERVATIONS AB We present an X-ray investigation of the elliptical galaxy NGC 507 in the Pisces cluster. We make use of archival ROSAT HRI and Chandra data, and of previously published PSPC data, to connect the large-scale structure of the halo to the core morphology. Our analysis, based on a bidimensional double beta model of the halo surface brightness, shows that the halo core (r < 2-3r(e)) and the external halo (r > 3r(e)) are characterized by different dynamical properties and suggests a different origin of the two components. The halo core has a complex morphology with a main X-ray emission peak, coincident with the center of the optical galaxy, and several secondary peaks. The spatial and spectral analysis of the central peak shows that this feature is produced by denser hot gas in the galaxy core. While both homogeneous and inhomogeneous cooling flow models predict a deposited mass exceeding the observed amount, our data support the scenario in which the gas is kinetically heated by stellar mass losses. Comparison with previously published studies suggests that the core of an X-ray extended galaxy is associated with the stellar distribution and has properties similar to the X-ray halos of compact galaxies. The secondary peaks are due instead to interactions between the radio-emitting plasma and the surrounding ISM, producing density fluctuations in the hot gas. We find that the energy input by the central radio source in the ISM is large enough to prevent gas cooling and may explain the failure of the cooling flow models. The total mass pro. le derived from the bidimensional model shows that a significant amount of dark matter is present at large radii. The dark halo extends on cluster scales and is likely associated with the whole cluster rather than with NGC 507. This structure is typical of many X-ray bright early-type galaxies and may explain the spatial and spectral differences with X-ray compact galaxies largely debated in the literature. The large-scale surface brightness distribution is irregular and more extended in the northeast direction. The displacement of the cluster halo from the optical galaxy and the filamentary structures observed in the halo core further suggest that the galaxy may be slowly moving within the group potential. Finally, we found that similar to20% of the sources detected by Kim & Fabbiano in the NGC 507 halo are due to point sources, while the nature of the remaining population is not clear. If associated with NGC 507, they could be either accreting binaries hosting a massive black hole or density clumps of the X-ray halo. C1 Univ Palermo, Sez Astron, DSFA, I-90134 Palermo, Italy. Osserv Astron Capodimonte, I-80131 Naples, Italy. Harvard Smithsonian Ctr Astrophys, High Energy Div, Cambridge, MA 02138 USA. RP Paolillo, M (reprint author), Univ Palermo, Sez Astron, DSFA, Piazza Parlamento 1, I-90134 Palermo, Italy. EM paolillo@astropa.unipa.it; pepi@head-cfa.harvard.edu; peres@astropa.unipa.it; kim@head-cfa.harvard.edu RI Paolillo, Maurizio/J-1733-2012 OI Paolillo, Maurizio/0000-0003-4210-7693 NR 66 TC 19 Z9 19 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 APR 1 PY 2003 VL 586 IS 2 BP 850 EP 867 DI 10.1086/367718 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500013 ER PT J AU Eskridge, PB Frogel, JA Taylor, VA Windhorst, RA Odewahn, SC Chiarenza, CATC Conselice, CJ de Grijs, R Matthews, LD O'Connell, RW Gallagher, JS AF Eskridge, PB Frogel, JA Taylor, VA Windhorst, RA Odewahn, SC Chiarenza, CATC Conselice, CJ de Grijs, R Matthews, LD O'Connell, RW Gallagher, JS TI Ultraviolet-optical pixel maps of face-on spiral galaxies: Clues for dynamics and star formation histories SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 6753, NGC 6782); galaxies : photometry; galaxies : spiral; galaxies : structure; ultraviolet : galaxies ID H-II REGIONS; SURFACE PHOTOMETRY; RINGED GALAXIES; DISK GALAXIES; STELLAR; MORPHOLOGY; DECOMPOSITION; PROFILES; TELESCOPE; ABUNDANCE AB Ultraviolet and optical images of the face-on spiral galaxies NGC 6753 and NGC 6782 reveal regions of strong ongoing star formation that are associated with structures traced by the old stellar populations. We use these images to construct NUV-(NUV-I(814)) pixel color-magnitude diagrams (pCMDs) that reveal plumes of pixels with strongly varying near-ultraviolet (NUV) surface brightness and nearly constant I(814) surface brightness. The plumes correspond to sharply bounded radial ranges, with (NUV- I(814)) at a given NUV surface brightness being bluer at larger radii. The plumes are parallel to both the reddening vector and simple model mixtures of young and old populations, thus neither reddening nor the fraction of the young population can produce the observed separation between the plumes. The images and radial surface brightness and color plots indicate that the separate plumes are caused by sharp declines in the surface densities of the old populations at radii corresponding to disk resonances. The maximum surface brightness of the NUV light remains essentially constant with radius, while the maximum I(814) surface brightness declines sharply with radius. A mid-ultraviolet (MUV) image of NGC 6782 shows emission from the nuclear ring. The distribution of points in an (MUV-NUV)-(NUV-I(814)) pixel color-color diagram is broadly consistent with the simple mixture model but shows a residual trend that the bluest pixels in (MUV-NUV) are the reddest pixels in (NUV-I(814)). This may be due to a combination of red continuum from late-type supergiants and [S III] emission lines associated with H II regions in active star-forming regions. We have shown that pixel mapping is a powerful tool for studying the distribution and strength of ongoing star formation in galaxies. Deep, multicolor imaging can extend this to studies of extinction and the ages and metallicities of composite stellar populations in nearby galaxies. C1 Minnesota State Univ, Dept Phys & Astron, Trafton Sci Ctr N 141, Mankato, MN 56001 USA. Ohio State Univ, Dept Astron, McPherson Lab, Columbus, OH 43210 USA. NASA Headquarters, Washington, DC 20546 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Eskridge, PB (reprint author), Minnesota State Univ, Dept Phys & Astron, Trafton Sci Ctr N 141, Mankato, MN 56001 USA. RI Conselice, Christopher/B-4348-2013; OI Conselice, Christopher/0000-0003-1949-7638; de Grijs, Richard/0000-0002-7203-5996 NR 45 TC 16 Z9 16 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 APR 1 PY 2003 VL 586 IS 2 BP 923 EP 938 DI 10.1086/367820 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500017 ER PT J AU Magnani, L Chastain, RJ Kim, CH Hartmann, D Truong, AT Thaddeus, P AF Magnani, L Chastain, RJ Kim, CH Hartmann, D Truong, AT Thaddeus, P TI CH, CO, and E(B-V) as molecular gas tracers in a translucent cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : clouds; ISM : molecules; molecular processes ID H-2 CONVERSION FACTOR; INTERSTELLAR-MEDIUM; H-I; INFRARED-EMISSION; MILKY-WAY; DIFFUSE; GALAXY; CIRRUS; TURBULENCE; DENSITY AB The effectiveness of three molecular hydrogen gas tracers-the CH(2)Pi(1/2), J = 1/2, F = 1-1 transition, the CO(1-0) transition, and the color excess, E(B-V)-is evaluated for the translucent molecular cloud MBM 16. The CH emission line and E(B-V) are well correlated with each other but not with the CO(1-0) emission line. It is likely that in translucent molecular clouds CO is not a linear tracer of the molecular hydrogen column density because, in these objects, the CO/H-2 ratio is undergoing rapid fluctuations as a function of the molecular hydrogen column density. For translucent and diffuse molecular clouds, and possibly for the translucent envelopes of giant molecular clouds, CH observations should be used to calibrate the CO to H-2 conversion factor. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Columbia Univ, New York, NY 10027 USA. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Univ Calif Berkeley, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Magnani, L (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. NR 41 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 APR 1 PY 2003 VL 586 IS 2 BP 1111 EP 1119 DI 10.1086/367883 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500026 ER PT J AU Osorio, M D'Alessio, P Muzerolle, J Calvet, N Hartmann, L AF Osorio, M D'Alessio, P Muzerolle, J Calvet, N Hartmann, L TI A comprehensive study of the L1551 IRS 5 binary system SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; circumstellar matter; stars : formation; stars : individual (L1551 IRS 5); stars : pre-main-sequence ID MILLIMETER-CONTINUUM OBSERVATIONS; AURIGA MOLECULAR CLOUD; YOUNG STELLAR OBJECTS; T-TAURI STARS; ACCRETION DISKS; INFRARED OBSERVATIONS; PROTOPLANETARY DISKS; CO; SPECTRUM; MODELS AB We model the Class I source L1551 IRS 5, adopting a flattened infalling envelope surrounding a binary disk system and a circumbinary disk. With our composite model, we calculate self-consistently the spectral energy distribution of each component of the L1551 IRS 5 system, using additional constraints from recent observations by ISO, the water ice feature from observations with SpeX, the SCUBA extended spatial brightness distribution at submillimeter wavelengths, and the VLA spatial intensity distributions at 7 mm of the binary disks. We analyze the sensitivity of our results to the various parameters involved. Our results show that a flattened-envelope collapse model is required to explain simultaneously the large-scale fluxes and the water ice and silicate features. On the other hand, we find that the circumstellar disks are optically thick in the millimeter range and are inclined so that their outer parts hide the emission along the line of sight from their inner parts. We also find that these disks have lower mass accretion rates than the infall rate of the envelope. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Osorio, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mosorio@cfa.harvard.edu; p.dalessio@astrosmo.unam.mx; jamesm@as.arizona.edu; ncalvet@cfa.harvard.edu; hartmann@cfa.harvard.edu NR 62 TC 39 Z9 39 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2003 VL 586 IS 2 BP 1148 EP 1161 DI 10.1086/367695 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500030 ER PT J AU Long, KS Reynolds, SP Raymond, JC Winkler, PF Dyer, KK Petre, R AF Long, KS Reynolds, SP Raymond, JC Winkler, PF Dyer, KK Petre, R TI Chandra CCD imagery of the northeast and northwest limbs of SN 1006 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (SN 1006); supernova remnants; X-rays : ISM ID SUPERNOVA REMNANT SN-1006; ULTRAVIOLET-ABSORPTION-LINES; X-RAY-EMISSION; NONLINEAR AMPLIFICATION; NONRADIATIVE SHOCKS; MAGNETIC-FIELD; COSMIC-RAYS; HIGH-ENERGY; ACCELERATION; INSTABILITIES AB We present deep images of the SN 1006 remnant (G327.6+14.6) with the ACIS instrument on the Chandra X-Ray Observatory. Two regions have been observed, the synchrotron-dominated northeast limb and the thermally dominated northwest limb, as well as a substantial portion of the interior of the remnant shell. The brightest features in the X-ray images correspond closely to radio features in the northeast and to Balmer-dominated. laments in the northwest. The spectra of the brighter. laments in the northeast are harder, with less prominent line emission than those in the northwest. In addition to highly elongated. laments, both images show enhanced clumps of emission well inside of the shock front that appear to be dominated by emission from oxygen. These probably arise from shock-heated ejecta, based on analysis of their X-ray spectra. We find no firm evidence for a halo of X-ray emission outside the shock to the northeast, as predicted by the Fermi shock-acceleration picture, in which relativistic electrons should be diffusing ahead of the shock. Our limits on upstream emission are less than 1.5% of the postshock levels in regions where the supernova remnant is brightest. This strongly suggests that the bright rims are flattened sheets nearly perpendicular to the plane of the sky and that the magnetic field strength jumps at the shock by a factor significantly larger than 4, as has been proposed if the shock puts significant energy into accelerating nonthermal ions. The spectra obtained of the northwest rim are all dominated by the helium-like ions of O, Ne, Mg, and Si expected from shocks with ionization (n(e)t) parameters of order 100 cm(-3) yr and electron temperatures of 0.5-1 keV, far lower than the postshock ion temperature implied by estimates of the shock speed obtained from the shape of the Halpha line. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Long, KS (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. NR 39 TC 117 Z9 119 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 2003 VL 586 IS 2 BP 1162 EP 1178 DI 10.1086/367832 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500031 ER PT J AU Akerlof, CW Biller, S Boyle, P Buckley, J Carter-Lewis, DA Catanese, M Cawley, MF Connaughton, V Fegan, DJ Finley, J Gaidos, J Hillas, AM Krennrich, F Lamb, RC Lessard, R McEnery, J Mohanty, G Porter, NA Quinn, J Rodgers, A Rose, HJ Samuelson, F Schubnell, MS Sembroski, G Srinivasan, R Weekes, TC Zweerink, J AF Akerlof, CW Biller, S Boyle, P Buckley, J Carter-Lewis, DA Catanese, M Cawley, MF Connaughton, V Fegan, DJ Finley, J Gaidos, J Hillas, AM Krennrich, F Lamb, RC Lessard, R McEnery, J Mohanty, G Porter, NA Quinn, J Rodgers, A Rose, HJ Samuelson, F Schubnell, MS Sembroski, G Srinivasan, R Weekes, TC Zweerink, J TI A search for correlations of TeV gamma rays with ultra-high-energy cosmic rays SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; galaxies : active; galaxies : individual (3C 147); gamma rays : observations ID BURSTS; SYSTEM; RADIATION; ASTRONOMY; PHOTONS; ARRAY AB A search was conducted for TeV gamma-rays emitted from the direction of the ultra-high-energy cosmic ray detected by the Fly's Eye experiment with energy E similar to 3 x 10(20) eV. No enhancement was found at a level of 10(-10)gamma cm(-2) s(-1) for E > 350 GeV. A steady source of ultra-high-energy cosmic ray protons or photons would be expected to produce a gamma-ray flux above this level. An upper limit was also set for the flux of TeV gamma-rays from 3C 147, the most prominent active galactic nucleus in the error box. C1 Univ Michigan, Dept Phys, Randall Lab 2477, Ann Arbor, MI 48109 USA. Univ Oxford, Dept Phys, Oxford OX1 3RH, England. Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. Univ Coll Dublin, Dept Phys, Dublin 4, Ireland. Iowa State Univ Sci & Technol, Dept Phys & Astron, Ames, IA 50011 USA. St Patricks Coll, Dept Expt Phys, Maynooth, Kildare, Ireland. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. RP Akerlof, CW (reprint author), Univ Michigan, Dept Phys, Randall Lab 2477, 500 E Univ Ave, Ann Arbor, MI 48109 USA. EM tweekes@cfa.harvard.edu RI McEnery, Julie/D-6612-2012 NR 34 TC 3 Z9 3 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2003 VL 586 IS 2 BP 1232 EP 1237 DI 10.1086/367825 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500036 ER PT J AU Homan, J Klein-Wolt, M Rossi, S Miller, JM Wijnands, R Belloni, T van der Klis, M Lewin, WHG AF Homan, J Klein-Wolt, M Rossi, S Miller, JM Wijnands, R Belloni, T van der Klis, M Lewin, WHG TI High-frequency quasi-periodic oscillations in the black hole X-ray transient XTE J1650-500 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (XTE J1650-500); stars : oscillations; X-rays : binaries; X-rays : stars ID MICROQUASAR GRO J1655-40; RXTE OBSERVATIONS; POWER SPECTRA; CANDIDATE; BINARIES; GRS-1915+105; DISCOVERY; J1550-564; SPIN; PCA AB We report the detection of high-frequency variability in the black hole X-ray transient XTE J1650-500. A quasi-periodic oscillation (QPO) was found at 250 Hz during a transition from the hard to the soft state. We also detected less coherent variability around 50 Hz that disappeared when the 250 Hz QPO showed up. There are indications that when the energy spectrum hardened the QPO frequency increased from similar to110 to similar to270 Hz, although the observed frequencies are also consistent with being 1 : 2 : 3 harmonics of each other. Interpreting the 250 Hz as the orbital frequency at the innermost stable orbit around a Schwarzschild black hole leads to a mass estimate of 8.2 M-circle dot. The spectral results by Miller et al., which suggest considerable black hole spin, would imply a higher mass. C1 Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. RP Homan, J (reprint author), Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy. EM homan@merate.mi.astro.it; klein@astro.uva.nl; srossi@merate.mi.astro.it; jmmiller@head-cfa.harvard.edu; radw@st-andrews.ac.uk; belloni@merate.mi.astro.it; michiel@astro.uva.nl; lewin@space.mit.edu NR 48 TC 55 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 APR 1 PY 2003 VL 586 IS 2 BP 1262 EP 1267 DI 10.1086/367699 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GP UT WOS:000181713500040 ER PT J AU Rodriguez, LF Porras, A Claussen, MJ Curiel, S Wilner, DJ Ho, PTP AF Rodriguez, LF Porras, A Claussen, MJ Curiel, S Wilner, DJ Ho, PTP TI The binary jet in L1551 IRS 5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : jets and outflows; stars : individual (L1551 IRS 5) ID IRS 5; L1551; SPECTROSCOPY; COLLIMATION; SYSTEM; STARS; DISKS AB We have used the Very Large Array with the Pie Town antenna of the Very Long Baseline Array to image for the first time L1551 IRS 5 at 3.5 cm with an angular resolution of similar to0."1. These observations clearly reveal the presence of a binary jet, with each component approximately centered on the 7 mm compact protoplanetary disks previously reported. As anticipated from results at various wavelengths, L1551 IRS 5 is a binary system where each star is surrounded by a disk and drives a collimated jet. The curved morphology of the northern jet, showing reflection symmetry, is suggestive of that expected for a source in a binary orbit. A region of radio emission located between the two jets could be a zone of shock interaction between the two outflows. C1 Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58190, Michoacan, Mexico. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rodriguez, LF (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Antigua Carretera Patzcuaro 8701, Morelia 58190, Michoacan, Mexico. EM l.rodriguez@astrosmo.unam.mx; a.porras@astrosmo.unam.mx; mclausse@nrao.edu; scuriel@astroscu.unam.mx; dwilner@cfa.harvard.edu; pho@cfa.harvard.edu NR 11 TC 35 Z9 35 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2003 VL 586 IS 2 BP L137 EP L139 DI 10.1086/374882 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658GQ UT WOS:000181713600007 ER PT J AU Robbins, MB Braun, MJ Finch, DW AF Robbins, MB Braun, MJ Finch, DW TI Discovery of a population of the endangered Red Siskin (Carduelis cucullata) in Guyana SO AUK LA English DT Article AB A heretofore unknown population of the endangered Red Siskin (Carduelis cucullata) was discovered in southwestern Guyana, similar to950 km from populations along the Venezuela coastal cordilleras. Most Venezuelan populations have been greatly reduced by the pet trade during the past 150 years, thus the newly discovered Guyana population represents an opportunity to insure the survival of this highly endangered species in the wild. Breeding of Guyanese siskins coincides with both breeding periods (May to early July and November-December) that have been documented in Venezuela. Breeding behavior, vocalizations, feeding habits, and immature plumages are described. C1 Univ Kansas, Museum Nat Hist, Div Birds, Lawrence, KS 66045 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Suitland, MD 20746 USA. Natl Museum Nat Hist, Smithsonian Inst, Lab Analyt Biol, Suitland, MD 20746 USA. WINGS, Tucson, AZ 85712 USA. RP Robbins, MB (reprint author), Univ Kansas, Museum Nat Hist, Div Birds, Lawrence, KS 66045 USA. NR 11 TC 4 Z9 5 U1 0 U2 2 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD APR PY 2003 VL 120 IS 2 BP 291 EP 298 DI 10.1642/0004-8038(2003)120[0291:DOAPOT]2.0.CO;2 PG 8 WC Ornithology SC Zoology GA 695KG UT WOS:000183829200004 ER PT J AU Vann, CD Megonigal, JP AF Vann, CD Megonigal, JP TI Elevated CO2 and water depth regulation of methane emissions: Comparison of woody and non-woody wetland plant species SO BIOGEOCHEMISTRY LA English DT Article DE elevated CO2; global change; methane emissions; methane oxidation; productivity; Taxodium distichum; wetlands ID CARBON-DIOXIDE; CH4 EMISSIONS; BOREAL MIRE; SOIL; RHIZOSPHERE; RICE; ROOT; OXIDATION; ENRICHMENT; ATMOSPHERE AB Elevated CO2 has been shown to increase methane emissions in herbaceous wetlands, but it is not clear that this will occur in wetlands dominated by woody plants or in wetlands that are not inundated. We determined the effects of elevated CO2 and water table position on methane emission and oxidation rates from plant-soil microcosms planted with a woody tree, Taxodium distichum, or an emergent aquatic macrophyte, Orontium aquaticum. Experiments were conducted in replicate glasshouses (n = 2) at CO2 concentrations of either 350 or 700 ppmv. Plants were grown from seed and subjected to two water level depths, flooded (+5 cm above the soil surface) and non-flooded (-10 cm for T. distichum and -6 cm for O. aquaticum). Elevated CO2 increased whole-plant photosynthetic rates in both water table treatments. Methane emission rates increased by 62 to 69% in the T. distichum treatment and 27 to 29% in the O. aquaticum treatment. Whole-plant photosynthesis and biomass were strongly correlated with methane emissions (r(2) greater than or equal to 0.75, P less than or equal to 0.01). This relationship provides evidence of a tight coupling between plant and microbial activity and suggests that similar relationships from other wetland studies measured at ambient CO2 can be extrapolated into the future. In the O. aquaticum, non-flooded treatment, methanotrophy consumed 14 and 22% ( replicate glasshouses) of the methane produced in the ambient treatment compared to 29 and 36% in the elevated CO2 treatment. However, there was no significant methane oxidation detected in the flooded treatment. We concluded that woody and non-woody wetland ecosystems growing in a future CO2-enriched atmosphere will emit more methane regardless of water table position, but the degree of stimulation will be sensitive to changes in water table position, particularly in forested wetlands. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. George Mason Univ, Fairfax, VA 22030 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 45 TC 56 Z9 66 U1 3 U2 64 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD APR-MAY PY 2003 VL 63 IS 2 BP 117 EP 134 DI 10.1023/A:1023397032331 PG 18 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 668MN UT WOS:000182297900001 ER PT J AU Caldas, A Robbins, RK AF Caldas, A Robbins, RK TI Modified Pollard transects for assessing tropical butterfly abundance and diversity SO BIOLOGICAL CONSERVATION LA English DT Article DE butterfly abundance; butterfly diversity; transects; Pollard; tropics ID TEMPORAL DIMENSIONS; SPECIES-DIVERSITY; ASSEMBLAGES AB This paper introduces and discusses the consistency and effectiveness of an inexpensive modification of Pollard transects for assessing the diversity and abundance of tropical butterfly communities in two national parks in Rio de Janeiro, Brazil. To measure butterfly abundance, students walked simultaneous timed transects at the interface of forest and cleared areas. They either counted the number of individuals observed or tabulated the number of specimens collected with nets. After a short training period, the number of butterflies observed or collected on simultaneous transects was statistically indistinguishable among student groups, and there was a significant positive correlation between observation counts and collected number of individuals. As a measure of species richness, the number of butterfly species sampled on each simultaneous transect was tabulated and did not differ statistically. To measure diversity, alpha of the logseries model was calculated for each collected sample, and statistical fit to a logseries model was determined. Although virtually all daily samples and the year's accumulated sample at one park fit the logseries model, about 35% of the daily samples and the entire year's sample did not fit at the other park. Despite these differences between the two parks, values for alpha from daily samples at both parks varied similarly (from 15 to 50 in almost all cases), and values from the entire year's samples were statistically indistinguishable. The repeatability of results among novices, such as students, suggests that timed transects have great promise for furthering our understanding of butterfly community demographics. Published by Elsevier Science Ltd. C1 Smithsonian Inst, Natl Museum Nat Hist, Sect Entomol, Dept Systemat Biol, Washington, DC 20560 USA. UERJ, Dept Biol Anim & Vegetal, BR-20550900 Rio De Janeiro, Brazil. RP Caldas, A (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. NR 40 TC 30 Z9 38 U1 1 U2 15 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 2003 VL 110 IS 2 BP 211 EP 219 AR PII S0006-3207(02)00190-8 DI 10.1016/S0006-3207(02)00190-8 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 642RR UT WOS:000180818400005 ER PT J AU Harrison, RD Hamid, AA Kenta, T Lafrankie, J Lee, HS Nagamasu, H Nakashizuka, T Palmiotto, P AF Harrison, RD Hamid, AA Kenta, T Lafrankie, J Lee, HS Nagamasu, H Nakashizuka, T Palmiotto, P TI The diversity of hemi-epiphytic figs (Ficus; Moraceae) in a Bornean lowland rain forest SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE canopy; niche specialization; rare species; species diversity; strangler fig; Urostigma ID VENEZUELAN PALM SAVANNA; STRANGLER FIG; WATER RELATIONS; TREE; CANOPY; GROWTH; ANTS; HEMIEPIPHYTES; ESTABLISHMENT; CONSEQUENCES AB The diversity and niche specificity of hemi-epiphytic figs in a lowland dipterocarp forest in Sarawak were investigated in 1998. Twenty-seven fig species (264 individuals, c. 120 ha) colonized a diversity of host taxa (35 families), but densities were very low and only 1.77% of trees >30 cm d.b.h. were occupied. There were no significant associations with host taxa or host-bark roughness but among 11 common species (greater than or equal to9 individuals) the distributions of all other parameters (host-d.b.h., height and position of colonization, crown illumination, soil-texture and slope-angle) were significantly different, and we identified five fig guilds. The guilds corresponded to canopy strata, and appeared to reflect the establishment microsite requirements of different species. A fundamental trade-off within the hemiepiphytic habit was revealed: Species colonizing larger hosts were rarer, because of lower host densities and more specific microsite requirements, but had better light environments and attained a larger maximum size. The single strangler species appeared to escape many of these constraints, and an important source of mortality caused by host-toppling, indicating the advantages of this strategy. Thus, the hemi-epiphytic figs in this community have come to fill a remarkable diversity of niches, despite low levels of competition, through the exigencies of a complex environment. (C) 2003 The Linnean Society of London. C1 Kyoto Univ, Ctr Ecol Res, Otsu, Shiga 5202113, Japan. Forest Res Ctr, Forest Dept Sarawak, Kuching Sarawak 93762, Malaysia. Nanyang Technol Univ, CTFS Asia Program, Singapore 1025, Singapore. Kyoto Univ, Kyoto Univ Museum, Yoshida Honmachi, Sakyo 6068501, Japan. Antioch New England Grad Sch, Dept Environm Studies, Keene, NH USA. RP Harrison, RD (reprint author), Smithsonian Trop Res Inst, APDO 2072, Balboa, Panama. RI Kenta, Tanaka/B-2652-2014 NR 61 TC 20 Z9 21 U1 2 U2 12 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 APR PY 2003 VL 78 IS 4 BP 439 EP 455 DI 10.1046/j.0024-4066.2002.00205.x PG 17 WC Evolutionary Biology SC Evolutionary Biology GA 672VW UT WOS:000182544500002 ER PT J AU Collin, R AF Collin, R TI The utility of morphological characters in gastropod phylogenetics: an example from the Calyptraeidae SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Calyptraea; Cheilea; Crepidula; Crucibulum; gastropod taxonomy ID SEX-CHANGE; CREPIDULA-FORNICATA; LARVAL; GROWTH; PLANA; MESOGASTROPODA; PROSOBRANCHIA; RAPANINAE; MOLLUSCA; PATTERNS AB Organismal taxonomy is often based on a single or a small number of morphological characters. When they are morphologically simple or known to be plastic, we may not have great confidence in the taxonomic conclusions of analyses based on these characters. For example, calyptraeid gastropod shells are well known for their simplicity and plasticity, and appear to be subject to frequent evolutionary convergences, but are nevertheless the basis for calyptraeid taxonomy. In a case like this, knowing how the pattern of relationships inferred from morphological features used in traditional taxonomy compares to the patterns of relationships inferred from other morphological characters or DNA sequence data would be useful. In this paper, I examine the relative utility of traditional taxonomic characters (shell characters), anatomical characters and molecular characters for reconstructing the phylogeny of calyptraeid gastropods. The results of an ILD test and comparisons of the recovered tree topologies suggest that there is conflict between the DNA sequence data and the morphological data. Very few of the nodes recovered by the morphological data were recovered by any other dataset. Despite this conflict, the inclusion of morphological data increased the resolution and support of nodes in the topology recovered from a combined dataset. The RIs and CIs of the morphological data on the best estimate topology were not any worse than these indices for the other datasets. This analysis demonstrates that although analyses can be misled by these convergences if morphological characters are used alone, these characters contribute significantly to the combined dataset. (C) 2003 The Linnean Society of London. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Collin, R (reprint author), Univ Chicago, Comm Evolutionary Biol, Culver Hull,Rm 402,1025 E 57th St, Chicago, IL 60637 USA. RI Collin, Rachel/G-2001-2010; OI Collin, Rachel/0000-0001-5103-4460 NR 68 TC 26 Z9 30 U1 0 U2 5 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 APR PY 2003 VL 78 IS 4 BP 541 EP 593 DI 10.1046/j.0024-4066.2002.00166.x PG 53 WC Evolutionary Biology SC Evolutionary Biology GA 672VW UT WOS:000182544500010 ER PT J AU Breitburg, DL Jordan, TE Lipton, D AF Breitburg, DL Jordan, TE Lipton, D TI Preface-from ecology to economics: Tracing human influence in the Patuxent River estuary and its watershed SO ESTUARIES LA English DT Editorial Material C1 Acad Nat Sci, Estuarine Res Ctr, St Leonard, MD 20678 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Dept Agr & Resource Econ, College Pk, MD 20742 USA. RP Breitburg, DL (reprint author), Acad Nat Sci, Estuarine Res Ctr, 10545 Mackall Rd, St Leonard, MD 20678 USA. NR 22 TC 1 Z9 2 U1 0 U2 3 PU ESTUARINE RES FEDERATION PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0160-8347 J9 ESTUARIES JI Estuaries PD APR PY 2003 VL 26 IS 2A BP 167 EP 170 DI 10.1007/BF02695959 PG 4 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 699JE UT WOS:000184052600001 ER PT J AU Jordan, TE Weller, DE Correll, DL AF Jordan, TE Weller, DE Correll, DL TI Sources of nutrient inputs to the Patuxent River estuary SO ESTUARIES LA English DT Article ID PARTIALLY STRATIFIED ESTUARY; ATLANTIC COASTAL-PLAIN; LONG-TERM TRENDS; CHESAPEAKE BAY; LAND-USE; ATMOSPHERIC NITROGEN; AGRICULTURAL WATERSHEDS; PARTICULATE MATTER; NITRATE-NITROGEN; AIR-TEMPERATURE AB We quantified annual nutrient inputs to the Patuxent River estuary from point and nonpoint sources and from direct atmospheric deposition. We also compared nonpoint source (NPS) discharges from Piedmont and Coastal Plain regions and from agricultural and developed lands. Using continuous automated-sampling, we measured discharges of water, nitrogen, phosphorus, organic carbon (C), and suspended solids from a total of 23 watersheds selected to represent various proportions of developed land and cropland in the Patuxent River basin and the neighboring Rhode River basin. The sampling period spanned two years that differed in annual precipitation by a factor of 1.7. Water discharge from the watershed to the Patuxent River estuary was 3.4 times higher in the wet year than in the dry year. Annual water discharges from the study watersheds increased as the proportion of developed land increased. As the proportion of cropland increased, there were increases in the annual flow-weighted mean concentrations of nitrate (NO3-), total nitrogen (TN), dissolved silicate (Si), total phosphate (TPO43-), total organic phosphorus (TOP), total P (TP), and total suspended solids (TSS) in NPS discharges. The effect of cropland on the concentrations of NO3- and TN was stronger for Piedmont watersheds than for Coastal Plain watersheds. As the proportion of developed land increased, there were increases in annual mean concentrations of NO3-, total ammonium (TNH4+), total organic N (TON), TN, total organic C (TOC), TPO43-, TOP, TP, and TSS and decreases in concentrations of Si. Annual mean concentrations of TON, TOC, forms of P, and TSS were highest in the wet year. Annual mean concentrations of NO3-, TNH4+, TN, and Si did not differ significantly between years. We directly measured NPS discharges from about half of the Patuxent River basin and estimated discharges from the other half of the basin using statistical models that related annual water flow and material concentrations to land cover and physiographic province. We compared NPS discharges to public data on point source (PS) discharges. We estimated direct atmospheric deposition of forms of N, P, and organic C to the Patuxent River estuary based on analysis of bulk deposition near the Rhode River. During the wet year, most of the total terrestrial and atmospheric inputs of forms of N and P came from NPS discharges. During the dry year, 53% of the TNH4+ input was from atmospheric deposition and 58% of the NO3- input was from PS discharges; NPS and PS discharges were about equally important in the total inputs of TN and TPO43-. During the entire 2-yr period, the Coastal Plain portion of the Patuxent basin delivered about 80% of the NPS water discharges to the estuary and delivered similar proportions of the NPS TNH4+, TN, TOP, and TSS. The Coastal Plain delivered greater proportions of the NPS TON, TOC, Si, and TP (89%, 90%, 93%, and 95%, respecfively) than of water, and supplied nearly all of the NPS TPO43- (99%). The Piedmont delivered 33% of the NPS NO3- while delivering only 20% of the NPS water to the estuary. We used statistical models to infer the percentages of NPS discharges supplied by croplands, developed lands, and other lands. Although cropland covers only 10% of the Patuxent River basin, it was the most important source of most materials in NPS discharge, supplying about 84% of the total NPS discharge of NO3-; about three quarters of the TPO43-, TOP, TP, and TSS; and about half of the TNH4+ and TN. Compared to developed land, cropland supplied a significantly higher percentage of the NPS discharges of NO3-, TN, TPO43-, TOP, TP, and TSS, despite the fact developed land covered 12% of the basin. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Jordan, TE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. OI Weller, Donald/0000-0002-7629-5437 NR 92 TC 55 Z9 59 U1 0 U2 8 PU ESTUARINE RES FEDERATION PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0160-8347 J9 ESTUARIES JI Estuaries PD APR PY 2003 VL 26 IS 2A BP 226 EP 243 DI 10.1007/BF02695964 PG 18 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 699JE UT WOS:000184052600006 ER PT J AU Weller, DE Jordan, TE Correll, DL Liu, ZJ AF Weller, DE Jordan, TE Correll, DL Liu, ZJ TI Effects of land-use change on nutrient discharges from the Patuxent River watershed SO ESTUARIES LA English DT Article ID GULF-OF-MEXICO; CHESAPEAKE BAY; UNITED-STATES; NITROGEN FLUX; ESTUARY; PHOSPHORUS; LANDSCAPE; PRECIPITATION; TRANSPORT; QUALITY AB We developed an empirical model integrating nonpoint source (NPS) runoff, point sources (PS), and reservoir management to predict watershed discharges of water, sediment, organic carbon, silicate, nitrogen, and phosphorus to the Patuxent River in Maryland. We estimated NPS discharges with linear models fit to measurements of weekly flow and 10 material concentrations from 22 study watersheds. The independent variables were the proportions of cropland and developed land, physiographic province (Coastal Plain or Piedmont), and time (week). An but one of the NPS models explained between 62% and 83% of the variability among concentration or flow measurements. Geographic factors (land cover and physiographic province) accounted for the explained variability in largely dissolved material concentrations (nitrate [NO(3)], Silicate [Si], and total nitrogen [TN]), but the explained variability in flow and particulates (sediment and forms of phosphorus) was more strongly related to temporal variability or its interactions with land cover and province. Average concentrations of all materials increased with cropland proportion and also with developed land (except Si), but changes in cropland produced larger concentration shifts than equivalent changes in developed land proportion. Among land cover transitions, conversions between cropland and forest-grassland cause the greatest changes in material discharges, cropland and developed land conversions are intermediate, and developed land and forest-grassland conversions have the weakest effects. Changing land cover has stronger effects on NO(3) and TN in the Piedmont than in the Coastal Plain, but for all other materials, the effects of land-use change are greater in the Coastal Plain. We predicted the changes in nutrient load to the estuary under several alternate land cover configurations, including a state planning scenario that extrapolates current patterns of population growth and land development to the year 2020. In that scenario, declines in NPS discharges from reducing cropland are balanced by NPS discharge increases from developing an area almost six times larger than the lost cropland. When PS discharges are included, there are net increases in total water, total phosphorus, and TN discharges. C1 Smithsonian Environm Res Ctr, Edgewater, MD 20137 USA. RP Weller, DE (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 20137 USA. EM wellerd@si.edu OI Weller, Donald/0000-0002-7629-5437 NR 76 TC 53 Z9 55 U1 1 U2 16 PU ESTUARINE RESEARCH FEDERATION PI PORT REPUBLIC PA 2018 DAFFODIL, PO BOX 510, PORT REPUBLIC, MD 20676 USA SN 0160-8347 J9 ESTUARIES JI Estuaries PD APR PY 2003 VL 26 IS 2A BP 244 EP 266 DI 10.1007/BF02695965 PG 23 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 699JE UT WOS:000184052600007 ER PT J AU White, GG Munroe, TA Austin, HM AF White, GG Munroe, TA Austin, HM TI Reproductive seasonality, fecundity, and spawning frequency of tautog (Tautoga onitis) in the lower Chesapeake Bay and coastal waters of Virginia SO FISHERY BULLETIN LA English DT Article ID MIDDLE ATLANTIC BIGHT; ADULT TAUTOG; FISHES; PATTERNS; LABRIDAE; GROWTH; AGE AB The tautog, Thutoga onitis (Linnaeus), ranges from Nova Scotia to South Carolina and has become a popular target for recreational and commercial fisheries. Although tautog are a multiple spawning species, reproductive potential, measured as annual fecundity, has not been estimated previously with methods (batch fecundity, spawning frequency) necessary for a species with indeterminate annual fecundity. A total of 960 tautog were collected from the mouth of the Rappahannock River in the lower Chesapeake Bay to 45 kin offshore of Virginia's coastline to investigate tautog reproductive biology in the southern portion of the species range. Tautog did not exhibit a 1:1 sex ratio; 56% were females. Male tautog reached 50% maturity at 218 mm TL, females at 224 mm TL. Tautog spawned from 7 April 1995 to 15 June 1995, at locations from the York River to 45 kin offshore. Batch fecundity estimates ranged from 2800 to 181,200 eggs per spawning for female tautog age 3-9, total length 259516 mm. Mean batch fecundity +/-SEM for female tautog ages 4-6 was 54,243 2472 eggs and 106,256 3837 eggs for females ages 7-9. Spawning frequency was estimated at 1.2 days, resulting in 58 spawning days per female in 1995. Estimates of potential annual fecundity for tautog ages 3-9 ranged from 160,000 to 10,510,000 eggs. C1 Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, NOAA, Washington, DC 20013 USA. RP White, GG (reprint author), Atlantic States Marine Fisheries Commiss, 1444 Eye St NW,6th Floor, Washington, DC 20005 USA. NR 44 TC 12 Z9 12 U1 0 U2 1 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD APR PY 2003 VL 101 IS 2 BP 424 EP 442 PG 19 WC Fisheries SC Fisheries GA 670CJ UT WOS:000182389600019 ER PT J AU Rasse, DP Li, JH Drake, BG AF Rasse, DP Li, JH Drake, BG TI Carbon dioxide assimilation by a wetland sedge canopy exposed to ambient and elevated CO2: measurements and model analysis SO FUNCTIONAL ECOLOGY LA English DT Article DE canopy structure; global change; leaf nitrogen; open-top chamber; Scirpus ID PLANT-COMMUNITIES; ATMOSPHERIC CO2; TEMPERATE FORESTS; ESTUARINE MARSH; SCIRPUS-OLNEYI; GAS-EXCHANGE; PHOTOSYNTHESIS; GROWTH; NITROGEN; FLUXES AB 1. The wetland sedge Scirpus olneyi Gray displays fast rates of CO2 assimilation and responds positively to increased atmospheric CO2 concentration. The present study was aimed at identifying the ecophysiological traits specific to S. olneyi that drive these CO2 -assimilation patterns under ambient and elevated CO2 conditions. 2. The net ecosystem exchange (NEE) of CO2 between S. olneyi communities and the atmosphere was measured in open-top chambers. 3. We developed a new mechanistic model for S. olneyi communities based on published ecophysiological data and additional measurements of photosynthetic parameters. 4. Our NEE measurements confirmed that S. olneyi communities have a high rate of summertime CO2 assimilation, with noontime peaks reaching 40 mumol CO2 m(-2) ground s(-1) on productive summer days, and that elevated CO2 increased S. olneyi CO2 assimilation by c . 35-40%. 5. Using S. olneyi -specific ecophysiological parameters, comparison with measured NEE showed that the model accurately simulated these high rates of CO2 uptake under ambient or elevated CO2 . 6. The model pointed to the Rubisco capacity of Scirpus leaves associated with their high total nitrogen content as the primary explanation for the high rates of CO2 assimilation, and indicated that the vertical-leaf canopy structure of S. olneyi had comparatively little influence on CO2 assimilation. C1 Univ Liege, B-4000 Liege, Belgium. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Drake, BG (reprint author), Univ Liege, 17 Allee 6 Aout, B-4000 Liege, Belgium. OI Daniel, Rasse/0000-0002-5977-3863 NR 36 TC 9 Z9 11 U1 2 U2 13 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD APR PY 2003 VL 17 IS 2 BP 222 EP 230 DI 10.1046/j.1365-2435.2003.00730.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 671GV UT WOS:000182457700009 ER PT J AU MacLeod, KG Fullagar, PD Huber, BT AF MacLeod, KG Fullagar, PD Huber, BT TI Sr-87/Sr-86 test of the degree of impact-induced slope failure in the Maastrichtian of the western North Atlantic SO GEOLOGY LA English DT Article DE Cretaceous-Tertiary boundary; strontium isotopes; slump; Maastrichtian; Ocean Drilling Program ID CRETACEOUS-TERTIARY BOUNDARY; STRONTIUM ISOTOPE STRATIGRAPHY; EXTINCTION; MARGIN; EVOLUTION; RECORD AB Analyses of Sr-87/Sr-86 in foraminifera and sedimentollogical observations suggest that the Chicxulub impact was not the trigger for slumps or a hiatus within the Maastrichtian section recovered at Ocean Drilling Program Sites 1049, 1050, and 1052 (subtropical western North Atlantic). The slumps and hiatus occur within a sequence dominated by pelagic chalk. The Sr-87/Sr-86 measurements show a general increase through the Maastrichtian at each site, but suggest chronostratigraphic gaps on the order of 10(6) yr across the slumps. Some of the slumps have burrowed upper surfaces and are composed of material that is older and coarser grained than the bounding chalks. Pelagic deposition punctuated by gravity flows easily explains the Maastrichtian record on Blake Nose, whereas an impact-based explanation for slumping is difficult to reconcile with sedimentological and geochemical observations. C1 Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP MacLeod, KG (reprint author), Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 NR 29 TC 9 Z9 9 U1 0 U2 1 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD APR PY 2003 VL 31 IS 4 BP 311 EP 314 DI 10.1130/0091-7613(2003)031<0311:SSTOTD>2.0.CO;2 PG 4 WC Geology SC Geology GA 662CN UT WOS:000181928700006 ER PT J AU Stix, J Kennedy, B Hannington, M Gibson, H Fiske, R Mueller, W Franklin, J AF Stix, J Kennedy, B Hannington, M Gibson, H Fiske, R Mueller, W Franklin, J TI Caldera-forming processes and the origin of submarine volcanogenic massive sulfide deposits SO GEOLOGY LA English DT Article DE calderas; volcanogenic massive sulfide deposits; fluids; subsidence ID IZU-BONIN ARC; SEA-FLOOR; HYDROTHERMAL SYSTEM; YELLOWSTONE; SUBSIDENCE; MOUNTAINS; COLLAPSE; MAGMA; LAKE AB (C)ertain volcanogenic massive sulfide (VMS) ore deposits form in submarine calderas. This association is well known, but the link between caldera formation and the origins of the deposits remains poorly understood. Here we show that the size and location of a VMS deposit within a submarine caldera may be determined by how and when the caldera formed. These spatial-temporal conditions control development of the hydrothermal system associated with the VMS deposit. We propose that caldera opening along outward-dipping faults promotes magma degassing, seawater influx, and high-temperature leaching, resulting in a metal-rich hydrothermal fluid. These outward-dipping faults are considered to provide critical pathways for ore-forming fluids responsible for some caldera-hosted VMS deposits and may also be fundamentally important for the formation of many other caldera-hosted ore deposit types. C1 McGill Univ, Dept Earth & Planetary Sci, Montreal, PQ H3A 2A7, Canada. Geol Survey Canada, Ottawa, ON K1A 0E8, Canada. Laurentian Univ, Dept Earth Sci, Mineral Explorat Res Ctr, Sudbury, ON P3E 2C6, Canada. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Univ Quebec, Chicoutimi, PQ G7H 2B1, Canada. RP Stix, J (reprint author), McGill Univ, Dept Earth & Planetary Sci, 3450 Univ St, Montreal, PQ H3A 2A7, Canada. NR 36 TC 44 Z9 45 U1 1 U2 10 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 2003 VL 31 IS 4 BP 375 EP 378 DI 10.1130/0091-7613(2003)031<0375:CFPATO>2.0.CO;2 PG 4 WC Geology SC Geology GA 662CN UT WOS:000181928700022 ER PT J AU James, HF Ericson, PGP Slikas, B Lei, FM Gill, FB Olson, SL AF James, HF Ericson, PGP Slikas, B Lei, FM Gill, FB Olson, SL TI Pseudopodoces humilis, a misclassified terrestrial tit (Paridae) of the Tibetan Plateau: evolutionary consequences of shifting adaptive zones SO IBIS LA English DT Article ID DNA-DNA HYBRIDIZATION; MAJOR LINEAGES; SEQUENCE DATA; C-MYC; PHYLOGENY; PARUS; GENE; TITMICE; CHICKADEES; PATTERNS AB Pseudopodoces humilis (Hume's Ground-Jay) is a small passerine bird that inhabits the high rocky steppes of the Tibetan (Qinghai-Xizang) Plateau. Although it was long classified as a small species of ground jay (Podoces ), two previous anatomical studies cast doubt on its assignment to the Corvidae (crows and jays). We studied the evolutionary relationships of Pseudopodoces using three independent datasets drawn from comparative osteology, the nuclear c-myc gene, and the mitochondrial cytochrome b gene. All three datasets agree on the placement of Pseudopodoces in the family Paridae (tits and chickadees). The cytochrome b data further suggest that Pseudopodoces may be closest to the Great Tit Parus major species group. Pseudopodoces is the only species of parid whose distribution is limited to treeless terrain. Its evolutionary relationships were long obscured by adaptations to open habitat, including pale, cryptic plumage; a long, decurved bill for probing in crevices among rocks or in the ground; and long legs for terrestrial locomotion. Despite these accommodations to a novel adaptive zone, its evolutionary affinity with the Paridae is clearly expressed in comparative osteology and genetics, and is supported by its habit of nesting in cavities. C1 Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. Swedish Museum Nat Hist, Dept Vertebrate Zool, SE-10405 Stockholm, Sweden. Smithsonian Inst, Natl Zool Pk, Dept Res, Washington, DC 20008 USA. Chinese Acad Sci, Inst Zool, Beijing 100080, Peoples R China. Natl Audubon Soc, New York, NY 10003 USA. RP James, HF (reprint author), Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. RI Slikas, Beth/E-7275-2013 NR 51 TC 48 Z9 62 U1 3 U2 22 PU BRITISH ORNITHOLOGISTS UNION PI TRING PA C/O NATURAL HISTORY MUSEUM, SUB-DEPT ORNITHOLOGY, TRING HP23 6AP, HERTS, ENGLAND SN 0019-1019 J9 IBIS JI Ibis PD APR PY 2003 VL 145 IS 2 BP 185 EP 202 DI 10.1046/j.1474-919X.2003.00170.x PG 18 WC Ornithology SC Zoology GA 660JY UT WOS:000181831100007 ER PT J AU Chave, J Condit, R Lao, S Caspersen, JP Foster, RB Hubbell, SP AF Chave, J Condit, R Lao, S Caspersen, JP Foster, RB Hubbell, SP TI Spatial and temporal variation of biomass in a tropical forest: results from a large census plot in Panama SO JOURNAL OF ECOLOGY LA English DT Article DE above-ground biomass change; carbon cycle; dry living above-ground biomass; tropical rain forest ID NET PRIMARY PRODUCTION; BARRO-COLORADO ISLAND; RAIN-FOREST; CARBON-DIOXIDE; NEOTROPICAL FOREST; ATMOSPHERIC CO2; LOWLAND FOREST; AMAZON FOREST; TREE; GROWTH AB 1 We estimated the dry, living, above-ground biomass (AGB) standing stock and its turnover in a 50-hectare forest plot located in moist tropical forest on Barro Colorado Island, Panama. The estimates were obtained using inventory data collected every 5 years from 1985 to 2000, including measurements of all trees greater than or equal to 1 cm diameter. 2 Four different allometric regressions relating trunk diameter and height with AGB were compared. Based on the most consistent method, we estimated that the Barro Colorado forest holds 281 +/- 20 Mg ha(-1) (1 Mg = 10(3) kg) of AGB, lianas included. A third of the AGB is stored in trees larger than 70 cm in diameter. 3 Stand-level AGB increment (growth plus recruitment) was highest in the period 1985-90 (7.05 +/- 0.32 Mg ha(-1) year(-1) , mean +/- 95% confidence limits based on samples of multiple hectares) and smallest in the period 1990-95 (5.25 +/- 0.26 Mg ha(-1) year(-1)), while AGB losses were similar during the three intervals (mean 5.43 +/- 0.72 Mg ha(-1) year(-1)). This resulted in significant differences in AGB change (defined as increment minus loss) among census intervals; including branchfalls, the AGB of Barro Colorado Island increased in 1985-90 (+0.82 +/- 0.84 Mg ha(-1) year(-1)), decreased in 1990-95 (-0.69 +/- 0.82 Mg ha(-1) year(-1)), and increased again in 1995-2000 (+0.45 +/- 0.70 Mg ha(-1) year(-1)). The 15-year average was +0.20 Mg ha(-1) year(-1), but with a confidence interval that spanned zero (-0.68 to 0.63 Mg ha(-1) year(-1)). 4 Branchfalls and partial breakage of stems had a significant influence on the AGB changes. They contributed an average of 0.46 Mg ha(-1) year(-1) to the AGB loss. About 5% of AGB increment was due to trees less than 10 cm in diameter. 5 To test whether the AGB of tropical forests is increasing due to climate change, we propose that in each forest type, at least 10 hectares of forest be inventoried, and that measurements of the small classes (< 10 cm diameter) as well as large size classes be included. Biomass loss due to crown damage should also be estimated. C1 UPS, CNRS, Lab Evolut & Divers Biol, F-31062 Toulouse, France. Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. Smithsonian Inst, Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Washington, DC 20560 USA. Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada. Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. Univ Georgia, Dept Bot, Athens, GA 30602 USA. RP Chave, J (reprint author), UPS, CNRS, Lab Evolut & Divers Biol, 118 Route Narbonne Batiment IVR3, F-31062 Toulouse, France. NR 70 TC 187 Z9 219 U1 12 U2 65 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD APR PY 2003 VL 91 IS 2 BP 240 EP 252 DI 10.1046/j.1365-2745.2003.00757.x PG 13 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 662UT UT WOS:000181967800007 ER PT J AU Leckie, RM Huber, B AF Leckie, RM Huber, B TI 2002 Joseph A. Cushman Award - Isabella Premoli Silva SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Biographical-Item C1 Univ Massachusetts, Amherst, MA 01003 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Leckie, RM (reprint author), Univ Massachusetts, Amherst, MA 01003 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD APR PY 2003 VL 33 IS 2 BP 171 EP 172 DI 10.2113/0330171 PG 2 WC Paleontology SC Paleontology GA 694AR UT WOS:000183751000006 ER PT J AU von Sternberg, R Cumberlidge, N AF von Sternberg, R Cumberlidge, N TI Autapomorphies of the endophragmal system in trichodactylid freshwater crabs (Crustacea : Decapoda : Eubrachyura) SO JOURNAL OF MORPHOLOGY LA English DT Article DE freshwater crabs; Trichodactylidae; Eubrachyura; endophragmal system; sella turcica; interosternites; junction plate ID BRACHYURA AB An examination of the thoracic endophragmal system in trichodactylid freshwater crabs revealed several derived features that appear restricted to this family. Trichodactylids have a highly reduced sella turcica with a rim-like overall configuration; as a consequence of sella turcica reduction the median septum is dorsoventrally diminished and exposed along its length. In addition, interosternite 7/8 is medially erased with the remnants restricted to the lateral regions of the sternum. The configurations of the sella turcica and interosternite 7/8 in trichodactylids underscore the monophyly of this family. The Dilocarcininae is characterized by having interosternites 5/6 through 7/8 restricted to the lateral sectors of the sternum, the lateral remnants of interosternite 4/5 forming prominent, rib-like ridges oriented diagonally to the longitudinal axis of the crab, and the median septum forming with interosternite 4/5 a Y-shaped pattern. These autapomorphies of the endophragmal system separate the trichodactylids from all other eubrachyurans and emphasize the morphological distinctness of the group. A description of the trichodactylid endophragmal junction plate is also provided. (C) 2003 Wiley-Liss, Inc. C1 Smithsonian Inst, Dept Syst Biol, NHB 163, Washington, DC 20013 USA. No Michigan Univ, Dept Biol, Marquette, MI 49855 USA. RP von Sternberg, R (reprint author), NIH, NLM, Natl Ctr Biotechnol Informat, GenBank, Bethesda, MD 20894 USA. EM Sternber@ncbi.nlm.nih.gov; Sternberg.Richard@nmnh.si.edu NR 29 TC 6 Z9 7 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD APR PY 2003 VL 256 IS 1 BP 23 EP 28 DI 10.1002/jmor.10072 PG 6 WC Anatomy & Morphology SC Anatomy & Morphology GA 655NU UT WOS:000181559600003 PM 12616572 ER PT J AU Faust, MA AF Faust, MA TI Protoperidinium belizeanum sp nov (Dinophyceae) from Manatee Cay, Belize, Central America SO JOURNAL OF PHYCOLOGY LA English DT Article DE biodiversity; dinoflagellates; distribution; Dinophyceae; ecology; coral reef-mangrove pond; morphology; Protoperidinium belizeanum sp nov.; scanning electron microscopy; taxonomy AB A new marine heterotrophic dinoflagellate species, Protoperidinium belizeanum sp. nov., from a coral reef-mangrove pond was identified from scanning electron micrographs. Recognition of this new species was based on unique features of the thecal morphology, which included cell size and shape, presence of short and wide postcingular plates, sulcal architecture, antapical spines, and intricate thecal plate patterns of ridged hexagonal depressions. The thecal plate formula is as follows: Po, X, 4', 3a, 7', 4C (3+t), 6S, 5''', 2''''. Species association of P. belizeanum sp. nov. within the genus Protoperidinium , its habitat, and associated dinoflagellates species are discussed. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Bot, Suitland, MD 20746 USA. RP Faust, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Bot, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 32 TC 0 Z9 0 U1 0 U2 2 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD APR PY 2003 VL 39 IS 2 BP 390 EP 394 PG 5 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 660YB UT WOS:000181861800016 ER PT J AU Arneson, L Wcislo, WT AF Arneson, L Wcislo, WT TI Dominant-subordinate relationships in a facultatively social, nocturnal bee, Megalopta genalis (Hymenoptera : Halictidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE Halictidae; bees; dominance; agonism social behavior ID LASIOGLOSSUM-ZEPHYRUM; SOLITARY; EXPERIENCE; CONFLICT; COLONIES; FAMILIARITY; ENCOUNTERS; HIERARCHY; BEHAVIOR; SIZE AB The potential for the formation of social relationships was explored for the facultatively social halictine bee, Megalopta genalis, using experimental circular arenas, Observing pairs of females from different nests, we examined the initiation of agonistic behavior, and the expression and relative frequency of dominance behavior in terms of phenotypic differences betA been interacting bees. Within pairs, older females with relatively larger ovaries tended to be dominant over younger females with smaller ovaries, and females with fewer nest-mates tended to initiate agonistic interactions. Bees also modified their behavior over a 24-hour time frame and were more pacific when paired with the same bee in repeated trials. Our observations suggest that these predominantly solitary bees have the capabilities to express cooperative and social dominance behavior typical of the halictines A with obligate social behavior. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 52 TC 29 Z9 29 U1 1 U2 4 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD APR PY 2003 VL 76 IS 2 BP 183 EP 193 PG 11 WC Entomology SC Entomology GA 664XR UT WOS:000182090400013 ER PT J AU Norden, BB Krombein, KV Deyrup, MA Edirisinghe, JP AF Norden, BB Krombein, KV Deyrup, MA Edirisinghe, JP TI Biology and behavior of a seasonally aquatic bee, Perdita (Alloperdita) floridensis Timberlake (Hymenoptera : Andrenidae : Panurginae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE Andrenidae; bees; Florida; Ilex; Perdita; submerged nests ID NESTING BIOLOGY AB The small panurgine bee. Perdita Timberlake, nests in sand during mid-April to mid-May in south-central Florida. This species is solitary. but often nests gregariously in dense aggregations. It is univoltine, with some larvae delaying emergence by a year, and is oligolectic, primarily foraging on gallberry. Ilex glabra (L) Gray. Details of nest construction, foraging, pollen transport and provisions, activity periods. and male behaviors are described. Mating is presumed to occur within nests and was never observed on host plants. Bees over-wintered as post-defecated larvae (prepupae) in a semi-diapause. The biology and behaviors associated with a prolonged period ffi e to six months) underwater for some prepupae are detailed. and the possible oxygenating role of algae in their survival is discussed. Predators and parasites associated with P. floridensis include: the cleptoparasitic bee, Sphecodes brachycephalus Mitchell; two multillids, Pseudomethoca torrida Krombein and Dasymutilla archboldi Schmidt and Mickek an undetermined species of mite: the asilid fly. Mallophorina clausicella (Macquart) and the harvester ant, Pogonomyrmex badius (Latreille). In addition. an undetermined nematode species, and mosquitofish, Gambusia holbrooki Girard A ere associated with P. floridensis nest sites. C1 Smithsonian Inst, Entomol Sect, Dept Systemat Biol, Washington, DC 20560 USA. Univ Peradeniya, Dept Zool, Peradeniya, Sri Lanka. RP Norden, BB (reprint author), Smithsonian Inst, Entomol Sect, Dept Systemat Biol, Washington, DC 20560 USA. NR 24 TC 7 Z9 7 U1 0 U2 2 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD APR PY 2003 VL 76 IS 2 BP 236 EP 249 PG 14 WC Entomology SC Entomology GA 664XR UT WOS:000182090400019 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Renaissance rivals: Michelangelo, Leonardo, Raphael, Titian. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 1 PY 2003 VL 128 IS 6 BP 94 EP 94 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 673WP UT WOS:000182603500043 ER PT J AU Riley, S AF Riley, S TI Brown eyes blue. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 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 2003 VL 128 IS 6 BP 130 EP 130 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 673WP UT WOS:000182603500197 ER PT J AU Mair, RW Wang, R Rosen, MS Candela, D Cory, DG Walsworth, RL AF Mair, RW Wang, R Rosen, MS Candela, D Cory, DG Walsworth, RL TI Applications of controlled-flow laser-polarized xenon gas to porous and granular media study SO MAGNETIC RESONANCE IMAGING LA English DT Article; Proceedings Paper CT 6th International Conference on the Recent Advances in Magnetic Resonance Applications to Porous Media CY SEP 08-12, 2002 CL UNIV ULM, ULM, GERMANY HO UNIV ULM DE Xe-129; He-3; diffusion; gases; laser-polarization; porous media; gas flow; diffusive diffraction ID HYPERPOLARIZED NOBLE-GASES; TO-VOLUME RATIO; FIELD-GRADIENT; DIFFUSION NMR; FLUIDS; CONVECTION; TORTUOSITY; TRANSPORT; MOTION; ROCKS AB We report initial NMR studies of continuous flow laser-polarized xenon gas, both in unrestricted tubing, and in a model porous media. The study uses Pulsed Gradient Spin Echo-based techniques in the gas-phase, with the aim of obtaining more sophisticated information than just translational self-diffusion coefficients. Pulsed Gradient Echo studies of continuous flow laser-polarized xenon gas in unrestricted tubing indicate clear diffraction minima resulting from a wide distribution of velocities in the flow field. The maximum velocity experienced in the flow can be calculated from this minimum, and is seen to agree with the information from the complete velocity spectrum, or motion propagator, as well as previously published images. The susceptibility of gas flows to parameters such as gas mixture content, and hence viscosity, are observed in experiments aimed at identifying clear structural features from echo attenuation plots of gas flow in porous media. Gas-phase NMR scattering, or position correlation flow-diffraction, previously clearly seen in the echo attenuation data from laser-polarized xenon flowing through a 2 mm glass bead pack is not so clear in experiments using a different gas mixture. A propagator analysis shows most gas in the sample remains close to static, while a small portion moves through a presumably near-unimpeded path at high velocities. (C) 2003 Elsevier Science Inc. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Cambridge, MA 02139 USA. Univ Massachusetts, Amherst, MA 01003 USA. RP Mair, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 29 TC 11 Z9 11 U1 0 U2 5 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0730-725X J9 MAGN RESON IMAGING JI Magn. Reson. Imaging PD APR-MAY PY 2003 VL 21 IS 3-4 BP 287 EP 292 DI 10.1016/S0730-725X(03)00156-5 PG 6 WC Radiology, Nuclear Medicine & Medical Imaging SC Radiology, Nuclear Medicine & Medical Imaging GA 702DD UT WOS:000184205700020 PM 12850720 ER PT J AU Fukami, H Omori, M Shimoike, K Hayashibara, T Hatta, M AF Fukami, H Omori, M Shimoike, K Hayashibara, T Hatta, M TI Ecological and genetic aspects of reproductive isolation by different spawning times in Acropora corals SO MARINE BIOLOGY LA English DT Article ID MONTASTRAEA-ANNULARIS; EVOLUTIONARY HISTORY; GENUS ACROPORA; REEF; MITOCHONDRIAL; SCLERACTINIA; PATTERNS; CNIDARIA; COMPLEX AB In Okinawa, Japan, we found several species of the coral genus Acropora that spawn 1.5-3 h earlier than other mass-spawning acroporids. In six early-spawning species, gamete bundles appear on the surface of the colony ("setting") about 1 h before sunset, whereas setting occurs about 1 h after sunset in the more common late mass spawners. These early spawners are divided further into two sub-groups: three species that release their gametes within 1 h after setting and three that release their gametes 1.5-2 h after setting. DNA phylogenetic analyses show that each of these groups forms an independent genetic clade. These genetic relationships suggest that different spawning times form the basis of reproductive isolation among these broadcast-spawning corals. Late spawning appears to be the ancestral state, and the shift of spawning to earlier times may have played a role in the speciation process in these sympatric species. C1 Ochanomizu Univ, Dept Biol, Tokyo 1128610, Japan. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Akajima Marine Sci Lab, Okinawa, Zamami Son 9013311, Japan. Seikai Natl Fisheries Res Inst, Okinawa, Ishigaki 9070451, Japan. RP Hatta, M (reprint author), Ochanomizu Univ, Dept Biol, Tokyo 1128610, Japan. NR 21 TC 39 Z9 40 U1 1 U2 9 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD APR PY 2003 VL 142 IS 4 BP 679 EP 684 DI 10.1007/s00227-002-1001-8 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 681JF UT WOS:000183032500007 ER PT J AU Lazzati, D Perna, R AF Lazzati, D Perna, R TI Time-dependent photoionization in a dusty medium - III. The effect of dust on the photoionization of metals SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dust, extinction; gamma-rays : bursts; X-rays : general; X-rays : ISM ID GAMMA-RAY BURST; CROSS-SECTIONS; ABSORPTION; GRB-990705; EVOLUTION; SPECTRUM; NUCLEI AB We use the time-dependent photoionization and dust destruction code recently developed by Perna and Lazzati to study the time evolution of the medium in a dusty gaseous cloud illuminated by a bright central source that sets on at time zero. We study the case of a bright source, which lasts for a time-scale much smaller than the recombination and dust creation time-scales. For this reason an equilibrium is never reached. We show that the presence of dust and its properties, such as its composition, can have a big effect on the time-scale for the evaporation of the soft X-ray absorption, in particular for ionizing sources with hard spectra. We discuss the profile of evaporation of the soft X-ray absorbing column, as well as how the apparent ionization state of the cloud evolves in time. We finally consider the apparent metallicity of the cloud that is left behind as a function of the cloud and ionizing source properties. 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. EM lazzati@ast.cam.ac.uk; rperna@cfa.harvard.edu NR 29 TC 10 Z9 10 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 1 PY 2003 VL 340 IS 2 BP 694 EP 704 DI 10.1046/j.1365-8711.2003.06334.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658VG UT WOS:000181740700031 ER PT J AU Labandeira, CC AF Labandeira, CC TI Reading the tree leaves SO NATURAL HISTORY LA English DT Letter C1 Smithsonian Inst, Washington, DC 20560 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER MUSEUM NAT HISTORY PI NEW YORK PA ATTN: LIBRARY SERIALS UNIT CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0028-0712 J9 NAT HIST JI Nat. Hist. PD APR PY 2003 VL 112 IS 3 BP 13 EP 13 PG 1 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 656ZN UT WOS:000181641100011 ER PT J AU Lin, J Soon, W Baliunas, SL AF Lin, J Soon, W Baliunas, SL TI Theories of solar eruptions: a review SO NEW ASTRONOMY REVIEWS LA English DT Review DE the Sun; eruptions; theoretical mechanisms; MHD models; magnetic reconnection ID CORONAL MASS EJECTIONS; FREE MAGNETIC-FIELDS; POST-FLARE LOOPS; FLUX-ROPE MODELS; 29 JULY 1973; SOFT-X-RAY; PHOTOSPHERIC MOTIONS; MERIDIONAL PLANE; 2-RIBBON FLARES; EMERGING FLUX AB This review highlights current theoretical research on eruptive phenomena in the solar atmosphere. We start by looking back upon the early theories and their development. Any theory and model of solar eruptions must explain two key aspects of eruption physics. The first aspect concerns the original cause of the eruption and the second pertains to the nature of the morphological features that form during its evolution. Those features include rapid ejection of large-scale magnetic flux and plasma into interplanetary space, and the separating of ribbons of Ha emission on the solar disk joined by a rising arcade of soft X-ray and Ha loops, with hard X-ray emission at their summits and feet. We intercompare relevant theories and models by discussing their advantages as well as by pointing out important aspects that need improvement, (C) 2002 Elsevier Science B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jlin@cfa.harvard.edu RI LIN, JUN/B-9890-2017 NR 197 TC 119 Z9 125 U1 2 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD APR PY 2003 VL 47 IS 2 BP 53 EP 84 DI 10.1016/S1387-6473(02)00271-3 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 661WW UT WOS:000181913700001 ER PT J AU Lovelock, CE Andersen, K Morton, JB AF Lovelock, CE Andersen, K Morton, JB TI Arbuscular mycorrhizal communities in tropical forests are affected by host tree species and environment SO OECOLOGIA LA English DT Article DE Glomales; Acaulospora morrowiae; Acaulospora mellea; Acaulospora foveata ID HYACINTHOIDES NON-SCRIPTA; RAIN-FOREST; ENDOMYCORRHIZAL FUNGI; ROOT COLONIZATION; SPATIAL PATTERNS; PLANT DIVERSITY; ACER-SACCHARUM; SOIL PATHOGENS; DYNAMICS; INOCULUM AB Arbuscular mycorrhizal (AM) fungi are mutualists with plant roots that are proposed to enhance plant community diversity. Models indicate that AM fungal communities could maintain plant diversity in forests if functionally different communities are spatially separated. In this study we assess the spatial and temporal distribution of the AM fungal community in a wet tropical rainforest in Costa Rica. We test whether distinct fungal communities correlate with variation in tree life history characteristics, with host tree species, and the relative importance of soil type, seasonality and rainfall. Host tree species differ in their associated AM fungal communities, but differences in the AM community between hosts could not be generalized over life history groupings of hosts. Changes in the relative abundance of a few common AM fungal species were the cause of differences in AM fungal communities for different host tree species instead of differences in the presence and absence of AM fungal species. Thus, AM fungal communities are spatially distinguishable in the forest, even though all species are widespread. Soil fertility ranging between 5 and 9 Mg/ha phosphorus did not affect composition of AM fungal communities, although sporulation was more abundant in lower fertility soils. Sampling soils over seasons revealed that some AM fungal species sporulate profusely in the dry season compared to the rainy season. On one host tree species sampled at two sites with vastly different rainfall, relative abundance of spores from Acaulospora was lower and that of Glomus was relatively higher at the site with lower and more seasonal rainfall. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Illinois, Program Ecol & Evolut, Urbana, IL 61801 USA. W Virginia Univ, Div Plant & Soil Sci, Morgantown, WV 26506 USA. 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 NR 88 TC 69 Z9 78 U1 2 U2 34 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD APR PY 2003 VL 135 IS 2 BP 268 EP 279 DI 10.1007/s00442-002-1166-3 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 676LQ UT WOS:000182753900013 PM 12698349 ER PT J AU Currie, CR Bot, ANM Boomsma, JJ AF Currie, CR Bot, ANM Boomsma, JJ TI Experimental evidence of a tripartite mutualism: bacteria protect ant fungus gardens from specialized parasites SO OIKOS LA English DT Article ID LEAF-CUTTING ANTS; URINARY-TRACT INFECTIONS; GROWING ANTS; HYMENOPTERA; FORMICIDAE; EVOLUTION; COOPERATION; AGRICULTURE; STIMULATION; MAINTENANCE AB Symbioses shape all levels of biological organization. Although symbiotic interactions are typically viewed as bipartite associations, with two organisms interacting largely in isolation from other organisms, the presence and importance of additional symbionts is becoming increasingly more apparent. This study examines the importance of a third mutualist within the ancient symbiosis between leaf-cutting ants and their fungal cultivars. Specifically, we experimentally examine the role of a filamentous bacterium (actinomycete), which is typically carried on the cuticle of fungus-growing ants, in suppressing the growth of a specialized microfungal parasite (Escovopsis) of the fungus garden. We conducted two-by-two factorial design experiments crossing the presence/absence of actinomycete with the presence/absence of Escovopsis within small sub-colonies of Acromyrmex octospinosus. In these experiments, infection by Escovopsis became much more extensive within fungus gardens and had a greater impact on the health of gat-dens in those sub-colonies with the bacterium removed from workers as compared to gardens with the bacterium still present on the ants. We establish that the actinomycete bacterium is most abundant on those major workers tending the garden, providing further support that the bacterium is involved in garden hygiene. We also found a significantly higher abundance of actinomycete on workers in colonies experimentally infected with Escovopsis as compared to uninfected control colonies. We suggest that mutualisms between antibiotic-producing microbes and higher organisms may be common associations that are mostly overlooked and that the role of symbionts in reducing the impact of parasites is likely an important aspect in the cost-benefit assessment of mutualisms. C1 Univ Kansas, Dept Ecol & Evolut Biol, Lawrence, KS 66045 USA. Aarhus Univ, Dept Ecol & Genet, Inst Biol Sci, DK-8000 Aarhus C, Denmark. Univ Copenhagen, Inst Zool, Dept Populat Ecol, DK-2100 Copenhagen E, Denmark. Univ Toronto, Dept Bot, Toronto, ON M5S 3B2, Canada. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Currie, CR (reprint author), Univ Kansas, Dept Ecol & Evolut Biol, 1200 Sunnyside Ave, Lawrence, KS 66045 USA. EM ccurrie@ku.edu RI Boomsma, Jacobus/M-2785-2014 OI Boomsma, Jacobus/0000-0002-3598-1609 NR 61 TC 95 Z9 102 U1 2 U2 41 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0030-1299 J9 OIKOS JI Oikos PD APR PY 2003 VL 101 IS 1 BP 91 EP 102 DI 10.1034/j.1600-0706.2003.12036.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 665EL UT WOS:000182106600010 ER PT J AU Forrey, RC Jonsell, S Saenz, A Froelich, P Dalgarno, A AF Forrey, RC Jonsell, S Saenz, A Froelich, P Dalgarno, A TI Cold collisions of spin-polarized metastable hydrogen atoms SO PHYSICAL REVIEW A LA English DT Article AB Cross sections and rate coefficients for collisions of two spin-polarized metastable hydrogen atoms are calculated at low energies and temperatures using complex scaling and Feshbach projection methods for the determination of the molecular potential-energy curves. The inclusion of the Lamb shift and fine-structure splitting of the excited n=2 atoms leads to an attractive van der Waals potential for two 2s(1/2) atoms with an exceptionally large coefficient. The quenching of the metastable atoms is dominated at temperatures below 20 mK by ionization. The calculated values for the total loss rate coefficient at 87 muK and 230 muK are within a factor of 2 or 3 of the error bars of recent measurements of metastable loss rate coefficients. C1 Penn State Univ, Berks Lehigh Valley Coll, Reading, PA 19610 USA. Umea Univ, Dept Phys, SE-90187 Umea, Sweden. Univ Konstanz, Fachbereich Chem, D-78457 Constance, Germany. Univ Uppsala, Dept Quantum Chem, S-75120 Uppsala, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Forrey, RC (reprint author), Penn State Univ, Berks Lehigh Valley Coll, Reading, PA 19610 USA. RI Jonsell, Svante/J-2251-2016 OI Jonsell, Svante/0000-0003-4969-1714 NR 10 TC 9 Z9 10 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD APR PY 2003 VL 67 IS 4 AR 040701 DI 10.1103/PhysRevA.67.040701 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 673WY UT WOS:000182604300005 ER PT J AU Moore, MG Sadeghpour, HR AF Moore, MG Sadeghpour, HR TI Controlling two-species Mott-insulator phases in an optical lattice to form an array of dipolar molecules SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; BOSONIC ATOMS; FORCES AB We consider the transfer of a two-species Bose-Einstein condensate (BEC) into an optical lattice with a density such that a Mott-insulator state with one atom per species per lattice site is obtained in a deep lattice regime. Depending on collisional and transition parameters, the result could be either a "mixed" or a "separated" Mott-insulator phase. Such a mixed two-species insulator would be well suited for the formation of dipolar molecules via photoassociation. The resulting array of dipolar molecules could then be used for the formation of a dipolar molecular condensate or for computation. For the case of a Rb-87-K-41 two-species BEC, however, the large interspecies scattering length makes it difficult to obtain the desired mixed Mott-insulator phase. To overcome this difficulty, we investigate the effect of varying the lattice frequency on the mean-field interaction and propose a favorable parameter regime, under which a lattice of dipolar molecules could be generated. 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. NR 19 TC 21 Z9 22 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 2003 VL 67 IS 4 AR 041603 DI 10.1103/PhysRevA.67.041603 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 673WY UT WOS:000182604300013 ER PT J AU Zygelman, B Dalgarno, A Jamieson, MJ Stancil, PC AF Zygelman, B Dalgarno, A Jamieson, MJ Stancil, PC TI Multichannel study of spin-exchange and hyperfine-induced frequency shift and line broadening in cold collisions of hydrogen atoms SO PHYSICAL REVIEW A LA English DT Article ID CROSS-SECTIONS; GROUND-STATE; LOW-TEMPERATURES; SCATTERING; MASER; ENERGIES; MOLECULE; RECOMBINATION; IONIZATION; OXYGEN AB We calculate the cross sections that characterize the frequency shift and broadening of the resonance magnetic hyperfine transition in atomic hydrogen due to collisions with hydrogen atoms in a masing cavity. We consider collision energies that correspond to the temperature range, 10 mK delay 3 days, suggesting that submillimeter wavelengths tend to peak first. Only marginal day-to-day variations in flux density (2- 3 sigma) have been detected at 1.3 mm. No significant flares on a short timescale (similar to1 hr) have been observed at 1.3 mm. We also failed to detect significant periodic signals at a level of 5% (3 sigma) from Sgr A* in a periodic searching window ranging from 10 minutes to 2.5 hr. The flares observed at the wavelengths between short-centimeter and submillimeter might be a result of collective mass ejections associated with X-ray flares that originate from the inner region of the accretion disk near the supermassive black hole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM jzhao@cfa.harvard.edu; kyoung@cfa.harvard.edu; rmcgary@cfa.harvard.edu; pho@cfa.harvard.edu; ttsutsumi@cfa.harvard.edu; flo@nrao.edu; mgoss@aoc.nrao.edu; gbower@astron.berkeley.edu NR 28 TC 79 Z9 80 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 20 PY 2003 VL 586 IS 1 BP L29 EP L32 DI 10.1086/374581 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 653RX UT WOS:000181451800007 ER PT J AU Palmer, PI Jacob, DJ Fiore, AM Martin, RV Chance, K Kurosu, TP AF Palmer, PI Jacob, DJ Fiore, AM Martin, RV Chance, K Kurosu, TP TI Mapping isoprene emissions over North America using formaldehyde column observations from space SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Isoprene; Formaldehyde; GOME; biogenic emissions; satellite instrument; volatile organic compounds ID VOLATILE ORGANIC-COMPOUNDS; OZONE MONITORING EXPERIMENT; SOUTHEASTERN UNITED-STATES; CARBONYL-COMPOUNDS; ATMOSPHERIC CHEMISTRY; TRANSPORT; OXIDATION; MECHANISM; MODEL; GOME AB [1] We present a methodology for deriving emissions of volatile organic compounds (VOC) using space-based column observations of formaldehyde ( HCHO) and apply it to data from the Global Ozone Monitoring Experiment (GOME) satellite instrument over North America during July 1996. The HCHO column is related to local VOC emissions, with a spatial smearing that increases with the VOC lifetime. Isoprene is the dominant HCHO precursor over North America in summer, and its lifetime (similar or equal to1 hour) is sufficiently short that the smearing can be neglected. We use the Goddard Earth Observing System global 3-D model of tropospheric chemistry (GEOS-CHEM) to derive the relationship between isoprene emissions and HCHO columns over North America and use these relationships to convert the GOME HCHO columns to isoprene emissions. We also use the GEOS-CHEM model as an intermediary to validate the GOME HCHO column measurements by comparison with in situ observations. The GEOS-CHEM model including the Global Emissions Inventory Activity (GEIA) isoprene emission inventory provides a good simulation of both the GOME data (r(2) = 0.69, n = 756, bias = + 11%) and the in situ summertime HCHO measurements over North America (r(2) = 0.47, n = 10, bias = -3%). The GOME observations show high values over regions of known high isoprene emissions and a day-to-day variability that is consistent with the temperature dependence of isoprene emission. Isoprene emissions inferred from the GOME data are 20% less than GEIA on average over North America and twice those from the U. S. EPA Biogenic Emissions Inventory System (BEIS2) inventory. The GOME isoprene inventory when implemented in the GEOS-CHEM model provides a better simulation of the HCHO in situ measurements than either GEIA or BEIS2 (r(2) = 0.71, n = 10, bias = -10%). C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Atom Div, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Div Mol Phys, Cambridge, MA 02138 USA. RP Palmer, PI (reprint author), Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. EM pip@io.harvard.edu RI Martin, Randall/A-2051-2008; Palmer, Paul/F-7008-2010; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; NR 48 TC 181 Z9 181 U1 6 U2 34 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 20 PY 2003 VL 108 IS D6 AR 4180 DI 10.1029/2002JD002153 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 667GK UT WOS:000182222800002 ER PT J AU Marshall, D Groat, L Giuliani, G Murphy, D Mattey, D Ercit, TS Wise, MA Wengzynowski, W Eaton, WD AF Marshall, D Groat, L Giuliani, G Murphy, D Mattey, D Ercit, TS Wise, MA Wengzynowski, W Eaton, WD TI Pressure, temperature and fluid conditions during emerald precipitation, southeastern Yukon, Canada: fluid inclusion and stable isotope evidence SO CHEMICAL GEOLOGY LA English DT Article; Proceedings Paper CT 16th Biennial European Current Research on Fluid Inclusions (ECROFI) CY MAY 02-06, 2001 CL OPORTO, PORTUGAL SP Fluids & Metallog Team, GIMEF, Dept Geol, Univ Porto Ctr Geol DE fluid inclusions; stable isotopes; emerald; thermobarometry; Yukon ID OXYGEN-ISOTOPE; H2O-CO2-NACL FLUIDS; SOUTH-AFRICA; MINERALIZATION; EVOLUTION; SYSTEM; FRACTIONATION; TRANSVAAL; EQUATION; COLOMBIA AB The Crown emerald veins are somewhat enigmatic, displaying characteristics that are common to emerald deposits of tectonic-hydrothermal origin and of igneous origin. The veins cut the Fire Lake mafic meta-volcanic rocks, occurring within 600 m of an outcrop of Cretaceous S-type granite. Field work and vein petrography are consistent with a polythermal origin for the veins. The primary vein mineralogy is quartz and tourmaline with variable sized alteration haloes consisting of tourmaline, quartz, muscovite, chlorite and emerald. The veins weather a buff brown colour due to jarosite, scheelite and minor lepidocrocite, which were precipitated during the waning stages of vein formation. Microthermometic studies of primary fluid inclusions within emerald growth zones are consistent with emerald precipitation from H2O-CO2-CH4 ( +/- N-2 +/- H2S) bearing saline brines. The estimated fluid composition is approximately 0.9391 mol% H2O, 0.0473 mol% CO2, 0.0077 mol% CH4 and 0.0059 mol% NaCl ( similar to 2 wt.% NaCl eq.). Fluid inclusion and stable isotope studies are consistent with vein formation in the temperature range 365-498 T, with corresponding pressures along fluid inclusion isochore paths ranging from 700 to 2250 bars. These data correlate with a very slow uplift rate for the region of 0.02-0.07 mm/year. Emerald deposits are generally formed when geological conditions bring together Cr (+/- V) and Be. Cr and V are presumed to have been derived locally from the mafic and ultramafic rocks during hydrothermal alteration. The Be is most likely derived from the nearby Cretaceous granite intrusion. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Simon Fraser Univ, Dept Earth Sci, Burnaby, BC V5A 1S6, Canada. Univ British Columbia, Vancouver, BC V6T 1Z4, Canada. Ctr Rech Petrog & Geochim, UPR A 6821, F-54501 Vandoeuvre Les Nancy, France. Govt Yukon, Yukon Geol Program, Whitehorse, YT Y1A 2C6, Canada. Univ London, Dept Geol, Egham TW20 OEX, Surrey, England. Canadian Museum Nat, Div Res, Ottawa, ON K1P 6P4, Canada. Smithsonian Inst, Mineral Sci NHB119, Washington, DC 20560 USA. Expatriate Resources Ltd, Vancouver, BC V6B 1L8, Canada. Archer Cathro & Associates 1981 Ltd, Vancouver, BC V6B 1L8, Canada. RP Marshall, D (reprint author), Simon Fraser Univ, Dept Earth Sci, Burnaby, BC V5A 1S6, Canada. NR 35 TC 8 Z9 9 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 J9 CHEM GEOL JI Chem. Geol. PD MAR 15 PY 2003 VL 194 IS 1-3 BP 187 EP 199 AR PII S0009-2541(02)00277-2 DI 10.1016/S0009-2541(02)00277-2 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 654RH UT WOS:000181509500011 ER PT J AU Schroll, S AF Schroll, S TI Mondrian, 1892-1914: The path to abstraction. SO LIBRARY JOURNAL LA English DT Book Review C1 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 MAR 15 PY 2003 VL 128 IS 5 BP 80 EP 80 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 672LZ UT WOS:000182523300025 ER PT J AU Doherty, M Johnston, S Green, AJ Roberts, MSE Romani, RW Gaensler, BM Crawford, F AF Doherty, M Johnston, S Green, AJ Roberts, MSE Romani, RW Gaensler, BM Crawford, F TI A search for the radio counterpart of the unidentified gamma-ray source 3EG J1410-6147 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE pulsars : individual : J1412-6145; pulsars : individual : J1413-6141 ID GALACTIC PLANE SURVEY; SUPERNOVA REMNANT; INNER GALAXY; YOUNG PULSAR; MILKY-WAY; H-I; EMISSION; G312.4-0.4; DISCOVERY; SPECTRUM AB We have made radio continuum, H I and X-ray observations in the direction of the unidentified EGRET source 3EG J1410-6147, using the Australia Telescope Compact Array and the Chandra X-ray Observatory. The observations encompass the supernova remnant (SNR) G312.4-0.4 and the two young pulsars PSRs J1412-6145 and J1413-6141. We derive a lower distance limit of 6 kpc to the SNR, although interpretation of positive velocity features in the H I spectrum may imply that the SNR is more distant than 14 kpc. PSR J1412-6145, with an age of 50 kyr, is the pulsar most probably associated with SNR G312.4-0.4. X-rays are not detected from either pulsar and diffuse X-ray emission near the bright western edge of the SNR is weak. Although there is circumstantial evidence that this western region is a pulsar wind nebula (PWN), the embedded pulsar PSR J1412-6145 is apparently not sufficiently powerful to explain the radio enhancement. The origin of the electron acceleration in this region and of the gamma-rays remains unidentified, unless the distance to PSR J1413-6141 is at least a factor of 3 lower than its dispersion measure distance. C1 Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Stanford Univ, Dept Phys, Stanford, CA 94025 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Haverford Coll, Dept Phys, Haverford, PA 19041 USA. RP Doherty, M (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM md@ast.cam.ac.uk RI Gaensler, Bryan/F-8655-2010 NR 37 TC 11 Z9 11 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 11 PY 2003 VL 339 IS 4 BP 1048 EP 1056 DI 10.1046/j.1365-8711.2003.06265.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650VD UT WOS:000181283300016 ER PT J AU Perna, R Lazzati, D Fiore, F AF Perna, R Lazzati, D Fiore, F TI Time-dependent photoionization in a dusty medium. II. Evolution of dust distributions and optical opacities SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : ISM ID GAMMA-RAY BURST; ACTIVE GALACTIC NUCLEI; X-RAY; ABSORPTION; DESTRUCTION; SPECTRUM; GRAINS; ENVIRONMENTS; CONSTRAINTS; AFTERGLOWS AB The interaction of a radiation field with a dusty medium is a relevant issue in several astrophysical contexts. We use the time-dependent photoionization code in a dusty medium developed by Perna & Lazzati to study the modi cations in the dust distribution and the relative optical opacities when a strong X-ray/UV radiation flux propagates into a medium. We find that silicates are preferentially destroyed with respect to graphite, and the extinction curve becomes significantly flatter (hence implying less reddening), with the characteristic bump at 2175 Angstrom being highly suppressed because of the destruction of the small graphite grains. This could explain the observational lack of such a feature in gamma-ray burst afterglow and active galactic nuclei spectra. For a very intense and highly variable source irradiating a compact and dense region, time variability in the optical opacity resulting from dust destruction can be observed on a relatively short timescale. We show that, under these circumstances, monitoring the time variability of the opacity can yield powerful clues to the properties of dust in the environment of the source. In particular, it allows one to break the observational degeneracy as to whether a gray extinction is the result of a low dust-to-gas ratio or of a dust grain distribution that is skewed toward large grains. C1 Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Osserv Astron Roma, I-00040 Rome, Italy. RP Perna, R (reprint author), Harvard Soc Fellows, 74 Mt Auburn St, Cambridge, MA 02138 USA. OI Fiore, Fabrizio/0000-0002-4031-4157 NR 29 TC 68 Z9 68 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 2003 VL 585 IS 2 BP 775 EP 784 DI 10.1086/346109 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650WU UT WOS:000181287200019 ER PT J AU Li, D Goldsmith, PF AF Li, D Goldsmith, PF TI HI narrow self-absorption in dark clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : atoms; ISM : clouds; ISM : molecules; radio lines : ISM ID WARM NEUTRAL HALOS; CARBON-MONOXIDE ABUNDANCE; MOLECULAR CLOUDS; INTERSTELLAR GAS; ATOMIC-HYDROGEN; MAGNETIC-FIELD; I OBSERVATIONS; MASSIVE CLOUD; LINE EMISSION; CORES AB We have used the Arecibo telescope to carry out a survey of 31 dark clouds in the Taurus/Perseus region for narrow absorption features in H I (21 cm) and OH (1667 and 1665 MHz) emission. We detected H I narrow self-absorption (HINSA) in 77% of the clouds that we observed. HINSA and OH emission, observed simultaneously, are remarkably well correlated. Spectrally, they have the same nonthermal line width and the same line centroid velocity. Spatially, they both peak at the optically selected central position of each cloud, and both fall off toward the cloud edges. Sources with clear HINSA features have also been observed in transitions of CO, (CO)-C-13, (CO)-O-18, and C I. HINSA exhibits better correlation with molecular tracers than with C I. The line width of the absorption feature, together with analyses of the relevant radiative transfer, provides upper limits to the kinetic temperature of the gas producing the HINSA. Some sources must have a temperature close to or lower than 10 K. The correlation of column densities and line widths of HINSA with those characteristics of molecular tracers suggests that a significant fraction of the atomic hydrogen is located in the cold, well-shielded portions of molecular clouds and is mixed with the molecular gas. The average number density ratio [H I] / [H-2] is 1.5 x 10(-3). The inferred H I density appears consistent with, but slightly higher than, the value expected in steady state equilibrium between formation of H I via cosmic-ray destruction of H-2 and destruction via formation of H-2 on grain surfaces. The distribution and abundance of atomic hydrogen in molecular clouds are critical tests of dark cloud chemistry and structure, including the issues of grain surface reaction rates, PDRs, circulation, and turbulent diffusion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Cornell Univ, Dept Astron, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. RP Li, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Goldsmith, Paul/H-3159-2016 NR 66 TC 66 Z9 67 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 10 PY 2003 VL 585 IS 2 BP 823 EP 839 DI 10.1086/346227 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650WU UT WOS:000181287200022 ER PT J AU Redfield, S Ayres, TR Linsky, JL Ake, TB Dupree, AK Robinson, RD Young, PR AF Redfield, S Ayres, TR Linsky, JL Ake, TB Dupree, AK Robinson, RD Young, PR TI A Far Ultraviolet Spectroscopic Explorer survey of coronal forbidden lines in late-type stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : profiles; stars : coronae; stars : late-type; ultraviolet : stars; X-rays : stars ID HIGH-RESOLUTION SPECTROGRAPH; OBSERVING STELLAR CORONAE; X-RAY-EMISSION; A-TYPE STARS; ROTATIONAL VELOCITIES; RADIAL-VELOCITIES; TRANSITION REGION; HERTZSPRUNG GAP; BINARY-SYSTEM; CAPELLA AB We present a survey of coronal forbidden lines detected in Far Ultraviolet Spectroscopic Explorer (FUSE) spectra of nearby stars. Two strong coronal features, Fe XVIII lambda974 and Fe XIX lambda1118, are observed in 10 of the 26 stars in our sample. Various other coronal forbidden lines, observed in solar ares, also were sought but not detected. The Fe XVIII feature, formed at log T = 6 : 8 K, appears to be free of blends, whereas the Fe XIX line can be corrupted by a C I multiplet. FUSE observations of these forbidden iron lines at spectral resolution = lambda/Deltalambda similar to 15,000 provides the opportunity to study dynamics of hot coronal plasmas. We find that the velocity centroid of the Fe XVIII feature deviates little from the stellar rest frame, confirming that the hot coronal plasma is confined. The observed line widths generally are consistent with thermal broadening at the high temperatures of formation and show little indication of additional turbulent broadening. The fastest rotating stars, 31 Com, alpha Aur Ab, and AB Dor, show evidence for excess broadening beyond the thermal component and the photospheric v sin i. The anomalously large widths in these fast-rotating targets may be evidence for enhanced rotational broadening, consistent with emission from coronal regions extending an additional DeltaR similar to 0.4-1.3 R-* above the stellar photosphere, or represent the turbulent broadening caused by flows along magnetic loop structures. For the stars in which Fe XVIII is detected, there is an excellent correlation between the observed Rontgensatellit (ROSAT) 0.2-2.0 keV soft X-ray flux and the coronal forbidden line flux. As a result, Fe XVIII is a powerful new diagnostic of coronal thermal conditions and dynamics that can be utilized to study high-temperature plasma processes in late-type stars. In particular, FUSE provides the opportunity to obtain observations of important transition region lines in the far-UV, as well as simultaneous measurements of soft X-ray coronal emission, using the Fe XVIII coronal forbidden line. C1 Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Natl Inst Stand & Technol, Boulder, CO 80309 USA. Univ Colorado, CASA, Boulder, CO 80309 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. RP Redfield, S (reprint author), Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. OI Redfield, Seth/0000-0003-3786-3486 NR 54 TC 39 Z9 39 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2003 VL 585 IS 2 BP 993 EP 1006 DI 10.1086/346129 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650WU UT WOS:000181287200037 ER PT J AU Uzzo, M Ko, YK Raymond, JC Wurz, P Ipavich, FM AF Uzzo, M Ko, YK Raymond, JC Wurz, P Ipavich, FM TI Elemental abundances for the 1996 streamer belt SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : abundances; Sun : corona ID SLOW SOLAR-WIND; ULTRAVIOLET CORONAGRAPH SPECTROMETER; SOURCE REGIONS; SOHO; MINIMUM; ORIGIN; TEMPERATURE; TELESCOPE; UVCS/SOHO; LINES AB The purpose of this paper is to explore the observed physical characteristics of the solar corona streamer belt from 1996 June 1 to August 5. The UV spectral data was collected by the Ultraviolet Coronagraph Spectrometer (UVCS) instrument on board the Solar and Heliospheric Observatory (SOHO) spacecraft. From this data the abundances of oxygen, silicon, and magnesium were determined on an almost daily basis during this time period at both the west and east limbs. The streamer belt was composed of both active and quiescent streamers, which allows for the comparison of these two categories of magnetic field structures. The depletion of these three elemental abundances in the core of quiescent streamers was found, as in previous observations. The variance in abundance with solar rotation was investigated as a consequence of the long time frame considered here. The first ionization potential (FIP) effect was present in the data, and the danger of exploring this phenomena by the traditional FIP bias was also covered. A comparison with in situ elemental abundance data from the Charge, Element, and Isotope Analysis System (CELIAS) instrument on SOHO provides evidence suggesting that active-region streamers and the outer leg structural component of quiescent streamers are definite contributors to the slow solar wind. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. Univ Maryland, College Pk, MD 20742 USA. RP Uzzo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 32 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 10 PY 2003 VL 585 IS 2 BP 1062 EP 1072 DI 10.1086/346132 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650WU UT WOS:000181287200043 ER PT J AU Hasan, SS Kalkofen, W van Ballegooijen, AA Ulmschneider, P AF Hasan, SS Kalkofen, W van Ballegooijen, AA Ulmschneider, P TI Kink and longitudinal oscillations in the magnetic network on the Sun: Nonlinear effects and mode transformation SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; Sun : magnetic fields; Sun : oscillations ID SOLAR TRANSITION REGION; STELLAR CONVECTION ZONES; PHOTOSPHERIC FLUX TUBES; ENERGY-BALANCE; INTERNETWORK OSCILLATIONS; SUMER OBSERVATIONS; TRANSVERSE WAVES; ATMOSPHERE; CHROMOSPHERE; GENERATION AB We examine the propagation of kink and longitudinal waves in the solar magnetic network. Previously, we investigated the excitation of network oscillations in vertical magnetic flux tubes through buffeting by granules and found that footpoint motions of the tubes can generate sufficient wave energy for chromospheric heating. We assumed that the kink and longitudinal waves are decoupled and linear. We overcome these limitations by treating the nonlinear MHD equations for coupled kink and longitudinal waves in a thin flux tube. For the parameters we have chosen, the thin tube approximation is valid up to the layers of formation of the emission features in the H and K lines of Ca II at a height of about 1 Mm. By solving the nonlinear, time-dependent MHD equations we are able to study the onset of wave coupling, which occurs when the Mach number of the kink waves is of the order of 0.3. We also investigate the transfer of energy from the kink to the longitudinal waves, which is important for the dissipation of the wave energy in shocks. We find that kink waves excited by footpoint motions of a flux tube generate longitudinal modes by mode coupling. For subsonic velocities, the amplitude of a longitudinal wave increases as the square of the amplitude of the transverse wave, and for amplitudes near Mach number unity, the coupling saturates and becomes linear when the energy is nearly evenly divided between the two modes. C1 Indian Inst Astrophys, Bangalore 560034, Karnataka, India. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Theoret Astrophys, D-69012 Heidelberg, Germany. RP Indian Inst Astrophys, Bangalore 560034, Karnataka, India. RI Hasan, Siraj/C-2927-2012; OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 52 TC 38 Z9 38 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 2003 VL 585 IS 2 BP 1138 EP 1146 DI 10.1086/346102 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 650WU UT WOS:000181287200049 ER PT J AU Bunyavejchewin, S LaFrankie, JV Baker, PJ Kanzaki, M Ashton, PS Yamakura, T AF Bunyavejchewin, S LaFrankie, JV Baker, PJ Kanzaki, M Ashton, PS Yamakura, T TI Spatial distribution patterns of the dominant canopy dipterocarp species in a seasonal dry evergreen forest in western Thailand SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE spatial patterns; dipterocarps; Thailand ID TROPICAL TREE; NEOTROPICAL FOREST; RAIN-FOREST; DIVERSITY; SEEDLINGS; DISPERSAL; DENSITY AB Population structure and spatial patterns were examined for four species of canopy dipterocarps (Anisoptera costata, Dipterocarpus alatus, Hopea odorata, Vatica cinerea) in a 50 ha plot in seasonal dry evergreen forest at the Huai Kha Khaeng Wildlife Sanctuary in western Thailand. Spatial dispersion was assessed with Morisita's index for quadrat sizes ranging from 61 m(2) to 25 ha; spatial attraction and repulsion between species and size classes were measured with Iwao's index. Only Vatica had a negative exponential diameter distribution suggesting continuous recruitment. The other species had either normal (Hopea) or irregular diameter distributions with peaks in the large size classes (Anisoptera, Dipterocarpus). All four species were significantly clumped at most quadrat sizes. At the local scale, saplings and poles of Hopea and Anisoptera were negatively associated with adults at quadrat sizes <1000-5000 m(2), while the distributions of Dipterocarpus and Vatica saplings and poles were independent of adult trees. In general, saplings and poles were always positively associated with each other. Spatial segregation among species may imply habitat specialization. A torus-translation analysis of habitat association for each of the dipterocarp species revealed both positive and negative species- specific associations. At HKK,most of the dipterocarps' spatial distributions were independent of each other and there was no evidence of strong spatial segregation among species. The irregular diameter distributions, clumping at large spatial scales, and lack of positive association between juvenile and adult stems suggest that many of the dipterocarps at the 50 ha plot may have established after a large-scale catastrophic disturbance. In the absence of catastrophic disturbance, we hypothesize that the Hopea and Anisoptera populations will eventually disappear from the plot because of a lack of suitable recruitment conditions. (C) 2002 Elsevier Science B.V. All rights reserved. C1 Royal Thai Forest Dept, Silvicultural Res Div, Forest Res Off, Bangkok 10900, Thailand. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Singapore 1025, Singapore. Univ Washington, Coll Forest Resources, Seattle, WA 98195 USA. Kyoto Univ, Grad Sch Agr, Kyoto 6068502, Japan. Harvard Univ, Arnold Arboretum, Cambridge, MA 02138 USA. Osaka City Univ, Fac Sci, Dept Biol, Sumiyoshi Ku, Osaka 5588585, Japan. RP Baker, PJ (reprint author), US Forest Serv, USDA, Pacific SW Res Stn, Inst Pacific Isl Forestry, 23 E Kawili St, Hilo, HI 96720 USA. OI Baker, Patrick/0000-0002-6560-7124 NR 38 TC 41 Z9 50 U1 4 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAR 3 PY 2003 VL 175 IS 1-3 BP 87 EP 101 AR PII S0378-1127(02)00126-3 DI 10.1016/S0378-1127(02)00126-3 PG 15 WC Forestry SC Forestry GA 654NY UT WOS:000181504000006 ER PT J AU Oliver, JE Weldon, PJ Petersen, KS Schmidt, WF Debboun, M AF Oliver, JE Weldon, PJ Petersen, KS Schmidt, WF Debboun, M TI Mosquito-deterring acid from pelage of gaur, Bos gaurus. SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 225th National Meeting of the American-Chemical-Society CY MAR 23-27, 2003 CL NEW ORLEANS, LA SP Amer Chem Soc C1 USDA ARS, BARC W, Chem Affecting Insect Behav Lab, Beltsville, MD 20705 USA. Smithsonian Inst, Conservat & Res Ctr, Washington, DC 20560 USA. USDA ARS, NRI, Environm Chem Lab, Washington, DC 20250 USA. EM oliverj@ba.ars.usda.gov NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR PY 2003 VL 225 MA AGFD-030 BP U73 EP U73 PN 1 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 761PU UT WOS:000187917800243 ER PT J AU Tuross, N AF Tuross, N TI Twilight zone of the fossilization process. SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 225th National Meeting of the American-Chemical-Society CY MAR 23-27, 2003 CL NEW ORLEANS, LA SP Amer Chem Soc C1 Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20740 USA. EM ntuross@lab.si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR PY 2003 VL 225 MA 131-GEOC BP U932 EP U932 PN 1 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 761PU UT WOS:000187917804336 ER PT J AU Kreamer, CM AF Kreamer, CM TI A tribute to Roy Sieber (Shaping the discipline of African art history) SO AFRICAN ARTS LA English DT Article C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. RP Kreamer, CM (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SPR PY 2003 VL 36 IS 1 BP 12 EP + PG 0 WC Art SC Art GA 721TH UT WOS:000185333100003 ER PT J AU Paerl, HW Steppe, TF Buchan, KC Potts, M AF Paerl, HW Steppe, TF Buchan, KC Potts, M TI Hypersaline cyanobacterial mats as indicators of elevated tropical hurricane activity and associated climate change SO AMBIO LA English DT Article ID BASIN AB The Atlantic hurricanes of 1999 caused widespread environmental damage throughout the Caribbean and US mid-Atlantic coastal regions. However, these storms also proved beneficial to certain microbial habitats; specifically, cyanobacteria-dominated mats. Modern mats represent the oldest known biological communities on earth, stromatolites. Contemporary mats are dominant biological communities in the hypersaline Bahamian lakes along the Atlantic hurricane track. We examined the impacts of varying levels of hypersalinity on 2 processes controlling mat growth, photosynthesis and nitrogen fixation, in Salt Pond, San Salvador Island, Bahamas. Hypersalinity (> 5 times sea-water salinity) proved highly inhibitory to these processes. Freshwater input from Hurricane Floyd and other large storms alleviated this salt-inhibition. A predicted 10 to 40 year increase in Atlantic hurricane activity accompanied by more frequent "freshening" events will enhance mat productivity, CO2 sequestration and nutrient cycling. Cyanobacterial mats are sensitive short- and long-term indicators of climatic and ecological changes impacting these and other waterstressed environments. C1 Univ N Carolina, Inst Marine Sci, Morehead City, NC 28557 USA. Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Virginia Tech, Ctr Genom, Blacksburg, VA USA. RP Paerl, HW (reprint author), Univ N Carolina, Inst Marine Sci, 3431 Arendell St, Morehead City, NC 28557 USA. NR 23 TC 20 Z9 20 U1 2 U2 10 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0044-7447 J9 AMBIO JI Ambio PD MAR PY 2003 VL 32 IS 2 BP 87 EP 90 DI 10.1639/0044-7447(2003)032[0087:HCMAIO]2.0.CO;2 PG 4 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 677GN UT WOS:000182798700003 PM 12733791 ER PT J AU Ryan, MJ Rand, W Hurd, PL Phelps, SM Rand, AS AF Ryan, MJ Rand, W Hurd, PL Phelps, SM Rand, AS TI Generalization in response to mate recognition signals SO AMERICAN NATURALIST LA English DT Article DE generalization gradients; mate recognition; preference functions; sexual selection; species recognition; tungara frogs ID FEMALE MATING PREFERENCES; PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; TUNGARA FROGS; ADVERTISEMENT CALLS; SPECIES RECOGNITION; NEOTROPICAL FROG; NEURAL NETWORKS; HYLA-EBRACCATA; OLFACTORY CUES AB Females usually exhibit strong and unequivocal recognition of conspecific mating signals and reject those of other sympatric heterospecifics. However, most species are allopatric with one another, and the degree to which females recognize mating signals of allopatric species is more varied. Such mating signals are often rejected but are sometimes falsely recognized as conspecific. We studied the dynamics of mate recognition in female tungara frogs (Physalaemus pustulosus) in response to a series of calls that were intermediate between the conspecific and each of five allopatric-heterospecific calls: two that elicited recognition from females in previous studies and three that did not. This study shows that females perceive variation in allopatric mating signals in a continuous manner with no evidence of perceptual category formation. The strength of recognition is predicted by how different the target stimulus is from the conspecific call within a series of calls. But the differences in recognition responses among call series are not predicted by the similarity of the call series to the conspecific call. The latter result suggests that the strength of recognition of allopatric signals might be influenced by processes of stimulus generalization and past evolutionary history. C1 Univ Texas, Ctr Integrated Biol C0930, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Tufts Univ, Sch Med, Dept Community Hlth, Boston, MA 02111 USA. Univ Alberta, Dept Psychol, Edmonton, AB T6G 2E9, Canada. Emory Univ, Ctr Behav Neurosci, Atlanta, GA 30329 USA. RP Ryan, MJ (reprint author), Univ Texas, Ctr Integrated Biol C0930, Austin, TX 78712 USA. RI Hurd, Peter/A-4342-2009 OI Hurd, Peter/0000-0002-4389-0846 NR 68 TC 54 Z9 58 U1 0 U2 11 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 MAR PY 2003 VL 161 IS 3 BP 380 EP 394 DI 10.1086/367588 PG 15 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 656MZ UT WOS:000181612700003 PM 12699219 ER PT J AU Heyer, WR Reid, YR AF Heyer, WR Reid, YR TI Does advertisement call variation coincide with genetic variation in the genetically diverse frog taxon currently known as Leptodactylus fuscus (Amphibia : Leptodactylidae)? SO ANAIS DA ACADEMIA BRASILEIRA DE CIENCIAS LA English DT Article DE advertisement calls; Leptodactylus fuscus; speciation ID HYLA ARENICOLOR COPE; NEOTROPICAL FROG; CANYON TREEFROG; ANURA; DIVERGENCE; TOADS AB The frog Leptodactylus fuscus is found throughout much of South America in open and disturbed habitats. Previous study of genetic differentiation in L fuscus demonstrated that there was lack of genetic exchange among population units consistent with multiple species, rather than a single species. We examine advertisement vocalizations of L. fuscus to determine whether call variation coincides with genetic differentiation. Calls were analyzed for 32 individual frogs from 25 localities throughout the distributional range of L. fuscus. Although there is variation in calls among geographic samples, call variation is not concordant with genetic variation or geographic distance and the call variation observed is less than that typically found among other closely related species of Leptodactylus. This study is an example of the rare pattern of strong genetic differentiation unaccompanied by salient differences in advertisement calls. The relative infrequency of this pattern as currently understood may only reflect the lack of detailed analyses of genetic and acoustic differentiation within population systems currently understood as single species with substantial geographic distributions. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Haskell Indian Nations Univ, Lawrence, KS 66044 USA. RP Heyer, WR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. NR 32 TC 25 Z9 29 U1 0 U2 3 PU ACAD BRASILEIRA DE CIENCIAS PI RIO JANEIRO PA RUA ANFILOFIO DE CARVALHO, 29, 3 ANDAR, 20030-060 RIO JANEIRO, BRAZIL SN 0001-3765 J9 AN ACAD BRAS CIENC JI An. Acad. Bras. Cienc. PD MAR PY 2003 VL 75 IS 1 BP 39 EP 54 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 656PC UT WOS:000181615300006 PM 12715049 ER PT J AU Bronson, CL Grubb, TC Sattler, GD Braun, MJ AF Bronson, CL Grubb, TC Sattler, GD Braun, MJ TI Mate preference: a possible causal mechanism for a moving hybrid zone SO ANIMAL BEHAVIOUR LA English DT Article ID BLACK-CAPPED CHICKADEES; HIGH-RANKING MALES; WINTER FLOCKS; PARUS-PALUSTRIS; WILLOW TITS; REPRODUCTIVE SUCCESS; TOWNSENDS WARBLERS; SEXUAL SELECTION; MARSH TITS; FEMALE AB The study of patterns and underlying mechanisms within hybrid zones may provide insight into speciation. Black-capped (Poecile atricapillus; BC) and Carolina (P. carolinensis; CA) chickadees hybridize in an east-west band in the U.S.A. from New Jersey to Kansas. Within the past century, the Ohio portion of this hybrid zone and the CA range to the south have been moving northward while the BC range has retracted. We examined mate preference in females of both species as one possible causal mechanism for this shift. To be conservative about the nomenclature and results, the samples are referred to as either 'BC-like' or 'CA-like' due to the observed genetic introgression in the study individuals. Given a choice within an aviary setting, in the aggregate, BC-like and CA-like females that had not observed the direct social interactions between a dyad of a BC-like male and a CA-like male preferred to associate with the BC-like male. In nature, both species form within-sex dominance hierarchies. In the aviary, CA-like males dominated BC-like males unless a CA-like male was substantially smaller. Once females of both types had observed the physical interaction of a particular heterospecific dyad, they associated preferentially with the dominant male, regardless of species type. Thus, the effect of CA male intrasexual dominance on female mate preference may be contributing to the northward movement of the hybrid zone. (C) 2003 Published by Elsevier Science Ltd on behalf of The Association for the Study of Animal Behaviour. C1 Ohio State Univ, Behav Ecol Grp, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. Liberty Univ, Dept Biol & Chem, Lynchburg, VA 24502 USA. Smithsonian Inst, Dept Systemat Biol, Suitland, MD 20746 USA. RP Bronson, CL (reprint author), Ohio State Univ, Dept Internal Med, Div Immunol, Heart & Lung Res Inst 425, 473 W 12th Ave, Columbus, OH 43210 USA. NR 61 TC 43 Z9 44 U1 0 U2 19 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD MAR PY 2003 VL 65 BP 489 EP 500 DI 10.1006/anbe.2003.2103 PN 3 PG 12 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 689HD UT WOS:000183484800009 ER PT J AU Reents-Budet, D Bishop, R AF Reents-Budet, D Bishop, R TI What can we learn from a Maya vase? (Ceramics, archaeology, chemical imagery) SO ARCHAEOLOGY LA English DT Article C1 Smithsonian Inst, Ctr Materials Res, Washington, DC 20560 USA. RP Reents-Budet, D (reprint author), Smithsonian Inst, Ctr Materials Res, Washington, DC 20560 USA. NR 0 TC 1 Z9 2 U1 0 U2 6 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 USA SN 0003-8113 J9 ARCHAEOLOGY JI Archaeology PD MAR-APR PY 2003 VL 56 IS 2 BP 26 EP 29 PG 4 WC Archaeology SC Archaeology GA 727ED UT WOS:000185643200006 ER PT J AU Erwin, DH AF Erwin, DH TI Impact at the Permo-Triassic boundary: A critical evaluation SO ASTROBIOLOGY LA English DT Article; Proceedings Paper CT 10th Rubey Colloquium CY FEB 08-09, 2002 CL LOS ANGELES, CA DE Permo-Triassic mass extinction; extraterrestrial impact; flood basalt volcanism ID FLOOD-BASALT VOLCANISM; MORY,A.J. ET-AL.; MASS EXTINCTION; WESTERN-AUSTRALIA; GIGANTIC RELEASE; CARNARVON BASIN; METHANE RELEASE; BOLIDE IMPACT; SOUTH-CHINA; EVENT AB The recognition in 1980 of a signature of an extraterrestrial impact at the Cretaceous-Tertiary boundary and its apparent involvement with the mass extinction generated considerable enthusiasm for impacts at other mass extinctions. Numerous claims of impact evidence for the Permo-Triassic mass extinction (251.6 Ma), the largest of the Phanerozoic mass extinctions, have generally been rejected, found wanting, or been difficult to reproduce. Despite this lack of repeatable support, considerable available evidence is consistent with an impact, including the rapidity of extinction, coincident carbon shift, and evident correlation between terrestrial and marine extinctions. However attractive the hypothesis, the coincidence with the Siberian flood basalts and the complex nature of the carbon shift are in conflict with an impact. The most intriguing possibility is that the greatest mass extinction of the Phanerozoic left signals very similar to the end-Cretaceous mass extinction but was produced by entirely Earth-bound processes. If true, this would tell us far more about the nature of ecosystems and how they fail than would identification of another impact. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Erwin, DH (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM erwin.doug@nmnh.si.edu RI Erwin, Douglas/A-9668-2009 NR 52 TC 12 Z9 15 U1 1 U2 5 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD SPR PY 2003 VL 3 IS 1 BP 67 EP 74 DI 10.1089/153110703321632426 PG 8 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 676LF UT WOS:000182753000005 PM 12804365 ER PT J AU Bloom, JS Berger, E Kulkarni, SR Djorgovski, SG Frail, DA AF Bloom, JS Berger, E Kulkarni, SR Djorgovski, SG Frail, DA TI The redshift determination of GRB 990506 and GRB 000418 with the Echellete Spectrograph Imager on Keck SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology : miscellaneous; cosmology : observations; gamma rays ID GAMMA-RAY BURSTS; MICROWAVE BACKGROUND-RADIATION; STARBURST GALAXIES; HOST GALAXY; EMISSION; AFTERGLOW; UNIVERSE; MAPS AB Using the Echellete Spectrograph Imager (ESI) on the Keck II 10 m telescope we have measured the redshifts of the host galaxies of gamma-ray bursts GRB 990506 and GRB 000418, z = 1.30658 +/- 0.00004 and 1.1181 +/- 0.0001, respectively. Thanks to the excellent spectral resolution of ESI (lambda/Deltalambda = 13000), we resolved the [O II] lambda727 doublet in both cases. The measured redshift of GRB 990506 is the highest known for a dark-burst GRB, though entirely consistent with the notion that dark and non-dark bursts have a common progenitor origin. The relative strengths of the [O II], He I [Ne III], and Hgamma emission lines suggest that the host of GRB 000418 is a starburst galaxy, rather than a LINER or Seyfert 2. Since the host of GRB 000418 has been detected at submillimeter wavelengths, these spectroscopic observations suggest that the submillimeter emission is due to star formation ( as opposed to AGN) activity. The [O II]-derived unobscured star formation rates are 13 and 55 M(circle dot) yr(-1) for the hosts of GRB 990506 and GRB 000418, respectively. In contrast, the star formation rate of the host of GRB 000418 derived from submillimeter observations is 20 times larger. C1 CALTECH, Palomar Observ, Pasadena, CA 91125 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Bloom, JS (reprint author), CALTECH, Palomar Observ, Mail Stop 105-24, Pasadena, CA 91125 USA. EM jbloom@cfa.harvard.edu NR 34 TC 42 Z9 43 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2003 VL 125 IS 3 BP 999 EP 1005 DI 10.1086/367805 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647LR UT WOS:000181094700001 ER PT J AU Darling, J Goldsmith, P Li, D Giovanelli, R AF Darling, J Goldsmith, P Li, D Giovanelli, R TI A search for 6.7 GHz methanol masers in OH megamaser galaxies at 0.11 z 0.27 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : ISM; galaxies : starburst; ISM : molecules; masers; radio emission lines ID MAGELLANIC CLOUDS; REGIONS AB We report the results of a search for 6.7 GHz methanol (CH3OH) maser emission in OH megamaser galaxies at 0.11 < z < 0.27. No detections were made in the 25 objects observed down to rms noise levels of roughly 0.6 mJy in 150 kHz channels. The OH megamaser sample includes OH emission of all observed types: narrow and broad, physically compact and extended, variable and quiescent, and from simple single lines to multicomponent complexes to lines with high-velocity wings. Our null result indicates that, for the widest possible range of OH megamaser environments, methanol masing does not scale with OH from Galactic masers to megamasers. These observations, however, are not sensitive enough to rule out methanol masing that scales with star formation from Galactic compact H II regions to starbursts associated with major mergers. This and previous work suggest that OH megamasers do not represent large ensembles of individual masers associated with star-forming regions. Maser models combined with observational constraints on the physical settings of OH megamasers indicate that 6.7 GHz methanol megamasers will not be detected by this survey if T-dust < 100 K or if n(CH3OH) &LE; n(OH). C1 Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Cornell Univ, Ithaca, NY 14853 USA. Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Darling, J (reprint author), Carnegie Inst Washington Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. RI Darling, Jeremy/A-7968-2009 OI Darling, Jeremy/0000-0003-2511-2060 NR 21 TC 14 Z9 14 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2003 VL 125 IS 3 BP 1177 EP 1181 DI 10.1086/367804 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647LR UT WOS:000181094700016 ER PT J AU Strader, J Brodie, JP Forbes, DA Beasley, MA Huchra, JP AF Strader, J Brodie, JP Forbes, DA Beasley, MA Huchra, JP TI Spectroscopy of globular clusters in the Fornax dwarf galaxy SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : dwarf; galaxies : individual (Fornax); galaxies : star clusters; Local Group ID OLD STELLAR POPULATIONS; COLOR-MAGNITUDE DIAGRAMS; SPHEROIDAL GALAXY; STAR-CLUSTERS; KECK SPECTROSCOPY; AGE INDICATOR; PALOMAR 12; METALLICITY; PHOTOMETRY; SPECTRA AB We present low-resolution, integrated Keck spectra of the five globular clusters (GCs) of the Fornax dwarf spheroidal galaxy. We find a tentative age spread among the clusters, with the GC H5 younger by 2-3 Gyr than the others. The clusters generally appear to be very metal-poor ([Fe/H] similar to 1.8), with the cluster H4 slightly more metal-rich at [Fe/H] = 1.5. We speculate that cluster H4 is similar to the Galactic GC Ruprecht 106, which lacks the [alpha/Fe] enhancement typical among metal-poor GCs in the Milky Way. High-resolution spectroscopy of individual cluster and field stars will be needed to sort out the surprisingly complex history of GC formation and evolution in this galaxy. C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Strader, J (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. EM strader@ucolick.org; brodie@ucolick.org; dforbes@astro.swin.edu.au; mbeasley@astro.swin.edu.au; huchra@cfa.harvard.edu NR 48 TC 43 Z9 43 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2003 VL 125 IS 3 BP 1291 EP 1297 DI 10.1086/367599 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647LR UT WOS:000181094700024 ER PT J AU Dobrzycki, A Macri, LM Stanek, KZ Groot, PJ AF Dobrzycki, A Macri, LM Stanek, KZ Groot, PJ TI Variability-selected quasars behind the Small Magellanic Cloud SO ASTRONOMICAL JOURNAL LA English DT Article DE Magellanic Clouds; quasars : general ID GRAVITATIONAL LENSING EXPERIMENT; PROPER MOTION; GALAXIES; SAMPLE; FIELD; QSOS AB We present follow-up spectroscopic observations of quasar candidates in the Small Magellanic Cloud selected by L. Eyer from the OGLE database. Of 12 observed objects identified as "QSO candidates, "five are confirmed as quasars, with emission redshifts ranging from 0.28 to 2.16. Two of these quasars were also recently identified independently in the MACHO database by Geha et al. We discuss the prospects of using the variability-based selection technique for quasar searches behind other dense stellar fields. An additional criterion utilizing a color-color diagram should reduce the number of stars in the candidate lists. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA. Katholieke Univ Nijmegen, Afdeling Sterrenkunde, NL-6500 GL Nijmegen, Netherlands. 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 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 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2003 VL 125 IS 3 BP 1330 EP 1335 DI 10.1086/346144 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647LR UT WOS:000181094700027 ER PT J AU Schlegel, EM AF Schlegel, EM TI Upper limits on the X-ray emission of "uranium" stars SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : general; stars : abundances; stars : general; supernovae : general; X-rays ID R-PROCESS NUCLEOSYNTHESIS; METAL-POOR STARS; ALL-SKY SURVEY; SUPERNOVA EXPLOSIONS; ABUNDANCES; GALAXY; SAMPLE AB A paper by Qian & Wasserburg suggests the optical absorption lines of uranium observed in the spectra of ultra metal-poor stars (defined as [Fe/H] < -3) arise from contamination from a supernova in a binary star system. Assuming the binary survived the explosion, a collapsed compact object may be present and implies potential accretion processes with accompanying X-ray emission. Upper limits on X-ray emission from an accreting compact object are described here. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schlegel, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 29 TC 2 Z9 2 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 2003 VL 125 IS 3 BP 1426 EP 1430 DI 10.1086/367597 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647LR UT WOS:000181094700036 ER PT J AU Smith, N Gehrz, RD Hinz, PM Hoffmann, WF Hora, JL Mamajek, EE Meyer, MR AF Smith, N Gehrz, RD Hinz, PM Hoffmann, WF Hora, JL Mamajek, EE Meyer, MR TI Mass and kinetic energy of the Homunculus Nebula around eta Carinae SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : individual (Homunculus Nebula); stars : individual (eta Carinae) ID HUBBLE-SPACE-TELESCOPE; TORUS AB We examine thermal infrared images of eta Car at wavelengths from 4.8 to 25 mum obtained with the MIRAC3 camera system at the Magellan Observatory, and we conclude that eta Car's circumstellar Homunculus Nebula contains much more mass (greater than or similar to 12 M) and kinetic energy (10(49.6)-10(50) ergs) than had previously been recognized. Excess far-infrared emission from a large mass of cold dust had been discovered recently by Morris et al., which they attributed to 110 K dust in a compact equatorial torus. Our images suggest, however, that roughly 10 M or more resides instead in the rapidly expanding polar lobes of the Homunculus, known to be ejected during eta Car's Great Eruption in the 19th century. Combining this large mass with reliable expansion speeds for the polar lobes allows us to estimate the large kinetic energy and efficient momentum transfer associated with the eruption. Most mass resides in a cool outer layer of the lobes, with dust at similar to140 K. This material is only revealed at 18-25 mum with high spatial resolution images that can separate adjacent dust components. Warmer dust at similar to200 K that has been recognized for some time ( responsible for previous mass estimates of 2-3 M-.) blankets the inner surfaces of the mostly hollow polar lobes as they are irradiated more directly by the central engine. C1 Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. 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 Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. NR 31 TC 167 Z9 167 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2003 VL 125 IS 3 BP 1458 EP 1466 DI 10.1086/346278 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647LR UT WOS:000181094700041 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 Plasma properties above coronal active regions inferred from SOHO/UVCS and radio spectrograph observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : corona; Sun : UV radiation; Sun : magnetic fields; Sun : radio radiation; shock waves ID SOLAR CORONA; FARADAY-ROTATION; SOHO; SPECTROMETER; BURSTS; SHOCK; VELOCITIES; UVCS/SOHO; STREAMERS; WAVES AB Information on coronal plasma was inferred from the joint analysis of type II radio bursts and SOHO UltraViolet Coronagraph Spectrometer (UVCS) observations. The data sample comprises 37 metric type II radio bursts observed by ground-based radio spectrographs in 1999, during the rising phase of the solar cycle. The coronal electron densities n(e) were estimated with the diagnostic provided by UVCS observations of the O VI doublet line intensities. Upper limits to the coronal Alfven speed above active regions were inferred from the derived shock speeds by requiring that the disturbances propagate at least faster than the local characteristic speed. Information on the magnetic field strength B and plasma beta in the middle corona were finally extracted from the coronal Alfven speed upper limits. A major improvement with respect to previous studies that used type II radio bursts to derive plasma properties, is that density profiles of the pre-shock plasma obtained a few hours before the passage of the shock were used instead of general electron density models taken from literature. Our main result is expressed by the inequality B(r) less than or equal to (0.6 +/- 0.3)(r - 1)(-1.2) G, that is valid in the range 1.5 less than or equal to r less than or equal to 2.3 solar radii, and is consistent with previous estimates of the magnetic field above coronal active regions. C1 Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mancuso, S (reprint author), Osserv Astron Torino, INAF, Strada Osservatorio 20, I-10025 Pino Torinese, Italy. NR 30 TC 30 Z9 30 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 MAR PY 2003 VL 400 IS 1 BP 347 EP 353 DI 10.1051/0004-6361:20021844 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 648XT UT WOS:000181177300036 ER PT J AU Kramer, C Richer, J Mookerjea, B Alves, J Lada, C AF Kramer, C Richer, J Mookerjea, B Alves, J Lada, C TI Dust properties of the dark cloud IC5146 - Submillimeter and NIR imaging SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : clouds; ISM : dust, extinction; ISM : evolution; ISM : structure; ISM : individual objects : IC5146 ID MOLECULAR CLOUDS; INTERSTELLAR DUST; STAR-FORMATION; CORES; EXTINCTION; GAS; TEMPERATURES; OPACITIES; CONTINUUM; EMISSION AB We present the results of a submillimeter dust continuum study of a molecular ridge in IC 5146 carried out at 850 mum and 450 mum with SCUBA on the James Clerk Maxwell Telescope (JCMT). The mapped region is similar to14'x2'.5 in size (similar to2 pc x 0.3 pc) and consists of at least four dense cores which are likely to be prestellar in nature. To study the dust properties of the ridge and its embedded cores, we combined the dust emission data with dust extinction data obtained by Lada et al. (1999) from the NIR colors of background giant stars. The ridge shows dust extinctions above similar to10 mag, rising up to 35 mag in the cores. A map of dust temperatures, constructed from the continuum flux ratios, shows significant temperature gradients: we find temperatures of up to similar to20 K in the outskirts and between the cores, and down to similar to10 K in the cores themselves. The cores themselves are almost isothermal, although their average temperatures vary between 10 K and 18 K. We used the extinction data to derive in addition a map of the dust emissivity parametrized by kappa' = kappa(850)/kappa(V). The average value of kappa' agrees well with the canonical value of Mathis (1990). We find that kappa' increases by a factor of similar to4 from similar to1.3x10(-5) to similar to5x10(-5) when the dust temperature decreases from similar to20 K to similar to12 K. A Monte Carlo simulation shows that this change is significant with regard to the estimated calibration uncertainties. This is consistent with models of dust evolution in prestellar cores by Ossenkopf & Henning (1994) which predict that grain coagulation and the formation of ices on grain surfaces in the cold, dense cloud interiors lead to a significant increase of the 850 mum dust opacity. This interpretation is furthermore supported by the previous detection of gas-phase depletion of CO in one of the IC 5146 cores (Kramer et al. 1999). Observations of dust fluxes at short wavelengths are however needed to verify this result. C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England. European So Observ, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kramer, C (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. OI Alves, Joao/0000-0002-4355-0921 NR 46 TC 71 Z9 71 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 MAR PY 2003 VL 399 IS 3 BP 1073 EP 1082 DI 10.1051/0004-6361:20021823 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646QR UT WOS:000181046200030 ER PT J AU Keshet, U Waxman, E Loeb, A Springel, V Hernquist, L AF Keshet, U Waxman, E Loeb, A Springel, V Hernquist, L TI Gamma rays from intergalactic shocks SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; gamma rays : theory; large-scale structure of universe; methods : numerical; radiation mechanisms : nonthermal; shock waves ID SMOOTHED PARTICLE HYDRODYNAMICS; MAGNETIC-FIELDS; SUPERNOVA-REMNANTS; COSMIC-RAYS; ORIGIN; GALAXIES; ACCELERATION; EMISSION; SIMULATIONS; CLUSTERS AB Structure formation in the intergalactic medium (IGM) produces large-scale, collisionless shock waves, in which electrons can be accelerated to highly relativistic energies. Such electrons can Compton-scatter cosmic microwave background photons up to gamma-ray energies. We study the radiation emitted in this process using a hydrodynamic cosmological simulation of a LambdaCDM universe. The resulting radiation, extending beyond TeV energies, has roughly constant energy flux per decade in photon energy, in agreement with the predictions of Loeb & Waxman. Assuming that a fraction xi(e)=0.05 of the shock thermal energy is transferred to the population of accelerated relativistic electrons, as inferred from collisionless nonrelativistic shocks in the interstellar medium, we find that the energy flux of this radiation, epsilon(2)(dJ/depsilon)similar or equal to50-160 eV cm(-2) s(-1) sr(-1), constitutes similar to10% of the extragalactic gamma-ray background flux. The associated gamma-ray point sources are too faint to account for the similar to60 unidentified EGRET gamma-ray sources, but GLAST should detect and resolve several gamma-ray sources associated with large-scale IGM structures for xi(e)similar or equal to0.03 and many more sources for larger xi(e). The intergalactic origin of the shock-induced radiation can be verified through a cross-correlation with, e. g., the galaxy distribution that traces the same structure. Its shock origin may be tested by cross-correlating its properties with radio synchrotron radiation, emitted as the same accelerated electrons gyrate in postshock magnetic fields. We predict that GLAST and Cerenkov telescopes such as MAGIC, VERITAS, and HESS should resolve gamma-rays from nearby (redshifts zless than or similar to0.01) rich galaxy clusters, perhaps in the form of a similar to5-10 Mpc diameter ringlike emission tracing the cluster accretion shock, with luminous peaks where the ring intersects galaxy laments detectable even at zsimilar or equal to0.025. C1 Weizmann Inst Sci, Dept Condensed Matter Phys, IL-76100 Rehovot, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Keshet, U (reprint author), Weizmann Inst Sci, Dept Condensed Matter Phys, IL-76100 Rehovot, Israel. RI WAXMAN, ELI/K-1557-2012 NR 70 TC 107 Z9 107 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 2003 VL 585 IS 1 BP 128 EP 150 DI 10.1086/345946 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646QV UT WOS:000181046500012 ER PT J AU Kochanek, CS White, M Huchra, J Macri, L Jarrett, TH Schneider, SE Mader, J AF Kochanek, CS White, M Huchra, J Macri, L Jarrett, TH Schneider, SE Mader, J TI Clusters of galaxies in the local universe SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; galaxies : clusters : general; large-scale structure of universe ID ALL-SKY SURVEY; MASS-TEMPERATURE RELATION; X-RAY-PROPERTIES; FLUX-LIMITED SAMPLE; MEDIUM-SENSITIVITY SURVEY; LUMINOSITY FUNCTION; NEARBY CLUSTERS; REDSHIFT SURVEY; T RELATION; HIERARCHICAL UNIVERSE AB We use a matched filter algorithm to find and study clusters in both N-body simulations artificially populated with galaxies and the Two Micron All Sky Survey (2MASS). In addition to numerous checks of the matched filter algorithm, we present results on the halo multiplicity function and the cluster number function. For a subset of our identified clusters we have information on X-ray temperatures and luminosities that we cross-correlate with optical richness and galaxy velocity dispersions. With all quantities normalized by the spherical radius corresponding to a mass overdensity of Delta(M)=200 or the equivalent galaxy number over-density of Delta(N)=200Omega(M)(-1) similar or equal to 666, we find that the number of L>L(*) galaxies in a cluster of mass M(200) is log N(*666)=(1.44+/-0.17)+(1.10+/-0.09)log(M(200)h/10(15) M(circle dot)), where the uncertainties are dominated by the scatter created by three choices for relating the observed quantities to the cluster mass. The region inside the virial radius has a K-band cluster mass-to-light ratio of (M/L)(K)=(116+/-46)h, which is essentially independent of cluster mass. Integrating over all clusters more massive than M(200)=10(14) h(-1) M(circle dot), the virialized regions of clusters contain similar or equal to7% of the local stellar luminosity, quite comparable to the mass fraction in such objects in currently popular LambdaCDM models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Univ Massachusetts, Dept Phys & Astron, Lederle Grad Res Ctr 640, Amherst, MA 01003 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ckochanek@cfa.harvard.edu; mwhite@astron.berkeley.edu; jhuchra@cfa.harvard.edu; lmacri@cfa.harvard.edu; jarrett@ipac.caltech.edu; schneider@messier.astro.edu; jmader@astro.as.utexas.edu RI White, Martin/I-3880-2015; OI White, Martin/0000-0001-9912-5070; Macri, Lucas/0000-0002-1775-4859 NR 120 TC 80 Z9 80 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 MAR 1 PY 2003 VL 585 IS 1 BP 161 EP 181 DI 10.1086/345896 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646QV UT WOS:000181046500014 ER PT J AU Kong, AKH DiStefano, R Garcia, MR Greiner, J AF Kong, AKH DiStefano, R Garcia, MR Greiner, J TI Chandra studies of the X-ray point source luminosity functions of M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); X-rays : binaries; X-rays : galaxies ID SUPERNOVA REMNANT CANDIDATES; HUBBLE-SPACE-TELESCOPE; GLOBULAR-CLUSTERS; ANDROMEDA GALAXY; M-31 AB Three different M31 disk fields, spanning a range of stellar populations, were observed by Chandra. We report the X-ray point source luminosity function (LF) of each region, and the LF of M31's globular clusters, and compare these with each other and with the LF of the galaxy's bulge. To interpret the results we also consider tracers of the stellar population, such as OB associations and supernova remnants. We find differences in the LFs among the fields, but cannot definitively relate them to the stellar content of the fields. We find that stellar population information, average and maximum source luminosities, X-ray source densities, and slopes of the LF are useful in combination. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 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 MAR 1 PY 2003 VL 585 IS 1 BP 298 EP 304 DI 10.1086/345947 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646QV UT WOS:000181046500025 ER PT J AU Hartmann, L AF Hartmann, L TI Comments on inferences of star formation histories and birth lines SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : formation; stars : pre-main sequence ID T-TAURI STARS; MAIN-SEQUENCE STARS; ORION NEBULA CLUSTER; LOW-MASS STARS; MOLECULAR CLOUDS; X-RAY; DISK ACCRETION; MAGNETOHYDRODYNAMIC TURBULENCE; STELLAR BIRTHLINE; LITHIUM AB Palla & Stahler have recently argued that star formation in Taurus and other nearby molecular clouds extends over a period of at least 10 Myr, implying quasi-static cloud evolution and star formation. Their conclusions contradict other recent results indicating that molecular clouds are transient objects and star formation proceeds rapidly. The Palla & Stahler picture implies that most molecular clouds should have extremely low rates of star formation and that in such inactive stages, the stellar initial mass function (IMF) should be strongly skewed toward producing stars with masses greater than or similar to 1 M.; neither prediction is supported by observations. I show that the Palla & Stahler conclusions for Taurus depend almost entirely on a small number of stars with masses greater than or similar to 1 M.; the lower mass stars show no evidence for such an extended period of star formation. I further show that most of the stars apparently older than 10 Myr in the direction of Taurus are probably foreground nonmembers. I also present birth line calculations that support the idea that the ages of the stars with masses greater than or similar to 1 M. have been systematically overestimated because birth line age corrections have been underestimated; such birth lines would eliminate the need to postulate skewed IMFs. The simplest and most robust explanation of current observations characterizing the vast majority of young stars in molecular clouds is that cloud and star formation is rapid and dynamic. 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 65 TC 124 Z9 124 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 MAR 1 PY 2003 VL 585 IS 1 BP 398 EP 405 DI 10.1086/345933 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646QV UT WOS:000181046500033 ER PT J AU Meakin, CA Bieging, JH Latter, WB Hora, JL Tielens, AGGM AF Meakin, CA Bieging, JH Latter, WB Hora, JL Tielens, AGGM TI Hubble Space Telescope/NICMOS near-infrared imaging of the proto planetary nebula OH 231.8+4.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary nebulae : individual (OH 231.8+4.2); stars : AGB and post-AGB ID MODEL SCATTERING ENVELOPES; LONG-SLIT SPECTROSCOPY; YOUNG STELLAR OBJECTS; OH 231.8+4.2; MOLECULAR OUTFLOW; BIPOLAR OUTFLOW; OH/IR STARS; JETS; OH231.8+4.2; EMISSION AB We present observations of the bipolar nebula OH 231.8+4.2, made with the Hubble Space Telescope (HST) NICMOS camera, in three wide filter bands (F205W, F160W, and F110W). The images have excellent dynamic range after removal of low-level instrumental artifacts. In the F205W filter (lambda approximate to 2.04 mum), we achieve a peak/rms of greater than 8000 with an angular resolution of 0."20 (FWHM). The combination of high dynamic range and angular resolution confirms previous observations but also reveals new features in the near-IR morphology of the nebula, which at these wavelengths is dominated by scattered light. The northern (approaching) lobe shows well-defined, limb-brightened edges. The central jet splits into two laments and exhibits some curvature between the center of the nebula and the end of the northern lobe. The southern (receding) lobe has a diffuse, occulent appearance without a sharply defined central jet, in contrast to the northern lobe. A sharpened version of the F205W image shows indications of turbulent structures both in the northern lobe and jet and in the southern lobe. A faint cylindrical halo of scattered light shows a sharp increase in surface brightness inside a radius of similar to4" from the center, possibly resulting from a transition from a spherical wind to a disk- or torus-like mass ejection, on the same timescale as the formation of the collimated fast wind seen in CO and HCO(+) images. We calculate the extinction through the nebula from the measured near-IR colors and a silicate grain model. For a simple geometric model of a dense central disk, we estimate a disk mass (gas and dust) in the range 0.03-0.06 M., relatively insensitive to grain size. The circumstance of an asymptotic giant branch (AGB) star with a massive, highly collimated, high-velocity bipolar flow may be understood in terms of the model of Soker & Rappaport if the central star underwent a change in mass-loss properties from a (roughly) spherical AGB wind to equatorially enhanced mass loss beginning similar to(1-3) X 10(3) yr ago. Supposing the presence of a dwarf companion in a suitable orbit, the bipolar nebula then is a consequence of a strong increase in mass loss as the central star evolves close to the tip of the AGB and will soon evolve to higher T(eff) and appear as a more typical proto planetary nebula. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Groningen, Kapteyn Astron Inst, NL-9700 Groningen, Netherlands. RP Meakin, CA (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM cmeakin@as.arizona.edu; jbieging@as.arizona.edu OI Hora, Joseph/0000-0002-5599-4650 NR 42 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2003 VL 585 IS 1 BP 482 EP 493 DI 10.1086/345951 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646QV UT WOS:000181046500041 ER PT J AU Kharchenko, V Rigazio, M Dalgarno, A Krasnopolsky, VA AF Kharchenko, V Rigazio, M Dalgarno, A Krasnopolsky, VA TI Charge abundances of the solar wind ions inferred from cometary X-ray spectra SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; comets : general; X-rays : general ID EXTREME-ULTRAVIOLET EMISSION; HALE-BOPP; C/1995 O1; EXCHANGE; HYAKUTAKE; NEUTRALS; SEARCH; EUVE AB An emission spectrum of X-rays from comet McNaught-Hartley (C/1999 T1) detected with the Chandra X-ray telescope is analyzed on the assumption that it results from electron captures by heavy ions of the solar wind colliding with the atoms and molecules of the cometary atmosphere. An accurate value of the relative abundance of O+8 and O+7 ions is obtained by comparing the spectrum derived from the measurement data with the predicted spectrum. A close match is found for an abundance ratio of O+8 to O+7 of 0.34 +/- 0.07, the uncertainty reflecting the measurement statistics. A similar analysis of the contribution from captures by Ne+9 ions leads to an abundance ratio of Ne+9 to O+7 of 0.02 with an uncertainty of 40%. The spectrum consists of many unresolved lines. The brightest feature is composed mostly of the 2 S-3(1) --> 1 S-1(0) spin-forbidden line of O+6 at 561 eV with 74% of the intensity and the 2 P-3(1) --> 1 S-1(0) intercombination line at 568 eV with 12%. The strongest of the O+7 lines is the Lyalpha transition at 654 eV with an intensity of 29%, relative to the O+6 lines. The sensitivity of cometary X-ray spectra to variations in the abundances of highly charged oxygen ions in the solar wind is investigated. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Kharchenko, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Krasnopolsky, Vladimir/L-5085-2013 NR 29 TC 75 Z9 75 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 MAR 1 PY 2003 VL 585 IS 1 BP L73 EP L75 DI 10.1086/374209 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646QW UT WOS:000181046600018 ER PT J AU Miller, JM Fabbiano, G Miller, MC Fabian, AC AF Miller, JM Fabbiano, G Miller, MC Fabian, AC TI X-ray spectroscopic evidence for intermediate-mass black holes: Cool accretion disks in two ultraluminous X-ray sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays : stars ID SPIRAL GALAXIES; CANDIDATES; EMISSION AB We have analyzed an XMM-Newton observation of the nearby spiral galaxy NGC 1313, which contains two "ultraluminous" X-ray (ULX) sources. We measure isotropic luminosities of L-x = 2.0 X 10(40) ergs s(-1) and 40 L-x = 6.6 X 10(39) ergs s(-1) for NGC 1313 X-1 and X-2 (0.2-10.0 keV, assuming a distance of 3.7 Mpc). The spectra statistically require soft and hard spectral components to describe the continuum emission; some prior studies of ULX sources have claimed cool soft components with lower statistics. The improvement over several single-component models exceeds the 8 sigma level of confidence for X-1; the improvement for X-2 is significant at the 3 sigma level. The soft components in these ULX spectra are well fitted by multicolor disk blackbody models with color temperatures of kT similar or equal to eV. This temperature differs markedly from those commonly measured in the spectra of stellar mass (10 M.) black holes in their brightest states (kT similar or equal to 1 keV). It is expected that the temperature of an accretion disk orbiting a black hole should decrease with increasing black hole mass. If the soft components we measure are due to emission from the inner region of an accretion disk, and disks extend close to the innermost stable circular orbit at the accretion rates being probed, the low color temperatures may be interpreted as spectroscopic evidence of black holes with intermediate masses: M-BH similar or equal to 10(3) M.. Simple Eddington scaling arguments suggest a minimum mass of M-BH similar to 10(2) M.. NGC 1313 X-1 and X-2 are found in optical nebulae, which may indicate that anisotropic emission geometries are unlikely to account for the fluxes observed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. RP Miller, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 185 Z9 186 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 2003 VL 585 IS 1 BP L37 EP L40 DI 10.1086/368373 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646QW UT WOS:000181046600010 ER PT J AU Winn, JN Patnaik, AR Wrobel, JM AF Winn, JN Patnaik, AR Wrobel, JM TI Interferometric phase calibration sources in the declination range 0 degrees to-30 degrees SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrometry; catalogs; radio continuum : general; techniques : interferometric ID NRAO PMN SURVEYS; SOURCE CATALOG; RADIO-SOURCES AB We present a catalog of 321 compact radio sources in the declination range 0degrees > delta > -30degrees. The positions of these sources have been measured with a two-dimensional rms accuracy of 35 milliarcseconds using the NRAO(6) Very Large Array. Each source has a peak flux density > 50 mJy at 8.4 GHz. We intend for this catalog to be used mainly for selection of phase calibration sources for radio interferometers, although compact radio sources have other scientific uses. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 2 Z9 2 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2003 VL 145 IS 1 BP 83 EP 87 DI 10.1086/345541 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 648KX UT WOS:000181151500005 ER PT J AU Sanz-Forcada, J Brickhouse, NS Dupree, AK AF Sanz-Forcada, J Brickhouse, NS Dupree, AK TI The structure of stellar coronae in active binary systems SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE stars : coronae; stars : flare; ultraviolet : stars; X-rays : stars ID EXTREME-ULTRAVIOLET-EXPLORER; CANUM-VENATICORUM BINARIES; LATE-TYPE STARS; TRANSITION-REGION STRUCTURE; XI-URSAE-MAJORIS; ALPHA-CENTAURI; AR-LACERTAE; RS CVN; INTERSTELLAR-MEDIUM; RADIAL-VELOCITIES AB A survey of 28 stars (22 active binary systems, plus six single stars or wide binaries for comparison) using extreme ultraviolet spectra has been conducted to establish the structure of stellar coronae in active binary systems from the emission measure distribution (EMD), electron densities, and scale sizes. Observations obtained by the Extreme Ultraviolet Explorer satellite (EUVE) during 9 years of operation are included for the stars in the sample. EUVE data allow a continuous EMD to be constructed in the range log T-e(K) similar to 5.6-7.4, using iron emission lines. These data are complemented with IUE observations to model the lower temperature range [log T-e(K) similar to 4.0-5.6]. Inspection of the EMD shows an outstanding narrow enhancement, or "bump" peaking around log T-e(K) similar to 6.9 in 25 of the stars, de ning a fundamental coronal structure. The emission measure per unit stellar area decreases with increasing orbital (or photometric) periods of the target stars; stars in binaries generally have more material at coronal temperatures than slowly rotating single stars. High electron densities (N(e)greater than or similar to10(12) cm(-3)) are derived at similar to log T-e(K) similar to 7.0 for some targets, implying small emitting volumes. The observations suggest the magnetic stellar coronae of these stars are consistent with two basic classes of magnetic loops: solar-like loops with maximum temperature around log T-e(K) similar to 6.3 and lower electron densities (N(e)greater than or similar to10(9)-10(10.5) cm(-3)), and hotter loops peaking around log T-e(K) similar to 6.9 with higher electron densities (N(e)greater than or similar to10(12) cm(-3)). For the most active stars, material exists at much higher temperatures [log T-e(K) greater than or equal to 6.9] as well. However, current ab initio stellar loop models cannot reproduce such a configuration. Analysis of the light curves of these systems reveals signatures of rotation of coronal material, as well as apparent seasonal (i.e., year-to-year) changes in the activity levels. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. RP Sanz-Forcada, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Sanz-Forcada, Jorge/C-3176-2017; OI Sanz-Forcada, Jorge/0000-0002-1600-7835; Brickhouse, Nancy/0000-0002-8704-4473 NR 84 TC 71 Z9 71 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2003 VL 145 IS 1 BP 147 EP 179 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 648KX UT WOS:000181151500008 ER PT J AU Lasso, E Naranjo, ME AF Lasso, E Naranjo, ME TI Effect of pollinators and nectar robbers on nectar production and pollen deposition in Hamelia patens (Rubiaceae) SO BIOTROPICA LA English DT Article DE Costa Rica; Hamelia patens; hummingbirds; La Selva; nectarivorous guild; nectar robbery; pollen deposition; tropical rain forest ID ROBBING BUMBLE BEES; SEED SET; ECOLOGICAL INTERACTIONS; IPOMOPSIS-AGGREGATA; PLANT FITNESS; HUMMINGBIRDS; INTENSITY; VISITORS; REPRODUCTION; AVAILABILITY AB We conducted experimental manipulations and field observations to determine the role of members of a nectarivorous guild (pollinators and robbers) on nectar production and pollen deposition in Hamelia patens at the La Selva Biological Station (Costa Rica). Seven pollinators (hummingbirds) and four robbers (I hummingbird and 3 perching birds) comprised the avian nectarivorous guild visiting H. patens during March 1997. In addition, two florivorous birds were observed visiting H. patens during the study. Pollinators accounted for 85.6 percent of the visits, robbers for 12.4 percent, and florivores for 2 percent of the visits. Visitation by pollinators and robbers was greatest when floral nectar was highest. No aggressive interactions between pollinators and robbers were observed during the study. Pollinators differed in their ability to carry and deposit pollen on the stigma. Territorial hummingbirds were the least effective pollinators but the most frequent visitors. Flowers were frequently robbed (71%) during the study. Flowers experimentally robbed did not increase nectar production compared to control flowers; therefore, robbery may not involve an extra energy investment in terms of nectar production. The number of pollen grains deposited on artificially robbed flowers was significantly less than the number found in flowers with extra nectar (nectar added) but did not differ from the number found in non-manipulated flowers, indicating that nectar robbers may not affect the foraging behavior of hummingbirds, and therefore pollen deposition. C1 Smithsonian Trop Res Inst, Ancon, Panama. Univ Los Andes Hechicera, Fac Ciencias, Dept Biol, Merida, Venezuela. RP Lasso, E (reprint author), Univ Illinois, Dept Plant Biol, 265 Morrill Hall,505 Goodwin Ave, Urbana, IL 61801 USA. OI Lasso, Eloisa/0000-0003-4586-8674 NR 44 TC 21 Z9 23 U1 5 U2 29 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2003 VL 35 IS 1 BP 57 EP 66 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 672PY UT WOS:000182530700007 ER PT J AU Hines, AH Jivoff, PR Bushmann, PJ van Montfrans, J Reed, SA Wolcott, DL Wolcott, TG AF Hines, AH Jivoff, PR Bushmann, PJ van Montfrans, J Reed, SA Wolcott, DL Wolcott, TG TI Evidence for sperm limitation in the blue crab, Callinectes sapidus SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Blue Crab Conference CY MAR, 2000 CL UNIV NORTH CAROLINA WILMINGTON, WILMINGTON, NC HO UNIV NORTH CAROLINA WILMINGTON ID CHIONOECETES-OPILIO BRACHYURA; OF-SAINT-LAWRENCE; SNOW CRAB; REPRODUCTIVE PRODUCTS; HOMARUS-AMERICANUS; SEXUAL COMPETITION; CHESAPEAKE BAY; EGG-PRODUCTION; FEMALE CHOICE; SEMINAL FLUID AB Reproductive success of female blue crabs may be limited by the amount of sperm received during the female's single, lifetime mating. Sperm must be stored in seminal receptacles until eggs are produced and fertilized months to years after mating. Further, intense fishing pressure impacts male abundance, male size and population sex ratio, which affect ejaculate quantity. We measured temporal variation in seminal receptacle contents in relation to brood production for two stocks differing in both fishing pressure on males and latitudinal effects on reproductive season: Chesapeake Bay, Maryland and Virginia, experienced intensive fishing and relatively short reproductive season; and the Indian River Lagoon, Florida, experienced lower exploitation and longer reproductive season. Nearly all (>98%) females were mated, and mating prevalence did not vary among sites during 1996. Seminal receptacle weight declined markedly for 2 mo following mating as seminal fluid disappeared to leave only spermatophores for long-term storage, which suggests that seminal fluid serves as a short-term sperm plug. Seminal receptacle weight in upper Chesapeake Bay declined by 31 % from 1992-1999, indicating that females received smaller ejaculates. In 1996, seminal receptacle contents were highest (3.75 g wet wt, 2.3 x 10(3) mug DNA, 1.2 x 10(9) sperm) in Florida, but were significantly lower by: 25% for weight and 50% for sperm number at the upper Chesapeake Bay site; and 30% for weight and 65% for sperm number at lower Chesapeake Bay sites. Generally, females receive 2-3 x 10(3) spermatophores and 10(8)-10(9) sperm cells for a full ejaculate, whereas females produce ca. 3 x 10(6) eggs per brood. Chesapeake Bay females appear to live about 3.5 yr, producing 1-3 broods (up to 9 x 10(6) eggs) per year and up to 6-7 broods (2.1 x 10(7) eggs) per lifetime. In contrast, Florida crabs produced up to 6-7 broods (2.1 X 101 eggs) per year. and up to 18 broods (5.4 x 10(7) eggs) per lifetime. In Florida, last broods produced by lab-held females were often infertile, indicating that females became sperm limited at the end of their lifetime. Experiments showed that male mating history affected female reproductive success, with females mated late in a sequence having only one third the brood hatching success of females mated early in the sequence. Sperm : egg ratios were estimated at 100: 1 to 400:1 for the first brood but only about 20:1 or 30:1 for maximum lifetime broods over 2 seasons, suggesting that about 67 x 10(6) sperm are used per brood of 3 x 10(6) eggs. A model of brood production and sperm depletion in blue crabs indicates that sperm limitation may be common in Florida as females age, and in Chesapeake Bay as a result of fishery-induced reductions in initial quantities of sperm transferred at mating. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. RP Hines, AH (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM hines@serc.si.edu NR 83 TC 62 Z9 66 U1 0 U2 10 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 MAR PY 2003 VL 72 IS 2 BP 287 EP 310 PG 24 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 732CV UT WOS:000185924000004 ER PT J AU Hines, AH AF Hines, AH TI Ecology of juvenile and adult blue crabs: Summary of discussion of research themes and directions SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Blue Crab Conference CY MAR, 2000 CL UNIV NORTH CAROLINA WILMINGTON, WILMINGTON, NORTH CAROLINA HO UNIV NORTH CAROLINA WILMINGTON ID CALLINECTES-SAPIDUS RATHBUN; CENTRAL CHESAPEAKE BAY; HABITAT FRAGMENTATION; POPULATION-DYNAMICS; DECAPOD CRUSTACEANS; TEMPORAL VARIATION; SHALLOW-WATER; NURSERY ROLE; ABUNDANCE; RECRUITMENT C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Hines, AH (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. NR 60 TC 9 Z9 9 U1 1 U2 5 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD MAR PY 2003 VL 72 IS 2 BP 423 EP 433 PG 11 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 732CV UT WOS:000185924000013 ER PT J AU Lipcius, RN Stockhausen, WT Seitz, RD Geer, PJ AF Lipcius, RN Stockhausen, WT Seitz, RD Geer, PJ TI Spatial dynamics and value of a marine protected area and corridor for the blue crab spawning stock in Chesapeake Bay SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Blue Crab Conference CY MAR, 2000 CL UNIV NORTH CAROLINA WILMINGTON, WILMINGTON, NC HO UNIV NORTH CAROLINA WILMINGTON ID CALLINECTES-SAPIDUS; CONSERVATION; MODEL AB In lower Chesapeake Bay, a 172,235 ha marine protected area and corridor (MPAC) was recently established to protect blue crab adult females either en route to or at the spawning grounds during the reproductive period. The MPAC was justified due to a recent substantial decline in spawning stock biomass. It was situated in waters deeper than 10 in throughout the lower bay due to the high abundances of adult females in this zone, and it was an expansion of a historical spawning sanctuary near the bay mouth to include northward extensions (upper and lower MPACs). We examined spatial dynamics of the blue crab spawning stock in relation to the MPAC through analyses of trawl Survey data (abundances of adult females and egg-bearing females from 1989-1997 and 1995-1997, respectively) partitioned by water depth, time (month and year), and spatial zone (upper MPAC, lower MPAC, MPAC Historical Sanctuary) during the reproductive period (June-September). Adult female abundance peaked at 6-14 m water depths. Consequently, nearly half of all adult females in the lower bay were deeper than 10 in, and therefore protected by the MPAC during the reproductive period, whereas the historical sanctuary protected about 1/3 that of the MPAC. All MPAC segments were utilized by adult females at different times of the spawning season, without consistent use of any particular segment. In contrast, abundance patterns of egg-bearing females were consistent and did not differ by developmental stage of the eggs. Peak abundances of egg-bearing females shifted from the northern to southern portions of the MPAC as the spawning season progressed. Differences in distribution of adult females and egg-bearing females demonstrated the importance of the expanded MPAC to the conservation of the spawning stock, which requires an extensive area to cover seasonal and yearly alterations in distribution. The expanded MPAC is much more effective than the historical sanctuary at protecting a consistent fraction of the blue crab spawning stock over the full spawning season and every year. Both the lower MPAC and historical sanctuary contained high abundances of adult females and egg-bearing females, and these segments therefore potentially function as corridors and spawning grounds. In contrast, whereas adult females were equally abundant in all MPAC segments, egg-bearing females were rarely common in the upper MPAC segment. Hence, the upper MPAC serves primarily as a corridor for females migrating to spawn or hatch their egg masses in the lower MPAC and historical sanctuary. The MPAC protects a major fraction of the spawning stock and spawning grounds both seasonally and yearly, and it encompasses a dispersal corridor for adult females in the deeper waters of Chesapeake Bay. The MPAC therefore serves as a foundation for long-term protection of the blue crab spawning stock, and should be utilized concurrently with complementary management measures to conserve the blue crab population in Chesapeake Bay. Furthermore, the MPAC for the blue crab in Chesapeake Bay may serve as a model system for investigating the value of marine protected areas for exploited marine populations with ontogenetically disjunct stages in the life cycle that encompass diverse habitats. C1 Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. RP Lipcius, RN (reprint author), Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, POB 1346, Gloucester Point, VA 23062 USA. EM rom@vims.edu NR 26 TC 25 Z9 25 U1 0 U2 11 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 MAR PY 2003 VL 72 IS 2 BP 453 EP 469 PG 17 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 732CV UT WOS:000185924000015 ER PT J AU Touwaide, A AF Touwaide, A TI Hellenism and hippocratism in Mediterranean Europe: On D. Coray SO BULLETIN OF THE HISTORY OF MEDICINE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0007-5140 J9 B HIST MED JI Bull. Hist. Med. PD SPR PY 2003 VL 77 IS 1 BP 195 EP 196 DI 10.1353/bhm.2003.0042 PG 2 WC Health Care Sciences & Services; History & Philosophy Of Science SC Health Care Sciences & Services; History & Philosophy of Science GA 655CB UT WOS:000181532800024 ER PT J AU Lagarde, F Bonnet, X Henen, B Legrand, A Corbin, J Nagy, K Naulleau, G AF Lagarde, F Bonnet, X Henen, B Legrand, A Corbin, J Nagy, K Naulleau, G TI Sex divergence in space utilisation in the steppe tortoise (Testudo horsfieldi) SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID GMELIN REPTILIA-TESTUDINIDAE; HOME-RANGE; MULTIPLE PATERNITY; SPERM STORAGE; POPULATION; MOVEMENT; TURTLES; ENVIRONMENT; DIMORPHISM; SELECTION AB In animal species without parental care, the fitness of males should increase with the number of females encountered, court, and fertilise, and the fitness of females depends strongly on the quantity and quality of resources acquired. This should translate into a marked sex differences in the patterns of space utilisation. We analysed the sex divergences in home range and movements pattern in the steppe tortoise (Testudo horsfieldi) in Uzbekistan. From the radio-tracking data of 36 individuals throughout the active season, the home range of the male steppe tortoise was estimated to be smaller than that of the female (24 vs. 57 ha), even when the analysis focused on the mating season only. During the mating season, males intensively patrolled a small area, going back and forth within their territory, thereby covering greater distances than females. The females movements were more unidirectional, resulting in large loops over a very extended home range. We proposed several nonexclusive hypothesis for such a pattern. C1 CNRS, Ctr Etude Biol Chize, F-79360 Villiers En Bois, France. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. Univ Calif Los Angeles, Dept Biol, Los Angeles, CA 90095 USA. RP Lagarde, F (reprint author), CNRS, Ctr Etude Biol Chize, F-79360 Villiers En Bois, France. RI Henen, Brian/S-6552-2016 OI Henen, Brian/0000-0003-3412-4944 NR 59 TC 21 Z9 21 U1 0 U2 12 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 2003 VL 81 IS 3 BP 380 EP 387 DI 10.1139/Z03-023 PG 8 WC Zoology SC Zoology GA 677BV UT WOS:000182787800004 ER PT J AU Cavender-Bares, J Wilczek, A AF Cavender-Bares, J Wilczek, A TI Integrating micro- and macroevolutionary processes in community ecology SO ECOLOGY LA English DT Editorial Material ID PHENOTYPIC PLASTICITY; EVOLUTION; PHYLOGENY; DIVERSITY; PLANTS; SPECIALIZATION; ADAPTATIONS; SPECIATION; BEETLES; FOREST C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Harvard Univ, Dept Organism & Evolut Biol, Cambridge, MA 02138 USA. RP Cavender-Bares, J (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM cavenderj@si.edu RI Cavender-Bares, Jeannine/K-5716-2013 NR 39 TC 39 Z9 40 U1 0 U2 17 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 2003 VL 84 IS 3 BP 592 EP 597 DI 10.1890/0012-9658(2003)084[0592:IMAMPI]2.0.CO;2 PG 6 WC Ecology SC Environmental Sciences & Ecology GA 656VF UT WOS:000181629500010 ER PT J AU Sims, HJ McConway, KJ AF Sims, HJ McConway, KJ TI Nonstochastic variation of species-level diversification rates within angiosperms SO EVOLUTION LA English DT Review DE angiosperms; diversity; evolutionary rates; likelihood; taxon pairs ID FLOWERING PLANTS; STRATIGRAPHIC RANGES; CONFIDENCE-INTERVALS; PHYLOGENETIC TREES; CENTRAL GEORGIA; FOSSIL FLOWERS; NUCLEOTIDE SUBSTITUTION; MOLECULAR PHYLOGENIES; ORGANISMAL DIVERSITY; EVOLUTIONARY PROCESS AB Variations in the origination and extinction rates of species over geological time often are linked with a range of factors, including the evolution of key innovations, changes in ecosystem structure, and environmental factors such as shifts in climate and physical geography. Before hypothesizing causality of a single factor, it is critical to demonstrate that the observed variation in diversification is significantly greater than one would expect due to natural stochasticity in the evolutionary branching process. Here, we use a likelihood-ratio test to compare taxonomic rate heterogeneity to a neutral birth-death model, using data on well-supported sister pairs of taxa and their species richness. We test the likelihood that the distribution of extant species among angiosperm genera and families could be the result of constant diversification rates. Results strongly support the conclusion that there is significantly more heterogeneity in diversity at the species level within angiosperms than would be expected due to stochastic processes. This result is consistent in datasets of genus pairs and family pairs and is not affected significantly by degrading pairs to simulate inaccuracy in the assumption of simultaneous origin of sister taxa. When we parse taxon pairs among higher groups of angiosperms, results indicate that a constant rates model is not rejected by rosid and basal eudicot pairs but is rejected by asterid and eumagnoliid pairs. These results provide strong support for the hypothesis that species-level rates of origination and/or extinction have varied nonrandomly within angiosperms and that the magnitude of heterogeneity varies among major groups within angiosperms. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Open Univ, Dept Stat, Milton Keynes MK7 6AA, Bucks, England. RP Sims, HJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM sims.hallie@nmnh.si.edu; k.j.mcconway@open.ac.uk RI McConway, Kevin/G-3729-2012 OI McConway, Kevin/0000-0002-0236-7231 NR 169 TC 29 Z9 29 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD MAR PY 2003 VL 57 IS 3 BP 460 EP 479 PG 20 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 666UA UT WOS:000182193800002 PM 12703936 ER PT J AU Fallon, SM Bermingham, E Ricklefs, RE AF Fallon, SM Bermingham, E Ricklefs, RE TI Island and taxon effects in parasitism revisited: Avian malaria in the Lesser Antilles SO EVOLUTION LA English DT Article DE avian malaria; coevolution; Haemoproteus; host-parasite interactions; Lesser Antilles; passerines; Plasmodium ID BLOOD PARASITES; HAEMATOZOAN INFECTIONS; MITOCHONDRIAL GENOME; REPRODUCTIVE SUCCESS; PLASMODIUM-ELONGATUM; NATURAL-SELECTION; SEXUAL SELECTION; PIED FLYCATCHER; GREAT TITS; HOST AB We identify and describe the distribution of 12 genetically distinct malaria parasite lineages over islands and hosts in four common passerine birds in the Lesser Antilles. Combined parasite prevalence demonstrates strong host effects, little or no island effect, and a significant host-times-island interaction, indicating independent outcomes of host-parasite infections among island populations of the same host species. Host- and/or island-specific parasite lineages do not explain these host-parasite associations; rather, individual lineages themselves demonstrate the same type of independent interactions. Unlike overall prevalence, individual parasite lineages show considerable geographic structure (i.e., island effects) as well as species effects indicating that parasite lineages are constrained in their ability to move between hosts and locations. Together, our results suggest an upper limit to the number of host individuals that malaria parasites, as a community, can infect. Within this limit, however, the relative frequency of the different lineages varies reflecting fine scale interactions between host and parasite populations. Patterns of host-parasite associations within this system suggest both historical co-evolution and ecologically dynamic and independent host-parasite interactions. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Fallon, SM (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. NR 60 TC 96 Z9 97 U1 2 U2 33 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 2003 VL 57 IS 3 BP 606 EP 615 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 666UA UT WOS:000182193800016 PM 12703950 ER PT J AU Bronson, CL Grubb, TC Braun, MJ AF Bronson, CL Grubb, TC Braun, MJ TI A test of the endogenous and exogenous selection hypotheses for the maintenance of a narrow avian hybrid zone SO EVOLUTION LA English DT Article DE endogenous selection; exogenous selection; hybrid zone; Poecile atricapilla; Poecile carolinensis; transplant experiment ID GRASSHOPPER PODISMA-PEDESTRIS; TRANSPLANT EXPERIMENTS; TOWNSENDS WARBLERS; NATURAL-SELECTION; MITOCHONDRIAL-DNA; CHICKADEES; HYBRIDIZATION; INVIABILITY; ASYMMETRIES; DROSOPHILA AB The contributions of genetic and environmental factors to differential reproductive success across hybrid zones have rarely been tested. Here, we report a manipulative experiment that simultaneously tested endogenous (genetic-based) and exogenous (environmental-based) selection within a hybrid zone. We transplanted mated pairs of two chickadee species (Poecile atricapilla and P. carolinensis) and their hybrids into isolated woodlots within their hybrid zone and monitored their reproductive success. Although clutch sizes were similar, based on an estimate of the genetic compatibility of a pair, hybrid pairs produced fewer nestlings and fledglings than did pairs of either parental species. According to a linear model generated from the data, a pure pair of either parental species would be expected to produce 1.91-2.48 times more fledglings per nesting attempt, respectively, than the average or least compatible pair in the experiment. Our result of decreased reproduction for hybrid pairs relative to parental species pairs within same environment (the hybrid zone in this experiment) support the endogenous selection hypothesis for maintenance of this hybrid zone. Because the experiment was conducted entirely within the hybrid zone (i.e., the same environment for parental and hybrid pairings), our data do not support the exogenous selection hypothesis as it predicts either all pairings doing poorly or the hybrid pairs more successful than the parental pairs. C1 Smithsonian Inst, Museum Support Ctr, Natl Museum Nat Hist, Lab Analyt Biol, Suitland, MD 20746 USA. Smithsonian Inst, Museum Support Ctr, Natl Museum Nat Hist, Dept Syst Biol, Suitland, MD 20746 USA. Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. RP Bronson, CL (reprint author), Ohio State Univ, Dept Internal Med, Div Immunol, Heart & Lung Res Inst 435, 473 W 12th Ave, Columbus, OH 43210 USA. NR 66 TC 41 Z9 41 U1 2 U2 14 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 2003 VL 57 IS 3 BP 630 EP 637 PG 8 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 666UA UT WOS:000182193800018 PM 12703952 ER PT J AU Stanley, JD Krom, MD Cliff, RA Woodward, JC AF Stanley, JD Krom, MD Cliff, RA Woodward, JC TI Short contribution: Nile flow failure at the end of the old kingdom, Egypt: Strontium isotopic and petrologic evidence SO GEOARCHAEOLOGY-AN INTERNATIONAL JOURNAL LA English DT Article ID HOLOCENE; FLUCTUATIONS; SEDIMENT; HISTORY; TROPICS; SAHARA; LAKES AB Strontium isotopic and petrologic information, obtained from sediment cores collected in the Nile delta of Egypt, indicate that paleoclimatic and Nile baseflow conditions changed considerably from about 4200 to 4000 cal yr B.P. in the Nile basin. Our study records a higher proportion of White Nile sediment transported during the annual floods at ca. 6100 cal yr B.P. than towards 4200 cal yr B.P., at which time suspended sediment from the Blue Nile formed a significantly larger fraction of the total load. This resulted from a decrease in vegetative cover and an increase in erosion rate accompanying the marked decline in rainfall. These new geoscience data indicate major changes in annual flooding and baseflow of the river Nile, marked short-term paleoclimatic-related events that may in part have led to the collapse of the Old Kingdom. (C) 2003 Wiley Periodicals, Inc. C1 Smithsonian Inst, Natl Museum Nat Hist, Geoarchaeol Global Change Program, Washington, DC 20560 USA. Univ Leeds, Sch Earth Sci, Leeds LS2 9JT, W Yorkshire, England. Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. RP Stanley, JD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Geoarchaeol Global Change Program, E-206, Washington, DC 20560 USA. NR 27 TC 50 Z9 55 U1 1 U2 33 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0883-6353 J9 GEOARCHAEOLOGY JI Geoarchaeology PD MAR PY 2003 VL 18 IS 3 BP 395 EP 402 DI 10.1002/gea.10065 PG 8 WC Archaeology; Geosciences, Multidisciplinary SC Archaeology; Geology GA 649GU UT WOS:000181199600004 ER PT J AU Coates, AG Aubry, MP Berggren, WA Collins, LS Kunk, M AF Coates, AG Aubry, MP Berggren, WA Collins, LS Kunk, M TI Early neogene history of the Central American arc from Bocas del Toro, western Panama SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article DE Neogene; Central America; Panama; Bocas del Toro; paleobathymetry; stratigraphy ID COSTA-RICA; LIMON-BASIN; PALEOENVIRONMENTS; STRATIGRAPHY; ISTHMUS AB A newly discovered sequence of lower to middle Miocene rocks from the eastern Bocas del Toro archipelago, western Panama, reveals the timing and environment of the earliest stages in the rise of the Isthmus of Panama in this region. Two new formations, the Punta Alegre Formation (lower Miocene, Aquitanian to Burdigalian) and the Valiente Formation (middle Miocene, Langhian to Serravallian), are here named and formally described. The Punta Alegre Formation contains a diagnostic microfauna of benthic and planktic foraminifera and calcareous nannofossils that indicate deposition in a 2000-m-deep pre-isthmian neotropical ocean from as old as 21.5-18.3 Ma. Its lithology varies from silty mudstone to muddy foraminiferal ooze with rare thin microturbidite layers near the top. The Valiente Formation, which ranges in age from 16.4 to ca. 12.0 Ma, lies with slight angular unconformity on the Punta Alegre Formation and consists of five lithofacies: (1) columnar basalt and flow breccia, (2) pyroclastic deposits, (3) coarse-grained volcaniclastic deposits, (4) coral-reef limestone with diverse large coral colonies, and (5) marine debris-flow deposits and microturbidites. These lithofacies are interpreted to indicate that after ca. 16 Ma a volcanic arc developed in the region of Bocas del Toro and that by ca. 12 Ma an extensively emergent archipelago of volcanic islands had formed. Ar-39/Ar-40 dating of basalt flows associated with the fossiliferous sedimentary rocks in the upper part of the Valiente Formation strongly confirms the ages derived from planktic foraminifera and nannofossils. Paleobathymetric analysis of the two new formations in the Valiente Peninsula and Popa Island, in the Bocas del Toro archipelago, shows a general shallowing from lower- through upper-bathyal to upper-neritic and emergent laharic and fluviatile deposits from ca. 19 to 12 Ma. The overlying nonconformable Bocas del Toro Group contains a lower transgressive sequence ranging from basal nearshore sandstone to upper-bathyal mudstone (ca. 8.15.3 Ma) and an upper regressive sequence (5.3-3.5 Ma). A similar paleobathymetric pattern is observed from the Gatun to Chagres Formations (12-6 Ma) in the Panama Canal Basin area and in the Uscari, Rio Banana, Quebrada Chocolate, and Moin Formations (8-1.7 Ma) in the southern Limon Basin of Costa Rica. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Montpellier, Inst Sci Evolut, Montpellier 5, France. Woods Hole Oceanog Inst, Dept Geol & Geophys, Woods Hole, MA 02543 USA. Florida Int Univ, Dept Earth Sci, Miami, FL 33199 USA. US Geol Survey, Denver Fed Ctr, Lakewood, CO 80225 USA. RP Coates, AG (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. NR 40 TC 69 Z9 76 U1 2 U2 16 PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER PI DENVER PA 720 S COLORADO BLVD, STE 960-S, DENVER, CO 80246 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAR PY 2003 VL 115 IS 3 BP 271 EP 287 DI 10.1130/0016-7606(2003)115<0271:ENHOTC>2.0.CO;2 PG 17 WC Geosciences, Multidisciplinary SC Geology GA 649EV UT WOS:000181194700002 ER PT J AU Aranda-Gomez, JJ Luhr, JF Housh, TB Connor, CB Becker, T Henry, CD AF Aranda-Gomez, JJ Luhr, JF Housh, TB Connor, CB Becker, T Henry, CD TI Synextensional Pliocene-Pleistocene eruptive activity in the Camargo volcanic field, Chihuahua, Mexico SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article DE basin and range province; Chihuahua; Mexico; extension faults; intraplate; Pliocene; slip rates ID WESTERN UNITED-STATES; NORTHERN MEXICO; SOUTHERN BASIN; LA-OLIVINA; CENOZOIC EXTENSION; TERTIARY VOLCANISM; ALKALI BASALTS; DURANGO-CITY; PETROLOGY; RANGE AB The Camargo volcanic field is the largest mafic alkalic volcanic field in the Mexican Basin and Range province, and the relationship between volcanism and normal faulting is especially strong. The Camargo volcanic field lies in the northern part of the province, midway between the Sierra Madre Occidental and Trans-Pecos Texas. It is formed by Pliocene-Pleistocene (4.7-0.09 Ma) intraplate mafic alkalic volcanic rocks, some of which contain peridotite, pyroxenite, and granulite xenoliths. The volcanic field covers similar to3000 km(2) and has an estimated volume of similar to 120 km(3) erupted from >300 recognized vents. Twenty-six new Ar-40/Ar-39 age determinations for the Camargo volcanic field and its environs show that volcanic activity began in the southwest part of the field and shifted toward the northeast at similar to15 mm/yr. The average magmatic eruption rate during growth of the field was similar to0.026 km(3)/k.y. The Camargo volcanic field lies within an accommodation zone with west-dipping faults and east-tilted blocks to the north and east-dipping faults and west-tilted blocks to the south. These faults are expressed in the volcanic field by a N30degreesW-trending graben with scarps up to similar to100 m high through its central part. Volcanism and faulting were at least in part coeval, and younger volcanic products commonly drape fault scarps that cut earlier lavas. Normal faulting is bracketed between 4.7 and 2.1 Ma and may have also migrated northeastward. Estimated vertical slip rates on four Pliocene faults range from 0.03 mm/yr, a likely long-term rate, to 1.67 mm/ yr, interpreted as a short-term rate operative during periods of active faulting. Northwest-striking normal faults that cut alluvial-fan deposits and Pleistocene lavas in the northern Camargo volcanic field and geomorphic evidence for recent uplift to the south of the volcanic field suggest that the region is still extending. C1 Univ Nacl Autonoma Mexico, Ctr Geociencias, Queretaro 76001, Mexico. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. Univ S Florida, Dept Geol, Tampa, FL 33620 USA. Berkeley Geochronol Ctr, Berkeley, CA 94709 USA. Univ Nevada, Nevada Bur Mines & Geol, Reno, NV 89557 USA. RP Aranda-Gomez, JJ (reprint author), Univ Nacl Autonoma Mexico, Ctr Geociencias, Campus Juriquilla,POB 1-742, Queretaro 76001, Mexico. NR 67 TC 31 Z9 32 U1 0 U2 1 PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER PI DENVER PA 720 S COLORADO BLVD, STE 960-S, DENVER, CO 80246 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAR PY 2003 VL 115 IS 3 BP 298 EP 313 DI 10.1130/0016-7606(2003)115<0298:SPPEAI>2.0.CO;2 PG 16 WC Geosciences, Multidisciplinary SC Geology GA 649EV UT WOS:000181194700004 ER PT J AU Watters, TR AF Watters, TR TI Lithospheric flexure and the origin of the dichotomy boundary on Mars SO GEOLOGY LA English DT Article DE Mars; tectonics; flexure; dichotomy boundary; elastic thickness ID ORBITER LASER ALTIMETER; CRUSTAL DICHOTOMY; THERMAL EVOLUTION; GLOBAL SURVEYOR; PLATE-TECTONICS; LOBATE SCARPS; GIANT IMPACT; TOPOGRAPHY; STRESS; CONVECTION AB The crustal dichotomy between the ancient highlands of the Southern Hemisphere and the young-appearing northern lowlands is a defining feature of Mars. In the Eastern Hemisphere the dichotomy boundary is marked by a prominent scarp and extensional and compressional tectonic features. Topographic data across the boundary returned from the Mars Global Surveyor indicate lithospheric flexure of the southern highlands. The topography of the boundary can be fit by a universal lithospheric deflection profile that corresponds to an elastic thickness of similar to31-36 km. Flexure of the southern highlands may be due to late Noachian-early Hesperian vertical loading of the northern lowlands. Fracturing and normal faulting along the boundary may be in response to bending stresses, while thrust faulting may result from a combination of stresses due to flexure, erosion, and global contraction. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 35 TC 30 Z9 30 U1 0 U2 1 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD MAR PY 2003 VL 31 IS 3 BP 271 EP 274 DI 10.1130/0091-7613(2003)031<0271:LFATOO>2.0.CO;2 PG 4 WC Geology SC Geology GA 649GN UT WOS:000181199100020 ER PT J AU Drake, JB Knox, RG Dubayah, RO Clark, DB Condit, R Blair, JB Hofton, M AF Drake, JB Knox, RG Dubayah, RO Clark, DB Condit, R Blair, JB Hofton, M TI Above-ground biomass estimation in closed canopy Neotropical forests using lidar remote sensing: factors affecting the generality of relationships SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE above-ground biomass; allometry; carbon cycle; Central America; environmental factors; forest structure; laser altimetry; lidar; remote sensing; tropical forests ID LARGE-FOOTPRINT LIDAR; TROPICAL RAIN-FOREST; LASER ALTIMETER; HEIGHT PROFILES; LANDSCAPE-SCALE; BIOSPHERE MODEL; COSTA-RICA; VEGETATION; SECONDARY; BRAZIL AB Aim Previous studies have developed strong, site-specific relationships between canopy metrics from lidar (light detecting and ranging) remote sensing data and forest structural characteristics such as above-ground biomass (AGBM), but the generality of these relationships is unknown. In this study, we examine the generality of relationships between lidar metrics and forest structural characteristics, including AGBM, from two study areas in Central America with different precipitation patterns. Location A series of tropical moist forest sites in Panama and a tropical wet forest in Costa Rica. Methods Canopy metrics (e.g. canopy height) were calculated from airborne lidar data. Basal area, mean stem diameter and AGBM were calculated from measurements taken as a part of ongoing forest dynamics studies in both areas. We examined the generality of relationship between lidar metrics and forest structure, and possible environmental effects (e.g. leaf phenology). Results We found that lidar metrics were strongly correlated (R-2:0.65-0.92) with mean stem diameter, basal area and AGBM in both regions. We also show that the relationships differed between these regions. Deciduousness of canopy trees in the tropical moist forest area accounted for the differences in predictive equations for stem diameter and basal area. The relationships between lidar metrics and AGBM, however, remained significantly different between the two study areas even after adjusting for leaf drop. We attribute this to significant differences in the underlying allometric relationships between stem diameter and AGBM in tropical wet and moist forests. Conclusions Important forest structural characteristics can be estimated reliably across a variety of conditions sampled in these closed-canopy tropical forests. Environmental factors such as drought deciduousness have an important influence on these relationships. Future efforts should continue to examine climatic factors that may influence the generality of the relationships between lidar metrics and forest structural characteristics and assess more rigorously the generality of field-derived allometric relationships. C1 Univ Maryland, Dept Geog, College Pk, MD 20742 USA. NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. NASA, Laser Remote Sensing Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Drake, JB (reprint author), Univ Georgia, Warnell Sch Forest Resources, Athens, GA 30602 USA. RI Knox, Robert/E-9657-2011; Blair, James/D-3881-2013; Beckley, Matthew/D-4547-2013 NR 58 TC 146 Z9 149 U1 5 U2 63 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0960-7447 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD MAR PY 2003 VL 12 IS 2 BP 147 EP 159 DI 10.1046/j.1466-822X.2003.00010.x PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 652TU UT WOS:000181396700006 ER PT J AU Rappole, JH Helm, H Ramos, MA AF Rappole, JH Helm, H Ramos, MA TI An integrative framework for understanding the origin and evolution of avian migration SO JOURNAL OF AVIAN BIOLOGY LA English DT Editorial Material ID BIRD POPULATION; FLYCATCHERS; ECOLOGY C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA. Max Planck Res Ctr Ornithol, D-82346 Andechs, Germany. World Bank, Global Environm Facil, Washington, DC 20433 USA. RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 64 TC 27 Z9 27 U1 0 U2 25 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 2003 VL 34 IS 1 BP 124 EP 128 PG 5 WC Ornithology SC Zoology GA 676GQ UT WOS:000182743300017 ER PT J AU Wright, TF Cortopassi, KA Bradbury, JW Dooling, RJ AF Wright, TF Cortopassi, KA Bradbury, JW Dooling, RJ TI Hearing and vocalizations in the orange-fronted conure (Aratinga canicularis) SO JOURNAL OF COMPARATIVE PSYCHOLOGY LA English DT Article ID PARAKEET MELOPSITTACUS-UNDULATUS; AUDITORY INTENSITY DISCRIMINATION; ACOUSTIC COMMUNICATION; THRESHOLDS; EVOLUTION; NOISE; SENSITIVITY; PERCEPTION; BIRDS; SONG AB The auditory sensitivities of the orange-fronted conure (Aratinga canicularis) were examined in relation to the spectral characteristics of its vocalizations. Absolute thresholds, masked thresholds, frequency difference limens, and intensity difference limens for pure tones were obtained using psychoacoustic techniques. In general, hearing abilities are similar to those found in many avian auditory generalists. One exception is the unusually low critical ratio (masked threshold) between 2.0 and 4.0 kHz, similar to that previously found in the budgerigar (Melopsittacus undulatus). These auditory sensitivities were compared with average spectra for (a) contact calls and (b) a general sample of vocalizations recorded from wild birds. The spectral regions of both greatest vocal energy and best auditory sensitivity were between 2.0 and 5.0 kHz. C1 Univ Maryland, Dept Psychol, College Pk, MD 20742 USA. Cornell Lab Ornithol, Macaulay Lib Nat Sounds, Ithaca, NY USA. RP Smithsonian Natl Zoo, Genet Mol Lab, 3001 Connecticut Ave, Washington, DC 20008 USA. EM tw98@umail.umd.edu FU NIDCD NIH HHS [DC00046, DC00198]; NIMH NIH HHS [F32 MH012111, MH12111] NR 40 TC 17 Z9 18 U1 2 U2 7 PU AMER PSYCHOLOGICAL ASSOC PI WASHINGTON PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA SN 0735-7036 EI 1939-2087 J9 J COMP PSYCHOL JI J. Comp. Psychol. PD MAR PY 2003 VL 117 IS 1 BP 87 EP 95 DI 10.1037/0735-7036.117.1.87 PG 9 WC Behavioral Sciences; Psychology; Psychology, Multidisciplinary; Zoology SC Behavioral Sciences; Psychology; Zoology GA 667WD UT WOS:000182256800011 PM 12735368 ER PT J AU Srygley, RB AF Srygley, RB TI Wind drift compensation in migrating dragonflies Pantala (Odonata : Libellulidae) SO JOURNAL OF INSECT BEHAVIOR LA English DT Article DE insect; flight; energetics; optimal migration; behavioral ecology; tropical ID NATURAL FREE-FLIGHT; BUTTERFLIES; LEPIDOPTERA; PHYSIOLOGY; SEAS AB Tailwind drift compensation serves to maximize a migrant's flight distance on a given amount of energy, and crosswind drift compensation serves to hold a course true and minimize the distance flown. With full or part compensation, airspeeds are predicted to increase with greater crosswind drift. To test whether migrating dragonflies compensated for wind drift, I measured the velocity and heading of Pantala hymenaea and P. flavescens in natural flight over a lake and the ambient wind speed and direction. P. hymenaea flew northeasterly (58degrees), whereas P. flavescens flew significantly more east-north easterly (74degrees) throughout the day. Pantala spp. demonstrated part compensation for changes in crosswind drift within individuals (mean compensation = 54%, P = 0.0000), evidence for use of a ground reference to correct for drift when flying over water. Among individuals, P. flavescens compensated for crosswind drift. P. hymenaea overcompensated and then drifted downwind on one morning and compensated for crosswind drift on the next. As predicted from optimal migration theory, airspeed (5.0 m/s for both species with no tailwind) decreased with tailwind velocity both among individuals ( data for both species pooled [n = 19]; P < 0.0001) and within each individual as it crossed the lake (P = 0.0016). C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Oxford, Dept Zool, Oxford OX1 3PS, England. RP Srygley, RB (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. NR 22 TC 21 Z9 27 U1 0 U2 10 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0892-7553 J9 J INSECT BEHAV JI J. Insect Behav. PD MAR PY 2003 VL 16 IS 2 BP 217 EP 232 DI 10.1023/A:1023915802067 PG 16 WC Entomology SC Entomology GA 683BJ UT WOS:000183126600004 ER PT J AU Ospina, CA Rodriguez, AD Ortega-Barria, E Capson, TL AF Ospina, CA Rodriguez, AD Ortega-Barria, E Capson, TL TI Briarellins J-P and polyanthellin A: New eunicellin-based diterpenes from the gorgonian coral Briareum polyanthes and their antimalarial activity SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID MARINE NATURAL-PRODUCTS; SCLEROPHYTIN-A; ASBESTINUM PALLAS; (-)-SCLEROPHYTIN-A; CONSTITUENTS; ACETATE AB A new chemical study of the hexane extract of the gorgonian Briareum polyanthes collected in Puerto Rico afforded 10 new diterpenes of the eunicellin class, briarellins 1-9 and polyanthellin A (10), along with the known diterpene briarellin D (11). The structures and relative stereochemistry of metabolites 1-10 were assigned on the basis of NMR studies, chemical methods, and comparisons to the spectral properties of 11. A reassessment of prior structural assignment for briarellin A and two known sclerophytin-type diterpenes, 13 and 14, is proposed. Antimalarial tests on 1-6 and 8-12 indicated that they were active against Plasmodium falciparum. C1 Univ Puerto Rico, Dept Chem, Rio Piedras, PR 00931 USA. Florida State Univ, Cell & Mol Biol Pathogens Unit, Inst Trop Med & Hlth Sci, Balboa, Panama. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Rodriguez, AD (reprint author), Univ Puerto Rico, Dept Chem, POB 23346, Rio Piedras, PR 00931 USA. EM arodrig@goliath.cnnet.clu.edu RI Johnson, Selena/K-3541-2013 FU FIC NIH HHS [1 UO1TW01021-01]; NINDS NIH HHS [U54-NS39408-04] NR 30 TC 39 Z9 42 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD MAR PY 2003 VL 66 IS 3 BP 357 EP 363 DI 10.1021/np0204500 PG 7 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 662AL UT WOS:000181923100007 PM 12662092 ER PT J AU Suarez, W Olson, SL AF Suarez, W Olson, SL TI Red-shouldered Hawk and Aplomado Falcon from quaternary asphalt deposits in Cuba SO JOURNAL OF RAPTOR RESEARCH LA English DT Article DE Aplomado Falcon; Falco femoralis; Red-Shouldered Hawk; Buteo lineatus; Antilles; Cuba; extinctions; fossil birds; Quaternary; West Indies ID AVES C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Museo Nacl Hist Nat, Havana 10100, Cuba. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 18 TC 2 Z9 2 U1 0 U2 3 PU RAPTOR RESEARCH FOUNDATION INC PI HASTINGS PA 14377 117TH STREET SOUTH, HASTINGS, MN 55033 USA SN 0892-1016 J9 J RAPTOR RES JI J. Raptor Res. PD MAR PY 2003 VL 37 IS 1 BP 71 EP 75 PG 5 WC Ornithology SC Zoology GA 673CJ UT WOS:000182561800011 ER PT J AU Andersen, NM Polhemus, DA AF Andersen, NM Polhemus, DA TI A new genus of terrestrial Mesoveliidae from the Seychelles (Hemiptera : Gerromorpha) SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Mesoveliidae; Seychelles; new genus; new species; zoogeography ID WATER-STRIDER; HETEROPTERA AB A new genus of Mesoveliidae, Seychellovelia, with a single included species, S. hygrobia n. sp., is described from the islands of Silhouette and Mahe in the granitic Seychelles. This new taxon is compared to other mesovehid genera, and its key morphological characters illustrated. Information is also provided on the habitat preferences of S. hygrobia, and an updated distributional map of mesoveliid genera on a world basis is provided, accompanied by a discussion of zoogeographical implications. C1 Univ Copenhagen, Zool Museum, DK-2100 Copenhagen, Denmark. Smithsonian Inst, Museum Natl Hist Nat, Dept Systemat Biol, Washington, DC 20560 USA. RP Andersen, NM (reprint author), Univ Copenhagen, Zool Museum, Univ Pk 15, DK-2100 Copenhagen, Denmark. NR 16 TC 11 Z9 13 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 2003 VL 111 IS 1 BP 12 EP 21 DI 10.1664/0028-7199(2003)111[0012:ANGOTM]2.0.CO;2 PG 10 WC Entomology SC Entomology GA 711KT UT WOS:000184740300002 ER PT J AU Polhemus, DA Polhemus, JT AF Polhemus, DA Polhemus, JT TI A review of the Veliinae of Vietnam (Heteroptera : Veliidae) with description of a new Velia species SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Asia; Veliidae; Vietnam; new species; new records; distributions AB The Veliinae of Vietnam are reviewed. and the new species Velia tonkina described from the Huong Lien Son mountains in the far north of the country. Three additional species of Veliinae, Chenevelia stridulans, Angilia bispinosa, and Angilia orientalis, are recorded from Vietnam for the first time. Distribution maps are provided for all these species, dorsal habitus illustrations are provided for Velia tonkina and Chenevelia stridulans, and illustrations of male genitalic structures are provided for Velia tonkina. C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. Colorado Entomol Inst, Englewood, CO 80110 USA. RP Polhemus, DA (reprint author), Smithsonian Inst, Dept Systemat Biol, MRC 105, Washington, DC 20560 USA. NR 7 TC 2 Z9 2 U1 0 U2 0 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SPR PY 2003 VL 111 IS 1 BP 29 EP 40 DI 10.1664/0028-7199(2003)111[0029:AROTVO]2.0.CO;2 PG 12 WC Entomology SC Entomology GA 711KT UT WOS:000184740300004 ER PT J AU Seago, A Lingafelter, SW AF Seago, A Lingafelter, SW TI Discovery of Crepidodera bella Parry (Coleoptera : Chrysomelidae : Alticini) in Maryland and redescription SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Crepidodera; Chrysomelidae; flea beetle; Maryland; Salix; willow; redescription; range extension AB Crepidodera bella Parry (Coleoptera: Chrysomelidae: Alticini), previously known only from Florida, South Carolina, Alabama, and Louisiana, is discovered in central Maryland. This species is sympatric with C. browni Parry on Salix nigra growing along swamps in the McKee-Besher Wildlife Management Area (39degrees04'30"N, 77degrees23'00"W). Morphological features of the integument and genitalia are described and compared to C. browni. C1 Cornell Univ, Ithaca, NY 14853 USA. Smithsonian Inst, Natl Museum Nat Hist, Res Training Program, Washington, DC 20560 USA. USDA, ARS, PSI, Systemat Entomol Lab, Washington, DC 20250 USA. RP Seago, A (reprint author), Cornell Univ, Ithaca, NY 14853 USA. RI Seago, Ainsley/B-4211-2009 NR 5 TC 2 Z9 2 U1 0 U2 0 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SPR PY 2003 VL 111 IS 1 BP 51 EP 56 DI 10.1664/0028-7199(2003)111[0051:DOCBPC]2.0.CO;2 PG 6 WC Entomology SC Entomology GA 711KT UT WOS:000184740300007 ER PT J AU Lingafelter, SW AF Lingafelter, SW TI New host and elevation records for Moneilema appressum LeConte (Coleoptera : Cerambycidae : Lamiinae) SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE Moneilenia; Echinocereus; Opuntia; cactus; Lamiinae; Arizona; hostplants; elevation record AB An isolated population of Moneilema appressum LeConte was discovered above Long Park in the Chiricahua Mountains of southeastern Arizona (31degrees52'44"N, 109degrees17'12"W) during July 2001. Specimens of this flightless lamiine cerambycid were observed hiding and walking in the junctures of Echinocereus coccineus Engelmann (Cactaceae) at 2,760 m (9,055 feet). These data represent new host plant and elevation records for this species. C1 USDA, ARS, PSI, Systemat Entomol Lab, Washington, DC 20250 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Lingafelter, SW (reprint author), USDA, ARS, PSI, Systemat Entomol Lab, Washington, DC 20250 USA. NR 10 TC 4 Z9 4 U1 1 U2 2 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SPR PY 2003 VL 111 IS 1 BP 57 EP 60 DI 10.1664/0028-7199(2003)111[0057:NHAERF]2.0.CO;2 PG 4 WC Entomology SC Entomology GA 711KT UT WOS:000184740300008 ER PT J AU Riley, S AF Riley, S TI Man and wife. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 1 PY 2003 VL 128 IS 4 BP 120 EP 120 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 673WN UT WOS:000182603400179 ER PT J AU Mate, JL AF Mate, JL TI Ecological, genetic, and morphological differences among three Pavona (Cnidaria : Anthozoa) species from the Pacific coast of Panama SO MARINE BIOLOGY LA English DT Article ID CORAL MONTASTRAEA-ANNULARIS; SCLERACTINIAN CORALS; EASTERN PACIFIC; REEF CORALS; INTERSPECIFIC AGGRESSION; REPRODUCTIVE ISOLATION; COMMUNITY STRUCTURE; COSTA-RICA; FERTILIZATION; POPULATIONS AB Ecological, genetic, and morphological differences among three Panamanian Pacific Pavona species with strongly developed collines (Pavona varians, P. frondifera, and P. chiriquiensis) were examined. Ecological factors included geographical distributions of species, habitat preferences, interspecific interactions, reproductive ecology, and tolerance to bleaching. Genetic differences were based on the electrophoretic analysis of ten allozyme loci. Morphological analyses consisted of tissue coloration, colony morphology, and measurements and counts of ten macro- and micro-skeletal characters. P. varians, present on reefs or in coral communities, is the most widely distributed and shows considerable morphological variation. P. chiriquiensis, a recently described species, encrusts basalt rock and has little morphological variation. P. frondifera is a reef dweller with a compact foliose morphology. Tissue coloration varies from light to dark brown in P. varians, from pink to brown in P. frondifera, and from brick red to brown or silvery in Pavona chiriquiensis. Also, the white to silvery polyp mouths of the latter species are a diagnostic feature that allows an easy identification in the field. Aggressive dominance during short-term interspecific interactions were as follows: Pavona chiriquiensis > P. varians > P. frondifera. P. chiriquiensis and P. varians showed contrasting responses to sea warming during the 1997-1998 El Nino, Southern Oscillation. Whereas entire P. chiriquiensis bleached and died within 4 weeks of exposure to 30-31degreesC, colonies of P. varians did so only on their upper surfaces. The response of P. frondifera to elevated temperatures was not observed because it is mainly present in the Gulf of Panama where coral bleaching was absent in 1997-1998. The genetic data indicated that P. chiriquiensis differed strongly from both P. varians and P. frondifera, with Nei's unbiased genetic distances of 0.434 and 0.379, respectively. A fixed difference between P. varians and P. frondifera, and P. chiriquiensis exists at the triose phosphate isomerase (TPI-2) locus. A nearly fixed difference between P. chiriquiensis and P. frondifera and between P. chiriquiensis and P. varians was found at the hexokinase (HK) locus. P. varians differed slightly from P. frondifera with Nei's unbiased genetic distance of 0.068. No fixed difference was found between P. varians and P. frondifera. There were strong differences between P. chiriquiensis and P. varians in spawning times and gamete characteristics. Spawning in P. varians and P. chiriquiensis is 12 h out of phase. Also, eggs of the former species are white to beige and positively buoyant whereas those of the latter species are dark green and neutrally to negatively buoyant. No reproductive data are yet available for P. frondifera. Calicular diameters are significantly greater in P. chiriquiensis than in the other two species. In contrast, corallum thickness is greater in P. varians and P. frondifera than in P. chiriquiensis. Canonical discriminant function analysis readily separated the three species. C1 Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. RP Mate, JL (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. NR 75 TC 8 Z9 9 U1 0 U2 7 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAR PY 2003 VL 142 IS 3 BP 427 EP 440 DI 10.1007/s00227-002-0956-9 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 670BR UT WOS:000182387900003 ER PT J AU Dick, CW Etchelecu, G Austerlitz, F AF Dick, CW Etchelecu, G Austerlitz, F TI Pollen dispersal of tropical trees (Dinizia excelsa: Fabaceae) by native insects and African honeybees in pristine and fragmented Amazonian rainforest SO MOLECULAR ECOLOGY LA English DT Article DE Apis mellifera; microsatellites; pollen flow; pollination; tropical rainforest; TwoGener analysis ID N INDEPENDENT LOCI; RAIN-FOREST; 2-GENERATION ANALYSIS; HABITAT FRAGMENTATION; GENETIC CONSEQUENCES; SPECIES RICHNESS; MATING SYSTEMS; DRY FOREST; SEED SET; BEES AB Tropical rainforest trees typically occur in low population densities and rely on animals for cross-pollination. It is of conservation interest therefore to understand how rainforest fragmentation may alter the pollination and breeding structure of remnant trees. Previous studies of the Amazonian tree Dinizia excelsa (Fabaceae) found African honeybees (Apis mellifera scutellata ) as the predominant pollinators of trees in highly disturbed habitats, transporting pollen up to 3.2 km between pasture trees. Here, using microsatellite genotypes of seed arrays, we compare outcrossing rates and pollen dispersal distances of (i) remnant D. excelsa in three large ranches, and (ii) a population in undisturbed forest in which African honeybees were absent. Self-fertilization was more frequent in the disturbed habitats (14%, n = 277 seeds from 12 mothers) than in undisturbed forest (10%, n = 295 seeds from 13 mothers). Pollen dispersal was extensive in all three ranches compared to undisturbed forest, however. Using a twogener analysis, we estimated a mean pollen dispersal distance of 1509 m in Colosso ranch, assuming an exponential dispersal function, and 212 m in undisturbed forest. The low effective density of D. excelsa in undisturbed forest (similar to0.1 trees/ha) indicates that large areas of rainforest must be preserved to maintain minimum viable populations. Our results also suggest, however, that in highly disturbed habitats Apis mellifera may expand genetic neighbourhood areas, thereby linking fragmented and continuous forest populations. C1 Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. INRA Domaine Hermitage, Lab Genet Ameliorat Arbres Forestiers, F-33612 Pierroton F Cestas, France. RP Dick, CW (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Dick, Christopher/A-8744-2008 NR 79 TC 206 Z9 220 U1 7 U2 52 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD MAR PY 2003 VL 12 IS 3 BP 753 EP 764 DI 10.1046/j.1365-294X.2003.01760.x PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 649WL UT WOS:000181230900017 PM 12675830 ER PT J AU Bate, MR Bonnell, IA Bromm, V AF Bate, MR Bonnell, IA Bromm, V TI The formation of a star cluster: predicting the properties of stars and brown dwarfs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE accretion, accretion discs; hydrodynamics; binaries : general; stars : formation; stars : low-mass, brown dwarfs; stars : luminosity function, mass function ID INITIAL MASS FUNCTION; ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; SMOOTHED PARTICLE HYDRODYNAMICS; ROTATING INTERSTELLAR CLOUDS; ELONGATED CYLINDRICAL CLOUDS; SOLAR-TYPE STARS; SELF-GRAVITATIONAL HYDRODYNAMICS; WEAKLY MAGNETIZED DISKS; LOCAL SHEAR INSTABILITY AB We present results from the largest numerical simulation of star formation to resolve the fragmentation process down to the opacity limit. The simulation follows the collapse and fragmentation of a large-scale turbulent molecular cloud to form a stellar cluster and, simultaneously, the formation of circumstellar discs and binary stars. This large range of scales enables us to predict a wide variety of stellar properties for comparison with observations. The calculation clearly demonstrates that star formation is a highly-dynamic and chaotic process. Star formation occurs in localized bursts within the cloud via the fragmentation both of dense molecular cloud cores and of massive circumstellar discs. Star-disc encounters form binaries and truncate discs. Stellar encounters disrupt bound multiple systems. We find that the observed statistical properties of stars are a natural consequence of star formation in such a dynamical environment. The cloud produces roughly equal numbers of stars and brown dwarfs, with masses down to the opacity limit for fragmentation (approximate to5 Jupiter masses). The initial mass function is consistent with a Salpeter slope (Gamma=-1.35) above 0.5 M(circle dot) , a roughly flat distribution (Gamma= 0) in the range 0.006-0.5 M(circle dot) , and a sharp cut-off below approximate to0.005 M(circle dot). This is consistent with recent observational surveys. The brown dwarfs form by the dynamical ejection of low-mass fragments from dynamically unstable multiple systems before the fragments have been able to accrete to stellar masses. Close binary systems (with separations less than or similar to10 au) are not formed by fragmentation in situ . Rather, they are produced by hardening of initially wider multiple systems through a combination of dynamical encounters, gas accretion, and/or the interaction with circumbinary and circumtriple discs. Finally, we find that the majority of circumstellar discs have radii less than 20 au due to truncation in dynamical encounters. This is consistent with observations of the Orion Trapezium cluster and implies that most stars and brown dwarfs do not form large planetary systems. C1 Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bate, MR (reprint author), Univ Exeter, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England. EM mbate@astro.ex.ac.uk NR 173 TC 474 Z9 475 U1 2 U2 10 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 MAR 1 PY 2003 VL 339 IS 3 BP 577 EP 599 DI 10.1046/j.1365-8711.2003.06210.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DN UT WOS:000181077300001 ER PT J AU Jonker, PG van der Klis, M Groot, PJ AF Jonker, PG van der Klis, M Groot, PJ TI The mass of the neutron star in the low-mass X-ray binary 2A 1822-371 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques : radial velocities; stars : individual : 2A 1822-371; stars : neutron; X-rays : stars ID CATACLYSMIC VARIABLES; SECONDARY STAR; RADIO PULSARS; DISCOVERY; X-1822-371; IRRADIATION; MODULATION; VELOCITY AB Using phase-resolved spectroscopic observations obtained with the Ultraviolet and Visual Echelle Spectrograph on the ESO Kueyen Very Large Telescope, supplemented by spectroscopic observations obtained with the Boller and Chivens spectrograph on the Walter Baade Magellan Telescope, we have found sinusoidal radial velocity variations with a semi-amplitude of 327 +/- 17 km s(-1) . From previous observations and from the fact that the epoch of minimum velocity arrived early with respect to the epoch calculated from pulse timing, we know that the companion star is suffering from irradiation. Since we most likely observed primarily the side of the companion star facing the observer at phase similar to0.75, the velocity quoted above is not the true radial velocity semi-amplitude of the companion star. Assuming a uniform contribution to the line profile from this hemisphere yields a radial velocity semi-amplitude of 280 +/- 26 km s(-1)for a systemic velocity of 54 +/- 24 km s(-1); if the contribution is instead weighted somewhat more towards the side of the companion facing the X-ray source then the true semi-amplitude is larger than this value. Together with the well-constrained inclination (81degrees < i < 84degrees) and the mass function determined from pulse-timing analysis(2.03 +/- 0.03 x 10(-2) M-circle dot ), we derive a lower limit to the mass of the neutron star and to that of the companion star of 0.97 +/- 0.24 and 0.33 +/- 0.05 M-circle dot , respectively (1sigma; including uncertainties in the inclination). We briefly discuss other aspects of the spectrum and the implications of our findings. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nijmegen, Dept Astrophys, Nijmegen, Netherlands. RP Jonker, PG (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RI Groot, Paul/K-4391-2016 OI Groot, Paul/0000-0002-4488-726X NR 35 TC 28 Z9 29 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 MAR 1 PY 2003 VL 339 IS 3 BP 663 EP 668 DI 10.1046/j.1365-8711.2003.06193.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DN UT WOS:000181077300009 ER PT J AU Strader, J Brodie, JP Huchra, JP AF Strader, J Brodie, JP Huchra, JP TI Spectroscopy of a globular cluster in the Local Group dwarf irregular NGC 6822 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE globular clusters : general; galaxies : individual : NGC 6822; galaxies : star clusters ID SMALL-MAGELLANIC-CLOUD; HUBBLE-SPACE-TELESCOPE; STAR-CLUSTERS; AGES; METALLICITY; NGC-6822; GALAXY AB We present low-resolution Keck spectroscopy for the globular cluster (GC) H VIII in the Local Group dwarf irregular galaxy NGC 6822. We find the metallicity of the cluster to be [Fe/H]=-1.58 +/- 0.28 and the age of the cluster to be 3-4 Gyr, slightly older than but consistent with previous age estimates. H VIII seems to be more metal-poor than most intermediate-age GCs in the Local Group, and appears most similar to the anomalous Small Magellanic Cloud clusters Lindsay 113 and NGC 339. C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Strader, J (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. NR 22 TC 6 Z9 6 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 2003 VL 339 IS 3 BP 707 EP 710 DI 10.1046/j.1365-8711.2003.06212.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DN UT WOS:000181077300015 ER PT J AU Steeghs, D Perryman, MAC Reynolds, A de Bruijne, JHJ Marsh, T Dhillon, VS Peacock, A AF Steeghs, D Perryman, MAC Reynolds, A de Bruijne, JHJ Marsh, T Dhillon, VS Peacock, A TI High-speed energy-resolved STJ photometry of the eclipsing dwarf nova IYUMa SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : eclipsing; stars : dwarf novae; stars : individual : IYUMa; novae, cataclysmic variables ID IY-URSAE-MAJORIS; CATACLYSMIC VARIABLES; BINARIES; SUPERHUMPS AB We present high-time-resolution photometry of the dwarf nova IY UMa using the S-Cam2 superconducting tunnel junction device attached to the 4.2-m William Herschel Telescope on La Palma. Exploiting the well-defined white dwarf and hotspot eclipse features, we derive an updated orbital ephemeris for IY UMa and an orbital period of 0.073 908 97(5) d. A white dwarf ingress/egress duration of 31 2 s along with the contact phases of the bright-spot gives M (1) = 0.79 0.04 M-circle dot and M (2) = 0.10 0.01 M-circle dot , corresponding to a mass ratio of q = 0.125 0.008. The white dwarf eclipse width of Deltaphi(WD) = 0.0637 then implies . A curious rise with a duration of 30 2 s is present in the orbital light curves during all three observed eclipses. It occurs between the end of white dwarf ingress and hotspot ingress, and is blue in colour. We suggest that the source of this light lies in the buried part of the gas stream, resulting in a compact, hot impact cavity. C1 Univ Southampton, Dept Phys & Astron, Southampton S017 1BJ, Hants, England. European Space Technol Ctr, Astrophys Missions Div, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dsteeghs@cfa.harvard.edu RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Perryman, Michael/0000-0002-3953-4750 NR 17 TC 26 Z9 26 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2003 VL 339 IS 3 BP 810 EP 816 DI 10.1046/j.1365-8711.2003.06226.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DN UT WOS:000181077300025 ER PT J AU Cooper, K AF Cooper, K TI Voices of a Thousand people: The Makah Cultural and Research Center SO MUSEUM NEWS LA English DT Book Review C1 Smithsonian Ctr Educ & Museum Studies, Washington, DC USA. RP Cooper, K (reprint author), Smithsonian Ctr Educ & Museum Studies, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 2003 VL 82 IS 2 BP 24 EP + PG 0 WC Art SC Art GA 651YX UT WOS:000181352500022 ER PT J AU Seitel, P AF Seitel, P TI Theorizing genres, interpreting works SO NEW LITERARY HISTORY LA English DT Article ID TANZANIA; BARDS C1 Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. RP Seitel, P (reprint author), Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. NR 21 TC 12 Z9 12 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0028-6087 J9 NEW LITERARY HIST JI New Lit. Hist. PD SPR PY 2003 VL 34 IS 2 BP 275 EP 297 DI 10.1353/nlh.2003.0023 PG 23 WC Literature SC Literature GA 696WA UT WOS:000183909500007 ER PT J AU Kress, WJ Htun, T AF Kress, WJ Htun, T TI A second species of Smithatris (Zingiberaceae) from Myanmar SO NOVON LA English DT Article DE Myanmar; Smithatris; Southeast Asia; Thailand; Zingiberaceae ID GENUS AB Smithatris myanmarensis, the second species of a previously monospecific genus, is described from Myanmar. This new species differs from its congener in Thailand by the overall smaller stature, elliptic leaf lamina with long petioles, dimorphic inflorescence bracts, corolla lobes of similar size and shape, the pouch formed by the labellum and lateral staminodes below the anther, and the shallowly lobed labellum. C1 Smithsonian Inst, US Natl Herbarium, Natl Museum Nat Hist, Washington, DC 20013 USA. Nat & Wildlife Conservat Div, Forest Dept, Insein, Yangon, Myanmar. RP Kress, WJ (reprint author), Smithsonian Inst, US Natl Herbarium, Natl Museum Nat Hist, MRC-166,POB 37012, Washington, DC 20013 USA. NR 6 TC 2 Z9 2 U1 2 U2 2 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 2003 VL 13 IS 1 BP 68 EP 71 DI 10.2307/3393567 PG 4 WC Plant Sciences SC Plant Sciences GA 661LD UT WOS:000181891300011 ER PT J AU Strong, MT AF Strong, MT TI Cypringlea, a new genus of Cyperaceae from Mexico SO NOVON LA English DT Article DE Cyperaceae; Cyperoideae; Cypringlea; Mexico; Scirpeae; Scirpus; Trichophorum AB Studies of the floral morphology of the Mexican endemics Scirpus analecta Beetle and Scirpus coahuilensis Svenson, including embryo morphology and scanning electron microscopy (SEM) studies of the achenes, achene pericarp, and perianth bristles, indicate that like Scirpus L.,they are members of the tribe Scirpeae Knuth ex Dumortier. However, they were found to possess a Carex-type embryo that is characteristic of Trichophorum Persoon. Because of differences in habitat, leaf blade development and morphology, inflorescence morphology, and the possession of rudimentary perianth bristles, they are shown to be better circumscribed in a genus of their own, Cypringlea M. T Strong. Cypringlea is described, and the combinations C. analecta (Beetle) M. I Strong and C. coahuilensis (Svenson) M. I Strong are validated. Drawings of the embryos, SEM images of the achenes, achene pericarp, and perianth bristles, and photographic images of herbarium type specimens of the plants are provided, and the relationships of Cypringlea to Scirpus and Trichophorum are discussed. C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. RP Strong, MT (reprint author), Smithsonian Inst, Dept Systemat Biol, MRC-166,10th & Constitut Ave, Washington, DC 20560 USA. NR 11 TC 9 Z9 12 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SPR PY 2003 VL 13 IS 1 BP 123 EP 132 DI 10.2307/3393577 PG 10 WC Plant Sciences SC Plant Sciences GA 661LD UT WOS:000181891300021 ER PT J AU Galvez, D Pearcy, RW AF Galvez, D Pearcy, RW TI Petiole twisting in the crowns of Psychotria limonensis: implications for light interception and daily carbon gain SO OECOLOGIA LA English DT Article DE crown architecture; petiole twisting; self-shading; light capture; carbon dioxide assimilation ID CORNUS-KOUSA CORNACEAE; TRIFOLIUM-REPENS; SOLAR TRACKING; LEAF DISPLAY; WHITE CLOVER; CAPTURE; FOREST; PLANTS; ARCHITECTURE; PHYTOCHROME AB We used Y-plant, a computer-based model of crown architecture, to examine the implications of leaf reorientation resulting from petiole bending in Psychotria limonensis (Rubiaceae) seedlings. During this reorientation process, bending of the petioles of lower leaves that are potentially self-shaded by the upper leaves rotates the lamina around the stem's orthotropic axis so that self-shading is reduced. Simulations of daily light capture and assimilation revealed a 66% increase in daily C gain due to reorientation of the leaves as compared to simulations where the leaves remained in their characteristic opposite decussate pattern set by the phyllotaxy. This was due to enhanced carbon (C) gain of the lower leaves because of the reduction of shading by upper developing leaves in the same vertical plane. The light signal for this movement was experimentally examined by placing leaf-shaped filters above already fully expanded leaves and following the resulting shade-avoiding movements. The filters were either neutral density shade cloth that reduced the photon flux density (PFD) but did not alter the red to far red ratio (R:FR) or a film that reduced the PFD equivalently but also reduced the R:FR. Leaf reorientation was much more rapid and complete under the low R:FR as compared to the high R:FR indicating involvement of a phytochrome photosensory system that detected the presence of a shading leaf. Plants in gaps were found to lack a reorientation response indicating that the reorientation is specific to the shaded understory environment. C1 Univ Calif Davis, Sect Evol & Ecol, Div Biol Sci, Davis, CA 95616 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Pearcy, RW (reprint author), Univ Calif Davis, Sect Evol & Ecol, Div Biol Sci, 1 Shields Ave, Davis, CA 95616 USA. NR 42 TC 24 Z9 28 U1 0 U2 9 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAR PY 2003 VL 135 IS 1 BP 22 EP 29 DI 10.1007/s00442-002-1158-3 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 672AB UT WOS:000182497200003 PM 12647100 ER PT J AU Becerro, MA Thacker, RW Turon, X Uriz, MJ Paul, VJ AF Becerro, MA Thacker, RW Turon, X Uriz, MJ Paul, VJ TI Biogeography of sponge chemical ecology: comparisons of tropical and temperate defenses SO OECOLOGIA LA English DT Article DE anti-predatory defenses; defense effectiveness; Mediterranean vs Indo-Pacific; latitudinal gradient; predator-prey relationships ID PLANT-HERBIVORE INTERACTIONS; BROWN ALGAL PHLOROTANNINS; MARINE NATURAL-PRODUCTS; PREDATORY REEF FISH; SECONDARY METABOLITES; GEOGRAPHIC-VARIATION; INDUCIBLE DEFENSES; CARIBBEAN SPONGES; CRAMBE-CRAMBE; TOXICITY AB Examples from both marine and terrestrial systems have supported the hypothesis that predation is higher in tropical than in temperate habitats and that, as a consequence, tropical species have evolved more effective defenses to deter predators. Although this hypothesis was first proposed for marine sponges over 25 years ago, our study provides the first experimental test of latitudinal differences in the effectiveness of sponge chemical defenses. We collected 20 common sponge species belonging to 14 genera from tropical Guam and temperate Northeast Spanish coasts (Indo-Pacific and Mediterranean biogeographic areas) and conducted field-based feeding experiments with large and small fish predators in both geographic areas. We use the term global deterrence to describe the deterrent activity of a sponge extract against all of the predators used in our experiments and to test the hypothesis that sponges from Guam are chemically better defended than their Mediterranean counterparts. Sympatric and allopatric deterrence refer to the average deterrent activity of a sponge against sympatric or allopatric predators. All of the sponges investigated in this study showed deterrent properties against some predators. However, 35% of the sponge species were deterrent in at least one but not in all the experiments, supporting the idea that predators can respond to chemical defenses in a species-specific manner. Tropical and temperate sponges have comparable global, sympatric, and allopatric deterrence, suggesting not only that chemical defenses from tropical and temperate sponges are equally strong but also that they are equally effective against sympatric and allopatric predators. Rather than supporting geographic trends in the production of chemical defenses, our data suggest a recurrent selection for chemical defenses in sponges as a general life-history strategy. C1 CSIC, Ctr Adv Studies, CEAB, Blanes 17300, GI, Spain. Univ Guam, Marine Lab, Mangilao, GU 96923 USA. Univ Barcelona, Dept Anim Biol Invertebrates, Barcelona 08028, Spain. Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Becerro, MA (reprint author), CSIC, Ctr Adv Studies, CEAB, Blanes 17300, GI, Spain. EM mikel@ceab.csic.es RI Becerro, Mikel/A-5325-2008; Uriz, Maria /J-9001-2012; Turon, Xavier/J-9211-2012; OI Turon, Xavier/0000-0002-9229-5541; Becerro, Mikel/0000-0002-6047-350X; Thacker, Robert/0000-0002-9654-0073 NR 91 TC 71 Z9 76 U1 4 U2 31 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 MAR PY 2003 VL 135 IS 1 BP 91 EP 101 DI 10.1007/s00442-002-1138-7 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 672AB UT WOS:000182497200011 PM 12647108 ER PT J AU Lovelock, CE Feller, IC AF Lovelock, CE Feller, IC TI Photosynthetic performance and resource utilization of two mangrove species coexisting in a hypersaline scrub forest SO OECOLOGIA LA English DT Article DE photosynthetic nitrogen use efficiency; photosynthetic water use efficiency; Avicennia germinans; Laguncularia racemosa; Florida ID NITROGEN-USE EFFICIENCY; WATER-USE EFFICIENCY; SPARTINA-ALTERNIFLORA; SALINITY; GROWTH; SOIL; SEEDLINGS; PLANT; FERTILIZATION; AVAILABILITY AB In a hypersaline mangrove scrub forest in northern Florida, coexisting trees of Laguncularia racemosa and Avicennia germinans were either fertilized with nitrogen or phosphorus, or not fertilized (controls). We aimed to test whether nutrient additions differentially altered photosynthetic performance and resource utilization in these two species. In control trees, photosynthetic rates were higher in L. racemosa than A. germinans. However, leaf nitrogen concentrations were higher in A. germinans than L. racemosa. Avicennia germinans responded to fertilization with nitrogen by increasing leaf nitrogen concentrations and rates of photosynthesis such that they were equivalent to photosynthesis in L. racemosa. Laguncularia racemosa did not show a response to nitrogen additions. Neither species showed strong responses to phosphorus fertilization. Avicennia germinans had high photosynthetic water-use efficiency (photosynthesis/transpiration), but low photosynthetic nitrogen-use efficiency (photosynthesis/leaf nitrogen). In contrast, L. racemosa had comparatively low photosynthetic water use efficiency and high photosynthetic nitrogen use efficiency. Leaf level characteristics lead us to hypothesize that coexistence of A. germinans and L. racemosa should occur where nitrogen levels are low and salinity is moderate, or at least moderate for some period of the year. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. 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; Feller, Ilka/0000-0002-6391-1608 NR 40 TC 60 Z9 69 U1 3 U2 26 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAR PY 2003 VL 134 IS 4 BP 455 EP 462 DI 10.1007/s00442-002-1118-y PG 8 WC Ecology SC Environmental Sciences & Ecology GA 655ZD UT WOS:000181582700001 PM 12647116 ER PT J AU Harrison, RD Yamamura, N AF Harrison, RD Yamamura, N TI A few more hypotheses for the evolution of dioecy in figs (Ficus, Moraceae) SO OIKOS LA English DT Article ID WASP MUTUALISM; SEX-RATIOS; WORLD FIGS; PHENOLOGY; SEED; POLLINATORS; POPULATIONS; COMMUNITY; DYNAMICS; ECOLOGY AB In figs (Ficus, Moraceae) there are two breeding systems: monoecy is the ancestral condition but approximately half the 750 odd species are functionally dioecious. Three hypotheses have been proposed for the evolution of dioecy in figs, invoking seasonality (Kjellberg et al. 1987), the reduction of non-pollinating wasp species (Kerdelhue and Rasplus 1996), and the persistence of pollinator populations within small groups of trees (Kameyama et al. 1999). However, there are two major problems with these ideas. Firstly, dioecy has probably evolved only twice (Weiblen 2000), which severely limits our ability to test between alternative hypotheses. Secondly, it is very simple to suggest ways in which dioecy can evolve from monoecy (Charnov 1982). To illustrate this problem, and enlarge on some recent progress in our understanding of functionally dioecious figs, we are proposing a few more hypotheses. C1 Kyoto Univ, Ctr Ecol Res, Otsu, Shiga 5202113, Japan. RP Harrison, RD (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 46 TC 39 Z9 44 U1 0 U2 10 PU BLACKWELL MUNKSGAARD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0030-1299 J9 OIKOS JI Oikos PD MAR PY 2003 VL 100 IS 3 BP 628 EP 635 DI 10.1034/j.1600-0706.2003.11829.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 662TD UT WOS:000181963700026 ER PT J AU Behrensmeyer, AK Stayton, CT Chapman, RE AF Behrensmeyer, AK Stayton, CT Chapman, RE TI Taphonomy and ecology of modern avifaunal remains from Amboseli Park, Kenya (vol 29, pg 52, 2002) SO PALEOBIOLOGY LA English DT Correction C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Univ Chicago, Dept Geol & Geophys, Chicago, IL 60637 USA. Idaho State Univ, ITRC, Pocatello, ID 83209 USA. RP Behrensmeyer, AK (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 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 2003 VL 29 IS 2 BP II EP II PG 1 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 682BM UT WOS:000183070500001 ER PT J AU Nelson, R Parker, G Hom, M AF Nelson, R Parker, G Hom, M TI A portable airborne laser system for forest inventory SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID STAND CHARACTERISTICS; CANOPY STRUCTURE; SCANNER DATA; BASAL AREA; LIDAR; VOLUME; BIOMASS; ALTIMETER; HEIGHT AB A simple, lightweight, inexpensive, portable airborne laser profiling system has been assembled from off-the-shelf, commercially available components. The system, which costs approximately $30,000, is designed to fly aboard small helicopters and single- or twin-engine high-wing aircraft without airframe modification, The system acquires first-return range and amplitude measurements at data rates up to 2000 hz (operator-con trolled) and has an operational envelope up to 300 m above terrain. The airborne laser profiling system includes the laser transmitter/receiver, differential GPS receiver, a CCD video camera and recorder, and a laptop computer which interleaves and records the GPS and laser range/amplitude data. The portable airborne laser system (PALS) was designed to acquire forest height measurements along linear flight transects in order to conduct regional or subcontinental forest inventories worldwide. This economical laser system now puts airborne laser mensuration within reach of operational foresters and researchers interested in making rapid forest structure and/or timber surveys in remote areas. PALS has been used to acquire over 5000 km of flight transect data over the state of Delaware. C1 NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Nelson, R (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Sci Syst & Applicat Inc, Code 923, Greenbelt, MD 20771 USA. EM ross@ltpmail.gsfc.nasa.gov; parker@serc.si.edu; mhom@pop900.gsfc.nasa.gov RI Nelson, Ross/H-8266-2014; OI Parker, Geoffrey/0000-0001-7055-6491 NR 28 TC 51 Z9 51 U1 1 U2 3 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD MAR PY 2003 VL 69 IS 3 BP 267 EP 273 PG 7 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 817QU UT WOS:000221192800004 ER PT J AU Yu, DH Williams, JF Chen, XJ Hayes, PA Bartschat, K Zeman, V AF Yu, DH Williams, JF Chen, XJ Hayes, PA Bartschat, K Zeman, V TI Cascade effects in the excitation of np(5)(n+1)p states of krypton and xenon atoms by polarized electrons SO PHYSICAL REVIEW A LA English DT Article ID GASES; NEON AB The integrated Stokes parameters of the decay photons from the excited np(5)(n+1)p[5/2](3), np(5)(n+1)p(')[3/2](2), and np(5)(n+1)p(')[3/2](1) (n=5 and 6) states of Kr and Xe, respectively, are measured from near threshold to 100 eV using incident polarized electrons. The effects of the cascade photons on the Stokes parameters have been investigated using a pulsed beam of polarized electrons. The cascade effects for the final excited states are more significant for the linear polarization P-1 parameter than for the circular polarization P-3 parameter and they do not always have depolarization effects. The integrated state multipoles, determined from the integrated Stokes parameters corrected for cascade effects, are closer to, but not in agreement with, the values from semirelativistic R matrix and relativistic distorted-wave approximation methods. C1 Univ Western Australia, Ctr Atom Mol & Surface Phys, Dept Phys, Perth, WA 6009, Australia. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Toronto, Dept Chem, Toronto, ON M5S 3H6, Canada. Univ Sci & Technol, Dept Modern Phys, Hefei, Peoples R China. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Yu, DH (reprint author), Univ Western Australia, Ctr Atom Mol & Surface Phys, Dept Phys, Perth, WA 6009, Australia. RI Bartschat, Klaus/I-2527-2012 NR 11 TC 0 Z9 0 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 2003 VL 67 IS 3 AR 032707 DI 10.1103/PhysRevA.67.032707 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 662TX UT WOS:000181965900050 ER PT J AU Stoner, R Walsworth, R AF Stoner, R Walsworth, R TI Balancing atoms probe fundamental symmetries SO PHYSICS WORLD LA English DT News Item C1 Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stoner, R (reprint author), Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-8585 J9 PHYS WORLD JI Phys. World PD MAR PY 2003 VL 16 IS 3 BP 24 EP 25 PG 2 WC Physics, Multidisciplinary SC Physics GA 665LQ UT WOS:000182122600034 ER PT J AU Field, CR AF Field, CR TI The Lincoln Memorial and American life SO PUBLIC HISTORIAN LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Field, CR (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA C/O JOURNALS DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD SPR PY 2003 VL 25 IS 2 BP 139 EP 141 PG 3 WC History SC History GA 703NN UT WOS:000184286500016 ER PT J AU Touwaide, A AF Touwaide, A TI Between imitation and plagiarism: Origins and influences in the 'Dioscorides' of Andres Laguna SO RENAISSANCE QUARTERLY LA English DT Book Review C1 Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU RENAISSANCE SOC AMER INC PI NEW YORK PA 24 WEST 12TH STREET, NEW YORK, NY 10011 USA SN 0034-4338 J9 RENAISSANCE QUART JI Renaiss. Q. PD SPR PY 2003 VL 56 IS 1 BP 197 EP 201 DI 10.2307/1262284 PG 5 WC Medieval & Renaissance Studies SC Arts & Humanities - Other Topics GA 652XW UT WOS:000181407000039 ER PT J AU Touwaide, A AF Touwaide, A TI Andres Laguna and humanist medicine: Philological studies SO RENAISSANCE QUARTERLY LA English DT Book Review C1 Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU RENAISSANCE SOC AMER INC PI NEW YORK PA 24 WEST 12TH STREET, NEW YORK, NY 10011 USA SN 0034-4338 J9 RENAISSANCE QUART JI Renaiss. Q. PD SPR PY 2003 VL 56 IS 1 BP 197 EP 201 DI 10.2307/1262284 PG 5 WC Medieval & Renaissance Studies SC Arts & Humanities - Other Topics GA 652XW UT WOS:000181407000038 ER PT J AU Touwaide, A AF Touwaide, A TI Medical humanists in Renaissance Valladolid SO RENAISSANCE QUARTERLY LA English DT Book Review C1 Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU RENAISSANCE SOC AMER INC PI NEW YORK PA 24 WEST 12TH STREET, NEW YORK, NY 10011 USA SN 0034-4338 J9 RENAISSANCE QUART JI Renaiss. Q. PD SPR PY 2003 VL 56 IS 1 BP 201 EP 205 DI 10.2307/1262285 PG 5 WC Medieval & Renaissance Studies SC Arts & Humanities - Other Topics GA 652XW UT WOS:000181407000041 ER PT J AU Touwaide, A AF Touwaide, A TI Sixteenth-century medical humanism at the University of Salamanca SO RENAISSANCE QUARTERLY LA English DT Book Review C1 Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU RENAISSANCE SOC AMER INC PI NEW YORK PA 24 WEST 12TH STREET, NEW YORK, NY 10011 USA SN 0034-4338 J9 RENAISSANCE QUART JI Renaiss. Q. PD SPR PY 2003 VL 56 IS 1 BP 201 EP 205 DI 10.2307/1262285 PG 5 WC Medieval & Renaissance Studies SC Arts & Humanities - Other Topics GA 652XW UT WOS:000181407000040 ER PT J AU Smith, DR AF Smith, DR TI A synopsis of the sawflies (Hymenoptera : Symphyta) of America south of the United States: Tenthredinidae (Nematinae, Heterarthrinae, Tenthredininae) SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article ID OLIGOSPILUS FORSTER HYMENOPTERA; NEMATUS; ARGENTINA AB The subfamilies Nematinae, Heterarthrinae, and Tenthredininae of the Tenthredinidae are reviewed for the Western Hemisphere south of the United States. A key is given for the seven subfamilies of Tenthredinidae for this region. Nematinae include six genera and 17 species, with the following new species: Pristiphora auricauda (Costa Rica), P. fernandezi (Colombia), P. fuscalae (Costa Rica), P. hansoni (Costa Rica), P. helveola (Mexico), and P. semialba (Venezuela). Heterarthrinae include three genera and eight species, with one new species, Brasinusa malaisei (Brazil). Tenthredininae include three genera and four species. All Tenthredininae and many of the Nematinae are southern extensions of northern groups into northern Mexico, and two species, Nematus oligospilus (Foerster) (Nematinae) and Caliroa cerasi (L.) (Heterarthrinae), are introductions into southern South America. All nine species of Pristiphora (Nematinae) and the genera Brasinusa and Notofenusa (Heterarthrinae) are endemic to the Neotropics. C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA. NR 98 TC 14 Z9 17 U1 0 U2 1 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD MAR PY 2003 VL 129 IS 1 BP 1 EP 45 PG 45 WC Entomology SC Entomology GA 667ZN UT WOS:000182265300001 ER PT J AU Stappers, BW Gaensler, BM Kaspi, VM van der Klis, M Lewin, WHG AF Stappers, BW Gaensler, BM Kaspi, VM van der Klis, M Lewin, WHG TI An x-ray nebula associated with the millisecond pulsar B1957+20 SO SCIENCE LA English DT Article ID CRAB-NEBULA; PARTICLE-ACCELERATION; SYNCHROTRON NEBULA; RADIO PULSARS; HIGH-ENERGY; BINARY; PSR1957+20; DISCOVERY; EMISSION; HST AB We have detected an x-ray nebula around the binary millisecond pulsar B1957+20. A narrow tail, corresponding to the shocked pulsar wind, is seen interior to the known Halpha bow shock and proves the long-held assumption that the rotational energy of millisecond pulsars is dissipated through relativistic winds. Unresolved x-ray emission likely represents the shock where the winds of the pulsar and its companion collide. This emission indicates that the efficiency with which relativistic particles are accelerated in the postshock flow is similar to that for young pulsars, despite the shock proximity and much weaker surface magnetic field of this millisecond pulsar. C1 Stichting ASTRON, NL-7990 Dwingeloo, Netherlands. Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 278, Canada. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Space Res Ctr, Cambridge, MA 02139 USA. RP Stappers, BW (reprint author), Stichting ASTRON, NL-7990 Dwingeloo, Netherlands. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 28 TC 93 Z9 93 U1 0 U2 0 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 28 PY 2003 VL 299 IS 5611 BP 1372 EP 1374 DI 10.1126/science.1079841 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 649DU UT WOS:000181192300045 PM 12610299 ER PT J AU Clark, KL Ruiz, GM Hines, AH AF Clark, KL Ruiz, GM Hines, AH TI Diel variation in predator abundance, predation risk and prey distribution in shallow-water estuarine habitats SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Chesapeake Bay; diel effects; Palaemonetes pugio; predation risk; prey response ID SUBMERGED AQUATIC VEGETATION; CALLINECTES-SAPIDUS RATHBUN; PERCH MORONE-AMERICANA; TIDAL SALT-MARSH; GULF-OF-MEXICO; CHESAPEAKE-BAY; BLUE CRABS; PALAEMONETES-PUGIO; FEEDING-HABITS; GRASS SHRIMP AB Predation by visual predators is often affected by light conditions and may therefore exhibit strong diel variation. The dominant predators on grass shrimp, Palaemonetes pugio, are finfish predators that are thought to locate their prey by visual cues. We examined the response of grass shrimp to diel variation in predation risk in the nearshore shallow waters of the Chesapeake Bay. We used diel shoreline seines to assess the relative abundance of predators, We assessed the relative risk of predation with shrimp tethered at refuge (30 cm) and nourefuge (60 cm) depths. To measure grass shrimp response to predation risk, we used dipnets to monitor habitat use. Four predominantly visual predators dominated the shoreline seine catches, Fundulus heteroclitus, Micropogonias undulatus, Morone americana and Morone saxatilis. Total predator abundance had a diel component, with dramatic nighttime decreases in total abundance, whereas guild composition and relative abundance remained unchanged. Relative predation risk for tethered shrimp exhibited significant time by habitat interaction. During the day, depth negatively affected survivorship of tethered shrimp while at night overall survivorship increased and there was no effect of depth. Shrimp habitats use reflected diel predation risks. Abundances in the near shore were highest during the day with decreased abundances at night. Together, the seine and tethering data highlight the importance for a refuge (e.g., shallow water) from predation during the daytime and a relaxation of predation pressure at night. Published by Elsevier Science B.V. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Clark, KL (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. OI Ruiz, Gregory/0000-0003-2499-441X NR 63 TC 58 Z9 60 U1 3 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD FEB 26 PY 2003 VL 287 IS 1 BP 37 EP 55 AR PII S0022-0981(02)00439-2 DI 10.1016/S0022-0981(02)00439-2 PG 19 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 646GG UT WOS:000181026800003 ER PT J AU Rufus, J Stark, G Smith, PL Pickering, JC Thorne, AP AF Rufus, J Stark, G Smith, PL Pickering, JC Thorne, AP TI High-resolution photoabsorption cross section measurements of SO2, 2: 220 to 325 nm at 295 K SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE ultraviolet absorption spectra; planetary atmospheres; photoabsorption cross sections ID FOURIER-TRANSFORM SPECTROMETER; HUBBLE-SPACE-TELESCOPE; SULFUR-DIOXIDE; ABSORPTION-SPECTRUM; UV; ULTRAVIOLET; SPECTROSCOPY; ATMOSPHERE; IO; REGION AB [1] High-resolution, ultraviolet SO2 photoabsorption cross section data are required for modeling density and temperature profiles of SO2 in solar system atmospheres. We report measurements of such cross sections on SO2 at 295 K for the (B) over tilde B-1(1) - (X) over tilde (1)A(1) and (C) over tilde B-1(2)-(X) over tilde (1)A(1) bands over the wavelength range 220 to 325 nm. Resolving powers of up to 550,000 were employed in order to study the congested spectrum of sharp SO2 features in parts of this region. Our data are compared to earlier values obtained with lower resolving power. C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Wellesley Coll, Dept Phys, Wellesley, MA USA. RP Rufus, J (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Huxley Bldg, London SW7 2BZ, England. NR 35 TC 40 Z9 40 U1 3 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 25 PY 2003 VL 108 IS E2 AR 5011 DI 10.1029/2002JE001931 PG 5 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 664RV UT WOS:000182075500003 ER PT J AU Shibatsuka, T Matsushita, S Kohno, K Kawabe, R AF Shibatsuka, T Matsushita, S Kohno, K Kawabe, R TI Multi-line observations of molecular gas in the central region of the low star-formation efficiency "starburst" galaxy NGC 4527 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies : individual (NGC 4527); galaxies : ISM; galaxies : starburst; ISM : molecules ID NEARBY SPIRAL GALAXIES; DENSE GAS; GALACTIC-CENTER; 1.49 GHZ; IC 342; CO; KINEMATICS; EMISSION; NGC-253; M82 AB We performed high-resolution CO (J = 2-1), CO (J = 1-0), HCN (J = 1-0), HCO+ (J = 1-0), and 3 mm continuum observations of the low star formation efficiency (SFE) "starburst" galaxy NGC 4527 with the Nobeyama Millimeter Array. From CO (J = 1-0) observations, we found two offset ridges with non-circular motion and a central gas concentration. The distribution and kinematics of NGC 4527 are very similar to those of barred spiral galaxies. The distribution of CO (J = 2-1) emission resembles the features of the concentrated component of CO (J = 1-0). HCN (J = 1-0) and HCO+ (J = 1-0) emissions concentrated toward the center have also been detected. The total mass of molecular gas detected in the central r < 30" is 2.5 x 10(9) MD. The HCN (J = 1-0)/CO (J = 1-0) integrated intensity ratio of 0.075 +/- 0.008 in the central r; 3"-4" region of NGC 4527 could suggest that the fraction of dense molecular gas to the total molecular gas is small compared with those of prototypical starburst galaxies, such as NGC 253. This suggests that the small dense gas fraction is responsible for the low SFE in the center of NGC 4527, though this interpretation could depend on aperture sizes of the observations. The ratio of the dynamical mass to molecular gas mass is 13% within the central region (r < 500 pc). This suggests that molecular gas within the r < 500 pc region could be in a state of gravitational instability. The low SFE, the small dense gas fraction, and the large amount of gravitationally unstable molecular gas can be explained if NGC 4527 is in the very early phase of starburst phenomena or a pre-starburst phase, and the formation of dense molecular gas will begin and the SFE will increase within a short time scale. C1 Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. RP Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. EM shiba@nro.nao.ac.jp NR 67 TC 7 Z9 7 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB 25 PY 2003 VL 55 IS 1 BP 87 EP 101 DI 10.1093/pasj/55.1.87 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 653MZ UT WOS:000181441500007 ER PT J AU Kohno, K Vila-Vilaro, B Sakamoto, S Kawabe, R Ishizuki, S Matsushita, S AF Kohno, K Vila-Vilaro, B Sakamoto, S Kawabe, R Ishizuki, S Matsushita, S TI Aperture synthesis CO (J=1-0) observations and near-infrared photometry of the non-barred Seyfert galaxy NGC 5033 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Review DE galaxies : active; galaxies : individual (NGC 5033); galaxies : ISM; galaxies : Seyfert; galaxies : structure ID ACTIVE GALACTIC NUCLEI; MOLECULAR INTERSTELLAR-MEDIUM; NOBEYAMA 45-M TELESCOPE; SUPERMASSIVE BLACK-HOLE; ON SPIRAL GALAXIES; STAR-FORMATION; CENTRAL REGIONS; MICRON SPECTROSCOPY; PHYSICAL CONDITIONS; DISK GALAXIES AB Aperture synthesis observations of CO (J = 1-0) emission and near-infrared broad-band photometry of the non-barred Seyfert galaxy NGC 5033 (D = 18.7 Mpc) were performed. Our 3."9 x 3."6 resolution CO observations reveal a perturbed distribution and the kinematics of molecular gas in the center of NGC 5033; we find the characteristic gaseous features that are widely observed in barred spiral galaxies, such as two bright CO peaks near the center (separated by similar to3" or 270 pc from the nucleus), two offset ridges of CO emission emanating from the CO peaks, and a CO ring (with a radius of similar to14" or 1.3 kpc). Double-peaked velocity profiles are also evident near the two CO peaks, implying that these CO peaks,are orbit crowding zones in a barred/oval potential. Although NIR data only give an upper limit of the possible bar lengths due to a large inclination of the NGC 5033 disk (i = 68degrees), our CO data clearly suggests the presence of a small (the semi-major axis of about 12"-15" or 1.1-1.4 kpc) nuclear bar (or oval structure) in the center of the "non-barred" galaxy NGC 5033. Our results demonstrate that high-resolution CO imaging-spectroscopy is useful to search for nuclear bars, even in highly inclined systems where isophoto fitting techniques are not applicable. We find that the gas mass-to-dynamical mass ratio, M-gas/M-dyn, is small (less than or equal to 1%) within a radius of 2" or 180 pc, in contrast to starburst nuclei. This implies that the starburst does not cohabitate in the type-1.5 Seyfert nucleus of NGC 5033. C1 Univ Tokyo, Astron Inst, Mitaka, Tokyo 1810015, Japan. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Tokyo, Astron Inst, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan. EM kkohno@ioa.s.u-tokyo.ac.jp; bvila@as.arizona.edu; seiichi@nro.nao.ac.jp; kawabe@nro.nao.ac.jp; ishizksm@cc.nao.ac.jp; smatsushita@cfa.harvard.edu NR 114 TC 4 Z9 4 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB 25 PY 2003 VL 55 IS 1 BP 103 EP 119 DI 10.1093/pasj/55.1.103 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 653MZ UT WOS:000181441500008 ER PT J AU Matsushita, S Matsuo, H AF Matsushita, S Matsuo, H TI FTS measurements of submillimeter-wave atmospheric opacity at Pampa la Bola: III. Water vapor, liquid water, and 183 GHz water vapor line opacities SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE atmospheric effects; instrumentation : spectrometer; site testing; submillimeter ID COMPLEX PERMITTIVITY; PHASE CORRECTION; NORTHERN CHILE; MAUNA-KEA; 1 THZ; MODEL; SITE; TRANSMISSION; MONITORS; ICE AB Further analysis has been made on the millimeter- and submillimeter-wave (100-1600 GHz or 3mm-188 mum) atmospheric opacity data taken with the Fourier Transform Spectrometer (FTS) at Pampa la Bola, 4800 m above the sea level in northern Chile, which is the site of the Atacama Large Millimeter/submillimeter Array (ALMA). Time-sequence plots of millimeter- and submillimeter-wave opacities show similar variations to each other, except for during the periods with liquid water (fog or clouds) in the atmosphere. Using millimeter- and submillimeter-wave opacity correlations under two conditions, which are affected and not affected by liquid water, we succeeded to separate the measured opacity into water vapor and liquid water opacity components. The water vapor opacity shows a good correlation with the 183 GHz water vapor line opacity, which is also covered in the measured spectra. On the other hand, the liquid water opacity and the 183 GHz line opacity show no correlation. Since only the water vapor component is expected to affect the phase of interferometers significantly, and the submillimeter-wave opacity is less affected by the liquid water component, it may be possible to use the submillimeter-wave opacity for a phase correction of submillimeter interferometers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ, Ctr Adv Technol, Mitaka, Tokyo 1818588, Japan. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA. EM smatsushita@cfa.harvard.edu; h.matsuo@nao.ac.jp RI Matsuo, Hiroshi/F-4807-2013 OI Matsuo, Hiroshi/0000-0003-3278-2484 NR 47 TC 11 Z9 11 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB 25 PY 2003 VL 55 IS 1 BP 325 EP 333 DI 10.1093/pasj/55.1.325 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 653MZ UT WOS:000181441500028 ER EF