FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Skinner, CJ Smith, HA Sturm, E Barlow, MJ Cohen, RJ Stacey, GJ AF Skinner, CJ Smith, HA Sturm, E Barlow, MJ Cohen, RJ Stacey, GJ TI A starburst origin of the OH-megamaser emission from the galaxy Arp220 SO NATURE LA English DT Article ID IC-4553 ARP-220 AB Ultraluminous infrared galaxies have been known for more than a decade, but the source of their very large far-infrared luminosities remains controversial. It may reflect a quasar-like active nucleus surrounded by a torus of dense gas and dust, the latter absorbing the energetic photons from the nuclear region and re-emitting at infrared wavelengths', or a huge burst of massive-star formation in dense dusty clouds of molecular gas close to the nucleus(2), which heats the surrounding dust. A number of ultraluminous galaxies are also a source of OH-megamaser emissions (intense laser-like spectral lines at microwave frequencies), an observation that may hold important clues as to the main power source in these galaxies. A general feature of many models(3,4) is that the masers are pumped radiatively by the absorption of infrared photons. Identifying the source of the maser pump may therefore indicate whether the ultimate energy source is a burst of star formation, or an active nucleus. Here we report the detection of a strong midinfrared OH absorption line in the prototypical megamaser and ultraluminous galaxy(5), Arp220. We find that the power absorbed in this line alone is sufficient to pump the megamaser emission seen at radio wavelengths. Moreover, the warm, extended nature of the pumping region is suggestive of a starburst origin for the ultraluminous infrared emissions. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. UNIV LONDON UNIV COLL,DEPT PHYS & ASTRON,LONDON WC1E 6BT,ENGLAND. UNIV MANCHESTER,NUFFIELD RADIO ASTRON LABS,MACCLESFIELD SK9 8DL,CHESHIRE,ENGLAND. CORNELL UNIV,DEPT ASTRON,ITHACA,NY 14853. RP Skinner, CJ (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. RI Barlow, Michael/A-5638-2009 OI Barlow, Michael/0000-0002-3875-1171 NR 16 TC 51 Z9 52 U1 0 U2 1 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD APR 3 PY 1997 VL 386 IS 6624 BP 472 EP 474 DI 10.1038/386472a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WR256 UT WOS:A1997WR25600044 ER PT J AU Jakab, PL AF Jakab, PL TI Otto Lilienthal: ''The greatest of the precursors'' SO AIAA JOURNAL LA English DT Review AB This brief treatment of Otto Lilienthal's overall aeronautical contribution details his aerodynamic research, the data as well as his data-gathering technique. Lilienthal's subsequent glider experiments also are covered from the perspective of both their technical and inspirational contributions. The heart of the paper is a discussion of the place of Lilienthal's aerodynamics in the work of others, primarily the Wright brothers, Included is a reassessment of the accuracy of Lilienthal's famous table of lift coefficients and the assumptions that the Wrights made in using Lilienthal's data. Historically, Lilienthal's data and their use by the Wrights has been one of the more complex and debated aspects of the Wright story. The article presents a brief review of how Lilienthal's contribution has been characterized and revised over time, with a discussion of the current thinking regarding the famous Lilienthal table of lift coefficients. RP Jakab, PL (reprint author), SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, DEPT AERONAUT, ROOM 3322-MRC 312, WASHINGTON, DC 20560 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD APR PY 1997 VL 35 IS 4 BP 601 EP 607 PG 7 WC Engineering, Aerospace SC Engineering GA WQ209 UT WOS:A1997WQ20900001 ER PT J AU Lellinger, DB AF Lellinger, DB TI Pteris deflexa and its allies SO AMERICAN FERN JOURNAL LA English DT Article AB The taxonomic status of Pteris deflexa and P. polita and the nomenclatural status of three other names used in this species group are clarified. RP Lellinger, DB (reprint author), SMITHSONIAN INST,DEPT BOT,MRC 166,WASHINGTON,DC 20560, USA. NR 6 TC 1 Z9 2 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD APR-JUN PY 1997 VL 87 IS 2 BP 66 EP 70 DI 10.2307/1547537 PG 5 WC Plant Sciences SC Plant Sciences GA XN726 UT WOS:A1997XN72600005 ER PT J AU Snyder, LM Klippel, WE AF Snyder, LM Klippel, WE TI Dog burials in the Greek world: The animals from an early iron age tomb at Kavousi SO AMERICAN JOURNAL OF ARCHAEOLOGY LA English DT Meeting Abstract C1 UNIV TENNESSEE,KNOXVILLE,TN 37996. SMITHSONIAN INST,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 1 U2 7 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 SN 0002-9114 J9 AM J ARCHAEOL JI Am. J. Archaeol. PD APR PY 1997 VL 101 IS 2 BP 368 EP 368 PG 1 WC Archaeology SC Archaeology GA WY808 UT WOS:A1997WY80800124 ER PT J AU Katsonopoulou, D Soter, S AF Katsonopoulou, D Soter, S TI Ancient Helike in the light of recent discoveries SO AMERICAN JOURNAL OF ARCHAEOLOGY LA English DT Meeting Abstract C1 SMITHSONIAN INST,WASHINGTON,DC 20560. NR 0 TC 2 Z9 2 U1 0 U2 1 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 SN 0002-9114 J9 AM J ARCHAEOL JI Am. J. Archaeol. PD APR PY 1997 VL 101 IS 2 BP 378 EP 378 PG 1 WC Archaeology SC Archaeology GA WY808 UT WOS:A1997WY80800163 ER PT J AU Grand, TI AF Grand, TI TI How muscle mass is part of the fabric of behavioral ecology in East African bovids (Madoqua, Gazella, Damaliscus, Hippotragus) SO ANATOMY AND EMBRYOLOGY LA English DT Article DE bovids; tissue composition; musculoskeletal anatomy; locomotor evolution; behavioral ecology; scale effects ID TISSUE COMPOSITION; MOTOR FUNCTION; BODY-WEIGHT; MAMMALS; PATTERNS; EXPLANATION; HERBIVORES; LOCOMOTION; ALLOMETRY; SYSTEM AB Tissue composition and the distribution of body mass are described for four genera of East African Bovidae (Madoqua, Gazella, Damaliscus, Hippotragus) with supporting data from four others (Neotragus, Oryx, Tragelaphus, Connochaetes). These species are high in muscle mass, an adaptation convergent with other highspeed terrestrial cursors, bounders, and saltators. The segments below the elbow/cubitus and knee/stifle/genu joints in small bovids are both lighter in percent of total body mass (8.6% TBM) and less heavily muscled (10-15% of total limb musculature) than those segments in macaques (13.6% TBM, 20-25% of the limb musculature). Bovid species differ from one another in the regional distribution of muscle mass. Madoqua kirkii (4-5 kg) concentrates muscle in the lumbar extensors and hindlimbs; large species such as Damaliscus dorcas (50-60 kg) and Hippotragus niger (160-200 kg) distribute it more evenly between the lumbar and cervical regions and between the hindlimbs and forelimbs. Gazella dorcas (10-20 kg) is quantitatively intermediate in those characteristics. The redistribution of muscle mass with increasing size correlates with the loss of axial bending of the vertebral column: in small, hindlimb dominant, 'dorsomobile' species such as Madoqua sagittal mobility increases stride length through 'extended' suspension; in large 'dorsostable' species such as Damaliscus and Hippotragus the vertebral column resists bending, consequently abbreviating or omitting this non-contact phase of the gait cycle. Locomotor adaptation as it is reflected in size, shape, and musculoskeletal structure is the key to habitat choice, dietary specialization, social structure, and male agonistic behavior and, therefore, central to the fabric of behavioral ecology. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RP Grand, TI (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT PATHOL,WASHINGTON,DC 20008, USA. NR 55 TC 14 Z9 14 U1 1 U2 7 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-2061 J9 ANAT EMBRYOL JI Anat. Embryol. PD APR PY 1997 VL 195 IS 4 BP 375 EP 386 DI 10.1007/s004290050058 PG 12 WC Anatomy & Morphology; Developmental Biology SC Anatomy & Morphology; Developmental Biology GA WR882 UT WOS:A1997WR88200009 PM 9108204 ER PT J AU Alves, J Hartmann, L Briceno, C Lada, CJ AF Alves, J Hartmann, L Briceno, C Lada, CJ TI Optical outburst of a pre-main-sequence object SO ASTRONOMICAL JOURNAL LA English DT Article ID T-TAURI STARS; BETA-PICTORIS PHENOMENON; EARLY STELLAR EVOLUTION; FU ORIONIS; MODERATE-RESOLUTION; YOUNG STARS; UX-ORIONIS; MASS-LOSS; PHOTOMETRY; ROTATION AB We present a study of CB34V, a pre-main-sequence object that has increased in brightness by similar to 3.7 mag in the red between 1951 November (1951.9) and 1996 February (1996.1). Our data consist of intermediate and high-resolution optical spectroscopy as well as optical and near-infrared photometry (BVRIJHK). We find that the color behavior of the CB34V brightness variation is peculiar, corresponding to a gray brightening. We demonstrate that CB34V is a pre-main-sequence object embedded in a small molecular cloud by 2.4 visual magnitudes. At optical wavelengths CB34V has a G5 (III-IV) spectral type and is rapidly rotating with a v sin i similar to 145+/-20 km s(-1). We estimate a current bolometric luminosity of 7 1, 3 --> 2, 6 --> 5, (CO)-C-13 2 --> 1, and (CO)-O-18 2 --> 1 transitions at the Caltech Submillimeter Observatory (CSO). The broad bipolar structure is optically thick in the (CO)-C-12 line. The (CO)-C-13 measurements imply a large outflow mass of 4800 M. (12% of the total cloud mass). Interferometric observations with the Owens Valley Radio Observatory (OVRO) millimeter array in the (CO)-C-13 1 --> 0 line resolve the gas into at least two outflows, one of which emanates from the 4.0 Jy, 110 GHz source identified with the UC H II region. An additional outflow is driven by an adjacent young, embedded object that contributes to the extended submillimeter continuum emission imaged with the CSO bolometer array camera. Lying in a separate core a few arcminutes away, the G45.07+0.13 UC H II region contains H2O masers and presents higher velocity (11 km s(-1)) yet more compact CO emission. An outflow has been detected in the CO 6 --> 5 transition, along with a compact submillimeter continuum source. OVRO observations in the CS J = 2 --> 1 transition confirm a compact outflow centered on the 98 GHz continuum source toward which infall is also seen in the form of redshifted absorption. The multiple outflows, higher CO antenna temperatures, more extended submillimeter and radio continuum emission, and lack of H2O masers all distinguish the core containing G45.12+0.13 as a more advanced site of massive star formation than the neighboring core containing G45.07+0.13. C1 CALTECH,PASADENA,CA 91125. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 55 TC 42 Z9 42 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 1997 VL 478 IS 1 BP 283 EP 294 DI 10.1086/303775 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WN497 UT WOS:A1997WN49700029 ER PT J AU Chen, H Grenfell, TG Myers, PC Hughes, JD AF Chen, H Grenfell, TG Myers, PC Hughes, JD TI Comparison of star formation in five nearby molecular clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, clouds; stars, formation; stars, fundamental parameters; stars, luminosity function, mass function; stars, pre-main-sequence ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MAIN-SEQUENCE STARS; DARK CLOUDS; DENSE CORES; IRAS OBSERVATIONS; CO OBSERVATIONS; T-ASSOCIATION; CHAMELEON-II; TAURUS AB We have calculated bolometric temperature (T-bol) and bolometric luminosity (L(bol)) for 383 young stellar objects (YSOs) in five molecular clouds within 200 pc in Corona Australis (CrA), Ophiuchus (Oph), Taurus (Tau), Chamaeleon (Cha), and Lupus (Lup). We used T-bol, L(bol), and bolometric luminosity-temperature (BLT) diagrams to characterize and compare the overall-star-formation activity of the clouds on a self-consistent basis. The main results are the following: (1) the YSO populations in the clouds can be differentiated by the fraction of their low-T-bol Sources, which increases systematically from Lup and Cha to Tau and to Oph and CrA. This trend is interpreted as increasing current star-forming activity in the same order; (2) the clouds with higher cold source fractions also seem to have higher bright source fractions; (3) In the BLT diagram, the CrA and Oph sources are more uniformly distributed while the Cha and Lup sources are aggregated near the zero-age mainsequence (ZAMS). Tau sources appear to be an intermediate case. Taurus also seems to contain more cold (T-bol < 1000 K) and low-luminosity (L(bol) < 1 L.) sources than the other complexes; (4) the YSOs show a characteristic distribution in the median BLT diagram. This distribution is qualitatively consistent with the early YSO evolution from a protostar to a pre-main-sequence star and provides a unique observational test to star-formation models; (5) for Lup pre-main-sequence stars, the ratio of their T-bol to T-eff increases during their approach to the ZAMS. This increase can be explained by the disk and envelope dissipation during the pre-main-sequence evolution; (6) the most active star-forming clouds (Oph and CrA) also have denser molecular cores as measured by (CO)-O-18 J = 1-0 line emission, suggesting that the star formation occurs in the densest parts of the molecular clouds; and (7) we find an anti-correlation between T-bol and (CO)-O-18 emission for the class 0 and I Tau sources (T-bol < 650 K). This shows that T-bol measures the intrinsic redness of YSOs, rather than their disk-envelope orientation. The disk orientation may have a more important effect on T-bol of the pre-main-sequence stars. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98148. NR 53 TC 62 Z9 62 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 1997 VL 478 IS 1 BP 295 EP 312 DI 10.1086/303769 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WN497 UT WOS:A1997WN49700030 ER PT J AU Mazeh, T Mayor, M Latham, DW AF Mazeh, T Mayor, M Latham, DW TI Eccentricity versus mass for low-mass secondaries and planets SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, spectroscopic; planetary systems ID PROPER-MOTION STARS; 40 SPECTROSCOPIC BINARIES; GRAVITATIONAL INSTABILITIES; ORBITAL ELEMENTS; DISK; SYSTEM; EVOLUTION; COMPANION; DYNAMICS; SAMPLE AB Spectroscopic orbits have been reported for six unseen companions orbiting solar-type stars with minimum possible masses in the range 0.5-10 Jupiter masses. The four least massive companions, around 51 Peg, 47 UMa, 55 Cnc, and tau Boo, have nearly circular orbits, while the two most massive companions, around HD 114762 and 70 Vir, have eccentricities of 0.35 and 0.40. We compare the orbital eccentricities of these six planet candidates with the eccentricities of the planets in the solar system, of the three planets found around the pulsar PSR B1957+12, and of the low-mass secondaries in a subsample of the spectroscopic binaries from the Carney-Latham proper-motion survey. The distribution of eccentricities for the combined samples displays a striking pattern: the companions with masses smaller than about 5 Jupiter masses have circular orbits, while the more massive companions have eccentric orbits. We outline four possible scenarios that might have produced this pattern of eccentricity versus mass. C1 OBSERV GENEVA,CH-1290 SAUVERNY,SWITZERLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Mazeh, T (reprint author), TEL AVIV UNIV,RAYMOND & BEVERLY SACKLER FAC EXACT SCI,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. NR 41 TC 20 Z9 20 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 1997 VL 478 IS 1 BP 367 EP 373 DI 10.1086/303776 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WN497 UT WOS:A1997WN49700037 ER PT J AU Drake, JJ Laming, JM Widing, KG AF Drake, JJ Laming, JM Widing, KG TI Stellar coronal abundances .5. Evidence for the first ionization potential effect in alpha centauri SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, abundances; stars, coronae; stars, individual (alpha Centauri); ultraviolet, stars ID EXTREME-ULTRAVIOLET SPECTRUM; SOLAR TRANSITION REGION; ATOMIC DATA; FE-XIV; LINE-INTENSITIES; INTERSTELLAR HYDROGEN; OSCILLATOR-STRENGTHS; COLLISION STRENGTHS; LEVEL POPULATIONS; COOL STARS AB We present an analysis of the EUV spectrum of the nearby binary alpha Cen AB (G2 V, KO V), observed by the Extreme Ultraviolet Explorer satellite (EUVE). Emission measure curves are constructed for elements with high and low first ionization potential (FIP) in order to investigate the coronal composition and determine whether or not a solar-like compositional fractionation mechanism ('' FIP effect'') is operating in the corona of alpha Cen. As pointed out in the recent analysis of the alpha Cen EUVE spectra by Mewe et al., the emission measure distribution is very much like that of the Sun. It peaks at log T similar to 6.3, has a minimum near log T similar to 5.5, and has a slope between these points of approximately 1.75 (EM proportional to T-7/4). The emission measure results for the different elements are not consistent with the underlying photospheric composition and indicate that the low-FIP elements are overabundant relative to the high-FIP elements by a factor of about 2. This result represents the first evidence of the FIP effect in solar-like stars with similar activity to that of the Sun. We also discuss the recently raised possibility that resonant scattering of line radiation might be important in EUV stellar spectra like that of alpha Cen. We conclude that this is unlikely and that the results of global plasma model-fitting techniques that have engendered this hypothesis have not taken into account the flux from spectral lines that are missing from current models of plasma radiative loss. C1 UNIV CALIF BERKELEY,CTR EUV ASTROPHYS,BERKELEY,CA 94720. USN,RES LAB,EO HULBURT CTR SPACE RES,WASHINGTON,DC 20375. RP Drake, JJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS-70,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 86 TC 67 Z9 67 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 1997 VL 478 IS 1 BP 403 EP 416 DI 10.1086/303755 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WN497 UT WOS:A1997WN49700041 ER PT J AU Kelson, DD vanDokkum, PG Franx, M Illingworth, GD Fabricant, D AF Kelson, DD vanDokkum, PG Franx, M Illingworth, GD Fabricant, D TI Evolution of early-type galaxies in distant clusters: The fundamental plane from Hubble Space Telescope imaging and Keck spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, clusters, general; galaxies, clusters, individual (C1 1358+62, MS 2053-04); galaxies, evolution; galaxies, fundamental parameters; galaxies, kinematics and dynamics ID ELLIPTICAL GALAXIES; PHOTOMETRY; POPULATION AB We present new results on the fundamental plane of galaxies in two rich clusters, Cl 1358+62 at z = 0.33 and MS 2053-04 at z = 0.58, based on Keck and Hubble Space Telescope observations. Our new data triple the sample of galaxies with measured fundamental plane parameters at intermediate redshift. The early-type galaxies in these clusters define very clear fundamental plane relations, confirming an earlier result for Cl 0024+16, at z = 0.39. This large sample allows us to estimate the scatter reliably. We find it to be low, at +/-0.067 in log r(e), or 17% in r(e), similar to that observed in comparable low-redshift clusters. This suggests that the structure of the older galaxies has changed little since z = 0.58. The M/L(V) ratios of early-type galaxies clearly evolve with redshift; the evolution is consistent with Delta log (M/L(V)) similar to -0.3z. The M/L(V) ratios of two E+A galaxies in Cl 1358+62 are also lower by a factor of similar to 3, consistent with the hypothesis that they underwent a starburst 1 Gyr previously. We conclude that the fundamental plane can therefore be used as a sensitive diagnostic of the evolutionary history of galaxies. Our data, when compared with the predictions of simple stellar population models, imply that the oldest cluster galaxies formed at high redshift (z > 2). We infer a different evolutionary history for the E+A galaxies, in which a large fraction of stars formed at z < 1. Larger samples spanning a larger redshift range are needed to determine the influence of starbursts on the general cluster population. C1 KAPTEYN ASTRON INST,NL-9700 AV GRONINGEN,NETHERLANDS. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Kelson, DD (reprint author), UNIV CALIF SANTA CRUZ,UNIV CALIF OBSERV,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064, USA. NR 34 TC 108 Z9 108 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 1997 VL 478 IS 1 BP L13 EP & DI 10.1086/310545 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WN500 UT WOS:A1997WN50000004 ER PT J AU Seljak, U Zaldarriaga, M AF Seljak, U Zaldarriaga, M TI Signature of gravity waves in the polarization of the microwave background SO PHYSICAL REVIEW LETTERS LA English DT Article ID GRAVITATIONAL-WAVES; RADIATION; ANISOTROPY AB Using spin-weighted decomposition of polarization in the cosmic microwave background (CMB) we show that a particular combination of Stokes Q and U parameters vanishes for primordial fluctuations generated by scalar modes, but does not for those generated by primordial gravity waves. Because of this gravity wave detection is not limited by cosmic variance as in the case of temperature fluctuations. We present the exact expressions for various polarization power spectra, which are valid on any scale. Numerical evaluation in inflation-based models shows that the expected signal is of the order of 0.5 mu K. which could be directly tested in future CMB experiments. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. RP Seljak, U (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 24 TC 499 Z9 499 U1 2 U2 11 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 17 PY 1997 VL 78 IS 11 BP 2054 EP 2057 DI 10.1103/PhysRevLett.78.2054 PG 4 WC Physics, Multidisciplinary SC Physics GA WN079 UT WOS:A1997WN07900006 ER PT J AU Kamionkowski, M Kosowsky, A Stebbins, A AF Kamionkowski, M Kosowsky, A Stebbins, A TI A probe of primordial gravity waves and vorticity SO PHYSICAL REVIEW LETTERS LA English DT Article ID MICROWAVE BACKGROUND-RADIATION; GRAVITATIONAL-WAVES; POLARIZATION; INFLATION; COBE AB A formalism for describing an all-sky map of the polarization of the cosmic microwave background is presented. The polarization pattern on the sky can be decomposed into two geometrically distinct components. One of these components is not coupled to density inhomogeneities. A nonzero amplitude for this component of polarization can only be caused by tensor or vector metric perturbations. This allows unambiguous identification of long-wavelength gravity waves or large-scale vortical flows at the time of last scattering. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. HARVARD UNIV,LYMAN LAB,DEPT PHYS,CAMBRIDGE,MA 02138. FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. RP Kamionkowski, M (reprint author), COLUMBIA UNIV,DEPT PHYS,538 W 120TH ST,NEW YORK,NY 10027, USA. NR 28 TC 419 Z9 419 U1 1 U2 4 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 17 PY 1997 VL 78 IS 11 BP 2058 EP 2061 DI 10.1103/PhysRevLett.78.2058 PG 4 WC Physics, Multidisciplinary SC Physics GA WN079 UT WOS:A1997WN07900007 ER PT J AU Campbell, BA Shepard, MK AF Campbell, BA Shepard, MK TI Effect of Venus surface illumination on photographic image texture SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY AB Radar images from Magellan have provided tremendous opportunities to study the geology and bulk dielectric properties of Venus, but many questions can only be addressed through direct photography or imaging spectroscopy of the surface. The thick atmosphere creates a situation of nearly isotropic illumination, so true shadows cannot exist for even very rough terrain. We carried out ray-tracing simulations for synthetic surfaces under both isotropic and directional illumination conditions. Relative to similar surfaces viewed under directional illumination, venusian terrain will exhibit and equal or greater range of mean brightness with changing roughness, but a concurrent reduction in the maximum possible standard deviation of brightness across any region of given roughness. The local variability of an image is often referred to as texture, and these results indicate that venus geologic units will appear more homogeneous in brightness than the same surfaces viewed under favorable directional illumination. In addition, the lack of a preferred lighting direction makes identification of surface structural patterns difficult. A similar situation may occur on Titan. C1 BLOOMSBURG UNIV PENN,DEPT GEOG & EARTH SCI,BLOOMSBURG,PA 17815. RP Campbell, BA (reprint author), SMITHSONIAN INST,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. NR 10 TC 2 Z9 2 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 15 PY 1997 VL 24 IS 6 BP 731 EP 734 DI 10.1029/97GL00598 PG 4 WC Geosciences, Multidisciplinary SC Geology GA WN972 UT WOS:A1997WN97200028 ER PT J AU Riley, SM AF Riley, SM TI The secret diary of Anne Boleyn - Maxwell,R SO LIBRARY JOURNAL LA English DT Book Review RP Riley, SM (reprint author), SMITHSONIAN INST LIB,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 SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 15 PY 1997 VL 122 IS 5 BP 90 EP 90 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA WM191 UT WOS:A1997WM19100219 ER PT J AU Graham, JA Phelps, RL Freedman, WL Saha, A Ferrarese, L Stetson, PB Madore, BF Silbermann, NA Sakai, S Kennicutt, RC Harding, P Bresolin, F Turner, A Mould, JR Rawson, DM Ford, HC Hoessel, JG Han, MS Huchra, JP Macri, LM Hughes, SM Illingworth, GD Kelson, DD AF Graham, JA Phelps, RL Freedman, WL Saha, A Ferrarese, L Stetson, PB Madore, BF Silbermann, NA Sakai, S Kennicutt, RC Harding, P Bresolin, F Turner, A Mould, JR Rawson, DM Ford, HC Hoessel, JG Han, MS Huchra, JP Macri, LM Hughes, SM Illingworth, GD Kelson, DD TI The Hubble Space Telescope Extragalactic Distance Scale Key Project .7. The discovery of Cepheids in the Leo I group galaxy NGC 3351 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cepheids; distance scale; galaxies, clusters, individual (Leo); galaxies, individual (NGC 3351) ID ABSOLUTE PEAK BRIGHTNESS; CCD PHOTOMETRY; INTERGALACTIC RING; GLOBULAR-CLUSTERS; NEUTRAL HYDROGEN; M96 GROUP; CONSTANT; SUPERNOVAE; NGC-3627; STARS AB We report of the discovery and properties of Cepheid variable stars in the barred spiral galaxy NGC 3351 which is a member of the Leo I group of galaxies. NGC 3351 is one of 18 galaxies being observed as part of the Hubble Space Telescope (HST) Key Project on;the Extragalactic Distance Scale which aims to determine the Hubble constant to 10% accuracy. Our analysis is based on observations made with the Wide Field Planetary Camera 2 during 1994 and early 1995. The Leo I group contains several bright galaxies of diverse types and is very suitable for linking together a number of secondary calibrators which can be employed at much greater distances than the Cepheid variables. We identify 49 probable Cepheids within NGC 3351 in the period range 10-43 days which have been observed at 12 epochs with the F555W filter and 4 epochs using the F814W filter. The HST F555W and F814W data have been transformed to the Johnson V and Cousins I magnitude systems, respectively. Photometry has principally been;carried out using the DAOPHOT/ALLFRAME package. Reference is made to parallel measurements being made with the DoPHOT package. Apparent period-luminosity functions for V and I have been constructed assuming values of mu(0) = 18.50 +/- 0.10 mag and E(B-V) = 0.10 mag for the distance modulus and reddening of the Large Magellanic Cloud. A true distance modulus of 30.01 +/- 0.19 mag is derived corresponding to a distance of 10.05 +/- 0.88 Mpc with a reddening E(V-I) = 0.15 mag. A comparison is made with distances estimated for other galaxies in the Leo I group using various distance indicators. There is good agreement with the surface brightness fluctuation and planetary nebula luminosity function methods as calibrated by the Cepheids in M31. C1 CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. NATL RES COUNCIL CANADA,HERZBERG INST ASTROPHYS,DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. CALTECH,CTR INFRARED PROC & ANAL,PASADENA,CA 91125. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,INST ADV STUDIES,WESTON,ACT 2611,AUSTRALIA. JOHNS HOPKINS UNIV,BALTIMORE,MD 21218. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. UNIV WISCONSIN,DEPT ASTRON,MADISON,WI 53706. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0HA,ENGLAND. UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064. RP Graham, JA (reprint author), CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,5241 BROAD BRANCH RD NW,WASHINGTON,DC 20015, USA. OI Macri, Lucas/0000-0002-1775-4859 NR 54 TC 73 Z9 73 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 1997 VL 477 IS 2 BP 535 EP 559 DI 10.1086/303740 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WM090 UT WOS:A1997WM09000002 ER PT J AU Mahadevan, R AF Mahadevan, R TI Scaling laws for advection-dominated flows: Applications to low-luminosity galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; cooling flows; galaxies, elliptical and lenticular, cD; radiation mechanisms, thermal; radio continuum, galaxies; X-rays, galaxies ID EARLY-TYPE GALAXIES; BLACK-HOLE; A-ASTERISK; ACCRETION; SPECTRUM; PLASMAS; MODEL; GAS AB We present analytical scaling laws for self-similar advection-dominated flows. The spectra from these systems range from 10(8) to 10(20) Hz and are determined by considering cooling of electrons through synchrotron, bremsstrahlung, and Compton processes. We show that the spectra can be quite accurately reproduced without detailed numerical calculations and that there is a strong testable correlation between the radio and X-ray fluxes from these systems. We describe how different regions of the spectrum scale with the mass of the accreting black hole, M, the accretion rate of the gas, M, and the equilibrium temperature of the electrons, T-e. We show that the universal radio spectral index of 1/3 observed in most elliptical galaxies (Slee et al.) is a natural consequence of self-absorbed synchrotron radiation from these flows. We also give expressions for the total luminosity of these flows and the critical accretion rate, M(crit), above which the advection solutions cease to exist. We find that for most cases of interest, the equilibrium electron temperature is fairly insensitive to M, M, and parameters in the model. We apply these results to low-luminosity black holes in galactic nuclei. We show that the problem posed by Fabian & Canizares of whether bright elliptical galaxies host dead quasars is resolved, as pointed out recently by Fabian & Rees, by considering advection-dominated hows. RP Mahadevan, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 35 TC 192 Z9 193 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 1997 VL 477 IS 2 BP 585 EP 601 DI 10.1086/303727 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WM090 UT WOS:A1997WM09000007 ER PT J AU BohmVitense, E Evans, NR Carpenter, K BeckWinchatz, B Robinson, R AF BohmVitense, E Evans, NR Carpenter, K BeckWinchatz, B Robinson, R TI The mass of the classical Cepheid S Muscae SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, visual; Cepheids; stars, evolution; stars, fundamental parameters; stars, individual (S Muscae); stars interiors ID PERIOD-LUMINOSITY RELATIONS; AGE MAIN-SEQUENCE; STELLAR MODELS; OPACITY TABLES; STARS; ATMOSPHERES; VARIABLES; COMPANIONS; EVOLUTION; BINARIES AB A good determination of the mass-luminosity relation for evolved stars on blue loops can determine the degree of excess mixing in the interiors of their main-sequence companions. In this study we determine the dynamical mass of the Cepheid binary S Muscae. This can be combined with its known luminosity and be fitted on evolutionary tracks to determine the amount of mixing in the main-sequence progenitor. Using the Goddard High Resolution Spectrograph on the Hubble Space Telescope we have measured the orbital radial velocity changes for the companion of the Cepheid S Mus. Spectra taken at minimum and maximum orbital velocities were cross-correlated. The velocity difference was measured to be 30.6+/-0.4 km s(-1). The difference for the orbital velocities of the Cepheid for the same phases was determined to be 26.9 km s(-1)+/-0.4 km s(-1). This gives a velocity ratio of 1.14+/-0.02, which gives us the mass ratio for the companions. Adding possible centering errors of the target in the entrance apertures the error limit would be increased to +/-0.06. The derived spectral types of the companion S Mus B range from B3 V to B5 V depending on the criterion used to determine it, with an average spectral type B3.8 V. Using the average spectral type and the main-sequence mass-spectral type relation from Andersen & Harmanec we find for S Mus B a mass of 5.2+/-0.2 M.. With the newly determined mass ratio the mass for the Cepheid S Mus A comes out to be 5.9(-0.6)(+0.7) M.. Taking the mass of 5.9 M. at face value and adopting the absolute visual magnitude of M(upsilon)=-4.29 (log L/L.=3.62) for the Cepheid S Mus this indicates mixing in its main-sequence progenitor slightly in excess of the one assumed for the Maeder and Meynet evolutionary tracks. The present uncertainties in mass and luminosity prevent, however, a firm conclusion about the exact degree of mixing. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. YORK UNIV,DEPT PHYS & ASTRON,N YORK,ON M3J 1P3,CANADA. NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. COMP SCI CORP,GREENBELT,MD 20771. RP BohmVitense, E (reprint author), UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195, USA. NR 52 TC 12 Z9 12 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 1997 VL 477 IS 2 BP 916 EP 925 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WM090 UT WOS:A1997WM09000033 ER PT J AU Gary, DE Hartl, MD Shimizu, T AF Gary, DE Hartl, MD Shimizu, T TI Nonthermal radio emission from solar soft X-ray transient brightenings SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun, radio radiation; Sun, X-rays, gamma rays ID ACTIVE REGIONS; TELESCOPE; FLARES; YOHKOH; MICROFLARES; DENSITY AB We compare microwave total power spectral data from the Owens Valley Radio Observatory Solar Array with soft X-ray transient brightenings observed with the Yohkoh soft X-ray telescope. We find that the transient brightenings are clearly detected in microwaves in 12 of 34 events (35%), possibly detected in another 17 of 34 events (50%), and only five of 34 events (15%) had no apparent microwave counterpart. Comparing the radio and soft X-ray characteristics, we find that (1) the soft X-ray peak is delayed relative to the microwave peak in 16 of 20 events, (2) the microwave flux is correlated with the flux seen in soft X-rays, (3) when radio fluence is used instead of radio flux (24 events) the correlation increases substantially, (4) the microwave spectra in the range 1-18 GHz vary greatly from event to event, (5) the microwave spectra often peak in the range 5-10 GHz (13 of 16 events), and (6) the microwave spectra of some events show narrowband spectra with a steep low-frequency slope. We conclude that the emission from at least some events is the result of a nonthermal population of electrons, and that transient brightenings as a whole can therefore be identified as microflares, the low-energy extension of the general flare energy distribution. Soft X-ray transient brightenings, and therefore microflares, cannot heat the corona. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV TOKYO,INST ASTRON,MITAKA,TOKYO 181,JAPAN. RP Gary, DE (reprint author), CALTECH,SOLAR ASTRON 264-33,PASADENA,CA 91125, USA. OI Gary, Dale/0000-0003-2520-8396 NR 24 TC 42 Z9 42 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 1997 VL 477 IS 2 BP 958 EP 968 DI 10.1086/303748 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WM090 UT WOS:A1997WM09000036 ER PT J AU Anderson, JD AF Anderson, JD TI Langley's aeronautical research: A modern critique and reassessment SO AIAA JOURNAL LA English DT Article AB Samuel Langley, third Secretary of the Smithsonian, was also the first U.S. government in-house researcher in aerodynamics. By 1890, he had carried put a carefully conceived, accurately engineered series of aerodynamic experiments that provided a database for the design of his steam-powered aerodromes, successfully flown in 1896. Langley's work is examined from a modern perspective. The aerodrome flights of 1896 are discussed. Particular emphasis is placed on a reassessment of Langley's aerodynamic experiments and data. The Langley law for the variation of power required as a function of velocity, which was immediately controversial in his time and remained so until the present, is finally explained for the first time, and the controversy removed. Also, Langley produced the first definitive data showing the aerodynamic superiority of high-aspect-ratio wings. Those data, if they had been properly appreciated by the Wright brothers, might have greatly improved their early glider designs. This presentation also compares and contrasts Langley's aerodynamic data with the contemporary data of Lilienthal. In general, Langley's aerodynamics, vis-a-vis the aerodynamics of Lilienthal and the Wright brothers, is brought into clearer focus. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560. RP Anderson, JD (reprint author), UNIV MARYLAND,DEPT AEROSP ENGN,COLLEGE PK,MD 20742, USA. NR 8 TC 0 Z9 0 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD MAR PY 1997 VL 35 IS 3 BP 409 EP 419 PG 11 WC Engineering, Aerospace SC Engineering GA WM098 UT WOS:A1997WM09800001 ER PT J AU Taylor, L AF Taylor, L TI Converging cultures: Art and identity in Spanish America SO AMERICAN QUARTERLY LA English DT Art Exhibit Review RP Taylor, L (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 SN 0003-0678 J9 AM QUART JI Am. Q. PD MAR PY 1997 VL 49 IS 1 BP 138 EP 161 DI 10.1353/aq.1997.0010 PG 24 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA WN869 UT WOS:A1997WN86900005 ER PT J AU Erwin, D Valentine, J Jablonski, D AF Erwin, D Valentine, J Jablonski, D TI The origin of animal body plans SO AMERICAN SCIENTIST LA English DT Article ID EVOLUTION; GENES C1 UNIV CALIF BERKELEY,DEPT INTEGRAT BIOL,BERKELEY,CA. UNIV CALIF BERKELEY,MUSEUM PALEONTOL,BERKELEY,CA. UNIV CHICAGO,DEPT GEOPHYS SCI,CHICAGO,IL 60637. UNIV CHICAGO,COMM EVOLUTIONARY BIOL,CHICAGO,IL 60637. RP Erwin, D (reprint author), NATL MUSEUM NAT HIST,DEPT PALEOBIOL,SMITHSONIAN INST,MRC-121,WASHINGTON,DC 20560, USA. RI Erwin, Douglas/A-9668-2009 NR 15 TC 57 Z9 63 U1 1 U2 13 PU SIGMA XI-SCI RES SOC PI RES TRIANGLE PK PA PO BOX 13975, RES TRIANGLE PK, NC 27709 SN 0003-0996 J9 AM SCI JI Am. Scientist PD MAR-APR PY 1997 VL 85 IS 2 BP 126 EP 137 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WH854 UT WOS:A1997WH85400011 ER PT J AU Forbes, DA Brodie, JP Huchra, J AF Forbes, DA Brodie, JP Huchra, J TI Hubble Space Telescope imaging of the globular cluster system NGC 58461 SO ASTRONOMICAL JOURNAL LA English DT Article ID PLANETARY CAMERA; STAR-CLUSTERS; GALAXIES; M87; ELLIPTICALS; PHOTOMETRY; DISCOVERY AB Bimodal globular cluster metallicity distributions have now been seen in a handful of large ellipticals. Here we report the discovery of a bimodal distribution in the dominant group elliptical NGC 5846, using the Hubble Space Telescope's Wide Field and Planetary Camera 2 (WFPC2). The two peaks are located at V-I=0.96 and 1.17, which roughly correspond to metallicities of [Fe/H]=-1.2 and -0.2, respectively. The luminosity functions of the blue and red subpopulations appear to be the same, indicating that luminosity does not correlate with metallicity within an individual galaxy's globular cluster system. Our WFPC2 data cover three pointings allowing us to examine the spatial distribution of globular clusters out to 30 kpc (or 2.5 galaxy effective radii). We find a power law surface density with a very flat slope, and a tendency for globular clusters to align close to the galaxy minor axis. An extrapolation of the surface density profile, out to 50 kpc, gives a specific frequency S-N=4.3+/-1.1. Thus NGC 5846 has a much lower specific frequency than other dominant ellipticals in clusters but is similar to those in groups. The central galaxy regions reveal some filamentary dust features, presumably from a past merger or accretion of a gas-rich galaxy. This dust reaches to the very nucleus and so provides an obvious source of fuel for the radio core. We have searched for proto-globular clusters that may have resulted from the merger/accretion and find none. Finally, we briefly discuss the implications of our results for globular cluster formation mechanisms. (C) 1997 American Astronomical Society. C1 UNIV BIRMINGHAM,SCH PHYS & SPACE RES,BIRMINGHAM B15 2TT,W MIDLANDS,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Forbes, DA (reprint author), UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064, USA. NR 44 TC 41 Z9 41 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1997 VL 113 IS 3 BP 887 EP & DI 10.1086/118308 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK846 UT WOS:A1997WK84600001 ER PT J AU Lacy, CHS Fekel, FC Mathieu, RD Morrell, NI Morse, JA Torres, G Willmarth, D AF Lacy, CHS Fekel, FC Mathieu, RD Morrell, NI Morse, JA Torres, G Willmarth, D TI The spectroscopic orbit of Pi Ceti SO ASTRONOMICAL JOURNAL LA English DT Article ID CHROMOSPHERICALLY ACTIVE STARS; B-TYPE STARS; PHOTOMETRY; SPECTRA; ABUNDANCES; CATALOG; GIANTS AB pi Ceti (HR 811, B7 V) has been known to be variable in its radial velocity for almost a century, but its relatively long period and small amplitude have conspired against a determination of its orbit. We have combined in an optimal fashion observations from early in this century with modern measurements to find the spectroscopic orbit with high accuracy. The orbit has a period of 7.45 years and a semiamplitude of 4.3 km/s. The measured eccentricity of e=0.00+/-0.07 is indistinguishable from circular, surprising for such a long period. The 76 radial velocity observations available extend over 12 cycles of the orbit. (C) 1997 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. TENNESSEE STATE UNIV, CTR EXCELLENCE INFORMAT SYST, NASHVILLE, TN 37203 USA. UNIV WISCONSIN, DEPT ASTRON, MADISON, WI 53706 USA. UNIV NACL LA PLATA, FAC CIENCIAS ASTRON & GEOFIS, LA PLATA, ARGENTINA. UNIV COLORADO, CTR ASTROPHYS & SPACE ASTRON, BOULDER, CO 80303 USA. NATL OPT ASTRON OBSERV, TUCSON, AZ 85726 USA. RP Lacy, CHS (reprint author), UNIV ARKANSAS, DEPT PHYS, FAYETTEVILLE, AR 72701 USA. NR 31 TC 4 Z9 4 U1 0 U2 0 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 1997 VL 113 IS 3 BP 1088 EP 1090 DI 10.1086/118325 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK846 UT WOS:A1997WK84600018 ER PT J AU Lacy, CHS AF Lacy, CHS TI Absolute dimensions and masses of YY Sagittarii and V526 Sagittarii SO ASTRONOMICAL JOURNAL LA English DT Article ID INTERNAL STRUCTURE CONSTANTS; APSIDAL MOTION; PHOTOMETRIC ORBIT; STELLAR AB Accurate masses and radii have been determined from new spectroscopic observations and previously published photometric orbits of YY Sgr (B5+B6) and V526 Sgr (B9.5+A2), two Southern eclipsing binaries with eccentric orbits and measured apsidal rotation. The measured properties, including apsidal rotation rate, are compared with recent theoretical predictions. The models indicate ages near 30 million and 200 million years for YY Sgr and V526 Sgr, respectively. The agreement between theory and observations is not entirely satisfactory for V526 Sgr. (C) 1997 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Lacy, CHS (reprint author), UNIV ARKANSAS,DEPT PHYS,FAYETTEVILLE,AR 72701, USA. NR 11 TC 13 Z9 13 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1997 VL 113 IS 3 BP 1091 EP 1094 DI 10.1086/118326 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK846 UT WOS:A1997WK84600019 ER PT J AU Fox, GK Code, AD Anderson, CM Babler, BL Bjorkman, KS Johnson, JJ Meade, MR Nordsieck, KH Sanders, WT Weitenbeck, AJ Zellner, NEB Edgar, RJ Lupie, OL AF Fox, GK Code, AD Anderson, CM Babler, BL Bjorkman, KS Johnson, JJ Meade, MR Nordsieck, KH Sanders, WT Weitenbeck, AJ Zellner, NEB Edgar, RJ Lupie, OL TI Solar system observations by the Wisconsin Ultraviolet PhotoPolarimeter Experiment .1. The first ultraviolet linear spectropolarimetry of Mars SO ASTRONOMICAL JOURNAL LA English DT Article ID MARTIAN DUST STORMS; POLARIMETRIC ANALYSIS; ATMOSPHERE; CLOUDS; SATURN; LIGHT; UV AB The first ultraviolet (UV) linear spectropolarimetry of Mars using the Wisconsin Ultraviolet PhotoPolarimeter Experiment (WUPPE) was obtained on 1995 March 12 at a phase angle of 21.7 degrees. A ground-based support observation was taken within 5 h, providing a total spectral coverage of 2100-10 200 Angstrom. The plane of polarization changes by 90 degrees at 4600 Angstrom. The UV polarization increases with decreasing wavelength, due to atmospheric scattering. A plane parallel, optically thin; atmosphere is used to model the polarization data, from which the optical depth of the atmosphere is derived. Assuming a pure CO2 atmosphere a total pressure of 6 mbar is obtained. The Lambert albedo of the surface is obtained in the wavelength range of 2100-3100 Angstrom. (C) 1997 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. RP Fox, GK (reprint author), UNIV WISCONSIN,SPACE ASTRON LAB,1150 UNIV AVE,MADISON,WI 53706, USA. OI Babler, Brian/0000-0002-6984-5752 NR 34 TC 1 Z9 1 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1997 VL 113 IS 3 BP 1152 EP 1157 DI 10.1086/118334 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK846 UT WOS:A1997WK84600027 ER PT J AU Fox, GK Code, AD Anderson, CM Babler, BL Bjorkman, KS Johnson, JJ Meade, MR Nordsieck, KH Sanders, WT Weitenbeck, AJ Zellner, NEB Edgar, RJ Lupie, OL AF Fox, GK Code, AD Anderson, CM Babler, BL Bjorkman, KS Johnson, JJ Meade, MR Nordsieck, KH Sanders, WT Weitenbeck, AJ Zellner, NEB Edgar, RJ Lupie, OL TI Solar system observations by the Wisconsin Ultraviolet Photopolarimeter Experiment .2. The first linear ultraviolet spectropolarimetry of Io SO ASTRONOMICAL JOURNAL LA English DT Article ID OPTICAL POLARIMETRY; GALILEAN SATELLITES; SURFACE; TELESCOPE; JUPITER; SPECTRA; SULFUR; MODEL; FROST; SO2 AB The Wisconsin Ultraviolet Photopolarimeter Experiment (WUPPE) observed Io during the Astro-l mission on 1990 December 7 and during the Astro-2 mission on 1995 March 4, 9, and 16 in the wavelength range 2100-3100 Angstrom with a resolution of 100 Angstrom. The albedo measurements are consistent with about 25% of the surface being covered by an SO2 frost. Polarimetric differences between the March 9 and 16 observations (orbital phase 288 degrees and 268 degrees, respectively) are interpreted as arising due to the rotational effect of two polarized regions on Io which are either associated with the volcanic site Pele or Hephaestus Patera and Viracocha Patera. (C) 1997 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. RP Fox, GK (reprint author), UNIV WISCONSIN,SPACE ASTRON LAB,1150 UNIV AVE,MADISON,WI 53706, USA. OI Babler, Brian/0000-0002-6984-5752 NR 30 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1997 VL 113 IS 3 BP 1158 EP 1165 DI 10.1086/118335 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK846 UT WOS:A1997WK84600028 ER PT J AU Koranyi, DM Strauss, MA AF Koranyi, DM Strauss, MA TI Testing the Hubble law with the IRAS 1.2 Jy redshift survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; galaxies, distances and redshifts; infrared, galaxies ID GALAXY LUMINOSITY FUNCTION; CHRONOMETRIC COSMOLOGY; NEARBY GALAXIES; VELOCITY-FIELD; SOURCE COUNTS; CUTOFF BIAS; DENSITY; ELIMINATION; MAGNITUDE; SAMPLES AB We test and reject the claim of Segal and coworkers that the correlation of redshifts and flux densities in a complete sample of IRAS galaxies favors a quadratic redshift-distance relation over the linear Hubble law. This is done, in effect, by treating the entire galaxy luminosity function as derived from the 60 mu m 1.2 Jy IRAS redshift survey of Fisher et al. as a distance indicator; equivalently, we compare the flux density distribution of galaxies as a function of redshift with predictions under different redshift-distance cosmologies, under the assumption of a universal luminosity function. This method does not assume a uniform distribution of galaxies in space. We find that this test has rather weak discriminatory power, as argued by Petrosian, and the differences between models are not as stark as one might expect a priori. Even so, we find that the Hubble law is indeed more strongly supported by the analysis than is the quadratic redshift-distance relation. We identify a bias in the Segal et al. determination of the luminosity function, which could lead one to mistakenly favor the quadratic redshift-distance law. We also present several complementary analyses of the density field of the sample; the galaxy density held is found to be close to homogeneous on large scales if the Hubble law is assumed, while this is not the case with the quadratic redshift-distance relation. C1 INST ADV STUDY,PRINCETON,NJ 08540. PRINCETON UNIV,DEPT ASTROPHYS SCI,PRINCETON,NJ 08544. RP Koranyi, DM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 46 TC 19 Z9 19 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1997 VL 477 IS 1 BP 36 EP 46 DI 10.1086/303669 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK037 UT WOS:A1997WK03700005 ER PT J AU Laor, A Fiore, F Elvis, M Wilkes, BJ McDowell, JC AF Laor, A Fiore, F Elvis, M Wilkes, BJ McDowell, JC TI The soft X-ray properties of a complete sample of optically selected quasars .2. Final results SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies, active; galaxies, nuclei; quasars, general; X-rays, galaxies ID ACTIVE GALACTIC NUCLEI; THIN ACCRETION DISKS; BIG BLUE BUMP; CONTINUUM ENERGY-DISTRIBUTIONS; ABSORPTION-LINE QUASAR; RADIO-QUIET QUASARS; SEYFERT-GALAXY; HIGH-REDSHIFT; SPECTRA; EMISSION AB We present the final results of a ROSAT PSPC program to study the soft X-ray emission properties of a complete sample of low-z quasars. This sample includes all 23 quasars from the Bright Quasar Survey with z less than or equal to 0.400 and N-HI(Gal) < 1.9 x 10(20) cm(-2). Pointed ROSAT PSPC observations were made for all quasars, yielding high signal-to-noise (S/N) spectra for most objects, which allowed an accurate determination of the spectral shape. The following main results were obtained: 1. The spectra of 22 of the 23 quasars are consistent, to within similar to 30%, with a single power-law model at rest-frame 0.2-2 keV. There is no evidence for significant soft excess emission with respect to the best-fit power law. We place a limit (95% confidence) of similar to 5 x 10(19) cm(-2) on the amount of excess foreground absorption by cold gas for most of our quasars. The limits are similar to 1 x 10(19) cm(-2) in the two highest S/N spectra. 2. The mean 0.2-2 keV continuum of quasars agrees remarkably well with an extrapolation of the mean 1050-350 Angstrom continuum recently determined by Zheng et al. (1996) for z > 0.33 quasars. This suggests that there is no steep soft component below 0.2 keV. 3. Significant X-ray absorption (tau > 0.3) by partially ionized gas (''warm absorber'') in quasars is rather rare, occurring for less than or similar to 5% of the population, which is in sharp contrast to lower luminosity active galactic nuclei (AGNs), where significant absorption probably occurs for similar to 50% of the population. 4. Extensive correlation analysis of the X-ray continuum emission parameters with optical emission-line parameters indicates that the strongest correlation is between the spectral slope alpha(x) and the H beta FWHM. A possible explanation for this remarkably strong correlation is a dependence of alpha(x) on L/L(Edd), as seen in Galactic black hole candidates. 5. The strong correlations between alpha(x) and L([O III]), Fe II/H beta, and the peak [O III] to H beta flux ratio are verified. The physical origin of these correlations is still not understood. 6. There appears to be a distinct class of ''X-ray-weak'' quasars, which form similar to 10% of the population (three out of 23), where the X-ray emission is smaller, by a factor of 10-30, than expected based on their luminosity at other bands and on their H beta luminosity. These may be quasars in which the direct X-ray source is obscured and only scattered X-rays are observed. 7. Thin accretion disk models cannot reproduce the observed 0.2-2 keV spectral shape, and they also cannot reproduce the tight correlation between the optical and soft X-ray emission. An as yet unknown physical mechanism must be maintaining a strong correlation between the optical and soft X-ray emission. 8. The H I/He I ratio in the high Galactic latitude ISM must be within 20%, and possibly within 5%, of the total H/He ratio of 10, which indicates that He in the diffuse H II gas component of the interstellar medium is mostly ionized to He II or He III. We finally note the intriguing possibility that although [alpha(x)] in radio-loud quasars (-1.15 +/- 0.14) is significantly flatter than in radio-quiet quasars (-1.72 +/- 0.09) the X-ray emission may not be related to the presence of radio emission. The difference in [alpha(x)] may result from the strong alpha(x) versus H beta FWHM correlation and the tendency of radio-loud quasars to have broader H beta. C1 CALTECH,PASADENA,CA 91125. OSSERV ASTRON ROMA,I-00040 MONTE PORZIO CATO,RM,ITALY. SAX,SCI DATA CTR,I-00131 ROME,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OI Wilkes, Belinda/0000-0003-1809-2364; Fiore, Fabrizio/0000-0002-4031-4157 NR 102 TC 465 Z9 466 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1997 VL 477 IS 1 BP 93 EP 113 DI 10.1086/303696 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK037 UT WOS:A1997WK03700009 ER PT J AU Prestwich, AH Joy, M Luginbuhl, CB Sulkanen, M Newberry, M AF Prestwich, AH Joy, M Luginbuhl, CB Sulkanen, M Newberry, M TI A search for the cooling flow accretion population: Optical and near-infrared imaging of NGC 1275 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, clusters, individual (Perseus); galaxies, cooling flows; galaxies, elliptical and lenticular, cD; galaxies, individual (NGC 1275); galaxies, photometry; X-rays, galaxies ID SURFACE PHOTOMETRY; GALAXIES; CLUSTERS; EMISSION; MATTER AB We present near-infrared and optical images of NGC 1275, the cD galaxy at the center of the Perseus cluster, and a well-known cooling how. Although cooling flows are common (perhaps occurring in > 50% of X-ray clusters) and the mass accreted over the lifetime of the cluster similar to 10(12) M., attempts to detect the cooled gas at wavelengths other than X-rays has met with limited success. In this paper, we measure the optical and near-infrared brightness profiles of NGC 1275, in an attempt to detect spatially extended low-mass stars that may have formed from the cooled gas. To measure the profiles to the required low flux levels, they have been corrected for overlapping galaxy halos and scattered light. We find that our profiles are inconsistent with models of low-mass star formation unless the initial mass function has an upper mass cutoff less than 0.1 M., or the mass of gas accumulated over the lifetime of the cluster is 1%-10% of that predicted from the X-ray mass accretion rate determined at the present epoch. C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,HUNTSVILLE,AL 35812. USN OBSERV,FLAGSTAFF STN,FLAGSTAFF,AZ 86002. AXIOM RES INC,TUCSON,AZ 85716. RP Prestwich, AH (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,MS4,CAMBRIDGE,MA 02138, USA. NR 26 TC 11 Z9 11 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1997 VL 477 IS 1 BP 144 EP 151 DI 10.1086/303693 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK037 UT WOS:A1997WK03700013 ER PT J AU Woo, JW Forrey, RC Cho, K AF Woo, JW Forrey, RC Cho, K TI Astrophysical extended X-ray absorption fine-structure analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; ISM, abundances; X-rays, general ID INTERSTELLAR GRAINS; EXAFS AB We present an astrophysical extended X-ray absorption fine-structure (EXAFS) analysis (AEA) tool. The AEA tool is designed to generate a numerical model of the modification to the X-ray absorption coefficient due to the EXAFS phenomenon. We have constructed a complete database (elements up to the atomic number 92) of EXAFS parameters: central atom phase shift (2 delta(1)), backscattering phase shift (phi(b)), and backscattering amplitude (F). Using the EXAFS parameter data base, the AEA tool can generate a numerical model of any compound when the atomic numbers of neighboring atoms and their distances to the central X-ray-absorbing atom are given. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. HARVARD UNIV,DEPT PHYS,CAMBRIDGE,MA 02138. HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. RP Woo, JW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 15 TC 11 Z9 11 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1997 VL 477 IS 1 BP 235 EP 240 DI 10.1086/303711 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK037 UT WOS:A1997WK03700023 ER PT J AU Yi, I Kenyon, SJ AF Yi, I Kenyon, SJ TI A laboratory for magnetized accretion disk model: Ultraviolet and X-ray emission from cataclysmic variable GK Persei SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries, close; stars, individual (GK Persei); stars, magnetic fields; stars, novae, cataclysmic variables ID T-TAURI STARS; NEUTRON STARS; INTERMEDIATE POLARS; RAPID OSCILLATIONS; WHITE-DWARFS; NOVA; OUTBURST; SPECTRA; DISTRIBUTIONS; INSTABILITY AB We analyze the ultraviolet spectrum of the cataclysmic variable GK Per at maximum light. The flat ultraviolet spectrum in this system requires a truncated inner accretion disk and an unusually flat radial temperature profile. This requirement is not satisfied by any nonmagnetic steady or nonsteady disk model. We consider a magnetized accretion disk model to explain the ultraviolet spectrum. The available data on the white dwarf spin and possible quasi-periodic oscillations constrain the magnetic field, B*, and the disk accretion rate, M, to lie along a well-defined spin-equilibrium condition (M/10(17) g s(-1)) similar to 100(B*/10(7) G)(2). Our self-consistent treatment of the magnetic torque on the disk flattens the disk temperature distribution outside the disk truncation radius. This modified temperature distribution is too steep to explain the UV spectrum for reasonable field strengths. X-ray heating is a plausible alternative to magnetic heating in GK Per. We estimate that the disk intercepts similar to 5% of the accretion energy in outburst, which results in an extra disk luminosity of similar to 5-10 L. Model spectra of optically thick disks are too blue to match observations. The UV spectrum of an optically thick disk with an optically thin, X-ray heated corona resembles the observed spectrum. The X-ray luminosity observed during the outburst indicates M < 10(18) g s(-1), which is a factor of 10 lower than that required to explain the ultraviolet luminosity. Radiation drag on material flowing inward along the accretion column lowers the shock temperature and reduces the X-ray luminosity. Most of the accretion energy is then radiated at extreme ultraviolet wavelengths. C1 SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. RP Yi, I (reprint author), INST ADV STUDY, OLDEN LANE, PRINCETON, NJ 08540 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 45 TC 10 Z9 10 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1997 VL 477 IS 1 BP 379 EP 389 DI 10.1086/303703 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK037 UT WOS:A1997WK03700033 ER PT J AU Eikenberry, SS Fazio, GG Ransom, SM Middleditch, J Kristian, J Pennypacker, CR AF Eikenberry, SS Fazio, GG Ransom, SM Middleditch, J Kristian, J Pennypacker, CR TI High time resolution infrared observations of the Crab Nebula pulsar and the pulsar emission mechanism SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation, detectors (solid state photomultiplier); pulsars, individual (PSR 0531+21); radiation mechanism, nonthermal; stars, neutron AB We present new, high signal-to-noise near-infrared observations of the Crab Nebula pulsar using the Solid State Photomultiplier instrument on the Multiple Mirror Telescope. Our observations cover the J (1.25 mu m), H (1.65 mu m), and K (2.2 mu m) infrared wavebands and have 20 mu s time resolution. Together with visible and UV observations made by the Hubble Space Telescope High-Speed Photometer, we have high time resolution observations covering over a decade in wavelength. We present the pulse profiles over this wavelength range, and we analyze the pulse shape as a function of wavelength, including the peak-to-peak phase separation, the peak full width half-maxima (FWHM), and the peak half-width half-maxima (HWHM). We also create both phase-averaged and phase-resolved color spectra of the pulsar emission. We find that the peak-to-peak phase separation shows a significant trend for an increase with wavelength, in rough agreement with models of the pulsar emission mechanism. The FWHM for peaks 1 and 2 also show a trend for increase with wavelength, again in qualitative agreement with the models. However, the HWHM for peaks 1 and 2 show significant differences in their wavelength dependences from the leading to trailing edges. This behavior is not predicted by current pulsar emission models, and the different wavelength dependences of the component HWHM values call into question the usefulness of FWHM measurements. Our spectral analyses show that the IR-UV dereddened phase-averaged color spectrum is essentially flat over more than a decade in frequency. This is in clear contrast to the X-ray and gamma-ray regimes, where the spectrum is falling steeply. The color spectra of peaks 1 and 2 are also essentially flat, but the ratio of the two shows statistically significant variations from a constant value. Finally, the color spectra of peaks 1 and 2 show significant differences from the leading to trailing edges. As with the HWHM, this behavior is not predicted by current pulsar emission models. C1 LOS ALAMOS NATL LAB,LOS ALAMOS,NM 87545. CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. KITT PEAK NATL OBSERV,TUCSON,AZ. RP Eikenberry, SS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 17 TC 28 Z9 28 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1997 VL 477 IS 1 BP 465 EP 474 DI 10.1086/303701 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WK037 UT WOS:A1997WK03700040 ER PT J AU Jivoff, P AF Jivoff, P TI The relative roles of predation and sperm competition on the duration of the post-copulatory association between the sexes in the blue crab, Callinectes sapidus SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE sperm competition; predation; post-copulatory mate association; blue crab ID CENTRAL CHESAPEAKE BAY; REPRODUCTIVE SUCCESS; SCOPIMERA-GLOBOSA; MATING-BEHAVIOR; RATHBUN; MATE; RISK; MOLT; INSEMINATION; SUBESTUARY AB In many species, post-copulatory mate guarding prevents other males from mating with the guarded female. In crabs; males stay with their mates to protect the female from predators because, in some species, mating occurs when she is soft and vulnerable after molting. I tested the relative roles of sperm competition and predation on the duration of the postcopulatory association in the blue crab, Callinectes sapidus. Unpaired females suffered greater predation mortality than paired females and males stayed with the female longer in the presence of predators than in their absence, suggesting that the post-copulatory association protects females during their vulnerable period. However, the association may also occur in blue crabs because of sperm competition since spermathecal contents of females in the field indicate that 12.4% mated twice. Females experimentally mated with two males contained both males ejaculates and each ejaculate had access to the unfertilized eggs, suggesting that the size of a male's ejaculate influences his fertilization rate in a multiply-mated female. Males stayed longest in response to a high risk of sperm competition. Longer post-copulatory associations allowed the first male's ejaculate to harden into a type of sperm plug, which limited the size of a second inseminator's ejaculate in a non-virgin female as compared with a virgin. Males passed larger ejaculates in the presence of rivals and when previous ejaculates were in the female spermathecae, another response to sperm competition. Larger ejaculates may need longer post-copulatory associations before a more effective sperm plug forms. Large males stayed with the female longer, which is consistent with their ability to pass larger ejaculates than small males and suggests that there may be costs to minimizing the duration of the postcopulatory association. In the field, associations last long enough to protect the female during her vulnerable phase and may ensure that the guarding male fertilizes the most eggs in the female, even if she remates. Thus, the post-copulatory association protects female blue crabs from additional inseminators as well as from predators. C1 UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 65 TC 63 Z9 69 U1 0 U2 10 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD MAR PY 1997 VL 40 IS 3 BP 175 EP 185 DI 10.1007/s002650050331 PG 11 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA WU111 UT WOS:A1997WU11100006 ER PT J AU Duke, NC Pinzon, ZS Prada, MC AF Duke, NC Pinzon, ZS Prada, MC TI Large-scale damage to mangrove forests following two large oil spills in Panama SO BIOTROPICA LA English DT Article DE aerial photography; deforestation mangrove; mapping; oil spill; Rhizophora mangle; sublethal damage; Panama ID COMMUNITIES AB Mangrove forests of Bahla Las Minas on the Caribbean coast of Panama were affected by large oil spills twice over the last 30 yr. Lethal and sublethal damage to these mangroves by the two spills was evaluated from aerial photographs, and in the field. The first spill occurred in 1968 when the tanker Witwater broke up and sunk, releasing 2.8-3.8 million liters of diesel oil and Bunker C fuel oil, and killing 49 ha of mangroves or 4 percent of the mangroves in the bay. The second was in 1986 when a Land tank at the Refineria Panama ruptured, releasing at least 8 million liters of crude oil, and killing 69 ha of mangroves or 6 percent of those in the bay. In each case, the areas affected most were the low to mid intertidal zone dominated by Rhizophora mangle. The extent and location of deforestation was site- and spill-specific, notably influenced by prevailing wind and tidal conditions. Some areas were deforested twice. Possible sublethal damage to surviving forests was assessed for the 1986 spill, noting that areas of unusually ''open'' canopy exceeded 307 ha. Field studies, reported elsewhere, confirmed that canopy leaf biomass decreased in ''open'' canopy sites where oil concentrations in surrounding sediments increased. Therefore, in 1986, a further 34 percent of mangrove forests in the bay probably suffered damage hem oiling, and the sum of these partially damaged forests plus the deforested areas more closely represents the total area of damage. It appears that only 18 percent of trees oiled in this bay eventually died, and the total area of damaged mangroves after the large 1986 oil spill was 5-6 times greater than the deforested areas alone. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RI Duke, Norman/K-5729-2013 OI Duke, Norman/0000-0003-2081-9120 NR 30 TC 49 Z9 51 U1 1 U2 17 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 1997 VL 29 IS 1 BP 2 EP 14 DI 10.1111/j.1744-7429.1997.tb00001.x PG 13 WC Ecology SC Environmental Sciences & Ecology GA XE477 UT WOS:A1997XE47700001 ER PT J AU Vennum, T AF Vennum, T TI Visions of sound: Musical instruments of first nations communities in northeastern America - Diamond,B, Cronk,MS, VonRosen,F SO CANADIAN HISTORICAL REVIEW LA English DT Book Review RP Vennum, T (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV TORONTO PRESS INC PI TORONTO PA JOURNALS DIVISION, 5201 DUFFERIN ST, DOWNSVIEW, TORONTO ON M3H 5T8, CANADA SN 0008-3755 J9 CAN HIST REV JI Can. Hist. Rev. PD MAR PY 1997 VL 78 IS 1 BP 161 EP 164 PG 4 WC History SC History GA WQ377 UT WOS:A1997WQ37700039 ER PT J AU Bushmann, PJ Atema, J AF Bushmann, PJ Atema, J TI Shelter sharing and chemical courtship signals in the lobster Homarus americanus SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID MATING-BEHAVIOR; RECOGNITION; CRUSTACEA; OLFACTION; DOMINANCE; URINE AB In a 3.7-m Y-maze flume study of social odor-mediated behavior of mature lobsters (Homarus americanus), females preferred male- but not female-occupied shelters over empty shelters: they detected them from a distance and spent much time trying to enter. Males did not show distant detection and preference for female shelters but did spend much time trying to enter female but not male shelters once nearby. Sheltered resident males showed strong aggression toward visiting males but only mild aggression to visiting females; intermolt and premolt females could enter resident male shelters, cohabit for at least 7 h, receive mating attempts, and sometimes mate. Premolt females or females with sperm plugs resisted mating attempts. Visiting females released more than four times and males more than seven times as much urine during a shelter approach compared with an equal time in isolation. Females with or without urine release entered male-occupied shelters successfully, but mating attempts rarely occurred when female urine release was blocked. Female urine block resulted in greatly increased resident male aggression toward her, reaching the same levels elicited by visiting males with or without urine block. The results show that female urine signals reduce male aggression and facilitate mating. C1 BOSTON UNIV,MARINE PROGRAM,MARINE BIOL LAB,WOODS HOLE,MA 02543. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 43 TC 44 Z9 44 U1 0 U2 11 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD MAR PY 1997 VL 54 IS 3 BP 647 EP 654 DI 10.1139/cjfas-54-3-647 PG 8 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA XB788 UT WOS:A1997XB78800015 ER PT J AU Yoshino, K Esmond, JR Parkinson, WH Ito, K Matsui, T AF Yoshino, K Esmond, JR Parkinson, WH Ito, K Matsui, T TI Absorption cross section measurements of water vapor in the wavelength region 120 nm to 188 nm (vol 211, pg 387, 1996) SO CHEMICAL PHYSICS LA English DT Correction, Addition C1 NATL LAB HIGH ENERGY PHYS,PHOTON FACTORY,TSUKUBA,IBARAKI 305,JAPAN. RP Yoshino, K (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 1 TC 9 Z9 10 U1 2 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD MAR 1 PY 1997 VL 215 IS 3 BP 429 EP 430 DI 10.1016/S0301-0104(96)00381-3 PG 2 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA WL139 UT WOS:A1997WL13900011 ER PT J AU Swofford, DL Siddall, ME AF Swofford, DL Siddall, ME TI Uneconomical diagnosis of cladograms: Comments on Wheeler and Nixon's method for Sankoff optimization SO CLADISTICS-THE INTERNATIONAL JOURNAL OF THE WILLI HENNIG SOCIETY LA English DT Article ID EVOLUTION; TREE AB We provide three simple examples demonstrating that Wheeler and Nixon's method of recoding ''stepmatrix'' characters can fail to yield most parsimonious reconstructions of character evolution under specified cost (transformation-weight) schemes. These examples variously indicate undercounting or overcounting of tree lengths due to an inappropriate assumption of independence among the recoded characters. Their method is therefore not equivalent to Sankoff's dynamic programming algorithm, contrary to their claim. (C) 1997 The Willi Hennig Society. C1 UNIV MICHIGAN,ZOOL MUSEUM,ANN ARBOR,MI 48109. RP Swofford, DL (reprint author), SMITHSONIAN INST,LAB MOL SYSTEMAT,MRC 534,WASHINGTON,DC 20560, USA. NR 10 TC 4 Z9 4 U1 1 U2 2 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0748-3007 J9 CLADISTICS JI Cladistics-Int. J. Willi Hennig Soc. PD MAR-JUN PY 1997 VL 13 IS 1-2 BP 153 EP 159 PG 7 WC Evolutionary Biology SC Evolutionary Biology GA YB227 UT WOS:A1997YB22700012 ER PT J AU Seeger, A AF Seeger, A TI A reply to Henry Kingsbury + Ethnomusicology and language SO ETHNOMUSICOLOGY LA English DT Article RP Seeger, A (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 1 Z9 1 U1 1 U2 1 PU SOC ETHNOMUSICOLOGY INC PI BLOOMINGTON PA MORRISON HALL, ROOM 005 INDIANA UNIVERSITY, BLOOMINGTON, IN 47405 SN 0014-1836 J9 ETHNOMUSICOLOGY JI Ethnomusicology PD SPR-SUM PY 1997 VL 41 IS 2 BP 250 EP 252 DI 10.2307/852606 PG 3 WC Music SC Music GA XK138 UT WOS:A1997XK13800006 ER PT J AU Stine, PS AF Stine, PS TI The organic machine: The remaking of the Columbia River - White,R SO HISTORIAN LA English DT Book Review RP Stine, PS (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU PHI ALPHA THETA PI ALLENTOWN PA THE HISTORIAN 50 COLLEGE DR, ALLENTOWN, PA 18104-6100 SN 0018-2370 J9 HISTORIAN JI Historian PD SPR PY 1997 VL 59 IS 3 BP 671 EP 672 PG 2 WC History SC History GA XF520 UT WOS:A1997XF52000037 ER PT J AU Cameron, AGW AF Cameron, AGW TI The origin of the moon and the single impact hypothesis .5. SO ICARUS LA English DT Article AB Previous papers in this series have described the smooth particle hydrodynamics (SPH) method, which has been employed to explore the possibility that a major planetary collision may have been responsible for the formation of the Moon. In those simulations the SPH code used particles of equal mass and fixed smoothing lengths; I have found that the results obtained were reliable regarding what happens to the interiors of the colliding planets. Because the particles placed into the surrounding space were isolated rather than overlapping, however, that part of the calculation was unreliable. Ten additional cases have been run with 5000 particles in the Protoearth and 5000 in the Impactor, with variable smoothing lengths. Three of the cases had Protoearth/Impactor mass ratios of 5:5, 6:4, and 7:3. The other cases had a mass ratio of 8:2 and a variety of angular momenta. All cases had zero velocity at infinity. In every case the product of the collision became surrounded by evaporated particles of rock vapor, forming an extended atmosphere; however, relatively little mass extended beyond the Roche lobe. If the Moon formed from a rock disk in orbit around the Earth, then some other mechanism would be needed to transport angular momentum and mass outward in the equatorial plane, so that rack condensates from the hot atmosphere would be precipitated beyond the Roche limit, thus providing material for collection into the Moon. Most of this atmospheric material was originally in the Impactor and was mixed with terrestrial rock before evaporation. Recent calculations by R. M. Canup and L. W. Esposito (1996, Icarus 119, 427-446) have shown that it is very difficult to form the Moon from a gaseous disk largely confined to within the Roche lobe. On the other hand, higher-angular-momentum collisions can leave a quite massive body in orbit about the Earth, and this could form much or essentially all of the Moon. These questions remain challenging and require further investigations, (C) 1997 Academic Press. RP Cameron, AGW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 13 TC 95 Z9 96 U1 1 U2 12 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 1997 VL 126 IS 1 BP 126 EP 137 DI 10.1006/icar.1996.5642 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WT567 UT WOS:A1997WT56700007 ER PT J AU Stanley, DJ Mart, Y Nir, Y AF Stanley, DJ Mart, Y Nir, Y TI Clay mineral distributions to interpret nile cell provenance and dispersal .2. Coastal plain from Nile delta to northern Israel SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE clay minerals; coastal erosion; Egyptian shelf; eolian; Gaza; hamra; High Aswan Dam; Israel coastal plain; Israeli rivers; kurkar; Levant margin; Mediterranean; Nile delta; Nile littoral cell; Sinai margin; Wadi El Arish ID SEDIMENT TRANSPORT; MEDITERRANEAN SEA; CONTINENTAL-SHELF; HEAVY MINERALS; EGYPT; EVOLUTION; PATTERNS; HISTORY; LAGOON AB This study identifies clay mineral assemblages between the eastern Nile delta and northern Israel to complement and refine interpretations of modern sediment provenance and dispersal patterns in the SE Mediterranean. Previous petrological investigations indicate that the River Nile has been the dominant source of sediment transported to the Levant Sea, whereas sediment contributions from Sinai, Gaza and Israeli rivers and coastal cliff exposures in this region have been minor. However, this sediment dispersal pattern, modelled as the Nile littoral cell, is now being altered as a response to the High Dam at Aswan, barrages along the Nile valley and in the Nile delta, and water diversion by the high-density canal system in the Nile delta. As a result, Nile sediment input identified by high proportions of smectite is presently derived from erosion of the delta margin rather than from direct dispersal by the river proper. The present investigation records important percentages of kaolinite in the clay fraction of samples recovered in coastal cliff exposures, from east of Bardawil lagoon and Wadi El Arish to the Lebanon-Israel border. Clay mineral assemblages in the fluvial channels on the coastal plain east of the Nile delta are considerably more variable: those west of El Arish are smectite-rich, while those on the plain east and north to the Tel Aviv region are kaolinite-rich; clay assemblages between Tel Aviv and Atlit are smectite-rich; still farther north, locally between Atlit and Haifa, assemblages in some fluvial channels comprise high percentages of illite, and those from north of Haifa to the Lebanese border record large proportions of kaolinite and illite. These laterally variable clay assemblages on the Sinai, Gaza and Israeli coastal margins are more closely related to the different source terrains in highlands that back the coastal plain than to distal Nile provenance. Modern clay minerals near the coast are derived from (1) rivers that flow seasonally from highlands in Sinai and Israel, (2) seasonally variable winds that carry dust from arid and semi-arid regions toward the coast, and (3) wave current erosion of coastal exposures. As the amount of distal Nile-derived clay from Egypt is reduced, these more proximal sources will likely to account for increasing proportions of clays supplied to Sinai and the SE Levant margin. C1 UNIV HAIFA, LEON RECONATI CTR, IL-31905 HAIFA, ISRAEL. GEOL SURVEY ISRAEL, IL-95501 JERUSALEM, ISRAEL. RP Stanley, DJ (reprint author), SMITHSONIAN INST, DELTAS GLOBAL CHANGE PROGRAM, E-206 NMNH, WASHINGTON, DC 20560 USA. NR 86 TC 22 Z9 22 U1 1 U2 4 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD SPR PY 1997 VL 13 IS 2 BP 506 EP 533 PG 28 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA WW936 UT WOS:A1997WW93600020 ER PT J AU Chai, P Chen, JSC Dudley, R AF Chai, P Chen, JSC Dudley, R TI Transient hovering performance of hummingbirds under conditions of maximal loading SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE aerodynamics; Archilochus colubris; hovering; hummingbird; load-lifting; maximal locomotor performance; muscle power output; temperature ID INSECT FLIGHT; POWER OUTPUT; AERODYNAMICS; MUSCLE; LIMITATIONS; ENERGETICS; HELIOX; BURST; BIRDS; LIFT AB Maximal load-lifting capacities of six ruby-throated hummingbirds (Archilochus colubris) were determined under conditions of burst performance. Mechanical power output under maximal loading was then compared with maximal hovering performance in hypodense gas mixtures of normodense air and heliox. The maximal load lifted was similar at air temperatures of 5 and 25 degrees C, and averaged 80% of body mass. The duration of load-lifting was brief, of the order of 1 s, and was probably sustained via phosphagen substrates. Under maximal loading, estimates of muscle mass-specific mechanical power output assuming perfect elastic energy storage averaged 206 W kg(-1), compared with 94 W kg(-1) during free hovering without loading. Under conditions of limiting performance in hypodense mixtures, maximal mechanical power output was much lower (131 W kg(-1), five birds) but was sustained for longer (4s), demonstrating an inverse relationship between the magnitude and duration of maximum power output. In free hovering flight, stroke amplitude and wingbeat frequency varied in inverse proportion between 5 and 25 degrees C, suggesting thermoregulatory contributions by the flight muscles. Stroke amplitude under conditions of maximal loading reached a geometrical limit at slightly greater than 180 degrees. Previous studies of maximum performance in flying animals have estimated mechanical power output using a simplified actuator disk model without a detailed knowledge of wingbeat frequency and stroke amplitude. The present load-lifting results, together with actuator disc estimates of induced power derived from hypodense heliox experiments, are congruent with previous load-lifting studies of maximum flight performance. For ruby-throated hummingbirds, the inclusion of wingbeat frequency and stroke amplitude in a more detailed aerodynamic model of hovering yields values of mechanical power output 34% higher than previous estimates. More generally, the study of performance limits in flying animals necessitates careful specification of behavioral context as well as quantitative determination of wing and body kinematics. C1 UNIV CALIF LOS ANGELES, DEPT BIOL, LOS ANGELES, CA 90024 USA. SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RP Chai, P (reprint author), UNIV TEXAS, DEPT ZOOL, AUSTIN, TX 78712 USA. NR 47 TC 63 Z9 64 U1 0 U2 6 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 EI 1477-9145 J9 J EXP BIOL JI J. Exp. Biol. PD MAR PY 1997 VL 200 IS 5 BP 921 EP 929 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA WR623 UT WOS:A1997WR62300007 PM 9100364 ER PT J AU Korth, WW Emry, RJ AF Korth, WW Emry, RJ TI The skull of Anchitheriomys and a new subfamily of beavers (Castoridae, Rodentia) SO JOURNAL OF PALEONTOLOGY LA English DT Article AB A nearly complete skull of Anchitheriomys from the Miocene of Nebraska allows description of the cranial foramina. In skull characters, Anchitheriomys most closely resembles Agnotocastor and Neatocastor among castorids; it retains primitive features that it shares with eutypomyids (position of the posterior palatine foramina, smooth palatal surface, nearly parallel tooth rows, retention of dP3) combined with derived features (elongate rostrum, procumbent incisors) that are shared only with Agnotocastor and Neatocastor. A new subfamily, Agnotocastorinae, is erected for this group of primitive beavers. C1 SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT PALEOBIOL, WASHINGTON, DC 20560 USA. RP Korth, WW (reprint author), ROCHESTER INST VERTEBRATE PALEONTOL, 928 WHALEN RD, PENFIELD, NY 14526 USA. NR 14 TC 14 Z9 14 U1 1 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 MAR PY 1997 VL 71 IS 2 BP 343 EP 347 PG 5 WC Paleontology SC Paleontology GA WU624 UT WOS:A1997WU62400014 ER PT J AU Meggers, BJ AF Meggers, BJ TI Archaeology in the lowland American tropics: Current analytical methods and recent applications - Stahl,PW SO JOURNAL OF THE ROYAL ANTHROPOLOGICAL INSTITUTE LA English DT Book Review RP Meggers, BJ (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROYAL ANTHROPOLOGICAL INST PI LONDON PA 50 FITZROY STREET, LONDON, ENGLAND W1P 5HS SN 0025-1496 J9 J ROY ANTHROPOL INST JI J. R. Anthropol. Inst. PD MAR PY 1997 VL 3 IS 1 BP 162 EP 164 DI 10.2307/3034375 PG 3 WC Anthropology SC Anthropology GA WW479 UT WOS:A1997WW47900015 ER PT J AU Murray, S Tell, LA Bush, M AF Murray, S Tell, LA Bush, M TI Zinc toxicosis in a Celebes ape (Macaca nigra) following ingestion of pennies SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Celebes ape; Macaca nigra; zinc toxicosis ID INDUCED HEMOLYTIC-ANEMIA; DOG; INTOXICATION AB An adult Celebes ape (Macaca nigra) was presented for a routine yearly evaluation. Abdominal radiographs revealed four radiodense metallic foreign objects resembling coins within the gastrointestinal tract. Hematologic abnormalities included a mild nonregenerative anemia and a mild leukocytosis, and the biochemical profile reflected renal dysfunction. Serum zinc levels were elevated. The animal was denied food for 24 hr in preparation for the endoscopic removal of the foreign objects. During this period, two partially eroded pennies were passed in the feces. Endoscopy was temporarily postponed, and the animal was offered food. Two days later a third penny was passed. When the fourth coin did not pass within the next 2 days, the animal was once again denied food, and the fourth coin was passed within 24 hr. Because of the temporal association between the fasting cycles and the passage of the coins, a causal relationship is suggested. Following the passage of all coins, serum zinc levels decreased, and hematologic and serum biochemical abnormalities improved. Six months later, all abnormalities had resolved. C1 NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. NATL ZOOL PK,WASHINGTON,DC 20008. NR 16 TC 6 Z9 6 U1 0 U2 2 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 1997 VL 28 IS 1 BP 101 EP 104 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA XH694 UT WOS:A1997XH69400015 PM 9226624 ER PT J AU Knowlton, N Mate, JL Guzman, HM Rowan, R Jara, J AF Knowlton, N Mate, JL Guzman, HM Rowan, R Jara, J TI Direct evidence for reproductive isolation among the three species of the Montastraea annularis complex in Central America (Panama and Honduras) SO MARINE BIOLOGY LA English DT Article ID REEF BUILDING CORAL; FERTILIZATION AB Montastraea annularis, M. faveolata, and M. franksi are three recently separated species that together dominate reefs of the tropical western Atlantic. Despite morphological, life-history, ecological and genetic differences, the legitimacy of their status as separate species has been questioned. This controversy stems from both the scarcity of unambiguous, diagnostic differences among them, and from the possibility of extensive hybridization associated with their approximately synchronous reproduction in sympatry. Here we report on fertilization trials and the timing of spawning, both of which suggest that the potential for hybridization may be limited. Crosses between M. faveolata (the most genetically distinctive taxon) and the other two species were largely unsuccessful, as were selfed matings for all three species. M. annularis is and M. franksi showed no evidence of fertilization barriers, but the timing of spawning typically differed between them by 1 to 2 h. We also found that spawning times in the field of M. annularis and M. faveolata were non-overlapping in 1995, and that the timing of spawning in M. annularis could be experimentally shifted forward by simulating earlier than natural sunsets. These findings from Panama and Honduras, particularly given their consistency with comparable observations and experiments elsewhere, provide evidence of reproductive isolation and support the separate species status of these three taxa. Some hybridization may occur under natural conditions at these sites, particularly between M. annularis and M. franksi. Rampant genetic interchange among these taxa in Central America seems unlikely, however, in the light of the concordant associations between morphology, reproductive biology and other characters which are observed. C1 UNIV MIAMI,ROSENSTIEL SCH MARINE & ATMOSPHER SCI,MIAMI,FL 33149. RP Knowlton, N (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 19 TC 112 Z9 118 U1 5 U2 23 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAR PY 1997 VL 127 IS 4 BP 705 EP 711 DI 10.1007/s002270050061 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA WQ425 UT WOS:A1997WQ42500020 ER PT J AU Russell, S AF Russell, S TI What use are calcium-aluminium-rich inclusions? SO METEORITICS & PLANETARY SCIENCE LA English DT Editorial Material RP Russell, S (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,DEPT MINERAL SCI,NHB-119,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 2 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD MAR PY 1997 VL 32 IS 2 BP 153 EP 153 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA WN693 UT WOS:A1997WN69300002 ER PT J AU Keane, B Dittus, WPJ Melnick, DJ AF Keane, B Dittus, WPJ Melnick, DJ TI Paternity assessment in wild groups of toque macaques Macaca sinica at Polonnaruwa, Sri Lanka using molecular markers SO MOLECULAR ECOLOGY LA English DT Article DE microsatellites; paternity; reproductive output; toque macaques ID MICROSATELLITE PCR PRIMERS; GENETIC-VARIABILITY; RHESUS-MONKEYS; REPRODUCTIVE SUCCESS; PRIMATE POPULATION; DOMINANCE; EXCLUSION; LOCI; FASCICULARIS; PROBABILITY AB Genetic variation at four microsatellite loci in conjunction with that at a highly variable allozyme locus was used to analyse paternity over a 12-year period in 13 social groups of toque macaques Macaca sinica inhabiting a natural forest in Polonnaruwa, Sri Lanka. paternity exclusion analysis revealed that the set of offspring produced by a female usually consists of half-siblings because few males father more than one offspring with a particular female. No evidence of offspring produced by matings between first degree relatives was found. The social unit in toque macaques was not identical to the reproductive unit and the possibility of paternity by males outside the social group should be considered when estimating male reproductive output. Although it was common for multiple males to father offspring in a social group each year, reproduction within a group during a breeding season tended to be limited to a few males. The mean number of males reproducing per group per year was independent of the number of males in a group. The paternity data suggests that many males may father relatively few offspring during their entire lives and that the effective population size for toque macaques may be much smaller than indicated by demographic data. C1 COLUMBIA UNIV,DEPT ANTHROPOL,NEW YORK,NY 10027. SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008. INST FUNDAMENTAL STUDIES,KANDY,SRI LANKA. COLUMBIA UNIV,DEPT BIOL SCI,NEW YORK,NY 10027. COLUMBIA UNIV,CTR ENVIRONM RES & CONSERVAT,NEW YORK,NY 10027. NR 50 TC 40 Z9 40 U1 1 U2 10 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD MAR PY 1997 VL 6 IS 3 BP 267 EP 282 DI 10.1046/j.1365-294X.1997.00178.x PG 16 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA WK617 UT WOS:A1997WK61700007 PM 9076981 ER PT J AU Harasewych, MG Adamkewicz, SL Blake, JA Saudek, D Spriggs, T Bult, CJ AF Harasewych, MG Adamkewicz, SL Blake, JA Saudek, D Spriggs, T Bult, CJ TI Phylogeny and relationships of pleurotomariid gastropods (Mollusca: Gastropoda): An assessment based on partial 18S rDNA and cytochrome c oxidase I sequences SO MOLECULAR MARINE BIOLOGY AND BIOTECHNOLOGY LA English DT Article ID RIBOSOMAL-SUBUNIT RNA; SYSTEMATICS; EVOLUTION; SNAIL AB The phylogenetic position of the ancient family Pleurotomariidae within the Molluscan class Gastropoda, as well as the relationships of its Recent genera and species, were assessed using an iterative, two-gene (18S rDNA and cytochrome c oxidase I) approach to phylogeny reconstruction. In order to orient the Pleurotomariidae within Gastropoda, partial 18S rDNA sequences were determined for 7 pleurotomariid and 22 other gastropods that span the major groups within the class as well as for one cephalopod and two polyplacophorans, which serve as outgroups. Cladistic analyses of a sequence of approximately 450 base pairs (bp) near the 5' end of the 18S rDNA support the monophyly of the following higher gastropod taxa: Patellogastropoda, Vetigastropoda, Neritopsina, Apogastropoda, and its subclades Caenogastropoda and Heterobranchia. The 18S rDNA sequences and 579 bp of cytochrome c oxidase I (COI) analyzed separately and together, indicate that Pleurotomariidae are included within Vetigastropoda but comprise a clade that is the sister group to the other families referred to this order. Monophyly of the Pleurotomariidae is also supported by the unique presence of seven separate inserts (ranging in length from 1 to 68 bp) within the V2 variable region of the 18S RNA. Relationships of the genera and species within Pleurotomariidae are fully resolved using ''total molecular evidence'' consisting of partial sequences of 18S rDNA and COI and including data on length variation within the inserts. C1 GEORGE MASON UNIV,DEPT BIOL,FAIRFAX,VA 22030. INST GEN RES,ROCKVILLE,MD 20850. RP Harasewych, MG (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. OI Blake, Judith/0000-0001-8522-334X NR 64 TC 64 Z9 65 U1 0 U2 2 PU BLACKWELL SCIENCE INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 SN 1053-6426 J9 MOL MAR BIOL BIOTECH JI Mol. Mar. Biol. Biotechnol. PD MAR PY 1997 VL 6 IS 1 BP 1 EP 20 PG 20 WC Biotechnology & Applied Microbiology; Marine & Freshwater Biology SC Biotechnology & Applied Microbiology; Marine & Freshwater Biology GA WZ155 UT WOS:A1997WZ15500001 PM 9116867 ER PT J AU Boyle, BJ Wilkes, BJ Elvis, M AF Boyle, BJ Wilkes, BJ Elvis, M TI The Cambridge-Cambridge ROSAT Serendipity Survey .5. Catalogue and optical identifications SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies, active; quasars, general; X-rays, general ID X-RAY-SPECTRA; QUASARS; QSOS; EVOLUTION; GALAXY; COUNTS; SAMPLE AB We report the results of a medium-depth X-ray survey of 20 ROSAT Position Sensitive Proportional Counter (PSPC) fields. 123 X-ray sources were detected down to a flux limit of S (0.5-2 keV) > 2 x 10(-14) erg s(-1) cm(-2) lying between that of the Einstein Extended Medium Sensitivity Survey (EMSS) and the deepest ROSAT surveys. Optical identifications of 110 of these sources have revealed 68 QSOs, 12 narrow-emission-line X-ray-luminous galaxies (NLXGs), 24 stars, two BL Lac objects, two galaxies and two clusters. CCD imaging reveals the possible presence of galaxy groups or clusters at the positions of a further four X-ray sources. The number-redshift and log N-log S relations of the 68 QSOs are in better agreement with the faster rate of cosmological evolution for X-ray QSOs derived from ROSAT deep surveys [L(X) proportional to(1 + z)(3.34+/-0.1), z(max) = 1.79] than with the evolution obtained from the EMSS [L(X) proportional to(1 + z)(2.55+/-0.1)], the latter being rejected at greater than the 3 sigma level as a model for the current sample. We present the optical spectra and measurements of the emission lines. The equivalent-width distributions are consistent with those of QSO samples selected in other wavebands. We find no evidence for an inverse correlation between line width and X-ray spectral slope as recently reported for other ROSAT QSO samples. C1 ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0EZ,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OI Wilkes, Belinda/0000-0003-1809-2364 NR 34 TC 27 Z9 27 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 1997 VL 285 IS 3 BP 511 EP 528 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WN236 UT WOS:A1997WN23600009 ER PT J AU Brandt, WN Mathur, S Elvis, M AF Brandt, WN Mathur, S Elvis, M TI A comparison of the hard ASCA spectral slopes of broad- and narrow-line Seyfert 1 galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Letter DE galaxies, active; X-rays, galaxies ID RAY; VARIABILITY; QUASARS AB The soft (approximate to 0.1-2.0 keV) X-ray spectra of narrow-line Seyfert 1 galaxies are known to be generally steeper than those of Seyfert 1 galaxies with broader optical permitted lines. This has been attributed to the presence of strong soft X-ray excesses, over the hard X-ray power law, in many narrow-line Seyfert 1s. Here we use the currently available ASCA data to systematically compare the harder (approximate to 2-10 keV) X-ray continua of soft ROSAT narrow-line Seyfert 1s with those of Seyfert 1s with larger HP FWHM. Our robust and non-parametric testing suggests, with high statistical significance, that soft ROSAT narrow-line Seyfert 1s have generally steeper intrinsic hard X-ray continua than Seyfert 1s with larger HP FWHM. The hard photon index trend appears similar to the previously known soft photon index trend, although with a reduced photon index spread. If the soft X-ray excesses of all Seyfert 1s are confined to below approximate to 1 keV they cannot directly affect the approximate to 2-10 keV spectra studied here. However, as suggested for the extreme narrow-line Seyfert 1 RE J 1034 + 393, a strong soft X-ray excess may affect the accretion disc corona which creates the underlying hard X-ray power law. If this is occurring, then more detailed study of this physical process could give clues about the formation of the underlying continua of all Seyferts. Other effects, such as intrinsic 2-10 keV continuum curvature, could also lead to the observed photon index trend and need further study. RP Brandt, WN (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Brandt, William/N-2844-2015 OI Brandt, William/0000-0002-0167-2453 NR 37 TC 81 Z9 83 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 1997 VL 285 IS 3 BP L25 EP L30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WN236 UT WOS:A1997WN23600003 ER PT J AU Weil, SE AF Weil, SE TI Romance versus realism: A reflection on the nature of museums SO MUSEUM NEWS LA English DT Article C1 SMITHSONIAN INST,CTR MUSEUM STUDIES,WASHINGTON,DC 20560. RP Weil, SE (reprint author), COLUMBIA UNIV,TEACHERS COLL,NEW YORK,NY 10027, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 1997 VL 76 IS 2 BP 52 EP & PG 0 WC Art SC Art GA WM556 UT WOS:A1997WM55600011 ER PT J AU Wasshausen, DC AF Wasshausen, DC TI Razisea ericae (Acanthaceae), a new species from Ecuador and adjacent Peru SO NOVON LA English DT Article AB Current research by the author on the Acanthaceae treatment for the Flora of Ecuador has resulted in the recognition of a new species from Amazonian Ecuador and Peru. Razisea ericae is described, illustrated, and compared with its closest relatives in Costa Rica, Panama, and Colombia. RP Wasshausen, DC (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 SN 1055-3177 J9 NOVON JI Novon PD SPR PY 1997 VL 7 IS 1 BP 88 EP 91 DI 10.2307/3392081 PG 4 WC Plant Sciences SC Plant Sciences GA XW600 UT WOS:A1997XW60000020 ER PT J AU Meldahl, KH Flessa, KW Cutler, AH AF Meldahl, KH Flessa, KW Cutler, AH TI Time-averaging and postmortem skeletal survival in benthic fossil assemblages: Quantitative comparisons among Holocene environments SO PALEOBIOLOGY LA English DT Article ID SHELL; BC; DISSOLUTION; SEDIMENTS; MEXICO AB We used radiocarbon ages on dead Holocene shells of the venerid bivalve Chione spp. to investigate how time-averaging and taphonomy in shallow marine benthic assemblages vary with sedimentary and tectonic setting. We compared shells collected from the sediment surface in five depositional environments from two regions of the Gulf of California, Mexico: Bahia Concepcion, a young faulted rift basin with high rates of terrigenous and carbonate sedimentation; and Bahia la Choya, an intertidal system along a sediment-starved shelf. Frequency distributions of shell ages in all environments form a hollow curve, with a mode at young ages and a long tail toward older ages. This pattern suggests that shells are added to the taphonomically active zone (TAZ) at roughly constant rates (via continuous shell deaths), and removed from the TAZ at random,either through destruction or by achieving final burial. Shell half-lives (the amount of time to remove half the shells from the TAZ) provide a comparative measure of time-averaging. Time-averaging varies with sedimentary and tectonic setting. The lowest amounts of time-averaging (shell half-lives of 90 to 165 years) occur in Bahia Concepcion, where rapid rates of terrigenous sedimentation (on fan-deltas) and carbonate sedimentation (in pocket bays) bury shells rapidly. Time-averaging is higher in the sediment-starved environments of Bahia la Choya (shell half-lives of 285 to 550 years). The highest amounts of time-averaging occur the inner tidal flats of Bahia la Choya (shell half-life of 550 years). Here the conjunction of low sedimentation rates with low rates of shell destruction (due to periodic tidal emergence) permits shells to persist in the TAZ for very long time spans. There is no systematic relationship between a shell's age and its taphonomic condition (taphonomic grade) in any environment, probably because of the complex and random nature of burial-exhumation in the TAZ. Age variance tends to increase with increasing taphonomic alteration: highly altered shells range in age from young to several thousand years old, while less altered shells are mostly young. The correspondence between time-averaging and the taphonomic condition of entire shell assemblages is also weak, but might be resolved with further study. These results provide quantitative data on time-averaging in benthic assemblages as a function of sedimentary and tectonic setting, and suggest some guidelines for facies appropriate for particular studies. Shallow marine rift basins like Bahia Concepcion can potentially contain within-horizon fossil assemblages representing time spans of only a few hundred years-time resolution of ten beyond reach in paleontology. In contrast, sediment-starved shelf habitats like Bahia la Choya are unlikely to yield assemblages with time resolution finer than several thousands of years. C1 UNIV ARIZONA,DEPT GEOSCI,TUCSON,AZ 85721. SMITHSONIAN INST,DEPT PALEOBIOL,WASHINGTON,DC 20560. RP Meldahl, KH (reprint author), OBERLIN COLL,DEPT GEOL,OBERLIN,OH 44074, USA. NR 61 TC 86 Z9 87 U1 0 U2 7 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 1997 VL 23 IS 2 BP 207 EP 229 PG 23 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA XF260 UT WOS:A1997XF26000005 ER PT J AU Flambaum, VV Murray, DW AF Flambaum, VV Murray, DW TI Limits on the monopole polarization magnetic field from measurements of the electric dipole moments of atoms, molecules, and the neutron SO PHYSICAL REVIEW A LA English DT Article ID SEARCH; INVARIANCE; VIOLATION; CHARGE; PARITY AB A radial magnetic field can induce a time-invariance-violating electric-dipole moment (EDM) in quantum systems. The EDMs of the Tl, Cs, Xe, and Hg atoms and the neutron that are produced by such a field are estimated. The contributions of such a field to the constants, chi of the T, P-odd interactions chi(e)N . s/s and chi(N)N . I/I are also estimated for the TlF, HgF, and YbF molecules [where s (I) is the electron (nuclear) spin and N is the molecular axis]. The best limit on the contact monopole field can be obtained from the measured value of the Tl EDM. The possibility of such a field being produced from polarization of the vacuum of electrically charged magnetic monopoles (dyons) by a Coulomb field is discussed, as well as the limit on these dyons. An alternative mechanism involves chromomagnetic and chromoelectric fields in QCD. C1 HARVARD UNIV,ITAMP,CAMBRIDGE,MA 02138. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP Flambaum, VV (reprint author), UNIV NEW S WALES,SCH PHYS,SYDNEY,NSW 2052,AUSTRALIA. NR 37 TC 4 Z9 4 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 1997 VL 55 IS 3 BP 1736 EP 1742 DI 10.1103/PhysRevA.55.1736 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA WN174 UT WOS:A1997WN17400027 ER PT J AU You, L Hoston, W Lewenstein, M AF You, L Hoston, W Lewenstein, M TI Low-energy excitations of trapped Bose condensates SO PHYSICAL REVIEW A LA English DT Article ID EINSTEIN CONDENSATION; ATOMS; GAS AB We use the Bogoliubov-Hartree theory to describe low-energy excitations of trapped Bose condensates. We construct the quasiparticle spectrum and the quasiparticle operators explicitly in terms of the bare atomic operators. Our results reveal interesting properties of spatially confined Bose condensates and are in excellent agreement with recent experiments. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOL PHYS, CAMBRIDGE, MA 02138 USA. MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. CTR ETUD SACLAY, SPAM, DRECAM, DSM, COMMISSARIAT ENERGIE ATOM, F-91191 GIF SUR YVETTE, FRANCE. RI Lewenstein, Maciej/I-1337-2014 OI Lewenstein, Maciej/0000-0002-0210-7800 NR 25 TC 70 Z9 70 U1 0 U2 5 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 MAR PY 1997 VL 55 IS 3 BP R1581 EP R1584 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA WN174 UT WOS:A1997WN17400006 ER PT J AU deQueiroz, K Good, DA AF deQueiroz, K Good, DA TI Phenetic clustering in biology: A critique SO QUARTERLY REVIEW OF BIOLOGY LA English DT Review ID INFERRING EVOLUTIONARY TREES; ESTIMATED PHYLOGENETIC TREES; NEIGHBOR-JOINING METHOD; NUCLEIC-ACID SEQUENCES; GENE-FREQUENCY DATA; SPATIAL AUTOCORRELATION; NATURAL-POPULATIONS; DISTANCE MATRICES; MAXIMUM-PARSIMONY; CHARACTER CONCEPT AB Phenetic clustering, the forming of hierarchical nonoverlapping groups strictly according to degree of similarity, has serious shortcomings as it is commonly used in biology. When used as a method for estimating phylogeny, phenetic clustering rests on a questionable assumption of correspondence between similarity and recency of common ancestry. This compromises its ability to reconstruct the correct branching sequence when rates of evolutionary divergence are unequal among lineages, as well as causing it to obscure rate differences even when the branching sequences is reconstructed correctly. When used as a method for analysing patterns for geographic variation and genetic continuity among populations, phenetic clustering rests on a questionable assumption of correspondence between similarity and degree of genetic continuity. This compromises its ability to identify genetically continuous units when their component populations are differentiated, and combined with its sensitivity to uneven geographic sampling, it can cause the method to yield misleading results if sampling patterns are not taken into consideration. Finally, even when used simply as a method for analysing patterns of similarity without regard to causal processes, phenetic clustering rests on a questionable assumption of nested hierarchical structure. This compromises its ability to represent similarity relationships accurately when those relationships exhibit a significant nonhierarchical component. For all of the common biological applications of phenetic clustering, there exist alternative analytical methods that do not suffer from the problems associated with phenetic clustering. The problems in question result not from the phenetic (similarity) data themselves, which often can be analysed in more appropriate ways, but from the phenetic clustering as well as the advantages of alternative methods have been known for many years. Advocacy of phenetic clustering at the expense of more appropriate methods can be explained as the result of constraints imposed by an implicit assumption of nested hierarchies that was part of the taxonomic context within which the methods were developed. C1 LOUISIANA STATE UNIV, MUSEUM NAT SCI, BATON ROUGE, LA 70803 USA. RP deQueiroz, K (reprint author), SMITHSONIAN INST, MUSEUM NATL HIST NAT, DEPT VERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. NR 171 TC 88 Z9 92 U1 0 U2 10 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0033-5770 EI 1539-7718 J9 Q REV BIOL JI Q. Rev. Biol. PD MAR PY 1997 VL 72 IS 1 BP 3 EP 30 DI 10.1086/419656 PG 28 WC Biology SC Life Sciences & Biomedicine - Other Topics GA WM696 UT WOS:A1997WM69600001 ER PT J AU Perez, M Reagon, BJ AF Perez, M Reagon, BJ TI Interview with Bernice Johnson Reagon SO RADICAL HISTORY REVIEW LA English DT Editorial Material RP Perez, M (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0163-6545 J9 RADICAL HIST REV JI Radic. Hist. Rev. PD SPR PY 1997 IS 68 BP 4 EP 24 PG 21 WC History SC History GA WV182 UT WOS:A1997WV18200001 ER PT J AU Lassalle, YM Perez, M AF Lassalle, YM Perez, M TI ''Virtually'' Puerto Rican: ''Dis''-locating Puerto Rican-ness and its privileged sites of production SO RADICAL HISTORY REVIEW LA English DT Article ID IDENTITY C1 SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560. RP Lassalle, YM (reprint author), CUNY BOROUGH MANHATTAN COMMUNITY COLL,NEW YORK,NY 10007, USA. NR 53 TC 2 Z9 2 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0163-6545 J9 RADICAL HIST REV JI Radic. Hist. Rev. PD SPR PY 1997 IS 68 BP 54 EP 78 PG 25 WC History SC History GA WV182 UT WOS:A1997WV18200003 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Associations unlimited. SO RQ LA English DT Database Review RP Kalfatovic, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER LIBRARY ASSN PI CHICAGO PA 50 E HURON ST, CHICAGO, IL 60611 SN 0033-7072 J9 RQ JI RQ PD SPR PY 1997 VL 36 IS 3 BP 441 EP 442 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA WZ982 UT WOS:A1997WZ98200015 ER PT J AU Ward, DC AF Ward, DC TI 'Love Again': Larkin and obscenity SO SEWANEE REVIEW LA English DT Article RP Ward, DC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU UNIV SOUTH PI SEWANEE PA SEWANEE REVIEW, SEWANEE, TN 37375 SN 0037-3052 J9 SEWANEE REV JI Sewanee Rev. PD SPR PY 1997 VL 105 IS 2 BP 227 EP 243 PG 17 WC Literary Reviews SC Literature GA XG737 UT WOS:A1997XG73700031 ER PT J AU Donahue, RA Dobson, AK Baliunas, SL AF Donahue, RA Dobson, AK Baliunas, SL TI Stellar active region evolution .1. Estimated lifetimes of chromospheric active regions and active region complexes SO SOLAR PHYSICS LA English DT Article ID MAIN-SEQUENCE STARS; CA-II H; K-EMISSION; DIFFERENTIAL ROTATION; MAGNETIC ACTIVITY; TIME-SERIES; SOLAR; FLUXES AB The lifetimes of chromospheric active regions and active region complexes ('active longitudes') for 35 lower-Main-Sequence stars observed at Mount Wilson Observatory are estimated from the relative distribution of pooled variance at different time scales. The time scale of active region evolution (i.e., the lifetime of large active regions) is approximately 50 days, while the lifetime of active region complexes is on the order of 1 year. These estimates can be used to clarify the contribution of active regions to variance in short-term (i.e., < 1 yr) time series data. Previously unpublished mean rotation periods are documented for several stars. C1 MT WILSON INST,PASADENA,CA 91106. WHITMAN COLL,DEPT ASTRON,WALLA WALLA,WA 99362. TENNESSEE STATE UNIV,CTR AUTOMATED SPACE SCI,NASHVILLE,TN 37203. TENNESSEE STATE UNIV,CTR EXCELLENCE INFORMAT SYST,NASHVILLE,TN 37203. RP Donahue, RA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 24 TC 22 Z9 22 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAR PY 1997 VL 171 IS 1 BP 191 EP 209 DI 10.1023/A:1004902307998 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WT120 UT WOS:A1997WT12000013 ER PT J AU Donahue, RA Dobson, AK Baliunas, SL AF Donahue, RA Dobson, AK Baliunas, SL TI Stellar active region evolution .2. Identification and evolution of variance morphologies in Ca II H+K time series SO SOLAR PHYSICS LA English DT Article ID MAIN-SEQUENCE STARS; EMISSION-LINE FLUXES; K-EMISSION; CHROMOSPHERIC VARIATIONS; DIFFERENTIAL ROTATION; H-EMISSION AB The relative distribution of pooled variance computed at various time scales for records of chromospheric activity has been calculated for approximately 100 stars observed at Mount Wilson Observatory. As shown in Paper I, analysis of the pooled variance provides a technique for estimating the lifetimes of stellar active regions and their influence on chromospheric time series used for determining rotation and activity cycle periods. Pooled variance diagrams may be divided into three morphological types which depend to a large extent on a star's mean level of chromospheric activity (i.e., age) and B - V color (i.e., mass), and possibly depend on star's evolutionary state. C1 MT WILSON INST,PASADENA,CA 91106. WHITMAN COLL,DEPT ASTRON,WALLA WALLA,WA 99362. TENNESSEE STATE UNIV,CTR AUTOMATED SPACE SCI,NASHVILLE,TN 37203. TENNESSEE STATE UNIV,CTR EXCELLENCE INFORMAT SYST,NASHVILLE,TN 37203. RP Donahue, RA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 14 Z9 14 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAR PY 1997 VL 171 IS 1 BP 211 EP 220 DI 10.1023/A:1004922323928 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WT120 UT WOS:A1997WT12000014 ER PT J AU Zumbado, MA Thompson, FC AF Zumbado, MA Thompson, FC TI New species of Sterphus (Diptera: Syrphidae) in Costa Rica with notes on other species existing in Costa Rica SO SOUTHWESTERN ENTOMOLOGIST LA Spanish DT Article AB Sterphus rufoabdominalis and gamezi are described. A new key to the species of Sterphus is given. Distribution notes are given for other Costa Rican species. C1 SMITHSONIAN INST,SYSTEMAT ENTOMOL LAB,USDA ARS,WASHINGTON,DC 20560. RP Zumbado, MA (reprint author), INST NACL BIODIVERSIDAD,DEPT ENTOMOL,AP 22-3100,SANTO DOMINGO,HEREDIA,COSTA RICA. NR 10 TC 4 Z9 5 U1 0 U2 0 PU SOUTHWESTERN ENTOMOLOGICAL SOC PI DALLAS PA 17360 COIT RD, DALLAS, TX 75252-6599 SN 0147-1724 J9 SOUTHWEST ENTOMOL JI Southw. Entomol. PD MAR PY 1997 VL 22 IS 1 BP 79 EP 90 PG 12 WC Entomology SC Entomology GA WU328 UT WOS:A1997WU32800008 ER PT J AU Berlocher, SH Swofford, DL AF Berlocher, SH Swofford, DL TI Searching for phylogenetic trees under the frequency parsimony criterion: An approximation using generalized parsimony SO SYSTEMATIC BIOLOGY LA English DT Editorial Material ID EVOLUTIONARY C1 SMITHSONIAN INST,MRC 534,MSC,LAB MOL SYSTEMAT,WASHINGTON,DC 20540. RP Berlocher, SH (reprint author), UNIV ILLINOIS,DEPT ENTOMOL,320 MORRILL HALL,505 S GOODWIN AVE,URBANA,IL 61801, USA. NR 14 TC 51 Z9 54 U1 0 U2 2 PU SOC SYSTEMATIC BIOLOGISTS PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY NHB 163, WASHINGTON, DC 20560 SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD MAR PY 1997 VL 46 IS 1 BP 211 EP 215 DI 10.2307/2413645 PG 5 WC Evolutionary Biology SC Evolutionary Biology GA WZ110 UT WOS:A1997WZ11000011 PM 11975353 ER PT J AU Lopez, JV Stephens, JC OBrien, SJ AF Lopez, JV Stephens, JC OBrien, SJ TI The long and short of nuclear mitochondrial DNA (Numt) lineages SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter C1 NCI,LAG GEN DIVERS,FREDERICK,MD 21702. RP Lopez, JV (reprint author), SMITHSONIAN TROP RES INST,NAOS MARINE LAB,UNIT 0948,APO,AA 34002, USA. RI Lopez, Jose/F-8809-2011 OI Lopez, Jose/0000-0002-1637-4125 NR 11 TC 3 Z9 3 U1 1 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD MAR PY 1997 VL 12 IS 3 BP 114 EP 114 DI 10.1016/S0169-5347(97)84925-7 PG 1 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA WJ600 UT WOS:A1997WJ60000017 PM 21238001 ER PT J AU Seidensticker, J AF Seidensticker, J TI Saving the tiger SO WILDLIFE SOCIETY BULLETIN LA English DT Article DE Asia; conservation; endangered species; Panthera tigris; tiger ID POPULATION RP Seidensticker, J (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 56 TC 15 Z9 17 U1 3 U2 13 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 SN 0091-7648 J9 WILDLIFE SOC B JI Wildl. Soc. Bull. PD SPR PY 1997 VL 25 IS 1 BP 6 EP 17 PG 12 WC Biodiversity Conservation SC Biodiversity & Conservation GA XA822 UT WOS:A1997XA82200004 ER PT J AU Wheeler, JW Nyalley, L Davis, DM Weldon, PJ AF Wheeler, JW Nyalley, L Davis, DM Weldon, PJ TI Additional sulfur compounds from the anal glands of the striped polecat, Ictonyx striatus (Mustelidae, Mammalia) SO ZEITSCHRIFT FUR NATURFORSCHUNG C-A JOURNAL OF BIOSCIENCES LA English DT Article DE Ictonyx striatus; striped polecat; anal gland secretions; 3-ethyl-1,2-pentanedithiolane; 1,3-pentanedithiol ID SAC SECRETION AB Two sulfur compounds have been identified in the anal gland secretions of captive-raised adults of the striped polecat (Ictonyx striatus), an African mustelid. 3-Ethyl-1,2-pentanedithiolane was observed in the secretions of an adult male and an adult female. 1,3-Pentanedithiol was observed in the male; this compound has not previously been reported from mustelid anal glands. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT SMALL MAMMALS,WASHINGTON,DC 20008. SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. RP Wheeler, JW (reprint author), HOWARD UNIV,DEPT CHEM,WASHINGTON,DC 20059, USA. NR 10 TC 3 Z9 3 U1 0 U2 1 PU VERLAG Z NATURFORSCH PI TUBINGEN PA POSTFACH 2645, W-7400 TUBINGEN, GERMANY SN 0939-5075 J9 Z NATURFORSCH C JI Z.Naturforsch.(C) PD MAR-APR PY 1997 VL 52 IS 3-4 BP 283 EP 285 PG 3 WC Biochemistry & Molecular Biology; Pharmacology & Pharmacy SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy GA WW571 UT WOS:A1997WW57100025 PM 9167280 ER PT J AU McLaughlin, BM Winter, TG McCann, JF AF McLaughlin, BM Winter, TG McCann, JF TI Balmer-alpha emission in proton-hydrogen collisions SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Review ID ION-ATOM COLLISIONS; COUPLED-STATE CALCULATIONS; H+-H COLLISIONS; TRIPLE CENTER APPROXIMATION; DISTORTED-WAVE THEORY; N = 2; ELECTRON-CAPTURE; CHARGE-TRANSFER; CROSS-SECTIONS; SINGLE IONIZATION AB Cross sections for excitation and capture processes into the n = 1, 2, and 3 states (including Balmer-alpha) and ionization have been calculated at intermediate proton collision energies with atomic hydrogen. In addition, the alignment, A(20), and polarization fraction, Pi(E), parameters have been calculated. A multi-state close-coupling approach using a triple-centre basis set together with selective perturbative methods are used to make predictions on Balmer-alpha emission. These results are compared with the available experimental data and various theoretical investigations for fast protons colliding with atomic hydrogen. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. PENN STATE UNIV,DEPT PHYS,LEHMAN,PA 18627. UNIV DURHAM,DEPT PHYS,ATOM & MOL PHYS GRP,DURHAM DH1 3LE,ENGLAND. NR 123 TC 38 Z9 38 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL, ENGLAND BS1 6BE SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD FEB 28 PY 1997 VL 30 IS 4 BP 1043 EP 1059 DI 10.1088/0953-4075/30/4/022 PG 17 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA WM293 UT WOS:A1997WM29300022 ER PT J AU Craddock, RA Crumpler, LS Aubele, JC Zimbelman, JR AF Craddock, RA Crumpler, LS Aubele, JC Zimbelman, JR TI Geology of central Chryse Planitia and the Viking 1 landing site: Implications for the Mars Pathfinder mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN SURFACE; WRINKLE RIDGES; IMPACT BASINS; ORIGIN; MORPHOLOGY; LANDERS; VALLES; RATES AB 1:500,000-scale geologic mapping in the central Chryse Planitia region of Mars was correlated with ''ground-truth'' data gathered by the Viking 1 lander, Materials within the Chryse basin can be subdivided into plains and channel units that are typically separated from one another by gradational contacts. Hesperian Ridged plains materials, unit 1 (Hr(1)) are the oldest materials mapped. Typically, these materials contain numerous fresh impact craters and have sharply defined, mare-like wrinkle ridges similar to those appearing on the lunar maria These materials grade into Hesperian Ridged plains materials, unit 2 (Hr(2)), which are characterized by buried and eroded impact craters and subdued wrinkle ridges, From analyses of crater age dates and their associated geologic contacts, channel materials appear to have formed at the same time as Hr(2) materials, and it is likely both units represent fluvial sediments, Measurements of buried craters contained in Hr(2) materials suggest that in places this unit may he similar to 50 m thick, but crater size-frequency distribution curves suggest that the areal average may be closer to similar to 170 m. Based on these observations, our interpretation is that Hr(2) materials were deposited into a standing body of water during channel formation. This interpretation implies that many of the rocks visible in the Viking 1 lander images were emplaced by fluvial processes. Possibly, finer-grained sediments remained in suspension and were subsequently transported out of Chryse Planitia and into the northern plains during draining of the ponded water. East-west trending surface undulations, visible in lander views toward the south, may represent aeolian dunes, lava flow fronts, or sediment waves formed at the bottom of the standing body of water, Broad physiographic units seen at the surface are not clearly visible in Viking orbiter images; however, they can be projected at the resolution of the orbiter images, These units show that concentrations of drift materials are oriented in a northwesterly direction, contrary to the strongest prevailing wind direction which is toward the northeast, These materials were probably deposited on Ridged plains materials, unit 2, during a period of time when aeolian processes were more active in the region. Both Earth-based radar and Viking thermal data suggest that the Mars Pathfinder landing site will be similar geologically to the Viking 1 site. If this is true, then the Mars Pathfinder mission provides the opportunity for building directly on results of the Viking program. Some of the outstanding questions that Mars Pathfinder may be able to address include determining the aeolian modification history of the Chryse Planitia region, the degree and possibly the relative rate of sediment induration, the fraction of rocks and boulders emplaced by impact processes, the possibility that some materials are the result of in situ weathering, and whether materials were emplaced by fluvial processes and the associated depositional environment. C1 BROWN UNIV,DEPT GEOL SCI,PROVIDENCE,RI 02912. RP Craddock, RA (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,MRC 315,ROOM 3776,WASHINGTON,DC 20560, USA. RI Craddock, Robert/B-3884-2013 NR 75 TC 18 Z9 18 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 25 PY 1997 VL 102 IS E2 BP 4161 EP 4183 DI 10.1029/97JE00058 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA WK420 UT WOS:A1997WK42000016 ER PT J AU Cooper, A Penny, D AF Cooper, A Penny, D TI Mass survival of birds across the Cretaceous-Tertiary boundary: Molecular evidence SO SCIENCE LA English DT Article ID MURINE SARCOMA-VIRUS; MOS PROTO-ONCOGENE; EVOLUTIONARY TREES; EXTINCTION; SEQUENCES; ORIGIN; DIVERSIFICATION; VOLCANISM; MAMMALS; EVENTS AB The extent of terrestrial vertebrate extinctions at the end of the Cretaceous is poorly understood, and estimates have ranged from a mass extinction to limited extinctions of specific groups. Molecular and paleontological data demonstrate that modern bird orders started diverging in the Early Cretaceous; at least 22 avian lineages of modern birds cross the Cretaceous-Tertiary boundary. Data for several other terrestrial vertebrate groups indicate a similar pattern of survival and, taken together, favor incremental changes during a Cretaceous diversification of birds and mammals rather than an explosive radiation in the Early Tertiary. C1 VICTORIA UNIV WELLINGTON,SCH BIOL SCI,WELLINGTON,NEW ZEALAND. SMITHSONIAN INST,NATL ZOOL PK,MOL GENET LAB,WASHINGTON,DC 20008. MASSEY UNIV,SCH BIOL SCI,PALMERSTON NORTH,NEW ZEALAND. RI Penny, David/E-9410-2011; Cooper, Alan/E-8171-2012 OI Cooper, Alan/0000-0002-7738-7851 NR 70 TC 345 Z9 360 U1 0 U2 52 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD FEB 21 PY 1997 VL 275 IS 5303 BP 1109 EP 1113 DI 10.1126/science.275.5303.1109 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WJ503 UT WOS:A1997WJ50300039 PM 9027308 ER PT J AU Clifton, KE AF Clifton, KE TI Mass spawning by green algae on coral reefs SO SCIENCE LA English DT Article ID SEXUAL REPRODUCTION; HALIMEDA BIOHERMS; SEA-URCHIN; DEFENSES; GAMETOGENESIS; COMMUNITIES; CHLOROPHYTA; RECRUITMENT; HERBIVORES; SEDIMENTS AB Predawn episodes of mass spawning by green algae (up to nine species in five genera on a single morning) intermittently cloud Caribbean waters. Species- and sex-specific bouts of anisogamous gamete release occurred synchronously and predictably on a given morning, with closely related species spawning al different times. Algal sexual reproduction was seasonal, but, unlike the mass-spawning behavior of other sessile marine organisms, showed no lunar or tidal cycling. The discovery of mass-spawning behavior by these algae has important implications for future studies of the reproductive ecology and speciation of a vital, yet poorly understood, component of the coral reef community. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. NR 55 TC 89 Z9 94 U1 1 U2 17 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD FEB 21 PY 1997 VL 275 IS 5303 BP 1116 EP 1118 DI 10.1126/science.275.5303.1116 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WJ503 UT WOS:A1997WJ50300041 ER PT J AU Fabbiano, G Juda, JZ AF Fabbiano, G Juda, JZ TI ROSAR observations of the Sombrero galaxy: Discovery of an X-ray active nucleus SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies, active; galaxies, individual (M104); galaxies, nuclei; X-rays, galaxies ID GALACTIC NUCLEI; EMISSION; SPECTRA; QUASARS; ATLAS AB The analysis of a high-resolution X-ray image of NGC 4594, obtained with the ROSAT HRI, shows at least three components of the X-ray emission. The most striking one is a pointlike source associated with the LINER nucleus, with (0.1-2.4) keV L(X) similar to 3.5 x 10(40) ergs s(-1). Comparison of the X-ray, H alpha, and radio emission of this source with those of active galactic nuclei suggests that it may be a low-luminosity version of the latter. If the X-ray emission is due to accretion onto the 5 x 10(8) M. black hole that may be present at the nucleus of NGC 4594, the accretion rates must be very low, since the luminosity is extremely sub-Eddington. Alternatively, the source may be heavily obscured and only reprocessed photons are detected in the ROSAT range. We also detect clumpy emission associated with the disk of NGC 4594, and diffuse (or not resolved) emission from the bulge. With the present data, including a reanalysis of the archival ROSAT PSPC observation of this galaxy, we cannot determine how much of this diffuse emission is due to a hot interstellar medium, and how much is instead due to the integrated emission of a population of evolved stellar sources. RP Fabbiano, G (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 52 TC 31 Z9 31 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1997 VL 476 IS 2 BP 666 EP 676 DI 10.1086/303636 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WH858 UT WOS:A1997WH85800018 ER PT J AU Mattox, JR Wagner, SJ Malkan, M McGlynn, TA Schachter, JF Grove, JE Johnson, WN Kurfess, JD AF Mattox, JR Wagner, SJ Malkan, M McGlynn, TA Schachter, JF Grove, JE Johnson, WN Kurfess, JD TI An intense gamma-ray flare of PKS 1622-297 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, individual (PKS 162 - 297); gamma rays, bursts; gamma rays, observations ID QUASI-STELLAR OBJECTS; EXTRAGALACTIC JETS; OPTICAL CATALOG; ACTIVE GALAXIES; PAIR CASCADES; EMISSION AB We report the observation by the Compton Gamma Ray Observatory of a spectacular flare of radio source PKS 1622-297. A peak flux of (17 +/- 3) x 10(-6) cm(-2) s(-1) (E > 100 MeV) was observed. The corresponding isotropic luminosity is 2.9 x 10(49) ergs s(-1). We find that PKS 1622-297 exhibits gamma-ray intraday variability. A flux increase by a factor of at least 3.6 was observed to occur in less than 7.1 hr (with 99% confidence). Assuming an exponential rise, the corresponding doubling time is less than 3.8 hr. A significant flux decrease by a factor of similar to 2 in 9.7 hr was also observed. Without beaming, the rapid flux change and large isotropic luminosity are inconsistent with the Elliot-Shapiro condition (assuming that gas accretion is the immediate source of power for the gamma-rays). This inconsistency suggests that the gamma-ray emission is beamed. A minimum Doppler factor of 8.1 is implied by the observed lack of pair-production opacity (assuming X-rays are emitted cospatially with the gamma-rays). Simultaneous observation by EGRET and OSSE finds a spectrum adequately fitted by a power law with photon index of -1.9. Although the significance is not sufficient to establish this beyond doubt, the high-energy gamma-ray spectrum appears to evolve from hard to soft as a flare progresses. C1 LANDESSTERNWARTE KONIGSTUHL,D-69117 HEIDELBERG,GERMANY. UNIV CALIF LOS ANGELES,LOS ANGELES,CA 90024. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20701. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. USN,RES LAB,WASHINGTON,DC 20375. RP Mattox, JR (reprint author), BOSTON UNIV,DEPT ASTRON,725 COMMONWEALTH AVE,BOSTON,MA 02215, USA. RI Johnson, Neil/G-3309-2014 NR 43 TC 113 Z9 115 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1997 VL 476 IS 2 BP 692 EP 697 DI 10.1086/303639 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WH858 UT WOS:A1997WH85800021 ER PT J AU Owens, A Denby, M Wells, A Keay, A Graessle, DE Blake, RL AF Owens, A Denby, M Wells, A Keay, A Graessle, DE Blake, RL TI The effect of X-ray absorption fine structure in soft X-ray astronomical telescopes SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation, detectors; space vehicles; telescopes; X-rays, general ID XANES AB Recent in-orbit measurements by high resolution soft X-ray telescopes have revealed low-level fine structure in target spectra that cannot be attributed to a celestial source. Ultimately, this can be traced to the ability of the new high spectral resolution silicon detectors to resolve X-ray absorption fine structure (XAFS) produced in the various detection subsystems. Based on measurements taken at the Daresbury Synchrotron Radiation Source (SRS) and the National Synchrotron Light Source (NSLS), we have modeled the full-up response function of the joint European X-ray Telescope (JET-X), taking into account edge structure generated in the detectors, filters, and mirrors. It is found that unfolding celestial source spectra using a response function in which the detailed edge shapes are calculated from standard absorption cross sections leads to the generation of spectral artifacts at every absorption edge. These in turn produce unacceptably high values of chi(2) in model fits for total source fluxes above similar to 4 x 10(4) counts. For JET-X, this corresponds to a source strength of similar to 0.4 millicrab observed for 10(5) s. Statistically significant ''linelike'' features are introduced into the derived source spectra with amplitudes as great as 10% of the source flux. For JET-X, these features rise above the 3 sigma level for integral source exposures above similar to 5 x 10(4) source counts. The largest. deviations in the residuals arise near 0.5 keV and 2.2 keV and are attributed to XAFS produced in the oxide surface layers of the CCD and the gold reflective surface of the mirrors, respectively. These results are significant for data interpretation tasks with the ASCA, JET-X, XMM, and Advanced X-Ray Astrophysics Facility (AXAF) telescopes. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. LOS ALAMOS NATL LAB,LOS ALAMOS,NM 87545. RP Owens, A (reprint author), UNIV LEICESTER,DEPT PHYS & ASTRON,LEICESTER LE1 7RH,LEICS,ENGLAND. NR 26 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1997 VL 476 IS 2 BP 924 EP 931 DI 10.1086/303628 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WH858 UT WOS:A1997WH85800042 ER PT J AU Park, S Finley, JP Snowden, SL Dame, TM AF Park, S Finley, JP Snowden, SL Dame, TM TI Evidence for an X-ray-emitting galactic bulge: Shadows cast by distant molecular gas SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy, structure; ISM, structure; X-rays, galaxies; X-rays, ISM ID CLOUD; ROSAT; IMAGE; SKY AB A mosaic of seven ROSAT PSPC pointed observations in the direction of (l, b similar to 10 degrees, 0 degrees) reveals deep X-ray shadows in the 0.5-2.0 keV band cast by dense molecular gas. The comparison between the observed on-cloud and off-cloud X-ray fluxes indicates that similar to 43% of the diffuse X-ray background in this direction in both the 0.75 and 1.5 keV bands originates behind the molecular gas, which is located at 2-4 kpc from the Sun. Given the short mean free path of X-rays in the 0.75 keV band in the Galactic plane (similar to 1 kpc assuming an average space density or 1 cm(-1)), this large percentage of the observed flux that originates beyond the molecular gas most likely indicates a strong enhancement in the distribution of X-ray-emitting gas in the Galactic center region, possibly associated with a Galactic X-ray bulge. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Park, S (reprint author), PURDUE UNIV,DEPT PHYS,1396 PHYS BLDG,W LAFAYETTE,IN 47907, USA. NR 31 TC 17 Z9 17 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1997 VL 476 IS 2 BP L77 EP & DI 10.1086/310501 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WH861 UT WOS:A1997WH86100006 ER PT J AU Coddington, JA Hormiga, G Scharff, N AF Coddington, JA Hormiga, G Scharff, N TI Giant female or dwarf male spiders? SO NATURE LA English DT Letter ID SEXUAL DIMORPHISM; ARANEAE; SIZE C1 GEORGE WASHINGTON UNIV,DEPT BIOL SCI,WASHINGTON,DC 20052. UNIV COPENHAGEN,ZOOL MUSEUM,DEPT ENTOMOL,DK-2100 COPENHAGEN,DENMARK. RP Coddington, JA (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560, USA. RI Hormiga, Gustavo/C-3874-2009; Scharff, Nikolaj/A-4787-2013 OI Scharff, Nikolaj/0000-0001-6809-2878 NR 15 TC 80 Z9 82 U1 0 U2 7 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD FEB 20 PY 1997 VL 385 IS 6618 BP 687 EP 688 DI 10.1038/385687a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WJ423 UT WOS:A1997WJ42300028 ER PT J AU Harasewych, MG AF Harasewych, MG TI The life and malacological contributions of R. Tucker Abbott (1919-1995) SO NAUTILUS LA English DT Item About an Individual RP Harasewych, MG (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 1 TC 2 Z9 2 U1 0 U2 0 PU TROPHON CORP PI SILVER SPRING PA 8911 ALTON PARKWAY, SILVER SPRING, MD 20910 SN 0028-1344 J9 NAUTILUS JI Nautilus PD FEB 19 PY 1997 VL 110 IS 2 BP 55 EP 75 PG 21 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA WK299 UT WOS:A1997WK29900004 ER PT J AU Wills, C Condit, R Foster, RB Hubbell, SP AF Wills, C Condit, R Foster, RB Hubbell, SP TI Strong density- and diversity-related effects help to maintain tree species diversity in a neotropical forest SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID TROPICAL TREE; RECRUITMENT; MORTALITY; HYPOTHESIS; DEPENDENCE; COMMUNITY; GROWTH AB Intraspecific density-dependent effects in the Barro Colorado Island (Panama) study area are far stronger, and involve far more species, than previously had been suspected. Significant effects on recruitment, many extremely strong, are seen for 67 out of the 84 most common species in the plot, including the 10 most common. Significant effects on the intrinsic rate of increase are seen in 54 of the 84 species. These effects are far more common than interspecific effects, and are predominantly of the type that should maintain tree diversity. As a result, the more diverse an area in the forest is, the higher is the overall rate of increase of the trees in that area, although sheer crowding has by itself a negative effect. These findings are consistent with, but do not prove, an important role for host-pathogen interactions (defined broadly) in the maintenance of diversity. Ways are suggested by which to test host-pathogen models and competing models. C1 UNIV CALIF SAN DIEGO, CTR MOL GENET, SAN DIEGO, CA 92093 USA. SMITHSONIAN TROP RES INST, PANAMA CITY, PANAMA. FIELD MUSEUM NAT HIST, DEPT BOT, CHICAGO, IL 60605 USA. PRINCETON UNIV, DEPT ECOL & EVOLUT, PRINCETON, NJ 08544 USA. RP Wills, C (reprint author), UNIV CALIF SAN DIEGO, DEPT BIOL, SAN DIEGO, CA 92093 USA. NR 34 TC 194 Z9 208 U1 4 U2 34 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 18 PY 1997 VL 94 IS 4 BP 1252 EP 1257 DI 10.1073/pnas.94.4.1252 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WJ621 UT WOS:A1997WJ62100037 PM 11038601 ER PT J AU Imamura, H Knapp, LW AF Imamura, H Knapp, LW TI A new species of deepwater flathead, Bembras adenensis (Scorpaeniformes: Bembridae) from the western Indian Ocean SO ICHTHYOLOGICAL RESEARCH LA English DT Article DE Bembras adenensis sp. nov; Gulf of Aden; B-japonica AB A new bembrid, Bembras adenensis, is described on the basis of specimens collected from the Gulf of Aden, western Indian Ocean. This species is easily distinguished from B. japonica, the only known congener of the genus, by the following combination of characters: larger orbital diameter, longer head length, pectoral-fin with a small black blotch near tip of upper rays, 3 gill rakers on upper gill arch, 19 pectoral-fin rays, and 15 anal-fin rays (vs. smaller orbital diameter, shorter head length, pectoral-fin with several small spots forming irregular bands, 2 gill rakers on upper gill arch, usually 17 pectoral-fin rays, and 14 anal-fin rays in B. japonica). C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560. RP Imamura, H (reprint author), TOHOKU NATL FISHERIES RES INST,HACHINOHE BRANCH,25-259 SAME,HACHINOHE,AOMORI 031,JAPAN. NR 17 TC 2 Z9 2 U1 0 U2 0 PU ICHTHYOLOGICAL SOC JAPAN PI TOKYO PA BUSINESS CENTER ACADEMIC SOC JAPAN, 5-16-9 HONKOMAGOME, BUNKYO-KU, TOKYO 113, JAPAN SN 1341-8998 J9 ICHTHYOL RES JI Ichthyol. Res. PD FEB 15 PY 1997 VL 44 IS 1 BP 9 EP 14 DI 10.1007/BF02672753 PG 6 WC Zoology SC Zoology GA WV834 UT WOS:A1997WV83400002 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The return of the real: The avant-garde at the end of the century - Foster,H SO LIBRARY JOURNAL LA English DT Book Review 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 SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 1997 VL 122 IS 3 BP 131 EP 131 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA WG362 UT WOS:A1997WG36200042 ER PT J AU Riley, S AF Riley, S TI The Sunday macaroni club - Lopez,S SO LIBRARY JOURNAL LA English DT Book Review 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 SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 1997 VL 122 IS 3 BP 162 EP 162 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA WG362 UT WOS:A1997WG36200221 ER PT J AU Zaldarriaga, M Seljak, U AF Zaldarriaga, M Seljak, U TI All-sky analysis of polarization in the microwave background SO PHYSICAL REVIEW D LA English DT Article ID GRAVITATIONAL-WAVES; ANISOTROPY; RADIATION AB Using the formalism of spin-weighted functions we present an all-sky analysis of polarization in the cosmic microwave background (CMB). Linear polarization is a second-rank symmetric and traceless tensor, which can be decomposed on a sphere into spin +/-2 spherical harmonics. These are the analogues of the spherical harmonics used in the temperature maps and obey the same completeness and orthogonality relations. We show that there exist two linear combinations of spin +/-2 multipole moments which have opposite parities and can be used to fully characterize the statistical properties of polarization in the CMB. Magnetic-type parity combination does not receive contributions from scalar modes and does not cross correlate with either temperature or electric-type parity combination, so there are four different power spectra that fully characterize statistical properties of CMB. We present their explicit expressions for scalar and tensor modes in the form of line of sight integral solution and numerically evaluate them for a representative set of models. These general solutions differ from the expressions obtained previously in the small scale limit both for scalar and tensor modes. A method to generate and analyze all-sky maps of temperature and polarization is given and the optimal estimators for various power spectra and their corresponding variances are discussed. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Zaldarriaga, M (reprint author), MIT,DEPT PHYS,CAMBRIDGE,MA 02139, USA. NR 27 TC 645 Z9 648 U1 3 U2 5 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD FEB 15 PY 1997 VL 55 IS 4 BP 1830 EP 1840 DI 10.1103/PhysRevD.55.1830 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA WK491 UT WOS:A1997WK49100015 ER PT J AU Dashevskaya, EI Nikitin, EE Perales, F Baudon, J AF Dashevskaya, EI Nikitin, EE Perales, F Baudon, J TI Qualitative analysis of the right-left scattering asymmetry in Ne(2p(5)3sP-3(2))+Ar low-energy collisions SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID DIFFERENTIAL CROSS-SECTIONS; POLARIZATION; ORIENTATION; ATOMS; POTENTIALS AB The experimental results on the right-left scattering asymmetry of helicopter-polarized Ne(2p(5)3s(3)P(j)) atoms, either in state \j = 2, m = +2 > or \j = 2, m = -2 > colliding with Ar, are presented and qualitatively interpreted in the framework of the sudden-locking model. It is shown that this model provides a simple description of key features of the cross section difference and the relation between it and the total cross section for scattering of unpolarized atoms. C1 UNIV PARIS 13,PHYS LASERS LAB,CNRS URA 182,F-93430 VILLETANEUSE,FRANCE. TECHNION ISRAEL INST TECHNOL,DEPT CHEM,IL-32000 HAIFA,ISRAEL. RP Dashevskaya, EI (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 16 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL, ENGLAND BS1 6BE SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD FEB 14 PY 1997 VL 30 IS 3 BP 703 EP 711 DI 10.1088/0953-4075/30/3/023 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA WK004 UT WOS:A1997WK00400023 ER PT J AU Colinvaux, P AF Colinvaux, P TI The idea of biodiversity: Philosophies of paradise - Takacs,D SO NATURE LA English DT Book Review RP Colinvaux, P (reprint author), SMITHSONIAN TROP RES INST,BOX 2072,BALBOA,PANAMA. NR 1 TC 1 Z9 1 U1 1 U2 5 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD FEB 13 PY 1997 VL 385 IS 6617 BP 591 EP 592 DI 10.1038/385591a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WH294 UT WOS:A1997WH29400036 ER PT J AU Tucker, DL Oemler, A Kirshner, RP Lin, H Shectman, SA Landy, SD Schechter, PL Muller, V Gottlober, S Einasto, J AF Tucker, DL Oemler, A Kirshner, RP Lin, H Shectman, SA Landy, SD Schechter, PL Muller, V Gottlober, S Einasto, J TI The Las Campanas Redshift Survey galaxy-galaxy autocorrelation function SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies, clusters, general; cosmology, observations; large-scale structure of Universe ID POWER-SPECTRUM; BIAS AB Measurements are presented of the observed redshift-space galaxy-galaxy autocorrelation function, xi(gg)(s), for the Las Campanas Redshift Survey (LCRS). For separations 2.0 1/8L(Sculptor), the luminosity of the Sculptor dSph. We verify this limit by testing the detectability of artificial dSph galaxies placed onto COSMOS/UKST fields. Several of the known dSph companions of the Milky Way are close to the detection limit of our technique, implying that the sample of dSphs is probably complete to the limits of current surveys. (C) 1997 American Astronomical Society. RP Kleyna, JT (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI KURTZ, Michael /B-3890-2009; OI Kenyon, Scott/0000-0003-0214-609X; Kurtz, Michael/0000-0002-6949-0090 NR 13 TC 9 Z9 9 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 1997 VL 113 IS 2 BP 624 EP 633 DI 10.1086/118282 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE934 UT WOS:A1997WE93400015 ER PT J AU Briceno, C Hartmann, LW Stauffer, JR Gagne, M Stern, RA Caillault, JP AF Briceno, C Hartmann, LW Stauffer, JR Gagne, M Stern, RA Caillault, JP TI X-ray surveys and the post-T Tauri problem SO ASTRONOMICAL JOURNAL LA English DT Article ID MAIN-SEQUENCE STARS; AURIGA DARK CLOUDS; ALL-SKY SURVEY; SOLAR NEIGHBORHOOD; MOLECULAR CLOUD; LITHIUM; CLUSTER; DISK AB Recent studies using the ROSAT All-Sky Survey (RASS) towards nearby star-forming regions have identified a widely dispersed population of X-ray active stars, and have suggested that these objects are older pre-main-sequence stars (post-T Tauri stars) located far from molecular clouds. We argue that the majority of these stars are not pre-main-sequence stars, but young main sequence stars of ages up to similar to 10(8) yr. A simple model assuming continuing star formation over the past 10(8) yr quantitatively reproduces the number, surface density, X-ray emission, and optical properties of the RASS sources; Most of these stars are old enough to have dispersed far from their birth sites in molecular clouds, producing a relatively homogeneous spatial distribution of X-ray sources near the galactic plane. We conclude that the RASS results yield little evidence for a post-T Tauri population. We emphasize the importance of recognizing this wide-spread spatial distribution of 10(8) yr stars in searches for possible older weak-emission T Tauri stars among X-ray selected samples in nearby star-forming regions. (C) 1997 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. LOCKHEED MARTIN,SOLAR & ASTROPHYS LAB,PALO ALTO,CA 94304. UNIV GEORGIA,DEPT PHYS & ASTRON,ATHENS,GA 30602. RI Gagne, Marc/C-1130-2013 NR 51 TC 104 Z9 104 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 1997 VL 113 IS 2 BP 740 EP 751 DI 10.1086/118293 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE934 UT WOS:A1997WE93400026 ER PT J AU Evans, NR Sugars, BJA AF Evans, NR Sugars, BJA TI The orbit of the classical Cepheid V350 Sgr SO ASTRONOMICAL JOURNAL LA English DT Article ID RADIAL-VELOCITIES; BINARIES; PERIOD; MASSES AB We have obtained velocities for the binary Cepheid V350 Sgr at the David Dunlap Observatory. An orbit has been derived combining these data with velocities from the literature. The spectral type of B9.0 V has been confirmed from an IUE spectrum, leading to a mass of the companion of 2.5 M.. The uncertainty in the mass is also discussed. (C) 1997 American Astronomical Society. C1 YORK UNIV,N YORK,ON M3J 1P3,CANADA. TORONTO SUN PUBLISHING CORP,TORONTO,ON M5A 3X5,CANADA. RP Evans, NR (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 25 TC 10 Z9 10 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 1997 VL 113 IS 2 BP 792 EP 799 DI 10.1086/118300 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE934 UT WOS:A1997WE93400033 ER PT J AU Trinchieri, G Fabbiano, G Kim, DW AF Trinchieri, G Fabbiano, G Kim, DW TI ROSAT PSPC observations of 5 X-ray bright early type galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: individual: NGC 533; galaxies: individual: NGC 2563; galaxies: individual: NGC 4649; galaxies: individual: NGC 7619; galaxies: individual: NGC 7626; X-rays: galaxies ID SPECTRAL PROPERTIES; POOR CLUSTERS; EMISSION; GAS AB We report on the ROSAT PSPC observations of 5 X-ray bright early-type galaxies. Their X-ray morphology is more complex than Einstein data had shown, ranging from the elipsoidal shape of NGC 533 to the similar to 200 kpc tail of NGC 7619. Hot gas at an average temperature of 0.8-1 keV dominates their X-ray emission. The spectral analysis is based on the assumption of a hot thin plasma at cosmic abundances, since the spectral resolution of the PSPC does not allow unambiguous measures of the model parameters (temperatures, low energy cut-off, metal abundance). However, the estimated temperature are not strongly affected by this choice. A temperature distribution of the hot interstellar medium is also derived. Higher temperatures are in some cases observed at larger radii, while the innermost 1' region is cooler in all of the objects studied. Due to the large range in distances however this corresponds to significantly different galaxy radii, from 5 kpc in NGC 4649 to 30 kpc in NGC 533. The temperature and density distributions derived are used to estimate the total mass of these systems, which span from M(T) similar to 10(12) - 10(13) M. and corresponding mass-to-light ratios M/L similar to 10-150 in solar units. Formal errors on the derived masses are estimated to be > 25%. Care must be taken in comparing results for different systems, since some of the emission attributed to these objects could suffer from the contribution for the groups and clusters they belong to. Accordingly, our mass estimates could reflect the effect of the cluster/group potential. C1 MAX PLANCK INST EXTRATERR PHYS, D-37075 GARCHING, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. CHUNGNAM NATL UNIV, DEPT ASTRON & SPACE SCI, TAEJON 305764, SOUTH KOREA. RP Trinchieri, G (reprint author), OSSERVATORIO ASTON BRERA, VIA BRERA 28, I-20121 MILAN, ITALY. NR 26 TC 52 Z9 52 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 1997 VL 318 IS 2 BP 361 EP 375 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WJ516 UT WOS:A1997WJ51600011 ER PT J AU Hernius, O Lagerkvist, CI Lindgren, M Tancredi, G Williams, GV AF Hernius, O Lagerkvist, CI Lindgren, M Tancredi, G Williams, GV TI UESAC - The Uppsala-ESO survey of asteroids and comets SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE minor planets, asteroids; surveys; solar system:, general AB More than 15 000 positions of moving objects have been detected on 74 plates and films obtained at the European Southern Observatory in Chile and the Anglo-Australian Observatory in Australia during Jupiter's oppositions in 1992 and 1993. Two or more positions have been secured for about 3400 asteroids, and orbits have so far been calculated for about 2500 asteroids. The majority of these asteroids are previously undetected. We present apparent magnitudes for all observed asteroids and absolute magnitudes for those asteroids with orbits. We present model-diameters based on a Monte Carlo approach using the albedo distribution found by the IRAS Minor Planet Survey (Tedesco et al. 1992). Model-diameters are also calculated for the asteroids observed in the Palomar-Leiden Survey of Faint Minor Planets, PLS, (van Houten et al. 1970). Statistics of orbital elements are presented and compared with the results of the PLS. C1 ASTRON OBSERV, S-75220 UPPSALA, SWEDEN. FAC CIENCIAS, DEPT ASTRON, MONTEVIDEO 11200, URUGUAY. INST PLANETARY EXPLORAT DLR, D-10489 BERLIN, GERMANY. SMITHSONIAN ASTROPHYS OBSERV, MINOR PLANET CTR, CAMBRIDGE, MA 02138 USA. OBSERV HELSINGIN YLIOPISTO, FIN-00014 HELSINGIN YLIOPISTO, FINLAND. NR 13 TC 3 Z9 3 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 1997 VL 318 IS 2 BP 631 EP 638 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WJ516 UT WOS:A1997WJ51600038 ER PT J AU Castelli, F Gratton, RG Kurucz, RL AF Castelli, F Gratton, RG Kurucz, RL TI Notes on the convection in the ATLAS9 model atmospheres SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars, atmospheres; stars, fundamental parameters; stars, individual, Procyon; Sun, general; convection ID NEGATIVE HYDROGEN-ION; INFRARED FLUX METHOD; COOL DWARF STARS; EFFECTIVE TEMPERATURES; ANGULAR DIAMETERS; BALMER LINES; SOLAR; CALIBRATION; ABUNDANCES; ABSORPTION AB The mixing-length theory for the convection, as it is used in the ATLAS9 code (Kurucz, 1993a), is summarized and discussed. We investigated the effect of the modification called ''approximate overshooting'' on the model structure of the Sun and of stars with T-eff included between 4000 K and 8500 K, log g included between 2.5 and 4.5, and metallicities [M/H] = 0.0 and [M/H] = -3.0. We found that the Kurucz solar model (SUNK94) with the ''overshooting'' option switched on reproduces more observations than that without ''overshooting''. In the H-gamma, and H-beta regions no solar model is able to reproduce the level of the true continuum deduced from high-resolution observations absolutely calibrated. At 486 nm the computed continuum is about 6.6% higher than that inferred from the observed spectrum. We found that the largest effect of the ''approximate overshooting'' on the model structure occurs for models with T-eff > 6250 K and it decreases with decreasing gravity. The differences in (b - y), (B - V), and (V - K) indices computed from models with the ''overshooting'' option switched on and off, correspond to T-eff differences which may amount up to 180 K, 100 K, 60 K respectively. The differences in T-eff from Balmer profiles may amount up to 340 K and they occur also for T-eff < 6250 K down to about 5000 K. The c(1) index yields gravity . differences Delta log g as a function of log g which, for each T-eff, grow to a maximum value. The maximum a log g decreases with increasing temperatures and ranges, for solar metallicity, from 0.7 dex at log g = 0.5 and T-eff = 5500 K to 0.2 dex at log g = 4.5 and T-eff = 8000 K. This behaviour does not change for [M/H] = -3.0. Comparisons with the observations indicate that model parameters derived with different methods are more consistent when the ''overshooting'' option is switched off (NOVER models), except for the Sun. In particular for Procyon, T-eff and log g from NOVER models are closer to the parameters derived from model independent methods than are T-eff and log g derived from the Kurucz (1995) grids. However, no model is able to explain the whole observed spectrum of either the Sun or Procyon with a unique T-eff, regardless of whether the ''overshooting'' option is switched on or off. Independently of the convection option, the largest differences in T-eff derived with different methods are of the order of 200 K for Procyon and 150 K for the Sun. C1 OSSERV ASTRON TRIESTE, I-34131 TRIESTE, ITALY. OSSERV ASTRON PADOVA, I-35122 PADUA, ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Castelli, F (reprint author), CNR, GRP NAZL ASTRON, VIA G TIEPOLO 11, I-34131 TRIESTE, ITALY. OI Gratton, Raffaele/0000-0003-2195-6805 NR 74 TC 467 Z9 468 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 FEB PY 1997 VL 318 IS 3 BP 841 EP 869 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WL896 UT WOS:A1997WL89600020 ER PT J AU Beaulieu, JP Sasselov, DD Renault, C Grison, P Ferlet, R VidalMadjar, A Maurice, E Prevot, L Aubourg, E Bareyre, P Brehin, S Coutures, C Delabrouille, N deKat, J Gros, M Laurent, B LachiezeRey, M Lesquoy, E Magneville, C Milsztajn, A Moscoso, L Queinnec, F Rich, J Spiro, M Vigroux, L Zylberajch, S Ansari, R Cavalier, F Moniez, M Gry, C Guibert, J Moreau, O Tajhmady, F AF Beaulieu, JP Sasselov, DD Renault, C Grison, P Ferlet, R VidalMadjar, A Maurice, E Prevot, L Aubourg, E Bareyre, P Brehin, S Coutures, C Delabrouille, N deKat, J Gros, M Laurent, B LachiezeRey, M Lesquoy, E Magneville, C Milsztajn, A Moscoso, L Queinnec, F Rich, J Spiro, M Vigroux, L Zylberajch, S Ansari, R Cavalier, F Moniez, M Gry, C Guibert, J Moreau, O Tajhmady, F TI The effect of metallicity on the Cepheid distance scale and its implications for the Hubble constant (H-0) determination SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE stars: cepheids; stars: fundamental parameters; galaxies: distances ID MAGELLANIC CLOUD CEPHEIDS; H-II REGIONS; SPACE-TELESCOPE; SPIRAL GALAXIES; VARIABLES; DISCOVERY; SEARCH; STARS; BAR AB Recent HST determinations of the expansion's rate of the Universe (the Hubble constant, H-0) assumed that the Cepheid Period-Luminosity relation at V and I are independent of metallicity (Freedman, et al., 1996, Saha et al., 1996, Tanvir et al., 1995). The three groups obtain different vales for H-0. We note that most of this discrepancy stems from the asumption (by both groups) that the Period-Luminosity relation is independent of metallicity. We come to this conclusion as a result of our study of the Period-Luminosity relation of 481 Cepheids with 3 millions two colour measurements in the Large Magellanic Cloud and the Small Magellanic Cloud obtained as a byproduct of the EROS microlensing survey. We find that the derived interstellar absorption corrections are particularly sensitive to the metallicity and when our result is applied to recent estimates based on HST Cepheids observations it makes the low-H-0 values higher and the high-H-0 value lower, bringing those discrepant estimates into agrement around H-0 approximate to 70 kms(-1) Mpc(-1). C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. CTR ETUD SACLAY, CEA, DSM, DAPNIA, F-91191 GIF SUR YVETTE, FRANCE. OBSERV MARSEILLE, F-13238 MARSEILLE 03, FRANCE. UNIV PARIS 11, CTR ORSAY, IN2P3, ACCELERATEUR LINEAIRE LAB, F-91405 ORSAY, FRANCE. CNRS, ASTRON SPATIALE LAB, F-13120 MARSEILLE, FRANCE. OBSERV PARIS, CNRS, INST NATL SCI UNIVERS, CTR ANAL IMAGES, F-75014 PARIS, FRANCE. RP Beaulieu, JP (reprint author), INST ASTROPHYS, CNRS, 98BIS BLVD ARAGO, F-75014 PARIS, FRANCE. NR 38 TC 41 Z9 42 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 FEB PY 1997 VL 318 IS 2 BP L47 EP L50 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WJ516 UT WOS:A1997WJ51600004 ER PT J AU Chantell, MC Akerlof, CW Badran, HM Buckley, J CarterLewis, DA Cawley, MF Connaughton, V Fegan, DJ Fleury, P Gaidos, J Hillas, AM Lamb, RC Pare, E Rose, HJ Rovero, AC Sarazin, X Sembroski, G Schubnell, MS Urban, M Weekes, TC Wilson, C AF Chantell, MC Akerlof, CW Badran, HM Buckley, J CarterLewis, DA Cawley, MF Connaughton, V Fegan, DJ Fleury, P Gaidos, J Hillas, AM Lamb, RC Pare, E Rose, HJ Rovero, AC Sarazin, X Sembroski, G Schubnell, MS Urban, M Weekes, TC Wilson, C TI A hybrid version of the Whipple observatory's air Cherenkov imaging camera for use in moonlight SO ASTROPARTICLE PHYSICS LA English DT Article ID GAMMA-RAYS; TEV AB A hybrid version of the Whipple Observatory's atmospheric Cherenkov imaging camera that permits observation during periods of bright moonlight is described. The hybrid camera combines a blue-light blocking filter with the standard Whipple imaging camera to reduce sensitivity to wavelengths greater than 360 nm, Data taken with this camera are found to be foe from the effects of the moonlit night-sky after the application of simple off-line noise filtering. This camera has been used to successfully detect TeV gamma rays, in bright moon light, from both the Crab Nebula and the active galactic nucleus Markarian 421 at the 4.9 sigma and 3.9 sigma levels of statistical significance, respectively, The energy threshold of the camera is estimated to be 1.1 (+0.6/-0.3) TeV from Monte Carlo simulations. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,AMADO,AZ 85645. UNIV MICHIGAN,RANDALL LAB PHYS,ANN ARBOR,MI 48109. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. ECOLE POLYTECH,LPNHE,F-91128 PALAISEAU,FRANCE. CNRS,IN2P3,F-91128 PALAISEAU,FRANCE. PURDUE UNIV,DEPT PHYS,W LAFAYETTE,IN 47907. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. INST ASTRON & FIS ESPACIO,RA-1428 BUENOS AIRES,DF,ARGENTINA. TANTA UNIV,DEPT PHYS,TANTA,EGYPT. IOWA STATE UNIV SCI & TECHNOL,DEPT PHYS & ASTRON,AMES,IA 50011. RP Chantell, MC (reprint author), UNIV CHICAGO,ENRICO FERMI INST,5640 S ELLIS AVE,CHICAGO,IL 60637, USA. NR 12 TC 6 Z9 6 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD FEB PY 1997 VL 6 IS 2 BP 205 EP 214 DI 10.1016/S0927-6505(96)00055-2 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA WJ608 UT WOS:A1997WJ60800008 ER PT J AU Stauffer, JR Balachandran, SC Krishnamurthi, A Pinsonneault, M Terndrup, DM Stern, RA AF Stauffer, JR Balachandran, SC Krishnamurthi, A Pinsonneault, M Terndrup, DM Stern, RA TI Rotational velocities and chromospheric activity of M dwarfs in the Hyades SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations, individual (Hyades); stars, activity; stars, chromospheres; stars, rotation ID LOW-MASS STARS; SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; T-TAURI STARS; EMISSION; EVOLUTION; VARIABILITY; BRAKING AB We have obtained high-resolution spectra of 52 K and M dwarf members of the Hyades open cluster. We have used these spectra to derive radial velocities, rotational velocities, and H alpha equivalent widths. Seven of the stars in our sample are double-lined spectroscopic binaries, and one is a spectroscopic triple. Of the apparently single stars, 13 have rotational velocities above our detection limit of 6 km s(-1) with the maximum rotational velocity being about 25 km s(-1). Given the relatively low mass for these stars, this modest spectroscopic rotational velocity of 25 km s(-1) corresponds to a rotational period of order 17 hr, and thus the most rapidly rotating Hyades M dwarfs actually are quite rapid rotators. Somewhat surprisingly, the components of the spectroscopic binaries are, if anything, on average apparently more slowly rotating than the single stars. Forty-nine of the stars in our sample are M dwarfs. There is a good rotation-activity correlation for this sample, with stars with v sin i > 12 km s(-1) having log (L(X)/L(Bol)) similar to -3 and H alpha equivalent widths saturating at similar to 4 Angstrom. There appear to be two branches of the rotation-activity relation as one approaches saturation, however-one set of stars approaches the saturation level at a very slow rotation rate (v sin i less than or equal to 6 km s(-1)), whereas the second set does not reach saturation until about v sin i = 12 km s(-1). The components of the double-lined spectroscopic binaries are generally members of the first set since they are quite active but generally slowly rotating. C1 UNIV MARYLAND, DEPT ASTRON, COLLEGE PK, MD 20742 USA. OHIO STATE UNIV, DEPT ASTRON, COLUMBUS, OH 43210 USA. LOCKHEED MARTIN SOLAR & ASTROPHYS LAB, PALO ALTO, CA 94304 USA. RP Stauffer, JR (reprint author), SMITHSONIAN ASTROPHYS OBSERV, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 57 TC 56 Z9 56 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP 604 EP 622 DI 10.1086/303567 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE355 UT WOS:A1997WE35500023 ER PT J AU Yang, J Ohashi, N Yan, J Liu, CP Kaifu, N Kimura, H AF Yang, J Ohashi, N Yan, J Liu, CP Kaifu, N Kimura, H TI Detection of infall motion from the circumstellar disk associated with the exciting source of HH 111 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM, individual (HH 111); ISM, jets and outflows ISM, molecules; stars, pre-main-sequence ID HERBIG-HARO OBJECTS; MOLECULAR OUTFLOWS; STELLAR JETS; YOUNG STARS; HL TAURI; HH-111; EMISSION; DUST; GAS; COLLAPSE AB Results from high-resolution interferometric observations toward the exciting source of the highly collimated bipolar jet HH 111 in the CS (2-1) line and 98 GHz continuum are presented. Intense emission in both the line and the continuum has been detected. The continuum emission at 98 GHz is peaked at the VLA source detected by Rodriguez & Reipurth, while the peak of CS emission is shifted 2'' to the west, consistent with the earlier (CO)-C-13 observation by Stapelfeldt & Scoville. Detailed velocity structure of the molecular gas has been revealed under the high velocity resolution of this observation. A molecular disk with an observed extent of similar to 0.04 pc (= 8 x 10(3) AU) and a total Velocity range of 2.9 km s(-1) around the exciting source of HH 111 is identified from both the morphological and the velocity structures of the CS emission. This disk, resolved at different velocity channels, is oriented almost perpendicular to the collimated optical jet and to the previously known bipolar molecular outflow, and its direction of rotation has been determined. The velocity fields of the disk can be explained in terms of both infall and rotation motions in the disk plane. From the comparison between the observed velocity fields and those expected from simple kinematic models that involve both infall and rotation, the observed velocities can be fitted approximately by an infall component parameterized as V-r = -0.5/(r/15'')(1/2) km s(-1) and a lower amplitude rotating component as V-phi = 0.3/(r/15'')(1/2) km s(-1). The disk infall rate deduced from the observed quantities is 6.9 x 10(-6) M(.) yr(-1), comparable to the accretion rate to the central star at the current epoch. The orientation of the molecular disk with respect to the collimated optical jet of HH 111 suggests that the infalling disk is associated with the driving source of HH 111. Additional support of this conclusion comes from the identification of a blueshifted outflow component of CS along the direction of the (CO)-C-12 molecular outflow associated with HH 111. C1 ACAD SINICA,PURPLE MT OBSERV,NANJING 210008,PEOPLES R CHINA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NATL ASTRON OBSERV,MITAKA,TOKYO 181,JAPAN. RP Yang, J (reprint author), NOBEYAMA RADIO OBSERV,MINAMISA KU,NAGANO 38413,JAPAN. NR 34 TC 17 Z9 18 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP 683 EP & DI 10.1086/303558 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE355 UT WOS:A1997WE35500028 ER PT J AU Hartmann, L Cassen, P Kenyon, SJ AF Hartmann, L Cassen, P Kenyon, SJ TI Disk accretion and the stellar birthline SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars, evolution; stars, formation; stars, pre-main-sequence ID T-TAURI STARS; AURIGA MOLECULAR CLOUD; SPECTRAL ENERGY-DISTRIBUTIONS; FU-ORIONIS OBJECTS; EVOLUTION; PROTOSTARS; MODELS; EMISSION AB We present a simplified analysis of some effects of disk accretion on the early evolution of fully convective, low-mass pre-main-sequence stars. Our analysis builds on the previous seminal work of Stahler, but it differs in that the accretion of material occurs over a small area of the stellar surface, such as through a disk or magnetospheric accretion column, so that most of the stellar photosphere is free to radiate to space. This boundary condition is similar to the limiting case considered by Palla & Stahler for intermediate-mass stars. We argue that for a wide variety of disk mass accretion rates, material will be added to the star with relatively small amounts of thermal energy. Protostellar evolution calculated assuming this ''low-temperature'' limit of accretion generally follows the results of Stahler because of the thermostatic nature of deuterium fusion, which prevents protostars from contracting below a ''birthline'' in the H-R diagram. Our calculated protostellar radii tend to fall below Stahler's at higher masses; the additional energy loss from the stellar photosphere in the case of disk accretion tends to make the protostar contract. The low-temperature disk accretion evolutionary tracks never fall below the deuterium-fusion birthline until the internal deuterium is depleted, but protostellar tracks can lie above the birthline in the H-R diagram if the initial radius of the protostellar core is large enough or if rapid disk accretion (such as might occur during FU Ori outbursts) adds significant amounts of thermal energy to the star. These possibilities cannot be ruled out by either theoretical arguments or observational constraints at present, so that individual protostars might evolve along a multiplicity of birthlines with a modest range of luminosity at a given mass. Our results indicate that there are large uncertainties in assigning ages for the youngest stars from H-R diagram positions, given the uncertainty in birthline positions. Our calculations also suggest that the relatively low disk accretion rates characteristic of T Tauri stars below the birthline cause low-mass stars to contract only slightly faster than normal Hayashi track evolution, so that ages for older pre-main-sequence stars estimated from H-R diagram positions are relatively secure. C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. RP Hartmann, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 46 TC 114 Z9 114 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP 770 EP 785 DI 10.1086/303547 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE355 UT WOS:A1997WE35500036 ER PT J AU Keto, E AF Keto, E TI The shapes of cross-correlation interferometers SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation, interferometers ID ALGORITHM AB Cross-correlation imaging interferometers designed in the shape of a curve of constant width offer better sensitivity and imaging characteristics than other designs because they sample the Fourier space of the image better than other shapes, for example, ''T's'' or ''Y's.'' In a doss-correlation interferometer each pair of antennas measures one Fourier component with a spatial wavenumber proportional to the separation of the pair. Placing the individual antennas of the interferometer along a curve of constant width, a curve that has the same diameter in all directions, guarantees that the spatial resolution of the instrument will be independent of direction because the measured Fourier components will have the same maximum spatial wavenumber in all directions. The most uniform sampling within this circular region in Fourier space will be created by the particular symmetric curve of constant width that has the lowest degree of rotational symmetry or fewest number of sides, which is the Reuleaux triangle. The constant width curve with the highest symmetry, the circle is the least satisfactory although still considerably better than T's or Y's. In all cases, the sampling can be further improved by perturbing the antenna locations slightly off a perfect curve to break down symmetries in the antenna pattern which cause symmetries and hence nonuniformities in the sampling pattern in Fourier space. Appropriate patterns of perturbations can be determined numerically. As a numerical problem, optimizing the sampling in Fourier space can be thought of as a generalization of the traveling salesman problem to a continuous two-dimensional space. Self-organizing neural networks which are effective in solving the traveling salesman problem are also effective in generating optimal interferometer shapes. The Smithsonian Astrophysical Observatory's Submillimeter Array, a cross-correlation imaging interferometer for astronomy, will be constructed with a design based on the Reuleaux triangle. C1 SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. RP Keto, E (reprint author), LAWRENCE LIVERMORE NATL LAB, LIVERMORE, CA 94550 USA. NR 16 TC 38 Z9 41 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP 843 EP 852 DI 10.1086/303545 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE355 UT WOS:A1997WE35500044 ER PT J AU Ford, E Kaaret, P Tavani, M Barret, D Bloser, P Grindlay, J Harmon, BA Paciesas, WS Zhang, SN AF Ford, E Kaaret, P Tavani, M Barret, D Bloser, P Grindlay, J Harmon, BA Paciesas, WS Zhang, SN TI Evidence from quasi-periodic oscillations for a millisecond pulsar in the low-mass X-ray binary 4U 0614+091 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars, general; stars, individual (4U 0614+091); stars, neutron; X-rays, stars ID TIMING EXPLORER; GX5-1 AB We have detected quasi-periodic oscillations (QPOs) near 1 kHz from the low-mass X-ray binary 4U 0614+091 in observations with the Rossi X-Ray Timing Explorer. The observations span several months and sample the source over a large range of X-ray luminosity. In every interval, QPOs are present above 400 Hz with fractional rms amplitudes from 3% to 12% over the full Proportional Counter Array energy band, At high count rates, two high-frequency QPOs are detected simultaneously. The difference in their frequency centroids is consistent with a constant value of 323 +/- 4 Hz in all observations. During one interval, a third signal is detected at 328 +/- 2 Hz. This suggests that the system has a stable ''clock'' that is most likely the neutron star with spin period 3.1 ms. Thus, our observations of 4U 0614+091, and those of 4U 1728-34 and KS 1731-260, provide the first evidence for millisecond pulsars within low-mass X-ray binary systems and reveal the ''missing-link'' between millisecond radiopulsars and the late stages of binary evolution in low-mass X-ray binaries. The constant difference in the high-frequency QPOs suggests a beat-frequency interpretation. In this model, the high-frequency QPO is associated with the Keplerian frequency of the inner accretion disk, and the lower frequency QPO is a ''beat'' between the differential rotation frequency of the inner disk and the spinning neutron star. Assuming the high-frequency QPO is a Keplerian orbital frequency for the accretion disk, we find a maximum mass of 1.9 M. and a maximum radius of 17 km for the neutron star. C1 COLUMBIA UNIV, COLUMBIA ASTROPHYS LAB, NEW YORK, NY 10027 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NASA, GEORGE C MARSHALL SPACE FLIGHT CTR, HUNTSVILLE, AL 35812 USA. UNIV ALABAMA, DEPT PHYS, HUNTSVILLE, AL 35899 USA. NASA, GEORGE C MARSHALL SPACE FLIGHT CTR, UNIV SPACE RES ASSOC, HUNTSVILLE, AL 35812 USA. RP Ford, E (reprint author), COLUMBIA UNIV, DEPT PHYS, 538 W 120TH ST, NEW YORK, NY 10027 USA. NR 23 TC 57 Z9 58 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP L123 EP L126 DI 10.1086/310483 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE356 UT WOS:A1997WE35600013 ER PT J AU Kumar, P Quataert, EJ AF Kumar, P Quataert, EJ TI Angular momentum transport by gravity waves and its effect on the rotation of the solar interior SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun, oscillations; Sun, rotation; stars, rotation AB We calculate the excitation of low-frequency gravity waves by turbulent convection in the Sun and the effect of the angular momentum carried by these waves on the rotation profile of the Sun's radiative interior. We find that the gravity waves generated by convection in the Sun provide a very efficient means of coupling the rotation in the radiative interior to that of the convection zone. In a differentially rotating star, waves of different azimuthal number have their frequencies in the local rest frame of the star Doppler shifted by different amounts. This leads to a difference in their local dissipation rate and hence a redistribution of angular momentum in the star. We find that the timescale for establishing uniform rotation throughout much of the radiative interior of the Sun is similar to 10(7) yr, which provides a possible explanation for the helioseismic observations that the solar interior is rotating as a solid body. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Kumar, P (reprint author), INST ADV STUDY,OLDEN LANE,PRINCETON,NJ 08540, USA. NR 8 TC 47 Z9 47 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP L143 EP L146 DI 10.1086/310477 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE356 UT WOS:A1997WE35600018 ER PT J AU LopezCruz, O Yee, HKC Brown, JP Jones, C Forman, W AF LopezCruz, O Yee, HKC Brown, JP Jones, C Forman, W TI Are luminous cD halos formed by the disruption of dwarf galaxies? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, clusters, general; galaxies, elliptical and lenticular, cD; galaxy, formation; galaxy, luminosity functions, mass function; galaxies, photometry ID COMA CLUSTER; RICH CLUSTERS; PHOTOMETRY; EVOLUTION; CORE AB From a total sample of 45 Abell clusters observed by the Einstein X-ray observatory, we present the results on the galaxy luminosity function (LF) for a group of seven clusters that were identified by the morphology of their LFs. The LFs were derived using photometric data to a completeness limit similar to 5.5 mag below M*. We found that a single Schechter function with an average alpha = -1.0 gives a good fit to these individual LFs within the magnitude range. These seven clusters have common properties, which indicate they form a homogeneous class of dynamically evolved clusters that can be characterized by the presence of a dominant cD galaxy, high richness, symmetrical single-peaked X-ray emission, and high gas mass. On the other hand, steep faint-end slopes (-2.0 less than or equal to alpha less than or equal to -1.4) are usually detected in poorer clusters. Our result gives a direct indication that the faint-end slope of the galaxy LF is subject to environmental effects. We propose that the flatness of the faint-end slope in these clusters results from the disruption of a large fraction of dwarf galaxies during the early stages of cluster evolution. The stars and gas from the disrupted galaxies are redistributed throughout the cluster potential during violent relaxation. This heuristic scenario can explain the origin of the luminous halos of cD galaxies and a large fraction of the gas content in the intracluster medium as a by-product. The correlation between the cluster gas mass determined from the modeling of the X-ray emission and the cD halo optical luminosity is presented to support the proposed model. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP LopezCruz, O (reprint author), UNIV TORONTO,DEPT ASTRON,TORONTO,ON M5S 3H8,CANADA. OI Forman, William/0000-0002-9478-1682 NR 34 TC 59 Z9 60 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP L97 EP L101 DI 10.1086/310474 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE356 UT WOS:A1997WE35600007 ER PT J AU Menten, KM Reid, MJ Eckart, A Genzel, R AF Menten, KM Reid, MJ Eckart, A Genzel, R TI The position of Sagittarius A*: Accurate alignment of the radio and infrared reference frames at the galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; galaxies, nuclei; galaxy, center; masers; stars, AGB and post-AGB; stars, mass-loss; stars, variables, other ID SIO MASER EMISSION; ACCRETING BLACK-HOLE; LATE-TYPE STARS; OH IR STARS; VELOCITY DISPERSION; GALAXY; MICRONS; PARSECS; SHELL; MODEL AB We present a novel approach to the long-standing problem of locating the position of the compact nonthermal radio source Sgr A* on infrared images of the Galactic center region. Using the Very Large Array, we have detected SiO and H2O maser emission toward several sources within the central parsec of our Galaxy. These masers arise from the innermost parts of circumstellar envelopes of giant and supergiant stars that are members of the nuclear star cluster and appear as compact infrared sources in a diffraction-limited 2.2 mu m infrared image. One of the SiO masers is associated with the M-type supergiant IRS 7, the most prominent 2.2 mu m point source in the Galactic center region. The radio data allow measurements of the maser positions relative to the compact nonthermal radio continuum source Sgr A* with milliarcsecond accuracy. Because stellar SiO masers near the Galactic center trace their host stars to within a few milliarcseconds, these relative positions can be used to calibrate the plate scale and rotation of the infrared image. Our method allows registration of the radio relative to the infrared reference frame with an estimated accuracy of 0 ''.03. Using the improved position accuracy we put a stringent upper limit on the 2.2 mu m flux density of Sgr A* that is significantly lower than values predicted by recent theoretical model calculations. C1 MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. RP Menten, KM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 39 TC 118 Z9 120 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP L111 EP & DI 10.1086/310472 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE356 UT WOS:A1997WE35600010 ER PT J AU Schechter, PL Bailyn, CD Barr, R Barvainis, R Becker, CM Bernstein, GM Blakeslee, JP Bus, SJ Dressler, A Falco, EE Fesen, RA Fischer, P Gebhardt, K Harmer, D Hewitt, JN Hjorth, J Hurt, T Jaunsen, AO Mateo, M Mehlert, D Richstone, DO Sparke, LS Thorstensen, JR Tonry, JL Wegner, G Willmarth, DW Worthey, G AF Schechter, PL Bailyn, CD Barr, R Barvainis, R Becker, CM Bernstein, GM Blakeslee, JP Bus, SJ Dressler, A Falco, EE Fesen, RA Fischer, P Gebhardt, K Harmer, D Hewitt, JN Hjorth, J Hurt, T Jaunsen, AO Mateo, M Mehlert, D Richstone, DO Sparke, LS Thorstensen, JR Tonry, JL Wegner, G Willmarth, DW Worthey, G TI The quadruple gravitational lens PG 1115+080: Time delays and models SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, observations; dark matter; distance scale; galaxies, distances and redshifts; gravitational lensing; quasars, individual (PG 1115+080) ID TRIPLE QUASAR; GALAXY AB Optical photometry is presented for the quadruple gravitational lens PG 1115+080. A preliminary reduction of data taken from 1995 November to 1996 June gives component C leading component B by 23.7 +/- 3.4 days and components Al and A2 by 9.4 days. A range of models has been fitted to the image positions, none of which gives an adequate fit. The best-fitting and most physically plausible of these, taking the lensing galaxy and the associated group of galaxies to be singular isothermal spheres, gives a Hubble constant of 42 km s(-1) Mpc(-1) for Omega = 1, with an observational uncertainty of 14%, as computed from the B - C time delay measurement. Taking the lensing galaxy to have an approximately E5 isothermal mass distribution yields H-0 = 64 km s(-1) Mpc(-1), while taking the galaxy to be a point mass gives H-0 = 84 km s(-1) Mpc(-1). The former gives a particularly bad fit to the position of the lensing galaxy, while the latter is inconsistent with measurements of nearby galaxy rotation curves. Constraints on these and other possible models are expected to improve with planned Hubble Space Telescope observations. C1 YALE UNIV,DEPT ASTRON,NEW HAVEN,CT 06520. MICHIGAN DARTMOUTH MIT OBSERV HC 04,TUCSON,AZ. MIT,HAYSTACK OBSERV,WESTFORD,MA 01886. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. MIT,DEPT EARTH ATMOSPHER & PLANETARY SCI,CAMBRIDGE,MA 02139. CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. HARVARD UNIV,SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. DARTMOUTH COLL,DEPT PHYS & ASTRON,HANOVER,NH 03755. NATL OPT ASTRON OBSERV,TUCSON,AZ 85726. UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106. NORDIC OPT TELESCOPE,E-38700 CANARY ISL,SPAIN. UNIV STERNWARTE MUENCHEN,D-81679 MUNICH,GERMANY. UNIV WISCONSIN,WASHBURN OBSERV,MADISON,WI 53706. RP Schechter, PL (reprint author), MIT,DEPT PHYS,CAMBRIDGE,MA 02139, USA. RI Hjorth, Jens/M-5787-2014; OI Hjorth, Jens/0000-0002-4571-2306; Blakeslee, John/0000-0002-5213-3548 NR 24 TC 84 Z9 84 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1997 VL 475 IS 2 BP L85 EP L88 DI 10.1086/310478 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE356 UT WOS:A1997WE35600004 ER PT J AU Stutchbury, BJM Piper, WH Neudorf, DL Tarof, SA Rhymer, JM Fuller, G Fleischer, RC AF Stutchbury, BJM Piper, WH Neudorf, DL Tarof, SA Rhymer, JM Fuller, G Fleischer, RC TI Correlates of extra-pair fertilization success in hooded warblers SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Wilsonia citrina; DNA fingerprinting; extra-pair fertilizations; mating system; sexual selection ID RED-WINGED BLACKBIRDS; REPRODUCTIVE SUCCESS; SEXUAL SELECTION; TREE SWALLOWS; BREEDING SYNCHRONY; FEMALE BIRDS; HIGH-QUALITY; MATE CHOICE; COPULATIONS; PATERNITY AB We examined correlates of extra-pair fertilization (EPF) success in the hooded warbler (Wilsonia citrina), a species where females pursue extra-pair matings. The good genes hypothesis predicts that females choose extra-pair mates with morphological or behavioral traits that reflect differences in male genetic quality. EPFs were common, as 35.3% (42/119) of broods contained extra-pair young (EPY) and 26.7% (95/356) of nestlings were the result of EPFs. There was a strong skew in male EPF success which increased the variance in annual male mating success 2-3 fold. However, male morphology did not predict EPF success, as extra-pair males were not older or larger than the males they cuckolded. Likewise, there were no significant correlations between the proportion of extra-pair young in a brood and male size or age. The good genes hypothesis predicts that high-duality males will be consistently preferred as genetic mates, but the number of young sired by a male with his social mate was not consistent from one year to the next, There was a significant negative correlation between female age and proportion of EPY produced, which could result if older females obtain higher-quality social mates. We found no strong evidence that females choose extra-pair mates for good genes, but females may use behavioral rather than morphological cues to assess relative male quality. C1 SMITHSONIAN INST,NATL ZOOL PK,GENET MOL LAB,WASHINGTON,DC 20008. RP Stutchbury, BJM (reprint author), YORK UNIV,DEPT BIOL,4700 KEELE ST,N YORK,ON M3J 1P3,CANADA. RI Piper, Walter/B-7908-2009 NR 46 TC 87 Z9 87 U1 4 U2 18 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD FEB PY 1997 VL 40 IS 2 BP 119 EP 126 DI 10.1007/s002650050324 PG 8 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA WL909 UT WOS:A1997WL90900008 ER PT J AU Tennyson, J AF Tennyson, J TI Phase factors in electron-molecule collision calculations SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article DE electron-molecule collisions; configuration interaction; R-matrix ID R-MATRIX METHOD; EXCITATION; HEH+; HYDROGEN AB At low impact energies, high quality electron-molecule collision calculations require target correlated wavefunctions representing several electronic states. Target correlation is usually introduced via a configuration interaction (CI) expansion. This approach introduces phase factors in coefficients of the target CI expansion between the N electron target calculation and the N + 1 electron scattering calculation. A method requiring rediagonalisation of the target calculation for each scattering symmetry was used (Orel et al., Phys Rev A 44 (1991) 4328) and widely copied. It is suggested that while this method accounts for the most serious phase problems, for certain calculations residual phase inconsistencies can arise. It is shown that the phase factors actually arise from different ordering of spin-orbitals in the N and N + 1 electron calculations. An alternative method based on the analysis of the electron configurations used in the scattering calculation is proposed. This method resolves all phase ambiguities and removes the need for redundant rediagonalisations of the target Hamiltonian. The price of this method is the need to understand in detail the algorithm used for generating antisymmetrised configurations. Implementation of this method as part of the UK molecular R-matrix codes which are based on the ALCHEMY package is discussed. C1 UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. RP Tennyson, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOL PHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Tennyson, Jonathan/I-2222-2012 OI Tennyson, Jonathan/0000-0002-4994-5238 NR 18 TC 16 Z9 16 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD FEB PY 1997 VL 100 IS 1-2 BP 26 EP 30 DI 10.1016/S0010-4655(96)00144-0 PG 5 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA WH798 UT WOS:A1997WH79800003 ER PT J AU Dove, CJ AF Dove, CJ TI Quantification of microscopic feather characters used in the identification of North American plovers SO CONDOR LA English DT Article DE plumulaceous; feathers; microcharacters; variation; Charadrius AB Variation in microscopic characters of plumulaceous barbs of six species of Charadrius was studied to quantify characters and test differences among taxa. Pluvialis squatarola was used for intergeneric comparisons. Intraspecific variation in feathers from the sternopectoral tract of C. vociferus was examined to define character parameters and to determine within-vane variation and vane symmetry. A significant difference was observed among the barbs of four regions within each vane of the same :Feather, but barbs from opposing vanes were not significantly different from one another Interspecific variation then was studied using discriminant function analysis. Pluvialis separated from all species of Charadrius. Two subgroups were apparent within Charadrius: semipalmatus, vociferus and montanus separated from wilsonia, alexandrinus and melodus. RP Dove, CJ (reprint author), NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 27 TC 17 Z9 23 U1 0 U2 3 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0010-5422 J9 CONDOR JI Condor PD FEB PY 1997 VL 99 IS 1 BP 47 EP 57 DI 10.2307/1370223 PG 11 WC Ornithology SC Zoology GA WP122 UT WOS:A1997WP12200006 ER PT J AU Snyder, NFR Derrickson, SR Beissinger, SR Wiley, JW Smith, TB Toone, WD Miller, B AF Snyder, NFR Derrickson, SR Beissinger, SR Wiley, JW Smith, TB Toone, WD Miller, B TI Captive breeding and conservation SO CONSERVATION BIOLOGY LA English DT Letter ID COLLECTION C1 NATL ZOOL PK, CONSERVAT & RES CTR, FRONT ROYAL, VA 22630 USA. YALE UNIV, SCH FORESTRY & ENVIRONM STUDIES, NEW HAVEN, CT 06511 USA. GRAMBLING STATE UNIV, GRAMBLING COOPERAT WILDLIFE PROJECT, GRAMBLING, LA 71245 USA. SAN FRANCISCO STATE UNIV, DEPT BIOL, SAN FRANCISCO, CA 94132 USA. SAN DIEGO WILD ANIM PK, ESCONDIDO, CA 92027 USA. Univ Nacl Autonoma Mexico, INST BIOL, CHAMELA RES STN, MELAQUE 48980, JALISCO, MEXICO. RP Snyder, NFR (reprint author), WILDLIFE PRESERVAT TRUST INT, POB 426, PORTAL, AZ 85632 USA. RI Beissinger, Steven/F-3809-2012 NR 12 TC 1 Z9 1 U1 1 U2 6 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 1997 VL 11 IS 1 BP 3 EP 5 PG 3 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA WJ111 UT WOS:A1997WJ11100003 ER PT J AU Steneck, RS Macintyre, IG Reid, RP AF Steneck, RS Macintyre, IG Reid, RP TI A unique algal ridge system in the Exuma Cays, Bahamas SO CORAL REEFS LA English DT Article ID TAXONOMIC REASSESSMENT; CORALLINACEAE; RHODOPHYTA; STROMATOLITES; HYDROLITHON; MORPHOLOGY; CARBONATE; REEFS AB An algal ridge system discovered along the Exuma Gays, Bahamas constructs bioherms to a thickness of at least 1.5 m and is associated with modern intertidal stromatolites. These algal ridges are unique because they grow in atypical environments characterized by relatively low wave energy, high rates of sedimentation and low rates of herbivory. They also are composed primarily of the branching crustose coralline alga, Neogoniolithon strictum, which heretofore was not known to form algal ridges. Lateral growth rates of crusts, vertical growth rates of branches and survivorship of transplanted N. strictum were greatest in the shallow fore reef zone of the algal ridge. The alga is also capable of surviving and growing when covered with sediment for at least 100 days. Under such conditions it transforms from a branched to an unbranched morphology. Parrotfish grazing, which is said to limit the abundance of branched corallines and algal ridges, was two orders of magnitude lower than in published accounts from other reef systems of the Caribbean and one order of magnitude less than that found on nearby coral reefs of the west Exuma Sound. Neogoniolithon strictum, a delicate and open-branched coralline, persisted for over a year without grazing damage when transplanted to a depth of 2.3 m. This algal ridge-building coralline becomes a well-indurated limestone following submarine lithification of sediment that infills the open branch framework. As a result, N. strictum ridges are comparable to the dense frameworks associated with most algal ridges. Observations of N. strictum -associated bioherms along Central America suggest this ridge system may exist elsewhere under conditions similar to those described for the Bahamas. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,MRC 125,DEPT PALEOBIOL,WASHINGTON,DC 20560. UNIV MIAMI,ROSENSTIEL SCH MARINE & ATMOSPHER SCI,MIAMI,FL 33149. RP Steneck, RS (reprint author), UNIV MAINE,DARLING MARINE CTR,DEPT OCEANOG,WALPOLE,ME 04573, USA. NR 34 TC 37 Z9 38 U1 0 U2 4 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD FEB PY 1997 VL 16 IS 1 BP 29 EP 37 DI 10.1007/s003380050056 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA WM144 UT WOS:A1997WM14400005 ER PT J AU Littler, MM Littler, DS Brooks, BL Koven, JF AF Littler, MM Littler, DS Brooks, BL Koven, JF TI A unique coral reef formation discovered on the Great Astrolabe Reef, Fiji SO CORAL REEFS LA English DT Article ID COMPETITION AB A spectacular mound-like reef formation (126 m in circumference, 10 m high) dominated by highly arched and record-size colonies of the unattached mushroom coral Halomitra pileus, along with 17 other species of the family Fungiidae, occurs in 31 m of water on the sedimentary lagoon floor of the Great Astrolabe Reef, Fiji. Core samples show radiocarbon dates which indicate that the formation hypothetically began building similar to 4500 y ago, with a calculated mean accretion rate of 2.2 mm . y(-1). The majority of fossil and living material is contributed by H. pileus colonies between 40-70 cm mean diameter, with some individuals up to 1.5 m in diameter. The size, fungiid diversity, and geological history of the bioherm is unprecedented and represents the first example of a coral reef constructed almost entirely by Fungiidae. RP Littler, MM (reprint author), SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT BOT,WASHINGTON,DC 20560, USA. NR 17 TC 16 Z9 16 U1 0 U2 3 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD FEB PY 1997 VL 16 IS 1 BP 51 EP 54 DI 10.1007/s003380050059 PG 4 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA WM144 UT WOS:A1997WM14400008 ER PT J AU Ricklefs, RE AF Ricklefs, RE TI Comparative demography of new world populations of thrushes (Turdus spp) SO ECOLOGICAL MONOGRAPHS LA English DT Article DE age ratios; birds; demography; fecundity; latitudinal gradients; life history; survival rate; Turdus thrushes ID DELAYED PLUMAGE MATURATION; PASSERINE BIRDS; SURVIVAL RATES; ECOLOGICAL CONSTRAINTS; REPRODUCTIVE EFFORT; EUROPEAN BIRDS; FOREST BIRDS; CLUTCH SIZE; EVOLUTION; HISTORY AB This analysis uses information obtained primarily from museum collections to estimate demographic parameters of populations of thrushes (Turdus spp.) from throughout the Western Hemisphere. Adult survival rates were estimated from the proportions of individuals >1 yr old in museum collections, assuming constant population size, discrete reproductive seasons, unbiased collecting, and maturity at 1 yr old. The effects of relaxing each of these assumptions were examined. The resulting biases were found to be small compared to differences between populations, and in several cases, they were opposite to the conventional wisdom that survival rate increases towards the equator. The annual survival rate of adults (S) is estimated without bias by E(S) = A/(A + I), which has a standard error of [(AI)/(A + I)(3)](1/2), where A is the number of adults in a collection and I is the number of immatures. In Turdus, adult and immature birds can be distinguished by the appearance of the secondary coverts, the immature forms of which are retained until the first postnuptial molt at approximate to 1 yr old. The present analysis included 8653 specimens from 30 populations of 19 species from Alaska to southern Patagonia. Additional data tabulated from museum specimens included numbers of juveniles, evidence of breeding, worn plumage, and molt. Estimated annual survival rates varied from a mean of 0.56 in temperate North American populations, to 0.68 in subtropical South American populations, 0.76 in lowland tropical populations, and 0.80 and 0.85 in tropical montane populations in Central and South Amer ica, respectively. Samples of adults and immatures restricted to the period immediately prior to the breeding season gave results that were indistinguishable from samples summed over the entire year. Survival rate was most strongly correlated with the difference between maximum and minimum mean monthly temperatures (r = -0.84). Thus, survival is inversely related to seasonality of temperature. An index to fecundity (J) was estimated by the frequency of juvenile specimens (generally <2 mo old) relative to those of adults in museum collections. This index was inversely related to annual adult survival. A relative index of prereproductive (generally Ist-yr) survival (S-a) was calculated as the annual adult mortality [1 - E(S)] divided by J. Estimated S,was independent of estimated S. Calculations of annual fecundity (F) from field studies on breeding of selected species supported both of these observations. These results, which are consistent with conclusions based upon broader comparisons among birds, suggest several hypotheses: (1) adult survival in Turdus populations is determined by physical conditions during the nonbreeding season, particularly various ecological effects of low temperature; (2) fecundity is sensitive to density-dependent feedbacks from adult population size and, possibly, to environmental factors correlated with other factors that independently affect adult survival; and (3) Ist-yr survival, age at maturity, or both, also are affected by density-dependent factors. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP Ricklefs, RE (reprint author), UNIV MISSOURI,DEPT BIOL,8001 NAT BRIDGE RD,ST LOUIS,MO 63121, USA. NR 82 TC 78 Z9 82 U1 2 U2 14 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 0012-9615 J9 ECOL MONOGR JI Ecol. Monogr. PD FEB PY 1997 VL 67 IS 1 BP 23 EP 43 DI 10.1890/0012-9615(1997)067[0023:CDONWP]2.0.CO;2 PG 21 WC Ecology SC Environmental Sciences & Ecology GA WH237 UT WOS:A1997WH23700002 ER PT J AU McCoy, TJ Keil, K Clayton, RN Mayeda, TK Bogard, DD Garrison, DH Wieler, R AF McCoy, TJ Keil, K Clayton, RN Mayeda, TK Bogard, DD Garrison, DH Wieler, R TI A petrologic and isotopic study of lodranites: Evidence for early formation as partial melt residues from heterogeneous precursors SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID FE-TI OXIDES; ORDINARY CHONDRITES; ACAPULCO METEORITE; COSMOGENIC NUCLIDES; IRON-METEORITES; OXYGEN ISOTOPES; EQUILIBRIA; MINERALOGY; OLIVINE; CLASSIFICATION AB We have conducted petrologic, chemical, and isotopic studies of lodranites in an attempt to constrain their genesis. Lodran, Gibson, Y-791491, Y-791493, Y-74357, Y-8002, Y-75274, MAC 88177, LEW 88280, EET 84302, FRO 90011, and QUE 93148 are classified as lodranites. Lodranites and acapulcoites are indistinguishable on the basis of oxygen isotopic compositions but are distinct in average grain sizes of their mafic silicates, with lodranites being significantly coarser-grained. Lodranites exhibit a diverse range of petrologic and mineralogic features: they range widely in mafic silicate compositions (Fa(3-13)), plagioclase (0-11.4 vol%), Fe,Ni metal (0.5-20 vol%), and troilite (0.2-5.3 vol%) contents; and shock levels (S1-S4). They appear to have experienced high peak temperatures and rapid cooling in the temperature range recorded by metallographic cooling rates (i.e., 700-350 degrees C). The only dated lodranite, Gibson, cooled to Ar closure temperatures at 4.49 +/- 0.01 Ga. Lodranites formed from chemically and isotopically heterogeneous precursors in which the mineral and oxygen isotopic compositions were correlated. Heating of their parent body to temperatures between similar to 1050-1200 degrees C resulted in formation of Fe,Ni-FeS and basaltic partial melts. Depletions of troilite and/or plagioclase in most lodranites testify to the removal of some of these partial melts, although melt migration was complex. Lodranites appear to have experienced a complex cooling history of slow cooling at high temperatures, followed by rapid cooling at intermediate temperatures, possibly related to breakup of the parent body. Lodranites were liberated from their parent body during 1-3 impact events, with most having cosmic ray exposure ages of 5.5-7 Ma. The acapulcoites are samples from the same parent body but were heated to lower temperatures and, thus, experienced lower degrees of partial melting. Copyright (C) 1997 Elsevier Science Ltd. C1 UNIV HAWAII MANOA, SCH OCEAN & EARTH SCI & TECHNOL, HAWAII INST GEOPHYS & PLANETOL, HONOLULU, HI 96822 USA. NASA, LYNDON B JOHNSON SPACE CTR, HOUSTON, TX 77058 USA. UNIV CHICAGO, ENRICO FERMI INST, CHICAGO, IL 60637 USA. ETH ZURICH, CH-8092 ZURICH, SWITZERLAND. RP McCoy, TJ (reprint author), SMITHSONIAN INST, DEPT MINERAL SCI, MRC 119, WASHINGTON, DC 20560 USA. RI Wieler, Rainer/A-1355-2010 OI Wieler, Rainer/0000-0001-5666-7494 NR 69 TC 87 Z9 89 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 FEB PY 1997 VL 61 IS 3 BP 623 EP 637 DI 10.1016/S0016-7037(96)00359-6 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA WK514 UT WOS:A1997WK51400011 ER PT J AU McCoy, TJ Keil, K Muenow, DW Wilson, L AF McCoy, TJ Keil, K Muenow, DW Wilson, L TI Partial melting and melt migration in the acapulcoite-lodranite parent body SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID DIFFERENTIATED ASTEROIDS; EXPLOSIVE VOLCANISM; UREILITE METEORITES; CHONDRITES; ORIGIN AB We review petrologic evidence that the acapulcoites and lodranites formed by <1 vol% to probably >20 vol% whole rock partial melting of a chondritic precursor material. At low degrees of partial melting, only Fe,Ni-FeS cotectic melting occurred. Migration distances for partial melts were short, resulting in the formation of acapulcoites with essentially chondritic troilite and plagioclase contents, but achondritic textures. At high degrees of partial melting, both Fe,Ni-FeS and basaltic (plagioclase-pyroxene) partial melts formed, and the melts may have migrated out of the source rock. The partial melt residues, which are more or less depleted in Fe,Ni-FeS and plagioclase, are the lodranites. Melt migration was complex: most acapulcoites, which experienced relatively low degrees of partial melting, lost little if any of the partial melt. One acapulcoite, LEW 86220, represents a unique case in which Fe,Ni-FeS and basaltic partial melts appear to have migrated from a lodranite source region into a cooler acapulcoite region, where they were trapped. In cases of the relatively high degrees of partial melting experienced by lodranites, melts may have been partly, selectively, or totally removed from the rocks, and Fe,Ni-FeS and/or basaltic partial melts may have been removed to different degrees and may, in fact, have been trapped on occasion in greater than chondritic proportions. We model vein and dike formation and melt migration by calculating the excess pressures and vein and dike sizes for varying degrees of partial melting. Our calculations are broadly consistent with observations, indicating that melt migration is inefficient at low degrees of partial melting and extremely efficient at high degrees of partial melting. Although the size of the acapulcoite-lodranite parent body and the volatile contents of the chondritic precursor rocks are poorly constrained, the lack of basaltic rocks in the world's meteorite collections complementary to the lodranites suggests that basaltic partial melts may have been accelerated off the body by explosive volcanism of the type envisioned by Wilson and Keil (1991) and ejected into space. The diversity of rocks from the acapulcoite-lodranite parent body may provide a basis for better understanding the diverse range of spectral subtypes recognized among the S-type asteroids. Copyright (C) 1997 Elsevier Science Ltd. C1 UNIV HAWAII MANOA,SCH OCEAN & EARTH SCI & TECHNOL,HAWAII INST GEOPHYS & PLANETOL,HONOLULU,HI 96822. NASA,LYNDON B JOHNSON SPACE CTR,HOUSTON,TX 77058. UNIV HAWAII MANOA,DEPT CHEM,HONOLULU,HI 96822. UNIV LANCASTER,INST ENVIRONM & BIOL SCI,DIV ENVIRONM SCI,LANCASTER LA1 4YQ,ENGLAND. RP McCoy, TJ (reprint author), SMITHSONIAN INST,DEPT MINERAL SCI,MRC 119,WASHINGTON,DC 20560, USA. NR 40 TC 88 Z9 88 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD FEB PY 1997 VL 61 IS 3 BP 639 EP 650 DI 10.1016/S0016-7037(96)00365-1 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA WK514 UT WOS:A1997WK51400012 ER PT J AU French, BM Koeberl, C Gilmour, I Shirey, SB Dons, JA Naterstad, J AF French, BM Koeberl, C Gilmour, I Shirey, SB Dons, JA Naterstad, J TI The Gardnos impact structure, Norway: Petrology and geochemistry of target rocks and impactites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID OSMIUM ISOTOPE SYSTEMATICS; SOUTHERN-NORWAY; TERRESTRIAL IMPACT; SHOCK METAMORPHISM; GEOMETRIC MODEL; VREDEFORT DOME; CRATER; AFRICA; RIES; METEORITES AB The Gardnos structure, Norway is an approximately circular area of anomalously fractured and brecciated rock, about 4.5 km in diameter, emplaced in a metamorphic terrane composed chiefly of granitic gneisses with minor amphibolite and quartzite. The original recognition of Gardnos as a deeply eroded impact structure between 900 and 406 Ma old has been followed up by detailed petrographic and chemical studies of approximately thirty samples of target rocks and various types of shocked rocks (impactites). Deep erosion of the structure has erased the original rim, removed much of the crater-fill deposits, and exposed large areas at or near the original crater floor. However, a wide variety of distinctive impactites -fractured and blackened quartzites in the sub-crater basement rocks, lithic breccias, and melt-bearing breccias-are still preserved. These impactites show petrographic and chemical characteristics that confirm an impact origin: distinctive Planar Deformation Features (PDFs) in quartz and feldspar, incipient melting of feldspar clasts in the melt-bearing breccias, close matches between the chemical composition of the breccias and mixtures of the target lithologies, and the detection of an extraterrestrial component. A minor extraterrestrial component (less than or equal to 0.15%) was detected in the melt-bearing breccias, based on significantly elevated Ir and Os contents and lower Os-187/Os-188 ratios compared to those in the target rocks. The Gardnos impactites are significantly enriched in C (5-10X) over the exposed target rocks. This may reflect the presence of a C-rich shale overlying the metamorphic basement at the time of impact; this idea is supported by delta(13)C values of -28.1 to -31.5 parts per thousand measured in the impactites. Mixing calculations show that the chemical compositions of the impactites can be reproduced by mixtures of target rocks ranging from approximately 60-90 wt% granite gneiss, 0-30 wt% amphibolite, 0-12 wt% quartzite, and 3-19 wt% of a C-rich shale component. The deeply eroded state of the structure and the preliminary state of detailed geologic mapping make crater reconstruction difficult. One possible scenario involves the impact of a 300 m diameter stony meteorite that released 10(19) J of energy and formed a transient cavity 3 km in diameter that evolved to a complex crater 5 km in diameter with a central uplift of about 350 m. The original crater was filled with at least 0.3 km(3) of allochthonous melt-matrix breccias containing about 0.06 km(3) of impact melt. The structure underwent low-grade (greenschist?) metamorphism in Caledonian time (about 400 Ma ago) and was subsequently eroded to its present appearance. The value of the Gardnos structure for further cratering studies lies in its easy access to large areas of the original crater floor zone, in the preservation of a possibly complete sequence of crater-fill breccias beneath a cap of elastic sediments, and in the unusual carbon enrichment of its impactites. Copyright (C) 1997 Elsevier Science Ltd. C1 UNIV VIENNA,INST GEOCHEM,A-1090 VIENNA,AUSTRIA. OPEN UNIV,PLANETARY SCI RES INST,MILTON KEYNES MK7 6AA,BUCKS,ENGLAND. CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,WASHINGTON,DC 20015. UNIV OSLO,GEOL MUSEUM,N-0562 OSLO,NORWAY. RP French, BM (reprint author), SMITHSONIAN INST,MRC-119,WASHINGTON,DC 20560, USA. OI Gilmour, Iain/0000-0002-2860-9489 NR 87 TC 58 Z9 58 U1 2 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD FEB PY 1997 VL 61 IS 4 BP 873 EP 904 DI 10.1016/S0016-7037(96)00382-1 PG 32 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA WN031 UT WOS:A1997WN03100015 ER PT J AU Zimbelman, JR AF Zimbelman, JR TI Planetary geology SO GEOTIMES LA English DT Article C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,REG PLANETARY IMAGE FACIL,WASHINGTON,DC 20560. GEOL SOC AMER,PLANETARY GEOL DIV,BOULDER,CO 80301. RP Zimbelman, JR (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 SN 0016-8556 J9 GEOTIMES JI Geotimes PD FEB PY 1997 VL 42 IS 2 BP 23 EP 24 PG 2 WC Geosciences, Multidisciplinary SC Geology GA WF545 UT WOS:A1997WF54500027 ER PT J AU Ball, AS Drake, BG AF Ball, AS Drake, BG TI Short-term decomposition of litter produced by plants grown in ambient and elevated atmospheric CO2 concentrations SO GLOBAL CHANGE BIOLOGY LA English DT Article DE carbon dioxide enrichment; climate change; plant litter; decomposition; soil respiration; tidal marsh ecosystem ID CARBON-DIOXIDE CONCENTRATION; LEAF LITTER; SOIL; RESPIRATION; NITROGEN; DYNAMICS; FORESTS; INSITU; LEAVES AB The effects of elevated atmospheric CO2 (ambient + 340 mu mol mol(-1)) on above-ground litter decomposition were investigated over a 6-week period using a field-based mesocosm system. Soil respiratory activity in mesocosms incubated in ambient and elevated atmospheric CO2 concentrations were not significantly different (t-test, P > 0.05) indicating that there were no direct effects of elevated atmospheric CO2 on litter decomposition. A study of the indirect effects of CO2 on soil respiration showed that soil mesocosms to which naturally senescent plant litter had been added (0.5% w/w) from the C-3 sedge Scirpus olneyi grown in elevated atmospheric CO2 was reduced by an average of 17% throughout the study when compared to soil mesocosms to which litter from Scirpus olneyi grown in ambient conditions had been added. In contrast, similar experiments using senescent material from the C-4 grass Spartina patens showed no difference in soil respiration rates between mesocosms to which litter from plants grown in elevated or ambient CO2 conditions had been added. Analysis of the C:N ratio and lignin content of the senescent material showed that, while the C:N ratio and lignin content of the Spartina patens litter did not vary with atmospheric CO2 conditions, the C:N ratio (but not the lignin content) of the litter from Scirpus olneyi was significantly greater (t-test; P < 0.05) when derived from plants grown under elevated CO2 (105:1 compared to 86:1 for litter derived from Scirpus olneyi grown under ambient conditions). The results suggest that the increased C:N ratio of the litter from the C-3 plant Scirpus olneyi grown under elevated CO2 led to the lower rates of biodegradation observed as reduced soil respiration in the mesocosms. Further longterm experiments are now required to determine the effects of elevated CO2 on C partitioning in terrestrial ecosystems. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 26 TC 33 Z9 35 U1 2 U2 16 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 1354-1013 J9 GLOB CHANGE BIOL JI Glob. Change Biol. PD FEB PY 1997 VL 3 IS 1 BP 29 EP 35 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA WG661 UT WOS:A1997WG66100004 ER PT J AU Vandiver, PB AF Vandiver, PB TI Jomon of Japan: The world's oldest pottery - Kendrick,DM SO JOURNAL OF ASIAN STUDIES LA English DT Book Review RP Vandiver, PB (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU ASSN ASIAN STUDIES INC PI ANN ARBOR PA UNIV MICH 1 LANE HALL, ANN ARBOR, MI 48109 SN 0021-9118 J9 J ASIAN STUD JI J. Asian Stud. PD FEB PY 1997 VL 56 IS 1 BP 210 EP 211 DI 10.2307/2646390 PG 2 WC Area Studies; Asian Studies SC Area Studies; Asian Studies GA XA937 UT WOS:A1997XA93700054 ER PT J AU Ralls, K Eberhardt, LL AF Ralls, K Eberhardt, LL TI Assessment of abundance of San Joaquin kit foxes by spotlight surveys SO JOURNAL OF MAMMALOGY LA English DT Article DE Vulpes macrotis mutica; kit fox; spotlighting; surveys AB Biologists of the California Department of Fish and Game have conducted quarterly spotlight surveys of San Joaquin kit foxes, Vulpes macrotis mutica, and potential species of prey along seven 48-km routes since 1970. The annual reproductive cycle of the foxes was reflected by a seasonal cycle in the counts. Counts of foxes during surveys in June were correlated with total precipitation during the previous rainfall season, but not with concurrent counts of prey. Number of foxes seen/0.8-km interval was more highly correlated with estimated sighting distance based on physical features, such as hills and plains, than with current vegetation density or type. Mean number of foxes counted per survey per route ranged from two to 20. Counts of foxes increased over time on one route, decreased over time on another, and showed a curvilinear trend on two routes. The average number of foxes seen over all routes did not show any long-term trend. However, small samples, missing data, and lack of replication limited statistical analysis and interpretation of surveys. Statistical tests on simulated data similar to the data collected during the surveys indicated that larger samples, which could be obtained by replication, would be needed to detect changes in the population of foxes with any efficiency (statistical power). An expanded spotlight-survey program of kit foxes, with additional routes and replicated surveys, could be used to monitor population trends throughout the range of this endangered subspecies. RP Ralls, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 19 TC 33 Z9 35 U1 2 U2 10 PU AMER SOC MAMMALOGISTS PI PROVO PA BRIGHAM YOUNG UNIV, DEPT OF ZOOLOGY, PROVO, UT 84602 SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD FEB PY 1997 VL 78 IS 1 BP 65 EP 73 DI 10.2307/1382639 PG 9 WC Zoology SC Zoology GA WK300 UT WOS:A1997WK30000007 ER PT J AU Frati, F Simon, C Sullivan, J Swofford, DL AF Frati, F Simon, C Sullivan, J Swofford, DL TI Evolution of the mitochondrial cytochrome oxidase II gene in collembola SO JOURNAL OF MOLECULAR EVOLUTION LA English DT Article DE collembola; mtDNA; cytochrome c oxidase subunit II; among-site rate variation; A + T bias; phylogeny; likelihood models ID C-OXIDASE; NUCLEOTIDE-SEQUENCE; DNA-SEQUENCES; ORGANIZATION; GENOME; PHYLOGENY; RATES; TREES; CODE; IDENTIFICATION AB The sequence of the mitochondrial COII gene has been widely used to estimate phylogenetic relationships at different taxomonic levels across insects. We investigated the molecular evolution of the COII gene and its usefulness for reconstructing phylogenetic relationships within and among four collembolan families. The collembolan COII gene showed the lowest A + T content of all insects so far examined, confirming that the well-known A + T bias in insect mitochondrial genes tends to increase from the basal to apical orders. Fifty-seven percent of all nucleotide positions were variable and most of the third codon positions appeared free to vary, Values of genetic distance between congeneric species and between families were remarkably high; in some cases the latter were higher than divergence values between other orders of insects, The remarkably high divergence levels observed here provide evidence that collembolan taxa are quite old; divergence levels among collembolan families equaled or exceeded divergences among pterygote insect orders. Once the saturated third-codon positions (which violated stationarity of base frequencies) were removed, the COII sequences contained phylogenetic information, but the extent of that information was overestimated by parsimony methods relative to likelihood methods, In the phylogenetic analysis, consistent statistical support was obtained for the monophyly of all four genera examined, but relationships among genera/families were not well supported. Within the genus Orchesella, relationships were well resolved and agreed with allozyme data. Within the genus Isotomurus, although three pairs of populations were consistently identified, these appeared to have arisen in a burst of evolution from an earlier ancestor, Isotomurus italicus always appeared as basal and I. palustris appeared to harbor a cryptic species; corroborating allozyme data. C1 UNIV CONNECTICUT,DEPT ECOL & EVOLUTIONARY BIOL,STORRS,CT 06269. SMITHSONIAN INST,LAB MOL SYSTEMAT,WASHINGTON,DC 20560. RP Frati, F (reprint author), UNIV SIENA,DIPARTIMENTO BIOL EVOLUT,VIA PA MATTIOLI 4,I-53100 SIENA,ITALY. NR 73 TC 151 Z9 163 U1 0 U2 12 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0022-2844 J9 J MOL EVOL JI J. Mol. Evol. PD FEB PY 1997 VL 44 IS 2 BP 145 EP 158 DI 10.1007/PL00006131 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA WF652 UT WOS:A1997WF65200004 PM 9069175 ER PT J AU Aponte, NE Ballantine, DL Norris, JN AF Aponte, NE Ballantine, DL Norris, JN TI Aglaothamnion halliae comb nov and A-collinsii sp. nov (Ceramiales, Rhodophyta): Resolution of nomenclatural and taxonomic confusion SO JOURNAL OF PHYCOLOGY LA English DT Article DE Aglaothamnion; Callithamnion; Ceramiaceae; Ceramiales; Rhodophyta; western Atlantic ID LIFE-HISTORY AB Specimens from the exsiccatae Phycotheca Boreali-Americana number 698 are shown to represent two distinct species. One of them, formerly known as Callithamnion halliae, is transferred to Aglaothamnion on the basis of its uninucleate cells. The specimens exhibit distichous branching and are ecorticate. A lectotype is proposed for one of the P.B.-A #698 specimens displaying these characters. Aglaothamnion halliae (Collins) comb. nov. is an earlier name for Aglaothamnion westbrookiae Rueness et L'Hardy-Halos. The second species, together with specimens of P.B.-A. #1896, has radial branching and corticated axes and is described herein as a new species, Aglaothamnion collinsii. The binomial Aglaothamnion boergesenii (Aponte et Ballantine) L'Hardy-Halos et Rueness in Aponte, Ballantine, et J. Norris is validated. A key to the tropical and warm-temperate western Atlantic species of Aglaothamnion is presented. C1 SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT BOT,WASHINGTON,DC 20560. RP Aponte, NE (reprint author), UNIV PUERTO RICO,DEPT MARINE SCI,POB 5000,MAYAGUEZ,PR 00681, USA. NR 46 TC 7 Z9 11 U1 1 U2 3 PU PHYCOLOGICAL SOC AMER INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 1997 VL 33 IS 1 BP 81 EP 87 DI 10.1111/j.0022-3646.1997.00081.x PG 7 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA WL640 UT WOS:A1997WL64000012 ER PT J AU He, FL Legendre, P LaFrankie, JV AF He, FL Legendre, P LaFrankie, JV TI Distribution patterns of tree species in a Malaysian tropical rain forest SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Donnelly statistic; Pasoh Forest; spatial pattern; species diversity ID JANZEN-CONNELL MODEL; SPATIAL PATTERN; DIVERSITY; COMPETITION; COEXISTENCE; MORTALITY; SURVIVAL; GAPS AB Spatial patterns of tree species were studied in a 50-ha tropical rain forest plot in the Pasoh forest, Malaysia. This forest is characterized by a high diversity and very high number of rare species. Out of the 745 species occurring with > five individuals, 80.4% had an aggregated distribution, 19.5% were randomly distributed and one species had a regular distribution. The spatial patterns of rare vs. common species, juvenile vs. adult trees, and coarse vs. fine scales were compared. Rare species are generally less aggregated than common ones and most of the randomly distributed species are rare. Spatial patterns shift from high clumping to looser intensity or random distribution when moving from juveniles to adults for the same species. No adult tree species display a regular pattern, however. Regular distributions were rarely found; this is probably due to intraspecific competition at a local scale. There is a negative correlation between per capita death rate and population density. This study suggests that the Pasoh forest and its high diversity are subjected to multiple controlling factors, e.g., topography, spacing effect, density-dependent processes and species rarity. The importance of any factor changes across spatial and temporal scales. C1 UNIV MONTREAL,DEPT SCI BIOL,MONTREAL,PQ H3C 3J7,CANADA. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 42 TC 154 Z9 226 U1 9 U2 42 PU OPULUS PRESS UPPSALA AB PI UPPSALA PA BOX 25137, S 752 25 UPPSALA, SWEDEN SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD FEB PY 1997 VL 8 IS 1 BP 105 EP 114 PG 10 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA XC688 UT WOS:A1997XC68800014 ER PT J AU Guinot, D Jamieson, BGM Tudge, CC AF Guinot, D Jamieson, BGM Tudge, CC TI Ultrastructure and relationships of spermatozoa of the freshwater crabs Potamon fluviatile and Potamon ibericum (Crustacea, Brachyura, Potamidae) SO JOURNAL OF ZOOLOGY LA English DT Article ID FIDDLER-CRAB; DECAPODA; SPERM; HETEROTREMATA; ACROSOME; ACTIN AB The spermatozoa of Potamon fluviatile and P. ibericum are virtually indistinguishable and do not support separate subgeneric rank (Potamon and Pontipotamon, respectively). Synapomorphic with the spermatozoa of the South African freshwater crab Potamonautes perlatus sidneyi are the elongation of the two centrioles and disposition of the centrioles almost parallel to each other, unknown elsewhere in the Brachyura, and reduction of the thickened ring (homoplasic with grapsids and gecarcinids). Other, probably synapomorphic, similarities of Potamon and Potamonautes include the wide inner acrosome zone, absence of a definite acrosome ray zone (homoplasic in other families) and the cleistospermial spermatophores. Further similarities, of questionable polarity, are the simple, not multilaminar, nuclear membrane and the tendency of the nuclear arms to wrap around the nucleus. Differences of Potamon From Potamonautes, which possibly support their present generic separation and give weak support to their former separate familial placement in the Potamidae and Potamonautidae respectively, are perforation of the operculum and the weak, rather than strong, development of a periopercular rim. Absence in Potamon and Potamonautes of an accessory opercular ring and a xanthid ring separates them from xanthids. No close affinities with other heterotreme families are seen but their assignment to the Heterotremata is not in doubt. Their spermatozoa lack two of the distinctive features of thoracotreme spermatozoa (apical button on the operculum and concentric lamellation of the outer acrosome zone). No clear correlates of spermatozoon structure with a freshwater existence are recognizable but reduction of the thickened ring possibly relates to peculiarities of the acrosome reaction. However, the production of spermatophores with single spermatozoa (cleistospermia) is possibly a device to prevent polyspermy and wastage of the small number of lecithotrophic eggs produced in potamids. C1 UNIV QUEENSLAND, DEPT ZOOL, BRISBANE, QLD 4072, AUSTRALIA. NATL MUSEUM NAT HIST, DEPT INVERTEBRATE ZOOL, SMITHSONIAN INST, WASHINGTON, DC 20560 USA. RP Guinot, D (reprint author), MUSEUM NATL HIST NAT, LAB ZOOL ARTHROPODES, 61 RUE BUFFON, F-75231 PARIS 05, FRANCE. NR 51 TC 14 Z9 14 U1 2 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0952-8369 J9 J ZOOL JI J. Zool. PD FEB PY 1997 VL 241 BP 229 EP 244 PN 2 PG 16 WC Zoology SC Zoology GA XF766 UT WOS:A1997XF76600002 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The fate of a gesture: Jackson Pollock and postwar American art - Ratcliff,C SO LIBRARY JOURNAL LA English DT Book Review 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 SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 1 PY 1997 VL 122 IS 2 BP 78 EP 78 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA WD907 UT WOS:A1997WD90700065 ER PT J AU Wood, TC Montali, RJ Wildt, DE AF Wood, TC Montali, RJ Wildt, DE TI Follicle-oocyte atresia and temporal taphonomy in cold-stored domestic cat ovaries SO MOLECULAR REPRODUCTION AND DEVELOPMENT LA English DT Article DE follicle; atresia; oocyte; egg; IVM; cat; taphonomy ID MEIOTIC MATURATION; CIRCULATING HORMONES; MAMMALIAN OOCYTES; SEXUAL-BEHAVIOR; INVITRO; FERTILIZATION; MORPHOLOGY; CULTURE; GROWTH AB In vitro oocyte maturation followed by in vitro fertilization (IVM/IVF) success in the domestic cat remains inferior to commonly studied livestock or laboratory species. The objectives here were [1) to histologically assess atresia status of freshly excised follicle/oocyte complexes, and (2) to evaluate taphonomic change (deterioration after excision) of these complexes after ovarian cold storage for up to 48 h. After excision of 50 ovarian pairs, one ovary was preserved immediately and the other stored in phosphate buffered saline (4 degrees C for 4, 8, 12, 24, or 48 h before fixation and examination. Ovals were classified as luteal if prominent corpora lutea (CL) were present or as follicular if antral follicles and no CL were present. Two classes of follicle-oocyte complexes (preantral and antral) were microscopically evaluated. Of the 2,280 complexes examined, 64.3% demonstrated clear evidence of slight to severe degeneration, with various stages being described and photographed for the first lime. There was no histological evidence indicating distinctive morphological[ differences between oocytes recovered from follicular Versus luteal donors. Storage of whole ovaries in cold saline inhibited taphonomic changes for 48 h after excision, in summary,there is marked variability in the number and quality of follicle populations in cat ovaries. A high percentage of full-sized follicular oocytes are under going atresia at any given time. However additional gross degeneration as a result of cold-storage appears modest for up to 48 h. Nonetheless, this high level of natural atresia in the cat likely contributes to comparatively lower IVM/IVF success than in other species. (C) 1997 Wiley-Liss, inc. C1 SMITHSONIAN INST, CONSERVAT & RES CTR, NATL ZOOL PK, FRONT ROYAL, VA 22630 USA. SMITHSONIAN INST, CONSERVAT & RES CTR, NATL ZOOL PK, WASHINGTON, DC 20560 USA. GEORGE MASON UNIV, DEPT BIOL, FAIRFAX, VA 22030 USA. NR 41 TC 60 Z9 62 U1 3 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1040-452X J9 MOL REPROD DEV JI Mol. Reprod. Dev. PD FEB PY 1997 VL 46 IS 2 BP 190 EP 200 DI 10.1002/(SICI)1098-2795(199702)46:2<190::AID-MRD9>3.0.CO;2-L PG 11 WC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology SC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology GA WE370 UT WOS:A1997WE37000009 PM 9021750 ER PT J AU Saar, SH Osten, RA AF Saar, SH Osten, RA TI Rotation, turbulence and evidence for magnetic fields in southern dwarfs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE convection; turbulence; stars, late-type; stars, magnetic fields; stars, rotation ID SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; II K-LINE; STELLAR ROTATION; VELOCITIES; SPECTRA; MACROTURBULENCE; EMISSION AB We model high-resolution spectra using a simple radiative transfer analysis to derive projected rotational velocities (v sin i) and macroturbulent velocity dispersions (v(mac)) for 49 southern dwarf stars (including many first-ever measurements). We compare our results with previous values, and estimate rotation periods (P-rot) and sin i values where possible. We confirm that v(mac) generally decreases with decreasing temperature for T-eff greater than or equal to 5000 K. Magnetically active stars tend to show enhanced values of v(mac). This may be due to a difference in the mean stellar convective properties, a change in the mean stellar temperature structure, or a combination of both. We identify a group of stars that exhibit correlations between the derived velocities and line Lande g(eff) values, implying the presence of significant surface magnetic flux. RP Saar, SH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS 58,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 50 TC 105 Z9 105 U1 0 U2 1 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 1 PY 1997 VL 284 IS 4 BP 803 EP 810 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WH887 UT WOS:A1997WH88700004 ER PT J AU Stott, AW Davies, E Evershed, RP Tuross, N AF Stott, AW Davies, E Evershed, RP Tuross, N TI Monitoring the routing of dietary and biosynthesised lipids through compound-specific stable isotope (delta C-13) measurements at natural abundance SO NATURWISSENSCHAFTEN LA English DT Article ID C-13; CARBON; TISSUE C1 UNIV BRISTOL,SCH CHEM,ORGAN GEOCHEM UNIT,BRISTOL BS8 1TS,AVON,ENGLAND. SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. RI STOTT, ANDREW /I-7920-2012 NR 21 TC 45 Z9 45 U1 0 U2 15 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD FEB PY 1997 VL 84 IS 2 BP 82 EP 86 DI 10.1007/s001140050354 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WM171 UT WOS:A1997WM17100007 PM 9121591 ER PT J AU Kitajima, K Mulkey, SS Wright, SJ AF Kitajima, K Mulkey, SS Wright, SJ TI Seasonal leaf phenotypes in the canopy of a tropical dry forest: Photosynthetic characteristics and associated traits SO OECOLOGIA LA English DT Article DE tropical canopy trees; leaf phenology; oxygen evolution rates; CO2 assimilation; phenotypic plasticity ID NITROGEN RELATIONS; C-3 PLANTS; TREE; LIGHT; ACCLIMATION; PHENOLOGY; CAPACITY; PATTERNS; LEAVES; SHADE AB We evaluated the hypothesis that photosynthetic traits differ between leaves produced at the beginning (May) and the end (November-December) of the rainy season in the canopy of a seasonally dry forest in Panama. Leaves produced at the end of the wet season were predicted to have higher photosynthetic capacities and higher water-use efficiencies than leaves produced during the early rainy season. Such seasonal phenotypic differentiation may be adaptive, since leaves produced immediately preceding the dry season are likely to experience greater light availability during their lifetime due to reduced cloud cover during the dry season. We used a construction crane for access to the upper canopy and sampled 1- to 2-month-old leaves marked in monthly censuses for six common tree species with various ecological habits and leaf phenologies. Photosynthetic capacity was quantified as light- and CO2-saturated oxygen evolution rates with a leaf-disk oxygen electrode in the laboratory (O-2max) and as light-saturated CO2 assimilation rates of intact leaves under ambient CO2 (A(max)). In four species, pre-dry season leaves had significantly higher leaf mass per unit area. In these four species, O-2max and A(max) per unit area and maximum stomatal conductances were significantly greater in pre-dry season leaves than in early wet season leaves, In two species, A(max) for a given stomatal conductance was greater in pre-dry season leaves than in early wet season leaves, suggesting a higher photosynthetic water-use efficiency in the former. Photosynthetic capacity per unit mass was not significantly different between seasons of leaf production in any species. In both early wet season and pre-dry season leaves? mean photosynthetic capacity per unit mass was positively correlated with nitrogen content per unit mass both within and among species. Seasonal phenotypic differentiation observed in canopy tree species is achieved through changes in leaf mass per unit area and increased maximum stomatal conductance rather than by changes in nitrogen allocation patterns. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV MISSOURI,ST LOUIS,MO 63121. RP Kitajima, K (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO,AA 34002, USA. RI Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 31 TC 54 Z9 58 U1 5 U2 28 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD FEB PY 1997 VL 109 IS 4 BP 490 EP 498 DI 10.1007/s004420050109 PG 9 WC Ecology SC Environmental Sciences & Ecology GA WM378 UT WOS:A1997WM37800002 PM 28307332 ER PT J AU Washburn, WE AF Washburn, WE TI Between 2 fires: American Indians in the Civil War - Hauptman,LM SO PACIFIC HISTORICAL REVIEW LA English DT Book Review RP Washburn, WE (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 JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0030-8684 J9 PAC HIST REV JI Pac. Hist. Rev. PD FEB PY 1997 VL 66 IS 1 BP 105 EP 106 PG 2 WC History SC History GA WN082 UT WOS:A1997WN08200009 ER PT J AU Pandolfi, JM Greenstein, BJ AF Pandolfi, JM Greenstein, BJ TI Taphonomic alteration of reef corals: Effects of reef environment and coral growth form .1. The Great Barrier Reef SO PALAIOS LA English DT Article ID BIOEROSION; SHELL AB Taphonomic alteration in coral death assemblages showed high variability with respect to reef environment and growth form at Orpheus Island on the Great Barrier Reef Australia. A greater degree of physical and biological alteration occurred in the lower-energy leeward Pioneer Bay site relative to the higher-energy windward Iris Point site. Greater degrees of taphonomic alteration also occurred at 6-7 m than 2-3 m water depth within each site. Clear gradients in the degree of taphonomic alteration of reef corals with reef environment indicate the utility of corals as taphonomic indicators in ancient reef settings. Because greater taphonomic differences between depths occurred at the high wave-energy site relative to the lour wave-energy site, differentiation of fossil reef taphofacies might be greatest in high energy reef settings. Interpretation of ancient reef sedimentary environments may be aided by analysis of taphonomic alteration. of reef corals. Massive corals suffered greater degrees of biological and physical alteration than free-living corals which suffered greater alteration than branching corals. The greater taphonomic alteration in more robust massive coral growth forms from Orpheus Island concurs with other studies that have suggested that bioerosion may be related to overall skeletal area and density, and amount of skeleton not covered by living tissue during the life of the coral. In addition, relative differences in production of coral morphotypes might result in. a greater number of less degraded branching than massive corals. A possible explanation for the two observations that corals in higher wave energy environments are less degraded than those from lower wave energy environments, and that fragile are better preserved than robust coral growth forms, is the differing amount of post-mortem residence time the corals spend in the 'taphonomically active zone'. C1 SMITHSONIAN TROP RES INST,CTR TROP PALEOECOL & ARCHAEOL,BALBOA,PANAMA. SMITH COLL,CLARK SCI CTR,DEPT GEOL,NORTHAMPTON,MA 01063. RI Pandolfi, John/A-3121-2009 OI Pandolfi, John/0000-0003-3047-6694 NR 36 TC 49 Z9 50 U1 1 U2 16 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 1731 E 71ST STREET, TULSA, OK 74136-5108 SN 0883-1351 J9 PALAIOS JI Palaios PD FEB PY 1997 VL 12 IS 1 BP 27 EP 42 DI 10.2307/3515292 PG 16 WC Geology; Paleontology SC Geology; Paleontology GA WH054 UT WOS:A1997WH05400004 ER PT J AU Booth, CR Morrow, JH Coohill, TP Cullen, JJ Frederick, JE Hader, DP HolmHansen, O Jeffrey, WH Mitchell, DL Neale, PJ Sobolev, I vanderLeun, J Worrest, RC AF Booth, CR Morrow, JH Coohill, TP Cullen, JJ Frederick, JE Hader, DP HolmHansen, O Jeffrey, WH Mitchell, DL Neale, PJ Sobolev, I vanderLeun, J Worrest, RC TI Impacts of solar UVR on aquatic microorganisms SO PHOTOCHEMISTRY AND PHOTOBIOLOGY LA English DT Editorial Material ID RADIATION C1 BIOSPHER INSTRUMENTS,SAN DIEGO,CA. ULTRAVIOLET CONSULTANTS,BOWLING GREEN,KY. DALHOUSIE UNIV,HALIFAX,NS,CANADA. UNIV CHICAGO,CHICAGO,IL 60637. UNIV ERLANGEN NURNBERG,D-8520 ERLANGEN,GERMANY. UNIV CALIF SAN DIEGO,SCRIPPS INST OCEANOG,LA JOLLA,CA 92093. UNIV W FLORIDA,PENSACOLA,FL 32514. MD ANDERSON CANC CTR,SMITHVILLE,TX. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. CHEM & POLYMER TECHNOL INC,ORINDA,CA. UNIV UTRECHT,NL-3508 TC UTRECHT,NETHERLANDS. CIESIN,WASHINGTON,DC. RP Booth, CR (reprint author), SCI & POLICY SERV INC,1333 H ST NW,W TOWER SUITE 100,WASHINGTON,DC 20002, USA. RI Cullen, John/B-6105-2008; Neale, Patrick/A-3683-2012 OI Cullen, John/0000-0002-7740-0999; NR 5 TC 29 Z9 32 U1 1 U2 2 PU AMER SOC PHOTOBIOLOGY PI AUGUSTA PA BIOTECH PARK, 1021 15TH ST, SUITE 9, AUGUSTA, GA 30901-3158 SN 0031-8655 J9 PHOTOCHEM PHOTOBIOL JI Photochem. Photobiol. PD FEB PY 1997 VL 65 IS 2 BP 252 EP 253 DI 10.1111/j.1751-1097.1997.tb08550.x PG 2 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA WK337 UT WOS:A1997WK33700011 ER PT J AU Marinescu, M Dalgarno, A Babb, JF AF Marinescu, M Dalgarno, A Babb, JF TI Retarded long-range potentials for the alkali-metal atoms and a perfectly conducting wall SO PHYSICAL REVIEW A LA English DT Article ID DIPOLE POLARIZABILITIES; COEFFICIENTS; ELECTRON AB The retarded long-range potentials for hydrogen and alkali-metal atoms in their ground states and a perfectly conducting wall are calculated. The potentials are given over a wide range of atom-wall distances and the validity of the approximations used is established. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OI Babb, James/0000-0002-3883-9501 NR 19 TC 34 Z9 35 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 FEB PY 1997 VL 55 IS 2 BP 1530 EP 1532 DI 10.1103/PhysRevA.55.1530 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA WH919 UT WOS:A1997WH91900085 ER PT J AU Lim, YA Mei, MC Kusumoto, IT Miyashiro, H Hattori, M Gupta, MP Correa, M AF Lim, YA Mei, MC Kusumoto, IT Miyashiro, H Hattori, M Gupta, MP Correa, M TI HIV-1 reverse transcriptase inhibitory principles from Chamaesyce hyssopifolia SO PHYTOTHERAPY RESEARCH LA English DT Article DE Chamaesyce hyssopifolia; HIV; Panamanian plant; reverse transcriptase ID RNA TUMOR-VIRUS; TANNINS; POLYMERASES; FLAVONOIDS; AIDS; DNA AB In the course of our studies on the development of anti-acquired immunodeficiency syndrome (AIDS) agents, we isolated corilagin, quercetin 3-O-beta-D-glucopyranoside and 1,3,4,6-tetra-O-galloyl-beta-D-glucopyranos from Chamaesyce hyssopifolia, as the main inhibitory substances against human immunodeficiency virus (HIV) reverse transcriptase, an enzyme essential for the proliferation of HIV. The IC50 of these substances were 20, 50 and 86 mu M, respectively, their modes of inhibition being non-competitive with respect to the substrate. (C) 1997 by John Wiley & Sons, Ltd. C1 RES INST WAKAN YAKU TRADIT SINO JAPANESE MED,TOYAMA 93001,JAPAN. UNIV PANAMA,HERBARIUM,PANAMA CITY,PANAMA. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV PANAMA,COLL PHARM,PHARMACOGNOSY RES CTR PANAMANIAN FLORA,PANAMA CITY,PANAMA. OI Gupta, Mahabir/0000-0002-9302-7864 NR 19 TC 20 Z9 23 U1 0 U2 1 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX, ENGLAND PO19 1UD SN 0951-418X J9 PHYTOTHER RES JI Phytother. Res. PD FEB PY 1997 VL 11 IS 1 BP 22 EP 27 DI 10.1002/(SICI)1099-1573(199702)11:1<22::AID-PTR951>3.0.CO;2-3 PG 6 WC Chemistry, Medicinal; Pharmacology & Pharmacy SC Pharmacology & Pharmacy GA WG712 UT WOS:A1997WG71200005 ER PT J AU Skillman, JB Winter, K AF Skillman, JB Winter, K TI High photosynthetic capacity in a shade-tolerant Crassulacean acid metabolism plant - Implications for sunfleck use, nonphotochemical energy dissipation, and susceptibility to photoinhibition SO PLANT PHYSIOLOGY LA English DT Article ID XANTHOPHYLL-CYCLE; CHLOROPHYLL FLUORESCENCE; ELECTRON-TRANSPORT; ABSORBENCY CHANGES; LEAVES; CAM; ADAPTATION; BROMELIAD; CARBON; YIELD AB Aechmea magdalenae Andre ex Baker, a constitutive Crassulacean acid metabolism (CAM) plant from the shaded Panamanian rain forest understory, has a maximum photosynthesis rate 2 to 3 times that of co-occurring C-3 species and a limited potential for photosynthetic acclimation to high light. Chlorophyll fluorescence measurements indicated that (a) compared with co-occurring C-3 species, photosynthetic electron transport in A. magdalenae responded more rapidly to light flecks of moderate intensity, attained a higher steady-state rate, and maintained a lower reduction state of plastoquinone during light flecks; (b) these characteristics were associated with phase III CO2 fixation of CAM; (c) when grown in full sun, A. magdalenae was chronically photoinhibited despite a remarkably high nonphotochemical quenching capacity, indicating a large potential for photoprotection; and (d) the degree of photoinhibition was inversely proportional to the length of phase III. Results from the light fleck studies suggest that understory A. magdalenae plants can make more efficient use of sun flecks for leaf carbon gain over most of the day than co-occurring C-3 species. The association between the duration of phase III and the degree of photoinhibition for A. magdalenae in high light is discussed in relation to the limited photosynthetic plasticity in this species. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. NR 42 TC 44 Z9 48 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 FEB PY 1997 VL 113 IS 2 BP 441 EP 450 PG 10 WC Plant Sciences SC Plant Sciences GA WH572 UT WOS:A1997WH57200017 ER PT J AU McCarthy, MC Travers, MJ Kovacs, A Chen, W Novick, SE Gottlieb, CA Thaddeus, P AF McCarthy, MC Travers, MJ Kovacs, A Chen, W Novick, SE Gottlieb, CA Thaddeus, P TI Detection and characterization of the cumulene carbenes H2C5 and H2C6 SO SCIENCE LA English DT Article ID CARBON-CHAIN CARBENE; LABORATORY DETECTION; PROPADIENYLIDENE AB Two cumulene carbenes, H2C5 and H2C6, were detected in a supersonic molecular beam by Fourier transform microwave spectroscopy. Their rotational and leading centrifugal distortion constants were determined with high accuracy, such that the entire radio spectrum can now be calculated. Like the known carbenes H2C2 and H2C4, both molecules have singlet electronic ground states and linear carbon-chain backbones. They can be produced in sufficiently high concentrations in the laboratory that their electronic spectra, expected to lie in the visible, should be readily detectable by laser spectroscopy. The microwave spectra of other, more exotic isomers may be detectable as well. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. WESLEYAN UNIV,DEPT CHEM,MIDDLETOWN,CT 06459. RP McCarthy, MC (reprint author), HARVARD UNIV,DIV ENGN & APPL SCI,29 OXFORD ST,CAMBRIDGE,MA 02138, USA. RI Kovacs, Attila/C-1171-2010; OI Kovacs, Attila/0000-0001-8991-9088; McCarthy, Michael/0000-0001-9142-0008 NR 31 TC 70 Z9 70 U1 2 U2 14 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JAN 24 PY 1997 VL 275 IS 5299 BP 518 EP 520 DI 10.1126/science.275.5299.518 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WE257 UT WOS:A1997WE25700040 ER PT J AU Clapham, PJ Palsboll, PJ AF Clapham, PJ Palsboll, PJ TI Molecular analysis of paternity shows promiscuous mating in female humpback whales (Megaptera novaengliae, Borowski) SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article ID HAWAIIAN WATERS; WEST-INDIES; NOVAEANGLIAE; BEHAVIOR AB It is widely assumed that the mating system of the humpback whale, Megaptera novaeangliae, is similar to that of most mammals in that it represents some form of polygyny or promiscuity, but this cannot be tested without observations of copulation or data on paternity of offspring. Microsatellite DNA markers were used to examine the paternity of calves born to individually identified mature female humpback whales from the Gulf of Maine. Skin biopsies were obtained from three females, and several (range: three to five) of their known offspring. Multiple paternity of offspring, indicated by the presence of at least three different paternal alleles, was evident in all three females at either three or four of the six microsatellite loci surveyed. Such promiscuous mating is expected given current knowledge of the social ecol species. It is also consistent with resightings of individually identified female humpbacks with different male associates during two or more breeding seasons. C1 CTR COASTAL STUDIES, CETACEAN RES PROGRAM, PROVINCETOWN, MA 02657 USA. UNIV COPENHAGEN, INST POPULAT BIOL, DK-2100 COPENHAGEN O, DENMARK. RP SMITHSONIAN INST, NHB 390, MRC 108, 10TH & CONSTITUT SW, WASHINGTON, DC 20560 USA. RI Palsboll, Per /G-6988-2011 OI Palsboll, Per /0000-0002-4198-7599 NR 26 TC 46 Z9 48 U1 0 U2 18 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JAN 22 PY 1997 VL 264 IS 1378 BP 95 EP 98 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA WF624 UT WOS:A1997WF62400014 PM 9061965 ER PT J AU Zeh, DW Zeh, JA Bermingham, E AF Zeh, DW Zeh, JA Bermingham, E TI Polyandrous, sperm-storing females: Carriers of male genotypes through episodes of adverse selection SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article ID EXTRA-PAIR PATERNITY; GENETIC-VARIATION; SEXUAL SELECTION; FLUCTUATING SELECTION; MULTIPLE PATERNITY; ENVIRONMENTS; POPULATIONS; DNA AB In the pseudoscorpion, Cordylochernes scorpioides, males experience sexual selection in two disparate and well-defined habitats. Populations inhabit decaying trees for several generations before dispersing under the elytra of the harlequin beetle, Acrocinus longimanus. Males compete to monopolize beetle abdomens as strategic sites for inseminating dispersing females. Using single-locus minisatellite DNA profiling to assign paternity for the offspring of dispersing females we found a strong, positive correlation between male size and reproductive success in the beetle environment. However, this intense selection is undermined by polyandry and the ability of females to score sperm and produce mixed-paternity broods. Although beetle-riding males achieved fertilizations with 70% of the females, paternity could not be assigned for 57% of the offspring. It is likely that many of these offspring were the products of within-tree inseminations since, in a sample of females intercepted in the act of boarding beetles, most (86%) carried sperm from pre-dispersal matings within trees. Polyandry and sperm storage may therefore enable smaller males unable to monopolize beetle mating territories, to circumvent the bottleneck of dispersal-generated sexual selection and thereby transmit their genes to future tree populations. Sperm stored within Females can thus provide the kind of resistant life-history stage shown by recent modelling to be critical for the maintenance of genetic variation by temporally fluctuating selection. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RP Zeh, DW (reprint author), UNIV HOUSTON, DEPT BIOL, HOUSTON, TX 77204 USA. NR 30 TC 35 Z9 35 U1 2 U2 6 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JAN 22 PY 1997 VL 264 IS 1378 BP 119 EP 125 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA WF624 UT WOS:A1997WF62400018 ER PT J AU Fiore, F Matt, G Nicastro, F AF Fiore, F Matt, G Nicastro, F TI Testing the ionized disc reprocessing model for the soft X-ray emission of quasars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies, active; galaxies, fundamental parameters; quasars, general; galaxies, Seyfert; X-rays, galaxies ID ACTIVE GALACTIC NUCLEI; ACCRETION DISKS; LINE-PROFILES; BLACK HOLES; SPECTRA; ULTRAVIOLET; BUMP; POLARIZATION; AGN AB One of the current explanations for the soft X-ray emission of active galactic nuclei (AGN) is reprocessing of the hard X-rays by partially ionized, optically thick matter. This idea is very appearing because it would explain the shape of the AGN soft X-ray spectrum in terms of atomic physics. While at present the reflection model correctly describes the soft X-ray spectra of a few low-luminosity Seyfert galaxies, it is not clear whether or not it can be applied to higher luminosity quasars. To investigate this issue quantitatively, we have fitted the high signal-to-noise ratio Position Sensitive Proportional Counter (PSPC) spectra of 11 AGN of different luminosities with a model consisting of a direct hard X-ray component, reflection from the ionized surface of an accretion disc and the direct thermal emission of the disc. We find that the AGN with an acceptable fit are a minority, and all have a low optical (and bolometric) luminosity, flat PSPC energy index alpha(PSPC) and the flattest alpha(OX) of the sample, while those with the worst fit all have high optical (and bolometric) luminosity, steep alpha(PSPC) and the steepest alpha(OX) of the sample. We conclude that either the reprocessing model is not correct and the form of the soft X-ray spectrum of AGN cannot be simply explained in terms of characteristic atomic features (i.e. highly ionized oxygen K-edges), or the origin of the soft X-ray emission of AGN is not 'universal'. C1 SAX SCI DATA CTR,I-00131 ROME,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CNR,IST ASTROFIS SPAZIALE,I-00044 FRASCATI,ITALY. UNIV ROMA TRE,DIPARTIMENTO FIS,I-00146 ROME,ITALY. RP Fiore, F (reprint author), OSSERV ASTRON ROMA,VIA OSSERV,I-00044 MONTE PORZIO CATO,ITALY. OI Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 47 TC 11 Z9 11 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 21 PY 1997 VL 284 IS 3 BP 731 EP 740 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE368 UT WOS:A1997WE36800019 ER PT J AU Badran, HM Urban, M Weekes, TC AF Badran, HM Urban, M Weekes, TC TI Development of a filter for operation of atmospheric Cherenkov telescopes close to the Moon SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article AB A filter has been developed and tested for the ARTEMIS experiment with solar-blind photomultiplier tubes. The filter consists of CoSO4, NiSO4, and 2,7-dimethyl-3,6-diazacyclohepta-2,6-diene perchlorate solutions in water. The filter transmission is about 65% in the wavelength range 230-270 nm. The Ni-Co solution allows a factor of 10 reduction in the background light from the Moon and the dye introduces another factor of 20. This reduction reduces significantly the systematics due to the position of the Moon. The new arrangement allows the center of the camera to be as close as 2 degrees from the Moon center without any bias to a specific direction from the moon at any phase. C1 ECOLE POLYTECH,CNRS,IN2P3,LPNHE,F-91128 PALAISEAU,FRANCE. TANTA UNIV,FAC SCI,DEPT PHYS,TANTA,EGYPT. RP Badran, HM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,POB 97,AMADO,AZ 85645, USA. NR 14 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JAN 21 PY 1997 VL 385 IS 2 BP 258 EP 264 DI 10.1016/S0168-9002(96)00896-0 PG 7 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA WF943 UT WOS:A1997WF94300010 ER PT J AU Chen, H Tafalla, M Greene, TP Myers, PC Wilner, DJ AF Chen, H Tafalla, M Greene, TP Myers, PC Wilner, DJ TI IRAS 20050+2720: An embedded young cluster associated with a multipolar outflow SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared, stars; ISM, jets and outflows; open clusters and associations,; individual (IRAS 20050 + 2720); stars, luminosity function, mass function; stars, pre-main-sequence ID MOLECULAR CLOUD; STELLAR OBJECTS; DARK CLOUDS; CIRCUMSTELLAR DISKS; OPHIUCHI CLOUD; IMAGING SURVEY; LOW-MASS; STARS; CORES; PROTOSTARS AB We obtained near-IR images at 1-5 mu m of IRAS 20050+2720, a very red far-infrared source with a multipolar outflow (as noted by Bachiller et al.). Of the 212 sources we detected, half of them are probably members of an embedded cluster around the IRAS source. More than 50% of the cluster members show near-IR excesses, suggesting that they are pre-main-sequence stars with circumstellar emission. The luminosity functions of the cluster show turnovers and slopes consistent with pre-main-sequence model predictions for an average cluster age of similar to 1 Myr. Three subclusters are identified within the cluster. One of them (subcluster A) appears to be associated with denser molecular gas and higher extinction than the other two subclusters. It also coincides with the IRAS source, a compact millimeter continuum source, and the center of the multipolar CO outflow. We identified in subcluster A several deeply embedded sources with sharply rising spectral energy distributions. These results support strongly the suggestion that the multipolar outflow is the result of simultaneous star formation within 0.1 pc of the IRAS source. We suggest that the cluster was formed in several episodes of star formation over the last similar to 1 Myr and that subcluster A represents the most recent episode that formed multiple young stars within similar to 0.1 Myr. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. NR 49 TC 22 Z9 22 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1997 VL 475 IS 1 BP 163 EP 172 DI 10.1086/303536 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WD179 UT WOS:A1997WD17900016 ER PT J AU Ohashi, N Hayashi, M Ho, PTP Momose, M AF Ohashi, N Hayashi, M Ho, PTP Momose, M TI Interferometric imaging of IRAS 04368+2557 in the last L1527 molecular cloud core: A dynamically infalling envelope with rotation SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; ISM, individual (L1527); ISM, kinematics and dynamics; stars, formation; stars, pre-main-sequence ID SMALL-SCALE STRUCTURE; DENSE CORES; HL TAURI; DARK CLOUDS; PROTOSTELLAR COLLAPSE; CIRCUMSTELLAR GAS; YOUNG STARS; DISKS; PROTOSTARS; EXTINCTION AB We report new interferometric observations of IRAS 04368 + 2557 (L1527) in (CO)-C-13 (J = 1-0), (CO)-O-18 (J = 1-0), and 2.7 mm continuum emission using the Nobeyama Millimeter Array. The continuum map shows a well-defined emission peak with slightly extended features. The extended features are consistent with an 800 mu m continuum map. The (CO)-C-13 map shows blueshifted and redshifted outflowing shells characterized by a bipolar V-shape structure with a wide opening angle toward the east and west of the central source. Near the systemic velocity, a slightly blueshifted X-shaped condensation was detected in (CO)-C-13 with its peak coincident with the central source. The symmetrical distribution of the X-shaped condensation centered on the central source suggests that it is a circumstellar envelope surrounding the central source. The (CO)-O-18 map shows a flattened structure elongated in the north-south direction, perpendicular to the outflow axis, centered on the central source. This flattened structure correlates spatially with the (CO)-C-13 X-shaped condensation. Both eastern and western edges of the flattened structure are concave, as the (CO)-C-13 X-shaped condensation also shows, and they are spatially well anticorrelated with the distribution of the outflowing shells in both blueshifted and redshifted velocities. The flattened structure is hence naturally interpreted as a disklike flattened envelope with an almost edge-on configuration. Its radius and gas mass are estimated to be similar to 2000 AU and similar to 0.038 M., respectively. The edge-on flattened envelope has both rotational and radial motions with the latter dominant. The large specific angular momentum carried by the envelope gas implies that the radial motion can be infall rather than outflow. The infall and rotation velocities are similar to 0.3 km s(-1) and similar to 0.05 km s(-1), respectively, at the envelope radius of 2000 AU. The flattened envelope is clearly not supported by rotation, but it is dynamically infalling. Its mass infall rate is similar to 1.1 x 10(-6) M. yr(-1) at 2000 AU in radius. This mass infall rate is consistent with that estimated from the bolometric luminosity of 1.4 L. and the mass of 0.1 M. of the central star. On the assumption that the mass infall rate is constant with time, the age of the central star is estimated to be similar to 10(5) yr, which is comparable to the typical age of protostars in Taurus, even though the central star in L1527 is identified as a very young class O source. The rotating motion of the flattened envelope is opposite to the large-scale rotation of the L1527 cloud, suggesting that the rotation of the flattened envelope did not originate from the large-scale rotation. C1 NATL ASTRON OBSERV,SUBARU PROJECT OFF,MITAKA,TOKYO 181,JAPAN. GRAD UNIV ADV STUDIES,DEPT ASTRON SCI,MINAMISA KU,NAGANO 38413,JAPAN. RP Ohashi, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 45 TC 117 Z9 117 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1997 VL 475 IS 1 BP 211 EP & DI 10.1086/303533 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WD179 UT WOS:A1997WD17900020 ER PT J AU Gray, DF Baliunas, SL AF Gray, DF Baliunas, SL TI The rotation of the G0 dwarf beta Comae SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, activity; stars, chromospheres; stars, individual (beta Comae); stars, rotation ID DIFFERENTIAL ROTATION; STELLAR ROTATION; COOL STARS; EMISSION AB The rotation of beta Comae (HR 4983, HD 114710, GO V) is studied using the available information from spectral line broadening and from rotational modulation. The line broadening yields nu sin i = 4.10 +/- 0.06 km s(-1), which agrees with previous values. Rotational modulation was looked for but not seen in the photospheric parameters of temperature and granulation, although this might be a result of data sampling not being well suited for modulation studies. Rotational modulation is seen in the S index of the Ca II chromospheric emission. Two period sequences characterize beta Comae between 1981 and 1994. The periods decline monotonically with time, paralleling the decline in magnetic activity as indicated by the average strength of the Ca II emission. We interpret the decrease in period as differential rotation coupled with systematic migration in latitude of the active regions. It is not possible to separate the differential rotation profile of beta Comae from its rate and sense of latitude migration. We compare the changes of beta Comae with the Sun's and point out similarities and differences. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Gray, DF (reprint author), UNIV WESTERN ONTARIO,DEPT ASTRON,LONDON,ON N6A 3K7,CANADA. NR 46 TC 14 Z9 14 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1997 VL 475 IS 1 BP 303 EP 312 DI 10.1086/303522 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WD179 UT WOS:A1997WD17900030 ER PT J AU Navascues, DBY Stauffer, JR Hartmann, L Balachandran, SC AF Navascues, DBY Stauffer, JR Hartmann, L Balachandran, SC TI The age of Gliese 879 and Fomalhaut SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, visual; circumstellar matter; stars, evolution stars, individual (Piscis Astrini, Gliese 879) ID SOLAR-TYPE STARS; LITHIUM ABUNDANCES; MAIN-SEQUENCE; OPEN CLUSTERS; K-DWARFS; HYADES; EVOLUTION; ROTATION; CATALOG; GEMINORUM AB We estimate here the age of one of the prototypes of the beta Pic-like stars, Fomalhaut, based on the properties of its common proper motion companion GI 879. By combining constraints derived from the lithium abundance, rotational velocity, H-R diagram position, and coronal activity we conclude that the age for GI 879, and hence the age for Fomalhaut, is 200 +/- 100 Myr. This age estimate agrees quite well with the completely independent age estimate derived directly from isochrone fitting to Fomalhaut's position in an H-R diagram, and thus confirms that circumstellar dust disks can persist in A stars for several hundred megayears. C1 REAL COLEGIO COMPLUTENSE,CAMBRIDGE,MA 02138. UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742. RP Navascues, DBY (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 50 TC 38 Z9 38 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1997 VL 475 IS 1 BP 313 EP 321 DI 10.1086/303518 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WD179 UT WOS:A1997WD17900031 ER PT J AU Brown, TM Kennelly, EJ Korzennik, SG Nisenson, P Noyes, RW Horner, SD AF Brown, TM Kennelly, EJ Korzennik, SG Nisenson, P Noyes, RW Horner, SD TI A radial velocity search for p-mode pulsations in eta Bootis SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, individual (eta Bootis); stars, oscillations; techniques, radial velocities AB The subgiant eta Boo (G5 IV) has been reported to show p-mode pulsations, as evidenced by variations in the equivalent width of its hydrogen Balmer lines (reported by Kjeldsen et al.). In an attempt to confirm this report, we observed eta Boo's radial velocity with the AFOE spectrograph for a total of 22 hours spread over seven successive nights in 1995 March. We find no evidence for the presence of excess power at the frequencies reported by Kjeldsen et al.; our upper limit corresponds to typical mode amplitudes of 0.5 m s(-1), about 3 times smaller than the velocity amplitudes they inferred. Signals with amplitudes larger than 0.5 m s(-1) may be present at other frequencies within the 0-1000 mu Hz range, but evidence for such signals is scanty, and typical mode amplitudes greater than 1.5 m s(-1) are clearly inconsistent with our observations. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. PENN STATE UNIV,UNIVERSITY PK,PA 16802. RP Brown, TM (reprint author), NATL CTR ATMOSPHER RES,HIGH ALTITUDE OBSERV,POB 3000,BOULDER,CO 80307, USA. NR 10 TC 34 Z9 34 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1997 VL 475 IS 1 BP 322 EP 327 DI 10.1086/303512 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WD179 UT WOS:A1997WD17900032 ER PT J AU Eikenberry, SS Fazio, GG AF Eikenberry, SS Fazio, GG TI Time evolution and the nature of the near-infrared jets in GRS 1915+105 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared, stars; stars, individual (GRS 1915+105); ISM, jets and outflows AB We observed the Galactic microquasar GRS 1915+105 in the K (2.2 mu m) band on 1995 October 16 and 17 UTC using the cryogenic optical bench (COB) infrared imager on the Kitt Peak National Observatory 2.1 m telescope with a 0.2'' pixel(-1) plate scale and under good (similar to 0.7'') seeing conditions. Using a neighboring star in the image frames to determine the point-spread function (PSF), we PSF-subtract the images of GRS 1915+105. We find no evidence of extended emission such as the apparent near-IR jets seen by Sams, Eckart, & Sunyaev in 1995 July. Simple modeling of the star plus jet structure allows us to place an upper limit on any similar emission at that position of K > 16.4 at the 95% confidence level, as compared to K = 13.9 as seen by Sams et al. This lack of extended IR flux during continued hard X-ray flaring activity confirms the hypothesis that the extended IR emission arises from the superluminal radio-emitting jets rather than reprocessing of the X-ray emission on other structures around the compact central object. Given the large apparent velocity of the radio-emitting jets, by the time of our observations the Sams et al. feature would have moved more than 1'' from GRS 1915+105, and we can place a limit of K > 17.7 (95% confidence level) on any infrared emission in this region. We can thus place an upper limit of tau < 28 days on the radiative timescale of the feature, which is consistent with synchrotron jet emission. RP Eikenberry, SS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 7 TC 11 Z9 11 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1997 VL 475 IS 1 BP L53 EP L55 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WD181 UT WOS:A1997WD18100014 ER PT J AU Herrnstein, JR Moran, JM Greenhill, LJ Diamond, PJ Miyoshi, M Nakai, N Inoue, M AF Herrnstein, JR Moran, JM Greenhill, LJ Diamond, PJ Miyoshi, M Nakai, N Inoue, M TI Discovery of a subparsec jet 4000 radii away from the central schwarzschild engine of NGC 4258 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies, individual (NGC 4258); galaxies, jets galaxies, nuclei; galaxies, Seyfert; masers ID ACTIVE GALACTIC NUCLEI; SPIRAL GALAXY NGC-4258; RELATIVISTIC JETS; STAR-FORMATION; EMISSION; MOTION; NEARBY; MASER; DISK AB We report the VLBI detection of compact continuum emission associated with the maser disk in NGC 4258. The strongest emission is located about 0.5 mas (0.015 pc) north of the dynamical center of the disk. It has an average flux density of about 3 mJy and varies by similar to 100% on timescales of weeks. We postulate that we have detected nonthermal synchrotron emission in the base of the northern jet, which is seen on parsec-to-kiloparsec scales in radio to X-ray emission. We also report a detection of emission from the southern jet which may be attenuated by thermal absorption in a layer of ionized gas above the molecular disk. The average flux density of the maser emission in the systemic velocity range is correlated with the flux density of the northern continuum emission. Together with the geometry of the disk, these data suggest that the masers amplify the southern continuum emission and that the southern and northern jet emission are correlated in strength. We discuss the results in the context of jet emission models and properties of other compact radio continuum sources. C1 NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. NATL ASTRON OBSERV,MIZUSAWA ASTROGEODYNAM OBSERV,MIZUSAWA,IWATE 023,JAPAN. NATL ASTRON OBSERV,NOBEYAMA RADIO OBSERV,MINAMISA KU,NAGANO 38413,JAPAN. RP Herrnstein, JR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 42,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 29 TC 69 Z9 69 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1997 VL 475 IS 1 BP L17 EP L20 DI 10.1086/310461 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WD181 UT WOS:A1997WD18100005 ER PT J AU Mazeh, T Martin, EL Goldberg, D Smith, HA AF Mazeh, T Martin, EL Goldberg, D Smith, HA TI Detecting faint secondaries of spectroscopic binaries: HD 101177B and 149414A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries, spectroscopic; stars, individual, HD 101177B; stars, individual, HD 149414A ID MASS-RATIO DISTRIBUTION; SOLAR-TYPE STARS; TODCOR; MULTIPLICITY; NEIGHBORHOOD; COMPANIONS; SYSTEMS; SAMPLE; DISC AB We have observed HD 101177B and 149414A, two known single-lined binaries, and directly measured the radial velocities of their secondaries, enabling us to derive the mass ratios of the two systems. Using high signal-to-noise ratio spectra obtained mostly with the William Herschel Telescope, and a new algorithm to analyse composite spectra, TODCOR, We show that the mass ratios of HD 101177B and 149414A are 0.48 +/- 0.03 and 0.57 +/- 0.02, respectively. These are two of the lowest mass ratios ever measured around normal G or K dwarf stars. These two systems demonstrate the potential of the present approach, which can turn many of the known single-lined binaries into double-lined systems. Such work has important implications for the study of the mass-ratio distribution of many samples of binaries. C1 NATL AIR & SPACE MUSEUM,SMITHSONIAN INST,ASTROPHYS LAB,WASHINGTON,DC 20560. INST ASTROFIS CANARIAS,E-38200 LA LAGUNA,TENERIFE,SPAIN. RP Mazeh, T (reprint author), TEL AVIV UNIV,RAYMOND & BEVERLY SACKLER FAC EXACT SCI,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. NR 31 TC 12 Z9 12 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 1997 VL 284 IS 2 BP 341 EP 347 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC928 UT WOS:A1997WC92800009 ER PT J AU Ciliegi, P Elvis, M Wilkes, BJ Boyle, BJ McMahon, RG AF Ciliegi, P Elvis, M Wilkes, BJ Boyle, BJ McMahon, RG TI The Cambridge-Cambridge ROSAT serendipity survey .4. The X-ray properties SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies, active; quasars, general; galaxies, Seyfert; X-rays, galaxies ID OPTICALLY SELECTED QUASARS; MEDIUM-SENSITIVITY SURVEY; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT QUASARS; SPECTRA; GALAXIES AB We present a detailed X-ray spectral analysis in the 0.1-2.4 keV ROSAT band of a complete sample of X-ray-selected AGN using the 80 AGNs in the Cambridge-Cambridge ROSAT Serendipity Survey (68 QSOs and 12. narrow-emission-line galaxies, NLXGs), We also make a comparison between the X-ray spectral properties of QSOs and NLXGs, For 36 objects we have enough net counts to allow an X-ray spectral fit, while for the other sources we characterize the spectrum using the hardness-ratio technique. A maximum-likelihood analysis is used to find the mean power-law energy spectral index [alpha(x)] and the standard deviation sigma for QSOs and NLXGs, assuming the intrinsic distribution to be Gaussian. We find no difference between QSOs and NLXGs: [alpha(x)] = 1.32 with dispersion sigma = 0.33 for the QSOs, and [alpha(x)] = 1.30 with sigma = 0.49 for the NLXGs. A single power law with a Galactic absorbing column density yields a good representation of the X-ray spectra for the majority of the sources, Only three objects show a significant deviation from this model, There is evidence in the NLXG sample for a flattening of the spectral slope alpha(x) with increasing redshift, and for a steepening of alpha(x) with increasing (L(2500 Angstrom)/L(x)). For the QSO sample we found no significant correlation. The lack of correlation between alpha(x) and z suggests that for the CRSS QSOs the power-law spectrum in the QSO rest-frame extends from the soft (similar to 0.1-2.4 keV) into the harder X-ray band (similar to 0.3-7.3 keV) with the same slope. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV MILAN,DIPARTIMENTO FIS,MILAN,ITALY. OSSERV ASTRON BRERA,I-20121 MILAN,ITALY. ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0EZ,ENGLAND. UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. RP Ciliegi, P (reprint author), UNIV CAMBRIDGE,INST ASTRON,MADINGLEY RD,CAMBRIDGE CB3 0HA,ENGLAND. OI Wilkes, Belinda/0000-0003-1809-2364 NR 29 TC 19 Z9 19 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 1997 VL 284 IS 2 BP 401 EP 415 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC928 UT WOS:A1997WC92800016 ER PT J AU Liu, WH AF Liu, WH TI The distribution of carbon monoxide in detached circumstellar envelopes SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM, molecules; molecular processes; stars, late-type ID CO; PHOTODISSOCIATION; IRC+10216; STARS AB Calculations are presented of the evolution of the distribution of carbon monoxide and its photodissociation products in detached circumstellar envelopes surrounding evolved late-type stars that have undergone intense mass loss. The CO molecules are more readily photodissociated in a detached shell than in an attached envelope because of the less effective shielding by H-2 and CO molecules and by the dust of the dissociating radiative held. At early stages of its evolution, the CO distribution follows closely the hydrogen distribution in the detached shell, because CO photodissociation is not significant except in the thin outermost layer of the shell. At the later stages, the CO shell occupies only the innermost layer of the detached shell because of the more effective CO photodissociation in the outer layer that occurs unless the gas is extremely clumpy. Observations of the CO photodissociation products, C and especially C+, are needed for the determination of the actual size of the detached shell. A comparison of the calculations and observations of the widths of the CO shells indicates a clumpy structure of the circumstellar gas, which is consistent with the patchy appearances and rectangular profiles of the optically thick CO emission from the shells. The carbon ionization ratio is a potentially useful diagnostic of the degree of clumpiness in the detached shells. Its determination through observations will be important in refining our understanding of the role of photodissociation in the detached circumstellar envelopes. RP Liu, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 17 TC 1 Z9 1 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1997 VL 474 IS 2 BP 724 EP 729 DI 10.1086/303492 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC498 UT WOS:A1997WC49800020 ER PT J AU Baliunas, SL Henry, GW Donahue, RA Fekel, FC Soon, WH AF Baliunas, SL Henry, GW Donahue, RA Fekel, FC Soon, WH TI Properties of Sun-like stars with planets: rho(1) Cancri, tau Bootis, and nu Andromedae SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars, activity; stars, late-type; techniques, photometric; techniques, spectroscopic ID ANGULAR DIAMETERS; VELOCITIES; ROTATION AB Planets have been reported orbiting the Sun-like stars rho(1) Cnc, tau Boo, and upsilon And based on low-amplitude radial velocity variations. We have derived information on the first two stars from analysis of spectra, as well as parallel records of high-precision Stromgren b and y photometry and Ca II H + K fluxes. In the case of rho(1) Cnc, the upper limit (peak to peak) of nondetection of photometric variability at the orbital period is Delta y similar to 0.0004 mag. The possibility of a planetary transit cannot be ruled out completely from the photometric data. Variations of the Ca II fluxes suggest a rotational period of similar to 42 days, in agreement with the inferred upsilon sin i similar to 2 km s(-1). The age of rho(1) Cnc is similar to 5 Gyr, based on its average Ca II flux and a relation between Ca II flux and age. The star tau Boo, unlike the other reported solar-type stars with planets, is relatively young (similar to 2 Gyr) Despite its young age, it is photometrically nonvariable at the orbital period with an amplitude of Delta(b + y)/2 similar to 0.0004 mag (peak to peak); however, small-amplitude interseasonal variability is seen. No planetary transits were found in the photometry, which limits the inclination of the planet's orbital plane to Earth's Line of sight to less than 83 degrees (where 90 degrees is coplanar). The Ca II record shows a weakly significant rotational period near 3.3 days, coincident with the orbital period of the companion. The Ca II record also shows a period of 116 days that has persisted for 30 years and is not seen in the photometric record. The persistence and timescale of this Ca II variation mean that it has no counterpart in Sun-like magnetic activity. The amplitude of the reflex velocity of the parent star (similar to 450 m s(-1)) is much larger than the radial velocity perturbations expected from the presence of either surface inhomogeneities or line-bisector variations. Thus the anticipated perturbations from those stellar effects do not refute the inference of reflex velocities. We have few Ca II flux measurements for upsilon And. Its age and rotational period are estimated to be similar to 5 Gyr and 12 days, respectively. Our results for rho(1) Cnc and tau Boo are consistent with the explanation of planets as the cause of the velocity variations. C1 TENNESSEE STATE UNIV,CTR EXCELLENCE INFORMAT SYST,NASHVILLE,TN 37203. MT WILSON INST,PASADENA,CA 91106. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Baliunas, SL (reprint author), TENNESSEE STATE UNIV,CTR AUTOMATED SPACE SCI,330 10TH AVE N,NASHVILLE,TN 37203, USA. NR 30 TC 64 Z9 64 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1997 VL 474 IS 2 BP L119 EP L122 DI 10.1086/310442 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC500 UT WOS:A1997WC50000011 ER PT J AU Carilli, CL Menten, KM Reid, RJ Rupen, MP AF Carilli, CL Menten, KM Reid, RJ Rupen, MP TI Neutral hydrogen 21 centimeter absorption at redshift 0.673 toward 1504+377 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, ISM; galaxies, jets; quasars, absorption lines; radio lines, galaxies ID CENTAURUS-A; MOLECULAR ABSORPTION; OBJECT PKS-1413+135; CO ABSORPTION; GALAXY; EMISSION; NUCLEUS; SPECTRA; DISK; GAS AB We detect the 21 cm line of neutral hydrogen in absorption at a redshift of 0.673 toward the 1 Jy radio source 1504+377. The 1504+377 radio source is located toward the center of what appears to be an inclined disk galaxy at z = 0.674. The 21 cm absorption line shows multiple velocity components over a velocity range of about 100 km s(-1), with a total H I column density of N(H I) = 3.8 X 10(19)(T-s/f) cm(-2). The velocity-integrated optical depth of this system is the largest yet seen for redshifted H I 21 cm absorption-line systems. The 21 cm absorption line is coincident in redshift with a previously detected broad molecular absorption line system. We do not detect H I 21 cm absorption associated with the narrow molecular absorption line system at z = 0.67150, nor do we detect absorption at these redshifts by the 18 cm lines of OH, nor by the 2 cm transition of H2CO. There is no evidence for a bright optical active galactic nucleus (AGN) in 1504+377, suggesting significant obscuration through the disk-a hypothesis supported by the strong absorption observed. The 1504+377 system resembles the ''red quasar'' PKS 1413+135, which has been modeled as an optically obscured AGN with a very young radio jet in the center of a gas-rich disk galaxy. The presence of very bright radio jets at the centers of these two disk galaxies presents a challenge to unification schemes for extragalactic radio sources and to models for the formation of radio-loud AGNs. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP Carilli, CL (reprint author), NATL RADIO ASTRON OBSERV,POB O,1003 LOPEZVILLE RD,SOCORRO,NM 87801, USA. NR 32 TC 18 Z9 18 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1997 VL 474 IS 2 BP L89 EP L93 DI 10.1086/310445 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC500 UT WOS:A1997WC50000004 ER PT J AU Greenhill, LJ Ellingsen, SP Norris, RP Gough, RG Sinclair, MW Moran, JM Mushotzky, R AF Greenhill, LJ Ellingsen, SP Norris, RP Gough, RG Sinclair, MW Moran, JM Mushotzky, R TI Extremely rapid variations of water maser emission from the Circinus galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, individual (Circinus); galaxies, kinematics and dynamics; galaxies, nuclei masers ID ACTIVE GALACTIC NUCLEI; VAPOR MASER; H2O MASERS; SPECTRUM; REGION; VARIABILITY; VELOCITIES; OH AB The water maser lines in the Seyfert nucleus of the Circinus galaxy vary on timescales as short as a few minutes. The amplitude of one line more than doubled in approximate to 10 minutes, reaching approximate to 37 Jy, which corresponded to an increase of approximate to 6 L., assuming isotropic emission, in a single maser feature on a size scale of about 1 AU, based on light-travel time. Other lines vary by up to about 30% on similar timescales. The variability is at least 2 orders of magnitude more rapid than any observed for other Galactic or extragalactic water masers. The intensity changes cannot be attributed easily to a mechanism of intrinsic fluctuations. The variability may be the result of strong interstellar diffractive scintillation along the line of sight within our Galaxy. This would be the first example of diffractive scintillation for any source at 22 GHz and for any source other than a pulsar. However, only the very shortest timescales for interstellar scintillation, obtained from pulsar observations and scaled to 22 GHz, correspond to the observed maser variability. Alternatively, the intensity changes may be a reaction to fluctuations in compact background or radiative pump sources and thereby may be related to variability of the central engine. The maser spectral features symmetrically bracket the systemic velocity of the galaxy, with components red- and blueshifted by about +/-(100-200) km s(-1). The spectrum of the Circinus maser is similar in some respects to that of the maser in NGC 4258, which probably traces a molecular disk rotating around a supermassive object. VLBI observations could reveal whether the maser source in the heart of the Circinus galaxy is part of a similar dynamical system. C1 UNIV TASMANIA,HOBART,TAS 7001,AUSTRALIA. CSIRO,AUSTRALIA TELESCOPE NATL FACIL,EPPING,NSW 2121,AUSTRALIA. NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. 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 36 TC 51 Z9 52 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1997 VL 474 IS 2 BP L103 EP L106 DI 10.1086/310434 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC500 UT WOS:A1997WC50000007 ER PT J AU Woo, R Habbal, SR AF Woo, R Habbal, SR TI Finest filamentary structures of the corona in the slow and fast solar wind SO ASTROPHYSICAL JOURNAL LA English DT Article DE interplanetary medium; solar wind; Sun, corona ID ELECTRON-DENSITY FLUCTUATIONS; DOPPLER SCINTILLATION; INTERPLANETARY DISTURBANCES; 0.3 AU; SPECTRUM; TURBULENCE; STREAMERS; SUN; SPEED; 1-AU AB Recent progress in our understanding of electron density fluctuations observed by radio occultation measurements has demonstrated that a break in the vicinity of 1 Hz in the temporal frequency spectrum of the density fluctuations provides a measure of the size of the finest filamentary structures in the solar corona. Breaks in frequency have been inferred from the density spectra deduced by Coles et al. from 1979-1980 Voyager phase scintillation and spectral broadening measurements. These results show that the finest filamentary structures are found in the extensions or stalks of coronal streamers-the likely sources of the slow solar wind-and are over a factor of 3 smaller than those in the fast wind emanating from coronal holes. The inferred sizes of the finest filamentary structures are approximately 6 km in the slow wind at 8 R. and 22 km in the fast wind at 9.1 R.. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Woo, R (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,MS 238-725,PASADENA,CA 91109, USA. NR 33 TC 48 Z9 48 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1997 VL 474 IS 2 BP L139 EP L142 DI 10.1086/310432 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC500 UT WOS:A1997WC50000016 ER PT J AU McCarthy, MC Travers, MJ Kalmus, P Gottlieb, CA Thaddeus, P AF McCarthy, MC Travers, MJ Kalmus, P Gottlieb, CA Thaddeus, P TI Microwave spectroscopy of the carbon chain radical C11H SO CHEMICAL PHYSICS LETTERS LA English DT Article ID MOLECULES; SUBSTITUTION; PARAMETERS; CLUSTER; SPECTRA AB The pure rotational spectrum of the carbon chain radical C11H has been observed in a pulsed supersonic molecular beam with a Fourier transform microwave spectrometer. Twelve rotational transitions in the frequency range 6-12 GHz, all split by lambda-type doubling and with resolved hyperfine structure in the lowest transitions, were assigned to C11H in its (II)-I-2 electronic ground state. Detection of this highly unsaturated reactive carbon chain establishes that linear radicals containing up to 11 carbon atoms are stable isomers. The density of C11H in our molecular jet is probably sufficiently high for detection of the electronic transitions of this radical by standard laser spectroscopic techniques. C1 HARVARD UNIV, DIV APPL SCI, CAMBRIDGE, MA 02138 USA. RP McCarthy, MC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 28 TC 10 Z9 10 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD JAN 3 PY 1997 VL 264 IS 1-2 BP 252 EP 256 DI 10.1016/S0009-2614(96)01242-0 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA WC716 UT WOS:A1997WC71600040 ER PT B AU Kalfatovic, MR DeHart, SG AF Kalfatovic, MR DeHart, SG BE Nixon, C Dengler, H Yersak, J TI Running to keep in place: Training library staff in information access SO 12TH ANNUAL COMPUTERS IN LIBRARIES '97, PROCEEDINGS LA English DT Proceedings Paper CT 12th Computers in Libraries Conference (CIL 97) CY MAR 10-12, 1997 CL ARLINGTON, VA SP Informat Today Inc C1 SMITHSONIAN INST LIB,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 0 PU INFORMATION TODAY INC PI MEDFORD PA 143 OLD MARLTON PIKE, MEDFORD, NJ 08055 BN 1-57387-040-4 PY 1997 BP 62 EP 65 PG 4 WC Information Science & Library Science SC Information Science & Library Science GA BJ45V UT WOS:A1997BJ45V00019 ER PT S AU Cranmer, SR Field, GB Noci, G Kohl, JL AF Cranmer, SR Field, GB Noci, G Kohl, JL BE Wilson, A TI The impact of UVCS/SOHO observations on models of ion-cyclotron resonance heating of the solar corona SO 31ST ESLAB SYMPOSIUM ON CORRELATED PHENOMENA AT THE SUN, IN THE HELIOSPHERE AND IN GEOSPACE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 31st ESLAB Symposium on Correlated Phenomena at the Sun, in the Heliosphere and in Geospace CY SEP 22-25, 1997 CL ESTEC, NOORDWIJK, NETHERLANDS SP ESA ESTEC HO ESTEC DE solar corona; solar wind; plasma physics AB We examine the compatibility between theoretical models and observations of the temperatures and anisotropic velocity distributions of hydrogen and minor ions in the solar corona. The UVCS instrument on board SOHO has measured hydrogen kinetic temperatures along lines of sight in coronal holes in excess of 3 x 10(6) K, and O+5 ion kinetic temperatures of at least 2 x 10(8) K. In addition, the velocity distributions in the radial direction (mainly perpendicular to the line of sight) are smaller, possibly implying temperature anisotropies of order T-perpendicular to/T-parallel to approximate to 100 for the oxygen ions. These properties can only be understood in terms of a mechanism which heats and accelerates heavier ions more than lighter ones (possibly proportionally to the ion mass to a power higher than unity), and preferentially in directions perpendicular to the magnetic field. We examine various features of plasma heating by the dissipation of high-frequency ion-cyclotron resonance Alfven waves, which may be the most natural physical mechanism to produce such plasma conditions. We present preliminary quantitative models of the ion motions in polar coronal holes, and show that such models can be used to predict the spectrum of waves required to reproduce the observations. Indeed, the more ionic species that are observed spectroscopically, the greater the extent in frequency space the wave spectrum can be inferred. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-660-0 J9 ESA SP PUBL PY 1997 VL 415 BP 89 EP 93 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK58J UT WOS:000072623300013 ER PT S AU Strachan, L Panasyuk, AV Fineschi, S Gardner, LD Raymond, JC Antonucci, E Giordano, S Romoli, M Noci, G Kohl, JL AF Strachan, L Panasyuk, AV Fineschi, S Gardner, LD Raymond, JC Antonucci, E Giordano, S Romoli, M Noci, G Kohl, JL BE Wilson, A TI Determination of 3D coronal structures from UVCS/SOHO synoptic observations SO 31ST ESLAB SYMPOSIUM ON CORRELATED PHENOMENA AT THE SUN, IN THE HELIOSPHERE AND IN GEOSPACE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 31st ESLAB Symposium on Correlated Phenomena at the Sun, in the Heliosphere and in Geospace CY SEP 22-25, 1997 CL ESTEC, NOORDWIJK, NETHERLANDS SP ESA ESTEC HO ESTEC DE solar corona; solar wind AB Daily coronal synoptic observations made with the Ultraviolet Coronagraph Spectrometer on SOHO (UVCS/SOHO) are used to create Carrington maps of line-of-sight intensities and spectral line widths for H I Lyman alpha and the O VI 1032/1037 doublet. These 2D maps can then be used as inputs to a tomographic inversion routine to produce 3D models of the corona out to 2.5 R. in the polar regions (3.0 R. in equatorial regions) The initial results for the determination of O5+ outflow velocities as a function of heliographic latitude is presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Strachan, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Romoli, Marco/H-6859-2012; OI Giordano, Silvio/0000-0002-3468-8566 NR 0 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-660-0 J9 ESA SP PUBL PY 1997 VL 415 BP 539 EP 542 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK58J UT WOS:000072623300087 ER PT B AU Narayan, R AF Narayan, R BE Wickramasinghe, DT Bicknell, GV Ferrario, L TI Advective disks SO ACCRETION PHENOMENA AND RELATED OUTFLOWS: IAU COLLOQUIUM 163 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 163 on Accretion Phenomena and Related Outflows CY JUL 15-19, 1996 CL PORT DOUGLAS, AUSTRALIA SP IAU AB Recent work on advection-dominated accretion flows (ADAFs) is reviewed. The article concentrates on an optically thin branch of ADAFs which is present at mass accretion rates below a critical value similar to (10(-2)-10(-1)) the Eddington rate. Models based on this branch have been quite successful at explaining a number of low-luminosity X-ray binaries and galactic nuclei, and some brighter systems. Some progress has also been made toward understanding the various spectral states of accreting black holes. It is argued that ADAFs may provide one of the best techniques for demonstrating the reality of event horizons in black holes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 9 Z9 9 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-41-4 J9 ASTR SOC P PY 1997 VL 121 BP 75 EP 89 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80B UT WOS:000073442600008 ER PT B AU Popham, R AF Popham, R BE Wickramasinghe, DT Bicknell, GV Ferrario, L TI Boundary layers in cataclysmic variables and pre-main-sequence stars SO ACCRETION PHENOMENA AND RELATED OUTFLOWS: IAU COLLOQUIUM 163 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 163 on Accretion Phenomena and Related Outflows CY JUL 15-19, 1996 CL PORT DOUGLAS, AUSTRALIA SP IAU AB The boundary layer region, where the accretion disk meets the accreting star, is crucial to understanding the spectra and evolution of accretion disk systems. Recent numerical modeling of the flow of the accreting material and radiation in the boundary layer has provided a better understanding of this region. I will describe the "standard" boundary layer structure predicted by the models for the case where the boundary layer is optically thick and geometrically thin in the vertical direction. Large variations in this structure can occur when the boundary layer becomes optically thin or geometrically thick. Boundary layer models have been applied to cataclysmic variables and accreting pre-main-sequence stars. I will discuss the boundary layer spectra predicted by the models and how well they agree with observations of these objects. The boundary layer also controls the transfer of angular momentum and energy between the disk and star. This can have important effects upon pre-main-sequence stellar evolution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Popham, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. NR 0 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-41-4 J9 ASTR SOC P PY 1997 VL 121 BP 230 EP 240 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80B UT WOS:000073442600025 ER PT B AU Esin, AA AF Esin, AA BE Wickramasinghe, DT Bicknell, GV Ferrario, L TI Heating and cooling of hot accretion flows by non local radiation SO ACCRETION PHENOMENA AND RELATED OUTFLOWS: IAU COLLOQUIUM 163 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Meeting Abstract CT IAU Colloquium 163 on Accretion Phenomena and Related Outflows CY JUL 15-19, 1996 CL PORT DOUGLAS, AUSTRALIA SP IAU C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-41-4 J9 ASTR SOC P PY 1997 VL 121 BP 700 EP 700 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80B UT WOS:000073442600104 ER PT B AU Garcia, MR Callanan, PJ AF Garcia, MR Callanan, PJ BE Wickramasinghe, DT Bicknell, GV Ferrario, L TI Optical and IR observations of Aql X-1 SO ACCRETION PHENOMENA AND RELATED OUTFLOWS: IAU COLLOQUIUM 163 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 163 on Accretion Phenomena and Related Outflows CY JUL 15-19, 1996 CL PORT DOUGLAS, AUSTRALIA SP IAU AB We have obtained optical spectra and IR photometry in an attempt to determine the orbital parameters of the Aq1 X-l system. Spectra from the MMT in October 1995 appear to detect the secondary, but are not sufficient to measure the mass function. IR photometry in and out of mini-outburst find K similar to 15.4, and may indicate that the disk contribution at It is modest during the mini-outburst. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Garcia, MR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-41-4 J9 ASTR SOC P PY 1997 VL 121 BP 705 EP 706 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80B UT WOS:000073442600108 ER PT B AU Schlegel, EM Mukai, K Ishida, M AF Schlegel, EM Mukai, K Ishida, M BE Wickramasinghe, DT Bicknell, GV Ferrario, L TI ASCA observations of the eclipsing IP XY Ari SO ACCRETION PHENOMENA AND RELATED OUTFLOWS: IAU COLLOQUIUM 163 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Meeting Abstract CT IAU Colloquium 163 on Accretion Phenomena and Related Outflows CY JUL 15-19, 1996 CL PORT DOUGLAS, AUSTRALIA SP IAU C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-41-4 J9 ASTR SOC P PY 1997 VL 121 BP 794 EP 794 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80B UT WOS:000073442600157 ER PT B AU Siemiginowska, A AF Siemiginowska, A BE Wickramasinghe, DT Bicknell, GV Ferrario, L TI Accretion disk instabilities and the quasar luminosity function SO ACCRETION PHENOMENA AND RELATED OUTFLOWS: IAU COLLOQUIUM 163 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 163 on Accretion Phenomena and Related Outflows CY JUL 15-19, 1996 CL PORT DOUGLAS, AUSTRALIA SP IAU AB We predict the quasar luminosity function (LF) from a population of sources with the activity driven by instabilities in an accretion disk. The ligth curve of a single source convolved with the mass distribution gives the quasar luminosity function at a given redshift. We model the observed LF at four different redshifts. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-41-4 J9 ASTR SOC P PY 1997 VL 121 BP 795 EP 796 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80B UT WOS:000073442600158 ER PT B AU Zhang, X AF Zhang, X BE Wickramasinghe, DT Bicknell, GV Ferrario, L TI A new physical mechanism to account for the "anomalous viscosity" in accretion disks SO ACCRETION PHENOMENA AND RELATED OUTFLOWS: IAU COLLOQUIUM 163 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 163 on Accretion Phenomena and Related Outflows CY JUL 15-19, 1996 CL PORT DOUGLAS, AUSTRALIA SP IAU AB A new physical mechanism responsible for producing significant radial mass accretion in the inner disk of spiral galaxies has recently been found (Zhang 1996, ApJ, 457, 125). Since this mechanism depends only on the skewness of the global patterns (one-armed or two-armed spiral patterns, as well as skewed central bars) in the underlying disks, and since this process is collective in nature and produces an effective viscosity many orders of magnitude larger than that due to the microscopic processes, it is likely to be an important candidate for the long sought-after "anomalous viscosity" in many types of astrophysical accretion disks which admit nonaxisymmetric instabilities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-41-4 J9 ASTR SOC P PY 1997 VL 121 BP 840 EP 841 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80B UT WOS:000073442600182 ER PT J AU Udalski, A Olech, A Szymanski, M Kaluzny, J Kubiak, M Mateo, M Krzeminski, W Stanek, KZ AF Udalski, A Olech, A Szymanski, M Kaluzny, J Kubiak, M Mateo, M Krzeminski, W Stanek, KZ TI The optical gravitational lensing experiment. The catalog of periodic variable stars in the galactic bulge .5. Periodic variables in fields: MM5-A, MM5-B, MM7-A and MM7-B SO ACTA ASTRONOMICA LA English DT Article DE catalogs; stars, variables AB We present the fifth part of the OGLE Catalog of Periodic Variable Stars in the Galactic bulge. 574 variable stars: 44 pulsating, 369 eclipsing and 161 miscellaneous type were detected in four fields located symmetrically in galactic lattitude around the Galactic center: MMS-A, MM5-B, MM7-A and MM7-B. The Catalog and individual observations are available in digital form from the OGLE Internet archive. C1 UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. CARNEGIE OBSERV,LAS CAMPANAS OBSERV,LA SERENA,CHILE. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Udalski, A (reprint author), UNIV WARSAW OBSERV,AL UJAZDOWSKIE 4,PL-00478 WARSAW,POLAND. NR 8 TC 44 Z9 44 U1 0 U2 0 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 1997 VL 47 IS 1 BP 1 EP 167 PG 167 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WY715 UT WOS:A1997WY71500001 ER PT J AU Udalski, A Szymanski, M Kaluzny, J Kubiak, M Mateo, M Krzeminski, W Stanek, KZ AF Udalski, A Szymanski, M Kaluzny, J Kubiak, M Mateo, M Krzeminski, W Stanek, KZ TI The Optical Gravitational Lensing Experiment. Journal of the 1995 observing season SO ACTA ASTRONOMICA LA English DT Article DE surveys; techniques, photometric AB We present the journal of the fourth - 1995 OGLE observing season. Logs and statistics of the main microlensing search and side projects are provided. C1 UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. CARNEGIE OBSERV,LAS CAMPANAS OBSERV,LA SERENA,CHILE. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Udalski, A (reprint author), UNIV WARSAW OBSERV,AL UJAZDOWSKIE 4,PL-00478 WARSAW,POLAND. NR 13 TC 17 Z9 17 U1 0 U2 0 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 1997 VL 47 IS 1 BP 169 EP 182 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WY715 UT WOS:A1997WY71500002 ER PT S AU Egloff, DA Fofonoff, PW Onbe, T AF Egloff, DA Fofonoff, PW Onbe, T BE Blaxter, JHS Southward, AJ TI Reproductive biology of marine cladocerans SO ADVANCES IN MARINE BIOLOGY, VOL 31 SE Advances in Marine Biology LA English DT Review ID DAPHNIA-MAGNA CRUSTACEA; AUSTRALIAN SALT LAKES; EGG AGE DISTRIBUTION; PENILIA-AVIROSTRIS; BYTHOTREPHES-CEDERSTROEMI; RESTING EGGS; VERTICAL DISTRIBUTIONS; CYCLIC PARTHENOGEN; SEASONAL DYNAMICS; PODON-SCHMACKERI C1 SMITHSONIAN ENVIRONM RES CTR, EDGEWATER, MD 21037 USA. HIROSHIMA UNIV, FAC APPL BIOL SCI, HIGASHIHIROSHIMA 739, JAPAN. RP Egloff, DA (reprint author), OBERLIN COLL, DEPT BIOL, OBERLIN, OH 44074 USA. NR 257 TC 46 Z9 50 U1 1 U2 9 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA SN 0065-2881 BN 0-12-026131-6 J9 ADV MAR BIOL JI Adv. Mar. Biol. PY 1997 VL 31 BP 79 EP 167 DI 10.1016/S0065-2881(08)60222-9 PG 89 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BH28M UT WOS:A1997BH28M00002 ER PT J AU Rogers, JD AF Rogers, JD TI Beyond subsistence: Plains archaeology and the postprocessual critique - Duke,P, Wilson,MC SO AMERICAN ANTIQUITY LA English DT Book Review RP Rogers, JD (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE WASHINGTON, DC 20002-3557 SN 0002-7316 J9 AM ANTIQUITY JI Am. Antiq. PD JAN PY 1997 VL 62 IS 1 BP 159 EP 160 DI 10.2307/282396 PG 2 WC Anthropology; Archaeology SC Anthropology; Archaeology GA WD770 UT WOS:A1997WD77000021 ER PT J AU Tilden, CD Oftedal, OT AF Tilden, CD Oftedal, OT TI Milk composition reflects pattern of maternal care in prosimian primates SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE prosimians; milk composition; nursing; lactation; maternal care ID LEMURS VARECIA-VARIEGATA; LACTATION; BEHAVIOR; SEALS; FOREST; YIELD; YOUNG AB Hypothesized relationships between milk composition and life history traits were examined by analyzing mid-lactation milks of seven lemurs (Eulemur fulvus, E. macaco, E. rubriventer E. mongoz, Varecia variegata, Hapalemur griseus, Lemur catta), three bushbabies (Otolemur crassicaudatus, O. garnettii, Galago moholi), and two lorises (Nycticebus coucang, Loris tardigradus); partial data were also obtained far the lemuroid Cheirogaleus medius. There were no significant differences in milk composition among species within either Eulemur or Otolemur, but the four genera for which multiple samples were available (Eulemur, Varecia, Otolemur, and Nycticebus) exhibited large composition differences. Eulemur milk was, on average, very dilute (9.9% dry matter) and low in energy (0.49 kcal/g). These milks contained 0.9% fat, 1.2% protein, and 8.4% carbohydrate on a fresh weight basis. Protein energy comprised only about 15% of total milk energy. Varecia had significantly higher dry matter (13.5%), fat (3.2%), protein (4.2%), gross energy (0.80 kcal/g), and protein energy:total energy ratio (28%) than Eulemur. Milks of the lorisoid genera Otolemur and Nycticebus were very similar, and both had significantly higher dry matter(18.3, 16.3%), fat (7.6, 7.0%), and gross energy concentration (1.27, 1.13 kcal/g) than either lemuroid genus. Otolemur milk was higher in protein than Nycticebus milk. We conclude that lorises, bushbabies, and perhaps cheirogaleids produce relatively rich, energy-dense milks in comparison with anthropoid primates. However, dilute milks appear to be uniformly found among species of Eulemur and perhaps in Lemur catta. The milk of Varecia (and perhaps Hapalemur) is intermediate in composition. Differences in milk composition among prosimians may be related to differences in maternal care: prosimians that carry their young during lactation produce more dilute milks than do species which leave their young unattended for prolonged periods. When looking at primates as a whole, however, the picture is somewhat less clear, since the milks of some ''parkers'' like Varecia do closely resemble those of large anthropoid primates who carry their young. (C) 1997 Wiley-Liss, Inc. C1 DUKE UNIV,DEPT BIOL ANTHROPOL & ANAT,DURHAM,NC 27706. SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. NR 71 TC 56 Z9 59 U1 2 U2 16 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PY 1997 VL 41 IS 3 BP 195 EP 211 PG 17 WC Zoology SC Zoology GA WK680 UT WOS:A1997WK68000003 PM 9057965 ER PT J AU Tommasini, PRI Piza, AFRD AF Tommasini, PRI Piza, AFRD TI Non-ideal Boson system in the Gaussian approximation SO ANNALS OF PHYSICS LA English DT Article ID DEPENDENT VARIATIONAL PRINCIPLE; EINSTEIN CONDENSATION; FIELD-THEORY; MODEL; GAS AB We investigate ground-stale and thermal properties of a system of non-relativistic bosons interacting through repulsive, two-body interactions in-a self-consistent Gaussian mean-held approximation which consists in writing the variationally determined density operator as the most general Gaussian functional of the quantized field operators. Finite temperature results are obtained in a grand canonical framework. Contact is made with the results of Let, Yang, and Huang in terms of particular truncations of the Gaussian approximation. The Full Gaussian approximation supports a Free phase or a thermodynamically unstable phase when contact Forces and a standard renormalization scheme are used. When applied to a Hamiltonian with zero range forces interpreted as an effective theory with a high momentum cutoff, the full Gaussian approximation generates a quasi-particle spectrum having an energy gap, in conflict with perturbation theory results. (C) 1997 Academic Press C1 UNIV SAO PAULO,INST FIS,BR-05389970 SAO PAULO,BRAZIL. RP Tommasini, PRI (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138, USA. NR 28 TC 7 Z9 7 U1 0 U2 0 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0003-4916 J9 ANN PHYS-NEW YORK JI Ann. Phys. PD JAN 1 PY 1997 VL 253 IS 1 BP 198 EP 218 DI 10.1006/aphy.1997.5625 PG 21 WC Physics, Multidisciplinary SC Physics GA WD771 UT WOS:A1997WD77100006 ER PT J AU Engel, MS Schultz, TR AF Engel, MS Schultz, TR TI Phylogeny and behavior in honey bees (Hymenoptera: Apidae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Apis; honey bees; dance language; nest architecture; phylogeny ID APIS-VECHTI MAA; GENUS-APIS; PERMUTATION TESTS; SEQUENCE; INFORMATION; CLADISTICS; CONGRUENCE; EVOLUTION; TREES; DRONE AB Methods for distinguishing phylogenetic signal from noise are employed to resolve conflicting phylogenies produced by 3 separate morphological and molecular data sets for the 6 species of the honey bee genus Apis. Morphological data from larvae are employed for the 1st time. The results support the phylogeny produced by separate analyses of the morphological and mitochondrial 16s ribosomal DNA (rDNA) data sets, and contradict the result produced by the mitochondrial COII data set. Additionally, these results support previous conclusions that 16s rDNA sequence data are more informative for species-level rather than tribal-level relationships in the corbiculate bees. Resolution of Apis phylogeny permits for the 1st time unambiguous reconstruction of the ancestral states for several important behavioral characters in honey bee evolution. C1 SMITHSONIAN INST, DEPT ENTOMOL, MUSEUM NATL HIST NAT, WASHINGTON, DC 20560 USA. RP Engel, MS (reprint author), CORNELL UNIV, DEPT ENTOMOL, COMSTOCK HALL, ITHACA, NY 14853 USA. RI Engel, Michael/C-5461-2012 OI Engel, Michael/0000-0003-3067-077X NR 82 TC 37 Z9 37 U1 0 U2 17 PU ENTOMOLOGICAL SOC AMER PI ANNAPOLIS PA 3 PARK PLACE, STE 307, ANNAPOLIS, MD 21401-3722 USA SN 0013-8746 EI 1938-2901 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD JAN PY 1997 VL 90 IS 1 BP 43 EP 53 PG 11 WC Entomology SC Entomology GA WE434 UT WOS:A1997WE43400004 ER PT J AU Soltis, DE Soltis, PS Nickrent, DL Johnson, LA Hahn, WJ Hoot, SB Sweere, JA Kuzoff, RK Kron, KA Chase, MW Swensen, SM Zimmer, EA Chaw, SM Gillespie, LJ Kress, WJ Sytsma, KJ AF Soltis, DE Soltis, PS Nickrent, DL Johnson, LA Hahn, WJ Hoot, SB Sweere, JA Kuzoff, RK Kron, KA Chase, MW Swensen, SM Zimmer, EA Chaw, SM Gillespie, LJ Kress, WJ Sytsma, KJ TI Angiosperm phylogeny inferred from 18S ribosomal DNA sequences SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Review ID RNA GENE-SEQUENCES; SEED PLANT PHYLOGENY; COMPLETE NUCLEOTIDE-SEQUENCE; CLADISTIC-ANALYSIS; MOLECULAR PHYLOGENY; RBCL SEQUENCES; EVOLUTIONARY HISTORY; SECONDARY STRUCTURE; TAXONOMIC ANALYSIS; FLOWERING PLANTS AB Parsimony analyses were conducted for 223 species representing all major groups of angiosperms using entire 18S ribosomal DNA (rDNA) sequences. Although no search swapped to completion, the topologies recovered are highly concordant with those retrieved via broad analyses based on the chloroplast gene rbcL. The general congruence of 18S rDNA and rbcL topologies further clarifies the broad picture of angiosperm phylogeny. In all analyses, the first-branching angiosperms are Amborellaceae, Austrobaileyaceae, Illiciaceae, and Schisandraceae, all woody magnoliids. These taxa are always followed by the paleoherb family Nymphaeaceae. This same general order of early-branching taxa is preserved with several suites of outgroups. In most searches, the remaining early-branching taxa represent Piperales and other orders of subclass Magnoliidae (sensu Cronquist). With the exception of Acorus, the monocots are supported as monophyletic and typically have as their sister Ceratophyllum. In most analyses, taxa with uniaperturate pollen form a grade at the base of the angiosperms; a large eudicot clade is composed primarily of taxa having triaperturate pollen. Two large subclades are present within the eudicots, one consisting largely of Rosidae and a second corresponding closely to Asteridae sensu late. Subclasses Dilleniidae and Hamamelidae are highly polyphyletic. These data sets of 185 rDNA sequences also permit an analysis of the patterns of molecular evolution of this gene. Problems deriving from both the prevalence of indels and uncertain alignment of 18S rDNA sequences have been overstated in previous studies. With the exception of a few well-defined regions, insertions and deletions are relatively uncommon in 18S rDNA; sequences are therefore easily aligned by eye across the angiosperms. Indeed, several indels in highly conserved regions appear to be phylogenetically informative. Initial analyses suggest that both stem and loop bases are important sources of phylogenetic information, although stem positions are prone to compensatory substitutions. Of the stem changes analyzed, only 27% destroy a base-pairing couplet; 73% maintain or restore base pairing. C1 SO ILLINOIS UNIV, DEPT PLANT BIOL, CARBONDALE, IL 62901 USA. SMITHSONIAN INST, LAB MOL SYSTEMAT, WASHINGTON, DC 20560 USA. UNIV WISCONSIN, DEPT BIOL SCI, MILWAUKEE, WI 53201 USA. WAKE FOREST UNIV, DEPT BIOL, WINSTON SALEM, NC 27109 USA. ROYAL BOT GARDENS, LAB MOL SYSTEMAT, RICHMOND TW9 3AB, SURREY, ENGLAND. ITHACA COLL, DEPT BIOL, ITHACA, NY 14850 USA. ACAD SINICA, INST BOT, NANKANG, TAIPEI, TAIWAN. CANADIAN MUSEUM NAT, DIV RES, OTTAWA, ON K1P 64P, CANADA. SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT BOT, WASHINGTON, DC 20560 USA. UNIV WISCONSIN, DEPT BOT, MADISON, WI 53706 USA. RP Soltis, DE (reprint author), WASHINGTON STATE UNIV, DEPT BOT, PULLMAN, WA 99164 USA. RI Chase, Mark /A-6642-2011; Zimmer, Elizabeth/G-3890-2011; Soltis, Pamela/L-5184-2015 NR 117 TC 344 Z9 359 U1 2 U2 16 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 1997 VL 84 IS 1 BP 1 EP 49 DI 10.2307/2399952 PG 49 WC Plant Sciences SC Plant Sciences GA WL514 UT WOS:A1997WL51400001 ER PT J AU Robinson, H Carr, GD King, RM Powell, AM AF Robinson, H Carr, GD King, RM Powell, AM TI Chromosome numbers in compositae, XVII: Senecioneae III SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article ID CHLOROPLAST DNA EVIDENCE; ASTERACEAE; EUPATORIEAE; WORLD AB A brief review is offered of major chromosome number variations in the Senecioneae based on recent delimitations of the tribe. An additional 78 chromosome reports are provided, including 19 new reports for species, with confirmed or expanded base numbers for the genera Gynoxys (x = 40), Lasiocephalus (x = 20), Pentacalia (x = 20, ca. 50), and Jessea (x = ca. 50). The base number for the tribe is x = 10, which is found in various multiples. The Blennospermatinae are one of the most distinct groups with a base of x = 9, considered an aneuploid reduction from x = 10. A new subtribe, Abrotanellinae, is established for the southern South American and southwest Pacific genus Abrotanella, which also has x = 9 and has often been placed in the Blennospermatinae. Numbers based on x = 30 and aneuploid reductions are found in the Tussilagininae, in many Australian Senecio, and in the Macaronesian Pericallis of the Senecioninae. The origin of such numbers is discussed. An anomalous North American group of Senecio (Packera) has variable numbers mostly near n = 23. Most Western Hemisphere Senecioninae have numbers of n = 20 or multiples thereof, with higher numbers in many Andean groups. Numbers of n = 10 or lower are mostly restricted to the Eastern Hemisphere, and groups like Emilia have recently dispersed from that area. Occurrences of n = 5 in Emilia, n = 10 in some American and Australian Senecio, and n = 14-16 in some tussilaginoids are considered as reductions. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA. Sul Ross State Univ, Dept Biol, Alpine, TX 79832 USA. RP Robinson, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. NR 95 TC 20 Z9 21 U1 2 U2 6 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 1997 VL 84 IS 4 BP 893 EP 906 DI 10.2307/2992034 PG 14 WC Plant Sciences SC Plant Sciences GA YR994 UT WOS:000071553500009 ER PT J AU Segall, P Davis, JL AF Segall, P Davis, JL TI GPS applications for geodynamics and earthquake studies SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES LA English DT Review DE crustal deformation; plate motions; volcanos; space geodesy; postglacial rebound ID GLOBAL POSITIONING SYSTEM; 1989 LOMA-PRIETA; CRUSTAL DEFORMATION MEASUREMENTS; ATMOSPHERIC MODELING ERRORS; BASE-LINE INTERFEROMETRY; CURRENT PLATE MOTIONS; 28 JUNE 1992; LANDERS EARTHQUAKE; WATER-VAPOR; GEODETIC MEASUREMENTS AB Geodetic measurements obtained with the Global Positioning System (GPS) are increasingly more widely applied in geophysical studies. In this paper, we review the changes to the technology of GPS geodesy over the last five years that are responsible for this increased applicability. We survey geophysical investigations employing GPS to measure coseismic, postseismic, and interseismic deformation; plate motion and crustal deformation at plate boundaries; volcano deformation; and the deformation associated with glacial isostatic adjustment and its application to sea-level studies. We emphasize the use of GPS determinations for the modeling of this wide variety of geophysical phenomena. We also discuss the recent advent of permanent GPS networks for regional geophysical studies, as well as the possible future of GPS surveying in light of the recent advances. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Segall, P (reprint author), STANFORD UNIV, DEPT GEOPHYS, STANFORD, CA 94305 USA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 119 TC 114 Z9 122 U1 3 U2 12 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0084-6597 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 1997 VL 25 BP 301 EP 336 DI 10.1146/annurev.earth.25.1.301 PG 36 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA XB772 UT WOS:A1997XB77200010 ER PT J AU Labandeira, CC AF Labandeira, CC TI Insect mouthparts: Ascertaining the paleobiology of insect feeding strategies SO ANNUAL REVIEW OF ECOLOGY AND SYSTEMATICS LA English DT Review DE mouthpart class; functional feeding group; dietary guild; morphological data; ecological attributes; mouthpart classes; fossil record; plant-insect interactions ID CAMPESTRIS MCDUNNOUGH EPHEMEROPTERA; BIVITTATUM MALLOCH DIPTERA; PRIMITIVE ANGIOSPERMS; REPRODUCTIVE-BIOLOGY; SOUTHERN AFRICA; PERMIAN DIAPHANOPTERODEA; FUNCTIONAL-MORPHOLOGY; EXTRAFLORAL NECTARIES; RELATIVE IMPORTANCE; FOSSIL EVIDENCE AB One of the most intensively examined and abundantly documented structures in the animal world is insect mouthparts. Major structural types of extant insect mouthparts are extensive, consisting of diverse variations in element structure within each of the five mouthpart regions-labrum, hypopharynx, mandibles, maxillae, and labium. Numerous instances of multielement fusion both within and among mouthpart regions result in feeding organs capable of ingesting in diverse ways foods that are solid, particulate, and liquid in form. Mouthpart types have a retrievable and interpretable fossil history in well-preserved insect deposits. In addition, the trace-fossil record of insect-mediated plant damage, gut contents, coprolites, and insect-relevant floral features provides complementary data documenting the evolution of feeding strategies during the past 400 million years. From a cluster analysis of insect mouthparts, I recognize 34 fundamental mouthpart classes among extant insects and their geochronological evolution by a five-phase pattern. This pattern is characterized, early in the Devonian, by coarse partitioning of food by mandibulate and piercing-and-sucking mouthpart classes, followed by a rapid rise in herbivore mouthpart types for fluid-and solid-feeding during the Late Carboniferous and Early Permian. Mouthpart innovation during the Late Triassic to Early Jurassic added mouthpart classes for fluid and aquatic particle-feeding. This ecomorphological expansion of mouthpart design was associated with the radiation of holometabolous insects, especially Diptera. The final phase of mouthpart class expansion occurred during the Late Jurassic and Early Cretaceous, with addition of surface-fluid-feeding mouthpart classes that subsequently became important during the ecological expansion of angiosperms. Conclusions about the evolution of mouthpart design are based on the mapping of phenetic mouthpart classes onto (ideally) cladistic phylogenies of lineages bearing those same mouthpart classes. The plotting of phenetic and associated ecological attributes onto baseline phylogenies is one of the most important uses of cladistic data. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol, Washington, DC 20560 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol, Washington, DC 20560 USA. EM labandeira.conrad@simnh.si.edu NR 367 TC 124 Z9 131 U1 4 U2 44 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4162 J9 ANNU REV ECOL SYST JI Annu. Rev. Ecol. Syst. PY 1997 VL 28 BP 153 EP 193 DI 10.1146/annurev.ecolsys.28.1.153 PG 41 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA YL493 UT WOS:000070961400007 ER PT J AU Drake, BG GonzalezMeler, MA Long, SP AF Drake, BG GonzalezMeler, MA Long, SP TI More efficient plants: A consequence of rising atmospheric CO2? SO ANNUAL REVIEW OF PLANT PHYSIOLOGY AND PLANT MOLECULAR BIOLOGY LA English DT Review DE CO2 and plants; CO2 and photosynthesis; CO2 and stomata; CO2 and respiration; plants and climate change ID CARBON-DIOXIDE ENRICHMENT; LONG-TERM EXPOSURE; RIBULOSE-1,5-BISPHOSPHATE CARBOXYLASE-OXYGENASE; LEAF GAS-EXCHANGE; LIRIODENDRON-TULIPIFERA L; SOURCE-SINK RELATIONS; WATER-USE EFFICIENCY; PHASEOLUS-VULGARIS L; BETULA-PENDULA ROTH; ELEVATED CO2 AB The primary effect of the response of plants to rising atmospheric CO2 (C-a) is to increase resource use efficiency. Elevated C-a reduces stomatal conductance and transpiration and improves water use efficiency, and at the same time it stimulates higher rates of photosynthesis and increases light-use efficiency. Acclimation of photosynthesis during long-term exposure to elevated C-a reduces key enzymes of the photosynthetic carbon reduction cycle, and this increases nutrient use efficiency. Improved soil-water balance, increased carbon uptake in the shade, greater carbon to nitrogen ratio, and reduced nutrient quality for insect and animal grazers are all possibilities that have been observed in field studies of the effects of elevated C-a. These effects have major consequences for agriculture and native ecosystems in a world of rising atmospheric C-a and climate change. C1 UNIV ESSEX, JOHN TABOR LABS, DEPT CHEM & BIOL SCI, COLCHESTER CO4 3SQ, ESSEX, ENGLAND. RP Drake, BG (reprint author), SMITHSONIAN ENVIRONM RES CTR, POB 28, EDGEWATER, MD 21037 USA. RI Long, Stephen/A-2488-2008; OI Long, Stephen/0000-0002-8501-7164; Gonzalez-Meler, Miquel/0000-0001-5388-7969 NR 251 TC 1071 Z9 1151 U1 74 U2 551 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1040-2519 J9 ANNU REV PLANT PHYS JI Annu. Rev. Plant Physiol. Plant Molec. Biol. PY 1997 VL 48 BP 609 EP 639 DI 10.1146/annurev.arplant.48.1.609 PG 31 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA XD140 UT WOS:A1997XD14000024 ER PT J AU Goddard, I AF Goddard, I TI Mythology of the Lenape. Guide and texts - Bierhorst,J SO ANTHROPOS LA English DT Book Review RP Goddard, I (reprint author), SMITHSONIAN INST,10TH & CONSTITUT AVE,NHB 85,MRC 100,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU ANTHROPOS INST PI FIBOURG PA EDITIONS ST-PAUL, PEROLLES 42, CH-1700 FIBOURG, SWITZERLAND SN 0257-9774 J9 ANTHROPOS JI Anthropos PY 1997 VL 92 IS 1-3 BP 217 EP 218 PG 2 WC Anthropology SC Anthropology GA WL885 UT WOS:A1997WL88500026 ER PT J AU Ward, DC AF Ward, DC TI Handwriting in America: a cultural history SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Book Review C1 Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. RP Ward, DC (reprint author), Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 1997 VL 37 IS 1-2 BP 23 EP 26 PG 4 WC Art SC Art GA 135PK UT WOS:000076811400005 ER PT J AU Ward, DC AF Ward, DC TI At beck and call: The representation of domestic servants in Nineteenth century American painting SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Book Review C1 Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. RP Ward, DC (reprint author), Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 1997 VL 37 IS 1-2 BP 23 EP 26 PG 4 WC Art SC Art GA 135PK UT WOS:000076811400004 ER PT J AU Krupnik, I Vakhtin, N AF Krupnik, I Vakhtin, N TI Indigenous knowledge in modern culture: Siberian Yupik ecological legacy in transition SO ARCTIC ANTHROPOLOGY LA English DT Article AB This article presents results of the survey of Siberian Yupik ecological knowledge conducted in Chukotka in 1995 as part of the project ''Environmental Change and Indigenous Knowledge in Siberia and Alaska.'' The study was aimed at documenting indigenous knowledge in transition, as it is currently shared by modern people of various backgrounds and age groups. As the interviews reveal, current transformation of indigenous ecological knowledge does not progress in direct conjunction with the loss of Native language nor with the extension of formal schooling, Actually, it creates a sort of ''mixed culture'' where certain traditional ideas and beliefs are reinterpreted and reformulated from the perspectives of other culture. As such, the expertise in Yupik knowledge (unlike expertise in Native language) often becomes a matter of individual choice and of personal drive and interest in one's Native tradition. This opens up the prospect of renewed strength and even of revival of Yupik ecological knowledge via the cultural revitalization movement which is currently taking place in Chukotka and elsewhere in the Arctic. C1 EUROPEAN UNIV ST PETERSBURG,ST PETERSBURG 191187,RUSSIA. RP Krupnik, I (reprint author), SMITHSONIAN INST,ARCTIC STUDIES CTR,WASHINGTON,DC 20560, USA. NR 52 TC 12 Z9 15 U1 3 U2 9 PU UNIV WISCONSIN PRESS PI MADISON PA JOURNAL DIVISION, 114 N MURRAY ST, MADISON, WI 53715 SN 0066-6939 J9 ARCTIC ANTHROPOL JI Arct. Anthropol. PY 1997 VL 34 IS 1 BP 236 EP 252 PG 17 WC Anthropology SC Anthropology GA XK884 UT WOS:A1997XK88400018 ER PT J AU Melchionne, K AF Melchionne, K TI Re-thinking site-specificity: Some critical and philosophical problems (Art display) SO ART CRITICISM LA English DT Article C1 Smithsonian Inst, Amer Museum Nat Art, Washington, DC 20560 USA. RP Melchionne, K (reprint author), Smithsonian Inst, Amer Museum Nat Art, Washington, DC 20560 USA. NR 16 TC 1 Z9 1 U1 0 U2 0 PU SUNY-STATE UNIV NY STONY BROOK PI STONY BROOK PA DEPT ART, STONY BROOK, NY 11794-5400 USA SN 0195-4148 J9 ART CRITICISM JI Art Crit. PY 1997 VL 12 IS 2 BP 36 EP 49 PG 14 WC Art SC Art GA YU970 UT WOS:000071775400004 ER PT B AU Tokarz, SP Roll, J AF Tokarz, SP Roll, J BE Hunt, G Payne, HE TI RoadRunner: An automated reduction system for long slit spectroscopic data SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB Driven by a dramatic, almost fivefold, increase in data flow, we developed a system, RoadRunner,(1) for the automatic and rapid reduction of CCD two-dimensional long slit data taken at the 1.5 meter telescope at the Fred L. Whipple Observatory on Mt. Hopkins. The typical 70 to 100 observations made in an average night are now routinely reduced in a few hours the following day. The reduction process takes the data from raw two-dimensional images to one-dimensional wavelength calibrated spectra with measured redshifts which have been checked for accuracy. The reduced spectra are stored in an on-line archive and are entered into a relational database. Standardizing observing protocols proved to be a requirement for designing an automated reduction system. RoadRunner, which is based on IRAF data reduction routines, has many internal checks for errors and anomalies and produces a data set of high quality. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Tokarz, SP (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 21 Z9 21 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 140 EP 143 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100033 ER PT B AU Stern, I AF Stern, I BE Hunt, G Payne, HE TI On fractal modeling in astrophysics: The effect of lacunarity on the convergence of algorithms for scaling exponents SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB Fractals and multifractals are used to model hierarchical, inhomogeneous structures in several areas of astrophysics, notably the distribution of matter at various scales in the universe. Current analysis techniques used to assert fractality or multifractality and extract scaling exponents from astrophysical data, however, have significant limitations and caveats. It is pointed out that some of the difficulties regarding the convergence rates of algorithms used to determine scaling exponents for a fractal or multifractal, are intrinsically related to its texture, in particular, to its lacunarity. A novel approach to characterize prefactors of cover functions, in particular, lacunarity, based on the formalism of regular variation (in the sense of Karasnata) is proposed. This approach allows deriving bounds on convergence rates for scaling exponent algorithms and may provide more precise characterizations for fractal-like objects of interest for astrophysics. An application of regular variation based fractal modeling to apollonian packing, which can be useful in cosmic voids morphology modeling, is also suggested. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Stern, I (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 2 Z9 2 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 222 EP 225 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100051 ER PT B AU Mink, DJ AF Mink, DJ BE Hunt, G Payne, HE TI WCSTools: Image world coordinate system utilities SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB The WCSTools are portable C utility programs and subroutines for setting and using the world coordinate system (WCS) of a FITS or IRAF image. The WCS describes the relationship between sky coordinates, such as right ascension and declination, and image pixels, and can be described using standard keywords in an image header. The subroutine library is currently used by the image display and browsing programs SAOimage, SAOtng, and Skycat to translate between image pixels and sky coordinates. Some subroutines have been improved and new ones have been added to read and write all legal FITS image data types and to deal with IRAF .imh (OIF) files as easily as FITS files. The programs in this package set the WCS of an image, convert between pixel and sky coordinates in an image, and find catalog stars in the region of the sky which the image covers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mink, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 32 Z9 32 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 249 EP 252 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100057 ER PT B AU Accomazzi, A Eichhorn, G Kurtz, MJ Grant, CS Murray, SS AF Accomazzi, A Eichhorn, G Kurtz, MJ Grant, CS Murray, SS BE Hunt, G Payne, HE TI Astronomical information discovery and access: Design and implementation of the ADS bibliographic services SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB The NASA Astrophysics Data System integrates a wealth of scientific bibliographic and data resources-originally generated in multiple formats and available from multiple providers-in three discipline-oriented, centralized databases. Search and retrieval of the bibliographies and data sources is possible via a set of World Wide Web forms and interface programs that transparently link the ADS's resources to those of other data providers. The approach followed in designing the ADS system is offered as a paradigm for building flexible networked information and discovery systems. The rationale behind the current technical implementation and the planned enhancements of the system are also discussed. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Accomazzi, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009; KURTZ, Michael /B-3890-2009 OI Eichhorn, Guenther/0000-0002-3032-1978; NR 0 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 357 EP 360 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100084 ER PT B AU Conroy, M Joye, W Herrero, J Doe, S Mistry, A AF Conroy, M Joye, W Herrero, J Doe, S Mistry, A BE Hunt, G Payne, HE TI ASC data analysis architecture SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB The AXAF Science Center (ASC) is using an "open architecture" approach to develop its data analysis environment. The system is a loosely coupled environment consisting of several major applications: visualizer, browser, fitter/modeler, as well as the data analysis tool-box. The ASC Data Model and Interprocess Communications (IPC) provide the data interface between applications and tools. The Navigator, CLI, and Profile Editor provide the user with different control methods to access these components. The modular design provides a flexible, configurable environment in which the user can create customized applications from the standard components. C1 Smithsonian Astrophys Observ, AXAF Sci Ctr, Cambridge, MA 02138 USA. RP Conroy, M (reprint author), Smithsonian Astrophys Observ, AXAF Sci Ctr, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 465 EP 468 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100110 ER PT B AU Herrero, J Oberdorf, O Conroy, M McDowell, J AF Herrero, J Oberdorf, O Conroy, M McDowell, J BE Hunt, G Payne, HE TI Implementation design of the ASC data model SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB The ASC data model provides an abstract description of AXAF datasets. Through the data model API, tools and applications will have efficient and transparent access to heterogeneous disk formats. To accomplish this, the data model will use a layered design. C1 Smithsonian Astrophys Observ, AXAF Sci Ctr, Cambridge, MA 02138 USA. RP Herrero, J (reprint author), Smithsonian Astrophys Observ, AXAF Sci Ctr, 60 Garden St,MS 81, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 469 EP 472 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100111 ER PT B AU He, H McDowell, J Conroy, M AF He, H McDowell, J Conroy, M BE Hunt, G Payne, HE TI ASC coordinate transformation - The pixlib library SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB We describe a coordinate library for AXAF data analysis. The library handles transformations between celestial coordinates and instrumental (mirror, focal plane, detector pixel) coordinate systems. The need for careful transformations is driven by the accuracy of the detectors and the attitude determination system. The coordinate systems are characterized by parameter files generated from experimental and calibration data. Transformation calculations are performed by matrix-representation routines for maximum flexibility. This library is implemented in ANSI C, and uses the SAO IRAF-compatible parameter interface. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP He, H (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 473 EP 476 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100112 ER PT B AU Nguyen, D Gaetz, T Jerius, D Stern, I AF Nguyen, D Gaetz, T Jerius, D Stern, I BE Hunt, G Payne, HE TI Modeling AXAF obstructions with the generalized aperture program. SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB The generalized aperture program is designed to simulate the effects on the incident photon stream of physical obstructions, such as thermal baffles and pre-and post-collimators. It can handle a wide variety of aperture shapes, and has provisions to allow alterations of the photons by the apertures. The philosophy behind the aperture program is that a geometrically complicated aperture may be modeled by a combination of geometrically simpler apertures. This is done by incorporating a language, lua, to lay out the apertures. User provided call-back functions enable the modeling of the interactions of the incident photon with the apertures. This approach allows for maximum flexibility, since the geometry and interactions of obstructions can be specified by the user at run time. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Nguyen, D (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 485 EP 487 PG 3 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100115 ER PT B AU Karovska, M Aldcroft, T Cameron, RA DePonte, J Birkinshaw, M AF Karovska, M Aldcroft, T Cameron, RA DePonte, J Birkinshaw, M BE Hunt, G Payne, HE TI The AXAF ground aspect determination system pipeline SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB This article describes the AXAF aspect determination pipeline and its components, and highlights a procedure for determining centroids-a crucial step in deriving the post-facto aspect solution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 488 EP 491 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100116 ER PT B AU Doe, S Siemiginowska, A Joye, W McDowell, J AF Doe, S Siemiginowska, A Joye, W McDowell, J BE Hunt, G Payne, HE TI Fitting and modeling in the ASC Data Analysis Environment SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 6th Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 22-26, 1996 CL OMNI CHARLOTTESVILLE HOTEL, CHARLOTTESVILLE, VA SP Natl Radio Astron Observ, Univ Virginia, Dept Astron & Comp Sci, Associated Univ Inc, European So Observ, Gemini 8m Telescopes Project, Infrared Proc & Anal Ctr, NASA, Natl Ctr Supercomp Appl, Natl Optical Astron Observ, Natl Res Council Canada, Natl Sci Fdn, Smithsonian Astrophys Observ, Space Telescope Sci Inst, GE Fanuc Automat, Sprint Communicat, Sun Microsyst Inc HO OMNI CHARLOTTESVILLE HOTEL AB As part of the AXAF Science Center (ASC) Data Analysis Environment, we will provide to the astronomical community a Fitting Application. We present a design of the application in this paper. Our design goal is to give the user the flexibility to use a variety of optimization techniques (Levenberg-Marquardt, maximum entropy, Monte Carlo, Powell, downhill simplex, CERN-Minuit, and simulated annealing) and fit statistics (chi(2), Cash, variance, and maximum likelihood); our modular design allows the user easily to add their own optimization techniques and/or fit statistics. We also present a comparison of the optimization techniques to be provided by the Application. The high spatial and spectral resolutions that will be obtained with AXAF instruments require a sophisticated data modeling capability. We will provide not only a suite of astronomical spatial and spectral source models, but also the capability of combining these models into source models of up to four data dimensions (i.e., into source functions f(E, x, y, t)). We will also provide tools to create instrument response models appropriate for each observation. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Doe, S (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 81, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-45-7 J9 ASTR SOC P PY 1997 VL 125 BP 492 EP 495 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BK80E UT WOS:000073444100117 ER PT J AU Epps, HW Fabricant, D AF Epps, HW Fabricant, D TI Field correctors for wide-field CCD imaging with Ritchey-Chretien telescopes SO ASTRONOMICAL JOURNAL LA English DT Article ID DISPERSION CORRECTOR; TELECENTRIC IMAGERY AB The increasing availability of large format CCDs has made it possible to construct imaging arrays covering a 5 to 10 cm square format at moderate cost. In an era of 8 to 10 m telescopes, these large imaging arrays may extend the scientific usefulness of 1 to 2 m class telescopes, particularly if excellent image quality can be maintained across the large field of view. Many of these telescopes have Ritchey-Chretien optics with dominant off-axis image aberrations of field curvature and astigmatism. We briefly review the literature of one and two element refractive correctors for Ritchey-Chretien telescopes, and present variants optimized for CCD imaging. We describe a new family of two element field correctors that can provide excellent images (less than or equal to 0.2 '') over a field diameter exceeding 0.5 degrees. These new correctors have five appealing features: (1) they are compact, (2) they use only spherical surfaces, (3) they are constructed from fused silica, with high transmission over the entire optical band, (4) ghost images are well controlled, and (5) one of the corrector elements can serve as the dewar vacuum window to minimize the number of glass-air surfaces. We present two element corrector designs for the 1.2 m telescope at the Whipple Observatory and the 2.4 m Hiltner Telescope at the Michigan-Dartmouth-M.I.T. Observatory, and describe how to design such a corrector with a modern optical design program. (C) 1997 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Epps, HW (reprint author), UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064, USA. NR 16 TC 6 Z9 6 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 1997 VL 113 IS 1 BP 439 EP 445 DI 10.1086/118266 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC671 UT WOS:A1997WC67100036 ER PT B AU Press, WH Rybicki, GB AF Press, WH Rybicki, GB BE Maoz, D Sternberg, A Leibowitz, EM TI Desperately seeking non-Gaussianity - The light curve of 0957+561 SO ASTRONOMICAL TIME SERIES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Florence-and-George-Wise-Observatory 25th Anniversary Symposium on Astronomical Time Series CY DEC 30, 1996-JAN 01, 1997 CL TEL AVIV UNIV, TEL AVIV, ISRAEL SP Florence & George Wise Observ, Tel Aviv Univ HO TEL AVIV UNIV AB ''Non-Gaussian'' is the casual explanation often given for anything unexpected in an astronomical time series. What better place to look for non-Gaussianity, therefore, than in the light curve of 0957+561, the gravitational lens that, until recently, had yielded frustratingly inconsistent determinations of its lag. We discuss the difficulties in measuring deviations from Gaussianity in weakly nonstationary processes (such as 1/f noise or random walk) and define a restricted set of ''well-behaved'' three-point statistics. An important special case of such a well-behaved statistic is the skew of a linear combination of the data, with coefficients summing to zero. Analytic and Monte Carlo calculations evaluate the performance of such a statistic in the case of a non-Gaussian ''wedge model'' (shot noise, with each shot having a rapid rise and slow decay). We find that even for as well studied an object as 0957+561, the detectability of any deviation from Gaussian is problematical at best. At present, one can rule out a wedge model only if the individual shots are as infrequent as one in 10-20 days. RP Press, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 12 Z9 12 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-4706-4 J9 ASTROPHYS SPACE SC L PY 1997 VL 218 BP 61 EP 72 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ58B UT WOS:A1997BJ58B00006 ER PT B AU Schild, RE Thomson, DJ AF Schild, RE Thomson, DJ BE Maoz, D Sternberg, A Leibowitz, EM TI The Q0957+561 time delay, quasar structure, and microlensing SO ASTRONOMICAL TIME SERIES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Florence-and-George-Wise-Observatory 25th Anniversary Symposium on Astronomical Time Series CY DEC 30, 1996-JAN 01, 1997 CL TEL AVIV UNIV, TEL AVIV, ISRAEL SP Florence & George Wise Observ, Tel Aviv Univ HO TEL AVIV UNIV RP Schild, RE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 5 Z9 5 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-4706-4 J9 ASTROPHYS SPACE SC L PY 1997 VL 218 BP 73 EP 84 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ58B UT WOS:A1997BJ58B00007 ER PT J AU Markevitch, M Vikhlinin, A AF Markevitch, M Vikhlinin, A TI Comparison of ASCA and ROSAT cluster temperatures: A2256, A3558, and AWM 7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, clusters, individual (A2256, A3558, AWM 7); galaxies, elliptical and lenticular, cD; intergalactic medium; methods, data analysis; X-ray, galaxies ID SHAPLEY SUPERCLUSTER; GALAXY CLUSTERS; RAY; GAS AB We address the consistency between ASCA and ROSAT spatially resolved cluster temperature measurements, which is of significant and immediate interest given the recent ASCA reports of temperature gradients in several hot clusters. We reanalyze ROSAT PSPC data on A2256 (originally analyzed by Briel & Henry) using the newer calibration and a technique less sensitive to the calibration uncertainties. We find a temperature decline with radius in good agreement with that of ASCA, although with much larger errors than those of ASCA. We also present ASCA temperature maps and radial profiles of two cooler clusters, A3558 and AWM 7. These are compared to the ROSAT results of Bardelli et al. and Neumann & Bohringer. In A3558, our analysis detects an asymmetric temperature pattern and a slight radial temperature decline at r similar to 0.5 h(-1) Mpc, in addition to the spectral complexity of the cD galaxy region. We do not detect any significant spatial temperature variations in AWM 7, except around the cD galaxy, in agreement with the earlier ASCA analysis of this cluster. Radial temperature profiles of these two clusters are in a qualitative agreement with those from ROSAT. However, while ASCA average temperatures (5.5 and 3.9 keV, respectively) agree with those from other high-energy instruments (Ginga and EXOSAT EXOSAT for A3558 and Einstein MPC and EXOSAT for AWM 7), ROSAT temperatures are lower by factors of 1.7 and 1.25, respectively. We find that including realistic estimates of the current ROSAT systematic uncertainties enlarges the temperature confidence intervals so that ROSAT measurements are consistent with others for these two clusters as well. Because of the limited energy coverage of ROSAT PSPC, its results for the hotter clusters are highly sensitive to calibration uncertainties. We conclude that within the present calibration accuracy, there is no disagreement between ASCA and other instruments. This adds confidence to the ASCA results on the hotter clusters which can at present be studied with precision only with this instrument. On the scientific side, a ROSAT temperature underestimate for A3558 may be responsible for the anomalously high gas to total mass fraction found by Bardelli et al. Our spatially resolved temperature measurement may indicate a recent or ongoing subcluster merger in this core member of the Shapely supercluster. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MOSCOW SPACE RES INST,MOSCOW 117810,RUSSIA. RP Markevitch, M (reprint author), UNIV VIRGINIA,DEPT ASTRON,CHARLOTTESVILLE,VA 22903, USA. NR 22 TC 52 Z9 52 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1997 VL 474 IS 1 BP 84 EP 90 DI 10.1086/303456 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WA682 UT WOS:A1997WA68200008 ER PT J AU Torres, G Stefanik, RP Latham, DW AF Torres, G Stefanik, RP Latham, DW TI The Hyades binary 51 Tauri: Spectroscopic detection of the primary, the distance to the cluster, and the mass-luminosity relation SO ASTROPHYSICAL JOURNAL LA English DT Review DE binaries, spectroscopic; open clusters and associations, individual (Hyades); stars, distances; stars, individual (51 Tauri) ID SOLAR-TYPE STARS; RADIAL-VELOCITY; STELLAR MODELS; TRIGONOMETRIC PARALLAXES; THEORETICAL ISOCHRONES; SPECKLE INTERFEROMETRY; HIPPARCOS PARALLAXES; ORBITAL ELEMENTS; MAIN-SEQUENCE; OPACITIES AB 51 Tauri has long been known as a double-lined spectroscopic binary (orbital period = 11 yr) with the peculiarity that only the velocities of the secondary component could be measured. We report here spectroscopic observations of this system that have enabled us tct measure velocities for the rapidly; rotating primary using TODCOR, a two-dimensional cross-correlation technique, and we have derived a dobule-lined orbit. In addition, 51 Tau is a visual binary resolved by speckle interferometry. By combining the astrometric and spectroscopic data, we have obtained the first complete visual-spectroscopic solution for the system, from which we derive the orbital parallax (pi(orb) = 0''.0179 +/- 0''.0006) and the individual masses (M(A) = 1.80 +/- 0.13 M(circle dot) and M(B) = 1.46 +/- 0.18 M(circle dot)). Based on this orbital parallax, we use ralative proper motions for a representative sample of cluster members to obtain a distance modulus for the cluster of m - M = 3.40 +/- 0.07 (47.8 +/- 1.6 pc). We compare the empirical mass-luminosity relation from all available direct mass determinations with recent theoretical models, and we take advantage of the unusual opportunity that we have absolute luminosities and colors to derive an age estimate of 600 Myr for the Hyades, by comparing with stellar evolution models without any arbitrary adjustments. RP Torres, G (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 105 TC 35 Z9 35 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1997 VL 474 IS 1 BP 256 EP 271 DI 10.1086/303465 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WA682 UT WOS:A1997WA68200019 ER PT J AU Tafalla, M Bachiller, R Wright, MCH Welch, WJ AF Tafalla, M Bachiller, R Wright, MCH Welch, WJ TI A study of the mutual interaction between the Monoceros R2 outflow and its surrounding core SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual (Monoceros R2); ISM, jets and outflows; ISM, kinematics and dynamics; stars, formation ID STAR-FORMING REGIONS; MOLECULAR OUTFLOW; BIPOLAR OUTFLOW; INFRARED OBSERVATIONS; LINE FORMATION; STELLAR WIND; DENSE CORES; MON R2; CLOUDS; NGC-2071 AB We present high-resolution (12''-24'') (CO)-C-12(J = 2-1), (CO)-C-13(2-1), CS(2-1), CS(3-2), and CS(5-4) maps of the central 4' x 4' of Mon R2 and study the bipolar outflow, the dense core, and their mutual interaction. The high-velocity (CO)-C-12 and (CO)-C-13 emissions that trace the bipolar outflow show that the outflow lobes are limb-brightened shells of accelerated gas that have the Mon R2 IR cluster near their apex and extend approximately toward the north and south. These shells of gas are clumpy, and their emission at the highest velocities arises from discrete condensations that move with the flow but each has slightly different speed. The CS data, on the other hand, trace ambient core at low velocities, but also trace the accelerated gas of the outflow at higher speeds. The ambient CS emission shows that the core has a cavity along the path of the outflow, and that the walls of this cavity coincide in position and orientation with the shells of the bipolar flow. The accelerated CS emission concentrates along the cavity walls and arises from the same clumpy shells of gas that form the outflow lobes in (CO)-C-12 and (CO)-C-13. This outflow material, therefore, is rather dense, and a solution of the CS radiative shows that it is as dense as the gas core (approximate to 4 x 10(5) cm(-3)), suggesting that what we see as outflow is in fact gas from the dense core that has been set into motion. With the same radiative transfer analysis of the CS lines, we estimate that from a total of 1000 M. of dense gas in the core, more than 170 M. have been accelerated and incorporated into the bipolar flow. In addition, the CS spectra show a systematic enhancement of the line width toward the IR cluster that suggests the outflow has increased the gas turbulence in its vicinity. The amount of kinetic energy contained in both the bipolar and turbulent motions is comparable to the total binding energy of the dense gas, and this shows that the action of the outflow on the core can be strong enough to affect the distribution of dense gas in the core. We therefore propose that the cavity in the dense gas is the result of the evacuation of a channel by the outflow, and that the material initially filling its volume has been accelerated and incorporated into the flow. The Mon R2 system, therefore, illustrates how bipolar molecular outflows form through the acceleration of ambient molecular gas and that the process of molecular outflow formation is accompanied by a partial destruction of the dense gas environment of the newly formed star. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OBSERV ASTRON NACL,E-28800 ALCALA DE HENARES,SPAIN. RP Tafalla, M (reprint author), UNIV CALIF BERKELEY,RADIO ASTRON LAB,901 CAMPBELL HALL,BERKELEY,CA 94720, USA. NR 57 TC 42 Z9 42 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1997 VL 474 IS 1 BP 329 EP 345 DI 10.1086/303447 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WA682 UT WOS:A1997WA68200025 ER PT J AU Mehringer, DM Menten, KM AF Mehringer, DM Menten, KM TI 44 GHz methanol masers and quasi-thermal emission in Sagittarius B2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual (Sagittarius B2); ISM, molecules; masers; radio lines, ISM ID STAR-FORMING REGIONS; CONTINUUM OBSERVATIONS; LINE OBSERVATIONS; MOLECULAR CLOUD; DARK CLOUDS; ORION-KL; SGR B2; CORE; WAVELENGTH; CENTIMETER AB The Very Large Array has been used to obtain approximate to 3'' resolution observations on the 44 GHz (7)0-->6(1)A(+) transition of CH3OH (methanol) in the Sgr B2 massive star-forming complex. A total of 18 compact regions showing maser emission are found, which are spread over 2.1 pc x 4.3 pc (alpha x delta) region. Many of these are offset far from known molecular cores and ultracompact H II regions and may trace the interaction region of cloud-cloud collision. There is no spatial coincidence between 44 GHz and 6.7 GHz CH3OH masers in this region, as expected, because the pumping mechanisms for these two transitions are different. Isotropic maser luminosities range between 1 x 10(-6) and 2.1 x 10(-5) L.. In addition, 17 regions with broad line width quasi-thermal 44 GHz CH3OH emission are identified, many of which are close to known molecular hot cores, in particular those associated with the Sgr B2(N) and Sgr B2(M) continuum sources. In Sgr B2(N), quasi-thermal emission appears to be associated with two 10'' diameter ionized shells. These ionized shells may have swept up and shocked molecular material as they expanded. Also, a quasi-thermal core is observed to be coincident with a source of continuum emission from dust and emission from more complex species. In Sgr B2(M), CH3OH quasi-thermal emission arises predominantly from the western portion of this region. The CH3OH fractional abundance in most of the quasi-thermal cores appears to be quite high at similar to 10(-6). It is argued that grain-surface chemistry is responsible for this high abundance. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Mehringer, DM (reprint author), UNIV ILLINOIS,210 ASTRON BLDG,1002 W GREEN ST,URBANA,IL 61801, USA. NR 43 TC 34 Z9 34 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1997 VL 474 IS 1 BP 346 EP 361 DI 10.1086/303454 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WA682 UT WOS:A1997WA68200026 ER PT J AU DAlessio, P Calvet, N Hartmann, L AF DAlessio, P Calvet, N Hartmann, L TI The structure and emission of accretion disks irradiated by infalling envelopes SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; radiative transfer; stars, individual (HL Tauri); stars, pre-main-sequence ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; AURIGA MOLECULAR CLOUD; EMBEDDED YOUNG STARS; HL-TAURI; CIRCUMSTELLAR DISKS; PROTOSTELLAR DISKS; MODELS; EVOLUTION; INTERFEROMETER AB We calculate the emission from steady viscous disks heated by radiation from an opaque infalling protostellar envelope. For typical envelope parameters used to explain the spectral energy distributions of protostellar sources, we find that the envelope heating raises the outer disk temperature dramatically. The resulting temperature distribution in the disk is a complicated function of both radial distance and vertical height above the disk midplane. We show that the visibility flux at lambda = 0.87 mm and the spectral energy distribution from submillimeter to radio wavelengths of the flat-spectrum T Tauri star HL Tau can be explained by emission from an accretion disk irradiated by its infalling envelope, whereas thermal emission from an infalling envelope from a steady viscous accretion disk cannot explain the observations. Our results suggest that the radiation fields of collapsing protostellar envelopes may strongly affect the structure of the pre-main-sequence accretion disks. C1 UNIV MASSACHUSETTS,FIVE COLL ASTRON DEPT,AMHERST,MA 01003. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP DAlessio, P (reprint author), UNIV NACL AUTONOMA MEXICO,INST ASTRON,APDO POSTAL 70-264,MEXICO CITY 04510,DF,MEXICO. NR 42 TC 58 Z9 58 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1997 VL 474 IS 1 BP 397 EP 406 DI 10.1086/303433 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WA682 UT WOS:A1997WA68200030 ER PT J AU Henry, GW Baliunas, SL Donahue, RA Soon, WH Saar, SH AF Henry, GW Baliunas, SL Donahue, RA Soon, WH Saar, SH TI Properties of sun-like stars with planets: 51 Pegasi, 47 Ursae majoris, 70 virginis, and HD 114762 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars, activity; stars, fundamental parameters ID LOWER MAIN-SEQUENCE; EMISSION-LINE FLUXES; K-EMISSION; STELLAR ROTATION; TIME VARIATIONS; MASS COMPANION; VELOCITIES; CONVECTION; PARAMETERS; HD-114762 AB Radial velocity variations have revealed planets orbiting 51 Peg, 47 UMa, and 70 Vir, and a low-mass companion orbiting HD 114762. We analyze parallel records of photometric measurements in Stromgren b and y and Johnson V, R, and I passbands and Ca II H and K fluxes in those stars. In the case of 51 Peg, the high precision of the differential photometric measurements made by the 0.75 m Automatic Photoelectric Telescope and the nonvariability of the star would allow the detection of a transit of a planet as small as Earth (corresponding to an amplitude of 0.0001 mag) if its orbit were nearly coplanar with our line of sight, No transits were observed. For 51 Peg and 70 Vir, the upper limit of nondetection of photometric variability at their companion's orbital periods is Delta(b + y)/2 < 0.0002 +/- 0.0002 mag. For HD 114762, it is Delta V < 0.0007 +/- 0.0004 mag. Such small amplitudes of photometric variability seem to eliminate periodic velocity variations expected from p-mode oscillations. All four stars are magnetically quiet; that is, they lack the typical Ca II and photometric variability due to rotation and activity cycles expected from surface magnetic activity in solar-type stars. Such quiescence produces an interesting observational bias that favors the detection of planets from low-amplitude radial velocity or photometric variations by minimizing the contribution from intrinsic stellar variability. We discuss the circumstances for which the probability of planet detections is improved by the reduced level of variability from surface magnetic activity in G and K stars. Stars with low variability in surface activity should be the best candidates for planet searches using radial velocity and photometric techniques. Searches for planets around younger, more active stars will be impeded by variations in velocity or brightness caused by time-varying surface features. The Ca II H and K fluxes indicate that all four stars are older than 5 Gyr. Ages were estimated from the average levels of Ca II H and K fluxes and an existing relationship of the decrease of Ca II fluxes with age on the lower main sequence and were drawn from previous results based on theoretical isochrone fitting. Values of the projected rotational velocity, v sin i, are determined for 70 Vir and 47 UMa from high-resolution spectra. C1 TENNESSEE STATE UNIV,CTR EXCELLENCE INFORMAT SYST,NASHVILLE,TN 37203. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MT WILSON OBSERV,PASADENA,CA 91106. RP Henry, GW (reprint author), TENNESSEE STATE UNIV,CTR AUTOMATED SPACE SCI,330 10TH AVE N,NASHVILLE,TN 37203, USA. NR 49 TC 56 Z9 56 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1997 VL 474 IS 1 BP 503 EP 510 DI 10.1086/303451 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WA682 UT WOS:A1997WA68200041 ER PT J AU Vikhlinin, A Forman, W Jones, C AF Vikhlinin, A Forman, W Jones, C TI Another collision for the Coma Cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, clusters, general; galaxies, ISM; X-rays, galaxies ID GALAXIES; SUBSTRUCTURE; EVOLUTION; GAS AB We describe a wavelet transform analysis of the ROSAT Position Sensitive Proportional Counter images of the Coma Cluster. On small scales, less than or equal to 1', the wavelet analysis shows substructure dominated by two extended sources surrounding the two brightest cluster galaxies, NGC 4874 and NGC 4889. On slightly larger scales, similar to 2', the wavelet analysis reveals a filament of X-ray emission originating near the cluster's center, curving to the south and east for similar to 25' in the direction of the galaxy NGC 4911, and ending near the galaxy NGC 4921. These results extend earlier ROSAT observations and further indicate the complex nature of the cluster's core. We consider two possible explanations for the production of the filamentary feature from interactions of the main cluster with a merging group. The feature could arise from either ram pressure stripped gas or a dark matter perturbation of tidally stripped material. RP Vikhlinin, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 58 Z9 58 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1997 VL 474 IS 1 BP L7 EP L10 DI 10.1086/310415 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WA684 UT WOS:A1997WA68400002 ER PT J AU Griffiths, RE Ratnatunga, KU Casertano, S Im, M Neuschaefer, LW Ostrander, EJ Ellis, RS Glazebrook, K Windhorst, RA Driver, SP Mutz, SB Green, RF Sarajedini, V Huchra, JP Tyson, AJ AF Griffiths, RE Ratnatunga, KU Casertano, S Im, M Neuschaefer, LW Ostrander, EJ Ellis, RS Glazebrook, K Windhorst, RA Driver, SP Mutz, SB Green, RF Sarajedini, V Huchra, JP Tyson, AJ TI The HST Medium Deep Survey: Progress towards resolution of the faint blue galaxy problem SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article; Proceedings Paper CT Workshop on Observational Cosmology - From Galaxies to Galaxy Systems CY JUL 04-07, 1995 CL BOLZANO, ITALY SP Ctr Interuniv Reg Astrofis & Cosmol, Trieste, CNR GNA, Roma, Univ Studi Trieste, Dipartimento Astron, Trieste, Int Ctr Theoret Phys, Trieste, Int Sch Adv Studies, Trieste, Osservatorio Astron, Trieste ID HUBBLE-SPACE-TELESCOPE; WIDE-FIELD CAMERA; DWARF GALAXIES; EVOLUTION; POPULATION; IDENTIFICATION; METHODOLOGY; SAMPLE; IMAGES AB WFPCS on HST has provided the means to make rapid progress towards solving a longstanding problem in observational cosmology, viz. the nature of the objects contributing to the faint blue galaxy counts. The solution to this problem Lies in the increasing number of irregular and peculiar systems seen as a function Of increasing magnitude. Galaxies in the Medium Deep Survey (MDS) have been reliably classified to magnitudes I-814 less than or similar to 22.0 in the F814W band, at a mean redshift (z) over bar similar to 0.5. A high proportion (similar to 40%) of these objects are irregular or anomalous and they have great diversity. They include compact galaxies, galaxies or protogalaxies with superluminous starforming regions, interacting pairs, and diffuse low surface brightness galaxies of various forms. These diverse objects contribute most of the excess counts in the I-band at our limiting magnitude, and probably explain most of the 'faint blue galaxy' excess. Of the irregular population (40% of the total), about 30% show multiple, high surface brightness nuclear components. At least half of the faint galaxies, however, appear to be similar to regular Hubble-sequence examples observed at low redshift. Furthermore, the relative proportion of spheroidal and disk systems of normal appearance is as expected from nearby samples, indicating that the bulk of the local giant galaxy population was in place at half the Hubble time. Little evolution in the properties of these giant galaxies has been observed. The clear picture which thus emerges from the MDS is one in which the giant ellipticals and spirals have been relatively stable since z = 0.7, whereas there is rapid evolution of the irregular galaxy population. This latter population is not at all homogeneous, however, and seems to comprise galaxies in formation as well as fading dwarf irregulars. We have found evidence for weak gravitational shear in the vicinity of field galaxies, and gravitational lenses in MDS and archival data, including the first two examples of HST-discovered "Einstein crosses" centered on elliptical galaxies. C1 Johns Hopkins Univ, Baltimore, MD 21218 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Arizona State Univ, Tempe, AZ 85287 USA. NOAO, Tucson, AZ USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. AT&T Bell Labs, Murray Hill, NJ 07974 USA. RP Griffiths, RE (reprint author), Johns Hopkins Univ, Baltimore, MD 21218 USA. RI Im, Myungshin/B-3436-2013; Driver, Simon/H-9115-2014; Glazebrook, Karl/N-3488-2015 OI Im, Myungshin/0000-0002-8537-6714; Driver, Simon/0000-0001-9491-7327; Glazebrook, Karl/0000-0002-3254-9044 NR 32 TC 0 Z9 0 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD, PO BOX 90, READING RG1 8JL, BERKS, ENGLAND SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1997 VL 36 IS 1-6 BP 355 EP 361 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU756 UT WOS:000071751100065 ER PT J AU Strelnitski, V AF Strelnitski, V TI Masers, lasers and the interstellar medium SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Modern Problems in Astrophysics CY SEP 23-28, 1996 CL MOSCOW UNIV, STERNBERG ASTRON INST, MOSCOW, RUSSIA SP Lebedev Phys Inst, Astro Space Ctr, Euroasian Astron Soc HO MOSCOW UNIV, STERNBERG ASTRON INST DE masers; radio lines, stars; stars, individual (MWC349A); interstellar medium ID MWC 349A; TURBULENCE; MWC-349; W49N; H2O AB This paper discusses recent results obtained by myself and mgr colleagues in three domains of astrophysics: interstellar supersonic turbulence, circumstellar disks, and natural masers and lasers. S.A. Kaplan, S.B. Pikelner, and I.S. Shklovskii were among those who, 30-40 years ago, laid the foundation of these domains. H2O masers become an effective probe of supersonic turbulence associated with mass outflow from very young stars. They demonstrate a very low ((<)(similar to)) fractal dimension of the spatial set on which turbulence dissipates its kinetic energy and, thereby, a strong intermittency of the turbulence. They also indicate that supersonic turbulence, like incompressible turbulence, has an inner scale, on which the bulk of turbulent energy dissipates in low-Mach, random shocks. H2O masers themselves find thereby a new pumping source in these random shocks. Masers in hydrogen recombination lines, discovered 8 years ago, originate in a circumstellar disk surrounding a massive star MWC 349A. They give a possibility to investigate kinematics and structure of the disk. Far-infrared hydrogen recombination lines, recently detected in MWC349A from the Kuiper Airborn Observatory, proved to be amplified as well. They are the first known natural amplifiers of electromagnetic waves in the laser wavelength domain. Analysis of their radiation, along with the radiation in other recombination lines, gives a possible key to understanding the lack of optical lasers in the Universe. C1 Smithsonian Inst, Washington, DC 20560 USA. New Mexico Inst Min & Technol, Socorro, NM 87801 USA. RP Strelnitski, V (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 31 TC 3 Z9 3 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 1997 VL 252 IS 1-2 BP 279 EP 287 DI 10.1023/A:1000892300429 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZH314 UT WOS:000073095200028 ER PT J AU Westphalen, G Kalberla, PMW Hartmann, D Burton, WB AF Westphalen, G Kalberla, PMW Hartmann, D Burton, WB TI Large velocity dispersion Hi in the galactic halo SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Modern Problems in Astrophysics CY SEP 23-28, 1996 CL MOSCOW UNIV, STERNBERG ASTRON INST, MOSCOW, RUSSIA SP Lebedev Phys Inst, Astro Space Ctr, Euroasian Astron Soc HO MOSCOW UNIV, STERNBERG ASTRON INST ID MILKY-WAY; DISK; CLOUDS; GALAXY; GAS AB The Leiden/Dwingeloo Survey (LDS) offers new possibilities for analysing Galactic HI with an outstanding sensitivity. The survey data have been carefully corrected for side-lobe contamination of the antenna and for baseline effects. At present this survey is the most reliable database for analysis of faint, large-scale HI features. Together with the longstanding dispute whether the Galactic halo is hot or cold, this motivated our investigations which are described in this paper. We have improved the stray-radiation correction procedure significantly by including reflections from the ground. HI-gas with an unusually large velocity dispersion (LVD) is revealed when these enhanced LDS Data are massively integrated. Gaussian decomposition of more than 250 integrated profiles for b > 20 degrees yields a complete set of 8500 HI-components representing the north galactic sky on 10 degrees x 10 degrees fields. LVD components were found in every direction of the sky having a characteristic dispersion of greater than or equal to 60 kms(-1) and column densities of greater than or equal to 1.4.10(19) cm(-2). We do not detect the HI-gas which is associated with the "Lockman-Layer" (sigma similar to 35 kms(-1)) and conclude therefore that his analysis was biased by instrumental effects. Correction of this bias in the Hell Survey data set makes the "Lockman-Layer" disappear and does show the LVD component reported here. The LVD gas exhibits minimal sub-rotation and extends several kpc into the Galactic halo. Its scale height is calculated to be greater than or equal to 2 kpc and a non-uniform distribution with respect to the distance rom the Galactic center is found. The distribution of the LVD gas is presented. Theoretical spectra are calculated from a simple model of the LVD halo and compared to the real data. The LVD gas seems to be a very sensitive indicator of violent disk phenomena. Two possible Galactic chimneys and a peculiar local velocity field are identified, Implications for the modelling of a Galactic halo with various components are discussed. Strict application of the principle, that the turbulent gas pressure plus magnetic and cosmic ray pressure equals the gravitational pull, leads to a stable halo, extending up to a = 3.3 kpc. C1 Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. RP Westphalen, G (reprint author), Univ Bonn, Inst Radioastron, Hugel 71, D-53121 Bonn, Germany. NR 30 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 1997 VL 252 IS 1-2 BP 289 EP 300 DI 10.1023/A:1000844417268 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZH314 UT WOS:000073095200029 ER PT J AU Reid, MJ Menten, KM AF Reid, MJ Menten, KM TI Shocks in the radio photospheres of long period variable stars SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Workshop on Dust and Molecules in Evolved Stars CY MAR 24-27, 1997 CL UMIST, MANCHESTER, ENGLAND HO UMIST C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 5 Z9 5 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 1997 VL 251 IS 1-2 BP 41 EP 47 DI 10.1023/A:1000799614772 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU829 UT WOS:000071760200009 ER PT J AU Crosas, M Menten, KM Young, K Phillips, TG AF Crosas, M Menten, KM Young, K Phillips, TG TI Radiative transfer in a turbulent expanding molecular envelope: Application to Mira SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Workshop on Dust and Molecules in Evolved Stars CY MAR 24-27, 1997 CL UMIST, MANCHESTER, ENGLAND HO UMIST C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. CALTECH, Pasadena, CA 91125 USA. RP Crosas, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 2 Z9 2 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 1997 VL 251 IS 1-2 BP 189 EP 192 DI 10.1023/A:1000740823858 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU829 UT WOS:000071760200040 ER PT J AU Dalgarno, A Stancil, PC Lepp, S AF Dalgarno, A Stancil, PC Lepp, S TI Molecules and dust in supernovae SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Workshop on Dust and Molecules in Evolved Stars CY MAR 24-27, 1997 CL UMIST, MANCHESTER, ENGLAND HO UMIST ID SN 1987A; RADIATIVE ASSOCIATION; INFRARED-SPECTRUM; SILICON MONOXIDE; CARBON-MONOXIDE; MU-M; SN-1987A; SPECTROSCOPY; SPECTROPHOTOMETRY; CONTINUUM AB Observations of molecules and dust in supernova SN 1987a and SN 1995ad are summarised and the inferred masses of CO and SiO are presented. The chemistry is used to argue that macroscopic mixing occurred in which the interpenetrating clumps in the ejecta retained their microscopic integrity. An explanation of the anomalous temperature structure is advanced. Molecular candidates for some of the unidentified spectral features are proposed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM adalgarno@cfa.harvard.edu NR 36 TC 9 Z9 9 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 1997 VL 251 IS 1-2 BP 375 EP 383 DI 10.1023/A:1000752015623 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU829 UT WOS:000071760200079 ER PT J AU Wilson, AS Elvis, M AF Wilson, AS Elvis, M TI The X-ray emission of NGC 1068 SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT NGC 1068 Workshop CY OCT 30-NOV 02, 1996 CL SCHLOSS RINGBERG, GERMANY SP Max Planck Inst Extraterrestr Phys ID SEYFERT-GALAXY NGC-1068 AB This paper summarises the X-ray properties of NGC 1068 from the observers perspective and reports new observations with the ROSAT HRI. Below similar or equal to 2 keV, the spectrum is steep and probably represents thermal emission from gas with temperature kT similar or equal to 0.1 - 0.6 keV. Above similar or equal to 2 keV, the spectrum is much flatter and may be described by a power-law with energy index alpha similar or equal to 0.3. Images with the ROSAT HRI reveal that about half the X-ray flux in the 0.1 - 2.4 keV band is extended on scales > 5 '' (360 pc). Recent ROSAT PSPC observations of starburst galaxies show integrated soft X-ray spectra which are very similar to that of NGC 1068 below 2 keV. The spatially extended, steep, soft X-ray emission of NGC 1068 probably originates through thermal emission from a hot wind driven by the disk starburst, the Seyfert nucleus or a combination of the two. On the other hand, the hard emission above 2 keV is almost certainly dominated by the Seyfert nucleus. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Wilson, AS (reprint author), UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742, USA. NR 20 TC 3 Z9 3 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 1997 VL 248 IS 1-2 BP 141 EP 148 DI 10.1023/A:1000565125435 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YB896 UT WOS:A1997YB89600018 ER PT J AU Greenhill, LJ Gwinn, CR AF Greenhill, LJ Gwinn, CR TI VLBI imaging of water maser emission form a nuclear disk in NGC 1068 SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT NGC 1068 Workshop CY OCT 30-NOV 02, 1996 CL SCHLOSS RINGBERG, GERMANY SP Max Planck Inst Extraterrestr Phys ID NGC-1068 C1 UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106. RP Greenhill, LJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MAIL STOP 42,CAMBRIDGE,MA 02138, USA. NR 14 TC 123 Z9 124 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 1997 VL 248 IS 1-2 BP 261 EP 267 DI 10.1023/A:1000554317683 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YB896 UT WOS:A1997YB89600031 ER PT J AU Eichhorn, G AF Eichhorn, G TI The digital library of the astrophysics data system SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article RP Eichhorn, G (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,MS-83,CAMBRIDGE,MA 02138, USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 NR 15 TC 7 Z9 7 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 1997 VL 247 IS 1-2 BP 189 EP 210 DI 10.1023/A:1000550614898 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA XW474 UT WOS:A1997XW47400017 ER PT B AU Lane, AP AF Lane, AP BE Novak, G Landsberg, RH TI Submillimeter transmission at South Pole SO ASTROPHYSICS FROM ANTARCTICA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT ASP Summer Scientific Symposium Conference on Astrophysics from Antarctica CY JUN 30-JUL 02, 1997 CL CHICAGO, IL SP Astron Soc Pacific, Natl Sci Fdn, Ctr Astrophys Res Antarctica AB Site testing measurements conducted by the Center for Astrophysical Research in Antarctica (CARA) have demonstrated that the South Pole is the best observatory site on Earth for submillimeter and millimeter astronomy. Skydip measurements taken at 492 GHz with the Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) throughout 1995 have provided the first systematic, long-term measurements of submillimeter-wave atmospheric transparency at an astronomical site. These data were taken concurrently with precipitable water vapor measurements; comparison shows that atmospheric constituents other than water vapor contribute to the opacity at submillimeter wavelengths at South Pole. Millimeter and submillimeter opacity and water vapor data for South Pole are compared with similar data for other observatory sites. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Lane, AP (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-61-9 J9 ASTR SOC P PY 1997 VL 141 BP 289 EP 295 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74N UT WOS:000076534200031 ER PT B AU Stark, AA AF Stark, AA BE Novak, G Landsberg, RH TI Future South Pole telescopes SO ASTROPHYSICS FROM ANTARCTICA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT ASP Summer Scientific Symposium Conference on Astrophysics from Antarctica CY JUN 30-JUL 02, 1997 CL CHICAGO, IL SP Astron Soc Pacific, Natl Sci Fdn, Ctr Astrophys Res Antarctica AB The South Pole is a superb site for large single-dish telescopes operating at wavelengths between 1 mm and 2 mu m. Sensitive instrumentation at these wavelengths will enable critical advances in observational cosmology. An offset wide-field submillimeter telescope, the South Pole 10 meter (SP 10m), has been proposed which is well suited for large-scale (square degree) mapping of line and continuum radiation at moderate spatial resolutions (4 " to 60 " beam size) and uniquely high sensitivity. A 2 meter class wide-field near-infrared telescope, the South Pole Infra-Red Imaging Telescope (SPIRIT), will be comparable in sensitivity to the largest ground-based telescopes at 2 mu m and 3 mu m, and will have a tip-tilt corrected isoplanatic patch which is several square arcminutes in size. A succeeding generation of even larger instruments with active primary mirrors could be much more sensitive than any other existing or planned telescope. A 6 m diameter unfilled aperture near-infrared telescope, POlar Stratospheric Telescope (POST) is proposed which would be supported in the stratosphere by a tethered aerostat balloon, and could provide the highest resolution images available between 2 mu m and 7 mu m wavelength. It is anticipated that an umbrella organization, the International Antarctic Observatory (IAO), will coordinate operations and outreach for these telescopes. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Stark, AA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-61-9 J9 ASTR SOC P PY 1997 VL 141 BP 349 EP 367 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74N UT WOS:000076534200039 ER PT B AU Correll, DL Weller, DE AF Correll, DL Weller, DE BE Baker, JE TI Nitrogen input-output budgets for forests in the Chesapeake Bay watershed SO ATMOSPHERIC DEPOSITION OF CONTAMINANTS TO THE GREAT LAKES AND COASTAL WATERS SE SETAC TECHNICAL PUBLICATIONS SERIES LA English DT Proceedings Paper CT Session on Atmospheric Deposition of Contaminants to the Great Lakes and Coastal Waters, at the SETAC 15th Meeting CY OCT 30-NOV 03, 1994 CL DENVER, CO SP Soc Environm Toxicol & Chem, SETAC Fdn Environm Educ AB We analyzed three kinds of information to evaluate the potential of forests in the Chesapeake Bay watershed to retain the nitrogen in atmospheric deposition. Long-term (13-y) measurements of nitrogen in precipitation and stream discharge for one forested watershed in the Inner Coastal Plain showed consistently high nitrogen retention. Annual wet precipitation deposited an average of 11.4 kg N/ha, of which 46% was nitrate and 26% ammonium. Dry deposition of nitrate estimated by net throughfall was 24% of wet nitrate deposition. The forest lost an average of 1.95 kg N/ha in annual stream discharge, of which 83% was organic-N. Stream discharges of nitrate and ammonium were only 3.2 and 5.4% of wet deposition inputs. A 1-year broad-scale survey indicated low nitrate outputs from forested watersheds in a variety of geological settings within the Chesapeake drainage. Nitrate concentrations were markedly higher in streams draining watersheds with some non-forested land, particularly cultivated lands. Consistently low nitrate outputs from a variety of forested watersheds suggest that high nitrogen retention is a common feature of forests in the Chesapeake Bay watershed. A literature study indicated that of 25 forested watersheds where precipitation inputs and stream discharges were measured, 21 retained most of the inorganic N from atmospheric inputs. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Correll, DL (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU SETAC PRESS PI PENSACOLA PA 1010 N 12TH AVE, PENSACOLA, FL 32501 USA BN 1-880611-10-4 J9 SETAC TECH PUBLICAT PY 1997 BP 431 EP 442 PG 12 WC Chemistry, Multidisciplinary; Environmental Sciences; Geosciences, Multidisciplinary; Toxicology SC Chemistry; Environmental Sciences & Ecology; Geology; Toxicology GA BK63H UT WOS:000072818300023 ER PT J AU Lovelock, CE Kyllo, D Popp, M Isopp, H Virgo, A Winter, K AF Lovelock, CE Kyllo, D Popp, M Isopp, H Virgo, A Winter, K TI Symbiotic vesicular-arbuscular mycorrhizae influence maximum rates of photosynthesis in tropical tree seedlings grown under elevated CO2 SO AUSTRALIAN JOURNAL OF PLANT PHYSIOLOGY LA English DT Article ID ATMOSPHERIC CARBON-DIOXIDE; RAIN-FOREST TREES; MINERAL-NUTRITION; PLANTS; PHOSPHORUS; RESPONSES; SOIL; ENRICHMENT; INFECTION; TRANSLOCATION AB To investigate the importance of phosphorus and carbohydrate concentrations in influencing photosynthetic capacity of tropical forest tree seedlings under elevated CO2, we grew seedlings of Beilschmiedia pendula (Sw.) Hemsl. (Lauraceae) under elevated CO2 concentrations either with or without vesicular-arbuscular (VA) mycorrhizae. VA-mycorrhizae increased phosphorus concentrations in all plant organs (leaves, stems and roots). Maximum rates of photosynthesis (A(max)) measured under saturating levels of CO2 and light were correlated with leaf phosphorus concentrations. VA-mycorrhizae also increased leaf carbohydrate concentrations, particularly under elevated CO2, but levels were low and within the range observed in naturally occurring forest species. Root carbohydrate concentrations were reduced in VA-mycorrhizal plants relative to non-mycorrhizal plants. These results indicate an important role for VA-mycorrhizae in controlling photosynthetic rates and sink strength in tropical trees, and thus in determining their response to future increases in atmospheric CO2 concentrations. C1 UNIV MISSOURI,DEPT BIOL,ST LOUIS,MO 63121. UNIV VIENNA,INST PLANT PHYSIOL,A-1091 VIENNA,AUSTRIA. RP Lovelock, CE (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. RI Popp, Marianne/E-7559-2012; Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 40 TC 19 Z9 19 U1 1 U2 17 PU C S I R O PUBLICATIONS PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD VICTORIA 3066, AUSTRALIA SN 0310-7841 J9 AUST J PLANT PHYSIOL JI Aust. J. Plant Physiol. PY 1997 VL 24 IS 2 BP 185 EP 194 PG 10 WC Plant Sciences SC Plant Sciences GA WY238 UT WOS:A1997WY23800009 ER PT J AU Pukazhenthi, BS Wildt, DE Pell, KM Howard, JG AF Pukazhenthi, BS Wildt, DE Pell, KM Howard, JG TI Slow cooling prevents cold-induced sperm acrosomal damage in the teratospermic domestic cat. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008. SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1997 VL 56 SU 1 BP 59 EP 59 PG 1 WC Reproductive Biology SC Reproductive Biology GA XG865 UT WOS:A1997XG86500099 ER PT J AU Brown, JL Swanson, WF Graham, LH AF Brown, JL Swanson, WF Graham, LH TI Reproductive patterns in male and female Pallas' cats determined by fecal steroid metabolite analysis. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 SMITHSONIAN INST,CONSERVAT & RES CTR,NATL ZOOL PK,FRONT ROYAL,VA. NR 0 TC 2 Z9 2 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1997 VL 56 SU 1 BP 88 EP 88 PG 1 WC Reproductive Biology SC Reproductive Biology GA XG865 UT WOS:A1997XG86500128 ER PT J AU Graham, LH Swanson, WF Wildt, DE Brown, JL AF Graham, LH Swanson, WF Wildt, DE Brown, JL TI High daily dosages of oral melatonin suppress ovarian follicular activity in the domestic cat. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1997 VL 56 SU 1 BP 123 EP 123 PG 1 WC Reproductive Biology SC Reproductive Biology GA XG865 UT WOS:A1997XG86500163 ER PT J AU Morrow, CJ Wolfe, BA Roth, TL Wildt, DE Bush, M Blumer, ES Atkinson, MW Monfort, SL AF Morrow, CJ Wolfe, BA Roth, TL Wildt, DE Bush, M Blumer, ES Atkinson, MW Monfort, SL TI Endocrine response in scimitar-horned oryx (Oryx dammah) treated with progesterone and prostaglandin F-2 alpha to synchronize ovulation for artificial insemination. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1997 VL 56 SU 1 BP 194 EP 194 PG 1 WC Reproductive Biology SC Reproductive Biology GA XG865 UT WOS:A1997XG86500234 ER PT J AU Swanson, WF Penfold, LM Brown, JL Munson, L Wildt, DE AF Swanson, WF Penfold, LM Brown, JL Munson, L Wildt, DE TI Normality of the maternal environment in domestic cats treated with gonadotropin-releasing hormone and exogenous gonadotropins. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 UNIV TENNESSEE,COLL VET MED,KNOXVILLE,TN. SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1997 VL 56 SU 1 BP 196 EP 196 PG 1 WC Reproductive Biology SC Reproductive Biology GA XG865 UT WOS:A1997XG86500236 ER PT J AU Penfold, LM Wildt, DE AF Penfold, LM Wildt, DE TI Morphologically normal sperm from teratospermic cats remain compromised in fertilization ability even after intra-cytoplasmic sperm injection (ICSI). SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1997 VL 56 SU 1 BP 197 EP 197 PG 1 WC Reproductive Biology SC Reproductive Biology GA XG865 UT WOS:A1997XG86500237 ER PT J AU Roth, TL Williamson, LR Bush, M Wildt, DE Monfort, SL AF Roth, TL Williamson, LR Bush, M Wildt, DE Monfort, SL TI Seasonal reproductive characteristics and steroid metabolite excretion in male scimitar-horned oryx (Oryx dammah). SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1997 VL 56 SU 1 BP 463 EP 463 PG 1 WC Reproductive Biology SC Reproductive Biology GA XG865 UT WOS:A1997XG86500500 ER PT J AU Monfort, SL Wolfe, BA Morrow, CJ Kehler, J Small, TW Penfold, LM Bush, M Wildt, DE AF Monfort, SL Wolfe, BA Morrow, CJ Kehler, J Small, TW Penfold, LM Bush, M Wildt, DE TI Kinetics of gonadotropin-induced follicle-oocyte development and maturation in the endangered Eld's deer (Cervus eldi thamin). SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1997 VL 56 SU 1 BP 525 EP 525 PG 1 WC Reproductive Biology SC Reproductive Biology GA XG865 UT WOS:A1997XG86500562 ER PT J AU Robinson, H AF Robinson, H TI New species of Aphanactis in Ecuador and Bolivia and new combinations in Selloa (Heliantheae: Asteraceae) SO BRITTONIA LA English DT Article DE Aphanactis; Selloa; Galinsoginae; Andes AB Aphanactis is redelimited to contain only the Andean species with reduced limbs on the ray corollas and peduncles that elongate at or after anthesis. Four species are described as new, A. antisanensis, A. barclayae, A. boliviana, and A. ollgaardii. Two species previously described in Aphanactis, A. macdonaldii and A. ligulata, are transferred to Selloa. RP Robinson, H (reprint author), SMITHSONIAN INST,DEPT BOT,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560, USA. NR 9 TC 1 Z9 2 U1 0 U2 0 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 SN 0007-196X J9 BRITTONIA JI Brittonia PD JAN-MAR PY 1997 VL 49 IS 1 BP 71 EP 78 DI 10.2307/2807697 PG 8 WC Plant Sciences SC Plant Sciences GA WW134 UT WOS:A1997WW13400006 ER PT J AU Funk, VA AF Funk, VA TI Misbrookea, a new monotypic genus removed from Werneria sl (Compositae: Senecioneae) SO BRITTONIA LA English DT Article DE Compositae; Senecioneae; Werneria; Misbrookea; Andes; Bolivia; Peru AB A new genus is described based on a species formerly found in Werneria s.l. It is named after a collector. Miss Winifred M. A. Brooke. The new genus, Misbrookea, is confined to dry, high-elevation areas in Peru and northern Bolivia. It is distinguished by its unusual, long, multicellular hairs that cover the leaves and involucre of the plant, the style apices with long, multicellular hairs and apparent vascular traces, and the pale or silvery gray-green color of the leaves and involucre. RP Funk, VA (reprint author), SMITHSONIAN INST,DEPT BOT,US NATL HERBARIUM,MRC 166,WASHINGTON,DC 20560, USA. NR 10 TC 2 Z9 2 U1 0 U2 1 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 SN 0007-196X J9 BRITTONIA JI Brittonia PD JAN-MAR PY 1997 VL 49 IS 1 BP 110 EP 117 DI 10.2307/2807702 PG 8 WC Plant Sciences SC Plant Sciences GA WW134 UT WOS:A1997WW13400010 ER PT S AU Thaddeus, P AF Thaddeus, P BE Latter, WB Radford, SJE Jewell, PR Mangum, JG Bally, J TI Present and future CO surveys SO CO: TWENTY-FIVE YEARS OF MILLIMETER-WAVE SPECTROSCOPY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 170th Symposium of the International-Astronomical-Union on CO - 25-Years of Millimeter-Wave Spectroscopy CY MAY 29-JUN 05, 1995 CL TUCSON, AZ SP Int Astron Union ID MOLECULAR CLOUDS; SPIRAL ARM; MILKY-WAY; GALAXY; M31; PLANE; HALO AB Much of what is known about molecular clouds and their relation to star formation and galactic structure has been obtained from the large scale CO surveys. For several reasons, however, these have been done less systematically and less completely than the early 21 cm surveys; a great deal remains to be done. After a very brief general summary of what has been learned, I will emphasize the work now underway on the outer Galaxy and at high and intermediate latitudes. I will also briefly describe work in progress on M31. It will be argued in conclusion that a complete Galactic CO survey at an angular resolution of 1' is quite feasible with a dedicated multiple-feed telescope. RP Thaddeus, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4283-6 J9 IAU SYMP PY 1997 IS 170 BP 3 EP 10 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH19C UT WOS:A1997BH19C00001 ER PT S AU Dame, TM AF Dame, TM BE Latter, WB Radford, SJE Jewell, PR Mangum, JG Bally, J TI A molecular worm in scutum SO CO: TWENTY-FIVE YEARS OF MILLIMETER-WAVE SPECTROSCOPY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 170th Symposium of the International-Astronomical-Union on CO - 25-Years of Millimeter-Wave Spectroscopy CY MAY 29-JUN 05, 1995 CL TUCSON, AZ SP Int Astron Union ID GALACTIC PLANE; CO SURVEY RP Dame, TM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4283-6 J9 IAU SYMP PY 1997 IS 170 BP 19 EP 21 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH19C UT WOS:A1997BH19C00003 ER PT S AU Digel, SW Hunter, SD Mukherjee, R DeGeus, EJ Grenier, IA Heithausen, A Kanbach, G Thaddeus, P AF Digel, SW Hunter, SD Mukherjee, R DeGeus, EJ Grenier, IA Heithausen, A Kanbach, G Thaddeus, P BE Latter, WB Radford, SJE Jewell, PR Mangum, JG Bally, J TI Molecular clouds observed with the EGRET gamma-ray telescope SO CO: TWENTY-FIVE YEARS OF MILLIMETER-WAVE SPECTROSCOPY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 170th Symposium of the International-Astronomical-Union on CO - 25-Years of Millimeter-Wave Spectroscopy CY MAY 29-JUN 05, 1995 CL TUCSON, AZ SP Int Astron Union ID RADIAL-DISTRIBUTION; INTERSTELLAR GAS; OUTER GALAXY; OPHIUCHUS; ORION; CO; MONOCEROS; EMISSION C1 CALTECH, PASADENA, CA 91125 USA. CTR ETUD SACLAY, F-91191 GIF SUR YVETTE, FRANCE. UNIV COLOGNE, COLOGNE, GERMANY. MAX PLANCK INST EXTRATERR PHYS, GARCHING, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Digel, SW (reprint author), NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD 20771 USA. RI Hunter, Stanley/D-2942-2012 NR 13 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4283-6 J9 IAU SYMP PY 1997 IS 170 BP 22 EP 24 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH19C UT WOS:A1997BH19C00004 ER PT S AU Pound, MW Goodman, AA AF Pound, MW Goodman, AA BE Latter, WB Radford, SJE Jewell, PR Mangum, JG Bally, J TI The Ursa Major molecular clouds SO CO: TWENTY-FIVE YEARS OF MILLIMETER-WAVE SPECTROSCOPY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 170th Symposium of the International-Astronomical-Union on CO - 25-Years of Millimeter-Wave Spectroscopy CY MAY 29-JUN 05, 1995 CL TUCSON, AZ SP Int Astron Union C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Pound, MW (reprint author), UNIV CALIF BERKELEY, RADIO ASTRON LAB, BERKELEY, CA 94720 USA. RI Pound, Marc/A-1600-2010 NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4283-6 J9 IAU SYMP PY 1997 IS 170 BP 33 EP 35 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH19C UT WOS:A1997BH19C00006 ER PT S AU Alves, J Lada, CJ AF Alves, J Lada, CJ BE Latter, WB Radford, SJE Jewell, PR Mangum, JG Bally, J TI Mapping dust extinction in molecular clouds SO CO: TWENTY-FIVE YEARS OF MILLIMETER-WAVE SPECTROSCOPY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 170th Symposium of the International-Astronomical-Union on CO - 25-Years of Millimeter-Wave Spectroscopy CY MAY 29-JUN 05, 1995 CL TUCSON, AZ SP Int Astron Union AB Infrared array cameras have enabled the measurement and mapping of dust extinction within molecular clouds to significantly greater optical depths and at significantly higher angular resolution than previously possible. In this paper we present a map of the dust extinction in the dark cloud L978 in Cygnus derived from a large-scale multi-wavelength infrared survey. Analysis of our observations reveals significant variations in cloud structure on scales smaller than our 1'.5 resolution, thus confirming trends previously observed in IC5146 dark cloud. RP Alves, J (reprint author), SMITHSONIAN ASTROPHYS OBSERV, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4283-6 J9 IAU SYMP PY 1997 IS 170 BP 47 EP 49 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH19C UT WOS:A1997BH19C00009 ER PT S AU Goodman, AA Barranco, JA Wilner, DJ Heyer, MH AF Goodman, AA Barranco, JA Wilner, DJ Heyer, MH BE Latter, WB Radford, SJE Jewell, PR Mangum, JG Bally, J TI Velocity coherence in dense cores SO CO: TWENTY-FIVE YEARS OF MILLIMETER-WAVE SPECTROSCOPY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 170th Symposium of the International-Astronomical-Union on CO - 25-Years of Millimeter-Wave Spectroscopy CY MAY 29-JUN 05, 1995 CL TUCSON, AZ SP Int Astron Union ID STAR-FORMATION; DARK CLOUDS; MOLECULAR CLOUDS AB By analysing the dependence of line width on size in NH3 maps of dense cores, and in (CO)-O-18 and OH maps of the gas around the cores, we find that: (1) on scales larger than the FWHM contour of an NH3 core, line width is correlated with size such that Delta upsilon alpha R(a) where a similar to 0.4; and (2) within the cores themselves, the power-law slope of the line width-size relation goes to zero (i.e., line width is constant). We interpret this result as evidence for a breakpoint between ''turbulent'' self-similar molecular clouds and ''velocity coherent cores'' which can collapse to form individual stars or small groups of stars. RP Goodman, AA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4283-6 J9 IAU SYMP PY 1997 IS 170 BP 116 EP 118 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH19C UT WOS:A1997BH19C00021 ER PT S AU Myers, PC AF Myers, PC BE Latter, WB Radford, SJE Jewell, PR Mangum, JG Bally, J TI Turbulence and collapse in star-forming molecular clouds SO CO: TWENTY-FIVE YEARS OF MILLIMETER-WAVE SPECTROSCOPY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 170th Symposium of the International-Astronomical-Union on CO - 25-Years of Millimeter-Wave Spectroscopy CY MAY 29-JUN 05, 1995 CL TUCSON, AZ SP Int Astron Union ID DENSE CORES; DARK CLOUDS; PROTOSTELLAR COLLAPSE; INTERSTELLAR CLOUDS; LINE FORMATION; OPHIUCHI; MASS; CO; TEMPERATURE; SIGNATURES AB We review developments in our knowledge of interstellar turbulence, and star-forming gravitational collapse. The turbulent motions in interstellar line widths are supersonic, by a factor exceeding similar to 10 on size scales similar to 1 pc, and are progressively smaller on smaller size scales, becoming subsonic by a factor similar to 10 for low-mass dense cores of size similar to 0.1 pc. Line width-size relations Delta upsilon similar to R(1/2) in single line over a wide range of cloud sizes probably reflect little more than virial balance. Line width-size relations over several lines within a cloud vary from low-mass to massive cores, and probably reflect the structure of the density and magnetic field within the cloud. Searches for infall in star-forming clouds rely on line broadening, line asymmetry, spatial variation of the line centroid, and red-shifted absorption. Early claims of infall based on CO lines, coarse angular and spectral resolution, and distant sources were sensitive only to large-scale homologous collapse. More recent observations are sensitive to ''inside-out'' collapse over sizes 0.01 pc and velocities 0.05 km s(-1), and appear consistent with gravitational infall in several well-studied low-mass sources. RP Myers, PC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 70 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4283-6 J9 IAU SYMP PY 1997 IS 170 BP 137 EP 147 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH19C UT WOS:A1997BH19C00025 ER PT S AU Lada, CJ AF Lada, CJ BE Latter, WB Radford, SJE Jewell, PR Mangum, JG Bally, J TI Twenty-five years of CO astronomy: Revealing the cold universe SO CO: TWENTY-FIVE YEARS OF MILLIMETER-WAVE SPECTROSCOPY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 170th Symposium of the International-Astronomical-Union on CO - 25-Years of Millimeter-Wave Spectroscopy CY MAY 29-JUN 05, 1995 CL TUCSON, AZ SP Int Astron Union ID YOUNG STELLAR OBJECTS; MOLECULAR CLOUDS; OUTFLOWS; GALAXY; GAS RP Lada, CJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 39 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4283-6 J9 IAU SYMP PY 1997 IS 170 BP 387 EP 396 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH19C UT WOS:A1997BH19C00069 ER PT J AU Huddleston, DH Stokes, ML Anderson, JD Soter, S AF Huddleston, DH Stokes, ML Anderson, JD Soter, S TI Interactive exhibit for the Smithsonian Institution's How Things Fly gallery SO COMPUTER APPLICATIONS IN ENGINEERING EDUCATION LA English DT Article; Proceedings Paper CT Southeastern Conference on Theoretical and Applied Mechanics XVIII CY APR 14-16, 1996 CL TUSCALOOSA, AL DE graphics-based interaction; aerodynamics AB Development of an interactive display for the Smithsonian Institution's How Things Fly gallery illustrating Fundamental aerodynamic principles associated with flight is described. Results from Reynolds-average Navier-Stokes simulations of various airfoil geometries and flight conditions are presented in a graphics-based interactive display implemented on an Intel 486/Pentium-class personal computer. This interactive display is one mechanism used to demonstrate basic aerodynamic principles to museum visitors in this new gallery within the National Air and Space Museum. (C) 1997 John Wiley & Sons, Inc. C1 MISSISSIPPI STATE UNIV,DEPT CIVIL ENGN,MISSISSIPPI STATE,MS 39762. MISSISSIPPI STATE UNIV,NSF,ENGN RES CTR COMPUTAT FIELD SIMULAT,MISSISSIPPI STATE,MS 39762. UNIV MARYLAND,DEPT AEROSP ENGN,COLLEGE PK,MD 20742. SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560. NR 13 TC 1 Z9 1 U1 0 U2 0 PU JOHN WILEY & SONS INC PI NEW YORK PA 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 1061-3773 J9 COMPUT APPL ENG EDUC JI Comput. Appl. Eng. Educ. PY 1997 VL 5 IS 1 BP 13 EP 20 DI 10.1002/(SICI)1099-0542(1997)5:1<13::AID-CAE2>3.3.CO;2-H PG 8 WC Computer Science, Interdisciplinary Applications; Education, Scientific Disciplines; Engineering, Multidisciplinary SC Computer Science; Education & Educational Research; Engineering GA XC228 UT WOS:A1997XC22800003 ER PT J AU McLaughlin, PA Lemaitre, R AF McLaughlin, PA Lemaitre, R TI Carcinization in the Anomura - fact or fiction? I. Evidence from adult morphology SO CONTRIBUTIONS TO ZOOLOGY LA English DT Review DE carcinization; Anomura; Paguroidea; Galatheoidea; Hippoidea; Lomoidea; Paguridae; Lithodidae; adult morphology; phylogeny ID HERMIT-CRAB; DECAPODA; CRUSTACEA; ANOMALA; AEGLIDAE AB Carcinization, or the process of becoming a crab, has been, and continues to be, a focal point of anomuran evolutionary hypotheses. Traditional examples of carcinization in the Anomura are most celebrated among hermit crabs but certainly are not limited to this group. Carcinization, if it has occurred, has done so independently in all major anomuran taxa. In this critique, the traditional examples of carcinization in the Anomura are reviewed and more modern variations on the theme assessed. Potential pathways of carcinization are examined from perspectives of adult morphology in the Paguroidea, Galatheoidea, Hippoidea and Lomoidea, with emphasis on the Paguroidea. Specific attention is given to the theoretical transformation of a hermit crab-like body form into a "king crab"-like lithodid crab. Resulting coercive evidence indicates: (1) that while the evolution of a crab-like body form certainly occurs, the traditional applications, based on inadequate and often inaccurate data, are flawed; and (2) that lithodid crabs did not arise from a hermit crab predecessor through the process of carcinization. C1 Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP McLaughlin, PA (reprint author), Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. NR 175 TC 73 Z9 76 U1 0 U2 4 PU NATURALIS BIODIVERSITY CENTER PI LEIDEN PA DARWINWEG 2, LEIDEN, 2333 CR, NETHERLANDS SN 1383-4517 EI 1875-9866 J9 CONTRIB ZOOL JI Contrib. Zool. PY 1997 VL 67 IS 2 BP 79 EP 123 PG 45 WC Zoology SC Zoology GA YU365 UT WOS:000071709800001 ER PT S AU Cranmer, SR Kohl, JL Noci, G Strachan, L Panasyuk, AV Romoli, M Fineschi, S Dobrzycka, D Raymond, JC Suleiman, RM O'Neal, RH AF Cranmer, SR Kohl, JL Noci, G Strachan, L Panasyuk, AV Romoli, M Fineschi, S Dobrzycka, D Raymond, JC Suleiman, RM O'Neal, RH BE Wilson, A TI UVCS/SOHO empirical models of solar coronal holes SO CORONA AND SOLAR WIND NEAR MINIMUM ACTIVITY - FIFTH SOHO WORKSHOP SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th SOHO Workshop on the Corona and Solar Wind Near Minimum Activity CY JUN 17-20, 1997 CL UNIV OSLO, INST THEORET ASTROPHYS, OSLO, NORWAY SP European Space Agcy, Univ Oslo, Norges Forskningsrad, NASA, Norwegian Space Ctr, Res Council Norway, SCOSTEP HO UNIV OSLO, INST THEORET ASTROPHYS DE solar corona; solar wind; coronal holes; UV radiation; line profiles AB We develop a self-consistent empirical model for the major plasma parameters in a solar-minimum coronal hole using UVCS/SOHO. The model describes the radial and latitudinal distribution of density, velocity, and kinetic temperature for electrons, neutral hydrogen, and ionized oxygen, during the period between November 1996 and April 1997. This model is intended to provide experimental values which can be used to constrain theoretical models of the fast solar wind. We present models of the three-dimensional electron density structure of coronal holes between 1.5 and 4 solar radii, including a statistical analysis of the distribution of polar plumes. We then compare observations of Lyman alpha and O VI 1032, 1037 emission lines with Doppler-dimming models, and iterate for optimal consistency in all derived velocities. The large line widths of H I atoms and O VI ions at most radii (corresponding to line-of-sight velocities around 250 and 500 km s(-1), respectively) are incompatible with either thermal equilibrium or common small-scale motions. The inferred kinetic temperatures are proportional to the ion mass to a higher power than unity. Also, the latitudinal dependence of intensity constrains the geometry of the wind velocity vectors, and superradial expansion is more consistent with observations than radial flow. We discuss the implications on various theoretical models of coronal heating and acceleration. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Romoli, Marco/H-6859-2012 NR 0 TC 3 Z9 3 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-299-0 J9 ESA SP PUBL PY 1997 VL 404 BP 295 EP 298 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK11J UT WOS:000071215200043 ER PT S AU Olsen, EL AF Olsen, EL BE Wilson, A TI Correspondence between the broadening of the Lyman-alpha line and the temperatures in the acceleration region of the solar wind SO CORONA AND SOLAR WIND NEAR MINIMUM ACTIVITY - FIFTH SOHO WORKSHOP SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th SOHO Workshop on the Corona and Solar Wind Near Minimum Activity CY JUN 17-20, 1997 CL UNIV OSLO, INST THEORET ASTROPHYS, OSLO, NORWAY SP European Space Agcy, Univ Oslo, Norges Forskningsrad, NASA, Norwegian Space Ctr, Res Council Norway, SCOSTEP HO UNIV OSLO, INST THEORET ASTROPHYS DE corona; spectroscopy AB In this study we investigate the Lyman-alpha line from neutral hydrogen in an eight-moment approximation, two-fluid, model of high speed solar wind. Compared to previous models, where the heat fluxes have been described by assuming the gas to be collision dominated, the eight-moment model gives larger proton coronal temperatures and a more profound acceleration of the solar wind. We show that the temperature maximum in the corona inferred from the observed Lyman-alpha line may be more than 20% lower than the proton temperature maximum. C1 Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Olsen, EL (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-299-0 J9 ESA SP PUBL PY 1997 VL 404 BP 527 EP 532 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK11J UT WOS:000071215200090 ER PT S AU Strachan, L Raymond, JC Panasyuk, AV Fineschi, S Gardner, LD Antonucci, E Giordano, S Romoli, M Noci, G Kohl, JL AF Strachan, L Raymond, JC Panasyuk, AV Fineschi, S Gardner, LD Antonucci, E Giordano, S Romoli, M Noci, G Kohl, JL BE Wilson, A TI Spectroscopic observations of the extend corona during the SOHO Whole Sun Month SO CORONA AND SOLAR WIND NEAR MINIMUM ACTIVITY - FIFTH SOHO WORKSHOP SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th SOHO Workshop on the Corona and Solar Wind Near Minimum Activity CY JUN 17-20, 1997 CL UNIV OSLO, INST THEORET ASTROPHYS, OSLO, NORWAY SP European Space Agcy, Univ Oslo, Norges Forskningsrad, NASA, Norwegian Space Ctr, Res Council Norway, SCOSTEP HO UNIV OSLO, INST THEORET ASTROPHYS DE UV spectroscopy; solar corona; solar wind AB The spatial distribution of plasma parameters in the extended corona are derived from UVCS/SOHO observations made during the Whole Sun Month Campaign (10 Aug. to 8 Sept. 1996). Daily coronal synoptic scans in H I Lyman alpha and O VI lambda lambda 1032 and 1037 Angstrom were used to make synoptic maps of integrated intensities and line of sight velocities for all three lines. Maps of bulk outflow velocities of O5+ based on the Doppler dimming of the O VI lines are also discussed. These results show several interesting correlations of plasma characteristics with coronal structures. For example, low latitude streamers show clear depletions of O5+ in their cores (Raymond et al., 1997) while high latitude active region streamers do not. Also the very broad LOS velocity distribution widths of O5+ are shown to be a clear signature of coronal holes while the velocity distributions for H-0 show a much smaller effect. Possible physical explanations for some of the observed features are discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Strachan, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Romoli, Marco/H-6859-2012 NR 0 TC 4 Z9 4 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-299-0 J9 ESA SP PUBL PY 1997 VL 404 BP 691 EP 696 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK11J UT WOS:000071215200122 ER PT B AU Field, GB Corbelli, E AF Field, GB Corbelli, E BE Persic, M Salucci, P TI Is dark matter in spiral galaxies interstellar gas? SO DARK AND VISIBLE MATTER IN GALAXIES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Dark and Visible Matter in Galaxies and Cosmological Implications CY JUL 02-05, 1996 CL SESTO PUSTERIA, ITALY SP Int Sch Adv Studies, Trieste Observ, Interdept Consortium Astrophys & Cosmol, Italian Natl Res Council AB We consider various ways in which interstellar hydrogen could be hidden in large enough amounts to account for the dark matter in the outer parts of spiral galaxies. Uniform optically thick atomic hydrogen disks and ionized hydrogen are ruled out observationally. Pressure confined optically thick atomic hydrogen clouds would be too large and gravitationally unstable, and would collapse to form more compact objects stabilized by some mechanism. Two possible forms of hidden hydrogen are clouds of H-2 molecules stabilized by opacity, like the clumpuscules proposed by Pfenniger and Combes (1994), and molecular or atomic clouds stabilized by turbulence and magnetic fields, like the giant molecular clouds observed in the solar neighborhood. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Field, GB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-37-6 J9 ASTR SOC P PY 1997 VL 117 BP 258 EP 265 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK79X UT WOS:000073437700035 ER PT J AU Marsden, BG AF Marsden, BG TI Orbit determination and evolution of comet C/1995 O1 (Hale-Bopp) SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT 1st International Conference on Comet Hale-Bopp CY FEB 02-05, 1998 CL TENERIFE, SPAIN ID TUTTLE AB The situation leading to the determination of the Hale-Bopp orbit is discussed, largely in terms of a procedure that generates two sequences of parabolic orbits. The comet is also considered in relation to the problem of the possibility of impact on the earth. The placement of its orbital nodes near the orbits of the earth and Jupiter is clearly an intriguing feature. The role of the prediscovery observation in 1993 is described, as it appeared both as a boon and a burden. Although evidence has been put forward that the Hale-Bopp nucleus is unusually large, it seems likely that nongravitational forces are noticeably affecting the comet's motion. While discussion of the comet's future long-term motion may be amenable to the usual treatment as a problem of diffusion, it is not entirely improbable that the present situation arose from a recent dramatic approach to Jupiter. It is shown that such a Jupiter encounter in June -2215 is not inconsistent with the non-existence of records at the comet's last perihelion passage, which could then have been the first to occur as close as 0.9 AU to the sun. Of course, the Jupiter encounter might also have given rise to the possible large satellite to Hale-Bopp discussed by Sekanina. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marsden, BG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 29 TC 6 Z9 6 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PY 1997 VL 79 IS 1-3 BP 3 EP 15 DI 10.1023/A:1006268813208 PG 13 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 284ZF UT WOS:000085362200002 ER PT J AU Irvine, WM Dickens, JE Lovell, AJ Schloerb, FP Senay, M Bergin, EA Jewitt, D Matthews, HE AF Irvine, WM Dickens, JE Lovell, AJ Schloerb, FP Senay, M Bergin, EA Jewitt, D Matthews, HE TI The HNC/HCN ratio in comets SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT 1st International Conference on Comet Hale-Bopp CY FEB 02-05, 1998 CL TENERIFE, SPAIN DE comets; interstellar molecules ID HYAKUTAKE; HNC AB The abundance ratio of the isomers HCN and HNC has been investigated in comet Hale-Bopp (C/1995 O1) through observations of the J = 4-3 rotational transitions of both species for heliocentric distances 0.93 < r<3 AU, both pre- and post-perihelion. After correcting for the optical depth of the stronger HCN line, we find that the column density ratio of HNC/HCN in our telescope beam increases significantly as the comet approaches the Sun. We compare this behavior to that predicted from an ion-molecule chemical model and conclude that the HNC is produced in significant measure by chemical processes in the coma; i.e., for comet Hale-Bopp, HNC is not a parent molecule sublimating from the nucleus. C1 Univ Massachusetts, Five Coll Radio Astron Observ, Amherst, MA 01003 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Joint Astron Ctr, Hilo, HI 96720 USA. RP Univ Massachusetts, Five Coll Radio Astron Observ, Amherst, MA 01003 USA. NR 19 TC 15 Z9 16 U1 1 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 EI 1573-0794 J9 EARTH MOON PLANETS JI Earth Moon Planets PY 1997 VL 78 IS 1-3 BP 29 EP 35 DI 10.1023/A:1006285703521 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 291GU UT WOS:000085726400006 PM 11543322 ER PT J AU Wulff, JL AF Wulff, JL TI Mutualisms among species of coral reef sponges SO ECOLOGY LA English DT Article DE coral reefs; diffuse mutualism; direct mutualism; facultative mutualism; sponge extensibility; sponge strength ID MARSH PLANTS; ASSOCIATIONS; POPULATIONS; FACILITATION; PRODUCTIVITY; COMPETITION; ABUNDANCE; SURVIVAL; PORIFERA; GROWTH AB Intimate associations among individuals of three common species of Caribbean coral reef sponges can be mutually beneficial. Both growth rate and survival are enhanced when heterospecific sponges adhere to each other, as demonstrated by experiments in which sponges of the same size and genotype were grown (1) in intimate association with conspecific vs. heterospecific sponges, (2) alone vs. in intimate association with conspecific sponges, and (3) alone on the primary substratum vs. attached to an intact branch of a conspecific or heterospecific sponge. Natural development and long-term dynamics of these associations were observed in unmanipulated individuals and also modelled by an experiment in which branches were exchanged between neighboring sponges. The three species studied (lotrochota birotulata, Amphimedon rubens, and Aplysina fulva) share an erect branching growth form but differ in tissue and skeletal characteristics sufficiently that they are in different orders of the Class Demospongiae. Reflecting these differences, the species are demonstrated to differ from each other in their susceptibility to a variety of environmental hazards, including predation by angelfishes and trunkfishes, predation by starfish, smothering by sediment, breakage by storm waves, pulverization by storm waves, toppling by storm waves, fragment mortality, and pathogens. Although the mechanisms by which growth rate is enhanced by adhering to a heterospecific sponge are unknown, these sponges appear to be able to decrease their loss rate by adhering tightly to sponges of species that differ from them in chemistry, tissue density, and skeletal construction, thereby increasing survival of hazards to which they would succumb when growing alone. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 52 TC 56 Z9 59 U1 2 U2 30 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 0012-9658 J9 ECOLOGY JI Ecology PD JAN PY 1997 VL 78 IS 1 BP 146 EP 159 PG 14 WC Ecology SC Environmental Sciences & Ecology GA WD345 UT WOS:A1997WD34500011 ER PT B AU Whigham, DF AF Whigham, DF BE Simpson, RD Christensen, NL TI Ecosystem functions and ecosystem values SO ECOSYSTEM FUNCTION AND HUMAN ACTIVITIES: RECONCILING ECONOMICS AND ECOLOGY LA English DT Proceedings Paper CT Workshop on Human Activity and Ecosystem Function - Reconciling Economics and Ecology CY OCT, 1995 CL WASHINGTON, DC SP Renewable Nat Resources Fdn, USDA Forest Serv, USDA Nat Resources Conservat Serv, US Bur Land Management, US Natl Biol Serv, US Natl Ocean & Atmospher Adm RP Whigham, DF (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. NR 0 TC 4 Z9 4 U1 0 U2 2 PU CHAPMAN & HALL INC PI NEW YORK PA 115 FIFTH AVENUE, NEW YORK, NY 10003 BN 0-412-09671-4 PY 1997 BP 225 EP 239 PG 15 WC Environmental Sciences; Environmental Studies SC Environmental Sciences & Ecology GA BH68H UT WOS:A1997BH68H00011 ER PT J AU Gentili, P Solis, MA AF Gentili, P Solis, MA TI Checklist and key of new world species of Omiodes Guenee with descriptions of four new Costa Rican species (Lepidoptera : Crambidae) SO ENTOMOLOGICA SCANDINAVICA LA English DT Article AB Omiodes Guenee is redescribed based on all New World species, including the type species O. humeralis Guenee. Four new species from Costa Rica, O. janzeni sp. n., O. hallwachsae sp. n., O. sirena sp. n., O. ochracea sp. n., are described. Ten new synonymies are established: Phostria discuridescens Hampson is =O. croeceiceps (Walker), Phostria cayennalis Schaus is =O. grandis (Druce), Omiodes ochrosoma Felder & Rogenhofer and Phryganodes gazalis Schaus are =O. pandaralis (Walker), Nacoleia lenticurvalis Hampson, Phryganodes anchoritalis Dyar, and Phostria duplicata Kaye are =O. confusalis (Dognin), O. cervinalis Amsel is =O. martyralis (Lederer), Nacoleia indicata ab. pigralis Dognin and Botis fortificalis Moschler are =O. metricalis (Moschler). One new combination is recognized: O. pandaralis (Walker) was transferred from Coelorhynchidia Hampson. A key and an updated checklist to the neotropical Omiodes species is provided, including O. indicata (Fabricius), a worldwide pest. Ten species that do not belong in Omiodes are retained until appropriate generic placements are identified. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Gentili, P (reprint author), Smithsonian Inst, Dept Entomol, MRC 127, Washington, DC 20560 USA. NR 8 TC 2 Z9 2 U1 0 U2 3 PU ENTOMOL SCANDINAVICA PI LUND PA DEPT OF SYST ZOOL HELGOVAVAGEN 3, S-223 62 LUND, SWEDEN SN 0013-8711 J9 ENTOMOL SCAND JI Entomol. Scand. PY 1997 VL 28 IS 4 BP 471 EP 492 PG 22 WC Entomology SC Entomology GA YZ033 UT WOS:000072213400008 ER PT J AU Mateo, MA Romero, J Perez, M Littler, MM Littler, DS AF Mateo, MA Romero, J Perez, M Littler, MM Littler, DS TI Dynamics of millenary organic deposits resulting from the growth of the Mediterranean seagrass Posidonia oceanica SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE accretion rates; decay rates; nutrient sink; radiocarbon dating; Western Mediterranean AB The Mediterranean seagrass Posidonia oceanica accumulates large quantities of organic debris as roots, rhizomes and leaf sheaths are progressively buried forming a bioconstruction called 'matte'. The organic material remains with little morphological alteration for millennia. Several strata from these accumulations in various P. oceanica meadows were sampled. Radiocarbon dating of samples yielded a range of 0-3370 years before present. From these data, accretion rates averaging 0.175 cm year(-1) (range: 0.061-0.414) were inferred. Significant differences between sites were found. Accretion rates showed significant differences between matte strata (i.e. with time), but no defined patterns were appreciated. Such differences were not coherent across sites. It is concluded that accretion rates are mainly controlled by local factors. Analysis of carbon, nitrogen and phosphorous in the organic debris showed that there was not a net release during the process of matte construction; in some sites, nitrogen and phosphorus concentration remained constant throughout the matte profile, while in the other sites, their concentration increased significantly with age. This confirms the role of P. oceanica meadows as sinks for biogenic elements. (C) 1997 Academic Press Limited. C1 UNIV BARCELONA,DEPT ECOL,BARCELONA 08028,SPAIN. SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560. RI Mateo, Miguel/J-8988-2012; Romero, Javier/A-8905-2013; OI Romero, Javier/0000-0002-2772-8486; Mateo, Miguel/0000-0001-7567-0277 NR 43 TC 120 Z9 123 U1 3 U2 29 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0272-7714 J9 ESTUAR COAST SHELF S JI Estuar. Coast. Shelf Sci. PD JAN PY 1997 VL 44 IS 1 BP 103 EP 110 DI 10.1006/ecss.1996.0116 PG 8 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA WG335 UT WOS:A1997WG33500008 ER PT B AU Murray, SS Chappell, JH Kenter, AT Kobayashi, K Kraft, RP Meehan, GR Zombeck, MV Fraser, GW Pearson, JF Lees, JE Brunton, AN Pearce, SE Barbera, M Collura, A Serio, S AF Murray, SS Chappell, JH Kenter, AT Kobayashi, K Kraft, RP Meehan, GR Zombeck, MV Fraser, GW Pearson, JF Lees, JE Brunton, AN Pearce, SE Barbera, M Collura, A Serio, S BE Siegmund, OHW Gummin, MA TI The AXAF High Resolution Camera (HRC): Calibration and recalibration at XRCF and beyond SO EUX, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on EUV, X-ray, and Gamma-Ray Instrumentation for Astronomy VIII CY JUL 30-AUG 01, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE x-ray detectors; calibration; flat field; microchannel plate High Resolution Camera; AXAF AB The High Resolution Camera (HRC) is a Microchannel Plate based imaging detector for the Advanced X-Ray Astrophysics Facility (AXAF) that will be placed in a high earth orbit scheduled for launch in August, 1998. An end-to-end calibration of the HRC and the AXAF High Resolution Mirror Assembly (HRMA) was carried out at the Marshall Space Flight Center's X-Ray Calibration Facility (XRCF). This activity was followed by several modifications to the HRC to improve its performance, and a series of flat field calibrations. In this paper, and the following companion papers, we discuss the calibration plans, sequences, and results of these tests. At the time of this conference, the HRC has been fully flight qualified and is being integrated into the Science Instrument Module (SIM) in preparation for integration into the AXAF spacecraft. RP Murray, SS (reprint author), SMITHSONIAN INST ASTROPHYS OBSERV,HIGH ENERGY ASTROPHYS DIV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI collura, alfonso/0000-0001-9534-1235; Barbera, Marco/0000-0002-3188-7420 NR 0 TC 53 Z9 53 U1 0 U2 1 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2536-2 J9 P SOC PHOTO-OPT INS PY 1997 VL 3114 BP 11 EP 25 DI 10.1117/12.283772 PG 15 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BJ87K UT WOS:A1997BJ87K00002 ER PT B AU Kenter, AT Chappel, JH Kobayashi, K Kraft, RP Meehan, GR Murray, SS Zombeck, MV Fraser, GW Pearson, JF Lees, JE Brunton, AN Pearce, SE Barbera, M Collura, A Serio, S AF Kenter, AT Chappel, JH Kobayashi, K Kraft, RP Meehan, GR Murray, SS Zombeck, MV Fraser, GW Pearson, JF Lees, JE Brunton, AN Pearce, SE Barbera, M Collura, A Serio, S BE Siegmund, OHW Gummin, MA TI Performance and calibration of the AXAF high resolution camera .1. Imaging readout SO EUX, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on EUV, X-ray, and Gamma-Ray Instrumentation for Astronomy VIII CY JUL 30-AUG 01, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE microchannel plate; AXAF; High Resolution Camera AB The High Resolution Camera (HRC) will be one of the two focal plane instruments on the Advanced X-ray Astrophysics Facility, (AXAF). AXAF will perform high resolution spectrometry and imaging in the X-ray band of 0.1 to 10 keV. The HRC instrument consists of two detectors, the HRC-I for imaging and the HRC-S for spectroscopy. Each HRC detector consists of a thin aluminized polyimide window, a chevron pair of microchannel plates (MCPs) and a crossed grid charge readout. The HRC-I is a 100 x 100 mm detector optimized for high resolution imaging and timing, the HRC-S is a similar to 30 x 300 mm detector optimized to function as the readout for the Low Energy Transmission Grating Spectrometer (LETGS). In this paper we present the absolute quantum efficiency, spatial resolution, point spread response function and count rate linearity of the HRC-I detector. Data taken at the HRC laboratory and at the Marshall Space flight Center X-ray Calibration Facility are presented. The development of the HRC is a collaborative effort between The Smithsonian Astrophysical Observatory, University of Leicester UK and the Osservatorio Astronomico, G.S. Vaiana, Palermo Italy. RP Kenter, AT (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Barbera, Marco/0000-0002-3188-7420 NR 0 TC 9 Z9 9 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2536-2 J9 P SOC PHOTO-OPT INS PY 1997 VL 3114 BP 26 EP 52 DI 10.1117/12.283777 PG 27 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BJ87K UT WOS:A1997BJ87K00003 ER PT B AU Kraft, RP Chappell, JH Kenter, AT Kobayashi, K Meehan, GR Murray, SS Zombeck, MV Fraser, GW Pearson, JF Lees, JE Brunton, AN Barbera, M Collura, A Serio, S AF Kraft, RP Chappell, JH Kenter, AT Kobayashi, K Meehan, GR Murray, SS Zombeck, MV Fraser, GW Pearson, JF Lees, JE Brunton, AN Barbera, M Collura, A Serio, S BE Siegmund, OHW Gummin, MA TI Performance and calibration of the AXAF High Resolution Camera II: the spectroscopic detector SO EUX, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on EUV, X-ray, and Gamma-Ray Instrumentation for Astronomy VIII CY JUL 30-AUG 01, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE X-rays; microchannel plates; X-ray detectors; AXAF High Resolution Camera; X-ray spectroscopy AB The High Resolution Camera (HRC) is one of two focal plane detector systems that will be flown on the Advanced X-ray Astrophysics Facility (AXAF). The HRC consists of two microchannel plate (MCP) detectors: one to provide large area, high position resolution imaging and timing (HRC-I), and a second (HRC-S) to provide a readout for the AXAF Low Energy Transmission Gratings. Each detector is composed of a chevron pair of CsI coated MCPs with a crossed grid charge detector and an Al/Polyimide UV/Ion shield. In this paper, we describe the operation, performance and calibration of the spectroscopic detector. In particular, we discuss the absolute quantum efficiency calibration, the point spread function of the instrument combined with the AXAF telescope, the count rate linearity, the spatial linearity, and the internal background of the instrument. Data taken in the laboratory and at the X-ray Calibration Facility at Marshall Space Flight Center are presented. RP Kraft, RP (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,MS-31,CAMBRIDGE,MA 02138, USA. OI collura, alfonso/0000-0001-9534-1235; Barbera, Marco/0000-0002-3188-7420 NR 0 TC 9 Z9 9 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2536-2 J9 P SOC PHOTO-OPT INS PY 1997 VL 3114 BP 53 EP 73 DI 10.1117/12.283785 PG 21 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BJ87K UT WOS:A1997BJ87K00004 ER PT B AU Meehan, GR Murray, SS Zombeck, MV Kraft, RP Kobayashi, K Chappell, JH Kenter, AT Barbera, M Collura, A Serio, S AF Meehan, GR Murray, SS Zombeck, MV Kraft, RP Kobayashi, K Chappell, JH Kenter, AT Barbera, M Collura, A Serio, S BE Siegmund, OHW Gummin, MA TI Calibration of the UV/ion shields for the AXAF High Resolution Camera SO EUX, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on EUV, X-ray, and Gamma-Ray Instrumentation for Astronomy VIII CY JUL 30-AUG 01, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE x-ray detectors; UV/ion shield; AXAF; High Resolution Camera AB The High Resolution Camera (HRC) is one of AXAF's two focal plane instruments. It consists of two detectors: the HRC-I which is optimized for direct imaging of x-ray sources; and the HRC-S which is optimized as the spectroscopic read-out of the Low Energy Transmission Grating (LETG). Both detectors are comprised of a chevron pair of micro-channel plates (MCPs) with a crossed grid charge detector (CGCD) and a UV/Ion shield (UVIS). The role of the UVIS is to minimize the detectors' sensitivity to low energy electrons, ions and UV light; while providing sufficient x-ray transmission in the 0.1 to 10 keV x-ray band. In this paper, we report the results of the flight UVIS calibration measurements. Specifically, x-ray and UV transmission measurements obtained at the HRC X-ray Test Facility of the Smithsonian Astrophysical Observatory, and x-ray transmission measurements of UVIS witness samples obtained at a synchrotron light source facility. RP Meehan, GR (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI collura, alfonso/0000-0001-9534-1235; Barbera, Marco/0000-0002-3188-7420 NR 0 TC 5 Z9 5 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2536-2 J9 P SOC PHOTO-OPT INS PY 1997 VL 3114 BP 74 EP 100 DI 10.1117/12.283790 PG 27 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BJ87K UT WOS:A1997BJ87K00005 ER PT J AU Barbera, M Collura, A Dara, A Leone, M Powell, FR Serio, S Varisco, S Zombeck, MV AF Barbera, M Collura, A Dara, A Leone, M Powell, FR Serio, S Varisco, S Zombeck, MV TI Effects of interference and oxidation on the UV/visible rejection properties of filters for soft x-ray detectors SO EXPERIMENTAL ASTRONOMY LA English DT Article DE x-ray; calibration; filters; interference; oxidation AB We report on UV/Visible transmission measurements of aluminum coated Lexan filters designed as UV blocking filters for soft x-ray detectors. Transmission of the filters in the 2300 - 8000 A wavelength range is significantly higher than expected. It cannot be accounted for applying a simple slab model of the transmission and adopting material properties reported in the literature. We show that this is due to interference effects which are strongly dependent on the filter geometry, and to oxidation of exposed aluminum surfaces and/or chemical interaction with the plastic support. The results of this work have led to the redesign of the Advanced X-ray Astrophysics Facility High Resolution Camera UV blocking filters. C1 CNR,IST APPL INTERDISCIPLINARI FIS,PALERMO,ITALY. UNIV PALERMO,IST FIS,PALERMO,ITALY. LUXEL CORP,FRIDAY HARBOR,WA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Barbera, M (reprint author), IST & OSSERVATORIO ASTRON GS VAIANA,PALERMO,ITALY. RI Leone, Maurizio/F-2353-2010; OI Leone, Maurizio/0000-0002-0292-7657; collura, alfonso/0000-0001-9534-1235; Barbera, Marco/0000-0002-3188-7420 NR 21 TC 12 Z9 12 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PY 1997 VL 7 IS 1 BP 51 EP 63 DI 10.1023/A:1007919005280 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA XT395 UT WOS:A1997XT39500004 ER PT S AU Melnick, GJ Dalgarno, A Erickson, NR Fazio, GG Goldsmith, PF Harwit, M Hollenbach, DJ Koch, DG Neufeld, DA Schieder, R Snell, RL Stauffer, JR Thaddeus, P Tolls, V Winnewisser, GF AF Melnick, GJ Dalgarno, A Erickson, NR Fazio, GG Goldsmith, PF Harwit, M Hollenbach, DJ Koch, DG Neufeld, DA Schieder, R Snell, RL Stauffer, JR Thaddeus, P Tolls, V Winnewisser, GF GP EUROPEAN SPACE AGCY TI The submillimeter wave astronomy satellite: Science objectives and instrument description SO FAR INFRARED AND SUBMILLIMETRE UNIVERSE: AN ESA SYMPOSIUM DEVOTED TO THE FAR INFRARED AND SUBMILLIMETRE TELESCOPE (FIRST) MISSION SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT ESA Symposium on the Far InfraRed and Submillimetre Universe CY APR 15-17, 1997 CL INST RADIO ASTRON MILLIMETR, GRENOBLE, FRANCE SP European Space Agcy HO INST RADIO ASTRON MILLIMETR AB The Submillimeter Wave Astronomy Satellite (SWAS) mission is dedicated to the study of star formation and interstellar chemistry. To carry out this mission, SWAS will survey dense (n(H2) > 10(3) cm(-3)) molecular clouds within our galaxy in either the ground-state or a low-lying transition of five astrophysically important species: H2O, (H1O)-O-18, O-2, CI, and (CO)-C-13. By observing these lines SWAS will: (1) test long-standing theories that predict that these species are the dominant coolants of molecular clouds during the early stages of their collapse to form stars and planets; and (2) supply heretofore missing information about the abundance of key species central to the chemical models of dense interstellar gas. SWAS will employ two independent Schottky barrier diode mixers, passively cooled to similar to 170 K, coupled to a 53 x 68-cm off-axis Cassegrain antenna with an aggregate surface error less than or equal to 11 mu m rms. During its baseline two-year mission, SWAS will observe giant and dark cloud cores with the goal of detecting or setting an upper limit on the water and molecular oxygen abundance of 3 x 10(-6) (relative to H-2) In addition, advantage will be taken of SWAS's relatively large beamsize of 3.3 x 4.2 arcminutes at 557 GHz and 3.8 x 4.8 arcminutes at 492 GHz to obtain large-area (similar to 1 degrees x 1 degrees) maps of giant and dark clouds in the (CO)-C-13 and CI lines. With the use of a 1.4 GHz bandwidth acousto-optical spectrometer, SWAS will have the ability to simultaneously observe the H2O, O-2, CI, and (CO)-C-13 lines. All measurements will be conducted with a velocity resolution of less than 1 km s(-1). RP Melnick, GJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV,MAIL STOP 66-60,GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 4 Z9 4 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-287-7 J9 ESA SP PUBL PY 1997 VL 401 BP 189 EP 194 PG 6 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BJ82Z UT WOS:A1997BJ82Z00027 ER PT S AU Kurucz, RL AF Kurucz, RL GP ESA TI Progress on model atmospheres and line data SO FIRST ISO WORKSHOP ON ANALYTICAL SPECTROSCOPY: WITH SWS, LWS, PHT-S, AND CAM-CVF SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 1st ISO Workshop on Analytical Spectroscopy CY OCT 06-08, 1997 CL MADRID, SPAIN SP European Space Agcy AB I can compute arbitrary-abundance models and spectra at high resolution using millions of atomic and diatomic molecular lines. I am improving the input line data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurucz, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 4 Z9 4 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-676-7 J9 ESA SP PUBL PY 1997 VL 419 BP 193 EP 199 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK66F UT WOS:000072989100029 ER PT S AU Kurucz, RL Megessier, C Andersen, J AF Kurucz, RL Megessier, C Andersen, J BE Bedding, TR Booth, AJ Davis, J TI Progress on model atmospheres and line data SO FUNDAMENTAL STELLAR PROPERTIES: THE INTERACTION BETWEEN OBSERVATION AND THEORY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 189th Symposium of the International-Astronomical-Union on Fundamental Stellar Properties - The Interaction Between Observation and Theory CY JAN 13-17, 1997 CL UNIV SYDNEY, WOMENS COLLEGE, SYDNEY, AUSTRALIA SP Int Astron Union HO UNIV SYDNEY, WOMENS COLLEGE ID ABUNDANCE AB I discuss errors in theory and in interpreting observations that are produced by the failure to consider resolution in space, time, and energy. I discuss convection in stellar model atmospheres and in stars. One dimensional convective models can never work well, but the errors in predicted diagnostics for temperature, gravity, and abundances can be calibrated. I discuss the variation of microturbulent velocity with depth, effective temperature, and gravity. These variations must be dealt with in computing models and grids and in any type of photometric calibration. I describe the state of the art in computing a model atmosphere and complete spectrum for stars with arbitrary abundances. I have made no significant progress on atomic or molecular line data for the last two years, but I will soon begin large scale production. I will continue to distribute the results on CD-ROMs, and I will make them available on the World Wide Web. C1 OBSERV MEUDON, F-92195 MEUDON, FRANCE. UNIV COPENHAGEN, DK-1168 COPENHAGEN, DENMARK. RP Kurucz, RL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 19 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4651-3 J9 IAU SYMP PY 1997 IS 189 BP 217 EP 226 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ51R UT WOS:A1997BJ51R00030 ER PT S AU Sasselov, DD AF Sasselov, DD BE Bedding, TR Booth, AJ Davis, J TI Pulsating stellar atmospheres SO FUNDAMENTAL STELLAR PROPERTIES: THE INTERACTION BETWEEN OBSERVATION AND THEORY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 189th Symposium of the International-Astronomical-Union on Fundamental Stellar Properties - The Interaction Between Observation and Theory CY JAN 13-17, 1997 CL UNIV SYDNEY, WOMENS COLLEGE, SYDNEY, AUSTRALIA SP Int Astron Union HO UNIV SYDNEY, WOMENS COLLEGE ID RADIATIVE-TRANSFER; LINE FORMATION; STARS AB We review the basic concepts, present state of theoretical models, and the future prospects for theory and observations of pulsating stellar atmospheres. Our emphasis is on radially pulsating cool stars, which dynamic atmospheres provide a general example for the differences with standard static model atmospheres. RP Sasselov, DD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 24 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4651-3 J9 IAU SYMP PY 1997 IS 189 BP 253 EP 260 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ51R UT WOS:A1997BJ51R00035 ER PT B AU Jones, C Forman, W David, L Churazov, E Gilfanov, M AF Jones, C Forman, W David, L Churazov, E Gilfanov, M BE Soker, N TI Cooling flows and shocks in the temperature structure of clusters SO GALACTIC AND CLUSTER COOLING FLOWS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Galactic and Cluster Cooling Flows CY AUG 05-08, 1996 CL UNIV HAIFA, ORANIM, ISRAEL HO UNIV HAIFA AB We address the observational effects of heating the intracluster medium through the outflow of early galactic winds and through shocks generated by the in fall of subclusters. We show that the ratio of the energy per unit mass in galaxies to that in gas is smallest for cool groups/clusters which we interpret as evidence for significant energy injection. This is confirmed by the weak variation of the entropy as a function of radius for coal groups/clusters, which is consistent with significant energy injection at early epochs. This contrasts with the strong increase in entropy for hot clusters suggesting that early energy injection was less significant and that considerable energy input occurs by shock heating from infalling gas. Evidence for the shock heating can be seen in new cluster temperature maps. For example, we present the temperature map for the Centaurus cluster of galaxies which shows non-isothermal temperature distributions, both a cool region in its care and a hotter localized region outside the central region. In general. we find 25% departures from the mean cluster temperature for even those clusters whose X-ray surface brightness distributions exhibit no evidence of any disturbance or irregularity. Based on the similarity of the observed temperature distributions with those found in numerical simulations, along with results from optical velocity data, we suggest that these temperature features arise from shock heating as additional subclusters accrete onto the cluster. In general for clusters, outside a central cool region, the gas in the core is fairly isothermal, with the exception of local departures, which appear to be associated with mergers. We also discuss the contributions to the total gas temperature of emission from the cooling flow and the hotter shocked regions and their effects an measuring cluster masses through the hydrostatic equation. Finally, we address the "beta problem" and show that much of the discrepancy between cluster gas temperatures and velocity dispersions results from the effects of substructure on the measured velocity dispersions within clusters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jones, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Churazov, Eugene/A-7783-2013 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-35-X J9 ASTR SOC P PY 1997 VL 115 BP 82 EP 91 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK79W UT WOS:000073437600011 ER PT B AU McNamara, BR AF McNamara, BR BE Soker, N TI Optical properties of cooling flow central cluster ellipticals SO GALACTIC AND CLUSTER COOLING FLOWS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Galactic and Cluster Cooling Flows CY AUG 05-08, 1996 CL UNIV HAIFA, ORANIM, ISRAEL HO UNIV HAIFA AB Central cluster galaxies in cooling flows show the signatures of gaseous accretion and ongoing star formation at rates ranging between similar to 1-100 M circle dot yr(-1). Their blue morphologies usually reflect the low net angular momentum content of the T<10(4) K gas from which the accretion population formed, and the effects of interactions between the cool gas and their FR I radio sources. For example, there is strong evidence that star formation is being triggered, in part, by interactions between the T<10(4) K gas and the radio sources in some objects. Disk star formation on kiloparsec scales is rare in cooling flows. The optically determined star formation rates, assuming the local initial mass function (IMF), are typically factors of 10-100 smaller than the cooling rates determined from X-ray observations, and signatures of the remaining material have not been identified outside of the X-ray band. The IMF is poorly understood in cooling flows; most of the cooling material may be deposited in low-mass stars or some other form of dark matter. Continued study of the interactions between raio sources and the intercluster medium will further our understanding of how elliptical galaxies, particularly radio ellipticals in the early universe, evolve. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McNamara, BR (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 30 Z9 30 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-35-X J9 ASTR SOC P PY 1997 VL 115 BP 109 EP 120 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK79W UT WOS:000073437600014 ER PT B AU Evans, IN Kellogg, EM McDermott, WC Ordway, MP Rosenberg, JM Wargelin, BJ AF Evans, IN Kellogg, EM McDermott, WC Ordway, MP Rosenberg, JM Wargelin, BJ BE Hoover, RB Walker, ABC TI High speed imager AXAF calibration microchannel plate detector SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE AXAF calibration; microchannel plate; x-ray instrumentation AB The design and implementation of the High Speed Imager (HSI) microchannel plate based imaging x-ray detector used for the calibration of the Advanced X-ray Astrophysics Facility (AXAF) High Resolution Mirror Assembly (HRMA) and Objective Transmission Gratings (OTGs) is described. The similarities between the HSI and the AXAF High Resolution Camera (HRC) are discussed, as well. as the modifications to the original WRC-like design needed to operate the detector at count rates up to similar to 2000 Hz used during the HRMA calibration. The imaging performance of the detector that is necessary to achieve the calibration error budget for the HRMA is discussed. Details of the actual performance of the HSI are provided in terms of key parameters such as spatial uniformity and linearity, imaging resolution, and counting rate limitations. The measurement techniques used to verify and calibrate the requisite detector performance are described. RP Evans, IN (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 18 EP 29 DI 10.1117/12.278848 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00002 ER PT B AU Fitch, JJ Blake, RL Burek, AJ Clark, AM Graessle, DE Harris, B Schwartz, DA Sweeney, J AF Fitch, JJ Blake, RL Burek, AJ Clark, AM Graessle, DE Harris, B Schwartz, DA Sweeney, J BE Hoover, RB Walker, ABC TI AXAF synchrotron witness mirror calibrations 2-12 keV SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE AXAF; X-ray reflectivity; iridium; optical constants; synchrotron radiation AB We have completed another full year of reflectance calibrations of AXAF witness mirrors at the National Synchrotron Light Source. At the NSLS, we have used Beamlines X8C (5-12 keV) and X8A (2-6.2 keV), sponsored by Los Alamos National Laboratory. All of the flats have been calibrated in the 5-12 keV range, and approximately 1/4 of all our flats have been calibrated in the 2-6.2 keV range. The repeatability in the coating processes reported in Denver has continued with the measurement of additional mirrors. Optical constants from reflectances have been derived for six of the eight AXAF mirror elements, and a degree of spatial uniformity information exists for three of these six. The addition of a semitransparent monitor has markedly increased efficiency of measurements in the 5-12 keV range, and efforts are being made to provide such a monitor detector for the lower energy ranges. We report the progress in reflectance data acquisition and optical constant derivations, and discuss implications of the results for the AXAF program. RP Fitch, JJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 30 EP 39 DI 10.1117/12.278867 PG 10 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00003 ER PT B AU Harris, B Burek, AJ Fitch, JJ Graessle, DE Schwartz, DA Blake, RL Gullikson, EM AF Harris, B Burek, AJ Fitch, JJ Graessle, DE Schwartz, DA Blake, RL Gullikson, EM BE Hoover, RB Walker, ABC TI Determination of optical constants for AXAF mirrors from 0.05-1.0 keV through reflectance measurements SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE AXAF; optical constants; x-rays; synchrotron radiation; x-ray reflectance; iridium AB We discuss calibration of the Advanced X-ray Astrophysics Facility (AXAF) High Resolution Mirror Assembly (HRMA) through the use elf surrogate coating process witness flats. Reflectance measurements of representative witness flats have been made at the Advanced Light Source (ALS) synchrotron facility over an energy range of 60 - 940 eV. We discuss the procedures used for these measurements and some preliminary results of our studies. The initial results show, for some energy regions, a reduction in reflectance expected from a pure iridium coating layer. The observed decrease in mirror reflectance is believed to be the combined result of the presence of an organic thin film on the mirror surfaces, plus the effects of carbon on the ALS beamline optics. It appears that the tested mirror surfaces have a maximum level of molecular contamination amounting to an effective carbon thickness of from 5-10 angstroms. The source of this contamination is not identified, although this amount is not surprising. RP Harris, B (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 40 EP 51 DI 10.1117/12.278876 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00004 ER PT B AU Graessle, DE Burek, AJ Fitch, JJ Harris, B Schwartz, DA Blake, RL AF Graessle, DE Burek, AJ Fitch, JJ Harris, B Schwartz, DA Blake, RL BE Hoover, RB Walker, ABC TI Optical constants from synchrotron reflectance measurements of AXAF witness mirrors, 2-12 keV SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE AXAF; X-ray reflectivity; iridium; optical constants; synchrotron radiation AB We report iridium optical constants fitted from synchrotron reflectance data. Specifically, we have used the NKFIT algorithm of D.L. Windt(1) to derive delta(E) and beta(E) from 2-12 keV reflectance calibrations of AXAF witness mirrors, The model is applied at each energy separately, to fit four to nine data points from reflectance-versus-energy scans at selected grazing angles. The stability of the model in the presence of gaussian noise has been tested extensively. We report the results of several bias studies, involving the generation and analysis of artificial data. Bias studies have been used to determine the optimal grazing angles to be scanned in the various X-ray energy ranges to condition the optical constants. They have also been used to investigate the effects of individual errant data points; on the resulting fits and derived optical constants. The results will aid in eliminating systematic errors in the derived optical constants. We also present results of our investigation of the Debye-Waller(2) and Nevot-Croce(3) roughness correction algorithms as applied to our measurements. The Nevot-Croce method gives a much better representation of the data, however its rigorous justification in this experiment is lacking, and the roughness parameter derived is not constant with energy, A more self-consistent model for roughness correction is sought. RP Graessle, DE (reprint author), SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138, USA. NR 0 TC 8 Z9 8 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 52 EP 64 DI 10.1117/12.278886 PG 13 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00005 ER PT B AU Gaetz, TJ Podgorski, WA Cohen, LM Freeman, MD Edgar, RJ Jerius, D VanSpeybroeck, L Zhao, P Kolodziejczak, J Weisskopf, M AF Gaetz, TJ Podgorski, WA Cohen, LM Freeman, MD Edgar, RJ Jerius, D VanSpeybroeck, L Zhao, P Kolodziejczak, J Weisskopf, M BE Hoover, RB Walker, ABC TI Focus and alignment of the AXAF optics SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE x-ray optics; Wolter type-I; AXAF; alignment AB We discuss the X-ray measurement of the focus and alignment of the AXAF (Advanced X-ray Astrophysics Facility) X-ray optics. The High Resolution Mirror Assembly (HRMA) consists of four nested Welter type I X-ray optics. The attainment of the program goals for high resolution imaging requires that the mirror foci be coincident, both axially and laterally; in addition, the relative tilts between optics within each mirror pair must be small. The mirror tilts and the parfocalization were measured at the X-Ray Calibration Facility (XRCF) at the Marshall Space Flight Center in Huntsville, Alabama during a series of tests in the winter/spring of 1996/1997. The X-ray measurements are compared to the optical alignment data obtained by Eastman Kodak using the HRMA Alignment and Test System (HATS) during HRMA assembly. From these data a preliminary model for the relative location and rigid-body orientation of the individual mirror elements is developed; this mirror model is a component of the SAO high fidelity HRMA raytrace model. RP Gaetz, TJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138, USA. NR 0 TC 7 Z9 7 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 77 EP 88 DI 10.1117/12.278839 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00007 ER PT B AU VanSpeybroeck, LP Jerius, D Edgar, R Gaetz, T Zhao, P Reid, P AF VanSpeybroeck, LP Jerius, D Edgar, R Gaetz, T Zhao, P Reid, P BE Hoover, RB Walker, ABC TI Performance expectation versus reality SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE x-ray optics; AXAF; performance predictions AB The AXAF (Advanced X-ray Astrophysics Facility) High Resolution Mirror Assembly (HRMA) now is complete and has been tested at the NASA Marshall Space Flight Center (MSFC) X-ray Calibration Facility (XRCF). The surface and alignment properties of the mirror were thoroughly measured before the X-ray test, which allowed accurate performance predictions to be performed. The preliminary analysis of the measured X-ray image distributions for all energies tested show excellent agreement with predictions made before the beginning of the test. There is a discrepancy between the measured and predicted effective areas; this typically is less than 5%, and is less than 13% for all energies measured. We present evidence that this discrepancy is due to uncertainties in the calibration of the test instrumentation, and therefore can be expected to be reduced when results from further instrument calibration tests now in progress are incorporated into the analysis. We predict that 65-80% (depending upon energy) of the flux from an imaged point source will be contained in a one arc second diameter aperture in flight. We expect the HRMA to more than fulfill the requirements necessary to achieve the AXAF scientific objectives. RP VanSpeybroeck, LP (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 65 Z9 65 U1 0 U2 1 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 89 EP 105 DI 10.1117/12.278890 PG 17 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00008 ER PT B AU Zhao, P Cohen, LM VanSpeybroeck, LP AF Zhao, P Cohen, LM VanSpeybroeck, LP BE Hoover, RB Walker, ABC TI AXAF HRMA mirror ring focus measurements SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE AXAF; HRMA; X-ray mirrors; ring focus AB We discuss the ring focus measurements for the Advanced X-ray Astrophysics Facility (AXAF) X-ray optics - the High Resolution Mirror Assembly (HRMA). The HRMA is an assembly of four pairs of nested Wolter Type-I grazing incidence mirrors coated with iridium (Trf. The ring focus measurements are an essential part of the AXAF ground calibration carried out at the X-Ragi Calibration Facility (XRCF) at the Marshall Space Flight Center (MSFC) in Huntsville, AL. The ring focus measurements reveal aspects of the test system distortions and the mirror surface figures which are difficult or impossible to detect in the focal plane, The measurement results show periodic modulations of the ring width which was caused by gravity and strain in the epoxy bonds that are part of the mechanical support system. The strongest component of the modulation has 12-fold symmetry due to the 12 flexures that support each mirror shell. We discuss the ring focus model and compare it with the test results to understand the test system distortions and the mirror glass imperfection, and to predict the impact for the AXAF mirror on-orbit performance. RP Zhao, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 4 Z9 4 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 106 EP 123 DI 10.1117/12.278840 PG 18 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00009 ER PT B AU Edgar, RJ Tsiang, EY Tennant, A Vitek, S Swartz, D AF Edgar, RJ Tsiang, EY Tennant, A Vitek, S Swartz, D BE Hoover, RB Walker, ABC TI Spectral fitting in AXAF calibration detectors SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE x-ray optics; Wolter type-I; AXAF; calibration; spectral fitting AB We discuss details of the spectral fitting procedures and algorithms used in deriving fine count rates for the calibration of AXAF (the Advanced X-ray Astrophysics Facility) during end-to-end testing in the winter and spring of 1996/1997. An approach involving simultaneously fitting both detector and source parameters was implemented within XSPEC, a standard x-fay spectral fitting package (Arnaud 1996). Theoretical and practical difficulties in fitting spectra taken with Flow Proportional Counters (FPC) and Solid State Detectors (SSD) will be discussed, including bath effects incorporated into the numerical model: and those which must be estimated outside the model. Sensitivity of the parameter of interest, the counts in a strong line in the spectrum, to changes and errors in the other fit parameters is explored. The impact of uncertainties on the overall absolute AXAF calibration is discussed. RP Edgar, RJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138, USA. NR 0 TC 4 Z9 4 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 124 EP 131 DI 10.1117/12.278841 PG 8 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00010 ER PT B AU Tsiang, EY Edgar, RE Vitek, S Tennant, A AF Tsiang, EY Edgar, RE Vitek, S Tennant, A BE Hoover, RB Walker, ABC TI JMKMOD, a software suite within XSPEC for the ground calibration of AXAF SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE AXAF X-ray optics; detectors; calibration; spectral fitting; synchrotron radiation AB We describe here the computer program for modeling the FPCs and SSDs used in the ground calibration, relative and absolute, of AXAF. The program is called as a subroutine by XSPEC. The design is hierarchical: at the lowest level are models for single electron spectra, upon which are based the computation of moment generating functions(mg;fs) for the detector response functions, Any number of discrete lines and a continuum are allowed. The continuum is the source X-ray spectrum as modified by intervening filters. The overall mgf is numerically transformed into the count spectrum via an inverse Fast Fourier Transform. The component mgfs have unit normalization, and final fitted normalizations give the count rate for each component. RP Tsiang, EY (reprint author), SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138, USA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 132 EP 141 DI 10.1117/12.278842 PG 10 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00011 ER PT B AU Romaine, S Hussain, A Everett, J Clark, A Bruni, R Gorenstein, P Ghigo, M Mazzoleni, F Citterio, O Pedulla, J AF Romaine, S Hussain, A Everett, J Clark, A Bruni, R Gorenstein, P Ghigo, M Mazzoleni, F Citterio, O Pedulla, J BE Hoover, RB Walker, ABC TI Application of multilayer coatings to replicated substrates SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE x-ray telescopes; multilayers; replicated substrates AB We are engaged in a program to develop focussing hard X-ray telescopes in a double conical or Welter 1 geometry that function up to 100 keV by employing small graze angles and multilayer coatings. Directly polished substrates are not an option because they are too thick to be nested efficiently. The only alternative is to fabricate the very thin substrates by replication. Our objective is the production of integral cylindrical substrates because they should result in better angular resolution than segmented foil geometries. In addition, integral cylinders would be mure resistant to possible stress from deep multilayer coatings than segmented ones. Both electroforming of nickel (method of SAX, JE:T-X, and XMM) and epoxy replication are under consideration. Both processes can utilize the same types of mandrels and separation agents. While electroforming can produce substrates that are thin, the high density of the nickel may result in high weight optics for some missions. For convenience, experimentation with replication and coating is being carried out initially on fiats. Our replication studies include trials with gold and carbon separation agents. This paper reports on our efforts with epoxy replicated optics. RP Romaine, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 6 Z9 6 U1 0 U2 3 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 253 EP 259 DI 10.1117/12.278854 PG 7 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00022 ER PT B AU Hussain, AM Romaine, S Gorenstein, P Everett, J Bruni, R Clark, A Ruane, M Fedyunin, Y AF Hussain, AM Romaine, S Gorenstein, P Everett, J Bruni, R Clark, A Ruane, M Fedyunin, Y BE Hoover, RB Walker, ABC TI Studying density vs. Ar-pressures for optimization of DC-magnetron sputter deposition of Ni/C multilayers for hard X-ray telescopes SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE DC-magnetron sputtering; X-ray Telescopes; multilayers; X-ray reflection measurements; AFM-measurements; Ar-pressure; Density; TEM-measurements AB The influence of varying the Ar-pressure in the process of depositing Ni/C multilayers by DC-magnetron sputtering has been studied, and Atomic Force Microscopy (AFM) measurements, X-ray characterization results and Transmission Electron Microscopy (TEM) results are presented. Single Ni and C films and Ni/C multilayers were deposited at Ar-pressures of 1.5, 3, 5 and 7 mTorr. The one-dimensional power spectral density data from the AFM measurements clearly indicate that the best densities and film qualities for both materials are obtained at lower Ar-pressures, i.e. 1.5 mTorr. RP Hussain, AM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 260 EP 266 DI 10.1117/12.278855 PG 7 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00023 ER PT B AU Kellogg, E Cohen, L Edgar, R Evans, I Freeman, M Gaetz, T Jerius, D McDermott, WC McKinnon, P Murray, S Podgorski, W Schwartz, D VanSpeybroeck, L Wargelin, B Zombeck, M Weisskopf, M Elsner, R ODell, S Tennant, A Kolodziejczak, J Garmire, G Nousek, J Kraft, S Scholze, F Thornagel, R Ulm, G Flanagan, K Dewey, D Bautz, M Texter, S Arenberg, J Carlson, R AF Kellogg, E Cohen, L Edgar, R Evans, I Freeman, M Gaetz, T Jerius, D McDermott, WC McKinnon, P Murray, S Podgorski, W Schwartz, D VanSpeybroeck, L Wargelin, B Zombeck, M Weisskopf, M Elsner, R ODell, S Tennant, A Kolodziejczak, J Garmire, G Nousek, J Kraft, S Scholze, F Thornagel, R Ulm, G Flanagan, K Dewey, D Bautz, M Texter, S Arenberg, J Carlson, R BE Hoover, RB Walker, ABC TI Absolute calibration of the AXAF telescope effective area SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers AB The prelaunch calibration of AXAF encompasses many aspects of the telescope. In principle, all that is needed is the complete point response function. This is, however, a function of energy, off-axis angle of the source, and operating mode of the facility. No single measurement would yield the entire result. Also, any calibration made prior to launch will be affected by changes in conditions after launch, such as the change from one g to zero g. The reflectivity of the mirror and perhaps even the detectors can change as well, for example by addition or removal of small amounts of material deposited on their surfaces. In this paper, we give a broad view of the issues in performing such a calibration, and discuss how they are being addressed in prelaunch preparation of AXAF;. As our title indicates, we concentrate here on the total throughput of the observatory. This can be thought of as the integral of the point response function, i.e. the encircled energy, out to the largest practical solid angle for an observation. Since there is no standard x-ray source in the sky whose flux is well known to the similar to 1% accuracy we are trying to achieve, we must do this calibration on the ground. We also must provide a means for monitoring any possible changes in this calibration from prelaunch until on-orbit operation can transfer the calibration to a celestial x-ray source whose emission is stable. In the paper, we analyze the elements of the absolute throughput calibration, which we call the Effective Area. We review the requirements for calibrations of components or subsystems of the AXAF facility, including the mirror, detectors, and gratings. We show how it is necessary to have an absolute calibrated detection system available during the prelaunch calibrations to measure the flux in the x-ray beam used for calibrating AXAF. We show how it is necessary to calibrate this ground-based detection system at standard man-made x-ray sources, such as electron storage rings. We present the status of all these calibrations, with indications of the measurements remaining to be done, even though the measurements on the AXAF flight optics and detectors will have been completed by the time this paper is presented. We evaluate progress toward the goal of making 1% measurements of the absolute x-ray flux from astrophysical sources, so that comparisons can be made with their emission at other wavelengths, in support of observations such as the Sunyaev-Zeldovitch effect, which can give absolute distance measurements independent of the traditional distance measuring techniques in astronomy. RP Kellogg, E (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Ulm, Gerhard/D-4798-2009; OI O'Dell, Stephen/0000-0002-1868-8056 NR 0 TC 7 Z9 7 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 515 EP 525 DI 10.1117/12.278885 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00051 ER PT B AU Wargelin, BJ Kellogg, EM McDermott, WC Evans, IN Vitek, SA AF Wargelin, BJ Kellogg, EM McDermott, WC Evans, IN Vitek, SA BE Hoover, RB Walker, ABC TI AXAF calibration: The HXDS flow proportional counters SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE AXAF; calibration; proportional counters; X-ray detectors AB The design, performance, and calibration of the seven Flow Proportional Counters (FPCs) used during AXAF ground calibration are described. Five of the FPCs served as Beam Normalization Detectors (BNDs), and two were used in the telescope focal plane in combination with a set of apertures to measure the point, response functions and effective areas of the AXAF mirrors and transmission gratings. The BNDs also provide standards for determining the effective areas of the several telescope/grating/flight-detector combinations. With useful energy resolution and quantum efficiency over the entire 100-eV to 10-keV AXAF energy band, the FPCs provided most of the data acquired during AXAF calibration. Although the principles of proportional counter operation ase relatively simple, AXAF's stringent calibration goals require detailed calibration and modeling of such effects as window-support-wire obscuration, window deformation between the support wires, electron diffusion and avalanche processes, gain nonuniformities, and gas pressure and temperature variations. Detector aperture areas and signal processing deadtime must also be precisely determined, and detector degradation during the many months of AXAF calibration must be prevented. The FPC calibration program is based on measurement of individual components (such as window transmission and aperture size) and the relative quantum efficiencies of complete detector systems, as well as absolute QE calibration of selected detectors at the BESSY synchrotron, an X-ray source of precisely known intensity. RP Wargelin, BJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV,MS-27,CAMBRIDGE,MA 01238, USA. NR 0 TC 6 Z9 6 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 526 EP 534 DI 10.1117/12.278887 PG 9 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00052 ER PT B AU McDermott, WC Kellogg, EM Wargelin, BJ Evans, IN Vitek, SA Tsiang, EY Schwartz, DA Edgar, R Kraft, S Scholze, F Thornagel, R Ulm, G Weisskopf, M Odell, S Tennant, A Kolodziejczak, J Zirnstein, G AF McDermott, WC Kellogg, EM Wargelin, BJ Evans, IN Vitek, SA Tsiang, EY Schwartz, DA Edgar, R Kraft, S Scholze, F Thornagel, R Ulm, G Weisskopf, M Odell, S Tennant, A Kolodziejczak, J Zirnstein, G BE Hoover, RB Walker, ABC TI The AXAF HXDS germanium solid state detectors SO GRAZING INCIDENCE AND MULTILAYER X-RAY OPTICAL SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Grazing Incidence and Multilayer X-ray Optical Systems CY JUL 27-29, 1997 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE AXAF; solid state detectors; X-ray detectors; absolute calibration AB The design, calibration, and performance of the High Purity Germanium (HPGe) solid state detectors (SSD's) used in the calibration of the Advanced X-ray Astrophysics Facility High Resolution Mirror Assembly (HRMA) is discussed. The focal plane SSD was used with various apertures to measure the point response function, as well as the effective area of the mirror. The good energy resolution of the detector allowed the effective energy of the mirrors to be measured with a single exposure using a continuum source. The energy resolution was also exploited in measuring the molecular contamination on the mirror surfaces. The SSD's are the transfer detector standards for the HRMA calibration over the energy range from 700 eV to 10 keV. The calibration of the SSD's was performed mostly at the PTB radiometry laboratory using the electron storage ring BESSY. The spectral and spacial distribution of the undispersed synchrotron radiation can be calculated from first principles using the Schwinger Equation. With the electron storage ring being run in a reduced current mode of a few electrons, uncertainties in the calculated flux are below 1%. A comparison of the measured and calculated flux made it possible to determine the detector efficiency with an uncertainty of typically 1%. Electronic effects such as pile-up, count rate linearity and deadtime have been investigated. RP McDermott, WC (reprint author), SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138, USA. RI Ulm, Gerhard/D-4798-2009 NR 0 TC 2 Z9 2 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-2535-4 J9 P SOC PHOTO-OPT INS PY 1997 VL 3113 BP 535 EP 543 DI 10.1117/12.278888 PG 9 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BJ31L UT WOS:A1997BJ31L00053 ER PT J AU Snyder, LM AF Snyder, LM TI Frankish Corinth: 1996 SO HESPERIA LA English DT Article RP Snyder, LM (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,MRC 112,WASHINGTON,DC 20560, USA. NR 18 TC 1 Z9 1 U1 0 U2 0 PU AMER SCHOOL CLASS STUDIES PI PRINCETON PA C/O INST FOR ADVANCED STUDY, PRINCETON, NJ 08540 SN 0018-098X J9 HESPERIA JI Hesperia PD JAN-MAR PY 1997 VL 66 IS 1 BP 7 EP & DI 10.2307/148474 PG 58 WC Archaeology SC Archaeology GA WL825 UT WOS:A1997WL82500002 ER PT S AU Green, PJ Aldcroft, TA Garcia, MR Slane, P Vrtilek, J AF Green, PJ Aldcroft, TA Garcia, MR Slane, P Vrtilek, J BE OFlaherty, KS TI Using the Tycho Catalogue for AXAF: Guiding and aspect reconstruction for half-arcsecond X-ray images SO HIPPARCOS VENICE '97 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Hipparcos Venice 97 CY MAY 13-16, 1997 CL VENICE, ITALY SP European Space Sgcy, City Venice, Fdn Cini DE space astrometry; X-rays AB AXAF, the Advanced X-ray Astrophysics Facility will be the third satellite in the series of great observatories in the NASA program, after the Hubble Space Telescope and the Gamma Ray Observatory. At launch in fall 1998, AXAF will carry a high resolution mirror, two imaging detectors, and two sets of transmission gratings (Holt 1993). Important AXAF features are: an order of magnitude improvement in spatial resolution, good sensitivity from 0.1-10keV, and the capability for high spectral resolution observations over most of this range. The Tycho Catalogue from the Hipparcos mission will serve as a primary part of the AXAF Guide and Aspect Star Catalog (AGASC), particularly as merged with other star catalogues. Incorporation of the Tycho Catalogue into AGASC will provide: (1) accurate positions and magnitudes for target acquisition and guiding; (2) the colours necessary for magnitude transformations to the AXAF Aspect Camera (ACA) system; (3) high internal astrometric accuracy for half-arcsecond post-facto image reconstruction; and (4) an external astrometric system that will tie AXAF X-ray image astrometry into the best positional system expected well beyond the mission lifetime and into the next millennium. RP Green, PJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-291-5 J9 ESA SP PUBL PY 1997 VL 402 BP 187 EP 190 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ70B UT WOS:A1997BJ70B00046 ER PT J AU Chambers, JE AF Chambers, JE TI Why Halley-types resonate but long-period comets don't: A dynamical distinction between short- and long-period comets SO ICARUS LA English DT Article AB Several recent studies have noted that the orbital evolution of many comets is influenced by mean-motion resonances with Jupiter. However, the distribution and relative importance of these resonances and the orbital characteristics of the comets affected have not been addressed to date. Here I show analytically that cometary orbits with periods greater than a critical value, P-c, (which depends upon the orbital inclination) are prevented from undergoing librations about a mean-motion resonance. Conversely, numerical integrations indicate that resonances play an important role in the dynamics of comets with P < P-c. The inclination-averaged value of P-c approximately coincides with the traditional and arbitrary dividing line between Halley-type and long-period comets, which explains why many of the former are currently observed to be in resonance, whereas the latter are not. Thus, we now have a dynamical justification for separating comets into those of short and long period. (C) 1997 Academic Press C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Chambers, JE (reprint author), CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,5241 BROAD BRANCH RD NW,WASHINGTON,DC 20015, USA. NR 10 TC 13 Z9 13 U1 1 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD JAN PY 1997 VL 125 IS 1 BP 32 EP 38 DI 10.1006/icar.1996.5567 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE897 UT WOS:A1997WE89700003 ER PT J AU Ceruzzi, P AF Ceruzzi, P TI Crossing the divide: Architectural issues and the emergence of the stored program computer, 1935-1955 SO IEEE ANNALS OF THE HISTORY OF COMPUTING LA English DT Article AB The rapid advance of computing technology since the 1940s has created an impression that all that happened in computing before then was somehow mere prologue to the real history. According to this popular notion, the computer age began with the invention of machines that computed at electronic speeds, that were capable of automatic sequence control with conditional branching, and that stored their programs internally. The classification of computing into ''generations'' with the ''first'' generation being those with vacuum tubes further reinforces this notion. This paper looks at some examples of machines built in the 1930s and 1940s that straddle both ages: machines that had some sort of sequence control partially electronic counting circuits, or primitive branching capabilities. In particular, I examine a few systems that reveal especially well the nature of this transition: the ensembles of punched card equipment used by L.J. Comrie and Wallace Eckert for scientific instead of business use; the ''Aberdeen Relay Calculator'' that IBM built for the U.S. Army; and the ''Card Programmed Calculator'' that Northrop Aircraft invented for engineering applications that IBM later marketed. RP Ceruzzi, P (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20506, USA. NR 62 TC 12 Z9 12 U1 0 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 SN 1058-6180 J9 IEEE ANN HIST COMPUT JI IEEE Ann. Hist. Comput. PD JAN-MAR PY 1997 VL 19 IS 1 BP 5 EP 12 DI 10.1109/85.560724 PG 8 WC Computer Science, Theory & Methods; History & Philosophy Of Science SC Computer Science; History & Philosophy of Science GA WC681 UT WOS:A1997WC68100002 ER PT J AU McCormick-Goodhart, MH Tumosa, CS Mecklenburg, MF AF McCormick-Goodhart, MH Tumosa, CS Mecklenburg, MF TI Predicting the environmental response of gelatin containing composite structures SO IMAGING SCIENCE JOURNAL LA English DT Article; Proceedings Paper CT Royal-Photographic-Society Conference on Photographic Gelatin CY SEP 15-19, 1997 CL CAMBRIDGE, ENGLAND SP Royal Photograph Soc AB The mechanical response of objects having a complex composite structure can be accurately modeled if the material properties of the individual components are characterized using the approach briefly described in this paper. The three dimensional surface of the equilibrium stress-strain state and the methods required for its determination were the subject of several years of research by the authors. More detailed explanation of the experimental technique and mathematical treatment can be found in previous papers by the authors. C1 Smithsonian Inst, Washington, DC 20560 USA. RP McCormick-Goodhart, MH (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ROYAL PHOTOGRAPHIC SOC PI BATH PA OCTAGON-MILSOM ST, BATH, AVON, ENGLAND BA1 1DN SN 1368-2199 J9 IMAGING SCI J JI Imaging Sci. J. PY 1997 VL 45 IS 3-4 BP 244 EP 245 PG 2 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA ZF146 UT WOS:000072867600035 ER PT J AU Wcislo, WT AF Wcislo, WT TI Social interactions and behavioral context in a largely solitary bee, Lasioglossum (Dialictus) figueresi (Hymenoptera, Halictidae) SO INSECTES SOCIAUX LA English DT Article DE social competition; dominance; social behavior; kinship ID LASIOGLOSSUM-(DIALICTUS)-FIGUERESI WCISLO; GENEALOGICAL RELATIONSHIP; DOMINANCE HIERARCHY; RECOGNITION; COMPETITION; EVOLUTION; CONFLICT; COLONIES; ZEPHYRUM; SIZE AB Understanding the development of behavioral differences among group members is a key to understanding social evolution or its loss. Social sweat bees (Halictinae) show distinct behaviors related to social competition and cooperation, and the frequencies of these behaviors differ for different functional groups (workers, guards, queens). These behaviors occur in solitary halictine bees under artificial conditions in a circular arena involving pairs of interacting bees. Reproductively active bees were tested, as were reproductively inactive bees, both from different nests and the same nests within a nesting aggregation. Among reproductively active bees, the first bee to display aggressive behavior more frequently had larger ovaries, and the first bee to withdraw from a social encounter more frequently had smaller ovaries. Body size did not influence these outcomes. The first bee placed in the arena was more likely to adopt an aggressive posture when bees first met, and the second bee placed in the arena was more likely to withdraw. Among reproductively inactive bees. females paired with a bee taken from the same nest were less likely to be aggressive than a bee paired with one from a different nest, suggesting familiarity (possibly kinship) can modulate aggressive behavior. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 49 TC 34 Z9 37 U1 1 U2 11 PU BIRKHAUSER VERLAG AG PI BASEL PA PO BOX 133 KLOSTERBERG 23, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PY 1997 VL 44 IS 3 BP 199 EP 208 DI 10.1007/s000400050041 PG 10 WC Entomology SC Entomology GA XW559 UT WOS:A1997XW55900002 ER PT J AU Arnoldi, MJ AF Arnoldi, MJ TI Status and identity in West Africa: Nyamakalaw of Mande - Conrad,DC, Frank,BE SO INTERNATIONAL JOURNAL OF AFRICAN HISTORICAL STUDIES LA English DT Book Review RP Arnoldi, MJ (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AFRICAN STUDIES CENTER PI BOSTON PA BOSTON UNIVERSITY 270 BAY STATE ROAD, BOSTON, MA 02215 SN 0361-7882 J9 INT J AFR HIST STUD JI Int. J. Afr. Hist. Stud. PY 1997 VL 29 IS 3 BP 615 EP 616 DI 10.2307/221379 PG 2 WC History SC History GA XT672 UT WOS:A1997XT67200023 ER PT J AU Bi, SP Du, SD Correll, DL AF Bi, SP Du, SD Correll, DL TI Estimation of aluminum speciation in surface waters of low ionic strength by a simple computer model SO INTERNATIONAL JOURNAL OF ENVIRONMENTAL ANALYTICAL CHEMISTRY LA English DT Article DE aluminum speciation; computer simulation; surface water ID HUMIC SUBSTANCES; NATURAL-WATERS; EQUILIBRIUM CALCULATIONS; AQUEOUS ALUMINUM; SOIL SOLUTIONS; NEW-YORK; CHEMISTRY; FLOW; PH; COMPLEXATION AB A simple computer model based on chemical equilibrium calculation for evaluating the aluminum speciation in surface waters of low ionic strength (I < 1 x 10(-4) M) was presented in this paper. The speciations of aluminum obtained by this model have been compared with those obtained experimentally and the reasons for the observed differences have been discussed. This model has been applied to the estimation of aluminum speciation in practical surface waters sampling from areas of the United Kingdom, United States and People's Republic of China. Some valuable conclusions are obtained. C1 Nanjing Univ, Dept Chem, State Pilot Lab Coast & Isl Exploitat, Nanjing, Peoples R China. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Bi, SP (reprint author), Nanjing Univ, Dept Chem, State Pilot Lab Coast & Isl Exploitat, Nanjing, Peoples R China. NR 38 TC 10 Z9 11 U1 0 U2 1 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD, PO BOX 90, READING RG1 8JL, BERKS, ENGLAND SN 0306-7319 J9 INT J ENVIRON AN CH JI Int. J. Environ. Anal. Chem. PY 1997 VL 68 IS 4 BP 479 EP 495 DI 10.1080/03067319708030848 PG 17 WC Chemistry, Analytical; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA 167AK UT WOS:000078610300006 ER PT J AU Ryland, JS AF Ryland, JS TI Reproduction in Zoanthidea (Anthozoa: Hexacorallia) SO INVERTEBRATE REPRODUCTION & DEVELOPMENT LA English DT Article; Proceedings Paper CT 7th International Congress on Invertebrate Reproduction CY AUG 05-11, 1995 CL UNIV OF CALIF AT SANTA CRUZ, SANTA CRUZ, CA SP Int Soc Invertebrate Reprod HO UNIV OF CALIF AT SANTA CRUZ DE Gametogenesis; fecundity; spawning; zoanthella; zoanthina; cloning; zooxanthellae; palytoxin; Great Barrier Reef ID GREAT-BARRIER-REEF; CORAL-REEF; TROPICAL ZOANTHID; CLONAL CNIDARIAN; ACTINIA-FRAGACEA; PROTOPALYTHOA SP; GROWTH; POPULATIONS; ECOLOGY AB The state of knowledge concerning the reproductive biology of zoanthids is reviewed. Colonies in the suborder Macrocnemina, with few exceptions, are gonochoric; those in Brachycnemina are probably basically hermaphroditic but accurate sampling in colonies that fragment is difficult and exceptions by species or populations occur. Two deepsea species of Epizoanthus breed continuously but temperate shallow water zoanthids, and those in the tropics outside similar to 15 degrees latitude are iteroparous with spawning in summer or when temperatures are rising. Oogenesis occurs over a few months but the spawning event may be very brief. Parazoanthus parasiticus in Bermuda spawns mainly on 1-2 nights in late August or September, apparently at full moon; Protopalythoa sp. 1, and probably Palythoa caesia in the Great Barrier Reef spawn 3-5 nights after full moon in November (early summer). These species with short, precisely defined spawning seasons may undergo a second, smaller-scale spawning event one month after the first. Some intertidal populations seem rarely to reproduce sexually, and there have been no studies on the annual cycles of zoanthids in near equatorial waters. With few exceptions gametogenesis occurs only in non-directive macrosepta; in hermaphroditic colonies oocytes and sperm cysts may be intermingled on the same septa or be separate. Germ cells in Isozoanthus giganteus originate only from the endocoelic face of the septa, but this has not been confirmed in other species. Nutritive structures (trophonemata) are present both in oocytes and sperm cysts, in the latter functioning also for the egress of sperm. Trophonemata may be conspicuous, as in Par, parasiticus, or poorly developed, as in Protopalythoa sp. 1. Live eggs vary from similar to 300 mu m (most zoanthids) to similar to 500 mu m diameter in Palythoa spp.; in the two mass spawning species from the Great Barrier Reef they are shed as compact ovoid egg (or egg/sperm) bundles. Fecundity in zoanthids, from few studies, is variable and dependent on polyp size; estimates of 100-300x10(3) ova 100 cm(-2) of colony have been made for Caribbean reef species. Internal brooding is known definitely only in Isozoanthus giganteus. Amongst zooxanthellate zoanthids, only Protopalythoa sp. 1 is known to transmit zooxanthellae via its oocytes. Several zoanthids are known to produce palytoxin but it is unclear to what extent the toxin accumulates in the ova. Larval development is summarized. Zoanthella-larvae are known to be produced in Palythoa, Protopalythoa and Sphenopus, and zoanthina-larvae in Isaurus and Zoanthus, all Brachycnemina. Larval type in Epizoanthus and Parazoanthus, both Macrocnemina, is unknown. Early metamorphosis of zoanthella and zoanthina larvae has been reported but not studied; older larvae, taken from the plankton, may have lost competency to settle. All zoanthids, except Sphenopus, form colonies, clones, or mixtures of the two, and propagate by budding. Attention is drawn to unusual methods of budding or cloning in Acrozoanthus, Isaurus, Palythoa, Sphenopus, and Parazoanthus axinellae. In reefal Isaurus, Protopalythoa, and Zoanthus actual colony size remains small due to fragmentation, but genet size may be substantial. Population structure depends on the interplay of recruitment, fragmentation, and local dispersal. C1 UNIV COLL SWANSEA, SCH BIOL SCI, SWANSEA SA2 8PP, W GLAM, WALES. RP Ryland, JS (reprint author), SMITHSONIAN MARINE STN, LINK PORT, FL 34946 USA. NR 68 TC 46 Z9 48 U1 1 U2 22 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0792-4259 EI 2157-0272 J9 INVERTEBR REPROD DEV JI Invertebr. Reprod. Dev. PD JAN PY 1997 VL 31 IS 1-3 BP 177 EP 188 DI 10.1080/07924259.1997.9672575 PG 12 WC Reproductive Biology; Zoology SC Reproductive Biology; Zoology GA WH555 UT WOS:A1997WH55500019 ER PT J AU Norman, MD Sweeney, MJ AF Norman, MD Sweeney, MJ TI The shallow-water octopuses (Cephalopoda: Octopodidae) of the Philippines SO INVERTEBRATE TAXONOMY LA English DT Article ID BODY PATTERNS AB The shallow-water octopuses of the Philippines are diagnosed on the basis of material collected in a series of expeditions by the Smithsonian Institution to the region between 1978 and 1990. Twenty species of shallow-water octopuses are recognised, 18 in the genus Octopus, and one species each in the genera Hapalochlaena and Cistopus. Three new species are described from Philippine waters: Octopus abaculus, O. nocturnus and O. pumilus. Octopuses reported in the earlier work of G. L. Voss on the cephalopod fauna of the Philippines are reviewed and identifications updated. A diagnostic key and illustrations are provided along with information on taxonomy, distribution, aspects of life history and importance in fisheries. C1 MUSEUM VIC,DEPT INVERTEBRATE ZOOL,MELBOURNE,VIC 3000,AUSTRALIA. NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,SMITHSONIAN INST,WASHINGTON,DC 20560. RP Norman, MD (reprint author), UNIV MELBOURNE,DEPT ZOOL,PARKVILLE,VIC 3052,AUSTRALIA. NR 80 TC 40 Z9 44 U1 0 U2 12 PU C S I R O PUBLICATIONS PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD VICTORIA 3066, AUSTRALIA SN 0818-0164 J9 INVERTEBR TAXON JI Invertebr. Taxon. PY 1997 VL 11 IS 1 BP 89 EP 140 DI 10.1071/IT95026 PG 52 WC Zoology SC Zoology GA WJ596 UT WOS:A1997WJ59600002 ER PT B AU Westermeyer, B Wang, CH Felley, J AF Westermeyer, B Wang, CH Felley, J BE Cibbarelli, PR Nixon, C TI Multimedia and SIRIS: Integrating multimedia data with an IOLS at the Smithsonian Institution SO IOLS '97: INTEGRATED ONLINE LIBRARY SYSTEMS, PROCEEDINGS - 1997: EXPANDING EXPECTATIONS LA English DT Proceedings Paper CT 12th Integrated Online Library Systems Meeting on Expanding Expectations (IOLS 97) CY MAY 14-15, 1997 CL NEW YORK, NY SP Informat Today Inc DE multimedia resources; digital resources; USMARC format; 856 tag; hyperlinks; museums AB This paper discusses pilot projects undertaken at the Smithsonian Institution to link multimedia resources to bibliographic records for retrieval via the Web. Since 1983 the Smithsonian Institution has maintained a shared catalog system called SIRIS (Smithsonian Institution Research Information System). This IOLS-based system contains bibliographic records describing collections held by libraries, archives and research offices across the Smithsonian Institution. Through use of industry standards (USMARC and Z39.50) and commercially available software, the Smithsonian Institution is linking full text, html publications, Images, and videos to records in the SIRIS catalogs. This paper is an overview of the pilot projects, including our project goals and discoveries. It concludes with a list of concerns we have about using current IOLS technologies for searching and presenting multimedia resources. C1 SMITHSONIAN INST,OFF INFORMAT TECHNOL,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 0 PU INFORMATION TODAY INC PI MEDFORD PA 143 OLD MARLTON PIKE, MEDFORD, NJ 08055 BN 1-57387-042-0 PY 1997 BP 161 EP 170 PG 10 WC Information Science & Library Science SC Information Science & Library Science GA BJ41Y UT WOS:A1997BJ41Y00020 ER PT B AU McCormackGoodhart, M AF McCormackGoodhart, M GP SOC IMAGING SCI & TECHNOL TI Moisture buffering properties of photographic materials SO IS&T 50TH ANNUAL CONFERENCE, FINAL PROGRAM AND PROCEEDINGS LA English DT Proceedings Paper CT 50th Annual Meeting of the Society-of-Imaging-Science-and-Technology CY MAY 18-23, 1997 CL CAMBRIDGE, MA SP Soc Imaging Sci & Technol AB Recent moisture content isoline studies of unhardened photographic gelatin revealed that the gelatin emulsion can over buffer a sealed or quasi-sealed microclimate when the gelatin is below its glass transition (T-g) temperature. This behavior causes a decreasing relative humidity in the microclimate upon cooling and increasing relative humidity upon heating. A stable RH level with wide change in temperature was also determined when the gelatin is above T-g. In this paper, the moisture buffering propel-ties of gelatin emulsions when acting in combination with typical photographic supports, i.e., paper, cellulose acetate, polyester, and resin coated paper, will be discussed. RP McCormackGoodhart, M (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC IMAGING SCIENCE & TECHNOLOGY PI SPRINGFIELD PA 7003 KILWORTH LANE, SPRINGFIELD, VA 22151 BN 0-89208-199-6 PY 1997 BP 578 EP 578 PG 1 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA BJ88J UT WOS:A1997BJ88J00153 ER PT B AU McCormickGoodhart, MH Holmes, J AF McCormickGoodhart, MH Holmes, J GP SOC IMAGING SCI & TECHNOL TI Preserving original image content in high-resolution digital archives SO IS&T 50TH ANNUAL CONFERENCE, FINAL PROGRAM AND PROCEEDINGS LA English DT Proceedings Paper CT 50th Annual Meeting of the Society-of-Imaging-Science-and-Technology CY MAY 18-23, 1997 CL CAMBRIDGE, MA SP Soc Imaging Sci & Technol AB High-resolution digital image archives Rave been an unrealistic goal to date because the Barge file sizes generated for each image have taxed both computer processing power and storage requirements, The new ''FlashPix(TM)'' file format dramatically alters the relationship between file size and access time, and projects are under way at the Smithsonian Institution and the Museum of Modem Act to evaluate new approaches to creating high quality digital images of objects in our museum collections. Strategies and benefits of high-resolution digital imaging for museums and archives are discussed in this paper. RP McCormickGoodhart, MH (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC IMAGING SCIENCE & TECHNOLOGY PI SPRINGFIELD PA 7003 KILWORTH LANE, SPRINGFIELD, VA 22151 BN 0-89208-199-6 PY 1997 BP 584 EP 587 PG 4 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA BJ88J UT WOS:A1997BJ88J00156 ER PT J AU Strickman, D Sithiprasasna, R Southard, D AF Strickman, D Sithiprasasna, R Southard, D TI Bionomics of the spider, Crossopriza lyoni (Araneae, Pholcidae), a predator of dengue vectors in Thailand SO JOURNAL OF ARACHNOLOGY LA English DT Article ID AEGYPTI AB The pholcid spider, Crossopriza lyoni (Blackwall 1867) is a common inhabitant of homes in a rural village in Chachoengsao Province, Thailand. Studies on the spider were initiated because its microhabitat closely coincided with that of adult Aedes aegypti (Linnaeus 1762), mosquito vectors of dengue virus. Laboratory observations showed that females deposited eggs 4-6 days after copulation. Females held the egg sac in their mouthparts for 11-13 days, until all spiderlings (mean = 34) had left the sac. Spiderlings did not feed until they had molted, but as soon as feeding commenced they were capable of overpowering a mosquito many times their own size. Sometimes spiderlings would share a single mosquito or eat a mosquito wrapped by the mother spider. Spiderlings separated from their mother grew more rapidly than those left with the mother and reached maturity in as little as 74 days. The spiders' principal means of capturing prey was to throw silk with the aid of the hind legs. Spiders used this method to immobilize mosquitoes which were entangled in the standing web or to catch flying mosquitoes. The mosquito was not bitten until the time of feeding, up to six days after capture. Feeding occurred on only 34-48% of the days, and spiders ate about one mosquito per day. Cannibalism was a significant mortality factor, accounting for 67-84% mortality in a cage of spiderlings. An enzyme-linked immunosorbent assay (FLISA) was adapted to test spider tissue for presence of dengue virus. The ELISA was used to show that spiders did not become infected when fed dengue-infected mosquitoes. The results of the study suggested that C. lyoni could form an important component of integrated control of Aedes aegypti mosquitoes in foci of dengue transmission. C1 UNIV MARYLAND,SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560. WALTER REED ARMY INST RES,ARMED FORCES RES INST MED SCI,APO,AP 96546. NR 26 TC 16 Z9 20 U1 1 U2 3 PU AMER ARACHNOLOGICAL SOC PI NEW YORK PA C/O NORMAN I PLATNICK, AMER MUSEUM NATURAL HISTORY, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024 SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 1997 VL 25 IS 2 BP 194 EP 201 PG 8 WC Entomology SC Entomology GA YJ979 UT WOS:A1997YJ97900005 ER PT J AU Kharchenko, V Tharamel, J Dalgarno, A AF Kharchenko, V Tharamel, J Dalgarno, A TI Kinetics of thermalization of fast nitrogen atoms beyond the hard sphere approximation SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article AB The thermalization of fast nitrogen atoms through elastic collisions with thermal oxygen atoms is studied by obtaining the energy distribution function of fast nitrogen atoms from a direct numerical solution of the Boltzmann kinetic equation. The kernel of the Boltzmann equation is constructed using quantum mechanically evaluated differential scattering cross sections. The contributions to the cross sections that arise from the six lowest NO molecular potential curves exhibit a marked dependence on both the energy and the scattering angle. It is shown that the classical scattering cross sections are an excellent approximation to the smooth curve obtained by averaging the quantum mechanical cross sections. The differences between the results of calculations of the collision kernel for the hard sphere cross sections and the actual cross sections are discussed and the steady state distribution function of the fast N atoms is compared with the results of kinetic calculations with the hard sphere approximation. Copyright (C) 1996 Elsevier Science Ltd. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. NR 11 TC 34 Z9 34 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD JAN PY 1997 VL 59 IS 1 BP 107 EP 115 DI 10.1016/S1364-6826(96)00081-8 PG 9 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA WL046 UT WOS:A1997WL04600008 ER PT J AU Kite, GC Scofield, AM Lees, DC Hughes, M Smith, NG AF Kite, GC Scofield, AM Lees, DC Hughes, M Smith, NG TI Alkaloidal glycosidase inhibitors and digestive glycosidase inhibition in specialist and generalist herbivores of Omphalea diandra SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE Urania fulgens; Lepidoptera; Uraniidae; Omphalea diandra; Euphorbiaceae; alkaloidal glycosidase inhibitors; glycosidases; sequestration; generalist/specialist herbivores ID POLYHYDROXY ALKALOIDS; ALPHA-HOMONOJIRIMYCIN; INSECTS; CASTANOSPERMINE AB Generalist herbivores of the neotropical liana Omphalea diandra (Euphorbiaceae) were compared to the specialist herbivore, larvae of the uraniid moth Urania fulgens, with respect to their ability to accumulate the alkaloidal glycosidase inhibitors (AGIs) produced by the plant and the resistance of their digestive glycosidases to inhibition by these AGIs. The generalist herbivores did not accumulate the AGI aglycones 2R,5R-dihydroxymethyl-3R,4R-dihydroxypyrrolidine (DMDP) and 2,6-dideoxy-2,6-imino-D-glycero-L-gulo-heptitol (HNJ) to the levels detected in larvae of U. fulgens, which contained 0.05-0.11% dry weight DMDP and 0.17-0.35% HNJ. Glucosides of DMDP and HNJ that were synthesized by O. diandra were either absent from both the generalist and the specialist herbivores or present at low levels (less than 0.01%), even though HNJ-glucoside was often the most abundant AGI in the foliage. Analyses of the herbivores' feces indicated that failure to accumulate AGIs was due to the compounds being metabolized rather than excreted. The digestive glycosidases of U. fulgens larvae were more resistant to inhibition by AGI aglycones than those of the generalist herbivores. Similarly, sucrose and maltose hydrolysis in two of the generalist lepidopteran herbivores, larvae of Panthiades ballus and Theope virgilius, was more resistant to inhibition by DMDP than in larvae of Spodopreta littoralis, a lepidopteran which does not encounter O. diandra in nature. There was little difference in the susceptibility to AGIs of glycosidases from the generalist coleopteran Rhabdopterus fulvipes, which naturally feeds on O. diandra, compared with the coleopteran Dermestes maculatus, which does not. The glucoside of HNJ was found to be a very patent inhibitor of trehalase activity in all the insects examined. AGIs are considered to reduce the nutritional value of O. diandra to nonadapted herbivores rather than be acutely toxic. Nevertheless, U. fulgens does appear to be unique among Omphalea-feeding insects in its ability to accumulate AGIs, suggesting that it gains some advantage from storing these compounds. C1 UNIV LONDON WYE COLL,DEPT BIOL SCI,ASHFORD TN25 5AH,KENT,ENGLAND. NAT HIST MUSEUM,DEPT ENTOMOL,LONDON SW7 5BD,ENGLAND. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP Kite, GC (reprint author), ROYAL BOT GARDENS,RICHMOND TW9 3AB,SURREY,ENGLAND. NR 24 TC 13 Z9 17 U1 0 U2 8 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD JAN PY 1997 VL 23 IS 1 BP 119 EP 135 DI 10.1023/B:JOEC.0000006349.84075.f0 PG 17 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA WL775 UT WOS:A1997WL77500008 ER PT J AU Lornell, K AF Lornell, K TI Last cavalier: The life and times of John A. Lomax, 1867-1948 - Porterfield,N SO JOURNAL OF COUNTRY MUSIC LA English DT Book Review RP Lornell, K (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU COUNTRY MUSIC FOUNDATION PI NASHVILLE PA 4 MUSIC SQUARE EAST, NASHVILLE, TN 37203 SN 0092-0517 J9 J COUNTRY MUSIC JI J. Ctry. Music PY 1997 VL 19 IS 2 BP 43 EP 44 PG 2 WC Music SC Music GA XU231 UT WOS:A1997XU23100015 ER PT J AU Jett, JA AF Jett, JA TI Recent literature on foraminifera SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Bibliography RP Jett, JA (reprint author), NATL MUSEUM NAT HIST,DEPT PALEOBIOL,SMITHSONIAN INST,MRC-121,WASHINGTON,DC 20560, USA. NR 0 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 SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD JAN PY 1997 VL 27 IS 1 BP 75 EP 78 PG 4 WC Paleontology SC Paleontology GA WH679 UT WOS:A1997WH67900008 ER PT J AU Alpert, Y Lanzerotti, LJ Rybachek, ST AF Alpert, Y Lanzerotti, LJ Rybachek, ST TI Oscillatory nature of the magnetosphere - III. Resonance oscillations. Some simulation SO JOURNAL OF GEOMAGNETISM AND GEOELECTRICITY LA English DT Article; Proceedings Paper CT 8th Quadrennial Solar Terrestrial Physics Symposium of SCOSTEP CY JUN 05-10, 1994 CL SENDAI, JAPAN AB The characteristics of the Fourier spectral frequency maxima F-s,F-max in the frequency band (F = 7-50) MHz which compose the extra low frequency e.m. waves-so called Pc2-Pc5 micropulsations, created in the magnetosphere an considered in this paper. It should be considered as an extended part of the data analysis presented in paper II (Alpert el al., 1995). The obtained characteristics of the spectra are compared with spectra of signals which can simulate the shapes of the envelopes of the examined records of the unfiltered magnetic field B(t). They are also confronted with spectral frequency maxi ma of different signals and with resonance frequencies of different resonators. This analysis con firms our conclusion that the found spectral maxima can be resonance frequencies-eigenvalues of a magnetospheric oscillating system. The resonance swinging of the background plasma oscillations, which creates strong packets of waves is also simulated by simple calculations. The variety of shapes of the filtered packets of waves as observed in the magnetosphere is obtained by these calculations. C1 AT&T Bell Labs, Harvard Smithsonian Ctr Astrophys, Lucent Technol, Naperville, IL 60566 USA. St Petersburg State Univ, St Petersburg, Russia. RP Alpert, Y (reprint author), AT&T Bell Labs, Harvard Smithsonian Ctr Astrophys, Lucent Technol, Naperville, IL 60566 USA. RI Rybachek, Svetlana/G-7192-2015 OI Rybachek, Svetlana/0000-0002-8603-4329 NR 2 TC 1 Z9 1 U1 0 U2 0 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 0022-1392 J9 J GEOMAGN GEOELECTR JI J. Geomagn. Geoelectr. PY 1997 VL 49 SU S BP S121 EP S130 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 135HU UT WOS:000076796600012 ER PT J AU Alpert, Y Lanzerotti, LJ AF Alpert, Y Lanzerotti, LJ TI Oscillatory nature of the magnetosphere - II. The em-background, strong packets of waves, resonances SO JOURNAL OF GEOMAGNETISM AND GEOELECTRICITY LA English DT Article; Proceedings Paper CT 8th Quadrennial Solar Terrestrial Physics Symposium of SCOSTEP CY JUN 05-10, 1994 CL SENDAI, JAPAN ID PERIOD MAGNETIC PULSATIONS; EXCITATION AB A new approach toward an understanding of the nature of ULF-ultra low frequency-em. waves observed in the magnetosphere is given in this paper. The work is based upon results derived from detailed studies of the Fourier spectra of experimental magnetic field data obtained at a number of different geomagnetic locations around the world: Cascade (L = 2.9; Iowa, U.S.A.): Iqaluit - NP (L = 13; Northwest Territories, Canada), Amundsen-Scott Station - SP (L = 13; Antarctica), and also at Tuckerton (L = 2.6; New Jersey), and Point Arena (L = 2.6; California). The frequency band of the examined oscillations is F similar or equal to (0.7 . 10(-3)-5 . 10(-2)) Hz and overlaps the frequencies of the so-called (Pc2-Pc5) micropulsations. We show that the em. oscillations of these packets of waves exist in any time both in quite and disturbed conditions in the em. background of the magnetosphere. They appear to be resonance oscillations occurring in the magnetosphere on the whole or on its parts. During the intervals studied, in the examined frequency range 12 fundamental resonance frequencies were found in the spectra of the NP and SP data and more than 20-25 resonance frequencies in the Tuckerton and Point Arena data.* The other resonance maxima disappear in the weak oscillations of the noise. In general, the em. background of the magnetosphere is of a "lined" structure. It is composed of the resonance oscillations (frequency maxima of its spectra), and by more weak oscillations-by noise. All these oscillations can be set swinging, producing isolated, short-lived packets of waves. The conditions for producing the swinging can be impulse/shock-excitations of the magnetospheric plasmas, swinging of the background oscillations by gyro-resonance instability, dynamic effects such as changes in the neutral winds, etc. Thus, the well-known multiple manifestations of hydromagnetic ULF waves and wave packets observed in the magnetosphere are considered to be the result of a single physical phenomenon: the fundamental em. oscillatory nature of the background magnectospheric plasma environment. C1 AT&T Bell Labs, Harvard Smithsonian Ctr Astrophys, Lucent Technol, Naperville, IL 60566 USA. RP Alpert, Y (reprint author), AT&T Bell Labs, Harvard Smithsonian Ctr Astrophys, Lucent Technol, Naperville, IL 60566 USA. NR 40 TC 1 Z9 1 U1 0 U2 0 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 0022-1392 J9 J GEOMAGN GEOELECTR JI J. Geomagn. Geoelectr. PY 1997 VL 49 SU S BP S85 EP S119 PG 35 WC Geosciences, Multidisciplinary SC Geology GA 135HU UT WOS:000076796600011 ER PT J AU Summers, K Bermingham, E Weigt, L McCafferty, S AF Summers, K Bermingham, E Weigt, L McCafferty, S TI Phenotypic and genetic divergence in three species of dart-poison frogs with contrasting parental behavior SO JOURNAL OF HEREDITY LA English DT Article ID DENDROBATES-PUMILIO; BROOD CARE; EVOLUTION; ALKALOIDS; SELECTION AB Why some species exhibit remarkable variation among populations while closely related species are relatively uniform remains unclear, The strawberry dart-poison frog (Dendrobates pumilio) exhibits spectacular color and pattern polmorphism among populations in the Bocas del Toro archipelago of Panama. In contrast, two other sympatric species of dart-poison frog, Phyllobates lugubris and Minyobafes sp., show little color or pattern variation among island populations, Here we demonstrate that the color and pattern variation among populations of D. pumilio is not matched by higher levels of mitochondrial DNA sequence divergence relative to P. lugubris or Minyobates sp. Thus, neutral divergence in allopatry is unlikely to have caused the geographical differences observed in D. pumilio. We suggest that strong sexual selection associated with female parental care in D. pumilio, which contrasts the male parental care of P. lugubris and Minyobates sp., may have driven divergence in coloration and pattern in D. pumilio. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. NR 35 TC 65 Z9 69 U1 4 U2 20 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-1503 J9 J HERED JI J. Hered. PD JAN-FEB PY 1997 VL 88 IS 1 BP 8 EP 13 PG 6 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA WH725 UT WOS:A1997WH72500002 PM 9048443 ER PT J AU Eberhard, WG AF Eberhard, WG TI Graverobbing by male Eulaema seabrai bees (Hymenoptera: Apidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article AB Male Eulaema seabrai apparently collect odoriferous substances from the hind tibiae of dead conspecific males. C1 UNIV COSTA RICA,ESCUELA BIOL,SAN JOSE,COSTA RICA. RP Eberhard, WG (reprint author), UNIV COSTA RICA,SMITHSONIAN TROP RES INST,CIUDAD UNIV,SAN JOSE,COSTA RICA. NR 2 TC 4 Z9 4 U1 0 U2 0 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JAN PY 1997 VL 70 IS 1 BP 66 EP 66 PG 1 WC Entomology SC Entomology GA XT962 UT WOS:A1997XT96200011 ER PT J AU Lefebvre, G Poulin, B AF Lefebvre, G Poulin, B TI Bird communities in Panamanian black mangroves: Potential effects of physical and biotic factors SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE arthropods; birds; climate; conservation; diet; feeding guilds; mangrove; Panama; phenology; physical factors ID GROWTH; DIET AB Isolated in forest patches, mangrove stands often experience different physical conditions (rainfall, tide, salinity) despite similar floristic composition and structure. These abiotic factors are known to influence mangrove phenology but their potential effect on the local invertebrate and bird fauna have not been investigated. This study contrasts two sites of black mangrove (Avicennia germinans) located on the Caribbean and Pacific coasts of Panama. The two mangrove sites are characterized by different rainfall and tide patterns, and consequently ground inundation and salinity. These mangrove sites also differed in their plant phenology as well as invertebrate and bird composition. Although 95% of the bird species sampled occur on both coasts, the two mangrove sites shared only 34%. Moreover, each bird community was composed of a particular feeding guild assemblage consistent with the abundance distribution of their invertebrate-prey. Because floristically similar mangrove stands can support different invertebrate and bird faunas, conservation efforts should target mangrove patches submitted to different physical factors in order to preserve biodiversity. C1 SMITHSONIAN TROP RES INST,ANCON,PANAMA. NR 38 TC 13 Z9 16 U1 3 U2 11 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 1997 VL 13 BP 97 EP 113 PN 1 PG 17 WC Ecology SC Environmental Sciences & Ecology GA WH632 UT WOS:A1997WH63200008 ER PT J AU Barnes, PAG Morton, B AF Barnes, PAG Morton, B TI The functional morphology of Mactrinula reevesii (Bivalvia: Mactroidea) in Hong Kong: Adaptations for a deposit-feeding lifestyle SO JOURNAL OF ZOOLOGY LA English DT Article ID SURF CLAM; SPISULA-SOLIDISSIMA; GROWTH; AGE AB The shallow subtidal mactrid bivalve Mactrinula reevesii is a deposit-feeder in the southern and south-eastern oceanic waters of Hong Kong. Buried obliquely, large quantities of fine sediment are taken into the mantle cavity and sorted on enormous labial palps. The small ctenidia probably have little value in collecting material, amounts taken in being too large. The mid gut is long and complexly folded inside the visceral mass. It is also capable of distension, although superficial visceral muscles maintain internal tonus. The rectum is narrow and creates compact faecal pellets. Most interest is in the ventral mantle margin which is, posterior to the pedal gape and the base of the inhalant siphon, united by a sheet of cuticle. There is no fourth pallial aperture. There are, however, two pairs of flaps extending along the posterior third of the internal ventral mantle surface. These arch over left and right mantle rejection tracts which transfer unwanted material to the base of the inhalant siphon for final expulsion. The mantle flaps prevent such material from being returned to the anterior end of the mantle cavity, for palp reprocessing, when new material arrives. They, thus, maximize sorting efficiency by separating unsorted from sorted and rejected material. Other mactrids have similar mantle flaps which they use in different ways, including the channelling of unwanted material to a fourth pallial aperture for expulsion, as in Lutraria lutraria. The Mactridae have thus evolved a unique method of increasing the efficiency of pseudofaecal waste rejection which has thereby facilitated the deposit-feeding lifestyle by the diverse representatives of this family. C1 UNIV HONG KONG,SWIRE INST MARINE SCI,HONG KONG,HONG KONG. RP Barnes, PAG (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 42 TC 3 Z9 3 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD, ENGLAND OX2 6DP SN 0952-8369 J9 J ZOOL JI J. Zool. PD JAN PY 1997 VL 241 BP 13 EP 34 PN 1 PG 22 WC Zoology SC Zoology GA XF765 UT WOS:A1997XF76500002 ER PT J AU Soapes, TF AF Soapes, TF TI The birth of the museum: History, theory, politics - Bennett,T SO LIBRARY QUARTERLY LA English DT Book Review RP Soapes, TF (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0024-2519 J9 LIBR QUART JI Libr. Q. PD JAN PY 1997 VL 67 IS 1 BP 78 EP 79 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA WD917 UT WOS:A1997WD91700005 ER PT J AU Agoramoorthy, G AF Agoramoorthy, G TI Apparent feeding associations between Alouatta seniculus and Odocoileus virginianus in Venezuela SO MAMMALIA LA English DT Article ID RED HOWLER MONKEYS; CHANCE C1 SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. NR 20 TC 6 Z9 6 U1 0 U2 1 PU MUSEUM NAT HIST NATURELLE PI PARIS PA 55 RUE DE BUFFON, 75005 PARIS, FRANCE SN 0025-1461 J9 MAMMALIA JI Mammalia PY 1997 VL 61 IS 2 BP 271 EP 273 PG 3 WC Zoology SC Zoology GA XW645 UT WOS:A1997XW64500015 ER PT J AU Murison, MA AF Murison, MA TI Analytical study of optical wavefront aberrations using Maple SO MAPLETECH LA English DT Article AB This paper describes a package for analytical ray tracing of relatively simple optical systems. AESOP (An Extensible Symbolic Optics Package) enables analysis of the effects of small optical element misalignments or other perturbations. (It is possible to include two or more simultaneous independent perturbations.) Wavefront aberrations and optical path variations can be studied as functions of the perturbation parameters. The power of this approach lies in the fact that the results can be manipulated algebraically, allowing determination of misalignment tolerances as well as developing physical intuition, especially in the picometer regime of optical path length variations. C1 SMITHSONIAN ASTROPHYS LAB,CAMBRIDGE,MA. NR 15 TC 0 Z9 0 U1 0 U2 1 PU BIRKHAUSER BOSTON INC PI CAMBRIDGE PA 675 MASSACHUSETTS AVE, CAMBRIDGE, MA 02139 SN 1061-5733 J9 MAPLETECH JI Mapletech PY 1997 VL 4 IS 2 BP 52 EP 62 PG 11 WC Computer Science, Software Engineering SC Computer Science GA YH386 UT WOS:A1997YH38600008 ER PT J AU Gallegos, CL Jordan, TE AF Gallegos, CL Jordan, TE TI Seasonal progression of factors limiting phytoplankton pigment biomass in the Rhode River estuary, Maryland (USA). I. Controls on phytoplankton growth SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE phytoplankton; estuary; growth; nutrients; grazing; light; temperature ID COASTAL-PLAIN ESTUARY; NUTRIENT-LIMITATION; CHESAPEAKE BAY; MICROZOOPLANKTON; NITROGEN; MICROPLANKTON; PRODUCTIVITY; CHLOROPHYLL; PHOSPHORUS; PLANKTON AB Experiments to measure phytoplankton growth rates and microzooplankton grazing rates, both with and without additions of nutrients, were conducted over a 5 yr span to determine the relative roles of physical factors, nutrients, and microzooplankton grazing in regulating phytoplankton pigment biomass in the Rhode River estuary (Maryland, USA). Microzooplankton grazing rate was overall only weakly correlated with phytoplankton growth rate, although fluctuations in the rates appeared to parallel one another for restricted periods. Grazing was about 73% of growth rate at ambient nutrients during 1995, a year in which the two were correlated. In winter and early spring, phytoplankton growth rates were low and unaffected by nutrient additions. In late spring, stimulation of growth by nutrient addition was more common, but microzooplankton grazing was partially effective in relieving nutrient Limitation. Growth enhancement by nutrient addition was most common in summer, and microzooplankton grazing was less effective at relieving nutrient limitation. For N addition stimulated phytoplankton growth in late spring and autumn, but only N addition stimulated growth in summer. Temperature constrained upper bounds of observed growth rates throughout the year, but many observed growth rates were far below the temperature-dependent maximum, even with nutrients added. Considered as a single group, temperature-normalized growth rates were poorly related to in situ daily photon flux; but the rates appeared to fall into species-dependent higher and lower groups. The higher growth rates were statistically associated with the diatoms Thalassiosira pseudonana, Thalassiosira sp., and Nitzschia longissima. The lower growth rates were associated with the dinoflagellates Gyrodinium uncatenum and Prorocentrum minimum. Results suggest that interpretation of bioassay experiments requires consideration of both grazing effects and species composition of the phytoplankton community. Nutrient stimulation of some slow growing assemblages may be difficult to detect in 1 d incubation experiments. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gallegos@serc.si.edu OI Gallegos, Charles/0000-0001-5112-0166 NR 37 TC 27 Z9 28 U1 0 U2 15 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 1997 VL 161 BP 185 EP 198 DI 10.3354/meps161185 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA YX982 UT WOS:000072100100018 ER PT J AU Gallegos, CL Jordan, TE AF Gallegos, CL Jordan, TE TI Seasonal progression of factors limiting phytoplankton pigment biomass in the Rhode River estuary, Maryland (USA). II. Modeling N versus P limitation SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE phytoplankton; estuary; nutrients; modeling ID NUTRIENT-LIMITATION; NITROGEN LIMITATION; GROWTH-KINETICS; CHESAPEAKE BAY; PHOSPHORUS; WATERS; CHLOROPHYLL; GRADIENT; INPUTS; BLOOMS AB Previously reported experiments demonstrated that N addition enhanced phytoplankton growth rate more frequently and to a greater extent than did addition of P alone. Here we develop a model of nutrient-Limited net phytoplankton production for the Rhode River estuary, Maryland (USA), to determine the sensitivity of observed patterns to changes in the manner in which nutrients are delivered to the system. The model successfully reproduced the seasonal pattern of phytoplankton chlorophyll variation for an average year, the relative timing of P and N limitation, and the interannual variability in the timing of the shift from P to N limitation. Manipulation of nutrient sources in the model suggested that the disappearance of N at the seaward boundary of the estuary is sufficient to produce the shift from P to N Limitation. Raising the modeled N:P ratio of sediment nutrient release to a value greater than that of the phytoplankton biomass caused co-limitation by both N and P in the summer, but no manipulations produced limitation solely by P in the summer. In the model, different computed indicators of nutrient limitation (i.e. ratios of available N:P, physiological indicators of internal nutrient pools, and computed growth stimulation by nutrient additions) generally identified the same nutrient as limiting at a particular time. The model demonstrates how observed shifts in nutrient limitation result from changes in delivery of N and P from the watershed, from the sediment, and from incoming phytoplankton. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gallegos@serc.si.edu OI Gallegos, Charles/0000-0001-5112-0166 NR 30 TC 13 Z9 13 U1 0 U2 2 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 1997 VL 161 BP 199 EP 212 DI 10.3354/meps161199 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA YX982 UT WOS:000072100100019 ER PT J AU Gallegos, CL Jordan, TE Correll, DL AF Gallegos, CL Jordan, TE Correll, DL TI Interannual variability in spring bloom timing and magnitude in the Rhode River, Maryland, USA: Observations and modeling SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE phytoplankton; spring bloom; estuarine; nitrogen; phosphorus ID COASTAL-PLAIN ESTUARY; LONG-TERM TRENDS; CHESAPEAKE BAY; NUTRIENT-LIMITATION; PHYTOPLANKTON PRODUCTION; NITROGEN LIMITATION; AQUATIC VEGETATION; CHLOROPHYLL; PHOSPHORUS; GROWTH AB The long-term average seasonal distribution of chlorophyll concentration in a central reach of the Rhode River estuary (Maryland, USA) has a peak in the spring of about 90 mg m(-3). Here we examine interannual variability in chlorophyll and nutrient concentrations in recent years. Years are classified as having an average bloom, extraordinary bloom, or no bloom, and patterns of nutrient concentration are described for each category. To determine processes associated with the different categories of behavior, we performed a generalized sensitivity analysis of a model of nutrient-limited phytoplankton net growth which was previously shown to simulate the chlorophyll concentration and the observed pattern of shift from P to N limitation in an average year. Model parameters controlling the delivery of N and P by the environment and the biological utilization of nutrients by the phytoplankton were drawn from random distributions based on literature reports or, where available, data from the Rhode River. Model output for each parameter set was classified according to which, if any, of the classes of bloom it exhibited. Environmental processes most responsible for the variability in predicted spring blooms were the rate of phosphorus release from the sediment, the timing of nitrate depletion at the seaward boundary, and the maximal nitrate concentration at the boundary. Simulation of bloom failure was most strongly associated with low rates of phosphorus release from the sediment. Phytoplankton physiological parameters most responsible for variability in categories of behavior were the nitrogen:chlorophyll conversion factor, and the maximum internal storage capacity for phosphorus. Blooms of extraordinary magnitude were associated with low nitrogen:chlorophyll ratios and high storage capacity for phosphorus. Results help identify key processes and parameters in need of further understanding as well as possible points for managerial intervention. RP Gallegos, CL (reprint author), SMITHSONIAN ENVIRONM RES CTR, POB 28, EDGEWATER, MD 21037 USA. OI Gallegos, Charles/0000-0001-5112-0166 NR 46 TC 19 Z9 19 U1 1 U2 2 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 1997 VL 154 BP 27 EP 40 DI 10.3354/meps154027 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA XR976 UT WOS:A1997XR97600003 ER PT J AU Stoecker, DK Li, AS Coats, DW Gustafson, DE Nannen, MK AF Stoecker, DK Li, AS Coats, DW Gustafson, DE Nannen, MK TI Mixotrophy in the dinoflagellate Prorocentrum minimum SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Prorocentrum; dinoflagellates; cryptophytes; mixotrophy; Chesapeake Bay ID MARIAE-LEBOURIAE DINOPHYCEAE; RED TIDE DINOFLAGELLATE; CHESAPEAKE BAY; PHAGOTROPHY; TRANSPORT; GONYAULAX; PATTERNS; ORGANISM; LIGHT AB Prorocentrum minimum (formerly also known as P. mariae-lebouriae) is a common bloom-forming, photosynthetic dinoflagellate in Chesapeake Bay, USA. II is also capable of ingesting other cells. In Chesapeake Bay, P, minimum usually co-occurs with cryptophytes. Ingested cryptophyte material is observable in the dinoflagellate under an epifluorescent microscope as orange-fluorescent inclusions (OFI). During April and May, the frequency of OFI was less than or equal to 10% in both surface and pycnocline assemblages. In summer, up to 50% of the P, minimum contained OFI. The frequency of OFI was positively correlated with cryptophyte abundance, but OFI were not frequent in all populations of P. minimum when cryptophyte densities were high. On-deck experimental incubations were done to determine the conditions that influence feeding. Light level and inorganic nutrient availability over the previous 24 h affect feeding. Incidence of feeding is lower when populations are maintained in the dark for 24 h than on a natural Light:dark cycle. Addition of nitrate and phosphate together can inhibit feeding. Ingestion has a diel pattern, with frequency of OFI highest in the afternoon and evening and lowest in the morning. Feeding is influenced by a complex of factors, but the spatial-temporal pattern of ingestion and the experiments both suggest that feeding is primarily a mechanism for obtaining limiting inorganic nutrients rather than a mechanism for supplementing carbon nutrition during light limitation. Ingestion of other protists, including competitors for light and nutrients, may be an important strategy which allows bloom-forming dinoflagellates to dominate plankton assemblages for extended periods and during changing nutrient regimes. C1 SMITHSONIAN ENVIRONM RES CTR, EDGEWATER, MD 21037 USA. RP Stoecker, DK (reprint author), UNIV MARYLAND, HORN POINT ENVIRONM LAB, CTR ENVIRONM & ESTUARINE STUDIES, CAMBRIDGE, MD 21613 USA. RI stoecker, diane/F-9341-2013 NR 27 TC 120 Z9 130 U1 4 U2 23 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 1997 VL 152 IS 1-3 BP 1 EP 12 DI 10.3354/meps152001 PG 12 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA XK651 UT WOS:A1997XK65100001 ER PT J AU Ferraris, JD Norenburg, JL AF Ferraris, JD Norenburg, JL TI Oxygen uptake during repeated exposure to temperature change: Physiological divergence in Panamanian cognate pairs and latitudinally distant populations of decapod crustacea SO MARINE ECOLOGY-PUBBLICAZIONI DELLA STAZIONE ZOOLOGICA DI NAPOLI I LA English DT Article DE fluctuating temperature; oxygen uptake; invertebrate; Decapoda ID MITOCHONDRIAL-DNA; ISTHMUS AB The emergence of the Isthmus of Panama subdivided the amphi-American biota. In the present study; Pacific and Atlantic populations of four cognate pairs of crabs were used to discern whether exposure to different thermal regimes in habitats, in the putative absence of gene flow, has resulted in physiological divergence. Populations that potentially form a common genetic pool were also used; these were populations of the Atlantic Panama cognate that occur in belize and Florida. Decreases in water temperature occur periodically in Pacific Panama and Florida, but nor in Atlantic Panama or Belize. In this study, physiological divergence in oxygen uptake was assessed in response to repeated exposure to either control and decreased temperature or control and increased temperature. Results indicate that, in only some of the genera tested, exposure to decreases in habitat temperature has resulted in divergence. Partial support is found for the corollary that adaptation to an environment with periods of decreased temperature results in reduced compensation during exposure to elevated temperature. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560. RP Ferraris, JD (reprint author), NHLBI,KIDNEY & ELECTROLYTE METAB LAB,NIH,10 CTR DR MSC 1598,BLDG 10,RM 6N307,BETHESDA,MD 20892, USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 26 TC 0 Z9 0 U1 1 U2 1 PU BLACKWELL WISSENSCHAFTS-VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0173-9565 J9 PSZNI MAR ECOL JI Mar. Ecol.-Pubbl. Stn. Zool. Napoli PY 1997 VL 18 IS 2 BP 127 EP 146 PG 20 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA XQ578 UT WOS:A1997XQ57800003 ER PT J AU Ferraris, JD Norenburg, JL AF Ferraris, JD Norenburg, JL TI Volume and ion regulation during repeated exposure to temperature change: Physiological divergence in trans-isthmian cognate pairs and latitudinally distant populations of decapod crustacea SO MARINE ECOLOGY-PUBBLICAZIONI DELLA STAZIONE ZOOLOGICA DI NAPOLI I LA English DT Article DE volume regulation; ion regulation; invertebrate; temperature; Decapoda ID INTERTIDAL NEMERTINE; MITOCHONDRIAL-DNA; PANAMA; SALINITY; DECEREBRATION; TIME; K+ AB When the Isthmus of Panama emerged as a land bridge, it set the stage for allopatric speciation in the marine fauna. In the present study Pacific and Atlantic populations of three cognate pairs of crabs were used to discern whether physiological divergence has occurred as a result of exposure to different thermal regimes in habitats and in the putative absence of gene flow. Additional comparison was made with Belize and Florida populations of the Atlantic Panama cognate. This was done to test the strength of correlation between physiological divergence and exposure to different thermal regimes in populations that potentially form a common genetic pool. Water temperatures decrease periodically in Pacific Panama and Florida but not in Atlantic Panama or Belize. Physiological divergence in volume and ion regulation was assessed in response to repeated exposure to either control and decreased temperature or to control and increased temperature. Results indicate that exposure to naturally occurring decreased temperatures in habitats has resulted in divergence. This divergence is demonstrated both in enhanced ability to regulate volume at decreased temperature and impaired ability to regulate volume at elevated temperature. C1 SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560. RP Ferraris, JD (reprint author), NHLBI,LKEM,NIH,10 CTR DR MSC 1598,BLDG 10,RM 6N307,BETHESDA,MD 20892, USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 32 TC 0 Z9 0 U1 0 U2 1 PU BLACKWELL WISSENSCHAFTS-VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0173-9565 J9 PSZNI MAR ECOL JI Mar. Ecol.-Pubbl. Stn. Zool. Napoli PY 1997 VL 18 IS 3 BP 193 EP 209 PG 17 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA YD553 UT WOS:A1997YD55300001 ER PT B AU Aldcroft, T Bechtold, J Foltz, C AF Aldcroft, T Bechtold, J Foltz, C BE Arav, N Shlosman, I Weymann, RJ TI Variability in radio-loud quasar associated absorption lines SO MASS EJECTION FROM ACTIVE GALACTIC NUCLEI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Mass Ejection from Active Galactic Nuclei CY FEB 19-21, 1997 CL CARNEGIE OBSERV, PASADENA, CA SP NASA HO CARNEGIE OBSERV AB We have discovered the first two examples of time variability in associated absorption lines (z(abs) similar to z(qso)) in radio-loud quasars (0835+5804 and 1157+0128). Associated absorption lines have long been observed, but a fundamental question about the nature of the absorbing gas has remained: is it in a nearby galaxy, or is it closely associated with the quasar itself? Our Ending, the result of a large spectroscopic survey with the Multiple Mirror telescope, gives strong evidence that in some cases the absorption is due to material which is intrinsic to the radio-loud quasar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Aldcroft, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 15 Z9 15 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-48-1 J9 ASTR SOC P PY 1997 VL 128 BP 25 EP 30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80H UT WOS:000073445300004 ER PT B AU Mathur, S AF Mathur, S BE Arav, N Shlosman, I Weymann, RJ TI Comments on the intrinsic X-ray/UV absorbers in AGNs SO MASS EJECTION FROM ACTIVE GALACTIC NUCLEI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Mass Ejection from Active Galactic Nuclei CY FEB 19-21, 1997 CL CARNEGIE OBSERV, PASADENA, CA SP NASA HO CARNEGIE OBSERV AB This talk discusses the unified X-ray/UV absorption models in AGNs. I will first review the models and discuss how they offer a unique opportunity to probe the near-nuclear environment of AGNs. Recently, however, the validity of these models has been questioned by a number of authors. I will discuss these papers and argue that the data/models presented there do not contradict the unified X-ray/UV picture. I will conclude by presenting our new HST spectrum of an X-ray warm absorber. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mathur, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-48-1 J9 ASTR SOC P PY 1997 VL 128 BP 161 EP 166 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80H UT WOS:000073445300024 ER PT B AU Green, PJ AF Green, PJ BE Arav, N Shlosman, I Weymann, RJ TI Soft X-ray absorption in BAL QSOs SO MASS EJECTION FROM ACTIVE GALACTIC NUCLEI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Mass Ejection from Active Galactic Nuclei CY FEB 19-21, 1997 CL CARNEGIE OBSERV, PASADENA, CA SP NASA HO CARNEGIE OBSERV AB Evidence mounts that weak soft X-ray emission is a defining characteristic of true broad absorption line quasars (BAL QSOs). Observations of BAL QSOs from the ROSAT All Sky Survey, and from deep ROSAT pointings reveal that these QSOs are weak in the soft Xray bandpass when compared to those with no marked optical/UV absorption. One glaring exception appeared to be the nearby BAL QSO PG 1416-129, a bright ROSAT soft X-ray source showing no evidence for intrinsic soft X-ray absorption. A new HST FOS spectrum of PG 1416-129, however, shows no evidence for BALs. On the basis of UV, X-ray and optical evidence, we conclude that PG 1416-129 is not now, and has never been a BAL QSO. If BAL QSOs harbor normal intrinsic spectral energy distributions, their observed soft X-ray weakness is most likely the result of absorption. The ubiquitous occurrence of weak soft X-ray emission with UV absorption (BALs) thus suggests that the absorbers in each energy regime are physically associated, if not identical. Warm absorbers are probably a general phenomenon in QSO nuclei, and fresh evidence is cited that they may affect the observed properties of a large fraction of QSOs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Green, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-48-1 J9 ASTR SOC P PY 1997 VL 128 BP 167 EP 172 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80H UT WOS:000073445300025 ER PT S AU Chase, WT Wang, QY AF Chase, WT Wang, QY BE Vandiver, PB Druzik, JR Merkel, JF Stewart, J TI Metallography and corrosion product studies on archaeological bronze fragments from the Qu Cun site SO MATERIALS ISSUES IN ART AND ARCHAEOLOGY V SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Materials Issues in Art and Archaeology V CY DEC 03-05, 1996 CL BOSTON, MA SP Mat Res Soc AB The authors studied a suite of fragments of corroded bronzes from the Tienma-Qu Cun site, a Western Zhou city and cemetery complex dating from ca. 1000 to ca. 650 B.C.. Conventional metallographic techniques were used along with scanning electron microscope, electron microprobe and x-ray diffraction. The bronzes are very varied in structure and composition. Most are cast, moderate-tin bronzes, but some are high or low in tin or lead. A few show a worked and annealed structure, and some of the cast bronzes were also heat treated (possibly by use as cooking pots). Corrosion patterns also vary greatly, from almost uncorroded to total mineralization. Periodic and sequential corrosion phenomena were detected, as well as patination applied when the bronzes were made. We had hoped to be able to ascertain the causes of the different penetration of corrosion in these samples, but that must remain for future work. RP Chase, WT (reprint author), SMITHSONIAN INST MRC 707,FREER GALLERY ART,DEPT CONSERVAT & SCI RES,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 SN 0272-9172 BN 1-55899-366-5 J9 MATER RES SOC SYMP P PY 1997 VL 462 BP 73 EP 79 PG 7 WC Archaeology; Art; Materials Science, Multidisciplinary SC Archaeology; Art; Materials Science GA BJ83R UT WOS:A1997BJ83R00009 ER PT S AU Vandiver, P Chia, S AF Vandiver, P Chia, S BE Vandiver, PB Druzik, JR Merkel, JF Stewart, J TI The pottery technology from Bukit Tengkorak, a 3000-5000 year old site in Borneo, Malaysia SO MATERIALS ISSUES IN ART AND ARCHAEOLOGY V SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Materials Issues in Art and Archaeology V CY DEC 03-05, 1996 CL BOSTON, MA SP Mat Res Soc RP Vandiver, P (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 SN 0272-9172 BN 1-55899-366-5 J9 MATER RES SOC SYMP P PY 1997 VL 462 BP 269 EP 277 PG 9 WC Archaeology; Art; Materials Science, Multidisciplinary SC Archaeology; Art; Materials Science GA BJ83R UT WOS:A1997BJ83R00028 ER PT J AU Fredriksson, K Brenner, PR Fredriksson, BJ Olsen, E AF Fredriksson, K Brenner, PR Fredriksson, BJ Olsen, E TI A nondestructive analytical method for stone meteorites - And a controversial discrepancy SO METEORITICS & PLANETARY SCIENCE LA English DT Article AB A method is described for whole rock analyses of major elements in stone meteorites using the electron microprobe and requiring only powdering of the sample, most of which can be retrieved after analysis for additional analytical studies, such as instrument neutron activation analysis (INAA), radiochemical neutron activation analysis (RNAA) and O-isotopic analysis. Whole individual chondrules of less than or equal to 1 mg can be analyzed. The method is especially attractive for meteorites in short supply or of great rarity. A total of 398 meteorites were analyzed by this method. The results compare favorably with wet chemical analyses. A study was made of seventeen ordinary chondrites to compare their whole rock (metal free) compositions with the averaged compositions of eleven to thirty-eight of their respective individual chondrules (a total of 374 chondrules). The oxide ratio Al2O3/CaO is generally lower in chondrules than in their respective chondrites, the disparity being larger for petrographic grade 5 than for grade 3. Ordinary chondrites are not simply the sum of their respective chondrules. Furthermore, correlations between CaO, Al2O3 and TiO2 are strong for chondrules in unequilibrated chondrites and nonexistent in equilibrated chondrites. Also H, L and LL chondrite groups have similar bulk compositions within their respective groups, in spite of the different proportions of chondrules, kinds of chondrules, chondrule debris, and matrix. All this brings into question the metamorphic classification in which high petrographic grades are the metamorphosed equivalents of low petrographic grades. C1 UNIV CHICAGO,DEPT GEOPHYS SCI,CHICAGO,IL 60637. RP Fredriksson, K (reprint author), SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560, USA. NR 5 TC 4 Z9 4 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JAN PY 1997 VL 32 IS 1 BP 55 EP 60 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA XK171 UT WOS:A1997XK17100013 ER PT J AU Ariskin, AA Petaev, MI Borisov, AA Barmina, GS AF Ariskin, AA Petaev, MI Borisov, AA Barmina, GS TI METEOMOD: A numerical model for the calculation of melting-crystallization relationships in meteoritic igneous systems SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CHEMICAL MASS-TRANSFER; MAGMATIC PROCESSES; EXPERIMENTAL PETROLOGY; LOW-PRESSURE; CHONDRITES; EQUILIBRIA; BASALTS; ORIGIN; LIQUIDS AB The METEOMOD model is a computer program designed to calculate melting-crystallization relationships in igneous systems compositionally similar to ordinary chondrites and basaltic achondrites. The core of METEOMOD is a set of empirically calibrated equations, called geothermometers, which describe equilibria between silicate melt and minerals such as olivine, orthopyroxene, pigeonite, augite, plagioclase, and metallic Fe in terms of pressure, temperature, and liquid compositions. The silicate mineral geothermometers are calibrated from a database containing the compositions of melts and minerals produced in melting experiments on 113 meteoritic and 141 synthetic systems. The metallic iron-silicate melt geothermometer is calibrated from a database of 396 melting experiments. The Meteorite Melting Model or METEOMOD calculates crystallization temperatures and contents of major end members in mineral solid solutions with accuracies of +/-10-15 degrees C and +/-1-2 mol%, respectively. Input parameters for the program are (1) increment in crystallization degree; (2) one of 12f(O2), buffers routinely used in petrology; (3) shift from the buffer in log units, if any; (4) a choice of equilibrium or fractional crystallization trajectory; (5) terminal crystallization degree; (6) contents of ten major elements in wt%; (7) a set of minor and trace elements in parts per million; (8) the number of initial compositions to be modeled in a single computation run. The output consists of a series of tables that list equilibrium temperatures, O fugacities, and proportions of melt and minerals and their compositions, as a function of the degree of crystallization. The results of application of METEOMOD to modeling of melting-crystallization of the St. Severin LL chondrite are compared with the experimental data of Jurewicz et al. (1995). C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Ariskin, AA (reprint author), VI VERNADSKII INST GEOCHEM & ANALYT CHEM,MOSCOW 117975,RUSSIA. NR 36 TC 23 Z9 23 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JAN PY 1997 VL 32 IS 1 BP 123 EP 133 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA XK171 UT WOS:A1997XK17100020 ER PT S AU Sternberg, A Yan, M Dalgarno, A AF Sternberg, A Yan, M Dalgarno, A BE vanDishoeck, EF TI Photon-dominated and X-ray dominated regions SO MOLECULES IN ASTROPHYSICS: PROBES AND PROCESSES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 178th Symposium of the International-Astronomical-Union on Molecules in Astrophysics - Probes and Processes CY JUL 01-05, 1996 CL LEIDEN, NETHERLANDS SP Int Astron Union ID MOLECULAR-HYDROGEN EMISSION; SPATIAL-RESOLUTION OBSERVATIONS; FLUORESCENT H-2 EMISSION; NEUTRAL ATOMIC CARBON; PHOTODISSOCIATION REGIONS; ULTRAVIOLET-RADIATION; INFRARED RESPONSE; DISSOCIATIVE SHOCK; INTERSTELLAR SO+; CROSS-SECTIONS AB A brief account is presented of the chemical characteristics of regions controlled by the absorption of X-rays. Recent studies of the infrared emission from molecular hydrogen and time-dependent effects in evolving photon-dominated regions are summarized. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Sternberg, A (reprint author), TEL AVIV UNIV, SCH PHYS & ASTRON, IL-69978 RAMAT AVIV, TEL AVIV, ISRAEL. NR 74 TC 4 Z9 4 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4538-X J9 IAU SYMP PY 1997 IS 178 BP 141 EP 153 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ12H UT WOS:A1997BJ12H00012 ER PT S AU Menten, KM AF Menten, KM BE vanDishoeck, EF TI Masers as chemical probes of star-forming regions SO MOLECULES IN ASTROPHYSICS: PROBES AND PROCESSES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 178th Symposium of the International-Astronomical-Union on Molecules in Astrophysics - Probes and Processes CY JUL 01-05, 1996 CL LEIDEN, NETHERLANDS SP Int Astron Union ID SUBMILLIMETER WATER MASERS; E-TYPE METHANOL; W3(OH); GHZ; OH; KINEMATICS; DISCOVERY; CLOUDS; LINES AB Maser emission from the OH, H2O, and CH3OH molecules is found toward hundreds of molecular cloud cores with recent and on-going star formation. The often very high intensities of the observed emission imply substantial abundances of the maser molecules, which are difficult or impossible to explain with ion-molecule gas phase chemistry. We summarize relevant observations which show that OH and Class II CH3OH masers form in the envelopes of ultracompact HII regions in which the high abundances of these molecules are produced by evaporation of methanol and water from icy dust grain mantles. In contrast, H2O masers form in outflows from protostellar objects, where high H2O abundances are produced by endothermic neutral-neutral reactions in hot postshock gas. Finally, we briefly discuss Class I CH3OH masers, which also arise in interstellar outflows. RP Menten, KM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 39 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4538-X J9 IAU SYMP PY 1997 IS 178 BP 163 EP 172 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ12H UT WOS:A1997BJ12H00014 ER PT S AU Neufeld, DA Chen, W Melnick, GJ DeGraauw, T Feuchtgruber, H Haser, L Lutz, D Harwit, M AF Neufeld, DA Chen, W Melnick, GJ DeGraauw, T Feuchtgruber, H Haser, L Lutz, D Harwit, M BE vanDishoeck, EF TI Detection of thermal water vapor emission from W hydrae SO MOLECULES IN ASTROPHYSICS: PROBES AND PROCESSES SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 178th Symposium of the International-Astronomical-Union on Molecules in Astrophysics - Probes and Processes CY JUL 01-05, 1996 CL LEIDEN, NETHERLANDS SP Int Astron Union AB We have detected four far-infrared emission lines of water vapor toward the evolved star W Hydrae, using the Short Wavelength Spectrometer (SWS) of the Infrared Space Observatory (ISO). This is the first detection of thermal water vapor emission from a circumstellar outflow. C1 SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. SPACE RES ORG NETHERLANDS, SPACE RES LAB, NL-9700 AV GRONINGEN, NETHERLANDS. MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. RP Neufeld, DA (reprint author), JOHNS HOPKINS UNIV, DEPT PHYS & ASTRON, 3400 N CHARLES ST, BALTIMORE, MD 21218 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4538-X J9 IAU SYMP PY 1997 IS 178 BP 385 EP 388 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ12H UT WOS:A1997BJ12H00034 ER PT S AU Marsden, BG AF Marsden, BG BE Remo, JL TI Overview of orbits SO NEAR-EARTH OBJECTS: UNITED NATIONS INTERNATIONAL CONFERENCE SE Annals of the New York Academy of Sciences LA English DT Article; Proceedings Paper CT International Conference on Near-Earth Objects CY APR 24-26, 1995 CL NEW YORK, NY SP Amer Museum Nat Hist, Explorers Club, NASA, Planetary Soc, Quantametrics Inc, Sandia Natl Labs, UN Off Outer Space Affairs AB After a brief summary of the distribution of both large and small bodies in the solar system, there follows a categorization of the various hazards from comets and asteroids, the concept of PHA, or ''potentially hazardous asteroid,'' being introduced to include one that is large enough and can pass close enough to the Earth's orbit that it might conceivably yield a globally-damaging impact in the forseeable furture. Future search stragtegies are discussed, as they involve increasing both sky coverage and faintness limit, arguments being given for ensuring much fainter detections in the general opposition region than at much smaller elongations. It is concluded that a proposed ''impact hazard scale'' is generally less useful than recognition of the PHA status. The current situation with regard to follow-up astrometric activity, particularly by amateur astronomers, is viewed favorably, but professional search activity is at a depressingly low level. RP Marsden, BG (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 10 TC 8 Z9 8 U1 0 U2 1 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-040-9 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 1997 VL 822 BP 52 EP 66 DI 10.1111/j.1749-6632.1997.tb48334.x PG 15 WC Astronomy & Astrophysics; Multidisciplinary Sciences SC Astronomy & Astrophysics; Science & Technology - Other Topics GA BJ16N UT WOS:A1997BJ16N00007 ER PT J AU Pen, UL AF Pen, UL TI Measuring the universal deceleration using angular diameter distances to clusters of galaxies SO NEW ASTRONOMY LA English DT Article DE distance scale; cosmology:observations; galaxies:clusters:general ID ABELL-2218; ABELL-370; EINSTEIN; GAS AB Recent simulations, as well as weak lensing and X-ray data, indicate that gas is a good tracer of the total mass in clusters. The constancy of the gas fraction f(g) in clusters of galaxies can thus be used as a novel distance indicator f(g) proportional to h(3/2)Ohm(b)/Ohm(0). Assuming spherical symmetry and hydrostatic equilibrium allows us to infer f(g) using only the beta-model parameters and an emission weighted temperature. Even though none of the factors h, Ohm(b), Ohm(0), is individually known to high precision, the relative distances between clusters at high redshift can be used to infer the deceleration parameter q(0). Using this new model, the local population of clusters has a scatter of only 15% in the Hubble relation. The 3 clusters at redshift z similar to 0.5 suggest q(0) = 0.85+/-0.29 with 1 - sigma statistical error. This result would argue against a cosmological constant. The method is robust to errors in the measurement of the core radius as long as the product of the central density and the core radius squared rho 0r(c)(2) are well determined. However, this result may still be subject to unknown systematics such as cooling flows, which will require more detailed temperature maps, weak lensing data and numerical simulations to model accurately. Future lensing and X-ray data will dramatically improve the statistics. (C) 1997 Elsevier Science B.V. RP Pen, UL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 40 TC 94 Z9 94 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1092 J9 NEW ASTRON JI New Astron. PY 1997 VL 2 IS 4 BP 309 EP 317 DI 10.1016/S1384-1076(97)00021-3 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA XV239 UT WOS:A1997XV23900001 ER PT J AU Chamberlain, CP Blum, JD Holmes, RT Feng, XH Sherry, TW Graves, GR AF Chamberlain, CP Blum, JD Holmes, RT Feng, XH Sherry, TW Graves, GR TI The use of isotope tracers for identifying populations of migratory birds SO OECOLOGIA LA English DT Article DE stable isotopes; deuterium; strontium; carbon; Dendroica caerulescens ID D/H RATIOS; HYDROGEN ISOTOPE; OXYGEN ISOTOPES; BONE PHOSPHATE; LEAF WATER; CARBON; DIET; CELLULOSE; EXCHANGE; C-13 AB To determine whether stable isotopes can be used for identifying the geographic origins of migratory bird populations, we examined the isotopic composition of hydrogen (deuterium, delta D), carbon (delta(13)C), and strontium (delta(87)Sr) in tissues of a migratory passerine, the black-throated blue warbler (Dendroica caerulescens), throughout its breeding range in eastern North America. delta D and delta(13)C values in feathers, which are grown in the breeding area, varied systematically along a latitudinal gradient, being highest in samples from the southern end of the species' breeding range in Georgia and lowest in southern Canada. In addition, delta D decreased from east to west across the northern part of the breeding range, from New Brunswick to Michigan. delta(87)Sr ratios were highest in the Appalachian Mountains, and decreased towards the west. These patterns are consistent with geographical variation in the isotopic composition of the natural environment, i.e., with that of precipitation, plants, and soils for delta D, delta(13)C and delta(87)S respectively. Preliminary analyses of the delta D and delta(13)C composition of feathers collected from warblers in their Caribbean winter grounds indicate that these individuals were mostly from northern breeding populations. Furthermore, variances in isotope ratios in samples from local areas in winter tended to be larger than those in summer, suggesting that individuals from different breeding localities may mix in winter habitats. These isotope markers, therefore, have the potential for locating the breeding origins of migratory species on their winter areas, for quantifying the degree of mixing of breeding populations on migratory and wintering sites, and for documenting other aspects of the population structure migratory animals - information needed for studies of year-round ecology of these species as well as for their conservation. Combining information from several stable isotopes will help to increase the resolution for determining the geographic origins of individuals in such highly vagile populations. C1 DARTMOUTH COLL, DEPT BIOL SCI, HANOVER, NH 03755 USA. TULANE UNIV, DEPT ECOL EVOLUT & ORGANISMAL BIOL, NEW ORLEANS, LA 70118 USA. SMITHSONIAN INST, DEPT VERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. RP Chamberlain, CP (reprint author), DARTMOUTH COLL, DEPT EARTH SCI, HANOVER, NH 03755 USA. NR 61 TC 278 Z9 294 U1 6 U2 74 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JAN PY 1997 VL 109 IS 1 BP 132 EP 141 DI 10.1007/s004420050067 PG 10 WC Ecology SC Environmental Sciences & Ecology GA WH547 UT WOS:A1997WH54700017 PM 28307603 ER PT J AU Stott, AW Evershed, RP Tuross, N AF Stott, AW Evershed, RP Tuross, N TI Compound-specific approach to the delta C-13 analysis of cholesterol in fossil bones SO ORGANIC GEOCHEMISTRY LA English DT Article; Proceedings Paper CT 17th International Meeting on Organic Geochemistry CY SEP 04-08, 1995 CL DONOSTIA, SPAIN SP Board European Assoc Organ Geochemists (EAOG) DE cholesterol in fossil bones; palaeodiet; delta C-13 in Cretaceous sediments; GC-C-IRMS ID CARBON ISOTOPE FRACTIONATION; DIET; ARCHAEOLOGY; NITROGEN; ANIMALS AB delta(13)C values for cholesterol isolated from fossil animals, namely those of whales dated at 9735 +/- 160 yr and 75000 +/- 15000 yr B.P., are reported. Gas chromatography (GC) showed that 12 and 15 mu g of cholesterol per gram dry weight of bone were recovered from the banes of these two fossil animals, respectively. Conventional gas chromatography-mass spectrometry (GC-MS) confirmed the identity of the ancient cholesterol and that the peaks separated by GC were of high purity. Gas chromatography-combustion-isotope ratio-mass spectrometry (GC-C-IRMS) of cholesterol recovered from the fossil specimens yielded delta(13)C values that plotted within the rang expected for the bulk fat of marine mammals. Significantly, the isotopic depletion between the cholesterol and collagen was similar for both ancient and modern whale bones, indicating reliable preservation of the delta(13)C signal between the ancient cholesterol and the protein constituents. The potential to derive delta(13)C values from individual Lipids, for which the carbon skeletons are completely unaffected by decay processes, significantly extends the scope of palaeodietary studies. (C) 1997 Elsevier Science Ltd. C1 UNIV BRISTOL,SCH CHEM,ORGAN GEOCHEM UNIT,BRISTOL BS8 1TS,AVON,ENGLAND. SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. RI STOTT, ANDREW /I-7920-2012 NR 17 TC 22 Z9 22 U1 4 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0146-6380 J9 ORG GEOCHEM JI Org. Geochem. PD JAN PY 1997 VL 26 IS 1-2 BP 99 EP 103 DI 10.1016/S0146-6380(96)00132-5 PG 5 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA XE807 UT WOS:A1997XE80700012 ER PT B AU Goddard, I AF Goddard, I BE Pentland, DH TI Writing and reading Mesquakie (Fox) SO PAPERS OF THE TWENTY-SEVENTH ALGONQUIAN CONFERENCE SE PAPERS OF THE ALGONQUIAN CONFERENCE LA English DT Proceedings Paper CT 27th Annual Algonquian Conference CY OCT 27-29, 1995 CL UNIV N CAROLINA, CHAPEL HILL, NC HO UNIV N CAROLINA C1 Smithsonian Inst, Washington, DC 20560 USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU UNIV MANITOBA PRESS PI WINNIPEG PA 244 ENGINEERING BLDG, WINNIPEG, MANITOBA R3T 2N2, CANADA J9 PAP ALGON CONF PY 1997 VL 27 BP 117 EP 134 PG 18 WC Anthropology; Language & Linguistics SC Anthropology; Linguistics GA BU19J UT WOS:000175292400008 ER PT S AU Meixner, M Campbell, MT Welch, WJ Likkel, L Tafalla, M AF Meixner, M Campbell, MT Welch, WJ Likkel, L Tafalla, M BE Habing, HJ Lamers, HJG TI Core-halo structures in the (CO)-C-12 emission of CIT6, AFGL618 and IRAS21282+5050 SO PLANETARY NEBULAE SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 180th Symposium of the International-Astronomical-Union CY AUG 26-30, 1996 CL GRONINGEN, NETHERLANDS SP Int Astronom Union, Kapteyn Astronom Inst, Royal Acad Sci, Univ Groningen, Fdn Sci, Board Univ Groningen, Kluwer Publishers C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. Univ Wisconsin, Eau Claire, WI 54702 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Meixner, M (reprint author), Univ Illinois, Dept Astron, MC-221,1002 W Green St, Urbana, IL 61801 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-4892-3 J9 IAU SYMP PY 1997 IS 180 BP 359 EP 359 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL56K UT WOS:000075895400170 ER PT B AU Latham, DW AF Latham, DW BE Soderblom, DR TI Radial-velocity searches for low-mass companions orbiting solar-type stars SO PLANETS BEYOND THE SOLAR SYSTEM AND THE NEXT GENERATION OF SPACE MISSIONS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Planets beyond the Solar System and the Next Generation of Space Missions CY OCT 16-18, 1996 CL SPACE TELESCOPE SCI INST, BALTIMORE, MD HO SPACE TELESCOPE SCI INST AB In this paper I attempt to give an overview of recent efforts to use stellar radial-velocity measurements to detect low-mass companions orbiting solar-type stars. Although spectroscopic orbits implying companions with minimum masses below the substellar limit have now been published for more than a dozen solar-type stars, the detections so far have been limited to periods shorter than 5 years and orbital semi-amplitudes larger than 50 ms(-1). These companions appear to be relatively rare; only a few percent of the stars surveyed have yielded companions with minimum masses in the range 1 to 80 Jupiter masses (MJ). Nevertheless, patterns are beginning to emerge for the orbital characteristics of the detected companions, and there is some hope that these characteristics can shed light on the roles of the various formation and evolutionary processes which may have been involved. Planets with orbital periods and masses similar to the gas giants in our own solar system have not yet been found with radial-velocity techniques, but there is promise of progress in this direction. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-39-2 J9 ASTR SOC P PY 1997 VL 119 BP 19 EP 28 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK79Z UT WOS:000073439700003 ER PT B AU Noyes, R Jha, S Korzennik, S Krockenberger, M Nisenson, P Brown, T Kennelly, E Horner, S AF Noyes, R Jha, S Korzennik, S Krockenberger, M Nisenson, P Brown, T Kennelly, E Horner, S BE Soderblom, DR TI The AFOE program of extra-solar planet research SO PLANETS BEYOND THE SOLAR SYSTEM AND THE NEXT GENERATION OF SPACE MISSIONS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Planets beyond the Solar System and the Next Generation of Space Missions CY OCT 16-18, 1996 CL SPACE TELESCOPE SCI INST, BALTIMORE, MD HO SPACE TELESCOPE SCI INST AB We describe the program for detection and characterization of extra-solar planets using the Advanced Fiber Optic Echelle (AFOE) spectrograph, developed at Mt. Hopkins Observatory jointly by SAO and HAO. The AFOE is capable of obtaining radial velocity precision better than 10 m s(-1) on relatively bright stars, and has produced data confirming the low mass companions to 51 Peg and tau Boo. We describe the current observing program for monitoring a number of solar-like stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Noyes, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-39-2 J9 ASTR SOC P PY 1997 VL 119 BP 119 EP 122 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK79Z UT WOS:000073439700015 ER PT B AU Reasenberg, RD Babcock, RW Chandler, JF Phillips, JD AF Reasenberg, RD Babcock, RW Chandler, JF Phillips, JD BE Soderblom, DR TI POINTS mission studies: Lessons for SIM SO PLANETS BEYOND THE SOLAR SYSTEM AND THE NEXT GENERATION OF SPACE MISSIONS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Planets beyond the Solar System and the Next Generation of Space Missions CY OCT 16-18, 1996 CL SPACE TELESCOPE SCI INST, BALTIMORE, MD HO SPACE TELESCOPE SCI INST AB POINTS (Precision Optical INTerferometer in Space) measures the angle between two widely separated stars. The nominal bright-star measurement accuracy of 2 microarcsec is achieved in two minutes of observing two mag 8 stars. POINTS comprises a metrology system and a pair of independent Michelson stellar interferometers, each with a pair of 35 cm subapertures and a 2 m baseline. The angle between the baselines is adjustable over the range 87 to 93 deg. The POINTS scientific mission is enhanced by a solar shield, which allows observation of stars as close as 10 deg from the Sun. Numerous mission simulations over the past 15 years have elucidated the consequences of the single measurement accuracy and instrument architecture. For simplicity and efficiency, we divide the target stars into two classes, "reference grid stars" and all others. Grid stars provide reference for other targets, and are also science targets. In the nominal mission, redundant grid-star observations are performed quarterly to determine the stars' positions, proper motions, and parallaxes. We showed more than a decade ago that, if the grid stars are observed with sufficient redundancy, the grid "locks up:" after the observations are combined in a weighted least squares estimate of star positions, proper motions, and parallaxes, the uncertainty in the angle between any pair of grid stars, whether directly observable or not, becomes comparable with the measurement uncertainty. We have used double-blind Monte-Carlo mission simulations to study the planet-finding capabilities of POINTS and to determine the reliable detection threshold with a nominal observing program. If we demand a negligible probability of false alarms, then with our standard observing schedule, the detection threshold for short-period planets is a signature with amplitude equal to the single-measurement observing precision, and orbital elements can usually be determined. For planets with periods longer than the mission, the threshold rises steeply with period. These studies of the POINTS mission yield seven lessons for the Space Interferometry Mission (SIM), which are discussed. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Reasenberg, RD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-39-2 J9 ASTR SOC P PY 1997 VL 119 BP 191 EP 205 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK79Z UT WOS:000073439700023 ER PT J AU Medlin, LK Kooistra, WHCF Potter, D Saunders, GW Andersen, RA AF Medlin, LK Kooistra, WHCF Potter, D Saunders, GW Andersen, RA TI Phylogenetic relationships of the 'golden algae' (haptophytes, heterokont chromophytes) and their plastids SO PLANT SYSTEMATICS AND EVOLUTION LA English DT Review DE Chrysophyceae; Haptophyceae; actin; chloroplast; chromophyte; diatoms; heterokont; plastid; phylogeny; rbcL; stramenopiles; SSU rRNA; tufA ID RIBOSOMAL-RNA SEQUENCES; CODING REGIONS; NUCLEOTIDE-SEQUENCES; CLASSIS NOV; GENE FAMILY; EVOLUTION; ORIGIN; ULTRASTRUCTURE; SYNUROPHYCEAE; CHRYSOPHYCEAE AB The phylogenetic relationships of the "golden algae", like all algae, were rarely addressed before the advent of electron microscopy because, based upon light microscopy, each group was so distinct that shared characters were not apparent. Electron microscopy has provided many new characters that have initiated phylogenetic discussions about the relationships among the "golden algae". Consequently, new taxa have been described or old ones revised, many of which now include non-algal protists and fungi. The haptophytes were first placed in the class Chrysophyceae but ultrastructural data have provided evidence to classify them separately. Molecular studies have greatly enhanced phylogenetic analyses based on morphology and have led to the description of additional new taxa. We took available nucleotide sequence data for the nuclear-encoded SSU rRNA, fucoxanthin/chlorophyll photosystem I/II, and actin genes and the plastid-encoded SSU rRNA, tufA, and rbcL genes and analysed these to evaluate phylogenetic relationships among the "golden algae", viz., the Haptophyceae (= Prymnesiophyceae) and the heterokont chromophytes (also known as chromophytes, heterokont algae, autotrophic stramenopiles). Using molecular clock calculations, we estimated the average and earliest probable time of origin of these two groups and their plastids. The origin of the haptophyte host-cell lineages appears to be more ancient than the origin of its plastid, suggesting that an endosymbiotic origin of plastids occurred late in the evolutionary history of this group. The pigmented heterokonts (heterokont chromophytes) also arose later, following an endosymbiotic event that led to the transfer of photosynthetic capacity to their heterotrophic ancestors. Photosynthetic haptophytes and heterokont chromophytes both appear to have arisen at or shortly before the Permian-Triassic boundary. Our data support the hypothesis that the haptophyte and heterokont chromophyte plastids have independent origins (i.e., two separate secondary endosymbioses) even though their plastids are similar in structure and pigmentation. Present evidence is insufficient to evaluate conclusively the possible monophyletic relationship of the haptophyte and heterokont protist host cells, even though haptophytes lack tripartite flagellar hairs. The molecular data, albeit weak, consistently fail to present the heterokont chromophytes and haptophytes as monophyletic. Phylogenetic resolution among all classes of heterokont chromophytes remains elusive even though molecular evidence has established the phylogenetic alliance of some classes (e.g., Phaeophyceae and Xanthophyceae). C1 Alfred Wegener Inst Polar & Marine Res, D-27570 Bremerhaven, Germany. Univ New Brunswick, Dept Biol, Fredericton, NB E3B 6E1, Canada. Univ Calif Davis, Dept Pomol, Davis, CA 95616 USA. NAOS Smithsonian Trop Res Inst, APO, AA 34002 USA. Bigelow Lab Ocean Sci, W Boothbay Harbor, ME 04575 USA. RP Medlin, LK (reprint author), Alfred Wegener Inst Polar & Marine Res, Handelshafen 12, D-27570 Bremerhaven, Germany. RI medlin, linda/G-4820-2010; Saunders, Gary/D-8767-2014 OI Saunders, Gary/0000-0003-4813-6831 NR 128 TC 3 Z9 3 U1 4 U2 11 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0378-2697 EI 1615-6110 J9 PLANT SYST EVOL JI Plant Syst. Evol. PY 1997 SU 11 BP 187 EP 219 PG 33 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA YQ019 UT WOS:000071339300012 ER PT B AU Segev, B AF Segev, B BE Mugnai, D Ranfagni, A Schulman, LS TI Time for tunneling causality and wave packets SO PROCEEDINGS OF THE ADRIATICO RESEARCH CONFERENCE ON TUNNELING AND ITS IMPLICATIONS LA English DT Proceedings Paper CT Adriatico Research Conference on Tunneling and Its Implications CY JUL 30-AUG 02, 1996 CL INT CTR THEORET PHYS, TRIESTE, ITALY SP Int Ctr Theoret Phys, UNESCO, Int Atom Energy Agcy HO INT CTR THEORET PHYS ID TRAVERSAL-TIME; REFLECTION TIMES; WIGNER FUNCTION; QUANTUM-THEORY; DWELL TIME; BARRIER; TRANSMISSION; SCATTERING; DELAY; PROBABILITIES AB Time dependence in the tunneling process is considered in phase-space. causality is preserved as the transmission propagator for Wigner functions incident on a barrier vanishes for coordinates ahead of free motion. The coordinate probability distribution of a transmitted wave packet is given by a series expansion in which moments of the freely propagating Wigner function are weighted by energy derivatives of the amplitude. The two components of the complex tunneling time appear as two real parameters which control the wave packet shape st different positions of the detector. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Segev, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 53 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 981-02-2905-4 PY 1997 BP 371 EP 387 PG 17 WC Physics, Atomic, Molecular & Chemical; Physics, Multidisciplinary; Physics, Nuclear; Physics, Particles & Fields SC Physics GA BM39J UT WOS:000078596200024 ER PT J AU Mathis, WN AF Mathis, WN TI A review of the shore-fly genus Diphuia cresson (Diptera: Ephydridae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE diptera; Ephydridae; shore flies; Diphuia; New World tropics; cladistics AB Diphuia Cresson is reviewed to include (1) the synonymy of D. nasalis Wirth with D. nitida Sturtevant and Wheeler, (2) the description of D. flinti, new species (Dominican Republic: El Seibo), and (3) a cladistic analysis of the genus. RP Mathis, WN (reprint author), SMITHSONIAN INST, DEPT ENTOMOL, MRC, NHB 169, WASHINGTON, DC 20560 USA. NR 14 TC 3 Z9 3 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 1997 VL 99 IS 1 BP 28 EP 36 PG 9 WC Entomology SC Entomology GA WN469 UT WOS:A1997WN46900002 ER PT J AU Krombein, KV Norden, BB AF Krombein, KV Norden, BB TI Nesting behavior of Krombeinictus nordenae Leclercq, a sphecid wasp with vegetarian larvae (Hymenoptera: Sphecidae: Crabroninae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Sphecidae; Crabroninae; Humboldtia; Sri Lanka; internode; myrmecophyte; cocoon; pollen AB Nesting behavior of the recently described Sri Lankan wasp, Krombeinictus nordenae Leclercq, is discussed. Females nest in the hollow internodes of the leguminous myrmecophyte, Humboldtia laurifolia Vahl. The biology of this stem-nesting crabronine is unique among Sphecidae in several aspects. An adult female exhibits remarkable maternal care, rearing one larva at a time, and feeding it progressively. Progressive provisioning has not been noted previously for any Crabroninae. Nests lack cell partitions and mature larvae are transported to the basal regions of their stems for cocoon spinning. The cocoon is also unlike that of any other known crabronine species, exhibiting adaptations to internode morphology and allowing movement of adults within the nest cavity. Finally, K. nordenae is remarkably different from all other known Sphecidae in feeding pollen rather than paralyzed arthropod prey to its larvae. RP Krombein, KV (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,MUSEUM NATL HIST NAT,MRC 165,WASHINGTON,DC 20560, USA. NR 4 TC 3 Z9 3 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 1997 VL 99 IS 1 BP 42 EP 49 PG 8 WC Entomology SC Entomology GA WN469 UT WOS:A1997WN46900004 ER PT S AU Weekes, TC Aharonian, F Fegan, DJ Kifune, T AF Weekes, TC Aharonian, F Fegan, DJ Kifune, T BE Dermer, CD Strickman, MS Kurfess, JD TI VHE and UHE gamma-ray astronomy in the EGRET era SO PROCEEDINGS OF THE FOURTH COMPTON SYMPOSIUM, PTS 1 AND 2: PT 1: THE COMPTON OBSERVATORY IN REVIEW; PT 2: PAPERS AND PRESENTATIONS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 4th Compton Symposium CY APR 27-30, 1997 CL WILLIAMSBURG, VA AB Although the basic techniques used in Very High and Ultra High Energy gamma-ray astronomy have been available for more than 30 years, it is only in the past decade (mostly in the EGRET era) :hat the disciplines have become viable with the production of verifiable results. Well-established steady sources include the Crab Nebula, PSR1706-44 and Vela as well as the AGNs, Markarian 421 and 501. The early successes of EGRET were a catalyst and accelerated the development of advanced atmospheric Cerenkov telescopes. The useful symbiosis that has developed between space and ground-based gamma-ray observations is the major subject of this review. C1 Harvard Smithsonian Ctr Astrophys, Whippie Observ, Amado, AZ 85645 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Whippie Observ, POB 97, Amado, AZ 85645 USA. NR 0 TC 7 Z9 7 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-659-X J9 AIP CONF PROC PY 1997 IS 410 BP 361 EP 383 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK17N UT WOS:000071400800021 ER PT S AU Eikenberry, SS Fazio, GG AF Eikenberry, SS Fazio, GG BE Dermer, CD Strickman, MS Kurfess, JD TI The infrared to gamma-ray pulse shape of the Crab Nebula pulsar SO PROCEEDINGS OF THE FOURTH COMPTON SYMPOSIUM, PTS 1 AND 2: PT 1: THE COMPTON OBSERVATORY IN REVIEW; PT 2: PAPERS AND PRESENTATIONS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 4th Compton Symposium CY APR 27-30, 1997 CL WILLIAMSBURG, VA AB We analyze the pulse shape of the Crab Nebula pulsar in the near-infrared, optical, ultraviolet, X-ray, and gamma-ray bands. We find that the phase separation between the two peaks of the pulse profile decreases nearly continuously as a function of energy over 7 decades of energy. We find that the differences between the energy dependences of the leading and trailing edge half-width half-maxima of both peaks found by Eikenberry et al. (1996a) also continue over 7 decades of energy. We show that the cusped shape of Peak 2 reverses direction between the infrared/optical and X-ray/gamma-ray bands, while the cusped shape of Peak 1 shows weak evidence of reversing direction between the X-ray and gamma-ray bands. These and many other pulse shape parameters are not predicted by current pulsar emission models, and offer new challenges for the development of such models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eikenberry, SS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-659-X J9 AIP CONF PROC PY 1997 IS 410 BP 547 EP 551 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK17N UT WOS:000071400800035 ER PT S AU Bloser, PF Grindlay, JE Barret, D Zhang, SN Harmon, BA Fishman, GJ Paciesas, WS AF Bloser, PF Grindlay, JE Barret, D Zhang, SN Harmon, BA Fishman, GJ Paciesas, WS BE Dermer, CD Strickman, MS Kurfess, JD TI BATSE observations of two hard x-ray outbursts from 4U1630-47 SO PROCEEDINGS OF THE FOURTH COMPTON SYMPOSIUM, PTS 1 AND 2: PT 1: THE COMPTON OBSERVATORY IN REVIEW; PT 2: PAPERS AND PRESENTATIONS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 4th Compton Symposium CY APR 27-30, 1997 CL WILLIAMSBURG, VA AB Analyzing data from the BATSE instrument on the Compton Gamma. Ray Observatory. we have found evidence of two hard X-ray outbursts from the ultra-soft transient and black hole candidate 4U 1630-47. Both outbursts are nearly simultaneous with observations at lower energies by other instruments, In July 1994, the source reached a hard X-ray (20-100 keV) flux of similar to 100 mCrab, with a possible brief flare of similar to 200 mCrab. BATSE occultation images confirm that this emission originated from 4U 1630-47. This outburst corresponds to an archival detection of the source by ASCA, as reported by Parmar et al. [9] In June 1996, during the extended outburst observed by RXTE [6], the 20-100 keV flux also reached similar to 100 mCrab. The origin of this emission was verified by BATSE images as well. Kuulkers et al. [5] present RXTE/ASM data from the same period of time. We compare the BATSE data with the ASCA and RXTE/ASM results in order to push our knowledge of this source's spectral characteristics into the hard X-ray range. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bloser, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-659-X J9 AIP CONF PROC PY 1997 IS 410 BP 952 EP 956 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK17N UT WOS:000071400800116 ER PT S AU Buckley, JH Boyle, P Burdett, A Gordo, JB Carter-Lewis, DA Catanese, M Cawley, MF Fegan, DJ Finley, JP Gaidos, JA Hillas, AM Krennrich, F Lamb, RC Lessard, RW Masterson, C McEnery, J Mohanty, G Quinn, J Rodgers, A Rose, HJ Samuelson, F Sembroski, GH Srinivasan, R Weekes, TC Zweerink, J AF Buckley, JH Boyle, P Burdett, A Gordo, JB Carter-Lewis, DA Catanese, M Cawley, MF Fegan, DJ Finley, JP Gaidos, JA Hillas, AM Krennrich, F Lamb, RC Lessard, RW Masterson, C McEnery, J Mohanty, G Quinn, J Rodgers, A Rose, HJ Samuelson, F Sembroski, GH Srinivasan, R Weekes, TC Zweerink, J BE Dermer, CD Strickman, MS Kurfess, JD TI Multiwavelength observations of Markarian 421 SO PROCEEDINGS OF THE FOURTH COMPTON SYMPOSIUM, PTS 1 AND 2: PT 1: THE COMPTON OBSERVATORY IN REVIEW; PT 2: PAPERS AND PRESENTATIONS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 4th Compton Symposium CY APR 27-30, 1997 CL WILLIAMSBURG, VA AB We report on TeV gamma-ray observations of Mrk 421 made with the Whipple Observatory's 10 m telescope over the period 1994 to 1996 and summarize the results of contemporaneous multiwavelength observations. These observations indicate short variability timescales (<1 hr) and correlations in the TeV gamma-ray, X-ray, extreme UV, and optical flux. The broadband spectrum for Mrk 421 determined from data taken in three epochs is presented and implications of these data on the physical parameters in the jet are discussed. C1 Harvard Smithsonian Ctr Astrophys, FL Whipple Observ, Amado, AZ 85645 USA. RP Buckley, JH (reprint author), Harvard Smithsonian Ctr Astrophys, FL Whipple Observ, POB 97, Amado, AZ 85645 USA. RI McEnery, Julie/D-6612-2012 NR 0 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-659-X J9 AIP CONF PROC PY 1997 IS 410 BP 1381 EP 1385 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK17N UT WOS:000071400800200 ER PT S AU Fiore, F Elvis, M AF Fiore, F Elvis, M BE Day, C Mukai, T Schweihm, G Philbrick, CR TI On the observational evidence for accreting black holes in quasars SO RADIATION FROM BLACK HOLES, FUTURE MISSIONS TO PRIMITIVE BODIES AND MIDDLE ATMOSPHERIC FINE STRUCTURES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT Symposia on Radiation from Black Holes, Future Missions to Primitive Bodies and Middle Atmospheric Fine Structures, at the 30th COSPAR Scientific Assembly CY JUL 11-21, 1994 CL HAMBURG, GERMANY SP Comm Space Res, Commiss E B & C, Int Astron Union ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; MICROLENSING EVENT; SEYFERT-1 GALAXIES; HIGH-REDSHIFT; COLD MATTER; VARIABILITY; EMISSION; DISKS; LINE AB We review (mainly high energy) observations which could lend support to (or dismiss) the hypothesis of an accreting central black hole in quasars. Direct imaging is not powerful (1). We focus on three main topics: 2) variability as a constraint of the quasar compactness; 3) X-ray continuum; 4) X-ray spectral features, expected from reprocessing of the X-ray radiation from matter near the X-ray source. We argue that the above observations provide a weaker evidence than once thought for a black hole as the engine of quasars. New tests will come from (5) the study of the evolution of the quasar Spectral Energy Distribution (SED) in the framework of models of quasar physical evolution. We present some new results, obtained comparing ROSAT X-ray observations of z=2-3 quasars with previous monitoring of low-z quasars, which represent a first steep in this direction. (C) 1997. Published by Elsevier Science Ltd on behalf of COSPAR. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Fiore, F (reprint author), OSSERV ASTRON ROMA, I-00136 ROME, ITALY. OI Fiore, Fabrizio/0000-0002-4031-4157 NR 56 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0273-1177 BN 0-08-043097-X J9 ADV SPACE RES-SERIES PY 1997 VL 19 IS 1 BP 85 EP 94 DI 10.1016/S0273-1177(97)00041-0 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BH61X UT WOS:A1997BH61X00012 ER PT J AU Roth, TL Armstrong, DL Barrie, MT Wildt, DE AF Roth, TL Armstrong, DL Barrie, MT Wildt, DE TI Seasonal effects on ovarian responsiveness to exogenous gonadotrophins and successful artificial insemination in the snow leopard (Uncia uncia) SO REPRODUCTION FERTILITY AND DEVELOPMENT LA English DT Article DE felid; seasonality; ovulation induction; laparoscopy; ovary ID DOMESTIC CAT; PANTHERA-UNCIA; CHORIONIC-GONADOTROPIN; INVITRO FERTILIZATION; LUTEINIZING-HORMONE; ACINONYX-JUBATUS; SEXUAL-BEHAVIOR; PROGESTERONE; EMBRYOGENESIS; STIMULATION AB Ovaries of the seasonally-breeding snow leopard (Uncia uncia) were examined to determine whether they were responsive to exogenous gonadotrophins throughout the year. The potential of laparoscopic artificial insemination (Al) also was assessed for producing offspring. During the non-breeding, pre-breeding, breeding and post-breeding seasons, females (n = 20) were treated with a standardized, dual-hormone regimen given intramuscularly (600 I.U. of equine chorionic gonadotrophin followed 80-84 h later with 300 I.U. of human chorionic gonadotrophin (hCG)). Laparoscopy was performed 45-50 h after administration of hCG, and all ovarian structures were described. Females with fresh corpora lutea (CL) were inseminated, and anovulatory females were subjected to follicular aspiration to examine oocyte quality. Snow leopards responded to exogenous gonadotrophins throughout the year. Mean number of total ovarian structures (distinct follicles mature in appearance plus CL) did not differ (P greater than or equal to 0.05) with season, but the proportion of CL:total ovarian structures was greater (P < 0.01) for the breeding season compared with all other seasons. The proportion of females ovulating was greater (P < 0.05) during the breeding and post-breeding seasons than during the pre-breeding and non-breeding seasons respectively. No Grade-1 quality oocytes were recovered from follicles of anovulatory females. Serum concentrations of oestradiol-17 beta appeared elevated in all females, and neither oestradiol-17 beta concentrations nor progesterone concentrations differed (P greater than or equal to 0.05) among seasons. Of 15 females artificially inseminated, the only one that was inseminated in the non-breeding season became pregnant and delivered a single cub. This is the first successful pregnancy resulting from Al in this endangered species. C1 OMAHAS HENRY DOORLY ZOO,OMAHA,NE 68107. OKLAHOMA CITY ZOO,OKLAHOMA CITY,OK 73111. SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. NR 42 TC 22 Z9 22 U1 2 U2 9 PU C S I R O PUBLICATIONS PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD VICTORIA 3066, AUSTRALIA SN 1031-3613 J9 REPROD FERT DEVELOP JI Reprod. Fertil. Dev. PY 1997 VL 9 IS 3 BP 285 EP 295 DI 10.1071/R96048 PG 11 WC Developmental Biology; Reproductive Biology; Zoology SC Developmental Biology; Reproductive Biology; Zoology GA XP328 UT WOS:A1997XP32800002 PM 9261877 ER PT S AU Ho, IC AF Ho, IC BE Franco, J Terlevich, R Serrano, A TI Young star clusters in starburst environments SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA: SERIE DE CONFERENCIAS, VOL 6, MAYO 1997: 1ST GUILLERMO HARO CONFERENCE ON ASTROPHYSICS - STARBURST ACTIVITY IN GALAXIES SE REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA, SERIE DE CONFERENCIAS LA English DT Proceedings Paper CT 1st Guillermo Haro Conference on Astrophysics - Starburst Activity in Galaxies CY APR 29-MAY 03, 1996 CL PUEBLA, MEXICO SP Univ Nacl Autonoma Mexico, Inst Astron DE galaxies, compact; galaxies, starburst; galaxies, stellar content; stars, formation AB Recent high-resolution observations with the Hubble Space Telescope (HST) reveal that young star clusters of extraordinary luminosity and compactness (''super star clusters'') are commonly found in starburst systems. Cluster formation appears to be a dominant mode of star formation in starbursts. The principal properties of the young clusters are summarized. A new UV HST imaging survey of the central regions of nearby galaxies indicates that young clusters form in a wide range of environments. Circumnuclear star-forming rings, in particular, are richly populated with clusters, and several examples from recent imaging studies are discussed. There has been much speculation that super star clusters represent present-day analogs of young globular clusters. I present evidence suggesting that at least some super star clusters indeed have masses and mass densities comparable to those of evolved globular clusters in the Milky Way. RP Ho, IC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS-42,CAMBRIDGE,MA 02138, USA. NR 0 TC 39 Z9 39 U1 0 U2 0 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 J9 REV MEX AST ASTR PY 1997 VL 6 BP 5 EP 13 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ20T UT WOS:A1997BJ20T00002 ER PT S AU Habbal, SR AF Habbal, SR BE Habbal, SR TI Imaging the source regions of the solar wind SO ROBOTIC EXPLORATION CLOSE TO THE SUN: SCIENTIFIC BASIS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Workshop on Scientific Basis for Robotic Exploration Close to the Sun CY APR 15-18, 1996 CL MARLBOROUGH, MA SP Smithsonian Astrophys Observ, NASA AB Remote sensing of the solar corona in the extreme ultraviolet and white light is an indispensable tool for probing the source and acceleration regions of the solar wind which are inaccessible to in situ plasma, particles and fields experiments. Imaging the solar disk and corona from the unique vantage point of the trajectory and the proximity of the Solar Probe spacecraft will provide the first ever opportunity to explore the small scale structures within coronal holes and streamers from viewing angles and with spatial resolutions never attained before. The extreme ultraviolet and white light wavelength ranges offer a powerful tool for diagnostic studies of this region. RP Habbal, SR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-618-2 J9 AIP CONF PROC PY 1997 IS 385 BP 105 EP 112 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH28X UT WOS:A1997BH28X00012 ER PT S AU Strachan, L Gardner, LD Smith, PL Kohl, JL AF Strachan, L Gardner, LD Smith, PL Kohl, JL BE Habbal, SR TI UV spectroscopy of the extended solar corona: Results from UVCS/Spartan SO ROBOTIC EXPLORATION CLOSE TO THE SUN: SCIENTIFIC BASIS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Workshop on Scientific Basis for Robotic Exploration Close to the Sun CY APR 15-18, 1996 CL MARLBOROUGH, MA SP Smithsonian Astrophys Observ, NASA AB Remote sensing of the solar corona using ultraviolet spectroscopy can be used to characterize the physical state of the plasma along a wide region around the trajectory of a near-Sun flyby spacecraft (solar probe). Data from such an instrument can be used to separate spatial from temporal variations in the data received from in situ instruments aboard the probe. We present results from the UVCS/Spartan space shuttle missions in order to show examples of diagnostic techniques that can be used to determine velocity distributions and bulk outflow velocities of protons and minor ions in the solar wind. RP Strachan, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-618-2 J9 AIP CONF PROC PY 1997 IS 385 BP 113 EP 120 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH28X UT WOS:A1997BH28X00013 ER PT S AU Esser, R Brickhouse, NS AF Esser, R Brickhouse, NS BE Habbal, SR TI Interdependence of solar wind models and solar wind observations SO ROBOTIC EXPLORATION CLOSE TO THE SUN: SCIENTIFIC BASIS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Workshop on Scientific Basis for Robotic Exploration Close to the Sun CY APR 15-18, 1996 CL MARLBOROUGH, MA SP Smithsonian Astrophys Observ, NASA AB A brief overview of the observations in the inner corona is presented together with three different solar wind models. It is shown that the very high dow speeds derived from the observations in the inner corona can be modeled if either the proton temperature is extremely high, or if there exists a mechanism that adds momentum to the flow much closer to the coronal base than in traditional Alfven wave driven models. These high flow speeds and the possibility that the proton temperature is very high have an influence on observations used to infer plasma parameters in the inner corona. This point is illustrated choosing the line ratio density diagnostic as an example. RP Esser, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-618-2 J9 AIP CONF PROC PY 1997 IS 385 BP 219 EP 226 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BH28X UT WOS:A1997BH28X00026 ER PT B AU Kochanek, CS Keeton, CR AF Kochanek, CS Keeton, CR BE Arnaboldi, M daCosta, GS Saha, P TI Gravitational lensing limits on early-type galaxies SO SECOND STROMLO SYMPOSIUM: THE NATURE OF ELLIPTICAL GALAXIES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 2nd Stromlo Symposium on the Nature of Elliptical Galaxies CY AUG 26-30, 1996 CL AUSTR ACAD SCI, CANBERRA, AUSTRALIA SP Austr Natl Univ, Mt Stromlo Observ, Austr Natl Univ, Siding Spring Observ, Austr Govt, Dept Ind Sci & Tourism, QANTAS, Austr Telescope Natl Facil, Univ Sydney, Res Ctr Theoret Astrophys, Anglo Austr Observ, Austr Acad Sci HO AUSTR ACAD SCI AB Gravitational lenses are a unique new constraint on the structure of galaxies. We review the evidence that most lenses are early-type galaxies, the optical properties of the lens galaxies, the evidence against constant MIL models, recent work on the axis ratios of the mass distribution, and the role stellar dynamics plays in gravitational lensing. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-36-8 J9 ASTR SOC P PY 1997 VL 116 BP 21 EP 31 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK73M UT WOS:000073252500003 ER PT B AU Romanowsky, AJ Kochanek, CS AF Romanowsky, AJ Kochanek, CS BE Arnaboldi, M daCosta, GS Saha, P TI New projections of triaxiality SO SECOND STROMLO SYMPOSIUM: THE NATURE OF ELLIPTICAL GALAXIES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 2nd Stromlo Symposium on the Nature of Elliptical Galaxies CY AUG 26-30, 1996 CL AUSTR ACAD SCI, CANBERRA, AUSTRALIA SP Austr Natl Univ, Mt Stromlo Observ, Austr Natl Univ, Siding Spring Observ, Austr Govt, Dept Ind Sci & Tourism, QANTAS, Austr Telescope Natl Facil, Univ Sydney, Res Ctr Theoret Astrophys, Anglo Austr Observ, Austr Acad Sci HO AUSTR ACAD SCI AB An elliptical galaxy is considered to consist of a triaxial luminous stellar distribution embedded in a triaxial "dark" halo. Differences in the triaxialities lead to kinematic misalignments, X-ray isophote twists, and gravitational lens model misalignments. We have numerically projected the X-ray emission of a model stellar and halo potential and compared it to the luminous galaxy projection for a variety of viewing angles. The two projections generally show a small misalignment, with an X-ray isophote twist of similar to 5 degrees occurring near the effective radius. The large misalignment observed in NGC 720 could not be well fit, suggesting that it requires an intrinsic misalignment of the halo and the galaxy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romanowsky, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-36-8 J9 ASTR SOC P PY 1997 VL 116 BP 107 EP 108 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK73M UT WOS:000073252500022 ER PT B AU Caldwell, N AF Caldwell, N BE Arnaboldi, M daCosta, GS Saha, P TI Parameter relations for dwarf elliptical galaxies SO SECOND STROMLO SYMPOSIUM: THE NATURE OF ELLIPTICAL GALAXIES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 2nd Stromlo Symposium on the Nature of Elliptical Galaxies CY AUG 26-30, 1996 CL AUSTR ACAD SCI, CANBERRA, AUSTRALIA SP Austr Natl Univ, Mt Stromlo Observ, Austr Natl Univ, Siding Spring Observ, Austr Govt, Dept Ind Sci & Tourism, QANTAS, Austr Telescope Natl Facil, Univ Sydney, Res Ctr Theoret Astrophys, Anglo Austr Observ, Austr Acad Sci HO AUSTR ACAD SCI AB Observations of dwarf ellipticals are reviewed, and new data on two M81 galaxies resolved into stars with HST are presented along with its impact on the luminosity-metallicity and surface brightness-metallicity relations. C1 Smithsonian Inst, FL Whipple Observ, Washington, DC 20560 USA. RP Caldwell, N (reprint author), Smithsonian Inst, FL Whipple Observ, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-36-8 J9 ASTR SOC P PY 1997 VL 116 BP 249 EP 258 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK73M UT WOS:000073252500052 ER PT B AU Mackie, G Fabbiano, G AF Mackie, G Fabbiano, G BE Arnaboldi, M daCosta, GS Saha, P TI Environmental and internal optical properties and the X-ray content of E and SOs SO SECOND STROMLO SYMPOSIUM: THE NATURE OF ELLIPTICAL GALAXIES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 2nd Stromlo Symposium on the Nature of Elliptical Galaxies CY AUG 26-30, 1996 CL AUSTR ACAD SCI, CANBERRA, AUSTRALIA SP Austr Natl Univ, Mt Stromlo Observ, Austr Natl Univ, Siding Spring Observ, Austr Govt, Dept Ind Sci & Tourism, QANTAS, Austr Telescope Natl Facil, Univ Sydney, Res Ctr Theoret Astrophys, Anglo Austr Observ, Austr Acad Sci HO AUSTR ACAD SCI AB We have compiled environmental (Tully 1988 rho(xyz), local density; Schweizer et al. 1990 Sigma, fine structure parameter) and internal (Trager et al. 1996 Lick group absorption indices) properties for E and SOs observed with Einstein. L-X/L-B is compared to all properties to determine their possible effect on gaseous X-ray content. Our main result is that the highest Sigma galaxies (dynamically youngest) have very low L-X/L-B suggesting a suppression or decrease in L-X/L-B occurs for the youngest merger candidate galaxies. A general trend of lower L-X/L-B with increasing rho(xyz) is consistent with the results of White and Sarazin (1991). Little evidence of stellar population indicators being directly linked with L-X/L-B is seen. A trend for the highest Hp galaxies (also having high Sigma) to have low L-X/L-B is probably related to the association of young stellar populations with mergers of interactions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mackie, G (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 9 Z9 9 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-36-8 J9 ASTR SOC P PY 1997 VL 116 BP 401 EP 404 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK73M UT WOS:000073252500081 ER PT J AU Cunningham, KJ Benson, RH RakicElBied, K McKenna, LW AF Cunningham, KJ Benson, RH RakicElBied, K McKenna, LW TI Eustatic implications of late Miocene depositional sequences in the Melilla Basin, northeastern Morocco SO SEDIMENTARY GEOLOGY LA English DT Article DE Messinian Salinity Crisis; Morocco; Melilla Basin; late Miocene; eustacy; depositional sequences ID TORTONIAN-MESSINIAN BOUNDARY; POLARITY TIME-SCALE; SALINITY CRISIS; SPAIN; CHRONOLOGY; HISTORY; AGE AB The age (similar to 5.78 Ma or lower chron C3r) of the major drawdown of the Paleo-Mediterranean Sea during the Messinian Salinity Crisis has been established by combining results from stratigraphy, paleontology, magnetostratigraphy, and argon dating for a late Miocene sedimentary succession in the Melilla Basin, NE Morocco. This event is inferred from a marine-to-continental series of carbonate and siliciclastic rocks that record the end of Messinian marine deposition in the Melilla Basin and presumably marks the final isolation of the Paleo-Mediterranean Sea. The evidence from the Melilla Basin is approximately coeval with an increase in benthic foraminiferal delta(18)O values from a deep-marine section in the Bou Regreg valley, NW Morocco (Hodell et al., 1994). This increase suggests that a glacio-eustatic lowering of sea level, at least, contributed to the final closure of the Mediterranean during the Messinian Salinity Crisis. The marine-to-continental succession onlaps a carbonate complex that contains evidence for multiple relative sea-level changes leading up to the main drawdown. From bottom to top, the carbonate complex is composed of: (1) an onlapping ramp; (2) a prograding bioclastic platform; (3) a prograding and, locally, downstepping Porites-reef complex; and (4) a topography-draping sequence composed of grainstones, Porites reefs, and stromatolites (terminal carbonate complex of Esteban, 1979). The transgressive ramp correlates to relatively low values of benthic foraminiferal delta(18)O values from a Tortonian-to-lower Messinian section at Bou Regreg (Hodell et al., 1994). This correlation indicates, at least in part, a link between rising sea level and a reduction in global ice volume during deposition of the ramp. A major fall in relative sea level (similar to 60 m) occurred near the demise of the reef complex during chron C3n.1n at 5.95 +/- 0.10 Ma. This signals the initiation of drawdown and changing environmental conditions in the Melilla Basin (a marginal basin), and perhaps the entire Paleo-Mediterranean Sea. A megabreccia interpreted as forming by solution collapse of evaporites on the basin margin of the reef complex occurs at the base of the terminal carbonate complex. Updip, a major subaerial unconformity separates the reef complex and terminal carbonate complex. Evaporite deposition likely occurred during this exposure event and has been dated at 5.82 +/- 0.02 Ma near the base of chron C3r. We contend that these evaporites, restricted to the shallow Melilla Basin, are related to the continuation of the initial stage of the major drawdown of the Paleo-Mediterranean Sea. C1 UNIV KANSAS,DEPT GEOL,LAWRENCE,KS 66045. NATL MUSEUM,SMITHSONIAN INST,WASHINGTON,DC 20560. SMITHSONIAN INST,RABAT,MOROCCO. OI Cunningham, Kevin/0000-0002-2179-8686 NR 45 TC 41 Z9 41 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0037-0738 J9 SEDIMENT GEOL JI Sediment. Geol. PD JAN PY 1997 VL 107 IS 3-4 BP 147 EP 165 DI 10.1016/S0037-0738(96)00037-1 PG 19 WC Geology SC Geology GA WE547 UT WOS:A1997WE54700001 ER PT S AU Bloser, PF Narita, T Grindlay, JE Shah, K AF Bloser, PF Narita, T Grindlay, JE Shah, K BE James, RB Schlesinger, TE Siffert, P Dusi, W Squillante, MR OConnell, M Cuzin, M TI Prototype imaging Cd-Zn-Te array detector SO SEMICONDUCTORS FOR ROOM-TEMPERATURE RADIATION DETECTOR APPLICATIONS II SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT 2nd Symposium on Semiconductors for Room-Temperature Radiation Detector Applications, at the 1997 MRS Fall Meeting CY DEC 01-05, 1997 CL BOSTON, MA SP Mat Res Soc, Amptek Inc, Bicron Corp, CEA LETI, US DOE, Off Nonproliferat, eV Products, Johnson Matthey Electr, Moxtek Inc, Noranda Adv Mat, RMD Inc, Sandia Natl Labs, Spire Corp AB We describe initial results of our program to develop and test Cd-Zn-Te (CZT) detectors with a pixellated array readout. Our primary interest is in the development of relatively thick CZT detectors for use in astrophysical coded aperture telescopes with response extending over the energy range similar to 10 - 600 keV. The coded aperture imaging configuration requires only relatively large area pixels (1-3 mm), whereas the desired high energy response requires detector thicknesses of at least 3-5 mm. We have developed a prototype detector employing a 10 x 10 x 5 mm CZT substrate and 4 x 4 pixel (1.5 mm each) readout with gold metal contacts for the pixels and continuous gold contact for the bias on the opposite detector face. This MSM contact configuration was fabricated by RMD and tested at Harvard for uniformity, efficiency and spatial as well as spectral resolution. We have developed an ASIC readout (IDE-VA-1) and analysis system and report results, including similar to 4% (FWHM) energy resolution at 60 keV. A prototype design for a full imaging detector array is discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bloser, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-392-4 J9 MATER RES SOC SYMP P PY 1997 VL 487 BP 153 EP 158 PG 6 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Nuclear Science & Technology SC Engineering; Materials Science; Nuclear Science & Technology GA BL33B UT WOS:000075187100022 ER PT S AU Freeman, M Boyd, D Lynch, N AF Freeman, M Boyd, D Lynch, N BE Guyenne, TD TI Thermal effects on imaging performance of the AXAF telescope SO SIXTH EUROPEAN SYMPOSIUM ON SPACE ENVIRONMENTAL CONTROL SYSTEMS, VOLS 1 AND 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 6th European Symposium on Space Environmental Control Systems CY MAY 20-22, 1997 CL NOORDWIJK, NETHERLANDS SP European Space Agcy AB In the paper the we discuss how the thermal behavior of the Advanced X-ray Astrophysics Facility (AXAF) optical system has been modeled and tested, and how these efforts have influenced the design of the telescope, especially as it relates the imaging performance. This includes the passive/active system covering the space-facing aperture known as the thermal ''precollimator'', the mechanical support system that allows the large optical elements to survive the rigors of test in one-G and launch yet minimally affecting on-orbit optical performance, and the active thermal control design of the telescope. Methodologies for the frequently difficult task of transferring results from thermal analysis software to mechanical finite-element analyzers to model thermal deformations are discussed. The complexity of these distortions of the surfaces of the mirror elements required the use of optical raytrace models to assess imaging performance of the telescope. A software tool was developed to allow the transfer of results from the several sources of mirror distortion data to an internally-developed raytrace package to assess performance. Several thermal cases and the resulting telescope performance predictions are shown. Examples of the use of these results in the design cycle to make critical decisions about hardware or the use of ultra-low expansivity materials are discussed. RP Freeman, M (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-283-4 J9 ESA SP PUBL PY 1997 VL 400 BP 667 EP 674 PG 8 WC Engineering, Aerospace SC Engineering GA BJ69Y UT WOS:A1997BJ69Y00082 ER PT S AU Raymond, JC Blair, WP Long, KS AF Raymond, JC Blair, WP Long, KS BE Dufour, RJ TorresPeimbert, S TI Ultraviolet H-2 emission from HH2 SO SIXTH TEXAS-MEXICO CONFERENCE ON ASTROPHYSICS: ASTROPHYSICAL PLASMAS NEAR AND FAR SE REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA, SERIE DE CONFERENCIAS LA English DT Proceedings Paper CT 6th Texas-Mexico Conference on Astrophysics : Astrophysical Plasmas - Near and Far CY MAR 06-08, 1997 CL RICE UNIV, HOUSTON, TX HO RICE UNIV DE ISM, jets and outflows; shock waves; ultraviolet, interstellar AB The Hopkins Ultraviolet Telescope spectrum of HH 2 shows Lyman band emission below 1200 Angstrom, and H-2 bands the quasi-continuum at longer wavelengths. It could arise either from Ly alpha fluorescence (as in other HH objects) or collisional excitation by hot electrons. It is difficult for the fluorescence hypothesis to explain the lack of individual strong features, while the collisional hypothesis must explain the mixing of hot electrons into molecular gas. The upper limit to the O VI flux appears to conflict badly with the predictions of bow shock models which match the observed line widths of HH2A' and HH2H. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 J9 REV MEX AST ASTR PY 1997 VL 7 BP 7 EP 13 PG 7 WC Astronomy & Astrophysics; Physics, Fluids & Plasmas SC Astronomy & Astrophysics; Physics GA BK86R UT WOS:000073706100002 ER PT J AU Heyman, IM AF Heyman, IM TI Smithsonian perspectives + In the ever-expanding field of anthropology, the Smithsonian still excels in research and exhibition SO SMITHSONIAN LA English DT Editorial Material RP Heyman, IM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD JAN PY 1997 VL 27 IS 10 BP 8 EP 8 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA WB296 UT WOS:A1997WB29600001 ER PT J AU Collins, MS Haverty, MI Thorne, BL AF Collins, MS Haverty, MI Thorne, BL TI The termites (Isoptera: Kalotermitidae, Rhinotermitidae, Termitidae) of the British Virgin Islands: Distribution, moisture relations, and cuticular hydrocarbons SO SOCIOBIOLOGY LA English DT Article AB A survey of the termites (Isoptera) of 19 islands of the British Virgin Islands (BVI) yielded at least eight species belonging to three families. The Kalotermitidae occurring in the BVI are Neotermes mona (Banks), Incisitermes species (appear close to I. snyderi (Light) and I. incisus (Silvestri)), Procryptotermes corniceps (Snyder), and Cryptotermes brevis (Walker). The only representative of the Rhinotennitidae we collected in the BVI is one or more undetermined species of Heterotermes (Froggatt). The three species of Termitidae found on Guana Island are Nasutitermes acajutlae (Holmgren), N. costalis (Holmgren) and Parvitermes wolcotti (Snyder). This report presents brief descriptions of the biology of these termites, along with summaries of the collection sites. Cuticular hydrocarbon composition is correlated with apparent moisture requirements of the termites and availability on the various islands. C1 US FOREST SERV,PACIFIC SW RES STN,USDA,BERKELEY,CA 94701. SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT ENTOMOL,WASHINGTON,DC 20560. UNIV MARYLAND,DEPT ENTOMOL,COLLEGE PK,MD 20742. NR 32 TC 10 Z9 10 U1 1 U2 1 PU CALIF STATE UNIV PI CHICO PA DEPT BIOL SCI, CHICO, CA 95929 SN 0361-6525 J9 SOCIOBIOLOGY JI Sociobiology PY 1997 VL 30 IS 1 BP 63 EP 76 PG 14 WC Entomology SC Entomology GA XP473 UT WOS:A1997XP47300005 ER PT S AU Myers, PC AF Myers, PC BE Holt, SS Mundy, LG TI Early star formation SO STAR FORMATION NEAR AND FAR - SEVENTH ASTROPHYSICS CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 7th Annual October Astrophysics Conference on Star Formation, Near and Far CY OCT, 1996 CL COLLEGE PK, MD SP Goddard Space Flight Ctr, Univ Maryland AB We describe recent progress in two areas of the early stages of star formation-initial conditions for making stellar groups, and kinematic evidence for star-forming infall. RP Myers, PC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 5 Z9 5 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-678-6 J9 AIP CONF PROC PY 1997 IS 393 BP 41 EP 50 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ23B UT WOS:A1997BJ23B00003 ER PT S AU Ohashi, N AF Ohashi, N BE Holt, SS Mundy, LG TI Dynamically infalling envelopes around low-mass protostar candidates SO STAR FORMATION NEAR AND FAR - SEVENTH ASTROPHYSICS CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 7th Annual October Astrophysics Conference on Star Formation, Near and Far CY OCT, 1996 CL COLLEGE PK, MD SP Goddard Space Flight Ctr, Univ Maryland AB Interferometric observations of two protostar candidates, L1551 IRS5 and IRAS 04368+2557(L1527), in Taurus have directly identified dynamically infalling motions in their circumstellar envelopes. The observed infalling envelopes have disklike structures, which are perpendicular to the associated outflows, with a thousand AU scale. In addition to infall, rotation was detected in the envelope around IRAS 04368+2557. This rotation is 5 times slower than the infall at 2000 AU in radius, suggesting that the envelope around IRAS 04368+2557 is not rotationally supported. Mass infall rates were estimated to be 10(-5) M. yr(-1) for L1551 IRS5, and 10(-6) M. yr(-1) for IRAS 04368+2557. RP Ohashi, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-678-6 J9 AIP CONF PROC PY 1997 IS 393 BP 93 EP 96 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ23B UT WOS:A1997BJ23B00011 ER PT S AU Wilner, DJ Mardones, D Myers, PC AF Wilner, DJ Mardones, D Myers, PC BE Holt, SS Mundy, LG TI Interferometric imaging of dense gas tracers in the protostellar collapse candidate L1527 SO STAR FORMATION NEAR AND FAR - SEVENTH ASTROPHYSICS CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 7th Annual October Astrophysics Conference on Star Formation, Near and Far CY OCT, 1996 CL COLLEGE PK, MD SP Goddard Space Flight Ctr, Univ Maryland AB We present 3'' (similar to 400 AU) OVRO and IRAM interferometer observations at lambda = 3.0 mm and 1.3 mm of L1527, one of the closest protostellar collapse candidates, We imaged high excitation lines of H2CO and HC3N in an effort to probe the highest densities, temperatures and infall velocities close to the L1527 protostar. The integrated intensity maps show an elongated structure of major axis size 20'' oriented perpendicular to the bipolar outflow axis. Spectral signatures associated with infall persist to the smallest scales observed. RP Wilner, DJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-678-6 J9 AIP CONF PROC PY 1997 IS 393 BP 109 EP 112 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ23B UT WOS:A1997BJ23B00015 ER PT S AU Mardones, D Myers, PC Tafalla, M Wilner, DJ Bachiller, R Garay, G AF Mardones, D Myers, PC Tafalla, M Wilner, DJ Bachiller, R Garay, G BE Holt, SS Mundy, LG TI A statistical study of infall motions in nearby young stellar objects SO STAR FORMATION NEAR AND FAR - SEVENTH ASTROPHYSICS CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 7th Annual October Astrophysics Conference on Star Formation, Near and Far CY OCT, 1996 CL COLLEGE PK, MD SP Goddard Space Flight Ctr, Univ Maryland AB We observed 49 nearby low mass pre-main-sequence stars in the H2CO 2(12) - 1(11), CS 2-1 (both optically thick) and N2H+ 1-0 (optically thin) mm-wavelength lines using the IRAM 30-m, SEST 15-m, and Haystack 37-m radio telescopes. The sources were selected from their spectral energy distributions (T-bol < 200 K) and distance (d < 400 pc). We find an overabundance of sources whose optically thick lines have blue-shifted asymmetry. We quantify the observed line asymmetries by measuring the difference in the peak velocities of the optically thick and optically thin lines. The observed distribution of velocity differences is skewed toward negative values of V-thick - V-thin velocities. This excess is statistically more significant toward the subsample of the class 0 sources (T-bol < 70 K) This can be most naturally explained if low T-bol sources tend to have inward motions. Kinematics of bipolar outflows or rotation can't reproduce the statistics if the source sample has randomly oriented symmetry axes. The statistical results are insensitive to variations in pointing, and are indistinguishable for the CS and H2CO line profiles. RP Mardones, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-678-6 J9 AIP CONF PROC PY 1997 IS 393 BP 113 EP 116 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ23B UT WOS:A1997BJ23B00016 ER PT S AU Williams, JP Myers, PC AF Williams, JP Myers, PC BE Holt, SS Mundy, LG TI Evidence for core collapse toward 3 young stellar clusters SO STAR FORMATION NEAR AND FAR - SEVENTH ASTROPHYSICS CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 7th Annual October Astrophysics Conference on Star Formation, Near and Far CY OCT, 1996 CL COLLEGE PK, MD SP Goddard Space Flight Ctr, Univ Maryland AB Observations of CS(2-1) and N2H+(1-O) emission toward three young stellar clusters, Serpens NW, NGC1333-IRAS4, and L1251B are discussed. Comparison of the spectra shows that the CS is self-absorbed in many positions, and generally in an asymmetric way (the blue side of the line being of greater intensity than the fed) that is characteristic of inward motions onto a warm central core. The predominance for the asymmetry to indicate infall, rather than outflow, in many positions in each core, and in all three sources, suggests that the effect is real, and that large scale core collapse is being observed. A simple one-dimensional model is described and fit to the line profiles resulting in an estimate of the mass infall rate in each case. RP Williams, JP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-678-6 J9 AIP CONF PROC PY 1997 IS 393 BP 387 EP 390 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ23B UT WOS:A1997BJ23B00063 ER PT S AU Ho, LC Filippenko, AV AF Ho, LC Filippenko, AV BE Holt, SS Mundy, LG TI Observational evidence for the present-day formation of globular clusters SO STAR FORMATION NEAR AND FAR - SEVENTH ASTROPHYSICS CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 7th Annual October Astrophysics Conference on Star Formation, Near and Far CY OCT, 1996 CL COLLEGE PK, MD SP Goddard Space Flight Ctr, Univ Maryland AB We present evidence that some of the compact, luminous, young star clusters recently discovered through images taken with the Hubble Space Telescope (HST) have masses comparable to those of old Galactic globular clusters. Three ''super star clusters'' in the centers of the nearby dwarf galaxies NGC 1569, NGC 1705, and NGC 4214 have been observed with the HIRES echelle spectrograph on the Keck 10 m telescope to measure the velocity dispersion of the stars. The velocity dispersion was measured successfully for the clusters in NGC 1569 and NGC 1705, which, when combined with the size estimates obtained from HST images, imply that the clusters have very large dynamical masses. The masses, mass densities, and predicted mass-to-light ratios (at t = 10-15 Gyr) of these two 10-Myr old clusters closely resemble those of the majority of evolved Galactic globular clusters. We interpret the results as evidence that these objects are genuinely young globular clusters. RP Ho, LC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-678-6 J9 AIP CONF PROC PY 1997 IS 393 BP 403 EP 405 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ23B UT WOS:A1997BJ23B00067 ER PT S AU Zhang, QZ Ho, PTP AF Zhang, QZ Ho, PTP BE Holt, SS Mundy, LG TI Star formation at the intermediate distances: Gravitational collapse in massive cores SO STAR FORMATION NEAR AND FAR - SEVENTH ASTROPHYSICS CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 7th Annual October Astrophysics Conference on Star Formation, Near and Far CY OCT, 1996 CL COLLEGE PK, MD SP Goddard Space Flight Ctr, Univ Maryland AB We present spectroscopic evidence of gravitational collapse in massive molecular cloud cores toward the W51 HII region complex. The NH3 (J,K)=(2,2) and (3,3) lines obtained at similar to 1'' angular resolution exhibit inverse P-Cygni or asymmetric profiles, suggesting inward motions of gas toward the central star. The infall motions appear to be localized to individual dense cores, contrary to the suggestion of overall collapse. The two collapsing cores are embedded in a more extended cloud of 1.6pc. If both cores are formed out of this cloud through fragmentation, it seems that both cores are now under collapse again in making the final product: massive OB stars. RP Zhang, QZ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-678-6 J9 AIP CONF PROC PY 1997 IS 393 BP 453 EP 456 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJ23B UT WOS:A1997BJ23B00076 ER PT J AU Becker, MA Magoshi, Y Sakai, T Tuross, NC AF Becker, MA Magoshi, Y Sakai, T Tuross, NC TI Chemical and physical properties of old silk fabrics + Biochemical analysis of 17 Japanese silk kimono lining fabrics SO STUDIES IN CONSERVATION LA English DT Article C1 NAT INST SERICULTURAL & ENTOMOL SCI, IBARAKI, OSAKA 305, JAPAN. KYOURITSU WOMENS UNIV, TOKYO, JAPAN. SMITHSONIAN INST, CONSERVATION ANAL LAB, WASHINGTON, DC 20560 USA. RP TOKYO NAT RES INST CULTURAL PROPERTIES, TOKYO 110, JAPAN. NR 18 TC 12 Z9 12 U1 0 U2 4 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0039-3630 EI 2047-0584 J9 STUD CONSERV JI Stud. Conserv. PY 1997 VL 42 IS 1 BP 27 EP 37 DI 10.2307/1506573 PG 11 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA WQ461 UT WOS:A1997WQ46100004 ER PT S AU Noci, G Kohl, JL Antonucci, E Tondello, G Huber, MCE Fineschi, S Gardner, LD Naletto, G Nicolosi, P Raymond, JC Romoli, M Spadaro, D Siegmund, OHW Benna, C Ciaravella, A Giordano, S Michels, J Modigliani, A Panasyuk, A Pernechele, C Poletto, G Smith, PL Strachan, L AF Noci, G Kohl, JL Antonucci, E Tondello, G Huber, MCE Fineschi, S Gardner, LD Naletto, G Nicolosi, P Raymond, JC Romoli, M Spadaro, D Siegmund, OHW Benna, C Ciaravella, A Giordano, S Michels, J Modigliani, A Panasyuk, A Pernechele, C Poletto, G Smith, PL Strachan, L BE Antonucci, E Shea, MA TI First results from UVCS/SOHO SO SUN AND ITS ATMOSPHERE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT E2.1 Symposium of COSPAR Scientific Commission E on the Sun and Its Atmosphere, at the 31st COSPAR Scientific Assembly CY JUL 14-SEP 21, 1996 CL BIRMINGHAM, ENGLAND SP Comm Space Res, European Space Agcy, Inst Space & Astron Sci ID KINETIC TEMPERATURES; SOLAR AB We present here the first results obtained by the Ultraviolet Coronagraph Spectrometer (UVCS) operating on board the SOHO satellite, The UVCS started to observe the extended corona at the end of January 1996; it routinely obtains coronal spectra in the 1145 Angstrom-1281 Angstrom, 984 Angstrom -1080 Angstrom ranges, and intensity data in the visible continuum, Through the composition of slit images it also produces monocromatic images of the extended corona, The performance of the instrument is excellent and the data obtained up to now are of great interest, We briefly describe preliminary results concerning polar coronal holes, streamers and a coronal mass ejection, in particular: the very large r.m.s. velocities of ions in polar holes (hundreds km/sec for OVI and MgX); the puzzling difference between the HI Ly-alpha image and that in the OVI resonance doublet, for most streamers; the different signatures of the core and external layers of the streamers in the width of the ion lines and in the OVI doublet ratio, indicating larger line-of-sight (l.o.s.) and outflow velocities in the latter. (C) 1997 COSPAR. Published by Elsevier Science Ltd. C1 Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. Univ Padua, Dipartimento Elettron & Informat, I-35131 Padua, Italy. European Space Agcy, Estec, Dept Space Sci, NL-2200 AG Noordwijk, Netherlands. Osservatorio Astrofis Catania, I-95125 Catania, Italy. Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Noci, G (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. RI Romoli, Marco/H-6859-2012; Naletto, Giampiero/S-6329-2016; OI Naletto, Giampiero/0000-0003-2007-3138; Giordano, Silvio/0000-0002-3468-8566; Benna, Carlo/0000-0003-1688-2434; Ciaravella, Angela/0000-0002-3127-8078; Spadaro, Daniele/0000-0003-3517-8688 NR 11 TC 55 Z9 55 U1 0 U2 1 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0273-1177 BN 0-08-043309-X J9 ADV SPACE RES PY 1997 VL 20 IS 12 BP 2219 EP 2230 DI 10.1016/S0273-1177(97)00895-8 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BK38L UT WOS:000071955600002 ER PT S AU Kohl, JH Noci, G Antonucci, E Tondello, G Huber, MCE Gardner, LD Nicolosi, P Fineschi, S Raymond, JC Romoli, M Spadaro, D Siegmund, OHW Benna, C Ciaravella, A Cranmer, SR Giordano, S Karovska, M Martin, R Michels, J Modigliani, A Naletto, G Panasyuk, A Pernechele, C Poletto, G Smith, PL Strachan, L AF Kohl, JH Noci, G Antonucci, E Tondello, G Huber, MCE Gardner, LD Nicolosi, P Fineschi, S Raymond, JC Romoli, M Spadaro, D Siegmund, OHW Benna, C Ciaravella, A Cranmer, SR Giordano, S Karovska, M Martin, R Michels, J Modigliani, A Naletto, G Panasyuk, A Pernechele, C Poletto, G Smith, PL Strachan, L BE Antonucci, E Page, DE TI Measurements of H I and O VI velocity distributions in the extended solar corona with UVCS/SOHO and UVCS/Spartan 201 SO SUN AND ITS ROLE IN THE HELIOSPHERE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT E2.2 Symposium of COSPAR Scientific Commission E on the Sun and Its Role in the Heliosphere, at the 31st COSPAR Scientific Assembly CY JUL 14-21, 1996-1997 CL BIRMINGHAM, ENGLAND SP Comm space Res, Comm E, European Space Agcy, Inst Space & Astronaut Sci ID WIND AB The Ultraviolet Coronagraph Spectrometer on the Solar and Heliospheric Observatory, UVCS/SOHO, and the Ultraviolet Coronal Spectrometer on the Spartan 201 satellite, UVCS/Spartan, have been used to measure H I 1215.61 Angstrom line profiles in polar coronal holes of the Sun at projected heliocentric heights between 1.5 and 3.0 R.. UVCS/SOHO also measured line profiles for H I 1025.72 Angstrom, O VI 1032/1037 Angstrom, and Mg X 625 Angstrom. The reported UVCS/SOHO observations were made between 5 April and 21 June 1996 and the UVCS/Spartan observations were made between 11 and 12 April 1993. Both sets of measurements indicate that a significant fraction of the protons along the line of sight in coronal holes have velocities larger than those for a Maxwellian velocity distribution at the expected electron temperature, Most probable speeds for O5+ velocity distributions along the lines of sight are smaller than those of H-0 at 1.5 R., are comparable at about 1.7 R. and become significantly larger than the H-0 velocities above 2 R.. There is a tendency for the O5+ line of sight velocity distribution in concentrations of polar plumes to be more narrow than those in regions away from such concentrations. UVCS/SOHO has identified 31 spectral lines in the extended solar corona. (C) 1997 COSPAR. Published by Elsevier Science Ltd. C1 UNIV FLORENCE, I-50125 FLORENCE, ITALY. OSSERV ASTRON TORINO, I-10025 PINO TORINESE, ITALY. UNIV PADUA, I-35131 PADUA, ITALY. EUROPEAN SPACE AGCY, EUROPEAN SPACE RES & TECHNOL CTR, DEPT SPACE SCI, NL-2200 AG NOORDWIJK, NETHERLANDS. OSSERV ASTROFIS CATANIA, I-95125 CATANIA, ITALY. UNIV CALIF BERKELEY, SPACE SCI LAB, BERKELEY, CA 94720 USA. OSSERV ASTROFIS ARCETRI, I-50125 FLORENCE, ITALY. UNIV TURIN, I-10125 TURIN, ITALY. INST ASTROPHYS SPATIALE, F-91405 ORSAY, FRANCE. OSSERV ASTRON PALERMO, PALERMO, ITALY. RP Kohl, JH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Romoli, Marco/H-6859-2012; Naletto, Giampiero/S-6329-2016; OI Naletto, Giampiero/0000-0003-2007-3138; Giordano, Silvio/0000-0002-3468-8566; Benna, Carlo/0000-0003-1688-2434; Ciaravella, Angela/0000-0002-3127-8078; Spadaro, Daniele/0000-0003-3517-8688; pernechele, claudio/0000-0002-7752-6268 NR 16 TC 25 Z9 25 U1 0 U2 2 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0273-1177 BN 0-08-043296-4 J9 ADV SPACE RES-SERIES PY 1997 VL 20 IS 1 BP 3 EP 14 DI 10.1016/S0273-1177(97)00472-9 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BJ54C UT WOS:A1997BJ54C00001 ER PT J AU Roubik, DW Segura, JAL DeCamargo, JMF AF Roubik, DW Segura, JAL DeCamargo, JMF TI New stingless bee genus endemic to Central American cloudforests: Phylogenetic and biogeographic implications (Hymenoptera: Apidae: Meliponini) SO SYSTEMATIC ENTOMOLOGY LA English DT Article AB Meliwillea bivea gen.n., sp.n. is the only known stingless bee genus endemic to Central America. External morphology and male genitalia show affinity of Meliwillea with Scaptotrigona. Its plesiomorphies and current sympatry with Scaptotrigona suggest Meliwillea is relictual and diverged in montane habitat during the Tertiary, predating the Pleistocene connection between Central and South America which allowed immigration by Scaptotrigona. Addition of Meliwillea to the list of Neotropical genera changes the phylogenetic position of Nannotrigona, making it sister to Paratrigona instead of Scaptotrigona. C1 UNIV COSTA RICA,ESCUELA BIOL,SAN JOSE,COSTA RICA. UNIV SAO PAULO,FAC FILOSOFIA CIENCIAS & LETRAS,DEPT BIOL,BR-05508 SAO PAULO,BRAZIL. RP Roubik, DW (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 35 TC 18 Z9 19 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0307-6970 J9 SYST ENTOMOL JI Syst. Entomol. PD JAN PY 1997 VL 22 IS 1 BP 67 EP 80 DI 10.1046/j.1365-3113.1997.d01-19.x PG 14 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA WP472 UT WOS:A1997WP47200003 ER PT S AU DiStefano, R Nelson, LA Lee, W Wood, TH Rappaport, S AF DiStefano, R Nelson, LA Lee, W Wood, TH Rappaport, S BE RuizLapuente, P Canal, R Isern, J TI Luminous supersoft X-ray sources as Type Ia progenitors SO THERMONUCLEAR SUPERNOVAE SE NATO ADVANCED SCIENCE INSTITUTES SERIES, SERIES C, MATHEMATICAL AND PHYSICAL SCIENCES LA English DT Proceedings Paper CT NATO Advanced Study Institute on Thermonuclear Supernovae CY JUN 20-30, 1995 CL PARADOR D'AIGUABLAVA, SPAIN SP NATO, Sci Affairs Div AB Accreting white dwarfs have long been considered as candidates for Type Ia supernova progenitors. With the discovery of luminous supersoft X-ray sources (LSXSs), a new class of white dwarf accretor has been proposed as a candidate progenitor system. This class, close-binary supersoft sources (CBSSs) is studied here. We combine a population synthesis analysis with detailed evolutionary calculations for individual systems. We find that there are uncertainties related to the possibility that some of these systems may experience a common envelope phase. Systems that do experience a common envelope that is fatal to further hydrogen accretion, can be expected to then undergo either C-O/He core mergers, or else a subsequent epoch of helium accretion onto a C-O white dwarf. The evolutionary calculations are essential to a meaningful computation of the rate of possible Type Ia explosions, and to reliable estimates of the uncertainties. In addition, the evolutionary calculations allow us to compute the amount of matter ejected prior to the explosion, and the history of local ionization due to the source. Some secondary characteristics of the supernova can therefore be predicted. Further, the possible existence of a pre-supernova nebula may allow surveys for nebulae in distant galaxies to successfully identify some progenitors. RP DiStefano, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 5 Z9 5 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0258-2023 BN 0-7923-4359-X J9 NATO ADV SCI I C-MAT PY 1997 VL 486 BP 147 EP 166 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG83F UT WOS:A1997BG83F00010 ER PT S AU Hoflich, P Khokhlov, A Wheeler, JC Nomoto, K Thielemann, FK AF Hoflich, P Khokhlov, A Wheeler, JC Nomoto, K Thielemann, FK BE RuizLapuente, P Canal, R Isern, J TI Explosion models, light curves, spectra and H-O SO THERMONUCLEAR SUPERNOVAE SE NATO ADVANCED SCIENCE INSTITUTES SERIES, SERIES C, MATHEMATICAL AND PHYSICAL SCIENCES LA English DT Proceedings Paper CT NATO Advanced Study Institute on Thermonuclear Supernovae CY JUN 20-30, 1995 CL PARADOR D'AIGUABLAVA, SPAIN SP NATO, Sci Affairs Div AB From the spectra and light curves it is clear that SNIa events are thermonuclear explosions of white dwarfs. However, details of the explosion are highly under debate. Here, we present detailed models which are consistent with respect to the explosion mechanism, the optical and infrared light curves (LC), and the spectral evolution. This leaves the description of the burning front and the structure of the white dwarf as the only free parameters. The explosions are calculated using one-dimensional Lagrangian codes including nuclear networks. Subsequently, optical and IR-LCs are constructed. Detailed NLTE-spectra are computed for several instants of time using the density, chemical and luminosity structure resulting from the LCs. The general methods and critical tests are presented (sect. 2). Different models for the thermonuclear explosion are discussed including detonations, deflagrations, delayed detonations, pulsating delayed detonations (PDD) and helium detonations (sect.3). Comparisons between theoretical and observed LCs and spectra provide an insight into details of the explosion and nature of the progenitor stars (sect. 4 & 5). We try to answer several related questions. Are subluminous SNe Ia a group different from 'normal' SN Ia (sect. 5)? Can we understand observed properties of the LCs and spectra (sect. 4)? What do we learn about the progenitor evolution and its metallicity (sect. 3, Figs. 4,5)? Do successful SN Ia models depend on the type of the host galaxy (Table 2)? RP Hoflich, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 13 Z9 13 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0258-2023 BN 0-7923-4359-X J9 NATO ADV SCI I C-MAT PY 1997 VL 486 BP 659 EP 679 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG83F UT WOS:A1997BG83F00040 ER PT S AU Spurr, RJD AF Spurr, RJD GP ESA TI Development of a prototype algorithm for the operational retrieval of height-resolved products from GOME SO THIRD ERS SYMPOSIUM ON SPACE AT THE SERVICE OF OUR ENVIRONMENT, VOLS. II & III SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 3rd ERS Symposium on Space at the Service of Our Environment CY MAR 14-21, 1997 CL FLORENCE, ITALY SP European Space Agcy AB GOME Level 2 products of total ozone column amounts have been generated on a routine operational basis since July 1996. These and the Level 1 radiance products are the major outputs from the ERS-2 ground segment COME Data Processor (GDP) at DLR in Germany. Off-fine scientific work has already shown the feasibility of ozone profile retrieval from GOME. The present paper demonstrates how the retrievals can be performed in an operational context. Height-resolved retrieval is based on the optimal estimation technique; cloud-contaminated scenes are treated in an equivalent reflecting surface approximation. The prototype must be able to handle GOME measurements routinely on a global basis. Requirements for the major components of the algorithm are described in detail; this incorporates an overall strategy for operational height-resolved retrieval from GOME. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Spurr, RJD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-656-2 J9 ESA SP PUBL PY 1997 VL 414 BP 621 EP 628 PG 4 WC Geosciences, Multidisciplinary; Remote Sensing SC Geology; Remote Sensing GA BL05P UT WOS:000074128900007 ER PT S AU Chance, K AF Chance, K GP ESA TI Quantitative spectroscopy for the analysis of GOME data SO THIRD ERS SYMPOSIUM ON SPACE AT THE SERVICE OF OUR ENVIRONMENT, VOLS. II & III SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 3rd ERS Symposium on Space at the Service of Our Environment CY MAR 14-21, 1997 CL FLORENCE, ITALY SP European Space Agcy DE global ozone monitoring experiment; rayleigh scattering; ring effect; spectroscopy AB Accurate analysis of the GOME data to obtain atmospheric constituents requires reliable, traceable spectroscopic parameters for atmospheric absorption and scattering. Results are summarized here for research that includes: the re-determination of Rayleigh scattering cross sections and phase functions for the 200-1000 nm range; analysis of solar spectra to obtain a high-resolution reference spectrum with excellent absolute vacuum wavelength calibration; Ring effect cross sections and phase functions determined directly from accurate molecular parameters of N-2 and O-2; O-2 A band line intensities and pressure broadening coefficients; and analysis of absolute accuracies for ultraviolet and visible absorption cross sections of O-3 and other trace species measurable by GOME. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chance, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Chance, Kelly/0000-0002-7339-7577 NR 0 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-656-2 J9 ESA SP PUBL PY 1997 VL 414 BP 659 EP 661 PG 3 WC Geosciences, Multidisciplinary; Remote Sensing SC Geology; Remote Sensing GA BL05P UT WOS:000074128900013 ER PT B AU Latham, DW Mathieu, RD Milone, AAE AF Latham, DW Mathieu, RD Milone, AAE BE Leung, KC TI The spectroscopic binary population of M67 SO THIRD PACIFIC RIM CONFERENCE ON RECENT DEVELOPMENT ON BINARY STAR RESEARCH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd Pacific Rim Conference on Recent Development on Binary Star Research CY OCT 26-NOV 01, 1995 CL CHIANG MAI, THAILAND SP Chiang Mai Univ, Thai Astronom Soc, Univ Nebraska Lincoln, Natl Res Council Thailand, Think Earth Thailand, Trantraphun Dept Store, Thailand, Tra Co Ltd, Thailand AB We summarize the status of a long-term project to characterize the population of spectroscopic binaries among the giants and dwarfs in the old open cluster M67. As of June 1995 we had accumulated more than 5500 radial velocity observations of 406 proper-motion cluster members, had identified 96 spectroscopic binaries, and had derived 53 orbital solutions. For primary stars in the range 1.1 to 1.2 solar masses, we derive a frequency of 13.3% for binaries with periods in the range 1 to 1000 days. For short-period main sequence binaries, there is a clear transition from circular to eccentric orbits, with a period of P = 12.4 days for the last circular orbit. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-50-3 J9 ASTR SOC P PY 1997 VL 130 BP 113 EP 116 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80J UT WOS:000073445600021 ER PT B AU Latham, DW Torres, G Metcalfe, TS Mathieu, RD AF Latham, DW Torres, G Metcalfe, TS Mathieu, RD BE Leung, KC TI CM Draconis and the primordial helium abundance SO THIRD PACIFIC RIM CONFERENCE ON RECENT DEVELOPMENT ON BINARY STAR RESEARCH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd Pacific Rim Conference on Recent Development on Binary Star Research CY OCT 26-NOV 01, 1995 CL CHIANG MAI, THAILAND SP Chiang Mai Univ, Thai Astronom Soc, Univ Nebraska Lincoln, Natl Res Council Thailand, Think Earth Thailand, Trantraphun Dept Store, Thailand, Tra Co Ltd, Thailand AB CM Draconis is the least massive main-sequence eclipsing double-lined spectroscopic binary currently known. We present a new double-lined orbital solution based on 233 echelle spectra obtained with the CfA Digital Speedometers over the past decade. Radial velocities for both components were determined using TODCOR, a two-dimensional correlation technique. We derive individual masses of M-A = 0.2307 +/- 0.0010 and M-B = 0.2136 +/- 0.0010 solar masses, and a mass ratio of q = 0.9260 +/- 0.0026. Following the analysis of Paczynski and Sienkiewicz (1984) we derive bulk helium abundances for the two components of Y-A = 0.32 and Y-B = 0.31. The uncertainty in the absolute value of these helium abundances is +/- 0.04, with the uncertainty in the parallax and the individual radii making the largest contributions. CM Draconis appears to be a member of Population II. Thus, there is some promise that it may be able to provide a useful test of the primordial helium abundance. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-50-3 J9 ASTR SOC P PY 1997 VL 130 BP 147 EP 151 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK80J UT WOS:000073445600029 ER PT J AU Jennions, MD AF Jennions, MD TI Stability in coral communities: A natural experiment SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Editorial Material ID DIVERSITY; DYNAMICS RP Jennions, MD (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 12 TC 9 Z9 9 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD JAN PY 1997 VL 12 IS 1 BP 3 EP 4 DI 10.1016/S0169-5347(96)30059-1 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA WB577 UT WOS:A1997WB57700002 PM 21237950 ER PT B AU Weekes, TC AF Weekes, TC BE Giovannelli, F Mannocchi, G TI TeV gamma rays from galactic sources SO VULCANO WORKSHOP 1996 - FRONTIER OBJECTS IN ASTROPHYSICS AND PARTICLE PHYSICS SE ITALIAN PHYSICAL SOCIETY CONFERENCE PROCEEDINGS (IPS) LA English DT Proceedings Paper CT Vulcano Workshop 1996 on Frontier Objects in Astrophysics and Particle Physics CY MAY 27-JUN 01, 1996 CL VULCANO, ITALY SP CNR, Ist Astrofis Spaziale, Frascati, Italy, CNR, Ist Cosmogeofis, Torino, Italy, Ist Nazl Fis Nucl, Frascati, Italy AB The status of the atmospheric Cerenkov imaging technique as it applies to gamma-ray astronomy above 200 GeV is reviewed. The technique has been successful in identifying signals from three plerions; these successes increase the interest in observing shell supernova remnants, the galactic plane and unidentified EGRET sources. The present status of TeV gamma-ray burst observations is discussed. RP Weekes, TC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,POB 97,AMADO,AZ 85645, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU EDITRICE COMPOSITORI PI BOLOGNA PA VIA STALINGRADO 97/2, 40128 BOLOGNA, ITALY BN 88-7794-096-4 J9 ITAL PHY SO PY 1997 VL 57 BP 231 EP 245 PG 15 WC Astronomy & Astrophysics; Physics, Condensed Matter SC Astronomy & Astrophysics; Physics GA BH93M UT WOS:A1997BH93M00019 ER PT B AU Kurtz, MJ AF Kurtz, MJ BE Kontizas, E Kontizas, M Morgan, DH Vettolani, GP TI Conquering ignorance: Data, information and knowledge SO WIDE-FIELD SPECTROSCOPY SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT 2nd Conference of the Working Group of IAU Commission 9 on Wide-Field Imaging CY MAY 20-25, 1996 CL ATHENS, GREECE SP Int Astron Union, Working Grp Commiss 8Greek Gen Secretariat Res & Technol, Natl Observ Athens, Observ Astron Trieste, Univ Athens, Athens Inst Italiano Cultura, French Embassy, Natl Mortgage Bank Greece RP Kurtz, MJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-4518-5 J9 ASTROPHYS SPACE SC L PY 1997 VL 212 BP R23 EP R25 PG 3 WC Astronomy & Astrophysics; Spectroscopy SC Astronomy & Astrophysics; Spectroscopy GA BJ07D UT WOS:A1997BJ07D00001 ER PT B AU Schlegel, EM AF Schlegel, EM BE Howell, S Kuulkers, E Woodward, C TI Proposing for AXAF for CVs SO WILD STARS IN THE OLD WEST: PROCEEDINGS OF THE 13TH NORTH AMERICAN WORKSHOP ON CATACLYSMIC VARIABLES AND RELATED OBJECTS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Wild Stars in the Old West - 13th North American Workshop on Cataclysmic Variables and Related Objects CY JUN 14-19, 1997 CL GRAND TETON NATL PARK, WY SP Univ Wyoming, Off Res, Univ Wyoming, Dept Phys & Astron, Astronom Soc Pacific C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Schlegel, EM (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-57-0 J9 ASTR SOC P PY 1997 VL 137 BP 467 EP 468 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74M UT WOS:000076533800069 ER PT B AU Garcia, MR McClintock, JE Narayan, R Callanan, PJ AF Garcia, MR McClintock, JE Narayan, R Callanan, PJ BE Howell, S Kuulkers, E Woodward, C TI Black hole event horizons and x-ray nova luminosities - Update SO WILD STARS IN THE OLD WEST: PROCEEDINGS OF THE 13TH NORTH AMERICAN WORKSHOP ON CATACLYSMIC VARIABLES AND RELATED OBJECTS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Wild Stars in the Old West - 13th North American Workshop on Cataclysmic Variables and Related Objects CY JUN 14-19, 1997 CL GRAND TETON NATL PARK, WY SP Univ Wyoming, Off Res, Univ Wyoming, Dept Phys & Astron, Astronom Soc Pacific C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Garcia, MR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-57-0 J9 ASTR SOC P PY 1997 VL 137 BP 506 EP 508 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74M UT WOS:000076533800089 ER PT J AU Viola, HJ AF Viola, HJ TI Undaunted courage: Meriwether Lewis, Thomas Jefferson, and the opening of the American West - Ambrose,SE SO WILLIAM AND MARY QUARTERLY LA English DT Book Review RP Viola, HJ (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU INST EARLY AMER HIST CULT PI WILLIAMSBURG PA BOX 220, WILLIAMSBURG, VA 23187 SN 0043-5597 J9 WILLIAM MARY QUART JI William Mary Q. PD JAN PY 1997 VL 54 IS 1 BP 273 EP 274 DI 10.2307/2953325 PG 2 WC History SC History GA WE297 UT WOS:A1997WE29700021 ER PT J AU Larco, L AF Larco, L TI Encounters with the Huacas: Ritual dialogue, music and healing in Northern Peru SO WORLD OF MUSIC LA English DT Article C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Larco, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 15 TC 3 Z9 3 U1 0 U2 0 PU FLORIAN NOETZEL VERLAG PI WILHELSMHAVEN PA HEINRICHSHOFEN BOOKS WORLD OF MUSIC POB 580, D-26353 WILHELSMHAVEN, GERMANY SN 0043-8774 J9 WORLD MUSIC JI World Music PY 1997 VL 39 IS 1 BP 35 EP 59 PG 25 WC Music SC Music GA YG310 UT WOS:000060461500003 ER PT J AU Seeger, A AF Seeger, A TI Music of the Warao of Venezuela, song people of the rain forest SO YEARBOOK FOR TRADITIONAL MUSIC LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Seeger, A (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU INT COUNCIL TRADITIONAL MUSIC PI NEW YORK PA COLUMBIA UNIV, DEPT MUSIC-MC 1815, 2960 BROADWAY, NEW YORK, NY 10027 USA SN 0740-1558 J9 YEARB TRADIT MUSIC JI Yearb. Tradit. Mus. PY 1997 VL 29 BP 160 EP 161 DI 10.2307/768309 PG 2 WC Music SC Music GA 154TK UT WOS:000077904800017 ER PT J AU Brown, JL Wasser, SK Wildt, DE Graham, LH Monfort, SL AF Brown, JL Wasser, SK Wildt, DE Graham, LH Monfort, SL TI Faecal steroid analysis for monitoring ovarian and testicular function in diverse mild carnivore, primate and ungulate species SO ZEITSCHRIFT FUR SAUGETIERKUNDE-INTERNATIONAL JOURNAL OF MAMMALIAN BIOLOGY LA English DT Article; Proceedings Paper CT 1st International Symposium on Physiology and Ethology of Wild and Zoo Animals CY 1996 CL BERLIN, GERMANY SP Deut Gesell Saugetierkunde, European Assoc Zoos & Aquaria, German Mammal Soc ID FECAL STEROIDS; ESTROUS-CYCLE; PROGESTERONE; EXCRETION; ESTRADIOL; FECES AB Faecal steroid metabolite monitoring has become a well-established tool for evaluating reproductive activity in diverse mammalian species. We have used this non-invasive technique systematically for developing longitudinal reproductive databases that have been useful for augmenting captive management and propagation of wildlife species. We rely upon a simple faecal steroid extraction technique that is both efficient and adaptable across taxa. Faecal oestradiol and progestogen (female) or androgen (male) metabolites are quantified in extracts using validated radioimmunoassays that have proven useful in a diversity of species. This paper presents examples from the more than 30 mammalian species that we have studied to date, illustrating a broad spectrum of uses for non-invasive faecal steroid monitoring. Data are presented on: 1) oestrous cyclicity (Alaskan moose, black rhinoceros, scimitar-horned oryx, African wild dog, sun bear, sloth bear, African elephant); 2) seasonality (black-footed ferret, black rhinoceros, sable antelope, yellow baboon, sun bear, scimitar-horned oryx); 3) pregnancy (black-footed ferret, maned wolf Alaskan moose, black rhinoceros, sun bear, sloth bear); and 4) evaluation of hormonal protocols (i.e., oestrous synchronization, ovulation induction) used with assisted reproductive techniques (scimitar-horned oryx). The non-invasive feature of faecal hormone monitoring, the ease of sample collection and the demonstration that excretion patterns reflect physiological function provide evidence for the enormous utility of this technique. Undoubtedly, a major benefit of this approach will be vastly improved basic knowledge that can be used to improve management strategies. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Ctr Wildlife Conservat, Seattle, WA 98103 USA. RP Brown, JL (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 15 TC 16 Z9 17 U1 0 U2 17 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0044-3468 J9 Z SAUGETIERKD JI Z. Saugetierkd.-Int. J. Mamm. Biol. PY 1997 VL 62 SU 2 BP 27 EP 31 PG 5 WC Zoology SC Zoology GA YQ997 UT WOS:000071446200006 ER PT J AU Graham, LH Brown, JL AF Graham, LH Brown, JL TI Non-invasive assessment of gonadal and adrenocortical function in felid species via faecal steroid analysis SO ZEITSCHRIFT FUR SAUGETIERKUNDE-INTERNATIONAL JOURNAL OF MAMMALIAN BIOLOGY LA English DT Article; Proceedings Paper CT 1st International Symposium on Physiology and Ethology of Wild and Zoo Animals CY 1996 CL BERLIN, GERMANY SP Deut Gesell Saugetierkunde, European Assoc Zoos & Aquaria, German Mammal Soc ID DOMESTIC CAT; METABOLISM; ESTRADIOL; FECES AB Radiolabeled oestradiol, progesterone, testosterone and cortisol were injected into domestic cats in separate trials to determine the primary route of steroid metabolite excretion, Greater than 80% of the metabolites for all steroids were excreted via the faeces 24 to 48 hr after injection. Steroid metabolites were extracted from faeces by boiling in 90% aqueous ethanol. Radioimmunoassays (RIA) for faecal oestradiol, progestogen, androgen and cortisol metabolites were validated for several felid species. Faecal oestradiol metabolites increased significantly above baseline during periods of observed oestrus or after exogenous equine chorionic gonadotropin administration, although mean baseline and peak concentrations varied considerably among species. Seasonal effects on faecal oestradiol metabolites were observed in several species including the clouded leopard and Pallas' cat. In general, faecal progestogen metabolites increased only after breeding or exogenous human chorionic gonadotropin administration. Although data suggest that most felids are primarily induced ovulators, occasional spontaneous ovulations were not uncommon in some species (e.g., clouded leopard). Increased faecal progestogen metabolites after non-fertile mating (i.e., non-pregnant luteal phase) lasted from 1/3 to 2/3 of the gestation length. Faecal androgen metabolite concentrations averaged similar to 400 ng/g dry faeces in intact domestic cat males while concentrations in castrate males, intact females and castrate females were nondetectable, suggesting that the quantified androgen metabolites were of testicular origin. There was a significant seasonal effect on faecal androgen metabolite excretion in male Pallas' cats with baseline concentrations observed during the summer months and elevated concentrations occurring from the end of September through April. The physiological relevance of immunoreactive faecal cortisol metabolites was determined in the domestic cat by an adrenocorticotropic hormone challenge. The resulting increased serum cortisol concentrations were followed by an increase in faecal cortisol metabolite excretion 24 to 48 hr later. In summary, faecal steroid metabolites are quantifiable by RIA and allow the non-invasive monitoring of gonadal and adrenal function in domestic and non-domestic felid species. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Brown, JL (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 14 TC 9 Z9 9 U1 2 U2 6 PU GUSTAV FISCHER VERLAG PI JENA PA VILLENGANG 2, D-07745 JENA, GERMANY SN 0044-3468 J9 Z SAUGETIERKD JI Z. Saugetierkd.-Int. J. Mamm. Biol. PY 1997 VL 62 SU 2 BP 78 EP 82 PG 5 WC Zoology SC Zoology GA YQ997 UT WOS:000071446200016 ER PT J AU Wemmer, C Rodden, M Pickett, C AF Wemmer, C Rodden, M Pickett, C TI Publication trends in zoo biology: A brief analysis of the first 15 years SO ZOO BIOLOGY LA English DT Editorial Material DE publication; research; zoos; aquariums AB Zoo Biology has completed 15 years as a professional journal dedicated to exsitu wildlife research. To assess the journal's representation of zoo and aquarium research, we examined some aspects of its publication record, based on analyses of 395 research articles. The taxonomic representation of Zoo Biology is heavily skewed toward research articles on mammals (73%), with articles on birds, reptiles, and invertebrates contributing only 10%, 7%, and 7%, respectively. Behavior and reproduction (sensu latu) are the predominating disciplinary themes of research, with heavy reliance on non-invasive endocrine methodology using RIA and EIA. The relatively small number of articles dealing with demography and genetics is surprising when one considers the eminent role such analyses have played in Species Survival Plans. Most contributions are multi-authored and arise from U.S. institutions, with collaborative ventures between toes and universities accounting for 26% of all articles. The academic community, however, contributed nearly one third of Zoo Biology's articles as non-collaborative contributions. University and aquarium affiliations are known to exist, but the products of such cooperation are not appearing in the pages of Zoo Biology. We conclude the taxonomic trends reflect a shortage of research-oriented staff in the zoo and aquarium profession, and a tendency for a significant number of zoo biologists to publish in taxon-oriented journals. (C) 1997 Wiley-Liss, Inc. RP Wemmer, C (reprint author), NATL ZOOL PK,CONSERVAT & RES CTR,1500 REMOUNT RD,FRONT ROYAL,VA 22630, USA. NR 5 TC 7 Z9 8 U1 1 U2 2 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1997 VL 16 IS 1 BP 3 EP 8 PG 6 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA WK636 UT WOS:A1997WK63600002 ER PT J AU Power, ML Oftedal, OT Savage, A Blumer, ES Soto, LH Chen, TC Holick, MF AF Power, ML Oftedal, OT Savage, A Blumer, ES Soto, LH Chen, TC Holick, MF TI Assessing vitamin D status of callitrichids: Baseline data from wild cotton-top tamarins (Saguinus oedipus) in Colombia SO ZOO BIOLOGY LA English DT Article DE cholecalciferol; nutrition; bone ID METABOLISM; PRIMATES; MARMOSET AB Bone disease related to vitamin D deficiency is an insidious problem in captive colonies of callitrichids. Currently a diagnosis of vitamin D deficiency may be made after the appearance of clinical pathology, usually bone deformities or fractures. The development of assays for vitamin D metabolites suggests it may be possible to detect incipient vitamin D deficiency before animals are adversely affected. However, there are few data on normative levels of these metabolites in any nonhuman primates. We collected blood samples from 18 wild cotton-top tamarins (Saguinus oedipus) from Colombia and assayed them for 25-hydroxy vitamin D(25-OH-D), the major circulating form of the vitamin, which is believed to be a good indicator of status. Serum concentrations of 25-OH-D averaged 76.4 ng/ml (range 25.5-120 ng/ml). This is high compared with human norms (10-55 ng/ml), but the range is lower than that reported in the literature for captive callitrichids. Juveniles had higher serum concentrations than did adults, and pregnant females had lower concentrations than did nonpregnant females. These data confirm that healthy callitrichids have higher circulating levels of 25-OH-D than do humans, but they suggest that the extremely high levels found in some captive animals (300-600 ng/ml) may be above normal. We propose that serum concentrations of 25-OH-D of 50-120 ng/ml can be considered normal for cotton-top tamarins and perhaps other callitrichids. If serum values much below 50 ng/ml are found during clinical evaluation, the possibility of incipient vitamin D deficiency should be considered. (C) 1997 Wiley-Liss, Inc. C1 ROGER WILLIAMS PK ZOO,PROVIDENCE,RI. INDERENA,COLOSO,COLOMBIA. BOSTON UNIV,SCH MED,VITAMIN D BONE & SKIN LAB,BOSTON,MA 02118. RP Power, ML (reprint author), SMITHSONIAN INST,NATL ZOOL PK,NUTR LAB,WASHINGTON,DC 20008, USA. NR 23 TC 13 Z9 13 U1 1 U2 7 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1997 VL 16 IS 1 BP 39 EP 46 PG 8 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA WK636 UT WOS:A1997WK63600006 ER PT J AU Oftedal, OT Chen, TC Schulkin, J AF Oftedal, OT Chen, TC Schulkin, J TI Preliminary observations on the relationship of calcium ingestion to vitamin D status in the green iguana (Iguana iguana) SO ZOO BIOLOGY LA English DT Article DE food selection; minerals; vitamin D deficiency; reptiles ID FEMALE RATS AB We hypothesized that vitamin D-deficient green iguanas with depleted calcium stores would seek to augment calcium intake by self-selection of a high calcium source. Eight green iguanas were offered free-choice ground oystershell in addition to their regular diet. Of these, two had not been exposed to ultraviolet (UV-B) radiation for >5 years and were demonstrated to be vitamin D-deficient by low circulating levels of the principal vitamin D metabolite, calcidiol (25-hydroxy-cholecalciferol). The six others had been exposed to a UV-B emitting bulb for the previous 3 years and had high circulating calcidiol levels. Average daily food intake (expressed as dry matter per kg body mass) did not differ between the Low-D and High-D iguanas. The daily oystershell intake of the Low-D iguanas (0.02-0.03 g/kg) was lower than that of the High-D iguanas (0.06-0.70 g/kg), leading to a significant difference in calcium intake. The failure of iguanas to increase calcium intake in response to vitamin D-deficiency was puzzling and suggests that vitamin D, as a steroid hormone, may play some role in the expression of calcium appetite. (C) 1997 Wiley-Liss, Inc. C1 GEORGETOWN UNIV,DEPT PHYSIOL & BIOPHYS,WASHINGTON,DC. BOSTON UNIV,SCH MED,VITAMIN D LAB,BOSTON,MA 02118. RP Oftedal, OT (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. NR 26 TC 7 Z9 7 U1 1 U2 3 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1997 VL 16 IS 3 BP 201 EP 207 DI 10.1002/(SICI)1098-2361(1997)16:3<201::AID-ZOO1>3.0.CO;2-E PG 7 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA WY302 UT WOS:A1997WY30200001 ER PT J AU Sukumar, R Krishnamurthy, V Wemmer, C Rodden, M AF Sukumar, R Krishnamurthy, V Wemmer, C Rodden, M TI Demography of captive Asian elephants (Elephas maximus) in Southern India SO ZOO BIOLOGY LA English DT Article DE Asian elephants; captive elephants; demography; reproduction; Southern India ID SEX-RATIOS; MULE DEER AB Historically, the Asian elephant has never bred well in captivity. We have carried out demographic analyses of elephants captured in the wild or born in captivity and kept in forest timber camps in southern India during the past century. The average fecundity during this period was 0.095/adult female/year. During 1969-89, however, the fecundity was higher at 0.155/adult female/year, which compares favorably with wild populations. There was a seasonality in births with a peak in January. The sex ratio of 129 male to 109 female calves at birth is not significantly different from equality, although the excess of male calves born mainly to mothers 20-40 years old may have biological significance. Mortality rates were higher in females than in males up to age 10, but much lower in females than in males above age 10 years. The population growth rate, based on the lower fecundity over the century, was 0.5% per year, and based on the higher fecundity during 1969-89, was 1.8% per year. The analyses thus showed that timber camp elephants in southern India could potentially maintain a stationary or increasing population without resorting to captures from the wild. Breeding efforts for elephants in toes can thus profitably learn from the experience of traditional management systems in parts of Asia. (C) 1997 Wiley-Liss, Inc. C1 INDIAN INST SCI,ASIAN ELEPHANT CONSERVAT CTR,BANGALORE 560012,KARNATAKA,INDIA. NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA. RP Sukumar, R (reprint author), INDIAN INST SCI,CTR ECOL SCI,BANGALORE 560012,KARNATAKA,INDIA. RI Raman, Sukumar/C-9809-2013 NR 20 TC 28 Z9 30 U1 3 U2 11 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1997 VL 16 IS 3 BP 263 EP 272 DI 10.1002/(SICI)1098-2361(1997)16:3<263::AID-ZOO6>3.0.CO;2-8 PG 10 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA WY302 UT WOS:A1997WY30200006 ER PT J AU Montgomery, ME Ballou, JD Nurthen, RK England, PR Briscoe, DA Frankham, R AF Montgomery, ME Ballou, JD Nurthen, RK England, PR Briscoe, DA Frankham, R TI Minimizing kinship in captive breeding programs SO ZOO BIOLOGY LA English DT Article DE inbreeding; genetic diversity; heterozygosity; reproductive fitness; mean kinship ID CONSERVATION GENETICS; DROSOPHILA-MELANOGASTER; MODELING PROBLEMS; SPECIES SURVIVAL; POPULATIONS; CONSEQUENCES; FITNESS; SIZES AB Captive populations of endangered species are managed to preserve genetic diversity and retain reproductive fitness. Minimizing kinship (MK) has been predicted to maximize the retention of gene diversity in pedigreed populations with unequal founder representation. MK was compared with maximum avoidance of inbreeding (MAI) and random choice of parents (RAND) using Drosophila melanogaster. Forty replicate populations of each treatment were initiated with unequal founder representation and managed for four generations. MK retained significantly more gene diversity and allelic diversity based on six microsatellite loci and seven allozyme loci than MAI or RAND. Reproductive fitness under both benign and competitive conditions did not differ significantly among treatments. Of the methods considered, MK is currently the best available for the genetic management of captive populations. (C) 1997 Wiley-Liss, Inc. C1 MACQUARIE UNIV,SCH BIOL SCI,KEY CTR BIODIVERS & BIORESOURCES,SYDNEY,NSW 2109,AUSTRALIA. SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. NR 37 TC 72 Z9 76 U1 1 U2 38 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1997 VL 16 IS 5 BP 377 EP 389 DI 10.1002/(SICI)1098-2361(1997)16:5<377::AID-ZOO1>3.0.CO;2-7 PG 13 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA XZ023 UT WOS:A1997XZ02300001 ER PT J AU Monfort, SL Wasser, SK Mashburn, KL Burke, M Brewer, BA Creel, SR AF Monfort, SL Wasser, SK Mashburn, KL Burke, M Brewer, BA Creel, SR TI Steroid metabolism and validation of noninvasive endocrine monitoring in the African wild dog (Lycaon pictus) SO ZOO BIOLOGY LA English DT Article DE fecal steroids; urinary steroids; estrogens; progesterone metabolites; testosterone; hormones ID OVARIAN-FUNCTION; REPRODUCTIVE FUNCTION; LUTEINIZING-HORMONE; SEXUAL-BEHAVIOR; FECAL STEROIDS; ESTROUS-CYCLE; PROGESTERONE; SERUM; BITCH; URINARY AB The purpose of this study was to validate noninvasive endocrine monitoring techniques for African wild dogs (Lycaon pictus) and to establish physiological validity of these methods by evaluating longitudinal reproductive-endocrine profiles in captive individuals. To determine the primary excretory by-products of ovarian steroid metabolism, [C-14]-progesterone and [H-3]-estradiol were co-administered to a female and all excreta were collected for 80 hr postinjection. Radiolabel excretion peaked less than or equal to 18 hr postinfusion, and progesterone and estradiol metabolites were excreted in almost equivalent proportions in urine (39.7 and 41.1%, respectively) and feces (60.3 and 58.9%, respectively). Most of the urinary metabolites were conjugated (estradiol, 94.3 +/- 0.3%; progesterone, 90.4 +/- 0.5%), so that immunoassays for pregnanediol-3 alpha-glucuronide (PdG) and estrogen conjugates (EC) were effective for assessing steroid metabolites. Two immunoreactive estrogens (estradiol and estrone) and at least one immunoreactive progesterone metabolite (3 alpha-hydroxy-5 alpha, pregnan-20-one) were detected in feces. Urine and fecal samples were collected (1-3 times per week) for 1.5 yr from one adult female and two adult males to assess longitudinal steroid metabolite excretion. Overall correlation of urinary PdG to matched, same-day fecal progesterone metabolites immunoreactivity was 0.38 (n = 71, P < 0.05). Similarly, urinary EC was correlated (P < 0.05) with same-day fecal estrogen immunoreactivity (r = 0.49, n = 71). During pregnancy and nonpregnant cycles, copulation occurred at the time of peak (or declining) estrogen metabolites and increasing progesterone metabolites concentrations. Estrus duration was 6-9 days and gestation lasted 69 days with parturition occurring coincident with a drop in progesterone metabolites. Males exhibited seasonal trends in fecal testosterone excretion with maximal concentrations from July to September coincident with peak mating activity. Although these limited longitudinal hormone profiles should be interpreted cautiously, noninvasive gonadal steroid monitoring suggests that: ii) both female and male wild dogs may exhibit reproductive seasonality in North America, (7) females are monoestrous, and (3) peak testicular activity occurs between August and October coincident with mating behavior. From a conversation perspective, noninvasive endocrine monitoring techniques should be useful for augmenting captive breeding programs, as well as for developing an improved understanding of the physiological mechanisms underlying reproductive suppression in response to social and ecological pressures. (C) 1997 Wiley-Liss, Inc. C1 CTR WILDLIFE CONSERVAT,SEATTLE,WA. UNIV WASHINGTON,SCH MED,SEATTLE,WA. CHICAGO ZOOL SOC,BROOKFIELD ZOO,BROOKFIELD,IL. ROCKEFELLER UNIV,FIELD RES CTR ECOL & ETHOL,MILLBROOK,NY. RP Monfort, SL (reprint author), SMITHSONIAN INST,CONSERVAT & RES CTR,1500 REMONT RD,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. NR 42 TC 52 Z9 56 U1 0 U2 11 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1997 VL 16 IS 6 BP 533 EP 548 DI 10.1002/(SICI)1098-2361(1997)16:6<533::AID-ZOO6>3.0.CO;2-B PG 16 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA YJ320 UT WOS:A1997YJ32000006 ER PT J AU DeQueiroz, K AF DeQueiroz, K TI Misunderstandings about the phylogenetic approach to biological nomenclature: A reply to Liden and Oxelman SO ZOOLOGICA SCRIPTA LA English DT Editorial Material ID TAXON NAMES; DEFINITIONS; STABILITY; MAMMALIA RP DeQueiroz, K (reprint author), SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT VERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. NR 27 TC 20 Z9 20 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD JAN PY 1997 VL 26 IS 1 BP 67 EP 70 PG 4 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA YF691 UT WOS:A1997YF69100006 ER PT J AU Stanley, DJ Warne, AG Dunbar, JB AF Stanley, DJ Warne, AG Dunbar, JB TI Eastern Mississippi delta: Late Wisconsin unconformity, overlying transgressive facies, sea level and subsidence SO ENGINEERING GEOLOGY LA English DT Article; Proceedings Paper CT Conference on Geology in the Lower Mississippi Valley - Implications for Engineering, the Half Century Since Fisk 1944 CY DEC 05-08, 1994 CL VICKSBURG, MS ID NILE DELTA; STRATIGRAPHY; SYSTEMS; PLAIN; MODEL; RISE AB Analysis of 92 engineering core logs located in the Balize sector of the eastern Mississippi delta focuses on the late Wisconsin unconformity and lithofacies of strata lying immediately below and above this stratigraphic horizon. This major sequence boundary is a key feature used to correlate strata across shelf and slope to the basin. Observations emphasize lithofacies distributions of the latest Pleistocene sediments underlying the unconformity, the late Pleistocene to early Holocene transgressive facies, and the immediately overlying deltaic deposits. Maps and a cross-section compiled with this information highlight the critical relation between lithofacies distributions and late Wisconsin sealevel oscillations. Core analysis reveals that the transgressive facies comprises distinct environments of deposition, offshore to onshore. Findings identify criteria to determine the approximate position of the shoreline at the late Wisconsin maximum sea-level lowstand and at the extent of early Holocene maximum marine inundation in the Balize complex. Mapping of lithologies along the late Wisconsin unconformity serves to improve correlation of sediment facies with changes in acoustic response along high-resolution seismic profiles. An estimate of long-term averaged land subsidence suggests lowering of at least 1 mm/year near the shelfedge during the past similar to 18 000 years. This mapping also refines sea-level response models for the Mississippi delta, including criteria to locate key paleogeographic features such as shelfedges and maximum flooding surfaces in other Recent marine deltas and in older, stacked deltaic sequences. RP Stanley, DJ (reprint author), SMITHSONIAN INST,NMNH,DELTAS GLOBAL CHANGE PROGRAM,WASHINGTON,DC 20560, USA. NR 58 TC 14 Z9 17 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0013-7952 J9 ENG GEOL JI Eng. Geol. PD DEC 30 PY 1996 VL 45 IS 1-4 BP 359 EP 381 DI 10.1016/S0013-7952(96)00022-1 PG 23 WC Engineering, Geological; Geosciences, Multidisciplinary SC Engineering; Geology GA WE891 UT WOS:A1996WE89100020 ER PT J AU Klassen, GJ AF Klassen, GJ TI Fusion complex of abdominal vertebrae 1-5 in boxfishes (Tetraodontiformes: ostraciidae): Reinterpreting character evolution SO COPEIA LA English DT Article AB Early workers consistently underestimated the number of vertebrae present in Ostraciidae, counting a fusion complex associated with the anterior portion of the vertebral column as the first vertebra, Tyler considered this complex to be reduced by progressive fusion, with these characters forming a linear transformation series from fusion of the first two vertebrae (Aracaninae) to fusion of the first four vertebrae (Ostraciinae from the Indo-Pacific), culminating in the fusion of the first five vertebrae (Ostraciinae from the Atlantic), The present analysis, and some of Tyler's own observations, shed doubt on that interpretation, and indicate that the fusion series forms a ''character complex'' with the fusion of vertebrae 1 + 2 and 3 + 4 being synapomorphic for the Ostraciinae and that the fusion of vertebrae 2 + 3 in Lactoria and in Acanthostracion + Lacrophrys are two independent events. Recognition of ''complex characters'' based on a priori assumptions of progressive evolution can lead to erroneous interpretations of character evolution. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DIV FISHERIES,WASHINGTON,DC 20560. NR 18 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS BUSINESS OFFICE PI CARBONDALE PA SOUTHERN ILLINOIS UNIV, DEPT ZOOLOGY, CARBONDALE, IL 62901-6501 SN 0045-8511 J9 COPEIA JI Copeia PD DEC 27 PY 1996 IS 4 BP 859 EP 865 DI 10.2307/1447648 PG 7 WC Zoology SC Zoology GA WA683 UT WOS:A1996WA68300012 ER PT J AU Fredericq, S Hommersand, MH Freshwater, DW AF Fredericq, S Hommersand, MH Freshwater, DW TI The molecular systematics of some agar- and carrageenan-containing marine red algae based on rbcL sequence analysis (vol 326, pg 125, 1996) SO HYDROBIOLOGIA LA English DT Correction, Addition C1 DUKE UNIV,DEPT BOT,DURHAM,NC 27708. NATL MUSEUM NAT HIST,DEPT BOT,SMITHSONIAN INST,WASHINGTON,DC 20560. UNIV N CAROLINA,DEPT BIOL,CHAPEL HILL,NC 27599. MARINE SCI RES CTR,WILMINGTON,NC 28403. NR 1 TC 1 Z9 1 U1 1 U2 4 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD DEC 27 PY 1996 VL 341 IS 3 BP 251 EP 251 DI 10.1007/BF00014690 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA WT113 UT WOS:A1996WT11300006 ER PT J AU Sorenson, MD Fleischer, RC AF Sorenson, MD Fleischer, RC TI Multiple independent transpositions of mitochondrial DNA control region sequences to the nucleus SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID RIBOSOMAL-RNA; STRONGYLOCENTROTUS-PURPURATUS; D-LOOP; GENOME; EVOLUTION; GENE; PSEUDOGENES; VERTEBRATES; SUBUNIT; HUMANS AB Transpositions of mtDNA sequences to the nuclear genome have been documented in a wide variety of individual taxa, but little is known about their taxonomic frequency or patterns of variation, We provide evidence of nuclear sequences homologous to the mtDNA control region in seven species of diving ducks (tribe Aythyini). Phylogenetic analysis places each nuclear sequence as a close relative of the mtDNA haplotypes of the specie(s) in which it occurs, indicating that they derive from six independent transposition events, all occurring within the last approximate to 1.5 million years, Relative-rate tests and comparison of intraspecific variation in nuclear and mtDNA sequences confirm the expectation of a greatly reduced rate of evolution in the nuclear copies, By representing mtDNA haplotypes from ancestral populations, nuclear insertions may be valuable in some phylogenetic analyses, but they also confound the accurate determination of mtDNA sequences, In particular, our data suggest that the presumably nonfunctional but more slowly evolving nuclear sequences often will not be identifiable by changes incompatible with function and may be preferentially amplified by PCR primers based on mtDNA sequences from related taxa. C1 SMITHSONIAN INST,NATL ZOOL PK,MOL GENET LAB,WASHINGTON,DC 20008. RI Sorenson, Michael/D-8065-2011 OI Sorenson, Michael/0000-0001-5375-2917 NR 33 TC 185 Z9 191 U1 0 U2 3 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD DEC 24 PY 1996 VL 93 IS 26 BP 15239 EP 15243 DI 10.1073/pnas.93.26.15239 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA WC204 UT WOS:A1996WC20400046 PM 8986794 ER PT J AU Bayer, FM AF Bayer, FM TI The gorgonacean genus Arthrogorgia (Octocorallia: Primnoidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Operations by National Marine Fisheries vessels in Alaskan waters have collected specimens of two species of the gorgonacean genus Arthrogorgia Kukenthal, 1908, one of them undescribed. A. utinomii, new species, is described and compared with A. ijimai (Kinoshita 1907), the type species, as well as with A. otsukai Bayer, 1952, and A. kinoshitai Bayer, 1952. All species are illustrated by scanning electron micrographs (SEM). RP Bayer, FM (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 12 TC 2 Z9 5 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 23 PY 1996 VL 109 IS 4 BP 605 EP 628 PG 24 WC Biology SC Life Sciences & Biomedicine - Other Topics GA WA761 UT WOS:A1996WA76100001 ER PT J AU Pettibone, MH AF Pettibone, MH TI Revision of the scaleworm genera Acholoe Claparede, Arctonoella Buzhinskaja, and Intoshella Darboux (Polychaeta: Polynoidae) with the erection of the new subfamily Acholoinae SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Four genera and five species of polynoids are reviewed and revised, including Acholoe Claparede, 1870, for A. astericola (Delle Chiaje, 1841), commensal with asteroids; Arctonoella Buzhinskaja, 1964, for A. sinagawaensis (Izuka, 1912); new genus Paractonoella, for P. indica (Day, 1973). n. comb., and P. aphthalma (Gallardo, 1968), n. comb., with ophiuroid (both as Intoshella); and Intoshella Darboux, 1900, for I. euplectellae (McIntosh, 1885), with glass sponge. All species are referred to the new subfamily Acholoinae, characterized by arctonoid type of prostomium and biramous parapodia with neuropodia deeply notched dorsally and ventrally, shorter rounded post-setal lobes and longer presetal acicular lobes, bifid distally, with longer supraacicular processes. RP Pettibone, MH (reprint author), SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT INVERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. NR 36 TC 5 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 DEC 23 PY 1996 VL 109 IS 4 BP 629 EP 644 PG 16 WC Biology SC Life Sciences & Biomedicine - Other Topics GA WA761 UT WOS:A1996WA76100002 ER PT J AU Child, CA Segonzac, M AF Child, CA Segonzac, M TI Sericosura heteroscela and S-cyrtoma, new species, and other Pycnogonida from Atlantic and Pacific hydrothermal vents, with notes on habitat and environment SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The first new hydrothermal vent pycnogonid from the Mid-Atlantic Ridge, Sericosura heteroscela, new species, is described and illustrated from specimens taken in 1727 m south of the Azores and other nearby localities in similar depths from vent areas just west of the azores, Males of this new species have extremely dimorphic anterior and posterior propodi. Another new species, S. cyrtoma, is described and figured from a hydrothermal vent at 13 degrees N off the Pacific coast of Mexico, in 2563 m. A juvenile specimen of a possibly new third Sericosura species is discussed and compared with S. venticola Child. The specimen was taken from vents north of Easter island, southeast Pacific, in 2578 m. The three species are compared with each other and with other known hydrothermal vent species in this genus, their distribution is discussed, and a Sericosura key is presented. Two known species in the genera Callipallene and Colossendeis are also listed from the same Mid-Atlantic vent areas. Descriptive remarks on the habitat and environment of the specimens are presented. C1 IFREMER,CTR BREST,CENTOB,DRO,EP,LEA,F-29280 PLOUZANE,FRANCE. RP Child, CA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 25 TC 6 Z9 6 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 23 PY 1996 VL 109 IS 4 BP 664 EP 676 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA WA761 UT WOS:A1996WA76100005 ER PT J AU Child, CA AF Child, CA TI The Pycnogonida types of William A. Hilton .2. The remaining undescribed species SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The four remaining questionable species named by W. A. Hilton between 1939 and 1942 are described as if they were newly discovered, are illustrated where necessary, and compared with others described by Hilton and other authors of American west coast pycnogonids. The species are: Achelia simplissima, A. spinoseta, Ammothella setosa, and Tanystylum duospinum. The latter species is found to be the earliest valid name for several synonym species described later. Another little known species, Achelia harrietae Marcus, 1940, is illustrated and compared with A. spinoseta, a close relation. A complete list of the 66 Hilton species with original names, dates of publication, and current identifications are given. RP Child, CA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 37 TC 3 Z9 3 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 23 PY 1996 VL 109 IS 4 BP 677 EP 686 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA WA761 UT WOS:A1996WA76100006 ER PT J AU Graves, GR AF Graves, GR TI Diagnoses of hybrid hummingbirds (Aves: Trochilidae). 2. Hybrid origin of Eriocnemis soderstromi Butler SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID AVES AB Eriocnemis soderstromi (Butler 1926) is shown to be a hybrid between E. nigrivestis, an endemic of the Volcan Pichincha region in Ecuador, and E. luciani, an inhabitant of timberline Andean forest from southern Colombia to Bolivia. This is the first report of intrageneric hybridization among the nine species of Eriocnemis. Plumage characters of the hybrid appear to be a blended intermediate of those of the parental species. External measurements of the hybrid are intermediate of those of parental species. RP Graves, GR (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 17 TC 6 Z9 6 U1 0 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 23 PY 1996 VL 109 IS 4 BP 764 EP 769 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA WA761 UT WOS:A1996WA76100016 ER PT J AU Riess, AG Press, WH Kirshner, RP AF Riess, AG Press, WH Kirshner, RP TI Is the dust obscuring supernovae in distant galaxies the same as dust in the milky way? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, observations; distance scale; dust, extinction; galaxies, ISM; supernovae, general ID IA SUPERNOVAE; STANDARD CANDLES; EXTINCTION; MAGNITUDE; CLUSTERS AB Previous attempts to correct type Ia supernovae (SN Ia's) for host galaxy extinction have given strange results: increased dispersion on the Hubble diagram or impossibly low values of the reddening ratio for dust in distant galaxies. The cause is the incorrect assumption that SN Ia's have a uniform intrinsic luminosity and color at maximum light. Our multicolor light-curve shape (MLCS) method establishes the relation between intrinsic luminosity and color for SN Ia's using information in lightcurve shapes. Here we estimate the B-V, V-R, and V-I color excess for 20 SN Ids using MLCS and estimate the reddening ratios of dust in distant galaxies. The ratios of selective to total absorption from dust in distant galaxies hosting SN Ia's are consistent with the galactic extinction law. The SN Ia's in late-type galaxies are often obscured by dust, while those in early-type galaxies are dust free. This suggests that SN Ia extinction is caused by interstellar (not circumstellar) dust, with similar optical properties as the dust in the Milky Way. RP Riess, AG (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 33 TC 92 Z9 93 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1996 VL 473 IS 2 BP 588 EP 594 DI 10.1086/178174 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VZ151 UT WOS:A1996VZ15100003 ER PT J AU Kochanek, CS AF Kochanek, CS TI The flat-spectrum radio luminosity function, gravitational lensing, galaxy ellipticities, and cosmology SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, theory; galaxies, elliptical and lenticular, cD; galaxies, luminosity function, mass function; galaxies, structure; gravitational lensing; radio continuum, galaxies ID PARKES SELECTED REGIONS; GALACTIC SOURCE SURVEY; SOURCE COUNTS; REDSHIFT SURVEY; DARK HALOS; 4.755 GHZ; 5 GHZ; LENSES; EVOLUTION; STATISTICS AB The number of lenses found in the JVAS survey of flat-spectrum radio sources for gravitational lenses is consistent with statistical models of optical surveys for lensed quasars. The 90% confidence limit on Omega(0) in flat cosmological models (Omega(0) + lambda(0) = 1) is approximately 0.15 less than or similar to Omega(0) less than or similar to 2. Depending on the RLF model, we predict 2.4-3.6 lenses in the JVAS survey and in the first paper part of the fainter CLASS survey and 0.3-0.6 lenses in the brighter PHFS survey for an Omega(0) = 1 model. The uncertainties are because of the small numbers of lenses (there are only 4 compact JVAS lenses) and the uncertainties in the radio luminosity function (RLF) caused by the lack of information on the redshift distribution of 10-300 mJy radio sources. If we force the models to produce the observed number of JVAS lenses, the mean redshift of a 50 mJy source varies from z(s) = 0.4 for Omega(0) = 0, to 1.9 for Omega(0) = 1, to almost 4.0 for Omega(0) = 2 when Omega(0) + lambda(0) = 1. The source fluxes and redshifts of the lenses in the JVAS and CLASS surveys are consistent with the statistical models. The numbers of four-image lenses found in the JVAS survey and in surveys for lensed quasars are mutually consistent but slightly larger than expected for models using the observed axis ratios of E and SO galaxies. The best fts to the lens data require a projected axis ratio of b/a = 0.50 with a 90% confidence range of 0.25 < b/a < 0.65. RP Kochanek, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, MS-51, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 76 TC 62 Z9 63 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1996 VL 473 IS 2 BP 595 EP 609 DI 10.1086/178175 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VZ151 UT WOS:A1996VZ15100004 ER PT J AU Kochanek, CS Kolatt, TS Bartelmann, M AF Kochanek, CS Kolatt, TS Bartelmann, M TI Proper motions of VLBI lenses, inertial frames, and the evolution of peculiar velocities SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; cosmology, theory; gravitational lensing; techniques, interferometric ID DMR SKY MAPS; GRAVITATIONAL LENS; PRIMORDIAL INHOMOGENEITY; COSMOLOGICAL CONSTANT; INDIVIDUAL STARS; SYSTEM; GALAXIES; Q2237+0305; MAGNIFICATION; MORPHOLOGY AB Precise determinations of the image positions in quad gravitational lenses using VLBI can be used to measure the relative transverse velocity of the lens galaxy and the observer. The typical proper motions are mu as yr(-1), so the timescale to measure the motion is 10 years. By measuring the dipole of the proper motions in an ensemble of lenses we can set limits on the deviation of the inertial frame defined by the lenses from that defined by the CMB dipole and estimate the Hubble constant. The residual proper motions after subtracting the dipole probe the evolution of peculiar velocities with redshift and can be used to estimate the density parameter Omega(0). For N lenses, VLBI measurement accuracies of sigma(0), and a baseline of T years, we estimate that the 2 sigma limit on the rms peculiar velocity of the lens galaxies is 3100(sigma(theta)/10 mu as)(yr/T)/N-1/2 km s(-1), and that the time required for the 2 sigma limit to reach the level of the local rms peculiar velocity upsilon(0,rms) is approximately 10N(-1/2)(upsilon(0,rms)/600 km s(-1))(-1)(sigma(theta)/10 mu as) yr. For a 10 yr baseline and N = 10 lenses we expect the 1 sigma limit on the misalignment with the CMB dipole to be Delta theta = 20 degrees or equivalently to obtain an upper limit of Delta H-0/H-0 < 0.34. C1 MAX PLANCK INST ASTROPHYS,D-85748 GARCHING,GERMANY. RP Kochanek, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS-51,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Bartelmann, Matthias/A-5336-2014 NR 56 TC 8 Z9 8 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1996 VL 473 IS 2 BP 610 EP 619 DI 10.1086/178176 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VZ151 UT WOS:A1996VZ15100005 ER PT J AU David, LP Jones, C Forman, W AF David, LP Jones, C Forman, W TI ROSAT PSPC observations of cool rich clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies, clusters, general; X-rays, galaxies ID LARGE-SCALE STRUCTURE; COLD DARK MATTER; X-RAY-EMISSION; INTRACLUSTER MEDIUM; SURFACE PHOTOMETRY; INFRARED-EMISSION; GALAXY FORMATION; POOR CLUSTERS; EVOLUTION; A2256 AB We present the results of ROSAT PSPC observations of three cool (kT less than or equal to 3 keV) Abell, clusters of galaxies (A262, A539, and A2589). Spatially resolved X-ray spectroscopy shows that the gas in these clusters is essentially isothermal beyond the central cooling how region. The PSPC spectra of A262 also show excess soft X-ray absorption above that expected from the galactic hydrogen column density. The excess absorption is not confined to the central cooling flow region but is distributed across the entire held of view with a slight increase in absorption at large radii. We show that this excess absorption coincides with a region of galactic cirrus observed by IRAS. Using the 100 mu m flux density toward A262, we derive a column density of molecular gas that is comparable to the column density of atomic gas and can account for the excess absorption. The spatial distribution of the molecular gas is also consistent with the observed variation in soft X-ray absorption across the PSPC held of view, Using the observed density and temperature profiles of the hot gas in these clusters, we determine their gravitating masses from the equation of hydrostatic equilibrium. The anisotropy parameter of the member galaxies is then calculated from the observed line-of-sight velocity dispersion and the X-ray-determined mass. For A262, we find that the early-type galaxies are virialized with a nearly isotropic velocity dispersion, while most of the spiral galaxies cannot be virialized for any value of the anisotropy parameter. There is also a strong alignment between the optical isophotes of the central dominant galaxy, the cluster X-ray isophotes in both A262 and A2589, and the large-scale orientation of the host superduster. These results are consistent with a formation scenario in which clusters form through the accretion of gas and galaxies along large-scale filaments. We also calculate the entropy profile of the hot gas for a sample of groups, cool clusters, and hot clusters. We find that the gas entropy in cool clusters increases very gradually with radius while rich clusters show a much steeper gradient. The entropy of the core gas (beyond the cooling flow region) is essentially a constant in groups and rich clusters. These results suggest that the diffuse gas in groups and clusters was preheated before, or during, gravitational collapse. The marginal radial increase in the gas entropy in groups indicates that gravitational heating was almost negligible and the gas passed through weak shocks only as it was accreted. The steeper entropy gradient in rich clusters is consistent with the stronger shock heating expected in more massive systems. RP David, LP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, SMITHSONIAN ASTROPHYS OBSERV, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 87 TC 53 Z9 54 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1996 VL 473 IS 2 BP 692 EP + DI 10.1086/178182 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VZ151 UT WOS:A1996VZ15100011 ER PT J AU VerdesMontenegro, L Ho, PTP AF VerdesMontenegro, L Ho, PTP TI The molecular core associated with HH 25-26: Contraction or expansion? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, clouds; ISM, individual (HH 25-26); ISM, jets and outflows; ISM, molecules; stars, pre-main-sequence ID HERBIG-HARO OBJECTS; AMMONIA; OUTFLOWS; CONTINUUM; REGIONS; STARS; CLOUD; GAS AB We mapped the star formation region HH 25-26 IR in the NH3(1, 1) and (2, 2) transitions using the VLA in its D configuration. The study has been made with 5 '' angular resolution and 0.3 km s(-1) velocity resolution. As has been seen before, there is an elongated NH3 core that lies perpendicular to the molecular outflow as traced in high-velocity CO emission. In this experiment, the NH3 core is resolved, showing a central cavity and a number of distinct velocity features. seating is seen at the position where the velocity features overlap spatially, and on the edges of the cavity, which is also seen as a reflection nebula with evidence for shock excitation. We have also detected what appears to be a new 1.3 cm continuum source on the wall of the cavity, associated with a 2.2 mu m point source and jetlike structure. It is not clear at this time whether this is a truly continuum emission or high-velocity ammonia emission. The overall kinematics is complicated. A velocity gradient can be seen, together with the signatures for expanding or contracting motions. We consider here two possible models: (a) st disk or ring structure, slowly rotating and contracting, and (b) an expanding cavity. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP CSIC, INST ASTROFIS ANDALUCIA, APDO 3004, E-18080 GRANADA, SPAIN. NR 17 TC 5 Z9 5 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 DEC 20 PY 1996 VL 473 IS 2 BP 929 EP 945 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VZ151 UT WOS:A1996VZ15100033 ER PT J AU Barret, D McClintock, JE Grindlay, JE AF Barret, D McClintock, JE Grindlay, JE TI Luminosity differences between black holes and neutron stars SO ASTROPHYSICAL JOURNAL LA English DT Review DE black hole physics; stars, neutron; X-rays, general; X-rays, stars ID X-RAY BINARIES; CENTAURUS X-4; GALACTIC-CENTER; OPTICAL OBSERVATIONS; EXOSAT OBSERVATIONS; DYNAMICAL EVIDENCE; COMPACT OBJECT; NOVA-OPHIUCHI; LIGHT-CURVE; CYGNUS X-1 AB We compare the X-ray (1-20 keV) and hard X-ray (20-200 keV) luminosities of black hole binaries (BHBs; i.e., binaries for which the mass of the compact object is known to exceed 3 M(.)) and X-ray bursters (neutron star binaries, NSBs). We discuss two ways of distinguishing a BHB from a NSB: (1) If the X-ray luminosity exceeds similar to 10(37) ergs s(-1), the hard X-ray luminosity of BHBs is relatively unaffected, whereas the hard X-ray luminosity of NSBs decreases drastically; and (2) the hard X-ray luminosity of BHBs is commonly in the range 10(37)-6 x 10(37) ergs s(-1), whereas for NSBs it is less than or similar to 10(37) ergs s(-1). We show that late in their decays transient BHBs (e.g., GRS 1124-68) have X-ray and hard X-ray luminosities comparable to those observed for NSBs. Thus BHBs can be distinguished from NSBs only at relatively high luminosities. We also compare NSBs with the so-called black hole candidates (BHCs; i.e., systems with similar spectral/temporal properties to BHBs). The X-ray and hard X-ray luminosities of LMC X-l, GRO J0422+32, GRS 1915+105, 4U 1543-47, and 4U 1630-47 are much larger than the maximum luminosities observed from NSBs, which supports the idea that they contain black holes. Three other BHCs, namely GRS 1716-249, 1E 1740.7-2942, and GRS 1758-258 (which all lack an ultrasoft spectral component), have hard X-ray luminosities at least a factor of similar to 2-3 above the maximum observed from NSBs, which suggests that these objects also contain black hole primaries. The case of GX 339-4 remains very uncertain because of the large uncertainty in its distance estimates (from 1.3 to 4 kpc). Assuming the larger distance, the X-ray and hard X-ray luminosities of the source, and its luminosity-related spectral changes which are similar to transient BHBs (e.g., GRS 1124-68), support the idea that it contains a black hole. Finally, the X-ray and hard X-ray luminosities of the puzzling X-ray source 4U 1957+11 are in the range of those observed for NSBs, consistent with the idea that it might contain a neutron star. If 4U 1957+11 is, in fact, a neutron star system, this would establish that the combination of a power-law tail and an ultrasoft component (which is present in the spectrum of 4U 1957 + 11) is not a unique spectral signature of an accreting black hole. C1 CTR ETUD SPATIALE RAYONNEMENTS,F-31029 TOULOUSE,FRANCE. RP Barret, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 119 TC 85 Z9 85 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1996 VL 473 IS 2 BP 963 EP 973 DI 10.1086/178206 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VZ151 UT WOS:A1996VZ15100035 ER PT J AU Blackman, EG Yi, I Field, GB AF Blackman, EG Yi, I Field, GB TI Relativistic precessing jets and cosmological gamma-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays, bursts; ISM, jets and outflows; pulsars, general ID WINDS AB We discuss the possibility that gamma-ray bursts may result from cosmological relativistic blob-emitting neutron star jets that precess past the line of sight. Beaming reduces the energy requirements, so that the jet emission can last longer than the observed burst duration. One precession mode maintains a short-duration timescale while a second keeps the beam from returning to the line of sight, consistent with the paucity of repeaters. The long life of these objects reduces the number required for production as compared to short-lived jets. Blobs can account for the time structure of the bursts. Here we focus largely on kinematic and timescale considerations of beaming, precession, and blobs-issues that are reasonably independent of the acceleration and jet collimation mechanisms. We do suggest that large amplitude electromagnetic waves could be a source of blob acceleration. C1 INST ADV STUDY,PRINCETON,NJ 08540. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Blackman, EG (reprint author), INST ASTRON,MADINGLEY RD,CAMBRIDGE CB3 0HA,ENGLAND. NR 28 TC 45 Z9 45 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1996 VL 473 IS 2 BP L79 EP L82 DI 10.1086/310403 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VZ154 UT WOS:A1996VZ15400005 ER PT J AU Honda, H Hirayama, M Watanabe, M Kunieda, H Tawara, Y Yamashita, K Ohashi, T Hughes, JP Henry, JP AF Honda, H Hirayama, M Watanabe, M Kunieda, H Tawara, Y Yamashita, K Ohashi, T Hughes, JP Henry, JP TI Detection of a temperature structure in the Coma cluster of galaxies with ASCA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, clusters, individual (Coma); galaxies, intergalactic medium; X-rays, galaxies ID X-RAY; GAS; EVOLUTION; SATELLITE; IRON AB Significant temperature variation is found from ASCA observations of the hot intracluster medium in the Coma cluster of galaxies. The whole cluster out to 1 degrees from the center was covered by 14 pointings. The temperature of the hot gas in the outside region is estimated by correcting for the stray-light effect from the bright center. The inferred temperature is lower than 4.5 keV in the west region and higher than 10 keV in the east, both offset by 40' (1.6 Mpc for H-0 = 50 km s(-1) Mpc(-1)) from the center. The temperature variation is not explained by a systematic error in the complex point-spread function of the ASCA X-ray telescope. The azimuthal variation of temperature is probably caused by recent mergers and may reflect an extended distribution of the dark matter. C1 TOKAI UNIV,DEPT PHYS,HIRATSUKA,KANAGAWA 25912,JAPAN. UNIV TOKYO,DEPT PHYS,BUNKYO KU,TOKYO 113,JAPAN. NAGOYA UNIV,DEPT PHYS,CHIKUSA KU,NAGOYA,AICHI 46401,JAPAN. TOKYO METROPOLITAN UNIV,DEPT PHYS,HACHIOJI,TOKYO 19203,JAPAN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. RP Honda, H (reprint author), INST SPACE & ASTRONAUT SCI,1-1 YOSHINODAI,3 CHOME,SAGAMIHARA,KANAGAWA 229,JAPAN. NR 26 TC 70 Z9 70 U1 2 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1996 VL 473 IS 2 BP L71 EP & DI 10.1086/310400 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VZ154 UT WOS:A1996VZ15400003 ER PT J AU Jucks, KW Johnson, DG Chance, KV Traub, WA Salawitch, RJ Stachnik, RA AF Jucks, KW Johnson, DG Chance, KV Traub, WA Salawitch, RJ Stachnik, RA TI Ozone production and loss rate measurements in the middle stratosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SULFURIC-ACID; UARS DATA; CHLORINE; NITROGEN; BROMINE; CLO; O-3; MESOSPHERE; CHEMISTRY; REDUCTION AB We present the first simultaneous measurements of HOx, NOx, and Cl-x radicals in the middle stratosphere obtained during a balloon flight at 34 degrees N in September 1989, along with calculations from a photochemical model, to show that NO, catalytic cycles dominate loss of ozone (O-3) for altitudes between 24 and 38 km; the observed abundance of ClO is lower than that expected for altitudes above 30 km on the basis of models using recommended rates and cross sections, reducing the relative importance of the Cl-x catalytic cycles for loss of O-3; and removal rates of O-3 derived from observed concentrations of rate limiting HOx, NOx, and Cl-x radicals balance computed production rates for altitudes between 32 and 38 km, a region where ozone is expected to be regulated primarily by photochemical processes. C1 CALTECH, JET PROP LAB, PASADENA, CA 91109 USA. RP Jucks, KW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Salawitch, Ross/B-4605-2009; OI Salawitch, Ross/0000-0001-8597-5832; Chance, Kelly/0000-0002-7339-7577 NR 46 TC 30 Z9 30 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 20 PY 1996 VL 101 IS D22 BP 28785 EP 28792 DI 10.1029/96JD02739 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA VZ788 UT WOS:A1996VZ78800014 ER PT J AU DiMichele, WA Phillips, TL AF DiMichele, WA Phillips, TL TI Clades, ecological amplitudes, and ecomorphs: Phylogenetic effects and persistence of primitive plant communities in the Pennsylvanian-age tropical wetlands SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Geological-Society-of-America CY 1994 CL SEATTLE, WA SP Paleontological Soc DE palaeobotany; palaeoecology; Pennsylvanian; tropical; extinction ID COAL-SWAMP VEGETATION; NORTH-AMERICA; FOSSIL PLANTS; SP-NOV; PATTERNS; PALEOECOLOGY; EURAMERICA; USA; REPRODUCTION; CORDAITALES AB Pennsylvanian-age wetland plant communities and landscape gradients exhibit persistent species composition and ecomorphic structure. Such patterns are attributable in large part to strong phylogenetic partitioning of ecological resource space at the level of higher taxa. Each of four major class-rank clades in tropical wetlands was centered in a physically distinct part of the lowland ecosystem. Once established in these physical settings clades tended to resist displacement until removed by physically driven extinction. Lycopsid trees were the principal dominants of the wettest habitats and had subpartitioned these environments along generic lines. Seed plants were the dominants on well to poorly drained elastic substrates, a diverse set of habitats reflected in high diversity of species and architectures. Sphenopsids were most abundant in aggradational environments subject to high levels of physical stress. Ferns initially were interstitial opportunists and colonizers of disturbed areas in a variety of environments. These ecological patterns were established in concert with the architectural radiation of the vascular plants, which occurred during the Devonian-Mississippian transition and established the major classes. Within the wetlands, the replacement of species by close relatives drawn from the same families or genera contributed significantly to persistence of communities and landscape gradients. Replacement was more likely to occur from within a clade where similar ecologies already existed, than from across major clades between which the basic ecologies were different. Possibly interacting with the phylogenetic factors were community and landscape level multispecies effects that may have placed limits on species replacement patterns. The existence of such emergent properties of multispecies assemblages is suggested by a breakdown of the system beginning with major, climatically induced extinctions at the Middle-Late Pennsylvanian transition. Following extinctions of the major Middle Pennsylvanian trees, opportunistic ferns gave rise to dominants in many parts of the wetlands, perhaps due to loss of some aspects of system self-regulation. As climatic drying continued seed plants began their largely passive rise to dominance in most kinds of habitats. C1 UNIV ILLINOIS,DEPT PLANT BIOL,URBANA,IL 61801. RP DiMichele, WA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. RI DiMichele, William/K-4301-2012 NR 110 TC 55 Z9 55 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD DEC 20 PY 1996 VL 127 IS 1-4 BP 83 EP 105 DI 10.1016/S0031-0182(96)00089-2 PG 23 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA WD158 UT WOS:A1996WD15800006 ER PT J AU Lemaitre, R Ng, PKL AF Lemaitre, R Ng, PKL TI Rediscovery and redescription of the rare hermit crab, Diogenes jubatus (Nobili, 1903) (Crustacea: Decapoda: Anomura: Diogenidae), from Singapore SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article AB A hermit crab recently captured near Singapore has proven to represent a rare species, Diogenes jubatus (Nobili, 1903). Originally described in the genus Troglopagurus Henderson, this is one of eight species now placed in the genus Diogenes Dana, which are characterized by a reduced intercalary rostriform process, and long dense setae on the chelipeds and ambulatory legs. Although D. jubatus has been previously compared to other similar species, no illustrations or complete description exist in the literature. Specimens of Nobili's species had not been reported since the original description nearly a century ago. A complete illustrated redescription of D. jubatus is presented, including coloration. Some observations on behaviour in an aquarium are included. Diagnostic characters and affinities with other species are discussed, and the taxonomic history of Nobili's species is summarized. RP Lemaitre, R (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20506, USA. RI Ng, Peter/J-7393-2012 NR 18 TC 3 Z9 3 U1 0 U2 2 PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES PI SINGAPORE PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE SN 0217-2445 J9 RAFFLES B ZOOL JI Raffles Bull. Zool. PD DEC 20 PY 1996 VL 44 IS 2 BP 323 EP 333 PG 11 WC Zoology SC Zoology GA WB187 UT WOS:A1996WB18700002 ER PT J AU Lopez, DS AF Lopez, DS TI Closure explained SO NATURE LA English DT Letter RP Lopez, DS (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD DEC 19 PY 1996 VL 384 IS 6610 BP 608 EP 608 DI 10.1038/384608b0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VZ296 UT WOS:A1996VZ29600014 ER PT J AU Asher, GW Berg, DK Beaumont, S Morrow, CJ ONeill, KT Fisher, MW AF Asher, GW Berg, DK Beaumont, S Morrow, CJ ONeill, KT Fisher, MW TI Comparison of seasonal changes in reproductive parameters of adult male European fallow deer (Dama dama dama) and hybrid Mesopotamian X European fallow deer (D d mesopotamica X D d dama) SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE fallow deer; Dama dama; genotype; hybridisation; breeding season ID CERVUS-ELAPHUS; TESTOSTERONE SECRETION; BREEDING-SEASON; LH; HYBRIDIZATION; INSEMINATION; DAVIDIANUS; PATTERN; GROWTH; CYCLE AB In a study, aimed at comparing seasonal reproductive development of European fallow deer (Dama dama dama) with Mesopotamian (D. d. mesopotamica) X European F-1 hybrids, five adult males of each genotype, which had been raised together since birth, were maintained as a bachelor group. Morphometric (body weight, neck circumference and testis diameter), endocrine (plasma testosterone concentrations) and seminal (ejaculate volume, spermatozoa per ejaculate and spermatozoa motility) parameters were recorded at fortnightly or monthly intervals for a 15-month period, and antler status was noted daily during the general periods of casting and velvet stripping. In addition, two bucks of each genotype were blood sampled via indwelling jugular catheters every 30 min for 24-h periods on five occasions (2-3 months intervals) during the year, and plasma was analysed for concentrations of testosterone and LH. Parameter profiles of the two genotypes were compared by global and time series ante-dependence covariance analysis to investigate overall profile similarity and the seasonal nature of any observed differences. Plasma hormone profiles from high-frequency blood sampling were subjected to PULSAR analysis to determine pulse frequency and amplitude. Throughout the study hybrid males were approximate to 30% heavier than European males. However, both genotypes exhibited dramatic but parallel patterns of body weight change (global P = 0.054). Neck circumference was correlated with body weight throughout (P < 0.05), with similar regression slopes between the genotypes at any sampling time (P > 0.10). Covariance adjustment to a common initial body weight was performed to eliminate the effects of large body weight differences on muscle hypertrophy and regression. While profiles of corrected neck circumference were significantly different at the global level (P < 0.01), analysis by time revealed differences occurring only during the latter period of muscular regression in spring. However, profiles of other parameters, including testis diameter, plasma testosterone concentrations, spermatozoa per ejaculate and percentage motile spermatozoa, exhibited significant displacement between genotypes (global P < 0.05) evident as 2-4 weeks advancement in the sexual development (late summer/autumn) and quiescence (spring) phases for hybrid males relative to European males. Furthermore, mean dates of antler casting and velvet stripping were significantly earlier by 2-3 weeks for hybrid males than European males (P < 0.05). High frequency blood sampling revealed markedly seasonal patterns of secretion of testosterone and LH, with hybrid males exhibiting an apparent earlier onset of high-amplitude testosterone 'surges' in February (late summer) compared to those occurring in April (autumn) for European males. When viewed collectively, the data indicate strongly that the Mesopotamian influence is evident in the earlier attainment of sexual development and fertility in late summer and autumn, and earlier onset of sexual quiescence in spring. This is in accord with anecdotal information on earlier reproductive patterns in purebred Mesopotamian fallow deer. C1 AGRES,RUAKURA AGR CTR,HAMILTON,NEW ZEALAND. SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. RP Asher, GW (reprint author), AGRES,INVERMAY AGR CTR,PRIVATE BAG 50034,MOSGIEL,NEW ZEALAND. NR 27 TC 10 Z9 12 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD DEC 16 PY 1996 VL 45 IS 3 BP 201 EP 215 DI 10.1016/S0378-4320(96)01577-1 PG 15 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA VZ045 UT WOS:A1996VZ04500004 PM 9227923 ER PT J AU Wolda, H Chandler, DS AF Wolda, H Chandler, DS TI Diversity and seasonality of tropical Pselaphidae and Anthicidae (Coleoptera) SO PROCEEDINGS OF THE KONINKLIJKE NEDERLANDSE AKADEMIE VAN WETENSCHAPPEN LA English DT Article ID NEW-HAMPSHIRE; OLD-GROWTH; BEETLES COLEOPTERA; 40-YEAR-OLD FOREST AB Diversity and seasonal abundance patterns in anthicid and pselaphid beetles were studied at six sites in the Republic of Panama by means of light-traps. Pselaphids were much richer in species than anthicids, and the latter were rare or absent at higher elevations. Many more species of pselaphids were found in these tropical samples than in any temperate zone samples known to us. Between-site similarities in species composition were generally low, much lower than between-year within-site similarities, but were highly correlated with such similarities calculated for other groups of insects from these same sites. Seasonal variation in abundance was characterized using circular statistics. The degree of seasonality, measured by the 'Mean Vector', was higher at the seasonal than at the less seasonal sites, but much lower than at most temperate zone sites. At two of the three sites where anthicids were relatively common, they had the mean of their seasonal distribution mainly at the late dry season and early rainy season, while the means of the pselaphids were found throughout the rainy season. At the third site, an aseasonal one, means of abundance of species of both families were found throughout the year. At two sites, but not at the other sites, many species had a distinct bimodal distribution. The between-site variation in seasonality was of the same order of magnitude as the within-site between-year variation. C1 SMITHSONIAN TROP RES INST,BALBOA,ANCON,PANAMA. UNIV NEW HAMPSHIRE,DEPT ZOOL,DURHAM,NH 03824. NR 49 TC 7 Z9 7 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS J9 P K NED AKAD WETENSC JI Proc. K. Ned. Akad. Wet. PD DEC 16 PY 1996 VL 99 IS 3-4 BP 313 EP 333 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA XU185 UT WOS:A1996XU18500009 ER PT J AU Doroshkevich, AG Tucker, DL Oemler, A Kirshner, RP Lin, H Shectman, SA Landy, SD Fong, R AF Doroshkevich, AG Tucker, DL Oemler, A Kirshner, RP Lin, H Shectman, SA Landy, SD Fong, R TI Large- and superlarge-scale structure in the Las Campanas redshift survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies, clusters, general; large-scale structure of Universe ID GALAXY DISTRIBUTION; DARK-MATTER; UNIVERSE; FILAMENTS; STATISTICS; TOPOLOGY; DENSITY; COUNTS; VOIDS; MODEL AB In this paper we employ a core-sampling analysis to find characteristic scales for the large- and the superlarge-scale structure (LSS and SLSS, respectively) in the Las Campanas Redshift Survey (LCRS), With this method, we show that the spatial distribution of galaxies can be roughly characterized as a superposition of three different populations of structural elements: the richest and most stable part is composed of sheet-like elements which can be identified with the SLSS; a system of rich filaments forms the stable part of the LSS; and a system of poor, sparsely populated filaments, lying preferentially in underdense regions, completes the LSS construction. The SLSS incorporates about 60 per cent of the galaxies within the full survey sample, and this value changes little for subsamples constrained by absolute magnitude. Hence, the number density of galaxies is heavily modulated by the SLSS. The spatial distribution of the SLSS elements is approximately Poissonian and is characterized by a mean separation of elements D-sc approximate to (77 +/- 9) (h-1) Mpc for the full LCRS sample. This value for D-sc depends only weakly on galaxy luminosity. The stable component of the LSS contains about 20 per cent of the galaxies in the full sample, and the spatial distribution of this component can also be approximated as Poissonian. This distribution is characterized for the full LCRS sample by the mean separation of filaments D-fc approximate to (30 +/- 2) h(-1) Mpc. The poorest and most sparsely populated component of the LSS contains about 20 per cent of the galaxies in the full LCRS sample. The spatial distribution of this component of the structure can also be described as Poissonian and can be characterized by a mean separation of filaments D-fc approximate to (12.9 +/- 0.3) h(-1) Mpc. The projected proper thickness of the sheets, t(pr), is approximate to (4-5) h(-1) Mpc, much smaller than the separation of the sheets themselves; hence, galaxies tend to be confined to a relatively small fraction of the survey volume. This heavy concentration of galaxies within the sheets of SLSS, however, is not necessarily accompanied by a similar concentration of dark matter. C1 ASTROPHYS INST POTSDAM, D-14482 POTSDAM, GERMANY. YALE UNIV, DEPT ASTRON, NEW HAVEN, CT 06520 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. OBSERV CARNEGIE INST WASHINGTON, PASADENA, CA 91101 USA. UNIV DURHAM, DEPT PHYS, DURHAM DH1 3LE, ENGLAND. RUSSIAN ACAD SCI, MV KELDYSH APPL MATH INST, MOSCOW 125047, RUSSIA. RP Doroshkevich, AG (reprint author), THEORET ASTROPHYS CTR, BLEGDAMSVEJ 17, DK-2100 COPENHAGEN O, DENMARK. NR 53 TC 37 Z9 37 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 15 PY 1996 VL 283 IS 4 BP 1281 EP 1310 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WA235 UT WOS:A1996WA23500020 ER PT J AU Meggers, BJ AF Meggers, BJ TI Paleoindians in the Brazilian Amazon SO SCIENCE LA English DT Letter RP Meggers, BJ (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ANTHROPOL,WASHINGTON,DC 20560, USA. NR 9 TC 1 Z9 1 U1 1 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD DEC 13 PY 1996 VL 274 IS 5294 BP 1823 EP 1823 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VY200 UT WOS:A1996VY20000006 ER PT J AU Riess, AG Press, WH Kirshner, RP AF Riess, AG Press, WH Kirshner, RP TI A precise distance indicator: Type Ia supernova multicolor light-curve shapes SO ASTROPHYSICAL JOURNAL LA English DT Review DE distance scale; dust, extinction; supernovae, general ID ABSOLUTE-MAGNITUDE DISTRIBUTIONS; WHITE-DWARF MODELS; HUBBLE CONSTANT; FIELD GALAXIES; LOCAL GROUP; STANDARD CANDLES; BIAS PROPERTIES; II SUPERNOVAE; MOTION; SCALE AB We present an empirical method that uses multicolor light-curve shapes (MLCSs) to estimate the luminosity, distance, and total line-of-sight extinction of Type Ia supernovae (SNe Ia). The empirical correlation between the MLCSs and the luminosity is derived from a ''training set'' of nine SN Ia light curves with independent distance and reddening estimates. We find that intrinsically dim SN Ia's are redder and have faster light curves than the bright ones, which are slow and blue. By 35 days after maximum, the intrinsic color variations become negligible. A formal treatment of extinction employing Bayes's theorem is used to estimate the best value and its uncertainty. Applying the MLCS method to both light curves and to color curves provides enough information to determine which supernovae are dim because they are distant, which are intrinsically dim, and which are dim because of extinction by dust. The precision of the MLCS distances is examined by constructing a Hubble diagram with an independent set of 20 SN Ia's. The dispersion of 0.12 mag indicates a typical distance accuracy of 5% for a single object, and the intercept yields a Hubble constant on the Sandage et al. Cepheid distance scale of H-0 = 64 +/- 3 (statistical) km s(-1) Mpc(-1) (+/- 6 total error). The slope of 0.2010 +/- 0.0035 mag over the distance interval 32.2 < mu < 38.3 yields the most precise confirmation of the linearity of the Hubble law. RP Riess, AG (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 118 TC 494 Z9 498 U1 2 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1996 VL 473 IS 1 BP 88 EP 109 DI 10.1086/178129 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX329 UT WOS:A1996VX32900009 ER PT J AU Sari, R Narayan, R Piran, T AF Sari, R Narayan, R Piran, T TI Cooling timescales and temporal structure of gamma-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays, bursts; hydrodynamics; radiation mechanisms, nonthermal; relativity; shock waves ID SPECTRA AB A leading mechanism for producing cosmological gamma-ray bursts (GRBs) is via ultrarelativistic particles in an expanding fireball. The kinetic energy of the particles is converted into thermal energy in two shocks, a forward shock and a reverse shock, when the outward flowing particles encounter the interstellar medium. The thermal energy is then radiated via synchrotron emission and Comptonization. We estimate the synchrotron cooling timescale of the shocked material in the forward and reverse shocks for electrons of various Lorentz factors, focusing in particular on those electrons whose radiation falls within the energy detection range of the BATSE detectors. We find that in order to produce the rapid variability observed in most bursts, the energy density of the magnetic field in the shocked material must be greater than about 1% of the thermal energy density. In addition, the electrons must be nearly in equipartition with the protons, since otherwise we do not have reasonable radiative efficiencies of GRBs. Inverse Compton scattering can increase the cooling rate of the relevant electrons, but the Comptonized emission itself is never within the BATSE range. These arguments allow us to pinpoint the conditions within the radiating regions in GRBs and to determine the important radiation processes. In addition, they provide a plausible explanation for several observations. The model predicts that the duty cycle of intensity variations in GRB light curves should be nearly independent of burst duration and should scale inversely as the square root of the observed photon energy. Both correlations are in agreement with observations. The model also provides a plausible explanation for the bimodal distribution of burst durations. There is no explanation, however, for the presence of a characteristic break energy in GRB spectra. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Sari, R (reprint author), HEBREW UNIV JERUSALEM, RACAH INST PHYS, IL-91904 JERUSALEM, ISRAEL. OI Narayan, Ramesh/0000-0002-1919-2730 NR 18 TC 161 Z9 164 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1996 VL 473 IS 1 BP 204 EP 218 DI 10.1086/178136 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX329 UT WOS:A1996VX32900016 ER PT J AU Ayres, TR Simon, T Stauffer, JR Stern, RA Pye, JP Brown, A AF Ayres, TR Simon, T Stauffer, JR Stern, RA Pye, JP Brown, A TI Sleuthing the dynamo: Hubble Space Telescope faint object spectrograph observations of solar-type dwarfs in young galactic clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations, general; stars, coronae; stars, emission-line, Be; stars, rotation; ultraviolet, stars ID LOWER MAIN-SEQUENCE; LATE-TYPE STARS; X-RAY-EMISSION; LOW-MASS STARS; MAGNETIC-FIELDS; COOL STARS; CHROMOSPHERIC ACTIVITY; ROTATIONAL VELOCITIES; STELLAR ACTIVITY; IUE OBSERVATIONS AB We have used the Faint Object Spectrograph of the Hubble Space Telescope to record the ultraviolet emissions of solar-type [(B-V)(0) similar to 0.6 mag] dwarf stars in young galactic clusters: five in the Hyades (t similar to 600 Myr); three in the Pleiades (t similar to 70 Myr); and two in alpha Persei (t similar to 50 Myr). Despite high levels of scattered light in the G130H (1140-1606 Angstrom) spectra, the key C IV lambda 1549 blend was detected in all of the targets. The 10(5) K emission displays a dramatic decline from the youngest to the oldest stars of the sample, well correlated with rotational velocity; evidence of flaring in the most active of the G dwarfs; a wide spread in intensity among the Pleiades stars; but a small dispersion among the Hyades stars. The Mg II lambda 2800 emission is strongly enhanced in the younger stars, and the 2000 Angstrom continuum is significantly elevated in the Hyades stars compared with the Sun. The hyperactive stars of the sample show an apparent saturation of their C Iv emission at high rotational velocities, analogous to that seen in X-rays. The rotation-activity relations possibly exhibit mild curvature, in addition to the saturation, which nevertheless maps onto a simple power law in f(X)/f(bol) versus f(CIV)/f(bol). The Sun apparently tracks a similar power law over the course of its magnetic activity cycle. We discuss these results in terms of simple magnetic loop models. We show that the nonlinear power-law variation of f(CIV)/f(bol) with rotational velocity (slope similar to 1.5, contrary to the suspected linear dependence of the magnetic filling factor) very likely arises from a systematic increase in the base pressures of the dominant coronal loops compared with their counterparts on the Sun. The nonlinear X-ray/C IV power law (slope similar to 1.7) separately indicates a significant increase in the mean apex temperature of the dominant coronal loops. We argue that the distribution of loop structures might change character from inactive stars like the Sun (dominated by X-ray-bright points and Active Region loops) to the hyperactive cluster stars (dominated by interregion large-scale structures or postflare loops). C1 UNIV HAWAII, INST ASTRON, HONOLULU, HI 96822 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. LOCKHEED MARTIN SOLAR & ASTROPHYS LAB, PALO ALTO, CA 94304 USA. UNIV LEICESTER, DEPT PHYS & ASTRON, LEICESTER LE1 7RH, LEICS, ENGLAND. RP UNIV COLORADO, CTR ASTROPHYS & SPACE ASTRON, CAMPUS BOX 391 CASA, BOULDER, CO 80309 USA. NR 79 TC 23 Z9 23 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1996 VL 473 IS 1 BP 279 EP 293 DI 10.1086/178143 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX329 UT WOS:A1996VX32900023 ER PT J AU Popham, R Kenyon, S Hartmann, L Narayan, R AF Popham, R Kenyon, S Hartmann, L Narayan, R TI Spectra and line profiles of FU Orionis objects: Comparisons between boundary layer models and observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars, pre-main-sequence; stars, rotation; stars, variables, other (FU Orionis) ID T-TAURI STARS; SEQUENCE ACCRETION DISKS; ANGULAR-MOMENTUM; YOUNG STARS; EVOLUTION; VARIABLES; ORIGIN AB We present solutions for the accretion disks and boundary layers in pre-main-sequence stars undergoing FU Orionis outbursts. These solutions differ from earlier disk solutions in that they include a self-consistent treatment of the boundary layer region. In a previous paper, Popham showed that these stars should stop accreting angular momentum once they spin up to modest rotation rates. Here we show that for reasonable values of a, these low angular momentum accretion rate solutions fit the spectra and line profiles observed in FU Orionis objects better than solutions with high rates of angular momentum accretion. We find solutions that fit the observations of FU Orionis and V1057 Cygni. These solutions have mass accretion rates of 2 and 1 x 10(-4) M. yr(-1), stellar masses of 0.7 and 0.5 M., and stellar radii of 5.75 and 5.03 R., respectively. They also have modest stellar rotation rates 8-9 x 10(-6) s(-1), comparable to the observed rotation rates of T Tauri stars, and angular momentum accretion rates of zero. This supports our earlier suggestion that FU Orionis outbursts may regulate the rotation rates of T Tauri stars. RP Popham, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS 51,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Narayan, Ramesh/0000-0002-1919-2730; Kenyon, Scott/0000-0003-0214-609X NR 38 TC 33 Z9 33 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1996 VL 473 IS 1 BP 422 EP 436 DI 10.1086/178155 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX329 UT WOS:A1996VX32900035 ER PT J AU Bailyn, CD Rubenstein, EP Slavin, SD Cohn, H Lugger, P Cool, AM Grindlay, JE AF Bailyn, CD Rubenstein, EP Slavin, SD Cohn, H Lugger, P Cool, AM Grindlay, JE TI Hubble Space Telescope observations of the post-core-collapse globular cluster NGC 6752: A search for cataclysmic variables SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, general; globular clusters, individual (NGC 6752); novae, cataclysmic variables; white dwarfs; X-rays, stars ID CLOSE BINARIES; STAR-CLUSTERS; NGC-6397 AB We report the results of HST WFPC2 observations of the core of NGC 6752. We identify two candidate cataclysmic variables (CVs) from their strong narrowband H alpha emission, periodic variability, and, in one case, a UV excess. We interpret the variability of these stars as being double-peaked, ellipsoidal light curves, in which case the orbital periods are 5.1 and 3.7 hr. The CV candidates fall at the edge of the error circle of one of the known X-ray sources in the cluster. C1 INDIANA UNIV,DEPT ASTRON,BLOOMINGTON,IN 47405. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Bailyn, CD (reprint author), YALE UNIV,DEPT ASTRON,POB 208101,NEW HAVEN,CT 06520, USA. NR 21 TC 26 Z9 26 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1996 VL 473 IS 1 BP L31 EP L34 DI 10.1086/310382 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX331 UT WOS:A1996VX33100008 ER PT J AU Guzman, HM Jarvis, KE AF Guzman, HM Jarvis, KE TI Vanadium century record from Caribbean reef corals: A tracer of oil pollution in Panama SO AMBIO LA English DT Article ID ATMOSPHERIC VANADIUM; HEAVY-METALS; SKELETONS; CONTAMINATION; GROWTH; WATER; LEAD; SPECTROMETRY; CADMIUM; OCEAN AB The Caribbean region is potentially one of the largest oil-producing areas in the world, and contamination by petroleum is threatening the marine environment. Vanadium (V), an abundant element in crude oils, was used as proxy tracer of oil pollution along the Caribbean coast of Panama. We develop a century chronology based on the concentration of vanadium (using ICP-MS) incorporated into annual growth bands of coral skeletons. The chronology for vanadium showed a relatively clear pattern where background seawater concentrations were observed in the early history of the corals followed by an increase after 1962, the initiation of a refinery operation. The vanadium chronology suggests that a major degradation process in the coastal zone could have started around the 1960s, but we were unable to confirm such an assumption due to the lack of long-term ecological and pollution data. The gradual increase of vanadium into the marine environment might be used as a pointer to oil pollution. C1 UNIV LONDON IMPERIAL COLL SCI TECHNOL & MED,CTR ANALYT RES & ENVIRONM,NERC,ICP,MS FACIL,ASCOT SL5 7TE,BERKS,ENGLAND. RP Guzman, HM (reprint author), SMITHSONIAN TROP RES INST,APARTADE 2072,BALBOA,PANAMA. NR 45 TC 39 Z9 42 U1 1 U2 14 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 DEC PY 1996 VL 25 IS 8 BP 523 EP 526 PG 4 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA WD971 UT WOS:A1996WD97100009 ER PT J AU Levin, RN AF Levin, RN TI Song behaviour and reproductive strategies in a duetting wren, Thryothorus nigricapillus .1. Removal experiments SO ANIMAL BEHAVIOUR LA English DT Article ID WHITE-THROATED SPARROWS; RED-WINGED BLACKBIRDS; TROPICAL HOUSE WRENS; FEMALE SONG; INDIVIDUAL RECOGNITION; AGELAIUS-PHOENICEUS; SINGING BEHAVIOR; COURTSHIP SONGS; PAIR BOND; TERRITORIAL AB Mate removal experiments were conducted to test the hypotheses that vocal duetting functions in pair bond maintenance and/or territory defence in the bay wren, Thryothorus nigricapillus, in the Republic of Panama. Males and females were observed while in established pairs, while alone after mate removal and following the arrival of a new mate. Duet repertoires and precision of duet performance were then compared in birds singing with old and new mates. Another experiment in which males were exchanged between two territories was similarly analysed. These experiments demonstrated that (1) individual repertoires and duet precision do not change following a change in mates, refuting the pair bond maintenance hypothesis, and (2) unpaired birds do not lose their territories, failing to support the hypothesis that duets are necessary for territory defence. Analysis of vocalization rates suggested that male and female songs serve different functions. Male vocal behaviour was sensitive to male mating status: when males were alone, their vocalization rates dramatically increased. However, males answered the songs of a new mate less frequently than they did those of their original mate. These results suggest that unpaired males sing to attract females and that males might use participation in duets to assess new mates. The function of duetting by males in established pairs remains unclear. Female song rates were unaffected by female mating status, suggesting that female songs may be directed to conspecific females. Results also indicated that territory residency may play a more important role in mate acquisition for males than it does for females. (C) 1996 The Association for the Study of Animal Behaviour C1 CORNELL UNIV,NEUROBIOL & BEHAV SECT,ITHACA,NY 14853. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 63 TC 93 Z9 94 U1 1 U2 21 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD DEC PY 1996 VL 52 BP 1093 EP 1106 DI 10.1006/anbe.1996.0257 PN 6 PG 14 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA WA303 UT WOS:A1996WA30300004 ER PT J AU Levin, RN AF Levin, RN TI Song behaviour and reproductive strategies in a duetting wren, Thryothorus nigricapillus .2. Playback experiments SO ANIMAL BEHAVIOUR LA English DT Article ID GIBBONS HYLOBATES-MUELLERI; RED-WINGED BLACKBIRDS; FEMALE SONG; EXPERIMENTAL-DESIGNS; AGELAIUS-PHOENICEUS; EXTERNAL VALIDITY; RESPONSES; PSEUDOREPLICATION; MAINTENANCE; TERRITORIAL AB Four series of song playbacks to paired and unpaired resident birds were used to test hypotheses proposed for the function of male song, female song and vocal duets in the bay wren, Thryothorus nigricapillus, in the Republic of Panama. One series of experiments served as a control and established that bay wrens distinguished the duets of conspecifics from those of heterospecifics; a second series indicated that these results were not dependent on which type of male vocalization was used as a stimulus. Two series of experiments compared the responses of paired and unpaired males and females to playbacks of male versus female song. Both paired and unpaired females responded strongly to playback of female song and weakly to playback of male song. These data are consistent with previous results that showed no effect of mating status on female song rates and support the hypothesis that female song functions in intra-sexual aggression, probably in the context of territorial defence. Furthermore, because females initiate all duets in this species, females may be singing independently of males, and thus it is only male behaviour that produces a duet. In contrast to what was observed in females, males responded strongly to playback of both male and female song, but paired males responded more strongly to playback of male song, and unpaired males responded more strongly to playback of female song. These results provide a preliminary indication that female songs are attractive to males and that males may participate in duets as a means of acoustically guarding their mates from other males. (C) 1996 The Association for the Study of Animal Behaviour C1 CORNELL UNIV,NEUROBIOL & BEHAV SECT,ITHACA,NY 14853. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RI Piper, Walter/B-7908-2009 NR 40 TC 101 Z9 103 U1 0 U2 13 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD DEC PY 1996 VL 52 BP 1107 EP 1117 DI 10.1006/anbe.1996.0258 PN 6 PG 11 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA WA303 UT WOS:A1996WA30300005 ER PT J AU Thompson, KV AF Thompson, KV TI Play-partner preferences and the function of social play in infant sable antelope, Hippotragus niger SO ANIMAL BEHAVIOUR LA English DT Article ID SQUIRREL-MONKEYS; BEHAVIOR; DOMINANCE; FLEHMEN; TESTS AB Play-partner preferences were investigated in 38 sable antelope calves observed in semi-captivity at the National Zoological Park's Conservation and Research Center near Front Royal, Virginia. All calves initiated play with peers but rarely played with yearlings or adults. Calves initiated play with most calves in their cohort but had strong preferences for one or two peers. Preferences were highly symmetrical and stable over time. Partners of similar age were preferred. Calves did not prefer individuals of the same sex, nor did they consistently favour individuals of one sex over the other. Calves initiated less play with related peers than expected by chance. Patterns of play-partner preference in infant sable antelope supported the concept of play as self assessment, whereby individuals continually compare their developmental competence with that of their peers. (C) 1996 The Association for the Study of Animal Behaviour C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RP Thompson, KV (reprint author), UNIV MARYLAND,COLL LIFE SCI,BIOL PROGRAM,DEPT ZOOL,COLLEGE PK,MD 20742, USA. RI Thompson, Katerina/B-6146-2009 NR 38 TC 26 Z9 26 U1 1 U2 9 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD DEC PY 1996 VL 52 BP 1143 EP 1155 DI 10.1006/anbe.1996.0261 PN 6 PG 13 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA WA303 UT WOS:A1996WA30300008 ER PT J AU Hamuy, M Phillips, MM Suntzeff, NB Schommer, RA Maza, J Antezana, R Wischnjewsky, M Valladares, G Muena, C Gonzalez, LE Aviles, R Wells, LA Smith, RC Navarrete, M Covarrubias, R Williger, GM Walker, AR Layden, AC Elias, JH Baldwin, JA Hernandez, M Tirado, H Ugarte, P Elston, R Saavedra, N Barrientos, F Costa, E Lira, P Ruiz, MT Anguita, C Gomez, X Ortiz, P DellaValle, M Danziger, J Storm, J Kim, YC Bailyn, C Rubenstein, EP Tucker, D Cersosimo, S Mendez, RA Siciliano, L Sherry, W Chaboyer, B Koopmann, RA Geisler, D Sarajedini, A Dey, A Tyson, N Rich, RM Gal, R Lamontagne, R Caldwell, N Guhathakurta, P Phillips, AC Szkody, P Prosser, C Ho, LC McMahan, R Baggley, G Cheng, KP Havlen, R Wakamatsu, K Janes, K Malkan, M Baganoff, F Seitzer, P Shara, M Sturch, C Hesser, J Hartigan, P Hughes, J Welch, D Williams, TB Ferguson, H Francis, PJ French, L Bolte, M Roth, J Odewahn, S Howell, S Krzeminski, W AF Hamuy, M Phillips, MM Suntzeff, NB Schommer, RA Maza, J Antezana, R Wischnjewsky, M Valladares, G Muena, C Gonzalez, LE Aviles, R Wells, LA Smith, RC Navarrete, M Covarrubias, R Williger, GM Walker, AR Layden, AC Elias, JH Baldwin, JA Hernandez, M Tirado, H Ugarte, P Elston, R Saavedra, N Barrientos, F Costa, E Lira, P Ruiz, MT Anguita, C Gomez, X Ortiz, P DellaValle, M Danziger, J Storm, J Kim, YC Bailyn, C Rubenstein, EP Tucker, D Cersosimo, S Mendez, RA Siciliano, L Sherry, W Chaboyer, B Koopmann, RA Geisler, D Sarajedini, A Dey, A Tyson, N Rich, RM Gal, R Lamontagne, R Caldwell, N Guhathakurta, P Phillips, AC Szkody, P Prosser, C Ho, LC McMahan, R Baggley, G Cheng, KP Havlen, R Wakamatsu, K Janes, K Malkan, M Baganoff, F Seitzer, P Shara, M Sturch, C Hesser, J Hartigan, P Hughes, J Welch, D Williams, TB Ferguson, H Francis, PJ French, L Bolte, M Roth, J Odewahn, S Howell, S Krzeminski, W TI BVRI light curves for 29 type Ia supernovae SO ASTRONOMICAL JOURNAL LA English DT Article AB BV(RI)(KC) light curves are presented for 27 type Ia supernovae discovered during the course of the Calan/Tololo Survey and for two other SNe Ia observed during the same period. Estimates of the maximum light magnitudes in the B, V, and I bands and the initial decline rate parameter Delta m(15)(B) are also given. (C) 1996 American Astronomical Society. C1 UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. UNIV CHILE,DEPT ASTRON,SANTIAGO,CHILE. EUROPEAN SO OBSERV,LA SILLA OBSERV,SANTIAGO 19,CHILE. YALE UNIV,DEPT ASTRON,NEW HAVEN,CT 06520. NATL OPT ASTRON OBSERV,KITT PEAK NATL OBSERV,TUCSON,AZ 85726. PRINCETON UNIV,DEPT ASTROPHYS SCI,PRINCETON,NJ 08544. COLUMBIA UNIV,DEPT ASTRON,NEW YORK,NY 10027. UNIV MONTREAL,DEPT PHYS,MONTREAL,PQ H3C 3J7,CANADA. UNIV MONTREAL,OBSERV MT MEGANT,MONTREAL,PQ H3C 3J7,CANADA. FRED LAWRENCE WHIPPLE OBSERV,AMADO,AZ 85645. UNIV CALIF SANTA CRUZ,UNIV CALIF OBSERV,LICK OBSERV,SANTA CRUZ,CA 95064. UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV N CAROLINA,DEPT PHYS & ASTRON,CHAPEL HILL,NC 27599. UNIV OXFORD,DEPT ASTROPHYS,OXFORD OX1 3RH,ENGLAND. CALIF STATE UNIV FULLERTON,DEPT PHYS,FULLERTON,CA 92634. ASTRON SOC PACIFIC,SAN FRANCISCO,CA 94112. GIFU UNIV,DEPT PHYS,GIFU 50111,JAPAN. BOSTON UNIV,DEPT ASTRON,BOSTON,MA 02215. UNIV CALIF LOS ANGELES,DIV ASTRON,LOS ANGELES,CA 90095. SPACE TELESCOPE SCI INST,COMP SCI CORP,BALTIMORE,MD 21218. DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. UNIV MASSACHUSETTS,FIVE COLL ASTRON DEPT,AMHERST,MA 01003. MCMASTER UNIV,DEPT PHYS & ASTRON,HAMILTON,ON L8S 4M1,CANADA. RUTGERS STATE UNIV,DEPT PHYS & ASTRON,PISCATAWAY,NJ 08855. UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. UNIV MELBOURNE,SCH PHYS,PARKVILLE,VIC 3052,AUSTRALIA. WHEELOCK COLL,BOSTON,MA 02215. SKY PUBLISHING CORP,CAMBRIDGE,MA 02138. UNIV MINNESOTA,SCH PHYS & ASTRON,MINNEAPOLIS,MN 55455. UNIV WYOMING,DEPT PHYS & ASTRON,LARAMIE,WY 82071. CARNEGIE INST WASHINGTON,LAS CAMPANAS OBSERV,LA SERENA,CHILE. RP Hamuy, M (reprint author), NATL OPT ASTRON OBSERV,CERRO TOLOLO INTER AMER OBSERV,CASILLA 603,LA SERENA,CHILE. RI Lira, Paulina/G-8536-2016; Costa, Edgardo /I-5274-2016; Maza, Jose/I-5722-2016; Ruiz, Maria Teresa/I-5770-2016; Mendez, Rene/H-9496-2015; Mendez, Rene/J-6608-2016; Hamuy, Mario/G-7541-2016; OI Costa, Edgardo /0000-0003-4142-1082; Maza, Jose/0000-0003-2068-1328; Ruiz, Maria Teresa/0000-0002-6799-1537; Welch, Doug/0000-0002-2350-0898; Tucker, Douglas/0000-0001-7211-5729 NR 10 TC 208 Z9 209 U1 0 U2 10 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 1996 VL 112 IS 6 BP 2408 EP 2437 DI 10.1086/118192 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX174 UT WOS:A1996VX17400003 ER PT J AU Forbes, DA Brodie, JP Huchra, J AF Forbes, DA Brodie, JP Huchra, J TI Globular cluster luminosity functions and the Hubble constant from WFPC2 imaging: The dominant group elliptical NGC 5846 SO ASTRONOMICAL JOURNAL LA English DT Article ID PHOTOMETRY; GALAXIES; DISTANCE; SYSTEMS; M87 AB The Hubble Space Telescope's Wide Field and Planetary Camera 2 (WFPC2) has several advantages over ground-based observations for the study of globular cluster luminosity functions (GCLFs) and distance determination. Here we present WFPC2 data on the globular clusters associated with NGC 5846. This giant elliptical is the dominant galaxy in a small, compact group located similar to 13 Mpc beyond the Virgo cluster. We have detected over 1200 globular clusters in three (central, north, and south) separate pointings. The luminosity functions in each of these pointings are statistically the same, indicating that the mean luminosity (mass) does not vary between similar to 3 and 30 kpc from the galaxy center. This suggests that dynamical friction and bulge shocking destruction processes are insignificant. We have fit a Gaussian and t(5) profile to the GCLF (of the combined pointings) and find that it is well represented by a turnover magnitude of m(V)(0)=25.05+/-0.10 and a dispersion of sigma=1.34+/-0.06. Our 50% incompleteness level is similar to 1 mag fainter than the turnover. After applying a metallicity correction to the ''universal'' GCLF turnover magnitude, we derive a distance modulus of (m-M)=32.32+/-0.23. For a group velocity V-CMB=1883+/-28 km s(-1), the Hubble constant is H-0=65+/-8 km s(-1) Mpc(-1). (C) 1996 American Astronomical Society. C1 UNIV BIRMINGHAM,SCH PHYS & SPACE RES,BIRMINGHAM B15 2TT,W MIDLANDS,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Forbes, DA (reprint author), UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064, USA. NR 27 TC 23 Z9 23 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 1996 VL 112 IS 6 BP 2448 EP & DI 10.1086/118194 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX174 UT WOS:A1996VX17400005 ER PT J AU DaCosta, GS Armandroff, TE Caldwell, N Seitzer, P AF DaCosta, GS Armandroff, TE Caldwell, N Seitzer, P TI The dwarf spheroidal companions to M31: WFPC2 observations of Andromeda I SO ASTRONOMICAL JOURNAL LA English DT Article ID COLOR-MAGNITUDE DIAGRAM; GALACTIC GLOBULAR-CLUSTERS; HORIZONTAL-BRANCH STARS; GIANT BRANCH; MILKY-WAY; GALAXY; PHOTOMETRY; HALO; SYSTEM; POPULATIONS AB Images have been obtained with the Hubble Space Telescope WFPC2 camera of Andromeda I, a dwarf spheroidal (dSph) galaxy that lies in the outer halo of M31. The resulting color-magnitude diagrams reveal for the first time the morphology of the horizontal branch in this system. We find that, in a similar fashion to many of the galactic dSph companions, the horizontal branch (HB) of And I is predominantly red. Combined with the metal abundance of this dSph, this red HB morphology indicates that And I can be classified as a ''second parameter'' system in the outer halo of M31. This result then supports the hypothesis that the outer halo of M31 formed in the same extended chaotic manner as is postulated for the outer halo of the Galaxy. In addition to the red HB stars, blue HB and RR Lyrae variable stars are also found in the And I color-magnitude diagram. The presence of these stars indicates that And I contains a minority population whose age is comparable to that of the galactic globular clusters. We estimate, however, that the bulk of the stellar population in And I is similar to 10 Gyr old. Thus, again like many of the galactic dSphs, there is clear evidence for an extended epoch of star formation in And I. A radial gradient in the And I HB morphology has also been discovered in the sense that there are relatively more blue HE stars beyond the galaxy's core radius. This may be evidence for more centrally concentrated star formation after the initial episode. Similar HB morphology gradients have also been identified in two of three galactic dSphs studied. The mean magnitude of the blue HB stars suggests that And I lies along the line-of-sight at the same distance as M31 to within similar to+/-70 kpc. Consequently, the true distance of And I from the center of M31 is between similar to 45 and similar to 85 kpc, with the higher estimates being more likely. Such distances are comparable to the galactocentric distances of the nearer Milky Way dSph companions Ursa Minor, Draco, and Sculptor. From the mean color of the lower giant branch, the mean metal abundance of And I is estimated as [Fe/H] = -1.45 +/- 0.2 dex, while the presence of an internal abundance spread with total range of similar to 0.6 dex is suggested by the intrinsic color width of the upper giant branch. A small population of faint blue stars, which we identify as blue stragglers, is also present. (C) 1996 American Astronomical Society. C1 NATL OPT ASTRON OBSERV,KITT PEAK NATL OBSERV,TUCSON,AZ 85726. SMITHSONIAN INST,FL WHIPPLE OBSERV,AMADO,AZ 85645. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. RP DaCosta, GS (reprint author), AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,WESTON,ACT 2611,AUSTRALIA. NR 72 TC 70 Z9 70 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 1996 VL 112 IS 6 BP 2576 EP & DI 10.1086/118204 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX174 UT WOS:A1996VX17400015 ER PT J AU Anderson, CM Weitenbeck, AJ Code, AD Nordsieck, KH Meade, MR Babler, BL Zellner, NEB Bjorkman, KS Fox, GK Johnson, JJ Sanders, WT Lupie, OL Edgar, RJ AF Anderson, CM Weitenbeck, AJ Code, AD Nordsieck, KH Meade, MR Babler, BL Zellner, NEB Bjorkman, KS Fox, GK Johnson, JJ Sanders, WT Lupie, OL Edgar, RJ TI Ultraviolet interstellar polarization of galactic starlight .1. Observations by the Wisconsin Ultraviolet Photo Polarimeter Experiment SO ASTRONOMICAL JOURNAL LA English DT Article ID WAVELENGTH DEPENDENCE; LINEAR-POLARIZATION; OPEN CLUSTERS; EXTINCTION; STARS; DUST AB The Wisconsin Ultraviolet Photo Polarimeter Experiment (WUPPE) flew twice as part of NASA's Astro Spacelab missions in 1990 December and 1995 March. A systematic survey of the interstellar polarization in the ultraviolet was one of the main projects on both flights. The program was carefully crafted to (1) sample the galactic plane as uniformly as practicable, (2) explore sight lines of diverse chemical composition and morphology, and (3) measure the shape of the UV polarization through the full range of known wavelengths of peak polarization in the optical. We present here Astro-2 data for 20 previously unobserved sight lines and combine these with previously published UV data and with optical observations from the University of Wisconsin's ground based facilities and elsewhere. We thus have spectropolarimetry from 1500 to 10,000 Angstrom for 35 galactic objects in which the polarization appears to be dominated by the interstellar component. The extrapolation of the empirical Serkowski formula based only on visual data does not provide a reliable representation of the UV polarization. We find that there are substantial differences in the amount of UV polarization relative to that in the visual. This may indicate that the small and large aligned grain populations are somewhat independent and this may in turn provide a new diagnostic of varying conditions in the interstellar medium. Finally, there are several cases in which the UV polarization is enhanced in the 2000-3000 Angstrom range. (C) 1996 American Astronomical Society. C1 UNIV WISCONSIN,DEPT PHYS,MADISON,WI 53706. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Anderson, CM (reprint author), UNIV WISCONSIN,SPACE ASTRON LAB,1150 UNIV AVE,MADISON,WI 53706, USA. OI Babler, Brian/0000-0002-6984-5752 NR 58 TC 39 Z9 39 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 1996 VL 112 IS 6 BP 2726 EP 2743 DI 10.1086/118217 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VX174 UT WOS:A1996VX17400028 ER PT J AU Barret, D Grindlay, JE Strickman, M Vedrenne, G AF Barret, D Grindlay, JE Strickman, M Vedrenne, G TI CGRO/OSSE observations of the X-ray burster 4U 1915-05 (XB 1916-053) SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE X-rays, stars; stars, individual 4U 1915-05; gamma-rays, observations, stars, neutron ID DISCOVERY AB The X-ray burster 4U 1915-05 was observed from January 24, 1995 through February 14, 1995 by the OSSE experiment aboard the Compton Gamma-Ray Observatory. While previous 1-30 keV observations suggested that 4U 1915-05 could be easily detectable by OSSE, no hard X-ray emission was detected, and stringent upper limits have been derived. The upper Limits are 1.4 10(-4) photons cm(-2) s(-1) and 6.5 10(-5) photons cm(-2) s(-1) in the 50-98 keV and 98-158 keV bands, respectively. This translates into luminosity limits of 1.4 10(35) ergs s(-1) and 1.7 10(35) ergs s(-1) assuming a source distance of 9.3 kpc. Based on the existing data, we define three distinct X-ray spectral states associated with three distinct intensity states of the source: high/very soft state, an intermediate/hard state and a low/(possibly) soft state with 1-37 keV X-ray luminosities of 1.2 10(37), 6 - 7 10(36) and 3 10(36) ergs s(-1), respectively. For these three states we have converted the OSSE upper limits into upper limits on any energy cutoff present in the X-ray to hard X-ray source spectrum. These upper limits range from similar to 10 keV up to 50 keV depending on source the intensity and spectral shape assumed. We found that they are consistent with the source being either in the high state or low state at the time of the OSSE observations. For the high state, the OSSE upper limits imply that less than similar to 4% of the total luminosity is radiated in the hard X-ray band. On the other hand, the source should have been detected in its intermediate state if the cutoff energy, as inferred from Ginga observations, is indeed larger than similar to 50 keV. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. USN,RES LAB,WASHINGTON,DC 20375. RP Barret, D (reprint author), CTR ETUD SPATIALE RAYONNEMENTS,CNRS,UPS,9 AV COLONEL ROCHE,BP 4346,TOULOUSE,FRANCE. NR 12 TC 2 Z9 2 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C269 EP C273 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300060 ER PT J AU Barret, D Grindlay, JE Bloser, PF Zhang, SN Fishman, GJ Harmon, BA Paciesas, WS Ford, E Kaaret, P Tavani, M AF Barret, D Grindlay, JE Bloser, PF Zhang, SN Fishman, GJ Harmon, BA Paciesas, WS Ford, E Kaaret, P Tavani, M TI BATSE observations of hard X-ray emission from X-ray bursters. Presentation of a CGRO/BATSE investigation and first results SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE Galaxy center; gamma-rays, observations; X-ray, bursts; X-rays, stars, ID BLACK-HOLE; EXOSAT OBSERVATIONS; GALACTIC-CENTER; DISCOVERY; SIGMA; BINARIES; NOVA AB We present an on-going BATSE/CGRO investigation devoted to search for hard X-ray emission from Xray bursters with the earth occultation and occultation transform imaging techniques. This is a collaboration between the BATSE team at the NASA/Marshall Space Flight Center, Columbia University and the Harvard Smithsonian Center for Astrophysics. In this paper, we first outline the scientific objectives of our investigation and briefly overview some results obtained within our collaboration. We present preliminary results on two Galactic center X-ray bursters Terzan 2 and GX354-0 for which simultaneous SIGMA data exist and we report on the possible BATSE detection of a hard X-ray outburst from 4U 1705-44. Finally, we discuss on the hard X-ray emission from neutron stars and review the different criteria that have been proposed for distinguishing them from black hole systems on the basis of the properties of their hard X-ray emission. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV SPACE RES ASSOC, HUNTSVILLE, AL 35806 USA. NASA, GEORGE C MARSHALL SPACE FLIGHT CTR, HUNTSVILLE, AL 35812 USA. UNIV ALABAMA, DEPT PHYS, HUNTSVILLE, AL 35899 USA. COLUMBIA UNIV, DEPT PHYS, NEW YORK, NY 10027 USA. RP UPS, CNRS, CESR, 9 AV COLONEL ROCHE, BP 4346, TOULOUSE, FRANCE. NR 35 TC 0 Z9 0 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 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C121 EP C127 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300024 ER PT J AU Bloser, PF Barret, D Grindlay, JE Zhang, SN Harmon, BA Fishman, GJ Paciesas, WS Ford, E Kaaret, P Tavani, M AF Bloser, PF Barret, D Grindlay, JE Zhang, SN Harmon, BA Fishman, GJ Paciesas, WS Ford, E Kaaret, P Tavani, M TI BATSE observations of two X-ray bursters: 4U 1820-30 and 4U 1915-05 SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE stars, 4U 1820-30, 4U 1915-05; X-rays, stars; gamma-rays, observations ID CLUSTER NGC 6624; NEUTRON-STARS; DISCOVERY; PERIOD; FLUX AB Using the BATSE instrument on the Compton Gamma Ray Observatory, the X-ray bursters 4U 1820-30 and 4U 1915-05 have been monitored in the hard X-ray band. In four years of data neither source was detected. We derive 2 sigma upper limits on 20-100 keV flux from 4U 1915-05 of 2.6 10(-2) photons cm(-2) s(-1) (90 mCrab) for 1 day integrations and 9.0 10(-3) photons cm(-2) s(-1) (30 mCrab) for 10 day integrations. For 4U 1820-30 the upper limits are 2.4 10(-2) photons cm(-2) s(-1) (80 mCrab) for 1 day integrations and 1.0 10(-2) photons cm(-2) s(-1) (30 mCrab) for 10 day integrations. These limits are not strong enough to constrain spectral models for the sources. The implications of these observations are discussed in light of BATSE results on other bursters. C1 CTR ETUD SPATIALE RAYONNEMENTS,CNRS,UPS,TOULOUSE,FRANCE. UNIV SPACE RES ASSOC,HUNTSVILLE,AL 35806. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899. COLUMBIA UNIV,DEPT PHYS,NEW YORK,NY 10027. RP Bloser, PF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 22 TC 1 Z9 1 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C275 EP C278 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300061 ER PT J AU Bloser, PF Barret, D Grindlay, JE Zhang, SN Harmon, BA Fishman, GJ Paciesas, WS AF Bloser, PF Barret, D Grindlay, JE Zhang, SN Harmon, BA Fishman, GJ Paciesas, WS TI BATSE observations of the ultra-soft X-ray transient 4U 1630-47 SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE stars, 4U 1630-47; X-rays, stars AB We have monitored the ultra-soft X-ray transient 4U 1630-47 in the hard X-ray band using the BATSE instrument on the Compton Gamma Ray Observatory. In a detailed analysis of the first year of data (May 1991 to April 1992), we have identified a possible similar to 3.5 sigma detection of a transient event in the light curve from TJD 8380-8410 (May 1991). In images made with the new BATSE occultation imaging technique, this event shows up as an excess consistent with the position of 4U 1630-47 to within the technique's angular resolution (similar to 1 degrees). Lacking independent data, and since the event does not concur with the observed 600 day period of the source, we cannot be certain that the outburst is associated with 4U 1630-47. In addition, we investigate those times during the BATSE data that the ephemeris for 4U 1630-47 does predict activity. Parmar et al. (1995) report the detection of 4U 1630-47 by ROSAT during an observation in September 1992. The source was not detected by BATSE and we derive a 2 sigma upper limit during September 1992 of similar to 2.2 10(-2) photons cm(-2) s(-1), or about 70 mCrab, for 5 day integrations. 600 days later in April 1994, we do find evidence of weak emission from 4U 1630-47 at a level of similar to 15 mCrab, owing to a fortuitous lack of interfering sources and good viewing geometry. We compare these results with previous X-ray observations of the source. C1 UPS,CTR ETUD SPATIALE RAYONNEMENTS,CNRS,TOULOUSE,FRANCE. UNIV SPACE RES ASSOC,HUNTSVILLE,AL 35806. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899. RP Bloser, PF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C191 EP C195 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300041 ER PT J AU Grindlay, JE Barret, D Bloser, PF Zhang, SN Fishman, GJ Harmon, BA Paciesas, WS AF Grindlay, JE Barret, D Bloser, PF Zhang, SN Fishman, GJ Harmon, BA Paciesas, WS TI BATSE survey for faint transients and black hole candidates SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE X-rays, stars; stars, GRO J1849-03, 4U 1630-47; black holes; gamma-rays, observations ID X-RAY-EMISSION AB We describe a project to search for faint X-ray transients that are likely to be black hole candidates (BHCs). Our overall objectives are to better constrain the total number of BHCs in the Galaxy and thus the formation and evolution of such systems. A secondary objective is to better understand the outburst mechanism in X-ray novae and the hard X-ray emission region in these systems. We report preliminary BATSE results for analysis of seven fields centered on known (historical) transients in which we search both for recurrent outbursts (to constrain recurrence times) as well as new sources. Preliminary light curves for each source region have been derived for the full 4 year BATSE data from occultation analysis, and occultation imaging has also been carried out to further constrain source positions. As reported in detail in companion papers, a new faint transient, GRO J1849-03 (cf. Zhang et al.), was discovered in one field, and probable hard X-ray outbursts of the recurrent transient 4U 1630-47 (cf. Bloser et al.) were detected for the first time at hard X-ray energies. Initial results for the remaining fields are discussed, and implications for an extended survey are mentioned. C1 UPS,CTR ETUD SPATIALE RAYONNEMENTS,CNRS,TOULOUSE,FRANCE. UNIV SPACE RES ASSOC,HUNTSVILLE,AL 35806. GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899. RP Grindlay, JE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C145 EP C148 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300029 ER PT J AU Manandhar, RP Grindlay, JE Thompson, DJ AF Manandhar, RP Grindlay, JE Thompson, DJ TI New EGRET/COMPTEL studies of globular clusters SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE pulsars, general; globular clusters, individual NGC 6397; globular clusters, individual NGC 6752; gamma rays, observations ID GAMMA-RAY EMISSION; MILLISECOND PULSARS; ECLIPSING BINARY; UPPER LIMITS; TERZAN-5 AB We present results of our Phase 2 program of observations of two nearby globular clusters, NGC 6397 and NGC 6752, with EGRET and COMPTEL to search for the integrated emission from their populations of millisecond pulsars, LMXBs (in quiescence), and CVs. Upper limits were derived for each cluster that are a factor of 2 more sensitive than in the general cluster survey of Michelson et al. (1994) using EGRET. Our COMPTEL limits are the first reported for the 1-30 MeV band for these clusters and are comparably sensitive to the EGRET limits for an assumed Crab-like spectrum yet can also constrain source spectra if they break at energies below 30 MeV. These limits are better than the COMPTEL limits recently reported for 47 Tuc by O'Flaherty et al. (1995). The lowest upper Limits, for NGC 6397, restrict the integrated luminosity to be below similar to 10(35) ergs s(-1) in either the COMPTEL or EGRET energy bands. A serendipitous source, GRO J1718-60, was detected (4.1 sigma) with EGRET, near (but not coincident with) NGC 6397. Although this source would be consistent with the nearby (1.7 degrees) pulsar J1704-60, the published spindown luminosity is too low for it to be a plausible counterpart. Constraints on the typical gamma-ray luminosity for millisecond pulsars and quiescent LMXBs are derived and discussed. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RI Thompson, David/D-2939-2012 OI Thompson, David/0000-0001-5217-9135 NR 33 TC 0 Z9 0 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C255 EP C260 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300057 ER PT J AU Narayan, R Yi, I Mahadevan, R AF Narayan, R Yi, I Mahadevan, R TI Advection-dominated accretion model of Sagittarius A* and other accreting black holes SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE black hole physics; gamma rays, theory; Galaxy, center ID SPECTRUM; GALAXY AB Viscous rotating accretion hows around black holes become advection-dominated when the accretion rate M over dot is sufficiently low. Most of the accretion energy in such flows is stored within the gas and advected radially inward. The temperature is therefore very high, and much of the radiation comes out in hard X-rays and gamma-rays. We have constructed an advection-dominated accretion flow model for the Galactic Center source Sagittarius A*. The model consists of a 7 10(5) M(.) black hole accreting at M over dot = 1.2 10(-5) alpha M(.)yr(-1), where alpha is the usual viscosity parameter. The model spectrum fits the observations from radio to gamma-rays quite well and explains the unusually low luminosity of the source. Since the model explicitly makes use of a horizon at the inner edge to swallow the advected energy, the success of the model strongly suggests that the central object in Sgr A* is a black hole. We further show that, if alpha is not much smaller than unity, then advection-dominated models can be applied even to higher luminosity black holes. The existence of Low and High States in black hole X-ray binaries, and the abrupt transition between the two states, find a natural explanation. The models also explain the close similarity in the hard X-ray/gamma-ray spectra of black hole X-ray binaries and active galactic nuclei. C1 INST ADV STUDY,PRINCETON,NJ 08540. RP Narayan, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 24 TC 3 Z9 3 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C287 EP C290 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300064 ER PT J AU Weekes, TC Akerlof, CW Biller, S Bird, D Boyle, P Bussons, J Buckley, J CarterLewis, DA Cawley, MF Catanese, M Chantell, M Connaughton, V Fegan, DJ Finley, J Gaidos, J Hillas, AM Lamb, RC Krennrich, F Lessard, R McEnery, J Meyer, DI Mohanty, G Quinn, J Rodgers, A Rose, HJ Sembroski, G Schubnell, MS Wilson, C Zweerink, J AF Weekes, TC Akerlof, CW Biller, S Bird, D Boyle, P Bussons, J Buckley, J CarterLewis, DA Cawley, MF Catanese, M Chantell, M Connaughton, V Fegan, DJ Finley, J Gaidos, J Hillas, AM Lamb, RC Krennrich, F Lessard, R McEnery, J Meyer, DI Mohanty, G Quinn, J Rodgers, A Rose, HJ Sembroski, G Schubnell, MS Wilson, C Zweerink, J TI Observations of gamma-ray sources at energies >300 GeV SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE galaxies, Mkn 421, Mkn 501; BL lacertae objects; gamma-rays, observations AB Results from recent observations with the Whipple Observatory gamma-ray telescope are reported; after the successful detection of Markarian (Mkn) 421 particular emphasis was put on the observation of nearby Bl Lacs. The Bl Lac, Mkn 501, which is similar to Mkn 421 in many ways, was detected for the first time as a gamma-ray source. Extensive coverage of Mkn 421 this season revealed unusual variability; one episode of intensity change in April, 1995 was measured with high statistical significance. Upper limits were found for a number of Bl Lacs with z < 0.1. C1 NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. UNIV MICHIGAN,RANDALL LAB PHYS,ANN ARBOR,MI 48109. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. IOWA STATE UNIV,DEPT PHYS & ASTRON,AMES,IA 50011. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. PURDUE UNIV,DEPT PHYS,W LAFAYETTE,IN 47907. RP Weekes, TC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,POB 97,AMADO,AZ 85645, USA. RI McEnery, Julie/D-6612-2012 NR 24 TC 0 Z9 0 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C603 EP C606 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300135 ER PT J AU Yi, I Narayan, R Barret, D McClintock, JE AF Yi, I Narayan, R Barret, D McClintock, JE TI Models of quiescent black hole and neutron star soft X-ray transients SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE accretion discs; black holes; X-rays, general ID ACCRETION AB When the mass accretion rate onto a black hole (BH) falls below a critical rate, over dotM(crit) similar to alpha(2)over dotM(Edd), accretion can occur via a hot optically thin flow where most of the dissipated energy is advected inward. We present such an advection-dominated model for the soft X-ray transient (SXT) A 0620-00. This source has a puzzlingly low X-ray luminosity in quiescence, similar to 6 10(30) erg s(-1) despite a relatively high mass accretion rate similar to 10(-10) M.yr(-1) deduced from its optical flux. The accreting gas makes a transition from a standard thin disc at large radii to an advection-dominated flow at small radii. The transition occurs when the effective temperature of the thin disc is similar to 10(4) K. Because of the very low accretion efficiency, similar to 10(-3) - 10(-4), in the inner flow, the model fits both the optical and X-ray data. We also present models for V404 Cyg and Nova Mus 1991 in quiescence. Quiescent neutron star (NS) transients are expected to appear very different from BH systems because the advected energy is re-radiated from the NS surface whereas a BH swallows the advected energy. We discuss models for NS SXTs. C1 INST ADV STUDY,PRINCETON,NJ 08540. RP Yi, I (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C187 EP C190 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300040 ER PT J AU Zhang, SN Harmon, BA Paciesas, WS Fishman, GJ Grindlay, JE Barret, D Tavani, M Kaaret, P Bloser, P Ford, E Titarchuk, L AF Zhang, SN Harmon, BA Paciesas, WS Fishman, GJ Grindlay, JE Barret, D Tavani, M Kaaret, P Bloser, P Ford, E Titarchuk, L TI Low state hard X-ray outburst from the X-ray burster 4U 1608-522 observed by BATSE/CGRO SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE stars, individual, 4U 1608-522; X-rays, stars; stars, neutron ID BINARIES AB A hard X-ray (low state) outburst lasting for about 170 days was observed with the Burst and Transient Source Experiment (BATSE) Large Area Detectors (LADs) from the X-ray burster 4U 1608-522 from June to December 1991. During the outburst, the flux slowly varied between 75 mCrab and 150 mCrab. Combined with a near simultaneous observation with the Ginga satellite, the low energy spectrum before the break energy is well determined to be a power law with photon index of about 1.75. The high energy spectrum above the break energy can be fit equally well by either the Sunyaev-Titarchuk (S-T) model or a broken power law model. For the first time, we have determined that a rather intense hard X-ray outburst from a neutron star system is associated with a soft X-ray (< 10 keV) low state and the power law photon spectrum breaks at about 65 keV. C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. COLUMBIA UNIV,DEPT PHYS,NEW YORK,NY 10027. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. GEORGE MASON UNIV,CSI,FAIRFAX,VA 22030. RP Zhang, SN (reprint author), UNIV SPACE RES ASSOC,HUNTSVILLE,AL 35806, USA. NR 24 TC 3 Z9 3 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C279 EP C282 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300062 ER PT J AU Zhang, SN Harmon, BA Paciesas, WS Fishman, GJ Finger, MH Robinson, CR Rubin, BC Grindlay, JE Barret, D Tavani, M Kaaret, P Bloser, P Ford, E AF Zhang, SN Harmon, BA Paciesas, WS Fishman, GJ Finger, MH Robinson, CR Rubin, BC Grindlay, JE Barret, D Tavani, M Kaaret, P Bloser, P Ford, E TI Periodic transient hard X-ray emission from GRO 1849-03 SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article; Proceedings Paper CT 3rd Compton Symposium CY JUN 12-14, 1995 CL MUNICH, GERMANY SP Max Planck Inst Extraterrestr Phys, Garching, Marx Planck Gesell, Deut Agentur Raumfahrtangelegenheiten, Deut Aerosp DE stars, individual, GRO 1849-03; X-rays, stars ID TIME-SERIES; SPACED DATA AB We have recently discovered periodic transient hard X-ray emission from a source, GRO 1849-03, possibly located in the 5 kpc arm of the galaxy, using archival BATSE data. The source produces hard X-ray outbursts at regular 241 day intervals. Each outburst lasts roughly 13 days, reaching a peak luminosity of 75 mCrab. The spectrum extends to at least 100 keV with a photon power law index of -2.8. We interpret the emission as due to close encounters between a compact object and a companion star in a binary system. C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. COLUMBIA UNIV,DEPT PHYS,NEW YORK,NY 10027. RP Zhang, SN (reprint author), UNIV SPACE RES ASSOC,HUNTSVILLE,AL 35806, USA. NR 23 TC 2 Z9 2 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD DEC PY 1996 VL 120 IS 4 SI SI BP C227 EP C230 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WC063 UT WOS:A1996WC06300049 ER PT J AU Ho, LC Filippenko, AV AF Ho, LC Filippenko, AV TI High-dispersion spectroscopy of a luminous, young star cluster in NGC 1705: Further evidence for present-day formation of globular clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, individual (NGC 1705, NGC 4214); galaxies, irregular galaxies, starburst; galaxies, star clusters; globular clusters, general ID SPACE-TELESCOPE OBSERVATIONS; GALAXY; M82; NGC-1705; MASS; STARBURST; NGC-1569; SPECTRA; SYSTEMS; SUPERGIANTS AB We present evidence that some of the compact, luminous, young star clusters discovered recently through images taken with the Hubble Space Telescope (HST) have masses comparable to those of old Galactic globular clusters. The ''super star cluster'' in the center of the nearby amorphous galaxy NGC 1705 has been observed with high dispersion at optical wavelengths using the HIRES echelle spectrograph on the Keck 10 m telescope. Numerous weak metal Lines arising from the atmospheres of cool supergiants have been detected in the integrated spectrum, permitting a direct measurement of the line-of-sight stellar velocity dispersion through cross-correlation with a template star; the result is sigma* = 11.4 +/- 1.5 km s(-1). Assuming that the system is gravitationally bound and using a cluster size measured from HST images, we apply the virial theorem to obtain the dynamical mass. Its derived mass [(8.2 +/- 2.1) x 10(4) M.], mass density (2.7 +/- 10(4) M. pc(-3)), and predicted mass-to-light ratio after aging by 10-15 Gyr [0.6-1.6 (M/L(V)).] closely resemble those of the majority of evolved Galactic globular clusters. The central cluster in NGC 1705 appears to be very similar in nature to one of the bright clusters in NGC 1569, which was discussed earlier this year by Ho & Filippenko. We also observed the brightest cluster in the Magellanic irregular galaxy NGC 4214, but no lines suitable for measuring its velocity dispersion were detected, most likely because of the very young age of the cluster. Although these observations need to be extended to a much larger sample of objects before generalizations can be made concerning the nature of similar clusters observed in other galaxies, our preliminary results are tantalizing and strongly suggest that, at least in two cases, we are witnessing globular clusters in their extreme youth. C1 UNIV CALIF BERKELEY, DEPT ASTRON, BERKELEY, CA 94720 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 78 TC 136 Z9 137 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1996 VL 472 IS 2 BP 600 EP 610 DI 10.1086/178091 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VW210 UT WOS:A1996VW21000017 ER PT J AU Ho, PTP Young, LM AF Ho, PTP Young, LM TI The contracting molecular cores e1 and e2 in W51 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual (W51); ISM, kinematics and dynamics; radio lines, ISM ID STAR-FORMING REGION; H-II-REGIONS; H2O MASER SOURCES; PROPER MOTIONS; AMMONIA MASER; GAS DISK; G10.6-0.4; COLLAPSE; DISTANCES; TAURI AB We report on observations of the star-forming region W51 in the NH3 (J, K)=(1, 1) and (2, 2) transitions at 1.3 cm. These observations have much greater sensitivity than our previous observations and they allow a kinematic analysis of the motions of the gas in two small star-forming cores. We present evidence for radial contraction of the gas in W51 e2 onto a young star and possibly also for similar contraction near W51 el. The H II region/molecular core W51 e2 seems to be in a stage where the central star has already arrived on the main sequence, whereas the cooler gas on scales of 0.1-0.2 pc is still. contracting onto the mass concentration at the center. In contrast to the interpretation of Rudolph et al., we propose that the contraction extends only over a few tenths of a parsec near e2 instead of over the entire W51 molecular cloud complex. C1 UNIV ILLINOIS,URBANA,IL 61801. RP Ho, PTP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 28 TC 31 Z9 32 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1996 VL 472 IS 2 BP 742 EP 754 DI 10.1086/178103 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VW210 UT WOS:A1996VW21000029 ER PT J AU Soon, WH Posmentier, ES Baliunas, SL AF Soon, WH Posmentier, ES Baliunas, SL TI Inference of solar irradiance variability from terrestrial temperature changes, 1880-1993: An astrophysical application of the sun-climate connection SO ASTROPHYSICAL JOURNAL LA English DT Article DE earth; solar-terrestrial relations; Sun, activity; Sun, fundamental parameters ID NORTH-SOUTH ASYMMETRY; ATMOSPHERIC CARBON-DIOXIDE; SURFACE AIR TEMPERATURES; GREENHOUSE GASES; CYCLE LENGTH; LUMINOSITY VARIATIONS; SULFATE AEROSOLS; TERM VARIATIONS; GLOBAL CLIMATE; BRIGHTNESS AB Information can be inferred on the timing and amplitude of solar total irradiance changes over 1880-1993 by simulating the global terrestrial surface temperature changes produced by these irradiance changes and comparing them with observed temperatures. The profiles of solar irradiance variations used in the climate simulations are adopted from several different proxies: (1) the length of the sunspot cycle, (2) the mean sunspot number, and (3) a composite proxy that includes the two previous indicators plus the equatorial solar rotation rate, the fraction of penumbral spot coverage, and the rate of decay of the sunspot cycle. We use a seasonal energy-conservation climate/upwelling-diffusion ocean model, forced by the assumed profiles of solar total irradiance variations, combined with variations in anthropogenic greenhouse gases. Optimized cases imply total irradiance changes during 1880-1993 in the range 0.18%-0.77%. If the solar irradiance profiles found from the climate simulations are required to be consistent with recent satellite observations, then the composite solar profile reconstructed by Hoyt & Schatten, combined with the anthropogenic greenhouse forcing, explains the highest fraction of the variance of observed global mean temperatures. In this case, the solar and greenhouse combination accounts for 92% of the observed long-term temperature variance during 1880-1993. The simulation implies that the solar part of the forcing alone would account for 71% of the global mean temperature variance, compared to 51% for the greenhouse gases' part alone. It also suggests a solar total irradiance variation of 0.5% during the interval 1880-1993. Such an amplitude of solar total irradiance change is consistent with astrophysical limits of brightness changes on timescales of decades to centuries independently derived from observations of solar-type stars (including the Sun). C1 MT WILSON OBSERV, MT WILSON, CA 91023 USA. LONG ISL UNIV, DIV SCI, BROOKLYN, NY 11201 USA. TENNESSEE STATE UNIV, CTR AUTOMATED SPACE SCI, NASHVILLE, TN 37203 USA. TENNESSEE STATE UNIV, CTR EXCELLENCE INFORMAT SYST, NASHVILLE, TN 37203 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 86 TC 55 Z9 56 U1 1 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1996 VL 472 IS 2 BP 891 EP 902 DI 10.1086/178119 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VW210 UT WOS:A1996VW21000045 ER PT J AU Hoflich, P Khokhlov, A Wheeler, JC Phillips, MM Suntzeff, NB Hamuy, M AF Hoflich, P Khokhlov, A Wheeler, JC Phillips, MM Suntzeff, NB Hamuy, M TI Maximum brightness and postmaximum decline of light curves of type supernovae Ia: A comparison of theory and observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, observations; cosmology, theory; distance scale; supernovae, general ID MEASURING EXTRAGALACTIC DISTANCES; 1991BG; MODELS AB We compare the observed correlations between the maximum brightness, postmaximum decline rate, and color at maximum light of Type Ia supernovae (SNs Ia) with model predictions. The observations are based on a total of 40 SNs Ia, including 29 SN of the Calan Tololo Supernova Search and 11 local SNs which cover a range of approximate to 2 mag in the absolute visual brightness. The observed correlations are not tight, one dimensional relations. Supernovae with the same postmaximum decline or the same color have a spread in visual magnitude of approximate to 0.7 mag. The dispersion in the color-magnitude relation may result from uncertainties in the distance determinations or the interstellar reddening within the host galaxy. The dispersion in the decline rate-magnitude relation suggests that an intrinsic spread in the supernova properties exists that cannot be accounted for by any single relation between visual brightness and postmaximum decline. Theoretical correlations are derived from a grid of models which encompasses delayed detonations, pulsating delayed detonations, the merging scenario, and helium detonations. We find that the observed correlations can be understood in terms of explosions of Chandrasekhar mass white dwarfs. Our models show an intrinsic spread in the relations of about 0.5 mag in the maximum brightness and approximate to 0.1 mag in the B-V color. Our study provides strong evidence against the mechanism of helium detonation for subluminous, red SNs Ia. C1 UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. UNIV BASEL,INST THEORET PHYS,CH-4056 BASEL,SWITZERLAND. USN,RES LAB,COMPUTAT PHYS & FLUID DYNAM LAB,WASHINGTON,DC 20375. CTIO,LA SERENA,CHILE. CTIO,TUCSON,AZ 85719. RP Hoflich, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Hamuy, Mario/G-7541-2016 NR 45 TC 85 Z9 85 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1996 VL 472 IS 2 BP L81 EP L84 DI 10.1086/310363 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VW211 UT WOS:A1996VW21100005 ER PT J AU Mirabel, IF Rodriguez, LF Chaty, S Sauvage, M Gerard, E Duc, PA CastroTirado, A Callahan, P AF Mirabel, IF Rodriguez, LF Chaty, S Sauvage, M Gerard, E Duc, PA CastroTirado, A Callahan, P TI Infrared observations of an energetic outburst in GRS 1915+105 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared, stars; radio continuum, stars; stars, individual (GRS 1915+105); X-rays, bursts; X-rays, stars ID X-RAY TRANSIENT AB In the course of an intense X-ray and radio outburst of GRS 1915+105, we observed a pair of radio-emitting clouds emerging from the compact core in opposite directions at relativistic speeds. At near-infrared wavelengths we observed the time-delayed reverberation of this radio flare/ejection event. Five days after the radio outburst, the source became redder as it brightened by similar to 1 mag in K(2.2 mu m), which suggests the appearance of a warm dust component. The enhanced infrared emission was close to 10% of the X-ray luminosity of the source and amounts to about 0.1% of the typical kinetic energy in the bulk motion of the relativistic ejecta in GRS 1915+105. C1 INST ASTRON & FIS ESPACIO,RA-1428 BUENOS AIRES,DF,ARGENTINA. UNIV NACL AUTONOMA MEXICO,INST ASTRON,MEXICO CITY 04510,DF,MEXICO. OBSERV PARIS,SECT MEUDON,DEPT ARPEGES,F-92195 MEUDON,FRANCE. EUROPEAN SO OBSERV,D-85748 GARCHING,GERMANY. INTA,LAB ASTROFIS ESPACIAL & FIS ESPACIAL,E-28080 MADRID,SPAIN. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP Mirabel, IF (reprint author), CTR ETUD SACLAY,DSM,DAPNIA,CEA,SERV ASTROPHYS,F-91191 GIF SUR YVETTE,FRANCE. NR 19 TC 30 Z9 30 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1996 VL 472 IS 2 BP L111 EP L114 DI 10.1086/310364 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VW211 UT WOS:A1996VW21100012 ER EF