FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Richmond, BG Fleagle, JG Kappelman, J Swisher, CC AF Richmond, BG Fleagle, JG Kappelman, J Swisher, CC TI First hominoid from the Miocene of Ethiopia and the evolution of the catarrhine elbow SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Review DE fossil apes; anthropoids; postcranium; forelimb; Turkanapithecus; Pliopithecus; multivariate analysis ID PHYLOGENETIC-RELATIONSHIPS; NORTHEASTERN HUNGARY; ANTHROPOID PRIMATES; NORTHERN KENYA; AGE; LOCOMOTION; MORPHOLOGY; RUDABANYA; HOMINIDS; BULUK AB The first known fossil ape from the early-middle Miocene of Fejej, Ethiopia, is described here. The specimen, FJ-18SB-68, is a partial ulna from a locality dated by (40)Ar/(39)Ar and paleomagnetic methods to a minimum age of 16.18 MYA. Compared to a variety of extant and fossil ulnae, FJ-18SB-68 is most similar to Turkanapithecus, Proconsul, and Pliopithecus, and appears to have been an arboreal quadruped with substantial forearm rotational mobility. Among the extant ulnae, canonical variates analysis successfully discriminates platyrrhines from catarrhines and within the latter, cercopithecoids from hominoids. Basal catarrhines (e.g., Aegyptopithecus) are platyrrhine-like in their morphology. Two basic trends appear to evolve from this generalized template: one with less mobile and more habitually pronated forearms, as seen in living and fossil cercopithecoids (including Victoriapithecus and Paracolobus), and another with greater forearm rotational mobility in fossil and modern hominoids. Primitive Miocene apes, including Proconsul, Turkanapithecus, and FJ-18SB-68, share with extant hominoids a more laterally positioned and laterally facing radial notch and an incipient trochlear keel. This morphology, along with a large insertion area for m. brachialis, suggests a departure from the more habitually pronated hand posture of monkeys and may indicate greater climbing abilities in these arboreally quadrupedal apes. Later Miocene apes, such as Oreopithecus and Dryopithecus share additional morphological features with hominoids, indicating considerable suspensory and climbing capabilities. (C) 1998 Wiley-Liss, Inc. C1 Smithsonian Inst, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. SUNY Stony Brook, Dept Anat Sci, Sch Med, Stony Brook, NY 11794 USA. Univ Texas, Dept Anthropol, Austin, TX 78712 USA. Berkeley Geochronol Ctr, Berkeley, CA 94709 USA. RP Richmond, BG (reprint author), Smithsonian Inst, Dept Anthropol, Human Origins Program, MRC 112, Washington, DC 20560 USA. EM Richmond.Brian@NMNH.SI.EDU NR 104 TC 23 Z9 24 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 1998 VL 105 IS 3 BP 257 EP 277 PG 21 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA ZD548 UT WOS:000072697600001 PM 9545073 ER PT J AU Jivoff, P Hines, AH AF Jivoff, P Hines, AH TI Female behaviour, sexual competition and mate guarding in the blue crab, Callinectes sapidus SO ANIMAL BEHAVIOUR LA English DT Article ID CENTRAL CHESAPEAKE BAY; WATER STRIDER; MATING-BEHAVIOR; GAMMARUS-PULEX; SCATOPHAGA-STERCORARIA; REPRODUCTIVE-BEHAVIOR; ORCONECTES-RUSTICUS; HOMARUS-AMERICANUS; PREDATION RISK; SELECTION AB Blue crabs mate immediately after the female's final moult. We tested the influence of female moult stage, sex ratio and male size on the pre-mating behaviour of both sexes, and the ability of males to pair with females and aggressively compete for access to females. We observed crabs in field enclosures and surveyed pre-copulatory mate-guarding patterns in the field. Female behaviour changed as they progressed through the final moult cycle, such that early moult-stage females avoided males, but late moult-stage females initiated pair formation. The changes in female behaviour influenced both the behaviour and pairing capability of males. Males courted and paired with late moult-stage females on their first attempt, but pursued early moult-stage females because their first attempts to pair often failed. In the field, early moult-stage females were paired less often than late moult-stage females. The pre-mating behaviour of both sexes also varied with sex ratio; when males were abundant, males traded courtship for forced capture and females courted less. Large males were more successful at take-overs, but did not pair more often with late moult-stage females, suggesting that large males do not consistently guard for less time than small males. The changes in female behaviour are consistent with the female's need to avoid the costs of guarding and suggest that females influence how pre-copulatory mate guarding occurs in this species. (C) 1998 The Association for the Study of Animal Behaviour. C1 Univ Maryland, Dept Zool, College Pk, MD 20742 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Jivoff, P (reprint author), Rutgers State Univ, Marien Field Stn, 800 Great Bay Blvd, Tuckerton, NJ 08087 USA. EM jivoff@ahab.rutgers.edu NR 66 TC 52 Z9 54 U1 0 U2 9 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD MAR PY 1998 VL 55 BP 589 EP 603 DI 10.1006/anbe.1997.0646 PN 3 PG 15 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA ZE497 UT WOS:000072798800009 ER PT J AU Kime, NM Rand, AS Kapfer, M Ryan, MJ AF Kime, NM Rand, AS Kapfer, M Ryan, MJ TI Consistency of female choice in the tungara frog: a permissive preference for complex characters SO ANIMAL BEHAVIOUR LA English DT Article ID SEXUAL SELECTION; PHYSALAEMUS-PUSTULOSUS; SENSORY EXPLOITATION; MATE CHOICE; REPEATABILITY; MODEL AB Previous phonotaxis experiments in the tungara frog, Physalaemus pustulosus, indicated a permissiveness in female preference that allows sexually selected complex call characters to be replaced with various alternative characters. Although they prefer complex to simple calls, females as a group did not discriminate between several alternative complex characters appended to the simple conspecific call. However, these studies did not address the possibility that the apparent permissiveness in female preference occurred because of an averaging of population data. The observed patterns in female preference could result from all females finding a certain set of call variants equally attractive, or from a polymorphism in female call preference. To discriminate between these two alternatives,; consistency of mate choice was determined for three pairs of calls that elicited no phonotactic bias in population studies. Individual females did not repeatedly choose one stimulus of a pair over the other, demonstrating that the patterns of permissiveness observed in the population are paralleled by similar patterns within females. A broad preference for complex calls in the P. pustulosus species group would permit the evolution of sexually selected call variation through sensory exploitation. (C) 1998 The Association for the Study of Animal Behaviour. C1 Univ Texas, Dept Zool, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Vienna, Inst Zool, A-1010 Vienna, Austria. RP Kime, NM (reprint author), Univ Texas, Dept Zool, Austin, TX 78712 USA. EM nmkime@mail.utexas.edu NR 22 TC 30 Z9 32 U1 0 U2 8 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD MAR PY 1998 VL 55 BP 641 EP 649 DI 10.1006/anbe.1997.0752 PN 3 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA ZE497 UT WOS:000072798800013 ER PT J AU Kaluzny, J Stanek, KZ Krockenberger, M Sasselov, DD Tonry, JL Mateo, M AF Kaluzny, J Stanek, KZ Krockenberger, M Sasselov, DD Tonry, JL Mateo, M TI Direct distances to nearby galaxies using detached eclipsing binaries and Cepheids. I. Variables in the field M31B SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries, eclipsing; Cepheids; galaxies, distances and redshifts; galaxies, individual (M31); Local Group ID PHOTOMETRY; STARS AB We have undertaken a long-term project, DIRECT, to obtain the direct distances to two important galaxies in the cosmological distance ladder - M31 and M33 - using detached eclipsing binaries (DEBs) and Cepheids. While rare and difficult to detect. DEBs provide us with the potential to determine these distances with an accuracy better than 5%. The extensive photometry obtained in order to detect DEBs provides us with good light curves for the Cepheid variables. These are essential to the parallel project to derive direct Baade-Wesselink distances to Cepheids in M31 and M33. For both Cepheids and eclipsing binaries, the distance estimates will be free of any intermediate steps. As a first step in the DIRECT project, between 1996 September and 1997 January we obtained 36 full nights on the Michigan-Dartmouth-MIT Observatory 1.3 m telescope and 45 full/partial nights on the F. L. Whipple Observatory 1.2 m telescope to search for DEBs and new Cepheids in the M31 and M33 galaxies. In this paper, first in a series, we present the catalog of variable stars, most of them newly detected, found in the field M31B [(alpha, delta) = (11.degrees 20, 41.degrees 59), J2000.0]. We have found 85 variable stars: 12 eclipsing binaries, 38 Cepheids, and 35 other periodic, possible long-period or nonperiodic variables. The catalog of variables, as well as their photometry and finding charts, is available via anonymous ftp and the World Wide Web. C1 Warsaw Univ Observ, PL-00478 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Kaluzny, J (reprint author), Warsaw Univ Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. EM jka@sirius.astrouw.edu.pl; kstanek@cfa.harvard.edu; krocken@cfa.harvard.edu; sasselov@cfa.harvard.edu; jt@avidya.ifa.hawaii.edu; mateo@astro.lsa.umich.edu NR 35 TC 89 Z9 89 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1998 VL 115 IS 3 BP 1016 EP 1044 DI 10.1086/300235 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZB173 UT WOS:000072443700013 ER PT J AU Oppenheimer, BD Kenyon, SJ Mattei, JA AF Oppenheimer, BD Kenyon, SJ Mattei, JA TI An analysis of AAVSO observations of Z Camelopardalis SO ASTRONOMICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars, individual (Z Camelopardalis); stars, variables, other ID DWARF NOVAE; VARIABLES; OUTBURST; PERIODS; STARS; CYGNI AB We analyze the AAVSO light curve for the cataclysmic variable Z Camelopardalis. The light curve includes 51,086 observations over 67 years. We classify outbursts into three main categories--common, plateau, and anomalous--based on the shape and duration of the outburst. Plateau outbursts are brighter and last longer than common outbursts. Some outbursts end in standstills in which the brightness stays constant roughly 1 mag below maximum light for a few days to 1000 days. The average energy output in a standstill is larger than that during an outburst cycle. FLU outbursts follow a pattern, the plateau outburst cycle, in which one or more common or anomalous outbursts occur between two plateau outbursts or a plateau outburst and a standstill. Short quiescent durations lead to a higher outburst frequency and more energetic outbursts in intervals dominated by standstills than in other lightcurve intervals. Our physical picture for Z Camelopardalis stars follows the standard disk instability mechanism for dwarf novae. The plateau outburst cycle is a series of minor, common "inside out" outbursts that lead to a major, plateau outburst that empties the accretion disk. Standstills occur when the mass transfer rate from the secondary star into the accretion disk surrounding the primary star is too large to produce dwarf nova outbursts. The system resembles a nova-like variable during standstill; it returns to the plateau outburst cycle when the mass transfer fate declines below some critical level. Our analysis suggests that irradiation of the secondary does not play a significant role in the evolution of M over dot. Solar-type magnetic cycles are a more plausible mechanism. C1 Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Oppenheimer, BD (reprint author), Amer Assoc Variable Star Observers, 25 Birch St, Cambridge, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 22 TC 15 Z9 15 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1998 VL 115 IS 3 BP 1175 EP 1189 DI 10.1086/300250 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZB173 UT WOS:000072443700027 ER PT J AU Dahmen, G Huttemeister, S Wilson, TL Mauersberger, R AF Dahmen, G Huttemeister, S Wilson, TL Mauersberger, R TI Molecular gas in the Galactic center region - II. Gas mass and N-H2/I-12(CO) conversion based on a (CO)-O-18(J=1 -> 0) survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy : center; radiative transfer; ISM : molecules; ISM : structure; galaxies : nuclei; radio lines : ISM ID CARBON-MONOXIDE EMISSION; RADIAL-DISTRIBUTION; INTERSTELLAR-MEDIUM; GAMMA-RAYS; CLOUDS; GALAXY; IC-342; KINEMATICS; NUCLEUS; NGC-253 AB The large scale structure and physics of molecular gas in the Galactic center region is discussed based on the detailed analysis of a 9' resolution survey of the Galactic center region in the J = 1 --> 0 line of (CO)-O-18. Emphasis is placed on the comparison with (CO)-C-12(1-0) data. The line shapes of (CO)-O-18(1-0) and (CO)-C-12(1-0) differ significantly. The ratio of the intensities of the two isotopomers in the Galactic center region is generally higher than the value of similar to 15 expected from the "Standard Conversion Factor" (SCF) of (CO)-C-12 integrated line intensity to H-2 column density. In the 9'-beam, this ratio is in the range from 30 to 200, mostly similar to 60 to 80. From LVG calculations, we estimate that the large scale (CO)-C-12(1-0) emission in the Galactic center region is of moderate (tau greater than or similar to 1) or low optical depth (tau < 1). Higher optical depths (tau greater than or equal to 10) are restricted to very limited regions such as SgrB2. In addition, we estimate H-2 densities and kinetic temperatures for different ranges of intensity ratios. A considerable amount of molecular mass is in a widespread molecular gas component with low densities and high kinetic temperatures. From our (CO)-O-18 measurements and from results based on dust measurements, the total molecular mass is found to be (3(-1)(+2)) . 10(7) M.. We show that the SCF is not valid toward the Galactic bulge. It overestimates the H-2 column density by an order of magnitude because the assumptions required for this factor of optically thick (CO)-C-12 emission and virialization of the molecular clouds are not fulfilled for a significant fraction of the molecular gas. Therefore, also one cannot apply a modified conversion factor to the Galactic center region since the N-H2/I-12CO ratio is highly variable and cannot be represented by a universal constant. Results from external galaxies indicate that the (CO)-C-12 emission is generally not a suitable tracer of H-2 masses in galactic bulges. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ London Queen Mary & Westfield Coll, Dept Phys, London E1 4NS, England. Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. Univ Arizona, Submillimeter Telescope Observ, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Huttemeister, S (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. NR 63 TC 106 Z9 108 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 MAR PY 1998 VL 331 IS 3 BP 959 EP 976 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZD690 UT WOS:000072713100029 ER PT J AU Keeton, CR Kochanek, CS AF Keeton, CR Kochanek, CS TI Gravitational lensing by spiral galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, spiral; galaxies, structure; gravitational lensing ID SMALLEST EINSTEIN RING; SURFACE MASS DENSITY; X-RAY CONSTRAINTS; DARK-MATTER; GALACTIC DISK; ABSORPTION; SYSTEM; LENSES; PKS1830-211; STATISTICS AB We study gravitational lensing by spiral galaxies, using realistic models consisting of halo, disk, and bulge components combined to produce a flat rotation curve. Proper dynamical normalization of the models is critical because a disk has less (projected) mass than does a spherical halo with the same rotation curve--a face-on Mestel disk has a lensing cross section only 41% as large as that of a comparable singular isothermal sphere. Lensing cross sections are sensitive to inclination and are dominated by edge-on galaxies that, if very flattened, produce a large number of lenses with an unobserved image geometry consisting of 2 or 3 images off to one side of the galaxy center and straddling the projected disk. The absence of this "disk" image geometry among known lenses suggests that lens galaxies cannot be highly flattened. When averaged over inclination, disk + halo models predict less than or similar to 10% more lenses than do pure halo models, except in cases in which the disk is unreasonably massive, so including a disk does not significantly increase the expected number of spiral galaxy lenses. Models with an exponential disk and a central bulge are sensitive to the properties of the bulge. In particular, an exponential disk model normalized to our Galaxy but without a bulge cannot produce multiple images, and including a bulge reduces the net flattening of edge-on galaxies. The dependence of the lensing properties on the masses and shapes of the halo, disk, and bulge means that a sample of spiral galaxy lenses would provide useful constraints on galactic structure. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keeton, CR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM ckeeton@cfa.harvard.edu; ckochanek@cfa.harvard.edu NR 67 TC 110 Z9 111 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1998 VL 495 IS 1 BP 157 EP 169 DI 10.1086/305272 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZA394 UT WOS:000072359100013 ER PT J AU Hartmann, L Calvet, N Gullbring, E D'Alessio, P AF Hartmann, L Calvet, N Gullbring, E D'Alessio, P TI Accretion and the evolution of T Tauri disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars, formation; stars, pre-main-sequence ID SPECTRAL ENERGY-DISTRIBUTIONS; SUBMILLIMETER CONTINUUM FLUX; LOCAL SHEAR INSTABILITY; WEAKLY MAGNETIZED DISKS; MAIN-SEQUENCE STARS; SOLAR NEBULA; YOUNG STARS; CIRCUMSTELLAR DISKS; ROTATIONAL EVOLUTION; MODELS AB Using results and calibrations from a previous paper (Gullbring et al. 1997), we estimate disk accretion rates for pre-main-sequence stars in the Taurus and Chamaeleon I molecular cloud complexes. The median accretion rate for T Tauri stars of age similar to 1 Myr is similar to 10(-8) M. yr(-1); the intrinsic scatter at a given age may be as large as 1 order of magnitude. There is a clear decline of mass accretion rates (M) over dot with increasing age t among T Tauri stars. Representing this decline as (M) over dot proportional to t(-eta), we estimate 1.5 less than or similar to eta less than or similar to 2.8; the large uncertainty is due to the wide range of accretion rates at a given age, the limited age range of the sample, and errors in estimating stellar ages and accretion luminosities. Adopting values of eta near the low end of this range, which are more likely given probable errors and the neglect of birthline age corrections, masses accreted during the T Tauri phase are roughly consistent with disk masses estimated from millimeter-wave dust emission. Similarity solutions for evolving, expanding disks are used to investigate observational constraints on disk properties employing a minimum of parameters. For an assumed power-law form of the disk viscosity with radius nu proportional to R(gamma), eta greater than or similar to 1.5 1.5 corresponds to gamma greater than or similar to 1. The limit gamma similar to 1 corresponds to a roughly constant "alpha" in the Shakura-Sunyaev (1973) viscosity parameterization; using current observed disk sizes, we estimate alpha similar to 10(-2) (on scales similar to 10-100 AU). Much of the observed variation in mass accretion rates can be accounted for by varying initial disk masses between 0.01 and 0.2 M., but this result may be strongly affected by the presence of binary companion stars. These results emphasize the need for older samples of stars for studying disk evolution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Invest Astron, Merida, Venezuela. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lhartmann@cfa.harvard.edu; ncalvet@cfa.harvard.edu; egullbring@cfa.harvard.edu; dalessio@astroscu.unam.mx NR 69 TC 765 Z9 766 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1998 VL 495 IS 1 BP 385 EP 400 DI 10.1086/305277 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZA394 UT WOS:000072359100034 ER PT J AU Kennelly, EJ Brown, TM Kotak, R Sigut, TAA Horner, SD Korzennik, SG Nisenson, P Noyes, RW Walker, A Yang, S AF Kennelly, EJ Brown, TM Kotak, R Sigut, TAA Horner, SD Korzennik, SG Nisenson, P Noyes, RW Walker, A Yang, S TI The oscillations of tau pegasi SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, individual (tau Pegasi); stars, oscillations ID LINE-PROFILE VARIATIONS; DELTA-SCUTI STARS; SIMULTANEOUS INTENSIVE PHOTOMETRY; HIGH-RESOLUTION SPECTROSCOPY; NONRADIAL PULSATIONS; MODE-IDENTIFICATION; THETA(2) TAURI; SPECTROGRAPH; CAMPAIGN; ROTATION AB We present extensive spectroscopic time series observations of the multiperiodic, rapidly rotating, delta Scuti star tau Pegasi. Information about the oscillations is contained within the patterns of line-profile variation of the star's blended absorption-line spectrum. We introduce the new technique of Doppler deconvolution with which to extract these patterns by modeling the intrinsic stellar spectrum and the broadening functions for each spectrum in the time series. Frequencies and modes of oscillation are identified from the variations using the technique of Fourier-Doppler imaging and a two-dimensional least-squares cleaning algorithm. We find a rich mode spectrum with degrees up to l = 20 and with frequencies below about 35 cycles day(-1). Those modes with the largest amplitudes have frequencies that lie within a narrow band. We conclude that the observed spectrum can be explained if the modes of tau Peg propagate in the prograde direction with l similar or equal to \m\ and with frequencies that are about equal in the corotating frame of the star. We discuss the implications of these results for the prospect of delta Scuti seismology. C1 Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ British Columbia, Dept Geophys & Astron, Vancouver, BC V6T 1Z4, Canada. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. RP Kennelly, EJ (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA. EM kennelly@hao.ucar.edu; brown@hao.ucar.edu; kotak@hao.ucar.edu; sigut@hao.ucar.edu; horner@astro.psu.edu; skorzennik@cfa.harvard.edu; pnisenson@cfa.harvard.edu; rnoyes@cfa.harvard.edu; awalker@astro.ubc.ca; yang@otter.phys.uvic.ca OI Kotak, Rubina/0000-0001-5455-3653 NR 49 TC 27 Z9 27 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1998 VL 495 IS 1 BP 440 EP 457 DI 10.1086/305268 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZA394 UT WOS:000072359100040 ER PT J AU Karpen, JT Antiochos, SK DeVore, CR Golub, L AF Karpen, JT Antiochos, SK DeVore, CR Golub, L TI Dynamic responses to magnetic reconnection in solar arcades SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; Sun, chromosphere; Sun, magnetic fields ID X-RAY JETS; H-ALPHA SURGES; EXPLOSIVE EVENTS; TELESCOPE; FLUX; ACCELERATION; ATMOSPHERE; MECHANISM; FIELDS; MODEL AB We present a numerical simulation of the interaction between two line dipoles through magnetic reconnection in the lower solar atmosphere, a process believed to be the origin of many manifestations of solar activity. This work differs from previous studies in that the held is sheared asymmetrically and that the dipoles have markedly unequal held strengths. This calculation already yielded one key discovery, denoted reconnection driven current filamentation, as described in a previous Astrophysical Journal letter. In this paper we focus on the chromospheric and coronal dynamics resulting from the shear-driven reconnection of unequal dipoles, discuss the important implications for chromospheric eruptions, compare our calculation with high-resolution Normal Incidence X-Ray Telescope observations of a surge, and contrast our results with the predictions of "fast reconnection" models. C1 USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. USN, Res Lab, Computat Phys & Fluid Dynam Lab, Washington, DC 20375 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Karpen, JT (reprint author), USN, Res Lab, EO Hulburt Ctr Space Res, Code 7670, Washington, DC 20375 USA. RI Karpen, Judith/E-1484-2012; Antiochos, Spiro/D-4668-2012; DeVore, C/A-6067-2015; OI Antiochos, Spiro/0000-0003-0176-4312; DeVore, C/0000-0002-4668-591X; Golub, Leon/0000-0001-9638-3082 NR 45 TC 60 Z9 60 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 MAR 1 PY 1998 VL 495 IS 1 BP 491 EP 501 DI 10.1086/305252 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZA394 UT WOS:000072359100044 ER PT J AU Cox, P Boulanger, F Huggins, PJ Tielens, AGGM Forveille, T Bachiller, R Cesarsky, D Jones, AP Young, K Roelfsema, PR Cernicharo, J AF Cox, P Boulanger, F Huggins, PJ Tielens, AGGM Forveille, T Bachiller, R Cesarsky, D Jones, AP Young, K Roelfsema, PR Cernicharo, J TI Infrared imaging and spectroscopy of the helix with ISOCAM SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared, ISM, lines and bands; planetary nebulae, individual (NGC 7293); stars, AGB and post-AGB; stars, mass loss ID PLANETARY-NEBULAE; LINE EMISSION; CENTRAL STARS; NGC-7293; H-2; ENVELOPES; SPECTRUM; GLOBULES; CO AB We report infrared images of the Helix Nebula centered at 6.9 mu m (LW3 filter) and 15 mu m (LW3 filter) obtained with ISOCAM on board the Infrared Space Observatory (ISO). Three fields were also measured using the ISOCAM circular variable filter (CVF). The CVF data show that the 5-16.6 mu m spectrum is dominated by the pure (v = 0-0) rotational lines of molecular hydrogen from the S(7) to the S(2) transitions. The strong S(5) H-2 line accounts for most of the emission detected in the LW2 filter. The only atomic lines detected are [Ne II] 12.81 mu m and [Ar III] 8.99 mu m, which are weak, and [Ne III] 15.55 mu m, which is strong and accounts for most of the emission in the LW3 filter. No emission bands or continuum of small dust particles are detected despite the carbon richness of the Helix Nebula. The H-2 emission traces the individual cometary globules of the molecular envelope of the nebula, whereas the [Ne III] emission is distributed along this envelope toward the inner regions of the ionized cavity. The intensities of H-2 rotational lines are accurately predicted using a rotational temperature of 900 +/- 50 K and column densities of similar to 3 x 10(18) cm(-2). The total luminosity in the H-2 lines similar to 4 L-circle dot (6% of the star luminosity) is much higher than predicted for photodissociation regions. The significant absence of mid-infrared dust. features indicates that in this evolved planetary nebula, the molecular-sized dust particles might have been destroyed by the exposure to the radiation field from the central hot star. C1 Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. NYU, Dept Phys, New York, NY 10003 USA. SRON, NL-9700 AV Groningen, Netherlands. Observ Grenoble, F-38041 Grenoble, France. Observ Astron Nacl IGN, Alcala De Henares 28800, Spain. Smithsonian Astrophys Lab, Cambridge, MA 02138 USA. CSIC, Inst Estructura Mat, E-28006 Madrid, Spain. RP Cox, P (reprint author), Univ Paris 11, Inst Astrophys Spatiale, Bat 425, F-91405 Orsay, France. RI Appourchaux, Thierry/F-4692-2010 NR 29 TC 23 Z9 23 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1998 VL 495 IS 1 BP L23 EP + DI 10.1086/311212 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZA395 UT WOS:000072359200006 ER PT J AU Girart, JM Estalella, R Ho, PTP AF Girart, JM Estalella, R Ho, PTP TI On the nature of the molecular condensation downstream from HH 80 North SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual, KH 80 North; ISM, jets and outflows; ISM, molecules; radio lines, ISM; stars, formation ID HERBIG-HARO OBJECTS; STAR-FORMING REGIONS; EMISSION; AMMONIA; CS; CLOUDS; CORES; LINE; NH3 AB We present HCO+ (J = 3 --> 2), (HCO+)-C-13 (J = 3 --> 2), CS (J = 5 --> 4), and (CO)-C-13 (J = 2 --> 1) Caltech Submillimeter Observatory observations toward the dense quiescent clump downstream from HH 80 North. This condensation is one in a class of sources that show anomalous molecular abundances, probably produced by UV radiation from a nearby shock. The HCO+ emission properties-location, size, center velocity, line widths, and excitation temperature-are similar to those of the ammonia emission, suggesting that it arises from the same region. The (HCO+)-C-13 (J = 3 --> 2) and CS (J = 5 --> 4) lines are marginally detected. Comparison between NH3, HCO+, and CS implies an ammonia enhancement relative to CS of at least I order of magnitude, whereas HCO+ shows only a weak enhancement relative to CS. These results are compatible with the radiative shock-induced chemistry models (Taylor & Williams; Wolfire & Konigl) when we take into account the extinction. Our results suggest that the dense clump detected in NH3 and HCO+ is illuminated by HH 80 North, making this region a good laboratory for studying the chemical processes in a quiescent clump radiatively excited by shocks. C1 Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Girart, JM (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61821 USA. RI Girart, Josep/O-1638-2014 OI Girart, Josep/0000-0002-3829-5591 NR 25 TC 20 Z9 20 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1998 VL 495 IS 1 BP L59 EP L62 DI 10.1086/311206 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZA395 UT WOS:000072359200015 ER PT J AU Pen, UL AF Pen, UL TI A high-resolution adaptive moving mesh hydrodynamic algorithm SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE hydrodynamics; large-scale structure of universe; methods, numerical ID SMOOTHED PARTICLE HYDRODYNAMICS; HYPERBOLIC CONSERVATION-LAWS; AXISYMMETRICAL CLOUD CORES; PIECEWISE PARABOLIC METHOD; AMBIPOLAR DIFFUSION; STAR-FORMATION; SIMULATIONS; CONTRACTION; SCHEMES; CODE AB An algorithm for simulating self-gravitating cosmological astrophysical fluids is presented. The advantages include a large dynamic range, parallelizability, high resolution per grid element, and fast execution speed. The code is based on a finite volume flux-conservative total variation diminishing (TVD) scheme for the shock-capturing hydro and an iterative multigrid solver for the gravity. The grid is a time-dependent field, whose motion is described by a generalized potential how. Approximately constant mass per cell can be obtained, which provides all the advantages of a Lagrangian scheme. The grid deformation combined with appropriate limiting and smoothing schemes guarantees a regular and well-behaved grid geometry, in which nearest neighbor relationships remain constant. The full hydrodynamic fluid equations are implemented in the curvilinear moving grid, which allows for arbitrary fluid flow relative to the grid geometry. This combination retains all the advantages of the grid-based schemes including high speed per fluid element and a rapid gravity solver. The current implementation is described, and empirical simulation results are presented. Accurate execution speed calculations are given in terms of floating point operations per time step per grid cell. This code is freely available to the community. C1 Harvard Soc Fellows, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pen, UL (reprint author), Harvard Soc Fellows, Cambridge, MA 02138 USA. EM upen@cfa.harvard.edu NR 36 TC 58 Z9 59 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 1998 VL 115 IS 1 BP 19 EP 34 DI 10.1086/313074 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY779 UT WOS:000072184300002 ER PT J AU Gossel, PP AF Gossel, PP TI Microbe hunters - Then and now. SO BULLETIN OF THE HISTORY OF MEDICINE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Gossel, PP (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0007-5140 J9 B HIST MED JI Bull. Hist. Med. PD SPR PY 1998 VL 72 IS 1 BP 143 EP 144 DI 10.1353/bhm.1998.0025 PG 2 WC Health Care Sciences & Services; History & Philosophy Of Science SC Health Care Sciences & Services; History & Philosophy of Science GA ZD505 UT WOS:000072692700038 ER PT J AU Judd, DD AF Judd, DD TI Exploring component stability using life-stage concordance in sabethine mosquitoes (Diptera : Culicidae) SO CLADISTICS-THE INTERNATIONAL JOURNAL OF THE WILLI HENNIG SOCIETY LA English DT Article ID COMBINING DATA; PHYLOGENETIC ANALYSIS; TAXONOMIC CONGRUENCE; SPECIES TREES; GENE TREES; DATA SETS; SYSTEMATICS; RECONSTRUCTION; EVOLUTION; CONSENSUS AB Morphological characters from sabethine mosquitoes were coded from larvae, pupae and adults, and life-stage partitions were evaluated to determine the contribution of each to the topology of a combined cladogram. Initial tests failed to find congruence between characters partitioned by life stage. However, when components from the combined analysis were tested using reduced taxon sets, a high degree of concordance between partitions was observed. A procedure for assessing individual life-stage contribution is employed, in which exhaustive searches are used to explore all possible arrangements for each of the selected components. Seven of the 10 components examined were able to recover the combined topology with a reduced taxon set. Congruent arrangements of taxa were typically observed for two or more life stages, although partitioned data were less resolved and frequently included aberrant topologies (those not supported by other partitioned or combined reduced taxon tree sets). In addition, none of the partitioned data sets gave robust results for all tests, suggesting that studies which emphasize character data from single life stages may support misleading arrangements of taxa. One component on the combined cladogram was not supported by any of the life-stage partitions when analysed separately. These results are complementary to "total evidence" approach, and demonstrate that partitions of data are useful for examining suits of characters which may cause some components of the "total evidence" tree to appear unstable. (C) 1998 The Willi Hennig Society. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Judd, DD (reprint author), Smithsonian Inst, Dept Entomol, NHB 169, Washington, DC 20560 USA. NR 62 TC 20 Z9 20 U1 1 U2 2 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0748-3007 J9 CLADISTICS JI Cladistics-Int. J. Willi Hennig Soc. PD MAR PY 1998 VL 14 IS 1 BP 63 EP 93 DI 10.1111/j.1096-0031.1998.tb00204.x PG 31 WC Evolutionary Biology SC Evolutionary Biology GA ZG779 UT WOS:000073038500003 ER PT J AU Dalling, JW Swaine, MD Garwood, NC AF Dalling, JW Swaine, MD Garwood, NC TI Dispersal patterns and seed bank dynamics of pioneer trees in moist tropical forest SO ECOLOGY LA English DT Article DE Cecropia insignis; gap colonization; Miconia argentea; pathogenic fungi; Panama; pioneer; seed dispersal; seed predation; seed rain; soil seed bank ID GAP-PHASE REGENERATION; RAIN-FOREST; SOIL; DISTANCE; PLANTS; RECRUITMENT; DISTURBANCE; PATHOGENS; EMERGENCE; VIABILITY AB Seed dispersal patterns and seed persistence in the soil should strongly influence the distribution of pioneer tree recruits in gaps. Nonetheless, seed distribution patterns for pioneers are poorly known, and processes controlling the fate of seeds in the soil have been little explored. We examined patterns of seed rain, seed abundance in the soil, and seed mortality of two common pioneer trees, Miconia argentea (Melastomataceae) and Cecropia insignis (Moraceae), on Barro Colorado Island, Panama. For each species, we selected four isolated, reproductive trees within a 50-ha forest dynamics plot. Seed rain and soil seed bank samples were collected, respectively, in mesh traps and from soil cores sampled along transects radiating away from the tree crowns. At below-crown sites, seed rain inputs far exceeded soil seed bank densities measured at the end of the fruiting season. For Miconia, the below-crown seed bank in the surface 3 cm of soil accounted for only 23% of seed rain, and for Cecropia, only 2%. However for Miconia, at distances >5 m from the crown seed bank densities exceeded the annual seed rain input. For both species log seed densities in the seed bank declined linearly with log distance from the crown and also decreased dramatically through the year. The annual loss rate of Miconia seeds was >90% below the crown and declined to 65% at 30 m from the crown. The annual loss rate for Cecropia was >90% at all distances. Seed losses in the seed bank could be largely attributed to mortality from pathogenic fungi. Fungicide treatment significantly increased seed survival in the soil for both species. For these two gap-dependent pioneer species, rapid seed-bank turnover rates and logarithmic declines in soil seed density with distance from adults suggested that both the spatial distribution and timing of gap formation may have influenced their chances of successful gap colonization. Recruitment from distant seed sources, or from seeds surviving in the soil after the death of the parent tree, may be relatively rare for these species. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Aberdeen, Dept Plant & Soil Sci, Aberdeen AB9 2UD, Scotland. Nat Hist Museum, Dept Bot, London SW7 5BD, England. RP Dalling, JW (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 68 TC 130 Z9 161 U1 4 U2 47 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD MAR PY 1998 VL 79 IS 2 BP 564 EP 578 DI 10.1890/0012-9658(1998)079[0564:DPASBD]2.0.CO;2 PG 15 WC Ecology SC Environmental Sciences & Ecology GA ZA653 UT WOS:000072387600016 ER PT J AU Nelson, SM Epstein, ME AF Nelson, SM Epstein, ME TI Butterflies (Lepidoptera : Papilionoidea and Hesperioidea) of Roxborough State Park, Colorado, USA: Baseline inventory, community attributes, and monitoring plan SO ENVIRONMENTAL MANAGEMENT LA English DT Article DE butterfly communities; grazing; inventory; monitoring; natural history ID BIODIVERSITY; ASSEMBLAGES AB Roxborough State Park in Colorado's Front Range was established in 1975 following a history of cattle and sheep ranching by private ownership. Survey work conducted from 1979 to 1995 resulted in the documentation of 93 species of butterflies. A variety of factors are responsible for the composition of the butterfly community: (1) overgrazing and its effect on the presence or absence of specific butterfly host plants, (2) habitat differences resulting from topographical and geological features; and (3) ecological and historical biogeography. This study provides data on community sampling adequacy, along with estimates of effort needed to monitor trends in abundance by using a community self-similarity curve and power analysis. An annual monitoring plan is proposed to assess trends in community composition. The plan includes collection of presence/absence and abundance data for select butterflies based on natural history information. C1 US Bur Reclamat, Tech Serv Ctr, Ecol Res & Invest Grp, Denver, CO 80225 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Nelson, SM (reprint author), US Bur Reclamat, Tech Serv Ctr, Ecol Res & Invest Grp, POB 25007, Denver, CO 80225 USA. NR 30 TC 8 Z9 8 U1 0 U2 5 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0364-152X J9 ENVIRON MANAGE JI Environ. Manage. PD MAR-APR PY 1998 VL 22 IS 2 BP 287 EP 295 DI 10.1007/s002679900104 PG 9 WC Environmental Sciences SC Environmental Sciences & Ecology GA YX163 UT WOS:000072012700012 ER PT J AU Vennum, T AF Vennum, T TI Shoshone ghost dance religion: Poetry songs and Great Basin context SO ETHNOMUSICOLOGY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Vennum, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC ETHNOMUSICOLOGY INC PI BLOOMINGTON PA MORRISON HALL, ROOM 005 INDIANA UNIVERSITY, BLOOMINGTON, IN 47405 USA SN 0014-1836 J9 ETHNOMUSICOLOGY JI Ethnomusicology PD SPR-SUM PY 1998 VL 42 IS 2 BP 369 EP 372 DI 10.2307/3113906 PG 4 WC Music SC Music GA 104EQ UT WOS:000075002100018 ER PT J AU Sorensen, SS Dunne, GC Hanson, RB Barton, MD Becker, J Tobisch, OT Fiske, RS AF Sorensen, SS Dunne, GC Hanson, RB Barton, MD Becker, J Tobisch, OT Fiske, RS TI From Jurassic shores to Cretaceous plutons: Geochemical evidence for paleoalteration environments of metavolcanic rocks, eastern California SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article ID PORPHYRY COPPER-DEPOSIT; MEXICAN VOLCANIC BELT; RITTER RANGE PENDANT; SIERRA-NEVADA; CALC-ALKALINE; OCEANIC-CRUST; IGNEOUS ROCKS; HYDROTHERMAL ALTERATION; CALDERA COMPLEX; K-METASOMATISM AB Volcanic and plutonic rocks exposed in east-central California record a long history of metasomatism and/or metamorphism within the Mesozoic Cordilleran continental are. We use whole-rock and mineral elemental compositions, along with standard and cathodoluminescence petrography to characterize alteration histories of Late Triassic to Middle Jurassic metavolcanic rocks in the Ritter Range, White-Inyo Mountains, and Alabama Hills. Although alkali-metasomatism is widespread and pervasive, ratios and abundances of Ce, Th, Tb, and Ta suggest that mafic protoliths from the White-Inyo Mountains were shoshonitic, whereas those from the Ritter Range were calc-alkaline. Alkali exchange apparently modified the compositions of many metavolcanic rocks. Much of this metasomatism may have occurred at low-temperature (T) conditions, and attended or shortly postdated deposition of the volcanic protoliths. High delta(18)O values for K-rich metatuffs from the Ritter Range suggest that the K-metasomatizing fluid was low-T seawater. In contrast, low delta(18)O values for K-rich metatuffs from the Alabama Hills and Inyo Mountains seem to reflect rock interaction with meteoric water prior to contact metamorphism. Jurassic metatuffs deposited in marine (Ritter Range) and nonmarine (Alabama Hills, Inyo Mountains) settings display similar degrees of K for Na (or Ca) exchange that were affected by isotopically distinct fluids, Some alkali-metasomatism of Jurassic metavolcanic rocks is related to Cretaceous plutonism. In the Ritter Range and Alabama Hills, these effects are localized around pluton contacts, appear to be more vein related than pervasive, and overprint K-metasomatized assemblages. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Calif State Univ Northridge, Dept Geol Sci, Northridge, CA 91330 USA. Science, Washington, DC 20005 USA. Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. Univ Calif Santa Cruz, Earth Sci Board, Santa Cruz, CA 95604 USA. RP Sorensen, SS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, NHB-119, Washington, DC 20560 USA. EM sorena@volcano.si.edu; bhanson@aaas.org NR 95 TC 21 Z9 21 U1 0 U2 5 PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER PI COLLEGE STN PA TEXAS A & M UNIV, DEPT GEOLOGY & GEOPHYSICS, COLLEGE STN, TX 77843-3115 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAR PY 1998 VL 110 IS 3 BP 326 EP 343 DI 10.1130/0016-7606(1998)110<0326:FJSTCP>2.3.CO;2 PG 18 WC Geosciences, Multidisciplinary SC Geology GA ZB102 UT WOS:000072435900004 ER PT J AU Wilf, P Wing, SL Greenwood, DR Greenwood, CL AF Wilf, P Wing, SL Greenwood, DR Greenwood, CL TI Using fossil leaves as paleoprecipitation indicators: An Eocene example SO GEOLOGY LA English DT Article ID RAIN-FOREST; LOS-TUXTLAS; LEAF SIZE; CLIMATE; RESPECT; MEXICO; FLORA AB Estimates of past precipitation are of broad interest for many areas of inquiry, including reconstructions of past environments and topography, climate modeling, and ocean circulation studies. The shapes and sizes of living leaves are highly sensitive to moisture conditions, and assemblages of fossil leaves of flowering plants have great potential as paleoprecipitation indicators. Most quantitative estimates of paleoprecipitation have been based on a multivariate data set of morphological leaf characters measured from samples of living vegetation tied to climate stations. However, when tested on extant forests, this method has consistently overestimated precipitation. We present a simpler approach that uses only the mean leaf area of a vegetation sample as a predictor variable but incorporates a broad range of annual precipitation and geographic coverage into the predictor set. The significant relationship that results, in addition to having value for paleoclimatic reconstruction, refines understanding of the long-observed positive relationship between leaf area and precipitation. Seven precipitation estimates for the Eocene of the Western United States are revised as lower than previously published but remain far wetter than the same areas today. Abundant moisture may have been an important factor in maintaining warm, frost-free conditions in the Eocene because of the major role of water vapor in retaining and transporting atmospheric heat. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Victoria Univ Technol, Dept Biol & Food Sci, Melbourne, Vic 8001, Australia. Monash Univ, Dept Geog & Environm Sci, Clayton, Vic 3168, Australia. RP Wilf, P (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. RI Greenwood, David/C-2758-2008; OI Greenwood, David/0000-0002-8569-9695; Wing, Scott/0000-0002-2954-8905; Wilf, Peter/0000-0001-6813-1937 NR 42 TC 164 Z9 179 U1 1 U2 32 PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER PI COLLEGE STN PA TEXAS A & M UNIV, DEPT GEOLOGY & GEOPHYSICS, COLLEGE STN, TX 77843-3115 USA SN 0091-7613 J9 GEOLOGY JI Geology PD MAR PY 1998 VL 26 IS 3 BP 203 EP 206 DI 10.1130/0091-7613(1998)026<0203:UFLAPI>2.3.CO;2 PG 4 WC Geology SC Geology GA ZB103 UT WOS:000072436000003 ER PT J AU Colinvaux, PA AF Colinvaux, PA TI A new vicariance model for Amazonian endemics SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Amazonia; climate change; refugial hypothesis; Pleistocene history; speciation; vicariance ID TEMPERATURE DEPRESSION AB It is unlikely that ice age climates of the Amazon were sufficiently arid to fragment the forest as required by the Haffer refugial hypothesis. However, glacial Amazon climates were colder and had reduced CO2 concentrations that would have had their strongest effects on the biota in the elevated areas stipulated to have been refugia. If local endemicity of butterflies or birds records Pleistocene speciation, this is because glacial climates provided cool, CO2 starved islands in a sea of continuous forest. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. NR 22 TC 46 Z9 49 U1 1 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X EI 1466-8238 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD MAR PY 1998 VL 7 IS 2 BP 95 EP 96 DI 10.2307/2997812 PG 2 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA ZZ224 UT WOS:000074708000001 ER PT J AU Ubelaker, SH AF Ubelaker, SH TI Fordisc 2.0: Personal computer forensic discriminant functions SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Software Review C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Ubelaker, SH (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 3 TC 0 Z9 1 U1 1 U2 6 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX PO19 1UD, ENGLAND SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD MAR-APR PY 1998 VL 8 IS 2 BP 128 EP 131 PG 4 WC Anthropology; Archaeology SC Anthropology; Archaeology GA ZL838 UT WOS:000073477200007 ER PT J AU Kidwell, PA AF Kidwell, PA TI Science in the field. SO ISIS LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Kidwell, PA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0021-1753 J9 ISIS JI Isis PD MAR PY 1998 VL 89 IS 1 BP 117 EP 118 DI 10.1086/383932 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA ZK286 UT WOS:000073304000021 ER PT J AU Stefanik, RP AF Stefanik, RP TI Planet quest: The epic discovery of alien solar systems. SO ISIS LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stefanik, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0021-1753 J9 ISIS JI Isis PD MAR PY 1998 VL 89 IS 1 BP 164 EP 164 DI 10.1086/383983 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA ZK286 UT WOS:000073304000076 ER PT J AU Melchionne, K AF Melchionne, K TI Living in glass houses: Domesticity, interior decoration, and environmental aesthetics SO JOURNAL OF AESTHETICS AND ART CRITICISM LA English DT Article C1 Smithsonian Inst, Natl Museum Amer Art, Washington, DC 20560 USA. RP Melchionne, K (reprint author), Smithsonian Inst, Natl Museum Amer Art, Washington, DC 20560 USA. NR 16 TC 6 Z9 6 U1 0 U2 2 PU AMER SOC AESTHETICS, DEPT OF PHILOSOPHY PI MILWAUKEE PA C/O CURTIS L CARTER, 404 CUDAHY HALL, MARQUETTE UNIV, PO BOX 1881, MILWAUKEE, WI 53201-1881 USA SN 0021-8529 J9 J AESTHET ART CRITIC JI J. Aesthet. Art Crit. PD SPR PY 1998 VL 56 IS 2 BP 191 EP 200 DI 10.2307/432257 PG 10 WC Art; Philosophy SC Art; Philosophy GA ZF341 UT WOS:000072887800010 ER PT J AU Stutchbury, BJM Morton, ES Piper, WH AF Stutchbury, BJM Morton, ES Piper, WH TI Extra-pair mating system of a synchronously breeding tropical songbird SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID SPERM COMPETITION; EASTERN BLUEBIRDS; FEMALE RAZORBILLS; MONOGAMOUS BIRD; PURPLE MARTINS; HOUSE SPARROW; PATERNITY; DNA; COPULATIONS; FERTILIZATIONS AB Extra-pair matings are now recognized as a fundamental component of avian mating systems. However, in tropical regions where breeding is typically asynchronous socially monogamous species appear to have low sperm competition and few extrapair matings. We predicted that if breeding synchrony promotes the evolution of extra-pair matings, then tropical species that breed synchronously, like the Clay-colored Robin Turdus grayi, should have abundant extra-pair young (EPY). Breeding began relatively abruptly during the dry season (Feb-Mar) in this non-migratory species, with a mean of 25% of females fertile on a given day. Overall, 53% of females produced EPY, and 38% of nestlings were EPY. Males have a long and conspicuous dawn chorus, which could be a result of intense male-male competition for extra-pair matings. Male songs are individually recognizable and males vary greatly in song output. Male song output declined significantly from the pre-nesting stage through the incubation stage, as would be expected if song is important in mate choice. Our results support the idea that breeding synchrony favors extra-pair matings, however further studies of tropical songbirds are needed to fully explore how ecology is tied to extra-pair mating systems. C1 York Univ, Dept Biol, N York, ON M3J 1P3, Canada. Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Smithsonian Inst, Natl Zool Pk, Mol Genet Lab, Washington, DC 20008 USA. RP Stutchbury, BJM (reprint author), York Univ, Dept Biol, 4700 Keele St, N York, ON M3J 1P3, Canada. NR 49 TC 39 Z9 40 U1 3 U2 27 PU MUNKSGAARD INT PUBL LTD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD MAR PY 1998 VL 29 IS 1 BP 72 EP 78 DI 10.2307/3677343 PG 7 WC Ornithology SC Zoology GA ZB694 UT WOS:000072498200010 ER PT J AU Correll, DL AF Correll, DL TI The role of phosphorus in the eutrophication of receiving waters: A review SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article; Proceedings Paper CT Symposium on Agricultural Phosphorus and Eutrophication CY NOV 05, 1996 CL INDIANAPOLIS, INDIANA SP ASA, Soil Sci Soc Amer, CSSA ID NUTRIENT LIMITATION; PHYTOPLANKTON GROWTH; CHEMICAL-COMPOSITION; PLANKTONIC ALGAE; LIMITED GROWTH; FRESH-WATER; LAKES; PHOSPHATE; NITROGEN; ENRICHMENT AB Phosphorus (P) is an essential element for all life forms, It is a mineral nutrient, Orthophosphate is the only form of P that autotrophs can assimilate. Extracellular enzymes hydrolyze organic forms of P to phosphate. Eutrophication is the overenrichment of receiving waters with mineral nutrients, The results are excessive production of autotrophs, especially algae and cyanobacteria, This high productivity leads to high bacterial populations and high respiration rates, leading to hypoxia or anoxia in poorly mixed bottom waters and at night in surface waters during calm, warm conditions, Low dissolved oxygen causes the loss of aquatic animals and release of many materials normally bound to bottom sediments including various forms of P, This release of P reinforces the eutrophication. Excessive concentrations of P is the most common cause of eutrophication in fresh,vater lakes, reservoirs, streams, and headwaters of estuarine systems. In the ocean, N becomes the key mineral nutrient controlling primary production. Estuaries and continental shelf waters are a transition zone, where excessive P and N create problems. It is best to measure and regulate total P inputs to whole aquatic ecosystems, but for an easy assay it is best to measure total P concentrations, including particulate P, in surface waters or NTP atomic ratios in phytoplankton. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Correll, DL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM correll@serc.si.edu NR 62 TC 625 Z9 691 U1 62 U2 494 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 USA SN 0047-2425 J9 J ENVIRON QUAL JI J. Environ. Qual. PD MAR-APR PY 1998 VL 27 IS 2 BP 261 EP 266 PG 6 WC Environmental Sciences SC Environmental Sciences & Ecology GA ZD782 UT WOS:000072723300004 ER PT J AU Petraglia, M AF Petraglia, M TI The Paleolithic of India and its bearing on the hominid record SO JOURNAL OF HUMAN EVOLUTION LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD MAR PY 1998 VL 34 IS 3 BP A17 EP A17 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA ZF994 UT WOS:000072954000030 ER PT J AU Sadler, PM AF Sadler, PM TI Psychometric models of student conceptions in science: Reconciling qualitative studies and distractor-driven assessment instruments SO JOURNAL OF RESEARCH IN SCIENCE TEACHING LA English DT Article ID MULTIPLE-CHOICE; PHYSICS; ITEM; MISCONCEPTIONS; STRATEGIES; RESPONSES; COGNITION AB We stand poised to many the fruits of qualitative research on children's conceptions with the machinery of psychometrics. This merger allows us to build upon studies of limited groups of subjects to generalize to the larger population of learners. This is accomplished by reformulating multiple choice tests to reflect gains in understanding cognitive development. This study uses psychometric modeling to rank the appeal of a variety of children's astronomical ideas on a single uniform scale. Alternative conceptions are captured in test items with highly attractive multiple choice distracters administered twice to 1250 8th through 12th-grade students at the start and end of their introductory astronomy courses. For such items, an unusual psychometric profile is observed-instruction appears to strengthen support for alternative conceptions before this preference eventually declines. This lends support to the view that such ideas may actually be markers of progress toward scientific understanding and are not impediments to learning. This method of analysis reveals the ages at which certain conceptions are more prevalent than others, aiding developers and practitioners in matching curriculum to student grade levels. This kind of instrument, in which distracters match common student ideas, has a profoundly different psychometric profile from conventional tests and exposes the weakness evident in conventional standardized tests. Distractor-driven multiple choice tests combine the richness of qualitative research with the power of quantitative assessment, measuring conceptual change along a single uniform dimension. (C) 1998 John Wiley & Sons, Inc. C1 Harvard Univ, Grad Sch Educ, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sadler, PM (reprint author), Harvard Univ, Grad Sch Educ, Longfellow 315, Cambridge, MA 02138 USA. NR 82 TC 66 Z9 67 U1 4 U2 12 PU JOHN WILEY & SONS INC PI NEW YORK PA 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0022-4308 J9 J RES SCI TEACH JI J. Res. Sci. Teach. PD MAR PY 1998 VL 35 IS 3 BP 265 EP 296 DI 10.1002/(SICI)1098-2736(199803)35:3<265::AID-TEA3>3.0.CO;2-P PG 32 WC Education & Educational Research SC Education & Educational Research GA YZ740 UT WOS:000072286800003 ER PT J AU Koob, S AF Koob, S TI Obsolete fill materials found on ceramics (History, art conservation) SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article C1 Smithsonian Inst, Freer Gallery Art, Dept Conservation & Sci Res, Washington, DC 20560 USA. RP Koob, S (reprint author), Smithsonian Inst, Freer Gallery Art, Dept Conservation & Sci Res, Washington, DC 20560 USA. NR 48 TC 6 Z9 6 U1 0 U2 0 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1156 15TH STREET, NW STE 320, WASHINGTON, DC 20005-1714 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SPR PY 1998 VL 37 IS 1 BP 49 EP 67 DI 10.2307/3179911 PG 19 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA ZX016 UT WOS:000074471800005 ER PT J AU Mamay, SH Hook, RW Hotton, N AF Mamay, SH Hook, RW Hotton, N TI Amphibian eggs from the Lower Permian of north-central Texas SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID ORIGIN AB Masses of small (up to 0.8 mm in diameter) oviform bodies were found in association with fossil plants as well as freshwater and terrestrial invertebrate and vertebrate remains in the Waggoner Ranch Formation (Wichita Group, Leonardian Series, Lower Permian) of Baylor County Texas; this is the first record of fossilized amphibian eggs. The eggs occur as compact, rounded masses and as irregular sheetlike or unilayered aggregates, some of which cover plant remains to which they may have been attached originally. Individual eggs consist of a compressed central body surrounded by a thin, apparently flexible membrane, and an outermost halolike covering, Characteristics of the egg masses and the morphology of individual eggs are indistinguishable from these of modern anuran amphibians. Because dissorophoid temnospondyls are phylogenetically related closely to Recent amphibians and are well represented in the Lower Permian of north-central Texas, dissorophoids are the most probable sourer of the eggs. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Univ Texas, Vertebrate Paleontol Lab, Austin, TX 78712 USA. RP Mamay, SH (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. NR 26 TC 2 Z9 2 U1 0 U2 1 PU SOC VERTEBRATE PALEONTOLOGY PI CHICAGO PA 401 NORTH MICHIGAN AVE, CHICAGO, IL 60611-4267 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAR PY 1998 VL 18 IS 1 BP 80 EP 84 PG 5 WC Paleontology SC Paleontology GA ZH633 UT WOS:000073131200007 ER PT J AU Emry, RJ Tyutkova, LA Lucas, SG Wang, BY AF Emry, RJ Tyutkova, LA Lucas, SG Wang, BY TI Rodents of the middle Eocene Shinzhaly fauna of Eastern Kazakstan SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article AB Fossil mammals of the Skinzhaly fauna occur in the Kolpak Formation. a sequence of Paleogene red beds exposed along the Shinzhaly River in Eastern Kazakstan. Most of the fossils are concentrated in a single bed 0.3 m thick. Screen washing of sediment from this bed has yielded small mammals, including several species of rodents: a zapodid, Akysiromys dalos; two cricetids, Pappocricetodon kazakstanicus, sp. nov. and Zhumgaromys gromovi, gen. et sp. nov.; and a chapartimyid, Saykanomys sp., cf. S. bohlini. Temporal correlation indicated by the rodents is in agreement with the middle Eocene (Irdinmanhan) age indicated by perissodactyls previously described from the Shimzhaly fauna. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol, Washington, DC 20560 USA. Natl Acad Sci Republic Kazakstan, Inst Zool, Alma Ata 480032, Kazakhstan. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. Acad Sinica, Inst Vertebrate Paleontol & Paleoanthropol, Beijing 100044, Peoples R China. RP Emry, RJ (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol, Washington, DC 20560 USA. NR 33 TC 10 Z9 12 U1 0 U2 2 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAR PY 1998 VL 18 IS 1 BP 218 EP 227 PG 10 WC Paleontology SC Paleontology GA ZH633 UT WOS:000073131200017 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Art and objecthood: Essays and reviews. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 1 PY 1998 VL 123 IS 4 BP 86 EP 86 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA YZ612 UT WOS:000072271500031 ER PT J AU Kuzoff, RK Sweere, JA Soltis, DE Soltis, PS Zimmer, EA AF Kuzoff, RK Sweere, JA Soltis, DE Soltis, PS Zimmer, EA TI The phylogenetic potential of entire 26S rDNA sequences in plants SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE 26S rDNA; LSU rDNA; expansion segments; cryptic sequence simplicity; molecular evolution; phylogenetic inference ID RIBOSOMAL-RNA GENE; SECONDARY STRUCTURE MODEL; NUCLEOTIDE-SEQUENCE; MOLECULAR COEVOLUTION; LARGE-SUBUNIT; EVOLUTIONARY TREES; DNA-SEQUENCES; SYSTEMATICS; RBCL; 18S AB 18S ribosomal RNA genes are the most widely used nuclear sequences for phylogeny reconstruction at higher taxonomic levels in plants. However, due to a conservative rate of evolution, 18S rDNA alone sometimes provides too few phylogenetically informative characters to resolve relationships adequately. Previous studies using partial sequences have suggested the potential of 26S or large-subunit (LSU) rDNA for phylogeny retrieval at taxonomic levels comparable to those investigated with 18S rDNA. Here we explore the patterns of molecular evolution of entire 26S rDNA sequences and their impact on phylogeny retrieval. We present a protocol for PCR amplification and sequencing of entire (similar to 3.4 kb) 26S rDNA sequences as single amplicons, as well as primers that can be used for amplification and sequencing. These primers proved useful in angiosperms and Gnetales and likely have broader applicability. With these protocols and primers, entire 26S rDNA sequences were generated for a diverse array of 15 seed plants, including basal eudicots, monocots, and higher eudicots, plus two representatives of Gnetales. Comparisons of sequence dissimilarity indicate that expansion segments (or divergence domains) evolve 6.4 to 10.2 times as fast as conserved core regions of 26S rDNA sequences in plants. Additional comparisons indicate that 26S rDNA evolves 1.6 to 2.2 times as fast as and provides 3.3 times as many phylogenetically informative characters as 18S rDNA; compared to the chloroplast gene rbcL, 26S rDNA evolves at 0.44 to 1.0 times its rate and provides 2.0 times as many phylogenetically informative characters. Expansion segment sequences analyzed here evolve 1.2 to 3.0 times faster than rbcL, providing 1.5 times the number of informative characters. Plant expansion segments have a pattern of evolution distinct from that found in animals, exhibiting less cryptic sequence simplicity, a lower frequency of insertion and deletion, and greater phylogenetic potential. C1 Washington State Univ, Dept Bot, Pullman, WA 99164 USA. Smithsonian Inst, Natl Museum Nat Hist, Lab Mol Systemat, Washington, DC 20560 USA. RP Kuzoff, RK (reprint author), Washington State Univ, Dept Bot, Pullman, WA 99164 USA. EM kuzoff@wsunix.wsu.edu RI Zimmer, Elizabeth/G-3890-2011; Soltis, Pamela/L-5184-2015 NR 67 TC 129 Z9 139 U1 1 U2 12 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0737-4038 EI 1537-1719 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD MAR PY 1998 VL 15 IS 3 BP 251 EP 263 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA ZA419 UT WOS:000072361600003 PM 9501492 ER PT J AU Peterson, PM Planchuelo, AM AF Peterson, PM Planchuelo, AM TI Bromus catharticus in South America (Poaceae : Bromeae) SO NOVON LA English DT Article ID PHYLOGENY; GLYCINE AB A new combination, Bromus catharticus var. rupestris, is made. Based on morphological evidence this taxon seems best recognized at the varietal level. Detailed illustrations of B. catharticus var. rupestris and B. catharticus var. catharticus are included along with morphological descriptions, distributions, and representative specimens. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot NHB166, Washington, DC 20560 USA. Univ Nacl Cordoba, Fac Ciencias Agropecuarias, CONICET, RA-5000 Cordoba, Argentina. RP Peterson, PM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot NHB166, Washington, DC 20560 USA. NR 30 TC 5 Z9 9 U1 0 U2 1 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SPR PY 1998 VL 8 IS 1 BP 53 EP 60 DI 10.2307/3391893 PG 8 WC Plant Sciences SC Plant Sciences GA ZK233 UT WOS:000073298700014 ER PT J AU Pruski, JF AF Pruski, JF TI Stenopadus andicola sp. nov. (Asteraceae : Mutisieae), a new generic record for Ecuador SO NOVON LA English DT Article AB A new species, Stenopadus andicola (Asteraceae: Mutisieae), is described from the Cordillera del Condor, Ecuador. It is the first member of the genus reported outside the Guayana Highland and is a new generic record for Ecuador. Stenopadus andicola is placed in section Stenopadus. C1 Smithsonian Inst, Dept Bot, US Natl Herbarium, Washington, DC 20560 USA. RP Pruski, JF (reprint author), Smithsonian Inst, Dept Bot, US Natl Herbarium, MRC-166, Washington, DC 20560 USA. NR 8 TC 5 Z9 5 U1 0 U2 2 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SPR PY 1998 VL 8 IS 1 BP 67 EP 69 DI 10.2307/3391896 PG 3 WC Plant Sciences SC Plant Sciences GA ZK233 UT WOS:000073298700017 ER PT J AU Yan, ZC Tambasco, M Drake, GWF AF Yan, ZC Tambasco, M Drake, GWF TI Energies and oscillator strengths for lithiumlike ions SO PHYSICAL REVIEW A LA English DT Article ID 2S GROUND-STATE; ISOELECTRONIC SEQUENCE; VARIATIONAL CALCULATIONS; 1S(2)2S STATES; FINE-STRUCTURE; 1/Z EXPANSION; LI; EIGENVALUES; CONVERGENCE; MEMBERS AB The Hylleraas-type variational method is used to calculate the energies of the lithium 1s(2)2s S-2 and 1s(2)2p P-2 isoelectronic sequences up to Z = 20. The oscillator strengths for the 1s(2)2s S-2 --> 1s(2)2p P-2 transitions are evaluated for Z up to 20, including finite nuclear mass effects, and the corresponding lifetimes are determined. The 1/Z expansion method is used to extend the variational results to larger values of Z. Relativistic corrections to the dipole transition moment squared are estimated by comparison with the relativistic many-body perturbation theory results of Johnson et al. [At. Data Nucl. Data Tables 64, 279 (1996)]. The final lifetime for the 1s(2)2p P-2 State of Lithium is in good agreement with recent high-precision measurements. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Windsor, Dept Phys, Windsor, ON N9B 3P4, Canada. RP Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. RI Yan, Zong-Chao/F-6668-2014 NR 43 TC 133 Z9 137 U1 0 U2 7 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 1998 VL 57 IS 3 BP 1652 EP 1661 DI 10.1103/PhysRevA.57.1652 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA ZB155 UT WOS:000072441900029 ER PT J AU Marinescu, M Dalgarno, A AF Marinescu, M Dalgarno, A TI Long-range diagonal adiabatic corrections for the ground molecular state of alkali-metal dimers SO PHYSICAL REVIEW A LA English DT Article ID COEFFICIENTS; FORCES AB We study long-range diagonal adiabatic corrections to the interaction potentials of the ground state of homonuclear alkali-metal dimers. We show that in the long-range limit the diagonal adiabatic matrix elements may be expressed as a series of inverse powers of the internuclear distance. Each of the nonzero coefficients of this expansion is a mass-dependent correction term to the dispersion coefficients. They are computed by using a complex integral representation, that transforms the molecular problem into an atomic one. Numerical results are presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. RP Marinescu, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 11 Z9 11 U1 0 U2 4 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 1998 VL 57 IS 3 BP 1821 EP 1826 DI 10.1103/PhysRevA.57.1821 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA ZB155 UT WOS:000072441900048 ER PT J AU Segev, B Wells, JC AF Segev, B Wells, JC TI Light-fronts approach to electron-positron pair production in ultrarelativistic heavy-ion collisions SO PHYSICAL REVIEW A LA English DT Article ID RELATIVISTIC ATOMIC-COLLISIONS; IMPACT-PARAMETER DEPENDENCE; STRONG EXTERNAL FIELDS; ELECTROMAGNETIC-FIELDS; SULFUR IONS; GAUGE TRANSFORMATIONS; COULOMB COLLISIONS; CHARGE-TRANSFER; ENERGY; PARTICLE AB We perform a gauge transformation on the time-dependent Dirac equation describing the evolution of an electron in a heavy-ion collision to remove the explicit dependence on the long-range part of the interaction. We solve, in an ultrarelativistic limit, the gauge-transformed Dirac equation using light-front variables and a light-fronts representation, obtaining nonperturbative results for the free pair-creation amplitudes in the collider frame. Our result reproduces the result of second-order perturbation theory in the small charge limit while nonperturbative effects arise for realistic charges of the ions. 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. RI Wells, Jack/D-3675-2016 OI Wells, Jack/0000-0002-5083-3030 NR 49 TC 43 Z9 43 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 1998 VL 57 IS 3 BP 1849 EP 1861 DI 10.1103/PhysRevA.57.1849 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA ZB155 UT WOS:000072441900051 ER PT J AU Finn, BS AF Finn, BS TI Introduction to the classic paper by J.W. Howell SO PROCEEDINGS OF THE IEEE LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Finn, BS (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 USA SN 0018-9219 J9 P IEEE JI Proc. IEEE PD MAR PY 1998 VL 86 IS 3 BP 581 EP 582 DI 10.1109/JPROC.1998.662881 PG 2 WC Engineering, Electrical & Electronic SC Engineering GA ZB270 UT WOS:000072454200012 ER PT J AU Field, GB AF Field, GB TI Lyman Spitzer, Jr. (1914-1997) SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Biographical-Item 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 1 TC 0 Z9 0 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR PY 1998 VL 110 IS 745 BP 215 EP 222 DI 10.1086/316135 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZF860 UT WOS:000072940500001 ER PT J AU Ward, DC AF Ward, DC TI 'In a Time of Violence': Poems SO SEWANEE REVIEW 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 UNIV SOUTH PI SEWANEE PA SEWANEE REVIEW, SEWANEE, TN 37375 USA SN 0037-3052 J9 SEWANEE REV JI Sewanee Rev. PD SPR PY 1998 VL 106 IS 2 BP 350 EP 358 PG 9 WC Literary Reviews SC Literature GA ZU107 UT WOS:000074162700042 ER PT J AU Ward, DC AF Ward, DC TI On 'Origin Like Water': Collected poems 1967-1987 SO SEWANEE REVIEW 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 UNIV SOUTH PI SEWANEE PA SEWANEE REVIEW, SEWANEE, TN 37375 USA SN 0037-3052 J9 SEWANEE REV JI Sewanee Rev. PD SPR PY 1998 VL 106 IS 2 BP 350 EP 358 PG 9 WC Literary Reviews SC Literature GA ZU107 UT WOS:000074162700041 ER PT J AU Poe, S AF Poe, S TI Sensitivity of phylogeny estimation to taxonomic sampling SO SYSTEMATIC BIOLOGY LA English DT Article DE multiple regression; modeling; phylogeny estimation; taxonomic sampling ID SYSTEMATICS; EVOLUTION; FOSSILS; TAXA; MORPHOLOGY; ASTERACEAE; SEQUENCES; MAMMALIA; NUMBERS; IMPACT AB Recent studies have shown that addition or deletion of taxa from a data matrix can change the estimate of phylogeny. I used 29 data sets from the literature to examine the effect of taxon sampling on phylogeny estimation within data sets. I then used multiple regression to assess the effect of number of taxa, number of characters, homoplasy, strength of support, and tree symmetry on the sensitivity of data sets to taxonomic sampling. Sensitivity to sampling was measured by mapping characters from a matrix of culled taxa onto optimal trees for that reduced matrix and onto the pruned optimal tree for the entire matrix, then comparing the length of the reduced tree to the length of the pruned complete tree. Within-data-set patterns can be described by a second-order equation relating fraction of tara sampled to sensitivity to sampling. Multiple regression analyses found number of taxa to be a significant predictor of sensitivity to sampling; retention index, number of informative characters, total support index, and tree symmetry were nonsignificant predictors. I derived a predictive regression equation relating fraction of taxa sampled and number of taxa potentially sampled to sensitivity to taxonomic sampling and calculated values for this equation within the bounds of the variables examined. The length difference be tween the complete tree and a subsampled tree was generally small (average difference of 0-2.9 steps), indicating that subsampling taxa is probably not an important problem for most phylogenetic analyses using up to 20 taxa. C1 Univ Texas, Dept Zool, Austin, TX 78712 USA. Univ Texas, Texas Mem Museum, Austin, TX 78712 USA. RP Poe, S (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Amphibians & Reptiles, Washington, DC 20560 USA. EM stevepoe@mail.utexas.edu NR 58 TC 95 Z9 96 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD MAR PY 1998 VL 47 IS 1 BP 18 EP 31 DI 10.1080/106351598261003 PG 14 WC Evolutionary Biology SC Evolutionary Biology GA ZK090 UT WOS:000073283900004 PM 12064237 ER PT J AU Rogers, JS Swofford, DL AF Rogers, JS Swofford, DL TI A fast method for approximating maximum likelihoods of phylogenetic trees from nucleotide sequences SO SYSTEMATIC BIOLOGY LA English DT Article DE approximations; maximum likelihood; parsimony; tree searching ID EVOLUTIONARY TREES; MITOCHONDRIAL-DNA; PARSIMONY; SUBSTITUTION; SIMULATION; INFERENCE; MODEL; RATES AB We have developed a rapid parsimony method for reconstructing ancestral nucleotide states that allows calculation of initial branch lengths that are good approximations to optimal maximum-likelihood estimates under several commonly used substitution models. Use of these approximate branch lengths (rather than fixed arbitrary values) as starting points significantly reduces the time required for iteration to a solution that maximizes the likelihood of a tree. These branch lengths are close enough to the optimal values that they can be used without further iteration to calculate approximate maximum-likelihood scores that are very close to the "exact" scores found by iteration. Several strategies are described for using these approximate scores to substantially reduce times needed for maximum-likelihood tree searches. C1 Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA. Smithsonian Inst, Lab Mol Systemat, Washington, DC 20560 USA. RP Rogers, JS (reprint author), Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA. EM jsrbs@uno.edu; swofford@onyx.si.edu NR 33 TC 103 Z9 104 U1 0 U2 8 PU TAYLOR & FRANCIS LTD PI LONDON PA ONE GUNPOWDER SQUARE, LONDON EC4A 3DE, ENGLAND SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD MAR PY 1998 VL 47 IS 1 BP 77 EP 89 PG 13 WC Evolutionary Biology SC Evolutionary Biology GA ZK090 UT WOS:000073283900008 PM 12064242 ER PT J AU Ibrahim, SA Avery, JW Weldon, PJ Wheeler, JW AF Ibrahim, SA Avery, JW Weldon, PJ Wheeler, JW TI Age-class differences in lipids from the paracloacal glands of the American alligator (Alligator mississippiensis) SO ZEITSCHRIFT FUR NATURFORSCHUNG C-A JOURNAL OF BIOSCIENCES LA English DT Article DE Alligator mississippiensis; paracloacal gland secretions; straight- and branched-chain esters; alcohols; fatty acids; beta-springene ID SECRETIONS; CROCODILIANS; TRIGONATUS AB The paracloacal gland secretions of immature and adult American alligators (Alligator mississippiensis) from Louisiana were analyzed by gas chromatography/mass spectrometry and nuclear magnetic resonance spectroscopy to investigate age-class differences in lipid composition. The secretions of both immature and adult alligators contain saturated C-14 and C-16 free fatty acids and decyl, undecyl, dodecyl, tetradecyl, and hexadecyl acetates. Compounds observed only in immature alligators include dodecanoic acid, C-12 and C-14 alcohols, C-10-C-14 butanoates, an array of C-8-C-18 3-methylbutanoates, C-12-C-15 hexanoates, C-12 and C-14 octanoates, a C-12 decanoate, C-10-C-14 dodecanoates, C-10-C-16 tetradecanoates, C-12 and C-14 hexadecanoates, a C-12 octadecanoate, and a diterpene hydrocarbon identified as (E,E)-7,11,15-trimethyl-3-methylenehexadeca-1,6,10,14-tetraene (beta-springene). Compounds observed only in adults include several C-7-C-16 free fatty acids and certain C-10-C-18 acetates. The age-class differences we observe in the paracloacal gland lipids of alligators from Louisiana are similar to those previously reported for alligators from Texas. C1 Howard Univ, Dept Chem, Washington, DC 20059 USA. USDA ARS, Beltsville Agr Res Ctr W, Insect Chem Ecol Lab, Beltsville, MD 20705 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Wheeler, JW (reprint author), Howard Univ, Dept Chem, Washington, DC 20059 USA. NR 11 TC 10 Z9 10 U1 0 U2 0 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 1998 VL 53 IS 3-4 BP 201 EP 209 PG 9 WC Biochemistry & Molecular Biology; Pharmacology & Pharmacy SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy GA ZL193 UT WOS:000073408100010 ER PT J AU Erwin, DH AF Erwin, DH TI Evolution - After the end: Recovery from extinction SO SCIENCE LA English DT Article ID ORDOVICIAN RADIATION; MARINE LIFE C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. RP Erwin, DH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. EM Erwin.Doug@nmnh.si.edu RI Erwin, Douglas/A-9668-2009 NR 13 TC 21 Z9 24 U1 0 U2 3 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 27 PY 1998 VL 279 IS 5355 BP 1324 EP 1325 DI 10.1126/science.279.5355.1324 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA YZ412 UT WOS:000072251800041 ER PT J AU Zaldarriaga, M Seljak, U Bertschinger, E AF Zaldarriaga, M Seljak, U Bertschinger, E TI Integral solution for the microwave background anisotropies in nonflat universes SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; dark matter; gravitation; large-scale structure of universe ID DARK-MATTER; RADIATION; PERTURBATIONS; MODELS AB We present an efficient method of computing cosmic microwave background (CMB) anisotropies in nonflat universes. First, we derive the Boltzmann equation for CMB temperature and polarization fluctuations produced by scalar perturbations in a general Robertson-Walker universe. We then apply the integral method in order to solve this equation, writing temperature and polarization anisotropies as a time integral over a geometrical term and a source term. The geometrical terms can be written using ultraspherical Bessel functions, which depend on curvature. These cannot be precomputed, as for flat space. Instead, we solve their differential equation directly for selected values of the multipoles. The resulting computational time is comparable to the flat-space case, improving over previous methods by 2-3 orders of magnitude. This allows one to compute highly accurate CMB temperature and polarization spectra, matter transfer functions, and their CMB normalizations for any cosmological model, thereby avoiding the need to use the various inexact fitting formulae that exist in the literature. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zaldarriaga, M (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. NR 40 TC 77 Z9 77 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1998 VL 494 IS 2 BP 491 EP 502 DI 10.1086/305223 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YZ796 UT WOS:000072292500002 ER PT J AU Zhang, QZ Ho, PTP Ohashi, N AF Zhang, QZ Ho, PTP Ohashi, N TI Dynamical collapse in W51 massive cores: CS (3-2) and CH3CN observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; ISM, clouds; ISM, individual (W51); ISM, kinematics and dynamics; stars, formation ID H-II REGIONS; RECOMBINATION LINE OBSERVATIONS; RADIO OBSERVATIONS; METHYL CYANIDE; STAR-FORMATION; VLA OBSERVATIONS; AMMONIA MASER; ORION-KL; CONTINUUM; EMISSION AB We present interferometric observations of the W51 region at 2 mm with the Nobeyama Millimeter Array. The 320 MHz band centered at 147 GHz covers transitions of the CS (3-2), CH3CN (8-7), H35 alpha, CH3OCH3 (7-6) and (6-6), and HCOOCH3 (12-11), as well as the 2 mm continuum. Toward two dense cores, W51e2 and W51e8, spectroscopic signatures of cloud collapse are present in all the molecular lines observed. Line asymmetries increase systematically toward transitions of larger optical depths, consistent with expected signatures of a centrally condensed infalling cloud. Furthermore, the disparity between the blueshifted and the redshifted emission of the CS line is enhanced when the line is synthesized at higher angular resolution. Given that the continuum source is embedded in the core, we are able to locate the emitting gas of the blueshifted emission on the rear side and the gas of the redshifted emission on the front side of the central star. The new observations confirm our infall interpretations regarding the e2 and e8 cores based on the NH3 data. The compact CH,CN emission allows us to identify velocity gradients in the e2 and e8 cores. The gradient in the e2 core is consistent with the spin-up motions proposed by Zhang Sr Ho in 1997. CH3CN emission reveals hot components in the W51e2, W51e8, and W51-North:dust cores. The rotational temperature in each core is greater than 100 K. In W51-North, we detected a dust peak coincident with the peak of the dense molecular core. There is no 3.6 cm continuum detected at a level of less than 1 mJy. Although H2O and OH masers in the neighborhood indicate outflow activities, high-velocity gas is not apparent in the CS (3-2). This source may represent an extremely early evolutionary stage: the phase of massive protostars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, QZ (reprint author), Natl Radio Astron Observ, 949 N Cherry Ave, Tucson, AZ 85721 USA. OI Zhang, Qizhou/0000-0003-2384-6589 NR 41 TC 102 Z9 105 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1998 VL 494 IS 2 BP 636 EP + DI 10.1086/305243 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YZ796 UT WOS:000072292500013 ER PT J AU Williams, JP Blitz, L AF Williams, JP Blitz, L TI A multitransition CO and CS (2-1) comparison of a star-forming and a non-star-forming giant molecular cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, clouds; ISM, individual (G216-2.5, Rosette Molecular Complex); ISM, molecules; ISM, structure; stars, formation ID FAR-INFRARED LUMINOSITY; OB ASSOCIATIONS; G216-2.5; COMPLEXES; GALAXY; ORION AB CO (3-2), CO (1-0), and CS (2-1) observations of clumps in the cold, low-luminosity cloud G216-2.5 discovered by Maddalena & Thaddeus are compared to the star-forming Rosette molecular cloud. The comparisons suggest that the clumps in a cloud may be characterized as being either dormant, incipient star forming, or star forming. In the Rosette molecular cloud, each set accounts for, respectively, 80%, 10%, and 10% of the total mass, but in G216-2.5, nearly 100% of the clumps are dormant. The physical conditions of the clumps in both clouds suggest a mass agglomeration evolutionary sequence from dormant to star-forming clumps. Detailed results for the clumps in both clouds are as follows. Clump excitation conditions are remarkably uniform in G216-2.5 but show wide variation in the Rosette. CO (3-2) integrated intensities and the ratio of(3-2) to (1-0) emission are significantly greater in the star-forming cloud and greatest of all in those clumps with embedded IRAS sources. The ratio of CO (3-2) to (1-0) line widths is also greater in the Rosette cloud. Peak clump CO (1-0) temperatures are greater in the Rosette than G216-2.5, implying higher gas kinetic temperatures, and are highest of all for those clumps associated with IRAS sources. The ratios of peak CO (3-2) to (1-0) temperatures, however, are comparable in the two clouds, which implies that the volume density of emitting gas in the clumps in each cloud is similar, n(H2) similar or equal to 10(3) cm(-3). The CS observations indicate the presence of denser gas, n(H2) similar to 10(5) cm(-3), in the clumps in each cloud. CS integrated intensities are generally an order of magnitude weaker than (CO)-C-13 emission in each cloud, but the ratio of the two is a factor of 2 less in G216-2.5. CS to (CO)-C-13 line width ratios are also lower in G216-2.5, which suggests that there is a deficiency of dense gas relative to the Rosette. Again, the star-forming clumps in the Rosette possess the highest ratios. In addition, CO (2-1) emission was mapped over the central region of G216-2.5 and compared to a CO (1-0) map. The ratio of (2-1) to (1-0) integrated intensities increases toward the clump edges, which is opposite to the Sakamoto et al. study of the Orion molecular cloud. High-resolution (CO)-C-13 (2-1) maps of one clump in each cloud are compared to (CO)-C-13 (1-0) maps for evidence of further fragmentation. The (2-1) radial profile is steeper than the (1-0) profile in each clump but decreases at the same relative rate in the two clumps despite their different absolute sizes. We conclude that the differences between clouds and clumps that are forming stars are most readily apparent in the warmer, denser gas traced by the CO (3-2) and CS (2-1) observations and note that there are two starless clumps in the Rosette molecular cloud with CO properties that are more characteristic of the star-forming clumps than the other starless clumps: these are the best candidates for the sites of future star formation in the cloud. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Williams, JP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Williams, Jonathan/B-1643-2009; OI Williams, Jonathan/0000-0001-5058-695X NR 33 TC 33 Z9 33 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1998 VL 494 IS 2 BP 657 EP 673 DI 10.1086/305233 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YZ796 UT WOS:000072292500014 ER PT J AU Rudiger, G von Rekowski, B Donahue, RA Baliunas, SL AF Rudiger, G von Rekowski, B Donahue, RA Baliunas, SL TI Differential rotation and meridional flow for fast-rotating solar-type stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; stars, rotation; turbulence ID TAYLOR-NUMBER PUZZLE; MAIN-SEQUENCE STARS AB Observations indicate that normalized surface differential rotation decreases for fast-rotating stars, that is, \Omega Delta\Omega proportional to Omega(-0.3). An increase of \Delta Omega\/Omega is provided, however, by the current Reynolds stress theory of differential rotation in stellar convection zones, without the inclusion of meridional dow. We compute both the pole-equator difference of the surface angular velocity and the meridional drift for various Taylor numbers to demonstrate that the inclusion of meridional how in the computations for fast rotation yields a systematic reduction of the resulting differential rotation. Our model's adiabatic and density-stratified convection zone, with stress-free surfaces and a thickness of 0.3 stellar radii, yields the relation \Delta Omega\/Omega proportional to Omega(-(0.15...0.30)) for stars with faster rotation than the Sun, in agreement with previous observations. If the Coriolis number rather than the Taylor number is varied, we find a maximum differential rotation of 20%. For stars with fast rotation, exponents of up to n ' similar or equal to 0.4 are found. All rotation laws exhibit superrotating equators. C1 Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Mt Wilson Observ, Pasadena, CA 91106 USA. Tennessee State Univ, Ctr Excellence Informat Syst, Ctr Automated Space Sci, Nashville, TN 37203 USA. RP Rudiger, G (reprint author), Astrophys Inst Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. NR 22 TC 27 Z9 27 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1998 VL 494 IS 2 BP 691 EP 699 DI 10.1086/305216 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YZ796 UT WOS:000072292500017 ER PT J AU Evans, NR Bohm-Vitense, E Carpenter, K Beck-Winchatz, B Robinson, R AF Evans, NR Bohm-Vitense, E Carpenter, K Beck-Winchatz, B Robinson, R TI Classical cepheid masses: U Aquilae SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, spectroscopic; Cepheids; stars, fundamental parameters; stars, individual (U Aquilae) ID RADIATIVE OPACITIES; STELLAR MODELS; LUMINOSITY; STARS; BINARIES; ORBIT AB We have obtained medium-resolution spectra (lambda/Delta lambda similar to 20,000) of the hot binary companion to the classical Cepheid U Aql with the Goddard High Resolution Spectrograph on the Hubble Space Telescope (HST). These have been used to determine the orbital velocity amplitude. Combining this with the orbital velocity amplitude of the Cepheid from the ground-based orbit and the mass of the companion inferred from its spectral type, we measure a mass of the Cepheid of 5.1 +/- 0.7 M.. We discuss the full sample of Cepheids for which we have determined masses with HST (S Mus, V350 Sgr, Y Car, and U Aql) and also SU Cyg (mass from IUE). The HST masses are in agreement with the luminosities predicted by recent evolutionary tracks with moderate overshoot. This comparison, however, may be altered by reassessment of Cepheid distances based on Hipparcos parallaxes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Comp Sci Corp, Astron Programs, Greenbelt, MD 20771 USA. RP Evans, NR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu; erica@bluemoon.astro.washington.edu; hrscarpenter@tmal.gsfc.nasa.gov; bbeck@bluemoon.astro.washington.edu; hrsrobinson@tma1.gsfc.nasa.gov RI Carpenter, Kenneth/D-4740-2012 NR 28 TC 17 Z9 17 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1998 VL 494 IS 2 BP 768 EP 772 DI 10.1086/305242 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YZ796 UT WOS:000072292500025 ER PT J AU Carilli, CL Harris, DE Pentericci, L Rottgering, HJA Miley, GK Bremer, MN AF Carilli, CL Harris, DE Pentericci, L Rottgering, HJA Miley, GK Bremer, MN TI An X-ray cluster at redshift 2.156? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, clusters, general; large-scale structure of universe; radio continuum, galaxies; X-rays, galaxies ID POWERFUL RADIO GALAXIES; MAGNETIC-FIELDS; CYGNUS-A; EMISSION AB We present X-ray observations of the narrow-line radio galaxy 1138-262 at z = 2.156 with the High Resolution Imager (HRI) on ROSAT. Observations at other wave bands, and in particular extremely high values of Faraday rotation of the polarized radio emission, suggest that the 1138-262 radio source is in a dense environment, perhaps a hot, cluster-type atmosphere. We detect X-ray emission from the vicinity of 1138-262, and we discuss possible origins for this emission. The X-ray, optical, and radio data all favor thermal emission from a hot cluster atmosphere as the mechanism responsible for the X-rays, although we cannot rule out a contribution from the active nucleus. If this interpretation is correct, then 1138-262 becomes the most distant, by far, of known X-ray-emitting clusters. The X-ray luminosity for 1138-262 is 6.7 +/- 1.3 x 10(44) ergs s(-1) for emitted energies between 2 and 10 keV. C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Smithsonian Astron Observ, Cambridge, MA 02138 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Carilli, CL (reprint author), Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA. NR 37 TC 14 Z9 14 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1998 VL 494 IS 2 BP L143 EP L146 DI 10.1086/311199 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YZ797 UT WOS:000072292600004 ER PT J AU McCarthy, MC Grabow, JU Travers, MJ Chen, W Gottlieb, CA Thaddeus, P AF McCarthy, MC Grabow, JU Travers, MJ Chen, W Gottlieb, CA Thaddeus, P TI Laboratory detection of the carbon chains HC(15)N and HC(17)N SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, molecules; line, identification; molecular data; molecular processes; radio lines ISM AB The linear cyanopolyynes HC(15)N and HC(17)N were detected in the laboratory by Fourier transform microwave spectroscopy. Enough rotational lines of each species were measured in the 5-11 GHz frequency range so that precise values for the rotational and centrifugal distortion constants can be determined and the entire rotational spectra of both molecules predicted to better than 1 km s(-1) in equivalent radial velocity over the range of interest to radio astronomy. Although there is a nearly constant decrement in line intensity from HC(3)N to HC(9)N of about seven, the decrement decreases by at least a factor of 2 on reaching HC(17)N, and as a result the lines of HC(17)N are nearly an order of magnitude stronger than predicted by extrapolation from the shorter cyanopolyynes. With a molecular weight of 219 amu and a rotational constant of slightly more than 50 MHz, HC(17)N is the longest carbon chain identified to date by high-resolution spectroscopy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 16 TC 42 Z9 42 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1998 VL 494 IS 2 BP L231 EP L234 DI 10.1086/311188 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YZ797 UT WOS:000072292600025 ER PT J AU Paczynski, B Stanek, KZ AF Paczynski, B Stanek, KZ TI Galactocentric distance with the OGLE and Hipparcos red clump stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy, center; Galaxy, fundamental parameters; Galaxy, stellar content; solar neighborhood; stars, horizontal-branch ID GALACTIC BAR; BULGE; WINDOW AB We compare red clump stars with parallaxes known to better than 10% in the Hipparcos catalog and corrected for interstellar extinction with the OGLE red clump stars in Baade's Window, also corrected for interstellar extinction. There are similar to 600 and similar to 10,000 such stars in the two data sets, respectively. We find empirically that the average I-band magnitude of red clump stars does not depend on their intrinsic color in the range 0.8 < (V-I)(0) < 1.4. The red clump luminosity function is well represented by a Gaussian with the peak at M-I0,M-m = -0.28 and the dispersion sigma(RC) approximate to 0.2 mag. This allows a single-step determination of the distance to the Galactic center and gives R-0 = 8.4 +/- 0.4 kpc. The number of red clump stars is so large that the formal statistical error is only similar to 1%. The local stars are relatively blue and have a small color dispersion: <(V -I)> = 1.01 and sigma(V-1) = 0.08, while for the bulge stars <(V-I)(0)> = 1.22 and sigma((V-1)0) = 0.14. Presumably, the bulge population has a broader range and a higher average metallicity than the local disk population. C1 Princeton Univ Observ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02174 USA. RP Paczynski, B (reprint author), Princeton Univ Observ, Peyton Hall, Princeton, NJ 08544 USA. EM bp@astro.princeton.edu; kstanek@cfa.harvard.edu NR 21 TC 156 Z9 161 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1998 VL 494 IS 2 BP L219 EP L222 DI 10.1086/311181 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YZ797 UT WOS:000072292600022 ER PT J AU Lynnerup, N Thomsen, JL Frohlich, B AF Lynnerup, N Thomsen, JL Frohlich, B TI Intra- and inter-observer variation in histological criteria used in age at death determination based on femoral cortical bone SO FORENSIC SCIENCE INTERNATIONAL LA English DT Article DE forensics; osteons; skeletal age estimation; variability ID ALGORITHM; OSTEONS AB The microscopic method of age at death determination was introduced by Kerley in 1965. The method, which relies on the quantification of selected elements in cortical bone tissue, has been widely used, and several other researchers have modified or added to the method. Yet, very few studies have been carried out dealing with the intra-and inter-observer error. Furthermore, when such studies have been completed, the statistical tools for assessing variability have not been adequate. This study presents the results of applying simple quantitative statistics on several counts of microscopic elements as observed on photographic images of cortical bone, in order to assess intra-and inter-observer error. Overall, substantial error was present at the level of identifying and counting secondary osteons, osteon fragments and Haversian canals. Only secondary osteons can be reliably identified, precluding the use of osteon fragments and Haversian canals. The observers in this study included experienced and inexperienced users of the microscopic method, yet the variability was uniformly large for all observers, suggesting fundamental problems in definition and identification of the structural elements. Until more rigorous definitions of such elements have been agreed upon, the use of microscopical methods must be discouraged as a sole or uncontrolled method of evaluating age at death. (C) 1998 Elsevier Science Ireland Ltd. C1 Univ Copenhagen, Lab Biol Anthropol, Panum Inst, Dept Forens Pathol, DK-2200 Copenhagen N, Denmark. Odense Univ, Inst Forens Med, Odense, Denmark. Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Lynnerup, N (reprint author), Univ Copenhagen, Lab Biol Anthropol, Panum Inst, Dept Forens Pathol, Blegdamsvej 3, DK-2200 Copenhagen N, Denmark. NR 29 TC 12 Z9 14 U1 5 U2 7 PU ELSEVIER SCI IRELAND LTD PI CLARE PA CUSTOMER RELATIONS MANAGER, BAY 15, SHANNON INDUSTRIAL ESTATE CO, CLARE, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD FEB 16 PY 1998 VL 91 IS 3 BP 219 EP 230 DI 10.1016/S0379-0738(97)00197-7 PG 12 WC Medicine, Legal SC Legal Medicine GA ZB830 UT WOS:000072512300006 PM 9530832 ER PT J AU Bennett, RA Wernicke, BP Davis, JL AF Bennett, RA Wernicke, BP Davis, JL TI Continuous GPS measurements of contemporary deformation across the northern Basin and Range province SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ZONE AB We have acquired and analyzed data from the northern Basin and Range (NEAR) continuous GPS network since July 1996. The RMS residual with respect to the best fitting lines through the individual station position estimates is 2-3 mm in the horizontal and 6-10 mm in the vertical. After the first 395 days of operation, uncertainties in horizontal velocity estimates are 1-2 mm/yr (1-sigma). Relative motion among NEAR sites located in eastern Nevada and in Utah is small, but east-west extension is significant assuming uniform strain accumulation across the whole network. The relative motion observed across the Wasatch fault zone is 2 +/- 2 mm/yr, east-west. Relative motions among stations in western Nevada and California, in contrast, are dominated by northwest, right-lateral shear. We infer an integrated grated deformation across the northern Basin and Range of 11 +/- 2 mm/yr, northwest. These rates are consistent with previous geodetic measurements. Our GPS velocity estimates, however, reveal a possibly abrupt transition from east-west extension in eastern Nevada and Utah to right-lateral shear in western Nevada. This transition is roughly coincident with the central Nevada seismic belt and is consistent with the right-oblique focal mechanisms of the 1954 Dixie Valley and Fairview Peak earthquakes. The transition also appears to correlate spatially with a transition in upper mantle structure. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Bennett, RA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 19 TC 55 Z9 57 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 15 PY 1998 VL 25 IS 4 BP 563 EP 566 DI 10.1029/98GL00128 PG 4 WC Geosciences, Multidisciplinary SC Geology GA YY192 UT WOS:000072122500040 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Sotheby's: The inside story. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 1998 VL 123 IS 3 BP 138 EP 138 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA YX080 UT WOS:000072004400066 ER PT J AU Riley, SM AF Riley, SM TI Tell me lies. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Riley, SM (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 1998 VL 123 IS 3 BP 169 EP 169 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA YX080 UT WOS:000072004400237 ER PT J AU Zhang, J Cui, W Juda, M McCammon, D Kelley, RL Moseley, SH Stahle, CK Szymkowiak, AE AF Zhang, J Cui, W Juda, M McCammon, D Kelley, RL Moseley, SH Stahle, CK Szymkowiak, AE TI Non-ohmic effects in hopping conduction in doped silicon and germanium between 0.05 and 1 K SO PHYSICAL REVIEW B LA English DT Article ID X-RAY SPECTROSCOPY; FIELD-DEPENDENCE; TRANSPORT; BOLOMETERS; ELECTRONS; TEMPERATURES; DETECTORS; 20-MK; NOISE; SI AB We have studied non-Ohmic effects In hopping conduction in moderately compensated ion-implanted Si:P, B (both n- and p-type) and neutron-transmutation-doped Ge:Ga,As over the temperature range 0.05-0.8 K and up to moderately strong electric fields. In the limit of small fields, where the current is proportional to applied voltage, the resistivities of these materials are approximated over a wide temperature range by the model of variable range hopping with a Coulomb gap: rho=rho(o) exp(T-o/T)(1/2). The samples included in this study have characteristic temperatures T-o in the range 1.4-60 K for silicon, and 22-60 K for germanium. We have compared our data to exponential and "hyperbolic-sine" field-effect models of the electrical nonlinearity: rho(E)=rho(0)e(-x) and rho(E)=rho(0)x/sinh(x), where x=eEl/kT, and to an empirical hot-electron model. The exponential field-effect model tends to be a good representation for the samples with high T-o at low T. The sinh model can match the data only at low fields. The hot-electron model fits our data well over a wide range of power in the low-T-o-high-T regime. We discuss the quantitative implications of these results for the application of these materials as thermometers for microcalorimeters optimized for high-resolution spectroscopy. [S0163-1829(98)05208-4]. C1 Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhang, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Moseley, Harvey/D-5069-2012; Kelley, Richard/K-4474-2012; OI Juda, Michael/0000-0002-4375-9688; Cui, Wei/0000-0002-6324-5772 NR 40 TC 45 Z9 45 U1 1 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD FEB 15 PY 1998 VL 57 IS 8 BP 4472 EP 4481 DI 10.1103/PhysRevB.57.4472 PG 10 WC Physics, Condensed Matter SC Physics GA YZ177 UT WOS:000072228000046 ER PT J AU Nason, JD Herre, EA Hamrick, JL AF Nason, JD Herre, EA Hamrick, JL TI The breeding structure of a tropical keystone plant resource SO NATURE LA English DT Article ID BARRO-COLORADO-ISLAND; FEMALE FIG WASPS; NEOTROPICAL TREE; GENE FLOW; CONSERVATION; DISPERSAL; CONSEQUENCES; PHENOLOGY; EVOLUTION; DENSITY AB Despite the recognized importance of maintaining viable populations of keystone plant resources in tropical wildlife parks and forested preserves, the critical question of what constitutes effective breeding units of these species has not been directly addressed. Here we use paternity analysis techniques to reconstruct the genotypes of pollen donor trees and to estimate pollen dispersal distances and breeding population size parameters for Panamanian populations of seven species of monoecious strangler figs (Ficus, Moraceae), a particularly widespread and influential group of keystone producers(1-3). Despite the minute size (1-2 mm) and short lifespan (2-3 d) of the species-specific wasp pollinators (Agaonidae, Chalcidoidea), pollen dispersal was estimated to occur routinely over distances of 5.8-14.2 km between widely spaced host trees, As a result of such extensive pollen movement, breeding units of figs comprise hundreds of intermating individuals distributed over areas of 106-632 km(2), an order of magnitude larger than has been documented for any other plant species. Moreover, these results should be generalizable to the 350 or so monoecious fig species that share this pollination system(4). The large areal extent of breeding units of these keystone plant resources has important implications for our understanding of both the evolution of tropical biodiversity and its maintenance by applied conservation efforts. C1 Univ Iowa, Dept Biol Sci, Iowa City, IA 52242 USA. Smithsonian Trop Res Inst, Ancon, Panama. Univ Georgia, Dept Bot, Athens, GA 30602 USA. Univ Georgia, Dept Genet, Athens, GA 30602 USA. RP Nason, JD (reprint author), Univ Iowa, Dept Biol Sci, 312 Chem Bldg, Iowa City, IA 52242 USA. NR 31 TC 191 Z9 207 U1 6 U2 39 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 12 PY 1998 VL 391 IS 6668 BP 685 EP 687 DI 10.1038/35607 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA YW872 UT WOS:000071982500049 ER PT J AU Falco, EE Kochanek, CS Munoz, JA AF Falco, EE Kochanek, CS Munoz, JA TI Limits on cosmological models from radio-selected gravitational lenses SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, observations; galaxies, distances and redshifts; gravitational lensing; radio continuum, galaxies ID PARKES SELECTED REGIONS; LUMINOSITY FUNCTION; REDSHIFT SURVEY; CONSTANT; GALAXIES; STATISTICS; UNIVERSE; QUASARS; DENSITY; CATALOG AB We are conducting a redshift survey of 177 flat-spectrum radio sources in three samples covering the 5 GHz flux ranges 50 - 100, 100 - 200, and 200 - 250 mJy. So far, we have measured 124 redshifts with completenesses of 80 %, 68 %, and 58 % for the bright, intermediate, and faint flux ranges. Using the newly determined redshift distribution, we can derive cosmological limits from the statistics of the six gravitational lenses in the Jodrell Bank-VLA Astrometric Survey sample of 2500 hat-spectrum radio sources brighter than 200 mJy at 5 GHz. For flat cosmological models with a cosmological constant, the limit using only radio data is Omega(0) > 0.27 at 2 sigma (0.47 < Omega(0) < 1.38 at 1 sigma). The limits are statistically consistent with those for lensed quasars, and the combined radio + optical sample requires Omega(0) > 0.38 at 2 sigma (0.64 < Omega(0) < 1.66 at 1 sigma) for our most conservative redshift completeness model, assuming that there are no quasar lenses produced by spiral galaxies. Our best-fit model improves by approximately 1 sigma if extinction in the early-type galaxies makes the lensed quasars fainter by Delta m = 0.58 +/- 0.45 mag, but we still find a limit of Omega(0) > 0.26 at 2 sigma in flat cosmologies. The increasing fraction of radio galaxies as compared to quasars at fainter radio fluxes (rising from similar to 10 % at 1 Jy to similar to 50 % at 0.1 Jy) explains why lensed optical emission is common for radio lenses and partly explains the red color of radio-selected lenses. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Falco, EE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 58 TC 188 Z9 189 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 1998 VL 494 IS 1 BP 47 EP 59 DI 10.1086/305207 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY520 UT WOS:000072155800005 ER PT J AU Carilli, CL Menten, KM Reid, MJ Rupen, MP Yun, MS AF Carilli, CL Menten, KM Reid, MJ Rupen, MP Yun, MS TI Redshifted neutral hydrogen 21 centimeter absorption toward red quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, ISM; quasars, absorption lines; radio lines, galaxies ID SPECTRUM RADIO-SOURCES; H-I ABSORPTION; GRAVITATIONAL LENS; EINSTEIN RING; ALPHA SYSTEMS; GALAXY; DUST; IDENTIFICATIONS; OBSCURATION; POPULATION AB We have searched for redshifted neutral hydrogen 21 cm absorption toward sources from the Stickel et al. "red quasar" subsample. The red quasar subsample is taken from the 1 Jy sample of flat-spectrum radio sources and is comprised of the 15 sources that are undetected on the POSS. Five of these red quasars have been searched for redshifted H I 21 cm absorption to optical depth levels of a few percent, and four show strong absorption, with neutral hydrogen column densities between 4 and 80 x 10(18) x (T-s/f) cm(-2). This 80 % success rate for the red quasars compares to the much lower success rate of only 11 % for detecting H I 21 cm absorption associated with optically selected Mg II absorption line systems. The large neutral hydrogen column densities seen toward the Stickel et al. red quasars provide circumstantial evidence supporting the dust-reddening hypothesis, as opposed to an intrinsically red spectrum for the AGN emission mechanism. The lower limits to rest-frame values of A, are between two and seven, leading to lower limits to the spin temperatures for the neutral hydrogen between 50 K and 1000 K, assuming a Galactic dust-to-gas ratio. We consider the question of biases in optically selected samples of quasars caused by dust obscuration. Overall, the data on the red quasar subsample support the models of Fall & Pei for dust obscuration by damped Ly alpha absorption line systems and suggest that (1) there may be a significant, but not dominant, population of quasars missing from optically selected samples because of dust obscuration, perhaps as many as 20 % at the POSS limit for an optical sample with a redshift distribution similar to the 1 Jy flat-spectrum quasar sample, and (2) optically selected samples may miss about one-half the high column density quasar absorption line systems. The redshifted H I 21 cm absorption line detections presented herein are toward the sources 0108 + 388 at z = 0.6685, 0500 + 019 at z = 0.5846, and 1504 + 377 at z = 0.6733. No absorption is seen toward 2149 + 056 at z = 0.740 at a level below that seen for the three detections, although there is some uncertainty in this case as to the expected line redshift. In some systems, the absorbing gas is in the vicinity of the AGN, as either circumnuclear material or material in the general ISM of the AGN's host galaxy, as is probably the case for 0108 + 388 and 1504 + 377, and in other systems the absorption is by gas associated with galaxies cosmologically distributed along the line of sight to the quasar, as may be the case for 0500 + 019. The Westerbork Synthesis Radio Telescope spectrum of 1504 + 377 confirms the lack of H I 21 cm absorption associated with the narrow molecular absorption line system at z = 0.67150. C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA. NR 45 TC 70 Z9 70 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 FEB 10 PY 1998 VL 494 IS 1 BP 175 EP 182 DI 10.1086/305191 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY520 UT WOS:000072155800014 ER PT J AU Doeleman, SS Lonsdale, CJ Greenhill, LJ AF Doeleman, SS Lonsdale, CJ Greenhill, LJ TI VLBI imaging of the 86 GHz SiO maser emission in the circumstellar envelope of VX Sagittarii SO ASTROPHYSICAL JOURNAL LA English DT Article DE masers; circumstellar matter; radio lines, stars; stars, individual (VX Sagittarii) ID LATE-TYPE STARS; INTERFEROMETRIC OBSERVATIONS; NUMERICAL-CALCULATIONS; LINEAR-POLARIZATION; MAGNETIC-FIELDS; MIRA VARIABLES; EVOLVED STARS; TRANSITIONS; INTENSITY AB We have observed and imaged the SiO maser source in the late-type star VX Sgr with a single VLBI baseline at 3.5 mm wavelength. Phase-referenced channel maps with a beamwidth of -0.4 mas show multiple components over a LSR velocity range of -1 to 24 km s(-1) and many of the maser features display velocity widths smaller than 1 km s(-1). The maser spots in this 86 GHz transition (v = 1, J = 2 --> 1) are arranged in an irregular ring-shaped configuration of diameter similar to 30 mas, echoing the structures found in the J = 1 --> 0 transition at 43 GHz around several Mira variables and VX Sgr itself. Unlike previous observations of SiO masers, in VX Sgr we detect a clear, systematic velocity gradient of similar to 0.6 km s(-1) AU(-1) among the strongest complex of masers on the southernmost portion of the ring structure. This velocity gradient can be interpreted as a rigid rotation of the circumstellar envelope with v sin i similar to 13 km s(-1). Maser emission is not detected on long (5000 km) baselines, which places a 0.1 mas lower limit on the size of strong maser spots. C1 MIT, Haystack Observ, Westford, MA 01886 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Doeleman, SS (reprint author), MIT, Haystack Observ, Off Route 40, Westford, MA 01886 USA. NR 35 TC 21 Z9 21 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 1998 VL 494 IS 1 BP 400 EP 408 DI 10.1086/305199 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY520 UT WOS:000072155800032 ER PT J AU Brown, TM Kotak, R Horner, SD Kennelly, EJ Korzennik, S Nisenson, P Noyes, RW AF Brown, TM Kotak, R Horner, SD Kennelly, EJ Korzennik, S Nisenson, P Noyes, RW TI A search for line shape and depth variations in 51 Pegasi and tau Bootis SO ASTROPHYSICAL JOURNAL LA English DT Article DE line, profiles; planetary systems; stars, individual (51 Pegasi, 7 Bootis); stars, oscillations AB Spectroscopic observations of 51 Pegasi and tau Bootis show no periodic changes in the shapes of their line profiles; these results for 51 Peg are in significant conflict with those reported by Gray & Hatzes. Our detection limits are small enough to rule out nonradial pulsations as the cause of the variability in tau Boo, but not in 51 Peg. The absence of line shape changes is consistent with these stars' radial velocity variability arising from planetary mass companions. C1 Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brown, TM (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, 3450 Mitchell Lane,POB 3000, Boulder, CO 80307 USA. OI Kotak, Rubina/0000-0001-5455-3653 NR 13 TC 16 Z9 16 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 1998 VL 494 IS 1 BP L85 EP L88 DI 10.1086/311168 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY522 UT WOS:000072156000020 ER PT J AU Mendez, M van der Klis, M van Paradijs, J Lewin, WHG Vaughan, BA Kuulkers, E Zhang, W Lamb, FK Psaltis, D AF Mendez, M van der Klis, M van Paradijs, J Lewin, WHG Vaughan, BA Kuulkers, E Zhang, W Lamb, FK Psaltis, D TI Discovery of a second kilohertz quasi-periodic oscillation peak in 4U 1608-52 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars, neutron; stars, individual (4U 1608-52); X-rays, stars ID RAY AB Using a new technique to improve the sensitivity to weak quasi-periodic oscillations (QPOs), we discovered a new QPO peak at about 1100 Hz in the March 1996 outburst observations of 4U 1608-52, simultaneous with the similar to 600-900 Hz peak previously reported from these data. The frequency separation between the upper and the lower QPO peaks varied significantly from 232.7 +/- 11.5 Hz on March 3 to 293.1 +/- 6.6 Hz on March 6. This is the first case of a variable kilohertz peak separation in an atoll source. We discuss to what extent this result could be accommodated in beat-frequency models such as proposed for the kilohertz QPOs. We measured the rms fractional amplitude of both QPOs as a function of energy, and we found that the relation is steeper for the lower than for the upper frequency peak. This is the first source where such a difference between the energy spectrum of the two kilohertz QPOs could be measured. C1 Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Univ Nacl La Plata, Fac Ciencias Astron & Geofis, RA-1900 La Plata, Buenos Aires, Argentina. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. MIT, Space Res Ctr, Cambridge, MA 02139 USA. CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. Univ Oxford, Nucl & Astrophys Lab, Oxford OX1 3RH, England. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mendez, M (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. RI Mendez, Mariano/C-8011-2012 OI Mendez, Mariano/0000-0003-2187-2708 NR 25 TC 93 Z9 93 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 10 PY 1998 VL 494 IS 1 BP L65 EP L69 DI 10.1086/311162 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY522 UT WOS:000072156000016 ER PT J AU Sari, R AF Sari, R TI The observed size and shape of gamma-ray burst afterglow SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays, bursts; hydrodynamics; relativity; shock waves AB The detection of delayed emission in X-ray, optical, and radio wavelength, or "afterglow," following a gamma-ray burst can be described as the emission of a relativistic shell decelerating upon collision with the interstellar medium. We show that the observed radiation surface has well-defined bright edges. We derive an explicit expression for the size as a function of time, and obtain the surface brightness distribution. This might be directly observed if the burst occurs at a small redshift so that its radio signal can be resolved. The size and shape are relevant for detailed analysis of scintillation or microlensing. We show that the effective Lorentz factor depends on the observed frequency and that it is higher for frequencies above the synchrotron typical frequency (optical and X-ray) than for low frequencies (radio). Consequently, transition to nonrelativistic evolution will be observed first in low frequencies and only a factor of similar to 2 later in the high frequencies. C1 Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sari, R (reprint author), Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. EM sari@shemesh.fiz.huji.ac.il NR 11 TC 98 Z9 98 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 1998 VL 494 IS 1 BP L49 EP L52 DI 10.1086/311160 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY522 UT WOS:000072156000012 ER PT J AU Boughman, JW AF Boughman, JW TI Vocal learning by greater spear-nosed bats SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE bat communication; Phyllostomus hastatus; group signatures; social learning ID DOLPHINS TURSIOPS-TRUNCATUS; CALLS; SIGNALS; PLASTICITY; MIMICRY; SONG; CONVERGENCE AB Vocal learning is well known among passerine and psittacine birds, but most data on mammals are equivocal. Specific benefits of vocal learning are poorly understood for most species. One case where vocal learning should be favoured by selection is where calls indicate group membership and group mates are unrelated. Female greater spear-nosed bats, Phyllostomus hastatus, live in stable groups of unrelated bats and use loud, broadband calls to coordinate foraging movements of social group mates. Bats benefit from group foraging. Calls differ between female social groups and cave colonies, and playback experiments demonstrate that bats perceive these acoustic differences. Here I show that the group distinctive structure of calls arises through vocal learning. Females change call structure when group composition changes, resulting in increased similarity among new social group mates. Comparisons of transfers with age-matched half-sibs indicate that call changes are not simply due to maturation, the physical environment or heredity. These results suggest that studies testing vocal learning in mammals could profit by focusing on vocalizations that signify group membership. C1 Univ Maryland, Dept Zool Res, Smithsonian Inst, College Pk, MD 20742 USA. Univ Maryland, Dept Zool, College Pk, MD 20742 USA. RP Boughman, JW (reprint author), Univ Maryland, Dept Zool Res, Smithsonian Inst, Natl Zool Pk, College Pk, MD 20742 USA. NR 39 TC 129 Z9 131 U1 2 U2 31 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 FEB 7 PY 1998 VL 265 IS 1392 BP 227 EP 233 DI 10.1098/rspb.1998.0286 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA YW976 UT WOS:000071993600009 PM 9493408 ER PT J AU Mackie, G Fabbiano, G AF Mackie, G Fabbiano, G TI Evolution of gas and stars in the merger galaxy NGC 1316 (Fornax A) SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies, individual (NGC 1316); galaxies, interactions; galaxies, peculiar; galaxies, photometry; galaxies, structure; X-rays ID HUBBLE-SPACE-TELESCOPE; SHELL GALAXIES; DISK GALAXIES; INTERSTELLAR MATTER; APERTURE SYNTHESIS; ELLIPTIC GALAXIES; NEUTRAL HYDROGEN; MOLECULAR GAS; IONIZED-GAS; X-RAYS AB We present optical and archival X-ray data on the disturbed-morphology radio elliptical galaxy NGC 1316 (Fornax A), which displays numerous low surface brightness shells, loops, and tails. An extended (81'' x 27'', or 9 kpc x 3 kpc) emission-line region (EELR) at a projected distance of 35 kpc from the nucleus has been discovered in an approximately 90 kpc x 35 kpc, 3.0 x 10(9) L-B. tidal tail. The position and extreme size of the EELR suggest that it is related to the merger process. We suggest that the ionization mechanism of the EELR is shock excitation and that the gas is a remnant from the merger progenitor. X-ray emission is detected near two tidal tails. Hot, similar to 5 x 10(6) K, gas is probably the predominant gas component in the tidal-tail interstellar medium. However, based on the current tidal-tail (cold + warm + hot) gas mass, a large fraction of the progenitor gas may already reside in the nucleus of NGC 1316. The numerous and varied tidal-tail system suggests that a disk-disk or disk-E merger could have taken place greater than or equal to 1 Gyr ago, while a low-mass, gas-rich galaxy would have started to merge similar to 0.5 Gyr ago. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mackie, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 52 TC 25 Z9 25 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 1998 VL 115 IS 2 BP 514 EP 524 DI 10.1086/300203 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW535 UT WOS:000071946100013 ER PT J AU Schlegel, EM Petre, R Loewenstein, M AF Schlegel, EM Petre, R Loewenstein, M TI ROSAT observations of X-ray-faint S0 galaxies: NGC 1380 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies, individual (NGC 1380); X-rays ID PSPC OBSERVATIONS; ELLIPTIC GALAXIES; EMISSION; SAMPLE; ABUNDANCES; DISCOVERY; SPECTRA; MATTER; ASCA; GAS AB We used the ROSAT Position Sensitive Proportional Counter (PSPC) to obtain a 13 ks exposure and the ROSAT HRI to obtain a 42.5 ks exposure of the faint SO galaxy NGC 1380. We show that the PSPC spectrum can be modeled as a thermal spectrum with kT similar to 0.5 keV, which is consistent with emission from a hot interstellar medium. We do not detect any emission from a hard component; the 90% upper limit is consistent with the trend for the scaled-up luminosities of X-ray-emitting point sources. The radial profiles from the PSPC and HRI data support the spectral fitting, because each profile is more sharply concentrated than the optical light (which reflects the stellar distribution), in contrast to other E/SO galaxies. The PSPC radial profile is consistent with emission from a point source, because of the larger point-spread function; the HRI profile reveals the presence of extended hot gas. We also extend the L(X)-L(B) plane, described by Matsumoto et al. in the range 10.8 < log L(B) < 11.3, to log L(B) similar to 10.5. We extend this plane separately for the hard discrete and the soft thermal components and show that the scaling relation for the hard component continues to at least log L(B) similar to 10.5. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. RP Schlegel, EM (reprint author), Smithsonian Astrophys Observ, Mail Stop 4,60 Garden St, Cambridge, MA 02138 USA. NR 45 TC 8 Z9 8 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 1998 VL 115 IS 2 BP 525 EP 534 DI 10.1086/300217 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW535 UT WOS:000071946100014 ER PT J AU Caldwell, N Armandroff, TE Da Costa, GS Seitzer, P AF Caldwell, N Armandroff, TE Da Costa, GS Seitzer, P TI Dwarf elliptical galaxies in the M81 Group: The structure and stellar populations of BK5N and F8D1 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies, abundances; galaxies, clusters, individual (M81); galaxies, dwarf; galaxies, stellar content; galaxies, structure ID COLOR-MAGNITUDE DIAGRAM; SURFACE BRIGHTNESS GALAXIES; GLOBULAR-CLUSTER SYSTEMS; SPHEROIDAL GALAXY; GIANT BRANCH; CCD PHOTOMETRY; METALLICITY RELATION; FORNAX CLUSTER; STAR-FORMATION; VIRGO CLUSTER AB those of the Local Group. It has therefore provided a different environment for the evolution of its member galaxies. We have carried out a CCD survey of the M81 Group to search for analogs to Local Group dwarf elliptical (dE) galaxies. All the M81 dwarfs previously identified in photographic surveys were recovered, and we also discovered several new systems whose surface brightnesses fall within the range found for Local Group dE's. We have obtained Hubble Space Telescope Wide Field Planetary Camera 2 images through the F555W and F814W filters of two M81 Group dE's, BK5N and a new system, designated F8D1. The resulting color-magnitude diagrams show the upper 2 mag of the red giant branch. The I magnitudes of the red giant branch tip in both galaxies yield distances that are consistent with membership in the M81 Group. Surface brightness and total magnitude measurements indicate that BK5N and F8D1 have similar central surface brightnesses (24.5 and 25.4 mag arcsec(-2) in V, respectively), but F8D1's larger length scale results in its being 3 mag more luminous than BK5N. BK5N lies on the relation between central surface brightness and absolute magnitude defined by Local Group dwarf elliptical galaxies, but F8D1 does not. F8D1 is more luminous for its central surface brightness than the relation predicts, similar to the large low surface brightness dwarf galaxies found in, for example, Virgo. The mean color of the giant branch is used to establish the mean abundance of each galaxy. F8D1, the more luminous galaxy, is significantly more metal-rich ([Fe/H] approximate to -1.0) than BK5N ([Fe/H] approximate to -1.7). Both BK5N and F8D1 lie on the relation between absolute magnitude and metal abundance defined by Local Group dwarf elliptical galaxies. However, as regards the relation between central surface brightness and metal abundance, BK5N again follows the Local Group dwarfs while F8D1 deviates significantly from this relation. This suggests that the total amount of luminous matter is more fundamental in controlling metal enrichment than the surface density of luminous matter. We have also used the color width of the giant branch compared with the photometric errors to establish abundance ranges in both galaxies, the sizes of which are comparable to those in Local Group dE's. From the numbers and luminosities of asymptotic giant branch stars more luminous than the red giant branch tip, we infer that, again like many of the Local Group dE's, both BK5N and F8D1 have had extended epochs of star formation. F8D1 contains stars as young as 3-4 Gyr, while in BK5N stars as young as similar to 8 GYr are present. The fractions of intermediate-age population, at similar to 30%, are similar in both galaxies. Further, one globular cluster has been found in F8D1, but none are present in BK5N. These numbers of clusters are consistent with our expectations from Local Group dwarfs. Overall, we iind that BK5N is similar in all respects to the Local Group dE's. Thus, despite the different environments of the M81 Group and the Local Group, dwarf galaxies of very similar properties are present in each. F8D1, on the other hand, has no Local Group counterpart and is indeed rare even in large clusters of galaxies. Our study of its stellar population is the first for a large, low surface brightness dwarf. C1 Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. Natl Opt Astron Observ, Kitt Peak Natl Observ, Tucson, AZ 85726 USA. Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Weston, ACT 2611, Australia. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Caldwell, N (reprint author), Smithsonian Inst, FL Whipple Observ, POB 97, Amado, AZ 85645 USA. NR 93 TC 91 Z9 91 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 1998 VL 115 IS 2 BP 535 EP 558 DI 10.1086/300233 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW535 UT WOS:000071946100015 ER PT J AU Fridlund, CVM Liseau, R Gullbring, E AF Fridlund, CVM Liseau, R Gullbring, E TI The physical structure of the Herbig Haro object HH 29 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars formation; ISM : jets and outflows; ISM : individual objects : HH 29 ID MOLECULAR OUTFLOWS; BOW SHOCK; HH-29; COMPLEX; MODELS; FIELD; STARS; CLOUD; JET; UV AB We have obtained Echelle spectra covering a number of important shock diagnostic emission lines, mapping out the full extent of the Herbig-Haro object HH 29. Through this, the velocity field, the level of excitation and the electron density have all been determined with a spatial resolution of 1 "-2 " and a spectral resolution of 10 km s(-1) -20 km s(-1) respectively. Our observations of shock diagnostic lines allow us to produce an empirical 3D description (velocity is the third dimension) of F(H alpha), the level of excitation and the electron density. Our results indicate that HH 29 is among the Herbig-Haro objects with the highest level of excitation. We derive electron densities of between a few thousand cm(-3) and 10(4) cm(-3) in 'clumps' interspersed in an 'inter-clump medium' of density similar to 300 cm(-3). The spatial scale of the clumps is less than or similar to 2 ", and the velocity dispersion of individual clumps is on the order of 30km s(-1) -50 km s(-1), implying that the 'knotty' structure obvious in high spatial resolution images also exist in 3 dimensions. Based on the morphological and spectroscopical data, HH 29 appears to consist of a number of HH-knots where the shock is located on the side of the object oriented towards the originating source in some and on the opposite side in others. We find that HH 29 is best explained as an aggregate of clumps interacting with ambient material on the side away from the originating source, and also being shocked by a faster wind on the side towards the originating source. C1 European Space Technol Ctr, European Space Agcy, Dept Space Sci, Div Astrophys, NL-2200 AG Noordwijk, Netherlands. Stockholm Observ, S-13336 Saltsjobaden, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02158 USA. RP Fridlund, CVM (reprint author), European Space Technol Ctr, European Space Agcy, Dept Space Sci, Div Astrophys, NL-2200 AG Noordwijk, Netherlands. EM mfridlun@estec.esa.nl; rene@astro.su.se; erik@astro.su.se NR 30 TC 5 Z9 5 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 1 PY 1998 VL 330 IS 1 BP 327 EP 335 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW755 UT WOS:000071970100044 ER PT J AU Kaluzny, J Kubiak, M Szymanski, M Udalski, A Krzeminski, W Mateo, M Stanek, KZ AF Kaluzny, J Kubiak, M Szymanski, M Udalski, A Krzeminski, W Mateo, M Stanek, KZ TI The optical gravitational lensing experiment. Variable stars in globular clusters - IV. Fields 104A-E in 47 Tucanae SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article DE globular clusters, individual, NGC 104; star, variables, other; blue stragglers; binaries, eclipsing; HR diagram; Magellanic clouds ID RR LYRAE STARS; SYSTEMS; MAGNITUDE; DISCOVERY; SEARCH AB Five fields located close to the center of the globular cluster NGC 104 = 47 Tuc were surveyed in a search for variable stars. We present V-band light curves for 42 variables. This sample includes 13 R.R Lyr stars - 12 of them belong to the Small Magellanic Cloud (SMC) and 1 is a background object from the galactic halo. Twelve eclipsing binaries were identified - 9 contact systems and 3 detached/semi-detached systems. Seven eclipsing binaries are located in the blue straggler region on the cluster color-magnitude diagram (CMD) and four binaries can be considered main-sequence systems. One binary is probably a member of the SMC. Eight. contact binaries are likely members of the cluster and one is most probably a foreground star. We show that for the surveyed region of 47 Tuc, the relative frequency of contact binaries is very lour as compared with other recently surveyed globular clusters. The sample of identified variables also includes 15 red variables with periods ranging from about 2 days to several weeks. A large fraction of these 15 variables probably belong to the SMC but a few stars are likely to be red giants in 47 Tuc. VI photometry for about 50 000 stars from the cluster fields was obtained as a by product of our survey(1). C1 Warsaw Univ Observ, PL-00478 Warsaw, Poland. Las Campanas Observ, Carnegie Observ, La Serena, Chile. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaluzny, J (reprint author), Warsaw Univ Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. NR 28 TC 31 Z9 31 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEXA PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD FEB PY 1998 VL 128 IS 1 BP 19 EP 28 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZA584 UT WOS:000072379200003 ER PT J AU Connaughton, V Akerlof, CW Biller, S Boyle, P Buckley, J Carter-Lewis, DA Catanese, M Cawley, MF Fegan, DJ Finley, J Gaidos, J Hillas, AM Lamb, RC Lessard, R McEnery, J Mohanty, G Porter, NA Quinn, J Rose, HJ Schubnell, MS Sembroski, G Srinivasan, R Weekes, TC Wilson, C Zweerink, J AF Connaughton, V Akerlof, CW Biller, S Boyle, P Buckley, J Carter-Lewis, DA Catanese, M Cawley, MF Fegan, DJ Finley, J Gaidos, J Hillas, AM Lamb, RC Lessard, R McEnery, J Mohanty, G Porter, NA Quinn, J Rose, HJ Schubnell, MS Sembroski, G Srinivasan, R Weekes, TC Wilson, C Zweerink, J TI A search for TeV gamma-ray bursts on a 1-second time-scale SO ASTROPARTICLE PHYSICS LA English DT Article DE TeV astronomy; gamma-ray bursts; primordial black holes ID PRIMORDIAL BLACK-HOLES; ASTRONOMY; ENERGIES AB Although atmospheric Cherenkov telescopes have restricted fields of view, their fluence sensitivity warrants a search for gamma-ray burst phenomena. A search for 400 GeV gamma-ray bursts on a 1 s time-scale using archival data taken between 1988 and 1992 with the Whipple Collaboration 10 m reflector is presented. No evidence of such bursts is found. Bursts of TeV gamma rays have been predicted from exotic astrophysical objects such as Primordial Black Holes and Cosmic Strings. An upper limit to the number density of exploding PBH of 3.0 +/- 1.0 x 10(6) pc(-3) yr(-1) is calculated. (C) 1998 Elsevier Science B.V. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Cambridge, MA 02138 USA. Natl Univ Ireland Univ Coll Dublin, Dublin 4, Ireland. Univ Michigan, Ann Arbor, MI 48109 USA. Univ Leeds, Leeds LS2 9JT, W Yorkshire, England. Iowa State Univ, Ames, IA 50011 USA. St Patricks Coll, Maynooth, Kildare, Ireland. Purdue Univ, W Lafayette, IN 47907 USA. RP Connaughton, V (reprint author), NASA, George C Marshall Space Flight Ctr, ES84, Huntsville, AL 35812 USA. EM vc@msfc.nasa.gov RI McEnery, Julie/D-6612-2012 NR 25 TC 18 Z9 18 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 1998 VL 8 IS 3 BP 179 EP 191 DI 10.1016/S0927-6505(97)00055-8 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA YX877 UT WOS:000072088700006 ER PT J AU Perna, R Loeb, A AF Perna, R Loeb, A TI Probing the mass fraction of MACHOs in extragalactic halos SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies, halos; gravitational lensing; quasars, general ID ACCRETION DISKS; GALACTIC HALO; DENSITY; QUASARS; GALAXIES; OBJECTS AB Current microlensing searches calibrate the mass fraction of the Milky Way halo that is in the form of massive astrophysical compact halo objects (MACHOs). We show that surveys like the Sloan Digital Sky Survey (SDSS) can probe the same quantity in halos of distant galaxies. Microlensing of background quasars by MACHOs in intervening galaxies would distort the equivalent width distribution of the quasar emission lines by an amplitude that depends on the projected quasar-galaxy separation. For a statistical sample of similar to 10(5) quasars as expected in the SDSS, this distortion is detectable at the greater than or similar to 2 sigma level out to a quasar-galaxy impact parameter of several tens of kpc, as long as extragalactic halos are made of MACHOs. Detection of this signal would test whether the MACHO fraction inferred for the Milky Way halo is typical of other galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perna, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 30 TC 2 Z9 2 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP 523 EP 528 DI 10.1086/305170 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW232 UT WOS:000071911700003 ER PT J AU Romanowsky, AJ Kochanek, CS AF Romanowsky, AJ Kochanek, CS TI Twisting of X-ray isophotes in triaxial galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, individual (NGC 720); galaxies, kinematics and dynamics; galaxies, structure; X-rays, galaxies ID CCD SURFACE PHOTOMETRY; COLD DARK MATTER; ELLIPTIC GALAXIES; INTRINSIC SHAPES; DISSIPATIONLESS COLLAPSE; ELONGATED ELLIPTICALS; SPHERICAL GALAXIES; MERGER REMNANTS; STELLAR-SYSTEMS; HALOS AB We investigate X-ray isophote twists created by triaxiality differences between the luminous stellar distributions and the dark halos in elliptical galaxies. For a typically oblate luminous galaxy embedded in a more prolate halo formed by dissipationless collapse, the triaxiality difference of Delta T similar or equal to 0.7 leads to typical isophote twists of [Delta psi(X)] similar or equal to 16 degrees +/- 19 degrees at 3 effective stellar radii. In a model that includes baryonic dissipation, the effect is smaller, with Delta T similar or equal to 0.3 and [Delta psi(X)] similar or equal to 5 degrees +/- 8 degrees. Thus, accurate measurements of X-ray isophote twists may be able to set constraints on the interactions between baryons and dissipationless dark matter during galaxy formation. The 30 degrees X-ray isophote twist in the E4 galaxy NGC 720 cannot be reproduced by our model, suggesting an intrinsic misalignment between the halo and the stars rather than a projection effect. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romanowsky, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS-10,60 Garden St, Cambridge, MA 02138 USA. NR 83 TC 19 Z9 19 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP 641 EP 649 DI 10.1086/305151 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW232 UT WOS:000071911700014 ER PT J AU Trotter, AS Moran, JM Rodriguez, LF AF Trotter, AS Moran, JM Rodriguez, LF TI Anisotropic radio scattering of NGC 6334B SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, individual (NGC 6334B); H II regions; ISM, individual (NGC 6334A); ISM, magnetic fields; radio continuum, ISM; scattering ID INTERSTELLAR-MEDIUM; BROADENED IMAGE; MAGNETOGASDYNAMIC TURBULENCE; DENSITY-FLUCTUATIONS; ALFVENIC TURBULENCE; GALACTIC-CENTER; SCINTILLATION; CYGNUS-X-3; OUTFLOWS; SHAPE AB The extragalactic radio source NGC 6334B is the most strongly scattered object known, with an angular size of 3" at 20 cm wavelength. Its angular size scales as the square of the observing wavelength, and its phase structure function has a power-law dependence on projected baseline length. These properties suggest that NGC 6334B is a point source, probably a quasar, scatter broadened by an intervening region of turbulent plasma. The line of sight to the source intercepts the northern lobe of the bipolar H II region NGC 6334A, which is probably the source of the scattering. We discuss observations of NGC 6334B with the VLA at 1.4, 2, 6, 20, and 90 cm, and with the VLBA at 1.4, 3.6, and 6 cm. The VLA observations indicate that the scattering disk of NGC 6334B is anisotropic, with an axial ratio of similar to 1.2 at 20 and 6 cm, and similar to 1.5 at 2 cm. This anisotropy is probably due to the effects of a magnetic field in the scattering medium. The position angle of the scattering disk implies that the mean projected magnetic field direction is parallel to the outflow from NGC 6334A. The position angle of the scattering disk rotates slightly between 6 and 2 cm; we use this rotation to place an upper limit on the outer scale of turbulence, r(out) less than or similar to 10(16) cm. We present a new algorithm to detect the presence of weak (<3 sigma) fringes in interferometric data. Detections of low-level excess visibility on long VLBA baselines at 3.6 cm place an upper limit on the inner dissipative scale of turbulence r(in) of 10(11-12) cm, while the baseline scaling of fringe visibility amplitude and the wavelength scaling of scattering-disk size place a lower limit on r, of 5 x 10(6) cm. Nearby high-velocity (-80 km s(-1)) H2O maser features show little sign of broadening, implying that they are in front of, or less than 100 pc behind, the scattering region. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Autonomous Univ Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Trotter, AS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 36 TC 34 Z9 35 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP 666 EP 679 DI 10.1086/305142 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW232 UT WOS:000071911700016 ER PT J AU Snowden, SL Egger, R Finkbeiner, DP Freyberg, MJ Plucinsky, PP AF Snowden, SL Egger, R Finkbeiner, DP Freyberg, MJ Plucinsky, PP TI Progress on establishing the spatial distribution of material responsible for the 1/4 kev soft X-ray diffuse background local and halo components SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; Galaxy, halo; X-rays, galaxies; X-rays, ISM ID H-I STRUCTURE; INTERSTELLAR-MEDIUM; MOLECULAR CLOUD; GALACTIC HALO; ROSAT; GAS; EMISSION; SPECTRUM; SUPERBUBBLE; REGIONS AB In this paper we present a new look at the distribution of emission responsible for the soft X-ray diffuse background (SXRB) using ROSAT all-sky survey data. This is prompted by the demonstration of the existence of extensive 1/4 keV emission in the Galactic halo that was not considered in the most successful previous model, in which the bulk of the observed 1/4 keV X-rays originated in a Local Hot Bubble (LHB) that surrounds the Sun. The basic distribution can be represented by two angularly varying Galactic components (the LHB and an X-ray halo) and an isotropic extragalactic component. In addition, there are the distinct enhancements of supernova remnants, superbubbles, and clusters of galaxies. Using the negative correlation between the SXRB and DIRBE-corrected IRAS 100 mu m intensity, we find a LHB that is similar to previous models, although it is possibly more limited in extent. The emission of the LHB varies by a factor of similar to 3.3 with direction and produces ROSAT 1/4 keV intensities between similar to 250 and similar to 820 x 10(-6) counts s(-1) arcmin(-2) (typically brighter at higher Galactic latitudes), with inferred emission measures of similar to 0.0018 to 0.0058 cm(-6) pc (assuming thermal ionization equilibrium). The distribution of the emission temperature of the LHB is peaked at 10(6.07) K with a range of +/-12% at FWHM. While this variation is small and is perhaps due to systematic uncertainties in the analysis, there is a suggestion of a cooler region in the anticenter direction consistent with previous studies. We derive halo plus extragalactic intensities that vary from similar to 400 to greater than or similar to 3000 x 10(-6) counts s(-1) arcmin(-2) outside the absorbing gas of the Galactic disk. As the low end of the range is comparable to what is expected for the extragalactic background, this implies that the halo emission varies considerably over the sky, with inferred emission measures ranging from near zero to >0.02 cm(-6) pc. The distribution of emission temperatures in the halo, again derived from thermal equilibrium emission models, peaks near 10(6.02) K and varies over +/-20% at FWHM. C1 Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Space Res Assoc, Greenbelt, MD USA. RP Snowden, SL (reprint author), Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RI Snowden, Steven/D-5292-2012 NR 89 TC 240 Z9 241 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP 715 EP + DI 10.1086/305135 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW232 UT WOS:000071911700020 ER PT J AU Luhman, KL Briceno, C Rieke, GH Hartmann, L AF Luhman, KL Briceno, C Rieke, GH Hartmann, L TI A young star near the hydrogen-burning limit SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, formation; stars, fundamental parameters; stars, low-mass, brown dwarfs; stars, pre-main-sequence ID BROWN DWARF; CLUSTER; PLEIADES; DISCOVERY; GIANTS; SEARCH AB We show that V410 X-ray 3, toward the L1495E star-forming complex, is an object with a mass of 0.08-0.15 M-. and an age of similar to 1 Myr. Nonetheless, it has emerged from its natal cloud and can be studied in detail throughout the optical and near-infrared, providing new insights into the character of very young and low-mass objects. It has spectral characteristics intermediate between those of late dwarfs and giants (e.g., first-overtone CO typical of an M6 dwarf, but K I, Na I, and TiO/VO typical of an M6 giant and CaH intermediate between the luminosity classes). Its optical and IR photometric colors are consistent with those of an M6 dwarf. If the latest theoretical evolutionary tracks are valid at young ages and low masses, it appears that the hydrogen-burning limit at an age of similar to 1 Myr occurs at a spectral type of M6-M7. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Cent Univ Venezuela, Postgrad Fis, Caracas, Venezuela. CIDA, Ctr Invest Astron, Merida, Venezuela. RP Luhman, KL (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NR 30 TC 52 Z9 52 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP 909 EP 913 DI 10.1086/305171 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW232 UT WOS:000071911700037 ER PT J AU Krishnamurthi, A Terndrup, DM Pinsonneault, MH Sellgren, K Stauffer, JR Schild, R Backman, DE Beisser, KB Dahari, DB Dasgupta, A Hagelgans, JT Seeds, MA Anand, R Laaksonen, BD Marschall, LA Ramseyer, T AF Krishnamurthi, A Terndrup, DM Pinsonneault, MH Sellgren, K Stauffer, JR Schild, R Backman, DE Beisser, KB Dahari, DB Dasgupta, A Hagelgans, JT Seeds, MA Anand, R Laaksonen, BD Marschall, LA Ramseyer, T TI New rotation periods in the Pleiades: Interpreting activity indicators SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, activity; stars, evolution; stars, rotation; X-rays, stars ID MAIN-SEQUENCE STARS; LOW-MASS STARS; SOLAR-TYPE STARS; X-RAY-EMISSION; ANGULAR-MOMENTUM; MICROSCOPIC DIFFUSION; MAGNETIC ACTIVITY; STELLAR MODELS; EVOLUTION; CLUSTER AB We present results of photometric monitoring campaigns of G, K, and M dwarfs in the Pleiades carried out in 1994-1996. We have determined rotation periods for 18 stars in this cluster. In this paper we examine the validity of using observables such as X-ray activity and the amplitude of photometric variations as indicators of angular momentum loss. We report the discovery of cool, slow rotators with high amplitudes of variation. This contradicts previous conclusions about the use of amplitudes as an alternate diagnostic of the saturation of angular momentum loss. We show that the X-ray data can be used as observational indicators of mass-dependent saturation in the angular momentum loss proposed on theoretical grounds. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA. Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA. RP Krishnamurthi, A (reprint author), Univ Colorado, Joint Inst Lab Astrophys, Campus Box 440, Boulder, CO 80303 USA. EM anita@astronomy.ohio-state.edu; terndrup@astronomy.ohio-state.edu; pinsono@astronomy.ohio-state.edu; sellgren@astronomy.ohio-state.edu; stauffer@cfa.harvard.edu; rschild@cfa.harvard.edu; dana@astro.fandm.edu; m_seeds@acad.fandm.edu; marschal@gettysburg.edu; ramseyer@goethe.uca.edu NR 44 TC 81 Z9 81 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP 914 EP 925 DI 10.1086/305173 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW232 UT WOS:000071911700038 ER PT J AU Drake, JJ Fruscione, A Hoare, MG Callanan, P AF Drake, JJ Fruscione, A Hoare, MG Callanan, P TI A deep Extreme Ultraviolet Explorer observation of the extreme ultraviolet transient RE J1255+266 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, close; novae, cataclysmic variables; ultraviolet, stars; X-rays, bursts ID WIDE-FIELD CAMERA; EUV TRANSIENT AB We report on the analysis of a deep Extreme Ultraviolet Explorer (EUVE) observation made with the Deep Survey and Spectrometer telescope, which included in the field the remarkable bright extreme ultraviolet (EUV) transient source RE J1255+266, discovered in 1994 June by the ROSAT Wide Field Camera (WFC). A careful analysis of the resulting Deep Survey (DS) Lexan/B (67-178 Angstrom) image, whose aggregated exposure time is 137 ks, has not revealed any trace of the source but has yielded a quite stringent formal upper limit on the quiescent EUVE DS count rate of 0.003 counts s(-1) (3 sigma) and a "visual" upper limit of 0.002 counts s(-1). An analysis based on blackbody spectra, pure hydrogen DA white dwarf models, and optically thin plasma model spectra has provided constraints on the source counterpart. The observed count rate upper limit is consistent with the optical identification proposed by Watson et al. in which a DA white dwarf is the primary component of a CV-like system involving a very low mass M dwarf secondary star. Our upper limit to the EUVE DS count rate, when compared with the count rate observed with the ROSAT WFC at the peak of the outburst, implies a brightening of the EUV source flux relative to quiescence by a factor of greater than 54,000. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leeds, Dept Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-3, Cambridge, MA 02138 USA. NR 16 TC 4 Z9 4 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP 926 EP 932 DI 10.1086/305153 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW232 UT WOS:000071911700039 ER PT J AU Garnavich, PM Kirshner, RP Challis, P Tonry, J Gilliland, RL Smith, RC Clocchiatti, A Diercks, A Filippenko, AV Hamuy, M Hogan, CJ Leibundgut, B Phillips, MM Reiss, D Riess, AG Schmidt, BP Schommer, RA Spyromilio, J Stubbs, C Suntzeff, NB Wells, L AF Garnavich, PM Kirshner, RP Challis, P Tonry, J Gilliland, RL Smith, RC Clocchiatti, A Diercks, A Filippenko, AV Hamuy, M Hogan, CJ Leibundgut, B Phillips, MM Reiss, D Riess, AG Schmidt, BP Schommer, RA Spyromilio, J Stubbs, C Suntzeff, NB Wells, L TI Constraints on cosmological models from Hubble Space Telescope observations of high-z supernovae SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, observations; galaxies, distances and redshifts; supernovae, general; supernovae, individual (SN 1995K, SN 1997ce, SN 1997cj, SN 1997ck) ID IA SUPERNOVA; LIGHT-CURVE; TESTS AB We have coordinated Hubble Space Telescope (HST) photometry with ground-based discovery for three supernovae: Type Ia supernovae near z approximate to 0.5 (SN 1997ce, SN 1997cj) and a third event at z = 0.97 (SN 1997 ck). The superb spatial resolution of HST separates each supernova from its host galaxy and leads to good precision in the light curves. We use these light curves and relations between luminosity, light-curve shape, and color calibrated from low-z samples to derive relative luminosity distances that are accurate to 10% at z approximate to 0.5 and 20% at z = 1. When the HST sample is combined with the distance to SN 1995K (z = 0.48), analyzed by the same precepts, we find that matter alone is insufficient to produce a flat universe. Specifically, for Omega(m) + Omega(Lambda) = 1, Omega(m) is less than 1 with more than 95% confidence, and our best estimate of Omega(m) is -0.1 +/- 0.5 if Omega(Lambda) = 0. Although this result is based on a very small sample whose systematics remain to be explored, it demonstrates the power of HST measurements for high-redshift supernovae. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Cerro Tololo Interamer Observ, La Serena, Chile. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. European So Observ, D-8046 Garching, Germany. Mt Stromlo & Siding Spring Observ, Weston, Australia. RP Garnavich, PM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Stubbs, Christopher/C-2829-2012; Hamuy, Mario/G-7541-2016; OI Stubbs, Christopher/0000-0003-0347-1724; Schmidt, Brian/0000-0002-8538-9195 NR 26 TC 382 Z9 386 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP L53 EP + DI 10.1086/311140 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW236 UT WOS:000071912100001 ER PT J AU Hunter, TR Neugebauer, G Benford, DJ Matthews, K Lis, DC Serabyn, E Phillips, TG AF Hunter, TR Neugebauer, G Benford, DJ Matthews, K Lis, DC Serabyn, E Phillips, TG TI G34.24+0.13MM: A deeply embedded proto-B star SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, formation; infrared, stars; ISM, individual (G34.24+0.13) ID H-II-REGIONS; ANGULAR-RESOLUTION CAMERA; METHANOL MASERS; EMISSION; W3(OH); GHZ; G34.3+0.2 AB By means of millimeter and submillimeter imaging, we have identified a massive protostellar object that coincides with a methanol maser and is not detectable in the continuum at centimeter wavelengths. Located 84 " (1.5 pc) southeast of the ultracompact H II (UCHII) region G34.26+0.15, the new object G34.24+0.13MM was discovered in a wide-field 350 mu m continuum image obtained with the Submillimeter High Angular Resolution Camera (SHARC) at the Caltech Submillimeter Observatory (CSO). Interferometric imaging at 225.7 and 110.7 GHz continuum has determined more precisely the position and angular diameter (2." 0, or 7600 AU) of the object. No source was detected at that position in 1.2-3.7 mu m imaging or 10 and 20 mu m photometry. Our observations are consistent with a cool dust core with temperature similar to 50 K, total gas mass 100 M-., and total luminosity in the range of 1600-6300 L-.. Considering the high luminosity and lack of compact radio continuum emission, we conclude that this core probably contains a deeply embedded proto-B star. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Hunter, TR (reprint author), Smithsonian Astrophys Observ, MS-78,60 Garden St, Cambridge, MA 02138 USA. RI Benford, Dominic/D-4760-2012; OI Benford, Dominic/0000-0002-9884-4206; Hunter, Todd/0000-0001-6492-0090 NR 28 TC 37 Z9 37 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP L97 EP + DI 10.1086/311142 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW236 UT WOS:000071912100012 ER PT J AU Wijnands, R Homan, J Van der Klis, M Kuulkers, E Van Paradijs, J Lewin, WHG Lamb, FK Psaltis, D Vaughan, B AF Wijnands, R Homan, J Van der Klis, M Kuulkers, E Van Paradijs, J Lewin, WHG Lamb, FK Psaltis, D Vaughan, B TI Discovery of kHz quasi-periodic oscillations in the Z source Cygnus X-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars, individual (Cygnus X-2); stars, neutron; X-rays, stars ID SPECTRA AB During observations with the Rossi X-Ray Timing Explorer from 1997 June 31 to July 3 we discovered two simultaneous kHz quasi-periodic oscillations (QPOs) near 500 and 860 Hz in the low-mass X-ray binary and Z source Cygnus X-2. In the X-ray color-color diagram and hardness intensity diagram (HID), a clear Z track was traced out, which shifted in the HID within 1 day to higher count rates at the end of the observation. Z track shifts are well known to occur in Cyg X-2; our observation for the first time catches the source in the act. A single kHz QPO peak was detected at the left end of the horizontal branch (HB) of the Z track, with a frequency of 731 +/- 20 Hz and an amplitude of 4.7(-0.6)(+0.8)% rms in the energy band 5.0-60 keV. Further to the right on the HB, at somewhat higher count rates, an additional peak at 532 +/- 43 Hz was detected with an rms amplitude of 3.0(-0.7)(+1.0). When the source moved down the HB, thus when the inferred mass accretion rate increased, the frequency of the higher frequency QPO increased to 839 +/- 13 Hz, and its amplitude decreased to 3.5(-0.3)(+0.4)% rms. The higher frequency QPO was also detected on the upper normal branch (NB) with an rms amplitude of 1.8(-0.4)(+0.6)% and a frequency of 1007 +/- 15 Hz; its peak width did not show a clear correlation with inferred mass accretion rate. The lower frequency QPO was most of the time undetectable, with typical upper limits of 2% rms; no conclusion on how this QPO behaved with mass accretion rate can be drawn. If the peak separation between the QPOs is the neutron star spin frequency (as required in some beat-frequency models), then the neutron star spin period is 2.9 +/- 0.2 ms (346 +/- 29 Hz). This discovery makes Cyg X-2 the fourth Z source that displays kHz QPOs. The properties of the kHz QPOs in Cyg X-2 are similar to those of other Z sources. Simultaneous with the kHz QPOs, the well-known horizontal-branch QPOs (HBOs) were visible in the power spectra. At the left end of the HB, the second harmonic of the HBO was also detected. We also detected six small X-ray bursts. No periodic oscillations or QPOs were detected in any of them, with typical upper limits of 6%-8% rms. C1 Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Univ Oxford, Nucl & Astrophys Lab, Oxford OX1 3RH, England. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. RP Wijnands, R (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. NR 22 TC 54 Z9 54 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1998 VL 493 IS 2 BP L87 EP L90 DI 10.1086/311138 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YW236 UT WOS:000071912100009 ER PT J AU Morton, ES AF Morton, ES TI Degradation and signal ranging in birds: memory matters SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article ID PARUS-MAJOR; CONSPECIFIC SONGS; UNDEGRADED SONGS; CAROLINA WREN; DISTANCE; FAMILIARITY; ACOUSTICS; RESPONSES; PLAYBACK C1 Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Morton, ES (reprint author), Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM NZPEM034@SIVM.SI.EDU NR 24 TC 16 Z9 16 U1 1 U2 5 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD FEB PY 1998 VL 42 IS 2 BP 135 EP 137 DI 10.1007/s002650050421 PG 3 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA YY852 UT WOS:000072193300008 ER PT J AU Morton, ES AF Morton, ES TI Ranging reconsidered - Reply to Naguib and Wiley SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Editorial Material C1 Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Morton, ES (reprint author), Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Royal, Front Royal, VA 22630 USA. NR 1 TC 4 Z9 4 U1 0 U2 0 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD FEB PY 1998 VL 42 IS 2 BP 147 EP 148 DI 10.1007/s002650050424 PG 2 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA YY852 UT WOS:000072193300011 ER PT J AU Roth, TL Weiss, RB Buff, JL Bush, LM Wildt, DE Bush, M AF Roth, TL Weiss, RB Buff, JL Bush, LM Wildt, DE Bush, M TI Heterologous in vitro fertilization and sperm capacitation in an endangered African antelope, the scimitar-horned oryx (Oryx dammah) SO BIOLOGY OF REPRODUCTION LA English DT Article ID ZONA-PELLUCIDA PENETRATION; BOVINE SPERM; ACROSOME REACTION; IN-VITRO; INTRACELLULAR PH; OVIDUCT FLUID; SPERMATOZOA; HEPARIN; BINDING; OOCYTES AB Scimitar-horned oryx sperm function was studied using protocols developed for domestic cattle. Objectives were to assess sperm 1) viability and motility in vitro over time, 2) capacitation in heparin-or calcium-supplemented medium, and 3) function in an in vitro fertilization system using heterologous (domestic COW) oocytes. Seminal aliquots were washed, and sperm were resuspended in 1) Talp with 5% fetal calf serum (TALP), 2) TALP + 10 mu M heparin, 3) TALP + 20 mu M heparin, and 4) TALP + 10 mM CaCl. At 0, 3, and 6 h, aliquots were evaluated for sperm motility, viability (using Hoechst 33258), and ability to acrosome-react when exposed to lysophosphatidylcholine (LC). Sperm function was assessed by evaluating fertilization and embryo development after coculture of in vitro-matured domestic cow oocytes with oryx sperm. Overall mean percentages of motile and viable sperm remained high at 6 h (> 60% and > 70%, respectively). Fewer (p < 0.05) sperm incubated in TALP + 10 mu M heparin for 6 h contained intact acrosomes after exposure to LC, but there were no differences between LC and control samples after incubation in TALP without heparin. LC-treated sperm in TALP + 10 mM CaCl contained fewer (p < 0.05) intact acrosomes at 3 and 6 h (52.6% and 31.2%, respectively) than paired controls (83.6% and 70.0%, respectively). Oryx sperm from all males were capable of fertilizing cow oocytes (range 17 of 26 [65.4%] to 25 of 26 [96.2%]). Of the 55 2-cell embryos produced, 34 (61.8%) developed to greater than or equal to 8 cells. Of the 24 uncleaved oocytes, 7 (29.2%) were polyspermic. These data demonstrate that processed sperm from the endangered scimitar-horned oryx remain vigorous in vitro for at least 6 h. Capacitation can be induced using cattle sperm-processing techniques, with sperm appearing most responsive to elevated CaCl concentrations. Most interesting was the successful production and development of hybrid embryos after coincubation of oryx sperm with cow oocytes, suggesting that the two bovid species have similar fertilization mechanisms. C1 Smithsonian Inst, Natl Zool Pk, NOAHS, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Roth, TL (reprint author), Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, 3400 Vine St, Cincinnati, OH 45220 USA. NR 47 TC 66 Z9 71 U1 0 U2 3 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD FEB PY 1998 VL 58 IS 2 BP 475 EP 482 DI 10.1095/biolreprod58.2.475 PG 8 WC Reproductive Biology SC Reproductive Biology GA YU844 UT WOS:000071761700026 PM 9475404 ER PT J AU Fiske, RS Cashman, KV Shibata, A Watanabe, K AF Fiske, RS Cashman, KV Shibata, A Watanabe, K TI Tephra dispersal from Myojinsho, Japan, during its shallow submarine eruption of 1952-1953 SO BULLETIN OF VOLCANOLOGY LA English DT Article DE submarine silicic dome; submarine pyroclastic cone; shallow submarine eruption; Myojinsho; submarine pyroclastic gravity flow ID UNZEN VOLCANO JAPAN; SHIMANE PENINSULA; PYROCLASTIC FLOWS; NEW-ZEALAND; SW JAPAN; ARC; SEDIMENTATION; DEPOSITS; ISLAND; QUEBEC AB A new and derailed bathymetric map of the Myojinsho shallow submarine volcano provides a framework to interpret the physical volcanology of its 1952-1953 eruption, especially how the silicic pyroclasts, both primary and reworked, enlarged the volcano and were dispersed into the surrounding marine environment. Myojinsho, 420 km south of Tokyo along the Izu-Ogasawara are, was the site of approximately 1000 phreatomagmatic explosions during the 12.5-month eruption. These explosions shattered growing dacite domes, producing dense clasts that immediately sank into the sea: minor amounts of pumice floated on the sea surface after some of these events. The Myojinsho cone has slopes of almost precisely 21 degrees in the depth range 300-700 m. We interpret this to be the result of angle-of-repose deposition of submarine pyroclastic gravity flows that traveled downslope in all directions. Many of these gravity flows resulted from explosions and associated dome collapse, but others were likely triggered by the remobilization of debris temporarily deposited on the summit and steep upper slopes of the cone, Tephra was repeatedly carried into air in subaerial eruption columns and fell into the sea within 1-2 km of the volcano's summit, entering water as deep as 400 m. Because the fall velocity of single particles decreased by a factor of similar to 30 in passing from air into the sea, we expect that the upper part of the water column was repeatedly choked with hyperconcentrations of fallout tephra. Gravitational instabilities within these tephra-choked regions could have formed vertical density currents that descended at velocities greater than those of the individual particles they contained. Upon reaching the sea floor. many of these currents probably continued to move downslope along Myojinsho's submarine slopes. Fine tephra was elutriated from the rubbly summit of the volcano by upwelling plumes of heated seawater that persisted for the entire duration of the eruption. Ocean currents carried this tephra to distal areas, where it presumably forms a pyroclastic component of deep-sea sediment. C1 Smithsonian Inst, Washington, DC 20560 USA. Univ Oregon, Dept Geol Sci, Eugene, OR 97403 USA. Japan Maritime Safety Agcy, Hydrog Dept, Chuo Ku, Tokyo 104, Japan. RP Fiske, RS (reprint author), Smithsonian Inst, MRC-119, Washington, DC 20560 USA. EM rfiske@volcano.si.edu NR 53 TC 73 Z9 75 U1 1 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0258-8900 J9 B VOLCANOL JI Bull. Volcanol. PD FEB PY 1998 VL 59 IS 4 BP 262 EP 275 DI 10.1007/s004450050190 PG 14 WC Geosciences, Multidisciplinary SC Geology GA YX647 UT WOS:000072062200003 ER PT J AU Wright, TL Takahashi, TJ AF Wright, TL Takahashi, TJ TI Hawaii bibliographic database SO BULLETIN OF VOLCANOLOGY LA English DT Article DE bibliography; computer; Hawaiian-Emperor chain; volcanology; eruption; earthquake; landslide AB The Hawaii bibliographic database has been created to contain all of the literature, from 1779 to the present, pertinent to the volcanological history of the Hawaiian-Emperor volcanic chain. References are entered in a PC- and Macintosh-compatible EndNote Plus bibliographic database with keywords and abstracts or (if no abstract) with annotations as to content. Keywords emphasize location. discipline, process, identification of new chemical data or age determinations. and type of publication. The database is updated approximately three times a year and is available to upload from an ftp site. The bibliography contained 8460 references at the time this paper was submitted for publication. Use of the database greatly enhances the power and completeness of library searches for anyone interested in Hawaiian volcanism. C1 US Geol Survey, Smithsonian Inst, NMNH, Washington, DC 20560 USA. US Geol Survey, Hawaii Natl Pk, HI 96718 USA. RP Wright, TL (reprint author), US Geol Survey, Smithsonian Inst, NMNH, NHB-119, Washington, DC 20560 USA. NR 1 TC 3 Z9 3 U1 1 U2 3 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0258-8900 J9 B VOLCANOL JI Bull. Volcanol. PD FEB PY 1998 VL 59 IS 4 BP 276 EP 280 DI 10.1007/s004450050191 PG 5 WC Geosciences, Multidisciplinary SC Geology GA YX647 UT WOS:000072062200004 ER PT J AU Fritsch, S Post, JE Suib, SL Navrotsky, A AF Fritsch, S Post, JE Suib, SL Navrotsky, A TI Thermochemistry of framework and layer manganese dioxide related phases SO CHEMISTRY OF MATERIALS LA English DT Article ID OCTAHEDRAL MOLECULAR-SIEVES; CRYSTAL-STRUCTURE DETERMINATIONS; RIETVELD REFINEMENT; OXIDE; CRYPTOMELANE; HOLLANDITE; BIRNESSITE; SODIUM AB The energetics of a set of natural and synthetic manganese dioxides having a framework or a layer structure were determined by high-temperature solution calorimetry using sodium molybdate as a solvent. Enthalpies of formation of the metastable manganese dioxides were calculated from the measured values of the enthalpies of drop solution. The stability of the open structure depends mostly on the nature of and the amount of the tunnel (or interlayer) cation and on the degree of hydration. It depends less strongly on the topology of the structure itself and on the average oxidation state of manganese. The synthesis of these metastable microporous materials is not limited by the energetics of the structure. C1 Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. Princeton Univ, Princeton Mat Inst, Princeton, NJ 08544 USA. Univ Connecticut, Dept Chem, Storrs, CT 06269 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Navrotsky, A (reprint author), Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. NR 35 TC 28 Z9 28 U1 1 U2 14 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0897-4756 J9 CHEM MATER JI Chem. Mat. PD FEB PY 1998 VL 10 IS 2 BP 474 EP 479 DI 10.1021/cm970104h PG 6 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA YY440 UT WOS:000072146800006 ER PT J AU Rivera, JHV Rappole, JH McShea, WJ Haas, CA AF Rivera, JHV Rappole, JH McShea, WJ Haas, CA TI Wood thrush postfledging movements and habitat use in northern Virginia SO CONDOR LA English DT Article DE fledgling dispersal; Wood Thrushes; Hylocichla mustelina; habitat use; juvenile movements; radiotelemetry ID NATAL DISPERSAL; BIRDS; PASSERINES; SELECTION; SPARROW AB We monitored 42 radio-tagged fledgling Wood Thrushes (Hylocichla mustelina) to investigate movement and habitat use during the postfledging period. Fledglings' mean (+/- SE) age at dispersal from the natal sites was 32.5 +/- 0.6 days post hatching. First dispersal sites were located 1.5 +/- 0.3 km from the natal site. All young joined flocks of juveniles, except three birds that remained solitary. Sixteen birds stayed at the first dispersal site until departure on migration, whereas nine visited additional dispersal sites. On 40 occasions, 15 fledglings moved up to 6 km from their dispersal sites. Before late August, 96.7% of fledglings' locations occurred in: (1) second growth scrub/deciduous sapling sites located along forest borders and abandoned farms (59.4%), (2) gypsy moth (Lymantria dispar) damaged deciduous forest (24.4%), and (3) Virginia pine (Pinus virginianus) forest with heavy deciduous understory (12.8%). Fruiting trees and shrubs used as food sources by juveniles fruit earlier in these habitats. After late August, an increased number of fledgling locations (14.1%) occurred in mature deciduous or mixed forest, possibly tracking the later fruiting cycles of understory plants in these habitats. Twenty-four of 33 fledglings left the study area in September. Mean age at departure was 81 +/- 5 days post hatching. We suggest that postfledging movements in Wood Thrushes are keyed by the availability of food resources and the presence of conspecifics, although other factors may play a role. We conclude that successful conservation of migratory species requires protection of habitats used during the postfledging period as well as those used during the nesting portion of the life cycle. C1 Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. Virginia Polytech Inst & State Univ, Dept Fisheries & Wildlife Sci, Blacksburg, VA 24061 USA. RP Rivera, JHV (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, 1500 Remount Rd, Front Royal, VA 22630 USA. RI Haas, Carola/B-5056-2009 OI Haas, Carola/0000-0002-5490-6882 NR 33 TC 122 Z9 122 U1 1 U2 15 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD FEB PY 1998 VL 100 IS 1 BP 69 EP 78 DI 10.2307/1369898 PG 10 WC Ornithology SC Zoology GA YX527 UT WOS:000072049500008 ER PT J AU Kleiman, DG Mallinson, JJC AF Kleiman, DG Mallinson, JJC TI Recovery and management committees for lion tamarins: Partnerships in conservation planning and implementation SO CONSERVATION BIOLOGY LA English DT Article AB Four international recovery and management committees act as official technical advisors to the Brazilian federal environmental agency-the Instituto Brasileiro do Meio Ambiente e dos Recursos Naturais Renovaveis-with respect to the conservation and management of both the in situ and ex situ populations of the endangered lion tamarins (Leontopithecus). The committees promote lion tamarins as "flagship" species, the ultimate intent being the preservation of the unique Atlantic rain forest (Mata Atlantica) ecosystem and its many, endemic plants and animals. We summarize the history, organization, structure, and functioning of these oversight management committees and their current role in guiding, motivating, and focusing conservation efforts for the Mata Atlantica of Brazil and the four endangered Leontopithecus species therein. We discuss the role of science in conservation planning for the species, funding mechanisms, the decision-making process, conflicts and their resolution, and criteria used for evaluating success. The benefits of this particular species recovery process include the establishment of collaborative partnerships between the Brazilian government and a multitude of individuals and organisations and the use of multidisciplinary, semi-autonomous teams to implement conservation activities. The major limitation of the management committees is their lack of a formal budget permanent staff. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Jersey Wildlife Preservat Trust, Trinity JE3 5BP, Jersey, England. RP Kleiman, DG (reprint author), Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. NR 56 TC 22 Z9 25 U1 1 U2 20 PU BLACKWELL SCIENCE INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 1998 VL 12 IS 1 BP 27 EP 38 DI 10.1046/j.1523-1739.1998.96287.x PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA YX924 UT WOS:000072094300005 ER PT J AU Ferry, JM Sorensen, SS Rumble, D AF Ferry, JM Sorensen, SS Rumble, D TI Structurally controlled fluid flow during contact metamorphism in the Ritter Range pendant, California, USA SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY LA English DT Article ID SILICEOUS DOLOMITIC LIMESTONES; REGIONAL METAMORPHISM; BALLACHULISH AUREOLE; HYDROTHERMAL SYSTEMS; ISOTOPE GEOCHEMISTRY; MINERAL REACTIONS; COOLING PLUTONS; STABLE ISOTOPES; SIERRA-NEVADA; OXYGEN AB The mineralogy and O-isotope geochemistry of siliceous limestones from the Ritter Range pendant constrain the geometry and amount of fluid flow during contact metamorphism associated with emplacement of a pluton of the Sierra Nevada Batholith. Wollastonite (Wo) replaces calcite (Cal) + quartz (Qtz) on a layer-by-layer basis in homoclinal beds that strike NW and dip almost vertically. At the peak of metamorphism (P approximate to 1500 bars, T approximate to 600 degrees C) fluid in equilibrium with Cal, Qtz, and Wo has composition X-CO2 = 0.28, requiring that the Wo-forming reaction was driven by infiltration of reactive H2O-rich fluid. The spatial distribution of Wo and Cal + Qtz records that peak metamorphic fluid flow was layer-parallel, upward. Bounds on the prograde time-integrated fluid flux associated with formation of Wo are set by: (1) the overlap in O-isotope composition between Wo-bearing and Wo-free rocks (>245 mol fluid/cm(2) rock); (2) the amount of fluid that would drive the Wo-reaction front upward to the present level of exposure from a point at depth where Cal, Qtz, and Wo would be in equilibrium with pure CO2 (<1615 mol/cm(2)). Back-reaction of Wo to Cal + Qtz records an additional time-integrated retrograde fluid flux of approximate to 200-1000 mol/cm(2). The direction and amount of flow inferred from mineralogical and isotopic data agree with the results of the hydrologic model for metamorphic fluid flow in the area of Hanson et al. (1993). Fingers of Wo-bearing rock that extend farthest from the fluid source along contacts between limestone and more siliceous rocks point to strong control of flow geometry at the 0.1-100 m scale exerted by premetamorphic structures. Studies that neglect structural control at this scale may fail to predict correctly fundamental aspects of contact metamorphic fluid flow. C1 Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Mineral Sci, Washington, DC 20560 USA. Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. RP Ferry, JM (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. EM jferry@jhu.edu NR 55 TC 37 Z9 39 U1 0 U2 4 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0010-7999 J9 CONTRIB MINERAL PETR JI Contrib. Mineral. Petrol. PD FEB PY 1998 VL 130 IS 3-4 BP 358 EP 378 DI 10.1007/s004100050371 PG 21 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA ZC630 UT WOS:000072600800012 ER PT J AU Stenroos, S DePriest, PT AF Stenroos, S DePriest, PT TI Small insertions at a shared position in the SSU rDNA of Lecanorales (lichen-forming Ascomycetes) SO CURRENT GENETICS LA English DT Article DE lecanorales; lichen-forming fungi; phylogeny; SSU rDNA ID RIBOSOMAL-RNA GENE; GROUP-I INTRONS; PCR PRIMERS; FUNGI; SECONDARY; DNA AB Small insertions are reported from the SSU rDNA of the genera Cladonia, Cladina, Stereocaulon, Pertusaria and Physcia (lichen-forming Lecanorales, Ascomycetes). The insertions range in length from 56 to 81 nucleotides, and occur at a shared position, 330 (relative to Escherichia coli), in a semi-conserved region of the SSU rDNA. These small insertions have a simple secondary structure with two stem-loops, and may represent degenerate group-I introns. Species of the same genus often have small insertions of similar lengths, secondary structures and sequences. These similarities suggest that the insertions are homologous and can provide phylogenetic information to support current classifications. Variable sequences of rDNA, such as the small insertions and group-I introns, may be powerful tools for resolving evolutionary relationships among genera and species. C1 Univ Turku, Dept Biol, Herbarium, FIN-20014 Turku, Finland. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Stenroos, S (reprint author), Univ Turku, Dept Biol, Herbarium, FIN-20014 Turku, Finland. RI DePriest, Paula/K-6633-2015 NR 23 TC 18 Z9 19 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0172-8083 J9 CURR GENET JI Curr. Genet. PD FEB PY 1998 VL 33 IS 2 BP 124 EP 130 DI 10.1007/s002940050317 PG 7 WC Genetics & Heredity SC Genetics & Heredity GA ZD385 UT WOS:000072679900006 PM 9506900 ER PT J AU Williams, ST Benzie, JAH AF Williams, ST Benzie, JAH TI Evidence of a biogeographic break between populations of a high dispersal starfish: Congruent regions within the Indo-West Pacific defined by color morphs, mtDNA, and allozyme data SO EVOLUTION LA English DT Article DE Allozymes; asteroidea; Indo-West Pacific biogeography; larval dispersal; Linckia laevigata; PCR-RFLP; population genetics ID LINCKIA-LAEVIGATA ECHINODERMATA; MITOCHONDRIAL-DNA VARIATION; LATE QUATERNARY; GENE FLOW; RESTRICTION DATA; BIRGUS-LATRO; COCONUT CRAB; PATTERNS; ZOOGEOGRAPHY; OCEAN AB Both mtDNA variation and allozyme data demonstrate that geographic groupings of different color morphs of the starfish Linckia laevigata are congruent with a genetic discontinuity between the Indian and Pacific Oceans. Populations of L. laevigata sampled from Thailand and South Africa, where an orange color morph predominates, were surveyed using seven polymorphic enzyme loci and restriction fragment analysis of a portion of the mtDNA including the control region. Both allozyme and DNA data demonstrated that these populations were significantly genetically differentiated from each other and to a greater degree from 23 populations throughout the West Pacific Ocean, where a blue color morph is predominant. The genetic structure observed in L. laevigata is consistent with traditional ideas of a biogeographic boundary between the Indian and Pacific Oceans except that populations several hundreds kilometers off the coast of north Western Australia (Indian Ocean) were genetically similar to and had the same color morphs as Pacific populations. It is suggested that gene flow may have continued (possibly at a reduced rate) between these offshore reefs in Western Australia and the West Pacific during Pleistocene falls in sea level, but at the same time gene flow was restricted between these Western Australian populations and those in both Thailand and South Africa, possibly by upwellings. The molecular data in this study suggest that vicariant events have played an important role in shaping the broadscale genetic structure of L. laevigata. Additionally, greater genetic structure was observed among Indian Ocean populations than among Pacific Ocean populations, probably because there are fewer reefs and island archipelagos in the Indian Ocean than in the Pacific, and because present-day surface ocean currents do not facilitate long-distance dispersal. C1 Australian Inst Marine Sci, Townsville MC, Qld 4810, Australia. James Cook Univ N Queensland, Dept Zool & Trop Ecol, Townsville, Qld 4811, Australia. RP Williams, ST (reprint author), NAOS, Marine Lab, Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Williams, Suzanne/A-9604-2008 OI Williams, Suzanne/0000-0003-2995-5823 NR 53 TC 146 Z9 148 U1 0 U2 17 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD FEB PY 1998 VL 52 IS 1 BP 87 EP 99 DI 10.2307/2410923 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA ZB079 UT WOS:000072433200010 ER PT J AU Seideman, T AF Seideman, T TI The role of a molecular phase in two-pathway excitation schemes SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SIMULTANEOUS OMEGA-1,OMEGA-3 EXCITATION; LASER CONTROL; UNIMOLECULAR REACTIONS; COHERENT; PHOTODISSOCIATION; DISTRIBUTIONS; INTERFERENCE AB The origin and potential implications of a molecular phase in coherent two-pathway excitation are analyzed by means of a time-independent, quantum mechanical theory. A unified model is developed describing unimolecular decay into several continua of general nature, where each breakup reaction takes place both directly and via a manifold of resonances. It is found that the molecular phase, observable in two pathway excitation experiments, correlates with the single-pathway fragmentation line shape, in agreement with recent measurements. We propose the measurement of molecular phases as a route to molecular properties which are silent in conventional observables. (C) 1998 American Institute of Physics. C1 Harvard Univ, Harvard Smithsonian Ctr, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Natl Res Council Canada, Steacie Inst Mol Sci, Ottawa, ON K1A 0R6, Canada. RP Seideman, T (reprint author), Harvard Univ, Harvard Smithsonian Ctr, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 26 TC 36 Z9 36 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD FEB 1 PY 1998 VL 108 IS 5 BP 1915 EP 1923 DI 10.1063/1.475571 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA YU725 UT WOS:000071748000021 ER PT J AU Stafford, BJ Thorington, RW AF Stafford, BJ Thorington, RW TI Carpal development and morphology in archontan mammals SO JOURNAL OF MORPHOLOGY LA English DT Article DE carpal reduction; scapholunate; hands; dermoptera; chiroptera; scandentia; ptilocercus; peromyscus; sciuridae AB Carpal morphology and development in bats, colugos, tree shrews, murids, and sciurids were studied in order to homologize carpal elements. Prenatal coalescence of discrete cartilaginous templates with a loss of a center of ossification appears to be the most common method of reducing carpal elements in these mammals. Only bats and colugos showed postnatal ossification between discrete elements as a method of reducing carpal elements. Carpal morphology of tree shrews is more diverse than previously reported. Ptilocercus shows a highly derived carpal morphology that may be related to its relatively greater arboreality. Dendrogale exhibits what is most likely the ancestral tupaiid carpal morphology. Carpal morphologies of Tupaia, Urogale, and Anathana are identical to each other. Carpal morphology differs between megachiropterans and microchiropterans. These differences may be related to different aerodynamic constraints between the suborders. The carpal morphology of microchiropterans is diverse and may reflect different adaptive regimes between microchiropteran families. Carpal morphology of the colugos shows both megachiropteran and microchiropteran characters. The function of these characters in colugos and bats (stabilization of the carpus in dorsiflexion) is proposed to be similar, although the locomotor roles may be quite different between these taxa. (C) 1998 Wiley-Liss, Inc. C1 Smithsonian Inst, Dept Vertebrate Zool, Div Mammals, Natl Museum Nat Hist, Washington, DC 20560 USA. CUNY, PHD Program Anthropol, New York, NY 10021 USA. CUNY, New York Consortium Evolutionary Primatol, New York, NY 10021 USA. RP Stafford, BJ (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Div Mammals, Natl Museum Nat Hist, NHB 390 MRC 108, Washington, DC 20560 USA. NR 67 TC 30 Z9 36 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD FEB PY 1998 VL 235 IS 2 BP 135 EP 155 DI 10.1002/(SICI)1097-4687(199802)235:2<135::AID-JMOR4>3.0.CO;2-8 PG 21 WC Anatomy & Morphology SC Anatomy & Morphology GA YQ077 UT WOS:000071345600004 PM 9438973 ER PT J AU Faust, MA AF Faust, MA TI Morphology and life cycle events Pyrophacus steinii (Schiller) Wall et Dale (dinophyceae) SO JOURNAL OF PHYCOLOGY LA English DT Article DE Belize, Central America; benthic; dinoflagellates; Dinophyceae; life cycle light microscopy; morphology; Pyrophacaceae; Pyrophacus steinii; scanning electron microscopy; taxonomy AB Cells of Pyrophacus steinii (Schiller) Wall et Dale are round and lens shaped and have and anteroposteriorly compressed theca. The epitheca has a truncated, conical horn and a hexagonally shaped apical pore plate with two arched slits positioned off center. The cingulum is equatorial, narrow, and deep. The hypotheca is flat. The sulcus is narrow, slightly curved, and recessed and does not reach the cell's antapex. The plate formula in these specimens of P. steinii is Po, 8', Oa, 13 ", 13C, 12''', 3p, 3'''' and 8S with a difference in the number of precingular (13 ") and postcingular (12''') plates. No additional posterior intercalary plates were present (Oap). Pregametic stages of P. steinii were observed during cell division via binary fission, with formation of two cells and multiple division with formation of four and eight cells. These newly formed cells were pale in color and were enclosed in double-layered hyaline membrane. Gametes with gymnodinoid morphology were observed within the parental cells. Planozygotes are large and round and enclosed in double-layered hyaline membrane. Mature cell forms are brown with a microgranular cytoplasm, storage bodies, and a red accumulation body. The hypnozygote exhibits triple-layered hyaline membrane, irregularly shaped and comparable with bulbous processes of Tuberculodinium vancampoae Rossigol resting cysts. Division within a hypnocyst of P. steinii involves shedding the parental theca and the development and emergence of two daughter cells with the size and morphology of pregametic cells. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Suitland, MD 20746 USA. RP Faust, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, 4201 Silver Hill Rd, Suitland, MD 20746 USA. EM faust.maria@nmnh.si.edu NR 31 TC 11 Z9 11 U1 0 U2 2 PU PHYCOLOGICAL SOC AMER INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 1998 VL 34 IS 1 BP 173 EP 179 DI 10.1046/j.1529-8817.1998.340173.x PG 7 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA ZB981 UT WOS:000072527700021 ER PT J AU Tarr, CL Fleischer, RC AF Tarr, CL Fleischer, RC TI Primers for polymorphic GT microsatellites isolated from the Mariana crow, Corvus kubaryi SO MOLECULAR ECOLOGY LA English DT Article DE Corvidae; Corvus; microsatellite; primers C1 Penn State Univ, Dept Biol, University Pk, PA 16802 USA. Penn State Univ, Inst Mol Evolutionary Genet, University Pk, PA 16802 USA. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Mol Genet Lab, Washington, DC 20008 USA. RP Tarr, CL (reprint author), Penn State Univ, Dept Biol, 208 Mueller Lab, University Pk, PA 16802 USA. NR 8 TC 16 Z9 16 U1 1 U2 9 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD FEB PY 1998 VL 7 IS 2 BP 253 EP 255 PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA ZB396 UT WOS:000072468300013 PM 9532766 ER PT J AU Wetterer, JK Schultz, TR Meier, R AF Wetterer, JK Schultz, TR Meier, R TI Phylogeny of fungus-growing ants (Tribe Attini) based on mtDNA sequence and morphology SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID CYTOCHROME-OXIDASE; MOLECULAR PHYLOGENY; GENE; HYMENOPTERA; FORMICIDAE AB We examined the phylogenetic relationships among taxa of attine or "fungus-growing" ants (Tribe Attini) using parsimony analyses of molecular and morphological data. We sequenced a region of mitochondrial DNA from 13 taxa of attines and from one closely related outgroup species, Wasmannia auropunctata. Our study sequence included the 3' end of the cytochrome c oxidase subunit I (CO I) locus (183 to 198 total sites; 91 informative sites), an intergenic spacer region of variable size (0 to 152 sites), the tRNA leucine locus (65 to 74 sites), and the 5' end of the cytochrome c oxidase subunit II (co II) locus (292 total sites; 140 informative sites). The inferred relationships among the attine taxa based on an unweighted analysis of the nucleotide sequence data closely matched the relationships inferred from an analysis of larval morphological characters from 11 of the taxa. In fact, the inferred relationships were completely congruent among the protein parsimony analysis of amino acid data, the morphology analysis, and "total evidence" analysis combining the amino acid and morphology data. The congruent conclusions we obtained from two independent data sets increases our confidence in the reliability of our analyses. (C) 1998 Academic Press. C1 Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. Smithsonian Inst, Dept Entomol, NMNH MRC 165, Washington, DC 20560 USA. Amer Museum Nat Hist, New York, NY 10024 USA. RP Wetterer, JK (reprint author), Columbia Univ, Ctr Environm Res & Conservat, 1200 Amsterdam Ave, New York, NY 10027 USA. EM jw272@columbia.edu RI Meier, Rudolf/A-7099-2011 OI Meier, Rudolf/0000-0002-4452-2885 NR 31 TC 88 Z9 95 U1 2 U2 17 PU ACADEMIC PRESS INC PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD FEB PY 1998 VL 9 IS 1 BP 42 EP 47 DI 10.1006/mpev.1997.0466 PG 6 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA ZH433 UT WOS:000073108500005 PM 9479692 ER PT J AU Davies-Vollum, KS Wing, SL AF Davies-Vollum, KS Wing, SL TI Sedimentological, taphonomic, and climatic aspects of Eocene swamp deposits (Willwood Formation, Bighorn Basin, Wyoming) SO PALAIOS LA English DT Article ID ALLUVIAL PALEOSOLS; USA; RIVER; PALEOCLIMATOLOGY; SEDIMENTATION; ACCUMULATION; PALEOCENE; DIVERSITY; AMERICA; SOILS AB Alluvially deposited carbonaceous beds are a major source of leaf compression fossils, but the accumulation of both the sediments and the fossils is poorly understood. We have studied the sediments and fossil plant assemblages of three laterally extensive carbonaceous beds from the Eocene of the Bighorn. Basin, Wyoming. Field, laboratory, and microscopic observations show that carbonaceous beds are highly heterogeneous, varying in the amount and type of organic matter, preservation of primary sedimentary structures, and the prevalence of paleosol features. Small-scale lateral and vertical variations indicate a mosaic of conditions in, the wet floodplain backswamp. The variables controlling this mosaic were primarily rate of clastic input and degree of substrate flooding which, in turn, influenced the amount of pedogenesis. Fossil plant assemblages occur in sediments least modified by pedogenesis, and the best preservation is in the distal, fine-grained portions of overbank flood deposits. There is no evidence for transport of plant material from channel to backswamp. Fossil leaves in a single quarry sample (i.e., those collected from within 10-20 cm stratigraphically and from an area of 4-10 m(2)) probably accumulated during one or several closely-spaced flood events. Quarry samples are thus spatially and temporally constrained "snapshots" of the vegetation that grew on the alluvial floodplain. Each carbonaceous bed is estimated to represent roughly 2,000 years, based on the length of fluvial avulsion cycles. Multiple quarry samples from the same carbonaceous bed can thus be considered coeval for most evolutionary or paleoclimatic analyses. In the central Bighorn Basin, laterally extensive carbonaceous beds are abundant in the lower and upper Willwood Formation, but essentially absent in the middle. We attribute this to tectonic and climatic change, especially to higher rates of sediment accumulation that caused greater dispersal of organic material within sediments and climatic drying that allowed degradation of organic material before it could be preserved. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. RP Davies-Vollum, KS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. OI Wing, Scott/0000-0002-2954-8905 NR 46 TC 39 Z9 40 U1 0 U2 1 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 1731 E 71ST STREET, TULSA, OK 74136-5108 USA SN 0883-1351 J9 PALAIOS JI Palaios PD FEB PY 1998 VL 13 IS 1 BP 28 EP 40 DI 10.2307/3515279 PG 13 WC Geology; Paleontology SC Geology; Paleontology GA YZ368 UT WOS:000072247400004 ER PT J AU Stanley, DJ Bernasconi, MP AF Stanley, DJ Bernasconi, MP TI Relict and palimpsest depositional patterns on the Nile shelf recorded by molluscan faunas SO PALAIOS LA English DT Article ID CONTINENTAL-SHELF; DELTA SHELF; EVOLUTION; EGYPT; SEDIMENTS; EROSION; RATES; CONE AB Infralittoral molluscs, whose normal living depths are less than 25 m, were recovered off the Nile delta between the coast and outer continental shelf and on the uppermost slope. At depths exceeding 25 m, these 13 species are interpreted as relict markers of former low sea-level stands of latest Pleistocene-to-Holocene age. Their concentration in coast-parallel belts also records the role of seafloor erosion by Holocene to modern bottom-current activity, and also displacement by bioturbation. Widespread distribution of reworked molluscan faunas and low rates (to <3 cm/1000 years) of sediment accumulation mapped on many parts of the shelf and upper slope record the overall sediment-starved nature of the Nile shelf: Where now concentrated in deep-water environments, infralittoral molluscs serve as markers to help define effects of the Holocene transgression, denote zones of intense erosion and biogenic reworking, and interpret both relict and reworked relict (palimpsest) patterns on. the modern Nile shelf. C1 Smithsonian Inst, Deltas Global Change Program, Washington, DC 20560 USA. Univ Calabria, Dipartimento Sci Terra, I-87036 Arcavacata, CS, Italy. RP Stanley, DJ (reprint author), Smithsonian Inst, Deltas Global Change Program, Paleobiol E-206 NMNH, Washington, DC 20560 USA. NR 33 TC 8 Z9 8 U1 1 U2 2 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 1731 E 71ST STREET, TULSA, OK 74136-5108 USA SN 0883-1351 J9 PALAIOS JI Palaios PD FEB PY 1998 VL 13 IS 1 BP 79 EP 86 DI 10.2307/3515283 PG 8 WC Geology; Paleontology SC Geology; Paleontology GA YZ368 UT WOS:000072247400008 ER PT J AU Hussein, MS Pato, MP AF Hussein, MS Pato, MP TI Semiclassical treatment of electron-molecule scattering within the vibron model SO PHYSICAL REVIEW A LA English DT Article ID ALGEBRAIC-EIKONAL APPROACH; ROTATION-VIBRATION SPECTRA; DIATOMIC-MOLECULES AB A semiclassical coupled-channels description of electron-molecule scattering is developed within the vibron model of diatomic molecules. The inclusive quasielastic scattering cross section is calculated for a typical system, The effect of the rotational coupling is taken into account by evaluating a rotationally inclusive cross section. [S1050-2947(98)04001-3]. C1 MIT, Ctr Theoret Phys, Nucl Sci Lab, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Paris 11, Inst Phys Nucl, Div Phys Theor, F-91496 Orsay, France. RP Hussein, MS (reprint author), Univ Sao Paulo, Inst Fis, Caixa Postal 66318, BR-05389970 Sao Paulo, Brazil. NR 14 TC 0 Z9 0 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 1998 VL 57 IS 2 BP 976 EP 983 DI 10.1103/PhysRevA.57.976 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA YW253 UT WOS:000071913800041 ER PT J AU Marsden, BG Williams, GV AF Marsden, BG Williams, GV TI The NEO confirmation page SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Workshop Tunguska 96 CY JUL 15-17, 1996 CL BOLOGNA, ITALY SP Univ Bologna, Dept Phys, Univ Bologna, Commiss Int Relat, Alessandro Volta Ctr Sci Culture, Emilia Romagna Reg Govt, Giorgio Abetti Astron Observ, Int Sci Fdn, Landau Network Coordinat Ctr, Luigi Negro Fdn, Russian Fdn Basic Res AB The use of a facility in the World Wide Web for the confirmation of candidate near-earth objects (NEOs) is described. This facility allows users to derive topocentric ephemerides of objects recorded on only a single night. The facility is operated by the Minor Planet Center, which subsequently distributes more detailed information by e-mail to its subscribers if and when an object is confirmed as an NEO. (C) 1998 Published by Elsevier Science Ltd. All rights reserved. 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 3 TC 7 Z9 7 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB-MAR PY 1998 VL 46 IS 2-3 BP 299 EP 302 DI 10.1016/S0032-0633(96)00153-5 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZN567 UT WOS:000073658800019 ER PT J AU Leigh, EG AF Leigh, EG TI Forest fragmentation: another perspective - Reply from E.G. Leigh SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Leigh, EG (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. NR 8 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD FEB PY 1998 VL 13 IS 2 BP 75 EP 75 DI 10.1016/S0169-5347(97)01312-8 PG 1 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA YV381 UT WOS:000071817100011 PM 21238204 ER PT J AU Reid, JW AF Reid, JW TI How "cosmopolitan" are the continental cyclopoid copepods? Comparison of the North American and Eurasian faunas, with description of Acanthocyclops parasensitivus sp.n. (Copepoda : Cyclopoida) from the USA SO ZOOLOGISCHER ANZEIGER LA English DT Article DE Acanthocyclops; Crustacea; Cyclopidae; new species; biogeography ID CRUSTACEA; CLADOCERA; GENUS; REDESCRIPTION; CYCLOPIDAE; TAXONOMY; RECORD; ALASKA; KIEFER; SARS AB Refinements of alpha-taxonomic methods have resulted in reconsideration and splitting of several "species" of continental (inland-water) cyclopid copepods (Crustacea). This process should continue as more careful morphological scrutiny, genetic comparisons, and cross-breeding tests are applied to additional taxa. The relative number of taxa supposedly shared between continents, or "cosmopolitan", has been declining upon re-examination; the world cyclopid fauna is no longer thought to be composed of a significant proportion of relatively few, widespread species. This process is illustrated through inspection of the faunas of North America and Eurasia. Presently a maximum of 32 (28%) of 114 North American cyclopid species and subspecies is considered to be holarctic, compared to 13 (68%) of the 19 North American species known at the beginning of this century. The species that are presently thought to be holarctic and an additional few morphologically similar, possibly sibling species are listed, and the taxonomic status of some is discussed. Acanthocyclops parasensitivus sp.n. from the eastern U.S.A. is described and compared with its European sibling species, A. sensitivus. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Reid, JW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20560 USA. EM Reid.Janet@nmnh.si.edu NR 47 TC 39 Z9 39 U1 3 U2 3 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0044-5231 J9 ZOOL ANZ JI Zool. Anz. PD FEB PY 1998 VL 236 IS 2-3 BP 109 EP 118 PG 10 WC Zoology SC Zoology GA ZB861 UT WOS:000072515400003 ER PT J AU Schlegel, EM Kirshner, RP AF Schlegel, EM Kirshner, RP TI SN1987C in Mrk 90=UGC 4438: Evolution of a type "IIn" to a type IIP? SO NEW ASTRONOMY LA English DT Article DE supernovae, individual, SN1987C ID X-RAY-EMISSION; LIGHT CURVES; SUPERNOVA 1987A; RADIO-EMISSION; MASS; SN-1990E; GALAXIES; SPECTRA; EJECTA; CLOUDS AB We describe three optical spectra and four photometric observations of SN1987C. The light curve is best described by a Type II-P template. The first spectrum of SN1987C, at day 53, is similar to spectra of other members of the "Type IIn'' subclass. Spectra at 80 and 231 days appear essentially identical to late-time spectra of normal Type II-P supernovae. The data provide clues to suggest that at least this example of a "IIn" object was a hidden Type II-P supernova during its early evolution. We believe that we have observed the effects of a transition from emission dominated by the kinetic energy of an expanding shell to emission dominated by the radioactive decay of synthesized isotopes. As far as we know, this is the first time such a transition has been observed. (C) 1998 Elsevier Science B.V. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schlegel, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ems@seska.harvard.edu; kirshner@itp.ucsb.edu NR 48 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1076 J9 NEW ASTRON JI New Astron. PD JAN 29 PY 1998 VL 3 IS 2 BP 125 EP 136 DI 10.1016/S1384-1076(98)00002-5 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY988 UT WOS:000072208700001 ER PT J AU Hau, M Wikelski, M Wingfield, JC AF Hau, M Wikelski, M Wingfield, JC TI A neotropical forest bird can measure the slight changes in tropical photoperiod SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE neotropical bird; seasonal breeding; tropical photoperiod; avian reproduction; Hyloph naevioides ID NEST PREDATION; ANNUAL CYCLE; PROTEIN; FOOD; RADIOIMMUNOASSAY; REPRODUCTION; SEASONALITY; COMMUNITY; PROXIMATE AB Many tropical birds breed seasonally, but it is largely unknown which environmental cues they use to time reproduction. Changes in tropical photoperiod have been regarded as too small to be used as a proximate environmental cue. This hypothesis, however, has never been rigorously tested. Here, we report on experimental evidence that photoperiodic changes characteristic of tropical latitudes stimulate reproductive activity in a neotropical bird from the forest understory. In the central Republic of Panama (9 degrees N), photoperiod varies annually between 12 hours (December) and 13 hours (June). Free-living spotted antbirds (Hylophylax n. naevioides) had regressed gonads in December, but increased gonads ahead of the rainy (the breeding) season in May Captive spotted antbirds exposed to a 'long' photoperiod of 13 hours increased gonadal size eight-fold and song activity six-fold over that of control birds remaining on a simulated 'short' photoperiod of 12 hours of daylight. Moreover, even a photoperiod of 12 hours 17 minutes was sufficient to stimulate gonadal growth in photostimulated birds over that of controls. The dramatic changes in gonadal development were not accompanied by similar changes in hormone titres such as luteinizing hormone and testosterone as expected from temperate zone birds. We propose a more general role of the tropical photoperiod in the regulation of seasonal events in tropical organisms, or in temperate zone species migrating to the tropics. C1 Univ Washington, Dept Zool, Seattle, WA 98195 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Hau, M (reprint author), Univ Washington, Dept Zool, Seattle, WA 98195 USA. EM hau@zoology.washington.edu NR 61 TC 120 Z9 120 U1 3 U2 24 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 1998 VL 265 IS 1391 BP 89 EP 95 DI 10.1098/rspb.1998.0268 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA YV412 UT WOS:000071820400002 ER PT J AU Barret, D Motch, C Predehl, P AF Barret, D Motch, C Predehl, P TI ROSAT and follow-up infrared observations of the X-ray burster KS 1731-260 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy : center; X-rays : stars; stars : individual : KS 1731-260; star : neutron; infrared : stars ID GALACTIC-CENTER; REGION AB We report on the ROSAT HRI (High Resolution Imager) observation of the X-ray burster KS 1731-260. The observation was split in two parts; the first took place in 1995, March 16 lasting for similar to 1 kilosecond and the second one between September 3rd and 14th, 1996 for about 5 kiloseconds. In both observations, KS 1731-260 was clearly detected with a count rate of 0.82 and 7.9 ctss respectively. From the first observation we found that the X-ray source is located at a position alpha = 17(h) 34(mm) 13.5(s) and delta = -26 degrees 05' 16.8" (equinox 2000) with an associated error radius of 10.1 arcsec (90% confidence level combining the attitude and centroid uncertainties). The position derived from the second part of the observation is consistent with the previous one. The ROSAT HRI position rules out the two counterparts that have been proposed so far. Our CFHT J and H infrared imaging of the HRI error box reveals at least 13 possible candidates. As expected from a comparison with other X-ray bursters, the upper limits derived for the infrared brightness of KS 1731-260 imply the presence of a low mass companion for the neutron star. We also report on a refined spectral analysis of the PSPC data taken during the all sky survey in September 1990. These data, together with data recorded by TTM and PCA/RXTE indicate that the column density towards KS 1731-260 varies between similar to 1 to 6 x 10(22) H atoms cm(-2); thus suggesting that the source is characterized by variable intrinsic absorption. The change in the HRI count rate could be better explained by a change in the column density between the two observations rather than by a true source intensity variation. The numerous detections of the source since its discovery in 1988 together with its recent monitoring by the RXTE/ASM show that KS 173 1-260 is a persistent source rather than a soft X-ray transient, as originally thought. C1 Ctr Etud Spatiale Rayonnements, CNRS, UPS, F-31028 Toulouse, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNRS, UA 1280, Observ Astron Strasbourg, F-67000 Strasbourg, France. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Barret, D (reprint author), Ctr Etud Spatiale Rayonnements, CNRS, UPS, 9 Av Colonel Roche,BP 4346, F-31028 Toulouse, France. NR 22 TC 20 Z9 21 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 JAN 20 PY 1998 VL 329 IS 3 BP 965 EP 970 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YT767 UT WOS:000071643000024 ER PT J AU Cagnoni, I Della Ceca, R Maccacaro, T AF Cagnoni, I Della Ceca, R Maccacaro, T TI A medium survey of the hard X-ray sky with the ASCA gas imaging spectrometer: The (2-10 keV) number counts relationship SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; surveys; X-rays, galaxies; X-rays, general ID DEEP ROSAT SURVEY; N-LOG-S; MEDIUM-SENSITIVITY SURVEY; BACKGROUND SPECTRUM; ORIGIN; GALAXIES AB In this paper, we report the first results of a medium survey program conducted in the 2-10 keV energy band using data from the GIS2 instrument onboard the ASCA satellite. We have selected from the ASCA public archive (as of 1996 February 14) 87 images suitable for this project. Sixty serendipitous X-ray sources with a signal-to-noise ratio greater than 3.5 were found. The 2-10 keV flux of the detected sources ranges from similar to 1.1 x 10(-13) ergs cm(-2) s(-1) to similar to 4.1 x 10(-12) ergs cm(-2) s(-1). Using this sample, we have extended thr description of the 2-10 keV log N(>S)-log S to a flux limit of similar to 6.3 x 10(-14) ergs cm(-2) s(-1) (the faintest detectable flux), i.e., about 2.7 orders of magnitude fainter than the Piccinotti et al. determination. The derived number-flux relationship is well described by a power-law model, N(>S) = K x S-alpha, with best-ft values alpha = 1.67 +/- 0.18 and K = 2.85 x 10(-21) deg(-2). At the flux limit of the survey, about 27% of the cosmic X-ray background in the 2-10 keV energy band is resolved in discrete sources. A flattening of the number-flux relationship, within a factor of 10 from the flux limit of the present survey, is expected in order to avoid saturation. The implications of these results for models of the origin of the hard X-ray background are briefly discussed. C1 Univ Milan, I-20133 Milan, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Brera, I-20121 Milan, Italy. RP Cagnoni, I (reprint author), Univ Milan, Via Celoria 16, I-20133 Milan, Italy. NR 44 TC 74 Z9 74 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1998 VL 493 IS 1 BP 54 EP 61 DI 10.1086/305097 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YV314 UT WOS:000071810800006 ER PT J AU Kalogera, V Webbink, RF AF Kalogera, V Webbink, RF TI Formation of low-mass X-ray binaries. II. Common envelope evolution of primordial binaries with extreme mass ratios SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, close; stars, evolution; stars, interiors; stars, neutron; X-rays, stars ID RADIO PULSARS; SUPERNOVA EXPLOSIONS; SOLAR NEIGHBORHOOD; ANGULAR-MOMENTUM; MAGNETIC BRAKING; NEUTRON-STARS; TRIPLE STARS; BLACK-HOLE; SYSTEMS; VELOCITIES AB We study the formation of low-mass X-ray binaries (LMXBs) through helium star supernovae in binary systems that have each emerged from a common envelope phase. LMXB progenitors must satisfy a large number of evolutionary and structural constraints, including survival through common envelope evolution, through the post-common envelope phase, where the precursor of the neutron star becomes a Wolf-Rayet star, and survival through the supernova event. Furthermore, the binaries that survive the explosion must reach interaction within a Hubble time and must satisfy stability criteria for mass transfer. These constraints, imposed under the assumption of a symmetric supernova explosion, prohibit the formation of short-period LMXBs transferring mass at sub-Eddington rates through any channel in which the intermediate progenitor of the neutron star is not completely degenerate. Barring accretion-induced collapse, the existence of such systems therefore requires that natal kicks be imparted to neutron stars. We use an analytical method to synthesize the distribution of nascent LMXBs over donor masses and orbital periods and evaluate their birthrate and systemic velocity dispersion. Within the limitations imposed by observational incompleteness and selection effects, and our neglect of secular evolution in the LMXB state, we compare our results with observations. However, our principal objective is to evaluate how basic model parameters (common envelope ejection efficiency, rms kick velocity, primordial mass ratio distribution) influence these results. We conclude that the characteristics of newborn LMXBs are primarily determined by age and stability constraints and the efficiency of magnetic braking and are largely independent of the primordial binary population and the evolutionary history of LMXB progenitors (except for extreme values of the average kick magnitude or of the common envelope ejection efficiency). Theoretical estimates of total LMXB birthrates are not credible, since they strongly depend on the observationally indeterminate frequency of primordial binaries with extreme mass ratios in long-period orbits. C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Kalogera, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM vicky@astro.uiuc.edu; webbink@astro.uiuc.edu NR 69 TC 69 Z9 69 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1998 VL 493 IS 1 BP 351 EP 367 DI 10.1086/305085 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YV314 UT WOS:000071810800030 ER PT J AU Kalogera, V AF Kalogera, V TI Formation of low-mass X-ray binaries. III. A new formation mechanism: Direct supernova SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, close; pulsars, general; stars, evolution; stars, neutron; supernovae, general; X-rays, stars ID TIDAL CAPTURE BINARIES; RADIO PULSARS; EVOLUTION; COLLAPSE; STARS; CIRCULARIZATION; EXPLOSIONS; ORIGIN; CHAOS AB We propose a new formation mechanism (direct-supernova) for low-mass X-ray binaries (LMXBs) that does not involve any prior phase of mass transfer. Survival through the supernova (SN) explosion and shrinkage of the orbit is achieved by a kick velocity of appropriate magnitude and direction imparted to the neutron star at its birth. We present analytical population synthesis calculations of LMXBs forming via both the direct-SN and the helium star SN mechanisms and compare the results. We find that the direct-SN channel contributes a nonnegligible fraction of the total LMXB population, depending strongly on the rms magnitude of the kick velocity. More importantly, the direct-SN mechanism provides a natural way for the formation of low-mass binary pulsars in nearly circular orbits with orbital periods in excess of similar to 100(d), which cannot have been formed via the helium star SN mechanism. C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Kalogera, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM vicky@astro.uiuc.edu NR 30 TC 26 Z9 26 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 JAN 20 PY 1998 VL 493 IS 1 BP 368 EP 374 DI 10.1086/305086 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YV314 UT WOS:000071810800031 ER PT J AU Kumar, P Quataert, EJ AF Kumar, P Quataert, EJ TI On the orbital decay of the PSR J0045-7319 binary SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, close; pulsars, individual (PSR J0045-7319); stars, early-type; stars, oscillations; stars, rotation ID RADIO PULSAR; TIDAL EVOLUTION; CLOSE BINARIES; NEUTRON-STAR; FRICTION; SYSTEMS; CAPTURE; MODES; SPIN AB Recent observations of PSR J0045-7319, a radio pulsar in a close eccentric orbit with a massive main-sequence B star companion, indicate that the system's orbital period is decreasing on a timescale similar to 5 x 10(5) yr. Timing observations of PSR J0045-7319 also indicate that the B star is rotating rapidly, perhaps close to its breakup rotation rate. For rapid (supersynchronous) prograde rotation of the B star, tidal dissipation leads to an increasing orbital period for the binary system, while for retrograde rotation of any magnitude, the orbital period decreases with time. We show that if tidal effects are to account for the observed orbital decay of the PSR J0045-7319 binary, the B star must have retrograde rotation. This implies that the supernova that produced the pulsar in this binary system likely had a dipole anisotropy. For a reasonably wide range of retrograde rotation rates, the energy in the dynamical tide of the B star needs to be dissipated in about one orbital period in order to account for the observed orbital evolution time. We show, however, that the radiative dissipation of the dynamical tide in a rigidly rotating B star is too inefficient by a factor of approximate to 10(3) regardless of the magnitude of the rotation rate. We describe how, when the surface of the B star is rotating nearly synchronously, the energy in the dynamical tide is dissipated in less than an orbital period, thus reconciling the theoretical and observed rates of orbital evolution. Nonlinear parametric decay of the equilibrium tide, for rigid retrograde rotation of the B star, may also be able to explain the observed rate of orbital evolution, although the margin of instability is too small to draw definitive conclusions about the relevance of this process for the PSR J0045-7319 binary. C1 Inst Adv Study, Princeton, NJ 08540 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kumar, P (reprint author), Inst Adv Study, Olden Lane, Princeton, NJ 08540 USA. NR 25 TC 14 Z9 14 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1998 VL 493 IS 1 BP 412 EP 425 DI 10.1086/305091 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YV314 UT WOS:000071810800036 ER PT J AU Balakrishnan, N Kharchenko, V Dalgarno, A AF Balakrishnan, N Kharchenko, V Dalgarno, A TI Quantum mechanical and semiclassical studies of N+N-2 collisions and their application to thermalization of fast N atoms SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID POTENTIAL-ENERGY SURFACE; RATE CONSTANTS; NITRIC-OXIDE; TERRESTRIAL THERMOSPHERE; VELOCITY DISTRIBUTION; ATMOSPHERIC REACTION; TIME EVOLUTION; NITROGEN-ATOMS; LORENTZ GAS; WAVE-PACKET AB Energy loss of fast N(S-4) atoms in a bath gas of N-2 molecules is investigated taking into account elastic and inelastic collisions. Quantum mechanical calculations using a vibrationally close-coupled rotationally sudden approach are performed to obtain the elastic scattering cross sections. Inelastic cross sections involving re-vibrational transitions of the molecules are determined from a quantum-classical approach in which the vibrational motion of the molecule is treated by the time-dependent quantum mechanical method and the remaining degrees of freedom described by classical mechanics. The computed angular and energy resolved cross sections are used to construct the Boltzmann kernel for energy relaxation of fast N(4S) atoms from which the parameters governing the thermalization are readily extracted. (C) 1998 American Institute of Physics. [S0021-9606(98)01903-5]. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Balakrishnan, N (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 35 TC 25 Z9 25 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JAN 15 PY 1998 VL 108 IS 3 BP 943 EP 949 DI 10.1063/1.475458 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA YR359 UT WOS:000071487500015 ER PT J AU Cameron, AGW AF Cameron, AGW TI Isotope astrophysics - Two cradles for the heavy elements SO NATURE LA English DT Editorial Material ID INTERSTELLAR C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cameron, AGW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 3 Z9 3 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD JAN 15 PY 1998 VL 391 IS 6664 BP 228 EP + DI 10.1038/34535 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA YR328 UT WOS:000071484400022 ER PT J AU Kamionkowski, M Kosowsky, A AF Kamionkowski, M Kosowsky, A TI Detectability of inflationary gravitational waves with microwave background polarization SO PHYSICAL REVIEW D LA English DT Article ID TENSOR PERTURBATIONS; UNIVERSE; FLUCTUATIONS; MODELS; CONSTRAINTS; ANISOTROPY; COSMOLOGY; RADIATION; COBE AB Inflation predicts specific relations between the amplitudes and spectral indices of the primordial spectrum of density (scalar metric) perturbations and gravitational waves (tensor metric perturbations). Detection of a stochastic gravitational-wave background is essential for identifying this unmistakable signature. Polarization of the cosmic microwave background can isolate these tensor modes in a model-independent way and thereby circumvent the cosmic-variance limit to detecting a small tensor signal with only a temperature map. Here we assess the detectability of a gravity-wave background with a temperature and polarization map. For detector sensitivities better than 10-20 mu K root sec, the sensitivity to a tensor signal is always dominated by the polarization map. With a detector sensitivity of order 1 mu K root sec, polarization could improve on a temperature-map sensitivity to tensor modes by two to three orders of magnitude. Even a small amount of reionization substantially enhances tensor-mode detectability. We also argue that the sensitivity of the Planck Surveyor to tensor modes is significantly improved with polarization, even taking into account the resulting degradation of the intensity determination in the high-frequency channels. C1 Columbia Univ, Dept Phys, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Lyman Lab Phys, Cambridge, MA 02138 USA. RP Kamionkowski, M (reprint author), Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA. EM kamion@phys.columbia.edu; akosowksy@cfa.harvard.edu OI Kamionkowski, Marc/0000-0001-7018-2055 NR 53 TC 94 Z9 94 U1 1 U2 2 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 JAN 15 PY 1998 VL 57 IS 2 BP 685 EP 691 DI 10.1103/PhysRevD.57.685 PG 7 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA YU015 UT WOS:000071671300006 ER PT J AU Puchnarewicz, EM Mason, KO Siemiginowska, A AF Puchnarewicz, EM Mason, KO Siemiginowska, A TI The ultraviolet spectrum of the narrow-line Seyfert 1 galaxy RE J1034+396 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; line, formation; galaxies, active; galaxies, individual, RE J1034+396; galaxies, Seyfert; X-rays, galaxies ID ACTIVE GALACTIC NUCLEI; ENERGY-DISTRIBUTIONS; EMISSION-LINES; REGION; VARIABILITY; NGC-5548; ORIGIN AB REJ1034+396 has one of the hottest big blue bumps of any Seyfert 1 (kT(BB) similar to 120 eV) and thus provides a valuable insight into the physics in the nuclei of active galaxies. In this paper, we present UV spectroscopy of REJ1034+396, taken with the Faint Object Spectrograph on the Hubble Space Telescope. With a spectral resolution of similar to 1-2 Angstrom FWHM and a typical signal-to-noise ratio of similar to 15 per diode, this is one of the first detailed UV spectra of an object in the narrow-line Seyfert 1 (NLS1) class, The spectrum probes the physics and kinematics of the high-ionization and coronal line gas, and the strength and form of the big blue bump component in the UV. We detect many emission lines, including Ly alpha: CIV lambda 1549, He II lambda 1640, CIII] lambda 1909 and Mg II lambda 2798. We also identify a feature at 2647 Angstrom (in the rest frame) with highly ionized iron ([Fe XI] lambda 2649); a line of the same species ([Fe XI] lambda 7892) has also been seen in the optical spectrum, The velocity widths of the UV lines are relatively narrow (FWHM<2000 km s(-1)), although CIV lambda 1549 appears to have a broad underlying component with a FWHM typical of quasars (similar to 5500 km s(-1)). The FWHM are similar to those of the optical lines, which suggests that all line emission in REJ1034+396, i.e. including that of high-and low-ionization species and the forbidden lines, may be dominated by an intermediate-velocity (FWHM similar to 1000 km s(-1)), intermediate-density (log N(e) similar to 7.5 cm(-3)) region of gas. The slope of the UV continuum (alpha(uv) similar to 0.9) is soft (i.e. red) relative to quasars and the UV to soft X-ray flux ratio is unusually low (the 0.2 keV/1200 Angstrom flux ratio is 1/200), implying that the big blue bump component is very weak in the UV. The present-epoch UV to soft X-ray continuum is consistent with earlier data, demonstrating that this extreme big blue bump component is also very stable, unlike many other NLS1s which show extreme patterns of variability. C1 UCL, Mullard Space Sci Lab, Surrey RH5 6NT, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Puchnarewicz, EM (reprint author), UCL, Mullard Space Sci Lab, Surrey RH5 6NT, England. NR 26 TC 9 Z9 9 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 1998 VL 293 IS 2 BP L52 EP L56 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YT932 UT WOS:000071661000002 ER PT J AU Hillenbrand, LA Hartmann, LW AF Hillenbrand, LA Hartmann, LW TI A preliminary study of the Orion Nebula Cluster structure and dynamics SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics, stellar dynamics; open clusters and associations, individual (Orion Nebula Cluster); stars, evolution ID INITIAL MASS FUNCTION; A MOLECULAR CLOUD; TRAPEZIUM CLUSTER; CARBON-MONOXIDE; STAR-FORMATION; MULTITRANSITION; CONSTRAINTS AB We use optical and near-infrared star counts to explore the structure and dynamics of the Orion Nebula Cluster !ONC). This very young (<1 Myr) cluster is not circularly symmetric in projection but is elongated north-south in a manner similar to the molecular gas distribution in the region, suggesting that the stellar system may still reflect the geometry of the protocluster cloud. Azimuthally averaged stellar source counts compare well with simple spherically symmetric, single-mass King cluster models. The model fits suggest that the inner Trapezium region should be regarded as the core of the ONC, not as a distinct entity as sometimes advocated. We estimate that the core radius of the cluster is 0.16-0.21 pc and that the central stellar density approaches 2 x 10(4) stars pc(-3). Adopting the stellar velocity dispersion from published proper-motion studies, virial equilibrium would require a total mass within about 2 pc of the Trapezium of similar to 4500 M., slightly more than twice the mass of the known stellar population and comparable to the estimated mass in molecular gas projected onto the same region of the sky. If greater than or similar to 20% of the remaining molecular gas is converted into stars, thus adding to the binding mass, given that the present stellar population alone has a total energy close to zero, the ONC is likely to produce a gravitationally bound cluster. The ONC also exhibits mass segregation, with the most massive (Trapezium) stars clearly concentrated toward the center of the cluster and some evidence for the degree of central concentration to decrease with decreasing mass down to 1-2 M., as would be expected for general mass segregation. Given the extreme youth of the stars compared with the estimated range of collisional relaxation times, the mass segregation is unlikely to be the result of cluster relaxation. Instead, we suggest that the mass segregation reflects a preference for higher mass stars to form in dense. central cluster regions. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hillenbrand, LA (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. NR 53 TC 481 Z9 485 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1998 VL 492 IS 2 BP 540 EP 553 DI 10.1086/305076 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU308 UT WOS:000071704200010 ER PT J AU Narayan, R Mahadevan, R Grindlay, JE Popham, RG Gammie, C AF Narayan, R Mahadevan, R Grindlay, JE Popham, RG Gammie, C TI Advection-dominated accretion model of Sagittarius A*: Evidence for a black hole at the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy, center; radiation mechanisms, thermal ID X-RAY BURSTER; SOURCE SGR-A; RADIO-SOURCE; CENTER REGION; CYGNUS X-1; GALAXY; SPECTRUM; LUMINOSITY; EMISSION; DISK AB Sagittarius A*, which is located at the Galactic center, is a puzzling source. It has a mass of M = (2.5) +/- 0.4) x 10(6) M., which makes it an excellent black hole candidate. Observations of stellar winds and other gas hows in its vicinity suggest a mass accretion rate of M over dot greater than or similar to few x 10(-6) M. yr(-1). However, such an accretion rate would imply a luminosity greater than 10(40) ergs(-1) if the radiative efficiency is the usual 10%, whereas observations indicate a bolometric luminosity less than 10(37) ergs(-1). The spectrum of Sgr A* is unusual, with emission extending over many decades of wavelength. We present a model of Sgr A* that is based on a two-temperature optically thin advection-dominated accretion flow. The model is consistent with the estimated M and M over dot and fits the observed fluxes in the centimeter/millimeter and X-ray bands, as well as upper limits in the submillimeter and infrared bands; the fit is less good in the radio spectrum below 86 GHz and in gamma-rays above 100 MeV. The very low luminosity of Sgr A* is explained naturally in the model by means of advection. Most of the viscously dissipated energy is advected into the central mass by the accreting gas, and therefore the radiative efficiency is extremely low, similar to 5 x 10(-6). A critical element of the model is the presence of an event horizon at the center that swallows the advected energy. The success of the model could thus be viewed as confirmation that Sgr A* is a black hole. 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. EM marayan@cfa.harvard.edu; rmahadevan@cfa.harvard.edu; jgrindlay@cfa.harvard.edu; popham@mpa-garching.mpg.de; cgammie@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 97 TC 302 Z9 306 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 JAN 10 PY 1998 VL 492 IS 2 BP 554 EP 568 DI 10.1086/305070 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU308 UT WOS:000071704200011 ER PT J AU Garay, G Moran, JM Rodriguez, LF Reid, MJ AF Garay, G Moran, JM Rodriguez, LF Reid, MJ TI The G19.6-0.2 region of star formation: Molecular and ionized environs SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; ISM, individual (G19.6-0.2); ISM, molecules; ISM, structure; radio lines, ISM; stars, formation ID H-II REGIONS; ULTRACOMPACT HII-REGIONS; HOT AMMONIA; VLA OBSERVATIONS; NH3 OBSERVATIONS; CLOUDS; IMPLOSION; G34.3+0.2; EMISSION; W3(OH) AB We present VLA observations, made with angular resolutions of 2 "-3 ", of the ionized gas (H66 alpha recombination line and 1.6 GHz continuum) and of the molecular gas ([2, 2] inversion transition of NH3) toward the star formation region known as G19.6-0.2. The observations of the ionized gas indicate the presence of five distinct H II regions that are excited by individual stars, implying the presence of a cluster of O-B stars. Three of the individual H II regions have ringlike structures, with sizes ranging from 0.1 to 0.4 pc, and have clumpy and inhomogeneous distributions of gas. Some of the ultracompact structures detected toward these regions with higher angular resolution (similar to 0.4 ") probably are associated with partially ionized clumps, which are externally ionized, and embedded within larger H II, regions. The brightest compact H II region within the complex shows a cometary-like morphology, which may be due to the expansion of ionized gas in an anisotropic medium. The ammonia observations show that the molecular emission arises from three distinct structures: a dense (similar to 9 x 10(6) cm(-3)) clump, located near the center of the cluster of H II regions, which has a size of similar to 0.05 pc and exhibits very broad line widths (similar to 9.5 km s(-1)), and two less dense (similar to 1 - 2 x 10(5) cm(-3)) clumps, one of which is detected in absorption toward the northernmost H II region. The physical relationship between these molecular structures and the ionized gas is discussed. We find that the cometary-like and the most compact H II region within the complex are intimately associated with the densest ammonia clump. The mean velocity of the ionized gas is blueshifted with respect to the mean velocity of the molecular clump by 3.5 km s(-1). We suggest that the star that excites this H II region was formed at the edge of the densest molecular clump. The ionized gas flowing toward the observer is undergoing expansion into the lower density interclump medium (champagne flow). In the opposite direction, the H II region is driving a shock into the dense molecular clump, compressing it and further increasing its density. The less dense ammonia clumps are probably heated and compressed by the shock fronts driven by the more extended H II regions. C1 Univ Chile, Dept Astron, Santiago, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Autonomous Univ Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Garay, G (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. RI Garay, Guido/H-8840-2013 OI Garay, Guido/0000-0003-1649-7958 NR 38 TC 25 Z9 25 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1998 VL 492 IS 2 BP 635 EP 649 DI 10.1086/305046 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU308 UT WOS:000071704200017 ER PT J AU Myers, PC Adams, FC Chen, H Schaff, E AF Myers, PC Adams, FC Chen, H Schaff, E TI Evolution of the bolometric temperature and luminosity of young stellar objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, evolution; stars, fundamental parameters; stars, pre-main-sequence ID AURIGA MOLECULAR CLOUD; LOW-MASS STARS; DENSE CORES; DARK CLOUDS; HL TAURI; PROTOSTARS; DISKS; POPULATION; COLLAPSE; CHAMELEON AB We model the broadband emission from a star-disk-envelope system to obtain expressions for the bolometric temperature T-bol and luminosity L-bol as functions of time, from the youngest class 0 protostars to stars on the zero-age main sequence. The model predicts evolution, driven by infall and contraction luminosity, in terms of position on the log T-bol-log L-bol diagram, a close analog of the H-R diagram. The evolutionary tracks depend on the envelope initial conditions, the main-sequence mass of the star, and the envelope dissipation timescale. The model L-bol rises due to infall and then falls due to contraction, while T-bol increases steadily toward the main sequence due to central heating and envelope dissipation. In order to smoothly join the protostellar and pre-main-sequence phases it is necessary to model the termination of infall as gradual rather than sudden. This change reduces the peak infall luminosity for the collapse of a singular isothermal sphere by a factor 4, bringing predicted infall luminosities into better agreement with observations. For stars of main-sequence mass 0.5 M., the model decrease in L-bol from its peak value of similar to 3 L. at T-bol similar to 250 K (class I) to similar to 0.4 L. at T-bol similar to 3000 K (class II/III) closely matches the observed decrease in median L-bol for young stellar objects in Chamaeleon, Corona Australis, Lupus, Ophiuchus, and Taurus. The model should be useful for estimating the distributions of mass and age, and for describing the birth history, of stars younger than 1 Myr in well-studied complexes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 66 TC 74 Z9 74 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1998 VL 492 IS 2 BP 703 EP 726 DI 10.1086/305048 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU308 UT WOS:000071704200022 ER PT J AU Muzerolle, J Calvet, N Hartmann, L AF Muzerolle, J Calvet, N Hartmann, L TI Magnetospheric accretion models for the hydrogen emission lines of T Tauri stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; line, profiles; radiative transfer; stars, pre-main-sequence ID ATOMIC-HYDROGEN; YOUNG STARS; BP-TAURI; VARIABILITY; PROFILES; WINDS; ORIGIN; DISKS; RATES; FLOWS AB Using a statistical equilibrium radiative transfer treatment, we examine the behavior of hydrogen emission lines arising from the magnetospheric infall zones of classical T Tauri stars. Having calculated self-consistent line profiles of the Balmer lines, Pa beta and Br gamma, we explore parameter space, examining the effects of the magnetospheric gas temperature and size on the line fluxes. We compare model and observed line fluxes for the Balmer lines and find a good match using a relatively small. range of parameters. We are also able to match the observed Br gamma line profile of the embedded object WL 16, which supports the use of the infrared lines in studying magnetospheric infall even in the earliest stages of star formation. Finally, we discuss constraints on the physical parameters and the possibility of using the emission lines as accretion rate indicators. C1 Univ Massachusetts, Five coll, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Invest Astron, Merida, Venezuela. RP Muzerolle, J (reprint author), Univ Massachusetts, Five coll, Dept Astron, Amherst, MA 01003 USA. NR 38 TC 182 Z9 182 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1998 VL 492 IS 2 BP 743 EP 753 DI 10.1086/305069 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU308 UT WOS:000071704200024 ER PT J AU Eikenberry, SS Fazio, GG Ransom, SM AF Eikenberry, SS Fazio, GG Ransom, SM TI ROSAT timing of the LMC pulsar 0540-69 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars, individual (PSR 0540-69); stars, neutron; X-rays, stars ID PSR 0540-69 AB We present a timing study of the young rotation-powered pulsar 0540-69 in the Large Magellanic Cloud, based on 130 ks of archival ROSAT data spanning a similar to 3 yr period. We use "f-(f) over dot" techniques to measure the pulsar frequency as a function of frequency derivative at 17 independent epochs. From these measurements we derive a timing solution with a braking index n = 2.5(-0.7)(+0.6), and we compare this solution to previous timing studies of 0540-69. Using this frequency-based solution, we create 27 pulse profiles and perform a time-of-arrival (TOA) analysis to investigate further the pulsar's timing behavior. While we can fit smooth spin-down models to subsets of the TOAs spanning up to 2 yr successfully, we are unable to obtain acceptable phase-coherent fits to the entire 3 yr set of TOAs. This behavior provides the first clear evidence for timing noise in 0540-69. We discuss the implications of these results for understanding previous studies of the timing behavior of 0540-69. 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 15 TC 13 Z9 13 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1998 VL 492 IS 2 BP 754 EP 760 DI 10.1086/305072 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU308 UT WOS:000071704200025 ER PT J AU Chen, W McCarthy, MC Travers, MJ Gottlieb, EW Munrow, MR Novick, SE Gottlieb, CA Thaddeus, P AF Chen, W McCarthy, MC Travers, MJ Gottlieb, EW Munrow, MR Novick, SE Gottlieb, CA Thaddeus, P TI Laboratory detection of a new carbon chain radical: H2CCCCN SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, molecules; line, identification; methods, laboratory; radio lines, ISM ID ROTATION AB The cyanopropynyl radical, H2CCCCN, was detected in a supersonic molecular beam by Fourier transform microwave spectroscopy. For the normal and N-15 species, 89 and 40 hyperfine components, respectively, from four successive rotational transitions (N = 2 --> 1 to 5 --> 4) in the lowest energy (K-a = 0) rotational ladder were measured between 8 and 22 GHz to an uncertainty of 5 kHz. With this data, the microwave constants of cyanopropynyl, including the fine and hyperfine coupling constants, are determined to very high accuracy, and the most interesting lines in the radio spectrum from an astronomical standpoint can now be calculated to a fraction of 1 km s(-1) in equivalent radial velocity. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Wesleyan Univ, Dept Chem, Middletown, CT 06459 USA. RP Chen, W (reprint author), Harvard Univ, Div Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 17 TC 9 Z9 10 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1998 VL 492 IS 2 BP 849 EP 853 DI 10.1086/305066 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU308 UT WOS:000071704200035 ER PT J AU Gingerich, O AF Gingerich, O TI On the revolutions of the heavenly spheres SO NATURE LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 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 JAN 8 PY 1998 VL 391 IS 6663 BP 140 EP 140 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA YQ378 UT WOS:000071380900039 ER PT J AU Gingerich, O AF Gingerich, O TI Johannes Kepler, The 'Harmony of the World' SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TIMES SUPPLEMENTS LIMITED PI MARKET HARBOROUGH PA TOWER HOUSE, SOVEREIGN PARK, MARKET HARBOROUGH LE87 4JJ, ENGLAND SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD JAN 2 PY 1998 IS 4944 BP 6 EP 6 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA YT335 UT WOS:000071591300008 ER PT J AU Gingerich, O AF Gingerich, O TI The music of the heavens - Kepler's harmonic astronomy SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TIMES SUPPLEMENTS LIMITED PI MARKET HARBOROUGH PA TOWER HOUSE, SOVEREIGN PARK, MARKET HARBOROUGH LE87 4JJ, ENGLAND SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD JAN 2 PY 1998 IS 4944 BP 6 EP 6 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA YT335 UT WOS:000071591300010 ER PT J AU Gingerich, O AF Gingerich, O TI Kepler's physical astronomy SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TIMES SUPPLEMENTS LIMITED PI MARKET HARBOROUGH PA TOWER HOUSE, SOVEREIGN PARK, MARKET HARBOROUGH LE87 4JJ, ENGLAND SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD JAN 2 PY 1998 IS 4944 BP 6 EP 6 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA YT335 UT WOS:000071591300009 ER PT J AU Hershler, R AF Hershler, R TI A systematic review of the hydrobiid snails (Gastropoda : Rissooidea) of the Great Basin, western United States. Part I. Genus Pyrgulopsis SO VELIGER LA English DT Review ID DEATH-VALLEY; CALIFORNIA; RIVER AB A recently completed field survey of springs throughout the Great Basin yielded collections of hydrobiid snails from more than 500 sites, and revealed a wealth of undescribed diversity of these small gastropods. In this, the first of a two-part taxonomic series treating this material, 58 new species of Pyrgulopsis Call & Pilsbry, 1886, are described; and new records are provided for 10 previously described members of this genus. Assignment of these novelties to Pyrgulopsis is done with the acknowledgement that this large genus, as currently constituted, is probably not monophyletic, but a more refined classification of these snails reflecting evolutionary relationships must await preparation of a phylogenetic analysis, which is beyond the scope of this work. Pyrgulopsis occur in a variety of spring-fed water bodies in the Great Basin, including brackish and/or thermal habitats. Although a few species are widespread in the region, local endemism is prevalent and 22 of the new species are known only from single localities. Several areas contain concentrations of locally endemic snails which may represent species flocks, notably Duckwater Valley (seven species) and southern Steptoe Valley (five species). This fauna is largely distributed in an allopatric fashion, although a few springs harbor two or three species. Most of the springs inhabited by hydrobiids in the region are small, fishless, and have been ignored by state and federal land management agencies. However, many of these sites are degraded by livestock grazing, water withdrawal, and other activities and will require protection in order to conserve snails and other native aquatic biota. Two of the novelties described herein have become extinct during the past two decades. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool Mollusks, Washington, DC 20560 USA. RP Hershler, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool Mollusks, NHB STOP 118, Washington, DC 20560 USA. NR 90 TC 64 Z9 65 U1 0 U2 3 PU CALIF MALACOZOOLOGICAL SOC INC PI SANTA BARBARA PA SANTA BARBARA MUSEUM NATURAL HISTORY, 2559 PUESTA DEL SOL RD, SANTA BARBARA, CA 93105 USA SN 0042-3211 J9 VELIGER JI Veliger PD JAN 2 PY 1998 VL 41 IS 1 BP 1 EP 132 PG 132 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA YQ668 UT WOS:000071411300001 ER PT S AU Narayan, R AF Narayan, R BE Holt, SS Kallman, TR TI Hot accretion flows - Key issues SO ACCRETION PROCESSES IN ASTROPHYSICAL SYSTEMS: SOME LIKE IT HOT! SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 8th Astrophysics Conference on Accretion Processes in Astrophysical Systems - Some Like It Hot CY OCT, 1997 CL COLLEGE PK, MD C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, 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 1-56396-767-7 J9 AIP CONF PROC PY 1998 IS 431 BP 15 EP 32 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL29Y UT WOS:000075033300002 ER PT S AU Gammie, CF AF Gammie, CF BE Holt, SS Kallman, TR TI Numerical models of accretion disks SO ACCRETION PROCESSES IN ASTROPHYSICAL SYSTEMS: SOME LIKE IT HOT! SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 8th Astrophysics Conference on Accretion Processes in Astrophysical Systems - Some Like It Hot CY OCT, 1997 CL COLLEGE PK, MD AB I review recent numerical studies of accretion disks, focusing on measurements of the turbulent shear stress, or cu, in the shearing box model. I conclude with a list of astronomically relevant open questions that can be settled via future numerical experiments. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gammie, CF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-767-7 J9 AIP CONF PROC PY 1998 IS 431 BP 99 EP 107 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL29Y UT WOS:000075033300011 ER PT S AU Psaltis, D Lamb, FK AF Psaltis, D Lamb, FK BE Holt, SS Kallman, TR TI Compton scattering and the X-ray spectra of accreting compact objects SO ACCRETION PROCESSES IN ASTROPHYSICAL SYSTEMS: SOME LIKE IT HOT! SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 8th Astrophysics Conference on Accretion Processes in Astrophysical Systems - Some Like It Hot CY OCT, 1997 CL COLLEGE PK, MD AB We present the results of detailed numerical calculations of the transport of radiation in spherical accretion flows onto compact objects. We show that Comptonization by the electron bulk motion should not be neglected in computing the X-ray spectra of accreting compact objects and demonstrate the importance of retaining the terms in the radiative transfer equation that are at least second-order in the electron bulk velocity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Psaltis, 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 AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-767-7 J9 AIP CONF PROC PY 1998 IS 431 BP 125 EP 128 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL29Y UT WOS:000075033300016 ER PT S AU Siemiginowska, A AF Siemiginowska, A BE Holt, SS Kallman, TR TI Evolution of accretion disks in AGN SO ACCRETION PROCESSES IN ASTROPHYSICAL SYSTEMS: SOME LIKE IT HOT! SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 8th Astrophysics Conference on Accretion Processes in Astrophysical Systems - Some Like It Hot CY OCT, 1997 CL COLLEGE PK, MD AB Thermal-viscous instabilities cause variations in the local accretion rate of the standard accretion disk around a supermassive black hole. We show that a part of the disk should exhibit the transition to the ADAF state because the local accretion rate becomes smaller than the critical accretion rate for that transition in the low state of the instability cycle. 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 AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-767-7 J9 AIP CONF PROC PY 1998 IS 431 BP 211 EP 214 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL29Y UT WOS:000075033300032 ER PT S AU Rybicki, GB Bromley, BC AF Rybicki, GB Bromley, BC BE Holt, SS Kallman, TR TI Spectral line signatures of relativistic disks SO ACCRETION PROCESSES IN ASTROPHYSICAL SYSTEMS: SOME LIKE IT HOT! SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 8th Astrophysics Conference on Accretion Processes in Astrophysical Systems - Some Like It Hot CY OCT, 1997 CL COLLEGE PK, MD AB We consider emission line formation in a thin accretion disk around a black hole, taking into account the differential flow of material in the disk. If the disk is optically thick in the line, local velocity gradients can cause the integrated intensity to have azimuthal dependence in the emitter frame. We examine this effect with simple parameterized models based on Sobolev theory to highlight the overall character of the changes in the observed line profile. The shape of the profile, which can serve as a diagnostic of the disk geometry and the spin of the black hole, may be significantly altered by the velocity-gradient effect. Specifically, we find that the effect causes a decrease of flux in the blue Doppler peak, which in turn would lead to an underestimate of the inner disk radius. If the inner radius were used as a signature of black hole rotation, as when the disk is not emissive within the marginally stable circular orbit, then the inferred rotation would be overestimated in cases where the emissivity of the disk has fairly shallow fall-off with radius. If the disk were emissive even within the marginally stable orbit, then the local azimuthal anisotropy of emission could produce features in the line profile which distinguish rotating from nonrotating black holes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rybicki, GB (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 1-56396-767-7 J9 AIP CONF PROC PY 1998 IS 431 BP 265 EP 268 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL29Y UT WOS:000075033300042 ER PT S AU Bromley, BC Miller, WA Pariev, VI AF Bromley, BC Miller, WA Pariev, VI BE Holt, SS Kallman, TR TI Bounds on the inner radius of emission around supermassive black holes SO ACCRETION PROCESSES IN ASTROPHYSICAL SYSTEMS: SOME LIKE IT HOT! SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 8th Astrophysics Conference on Accretion Processes in Astrophysical Systems - Some Like It Hot CY OCT, 1997 CL COLLEGE PK, MD AB Observations of iron K-alpha fluorescence lines in Seyfert galaxies provide strong evidence for an accretion disk around a supermassive black hole as the source of the line emission. Here we consider a diagnostic of a disk line profile, based on the minimum and maximum frequency of emission, to robustly constrain the inner radius of the disk. This diagnostic is applied to spectra from Seyfert I galaxies (Iwasawa et al. 1996 [1]; Nandra et al. 1997 [2]), and a composite Seyfert II spectrum (Turner et al. 1997 [3]). We are able to place firm bounds on the inner radius of emission from the bright nucleus in MCG-6-30-15; we find that the disk extends to within 6.2 R-g of the central black hole, independent of inclination angle (R-g, is GM/c(2) for a black hole of mass M). With inclination angle constraints-we find 29 +/- 5 degrees from frequency extrema of the [1] data-the inner radius bounded by 5.2 +/- 0.6 R-g. The frequency extrema of composite Seyfert I and II spectra both show inner radii below about 20 R-g, and are consistent with modest inclination angles (i < 45 degrees). Hence, at the present noise level, the data do not support Seyfert unification models based on orientation effects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bromley, BC (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 1-56396-767-7 J9 AIP CONF PROC PY 1998 IS 431 BP 269 EP 272 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL29Y UT WOS:000075033300043 ER PT S AU Schlegel, EM Kallman, T Mukai, K Ishida, M AF Schlegel, EM Kallman, T Mukai, K Ishida, M BE Holt, SS Kallman, TR TI An ASCA observation of the eclipsing cataclysmic variable XY Ari SO ACCRETION PROCESSES IN ASTROPHYSICAL SYSTEMS: SOME LIKE IT HOT! SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 8th Astrophysics Conference on Accretion Processes in Astrophysical Systems - Some Like It Hot CY OCT, 1997 CL COLLEGE PK, MD AB We report on a 32 ksec ASCA observation of the eclipsing cataclysmic variable XY Ari. The ASCA data are best fit by a power law indicating that material with a range of temperatures contributes to the total emission. The Fe line behavior is complex and varies with orbital phase. A 6.55 keV line with an equivalent width of similar to 220 eV is detected in the phase range similar to 0.10-0.30. A 6.4 keV line with an equivalent width of similar to 400 eV is detected in the range similar to 0.30-0.50., Upper limits on the equivalent widths of similar to 100-150 eV exist on both lines in the 0.50-0.90 phase range. 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 AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-767-7 J9 AIP CONF PROC PY 1998 IS 431 BP 475 EP 478 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL29Y UT WOS:000075033300080 ER PT J AU Kaluzny, J Wysocka, A Stanek, KZ Krzeminski, W AF Kaluzny, J Wysocka, A Stanek, KZ Krzeminski, W TI BVI CCD photometry of the globular cluster 47 Tuc SO ACTA ASTRONOMICA LA English DT Article DE globular clusters : individual : 47 Tuc; techniques : photometric; Stars : distances ID HUBBLE-SPACE-TELESCOPE; BLUE STRAGGLER; COLOR-MAGNITUDE; METAL-RICH; MILKY-WAY; 47-TUCANAE; STARS; CORE; POPULATIONS; TUCANAE AB We present BVI photometry for about 16000 stars from a 220 square arcmin field centered 8 arcmin East of the center of 47 Tuc. We have identified eight likely blue stragglers located in the outer parts of the cluster. Four of these objects are easy targets for spectroscopic studies with ground-based telescopes. Six candidates for blue horizontal branch stars were identified. However, it is possible that all or most of them belong in fact to the SMC halo. One faint blue star being candidate for a cataclysmic variable was found close to the cluster center. The average I-band magnitude for stars forming the red giant branch clump is determined at I-0 = 13.09 +/- 0.005 mag. This in turn implies distance modulus of the cluster (m - M)(0,47Tuc) = 13.32 +/- 0.03 +/- 0.036 mag(statistical plus systematic error), if we adopt M-I,M-m = -0.23 +/- 0.03 mag for the average absolute luminosity of Hipparcos-calibrated clump giants, following Paczynski and Stanek and Stanek and Garnavich. This distance modulus of 47 Tuc is lower by 0.2-0.25 mag than its recent estimates based on Hipparcos parallaxes for subdwarfs. We discuss possible reasons for this discrepancy. The photometric data are available through the anonymous ftp service. C1 Warsaw Univ Observ, PL-00478 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Observ, Las Campanas Observ, La Serena, Chile. RP Kaluzny, J (reprint author), Warsaw Univ Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. NR 33 TC 33 Z9 34 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 1998 VL 48 IS 3 BP 439 EP 453 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122PW UT WOS:000076081500005 ER PT J AU Mochejska, BJ Kaluzny, J Krockenberger, M Sasselov, DD Stanek, KZ AF Mochejska, BJ Kaluzny, J Krockenberger, M Sasselov, DD Stanek, KZ TI Identification and photometry of globular clusters in M31 and M33 Galaxies SO ACTA ASTRONOMICA LA English DT Article DE Galaxies : individual : M31, M33; catalogs ID SYSTEM; SEARCH; CANDIDATES AB We have used the data from the DIRECT project to search for new globular cluster candidates in the M31 and M33 galaxies. We have found 67 new objects in M31 and 35 in M33 and confirmed 38 and 16 previously discovered ones. A VI and BVI photometry has been obtained for all the clusters in M31 and M33, respectively. Luminosity functions have been constructed for the clusters in each galaxy and compared with that of the Milky Way. C1 Warsaw Univ Observ, PL-00478 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mochejska, BJ (reprint author), Warsaw Univ Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. NR 21 TC 48 Z9 48 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 1998 VL 48 IS 3 BP 455 EP 488 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122PW UT WOS:000076081500006 ER PT J AU You, L Hoston, W Lewenstein, M Marinescu, M AF You, L Hoston, W Lewenstein, M Marinescu, M TI Low energy excitation spectra of trapped bose condensates SO ACTA PHYSICA POLONICA A LA English DT Article; Proceedings Paper CT International Conference on Quantum Optics IV CY JUN 17-24, 1997 CL JASZOWIEC, POLAND ID COLLECTIVE EXCITATIONS; EINSTEIN CONDENSATION; EXCITED-STATES; GAS AB We discuss our numerical studies of the low energy excitations of trapped Bose condensates using a Bogoliubov-Hartree treatment. In the zero temperature limit, the lowest few excitation frequencies calculated within the Bogoliubov approximation agree well with the experimental data. Finite temperature results obtained using the Popov approximation display qualitative differences from the experimental data close to the critical temperature region. Details of our numerical approach are presented and comparison with other results is discussed. C1 Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Ctr Etud Saclay, SPAM, DRECAM, DSM,Commissariat Energie Atom, F-91191 Gif Sur Yvette, France. RP You, L (reprint author), Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. RI Lewenstein, Maciej/I-1337-2014 OI Lewenstein, Maciej/0000-0002-0210-7800 NR 52 TC 7 Z9 7 U1 0 U2 0 PU POLISH ACAD SCIENCES INST PHYSICS PI WARSAW PA AL LOTNIKOW 32-46, PL-02-668 WARSAW, POLAND SN 0587-4246 J9 ACTA PHYS POL A JI Acta Phys. Pol. A PD JAN PY 1998 VL 93 IS 1 BP 211 EP 235 PG 25 WC Physics, Multidisciplinary SC Physics GA YU318 UT WOS:000071705300018 ER PT S AU Grindlay, JE AF Grindlay, JE BE Riedler, W Torkar, K TI Balloon-borne hard X-ray imaging and future surveys SO ACTIVE EXPERIMENTS IN SPACE PLASMAS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 31st COSPAR Scientific Assembly CY JUL 14-21, 1996 CL BIRMINGHAM, ENGLAND SP Comm Space Res, World Climate Res Programme, European Space Agcy, NOAA, Natl Environm Satellite Data & Informat Sci, Sci Comm Ocean Res, Int Union Geol Sci, Int Astronaut Federat, Int Decade Nat Disaster Reduct, UNESCO, UN, Off Outer Space Affairs ID TELESCOPE; DETECTORS; ASTRONOMY AB Several payloads for hard X-ray (20-600 keV) imaging with coded aperture telescopes have been developed for balloon flight observations of cosmic x-ray sources. We briefly review the characteristics of these, particularly the EXITE2 system. The recent NASA program to develop an extended long duration (100d) balloon flight capability employing super-pressure balloons would allow a qualitatively new hard x-ray imaging experiment: the Energetic X-ray Imaging Survey Telescope-Long Integration Time Experiment (EXIST-LITE). The longer continuous viewing times (per source) available from an LDB platform than from low earth orbit would enable both surveys and objectives complementary to the EXIST mission proposed for a MIDEX satellite. We summarize the scientific objectives of EXIST-LITE, a possible instrumentation approach incorporating a large area array of Cd-Zn-Te (CZT) detectors, and our program for the development and balloon flight testing of relatively thick (5mm) CZT detector arrays. (C) 1998 COSPAR. Published by Elsevier Science Ltd. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 2 Z9 2 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0273-1177 BN 0-08-043460-6 J9 ADV SPACE RES PY 1998 VL 21 IS 7 BP 999 EP 1008 DI 10.1016/S0273-1177(97)01088-0 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BL02N UT WOS:000074073000012 ER PT S AU Moran, JM AF Moran, JM BE Phillips, TG TI The Submillimeter Array SO ADVANCED TECHNOLOGY MMW, RADIO, AND TERAHERTZ TELESCOPES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Conference on Advanced Technology MMW, Radio, and Terahertz Telescopes CY MAR 26-28, 1998 CL KONA, HI SP SPIE, European So Observ DE interferometry; SIS receivers; submillimeter wavelength astronomy AB The design and current construction status of the Submillimeter Array is discussed. The array mill consist of eight 6-m elements that are reconfigurable to achieve baselines from 8 to 508 m. The array will be located on Mauna Kea in Millimeter Valley, at an elevation of 4,080 m, and will cover all bands from 180 to 900 GHz. Provisions are being made to include the CSO and JCMT telescopes in the array, which will substantially increase its capability. Most of the development and assembly is underway at the test site in Westford, Massachusetts and in Taiwan. Holography and radiometry of planets at 3.3 mm wavelength have been carried out on the prototype antenna of the array. It is expected to reach its performance specifications, which include 12 mu m surface accuracy and 1 " pointing. The prototype correlator is complete and board replication is underway. Most of the civil work at the site is complete. Interferometric tests of two antennas in Westford are expected to begin in mid-1998, and similar tests on Mauna Kea are expected to begin in 1999. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moran, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 28 Z9 28 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2804-3 J9 P SOC PHOTO-OPT INS PY 1998 VL 3357 BP 208 EP 209 DI 10.1117/12.317355 PG 2 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL55D UT WOS:000075850400022 ER PT S AU Melnick, GJ AF Melnick, GJ BE Phillips, TG TI The Submillimeter Wave Astronomy Satellite: Science objectives and instrument description SO ADVANCED TECHNOLOGY MMW, RADIO, AND TERAHERTZ TELESCOPES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Conference on Advanced Technology MMW, Radio, and Terahertz Telescopes CY MAR 26-28, 1998 CL KONA, HI SP SPIE, European So Observ DE spectroscopy; submillimeter, star formation; cloud cooling, space astronomy 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(H-2)>10(3) cm(-3)) molecular clouds within our galaxy in either the ground-stale or a low-lying transition of five astrophysically important species; H2O, (H2O)-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 13CO 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, H-2 O-18, O-2,CI, and (CO)-C-13 lines. All measurements will be conducted with a velocity resolution of less than 1 km s(-1). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Melnick, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 3 Z9 3 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2804-3 J9 P SOC PHOTO-OPT INS PY 1998 VL 3357 BP 348 EP 358 DI 10.1117/12.317419 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL55D UT WOS:000075850400036 ER PT S AU Stark, AA Carlstrom, JE Israel, FP Menten, KM Peterson, JB Phillips, TG Sironi, G Walker, CK AF Stark, AA Carlstrom, JE Israel, FP Menten, KM Peterson, JB Phillips, TG Sironi, G Walker, CK BE Phillips, TG TI Plans for a 10-m submillimeter-wave telescope at the South Pole SO ADVANCED TECHNOLOGY MMW, RADIO, AND TERAHERTZ TELESCOPES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Conference on Advanced Technology MMW, Radio, and Terahertz Telescopes CY MAR 26-28, 1998 CL KONA, HI SP SPIE, European So Observ DE Antarctic; South Pole; submillimeter; astronomy; telescopes AB A 10 meter diameter submillimeter-wave telescope has been proposed for installation and scientific use at the NSF Amundsen-Scott South Pole Station. Current evidence indicates that the South Pole is the best submillimeter-wave telescope site among all existing or proposed ground-based observatories. Proposed scientific programs place stringent requirements on the optical quality of the telescope design. In particular, reduction of the thermal background and offsets requires an off-axis, unblocked aperture, and the large field of view needed for survey observations requires shaped optics. This mix of design elements is well-suited for large-scale (square degree) mapping of line and continuum radiation from submillimeter-wave sources at moderate spatial resolutions (4 to 60 arcsecond beam size) and high sensitivity (milliJansky flux density levels:). The telescope will make arcminute angular scale, high frequency Cosmic Microwave Background measurements from the best possible ground-based site, using an aperture which is larger than is currently possible on orbital or airborne platforms. The telescope design is homologous. Gravitational changes in pointing and focal length will be accommodated by active repositioning of the secondary mirror. The secondary support, consisting of a large, enclosed beam, permits mounting of either a standard set of Gregorian optics, or prime focus instrumentation packages for CMBR studies. A, tertiary chopper is located at the exit pupil of the instrument. An optical design with a hyperboloidal primary mirror and a concave secondary mirror provides a flat focal surface. The relatively large classical aberrations present in such an optical arrangement can be small compared to diffraction at submillimeter wavelengths. Effective use of this telescope will require development of large (1000 element) arrays of submillimeter detectors which are background-limited when illuminated by antenna temperatures near 50 K. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Stark, AA (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS78, Cambridge, MA 02138 USA. RI Peterson, Jeffrey/O-4794-2014 OI Peterson, Jeffrey/0000-0003-1340-818X NR 0 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2804-3 J9 P SOC PHOTO-OPT INS PY 1998 VL 3357 BP 495 EP 506 DI 10.1117/12.317383 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL55D UT WOS:000075850400051 ER PT J AU Fortunato, H AF Fortunato, H TI Reconciling observed patterns of temporal occurrence with cladistic hypotheses of phylogenetic relationship SO AMERICAN MALACOLOGICAL BULLETIN LA English DT Article DE phylogeny; fossil record; consistency; morphology; gastropods; Strombina ID CONFIDENCE-INTERVALS; STRATIGRAPHIC RANGES; FOSSIL RECORD; CHEILOSTOME BRYOZOA; EVOLUTION; RECONSTRUCTION; FORAMINIFERA; HORIZONS; CLADE AB Cladistic analyses of well-sampled groups with a complete and abundant fossil record can yield phylogenetic hypotheses that conflict with stratigraphic data, even to the extent of supporting phylogenies that appear to invert the stratigraphy. This is most probably due to the convergent evolution of similar morphologies (i. e. homoplasy), rather than the inadequacy of the fossil record. Several ways have been proposed to resolve this problem (stratophenetics, stratocladistics, character refinement, etc.). This paper proposes an iteractive technique to construct a tree more consistent with the observed fossil record by building separate phylogenies for different stratigraphic intervals which can then be assembled into a composite phylogeny. Columbellid gastropods of the genus Strombina Morch, 1852, were used to test this approach. Strombina originated and diversified in the Caribbean during the Miocene and Pliocene. During the Pliocene, they became nearly extinct in the Caribbean, but diversified in the eastern Pacific. Phylogenies of 42 species based only on shell morphology (49 characters, 186 states) yielded trees with high stratigraphic inconsistency and ghost lineages that require the presence of descendants 10 million years or more before the first appearance of their hypothesized ancestors. Removal of species that originated after the Pliocene resolved most of these stratigraphic inconsistencies although some ghost lineages remained. This Miocene/Pliocene nee was then used to root the trees illustrating the relationships among Pleistocene/Holocene species. This final composite tree is more consistent with the hypothesized fossil record for the group than the original tree. C1 Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. RP Fortunato, H (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Box 2072, Balboa, Panama. EM stri03.ancon.fortunae@ic.si.edu NR 66 TC 11 Z9 10 U1 1 U2 1 PU AMER MALACOLOGICAL SOC, INC PI WILMINGTON PA DELAWARE MUSEUM NATURAL HISTORY, BOX 3937, WILMINGTON, DE 19807-0937 USA SN 0740-2783 J9 AM MALACOL BULL JI Am. Malacol. Bull. PY 1998 VL 14 IS 2 BP 191 EP 200 PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 160RT UT WOS:000078245300013 ER PT J AU Jennions, MD AF Jennions, MD TI The effect of leg band symmetry on female-male association in zebra finches SO ANIMAL BEHAVIOUR LA English DT Article ID MALE SEXUAL ORNAMENTS; FLUCTUATING ASYMMETRY; MATE CHOICE; BEAK COLOR; SELECTION; PREFERENCE; BIRDS; TAILS; WINGS AB Studies have shown that female zebra finches, Taeniopygia guttata, prefer to associate with males wearing symmetric leg band combinations. In this study, I used a four-choice chamber apparatus to investigate this preference, and to determine whether it is influenced by band coloration. I created band combinations by banding males with four leg bands. The symmetrical combinations consisted of two bands on each leg; the asymmetrical combinations consisted of three bands on one leg and one band on the other leg. For each of the symmetry treatments, all four bands were either light green or red. Females did not spend significantly more time associating with males wearing symmetrical bands or with males wearing red bands. The duration of male-female associations was not influenced by an interaction between symmetry category and band colour treatment. None of 10 females spent the most time with males with red symmetrical bands. (C) 1998 The Association for the Study of Animal Behaviour. C1 Univ Oxford, Dept Zool, Anim Behav Res Grp, Oxford OX1 3PS, England. RP Jennions, MD (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM gam128@gamboa.si.edu RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 38 TC 26 Z9 27 U1 1 U2 4 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD JAN PY 1998 VL 55 BP 61 EP 67 DI 10.1006/anbe.1997.0579 PN 1 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA YV103 UT WOS:000071789700007 ER PT J AU Wagner, RH Schug, MD Morton, ES AF Wagner, RH Schug, MD Morton, ES TI Studying paternity and paternal care: the value of negative results SO ANIMAL BEHAVIOUR LA English DT Editorial Material ID PURPLE MARTINS; PARENTAL EFFORT; CONFIDENCE C1 York Univ, Dept Biol, N York, ON M3J 1P3, Canada. Cornell Univ, Dept Genet & Dev, Ithaca, NY 14853 USA. Smithsonian Inst, Conservat & Res Ctr, Washington, DC 20560 USA. RP Wagner, RH (reprint author), York Univ, Dept Biol, 4700 Keele St, N York, ON M3J 1P3, Canada. NR 6 TC 6 Z9 6 U1 2 U2 2 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JAN PY 1998 VL 55 BP 239 EP 240 DI 10.1006/anbe.1997.0605 PN 1 PG 2 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA YV103 UT WOS:000071789700027 ER PT J AU Labandeira, CC AF Labandeira, CC TI Early history of arthropod and vascular plant associations SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES LA English DT Review DE fossil record; Paleozoic; herbivory; detritivory; coprolites; gut contents; insects; plant-insect interactions ID REPRODUCTIVE-BIOLOGY; INSECT POLLINATION; FOSSIL RECORD; TERRESTRIAL ARTHROPODS; ANIMAL INTERACTIONS; GROUND PLAN; LEAF MINES; HERBIVORY; ANGIOSPERM; ORIGIN AB Although research on modern plant-arthropod associations is one of the cornerstones of biodiversity studies, very little of that interest has percolated down to the fossil record. Much of this neglect is attributable to dismissal of Paleozoic plant-arthropod interactions as being dominated by detritivory, with substantive herbivory not emerging until the Mesozoic. Recent examination of associations from some of the earliest terrestrial communities indicates that herbivory probably extends to the Early Devonian, in the form of spore feeding and piercing-and-sucking. External feeding on pinnule margins and the intimate and intricate association of galling are documented from the Middle and Late Pennsylvanian, respectively. During the Early Permian, the range of external foliage feeding extended to hole feeding and skeletonization and was characterized by the preferential targeting of certain seed plants. At the close of the Paleozoic, surface fluid feeding was established, but there is inconclusive evidence for mutualistic relationships between insect pollinivores and seed plants. These data are gleaned from the largely separate trace-fossil records of gut contents, coprolites, and plant damage and the body-fossil records of plant reproductive and vegetative structures, insect mouthparts, and ovipositors. While these discoveries accentuate the potential for identifying particular associations, the greatest theoretical demand is to establish the spectrum and level of intensity for the emergence of insect herbivory in a range of environments during the Pennsylvanian and Permian. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Labandeira, CC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM labandec@nmnh.si.edu NR 401 TC 133 Z9 140 U1 7 U2 42 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 1998 VL 26 BP 329 EP 377 DI 10.1146/annurev.earth.26.1.329 PG 49 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA ZQ991 UT WOS:000073923900014 ER PT J AU Wing, SL Boucher, LD AF Wing, SL Boucher, LD TI Ecological aspects of the Cretaceous flowering plant radiation SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES LA English DT Review DE angiosperms; Cretaceous; paleoecology; diversification; evolution ID EASTERN NORTH-AMERICA; CEDAR MOUNTAIN FORMATION; POTOMAC GROUP; ANGIOSPERM FLOWERS; SP-NOV; FOSSIL EVIDENCE; DICOTYLEDONOUS WOOD; WESTERN INTERIOR; NEW-JERSEY; LIVINGSTON ISLAND AB The first flowering plant fossils occur as rare, undiverse pollen grains in the Early Cretaceous (Valanginian-Hauterivian). Angiosperms diversified slowly during the Barremian-Aptian but rapidly during the Albian-Cenomanian. By the end of the Cretaceous, at least half of the living angiosperm orders were present, and angiosperms were greater than 70% of terrestrial plant species globally. The rapid diversification of the group, and its dominance in modem vegetation, has led to the idea that the Cretaceous radiation of angiosperms also represents their rise to vegetational dominance. Paleoecological data cast a different light on the Cretaceous radiation of angiosperms. Analyses of sedimentary environments indicate that angiosperms not only originated in unstable habitats but remained centered there through most of the Cretaceous. Morphology of leaves, seeds, and wood is consistent with the status of most Cretaceous angiosperms as herbs to small trees with early successional strategy. The diversification of flowering plants in the Cretaceous represents the evolution of a highly speciose clade of weeds but not necessarily a major change in global vegetation. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Wing, SL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, NHB 121, Washington, DC 20560 USA. EM wings@nmnh.si.edu; boucherl@nmnh.si.edu OI Wing, Scott/0000-0002-2954-8905 NR 163 TC 152 Z9 159 U1 0 U2 29 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 1998 VL 26 BP 379 EP 421 DI 10.1146/annurev.earth.26.1.379 PG 43 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA ZQ991 UT WOS:000073923900015 ER PT J AU Bateman, RM Crane, PR DiMichele, WA Kenrick, PR Rowe, NP Speck, T Stein, WE AF Bateman, RM Crane, PR DiMichele, WA Kenrick, PR Rowe, NP Speck, T Stein, WE TI Early evolution of land plants: Phylogeny, physiology, and ecology of the primary terrestrial radiation SO ANNUAL REVIEW OF ECOLOGY AND SYSTEMATICS LA English DT Review DE biomechanics; cladistics; evolutionary radiation; novelty radiation; paleobotany; systematics ID RNA GENE-SEQUENCES; PALEOZOIC ATMOSPHERIC CO2; EARLY VASCULAR PLANTS; RBCL SEQUENCES; FOSSIL PLANTS; MORPHOLOGICAL DISPARITY; BIOMECHANICAL ANALYSIS; CLADISTIC APPROACH; AGLAOPHYTON-MAJOR; SEED PLANTS AB The Siluro-Devonian primary radiation of land biotas is the terrestrial equivalent of the much-debated Cambrian "explosion" of marine faunas. Both show the hallmarks of novelty radiations (phenotypic diversity increases much more rapidly than species diversity across an ecologically undersaturated and thus low-competition landscape), and both ended with the formation of evolutionary and ecological frameworks analogous to those of modem ecosystems. Profound improvements in understanding early land plant evolution reflect recent liberations from several research constraints: Cladistic techniques plus DNA sequence data from extant relatives have prompted revolutionary reinterpretations of land plant phylogeny, and thus of systematics and character-state acquisition patterns. Biomechanical and physiological experimental techniques developed for extant plants have been extrapolated to fossil species, with interpretations both aided and complicated by the recent knowledge that global landmass positions, currents, climates, and atmospheric compositions have been profoundly variable (and thus nonuniformitarian) through the Phanerozoic. Combining phylogenetic and paleoecological data offers potential insights into the identity and function of key innovations, though current evidence suggests the importance of accumulating within lineages a critical mass of phenotypic character. Challenges to further progress include the lack of sequence data and paucity of phenotypic features among the early land plant clades, and a fossil record still inadequate to date accurately certain crucial evolutionary and ecological events. C1 Royal Bot Gardens, Edinburgh EH3 5LR, Midlothian, Scotland. Field Museum Nat Hist, Dept Geol, Chicago, IL 60605 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol, Washington, DC 20560 USA. Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. Univ Montpellier 2, Lab Paleobot, Inst Sci Evolut, UMR 5554 CNRS, F-34095 Montpellier 05, France. Univ Freiburg, D-79104 Freiburg, Germany. SUNY Binghamton, Dept Biol Sci, Binghamton, NY 13902 USA. RP Bateman, RM (reprint author), Royal Bot Gardens, 20A Inverleith Row, Edinburgh EH3 5LR, Midlothian, Scotland. EM r.bateman@rbge.org.uk RI DiMichele, William/K-4301-2012; Speck, Thomas/N-9208-2013 NR 141 TC 163 Z9 173 U1 13 U2 64 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 1998 VL 29 BP 263 EP 292 DI 10.1146/annurev.ecolsys.29.1.263 PG 30 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 150DQ UT WOS:000077648200010 ER PT J AU Snyder, LM AF Snyder, LM TI A history of dogs in the early Americas SO ARCHAEOLOGY LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Snyder, LM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 USA SN 0003-8113 J9 ARCHAEOLOGY JI Archaeology PD JAN-FEB PY 1998 VL 51 IS 1 BP 70 EP + PG 7 WC Archaeology SC Archaeology GA YP195 UT WOS:000071252100031 ER PT J AU Snyder, LM AF Snyder, LM TI The lost history of the canine race SO ARCHAEOLOGY LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Snyder, LM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 USA SN 0003-8113 J9 ARCHAEOLOGY JI Archaeology PD JAN-FEB PY 1998 VL 51 IS 1 BP 70 EP + PG 7 WC Archaeology SC Archaeology GA YP195 UT WOS:000071252100030 ER PT J AU Zilczer, JK AF Zilczer, JK TI Raymond Duchamp-Villon and the American avant-garde (Sculptor, architectural designer, and activist in the modernist cause, 1876-1918) SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. NR 41 TC 1 Z9 1 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 1998 VL 38 IS 1-2 BP 14 EP 27 PG 14 WC Art SC Art GA 499LA UT WOS:000172571600002 ER PT J AU Fern, A AF Fern, A TI N.C. Wyeth: A biography SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 1998 VL 38 IS 1-2 BP 46 EP 48 PG 3 WC Art SC Art GA 499LA UT WOS:000172571600005 ER PT J AU Mann, DH Crowell, AL Hamilton, TD Finney, BP AF Mann, DH Crowell, AL Hamilton, TD Finney, BP TI Holocene geologic and climatic history around the Gulf of Alaska SO ARCTIC ANTHROPOLOGY LA English DT Article; Proceedings Paper CT International Seminar on the Origins, Development, and Spread of Prehistoric North Pacific-Bering Sea Maritime Cultures CY JUN 02-08, 1993 CL TOKAI UNIV, HONOLULU, HAWAII SP Natl Sci Fdn, Int Div, Japan Soc Promot Sci HO TOKAI UNIV ID QUATERNARY VEGETATION HISTORY; QUEEN-CHARLOTTE-ISLANDS; ST-AUGUSTINE VOLCANO; MEDIEVAL WARM PERIOD; SOUTH-CENTRAL ALASKA; NORTH PACIFIC COAST; SEA-LEVEL RECORD; BRITISH-COLUMBIA; GLACIER FLUCTUATIONS; SOUTHEASTERN ALASKA AB Though not as dramatic as during the last Ice Age, pronounced climatic changes occurred in the northeastern Pacific over the last 10,000 years. Summers warmer and drier than today's accompanied a Hypsithermal interval between 9 and 6 ka. Subsequent Neoglaciation was marked by glacier expansion after 5-6 ka and the assembly of modern-type plant communities by 3-4 ka. The Neoglacial interval contained alternating cold and warm intervals, each lasting several hundred years to one millennium, and including both the Medieval Warm Period (ca. AD 900-1350) and the Little Ice Age (ca. AD 1350-1900). Salmon abundance fluctuated during the Little Ice Age in response to local glaciation and probably also to changes in the intensity of the Aleutian Low. Although poorly understood at present, climate fluctuations at all time scales were intimately connected with oceanographic changes in the North Pacific Ocean. The Gulf of Alaska region is tectonically highly active, resulting in a history of frequent geological catastrophes during the Holocene. Twelve to 14 major volcanic eruptions occurred since 12 ka. At intervals of 20-100 years, large earthquakes have raised and lowered sea level instantaneously by meters and generated destructive tsunamis. Sea level has often varied markedly between sites only 50-100 km apart due to tectonism and the isostatic effects of glacier fluctuations. C1 Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. Smithsonian Inst, Arctic Studies Ctr, Anchorage, AK 99501 USA. US Geol Survey, Anchorage, AK 99508 USA. Univ Alaska, Inst Marine Sci, Fairbanks, AK 99775 USA. RP Mann, DH (reprint author), Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. NR 96 TC 30 Z9 31 U1 0 U2 7 PU UNIV WISCONSIN PRESS PI MADISON PA JOURNAL DIVISION, 2537 DANIELS ST, MADISON, WI 53718 USA SN 0066-6939 J9 ARCTIC ANTHROPOL JI Arct. Anthropol. PY 1998 VL 35 IS 1 BP 112 EP 131 PG 20 WC Anthropology SC Anthropology GA 150ZP UT WOS:000077696700008 ER PT J AU Fitzhugh, WW Golovnev, AV AF Fitzhugh, WW Golovnev, AV TI The Drovyanoy 3 shaman's cache: Archaeology, ethnography, and "Living Yamal" SO ARCTIC ANTHROPOLOGY LA English DT Article ID NORTH AB This paper presents field data and interpretations from a 1994 archaeological find at Cape Drovyanoy in northeastern Yamal, Western Siberia, that documents a unique aspect of Yamal Nenets spiritual life. A cache of shaman's equipment dating to the late 1930s provides evidence for religious traditions that are fast disappearing. In the future, many of these traditions may only be studied archaeologically. Archaeological data on religious caches and offerings, as at the Ust'Poluy site and the Sirt'ye Sale and Bolvanskii Nos sites, are rare. The present study also illustrates the importance of ethnological and archaeological collaboration and discusses ethical issues faced by field researchers who must sometimes make decisions in the field without Native consultation. C1 Smithsonian Inst, Dept Anthropol, Arctic Studies Ctr, Washington, DC 20560 USA. Inst Hist & Archaeol, Ethnog Dept, Urals Branch, Ekaterinburg, Russia. RP Fitzhugh, WW (reprint author), Smithsonian Inst, Dept Anthropol, Arctic Studies Ctr, Washington, DC 20560 USA. RI Golovnev, Andrei/F-6385-2016 OI Golovnev, Andrei/0000-0002-5716-655X NR 57 TC 1 Z9 1 U1 2 U2 13 PU UNIV WISCONSIN PRESS PI MADISON PA JOURNAL DIVISION, 2537 DANIELS ST, MADISON, WI 53718 USA SN 0066-6939 J9 ARCTIC ANTHROPOL JI Arct. Anthropol. PY 1998 VL 35 IS 2 BP 177 EP 198 PG 22 WC Anthropology SC Anthropology GA 203VC UT WOS:000080727700016 ER PT J AU Krupnik, I AF Krupnik, I TI Jesup genealogy: Intellectual partnership and Russian-American cooperation in Arctic North Pacific anthropology Part I. From the Jesup expedition to the Cold War, 1897-1948 SO ARCTIC ANTHROPOLOGY LA English DT Review AB This paper covers the first five decades in the development of a common intellectual legacy and the tradition of Russian-American partnership established by the Jesup North Pacific Expedition, 1897-1902. The senior members of the Jesup team on both sides were Very active in promoting the key Jesup paradigms of trans-Pacific cultural connections and diffusions, in advancing international contacts and research exchanges, and in training the next generation of scholars. The tradition, however, was abandoned by younger students, and suffered from the political turmoils of the century and the physical destruction of much of the Siberian ethnography in Russia. The original Jesup legacy was quickly replaced by another variety that featured Eskimo archaeology and the early prehistory of Beringia. The entire post-Jesup story thus reads as a textbook case of the "reinvention of tradition." The legacy enshrined by the founding group was finally reestablished by the fourth generation with no direct exposure to the original creed. C1 Natl Museum Nat Hist, Smithsonian Inst, Arctic Studies Ctr, Washington, DC 20560 USA. RP Krupnik, I (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Arctic Studies Ctr, Washington, DC 20560 USA. NR 270 TC 3 Z9 4 U1 1 U2 3 PU UNIV WISCONSIN PRESS PI MADISON PA JOURNAL DIVISION, 2537 DANIELS ST, MADISON, WI 53718 USA SN 0066-6939 J9 ARCTIC ANTHROPOL JI Arct. Anthropol. PY 1998 VL 35 IS 2 BP 199 EP 226 PG 28 WC Anthropology SC Anthropology GA 203VC UT WOS:000080727700017 ER PT B AU Dallmeier, F AF Dallmeier, F BE Bachmann, P Kohl, M Paivinen, R TI Measuring and monitoring forest biodiversity: The SI/MAB model SO ASSESSMENT OF BIODIVERSITY FOR IMPROVED FOREST PLANNING SE FORESTRY SCIENCES LA English DT Proceedings Paper CT Conference on Assessment of Biodiversity for Improved Planning CY OCT 07-11, 1996 CL MONTE VERITA, SWITZERLAND SP European Forest Inst, Joensuu, Swiss Fed Inst Technol, Zurich, Swiss Fed Inst Forest Snow & Landscape Res, Birmensdorf AB Over the past decade, the Smithsonian Institution/Man and the Biosphere Biological Diversity Program (SI/MAB) has developed a biodiversity monitoring protocol and refined it through testing at a number of sites. The protocol has been adopted by SI/MAB colleagues and partners around the world, forming the basis for consistent measuring and monitoring at hundreds of biodiversity monitoring plots, facilitating the transfer of comparable data, and providing the framework for data analysis and dissemination to users. Program staff have trained more than 700 participants in the SI/MAB protocol and in use of BioMon (SI/MAB's computerized data management system) at annual six-week international courses and through on-site two-week courses in more than two dozen countries. Staff have also been instrumental in setting up and maintaining international biodiversity information exchange networks. The primary goals of the program - to gather, analyse, and disseminate information about biodiversity at selected forested sites throughout the world and to foster co-operation among researchers and decision-makers - are being met. The outlook for strengthening established networks and expanding the program into new areas is bright. C1 Smithsonian Inst, SIMAB Biodivers Program, Washington, DC 20560 USA. RP Dallmeier, F (reprint author), Smithsonian Inst, SIMAB Biodivers Program, 1100 Jefferson Dr SW,Suite 3123, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-4872-9 J9 FOR SCI PY 1998 VL 51 IS 18 BP 15 EP 29 PG 15 WC Forestry SC Forestry GA BL25C UT WOS:000074895600002 ER PT B AU Mink, DJ Kurtz, MJ AF Mink, DJ Kurtz, MJ BE Albrecht, R Hook, RN Bushouse, HA TI RVSAO 2.0 - A radial velocity package for IRAF SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB RVSAO 2.0 is the latest release of a package for calculating apparent radial velocities of celestial objects from observed spectral shifts. There are two main tasks in the package, XCSAO and EMSAO. XCSAO cross-correlates the Fourier transform of an object's spectrum against the transforms of a set of template spectra with known spectral shifts to obtain a velocity and error. EMSAO finds emission lines in a spectrum and computes the observed centers, getting individual shifts and errors for each line as well as a single velocity combining all of the lines. Three tasks which are new in this release are SUMSPEC, which combines spectra after shifting them all to a specified redshift, LINESPEC, which creates a spectrum at a specified redshift from a list of rest wavelengths, and BCVCORR, which computes the correction needed to translate the observed radial velocity to one relative to the solar system barycenter. Full documentation of this software, including numerous examples of its use, is on-line at http://tdc-www.harvard.edu/iraf/rvsao/. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Mink, DJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI KURTZ, Michael /B-3890-2009 NR 0 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 93 EP 96 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000021 ER PT B AU Wang, Z AF Wang, Z BE Albrecht, R Hook, RN Bushouse, HA TI Packaging radio sub-millimeter spectral data in FITS SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB We report on an experiment to incorporate the multiple extension FITS file format in building data processing software for spectroscopic observations in radio and millimeter-submillimeter wavelengths. By packaging spectral header information into table extensions and the actual spectral data into either table or image extensions, this approach provides a convenient and effective way to organize large amount of spectroscopic data, especially for pipeline-like processing tasks. Tests conducted based on a software package developed for the SWAS mission have demonstrated this to be a viable alternative to the conventional ways of organizing spectral data at these wavelengths. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wang, Z (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 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 125 EP 128 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000029 ER PT B AU Mandel, E Murray, SS AF Mandel, E Murray, SS BE Albrecht, R Hook, RN Bushouse, HA TI Other people's software SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB Why do we continually re-invent the astronomical software wheel? Why is it so difficult to use "other people's software"? Leaving aside issues such as money, power, and control, we need to investigate practically how we can remove barriers to software sharing. This paper will offer a starting point for software cooperation, centered on the concept of "minimal software buy-in". C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Mandel, E (reprint author), Smithsonian Astrophys Observ, 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 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 142 EP 145 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000033 ER PT B AU Conroy, M Mandel, E Roll, J AF Conroy, M Mandel, E Roll, J BE Albrecht, R Hook, RN Bushouse, HA TI Building software from heterogeneous environments SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB The past decade has witnessed a movement within the astronomical software community towards Open Systems. This trend has allowed projects and users to build customized processing systems from existing components. We present examples of user-customizable systems that can be built from existing tools, based on commonly-used infrastructure: a parameter interface library, FITS file format, Unix, and the X Windows environment. With these common tools, it is possible to produce customized analysis systems and automated reduction pipelines. C1 Smithsonian Astrophys Observ, Cambridge, MA 01801 USA. RP Conroy, M (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 01801 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 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 150 EP 153 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000035 ER PT B AU Doe, S Ljungberg, M Siemiginowska, A Joye, W AF Doe, S Ljungberg, M Siemiginowska, A Joye, W BE Albrecht, R Hook, RN Bushouse, HA TI Fitting and modeling of AXAF data with the ASC fitting application SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB The AXAF mission will provide X-ray data with unprecedented spatial and spectral resolution. Because of the high quality of these data, the AXAF Science Center will provide a new data analysis system-including a new fitting application. Our intent is to enable users to do fitting that is too awkward with, or beyond, the scope of existing astronomical fitting software. Our main goals are: 1) to take advantage of the full capabilities of the AXAF, we intend to provide a more sophisticated modeling capability (i.e., models that are f(x, y, E, t), models to simulate the response of AXAF instruments, and models that enable "joint-mode" fitting, i.e., combined spatial-spectral or spectral-temporal fitting); and 2) to provide users with a wide variety of models, optimization methods, and fit statistics. In this paper, we discuss the use of an object-oriented approach in our implementation, the current features of the fitting application, and the features scheduled to be added in the coming year of development. Current features include: an interactive, command-line interface; a modeling language, which allows users to build models from arithmetic combinations of base functions; a suite of optimization and fit statistics; the ability to perform fits to multiple data sets simultaneously; and, an interface with SM and SAOtng to plot or image data, models, and/or residuals from a fit. We currently provide a modeling capability in one of two dimensions, and have recently made an effort to perform spectral fitting in a manner similar to XSPEC. We also allow users to dynamically link the fitting application to their own algorithms. Our goals for the coming year include incorporating the XSPEC model library as a subset of models available in the application, enabling "joint-mode" analysis and adding support for new algorithms. C1 Smithsonian Astrophys Observ, AXAF Sci Ctr, Cambridge, MA 02138 USA. RP Doe, S (reprint author), Smithsonian Astrophys Observ, AXAF Sci Ctr, MS 81,60 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 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 157 EP 160 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000036 ER PT B AU He, H McDowell, J Conroy, M AF He, H McDowell, J Conroy, M BE Albrecht, R Hook, RN Bushouse, HA TI ASC coordinate transformation - The Pixlib library, II SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB Pixlib, an AXAF Science Center (ASC) coordinate library, has been developed as the continuing effort of (He 1997). Its expansion includes, handling of the High Resolution Mirror Assembly (HRMA) X-ray Detection System (HXDS) stage dither and the five-axis mount (FAM) attachment point movements, correction of misalignments of the mirror mount relative to X-ray calibration facility (XRCF) and to the default FAM axes, as well as solution of sky aspect offsets of flight, etc. In this paper, we will discuss the design and the configuration of the pixlib system, and show, as an example, how to integrate the library into ASC data analysis at XRCF. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP He, H (reprint author), Harvard Smithsonian Ctr Astrophys, 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 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 208 EP 211 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000049 ER PT B AU Eichhorn, G Accomazzi, A Grant, CS Kurtz, MJ Murray, SS AF Eichhorn, G Accomazzi, A Grant, CS Kurtz, MJ Murray, SS BE Albrecht, R Hook, RN Bushouse, HA TI New capabilities of the ADS abstract and article service SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB The ADS abstract service at: http://adssvww.harvard.edu has been updated considerably in the last year. New capabilities in the search engine include searching for multi-word phrases and searching for various logical combinations of search terms. Through optimization of the custom built search software, the search times were decreased by a factor of 4 in the last year. The WWW interface now uses WWW cookies to store and retrieve individual user preferences. This allows our users to set preferences for printing, accessing mirror sites, fonts, colors, etc. Information about most recently accessed references allows customized retrieval of the most recent unread volume of selected journals. The information stored in these preferences is kept completely confidential and is not used for any other purposes. Two mirror sites (at the CDS in Strasbourg, France and at NAO in Tokyo, Japan) provide faster access for our European and Asian users. To include new information in the ADS as fast as possible, new indexing and search software was developed to allow updating the index data files within minutes of receipt of time critical information (e.g., IAU Circulars which report on supernova and comet discoveries). The ADS is currently used by over 10,000 users per month, which retrieve over 4.5 million references and over 250,000 full article pages each month. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Eichhorn, G (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 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 378 EP 381 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000088 ER PT B AU Zografou, P Chary, S DuPrie, K Estes, A Harbo, P Pak, K AF Zografou, P Chary, S DuPrie, K Estes, A Harbo, P Pak, K BE Albrecht, R Hook, RN Bushouse, HA TI The ASC data archive for the AXAF ground calibration SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB A data archive is near completion at the ASC to store and provide access to AXAF data. The archive is a distributed Client/Server system. It consists of a number of different servers which handle flat data files, relational data, replication across multiple sites and the interface to the WWW. There is a 4GL client interface for each type of data server, C++ and Java API and a number of standard clients to archive and retrieve data. The architecture is scalable and configurable in order to accommodate future data types and increasing data volumes. The first release of the system became available in August 1996 and has been successfully operated since then in support of the AXAF calibration at MSFC. This paper presents the overall archive architecture and the design of client and server components as it was used during ground calibration. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Zografou, P (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 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 391 EP 394 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000091 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 Albrecht, R Hook, RN Bushouse, HA TI Mirroring the ADS bibliographic databases SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB During the past year the Astrophysics Data System has set up two mirror sites for the benefit of users around the world with a slow network connection to the main ADS server in Cambridge, MA. In order to clone the ADS abstract and article services on the mirror sites, the structure of the bibliographic databases, query forms and search scripts has been made both site- and platform-independent by creating a set of configuration parameters that define the characteristics of each mirror site and by modifying the database management software to use such parameters. Regular updates to the databases are performed on the main ADS server and then mirrored on the remote sites using a modular set of scripts capable of performing both incremental and full updates. The use of software packages capable of authentication, as well as data compression and encryption, permits secure and fast data transfers over the network, making it possible to run the mirroring procedures in an unsupervised fashion. 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 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 395 EP 399 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000092 ER PT B AU Chary, S Zografou, P AF Chary, S Zografou, P BE Albrecht, R Hook, RN Bushouse, HA TI Search and retrieval of the AXAF data archive on the Web using Java SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB An important component of the AXAF Data Archive is the interface through the WWW. Internet applications are moving beyond delivering static content to more complex dynamic content and transaction processing. While HTML and CGI based interfaces have been possible for some time, it was not until the advent of JDBC (Java(1) Database Connectivity) that a uniform and powerful interface to the different types of servers in the archive, with secure access to proprietary data, could become a reality. This paper presents a multi-tier architecture which integrates the data servers, Web server and a HTTP/JDBC gateway and enables data on any of the data servers in the AXAF archive to be available to clients using a Web browser. This Web-based solution to data browsing is currently available for the contents of the AXAF observing catalog and other catalogs in the archive. A Java API for other database applications to access the data is presented. Performance issues and security limitations and workarounds are discussed. C1 Smithsonian Astrophys Observ, AXAF Sci Ctr, Cambridge, MA 02138 USA. RP Chary, S (reprint author), Smithsonian Astrophys Observ, AXAF Sci Ctr, 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 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 408 EP 411 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000095 ER PT B AU Kurtz, MJ Eichhorn, G Accomazzi, A Grant, C Murray, SS AF Kurtz, MJ Eichhorn, G Accomazzi, A Grant, C Murray, SS BE Albrecht, R Hook, RN Bushouse, HA TI Keeping bibliographies using ADS SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB Nearly every working astronomer now uses the NASA Astrophysics Data System Abstract Service regularly to access the technical literature. Several advanced features of the system are not very well used, but could be quite useful. Here we describe one of them. Astronomers can use the ADS to maintain their publication lists; a simple http link can bring a current bibliography at any time. In this paper we show how to form the link, how to include papers which ADS does not currently have, and how to deal with name changes. The ADS can be reached at: http://adswww.harvard.edu/. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kurtz, MJ (reprint author), Smithsonian Astrophys Observ, 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 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 478 EP 480 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000110 ER PT B AU Nguyen, D DuPrie, K Zografou, P AF Nguyen, D DuPrie, K Zografou, P BE Albrecht, R Hook, RN Bushouse, HA TI A multidimensional binary search tree for star catalog correlations SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS VII (ADASS) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 1997 Conference of the Astronomical Data Analysis Software and Systems (ADASS) CY SEP 14-17, 1997 CL SONTHOFEN, GERMANY SP European So Observ, European Space Agcy, Space Telescope European Coordinating Facil, Space Telescope Sci Inst, Natl Radio Astron Observ, Sun Microsyst Detuschland, CREASO, Sybase Serv, Pink Aviat Serv AB A multi-dimensional binary search tree, k-d tree, is proposed to support range queries in multi-key data sets. The algorithm can been used to solve a near neighbors problem for objects in a 19 million entries star catalog, and can be used to locate radio sources in cluster candidates for the X-ray/SZ Hubble constant measurement technique. Objects are correlated by proximity in a RA-Dec range and by magnitude. Both RA and Dec have errors that must be taken into account. This paper will present the k-d tree design and its application to the star catalog problem. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Nguyen, D (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-65-1 J9 ASTR SOC P PY 1998 VL 145 BP 485 EP 487 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74V UT WOS:000076551000112 ER PT S AU Carleton, NP Traub, WA Angel, JRP AF Carleton, NP Traub, WA Angel, JRP BE Reasenberg, RD TI Interferometric capability for the Magellan Project SO ASTRONOMICAL INTERFEROMETRY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Conference on Astronomical Interferometry CY MAR 20-24, 1998 CL KONA, HI SP SPIE, European So Observ DE interferometry; telescopes; infrared; high-resolution AB The Magellan Project is building two 6.5-m telescopes, 60 m apart, at the Las Campanas Observatory in Chile. There are ongoing plans to combine the beams of the two main telescopes, and of smaller auxiliary telescopes, for interferometric measurements. In this paper we consider the array of auxiliary telescopes as a stand-alone instrument, recognizing that it will operate as such for some large fraction of the time. Our interest is sharpened by the availability of six 1.8-m optical systems (mirrors and cells), retired from the Smithsonian-Arizona Multiple-Mirror Telescope in preparation for the installation of a single-mirror 6.5-m system. We have completed a design for a 1.8-m telescope, in which the MMT components are supported on a proven tripod mount. The optics-support structure uses steel for stiffness, and low-thermal-expansion rods for passive stability. This array will be a powerful tool for the investigation of stellar limb darkening, surface features, and changes of diameter in pulsations, as well as dust disks, shells. and binary companions. The 1.8-m telescopes on good sites such as Magellan's should be able to operate at full aperture for interferometry at 2.2 mu m. They should therefore be able to reach to magnitude K=10 or so, and thus to cover substantial samples of both main-sequence and pre-main-sequence stars, and of fully evolved stars as well. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Carleton, NP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2797-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3350 BP 733 EP 735 DI 10.1117/12.317139 PN 1-2 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics; Optics SC Engineering; Astronomy & Astrophysics; Optics GA BL55C UT WOS:000075850300081 ER PT S AU Traub, WA AF Traub, WA BE Reasenberg, RD TI Recent results from the IOTA interferometer SO ASTRONOMICAL INTERFEROMETRY, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Conference on Astronomical Interferometry CY MAR 20-24, 1998 CL KONA, HI SP SPIE, European So Observ DE interferometry; telescopes; visible; infrared; single-mode fibers AB The IOTA interferometer has been ill scheduled operation since 1995 with two 0.45 m telescopes, and baselines of up to 38 m; a third telescope will be installed in 1998 and three-beam combination will be implemented in 1999. We currently have three major detection systems, built around a CCD, a NICMOS3, and the FLUOR fiber beam combiner. A piezo-driven rapid scan delay is also available. Our experience in using these systems is reviewed here. and the corresponding magnitude limits of fringe measurements in the V, R, I, J, H, K bands are discussed. Recent results from these new detector systems include measurements of stellar diameters and temperatures, stellar surface features, and circumstellar dust emission. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Traub, WA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 29 Z9 29 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2797-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3350 BP 848 EP 855 DI 10.1117/12.317152 PN 1-2 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Optics SC Engineering; Astronomy & Astrophysics; Optics GA BL55C UT WOS:000075850300094 ER PT J AU Barmby, P Huchra, JP AF Barmby, P Huchra, JP TI Kinematics of the Hercules supercluster SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology, observations; dark matter; galaxies, clusters, individual (Hercules) ID SURFACE-BRIGHTNESS GALAXIES; AUTOMATED PLATE SCANNER; PALOMAR SKY SURVEY; RICH CLUSTERS; X-RAY; ABELL CLUSTERS; VELOCITY DISPERSIONS; SPIRAL GALAXIES; REDSHIFT SURVEY; DENSE CLUSTERS AB The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the KMM mixture-modeling algorithm to separate the galaxies into clusters: we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 82(-55)(+68) and 715(-61)(+81) km s(-1), respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, & Huchra and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6 +/- 2.0) x 10(15) hi Mo; with the supercluster luminosity, (1.4 +/- 0.2) x 10(13) h(-2) L-circle dot, this yields Omega approximate to 0.34 + 0.1. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 91 TC 35 Z9 35 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JAN PY 1998 VL 115 IS 1 BP 6 EP 25 DI 10.1086/300179 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ454 UT WOS:000071389200003 ER PT J AU Conner, SR Cooray, AR Fletcher, AB Burke, BF Lehar, J Garnavich, PM Muxlow, TWB Thomasson, P Blakeslee, JP AF Conner, SR Cooray, AR Fletcher, AB Burke, BF Lehar, J Garnavich, PM Muxlow, TWB Thomasson, P Blakeslee, JP TI Ringlike structure in the radio lobe of MG 0248+0641 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, individual (MG 0248+0641); galaxies, jets ID ACTIVE GALACTIC NUCLEI; GRAVITATIONAL LENS; EINSTEIN RING; GALAXIES; POLARIZATION; CANDIDATE; CLUSTERS; EMISSION; BUBBLES; ORIGIN AB We present radio and optical observations of MG 0248 + 0641, which contains a kiloparsec-scale ringlike structure in one of its radio lobes. The radio observations show a typical core-double morphology: a central core between two lobes, each of which has a hot spot. The western radio lobe appears as a nearly continuous ring, with linear polarization electric field vectors that are oriented in a radial direction from the ring's center. We consider several different interpretations for the nature of this ring, including gravitational lensing of a normal jet by a foreground galaxy. Even though simple lensing models can describe the ring morphology reasonably well, the high linear polarization seen around the ring cannot be easily explained, and no lensing object has yet been found in deep optical and infrared searches within the extent of the ring. If the radio ring is indeed caused by gravitational lensing, the implied mass-to-light ratio is typical of the very high values seen in other candidate "dark" gravitational lenses. The chance interposition of a Galactic supernova remnant, nova, planetary nebula, or H II region has been ruled out. The highly polarized ring of MG 0248+0641 is much like the prominent ring seen in 3C 219 and the multiple ones in 3C 310 and Hercules A, suggesting that similar physical processes are producing shell structures in these radio galaxies. The ring in MG 0248 + 0641 may be caused by the formation of "bubbles" as a result of instabilities in the energy flow down the western radio jet. It may also be possible that the required instabilities are triggered by the infall of gas, via tidal interaction of the central source with a nearby galaxy. This scenario may be indicated by our marginal detection of an optical source close to the western hot spot. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Manchester, Nuffield Radio Astron Labs, Jodrell Bank, Macclesfield SK11 9DL, Cheshire, England. CALTECH, Palomar Observ, Pasadena, CA 91125 USA. RP Conner, SR (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. OI Muxlow, Thomas/0000-0001-5797-8796 NR 37 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 1998 VL 115 IS 1 BP 37 EP 48 DI 10.1086/300182 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ454 UT WOS:000071389200005 ER PT J AU Kissler-Patig, M Brodie, JP Schroder, LL Forbes, DA Grillmair, CJ Huchra, JP AF Kissler-Patig, M Brodie, JP Schroder, LL Forbes, DA Grillmair, CJ Huchra, JP TI Keck spectroscopy of globular clusters around NGC 1399 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies, individual (NGC 1399); galaxies, star clusters; globular clusters, general ID ELLIPTIC GALAXIES; METALLICITY; SYSTEMS; DYNAMICS; M87; PHOTOMETRY; KINEMATICS; NGC-1399; VELOCITY; MASSES AB We report moderate-resolution, high signal-to-noise ratio spectroscopy of globular clusters around NGC 1399, the central cD galaxy in the Fornax Cluster. We address issues as diverse as elemental abundances of globular clusters versus stellar populations in elliptical galaxies, blue horizontal branches in metal-rich globular clusters, broadband colors as metallicity tracers, possible overestimation of the age-metallicity degeneracy in globular clusters, and dark matter in the halo of NGC 1399. We obtained spectra for 21 globular cluster candidates with multislit spectroscopy using the Low Resolution Imaging Spectrograph on the Keek I Telescope. Our sample turned out to include 18 globular clusters, one star, and two low-redshift late-type galaxies (z similar or equal to 0.3). The mean velocity of our globular cluster sample is 1293 +/- 71 km s(-1), and its velocity dispersion is 302 +/- 51 km s(-1). Both are slightly lower than, but in agreement with, previously derived values. We derive a mass of (1-5) x 10(12) M-circle dot within 28 kpc for the galaxy, and an M/L-B ratio of 36 +/- 20 or 76 +/- 40 M-circle dot/L-circle dot(B), depending on the mass estimator. Both estimates indicate that dark matter dominates the potential at 6r(eff). The derived elemental abundances for the globular clusters span the entire range observed in the Milky Way and M31, with a mean metallicity of our sample around [Fe/H] similar or equal to -0.8 dex. This implies that the two major subpopulations reported from photometry could have formed by the same processes that formed halo and disk/bulge globular clusters in the Local Group spiral galaxies. Two globular clusters, which we associate with a group of very red globular clusters, representing about 5% of the total system, clearly stand out and exhibit metal abundances as high as those observed for stellar populations in giant elliptical galaxies. In addition, they display surprisingly high H beta and H gamma indices that are not explained by any age/metallicity combination of existing models. The high Mg and H beta values in these clusters could, however, be explained by the presence of blue horizontal branches. Finally, we find that V-I and metallicity are well correlated in the globular cluster system, but also that the slope of the relation is twice as flat at high metallicities as an extrapolation from the relation for Milky Way globular clusters. This implies that the mean metallicities of globular cluster systems in elliptical galaxies are lower, and cover a smaller range, than ones previously derived from broadband V-I colors. C1 Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. EM mkissler@ucolick.org; brodie@ucolick.org; linda@ucolick.org; forbes@star.sr.bham.ac.uk; carl@bb1.jpl.nasa.gov; huchra@fang.harvard.edu NR 61 TC 133 Z9 133 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JAN PY 1998 VL 115 IS 1 BP 105 EP 120 DI 10.1086/300186 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ454 UT WOS:000071389200010 ER PT J AU Wilner, DJ Reynolds, SP Moffett, DA AF Wilner, DJ Reynolds, SP Moffett, DA TI CO observations toward the supernova remnant 3C 391 SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM, individual (3C 391); ISM, molecules; supernova remnants ID MOLECULAR CLOUDS; H-I; GALAXY; IC-443; 3C-391; SHOCK AB We present observations of CO J = 1-0 emission toward 3C 391, a supernova remnant whose radio continuum and X-ray emission suggest evolution near a strong density gradient in the surrounding medium. The CO maps reveal that the remnant is located at the edge of a molecular cloud, and the CO emission shows a striking correspondence with the "breakout" morphology of the remnant traced by radio continuum emission. These data support the idea that the progenitor star exploded within a dense molecular cloud and that the supernova blast wave has now broken out through the cloud boundary. Bright radio emission coincident with strong CO emission suggests that the blast wave accelerates electrons to energies of at least 20 GeV, even as it moves into dense neutral material. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 45 Z9 45 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 1998 VL 115 IS 1 BP 247 EP 251 DI 10.1086/300190 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ454 UT WOS:000071389200022 ER PT J AU Kenyon, SJ Lada, EA Barsony, M AF Kenyon, SJ Lada, EA Barsony, M TI The near-infrared extinction law and limits on the pre-main-sequence population of the rho Ophiuchi dark cloud SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared radiation; ISM, general; stars, formation ID YOUNG STELLAR OBJECTS; INTERSTELLAR EXTINCTION; MOLECULAR CLOUD; ULTRAVIOLET EXTINCTION; MILKY-WAY; STARS; (CO)-C-13; SYSTEMS; TAURUS; DUST AB We describe new techniques to measure the near-infrared extinction law and to place limits on the pre-main-sequence stellar population of a dark cloud. We analyze JHK imaging data for the central 1 deg(2) of the rho Ophiuchi cloud core and show that nearly all stars projected onto regions of low CS intensity, I-CS less than or equal to 10 K km s(-1), are background stars. Most sources at larger CS intensities lie within cloud material. We use the background stars to derive the slope of the near-IR extinction law, EJ-H/EH-K = 1.57 +/- 0.03. This result is consistent with previous extinction laws but has a factor of 2-3 smaller uncertainty. The new rho Oph extinction law yields strong constraints on the number of previously undiscovered pre-main-sequence stars in the cloud, 46 +/- 11, and the number of previously undiscovered young stars with near-IR excesses, 15 +/- 4. Neither limit exceeds the number of known pre-mainsequence stars in the cloud, similar to 100. Thus, current samples of pre-main-sequence stars ale reasonably complete for K less than or equal to 14. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Gainesville, FL 32608 USA. Univ Calif Riverside, Dept Phys, Riverside, CA 92521 USA. RP Kenyon, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; lada@astro.ufl.edu; fun@nusun.ucr.edu OI Kenyon, Scott/0000-0003-0214-609X NR 61 TC 59 Z9 60 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 1998 VL 115 IS 1 BP 252 EP 262 DI 10.1086/300188 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ454 UT WOS:000071389200023 ER PT J AU Christian, DJ Drake, JJ Mathioudakis, M AF Christian, DJ Drake, JJ Mathioudakis, M TI Extreme Ultraviolet Explorer Right Angle Program observations of cool stars SO ASTRONOMICAL JOURNAL LA English DT Article DE stars, late-type; ultraviolet emission ID SKY SURVEY OBSERVATIONS; HYADES CLUSTER; MAGNETIC-STRUCTURE; STELLAR CORONAE; EMISSION; REGION; EXOSAT AB The Extreme Ultraviolet Explorer (EUVE) Right Angle Program (RAP) obtains photometric data in four bands centered at similar to 100 Angstrom (Lexan/B), similar to 200 Angstrom (Al/Ti/C), similar to 400 Angstrom (Ti/Sb/Al), and similar to 550 Angstrom (Sn/SiO) during pointed spectroscopic observations. RAP observations are up to 20 times more sensitive than those in the EUVE all-sky survey. We present RAP observations of two dozen late-type stars: ED +03 degrees 301, ED +05 degrees 300, HR 1262, ED +23 degrees 635, ED +22 degrees 669, Melotte 25 VB 334, Melotte 25 1366, Melotte 25 59, Melotte 25 65, theta(1) Tau, V834 Tau, GJ 2037, BE -21 degrees 1074, GJ 205, RE J0532-030, GJ 9287A, HT Vir, ED +46 degrees 1944, Proxima Cen, alpha Cen A/B, HR 6094, HR 8883, CPD -48 degrees 10901, and HR 8964. We derive surface fluxes from the Lexan/B and Al/Ti/C count rates and cataloged ROS.-IT Position Sensitive Proportional Counter (PSPC) data. The EUVE surface fluxes are reasonably correlated with surface fluxes calculated from PSPC measurements. The time variability of the sources has been examined. Most of the sources show no significant variability at the 99% confidence level. Flares were detected from the K7 V star Melotte 25 VA 334, the K3 V star V834 Tau IHD 29697), and the K3 + K8 Hyades binary ED +22 degrees 669. The ED +22 degrees 669 count rate at the peak of the fare is a factor of 6 higher than the quiescent count rate, with a peak Lexan/B luminosity of 7.9 x 10(29) ergs s(-1). The V834 Tau flare was detected in both Lexan/B and Al/Ti/C bands. The peak luminosity of the flare is 1.6 x 10(29)and 8 x 10(28) ergs s(-1) for Lexan/B and Al/Ti/C, respectively. C1 Univ Calif Berkeley, Ctr Euv Astrophys, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Athens, Dept Phys, Sect Astrophys Astron & Mech, GR-15784 Zografos, Greece. RP Christian, DJ (reprint author), Univ Calif Berkeley, Ctr Euv Astrophys, 2150 Kittredge St, Berkeley, CA 94720 USA. NR 38 TC 7 Z9 7 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 1998 VL 115 IS 1 BP 316 EP 324 DI 10.1086/300185 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ454 UT WOS:000071389200029 ER PT J AU Kim, DW Elvis, M AF Kim, DW Elvis, M TI X-ray selected red, absorbed quasars SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT X-ray Surveys Workshop - To Mark the Occasion of the 35th Anniversary of the Birth of X-Ray Astronomy and the 7th Anniversary of the First Light of ROSAT CY JUN 18-20, 1997 CL POTSDAM, GERMANY SP Astrophysikal Inst Potsdam, NASA Goddard Space Flight Ctr X-Ray Astrophys Branch C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea. RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI BERLIN PA MUHLENSTRASSE 33-34, D-13187 BERLIN, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 1998 VL 319 IS 1-2 BP 28 EP 28 DI 10.1002/asna.2123190111 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY346 UT WOS:000072137900010 ER PT J AU Nicastro, F Elvis, M Fiore, F AF Nicastro, F Elvis, M Fiore, F TI X-ray color selected warm absorbers SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT X-ray Surveys Workshop - To Mark the Occasion of the 35th Anniversary of the Birth of X-Ray Astronomy and the 7th Anniversary of the First Light of ROSAT CY JUN 18-20, 1997 CL POTSDAM, GERMANY SP Astrophysikal Inst Potsdam, NASA Goddard Space Flight Ctr X-Ray Astrophys Branch C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Roma, I-00040 Monteporzio Catone, RM, Italy. CNR, Ist Astrofis Spaziale, I-00131 Rome, Italy. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 5 TC 0 Z9 0 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI BERLIN PA MUHLENSTRASSE 33-34, D-13187 BERLIN, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 1998 VL 319 IS 1-2 BP 30 EP 30 DI 10.1002/asna.2123190113 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY346 UT WOS:000072137900012 ER PT J AU Della Ceca, R Cagnoni, I Maccacaro, T AF Della Ceca, R Cagnoni, I Maccacaro, T TI The 2-10 keV number counts relationship SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT X-ray Surveys Workshop - To Mark the Occasion of the 35th Anniversary of the Birth of X-Ray Astronomy and the 7th Anniversary of the First Light of ROSAT CY JUN 18-20, 1997 CL POTSDAM, GERMANY SP Astrophysikal Inst Potsdam, NASA Goddard Space Flight Ctr X-Ray Astrophys Branch AB We are using data from the GIS2 instrument onboard the ASCA satellite to perform a medium survey in the 2-10 keV energy band. We discuss here first results on the description of the 2-10 keV; number-flux relationship down to a flux limit of similar to 6.3 x 10(-14) ergs cm(-2) s(-1) (the faintest detectable flux), i.e. about 2.7 orders of magnitude fainter than the Piccinotti et al., (1982) determination. The main goal of this program is to define a sample of hard X-ray selected AGNs in order to evaluate their contribution to the X-ray background and to test AGNs unification models. END. C1 Osservatorio Astron Brera, I-20121 Milan, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02318 USA. RP Della Ceca, R (reprint author), Osservatorio Astron Brera, Via Brera 28, I-20121 Milan, Italy. OI Della Ceca, Roberto/0000-0001-7551-2252 NR 5 TC 1 Z9 1 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI BERLIN PA MUHLENSTRASSE 33-34, D-13187 BERLIN, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 1998 VL 319 IS 1-2 BP 64 EP 64 DI 10.1002/asna.2123190128 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY346 UT WOS:000072137900027 ER PT J AU Schwartz, DA AF Schwartz, DA TI Operational capabilities of AXAF for surveys SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT X-ray Surveys Workshop - To Mark the Occasion of the 35th Anniversary of the Birth of X-Ray Astronomy and the 7th Anniversary of the First Light of ROSAT CY JUN 18-20, 1997 CL POTSDAM, GERMANY SP Astrophysikal Inst Potsdam, NASA Goddard Space Flight Ctr X-Ray Astrophys Branch DE X-rays : general; telescopes; instrumentation; miscellaneous AB The Advanced X-ray Astrophysics Facility (AXAF) will offer us all great opportunities for surveys. The exceptional resolution of the AXAF mirrors, will yield unsurpassed deep surveys, and the energy resolution of the ACIS will allow unique contributions to the AXAF version of previous "medium sensitivity" and "slew" surveys. At this workshop we presented some preliminary results of the calibration of the AXAF flight mirrors. Off-axis imaging, chromatic effects of vignetting, and the asymmetry of the off-axis response will be important for planning and analyzing surveys. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI BERLIN PA MUHLENSTRASSE 33-34, D-13187 BERLIN, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 1998 VL 319 IS 1-2 BP 121 EP 124 DI 10.1002/asna.2123190157 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY346 UT WOS:000072137900056 ER PT J AU Grindlay, JE AF Grindlay, JE TI Surveying the hard x-ray sky: imaging in space and time SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT X-ray Surveys Workshop - To Mark the Occasion of the 35th Anniversary of the Birth of X-Ray Astronomy and the 7th Anniversary of the First Light of ROSAT CY JUN 18-20, 1997 CL POTSDAM, GERMANY SP Astrophysikal Inst Potsdam, NASA Goddard Space Flight Ctr X-Ray Astrophys Branch DE x-ray surveys; x-ray binaries; black holes; neutron stars; AGN AB One of the few remaining astronomical bands (factor of similar to 10 in energy range) still without an all-sky imaging survey is the hard x-ray band (10-600 keV). This is in spite of sensitive imaging all-sky surveys already conducted at soft x-ray (0.2-2 keV; ROSAT) and soft/hard gamma-ray (similar to 750 keV - 10 GeV; COMPTEL/EGRET) energies and imminent for medium x-ray energies (2-10 keV; ABRIXAS). A hard x-ray imaging survey conducted with wide-field coded aperture telescopes allows both hight sensitivity (and spatial/spectral resolution) and broad temporal coverage. We derive a generalized survey sensitivity/temporal parameter, Q, and compare previous and planned hard x-ray surveys with the proposed EXIST mission. Key scientific objectives that could be addressed with the enhanced capability of EXIST are outlined. C1 Harvard Smithsonian Ctr Astrophys, Harvard Observ, Cambridge, MA 02138 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, Harvard Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 1 Z9 1 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI BERLIN PA MUHLENSTRASSE 33-34, D-13187 BERLIN, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 1998 VL 319 IS 1-2 BP 133 EP 136 DI 10.1002/asna.2123190160 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY346 UT WOS:000072137900059 ER PT J AU Hudec, R Pina, L Inneman, A Gorenstein, P AF Hudec, R Pina, L Inneman, A Gorenstein, P TI Schmidt wide field X-ray telescope prototype SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT X-ray Surveys Workshop - To Mark the Occasion of the 35th Anniversary of the Birth of X-Ray Astronomy and the 7th Anniversary of the First Light of ROSAT CY JUN 18-20, 1997 CL POTSDAM, GERMANY SP Astrophysikal Inst Potsdam, NASA Goddard Space Flight Ctr X-Ray Astrophys Branch C1 Acad Sci Czech Republ, Inst Astron, CZ-25165 Ondrejov, Czech Republic. Czech Tech Univ, Fac Nucl Engn, CZ-11519 Prague, Czech Republic. Czech Tech Univ, Fac Mech Engn, Dept Precis Mech & Opt, Prague, Czech Republic. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hudec, R (reprint author), Acad Sci Czech Republ, Inst Astron, CZ-25165 Ondrejov, Czech Republic. RI Hudec, Rene/G-9018-2014 NR 2 TC 2 Z9 2 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI BERLIN PA MUHLENSTRASSE 33-34, D-13187 BERLIN, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 1998 VL 319 IS 1-2 BP 145 EP 145 DI 10.1002/asna.2123190164 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YY346 UT WOS:000072137900063 ER PT J AU Prosser, CF Randich, S AF Prosser, CF Randich, S TI Identification of new low-mass members of the Alpha Persei open cluster by ROSAT. I. SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE open clusters and associations, individual (alpha Persei, Melotte 20); stars, late-type; stars, coronae; stars, activity; X-rays, stars ID STANDARD STARS; X-RAY; COUSINS AB Following the work of Randich et al. (1996) involving a ROSAT raster scan survey of the alpha Persei open cluster, we present here the results of a photometric/spectroscopic program examining the possible optical counterparts to a group of 73 X-ray sources in the raster survey which were not matched to catalogued stars. Of the 73 sources investigated, similar to 40 have an optical counterpart with photometry acceptable for cluster membership and similar to 20 of these also have radial velocities consistent with membership. We discuss the X-ray properties of these potential new members and why they may not have been identified in earlier membership surveys of this cluster. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-8046 Garching, Germany. RP Prosser, CF (reprint author), Natl Opt Astron Observ, Tucson, AZ 85726 USA. EM cprosser@noao.edu; randich@arcetri.astro.it OI Randich, Sofia/0000-0003-2438-0899 NR 19 TC 12 Z9 12 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI BERLIN PA MUHLENSTRASSE 33-34, D-13187 BERLIN, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 1998 VL 319 IS 4 BP 201 EP 214 DI 10.1002/asna.2123190402 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 118UT UT WOS:000075859300001 ER PT J AU Prosser, CF Randich, S Simon, T AF Prosser, CF Randich, S Simon, T TI Identification of new low-mass members of the Alpha Persei open cluster by ROSAT. II. SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE open clusters and associations, individual (alpha Persei, Melotte 20); stars, late-type; stars, coronae; stars, activity; X-rays, stars ID M-DWARFS; PHOTOMETRY; STARS AB The present investigation examines possible optical counterparts to 130 X-ray sources in the region of the alpha Persei open cluster (d similar to 170pc, age similar to 50 Myr) resulting from the analysis of three 22-25 ksec ROSAT PSPC pointings. In the same manner as for 73 X-ray sources from a raster survey in alpha Per (Prosser & Randich 1998), CCD photometry is employed to obtain magnitudes and colors for stars/objects close to the X-ray positions, with additional echelle and low-dispersion H alpha spectra provided for some stars. For almost 60 X-ray sources, an optical counterpart with photometry acceptable for cluster membership is identified, some of which can be excluded from membership on the basis of discrepant radial velocity or X-ray characteristics. On the order of 30 new members or likely members associated with X-ray sources have been identified based on available data. A photometric rotation period has been obtained for one rapid rotator identified in X-rays. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-8046 Garching, Germany. Inst Astron, Honolulu, HI USA. RP Prosser, CF (reprint author), Natl Opt Astron Observ, Tucson, AZ 85726 USA. OI Randich, Sofia/0000-0003-2438-0899 NR 13 TC 21 Z9 21 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI BERLIN PA MUHLENSTRASSE 33-34, D-13187 BERLIN, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 1998 VL 319 IS 4 BP 215 EP 234 DI 10.1002/asna.2123190403 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 118UT UT WOS:000075859300002 ER PT J AU Buckley, JH Akerlof, CW Carter-Lewis, DA Catanese, M Cawley, MF Connaughton, V Fegan, DJ Finley, JP Gaidos, JA Hillas, AM Krennrich, F Lamb, RC Lessard, RW McEnery, JE Mohanty, G Quinn, J Rodgers, AJ Rose, HJ Rovero, AC Schubnell, MS Sembroski, G Srinivasan, R Weekes, TC Zweerink, J AF Buckley, JH Akerlof, CW Carter-Lewis, DA Catanese, M Cawley, MF Connaughton, V Fegan, DJ Finley, JP Gaidos, JA Hillas, AM Krennrich, F Lamb, RC Lessard, RW McEnery, JE Mohanty, G Quinn, J Rodgers, AJ Rose, HJ Rovero, AC Schubnell, MS Sembroski, G Srinivasan, R Weekes, TC Zweerink, J TI Constraints on cosmic-ray origin from TeV gamma-ray observations of supernova remnants SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE gamma-rays : observations; SNRs; cosmic rays; ISM : IC 443, gamma Cyg SNR, W 44 ID 11 CM WAVELENGTH; PARTICLE-ACCELERATION; SHOCK ACCELERATION; X-RAY; MOLECULAR CLOUDS; NOVA REMNANT; ELECTRON ACCELERATION; GALACTIC PLANE; ENERGY-SPECTRA; TYCHO AB If supernova remnants (SNRs) are the site of cosmic-ray acceleration, the associated nuclear interactions should result in an observable flux of gamma-rays for the nearest SNRs. Measurements of the TeV gamma-ray flux from six nearby, radio-bright SNRs have been made with the Whipple Observatory imaging air Cerenkov telescope over the period September 1993 to June 1996. No significant emission has been detected and upper limits on the >300 GeV flux are reported. Three of these SNRs (IC443, gamma-Cygni and W44) are spatially coincident with low-latitude otherwise unidentified sources detected with the Energetic Gamma-Ray Experiment Telescope (EGRET). If the EGRET gamma-ray fluxes result from cosmic-ray interactions then the EGRET and Whipple data are found to be collectively inconsistent with a cosmic-ray source spectrum flatter than similar to E-2.4. The Whipple upper limits for IC443 and gamma-Cygni are also inconsistent with a priori predictions if these remnants are indeed expanding into regions where the average density of the interstellar medium is enhanced by the presence of molecular clouds. These data weaken the case for the simplest models of shock acceleration and energy dependent propagation of cosmic rays. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Univ Michigan, Randall Lab Phys, Ann Arbor, MI 48109 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. St Patricks Coll, Dept Phys, Maynooth, Kildare, Ireland. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Natl Univ Ireland Univ Coll Dublin, Dept Phys, Dublin 4, Ireland. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. RP Buckley, JH (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. NR 119 TC 117 Z9 117 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 1998 VL 329 IS 2 BP 639 EP 658 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ939 UT WOS:000071439900028 ER PT J AU Kramer, C Alves, J Lada, C Lada, E Ungerechts, S Walmsley, M AF Kramer, C Alves, J Lada, C Lada, E Ungerechts, S Walmsley, M TI The millimeter wavelength emissivity in IC5146 SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE interstellar medium : clouds; dust, extinction; individual objects : IC5146 ID DUST OPACITIES; EXTINCTION; GAS AB We have observed a core in the northern streamer of the IC5146 cloud using the MPIfR 19-channel Bolometer system on the IRAM 30m telescope at a wavelength of 1.2 mm. We smoothed our observations to the same angular resolution (30") as a new map of the NIR extinction of this cloud (Lada, Alves, and Lada 1998) and in this way obtained direct measurements of the ratio of millimeter emissivity to dust extinction. Our results are compatible with a ratio of the visual extinction coefficient kappa(V) to the 1.2 mm grain absorption coefficient kappa(1.2) of (4 +/- 2) X 10(4). This is in good agreement with the theoretical predictions for bare interstellar grains (Draine & Lee 1984; Mathis 1990). Within the errors our measurements are also consistent with recent models of grains with ice mantles whose size distribution has been modified due to coagulation but whose millimeter emissivities are not a strong function of grain size (Ossenkopf & Henning 1994). We find that the ratio of millimeter grain emissivity to visual extinction varies roughly inversely with the visual extinction over our map and interpret this as implying a gradient in dust temperature from roughly 8 K in the core interior (A(V) > 20 mag) to 20 K in regions of low (5 mag) extinction. One consequence of our result is that the 1.2 mm intensity, by itself, is not a good tracer of mass in this cloud. C1 Inst Radioastron Milimetrica, E-18012 Granada, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Kramer, C (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. NR 19 TC 20 Z9 20 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 JAN PY 1998 VL 329 IS 2 BP L33 EP L36 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ939 UT WOS:000071439900004 ER PT J AU Fiore, F Elvis, M Giommi, P Padovani, P AF Fiore, F Elvis, M Giommi, P Padovani, P TI X-ray spectral survey of WGACAT quasars. I. Spectral evolution and low-energy cutoffs SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars, general; radio continuum, galaxies; X-rays, galaxies ID COMPLETE SAMPLE; ROSAT SPECTRA; RADIO-SOURCES; ABSORPTION; OBJECTS; GALAXIES; CATALOG; PSPC AB We have used the WGA catalog of ROSAT Position Sensitive Proportional Counter (PSPC) X-ray sources to study the X-ray spectrum of about 500 quasars in the redshift interval 0.1-4.1, detected with a signal-to-noise ratio better than 7. We have parameterized the PSPC spectrum in terms of two "effective energy spectral indices," alpha(s) (0.1-0.8 keV), and alpha(H) (0.4-2.4 keV), which allows for the different Galactic N-H along the quasars' line of sight. We have used these data to explore the questions raised by the initial PSPC high-redshift quasar studies, and in particular the occurrence of low-energy X-ray cutoffs in high-redshift radio-loud quasars. We have also studied the emission spectra of a large sample of radio-loud and radio-quiet quasars and studied their differences. We find that low-energy X-ray cutoffs are more commonly (and perhaps exclusively) found in radio-loud quasars. Therefore, the low-energy X-ray cutoffs are physically associated with the quasars, and not with intervening systems, since those would affect radio-quiet and radio-loud equally. We suggest that photoelectric absorption is a likely origin of these cutoffs. The number of "cutoffs" in radio-loud quasars significantly increases with redshift rather than with luminosity. A partial correlation analysis confirms that alpha(S) is truly anticorrelated with redshift at the 99.9% confidence level, indicating evolution with cosmic epoch, and not a luminosity effect. Conversely, for alpha(H) the observed anticorrelation with redshift is mostly due to a strong dependence on luminosity. In radio-quiet quasars, we find marginal evidence for a flattening of alpha(H) (P = 4.5%), going from z < 1 to z = 2; in agreement with previous studies. Radio-loud quasars at z < 2.2 instead show a "concave" spectrum (alpha(H) < alpha(S) by similar to 0.2). This new result is consistent with the widespread suggestion that the flatter X-ray spectra of radio-loud quasars may be due to an additional component above those seen in radio-quiet quasars. However, it might also imply different processes at work in radio-loud and radio-quiet sources. At z greater than or similar to 2 the average soft and hard indices are similar and are both significantly smaller than at lower redshifts. This can be due to the soft component of radio-loud quasars being completely shifted out of the PSPC band at z > 2. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Rm, Italy. BeppoSAX Sci Data Ctr, Rome, Italy. Univ Roma Tor Vergata 2, Dipartimento Fis, I-00133 Rome, Italy. RP Fiore, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI giommi, paolo/0000-0002-2265-5003; Padovani, Paolo/0000-0002-4707-6841; Fiore, Fabrizio/0000-0002-4031-4157 NR 56 TC 70 Z9 70 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1998 VL 492 IS 1 BP 79 EP 90 DI 10.1086/305024 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ455 UT WOS:000071389300008 ER PT J AU Elvis, M Fiore, F Giommi, P Padovani, P AF Elvis, M Fiore, F Giommi, P Padovani, P TI X-ray spectral survey of WGACAT quasars. II. Optical and radio properties of quasars with low-energy X-ray cutoffs SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars, general; radio continuum, galaxies; X-rays, galaxies ID HIGH-REDSHIFT QUASARS; ABSORPTION FEATURE; COMPLETE SAMPLE; GALAXY 3C-109; LOUD QUASARS; 5 GHZ; ALPHA; S4; SPECTROPHOTOMETRY; POLARIZATION AB We have selected quasars with X-ray colors suggestive of a low-energy cutoff, from the ROSAT Position Sensitive Proportional Counter (PSPC) pointed observations archive. We examine the radio and optical properties of these 13 quasars. Five out of the seven quasars with good optical spectra show associated optical absorption lines, with two having high Av candidate systems. Two other cutoff quasars show reddening associated with the quasar. We conclude that absorption is highly likely to be the cause of the X-ray cutoffs, and that the absorbing material is associated with the quasars, not intervening along the line of sight. The suggestion that gigahertz peaked sources are associated with X-ray cutoffs remains unclear with this expanded sample. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Rm, Italy. BeppoSAX Sci Data Ctr, Rome, Italy. Univ Roma Tor Vergata 2, Dipartimento Fis, I-00133 Rome, Italy. Space Telescope Sci Inst, ESA, Dept Space Sci, Baltimore, MD 21218 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI giommi, paolo/0000-0002-2265-5003; Padovani, Paolo/0000-0002-4707-6841; Fiore, Fabrizio/0000-0002-4031-4157 NR 90 TC 30 Z9 30 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1998 VL 492 IS 1 BP 91 EP 97 DI 10.1086/305025 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ455 UT WOS:000071389300009 ER PT J AU Hartmann, D Magnani, L Thaddeus, P AF Hartmann, D Magnani, L Thaddeus, P TI A survey of high-latitude molecular gas in the northern Galactic hemisphere SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, abundances; ISM, clouds; ISM, molecules; surveys ID CO SURVEY; MILKY-WAY; CLOUDS; EMISSION; QUADRANT; CIRRUS AB We surveyed the northern Galactic hemisphere (NGH) at b greater than or equal to 30 degrees in the CO (1-0) emission line to determine the surface filling factor of molecular gas at high Galactic latitudes and to search for heretofore unknown molecular clouds. The NGH was sampled on a locally Cartesian grid with 1 degrees (true-angle) spacing in Galactic longitude and latitude. Of the 11,478 points in our grid, we observed all 10,562 positions that rise to an elevation above 30 degrees in Cambridge, MA, the site of the 1.2 m millimeterwave telescope that was used for the survey. Only 26 lines of sight showed CO emission. Monte Carlo simulations based on our sampling grid and with cloud sizes, in a uniform distribution, ranging from 0 to 2 deg(2) suggest that the survey is similar to 70% complete. Power-law distributions yield fractional completenesses that are typically a factor of 2 lower. The surface filling factor, corrected for the incompleteness of our sampling grid, is 0.004-0.008, depending on which cloud size distribution is used. These values are substantially lower than what is found in the southern Galactic hemisphere at b less than or equal to -30 degrees. Adopting as the CO to H(2) conversion ratio N(H2)/W(CO) = 2.5 x 10(20) cm(-2) (K km s(-1))(-1), the mass surface density of molecular gas in the north ranges from 0.015 +/- 0.009 to 0.035 +/- 0.020 M. pc(-2). With the exception of four fairly significant aggregations of clouds (the complexes associated with the Polaris flare, Ursa Major, Draco, and L134), and a handful of isolated cloudlets, the northern Galactic hemisphere at b greater than or equal to 30 degrees is found to be largely free of molecular gas. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. RP Hartmann, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 72, Cambridge, MA 02138 USA. NR 39 TC 37 Z9 37 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1998 VL 492 IS 1 BP 205 EP 212 DI 10.1086/305019 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ455 UT WOS:000071389300018 ER PT J AU Gullbring, E Hartmann, L Briceno, C Calvet, N AF Gullbring, E Hartmann, L Briceno, C Calvet, N TI Disk accretion rates for T Tauri stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars, pre-main-sequence ID MAGNETIC NEUTRON STARS; YOUNG STARS; MAGNETOSPHERIC ACCRETION; UBVRI PHOTOMETRY; VARIABILITY; EXTINCTION; EVOLUTION; COUSINS; CATALOG; ORIGIN AB We present new measurements of disk accretion rates for T Tauri stars in the Taurus molecular cloud complex. Our results are based on intermediate-resolution spectrophotometry from 3200 to 5200 Angstrom, which is used to derive the excess hot continuum emission produced by accretion onto the central star. Previous estimates of T Tauri accretion rates in the literature differ by as much as 1 order of magnitude; our measurements agree better with the lowest estimates, and we discuss the problems and systematic effects that led to the previous disagreement. In particular, we note that the stellar photospheric emission from nonaccreting T Tauri stars exhibits color anomalies compared to main-sequence stars; these anomalies make the estimated extinction depend upon the color index used. We argue that the V-R index is a reasonable compromise to match with optically derived spectral types, and that V-I and V-J are much more likely to be biased by cooler companion stars and starspots. We develop a calibration with which approximate mass accretion rates can be derived for T Tauri stars based on broadband photometry and spectral types, which should enable accretion rates to be estimated for large samples with greater ease. C1 Cent Univ Venezuela, Caracas, Venezuela. CIDA, Ctr Invest Astron, Merida, Venezuela. RP Gullbring, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM egullbring@cfa.harvard.edu; lhartmann@cfa.harvard.edu NR 53 TC 561 Z9 564 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1998 VL 492 IS 1 BP 323 EP 341 DI 10.1086/305032 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ455 UT WOS:000071389300029 ER PT J AU Gammie, CF Menou, K AF Gammie, CF Menou, K TI On the origin of episodic accretion in dwarf novae SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; MHD; novae, cataclysmic variables; turbulence ID DIFFERENTIALLY ROTATING-DISKS; NUMERICAL SIMULATIONS; DRIVEN ACCRETION; ANGULAR-MOMENTUM; BINARY-SYSTEMS; SS-CYGNI; STABILITY; DYNAMO; SHOCKS; INSTABILITY AB We show that dwarf nova disks in quiescence have rather low magnetic Reynolds numbers, of order 10(3). Numerical simulations of magnetized accretion disks suggest that under these conditions magnetohydrodynamic turbulence and the associated angular momentum transport is sharply reduced. This could be the physical origin of episodic accretion in dwarf nova disks. If so, the standard disk instability model needs to be revised. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, CNRS, DARC, F-92195 Meudon, France. RP Gammie, CF (reprint author), Harvard Smithsonian Ctr Astrophys, MS-51,60 Garden St, Cambridge, MA 02138 USA. OI Gammie, Charles /0000-0001-7451-8935 NR 34 TC 67 Z9 67 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1998 VL 492 IS 1 BP L75 EP L78 DI 10.1086/311091 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ456 UT WOS:000071389400019 ER PT J AU Munoz, JA Falco, EE Kochanek, CS Lehar, J Herold, LK Fletcher, AB Burke, BF AF Munoz, JA Falco, EE Kochanek, CS Lehar, J Herold, LK Fletcher, AB Burke, BF TI MGC 2214+3550: A new binary quasar SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars, individual (MGC 2214+3550) ID 5 GHZ SURVEY; GRAVITATIONAL LENS; Q2237+0305; DISCOVERY AB We report the discovery of a binary quasar, MGC 2214+3550A,B, whose components have similar optical spectra at a redshift of z = 0.88. The quasars are separated on the sky by 3.0 " and have a magnitude difference of Delta m(l) = 0.5 mag. The VLA radio map at 3.6 cm shows a single 47 mJy radio source with a core-jet morphology that is coincident with the brighter optical quasar A. Gravitational lensing is ruled out by the lack of radio emission from quasar B and the lack of any visible galaxies to act as the lens. We conclude that MGC 2214+3550A and B are physically associated. With a projected separation of 12.7 h(-1) kpc (Omega(0) = 1), MGC 2214+3550A,B is one of the smallest z > 0.5 binary quasars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Cambridge, MA 02139 USA. RP Munoz, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 33 TC 13 Z9 13 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 1998 VL 492 IS 1 BP L9 EP L12 DI 10.1086/311093 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YQ456 UT WOS:000071389400003 ER PT J AU Goodman, AA Barranco, JA Wilner, DJ Heyer, MH AF Goodman, AA Barranco, JA Wilner, DJ Heyer, MH TI Velocity coherence in dense cores SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article; Proceedings Paper CT Conference on Molecular Spectroscopy in the 1 to 10 GHz Range with the Upgraded Arecibo Telescope CY OCT 19-20, 1995 CL ARECIBO OBSERV NATL ASTRONOMY & IONOSPHERE CTR, ARECIBO, PUERTO RICO HO ARECIBO OBSERV NATL ASTRONOMY & IONOSPHERE CTR DE interstellar medium; molecules : OH, (CO)-O-18, NH3; turbulence; star formation; radio lines ID STAR-FORMATION; DARK CLOUDS; MOLECULAR CLOUDS AB By analyzing 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 nu proportional to R-a where a similar to 0 2; 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. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts, Five Coll Radio Astron Observ, Amherst, MA 01003 USA. RP Goodman, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 8 TC 3 Z9 3 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 1998 VL 37 IS 1-2 BP 109 EP 111 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ZV549 UT WOS:000074316200009 ER PT J AU Munoz, JA Falco, EE Kochanek, CS Lehar, J McLeod, BA AF Munoz, JA Falco, EE Kochanek, CS Lehar, J McLeod, BA TI The CASTLES project SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 3rd Scientific Meeting of the Spanish-Astronomical-Society (SEA) CY SEP 21-24, 1998 CL LA LAGUNA, SPAIN SP Spainish Astronom Soc AB We describe the goals of the CASTLES (CfA-Arizona-Space-Telescope-LEns-Survey)(1) project including a sample of NICMOS images of gravitational lenses and a brief list of the preliminary findings. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Munoz, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 34 Z9 34 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 1998 VL 263 IS 1-4 BP 51 EP 54 DI 10.1023/A:1002120921330 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 250BP UT WOS:000083369400010 ER PT J AU Navascues, DBY Stauffer, JR Bouvier, J AF Navascues, DBY Stauffer, JR Bouvier, J TI Brown Dwarfs and very low mass stars: Towards a new age scale for young open clusters SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 3rd Scientific Meeting of the Spanish-Astronomical-Society (SEA) CY SEP 21-24, 1998 CL LA LAGUNA, SPAIN SP Spainish Astronom Soc ID MAIN-SEQUENCE; PLEIADES; LITHIUM C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Grenoble, F-38041 Grenoble, France. RP Navascues, DBY (reprint author), Max Planck Inst Astron, Konisgtuhl 17, D-69117 Heidelberg, Germany. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 10 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 1998 VL 263 IS 1-4 BP 239 EP 242 DI 10.1023/A:1002174614429 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 250BP UT WOS:000083369400053 ER PT J AU Navascues, DBY Stauffer, JR Bouvier, J Martin, EL AF Navascues, DBY Stauffer, JR Bouvier, J Martin, EL TI The mass function at the end of the main sequen the M35 Open Cluster SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 3rd Scientific Meeting of the Spanish-Astronomical-Society (SEA) CY SEP 21-24, 1998 CL LA LAGUNA, SPAIN SP Spainish Astronom Soc ID STARS C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Grenoble, F-38041 Grenoble, France. Univ Calif Berkeley, Berkeley, CA 94720 USA. RP Navascues, DBY (reprint author), Max Planck Inst Astron, Konisgtuhl 17, D-69117 Heidelberg, Germany. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 9 TC 4 Z9 4 U1 0 U2 2 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 1998 VL 263 IS 1-4 BP 303 EP 306 DI 10.1023/A:1002180229392 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 250BP UT WOS:000083369400069 ER PT J AU Eff-Darwich, A Korzennik, SG Cortes, TR Hernandez, FP Palle, P AF Eff-Darwich, A Korzennik, SG Cortes, TR Hernandez, FP Palle, P TI The solar rotation rate Omega(R, theta) SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 3rd Scientific Meeting of the Spanish-Astronomical-Society (SEA) CY SEP 21-24, 1998 CL LA LAGUNA, SPAIN SP Spainish Astronom Soc ID CORE ROTATION; P-MODE AB In recent years, the capability to detect and analyse solar oscillation acoustic modes has greatly improved. The development of ground based networks like GONG or BiSON and the use of space platforms like SOHO has allowed us to study the structure and dynamics of the Sun with unprecedented precision. In this work we explore the distribution of the rotation in the solar interior, specially in the core. This kind of information is essential in order to study the physical processes involved in the evolution of the Sun and many other stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. Inst Astrofis Canarias, Tenerife 38205, Spain. RP Eff-Darwich, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02139 USA. RI Palle, Pere/H-4720-2015 NR 9 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 1998 VL 263 IS 1-4 BP 347 EP 350 DI 10.1023/A:1002103822548 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 250BP UT WOS:000083369400080 ER PT J AU Micela, G Sciortino, S Harnden, FR Rosner, R AF Micela, G Sciortino, S Harnden, FR Rosner, R TI X-ray variability and rotation in the pleiades cluster SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Non-Sleeping Universe Conference CY NOV 24-29, 1997 CL UNIV PORTO, CTR ASTROPHYS, OPORTO, PORTUGAL SP Junta Nacl Investigacao Cientifica Technol, Ctr Astrofisica Univ Porto, Camara Municipal Porto, Inst Vinho Porto HO UNIV PORTO, CTR ASTROPHYS ID COUNTING DETECTOR IMAGES; WAVELET TRANSFORMS; EINSTEIN; ROSAT C1 Osservatorio Astron Palermo, I-90134 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Micela, G (reprint author), Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. NR 8 TC 4 Z9 4 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 1998 VL 261 IS 1-4 BP 105 EP 106 DI 10.1023/A:1002005812163 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 249KU UT WOS:000083332900024 ER PT J AU Owocki, SP Cranmer, SR Gayley, KG AF Owocki, SP Cranmer, SR Gayley, KG TI Mass loss from rotating hot-stars: Inhibition of wind compressed disks by nonradial line-forces SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 5th Workshop of the GDR-Nilieux-Circumstellaires-French-Working-Group of the CNRS CY SEP 22-25, 1997 CL MONT SAINTE ODILE, FRANCE SP CNRS, GDR Milieux Circumstellaires French Working Grp ID RADIATION-DRIVEN WINDS; STELLAR WINDS; B-STARS; HD-93521 AB We review the dynamics of radiatively driven mass loss from rapidly rotating hot-stars. We first summarize the angular momentum conservation process that leads to formation of a Wind Compressed Disk (WCD) when material from a rapidly rotating star is driven gradually outward in the radial direction. We next describe how stellar oblateness and asymmetries in the Sobolev line-resonance generally leads to nonradial components of the driving force is a line-driven wind, including an azimuthal spin-down force acting against the sense of the wind rotation, and a latitudinal force away from the equator. We summarize results from radiation-hydrodynamical simulations showing that these nonradial forces can lead to an effective suppression of the equatorward flow needed to form a WCD, as well as a modest (similar to 25%) spin-down of the wind rotation. Furthermore, contrary to previous expectations that the wind mass flux should be enhanced by the reduced effective gravity near the equator, we show here that gravity darkening effects can actually lead to a reduced mass loss, and thus lower density, in the wind from the equatorial region. Finally, we examine the equatorial bistability model, and show that a sufficiently strong jump in wind driving parameters can, in principle, overcome the effect of reduced radiative driving flux, thus still allowing moderate enhancements in density in an equatorial, bistability zone wind. C1 Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Iowa, Dept Phys & Astron, Ames, IA 50011 USA. RP Owocki, SP (reprint author), Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. NR 22 TC 24 Z9 24 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 1998 VL 260 IS 1-2 BP 149 EP 159 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 202FL UT WOS:000080641400015 ER PT J AU Backman, DE Stauffer, JR AF Backman, DE Stauffer, JR TI Dust disks around main sequence stars SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on ISOs View on Stellar Evolution CY JUL 01-04, 1997 CL NOORDWIJKERHOUT, NETHERLANDS SP Space Res Org Netherlands, Astron Inst Anton Pannekoek, Univ Amsterdam, Kapteyn Fund ID FAR-INFRARED EMISSION; BETA-PICTORIS; EVOLUTION; VEGA; PLANETS; EXCESS; DEBRIS; SHELL; IRAS; AGE AB Many nearby main sequence stars are surrounded by cool dust radiating strongly in the far-IR. The characteristics of some of the prototype systems will be discussed. The dust is understood to represent debris related to planet formation, and the known disk systems may be dense analogs of the Kuiper Belt structure in our outer solar system. ISO observing programs plan to address questions regarding how common planetary material is around normal stars and how its amount and location depend on system age. These questions are central to an understanding of the place of the "Vega/beta Pic" disks in stellar evolution. Preliminary results from the first year of ISO operation will be reported. C1 Franklin & Marshall Coll, Lancaster, PA 17604 USA. Univ Denver, Denver, CO 80208 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Backman, DE (reprint author), Franklin & Marshall Coll, Lancaster, PA 17604 USA. NR 33 TC 1 Z9 1 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 1998 VL 255 IS 1-2 BP 91 EP 102 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 111YE UT WOS:000075465800014 ER PT S AU Dalgarno, A AF Dalgarno, A BE Mohr, PJ Wiese, WL TI Atomic and molecular data for cosmology SO ATOMIC AND MOLECULAR DATA AND THEIR APPLICATIONS: ICAMDATA - FIRST INTERNATIONAL CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 1st International Conference on Atomic and Molecular Data and Their Applications (ICAMDATA) CY SEP 29-OCT 02, 1997 CL NATL INST STAND & TECHNOL, GAITHERSBURG, MD SP Amer Inst Phys, US Dept Commerce, Technol Adm, Natl Inst Stand & Technol, Stand Reference Data Program, Natl Inst Stand & Technol, Atom Phys Div, Phys Lab, Elect Power Res Inst, US DOE, Off Fus Energy Sci, Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Molec Phys, USN, Naval Res Lab, SEMATECH, NASA, Off Space Sci HO NATL INST STAND & TECHNOL AB An account is given of some of the atomic and molecular data needed in the interpretation of cosmological observations and in the construction of models of the evolution of the early Universe through the recombination era. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-751-0 J9 AIP CONF PROC PY 1998 VL 434 BP 193 EP 201 PG 9 WC Physics, Applied; Physics, Atomic, Molecular & Chemical; Physics, Multidisciplinary SC Physics GA BL48Y UT WOS:000075685200013 ER PT S AU Smith, P Brown, L Rumble, J Tawara, H AF Smith, P Brown, L Rumble, J Tawara, H BE Mohr, PJ Wiese, WL TI Standardization of databases; data assessment; and uncertainty statements SO ATOMIC AND MOLECULAR DATA AND THEIR APPLICATIONS: ICAMDATA - FIRST INTERNATIONAL CONFERENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 1st International Conference on Atomic and Molecular Data and Their Applications (ICAMDATA) CY SEP 29-OCT 02, 1997 CL NATL INST STAND & TECHNOL, GAITHERSBURG, MD SP Amer Inst Phys, US Dept Commerce, Technol Adm, Natl Inst Stand & Technol, Stand Reference Data Program, Natl Inst Stand & Technol, Atom Phys Div, Phys Lab, Elect Power Res Inst, US DOE, Off Fus Energy Sci, Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Molec Phys, USN, Naval Res Lab, SEMATECH, NASA, Off Space Sci HO NATL INST STAND & TECHNOL C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, P (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 1-56396-751-0 J9 AIP CONF PROC PY 1998 VL 434 BP 401 EP 402 PG 2 WC Physics, Applied; Physics, Atomic, Molecular & Chemical; Physics, Multidisciplinary SC Physics GA BL48Y UT WOS:000075685200026 ER PT J AU Rappole, JH McDonald, MV AF Rappole, JH McDonald, MV TI Response to Latta and Baltz (1997) SO AUK LA English DT Editorial Material ID MIGRATORY BIRDS; HABITAT QUALITY; FRAGMENTATION; WARBLERS; FORESTS; MIGRANT C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Cent Arkansas, Dept Biol, Conway, AR 72035 USA. RP Rappole, JH (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM nzpem033@sivm.si.edu NR 47 TC 7 Z9 7 U1 2 U2 3 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD JAN PY 1998 VL 115 IS 1 BP 246 EP 251 PG 6 WC Ornithology SC Zoology GA YR355 UT WOS:000071487100032 ER PT J AU Lovelock, CE AF Lovelock, CE TI Observations of the photosynthetic physiology of tree species within the C-3 monocotyledon genus Pandanus, and comparison with dicotyledon C-3 tree species SO AUSTRALIAN JOURNAL OF BOTANY LA English DT Article ID RELATIVE GROWTH-RATE; SHADE TOLERANCE; LIFE-SPAN; LIGHT; ACCLIMATION; PLANTS; ALLOCATION; SEEDLINGS; LEAVES AB Photosynthetic characteristics of tree species from the tropical C-3 monocotyledon genus Pandanus were compared with C-3 dicotyledon species growing in similar environments. The Pandanus species had similar maximum photosynthetic rates (A(max)) to dicotyledon tree species in leaves from both sun and shaded environments when A(max) was expressed on an area basis. Because of the low specific leaf area of the schlerophyllous leaves of the Pandanus compared to the dicotyledon species, the similarity in A(max) was no longer evident when A(max) was expressed on a dry-weight basis. Leaf dark respiration rates of the Pandanus on a leaf area and weight basis were generally lower than the shade-intolerant dicotyledons and similar to the shade-tolerant dicotyledon species. Low dark respiration rates and low specific leaf area of the Pandanus may be important characteristics for growth and survival in environments where resource levels are low and the likelihood of tissue damage is high. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Lovelock, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM lovelock@serc.si.edu RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 21 TC 0 Z9 0 U1 0 U2 2 PU C S I R O PUBLICATIONS PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0067-1924 J9 AUST J BOT JI Aust. J. Bot. PY 1998 VL 46 IS 1 BP 103 EP 110 DI 10.1071/BT96106 PG 8 WC Plant Sciences SC Plant Sciences GA ZJ687 UT WOS:000073242400008 ER PT J AU Thiele, A Krause, GH Winter, K AF Thiele, A Krause, GH Winter, K TI In situ study of photoinhibition of photosynthesis and xanthophyll cycle activity in plants growing in natural gaps of the tropical forest SO AUSTRALIAN JOURNAL OF PLANT PHYSIOLOGY LA English DT Article ID PHOTOSYSTEM-II; FLUORESCENCE; RECOVERY; LEAVES; LIGHT; CANOPY; PIGMENTS; STRESS AB Photoinhibition of photosynthesis was studied in situ in leaves of several species of plants growing in natural treefall gaps of a tropical lowland forest (Barro Colorado Island, Panama). Leaves showed several features typical of sun-acclimation: relatively high pools of total carotenoids and xanthophyll cycle pigments and high ratios of chlorophyll a to b. During 1-2 h periods of exposure to direct mid-day sun, all leaves experienced substantial photoinhibition as indicated by a marked decline in the ratio of variable to maximum chlorophyll a fluorescence emission, F-V/F-M, detected after 10 min of dark adaptation. After return to shade, these 'dark-adapted' F-V/F-M, ratios increased with biphasic kinetics, similar to previous findings under controlled conditions in the laboratory, A phase lasting about 1 h accounted for most of the recovery of F-V/F-M and was followed by a slow phase which proceeded until sunset. The decline in F-V/F-M during photoinhibition and the fast phase of recovery correlated closely with the amounts of zeaxanthin in the leaves. Given the small portion of the second recovery phase which has previously been attributed to turnover of the D1 protein in Photosystem II, high xanthophyll cycle activity in these gap leaves is probably responsible for the major part of photoinhibition, providing an efficient energy dissipation pathway during periods of high sunlight exposure. C1 Univ Dusseldorf, Inst Plant Biochem, D-40225 Dusseldorf, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Krause, GH (reprint author), Univ Dusseldorf, Inst Plant Biochem, Univ Str 1, D-40225 Dusseldorf, Germany. EM ghkrause@uni-duesseldorf.de NR 31 TC 74 Z9 77 U1 0 U2 3 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 1998 VL 25 IS 2 BP 189 EP 195 PG 7 WC Plant Sciences SC Plant Sciences GA ZF984 UT WOS:000072952900008 ER PT J AU Brown, JL AF Brown, JL TI How to study reproduction in wild cats and live to tell the tale. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1998 VL 58 SU 1 MA M4 BP 23 EP 23 PG 1 WC Reproductive Biology SC Reproductive Biology GA ZX708 UT WOS:000074546000014 ER PT J AU Wildt, DE Wolf, KN Howard, J AF Wildt, DE Wolf, KN Howard, J TI Biopolitics, reproduction and conservation of endangered species. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1998 VL 58 SU 1 MA M6 BP 23 EP 24 PG 2 WC Reproductive Biology SC Reproductive Biology GA ZX708 UT WOS:000074546000016 ER PT J AU Graham, LH Swanson, WF Wildt, DE Brown, JL AF Graham, LH Swanson, WF Wildt, DE Brown, JL TI Melatonin pre-treatment mitigates ovarian hyperstimulation by exogenous gonadotropins in the domestic cat. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Natl Zool Pk, Conserv & Res Ctr, Front Royal, VA USA. Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, Cincinnati, OH USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1998 VL 58 SU 1 MA 95 BP 101 EP 101 PG 1 WC Reproductive Biology SC Reproductive Biology GA ZX708 UT WOS:000074546000141 ER PT J AU Howard, JG Wolf, KN Marinari, PE Kreeger, JS Anderson, TR Vargas, A Wildt, DE AF Howard, JG Wolf, KN Marinari, PE Kreeger, JS Anderson, TR Vargas, A Wildt, DE TI Delayed onset of sperm production in 1-year old male black-footed ferrets. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Smithsonian Inst, Conservat & Res Ctr, Washington, DC 20560 USA. US Fish & Wildlife Serv, Natl Black Footed Ferret Conservat Ctr, Laramie, WY USA. NR 0 TC 4 Z9 4 U1 0 U2 2 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1998 VL 58 SU 1 MA 170 BP 124 EP 125 PG 2 WC Reproductive Biology SC Reproductive Biology GA ZX708 UT WOS:000074546000216 ER PT J AU Pukazhenthi, BS Spindler, R Wildt, DE AF Pukazhenthi, BS Spindler, R Wildt, DE TI Short term exposure to room temperature disrupts the meiotic spindle of in vitro matured domestic cat oocytes. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1998 VL 58 SU 1 MA 201 BP 134 EP 134 PG 1 WC Reproductive Biology SC Reproductive Biology GA ZX708 UT WOS:000074546000247 ER PT J AU Tardif, SD Power, ML Power, RA Layne, DG Oftedal, OT AF Tardif, SD Power, ML Power, RA Layne, DG Oftedal, OT TI Lactation performance in marmoset monkeys: Relation to infant growth and maternal condition. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. Kent State Univ, Dept Biol Sci, Kent, OH 44242 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1998 VL 58 SU 1 MA 212 BP 137 EP 137 PG 1 WC Reproductive Biology SC Reproductive Biology GA ZX708 UT WOS:000074546000258 ER PT J AU Roth, TL McRae, MA Brown, JL Kroll, JL Bellem, AC O'Brien, JK Romo, JS AF Roth, TL McRae, MA Brown, JL Kroll, JL Bellem, AC O'Brien, JK Romo, JS TI The reproductive physiology of a living fossil - The sumatran rhinoceros (Dicerorhinus sumatrensis). SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, Cincinnati, OH USA. Smithsonian Inst, Conserv & Res Ctr, Front Royal, VA USA. NR 0 TC 1 Z9 1 U1 0 U2 3 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1998 VL 58 SU 1 MA 333 BP 176 EP 176 PG 1 WC Reproductive Biology SC Reproductive Biology GA ZX708 UT WOS:000074546000379 ER PT J AU Anzalone, CR Bench, GS Balhorn, R Wildt, DE AF Anzalone, CR Bench, GS Balhorn, R Wildt, DE TI Chromatin alterations in sperm of teratospermic domestic cats. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Univ Calif Lawrence Livermore Natl Lab, Livermore, CA USA. NR 0 TC 5 Z9 5 U1 0 U2 5 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 1998 VL 58 SU 1 MA 364 BP 185 EP 185 PG 1 WC Reproductive Biology SC Reproductive Biology GA ZX708 UT WOS:000074546000410 ER PT J AU Rasmussen, HN Whigham, DF AF Rasmussen, HN Whigham, DF TI The underground phase: a special challenge in studies of terrestrial orchid populations SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article; Proceedings Paper CT Meeting on Orchid Population Biology - Conservation and Challenges CY NOV, 1995 CL LINNEAN SOC, LONDON, ENGLAND SP Botan Soc Brit Isles HO LINNEAN SOC DE Corallorhiza; demography; germination; Goodyera; life history; Liparis; mycotrophy; Orchidaceae; seed; seedling (protocorm) ID IN-SITU; SPECIFICITY AB Orchid seeds are minute and the first seedling stages of terrestrial species are underground, so there is little knowledge about the biology of the early life history and the size of seed/seedling populations relative to the number of plants that eventually emerge above ground. A recently developed field sowing technique makes it possible to explore a variety of topics such as the length of time that seeds spend as part of the soil seed bank, the phenology of seed germination: substrate requirements for germination, dependence of germination on fungal availability, substrate requirements and growth rate of seedlings, seedling phenology and development, and seedling-fungus specificity patterns in the soil. Several of these applications are relevant for conservation issues. Studies of Goodgera pubescens, Corallorhiza odontorhiza and Liparis lilifolia show considerable variation in germination strategies, patterns of seedling development and establishment, substrate requirements, and levels of specificity with the fungi. (C) 1998 The Linnean Society of London. C1 Danish Inst Agr Sci, Dept Ornamentals, DK-5792 Arslev, Denmark. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Rasmussen, HN (reprint author), Danish Inst Agr Sci, Dept Ornamentals, Kirstinebjerg Vej 10, DK-5792 Arslev, Denmark. RI Rasmussen, Hanne/P-5485-2014; OI Rasmussen, Hanne/0000-0002-0181-9304; Whigham, Dennis/0000-0003-1488-820X NR 29 TC 44 Z9 49 U1 1 U2 23 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD JAN-FEB PY 1998 VL 126 IS 1-2 BP 49 EP 64 DI 10.1111/j.1095-8339.1998.tb02515.x PG 16 WC Plant Sciences SC Plant Sciences GA ZG513 UT WOS:000073011200005 ER PT J AU Soreng, RJ Davis, JI AF Soreng, RJ Davis, JI TI Phylogenetics and character evolution in the grass family (Poaceae): Simultaneous analysis of morphological and chloroplast DNA restriction site character sets SO BOTANICAL REVIEW LA English DT Review ID RBCL SEQUENCE DATA; TRANSFER-RNA GENES; RIBOSOMAL DNA; CLADISTIC-ANALYSIS; DOMINICAN AMBER; LARGE SUBUNIT; PLASTID GENE; GRAMINEAE; GENOME; SYSTEMATICS AB A phylogenetic analysis of the grass family (Poaceae) was conducted using two character sets, one representing variation in 364 mapped and cladistically informative restriction sites from all regions of the chloroplast genome, the other representing variation in 42 informative "structural characters." The structural character set includes morphological, anatomical, chromosomal, and biochemical features, pins structural features of the chloroplast genome. The taxon sample comprises 75 exemplar taxa, including 72 representatives of Poaceae and one representative of each of three related families (Flagellariaceae, Restionaceae, and Joinvilleaceae); Flagellaria served as the outgroup for the purpose of cladogram rooting. Among the grasses, 24 tribes and all 16 subfamilies of grasses recognized by various modern authors were sampled. Transformations of structural characters are mapped onto the phylogenetic hypotheses generated by the analysis, and interpreted with respect to biogeography and the evolution of wind pollination in the grass family A major goal of the study was to test the monophyly of several putatively natural groups, including Bambusoideae, Pooideae, Arundinoideae, and the "PACC clade" (the latter comprising subfamilies Panicoideae, Arundinoideae, Chloridoideae, and Centothecoideae), as well as to analyze the phylogenetic structure within these groups and others. Several genera of controversial placement (Amphipogon, Anisopogon, Anomochloa, Brachyelytrum, Diarrhena, Eremitis, Ehrharta, Lithachne, Lygeum, Nardus, Olyra, Pharus, and Streptochaeta) also were included, with the goal of determining their phylogenetic affinities. The two character sets were analyzed separately, and a simultaneous analysis of the combined matrices also was conducted. The combined data set also was analyzed using homoplasy-implied weights. Among major results of the combined unweighted analysis were resolution of a sister-group relationship between Joinvillea and Poaceae; resolution of a clade comprising Anomochloa and Streptochaeta as the sister of all other grasses, with Pharus the next group to diverge from the lineage that includes all remaining grasses; and resolution of other taxa often assigned to Bambusoideae s.l. (including Ehrharta and Oryzeae, and excluding a few other taxa as noted) as a paraphyletic assemblage, within which is nested a clade that consists of Brachyelytrum, the PACC clade (including Amphipogon), and Pooideae (including Brachypodieae, Stipeae, Anisopogon, Diarrhena, Lygeum, and Nardus). Within the PACC clade, Aristida is identified as the sister of all other elements of the group; Chloridoideae, Centothecoideae, and Panicoideae are each resolved as monophyletic, the latter two being sister-groups; and the remaining Arundinoid elements constitute a paraphyletic group within which are nested these three subfamilies. Within the Pooideae, four "core tribes" (Bromeae, Hordeeae [i.e., Triticeae], Agrostideae [i.e., Aveneae], and Poeae, the latter including Sesleria) are resolved as a monophyletic group that is nested among the remaining elements of the subfamily (Brachypodieae, Meliceae, Stipeae, Anisopogon, Diarrhena, Lygeum, and Nardus). A second principal goal of the analysis was to identify structural synapomorphies of clades. Among the synapomorphies identified for some of the major clades are the following: gain of a 6. 4 kb inversion in the chloroplast genome in Joinvillea and the grasses; reduction to 1 ovule per pistil, gain of a lateral "grass-type" embryo, and gain of an inversion around the gene trnT in the chloroplast genome in the grasses; loss of arm cells in the clade that consists of Brachyelytrum, Pooideae, and the PACC clade; loss of the epiblast and gain of an elongate mesocotyl internode in the PACC clade; gain of proximal female-sterile florets in female-fertile spikelets, gain of overlapping embryonic leaf margins, and gain of Panicum-type endosperm starch grains in the clade that comprises Centothecoideae and Panicoideae; and loss of the scutellar tail of the embryo in Pooideae (in one of two alternative placements of Pooideae among other groups). These findings are consistent with an origin and early diversification of grasses as forest understory herbs, followed by one or more radiations into open habitats, concomitant with multiple origins of C-4 photosynthesis and specialization for wind pollination. C1 Cornell Univ, LH Bailey Hortorium, Ithaca, NY 14853 USA. RP Soreng, RJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. NR 210 TC 111 Z9 139 U1 0 U2 15 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0006-8101 J9 BOT REV JI Bot. Rev. PD JAN-MAR PY 1998 VL 64 IS 1 BP 1 EP 85 DI 10.1007/BF02868851 PG 85 WC Plant Sciences SC Plant Sciences GA ZG827 UT WOS:000073043900001 ER PT B AU Briceno, C Hartmann, L Stauffer, J Martin, EL AF Briceno, C Hartmann, L Stauffer, J Martin, EL BE Rebolo, R Martin, EL Osorio, MRZ TI A deep CCD survey for very low-mass pre-main sequence stars in Taurus SO BROWN DWARFS AND EXTRASOLAR PLANETS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Brown Dwarfs and Extrasolar Planets CY MAR 17-21, 1997 CL PUERTO LA CRUZ, SPAIN SP European Union, Ist Astrofis Canarias, Spanish Min Educ & Culture, Gen Directorate Higher Educ AB We present here the preliminary results of a CCD survey aimed at obtaining the first extensive sample of very low-mass pre-main sequence objects in the Taurus star-forming region. The first List of CCD-selected stars in the dark clouds B209, L1495 and L1551 have been subject to follow up spectroscopy for identifying true pre-main sequence objects. So far we have found 3 new T Tauri stars with masses M less than or similar to 0.1 M., the faintest and reddest pre-main sequence stars yet identified in this star-forming region. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Briceno, C (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 1-886733-54-6 J9 ASTR SOC P PY 1998 VL 134 BP 36 EP 42 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK82B UT WOS:000073481100005 ER PT B AU Latham, DW Stefanik, RP Mazeh, T Torres, G Carney, BW AF Latham, DW Stefanik, RP Mazeh, T Torres, G Carney, BW BE Rebolo, R Martin, EL Osorio, MRZ TI Low-mass companions found in a large radial-velocity survey SO BROWN DWARFS AND EXTRASOLAR PLANETS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Brown Dwarfs and Extrasolar Planets CY MAR 17-21, 1997 CL PUERTO LA CRUZ, SPAIN SP European Union, Ist Astrofis Canarias, Spanish Min Educ & Culture, Gen Directorate Higher Educ AB In 1981 we undertook a survey of a proper-motion-selected sample of solar-type stars, to study the kinematics and chemistry of the halo and disk populations in our Galaxy. For the past: 15 years Me have monitored the radial velocities of more than 1400 stars in this sample, to determine the frequency and orbital characteristics of the spectroscopic binaries. In this paper me summarize the results for the low-mass companions found in this survey, and we use the distribution of orbital eccentricity versus minimum mass as a framework far outlining some of the mechanisms that may be involved in the formation and orbital evolution of planets and brown dwarfs. 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 6 Z9 6 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-54-6 J9 ASTR SOC P PY 1998 VL 134 BP 178 EP 187 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK82B UT WOS:000073481100026 ER PT J AU Cole, L Vorontsova, M AF Cole, L Vorontsova, M TI Species of Pyuridae (Ascidiacea) from South Vietnam SO BULLETIN OF MARINE SCIENCE LA English DT Article ID PYURA AB Four species of the family Pyuridae from South Vietnam are listed and discussed, with habitat and breeding notes added. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Cole, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Stop 163, Washington, DC 20560 USA. NR 21 TC 5 Z9 7 U1 0 U2 0 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 1998 VL 62 IS 1 BP 1 EP 6 PG 6 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 129PT UT WOS:000076472700001 ER PT J AU Boucaud-Camou, E Roper, CFE AF Boucaud-Camou, E Roper, CFE TI The digestive system of rhynchoteuthion paralarvae (Cephalopoda : Ommastrephidae) SO BULLETIN OF MARINE SCIENCE LA English DT Article AB The anatomy of the digestive system and the digestive system enzymes of three types of rhynchoteuthion paralarvae A ', B ', and C ' (Illex) were studied. No differences among the three were found. The main features of the digestive system of these species of paralarval Ommastrephidae are described. The buccal mass is comprised of a beak and radula with conspicuous teeth. The well developed posterior salivary glands contain glandular tissue with two cell types: A, goblet cell, and B, granular cell. The esophagus is lined with a thin cuticle, but the stomach lacks cuticle and has a more strongly developed muscular wall than the esophagus. The large vestibule is lined with ciliated and glandular cells. Some primary folds of ciliated epithelial cells begin to develop in the caecum. The digestive gland is compact, round, red-pigmented and enclosed in a thick elastic capsule; it contains conspicuous inclusions: large boules, typical brown-body vacuoles and numerous lipid droplets. Thirteen hydrolases involved in digestive processes were examined. High proteasic activity and histochemically undetectable amylasic activity suggest a carnivorous diet. The occurrence of typical lysosomal enzymes in the digestive gland reveals a high intracellular digestive activity. The digestive system appeared to be developed and functional in the smallest specimens examined (ML: mantle length 1-2 mm). Typically juvenile features include the anterior part of the digestive system which is more highly developed than the posterior part, thus it is more functionally important than the posterior part. The muscular wall of the posterior part of the digestive tract is very thin: tractus with long cilia probably move food. Because the caecal leaflets are not yet fully developed, the digestive gland probably assumes the greatest part of the digestive and absorptive functions in paralarvae. C1 Univ Caen, Biol & Biotechnol Marines Lab, F-14032 Caen, France. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Smithsonian Marine Stn, Ft Pierce, FL 34946 USA. RP Boucaud-Camou, E (reprint author), Univ Caen, Biol & Biotechnol Marines Lab, F-14032 Caen, France. NR 21 TC 7 Z9 7 U1 0 U2 0 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 1998 VL 62 IS 1 BP 81 EP 87 PG 7 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 129PT UT WOS:000076472700007 ER PT J AU Musser, GG Carleton, MD Brothers, EM Gardner, AL AF Musser, GG Carleton, MD Brothers, EM Gardner, AL TI Systematic studies of oryzomyine rodents (Muridae, Sigmodontinae): Diagnoses and distributions of species formerly assigned to Oryzomys "capito" SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Review ID ATLANTIC FOREST; CENTRAL BRAZIL; MAMMALS; POPULATION; CRICETIDAE; ECOLOGY; RATS; OLIGORYZOMYS; COMMUNITY; EVOLUTION AB We describe the morphological species boundaries and geographic distributions of 10 Neotropical Oryzomys based on analyses of museum specimens (skins and skulls, examples preserved in fluid, chromosomal spreads, and information about collection sites from skin tags, field catalogs, and other sources). These species have been regarded as members of an Oryzomys capito complex and for a long time were consolidated into a single entity identified as O. capito. Our study documents the following: 1. Defining the limits of species within the O. capito complex first requires a comprehensive review and rigorous definition of O. capito itself. We consider Fischer's (1814) Mus megacephalus to be valid and available, designate a neotype to bear the name, and reinstate it as a senior synonym of capito Olfers (1818). We then provide a working definition of O. megacephalus and its close relative, O. laticeps, derived from analyses of morphometric variation, estimates of geographic distributions, and evaluations of synonyms. In our view, O. megacephalus occurs in Amazonia but also extends into eastern Paraguay; its synonyms are capito Olfers (1818), cephalotes Desmarest (1819), velutinus Alien and Chapman (1893), goeldi Thomas (1897), modestus Alien (1899), and perenensis Allen (1901). Oryzomys laticeps Lund (1840) occurs in the Atlantic Forest region of eastern Brazil. We designate a lectotype for laticeps and allocate the names saltator Winge (1887) and oniscus Thomas (1904) as synonyms. 2. We provide the first comprehensive taxonomic revision of Oryzomys yunganus Thomas (1902). Its range covers tropical evergreen rainforest formations in the Guiana Region and the Amazon Basin where, as documented by voucher specimens, it has been collected at the same localities as O. megacephalus, O. nitidus, and O. macconnelli. Specimens of O. yunganus can be distinguished from those of the other three by a combination of body size, pelage texture and coloration, pattern of carotid arterial circulation, occlusal patterns of second upper and lower molars, cranial proportions, and chromosomal features. Appreciable intraspecific geographic variation occurs in diploid number of chromosomes and frequency of occurrence of the hypothenar plantar pad, but sampling inadequacies obscure the significance of this variation. Large body size is characteristic of populations in the western Amazon Basin and in the tepui region of eastern Venezuela; smaller size characterizes populations in the Guianas and along the eastern margin of the Amazon Basin. No other scientific name has been correctly associated with the species. Samples from Mirador, Palmera, and Mera in the western Andean foothills of central Ecuador possess a combination of pelage, cranial, and dental traits that distinguish them from all samples of O. yunganus. These specimens are the basis for a new species we describe here, one that is more closely related to O. yunganus than to any other member of the former O. "capito" complex. 3. We redescribe Oryzomys bolivaris (reviewed by Pine, 1971, under the name O. bombycinus), amplify its geographic range, and contrast it with O. talamancae and O. alfaroi, two sympatric congeners with which it is often confused. A distinctive set of morphological traits allows unambiguous identification of specimens belonging to O. bolivaris. It is a trans-Andean species recorded from very wet tropical evergreen rain forests extending from eastern Honduras and Nicaragua through Costa Rica and Panama to western Colombia and Ecuador. Alien's (1901) bolivaris is the oldest name for this species; castaneus Alien (1901), rivularis Alien (1901), bombycinus Goldman (1912), alleni Goldman (1915), and orinus Pearson (1939) are synonyms. 4. We revise the definition of Oryzomys talamancae Alien (1891) provided by Musser and Williams (1985), document additional specimens, describe karyotypes from Ecuadoran and Venezuelan samples, and contrast its morphology, chromosomes, and distribution with those of O. alfaroi and O. megacephalus. The geographic dis tribution of O. talamancae is also trans-Andean, but it inhabits a wider variety of habitats than does O. bolivaris. We also provide a new synonymy and identify the following scientific names as syn onyms of O. talamancae: mollipilosus Alien (1899), magdalenae Alien (1899), villosus Alien (1899), sylvaticus Thomas (1900), panamensis Thomas (1901), medius Robinson and Lyon (1901), and carrikeri Alien (1908). 5. We present hypotheses of species boundaries of four morphologically similar species that we identify as members of the Oryzomys nitidus group: O. nitidus Thomas (1884), O. macconnelli Thomas (1910), O. russatus Wagner (1848), and a species described as new. We recognize the four species by morphological and chromosomal traits, and contrast characteristics of each species with one another. One synonym, boliviae Thomas (1901), is associated with O. nitidus, and two scientific names, incertus Alien (1913) and mureliae Alien (1915), are allocated to O. macconnelli. Synonyms of O. russatus are physodes Brants (1827), intermedia Leche (1886), coronatus Winge (1887), lamia Thomas (1901), legatus Thomas (1925), kelloggi Avila-Pires (1959), and moojeni Avila-Pires (1959). We designate lectotypes for russatus and intermedia and identify the holotype of coronatus. Based on voucher specimens, the geographic distribution of O. nitidus is mainly along the Andean foothills and adjacent lowlands in Peri, Bolivia, and nearby western Brazil, but scattered records document its eastward extension through south-central Brazil to Paraguay and northeastern Argentina. Oryzomys macconnelli inhabits the tropical evergreen rain forests of Amazonia. Its distribution partially overlaps that of O. nitidus in western Amazonia, where the two species have been collected together at one locality in Peru, and it is sympatric with the new species, which is recorded only from the lower regions of rios Xingu and Tocantins in northern Para, Brazil. The distribution of O. russatus is documented by specimens from southeastern and south-central Brazil, southern Bolivia, and northern Argentina; its range is allopatric to those of O. macconnelli, the new species, and O. nitidus except in southern Bolivia, where the latter was collected at the same site with O. russatus. We also examined types and descriptions of taxa associated with Oryzomys subflavus and O. ratticeps to determine if any of those names actually reference members of the O, nitidus group. Although the original description of subflavus Wagner (1842) is vague, the holotype clearly represents an example of that very distinctive species; vulpinus Lund (1840), for which we designate a lectotype, and vulpinoides Schinz (1845) are synonyms of O. subflavus. The oldest name for the species currently known as Oryzomys ratticeps is Mus angouya Fischer (1814), a name not based on a specimen but on Azara's (1801) description of "Rat troisieme, ou Rat Angouya." Azara's account is so general that it could also apply to individuals of O. subflavus, O. nitidus, of O. russatus, To stabilize the nomenclature of these species, we designate a neotype for Mus angouya Fischer(1814) and treat the following scientific names as synonyms: buccinatus Olfers (1818), leucogaster Wagner(1845), ratticeps Hensel (1872), rex Winge (1887), tropicius Thomas (1924), and paraganus Thomas (1924). We also designate lectotypes for leucogaster and ratticeps. We have not analyzed phylogenetic relationships among the species in the farmer O. "capito" complex discussed here. Documenting morphological and distributional boundaries of other biological species now grouped in the genus Oryzomys (alfaroi and its close relatives, for example) must precede, in our view, attempts at phylogenetic reconstruction. C1 Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. Smithsonian Inst, Natl Museum Nat Hist, US Geol Survey, Biol Resources Div, Washington, DC 20560 USA. RP Musser, GG (reprint author), Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. NR 320 TC 0 Z9 0 U1 2 U2 8 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0090 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 1998 IS 236 BP 10 EP + PG 369 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA ZC721 UT WOS:000072609900001 ER PT J AU Graus, RR Macintyre, IG AF Graus, RR Macintyre, IG TI Global warming and the future of Caribbean coral reefs SO CARBONATES AND EVAPORITES LA English DT Article ID COMPUTER-SIMULATION; WESTERN ATLANTIC; SEA-LEVEL; ZONATION AB Computer simulations with the COREEF model (Graus et al. 1984) demonstrate that the growth of Caribbean coral reefs will be unable to match all but the most optimistic predicted rates of sea level rise that global warming is expected to cause over the next few centuries, and, therefore, these reefs will gradually become more submerged. As they deepen, higher waves will propagate into back-reef areas, altering the ecological and sedimentological zonation patterns and accelerating the erosion of leeward shelves and shores. Resuspended sediment will increase the turbidity, causing the demise of sediment-sensitive corals and possibly entire reef communities. C1 No Virginia Community Coll, Div Sci & Appl Technol, Alexandria, VA 22311 USA. Smithsonian Inst, Nat Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Graus, RR (reprint author), No Virginia Community Coll, Div Sci & Appl Technol, Alexandria, VA 22311 USA. NR 24 TC 8 Z9 11 U1 0 U2 6 PU NORTHEASTERN SCIENCE FOUNDATION INC PI TROY PA PO BOX 746, TROY, NY 12181-0746 USA SN 0891-2556 J9 CARBONATE EVAPORITE JI Carbonates Evaporites PY 1998 VL 13 IS 1 BP 43 EP 47 PG 5 WC Geology SC Geology GA ZV172 UT WOS:000074277300006 ER PT J AU Steneck, RS Miller, TE Reid, RP Macintyre, IG AF Steneck, RS Miller, TE Reid, RP Macintyre, IG TI Ecological controls on stromatolite development in a modern reef environment: A test of the ecological refuge paradigm SO CARBONATES AND EVAPORITES LA English DT Article ID STOCKING-ISLAND; EXUMA-CAYS; BAHAMAS; COMMUNITIES AB Paleontological and neontologicaI studies suggest that stromatolite development may be limited to environments where ecological processes such as colonization (recruitment), growth competition, and predation (herbivory) are low. We quantitatively tested this "ecological refuge paradigm" at st unique stromatolite-reef complex at Stocking Island, Bahamas where three contiguous zones grade in dominance from stromatolites in the back reef to a macroalgal turf in the reef flat to reef building corals and coralline algae and reef fishes in the fore reef. At two independent transacts along this gradient, we quantified the distribution and abundance of the dominant organisms and measured the rates of the above-listed ecological processes and determined survival and growth of stromatolite, turf, and coralline algae transplanted to each of the three zones. We also measured both the sediment dynamics and temperature profiles along this gradient to determine if these may be controlling the ecological processes. Stromatolites dominate the back reef zone where species diversity (especially among eukaryotes) and associated ecological pressures were low. Measured rates of colonization from calcified (i.e., coralline) and noncalcified macroalgae and filamentous turf algae were lowest in the back reef (i.e., <5% substrate colonization/y) and highest in the fore reef (95% substrate colonization/y). This suggests that competition for space was lowest in the stromatolite zone. Growth and survival rates of transplanted coralline algae were low in both the back reef (3 mm/y and 20-40% annual survival rates) and reef flat (<2 mm/y, 0% surviving) and highest in the fore reef(about 10 mm/y, 80% surviving). Foraging activity from all fishes was lowest in the back reef (total 0.4 bites/m(2)/h) and reef flat (0 bites/m(2)/h) and highest in fore reef (900 -2200 bites/m(2)/h mostly from omnivorous wrasses). Herbivory from all potential sources was below detectable levels in the stromatolite zone and was highest in the fore reef. The ecological refuge found in the back reef stromatolite zone resulted primarily from periodic sediment inundation. Most eukaryotic reef-dwelling organisms cannot persist under as much as 700 mm of sediment for periods up to 100 days. Although the reef flat suffered both desiccation and thermal stress (averaging more than 5 degrees C greater daily temperature fluctuation than the fore reef), natural and transplanted eukaryotic turf algae thrived there. Although transplanted stromatolites survived best in the back reef (about 80% of the original transplant surviving/y), they also persisted in the fore reef (about 40% surviving per year). Therefore, Schizothrix-dominated stromatolites can persist in fore reef environments but because of the presence of other organisms and associated ecological pressures, their laminated microbial-produced structure is lost or obscured While the sediment and the organisms necessary for stromatolite formation exist in this and probably in other modem reef environments, their reef-building contribution will be low except in unusual habitats where abiotic stresses maintain an ecological refuge. C1 Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 125, Washington, DC 20560 USA. RP Steneck, RS (reprint author), Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. NR 45 TC 14 Z9 14 U1 0 U2 10 PU NORTHEASTERN SCIENCE FOUNDATION INC PI TROY PA PO BOX 746, TROY, NY 12181-0746 USA SN 0891-2556 J9 CARBONATE EVAPORITE JI Carbonates Evaporites PY 1998 VL 13 IS 1 BP 48 EP 65 PG 18 WC Geology SC Geology GA ZV172 UT WOS:000074277300007 ER PT B AU Zhang, XL AF Zhang, XL BE Sofue, Y TI Secular dynamical evolution of spiral galaxies and the formation of Galactic Bulges SO CENTRAL REGIONS OF THE GALAXY AND GALAXIES LA English DT Proceedings Paper CT 184th Symposium of the International-Astronomical-Union CY AUG 18-22, 1997 CL TOKYO, JAPAN SP Int Astronom Union AB We show that a recently discovered spiral-induced radial mass accretion process could account for the formation of the Galactic Bulge in a Hubble time. This process is thus expected to be important in the formation of bulges in spiral galaxies, and in the secular evolution of galaxies along the Hubble sequence from late to earlier types. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, XL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS78, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-5060-X PY 1998 BP 29 EP 30 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM57Y UT WOS:000079158500008 ER PT B AU Lee, CW Lee, HM Ann, HB Kwon, KH AF Lee, CW Lee, HM Ann, HB Kwon, KH BE Sofue, Y TI Dynamics of the Galactic Center molecular clouds SO CENTRAL REGIONS OF THE GALAXY AND GALAXIES LA English DT Proceedings Paper CT 184th Symposium of the International-Astronomical-Union CY AUG 18-22, 1997 CL TOKYO, JAPAN SP Int Astronom Union ID KINEMATICS AB We have performed Smoothed Particle Hydrodynamics (SPH) simulations in order to understand the dynamical structures of Galactic Center molecular clouds. In our study it was found that the structures of GC molecular clouds could be induced by the combined effects of a gravitational perturbation by rotating bar potential and the hydrodynamic collisions between the clouds. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, CW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-5060-X PY 1998 BP 197 EP 199 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM57Y UT WOS:000079158500083 ER PT B AU Reid, MJ Readhead, ACS Vermeulen, R Treuhaft, R AF Reid, MJ Readhead, ACS Vermeulen, R Treuhaft, R BE Sofue, Y TI Progress toward a trigonometric parallax of SGR A* SO CENTRAL REGIONS OF THE GALAXY AND GALAXIES LA English DT Proceedings Paper CT 184th Symposium of the International-Astronomical-Union CY AUG 18-22, 1997 CL TOKYO, JAPAN SP Int Astronom Union C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-5060-X PY 1998 BP 435 EP 436 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM57Y UT WOS:000079158500170 ER PT B AU Ho, LC Filippenko, AV Sargent, WLW AF Ho, LC Filippenko, AV Sargent, WLW BE Sofue, Y TI Demographics of nuclear activity in nearby galaxies SO CENTRAL REGIONS OF THE GALAXY AND GALAXIES LA English DT Proceedings Paper CT 184th Symposium of the International-Astronomical-Union CY AUG 18-22, 1997 CL TOKYO, JAPAN SP Int Astronom Union ID DWARF SEYFERT NUCLEI; SEARCH C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ho, LC (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-5060-X PY 1998 BP 463 EP 464 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM57Y UT WOS:000079158500180 ER PT B AU Pen, UL AF Pen, UL BE Byun, YI Ng, KW TI Reconstructing nonlinear stochastic bias from velocity space distortions SO COSMIC MICROWAVE BACKGROUND AND LARGE SCALE STRUCTURE OF THE UNIVERSE SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 5th Taipei Astrophysics Workshop on Cosmology CY DEC 18-21, 1997 CL TAIPEI, TAIWAN SP Natl Cent Univ, Acad Sinica, ROC Natl Sci Council, Natl Ctr Theoret Sci AB We propose a strategy to measure the dark matter power spectrum using minimal assumptions about the galaxy distribution and the galaxy-dark matter cross-correlations. We argue that on sufficiently large scales the central limit theorem generically assures Gaussianity, but not coherence. Asymptotically, the only surviving parameters on a given scale are galaxy variance sigma, bias b = Omega(.6)/beta and the galaxy-dark matter correlation coefficient r. These can all be determined by measuring the quadrupole and octupole distortions in the power spectrum. Measuring them simultaneously may restore consistency between all beta determinations independent of galaxy type. The leading deviations from Gaussianity are conveniently parameterized by an Edgeworth expansion. In the mildly non-linear regime, two additional parameters describe the full picture: the skewness parameter s and non-linear bias bz. They can both be determined from the measured skewness combined with second order perturbation theory or from an N-body simulation. By measuring the redshift distortion of the skewness, one can measure the density parameter Omega with minimal assumptions about the galaxy formation process. This formalism also provides a convenient parametrization to quantify statistical galaxy formation properties. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pen, UL (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 1-886733-71-6 J9 ASTR SOC P PY 1998 VL 151 BP 136 EP 139 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75F UT WOS:000076565500020 ER PT B AU Habbal, SR Gloeckler, G McNutt, RL Tsurutani, BT AF Habbal, SR Gloeckler, G McNutt, RL Tsurutani, BT BE Harris, RA Priest, ER MorenoInsertis, F TI The solar probe mission: A search for the origin of the solar wind and an unprecedented view of the solar surface SO CROSSROADS FOR EUROPEAN SOLAR AND HELIOSPHERIC PHYSICS, PROCEEDINGS: RECENT ACHIEVEMENTS AND FUTURE MISSION POSSIBILITIES LA English DT Proceedings Paper CT Conference on a Crossroads for European Solar and Heliospheric Physics CY MAR 23-27, 1998 CL CANARY ISL, SPAIN SP European Space Agency, Inst Astrofisica Canarias (IAC), ESA Solar Physics Planning Grp (SPPG) DE space missions; solar wind; solar surface AB Despite significant advances in space exploration, in particular with the recent observations from Ulysses and SOHO, the basic questions of solar wind origin and solar surface topology over the poles can only be resolved with a near-Sun Solar Probe mission. Flying along a trajectory perpendicular to the Earth-Sun line during its perihelion passage, Solar Probe will use in-situ and imaging measurements to provide the first three-dimensional view of the corona. direct high spatial and temporal resolution observations of solar polar regions and magnetic fields, and local sampling of the near Sun environment down to 3 R-s from the solar surface. The trajectory will enable the first helioseismic measurements over the poles. The high sampling rate will enable the resolution of fine magnetic structures at all latitudes starting from the pole, through imaging and plasma and field in situ measurements. The NASA Solar Probe is an approved mission to be launched in 2007 with a first perihelion pass at solar maximum in 2010 and a second perihelion pass in 2014 at solar minimum. This review summarizes the latest observations and measurements of the solar wind. It describes the baseline NASA Solar Probe mission, its prime objectives, and its science core payload. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Habbal, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI McNutt, Ralph/E-8006-2010 OI McNutt, Ralph/0000-0002-4722-9166 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 BN 92-9092-668-6 PY 1998 BP 83 EP 90 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BL72Z UT WOS:000076481300010 ER PT B AU Golub, L AF Golub, L BE Harris, RA Priest, ER MorenoInsertis, F TI The HIREX mission SO CROSSROADS FOR EUROPEAN SOLAR AND HELIOSPHERIC PHYSICS, PROCEEDINGS: RECENT ACHIEVEMENTS AND FUTURE MISSION POSSIBILITIES LA English DT Proceedings Paper CT Conference on a Crossroads for European Solar and Heliospheric Physics CY MAR 23-27, 1998 CL CANARY ISL, SPAIN SP European Space Agency, Inst Astrofisica Canarias (IAC), ESA Solar Physics Planning Grp (SPPG) AB The primary aim of the High Resolution Explorer (HIREX) mission is to attack the problem of understanding the structuring and dynamics of astrophysical plasmas. We study the plasma universe by carrying out ground-breaking studies of plasmas on the Sun, with the additional capability of observing planets, galactic and extragalactic objects at the finest possible spatial and temporal scales, with multiple temperature images, with line-of-sight velocity maps, and with large-field coverage. We achieve this goal using two telescopes to image plasmas at temperatures from log T = 5.4-7.4, and field of view from 33 arcmin at pixel size of 0.5 " to 1.3 arcmin at 0.01 ". Observations with HIREX will be a voyage of discovery, observing: plasmas with spatial resolution far beyond the current state-of-the-art in any wavelength regime save radio VLBI. The High Resolution telescope will follow the evolution of similar to 7 km solar structures within coronal loops at high time resolution while the context telescope simultaneously observes the surrounding plasma in individual spectral lines from each ionization state of iron between Fe IX and Fe XIV, as well as He II and Fe XXIV, covering temperatures from < 10(5) K to > 10(7) K. We also obtain line-of-sight velocities with 50 km/s resolution over the full Sun. HIREX makes substantial contributions to understanding the basic physics that underlies all of plasma astrophysics: reconnection theory, wave propagation, plasma confinement, plasma heating, and MHD turbulence in low-beta plasmas, The enormous and unprecedented dynamic range in spectral and spatial coverage, combined with ultra-high spatial resolution, will allow us to carry out unique physical measurements for processes ranging from global scale disruptions to micro-scale instabilities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Golub, L (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 BN 92-9092-668-6 PY 1998 BP 157 EP 167 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BL72Z UT WOS:000076481300016 ER PT S AU Burek, AJ Graessle, DE Blake, RL AF Burek, AJ Graessle, DE Blake, RL BE Macrander, AT Freund, AK Ishikawa, T Mills, DM TI Use of Na-beta alumina crystals in a soft x-ray synchrotron beamline SO CRYSTAL AND MULTILAYER OPTICS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Crystal amd Multilayer Optics CY JUL 21-22, 1998 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE x-rays; crystals; synchrotron radiation; calibration; AXAF ID MONOCHROMATOR CRYSTAL; PERFORMANCE; RADIATION AB We report on the use of Na - beta alumina crystals in a synchrotron soft x-ray monochromator. With a grating spacing of 22.53 Na - beta alumina allows coverage of the 6 - 2 keV energy region not available to high resolution Si or Ge crystals. The crystal is shown to have an intrinsic energy resolving power E/Delta E of 800 - 1300 in first order with relatively high throughput. Second order (2d = 11.26 A) is also strong, with a potential resolving power E/Delta E of 5000. The refractory nature of the crystal allows it to survive synchrotron heat loading without the damage experienced by organic long grating spacing crystals. The crystal is readily cleaved simplifying fabrication, alignment and mounting. Drawbacks include strong second order harmonics and strong anomalous dispersion effects from Na and Al. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Burek, AJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 14 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2903-1 J9 P SOC PHOTO-OPT INS PY 1998 VL 3448 BP 64 EP 75 DI 10.1117/12.332530 PG 12 WC Materials Science, Characterization & Testing; Optics; Physics, Applied; Physics, Nuclear SC Materials Science; Optics; Physics GA BM32S UT WOS:000078392600008 ER PT J AU Tyler, JC AF Tyler, JC TI A new family for a long known but undescribed acanthopterygian fish from the Eocene of Monte Bolca, Italy: Sorbiniperca scheuchzeri gen. & sp. nov. SO ECLOGAE GEOLOGICAE HELVETIAE LA English DT Article DE fish; fossil; Eocene; Monte Bolca; Italy; acanthopterygian ID SURGEONFISHES PERCOMORPHA; RECENT GENERA; PHYLOGENY; ACANTHURIDAE AB Sorbiniperca scheuchzeri, new species, new genus, new family (Sorbinipercidae), is described on the basis of three specimens from the Middle Eocene of Monte Bolca, Italy. One of these specimens was illustrated by Johann Jakob Scheuchzer as early as 1709 but was not described. The new taxon has a unique combination of derived characteristics that relate it to the zeiform + tetraodontiform and, perhaps, caproid clades of acanthopterygians, probably near to one of the branchings of the zeiform + tetraodontiform, beryciform, and lower percomorph clades from one another. C1 Smithsonian Inst, Natl Museum Amer Hist MRC 106, Washington, DC 20560 USA. RP Tyler, JC (reprint author), Smithsonian Inst, Natl Museum Amer Hist MRC 106, Washington, DC 20560 USA. NR 38 TC 3 Z9 3 U1 0 U2 1 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0012-9402 J9 ECLOGAE GEOL HELV JI Eclogae Geol. Helv. PY 1998 VL 91 IS 3 BP 521 EP 540 PG 20 WC Geology SC Geology GA 165WN UT WOS:000078545000017 ER PT S AU Cheimets, P Bookbinder, J Davis, W Golub, L AF Cheimets, P Bookbinder, J Davis, W Golub, L BE Siegmund, OHW Gummin, MA TI Novel mirror mount design, TRACE primary mirror SO EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY IX 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 IX CY JUL 22-24, 1998 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE mirror mount; optics AB Orbiting X-ray and XUV observatories are pushing the achievable image resolution and with it, the requirements on mounted mirror performance. The Transitional Region and Coronal Explorer (TRACE) observatory uses a center mounted primary mirror that must maintain its orientation in roll as well as pitch and yaw. A conformable bedding was used to support the mirror against the expected launch loads in a re-assemblable mount, without inducing unacceptable mirror distortion. The novel mirror mount design is discussed, and its resulting performance described. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cheimets, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2900-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3445 BP 28 EP 37 DI 10.1117/12.330320 PG 10 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BM19Y UT WOS:000078010600003 ER PT S AU Cheimets, P Bookbinder, J Deluca, E Caldwell, D Davis, W Golub, L AF Cheimets, P Bookbinder, J Deluca, E Caldwell, D Davis, W Golub, L BE Siegmund, OHW Gummin, MA TI Large area thin aluminum filter design, handling and testing. SO EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY IX 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 IX CY JUL 22-24, 1998 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE aluminum; filters; XUV AB The process of observing the Sun in the X-ray and eXtreme UltraViolet (XUV), as we are now doing with the TRACE telescope, requires blocking the tremendous amount of visible and infrared light that dominates the flux from the sun. If it is not blocked, the energy will swamp the desired spectrum and cause thermal problems inside the telescope. The most effective approach removing the energy is by filtering the incoming light. One of the best materials for eliminating the undesirable wavelengths is aluminum, which is semi-transparent to X-ray and XUV, but blocks most light with wavelength redward of 850 (A) over cap. Unfortunately the aluminum must be extremely thin, <1600 (A) over cap thick, to provide the necessary XUV transparency. To overcome the structural problem of supporting large areas of extremely thin aluminum, the aluminum film is bonded on a nickel mesh. This paper discusses the engineering difficulties related to using thin aluminum prefilters. The discussion is split into several parts: designing the filter to achieve the desired optical properties, designing the filter assembly to survive launch, developing handling procedures for filter assembly, deal with issues related to surviving solar/vacuum exposure, testing the filter integrity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cheimets, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI DeLuca, Edward/0000-0001-7416-2895 NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2900-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3445 BP 96 EP 106 DI 10.1117/12.330267 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BM19Y UT WOS:000078010600009 ER PT S AU Bloser, P Grindlay, J Narita, T Harrison, F AF Bloser, P Grindlay, J Narita, T Harrison, F BE Siegmund, OHW Gummin, MA TI CdZnTe background measurement at balloon altitudes with an active BGO shield SO EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY IX 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 IX CY JUL 22-24, 1998 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE CdZnTe; background; shielding; balloon flights; hard X-ray astronomy; instrumentation AB We report results of an experiment conducted in May 1997 to measure CdZnTe background and background reduction schemes in space flight conditions similar to those of proposed hard S-ray astrophysics missions. A 1 cm(2) CdZnTe detector was placed adjacent to a thick EGO anticoincidence shield and flown piggybacked onto the EXITE2 scientific balloon payload. The planar shield was designed to veto background counts produced by local gamma-ray production in passive material and neutron interactions in the detector. The CdZnTe and EGO were partially surrounded by a Pb-Sn-Cu shield to approximate the grammage of an S-ray collimator, although the field of view was still similar to 2 pi sr. At an altitude of 127000 feet we find a reduction in background by a factor of 6 at 100 keV. The non-vetoed background is 9 x 10(-4) cts cm(-2) s(-1) keV(-1) at 100 keV, about a factor of 2 higher than that of the collimated (4.5 degrees FWHM) EXITE2 phoswich detector. We compare our recorded spectrum with that expected from simulations using GEANT and find agreement within a factor of 2 between 30 and 300 keV. We also compare our results with those of previous experiments using passive lead and active NaI shields, and discuss possible active shielding schemes in future astronomy missions employing large arrays of CdZnTe detectors. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bloser, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 6 Z9 6 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2900-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3445 BP 186 EP 196 DI 10.1117/12.330275 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BM19Y UT WOS:000078010600017 ER PT J AU Rosenberger, AL Calvo, CM AF Rosenberger, AL Calvo, CM TI Digital morphology: The Smithsonian's BioVisualization Lab SO EVOLUTIONARY ANTHROPOLOGY LA English DT News Item C1 Smithsonian Inst, Museum Natl Hist Nat, Biovisualizat Lab, Natl Partners Program, Washington, DC 20560 USA. Mississippi State Univ, Sch Architecture, Digital Res & Imaging Lab, Mississippi State, MS 39762 USA. RP Rosenberger, AL (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Biovisualizat Lab, Natl Partners Program, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 1060-1538 J9 EVOL ANTHROPOL JI Evol. Anthropol. PY 1998 VL 6 IS 3 BP 77 EP 78 DI 10.1002/(SICI)1520-6505(1998)6:3<77::AID-EVAN1>3.0.CO;2-T PG 2 WC Anthropology SC Anthropology GA ZW254 UT WOS:000074391000001 ER PT J AU Plume, R Bergin, EA Williams, JP Myers, PC AF Plume, R Bergin, EA Williams, JP Myers, PC TI Electron abundance in dense cloud cores - Implications for star formation SO FARADAY DISCUSSIONS LA English DT Article; Proceedings Paper CT General Discussion on Chemistry and Physics of Molecules and Grains in Space CY APR 15-17, 1998 CL UNIV NOTTINGHAM, NOTTINGHAM, ENGLAND HO UNIV NOTTINGHAM ID INTER-STELLAR CLOUDS; TAURUS DARK CLOUDS; MOLECULAR CLOUDS; INTERSTELLAR CLOUDS; CARBON-MONOXIDE; INFRARED-SPECTROSCOPY; AMBIPOLAR DIFFUSION; CHEMICAL EVOLUTION; THERMAL BALANCE; CHEMISTRY AB By combining observations of the J = 1 --> 0 transitions of (CO)-O-18 and (HCO+)-C-13, and the J = 1 --> 0 and 2 --> 1 transitions of DCO+, and a model of molecular cloud chemistry, we have obtained the electron abundance (X-e drop n(e)/n(H2)) in a sample of 20 low-mass and 7 high-mass molecular cloud cores. We find that the electron abundances are confined to a relatively narrow range of -7.5 < log(X-e)< -6.5 with very little scatter about the mean values of < log(X-e)> = -7.04; sigma = 0.22 (low-mass cores) and < log(X-e)> = -7.11; sigma = 0.15 thigh-mass cores). These values are consistent with the standard view that the ionization in dense cloud cores is dominated by cosmic rays, provided that zeta(H2) approximate to 5 x 10(-17) s(-1). These electron abundances also imply that the neutrals are only marginally coupled to the magnetic field (W approximate to 5-8) with only ca. 10% the core radius being cut off from magneto-hydrodynamic (MHD) wave propagation. The coupling parameter (RI) also suggests that ambipolar diffusion timescales are about an order of magnitude larger than the freefall timescale. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Plume, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 46 TC 5 Z9 5 U1 0 U2 0 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON ROAD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 0301-7249 J9 FARADAY DISCUSS JI Faraday Discuss. PY 1998 VL 109 BP 47 EP 60 DI 10.1039/a800076j PG 14 WC Chemistry, Physical SC Chemistry GA 127MB UT WOS:000076353800004 ER PT J AU Stancil, PC Dalgarno, A AF Stancil, PC Dalgarno, A TI Chemical processes in astrophysical radiation fields SO FARADAY DISCUSSIONS LA English DT Article; Proceedings Paper CT General Discussion on Chemistry and Physics of Molecules and Grains in Space CY APR 15-17, 1998 CL UNIV NOTTINGHAM, NOTTINGHAM, ENGLAND HO UNIV NOTTINGHAM ID PHOTODETACHMENT CROSS-SECTIONS; SUPERNOVA 1987A; EARLY UNIVERSE; ASSOCIATION; CHEMISTRY; EMISSION; SN-1987A; ION AB The effects of stimulated photon emission on chemical processes in a radiation field are considered and their influence on the chemistry of the early universe and other astrophysical environments is investigated. Spontaneous and stimulated radiative attachment rate coefficients for H-, Li- and C- are presented. C1 Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dalgarno, A (reprint author), Oak Ridge Natl Lab, Div Phys, POB 2008, Oak Ridge, TN 37831 USA. NR 23 TC 18 Z9 18 U1 0 U2 0 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON ROAD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 0301-7249 J9 FARADAY DISCUSS JI Faraday Discuss. PY 1998 VL 109 BP 61 EP 69 DI 10.1039/a800074c PG 9 WC Chemistry, Physical SC Chemistry GA 127MB UT WOS:000076353800005 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 Chemistry in cometary comae SO FARADAY DISCUSSIONS LA English DT Article; Proceedings Paper CT General Discussion on Chemistry and Physics of Molecules and Grains in Space CY APR 15-17, 1998 CL UNIV NOTTINGHAM, NOTTINGHAM, ENGLAND HO UNIV NOTTINGHAM ID DENSE INTERSTELLAR CLOUDS; ABUNDANCE RATIO; ORGANIC-MATTER; HCN; MOLECULES; ICE; HNC; TEMPERATURE; ENRICHMENT; DEPLETION AB Significant gas-phase chemistry occurs in the comae of bright comets, as is demonstrated here for the case of Comet Hale-Bopp. The abundance ratio of the two isomers, hydrogen cyanide and hydrogen isocyanide, is shown to vary with heliocentric distance in a way that is consistent with production of HNC by ion-molecule chemistry initiated by the photoionization of water. Likewise, the first maps of emission from HCO+ show an abundance and an extended distribution that are consistent with the same chemical model. 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 55 TC 31 Z9 31 U1 0 U2 1 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-6640 EI 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 1998 VL 109 BP 475 EP 492 DI 10.1039/a709289j PG 18 WC Chemistry, Physical SC Chemistry GA 127MB UT WOS:000076353800028 PM 9809016 ER PT B AU Whigham, DF Lynch, JF AF Whigham, DF Lynch, JF BE Dallmeier, F Comiskey, JA TI Responses of plants and birds to hurricane disturbances in a dry tropical forest of Quintana Roo, Mexico SO FOREST BIODIVERSITY IN NORTH, CENTRAL AND SOUTH AMERICA, AND THE CARIBBEAN: RESEARCH AND MONITORING SE MAN AND THE BIOSPHERE SERIES LA English DT Proceedings Paper CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv ID YUCATAN PENINSULA; CARIBBEAN HURRICANES; PUERTO-RICO; DYNAMICS; PATTERNS; GROWTH; VEGETATION; SOIL C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Whigham, DF (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 28 TC 1 Z9 1 U1 0 U2 4 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-964-5 J9 MAN BIOSPH PY 1998 VL 21 BP 165 EP 186 PG 22 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BM34Q UT WOS:000078438000009 ER PT B AU Dallmeier, F Comiskey, JA Scatena, FN AF Dallmeier, F Comiskey, JA Scatena, FN BE Dallmeier, F Comiskey, JA TI Five years of forest dynamics following Hurricane Hugo in Puerto Rico's Luquillo experimental forest SO FOREST BIODIVERSITY IN NORTH, CENTRAL AND SOUTH AMERICA, AND THE CARIBBEAN: RESEARCH AND MONITORING SE MAN AND THE BIOSPHERE SERIES LA English DT Proceedings Paper CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv ID TROPICAL FOREST; RAIN-FOREST; SUBTROPICAL WET; DAMAGE; TREES; MOUNTAINS; DISTURBANCE; IMPACT; AVAILABILITY; LITTERFALL C1 Smithsonian Inst, SI MAB Biodivers Program, Washington, DC 20560 USA. RP Dallmeier, F (reprint author), Smithsonian Inst, SI MAB Biodivers Program, Quad 3123 MRC 705, Washington, DC 20560 USA. NR 49 TC 6 Z9 6 U1 0 U2 0 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-964-5 J9 MAN BIOSPH PY 1998 VL 21 BP 231 EP 248 PG 18 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BM34Q UT WOS:000078438000012 ER PT B AU Comiskey, JA Dallmeier, F Foster, R AF Comiskey, JA Dallmeier, F Foster, R BE Dallmeier, F Comiskey, JA TI Forest structure and diversity in managed and unmanaged rainforest of Beni, Bolivia SO FOREST BIODIVERSITY IN NORTH, CENTRAL AND SOUTH AMERICA, AND THE CARIBBEAN: RESEARCH AND MONITORING SE MAN AND THE BIOSPHERE SERIES LA English DT Proceedings Paper CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv ID TREE SPECIES RICHNESS; MIDDLE CAQUETA AREA; RAIN-FORESTS; NW AMAZONIA; COLOMBIA; COMMUNITY; PATTERNS C1 Smithsonian Inst, MAB Biodivers Program, Washington, DC 20560 USA. RP Comiskey, JA (reprint author), Smithsonian Inst, MAB Biodivers Program, Quad 3123 MRC 705, Washington, DC 20560 USA. NR 31 TC 5 Z9 5 U1 0 U2 0 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-964-5 J9 MAN BIOSPH PY 1998 VL 21 BP 663 EP 680 PG 18 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BM34Q UT WOS:000078438000035 ER PT B AU Graham, R Dallmeier, F Comiskey, JA AF Graham, R Dallmeier, F Comiskey, JA BE Dallmeier, F Comiskey, JA TI Quantitative ethnobotany: A tool for linking permanent plot research to forest use in the Beni Biosphere Reserve, Bolivia SO FOREST BIODIVERSITY IN NORTH, CENTRAL AND SOUTH AMERICA, AND THE CARIBBEAN: RESEARCH AND MONITORING SE MAN AND THE BIOSPHERE SERIES LA English DT Proceedings Paper CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv ID USEFUL PLANTS; CONSERVATION; VALUATION; TAMBOPATA; PERU C1 Smithsonian Inst, MAB Biodivers Program, Int Ctr, Washington, DC 20560 USA. RP Graham, R (reprint author), Smithsonian Inst, MAB Biodivers Program, Int Ctr, 1100 Jefferson Dr SW, Washington, DC 20560 USA. NR 30 TC 0 Z9 0 U1 0 U2 1 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-964-5 J9 MAN BIOSPH PY 1998 VL 21 BP 701 EP 713 PG 13 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BM34Q UT WOS:000078438000037 ER PT B AU Comiskey, JA Dallmeier, F AF Comiskey, JA Dallmeier, F BE Dallmeier, F Comiskey, JA TI Forest biodiversity research and monitoring in the new world SO FOREST BIODIVERSITY IN NORTH, CENTRAL AND SOUTH AMERICA, AND THE CARIBBEAN: RESEARCH AND MONITORING SE MAN AND THE BIOSPHERE SERIES LA English DT Meeting Abstract CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv C1 Smithsonian Inst, MAB Biodivers Program, Washington, DC 20560 USA. RP Comiskey, JA (reprint author), Smithsonian Inst, MAB Biodivers Program, Quad 3123 MRC 705, Washington, DC 20560 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-964-5 J9 MAN BIOSPH PY 1998 VL 21 BP 749 EP 756 PG 8 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BM34Q UT WOS:000078438000040 ER PT B AU Dallmeier, F Comiskey, JA AF Dallmeier, F Comiskey, JA BE Dallmeier, F Comiskey, JA TI Forest biodiversity assessment, monitoring, and evaluation for adaptive management SO FOREST BIODIVERSITY RESEARCH, MONITORING AND MODELING: CONCEPTUAL BACKGROUND AND OLD WORLD CASE STUDIES SE MAN AND THE BIOSPHERE SERIES LA English DT Proceedings Paper CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv C1 Smithsonian Inst, SI MAB Biodivers Program, Washington, DC 20560 USA. RP Dallmeier, F (reprint author), Smithsonian Inst, SI MAB Biodivers Program, Quad 3123 MRC 705, Washington, DC 20560 USA. NR 0 TC 5 Z9 7 U1 0 U2 1 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-963-7 J9 MAN BIOSPH PY 1998 VL 20 BP 3 EP 15 PG 13 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BL23R UT WOS:000074779600001 ER PT B AU Condit, R Foster, RB Hubbell, SP Sukumar, R Leigh, EG Manokaran, N de Lao, SL LaFrankie, JV Ashton, PS AF Condit, R Foster, RB Hubbell, SP Sukumar, R Leigh, EG Manokaran, N de Lao, SL LaFrankie, JV Ashton, PS BE Dallmeier, F Comiskey, JA TI Assessing forest diversity on small plots: Calibration using species individual curves from 50-ha plots SO FOREST BIODIVERSITY RESEARCH, MONITORING AND MODELING: CONCEPTUAL BACKGROUND AND OLD WORLD CASE STUDIES SE MAN AND THE BIOSPHERE SERIES LA English DT Proceedings Paper CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Condit, R (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 0 TC 39 Z9 41 U1 0 U2 3 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-963-7 J9 MAN BIOSPH PY 1998 VL 20 BP 247 EP 268 PG 22 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BL23R UT WOS:000074779600014 ER PT B AU Hayek, LAC Buzas, MA AF Hayek, LAC Buzas, MA BE Dallmeier, F Comiskey, JA TI SHE analysis: An integrated approach to the analysis of forest biodiversity SO FOREST BIODIVERSITY RESEARCH, MONITORING AND MODELING: CONCEPTUAL BACKGROUND AND OLD WORLD CASE STUDIES SE MAN AND THE BIOSPHERE SERIES LA English DT Proceedings Paper CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv C1 Smithsonian Inst, Washington, DC 20560 USA. RP Hayek, LAC (reprint author), Smithsonian Inst, NHB MRC-136, Washington, DC 20560 USA. NR 0 TC 10 Z9 10 U1 0 U2 0 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-963-7 J9 MAN BIOSPH PY 1998 VL 20 BP 311 EP 321 PG 11 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BL23R UT WOS:000074779600017 ER PT B AU Dallmeier, F Comiskey, JA AF Dallmeier, F Comiskey, JA BE Dallmeier, F Comiskey, JA TI Outlook on forest biodiversity research, monitoring and modeling framework SO FOREST BIODIVERSITY RESEARCH, MONITORING AND MODELING: CONCEPTUAL BACKGROUND AND OLD WORLD CASE STUDIES SE MAN AND THE BIOSPHERE SERIES LA English DT Proceedings Paper CT International Symposium on Measuring and Monitoring Forest Biological Diversity - the International Network of Biodiversity Plots CY MAY 23-25, 1995 CL WASHINGTON, D.C. SP Smithsonian Inst, Man & Biosphere Biodivers Program, Natl Museum Nat Hist, John D & Catherine T MacArthur Fdn, US Man & Biosphere Program, UNESCO, Man & Biosphere Programme, Intl Union Forestry Res Org, Ctr Int Forestry Res, US Natl Pk Serv, US Natl Biol Serv, USDA Forest Serv C1 Smithsonian Inst, SI MAB Divers Program, Washington, DC 20560 USA. RP Dallmeier, F (reprint author), Smithsonian Inst, SI MAB Divers Program, Quad 3123 MRC 705, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU PARTHENON PUBLISHING GROUP LTD PI LANCASTER PA CASTERTON HALL, CARNFORTH, LANCASTER LA6 2LA, ENGLAND BN 1-85070-963-7 J9 MAN BIOSPH PY 1998 VL 20 BP 649 EP 655 PG 7 WC Ecology; Forestry SC Environmental Sciences & Ecology; Forestry GA BL23R UT WOS:000074779600038 ER PT S AU Traub, WA AF Traub, WA BE deHaseth, JA TI Atmospheric FTS SO FOURIER TRANSFORM SPECTROSCOPY SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 11th International Conference on Fourier Transform Spectroscopy (ICOFTS 11) CY AUG 10-15, 1997 CL ATHENS, GA AB The chemical state of the upper atmosphere can be determined from FTS measurements of its infrared thermal emission spectrum. The atmosphere is self-luminous in this band, and can be measured in any direction, day or night. This paper focuses on results from the Smithsonian's far-infrared spectrometer FIRS-2. The techniques of emission and absorption spectroscopy are compared, and the unique features of FIRS-2 discussed. The driving force behind each FIRS-2 flight campaign has been the issue of ozone depletion in the stratosphere. In the Arctic winter vortex we measured large scale chemical change and vertical subsidence of the stratosphere. On a balloon platform we measured the abundances of radical and precursor species which control ozone loss in the middle stratosphere. We show evidence for two cases of "missing chemistry" in the stratosphere. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Traub, WA (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 1-56396-746-4 J9 AIP CONF PROC PY 1998 IS 430 BP 60 EP 73 DI 10.1063/1.55736 PG 14 WC Chemistry, Analytical; Chemistry, Physical; Instruments & Instrumentation; Polymer Science; Spectroscopy SC Chemistry; Instruments & Instrumentation; Polymer Science; Spectroscopy GA BL29A UT WOS:000075012400006 ER PT B AU Romanowsky, AJ AF Romanowsky, AJ BE Zaritsky, D TI Orbit modeling of the lensing galaxy in 0957+561 SO GALACTIC HALOS: A UC SANTA CRUZ WORKSHOP SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Galactic Halos - a UC Santa Cruz Workshop CY AUG 11-15, 1997 CL UNIV CALIF SANTA CRUZ, SANTA CRUZ, CA SP Lick Observ, Natl Sci F, Astron Soc Pacific HO UNIV CALIF SANTA CRUZ AB The gravitational lens system 0957+561 can be used to determine the Hubble constant Ho given an estimate of the lensing galaxy's halo velocity dispersion sigma(0), where H-0 proportional to sigma(0)(2). We employ orbit modeling to study the conversion of a measured central projected stellar velocity dispersion sigma(p) to sigma(0). The model uncertainty is enormous, due to the freedom from the orbit anisotropy variation. Even with the added requirements that the velocity dispersion sigma(p)(R) and fourth-order Gauss-Hermite velocity moment h(4)(R) profiles are similar to those of nearby elliptical galaxies, the resulting uncertainty in H-0, while decreased, is still too large to be useful. 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 1-886733-56-2 J9 ASTR SOC P PY 1998 VL 136 BP 317 EP 319 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74E UT WOS:000076528200060 ER PT J AU Alroy, J AF Alroy, J TI Diachrony of mammalian appearance events: Implications for biochronology SO GEOLOGY LA English DT Article ID RESOLUTION AB A multivariate biochronological analysis of the North American mammal fossil record has established an independent ordering of appearance events for all described genera and species. This geochronologically confirmed hypothesis shows that first and last appearances in different parts of the continent are highly diachronous. Additional results show that (1) despite this diachrony, the new event sequence is compatible with a previously hypothesized sequence of immigrant first appearances; (2) immigrant genera are not particularly widespread, abundant, or synchronous in their appearances; (3) last appearances, large-mammal appearances, and species-level appearances are the most reliable; and (4) most of the observed diachrony appears to result from undersampling. Because diachrony has little effect on the overall multivariate analysis, and because the differences among classes of events are not extreme, joint analyses of all known appearance events are preferable to the a priori selection of particular appearance events as time indicators. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Alroy, J (reprint author), Smithsonian Inst, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. RI Alroy, John/B-4585-2009 NR 15 TC 27 Z9 26 U1 0 U2 1 PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER PI COLLEGE STN PA TEXAS A & M UNIV, DEPT GEOLOGY & GEOPHYSICS, COLLEGE STN, TX 77843-3115 USA SN 0091-7613 J9 GEOLOGY JI Geology PD JAN PY 1998 VL 26 IS 1 BP 23 EP 26 DI 10.1130/0091-7613(1998)026<0023:DOMAEI>2.3.CO;2 PG 4 WC Geology SC Geology GA YR155 UT WOS:000071465600006 ER PT S AU Narita, T Bloser, P Grindlay, J Sudharsanan, R Reiche, C Stenstrom, C AF Narita, T Bloser, P Grindlay, J Sudharsanan, R Reiche, C Stenstrom, C BE Doty, FP Hoover, RB TI Development of prototype pixellated PIN CdZnTe detectors SO HARD X-RAY AND GAMMA-RAY DETECTOR PHYSICS AND APPLICATIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Hard X-Ray and Gamma-Ray Detector Physics and Applications CY JUL 22-23, 1998 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE CdZnTe; PIM; MSM; pixellated-imaging detectors; hard X-ray imaging AB We report initial results from the design and evaluation of two pixellated PIN Cadmium Zinc Telluride detectors and an ASIC-based readout system. The prototype imaging PIN detectors consist of 4 x 4 1.5 mm square indium anode contacts with 0.2 mm spacing and a solid cathode plane on 10 x 10 mm CdZnTe substrates of thickness 2 mm and 5 mm. The detector readout system, based on low noise preamplifier ASICs, allows for parallel readout of all channels upon cathode trigger. This prototype is under development for use in future astrophysical hard X-ray imagers with 10-600 keV energy response. Measurements of the detector uniformity, spatial resolution, and spectral resolution will be discussed and compared with a similar pixellated MSM detector. Finally, a prototype design for a large imaging array is outlined. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narita, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 8 Z9 8 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2901-5 J9 P SOC PHOTO-OPT INS PY 1998 VL 3446 BP 218 EP 227 DI 10.1117/12.312894 PG 10 WC Materials Science, Multidisciplinary; Physics, Nuclear SC Materials Science; Physics GA BM19Z UT WOS:000078010800022 ER PT J AU Thiel, M Stearns, LM Watling, L AF Thiel, M Stearns, LM Watling, L TI Effects of green algal mats on bivalves in a New England mud flat SO HELGOLANDER MEERESUNTERSUCHUNGEN LA English DT Article ID LONG-TERM CHANGES; MACROALGAL MATS; COMMUNITY STRUCTURE; DRIFTING ALGAE; EUTROPHICATION; ACCUMULATIONS; ZOOBENTHOS; RESPONSES; MUDFLATS; SEA AB Concurrent with the spread of green algal mats on tidal flats, reports of macrofauna die-offs under dense algal mats have increased in numbers. Bivalves seem to be particularly affected by persistent dense algal mats. Bivalve species with a long extendible siphon seem to be less affected underneath algal mats, but no distinction has been made in the past between species with short and those with long siphons. We examined effects of green algal mats on two bivalve species with relatively long siphons, Mya arenaria and Macoma balthica, on an intertidal mudflat in New England. Abundances of M. arenaria declined substantially during the study period when a thick green algal mat covered the mudflat for several months. Numbers of the small bivalve Gemma gemma also decreased substantially, whereas abundances of M. balthica showed minimal variation during the time of algal coverage. In algae removal/addition experiments numbers of M, arenaria decreased, but effects were only significant in an algal addition to previously algal-free mudflat areas. Abundance of M. balthica did not change significantly in the algal removal/addition experiments. Over the time period of the experiment (9 weeks), M. arenaria showed measurable size increase in uncovered mudflat areas, but not underneath algal mats. Similarly, M, balthica only increased in size in the uncovered mudflat area. From these results it is concluded that M. balthica can survive time periods of dense algal coverage because it is able to penetrate through the algal mat with its long extendible siphon, and thus can reach well-oxygenated water layers above the mat. M. arenaria with its thick, less extendible, siphon cannot push through dense algal mats and therefore is more likely to die underneath persistent algal mats. C1 Smithsonian Marine Stn, Ft Pierce, FL 34946 USA. Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. RP Thiel, M (reprint author), Smithsonian Marine Stn, 5612 Old Dixie Highway, Ft Pierce, FL 34946 USA. NR 27 TC 11 Z9 12 U1 0 U2 11 PU BIOLOGISCHE ANSTALT HELGOLAND PI BREMERHAVEN PA BIBLIOTHEK COLUMBUSSTR, D-27568 BREMERHAVEN, GERMANY SN 0174-3597 J9 HELGOLANDER MEERESUN JI Helgol. Meeresunters. PY 1998 VL 52 IS 1 BP 15 EP 28 DI 10.1007/BF02908732 PG 14 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 105LQ UT WOS:000075074900002 ER PT S AU Elvis, M AF Elvis, M BE Koyama, K Kitamoto, S Itoh, M TI AXAF in context: A revolution SO HOT UNIVERSE SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 188th Symposium of the International-Astronomical-Union - The Hot Universe CY AUG 26-30, 1997 CL KYOTO, JAPAN SP Int Astron Union C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 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 0-7923-5058-8 J9 IAU SYMP PY 1998 IS 188 BP 79 EP 82 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM04D UT WOS:000077472500018 ER PT S AU Fabbiano, G AF Fabbiano, G BE Koyama, K Kitamoto, S Itoh, M TI Super-Eddington sources in galaxies SO HOT UNIVERSE SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 188th Symposium of the International-Astronomical-Union - The Hot Universe CY AUG 26-30, 1997 CL KYOTO, JAPAN SP Int Astron Union ID X-RAY SOURCES; SPIRAL GALAXIES; M33; EMISSION; OUTBURST; NGC-3628; SN-1978K; NGC-1313; NUCLEUS C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 5 Z9 5 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-5058-8 J9 IAU SYMP PY 1998 IS 188 BP 93 EP 96 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM04D UT WOS:000077472500021 ER PT S AU Torii, K Tsunemi, H Slane, P AF Torii, K Tsunemi, H Slane, P BE Koyama, K Kitamoto, S Itoh, M TI X-ray study of Crab-like and composite SNRs SO HOT UNIVERSE SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 188th Symposium of the International-Astronomical-Union - The Hot Universe CY AUG 26-30, 1997 CL KYOTO, JAPAN SP Int Astron Union ID G292.0+1.8 C1 Osaka Univ, Suita, Osaka 565, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torii, K (reprint author), Osaka Univ, Suita, Osaka 565, Japan. NR 9 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 0-7923-5058-8 J9 IAU SYMP PY 1998 IS 188 BP 258 EP 259 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM04D UT WOS:000077472500073 ER PT J AU Kinzie, RA Banaszak, AT Lesser, MP AF Kinzie, RA Banaszak, AT Lesser, MP TI Effects of ultraviolet radiation on primary productivity in a high altitude tropical lake SO HYDROBIOLOGIA LA English DT Article DE ultraviolet radiation; primary productivity; tropical lakes ID UV-B RADIATION; AMINO-ACIDS; PHYTOPLANKTON PHOTOSYNTHESIS; ANTHOPLEURA-ELEGANTISSIMA; NATURAL PHYTOPLANKTON; ABSORBING COMPOUNDS; OZONE-DEPLETION; MARINE DIATOMS; REEF; INHIBITION AB The aquatic photosynthetic community in Lake Waiau (elev. 3980 m, lat. 19 degrees 48' N) is exposed to intense solar ultraviolet radiation (UVR) due to the high altitude and low latitude. There is a strong negative effect of UVR on photosynthesis both in the planktonic and benthic mat communities in the lake. The mats apparently receive some protection from UVR-absorbing mycosporine-like amino acids (MAAs), while the planktonic primary producers do not appear to have such protection and exhibit no net photosynthesis at levels of UVR characteristic of the lake surface at midday. These forms may be meroplanktonic or rely on vertical mixing for protection from extended periods of exposure to UVR. C1 Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ New Hampshire, Dept Zool, Durham, NH 03824 USA. Univ New Hampshire, Ctr Marine Biol, Durham, NH 03824 USA. RP Kinzie, RA (reprint author), Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA. NR 71 TC 22 Z9 26 U1 0 U2 5 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 385 BP 23 EP 32 DI 10.1023/A:1003489121985 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 183VX UT WOS:000079575800004 ER PT J AU Thiel, M Watling, L AF Thiel, M Watling, L TI Effects of green algal mats on infaunal colonization of a New England mud flat - long-lasting but highly localized effects SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 32nd European Marine Biology Symposium CY AUG 16-22, 1997 CL KRISTINEBERG MARINE RES STN, LYSEKIL, SWEDEN SP Goteborg Univ,Marine Res Ctr, Royal Swedish Acad Sci, Swedish Environm Protect Agcy, Swedish Nat Sci Res Council, Swedish Council Forestry & Agr Res, Community Lysekil, Bohus County Council, Provincial Govt Goteborg & Bohus Ian, Goteborg & Bohus Ian Vattenvardsforbund, EU Objective 2 Reg Fyrstad, Munkedals AB, Preem Environm Fdn, AB Volvo Penta, Akzo Nobel Surface Chem AB, Neste Oxo AB, Borealis AB, Hydro plast AB, Vattenfall Generat Serv AB HO KRISTINEBERG MARINE RES STN DE algal mats; soft-bottom infauna; community change; mud flats; reproduction ID COMMUNITY STRUCTURE; MACROALGAL MATS; LARVAL SETTLEMENT; DRIFTING ALGAE; TERM CHANGES; WADDEN SEA; ESTUARINE; EUTROPHICATION; ACCUMULATIONS; ZOOBENTHOS AB The response of benthic infauna to green algal mats is commonly examined in either small-scale short-term experiments or large-scale long-term data sets that are averaged over large areas. In this study, we used a small-scale approach to study long-term effects caused by the recurring appearance of green algal mats in the early 1990's on a New England mud flat. Algal mats frequently covered the inner parts of the mud flat, where algae persisted for 6 months between July and December, and were incorporated into the sediment after the growth season. These inner parts of the mud hat differed from the outer parts, where green algae never occurred. Between 1979 and 1996, infaunal numbers increased ten-fold at the 37 stations in the inner part, but not at the 19 stations in the outer part of the mud flat. Detritus-feeding annelids primarily contributed to the numerical increase of infaunal colonizers; grazing gastropods and amphipods, and suspension- and filter-feeding bivalves showed no change. The recurring development and deposition of green algae in the inner part of the mud flat resulted in a localized yet persistent change in the infaunal community. The results suggest that it is necessary to follow the fate of algal mars after the growth season. We propose that effects on infaunal colonizers are most severe and long-lasting where decaying algal mats finally become incorporated into the sediment. Brood protecting annelids are most likely to benefit from detrital material provided by moderately dense algal mats. C1 Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. RP Thiel, M (reprint author), Smithsonian Marine Stn, 5612 Old Dixie, Ft Pierce, FL 34946 USA. EM thiel@sms.hboi.edu NR 39 TC 34 Z9 34 U1 1 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 375-76 BP 177 EP 189 DI 10.1023/A:1017040401990 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 137ZZ UT WOS:000076948100016 ER PT J AU Rogers, AD Thorpe, JP Gibson, R Norenburg, JL AF Rogers, AD Thorpe, JP Gibson, R Norenburg, JL TI Genetic differentiation of populations of the common intertidal nemerteans Lineus ruber and Lineus viridis (Nemertea, Anopla) SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 4th International Conference on Nemertean Biology CY JUL 14-19, 1995 CL PACIFIC GROVE, CA DE Heteronemertea; genetic differentiation; North Atlantic ID NATURAL-POPULATIONS; DISPERSAL; INVERTEBRATES; FLOW; HETERONEMERTEA; POLYMORPHISMS; ORGANISMS; DISTANCE; NUCLEAR; WATER AB Specimens of the common intertidal nemerteans Lineus ruber and L. viridis were collected from sites along the west and Southwest coasts of Britain, northern France and North America. Allele frequencies of up to 13 putative enzyme loci were estimated for all populations of L. ruber and L. viridis. Estimates of genetic variation were low for populations of L. ruber (H(obs) 0.008-0.052) but were higher for populations of L. viridis (H(obs) 0.068-0.153). Exact tests for conformity of observed genotype frequencies to those expected under Hardy-Weinberg equilibrium failed to detect significant deviations for L. ruber or L. viridis. F-statistics were affected by small sample size and low expected values in some populations, but, F(ST) was significantly different from zero for most loci examined for both Lineus ruber and L. viridis. This indicated a significant degree of population structuring for both species (only a moderate level of gene-flow). Intraspecific comparisons of genetic distance and genetic identity showed little evidence of genetic differentiation between populations separated by large geographic distances (1000s of km). There was no apparent relationship between genetic distance between populations and the geographic distance separating them. Possible explanations for this lack of genetic differentiation between populations of L. ruber and L. viridis are discussed. These include a lack of variation in the enzyme loci sampled caused by population dynamics, balancing selection in the enzyme loci sampled, large introductions between populations and passive dispersal. C1 Univ Liverpool, Port Erin Marine Lab, Port Erin IM9 6JA, Man, England. Liverpool John Moores Univ, Sch Biol & Earth Sci, Liverpool L3 3AF, Merseyside, England. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Rogers, AD (reprint author), Univ Southampton, Div Biodivers & Ecol, Biomed Sci Bldg,Bassett Crescent E, Southampton SO16 7PX, Hants, England. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 78 TC 4 Z9 4 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 365 BP 1 EP 11 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 114XX UT WOS:000075635400002 ER PT J AU Norenburg, J Roe, P AF Norenburg, J Roe, P TI Special issue: Fourth International Conference on Nemertean Biology - Preface SO HYDROBIOLOGIA LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. Calif State Univ Stanislaus, Dept Biol Sci, Turlock, CA 95382 USA. RP Norenburg, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20560 USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 0 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 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 365 BP IX EP IX PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 114XX UT WOS:000075635400001 ER PT J AU Norenburg, JL Roe, P AF Norenburg, JL Roe, P TI Reproductive biology of several species of recently collected pelagic nemerteans SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 4th International Conference on Nemertean Biology CY JUL 14-19, 1995 CL PACIFIC GROVE, CA DE deep sea; pelagic; nemertean; nurse cell; reproductive strategy ID LIFE-HISTORY; NEMERTINE AB The reproductive biology and morphology of six polystiliferous and one monostiliferous species of pelagic nemerteans was studied in specimens recently collected off California. Depth distributions for these specimens ranged from 250 m to 3250 m, with most specimens obtained between 700 m and 1750 m. Length of sexually mature individuals ranged from 2 mm for the monostiliferan to 61 mm for a male Phallonemertes cf: murrayi. Among P. cf. murrayi and Nectonemertes cf: mirabilis,which yielded the largest specimens studied, mature males were larger than mature females and mature animals were larger than those in which gonads were not apparent. Females typically outnumbered males, although N. cf: mirabilis approached a 1:1 sex ratio. In the polystiliferans studied by light microscopy, accessory ovarian cells appeared to translocate yolk or yolk precursors to oocytes via cytoplasmic bridges, a mechanism typically associated with nurse cells and not previously reported from nemerteans. Mature oocytes 0.5-1 mm in diameter were common, making them very large compared to those of benthic nemerteans. Sperm possessed elongated heads and nuclei. In general, the pelagic nemerteans studied appeared: a) to produce relatively few mature gametes at a time, b) spawn in close proximity to each other, c) undergo iteroparous reproduction, and d) display moderately long-lived life cycles. In addition, data for P. cf. murrayi and possibly N. cf. mirabilis demonstrates potential seasonal peaks in reproductive activity. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. Calif State Univ Stanislaus, Dept Biol Sci, Turlock, CA 95382 USA. RP Norenburg, JL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 39 TC 13 Z9 13 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 365 BP 73 EP 91 PG 19 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 114XX UT WOS:000075635400008 ER PT J AU Crandall, FB Norenburg, JL Gibson, R AF Crandall, FB Norenburg, JL Gibson, R TI Gonadogenesis, embryogenesis, and unusual oocyte origin in Notogaeanemertes folzae Riser, 1988 (Nemertea, Hoplonemertea) SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 4th International Conference on Nemertean Biology CY JUL 14-19, 1995 CL PACIFIC GROVE, CA DE hermaphroditism; viviparity; reproduction; taxonomic redescription ID TERRESTRIAL; EVOLUTION AB Notogaeanemertes folzae Riser, 1988, is a supralittoral hoplonemertean from New Zealand allied to the 'group 1' terrestrial and semiterrestrial genera. The original description noted that it, like a few other 'group 1' forms, is hermaphroditic and that it is viviparous. The present study found that, in addition to testes and ovaries, mature individuals contain mixed gonads, most with testis tissue predominating and some oocytes in various stages of development, but also some of primarily ovarian character with spermatogenic nodules. Oogenesis in this species appears to be unique among nemerteans. Small immature oocytes are found embedded among the ganglionic cells of the lateral nerve cords, from which they appear to erupt and migrate into the parenchyma where differentiation takes place along divergent pathways leading to functional ovaries or testes. No anlagen for gonads, other than the erupting oocytes, have been found. Embryonic development is described and is generally similar to other viviparous nemerteans, except that developing gonads can be found in large embryos. In one case a portion of the sac containing the embryo is comprised of testis tissue. New morphological observations on other organs and tissues of this species are also presented. C1 Turkey Run Res Inst, Mclean, VA 22101 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. Liverpool John Moores Univ, Sch Biol & Earth Sci, Liverpool L3 3AF, Merseyside, England. RP Crandall, FB (reprint author), Turkey Run Res Inst, 900 Turkey Run Rd, Mclean, VA 22101 USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 25 TC 6 Z9 6 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 365 BP 93 EP 107 PG 15 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 114XX UT WOS:000075635400009 ER PT J AU Norenburg, JL Roe, P AF Norenburg, JL Roe, P TI Observations on musculature in pelagic nemerteans and on pseudostriated muscle in nemerteans SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 4th International Conference on Nemertean Biology CY JUL 14-19, 1995 CL PACIFIC GROVE, CALIFORNIA DE nemertea; striated muscle; anatomy; systematics; pelagic; phylogeny ID HOPLONEMERTEANS AB Histological study of 43 pelagic polystiliferans shows that a pseudostriated, or obliquely striated, musculature is a common characteristic of the rhychocoel wall of seven of eight polystiliferan species examined, representing four of five supposedly widely divergent genera. This kind of muscle tissue was previously reported from pelagic hoplonemerteans by Korotkevich, in 1955, but without a clear description. Both her report and the existence of this muscle type have gone unnoticed in subsequent literature. We also document an earlier, unpublished, ultrastructural discovery of pseudostriation in the body wall of a pelagic polystiliferan and report several more instances in our light microscopic material. We describe an overlooked aspect of the proboscis insertion; that is, the inner longitudinal musculature of the proboscis is confluent with the longitudinal musculature of the rhynchocoel, whereas the outer longitudinal muscle of the proboscis extends to the body wall as proboscis fixators. We note that the so-called circular muscle of the rhynchocoel in some species actually comprises crossed diagonal fibers. We report, for the first time, the presence of crossed diagonal musculature in the body wall of some pelagic polystiliferans. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. Calif State Univ Stanislaus, Dept Biol Sci, Turlock, CA 95382 USA. RP Norenburg, JL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 30 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 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 365 BP 109 EP 120 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 114XX UT WOS:000075635400010 ER PT J AU Christy, JH Goshima, S Backwell, PRY Kreuter, TJ AF Christy, JH Goshima, S Backwell, PRY Kreuter, TJ TI Nemertean predation on the tropical fiddler crab Uca musica SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 4th International Conference on Nemertean Biology CY JUL 14-19, 1995 CL PACIFIC GROVE, CALIFORNIA DE hoplonemertean; fiddler crab; predatory behavior; anti-predator defenses; intertidal; Panama ID BIOLOGY AB We saw 79 predatory interactions between a new species of monostiliferous, suctorial hoplonemertean and the fiddler crabs Uca musica (77 cases) and U. stenodactylus (2 cases). At an intertidal sand bar in the Pacific entrance of the Panama Canal, worms ate about 0.1% of the adult crab population per day. The mode of attack and the spatial and temporal distributions of interactions suggest the worm is an ambush predator. When struck by a worm's sticky, mucous-covered proboscis, crabs produced copious foam from their buccal area. Mucous-laden crabs that escaped, again foamed indicating that the foam may counteract the mucus. If the attack led to a kill, the struggling crab soon became quiescent, as is typical in other nemertean-prey interactions. The worm inverted its proboscis, found ingress to the crab's body and fed. Crabs escaped by autotomizing appendages entwined by the proboscis, by forcefully pulling away and by remaining quiescent, then moving away when the worm inverted its proboscis and before it entered the crab. Immobility, a response to visual predators, may falsely indicate paralysis to the worm and cause it to invert its proboscis, thereby providing the crab with an opportunity to escape. This predator-prey interaction seems to incorporate generalized predator tactics and fortuitous prey defenses that give worms and crabs about an even chance of success. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Hokkaido Univ, Fac Fisheries, Dept Biol & Aquaculture, Hakodate, Hokkaido 041, Japan. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RI Backwell, Patricia/C-8883-2009 NR 16 TC 7 Z9 7 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 365 BP 233 EP 239 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 114XX UT WOS:000075635400020 ER PT J AU Thiel, M Zubillaga, GF AF Thiel, M Zubillaga, GF TI The temporal and spatial occurrence of Tetrastemma fozensis (Hoplonemertini) in intertidal bivalves SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 4th International Conference on Nemertean Biology CY JUL 14-19, 1995 CL PACIFIC GROVE, CA DE Scrobicularia plana; Tetrastemma fozensis; intertidal; parasites; pollution ID SCROBICULARIA-PLANA; ESTUARY; SPAIN; SEDIMENT; WATER; POLLUTION; TOXICITY; RIA AB The bivalve Scrobicularia plana, which is commonly found on tidal flats in northwestern Europe, has disappeared from many locations during the past two decades. Its local disappearance has been suspected to be a result of pollution, but other factors such as parasites have also been discussed. The occurrence of Tetrastemma fozensis, a small hoplonemertine inhabiting the mantle cavity of S. plana, was examined in bivalves from six different estuaries in northern Spain. The bivalves are easily collected, and the nemertines leave the bivalves when placed in a small jar with seawater for 72 h. Regular examinations at 6-10 wk intervals of S. plana from the estuary of Plencia revealed that the percentage of bivalves containing nemertines T. fozensis decreased during the summer months, but was above 70% during the rest of the year. In most estuaries about 40-60% of the bivalves contained nemertines, but in March 1994, 100% of the bivalves from the estuary of Hendaye were hosts for nemertines. Nemertines were not found in S. plana from the highly polluted estuary of Bilbao in either March or September 1994. The number of nemertines within individual bivalves was positively correlated with the size of the bivalves in locations where the percentage of bivalves containing nemertines was above 75%. In one estuary where the nemertines disappeared almost completely from the bivalves between March 1994 and September 1994, parasitic copepods appeared within some bivalves in September 1994. The ecology of the nemertine T. fozensis still remains largely unknown, but we suspect that the nemertines may be beneficial for their hosts. C1 Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. Univ Basque Country, Fac Ciencias, Dept Biol Anim & Genet, E-48080 Bilbao, Spain. RP Thiel, M (reprint author), Smithsonian Marine Stn, 5612 Old Dixie Highway, Ft Pierce, FL 34946 USA. NR 26 TC 6 Z9 6 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 365 BP 257 EP 262 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 114XX UT WOS:000075635400023 ER PT J AU Feller, RJ Roe, P Norenburg, JL AF Feller, RJ Roe, P Norenburg, JL TI Dietary immunoassay of pelagic nemerteans by use of cross-reacting polyclonal antibodies: preliminary findings SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 4th International Conference on Nemertean Biology CY JUL 14-19, 1995 CL PACIFIC GROVE, CA DE Nemertea; diet; immunoassay; pelagic; polyclonal antibody ID FOOD WEB ANALYSIS; BIOLOGY; HOPLONEMERTEA; COMMUNITY AB With little data on the diet of pelagic nemerteans, a preliminary immunoassay survey of the gut contents of three species from the Pacific Ocean was performed using non-specific, cross-reacting polyclonal antibodies. Results suggest that Nectonemertes cf. mirabilis, Phallonemertes cf. murrayi, and Cuneonemertes elongata contained somewhat different types of prey. Worms elicited strong responses when probed with antibodies to squid-like mollusks and to mysids and shrimp. Heteropods are more likely ingested than pteropods. Additional studies must be done to confirm these highly suggestive results. C1 Univ S Carolina, Dept Biol Sci, Marine Sci Program, Columbia, SC 29208 USA. Univ S Carolina, Belle W Baruch Inst Marine Biol & Coastal Res, Columbia, SC 29208 USA. Calif State Univ Stanislaus, Dept Biol Sci, Turlock, CA 95382 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20560 USA. RP Feller, RJ (reprint author), Univ S Carolina, Dept Biol Sci, Marine Sci Program, Columbia, SC 29208 USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 23 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PY 1998 VL 365 BP 263 EP 269 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 114XX UT WOS:000075635400024 ER PT B AU Spurr, RJD Chance, K AF Spurr, RJD Chance, K BE Stein, TI TI BIAS: An algorithm for the retrieval of trace gas vertical columns from near-infrared earthshine measurements by the SCIAMACHY spectrometer SO IGARSS '98 - 1998 INTERNATIONAL GEOSCIENCE AND REMOTE SENSING SYMPOSIUM, PROCEEDINGS VOLS 1-5: SENSING AND MANAGING THE ENVIRONMENT SE IEEE International Symposium on Geoscience and Remote Sensing (IGARSS) LA English DT Proceedings Paper CT 1998 International Geoscience and Remote Sensing Symposium (IGARSS 98) on Sensing and Managing the Environment CY JUL 06-10, 1998 CL SEATTLE, WA SP IEEE, Geosci & Remote Sensing Soc, Univ Washington, NASA, NOAA, USN, Off Naval Res, Natl Space Dev Agcy Japan, Int Union Radio Sci C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Spurr, RJD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 50, Cambridge, MA 02138 USA. OI Chance, Kelly/0000-0002-7339-7577 NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-4403-0 J9 INT GEOSCI REMOTE SE PY 1998 BP 2627 EP 2629 DI 10.1109/IGARSS.1998.702300 PG 3 WC Geosciences, Multidisciplinary; Remote Sensing SC Geology; Remote Sensing GA BL34S UT WOS:000075217100848 ER PT S AU Tollestrup, EV Willner, SP AF Tollestrup, EV Willner, SP BE Fowler, AM TI Multiple-beam wide-field infrared cameras for the MMT and Whipple Observatories SO INFRARED ASTRONOMICAL INSTRUMENTATION, PTS 1-2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Conference on Infrared Astronomical Instrumentation CY MAR 23-25, 1998 CL KONA, HI SP Int Soc Opt Engn, European So Observ DE infrared camera; multiple beam camera AB Two wide field, multiple beam, near IR cameras are being developed for the MMT and Whipple Observatories. For the MMT a triple beamed, 1024x1024 pixel camera for the 6.5-m f/5 is being designed. As a prototype for the MMT and for use on the Whipple Observatory 1.2-m telescope, a dual beamed, 256x256 InSb array camera with three selectable magnifications has been built and in use for the past year. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Tollestrup, EV (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2801-9 J9 P SOC PHOTO-OPT INS PY 1998 VL 3354 BP 502 EP 511 DI 10.1117/12.317276 PN 1-2 PG 10 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL60J UT WOS:000075982700056 ER PT S AU Fazio, GG Hora, JL Willner, SP Stauffer, JR Ashby, MLN Wang, Z Tollestrup, EV Pipher, J Forrest, W McCreight, C Moseley, SH Hoffmann, WF Eisenhardt, P Wright, EL AF Fazio, GG Hora, JL Willner, SP Stauffer, JR Ashby, MLN Wang, Z Tollestrup, EV Pipher, J Forrest, W McCreight, C Moseley, SH Hoffmann, WF Eisenhardt, P Wright, EL BE Fowler, AM TI The Infrared Array Camera (IRAC) for the Space Infrared Telescope Facility (SIRTF) SO INFRARED ASTRONOMICAL INSTRUMENTATION, PTS 1-2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Conference on Infrared Astronomical Instrumentation CY MAR 23-25, 1998 CL KONA, HI SP Int Soc Opt Engn, European So Observ DE infrared instrumentation; infrared camera; infrared detectors; astronomy; spacecraft instruments; SIRTF AB The Space Infrared Telescope Facility (SIRTF) contains three focal plane instruments, one of which is the Infrared Array Camera (IRAC). IRAC is a four-channel camera that provides simultaneous 5.12 x 5.12 arcmin images at 3.6, 4.5, 5.8, and 8 microns. The pixel size is 1.2 arcsec in all bands. Two adjacent fields of view in the SIRTF focal plane are viewed by the four channels in pairs (3.6 and 5.8 microns; 4.5 and 8.0 microns). All four detector arrays in the camera are 256 x 256 pixels in size, with the two short wavelength channels using InSb and the two longer wavelength channels using Si:As IBC detectors. The IRAC sensitivities (5 sigma, 200 sec) at 3.6, 4.5, 5.8, and 8.0 microns are 6, 7, 36, and 54 microJanskys, respectively. Two of the most important scientific objectives of IRAC will be to carry out surveys to study galaxy formation and evolution during the early stage of the Universe, and to search for brown dwarfs and superplanets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fazio, GG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hora, Joseph/0000-0002-5599-4650 NR 0 TC 44 Z9 44 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2801-9 J9 P SOC PHOTO-OPT INS PY 1998 VL 3354 BP 1024 EP 1031 DI 10.1117/12.317225 PN 1-2 PG 8 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL60J UT WOS:000075982700112 ER PT J AU Mueller, UG Wcislo, WT AF Mueller, UG Wcislo, WT TI Nesting biology of the fungus-growing ant Cyphomyrmex longiscapus Weber (Attini, Formicidae) SO INSECTES SOCIAUX LA English DT Article DE Cyphomyrmex longiscapus; fungus-growing ants; nesting biology; ant-fungus symbiosis AB The fungus-growing ant Cyphomymrex longiscapus Weber (Attini, Formicidae) exhibits one of the most peculiar nesting habits of all attine ants. It constructs semi-pendant nests resembling miniature swallow nests at vertical embankments or under overhanging logs and fashions entrances with funnel-like "auricles" constructed of clay. The entrance auricle surrounds a large nest opening that exposes the garden and renders it susceptible to desiccation. The distribution of C. longiscapus therefore is limited to wetter habitats. Nests are strictly monogynous. Queenright nests of C. longiscapus can be collected easily because of its conspicuous and shallow nest architecture, making this species an ideal candidate for population surveys of geographic variation in symbiont diversity, garden substrate, or parasitism in a lower attine ant. C1 Univ Maryland, Dept Zool, College Pk, MD 20742 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Mueller, UG (reprint author), Univ Maryland, Dept Zool, College Pk, MD 20742 USA. NR 13 TC 35 Z9 36 U1 1 U2 9 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PY 1998 VL 45 IS 2 BP 181 EP 189 DI 10.1007/s000400050078 PG 9 WC Entomology SC Entomology GA ZU886 UT WOS:000074245800006 ER PT J AU Schultz, TR Bekkevold, D Boomsma, JJ AF Schultz, TR Bekkevold, D Boomsma, JJ TI Acromyrmex insinuator new species: an incipient social parasite of fungus-growing ants SO INSECTES SOCIAUX LA English DT Article DE Acromyrmex; Pseudoatta; social parasitism; fungus-growing ants; Attini ID HYMENOPTERA; FORMICIDAE; EVOLUTION; QUEENS AB The two known social parasites of fungus-growing ants (tribe Attini) occupy an advanced grade of social parasitism characterized by absence of a worker caste and highly derived morphology and behavior. In contrast, the Panamanian Acromyrmex insinuator new species, described here, appears to occupy an early grade of social parasitism in which males, females, and minor workers are nearly indistinguishable from those of the host species. Based on allozyme and morphological evidence, the host, A. octospinosus ssp. echinatior, is clearly different and reproductively isolated from the sympatric A. octospinosus ssp. octospinosus, and is therefore elevated to species status. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 165, Washington, DC 20560 USA. Univ Aarhus, Dept Ecol & Genet, DK-8000 Aarhus, Denmark. RP Schultz, TR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 165, Washington, DC 20560 USA. RI Boomsma, Jacobus/M-2785-2014 OI Boomsma, Jacobus/0000-0002-3598-1609 NR 27 TC 43 Z9 44 U1 0 U2 12 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PY 1998 VL 45 IS 4 BP 457 EP 471 DI 10.1007/s000400050101 PG 15 WC Entomology SC Entomology GA 145EM UT WOS:000077358100007 ER PT J AU Ortner, DJ Mays, S AF Ortner, DJ Mays, S TI Dry-bone manifestations of rickets in infancy and early childhood (Osteoarchaeology, medieval period) SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE rickets; metabolic disease C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. Univ Bradford, Dept Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England. Ancient MOnuments Lab, English Heritage, London W1X 1AB, England. RP Ortner, DJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 7 TC 49 Z9 49 U1 0 U2 6 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX PO19 1UD, ENGLAND SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD JAN-FEB PY 1998 VL 8 IS 1 BP 45 EP 55 DI 10.1002/(SICI)1099-1212(199801/02)8:1<45::AID-OA405>3.0.CO;2-D PG 11 WC Anthropology; Archaeology SC Anthropology; Archaeology GA ZE696 UT WOS:000072821100005 ER PT J AU Early, J AF Early, J TI Memories of Black arts spirits - Kofi Bailey and Atlanta in the 1960s SO INTERNATIONAL REVIEW OF AFRICAN AMERICAN ART LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Early, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 3 TC 1 Z9 1 U1 0 U2 0 PU MUSEUM AFR AMER ART PI LOS ANGELES PA 4005 CRENSHAW BLVD, LOS ANGELES, CA 90008-2534 USA SN 1045-0920 J9 INT REV AFR AM ART JI Int. Rev. Afr. Am. Art PY 1998 VL 15 IS 1 BP 27 EP 30 PG 4 WC Art SC Art GA 100PP UT WOS:000074824800006 ER PT J AU Tudge, CC Jamieson, BGM Sandberg, L Erseus, C AF Tudge, CC Jamieson, BGM Sandberg, L Erseus, C TI Ultrastructure of the mature spermatozoon of the king crab Lithodes maja (Lithodidae, Anomura, Decapoda): further confirmation of a lithodid-pagurid relationship SO INVERTEBRATE BIOLOGY LA English DT Article DE spermatozoa; spermatophore; phylogeny; hermit crabs ID SPERMATOPHORE; PHYLOGENY; CRUSTACEA AB Ultrastructure of the spermatophore and spermatozoon of the king crab Lithodes maja is described and illustrated, The spermatophore is a pedunculate structure of which the major components are the sperm-filled ampulla, stalk, pedestal, and a smaller accessory ampulla at the base of the main ampulla. Each spermatozoon features a subspherical, concentrically zoned acrosomal vesicle, capped by a centrally perforate operculum and posteriorly embedded in the cytoplasm, and a large globular nucleus. Three microtubular arms emerge from the cytoplasm below the acrosomal vesicle. The spermatophores and spermatozoa share many features with those of their nearest postulated relatives-members of the Paguridae (the genus Pagurus in particular), Spermatophore characters that link L. maja with pagurids are the presence of the accessory ampulla (synapomorphy, also with the parapagurids) and the homogeneous granular nature of the spermatophore wall. Sperm characters include the simple concentric zonation of the acrosomal vesicle, the shape and differentiation of the operculum (synapomorphic with Paguridae), the electron-dense plume in the base of the acrosomal chamber (synapomorphy with Pagurus), and absence of microvillar projections in this chamber. Several features in which L. maja differs from species in the genus Pagurus include the central perforation in the operculum, the absence of reticulated acrosome zones, and indications of an irregular flange in some planes of the acrosomal vesicle (possible autapomorphy). C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20560 USA. Univ Queensland, Dept Zool, Brisbane, Qld 4072, Australia. Swedish Museum Nat Hist, Dept Invertebrate Zool, S-10405 Stockholm, Sweden. RP Tudge, CC (reprint author), Museum Victoria, Crustacean Lab, 71 Victoria Crescent, Abbotsford, Vic 3067, Australia. NR 47 TC 20 Z9 21 U1 0 U2 0 PU AMER MICROSCOPICAL SOC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1077-8306 J9 INVERTEBR BIOL JI Invertebr. Biol. PY 1998 VL 117 IS 1 BP 57 EP 66 DI 10.2307/3226852 PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA YV183 UT WOS:000071797700007 ER PT J AU Frick, JE AF Frick, JE TI Evidence of matrotrophy in the viviparous holothuroid echinoderm Synaptula hydriformis SO INVERTEBRATE BIOLOGY LA English DT Article DE reproduction; hermaphrodite; viviparity; ovoviviparity; holothurian ID CUCUMBER LEPTOSYNAPTA-CLARKI; EGG POLARITY; SEA STAR; EVOLUTION; HERMAPHRODITISM; INVERTEBRATES; REPRODUCTION; VERTEBRATES; MECHANISMS; NUTRITION AB Synaptula hydriformis is a holothuroid echinoderm that retains its young in the adult perivisceral coelom. It is also a simultaneous hermaphrodite and is probably self-fertilizing. Eggs are released from the germinal epithelium into the lumen of the ovotestis tubule, and from there into the perivisceral coelom. S. hydriformis is viviparous: eggs are never released to the outside of the adult organism, but develop internally until juveniles are released. It is also matrotrophic: the young rely on the parent to supply nutrition in excess of that supplied by yolk in the egg. The increase in both dry and organic weight from egg to 8-mm juvenile is in excess of 100X. The additional nutrition is supplied as coelomocytes and molecules present in adult coelomic fluid. Brooded juveniles consume naturally occurring particulates and experimentally introduced 50-nm and 1-mu m microspheres from the adult perivisceral coelom. C-14-palmitic acid was also ingested by brooded juveniles and was incorporated into juvenile tissue, indicating that consumed nutrients are metabolized. C1 Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. Smithsonian Marine Stn, Ft Pierce, FL USA. RP Frick, JE (reprint author), Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. EM jefrick@clemson.edu NR 55 TC 17 Z9 17 U1 0 U2 21 PU AMER MICROSCOPICAL SOC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1077-8306 J9 INVERTEBR BIOL JI Invertebr. Biol. PY 1998 VL 117 IS 2 BP 169 EP 179 DI 10.2307/3226968 PG 11 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA ZP483 UT WOS:000073758000008 ER PT J AU Ebert, D AF Ebert, D TI Behavioral asymmetry in relation to body weight and hunger in the tropical social spider Anelosimus eximius (Araneae, Theridiidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article ID DIVISION-OF-LABOR; STEGODYPHUS-MIMOSARUM; PREY CAPTURE; SEX-RATIOS; SIZE; EUSOCIALITY; COOPERATION AB It has been hypothesized that larger females of the social neotropical spider Anelosimus eximius (Keyserling 1884) (family Theridiidae) take advantage of the food captured by smaller females, and thus maintain a higher social rank within a colony. To test this hypothesis, the behavior of adult females in three colonies of A. eximius was observed in the Panama rain forest. Adult spiders with low body weights did most of the building, cleaning and repairing of the communal web, while heavier spiders more often took care of egg sacs. The latter stayed mostly inside safe retreats while low-weight spiders were mostly outside the retreats, where mortality was high. Reproducing spiders were of high body weight. To test whether this behavioral asymmetry is related to the nutritional condition of a female a manipulation experiment was conducted. A comparison of adult females, which were either well fed or starved, showed that starved females do more web maintenance, spend more time outside the retreats and more often take part in attacking prey. I conclude that both hunger (recent feeding success) and general nutritional condition (body weight) are the cues for the observed behavioral asymmetry in colonies of Anelosimus eximius. It is currently unknown whether the observed asymmetry is stable over time or whether it is age-related. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Ebert, D (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. RI Ebert, Dieter/B-5502-2009 OI Ebert, Dieter/0000-0003-2653-3772 NR 32 TC 24 Z9 24 U1 0 U2 10 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 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 1998 VL 26 IS 1 BP 70 EP 80 PG 11 WC Entomology SC Entomology GA 108QG UT WOS:000075276500006 ER PT J AU Eberhard, WG Huber, BA AF Eberhard, WG Huber, BA TI Courtship, copulation, and sperm transfer in Leucauge mariana (araneae, tetragnathidae) with implications for higher classification SO JOURNAL OF ARACHNOLOGY LA English DT Article ID JUMPING SPIDERS ARANEAE; CRYPTIC FEMALE CHOICE; MATING-BEHAVIOR; SEXUAL SELECTION; SALTICIDAE; INSECTS; DISPLAY; BIOLOGY AB The courtship behavior of male Leucauge mariana (Keyserling 1881) spiders that occurred both prior to and during copulation is described, along with the positions and movements of the male genitalia. The great variation in male behavior suggests that it does not function in species recognition. Several kinds of female response an necessary if a male is to successfully inseminate her. Males made two types of insertion, involving different movements of palpal sclerites, and copulations with virgin females differed quantitatively and qualitatively from those with non-virgins. Males deposited encapsulated sperm and other material in an outer chamber of the female's spermatheca early in copulation. Later stages of copulation involved deposition of material on the surface of the female's epigynum that sometimes resulted, with the apparent addition of material by the female, in the formation of a plug on the epigynum. Sperm were decapsulated in the female soon after insemination, perhaps as a result of the action of a female glandular product, and later were found in two other chambers of her spermathecae. Contrary to previous discussions, male and female cheliceral clasping behavior accompanying copulation does not explain why the palpal morphology of these spiders is relatively simple. Cheliceral clasping was similar, though not identical, to that of several other tetragnathine spiders. Cheliceral clasping and details of how male palps engage the female may provide synapomorphies linking Leucauge to tetragnathines. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Eberhard, WG (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 74 TC 46 Z9 49 U1 0 U2 11 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 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 1998 VL 26 IS 3 BP 342 EP 368 PG 27 WC Entomology SC Entomology GA 154PT UT WOS:000077898000010 ER PT J AU Kharchenko, V Balakrishnan, N Dalgarno, A AF Kharchenko, V Balakrishnan, N Dalgarno, A TI Thermalization of fast nitrogen atoms in elastic and inelastic collisions with molecules of atmospheric gases SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article ID TERRESTRIAL THERMOSPHERE; ENERGY-TRANSFER; KINETICS AB The energy relaxation of fast nitrogen atoms due to elastic and inelastic collisions with molecules in the atmosphere is studied. A new formula for the energy relaxation kernel in the Boltzmann kinetic equation, which applies equally to elastic and inelastic collisions, is derived. Angular and energy dependent differential cross sections are used in calculations of the energy transfer rate. The energy relaxation kernel is evaluated for inelastic N+N-2 collisions with numerically determined differential cross sections for rotational and vibrational excitation of the N-2 molecules. The mean rate of energy loss, the average energy transfer per collision and mean thermalization times are calculated as functions of the kinetic energy of the nitrogen atoms. The contributions of elastic and inelastic scattering to the thermalization of N atoms in the terrestrial atmosphere are analyzed. The energy distribution functions of the fast nitrogen atoms are evaluated for thermospheric conditions. They depart significantly from a Maxwellian distribution at high energies. (C) 1998 Elsevier Science Ltd. Al rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Kharchenko, V (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 24 TC 26 Z9 26 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD JAN PY 1998 VL 60 IS 1 BP 95 EP 106 DI 10.1016/S1364-6826(97)82763-0 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA YX888 UT WOS:000072090300010 ER PT J AU Liu, CJ Olsson, RK Huber, BT AF Liu, CJ Olsson, RK Huber, BT TI A benthic paleohabitat for Praepararotalia gen. nov. and Antarcticella Loeblich and Tappan SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID CARBON ISOTOPIC COMPOSITION; PLANKTONIC-FORAMINIFERA; PALEOCEANOGRAPHIC SIGNIFICANCE; EXTINCTION EVENT; MASS EXTINCTION; OXYGEN; SEA; OCEAN; PALEOECOLOGY; SEDIMENT AB Globorotalia inconspicua Howe, G. aculeata Jenkins, G. perclara Loeblich and Tappan (senior synonym of G, reissi Loeblich and Tappan), Globigerina pauciloculata Jenkins, and Candeina antarctica Leckie and Webb are Cenozoic species interpreted to have been adapted to a planktic habitat. Their restriction, however, to shallow marine or marginal marine paleoenvironments suggests that they were benthic species. These taxa are associated with reduced planktic foraminiferal diversity, a low P/B (planktic/benthic) ratio, and an inner shelf benthic foraminiferal biofacies. A new genus, Praepararotalia, is erected for several species interpreted to be phylogenetically related to the benthic genus Pararotalia, Praepararotalia cretacea (new species), which is described from the Maastrichtian Navesink Formation in New Jersey, gave rise to the early Paleocene species Praepararotalia perclara. In addition, stable isotopic (delta(18)O and delta(13)C) Signatures of all praepararotaliid species in this study cluster closer to benthic foraminiferal signatures and are distinct from normal marine planktic taxa from the Cretaceous and the Paleocene. A benthic paleohabitat is suggested for the Danian species Antarcticella pauciloculata (Jenkins) because of its dominant occurrence in shallow facies of marginal basins in the southern high latitudes. The species may be phylogenetically linked to P. cretacea n. sp. and is apparently the stem taxon of a Southern Ocean Paleogene evolutionary lineage that includes A, cecionii (Canon and Ernst), A. zeocenica (Hornibrook and Jenkins), and A, antarctica (Leckie and Webb). C1 Rutgers State Univ, Dept Geol Sci, New Brunswick, NJ 08903 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Liu, CJ (reprint author), Rutgers State Univ, Dept Geol Sci, New Brunswick, NJ 08903 USA. NR 69 TC 29 Z9 30 U1 0 U2 2 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD JAN PY 1998 VL 28 IS 1 BP 3 EP 18 PG 16 WC Paleontology SC Paleontology GA YT878 UT WOS:000071655200002 ER PT J AU Gribble, RF Stern, RJ Newman, S Bloomer, SH O'Hearn, T AF Gribble, RF Stern, RJ Newman, S Bloomer, SH O'Hearn, T TI Chemical and isotopic composition of lavas from the Northern Mariana Trough: Implications for magmagenesis in back-arc basins SO JOURNAL OF PETROLOGY LA English DT Article DE arc magma; back-arc basin basalt; isotope geochemistry; Mariana Islands; trace elements ID MAGMATIC EVOLUTION; VOLCANIC-ROCKS; TRACE-ELEMENT; ISLAND ARC; SHOSHONITIC VOLCANISM; SUBMARINE LAVAS; MARGINAL BASINS; WESTERN PACIFIC; PHILIPPINE SEA; BASALTS AB We report the results of a geochemical and isotopic study of mostly basaltic glasses recovered from 25 dredge stations along the northernmost 500 km of the Mariana Trough extension axis. The distribution of samples links regions of seafloor spreading to the south with regions farther north where a progression of rifting styles accompanies the earliest stages of bark-arc basin extension. Petrographic, chemical and isotopic compositions of igneous rocks reflect the changing styles of extension, with typical back-arc basin basalts in the south which become increasingly similar to arc lavas to the north. Felsic lavas also appear along the extensional axis in the north. Glassy, sparsely phyric basalts characterize regions of seafloor spreading. Felsic lavas and porphyritic basalts occur in the northern, rifting portion. Geochemical and isotopic compositions distinguish between mature an portions (Ce/Pb <10, Ba/La >20; Pb-206/Pb-204 >18.5, Sr-87/Sr-86 >0.7032, epsilon(Nd) < + 8) and regions of back-arc spreading (Ce/Pb >10, Ba/La <20; Pb-206/Pb-204 <18.9, Sr-87/Sr-86 <0.7032, epsilon(Nd) > + 7). Samples from along the extensional axis of the northern Mariana Trough show progressive changes in chemical and isotopic compositions, from back-arc basin basalts that formed by seafloor spreading northward through increasingly arc-like basalts, until lavas that are in distinguishable from arc lavas are encountered in the northernmost portion of the rift. Batch-melting models indicate that northernmost degrees of melting, with 13 +/- 5% melting where seafloor spreading occurs, doubling to 28 +/- 8% for the northernmost part of the rift axis. The greater degree of melting in the north reflects the greater amount of water added to the mantle source, reflecting the arc-like nature of the source region and melt generation style characteristic of the initial stages of back-arc basin formation. Our data indicate that F = 0.44W + 0.07, where F is the degree of mantle melting and W is the percent water in the mantle. 'True' back-arc basin basalts are generated by adiabatic decompression associated with mantle upwelling in mature extensional settings. Eruption of 'true' bark-arc basin basalts accompanies seafloor spreading, which begins when the basin is 100-150 km wide. The arc is disrupted during early rift formation, because arc magmatism is captured by the extension axis, but the generation of an melts by hydrous melting of the mantle wedge continues whether or not back-an extension is occurring. Back-arc basin seafloor spreading requires development of an upwelling mantle flow regime, allowing melting by adiabatic decompression, similar to that responsible for mid-ocean ridge basalt (MORB). The arc begins to re-form once extension progresses nearly to the point of seafloor spreading. C1 Univ Texas, Ctr Lithospher Studies, Richardson, TX 75083 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Oregon State Univ, Dept Geosci, Corvallis, OR 97331 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Stern, RJ (reprint author), Univ Texas, Ctr Lithospher Studies, POB 830688, Richardson, TX 75083 USA. NR 82 TC 180 Z9 194 U1 1 U2 21 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 J9 J PETROL JI J. Petrol. PD JAN PY 1998 VL 39 IS 1 BP 125 EP 154 DI 10.1093/petrology/39.1.125 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA YW400 UT WOS:000071931500005 ER PT J AU Jewgenow, K Penfold, LM Meyer, HHD Wildt, DE AF Jewgenow, K Penfold, LM Meyer, HHD Wildt, DE TI Viability of small preantral ovarian follicles from domestic cats after cryoprotectant exposure and cryopreservation SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID OOCYTES FOLLOWING CRYOPRESERVATION; IN-VITRO; MOUSE OOCYTES; FOLLICULAR OOCYTES; FERTILIZATION INVITRO; MATURATION; OOGENESIS; 1,2-PROPANEDIOL; COMPETENCE; SPINDLE AB About 1500 preantral follicles can be recovered from a single cat ovary by mechanical dissection. This is a potentially rich source of genetic material if ova could be preserved and grown in vitro, especially from rare or endangered species that die abruptly or are ovariectomized for medical reasons. The aims of this study were to examine cryoprotectant toxicity and then the potential of successfully cryopreserving preantral cat follicles. In the initial toxicity trial, isolated cat follicles (40-90 mu m) were exposed to dimethylsulfoxide, glycerol, 1,2-propandiol or ethylene glycol at 0 degrees C for 15 min. Follicle viability was assessed by supravital staining using a combination of Trypan blue and Hoechst 33258 at 0 h, and after 18 h and 1 week of culture. Percentages of follicles with intact oocytes and granulosa cells were similar (P > 0.05) among control (no cryoprotectant), dimethylsulfoxide, 1,2-propandiol and ethylene glycol treatments at all time points, but were reduced (P < 0.05) after glycerol exposure. On the basis of this finding, dimethylsulfoxide and 1,2-propandiol were used to cryopreserve intact follicles, and post-thaw viability was assessed by supravital staining and 5-bromo-2'-deoxyuridine uptake into oocytes and granulosa cells during culture. Of control (noncryopreserved) follicles, 31.4%+/-2.9%, 18.8%+/-1.9% and 16.2%+/-1.6% were intact after 0 h, 18 h and 1 week of culture, respectively. Uptake of 5-bromo-2'-deoxyuridine occurred in approximately 20% of follicles at all time points. On the basis of the presence of both a healthy oocyte and granulosa cells, cryopreservation in dimethylsulfoxide or 1,2-propandiol allowed approximately 19% of follicles to survive. Approximately 10% demonstrated clear evidence of cell activity that was sustainable for I week. In conclusion, the cat ovary contains a population of: preantral follicles that are not adversely affected by short-term exposure to most conventional cryoprotectants. Furthermore, there is a subpopulation of these follicles capable of surviving cryopreservation, remaining structurally intact and physiologically active after thawing. C1 Inst Zoo Biol & Wildlife Res, D-10252 Berlin, Germany. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Jewgenow, K (reprint author), Inst Zoo Biol & Wildlife Res, PF 1103, D-10252 Berlin, Germany. NR 42 TC 50 Z9 56 U1 1 U2 2 PU SOC REPRODUCTION FERTILITY PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE CB5 8DT, ENGLAND SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD JAN PY 1998 VL 112 IS 1 BP 39 EP 47 PG 9 WC Reproductive Biology SC Reproductive Biology GA ZA429 UT WOS:000072340100005 PM 9538328 ER PT J AU Early, E Thompson, A Johnson, C DeLuisi, J Disterhoft, P Wardle, D Wu, E Mou, WF Sun, YC Lucas, T Mestechkina, T Harrison, L Berndt, J Hayes, D AF Early, E Thompson, A Johnson, C DeLuisi, J Disterhoft, P Wardle, D Wu, E Mou, WF Sun, YC Lucas, T Mestechkina, T Harrison, L Berndt, J Hayes, D TI The 1995 North American Interagency Intercomparison of Ultraviolet Monitoring Spectroradiometers SO JOURNAL OF RESEARCH OF THE NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY LA English DT Article DE environmental monitoring; intercomparison; solar ultraviolet; spectroradiometers ID MERCURY PENCIL LAMPS; SPECTRAL-LINES AB Concern over stratospheric ozone depletion has prompted several government agencies in North America to establish networks of spectroradiometers for monitoring solar ultraviolet irradiance at the surface of the Earth. To assess the ability of spectroradiometers to accurately measure solar ultraviolet irradiance, and to compare the results between instruments of different monitoring networks, the second North American Intercomparison of Ultraviolet Monitoring Spectroradiometers was held June 12 to 23, 1995 at Table Mountain outside Boulder, Colorado, USA. This Intercomparison was coordinated by the National Institute of Standards and Technology (NIST) and the National Oceanic and Atmospheric Administration (NOAA). Participating agencies were the Environmental Protection Agency; the National Science Foundation; the Smithsonian Environmental Research Center; the Department of Agriculture; and the Atmospheric Environment Service, Canada. Instruments were characterized for wavelength uncertainty, bandwidth, stray-light rejection, and spectral irradiance responsivity, the latter with a NIST standard lamp operating in a specially designed field calibration unit. The spectral irradiance responsivity, determined once indoors and twice outdoors, demonstrated that while the responsivities changed upon moving the instruments, they were relatively stable when the instruments remained outdoors. Synchronized spectral scans of the solar irradiance were performed over several days. Using the spectral irradiance responsivities determined with the NIST standard lamp and three different convolution functions to account for the different bandwidths of the instruments, the measured solar irradiances generally agreed to within 3 %. C1 NIST, Gaithersburg, MD 20899 USA. NOAA, Boulder, CO 80303 USA. Environm Canada, Atomospher Environm Serv, Toronto, ON M3H 5T4, Canada. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Biospher Inc, San Diego, CA 92110 USA. SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12205 USA. Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. RP Early, E (reprint author), NIST, Gaithersburg, MD 20899 USA. NR 10 TC 26 Z9 26 U1 0 U2 1 PU US GOVERNMENT PRINTING OFFICE PI WASHINGTON PA SUPERINTENDENT DOCUMENTS,, WASHINGTON, DC 20402-9325 USA SN 1044-677X J9 J RES NATL INST STAN JI J. Res. Natl. Inst. Stand. Technol. PD JAN-FEB PY 1998 VL 103 IS 1 BP 15 EP 62 DI 10.6028/jres.103.002 PG 48 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA ZD982 UT WOS:000072745200002 PM 28009371 ER PT J AU Macintyre, IG Reid, RP AF Macintyre, IG Reid, RP TI Recrystallization in living porcelaneous foraminifera (Archaias angulatis): Textural changes without mineralogic alteration SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article ID CALCITE; DIAGENESIS AB Mineralogic stabilization of porcelaneous foraminifera has been cited as an example of diagenesis in which chemical change occurs without any textural alteration. In contrast, our study of living specimens of a common species of this group, Archaias angulatis, indicates a sequence in which textural alteration of the magnesium calcite skeleton occurs without loss of magnesium from the test, In samples of A, angulatis from Florida Bag, Florida, skeletal rods (1-2 mu m long and 0.1 mu m wide) are extensively recrystallized to dense minimicrite (0.05-0.1 mu m anhedral equant crystals), Both rods and minimicrite contain 9-11.5 mole % MgCO3. Micritization increases with age of the skeletons and occurs more rapidly in septal and basal walls than in lateral walls and pillars, Recrystallization could be due to change in the partial pressure of CO2 resulting from changing distributional patterns of respiration and photosynthesis of algal symbionts. Recrystallization within living foraminifera has important implications for studies of fossil diagenesis and biomineralization. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. RP Macintyre, IG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. NR 26 TC 25 Z9 28 U1 0 U2 1 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 1731 E 71ST STREET, TULSA, OK 74136-5108 USA SN 1073-130X J9 J SEDIMENT RES JI J. Sediment. Res. PD JAN PY 1998 VL 68 IS 1 BP 11 EP 19 PN A PG 9 WC Geology SC Geology GA YT303 UT WOS:000071587200004 ER PT J AU McGovern, CF AF McGovern, CF TI Acquired of the angels: The lives and works of master guitar makers John D'Angelico and James L. D'Aquisto SO JOURNAL OF THE AMERICAN MUSICAL INSTRUMENT SOCIETY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP McGovern, CF (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER MUSIC INSTRUMENT SOC PI HEMPSTEAD PA MUSIC DEPT, EMILY LOWE HALL 112 HOFSTRA UNIVERSITY, HEMPSTEAD, NY 11362 USA SN 0362-3300 J9 J AM MUSIC INSTRUM S JI J. Am. Music. Instrum. Soc. PY 1998 VL 24 BP 154 EP 156 PG 3 WC Music SC Music GA 136TG UT WOS:000076874800009 ER PT J AU McGovern, CF AF McGovern, CF TI Great guitars SO JOURNAL OF THE AMERICAN MUSICAL INSTRUMENT SOCIETY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP McGovern, CF (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER MUSIC INSTRUMENT SOC PI HEMPSTEAD PA MUSIC DEPT, EMILY LOWE HALL 112 HOFSTRA UNIVERSITY, HEMPSTEAD, NY 11362 USA SN 0362-3300 J9 J AM MUSIC INSTRUM S JI J. Am. Music. Instrum. Soc. PY 1998 VL 24 BP 154 EP 156 PG 3 WC Music SC Music GA 136TG UT WOS:000076874800008 ER PT J AU Pessier, AP Hamilton, VT Foreyt, WJ Parish, S McElwain, TL AF Pessier, AP Hamilton, VT Foreyt, WJ Parish, S McElwain, TL TI Probable elaeophorosis in a moose (Alces alces) from eastern Washington state SO JOURNAL OF VETERINARY DIAGNOSTIC INVESTIGATION LA English DT Article C1 Washington State Univ, Dept Vet Microbiol & Pathol, Pullman, WA 99164 USA. Washington State Univ, Dept Vet Clin Sci, Pullman, WA 99164 USA. Washington State Univ, Washington Anim Dis Diagnost Lab, Pullman, WA 99164 USA. RP Pessier, AP (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Pathol, Washington, DC 20008 USA. NR 5 TC 2 Z9 3 U1 0 U2 2 PU AMER ASSOC VETERINARY LABORATORY DIAGNOSTICIANS INC PI TURLOCK PA PO BOX 1522, TURLOCK, CA 95381 USA SN 1040-6387 J9 J VET DIAGN INVEST JI J. Vet. Diagn. Invest. PD JAN PY 1998 VL 10 IS 1 BP 82 EP 84 PG 3 WC Veterinary Sciences SC Veterinary Sciences GA ZE267 UT WOS:000072774900014 PM 9526866 ER PT J AU Garrott, RA Monfort, SL White, PJ Mashburn, KL Cook, JG AF Garrott, RA Monfort, SL White, PJ Mashburn, KL Cook, JG TI One-sample pregnancy diagnosis in elk using fecal steroid metabolites SO JOURNAL OF WILDLIFE DISEASES LA English DT Article DE Cervus elaphus; physiology; radioimmunoassay; reproduction; techniques ID PAPIO-CYNOCEPHALUS-CYNOCEPHALUS; FREE-RANGING ELK; FECES; URINARY; SNOW AB Recent research has demonstrated the potential of pregnancy diagnosis in elk (Cervus elaphus nelsoni) using immunoassays of fecal steroid concentration. However, multiple samples are required to insure accurate results, limiting its utility for free-ranging animals. We attempted to develop an accurate one-sample pregnancy diagnosis using 153 fecal samples that were collected from free-ranging, radio-collared, adult female elk in Yellowstone National Park (Wyoming, USA) and from captive elk maintained at the Starkey Research Facility (La Grande, Oregon, USA) February through April 1992 and 1997. The pregnancy status of each animal was diagnosed using serum pregnancy-specific protein B (PSPB) assays providing fecal samples from 38 nonpregnant and 115 pregnant animals. Fecal radioimmunoassay (RIA) indicated that mean (+/-SD) progestagens (P-4) were elevated significantly in pregnant (2.96 +/- 1.49 mu g/gm) compared to nonpregnant (0.43 +/- 0.26 mu g/gm) individuals. Confidence intervals (1.96 +/- SE) for the two groups were widely separated (nonpregnant 0.34-0.51, pregnant 2.69-3.24) with little overlap in the range of concentrations measured for each group (nonpregnant 0.09-0.98, pregnant 0.90-8.29). These results indicate that fecal progestagens RIA provides a reliable method of noninvasive pregnancy diagnosis using single fecal samples collected from elk during late gestation. However, independent validation of the suggested discrimination criteria should be performed before routine application. C1 Montana State Univ, Dept Biol, Bozeman, MT 59717 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. Calif Polytech State Univ Fdn, Dept Biol Sci, San Luis Obispo, CA 93451 USA. Natl Council Paper Ind Air & Stream Improvement, Forestry & Range Sci Lab, La Grande, OR 97850 USA. RP Garrott, RA (reprint author), Montana State Univ, Dept Biol, 310 Lewis Hall, Bozeman, MT 59717 USA. NR 19 TC 28 Z9 29 U1 1 U2 2 PU WILDLIFE DISEASE ASSN, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD JAN PY 1998 VL 34 IS 1 BP 126 EP 131 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA YU630 UT WOS:000071737800014 PM 9476233 ER PT B AU Eichhorn, G AF Eichhorn, G BE Grothkopf, U Andernach, H StevensRayburn, S Gomez, M TI Linking in the astrophysics data system SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY III (LISA III) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Library and Information Services in Astronomy III (LISA III) CY APR 21-24, 1998 CL PUERTO LA CRUZ, SPAIN SP Astron Soc Pacific, Ayuntamiento Orotava, Cabildo Insular Tenerife, Universidades & Investigac Gobierno Canarias, Direcc Gen, European Union, Iberia, Patronato Turismo Cabildo La Palma, Patronato Turismo Cabildo Insular Tenerife AB The Astrophysics Data System (ADS) provides access to references, abstracts and full journal articles of the Astronomy/Astrophysics, Space Instrumentation, and Physics/Geophysics literature. The Astrophysics Data System is part of an Astronomy-wide collaboration called Urania. The members of this collaboration make a variety of information available on-line and provide cross-links between their data holdings and other information providers. This allows the users of this system to easily find related information, regardless of where they start. The ADS can be accessed at: http://adswww.harvard.edu/. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Eichhorn, G (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 NR 3 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 1-886733-73-2 J9 ASTR SOC P PY 1998 VL 153 BP 118 EP 125 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM36G UT WOS:000078497400015 ER PT B AU Eichhorn, G Accomazzi, A Kurtz, MJ Grant, CS AF Eichhorn, G Accomazzi, A Kurtz, MJ Grant, CS BE Grothkopf, U Andernach, H StevensRayburn, S Gomez, M TI The Astrophysics Data System SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY III (LISA III) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Library and Information Services in Astronomy III (LISA III) CY APR 21-24, 1998 CL PUERTO LA CRUZ, SPAIN SP Astron Soc Pacific, Ayuntamiento Orotava, Cabildo Insular Tenerife, Universidades & Investigac Gobierno Canarias, Direcc Gen, European Union, Iberia, Patronato Turismo Cabildo La Palma, Patronato Turismo Cabildo Insular Tenerife AB The NASA Astrophysics Data System has been very successful in providing the researcher and librarian the capability to effectively search the astronomical and space science literature from their desktop. It currently provides access to four searchable databases of scientific bibliographic references and a large archive of full-text documents which includes all the major astronomical journals. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Eichhorn, G (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 NR 2 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 1-886733-73-2 J9 ASTR SOC P PY 1998 VL 153 BP 277 EP 280 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM36G UT WOS:000078497400037 ER PT B AU Kurtz, MJ Eichhorn, G AF Kurtz, MJ Eichhorn, G BE Grothkopf, U Andernach, H StevensRayburn, S Gomez, M TI The historical literature of astronomy, via ADS SO LIBRARY AND INFORMATION SERVICES IN ASTRONOMY III (LISA III) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Library and Information Services in Astronomy III (LISA III) CY APR 21-24, 1998 CL PUERTO LA CRUZ, SPAIN SP Astron Soc Pacific, Ayuntamiento Orotava, Cabildo Insular Tenerife, Universidades & Investigac Gobierno Canarias, Direcc Gen, European Union, Iberia, Patronato Turismo Cabildo La Palma, Patronato Turismo Cabildo Insular Tenerife AB Nearly every working astronomer now uses the NASA Astrophysics Data System Abstract Service regularly to access the modern technical literature. The ADS has begun a long term project to put the most important historical literature of astronomy on-line. This paper presents a progress report, details our short term goals, and requests the assistance of astronomical bibliophiles to make the collection complete and useful. The ADS can be reached at: http://adswww.harvard.edu/. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kurtz, MJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 NR 5 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 1-886733-73-2 J9 ASTR SOC P PY 1998 VL 153 BP 293 EP 296 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM36G UT WOS:000078497400041 ER PT J AU Hosack, DA Miller, KV Marchinton, RL Wemmer, CM Monfort, SL AF Hosack, DA Miller, KV Marchinton, RL Wemmer, CM Monfort, SL TI Stag exposure augments urinary progestagen excretion in Eld's Deer hinds Cervus eldi thamin SO MAMMALIA LA English DT Article ID AUSTRALIAN CASHMERE GOAT; LUTEAL PHASE DEFECTS; RED DEER; SCENT-URINATION; PROGESTERONE; OVARIAN; EWES; STIMULATION; PHEROMONES; ANESTRUS AB This 2-year study investigated Eld's deer (Cervus eldi thamin) stag influences on ovarian activity of hinds. Immunoreactive urinary pregnanediol-3 alpha-glucuronide (PdG) excretion was used to characterize ovarian activity patterns. Results from Year 1 studies revealed that females exposed to stag urine increased (P<0.05) progesterone metabolites during the first three estrous cycles of the reproductive season, compared to non-urine exposed hinds. Due to experimental design limitations, the unequivocal importance of urine could not be established. Year 2 studies sought to answer a more basic question: Does male presence or absence affect estrous cyclicity in Eld's deer? Compared to hinds maintained in complete isolation from stags, PdG excretion during the first two seasonal estrous cycles was increased (P<0.05) in hinds maintained in either a mixed-sex barn setting or housed continuously with a single stag. The increase in urinary progesterone excretion during the luteal phase of the estrous cycle was manifested as an increase in magnitude, rather than an increase in the length of the luteal phase. These data suggest that the reproductive axis of female Eld's deer is sensitive to male presence, and suggests a mechanism whereby stags may enhance fertility in hinds. C1 Univ Georgia, Sch Forest Resources, Athens, GA 30602 USA. Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Washington, DC 20560 USA. RP Hosack, DA (reprint author), Univ Georgia, Sch Forest Resources, Athens, GA 30602 USA. NR 48 TC 1 Z9 1 U1 2 U2 4 PU MUSEUM NAT HIST NATURELLE PI PARIS PA 55 RUE DE BUFFON, 75005 PARIS, FRANCE SN 0025-1461 J9 MAMMALIA JI Mammalia PY 1998 VL 62 IS 3 BP 341 EP 350 DI 10.1515/mamm.1998.62.3.341 PG 10 WC Zoology SC Zoology GA 156GD UT WOS:000077992500002 ER PT J AU Christy, JH Morgan, SG AF Christy, JH Morgan, SG TI Estuarine immigration by crab postlarvae: mechanisms, reliability and adaptive significance SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE larval migration; crab postlarvae; estuary; nocturnal flood tide immigration ID FLOOD-TIDE TRANSPORT; BLUE-CRAB; CALLINECTES-SAPIDUS; CHESAPEAKE BAY; YORK-RIVER; BRACHYURAN MEGALOPAE; LARVAL RELEASE; NORTH-CAROLINA; FIDDLER-CRABS; PLANKTONIC AVAILABILITY AB Most estuarine crab larvae emigrate from estuaries soon after they hatch. develop to the postlarval stage in the coastal ocean and then immigrate to estuaries and settle in adult habitats. We studied the patterns and mechanisms of immigration by postlarvae of 9 crab taxa in the small, high-salinity North Inlet estuary (South Carolina, USA) by sampling the plankton daily for 32 d over the length of the estuary. A concurrent study of larval production and flux showed that all taxa rapidly emigrate, thereby establishing empirically the importance of immigration in this estuary and giving us the rare opportunity to compare the relative species abundance of emigrating larvae and immigrating postlarvae. Contrary to the popular view that planktonic development in the sea uncouples larval recruitment from production, the community composition of emigrants and immigrants were comparable. Postlarvae immigrated at night and primarily on large amplitude flood tides. We show that this pattern is common in other estuaries and we argue that it reduces fish predation on immigrating postlarvae. Saltatory, up-estuary immigration was evident in 5 species that moved from the lower to the upper estuary (4 km) in 1 to 3 d. Although immigration rates have not been measured directly in other estuaries, a study of postlarval settlement in Mobile Bay suggests that rates may vary geographically in relation to variation in the tidal regime. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. EM christyj@naos.si.edu NR 87 TC 59 Z9 61 U1 0 U2 6 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 1998 VL 174 BP 51 EP 65 DI 10.3354/meps174051 PG 15 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 152XB UT WOS:000077801500005 ER PT J AU Guzman, HM Tudhope, AW AF Guzman, HM Tudhope, AW TI Seasonal variation in skeletal extension rate and stable isotopic (C-13/C-12 and O-18/O-16) composition in response to several environmental variables in the Caribbean reef coral Siderastrea siderea SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE coral skeleton; stable isotopes; panama; reefs ID DENSITY BAND FORMATION; MAJOR OIL-SPILL; SOUTHERN-OSCILLATION; SCLERACTINIAN CORALS; COSTA-RICA; RED-SEA; BIOLOGICAL CARBONATES; MONTASTREA-ANNULARIS; FRINGING REEF; GROWTH AB The potential of the massive reef building coral Siderastrea siderea to be a reliable archive of past environmental variations was investigated by means of a field experiment conducted on a fringing reef in Panama. Over a 14 mo experimental period, 5 closely spaced and shallow subtidal coral colonies were cored at 1 mo intervals. These cores were subsequently analysed to determine linear extension (growth) and the delta(13)C and delta(18)O of each monthly growth increment. Environmental conditions were recorded continuously by instruments deployed within a distance of 10 to 110 m from the corals. The environmental variables sea surface temperature (SST), salinity, wind, sun and rainfall were all well correlated with one another, reflecting the dominant seasonal cycle in the region. Of the 3 skeletal attributes considered in this study, skeletal delta(18)O showed the strongest correlation with this seasonal cycle. The seasonal variations in skeletal delta(18)O are attributed to changes in SST (accounting for ca 60 % of the delta(18)O signal) and inferred changes in water isotopic composition due to rainfall and runoff (ca 40% of the delta(18)O signal). Although these results indicate that this coral is capable of yielding high-resolution paleoenvironmental records from retrospective analysis of the skeleton, there were significant and unexplained between-colony differences in mean delta(18)O. Therefore, for this species of coral in this setting, great care must be taken before interpreting the regional environmental significance of either gradual changes in mean delta(18)O through the length of a single long coral core, or differences between modern and ancient (fossil) colonies. Although skeletal delta(13)C and growth rate did show some relatively weak but significant correlations with some of the environmental variables, especially when the records from all colonies were combined, it was concluded that these attributes have relatively low potential for regional paleoenvironmental reconstruction. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Edinburgh, Dept Geol & Geophys, Edinburgh EH9 3JW, Midlothian, Scotland. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM guzmanh@naos.si.edu RI kohki, sowa/D-2955-2011 NR 56 TC 32 Z9 33 U1 3 U2 9 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 1998 VL 166 BP 109 EP 118 DI 10.3354/meps166109 PG 10 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA ZW639 UT WOS:000074431800010 ER PT J AU Perry, EA Amos, W AF Perry, EA Amos, W TI Genetic and behavioral evidence that harbor seal (Phoca vitulina) females may mate with multiple males SO MARINE MAMMAL SCIENCE LA English DT Article ID MATING-BEHAVIOR; BREEDING-SEASON; HUMAN DNA; PATERNITY; SYSTEMS; CONCOLOR; SUCCESS C1 Mem Univ Newfoundland, Dept Psychol, St Johns, NF A1B 3X9, Canada. Univ Cambridge, Dept Genet, Cambridge CB2 3EH, England. RP Perry, EA (reprint author), Smithsonian Inst, Natl Zool Pk, Genet Mol Lab, Washington, DC 20008 USA. NR 20 TC 3 Z9 3 U1 0 U2 5 PU SOC MARINE MAMMALOGY PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JAN PY 1998 VL 14 IS 1 BP 178 EP 182 DI 10.1111/j.1748-7692.1998.tb00704.x PG 5 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA YR330 UT WOS:000071484600017 ER PT S AU Triadan, D AF Triadan, D BE Spielmann, KA TI Socio-demographic implications of Pueblo IV ceramic production and circulation: Sourcing White Mountain Red Ware from the Grasshopper Region, Arizona SO MIGRATION AND REORGANIZATION: THE PUEBLO IV PERIOD IN THE AMERICAN SOUTHWEST SE ARIZONA STATE UNIVERSITY ANTHROPOLOGICAL RESEARCH PAPERS LA English DT Proceedings Paper CT Seminar on Pueblo IV Prehistory CY 1995 CL TEMPE, AZ ID ARCHAEOLOGICAL CERAMICS; SOUTHWEST AB White Mountain Red Ware, a painted pottery ware originating on the southern Colorado Plateau, has been frequently used to reconstruct pueblo socio-political and socio-economical organization, and to evaluate trade routes and exchange patterns in the American Southwest, It becomes a prominent decorated ware in the Grasshopper region and adjacent areas in the Arizona mountains during the aggregation phase of the fourteenth century. Compositional analysis of a large sample of reconstructible vessels and sherds from Grasshopper Pueblo and contemporary sites of the surrounding regions sheds new light on the production and circulation of White Mountain Red Ware, as well as socio-demographic patterns in the east-central Arizona mountains during the Pueblo IV period. C1 Smithsonian Inst, Washington, DC 20560 USA. NR 58 TC 0 Z9 0 U1 2 U2 2 PU ARIZONA STATE UNIV DEPT ANTHROPOLOGY PI TEMPE PA TEMPE, AZ 85281 USA SN 0271-0641 BN 0-936249-09-9 J9 ANTHR RES P PY 1998 IS 51 BP 233 EP 252 PG 20 WC Anthropology; Archaeology SC Anthropology; Archaeology GA BM26X UT WOS:000078229900012 ER PT S AU Bookbinder, J Cheimets, P Davis, B Caldwell, D Golub, L DeLuca, E AF Bookbinder, J Cheimets, P Davis, B Caldwell, D Golub, L DeLuca, E BE Korendyke, CM TI HIREX: Results of the mission concept study SO MISSIONS TO THE SUN II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on the Missions to the Sun II CY JUL 22-23, 1998 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE sun; corona; X-ray instrumentation AB HIREX is a suite of three complementary solar-pointed instruments that is being proposed to NASA under the NASA MIDEX announcement of opportunity. The main instrument is a 0.6m clear aperture, 240m effective focal Length normal incidence XUV telescope operated at 171 Angstrom, with a spatial resolution of 0.01 " (pixel size), This main telescope is complemented by two other instruments: A 0.3m context telescope that images in a wavelength range that covers the UV and XUV spectral regime, based on the TRACE design. This context telescope places the high magnification, limited field of view images created by the high resolution telescope in both spatial and temperature context. A spectrometer covering the spectral range from 170 - 220 Angstrom, based on the SERTS design, The primary aim of the High Resolution Explorer (HIREX) mission is to attack the problem of understanding the structuring and dynamics of astrophysical plasmas. We study the plasma universe by carrying out ground-breaking studies of plasmas on the Sun, with the additional capability of observing planets, galactic and extragalactic objects at the finest possible spatial and temporal scales, and at multiple temperatures. The High Resolution Telescope will follow the evolution of similar to 15 km solar structures within coronal loops at high time resolution while the context imaging telescope simultaneously observes the surrounding plasma with lower spatial resolution (0.25 " pixels) but a significantly larger field of view, 8', A second context instrument will provide high resolution spectroscopy of the plasma with a spatial resolution of approximately 1.0 ", To minimize mission costs, both context instruments are near-duplicates of previously built instruments: the imager is based on the Transition Region and Coronal Explorer (TRACE) and the spectrograph on the Solar EUV Rocket Telescope and Spectrograph (SERTS). This paper focuses on the design issues for the High Resolution Telescope. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bookbinder, J (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 NR 0 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2897-3 J9 P SOC PHOTO-OPT INS PY 1998 VL 3442 BP 22 EP 33 DI 10.1117/12.330261 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BM19X UT WOS:000078010300003 ER PT J AU Perry, EA Boness, DJ Fleischer, RC AF Perry, EA Boness, DJ Fleischer, RC TI DNA fingerprinting evidence of nonfilial nursing in grey seals SO MOLECULAR ECOLOGY LA English DT Article DE DNA fingerprinting; fostering; grey seal; Halichoerus grypus; kin selection; nonfilial nursing ID HALICHOERUS-GRYPUS; SITE FIDELITY; NORTH-RONA; GRAY SEAL; DISPERSION; COLONIES; SCOTLAND; ADOPTION; BAT AB We tested the hypothesis that kin selection may play a role in fostering behaviour in grey seals. Fostering frequency varied among three colonies, ranging from 3% to 28%. Band-sharing coefficients (S) of DNA fingerprints, from two multilocus probes, were used to predict relatedness (r). Mean r did not differ between foster mother-pup pairs and the expected r = 0 for presumed unrelated female-pup pairs. Likewise, mean r between fostered and filial pups compared to r between presumed unrelated pups within the same beaches did not differ. Mean S values of presumed unrelated pups on different beaches within the two smallest colonies were indistinguishable, indicating that there is not increased variation in relatedness in small colonies. These results suggest that kin selection does not play a significant role in the maintenance of grey seal fostering behaviour. C1 Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. RP Perry, EA (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. EM eperry@athena.nwafc.nf.ca NR 24 TC 20 Z9 20 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JAN PY 1998 VL 7 IS 1 BP 81 EP 85 DI 10.1046/j.1365-294x.1998.00313.x PG 5 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA YV137 UT WOS:000071793100008 PM 9465418 ER PT J AU Pukazhenthi, BS Wildt, DE Ottinger, MA Howard, J AF Pukazhenthi, BS Wildt, DE Ottinger, MA Howard, J TI Inhibition of domestic cat spermatozoa acrosome reaction and zona pellucida penetration by tyrosine kinase inhibitors SO MOLECULAR REPRODUCTION AND DEVELOPMENT LA English DT Article DE domestic cat; teratospermia; tyrosine kinase; capacitation; acrosome reaction ID HUMAN SPERM CAPACITATION; FREE HAMSTER OVA; MOUSE SPERMATOZOA; FERTILIZATION INVITRO; GAMETE INTERACTION; FELIS-BENGALENSIS; PROTEIN; PHOSPHORYLATION; PROGESTERONE; INDUCTION AB Spermatozoa from teratospermic domestic cats (> 60% morphologically abnormal spermatozoa per ejaculate) consistently exhibit lower levels of oocyte penetration in vitro than their normospermic (< 40% abnormal spermatozoa per ejaculate) counterparts. This could be caused by structural abnormalities or intracellular defects resulting in disruption of normal cellular functions. Spermatozoa from teratospermic cats also ave compromised in the ability to capacitate and undergo the acrosome reaction (AR) in vitro. Further, we recently identified two tyrosine phosphorylated proteins (95- and 160-kDa) localized over the acrosome region in domestic cat spermatozoa. Phosphorylation of these proteins is reduced in teratospermic compared with normospermic ejaculates. To begin to understand the relationship between tyrosine phosphorylation and sperm function, we examined the effects of two protein tyrosine kinase inhibitors (tyrphostin RG-50864 and genistein) on (1) sperm motility; (2) protein tyrosine phosphorylation; (3) the ionophore A23187-induced AR; (4) the spontaneous and zona pellucida (ZP)-induced AR, and (5) the ability of spermatozoa from normospermic cats to penetrate conspecific ZP-intact oocytes. Over a wide range of concentrations, neither inhibitor affected sperm percentage motility during incubation (P > 0.05). Preincubation with either inhibitor reduced tyrosine phosphorylation of both (95- and 160-kDa) sperm proteins. Although both inhibitors blocked the ZP-induced AR, neither influenced the spontaneous AR nor the A23187-induced AR, suggesting that tyrosine phosphorylation may be involved in physiologic AR. No differences (P > 0.05) were observed in the ability of control or inhibitor-treated spermatozoa to bind to or penetrate the outer ZP layer. However, percentages of oocytes with treated spermatozoa in the inner ZP (tyrphostin, 8.7%; genistein, 20.4%) and perivitelline space (tyrphostin, 0%; genistein, 2.3%) were less (P < 0.001) than untreated controls (inner ZP, 62.7%; perivitelline space, 10.2%). These results (1) demonstrate that ZP-induced acrosomal exocytosis in domestic cat spermatozoa is regulated via a tyrosine kinase-dependent pathway and (2) suggest that defects in these Signaling pathways may represent one of the causes for compromised sperm function in teratospermic males. (C) 1998 Wiley-Liss, inc. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT REPROD PHYSIOL,WASHINGTON,DC 20008. SMITHSONIAN INST,CONSERVAT & RES CTR,WASHINGTON,DC 20008. UNIV MARYLAND,DEPT ANIM & AVIAN SCI,COLLEGE PK,MD 20742. FU NICHD NIH HHS [R01 HD 23853] NR 52 TC 41 Z9 41 U1 0 U2 4 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 1040-452X J9 MOL REPROD DEV JI Mol. Reprod. Dev. PD JAN PY 1998 VL 49 IS 1 BP 48 EP 57 DI 10.1002/(SICI)1098-2795(199801)49:1<48::AID-MRD6>3.0.CO;2-O PG 10 WC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology SC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology GA YJ368 UT WOS:A1998YJ36800006 PM 9406195 ER PT J AU Backwell, P Jennions, M Passmore, N Christy, J AF Backwell, P Jennions, M Passmore, N Christy, J TI Synchronized courtship in fiddler crabs SO NATURE LA English DT Letter ID CHOICE C1 Univ Witwatersrand, Dept Zool, ZA-2050 Johannesburg, South Africa. Smithsonian Trop Res Inst, Balboa, Panama. RP Backwell, P (reprint author), Univ Witwatersrand, Dept Zool, ZA-2050 Johannesburg, South Africa. RI Jennions, Michael/C-7560-2009; Backwell, Patricia/C-8883-2009 OI Jennions, Michael/0000-0001-9221-2788; NR 5 TC 70 Z9 73 U1 0 U2 10 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD JAN 1 PY 1998 VL 391 IS 6662 BP 31 EP 32 DI 10.1038/34076 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA YP888 UT WOS:000071326100033 ER PT J AU Bromley, BC Miller, WA Pariev, VI AF Bromley, BC Miller, WA Pariev, VI TI The inner edge of the accretion disk around a supermassive black hole SO NATURE LA English DT Article ID MCG-6-30-15 AB Massive black holes are generally thought to exist at the centres of galaxies', but an unambiguous identification of a black hole has been impeded by a lack of evidence for the strong-field relativistic effects expected in the vicinity of such an object. Several years ago, a very broad iron emission line was discovered in the active galaxy MCG-6-30-15, indicative of emission from an accretion disk near the event horizon of a black hole, But this interpretation, based on the line profile, was somewhat model dependent (refs 2-5). Here we present an analysis of the iron-line emission from MCG-6-30-15 that is insensitive to the details (for example, disk thickness and emissivity) of the disk model used. We find that the inner edge of the disk material giving rise to the line is within 2.6 +/- 0.3 times the Schwarzschild radius-the event horizon of a non-rotating black hole-at the 95% confidence level. Changes to the disk parameters can only decrease the inner radius of the emitting region, and so we can be confident that we are observing emission from gravitationally bound material in the strong-field region of a supermassive black hole. Moreover, we find that the black hole is rotating at a rate which is greater than or similar to 23 +/- 17% of the theoretical maximum, although this conclusion is model dependent. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Los Alamos Natl Lab, MS B288, Los Alamos, NM 87545 USA. PN Lebedev Phys Inst, Moscow 117924, Russia. RP Bromley, BC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. NR 13 TC 42 Z9 42 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 JAN 1 PY 1998 VL 391 IS 6662 BP 54 EP 56 DI 10.1038/34130 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA YP888 UT WOS:000071326100044 ER PT S AU Fazio, GG Clemens, DP AF Fazio, GG Clemens, DP BE McLean, BJ Golombek, DA Hayes, JJE Payne, HE TI SIRTF surveys and legacy science SO NEW HORIZONS FROM MULTI-WAVELENGTH SKY SURVEYS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 179th Symposium of the International-Astronomical-Union on New Horizons from Multi-Wavelength Sky Surveys CY AUG 26-30, 1996 CL JOHNS HOPKINS UNIV, BALTIMORE, MARYLAND SP Int Astron Union HO JOHNS HOPKINS UNIV C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fazio, GG (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 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 0-7923-4802-8 J9 IAU SYMP PY 1998 IS 179 BP 109 EP 111 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK53M UT WOS:000072466600018 ER PT B AU van Ballegooijen, AA Cartledge, NP Priest, ER AF van Ballegooijen, AA Cartledge, NP Priest, ER BE Webb, D Rust, D Schmieder, B TI Magnetic flux transport and formation of filament channels SO NEW PERSPECTIVES ON SOLAR PROMINENCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 167 on New Perspectives on Solar Prominences CY APR 28-MAY 03, 1997 CL CTR PAUL LANGEVIN, AUSSOIS, FRANCE SP Intl Astron Union, Sci Comm Solar Terr Phys, European Off Aerosp Res & Dev, CNRS, Observ Paris, CEA, Ctr Natl Etud Spat HO CTR PAUL LANGEVIN AB We present a model of the transport of photospheric and coronal magnetic fields with the aim of explaining the observed global pattern of dextral and sinistral filaments on the quiet sun. The model is based on the assumption that the axial field in a filament channel originates in the surrounding coronal arcade. The model predicts that switchbacks in the polarity inversion line have opposite chirality on the two arms of the switchback: the higher latitude "lead" arm has sinistral (dextral) orientation in the North (South), while the lower latitude "return" arm has dextral (sinistral) orientation. This is in conflict with prominence observations which show that the chirality is the same on the two arms of a switchback. The model predicts the wrong sign of the axial field in polar crown filaments. This suggests that axial field in quiescent filaments are not produced by differential rotation acting on the surrounding coronal arcades. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Dept Math & Computat Sci, St Andrews KY16 9SS, Fife, Scotland. RP van Ballegooijen, AA (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 1-886733-70-8 J9 ASTR SOC P PY 1998 VL 150 BP 265 EP 268 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75E UT WOS:000076565100052 ER PT B AU Ciaravella, A Raymond, JC Fineschi, S Gardner, L Michels, J O'Neal, R Kohl, J Romoli, M Noci, G Venna, C Giordano, S Antonucci, E AF Ciaravella, A Raymond, JC Fineschi, S Gardner, L Michels, J O'Neal, R Kohl, J Romoli, M Noci, G Venna, C Giordano, S Antonucci, E BE Webb, D Rust, D Schmieder, B TI Ultraviolet spectroscopy of a coronal mass ejection SO NEW PERSPECTIVES ON SOLAR PROMINENCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 167 on New Perspectives on Solar Prominences CY APR 28-MAY 03, 1997 CL CTR PAUL LANGEVIN, AUSSOIS, FRANCE SP Intl Astron Union, Sci Comm Solar Terr Phys, European Off Aerosp Res & Dev, CNRS, Observ Paris, CEA, Ctr Natl Etud Spat HO CTR PAUL LANGEVIN AB A coronal mass ejection (CME) event was observed on December 23, 1996 with the Ultraviolet Coronagraph Spectrometer in both ultraviolat Fed viable light channels at 0.5 R-circle dot over the solar limb. The CME was followed during its evolution in the bright lines of Ly alpha (1216 Angstrom), Ly beta (1026 Angstrom), Ly gamma (972 Angstrom), C III (977 Angstrom) and the OVI daublet (1032, 1037 Angstrom) and in several weaker lines. The Ly alpha peak intensity shows an excursion of two orders of magnitude during the CME evolution, and blue shifts up to 0.8 Angstrom, (similar to 200 km/sec). The data provide the emission measure in the Log T range 4.0-5.5 with a 0.3 sampling. Line intensities and profiles have been measured, providing important diagnostics for a detailed study of the CME's physical and dynamical parameters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ciaravella, A (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 ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-70-8 J9 ASTR SOC P PY 1998 VL 150 BP 370 EP 375 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75E UT WOS:000076565100074 ER PT J AU Kudoh, H Whigham, DF AF Kudoh, H Whigham, DF TI The effect of petal size manipulation on pollinator/seed-predator mediated female reproductive success of Hibiscus moscheutos SO OECOLOGIA LA English DT Article DE corolla size; fruit abortion; floral display; pollen predator; pre-dispersal seed predator ID DISPERSAL SEED PREDATION; PLANT ANIMAL INTERACTIONS; ALPINE SKY PILOT; IPOMOPSIS-AGGREGATA; POLEMONIUM-VISCOSUM; FLORAL DISPLAY; WILD RADISH; OVIPOSITION CHOICES; INFLORESCENCE SIZE; POLLEN REMOVAL AB The effects of petal-size manipulations on the behavior of pollinators and pollen/seed predators, and on pollen removal and deposition, were studied in Hibiscus moscheutos (Malvaceae) populations. The ultimate effects on the female reproductive success of flowers, such as fruit set, seed predation rate, and final seed set were also measured. We applied three levels of petal removal (100%, 50%, and 0% size reduction in radius) to flowers in natural populations. Two pollinators (Bombus pennsylvanicus and Ptilothrix bombiformis) ignored flowers without petals, suggesting that pollinators use petals as a visual cue to locate flowers. Consequently, 100% petal removal reduced female reproductive success considerably, mainly through a higher rate of fruit abortion due to failure of pollen deposition on stigmas. No significant differences between the 50% petal removal treatment and uncut control were detected in any components of female success examined. The results, therefore, suggest that differences in petal size have little influence on female reproductive success of Hibiscus flowers at our study site. Final seed set varied considerably depending on the larval densities of two coleopteran seed predators (Althaeus hibisci and Conotrachelus fissunguis). A. hibisci responded to petal size, and a higher density of adults was found in flowers in which petal size had not been reduced. Because Althaeus feed on pollen as adults and no effect of petal size on seed predation was detected, the preference of Althaeus for larger flowers may represent a foraging strategy for adult beetles and may exert counteracting selection pressure on petal size through male reproductive success of flowers. C1 Tokyo Metropolitan Univ, Fac Sci, Dept Biol, Hachioji, Tokyo 1920397, Japan. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Kudoh, H (reprint author), Tokyo Metropolitan Univ, Fac Sci, Dept Biol, Minami Osawa 1-1, Hachioji, Tokyo 1920397, Japan. EM kudoh-hiroshi@c.metro-u.ac.jp OI Whigham, Dennis/0000-0003-1488-820X NR 47 TC 58 Z9 60 U1 3 U2 23 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PY 1998 VL 117 IS 1-2 BP 70 EP 79 DI 10.1007/s004420050633 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 144YZ UT WOS:000077344700010 PM 28308508 ER PT J AU Litchman, E AF Litchman, E TI Population and community responses of phytoplankton to fluctuating light SO OECOLOGIA LA English DT Article DE temporal heterogeneity; light fluctuations; phytoplankton; community structure; diversity ID NATURAL PHYTOPLANKTON; VARIABLE ENVIRONMENT; LIMITING NUTRIENTS; OPTICAL-PROPERTIES; DARK CYCLES; GROWTH-RATE; PHOTOSYNTHESIS; MODEL; COMPETITION; WATER AB Light is a major resource in aquatic ecosystems and has a complex pattern of spatio-temporal variability, yet the effects of dynamic light regimes on communities of phytoplankton are largely unexplored. I examined whether and how fluctuating light supply affects the structure and dynamics of phytoplankton communities. The effect of light fluctuations was tested at two average irradiances: low, 25 mu mol quanta m(-2) s(-1) and high, 100 mu mol quanta m(-2) s(-1) in 2- and 18-species communities of freshwater phytoplankton. Species diversity, and abundances of individual species and higher taxa, depended significantly on both the absolute level and the degree of variability in light supply, while total density, total biomass, and species richness responded only to light level. In the two-species assemblage, fluctuations increased diversity at both low and high average irradiances and in the multispecies community fluctuations increased diversity at high irradiance but decreased diversity at low average irradiance. Species richness was higher under low average irradiance and was not affected by the presence or absence of fluctuations. Diatom abundance was increased by fluctuations, especially at low average irradiance, where they became the dominant group, while cyanobacteria and green algae dominated low constant light and all high light treatments. Within each taxonomic group, however, there was no uniform pattern in species responses to light fluctuations: both the magnitude and direction of response were species-specific. The temporal regime of light supply had a significant effect on the growth rates of individual species grown in monocultures. Species responses to the regime of light supply in monocultures qualitatively agreed with their abundances in the community experiments. The results indicate that the temporal regime of light supply may influence structure of phytoplankton communities by differentially affecting growth rates and mediating species competition. C1 Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. RP Litchman, E (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 55 TC 53 Z9 58 U1 4 U2 29 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PY 1998 VL 117 IS 1-2 BP 247 EP 257 DI 10.1007/s004420050655 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 144YZ UT WOS:000077344700032 PM 28308494 ER PT J AU Wright, DH Patterson, BD Mikkelson, GM Cutler, A Atmar, W AF Wright, DH Patterson, BD Mikkelson, GM Cutler, A Atmar, W TI A comparative analysis of nested subset patterns of species composition SO OECOLOGIA LA English DT Review DE nested subsets; meta-community structure; biogeography; beta diversity; landscape ecology ID AREA; ISLANDS; ARCHIPELAGOES; BIOGEOGRAPHY; ASSEMBLAGES; HABITAT; DISTRIBUTIONS; CONSERVATION; IMMIGRATION; EXTINCTION AB We present a broad comparative assessment of nested subsets in species composition among ecological communities. We assembled presence-absence data from a broad range of taxa, geographic regions, and spatial scales; and subjected this collection of datasets to common analyses, including a variety of metrics for measuring nestedness and null hypotheses against which to evaluate them. Here we identify ecological patterns in the prevalence and strength of nested subset structure, and assess differences and biases among the available methodologies. In all, we compiled 279 presence-absence matrices, of which 163 do not overlap in their coverage of species and sites. The survey includes studies on vertebrates, arthropods, mollusks, plants, and other taxa; from north temperate, tropical, and south temperate latitudes. Our results were as follows. Statistically significant nestedness was common. Assemblages from landbridge archipelagos were strongly nested, and immigration experiments were least nested. This adds further empirical support to the hypothesis that extinction plays a major role in producing nested structure. Nestedness was positively correlated with the ratio of the areas of the largest and smallest sites, suggesting that the range in area of sites affects nestedness. Taxonomic differences in nestedness were weak. Higher taxonomic levels showed stronger nesting than their constituent lower taxa. We observed no effect of distance of isolation on nestedness; nor any effects of latitude. With regard to methodology, the metrics Nc and Ut yielded similar results, although Nc proved slightly more flexible in use, and deals differently with tied sites. Similarities also exist in the behavior of N0 ("N") and Up, and between N1 and Ua. Standardized nestedness metrics were mostly insensitive to matrix size, and were useful in comparative analyses among presence-absence matrices. Most metrics were affected by the proportion of presences in the matrix. All analyses of nestedness, therefore, should test for bias due to matrix fill. We suggest that the factors controlling nested subset structure can be thought of as four filters that species pass to occur at a site: a sampling filter, a distance filter, a habitat filter, and an area filter - and three constraints on community homogeneity: evolutionary history, recent history, and spatial variation in the environment. The scale of examination can also have important effects on the degree of nestedness observed. C1 Field Museum Nat Hist, Ctr Evolutionary & Environm Biol, Chicago, IL 60605 USA. US Fish & Wildlife Serv, Sacramento, CA 95821 USA. Univ Chicago, Comm Conceptual Fdn Sci, Chicago, IL 60637 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Paleobiol, Washington, DC 20560 USA. AICS Res Inc, University Pk, NM 88003 USA. RP Patterson, BD (reprint author), Field Museum Nat Hist, Ctr Evolutionary & Environm Biol, Roosevelt Rd & Lake Shore Dr, Chicago, IL 60605 USA. NR 41 TC 369 Z9 388 U1 2 U2 92 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JAN PY 1998 VL 113 IS 1 BP 1 EP 20 PG 20 WC Ecology SC Environmental Sciences & Ecology GA YL928 UT WOS:000071009200001 ER PT S AU Szentgyorgyi, A Cheimets, P Eng, R Fabricant, D Geary, J Hartmann, L Pieri, M Roll, J AF Szentgyorgyi, A Cheimets, P Eng, R Fabricant, D Geary, J Hartmann, L Pieri, M Roll, J BE DOdorico, S TI Hectochelle: a multi-object echelle spectrograph for the converted MMT SO OPTICAL ASTRONOMICAL INSTRUMENTATION, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Optical Astronomical Instrumentation Conference CY MAR 26-28, 1998 CL KONA, HI SP SPIE, European So Observ, Amer Astron Soc, Astron Soc Pacific, Canadian Astron Soc DE echelle spectrograph; high resolution spectroscopy AB The Hectochelle will be a fiber-fed, multi-object spectrograph for the post-conversion MMT which will take 255 simultaneous spectra at a resolution of 32,000-40,000. The absolute efficiency, including optical fiber losses, is predicted to be 6%-10%, depending on the position of a line within a diffractive order. In one hour, features with 60 m Angstrom should be resolved in m(R) = 18 stars with a signal to noise of 10. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Szentgyorgyi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 47 Z9 48 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2802-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3355 BP 242 EP 252 DI 10.1117/12.316766 PN 1-2 PG 3 WC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics GA BL41A UT WOS:000075411500025 ER PT S AU Conroy, TA Roll, JB Wyatt, WF Mink, DJ McLeod, BA AF Conroy, TA Roll, JB Wyatt, WF Mink, DJ McLeod, BA BE DOdorico, S TI Coping with data deluge - a data system for the Megacam SO OPTICAL ASTRONOMICAL INSTRUMENTATION, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Optical Astronomical Instrumentation Conference CY MAR 26-28, 1998 CL KONA, HI SP SPIE, European So Observ, Amer Astron Soc, Astron Soc Pacific, Canadian Astron Soc DE MMT; pipeline; computer architecture; mosaic; visualization AB Megacam is a wide-field optical imager for the converted MMT that uses thirty-six 2048 by 4608 pixel CCDs to cover a 24' x 24' format. We describe a computer architecture designed to accommodate the expected data volume and show benchmark results from prototype implementations that demonstrate the performance attained by each of the design decisions. We show that our time budget allotments can be met using a modular, scalable architecture design that exploits the natural parallelization of multiple, identical detector components. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Conroy, TA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Mink, Jessica/0000-0003-3594-1823 NR 0 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2802-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3355 BP 264 EP 274 DI 10.1117/12.316808 PN 1-2 PG 3 WC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics GA BL41A UT WOS:000075411500027 ER PT S AU Cheimets, P Szentgyorgyi, AH Pieri, MR AF Cheimets, P Szentgyorgyi, AH Pieri, MR BE DOdorico, S TI Mosaicked echelle grating support for the Hectochelle fiber-fed spectrograph SO OPTICAL ASTRONOMICAL INSTRUMENTATION, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Optical Astronomical Instrumentation Conference CY MAR 26-28, 1998 CL KONA, HI SP SPIE, European So Observ, Amer Astron Soc, Astron Soc Pacific, Canadian Astron Soc DE echelle grating; mosaicked grating; optical alignment AB This paper presents the design of an assembly to support the Hectochelle multi-object spectrograph grating. The grating consists of two mosaicked, 420mm by 320mm by 74mm thick, 110 line/mm echelle grating segments, nominally operated at a 72 degrees angle of incidence. The fact that the grating consists of 2 segments that must be co-aligned to within 0.27 arcsecs creates a challenging design problem. After much preliminary examination, two support designs were studied, one utilizing Invar, and the other, selected for development, using a Zerodur support structure. The trade study to select the final design is discussed. The Zerodur design was selected because it maintained higher grating stability throughout the operating temperature range than the Invar design. The Zerodur design concept is discussed in detail, including the results of finite element modeling that shows system feasibility. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cheimets, P (reprint author), Harvard Smithsonian Ctr Astrophys, 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 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2802-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3355 BP 333 EP 342 DI 10.1117/12.316749 PN 1-2 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics GA BL41A UT WOS:000075411500034 ER PT S AU McLeod, BA Gauron, TM Geary, JC Ordway, MP Roll, JB AF McLeod, BA Gauron, TM Geary, JC Ordway, MP Roll, JB BE DOdorico, S TI Megacam: paving the focal plane of the MMT with silicon SO OPTICAL ASTRONOMICAL INSTRUMENTATION, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Optical Astronomical Instrumentation Conference CY MAR 26-28, 1998 CL KONA, HI SP SPIE, European So Observ, Amer Astron Soc, Astron Soc Pacific, Canadian Astron Soc DE CCDs; imaging; cameras; astronomy; telescope guiding AB Megacam is a 36 CCD mosaic camera that will cover a 24' x 24' field of view at the f/5 wide-field focus of the converted 6.5 m Multiple Mirror Telescope. The mosaic is a 9 x 4 array of thinned 2048 x 4608 pixel CCDs with 13.5 mu m pixels. The CCDs are dual-output EEV devices in a custom package to allow the devices to be closely butted on all four sides. The dewar will be mounted to a 2 m diameter assembly that contains the filter wheels (for 30 x 30 cm filters) and the shutter. Telescope guiding will be accomplished with two additional CCDs mounted at the edges of the focal plane. The guider CCDs will be operated slightly defocused, one on either side of focus, to allow simultaneous focusing and guiding. Guide stars will be selected by reading out the full guider frame, after which only a small area surrouding the guide star will be read out. Our simulations show that the defocused guide star images will also be useful for low order wavefront sensing, allowing corrections to the telescope collimation. We are developing a new CCD controller capable of reading the full Megacam in 24 seconds. This controller will also be used to operate the guide chips. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McLeod, BA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 17 Z9 17 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2802-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3355 BP 477 EP 486 DI 10.1117/12.316779 PN 1-2 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics GA BL41A UT WOS:000075411500048 ER PT S AU Geary, JC Amato, SM AF Geary, JC Amato, SM BE DOdorico, S TI Camera electronics for the 72-channel SAO Megacam SO OPTICAL ASTRONOMICAL INSTRUMENTATION, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT SPIE Optical Astronomical Instrumentation Conference CY MAR 26-28, 1998 CL KONA, HI SP SPIE, European So Observ, Amer Astron Soc, Astron Soc Pacific, Canadian Astron Soc DE camera; electronics; controller; CCD AB The S.A.O. Megacam focal plane will consist of 36 large CCDs (2K X 4.5K format), each with 2 output ports running at pixel rates up to 200 kHz. The unbinned data field is thus as large as 324 megawords and is presented at a sustained data rate during readout approaching 28 megabytes/sec. We have developed a simple camera controller to deal with the problem of handling so many channels and their digitized outputs at fairly high speeds. We also present some results from ongoing efforts to optimize the 200 kHz signal processing chain for low noise and low crosstalk. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Geary, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 8 Z9 8 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2802-7 J9 P SOC PHOTO-OPT INS PY 1998 VL 3355 BP 539 EP 546 DI 10.1117/12.316830 PN 1-2 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Remote Sensing; Optics GA BL41A UT WOS:000075411500055 ER PT J AU Stuwe, M Abdul, JB Nor, BM Wemmer, CM AF Stuwe, M Abdul, JB Nor, BM Wemmer, CM TI Tracking the movements of translocated elephants in Malaysia using satellite telemetry SO ORYX LA English DT Article AB Malaysia incurs damage worth millions of dollars annually from elephants feeding in plantations. In response, the Malaysian Wildlife Department has translocatcd over 392 elephants from plantations into protected areas since 1974. Dense rain forest and steep terrain at the release sires have made it near impossible to follow the movements of the released elephants and evaluate the success of the programme. In October 1995, a translocated female elephant was fitted with a satellite transmitter to determine its post-release movements. By August 1996, the female had moved within a range of 7000 sq km. the movements were erratic initially and covered a large area. They were followed by a shift in location twice, each time covering successively smaller areas. Attempts to locate and follow the female on the ground revealed no evidence that she travelled in a group. A second, male elephant was equipped with a satellite transmitter in February 1996 and by August 1996, it had moved within a range of 350 sq km. An attempt to locate and follow the male on the ground provided evidence that he was in a group of at least three individuals. The difference in the behaviour of the two elephants, released at exactly the same location, is striking, but additional elephants need to be followed to increase sample size and allow a scientific explanation of the findings. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. Dept Wildlife & Natl Parks, Kuala Lumpur 50664, Malaysia. RP Stuwe, M (reprint author), Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. NR 16 TC 15 Z9 15 U1 0 U2 7 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0030-6053 J9 ORYX JI Oryx PD JAN PY 1998 VL 32 IS 1 BP 68 EP 74 DI 10.1046/j.1365-3008.1998.00019.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA YR798 UT WOS:000071531300018 ER PT J AU Horton, JO AF Horton, JO TI Slavery and freedom in Delaware, 1619-1865 SO PENNSYLVANIA MAGAZINE OF HISTORY AND BIOGRAPHY LA English DT Book Review C1 George Washington Univ, Washington, DC 20052 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Horton, JO (reprint author), George Washington Univ, Washington, DC 20052 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU HISTORICAL SOC PA PI PHILADELPHIA PA 1300 LOCUST ST, PHILADELPHIA, PA 19107 USA SN 0031-4587 J9 PENN MAG HIST BIOG JI Pa. Mag. Hist. Biogr. PD JAN-APR PY 1998 VL 122 IS 1-2 BP 147 EP 149 PG 3 WC History SC History GA ZK254 UT WOS:000073300800019 ER PT J AU Faust, MA Steidinger, KA AF Faust, MA Steidinger, KA TI Bysmatrum gen. nov. (Dinophyceae) and three new combinations for benthic scrippsielloid species SO PHYCOLOGIA LA English DT Article ID CALCAREOUS RESTING CYST; COMB-NOV; MARINE DINOFLAGELLATE; POOL DINOFLAGELLATE; REDESCRIPTION; PERIDINIALES AB A new generic name is proposed, Bysmatrum gen. nov., for three Scrippsiella species: B. subsalsum comb. nov., B. arenicola comb, nov., and B. caponii comb. nov. These three benthic marine species share a number of morphological characteristics: apical plate 1' is wide, asymmetric, and pentagonal and ends at the anterior margin of the cingulum; intercalary plates 2a and 3a are separated by apical plate 3' and 4 "; the apical pore complex is a recessed chamber with a large P-o plate, elongated X plate, and a raised dome at the center; six cingular plates and four sulcal plates are present; and the thecal surface is vermiculate to reticulate. In contrast, other scrippsielloid species are planktonic, and their morphology differs from the three Bysmatrum species. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, Suitland, MD 20746 USA. Florida Marine Res Inst, Dept Environm Protect, St Petersburg, FL 33701 USA. RP Faust, MA (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, 4201 Silver Hill Rd, Suitland, MD 20746 USA. NR 31 TC 21 Z9 22 U1 0 U2 0 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD JAN PY 1998 VL 37 IS 1 BP 47 EP 52 DI 10.2216/i0031-8884-37-1-47.1 PG 6 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 102NV UT WOS:000074931400007 ER PT J AU Nevalainen, J Vilhu, O Poutanen, J Gilfanov, M Vargas, M AF Nevalainen, J Vilhu, O Poutanen, J Gilfanov, M Vargas, M TI Two-phase spectrum of the black hole candidate 1E1740.7-2942 SO PHYSICA SCRIPTA LA English DT Article; Proceedings Paper CT Nordic Conference in Theoretical High Energy Astrophysics CY SEP 14-16, 1997 CL COPENHAGEN, DENMARK SP Danish Space Res Inst, Nord Inst Theoret Phys, Nord Acad Adv Study ID X-RAY; MOLECULAR CLOUD; 1E-1740.7-2942; GINGA AB Combined ASCA and SIGMA data of 1E1740.7-2942 during its standard state (September 1993 and 1994) were successfully fitted with a two-phase model ISM (iterative scattering method) [1]. The classical cold accretion disk does not extend up to the innermost stable orbit, but is truncated at similar to 30 GM/c(2). A hot inner disk has electron temperature T-e approximate to 60 keV and radial Thomson optical depth tau approximate to 2.4. The cold disk radiates approximate to 40 % of the total luminosity with (M) over dot approximate to 0.04(M) over dot(Edd) of 10M.. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. Univ Helsinki, FIN-00014 Helsinki, Finland. Astron Observ, SE-75120 Uppsala, Sweden. NORDITA, DK-2100 Copenhagen, Denmark. Stockholm Observ, SE-13336 Saltsjobaden, Sweden. MPI Astrophys, D-86740 Garching, Germany. Moscow Space Res Inst, IKI, Moscow 117810, Russia. CEA Saclay, DSM, DAPNIA, SAp, F-91191 Gif Sur Yvette, France. RP Nevalainen, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA. RI Poutanen, Juri/H-6651-2016 OI Poutanen, Juri/0000-0002-0983-0049 NR 18 TC 0 Z9 0 U1 0 U2 0 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0281-1847 J9 PHYS SCRIPTA JI Phys. Scr. PY 1998 VL T77 BP 86 EP 87 DI 10.1088/0031-8949/1998/T77/025 PG 2 WC Physics, Multidisciplinary SC Physics GA 150TA UT WOS:000077680300027 ER PT J AU Forman, W Jones, C Vikhlinin, A David, L AF Forman, W Jones, C Vikhlinin, A David, L TI Cosmological implications of X-ray observations of clusters of galaxies SO PHYSICA SCRIPTA LA English DT Article; Proceedings Paper CT Nordic Conference in Theoretical High Energy Astrophysics CY SEP 14-16, 1997 CL COPENHAGEN, DENMARK SP Danish Space Res Inst, Nord Inst Theoret Phys, Nord Acad Adv Study ID COMA CLUSTER; SUBSTRUCTURE; PERSEUS; A2256; MORPHOLOGIES; CONSTRAINTS; CENTAURUS; DENSITY; MODELS; ROSAT AB We discuss the morphology and substructure in clusters of galaxies and their relation to large scale structures such as filaments. As predicted by numerical simulations, the small scale structures in clusters are co-aligned with the much larger filamentary structures in which the clusters are embedded and from which they formed. For regular clusters, we review the potential of X-ray observations to derive gravitating masses to large radii. Using a small sample of observations, we show that the baryon fraction rises to a typical value of about 25% which, in the standard Big Bang scenario, argues for a low value of Omega. We briefly indicate the potential for future X-ray studies of clusters with AXAF, XMM, and SRG. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Inst Space Res, Moscow, Russia. RP Forman, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 0 Z9 0 U1 0 U2 0 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0281-1847 J9 PHYS SCRIPTA JI Phys. Scr. PY 1998 VL T77 BP 103 EP 107 DI 10.1088/0031-8949/1998/T77/031 PG 5 WC Physics, Multidisciplinary SC Physics GA 150TA UT WOS:000077680300033 ER PT J AU Nevalainen, J Pedersen, K AF Nevalainen, J Pedersen, K TI SIXA simulations of the hot cluster of galaxies a2163 SO PHYSICA SCRIPTA LA English DT Article; Proceedings Paper CT Nordic Conference in Theoretical High Energy Astrophysics CY SEP 14-16, 1997 CL COPENHAGEN, DENMARK SP Danish Space Res Inst, Nord Inst Theoret Phys, Nord Acad Adv Study AB We present simulated SIXA spectra of the hottest known cluster of galaxies Abell 2163. SMA is an array of solid state detectors located in the focal plane of one of the two SODART telescopes onboard SPECTRUM-RONTGEN-GAMMA. We hereby demonstrate the capabilities of SMA to perform spatially resolved spectroscopy of hot clusters. In a 30 ksec exposure, the temperature of the hot gas can be reliably derived from the central pixel as well as in the 2nd and 3rd pixel rings whereas the iron abundance can be determined in the central pixel and the 2nd pixel ring. SIXA will thus significantly improve current temperature and abundance measurements of the hot gas in clusters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. Univ Helsinki, FIN-00014 Helsinki, Finland. Danish Space Res Inst, Copenhagen, Denmark. RP Nevalainen, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0281-1847 J9 PHYS SCRIPTA JI Phys. Scr. PY 1998 VL T77 BP 120 EP 121 DI 10.1088/0031-8949/1998/T77/036 PG 2 WC Physics, Multidisciplinary SC Physics GA 150TA UT WOS:000077680300038 ER PT S AU Mittlefehldt, DW McCoy, TJ Goodrich, CA Kracher, A AF Mittlefehldt, DW McCoy, TJ Goodrich, CA Kracher, A BE Papike, JJ TI Non-chondritic meteorites from asteroidal bodies SO PLANETARY MATERIALS SE REVIEWS IN MINERALOGY LA English DT Review ID EUCRITE PARENT BODY; ANGRA-DOS-REIS; EARLY SOLAR-SYSTEM; U-TH-PB; ND ISOTOPIC SYSTEMATICS; STONY-IRON METEORITES; RARE-EARTH ELEMENTS; NILPENA POLYMICT UREILITE; FE-NI-P; SM-ND C1 Lockheed Martin SMSS Co, Basic & Appl Res Dept C23, Houston, TX 77058 USA. Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. Max Planck Inst Chem, Abt Kosmochem, D-55020 Mainz, Germany. Iowa State Univ, Dept Geol Sci, Ames, IA 50011 USA. RP Mittlefehldt, DW (reprint author), Lockheed Martin SMSS Co, Basic & Appl Res Dept C23, Houston, TX 77058 USA. NR 675 TC 21 Z9 21 U1 4 U2 36 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0275-0279 BN 0-939950-46-4 J9 REV MINERAL PY 1998 VL 36 BP D1 EP D195 PG 195 WC Mineralogy SC Mineralogy GA BM09T UT WOS:000077625800004 ER PT S AU Vessot, RFC Mattison, EM AF Vessot, RFC Mattison, EM GP IEEE IEEE TI High accuracy time and frequency from space SO PROCEEDINGS OF THE 1998 IEEE INTERNATIONAL FREQUENCY CONTROL SYMPOSIUM SE PROCEEDINGS OF THE IEEE INTERNATIONAL FREQUENCY CONTROL SYMPOSIUM LA English DT Proceedings Paper CT IEEE International Frequency Control Symposium CY MAY 27-29, 1998 CL PASADENA, CA SP IEEE, Ultrasonics Ferroelectr & Frequency Control Soc AB Accurate time and frequency are fundamental components of modern metrology. The potential now exists to provide global access to a primary time and frequency laboratory operating aboard an orbiting space platform. Such a laboratory could provide primary time and frequency, in terms of the internationally agreed definition of the second,(1) with unprecedented accuracy. Operated in space, a frequency standard based on freely drifting atoms(2) could provide accuracy approaching 1 pit in 10(16), higher than is currently available. This capability, in turn, would enable a globally shared basis for the unit of length in terms of the definition of the meter.(3) This paper reviews the concept of such a frequency standard and the availability of components and systems for its operation. We discuss the possibility of highly precise time and frequency transfer, based on previously developed and tested microwave and pulsed laser technology, along with the corrections required to account for effects of general relativity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vessot, RFC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 2 Z9 4 U1 1 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1075-6787 BN 0-7803-4373-5 J9 P IEEE INT FREQ CONT PY 1998 BP 336 EP 345 DI 10.1109/FREQ.1998.717925 PG 10 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BL72D UT WOS:000076440400058 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, WN Zatwarnicki, T TI A review of the West Indian species of Mimapsilopa Cresson (Diptera : Ephydridae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE review; Diptera; Ephydridae; shore flies; Mimapsilopa; M-cubensis; M-dominicana; M-bacoa; West Indies AB Five species of Mimapsilopa are reported from the West Indies (including Trinidad and Tobago), including three that are new: M. cubensis (Cuba. Pinar del Rio: Soroa (2 km NW, 22 degrees 48.6'N, 83 degrees 1.0'W); M. dominicana (Dominican Republic. La Vega: Salto Guasara (near Jarabacoa; 19 degrees 04.4'N, 70 degrees 42.1'W; 680 m); and M. bacoa (Dominican Republic. La Vega: Jarabacoa (5 km S; 19 degrees 05.8'N, 70 degrees 36.5'W; 640 m). Two of the new species, M. cubensis and M. dominicana, are sister species, forming a monophyletic lineage within Mimapsilopa that is characterized by the wide face and greatly enlarged antenna of the male. The third new species is closely related to M. cressoni Lizarralde de Grosso. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. Univ Agr, Dept Zool, PL-50205 Wroclaw, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169, Washington, DC 20560 USA. OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 14 TC 5 Z9 6 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 1998 VL 100 IS 1 BP 7 EP 24 PG 18 WC Entomology SC Entomology GA YW257 UT WOS:000071914200002 ER PT J AU Polhemus, DA AF Polhemus, DA TI Nysius aa (Heteroptera : Lygaeidae), a new species of micropterous Wekiu bug from the summit of Mauna Loa Volcano, Hawaii SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Lygaeidae; micropterous; alpine; aeolian; Hawaii; Mauna Kea; Mauna Loa AB Nysius aa, a micropterous lygaeid bug, is described from the upper slopes of Mauna Loa volcano on the island of Hawaii. This new species appears to be the sister species of Nysius wekiuicola Ashlock and Gagne, which is endemic to aeolian desert habitats in the summit region of adjacent Mauna Kea volcano. Detailed morphological comparisons between the two species are presented, accompanied by a distribution map and figures of key characters. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Polhemus, DA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 105, Washington, DC 20560 USA. NR 5 TC 3 Z9 5 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 1998 VL 100 IS 1 BP 25 EP 31 PG 7 WC Entomology SC Entomology GA YW257 UT WOS:000071914200003 ER PT J AU Davis, DR AF Davis, DR TI A revision of the genus Lamyristis Meyrick (Lepidoptera : Psychidae) and proposal of a new related genus Acoremata from Southeast Asia SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Arrhenophanidae; bagworm moth; Acoremata; Lamyristis; Parameristis AB The southeast Asian genus Lamyristis Meyrick 1911, including its synonym Parameristis Meyrick 1919, is revised. Previously assigned by various authors to the families Plutellidae, Yponomeutidae, or Tineidae, its proper placement within the Psychidae was recognized recently by Robinson and Tuck (1996). Included species are L. leucopselia Meyrick, L. eremaea (Meyrick), and L. bruneiensis, new species. A new genus and species, Acoremata aquila, is also described and illustrated. At least one synapomorphy, the broad, flattened scale vestiture of the foreleg, closely associates the two genera. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Davis, DR (reprint author), Smithsonian Inst, Dept Entomol, MRC 127, Washington, DC 20560 USA. NR 15 TC 1 Z9 1 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 1998 VL 100 IS 1 BP 114 EP 125 PG 12 WC Entomology SC Entomology GA YW257 UT WOS:000071914200012 ER PT J AU Fabricant, D Cheimets, P Caldwell, N Geary, J AF Fabricant, D Cheimets, P Caldwell, N Geary, J TI The FAST spectrograph for the Tillinghast telescope SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB We describe a high-throughput optical spectrograph that has been in operation at the Cassegrain focus of the 1.5-m Tillinghast reflector since 1994 January. FAST has a 3'-long slit and is typically operated at resolutions between 1 and 6 Angstrom. With a collimated beam diameter of similar to 100 mm, FAST (with a 300 lines mm(-1) grating and a 1." 5-wide slit) offers 4000 Angstrom of spectral coverage at 3 Angstrom resolution. FAST's optics are primarily reflective, are adequately sized to prevent vignetting, and use high-performance coatings. The high measured system peak-efficiency of 26% (fraction of light incident on the primary detected at the CCD) demonstrates that the throughput of reflective optics can be quite competitive with that of refractive optics. FAST's structure is constructed from graphite-epoxy composite panels, which have an excellent stiffness-to-weight ratio and low thermal expansion, resulting in low flexure and excellent focus stability. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabricant, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 196 Z9 196 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JAN PY 1998 VL 110 IS 743 BP 79 EP 85 DI 10.1086/316111 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YU680 UT WOS:000071743200011 ER PT J AU Cooke, R AF Cooke, R TI Human settlement of Central America and northern most South America (14,000-8000 BP) SO QUATERNARY INTERNATIONAL LA English DT Article; Proceedings Paper CT Symposium on the Archaeology of the Pleistocene-Holocene Transition, at the XIV INQUA Congress CY AUG, 1995 CL BERLIN, GERMANY ID LAKE VALENCIA; PANAMA; VENEZUELA; COLOMBIA; OCCUPATION; HISTORY; POLLEN; BASIN; LYNCH; SITE AB A human presence in Central America, Colombia and Venezuela (outside 'Amazonia') before the Late Glacial Stage( approximate to 14,000-10,000 BP) requires substantiation. In Venezuela, hunter-foragers who used elongate, thick bifacial projectile points preyed upon megamammals (e.g. gomphotheres) before the onset of a (approximate to 12,000-11,000 BP) warming stage, particularly visible in highland Colombia (Guantiva Interstadial). Some archaeologists argue for a distinct pre-12,000 BP population centered on the Sabana de Bogota (Colombia, approximate to 2500 m). Their 'Abriense' stone tool kit lacked bifacial reduction, and continued to be used well into the Holocene. In Central America, no human cultural remains yet pre-date the widespread, but poorly documented 'Palaeoindian' horizon. This coincides chronologically with the approximate to 11,000-10,000 BP cold stage equivalent to the Younger Dryas (in Colombia, 'El Abra Stadial'). Makers of lanceolate ('Clovis') and stemmed ('Fish-Tail') fluted points, carefully trimmed scrapers, burins and perforators, 'Paleoindians' have also been identified in northwest South America. Palaeoenvironmental data suggest that they moved around in many different vegetation types. In general, these were unlike modern potential vegetation because temperatures and annual rainfall were still lower than those of today. Human material culture at the onset of the Holocene (10,500 +/- 700 BP depending on region) does not seem not to have changed as rapidly as climate and vegetation. But the disappearance of fluted projectile points and the Late Pleistocene megafauna may be causally related. Presently, it is difficult to distinguish widespread and short-lived diachronic changes in human culture, from culturally diverse populations living synchronously in different geographic areas. Some archaeologists argue that early Holocene forest expansion and foraging territory contraction were responsible for socioeconomic diversification and a gradual shift from mobile hunting and gathering to a more sylvan way of life. This emphasized the intensive collection and incipient domestication of forest products (e.g. palms and root crops), and the hunting of deer and rodents. (C) 1998 INQUA/Elsevier Science Ltd. All rights reserved. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Cooke, R (reprint author), Smithsonian Trop Res Inst, Apdo 2072, Balboa, Panama. NR 96 TC 4 Z9 6 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 J9 QUATERN INT JI Quat. Int. PY 1998 VL 50 BP 177 EP 190 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 101ZT UT WOS:000074899300015 ER PT B AU Moran, JM AF Moran, JM BE Zensus, JA Taylor, GB Wrobel, JM TI Thirty years of VLBI: Early days, successes, and future SO RADIO EMISSION FROM GALACTIC AND EXTRAGALACTIC COMPACT SOURCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 164 on Radio Emission from Galactic and Extragalactic Compact Sources CY APR 21-26, 1997 CL NEW MEXICO INST MIN & TECHNOL, MACEY CTR, SOCORRO, NM SP Int Astron Union, Commiss 28 Galaxies, Int Astron Union, Commiss 40 Radio Astron, Union Radio Sci Int, Commiss J Radio Astron, Associated Univ Inc HO NEW MEXICO INST MIN & TECHNOL, MACEY CTR AB The early days of VLBI are discussed, with emphasis on the fifteen experiments performed in the U.S. and Canada in 1967. Some key technical ideas are described that influenced the development of the technique, including digital fringe rotation, bandwidth synthesis, spectral phase referencing, phase closure and self-calibration, and water vapor radiometry. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moran, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 3 Z9 3 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-64-3 J9 ASTR SOC P PY 1998 VL 144 BP 1 EP 10 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75N UT WOS:000076608500001 ER PT B AU Greenhill, LJ AF Greenhill, LJ BE Zensus, JA Taylor, GB Wrobel, JM TI Water in NGC 1068 SO RADIO EMISSION FROM GALACTIC AND EXTRAGALACTIC COMPACT SOURCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 164 on Radio Emission from Galactic and Extragalactic Compact Sources CY APR 21-26, 1997 CL NEW MEXICO INST MIN & TECHNOL, MACEY CTR, SOCORRO, NM SP Int Astron Union, Commiss 28 Galaxies, Int Astron Union, Commiss 40 Radio Astron, Union Radio Sci Int, Commiss J Radio Astron, Associated Univ Inc HO NEW MEXICO INST MIN & TECHNOL, MACEY CTR AB We report the first VLBI images of the NGC1068 H2O maser that include the full 600 km s(-1) spread of the emission. The structure of the source is suggestive of an edge-on massive disk that is probably bound by the central engine of this AGN. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-64-3 J9 ASTR SOC P PY 1998 VL 144 BP 221 EP 222 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75N UT WOS:000076608500095 ER PT B AU Argon, AL Greenhill, LJ Moran, JM Reid, MJ Menten, KM AF Argon, AL Greenhill, LJ Moran, JM Reid, MJ Menten, KM BE Zensus, JA Taylor, GB Wrobel, JM TI Proper motions and the distance to a water vapor maser in the galaxy M33 SO RADIO EMISSION FROM GALACTIC AND EXTRAGALACTIC COMPACT SOURCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 164 on Radio Emission from Galactic and Extragalactic Compact Sources CY APR 21-26, 1997 CL NEW MEXICO INST MIN & TECHNOL, MACEY CTR, SOCORRO, NM SP Int Astron Union, Commiss 28 Galaxies, Int Astron Union, Commiss 40 Radio Astron, Union Radio Sci Int, Commiss J Radio Astron, Associated Univ Inc HO NEW MEXICO INST MIN & TECHNOL, MACEY CTR AB The relative proper motions of water vapor maser features in the H II region IC 133 have been used to determine a distance to the galaxy M33 that is independent of the usual calibrations associated with extragalactic distance estimates, e.g., extinction and metallicity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Argon, AL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, 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 1-886733-64-3 J9 ASTR SOC P PY 1998 VL 144 BP 235 EP 236 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75N UT WOS:000076608500102 ER PT B AU Trotter, AS Moran, JM Greenhill, LJ AF Trotter, AS Moran, JM Greenhill, LJ BE Zensus, JA Taylor, GB Wrobel, JM TI Water maser emission and the parsec-scale jet in NGC 3079 SO RADIO EMISSION FROM GALACTIC AND EXTRAGALACTIC COMPACT SOURCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 164 on Radio Emission from Galactic and Extragalactic Compact Sources CY APR 21-26, 1997 CL NEW MEXICO INST MIN & TECHNOL, MACEY CTR, SOCORRO, NM SP Int Astron Union, Commiss 28 Galaxies, Int Astron Union, Commiss 40 Radio Astron, Union Radio Sci Int, Commiss J Radio Astron, Associated Univ Inc HO NEW MEXICO INST MIN & TECHNOL, MACEY CTR AB We have imaged the H2O maser and 22, 8, & 5 GHz continuum in the nucleus of NGC 3079, using the NRAO VLBA. The maser features are distributed over similar to 2 pc along an axis aligned with the plane of the kpc-scale edge-on molecular disk. The masers are not angularly coincident with any detected continuum emission. The two brightest continuum features, which trace a parsec-scale jet, have similar spectra that peak at frequencies nu > 5 GHz. We also detected faint maser emission along the jet axis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Trotter, AS (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 1-886733-64-3 J9 ASTR SOC P PY 1998 VL 144 BP 239 EP 240 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75N UT WOS:000076608500104 ER PT B AU Reid, MJ Readhead, ACS Vermeulen, RC Treuhaft, RN AF Reid, MJ Readhead, ACS Vermeulen, RC Treuhaft, RN BE Zensus, JA Taylor, GB Wrobel, JM TI Toward a trigonometric parallax of Sgr A* SO RADIO EMISSION FROM GALACTIC AND EXTRAGALACTIC COMPACT SOURCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 164 on Radio Emission from Galactic and Extragalactic Compact Sources CY APR 21-26, 1997 CL NEW MEXICO INST MIN & TECHNOL, MACEY CTR, SOCORRO, NM SP Int Astron Union, Commiss 28 Galaxies, Int Astron Union, Commiss 40 Radio Astron, Union Radio Sci Int, Commiss J Radio Astron, Associated Univ Inc HO NEW MEXICO INST MIN & TECHNOL, MACEY CTR AB We initiated a project with the VLBA to measure directly the distance to the Galactic Center, R-0, via a trigonometric parallax. Here we describe the observing program and the first results-direct imaging of the effects of the Sun's orbit about the Galactic Center. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 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 1-886733-64-3 J9 ASTR SOC P PY 1998 VL 144 BP 335 EP 336 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75N UT WOS:000076608500146 ER PT B AU Strelnitski, VS Alexander, J Moran, JM Reid, MJ AF Strelnitski, VS Alexander, J Moran, JM Reid, MJ BE Zensus, JA Taylor, GB Wrobel, JM TI Spatially resolved H2O masers as probes of supersonic turbulence SO RADIO EMISSION FROM GALACTIC AND EXTRAGALACTIC COMPACT SOURCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 164 on Radio Emission from Galactic and Extragalactic Compact Sources CY APR 21-26, 1997 CL NEW MEXICO INST MIN & TECHNOL, MACEY CTR, SOCORRO, NM SP Int Astron Union, Commiss 28 Galaxies, Int Astron Union, Commiss 40 Radio Astron, Union Radio Sci Int, Commiss J Radio Astron, Associated Univ Inc HO NEW MEXICO INST MIN & TECHNOL, MACEY CTR AB VLBI of the H2O maser sources associated with outflows from young stars reveals, besides the regular velocity component (expansion and rotation), a random component suggestive of highly supersonic turbulence generated by the interaction of the star's jets with the quiescent ambient gas. Our analysis of the geometry and velocity statistics in Sgr B-2(M)-H2O demonstrates low fractal dimension of the turbulence and strong deviations of the velocity increments from Gaussian statistics-both indicating strong intermittency of the turbulent energy dissipation. These properties are discussed, along with the two-point velocity scaling law, and compared with the related properties of incompressible turbulence. C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Strelnitski, VS (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 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 1-886733-64-3 J9 ASTR SOC P PY 1998 VL 144 BP 369 EP 370 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75N UT WOS:000076608500163 ER PT B AU Ratner, MI Lebach, DE Shapiro, II Bartel, N Bietenholz, MF Ransom, RR Lestrade, JF AF Ratner, MI Lebach, DE Shapiro, II Bartel, N Bietenholz, MF Ransom, RR Lestrade, JF BE Zensus, JA Taylor, GB Wrobel, JM TI Progress in VLBI stellar astrometry for the NASA Stanford Relativity Mission (Gravity Probe B) SO RADIO EMISSION FROM GALACTIC AND EXTRAGALACTIC COMPACT SOURCES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT IAU Colloquium 164 on Radio Emission from Galactic and Extragalactic Compact Sources CY APR 21-26, 1997 CL NEW MEXICO INST MIN & TECHNOL, MACEY CTR, SOCORRO, NM SP Int Astron Union, Commiss 28 Galaxies, Int Astron Union, Commiss 40 Radio Astron, Union Radio Sci Int, Commiss J Radio Astron, Associated Univ Inc HO NEW MEXICO INST MIN & TECHNOL, MACEY CTR AB The NASA/Stanford Relativity Mission (Gravity Probe B) is to test the unverified "frame-dragging" prediction of general relativity through measurements of the precessions of orbiting gyroscopes. For mission accuracy goals to be met, the proper motion of a "guide star," whose position will be used as an inertial reference, must be determined in an extragalactic reference frame with a standard error less than 0.5 mas/yr. We discuss our VLBI observations of the current guide-star candidates (radio stars HR1099, HR5110, and HR8703) and our techniques for obtaining differential astrometric positions with the needed accuracy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ratner, MI (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 1-886733-64-3 J9 ASTR SOC P PY 1998 VL 144 BP 385 EP 386 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL75N UT WOS:000076608500171 ER PT J AU Rocha, CEF Iliffe, TM Reid, JW Suarez-Morales, E AF Rocha, CEF Iliffe, TM Reid, JW Suarez-Morales, E TI A new species of Halicyclops (Copepoda, Cyclopoida, Cyclopidae) from cenotes of the Yucatan Peninsula, Mexico, with an identification key for the species of the genus from the Caribbean region and adjacent areas SO SARSIA LA English DT Article DE Copepoda; Halicyclops; Caribbean fauna; cenotes; Mexico ID CRUSTACEA AB Halicyclops cenoticola sp. nov. is described from cenotes of the Yucatan Peninsula, Mexico. The new species shares exclusively with H. caridophilus and H. tetracanthus the presence of 2 inner setae on the leg 5 exopod in the males. As far as is known, the new species is distinguished from all its congeners in having the dorsal caudal seta as long as the outer middle caudal seta; legs 2 and 3 are dimorphic concerning the structure of the 3 inner setae on the. terminal endopodal segment; and leg 6 of both the male and female consists of only 2 elements. An identification key for the Halicyclops species known from the Caribbean Region, the Gulf uf Mexico. Bermuda, and the coast of French Guiana is included. C1 Univ Sao Paulo, Inst Biociencias, Dept Zool, BR-05422970 Sao Paulo, Brazil. Texas A&M Univ, Dept Marine Biol, Galveston, TX 77553 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Colegio Frontera Sur Chetumal, Chetumal 77000, Quintana Roo, Mexico. RP Rocha, CEF (reprint author), Univ Sao Paulo, Inst Biociencias, Dept Zool, Caixa Postal 11461, BR-05422970 Sao Paulo, Brazil. NR 33 TC 6 Z9 8 U1 0 U2 0 PU UNIV BERGEN PI BERGEN PA DEPT FISHERIES/MAR. BIOLOGY BERGEN HIGH TECH CTR, N-5020 BERGEN, NORWAY SN 0036-4827 J9 SARSIA JI Sarsia PY 1998 VL 83 IS 5 BP 387 EP 399 PG 13 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 153EH UT WOS:000077819800004 ER PT S AU Kurosu, TP Chance, KV Spurr, RJD AF Kurosu, TP Chance, KV Spurr, RJD BE Russell, JE TI Cloud retrieval algorithm for the European Space Agency's Global Ozone Monitoring Experiment SO SATELLITE REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE III SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Satellite Remote Sensing of Clouds and the Atmosphere III CY SEP 21-23, 1998 CL BARCELONA, SPAIN SP CNR, NASA, European Opt Soc, Commiss European Communities, Directorate Gen Sci Res & Dev, Soc Photo Opt Instrumentat Engineers DE cloud detection; cloud retrieval; satellite remote sensing; GOME ID ROTATIONAL RAMAN-SCATTERING; BACKSCATTER ULTRAVIOLET MEASUREMENTS; RADIATIVE-TRANSFER MODEL; TOP HEIGHT; A-BAND; SATELLITE; GOMETRAN AB The Global Ozone Monitoring Experiment (GOME) on board the ERS-2 satellite is an across-track nadir-viewing spectrometer which measures solar light reflected from the Earth's atmosphere and surface in the UV visible. The cloud retrieval algorithm presented here combines spectral threshold tests on GOME's broad-band radiances (similar to 150 nm spectral resolution) with the fitting of reflectances to GOME's moderately high resolution spectra (0.4 nm) in and around the O-2 A band to retrieve cloud-cover fraction, cloud-top height and cloud optical thickness. The algorithm utilizes the latest O-2 spectroscopic data and features dynamical updating procedures to provide global threshold sets of GOME reflectances. Auxiliary information is obtained from GOME measurements of the Ring effect and the degree of polarization of the Earth's radiation field. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurosu, TP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 24 TC 2 Z9 2 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2954-6 J9 P SOC PHOTO-OPT INS PY 1998 VL 3495 BP 17 EP 26 DI 10.1117/12.332696 PG 4 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BM38V UT WOS:000078582400003 ER PT S AU Chance, K Spurr, RJD Kurosu, TP AF Chance, K Spurr, RJD Kurosu, TP BE Russell, JE TI Atmospheric trace gas measurements from the European Space Agency's Global Ozone Monitoring Experiment SO SATELLITE REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE III SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Satellite Remote Sensing of Clouds and the Atmosphere III CY SEP 21-23, 1998 CL BARCELONA, SPAIN SP CNR, NASA, European Opt Soc, Commiss European Communities, Directorate Gen Sci Res & Dev, Soc Photo Opt Instrumentat Engineers DE remote sensing; GOME; stratosphere; troposphere AB The Global Ozone Monitoring Experiment (GOME) was launched on the European Space Agency's ERS-2 satellite on April 20, 1995. GOME measures the Earth's atmosphere in the nadir geometry, using four spectrometers that cover the UV and visible (238-794 nm) at moderate resolution (0.2 nm in the UV, 0.4 nm in the visible), employing silicon diode array detectors. GOME takes some 30,000 spectra per day, obtaining full global coverage at 40x320 km(2) resolution in three days. It provides measurements of ozone (including the tropospheric distribution), NO2, SO2, H2CO, H2O, BrO, ClO, and OClO. We directly fit GOME radiance spectra using nonlinear least-squares analysis to obtain column amounts of several trace species, including ClO, BrO, SO2, and H2CO. The use of recent improvements in the underlying physics and spectroscopy permits the fitting of radiances to very high precision, approaching 2x10(-4)(optical thickness) in favorable cases, for standard 1.5 s integration time GOME measurements. Examples of the fitting of BrO and SO2 are presented here. 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 9 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2954-6 J9 P SOC PHOTO-OPT INS PY 1998 VL 3495 BP 230 EP 234 DI 10.1117/12.332701 PG 3 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BM38V UT WOS:000078582400024 ER PT B AU Kochanek, CS AF Kochanek, CS BE Smith, EP Koratkar, A TI Gravitational lenses and NGST SO SCIENCE WITH THE NGST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Science with the NGST CY APR 07-09, 1997 CL GODDARD SPACE FLIGHT CTR, GREENBELT, MD SP Natl Aeronaut & Space Adm, Space Telescope Sci Inst, European Space Agcy, TRW Inc, Astron Soc Pacific HO GODDARD SPACE FLIGHT CTR AB We briefly review the status of gravitational lensing observations, their problems, and NGST as the solution. We also discuss the lensing effects expected for any population of very high redshift sources (z > 5) found by NGST. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, 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 1-886733-53-8 J9 ASTR SOC P PY 1998 VL 133 BP 96 EP 105 PG 10 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BK82A UT WOS:000073481000010 ER PT B AU Boroson, B AF Boroson, B BE Brandt, JC Ake, TB Petersen, CC TI GHRS observations of X-ray binaries SO SCIENTIFIC IMPACT OF THE GODDARD HIGH RESOLUTION SPECTROGRAPH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on the Scientific Impact of the Goddard High Resolution Spectrograph CY SEP 11-12, 1996 CL GODDARD SPACE FLIGHT CTR, GREENBELT, MD HO GODDARD SPACE FLIGHT CTR AB The GHRS has brought to the study of X-ray binaries the ability to resolve the doppler shifts of accretion flows (typically several hundred km s(-1)) in the strong UV emission lines. Four major observing programs used the GHRS to observe neutron-star X-ray binaries, including Scorpius X-l and Cygnus X-2 (fed by Roche lobe overflow of low mass companions), the massive wind-fed system LMC X-4, and the intermediate mass X-ray pulsar Hercules X-l. Strong emission lines of N v, Si Iv, O v, C Iv, and He II provide a wealth of information about abundances and X-ray illumination of accreting gas. Doppler shifts and doublet ratios provide powerful diagnostics of accretion disks and wind flows. Finally, these observations combined high spectral resolution with high time resolution (readout times as low as 50 ms), allowing rapid UV variability to be correlated with X-ray variability (all four sources were observed simultaneously with the Advanced Satellite for Cosmology & Astrophysics of the Rossi X-ray Timing Explorer). Physical implications of all four observations are reviewed. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Boroson, B (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 1-886733-63-5 J9 ASTR SOC P PY 1998 VL 143 BP 99 EP 112 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74U UT WOS:000076566800008 ER PT B AU Evans, NR Bohm-Vitense, E Beck-Winchatz, B Carpenter, K Robinson, R AF Evans, NR Bohm-Vitense, E Beck-Winchatz, B Carpenter, K Robinson, R BE Brandt, JC Ake, TB Petersen, CC TI The mass of the classical Cepheid S Muscae SO SCIENTIFIC IMPACT OF THE GODDARD HIGH RESOLUTION SPECTROGRAPH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on the Scientific Impact of the Goddard High Resolution Spectrograph CY SEP 11-12, 1996 CL GODDARD SPACE FLIGHT CTR, GREENBELT, MD HO GODDARD SPACE FLIGHT CTR AB Cepheid masses are a key element used to test evolutionary tracks of intermediate-mass stars. Using the GHRS in the Echelle-B mode, we have measured the orbital radial-velocity changes for the com panion of the Cepheid S Muscae (S Muscae B). Spectra taken at minimum and maximum orbital velocities were cross-correlated and produced a velocity difference of 30.6 +/- 1.0 km s(-1). The Cepheid orbital-velocity difference for the same phases is 26.9 +/- 0.4 km s(-1), leading to a mass ratio of 1.14 +/- 0.03. Determinations of the spectral type of the companion S Mus B range from B3 V to B5 V, with an average spectral type of B3.8 V. This spectral type combined with the main-sequence mass-spectral type relation from Andersen (1991) and Harmanec (1988) results in a mass of 5.2 +/- 0.2 M.. This mass and the mass ratio yield a mass of 5.9 (+0.7)(-0.6) M. for the Cepheid S Muscae A. This mass plus the absolute magnitude of M-V = -4.29 (log L/L. = 3.62) of the Cepheid indicate that core convective overshoot in its main-sequence progenitor was slightly in excess of the value used to produce the Geneva evolutionary tracks. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Carpenter, Kenneth/D-4740-2012 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 1-886733-63-5 J9 ASTR SOC P PY 1998 VL 143 BP 309 EP 312 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74U UT WOS:000076566800035 ER PT B AU Evans, NR Bohm-Vitense, E Beck-Winchatz, B Carpenter, K Robinson, R AF Evans, NR Bohm-Vitense, E Beck-Winchatz, B Carpenter, K Robinson, R BE Brandt, JC Ake, TB Petersen, CC TI The mass of the classical Cepheid V350 Sgr SO SCIENTIFIC IMPACT OF THE GODDARD HIGH RESOLUTION SPECTROGRAPH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on the Scientific Impact of the Goddard High Resolution Spectrograph CY SEP 11-12, 1996 CL GODDARD SPACE FLIGHT CTR, GREENBELT, MD HO GODDARD SPACE FLIGHT CTR AB Two medium-resolution spectra of the hot (B9.0 V) companion of the Cepheid V350 Sgr have been obtained in the wavelength range 1840 to 1880 Angstrom using the GHRS. These spectra are very similar to the spectra of the AO V standard alpha Lyr convolved with a rotational-broadening function of 150 km s(-1), indicating that V350 Sgr B has a high rotational velocity. The velocity difference between the spectra of V350 Sgr B at two orbital phases is measured to be 22.1 +/- 8 km s(-1). The large error results primarily from the high rotational velocity. The orbital velocity of the Cepheid at the same two phases is known from the ground-based orbit determined by Evans & Sugars (1997). The spectral type of the companion was determined from comparing IUE low-resolution spectra with spectral standard stars. V350 Sgr B is an excellent match with the B9 V standard. Using the new data on the masses of eclipsing binaries from Andersen (1991), this corresponds to a mass of 2.5 +/- 0.1 M.. Combining this mass with the orbital-velocity amplitude ratio of the Cepheid and the companion, a mass of 5.0 +/- 2.0 M. is derived for the Cepheid. A Cepheid mass, together with its luminosity, is a good test of evolutionary calculations. Specifically, main-sequence core convective overshoot is a parameter that affects the later stages of evolution strongly, but is still uncertain. Unfortunately, because of the large error in the mass determination of V350 Sgr A, it is only a weak discriminant between overshoot values. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Carpenter, Kenneth/D-4740-2012 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 1-886733-63-5 J9 ASTR SOC P PY 1998 VL 143 BP 313 EP 316 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74U UT WOS:000076566800036 ER PT B AU Smith, PL Thorne, AP Learner, RCM Pickering, JC Kling, R Mende, W Kock, M AF Smith, PL Thorne, AP Learner, RCM Pickering, JC Kling, R Mende, W Kock, M BE Brandt, JC Ake, TB Petersen, CC TI Improved VUV spectroscopy of doubly ionized atoms SO SCIENTIFIC IMPACT OF THE GODDARD HIGH RESOLUTION SPECTROGRAPH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on the Scientific Impact of the Goddard High Resolution Spectrograph CY SEP 11-12, 1996 CL GODDARD SPACE FLIGHT CTR, GREENBELT, MD HO GODDARD SPACE FLIGHT CTR AB The high quality of satellite observations of stellar VUV spectra has underlined the inadequacy of the laboratory data base used to interpret these observations, particularly for the spectra of doubly charged ions. We report use of a Penning discharge and a VUV Fourier Transform Spectrometer to study the spectrum of Fe2+ (Fe III) with high resolution and good signal-to-noise ratio. Use of this apparatus should produce VUV wavelengths with uncertainties of a few parts in 10(7) and branching ratios with uncertainties of a few percent. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, PL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 6 Z9 6 U1 2 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-886733-63-5 J9 ASTR SOC P PY 1998 VL 143 BP 395 EP 398 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74U UT WOS:000076566800058 ER PT S AU Eff-Darwich, A Perez-Hernandez, F AF Eff-Darwich, A Perez-Hernandez, F GP EUROPEAN SPACE AGCY EUROPEAN SPACE AGCY TI A modified SOLA structure inversion technique SO SOHO 6/GONG 98 WORKSHOP ON STRUCTURE AND DYNAMICS OF THE INTERIOR OF THE SUN AND SUN-LIKE STARS, VOLS 1 AND 2: VOL 1: SESSIONS I-III, VOL 2: SESSIONS IV-VI SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT SOHO 6/GONG 98 Workshop on Structure and Dynamics of the Interior of the Sun and Sun-Like Stars CY JUN 01-04, 1998 CL BOSTON, MA SP European Space Agcy, NASA, Natl Sci Fdn, Smithsonian Astrophys Observ DE solar interior structure; inversions AB In a previous work (Eff-Darwich & Perez-Hernandez 1997), it was presented a new inversion method based on the Regularized Least Squares technique. This method, called OMD (Optimal Mesh Distribution) finds the optimal mesh and smoothing function by means of a deep analysis of the basis functions of the inversion problem. In the present work, the spatial resolution analysis developed for OMD to find the optimal mesh, has been adapted to a different inversion procedure, the SOLA (Substractive Optimal Local Averages) method (Pijpers & Thompson 1994). With the modification we have implemented in SOLA, the time and work necessary to obtain the solution have been minimised. Such modification consists on defining the width of the averaging kernels (critical point in SOLA) from the spatial resolution derived for OMD. The modified SOLA method has been successfully applied to structure inversions. A comparison with other inversion techniques allows us to study the effects of the inversion procedure in the solution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eff-Darwich, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 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 92-9092-672-4 J9 ESA SP PUBL PY 1998 VL 418 BP 449 EP 452 PN 1&2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM37B UT WOS:000078509100085 ER PT S AU Baudin, F Korzennik, SG AF Baudin, F Korzennik, SG GP EUROPEAN SPACE AGCY EUROPEAN SPACE AGCY TI On the precision of time/distance measurements SO SOHO 6/GONG 98 WORKSHOP ON STRUCTURE AND DYNAMICS OF THE INTERIOR OF THE SUN AND SUN-LIKE STARS, VOLS 1 AND 2: VOL 1: SESSIONS I-III, VOL 2: SESSIONS IV-VI SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT SOHO 6/GONG 98 Workshop on Structure and Dynamics of the Interior of the Sun and Sun-Like Stars CY JUN 01-04, 1998 CL BOSTON, MA SP European Space Agcy, NASA, Natl Sci Fdn, Smithsonian Astrophys Observ DE sun; local seismology; uncertainty estimation AB "Time-distance" analysis is an emerging tool for local helioseismology, pioneered by Duvall et al. 1993. Like other seismological analysis techniques, time-distance analysis allow us to infer internal physical properties of the Sun from measurements made at the surface by solving an inverse problem. In the case of time-distance analysis, the observed quantities are travel times of acoustic waves from one point of the surface to another (or between group of points). These travel times are estimated by fitting a wavelet to the correlation function computed from time-series of velocities averaged along annuli of given radius. The precision with which these measurements can be made is a crucial parameter of the inverse problem, and controls the achievable trade-off between resolution and uncertainty magnification. In the work presented here, we investigate the precision of these measurements, and how this precision varies with some of the parameters of the analysis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Baudin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 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 92-9092-672-4 J9 ESA SP PUBL PY 1998 VL 418 BP 611 EP 615 PN 1&2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM37B UT WOS:000078509100114 ER PT S AU Eff-Darwich, A Korzennik, SG AF Eff-Darwich, A Korzennik, SG GP EUROPEAN SPACE AGCY EUROPEAN SPACE AGCY TI The rotation of the solar core: Compatibility of the different data sets available SO SOHO 6/GONG 98 WORKSHOP ON STRUCTURE AND DYNAMICS OF THE INTERIOR OF THE SUN AND SUN-LIKE STARS, VOLS 1 AND 2: VOL 1: SESSIONS I-III, VOL 2: SESSIONS IV-VI SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT SOHO 6/GONG 98 Workshop on Structure and Dynamics of the Interior of the Sun and Sun-Like Stars CY JUN 01-04, 1998 CL BOSTON, MA SP European Space Agcy, NASA, Natl Sci Fdn, Smithsonian Astrophys Observ DE solar interior rotation; inversions AB A combination of inverse and forward analysis techniques has been applied to p-mode rotational splittings to infer the solar rotation rate in the deeper regions of the sun (r < 0.35R.). A forward technique was used to study the compatibility of different low degree splittings sets, complemented by the well known rotation rate in the upper part of the radiative region and the convection zone (for r greater than or equal to 0.35R.). Two different inversion methods were applied to selected sets of rotational splittings in order to infer the rotation rate in the solar core (down to r approximate to 0.18R.). We also studied the signature of a super-rotating solar core (r < 0.18R.) in the different splittings data sets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eff-Darwich, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 6 Z9 6 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-672-4 J9 ESA SP PUBL PY 1998 VL 418 BP 685 EP 692 PN 1&2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM37B UT WOS:000078509100128 ER PT S AU Baudin, F Hernandez, IG Patron, J AF Baudin, F Hernandez, IG Patron, J CA SOI Ring Diagrams Team GP EUROPEAN SPACE AGCY EUROPEAN SPACE AGCY TI Homomorphic deconvolution applied to ring diagram analysis SO SOHO 6/GONG 98 WORKSHOP ON STRUCTURE AND DYNAMICS OF THE INTERIOR OF THE SUN AND SUN-LIKE STARS, VOLS 1 AND 2: VOL 1: SESSIONS I-III, VOL 2: SESSIONS IV-VI SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT SOHO 6/GONG 98 Workshop on Structure and Dynamics of the Interior of the Sun and Sun-Like Stars CY JUN 01-04, 1998 CL BOSTON, MA SP European Space Agcy, NASA, Natl Sci Fdn, Smithsonian Astrophys Observ DE sun; local seismology; ring diagrams; analysis method AB Ring diagram analysis and homomorphic deconvolution are two techniques used independently in solar seismology. The use of homomorphic deconvolution coupled to ring analysis may improve the precision of the latter technique, as the former does for regular time series analysis. In order to compare the use of the classical Fourier Transform and the homomorphic deconvolution, ring diagram analysis using both techniques has been applied to the same data set. Results are compared at different steps in the analysis, qualitatively and quantitatively. Results from the homomorphic deconvolution are similar to those of the Fourier Transform. However, some discrepancies sometimes larger than the observed uncertainties are observed, discrepancies whose origin is still unclear. The precision of the deconvolution is in general better than that of Fourier Transform, up to a factor of two in the best cases. These preliminary results encourage us to explore the possibilities of the homomorphic deconvolution coupled to ring diagram analysis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Baudin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 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 92-9092-672-4 J9 ESA SP PUBL PY 1998 VL 418 BP 721 EP 724 PN 1&2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM37B UT WOS:000078509100134 ER PT S AU Korzennik, SG AF Korzennik, SG GP EUROPEAN SPACE AGCY EUROPEAN SPACE AGCY TI Observational analysis of asymmetries in velocity and intensity power spectra SO SOHO 6/GONG 98 WORKSHOP ON STRUCTURE AND DYNAMICS OF THE INTERIOR OF THE SUN AND SUN-LIKE STARS, VOLS 1 AND 2: VOL 1: SESSIONS I-III, VOL 2: SESSIONS IV-VI SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT SOHO 6/GONG 98 Workshop on Structure and Dynamics of the Interior of the Sun and Sun-Like Stars CY JUN 01-04, 1998 CL BOSTON, MA SP European Space Agcy, NASA, Natl Sci Fdn, Smithsonian Astrophys Observ DE Sun : oscillations AB In order to properly characterize the limit spectrum of the solar oscillations, we have computed averaged power spectra of both velocity and intensity time-series, using SOI/MDI observations. We have computed 9th order sine multi-tapered power spectra and averaged small portion of these spectra, centered on the corresponding eigenfrequency, for a subset of zonal or sectoral modes. By averaging only zonal or sectoral power spectra, the resulting spatial leakage pattern is simple enough to be easily understood. We present and discussed detailed comparisons of these profiles, and show that not only the mode profile displays some intrinsic asymmetry, but that the amplitude of the spatial leaks display some asymmetry as well. Both type of asymmetries have been quantified and are shown to be a function of frequency. Comparison with the expected leakage asymmetry due to the horizontal components of the velocity indicates good agreement, to within a factor few, but fails to agree in details. The leakage asymmetry observed in intensity power spectra remains puzzling. A direct consequence of this leakage asymmetry is to offset the power distribution of unresolved power ridges (where the modes are short lived, i.e., for high frequency and/or high degree modes). It also explains the apparent frequency differences that are observed between velocity and intensity when these are estimated by fitting unresolved ridges. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 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 92-9092-672-4 J9 ESA SP PUBL PY 1998 VL 418 BP 933 EP 938 PN 1&2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BM37B UT WOS:000078509100175 ER PT S AU Fruscione, A AF Fruscione, A BE Walker, HJ Welsh, WF Caraveo, PA Gabriel, A TI AGN variability: An extreme ultraviolet view from deep EUVE observations SO SPACE BASED ASTRONOMY: ISO, AGN, RADIOPULSARS AND THE SUN SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT E1.3, E1.4, E1.5 and E2.3 Symposia of COSPAR Scientific Commission E on Space Based Astronomy - ISO, AGN Radiopulsars and the Sun at the 31st COSPAR Scientific Assembly CY JUL 14-21, 1996 CL BIRMINGHAM, ENGLAND SP Comm Space Res, European Space Agcy, Inst Space & Astronaut Sci, Int Astron Union AB We present highlights from the most recent results on extreme ultraviolet (EUV) variability-obtained during some very long observations (more than 3 weeks in a few cases) of extragalactic objects with the Extreme Ultraviolet Explorer (EUVE) satellite. (C)1998 COSPAR. Published by Elsevier Science Ltd. C1 Smithsonian Astrophys Observ, Cambridge, MA 02178 USA. RP Fruscione, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-70, Cambridge, MA 02178 USA. NR 10 TC 2 Z9 2 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0273-1177 BN 0-08-043310-3 J9 ADV SPACE RES PY 1998 VL 21 IS 1-2 BP 83 EP 86 DI 10.1016/S0273-1177(97)00617-0 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BK61F UT WOS:000072736800011 ER PT S AU Vial, JC Koutchmy, S Habbal, SR AF Vial, JC Koutchmy, S Habbal, SR CA Cor-I Team BE Walker, HJ Welsh, WF Caraveo, PA Gabriel, A TI Cor-I: A coronal white-light imager for a solar probe SO SPACE BASED ASTRONOMY: ISO, AGN, RADIOPULSARS AND THE SUN SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT E1.3, E1.4, E1.5 and E2.3 Symposia of COSPAR Scientific Commission E on Space Based Astronomy - ISO, AGN Radiopulsars and the Sun at the 31st COSPAR Scientific Assembly CY JUL 14-21, 1996 CL BIRMINGHAM, ENGLAND SP Comm Space Res, European Space Agcy, Inst Space & Astronaut Sci, Int Astron Union AB Solar and heliospheric observations acquired over several decades, have shown that the corona is a highly structured medium. There is no doubt that these structures reflect the response of the coronal plasma confined by the highly inhomogeneous magnetic field - to different forms of energy input. While in-situ plasma measurements have provided the characteristic properties of both fast and slow solar winds, they have fallen short in connecting them to the source regions of the wind. A near-Sun flyby mission offers an unprecedented opportunity to explore the solar wind at distances much closer to the Sun than ever achieved before. However, it is essential that in-situ measurements be coordinated with simultaneous <(imaging)under bar> of the structures encountered in the corona. We present the concept and design of a white-light imager called Cor-I, as a key instrument for a near-Sun flyby mission which makes it possible to distinguish spatial structures from temporal changes in the plasma parameters. With the inference of the electron density from the Thomson scattered emission, white-light measurements are also a very powerful tool for quantitative studies of the acceleration region of the solar wind. In addition, the proposed instrument carries the potential for discovery of transient events and waves in these parts of the acceleration region of fast and slow solar winds that are inaccessible to in-situ plasma instruments. (C) 1998 COSPAR. Published by Elsevier Science Ltd. C1 Inst Astrophys Spatiale, F-91405 Orsay, France. Inst Astrophys, F-75014 Paris, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vial, JC (reprint author), Inst Astrophys Spatiale, F-91405 Orsay, France. NR 8 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 0-08-043310-3 J9 ADV SPACE RES PY 1998 VL 21 IS 1-2 BP 291 EP 294 DI 10.1016/S0273-1177(97)00983-6 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BK61F UT WOS:000072736800037 ER PT J AU Raymond, JC Suleiman, R Kohl, JL Noci, G AF Raymond, JC Suleiman, R Kohl, JL Noci, G TI Elemental abundances in coronal structures SO SPACE SCIENCE REVIEWS LA English DT Review DE abundances; coronal streamers ID SOLAR-FLARES; IRON; PLASMAS AB A great deal of evidence for elemental abundance variations among different structures in the solar corona has accumulated over the years. Many of the observations show changes in the relative abundances of high- and low-First Ionization Potential elements, but relatively few show the absolute elemental abundances. Recent observations from the SOHO satellite give absolute abundances in coronal streamers. Along the streamer edges, and at low heights in the streamer, they show roughly photospheric abundances for the low-FIP elements, and a factor of 3 depletion of high-PIP elements. In the streamer core at 1.5 R., both high- and low-PIP elements are depleted by an additional factor of 3, which appears to result from gravitational settling. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, I-50125 Florence, Italy. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu; kohl@cfa.harvard.edu NR 24 TC 16 Z9 16 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PY 1998 VL 85 IS 1-2 BP 283 EP 289 DI 10.1023/A:1005162803316 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 149ZF UT WOS:000077636600026 ER PT J AU Cranmer, SR Kohl, JL Noci, G AF Cranmer, SR Kohl, JL Noci, G TI UVCS/SOHO: The first two years SO SPACE SCIENCE REVIEWS LA English DT Review DE corona; solar wind; UV radiation; spectroscopy; line profiles ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; EXTENDED SOLAR CORONA; VELOCITY DISTRIBUTIONS; WIND; HYDROGEN AB The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) has observed the extended solar corona between 1 and 10 R. for more than two years. We review spectroscopic and polarimetric measurements made in coronal holes, equatorial streamers, and coronal mass ejections, as well as selected non-solar targets. UVCS/SOHO has provided a great amount of empirical information about the physical processes that heat and accelerate the solar wind, and about detailed coronal structure and evolution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, I-50125 Florence, Italy. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kohl@cfa.harvard.edu NR 43 TC 8 Z9 8 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PY 1998 VL 85 IS 1-2 BP 341 EP 348 DI 10.1023/A:1005175106042 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 149ZF UT WOS:000077636600031 ER PT S AU Reasenberg, RD Phillips, JD AF Reasenberg, RD Phillips, JD BE Bely, PY Breckinridge, JB TI Design of a spaceborne astrometric survey instrument SO SPACE TELESCOPES AND INSTRUMENTS V, PTS 1-2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Space Telescopes and Instruments V Conference CY MAR 25-28, 1998 CL KONA, HI SP Int Soc Optical Engn, European So Observ DE astrometry; space; instrument; optical AB We have investigated the design of a small astrometric and photometric survey instrument in the Hipparcos tradition. Such a mission will support a rich and diverse ensemble of scientific investigations. The design objectives, which have been met in this study, are to be able to measure 10(7) stars over the full sky, with an accuracy of 0.05 mas for mag < 9 and 20 mas for mag 15. A scanning survey instrument that uses CCD detectors is able to measure many stars simultaneously. As compared to a pointed astrometric instrument of comparable size, the survey instrument generally has much higher measurement throughput (sum over targets of the inverse variance), but on average, less scientific interest per target. An instrument for astrometry, unlike those for imaging, can be compact and yet scientifically productive. We report on a study of a Fast Astrometric Mapping Explorer (FAME-98) and an examination of standard approaches for scanning astrometric missions. We fmd some of these standard approaches wanting. We have concluded that a scanning astrometric instrument performs better if it spins faster, precesses faster, and has a shorter focal length than is conventionally expected. Further, we have shown that the use of solar radiation pressure instead of gas jets, as a means of precessing the spacecraft, yields a stronger astrometric solution, because the rotation is not broken into disjoint segments. Finally, we have shown that an elongated primary mirror is not advantageous, and that the central portion of the primary mirror contributes little to the astrometric accuracy of the instrument. A first look at the pivotal issue of systematic error has uncovered no serious problems, although careful engineering will be essential. Because the spacecraft is equipped with a solar shield, which keeps it in shadow, the temperatures of critical instrument components are stable at the mK level on the time scale of the spacecraft rotation period. The analysis has underscored three instrumental differences between a survey astrometric mission and a pointed astrometric mission. For a survey mission, the aperture shape does not matter, a large-area detector enhances the scientific throughput, and there is no advantage to an interferometer over a telescope. 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 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2803-5 J9 P SOC PHOTO-OPT INS PY 1998 VL 3356 BP 622 EP 634 DI 10.1117/12.324484 PN 1-2 PG 13 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL60U UT WOS:000075998200061 ER PT S AU Phillips, JD Reasenberg, RD AF Phillips, JD Reasenberg, RD BE Bely, PY Breckinridge, JB TI Optical system for an astrometric survey from space SO SPACE TELESCOPES AND INSTRUMENTS V, PTS 1-2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Space Telescopes and Instruments V Conference CY MAR 25-28, 1998 CL KONA, HI SP Int Soc Optical Engn, European So Observ DE astrometry; space; instrument; optical design; estimation AB We present an optical design for a spaceborne instrument, of about 1/2 m aperture, to perform a combined astrometric and photometric survey via a scan similar to that of Hipparcos. A CCD detector array with Time Delayed Integration will permit an astrometric mission accuracy better than 50 microarcseconds for stars brighter than 10th magnitude, 1 1/2 orders better than Hipparcos. The passband is nominally 0.4 to 0.9 microns. For the instrument to have both high measurement rate and high accuracy, the optical system must satisfy several requirements. It should have aberration well under diffraction, for high precision in centroiding and as a means of keeping unmodeled shifts of the image centroids small. The system should have a wide field of view so that there is a large overlap of successive scans, have a large field of view for scientific throughput (sum over targets of the inverse variance), and have low image distortion so that the stellar images move at constant rate along columns of detector pixels. The design presented meets these requirements using aspheric surfaces that are manufacturable. We have demonstrated that the instrument will determine the temperature of an observed star without requiring a dispersive element or color filters. The design is thus free of transmissive elements, and protected from the systematic errors that they might have induced, e.g., due to thermal variation and to chromatic effects. This study was inspired by our previous consideration of scientific throughput. Our study of data reduction from a scanning astrometric survey mission demonstrated that there is a substantial gain in mission accuracy if the spacecraft precesses without discontinuities such as those that result from gas jet firings. Our study of methods of precessing the spacecraft showed that smooth rotation would be possible using solar radiation pressure, but only if the spacecraft rotation rate were increased. Maintaining the integration time for each object would require an optical design of shorter focal length. Meanwhile, our study of mission accuracy as a function of focal length showed that another increase of accuracy would result from shorter focal length, via the greater number of lower-accuracy measurements. Therefore we performed this optical study to find a design with shorter focal length, having a proportionate increase in field of view. We conceived and investigated a family of short focal length, wide-field designs, and developed a methodology to facilitate selection from among them. The new baseline design achieves diffraction-limited images over a 2.2 degrees FOV with a 1.1 degrees square central blockage, and has a 7.5 m focal length. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Phillips, JD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St,MS63, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2803-5 J9 P SOC PHOTO-OPT INS PY 1998 VL 3356 BP 832 EP 843 DI 10.1117/12.324437 PN 1-2 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL60U UT WOS:000075998200082 ER PT S AU Murray, SS Chappell, JH Kenter, AT Kraft, RP Meehan, GR Zombeck, MV AF Murray, SS Chappell, JH Kenter, AT Kraft, RP Meehan, GR Zombeck, MV BE Bely, PY Breckinridge, JB TI The AXAF High Resolution Camera (HRC): The challenge of calibration SO SPACE TELESCOPES AND INSTRUMENTS V, PTS 1-2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Space Telescopes and Instruments V Conference CY MAR 25-28, 1998 CL KONA, HI SP Int Soc Optical Engn, European So Observ DE x-ray detectors; calibration; flat field; microchannel plate High Resolution Camera; AXAF AB The High Resolution Camera (HRC) is a Microchannel Plate based, photon counting, imaging detector for the Advanced X-Ray Astrophysics Facility (AXAF) that will be placed in a high earth orbit scheduled for launch in December, 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 preceded by various subsystems level calibrations of the detector components, but only through complete end-to-end testing was it possible to fully study the instrument and identify areas for improvement. As a result, several modifications were made to the HRC. These were followed by a series of flat field calibrations used to "correct" the end-to-end results for flight. C1 Smithsonian Inst Astrophys Observ, High Energy Astrophys Div, Cambridge, MA 02138 USA. RP Murray, SS (reprint author), Smithsonian Inst Astrophys Observ, High Energy Astrophys Div, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 11 Z9 11 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2803-5 J9 P SOC PHOTO-OPT INS PY 1998 VL 3356 BP 974 EP 984 DI 10.1117/12.324500 PN 1-2 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL60U UT WOS:000075998200098 ER PT S AU Barnes, PJ McDermott, WM Edgar, RJ Kellogg, EM AF Barnes, PJ McDermott, WM Edgar, RJ Kellogg, EM BE Bely, PY Breckinridge, JB TI Towards a solid-state detector response function for AXAF Calibration SO SPACE TELESCOPES AND INSTRUMENTS V, PTS 1-2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Space Telescopes and Instruments V Conference CY MAR 25-28, 1998 CL KONA, HI SP Int Soc Optical Engn, European So Observ DE AXAF; solid state detectors; detector modelling; detector response function AB As part of the extensive ground testing of the Advanced X-ray Astrophysics Facility (AXAF), x-ray detectors of standard design (flow-proportional counters and solid-state devices) were used as secondary absolute calibrators. In order to realise the overall facility calibration goal, these detectors need to be calibrated in turn on a primary x-ray standard. This exercise consists of accurately determining the detectors' response to monochromatic x-rays of different energies. Our data were obtained on various beamlines at the BESSY synchrotron storage ring, which is a very accurately calibrated standard x-ray source. Here we report progress in understanding the response function of the solid-state devices (SSDs). The response is modelled using JMKmod in the XSPEC package, and includes effects of pileup, incomplete charge collection, fluorescent escape, and other secondary processes. Knowledge of the SSD response function will permit precise removal of SSD detector effects from AXAF calibration data, and therefore allow accurate calibration of the AXAF system's effective area and other performance parameters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barnes, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 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 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2803-5 J9 P SOC PHOTO-OPT INS PY 1998 VL 3356 BP 1046 EP 1056 DI 10.1117/12.324458 PN 1-2 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BL60U UT WOS:000075998200105 ER PT S AU Lorenzini, EC Cosmo, ML Kaiser, M Bangham, M Dionne, H Vonderwell, D Johnson, L AF Lorenzini, EC Cosmo, ML Kaiser, M Bangham, M Dionne, H Vonderwell, D Johnson, L BE Middour, JW Sackett, LL DAmario, LA Byrnes, DV TI Mission analysis of a tethered system for LEO to GEO orbital transfers SO SPACEFLIGHT MECHANICS 1998, VOL 99, PTS 1 AND 2 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 8th Annual Space Flight Mechanics Meeting CY FEB 09-11, 1998 CL MONTEREY, CA SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, AAS, Space Flight Mech Tech Comm, AIAA, Astrodynam Tech Comm AB The use of spaceborne tethers is investigated for designing a reusable system to transfer payloads up to 4000 kg from LEO to GEO. The study indicates that a two-stage tethered system is preferable to a single-stage tethered system, on a mass basis, with present-day tether materials. A first stage in LEO and a second stage in medium Earth orbit provide the required Delta V for injecting the payload into geotransfer orbit. The orbits of the stages are resonant in order to provide periodic encounters and are optimized with the goal of reducing the overall system mass. The close-approach dynamics between the second stage and the payload released from the first stage is simulated to demonstrate the salient features of this non-conventional rendezvous. The system requirement of one transfer per month for two years of operation without refueling is adopted for computing the propellant needed to reboost the stages. Tn conclusion, a two-stage tethered system is more competitive, on a mass basis, than a chemical upper stage after only two transfers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lorenzini, EC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 80, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-87703-450-8 J9 ADV ASTRONAUT SCI PY 1998 VL 99 BP 3 EP 20 PN 1&2 PG 18 WC Engineering, Aerospace SC Engineering GA BL82A UT WOS:000076812300001 ER PT B AU Myers, PC Mardones, D AF Myers, PC Mardones, D BE Yun, JL Liseau, R TI Young protostars and inward motions in low-mass dense cores SO STAR FORMATION WITH INFRARED SPACE OBSERVATORY (ISO) SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Star Formation with the Infrared Space Observatory CY JUN 24-26, 1997 CL LISBON, PORTUGAL SP Univ Lisbon, Res Grp Astron & Astrophys, JNICT, Gulbenkian Fdn, Fundacao Fac Ciencias Univ Lisboa AB We present ISOCAM observations of multiple star formation in low-mass dense cores, and recent evidence for infall motions in four types of object: a sample of 47 class 0 and class I protostars, the environment of a protostar in an isolated, thermally supported dense core (L1527), the environment of a protostar in a turbulent dense core associated with a small stellar group (L1251B), and a thermally supported, low-mass starless core (L1544). The survey sample shows that class 0 and not class I sources have significant evidence for infall motions. The mapping studies show evidence for infall asymmetry extended over 0.03 - 0.1 pc. In L1544 the large spatial extent and the absence of a point source of infrared luminosity together appear inconsistent with the well-known "inside-out" collapse model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Myers, PC (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 1-886733-52-X J9 ASTR SOC P PY 1998 VL 132 BP 173 EP 182 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BK81Z UT WOS:000073480900025 ER PT B AU Dalgarno, A Stancil, PC Lepp, S AF Dalgarno, A Stancil, PC Lepp, S BE Mezzacappa, A TI Molecular processes in the early Universe SO STELLAR EVOLUTION, STELLAR EXPLOSIONS AND GALACTIC CHEMICAL EVOLUTION LA English DT Proceedings Paper CT 2nd Oak Ridge Symposium on Atomic and Nuclear Astrophysics CY DEC 02-06, 1997 CL OAK RIDGE, TN AB A review is presented of the processes that occur in the early Universe in the formation of neutral molecules and molecular ions in a gas mixture of hydrogen, deuterium, helium and lithium. Attention is drawn to processes for which more reliable data on reaction coefficients are needed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND BN 0-7503-0555-X PY 1998 BP 137 EP 143 PG 7 WC Astronomy & Astrophysics; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BL90Y UT WOS:000077110500017 ER PT B AU McCarthy, MC AF McCarthy, MC BE Mezzacappa, A TI Large organic molecules in the laboratory and in space SO STELLAR EVOLUTION, STELLAR EXPLOSIONS AND GALACTIC CHEMICAL EVOLUTION LA English DT Proceedings Paper CT 2nd Oak Ridge Symposium on Atomic and Nuclear Astrophysics CY DEC 02-06, 1997 CL OAK RIDGE, TN AB A surprising property of molecular clouds is the prevalence of highly unsaturated carbon compounds in a regime dominated by hydrogen. In rich interstellar and circumstellar sources, most of the more than 85 polyatomic molecules detected to date are linear carbon chains with alternating single and triple bonds, including 11 of the 19 with more than six atoms; many more can probably be found if rest frequencies can be measured in the laboratory. Laboratory detection has proved challenging, but recent advances have partly overcome this difficulty, yielding 28 new quite long carbon chains of astrophysical interest in the past two years; four of these have already been found in space, including the largest interstellar molecule HC11N. In addition to summarizing these developments, the results are given of several recent radioastronomical observations that demonstrate the wide distribution of the chemical bond in space and the important role carbon chains play in probing the physical and chemical conditions of interstellar molecular clouds and circumstellar shells. C1 Smithsonian Astrophys Observ, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Smithsonian Astrophys Observ, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND BN 0-7503-0555-X PY 1998 BP 205 EP 214 PG 10 WC Astronomy & Astrophysics; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BL90Y UT WOS:000077110500025 ER PT B AU Brickhouse, NS AF Brickhouse, NS BE Mezzacappa, A TI Stellar coronal structure SO STELLAR EVOLUTION, STELLAR EXPLOSIONS AND GALACTIC CHEMICAL EVOLUTION LA English DT Proceedings Paper CT 2nd Oak Ridge Symposium on Atomic and Nuclear Astrophysics CY DEC 02-06, 1997 CL OAK RIDGE, TN AB Stellar coronae cannot be spatially resolved, and yet we can infer structure using spectroscopic diagnostics and time-variable emission. Moderate resolution spectroscopic observations in the X-ray and EUV reveal features qualitatively different from solar coronal phenomena. Quantifying the properties of stellar structures is highly dependent on accurate and complete atomic data, as will be illustrated. This article will also address goals and opportunities for stellar coronal physics with the next generation of X-ray telescopes, particularly the high resolution gratings on AXAF and XMM. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Brickhouse, NS (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND BN 0-7503-0555-X PY 1998 BP 273 EP 282 PG 10 WC Astronomy & Astrophysics; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BL90Y UT WOS:000077110500033 ER PT B AU van Ballegooijen, AA AF van Ballegooijen, AA BE Balasubramaniam, KS Harvey, JW Rabin, DM TI Understanding the solar cycle SO SYNOPTIC SOLAR PHYSICS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 18th National-Solar-Observatory/Sacramento-Peak Summer Workshop on Synoptic Solar Physics CY SEP 08-12, 1997 CL SUNSPOT, NM SP Natl Solar Observ, Natl Optical Astron Observ, Natl Sci Fdn, Div Atmospher Sci, NASA, Space Sci Div, Off Space Sci, USAF, Off Sci Res, European Off Aerosp Res & Dev, Asian Off Aerosp Res & Dev, USAF, Air Force Res Lab, Space Hazards Branch AB The physical processes underlying the solar cycle are discussed. It is argued that the sun's toroidal magnetic field is stored in the lower part of the overshoot region at the base of the convection zone, and that active regions emerge as a result of occasional disturbances of this toroidal field by overshooting convection. A simple model of the dynamo is presented. Using measurements of the sun's polar magnetic flux (5 x 10(22) MX per hemisphere), I estimate that the toroidal flux at cycle maximum is about 5.5 x 10(23) Mx per hemisphere, independent of the details of the internal angular velocity distribution. The estimated rate of toroidal flux loss due to the emergence of active region is compatible with the existence of a steady cycle. The decay of active regions must involve retraction of Omega-loops in the convection zone and repair of the toroidal flux system. A simple model of this retraction process is presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Ballegooijen, AA (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 1-886733-60-0 J9 ASTR SOC P PY 1998 VL 140 BP 17 EP 29 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74T UT WOS:000076547800002 ER PT B AU Panasyuk, AV Strachan, L Fineschi, S Gardner, LD Raymond, J Kohl, JL AF Panasyuk, AV Strachan, L Fineschi, S Gardner, LD Raymond, J Kohl, JL BE Balasubramaniam, KS Harvey, JW Rabin, DM TI Tomographic reconstructions of the Corona from UVCS/SOHO synoptic observations SO SYNOPTIC SOLAR PHYSICS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 18th National-Solar-Observatory/Sacramento-Peak Summer Workshop on Synoptic Solar Physics CY SEP 08-12, 1997 CL SUNSPOT, NM SP Natl Solar Observ, Natl Optical Astron Observ, Natl Sci Fdn, Div Atmospher Sci, NASA, Space Sci Div, Off Space Sci, USAF, Off Sci Res, European Off Aerosp Res & Dev, Asian Off Aerosp Res & Dev, USAF, Air Force Res Lab, Space Hazards Branch AB Synoptic observations from the Ultraviolet Coronagraph Spectrometer on SOHO are used to obtain spectral profiles and, intensities (integrated along the line-of-sight) for a number of emission lines in the corona including H I Ly alpha and the O VI 1032/1037 doublet. The UVCS synoptic program makes a complete scan around the Sun once per day covering heights from 1.5 to 3 R. in the equatorial regions and heights from 1.5 to 2.5 R. in the polar and midlatitude regions. These data provide a direct measure of the line-of-sight velocities for the emitting atoms or ions. Further analysis can be used to derive densities, temperatures, and outflow velocities for hydrogen and O5+ ions in particular. Here we present the results from our efforts to resolve the line-of-sight distribution of intensities with the help of 3D reconstruction techniques. In theory, it is possible to resolve 3D spatial structures using these techniques but the analysis of the synoptic data can be complicated due to the fact that the corona is not stationary, but evolving over time. We will discuss these complications and some first results for the tomographic reconstructions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Panasyuk, AV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Giordano, Silvio/0000-0002-3468-8566 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 1-886733-60-0 J9 ASTR SOC P PY 1998 VL 140 BP 407 EP 411 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BL74T UT WOS:000076547800043 ER PT J AU Jakab, PL AF Jakab, PL TI The Peenemunde wind tunnels: A memoir SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Dept Aeronaut, Washington, DC 20560 USA. RP Jakab, PL (reprint author), Smithsonian Inst, Natl Air & Space Museum, Dept Aeronaut, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JAN PY 1998 VL 39 IS 1 BP 128 EP 130 DI 10.2307/3107010 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA YW246 UT WOS:000071913100009 ER PT J AU Roth, TL Weiss, RB Bush, LM Bush, M AF Roth, TL Weiss, RB Bush, LM Bush, M TI Using heterologous in vitro fertilization to evaluate sperm cryopreservation methods in the scimitar-horned oryx (Oryx dammah) SO THERIOGENOLOGY LA English DT Meeting Abstract C1 Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, Cincinnati, OH 45220 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCIENCE INC PI NEW YORK PA 655 AVENUE OF THE AMERICAS, NEW YORK, NY 10010 USA SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD JAN 1 PY 1998 VL 49 IS 1 BP 265 EP 265 DI 10.1016/S0093-691X(98)90618-5 PG 1 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA YT213 UT WOS:000071577200129 ER PT J AU Swanson, WF Penfold, LM Wildt, DE AF Swanson, WF Penfold, LM Wildt, DE TI Developmental capacity of IVF-derived domestic cat embryos following transfer to naturally-estrual, GnRH-treated recipients SO THERIOGENOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. NR 0 TC 5 Z9 5 U1 0 U2 1 PU ELSEVIER SCIENCE INC PI NEW YORK PA 655 AVENUE OF THE AMERICAS, NEW YORK, NY 10010 USA SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD JAN 1 PY 1998 VL 49 IS 1 BP 267 EP 267 DI 10.1016/S0093-691X(98)90620-3 PG 1 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA YT213 UT WOS:000071577200131 ER PT S AU Dupree, AK AF Dupree, AK BE Wamsteker, WQ Riestra, RG Harris, B TI The IUE legacy: Chromospheres and winds in cool stars SO ULTRAVIOLET ASTROPHYSICS BEYOND THE IUE FINAL ARCHIVE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Conference on Ultraviolet Astrophysics Beyond the IUE Final Archive CY NOV 11-14, 1997 CL SEVILLE, SPAIN SP European Space Agcy, European Astron Soc, Soc Espanola Astron, NASA, Particle Phys & Astron Res Council DE cool stars; chromospheres; winds; hybrid stars; Betelgeuse; Capella; Alpha Aqr AB Highlights of IUE studies for cool stars are selected and reviewed with particular emphasis on the physics of cool star atmospheres and winds. We can now define the presence and behavior of chromospheres and winds across the cool half of the Hertzsprung-Russell diagram. The longevity of the IUE satellite also created a unique opportunity to evaluate the long-term ultraviolet behavior of selected stars. Surprising variabilities, and in some cases periodicities were revealed; in other instances none appeared where expected. IUE has provided a foundation for subsequent measures at different energy bands and with different techniques using the Hubble Space Telescope and Extreme UltraViolet Explorer (EUVE) satellite. IUE spectra frequently provide the critical link between the stellar photosphere and corona to understand the structure and energy balance of a cool star atmosphere. Several classic objects are discussed in detail including: Alpha Ori (HD 39801), Capella (HD 34029), and the hybrid star Alpha Aqr (HD 209750). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dupree, AK (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 92-9092-652-X J9 ESA SP PUBL PY 1998 VL 413 BP 75 EP 82 PG 8 WC Physics, Applied SC Physics GA BK94P UT WOS:000073921300010 ER PT S AU Fineschi, S Gardner, LD Kohl, JL Romoli, M Noci, G AF Fineschi, S Gardner, LD Kohl, JL Romoli, M Noci, G BE Fineschi, S TI Grating stray-light analysis and control in the UVCS/SOHO SO X-RAY AND ULTRAVIOLET SPECTROSCOPY AND POLARIMETRY II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Ultraviolet Spectroscopy and Polarimetry II CY JUL 23-24, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE UV space optics; UV spectroscopy; stray-light ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; SOLAR AB The Ultraviolet Coronagraph Spectrometer (UVCS) of the Solar and Heliospheric (SOHO) mission has been developed for spectroscopic and polarimetric determinations of temperatures, densities and flow velocities in the extended solar corona. The instrument consists of a visible light (VL) polarimeter, and two ultraviolet (UV) spectrometers, optimized for the H I Lyman alpha (Ly-alpha) line (lambda 1216 Angstrom) and for the O VI doublet (lambda 1032/1037 Angstrom). The stray-light profile of the Ly-alpha holographic grating has been measured, in a laboratory set-up, in both the spatial and spectral directions. The observed profile has been found Go be a combination of two components: the scattering from the grating surface, and the Fraunhofer diffraction due to the vignetting of the grating. An analytical expression for the scattering component of the grating point spread function (PSF) has been derived from a simple model of the grating surface roughness. The stray-light profile generated by the analytical expression of the grating PSF gives a good fit of stray-light profile measured in the laboratory This instrument function has been be used in the analysis of in-flight UVCS observations of the profile of electron scattered Ly-alpha from the solar corona. These observations have resulted, for the first time, in the most direct measurement of the coronal electron temperature. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fineschi, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Romoli, Marco/H-6859-2012 NR 7 TC 18 Z9 18 U1 2 U2 8 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2898-1 J9 P SOC PHOTO-OPT INS PY 1998 VL 3443 BP 67 EP 74 DI 10.1117/12.333614 PG 8 WC Optics; Physics, Applied; Spectroscopy SC Optics; Physics; Spectroscopy GA BM32Q UT WOS:000078392000008 ER PT S AU Patnaude, D Pease, D Donnelly, H Juda, M Jones, C Murray, S Zombeck, M Kraft, R Kenter, A Meehan, G Elsner, R Swartz, D AF Patnaude, D Pease, D Donnelly, H Juda, M Jones, C Murray, S Zombeck, M Kraft, R Kenter, A Meehan, G Elsner, R Swartz, D BE Hoover, RB Walker, ABC TI Effective area of the AXAF high resolution camera (HRC) SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE detectors; X-rays; calibration ID PROPORTIONAL-COUNTERS; CALIBRATION; PERFORMANCE; DETECTORS AB The Advanced X-ray Astrophysics Facility High Resolution Camera was calibrated at NASA's X-ray Calibration Facility during March and April 1997. We have undertakes an analysis of the effective area of the combined High Resolution Mirror Assembly / High Resolution Camera using all data presently available from these tests. In this contribution we discuss our spectral fitting of the beam-normalization detectors, our method of removing higher order contamination lines present in the spectra, and the corrections for beam non-uniformities. Using an approach based upon the mass absorption cross-section of Cesium Iodide, we determine the quantum efficiency in the microchannel plates. We model the secondary electron absorption depth as a function of energy, which we expect to be relatively smooth. This is then combined with the most recent model of the telescope to determine the ensemble effective area for the HRC. The ensemble effective area is a product of the telescope effective area, the transmission of the UV-Ion shield, and the quantum efficiency of the microchannel plates, We focus our attention on the microchannel plate quantum efficiency, using previous results for the UV-lon shield transmission and telescope effective area. We also address future goals and concerns. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Patnaude, D (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 93 EP 105 DI 10.1117/12.331294 PG 13 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400008 ER PT S AU Graessle, DE Blake, RL Burek, AJ Dyson, SE Fitch, JJ Schwartz, DA Soufli, R AF Graessle, DE Blake, RL Burek, AJ Dyson, SE Fitch, JJ Schwartz, DA Soufli, R BE Hoover, RB Walker, ABC TI Modeling of synchrotron reflectance calibrations of AXAF iridium-coated witness mirrors over 2-12 keV SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE X-ray; AXAF; synchrotron; reflectance; optical constants ID X-RAY-SCATTERING; OPTICAL-CONSTANTS; ROUGHNESS; REFLECTIVITY AB As calibrations of AXAF mirrors in the 2-12 keV range are near completion, we can report that the archive is complete for the scheduled number of mirrors over the 5-12 keV range, and also over the 2010-6200 eV range. Analysis of the results for optical constants and coating layer parameters is now proceeding rapidly. To date, we have derived optical constants from 39 mirrors over 5-12 keV using our existing Fresnel Equation model, with uniform layers of Ir, Cr, and Zerodur, and the roughness algorithm of Nevot and Croce.(1) The analysis method has been presented in our earlier papers, but its application has been expanded to all three varieties of witness mirrors used in AXAF's qualification and production coating runs. For the first and most consistent variety, which have 1 Angstrom roughness, reflectances are indistinguishable from mirror to mirror save for thickness variations between coating runs. Residuals of the fits for optical constants become large (>1%) when reflectance values below 18% are included in the fits. If such data points are ignored, values of delta(E) and beta(E) very much like those of Henke et al. over 5-11 keV are obtained. Residuals are at the 0.6%-0.8% level, which meets calibration requirements but exceeds experimental noise. For the second variety of witness mirror, polished to obtain roughness specification similar to the flight mirrors (3-5 Angstrom), fits approximately within the noise level of the measurements may be obtained over 5-11 keV, for reflectance values down to 5%. The delta(E) is essentially the same as that obtained from the 1 iq flats; however beta(E) is higher by approximately 3-4% systematically, and the mirror-to-mirror variation is larger. The third variety of mirror was obtained with 5-7 Angstrom nominal roughness. Residuals to the fits are large for the entire range of angles, in some cases exceeding 2% with a sinusoidal character through the critical angle. Coating layer depths are similar to those found for the other mirror types, with good precision. We discuss results along with possible improvements to the model and experiments to verify it. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Graessle, DE (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 4 Z9 4 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 140 EP 159 DI 10.1117/12.331233 PG 20 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400011 ER PT S AU Allen, CL Plucinsky, PP McNamara, BR Edgar, RJ Schulz, NS Woo, JW AF Allen, CL Plucinsky, PP McNamara, BR Edgar, RJ Schulz, NS Woo, JW BE Hoover, RB Walker, ABC TI Analysis of the AXAF HRMA+ACIS effective area measurements from the XRCF SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE AXAF; ACIS; HRMA; X-rays; calibration; charge coupled devices (CCD) AB We describe the analysis of effective area measurements for the AXAF High Resolution Mirror Assembly (HRMA) and the AXAF CCD Imaging Spectrometer (ACIS). The measurements were obtained at the X-Ray Calibration Facility (XRCF) in Huntsville, AL, during April 1997. Measurements obtained with two frontside-illuminated (FI) charge-coupled devices (CCDs) in the imaging array and the backside-illuminated (BI) CCD located on-axis in the spectroscopic array are considered. We compare the XRCF effective area measurements to independent, semiempirical model predictions constructed using the product of the efficiencies of the AXAF components (mirror, filter, CCD). The XRCF measurements, in general, confirm the reliability of the model at most energies, but only after correcting the data for several effects related to event pileup. However, after applying the corrections, the the uncertainties in the XRCF measurements remain uncomfortably large. We suggest several future avenues of investigation that should improve our knowledge of the HRMA+ACIS effective area. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Allen, CL (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 198 EP 209 DI 10.1117/12.331237 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400015 ER PT S AU Zhao, P Austin, RA Edgar, RJ Elsner, RF Gaetz, TJ Graessle, DE Jerius, D Kolodziejczak, JJ McDermott, WC O'Dell, SL Sulkanen, ME Schwartz, DA Smartz, DA Tennant, AF Van Speybroeck, LP Wargelin, BJ Weisskopf, MC Zirnstein, CG AF Zhao, P Austin, RA Edgar, RJ Elsner, RF Gaetz, TJ Graessle, DE Jerius, D Kolodziejczak, JJ McDermott, WC O'Dell, SL Sulkanen, ME Schwartz, DA Smartz, DA Tennant, AF Van Speybroeck, LP Wargelin, BJ Weisskopf, MC Zirnstein, CG BE Hoover, RB Walker, ABC TI AXAF mirror effective area calibration using the C-continuum source and solid state detectors SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE AXAF; HRMA; X-ray mirror; X-ray sources; calibration; effective area; solid state detector; raytrace AB The Advanced X-ray Astrophysics Facility (AXAF) X-ray mirrors underwent thorough calibration using the X-Ray Calibration Facility (XRCF) at the Marshall Space Flight Center (MSFC) in Huntsville, AL from late 1996 to early 1997. The X-ray calibration made novel use of the S-ray continuum from a conventional electron-impact source. Taking advantage of the good spectral resolution of solid-state detectors, continuum measurements proved advantageous in calibrating the effective area of AXAF's High-Resolution Mirror Assembly (HRMA) for the entire AXAF energy band. The measurements were made by comparing the spectrum detected by a SSD at the focal plane with the spectrum detected by a beam normalization SSD. The HRMA effective area was calibrated by comparing the measurements with the HRMA raytrace model. The HRMA on-orbit performance predictions are made using the calibration results. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Zhao, P (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 5 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 234 EP 257 DI 10.1117/12.331240 PG 24 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400018 ER PT S AU Gorenstein, P AF Gorenstein, P BE Hoover, RB Walker, ABC TI Deployable ultra-high throughput telescope: Concept SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE X-ray astronomy; X-ray optics AB We describe a method of building and deploying an ultra high throughput X-ray observatory with 2 x 10(5) cm(2) of effective area (2 keV) for the era following the Constellation X-ray Mission and XEUS. It is based upon a single focus telescope. Replacing and adding detectors are possible. Instead of an optical bench, the detector uses electric propulsion with plasma thrusters and ion engines to maintain its station at the focus and repositioning itself for new targets. The preferred site is the L2 point; a high circular orbit is also possible. Additional or replacement detectors equipped with ion/plasma engines are launched on much smaller rockets and rendez-vous with the telescope. We describe how such a telescope with an angular resolution of a few arcseconds could be fabricated. As an example, we consider a 7 m x 7 m aperture, 100 m focal length standard Kirkpatrick-Baez optic. It is segmented into several hundred modules of identical size. A co-aligned group of segments is equipped with a fiducial and a positioning system for alignment to a common focus in space. With subdivided reflector substrates made from light weight advanced composite materials the launch mass of the telescope spacecraft is within the capability of current vehicles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gorenstein, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 24 Z9 24 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 382 EP 392 DI 10.1117/12.331253 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400031 ER PT S AU Romaine, S Everett, J Bruni, R Ivan, A Gorenstein, P AF Romaine, S Everett, J Bruni, R Ivan, A Gorenstein, P BE Hoover, RB Walker, ABC TI Characterization and multilayer coating of cylindrical X-ray optics for X-ray astronomy SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE X-ray telescopes; multilayers; X-ray optics AB We are engaged in a program to develop focusing hard X-ray optics for future X-ray astronomy missions. Optics are being developed to focus X-rays up to and beyond 80 keV. Emphasis is on the multilayer coating of integral cylindrical optics which will provide the highest spatial resolution. A chamber geometry has been designed to allow the uniform coating of the inside surface of integral cylinders. The building and testing of this system has taken place over the past year. Linear DC magnetron cathodes are used to sputter the multilayer films. Initial results from both longitudinal and azimuthal uniformity coating tests are presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romaine, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 10 Z9 10 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 552 EP 555 DI 10.1117/12.331275 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400051 ER PT S AU Ivan, A Romaine, SE Bruni, RJ Everett, JE Gorenstein, P AF Ivan, A Romaine, SE Bruni, RJ Everett, JE Gorenstein, P BE Hoover, RB Walker, ABC TI Characterization of graded-d spacing multilayers for hard X-ray telescopes SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE X-ray telescopes; graded d-spacing multilayers; X-ray optics AB The Multilayer Facility at the Center for Astrophysics is involved in developing graded-d spacing multilayers for coating Xray optics for hard X-ray focusing telescopes [1]. Graded d spacing W/C multilayers have been fabricated on flat substrates of silicon and characterized using specular X-ray reflectivity, AFM, and TEM. Results are presented and compared with theoretical models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ivan, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 556 EP 563 DI 10.1117/12.331276 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400052 ER PT S AU Romaine, S Everett, J Bruni, R Ivan, A Gorenstein, P Ghigo, M Mazzoleni, F Citterio, O Pedulla, J AF Romaine, S Everett, J Bruni, R Ivan, A Gorenstein, P Ghigo, M Mazzoleni, F Citterio, O Pedulla, J BE Hoover, RB Walker, ABC TI Progress in replication of substrates for multilayer coatings SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE X-ray telescopes; multilayers; replicated substrates ID SURFACE AB Studies are being carried out to compare the performance of several different separation materials used in the replication process. This report presents the results obtained during the second year of a program which consists of replicating smooth, thin substrates, depositing multilayer coatings upon them, and evaluating their performance. Replication and multilayer coatings are both critically important to the development of focussing hard X-ray telescopes that function up to 100 keV. The activities of the current year include extending the comparison between sputtered amorphous carbon and evaporated gold to include sputtered as well as evaporated gold. The figure of merit being the smoothness of the replica which has a direct effect on the specular reflectivity. These results were obtained with epoxy replication, but they should be applicable to electroformed nickel, the process we expect to use for the ultimate replicated optics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romaine, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 6 Z9 6 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 564 EP 568 DI 10.1117/12.331277 PG 5 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400053 ER PT S AU Burek, AJ Cobuzzi, JC Fitch, JJ Graessle, DE Ingram, RH Sweeney, JB Blake, RL Francoeur, R Sullivan, ES AF Burek, AJ Cobuzzi, JC Fitch, JJ Graessle, DE Ingram, RH Sweeney, JB Blake, RL Francoeur, R Sullivan, ES BE Hoover, RB Walker, ABC TI Development of beamline U3A for AXAF synchrotron reflectivity calibrations SO X-RAY OPTICS, INSTRUMENTS, AND MISSIONS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray Optics, Instruments, and Missions CY JUL 19-22, 1998 CL SAN DIEGO, CA SP SPIE Int Soc Opt Engn DE AXAF; x-rays; calibration; monochromator; synchrotron radiation ID LINE AB We discuss the development of beamline U3A at NSLS for AXAF telescope witness mirror reflectivity calibrations in the 1 - 2 keV energy range. The beamline was originally constructed as a white light beamline and has been upgraded with the addition of a monochromator to meet the needs of the AXAF calibration program. The beamline consists of an upstream horizontally focussing gold coated elliptical mirror, a differential pumping section, a sample/filter chamber, a monochromator and a downstream filter set. The mirror is set at a 2 degree incident angle for a nominal high energy cutoff at 2 keV. The monochromator is a separated element, scanning, double crystal-multilayer design having low to moderate energy resolution. A fixed exit beam is maintained through the 7-70 degree Bragg angle range by longitudinal translation of the second scanning crystal. Tracking is achieved by computer control of the scan motors with lookup table positioning of the crystal rotary tables. All motors are in vacuum and there are no motional feedthroughs. Several different multilayer or crystal pairs are co-mounted on the monochromator crystal holders and can be exchanged in situ. Currently installed are a W/Si multilayer pair N=60, 2d=75A), beryl (2d=15.96A), and Na-beta alumina (2d=22.53A) allowing energy coverage from 180 eV to 2000 eV. Measurements with Na-beta alumina and beryl show that beam impurity less than 0.1% can be achieved in the 1-2 keV energy range. Measured resolving powers are E/Delta E=60 for W/Si, 500 - 800 for beta alumina and 1500 to 3000 for beryl. Initial results suggest that signal to noise and beam purity are adequate in the 1-2 keV region to achieve the 1% calibration accuracy required by AXAF. This allows overlap of Ir MV edge data taken on x-ray beamline X8A and with low energy data taken on ALS beamline 6.3.2. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Burek, AJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 6 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-2899-X J9 P SOC PHOTO-OPT INS PY 1998 VL 3444 BP 584 EP 597 DI 10.1117/12.331281 PG 14 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BM32R UT WOS:000078392400056 ER PT J AU Bilby, K AF Bilby, K TI A day for the hunter, a day for the prey: Popular music and power in Haiti SO YEARBOOK FOR TRADITIONAL MUSIC LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Bilby, K (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 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 1998 VL 30 BP 141 EP 143 DI 10.2307/768560 PG 3 WC Music SC Music GA 146DB UT WOS:000077411800013 ER PT J AU Potts, R AF Potts, R TI Environmental hypotheses of hominin evolution SO YEARBOOK OF PHYSICAL ANTHROPOLOGY, VOL 41 - 1998 SE YEARBOOK OF PHYSICAL ANTHROPOLOGY LA English DT Review DE climate; habitat; adaptation; variability selection; fossil humans; stone tools ID SOUTHERN KENYA RIFT; LAKE TURKANA BASIN; OLDUVAI-GORGE; EAST-AFRICA; AUSTRALOPITHECUS-AFARENSIS; OLORGESAILIE FORMATION; PLIOCENE HOMINIDS; ISOTOPIC EVIDENCE; EARLY PLEISTOCENE; SCAVENGING NICHE AB The study of human evolution has long sought to explain major adaptations and trends that led to the origin of Homo sapiens. Environmental scenarios have played a pivotal role in this endeavor. They represent statements or, more commonly, assumptions concerning the adaptive context in which key hominin traits emerged. In many cases, however, these scenarios are based on very little if any data about the past settings in which early hominins lived. Several environmental hypotheses of human evolution are presented in this paper. Explicit test expectations are laid out, and a preliminary assessment of the hypotheses is made by examining the environmental records of Olduvai, Turkana, Olorgesailie, Zhoukoudian, Combe Grenal, and other hominin localities. Habitat-specific hypotheses have prevailed in almost all previous accounts of human adaptive history. The rise of African dry savanna is often cited as the critical event behind the development of terrestrial bipedality, stone toolmaking, and encephalized brains, among other traits. This savanna hypothesis has been countered recently by the woodland/forest hypothesis, which claims that Pliocene hominins had evolved in and were primarily attracted to closed habitats. The ideas that human evolution was fostered by cold habitats in higher latitudes or by seasonal variations in tropical and temperate zones also have their proponents. An alternative view, the variability selection hypothesis, states that large disparities in environmental conditions were responsible for important episodes of adaptive evolution. The resulting adaptations enhanced behavioral versatility and ultimately ecological diversity in the human lineage. Global environmental records for the late Cenozoic and specific records at hominin sites show the following: 1) early human habitats were subject to large-scale remodeling over time; 2) the evidence for environmental instability does not support habitat-specific explanations of key adaptive changes; 3) the range of environmental change over time was more extensive and the tempo far more prolonged than allowed by the seasonality hypothesis; and 4) the variability selection hypothesis is strongly supported by the persistence of hominins through long sequences of environmental remodeling and the origin of important adaptations in periods of wide habitat diversity. Early bipedality, stone transport, diversification of artifact contexts, encephalization, and enhanced cognitive and social functioning all may reflect adaptations to environmental novelty and highly varying selective contexts. Yrbk Phys Anthropol 41:93-136, 1998. (C) 1998 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Potts, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 203 TC 204 Z9 211 U1 26 U2 107 PU WILEY-LISS, INC PI NEW YORK PA 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0096-848X J9 YEARB PHYS ANTHROPOL PY 1998 VL 41 BP 93 EP 136 PG 44 WC Anthropology SC Anthropology GA BM40T UT WOS:000078652400004 ER PT J AU Ruiz-Miranda, CR Wells, SA Golden, R Seidensticker, J AF Ruiz-Miranda, CR Wells, SA Golden, R Seidensticker, J TI Vocalizations and other behavioral responses of male cheetahs (Acinonyx jubatus) during experimental separation and reunion trials SO ZOO BIOLOGY LA English DT Article DE affiliative behavior; coalitions; husbandry; distress; attachment; Felidae ID REPRODUCTION; STRESS; CATS AB In this study we assessed the extent of psychological attachment between male cheetahs living in same sex pairs in toes by recording the behavior and vocalizations of two male coalitions (siblings and nonsiblings) during four experimental separations and reunions of each coalition. Both coalitions showed higher vocalization rates and walking rates during separations than during reunions, and during separations cheetahs spent less time resting and more time vocalizing, walking, or standing than during baseline observations. Compared to the nonsibling coalition, the sibling coalition showed a significantly higher vocalization rate during separations and more affiliative behavior during reunions. The most common calls emitted during separations were chirps, followed by eeaows and stutters. The chirps showed the highest level of individual distinctiveness. Eeaows comprised a significantly higher percentage of the calls during separations for nonsiblings that for siblings. The only vocalization heard during reunion was the stutter. We hypothesize that chirps emitted during separations communicate desire to reunite, individual identity, and have a structure that facilitates locating the caller. The results of this study suggest that male cheetahs, both sibling and nonsibling, develop strong psychological attachments to each other. The separation of existing coalitions can create stressful conditions for coalition members. We suggest that raising and maintaining coalitions of male cheetahs in coalitions in toes is a viable husbandry technique. (C) 1998 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Ruiz-Miranda, CR (reprint author), Univ Estadual Norte Fluminense, CBB, LCA, Ave Alberto Lamego 2000, BR-28015620 Campos Dos Goytacazes, RJ, Brazil. RI Ruiz-Miranda, Carlos/A-4719-2008; Ruiz-Miranda, Carlos/H-7308-2015; Ruiz, Carlos/I-4446-2016; OI Ruiz-Miranda, Carlos/0000-0001-9786-5315; Ruiz-Miranda, Carlos/0000-0001-7360-0304; Wells, Stuart/0000-0002-5612-9538 NR 42 TC 12 Z9 13 U1 4 U2 18 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1998 VL 17 IS 1 BP 1 EP 16 DI 10.1002/(SICI)1098-2361(1998)17:1<1::AID-ZOO1>3.0.CO;2-D PG 16 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA YX265 UT WOS:000072022900001 ER PT J AU Wielebnowski, N Brown, JL AF Wielebnowski, N Brown, JL TI Behavioral correlates of physiological estrus in cheetahs SO ZOO BIOLOGY LA English DT Article DE Acinonyx jubatus; estradiol; estrous behavior; fecal steroids ID NORTH-AMERICAN ZOOS; ACINONYX-JUBATUS; DOMESTIC CAT; OVARIAN ACTIVITY; ESTRADIOL-17-BETA; PROGESTERONE; PREGNANCY; STEROIDS; QUALITY; PLASMA AB Historically, the cheetah (Acinonyx jubatus) has been known for its poor reproductive performance in captivity. Although breeding success has improved over the past decade, the percentage of breeders in the captive population is still low and successful propagation unpredictable. Estrus in this species has been reported as "silent" by some, therefore contributing to breeding problems by making appropriate timing of pair introductions difficult. To investigate whether any observable behavioral changes may be associated with estrus, we carried out quantitative behavioral observations and concomitant noninvasive monitoring of estradiol metabolites excreted in feces of 14 captive female cheetahs for periods of 5-22 consecutive weeks. We found that changes in fecal estradiol concentrations correlated significantly with variation in the occurrence of several types of behaviors, including rolling, rubbing, sniffing, vocalizing, and urine spraying. However, the number and types of correlated behaviors varied across females, revealing no single behavior indicative of estrus, but rather a constellation of behaviors that increased in frequency when estradiol concentrations were elevated. There was no significant difference in the overall average estradiol concentrations or peak values of the females that had previously mated and conceived compared to those of the females that had failed to breed. Successful breeders appeared to show significantly higher rates of rubbing and rolling than nonbreeders. However, rates of rubbing, rolling, and urine spraying also were found to increase with age, and older individuals were more likely to have bred. The results of this study indicate that estrus in the cheetah cannot be regarded as "silent" since the frequencies of some behaviors appear to covary with fluctuating estradiol levels. However, behavioral monitoring of estrus may nevertheless be difficult and time-consuming due to individual variation and subtle changes in behavioral frequencies rather than changes in the types of behaviors displayed. Zoo Biol 17:193-209, 1998. (C) 1998 Wiley-Liss, Inc. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Wielebnowski, N (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM nwielebn@sivm.si.edu NR 67 TC 34 Z9 36 U1 3 U2 27 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1998 VL 17 IS 3 BP 193 EP 209 DI 10.1002/(SICI)1098-2361(1998)17:3<193::AID-ZOO4>3.0.CO;2-4 PG 17 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA ZX196 UT WOS:000074489000004 ER PT J AU Hutchins, M Roberts, M Cox, C Crotty, MJ AF Hutchins, M Roberts, M Cox, C Crotty, MJ TI Marsupials and monotremes: A case study in regional collection planning SO ZOO BIOLOGY LA English DT Article DE Taxon Advisory Group; institutional collection plan ID CONSERVATION; MANAGEMENT; DISEASES; ARK AB Cooperative collection planning is critical to the future of zoological parks and aquariums, yet few published models currently exist for collection plan development and implementation. In particular, there has been little discussion about the relationship between regional and institutional collection planning or about what defines a quality regional collection plan (RCP). This article documents the regional collection planning process adopted by the AZA Marsupial and Monotreme Taxon Advisory Group (TAG). More specifically, it outlines the philosophical foundation of the North American RCP for Marsupials and Monotremes, the organizational structure developed by the TAG to facilitate communication, evaluation and institutional participation, and other important details of the planning process. It also documents how the RCP was used by one institution (Los Angeles Zoo) to formulate its Institutional Collection Plan (ICP). (C) 1998 Wiiey-Liss, Inc. C1 Amer Zoo & Aquarium Associat, Execut Off, Conservat Ctr, Bethesda, MD 20814 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Los Angeles Zoo, Los Angeles, CA USA. RP Hutchins, M (reprint author), Amer Zoo & Aquarium Associat, Execut Off, Conservat Ctr, 7970-D Old Georgetown Rd, Bethesda, MD 20814 USA. NR 43 TC 4 Z9 4 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1998 VL 17 IS 5 BP 433 EP 451 DI 10.1002/(SICI)1098-2361(1998)17:5<433::AID-ZOO8>3.0.CO;2-0 PG 19 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 134UC UT WOS:000076761100008 ER PT J AU Kalko, EKV AF Kalko, EKV TI Organisation and diversity of tropical bat communities through space and time SO ZOOLOGY-ANALYSIS OF COMPLEX SYSTEMS LA English DT Article; Proceedings Paper CT 91st Annual Meeting of the Deutsche-Zoologische-Gesellschaft CY JUN 01-04, 1998 CL LEIPZIG, GERMANY SP Deutsch Zool Gesell DE guilds; resources; conservation; behavior; inventories ID DIPTEROCARP RAIN-FOREST; FRUIT-EATING BATS; ECHOLOCATION CALLS; FRENCH-GUIANA; ARTIBEUS-JAMAICENSIS; INSECTIVOROUS BATS; TROPHIC STRUCTURE; SPECIES RICHNESS; FORAGING ECOLOGY; PHYLLOSTOMIDAE AB Tropical bat communities are characterized by high species diversity and relative abundance. Due to their diverse feeding ecologies, bats play indispensable roles in tropical forests as seed dispersers, pollinators, and predators of arthropods. However, despite of their importance, little is known about factors that promote diversity in this taxon as well as interactions between bats and their environment. First results suggest that Neotropical bat communities are highly structured. I explore factors that may contribute to the observed pattern. Partitioning of resources in space and time facilitates coexistence of species within local species assemblages. I discuss future perspectives for comprehensive studies of species assemblages that combine macroecological (top-down) and microecological (bottom-up) approaches. Foremost, I underline the need for comprehensive inventory techniques. In conclusion, comparative community studies of bats with standardized methodologies are crucial for a better understanding how environmental change may influence these species assemblages and in turn, plants and animals affected by them. C1 Univ Tubingen, D-72076 Tubingen, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Kalko, EKV (reprint author), Univ Tubingen, Morgenstelle 28, D-72076 Tubingen, Germany. EM Elisabeth-Kalko@uni-tuebingen.de NR 108 TC 89 Z9 109 U1 2 U2 24 PU GUSTAV FISCHER VERLAG PI JENA PA VILLENGANG 2, D-07745 JENA, GERMANY SN 0944-2006 J9 ZOOL-ANAL COMPLEX SY JI Zool.-Anal. Complex Syst. PY 1998 VL 101 IS 4 BP 281 EP 297 PG 17 WC Zoology SC Zoology GA 172VW UT WOS:000078946800006 ER PT J AU Markevitch, M Vikhlinin, A AF Markevitch, M Vikhlinin, A TI Dark matter and baryon fraction at the virial radius in Abell 2256 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies, clusters, individual (A2256); intergalactic medium; X-rays, galaxies ID X-RAY SPECTROSCOPY; GALAXY CLUSTERS; COMA CLUSTER; INTRACLUSTER GAS; EMITTING GAS; A2256; MASS; DYNAMICS; TEMPERATURE; MORPHOLOGY AB We combine high-quality ASCA and ROSAT X-ray data to constrain the radial dark matter distribution in the primary cluster of Abell 2256, free from the assumption of gas isothermality. Both instruments indicate that the temperature declines with radius. The region including the central galaxy has a multicomponent spectrum, which results in a wide range of allowed central gas temperatures. We find that the secondary subcluster has a temperature and luminosity typical of a rich cluster; however, the ASCA temperature map shows no signs of an advanced merger in this double system. It is therefore assumed that the primary cluster is in hydrostatic equilibrium. The data then require dark matter density profiles steeper than p proportional to r(-2.5) in the cluster outer part. Acceptable models have a total mass within r = 1.5 h(-1) Mpc (approximately the virial radius) of 6.0 +/- 1.5 x 10(14) h(-1) M. at the 90% confidence level. This is about 1.6 times smaller than the mass derived assuming isothermality. The gas fraction is correspondingly higher and is 0.08 +/- 0.02 h(-3/2). A lower limit on the fraction of gas in the total local density at the same radius is 0.09 h(-3/2), which is twice the isothermal value. Near the center, dark matter profiles with and without central cusps are consistent with the data. Our inferred total mass inside the X-ray core (r = 0.26 h(-1) Mpc) is 1.28 +/- 0.08 x 10(14) h(-1) M., which exceeds the isothermal value by a factor of 1.4. Although the confidence intervals above may be underestimates, since they do not include uncertainties arising from asymmetry and departures from hydrostatic equilibrium, the behavior of the mass distribution, if applicable to other clusters, can bring X-ray and lensing mass estimates into better agreement but aggravate the "baryon catastrophe." The observed considerable increase in the gas content with radius, not anticipated by simulations, may imply that a significant fraction of thermal gas energy comes from sources other than gravity and merger shocks, such as supernovae-driven galactic winds, for example. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Russian Acad Sci, Space Res Inst, Moscow 117901, Russia. RP Markevitch, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM maxim@head-cfa.harvard.edu; alexey@head-cfa.harvard.edu NR 66 TC 43 Z9 43 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1997 VL 491 IS 2 BP 467 EP 476 DI 10.1086/304972 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YN295 UT WOS:000071152600005 ER PT J AU Koratkar, A Evans, I Pesto, S Taylor, C AF Koratkar, A Evans, I Pesto, S Taylor, C TI A detailed comparison of Hubble Space Telescope Faint Object Spectrograph and IUE ultraviolet spectra of selected Seyfert nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, individual (Markarian 509, NGC 3783, NGC 5548); galaxies, Seyfert; ultraviolet, galaxies AB Despite the contributions of the Hubble Space Telescope Faint Object Spectrograph (FOS) to the archive of UV observations of active galactic nuclei, the vast majority of UV reference data were obtained using the international Ultraviolet Explorer (IUE) satellite. These data remain important since they provide historical information about the intensities of the UV continua and emission lines that is needed to constrain models of the active nucleus. A detailed comparison of the FOS and IUE data is critical to understanding how the measurable quantities depend on the individual instrumental calibrations, and how any conclusions derived from modeling the observations may vary depending on the source of the UV data. Rigorous comparison of FOS and IUE spectra have so far been performed only for spectrophotometric standard star observations that are acquired accurately and have high signal-to-noise ratios. We compare typical FOS spectra that were not acquired and observed with the strict regimen that is used for standard-star observations, especially in the pre-COSTAR era. All nonproprietary UV FOS spectrophotometric archival data for the Seyfert 1 galaxies Mrk 509, NGC 3783, and NGC 5548 that have near-simultaneous (within 24 hr) IUE observations are used in the analysis. These data demonstrate that the absolute photometric calibrations of the FOS and IUE agree within similar to 5% in absolute flux for two of the objects. For NGC 5548, the FOS and IUE flux data disagree by similar to 50% in the 1200-2000 Angstrom region. In this object there may be evidence for flux nonlinearity of the IUE detector and a contribution from the host galaxy redward of 2800 Angstrom. Cross-correlation of the FOS and IUE spectra reveals no zero-point wavelength shift larger than the IUE wavelength calibration errors. Comparison of line flux measurements from both the FOS and IUE spectra show that for strong emission lines (e.g., Ly alpha, C IV, and Mg II) the measured intensities always agree within 15%, while for moderately strong lines (e.g., N V, Si IV/O IV, He II, and C III]) the agreement is similar to 30% (1 sigma). Weak lines (e.g., O I, C II, N IV], O III], and N III]) may not even be detected in the IUE spectra, and when they are detected the disagreement between the measured fluxes can be very large. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Koratkar, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. NR 11 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1997 VL 491 IS 2 BP 536 EP 544 DI 10.1086/305005 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YN295 UT WOS:000071152600012 ER PT J AU Goldsmith, PF Bergin, EA Lis, DC AF Goldsmith, PF Bergin, EA Lis, DC TI Carbon monoxide and dust column densities: The dust-to-gas ratio and structure of three giant molecular cloud cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, abundances; ISM, clouds; ISM, molecules; radio lines, ISM ID STAR-FORMING REGIONS; MILLIMETER CONTINUUM OBSERVATIONS; HIGH-RESOLUTION IMAGES; INTER-STELLAR CLOUDS; ORION-KL; DARK CLOUD; TEMPERATURE DISTRIBUTIONS; SUBMILLIMETER CONTINUUM; CIRCUMSTELLAR DISKS; INTERSTELLAR GRAINS AB We have observed emission in the three lowest rotational transitions of the optically thin species C(18)O and the dust continuum emission at three millimeter/submillimeter wavelengths. By employing the proper combination of the intensities of the three lowest rotational transitions of C(18)O, we can obtain the total molecular column density, with relatively little sensitivity to density and temperature variations along the line of sight. We use the line and continuum data to determine column densities of the dust and gas across three giant molecular cloud cores. We find that two of the three sources, M17 and Cepheus A, have the same gas column density-to-dust optical depth ratio, given by log [N(C(18)O)/tau(790 mu m)] = 18.8. In the third source, the Orion molecular cloud, the gas-to-dust ratio is typically a factor of 3 lower than in the other two sources. The gas-to-dust ratio shows only a small (factor less than or equal to 3) variation across the region of M17 that we have mapped and a comparable reduction at the center of Cepheus A relative to the cloud edge. We have good evidence for the correlation of the continuum emission in different bands for the Orion molecular cloud and find the frequency dependence of the optical depth in the densest regions near the embedded sources to be given by tau proportional to nu(1.9). For positions away from the embedded sources, there is a larger scatter in the data points, with a suggestion that the frequency dependence is steeper, such that tau proportional to nu(2.4). This may be an indication of a change in the grain properties between less dense and very dense regions and is consistent with the results of grain growth. Using standard values for the fractional abundance of C(18)O relative to H(2), the mean densities of the cloud cores are 3-5 x 10(4) cm(-3). These regions appear to be close to virial equilibrium. The dense gas [revealed by multiple transition studies of tracers such as CS and HC(3)N to have n(H(2))similar or equal to 10(6) cm(-3)] has a volume filling factor of a few percent. Assuming a fractional abundance of C(18)O equal to 1.7 x 10(-7), we find that the 790 mu m dust optical depth to mass column density ratio for M17 and Cepheus A is 0.0062 cm(2) g(-1), while the average value for the Orion molecular cloud is a factor of 3 larger. C1 Cornell Univ, Dept Astron, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Downs Lab Phys 320 47, Pasadena, CA 91125 USA. RP Goldsmith, PF (reprint author), Cornell Univ, Dept Astron, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. RI Goldsmith, Paul/H-3159-2016 NR 99 TC 106 Z9 106 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1997 VL 491 IS 2 BP 615 EP 637 DI 10.1086/304986 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YN295 UT WOS:000071152600017 ER PT J AU Tafalla, M Myers, PC AF Tafalla, M Myers, PC TI Velocity shifts in L1228: The disruption of a core by an outflow SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual (L1228); ISM, jets and outflows; ISM, kinematics and dynamics; stars, formation ID MOLECULAR OUTFLOWS; DENSE CORES; BIPOLAR OUTFLOW; STAR FORMATION; YOUNG STARS; DARK CLOUDS; L1551 IRS-5; PROTOSTARS; EMISSION; SHELL AB We present (CO)-C-12(1-0), (CO)-C-13(1-0), CS(2-1), and C3H2(2(12)-1(01)) observations of the L1228 outflow and dense core with resolutions between 50 " and 25 ". The bipolar molecular outflow originates from IRAS 20582+7724 and extends over almost 15' (approximate to 1.2 pc). It has a well-collimated blue lobe and less collimated red lobe, which is split into two branches that diverge from the IRAS position. The two CO outflow lobes are well aligned with previously observed high-excitation emission from H-2 and H alpha, although these emissions present bendings from a straight line, suggesting that the outflow driving wind changes direction by interacting with the ambient cloud. The dense gas in the core also shows evidence for acceleration in the outflow direction, although its velocity is significantly lower than that of the CO emission. The dense gas acceleration appears in the CS and C3H2 spectra as velocity shifts in the line centroid on the order of one C3H2 full line width (approximate to 0.4 km s(-1)). These shifted line profiles are not accompanied by any significant emission at ambient core velocities. Furthermore, there is very little or no quiescent C3H2 emission toward the outflow lobes, as if the outflow acceleration had been so efficient that all the dense gas has been set into motion. This acceleration, in addition, has occurred without appreciable line width enhancement, suggesting that it has not increased substantially the turbulence of the gas. From the large size of the velocity shifts (comparable to the gas escape velocity) and from our energetics estimates, we infer that the L1228 outflow could significantly disperse the dense gas in the core by the time the outflow phase ends. C1 Harvard Smithsonian Ctr Astrophys, MS 42, Cambridge, MA 02138 USA. RP Tafalla, M (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42, 60 Garden St, Cambridge, MA 02138 USA. EM tafalla@cfa.harvard.edu; pmyers@cfa.harvard.edu NR 45 TC 31 Z9 31 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 20 PY 1997 VL 491 IS 2 BP 653 EP 662 DI 10.1086/304968 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YN295 UT WOS:000071152600019 ER PT J AU Ofman, L Romoli, M Poletto, G Noci, G Kohl, JL AF Ofman, L Romoli, M Poletto, G Noci, G Kohl, JL TI Ultraviolet coronagraph spectrometer observations of density fluctuations in the solar wind SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; solar wind; sun, corona; sun, magnetic fields; waves ID HOLES AB Recent Ultraviolet Coronagraph Spectrometer (UVCS) white-light channel (WLC) observations on board the Solar and Heliospheric Observatory (SOHO) indicate quasi-periodic variations in the polarized brightness (pB) in the polar coronal holes, This is the first observation of possible signatures of compressional waves high above the limb (at heliocentric distances in the range 1.9-2.45 R.). The Fourier power spectrum of the pB time series at 1.9 R. shows significant peak at about 6 minutes and possible fluctuations on longer timescales (20-50 minutes), The observation at 1.9 R. is the only currently available WLC data set with sufficient cadence to resolve the 6 minute period. These preliminary observations may result from density fluctuations caused by compressional waves propagating in polar coronal holes. We stress that our results are preliminary, and we plan future high-cadence observations in both plume and interplume regions of coronal holes, Recently, Ofman & Davila used a 2.5 D MHD model and found that Alfven waves with an amplitude of 20-70 km s(-1) at the base of the coronal hole can generate nonlinear, high-amplitude compressional waves that can contribute significantly to the acceleration of the fast solar wind, The nonlinear solitary-like waves appear as fluctuations in the density and the radial outflow velocity and contribute significantly to solar wind acceleration in open magnetic field structures, The motivation for the reported observations is the MHD model prediction. C1 Hughes STX, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Univ Florence, Dept Astron & Space Sci, I-50125 Florence, Italy. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ofman, L (reprint author), Hughes STX, Code 682, Greenbelt, MD 20771 USA. RI Romoli, Marco/H-6859-2012 NR 17 TC 147 Z9 147 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 1997 VL 491 IS 2 BP L111 EP L114 DI 10.1086/311067 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YN296 UT WOS:000071152700012 ER PT J AU Spergel, D Pen, UL AF Spergel, D Pen, UL TI Cosmology in a string-dominated universe SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, theory; large-scale structure of universe ID MICROWAVE BACKGROUND ANISOTROPIES; COSMIC STRINGS; DARK-MATTER; CONSTANT; MODELS; FLAT; TOPOLOGY; DENSITY AB The string-dominated universe is a flat universe that locally resembles an open universe and Bts dynamical measures of power spectra, cluster abundances, redshift distortions, lensing constraints, luminosity, angular diameter distance relations, and microwave background observations. We show examples of networks that might give rise to recent string-domination when formed by a phase transition near the electro-weak symmetry breaking scale. We discuss how future observations can distinguish this model from other cosmologies. C1 Princeton Univ Observ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Spergel, D (reprint author), Princeton Univ Observ, Peyton Hall, Princeton, NJ 08544 USA. RI Spergel, David/A-4410-2011 NR 54 TC 95 Z9 96 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 20 PY 1997 VL 491 IS 2 BP L67 EP + DI 10.1086/311074 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YN296 UT WOS:000071152700001 ER PT J AU DaviesVollum, KS AF DaviesVollum, KS TI Early Palaeocene palaeoclimatic inferences from fossil floras of the western interior, USA SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE K-T boundary; palaeoclimate; leaf physiognomy; North America ID CRETACEOUS-TERTIARY BOUNDARY; EASTERN MONTANA; TEMPERATURE; TERRESTRIAL; EXTINCTION; VEGETATION; CLIMATES; IMPACT; PALEOCLIMATES; PALEOSOLS AB Twenty one early Palaeocene floral assemblages were collected from a variety of alluvial depositional environments from sites in the Williston, Powder River and Raton basins of the western interior of the USA. Leaf fossils were assigned to morphotypes and their physiognomy was quantified for palaeoclimatic analysis. Two methods were used; Climate Leaf Analysis Multi variate Program (CLAMP) and Leaf Margin Analysis (LMA). Temperature estimates and trends derived from CLAMP and LMA indicate that early Palaeocene palaeotemperatures decreased from the latest Cretaceous, particularly in northern areas of North America. Climatic zones shifted southwards from their latest Cretaceous positions, resulting in a steepened north-south temperature gradient and decreased equability in the early Palaeocene. Sub-tropical conditions prevailed as far north as the Raton Basin with the 20 degrees C mean annual temperature isotherm (megathermal-mesothermal boundary) located at approximately 45 degrees N palaeolatitude. The 13 degrees C mean annual temperature isotherm (mesothermal-microthermal boundary) was located at approximately 55 degrees N palaeolatitude to the south of the Williston Basin. CLAMP estimates indicate that precipitation increased significantly in all areas sampled directly after the K-T boundary event, especially in the southern Rockies. Precipitation levels decreased somewhat after this initial peak but remained high throughout the early Palaeocene. Evidence from this and other studies suggests that seasonality increased from the latest Cretaceous into the Palaeocene and was most pronounced in central and northerly areas of the North American continent. (C) 1997 Elsevier Science B.V. RP SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT PALEOBIOL, MRC 121, WASHINGTON, DC 20560 USA. NR 88 TC 15 Z9 17 U1 1 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD DEC 15 PY 1997 VL 136 IS 1-4 BP 145 EP 164 DI 10.1016/S0031-0182(97)00092-8 PG 20 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA YL241 UT WOS:A1997YL24100010 ER PT J AU Volkmer-Ribeiro, C Rutzler, K AF Volkmer-Ribeiro, C Rutzler, K TI Pachyrotula, a new genus of freshwater sponges from New Caledonia (Porifera : Spongillidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Characteristics found during a review of the type material of Spongilla (Stratospongilla) raceki Rutzler from New Caledonia point to a new, monotypic genus, Pachyrotula. This new genus is closely related to Heterorotula Penney & Racek and to Houssayella Bonetto & Ezcurra De Drago. Heterorotula also occurs in New Caledonia and is represented by the species H. caledonensis new species and H. multidentata (Weltner). These species, along with Oncosclera diahoti (Rutzler), new combination, are indicators of a rare and particular freshwater sponge fauna of this island. C1 Fdn Zoobot Rio Grande Do Sul, Museu Ciencias Nat, BR-90690000 Porto Alegre, RS, Brazil. Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Volkmer-Ribeiro, C (reprint author), Fdn Zoobot Rio Grande Do Sul, Museu Ciencias Nat, Rua Dr Salvador Franca 1427, BR-90690000 Porto Alegre, RS, Brazil. NR 9 TC 3 Z9 3 U1 1 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 12 PY 1997 VL 110 IS 4 BP 489 EP 501 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA YL980 UT WOS:000071014700001 ER PT J AU Bayer, FM AF Bayer, FM TI Narella nuttingi, a new gorgonacean octocoral of the family Primnoidae (Anthozoa) from the eastern Pacific SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Specimens originally reported by Nutting (1908) as Stachyodes dichotoma Versluys from Albatross explorations in Hawaiian waters are shown to be misidentified and are now described as a new species, Narella nuttingi. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Bayer, FM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 18 TC 2 Z9 2 U1 1 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 12 PY 1997 VL 110 IS 4 BP 511 EP 519 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA YL980 UT WOS:000071014700003 ER PT J AU Pettibone, MH AF Pettibone, MH TI Revision of the scaleworm genus Eulagisca McIntosh (Polychaeta : Polynoidae) with the erection of the subfamily Eulagiscinae and the new genus Pareulagisca SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new subfamily of Polynoidae, Eulagiscinae, is established for Eulagisca McIntosh, to include the type species E. corrientis, E. gigantea Monro, E. puschkini Averincev, and two new species, E. uschakovi and E. macnabi, all from the Antarctic and Subantarctic regions, and the new genus Pareulagisca for P. panamensis (Hartman), new combination, from the central Pacific Panama region. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Pettibone, MH (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 18 TC 0 Z9 1 U1 1 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 12 PY 1997 VL 110 IS 4 BP 537 EP 551 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA YL980 UT WOS:000071014700005 ER PT J AU Reid, JW AF Reid, JW TI Argyrodiaptomus nhumirim, a new species, and Austrinodiaptomus kleerekoperi, a new genus and species, with redescription of Argyrodiaptomus macrochaetus Brehm, new rank, from Brazil (Crustacea : Copepoda : Diaptomidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID CALANOIDA AB Two species of diaptomid calanoid copepods are described, and one species is redescribed from Brazilian specimens. Argyrodiaptomus nhumirim, new species, inhabits small fishless freshwater ponds in the Pantanal, State of Mate Grosso do Sul. Argyrodiaptomus furcatus var. macrochaetus Brehm is redescribed from the State of Rio Grande do Sul and raised to species rank. A new genus and species Austrinodiaptomus kleerekoperi is described, also from Rio Grande do Sul. Diaptomus s.l. inexspectatus Brehm is transferred to Austrinodiaptomus. The first record from the State of Sergipe is given for Argyrodiaptomus azevedoi (Wright). C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, MRC 163, Washington, DC 20560 USA. RP Reid, JW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, MRC 163, Washington, DC 20560 USA. NR 36 TC 6 Z9 6 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 12 PY 1997 VL 110 IS 4 BP 581 EP 600 PG 20 WC Biology SC Life Sciences & Biomedicine - Other Topics GA YL980 UT WOS:000071014700010 ER PT J AU Williams, AB AF Williams, AB TI Two new species and a range extension of mud shrimps, Upogebia, from Pacific Costa Rica and Mexico (Decapoda : Thalassinidea : Upogebiidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Two new species of mud shrimps are described from the Pacific side of Middle America, Upogebia baldwini from the state of Nayarit, Mexico, and U. vargasae from Puntarenas Province, Costa Pica. The geographic range of the poorly known U. burkenroadi Williams, 1986 is extended from its type locality in the state of Sonora, Mexico to a documented Costa Rican occurrence. The new species are illustrated, and a key for identification of eastern Pacific species of Upogebia (Williams 1986) is amended to accommodate the new species. Cataloged lots of each species collected are listed. C1 Natl Museum Nat Hist, Smithsonian Inst, Natl Marine Fisheries Serv Systemat Lab, Washington, DC 20560 USA. RP Williams, AB (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Natl Marine Fisheries Serv Systemat Lab, Washington, DC 20560 USA. NR 4 TC 4 Z9 5 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 12 PY 1997 VL 110 IS 4 BP 617 EP 623 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA YL980 UT WOS:000071014700013 ER PT J AU Olson, SL Walker, CA AF Olson, SL Walker, CA TI A trans-Atlantic record of the fossil tropicbird Heliadornis ashbyi (Aves : Phaethontidae) from the Miocene of Belgium SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The fossil tropicbird Heliadornis ashbyi Olson, previously known from the unique holotype from the middle Miocene Calvert Formation of Maryland, is here recorded from a contemporaneous site in Belgium based on a nearly complete humerus. Its trans-Atlantic occurrence at a much higher latitude suggests that Heliadornis may have been the higher-latitude sister group of the extant tropical genus Phaethon, much as within the Sulidae gannets of the genus Morus are the higher latitude counterparts of the tropical boobies of the genus Sula. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. Nat Hist Museum, Dept Zool, Bird Grp, Tring HP23 6AP, Herts, England. RP Olson, SL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. NR 8 TC 4 Z9 5 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 12 PY 1997 VL 110 IS 4 BP 624 EP 628 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA YL980 UT WOS:000071014700014 ER PT J AU Carleton, MD Van der Straeten, E AF Carleton, MD Van der Straeten, E TI Morphological differentiation among Subsaharan and north African populations of the Lemniscomys barbarus complex (Rodentia : Muridae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Morphometric evaluation discloses patterns of craniodental variation which demonstrate that populations currently assigned to Lemniscomys barbarus consist of two species: L. barbarus (Linnaeus 1766) and L. zebra (Heuglin 1864). One species-group epithet is herein allocated to the junior synonymy of L. barbarus (ifniensis Morales Agacino 1935), ten to L. zebra (spekei De Winton 1897, dunni Thomas 1903, convictus Osgood 1910, albolineatus Osgood 1910, manteufeli Matschie 1911, oweni Thomas 1911b, nigeriae Thomas 1912, olga Thomas & Hinton 1921, nubalis Thomas & Hinton 1923, and orientalis Hatt 1935), and a lectotype is designated for Mns zebra Heuglin (1864). No subspecies are recognized for either species, but the substantial heterogeneity documented within L. zebra advises continued study of those populations. The geographic occurrence of L. barbarus is restricted to scrub vegetation along a narrow coastal strip in Morocco, Algeria, and Tunisia; whereas, L. zebra is widely distributed over dry grassland and savanna biomes south of the Sahara Desert, from Senegal in West Africa to central Sudan in East Africa, and southwards to northcentral Tanzania. Lemniscomys hoogstraali Dieterlen (1991), known only by the holotype from eastcentral Sudan, is retained as a third member of the barbarus group. The species L. barbarus represents another example of small mammal endemic to the Barbarian province (Maghreb) of northwest Africa. C1 Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, Washington, DC 20560 USA. Univ Antwerp, Rijksuniv Ctr Antwerp, Dept Biol, B-2020 Antwerp, Belgium. RP Carleton, MD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, Washington, DC 20560 USA. NR 86 TC 17 Z9 19 U1 1 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 12 PY 1997 VL 110 IS 4 BP 640 EP 680 PG 41 WC Biology SC Life Sciences & Biomedicine - Other Topics GA YL980 UT WOS:000071014700016 ER PT J AU Kochanek, CS AF Kochanek, CS TI Rebuilding the Cepheid distance scale .1. A global analysis of Cepheid mean magnitudes SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; distance scale; galaxies, distances and redshifts ID PERIOD-LUMINOSITY RELATION; HUBBLE-SPACE-TELESCOPE; H-II REGIONS; ABSOLUTE PEAK BRIGHTNESS; LIGHT-CURVE SHAPES; MAGELLANIC CLOUDS; KEY PROJECT; METALLICITY DEPENDENCE; INFRARED PHOTOMETRY; CLASSICAL CEPHEIDS AB We develop a statistical method for using multicolor photometry to determine distances using Cepheid variables, including the effects of temperature, extinction, and metallicity, and apply it to UBVRIJHK photometry of 694 Cepheids in 17 galaxies. We derive homogeneous distance, extinction, and uncertainty estimates for four models, starting from the standard extragalactic method and then adding the physical effects of temperature distributions and extinction distributions, requiring positive definite extinctions and metallicity. While we find general agreement with published distances when we make similar systematic assumptions, there is a clear problem in the standard distances because they require Cepheids with negative extinctions, particularly in low-metallicity galaxies, unless the mean LMC extinction exceeds E(B - V) greater than or similar to 0.20. The problem can be explained by the physically expected metallicity dependence of the Cepheid distance scale, where metal-poor Cepheids are hotter and possibly fainter at V and I than metal-rich Cepheids, or by large systematic errors in Cepheid photometry. For V and I we found that the mean magnitude change is -0.14 +/- 0.14 mag dex(-1) and the mean color change is 0.13 +/- 0.04 mag dex(-1), with the change in color dominating the change in distance. The effect on Type Ta supernova estimates of the Hubble constant is dramatic because most were found in the metal-poor galaxies with the bluest Cepheids. The Type Ia multicolor light-curve shape method estimate for H-0 formally rises from 69 +/- 8 to 80 +/- 6 km s(-1) Mpc(-1) with correction. RP Kochanek, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, MS-51, CAMBRIDGE, MA 02138 USA. NR 63 TC 74 Z9 75 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1997 VL 491 IS 1 BP 13 EP 28 DI 10.1086/304934 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL507 UT WOS:A1997YL50700003 ER PT J AU Kaluzny, J Stanek, KZ Garnavich, PM Challis, P AF Kaluzny, J Stanek, KZ Garnavich, PM Challis, P TI Two confirmed cataclysmic variables in the old stellar cluster NGC 6791 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters, general; novae, cataclysmic variables; open clusters and associations, individual (NGC 6791) ID CCD PHOTOMETRY; NGC-6791; STARS; SEARCH; BRANCH; M67 AB Based on new CCD photometry and spectroscopy we confirm the presence of two cataclysmic variables (CVs) in the very old open cluster NGC 6791. One of these variables, known as B8, was observed by Rucinski, Kaluzny, & Hilditch to undergo a large-magnitude outburst in 1995. The spectrum of this star outside the outburst, obtained by us with Multiple Mirror Telescope, clearly shows emission lines characteristic of dwarf novae. We observed the second star, known as B7, to undergo a large (similar to 3 mag) drop in its brightness over similar to 10 days. The spectrum of B7 obtained in the high state resembles spectra of nova-like CVs. This star is likely a member of the UX UMa subtypes of CVs. Variables B7 and B8 represent only the second and the third cataclysmic variables known in open clusters. Variable B7 has observational characteristics that would make it difficult to identify as a CV with some of the methods currently being used in surveys for CVs in globular clusters. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Kaluzny, J (reprint author), UNIV WARSAW OBSERV,AL UJAZDOWSKIE 4,PL-00478 WARSAW,POLAND. NR 28 TC 21 Z9 21 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 10 PY 1997 VL 491 IS 1 BP 153 EP 158 DI 10.1086/304960 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL507 UT WOS:A1997YL50700015 ER PT J AU Staguhn, J Stutzki, J Chamberlin, RA Balm, SP Stark, AA Lane, AP Schieder, R Winnewisser, G AF Staguhn, J Stutzki, J Chamberlin, RA Balm, SP Stark, AA Lane, AP Schieder, R Winnewisser, G TI Observations of [C I] and CO absorption in cold, low-density cloud material toward the Galactic center broad-line emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy, abundances; galaxy, center; ISM, atoms; ISM, general; ISM, molecules; radio lines, ISM ID MOLECULAR CLOUDS; ATOMIC CARBON; DARK CLOUD; SUBMILLIMETER AB We report the detection of a deep P-3(1) --> P-3(0) (C I) absorption feature at upsilon(LSR) = 12 km s(-1) with a line width of 6 km s(-1) toward extended line emission at a distance of 11' from Sgr C. The 492 GHz observations were made with the Antarctic Submillimeter Telescope and Remote Observatory. The absorption feature allows the derivation of lower limits for the C I column density in the cold foreground material. The feature is unlikely to be caused by self-absorption within the [C I]-emitting cloud because it is observed over a region at least 4' across and is also seen in emission 22' north of the Galactic plane in (CO)-C-12 J = 2-1. In order to determine the temperature and the abundance ratio of C I to CO in the foreground gas, we compare the observations with (CO)-C-12 and (CO)-C-13 J = 1-0 observations obtained with the Bell Labs 7 m antenna and with (CO)-C-12 and (CO)-C-13 J = 2-1 observations made with the Kolner Observatorium fur Submillimeter und Millimeter Astronomie 3 m telescope. All these observations have about the same beam size. On the assumption that the background emission is not spatially associated with the absorbing cloud(s), a consistent model for the observed line intensities yields an excitation temperature of 3.5 K for (CO)-C-13 and 5 K for [C I], which implies low volume densities, n(H-2) less than or similar to 10(3) cm(-3). The measured abundance ratio of C I to (CO)-C-13 is similar to 34. This value is consistent with photochemical model calculations that predict an abundance ratio of C I to (CO)-C-12 of similar to 1 and a (CO)-C-12 to (CO)-C-13 ratio of similar to 30 (reduced in comparison to the intrinsic C-12 to C-13 isotopic ratio of 60 by fractionation). The observed (CO)-C-13 column density corresponds to an A(v) of 4.6 mag, i.e., the hydrogen column density N(H) is similar to 9 x 10(21) Cm-2. This, together with the observed [C I] line width, indicates that the absorption is likely due to several translucent clouds. We compare our results with line fluxes derived from the large-scale, low-resolution COBE FIRAS spectral line survey of [C I] P-3(1) --> P-3(0) and [C I] P-3(2) --> P-3(1) emission in the Galactic plane. Taking into account beam filling, the lower limit for the column density of cold (T-ex less than or equal to 10 K) C I that is traced by our absorption observations is at least a factor of 2 higher than the column density of the warmer C I(T-ex greater than or equal to 20 K) detected in emission by COBE. Our results suggest that a substantial fraction of atomic carbon in the interstellar medium may be difficult to detect in [C I] emission, owing to its low excitation. C1 BOSTON UNIV,DEPT ASTRON,BOSTON,MA 02215. CALTECH,SUBMILLIMETER OBSERV,HILO,HI 96720. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF LOS ANGELES,DEPT PHYS & ASTRON,LOS ANGELES,CA 90095. RP Staguhn, J (reprint author), UNIV COLOGNE,INST PHYS 1,ZULPICHER STR 77,D-50937 COLOGNE,GERMANY. NR 36 TC 3 Z9 3 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 1997 VL 491 IS 1 BP 191 EP 199 DI 10.1086/304928 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL507 UT WOS:A1997YL50700020 ER PT J AU Ciaravella, A Raymond, JC Fineschi, S Romoli, M Benna, C Gardner, L Giordano, S Michels, J ONeal, R Antonucci, E Kohl, J Noci, G AF Ciaravella, A Raymond, JC Fineschi, S Romoli, M Benna, C Gardner, L Giordano, S Michels, J ONeal, R Antonucci, E Kohl, J Noci, G TI Ultraviolet Coronagraph Spectrometer observation of the 1996 December 23 coronal mass ejection SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun, corona; sun, prominences; sun, UV radiation ID SOLAR AB The Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliospheric Observatory (SOHO) observed a spectacular coronal mass ejection (CME) caused by a prominence eruption on 1996 December 23. The evolution of the ejected prominence material was followed for 1 hr and 50 minutes. The observation consists of a series of 5 minute exposures, at a fixed heliocentric distance of 1.5 R circle dot in several spectral ranges. The Lyman lines of hydrogen brighten more than 2 orders of magnitude during the CME. The C III 977.02 Angstrom line is very bright, and many other low-temperature lines have been detected. Line intensities and profiles provide important diagnostics for the physical and dynamical parameters of the ejected plasma. Lines widths show nonthermal line broadening due to a plasma expansion with velocity larger than 50 km s(-1). The Ly alpha inside the CME region shows red and blue shifts, up to 0.2 Angstrom (50 km s(-1)) and 0.8 Angstrom (200 km s(-1)), respectively. A preliminary estimate shows a flat emission measure distribution 3 or 4 orders of magnitude smaller than typical prominence emission measures. Essentially the same structure in space and velocity is seen in the Lyman lines, in C III (10(5) K) and in 0 VI (3 x 10(5) K). C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV FLORENCE,DIPARTIMENTO ASTRON & SCI SPAZIO,I-50125 FLORENCE,ITALY. UNIV TURIN,I-10125 TURIN,ITALY. OSSERV ASTRON TORINO,I-10125 PINO TORINESE,ITALY. RP Ciaravella, A (reprint author), EUROPEAN SPACE AGCY,ESTEC,NL-2200 AG NOORDWIJK,NETHERLANDS. RI Romoli, Marco/H-6859-2012; OI Benna, Carlo/0000-0003-1688-2434; Ciaravella, Angela/0000-0002-3127-8078; Giordano, Silvio/0000-0002-3468-8566 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 1997 VL 491 IS 1 BP L59 EP & DI 10.1086/311048 PN 2 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL509 UT WOS:A1997YL50900015 ER PT J AU Newman, LJ Cannon, LRG AF Newman, LJ Cannon, LRG TI Nine new species of Pseudobiceros (Platyhelminthes : Polycladida) from the Indo-Pacific SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article DE Pseudobiceros; Pseudocerotidae; polycladida; taxonomy ID PATTERN; COLOR AB Nine new species of marine flatworms (Platyhelminthes: Polycladida) belonging to the genus Pseudobiceros Faubel, 1984 are described from Indo-Pacific coral reefs including: the northern and southern Great Barrier Reef, eastern Australia; Ningaloo Reef and Exmouth, Western Australia; Madang, Papua New Guinea; and Koror, Palau, Micronesia. In addition, new records are given for seven recognised species from a range of Indo-Pacific locations. C1 Univ Queensland, Dept Zool, St Lucia, Qld 4072, Australia. RP Newman, LJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 36 TC 14 Z9 16 U1 0 U2 6 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 7 PY 1997 VL 45 IS 2 BP 341 EP 368 PG 28 WC Zoology SC Zoology GA YN006 UT WOS:000071123600013 ER PT J AU Ruiz, GM Carlton, JT Grosholz, ED Hines, AH AF Ruiz, GM Carlton, JT Grosholz, ED Hines, AH TI Global invasions of marine and estuarine habitats by non-indigenous species: Mechanisms, extent, and consequences SO AMERICAN ZOOLOGIST LA English DT Article; Proceedings Paper CT Symposium on Molecules to Mudflats, at the Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY DEC 26-30, 1995 CL WASHINGTON, D.C. SP Soc Integrat & Comparat Biol ID SAN-FRANCISCO BAY; CLAM POTAMOCORBULA-AMURENSIS; EUROPEAN GREEN CRAB; SHIPS BALLAST WATER; NATIVE MUD SNAILS; BIOLOGICAL INVASIONS; COMPETITIVE DISPLACEMENT; DREISSENA-POLYMORPHA; REMARKABLE INVASION; CARCINUS-MAENAS AB Non-indigenous species (NIS) are increasingly conspicuous in marine and estuarine habitats throughout the world, as the number, variety, and effects of these species continue to accrue. Most of these NIS invasions result from anthropogenic dispersal. Although the relative importance of different dispersal mechanisms varies both spatially and temporally, the global movement of ballast water by ships appears to be the largest single vector for NIS transfer today, and many recent invasions have resulted from this transfer. The rate of new invasions may have increased in recent decades, perhaps due to changes in ballast water transport. Estuaries have been especially common sites of invasions, accumulating from tens to hundreds of NIS per estuary that include most major taxonomic and trophic groups. We now know of approximately 400 NIS along the Pacific, Atlantic and Gulf coasts of the U.S., and hundreds of marine and estuarine NIS are reported from other regions of the world. Although available information about invasions is limited to a few regions and underestimates the actual number of NIS invasions, there are apparent differences in the frequency of NIS among sites. Mechanisms responsible for observed patterns among sites likely include variation in supply of NIS, and perhaps variation in properties of recipient or donor communities, but the role of these mechanisms has not been tested. Although our present knowledge about the extent, patterns and mechanisms of marine invasions is still in its infancy, it is clear that NIS are a significant force of change in marine and especially estuarine communities globally. Taxonomically diverse NIS are having significant effects on many, if not most, estuaries that fundamentally alter population, community, and ecosystems processes. The impacts of most NIS remain unknown, and the predictability of their direct and indirect effects remains uncertain. Nonetheless, based upon the documented extent of NIS invasions and scope of their effects, studies of marine communities that do not include NIS are increasingly incomplete. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Williams Coll Mystic Seaport, Maritime Studies Program, Mystic, CT 06355 USA. Univ New Hampshire, Dept Zool, Durham, NH 03824 USA. RP Ruiz, GM (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. OI Ruiz, Gregory/0000-0003-2499-441X NR 103 TC 472 Z9 508 U1 19 U2 135 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 1997 VL 37 IS 6 BP 621 EP 632 PG 12 WC Zoology SC Zoology GA YU144 UT WOS:000071686700020 ER PT J AU Geller, MJ Kurtz, MJ Wegner, G Thorstensen, JR Fabricant, DG Marzke, RO Huchra, JP Schild, RE Falco, EE AF Geller, MJ Kurtz, MJ Wegner, G Thorstensen, JR Fabricant, DG Marzke, RO Huchra, JP Schild, RE Falco, EE TI The century survey: A deeper slice of the universe SO ASTRONOMICAL JOURNAL LA English DT Article ID CFA REDSHIFT SURVEY; LUMINOSITY FUNCTION; FAINTER GALAXIES; X-RAY; DENSITY; VELOCITY; CLUSTER; SAMPLE; FIELD; ZONE AB The ''Century Survey'' (CS hereafter) is a complete redshift survey of a 1 degrees wide strip, It covers 0.03 steradians to a limiting m(R) = 16.13, The survey is 98.4% complete and contains 1762 galaxies. Large-scale features in the survey are qualitatively similar to those in other surveys: there are large voids surrounded or nearly surrounded by thin dense regions which are sections of structures like (and including) the Great Wall. The survey crosses the classical Corona Borealis supercluster. The galaxy density enhancement associated with this system extends for greater than or similar to 100h(-1) Mpc (the Hubble constant is H-0=100h km s(-1) Mpc(-1)). The Schechter (1976, ApJ, 203, 297) luminosity function parameters for the CS are: M-CS* = -20.73(-0.18)(+0.17), alpha(CS) = -1.17(-0.19)(+0.19), and phi(CS)*=0.0250+/-0.0061 Mpc(-3) mag(-1). In concert with the ESO Key Program (Vettolani er al. 1997, A&A, 325, 954; Zucca et al. 1997, A&A, 326, 477) and the AUTOFIB (Ellis et al, 1996, MNRAS, 280, 235) surveys, the CS indicates that the absolute normalization of the luminosity function exceeds estimates based on shallower and/or sparser surveys. (C) 1997 The American Astronomical Society. [S0004-6256(97)04212-X]. C1 DARTMOUTH COLL,DEPT PHYS & ASTRON,HANOVER,NH 03755. DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. RP Geller, MJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI KURTZ, Michael /B-3890-2009; OI Kurtz, Michael/0000-0002-6949-0090 NR 45 TC 80 Z9 80 U1 0 U2 3 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 1997 VL 114 IS 6 BP 2205 EP & DI 10.1086/118640 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL191 UT WOS:A1997YL19100001 ER PT J AU Barth, AJ Reichert, GA Ho, LC Shields, JC Filippenko, AV Puchnarewicz, EM AF Barth, AJ Reichert, GA Ho, LC Shields, JC Filippenko, AV Puchnarewicz, EM TI Ultraviolet emission from the liner nucleus of NGC 6500 SO ASTRONOMICAL JOURNAL LA English DT Article ID PHOTOIONIZATION MODELS; GALACTIC NUCLEI; GALAXIES; EXTINCTION; TELESCOPE; SPECTRUM; NGC-4579; NGC-6500; STARS; DUST AB As a step towards clarifying the ionization mechanism of LINERs, we have used the Hubble Space Telescope Faint Object Spectrograph to obtain an ultraviolet spectrum of the nucleus of NGC 6500. This is the first time that such a spectrum has been taken of a ''LINER 2'' nucleus-that is, a LINER lacking broad permitted emission lines like those in Type 1 Seyfert nuclei. Compared with more luminous Seyfert nuclei, the ultraviolet emission-line spectrum of. NGC 6500 is remarkable for its low-excitation character: C III] lambda 1909, C II] lambda 2326, and Mg II lambda 2800 are the strongest collisionally-excited lines in the spectrum, and C IV lambda 1549 is not detected. We use the emission-line fluxes to test the hypothesis, advanced by Dopita & Sutherland (1995, ApJ, 455, 468), that the narrow-line regions of LINERs are primarily excited by fast (150-500 km s(-1)) shocks, rather than photoionized by a central continuum source. The fast shock models are a poor match to the observed spectrum, as they predict much stronger emission than is observed for high-excitation lines such as C IV lambda 1549. Photoionization by an obscured nonstellar continuum source, or possibly ionization by slower (similar to 100 km s(-1)) shocks, are more likely explanations for the emission-line ratios. The origin of the ultraviolet continuum is unclear; its overall spectral shape is reasonably well matched by spectral evolution models for single-burst populations with ages in the range 70-100 Myr, but no definite stellar absorption features due to young stars are present. Alternately, the ultraviolet continuum (or some fraction of it) may be scattered radiation from a hidden active nucleus. We tentatively detect a broad He II lambda 4686 emission feature, which may be due to Wolf-Rayet stars, although the ultraviolet spectrum does not show any clear Wolf-Rayet signatures. We also find that NGC 6500 is weakly detected in an archival ROSAT HRI image with a luminosity of similar to 5 X 10(40) erg s(-1) in the 0.1-2.4 keV band, within the normal range for LINERs. (C) 1997 American Astronomical Society. [S0004-6256(97)00812-1]. C1 NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD 20771 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. OHIO UNIV, DEPT PHYS & ASTRON, ATHENS, OH 45701 USA. UCL, MULLARD SPACE SCI LAB, DORKING RH5 6NT, SURREY, ENGLAND. RP Barth, AJ (reprint author), UNIV CALIF BERKELEY, DEPT ASTRON, 601 CAMPBELL HALL, BERKELEY, CA 94720 USA. OI Barth, Aaron/0000-0002-3026-0562 NR 53 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 1997 VL 114 IS 6 BP 2313 EP 2322 DI 10.1086/118650 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL191 UT WOS:A1997YL19100011 ER PT J AU Smith, HA Strelnitski, V Miles, JW Kelly, DM Lacy, JH AF Smith, HA Strelnitski, V Miles, JW Kelly, DM Lacy, JH TI Mid-infrared hydrogen recombination line emission from the maser star SO ASTRONOMICAL JOURNAL LA English DT Article ID MWC 349A; MWC-349; SPECTROSCOPY; INTENSITIES; OUTFLOW; IONS AB We have detected and spectrally resolved the mid-IR hydrogen recombination lines H6 alpha (12.372 mu m), H7 alpha (19.062 mu m), H7 beta (11.309 mu m), and H8 gamma (12.385 mu m) from the star MWC 349A. This object has strong hydrogen maser emission reported in the millimeter and submillimeter hydrogen recombination lines from H36 alpha to H21 alpha, and laser emission seen in the H15 alpha, H12 alpha and H10 alpha lines. The lasers/masers are thought to arise predominantly in a Keplerian disk around the star. The mid-IR lines we measure do not show evident signs of lasing, and can be adequately modeled as arising from the strong stellar wind, with a component arising from a quasi-static atmosphere around the disk, similar to what is hypothesized for the near-IR (less than or equal to 4 mu m) recombination lines, Since population inversions are expected to exist in the levels producing these mid-IR transitions, even at electron densities where they could produce significant amplification (from 10(8) even up to 10(11) cm(-3)), our results imply that the disk does not contain such high-density ionized gas over long enough path lengths to produce a gain greater than or equal to 1. More modest laser emission might be present from smaller zones, for example, from high-density clumps within the disk, but is minor compared to the spontaneous background Line emission from the rest of the source. The results reinforce the interpretation of the three reported far-IR lines as true lasers. (C) 1997 American Astronomical Society. C1 MARIA MITCHELL OBSERV,NANTUCKET,MA 02554. LOCKHEED MARTIN ADV TECHNOL CTR,PALO ALTO,CA 94304. UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. RP Smith, HA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 30 TC 6 Z9 6 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 1997 VL 114 IS 6 BP 2658 EP 2663 DI 10.1086/118675 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL191 UT WOS:A1997YL19100036 ER PT J AU Curiel, S Raga, A Raymond, J NoriegaCrespo, A Canto, J AF Curiel, S Raga, A Raymond, J NoriegaCrespo, A Canto, J TI HST images of the high-excitation Herbig-Haro object HH 32 SO ASTRONOMICAL JOURNAL LA English DT Article ID BOW-SHOCK; STELLAR JET; EMISSION; MODELS; AS-353A/HH-32; PERFORMANCE; COMPLEX; TAURI; HH-32; WFPC2 AB We present high angular resolution emission-line and continuum images of the remarkable Herbig-Haro jet HH 32 obtained with the Wide Field and Planetary Camera 2 (WFPC2) aboard the Hubble Space Telescope. We have obtained narrow band [S II] lambda lambda 6716,6731, [N II] lambda 6583 and H alpha images, as well as an R continuum image, of this HH jet. The 0.'' 1 spatial resolution (corresponding to 30 AU at the distance of HH 32) and the high signal-to-noise ratio of these WFPC2 images allow us to study this highly collimated outflow in unprecedented detail. The images show differences between the stratification of the different emission lines. The knots are clearly resolved into complex structures that resemble working surfaces. The western side of the jet starts in a funnel-shaped structure that points toward the bright condensations HH 32D, 32B, and 32A, while on the other side of the jet the dominant structure is an arc-like feature that points almost directly away from the young star AS 353A. The HH 32A condensation exhibits a region strong in [S II] that we identify as the Mach Disk at the tip of the jet. Finally, the HST images are used in combination with previous, high resolution ground based observations (obtained with the Canada-France-Hawaii telescope) to obtain proper motion determinations. We find that the kinematical properties deduced from these proper motions are consistent with those of a jet moving at about 300 km/s, penetrating into the maternal cloud at an angle of 70 degrees between the outflow axis and the plane of the sky. This is also consistent with the properties deduced from previously obtained high resolution spectra of HH 32. We find that the kinematical properties deduced from these proper motions are completely consistent with previous proper motion measurements, as well as with the properties deduced from previously obtained, high resolution spectra of HH 32. (C) 1997 American Astronomical Society. [S0004-6256(97)01012-1]. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CALTECH,JET PROP LAB,CTR INFRARED PROC & ANAL,PASADENA,CA 91125. RP Curiel, S (reprint author), UNIV NACL AUTONOMA MEXICO,INST ASTRON,AP 70-264,MEXICO CITY 04510,DF,MEXICO. NR 35 TC 20 Z9 20 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 1997 VL 114 IS 6 BP 2736 EP & DI 10.1086/118682 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL191 UT WOS:A1997YL19100043 ER PT J AU Torres, G Stefanik, RP Andersen, J Nordstrom, B Latham, DW Clausen, JV AF Torres, G Stefanik, RP Andersen, J Nordstrom, B Latham, DW Clausen, JV TI Absolute dimensions of eclipsing binaries .22. The unevolved F-type system HS hydrae SO ASTRONOMICAL JOURNAL LA English DT Article ID SPECTROSCOPIC BINARIES; MODEL ATMOSPHERES; A-STAR; B-STAR; UVBY; TEMPERATURE; PHOTOMETRY; EVOLUTION; MASSES AB We have redetermined the masses of the unevolved F-type eclipsing binary HS Hya (P=1.57 days) from 70 observations with the CfA digital speedometers, combined with other observations from the literature. Analysis of our radial velocities determined with a two-dimensional cross-correlation technique shows the presence of a third star in the system, which we find to be most likely an M0 dwarf with a mass of similar to 0.5 M. in a 190-day orbit of small eccentricity and apparently co-planar with the eclipsing system. We also reanalyze an earlier set of light curves in the uvby system, using modern analysis techniques and combining all available spectroscopic and photometric data in the analysis. The resulting masses for the eclipsing stars are M-A=1.255+/-0.008 M. and M-B=1.219+/-0.007 M., similar to 6% smaller and similar to 6 times more accurate than previous values. The radii are R-A=1.275+/-0.007 R. and R-B=1.216+/-0.007 R., and the effective temperatures T-A=6500+/-50 K, T-B=6400+/-50 K; further properties of the stars are given in Table 7. Current stellar evolution models for the observed metallicity (slightly below solar) match the observed properties of both stars in HS Hya very well for a single, but strongly model-dependent age of similar to 1.0 Gyr. A precise spectroscopic determination of [Fe/H] for HS Hya is needed to further refine comparison with theoretical models. (C) 1997 The American Astronomical Society. [S0004-6256(97)04412-9]. C1 NBIFAFG,ASTRON OBSERV,DK-2100 COPENHAGEN,DENMARK. RP Torres, G (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 44 TC 49 Z9 50 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 1997 VL 114 IS 6 BP 2764 EP 2777 DI 10.1086/118685 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL191 UT WOS:A1997YL19100046 ER PT J AU Dahmen, G Huttemeister, S Wilson, TL Mauersberger, R Linhart, A Bronfman, L Tieftrunk, AR Meyer, K Wiedenhover, W Dame, TM Palmer, ES May, J Aparici, J MacAuliffe, F AF Dahmen, G Huttemeister, S Wilson, TL Mauersberger, R Linhart, A Bronfman, L Tieftrunk, AR Meyer, K Wiedenhover, W Dame, TM Palmer, ES May, J Aparici, J MacAuliffe, F TI Molecular gas in the Galactic center region .1. Data from a large scale (CO)-O-18(J=1->0) survey SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article DE telescopes; surveys; ISM, molecules, structure; galaxy, center; radio lines, ISM ID SOUTHERN MILKY-WAY; CARBON-MONOXIDE; CO SURVEY; CLOUD COMPLEX; CALIBRATION; GALAXY; SAGITTARIUS; RESOLUTION; EMISSION; PLANE AB A large scale survey of the Galactic center region in the (CO)-O-18(J = 1 --> 0) transition is presented. This survey was obtained with the 1.2 m Southern Millimeter-Wave Telescope (SMWT) at the Cerro Tololo Interamerican Observatory (CTIO) near La Serena, Chile. It covers the region 1.degrees 05 less than or equal to iota less than or equal to +3.degrees 6 and -0.degrees 9 less than or equal to b less than or equal to +0.degrees 75 with a grid spacing of 9', i.e. the sampling is at full FWHP beamwidth. 357 positions were in total observed. After reviewing the instrumentation of the 1.2m SMWT, the observing techniques, and the methods used in the data reduction, the data of the survey are presented and morphologically described. In addition, data of the HNCO(5(0,5) -4(0,4)) line are presented, which was also included in the large bandwidth of the spectrometer. (CO)-C-12(1 - 0) measurements performed for comparison purposes are presented and compared with other (CO)-C-12 results The maps of the (CO)-O-18(1 - 0) survey demonstrate that there are great differences between the distribution of the optically thin (CO)-O-18(1 - 0) emission and the usually optically thick (CO)-C-12(1 - 0) emission. C1 UNIV BONN,INST RADIOASTRON,D-53121 BONN,GERMANY. MAX PLANCK INST RADIOASTRON,D-53121 BONN,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CHILE,DEPT ASTRON,SANTIAGO,CHILE. UNIV LONDON QUEEN MARY & WESTFIELD COLL,DEPT PHYS,LONDON E1 4NS,ENGLAND. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. EUROPEAN SO OBSERV,SWEDISH ESO SUBMILLIMETRE TELESCOPE,SANTIAGO 19,CHILE. RI Bronfman, Leonardo/H-9544-2013 OI Bronfman, Leonardo/0000-0002-9574-8454 NR 60 TC 34 Z9 34 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 1997 VL 126 IS 2 BP 197 EP 236 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YK915 UT WOS:A1997YK91500001 ER PT J AU Rawson, DM Macri, LM Mould, JR Huchra, JP Freedman, WL Kennicutt, RC Ferrarese, L Ford, HC Graham, JA Harding, P Han, MS Hill, RJ Hoessel, JG Hughes, SMG Illingworth, GD Madore, BF Phelps, RL Saha, A Sakai, S Silbermann, NA Stetson, PB AF Rawson, DM Macri, LM Mould, JR Huchra, JP Freedman, WL Kennicutt, RC Ferrarese, L Ford, HC Graham, JA Harding, P Han, MS Hill, RJ Hoessel, JG Hughes, SMG Illingworth, GD Madore, BF Phelps, RL Saha, A Sakai, S Silbermann, NA Stetson, PB TI The extragalactic distance scale key project .8. The discovery of cepheids and a new distance to NGC 3621 using the Hubble Space Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE cepheids; distance scale; galaxies, distances and redshifts; galaxies, individual (NGC 3621); galaxies, photometry ID CCD PHOTOMETRY; CALIBRATION; GALAXIES; PERFORMANCE; CONSTANT; WFPC2; M100 AB We report on the discovery of Cepheids in the field spiral galaxy NGC 3621, based on observations made with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). NGC 3621 is one of 18 galaxies observed as a part of the HST Key Project on the Extragalactic Distance Scale, which aims to measure the Hubble constant to 10% accuracy. Sixty-nine Cepheids with periods in the range 9-60 days were observed over 12 epochs using the F555W filter, and over four epochs using the F814W filter. The HST F555W and F814W data were transformed to the Johnson V and Kron-Cousins I magnitude systems, respectively. Photometry was performed using two-independent packages, DAOPHOT II/ALLFRAME and DoPHOT. Period-luminosity relations in the V and I bands were constructed using 36 fairly isolated Cepheids present in our set of 69 variables. Extinction-corrected distance moduli relative to the LMC of 10.63 +/- 0.09 and 10.56 +/- 0.10 mag were obtained using the ALLFRAME and DoPHOT data, respectively. True distance moduli of 29.13 +/- 0.18 and 29.06 +/- 0.18 mag, corresponding to distances of 6.3 +/- 0.7 and 6.1 +/- 0.7 Mpc, were obtained by assuming values of mu(0) = 18.50 +/- 0.10 mag and E(V-I) = 0.13 mag for the distance modulus and reddening of the LMC, respectively. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. CALTECH,CTR INFRARED PROC & ANAL,PASADENA,CA 91125. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,WASHINGTON,DC 20015. UNIV WISCONSIN,DEPT ASTRON,MADISON,WI 53706. NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0EZ,ENGLAND. UNIV CALIF SANTA CRUZ,LICK OBSERV,UCO,SANTA CRUZ,CA 95064. NATL RES COUNCIL CANADA,HERZBERG INST ASTROPHYS,DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. RP Rawson, DM (reprint author), AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,INST ADV STUDIES,WESTON,ACT 2611,AUSTRALIA. OI Macri, Lucas/0000-0002-1775-4859 NR 32 TC 41 Z9 41 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 1 PY 1997 VL 490 IS 2 BP 517 EP & DI 10.1086/304882 PN 1 PG 398 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YJ454 UT WOS:A1997YJ45400006 ER PT J AU Mahadevan, R Quataert, E AF Mahadevan, R Quataert, E TI Are particles in advection-dominated accretion flows thermal? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies, elliptical and lenticular, cD; radiation mechanisms, thermal; radio continuum, galaxies ID BLACK-HOLES; MODEL; SYNCHROTRON; SPECTRUM; PLASMAS; DISKS; M31 AB We investigate the form of the momentum distribution function for protons and electrons in an advection-dominated accretion flow (ADAF). We show that for all accretion rates, Coulomb collisions are too inefficient to thermalize the protons. The proton distribution function is therefore determined by the viscous heating mechanism, which is unknown. The electrons, however, can exchange energy quite efficiently through Coulomb collisions and the emission and absorption of synchrotron photons. We find that for accretion rates greater than similar to 10(-3) of the Eddington accretion rate, the electrons have a thermal distribution throughout the accretion flow. For lower accretion rates, the electron distribution function is determined by the electron's source of heating, which is primarily adiabatic compression. Using the principle of adiabatic invariance, we show that an adiabatically compressed, collisionless gas maintains a thermal distribution until the particle energies become relativistic. We derive a new, nonthermal distribution function for relativistic energies and provide analytic formulae for the synchrotron radiation from this distribution. Finally, we discuss its implications for the emission spectra from ADAFs. RP Mahadevan, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 43 TC 54 Z9 53 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 1997 VL 490 IS 2 BP 605 EP 618 DI 10.1086/304908 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YJ454 UT WOS:A1997YJ45400012 ER PT J AU Magnier, EA Primini, FA Prins, S vanParadijs, J Lewin, WHG AF Magnier, EA Primini, FA Prins, S vanParadijs, J Lewin, WHG TI ROSAT HRI observations of M31 supernova remnants SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, individual (M31); galaxies, ISM; supernova remnants; X-rays, ISM ID INTERSTELLAR-MEDIUM; NOVA REMNANTS; DIFFUSE; GAS; CANDIDATES; IONIZATION AB We have observed M31 using the ROSAT HRI. We have searched for X-ray emission from supernova remnants (SNRs) previously identified from surveys using narrowband optical observations. We find that a surprisingly small number of the identified SNRs are detected in X-rays at a threshold of approximate to 10(35) ergs s(-1). The absence of detected X-ray flux from many of the optically identified SNRs suggests that the local ISM density in the vicinity of these SNRs is typically quite low, less than 0.1 cm(-3). The few that have been detected likely represent the upper end of the density distribution, having implied ambient densities in the range 0.1 to >10 cm(-3). Since H I observations show that all SNRs are in regions with large column densities, which implies densities of 1-10 cm(-3), a multicomponent ISM must be invoked. Our measured densities are upper limits for the dominant low-density component of the ISM. C1 OREGON STATE UNIV,DEPT PHYS,CORVALLIS,OR 97331. UNIV AMSTERDAM,ASTRON INST ANTON PANNEKOEK,NL-1098 SJ AMSTERDAM,NETHERLANDS. UNIV AMSTERDAM,CTR HIGH ENERGY ASTROPHYS,NL-1098 SJ AMSTERDAM,NETHERLANDS. MIT,CAMBRIDGE,MA 02139. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899. RP Magnier, EA (reprint author), UNIV WASHINGTON,DEPT ASTRON 351580,SEATTLE,WA 98195, USA. OI Primini, Francis/0000-0002-6077-0643 NR 17 TC 15 Z9 15 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 1997 VL 490 IS 2 BP 649 EP 652 DI 10.1086/304917 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YJ454 UT WOS:A1997YJ45400016 ER PT J AU Garnavich, PM NoriegaCrespo, A Raga, AC Bohm, KH AF Garnavich, PM NoriegaCrespo, A Raga, AC Bohm, KH TI Highly collimated molecular hydrogen jets near iras 05487+0255: Near-infrared imaging and spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared, ISM, lines and bands; ISM, individual (IRAS 05487 + 0255); ISM, jets and outflows; stars, formation ID HERBIG-HARO OBJECTS; PROPER MOTIONS; ORION; VELOCITY; LINE; H-2; OUTFLOWS; EMISSION; SHOCKS; HH-110 AB We present new narrowband near-infrared images together with K-band spectra of highly collimated bipolar jets close to the IRAS 05487+0255 source. The jets are located similar to 50 '' west of the Herbig-Haro 110 outflow. The jets are not visible at optical wavelengths and therefore do not fall into the ''standard'' Herbig-Haro object classification scheme. Nevertheless, they belong to an ever growing group of molecular hydrogen jets associated with young stellar objects that are optically undetected. The jets are very well collimated, with length-to-width ratios of similar to 10-20. The spectra of the jet and its counterjet in the K band show a limited number of H-2 emission lines that make it difficult to obtain an accurate excitation temperature. We estimate T-ex = 1104+/-67 K and T-ex = 920+/-156 K for the red and blue jet components, respectively. The radial velocities of the jet and counterjet, based on the shift of the (1,0) S(1) 2.121 mu m line, are similar to-275+/-50 km s(-1) and similar to 180+/-50 km s(-1), respectively, suggesting an angle of similar to 30 degrees-45 degrees between the jet and the line of sight. The H-2 emission di the entire jet extends for ar least 40 '', similar to 0.1 pc at the distance of Orion. If the flow velocity is comparable to that of the radial velocities, then the dynamical age of the system is quite short (similar to 500 yr), consistent with a young jet arising from an embedded source. Entrainment in a turbulent mixing layer may explain this morphology and spectral character. C1 CALTECH,JET PROP LAB,CTR INFRARED PROC & ANAL,PASADENA,CA 91125. NATL AUTONOMOUS UNIV MEXICO,INST ASTRON,MEXICO CITY 04510,DF,MEXICO. UNIV WASHINGTON,DEPT ASTRON FM20,SEATTLE,WA 98195. RP Garnavich, PM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 31 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 DEC 1 PY 1997 VL 490 IS 2 BP 752 EP 757 DI 10.1086/304887 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YJ454 UT WOS:A1997YJ45400025 ER PT J AU Antonucci, E Kohl, JL Noci, G Tondello, G Huber, MCE Gardner, LD Nicolosi, P Giordano, S Spadaro, D Ciaravella, A Raymond, CJ Naletto, G Fineschi, S Romoli, M Siegmund, OHW Benna, C Michels, J Modigliani, A Panasyuk, A Pernechele, C Smith, PL Strachan, L Ventura, R AF Antonucci, E Kohl, JL Noci, G Tondello, G Huber, MCE Gardner, LD Nicolosi, P Giordano, S Spadaro, D Ciaravella, A Raymond, CJ Naletto, G Fineschi, S Romoli, M Siegmund, OHW Benna, C Michels, J Modigliani, A Panasyuk, A Pernechele, C Smith, PL Strachan, L Ventura, R TI Velocity fields in the solar corona during mass ejections as observed with UVCS-SOHO SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; sun, corona; techniques, spectroscopic; ultraviolet, stars AB This Letter presents the observations of the first two coronal mass ejections (CMEs) obtained with the Ultraviolet Coronagraph Spectrometer of SOHO. Both CMEs were observed at high spectral resolution in the ultraviolet domain. The first event on 1996 June 6-7 was observed in H I Ly alpha lambda 1216 and Ly beta lambda 1026, O VI lambda lambda 1032 and 1037, Si XII lambda lambda 499 and 521 and imaged within 1.5 and 5 R-.. The second event on 1996 December 23 was observed in several H I lines and cool lines such as C III lambda 977, N III lambda lambda 990-992, and O V lambda 630. The analysis of line profiles has allowed us to determine the line-of-sight velocities of the extended corona during a mass ejection. In particular there is evidence for mass motions consistent with untwisting magnetic fields around an erupted flux tube in one of the events and line of sight velocities of 200 km s(-1) in the early phase of the second event presumably related to the expansion of the leading arch of the transient. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV FLORENCE,FLORENCE,ITALY. UNIV PADUA,PADUA,ITALY. EUROPEAN SPACE AGCY,ESTEC,DEPT SPACE SCI,NL-2200 AG NOORDWIJK,NETHERLANDS. UNIV TURIN,TURIN,ITALY. OSSERV ASTROFIS CATANIA,I-95125 CATANIA,ITALY. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. RP Antonucci, E (reprint author), OSSERV ASTRON TORINO,I-10025 PINO TORINESE,ITALY. RI Romoli, Marco/H-6859-2012; Ventura, Rita/B-7524-2016; Naletto, Giampiero/S-6329-2016; OI Ventura, Rita/0000-0002-5152-0482; Naletto, Giampiero/0000-0003-2007-3138; Benna, Carlo/0000-0003-1688-2434; Ciaravella, Angela/0000-0002-3127-8078; Spadaro, Daniele/0000-0003-3517-8688; Giordano, Silvio/0000-0002-3468-8566 NR 11 TC 18 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 DEC 1 PY 1997 VL 490 IS 2 BP L183 EP & DI 10.1086/311028 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YJ477 UT WOS:A1997YJ47700015 ER PT J AU Pen, UL AF Pen, UL TI Generating cosmological Gaussian random fields SO ASTROPHYSICAL JOURNAL LA English DT Article DE large-scale structure of universe; methods, numerical ID CLUSTERS; GALAXIES; STATISTICS AB We present a generic algorithm for generating Gaussian random initial conditions for cosmological simulations on periodic rectangular lattices. We show that imposing periodic boundary conditions on the real-space correlator and choosing initial conditions by convolving a white noise random field results in a significantly smaller error than the traditional procedure of using the power spectrum. This convolution picture produces exact correlation functions out to separations of L/2, where L is the box size, which is the maximum theoretically allowed. This method also produces top-hat sphere fluctuations that are exact at radii R less than or equal to L/4. It is equivalent to windowing the power spectrum with the simulation volume before discretizing, thus bypassing sparse sampling problems. The mean density perturbation in the volume is no longer constrained to be zero, allowing one to assemble a large simulation using a series of smaller ones. This is especially important for simulations of Ly alpha systems where small boxes with steep power spectra are routinely used. We also present an extension of this procedure that generates exact initial conditions for hierarchical grids at negligible cost. RP Pen, UL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 13 TC 25 Z9 25 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 1997 VL 490 IS 2 BP L127 EP L130 DI 10.1086/311042 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YJ477 UT WOS:A1997YJ47700002 ER PT J AU Yu, W Zhang, SN Harmon, BA Paciesas, WS Robinson, CR Grindlay, JE Bloser, P Barret, D Ford, EC Tavani, M Kaaret, P AF Yu, W Zhang, SN Harmon, BA Paciesas, WS Robinson, CR Grindlay, JE Bloser, P Barret, D Ford, EC Tavani, M Kaaret, P TI kHz quasi-periodic oscillation in island state of 4U 1608-52 as observed with RXTE/PCA SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, individual (4U 1608-52); stars, neutron; X-rays, stars ID RAY; 4U-1608-52 AB We report RXTE/PCA observations of 4U 1608-52 on March 15, 18, and 22 immediately after the outburst in early 1996. The persistent count rates ranged from 190 to 450 counts s(-1) (1-60 keV). During this period of time, 4U 1608-52 was in the island state. We detected quasi-periodic oscillation (QPO) features in the power density spectra (PDS) at 567-800 Hz on March 15 and 22, with source fractional root mean square (rms) amplitude of 13%-17% and widths of 78-180 Hz. The average rms amplitude of these QPO features is positively correlated with the energy. Our results imply that the neutron star spin frequency is possibly between 300 and 365 Hz. C1 UNIV SPACE RES ASSOC,HUNTSVILLE,AL 35806. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UPS,CNRS,CTR ETUD SPATIALE RAYONNEMENTS,F-31028 TOULOUSE 04,FRANCE. COLUMBIA UNIV,COLUMBIA ASTROPHYS LAB,NEW YORK,NY 10027. RP Yu, W (reprint author), INST HIGH ENERGY PHYS,LCRHEA,BEIJING 100039,PEOPLES R CHINA. NR 23 TC 35 Z9 36 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 1997 VL 490 IS 2 BP L153 EP L156 DI 10.1086/311033 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YJ477 UT WOS:A1997YJ47700008 ER PT J AU Zweerink, JA Akerlof, CW Biller, SD Boyle, P Buckley, JH Burdett, A Gordo, JB CarterLewis, DA Catanese, M Cawley, MF Fegan, DJ Finley, JP Gaidos, JA Hillas, AM Krennrich, F Lamb, RC Lessard, RW McEnery, JE Mohanty, G Quinn, J Rodgers, AJ Rose, HJ Samuelson, FW Schubnell, MS Sembroski, G Srinivasan, R Weekes, TC Wilson, C AF Zweerink, JA Akerlof, CW Biller, SD Boyle, P Buckley, JH Burdett, A Gordo, JB CarterLewis, DA Catanese, M Cawley, MF Fegan, DJ Finley, JP Gaidos, JA Hillas, AM Krennrich, F Lamb, RC Lessard, RW McEnery, JE Mohanty, G Quinn, J Rodgers, AJ Rose, HJ Samuelson, FW Schubnell, MS Sembroski, G Srinivasan, R Weekes, TC Wilson, C TI The Tev gamma-ray spectrum of Markarian 421 during an intense flare SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects; individual (Markarian 421); gamma rays, observations ID INTERGALACTIC INFRARED RADIATION; ACTIVE GALAXY MARKARIAN-421; PHOTONS; ABSORPTION; ENERGIES; EMISSION; 3C-279 AB We present the gamma-ray spectrum of the BL Lacertae object, Markarian 421, above 500 GeV during its most intense recorded TeV flare, on 1996 May 7. The spectrum is well fitted by a power law with an exponent of -2.56 +/- 0.07 +/- 0.1 (statistical and systematic errors). The spectrum extends above 5 TeV with no evidence for a cutoff, favoring determinations of the extragalactic infrared energy density that do not produce a sharp cutoff at these energies. C1 UNIV MICHIGAN,RANDALL LAB PHYS,ANN ARBOR,MI 48109. UNIV LEEDS,DEPT PHYS & ASTRON,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. HARVARD SMITHSONIAN CTR ASTROPHYS,FRED LAWRENCE WHIPPLE OBSERV,AMADO,AZ 85645. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. PURDUE UNIV,DEPT PHYS,W LAFAYETTE,IN 47907. CALTECH,SPACE RADIAT LAB,PASADENA,CA 91125. RP Zweerink, JA (reprint author), IOWA STATE UNIV,DEPT PHYS & ASTRON,AMES,IA 50011, USA. NR 38 TC 32 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 1997 VL 490 IS 2 BP L141 EP L144 DI 10.1086/311036 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YJ477 UT WOS:A1997YJ47700005 ER PT J AU Jivoff, P AF Jivoff, P TI Sexual competition among male blue crab, Callinectes sapidus SO BIOLOGICAL BULLETIN LA English DT Article ID CARCINUS-MAENAS CRUSTACEA; SPERM COMPETITION; CHESAPEAKE-BAY; REPRODUCTIVE SUCCESS; MATING SUCCESS; GAMMARUS-PULEX; DROSOPHILA-MELANOGASTER; ORCONECTES-RUSTICUS; CHIONOECETES-BAIRDI; SIZE AB Experiments and field data on blue crab, Callinectes sapidus, from mid-Chesapeake Bay between 1991 and 1994 were used to test whether large males have advantages over small males in accessing females and in sperm competition, In the field, large males were paired more often, especially with large, more fecund females. However, the variance in the relationship between male and female size in mating pairs was high, suggesting that mating with large females may not be the primary determinant of male reproductive success. Large males had proportionately longer chelipeds, which may provide an advantage in aggressive interactions for females or in struggles to control females, Previous work indicates that sperm competition may occur in blue crabs and that ejaculate size may influence a male's ability to compete during sperm competition. Large males stored more seminal fluid and spermatophores and passed a larger volume of ejaculate to each mate than did small males. Ejaculate volume averaged 47% of a male's stored supply. However, ejaculate volume increased with the duration of copulation but decreased with successive matings, such that males needed about 15 days between matings to pass similar-sized ejaculates to successive mates. Pre-copulatory mate guarding may serve as a time to replenish ejaculate contents, and thus its duration also influences a male's performance in sperm competition. C1 Univ Maryland, Dept Zool, College Pk, MD 20742 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Jivoff, P (reprint author), Rutgers State Univ, Marine Field Stn, 800 Great Bay Blvd, Tuckerton, NJ 08087 USA. EM jivoff@ahab.rutgers.edu NR 85 TC 59 Z9 61 U1 0 U2 8 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 J9 BIOL BULL JI Biol. Bull. PD DEC PY 1997 VL 193 IS 3 BP 368 EP 380 DI 10.2307/1542939 PG 13 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA YR505 UT WOS:000071502000008 ER PT J AU Feller, IC Mathis, WN AF Feller, IC Mathis, WN TI Primary herbivory by wood-boring insects along an architectural gradient of Rhizophora mangle SO BIOTROPICA LA English DT Article DE diversity; herbivory; inquilines; mangrove; plant architecture; primary xylovory; Rhizophora mangle; species richness; twig-feeding guild; wood-boring insects ID MANGROVE; PATTERNS; COMMUNITIES; GROWTH AB We investigated the distribution of primary xylovores in Rhizophora mangle (red mangrove) first-order branches, i.e., "twigs", along an architectural gradient on Belizean mangrove cays. Greater structural diversity in R. mangle architecture, xylovore availability, occurrence of natural enemies, and habitat do not result in variable xylovore species richness. Despite large differences in architectural complexity, tall, fringe, dwarf, and sapling trees host the same set of primary twig borers. However, call trees support greater diversity and abundance of twig inquilines than other tree forms. Primary twig borers have a key role in structuring these mangrove communities because their galleries and pupal chambers provide habitats for numerous species of secondary xylovores and inquilines. We also measured the amount of leaf area removed from R. mangle's canopy by wood-and leaf-feeding herbivores. Vigorously growing tall and sapling trees sustain greater losses because of twig borers than dwarf trees. However, xylovory in fringe trees was nor different from any of che other categories. Cumulative herbivory was greatest in the tall trees. In most cases, leaf-area loss as an indirect or collateral result of primary xylovory equaled or exceeded leaf-area loss as a direct result of folivory. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Feller, IC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. OI Feller, Ilka/0000-0002-6391-1608 NR 40 TC 36 Z9 39 U1 2 U2 15 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD DEC PY 1997 VL 29 IS 4 BP 440 EP 451 DI 10.1111/j.1744-7429.1997.tb00038.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA YQ473 UT WOS:000071391300005 ER PT J AU Greenberg, R Bichier, P Sterling, J AF Greenberg, R Bichier, P Sterling, J TI Bird populations in rustic and planted shade coffee plantations of eastern Chiapas, Mexico SO BIOTROPICA LA English DT Article DE Chiapas; coffee plantations; Inga; migratory birds; seasonality; shade coffee ID COMMUNITIES; DYNAMICS AB Much of the remaining "forest" vegetation in eastern Chiapas, Mexico is managed for coffee on. In this region coffee is grown under either the canopy of nat ural forest or under a planted canopy dominated by Inga spp. Despite the large differences in diversity of dominant plant species, both planted and rustic shade coffee plantations support a high overall diversity of bird species; we recorded approximately 105 species in each plantation type on fixed radius point counts. We accumulated a combined species list of 180 species on repeatedly surveyed transects through both coffee plantation types. These values are exceeded regionally only by moist tropical forest. Of the habitats surveyed, shade coffee was second only to acacia groves in the abundance and diversity of Nearctic migrants. The two plantation types have similar bird species lists and both are similar in composition to the dominant woodland-mixed pine-oak. Both types of shade coffee plantation habitats differ from other local habitats in supporting highly seasonal bird populations. Survey numbers almost double during the dry season-an increase that is found in omnivorous migrants and omnivorous, frugivorous, and nectarivorous resident species. Particularly large influxes were found for Tennessee warblers (Vermivora peregrina) and northern orioles (Icterus galbula) in Inga dominated plantations. C1 Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. RP Greenberg, R (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. NR 25 TC 147 Z9 159 U1 3 U2 17 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD DEC PY 1997 VL 29 IS 4 BP 501 EP 514 DI 10.1111/j.1744-7429.1997.tb00044.x PG 14 WC Ecology SC Environmental Sciences & Ecology GA YQ473 UT WOS:000071391300011 ER PT J AU Gilbert, GS Talaro, N Howell, CA Symstad, A AF Gilbert, GS Talaro, N Howell, CA Symstad, A TI Multiple-scale spatial distribution of the fungal epiphyll Scolecopeltidium on Trichilia spp. in two lowland moist tropical forests SO CANADIAN JOURNAL OF BOTANY-REVUE CANADIENNE DE BOTANIQUE LA English DT Article DE Trichilia tuberculata; Trichilia moritzii; Loculoascomycete; density dependence; Panama; Costa Rica ID DISPERSAL DISTANCE; CANKER DISEASE; TREE; SEEDLINGS; DIVERSITY; DENSITY; PATHOGENS; ECOLOGY; SEED AB The leaf-inhabiting fungus Scolecopeltidium mayteni (Micropeltaceae) is common on Trichilia tuberculata in lowland tropical forests on Barro Colorado Island, Panama, and on Trichilia moritzii in Corcovado National Park, Costa Pica. The sexual reproductive structures (ascomata) of the fungus have a clumped or random distribution on leaflet surfaces. The density of ascomata correlates well with the density of hyphae on the leaf surface and is a good indicator of the intensity of fungal colonization. Most of the variability in colonization is at a leaf-to-leaf level rather than among leaflets or among plants. Intensity of fungal colonization is directly related to the light environment of the leaflet or plant, but not to the density of hosts. The Scolecopeltidium-Trichilia system is well suited for studies on ecological factors affecting host-fungal symbioses in natural plant communities. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. RP Gilbert, GS (reprint author), Univ Calif Berkeley, Dept Enviromn Sci Policy & Management, 151 Hilgard Hall,MC 3110, Berkeley, CA 94720 USA. RI Gilbert, Gregory/C-2595-2008 NR 24 TC 6 Z9 6 U1 0 U2 2 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4026 J9 CAN J BOT JI Can. J. Bot.-Rev. Can. Bot. PD DEC PY 1997 VL 75 IS 12 BP 2158 EP 2164 PG 7 WC Plant Sciences SC Plant Sciences GA ZA839 UT WOS:000072407200014 ER PT J AU Barboza, PS Farley, SD Robbins, CT AF Barboza, PS Farley, SD Robbins, CT TI Whole-body urea cycling and protein turnover during hyperphagia and dormancy in growing bears (Ursus americanus and U-arctos) SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID FASTING POLAR BEARS; BLACK BEARS; SERUM UREA; NITROGEN-METABOLISM; SKELETAL-MUSCLES; WINTER SLEEP; SEAL PUPS; CREATININE; CONSERVATION; HIBERNATION AB Subadult bears were studied during their autumn hyperphagia (n = 3) and winter dormancy (n = 6). Urea kinetics were measured with C-14- and N-15-urea, protein turnover was estimated with N-15-glycine, and body composition was assessed with H-3-water. Reduced amino acid degradation in winter was indicated by declines in plasma urea and aminotransferase activities, and lower urea production than in autumn (4.7 vs. 27.5 mmol urea-N.kg(-0.75).d(-1)). Only 7.5% of urea produced in hyperphagic bears was degraded and just 1.1% of the degraded N reutilized as amino-N. Dormant bears reutilized 99.7% of urea produced, indicating thorough microbial ureolysis and urea-N resorption. Low rates of body N loss during dormancy suggested losses of non-urea N as creatinine. Protein turnover rates (15.2-21.5 g.kg(-0.75).d(-1)) were similar between seasons and reflected the apparent maintenance of hepatic, intestinal, and muscular functions through dormancy. Protein synthesis accounted for 32% of energy expended in dormancy, which was mainly (91.5%) derived from fat oxidation. Consistent organ function and body temperature in dormant bears enables recycling of urea-N, which minimizes body protein loss and conserves mobility. In comparison with heterothermic hibernation, ursid dormancy would provide greater flexibility during winter and facilitate rapid resumption of foraging and growth in spring. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Washington State Univ, Dept Nat Resource Sci, Pullman, WA 99164 USA. RP Barboza, PS (reprint author), Univ Alaska, Inst Arctic Biol, POB 757000, Fairbanks, AK 99775 USA. EM ffpsb@aurora.alaska.edu RI Jansen, Heiko/A-5770-2008 NR 62 TC 67 Z9 67 U1 1 U2 33 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD DEC PY 1997 VL 75 IS 12 BP 2129 EP 2136 DI 10.1139/z97-848 PG 8 WC Zoology SC Zoology GA YW150 UT WOS:000071903500023 ER PT J AU Graves, GR AF Graves, GR TI Geographic clines of age ratios of Black-throated Blue Warblers (Dendroica caerulescens) SO ECOLOGY LA English DT Article DE age ratio; Appalachian Mountains; Black-throated Blue Warbler; Dendroica caerulescens; despotism; dispersal; geographic clines; multiple brooding; source-sink dynamics ID POPULATION-DYNAMICS; NEOTROPICAL MIGRANT; SPATIAL VARIATION; HABITAT QUALITY; ABUNDANCE; DISPERSAL; BIRDS; DEMOGRAPHY; MATURATION; SINKS AB I investigated the age structure of breeding populations of Black-throated Blue Warblers (Dendroica caerulescens) in eastern North America. The proportion of yearling males increases as relative abundance decreases toward the margins of the breeding range. Geographic dines in age structure are hypothesized to correlate with gradients in habitat quality radiating from the Appalachian Mountains, the probable axis of source populations. Data from the southern Appalachians suggest that despotism of older males may impose a ceiling on the proportion of yearlings in saturated high-quality habitats, regardless of local productivity. Populations that exhibit low variance in yearling recruitment and high population densities may fall toward the ''source'' end of the ''source-sink'' continuum, and vice versa. It is hypothesized that the regional distribution of source and sink populations of the Black-throated Blue Warbler might closely mirror the prevalence of successful multiple brooding. C1 SMITHSONIAN INST, MUSEUM NATL HIST NAT, DEPT VERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. NR 59 TC 30 Z9 31 U1 0 U2 9 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD DEC PY 1997 VL 78 IS 8 BP 2524 EP 2531 PG 8 WC Ecology SC Environmental Sciences & Ecology GA YK726 UT WOS:A1997YK72600020 ER PT J AU Bennett, RA Wernicke, BP Davis, JL Elosegui, P Snow, JK Abolins, MJ House, MA Stirewalt, GL Ferrill, DA AF Bennett, RA Wernicke, BP Davis, JL Elosegui, P Snow, JK Abolins, MJ House, MA Stirewalt, GL Ferrill, DA TI Global positioning system constraints on fault slip rates in the Death Valley region, California and Nevada SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID STRAIN ACCUMULATION; SHEAR ZONE; DEFORMATION; EARTHQUAKES; BASIN AB We estimated horizontal velocities at 15 locations in the vicinity of Yucca Mountain, Nevada, from Global Positioning System surveys conducted between 1991 and 1996. We used these velocity estimates to infer slip rates an two major Quaternary faults within the eastern California shear zone (ECSZ), the Hunter Mountain and Death Valley faults. The sum of slip rates across the two faults is well determined at 5 +/- 1 mm/yr (1-sigma). Between 3 to 5 mm/yr of this motion appears to be accommodated along the Death Valley fault, implying 30-50 m of strain accumulation over the next 10,000 yr. If so, there is potential for 5 to 10 M-w 6.5-7.5 earthquakes during this period, a finding consistent with paleoseismological studies of the fault zone. Yucca Mountain, which lies 50 km east of the ECSZ, is the proposed location for the disposal of high-level nuclear waste in the United States. C1 CALTECH,PASADENA,CA 91125. CTR NUCL WASTE REGULATORY ANAL,SAN ANTONIO,TX 78238. INST ESTUDIS ESPECIALS DE CATALUNYA,BARCELONA,SPAIN. RP Bennett, RA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS 42,CAMBRIDGE,MA 02138, USA. RI Davis, James/D-8766-2013; OI Davis, James/0000-0003-3057-477X; Ferrill, David/0000-0002-3486-5526 NR 15 TC 29 Z9 29 U1 1 U2 6 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 DEC 1 PY 1997 VL 24 IS 23 BP 3073 EP 3076 DI 10.1029/97GL02951 PG 4 WC Geosciences, Multidisciplinary SC Geology GA YJ981 UT WOS:A1997YJ98100033 ER PT J AU Melson, WG Post, JE Wise, MA Sorenson, SS Fiske, RS Luhr, JF MacPherson, GJ McCoy, TJ AF Melson, WG Post, JE Wise, MA Sorenson, SS Fiske, RS Luhr, JF MacPherson, GJ McCoy, TJ TI Diamonds to diamonds: A tour of the Smithsonian's new geology, gems, & minerals hall SO GEOTIMES LA English DT Article AB This major new exhibit offers a tour of Earth and solar system treasures that begins with the famous Hope Diamond and ends with the diamond dust of a now dead star. World-class specimens and interactive displays invite the visitor to linger and learn about the planet's origins and resources. RP Melson, WG (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT MINERAL SCI,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 SN 0016-8556 J9 GEOTIMES JI Geotimes PD DEC PY 1997 VL 42 IS 12 BP 16 EP & PG 6 WC Geosciences, Multidisciplinary SC Geology GA YK105 UT WOS:A1997YK10500019 ER PT J AU Benner, LAM Ostro, SJ Giorgini, JD Jurgens, RF Mitchell, DL Rose, R Rosema, KD Slade, MA Winkler, R Yeomans, DK Campbell, DB Chandler, JF Shapiro, II AF Benner, LAM Ostro, SJ Giorgini, JD Jurgens, RF Mitchell, DL Rose, R Rosema, KD Slade, MA Winkler, R Yeomans, DK Campbell, DB Chandler, JF Shapiro, II TI Radar detection of near-earth asteroids 2062 Aten, 2101 Adonis, 3103 Eger, 4544 Xanthus, and 1992 QN SO ICARUS LA English DT Article DE asteroids; radar; Aten; Adonis; Eger; Xanthus ID GREENLAND ICE-SHEET; DYNAMICS; OBJECTS; APOLLO; VENUS AB We describe Doppler-only radar observations of near-Earth asteroids 2062 Aten, 2101 Adonis, 3103 Eger, 4544 Xanthus, and 1992 QN that were obtained at Arecibo and Goldstone between 1984 and 1996. Estimates of the echo spectral bandwidths, radar cross sections, and circular polarization ratios of these objects constrain their pole-on breadths, radar albedos, surface roughnesses, taxonomic classes, rotation periods, and pole directions. Aten's bandwidth is consistent with its radiometrically determined diameter of 0.9 km. Adonis has a rotation period P less than or equal to 11 h and an effective diameter (the diameter of a sphere with the same projected area as the asteroid) between 0.3 and 0.8 km. The radar properties of Adonis suggest it is not a member of taxonomic classes C or M. The effective diameter of Xanthus is between 0.4 and 2.2 km with a rotation period P less than or equal to 20 h. Echoes from 1992 QN constrain the asteroid's pole-on breadth to be greater than or equal to 0.6 km and probably exclude it from the C and M taxonomic classes. The strongest Eger echoes are asymmetric with bandwidths that set lower bounds of 1.5 and 2.3 km on the minimum and maximum breadths of the asteroid's pole-on silhouette. If Eger is modeled as a 1.5 x 2.3 km biaxial ellipsoid, then its effective diameter for an equatorial view is 1.5 km end-on and 1.9 km broadside or pole-on, implying a geometric albedo smaller than published values but still consistent with a classification as an E-type object, The near-unity circular polarization ratios of Adonis, Eger, and 1992 QN are among the highest values measured for any asteroid extreme near-surface roughness at centimeter to meter scales. (C) 1997 Academic Press. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Benner, LAM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM lance@think.jpl.nasa.gov NR 47 TC 26 Z9 26 U1 1 U2 2 PU ACADEMIC PRESS INC PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC PY 1997 VL 130 IS 2 BP 296 EP 312 DI 10.1006/icar.1997.5834 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YX415 UT WOS:000072037700006 ER PT J AU Lis, DC Keene, J Young, K Phillips, TG Bockelee-Morvan, D Crovisier, J Schilke, P Goldsmith, PF Bergin, EA AF Lis, DC Keene, J Young, K Phillips, TG Bockelee-Morvan, D Crovisier, J Schilke, P Goldsmith, PF Bergin, EA TI Spectroscopic observations of Comet C 1996 B2 (Hyakutake) with the Caltech submillimeter observatory SO ICARUS LA English DT Article ID DENSE INTERSTELLAR CLOUDS; ABUNDANCE RATIO; MILLIMETER WAVELENGTHS; PARENT MOLECULES; P-HALLEY; HCN; P/HALLEY; WATER; FORMALDEHYDE; CARBON AB The apparition of Comet C/1996 B2 (Hyakutake) offered an unexpected and rare opportunity to probe the inner atmosphere of a comet with high spatial resolution and to investigate with unprecedented sensitivity its chemical composition, We present observations of over 30 submillimeter transitions of HCN, H(13)CN, HNC, HNCO, CO, CH(3)OH, and H(2)CO in Comet Hyakutake carried out between 1996 March 18 and April 9 at the Caltech Submillimeter Observatory, Detections of the H(13)CN (4-3) and HNCO (16(0,16)-15(0,15)) transitions represent the first observations of these species in a comet. In addition, several other transitions, including HCN (8-7), CO (4-3), and CO (6-5) are detected for the first time in a comet as is the hyperfine structure of the HCN (4-3) line. The observed intensities of the HCN (4-3) hyperfine components indicate a line center optical depth of 0.9 +/- 0.2 on March 22.5 UT. The HCN/HNC abundance ratio in Comet Hyakutake at a heliocentric distance of 1 AU is similar to that measured in the Orion extended ridge-a warm, quiescent molecular cloud, The HCN/H(13)CN abundance ratio implied by our observations is 34 +/- 12, similar to that measured in giant molecular clouds in the galactic disk but significantly lower than the Solar System (12)C/(13)C ratio. The low HCN/H(13)CN abundance ratio may be in part due to contamination by an SO(2) line blended with the H(13)CN (4-3) line, In addition, chemical models suggest that the HCN/H(13)CN ratio can be affected by fractionation during the collapse phase of the protosolar nebula; hence a low HCN/H(13)CN ratio observed in a comet is not inconsistent with the solar system (12)C/(13)C isotopic ratio, The abundance of HNCO relative to water derived from our observations is (7 +/- 3) x 10(-4), The HCN/HNCO abundance ratio is similar to that measured in the core of Sagittarius B2 molecular cloud. Although a photo-dissociative channel of HNCO leads to CO, the CO produced by HNCO is a negligible component of cometary atmospheres. Production rates of HCN, CO, H(2)CO, and CH(3)OH are presented, Inferred molecular abundances relative to water are typical of those measured in comets at 1 AU from the Sun. The exception is CO, for which we derive a large relative abundance of 30%. The evolution of the HCN production rate between March 20 and March 30 suggests that the increased activity of the comet was the cause of the fragmentation of the nucleus, The time evolution of the H(2)CO emission suggests production of this species from dust grains. (C) 1997 Academic Press. C1 CALTECH, Submillimeter Observ, Pasadena, CA 91125 USA. Observ Meudon, F-92195 Meudon, France. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Cornell Univ, NAIC, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lis, DC (reprint author), CALTECH, Submillimeter Observ, MS 320-47, Pasadena, CA 91125 USA. EM dcl@medoc.caltech.edu RI Goldsmith, Paul/H-3159-2016 NR 58 TC 72 Z9 72 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC PY 1997 VL 130 IS 2 BP 355 EP 372 DI 10.1006/icar.1997.5833 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YX415 UT WOS:000072037700011 ER PT J AU Kondratas, R AF Kondratas, R TI Spectacles and other vision aids: A history and guide to collecting. SO ISIS LA English DT Book Review C1 Natl Museum Amer Hist, Div Sci Med & Soc, Smithsonian Inst, Washington, DC 20560 USA. Natl Museum Amer Hist, Dept Hist, Smithsonian Inst, Washington, DC USA. RP Kondratas, R (reprint author), Natl Museum Amer Hist, Div Sci Med & Soc, Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0021-1753 J9 ISIS JI Isis PD DEC PY 1997 VL 88 IS 4 BP 700 EP 701 DI 10.1086/383860 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA YZ855 UT WOS:000072300900013 ER PT J AU Warner, DJ AF Warner, DJ TI Sympathetic attractions: Magnetic practices, beliefs, and symbolism in eighteenth-century England. SO ISIS LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Phys Sci Collect, Washington, DC 20560 USA. RP Warner, DJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Phys Sci Collect, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0021-1753 J9 ISIS JI Isis PD DEC PY 1997 VL 88 IS 4 BP 712 EP 712 DI 10.1086/383873 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA YZ855 UT WOS:000072300900028 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI Aiming at targets: The autobiography of Robert C. Seamans, Jr. SO ISIS LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5801 S ELLIS AVENUE, CHICAGO, IL 60637 USA SN 0021-1753 J9 ISIS JI Isis PD DEC PY 1997 VL 88 IS 4 BP 743 EP 744 DI 10.1086/383910 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA YZ855 UT WOS:000072300900065 ER PT J AU Galili, E Stanley, DJ Sharvit, J WeinsteinEvron, M AF Galili, E Stanley, DJ Sharvit, J WeinsteinEvron, M TI Evidence for earliest olive-oil production in submerged settlements off the Carmel coast, Israel SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Carmel coast; Israel; submerged settlements; late neolithic; olive-oil extraction ID SEA-LEVEL; OLD-WORLD; LEVANT; BP AB Thousands of crushed olive stones with olive pulp are concentrated in pits at the Kfar Samir prehistoric settlement off the Carmel coast south of Haifa. Observations at this site, and at other Late Neolithic to Early Chalcolithic offshore settlements in this region, record an olive-oil technology that began along the Carmel coastal plain as early as 6500 years ago. This is about 500 years earlier than previously held. These new finds help define the technology of olive-oil production and refine the chronological definition of cultural units along the southern Levant coast during the 7th millennium BP: a time of major transition between the end of the Neolithic and beginning of the Chalcolithic. (C) 1997 Academic Press Limited. C1 SMITHSONIAN INST,DELTAS GLOBAL CHANGE PROGRAM,WASHINGTON,DC 20560. UNIV HAIFA,ZINMAN INST ARCHAEOL,IL-31905 HAIFA,ISRAEL. RP Galili, E (reprint author), ISRAEL ANTIQUITIES AUTHOR,MARINE ARCHAEOL BRANCH,POB 180,IL-30350 ATLIT,ISRAEL. NR 37 TC 40 Z9 41 U1 2 U2 7 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD DEC PY 1997 VL 24 IS 12 BP 1141 EP 1150 DI 10.1006/jasc.1997.0193 PG 10 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA YL182 UT WOS:A1997YL18200008 ER PT J AU Ehrenfeld, JG Han, XG Parsons, WFJ Zhu, WX AF Ehrenfeld, JG Han, XG Parsons, WFJ Zhu, WX TI On the nature of environmental gradients: temporal and spatial variability of soils and vegetation in the New Jersey Pinelands SO JOURNAL OF ECOLOGY LA English DT Article DE environmental gradients; nitrogen availability; organic horizon; Pinelands; shrub communities; soil moisture; soil variability; spatial pattern; spodosol; vegetation ID NITROGEN MINERALIZATION; FOREST-FLOOR; LATERAL VARIABILITY; PARALLEL ANALYSIS; BRITISH-COLUMBIA; TREEFALL GAPS; NITRIFICATION; AVAILABILITY; PATTERNS; ROOTS AB 1 Environmental variability can occur over various spatial scales, ranging from small patches at the scale of individual plants to long gradients over hundreds of metres. 2 In the New Jersey Pinelands, different species in the diverse shrub understorey of pitch pine (Pinus rigida Mill.) forests are patterned at these various scales, 3 Soil moisture, extractable NH4-N and N mineralization rate vary in complex ways, with the scale of spatial patterning changing over time and with depth in the soil profile. Moisture in both mineral and organic horizons, and NH4-N in the organic horizon, have patterns that are more stable over time than the mineralization rate in either horizon, or the NH4-N concentrations in the mineral horizon. 4 Vegetation patterns, as captured in principal components analysis, were poorly explained by any of the soil properties. Only the more temporally stable properties showed any relationship with vegetation patterns. 5 These results suggest that environmental gradients reflect patterns of environmental variation in four dimensions, Variation in the vertical dimension and over time is as pronounced and important as variation in the horizontal dimensions. 6 Many methods used to analyse vegetation implicitly assume temporal and spatial stability of environmental properties, Our results suggest that a more complex, four-dimensional assessment of environmental variation should be incorporated into models of vegetation-environment relationships. C1 Dept Ecol Evolut & Nat Resources, New Brunswick, NJ 08903 USA. Acad Sinica, Inst Bot, Beijing 100044, Peoples R China. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Fordham Univ, Calder Ecol Ctr, Armonk, NY 10504 USA. RP Ehrenfeld, JG (reprint author), Rutgers State Univ, Cook Coll, 126 Environm & Nat Resource Sci Bldg, New Brunswick, NJ 08903 USA. RI Han, Xingguo/K-7552-2016 OI Han, Xingguo/0000-0002-1836-975X NR 57 TC 52 Z9 60 U1 3 U2 21 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD DEC PY 1997 VL 85 IS 6 BP 785 EP 798 DI 10.2307/2960602 PG 14 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA YL835 UT WOS:000070998600006 ER PT J AU Wijesinghe, DK Whigham, DF AF Wijesinghe, DK Whigham, DF TI Costs of producing clonal offspring and the effects of plant size on population dynamics of the woodland herb Uvularia perfoliata (Liliaceae) SO JOURNAL OF ECOLOGY LA English DT Article DE canopy gaps; reproductive costs; reserve formation; shade tolerant; storage roots; vegetative propagation ID WILD STRAWBERRY POPULATIONS; LADYS-SLIPPER ORCHID; ASTER-ACUMINATUS; TRANSPLANTED RAMETS; RESOURCE-ALLOCATION; CLINTONIA-BOREALIS; FRUIT PRODUCTION; FOREST HERBS; LEAF-AREA; REPRODUCTION AB 1 Clonal propagation is an important means of population increase in many temperate woodland herbs. The production of vegetative propagules is often limited by the patchy availability of light in the understorey. A field study and a greenhouse experiment investigated the patterns of clonal growth under different light conditions in the shade-tolerant herb species Uvularia perfoliata. 2 In the field study, vegetative propagation in four populations, two growing under closed canopy and two in gaps, was compared. A significantly higher proportion of plants in gap populations produced clonal offspring than plants from closed-canopy populations, possibly because of higher light availability. The cost to plants of producing clonal offspring was seen as a significantly lower probability of survival and reduced capacity of the survivors for future clonal propagation. 3 In the greenhouse experiment, offspring ramets of three size classes (small, medium and large) from both closed-canopy and gap sites were grown under low and high light conditions. Plants grown from larger ramets from both sites produced more clonal offspring and invested more biomass in reserves and clonal propagation than plants grown from small ramets. Counter to our expectations, plants did not produce more clonal offspring in high light than in low light. However, plants invested more biomass in clonal propagation in high light, especially if they were grown from larger ramets. The only evidence for adaptation to conditions at the site of origin was that increased reserve allocation in high light was more marked in plants from gaps. The effect of ramet size on performance was stronger than the effect of light level or site of origin of plants, although plants grown from larger ramets also benefited more from high light. 4 Unless plants have sufficient biomass and morphological capacity their positive response to high light is delayed. Although clonal propagation is always costly, costs are less severe in gaps where plants have the potential to produce clonal offspring repeatedly in consecutive seasons. Our results also show that plant size has a potential long-term effect on population dynamics of this species, with the advantages of large size expressed over several generations. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Wijesinghe, DK (reprint author), Univ Sussex, Sch Biol Sci, Brighton BN1 9QG, E Sussex, England. NR 41 TC 33 Z9 40 U1 2 U2 8 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD DEC PY 1997 VL 85 IS 6 BP 907 EP 919 DI 10.2307/2960611 PG 13 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA YL835 UT WOS:000070998600015 ER PT J AU Kuhlmann, ML AF Kuhlmann, ML TI Regulation of fish reproduction by a predatory gastropod: an experimental investigation of indirect effects in a seagrass community SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE blenny; Chasmodes saburrae; gastropod predation; horse conch; indirect effect; reproduction ID BENTHIC COMMUNITY; HERMIT CRABS; PREY; COMPETITION; STRESS; SIZE AB The indirect effects of the horse conch, a predatory gastropod, on reproduction in a suite oft fishes that use the shells of the gastropod's main prey (the pen shell Atrina rigida (Sol.)) as nest sites in St. Joseph Bay, Florida, was investigated by examining the two links (direct interactions) that create the indirect effect. The horse conch-A. rigida predator-prey interaction was quantified by measuring predator feeding rate and distribution across a range of prey density. To determine the effect of A. rigida mortality on fish reproduction, the rate of shell availability was experimentally manipulated and egg production measured in four fish species. Horse conch feeding rate and distribution were not functions of prey density, but A. rigida mortality was correlated with conch abundance, supporting previous evidence that horse conchs regulate new shell availability. increased rates of shell availability caused increases in the number of clutches laid and average clutch size in one fish species, Chasmodes saburrae Jordan & Gilbert, probably because new shells provide a greater surface area for eggs compared to older shells. These results suggest that horse conchs indirectly affect C. saburrae reproduction both at the level of the individual (clutch size) and the population (egg production) by regulating the availability of new shells, Because prey density had little effect on the predator, variation in the indirect effect of conchs on fish reproduction win be primarily influenced by the distribution of the predator, not A. rigida. (C) 1997 Elsevier Science B.V. C1 Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. RP Kuhlmann, ML (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 39 TC 4 Z9 4 U1 2 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD DEC 1 PY 1997 VL 218 IS 2 BP 199 EP 214 DI 10.1016/S0022-0981(97)00074-9 PG 16 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA YR565 UT WOS:000071508000003 ER PT J AU Tchesunov, AV Hope, WD AF Tchesunov, AV Hope, WD TI Thalassomermis megamphis n. gen., n. sp. (Mermithidae : Nemata) from the bathyal south Atlantic Ocean SO JOURNAL OF NEMATOLOGY LA English DT Article DE abyssal; Benthimermithidae; deep-sea; Foraminifera; marine nematode; Mermithidae; parasite; Rhaptothyreidae; Thalassomermis megamphis n. gen., n. sp.; taxonomy AB Thalassomermis megamphis n. gen., n. sp. (Mermithidae: Nemata) was extracted from sediment collected off the coast of Brazil at a depth of approximately 1,000 m. Although the food of this new nematode is unknown, the reduction of the stoma and esophagus and presence of a trophosome indicate that it is parasitic in its juvenile stages. Thalassomenis megamphis n. gen., n, sp. is assigned to Mermithidae because of its similarity to that family in the appearance of the cephalic sensory receptors, the long and tubular vagina, and copulatory muscles of the male extending posteriorly throughout most of the length of the tail. Thalassomermis megamphis n. gen., n. sp. differs from all other members of Mermithidae by the large, lenticular, intracuticular amphidial fovea with coiled, emergent terminal filaments as well as the small amphidial aperture situated over the center of the fovea. C1 Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. Smithsonian Inst, Dept Invertebrate Zool, Museum Natl Hist Nat, Washington, DC 20560 USA. RP Tchesunov, AV (reprint author), Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. NR 30 TC 7 Z9 8 U1 0 U2 0 PU SOC NEMATOLOGISTS PI LAKELAND PA 3012 SKYVIEW DRIVE, LAKELAND, FL 33801-7072 USA SN 0022-300X J9 J NEMATOL JI J. Nematol. PD DEC PY 1997 VL 29 IS 4 BP 451 EP 464 PG 14 WC Zoology SC Zoology GA ZB969 UT WOS:000072526500004 PM 19274181 ER PT J AU Liu, ZJ Hallberg, GR Zimmerman, DL Libra, RD AF Liu, ZJ Hallberg, GR Zimmerman, DL Libra, RD TI Detecting changes in the spatial distribution of nitrate contamination in ground water SO JOURNAL OF THE AMERICAN WATER RESOURCES ASSOCIATION LA English DT Article DE spatial distribution; trend surface analysis; nitrate; ground water; water quality; non-point source pollution; agriculture ID NITROGEN AB Many studies of ground water pollution in general and nitrate contamination in particular have often relied on a one-time investigation, tracking of individual wells, or aggregate summaries. Studies of changes in spatial distribution of contaminants over time are lacking. This paper presents a method to compare spatial distributions for possible changes over time. The large-scale spatial distribution at a given time can be considered as a surface over the area (a trend surface). The changes in spatial distribution from period to period can be revealed by the differences in the shape and/or height of surfaces. If such a surface is described by a polynomial function, changes in surfaces can be detected by testing statistically for differences in their corresponding polynomial functions. This method was applied to nitrate concentration in a population of wells in an agricultural drainage basin in Iowa, sampled in three different years. For the period of 1981-1992, the large-scale spatial distribution of nitrate concentration did not show significant change in the shape of spatial surfaces; while the magnitude of nitrate concentration in the basin, or height of the computed surfaces showed significant fluctuations. The change in magnitude of nitrate concentration is closely related to climatic variations, especially in precipitation. The lack of change in the shape of spatial surfaces means that either the influence of land use/nitrogen management was overshadowed by climatic influence, or the changes in land use/management occurred in a random fashion. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Iowa, Hyg Lab, Iowa City, IA 52242 USA. Univ Iowa, Dept Stat & Actuarial Sci, Iowa City, IA 52242 USA. Iowa Dept Nat Resources, Geol Survey Bur, Iowa City, IA 52242 USA. RP Liu, ZJ (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 32 TC 6 Z9 6 U1 1 U2 2 PU AMER WATER RESOURCES ASSOC PI HERNDON PA 950 HERNDON PARKWAY SUITE 300, HERNDON, VA 20170-5531 USA SN 0043-1370 J9 J AM WATER RESOUR AS JI J. Am. Water Resour. Assoc. PD DEC PY 1997 VL 33 IS 6 BP 1209 EP 1218 DI 10.1111/j.1752-1688.1997.tb03547.x PG 10 WC Engineering, Environmental; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA YR465 UT WOS:000071498000006 ER PT J AU Liu, ZJ Hallberg, GR Malanson, GP AF Liu, ZJ Hallberg, GR Malanson, GP TI Structural equation modeling of dynamics of nitrate contamination in ground water SO JOURNAL OF THE AMERICAN WATER RESOURCES ASSOCIATION LA English DT Article DE structural equation modeling; nitrate dynamics; ground water; non-point source pollution; agriculture ID NITROGEN AB Most research on the temporal aspect of nitrate pollution in water resources has focused on surface water. Comprehensive studies on the dynamics of nitrate in ground water are lacking, especially on a drainage basin scale and for relatively long periods of time. In this study, structural equation modeling is applied in investigating the influences of climate, hydrology, and nitrogen management in agricultural production on nitrate concentration in the Big Spring Basin, Iowa, over a 10-year period. The study shows that for given hydrogeological settings, nitrogen management practices and climate are the two most important factors that affect nitrate dynamics. The long-term trend of nitrate is closely related to the nitrogen input primarily determined by management practices. The potential effects of nitrogen management, however, are contingent on the variations of climate. The improvements in water quality (reduced nitrate concentration and loads) in relation to improved nitrogen management are often overshadowed by the impact of climate, especially in extremely dry or wet years. The variations of climate and hydrology have much greater impacts on the nitrate dynamics than the changes in nitrogen input. This study reveals significant seasonal variation in the relations between nitrate concentration and influencing factors, which is also closely related to the seasonal variation in climate. Assessment of management practices and resultant water quality should consider the impact of short- and long-term climate dynamics. C1 Univ Iowa, Hyg Lab, Iowa City, IA 52242 USA. Univ Iowa, Dept Geog, Iowa City, IA 52242 USA. RP Liu, ZJ (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 41 TC 9 Z9 9 U1 0 U2 3 PU AMER WATER RESOURCES ASSOC PI HERNDON PA 950 HERNDON PARKWAY SUITE 300, HERNDON, VA 20170-5531 USA SN 0043-1370 J9 J AM WATER RESOUR AS JI J. Am. Water Resour. Assoc. PD DEC PY 1997 VL 33 IS 6 BP 1219 EP 1235 DI 10.1111/j.1752-1688.1997.tb03548.x PG 17 WC Engineering, Environmental; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA YR465 UT WOS:000071498000007 ER PT J AU Florentine, FA Anderson, L MacLennan, D Whitehead, LA AF Florentine, FA Anderson, L MacLennan, D Whitehead, LA TI Lighting high bay areas with electrodeless lamps SO JOURNAL OF THE ILLUMINATING ENGINEERING SOCIETY LA English DT Article AB At the National Air and Space Museum (NASM), Smithsonian institution, in Washington, DC, the existing high intensity discharge luminaires in three high bay areas have reached the end of their effective useful life. The standard mercury lamp and the magnetic ballast in an open front fixture presented serious maintenance as well as disposal problems. Retrofitting of existing equipment had been accomplished to correct the most serious problems, but the museum desired a long-term solution involving innovative approaches to the illumination of the space, The design solution involved the Department of Energy; Fusion Lighting System of Rockville, MD, Lorne Whitehead of Vancouver, BC; and NASM. The result was a prototype sulfur lighting system (SLS), which includes an electrodeless light source driven by microwave energy and a 250 mm diameter by 23 m long light pipe. Three light sources and three light pipes have been installed on a north-south asis, mounted near the existing luminaires. The SLS provides ease of access for maintenance, a collimated light pattern, and a long life, energy efficient source. The SLS employs total internal reflection (TIR) principles for the distribution of light. The TIR principle decreases apparent glare while collimating die light into the high bay area. The SLS has a color rendering index greater than 80, far exceeding the exisiting systems' CRI of 50 or less. The prototype, as well as the old system, has been installed and is operational. Both systems have been measured by Lawrence Berkeley Laboratory. Both systems' data have been compiled into charts showing the energy savings and changes in light levels. C1 CONSERVAT & RENEWABLE ENERGY, DEPT ENERGY, WASHINGTON, DC USA. FUS LIGHTING, VISIBLE LIGHTING, ROCKVILLE, MD USA. UNIV BRITISH COLUMBIA, DEPT PHYS, VANCOUVER, BC, CANADA. RP Florentine, FA (reprint author), SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, WASHINGTON, DC 20560 USA. OI Whitehead, Lorne/0000-0002-4170-0033 NR 19 TC 8 Z9 9 U1 0 U2 1 PU ILLUMINAT ENG SOC NORTH AMER PI NEW YORK PA 120 WALL ST, 17TH FL, NEW YORK, NY 10005-4001 SN 0099-4480 J9 J ILLUM ENG SOC JI J. Illum. Eng. Soc. PD WIN PY 1997 VL 26 IS 1 BP 27 EP + PG 10 WC Optics SC Optics GA XA026 UT WOS:A1997XA02600019 ER PT J AU Polhemus, DA Polhemus, JT AF Polhemus, DA Polhemus, JT TI A review of the genus Limnometra Mayr in New Guinea, with the description of a very large new species (Heteroptera : Gerridae) SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Review AB The species of the water strider genus Limnometra occuring on New Guinea and proximate islands are reviewed, and a very large new species, L. grallator, is described from the southern flanks of the central highlands. On the basis of male endosomal sclerotization, this new species appears to be most closely related to L. kallisto (Kirkaldy), a much smaller species also endemic to greater New Guinea. A key to all New Guinea Limnometra species is provided, accompanied by illustrations of the male endosomal sclerites and range maps. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Polhemus, DA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 105, Washington, DC 20560 USA. NR 3 TC 2 Z9 4 U1 1 U2 1 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD WIN-SPR PY 1997 VL 105 IS 1-2 BP 24 EP 39 PG 16 WC Entomology SC Entomology GA YZ920 UT WOS:000072308000003 ER PT J AU Domning, DP Emry, RJ Portell, RW Donovan, SK Schindler, KS AF Domning, DP Emry, RJ Portell, RW Donovan, SK Schindler, KS TI Oldest West Indian land mammal: Rhinocerotoid ungulate from the Eocene of Jamaica SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article C1 Howard Univ, Dept Anat, Washington, DC 20059 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. Univ W Indies, Dept Geog & Geol, Kingston 7, Jamaica. Lowell Observ, Flagstaff, AZ 86001 USA. RP Domning, DP (reprint author), Howard Univ, Dept Anat, Washington, DC 20059 USA. RI Donovan, Stephen/O-1285-2015 NR 25 TC 18 Z9 22 U1 0 U2 2 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD DEC PY 1997 VL 17 IS 4 BP 638 EP 641 PG 4 WC Paleontology SC Paleontology GA YM299 UT WOS:000071049700002 ER PT J AU Spelman, LH Jochem, WJ Sumner, PW Redmond, DP Stoskopf, MK AF Spelman, LH Jochem, WJ Sumner, PW Redmond, DP Stoskopf, MK TI Postanesthetic monitoring of core body temperature using telemetry in North American river otters (Lutra canadensis) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE river otter; Lutra canadensis; telemetry; temperature; anesthesia ID ANESTHESIA; ENDOTHERMS; FEED; FOOD AB Remote thermal telemetry was performed on North American river otters (Lutra canadensis) during the 1995 North Carolina Wildlife Resources Commission Otter Restoration Project. Otters were anesthetized with either ketamine-midazolam (n = 11) or tiletamine-zolazepam (n = 9) combinations. Based upon initial rectal temperatures, mild to moderate hyperthermia (39.4-40.5 degrees C) developed in five otters given ketamine-midazolam and three otters given tiletamine-zolazepam. Following anesthetic induction, each otter received an ingestible temperature transmitter. Dependent upon gastrointestinal transit time and transmitter battery life, core body temperature was monitored for up to 13.75 hr postanesthesia. Thermal telemetry revealed a gradual decline in core temperature in all otters after anesthetic recovery (30-60 min). Median core temperature stabilized subsequently within 0.3 degrees C of resting temperature (38.4 degrees C) 1.75 hr after initial injection in otters given tiletamine-zolazepam and 2.75 hr in otters given ketamine-midazolam. Minor fluctuations in body temperature (less than 1 degrees C) occurred in most otters from 6 to 13.75 hr and were attributed to variations in physical activity. C1 N Carolina State Univ, Coll Vet Med, Environm Med Consortium, Raleigh, NC 27606 USA. N Carolina Wildlife Resources Commiss, Raleigh, NC 27604 USA. Walter Reed Army Med Ctr, Walter Reed Army Inst Res, Dept Behav Biol, Washington, DC 20307 USA. Res Triangle Inst, Biomed Engn Program, Res Triangle Pk, NC 27709 USA. RP Spelman, LH (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave, Washington, DC 20008 USA. NR 18 TC 5 Z9 5 U1 0 U2 7 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD DEC PY 1997 VL 28 IS 4 BP 413 EP 417 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA ZA013 UT WOS:000072319000008 PM 9523635 ER PT J AU Spelman, LH Sumner, PW Karesh, WB Stoskopf, MK AF Spelman, LH Sumner, PW Karesh, WB Stoskopf, MK TI Tiletamine-zolazepam anesthesia in North American river otters (Lutra canadensis) and its partial antagonism with flumazenil SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE river otter; Lutra canadensis; anesthesia; tiletamine-zolazepam; flumazenil ID MIDAZOLAM; TELAZOL; WILD AB North American river otters (Lutra canadensis) were anesthetized with tiletamine-zolazepam or tiletamine-zolazepam-flumazenil combinations in cooperation with the North Carolina Wildlife Resources Commission Otter Restoration Project for evaluation of physiologic changes during anesthesia. Sixteen otters received tiletamine-zolazepam (4 mg/kg combined, i.m.) in 1994. Induction and recovery times were recorded and physiologic data (heart rate and rhythm, respiratory rate, rectal temperature, relative oxyhemoglobin saturation, and mean arterial blood pressure) were collected at 5-min intervals. Respiratory depression developed initially in all otters, and median relative oxyhemoglobin saturation remained below 90% for the first 15 min of anesthesia. Anesthetic induction with tiletamine-zolazepam was rapid and smooth, but recovery was prolonged (median = 89 min) and characterized by persistent head motion. In 1995, flumazenil was evaluated as a partial antagonist for tiletamine-zolazepam anesthesia in otters. Sixteen otters were anesthetized with tiletamine-zolazepam (4 mg/kg combined, i.m.) and given flumazenil (1 mg per 25 mg of zolazepam) after 20 min. Flumazenil markedly shortened recovery time in all otters anesthetized with tiletamine-zolazepam (median = 65 min) with no adverse effects. C1 N Carolina State Univ, Coll Vet Med, Environm Med Consortium, Raleigh, NC 27606 USA. N Carolina Wildlife Resources Commiss, Raleigh, NC 27604 USA. Wildlife Conservat Soc, Vet Field Program, Bronx, NY 10460 USA. RP Spelman, LH (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. NR 18 TC 19 Z9 19 U1 0 U2 4 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD DEC PY 1997 VL 28 IS 4 BP 418 EP 423 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA ZA013 UT WOS:000072319000009 PM 9523636 ER PT J AU Smith, BD AF Smith, BD TI Reconsidering the Ocampo caves and the era of incipient cultivation in Mesoamerica SO LATIN AMERICAN ANTIQUITY LA English DT Article ID NORTH-AMERICA; AMS DATES; MAIZE; CUCURBITACEAE; DOMESTICATION; REEVALUATION; AGRICULTURE; TEHUACAN; FARMERS; VALLEY C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 66 TC 32 Z9 32 U1 1 U2 2 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD DEC PY 1997 VL 8 IS 4 BP 342 EP 383 DI 10.2307/972107 PG 42 WC Archaeology SC Archaeology GA YQ793 UT WOS:000071423800004 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Building the Getty. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD DEC PY 1997 VL 122 IS 20 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA YL861 UT WOS:000071001200034 ER PT J AU de Forges, BR Jamieson, BGM Guinot, D Tudge, CC AF de Forges, BR Jamieson, BGM Guinot, D Tudge, CC TI Ultrastructure of the spermatozoa of Hymenosomatidae (Crustacea : Brachyura) and the relationships of the family SO MARINE BIOLOGY LA English DT Article ID CRABS CRUSTACEA; DECAPODA; HETEROTREMATA AB The spermatozoa of the genus Odiomaris Ng and Richer de Forges, 1996 (=Amarinus Lucas, 1980) have the components typical of eubrachyuran (Heterotremata + Thoracotremata) sperm, but differ significantly from all other investigated eubrachyurans in at least ten characteristics: (1) presence of an epiopercular dome; (2) separation of all but the central region of the operculum from the remainder of the acrosome by an infra-opercular rim; (3) the fact that the acrosome is smaller in volume than the nucleus; (4) the acrosome is strongly emergent from the nucleus, being surrounded only basally by nuclear material; (5) the cytoplasmic sheath, ending anteriorly with the nucleus, is also basal; (6) division of the acrosome contents into an inner and outer acrosome zone is scarcely apparent in longitudinal section as the inner zone is narrow and of doubtful homology; (7) the thin, putative inner acrosome zone is anteriorly almost septate owing to several longitudinal corrugations; (8) basally there is a unique "fringe zone"; (9) the acrosome, including the epinuclear dome, is longer than wide; (10) the unique helical and posterolateral disposition of the nuclear arms. From a purely spermatological viewpoint, Odiomaris (as exemplified by O. pilosus and O. estuarius), and provisionally the Hymenosomatidae, are thus excluded from the Thoracotremata, in which they were formerly placed, nor are they readily placeable in the Heterotremata. C1 Univ Queensland, Dept Zool, Brisbane, Qld 4072, Australia. ORSTOM, Noumea, New Caledonia. Museum Natl Hist Nat, Lab Zool Arthropodes, F-75231 Paris 05, France. Smithsonian Inst, Washington, DC 20560 USA. RP Jamieson, BGM (reprint author), Univ Queensland, Dept Zool, Brisbane, Qld 4072, Australia. NR 38 TC 11 Z9 11 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD DEC PY 1997 VL 130 IS 2 BP 233 EP 242 DI 10.1007/s002270050243 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA YQ927 UT WOS:000071438600012 ER PT J AU Thiel, M AF Thiel, M TI Reproductive biology of a filter-feeding amphipod, Leptocheirus pinguis, with extended parental care SO MARINE BIOLOGY LA English DT Article ID SCULPTA HOLMES CRUSTACEA; COROPHIUM-VOLUTATOR; ARTIFICIAL SPONGES; BORING AMPHIPOD; LIFE-HISTORY; AMPITHOIDAE; TANAIDACEA; BEHAVIOR; ECOLOGY; HABITAT AB Leptocheirus pinguis (Stimpson, 1853) is a widely distributed, abundant, endobenthic amphipod that engages in extended parental care, i.e. females host their juveniles in their burrows for extended time periods. I examined reproduction and population biology of L. pinguis at mean low water (MLW) in muddy sediment in Lowes Cove, Maine, USA. Cores around individual burrows were taken monthly in 1994 and 1995, and four seasonal samples were taken at different tidal heights. During the major reproductive periods in spring/early summer and in the fall, females produced several consecutive broods and hosted growing offspring in their burrows. Juveniles remained in their mothers' burrows until they reached a length of 5 mm (approximately one-third adult size) or more. At the study site, the majority of amphipods in individual burrows were adult females. Following the main reproductive periods, subadult individuals were found in their own burrows, but densities did not increase following the reproductive period in spring/early summer 1994, probably because large numbers of L. pinguis emigrated via the water column between June and December. L. pinguis is an annual species. Many members of the cohort born in spring/ early summer start reproducing in the fall, and survive until the following spring when they produce several broods. Members of the cohort born in the fall start reproducing the following spring and also produce several consecutive broods. Both the spring/early summer and fall cohorts die off after the major reproductive period in the following spring/early summer. High standing stocks of microphytobenthos occur in soft-bottoms at MLW, and I conclude that L. pinguis can engage in extended parental care there because its food is abundant year-round. The limited expandability and low stability of burrows in soft-bottoms at MLW do not permit long persistence of parent-offspring groups in L. pinguis. C1 Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. RP Thiel, M (reprint author), Smithsonian Marine Stn, 5612 Old Dixie Highway, Ft Pierce, FL 34946 USA. NR 50 TC 10 Z9 10 U1 0 U2 2 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD DEC PY 1997 VL 130 IS 2 BP 249 EP 258 DI 10.1007/s002270050245 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA YQ927 UT WOS:000071438600014 ER PT J AU Slikas, B AF Slikas, B TI Phylogeny of the avian family Ciconiidae (storks) based on cytochrome b sequences and DNA-DNA hybridization distances SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Review ID MITOCHONDRIAL-DNA; NUCLEOTIDE-SEQUENCES; WORLD VULTURES; MAJOR LINEAGES; EVOLUTION; TREES; GENE; MARSUPIALS; STABILITY; GENOME AB This study is a phylogenetic analysis of the avian family Ciconiidae, the storks, based on two molecular data sets: 1065 base pairs of sequence from the mitochondrial cytochrome b gene and a complete matrix of single-copy nuclear DNA-DNA hybridization distances. Sixteen of the nineteen stork species were included in the cytochrome b data matrix, and fifteen in the DNA-DNA hybridization matrix. Both matrices included outgroups from the families Cathartidae (New World vultures) and Threskiornithidae (ibises, spoonbills). Optimal trees based on the two data sets were congruent in those nodes with strong bootstrap support. In the best-fit tree based on DNA-DNA hybridization distances, nodes defining relationships among very recently diverged species had low bootstrap support, while nodes defining more distant relationships had strong bootstrap support. In the optimal trees based on the sequence data, nodes defining relationships among recently diverged species had strong bootstrap support, while nodes defining basal relationships in the family had weak support and were incongruent among analyses. A combinable-component consensus of the best-fit DNA-DNA hybridization tree and a consensus tree based on different analyses of the cytochrome b sequences provide the best estimate of relationships among stork species based on the two data sets. (C) 1997 Academic Press. C1 Acad Nat Sci Philadelphia, Philadelphia, PA 19103 USA. Univ Penn, Dept Biol, Leidy Labs, Philadelphia, PA 19104 USA. RP Slikas, B (reprint author), Smithsonian Inst, Natl Zool Pk, Genet Mol Lab, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Slikas, Beth/E-7275-2013 NR 104 TC 33 Z9 38 U1 0 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD DEC PY 1997 VL 8 IS 3 BP 275 EP 300 DI 10.1006/mpev.1997.0431 PG 26 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA YL946 UT WOS:000071011300001 PM 9417889 ER PT J AU Brandt, WN Mathur, S Reynolds, CS Elvis, M AF Brandt, WN Mathur, S Reynolds, CS Elvis, M TI X-ray absorption by ionized oxygen in ASCA spectra of the infrared quasar IRAS 13349+2438 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies, active; galaxies, individual, IRAS 13349+2438; X-rays, galaxies ID LINE SEYFERT-1 GALAXIES; ACTIVE GALACTIC NUCLEI; DUST GRAINS; HOT GAS; ABSORBER; PHYSICS AB We present evidence for X-ray absorption by ionized oxygen in ASCA spectra of the prototype infrared quasar IRAS 13349+2438, This powerful (L-bol greater than or similar to 2 x 10(46) erg s(-1)) quasar was studied in detail with ROSAT, and the combination of the X-ray data and optical/near-infrared spectropolarimetry strongly suggested the presence of a dusty ionized ('warm') absorber along the line of sight to the central X-ray source, The ASCA spectra, in contrast to an earlier claim, show evidence for ionized oxygen edges, and the presence of such edges appears to provide the most physically plausible interpretation of the data. Thus, the ASCA spectra support the dusty warm absorber hypothesis. The ASCA data also allow the physical properties of the warm absorber to be constrained far better than before, A one-zone warm absorber model indicates the ionized column to be in the range (2-6) x 10(21) cm(-2), and it gives an ionization parameter of xi = 31(-12)(+12) erg cm s(-1). The dusty warm absorber appears to have a density of less than or similar to 3 x 10(8) cm(-3), and it is probably located outside the broad-line region. The dust in the warm absorber cm does not appear to have been heavily sputtered or destroyed via other means. Based on the ASCA fitting, we suggest that ultraviolet absorption lines from the warm absorber may be detectable and discuss how they can be used to further constrain the warm absorber properties, We compare and contrast the X-ray properties of IRAS 13349+2438 with those of broad absorption line quasars, We comment on the steep > 2 keV continuum of IRAS 13349+2438 and examine the relevance to some models of radiative Fe II formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. 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 40 TC 36 Z9 36 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 1997 VL 292 IS 2 BP 407 EP 413 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL833 UT WOS:000070998400020 ER PT J AU White, DA Jones, C Forman, W AF White, DA Jones, C Forman, W TI An investigation of cooling flows and general cluster properties from an X-ray image deprojection analysis of 207 clusters of galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; galaxies, clusters, general; cooling flows; galaxies, fundamental parameters; intergalactic medium; X-rays, galaxies ID VELOCITY DISPERSIONS; RICH CLUSTERS; ABELL CLUSTERS; RADIO-SOURCES; EXOSAT OBSERVATIONS; ABSORBING MATTER; COMPLETE SAMPLE; POOR CLUSTERS; EMITTING GAS; REDSHIFTS AB In this paper we present an X-ray image deprojection analysis of Einstein Observatory imaging data on 207 clusters of galaxies. The resulting radial profiles for luminosity, temperature and electron density variations are determined from the cluster surface-brightness profiles according to gravitational potential constraints from average X-ray temperatures and optical velocity dispersions. This enables us to determine cooling flow and other cluster properties, such as baryon fractions, Sunyaev-Zel'dovich microwave decrements and Thomson depths. From the results we have compiled a catalogue of the detected cooling flows, and investigated their effects on general cluster properties. To assist in the analysis, we have constructed self-consistent correlations between the cluster X-ray luminosity, temperature and optical velocity dispersion, using 'orthogonal distance' regression to account for errors in both dimensions of the data. These fits indicate that, in general, the temperatures of clusters are isothermal, and that they have spectral p-values consistent with unity (if the dependence of luminosity on temperature is assumed to be quadratic). We find that the X-ray luminosity, temperature and optical velocity dispersion relations depend significantly on the cooling flow mass-deposition rate, through characteristic differences in the density profiles. Clusters of similar cooling flow mass-deposition rate exhibit self-similar density profiles, with larger cooling flows showing higher central densities. This leads to scatter in the luminosity-related correlations within the X-ray luminosity, temperature and optical velocity dispersion plane. The segregation in density also leads to dispersion in other related properties such as 'half-light radii' and baryon fractions. The baryon fraction in the cores of cooling flow clusters appears to be higher, but as the density profiles tend to a similar value at larger radii, irrespective of cooling flow property, so too do the baryon fraction profiles appear to rise to a concordant value of greater than 10 per cent at 1 Mpc. Thus this sample indicates that clusters, as a whole, are inconsistent with primordial nucleosynthesis baryon fraction prediction, for a flat universe, of 6 per cent. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP White, DA (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM daw@ast.cam.ac.uk NR 68 TC 369 Z9 370 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 1997 VL 292 IS 2 BP 419 EP 467 PG 49 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YL833 UT WOS:000070998400022 ER PT J AU Losos, JB de Queiroz, K AF Losos, JB de Queiroz, K TI Darwin's lizards SO NATURAL HISTORY LA English DT Article C1 Washington Univ, St Louis, MO 63130 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Vertebrate Zool, Washington, DC 20560 USA. Smithsonian Inst, Museum Natl Hist Nat, Div Amphibians & Reptiles, Washington, DC 20560 USA. RP Losos, JB (reprint author), Washington Univ, St Louis, MO 63130 USA. NR 0 TC 1 Z9 1 U1 0 U2 3 PU AMER MUSEUM NAT HISTORY PI NEW YORK PA ATTN: LIBRARY SERIALS UNIT CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0028-0712 J9 NAT HIST JI Nat. Hist. PD DEC PY 1997 VL 106 IS 11 BP 34 EP 39 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA ZA510 UT WOS:000072370500014 ER PT J AU Skog, LE Kvist, LP AF Skog, LE Kvist, LP TI Novae Gesneriaceae Neotropicarum VII: New combinations SO NOVON LA English DT Article AB Study of Gesneriaceae for the Flora of Ecuador and the Catalogue of the Vascular Plants of Ecuador has shown that some recently published new species need to be transferred with new combinations in Columnea: C. filifera, C. katzensteinii, C. mastersonii, C. medicinalis, C. ornata, and C. tandapiana, or included as synonyms of previously published species. C1 Smithsonian Inst, US Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Royal Vet & Agr Univ, Unit Forestry, DK-1871 Copenhagen C, Denmark. RP Skog, LE (reprint author), Smithsonian Inst, US Natl Museum Nat Hist, Dept Bot, NHB-166, Washington, DC 20560 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD WIN PY 1997 VL 7 IS 4 BP 413 EP 416 DI 10.2307/3391774 PG 4 WC Plant Sciences SC Plant Sciences GA YR962 UT WOS:000071549600019 ER PT J AU Weitzmann, AL Skog, LE Wang, WT Pan, KY Li, ZY AF Weitzmann, AL Skog, LE Wang, WT Pan, KY Li, ZY TI New taxa, new combinations, and notes on Chinese Gesneriaceae SO NOVON LA English DT Article AB Preparation of the Gesneriaceae for the Flora of China has revealed new taxa, including one new genus, Paraisometrum; thirteen new species, Chirita atroglandulosa, C. napoensis, C. pungentisepala, C. pycnantha, C. shouchengensis, C. shuii, C. skogiana, C. wangiana, Didymocarpus subpalmatinervis, Hemiboea wangiana, Opithandra burttii, Oreocharis dentata, Paraisometrum mileense; and seven new combinations, Chirita demissa, Hemiboea subcapitata var. guangdongensis, Lysionotus microphyllus var. omeiensis, Lysionotus pauciflorus var. ikedae, Oreocharis aurea var. cordato-ovata, Paraboea glutinosa, and Tengia scopulorum var. potiflora. The new taxa are described, discussed, and compared with related taxa. The transfer and status changes are justified. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Chinese Acad Sci, Inst Bot, Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. RP Weitzmann, AL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC-166, Washington, DC 20560 USA. NR 7 TC 14 Z9 19 U1 1 U2 5 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD WIN PY 1997 VL 7 IS 4 BP 423 EP 435 DI 10.2307/3391777 PG 13 WC Plant Sciences SC Plant Sciences GA YR962 UT WOS:000071549600022 ER PT J AU Huber, BT Bijma, J Darling, K AF Huber, BT Bijma, J Darling, K TI Cryptic speciation in the living planktonic foraminifer Globigerinella siphonifera (d'Orbigny) SO PALEOBIOLOGY LA English DT Article ID SACCULIFER BRADY; GLOBOROTALIA FOHSELLA; EQUATORIAL PACIFIC; CLADE GLOBOCONELLA; LINEAGE; EVOLUTION; OXYGEN; TESTS; SEA; AEQUILATERALIS AB Two living forms of Globigerinella siphonifera (d'Orbigny), presently identified as Type I and Type II, can easily be distinguished and collected by SCUBA divers because of differences in appearance, arrangement of the rhizopodial network, and the presence or absence of commensals. Additional biological differences are apparent from laboratory culture experiments; Type I individuals survive significantly longer than Type II under conditions of darkness and starvation and have significantly slower chamber formation rates. Stable isotopic analyses of Types I and II also reveal notable differences, with Type I consistently yielding more negative delta(18)O and delta(13)C values. Results of Mg/Ca ratio analyses indicate that Type II specimens precipitated their shells in slightly cooler (deeper) surface waters than Type I specimens. These observations and results from DNA sequencing unequivocally demonstrate that G. siphonifera Types I and II should be regarded as biological sister species. Contrarily, biometric analysis of the empty shells reveals few significant differences between G. siphonifera Types I and II. Of all the features measured from X-ray and SEM images of serially dissected specimens, only shell porosity yields readily discernible differences, with Type I adult chambers averaging 10-20% porosity and Type II adult chambers averaging 4-7% porosity. Statistically significant differences between Type I and II populations are revealed in maximum test diameter (Type I is typically larger) and coiling (Type I is typically more evolute), but these differences do not justify species level distinction of Types I and II using traditional paleontological species concepts. On the basis of the above evidence, and since all specimens were collected at the same location at similar to 3-8 m water depth, we conclude that G. siphonifera Types I and II are living examples of cryptic speciation, whereby biological speciation has occurred in the absence of discernable change in shell morphology. However, it is not clear when or where this speciation took place. Preliminary study of deep-sea cores from the Caribbean and Pacific sides of the Isthmus of Panama reveals a predominance of specimens with Type II porosity values, with rare occurrence of specimens yielding Type I porosity values. Systematic downcore measurement of shell porosity and tightness of coiling needs to be extended back to the middle Miocene, when G. siphonifera first appeared, to determine the timing of the Type I and II morphological divergence. Postulated mechanisms for reproductive isolation and speciation of Types I and II include alloparapatric, depth parapatric, and sympatric speciation. These models could be tested if further analysis of fossil G. siphonifera shells allows determination of the timing of speciation, the preferred depth distribution, and the history of geographic distribution of Types I and II. C1 ALFRED WEGENER INST POLAR & MARINE RES,D-2850 BREMERHAVEN,GERMANY. UNIV EDINBURGH,GRANT INST GEOL,DEPT GEOL & GEOPHYS,EDINBURGH EH9 3JW,MIDLOTHIAN,SCOTLAND. RP Huber, BT (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,MRC NHB 121,WASHINGTON,DC 20560, USA. OI Bijma, Jelle/0000-0003-4371-1438 NR 79 TC 111 Z9 116 U1 1 U2 3 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD WIN PY 1997 VL 23 IS 1 BP 33 EP 62 PG 30 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA WU577 UT WOS:A1997WU57700003 ER PT J AU Wagner, PJ AF Wagner, PJ TI Patterns of morphologic diversification among the Rostroconchia SO PALEOBIOLOGY LA English DT Review ID PHYLOGENETIC ANALYSIS; CONFIDENCE-INTERVALS; EVOLUTIONARY RATES; MASS EXTINCTION; FOSSIL RECORD; DIVERSITY; DISPARITY; TESTS; DNA; MORPHOSPACE AB Morphologic diversification among rostroconch molluscs is explored using multiple phylogenies derived from different methods. In addition to strict parsimony, phylogenetic estimates were derived using four different methods that employ stratigraphic data. The resultant phylogenies are generally very similar to one another and to the phylogeny proposed by Pojeta and Runnegar (1976). All estimates (including the Pojeta and Runnegar estimate) imply much lower morphologic separations among post-Ordovician rostroconchs (measured here as the frequency of character state change per branch) than among Cambro-Ordovician rostroconhs. However, the data do not suggest that morphologic evolution became more constrained among rostroconchs as a whole, but instead suggest a reduced characteristic rate of morphologic change in the clade that happened to survive the end-Ordovician extinction. Likelihood ratio tests provide strongest support for the hypothesis that morphologic evolution was more constrained within a derived subclade (corresponding to previous definitions of the Conocardioidea, minus the Eopteriidae) than it was in a broad paraphylum (corresponding to the Ribeirioidea + Eopteriidae). Estimates from each of the phylogenetic methods lead to the same conclusions. Various metrics indicate that the pattern is not due to poor sampling of Cambro-Ordovician species and thus merits a biological explanation. Nonphylogenetic analyses of morphologic disparity suggest a similar history of morphologic evolution, including the apparent difference in characteristic rates of morphologic evolution between paraclade and subclade. C1 SMITHSONIAN INST,DEPT PALEOBIOL,MRC 121,WASHINGTON,DC 20560. RI Wagner, Peter/A-5514-2009 OI Wagner, Peter/0000-0002-9083-9787 NR 108 TC 80 Z9 81 U1 0 U2 6 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD WIN PY 1997 VL 23 IS 1 BP 115 EP 150 PG 36 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA WU577 UT WOS:A1997WU57700007 ER PT J AU Korobov, VI Shimamura, I AF Korobov, VI Shimamura, I TI Auger transition rates for metastable states of antiprotonic helium He+(p)over-bar SO PHYSICAL REVIEW A LA English DT Article ID ATOMS; V=N-L-1=2 AB The rates of Auger transitions of antiprotonic helium He-4(+)(p) over bar and He-3(+)(p) over bar are calculated by using a variational scattering method with an elaborate three-body trial function. The shift of the energy levels of these systems due to the coupling with the Auger-decay channels is also obtained from this calculation. Thus an improvement is made over the previously calculated nonrelativistic energies. Together with the relativistic corrections calculated elsewhere, the theoretical transition wavelength between the states (n,l)=(37,34) and (38,33) of H-4(+)(p) over bar, for example, is significantly improved to be 713.593 nm, which compares well with the experimental value 713.578+/-0.006 nm. The calculated Auger lifetime of the level (38,33) is 3.2 ps, as compared with the value 4.1+/-0.2 ps deduced from the measured line broadening. Auger rates are calculated also using Fermi's golden-rule formula with a regular Coulomb function with no phase shift for the Auger electron. The results agree fairly well with the accurate variational results. [S1050-2947(97)05912-X]. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOL PHYS, CAMBRIDGE, MA 02138 USA. RP Korobov, VI (reprint author), RIKEN, INST PHYS & CHEM RES, WAKO, SAITAMA 35101, JAPAN. RI Korobov, Vladimir/D-7849-2013 OI Korobov, Vladimir/0000-0003-3724-0270 NR 26 TC 57 Z9 58 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD DEC PY 1997 VL 56 IS 6 BP 4587 EP 4594 DI 10.1103/PhysRevA.56.4587 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA YK233 UT WOS:A1997YK23300035 ER PT J AU Kerman, AK Tommasini, P AF Kerman, AK Tommasini, P TI Gaussian time-dependent variational principle for bosons: Contact interaction in one dimension SO PHYSICAL REVIEW B LA English DT Article ID BOSE-EINSTEIN CONDENSATION; GAS; ATOMS AB We investigate the Dirac time-dependent variational method using a Gaussian trial functional for an infinite one-dimensional system of bosons interacting through a repulsive contact interaction. The method produces a set of nonlinear time-dependent equations for the variational parameters. By solving the static equations we have calculated the ground state energy per particle. We have also considered small oscillations about the equilibrium and obtain mode equations which lead us to a gapless dispersion relation. The existence of an exact numerical solution for the ground-state energy and excitations obtained by Lieb allow us to compare with the Gaussian results. We can also, as the system becomes less dilute, see the improvement of the results as compared with the Bogoliubov scheme. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. RP Kerman, AK (reprint author), MIT,CTR THEORET PHYS,NUCL SCI LAB,CAMBRIDGE,MA 02139, USA. NR 24 TC 4 Z9 4 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0163-1829 J9 PHYS REV B JI Phys. Rev. B PD DEC 1 PY 1997 VL 56 IS 22 BP 14733 EP 14744 DI 10.1103/PhysRevB.56.14733 PG 12 WC Physics, Condensed Matter SC Physics GA YL011 UT WOS:A1997YL01100075 ER PT J AU Heyman, IM AF Heyman, IM TI Smithsonian official tells why Enola Gay exhibit was shot down SO PHYSICS TODAY LA English DT Letter RP Heyman, IM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD DEC PY 1997 VL 50 IS 12 BP 96 EP 96 DI 10.1063/1.882042 PG 1 WC Physics, Multidisciplinary SC Physics GA YJ169 UT WOS:A1997YJ16900032 ER PT J AU Mader, JA Shafter, AW AF Mader, JA Shafter, AW TI A photometric study of the peculiar binary star V Sagittae SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID CLOSE BINARIES; MASS-TRANSFER; LIGHT; EVOLUTION; ECLIPSE; CURVES AB High-speed photometric UBV observations of the novalike variable V Sagittae conducted during 1994 and 1995 are reported. The data consist of a total of 152 hr of observations, covering the entire 12.3 hr orbital period. Analysis of the photometry using the new Wilson eclipsing-binary code suggests a model where mass is being transferred from a 0.86 M., evolved, helium-burning star, which fills its Roche lobe, to a 3.48 M. evolved companion. Thirteen new timings of primary eclipse in conjunction with published timings from 1946 to 1996 show that the orbital period is changing at a rate (P) OVER DOT = -5.1(+/-1.0) x 10(-10). We derive a lower limit to the mass-loss rate from the primary star of (M) OVER DOT (1) similar to 4.4(+/-0.1) x 10(-7) M. yr(-1). V Sge appears to be in a short-lived evolutionary state with a lifetime of similar to 2 x 10(6) yr. C1 San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Mader, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 12 Z9 12 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 1997 VL 109 IS 742 BP 1351 EP 1358 DI 10.1086/134015 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YM430 UT WOS:000071062700005 ER PT J AU Kalogera, V AF Kalogera, V TI Formation of low-mass X-ray binaries SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Kalogera, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 6 Z9 6 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 1997 VL 109 IS 742 BP 1394 EP 1394 DI 10.1086/134019 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YM430 UT WOS:000071062700009 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The Columbia encyclopedia on CD-ROM. SO REFERENCE & USER SERVICES QUARTERLY LA English DT Software Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER LIBRARY ASSOC PI CHICAGO PA 50 E HURON ST, CHICAGO, IL 60611 USA SN 1094-9054 J9 REF USER SERV Q JI Ref. User Serv. Q. PD WIN PY 1997 VL 37 IS 2 BP 200 EP 200 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA ZT090 UT WOS:000074047400010 ER PT J AU Maddison, DR Swofford, DL Maddison, WP AF Maddison, DR Swofford, DL Maddison, WP TI Nexus: An extensible file format for systematic information SO SYSTEMATIC BIOLOGY LA English DT Article DE computer program; file format; NEXUS; systematics ID EVOLUTION; TREE AB NEXUS is a file format designed to contain systematic data for use by computer programs. The goals of the format are to allow future expansion, to include diverse kinds of information, to be independent of particular computer operating systems, and to be easily processed by a program. To this end, the format is modular, with a file consisting of separate blocks, each containing one particular kind of information, and consisting of standardized commands. Public blocks (those containing information utilized by several programs) house information about taxa, morphological and molecular characters, distances, genetic codes, assumptions, sets, trees, etc.; private blocks contain information of relevance to single programs. A detailed description of commands in public blocks is given. Guidelines are provided for reading and writing NEXUS files and for extending the format. C1 Univ Arizona, Dept Entomol, Tucson, AZ 85721 USA. Smithsonian Inst, Lab Mol Systemat, MSC, Washington, DC 20560 USA. Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. RP Maddison, DR (reprint author), Univ Arizona, Dept Entomol, Tucson, AZ 85721 USA. NR 18 TC 242 Z9 249 U1 1 U2 11 PU TAYLOR & FRANCIS LTD PI LONDON PA ONE GUNPOWDER SQUARE, LONDON EC4A 3DE, ENGLAND SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD DEC PY 1997 VL 46 IS 4 BP 590 EP 621 DI 10.2307/2413497 PG 32 WC Evolutionary Biology SC Evolutionary Biology GA YX756 UT WOS:000072074100002 PM 11975335 ER PT J AU Wcislo, WT Danforth, BN AF Wcislo, WT Danforth, BN TI Secondarily solitary: the evolutionary loss of social behavior SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID PHYLOGENETIC APPROACH; APHELOCOMA JAYS; HYMENOPTERA; HALICTIDAE; RECONSTRUCTION; POPULATION; BIRDS; BEES AB Studies of social behaviour frequently assume that evolution proceeds from a solitary state to a social one, and that social lineages give rise to lineages that are also social, excluding parasitic taxa. Recent phylogenetic studies of some bees contradict this assumption, and more examples are known or hypothesized in other animals. Social behavior can be lost to give rise to species that are secondarily solitary. Studies of the conditions that lead to the suppression or loss of social behavior can help to illuminate those factors that lead to its origins and maintenance. C1 CORNELL UNIV,DEPT ENTOMOL,ITHACA,NY 14853. RP Wcislo, WT (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO,AA 34002, USA. NR 56 TC 105 Z9 110 U1 6 U2 40 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 DEC PY 1997 VL 12 IS 12 BP 468 EP 474 DI 10.1016/S0169-5347(97)01198-1 PG 7 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA YG725 UT WOS:A1997YG72500007 PM 21238162 ER PT J AU Glade, WP Tavis, LA AF Glade, WP Tavis, LA TI Actualizing the developmental response of multinational corporations: The case of agribusiness in the Mexican countryside SO UNIVERSITY OF PENNSYLVANIA JOURNAL OF INTERNATIONAL ECONOMIC LAW LA English DT Article; Proceedings Paper CT Law and Ethics in Emerging Markets Symposium CY MAY, 1997 CL UNIV PENN, WHARTON SCH, PHILADELPHIA, PENNSYLVANIA HO UNIV PENN, WHARTON SCH C1 Univ Texas, Inst Latin Amer Studies, Mexican Ctr, Austin, TX 78712 USA. Smithsonian Inst, Woodrow Wilson Int Ctr Scholars, Washington, DC 20560 USA. RP Glade, WP (reprint author), Univ Texas, Inst Latin Amer Studies, Mexican Ctr, Austin, TX 78712 USA. NR 43 TC 0 Z9 0 U1 0 U2 0 PU UNIV PENN LAW SCH PI PHILADELPHIA PA 3400 CHESTNUT ST, PHILADELPHIA, PA 19104-6204 USA SN 1086-7872 J9 U PA J INT ECON LAW JI Univ. Pa. J. Int. Econ. Law PD WIN PY 1997 VL 18 IS 4 BP 1211 EP 1234 PG 24 WC Law SC Government & Law GA YV545 UT WOS:000071835800005 ER PT J AU Balakrishnan, N Forrey, RC Dalgarno, A AF Balakrishnan, N Forrey, RC Dalgarno, A TI Threshold phenomena in ultracold atom-molecule collisions SO CHEMICAL PHYSICS LETTERS LA English DT Article ID INDUCED VIBRATIONAL-RELAXATION; RATES; SCATTERING; BEHAVIOR AB Vibrational relaxation cross sections for an atom-molecule collision are calculated by explicit numerical solution of the coupled equations of scattering theory and shown to follow an inverse velocity dependence at very low initial kinetic energies of the incident atom, in accordance with Wigner's threshold law. Rate constants for H + H-2 (upsilon, j = 0) --> H + H-2(upsilon') < upsilon, j = 0) are calculated for all the vibrational levels of H-2 and found to vary by seven orders of magnitude between the deepest level upsilon = 0 and the vibrational level upsilon = 12. (C) 1997 Elsevier Science B.V. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Balakrishnan, N (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 63 Z9 64 U1 2 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD NOV 28 PY 1997 VL 280 IS 1-2 BP 1 EP 4 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA YN622 UT WOS:000071188400001 ER PT J AU Balakrishnan, N Kharchenko, V Forrey, RC Dalgarno, A AF Balakrishnan, N Kharchenko, V Forrey, RC Dalgarno, A TI Complex scattering lengths in multi-channel atom-molecule collisions SO CHEMICAL PHYSICS LETTERS LA English DT Article ID LASER AB It is shown that in the presence of inelastic scattering, zero energy elastic and inelastic scattering can be characterized by a complex scattering length, the imaginary part of which is related directly to the total inelastic scattering cross section. Collisions between H atoms and vibrationally excited H-2, molecules are investigated. Zero energy cross sections for all vibrational states of H-2 and the corresponding complex scattering lengths are reported using accurate quantum mechanical calculations. We obtain large values of the elastic cross sections which we attribute to s-wave bound and quasi-bound states of H ... H-2(v). The energies and lifetimes of the quasi-bound states are extracted from the complex scattering lengths. (C) 1997 Elsevier Science B.V. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Balakrishnan, N (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 93 Z9 94 U1 0 U2 6 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 NOV 28 PY 1997 VL 280 IS 1-2 BP 5 EP 9 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA YN622 UT WOS:000071188400002 ER PT J AU Behrensmeyer, AK Todd, NE Potts, R McBrinn, GE AF Behrensmeyer, AK Todd, NE Potts, R McBrinn, GE TI Late Pliocene faunal turnover in the Turkana Basin, Kenya and Ethiopia SO SCIENCE LA English DT Article ID PLIOPLEISTOCENE AB Analysis of a large sample of well-dated fossil mammals from localities in tl-e Turkana Basin of Kenya and Ethiopia revealed sampling biases that affect patterns of faunal turnover during the late Pliocene, When these biases were accounted for, results indicated that 58 to 77 percent of the mammal species were replaced between 3.0 and 1.8 million years ago (Ma), Overall diversity increased from 3.0 to 2.0 Ma but then declined. No distinct turnover pulse is seen between 2.8 and 2.5 Ma; instead, the most significant period of faunal change began after 2.5 Ma and continued through 1.8 Ma. C1 SMITHSONIAN INST,MUSEUM NATL HIST NAT,NHB MRC 121,EVOLUT TERR ECOSYST PROGRAM,WASHINGTON,DC 20560. NR 56 TC 142 Z9 144 U1 0 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD NOV 28 PY 1997 VL 278 IS 5343 BP 1589 EP 1594 DI 10.1126/science.278.5343.1589 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA YJ874 UT WOS:A1997YJ87400030 ER PT J AU Zhu, L Suto, K Fiss, JA Wada, R Seideman, T Gordon, RJ AF Zhu, L Suto, K Fiss, JA Wada, R Seideman, T Gordon, RJ TI Effect of resonances on the coherent control of the photoionization and photodissociation of HI and DI SO PHYSICAL REVIEW LETTERS LA English DT Article ID LASER CONTROL; HIGH-RESOLUTION; AUTOIONIZATION; PHASE; EXCITATION; IONIZATION AB The phase lag between the ionization and dissociation products of HI and DI molecules obtained by one- and three-photon excitation was measured as a function of excitation energy in the vicinity of a molecular resonance. The phase lag was observed to have an asymmetric profile with a deep minimum near the center of the resonance. A strong isotope effect was also observed. A theoretical analysis, using projection operators to partition the Lippmann-Schwinger equation, showed that a molecular phase is responsible for the energy dependence of the phase lag. C1 KYOTO UNIV,DEPT MOL ENGN,KYOTO 60601,JAPAN. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. NATL RES COUNCIL CANADA,STEACIE INST MOL SCI,OTTAWA,ON K1A 0R6,CANADA. RP Zhu, L (reprint author), UNIV ILLINOIS,DEPT CHEM MC 111,845 W TAYLOR ST,CHICAGO,IL 60607, USA. NR 23 TC 100 Z9 100 U1 1 U2 7 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD NOV 24 PY 1997 VL 79 IS 21 BP 4108 EP 4111 DI 10.1103/PhysRevLett.79.4108 PG 4 WC Physics, Multidisciplinary SC Physics GA YH018 UT WOS:A1997YH01800016 ER PT J AU Stibbe, DT Tennyson, J AF Stibbe, DT Tennyson, J TI Ab initio calculations of vibrationally resolved resonances in electron collisions with H-2, HD, and D-2 SO PHYSICAL REVIEW LETTERS LA English DT Article ID MOLECULAR-HYDROGEN; DIATOMIC-MOLECULES; EXCITATION; THRESHOLD; IMPACT; STATES; H2 AB Adiabatic R-matrix scattering calculations for vibrationally resolved resonance series a, b, and c are presented and compared with experimental studies for e-H-2, e-D-2, and e-HD. The excellent agreement allows a complete theoretical explanation of the series from which definitive assignments of parentage and symmetry can be made. It also explains the long-standing disagreements among and between previous theoretical and experimental results. More generally, these results provide the first corroboration of the idea of multiple parent states and parent state swapping of Feshbach-type resonances in molecules. C1 UCL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. RP 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 28 TC 23 Z9 23 U1 2 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD NOV 24 PY 1997 VL 79 IS 21 BP 4116 EP 4119 DI 10.1103/PhysRevLett.79.4116 PG 4 WC Physics, Multidisciplinary SC Physics GA YH018 UT WOS:A1997YH01800018 ER PT J AU Seideman, T Guo, H AF Seideman, T Guo, H TI Theory of desorption induced by electronic transitions .2. The strong interaction regime SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID LASER-INDUCED DESORPTION; STIMULATED DESORPTION; SURFACE PHOTOCHEMISTRY; STATE DISTRIBUTIONS; MEDIATED PHOTODESORPTION; VIBRATIONAL-EXCITATION; ENERGY DISTRIBUTIONS; METAL-SURFACES; QUANTUM-THEORY; WAVE-PACKET AB The dynamics of desorption induced by electronic transitions is studied using a recently formulated quantum mechanical method [J. Chem. Phys. 106, 417 (1997)]. We consider two qualitatively different model Hamiltonians representing the limits of desorption induced by a single and by multiple electronic transitions and at the same time the limits of resonance-mediated and direct nuclear dynamics. The photodesorption probability of NH3/Cu induced by low-intensity, nanosecond pulses is dominated by a resonant component and determined by the competition of desorption with vibrational relaxation. The probability is linear in the excitation intensity but highly nonlinear in the nonradiative coupling. The photodesorption of NO/Pd induced by intense, femtosecond pulses involves complex electronic dynamics and its vibrational dynamics is mostly direct. Multiple transitions to an ionic state are shown formally and numerically. These give rise to several thresholds in the time-resolved desorption probability. A power-law fluence dependence is found, consistent with observations. (C) 1997 American Institute of Physics. [S0021-9606(97)01244-0]. C1 NATL RES COUNCIL CANADA,STEACIE INST,OTTAWA,ON K1A 0R6,CANADA. HARVARD UNIV,HARVARD SMITHSONIAN CTR,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. UNIV TOLEDO,DEPT CHEM,TOLEDO,OH 43606. RI Guo, Hua/J-2685-2014 OI Guo, Hua/0000-0001-9901-053X NR 80 TC 11 Z9 11 U1 2 U2 6 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 22 PY 1997 VL 107 IS 20 BP 8627 EP 8636 DI 10.1063/1.475015 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA YG958 UT WOS:A1997YG95800044 ER PT J AU Wuethrich, B AF Wuethrich, B TI Paleontology - Will fossil from down under upend mammal evolution? SO SCIENCE LA English DT Editorial Material RP Wuethrich, B (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560, USA. NR 0 TC 4 Z9 4 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD NOV 21 PY 1997 VL 278 IS 5342 BP 1401 EP 1402 DI 10.1126/science.278.5342.1401 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA YG858 UT WOS:A1997YG85800020 ER PT J AU Stancil, PC Dalgarno, A AF Stancil, PC Dalgarno, A TI The radiative association of H and D SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; early universe ID MOLECULE; ENERGIES; SPECTRUM; HYDROGEN; LINE; H-2 AB The formation of the deuterated hydrogen molecule HD by the radiative association of H and D is investigated. Spontaneous association and stimulated association in a blackbody radiation field are considered. For a collision temperature of 1000 K, the rate coefficient for spontaneous radiative association is 1.0 x 10(-26) cm(3) s(-1). At the same collision temperature, the rate coefficient is enhanced by stimulated association to 1.8 x 10(-26) cm(3) s(-1) for a radiation temperature of 10,000 K. The role of radiative association in the deuterium chemistry of the early universe is discussed. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Stancil, PC (reprint author), OAK RIDGE NATL LAB,DIV PHYS,POB 2008,OAK RIDGE,TN 37831, USA. NR 18 TC 26 Z9 26 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 NOV 20 PY 1997 VL 490 IS 1 BP 76 EP 78 DI 10.1086/304878 PN 1 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YG999 UT WOS:A1997YG99900009 ER PT J AU Lazarian, A Goodman, AA Myers, PC AF Lazarian, A Goodman, AA Myers, PC TI On the efficiency of grain alignment in dark clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM, clouds; polarization ID INTERSTELLAR DUST PARTICLES; CROSS-SECTION ALIGNMENT; INTER-STELLAR GRAINS; MAGNETIC-FIELD; MOLECULAR CLOUDS; SUPRATHERMAL ROTATION; INFRARED POLARIMETRY; MECHANICAL ALIGNMENT; SIZE DISTRIBUTION; POLARIZATION AB A quantitative analysis of grain alignment in the filamentary dark cloud L1755 in Ophiuchus is presented. We show that the observed decrease of the polarization-to-extinction ratio for the inner parts of this quiescent dark cloud can be explained as a result of the decrease of the efficiency of grain alignment. We make quantitative estimates of grain alignment efficiency for six mechanisms involving grains with either thermal or suprathermal rotation, interacting with either magnetic field or gaseous how. We also make semiquantitative estimates of grain alignment by radiative torques. We show that in conditions typical of dark cloud interiors, all known major mechanisms of grain alignment fail. All the studied mechanisms predict polarization at least an order of magnitude below the currently detectable levels of similar to 1%. On the contrary, in the dark cloud environments where A(v) <1, the grain alignment can be much more efficient. There the alignment of suprathermally rotating grains with superparamagnetic inclusions, and possibly also radiative torques, account for observed polarization. These results apply to L1755, which we model in detail, and probably also to B216 and other similar dark clouds. Our study suggests an explanation for the difference in results obtained through polarimetry of background starlight and polarized thermal emission from the dust itself. We conjecture that the emission polarimetry selectively reveals aligned grains in the environment far from thermodynamic equilibrium, as opposed to starlight polarization studies that probe the alignment of grains all the way along the line of sight, including the interiors of dark quiescent clouds, where no alignment is possible. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. HARVARD UNIV, DEPT ASTRON, CAMBRIDGE, MA 02138 USA. RP Lazarian, A (reprint author), PRINCETON UNIV OBSERV, PEYTON HALL, PRINCETON, NJ 08544 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 73 TC 105 Z9 105 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 NOV 20 PY 1997 VL 490 IS 1 BP 273 EP 280 DI 10.1086/304874 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YG999 UT WOS:A1997YG99900029 ER PT J AU Vrtilek, SD Boroson, B Cheng, FH McCray, R Nagase, F AF Vrtilek, SD Boroson, B Cheng, FH McCray, R Nagase, F TI Simultaneous Hubble Space Telescope and ASCA observations of LMC X-4: X-ray ionization effects on a stellar wind SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries, eclipsing; pulsars, individual (LMC X-4); stars, mass loss; stars, neutron ID ROSAT OBSERVATIONS; HZ-HERCULIS; PERIODICITY; DISCOVERY; LMC-X-4; HERCULES-X-1; SPECTROSCOPY; PULSATIONS; PRECESSION; DISKS AB We present first results from simultaneous ultraviolet (HST/GHRS) and X-ray (ASCA) observations of the 13.5 s pulsar LMC X-4, taken in 1996 May. The ASCA observations covered 1.12 binary orbits (1.58 days), and the Hubble Space Telescope observations were centered on this for roughly 0.4 orbital phase coverage (0.56 days). The Goddard High Resolution Spectograph data are the highest resolution (both temporal and spectral) ultraviolet spectra ever taken of LMC X-4. With generally accepted parameters for the source, fits to the UV continuum, using a model that incorporates X-ray heating of the companion star and the accretion disk, yield a mass accretion rate (M) over dot = 4.0 x 10(-8) M-. yr(-1); the X-ray luminosity implied by this value is consistent with the X-ray flux measured during simultaneous observations (3.2 x 10(-10) ergs cm(-2) s(-1)). The model accurately predicts observed B-magnitude and ultraviolet variations over both orbital and long-term periods. The ultraviolet P Cygni lines show dramatic changes with orbital phase, with strong broad absorption near X-ray eclipse and narrow absorption when the X-ray source is in the line of sight. We interpret this as a result of X-ray photoionization of the stellar wind; when the neutron star is in front of the normal star, the wind absorption disappears and mainly the photospheric absorption lines are visible. The X-ray pulse period measured during our observations, 13.5090 +/- 0.0002 s, is consistent with steady spin-down over the past 10 years. No pulsations were detected in the ultraviolet observations, with upper limits to the pulsed fraction around N V and C IV of 1.8% and 2.7% in the continuum and 7% and 12% in the absorption troughs, respectively. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. VILLANOVA UNIV, DEPT ASTRON & ASTROPHYS, VILLANOVA, PA 19085 USA. UNIV COLORADO, JOINT INST LAB ASTROPHYS, BOULDER, CO 80309 USA. INST SPACE & ASTRONAUT SCI, SAGAMIHARA, KANAGAWA 229, JAPAN. NR 35 TC 16 Z9 16 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 NOV 20 PY 1997 VL 490 IS 1 BP 377 EP 382 DI 10.1086/512792 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YG999 UT WOS:A1997YG99900038 ER PT J AU Serabyn, E Carlstrom, J Lay, O Lis, DC Hunter, TR Lacy, JH Hills, RE AF Serabyn, E Carlstrom, J Lay, O Lis, DC Hunter, TR Lacy, JH Hills, RE TI High-frequency measurements of the spectrum of Sagittarius A* SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, nuclei; galaxy, center ID GALACTIC-CENTER; BLACK-HOLE; ANATOMY; COMPLEX; CAVITY; VLBI; FLUX AB We report near-simultaneous interferometric measurements of the spectrum of Sagittarius A* over the 5-354 GHz range and single-dish observations that have yielded the first detection of Sgr A* at 850 GHz. We confirm that Sgr A*'s spectrum rises more steeply at short millimeter wavelengths than at centimeter wavelengths, leading to a near-millimeter/submillimeter excess that dominates its luminosity. Below 900 GHz, Sgr A*'s observed luminosity is 70 +/- 30 L.. A new upper limit to Sgr A*'s 24.3 mu m flux, together with a compilation of other extant IR data, imply a far-infrared spectral turnover, which can result from either an intrinsic synchrotron cutoff or excess extinction near Sgr A*. If the former applies, Sgr A*'s total synchrotron luminosity is <10(3) L., while in the latter case it is <3 x 10(4) L. if spherical symmetry also applies. C1 UNIV CHICAGO, DEPT ASTRON & ASTROPHYS, CHICAGO, IL 60637 USA. NASA, AMES RES CTR, MOFFETT FIELD, CA 94035 USA. SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. UNIV TEXAS, AUSTIN, TX 78712 USA. MULLARD RADIO ASTRON OBSERV, CAMBRIDGE CB3 OHE, ENGLAND. CALTECH, PASADENA, CA 91125 USA. OI Hunter, Todd/0000-0001-6492-0090 NR 29 TC 73 Z9 73 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1997 VL 490 IS 1 BP L77 EP + DI 10.1086/311010 PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YH001 UT WOS:A1997YH00100019 ER PT J AU Seideman, T AF Seideman, T TI Time-resolved photoelectron angular distributions: A nonperturbative theory SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ENHANCED MULTIPHOTON IONIZATION; WAVE-PACKET DYNAMICS; INTENSE LASER FIELDS; FLUORESCENCE POLARIZATION; MOLECULAR ALIGNMENT; BRANCHING RATIOS; PHOTO-IONIZATION; ELECTRIC-FIELD; SPECTROSCOPY; STATE AB We describe a quantum mechanical framework for the calculation of angle-and energy-resolved photoelectron flux in pump probe scenarios. The theory spans the limits of weak-to-strong field-matter interaction range and the ladder of transitions to al!angular momentum states. It allows insight into the type of information that can be extracted from time-resolved photoelectron distributions with regard to the wavepacket dynamics in the probed manifold. In the strong pump case it suggests the possibility of gaining insight also regarding the ionization dynamics, complementary to that extracted from weak-field CW studies. Various limits and several averaged observables are discussed and an efficient computational method is suggested. (C) 1997 American Institute of Physics. C1 NATL RES COUNCIL CANADA,STEACIE INST MOL SCI,OTTAWA,ON K1A 0R6,CANADA. RP Seideman, T (reprint author), HARVARD UNIV,HARVARD SMITHSONIAN CTR,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138, USA. NR 64 TC 57 Z9 57 U1 0 U2 6 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 15 PY 1997 VL 107 IS 19 BP 7859 EP 7868 DI 10.1063/1.475098 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA YG655 UT WOS:A1997YG65500028 ER PT J AU Riley, SM AF Riley, SM TI The prodigy - Hynd,N SO LIBRARY JOURNAL LA English DT Book Review RP Riley, SM (reprint author), SMITHSONIAN INST LIBS,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 15 PY 1997 VL 122 IS 19 BP 76 EP 76 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA YF993 UT WOS:A1997YF99300204 ER PT J AU Yan, ZC Drake, GWF AF Yan, ZC Drake, GWF TI Computational methods for three-electron atomic systems in Hylleraas coordinates SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID VARIATIONAL CALCULATIONS; 3-ELECTRON PROBLEM; INTEGRALS; EXPANSION; LITHIUM; STATES; LI AB General methods for evaluating three-electron integrals in Hylleraas coordinates are given. Formulae are obtained for the matrix elements of various operators arising in Hylleraas-type variational calculations for states of arbitrary angular momentum. For the calculations of Breit interaction, a number of reduction relations are developed for the elimination of singularities in some singular integrals. A numerically stable scheme is presented for the case when one of the powers of r(ij) is -2. C1 UNIV WINDSOR,DEPT PHYS,WINDSOR,ON N9B 3P4,CANADA. RP Yan, ZC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Yan, Zong-Chao/F-6668-2014 NR 17 TC 50 Z9 50 U1 0 U2 3 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 NOV 14 PY 1997 VL 30 IS 21 BP 4723 EP 4750 DI 10.1088/0953-4075/30/21/012 PG 28 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA YH110 UT WOS:A1997YH11000012 ER PT J AU Brandt, WN Ward, MJ Fabian, AC Hodge, PW AF Brandt, WN Ward, MJ Fabian, AC Hodge, PW TI ROSAT HRI observations of the local group galaxies IC 10, NGC 147 and NGC 185 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars, individual, TV Cas; stars, individual, BH Cas; galaxies, individual, IC 10; galaxies, individual, NGC 147; galaxies, individual, NGC 185; x-rays, general ID WOLF-RAYET STARS; IC-10; BINARIES; EVOLUTION; DISTANCE; EMISSION; SPECTRA AB We report on pointed X-ray observations of IC 10, NGC 147 and NGC 185 made with the ROSAT High Resolution Imager (HRI). These are three Local Group galaxies that have never been previously studied in detail in the X-ray regime. IC 10 is the closest starburst galaxy to our own Galaxy, and NGC 147 and NGC 185 are companions to M31. We have discovered a variable X-ray source coincident with IC 10. The source is located near the centre of a large, non-thermal bubble of radio emission, and it is positionally coincident with an emission-line star in IC 10 which has been classified as a WN-type Wolf-Rayet star. We demonstrate that a confusing foreground or background source is improbable. The X-ray source is probably an X-ray binary in IC 10, and it may be a Wolf-Rayet + black hole binary. The source has mean and maximum 0.1-2.5 keV isotropic luminosities of about 2 and 4 x 10(38) erg s(-1), respectively. We do not detect any sources in the central regions of NGC 147 or NGC 185. We place upper limits on their central X-ray emission, and we list all X-ray sources coincident with their outer extents. We also present the first X-ray detections of the well-studied Algol-type binary TV Gas and the W UMa-type binary BH Gas, which were both serendipitously observed during our IC 10 pointing. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. UNIV LEICESTER,DEPT PHYS & ASTRON,XRAY ASTRON GRP,LEICESTER LE1 7RH,LEICS,ENGLAND. UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195. RI Brandt, William/N-2844-2015 OI Brandt, William/0000-0002-0167-2453 NR 49 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 NOV 11 PY 1997 VL 291 IS 4 BP 709 EP 716 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YH485 UT WOS:A1997YH48500010 ER PT J AU Simcoe, R McLeod, KK Schachter, J Elvis, M AF Simcoe, R McLeod, KK Schachter, J Elvis, M TI Obscuration in the host galaxies of soft X-ray-selected Seyfert nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, ISM; galaxies, nuclei; galaxies, Seyfert; galaxies, structure; X-rays, galaxies ID ACTIVE GALACTIC NUCLEI; MOLECULAR GAS; CENTAURUS-A; LUMINOSITY; QUASARS; EMISSION; SAMPLE AB We define a new sample of 96 low-redshift (z < 0.1), soft X-ray-selected Seyfert galaxies from the catalog of the Einstein Slew Survey. We probe the geometry and column depth of obscuring material in the host-galaxy disks using galactic axial ratios determined mainly from the Digitized Sky Survey. The distribution of host-galaxy axial ratios clearly shows a bias against edge-on spirals, which confirms the existence of a geometrically thick layer of obscuring material in the host-galaxy planes. Soft X-ray selection recovers some of the edge-on objects missed in UV and visible surveys but still results in 30% incompleteness for type 1 nuclei. We speculate that thick rings of obscuring material such as the ones we infer for these Seyfert galaxies might be commonly present in early-type spirals, sitting at the inner Lindblad resonances of the nonaxisymmetric potentials of the host galaxies. C1 SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. NR 43 TC 28 Z9 28 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 NOV 10 PY 1997 VL 489 IS 2 BP 615 EP 622 DI 10.1086/304819 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YF300 UT WOS:A1997YF30000014 ER PT J 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 TI A search for infall motions toward nearby young stellar objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, jets and outflows; ISM, kinematics and dynamics; ISM, molecules; radio lines, stars; stars, formation; stars, pre-main-sequence ID DENSE CORES; STAR-FORMATION; DARK CLOUDS; BOK GLOBULES; PROTOSTELLAR COLLAPSE; MOLECULAR OUTFLOWS; LINE FORMATION; IRAS; JET; PROTOSTARS AB We report observations of 47 candidate protostars in two optically thick lines [H2CO (2(12)-1(11)) and CS (2-1)] and one optically thin line [N2H+ (1-0)] using the IRAM 30 m, SEST 15 m, and Haystack 37 m radio telescopes. The sources were selected for the redness of their spectra (T-bol < 200 K) and their near distance (d < 400 pc). Most of the sources have asymmetric, optically thick lines. The observed distribution of velocity differences, delta V = (V-thick - V-thin)/Delta V-thin, is skewed toward negative (blueshifted) velocities for both the H2CO and CS samples. This excess is much more significant for class 0 than for class I sources, suggesting that we detect infall motions toward class 0 and not toward class I sources. This indicates a difference in the physical conditions in the circumstellar envelopes around class I and class 0 sources, but it does not rule out the presence of infall onto class I sources by, for example, lower opacity gas. Bipolar outflows alone, or rotation alone, cannot reproduce these statistics if the sample of sources has randomly oriented symmetry axes. We identify 15 spectroscopic infall candidates, six of which are new. Most of these infall candidates have primarily turbulent rather than thermal motions and are associated with clusters rather than being isolated. C1 OBSERV ASTRON NACL,E-28800 ALCALA DE HENARES,SPAIN. UNIV CHILE,SANTIAGO,CHILE. RP Mardones, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Garay, Guido/H-8840-2013; Mardones, Diego/I-5719-2016 OI Garay, Guido/0000-0003-1649-7958; NR 74 TC 216 Z9 216 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 NOV 10 PY 1997 VL 489 IS 2 BP 719 EP 733 DI 10.1086/304812 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YF300 UT WOS:A1997YF30000021 ER PT J AU Girart, JM Estalella, R Anglada, G Torrelles, JM Ho, PTP Rodriguez, LF AF Girart, JM Estalella, R Anglada, G Torrelles, JM Ho, PTP Rodriguez, LF TI The ammonia core in L723: Hot spots at the center of the quadrupolar molecular outflow SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual, L723; ISM, jets and outflows; ISM, molecules; masers; radio lines, ISM; stars, formation ID STAR-FORMATION; CLOUD CORES; DARK CLOUDS; REGIONS; COLLAPSE; DISK; GAS AB We present the results of VLA NH3 and H2O observations, as well as Haystack (CO)-C-13, (CO)-O-18, and H2O observations toward the center of the peculiar quadrupolar molecular outflow in L723. In NH3 we detected a high-density structure, similar to 17 (similar to 0.15 pc) long, elongated in roughly the east-west direction, with the radio continuum source VLA 2 located near its center. We find evidence in the ammonia maps for heating and line broadening toward VLA 2, confirming that this source is driving the large lobe pair of the quadrupolar molecular outflow. Additionally, H2O maser emission is detected toward this radio continuum source. A second, very compact ammonia ''hot spot'' is observed 10'' west of VLA 2. This ''hot spot'' may be heated by a deeply embedded (still undetected) young stellar object that could be the driving source of the more compact pair of molecular outflow lobes. No ammonia emission is detected at the position of the source VLA 1, which is probably a line-of-sight source. C1 UNIV BARCELONA, DEPT ASTRON & METEOROL, E-08028 BARCELONA, SPAIN. Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. CSIC, INST ASTROFIS ANDALUCIA, E-18080 GRANADA, SPAIN. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Torrelles, Jose Maria/0000-0002-6896-6085 NR 30 TC 22 Z9 22 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 NOV 10 PY 1997 VL 489 IS 2 BP 734 EP + DI 10.1086/304795 PN 1 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YF300 UT WOS:A1997YF30000022 ER PT J AU Torrelles, JM Gomez, JF Rodriguez, LF Ho, PTP Curiel, S Vazquez, R AF Torrelles, JM Gomez, JF Rodriguez, LF Ho, PTP Curiel, S Vazquez, R TI A radio jet-H2O maser system in W75N(B) at a 200 AU scale: Exploring the evolutionary stages of young stellar objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE H 11 regions; ISM, individual (W75N); ISM, jets and outflows; masers; stars, formation ID H-II REGIONS; CONTINUUM EMISSION; MOLECULAR OUTFLOW; VLA OBSERVATIONS; WATER MASERS; H2O MASERS; JET; STAR; OH; CORE AB We have observed simultaneously with the VLA in its A configuration the 1.3 cm continuum and H2O maser emission toward the star-forming region W75N(B) with 0''11 resolution using a powerful cross-calibration technique. Three continuum sources (VLA 1, VLA 2, and VLA 3) were detected in a region of 1.''5. VLA 1 is elongated (0.''43 x 0.''12) approximately in the direction of the bipolar molecular outflow observed at scales of 2'. The frequency dependence of the flux density and size are consistent with an optically partially thick ionized thermal biconical jet. VLA 2 appears unresolved, while VLA 3 shows a bright core plus extended emission. We detected 29 H2O maser spots (spatial components) in a region of 13'' x 7'' around W75N(B). These masers are mainly distributed in two clusters, one associated with VLA 1 (11 maser spots), and the other one associated with VLA 2 (eight maser spots). One H2O maser spot is associated with VLA 3. The masers associated with VLA 1 are distributed along the major axis of the radio jet. We conclude that VLA 1 is the powering source of the extended bipolar molecular outflow and that the water masers along the radio jet axis are delineating the outflow at scales of 1'' On the other hand, the eight masers coincident with VLA 2 are distributed in a shell of 0.''18 x 0.''10, with a rough north-south velocity segregation that could indicate bound motions around this continuum source. From the comparison of H2O and OH maser distribution in the region with respect to the three radio sources, we consider an evolutionary scheme in which H2O masers are excited in gravitationally bound material (e.g., in circumstellar disks) in less evolved young stellar objects (YSOs), while in more evolved YSOs H2O masers preferentially trace outflows. C1 INTA, LAB ASTROFIS ESPACIAL & FIS FUNDAMENTAL, E-28080 MADRID, SPAIN. Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Torrelles, JM (reprint author), CSIC, INST ASTROFIS ANDALUCIA, APDO CORREOS 3004, E-18080 GRANADA, SPAIN. RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 38 TC 88 Z9 89 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 NOV 10 PY 1997 VL 489 IS 2 BP 744 EP 752 DI 10.1086/304824 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YF300 UT WOS:A1997YF30000023 ER PT J AU Esin, AA McClintock, JE Narayan, R AF Esin, AA McClintock, JE Narayan, R TI Advection-dominated accretion and the spectral states of black hole X-ray binaries: Application to Nova Muscae 1991 SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; black hole physics; X-rays, stars ID ACTIVE GALACTIC NUCLEI; CYGNUS X-1; RELATIVISTIC PLASMAS; COLD MATTER; DISK MODEL; INSTABILITY; TRANSIENTS; EMISSION; DISCOVERY; VARIABILITY AB Black hole X-ray binaries (BHXBs) are known to display five distinct spectral states. In order of increasing luminosity these are the quiescent state, low state, intermediate state, high state, and very high state. We present a self-consistent model of accretion flows around black holes that unifies all of these states except the very high state. The model is an extension of the following paradigm, which has been applied successfully to the quiescent state. The accretion flow consists of two zones, an inner advection-dominated accretion flow (ADAF) that extends from the black hole horizon to a transition radius r(tr), and an outer thin accretion disk that is present beyond r(tr). Above the disk is a hot corona, which is a continuation of the inner ADAF. The model consistently treats the dynamics of the accreting gas, the thermal balance of the ions and electrons in the two-temperature ADAF and corona, and the radiation processes that produce the observed spectrum. At low mass accretion rates, (m) over dot less than or similar to 0.01 (in Eddington units), the inner ADAF zone in the model radiates extremely inefficiently, and the outer thin disk is restricted to large radii (r(tr) similar to 10(2)-10(4), in Schwarzschild units). The luminosity therefore is low, and this configuration is identified with the quiescent state. For (m) over dot greater than or similar to 0.01 and up to a critical value (m) over dot(crit) similar to 0.08, the radiative efficiency of the ADAF increases rapidly and the system becomes fairly luminous. The spectrum is very hard and peaks around 100 keV. This is the low state. The exact value of (m) over dot(crit) depends on the viscosity parameter alpha ((m) over dot(crit) similar to 1.3 alpha(2); the paper assumes alpha = 0.25). For values of (m) over dot > (m) over dot(crit) and up to a second critical value about 10% higher, the ADAF progressively shrinks in size, the transition radius decreases, and the X-ray spectrum changes continuously from hard to soft. We identify this stage with the intermediate state. Finally, when (m) over dot is sufficiently large, the inner ADAF zone disappears altogether and the thin accretion disk extends down to the marginally stable orbit. The spectrum is dominated by an ultrasoft component with a weak hard tail. This is the high state. Model spectra calculated with this unified scenario agree well with observations of the quiescent, low, intermediate, and high states. Moreover, the model provides a natural explanation for the low state to high state transition in BHXBs. We also make a tentative proposal for the very high state, but this aspect of the model is less secure. An important feature of the model is that it is essentially parameter free. We test the model against observations of the soft X-ray transient Nova Muscae during its 1991 outburst. The model reproduces the observed light curves and spectra surprisingly well and makes a number of predictions that can be tested by observations of other BHXBs. RP Esin, AA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 109 TC 712 Z9 717 U1 2 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1997 VL 489 IS 2 BP 865 EP 889 DI 10.1086/304829 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YF300 UT WOS:A1997YF30000033 ER PT J AU Forrey, RC Balakrishnan, N Dalgarno, A Lepp, S AF Forrey, RC Balakrishnan, N Dalgarno, A Lepp, S TI Quantum mechanical calculations of rotational transitions in H-H-2 collisions SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular data; molecular processes ID POTENTIAL-ENERGY SURFACE; SWS SPECTROSCOPY; STARBURST GALAXY; EXCITATION; ATOMS; H-3 AB We report quantum mechanical cross sections and rate coefficients for rotational transitions due to collisions of hydrogen atoms with hydrogen molecules. The sensitivity of the results to the nature of the potential energy surface and to the scattering formulation is investigated. We find that the rigid rotor and harmonic oscillator approximations are inadequate to describe the dynamics. We make use of the most reliable of the potential energy surfaces in a close-coupled description of the nonreactive scattering that takes the vibrational motion into account, and we calculate rate coefficients for rotational transitions at temperatures below 1000 K, where the reactive channels may be neglected. C1 UNIV NEVADA,DEPT PHYS,LAS VEGAS,NV 89154. RP Forrey, RC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 40 Z9 40 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 NOV 10 PY 1997 VL 489 IS 2 BP 1000 EP 1003 DI 10.1086/304827 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YF300 UT WOS:A1997YF30000046 ER PT J AU Thomsen, JL Simonsen, KW Felby, S Frohlich, B AF Thomsen, JL Simonsen, KW Felby, S Frohlich, B TI A prospective toxicology analysis in alcoholics SO FORENSIC SCIENCE INTERNATIONAL LA English DT Article DE alcoholic; ketoacidosis; intoxication; forensic medicine ID KETOACIDOSIS AB A prospective and comprehensive investigation was done on 73 medico-legal autopsies in alcoholics. The results of the toxicology analyses are described. Alcohol intoxication was the cause of death in 8%, combined alcohol/drug intoxication in 15% and drugs alone in 19%. Alcoholic ketoacidosis was found to be the cause of death in 7%. Altogether toxicology analyses were necessary for determining the cause of death in 51% of the cases. In four cases the cause of death would not have been found, had this investigation not been made. It is concluded that toxicology analyses should be the rule rather than the exception in deaths in alcoholics. (C) 1997 Elsevier Science Ireland Ltd. C1 Odense Univ, Inst Forens Med, DK-5000 Odense C, Denmark. Univ Copenhagen, Inst Forens Med, Dept Forens Chem, Copenhagen, Denmark. Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Thomsen, JL (reprint author), Odense Univ, Inst Forens Med, Winslowparken 17, DK-5000 Odense C, Denmark. NR 5 TC 15 Z9 15 U1 0 U2 0 PU ELSEVIER SCI IRELAND LTD PI CLARE PA CUSTOMER RELATIONS MANAGER, BAY 15, SHANNON INDUSTRIAL ESTATE CO, CLARE, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD NOV 10 PY 1997 VL 90 IS 1-2 BP 33 EP 40 DI 10.1016/S0379-0738(97)00142-4 PG 8 WC Medicine, Legal SC Legal Medicine GA YN533 UT WOS:000071178100005 PM 9438363 ER PT J AU You, L Walsworth, R Hoston, W AF You, L. Walsworth, R. Hoston, W. TI Higher energy collective excitations in trapped Bose condensates SO OPTICS EXPRESS LA English DT Article AB We investigate theoretically the collective excitations of trapped Bose condensates with energies of the order of the chemical potential of the system. For the MIT sodium Bose condensate in a Cloverleaf trap, we find interesting level crossing behavior for high energy excitations and calculate the spatial magnetic dipole moments for selective creation of condensate excitations. (c) 1997 Optical Society of America C1 [You, L.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Walsworth, R.; Hoston, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hoston, W.] MIT, Dept Phys, Cambridge, MA 02139 USA. RP You, L (reprint author), Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. EM Li.You@physics.gatech.edu FU U.S. Office of Naval Research [14-97-1-0633]; NSF [PHY-9722410]; National Science Foundation through the Institute for Theoretical Atomic and Molecular Physics at Harvard University; Smithsonian Astrophysical Observatory FX This work is supported by the U.S. Office of Naval Research grant No. 14-97-1-0633 and by the NSF grant No. PHY-9722410. The work of W. H. is supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic and Molecular Physics at Harvard University and the Smithsonian Astrophysical Observatory. NR 31 TC 4 Z9 4 U1 0 U2 0 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD NOV 10 PY 1997 VL 1 IS 10 BP 293 EP 300 PG 8 WC Optics SC Optics GA V23QC UT WOS:000208356300005 PM 19373415 ER PT J AU Simbotin, I Marinescu, M Sadeghpour, HR Dalgarno, A AF Simbotin, I Marinescu, M Sadeghpour, HR Dalgarno, A TI Resonant Raman scattering in O-2 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SCHUMANN-RUNGE BANDS; PREDISSOCIATION LINEWIDTHS; FLUORESCENCE; SPECTROSCOPY; DEPENDENCE; SPECTRA; OXYGEN; LASER AB Raman scattering of molecular oxygen in the region of the Schumann-Runge absorption band system is calculated from first principles in the second order of perturbation theory in the interaction of photon-electron operator. Quantitative predictions are given for the cross sections for scattering of photons and a detailed comparison is made with available measurements. The behavior of Raman spectra near the predissociating rovibronic level (upsilon' = 5,N') in the B (3) Sigma(u)(-) electronic State of O-2 is investigated and shown to have significant dependence on the detuning of the incident laser frequency. By casting the Raman transition matrix in a form similar to the Fano formalism, we are able to investigate the nature of the resonant and nonresonant scattering in the language of configuration interaction. By varying the predissociating width of the (upsilon' = 5,N') resonance, we make a comparison with an earlier time-dependent wave-packet analysis. We also calculate the depolarization ratio of the scattered photons parallel and perpendicular to the polarization of the incident laser beam for the different Raman branches for lines terminating in the v '' = 1 and v '' = 6 levels and comment on the relationship between resonant Raman scattering and fluorescence emission. (C) 1997 American Institute of Physics. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 22 TC 4 Z9 4 U1 1 U2 6 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 8 PY 1997 VL 107 IS 18 BP 7057 EP 7066 DI 10.1063/1.474948 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA YE668 UT WOS:A1997YE66800006 ER PT J AU Cote, R Dalgarno, A AF Cote, R Dalgarno, A TI Mechanism for the production of vibrationally excited ultracold molecules of Li-7(2) SO CHEMICAL PHYSICS LETTERS LA English DT Article ID SCATTERING LENGTH; ATOMS; TRANSITION; STATES; PHOTOASSOCIATION; SPECTROSCOPY; LI-6(2) AB A scheme is described by which translationally cold molecules can be created in specific rotational and vibrational levels and it is suggested they be employed to test Wigner's threshold laws for inelastic collisions. Calculations are presented of the spontaneous emission probabilities and the absorption oscillator strengths of transitions between the vibrational energy levels of the ground and excited triplet states of the molecules Li-7(2). The fractions of transitions into the continuum and Into the discrete levels are estimated and it is shown that the translationally cold molecules can be produced efficiently in photoassociation experiments. The photoabsorption rate coefficients are computed. (C) 1997 Elsevier Science B.V. RP Cote, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 66 Z9 66 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD NOV 7 PY 1997 VL 279 IS 1-2 BP 50 EP 54 DI 10.1016/S0009-2614(97)00937-8 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA YK053 UT WOS:A1997YK05300008 ER PT J AU Peng, GY Luhr, JF McGee, JJ AF Peng, GY Luhr, JF McGee, JJ TI Factors controlling sulfur concentrations in volcanic apatite SO AMERICAN MINERALOGIST LA English DT Article ID RARE-EARTH ELEMENTS; ELECTRON-MICROPROBE ANALYSIS; ANHYDRITE-BEARING PUMICES; EL-CHICHON VOLCANO; MOUNT-ST-HELENS; DIOXIDE EMISSIONS; CRYSTAL-CHEMISTRY; OXYGEN FUGACITY; MELT EQUILIBRIA; 1982 ERUPTIONS AB Apatite crystals from two types of samples were analyzed by electron microprobe for 15 major and trace elements: (1) apatite in H2O- and S-saturated experimental charges of the 1982 El Chichon trachyandesite and (2) apatite in volcanic rocks erupted from 20 volcanoes. The SO3 contents of the experimental apatite increase with increasing oxygen fugacity (fO(2)), from less than or equal to 0.04 wt% in reduced charges buffered by fayalite-magnetite-quartz (FMQ), to 1.0-2.6 wt% in oxidized charges buffered by manganosite-hausmanite (MNH) or magnetite-hematite (MTH). The SO3 contents of MNH- and MTH-buffered apatite also generally increase with increasing pressure from 2 to 4 kbar and decreasing temperature from 950 to 800 degrees C. The partition coefficient for SO3 between apatite and oxidized melt increases with decreasing temperature but appears to be independent of pressure. Apatites in volcanic rocks show a wide range of SO3 contents (<0.04 to 0.63 wt%). Our sample set includes one group known to contain primary anhydrite and a second group inferred to have been free of primary anhydrite, No systematic differences in apatite S contents are observed between these two groups. Our study was initiated to define the factors controlling S contents in apatite and to evaluate the hypothesis that high S contents in apatite could be characteristic of S-rich anhydrite-bearing magmas such as those erupted from El Chichon in 1982 and Pinatubo in 1991, This hypothesis is shown to be invalid, probably chiefly a consequence of the slow intra-crystalline diffusion that limits re-equilibration between early formed apatite and the evolving silicate melt. Contributing factors include early crystallization of most apatite over a relatively small temperature interval, common late-stage magmatic enrichment of S, progressive oxidation during magmatic evolution, and strong controls on S contents in apatite exerted by fO(2), temperature, and pressure. C1 US GEOL SURVEY, RESTON, VA 22092 USA. RP Peng, GY (reprint author), SMITHSONIAN INST, DEPT MINERAL SCI, NHB-119, WASHINGTON, DC 20560 USA. NR 77 TC 61 Z9 66 U1 4 U2 24 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD NOV-DEC PY 1997 VL 82 IS 11-12 BP 1210 EP 1224 PG 15 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA YG094 UT WOS:A1997YG09400017 ER PT J AU Sorenson, LG Nolan, PM Brown, AM Derrickson, SR Monfort, SL AF Sorenson, LG Nolan, PM Brown, AM Derrickson, SR Monfort, SL TI Hormonal dynamics during mate choice in the northern pintail: a test of the 'challenge' hypothesis SO ANIMAL BEHAVIOUR LA English DT Article ID WHITE-CROWNED SPARROWS; STRESS-INDUCED INHIBITION; DUCK ANAS-PLATYRHYNCHOS; RED-WINGED BLACKBIRDS; MALE JAPANESE QUAIL; MALE SONG SPARROWS; MELOSPIZA-MELODIA; LUTEINIZING-HORMONE; STEROID-HORMONES; PLASMA-LEVELS AB In previous mate choice experiments, we found no relationship between dominance rank and pairing success in male northern pintails, Anas acuta. Once chosen by a female, however, males became aggressive, initiated fights with higher-ranked males and quickly established dominance. In the present study, we tested a variation of the 'challenge' hypothesis, that the behavioural stimuli associated with acquiring and defending a mate induce an increase in testosterone level, which in turn facilitates aggressive behaviours required for males to establish dominance. We measured plasma hormone levels (testosterone, dihydrotestosterone, luteinizing hormone and corticosterone) before and after mate choice in two experiments in which males competed for a single female (experiments 1 and 2) and in a control experiment in which no female was introduced (experiment 3). We used groups of either three adult males (experiment 1) or one adult and two yearling males (experiments 2 and 3). Contrary to expectation, in experiment 1, plasma levels of corticosterone increased significantly and testosterone levels decreased in chosen males following mate choice. The magnitude of change in corticosterone was positively correlated with the rate of aggression by males. Chosen adult males in experiment 2 showed similar patterns of hormone change (corticosterone increase and testosterone decrease), although not all changes were significant. Hormone levels of unchosen yearlings in experiment 2 and control adults and yearlings in experiment 3 showed no changes. The results are consistent with the hypothesis that behavioural stimuli associated with successful pair formation induce a transitory increase in circulating levels of corticosterone, which in turn mediates the behavioural response of increased aggression leading to the establishment of dominance following mate choice. A short-term increase in corticosterone may be adaptive in this situation because it would mobilize energy stores needed by the: male to defend the new pair bond and establish dominance. (C) 1997 The Association for the Study of Animal Behaviour. C1 SMITHSONIAN INST, CONSERVAT & RES CTR, US NATL ZOOL PK, FRONT ROYAL, VA 22630 USA. AUBURN UNIV, DEPT ZOOL, AUBURN, AL 36849 USA. UNIV TORONTO, ERINDALE COLL, DEPT BIOL, TORONTO, ON L5L 1C6, CANADA. NR 73 TC 36 Z9 36 U1 1 U2 12 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD NOV PY 1997 VL 54 BP 1117 EP 1133 DI 10.1006/anbe.1997.0554 PN 5 PG 17 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA YJ174 UT WOS:A1997YJ17400007 ER PT J AU Kerman, AK Tommasini, P AF Kerman, AK Tommasini, P TI Gaussian time-dependent variational principle for Bosons .1. Uniform case SO ANNALS OF PHYSICS LA English DT Article ID BOSE-EINSTEIN CONDENSATION; GAS AB We investigate the Dirac time-dependent variational method for a system of non-ideal Bosons interacting through an arbitrary two body potential. The method produces a set of non-linear time dependent equations for the variational parameters. In particular we have considered small oscillations about equilibrium. We obtain generalized RPA equations that can be understood as interacting quasi-bosons, usually mentioned in the literature as having a gap. The result of this interaction provides us with scattering properties of these quasi-bosons including possible bound-states, which can include zero modes. In fact the zero mode bound state can be interpreted as a new quasi-boson with a gapless dispersion relation. Utilizing these results we discuss a straightforward scheme for introducing temperature. (C) 1997 Academic Press. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. RP Kerman, AK (reprint author), MIT,NUCL SCI LAB,CTR THEORET PHYS,CAMBRIDGE,MA 02139, USA. NR 17 TC 13 Z9 13 U1 0 U2 1 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 NOV 1 PY 1997 VL 260 IS 2 BP 250 EP 274 DI 10.1006/aphy.1997.5723 PG 25 WC Physics, Multidisciplinary SC Physics GA YG045 UT WOS:A1997YG04500003 ER PT J AU Alarie, Y Wang, LJ Nilsson, AN Spangler, PJ AF Alarie, Y Wang, LJ Nilsson, AN Spangler, PJ TI Larval morphology of four genera of the tribe Hyphydrini Sharp (Coleoptera : Dytiscidae : Hydroporinae) with an analysis of their phylogenetic relationships SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Coleoptera; Dytiscidae; Hyphydrini; larval morphology; chaetotaxy and porotaxy; phylogeny ID PRIMARY SETAE; PORES; ADEPHAGA AB Description of structures of the larvae of 4 genera (Desmopachria Babington, Hyphydrus Illiger, Microdytes Balfour-Browne, and Pachydrus Sharp) of the tribe Hyphydrini Sharp is presented. The chaetotaxy and porotaxy of the cephalic capsule, head appendages, legs, last abdominal segment, and urogomphi are discussed in detail. Within the subfamily Hydroporinae, the Hyphydrini are hypothesized to constitute a monophyletic assemblage based on the following 7 synapomorphies: (1) absence of pore PAj, (2) epicranial plates meeting at the ventral midline, (3) absence of pore FRb, (4) medioventral position of seta FR6, (5) absence of pore ANh, (6) abdominal segment 6 sclerotized ventrally, and (7) proximal insertion of the primary seta UR8 on urogomphomere 2. It is proposed that Pachydrus occupies a basal position within the Hyphydrini. A monophyletic origin is indicated for Macrodytes, Desmopachria, and Hyphydrus based on the shared presence of an elongated prementum and a more proximal insertion of seta UR8 on urogomphomere 2. Desmopachria and Hyphydrus are related phylogenetically by the absence of lateral notches on the frontoclypeus, the presence of at least 1 secondary seta on ventral surface of the siphon (3rd instar), and the short and spiniform appearance of the primary seta UR5 in 1st instars. C1 Laurentian Univ, Dept Biol, Sudbury, ON P3E 2C6, Canada. Natl Taiwan Univ, Dept Entomol & Plant Pathol, Taipei 10764, Taiwan. Umea Univ, Dept Anim Ecol, S-90187 Umea, Sweden. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Alarie, Y (reprint author), Laurentian Univ, Dept Biol, Sudbury, ON P3E 2C6, Canada. NR 43 TC 23 Z9 24 U1 0 U2 0 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD NOV PY 1997 VL 90 IS 6 BP 709 EP 735 PG 27 WC Entomology SC Entomology GA YU571 UT WOS:000071731200001 ER PT J AU Rand, H AF Rand, H TI Gorky's 'Waterfalls' (1943) (Tracing the sources of Arshile Gorky's paintings with the same title) SO ARTNEWS LA English DT Article C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Rand, H (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ARTNEWS ASSOCIATES PI NEW YORK PA 48 WEST 38TH STREET, NEW YORK, NY 10018 USA SN 0004-3273 J9 ART NEWS JI Artnews PD NOV PY 1997 VL 96 IS 10 BP 118 EP + PG 0 WC Art SC Art GA YD879 UT WOS:000060194300025 ER PT J AU Sneden, C Kraft, RP Shetrone, MD Smith, GH Langer, GE Prosser, CF AF Sneden, C Kraft, RP Shetrone, MD Smith, GH Langer, GE Prosser, CF TI Star-to-star abundance variations among bright giants in the metal-poor globular cluster M15 SO ASTRONOMICAL JOURNAL LA English DT Article ID NEUTRON-CAPTURE ELEMENTS; HIGH-DISPERSION SPECTROSCOPY; S-PROCESS NUCLEOSYNTHESIS; HALO GIANTS; RED GIANTS; OXYGEN ABUNDANCES; NITROGEN ABUNDANCES; OMEGA-CENTAURI; ECHELLE-SPECTROMETER; CHEMICAL-COMPOSITION AB We find significant star-to-star variations in the abundances of both the light elements oxygen, sodium, magnesium, and aluminum, and the neutron capture elements barium and europium in a sample of eighteen bright M15 giants. The oxygen and sodium abundances are strongly anticorrelated as are the magnesium and aluminum abundances. Sodium and aluminum are correlated. Hence, there are M15 giants with large sodium and aluminum ''enhancements'' and smaller oxygen and magnesium ''depletions'' as well as giants with more ''normal'' abundances of these light elements. The correlations are very similar to those found earlier in M13, M10, and M92. The CNO abundance sum is approximately the same in the five M15 giants for which all three elements have been observed. This abundance pattern is most likely the result of proton-capture nucleosynthesis and most easily explained if it takes place within the stars that we have observed. The barium and europium variations are unlikely to be the result of nucleosynthesis within the stars that we have observed. They provide strong evidence for ''primordial'' neutron-capture abundance variations in a cluster other than omega Cen. The range in both [Eu/Fe] and [Ba/Fe] is about 0.6 dex. The abundances are strongly correlated and appear to fall into two groups, one with larger Eu and Ba abundances, the other with values of [Eu/Fe] and [Ba/Fe] that are about 0.35 dex smaller. The mean value of [Ba/Eu] is the same for both groups, and falls between the pure r-process value and the solar system r+s process mix. The light element abundances apparently do not correlate with the neutron-capture abundances even though both vary over a significant (often large) range. We find no evidence for star-to-star variations in either [Fe/H] or [Ca/Fe]. We have looked for small differences in [Fe/H] and [Ca/Fe] between stars with large and small values of [Eu/Fe] and [Ba/Fe]; the average values of [Fe/H] and [Ca/Fe] are the same for both. Hence, we find that there are large variations in the abundances of a number of elements (but not all of them) in M15, a cluster only recently thought to have a uniform composition. The abundances of the light elements (C, N, O, Na, Mg, and Al) are strongly correlated as are the abundances of the neutron-capture elements (Eu, Ba), but variations in the abundances of light and neutron-capture elements seem to be independent of each other, and both appear to be independent of the Fe and Ca abundances. (C) 1997 American Astronomical Society. C1 UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. UNIV CALIF SANTA CRUZ,BOARD STUDIES ASTRON & ASTROPHYS,LICK OBSERV,UCO,SANTA CRUZ,CA 95064. COLORADO COLL,DEPT PHYS,COLORADO SPRINGS,CO 80903. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Sneden, C (reprint author), UNIV TEXAS,MCDONALD OBSERV,AUSTIN,TX 78712, USA. NR 80 TC 177 Z9 177 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 NOV PY 1997 VL 114 IS 5 BP 1964 EP 1981 DI 10.1086/118618 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YD884 UT WOS:A1997YD88400020 ER PT J AU Shen, ZQ Wan, TS Moran, JM Jauncey, DL Reynolds, JE Tzioumis, AK Gough, RG Ferris, RH Sinclair, MW Jiang, DR Hong, XY Liang, SG Costa, ME Tingay, SJ McCulloch, PM Lovell, JEJ King, EA Nicolson, GD Murphy, DW Meier, DL vanOmmen, TD Edwards, PG White, GL AF Shen, ZQ Wan, TS Moran, JM Jauncey, DL Reynolds, JE Tzioumis, AK Gough, RG Ferris, RH Sinclair, MW Jiang, DR Hong, XY Liang, SG Costa, ME Tingay, SJ McCulloch, PM Lovell, JEJ King, EA Nicolson, GD Murphy, DW Meier, DL vanOmmen, TD Edwards, PG White, GL TI A 5-GHz southern hemisphere VLBI survey of compact radio sources .1. SO ASTRONOMICAL JOURNAL LA English DT Review ID BL-LACERTAE OBJECTS; FREQUENCY VARIABLE SOURCES; ACTIVE GALACTIC NUCLEI; MILLIMETER CONTINUUM MEASUREMENTS; CORE-DOMINATED QUASARS; COMPLETE SAMPLE; AO 0235+164; SPECTROSCOPIC OBSERVATIONS; MILLIARCSECOND STRUCTURE; OPTICAL POLARIZATION AB We report the results of a 5-GHz southern hemisphere VLBI survey of compact extragalactic radio sources. These observations were undertaken with the SHEVE array plus Shanghai station in 1992 November. A sample of 22 sources was observed and images of 20 of them were obtained. Of the 20 sources imaged, 15 showed core-jet structure, I had a two-sided jet, and 4 had only single compact cores. Eleven of the 16 core-jet (including one two-sided jet) sources showed some evidence of bent jets. No compact doubles were found. A comparison with previous images and the temporal variability of the radio flux density showed evidence for superluminal motion in four of the sources. Five sources were high-energy (> 100 MeV) gamma-ray sources. Statistical analysis showed the dominance of highly polarized quasars among the detected gamma-ray sources, which emphasizes the importance of beaming effect in the gamma-ray emission. (C) 1997 American Astronomical Society. C1 SHANGHAI ASTRON OBSERV,SHANGHAI 200030,PEOPLES R CHINA. CSIRO,AUSTRALIA TELESCOPE NATL FACIL,EPPING,NSW 2121,AUSTRALIA. UNIV WESTERN AUSTRALIA,DEPT PHYS,NEDLANDS,WA 6009,AUSTRALIA. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,WESTON,ACT 2611,AUSTRALIA. UNIV TASMANIA,DEPT PHYS,HOBART,TAS 7001,AUSTRALIA. HARTEBEESTHOEK RADIO ASTRON OBSERV,ZA-1740 KRUGERSDORP,SOUTH AFRICA. CALTECH,JET PROP LAB,PASADENA,CA 91109. UNIV ADELAIDE,DEPT PHYS,ADELAIDE,SA 5005,AUSTRALIA. UNIV WESTERN SYDNEY NEPEAN,DEPT PHYS,NEPEAN,NSW 2747,AUSTRALIA. RP Shen, ZQ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Tingay, Steven/B-5271-2013; van Ommen, Tas/B-5020-2012; King, Edward/A-1473-2012 OI van Ommen, Tas/0000-0002-2463-1718; King, Edward/0000-0002-6898-2130 NR 114 TC 44 Z9 45 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 NOV PY 1997 VL 114 IS 5 BP 1999 EP 2015 DI 10.1086/118621 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YD884 UT WOS:A1997YD88400023 ER PT J AU Greene, TP Lada, CJ AF Greene, TP Lada, CJ TI Near-infrared spectra of flat-spectrum protostars: Extremely young photospheres revealed SO ASTRONOMICAL JOURNAL LA English DT Article ID T-TAURI STARS; ACCRETION DISKS; OBJECTS AB We present new high resolution (R similar or equal to 21,000) near-infrared (lambda=2 mu m) spectroscopic observations of a sample of flat-spectrum and Class II young stellar objects in the rho Ophiuchi dark cloud. Our observations of the hat-spectrum sources are the first to reveal details about the atmospheres of objects so young that they are still in the protostellar stages of early stellar evolution. The flat-spectrum objects exhibit molecular (GO) and atomic (Na, Sc, Si) line shapes which are consistent with those expected for rotating stellar photospheres. No clear spectroscopic signatures of Line formation in Keplerian circumstellar disks are found. The 2.294 mu m nu=0-2 CO spectra show that the flat-spectrum objects are rotating more rapidly ([upsilon sin i]similar or equal to 26 km s(-1)) than the Class II pre-main-sequence stars in our sample ([upsilon sin i]similar or equal to 12 km s(-1)). Analysis of the relative strengths of the atomic Lines of the two flat-spectrum sources GY21 and VSSG17 indicates that these objects have late spectral types, MO and M2 (or later), respectively. Their surface ,gravities are more similar to those of late-type dwarfs or pre-main-sequence subgiant stars than to those of late-type stellar giants or FU Ori stars. These characteristics can be understood if the absorption lines of flat-spectrum sources arise in stellar (rather than disk) atmospheres that are similar to those of pre-main-sequence subgiant T Tauri stars but are accreting mass from their circumstellar disks at higher rates. (C) 1997 American Astronomical Society. C1 SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. RP Greene, TP (reprint author), UNIV HAWAII, INST ASTRON, 2680 WOODLAWN DR, HONOLULU, HI 96822 USA. NR 26 TC 44 Z9 44 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1997 VL 114 IS 5 BP 2157 EP 2165 DI 10.1086/118636 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YD884 UT WOS:A1997YD88400038 ER PT J AU Fullerton, AW Massa, DL Prinja, RK Owocki, SP Cranmer, SR AF Fullerton, AW Massa, DL Prinja, RK Owocki, SP Cranmer, SR TI Wind variability of B supergiants .3. Corotating spiral structures in the stellar wind of HD 64760 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars, early-type; stars, mass-loss; stars, oscillations; stars, magnetic fields; stars, individual, HD 64760 (HR 3090) ID RADIATION-DRIVEN WINDS; TIME-SERIES ANALYSIS; HOT LUMINOUS STARS; INTERACTION REGIONS; MASSIVE STARS; LINE-PROFILE; HD-64760; MODELS AB Fourier analysis of two spectroscopic time series obtained with the IUE observatory confirm that the ultraviolet stellar wind profiles of HD 64760 (B0.5 Ib) are periodically variable. The periodic component consists of modulations that extend over most of the P Cygni absorption trough, and can frequently be traced through the emission lobe. The modulations coexist with variations due to the propagation of discrete absorption components, but there does not seem to be a direct link between these two types of variability. In a long time series obtained in 1995 January during the IUE MEGA Campaign, the modulations in the P Cygni profiles of the Si III, Si IV, C IV, and N V resonance lines were dominated by two sinusoidal variations with semi-amplitudes between similar to 5-10% of the continuum flux and periods of 1.202 +/- 0.004 and 2.44 +/- 0.04 days. The weak emission-lobe variability was predominantly due to the 2.4-day modulation. In the absorption trough, the ratio of the amplitude of the 1.2-day modulation to the amplitude of the 2.4-day modulation increased systematically as a function of ionization potential. For both periods, the distribution of the phase constant with position in the absorption trough exhibited a maximum near -710 km s(-1), and decreased symmetrically toward larger and smaller velocities. There was a systematic decrease in the value of the maximum phase between Si Iv and N v. Only the 2.4-day period was present in a shorter time series obtained in 1993 March, when its amplitude was nearly twice its 1995 value and it was more concentrated toward smaller velocities in the absorption trough. There is no clear evidence for phase bowing in the 1993 data. Since the 2.4- and 1.2-day periods are approximately a half and a quarter of the estimated rotational period of HD 64760, respectively, we interpret the modulations in terms of 2 (1993) and 4 (1995) broad, corotating circumstellar structures that modulate the optical depth of the stellar wind. The bowed distribution of phase implies that the structures are azimuthally extended, probably spiral-shaped arms, and we develop a kinematic interpretation of the projected velocity associated with the phase turnover in terms of the degree of bending of the spirals. We derive a value for the exponent governing the radial expansion of the wind of beta approximate to 1, which is in good agreement with the canonical value for smooth, spherically symmetric winds and suggests that the spiral structures are long-lived perturbations through which material flows. The systematic phase lag associated with higher ions suggests that they are preferentially located along the inner, trailing edge of the spiral, as expected if the structures are formed by the collision of fast and slow winds originating from equally-spaced longitudinal sectors of the stellar surface. Although a photospheric process is implicated in the origin of these structures, it is not clear that magnetic fields or nonradial pulsations could readily account for the switch between 2- and 4-equally spaced surface patches that evidently occurred between 1993 and 1995. C1 HUGHES STX, GREENBELT, MD 20770 USA. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. UNIV DELAWARE, BARTOL RES INST, NEWARK, DE 19716 USA. SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. RP Fullerton, AW (reprint author), UNIV STERNWARTE, SCHEINERSTR 1, D-81679 MUNICH, GERMANY. NR 45 TC 69 Z9 69 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 NOV PY 1997 VL 327 IS 2 BP 699 EP 720 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YF731 UT WOS:A1997YF73100034 ER PT J AU Nordstrom, B Stefanik, RP Latham, DW Andersen, J AF Nordstrom, B Stefanik, RP Latham, DW Andersen, J TI Radial velocities, rotations, and duplicity of a sample of early F-type dwarfs SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article DE methods, statistical; techniques, radial velocities; stars, binaries, spectroscopic; stars, kinematics; Galaxy, solar neighbourhood ID UVBY PHOTOMETRY; SPECTROSCOPIC BINARIES; STARS BRIGHTER AB We present new radial and rotational velocities for 595 nearby early F dwarfs, based on digital spectra cross-correlated with individually optimised synthetic template spectra. The selection of optimum templates, the determination of rotational velocities, and the extraction of velocities from the blended spectra of double-lined spectroscopic binaries are discussed in some detail. We find 170 spectroscopic binaries in the sample and determine orbits for 18 double-lined and 2 single-lined binaries, including some spectroscopic triples. 73 stars are listed with too rapid rotation to yield useful radial velocities (i.e. v sin i > 120 km s(-1)). We discuss the binary frequency in the sample, and the influence of unrecognised binaries on the definition of clean metallicity groups of young F dwarfs and the determination of their kinematical properties. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Nordstrom, B (reprint author), NIELS BOHR INST ASTRON PHYS & GEOPHYS,ASTRON OBSERV,JULIANE MARIES VEJ 30,DK-2100 COPENHAGEN,DENMARK. NR 22 TC 49 Z9 51 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 NOV PY 1997 VL 126 IS 1 BP 21 EP 30 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YH004 UT WOS:A1997YH00400004 ER PT J AU Srinivasan, R Boyle, PJ Buckley, JH CarterLewis, DA Catanase, M Cawley, MF Colombo, E Fegan, DJ Finley, JP Gaidos, JA Gordo, JB Hillas, AM Krennrich, F Lamb, RC Lessard, RW McEnery, JM Moriarty, P Quinn, J Rose, HJ Samuelson, FW Sembroski, G Weekes, TC Wilson, C Zweerink, J AF Srinivasan, R Boyle, PJ Buckley, JH CarterLewis, DA Catanase, M Cawley, MF Colombo, E Fegan, DJ Finley, JP Gaidos, JA Gordo, JB Hillas, AM Krennrich, F Lamb, RC Lessard, RW McEnery, JM Moriarty, P Quinn, J Rose, HJ Samuelson, FW Sembroski, G Weekes, TC Wilson, C Zweerink, J TI Very high-energy observations of PSR B1951+32 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays, observations; pulsars, individual (PSR B1951+32); supernova remnants ID GAMMA-RAYS; PULSAR; RADIATION; NEBULA AB PSR B1951 + 32 is a gamma-ray pulsar detected by the Energetic Gamma Ray Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The pulsar energy spectrum is consistent with an unbroken power law with differential photon index of -1.8 +/- 0.1 between 50 MeV and 10 GeV. The EGRET data shows no evidence for a spectral turnover. Here we report on the first observations of PSR B1951 + 32 beyond 30 GeV. The observations were carried out with the 10 m gamma-ray telescope at the Whipple Observatory on Mount Hopkins, Arizona. In 8.1 hours of observation we find no evidence for steady or periodic emission from PSR B1951 + 32 above similar to 260 GeV, Flux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models. C1 NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. IOWA STATE UNIV,DEPT PHYS & ASTRON,AMES,IA 50011. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. UNIV LEEDS,DEPT PHYS & ASTRON,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. CALTECH,SPACE RADIAT LAB,PASADENA,CA 91125. REG TECH COLL,GALWAY,IRELAND. HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,AMADO,AZ 85645. RP Srinivasan, R (reprint author), PURDUE UNIV,DEPT PHYS,W LAFAYETTE,IN 47907, USA. NR 31 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 NOV 1 PY 1997 VL 489 IS 1 BP 170 EP 174 DI 10.1086/304781 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YE139 UT WOS:A1997YE13900016 ER PT J AU Close, LM Roddier, F Hora, JL Graves, JE Northcott, M Roddier, C Hoffman, WF Dayal, A Fazio, GG Deutsch, LK AF Close, LM Roddier, F Hora, JL Graves, JE Northcott, M Roddier, C Hoffman, WF Dayal, A Fazio, GG Deutsch, LK TI Adaptive optics infrared imaging polarimetry and optical HST imaging of Hubble's variable nebula (R Monocerotis NGC 2261): A close look at a very young active Herbig Ae/Be star SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; astrometry; circumstellar matter; stars, formation; stars, imaging; stars, individual (R Monocerotis); stars, pre-main-sequence; techniques, image processing ID STANDARD STARS; ARRAY CAMERA; HL TAURI; POLARIZATION; TELESCOPE; NGC-2261; EMISSION; OUTFLOW; ORIGIN; SYSTEM AB We present high-resolution (FWHM = 0''.2) near-IR (J, H, and K') adaptive optics images of the Herbig Ae/Be star R Monocerotis. Optical Hubble Space Telescope (HST) WFPC2 PC camera archival images are also presented. For the first time, adaptive optics was utilized to make high-resolution (FWHM = 0''.2) IR-imaging polarimetry maps of R Mon. In addition, the first mld-IR array images (at 11.7 and 20.8 mu m) of R Mon have been obtained. We also present new 3.16, 3.93, and 4.67 mu m images. We have found that R Mon is a 0''.69 binary star with a companion that dereddens onto the classical T Tauri locus. Based on the near-infrared photometry of this companion we believe it is a 1,5 M., very young (< 3 x 10(5) yr) classical T Tauri star. The close presence of a young companion suggests that R Mon itself is a rare example of a very young isolated massive star. At the highest resolutions, R Mon is revealed to be extended by similar to 0''.1 east-west, and similar to 0''.05 north-south in the visible. The young R Mon star is not directly visible in the optical but appears as a resolved conical reflection nebula in scattered light. At infrared wavelengths, the dense circumstellar dust is penetrated and R Mon appears to be an unresolved point source located at 0''.06 +/- 0''.02 south of the peak optical flux. The large-scale optical-IR morphology of R Mon and its large reflection nebula (NGC 2261) suggests a thin bipolar parabolic shell of dust. The appearance of the parabolic shell is consistent with an inclination of 20 degrees +/- 10 degrees from the plane of the sky. This inclination implies that R Mon is located 760(-280)(+800) pc distant based on previous proper-motion and radial velocity measurements of R Mon's jet. Our high-resolution (FWHM similar to 0''.2) adaptive optics infrared polarimetry maps agree with the current interpretation that NGC 2261 is a reflection nebula illuminated by R Mon. Interior to the parabolic shell there is a complex of twisted filaments along the eastern edge. These filaments resemble a double-helical structure which is well described by a power law from similar to 10(3) to 10(5) AU from R Mon. This double helix may trace a twisted magnetic field above R Mon. Based on H I emission-line ratios, we find the direct extinction toward R Mon to be A(V) = 13.1 mag in the infrared (lambda > 1.28 mu m), falling to a lower value of A(V) = 3.6 mag in the optical (lambda < 1.28 mu m), where scattered light increasingly lowers the effective extinction in the line ratios. The large A, = 13.1 extinction is likely due to the dusty atmosphere of an inclined R similar to 100 AU optically thick accretion disk: surrounding R Mon. A simple model of such an accretion disk + star system (with M-acc similar to 8 x 10(-5) M., yr(-1), M-* 10.4 M-., R-* = 2 R., and T-* similar to 3.5 x 10(4) K) reproduces the observed dereddened R Mon spectral energy distribution (SED) from the optical (0.4 mu m) to the millimeter region. Consideration of the lower extinction (A(V) = 3.6) on the path followed by the scattered visible light eliminated ani need for an inner ''gap'' in the accretion disk model to reproduce the SED. In general, young stellar objects (YSOs) that are obscured in the optical but directly visible in the infrared will have different effective optical and infrared extinctions. Infrared extinctions derived from optical observations dominated by scattered Light will be underestimates of the true IR extinction along the direct path. The use of an independent estimator of both the optical and infrared extinctions such as common upper-level H I recombination lines is highly desirable. The utilization of the correct optical and infrared extinctions may relieve the need for optically thin inner-disk gaps to explain YSO near-IR SEDs. C1 UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. BOSTON UNIV,DEPT ASTRON,BOSTON,MA 02215. RP Close, LM (reprint author), UNIV HAWAII,INST ASTRON,2680 WOODLAWN DR,HONOLULU,HI 96822, USA. OI Hora, Joseph/0000-0002-5599-4650 NR 55 TC 49 Z9 49 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 NOV 1 PY 1997 VL 489 IS 1 BP 210 EP & DI 10.1086/304777 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YE139 UT WOS:A1997YE13900019 ER PT J AU Hameury, JM Lasota, JP McClintock, JE Narayan, R AF Hameury, JM Lasota, JP McClintock, JE Narayan, R TI Advection-dominated flows around black holes and the X-ray delay in the outburst of GRO J1655-40 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars, individual (GRO J1655-40); X-rays, stars ID DWARF NOVA OUTBURSTS; DISK-INSTABILITY MODEL; ACCRETION DISK; TRANSIENTS; TRANSITION; EVOLUTION; STARS AB We show that the time delay between the optical and X-ray outbursts of the black hole soft X-ray transient source GRO J1655-40, observed in 1996 April, suggests that the accretion flow in this object must consist of two components: a cold outer accretion disk and an extremely hot inner advection-dominated accretion flow (ADAF). In quiescence, the model predicts a spectrum that is in good agreement with observations, with most Of the observed radiation coming from the ADAF. By fitting the observed spectrum, we estimate the mass accretion rate of the quiescent system and the transition radius between the disk and the ADAF. We present a detailed numerical simulation of a dwarf nova-type instability in the outer disk. The resulting heat front reaches the ADAF cavity promptly; however, it must then propagate inward slowly on a viscous timescale, thereby delaying the onset of the X-ray flux. The model reproduces the observed optical and X-ray light curves of the 1996 April outburst, as well. as the 6 day X-ray delay. Further, the model gives an independent estimate of the quiescent mass accretion rate that is in very good agreement with the rate estimated from fitting the quiescent spectrum. We show that a pure thin disk model without an ADAF zone requires significant tuning to explain the X-ray delay; moreover, such a model does not explain the quiescent X-ray emission of GRO J1655-40. C1 OBSERV PARIS,SECT MEUDON,DEPT ASTROPHYS RELAT & COSMOL,F-92195 MEUDON,FRANCE. CNRS,UPR 176,F-92195 MEUDON,FRANCE. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Hameury, JM (reprint author), OBSERV STRASBOURG,CNRS,URA 1280,11 RUE UNIV,F-67000 STRASBOURG,FRANCE. OI Narayan, Ramesh/0000-0002-1919-2730 NR 47 TC 93 Z9 93 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 NOV 1 PY 1997 VL 489 IS 1 BP 234 EP 243 DI 10.1086/304780 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YE139 UT WOS:A1997YE13900022 ER PT J AU Raymond, JC Blair, WP Long, KS AF Raymond, JC Blair, WP Long, KS TI Hopkins ultraviolet telescope observations of H-2 emission from HH 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular processes; shock waves; stars, pre-main-sequence; ultraviolet, stars ID HERBIG-HARO OBJECTS; MOLECULAR-HYDROGEN; PROTOSTELLAR JETS; SHOCK-MODELS; BOW SHOCK; SPECTRA; PERFORMANCE; CALIBRATION; SIMULATIONS; EXCITATION AB The Hopkins Ultraviolet Telescope spectrum of HH 2 shows Lyman band emission below 1200 Angstrom, and it reveals H-2 bands in the quasi-continuum at longer wavelengths. The H-2 emission could arise either from Ly alpha fluorescence (as in other HH objects) or from collisional excitation by hot electrons. The fluorescence hypothesis encounters some difficulty in explaining the lack of individual strong features, while the collisional hypothesis must explain the mixing of hot electrons into the molecular gas before photoionization or collisions with H atoms dissociate the molecules. The spectrum also provides a stringent upper limit to the O VI flux. The upper limit appears to conflict badly with the predictions of bow-shock models that match the observed line widths of HII 2A' and HH 2H. C1 JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. RP Raymond, JC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 41 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 NOV 1 PY 1997 VL 489 IS 1 BP 314 EP 318 DI 10.1086/304787 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YE139 UT WOS:A1997YE13900028 ER PT J AU Habbal, SR Woo, R Fineschi, S ONeal, R Kohl, J Noci, G Korendyke, C AF Habbal, SR Woo, R Fineschi, S ONeal, R Kohl, J Noci, G Korendyke, C TI Origins of the slow and the ubiquitous fast solar wind SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun, corona; Sun, solar wind ID POLAR CORONAL HOLE AB We present in this Letter the first coordinated radio occultation measurements and ultraviolet observations of the inner corona below 5.5R(s), obtained during the Galileo solar conjunction in 1997 January, to establish the origin of the slow solar wind. Limits on the flow speed are derived from the Doppler dimming of the resonantly scattered component of the oxygen 1032 and 1037.6 Angstrom lines as measured with the ultraviolet coronagraph spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO). White light images of the corona from the large-angle spectroscopic coronagraph (LASCO) on SOHO taken simultaneously are used to place the Doppler radio scintillation and ultraviolet measurements in the context of coronal structures. These combined observations provide the first direct confirmation of the view recently proposed by Woo & Martin that the slow solar wind is associated with the axes, also known as stalks, of streamers. Furthermore, the ultraviolet observations also show how the fast solar wind is ubiquitous in the inner corona and that a velocity shear between the fast and slow solar wind develops along the streamer stalks. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. UNIV FLORENCE,I-50125 FLORENCE,ITALY. USN,RES LAB,EO HULBURT CTR SPACE RES,WASHINGTON,DC 20375. RP Habbal, SR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 30 TC 102 Z9 104 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 NOV 1 PY 1997 VL 489 IS 1 BP L103 EP & DI 10.1086/310970 PN 2 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YE140 UT WOS:A1997YE14000025 ER PT J AU Wanders, I Peterson, BM Alloin, D Ayres, TR Clavel, J Crenshaw, DM Horne, K Kriss, GA Krolik, JH Malkan, MA Netzer, H OBrien, PT Reichert, GA RodriguezPascual, PM Wamsteker, W Alexander, T Anderson, KSJ Benitez, E Bochkarev, NG Burenkov, AN Cheng, FZ Collier, SJ Comastri, A Dietrich, M DultzinHacyan, D Espey, BR Filippenko, AV Gaskell, CM George, IM Goad, MR Ho, LC Kaspi, S Kollatschny, W Korista, KT Laor, A MacAlpine, GM Mignoli, M Morris, SL Nandra, K Penton, S Pogge, RW Ptak, RL RodriguezEspinoza, JM SantosLleo, M Shapovalova, AI Shull, JM Snedden, SA Sparke, LS Stirpe, GM Sun, WH Turner, TJ Ulrich, MH Wang, TG Wei, C Welsh, WF Xue, SJ Zou, ZL AF Wanders, I Peterson, BM Alloin, D Ayres, TR Clavel, J Crenshaw, DM Horne, K Kriss, GA Krolik, JH Malkan, MA Netzer, H OBrien, PT Reichert, GA RodriguezPascual, PM Wamsteker, W Alexander, T Anderson, KSJ Benitez, E Bochkarev, NG Burenkov, AN Cheng, FZ Collier, SJ Comastri, A Dietrich, M DultzinHacyan, D Espey, BR Filippenko, AV Gaskell, CM George, IM Goad, MR Ho, LC Kaspi, S Kollatschny, W Korista, KT Laor, A MacAlpine, GM Mignoli, M Morris, SL Nandra, K Penton, S Pogge, RW Ptak, RL RodriguezEspinoza, JM SantosLleo, M Shapovalova, AI Shull, JM Snedden, SA Sparke, LS Stirpe, GM Sun, WH Turner, TJ Ulrich, MH Wang, TG Wei, C Welsh, WF Xue, SJ Zou, ZL TI Steps toward determination of the size and structure of the broad-line region in active galactic nuclei .11. Intensive monitoring of the ultraviolet spectrum of NGC 7469 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies, active; galaxies, individual (NGC 7469); galaxies, Seyfert; ultraviolet, galaxies ID SHORT-TIMESCALE VARIABILITY; MULTIWAVELENGTH OBSERVATIONS; SEYFERT-GALAXIES; EMISSION-LINES; NGC-5548; CONTINUUM; NGC-4151; QUASARS; IUE; GEOMETRY AB From 1996 June 10 to July 29, the International Ultraviolet Explorer monitored the Seyfert 1 galaxy NGC 7469 continuously in an attempt to measure time delays between the continuum and emission-line fluxes. From the time delays, one can estimate the size of the region dominating the production of the UV emission lines in this source. We find the strong UV emission lines to respond to continuum variations with time delays of about 2.(d)3-3.(d)1 for Ly alpha, 2.(d)7 for C IV lambda 1549, 1.(d)9-2.(d)4 for N V lambda 1240, 1.(d)7-1.(d)8 for Si IV lambda 1400, and 0.(d)7-1.(d)0 for He II lambda 1640. The most remarkable result, however, is the detection of apparent time delays between the different UV continuum bands. With respect to the UV continuum flux at 1315 Angstrom, the flux at 1485 Angstrom, 1740 Angstrom, and 1825 Angstrom lags with time delays of 0.(d)21, 0.(d)35, and 0.(d)28, respectively. Determination of the significance of this detection is somewhat problematic since it depends on accurate estimation of the uncertainties in the lag measurements, which are difficult to assess. We attempt to estimate the uncertainties in the time delays through Monte Carlo simulations, and these yield estimates of similar to 0.(d)07 for the 1 sigma uncertainties in the interband continuum time delays. Possible explanations for the delays include the existence of a continuum-flux reprocessing region close to the central source and/or a contamination of the continuum flux with a very broad time-delayed emission feature such as the Balmer continuum or merged Fe II multiplets. C1 UNIV ST ANDREWS, SCH PHYS & ASTRON, ST ANDREWS KY16 9SS, FIFE, SCOTLAND. CTR ETUD SACLAY, SERV ASTROPHYS, F-91191 GIF SUR YVETTE, FRANCE. UNIV COLORADO, CTR ASTROPHYS & SPACE ASTRON, BOULDER, CO 80309 USA. EUROPEAN SPACE AGCY, ISO PROJECT, MADRID 28080, SPAIN. NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, COMP SCI CORP, GREENBELT, MD 20771 USA. JOHNS HOPKINS UNIV, DEPT PHYS & ASTRON, BALTIMORE, MD 21218 USA. UNIV CALIF LOS ANGELES, DEPT ASTRON, LOS ANGELES, CA 90024 USA. TEL AVIV UNIV, RAYMOND & BEVERLY SACKLER FAC EXACT SCI, SCH PHYS & ASTRON, IL-69978 TEL AVIV, ISRAEL. TEL AVIV UNIV, RAYMOND & BEVERLY SACKLER FAC EXACT SCI, WISE OBSERV, IL-69978 TEL AVIV, ISRAEL. UNIV LEICESTER, DEPT PHYS & ASTRON, LEICESTER LE1 7RH, LEICS, ENGLAND. EUROPEAN SPACE AGCY, IUE OBSERV, MADRID 28080, SPAIN. MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. NEW MEXICO STATE UNIV, DEPT ASTRON, DEPT 4500, LAS CRUCES, NM 88003 USA. UNIV NACL AUTONOMA MEXICO, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. MOSCOW MV LOMONOSOV STATE UNIV, STERNBERG ASTRON INST, MOSCOW 119899, RUSSIA. RUSSIAN ACAD SCI, SPECIAL ASTROPHYS OBSERV, NIZHNII ARKHYZ 357147, KARACHAJ CHERKE, RUSSIA. UNIV SCI & TECHNOL, CTR ASTROPHYS, HEFEI, PEOPLES R CHINA. OSSERVATORIO ASTRON BOLOGNA, I-40126 BOLOGNA, ITALY. LANDESSTERNWARTE HEIDELBERG, KONIGSTUHL, D-69117 HEIDELBERG, GERMANY. UNIV CALIF BERKELEY, DEPT ASTRON, BERKELEY, CA 94720 USA. UNIV NEBRASKA, DEPT PHYS & ASTRON, LINCOLN, NE 68588 USA. NASA, GODDARD SPACE FLIGHT CTR, HIGH ENERGY ASTROPHYS LAB, GREENBELT, MD 20771 USA. UNIV SPACE RES ASSOC, WASHINGTON, DC USA. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV STERNWARTE GOTTINGEN, D-37083 GOTTINGEN, GERMANY. UNIV KENTUCKY, DEPT PHYS & ASTRON, LEXINGTON, KY 40506 USA. TECHNION ISRAEL INST TECHNOL, DEPT PHYS, IL-32000 HAIFA, ISRAEL. UNIV MICHIGAN, DEPT ASTRON, ANN ARBOR, MI 48109 USA. DOMINION ASTROPHYS OBSERV, VICTORIA, BC V8X 4M6, CANADA. BOWLING GREEN STATE UNIV, DEPT PHYS & ASTRON, BOWLING GREEN, OH 43403 USA. INST ASTROFIS CANARIAS, E-38200 LA LAGUNA, TENERIFE, SPAIN. LAEFF, E-28080 MADRID, SPAIN. UNIV COLORADO, JOINT INST LAB ASTROPHYS, BOULDER, CO 80309 USA. NATL INST STAND & TECHNOL, BOULDER, CO 80309 USA. UNIV WISCONSIN, DEPT ASTRON, MADISON, WI 53706 USA. NATL CENT UNIV, INST ASTRON, CHUNGLI 32054, TAIWAN. EUROPEAN SO OBSERV, D-85748 GARCHING, GERMANY. UNIV TEXAS, MCDONALD OBSERV, AUSTIN, TX 78712 USA. UNIV TEXAS, DEPT ASTRON, RLM 15308, AUSTIN, TX 78712 USA. CHINESE ACAD SCI, BEIJING ASTRON OBSERV, BEIJING 100080, PEOPLES R CHINA. RP Wanders, I (reprint author), OHIO STATE UNIV, DEPT ASTRON, 174 W 18TH AVE, COLUMBUS, OH 43210 USA. RI Morris, Simon/G-7981-2011; 王, 挺贵/B-8293-2013; Stirpe, Giovanna/O-9393-2015; Mignoli, Marco/O-9426-2015; Comastri, Andrea/O-9543-2015; OI Morris, Simon/0000-0003-4866-110X; Stirpe, Giovanna/0000-0002-3702-8731; Mignoli, Marco/0000-0002-9087-2835; Comastri, Andrea/0000-0003-3451-9970; Espey, Brian/0000-0002-2457-1380; Gaskell, C/0000-0003-4888-2009; SUN, WEI-HSIN/0000-0002-7474-8658 NR 39 TC 121 Z9 121 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 1997 VL 113 IS 1 BP 69 EP 88 DI 10.1086/313054 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA YD367 UT WOS:A1997YD36700003 ER EF