%R=BibCode
%A=Authors
%B=Abstract
%c=Copyright
%D=Date of publication
%E=Electronic file
%F=Original File
%I=Institute and/or Footnotes
%J-last page
%K=Keywords
%T=Title

%R 1998PASP..110.1389B
%F ori/PASPv110n754
%J-1393
%T A Planet with a 3.1 Day Period around a Solar Twin(1). (Research Note).
%A Butler, R.Paul (2)
%A Marcy, Geoffrey W. (3)
%A Vogt, Steven S. (4)
%A Apps, Kevin (5)
%B  Doppler measurements from the Keck/HIRES spectrometer of the G3 V star
   HD 187123 reveal Keplerian variations with a period of 3.097 days and a semiamplitude
   of 72 m.s^-1^. An orbital fit yields a companion mass of M=0.52 M_JUP_/ {\rf
   sin}i, a semimajor axis of a=0.042 AU, and an eccentricity of e=0.03 (consistent
   with zero). HD 187123 appears similar to the Sun in mass, age, chromosphere,
   and rotation rate. Although unlikely, non-Keplerian explanations for the
   Doppler variations, such as spots and pulsation, cannot be ruled out and
   require future photometry and spectroscopy.
%K Stars: Planetary Systems
%K Stars: Individual: Henry Draper Number: HD 187123
%K Research Notes
%I (1) Based on observations obtained at the W. M. Keck Observatory, which
   is operated jointly by the University of California and the California Institute
   of Technology.
%I (2) Anglo-Australian Observatory, P.O. Box 296, Epping, NSW 1710, Australia;
   (paul@aaoepp.aao.gov.au).
%I (3) Department of Physics and Astronomy, San Francisco State University,
   San Francisco, CA 94132; and Department of Astronomy, University of California
   at Berkeley, Berkeley, CA 94720.
%I (4) UCO/Lick Observatory, University of California at Santa Cruz, Santa
   Cruz, CA, 95064.
%I (5) Physics and Astronomy, University of Sussex, Falmer, Brighton BN1
   9QJ, England, UK.

%R 1998PASP..110.1394H
%F ori/PASPv110n754
%J-1399
%T EUVE J0425.6-5714: A Newly Discovered AM Herculis Star.
%A Halpern, J.P.
%A Leighly, K.M.
%I Columbia Astrophysics, Columbia University, 550 West 120th Street, New York,
   NY 10027
%A Marshall, H.L.
%I Eureka Scientific, Inc., 2452 Delmer Street, Suite 100, Oakland, CA 94602
%A Eracleous, M. (1)
%I Department of Astronomy, University of California, Berkeley, CA 94720
%A Storchi-Bergmann, T. (2)
%I Departamento de Astronomia, IF-UFRGS, CP 15051, CEP 91501-970, Porto Allegre,
   RS, Brazil
%B  We detected a new AM Her star serendipitously in a 25 day observation
   with the {\em EUVE} satellite. A coherent period of 85.82 minutes is present
   in the {\em EUVE} Deep Survey imager light curve of this source. A spectroscopic
   optical identification is made with a 19th magnitude blue star that has H
   and He emission lines, and broad cyclotron humps typical of a magnetic cataclysmic
   variable. A lower limit to the polar magnetic field of 50 MG is estimated
   from the spacing of the cyclotron harmonics. EUVE J0425.6-5714 is also detected
   in archival {\em ROSAT} HRI observations spanning 2 months, and its stable
   and highly structured light curve permits us to fit a coherent ephemeris
   linking the {\em ROSAT} and {\em EUVE} data over a 1.3 yr gap. The derived
   period is 85.82107+/-0.00020 minutes, and the ephemeris should be accurate
   to 0.1 cycles until the year 2005. A narrow but partial X-ray eclipse suggests
   that this object belongs to the group of AM Her stars whose viewing geometry
   is such that the accretion stream periodically occults the soft X-ray emitting
   accretion spot on the surface of the white dwarf. A nondetection of hard
   X-rays from {\em ASCA} observations that are contemporaneous with the {\em
   ROSAT} HRI shows that the soft X-rays must dominate by at least an order
   of magnitude, which is consistent with a known trend among AM Her stars with
   large magnetic fields. This object should not be confused with the Seyfert
   galaxy 1H 0419-577 (=LB 1727), another X-ray/EUV source that lies only 3'.95
   away and that was the principal target of these monitoring observations.
%K Stars: Novae, Cataclysmic Variables
%K Stars: Individual: Alphanumeric: \objS{RX J0425.6-5714}{EUVE J0425.6-5714}
%K X-Rays
%I (1) Hubble Fellow.
%I (2) Visiting Astronomer, Cerro Tololo Inter-American Observatory, National
   Optical Astronomy Observatories, which is operated by AURA, Inc., under a
   cooperative agreement with the National Science Foundation.

%R 1998PASP..110.1400K
%F ori/PASPv110n754
%J-1404
%T The 1996 Superoutburst of the New SU UMa-Type Dwarf Nova HS Virginis.
%A Kato, Taichi
%A Nogami, Daisaku
%A Masuda, Seiji ,
%A Baba, Hajime
%I Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku,
   Kyoto 606-8502, Japan; (tkato@kusastro.kyoto-u.ac.jp), (nogami@kusastro.kyoto-u.ac.jp),
   (masuda@kusastro.kyoto-u.ac.jp), (baba@kusastro.kyoto-u.ac.jp)
%B  We report long-term and time-resolved photometric observations of the
   dwarf nova HS Vir (=PG 1341-079). Time-resolved photometry during the bright
   outburst in 1996 March revealed superhumps with a period of 0.08059+/-0.00003
   days, which first firmly confirmed HS Vir as a genuine member of SU UMa-type
   dwarf novae. HS Vir is rather unusual in the smallness (2.7-3.5 mag for brightest
   superoutbursts) of outburst amplitudes. The marked diversity inferred from
   the comparison with SX LMi may reflect different mechanisms responsible for
   the smallness of outburst amplitudes in these dwarf novae.
%K Stars: Novae, Cataclysmic Variables
%K Stars: Individual: Constellation Name: HS Virginis
%K Stars: White Dwarfs

%R 1998PASP..110.1405T
%F ori/PASPv110n754
%J-1411
%T Spectroscopy of the Cataclysmic Binaries CY Lyrae, TW Trianguli, and VW Vulpeculae(1).
%A Thorstensen, John R.
%A Taylor, Cynthia J.
%I Department of Physics and Astronomy, 6127 Wilder Laboratory, Dartmouth College,
   Hanover, NH 03755-3528; (thorstensen@dartmouth.edu)
%A Kemp, Jonathan
%I Department of Astronomy, Columbia University, 550 West 120th Street, New
   York, NY 10027; (jonathan@astro.columbia.edu)
%B  From H{alpha} radial velocities taken in quiescence we find orbital
   periods of 0.1591+/-0.0004 days, or 3.82 hr, for CY Lyr, 0.207584+/-0.000007
   days, or 4.98 hr, for TW Tri, and 0.16870+/-0.00007 days, or 4.05 hr, for VW
   Vul. The period of VW Vul is much longer than a previously published value,
   and the spectrum suggests that we caught this Z Cam star in standstill. The
   revision of VW Vul's period resolves its problematic status as a short-period
   dwarf nova that did not show superoutbursts. The quiescent spectra of CY
   Lyr and TW Tri are typical of dwarf novae between outbursts, and both show
   the contribution of a late-type secondary, of type ~M3.5 in CY Lyr and ~M1
   in TW Tri. From the M-dwarf contribution in the quiescent spectrum we estimate
   distances of ~330 pc for CY Lyr and ~800 pc for TW Tri. On 1997 June 30 UT
   we observed CY Lyr in a rise to outburst, and we present spectra obtained
   approximately hourly as the object brightened.
%K Stars: Binaries: Close
%K Stars: Binaries: Spectroscopic
%K Stars: Distances
%K Stars: Novae, Cataclysmic Variables
%I (1) Based on observations obtained at MDM Observatory.

%R 1998PASP..110.1412B
%F ori/PASPv110n754
%J-1415
%T A Search for an Emission-Line Region in the Hydrogen-deficient Carbon Star
   HD 182040.
%A Brunner, Andrew R.
%A Clayton, Geoffrey C.
%I Department of Physics and Astronomy, Louisiana State University, Baton Rouge,
   LA 70803; (brunner@rouge.phys.lsu.edu), (gclayton@rouge.phys.lsu.edu)
%A Ayres, T.R.
%I CASA, University of Colorado, Boulder, CO 80309; (ayres@vulcan.Colorado.edu)
%B  A long-exposure short-wavelength {\em IUE} spectrum of the hydrogen-deficient
   carbon (HdC) star HD 182040 does not show any detectable emission in the
   C II {lambda}1335 line. It is not certain whether this absence of emission
   is intrinsic or due to the large uncertainties in the distance, absolute
   luminosity, and reddening toward HD 182040. If intrinsic, this absence of
   emission along with the absence of an IR excess from circumstellar dust imply
   that little or no mass loss is occurring at present from this star even though
   it is very similar spectroscopically to the R Coronae Borealis (RCB) stars.
   This result also suggests that the emission-line gas and the circumstellar
   dust may result from the same mass-loss mechanism in the RCB stars.
%K Stars: Circumstellar Matter
%K Infrared: Stars
%K Stars: Carbon
%K Stars: Chemically Peculiar
%K Ultraviolet: Stars

%R 1998PASP..110.1416M
%F ori/PASPv110n754
%J-1422
%T The Wolf-Rayet Binary WR 141 (WN5o + O5 V-III) Revisited.
%A Marchenko, Sergey V. (1)
%A Moffat, Anthony F.J. (1)
%A Eenens, Philippe R.J. (2)
%B  We combine all previously published radial velocity measurements of
   the spectroscopic binary WR 141 with new CCD data from 1988-1989 and 1992,
   complemented by polarimetric broadband measurements from 1989. This enables
   us to refine the orbital elements [P=21.6895 days, e=0.018, K_WR_=118 km.s^-1^, 
   K_O_=163-194 km.s^-1^], estimate the masses of the components [M_WR_=36-54
   M_{sun}_, M_O_=26-33 M_{sun}_ for orbital inclination i=68{deg}], and restore
   the spectrum of the O star via a specifically designed decomposition algorithm.
   Along with pronounced erratic variations, the spectral lines of the WR component
   demonstrate systematic phase-locked variability induced by the radiation
   field of the hot, luminous O companion.
%K Stars: Binaries: Spectroscopic
%K Stars: Wolf-Rayet
%K Stars: Individual: Alphanumeric: WR 141
%I (1) D\'epartement de Physique, Universit\'e de Montr\'eal, C.P. 6128, Succ.
   Centre-Ville, Montr\'eal, Qu\'ebec, Canada, H3C 3J7; and Observatoire du Mont
   M\'egantic; (sergey@astro.umontreal.ca), (moffat@astro.umontreal.ca).
%I (2) Departamento de Astronom\'ia, Universidad de Guanajuato, Apdo. Postal
   144, 36000 Guanajuato Gto, Mexico; (eenens@carina.astro.ugto.mx).

%R 1998PASP..110.1423R
%F ori/PASPv110n754
%J-1427
%T H{alpha} Emission Stars in the Case-Hamburg Luminous Stars Surveys.
%A Reed, B.Cameron
%I Department of Physics, Alma College, Alma, MI 48801; (reed@alma.edu)
%B  MK spectral classifications of over 2500 Case-Hamburg luminous stars
   are examined to determine whether those for which H{alpha} was reported in
   emission in the original surveys (but for which blue-region emission was
   not noted) are more likely to have MK classifications indicating blue-region
   emission than their non-H{alpha} counterparts; this proves to be the case.
   In addition, stars with H{alpha} emission are less likely to be supergiants
   than their non-H{alpha} counterparts, and, when emission is indicated in
   the MK classification, one is much more likely to be dealing with a luminosity
   class V or III star than a bright giant or supergiant.
%K Stars: Early-Type
%K Stars: Emission-Line, Be

%R 1998PASP..110.1428P
%F ori/PASPv110n754
%J-1430
%T Period Changes, Evolution, and Multiperiodicity in the Peculiar Population
   II Cepheid RU Camelopardalis.
%A Percy, John R.
%A Hale, Jonathan
%I Erindale Campus, and Department of Astronomy, University of Toronto, Mississauga,
   ON, Canada L5L 1C6; (jpercy@erin.utoronto.ca)
%B  We have studied the period change in the peculiar Population II Cepheid
   RU Cam, which abruptly decreased in amplitude in 1965-1966. The {\em O}-{\em
   C} diagram prior to 1965-1966 can best be explained as the superposition
   of small, random, cycle-to-cycle changes in period, plus a constant linear
   decrease whose timescale (31,000 yr) is consistent with evolutionary predictions.
   The {\em O}-{\em C} diagram after 1965-1966 can best be explained as the
   superposition of much larger random, cycle-to-cycle changes (which mask the
   evolutionary changes), plus wavelike changes in {\em O}-{\em C} on a timescale
   of 10-20 periods. These--and the variations in the amplitude of the star that
   occur on the same timescale--may be due to multiperiodicity.
%K Stars: Variables: Cepheids
%K Stars: AGB and Post-AGB
%K Stars: Evolution
%K Stars: Individual: Constellation Name: RU Camelopardalis
%K Stars: Peculiar
%K Stars: Population II

%R 1998PASP..110.1431P
%F ori/PASPv110n754
%J-1433
%T Pulsation Modes in Small-Amplitude Red Variable Stars.
%A Percy, John R.
%A Parkes, Michael
%I Erindale Campus and Department of Astronomy, University of Toronto, Mississauga,
   ON, Canada L5L 1C6; (jpercy@erin.utoronto.ca)
%B  We have investigated the pulsation modes of small-amplitude red variables
   with well-determined periods and accurate {\em Hipparcos} parallaxes by comparing
   observational and theoretical {\em Q}-values. In our sample of 13 stars,
   one appears to be pulsating in the third overtone, nine in the first or second
   overtone, and three in the fundamental or first overtone. This result is
   consistent with the predictions of recent pulsation models by Xiong et al.
%K Stars: AGB and Post-AGB
%K Stars: Late-Type
%K Stars: Oscillations
%K Stars: Variables: Other

%R 1998PASP..110.1434S
%F ori/PASPv110n754
%J-1447
%T Digital Objective Prism Spectroscopy and Astrometry: Quantitative Methods
   and Application to High-Velocity Stars.
%A Stock, Jurgen (1)(2)
%I Centro de Investigaciones de Astronomia, Merida, Venezuela
%A Rose, James A. (1)
%I Department of Physics and Astronomy, University of North Carolina, Chapel
   Hill, NC 27599and
%A Agostinho, Rui J.
%I Department of Physics, University of Lisbon, Lisbon, Portugal
%B  We describe methods for extracting quantitative spectra and astrometric
   positions from objective prism plates. In particular, we have studied 7161
   stars in eight fields along the south Galactic meridian using the 6{deg}+4{deg}
   objective prisms on the Curtis Schmidt telescope at Cerro Tololo Inter-American
   Observatory. In this paper we concentrate on techniques for deriving radial
   velocities and astrometric positions from opposed dispersion plate pairs.
   For our data the typical accuracy in radial velocity is ~8 km.s^-1^. A catalog
   of 108 stars with high radial velocities is presented, which is complete
   (and unbiased in either kinematics or metallicity) to a limiting {\em B}
   magnitude of 12.5 in the eight fields studied. Only two of this sample of
   108 stars have previously reported radial velocities.
%K Galaxy: Kinematics and Dynamics
%K Stars: Kinematics
%K Astrometry
%K Techniques: Radial Velocities
%I (1) Visiting Astronomer, Cerro Tololo Inter-American Observatory, National
   Optical Astronomy Observatories, operated by the Association of Universities
   for Research in Astronomy, Inc., under contract with the National Science
   Foundation.
%I (2) Guest Investigator, University of Lisbon, Lisbon, Portugal.

%R 1998PASP..110.1448S
%F ori/PASPv110n754
%J-1463
%T On the Photometric Consequences of Charge-Transfer Inefficiency in WFPC2.
%A Stetson, Peter B. (1)(2)
%I Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National
   Research Council, 5071 West Saanich Road, Victoria, BC V8X 4M6, Canada; and
   Mount Stromlo and Siding Spring Observatories, Institute of Advanced Studies,
   Australian National University, Weston Creek, ACT 2611, Australia; (peter.stetson@hia.nrc.ca)
%B  Charge-transfer effects in photometry with Wide Field Planetary Camera
   2 (WFPC2) aboard the {\em Hubble Space Telescope} are investigated by a comparison
   of WFPC2 observations with ground-based photometry for the Galactic globular
   clusters {omega} Centauri and NGC 2419. Simple numerical formulae describing
   the fraction of lost signal as functions of position on the detector, stellar
   brightness, and the diffuse sky brightness recorded in an image are presented,
   and the resulting corrections are compared with those previously derived
   by Whitmore & Heyer. Significant lost-charge effects are seen that are proportional
   to both the {\em Y}-coordinate (i.e., the number of shifts along the parallel
   register during readout) and the {\em X}-coordinate (number of shifts along
   the serial register). A ``typical'' star image (one containing ~ 10^4^ photoelectrons)
   near the center of a ``typical'' intermediate-length exposure (one with a diffuse
   sky brightness of ~10 {\em e}^-^.pixel^-1^, obtained at a camera temperature
   of -88{deg} C) loses approximately 2% of its electrons to charge traps during
   readout; a star in the corner of the image most remote from the readout electronics
   loses twice that. The percentage of charge lost decreases as the star brightness
   or the diffuse sky brightness increases. Charge losses during the brief period
   when WFPC2 was operated at a temperature of -76{deg} C were approximately 85%
   greater, but apart from that, no significant change in the charge-transfer
   losses with time during the first 3.5 years of WFPC2's mission is evident,
   except possibly a weak effect for the very faintest star images. These results
   are quite similar to those of Whitmore & Heyer, which were based on a much
   smaller data set, but there are some differences in detail. Even with the
   present set of corrections, additional sources of calibration uncertainty
   that I am unable identify or characterize with the available data probably
   limit the {\em external} accuracy of photometry from WFPC2 to of order 1%-2%.
%K Techniques: Photometric
%I (1) Guest user, Canadian Astronomy Data Centre, which is operated for
   the National Research Council and the Canadian Space Agency by the Dominion
   Astrophysical Observatory, part of the Herzberg Institute of Astrophysics.
%I (2) Guest user, Isaac Newton Group Archive, which until 1998 October
   31 was operated by the Royal Greenwich Observatory.

%R 1998PASP..110.1464K
%F ori/PASPv110n754
%J-1466
%T Self-consistent Photometric Calibration of a Mosaic Survey with Overlaps.
%A Koranyi, Daniel M.
%A Kleyna, Jan ,
%A Grogin, Norman A.
%I Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge,
   MA 02138; (dkoranyi@cfa.harvard.edu), (jkleyna@cfa.harvard.edu), (ngrogin@cfa.harvard.edu)
%B  We describe a robust and computationally efficient technique for arriving
   at a set of self-consistent zero points for a set of overlapping photometric
   and nonphotometric images. This method allows the calibration of an entire
   survey from only a few photometric frames or at least the determination of
   mutually self-consistent zero points in the absence of any photometric reference.
%K Methods: Data Analysis
%K Methods: Observational

%R 1998PASP..110.1467J
%F ori/PASPv110n754
%J-1478
%T The Effects of Digitization on Nonstationary Stochastic Signals with Applications
   to Pulsar Signal Baseband Recording.
%A Jenet, F.A.
%I California Institute of Technology, Space Radiation Laboratory, Mail Code
   206-49 Pasadena, CA 91125; (merlyn@srl.caltech.edu)
%A Anderson, S.B.
%I California Institute of Technology, Space Radiation Laboratory, Mail Code
   206-49 Pasadena, CA 91125; (sba@srl.caltech.edu)
%B  The process of digitizing a stochastic signal introduces systematic
   distortions into the resulting digitized data. Further processing of these
   data may result in the appearance of unwanted artifacts, especially when
   the input signal was generated by a nonstationary stochastic process. In
   this paper the magnitude of these distortions are calculated analytically
   and the results are applied to a specific example found in pulsar signal
   processing. A pulsar signal is an excellent example of a nonstationary stochastic
   process. When analyzing pulsar data, the effects of interstellar medium (ISM)
   dispersion must be removed by digitally filtering the received signal. The
   distortions introduced through the digitization process cause unwanted artifacts
   to appear in the final ``dedispersed'' signal. These artifacts are demonstrated
   using actual 2-bit (4-level) digitized data of the pulsar PSR B0833-45 (Vela).
   Techniques are introduced that simultaneously minimize these artifacts and
   maximize the signal-to-noise ratio of the digitized data. The distortion
   analysis and artifact removal techniques described in this paper hold for
   an arbitrary number of input digitization thresholds (i.e., number of bits).
   Also presented are tables of the optimum digitizer thresholds for both uniform
   and nonuniform input threshold digitizers.
%K Methods: Analytical
%K Methods: Data Analysis
%K Stars: Pulsars: General

%R 1998PASP..110.1479V
%F ori/PASPv110n754
%J-1486
%T SCORE: A Mid-Infrared Echelle Format Spectrograph with No Moving Parts.
%A Van Cleve, Jeffrey
%A Gull, G.E.
%A Rinehart, S.A.
%A Smith, J.D.
%A Wilson, J.C.
%A Houck, J.R.,
%A Colonno, Mike
%I Space Sciences, Cornell University, Ithaca, NY 14853
%A Brown, R.
%A Blalock, W.
%I Ball Aerospace and Technologies Corporation, AR 1, 1600 Commerce Street,
   Boulder, CO 80306
%B  SCORE ({\em SIRTF} Cornell Echelle) is a mid-infrared spectrograph with
   a resolution of {lambda}M{Delta}{lambda}=600 covering the entire ground-based
   10 {mu}m atmospheric window in a single exposure. It was built as a proof
   of concept for one of the {\em SIRTF} ({\em Space Infrared Telescope Facility})
   instruments. It has no moving mechanical parts. SCORE was designed to operate
   properly upon assembly needing nothing more than a one-time focus adjustment.
   The instrument has been adapted for use on the Palomar 200 inch (5 m) Hale
   telescope and has been used there successfully. The demonstrated starting
   sensitivity is 105 mJy (1 {sigma} in 100 s at 10 {mu}m). A direct extrapolation
   to {\em SIRTF} conditions predicts a sensitivity between 60 and 90 better
   than demonstrated on the 200 inch telescope for the same elapsed observing
   time. Algorithms for reducing the data have been developed in IDL and are
   discussed. Sample astronomical observations demonstrating SCORE's operation
   are also presented.
%K Infrared: General
%K Instrumentation: Spectrographs

%R 1998PASP..110.1487K
%F ori/PASPv110n754
%J-1498
%T COSMIC: A Multiobject Spectrograph and Direct Imaging Camera for the 5 Meter
   Hale Telescope Prime Focus.
%A Kells, W. (1)
%A Dressler, A.
%A Sivaramakrishnan, A. (2)
%A Carr, D.,
%A Koch, E.
%I Observatories of the Carnegie Institution of Washington, 813 Santa Barbara
   Street, Pasadena, CA 91101and
%A Epps, H.
%A Hilyard, D.,
%A Pardeilhan, G. (3)
%I Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA
   95064
%B  We describe the design, construction, and operation of the Carnegie
   Observatories Spectroscopic Multislit and Imaging Camera (COSMIC) for the
   prime focus of the Hale 5 m telescope at Palomar Observatory. COSMIC is a
   reimaging grism spectrograph with a 13.65 arcmin square field of view, which
   can also be used as a direct imaging camera with a 9.75 arcmin square field
   of view. The wavelength coverage extends from 350 nm to almost 1 {mu}m; the
   detector is a thinned, back-illuminated SITe 2048x2048 CCD with high quantum
   efficiency and excellent cosmetics. Multislit aperture masks are produced
   photographically, with spectra of up to ~50 objects fitted on a single row
   of a slit mask. The instrument exhibits very little flexure and uses an active
   thermal control to maintain focus over a wide range of ambient temperature.
   In direct mode COSMIC is typically used with Kron-Cousins, Gunn, and narrow
   bandpass filters. The instrument achieves throughputs of greater than 50%
   for direct imaging and, in spectroscopic mode, a peak efficiency at 5500
   {AA} of slightly better than 24% of light falling on the 5 m mirror. COSMIC
   is optimized for faint-object imaging, down to Gunn r=26 mag, and multiobject
   spectroscopy, down to r=23 mag, with typically 30 objects per spectroscopic
   exposure.
%K Instrumentation: Spectrographs
%K Methods: Observational
%I (1) Current address: LIGO Project, California Institute of Technology,
   Pasadena, CA 91125.
%I (2) Current address: Space Telescope Science Institute, 3700 San Martin
   Drive, Baltimore, MD 21218.
%I (3) Current address: Strasbaugh, Inc., 825 Buckely Road, San Luis Obispo,
   CA 93401.

%R 1998PASP..110.1499O
%F ori/PASPv110n754
%J-1510
%T Faint OH ({nu}' = 10), ^17^OH, and ^18^OH Emission Lines in the Spectrum
   of the Night Airglow(1,)(2).
%A Osterbrock, Donald E.
%A Fulbright, Jon P.
%I University of California Observatories/Lick Observatory Board of Studies
   in Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064;
   (don@ucolick.org), (jfulb@ucolick.org)
%A Cosby, Philip C.
%I Molecular Physics Laboratory, SRI International, Menlo Park, CA 94025; (cosby@mplvax.sri.com)
%A Barlow, Thomas A.
%I Infrared Processing and Analysis Center, California Institute of Technology
   Pasadena, CA 91125; (tab@ipac.caltech.edu)
%B  We co-added night-sky spectra, recorded as by-products of exposures
   with the high-resolution echelle spectrograph (HIRES) of the Keck I 10 m
   telescope on stars and quasars over a period of approximately 2(1)/(2) years,
   to obtain a resultant spectrum with total exposure time ranging from 120
   to 24 hr over the wavelength range 5720-8810 {AA}. On this very high signal-to-noise
   ratio spectrum, OH emission lines from the upper vibrational level {nu}'=10,
   previously undetected in the night airglow, were measured and identified.
   Estimates are made for the relative population of OH ({nu}'=10), and possible
   secondary mechanisms exciting this level are discussed. Also, lines of the
   isotopic molecules ^18^OH and ^17^OH were detected and measured, and the
   relative populations of these heavy isotopomers are discussed. Lines of the
   isotopic molecule OD were not detected, for reasons that are discussed, but
   predicted wavelengths of such lines were calculated and are listed for possible
   future use with even better signal-to-noise ratio spectra, preferably at
   longer wavelengths.
%K Earth
%K Physical Data and Processes
%I (1) Lick Observatory Bulletin 1380.
%I (2) Based on observations obtained at the W. M. Keck Observatory, which
   is operated by the California Institute of Technology and the University
   of California.

%R 1998PASP..110.1511F
%F ori/PASPv110n754
%J-1512
%T High-Energy Processes in Accreting Black Holes(1). (Conference Highlights).
%A Fabian, Andrew C. (2)
%A Poutanen, Juri (3)
%A Svensson, Roland (3)
%K Conference Highlights
%I (1) Conference was held 1998 June 29-July 4 in Gr\"aft{aa}vallen, Sweden.
   Proceedings will be edited by Juri Poutanen and Roland Svensson and published
   in the {\em ASP Conference Series}.
%I (2) Institute of Astronomy, Madingley Road, Cambridge, CB3 OHA, England,
   UK.
%I (3) Stockholm Observatory, SE-133 36, Saltsj\"obaden, Sweden.

%R 1998PASP..110.1513B
%F ori/PASPv110n754
%J-1514
%T Solar and Stellar Activity: Similarities and Differences(1). (Conference
   Highlights).
%A Butler, C.J.
%A Doyle, J.G.,
%A Bailey, M.E.
%I Armagh Observatory
%K Conference Highlights
%I (1) Conference was held in Armagh, Northern Ireland, in 1998 September.
   Proceedings will be edited by C. J. Butler and J. G. Doyle and published
   in the {\em ASP Conference Series}.

%R 1998PASP..110.1515P
%F ori/PASPv110n754
%J-1516
%T The Stellar Content of Local Group Galaxies: IAU Symposium 192(1). (Conference
   Highlights).
%A Pritchet, Chris
%I University of Victoria
%K Conference Highlights
%I (1) Conference was held in Cape Town, South Africa, in 1998 September.
   Proceedings will be edited by P. A. Whitelock and R. D. Cannon and published
   in the {\em ASP Conference Series}.