%...Journal: PASP
%...MainTag: '<UCP-HEADER'
%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 2000PASP..112..293S
%F ori/PASPv112n769
%J-296
%T Episodes in the Discovery of Variations in the Chemical Composition of Stars
   and Galaxies(1). (Millennium Essay).
%A Sandage, Allan
%I The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara
   Street, Pasadena, CA 91101
%B Five episodes from the 1950s are reviewed that led to a fundamental
   change in prevalent hypotheses of how, when, and where the chemical elements
   were formed. The episodes are (1) the discovery that all stars do not have
   the same abundance ratios of heavy elements to hydrogen, and the inventions
   of methods to detect and measure the variations, culminating in the fundamental
   paper by Chamberlain and Aller; (2) Roman's discovery of the ultraviolet
   excess in 17 high-velocity F subdwarfs, and the subsequent discovery of the
   excess in globular cluster stars; (3) the development of the understanding
   of the physics of the H-R diagram and the evolution of stars, explaining
   the various sequences in that diagram; (4) Hoyle's idea of the recyclying
   of the products of nucleosynthesis from stellar interiors of evolving stars
   through the interstellar medium by stellar mass loss and supernovae explosions;
   and (5) the development of the theory of the various nuclear processes in
   stellar interiors by a small number of different buildup mechanisms (equilibrium
   burning, slow neutron capture using normally produced neutrons, proton capture,
   and fast neutron capture in supernova explosions) that can produce all the chemical
   elements.
%K Galaxies: Abundances
%K Galaxies: Evolution
%K Galaxies: Formation
%K Stars: Evolution
%K Stars: Formation
%I (1) This Essay is one of a series of invited contributions which will appear
   in the PASP throughout the year 2000 to mark the upcoming millennium. (Eds.)

%R 2000PASP..112..297T
%F ori/PASPv112n769
%J-314
%T Isolated Neutron Stars: Accretors and Coolers. (Invited Review).
%A Treves, Aldo
%I Dipartimento di Scienze, Universit\`a dell'Insubria, Via Lucini 3, 22100 Como, Italy;
   (treves@uni.mi.astro.it)
%A Turolla, Roberto
%I Dipartimento di Fisica, Universit\`a di Padova, Via Marzolo 8, 35131 Padova, Italy;
   (turolla@pd.infn.it)
%A Zane, Silvia
%I Nuclear and Astrophysics Laboratory, University of Oxford, Keble Road, Oxford
   OX1 3RH, England; (zane@astro.ox.ac.uk) and
%A Colpi, Monica
%I Dipartimento di Fisica, Universit\`a degli Studi di Milano Bicocca, Piazza della
   Scienza 3, 20126 Milano, Italy; (colpi@uni.mi.astro.it)
%B As many as 10^9^ neutron stars populate the Galaxy, but only {approx}10^3^
   are directly observed as pulsars or as accreting sources in X-ray binaries.
   In principle, also the accretion of the interstellar medium may make isolated
   neutron stars shine, and their weak luminosity could be detected in soft
   X-rays. Recent {\em ROSAT} observations have convincingly shown that neutron stars
   accreting from the interstellar medium are extremely rare, if observed at
   all, in contrast with earlier theoretical predictions. Until now two possible
   explanations for their elusiveness have been proposed: their velocity distribution
   may peak at ~200-400 km.s^-1^, as inferred from pulsar statistics, and this would
   severely choke accretion; the magnetic field may decay on timescales ~10^8^-10^9^
   yr, preventing a large fraction of neutron stars from entering the accretor
   stage. The search for accreting neutron stars has produced up to now a handful
   of promising candidates. While little doubt is left that these objects are indeed
   isolated neutron stars, the nature of their emission is still controversial.
   In particular, accreting objects can be confused with much younger, cooling
   neutron stars. However, a combination of observations and theoretical modeling
   may help in discriminating between the two classes.
%K Celestial Mechanics, Stellar Dynamics
%K Stars: Neutron
%K X-Rays

%R 2000PASP..112..315W
%F ori/PASPv112n769
%J-319
%T First Light Adaptive Optics Images from the Keck II Telescope: A New Era
   of High Angular Resolution Imagery. (Research Note).
%A Wizinowich, P.
%A Acton, D.S.
%A Shelton, C.
%A Stomski, P.
%A Gathright, J.
%A Ho, K.
%A Lupton, W.,
%A Tsubota, K.
%I W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI 96743; (peterw@keck.hawaii.edu),
   (sacton@keck.hawaii.edu), (cshelton@keck.hawaii.edu), (pstomski@keck.hawaii.edu),
   (johng@keck.hawaii.edu), (kho@keck.hawaii.edu), (wlupton@keck.hawaii.edu),
   (ktsubota@keck.hawaii.edu)
%A Lai, O.
%I Canada-France-Hawaii Telescope Corp., P.O. Box 1597, Kamuela, HI 96743; (lai@cfht.hawaii.edu)
%A Max, C.
%A Brase, J.
%A An, J.
%A Avicola, K.
%A Olivier, S.
%A Gavel, D.,
%A Macintosh, B.
%I Lawrence Livermore National Laboratory, P.O. Box 808, Livermore, CA 94550;
   (max1@llnl.gov), (brase1@llnl.gov), (an1@llnl.gov), (avicola1@llnl.gov),
   (olivier1@llnl.gov), (gavel1@llnl.gov), (macintosh1@llnl.gov)
%A Ghez, A.
%A Larkin, J.
%I UCLA Department of Physics and Astronomy, P.O. Box 951562, Los Angeles, CA 90095;
   (ghez@astro.ucla.edu), (larkin@astro.ucla.edu)
%B Adaptive optics (AO) is a technology that corrects in real time for the
   blurring effects of atmospheric turbulence, in principle allowing Earth-bound
   telescopes to achieve their diffraction limit and to ``see'' as clearly as
   if they were in space. The power of AO using natural guide stars has been
   amply demonstrated in recent years on telescopes up to 3-4 m in diameter.
   The next breakthrough in astronomical resolution was expected to occur with
   the implementation of AO on the new generation of large, 8-10 m diameter
   telescopes. In this paper we report the initial results from the first of
   these AO systems, now coming on line on the 10 m diameter Keck II Telescope.
   The results include the highest angular resolution images ever obtained from
   a single telescope (0".022 and 0".040 at 0.85 and 1.65 {mu}m wavelengths,
   respectively), as well as tests of system performance on three astronomical
   targets.
%K Galaxies: Structure
%K Galaxy: Center
%K Instrumentation: Adaptive Optics
%K Planets and Satellites: Individual: Neptune

%R 2000PASP..112..320B
%F ori/PASPv112n769
%J-327
%T Microlensing of Broad Absorption Line Quasars: Polarization Variability.
%A Belle, Kunegunda E.
%I Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071;
   (keb@tana.uwyo.edu) and
%A Lewis, Geraint F.
%I Department of Physics and Astronomy, University of Victoria, Victoria, BC
   V8W 3P6, Canada; (gfl@uvastro.phys.uvic.ca); and Astronomy Department, University
   of Washington, Seattle, WA 98195; (gfl@astro.washington.edu)
%B Roughly 10% of all quasars exhibit broad absorption line (BAL) features
   which appear to arise in material outflowing at high velocity from the active
   galactic nucleus. The details of this outflow are, however, very poorly constrained,
   and the particular nature of the BAL material is essentially unknown. Recently,
   new clues have become available through polarimetric studies, which have
   found that BAL troughs are more polarized than the quasar continuum radiation.
   To explain these observations, researchers have developed models where the
   BAL material outflows equatorially across the surface of the dusty torus.
   In these models, however, several sources of the BAL polarization are possible.
   Here we demonstrate how polarimetric monitoring of gravitationally lensed
   quasars, such as H1413+117, during microlensing events not only can distinguish
   between two currently popular models but also can provide further insight
   into the structure at the cores of BAL quasars.
%K Galaxies: Quasars: Absorption Lines
%K quasars: individual (\objS{QSO 1413+117}{H1413+117})

%R 2000PASP..112..328G
%F ori/PASPv112n769
%J-334
%T Spectral-Line Profiles in Daytime Skylight.
%A Gray, David F.
%A Tycner, Christopher
%A Brown, Kevin
%I Department of Physics and Astronomy, University of Western Ontario, London,
   ON N6A 3K7, Canada; (dfgray@uwo.ca)
%B The 1.2 m telescope and coud\'e spectrograph at our Elginfield Observatory
   was used to investigate the suitability of daytime skylight as a reference
   spectrum for astrophysical work. We show that with sufficient care, skylight
   does give the flux (or disk-integrated) spectrum of the Sun, allowing direct
   comparison with other stars. The line profiles in skylight become shallower
   with increasing angular separation from the Sun up to {approx}100{deg}, and then
   for larger angles they deepen slightly again. The amplitude of this variation
   is typically 3%-4% of the depth of the line. If the profiles are normalized
   to their central depths, their shapes remain unaltered. This implies that
   astrophysical analyses based on the shapes of spectral lines or ratios of
   depths of spectral lines in skylight should not be seriously affected. However, equivalent
   widths are not conserved; they can be reduced by up to the same 3%-4% unless
   care is taken to observe the sky close to the Sun or unless the angular variation
   is measured, as described here, and corrections applied. The skylight variations
   can be explained as a combination of aerosol and Rayleigh-Brillouin scattering.
   There is no discernible dependence with altitude of the Sun, ruling out a significant
   ground-albedo effect.
%K Stars: Atmospheres
%K Stars: Fundamental Parameters
%K Sun
%K Techniques: Spectroscopic

%R 2000PASP..112..335Y
%F ori/PASPv112n769
%J-342
%T Photometric Oscillations at about 200 Days in the Symbiotic Variable PU Vulpeculae.
%A Yoon, T.S. (1)
%I Department of Astronomy and Atmospheric Sciences, Kyungpook National University,
   Taegu 702-701, South Korea; (yoonts@bh.kyungpook.ac.kr)
%A Honeycutt, R.K.
%I Astronomy Department, Indiana University, Swain Hall West, Bloomington, IN
   47405; (honey@astro.indiana.edu)
%B We show that as PU Vul fell to full quiescence in 1994, following a
   long outburst, the system developed well-defined 0.2 mag oscillations with
   a characteristic period of ~211 days. This quasi-periodicity is distinctly
   different from the behavior seen during late decline from outburst, where
   weaker photometric variations near 317, 227, and 120 days were seen. Suggested
   causes for this variation are discussed.
%K Stars: Binaries: Symbiotic
%K Stars: Individual: Constellation Name: PU Vulpeculae
%I (1) Also Visiting Scholar, Indiana University.

%R 2000PASP..112..343B
%F ori/PASPv112n769
%J-348
%T {\em EUVE} Observations of the Magnetic Cataclysmic Variable QQ Vulpeculae.
%A Belle, Kunegunda E.
%A Howell, Steve B. (1)
%A Mills, Amy
%I Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071;
   (keb@tana.irastro.uwyo.edu), (howell@psi.edu)
%B We present simultaneous X-ray ({lambda}_peak_~44 {AA}) and EUV ({lambda}_peak_=89 {AA})
   light curves for the magnetic cataclysmic variable QQ Vulpeculae, obtained
   with the {\em EUVE} satellite. We find that the unique shape of the X-ray
   light curve is different from previously obtained X-ray light curves of QQ
   Vul and provides evidence for two-pole accretion. Detailed examination of
   the photometric data indicates that QQ Vul undergoes a stellar eclipse of
   the X-ray-emitting region, indicative of a high binary inclination. We discuss
   possible implications for the nature of this system given the observed shape
   of its EUV and X-ray light curves.
%K Stars: Novae, Cataclysmic Variables
%K stars: individual (QQ Vulpeculae)
%K Ultraviolet Emission
%K X-Rays
%I (1) Present address: Head, Astrophysics Group, Planetary Science Institute, 620
   North 6th Avenue, Tucson, AZ 85705.

%R 2000PASP..112..349C
%F ori/PASPv112n769
%J-353
%T The Orbital Period of the Eclipsing Dwarf Nova V729 Sagittarii.
%A Cieslinski, D.
%I Divis\~ao de Astrof\'isica, Instituto Nacional de Pesquisas Espaciais, CP 515,
   12201-970 S\~ao Jos\'e dos Campos, SP, Brazil; (deo@das.inpe.br)
%A Steiner, J.E.
%I Laborat\'orio Nacional de Astrof\'isica-LNA/CNPq, CP 21, 37500-000 Itajub\'a, Brazil;
   and Instituto Astron\^omico e Geof\'isico, Universidade de S\~ao Paulo, CP 9638,
   01065-970 S\~ao Paulo, SP, Brazil; (steiner@lna.br)
%A Pereira, P.C.R.
%I Departamento de Astronomia, Observat\'orio Nacional-CNPq/MCT, Rua Gal. Jos\'e
   Cristino, 77, 20921-400, Rio de Janeiro, RJ, Brazil; (pcp@maxwell.on.br) and
%A Pereira, M.G.
%I Divis\~ao de Astrof\'isica, Instituto Nacional de Pesquisas Espaciais, CP 515,
   12201-970 S\~ao Jos\'e dos Campos, SP, Brazil; (marildo@das.inpe.br)
%B We have discovered that V729 Sgr, an object listed as a possible rapid irregular
   variable in the fourth edition of the General Catalogue of Variable Stars,
   is an eclipsing cataclysmic variable with an orbital period of 0.1734055
   days and an eclipse depth of 0.2-0.5 mag. The shape of the light curve is
   quite variable. When observed in the {\em R} filter the light curve presents
   a pronounced sinusoidal modulation with an amplitude of ~0.4-0.5 mag. In
   addition, brightness variations with timescales and characteristics suggesting
   dwarf nova eruptions are seen in the historical photometric data and in the
   our own data. We classify V729 Sgr as a new member of dwarf nova class, possibly
   of Z Cam type.
%K Stars: Binaries: Eclipsing
%K stars: individual (V729 Sagittarii)
%K Stars: Novae, Cataclysmic Variables

%R 2000PASP..112..354S
%F ori/PASPv112n769
%J-358
%T EC 11481-2303: A Peculiar Hot High-Gravity Pre-White Dwarf.
%A Stys, D.
%A Slevinsky, R.
%A Sion, E.M.,
%A Saffer, R.
%I Department of Astronomy and Astrophysics, Villanova University; (Edward.Sion@Villanova.edu)
%A Holberg, J.B.
%I Lunar and Planetary Lab. West, University of Arizonaand
%A O'Donoghue, Darragh
%A Kilkenny, D.
%A Stobie, R.S.,
%A Koen, C.
%I South African Astronomical Observatory, P.O. Box 9, Observatory, South Africa
%B We report the discovery of a peculiar new hot high-gravity predegenerate
   star, EC 11481-2303 from the Edinburgh-Cape Blue Object Survey, based upon
   the analysis of far-UV {\em International Ultraviolet Explorer} ({\em IUE})
   echelle and low-resolution spectra and an optical spectrum. The {\em IUE} spectra
   reveal the presence of far-UV photospheric/circumstellar high-ionization
   absorption features due to N V {lambda}{lambda}1238, 1242, Si IV {lambda}{lambda}1393,
   1402, C IV {lambda}{lambda}1548, 1550, and He II {lambda}1640. The mean velocity
   of these features is -17.5 km.s^-1^. In addition, there is low-ionization interstellar
   absorption at an average velocity of -5.6 km.s^-1^. The interstellar lines
   are strong and imply a distance of more than 500 pc. The optical spectrum
   is dominated by Stark-broadened Balmer absorption, a sharp He II {lambda}4686
   feature, and the absence of Balmer members higher than H8. A best-fit model
   atmosphere to the optical data yields T_eff_=41,790 K and logg=5.84, suggesting
   an extended horizontal branch sdOB subdwarf. However, synthetic spectral
   fits to the far-UV spectrum do not provide a consistent fit to both the Ly{alpha}
   region and the far-UV continuum of EC 11481-2303. It is possible that EC
   11481-2303 is an unresolved binary. Follow-up ground-based and far-UV studies
   are encouraged to discern the possible nature of any binary companion.
%K Stars: Subdwarfs
%K Stars: White Dwarfs

%R 2000PASP..112..359L
%F ori/PASPv112n769
%J-362
%T A Double-lined Spectroscopic Binary in the Open Cluster Trumpler 14.
%A Levato, Hugo (1)
%A Malaroda, Stella (2)
%I Complejo Astron\'omico El Leoncito, CC 467, 5400 San Juan, Argentina; (levato@infovia.com.ar),
   (malaroda@castec.edu.ar)
%A Morrell, Nidia (1)(3)
%I Facultad de Ciencias Astron\'omicas y Geof\'isicas de la UNLP, Paseo del Bosque
   s/n., 1900 La Plata, Argentina; (nidia@fcaglp.unlp.edu.ar)
%A Garc\'ia, Beatriz (1)
%I Centro Regional de Investigaciones Cient\'ificas, CRICYT, Casilla de Correo 131,
   5500 Mendoza, Argentina; (bgarcia@lab.cricyt.edu.ar)
%A Grosso, M\'onica (4)
%I Complejo Astron\'omico El Leoncito, CC 467, 5400 San Juan, Argentina; (mgrosso@castec.edu.ar)
%B We present the results of a determination of the preliminary orbital elements
   of the spectroscopic binary FMM 3 in the field of the open cluster Trumpler
   14. The spectrum of this binary shows two sets of lines that are roughly
   similar. The period found was around 5 days (P=5.0339+/-0.0003), and the orbit
   is eccentric (e=0.51+/-0.02). These values were adopted from the combined solution
   for both components. The mass ratio of the system is 0.76+/-0.06.
%K Stars: Binaries: Spectroscopic
%K Galaxy: Open Clusters and Associations: Individual: Name: \objS{Cl Trumpler 14}{Trumpler 14}
%I (1) Member of the Carrera del Investigador Cient\'ifico del Consejo Nacional
   de Investigaciones Cient\'ificas y T\'ecnicas de la Rep\'ublica Argentina.
%I (2) Member of the Carrera del Investigador Cient\'ifico de la Comisi\'on
   de Investigaciones Cient\'ificas de la Provincia de Buenos Aires.
%I (3) Visiting Astronomer, Complejo Astron\'omico El Leoncito (CASLEO). CASLEO
   is operated under agreement of the Universidad Nacional de La Plata, the
   Universidad Nacional de C\'ordoba, the Universidad Nacional de San Juan, and
   CONICET.
%I (4) Member of the Carrera del T\'ecnico, Consejo Nacional de Investigaciones
   Cient\'ificas y T\'ecnicas.

%R 2000PASP..112..363P
%F ori/PASPv112n769
%J-366
%T Long-Term {\em VRI} Photometry of {rho} Cassiopeiae.
%A Percy, John R.
%A Kolin, David L.
%I Erindale Campus, and Department of Astronomy, University of Toronto, Mississauga,
   ON L5L 1C6, Canada; (jpercy@erin.utoronto.ca)
%A Henry, Gregory W.
%I Center of Excellence in Information Systems, Tennessee State University, Nashville,
   TN 37203-3401; (henry@schwab.tsuniv.edu)
%B We report over 5700 days (15 years) of {\em VRI} photometry of the yellow
   hypergiant variable star {rho} Cassiopeiae. The {\em V-I} color curve is
   generally in phase with the {\em V} light curve on timescales of a few hundred
   days, but there is a 4000 day variation in {\em V-I} which is absent from
   the light curve. The approximate ratio of {Delta}({\em V-I})/{Delta}{\em
   V} is 0.46. The most conspicuous period in the light curve, in the autocorrelation
   diagram, and in the power spectrum is about 820 days. Less significant periods
   of 380, 510, and 645 days also appear in the power spectrum, and there are
   many subcycles in the light curve with lengths of 200-500 days. Since the most
   recent comprehensive analysis of the light curve of {rho} Cas found a dominant
   period of 300 days, we conclude that the behavior of the star is quite variable
   with time.
%K Stars: Variables: Cepheids
%K Stars: Circumstellar Matter
%K Stars: Individual: Constellation Name: {rho} Cassiopeiae
%K Stars: Variables: Other

%R 2000PASP..112..367B
%F ori/PASPv112n769
%J-383
%T Rotation Curve Measurement using Cross-Correlation(1).
%A Barton, Elizabeth J. (2)
%A Kannappan, Sheila J.
%A Kurtz, Michael J.,
%A Geller, Margaret J.
%I Harvard-Smithsonian Center for Astrophysics
%B Long-slit spectroscopy is entering an era of increased spatial and spectral
   resolution and increased sample size. Improved instruments reveal complex
   velocity structure that cannot be described with a one-dimensional rotation
   curve, yet samples are too numerous to examine each galaxy in detail. Therefore,
   one goal of rotation curve measurement techniques is to flag cases in which
   the kinematic structure of the galaxy is more complex than a single-valued
   curve.\par We examine cross-correlation as a technique that is easily automated
   and works for low signal-to-noise spectra. We show that the technique yields
   well-defined errors which increase when the simple spectral model (template)
   is a poor match to the data, flagging those cases for later inspection.\par
   We compare the technique to the more traditional, parametric technique of
   simultaneous emission-line fitting. When the line profile at a single slit
   position is non-Gaussian, the techniques disagree. For our model spectra
   with two well-separated velocity components, assigned velocities from the
   two techniques differ by up to ~52% of the velocity separation of the model
   components. However, careful use of the error statistics for either technique
   allows one to flag these non-Gaussian spectra.
%K Methods: Data Analysis
%K Techniques: Radial Velocities
%I (1) Observations reported in this paper were obtained at the Multiple
   Mirror Telescope Observatory, a facility operated jointly by the University
   of Arizona and the Smithsonian Institution.
%I (2) Present address: National Research Council of Canada, Herzberg Institute of
   Astrophysics, Dominion Astrophysical Observatory, 5071 West Saanich Road,
   RR5, Victoria, BC V8X 4M6, Canada; (Betsy.Barton@hia.nrc.ca).

%R 2000PASP..112..384L
%F ori/PASPv112n769
%J-396
%T CoolSpec: A Near-Infrared Long-Slit Spectrometer for McDonald Observatory.
%A Lester, Dan F.
%A Hill, Gary J.
%A Doppmann, Greg
%A Froning, C.S.
%I McDonald Observatory and Department of Astronomy, University of Texas, Austin,
   TX 78712; (dfl@astro.as.utexas.edu)
%B This paper describes the design, operational goals, and some science accomplishments
   of the CoolSpec near-infrared spectrometer on the McDonald Observatory 2.7
   m Harlan Smith telescope. CoolSpec is a novel and economical design, in which
   an existing infrared imager is mated to a separate spectrograph, both of
   which are separately cooled.
%K Infrared: General
%K Instrumentation: Spectrographs

%R 2000PASP..112..397R
%F ori/PASPv112n769
%J-408
%T TASS Mark III Photometric Survey of the Celestial Equator.
%A Richmond, Michael W. (1)
%A Droege, Thomas F.
%A Gombert, Glenn (2)
%A Gutzwiller, Michael
%A Henden, Arne A. (3)
%A Albertson, Chris
%A Beser, Nicholas (4)
%A Molhant, Norman
%A Johnson, Herb (5)
%B The Amateur Sky Survey (TASS) is a loose confederation of amateur and professional
   astronomers. We describe the design and construction of our Mark III system,
   a set of wide-field drift-scan CCD cameras which monitor the celestial equator
   down to 13th magnitude in several passbands. We explain the methods by which
   images are gathered, processed, and reduced into lists of stellar positions
   and magnitudes. Over the period 1996 October to 1998 November, we compiled
   a large database of photometric measurements. One of our results is the {\em
   tenxcat} catalog, which contains measurements on the standard Johnson-Cousins
   system for 367,241 stars; it contains links to the light curves of these
   stars as well.
%K Catalogs
%K Instrumentation: Miscellaneous
%K Stars: General
%K Surveys
%I (1) Physics Department, Rochester Institute of Technology, Rochester,
   NY 14623-5603; (mwrsps@rit.edu).
%I (2) Miami Valley Astronomical Society.
%I (3) USRA/US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86002.
%I (4) Applied Physics Lab, Johns Hopkins University.
%I (5) New Jersey Astronomical Association, High Bridge, NJ 08829.

%R 2000PASP..112..409R
%F ori/PASPv112n769
%J-416
%T {\em BVR} Photometry of Northern Hemisphere Luminous Stars. V. 123 Stars
   in the First Two Galactic Quadrants and the Distribution of O-B2 Supergiants(1).
%A Reed, B.Cameron
%I Department of Physics, Alma College Alma, MI 48801; (reed@alma.edu)
%A Reed, Laureen G.
%I Department of Physics, Saginaw Valley State University, University Center,
   MI 48710; (lgreed@svsu.edu)
%B CCD-based {\em BVR} photometry of 123 previously unobserved stars drawn
   from volumes I, II, III, and V of the {\em Luminous Stars in the Northern
   Milky Way} catalog (LS catalog) is reported. In addition, the Galactic distribution
   of over 400 LS-catalog supergiants as derived from spectroscopic parallaxes
   is examined.
%K Stars: Early-Type
%I (1) This research was performed at the Lowell Observatory 31 inch telescope, which,
   under an agreement with Northern Arizona University and the NURO consortium,
   is operated 60% of the time as the National Undergraduate Research Observatory.

%R 2000PASP..112..417G
%F ori/PASPv112n769
%J-418
%T Correction to a Paper on HD 207739.
%A Griffin, R.F.
%I The Observatories, Madingley Road, Cambridge CB3 0HA, England; (rfg@ast.cam.ac.uk)
%K stars: individual (HD 207739)

%R 2000PASP..112..419S
%F ori/PASPv112n769
%J-419
%T Multiwavelength Analyses of Classical Carbon-Oxygen Novae(1). (Dissertation
   Summary).
%A Schwarz, Gregory J.
%I Current address: Steward Observatory, University of Arizona, 933 North Cherry Avenue,
   Tucson, AZ 85721; (gschwarz@grumpy.as.arizona.edu)Thesis work conducted at
   Arizona State UniversityPh.D. thesis directed by Sumner Starrfield; Ph.D.
   degree awarded 1999 August
%K Dissertation Summaries
%K Stars: Novae, Cataclysmic Variables
%I (1) The full dissertation can be read on the web at <http://brian.la.asu.edu/~schwarz/main/main.html>.

%R 2000PASP..112..420C
%F ori/PASPv112n769
%J-421
%T Structure and Dynamics of Early-Type Disk Galaxies. (Dissertation Summary).
%A Corsini, Enrico Maria
%I Current address: Osservatorio Astrofisico dell'Universit\`a di Padova, via
   dell'Osservatorio 8, I-36012 Asiago (VI), Italy; (corsini@pd.astro.it)Thesis work
   conducted at Dipartimento di Astronomia dell'Universit\`a di Padova, Padova, ItalyPh.D.
   thesis directed by Francesco Bertola; Ph.D. degree awarded 1999
%K Dissertation Summaries
%K Galaxies: Elliptical and Lenticular, cD
%K Galaxies: Kinematics and Dynamics
%K Galaxies: Spiral
%K Galaxies: Structure

%R 2000PASP..112..422G
%F ori/PASPv112n769
%J-422
%T Close Approaches of Stars to the Solar System Based on {\em Hipparcos} Data.
   (Dissertation Summary).
%A Garc\'ia-S\'anchez, Joan
%I Current address: Departament d'Astronomia i Meteorologia, Universitat de Barcelona,
   Av. Diagonal 647, E-08028, Barcelona, Spain; (jgarcia@fajmpp0.am.ub.es)Thesis work
   conducted at Universitat de BarcelonaPh.D. thesis directed by Paul R. Weissman
   and Josep M. Paredes; Ph.D. degree awarded 1999
%K Comets: General
%K Galaxy: Solar Neighborhood
%K Solar System: General
%K Stars: Kinematics

%R 2000PASP..112..423C
%F ori/PASPv112n769
%J-423
%T Dynamics of Galaxies: From the Early Universe to the Present(1). (Conference
   Highlights).
%A Combes, Fran\c{c}oise
%A Mamon, Gary
%A Charmandaris, Vassilis
%I Observatoire de Paris,
%I IAP and Observatoire de Paris,
%I Observatoire de Paris and Cornell University
%K Conference Highlights
%I (1) The Conference was the 15th IAP (Institut d'Astrophysique de Paris)
   meeting and was held in Paris, France, on 1999 July 9-13. Proceedings will
   be edited by F. Combes, G. Mamon, and V. Charmandaris and published in the
   ASP Conference Series (Vol. 197).

%R 2000PASP..112..424M
%F ori/PASPv112n769
%J-426
%T Green Bank Workshop on Warm Ionized Gas in Galaxies(1). (Conference Highlights).
%A Minter, Anthony H.
%A Lockman, Felix J.
%A Balser, Dana S.
%I National Radio Astronomy Observatory
%A Reynolds, R.J.
%A Savage, Blair D.
%I University of Wisconsin, Madison
%A Cordes, James M.
%I Cornell University
%A Rand, Richard J.
%I University of New Mexicoand
%A Shull, J.Michael
%I University of Colorado, Boulder
%K Conference Highlights
%I (1) Conference was organized and hosted by the National Radio Astronomy Observatory
   and was held in Green Bank, West Virginia, on 1999 September 23-25. The National
   Radio Astronomy Observatory is a facility of the National Science Foundation
   operated under cooperative agreement with Associated Universities, Inc.

%R 2000PASP..112..427S
%F ori/PASPv112n769
%J-428
%T Physics of the Solar Corona and Transition Region(1). (Conference Highlights).
%A Schrijver, C.J.
%A Hurlburt, N.E.
%I Advanced Technology Center of Lockheed-Martin Missiles and Space
%K Conference Highlights
%I (1) Conference was held in Monterey, CA, on 1999 August 24-27. Proceedings
   are published in the topical issues of {\em Solar Physics} of 1999 December
   and 2000 April.