%...Journal: PASP
%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 1999PASP..111....1K
%F ori/PASPv111n755
%J-30
%T The Ultraviolet and Optical Continuum Emission in Active Galactic Nuclei:
   The Status of Accretion Disks. (Invited Review).
%A Koratkar, Anuradha
%I Space Telescope Science Institute, Baltimore, MD 21218; (koratkar@stsci.edu)
%A Blaes, Omer
%I Physics Department, University of California, Santa Barbara, CA 93106; (blaes@vela.physics.ucsb.edu)
%B  A fundamental component of models of active galactic nuclei (AGNs) is
   an accretion disk around a supermassive black hole. However, the nature of
   this accretion disk is not well understood, and current models do not provide
   a satisfactory explanation of the optical/UV continuum observed in AGNs.
   In this paper we review the substantial theoretical and observational progress
   made in the field. We also try to point out future research directions that
   would be fruitful in trying to obtain a complete, self-consistent model of
   the continuum-emitting regions.
%K accretion, accretion disks
%K Polarization
%K Galaxies: Quasars: General
%K Ultraviolet Emission
%K Invited Reviews

%R 1999PASP..111...31O
%F ori/PASPv111n755
%J-44
%T Retrieving Bulge and Disk Parameters and Asymptotic Magnitudes from the Growth
   Curves of Galaxies.
%A Okamura, Sadanori
%A Yasuda, Naoki (1)
%A Shimasaku, Kazuhiro ,
%A Yagi, Masafumi (1)
%I Department of Astronomy and Research Center for the Early Universe, School
   of Science, University of Tokyo, Bunkyo-ku, Tokyo, 113-0033 Japan; (okamura@astron.s.u-tokyo.ac.jp)
   and
%A Weinberg, David H.
%I Department of Astronomy, Ohio State University, Columbus, OH, 43210; (dhw@astronomy.ohio-state.edu)
%B  We show that the growth curves of galaxies can be used to determine
   their bulge and disk parameters and bulge-to-total luminosity ratios, in
   addition to their conventional asymptotic magnitudes, provided that the point
   spread function is accurately known and signal-to-noise ratio is modest (SMN{gsim}30).
   The growth curve is a fundamental quantity that most future large galaxy
   imaging surveys will measure. Bulge and disk parameters retrieved from the
   growth curve will enable us to perform statistical studies of luminosity
   structure for a large number of galaxies.
%K Galaxies: Fundamental Parameters
%K Galaxies: Photometry
%K Galaxies: Structure
%I (1) Present address: National Astronomical Observatory, Mitaka, Tokyo,
   181-8588 Japan.

%R 1999PASP..111...45M
%F ori/PASPv111n755
%J-49
%T The Meinunger ``Nicht Rote'' Objects.
%A Margon, Bruce
%A Deutsch, Eric W.
%I Department of Astronomy, University of Washington, Box 351580, Seattle, WA
   98195-1580; (margon@astro.washington.edu), (deutsch@astro.washington.edu)
%B  Four high-latitude slow variable stars have been noted by Meinunger
   as ``nicht rote'' (``not red'') objects and thus curious. We have previously
   reported that one of these objects, CC Boo, is in fact a QSO. Here we present
   observations demonstrating that the remaining three are also highly variable
   active galactic nuclei. The most interesting object of the four is perhaps
   S10765 (=NGP9 F324-0276706), which proves to be a resolved galaxy at z=0.063.
   Despite the rapid and large reported variability amplitude ({Delta}m~1.6
   mag), the spectrum is that of a perfectly normal galaxy, with no emission
   lines or evident nonthermal continuum. We also present new spectroscopic
   and photometric observations for AR CVn, suggested by Meinunger to be an
   RR Lyrae star despite its very faint magnitude (<B>=19.4). The object is
   indeed one of the most distant RR Lyrae stars known, at a galactocentric
   distance of ~40 kpc.
%K Galaxies: Active
%K Galaxy: Halo
%K Galaxies: Quasars: General
%K Stars: Variables: RR Lyrae Variable

%R 1999PASP..111...50F
%F ori/PASPv111n755
%J-56
%T Planetary Companions around Two Solar-Type Stars: HD 195019 and HD 217107(1).
%A Fischer, Debra A. (2)
%A Marcy, Geoffrey W. (2)
%A Butler, R.Paul (3)
%A Vogt, Steven S. (4)
%A Apps, Kevin (5)
%B  We have enlarged the sample of stars in the planet search at Lick Observatory.
   Doppler measurements of 82 new stars observed at Lick Observatory, with additional
   velocities from Keck Observatory, have revealed two new planet candidates.
   The G3 V/IV star, HD 195019, exhibits Keplerian velocity variations with
   a period of 18.27 days, an orbital eccentricity of 0.03+/-0.03, and M{\rf sin}i=3.51
   M_JUP_. Based on a measurement of Ca II H and K emission, this star is chromospherically
   inactive. We estimate the metallicity of HD 195019 to be approximately solar
   from {\em ubvy} photometry. The second planet candidate was detected around
   HD 217107, a G7 V star. This star exhibits a 7.12 day Keplerian period with
   eccentricity 0.14+/-0.05 and M{\rf sin}i=1.27 M_JUP_. HD 217107 is also chromospherically
   inactive. The photometric metallicity is found to be [FeMH]=+0.29+/-0.1 dex.
   Given the relatively short orbital period, the absence of tidal spin-up in
   HD 217107 provides a theoretical constraint on the upper limit of the companion
   mass of less than 11 {\em M}_JUP_.
%K Stars: Planetary Systems
%K Stars: Individual: Henry Draper Number: HD 195019
%K Stars: Individual: Henry Draper Number: HD 217107
%I (1) Based on observations obtained at Lick Observatory, which is operated
   by the University of California, and 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) Department of Physics and Astronomy, San Francisco State University,
   San Francisco, CA 94132 and Department of Astronomy, University of California,
   Berkeley; (fischer@stars.sfsu.edu).
%I (3) Anglo-Australian Observatory, P.O. Box 296, NSW 1710 Epping, Australia.
%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,
   England 9QJ.

%R 1999PASP..111...57H
%F ori/PASPv111n755
%J-62
%T A Test for Large-Scale Systematic Errors in Maps of Galactic Reddening.
%A Hudson, Michael J.
%I Department of Physics and Astronomy, University of Victoria, P.O. Box 3055,
   Victoria, BC, V8W 3P6, Canada; (hudson@uvastro.phys.uvic.ca)
%B  Accurate maps of Galactic reddening are important for a number of applications,
   such as mapping the peculiar velocity field in the nearby universe. Of particular
   concern are systematic errors which vary slowly as a function of position
   on the sky, as these would induce spurious bulk flow. We have compared the
   reddenings of Burstein & Heiles (BH) and those of Schlegel, Finkbeiner, &
   Davis (SFD) to independent estimates of the reddening, for Galactic latitudes
   |b|>10{deg}. Our primary source of Galactic reddening estimates comes from
   comparing the difference between the observed B-V colors of early-type galaxies,
   and the predicted B-V color determined from the B-V-Mg_2_ relation. We have
   fitted a dipole to the residuals in order to look for large-scale systematic
   deviations. There is marginal evidence for a dipolar residual in the comparison
   between the SFD maps and the observed early-type galaxy reddenings. If this
   is due to an error in the SFD maps, then it can be corrected with a small
   (13%) multiplicative dipole term. We argue, however, that this difference
   is more likely to be due to a small (0.01 mag) systematic error in the measured
   B-V colors of the early-type galaxies. This interpretation is supported by
   a smaller, independent data set (globular cluster and RR Lyrae stars), which
   yields a result inconsistent with the early-type galaxy residual dipole.
   BH reddenings are found to have no significant systematic residuals, apart
   from the known problem in the region 230{deg}<l<310{deg}, -20{deg}<b<20{deg}.
%K ISM: Dust, Extinction
%K Galaxies: Distances and Redshifts
%K Galaxies: Elliptical and Lenticular, cD
%K Galaxy: Globular Clusters: General
%K Stars: Variables: Other

%R 1999PASP..111...63F
%F ori/PASPv111n755
%J-75
%T Correcting for the Effects of Interstellar Extinction.
%A Fitzpatrick, Edward L.
%I Department of Astronomy and Astrophysics, Villanova University, Mendel Hall,
   Villanova, PA 19085
%B  This paper addresses the issue of how best to correct astronomical data
   for the wavelength-dependent effects of Galactic interstellar extinction.
   The main general features of extinction from the IR through the UV are reviewed,
   along with the nature of observed spatial variations. The enormous range
   of extinction properties found in the Galaxy, particularly in the UV spectral
   region, is illustrated. Fortunately, there are some tight constraints on
   the wavelength dependence of extinction and some general correlations between
   extinction curve shape and interstellar environment. These relationships
   provide some guidance for correcting data for the effects of extinction.
   Several strategies for dereddening are discussed along with estimates of
   the uncertainties inherent in each method. In the Appendix, a new derivation
   of the wavelength dependence of an average Galactic extinction curve from
   the IR through the UV is presented, along with a new estimate of how this
   extinction law varies with the parameter R{equiv}A{\fen V}/{\em E}({\em B}-{\em
   V}). These curves represent the true monochromatic wavelength dependence
   of extinction and, as such, are suitable for dereddening IR-UV spectrophotometric
   data of any resolution and can be used to derive extinction relations for
   any photometry system.
%K ISM: Dust, Extinction

%R 1999PASP..111...76D
%F ori/PASPv111n755
%J-83
%T Time-resolved Spectroscopy of V Sagittae.
%A Diaz, Marcos P.
%I Laborat\'orio Nacional de Astrof\'isica/CNPq, 37500-000, MG, Itajub\'a, Brazil;
   (marcos@lna.br)
%B  An observational study of the peculiar binary V Sagittae is presented
   with the aim of constraining the stellar masses and current models for the
   mass transfer in this system. The radial velocity curves of the H{beta} and
   He II {lambda}4686 emission lines at low photometric state are derived. Possible
   physical scenarios for the line-forming region are discussed on the basis
   of the line profile orbital behavior. In addition, an exploratory analysis
   of the X-ray data on V Sge is made with the aim of addressing quantitatively
   the proposed models for this binary.{\em Subject headings}:
%K Stars: Binaries: Eclipsing
%K Stars: Novae, Cataclysmic Variables
%K Stars: Individual: Constellation Name: V Sagittae
%K Stars: Mass Loss
%K X-Rays

%R 1999PASP..111...84V
%F ori/PASPv111n755
%J-93
%T Carbon, Nitrogen, and Oxygen Abundances of Selected Stars in the Hertzsprung
   Gap.
%A Vanture, Andrew D.
%I Astronomy Department, University of Washington, Seattle, WA 98195; and Science
   Division, Everett Community College, 801 Wetmore Avenue, Everett, WA 98201;
   (avanture@evcc.ctc.edu), (vanture@astro.washington.edu)
%A Wallerstein, George (1)
%I Astronomy Department, University of Washington, Seattle, WA 98195; (wall@astro.washington.edu)
%B  The iron, carbon, nitrogen, and oxygen abundances for several stars
   whose characteristics place them in the Hertzsprung gap have been derived
   from high-resolution spectra. These stars were selected based on the fact
   that previous studies have shown them to have peculiar carbon, nitrogen,
   or lithium abundances considering their position in the Hertzsprung-Russell
   diagram. When combined with the lithium abundances derived by Wallerstein
   and coworkers, the carbon, nitrogen, and oxygen abundances indicate that
   the sample of stars can generally be broken into two categories--lower luminosity
   dwarfs or subgiants that are unmixed and higher luminosity mixed giants.
   Among the sample are two stars, HR 7606 and HR 8626, which previously have
   been identified by Bidelman as ``low-velocity CH stars.'' These stars show
   metallicities of [FeMH]~-0.5 and solar abundances of carbon, nitrogen, and
   oxygen. The strength of the CH band in these stars is probably an artifact
   of a mild metal deficiency and the absence of substantial mixing of CN processed
   materials to the surface of the star rather than an unusual nucleosynthetic
   history.
%K Stars: Abundances
%K Stars: Chemically Peculiar
%K Stars: Evolution
%K Stars: Late-Type
%I (1) Visiting Astronomer, Dominion Astrophysical Observatory, Victoria
   BC, Canada.

%R 1999PASP..111...94P
%F ori/PASPv111n755
%J-97
%T Long-Term Changes in Mira Stars. I. Period Fluctuations in Mira Stars.
%A Percy, John R.
%A Colivas, Ted
%I Erindale Campus, University of Toronto, Mississauga, ON, Canada L5L 1C6;
   (jpercy@erin.utoronto.ca)
%B  It has been known since the pioneering work of Eddington & Plakidis
   that the period changes in Mira stars are dominated by the effects of random
   cycle-to-cycle fluctuations in period, at least in the limited sample of
   stars that were studied. We have extended their work, using a portion of
   the American Association of Variable Star Observers (AAVSO) international
   database of variable star observations: times and magnitudes of maximum and
   minimum magnitude of 391 bright Mira stars over 75 yr (Kowalsky et al.).
   The Eddington & Plakidis model fits the data in almost every case, at least
   over a time interval of several tens of cycles. There is a weak correlation
   between the fractional period fluctuation, per cycle, and the period (or
   color) of the star, but not with the amplitude or chemical type (M, S, or
   C).
%K Stars: Variables: Miras
%K Stars: AGB and Post-AGB
%K Stars: Carbon
%K Stars: Evolution
%K Stars: Late-Type
%K Stars: Oscillations

%R 1999PASP..111...98P
%F ori/PASPv111n755
%J-103
%T Long-Term Changes in Mira Stars. II. A Search for Evolutionary Period Changes
   in Mira Stars.
%A Percy, John R.
%A Au, Winnie W.-Y.
%I Erindale Campus, and Department of Astronomy, University of Toronto, Mississauga,
   Ontario, L5L 1C6, Canada; (jpercy@erin.utoronto.ca)
%B  The (O-C) diagrams of Mira stars are dominated by the effects of random,
   cycle-to-cycle fluctuations in period. Nevertheless, it is possible to average
   these effects over many stars with similar properties and compare the average
   apparent period change with that predicted by evolutionary models. The average
   rate of period change for a 1.0 {\em M}_{sun}_ model, averaged over the Mira
   phase, is +28x10^-6^ days.day^-1^ if the pulsation is in the fundamental
   mode, and +11x10^-6^ days.day^-1^ if it is in the first overtone mode (as
   most Mira star pulsation is now believed to be). The observed changes are
   not inconsistent with these results, in the sense that (1) positive period
   changes outnumber negative ones and (2) the average period change of all
   of the M type Miras is +16x10^-6^ days.day^-1^; the median value is +14.5x10^-6^
   days.day^-1^. Of the seven M type Miras with [V-12 {mu}m] colors greater
   than 13.5, six had positive period changes. There is some evidence that C
   type Miras have larger period changes than M and S types.
%K Stars: Variables: Miras
%K Stars: AGB and Post-AGB
%K Stars: Carbon
%K Stars: Evolution
%K Stars: Late-Type
%K Stars: Oscillations

%R 1999PASP..111..104L
%F ori/PASPv111n755
%J-110
%T Telescope Alignment by Out-of-Focus Stellar Image Analysis.
%A Luna, E.
%I Instituto de Astronom\'ia and Observatorio Astron\'omico Nacional, Universidad
   Nacional Aut\'onoma de M\'exico, Apdo. Postal 877, Ensenada, B.C. 22830, M\'exico;
   (eala@bufadora.astrosen.unam.mx)
%A Cordero, A.
%I Benem\'erita Universidad Aut\'onoma de Puebla, Apdo. Postal 1152, Puebla Pue.
   72000, M\'exicoand
%A Valdez, J.
%A Guti\'errez, L.,
%A Salas, L.
%I Instituto de Astronom\'ia and Observatorio Astron\'omico Nacional, Universidad
   Nacional Aut\'onoma de M\'exico, Apdo. Postal 877, Ensenada, B.C. 22830, M\'exico
%B  We present an analysis of the familiar method of analyzing out-of-focus
   stellar images to align Cassegrain reflector telescopes. We measure the asymmetry
   in the out-of-focus image as the difference in positions of the centers of
   the bordering circles. By exact raytracing we find that the asymmetry can
   be expressed as a linear combination of tip/tilt and displacement of the
   secondary mirror. Furthermore and surprisingly, the difference in the positions
   of the centers does not depend on the amount of defocus, and so only two
   parameters of the linear combination are needed to align the telescope. These
   parameters depend only on the telescope design parameters. Finally, we report
   experimental results carried out with the 1.5 m telescope of UNAM, which
   verify the outlined numerical results.
%K Instrumentation: Miscellaneous
%K Methods: Observational
%K Techniques: Miscellaneous
%K Telescopes

%R 1999PASP..111..111C
%F ori/PASPv111n755
%J-117
%T Fringe Visibility Estimators for the Palomar Testbed Interferometer.
%A Colavita, M.M.
%I Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove
   Drive, Pasadena, CA 91109; (Mark.Colavita@jpl.nasa.gov)
%B  Visibility estimators and their performance are presented for use with
   the Palomar Testbed Interferometer (PTI). One operational mode of PTI is
   single-baseline visibility measurement using path length modulation with
   synchronous readout by a NICMOS-3 infrared array. Visibility is estimated
   from the fringe quadratures, either incoherently, or using source phase referencing
   to provide a longer coherent integration time. The visibility estimators
   differ those used with photon-counting detectors in order to account for
   biases attributable to detector offsets and read noise. The performance of
   these estimators is affected not only by photon noise, but also by the detector
   read noise and errors in estimating the bias corrections, which affect the
   incoherent and coherent estimators differently. Corrections for visibility
   loss in the coherent estimators using the measured tracking jitter are also
   presented.
%K Atmospheric Effects
%K Instrumentation: Detectors
%K Instrumentation: Interferometers
%K Techniques: Interferometric

%R 1999PASP..111..118I
%F ori/PASPv111n755
%J-118
%T Star Formation and Environment in a Sample of Galaxies in Compact Groups.
   (Dissertation Summary).
%A Iglesias-P\'aramo, Jorge
%I Current address: Instituto de Astrof\'isica de Canarias, 38200 La Laguna, S/C
   de Tenerife, Spain; (jiglesia@ll.iac.es) Thesis work conducted at Instituto
   de Astrof\'isica de Canarias; Ph.D. degree awarded 1998Ph.D. thesis directed
   by Jos\'e M. V\'ilchez
%K Dissertation Summaries

%R 1999PASP..111..119W
%F ori/PASPv111n755
%J-120
%T Activity in Galaxies and Related Phenomena: IAU Symposium 194(1). (Conference
   Highlights).
%A Weedman, Daniel
%I Department of Astronomy and Astrophysics, Pennsylvania State University
%K Conference Highlights
%I (1) Conference was held in Byurakan, Armenia in 1998 August. Proceedings
   will be edited by Y. Terzian, D. Weedman, and E. Khachikian and published
   in the ASP Conference Series.

%R 1999PASP..111..121M
%F ori/PASPv111n755
%J-122
%T Ultraviolet-Optical Space Astronomy beyond {\em HST}(1). (Conference Highlights).
%A Morse, Jon A.
%A Shull, J.Michael
%I Department of Astrophysical and Planetary Sciences, Center for Astrophysics
   and Space Astronomy, University of Colorado
%K Conference Highlights
%I (1) Conference was held in Boulder, Colorado in 1998 August. The proceedings
   will be edited by J. A. Morse, J. M. Shull, and A. L. Kinney and published
   in the ASP Conference Series.

%R 1999PASP..111..123E
%F ori/PASPv111n755
%J-124
%T Harmonizing Cosmic Distance Scales in a Post-{\em Hipparcos} Era(1). (Conference
   Highlights).
%A Egret, Daniel
%A Heck, Andr\'e
%I Strasbourg Astronomical Observatory, Universit\'e Louis Pasteur, Strasbourg,
   France
%K Conference Highlights
%I (1) Conference was held in Haguenau, France, in 1998 September. Proceedings
   will be edited by Daniel Egret and Andr\'e Heck and published in the ASP Conference
   Series.

%R 1999PASP..111..125W
%F ori/PASPv111n755
%J-126
%T Asymptotic Giant Branch Stars: IAU Symposium 191(1). (Conference Highlights).
%A Waelkens, C.
%A Le Bertre, T.,
%A Lebre, A.
%I Catholic University of Leuven, Belgium, Observatoire de Paris, France,
   University of Montpellier II, France
%K Conference Highlights
%I (1) Conference was held in Montpellier, France in 1998 August. Proceedings
   will be edited by T. Le Bertre, A. L\`ebre, & C. Waelkens and published in
   the IAU Symposium Series.

%R 1999PASP..111..127R
%F ori/PASPv111n755
%J-128
%T Nineteenth NSO/SP International Workshop on High-Resolution Solar Physics:Theory,
   Observations, and Techniques(1). (Conference Highlights).
%A Rimmele, Thomas
%A Balasubramaniam, K.S.,
%A Radick, Richard
%I National Solar Observatory, Sunspot, NM
%K Conference Highlights
%I (1) Conference was held in Sunspot, NM from 1998 September 28 to October
   2.. The proceedings will be edited by T. Rimmele, K. S. Balasubramaniam,
   and R. Radick and published in the ASP Conference Series