%...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
%Z=Editor's Notes sup. meterial

%R 2001PASP..113..405G
%F ori/PASPv113n782
%J-408
%T The Unexplored Redshift Survey(1). (Millennium Essay).
%A Geller, Margaret J.
%I Smithsonian Astrophysical Observatory, Cambridge, MA 02138
%B Redshift surveys remain an important constraint on cosmological parameters
   and a key to characterizing the nature and evolution of the large-scale distribution
   of galaxies. I discuss redshift surveys as a route to exploration of other
   issues associated with large-scale structure including the low surface brightness
   universe and the links between star formation and the galaxy distribution.
%K Cosmology: Large-Scale Structure of Universe
%K Galaxies: Distances and Redshifts
%K Surveys
%K Galaxies: Interactions
%K Millennium Essays
%K Stars: Formation
%K X-rays: galaxies
%K X-rays: galaxies: clusters
%I (1) This Essay is one of a series of invited contributions appearing
   in the {\em PASP} throughout the years 2000 and 2001 to mark the new millennium.
   (Eds.)

%R 2001PASP..113..409F
%F ori/PASPv113n782
%J-435
%T The Potential of White Dwarf Cosmochronology(1). (Invited Review).
%A Fontaine, G.
%A Brassard, P.
%A Bergeron, P.
%I D\'epartement de Physique, Universit\'e de Montr\'eal, C.P. 6128, Succ. Centre-Ville,
   Montr\'eal, QC H3C 3J7, Canada; (fontaine@astro.umontreal.ca), (brassard@astro.umontreal.ca),
   (bergeron@astro.umontreal.ca)
%B In the light of recent significant progress on both the observational and
   theoretical fronts, we review the status of white dwarf stars as cosmochronometers.
   These objects represent the end products of stellar evolution for the vast
   majority of stars and, as such, can be used to constrain the ages of various
   populations of evolved stars in the Galaxy. For example, the oldest white
   dwarfs in the solar neighborhood (the remnants of the very first generation
   of intermediate-mass stars in the Galactic disk) are still visible and can
   be used, in conjunction with cooling theory, to estimate the age of the disk.
   More recent observations suggest the tantalizing possibility that a population
   of very old white dwarfs inhabits the Galactic halo. Such a population may
   contribute significantly to baryonic ``dark'' matter in the Milky Way and may
   be used to obtain an independent estimate of the age of the halo. In addition,
   white dwarf cosmochronology is likely to play a very significant role in
   the coming era of giant 8-10 m telescopes when faint white dwarf populations
   should be routinely discovered and studied in open and globular clusters.
%K Galaxy: Fundamental Parameters
%K Galaxy: Halo
%K Galaxy: Globular Clusters: General
%K Invited Reviews
%K Galaxy: Solar Neighborhood
%K Stars: Atmospheres
%K Stars: Evolution
%K Stars: White Dwarfs
%I (1) Based, in part, on the C. S. Beals Lecture presented by G. Fontaine
   at the Annual General Meeting of the Canadian Astronomical Society held in Vancouver
   (2000 May).

%R 2001PASP..113..436B
%F ori/PASPv113n782
%J-438
%T A Coronagraph with a Variable-Diameter Occulting Disk.
%A Bourget, P.
%A Veiga, C.H.
%A Vieira Martins, R.
%I Observat\'orio Nacional, Rua General Jos\'e Cristino 77, 20921-400 Rio de Janeiro,
   Brazil; (pierre@on.br), (cave@on.br), (rvm@on.br)
%B In order to optimize the occulting process of a classical Lyot coronagraph
   for imaging faint satellites next to Jovian planets, we designed a coronagraph
   with a variable-diameter occulting disk (Hg mask). We present the description
   of the Hg-mask coronagraph developed at the Observat\'orio Nacional, Rio de
   Janeiro, and the imaging test on Neptune's satellite Proteus.
%K Instrumentation: Miscellaneous
%K Planets and Satellites: Individual: Neptune
%K planets and satellites: individual (Proteus)

%R 2001PASP..113..439B
%F ori/PASPv113n782
%J-451
%T The Vulcan Photometer: A Dedicated Photometer for Extrasolar Planet Searches.
%A Borucki, William J. (1)
%A Caldwell, Douglas
%A Koch, David G.
%A Webster, Larry D.
%I NASA Ames Research Center, Moffett Field, CA 94035
%A Jenkins, Jon M.
%I SETI Institute, Mountain View, CA 94043
%A Ninkov, Zoran
%I Rochester Institute of Technology, Rochester, NY 14623
%A Showen, Robert
%I Raytheon Systems Company, Moffett Field, CA 94035
%B A small CCD photometer dedicated to the detection of extrasolar planets has
   been developed and put into operation at Mount Hamilton, California. It simultaneously
   monitors 6000 stars brighter than 13th magnitude in its 49 deg^2^ field of
   view. Observations are conducted all night every clear night of the year.
   A single field is monitored at a cadence of eight images per hour for a period
   of about 3 months. When the data are folded for the purpose of discovering
   low-amplitude transits, transit amplitudes of 1% are readily detected. This
   precision is sufficient to find Jovian-size planets orbiting solar-like stars,
   which have signal amplitudes from 1% to 2% depending on the inflation of
   the planet's atmosphere and the size of the star. An investigation of possible
   noise sources indicates that neither star field crowding, scintillation noise,
   nor photon shot noise are the major noise sources for stars brighter than
   visual magnitude 11.6.\par Over one hundred variable stars have been found
   in each star field. About 50 of these stars are eclipsing binary stars, several
   with transit amplitudes of only a few percent. Three stars that showed only
   primary transits were examined with high-precision spectroscopy. Two were
   found to be nearly identical stars in binary pairs orbiting at double the
   photometric period. Spectroscopic observations showed the third star to be
   a high mass ratio single-lined binary. On 1999 November 22 the transit of
   a planet orbiting HD 209458 was observed and the predicted amplitude and
   immersion times were confirmed. These observations show that the photometer
   and the data reduction and analysis algorithms have the necessary precision
   to find companions with the expected area ratio for Jovian-size planets orbiting
   solar-like stars.
%K Instrumentation: Photometers
%K planetary systems: formation
%I (1) (wborucki@mail.arc.nasa.gov).

%R 2001PASP..113..452C
%F ori/PASPv113n782
%J-462
%T The VLT-VIRMOS Mask Manufacturing Unit.
%A Conti, G.
%A Mattaini, E.
%A Chiappetti, L.
%A Maccagni, D.
%A Sant'Ambrogio, E.
%A Bottini, D.
%A Garilli, B.
%I CNR, Istituto di Fisica Cosmica ``G. Occhialini'', via Bassini 15, I-20133
   Milano, Italy; (conti@ifctr.mi.cnr.it)
%A Le F\`evre, O.
%A Saisse, M.
%A Vo\"et, C.
%I Laboratoire d'Astrophysique de Marseille, Traverse du Siphon, F-13376 Marseille,
   France; (Olivier.LeFevre@astrsp-mrs.fr)
%A Caputi, O.
%A Cascone, E.
%A Mancini, D.
%A Mancini, G.
%A Perrotta, F.
%A Schipani, P.
%I Osservatorio Astronomico di Capodimonte, via Moiariello 16, I-80131 Napoli, Italy;
   (mancini@cerere.na.astro.it)
%A Vettolani, G.
%I CNR, Istituto di Radioastronomia, via Gobetti 101, I-40129 Bologna, Italy;
   (vettolani@ira.bo.cnr.it)
%B The VIRMOS Consortium had the task to design and manufacture two spectrographs
   for the ESO Very Large Telescope, VIMOS (Visible Multi-Object Spectrograph)
   and NIRMOS (Near Infrared Multi-Object Spectrograph). This paper describes
   how the mask manufacturing unit (MMU), which cuts the slit masks to be used
   with both instruments, meets the scientific requirements and manages the
   storage and the insertion of the masks into the instrument. The components
   and the software of the two main parts of the MMU, the mask manufacturing
   machine and the mask handling system, are illustrated together with the mask material
   and with the slit properties. Slit positioning is accurate within 15 {mu}m,
   equivalent to 0".03 on the sky, while the slit edge roughness has an rms
   on the order of 0.03 pixels on scales of a slit 5" long and of 0.01 pixels
   on the pixel scale (0".205). The MMU was successfully installed during 2000
   July/August at the Paranal Observatory and is now operational for spectroscopic
   mask cutting, in compliance with the requested specifications.
%K Instrumentation: Spectrographs

%R 2001PASP..113..463D
%F ori/PASPv113n782
%J-468
%T An Automated Scheme for the Large-Scale Survey of Herbig-Haro Objects.
%A Deng, Licai (1)(3)(4)(5)
%A Yang, Ji (2)(3)(4)
%A Zheng, Zhongyuan (1)(3)(4)
%A Jiang, Zhaoji (1)(3)(4)
%B Owing to their spectral properties, Herbig-Haro (HH) objects can be
   discovered using photometric methods through a combination of filters, sampling
   the characteristic spectral lines and the nearby continuum. The data are
   commonly processed through direct visual inspection of the images. To make
   data reduction more efficient and the results more uniform and complete,
   an automated searching scheme for HH objects is developed to manipulate the
   images using IRAF. This approach helps to extract images with only intrinsic
   HH emissions. By using this scheme, the pointlike stellar sources and extended
   nebulous sources with continuum emission can be eliminated from the original
   images. The objects with only characteristic HH emission become prominent
   and can be easily picked up. In this paper our scheme is illustrated by a
   sample field and has been applied to our surveys for HH objects.
%K ISM: Herbig-Haro objects
%K Methods: Data Analysis
%K Methods: Miscellaneous
%I (1) Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing
   100012, China.
%I (3) BAC: Chinese Academy of Sciences-Peking University Joint Beijing
   Astrophysical Center.
%I (4) Chinese National Astronomical Observatories, Chinese Academy of Sciences,
   A20 Datun Road, Chaoyang District, Beijing 100012, China.
%I (5) (denglicai@china.com).
%I (2) Purple Mountain Observatory, Academia Sinica, Nanjing 210008, China.

%R 2001PASP..113..469H
%F ori/PASPv113n782
%J-472
%T On Echo Outbursts and ER UMa Supercycles in SU UMa-Type Cataclysmic Variables.
%A Hellier, Coel
%I Department of Physics, Keele University, Staffordshire ST5 5BG, UK; (ch@astro.keele.ac.uk)
%B I present a variation on Osaki's tidal thermal instability model for
   SU UMa behavior. I suggest that in systems with the lowest mass ratios, the
   angular momentum dissipation in an eccentric disk is unable to sustain the
   disk on the hot side of the thermal instability. This decoupling of the tidal
   and thermal instabilities in systems with q{<~}0.07 allows a better explanation
   of the ``echo'' outbursts of EG Cnc and the short supercycles of RZ LMi and
   DI UMa. The idea might also apply to the soft X-ray transients.
%K accretion, accretion disks
%K Stars: Binaries: Close
%K Stars: Novae, Cataclysmic Variables

%R 2001PASP..113..473H
%F ori/PASPv113n782
%J-481
%T Similarities between Stunted Outbursts in Nova-like Cataclysmic Variables
   and Outbursts in Ordinary Dwarf Novae.
%A Honeycutt, R.K.
%I Astronomy Department, Indiana University, Swain Hall West, Bloomington, IN
   47405; (honey@astro.indiana.edu)
%B Stunted outbursts have been reported in old novae and nova-like cataclysmic
   variables by Honeycutt, Robertson, and Turner. These 0.4-1 mag outbursts
   were concluded to be either mass transfer events or disk outbursts similar
   to dwarf nova eruptions, but seen under unusual conditions. Honeycutt, Robertson,
   and Turner did not have enough evidence to favor either of these possibilities.
   This paper uses additional long-term photometry and analysis to argue that
   the similarities of these stunted outbursts to dwarf nova eruptions are now
   so numerous that the dwarf nova outburst choice is strongly favored. The
   similarities discussed here include the range of outburst spacings, the coherence
   and stability of the outbursts, and the presence of isolated outburst/dip pairs.
   As part of this discussion we note the presence of unexpectedly stable clocks
   over 9 years for the repetition interval of dwarf nova outbursts in SY Cnc
   and of stunted outbursts in FY Per.
%K Stars: Novae, Cataclysmic Variables
%K stars: individual (DI Lacertae)
%K stars: individual (RW Trianguli)
%K stars: individual (SW Sextantis)
%K Stars: Individual: Constellation Name: BH Lyncis
%K stars: individual (V841 Ophiuchi)
%K stars: individual (GI Monocerotis)
%K stars: individual (CT Serpentis)
%K stars: individual (FY Persei)
%K Stars: Individual: Constellation Name: SS Cygni
%K Stars: Individual: Constellation Name: HX Pegasi
%K Stars: Individual: Constellation Name: SY Cancri
%K Stars: Individual: Constellation Name: RW Sextantis
%K Stars: Individual: Constellation Name: Q Cygni
%K Stars: Individual: Constellation Name: CP Lacertae
%K stars: individual (V825 Herculis)
%K Stars: Individual: Constellation Name: AH Herculis
%K Stars: Individual: Constellation Name: HX Pegasi
%K Stars: Individual: Constellation Name: Z Camelopardalis

%R 2001PASP..113..482H
%F ori/PASPv113n782
%J-489
%T Optical Photometry of the Double-lined Cataclysmic Variable Phoenix 1.
%A Hoard, D.W.
%A Wachter, S.
%I Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile; (dhoard@noao.edu),
   (swachter@noao.edu)
%A Kim-Quijano, Jessica (1)
%I Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218;
   (jkim@stsci.edu)
%B We have obtained 7 nights of time-resolved {\em VI} photometry of the
   double-lined cataclysmic variable Phoenix 1. We detect two candidate orbital
   periods, 0.1344 day and 0.2683 day. The former, which would correspond to
   a single modulation caused by viewing the irradiated face of the secondary
   star, is the less favored choice based on the folded light curves. The latter,
   which would correspond to a double modulation with unequal minima depths
   caused by ellipsoidal variation of the secondary star, is inconsistent with
   the observed late spectral type (M2-5) of the secondary star. However, we
   discuss some recent results from the literature that may make it possible
   to reconcile the longer orbital period and later spectral type. Some ambiguity
   remains as to which of these two periods is the true orbital period.
%K accretion, accretion disks
%K Stars: Novae, Cataclysmic Variables
%K Stars: Individual: Constellation Name: Phoenix 1
%I (1) 1999 participant in the Cerro Tololo Inter-American Observatory Research
   Experiences for Undergraduates (REU) Program.

%R 2001PASP..113..490W
%F ori/PASPv113n782
%J-500
%T A Search for Binary Hot Subdwarfs. I. {\em BVRI} Photometry of Palomar-Green
   Survey sdO Stars.
%A Williams, Tom
%A McGraw, John T.
%A Grashuis, Randy
%I Department of Physics and Astronomy, University of New Mexico, Albuquerque,
   NM 87131; (tw@as.unm.edu)
%B Nine binary candidates have been identified from a sample of 64 hot subdwarf
   sdO/OB/OC stars selected from the Palomar-Green Survey. Three of the binary
   candidates had been identified previously. The binary candidates emerged
   from {\em BVRI} photometric observations and were identified by their intrinsic
   color excesses in two-color plots and by comparison to synthetic binary system
   colors. The data presented here are the initial results of a larger program
   aimed at identifying helium-rich hot subdwarf binary systems suitable for
   more detailed investigation of their fundamental stellar parameters and evolutionary status.
%K Stars: Binaries: General
%K Stars: Fundamental Parameters
%K Stars: Horizontal-Branch

%R 2001PASP..113..501H
%F ori/PASPv113n782
%J-506
%T R Centauri: An Unusual Mira Variable in a He-Shell Flash.
%A Hawkins, G.
%A Mattei, J.A.
%A Foster, G.
%I American Association of Variable Star Observers (AAVSO), 25 Birch Street,
   Cambridge, MA 02138; (hawkins@aavso.org), (jmattei@aavso.org), (gfoster@aavso.org)
%B We present an analysis of AAVSO visual observations of the Mira variable R
   Cen from 1918 to 2000. The period of the dominant mode has been steadily decreasing
   from 550 days at JD 2,434,000 (1951) to its present value of 505-510 days.
   In the same interval, the pulsational amplitude has decreased by 3 mag, from
   5.5-11.8 {\em V} to 6.3-9.1 {\em V}. We suggest that both are caused by a
   He-shell flash, as the period decrease is similar to that of other He-shell
   flash stars such as R Hya, R Aql, and T UMi. The period change is consistent
   with the luminosity drop expected immediately after the flash, as predicted
   by He-shell flash models for stars of 2-3 {\em M}_{sun}_ or less.\par The
   light curve shows the familiar pattern of alternating deep and shallow minima,
   giving the appearance of double maxima. While the amplitude of the main mode
   has decreased 3 mag in the last 50 years, the amplitude of the secondary
   mode near 274 days has remained almost constant, so that the double maxima
   have nearly vanished from the light curve in recent years. The power spectrum
   between 1930 and 1966 shows harmonics up to 8 times the main frequency at
   1/548 cycle.day^-1^. The most likely explanation for the double-peaked light
   curve is a resonance between two modes.
%K Stars: Variables: Miras
%K Stars: AGB and Post-AGB
%K stars: individual (R Centauri)
%K Stars: Late-Type

%R 2001PASP..113..507B
%F ori/PASPv113n782
%J-507
%T Raman Scattering in Symbiotic Stars. (Dissertation Summary).
%A Birriel,  Jennifer J.
%I Current address: Department of Physics and Astronomy, Carleton College, Northfield, MN
   55057; (jbirriel@carleton.edu)Thesis work conducted at Department of Physics
   and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260Ph.D. thesis
   directed by Regina E. Schulte-Ladbeck; Ph.D. degree awarded 2000 August
%K Stars: Binaries: General
%K Stars: Circumstellar Matter
%K Stars: Mass Loss
%K Dissertation Summaries

%R 2001PASP..113..508F
%F ori/PASPv113n782
%J-509
%T Gamma-Ray Bursts in the Afterglow Era: Second Workshop(1). (Conference Highlights).
%A Feroci, Marco
%I Istituto di Astrofisica Spaziale, CNR, Rome
%K Conference Highlights
%K gamma rays: bursts
%I (1) Conference was held at CNR Headquarters in Rome, Italy, on 2000 October 17-20.
   Proceedings will be edited by E. Costa, F. Frontera, and J. Hjorth and published
   in the ESO Proceedings Series.

%R 2001PASP..113..510V
%F ori/PASPv113n782
%J-511
%T Cosmic Evolution(1). (Conference Highlights).
%A Vangioni-Flam, Elisabeth
%A Cass\'e, Michel
%I Institut d'Astrophysique de Paris
%K Conference Highlights
%I (1) Conference was held in Paris, France, in 2000 November. Proceedings
   will be edited by Roger Ferlet, Martin Lemoine, and Elisabeth Vangioni-Flam
   and published by World Scientific.

%R 2001PASP..113..512G
%F ori/PASPv113n782
%J-513
%T {eta} Carinae and Other Mysterious Stars: Hidden Opportunities for Emission
   Spectroscopy(1). (Conference Highlights).
%A Gull, Theodore R.
%I NASA Goddard Space Flight Center, Laboratory for Astronomy and Solar Physics, Code
   681, Greenbelt, MD 20771
%K Conference Highlights
%I (1) Conference was held in Hven, Sweden, in 2000 August. Proceedings
   will be edited by Theodore R. Gull, Sveneric Johansson, and Kris Davidson
   and published in the ASP Conference Series.

%R 2001PASP..113..514C
%F ori/PASPv113n782
%J-514
%T Review Articles in the {\em PASP}. (Editorial).
%A Cowley, Anne
%A Hartwick, David
%I {\em PASP} Editors, Arizona State University and University of Victoria;
   (pasp@asu.edu), (pasp@uvic.ca)