%...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..113.1309B
%F ori/PASPv113n789
%J-1311
%T The Future of Gravitational Optics(1). (Millenium Essay).
%A Blandford, R.D.
%I 130-33 California Institute of Technology, 1200 East California Boulevard,
   Pasadena, CA 91125
%B In this speculative, millennial essay, I try to anticipate what sort
   of novel gravitational optics investigations might be undertaken after it
   becomes possible to map and monitor roughly 10^12^ sources (of which 10^9^
   may be usefully variable) comprehensively throughout electromagnetic and
   other spectra over the whole sky. Existing techniques suffice to produce
   three-dimensional maps of the dark matter distribution of the accessible
   universe, to explore black hole spacetimes, and to magnify images of the
   first luminous sources, terrestrial planets, and compact objects.
%K Cosmology: Gravitational Lensing
%I (1) This Essay is one of a series of invited contributions that will
   appear in the {\em PASP} throughout the years 2000 and 2001 to mark the new
   millennium. (Eds.)

%R 2001PASP..113.1312C
%F ori/PASPv113n789
%J-1325
%T Galaxy Correlation Statistics of Mock Catalogs for the DEEP2 Survey.
%A Coil, Alison L. (1)
%A Davis, Marc (1)
%A Szapudi, Istvan (2)
%B The Deep Extragalactic Evolutionary Probe 2 (DEEP2) project will obtain
   redshifts for ~60,000 galaxies in the range z=~0.7-1.5 in a comoving volume
   of roughly 7x10^6^ Mpc^3^ {\em h}^-3^ for a {Lambda} cold dark matter universe.
   The survey will map four separate 2{deg}x0{deg}.5 strips of the sky. To study
   the expected clustering within the survey volume, we have constructed mock
   galaxy catalogs from the GIF and Hubble Volume simulations developed by the
   Virgo consortium. We present two- and three-point correlation analyses of
   these mock galaxy catalogs to test how well we will measure these statistics,
   particularly in the presence of selection biases, which will limit the surface
   density of galaxies that we can select for spectroscopy. We find that although
   the projected angular two-point correlation function w({theta}) is strongly
   affected, neither the two-point nor three-point correlation functions, {xi}(r)
   and {zeta}(r), are significantly compromised. We will be able to make simple
   corrections to account for the small amount of bias introduced. We quantify
   the expected redshift distortions due to random orbital velocities of galaxies
   within groups and clusters (``fingers of God'') on small scales of ~1 Mpc {\em
   h}^-1^ using the pairwise velocity dispersion {sigma}_12_ and galaxy-weighted
   velocity dispersion {sigma}_1_. We are able to measure {sigma}_1_ to a precision
   of ~10%. We also estimate the expected large-scale coherent infall of galaxies
   due to supercluster formation (``Kaiser effect''), as determined by the quadrupole-to-monopole
   ratio {xi}_2_/{xi}_0_ of {xi}(r_p_, {pi}). From this measure we will be able
   to constrain {beta} to within ~0.1 at z=1.\par For the DEEP2 survey we will
   combine the correlation statistics with galaxy observables such as spectral
   type, morphology, absolute luminosity, and line width to enable a measure
   of the relative biases in different galaxy types. Here we use a counts-in-cells
   analysis to measure {sigma}_8_ as a function of redshift and determine the
   relative bias between galaxy samples based on absolute luminosity. We expect
   to measure {sigma}_8_ to within 10% and detect the evolution of relative
   bias with redshift at the 4-5 {sigma} level, with more precise measurements
   for the brighter galaxies in our survey.
%K Galaxies: Distances and Redshifts
%K Galaxies: Evolution
%K Galaxies: Statistics
%K Cosmology: Large-Scale Structure of Universe
%K Surveys
%I (1) Department of Astronomy, 601 Campbell Hall, University of California,
   Berkeley, Berkeley, CA 94720-3411; (acoil@astro.berkeley.edu), (marc@astro.berkeley.edu).
%I (2) Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive,
   Honolulu, HI 96822; (szapudi@ifa.hawaii.edu).

%R 2001PASP..113.1326G
%F ori/PASPv113n789
%J-1348
%T A Robotic Wide-Angle H{alpha} Survey of the Southern Sky.
%A Gaustad, John E.
%I Department of Physics and Astronomy, Swarthmore College, Swarthmore, PA 19081;
   (jgausta1@swarthmore.edu)
%A McCullough, Peter R. (1)
%I Department of Astronomy, University of Illinois, Urbana, IL 61801; (pmcc@astro.uiuc.edu)
%A Rosing, Wayne
%I Las Cumbres Observatory, 1297 West Mountain Drive, Santa Barbara, CA 93103;
   (wrosing@lco.org)
%A Van Buren, Dave
%I Extrasolar Research Corporation, Niskayuna, NY 12309; (vanburen@extrasolar.com)
%B We have completed a robotic wide-angle imaging survey of the southern
   sky ({delta}=+15{deg} to -90{deg}) at 656.3 nm wavelength, the H{alpha} emission
   line of hydrogen. Each image of the resulting Southern H{alpha} Sky Survey
   Atlas (SHASSA) covers an area of the sky 13{deg} square at an angular resolution
   of approximately 0'.8 and reaches a sensitivity level of 2 R (1.2x10^-17^
   ergs cm^-2^.s^-1^.arcsec^-2^) pixel^-1^, corresponding to an emission measure
   of 4 cm^-6^.pc and to a brightness temperature for microwave free-free emission
   of 12 {mu}K at 30 GHz. Smoothing over several pixels allows features as faint
   as 0.5 R to be detected.
%K Cosmology: Cosmic Microwave Background
%K ISM: H II Regions
%K Instrumentation: Miscellaneous
%K ISM: Structure
%K Surveys
%K Techniques: Image Processing
%I (1) Cottrell Scholar of Research Corporation.

%R 2001PASP..113.1349H
%F ori/PASPv113n789
%J-1364
%T {\em BVRI} Photometry of Supernovae.
%A Ho, Wynn C.G. (1)(2)
%A Van Dyk, Schuyler D. (3)
%A Peng, Chien Y. (4)
%A Filippenko, Alexei V. (5)
%A Leonard, Douglas C. (6)
%A Matheson, Thomas (7)
%A Treffers, Richard R. (8)
%I Department of Astronomy, 601 Campbell Hall, University of California, Berkeley,
   CA 94720-3411
%A Richmond, Michael W. (9)
%I Department of Physics, Rochester Institute of Technology, Rochester, NY 14623-5603
%B We present optical photometry of one Type IIn supernova (1994Y) and nine
   Type Ia supernovae (1993Y, 1993Z, 1993ae, 1994B, 1994C, 1994M, 1994Q, 1994ae,
   and 1995D). SN 1993Y and SN 1993Z appear to be normal SN Ia events with similar
   rates of decline, but we do not have data near maximum brightness. The colors
   of SN 1994C suggest that it suffers from significant reddening or is intrinsically
   red. The light curves of SN 1994Y are complicated; they show a slow rise
   and gradual decline near maximum brightness in {\em VRI} and numerous changes
   in the decline rates at later times. SN 1994Y also demonstrates color evolution
   similar to that of the SN IIn 1988Z, but it is slightly more luminous and
   declines more rapidly than SN 1988Z. The behavior of SN 1994Y indicates a
   small ejecta mass and a gradual strengthening of the H{alpha} emission relative
   to the continuum.
%K Stars: Supernovae: General
%K supernovae: individual (SN 1993Y)
%K supernovae: individual (SN 1993Z)
%K supernovae: individual (SN 1993ae)
%K supernovae: individual (SN 1994B)
%K supernovae: individual (SN 1994C)
%K supernovae: individual (SN 1994M)
%K supernovae: individual (SN 1994Q)
%K supernovae: individual (SN 1994Y)
%K supernovae: individual (SN 1994ae)
%K supernovae: individual (SN 1995D)
%I (1) Also associated with Space Sciences Laboratory, and Department of
   Physics, University of California, Berkeley.
%I (2) Present address: Department of Astronomy, Cornell University, Ithaca,
   NY 14853; (wynnho@astro.cornell.edu).
%I (3) Present address: Infrared Processing and Analysis Center, 100-22,
   California Institute of Technology, Pasadena, CA 91125; (vandyk@ipac.caltech.edu).
%I (4) Present address: Steward Observatory, University of Arizona, Tucson,
   AZ 85721; (cyp@as.arizona.edu).
%I (5) (alex@astro.berkeley.edu).
%I (6) Present address: Department of Astronomy, University of Massachusetts,
   Amherst, MA 01003-9305; (leonard@nova.astro.umass.edu).
%I (7) Present address: Harvard-Smithsonian Center for Astrophysics, 60
   Garden Street, Cambridge, MA 02138; (tmatheso@cfa.harvard.edu).
%I (8) (treffers@pacbell.net).
%I (9) (mwrsps@rit.edu).

%R 2001PASP..113.1365B
%F ori/PASPv113n789
%J-1377
%T Lick Spectral Indices for Super-Metal-rich Stars(1).
%A Buzzoni, A.
%I Telescopio Nazionale Galileo, A.P. 565, E-38700 Santa Cruz de La Palma, Canary
   Islands, Spain; and Osservatorio Astronomico di Brera, Milano, Italy; (buzzoni@tng.iac.es)
%A Chavez, M.
%I Instituto Nacional de Astrof\'isica, Optica y Electr\'onica, A.P. 51 y 216, 72000
   Puebla, Mexico; (mchavez@inaoep.mx)
%A Malagnini, M.L.
%I Dipartimento di Astronomia, Universit\`a di Trieste, Via G. B. Tiepolo 11,
   I-34131 Trieste, Italy; (malagnini@ts.astro.it)
%A Morossi, C.
%I Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34131 Trieste,
   Italy; (morossi@ts.astro.it)
%B We present Lick spectral indices for a complete sample of 139 candidate
   super-metal-rich stars of different luminosity classes (MK type from I to
   V). For 91 of these stars we were able to identify, in an accompanying paper,
   the fundamental atmosphere parameters. This confirms that at least 2/3 of
   the sample consists of stars with [Fe/H] in excess of +0.1 dex. Optical indices
   for both observations and fiducial synthetic spectra have been calibrated
   to the Lick system according to Worthey et al. and include the Fe I indices
   of Fe5015, Fe5270, and Fe5335 and the Mg I and MgH indices of Mg_2_ and Mg
   {\em b} at 5180 {AA}. The internal accuracy of the observations is found to
   be {sigma}(Fe5015)=+/-0.32 {AA}, {sigma}(Fe5270)=+/-0.19 {AA}, {sigma}(Fe5335)=+/-0.22
   {AA}, {sigma}(Mg_2_)=+/-0.004 mag, and {sigma}(Mg b)=+/-0.19 {AA}. This is about a
   factor of 2 better than the corresponding theoretical indices from the synthetic
   spectra, the latter being a consequence of the intrinsic limitations in the
   input physics, as discussed by Chavez et al.\par By comparing models and
   observations, we find no evidence for nonstandard Mg versus Fe relative abundance,
   so [Mg/Fe]=0, on the average, for our sample. Both the Worthey et al. and
   Buzzoni et al. fitting functions are found to suitably match the data and
   can therefore confidently be extended for population synthesis application
   also to supersolar metallicity regimes. A somewhat different behavior of
   the two fitting sets appears, however, beyond the temperature constraints
   of our stellar sample. Its impact on the theoretical output is discussed,
   as far as the integrated Mg_2_ index is derived from synthesis models of
   stellar aggregates. A two-index plot, such as Mg_2_ versus Fe5270, is found
   to provide a simple and powerful tool for probing distinctive properties
   of single stars and stellar aggregates as a whole. The major advantage, over
   a classical CM diagram, is that it is both reddening free and distance independent.
%K Galaxy: Stellar Content
%K Stars: Abundances
%K Stars: Atmospheres
%K Stars: Fundamental Parameters
%I (1) Based on observations collected at the Instituto Nacional de Astrof\'isica,
   Optica y Electr\'onica (INAOE) ``G. Haro'' Observatory, Cananea (Mexico).

%R 2001PASP..113.1378G
%F ori/PASPv113n789
%J-1385
%T Betelgeuse: Giant Convection Cells.
%A Gray, David F.
%I Department of Physics and Astronomy, University of Western Ontario, London,
   ON N6A 3K7, Canada; (dfgray@uwo.ca)
%B Spectroscopic observations of the M supergiant star Betelgeuse were
   taken at the Elginfield Observatory over 17 months in the 1999-2000 observing
   seasons in order to search for giant convection cells. Although the photospheric
   spectral lines show some temporal variations, mainly in their depths (consistent
   with a previously study), the Doppler shift distribution inferred from them
   is remarkably stable. The spectral lines show characteristic macroturbulence
   dispersion ~15 km.s^-1^ and cover a full span of +/-50-60 km.s^-1^. The widths
   of the lines show occasional as well as longer term changes of a few percent
   but no evidence for giant convection cells. These spectroscopic observations
   are more consistent with a classical picture of nonthermal photospheric velocities
   in which large numbers of convection cells appear on the stellar disk at
   all times.
%K Stars: Atmospheres
%K Stars: Late-Type
%K Stars: Variables: Other
%K Stars: Supergiants

%R 2001PASP..113.1386M
%F ori/PASPv113n789
%J-1392
%T Position and Variability of 2A 1704+241.
%A Morgan, W.A. Jr
%I Department of Physics and Astronomy, Dickinson College, P.O. Box 1773, Carlisle,
   PA 17013; (morgan@dickinson.edu)
%A Garcia, M.R.
%I Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge,
   MA 02138; (mgarcia@head-cfa.harvard.edu)
%B We present results of analyses of observations of the X-ray source 2A
   1704+241 with the {\em ROSAT} Position Sensitive Proportional Counter (PSPC)
   and the High Resolution Imager (HRI). The source 2A 1704+241 was first associated
   with the M giant star HD 154791 based on observations with the {\em HEAO
   1} scanning modulation collimator and the {\em Einstein} IPC and analysis
   of a spectrum of HD 154791 obtained with the {\em International Ultraviolet
   Explorer}. This identification was unusual because there are few bright X-ray
   binaries associated with an M giant star. We observed 2A 1704+241 with the
   PSPC and the HRI in order to determine more accurately the position of the
   X-ray source and in order to study the previously seen 900 s variability
   in the {\em Einstein} data. Based on the previous identification and determination
   of the position of MS 1703.7+2417, an active galactic nucleus in the field,
   and the position of three previously unreported X-ray sources that we have
   associated with stars in the USNO-A2.0 catalog, we have greatly reduced the
   X-ray positional error of 2A 1704+241. HD 154791 remains the prime candidate
   as the optical counterpart of the X-ray source. While the 50% modulation
   in the X-ray flux seen by the {\em Einstein} IPC is apparent in the {\em
   ROSAT} data, it appears to be at a slightly different frequency.
%K Astrometry
%K stars: individual (HD 154791)
%K stars: individual (2A 1704+241)
%K X-rays: stars

%R 2001PASP..113.1393L
%F ori/PASPv113n789
%J-1405
%T A Finding List of Faint UV-bright Stars in the Galactic Plane. VI.
%A Lanning, Howard H.
%I Computer Sciences Corporation/Science Programs, Space Telescope Science Institute,
   3700 San Martin Drive, Baltimore, MD 21218; (lanning@stsci.edu)
%A Meakes, Michael
%I Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218;
   (meakes@stsci.edu)
%B Three additional plates from the Sandage two-color survey of the Galactic
   plane have been examined, yielding identifications of 113 UV-bright stars.
   Plates were obtained using the Palomar 48 inch Oschin Schmidt telescope and
   cover a field of view of 43 deg^2^. The plates were centered at the Galactic
   longitude ({\em l}) and latitude ({\em b}) coordinates of 141{deg}, +6{deg}; 164{deg},
   +0{deg}; and 164{deg}, -6{deg}. Sources identified range in {\em U}-{\em B} color from
   {\em U}-B~-0.1 to {\em U}-B~-1.2 and in magnitude from m_B_~10 to ~20. Accurate
   J2000.0 coordinates and finding charts are provided for all the UV candidates
   included. Some of the more interesting sources are discussed. Previously
   identified objects described in the literature are noted.
%K Stars: Early-Type
%K Stars: Emission-Line, Be
%K Stars: Subdwarfs
%K Surveys
%K Stars: White Dwarfs

%R 2001PASP..113.1406L
%F ori/PASPv113n789
%J-1419
%T Characterization of Lenslet Arrays for Astronomical Spectroscopy.
%A Lee, David (1)
%A Haynes, Roger
%I Anglo-Australian Observatory, P.O. Box 296, Epping, NSW 1710, Australia;
   (dl@aaoepp.aao.gov.au), (rh@aaoepp.aao.gov.au)
%A Ren, Deqing (2)
%A Allington-Smith, Jeremy
%I Astronomical Instrumentation Group, University of Durham, Physics Department,
   South Road, Durham, DH1 3LE, UK; (j.r.allington-smith@durham.ac.uk), (deqing.ren@durham.ac.uk)
%B Microlens arrays are now widely used in a variety of astronomical instruments
   that require high performance. This paper describes the applications of microlenses
   in astronomical spectroscopy and discusses the necessary performance requirements.
   A variety of optical tests, including high dynamic range point-spread function
   measurements and determination of encircled energy, were developed to characterize
   the performance of a variety of lenslet arrays. Results are presented that indicate
   the best types of lenslet array for use for astronomical spectroscopy.
%K Instrumentation: Spectrographs
%I (1) Present address: Corning Optical Fibres, Ltd., 2d Avenue, Deeside
   Industrial Park, Deeside, CH5 2NX, UK; leed1@corning.com.
%I (2) Present address: National Solar Observatory, P.O. Box 62, Sunspot,
   NM 88349; ren@nso.edu.

%R 2001PASP..113.1420V
%F ori/PASPv113n789
%J-1427
%T Cosmic-Ray Rejection by Laplacian Edge Detection.
%A van Dokkum, Pieter G. (1)
%I California Institute of Technology, MS 105-24, Pasadena, CA 91125; (pgd@astro.caltech.edu)
%B Conventional algorithms for rejecting cosmic rays in single CCD exposures
   rely on the contrast between cosmic rays and their surroundings and may produce
   erroneous results if the point-spread function is smaller than the largest
   cosmic rays. This paper describes a robust algorithm for cosmic-ray rejection,
   based on a variation of Laplacian edge detection. The algorithm identifies
   cosmic rays of arbitrary shapes and sizes by the sharpness of their edges
   and reliably discriminates between poorly sampled point sources and cosmic
   rays. Examples of its performance are given for spectroscopic and imaging
   data, including {\em Hubble Space Telescope} Wide Field Planetary Camera
   2 images.
%K Instrumentation: Detectors
%K Methods: Data Analysis--techniques: image processing
%I (1) Hubble Fellow.

%R 2001PASP..113.1428E
%F ori/PASPv113n789
%J-1435
%T A Technique for Ultrahigh-Precision CCD Photometry.
%A Everett, Mark E. (1)
%A Howell, Steve B. (1)
%I Astrophysics Group, Planetary Science Institute, 620 North 6th Avenue, Tucson,
   AZ 85705; (everett@psi.edu), (howell@psi.edu)
%B We present techniques for wide-field ultrahigh-precision time-sampled
   CCD photometry. Representing a survey of field stars, our data consist of
   {\em UBVRI} photometry and a {\em V}-band time series of exposures on 5 consecutive
   nights covering 11,500 stars in a ~1 deg^2^ field. The resulting light curves
   reach precisions of 0.0020 mag per exposure in the brightest stars (V~14).
   Light curves binned and averaged over 4.5 hr reach precisions of 0.00019
   mag for the brightest stars. We present example light curves and discuss
   one application for surveys of this type: the search for transits by extrasolar
   planets.
%K Stars: Variables: General
%K Techniques: Photometric
%I (1) Visiting Astronomer, Kitt Peak National Observatory.

%R 2001PASP..113.1436S
%F ori/PASPv113n789
%J-1437
%T The Morphology, Environment, and Interstellar Medium of Early-Type Galaxies
   as a Means for Studying the Evolution of Galaxies Outside of Clusters. (Dissertation
   Summary).
%A Saucedo-Morales, Julio C\'esar
%I Current address: \'Area de Astronom\'ia, Departamento de Investigaci\'on en F\'isica
   de la Universidad de Sonora, Rosales y Bulevar Transversal, 8300 Hermosillo
   Sonora, Mexico; (jsaucedo@cosmos.astro.uson.mx)Thesis work conducted at Steward
   Observatory, University of ArizonaPh.D. thesis directed by John Bieging;
   Ph.D. degree awarded 2000 August
%K Galaxies: Elliptical and Lenticular, cD
%K Galaxies: Evolution
%K Galaxies: Formation
%K Galaxies: ISM
%K Galaxies: Photometry

%R 2001PASP..113.1438P
%F ori/PASPv113n789
%J-1439
%T Supernova Remnants and Cosmic-Ray Acceleration in Nearby Galaxies. (Dissertation
   Summary).
%A Pannuti, Thomas G.
%I Current address: Massachusetts Institute of Technology Center for Space Research,
   77 Massachusetts Avenue, NE80-6015, Cambridge, MA 02139; (tpannuti@space.mit.edu)Thesis
   work conducted at Department of Physics and Astronomy, University of New
   MexicoPh.D. thesis directed by Nebojsa Duric; Ph.D. degree awarded 2000 December
%K ISM: Cosmic Rays
%K Galaxies: Individual: NGC Number: NGC 300
%K Galaxies: Individual: NGC Number: NGC 7793
%K Galaxies: Individual: NGC Number: NGC 6946
%K Galaxies: Spiral
%K ISM: Supernova Remnants