%...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 2004PASP..116..187T
%F ori/PASPv116n817 
%J-265
%DOI 10.1086/383241
%T Astrophysics in 2003. (Invited Review).
%A Trimble, Virginia
%I Department of Physics and Astronomy, University of California, Irvine, CA
   92697; and Astronomy Department, University of Maryland, College Park, MD
   20742; (vtrimble@astro.umd.edu)
%A Aschwanden, Markus J.
%I Lockheed Martin Advanced Technology Center, Solar and Astrophysics Laboratory,
   Organization ADBS, Building 252,3251 Hanover Street, Palo Alto, CA 94304;
   (aschwand@lmsal.com)
%B Five coherent sections appear this year, addressing solar physics, cosmology
   (with {\em WMAP} highlights), gamma-ray bursters (and their association with
   Type Ia supernovae), extra-solar-system planets, and the formation and evolution
   of galaxies (from reionization to assemblage of Local Group galaxies). There
   are also eight incoherent sections that deal with other topics in stellar,
   galactic, and planetary astronomy and the people who study them. Invited
   Reviews

%R 2004PASP..116..266B
%F ori/PASPv116n817 
%J-000277
%DOI 10.1086/382735
%T Wide-Field Millimagnitude Photometry with the HAT: A Tool for Extrasolar
   Planet Detection.
%A Bakos, G.(1)(2)(3)
%A Noyes, R.W.(1)
%A Kov\'acs, G.(2)
%A Stanek, K.Z.(1)
%A Sasselov, D.D.(1)
%A Domsa, I.(2)
%B We discuss the system requirements for obtaining millimagnitude photometric
   precision over a wide field using small-aperture, short focal length telescope
   systems such as those being developed by a number of research groups to search
   for transiting extrasolar planets. We describe a Hungarian Automated Telescope
   (HAT) system, which attempts to meet these requirements. The attainable precision
   of HAT has been significantly improved by a technique in which the telescope
   is made to execute small pointing steps during each exposure so as to broaden
   the effective point-spread function (PSF) of the system to a value more compatible
   with the pixel size of our CCD detector. Experiments during a preliminary
   survey (spring 2003) of two star fields with the HAT-5 instrument allowed
   us to optimize the HAT photometric precision using this method of PSF broadening;
   in this way we have been able to achieve a precision as good as 2 mmag on
   brighter stars. We briefly describe development of a network of longitudinally
   spaced HAT telescopes (HATNet).
%K Instrumentation: Miscellaneous
%K Telescopes
%K Techniques: Photometric
%K planetary systems
%K Stars: Variables: Other
%K Methods: Data Analysis
%I (1) Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge,
   MA 02138; (gbakos@cfa.harvard.edu), (rnoyes@cfa.harvard.edu), (kstanek@cfa.harvard.edu),
   (dsasselov@cfa.harvard.edu).
%I (2) Konkoly Observatory, P.O. Box 67, H-1525, Budapest, Hungary; (kovacs@konkoly.hu),
   (domsa@konkoly.hu).
%I (3) Predoctoral Fellow, Smithsonian Astrophysical Observatory.

%R 2004PASP..116..278D
%F ori/PASPv116n817 
%J-289
%DOI 10.1086/382756
%T Photometry of a Sodium Laser Guide Star at the Starfire Optical Range.
%A Drummond, Jack (1)
%A Telle, John (1)
%A Denman, Craig (1)
%A Hillman, Paul (1)
%A Tuffli, Andrea (2)
%B Measurements of a laser-pumped sodium guide star produced over the Starfire
   Optical Range in 2002 November show that the brightness of the spot produced
   by 11.5 W of linearly polarized power on the sky was equivalent to a V=8.0
   mag star. However, taking into account that the transmission through a {\em
   V} filter is only 55% at the wavelength of sodium, its corrected magnitude,
   V_1_, was 7.4, or 800 photons/s/cm2 at the top of the telescope. In
   2003 March, tests with linearly and then circularly polarized beams out of
   the telescope showed that a circularly polarized beam from 12 W of power
   out of the telescope produced a spot with V_1_=7.1 (1015 photons/s/cm2
   at the top of the telescope), 0.7 mag brighter than a linearly polarized
   beam from 11.1 W of power out of the telescope. Over the 4 nights of experiments
   over two seasons, the apparent 2{sigma} width of the spot varied between
   3".6 and 4".6, or 1.6 and 2.0 m at 92 km altitude, and its length through
   the sodium layer was 4.6-8.5 km, but no variation of spot size with power
   on the sky was seen.
%K instrumentation: lasers
%K Instrumentation: Adaptive Optics
%K Polarization
%K atomic processes
%I (1) Starfire Optical Range, Directed Energy Directorate, Air Force Research
   Laboratory, Kirtland Air Force Base, NM 87117-5776.
%I (2) Boeing LTS, The Boeing Company, P.O. Box 5670, Kirtland Air Force
   Base, NM 87185.

%R 2004PASP..116..290P
%F ori/PASPv116n817 
%J-294
%DOI 10.1086/382664
%T Horace Welcome Babcock (1912-2003). (Obituary).
%A Preston, George W.
%I Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101; (gwp@ociw.edu)
%B Over a span of 40 years, Horace Babcock invented numerous astronomical
   instruments and procedures, the most important of which continue to be used
   after his death. Along the way he created a branch of astrophysics and founded
   one of the world's premier astronomical observatories.
%K Instrumentation: Miscellaneous
%K Obituaries, Biographies
%K Sun: magnetic fields
%K Stars: Magnetic Fields