ADC/CDS Standard Document for Catalog:
/journal_tables/AJ/112/601/

1. Use the ADC Data Viewer Suite to visualize the data.
2. Get the data files via anonymous FTP. (See Note.)

J/AJ/112/601               UV photometry in M79 (Hill+ 1996)
================================================================================
UIT: New ultraviolet stellar photometry and surface brightness 
profiles of the globular cluster M 79 (NGC 1904)
     Hill R.S., Cheng K.-P., Smith E.P., Hintzen P.M.N., Bohlin R.C.,
     OConnell R.W., Roberts M.S., Smith A.M., Stecher T.P.
    <Astron. J. 112, 601 (1996)>
    =1996AJ....112..601H
================================================================================
ADC_Keywords: Clusters, globular ; Photometry, ultraviolet
Mission_Name: Ultraviolet Imaging Telescope

Abstract:
    Ultraviolet photometry is presented for the globular cluster M79 (NGC
    1904) according to the final calibration of the images obtained on the
    Astro-1 Spacelab mission by the Ultraviolet Imaging Telescope. These
    results include both point-source and surface photometry at 152nm and
    249nm. An ultraviolet color-magnitude (C-M) diagram in these
    bandpasses is presented. The detected stars are also cross-matched
    with the ground-based photometry of Ferraro et al.
    (1992MNRAS.256..391F) to produce C-M and two-color diagrams covering a
    4000A span in wavelength. The observed horizontal branch (HB) is
    compared with stellar interior models of the zero-age HB (ZAHB). Many
    stars are found in post-HB evolutionary stages more luminous than the
    ZAHB. The distribution of stars along the ZAHB in m152-m249 color is
    investigated, and an indication of possible bimodality is found. The
    relative population of the blue HB tail may vary with radius for radii
    greater than 1'. Ultraviolet surface brightness and color-index
    profiles are presented. The previously reported central gradient in
    the m152-V color index is confirmed, and a faint diffuse component is
    detected outside a radius of 40" in the 152nm band. Two possible
    causes of the central color gradient are discussed: mass segregation,
    and the destruction of red giant envelopes by enhanced mass loss in
    the cluster core.

File Summary:
--------------------------------------------------------------------------------
 FileName    Lrecl    Records   Explanations
--------------------------------------------------------------------------------
ReadMe          80          .   This file
table3.dat      82        136   UV stellar photometry of M79
--------------------------------------------------------------------------------

Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
   Bytes Format  Units   Label      Explanations
--------------------------------------------------------------------------------
   1-  3  I3     ---       Star     Ordinal number of UIT-detected star in M79
       5  A1     ---       Note    *[g] Table note mark
   7-  8  I2     h         RAh      Right ascension (J2000)
  10- 11  I2     min       RAm      Right ascension (J2000)
  13- 17  F5.2   s         RAs      Right ascension (J2000)
      19  A1     ---       DE-      Declination sign
  20- 21  I2     deg       DEd      Declination (J2000)
  23- 24  I2     arcmin    DEm      Declination (J2000)
  26- 29  F4.1   arcsec    DEs      Declination (J2000)
  32- 36  F5.2   mag       m152    *UIT magnitude in the 152nm (B1) band
  38- 42  F5.2   mag       C152-249 UIT color index 152nm (B1) - 249nm (A1)
  44- 48  F5.3   mag     e_m152     Formal error in UIT 152nm (B1) magnitude
  50- 54  F5.3   mag     e_m249     Formal error in UIT 249nm (A1) magnitude
  56- 60  F5.1   arcsec    R        Distance of UIT source from cluster center
  62- 65  A4     ---       Qnote   *Note on quality of observation
  67- 70  I4     ---       IDF92   *? Star number from Ferraro et al., 1992
  72- 76  F5.2   mag       B-VF92   ? B-V color index from Ferraro et al., 1992
  78- 82  F5.2   mag       VmagF92  ? V magnitude from Ferraro et al., 1992
--------------------------------------------------------------------------------
Note on Note:
  Table note mark "g": Star 94=UIT-1 and star 76 = UIT-2 as
  discussed in Paper I (Hill, R. S. et al. 1992ApJ...395L..17H).
  Stars 26, 67, 100, 109, and 127 are in the area observed by F92
  but have no F92-HB match with B-V<0.4. Stars 111, 120, and 122
  are ambiguously matched by two or more F92 (1992MNRAS.256..391F) HB stars.
Note on m152:
  UIT magnitude in the 152nm (B1) band. Magnitudes are defined as
  -2.5*log(flux)-21.1, where log is base 10, and flux is f sub
  lambda in units of ergs/cm2/s/A.
Note on Qnote:
  Note on quality of observation.
 *: UIT source is within 5 pixels (5.7arcsec) of more than one HB star of F92;
    if an F92 number is given, it is judged the most likely candidate according
    to color index and distance from the UIT source position.
 C: Obvious crowding in one or both UIT bands, as determined by inspection;
     stars without this note may still be affected by crowding if r<~40arcsec.
 Lowercase f or n: An aperture magnitude is substituted for a PSF magnitude
   with error greater than 0.2mag, for image FUV0141 or NUV0124, respectively.
 Entries 134-136 have aperture photometry only.
Note on IDF92:
  The complete reference F92 is the following: Ferraro, F. R., Clementini,
  G., Fusi Pecci, F., Sortino, R., and Buonanno, R., (1992MNRAS.256..391F)
--------------------------------------------------------------------------------

Origin: AAS CD-ROM series, Volume 7, 1996         Lee Brotzman [ADS] 13-Aug-1996
================================================================================
(End)                                                         [CDS]  30-Jan-1997