III/131     Spectroscopic Stellar Abundance Analyses (Koeppen 1988)
================================================================================
A Critical Catalogue of Spectroscopic Stellar Abundance Analyses
    Koeppen J.
   <CDS Inf. Bull. No. 34, p. 143 (1988)>
   =1988BICDS..34..143K
================================================================================
ADC_Keywords: Abundances

Description:
    The original catalogue (files *.ori) contains condensed descriptions
    of all spectroscopic abundance analyses (as far as the metallicity is
    derived) are given for normal stars (chemically peculiar stars are not
    included). Based on these descriptions, the "best" abundance
    determination(s) have been selected and indicated by a quality code.
    Index files and software tools are included in the catalog.

File Summary:
--------------------------------------------------------------------------------
 FileName   Lrecl  Records   Explanations
--------------------------------------------------------------------------------
ReadMe         80        .   This file
stars.dat      68      730  *The main index of analyzed stars
intro.ori      72      735   Explanations concerning the next files:
hdstars.ori    72    17205   Detailed results about HD stars
dmstars.ori    72      751   Detailed results about Durchmusterung stars
cluster.ori    72     2085   Detailed results about cluster stars not in HD
otherst.ori    72       90   Detailed results Other stars
indexst.ori    72     4864   Indexes
refs.ori       72     2646   References (383), List of stars with extensive
                             line lists (2227), Some more line lists (37)
programs.ori   72     3733  *Software Tools (FORTRAN programs)
--------------------------------------------------------------------------------
Note on stars.dat: file created in March 1997 at CDS from indexst.ori
Note on programs.ori: the programs were used to generate the indexes
     in 1987 on a mainframe; they were not adapted to PCs or
     workstations.
--------------------------------------------------------------------------------

See also:
    III/165 : Catalogue of [Fe/H] determinations (Cayrel et al., 1992)

Byte-by-byte Description of file: stars.dat
--------------------------------------------------------------------------------
   Bytes Format Units   Label     Explanations
--------------------------------------------------------------------------------
   1- 15  A15   ---     Name      Star name
  17- 31  A15   ---     SpType    Spectral classification
  34- 35  I2    h       RAh       [0/23]? Right Ascension 1950 (hours)
  37- 40  F4.1  min     RAm       [0/60[? Right Ascension 1950 (minutes)
      43  A1    ---     DE-       Declination 1950 (sign)
  44- 45  I2    deg     DEd       [0/90[? Declination 1950 (degrees)
  47- 48  I2    arcmin  DEm       [0/60[? Declination 1950 (minutes)
  52- 56  F5.2  mag     Vmag      ? Visual magnitude (from SIMBAD)
  59- 62  A4    ---     FeClass  *[-+0? ] Iron abundance given in classes (1)
  65- 68  A4    ---     Qual     *[RLI? ()] Quality of best analysis (2)
--------------------------------------------------------------------------------
Note (1): The iron abundance is given in classes of [Fe/H]
      (log(Fe/H) relative to the abundance of the Sun) :
      +             [Fe/H] >= +0.3    overabundance
      0      -0.3 < [Fe/H] <= +0.3    solar abund.
      -      -0.6 < [Fe/H] <= -0.3    under abund.
      --     -1.0 < [Fe/H] <= -0.6       ditto
      ---    -2.0 < [Fe/H] <= -1.0       ditto
      ----          [Fe/H] <= -2.0       ditto
      ?      Fe/H either not determined (e.g. in hot stars) or
             the abundances from the available analyses differ
             wildly from each other, e.g. in Vega and Deneb.
             As a consequence those studies which use such a star
             as a reference, also inherit this question mark!

Note (2): the codes are:
    R = "RECOMMENDABLE"
        State-of-the-art analysis or nearly so:
        use of models to take fully into account the temperature
        stratification in the atmosphere, use of appropriate
        line-blanketing and NLTE-effects where necessary.
        Use of the broadest possible observational data, both
        in respect of wavelengths (IR...UV where appropriate),
        and variety (scans, photometry, line profiles).
    L = "LIMITATIONS":
        Not quite the best possible analysis by today's(1987)
        means. The analysis is recommendable despite some
        limitations. Examples:
         * using un-blanketed models for cool stars, for which
           line-blanketed models are necessary and available;
         * using only optical data for hot stars, where the most
           important part of the spectrum lies in the ultraviolet;
         * using single slab models('coarse analysis') though
           model atmospheres are available -- J. Koeppen accepts
           only differential studies.
    I = "IMPROVEMENT NEEDED":
        Analysis with serious limitations, such as:
         * absolute curve-of-growth analysis;
         * very limited observational base.
        Therefore it could be desirable to have this star re-observed
        or the data re-analyzed with more modern techniques.
   ( ) = Brackets indicate that this is the only analysis available
     ? = Question mark indicates that information about the analysis
        method was found to be insufficient to make a definitive
        choice of the quality grade, e.g.:
        paper mentions analysis only very briefly.
--------------------------------------------------------------------------------

================================================================================
(End)        Joachim Koeppen, Francois Ochsenbein [Strasbourg Obs.]  05-Mar-1997