ADC/CDS Standard Document for Catalog:
/journal_tables/A+A/290/885/

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

J/A+A/290/885       Abundances of very metal-poor stars          (Primas+, 1994)
================================================================================
Abundances of four very metal-poor stars of the BPS survey
       Primas F., Molaro P., Castelli F.
      <Astron. Astrophys. 290, 885 (1994)>
      =1994A&A...290..885P      (SIMBAD/NED Reference)
================================================================================
ADC_Keywords: Stars, metal-deficient; Abundances
Keywords: stars: abundances - stars: population II - Galaxy: abundances -
          Galaxy: halo

Abstract:
    High resolution CASPEC and EMMI spectra (R=~10^4^) of the faint 
    metal-deficient candidates CS 22891-209, CS 22897-8, CS 22948-66 and 
    CS 22968-14 taken from the survey of Beers et al. (1985, BPS) are analyzed
    for abundances. The fine analysis with LTE model atmospheres gives an iron
    metallicity for the four stars between -3.15 and -3.45 in good agreement 
    with the abundances inferred from CaII K index by Beers et al. (1992). 
    These four objects considerably augment the number of spectroscopically 
    studied stars at the low metallicity extreme. We found the {alpha}-elements
    Mg, Ca, Si, and Ti enhanced, and the iron-peak elements Sc, Mn and Cr 
    tracking closely iron with the typical pattern of the more metallic halo 
    stars. Aluminum results deficient with respect both to iron and to 
    magnesium showing a strong odd-even effect, but for [Fe/H]<=-3.0[Al/Mg] 
    levels out into a plateau around -1.0, showing a primary behaviour. [Na/Fe]
    is =~-0.2 and only compared to magnesium it shows a mild odd-even effect. 
    The heavy elements Sr and Ba show a large scatter which is not observed for
    other elements and cannot be due to observational errors only. In the case 
    of CS 22891-209 they are particularly overabundant with [Sr,Ba/Fe]=~0.9. 
    The spread might reflect the presence of strong inhomogeneities in the 
    interstellar gas at the earliest stages of Galaxy formation. This might be
    an important signature of the still elusive processes of the early 
    formation of these elements observed in old stars. 

File Summary:
--------------------------------------------------------------------------------
 FileName     Lrecl    Records    Explanations
--------------------------------------------------------------------------------
ReadMe          80          .    This file
table3         128        207    Equivalent widths and abundances for all the
                                  lines detected in our stars
table3.tex     144        310    LaTeX version of table3
--------------------------------------------------------------------------------

Byte-by-byte Description of file: table3
--------------------------------------------------------------------------------
   Bytes Format  Units   Label   Explanations
--------------------------------------------------------------------------------
   1-  4  A4     ---     El.     Element
       6  A1     ---     Aver    A 'A' indicates average
   7- 13  F7.2   0.1nm   W       []? Wavelength
  15- 18  F4.2   eV      Chi     []? Excitation potential
  20- 24  F5.2   ---     log(gf) []? log of oscillation strength
  27- 29  I3     0.1pm   EW1     []? Equivalent width for CD-38 245
      30  A1     ---   n_EW1     [+*] Note on equivalent width (1)
  31- 36  F6.2   ---     logA1   []? Abundance (logN/logN_tot_) for CD-38 245
  40- 43  F4.2   ---   e_logA1   []? rms uncertainty of logA1 for average
  46- 48  I3     0.1pm   EW2     []? Equivalent width for CS 22891-209
      49  A1     ---   n_EW2     [+*] Note on equivalent width (1)
  50- 55  F6.2   ---     logA2   []? Abundance (logN/logN_tot_) for CS 22891-209
  59- 62  F4.2   ---   e_logA2   []? rms uncertainty of logA2 for average
  65- 67  I3     0.1pm   EW3     []? Equivalent width for CS 22897-8
      68  A1     ---   n_EW3     [+*] Note on equivalent width (1)
  69- 74  F6.2   ---     logA3   []? Abundance (logN/logN_tot_) for CS 22897-8
  78- 81  F4.2   ---   e_logA3   []? rms uncertainty of logA3 for average
  84- 86  I3     0.1pm   EW4     []? Equivalent width for CS 22948-66
      87  A1     ---   n_EW4     [+*] Note on equivalent width (1)
  88- 93  F6.2   ---     logA4   []? Abundance (logN/logN_tot_) for CS 22948-66
  97-100  F4.2   ---   e_logA4   []? rms uncertainty of logA4 for average
     102  A1     ---   l_EW5     limit flag on EW5
 103-105  I3     0.1pm   EW5     []? Equivalent width for CS 22968-14
     106  A1     ---   n_EW5     [+*] Note on equivalent width (1)
     107  A1     ---   l_logA5   limit flag on logA5
 108-113  F6.2   ---     logA5   []? Abundance (logN/logN_tot_) for CS 22968-14
 117-120  F4.2   ---   e_logA5   []? rms uncertainty of logA5 for average
 124-128  F5.2  [Sun]    logASun []? Solar abundance (logN/logN_tot_)
-------------------------------------------------------------------------------
Note (1): * : Lines not included in WIDTH;
          + : Lines with an abundance greater than 1{sigma}.
--------------------------------------------------------------------------------
================================================================================
(End)                                        Patricia Bauer  [CDS]   30-Jun-1994