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J/PASP/109/883                Globular metallicity scale. I. (Rutledge+ 1997)
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Galactic globular cluster metallicity scale from the Ca II triplet I. Catalog
     Rutledge G.A., Hesser J.E., Stetson P.B., Mateo M., Simard L.,
     Bolte M., Friel E.D., Copin Y.
    <Publ. Astron. Soc. Pac. 109, 883 (1997)>
    =1997PASP..109..883R
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ADC_Keywords: Clusters, globular ; Photometry, calcium triplet ;
              Radial velocities

Abstract:
    We have obtained 2640 CCD spectra with resolution ~4{AA} in the region
    7250-9000{AA} for 976 stars lying near the red giant branches in
    color-magnitude diagrams of 52 Galactic globular clusters. Radial
    velocities of ~16km/s accuracy per star determined from the spectra
    are combined with other criteria to assess quantitative membership
    probabilities. Measurements of the equivalent widths of the infrared
    calcium triplet lines yield a relative metal-abundance ranking with a
    precision that compares favorably to other techniques. Regressions
    between our system and those of others are derived. Our reduction
    procedures are discussed in detail, and the resultant catalog of
    derived velocities and equivalent widths is presented. The metal
    abundances derived from these data will be the subject of a future
    paper.
    (c)  Astronomical Society of the Pacific

File Summary:
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 FileName    Lrecl    Records   Explanations
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ReadMe          80          .   This file
table9.dat      95        766   Individual star data and results
table9.tex     140        886   AASTeX version of table9.dat
table9.ps       72       3870   PostScript version
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See also:
    VII/195 : Globular Clusters in the Milky Way (Harris, 1996)

Byte-by-byte Description of file: table9.dat
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   Bytes Format  Units      Label      Explanations
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   1-  8  A8     ---        Cluster   *Cluster name
  11- 25  A15    ---        Star       Star name
  27- 30  I4     km/s       DRV       *Calulated velocity minus cluster velocity
  33- 37  F5.2   mag        V(HB)-Vmag V magnitude of star above the horizontal
                                          branch
  40- 43  F4.2   mag        (B-V)0    *? Dereddened B-V color
  45- 48  F4.2   0.1nm      dCa        Weighted mean {SIGMA}Ca (net Ca II index)
                                        of the star
  50- 53  F4.2   0.1nm    e_dCa        External error of dCa
  55- 56  I2     %          Pmu        ? Probability of membership from
                                           proper-motion data
  58- 59  I2     %          Pvel       Probability of membership from our
                                         calculated velocities
  61- 64  F4.2   ---        fp        *? f_p_ value
  66- 69  F4.2   ---        fr        *? f_r_ value
  71- 74  F4.2   ---        w         *? w value
  76- 77  I2     ---        Nspect    Number of spectra analyzed for the star
  79- 88  A10    ---        Night    *Night the star was observed
  90- 95  A6     ---        Notes    *Notes
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Note on Cluster:
  Name of the globular cluster, repeated for each observed star in that
  cluster. The authors also included the following alternative names for
  some clusters:
    NGC 104 = 47 Tuc    NGC 6273 = M 19
    NGC 4590 = M 68     NGC 6637 = M 69
    NGC 5904 = M 5      NGC 6681 = M 70
    NGC 6093 = M 80     NGC 6717 = Pal 9
    NGC 6121 = M 4      NGC 6809 = M 55
    NGC 6171 = M 107    NGC 6981 = M 72
    NGC 6218 = M 12     NGC 7089 = M 2
    NGC 6254 = M 10     NGC 7099 = M 30
    NGC 6266 = M 62
Note on DRV:
  Difference between the authors' calculated velocity of the star (see Section 4
  of the printed paper) and the velocity given in the MWGC catalog
  (Cat. <VII/195>.
Note on (B-V)0:
  Dereddened B-V color of the star determined with E(B-V) from the MWGC catalog.
Note on fp, fr, w:
  The f_p, f_r, and final weight, w, respectively, used in the authors' fitting
   technique to calculate the reduced equivalent width, W' of the the cluster.
   See Section 6 of the printed paper for technique, and Table 2 of the paper
   for W' values; the weight has been scaled in each cluster
Note on Night:
  The nights the star was observed, where the first number indicates the
   observing run, and the other numbers indicate the specific night of
   observation. Therefore, 1-1 represents 1989 April 13, 1-2 represents
   1989 April 14, ..., and 2-1 represents 1989 July 13.
Note on Notes:
  0: Star not used to compute reduced EW for cluster,
  1: See cluster notes in Appendix A,
  2: Weak TiO present,
  3: Strong TiO present,
  4: Possible AGB star,
  5: Possible HB star,
  6: Non-cluster member based on position in CMD,
  7: Crowded field,
  8: Uncertain ID,
  9: Star has weak {SIGMA}Ca for V_HB - V position,
 10: Star has strong {SIGMA}Ca for V_HB - V position,
 11: Suntzeff & Kraft (1996AJ....111.1913S) suggest that line strength is
      variable.
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References:
    Rutledge et al., Paper II.  1997PASP..109..907R

Origin: AAS CD-ROM series, Volume 9, 1997         Lee Brotzman [ADS] 04-Nov-1997
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(End)                                                         [CDS]  06-Feb-1998