J/PASP/109/883 Globular metallicity scale. I. (Rutledge+ 1997)
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 1997PASP..109..883R
ADC_Keywords: Clusters, globular ; Photometry, calcium triplet ;
Radial velocities
Abstract:
We have obtained 2640 CCD spectra with resolution ∼4Å in the region
7250-9000Å 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 *? fp value
66- 69 F4.2 --- fr *? fr 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 1996AJ....111.1913S) suggest that line strength is
variable.
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References:
Rutledge et al., Paper II. 1997PASP..109..907R 1997PASP..109..907R
Origin: AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 04-Nov-1997
(End) [CDS] 06-Feb-1998