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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
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:
FileName Lrecl Records Explanations
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
See also: VII/195 : Globular Clusters in the Milky Way (Harris, 1996) Byte-by-byte Description of file: table9.dat
Bytes Format Units Label Explanations
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
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.
References: Rutledge et al., Paper II. 1997PASP..109..907R Origin: AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 04-Nov-1997
(End) [CDS] 06-Feb-1998
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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