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5 A review and a description of the catalog

The catalog discussed here has been derived by choosing suitable input data (mostly from the literature), applying initial corrections to those data, and then subjecting them to a statistical analysis. Improvements in the published data include 1) correction to a common temperature scale, 2) correction of the output averages to a zero point which is presumably uniform, and 3) derivation of rms errors for those averages. The final version of the catalog is available from the Strasbourg Astronomical Data Center (CDS) and has entries for 941 stars. A sample of the catalog is given in Table 7.


 

 
Table 7: A sample of the [Fe/H] catalog${\rm ^a}$.

Catalog
      No. of  
number${\rm ^b}$ [Fe/H] $\sigma$ $\phantom{{\rm ^c}}\nu{\rm ^c}$ sources Sources${\rm ^d}$

400
-0.274 0.058 99.0 3 565, 2055, 2072
693 -0.414 0.045 99.0 3 565, 624, 2003
739 -0.122 0.054 99.0 2 624, 2003
1461 0.138 0.079 99.0 3 166, 2001, 2004
1671 -0.130 0.100 17.2 1 2003
$^{{\rm a}}$
This sample reproduces catalog entries, but differs from the catalog in format. For [Fe/H] and $\sigma$, units are dex.
$^{{\rm b}}$
The numbers listed are HD numbers. In the catalog, prefixes designate other star catalogs, while "A'' and "B'' suffixes designate components of binaries (when required).
$^{{\rm c}}$
This is the number of degrees of freedom.
$^{{\rm d}}$
The numbers correspond to the following literature sources: 166, Branch & Bell (1971); 565, Balachandran (1990); 624, Edvardsson et al. (1993); 2001, Raff (1976); 2003, Nissen (1981); 2004, Clegg et al. (1981); 2055, Fuhrmann (1998); 2072, Chen et al. (2000). In the catalog, a complete list of numbers and references appears in a supplementary list.


Acknowledgements
Dr. G. Basri alerted me to the existence of Dr. Valenti's Ph.D. Thesis, and Drs. Basri and Valenti then made a copy of that thesis available to me. Phil Warner set up for my use the plot package used to produce Fig. 1. Mike and Lisa Joner proofread the paper carefully, and two anonymous referees made a number of constructive suggestions for improving the paper. I cheerfully thank all these individuals while noting that page charges for this paper have been generously underwritten by the College of Physical and Mathematical Sciences and the Physics and Astronomy Department of Brigham Young University.


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