Equivalent widths for Fe-group lines in field and cluster metal poor stars.

Abundances of Fe-group elements in field and cluster metal poor stars have been presented in Gratton and Sneden (1990). Presented here is a tabulation of the equivalent widths used in that paper. Errors in these equivalent widths are + or - 2 mA for field stars (observed at a resolution of 50,000 and S/N of 150 or less), and + or - 10 mA in cluster giants (observed at a resolution of 20,000 and S/N of 100 or less). These errors are mainly due to uncertainties (about 1-1.5) in the location of the continuum level.