survey stars are generally higher at the low metallicity end of the scale, and lower at the high metallicity end of the scale, as compared to the old calibration. The abundance estimates for the cooler stars with $0.5 <
(B-V)_o \le 1.2$ have changed relatively less.

As part of the re-calibration effort, Table 7 of Beers et al. (1999) lists averaged high-resolution abundance determinations from the literature for 551 stars. For stars which also appear in the revised catalog, we adopted these averaged abundance determinations.

The catalog of Cayrel de Strobel et al. (1997) provides detailed information on abundances for stars with determinations based on high-resolution spectroscopy. Suitably averaged abundances for stars which did not appear in Beers et al. (1999) were adopted for the revised catalog listing. A number of stars from MFF have been shown by Ryan & Lambert (1995) to suffer from mis-estimated abundances (generally too low) arising from a faulty calibration of DDO photometry. For MFF stars with high-resolution abundances obtained by Ryan & Lambert, we simply adopt their values. For other MFF stars which are included in the revised catalog, the abundances should be considered uncertain.

Metallicity estimates for the revised catalog are reported in 