adopted positions, respectively. The source of the position is indicated in column (4).

Revisions of Abundance Estimates, Velocities, and Distances
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Revisions of Abundance Estimates
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Roughly 45 % of the stars in the revised catalog were originally identified during the course of the HK objective-prism survey. In the BSL catalog the abundance estimates for these stars were obtained from a calibration of the strength of the CaII K line as a function of $(B-V)_o$ color described in Beers et al. (1990). This calibration is now known to suffer from several deficiencies, the most worrisome of which is the fact that assigned abundances in the range $\feh > -1.5$ are less than optimal as a result of the saturation of the CaII K line, in particular at cooler temperatures. Stars in the metallicity regime $-2.0 \le \feh \le -1.0$ represent the transition between the halo and thick disk populations, and in particular, may be members of the MWTD component of the Galaxy, hence it is important that the abundances be correctly estimated. At the low end of the metallicity scale ($\feh < -2.5
$), the lack of available calibrators in the Beers et al. (1990) treatment resulted in stellar abundance 