et al. (1999).

In order to estimate distances for the hotter main-sequence gravity A-type stars (i.e., those with colors $-0.10 \le (B-V)_o \le 0.34$) we apply a small vertical shift to the $M_V$ vs $(B-V)_o$ relation for the Pleiades so that it matches that of the Hyades at $(B-V)_o = 0.34$. To account for the expected decline in luminosity with decreasing abundance, the adjusted Pleiades line is corrected by applying shifts of the same size as those derived for the cooler stars on the main sequence of the metal-poor globulars as compared to the Hyades. We note that this is only one of several choices we could have made, and it may not be the optimal one, but it should serve for the present purpose.

Taking all of the above information into account, distances are then estimated by means of an iteration procedure which includes modification of the interstellar reddening. These distances, $D_{pho}$, are indicated in column (2) of Table 1B. In some cases there was no reliable photometry or classification available, and, occasionally, our iteration scheme failed to converge. In these circumstances we made use of the distances provided in the original BSL catalog (who, in such cases, adopted 