then used to convert the GSC $B$ magnitude estimate to an approximate $V$ magnitude. Given the multiple approximations in these procedures, these estimates should be regarded with appropriate caution – these stars are indicated in Table 1A with parentheses around the $V$ and $B-V$ magnitude estimates. In a few cases, apparent magnitudes for HK survey stars that were not found in the GSC are estimated from the intensity of the spectrum on the original prism plate, and are indicated as such with brackets around the $V$ and $B-V$ magnitudes in the table.

For a number of stars, $V$ magnitudes and $b-y$ colors are available from Schuster et al. (1996), Schuster et al. (2000), or Anthony-Twarog et al. (2000). For these stars, we have listed an approximate $B-V$ color obtained by adopting the transformation $B-V= 1.35\; (b-y)$, and indicate these cases with parentheses about the approximate $B-V$ color in . For RR Lyrae variables, the intensity-averaged $V$ magnitudes, where available, are taken from either Layden (1994), Layden et al. (1996), or Fernley et al. (1998). The adopted photometric quantities are reported in columns (10) and (11) of Table 1A; the source of the photometry is given in column (12); a reddening 