revised classifications provide photometric distance estimates which are more consistent with the [*Hipparcos*]{} parallaxes, as described below. Revised classifications are also provided for a number of the HK survey stars, based on more recent observations.

There still remains some uncertainty in the classification of a number of stars with relatively blue colors \[$0.3 \le (B-V)_o \le 0.5$\]. If the corresponding stars have $(U-B)_o$ color data from the HK survey, the stars are classified as FHB if $(U-B)_o > -0.1$, or TO if $(U-B)_o \le -0.1$ (Wilhelm, Beers, & Gray 1999). This crude discrimination scheme is adequate for stars with abundances $\feh<-1.5$. For more metal-rich stars, we also consider the alternative classification as possible, and assign a classification of FHB/TO.

### Templates for Distance Estimation

RR Lyrae distance scales have been reconsidered extensively subsequent to the release of the [*Hipparcos*]{} Catalogue, based on a variety of methods including main-sequence fitting, the Baade-Wesselink method, and statistical parallax. Combining all of the results, Chaboyer (1999) proposed the following $M_V$ [*vs.*]{} $\feh$ relation:

$$M_V (RR) = 0.23 ( \feh + 1.6 ) + 0.56 \ ,$$

where $M_V (RR)$ denotes the absolute magnitude of RR Lyrae stars. We adopt this relation to estimate the 