estimate (as described below) is listed in column (13).

### Estimates of Reddening

Our primary source of total reddening in the directions of the sample stars is the new map of Schlegel, Finkbeiner, & Davis (1998, hereafter SFD) based on [*COBE*]{} and [*IRAS*]{} measurements of dust emission in the Galaxy. The SFD map is superior to the widely used map of Burstein & Heiles (1982, hereafter BH) in its spatial resolution and its zero point (see also Gould & Popowski 1998 for arguments in favor of the SFD map). Note, however, that Arce & Goodman (1999) caution that the SFD map overestimates the reddening values when the color excess $E_{B-V}$ is more than about 0.15 mags, where SFD’s calibration from dust column density to reddening may no longer be accurate. For the small number of stars where this large reddening applies, we have adopted estimates from the BH map, where available. The few program stars in such highly reddened directions are generally located at small distances from the Sun, so that the effects of correction for reddening on distance estimates are small.

We adopt a $V$-band absorption $A_V = 3.1 E_{B-V}$ and assume that the dust layer has a scale 