  We present Keck 10-meter/LRIS spectra of candidate red giants in the halo of
M31, located at a projected radius of R=19kpc on the minor axis. These
spectroscopic targets have been selected using a combination of UBRI-based and
morphological screening to eliminate background galaxies. Radial velocity
measurements are used to separate M31 halo giants from foreground Milky Way
dwarf stars, M31 disk stars, and residual background galaxies. The metallicity
of each M31 halo giant is measured using standard photometric and spectroscopic
techniques, the latter based on the strength of the CaII triplet. The various
[Fe/H] estimates are in rough agreement with one another. The data reveal a
large spread (>2dex) in [Fe/H] in M31's halo; there is no strong radial [Fe/H]
gradient. LRIS and HIRES spectra are also presented for red giants in five
dwarf spheroidal satellites of M31: AndI, AndIII, AndV, AndVI, and AndVII.
There appears to be a significant metallicity spread in AndVI and possibly in
AndI. The new radial velocity data on these outer dwarfs are used to constrain
the total mass of M31: the best estimate is under 10^(12)Msun, somewhat less
than the best estimate for the Milky Way.
