  We present results from a Keck spectroscopic survey of red giants in a field
near M31's major axis, ~34kpc in projection from the nucleus, near the globular
cluster G1. We use multislit LRIS spectroscopy to measure the CaII triplet in
41 stars with apparent mags 20<I<22. Of these, 23 stars are found to have
radial velocities v<-200km/s indicating they are giants in M31; the rest are
probably foreground Galactic stars. About 2/3 of the M31 members concentrate at
v=-451km/s, with a velocity spread of sigma=27km/s, which suggests that they
belong to the outer disk or perhaps a cold debris trail in the halo. The
group's mean velocity is consistent with that of nearby HI gas and models of
M31's disk velocity field but not with G1 or M31's systemic velocity. We use
V,I photometry to estimate a mean metallicity of <[Fe/H]>=-0.8 for these
potential M31 outer disk stars. Six of the 23 M31 members v and [Fe/H] values
consistent with those of G1 (after accounting forits intrinsic spread in both):
one of these stars lies within G1's projected tidal radius and is a likely
member; the remaining 5 stars are not physically close to G1 but may represent
its tidal debris. More data are needed to confirm the nature of these 5 stars
as it is likely that they represent M31's smooth halo population. We might have
expected to detect tidal debris if G1 were the remnant core of a dwarf galaxy
being accreted by M31; instead, the majority of M31 giants in this field are
metal-rich and belong to what is evidently the outer disk of M31, and only a
small fraction (<~20%) could possibly have originated in G1.
