  We present first results from a Keck/DEIMOS spectroscopic survey of red giant
branch (RGB) stars in M33. The radial velocity distributions of the stars in
our fields are well described by three Gaussian components, corresponding to a
candidate halo component with an uncorrected radial velocity dispersion of
sigma ~ 50km/s, a candidate disk component with a dispersion sigma ~ 16km/s,
and a third component offset from the disk by ~ 50km/s, but for which the
dispersion is not well constrained. By comparing our data to a model of M33
based upon its HI rotation curve, we find that the stellar disk is offset in
velocity by ~ 25km/s from the HI disk, consistent with the warping which exists
between these components. The spectroscopic metallicity of the halo component
is [Fe/H] ~ -1.5, significantly more metal-poor than the implied metallicity of
the disk population ([Fe/H] ~ -0.9), which also has a broader colour dispersion
than the halo population. These data represent the first detections of
individual stars in the halo of M33 and, despite being ~ 10 times less massive
than M31 or the Milky Way, all three of these disk galaxies have stellar halo
components with a similar metallicity. The color distribution of the third
component is different to the disk and the halo, but is similar to that
expected for a single, coeval, stellar population, and could represent a
stellar stream. More observations are required to determine the true nature of
this intriguing third kinematic component in M33.
