We investigate the origin of stellar
halos using a high resolution cosmological SPH + N-Body simulation that
includes all the major physical processes involved in galaxy formation
self-consistently (Governato et al 2007). This simulation allows us to
study the competing importance of dissipative in-situ star formation
and accretion off of subhalos in the building of a stellar halo in a
$Lambda$CDM universe. We find that the Milky Way-sized galaxy in the
simulation is surrounded by a kinematically defined stellar halo with
more than one distinct population. We search for tracers of this
complex formation history in a sample defined to match a SDSS-like
observer. 3-D stellar velocities are analyzed for signatures which
might be helpful in understanding the buildup of the Milky Way's stellar halo.
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