  We validate the Bond et al. (2010) kinematic models for the Milky Way's disk
and halo stars with Gaia Data Release 3 data. Bond et al. constructed models
for stellar velocity distributions using stellar radial velocities measured by
the Sloan Digital Sky Survey (SDSS) and stellar proper motions derived from
SDSS and the Palomar Observatory Sky Survey astrometric measurements. These
models describe velocity distributions as functions of position in the Galaxy,
with separate models for disk and halo stars that were labeled using SDSS
photometric and spectroscopic metallicity measurements. We find that the Bond
et al. model predictions are in good agreement with recent measurements of
stellar radial velocities and proper motions by the Gaia survey. In particular,
the model accurately predicts the skewed non-Gaussian distribution of
rotational velocity for disk stars and its vertical gradient, as well as the
dispersions for all three velocity components. Additionally, the spatial
invariance of velocity ellipsoid for halo stars when expressed in spherical
coordinates is also confirmed by Gaia data at galacto-centric radial distances
of up to 15 kpc.
