  The evolution of the parameters of the residual velocity ellipsoid of hot
subdwarfs (HSDs) with their position relative to the Galactic plane is traced,
using the HSDs selected by Geier et al. from the Gaia DR2 catalog. Parameters
of the Galactic rotation are determined for two $|z|$ zones. These are used to
estimate the gradient of the circular rotation velocity, $V_0,$ versus $|z|,$
found to be $\Delta V_0/\Delta |z|=-71\pm7$ km s$^{-1}$ kpc$^{-1}$. The size of
the residual velocity ellipsoid is
$(\sigma_1,\sigma_2,\sigma_3)=(36.1,27.6,22.8)\pm(0.4,0.8,0.6)$ km/s for HSDs
at $|z|<0.5$ kpc and
$(\sigma_1,\sigma_2,\sigma_3)=(56.9,55.8,39.7)\pm(0.9,1.1,0.8)$ km/s for HSDs
at $|z|\geq0.5$ kpc. When forming the HSD residual velocities, the Galactic
rotation was taken into account using individual approaches for each $z$ zone.
Parameters of the residual velocity ellipsoids for HSDs located in four
plane-parallel layers are also determined. The size of the ellipsoid increases
with $z,$ and the inclination of the first axis relative to the Galactic plane
also increases. This inclination is close to zero in zones close to the
Galactic plane, $z\sim\pm0.2$ kpc, and rises to $\mp12\pm4^\circ$ for
$z\sim\pm0.9$ kpc.
