  We have studied the kinematic properties of the candidates for hot subdwarfs
(HSDs) selected by Geier et al. from the Gaia DR2 catalogue. We have used a
total of 12 515 stars with relative trigonometric parallax errors less than
30\%. The HSDs are shown to have different kinematics, depending on their
positions on the celestial sphere. For example, the sample of low-latitude
$(|b|<20^\circ)$ HSDs rotates around the Galactic center with a linear velocity
$V_0=221\pm5$ km s$^{-1}$. This suggests that they belong to the Galactic thin
disk. At the same time, they lag behind the local standard of rest by $\Delta
V_\odot\sim16$ km s$^{-1}$ due to the asymmetric drift. The high-latitude
($|b|\geq20^\circ$) HSDs rotate with a considerably lower velocity,
$V_0=168\pm6$ km s$^{-1}$. Their lagging behind the local standard of rest is
already $\Delta V_\odot\sim40$ km s$^{-1}$. Based on the entire sample of 12
515 HSDs, we have found a positive rotation around the $x$ axis significantly
differing from zero with an angular velocity $\omega_1=1.36\pm0.24$ km s$^{-1}$
kpc$^{-1}$. We have studied the samples of HSDs that are complete within
$r<1.5$ kpc. Based on them, we have traced the evolution of the parameters of
the residual velocity ellipsoid as a function of both latitude $|b|$ and
coordinate $|z|.$ The following vertical disk scale heights have been found:
$h=180\pm6$ and $290\pm10$ pc from the low- and high-latitude HSDs,
respectively. A new estimate of the local stellar density
$\Sigma_{out}=53\pm4~M_{\odot}$/kpc$^2$ kpc$^{-2}$ has been obtained for
$z_{out}=0.56$ kpc from the high-latitude HSDs.
