Kinematics of Hot Subdwarfs from the Gaia DR2 Catalogue
  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.
