  We have analyzed the kinematics of OB stars from the list by Xiang et al.
(2021) that contains $\sim$13 000 single OB stars. For these stars there are
photometric distance estimates and proper motions from the Gaia catalogue and
line-of-sight velocities from the LAMOST catalogue. Based on a sample of single
OB stars and using the photometric distances and proper motions of stars from
the Gaia EDR3 catalogue, we have found the group velocity components
$(U_\odot,V_\odot,W_\odot)=(9.63,9.93,7.45)\pm(0.27,0.34,0.10)$ km s$^{-1}$,
and the following parameters of the angular velocity of Galactic rotation:
$\Omega_0=29.20\pm0.18$ km s$^{-1}$ kpc$^{-1}$, $\Omega^{'}_0=-4.150\pm0.046$
km s$^{-1}$ kpc$^{-2}$ and $\Omega^{''}_0=0.795\pm0.018$ km s$^{-1}$
kpc$^{-3}$, where the error per unit weight $\sigma_0$ is 9.56 km s$^{-1}$ and
$V_0=236.5\pm3.3$ km s$^{-1}$ (for the adopted $R_0=8.1\pm0.1$ kpc). Based on
the same OB stars, we have found the residual velocity dispersions
$(\sigma_1,\sigma_2,\sigma_3)=(15.13,9.69,7.98)\pm(0.07,0.05,0.04)$ km
s$^{-1}$. We show that using the line-of-sight velocities increases
significantly the space velocity dispersion and leads to a biased estimate of
the velocity $U_\odot$. A comparison of the distances scales used has shown
that the photometric distances from Xiang et al. (2021) should be lengthened
approximately by 10%.
