  We consider young distant stars from the Gaia TGAS catalog. These are 250
classical Cepheids and 244 OB stars located at distances up to 4 kpc from the
Sun. These stars are used to determine the Galactic rotation parameters using
both trigonometric parallaxes and proper motions of the TGAS stars. In this
case the considered stars have relative parallax errors less than 200%.
Following the well-known statistical approach, we assume that the kinematic
parameters found from the line-of-sight velocities $V_r$ are less dependent on
errors of distances than the found from the velocity components $V_l$. From
values of the first derivative of the Galactic rotation angular velocity
$\Omega{'}_0$, found from the analysis of velocities $V_r$ and $V_l$
separately, the scale factor of distances is determined. We found that from the
sample of Cepheids the scale of distances of the TGAS should be reduced by 3%,
and from the sample of OB stars, on the contrary, the scale should be increased
by 9%.
