$R=2h$ from the equation (2). Radial velocity dispersion of stars $c_r$, if it was not given in the cited literature, was determined from $c_{obs}(R)$ measured along the major axis of a galaxy: $$\label{Eq-c-obs}
c_{obs}^2 = c_{\phi}^2 \sin^2 i + {c_z}^2 \cos^2 i \,,$$ which leads to: $$\label{Eq-cr-cobs}
c_r=c_{obs}\cdot \left[(c_{\phi} / c_r)^2 \sin^2 i + (c_z/c_r)^2 \cos^2 i\right]^{-1/2}
\,.$$ where $c_{\phi}$ and $c_z$ are azimuthal and vertical components of velocity dispersions correspondingly, and $i$ is the inclination of a disk. Radial and azimuthal velocity dispersions are interconnected by Lindblad formula $c_{\phi}/c_r=\kappa/ 2\Omega$ following from the epicyclic approximation. Direct measurements of $c_z/c_r$ ratio in galaxies show that in majority of cases it lies in the interval 0.4—0.7 (Shapiro et al. (2003)). In current work it was taken to be 1/2.

In most cases rotation curve $V(R)$ has a plateau at the distance of two disk radial scalelenghts, so the $\kappa/\Omega $ ratio can be taken as $\sqrt 2$. For the increasing or decreasing rotation curves we applied the corresponding corrections. If only the stellar rotation curve $V_*(R)$ was available for a galaxy, the approximate asymmetric drift correction was introduced following Neistein et al. (1999). Note, that for $c_r/V_c>0.5$ this correction is inevitably 