$R=2h$ (Fig. 4), being shifted to higher values of $M_{d}/M_t$ and densities. These differences are statistically significant: according to the Wilcoxon criterion, the level of significance $\alpha=0.99$. From the distribution of $M_{d}/M_t$ (Fig. 3) it follows that for most of galaxies disk to total mass (inside $R=4h$) ratios lay in the interval 0.4—0.8, independently of color and morphological type (if to exclude galaxies with apparently overheated disks, for which these ratios remain uncertain).

\[h!\] ![Diagram “$\sigma(2h)$ — morphological type”. Pair members are marked by asterisks. Straight horizontal line separates galaxies with $\sigma(2h)=500 M_{sun}/$pc$^2$ level, which definitely evidences the overestimation of their mass.](pic3.jpg "fig:"){width="14cm"}

If to consider the disky galaxies as systems with marginally stable disks, one can plot the relation $M_d$—$V_c$ (baryonic Tully-Fisher relation), connecting the most important parameter of stellar disk (a mass) with the parameter determined mostly by massive halo (rotation velocity). This diagram is shown in Fig. 5 (galaxies with $M_{d}/M_t>1$ are excluded). The relation obtained by McGaugh (2005) for a large sample of galaxies, disk masses of which were estimated from their luminosities and colors, is also shown by straight line for comparison. From this figure it follows that disk masses estimated from the marginal stability 