![(a) Diagram “$c_r/V_c$ — morphological type”. (b) Diagram “$V_c$—$c_r$”. Galaxies with types later than Sa are marked by open circles; a straight line corresponds to the mean value of $c_r/V_c$.](crvctype.jpg "fig:"){width="12cm"} ![(a) Diagram “$c_r/V_c$ — morphological type”. (b) Diagram “$V_c$—$c_r$”. Galaxies with types later than Sa are marked by open circles; a straight line corresponds to the mean value of $c_r/V_c$.](vccr1.jpg "fig:"){width="12cm"}

\[h!\] ![Diagram “$M_{d}/M_t$ — $(B-V)_0$”. A horizontal line marks $M_{d}/M_t=1$. Points above this line correspond to the galaxies with certainly overheated disks. Open circles represent the galaxies with types later than Sa. Typical errors of $M_{d}/M_t$ caused by the uncertainty of stellar velocity dispersion estimates are about 40%.](pic4.jpg "fig:"){width="12cm"}

As far as $M_d$ we found is in general case the upper limit of mass of a disk, the values $ M_d/M_t \ge 1 $ obtained for some galaxies (see Fig. 3) have no physical sense and indicate unambiguously the significant overestimation of disk masses, or, in other words, the disk overheating. Almost all of these objects are lenticular galaxies with a high color indexes $(B-V)_0>0.7$.

Lenticular galaxies differ from other galaxies of the sample by their distributions of both $M_{d}/M_t$ ratios (Fig. 3) and “marginal” surface densities at 