together with other data and the references to the data sources are listed in Table 1. It contains:\
([*1*]{}) Name.\
([*2*]{}) Morphological type.\
([*3*]{}) Radial disk scalelength $h$ used in the paper.\
([*4*]{}) Ratio of radial velocity dispersion to circular velocity at $R=2h$.\
([*5*]{}) Disk surface density corresponding to the marginal stability condition at $R=2h$.\
([*6*]{}) Mass-to-light ratio of a disk, marginally stable at $R=2h$ ($B$-band).\
([*7*]{}) Ratio of mass of the disk, marginally stable at $R=2h$, to the total mass $M_t$ within $R=4h$, where $M_t = 4 V_c^2 h / G$ and $V_c$ is circular velocity. Cases of $M_{d}/M_t >1$ indicate a significant dynamical overheating of a disk.\
([*8*]{}) Velocity dispersion and rotation velocity data sources.\
Diagrams “$(M/L_B)_{d}$—$(B-V)_0$” for stellar disks are shown in Fig. 1, where disks masses $M_d$ are obtained from the gravitational stability condition at $R=2h$.[^1] For the Galaxy the mean color index for $Sbc$ type was used (Buta et al., 1994). A straight line reproduces model relation obtained by Bell, de Jong (2001) for old stellar systems with different present-day star formation rate (SFR) using modified (bottom-light) Salpeter initial mass function (IMF). It is worth noting that the light extinction inside the galaxies that may 