  Within the disk model framework used to approximately describe flattened
galaxies, we develop an iterative method of determining column mass density
from rotation curve supplemented with isotropic velocity dispersion profile.
This generalizes our previous iterative method to the case when the velocity
dispersion becomes important. We show on the example of UGC 6446 galaxy, that
taking the velocity dispersion into account results in some observational
signatures in the behavior of the local mass-to-light ratio. Along with
galactic magnetic fields, this is another factor allowing to substantially
reduce the local mass-to-light ratio at galactic outskirts. Taking the velocity
dispersion into account may also have some consequences for the division of
mass distribution between various mass components in modeling rotation curves.
