Supermassive Black Holes and Kinematics of Disc Galaxies
  The statistical relations between the masses of supermassive black holes
(SMBHs) in disk galaxies and the kinematic properties of their host galaxies
are analyzed. We use the radial velocity profiles for several galaxies obtained
earlier at the 6-m telescope of the Special Astrophysical Observatory of the
Russian Academy of Sciences parallel with the data for other galaxies taken
from the literature. We demonstrate that the SMBH masses correlate well with
the velocities of rotation of disks at a fixed distance R \approx 1 kpc (V1),
which characterize the mean density of the central region of the galaxy. The
SMBH masses correlate appreciably weaker with the asymptotic velocity at large
distances from the center and with the angular velocity at the optical radius
R_{25}. We suggest that the growth of the SMBH occurs inside of the forming
"classical" bulge during a monolithic collapse of gas in the central kpc-size
region of the protogalaxy. We have also found a correlation between the SMBH
mass and the total (indicative) mass of the galaxy M_{25} within the optical
radius R_{25}, which includes both baryonic and "dark" mass. The masses of the
nuclear star clusters in early-type disk galaxies (based on the catalog of Seth
et al.) are also scaled with the dynamical mass M_{25}, whereas the
correlations with the luminosity and velocity of rotation of galaxies are
practically absent for them. For a given M_{25} the masses of the nuclear
clusters are, on average, nearly order of magnitude higher in S0-Sbc galaxies
than in late-type galaxies.
