Supermassive Black Holes and Nuclear Star Clusters: Connection with the
  Host Galaxy Kinematics and Color
  We consider the relationship between the masses of the central objects in
disky galaxies - supermassive black holes (SMBHs) and nuclear star clusters
(NCs) - and various parameters of parent galaxies: velocity of rotation
$V_{(2)}$ at $R= 2$ kpc, maximal velocity of rotation $V_{\textrm{max}}$, the
indicative dynamical mass $M_{25}$, the total mass of the stellar population
$M_{*}$, and the total color index ($B{-}V$). The mass of nuclear clusters
$M_{\rm nc}$ correlates more closely with the kinematic parameters and total
mass of galaxies than the mass of central black holes $M_{\rm bh}$, including
correlation with the velocity $V_{\textrm{max}}$, which characterizes the
virial mass of the dark halo. On average, lenticular galaxies are distinguished
by higher masses $M_{\rm bh}$ compared to other types of galaxies with similar
characteristics. The dependence of masses of central objects on the color index
is bimodal: galaxies of the red group (red-sequence), which have ($B{-}V) >
0.6{-}0.7$, being mostly early-type galaxies, differ from bluer galaxies, by
higher values of $M_{\rm nc}$ and $M_{\rm bh}$. The red-group galaxies have
systematically higher $M_{\rm bh}$ values, even when the host-galaxy parameters
are similar. In contrast, in the case of nuclear stellar clusters, the "blue"
and "red" galaxies form unified sequences at the diagrams. The results agree
with scenarios in which most red-group galaxies form as a result of the partial
or complete loss of interstellar gas in a stage of high nuclear activity in
galaxies whose central black-hole mass exceeds $10^6 {-} 10^7 M_{\odot}$
(depending on the total mass of a galaxy). Most of galaxies with $M_{\rm bh}>
10^7 M_{\odot}$ are lenticular galaxies (types S0, E/S0), whose disks are
usually devoid of gas.
