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We consider the relationship between the masses of the central objects indisky 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 $V_{\textrm{max}}$, theindicative 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 totalmass of galaxies than the mass of central black holes $M_{\rm bh}$, includingcorrelation with the velocity $V_{\textrm{max}}$, which characterizes thevirial mass of the dark halo. On average, lenticular galaxies are distinguishedby higher masses $M_{\rm bh}$ compared to other types of galaxies with similarcharacteristics. The dependence of masses of central objects on the color indexis 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, byhigher values of $M_{\rm nc}$ and $M_{\rm bh}$. The red-group galaxies havesystematically higher $M_{\rm bh}$ values, even when the host-galaxy parametersare similar. In contrast, in the case of nuclear stellar clusters, the "blue"and "red" galaxies form unified sequences at the diagrams. The results agreewith scenarios in which most red-group galaxies form as a result of the partialor complete loss of interstellar gas in a stage of high nuclear activity ingalaxies 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 areusually devoid of gas.

Supermassive Black Holes and Nuclear Star Clusters: Connection with the Host Galaxy Kinematics and Color