We present the distribution of a statistical sample of nearby galaxies in the {kappa}-space ({kappa1}{prop.to}logM, {kappa}2{prop.to}log(Ie)^3^*M/L, {kappa}3{prop.to}M/L). Our study is based on near-IR (H-band: {lamdba}=1.65{mu}m) observations, for the first time comprising early- and late-type systems. Our data confirm that the mean effective dynamical mass-to-light ratio M/L of the E+S0+S0a galaxies increases with increasing effective dynamical mass M, as expected from the existence of the Fundamental Plane relation. Conversely, spiral and Im/BCD galaxies show broad distribution in M/L with no detected trend of M/L with M, the former galaxies having M/L values about twice larger than the latter, on average. For all the late-type galaxies, the M/L increases with decreasing effective surface intensity Ie, consistent with the existence of the Tully-Fisher relation.