SHMR (f_⋆ − M_h, left), stellar mass-velocity scaling law (M_⋆ − V_gal, middle), and the relation between galaxy velocity and halo velocity (V_gal − V_h, right) for the population of late types (blue) and massive early types (red). Top-middle and top-right panels: the characteristic velocity of galaxies V_gal is the velocity along the flat parts of HI rotation curves for late types (V_flat, Lelli et al. 2016b) and the velocity dispersion of stars within 1 kpc for early types (σ_{⋆, 1 kpc}, Brodie et al. 2014). Bottom-middle and bottom-right panels: we substitute the observed V_gal with the circular velocity evaluated at the same radius (2R_e) for both galaxy types. In all panels, we show power-law fits to the data of late types (blue dashed lines) and early types (red dotted lines).