Distributions of the effective radius R_e of the bulge (or Sérsic) component (left), and h_e of the disk (or exponential) component (right) of all types of EFIGI galaxies with Inclination ≤ 2, as a function of the bulge-to-total ratio B/T_g in the g band, identified in Quilley & de Lapparent (2022) as a tracer of Hubble type. Both panels are color-coded with the Hubble type of the galaxy, with subplots corresponding late (spiral and Im) types on the left, and to early (E and S0) types on the right. The corresponding ODR fits are plotted in each panel. The indicative positions in B/T_g, R_e and h_e for the Sd, Sdm, and Sm types are added in both panels (see text for details). For the Im types (added in the right panel), the effective radii from the single-Sérsic modeling are added at an arbitrary small B/T_g value (see text). These graphs show that for spiral types, R_e increase strongly with B/T_g, whereas there is only a weak increase in h_e with B/T_g. S0 and E galaxies have the highest B/T_g values, but only some of them actually have the highest R_e or h_e, with a tail of S0 toward lower values encompassing ∼1 dex for both their R_e and h_e. The smallest S0 R_e correspond to the smallest R_e of early spirals (left panel), and the smallest S0 h_e correspond to the intermediate h_e between those of the smallest disks (Sm types) and of the Im galaxies (right panel).