Upper panels: pressure as a function of the baryon number density (up to the highest central density n_cen found in the most massive neutron stars) for the softest (BSk19, panel a) and the stiffest (BSk21, panel b) of our nucleonic EoSs (dashed lines) and for the corresponding EoSs with a quark phase transition (solid lines). Lower panels: energy per baryon (defined by e = ℰ/n − m_nc² where m_n is the neutron mass) as a function of the baryon density for the softest (BSk19, panel c) and the stiffest (BSk21, panel d) of our nucleonic EoSs (dashed lines) and for the corresponding EoSs with a quark phase transition (solid lines). The shaded areas indicate the region of phase coexistence at densities n_N ≤ n ≤ n_X.