Post-CE orbital period (top) and binary separation (bottom) as a function of secondary mass for the sample of 62 PCEBs. Symbols are the same as in Fig. 2. The solid and dashed lines correspond to the best linear fit for the 62 systems and for the 60 systems with 0.08   M_⊙ ≤ M₂ ≤ 1.0   M_⊙ (excluding the PCEBs with the highest and lowest secondary masses), respectively, while the gray line corresponds to the CV birthline based on the mass-radius relation given in Rebassa-Mansergas et al. (2007).