Final masses of planets as a function of initial radius r₀ and initial time t₀ in the disc with Z = 1.0% (top) and Z = 1.5% (bottom). The lines inside the plots correspond to the same meaning as the lines in Fig. 4. Planets below the purple line are subject to dynamical corotation torques (Paardekooper 2014), while planets below the green line are subject to type-III migration (Masset & Papaloizou 2003), indicating that their final orbital position does not correspond exactly to the position indicated by the black lines.