Location and formation time of the furthest cores simulated in different scenarios from Table 2 when protoplanets emerge at t_0,p = 0.2 Myr (left). Scenarios with the same St are highlighted by their colored groups. Final location of the furthest cores after gas accretion (Sect. 4.1) and type II migration (Sect. 2.5) at the end of the disk lifetime of 5 Myr (right). An example growth track is shown at the bottom-right to facilitate the readability of the axes. In all scenarios, protoplanets migrate several AU during gas accretion. This phenomenon is visually depicted as a significant horizontal displacement from the diagonal line r_core = r_f. The displacement is more pronounced in disks with high St (purple and blue groups) due to an earlier formation of the cores.