As in Fig. 3, but now for different values of the planet-to-star mass ratio q as indicated by labels of individual panels. The viscosity transition is parameterized with α_DZ = 10⁻³ and α_MRI = 5 × 10⁻² (see top panel of Fig. 4 for corresponding migration tracks of individual planets). In panels a-e that exhibit the migration trap, we show the state of the simulation at t_mig = 40000 P_orb. In panel f, the planet is not trapped and thus we show the state at t_mig = 9000 P_orb when the planet is roughly at the same radial distance as in panel e.