Migration map of the three disk profiles used (Eq. (1)) at t=0 including the repulsive inner edge. Positive values of ${\tau }_a^{-1}$ indicate outward migration. The solid gray line marks the zero-torque locus and dashed lines show the locations where τ_a= ± 1 Myr. For the flat and steep disks, there is a migration trap near the pressure bump at 1 au that suppresses migration until planets reach ∼ 2 M_⊕, at which point they saturate the corotation torque and migrate inwards.