Planet evolution maps in the Ida et al. (2016) disk model at α = 5.4 × 10⁻³. As in Fig. 2, planets that are below the dashed blue line have reached pebble isolation mass and accrete gas. Planets that are interior to the dashed white line have reached runaway gas accretion and can grow very massive. The pebble flux is in all plots. As in the Bitsch et al. (2015b) disk, the formulae produce really similar results, however planets grow much lighter with the same pebble fluxes in the Ida et al. (2016) model due to the region of outwards migration from corotation torques being smaller.