Numerically integrated growth tracks for core accretion to the pebble isolation mass followed by gas accretion. We start the protoplanets at a mass of M₀ = 0.01 M_E at t₀ = 0.9  Myr (except for the α = St = 0.01 growth trackstarting from 25 AU, which we start at t₀ = 0.3 Myr) in a protoplanetary disc that evolves over a total time of 3 Myr. The dots indicate the time for the growth track that successfully forms a Jupiter analogue (small dots are separated by 0.2 Myr, large dots indicate a time of 3, 2 and 1 Myr). Weuse a migration model where the migration rate is reduced by multiplication with the relative gap height, following Kanagawa et al. (2018). The migration rate is therefore inversely proportional to the planet mass beyond the pebble isolation mass. This results in gas accretion over a few astronomical units of migration.