Top: Cumulative distribution of the planetary masses in our simulations (red) and their detections (black) as well as from the simulations of Izidoro et al. (2021) (purple) after 100 Myr of integration time. We also overplot the masses from the Kepler observations using the mass-radius relationship of Wolfgang et al. (2016). Bottom: Time evolution of the pebble isolation mass in our model, following the recipe of Bitsch et al. (2018b). Here t = 0 corresponds to the starting time of the simulations, so to a disc that is already 2 Myr old in the framework of Bitsch et al. (2015a).