Profiles of the gas disc after the relaxation phase, which serve as the initial conditions for our simulations. From top to bottom panels: opacity κ, the aspect ratio h = H∕r, the temperature T, and the surface density Σ. The grey boxes indicate the extent of the damping zones at the inner and outer BC. The vertical dotted lines show the snowline, and the transition between the viscous heating and the stellar irradiation regions, in the case of the nominal simulation. Some of the simulations actually use the same disc as the nominal one. For totmass_20ME simulation we had to use an outer disc, spanning from 8 to 40 au. Similarly, we used a slightly larger disc (up to 16 au) for the simulation embryos_0.1ME_120.