Final elemental abundances of the planetary atmospheres (top) and their corresponding growth tracks (bottom) for three different scenarios: pebble accretion-only (left), planetesimal formation (middle), and pebble and planetesimal accretion (right). The horizontal blue line in the first row indicates the solar abundance, while the vertical violet lines in the second row show the evaporation fronts of the chemical species included in our model for a disc viscosity of α = 5 × 10⁻⁴. The solid lines of the growth tracks correspond to core formation, while the dotted lines correspond to the gas accretion phase. The disc viscosities are colour-coded following the scale at the right.