Same as Fig. 4 but with α_v = 10⁻³ and Ṁ_g,0 = 10⁻⁸ M_⊙/yr. We find similar results in both the irradiated case (left) and the viscously heated case (right) compared to our nominal model. In the irradiated case, the fraction of super-Earths saturates at a lower stellar mass due to efficient inward migration. In the viscously heated case, we find that the fraction of close-in super-Earth still decreases with increasing stellar mass for large discs but the reduction is slightly lower compared to our nominal model.