Same as Fig. 1, but using α = 0.0054 (top) and α = 10⁻⁴ (bottom)for the pebble isolation mass, but keeping the disc structure the same for the pebble isolation mass estimates. The change of the α parameter changes the pebble isolation mass, but the trend is similar for different α values: a large fraction of super-Earth planets are more massive than the pebble isolation mass when the disc reaches an age of 1 Myr.