Same as Fig. 4 but with pebble fragmentation velocities set to 1 m/s for dry pebble inside the water iceline and 10 m/s for icy pebbles outside the water iceline. The reduction of super-Earths for higher stellar masses is slightly stronger in the viscous case, as the dry region of the disc – where pebbles are small and planet formation is inefficient - extends farther away from the star for higher stellar masses. In the irradiated case, the results are relatively unchanged.