Radius distribution after 3 Gyr when taking into account photo-evaporative mass loss. We only show the results for the migration model where we vary the inner edge. Further, for planets below the pebble isolation mass or planets where the atmosphere was completely stripped, we recalculate the radii by including a steam atmosphere as described in Appendix H. Several of the planets with sizes >2 R_⊕ lost a significant part of their atmosphere, filling up the radius valley slightly. However, the valley persists even after photoevaporation.