Mass-loss rates of the initial planet population calculated from the analytical approximation of Caldiroli et al. (2022, Appendix A). The mass-loss rate is parametrized as a function of R_p, M_p, a, M_*, and F_XUV, based on the output of the first-principle 1D photoevaporation code ATES (Caldiroli et al. 2021). The shaded lower region indicates planets with radii <2.5R_E, which are potentially rocky. We do produce spectra for these planets that we include in sunset, but do not include them when analyzing our final planet population in Sect. 3.