Correlations between various bulk parameters of the final planet population. The gravitational potential ϕ is calculated directly from the planet mass and radius as reported in the NASA Exoplanet Archive. The XUV flux F_XUV comes from the stellar SED template. The mass-loss rate $\dot{M}$ is given by the Caldiroli et al. (2022) analytical approximation. The isothermal Parker wind temperature T₀ is a free model parameter whose value is determined through an iterative process. It satisfies the self-consistency criterion that it is equal to the maximum of the corresponding nonisothermal temperature profile (see Sec. 2.3). The escape parameter λ is calculated from ϕ and the sound speed, which depends on T₀ and the averaged mean particle mass $\overline{\mu }$ (see Lampón et al. 2020).