Planetary & stellar parameters from SED fitting

This full sample, as well as a sample filtered for host stellar masses between 0.8 and 1.2M_{sun}_, were then used to derive the slope and position of the radius valley as a function of orbital period, insolation flux, and stellar mass to compare them to predictive models and previous observational results. Our results are consistent with thermally driven mass loss with a planet radius versus orbital period slope of R_p_=P**(-0.142_-0.006_^+0.006^) x e**(0.896_-0.010_^+0.012^) for the full sample, leaning toward core-powered mass loss.

The planet radius versus insolation flux slope of R_p_=S_p_**(0.136_-0.014_^+0.014^)xe**(-0.085_-0.030_^+0.031^) for the filtered sample leaned toward photoevaporation. Also, the slope as a function of stellar mass for both samples appears more consistent with thermally driven processes when compared to models and previous studies.