Notes. R_* and T_* are the stellar radius and effective temperature, respectively, a is the planet-star distance, and M_p, R_p, and T_p are the planetary mass, radius, and equilibrium temperature, respectively. The equilibrium temperature is computed as $T_p=\sqrt{R_{\star }/(2a)}{T}_{\star }$, where the albedo and emissivity are implicitly assumed to be 0 and 1, respectively. ^a Collier Cameron et al. (2010), Smith et al. (2011), Lehmann et al. (2015), Hardy et al. (2015). ^b Boyajian et al. (2015), Southworth (2010). ^c Boyajian et al. (2015), Paredes et al. (2021). ^d Faedi et al. (2011). ^e Torres (2007), Southworth (2010), Melo et al. (2024). ^f Harpsθe et al. (2013), Cloutier et al. (2021).