Notes. Stellar bolometric luminosities, L*, and planet instellation, S_p, computed by us as in Cifuentes et al. (2020) and Martínez-Rodríguez et al. (2019), respectively (L_⊙ = 3.828 × 10²⁶ W, S_⊕ = 1361 Wm⁻²). The remaining star and planet parameters were taken from Gaia Collaboration (2021a, Gaia EDR3 d), Skrutskie et al. (2006, 2MASS J), Alonso-Floriano et al. (2015, and references therein, spectral type), and the references are listed in the last column. ^(a)LTT 1445 A has a second transiting planet with a precise mass determination of and a minimum radius of 1.15 R_⊕. Winters et al. (2022) could not determine the radius directly as the signal-to-noise ratio of their light curve permits both grazing and non-grazing configurations. ^(b)See this work for new planet parameters of Gl 486 b. ^(c)Gl 357 has at least two more non-transiting planets detected via RV with approximate minimum masses of 3.40 M_⊕ and 6.1 M_⊕ (Luque et al. 2019). ^(d)AU Mic, a member of the young β Pictoris moving group, has a second transiting planet with precise radius determination of and a 5σ upper limit on the mass of 20.3 M_⊕. Cale et al. (2021) could not determine the mass directly as the stellar activity amplitude is one order of magnitude greater than the planet semi-amplitude.

References. But04: Butler et al. (2004); Cal21: Cale et al. (2021); Gil17: Gillon et al. (2017a); Lam21: Lam et al. (2021); Lan14: Lanotte et al. (2014); Luq19: Luque et al. (2019); Luq22: Luque et al. (2022); Mot15: Motalebi et al. (2015); Pla20: Plavchan et al. (2020); Tri18: Trifonov et al. (2018); Tri21: Trifonov et al. (2021); Win19: Winters et al. (2019); Win22: Winters et al. (2022).