This table details the stellar parameters and abundances we derived. The stellar masses and radii are derived from relations in Mann et al. (2015) and Mann et al. (2019), using K-band magnitudes from 2MASS and parallaxes from Gaia DR3. Surface gravities are derived from calculated masses and radii. The [M/H] values reported here are the final values derived from stellar abundances in this paper; the initial [M/H] values used in the stellar abundance calculations described in Section 3.2 are given in Section 3.1. As we did not calculate effective temperature, however, the values reported in Section 3.1 are repeated here. For reference, solar values of Fe/Mg and Mg/Si are ${0.80}_{-0.10}^{+0.11}$ and ${1.23}_{-0.13}^{+0.15}$ respectively (Asplund et al. 2009). All of the microturbulences and some of the macroturbulences calculated have unreasonably wide uncertainties or physically implausible parameter ranges when fit as described in Section 3.2; we therefore estimated these parameter ranges by eye and report them instead.

¹ The [Mg/H] and [Si/H] abundances for GJ 1132 and LHS 1140 are not considered reliable, due to the low number of spectral lines used and their poor quality. See Section 3.2 for more details; the unreliable abundances are reported in Table C.1 for completeness.

² The Fe/Mg values calculated for GJ 1132 and LHS 1140 are calculated by assuming [Mg/H] is equal to the calculated [Ti/H] value; see Section 3.2 for more details.

³ From Xue et al. (2024).

⁴ From Crossfield et al. (2022).

⁵ From Bonfanti et al. (2024).

⁶ From Schweitzer et al. (2019).

⁷ From Marfil et al. (2021).

⁸ From Demangeon et al. (2021).

⁹ From Cadieux et al. (2024b).

¹⁰ From Van Eylen et al. (2021).