Notes. Projected rotational velocities (υ sin i) for our analyses were taken from Morin et al. (2008) for AD Leo and Reiners et al. (2018) for PM J18482+0741. For CN Leo, EV Lac, and DS Leo, v sin i estimates were taken from Cristofari et al. (2023a), who revised some values based on rotation periods and radii. Inclinations were derived from υ sin i, P_rot and radii. ^a Inclinations computed assuming a 1.0 km s⁻¹ uncertainty on υ sin i. ^b In the present analysis, we fixed υ sin i and fit ζ_RT. Consequently, broadening arising from non-physical or unidentified sources may lead to larger ζ_RT estimates. ^c For Barnard’s star, we additionally fit for the [α/Fe] parameter (see Cristofari et al. 2022a), yielding [α/Fe] = 0.09 ± 0.10 dex. ^d Maximum υ sin i assuming an inclination of 90°.