Abstract We present results from a five year campaign to gather multiepoch, high-resolution spectra of a volume-complete sample of 413 M dwarfs with masses 10%–30% that of the Sun within 15 pc. We report weighted mean systemic radial velocities (RV) and rotational broadening measurements ( v sin i ) for our targets. Our typical relative RV uncertainties are less than 50 m s −1 for the isolated, slowly rotating targets in our sample and increase, though remain less than 1 km s −1 , for more rapidly rotating stars. The majority of the single stars in our sample (71 ± 3%) have rotational broadening below our detection limit of 3.4 km s −1 . When combined with astrometric data, our RVs allow us to calculate Galactic space motions, which we use to assign thin or thick disk membership. We determine that 81% and 8% of our sample are highly probable thin and highly probable thick disk members, respectively. We report seven new multilined multiple systems and identify six additional targets with velocity variations indicative of long-period binaries, of which three are new detections. Finally, we find no significant difference in the stellar multiplicity rates of the thin disk (22 ± 2%) and thick disk (21 ± 8%) populations in our sample, implying that mid-M dwarfs do not significantly lose companions at these relative ages. Our survey more than triples the number of these fully convective stars with complete astrometric data and uniformly derived, multiepoch, high-resolution RVs and rotational broadening measurements.
Winters et al. (Tue,) studied this question.
Synapse has enriched 5 closely related papers on similar clinical questions. Consider them for comparative context: