References. Cas08: Casagrande et al. (2008); Mor08: Morales et al. (2008); Jen09: Jenkins et al. (2009); Lepl3: Lépine et al. (2013); Rajl3: Rajpurohit et al. (2013); Stel3: Stelzer et al. (2013); Gail4: Gaidos et al. (2014); Foul8: Fouqué et al. (2018); Pasl8: Passegger et al. (2018); Raj18: Rajpurohit et al. (2018); Houl9: Houdebine et al. (2019); Hojl9: Hojjatpanah et al. (2019); Kuzl9: Kuznetsov et al. (2019); Schl9: Schweitzer et al. (2019); Pas 19: Passegger et al. (2019); AK20: Antoniadis-Karnavas et al. (2020); Cif20: Cifuentes et al. (2020); Mar21: Marfil et al. (2021).

Notes. ^(a) The T_eff determined by us from the stellar bolometric luminosity, interferometric radius, and Stefan-Boltzman law is 3291 ± 75 K. ^(b) Cifuentes et al. (2020) demonstrated that Casagrande et al. (2008) T_eff of M dwarfs, in contrast to FGK stars, are unreliable. ^(c) Jenkins et al. (2009) T_eff were determined using the V − K_s relations taken from Casagrande et al. (2008), while Cifuentes et al. (2020) again demonstrated that in the Gaia era the Johnson photometry should not be used for deriving parameters of M dwarfs.