AllV I line regions fitted to the observed CARMENES spectrum (thick gray) of a typical M0.0 V star (J14257+236W). The model corresponding to the best-fit V abundance, using the Schw19 stellar parameters, is shown in green dot-dashed lines. Individual V I HFS components and their relative strengths, as given by log (gfλ) − θχ, are shown in vertical gray lines above each feature. Notable contaminating lines (i.e., expected depth > 0.05) inside the V I features from other species are marked in blue (for TiO) and red.