Notes. The two components of the Li I doublet were fit simultaneously. Also shown are the solar abundances inferred via the solar twins in the sample; the value for the Li I doublet in brackets was adopted from the literature (Sect. 3.2). The final columns show the typical absolute abundance corrections (log ɛ^Non-LTE − log ɛ^LTE) for each line: median results are shown in (T_eff∕K ± 250, log g∕cm s⁻² ± 0.5) regions corresponding to spectral and luminosity classes K V (5000, 4.5), F V (6500, 4.0), and K III (4250, 2.0). The most negative and positive corrections for a given line are highlighted, and no results are shown for where the lines were too weak to be detected.

References. (1) Yan et al. (1998); (2) Hibbert et al. (1993); (3) Hibbert et al. (1991); (4) Froese Fischer et al. (2006); (5) Chang & Tang (1990); (6) Kelleher & Podobedova (2008); (7) Garz (1973); (8) O’Brian & Lawler (1991); (9) Trubko et al. (2017); (10) Smith (1988); (11) Smith & Raggett (1981); (12) Den Hartog et al. (2011); (13) Davidson et al. (1992).