Comparison of the disentangled and best-fit model spectra of the secondary star with error ranges, along with a model spectrum having the Brott et al. (2011) CNO baseline abundances. From left to right, the lines C IIIλ 5696, C IVλ 5801, N IIIλλ 4634, 4641, and O III 5592 are shown, with a similar legend as Fig. A.5. The two leftmost panels argue for an elevated carbon abundance with respect to baseline, although as discussed in Sect. 4.2, the issues of C IIIλ 5696 prohibits making quantitative conclusions.