Comparison of optical lines of fits obtained with different methods. The top row shows lines of H31, for which the parameters of Bestenlehner et al. (2020) and this work agree well: this level of agreement is representative for most stars in the sample. The bottom row shows lines of R136a7, where there is some discrepancy between the parameters of Bestenlehner et al. (2020) and our results. The difference is especially clear in He ii λ4686, and seems related to differences in T_eff and .