A comparison of the disentangled and fitted line profiles of the Hγ (top) and Hδ (bottom) Balmer lines of the primary. Renormalised disentangled spectra are shown by black dots, while the best-fitting synthetic line profiles derived via optimisation in the OSTAR grid of non-LTE spectra calculated by Lanz & Hubeny (2003) are shown as solid lines. Blends conspicuous on hydrogen line profiles due to the various metals are not fitted. Theoretical spectra calculated for the solar abundance were used.