Fits to the He I 4388 Å and He II 4541 Å lines. The ionisation balance of He I and He II was used in the determination of T_eff for the stars. The blue data are the disentangled spectra and the red lines the best fits. The upper row is for the primary stars, and the lower row is for the secondary stars. The lower signal-to-noise ratio (S/N) for the secondary components arises because they are fainter than the primary components. The absence of He II 4541 Å absorption in V1034 Sco B and V346 Cen B is obvious and indicates that T_eff < 23 000 K.