Profile synthesis of the far-UV O VI λλ 1032, 1038 based on the observed Raman bands in Sanduleak’s star. The O VI emitting nebula is reconstructed by summing up the contribution of three emitting regions from (a) BEP, REP, and (b) CEP of the accretion disk, (c) the bipolar outflow, and (d) the optically thick compact component. The bottom two panels show the reconstructed O VI λλ 1032 (left) and 1038 (right) line profiles. The vertical dotted line in each plot represents the average velocity (taken as zero-point of ΔV_{O VI}) of BEP and REP of the accretion disk. The parameters of the five Gaussian components are summarized in Table 1. See also Section 3.