Fig. C.1.

Top row: line profiles ((a) Si IV λ 4089, (b) O III λ 5592, (c) C IV λ 5812, (d) He I λ 4120, (e) He I λ 4713, (f) He I λ 4922, and (g) He I λ 5016) of the separated spectra obtained after application of the brightness ratio for the primary (left panel) and secondary (right panel) stars. Bottom row: Fourier transform of these lines (in black) and best-match rotational profile (in red) for the primary (left panel) and secondary (right panel) stars.
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