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Fig. 9


Radial velocities of the peak of the He II λ 4686 emission line as a function of phase of the eclipsing binary. The orbital phases are computed with the quadratic ephemerides. The red dots yield the raw heliocentric RVs, whereas the black dots were corrected for the epoch-dependence of the systemic velocity. The best-fit S-wave relation (corresponding to vx = 28.8 km s−1, vy = 232.3 km s−1 and vz = 24.8 km s−1) is shown overplotted on the data.

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