Two nights of phase-resolved medium-resolution Very Large Telescope spectroscopy of the extra-galactic low-mass X-ray binary LMC X-2 have revealed a 0.32 ± 0.02 d spectroscopic period in the radial velocity curve of the He ii λ4686 emission line that we interpret as the orbital period. However, similar to previous findings, this radial velocity curve shows a longer term variation that is most likely due to the presence of a precessing accretion disc in LMC X-2. This is strengthened by He ii λ4686 Doppler maps that show a bright spot that is moving from night to night. Furthermore, we detect narrow emission lines in the Bowen region of LMC X-2, with a velocity of Kem = 351 ± 28 km s-1, that we tentatively interpret as coming from the irradiated side of the donor star. Since K em must be smaller than K2, this leads to the first upper limit on the mass function of LMC X-2 of f(M1) ≥ 0.86 M ⊙ (95 per cent confidence), and the first constraints on its system parameters. © 2007 RAS.
Publication Source (Journal or Book title)
Monthly Notices of the Royal Astronomical Society
Cornelisse, R., Steeghs, D., Casares, J., Charles, P., Shih, I., Hynes, R., & O'Brien, K. (2007). A signature of the donor star in the extra-galactic X-ray binary LMC X-2. Monthly Notices of the Royal Astronomical Society, 381 (1), 194-200. https://doi.org/10.1111/j.1365-2966.2007.12233.x