The very massive X-ray bright binary system Wack 2134 (= WR 21a)

From the radial velocities of the N IV lambda 4058 and He II lambda 4686 emission lines, and the N V lambda 4604-20 absorption lines, determined in digital spectra, we report the discovery that the X- ray bright emission line star Wack2134 (= WR21a) is a spectroscopic binary system with an orbital period of 31.673 +/- 0.002 d. With this period, the N IV and He II emission and N V absorption lines, which originate in the atmosphere of the primary component, define a rather eccentric binary orbit (e = 0.64 +/- 0.03). The radial velocity variations of the N V absorptions have a lower amplitude than those of the He II emission. Such a behaviour of the emission line radial velocities could be due to distortions produced by a superimposed absorption component from the companion. High-resolution echelle spectra observed during the quadrature phases of the binary show H and He II absorptions of both components with a radial velocity difference of about 541 km s(-1). From this difference, we infer quite high values of the minimum masses, of about 87 and 53M(circle dot) for the primary and secondary components, respectively, if the radial velocity variations of the He II emission represent the true orbit of the primary. No He I absorption lines are observed in our spectra. Thus, the secondary component in the Wack2134 binary system appears to be an early O-type star. From the presence of H, He II and N V absorptions, and N IV and C IV emissions, in the spectrum of the primary component, it most clearly resembles those of Of/WNLha-type stars.