The massive stars binary fraction in young open clusters I. NGG 6231 revisited

We present the results of a long-term HiRes spectroscopic campaign on the O-type stars in NGC 6231. We revise the spectral classification and multiplicity of these objects and we constrain fundamental properties of the O-star population. Almost three quarters of the O-type stars in the cluster are members of a binary system. The minimum binary fraction is 0.63, with half the O-type binaries having an orbital period of the order of a few days. The eccentricities of all the short-period binaries are revised downward, and now match a normal period-eccentricity distribution. The mass-ratio distribution shows a large preference for O+OB binaries, ruling out the possibility that, in NGC 6231, the companion of an O-type star is drawn from a Salpeter IMF. Obtained on a complete and homogeneous population of O-type stars, these constraints further provide strong observational guidelines for the formation and early-evolution of O stars.