The massive star binary fraction in young open clusters I. NGC 6231 revisited

TL;DR

This study provides a detailed analysis of the binary fraction, orbital properties, and mass ratios of O-type stars in NGC 6231, offering new insights into their formation and early evolution.

Contribution

It revises the spectral classification and multiplicity of O stars in NGC 6231, establishing a high binary fraction and detailed orbital characteristics based on long-term spectroscopy.

Findings

Approximately 75% of O stars are in binary systems.

Most binaries have short orbital periods of a few days.

Mass ratios favor O+OB binaries over random IMF sampling.

Abstract

We present the results of a long-term high-resolution spectroscopy campaign on the O-type stars in NGC 6231. We revise the spectral classification and multiplicity of these objects and we constrain the 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 henceforth 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 randomly drawn from a standard IMF. Obtained from a complete and homogeneous population of O-type stars, our conclusions provide interesting observational constraints to be confronted with the formation and early-evolution theories of O stars.