NGC 6231: X-ray properties of the early-type star population

Abstract

Based on a deep XMM-Newton observation of the young open cluster NGC 6231, we derive the main X-ray properties of its early-type star population. Among the 610 X-ray sources detected in the field, 42 are associated with early-type stars. We investigate their $L_\mathrm{X} / L_\mathrm{bol}$ relationship and we confirm the clear dichotomy between O- and B-type stars. The cut-off line between the two behaviours occurs at $L_\mathrm{bol} \sim 10^{38}$ erg s$^{-1}$ as previously proposed by \citet{BSC97}. The distinction between single and binary stars is not clear cut, except for the colliding wind system HD 152248. The X-ray detected B-stars in NGC 6231 appear to be more luminous than predicted from the \citeauthor{BSC97} relation. Though this suggests a bimodal distribution of the B-star X-ray emission, we caution however that these results might be biased by detection limits. Finally we investigate the X-ray variability of the detected sources and we find that about 40% of the X-ray emitters in the field of view present consistent signs of variability in the EPIC instruments. This fraction is much larger than previously thought. About one third of the early-type stars population, either singles or binaries, further shows variability. These variations do not seem to be exclusively related to binarity and could thus not be systematically interpreted in the framework of a wind-wind collision phenomenon.