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Star clusters near intermediate and high mass young stars

A number of 43 high mass O-type stars within 2 kpc of the Sun are not known to be current, nor former member of clusters/OB-associations. We try to elucidate their formation history by looking deeper into their local stellar environment, by evaluating their spatial velocities, and their location in the Galaxy with respect to young stellar clusters. We find that 5 stars are in fact member of a small cluster and that nearly half (22 objects) could have undergone a dynamical ejection from a young cluster. Based on the current available data, 6% of the Galactic O-type stars cannot be associated with a stellar cluster. Finally by assuming that all stars are formed in clusters, that follow a powerlaw in size distribution we calculate the expected statistics regarding isolated O stars and O stars in OB-associations.