Fig. 2
The O stars in the four groups richest in O stars. The solid lines correspond to stellar tracks, and the dashed lines are isochrones with a separation of 2 Myr. The stellar models are from Meynet et al. (1997) (upper left), Limongi & Chieffi (2006) (upper right), Schaller et al. (1992) (lower left), and Meynet & Maeder (2005) (lower right). As our analysis only allows a limited set of discrete values, many of the points contain multiple stars.
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