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Fig. 6


HR diagram with O stars shown with squares and WNh stars with a star. Both the evolutionary tracks (in colour) and the isochrones (in black) are overplotted. The ZAMS is plotted with a thicker line. In the top panel, the tracks are taken from the models of Ekström et al. (2012) without rotation. In the bottom panel, both the models with (dashed lines) and without (solid lines) rotation from Chieffi & Limongi (2013) are plotted. The error bar in log (T) and log (L/L) is shown on the bottom left. Our determined cluster age and stars properties are not significantly affected by the choice of rotation speed or model.

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