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Fig. 4


TCDs and CMDs for stars located in the areas of NGC 3572, Trumpler 18, and NGC 3590. In all panels filled (green or blue) circles depict adopted likely members for each cluster; open black squares are stars with available spectral classification and small light gray dots are not classified or field stars. In the upper panels (a)c)) we present the TCDs. Solid lines in them are ZAMSs (Sung et al. 2013), both in their normal location and shifted along the reddening path (red arrow) in agreement with the adopted color excesses (see Table 6). In the middle panels (d)f)) the gray lines represent solar metallicity isochrones, which include mass loss and overshooting (Marigo et al. 2008), for three different ages and are plotted in years. In the lower panels (g)i)), the solid lines are ZAMSs for each cluster, corrected for distance and reddening.

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