Fig. B.2.
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CMDs for the PM member stars. Left and middle panels: Optical Gaia EDR3 CMDs. A family of PARSEC isochrones was fit in order to derive the uncertainties on the age and on the metallicity estimates. Right panel: NIR (VVVX and/or 2MASS) CMDs. In all panels the red lines depict the PARSEC isochrones with age and metallicity listed in Table 2 for each cluster. In the CMDs the cyan areas represent overdensities, whereas the black areas are underdensities.
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