Present-day mass function of Pismis 5, Pismis 5_A, Pismis 5_B, QZ 1, Alessi 43, Collinder 197, BH 56, and NGC 2546. The stellar mass is assigned to each source by nearest-neighbor interpolation in the Gaia colour–magnitude space (BP − RP vs. M_G) using the PARSEC isochrones. The Y-axis is shifted manually by 2 units so that the mass function of each cluster is visible. The dashed lines are the fitted mass functions and the quantity α is the fitted slope. The error bars represent Poissonian uncertainties () (Bisht et al. 2019).