Open cluster dissolution rate and the initial cluster mass function in the solar neighbourhood - Modelling the age and mass distributions of clusters observed by Gaia

Open Access

Fig. 18

Comparison of the distribution of age (top) and mass (bottom) between the simulations (colour-coded KDEs) and the observations (blue histogram with fitted black KDE) considering $t_{4}^{tot} = 2$ $t_4^{{\rm{tot}}} = 2$ Gyr and γ from 0.2 to 0.7 using the ICMF from Trujillo-Gomez et al. (2019).

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