Notes. Best likelihood parameters from our mass profile fits for each simulated globular cluster at z = 0. The first three columns yield the fits when using a Zhao (1996)αβγ model with fixed α = 2 and β = 5 (as in the classic Plummer model) for better convergence, while the last three columns yield the fits when adopting a Kazantzidis et al. (2004) model. Each three columns display the scale radius a, inner slope γ and mass fraction f relative to the first dark matter shell explained in Section 4.2.2, defined as M_•, 1. For details, see Eqs. 5 and 6.