Stellar velocity dispersion: Series of plots for GC5. The upper plots relate to the simulations devoid of dark matter mini-halos (⋆), while the lower plots indicate the results for the globular clusters formed in such mini-halos (⋆•). The two columns on the left display hand-picked snapshots where the radial velocity dispersion profile (i.e, σ_r(r)) resembled better to an isolated case without a dark matter mini-halo (left), and with a massive dark matter mini-halo (right), according to Fig. 2 from Peñarrubia et al. (2017). The column on the right presents the evolution of the maximum value of the radial velocity dispersion profile (i.e, σ_rmax), for each scenario concerning the dark matter mini-halo, colour-coded according to the distance of the cluster to the centre of the host galaxy (i.e. r_orbit), with two vertical dashed lines corresponding to the instants from the two columns on the left. These plots argue that the tidal field from the host galaxy tends to have a much greater impact on inflating the velocity dispersion than the presence of a dark matter mini-halo. In fact, such mini-halos help to protect the cluster from tidal effects, rather than contributing to it.