Fig. D.1.

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Evolution of scale radii: Evolution of the GC+DM system tidal radius (rt, blue) and of the half-mass radius of the bound dark matter particles (r1/2, •, black), for each simulated cluster. We observe that clusters who lost most of their dark matter mini-halo (i.e. GC1 and GC2) presented rt > r1/2, • at some point of their orbital evolution, similarly to the relation for sub-halo disruption from Hayashi et al. (2003).
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