method requires then to determine the destroyed satellites before applying our Z12-inspired correction to VL2: to evaluate the luminous satellite population, we require the two following corrections: a) to account for the destruction by tidal stripping, and b) to account for suppression in star formation.

The first correction we apply to VL2 N-body satellites is the destruction rates by tidal stripping. For that, we need a relation between the mass retained since the infall and the change in the velocity (e.g., $v_{{\rm max}}$) in the same time interval.

We compute that relation applying our semi-analytical model, using the same satellites with which we calculated the relation $\Delta v_{{\rm c,1kpc}}$-$v_{{\rm infall}}$ (see DP09, appendix A, for the first phase). This population of satellites is split into three groups defined below.

We plot the result in Fig. \[fig:Dv-M\]. The filled circles represent the cored DMB satellites, having baryonic fraction $M_{b}/M_{500}>0.01$, while the open circles show the cuspy DMB satellites, with baryonic fraction $M_{b}/M_{500}<0.01$ (see Governato et al. (2012)). The open diamonds represent the DMO satellites.

The plot shows that DMB satellites loose more mass than DMOs. This can be explained by the following reasons: 1) DMB satellites contain gas, contrary to DMOs; 