tidal heating (recall the latter to be absent in Z12) that mimics the effect of flattening of the cusp. To this we add other corrections (e.g., tidal destruction and UV heating effects on subhaloes) discussed in DP09 and apply them to the satellites of the VL2 simulation, following the same principles as B13.

We stress again that in our model: a) contrary to Z12 and B13, the density profile flattening is due to DF and not to SF; b) tidal heating and disc shocking are taken into account differently from Z12 and B13; c) our model does not suffer from the numerical effect producing “artificially rich satellites in the Z12 simulations.

Since the second phase contains the new method we propose to solve the problems involving the number and mass of satellites, we give its description in what follows.

Mass loss caused by tidal stripping and tidal heating
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The second phase considers the effects of the interaction between the main halo and the satellite.

We follow a combination of TB01 with P10 models’ procedures that properly take into account tidal stripping and heating after infall to extract accurate $v_{max}$ values. TB01 compared their model with high resolution simulations, while 