P10 checked theirs, in their Appendix A, through high resolution N-body simulations.

The TB01 model follows the merger history, growth of the interacting satellites and tracks the substructure evolution, taking into account the mass loss due to tidal stripping, tidal heating, as well as enhancement of stripping due to the disc, in the host halo. The P10 model is fundamentally based on TB01, however not including tidal heating. Our model assumes the same DM host halo NFW (Navarro, Frenk & White 1996) density profile as P10. It also neglects, as P10 and contrary to TB01, the effect of its baryonic bulge. The latter assumption is justified by the disc’s much larger mass than the bulge’s, and its 10 times larger density gradient than found in the bulge or the halo. Such gradient endows the disk with 100 times more heating efficiency on the satellites than the other components. This semi-analytic model, indicated as TBP model, is described in Appendix \[Dynamics of the satellites\].

At this point we may put together the mass decrease in satellites due to phase 1 (core flattening due to interaction of baryonic clumps with DM), and that due to tidal stripping and heating.

In Fig. \[fig:DMO-DMB\] 