from baryons clumps to DM through dynamical friction (DF) (El-Zant et al. 2001, 2004; Ma & Boylan-Kolchin 2004; Nipoti et al. 2004; Romano-Diaz et al. 2008, 2009; DP09; Cole et al. 2011; Inoue & Saitoh 2011). We use DP09 to calculate the flattening of isolated satellites through the mechanism based on DF. In order to study the effect of tidal stripping and heating on the satellites, we use a combination of the procedures from Taylor & Babul (2001) (TB01) with that from P10. Our model differs from the TB01 and P10 models because we use a semi-analytical model based on DF (combination coined hereafter TBP model). In addition to the difference in the cuspy to cored profile mechanism, already present in B13, our TBP based model is properly taking into account the tidal heating mechanism. Such tidal heating is not captured in the SPH simulations from which Z12 derive their correction (as stressed in Sect. 4 of B13), since, as they point out, this would require a very high resolution to be captured (Choi et al. 2009). Moreover, we properly take into account disk shocking while this is neglected in Z12[^7]: we account for the effects of satellites passing through 