We perform controlled numerical experiments to asses the effect of baryon mass loss on the inner structure of large galactic dark matter haloes. This mass expulsion is intended to mimic both the supernovae and AGN feedbacks, as well as the evolution of stellar populations. This study is meant in particular for precursors of massive Early Type Galaxies, wherein strong AGN feedback (often dubbed “QSO mode” in galaxy formation models) has been proposed to remove on a short timescale, of the order of a few dynamical times, a substantial fraction of their baryons. In a previous paper we evaluated the observational consequences (size increase) of this process on the galactic structure (Ragone-Figueroa & Granato 2011). Here we focus on the distribution of dark matter in the galactic region. It is shown that the inner region of the DM halo expands and its density profile flattens by a sizeable amount, with little dependence on the expulsion timescale. We also evaluate the effect of the commonly made approximation of treating the baryonic component as a potential that changes in intensity without any variation in shape. This approximation leads to some underestimates of the halo expansion and its slope flattening. We conclude that cuspy density profiles in ETGs could be difficult to reconcile with an effective AGN (or stellar) feedback during the evolution of these systems.