  We use cosmological simulations to study the effects of supernova (SN)
feedback on the dark matter distribution in galaxies. We simulate the formation
of a Milky-Way type galaxy using a version of the SPH code GADGET2 which
includes chemical enrichment and energy feedback by SN, a multiphase model for
the gas component and metal-dependent cooling. We analyse the impact of the
main three input SN feedback parameters on the amplitude and shape of the dark
matter density profiles, focusing on the inner regions of the halo. In order to
test the dependence of the results on the halo mass, we simulated a scale-down
version of this system. First results of this ongoing work show that the dark
matter distribution is affected by the feedback, through the redistribution of
the baryons. Our findings suggest that the response of the dark matter halo
could be the result of a combination of several physical parameters such as the
amount of stellar mass formed at the centre, its shape, and probably the bursty
characteristics of the star formation rate. As expected, we find that the dark
matter haloes of small galaxies are more sensitive to SN feedback. Higher
resolution simulations are being performed to test for numerical effects.
