NIHAO-XXIII: Dark Matter density shaped by Black Hole feedback
  We present a systematic analysis of the reaction of dark matter distribution
to galaxy formation across more than eight orders of magnitude in stellar mass.
We extend the previous work presented in the NIHAO-IV paper (Tollet et al.) by
adding 46 new high resolution simulations of massive galaxies performed with
the inclusion of Black Hole feedback. We show that outflows generated by the
AGN are able to partially counteract the dark matter contraction due to the
large central stellar component in massive haloes. The net effect is to relax
the central dark matter distribution that moves to a less cuspy density
profiles at halo masses larger than $\approx 3 \times 10^{12}$ M$_{\odot}$. The
scatter around the mean value of the density profile slope ($\alpha$) is fairly
constant ($\Delta\alpha \approx 0.3$), with the exception of galaxies with halo
masses around $10^{12}$ M$_{\odot}$, at the transition from stellar to AGN
feedback dominated systems, where the scatter increases by almost a factor
three. We provide useful fitting formulas for the slope of the dark matter
density profiles at few percent of the virial radius for the whole stellar mass
range: $10^5-10^{12}$ M$_{\odot}$ ($2 \times 10^9-5 \times 10^{13}$ M$_{\odot}$
in halo mass).
