  Using N-body simulations we show that the process of formation of the
brightest cluster galaxy through dissipationless galactic cannibalism can
affect the inner cluster dark matter density profile. In particular, we use as
realistic test case the dynamical evolution of the galaxy cluster C0337-2522 at
redshift z=0.59, hosting in its centre a group of five elliptical galaxies
which are likely to be the progenitor of a central giant elliptical. After the
formation of the brightest cluster galaxy, the inner cluster dark matter
density profile is significantly flatter (logarithmic slope 0.49<beta<0.90)
than the original cusp (beta=1), as a consequence of dynamical friction heating
of the massive galaxies against the diffuse cluster dark matter. In our
simulations we have assumed that the cluster galaxies are made of stars only.
We also show that the presence of galactic dark matter haloes can steepen the
cluster central density profile. We conclude that galactic cannibalism could be
a viable physical mechanism to reconcile - at least at the cluster scale - the
flat dark matter haloes inferred observationally in some galaxy clusters with
the steep haloes predicted by cosmological simulations.
