  We test the proposal by El-Zant et al that the dark matter density of halos
could be reduced through dynamical friction acting on heavy baryonic clumps in
the early stages of galaxy formation. Using N-body simulations, we confirm that
the inner halo density cusp is flattened to 0.2 of the halo break radius by the
settling of a single clump of mass \ga 0.5% of the halo mass. We also find that
an ensemble of 50 clumps each having masses \ga 0.2% can flatten the cusp to
almost the halo break radius on a time scale of \sim9 Gyr, for an NFW halo of
concentration 15. We summarize some of the difficulties that need to be
overcome if this mechanism is to resolve the apparent conflict between the
observed inner densities of galaxy halos and the predictions of LCDM.
