  Observed cusps with density profiles $\rho\propto r^{-1}$ or shallower, in
the central regions of galaxies, cannot be reproduced in the standard Cold Dark
Matter (CDM) picture of hierarchical clustering. Previous claims to the
contrary were based on simulations with relatively few particles, and
substantial softening. We present simulations with particle numbers an order of
magnitude higher, and essentially no softening, and show that typical central
density profiles are clearly steeper than $\rho\propto r^{-1}$. The observed
shallower profiles may have formed through the smoothing effect of the
spiral-in of central black holes in previous merger phases. In addition, we
confirm the presence of a temperature inversion in the inner 5 kpc of massive
galactic halos, and illustrate its formation as a natural result of the merging
of unequal progenitors.
