  We study the surface brightness profiles of a sample of brightest cluster
galaxies (BCGs) with 0.3<z<0.9. The BCGs are selected from the first
Red-sequence Cluster Survey and an X-ray cluster survey. The surface brightness
profiles of the BCGs are measured using HST ACS images, and most of them can be
well modeled by a Sersic profile with index ~ 6 and half-light radius ~ 30 kpc.
Although the single Sersic model fits the profiles well, we argue that the
systematics in the sky background measurement and the coupling between the
model parameters make the comparison of the model parameters ambiguous. Direct
comparison of the BCG profiles, on the other hand, has revealed an inside-out
growth for these most massive galaxies: as the mass of a BCG increases, the
central mass density of the galaxy increases slowly ($\rho_{1kpc} \propto
M*^{0.39}$), while the slope of the outer profile grows continuously shallower
($\alpha \propto M*^{-2.5}$). Such a fashion of growth continues down to the
less massive early-type galaxies (ETGs), without apparent distinction between
BCGs and non-BCGs. For the very massive ETGs and BCGs, the slope of the
Kormendy relation starts to trace the slope of the surface brightness profiles
and becomes insensitive to subtle profile evolution. These results are
generally consistent with dry mergers being the major driver of the mass growth
for BCGs and massive ETGs. We also find strong correlations between the
richness of clusters and the properties of BCGs: the more massive the clusters
are, the more massive the BCGs ($M*_{bcg} \propto M_{clusters}^{0.6}$) and the
shallower their surface brightness profiles. After taking into account the bias
in the cluster samples, we find the masses of the BCGs have grown by at least a
factor of 1.5 from z=0.5 to z=0, in contrast to the previous findings of no
evolution. Such an evolution validates the expectation from the LCDM model.
