  We present our study of the evolution of brightest cluster galaxies based on
data from the Las Campanas Distant Cluster Survey (Gonzalez et al. 2001) and
HST optical and IR imaging. We briefly discuss the technique that enabled us to
use short (~ 3 min) exposures and a small (1m) telescope to efficiently survey
about 130 sq. deg. of sky for high-z galaxy clusters. Follow-up imaging is used
to construct a sample of several tens of BCGs at 0.3 < z < 0.9 with which to
explore their evolution. In particular, we examine the luminosity and color
evolution of these galaxies. We confirm the previous results that 1) BCGs in
different environments evolve differently (eg. Burke et al 2000), 2) BCGs,
particularly those in low-mass clusters, must be accreting significantly since
z ~ 1 (Aragon-Salamanca et al. 1998). From measurments of the colors vs.
redshift, we conclude that this accretion must consist of old stellar
populations. Using HST NICMOS and WFPC2 images, we find preliminary evidence
for evolution in the sizes of BCGs that is consistent with the accretion model
presented in standard hierarchical models (Aragon-Salamanca et al. 1998), but
puzzling differences between NICMOS and WFPC2 scale lengths precludes a
definitive conclusion.
