  The potential of the Surface Brightness Fluctuation (SBF) method to determine
distances to dwarf ellipticals in nearby clusters is investigated. We find that
for the Fornax cluster, the SBF method yields reliable results down to very
faint magnitudes, in our case down to M_V ~- 11 mag when observing for about 1
hour at good seeing with an 8m-class telescope in the I-filter. Comparison
between real and simulated data for the Centaurus Cluster shows that our
simulations do not overestimate the achievable S/N of the SBF method.
