  We present the analysis of deep optical imaging of the galaxy cluster Abell
133 with the IMACS instrument on Magellan. Our multi-band photometry enables
stellar mass measurements in the cluster member galaxies down to a mass limit
of $M_\star=3\times10^8\,M_\odot$ ($\approx 0.1$ of the Large Magellanic Cloud
stellar mass). We observe a clear difference in the spatial distribution of
large and dwarf galaxies within the cluster. Modeling these galaxies
populations separately, we can confidently track the distribution of stellar
mass locked in the galaxies to the cluster's virial radius. The extended
envelope of the cluster's brightest galaxy can be tracked to $\sim 200$ kpc.
The central galaxy contributes $\sim 1/3$ of the the total cluster stellar mass
within the radius $r_{500c}$.
