The evolution of galaxies in dense environments can be affected by close encounters with neighbouring galaxies and interactions with the intracluster medium. Dwarf galaxies are important as their low mass makes them more susceptible to these effects than giant systems. Combined luminosity functions (LFs) in the r-and u-band of 15 galaxy clusters were constructed using archival data from the Canada-France-Hawaii Telescope. LFs were measured as a function of cluster-centric radius from stacked cluster data. Marginal evidence was found for an increase in the faint-end slope of the u-band LF relative to the r -band with increasing cluster-centric radius. The dwarf-togiant ratio (DGR) was found to increase toward the cluster outskirts, with the u-band DGR increasing faster with cluster-centric radius compared to the r -band. The dwarf galaxy blue fraction was found to be a factor of ∼ 2 times larger than the giant galaxy blue fraction over all measured cluster-centric distance (∼ 5σ level). The central concentration (C) was used as a proxy to distinguish nucleated versus non-nucleated dwarf galaxies. The ratio of high-C to low-C dwarf galaxies was found to be ∼ 2 times greater in the inner cluster region compared to the cluster outskirts (2.8σ level). The faint-end slope of the r-and u-band LF for the cluster outskirts (0.6 ≤ r/r 200 < 1.0) is steeper than the SDSS field LF. Decrease in the faint-end slope of the r-and u-band cluster LFs towards the cluster centre is consistent with the quenching of star formation via ram pressure stripping and galaxy-galaxy interactions.

We present the first measurement of the globular cluster population surrounding the elliptical galaxy J07173724+3744224 (z = 0.1546). This galaxy is located in the foreground in the field-of-view of the Hubble Space Telescope (HST) Frontier Fields observations of galaxy cluster MACS J0717.5+3745 (z = 0.5458). Based on deep HST ACS F435W, F606W, and F814W images, we find a total globular cluster population of N t ot = 3441 ± 1416. Applying the appropriate extinction correction and filter transformation from ACS F814W to the Johnson V-band, we determine that the host galaxy has an absolute magnitude of M V = −22.2. The specific frequency was found to be S N = 4.5 ± 1.8. The radial profile of the globular cluster system was best fit using a powerlaw of the form σ ∼ R −0.6 , with the globular cluster population found to be more extended than the halo light of the host galaxy (σ halo ∼ R −1.7 ). The F435W−F814W colour distribution suggests a bimodal population, with red globular clusters 1 − 3× more abundant than blue clusters. These results are consistent with the host elliptical galaxy J07173724+3744224 having formed its red metal-rich GCs in situ, with the blue metal-poor globular clusters accreted from low-mass galaxies.