(see Figure \[fig:pgc175370\]).

Results and Discussion {#sec:results}
======================

Radial distributions
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Radial profiles of the surface density of UDGs were made for each of the six clusters and are shown in Figure \[fig:radial-profiles\]. The location of the BCG was adopted as the cluster centre, or in the case of multiple BCGs, their midpoint; these are listed in Table \[tab:clusters\]. For each cluster, the leftmost panels in Figure \[fig:radial-profiles\] show the raw observed radial densities (black points) along with the density of background sources estimated from the number of XDF sources that satisfy each cluster’s UDG cut (gray dotted line, roughly ${\sim}2~\mathrm{arcmin}^{-2}$). The central panels shows the profile after correcting for the completeness in each radial bin (right panels) and subtracting off the background density. In all six clusters, either a central depletion or a flattening out of the radial profile of UDGs is observed. This behaviour has been described in several nearby clusters [e.g. @vdb2016; @mancerapina2018] and is thought to be caused by the tidal disruption of UDGs near the centres of galaxy clusters. However, using simulations, [@sales2019] find that the surface density of UDGs rises continually towards the centre of a Virgo-like cluster. At radii inside ${\sim}0.4 \times R_{200}$, 