Cluster core radii taken from Baumgardt & Hilker (2018) as a function of the average change in position between our initial and final snapshots (initial—present day). Note the possible trend of increasing core radius (reflecting little internal dynamical evolution) as a function of decreasing change in position (change in tidal forces) among our trapped GCs. The only outliers to the trend are the young, metal-rich GC Pal 11 (discussed in Section 4.1) and the ancient, metal-poor GC NGC 4372 (Section 4.3). Possible explanations for both are given in the corresponding sections.