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It is clear that within the class of ultra-diffuse galaxies (UDGs) there isan extreme range in the richness of their associated globular cluster (GC)systems. Here, we report the structural properties of five UDGs in the Perseuscluster based on deep Subaru / Hyper Suprime-Cam imaging. Three appear GC-poorand two appear GC-rich. One of our sample, PUDG\_R24, appears to be undergoingquenching and is expected to fade into the UDG regime within the next $\sim0.5$Gyr. We target this sample with Keck Cosmic Web Imager (KCWI) spectroscopy toinvestigate differences in their dark matter halos, as expected from theirdiffering GC content. Our spectroscopy measures both recessional velocities,confirming Perseus cluster membership, and stellar velocity dispersions, tomeasure dynamical masses within their half-light radius. We supplement our datawith that from the literature to examine trends in galaxy parameters with GCsystem richness. We do not find the correlation between GC numbers and UDGphase space positioning expected if GC-rich UDGs environmentally quench at highredshift. We do find GC-rich UDGs to have higher velocity dispersions thanGC-poor UDGs on average, resulting in greater dynamical mass within thehalf-light radius. This agrees with the first order expectation that GC-richUDGs have higher halo masses than GC-poor UDGs.

Ultra-Diffuse Galaxies in the Perseus Cluster: Comparing Galaxy Properties with Globular Cluster System Richness