The Disturbed and Globular Cluster-Rich Ultra-diffuse Galaxy UGC 9050-Dw1

We investigate the ultra-diffuse galaxy (UDG) UGC 9050-Dw1, which was selected because of its disturbed morphology as part of a larger sample of UDGs that display evidence for significant interactions. We use the Hubble Space Telescope’s Advanced Camera for Surveys to identify globular clusters (GCs) associated with UGC 9050-Dw1, and the Jansky Very Large Array to measure its $\mathrm{H}\mathrm{I}$ content. UGC 9050-Dw1, a neighbor to the low surface brightness spiral UGC 9050, exhibits a unique UV bright central ``clump’’ with clearly associated $\mathrm{H}\mathrm{I}$ gas and an extended stellar tidal plume to the north. We identify $52_{-6}^{+4}$ GCs, implying a specific frequency $S_{\mathrm{N}}=122_{-24}^{+30}$, one of the highest reported for a UDG of this luminosity. Additionally, $\sim 20\mathrm{\%}$ of the total light of the galaxy is contributed by GCs. Nearly uniform GC colors suggest they were formed during a single intense episode of star formation. We propose that UGC 9050-Dw1 formed via a rare dwarf merger event where induced, clumpy star formation led to its current observed properties.