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The dominant physical formation mechanism(s) for ultra-diffuse galaxies(UDGs) is still poorly understood. Here, we combine new, deep imaging from theJeanne Rich Telescope with deep integral field spectroscopy from the Keck IItelescope to investigate the formation of UDG1137+16 (dw1137+16). Our newanalyses confirm both its environmental association with the low density UGC6594 group, along with its large size of 3.3 kpc and status as a UDG. The newimaging reveals two distinct stellar components for UDG1137+16, indicating thata central stellar body is surrounded by an outer stellar envelope undergoingtidal interaction. Both the components have approximately similar stellarmasses. From our integral field spectroscopy we measure a stellar velocitydispersion within the half-light radius (15 $\pm$ 4 $\mathrm{km\ s^{-1}}$) andfind that UDG1137+16 is similar to some other UDGs in that it is likely darkmatter dominated. Incorporating literature measurements, we also examine thecurrent state of UDG observational kinematics. Placing these data on thecentral stellar velocity dispersion -- stellar mass relation, we suggest thereis little evidence for UDG1137+16 being created through a strong tidalinteraction. Finally, we investigate the constraining power current dynamicalmass estimates (from stellar and globular cluster velocity dispersions) have onthe total halo mass of UDGs. As most are measured within the half-light radius,they are unable to accurately constrain UDG total halo masses.

A Photometric and Kinematic Analysis of UDG1137+16 (dw1137+16): Probing Ultra-Diffuse Galaxy Formation in a Group Environment