  The dominant physical formation mechanism(s) for ultra-diffuse galaxies
(UDGs) is still poorly understood. Here, we combine new, deep imaging from the
Jeanne Rich Telescope with deep integral field spectroscopy from the Keck II
telescope to investigate the formation of UDG1137+16. Our new analyses confirm
both its environmental association with the low density UGC 6594 group, along
with its large size of 3.3 kpc and status as a UDG. The new imaging reveals two
distinct stellar components for UDG1137+16, indicating that a central stellar
body is surrounded by an outer stellar envelope undergoing tidal interaction.
Both the components have approximately similar stellar masses. From our
integral field spectroscopy we measure a stellar velocity dispersion within the
half-light radius (15 $\pm$ 4 $\mathrm{km\ s^{-1}}$) and find that UDG1137+16
is similar to some other UDGs in that it is likely dark matter dominated.
Incorporating literature measurements, we also examine the current state of UDG
observational kinematics. Placing these data on the central stellar velocity
dispersion -- stellar mass relation, we suggest there is little evidence for
UDG1137+16 being created through a strong tidal interaction. Finally, we
investigate the constraining power current dynamical mass estimates (from
stellar and globular cluster velocity dispersions) have on the total halo mass
of UDGs. As most are measured within the half-light radius, they are unable to
accurately constrain UDG total halo masses.
