  The ultra-faint dwarf galaxy Leo V has shown both photometric overdensities
and kinematic members at large radii, along with a tentative kinematic
gradient, suggesting that it may have undergone a close encounter with the
Milky Way. We investigate these signs of disruption through a combination of i)
high-precision photometry obtained with the Hubble Space Telescope (HST), ii)
two epochs of stellar spectra obtained with the Hectochelle Spectrograph on the
MMT, and iii) measurements from the Gaia mission. Using the HST data, we
examine one of the reported stream-like overdensities at large radii, and
conclude that it is not a true stellar stream, but instead a clump of
foreground stars and background galaxies. Our spectroscopic analysis shows that
one known member star is likely a binary, and challenges the membership status
of three others, including two distant candidates that had formerly provided
evidence for overall stellar mass loss. We also find evidence that the proposed
kinematic gradient across Leo V might be due to small number statistics. We
update the systemic proper motion of Leo V, finding $(\mu_\alpha \cos\delta,
\mu_\delta)= (0.009\pm0.560$, $-0.777\pm0.314)$ mas yr$^{-1}$, which is
consistent with its reported orbit that did not put Leo V at risk of being
disturbed by the Milky Way. These findings remove most of the observational
clues that suggested Leo V was disrupting, however, we also find new plausible
member stars, two of which are located >5 half-light radii from the main body.
These stars require further investigation. Therefore, the nature of Leo V still
remains an open question.
