  A likely tidal disruption of a star by the intermediate-mass black hole
(IMBH) of a dwarf galaxy was recently identified in association with Abell
1795. Without deep spectroscopy for this very faint object, however, the
possibility of a more massive background galaxy or even a disk-instability
flare from a weak AGN could not be dismissed. We have now obtained 8 hours of
Gemini spectroscopy which unambiguously demonstrate that the host galaxy is
indeed an extremely low-mass $(M_\ast\sim 3\times 10^8\; {\rm M}_{\odot})$
galaxy in Abell 1795, comparable to the least-massive galaxies determined to
host IMBHs via other studies. We find that the spectrum is consistent with the
X-ray flare being due to a tidal disruption event rather than an AGN flare. We
also set improved limits on the black hole mass $({\rm log}[M_{\bullet}/{\rm
M}_{\odot}] \sim 5.3 - 5.7)$ and infer a 15-year X-ray variability of a factor
of $> 10^4$. The confirmation of this galaxy-black hole system provides a
glimpse into a population of galaxies that is otherwise difficult to study, due
to the galaxies' low masses and intrinsic faintness, but which may be important
contributors to the tidal disruption rate.
