  One way an Active Galactic Nucleus (AGN) influences the evolution of their
host galaxy is by generating a large-scale (kpc-scale) outflow. The content,
energetics, and impact of such outflows depend on the properties of both the
AGN and host galaxy, and understanding the relationship between them requires
measuring the properties of all three. In this paper, we do so by analyzing
recent radio and optical integral field unit (IFU) spectroscopic observations
of MaNGA 1-166919. Our results indicate that the bi-conical outflow in this
galaxy is powered by a low-luminosity, low-Eddington ratio AGN ejecting
material that drives ~100-200 km/s shocks into the surrounding interstellar
medium (ISM) -- producing the hot, ionized gas and relativistic particles
associated with the observed outflow. The energetics of the relativistic and
ionized gas material produced at this shock are comparable, and both the mass
outflow and kinetic power of the ionized gas in this outflow are higher than
other AGN with similar bolometric luminosities. Lastly, while the host galaxy's
total star formation rate is comparable to that of other star-forming galaxies
with a similar stellar mass, there is evidence that the outflow both suppresses
and enhances star formation in its immediate surroundings.
