  We explore the kinematics of the stars, ionized gas, and warm molecular gas
in the Seyfert 2 galaxy Mrk~3 (UGC~3426) on nuclear and galactic scales with
{\it Gemini} Near-Infrared Field Spectrograph (NIFS) observations, previous
{\it Hubble Space Telescope} data, and new long-slit spectra from the {\it
Apache Point Observatory} ({\it APO}) 3.5 m telescope. The {\it APO} spectra
are consistent with our previous suggestion that a galactic-scale gas/dust disk
at PA $=$ 129\arcdeg, offset from the major axis of the host S0 galaxy at PA
$=$ 28\arcdeg, is responsible for the orientation of the extended narrow-line
region (ENLR). The disk is fed by an H~I tidal stream from a gas-rich spiral
galaxy (UGC~3422) $\sim$100 kpc to the NW of Mrk 3, and is ionized by the AGN
to a distance of at least $\sim$20\arcsec\ ($\sim$5.4 kpc) from the central
supermassive black hole (SMBH). The kinematics within at least 320 pc of the
SMBH are dominated by outflows with radial (line of sight) velocities up to
1500 km s$^{-1}$ in the ionized gas and 500 km s$^{-1}$ in the warm molecular
gas, consistent with in situ heating, ionization, and acceleration of ambient
gas to produce the narrow-line region (NLR) outflows. There is a disk of
ionized and warm molecular gas within $\sim$400 pc of the SMBH that has
re-oriented close to the stellar major axis but is counter-rotating, consistent
with claims of external fueling of AGN in S0 galaxies.
