  We present the kinematics of the ionized gas over the inner 140 arcsec (10
kpc) of NGC 1068 from observations with the HIFI Fabry-Perot interferometer.
There is clear evidence for density wave streaming and bar-driven streaming
across the field, with bi-symmetric arms that penetrate to within 200 pc of the
nucleus. CO maps show linear structures along (although slightly offset from)
the bar consistent with a strong shock. Along the spiral arms which encircle
the bar, the HII regions lie downstream of the CO gas in the rest frame of the
bar, as do the dust lanes, only if the gas outruns the stellar bar. As a first
step towards understanding the details of the gas kinematics, and attempting to
determine the mass inflow rate towards the nucleus, we build a mass model for
the central disk constrained by near-infrared images. We plan to use this model
as gravitational background potential for hydro-dynamical simulations of the
gas response to the bar. Comparing these with the data presented should enable
us to constrain various quantities such as pattern speed, stellar mass-to-light
ratio, central mass concentration, and gas fueling rate.
