  We present spatially resolved kinematics of the interstellar NaI D 5890,5896
doublet absorption and 12CO(1-0) emission across the inner ~2x1 kpc of the disk
of M82. These data were obtained with the DensePak IFU on the WIYN telescope
and the Caltech Owens Valley Radio Observatory (OVRO) millimetre array. By
measuring the NaI and CO (and Halpha kinematics from a previous study) at the
same spatial resolution, and employing the same line fitting method, we have
been able to make meaningful comparisons between the ionized, neutral and
molecular gas phases. We detect a component of the NaI line throughout the
inner disk with velocities that are forbidden by the known galactic rotation.
We interpret this as originating in counter-rotating or perhaps inflowing
material. In the southern plume, we find clear evidence of entrained CO gas
with kinematics consistent with that of Halpha. On the northern side, the CO
kinematics appear to trace more static clouds in the inner halo that could be
pre-existing or tidal in origin. We find no evidence that NaI absorption is
kinematically associated with the outflow. We conclude that a combination of
lack of velocity resolution and confusion of due to the high inclination of the
system is acting to prevent detection. Thus, in the search for neutral outflows
from galaxies, the signature high velocity components may easily be missed in
observations at low spectral resolution and/or sensitivity, and particularly so
in highly inclined systems.
