NOEMA High Fidelity Imaging of the Molecular Gas in and around M82
  We present a 154 pointing IRAM NOEMA mosaic of the CO(1-0) line emission in
and around the nearby starburst galaxy M82. The observations, complemented by
zero--spacing observations, reach a spatial resolution of $\sim$30 pc ($\sim
1.9^{\prime\prime}$) at 5.0 km s$^{-1}$ spectral resolution, sufficient to
resolve the molecular gas in the central starburst disk, the outflow, as well
as the tidal streamers. The resulting moment and peak brightness maps show a
striking amount of structure. Using a clump decomposition algorithm, we analyse
the physical properties (e.g., radii $R$, line widths $\sigma$, and masses $M$)
of $\sim2000$ molecular clouds. To first order, the clouds' properties are very
similar, irrespective of their environment. This also holds for the size-line
width relations of the clouds. The distribution of clouds in the $\sigma^2/R$
vs. column density $\Sigma$ space suggests that external pressure does not play
a significant role in setting their physical parameters in the outflow and the
streamers. We find that the clouds in the streamers stay approximately constant
in size ($R \sim 50$ pc) and mass ($M \sim 10^5$ M$_\odot$) and do not vary
with their projected distance from M82's center. The clouds in the outflow, on
the other hand, appear to decrease in size and mass with distance towards the
Southern outflow. The reduction in the molecular gas luminosity could be
indicative of cloud evaporation of embedded clouds in the hot outflow.
