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We present a wide area (~ 8 x 8 kpc), sensitive map of CO (2-1) emissionaround the nearby starburst galaxy M82. Molecular gas extends far beyond thestellar disk, including emission associated with the well-known outflow as faras 3 kpc from M82's midplane. Kinematic signatures of the outflow are visiblein both the CO and HI emission: both tracers show a minor axis velocitygradient and together they show double peaked profiles, consistent with a hotoutflow bounded by a cone made of a mix of atomic and molecular gas. Combiningour CO and HI data with observations of the dust continuum, we study thechanging properties of the cold outflow as it leaves the disk. While H_2dominates the ISM near the disk, the dominant phase of the cool medium changesas it leaves the galaxy and becomes mostly atomic after about a kpc. Severalarguments suggest that regardless of phase, the mass in the cold outflow doesnot make it far from the disk; the mass flux through surfaces above the diskappears to decline with a projected scale length of ~ 1-2 kpc. The coolmaterial must also end up distributed over a much wider angle than the hotoutflow based on the nearly circular isophotes of dust and CO at low intensityand the declining rotation velocities as a function of height from the plane.The minor axis of M82 appears so striking at many wavelengths because theinterface between the hot wind cavity and the cool gas produces Halpha, hotdust, PAH emission, and scattered UV light. We also show the level at which aface-on version of M82 would be detectable as an outflow based on unresolvedspectroscopy. Finally, we consider multiple constraints on the CO-to-H$_2$conversion factor, which must change across the galaxy but appears to be only afactor of ~ 2 lower than the Galactic value in the outflow.

The Multi-Phase Cold Fountain in M82 Revealed by a Wide, Sensitive Map of the Molecular ISM