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[Abridged] We present maps of the main cooling lines of the neutral atomicgas ([OI] at 63 and 145 micron and [CII] at 158 micron) and in the [OIII] 88micron line of the starburst galaxy M82, carried out with the PACS spectrometeron board the Herschel satellite. By applying PDR modeling we derive maps of themain ISM physical parameters, including the [CII] optical depth, atunprecedented spatial resolution (~300 pc). We can clearly kinematicallyseparate the disk from the outflow in all lines. The [CII] and [OI]distributions are consistent with PDR emission both in the disk and in theoutflow. Surprisingly, in the outflow, the atomic and the ionized gas traced bythe [OIII] line both have a deprojected velocity of ~75 km/s, very similar tothe average velocity of the outflowing cold molecular gas (~ 100 km/s) andseveral times smaller than the outflowing material detected in Halpha (~ 600km/s). This suggests that the cold molecular and neutral atomic gas and theionized gas traced by the [OIII] 88 micron line are dynamically coupled to eachother but decoupled from the Halpha emitting gas. We propose a scenario wherecold clouds from the disk are entrained into the outflow by the winds wherethey likely evaporate, surviving as small, fairly dense cloudlets (n_H\sim500-1000 cm^-3, G_0\sim 500- 1000, T_gas\sim300 K). We show that the UV photonsprovided by the starburst are sufficient to excite the PDR shells around themolecular cores. The mass of the neutral atomic gas in the outflow is \gtrsim5-12x 10^7 M_sun to be compared with that of the molecular gas (3.3 x 10^8M_sun) and of the Halpha emitting gas (5.8 x 10^6 M_sun). The mass loadingfactor, (dM/dt)/SFR, of the molecular plus neutral atomic gas in the outflow is~ 2. Energy and momentum driven outflow models can explain the data equallywell, if all the outflowing gas components are taken into account.

Spectroscopic FIR mapping of the disk and galactic wind of M82 with Herschel-PACS