2012ApJ...761...55M

The M82 "cap" is a gas cloud at a projected radius of 11.6 kpc along the minor axis of this well-known superwind source. The cap has been detected in optical line emission and X-ray emission and therefore provides an important probe of the wind energetics. In order to investigate the ionization source of the cap, we observed it with the Kyoto3DII Fabry-Perot instrument mounted on the Subaru Telescope. Deep continuum, Hα, [N II]λ6583/Hα, and [S II]λλ6716,6731/Hα maps were obtained with subarcsecond resolution. The superior spatial resolution compared to earlier studies reveals a number of bright Hα emitting clouds within the cap. The emission line widths ( ≲ 100 km/s FWHM) and line ratios in the newly identified knots are most reasonably explained by slow to moderate shocks velocities (v_shock= 40-80 km/s) driven by a fast wind into dense clouds. The momentum input from the M82 nuclear starburst region is enough to produce the observed shock. Consequently, earlier claims of photoionization by the central starburst are ruled out because they cannot explain the observed fluxes of the densest knots unless the UV escape fraction is very high (f _esc> 60%), i.e., an order of magnitude higher than observed in dwarf galaxies to date. Using these results, we discuss the evolutionary history of the M82 superwind. Future UV/X-ray surveys are expected to confirm that the temperature of the gas is consistent with our moderate shock model.