HERSCHEL-SPIRE IMAGING SPECTROSCOPY OF MOLECULAR GAS IN M82

We present new Herschel-SPIRE imaging spectroscopy (194-671 mu m) of the bright starburst galaxy M82. Covering the CO ladder from J = 4 -> 3 to J = 13 -> 12, spectra were obtained at multiple positions for a fully sampled similar to 3 x 3 arcmin map, including a longer exposure at the central position. We present measurements of (CO)-C-12, (CO)-C-13, [CI], [NII], HCN, and HCO+ in emission, along with OH+, H2O+, and HF in absorption and H2O in both emission and absorption, with discussion. We use a radiative transfer code and Bayesian likelihood analysis to model the temperature, density, column density, and filling factor of multiple components of molecular gas traced by (CO)-C-12 and (CO)-C-13, adding further evidence to the high-J lines tracing a much warmer (similar to 500 K), less massive component than the low-J lines. The addition of (CO)-C-13 (and [CI]) is new and indicates that [CI] may be tracing different gas than (CO)-C-12. No temperature/density gradients can be inferred from the map, indicating that the single-pointing spectrum is descriptive of the bulk properties of the galaxy. At such a high temperature, cooling is dominated by molecular hydrogen. Photon-dominated region (PDR) models require higher densities than those indicated by our Bayesian likelihood analysis in order to explain the high-J CO line ratios, though cosmic-ray-enhanced PDR models can do a better job reproducing the emission at lower densities. Shocks and turbulent heating are likely required to explain the bright high-J emission.