The Galactic Centre-a laboratory for starburst galaxies (?)

The Galactic centre-as the closest galactic nucleus-holds both intrinsic interest and possibly represents a useful analogue to starburst nuclei which we can observe with orders of magnitude finer detail than these external systems. The environmental conditions in the GC-here taken to mean the inner 200 pc in diameter of the Milky Way-are extreme with respect to those typically encountered in the Galactic disk. The energy densities of the various GC ISM components are typically ∼two orders of magnitude larger than those found locally and the star-formation rate density ∼three orders of magnitude larger. Unusually within the Galaxy, the Galactic centre exhibits hard-spectrum, diffuse TeV (=10 ¹² eV) gamma-ray emission spatially coincident with the region's molecular gas. Recently the nuclei of local starburst galaxies NGC 253 and M82 have also been detected in gamma-rays of such energies. We have embarked on an extended campaign of modelling the broadband (radio continuum to TeV gamma-ray), non-thermal signals received from the inner 200 pc of the Galaxy. On the basis of this modelling we find that star-formation and associated supernova activity is the ultimate driver of the region's non-thermal activity. This activity drives a large-scale wind of hot plasma and cosmic rays out of the GC. The wind advects the locally-accelerated cosmic rays quickly, before they can lose much energy in situ or penetrate into the densest molecular gas cores where star-formation occurs. The cosmic rays can, however, heat/ionize the lower density/warm H 2 phase enveloping the cores. On very large scales (∼10 kpc) the non-thermal signature of the escaping GC cosmic rays has probably been detected recently as the spectacular "Fermi bubbles" and corresponding "YWMAP haze".