A spatial and spectral analysis of the emission from the supernova remnant G266.2-1.2

G266.2-1.2 is a recently discovered supernova remnant observed to produce faint radio and Xray emission as well as TeV gamma rays. The age, distance, and gamma-ray emission mechanism have been a source of controversy. To help determine the age and distance, we present the results of an analysis of our 2003 and 2008 Chandra observations of the northwestern region. These results show that the remnant is expanding at the rate of 0.43±0.09 arcsec yr-1 from which the age and distance are inferred to be 2-9 kyr and 1-3 kpc, respectively. Furthermore, the ambient density is inferred to be less than 0.1 cm-3, perhaps much less. To help determine whether the TeV gamma rays are produced by electrons or protons, we present the results of a joint spectral analysis of some radio, X-ray, and gamma-ray data. It is possible to fit the broad-band data with a simple, single-zone, leptonic model. However, if the TeV emission is dominated by the decay of neutral pions, then very-high-energy protons must outnumber very-high-energy electrons by a ratio that is much larger than the ratio observed locally (i.e. the ratio expected from charge conservation).