The Nature of a Cosmic-Ray Accelerator, CTB 37 B, Observed with Suzaku and Chandra

We report on Suzaku and Chandra observations of the young supernova remnant CTB 37 B, from which TeV gamma-rays were detected by the H.E.S.S. Cherenkov telescope. The 80 ks Suzaku observation provided us with a clear image of diffuse emission and high-quality spectra. The spectra revealed that the diffuse emission is comprised of thermal and non-thermal components. The thermal component can be represented by an NEI model with a temperature, a pre-shock electron density and an age of 0.9 +/- 0.2 keV, 0.4 +/- 0.1 cm(-3), and 650(-300)(+2500) yr, respectively. This suggests that the explosion of CTB 37 B occurred ill a low-density space. A non-thermal power-law component was found from the southern region of CTB 37 B. Its photon index of similar to 1.5 and a high roll-off energy (greater than or similar to 15 keV) indicate efficient cosmic-ray acceleration. A comparison of this X-ray spectrum with the TeV gamma-ray spectrum leads us to conclude that the TeV gamma-ray emission seems to be powered by either multi-zone Inverse Compton scattering or the decay of neutral pions. The point source resolved by Chandra near the shell is probably associated with CTB 37 B, because of the common hydrogen column density with the diffuse thermal emission. Spectral and temporal characteristics Suggest that this source is a new anomalous X-ray pulsar.