Observation of supernova remnants with the CAT Cherenkov imaging telescope
G. Mohanty, L.-M. Chounet, B. Degrange, P. Fleury, G. Fontaine, L. Iacoucci, F. Piron
R. Bazer-Bachi, J.-P. Dezalay, I. Malet, A. Musquere, J.-F. Olive
G. Debiais, B. Fabre, E. Nuss
X. Moreau, K. Ragan, C. Renault, M. Rivoal, K. Schahmaneche, J.-P. Tavernet
A. Djannati-Ataï , P. Espigat, M. Punch
P. Goret, C. Gouiffes, I. A. Grenier
Supernova remnants (SNR) can be broadly classified into two types:
plerionic or plasma-filled SNR, like the Crab Nebula, and shell-type SNR,
like Cassiopeia A (Cas A), where the emission is concentrated rather in a
shell-like region, believed to be the shock front where the supernova
expansion impinges on surrounding material. For plerions, the high-energy
gamma-ray emission is generally interpreted in terms of a synchrotron
self-Compton (SSC) model (de Jager et al). The observed non-thermal X-ray
emission from Cas A strongly indicates the presence of TeV electrons which
can produce high-energy gamma rays by bremsstrahlung. The inverse Compton
scattering of these gamma rays can further give rise to Very High Energy (VHE)
radiation, which can be further supplemented at the highest energies by
gamma-rays arising from the decay of p0's created in nucleonic
interactions of an associated high-energy cosmic-ray component (Baring et al,
Ellison et al).
VHE observations of the Crab Nebula and Cas A, made with the CAT
atmospheric Cherenkov imaging telescope are used to constrain models for
production of gamma rays in SNR. For both plerionic and
shell-type SNR, these observations serve primarily to impose a limit on the
magnetic field in the region where the particles are accelerated.
File translated from TEX by TTH, version 2.32.
On 16 Jul 1999, 09:19.