The energy budget and expense of high energy processes in the Universe are uncovered by utilizing the very high energy gamma-ray window. Supernova explosions impart enormous energy into surrounding matter via shock fronts. As a result, matter are accelerated to TeV energies. Compact objects left over after supernova explosions have extremely high magnetic fields and rotation rate. In the case of young pulsars, we see in Figure 5 that a major part of the gspindown energy h available from pulsars is output in the form of gamma-rays.
Active galaxies contain tightly beamed jets, along which matter becomes ultra relativistic.
Enormous spatial densities of energy are expected near compact objects like black holes and neutron stars. Origin of Cosmic Rays Cosmic rays and gamma-rays are linked to the same source via particle interactions. Moreover, the isotropic trajectories of cosmic rays impart a random orientation to their Cherenkov images in the focal plane. Gamma-ray images are aligned to their source. The Chereknov image is parametrized at the focal plane by a multi-pixel array of phototubes.