Radio and X-ray emission from core-collapse supernovae

Core-collapse supernovae mark the death of stars more massive than approximately 8 M_solar. The presupernova evolution depends on the initial mass and metallicity of the star. Depending on the initial conditions, the star may end up as supernova of type II, IIb, IIP, Ib,or Ic. Radiation & winds of progenitors modifies the circumstellar matter of the explosion. I will present a study which is underway to understand the radio and x-ray emission from these explosions. Progenitors can be understood by studying their evolution using stellar evolution codes. A characterization of the emission will lead to a better understanding of the supernovae progenitors, and put constraints on their presupernova evolution.
The x-ray emission from young type Ib/IC events is also studied to find the thermal/IC component in X-ray bands and distinguish between the various modes of X-ray production in young supernovae. Charged particles are accelerated to relativistic energies by the shock waves generated by these explosions. These relativistic particles are responsible for bulk of radio emission from young star forming galaxies. We have detected radio emission from green peas galaxies, which have low stellar mass, low metallicity, and very high star formation.