The gamma-ray signal from type IIP core-collapse supernovae

The shock wave resulting from the core-collapse of a massive star can accelerate particles up to PeV energies in the first few days to weeks after the explosion. This can lead to the production of a potentially detectable gamma-ray signal. The gamma-ray flux however is strongly affected by the two photon-annihilation process, where gamma-ray photons interact with photons from the SN photosphere. This process hampers the detection of gamma-rays from core-collapse supernovae at very high energies. In order to probe the detectability of the gamma-rays with current and upcoming gamma-ray facilities, we estimate the gamma-ray flux from typical type IIP core collapse supernovae (CCSNe). These are the most common type of supernovae, and are presumed to arise from red supergiant progenitors. We include a detailed time-dependent calculation of two-photon absorption. Our results will be very useful in creating a strategic observing program to detect CCSNe with the next generation gamma-ray observatory, such as the Cherenkov Telescope Array (CTA).