Studies of supernovae and their remnants based on gamma-ray observations with H.E.S.S.

Cosmic rays (CRs) are particles coming from space that constantly bombard Earth. Their origin remains partly unknown. As CRs are charged particles and are deflected by interstellar magnetic fields, they cannot trace back their sources. Instead, neutral messengers are used, such as gamma-rays produced by CRs in the acceleration sites. Supernova remnants (SNRs) are known sources of CRs, and are believed to be responsible for the bulk of the Galactic CRs. However, they can only account for CRs with energies below 100 TeV.
We describe here analyses of gamma-ray observations with the H.E.S.S. telescope, with the aim to study the gamma-ray emission of SNRs and their ability to be powerful CRs accelerators.
We report and interpret the detection at TeV energies of the ~2500 yr old SNR N132D and the historical Kepler’s SNR (the remnant of SN1604).
In addition, we searched for gamma-ray emission from supernovae (SNe), i.e. the earliest stages of SNR evolution. We analyzed data towards nine objects serendipitously observed with H.E.S.S. and from two nearby SNe with dedicated observations. No significant excess was observed for any of these SNe, and upper limits (ULs) on the flux are derived, leading to constraints on the SN environments. Finally, we searched for a signal at the edge of the Fermi Bubbles at large Galactic latitude. No significant signal was found, and ULs on the Fermi Bubbles flux were obtained and discussed in regards to systematic errors and along with predictions for further observations.