Speaker
Francois Brun
(CEA Saclay)
Description
The supernova remnant (SNR) W49B is a mixed-morphology remnant interacting with molecular clouds (MC) which originated in a Type Ib/Ic supernova explosion that occurred between one to four thousand years ago. It has one of the highest radio surface brightnesses, and is one of the brightest X-ray SNRs of our Galaxy. Gamma-ray observations of SNR/MC are a powerful tool to constrain the origin of Galactic cosmic rays, as they can probe the acceleration of hadrons through their interaction with the surrounding medium and subsequent emission of high-energy photons.
W49B has been detected in gamma-rays at high energies (0.1-100GeV) and very high energies (> 100 GeV) with the Fermi-LAT and the H.E.S.S. Cherenkov telescopes, respectively. The latest results obtained on W49B with these instruments will be presented. In particular, we will report on the detection of a spectral break at low energies with the Fermi-LAT, similar to that previously found in other SNRs and interpreted as the signature of gamma-ray emission produced through neutral-pion decay. The implications of these results on the particle population and the physical processes leading to the observed gamma-ray emission in W49B will be discussed.
| Registration number following "ICRC2015-I/" | 562 |
|---|---|
| Collaboration | H.E.S.S. |
Primary author
Francois Brun
(CEA Saclay)
Co-authors
Junichiro Katsuta
(Hiroshima University)
Marianne Lemoine-Goumard
(CNRS)
Tobias Jogler
(SLAC)
Vincent Marandon
(MPIK)
