2013/08/02 by Fabio Zandanel, P. Colin, Zandanel, Fabio +15
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #Radio Astronomy Observations and Technology
paper · pdf · doi:10.48550/arxiv.1308.0492
openalex publication_date 2013/08/02 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In order to detect the gamma-ray emission from cosmic ray (CR) interactions with the intra-cluster medium, the ground-based imaging Cherenkov telescope MAGIC conducted the deepest-to-date observational campaign targeting a galaxy cluster at very high-energies (> 100 GeV) and observed the Perseus cluster for a total of 85 hr during 2009-2011. The observations constrain the average CR-to-thermal pressure ratio to be 1-2% and the maximum CR acceleration efficiency at structure formation shocks to be <50%. Alternatively, this may argue for non-negligible CR transport processes such as CR streaming and diffusion into the outer cluster regions. Additionally, assuming that the Perseus radio mini-halo is generated by secondaries created in hadronic CR interactions, the central magnetic field is limited to be > 4-9 muG. This range is well below the field strength inferred from Faraday rotation measurements and, therefore, the hadronic model remains a plausible explanation of the Perseus radio mini-halo. Following this successful campaign, MAGIC is continuing collecting data on Perseus.