Constraining Sources of Ultra High Energy Cosmic Rays Using High Energy Observations with the Fermi Satellite

Abstract

We analyze the conditions that enable acceleration of particles to ultra-high energies, ~10^{20} eV (UHECRs). We show that broad band photon data recently provided by WMAP, ISOCAM, Swift and Fermi satellites, yield constraints on the ability of active galactic nuclei (AGN) to produce UHECRs. The high energy (MeV - GeV) photons are produced by Compton scattering of the emitted low energy photons and the cosmic microwave background or extra-galactic background light. The ratio of the luminosities at high and low photon energies can therefore be used as a probe of the physical conditions in the acceleration site. We find that existing data excludes core regions of nearby radio-loud AGN as possible acceleration sites of UHECR protons. However, we show that giant radio lobes are not excluded. We apply our method to Cen A, and show that acceleration of protons to ~10^{20} eV can only occur at distances >~ 100 kpc from the core.

Extended discussion on former results; Accepted for publication in JCAP

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• A two-component jet model for the tidal disruption event Swift J164449.3+573451
• Fossil shell in 3C 84 as TeV $\gamma$-ray emitter and cosmic-ray accelerator
• Constraints on Physical Conditions for the Acceleration on Ultra-high-energy Cosmic Rays in Nearby Active Galactic Nuclei Observed with the Fermi Large Area Telescope
• X-ray Spectra From Weakly Magnetized Accretion Flows
• Ultra high-energy cosmic rays from beyond the Greisen-Zatsepin-Kuz'min horizon