The recent discovery of the γ -ray emission from the lobes of the closest radio galaxy Centaurus A by Fermi implies the presence of high-energy electrons at least up to γ ∼ 10^5–10^6. These high-energy electrons are required to interpret the observed γ -ray radiation in terms of inverse Compton emission off the cosmic microwave background (IC/CMB), the widely accepted scenario to describe the X-ray emission of radio galaxy lobes. In this Letter, we consider the giant radio lobes of FR II radio galaxies showing that it is possible to maintain electrons at energies γ ∼ 10^5–10^6, assuming an acceleration scenario (driven by turbulent magnetic fields) that compensates radiative losses. In addition, we consider the contribution to the diffuse extragalactic γ -ray background due to the IC/CMB emission of FR IIs’ lobes, showing its relevance in the keV to MeV energy range.
Fueling Lobes of Radio Galaxies: Statistical Particle Acceleration and the Extragalactic γ-ray Background
MASSARO, Francesco;
2011-01-01
Abstract
The recent discovery of the γ -ray emission from the lobes of the closest radio galaxy Centaurus A by Fermi implies the presence of high-energy electrons at least up to γ ∼ 10^5–10^6. These high-energy electrons are required to interpret the observed γ -ray radiation in terms of inverse Compton emission off the cosmic microwave background (IC/CMB), the widely accepted scenario to describe the X-ray emission of radio galaxy lobes. In this Letter, we consider the giant radio lobes of FR II radio galaxies showing that it is possible to maintain electrons at energies γ ∼ 10^5–10^6, assuming an acceleration scenario (driven by turbulent magnetic fields) that compensates radiative losses. In addition, we consider the contribution to the diffuse extragalactic γ -ray background due to the IC/CMB emission of FR IIs’ lobes, showing its relevance in the keV to MeV energy range.
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