SIMBAD references

A few radio galaxies have been discovered to emit GeV-TeV γ-ray emission in spite of the relatively large viewing angles of their jets. We consider a scenario in which such large-angle γ-ray emission is preferentially produced by isotropically distributed relativistic electrons in the kpc-scale jet. These electrons Comptonize soft non-thermal radiation from the inner jet, which is beamed due to its relativistic motion. In terms of such a model, we interpret the recently discovered TeV γ-ray emission from the kpc-scale jets in Centaurus A (Cen A). Interestingly, due to the geometry of the inverse Compton scattering process, the intensity of the γ-ray emission from the counter-jet is predicted to be on a higher level than the emission from the jet. This is true provided that both the jet and the counter-jet are twins, i.e. the physical processes in the jet and counter-jet result in the acceleration of particles in a similar way. However, in general, the jet and counter-jet can differ significantly. Therefore, their relative contribution to the γ-ray emission from the jets in Cen A can become more complicated. Investigation of the distribution of the TeV γ-ray emission along jets of nearby radio galaxies with next-generation telescopes should provide constraints on the considered model and the content of the kpc-scale jets.