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A few radio galaxies have been discovered to emit GeV-TeV gamma-ray emissionin spite of relatively large viewing angles of their jets. We consider ascenario in which such large angle gamma-ray emission is preferentiallyproduced by isotropically distributed relativistic electrons in the kpc scalejet. These electrons comptonize soft, non-thermal radiation from the inner jetwhich is beamed due to its relativistic motion. In terms of such a model, weinterpret recently discovered TeV gamma-ray emission from the kpc scale jets inCen~A. Interestingly, due to the geometry of the inverse Compton scatteringprocess, intensity of the gamma-ray emission from the counter-jet is predictedto be on a higher level than the emission from the jet. This is true providedthat both, a jet and a counter-jet, are twins, i.e. the physical processes inthe jet and counter-jet result in the acceleration of particles in a similarway. However, in general, the jet and counter-jet can differ significantly.Therefore, their relative contribution to the gamma-ray emission from the jetsin Cen~A can become more complicated. Investigation of the distribution of theTeV gamma-ray emission along jets of nearby radio galaxies with the nextgeneration telescopes should provide constraints on the considered model andthe content of the kpc-scale jets.

GeV-TeV gamma-rays produced by electrons in the kpc scale jet as a result of comptonization of the inner jet emission