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Radio and $\gamma$-ray measurements of large lobes of several radio galaxiesprovide adequate basis for determining whether emission in these widelyseparated spectral regions is largely by energetic electrons. This is very muchof interest as there is of yet no unequivocal evidence for a significantenergetic proton component to account for $\gamma$-ray emission by neutral piondecay. A quantitative assessment of the proton spectral distributionnecessitates full accounting of the local and background radiation fields inthe lobes; indeed, doing so in our recent analysis of the spectral energydistribution of the Fornax A lobes considerably weakened previous conclusionson the hadronic origin of the emission measured by the Fermi satellite. Wepresent the results of similar analyses of the measured radio, X-ray and$\gamma$-ray emission from the lobes of Centaurus A, Centaurus B, and NGC 6251.The results indicate that the measured $\gamma$-ray emission from these lobescan be accounted for by Compton scattering of the radio-emitting electrons offthe superposed radiation fields in the lobes; consequently, we set upper boundson the energetic proton contents of the lobes.

Non-thermal emission in radio galaxy lobes: II. Centaurus A, Centaurus B, and NGC 6251