Electron acceleration and advection model for the high energy emission from the large scale jet of AGNs

The detection of hard X-ray emission from the kilo-parsec scale jet of active galactic nuclei cannot be interpreted as the synchrotron emission mechanism from the electron distri- bution responsible for the radio/optical emission. The X-ray emission when interpreted as the inverse-Compton scattering of cosmic microwave background photons (IC/CMB process), the Compton spectral component will peak at GeV energy. The non-detection of significant gamma-ray flux from these large-scale jets by Fermi disfavoured this model, particularly at low redshifts. Alternately, synchrotron emission from a different electron population is suggested. However, the X-ray emissions from the jet of AGN at high red- shift are usually interpreted as IC/CMB process, due to the increase in cosmic microwave background (CMB) photon density. But, recent Fermi 𝛾-ray flux upper limit estimates on jet emission from the high redshift source J1510+5702 questions the validity of the IC/CMB model. In this work, we consider a model where the multi-spectral component (MSC) emissions from the large-scale jets of AGN is explained using accelerated and advected electron distributions 1. The synchrotron emission from these two electron distribution is capable of interpreting the MSC jet emission from the jet of J1510+5702.