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.