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NGC 1068 is a nearby widely studied Seyfert II galaxy presenting radio,infrared, X- and $\gamma$-ray emission as well as strong evidence forhigh-energy neutrino emission. Recently, the evidence for neutrino emissioncould be explained in a multimessenger model in which the neutrinos originatefrom the corona of the active galactic nucleus (AGN). In this environment$\gamma$-rays are strongly absorbed, so that an additional contribution frome.g. the circumnuclear starburst ring is necessary. In this work, we discusswhether the radio jet can be an alternative source of the $\gamma$-rays betweenabout $0.1$ and $100$ GeV as observed by Fermi-LAT. In particular, we includeboth leptonic and hadronic processes, i.e. accounting for inverse Comptonemission and signatures from $pp$ as well as $p\gamma$ interactions. In orderto constrain our calculations, we use VLBA and ALMA observations of the radioknot structures, which are spatially resolved at different distances from thesupermassive black hole. Our results show that the best leptonic scenario forthe prediction of the Fermi-LAT data is provided by the radio knot closest tothe central engine. For that a magnetic field strength $\sim 1\,\text{mG}$ isneeded as well as a strong spectral softening of the relativistic electrondistribution at $(1-10)\,\text{GeV}$. However, we show that neither such a weakmagnetic field strength nor such a strong softening is expected for that knot.A possible explanation for the $\sim$ 10 GeV $\gamma$-rays can be provided byhadronic pion production in case of a gas density $\gtrsim10^4\,\text{cm}^{-3}$. Nonetheless, this process cannot contributesignificantly to the low energy end of the Fermi-LAT range. We conclude thatthe emission sites in the jet are not able to explain the $\gamma$-rays in thewhole Fermi-LAT energy band.

On the possible jet contribution to the ${\gamma}$-ray luminosity in NGC 1068