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IceCube has recently reported the detection of $\sim 1-10 \,{\rm TeV}$neutrinos from the nearby active galaxy, NGC 1068. The lack of TeV-scaleemission from this source suggests that these neutrinos are generated in thedense corona that surrounds NGC 1068's supermassive black hole. In this paper,we present a physical model for this source, including the processes of pairproduction, pion production, synchrotron, and inverse Compton scattering. Wehave also performed a new analysis of Fermi-LAT data from the direction of NGC1068, finding that the gamma-ray emission from this source is very soft butbright at energies below $\sim 1 \, {\rm GeV}$. Our model can predict agamma-ray spectrum that is consistent with Fermi-LAT observations, but only ifthe magnetic field within the corona of this active galactic nucleus (AGN) isquite high, namely $B\gtrsim 6 \, {\rm kG}$. To explain the observed neutrinoemission, this source must accelerate protons with a total power that iscomparable to its intrinsic X-ray luminosity. In this context, we consider twoadditional nearby active galaxies, NGC 4151 and NGC 3079, which have beenidentified as promising targets for IceCube.

On the Neutrino and Gamma-Ray Emission from NGC 1068