The gamma-ray and neutrino sky: a consistent picture of Fermi-LAT, H.E.S.S., Milagro, and IceCube results

In this Letter we propose a novel interpretation of the anomalous TeV gamma-ray diffuse emission observed by Milagro in the inner Galactic plane consistent with the signal reported by H.E.S.S. in the Galactic ridge; remarkably, our picture also accounts for a relevant portion of the neutrino flux measured by IceCube. Our scenario is based on a recently proposed phenomenological model characterized by radially-dependent cosmic-ray (CR) transport properties. Designed to reproduce both Fermi-LAT gamma-ray data and local CR observables, this model offers for the first time a self-consistent picture of both the GeV and the TeV sky.We compute the γ-ray and neutrino diffuse emission of the Galaxy on the basis of a recently proposed phenomenological model characterized by radially dependent cosmic-ray (CR) transport properties. We show how this model, designed to reproduce both Fermi-LAT γ-ray data and local CR observables, naturally reproduces the anomalous TeV diffuse emission observed by Milagro in the inner Galactic plane. Above 100 TeV our picture predicts a neutrino flux that is about five (two) times larger than the neutrino flux computed with conventional models in the Galactic Center region (full-sky). Explaining in that way up to ∼25% of the flux measured by IceCube, we reproduce the full-sky IceCube spectrum adding an extra-Galactic component derived from the muonic neutrinos flux in the northern hemisphere. We also present precise predictions for the Galactic plane region where the flux is dominated by the Galactic emission.We compute the gamma-ray and neutrino diffuse emission of the Galaxy on the basis of a recently proposed phenomenological model characterized by radially dependent cosmic-ray (CR) transport properties. We show how this model, designed to reproduce both Fermi-LAT gamma-ray data and local CR observables, naturally reproduces the anomalous TeV diffuse emission observed by Milagro in the inner Galactic plane. Above 100 TeV our picture predicts a neutrino flux that is about five (two) times larger than the neutrino flux computed with conventional models in the Galactic Center region (full-sky). Explaining in that way up to $\sim 25 \%$ of the flux measured by IceCube, we reproduce the full-sky IceCube spectrum adding an extra-Galactic component derived from the muonic neutrino flux in the northern hemisphere. We also present precise predictions for the Galactic plane region where the flux is dominated by the Galactic emission