  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.
