Abstract. We construct realistic maps of the expected neutrino and γ-ray emissions above the TeV originated from the hadronic scattering of cosmic rays (CR) with the interstellar medium (ISM). Differently from previous works, where a uniform CR density was assumed, we estimate the spatial distribution of primary nuclei by means of numerical simulations considering several models of the galactic magnetic field. Assuming that CR sources are supernova remnants (SNR), we use a distribution of those objects as estimated from observations of pulsars and progenitor stars. For the ISM distribution, we adopt most recent data both for the atomic and molecular hydrogen. With respect to previous results, we find the ν and γ-ray emissions to be more peaked along the galactic equator and in the galactic centre which improves significantly the perspectives of a positive detection. We compare our predictions with present experimental upper limits both for the γ-rays and the neutrinos and show that air shower array experiments may soon be able to detect the γ-ray emission from the galactic plane. Finally, we discuss the perspectives that a neutrino telescope of kilometric scale based in the North hemisphere has to measure the diffuse emission from the inner Galaxy. 1
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