  In this contribution we will discuss recent results concerning the intensity
and the angular distribution of the gamma-ray and neutrino emissions as should
be originated from the hadronic scattering of cosmic rays (CR) with the
interstellar medium (ISM). We assumed that CR sources are supernova remnants
(SNR) and estimated the spatial distribution of primary nuclei by solving
numerically the diffusion equation. For the ISM, we considered recent models
for the 3D spatial distributions of molecular hydrogen. Respect to previous
results, we find the secondary gamma-ray and neutrino 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 the experimental limits/observations by MILAGRO and TIBET (for
the gamma-rays) and by AMANDA-II (for the neutrinos) and discuss the detection
perspectives for a km3 neutrino telescope to be built in the North hemisphere.
