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The Fermi-LAT data accumulated over 7 years of {\gamma}-ray observations,together with the high resolution gas (CO & HI) and the dust opacity maps, areused to study the emissivity of {\gamma}-rays induced by interactions of cosmicrays (CRs) with the interstellar medium. Based on the dust opacity templates,the {\gamma}-ray emissivity was measured for 36 segments of the Galactic plane.Furthermore, the {\gamma}-ray emissivity was evaluated in six Galactocentricrings. Both the absolute emissivity and the energy spectra of {\gamma}-raysderived in the interval 0.2-100 GeV show significant variations along thegalactic plane. The density of CRs, derived under the assumption that{\gamma}-rays are predominately produced in CR interactions with theinterstellar gas, is characterised by a strong radial dependence. In the innerGalaxy the CR density substantially exceeds the density in the outer parts ofthe Galaxy: by a factor of a few at 10 GeV, and by more than an order ofmagnitude at 1 TeV. Remarkably, the energy distribution of CRs appears to besubstantially harder than the energy spectrum obtained from direct measurementsof local CRs. At the same time, the flux and the energy spectrum of multi-GeVprotons derived from {\gamma}-ray data in the outskirts of the Galaxy is quiteclose to the measurements of local CRs.

Radial distribution of the diffuse gamma-ray emissivity in the galactic disk