A fundamental problem of cosmic ray (CR) physics is the determination of the average properties of Galactic CRs outside the Solar system. Starting from COS-B data in the 1980s, gamma-ray observations of molecular clouds in the Gould Belt above the Galactic plane have been used to deduce the Galactic CR energy spectrum. We reconsider this problem in view of the improved precision of observational data, which in turn require a more precise treatment of photon production in proton-proton scatterings. We show that the spectral shape $dN/dp\propto p^{-2.85}$ of CR protons as determined by the PAMELA Collaboration in the energy range $80\mathrm{GeV}<p\mathrm{c}<230\mathrm{GeV}$ is consistent with the photon spectra from molecular clouds observed with Fermi-LAT down to photon energies $E\sim 1–2\mathrm{GeV}$. Adding a break of the CR flux at 3 GeV, caused by a corresponding change of the diffusion coefficient, improves further the agreement in the energy range 0.2–3 GeV.

• Received 25 May 2012

DOI:https://doi.org/10.1103/PhysRevD.86.043004