Diffuse Galactic gamma rays, cosmic-ray nucleons and antiprotons

The excess of continuum γ-ray emission from the Galaxy above 1 GeV is an unsolved puzzle. It may indicate that the interstellar nucleon or electron spectra are harder than local direct measurements, as could be the case if a local source of cosmic rays were to dominate the nearby flux. It is however difficult to distinguish between the two cases. Cosmic-ray secondary antiprotons provide a way to resolve this issue. We have made a calculation of the cosmic-ray secondary antiproton spectrum in our model, which computes selfconsistently propagation of primary and secondary nucleons, and electrons. Fragmentation and energy losses are computed using realistic distributions for the interstellar gas and radiation fields, and diffusive reacceleration is also incorporated. Our study shows that accurate measurements of the antiproton flux, especially at high energies, could provide a diagnostic of the interstellar nucleon spectrum allowing us to test the hard nucleon spectrum hypothesis. Present antiproton data above 3 GeV indicate that it can already be excluded at the few σ level.