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Fig. 4


SED of three GMCs, R CrA a), Orion B b) and Perseus OB2 c) as measured by LAT (points). For comparison, the expected γ-ray flux produced via pp interactions assuming that the CR spectrum inside the clouds is identical to the local one measured by PAMELA (red dashed lines) is also shown. The black solid curves represent the γ-ray fluxes calculated for a spectrum of CR protons which at high energies coincides with the PAMELA measurements, but towards low energies, down to 1 GeV, continues as a power-law with an index 2.85.

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