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Fig. 7


Average spectral energy distribution of the γ-ray emissivity per gas nucleon, qSB, found in the atomic gas of the superbubble for an H I spin temperature of 150 K (magenta diamonds, solid lines) and for the optically thin H I case (magenta circles, dashed lines). The blue squares show the average emissivity, qLIS, found in the local ISM for a spin temperature of 140 K (Casandjian 2015). The black line gives the γ-ray emissivity per gas nucleon inferred from the CR spectrum measured in the Solar System (see text).

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