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Abstract The aim of this work is to improve models for the γ-ray discrete or small-scale structure related to H2 interstellar gas. Reliably identifying this contribution is important to disentangle γ-ray point sources from interstellar gas, and to better characterize extended γ-ray signals. Notably, the Fermi–LAT Galactic center (GC) excess, whose origin remains unclear, might be smooth or pointlike.
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