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The High Energy Stereoscopic System (HESS), the Major Atmospheric Gamma-rayImaging Cherenkov Telescope (MAGIC), and the Very Energetic Radiation ImagingTelescope Array System (VERITAS) have observed diffuse gamma-ray emissionstrongly correlated with the central molecular zone in the Galactic center. Themost accepted scenario to generate this emission is via a hadronic interactionbetween cosmic rays (CRs) and ambient gas, where CRs are accelerated from acentral and continuous source of 1 PeV protons (PeVatron). We explore theinfluence of the three-dimensional (3D) shape of the central molecular zone onthe indirect observation of the CR energy density via gamma-ray detection. Wesimulated synthetic gamma-ray maps using a CR diffusion model with sphericalinjection, one isotropic diffusion coefficient, no advection, andmono-energetic particles of 1 PeV. Also, we used two different 3D gasdistributions considering the observed gas column density, both with andwithout an inner cavity. We find that when using a persistent CR source, adisk-like gas distribution is needed to reproduce the existing CR indirectobservations. This is in agreement with the continuous gas distribution impliedby some dynamical models and studies based on the comparison of emission andabsorption molecular lines. However, it contradicts several models of thecentral molecular zone, which imply that this structure has a significant innercavity. This tension can be reconciled by an additional, impulsive CRinjection. If the central molecular zone has a cavity, a composite CRpopulation, coming from the stellar winds of the Wolf-Rayet stars in thecentral 0.5 pc and the supernova Sgr A East, produces a good match to theobserved gamma-ray morphology in the Galactic center.

Galactic center gamma-ray production by cosmic rays from stellar winds and Sgr A East