HESS observed an extended gamma-ray emission correlated with the morphology of the central molecular zone in the Galactic center. The most accepted scenario to generate this emission is via a hadronic interaction between cosmic rays and ambient gas. In this work, we explore the influence of the 3-D shape of the central molecular zone on the indirect observation of the cosmic rays and verify if more realistic cosmicray dynamics for the Galactic center environment are consistent with current gammaray observations. We found that using a proton source consistent with particles accelerated in the persistent Wolf-Rayet wind collision in the central 0.5 pc and a simplified cosmic-ray diffusion, a disk-like gas distribution is needed to reproduce the existing gamma-ray observations. However, it contradicts several models of the central molecular zone, which imply that this structure has a significant inner cavity. This tension can be reconciled by an additional impulsive cosmic-ray injection from SN Sgr A East. Additionally, in order to reproduce the existing observations adopting more realistic cosmic-ray dynamics, a ring-like gas distribution and cosmic-ray acceleration from the Arches, Quintuplet, and Nuclear clusters, plus SN Sgr A East are required.
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