Speaker
Description
In this paper, we analyze the massive star-forming region W51, located in the Sagittarius arm and considered one of the most active regions in the Galaxy. The region contains six embedded stellar clusters, including one system with two distinct sub-regions of stellar concentration. Our focus is the analysis of these clusters using a model of particle injection at the collective wind termination shock, followed by acceleration through diffusive shock acceleration. The particle transport is described by advection and diffusion processes through the bubbles until the particles escape into the interstellar medium (ISM), allowing us to model both the spatial and energy distribution of the particles and the observed gamma-ray emission. To do this, we applied the model to the clusters in the region, estimating their physical parameters and individual properties, together with an analysis of the HI and H2 gas densities, which allowed us to estimate the total gas column density of the region. The model results were then compared with the gamma-ray observations from the Fermi-LAT , LHAASO, MAGIC, and H.E.S.S experiments. We considered different turbulence scenarios, including Kraichnan and Bohm spectra, with the Bohm scenario providing the best description of the emission at the highest energies. We also produced gamma-ray maps of the region at different energies, allowing for a more robust spatial analysis of the emission. Our results show that the ensemble of clusters in W51 can explain the observed gamma-ray emission from the region.
| CPF | 110.328.079-11 |
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