2024MNRAS.532.2006W

We analyse the GeV γ-ray emission from the W3 complex using about 14 years of Pass 8 data recorded by the Fermi Large Area Telescope (Fermi-LAT). We resolve the γ-ray emissions around W3 into two components: an elliptical Gaussian overlapping with the molecular gas and a point-like source near the cluster W3 Main. The pion-bump feature of SED for the elliptical Gaussian together with the better fitting result of pion decay model favour the hadronic origin. We further argue that the cosmic rays (CRs) could originate from the interactions between cluster winds and the shock produced by the SNR HB3. The point-like source positionally coincident with the star cluster W3 Main indicates it may be directly powered by near clusters, while its fainter γ-ray emissions below 10 GeV are possibly due to the shelter from dense gas making the low-energy CRs incapable of penetrating the dense materials. Meanwhile, we cannot rule out that the γ-ray emissions originate from the interaction of accelerated protons in SNR with the ambient gas.