| Abstract : | Massive stars (M > 8M_solar) greatly influence the evolution of their host galaxies through their extreme mechanical and radiative feedback. But their formation mechanisms are not clearly understood. In this regard, the observational study of the young massive stars is important for understanding their mass accumulation processes. Class II 6.7 GHz methanol maser emission (MME) is a reliable proxy for tracing the early stages of massive stars. Hence, we have selected the sites AFGL 5180 and AFGL 6366S, each hosting a Class II 6.7 GHz MME. Dust continuum images reveal the hub-filament system (HFS) toward each site and a filamentary connection (length ~ 3 pc) between them. The hub toward AFGL 5180 harbors several compact VLA 8.46 GHz radio continuum emissions, suggesting the presence of a small cluster of massive stars. The star formation activity (e.g., YSOs, outflows) is evident toward the entire filament, which is more concentrated toward the ends. The 12CO/13CO/C18O molecular line data reveal that MMEs are physically associated with the same filamentary cloud, allowing us to discard the earlier proposed cloud-cloud collision scenario in these sites. The high-resolution (~0".1-0".8) near infra-red (IR) images and ALMA 1.3 mm dust continuum map reveal an IR-bright high mass protostar (mass ~ 8.2M_solar) toward AFGL 5180. Overall, our initial results hint at the connection between HFSs and the end-dominated collapse of the filament at an evolved stage. In this talk, I will discuss these results regarding the mass accumulation processes involved in the early stage of massive star formation. |
