Abstract
To investigate the star-formation process, we present a multi-wavelength study of a massive star-forming site RAFGL 5085, which has been associated with the molecular outflow, Hii region and near-infrared cluster. The continuum images at 12, 250, 350 and 500 $$\mu $$ m show a central region (having $$M_\textrm{clump}\sim 225$$ $$M_{\odot }$$ ) surrounded by five parsec-scale filaments, revealing a hub-filament system (HFS). In the Herschel column density ( $$N(\textrm{H}_{2})$$ ) map, filaments are identified with higher aspect ratios (length/diameter) and lower $$N(\textrm{H}_{2})$$ values ( $$\sim $$ 0.1– $$2.4 \times 10^{21}$$ cm $$^{-2}$$ ), while the central hub is found with a lower aspect ratio and higher $$N(\textrm{H}_{2})$$ values ( $$\sim $$ 3.5– $$7.0 \times 10^{21}$$ cm $$^{-2}$$ ). The central hub displays a temperature range of [19, 22.5] K in the Herschel temperature map, and is observed with signatures of star formation (including radio continuum emission). The JCMT $$^{13}$$ CO(J $$=$$ 3–2) line data confirm the presence of HFS and its hub is traced with supersonic and non-thermal motions having higher Mach number and lower thermal to non-thermal pressure ratio. In the $$^{13}$$ CO position–velocity diagrams, velocity gradients along the filaments towards the HFS appear to be observed, suggesting the gas flow in the RAFGL 5085 HFS and the applicability of the clump-fed scenario.
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