http://arxiv.org/abs/2210.04658
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${\rm clump}$ $\sim$225 M${\odot}$) surrounded by five parsec-scale filaments, revealing a hub-filament system (HFS). In the {\it Herschel} column density ($N({{\rm{H}}}{2})$) map, filaments are identified with higher aspect ratios (length/diameter) and lower $N({{\rm{H}}}{2})$ values ($\sim$0.1–2.4 $\times$10$^{21}$ cm$^{-2}$), while the central hub is found with a lower aspect ratio and higher $N({{\rm{H}}}_{2})$ 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 {\it 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 the 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 toward the HFS appear to be observed, suggesting the gas flow in the RAFGL 5085 HFS and the applicability of the clump-fed scenario.
L. Dewangan, N. Bhadari, A. Maity, et. al.
Tue, 11 Oct 22
50/92
Comments: 15 pages, 8 figures; Accepted for publication in Journal of Astrophysics and Astronomy (JOAA)
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