  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.
