  Hub-filament systems (HFSs) being the potential sites of formation of star
clusters and high mass stars, provide a test bed for the current theories that
attempt to explain star formation globally. It is thus important to study a
large number of HFSs using both intensity and velocity information to constrain
these objects better observationally. We present here a study of the
hub-filament system associated with G6.55-0.1 using newly obtained observations
of radio continuum and $J$=2--1 transition of CO, $^{13}$CO, and C$^{18}$O. The
radio continuum maps show multiple peaks that coincide with far-infrared dust
continuum peaks indicating the presence of more than one young massive stars in
the hub of the HFS. We used the velocity information from the C$^{18}$O(2--1)
map to (a) show that the source G6.55-0.1 is not physically associated with the
SNR W28 and (b) disentangle and identify the velocity components genuinely
associated with G6.55-0.1. Among the velocity-coherent structures identified,
the two filaments at 13.8 and 17.3 km s$^{-1}$ contribute a total mass
accretion rate of $\sim$3000 M$_{\odot}$ Myr$^{-1}$ to the hub. Both the
filaments also show V-shaped structure, characteristic of gravitational
collapse, in their velocity profile at the location of the hub. Estimated mass
per unit length of the segments of the filaments are smaller than the critical
line masses derived from virial equilibrium considerations. This suggests that
while the filaments are not gravitationally collapsing as a whole, the spectra
from the hub indicate that the inner parts are dynamically decoupled and
collapsing to form stars.
