Correlation of gas dynamics and dust in the evolved filament
  G82.65-02.00
  The combination of line and continuum observations can provide vital insights
to the formation and fragmentation of filaments and the initial conditions for
star formation. We have carried out line observations to map the kinematics of
an evolved, actively star forming filament G82.65-2.00. The filament was first
The combination of line and continuum observations can provide vital insights
to the formation and fragmentation of filaments and the initial conditions for
star formation. We have carried out line observations to map the kinematics of
an evolved, actively star forming filament G82.65-2.00. The filament was first
identified from the Planck data as a region of particularly cold dust emission
and was mapped at 100-500 $\mu$m as a part of Herschel key program Galactic
Cold Cores.
  The observations reveal several velocity components in the field, with
strongest line emission concentrated to velocity range $\sim [3,5]$ km $\rm
s^{-1}$. The column density of molecular hydrogen along the filament varies
from 1.0 to 2.3 $\times 10^{22}$ $\rm cm^{2}$. We have examined six cold clumps
from the central part of the filament. The clumps have masses in the range $10
- 20$ $M_{\odot}$ ($\sim70M_{\odot}$ in total) and are close to or above the
virial mass. Furthermore, the main filament is heavily fragmented and most of
the the substructures have a mass lower than or close to the virial mass,
suggesting that the filament is dispersing as a whole. Position-velocity maps
of $\rm ^{12}CO$ and $\rm ^{13}CO$ lines indicate that at least one of the
striations is kinematically connected to two of the clumps, potentially
indicating mass accretion from the striation onto the main filament. We
tentatively estimate the accretion rate to be $\dot{M}$ = $2.23 \times 10^{-6}$
$ M_{\odot} / \rm year$.
