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The combination of line and continuum observations can provide vital insightsto the formation and fragmentation of filaments and the initial conditions forstar formation. We have carried out line observations to map the kinematics ofan evolved, actively star forming filament G82.65-2.00. The filament was firstThe combination of line and continuum observations can provide vital insightsto the formation and fragmentation of filaments and the initial conditions forstar formation. We have carried out line observations to map the kinematics ofan evolved, actively star forming filament G82.65-2.00. The filament was firstidentified from the Planck data as a region of particularly cold dust emissionand was mapped at 100-500 $\mu$m as a part of Herschel key program GalacticCold Cores.  The observations reveal several velocity components in the field, withstrongest line emission concentrated to velocity range $\sim [3,5]$ km $\rms^{-1}$. The column density of molecular hydrogen along the filament variesfrom 1.0 to 2.3 $\times 10^{22}$ $\rm cm^{2}$. We have examined six cold clumpsfrom 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 thevirial mass. Furthermore, the main filament is heavily fragmented and most ofthe the substructures have a mass lower than or close to the virial mass,suggesting that the filament is dispersing as a whole. Position-velocity mapsof $\rm ^{12}CO$ and $\rm ^{13}CO$ lines indicate that at least one of thestriations is kinematically connected to two of the clumps, potentiallyindicating mass accretion from the striation onto the main filament. Wetentatively estimate the accretion rate to be $\dot{M}$ = $2.23 \times 10^{-6}$$ M_{\odot} / \rm year$.

Correlation of gas dynamics and dust in the evolved filament G82.65-02.00