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 $\times {10}^{22}$ $\mathrm{c}{\mathrm{m}}^2$. We have examined six cold clumps from the central part of the filament. The clumps have masses in the range $10

• 20$ $M_{\odot }$ ($\sim 70M_{\odot }$ 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 ${}^{12}\mathrm{C}\mathrm{O}$ and ${}^{13}\mathrm{C}\mathrm{O}$ 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 $\dot{M}$ = $2.23\times {10}^{-6}$ $M_{\odot }\mathrm{/}\mathrm{y}\mathrm{e}\mathrm{a}\mathrm{r}$.