the surface density contours of the selected YSOs [see @casertano85; @gutermuth09; @bressert10; @dewangan17 for more details]. Adopting the similar analysis as carried out in @dewangan17, the surface density map of all the selected YSOs has been produced using a 5$\arcsec$ grid and 6 NN at a distance of 1.8 kpc. The surface density contours with the levels of 30, 40, 60, and 85 YSOs/pc$^{2}$ are shown in Figures \[fig11\]b, \[fig11\]c, and \[fig11\]d. In Figure \[fig11\]b, we have also marked the positions of the identified seven CS cores [from @lee11]. Using the continuum map at 2.7 mm and the CS line data, @lee11 also reported that massive protostar candidates are forming in two of these dense cores. In Figures \[fig11\]c and \[fig11\]d, the surface density contours are overlaid on the [*Herschel*]{} column density and temperature maps, respectively. Figure \[fig11\]d reveals a spatial correlation between the embedded clusters (with surface density $\geq$ 30 YSOs/pc$^{2}$) and the higher column density materials (including [*Herschel*]{} clumps and dense CS cores).

Together, the central part of the filamentary feature is associated with massive dust clumps, dense CS cores, massive protostar candidates, and clusters of YSOs.

Kinematics of molecular gas {#sec:coem}
---------------------------

To study the molecular gas 