of M$_{clump}$ and R$_{clump}$. The calculations assume that each clump has a spherical geometry. The values of $n_{\mathrm H_2}$ for all the clumps are found between 2200 and 5500 cm$^{-3}$. In the direction of the elongated filamentary feature, several clumps are found (see IDs 8–22 in Figure \[fig2\]c and also Table \[tab1\]). Among these clumps, seven clumps (e.g., 13, 15, 16, 17, 19, 21, and 22) have masses more or equal to 30 M$_{\odot}$, which are also small scale clumps except the clump ID 16. The clump ID 16 is located toward the central part of the filamentary feature (see also Figure \[fig2a\]a). Additionally, the sub-mm emission toward the clump 13 is prominently seen in the [*Herschel*]{} images.

Using the [*Herschel*]{} column density contour map, a zoomed-in view of the central part of the filamentary feature is presented in Figure \[fig2a\]a. As pointed out above, the [*Herschel*]{} column density map shows no emission toward the region, where the diffuse H$\alpha$ emission (or infrared shell) is observed. However, in the direction of clump ID 16, we do not find any column density deficient region due to the choice of a lower column density threshold in the [*clumpfind*]{}. Hence, in Figure \[fig2a\]a, 