we have further employed the [*clumpfind*]{} using higher column density contour levels (i.e., (9, 11, 13, 15, 19, 23, 30, 40, 50, 60) $\times$ 10$^{21}$ cm$^{-2}$). A total of five clumps are identified toward the central part of the filamentary feature (or the clump ID 16), and are labeled as A, B, C, D, and E in the figure. The positions of these clumps are marked in Figure \[fig2a\]b, and their boundaries are also indicated in the figure. In Figure \[fig2a\]b, one can also clearly see the column density deficient region toward the diffuse H$\alpha$ emission (or infrared shell). Table \[tab1\] also lists the values of M$_{clump}$, R$_{clump}$, and $n_{\mathrm H_2}$ of these five clumps. The clump masses vary between 45 M$_{\odot}$ and 300 M$_{\odot}$. The values of $n_{\mathrm H_2}$ are obtained between $\sim$1.3 $\times$ 10$^{4}$ and $\sim$5.5 $\times$ 10$^{4}$ cm$^{-3}$. These dense and massive clumps (i.e., “A"–“E") are distributed toward the IRDCs.

Using the [*Herschel*]{} temperature map, a zoomed-in view of the central part of the filamentary feature is also shown in Figure \[fig2a\]c. The cold region (T$_{d}$ $\sim$13.5–15 K) is associated with the massive clump “A", and is surrounded by a relatively warm dust emission (T$_{d}$ $\sim$15–18 K). 