(i.e., 2.8), $Area_{pix}$ is the area subtended by one pixel (i.e., 6$''$/pixel), and $\Sigma N(\mathrm H_2)$ is the total column density [see also @dewangan17]. The other two filaments show a temperature range of about 13–13.5 K, and seem to be directed toward the central part of the filamentary feature. The locations of the infrared shell and the IRDCs are located within the central part of the filamentary feature, which is indicated in the [*Herschel*]{} maps. One can note that a column density deficient region is found in the direction of the infrared shell (see Figure \[fig2\]b and also Figure \[fig2a\]a). The central part of the filamentary feature is traced using a column density contour with the level of $\sim$9–11 $\times$ 10$^{21}$ cm$^{-2}$, where the maximum value of the column density is estimated to be $\sim$3.7 $\times$ 10$^{23}$ cm$^{-2}$. Earlier, @krumholz08 reported a threshold value of 1 gm cm$^{-2}$ (or corresponding column density $\sim$3 $\times$ 10$^{23}$ cm$^{-2}$) for formation of massive stars. Hence, it is likely that massive stars can be formed within the central part of the filamentary feature. Interestingly, @lee11 suggested the presence of massive protostar candidates toward the dense cores. The [*Herschel*]{} temperature map shows an extended temperature 