the infrared shell (see arrows in Figure \[fig1\]d). One can also note that the sub-mm 850 $\mu$m continuum peaks (i.e., peak1, peak2, and peak3) are also found toward the IRDCs (see Figures \[fig1\]a and \[fig1\]c).

Figure \[fig1\]e displays the inverted gray-scale IPHAS H$\alpha$ image. The locations of the infrared shell, the H[ii]{} region, and IRAS 05345+3157 are also indicated in Figure \[fig1\]e. The diffuse H$\alpha$ emission is known as a tracer of the ionized emission, which is distributed within the infrared shell powered by massive stars located in the evolved infrared cluster [e.g., @chen03]. In Figure \[fig1\]f, we display the [*Spitzer*]{} ratio map of 4.5 $\mu$m/3.6 $\mu$m emission, indicating the presence of bright and black regions. More information on the procedures for obtaining the [*Spitzer*]{} ratio map can be found in @dewangan17. The positions of previously reported Molecular Hydrogen emission-line Objects [MHOs; from @wolf17] are also shown in the figure (see hexagons in Figure \[fig1\]f). In the ratio map, the bright regions show the excess of 4.5 $\mu$m emission, and are not associated with the diffuse H$\alpha$ emission. On the other hand, the domination of 3.6 $\mu$m emission is inferred though the black or dark gray regions seen in the 