In the literature, we find that the clump “A" has been explored extensively, and is associated with the previously known signatures of ongoing (massive) SF (see also the sub-mm 850 $\mu$m continuum peak1 in Figure \[fig1\]c). In the direction of the infrared shell, the [*Herschel*]{} column density and temperature maps show the low column density tracing the cleared out region associated with the warm dust emission (T$_{d}$ $\sim$20–26.5 K) or the evolved infrared cluster. Using the WISE 12 $\mu$m image, Figure \[fig2a\]d shows a zoomed-in view of the central part, where the positions of the identified seven CS cores [from @lee11] are also marked. All the CS cores are depicted toward the cold region (T$_{d}$ $\sim$13.5–15 K) traced in the [*Herschel*]{} temperature map. The relatively warmer region (T$_{d}$ $\sim$15–18 K) is seen in the direction of the area, where the noticeable diffuse 8.0 and 12.0 $\mu$m emission is evident (see arrows in Figure \[fig1\]c). It seems that the observed extended temperature structure indicates the distribution of the warm dust emission in the PDRs (see Figure \[fig2a\]c). It implies that the physical environment of AFGL 5157 appears to be affected by the intense energetic feedback of massive stars (i.e., stellar wind, 