by @lee11, were within the ammonia filaments. Based on the observed results toward the dense NH$_{3}$ core and the H$_{2}$ shell, at least two distinct epochs of SF were reported in AFGL 5157 [e.g., @wolf17]. The evolved SF phase has been reported toward the infrared cluster or the H$_{2}$ shell, while the younger phase of SF (timescale $\sim$10$^{4}$–10$^{5}$ yr) is thought to be associated with the dense NH$_{3}$ core [see also Figure 3 in @chen03]. It was also argued that the evolved infrared cluster might have triggered the younger phase of SF associated with the dense NH$_{3}$ core and northwest areas [@chen03]. Note that all the earlier works were mainly focused to an area of $\sim$1.8 pc $\times$ $\sim$1.8 pc containing AFGL 5157.

The study of the physical environment at large-scale ($>$ 10 pc) is not yet reported in AFGL 5157. We do not find any study for examining embedded filaments, young stellar objects (YSOs), and the velocity structure of molecular gas on a wide-scale around AFGL 5157. Our present paper focuses on understanding the exact SF mechanisms occurring in AFGL 5157. In this context, a multi-wavelength approach has been adopted in this paper. A detailed analysis of $^{12}$CO(1-0) and 