@nakamura12; @nakamura14; @henshaw13; @fukui14; @dewangan17; @dewangan19a; @dewangan19]. In the hydrodynamical simulations of the collision process, massive clumps and cores are produced at the junction of two filamentary molecular clouds or the shock-compressed interface layer [e.g., @habe92; @anathpindika10; @inoue13; @haworth15a; @haworth15b; @torii17; @balfour17; @bisbas17 and references therein], where massive stars can be formed. However, the observational confirmation of such physical process or a colliding event is a very difficult task, and can be investigated via the knowledge of molecular gas motion toward the filaments and the zones of interacting/colliding filaments.

Situated at a distance of 1.8 kpc [@snell88; @torrelles92a], AFGL 5157/IRAS 05345+3157 is an active site of SF, which is also known as NGC 1985 or Mol 11. In the direction of IRAS 05345+3157, an extended shell detected in H$_{2}$ was reported, which was found to surround a cluster of infrared sources centered on the IRAS position [@chen99; @chen03; @reipurth08; @varricatt10; @wolf17]. @chen99 suggested the presumptive age of this infrared cluster to be 10$^{6}$ yr, which was referred to as an evolved cluster in AFGL 5157 [see also @chen03]. These authors suggested that massive stars located in this evolved cluster can be responsible for the H$_{2}$ shell through their UV fluorescence. 