found to host the embedded filaments (i.e., fs1 and fs2) and several H[ii]{} regions. The filaments are not associated with any radio continuum emission, and exhibit T$_\mathrm{d}$ of $\sim$17–19 K. In our selected system, a relatively warm dust emission (T$_\mathrm{d}$ $\sim$ 21–29 K) is also found toward the H[ii]{} regions excited by OB-type stars (see Table \[tab2\]). These results together show the existence of two distinct environments in the selected physical system, which differ substantially in their dust temperatures (see Section \[sec:hermap\]). The elongated filament (“fs1"; length $\sim$17 pc; T$_\mathrm{d}$ $\sim$19 K) is characterized as a thermally supercritical filament, and appears to be on the verge of collapse (see Section \[sec:hermap\]). Based on the distribution of Class I YSOs [mean age $\sim$0.44 Myr; @evans09], the early phase of SF activities is investigated toward the filaments and the H[ii]{} regions (age $\sim$0.35 – 1.0 Myr) in the system (see Section \[sec:sf\]).

Star Formation Scenarios
------------------------

Considering the presence of multiple velocity components and massive O-type stars, one can explore the applicability of the triggered SF scenarios concerning the expansion of H[ii]{} regions [e.g., @elmegreen77; @bertoldi89; @whitworth94; @lefloch94; @elmegreen98; @deharveng05; @dale07; @bisbas15; @walch15; @kim18; @haid19] and the colliding/converging flows from two velocity 