similar procedures as reported in @dewangan17, we produce the surface density map of all the selected Class I YSOs using a 15$''$ grid and 6 NN at a distance of 2.6 kpc.

Kinematics of molecular gas {#sec:coem}
---------------------------

In Figure \[fig4\]a, we display the positions of 88 ATLASGAL clumps (having d $\sim$2.6 kpc and V$_\mathrm{lsr}$ range $\sim$\[30, 56\] km s$^{-1}$). Figure \[fig4\]b presents the distribution of V$_\mathrm{lsr}$ of 88 clumps against the Galactic longitude. In the direction of [*l*]{} = 13$\degr$.08–13$\degr$.4, this plot suggests the presence of at least two clouds (at \[30, 41\] km s$^{-1}$ (or around 35 km s$^{-1}$) and \[48, 56\] km s$^{-1}$ (or around 53 km s$^{-1}$)) containing the dust clumps. Furthermore, we also find two clumps with V$_{lsr}$ of $\sim$45 km s$^{-1}$ toward [*l*]{} $\approx$ 13$\degr$.1. A majority of the ATLASGAL dust clumps are associated with the gas at \[30, 41\] km s$^{-1}$. In the direction of our selected system, our analysis of the clumps indicates the presence of at least three velocity components. Previously, three cloud components at 35, 45, and 58 km s$^{-1}$ were also reported toward the W33 complex [see @kohno18]. In this section, we have analyzed the FUGIN molecular line data 