value for the W33 complex. Following the previous work of @kohno18, in this paper, we compute the ages of the ionized clumps for a value of $n_{0}$ = 10$^{4}$ cm$^{-3}$. The calculation uses the isothermal sound velocity in the ionized gas [$c_{s}$ = 11 km s$^{-1}$; @bisbas09], the radius of the H[ii]{} region ($R_{HII}$), $n_{0}$, and $N_\mathrm{uv}$. Dynamical ages of the ionized clumps vary between $\sim$0.35 – 1.0 Myr (see Table \[tab2\]). The bubble N10 (see ID \#c10 in Table \[tab2\]) is found to be excited by an O9.5V–O9V star (age $\sim$0.65 Myr), which is located away from the W33 complex. At least seven NVSS clumps (see IDs \#c1–c7) are located toward the W33 complex (area $\sim$15 pc $\times$ 15 pc; see a broken box in Figure \[fig1\]c), which contains OB stars (age $\sim$0.35 – 0.85 Myr). More description of the analysis can be found in @dewangan17. The implication of the ages of these ionized clumps is discussed in Section \[sec:disc\].

Dust temperature and column density maps {#sec:hermap}
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In order to study the embedded structures in our selected target area, we have obtained the [*Herschel*]{} temperature and column density ($N(\mathrm H_2)$) maps from the site. The spatial resolution of 