Extended HNCO, SiO, and HC₃N Emission in 43 Southern Star-forming Regions

We have selected 43 southern massive star-forming regions to study the spatial distribution of HNCO 4$_{04}$-3$_{03}$, SiO 2-1 and HC$_{3}$N 10-9 line emission investigate their association with dust emission. The morphology 4$_{04}$-3$_{03}$ agrees well tends originate from more compact than 2-1. divided our sources into three groups: those in Central Molecular Zone (CMZ), associated bubbles (Bubble), remaining sources, which are termed 'normal star forming regions' (NMSFR). These groups, subdivided different categories respect widths, integrated intensities, column densities, hint at presence physical chemical processes. find that temperature $T_{\rm d}$, abundance ratios $N_{\rm HNCO}/N_{\rm SiO}$ HC3N}$ show a decreasing trend towards central dense CMZ while HC3N}/N_{\rm moves opposite direction. Moreover, better agreement is found between d}$ Bubble NMSFR category sources. Both outflow inflow activities been eight sixteen bubble low detection rate indicates these wing either below sensitivity limit or bulk may be produced by expansion an H{\sc\,ii} region supernova remnant, has pushed molecular gas away shock yielding SiO.