Extended HNCO, SiO, and HC$_{3}$N emission in 43 southern star-forming regions

TL;DR

This study maps and analyzes the spatial distribution of specific molecular emissions in 43 southern star-forming regions, revealing variations in physical and chemical processes across different environments.

Contribution

It provides a detailed comparison of molecular emissions and dust properties in diverse star-forming regions, highlighting differences in physical conditions and chemical abundances.

Findings

HC3N emission is more compact than HNCO and SiO.

Dust temperature and molecular abundance ratios vary across regions.

Evidence of outflow and inflow activities in several sources.

Abstract

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