Dissecting the morphology of star forming complex S193

TL;DR

This study comprehensively analyzes the star-forming complex S193 across multiple wavelengths, revealing its stellar clusters, dust distribution, ionized regions, and molecular gas dynamics, suggesting feedback-triggered star formation.

Contribution

It provides a detailed multi-wavelength characterization of S193, including identification of clusters, dust clumps, and gas kinematics, highlighting feedback effects in star formation.

Findings

Identification of 16 cold dust clumps.

Detection of two velocity components in molecular gas.

Evidence of feedback-triggered star formation.

Abstract

We have studied a star-forming complex S193 using near-infrared (NIR) observations and other archival data covering optical to radio wavelengths. We identified stellar clusters in the complex using the NIR photometric data and estimated the membership and distance of the clusters. Using the mid-infrared (MIR) and far-infrared (FIR) images, the distribution of the dust emission around H\,{\sc ii} regions is traced in the complex. The $Herschel$ column density and temperature maps analysis reveal 16 cold dust clumps in the complex. The H$\alpha$ image and 1.4 GHz radio continuum emission map are employed to study the ionised gas distribution and infer the spectral type and the dynamical age of each H\,{\sc ii} region/ionised clump in the complex. The $^{12}$CO(J =3$-$2) and $^{13}$CO(J =1$-$0) molecular line data hint at the presence of two velocity components around [-43,-46] and [-47,-50] km/s, and their spatial distribution reveals two overlapping zones toward the complex. By investigating the immediate surroundings of the central cluster [BDS2003]57 and the pressure calculations, we suggest that the feedback from the massive stars seems responsible for the observed velocity gradient and might have triggered the formation of the central cluster [BDS2003]57.}