Triggered star formation around mid-infrared bubbles in G8.14+0.23 H II region

TL;DR

This study investigates how expanding H II regions around MIR bubbles in G8.14+0.23 trigger star formation, revealing collected material, YSO clusters, and massive YSOs, supporting the collect-and-collapse process.

Contribution

It provides multi-wavelength observational evidence for triggered star formation via bubble expansion and assesses the collect-and-collapse mechanism in G8.14+0.23.

Findings

Detection of 244 YSOs, with 37% in clusters.

Alignment of dynamical and fragmentation timescales.

Identification of two massive embedded YSOs.

Abstract

Mid-infrared (MIR) shells or bubbles around expanding H II regions have received much attention due to their ability to initiate a new generation of star formation. We present multi-wavelength observations around two bubbles associated with a southern massive star-forming (MSF) region G8.14+0.23, to investigate the triggered star formation signature on the edges of the bubbles by the expansion of the H II region. We have found observational signatures of the collected molecular and cold dust material along the bubbles and the 12CO(J=3-2) velocity map reveals that the molecular gas in the bubbles is physically associated around the G8.14+0.23 region. We have detected 244 young stellar objects (YSOs) in the region and about 37% of these YSOs occur in clusters. Interestingly, these YSO clusters are associated with the collected material on the edges of the bubbles. We have found good agreement between the dynamical age of the H II region and the kinematical time scale of bubbles (from the 12CO(J=3-2) line data) with the fragmentation time of the accumulated molecular materials to explain possible "collect-and-collapse" process around the G8.14+0.23 region. However, one can not entirely rule out the possibility of triggered star formation by compression of the pre-existing dense clumps by the shock wave. We have also found two massive embedded YSOs (about 10 and 22 Msolar) which are associated with the dense fragmented clump at the interface of the bubbles. We conclude that the expansion of the H II region is also leading to the formation of these two young massive embedded YSOs in the G8.14+0.23 region.