# CO observations of the molecular gas in the galactic HII region Sh2-48; Evidence for cloud-cloud collision as a trigger of high-mass star formation

## TL;DR

This study uses CO observations to analyze the molecular gas in the galactic HII region Sh2-48, providing evidence that a cloud-cloud collision likely triggered the high-mass star formation there.

## Contribution

It presents new CO data and interprets the velocity structure as resulting from a cloud-cloud collision, linking it to star formation in Sh2-48.

## Key findings

- Velocity distribution consistent with cloud-cloud collision
- Collision timescale matches HII region formation age
- Evidence supports collision-triggered star formation

## Abstract

Sh2-48 is a Galactic HII region located at 3.8 kpc with an O9.5-type star identified at its center. As a part of the FOREST Unbiased Galactic plane Imaging survey using the Nobeyama 45-m telescope (FUGIN) project, we obtained the CO J=1-0 dataset for a large area of Sh2-48 at a spatial resolution of 21"(~0.4 pc), which we used to find a molecular cloud with a total molecular mass of ~3.8x10^4 Mo associated with Sh2-48. The molecular cloud has a systematic velocity shift within a velocity range ~42-47 km/s . On the lower velocity side the CO emission spatially corresponds with the bright 8 {\mu}m filament at the western rim of Sh2-48, while the CO emission at higher velocities is separated at the eastern and western sides of the 8{\mu}m filament. This velocity change forms V-shaped, east-west-oriented feature on the position-velocity diagram. We found that these lower and higher-velocity components are, unlike the infrared and radio continuum data, physically associated with Sh2-48. To interpret the observed V-shaped velocity distribution, we assessed a cloud-cloud collision scenario and found from a comparison between the observations and simulations that the velocity distribution is an expected outcome of a collision between a cylindrical cloud and a spherical cloud, with the cylindrical cloud corresponding to the lower-velocity component, and the two separated components in the higher-velocity part interpretable as the collision-broken remnants of the spherical cloud. Based on the consistency of the ~1.3Myr estimated formation timescale of the HII region with that of the collision, we concluded that the high-mass star formation in Sh2-48 was triggered by the collision.