Description
The SEDIGISM survey reveals properties of molecular clouds located in a range of environments across our Galaxy. Here we show our analysis on the kinematical properties of such molecular clouds, using the 13CO$(2-1)$ line emission. By analysing the light from this emission, we are studying whether clouds from different environments have different preferred direction of rotation compared to that of the Galaxy as a whole. This could potentially give insights into how star formation differs in these environments. Additionally, we are investigating the correlation (or lack thereof) between the surface density structure and the velocity fields of these clouds, and relate this to their embedded star formation. The presence of a correlation between these two variables could potentially help us understand the way in which molecular clouds evolve and collapse to form stars.
