The Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium (SEDIGISM) survey has produced high (spatial
and spectral) resolution 13CO (2–1) maps of the Milky Way. It has allowed us to investigate the molecular interstellar medium in the
inner Galaxy at an unprecedented level of detail and characterise it into ...
The Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium (SEDIGISM) survey has produced high (spatial
and spectral) resolution 13CO (2–1) maps of the Milky Way. It has allowed us to investigate the molecular interstellar medium in the
inner Galaxy at an unprecedented level of detail and characterise it into molecular clouds. In a previous paper, we have classified the
SEDIGISM clouds into four morphologies. However, how the properties of the clouds vary for these four morphologies is not well
understood. Here, we use the morphological classification of SEDIGISM clouds to find connections between the cloud morphologies,
their integrated properties, and their location on scaling relation diagrams. We observe that ring-like clouds show the most peculiar
properties, having, on average, higher masses, sizes, aspect ratios and velocity dispersions compared to other morphologies. We
speculate that this is related to the physical mechanisms that regulate their formation and evolution, for example, turbulence from
stellar feedback can often results in the creation of bubble-like structures. We also see a trend of morphology with virial parameter
whereby ring-like, elongated, clumpy and concentrated clouds have virial parameters in a decreasing order. Our findings provide a
foundation for a better understanding of the molecular cloud behaviour based on their measurable properties.