2025MNRAS.538.2445D

We present a study of giant molecular cloud (GMC) properties in the Andromeda galaxy (M31) using CO(3-2) data from the James Clerk Maxwell Telescope (JCMT) in selected regions across the disc and in the nuclear ring, and comparing them with CO(1-0) observations from the Institut de Radioastronomie Millimetrique (IRAM) 30m telescope in the same regions. We find that GMCs in the centre of M31 generally exhibit larger velocity dispersions ($\sigma$) and sizes (R) compared to those in the disc, while their average surface density ($\Sigma$) and turbulent pressure ($P_{\rm turb}$) are lower. This low turbulent pressure in the central region is primarily due to the low density of molecular gas. The estimated GMC properties depend on the choice of CO transitions. Compared to CO(1-0), CO(3-2) exhibits smaller velocity dispersion and equivalent radius but higher surface density. These differences highlight the distinct physical conditions probed by different molecular gas tracers. We estimate the virial parameter $\alpha _{\rm vir}\propto \sigma ^2 R/\Sigma$ and find that most molecular clouds exhibit high values ($\alpha _{\rm vir} \sim 4{\!-\!}6$) for both CO transitions, indicating that they are unbound. Furthermore, clouds in the nuclear ring display even larger $\alpha _{\rm vir}$ values of ${\lesssim} 100$, suggesting that they may be highly dynamic, short-lived structures, although they could potentially achieve equilibrium under the external pressure exerted by the surrounding interstellar medium.