2022MNRAS.517..675D

We present simulations of the formation and evolution of clusters in spiral arms. The simulations follow two different spiral arm regions, and the total gas mass is varied to produce a range of different mass clusters. We find that including photoionizing feedback produces the observed cluster mass-radius relation, increasing the radii of clusters compared to without feedback. Supernovae have little impact on cluster properties. We find that in our high-density, high gas mass simulations, star formation is less affected by feedback, as star formation occurs rapidly before feedback has much impact. In our lowest gas density simulation, the resulting clusters are completely different (e.g. the number of clusters and their masses) from the case with no feedback. The star formation rate is also significantly suppressed. The fraction of stars in clusters in this model decreases with time flattening at about 20 per cent. In our lowest gas simulation model, we see the formation of a star-forming group with properties similar to an OB association, in particular similar to Orion Ia. We suggest that low densities and stronger initial dynamics are conducive to forming associations rather than clusters. In all models, cluster formation is complex with clusters merging and splitting. The most massive clusters that form have tended to undergo more mergers.