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We explore the relative role of small-scale fragmentation and global collapsein low-metallicity clouds, pointing out that in such clouds the cooling timemay be longer than the dynamical time, allowing the cloud to collapse globallybefore it can fragment. This, we suggest, may help to explain the formation ofthe low-metallicity globular cluster population, since such dense stellarsystems need a large amount of gas to be collected in a small region (withoutsignificant feedback during the collapse). To explore this further, we carryout numerical simulations of low-metallicity Bonner-Ebert stable gas clouds,demonstrating that there exists a critical metallicity (between 0.001 and 0.01$Z_\odot$) below which the cloud collapses globally without fragmentation. Wealso run simulations including a background radiative heating source, showingthat this can also produce clouds that do not fragment, and that the criticalmetallicity -- which can exceed the no-radiation case -- increases with theheating rate.

Slow Cooling in Low Metallicity Clouds: An Origin of Globular Cluster Bimodality?