 (0.0,0.0)[![To illustrate the onset of the fragmentation process in the $Z=00^{-0}~\rm{Z}_{\odot}$ simulation, the graphs show the densities of the particles, plotted as a function of their position. Note that for each plot, the particle data has been centered on the region of interest. Results are plotted for three different output times, ranging from the time that the first star forms ($t_{\rm{SF}}$) to $000$ years afterwards. The densities lying between the two horizontal dashed lines denote the range over which dust cooling lowers the gas temperature. We also plot the mass function for a metallicity of $Z=00^{-0}~\rm{Z}_{\odot}$ and mass resolution $0.000~\rm{M}_{\odot}$ and $0.000~\rm{M}_{\odot}$, respectively. Note the similarity between the results of the low-resolution and high-resolution simulations. The onset of dust cooling in the $Z=00^{-0}~\rm{Z}_{\odot}$ cloud results in a stellar cluster which has a mass function similar to that for present-day stars, in that the majority of the mass resides in the low-mass objects. This contrasts with the $Z=00^{-0}~\rm{Z}_{\odot}$ and primordial clouds, in which the bulk of the cluster mass is in high-mass stars (see Clark et al. 0000).](f0