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State-of-the-art cosmological hydrodynamical simulations of galaxy formationhave reached the point at which their outcomes result in galaxies with evermore realism. Still, the employed sub-grid models include several freeparameters such as the density threshold, $n$, to localize the star-forminggas. In this work, we investigate the possibilities to utilize the observedclustered nature of star formation (SF) in order to refine SF prescriptions andconstrain the density threshold parameter. To this end, we measure theclustering strength, correlation length and power-law index of the two-pointcorrelation function of young ($\tau<50$ Myr) stellar particles and compare ourresults to observations from the HST Legacy Extragalactic UV Survey (LEGUS).Our simulations reveal a clear trend of larger clustering signal and power-lawindex and lower correlation length as the SF threshold increases with only milddependence on galaxy properties such as stellar mass or specific star formationrate. In conclusion, we find that the observed clustering of SF is inconsistentwith a low threshold for SF ($n<1$ cm$^{-3}$) and strongly favours a high valuefor the density threshold of SF ($n>10$ cm$^{-3}$), as for example employed inthe NIHAO project.

An observational test for star formation prescriptions in cosmological hydrodynamical simulations