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Redshifted 21cm measurements of the structure of ionised regions that growduring reionization promise to provide a new probe of early galaxy andstructure formation. One of the challenges of modelling reionization is toaccount both for the sub-halo scale physics of galaxy formation and the regionsof ionization on scales that are many orders of magnitude larger. To bridgethis gap we first calculate the statistical relationship between ionizingluminosity and Mpc-scale overdensity using detailed models of galaxy formationcomputed using relatively small volume - ($\sim$100Mpc/$h$)$^{3}$, highresolution dark matter simulations. We then use a Monte-Carlo technique toapply this relationship to reionization of the intergalactic medium withinlarge volume dark matter simulations - ($>$1Gpc/$h$)$^{3}$. The resultingsimulations can be used to address the contribution of very large scaleclustering of galaxies to the structure of reionization, and show that volumeslarger than 500Mpc/$h$ are required to probe the largest reionization featuresmid-way through reionization. As an example application of our technique, wedemonstrate that the predicted 21cm power spectrum amplitude and gradient couldbe used to determine the importance of supernovae feedback for early galaxyformation.

A hybrid multi resolution scheme to efficiently model the structure of reionization on the largest scales