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In this paper we present calculations of the UV luminosity function from theDark-ages Reionization And Galaxy-formation Observables from NumericalSimulations (DRAGONS) project, which combines N-body, semi-analytic andsemi-numerical modelling designed to study galaxy formation during the Epoch ofReionization. Using galaxy formation physics including supernova feedback, themodel naturally reproduces the UV LFs for high-redshift star-forming galaxiesfrom $z{\sim}5$ through to $z{\sim}10$. We investigate the luminosity--starformation rate (SFR) relation, finding that variable SFR histories of galaxiesresult in a scatter around the median relation of $0.1$--$0.3$ dex depending onUV luminosity. We find close agreement between the model and observationallyderived SFR functions. We use our calculated luminosities to investigate theluminosity function below current detection limits, and the ionizing photonbudget for reionization. We predict that the slope of the UV LF remains steepbelow current detection limits and becomes flat at$M_\mathrm{UV}{\gtrsim}{-14}$. We find that $48$ ($17$) per cent of the totalUV flux at $z{\sim}6$ ($10$) has been detected above an observational limit of$M_\mathrm{UV}{\sim}{-17}$, and that galaxies fainter than$M_\mathrm{UV}{\sim}{-17}$ are the main source of ionizing photons forreionization. We investigate the luminosity--stellar mass relation, and find acorrelation for galaxies with $M_\mathrm{UV}{<}{-14}$ that has the form$M_*{\propto}10^{-0.47M_\mathrm{UV}}$, in good agreement with observations, butwhich flattens for fainter galaxies. We determine the luminosity--halo massrelation to be $M_\mathrm{vir}{\propto}10^{-0.35M_\mathrm{UV}}$, finding thatgalaxies with $M_\mathrm{UV}{=}{-20}$ reside in host dark matter haloes of$10^{11.0\pm 0.1}\mathrm{M_\odot}$ at $z{\sim}6$, and that this mass decreasestowards high redshift.

Dark-ages reionization & galaxy formation simulation IV: UV luminosity functions of high-redshift galaxies