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We investigate the evolution of the galaxy stellar mass function athigh-redshift ($z\ge 5$) using a pair of large cosmological hydrodynamicalsimulations: {\em MassiveBlack} and {\em MassiveBlack-II}. By combining thesesimulations we can study the properties of galaxies with stellar masses greaterthan $10^{8}\,{\rm M_{\odot}}\,h^{-1}$ and (co-moving) number densities of$\log_{10}(\phi\, [{\rm Mpc^{-3}\,dex^{-1}}\,h^{3}])>-8$. Observationaldeterminations of the galaxy stellar mass function at very-high redshifttypically assume a relation between the observed UV luminosity and stellarmass-to-light ratio which is applied to high-redshift samples in order toestimate stellar masses. This relation can also be measured from thesimulations. We do this, finding two significant differences with the usualobservational assumption: it evolves strongly with redshift and has a differentshape. Using this relation to make a consistent comparison between galaxystellar mass functions we find that at $z=6$ and above the simulationpredictions are in good agreement with observed data over the whole mass range.Without using the correct UV luminosity and stellar mass-to-light ratio, thediscrepancy would be up to two orders of magnitude for large galaxies$>10^{10}\,{\rm M_{\odot}}\,h^{-1}$. At $z=5$, however the stellar massfunction for low mass $<10^{9}\,{\rm M_{\odot}}\,h^{-1}$ galaxies isoverpredicted by factors of a few, consistent with the behaviour of the UVluminosity function, and perhaps a sign that feedback in the simulation is notefficient enough for these galaxies.

Confronting predictions of the galaxy stellar mass function with observations at high-redshift