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We present high-redshift predictions of the star-formation-rate distributionfunction (SFR DF), UV luminosity function (UV LF), galactic stellar massfunction (GSMF), and specific star-formation rates (sSFRs) of galaxies from thelatest version of the Munich semi-analytic model L-Galaxies. We find a good fitto both the shape and normalisation of the SFR DF at $z=4-7$, apart from aslight under-prediction at the low SFR end at $z=4$. Likewise, we find a goodfit to the faint number counts for the observed UV LF; at brighter magnitudesour predictions lie below the observations, increasingly so at higherredshifts. At all redshifts and magnitudes, the raw (unattenuated) numbercounts for the UV LF lie above the observations. Because of the good agreementwith the SFR we interpret our under-prediction as an over-estimate of theamount of dust in the model for the brightest galaxies, especially athigh-redshift. While the shape of our GSMF matches that of the observations, welie between (conflicting) observations at $z=4-5$, and under-predict at$z=6-7$. The sSFRs of our model galaxies show the observed trend of increasingnormalisation with redshift, but do not reproduce the observed mass dependence.Overall, we conclude that the latest version of L-Galaxies, which is tuned tomatch observations at $z\leq3$, does a fair job of reproducing the observedproperties of galaxies at $z\geq4$. More work needs to be done on understandingobservational bias at high-redshift, and upon the dust model, before strongconclusions can be drawn on how to interpret remaining discrepancies betweenthe model and observations.

Galaxy formation in the PLANCK cosmology - III. The high-redshift universe