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We present a model for the evolution of the galaxy ultraviolet (UV)luminosity function (LF) across cosmic time where star formation is linked tothe assembly of dark matter halos under the assumption of a mass dependent, butredshift independent, efficiency. We introduce a new self-consistent treatmentof the halo star formation history, which allows us to make predictions at$z>10$ (lookback time $\lesssim500$ Myr), when growth is rapid. With acalibration at a single redshift to set the stellar-to-halo mass ratio, and nofurther degrees of freedom, our model captures the evolution of the UV LF overall available observations ($0\lesssim z\lesssim10$). The significant drop inluminosity density of currently detectable galaxies beyond $z\sim8$ isexplained by a shift of star formation toward less massive, fainter galaxies.Assuming that star formation proceeds down to atomic cooling halos, we derive areionization optical depth $\tau = 0.056^{+0.007}_{-0.010}$, fully consistentwith the latest Planck measurement, implying that the universe is fullyreionized at $z=7.84^{+0.65}_{-0.98}$. In addition, our model naturallyproduces smoothly rising star formation histories for galaxies with $L\lesssimL_*$ in agreement with observations and hydrodynamical simulations. Before theepoch of reionization at $z>10$ we predict the LF to remain well-described by aSchechter function, but with an increasingly steep faint-end slope($\alpha\sim-3.5$ at $z\sim16$). Finally, we construct forecasts for surveyswith \JWST~and \WFIRST and predict that galaxies out to $z\sim14$ will beobserved. Galaxies at $z>15$ will likely be accessible to JWST and WFIRST onlythrough the assistance of strong lensing magnification.

The Galaxy UV Luminosity Function Before the Epoch of Reionization