We report the first direct and robust measurement of the faint-end slope of the Lyman-alpha emitter (LAE) luminosity function at z = 5.7. Candidate LAEs from a low-spectral-resolution blind search with IMACS on Magellan-Baade were targeted at higher resolution to distinguish high redshift LAEs from foreground galaxies. All but 2 of our 42 single-emission-line systems have flux F $< 2.0 times 10^{-17}$ ergs s$^{-1}$ cm$^{-2}$, making these the faintest emission-lines observed for a z = 5.7 sample with known completeness, an essential property for determining the faint end slope of the LAE luminosity function. We find 13 LAEs as compared to 29 foreground galaxies, in very good agreement with the modeled foreground counts predicted in Dressler et al. (2011a) that had been used to estimate a faint-end slope of $alpha$ = -2.0 for the LAE luminosity function. A 32% LAE fraction, LAE/(LAE+foreground), within the flux interval F = $2-20 times 10^{-18}$ ergs s$^{-1}$ cm$^{-2}$, constrains the faint end slope of the luminosity function to -2.35 < $alpha$ < -1.95 (1-$sigma$). We show how this steep LF should provide, to the limit of our observations, more than 20% of the flux necessary to maintain ionization at z=5.7, with a factor-of-ten extrapolation in flux reaching more than 55%. This is in addition to a comparable contribution from Lyman Break Galaxies M$_{UV} le$ -18. We suggest that this bodes well for a sufficient supply of Lyman continuum photons by similar, low-mass star forming galaxies within the reionization epoch at z $approx$ 7, only 250 Myr earlier.
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