Examples of how Schechter fits are applied to mass functions (left) and luminosity functions (right) at 3.42 < z < 3.87. The luminosity function in this case is when we apply DL14 Entire to FARMER LP. In both cases, we applied the CANDELS correction to the sample before fitting the Schechter curves. We extrapolate galaxies corresponding to the difference between the projected curves and the existing functions. While there are slight discrepancies at high mass or luminosity, this is acceptable as this extrapolation method focuses on dim galaxies, and there are higher errors for the bright end of these functions (as shown in Fig. 8).