Demonstration of the effects that arise from allowing the nebular emission lines to be fainter than the continuum in the faintest sources. This enables us to flatten an intrinsically steep UV LF (α ∼ −2, in grey) into a flatter nebular emission line LF (α ∼ −1.89, in black). In red is the Schechter least square fit (α = −1.89, log₁₀L^* = 42.09, log₁₀ϕ_* = −3.63) of the simulated [O III]+Hβ LF. The bright end is dashed, as the effect applied yields non-Schechter-like profile on the bright end.