Apparent evolution of the faint-end slope α (upper panel), characteristic luminosities M* (middle panel), and normalization ϕ ^* (lower panel) of the UV LF with redshift. The red circles present the current LF constraints at z = 2–9 and those of Oesch et al. (2018a) at z ∼ 10, while the blue, green, and magenta circles give the Wyder et al. (2005), Arnouts et al. (2005), and Moutard et al. (2020) constraints at z ∼ 0.05, z ∼ 0.4, and over the redshift range z ∼ 0.3–1.5. The shaded red line illustrates our best-fit relation for the evolution (Section 3.4). The evolution of the faint-end slope α is now extremely well determined as a function of redshift and remarkably consistent with the evolution expected based on the change in slope of the halo mass function (Tacchella et al. 2013, Bouwens et al. 2015a; Mason et al. 2015; Mashian et al. 2016; Tacchella et al. 2018; Park et al. 2019; Bouwens et al. 2021a). Previous work by Bouwens et al. (2015a), Parsa et al. (2016), and Finkelstein (2016) arrived at very similar dα/dz trends as to what was found here by fitting to the available α determinations.