Obscured luminosity fraction as a function of stellar mass for the full sample (left) and separated by redshift (right). Obscured fraction is defined as the obscured UV to total (intrinsic) UV luminosity at 1550 Å, inferred from the best-fit UV-to-IR SEDs. We show the moving median (dashed thick lines), moving weighted-average (dotted line) and best-fit curve (solid lines) to the samples at M_* > 4 × 10⁸ M_⊙, where the data is mass-complete. In the left panel, we also show the Whitaker et al. (2017) fit to z = 0.5 − 2.5 with an orange curve. The Whitaker et al. (2017) study was based on Spitzer/MIPS data with a wider area but biased to more obscured systems. Our weighted-average trend is also dominated by the heavily obscured systems, and therefore similar to the (Whitaker et al. 2017) curve. However, the median trend that is more representative of the full population captured by the deeper MIRI data (relative to the MIPS data) is systematically lower. Furthermore, as is shown in the right panel, there is no redshift evolution in this relation in our sample.