Each panel is similar to Figure 13, but with different methodological choices relative to our nominal choices. In Figure 13, we use selection criteria that require 2σ detections of each line and P1 > −0.3 and P3 > 0.55 to define a Seyfert, we use J. Kormendy & L. C. Ho (2013) to estimate the black hole mass, and we use the dust-corrected L(Hβ)_corr and the relationship in H. Netzer (2019) to estimate the bolometric luminosity.