and molecular gas masses as a function of L_FIR for our AGN sample (red circles) and inactive galaxies (blue squares; Tacconi et al. 2018). To display the distribution of the two samples in the plot, we performed a bisector fit by adopting a Bayesian framework (see text). The dispersion of the fits is given by plotting 500 realizations of the bisector fit. Where the fits are better constrained (log L_FIR/L_⊙ = 12.2) AGN show CO luminosities 0.43 dex lower than inactive galaxies at the ∼2σ level.