Notes. All the QSO2s’ properties are from Ramos Almeida et al. (2025), except for N${}_{\mathrm{H}}^{\mathrm{CO}}$, which we recalculated using the CO(2-1) and CO(3-2) observations with beam sizes of ∼0.2–0.3″ from Audibert et al. (2025), in apertures equal to the corresponding beam sizes, and assuming α_CO = 4.35 M_⊙ (K km s⁻¹ pc²)⁻¹ and R₂₁ = R₃₁ = 1. In the case of the Seyfert 2 galaxies, S_9.7 is from García-Bernete et al. (2024a), L_bol from Koss et al. (2017), and estimated from the 14–150 keV intrinsic luminosity, and λ_Edd and galaxy inclination from García-Burillo et al. (2024) and Zhang et al. (2024). For NGC 7319, λ_Edd was calculated using L_bol and a black hole mass of 2.4 × 10⁶ M_⊙. N${}_{\mathrm{H}}^{\mathrm{CO}}$ were calculated from the ALMA CO data used in García-Burillo et al. (2024), which have beam sizes of ∼0.1–0.2″, and in Esparza-Arredondo et al. (2025) for MCG-5-23-16 (beam size of 0.65″ × 0.53″), using the same assumptions as for the QSO2s. For NGC 7319, a 3σ upper limit for N${}_{\mathrm{H}}^{\mathrm{CO}}$ was obtained from NOEMA CO(1-0) observations with a beam size of 0.6″ × 0.3″ (PI: M. Pereira-Santaella), assuming Δv_FWHM = 250 km s⁻¹ and Δv = 50 km s⁻¹ and using Equation (1) in Koay et al. (2016). The N${}_{\mathrm{H}}^{\mathrm{CO}}$ values of the QSO2s are comparatively more beam-diluted than those of Seyfert galaxies because of the different beam sizes (∼500 pc for the QSO2s versus ∼50–200 pc in the Seyferts).