Notes. Luminosities are expressed in units of 10¹⁰ K km s⁻¹ pc², the masses in units of 10¹⁰ M_⊙ and the column densities in units of 10²³ cm⁻². Column description: (1) ID of the sources. (2) Integrated flux of the observed transition (in units of Jy km s⁻¹), derived multiplying the flux density (second column of Table 4) by the FWHM of the line (third column in Table 3, for XID 666 we assumed that the line width is equal to the sum of the FWHM of the two line components). For the undetected sources we assumed a line width of 400 km s⁻¹. (3) Luminosity of the observed transition derived from F_CO. (4) Flux density at 850(1 + z) μm (in units of μJy), derived from the observed ∼2.1 mm flux density assuming a modified black body (MBB) model. (5) Conversion methods adopted to compute the CO(1–0) transition luminosity : “SMG CO-SLED” and “QSO CO-SLED” refer to two conversion factors, typical for SMGs and QSOs, respectively, between and (see text), while “MBB” exploits the relation found by Scoville et al. (2016). (6) Derived CO(1–0) transition luminosities. (7) Total gas mass assuming a CO luminosity-to-molecular gas mass (M_H2) conversion factor α_CO = 0.8 M_⊙ (K km s⁻¹ pc²)⁻¹, and considering the atomic gas mass equal to ∼M_H2/5 (Calura et al. 2014). (8) Column densities in the spherical geometry, assuming as a path length of the light the radius of the sphere. (9) (10) (11) Gas mass, infrared SED-fitting column density, and X-ray spectral fitting column density, respectively, derived by Circosta et al. (2019). The upper limits for the undetected sources are given at the 3σ upper level. Column densities refer to the uniform spherical model.