Notes. Molecular gas: For each target we report the upper level of the CO transition, J_up, and the excitation correction, r_{Jup, 1} (see Notes in Table C.1). For COSB011 and XID2028, the CO(1-0) luminosity was derived extrapolating the ground-state transition flux from the QSOs SLEDs. We also indicate the luminosity-to-gas-mass conversion factors used to derive the gas mass in the different papers, as follows: ^⋆: α_CO = 3.6; ^□: α_CO = 1.0; ∘: α_CO = 0.8. The sample of dusty AGN comprises a large number of sources associated with evidence of multiphase outflows: broad and shifted components in the [O III] emission lines (e.g. Coppin et al. 2008; Perna et al. 2015a; Polletta et al. 2011) and in molecular CO lines (e.g. Banerji et al. 2017; Brusa et al. 2018; Fan et al. 2018; Stefan et al. 2015) are usually found in these targets. For a small number of sources there are also indications of ongoing mergers (W0149+2350, SMMJ030227, 3C 298). For these sources, characterised by complex CO line profiles, we report in the Table (and in the figures) the total molecular luminosities and masses obtained integrating over all the different kinematic components. X-ray luminosities and Column densities: X-ray luminosities refer to the 2–10 keV rest-frame absorption-corrected luminosities; column densities are derived from X-ray spectroscopic analysis for all but no. 226 and no. 682, for which N_H is derived from the hardness ratio, following the prescriptions in Elvis et al. (2012). To our knowledge, the only CT sources with molecular line observations are XID403 (from C10, G14), SW022513, and SW022550 (from P11), and GMASS953 (from T18). The source C1148 (from K17), detected with 20 net counts in X-ray, is a candidate CT source (see Sect. 4.1). The few CT sources at z > 1 are tabulated in the lower part of the table. Stellar masses and IR luminosities: A08, B18, E14, F18, G14, K17, St15 (from Leipski et al. 2013), St17, Po17 (from T18), Va17 (from Podigachoski et al. 2015), and Y10 host galaxy properties are obtained with a two-component (AGN+galaxy) SED fit; their IR luminosities refer therefore to the only stellar component. B13: IR luminosities are obtained from the 1.4 GHz continuum. Ba17: IR luminosities are obtained using a modified greybody model assuming dust temperature and dust emissivity values (T = [41, 47]; β = [1.6, 1.95]), and rescaling the model to match the 3mm observations. C08: stellar mass from Wardlow (2011); L_IR assuming a dust temperature of T = 40 K and a dust emissivity factor of ν^β, with β = 1.5, rescaling a modified greybody model to match the 850 or 1200 μm photometry. F14: stellar IR luminosity is obtained with a two-component (AGN+galaxy) SED fit, but is not well constrained due to the lack of data above the 22 μm. P11: stellar IR luminosities are obtained with a two-component (AGN+galaxy) SED fit, but is not well constrained due to the lack of data between 24 μm and 1.2mm. M_star from H-band luminosity. S12: IR luminosity is obtained by fitting the far-IR SED with a greybody model. Sp16: SFR and stellar mass from 3D-HST catalogue (Momcheva et al. 2015, i.e. without considering AGN component). The source is undetected in any Herschel/PACS or SPIRE bands. The infrared luminosity is derived from SFR, using the following prescription: L_IR = SFR × 10¹⁰ L_⊙ (Kennicutt 1998, correcting for a Chabrier IMF). Y10: these sources are undetected in SPIRE bands; far-IR emission is constrained using upper limits and mid-IR Spitzer spectra. Column (1): target name; Column (2): coordinates; Column (3): redshift; Column (4): J_up refers to the upper level of the (J_up → J_up − 1) CO transition; Column (5): the excitation correction defined as r_{Jup, 1} = CO(J_up → J_up − 1)/CO(1 → 0); Column (6): CO(1-0) luminosity; Column (7): gas mass; Column (8): stellar mass; Column (9): 8–1000 μm IR luminosity; Column (10): reference for the paper from which we derived CO and far-IR measurements, as well as assumed excitation correction and α_CO conversion factors. Columns (11) and (12): column density and 2–10 keV rest-frame absorption-corrected luminosities derived from X-ray spectroscopic analysis (see below). Column (13): reference for the paper from which we derived X-ray properties.

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