Notes. Surface densities in Cols. (2) and (10) are normalized to the B-band 25 mag arcsec⁻² area, while the SFR surface density in Col. (3) is normalized to the star-forming area only. The CO luminosity in Col. (7) was derived from the CO velocity-integrated main beam brightness temperature and subsequent multiplication with the aperture correction factor in Col. (6). For galaxies with CO detection, M_H2obs in Col. (8) was calculated from the CO luminosity in Col. (7) via application of the conversion factor in Col. (5). For galaxies with positive CO and H I detection, M_gasobs is the sum of the atomic mass from Pardy et al. (2014) and the molecular mass in Col. (8). Total gas masses M_gasest in Col. (11) were derived from the dust masses using a metallicity-dependent gas-to-dust ratio shown in Col. (4). The estimated molecular mass M_H2est is the result of the dust-based total mass M_gasest minus the observed atomic gas mass. The total gas surface density in Col. (12), the total gas depletion time τ_gas in Col. (13), as well as the total gas fraction f_gas = M_gasest/(M * +M_gasest) in Col. (14) use the dust-based total gas mass estimate. The atomic gas fraction f_HI is the ratio between the observed H I gas mass and the total dust-based gas mass. The molecular gas fraction f_mol is the ratio between the estimated molecular gas mass and the total dust-based gas mass. The PDR gas mass fractions in Col. (17) are the γ values from Table 8 on a linear scale. We note that the large discrepancies between the reported upper limits in Cols. (8) and (10) and the dust-based estimated quantities are likely the result of beam dilution, that is, the upper limits are likely misleading. The units of the derived quantities are: (2), (3): M_⊙ yr⁻¹ kpc⁻² (5): (K km s⁻¹ pc²)⁻¹ (7): K km s⁻¹ pc² (8)−(11): M_⊙ (12): M_⊙ pc⁻² (13): yr.