Example of ALMA spectra and far-IR spectral energy distribution. Left: red open squares and arrows indicate detections and 3σ upper limits on the IR photometry that we modeled. Blue open circles indicate radio measurements, which we did not include in the fitting. The gray dashed and dotted-dashed lines mark the best-fit Draine & Li (2007) and Mullaney et al. (2011) templates for the star-forming and AGN components, respectively. A stellar template was included when modeling the IRAC bands, but we do not show it to avoid confusion. The black solid line indicates the sum of all the templates. Right: ALMA spectra with detected CO (2 − 1) (green), CO (5 − 4) (orange), CO (7 − 6) (purple), and [C I] (yellow) transitions (CO (4 − 3) is not available for this source). The solid red line indicates the best-fit Gaussian model. The black tick shows the expected line position based on the optical redshift z_spec, opt. The full compilation of SEDs and spectra from which we extracted reliable line measurements (Sect. 3.2.2) is available at http://doi.org/10.5281/zenodo.3967380.