Notes. Table columns: (1) identification number from Laigle et al. (2016), as in Calabrò et al. (2018); (2) spectroscopic redshift inferred from Magellan spectra; (3) total attenuation A_V, tot toward the center in a mixed model geometry, calculated in Calabrò et al. (2018) and explained in Section 2 ; (4) FWHM size in radio 3 GHz band (from VLA-COSMOS); ^†: fit with a single 2D Gaussian but with fixed axis ratio and position angle (1 and 0); ^‡: fit with a Double 2D Gaussian, we give here the total FWHM (average of single component sizes + separation between the two); we put a 3σ upper limit for unresolved sources, while the remaining starbursts are fit with a single 2D Gaussian and free parameters; (5) line velocity width of emission lines, derived from fitting the Magellan spectra with MPFIT (for double Gaussians, this quantity is the sum of the single Gaussian FWHM and the separation in velocity between the two peaks); (6,7,8) observed equivalent width of Hα,Paβ and Hδ, the latter coming from zCOSMOS or SDSS optical spectra; (9,10) fluxes of [O III]λ5007 Å and Hβ (in units of 10⁻¹⁷) inferred from optical spectra. Hβ fluxes have been corrected for underlying absorption assuming EW_abs = 5 Å as determined from Bruzual & Charlot (2003) synthetic stellar spectra; (11) bolometric AGN luminosity derived as 1.4 × L_AGN, IR, the latter being the AGN luminosity in the infrared inferred from SED fitting (see Liu et al. 2018 and Jin et al. 2018 for the methodology); (12) significance of mid-IR dusty-torus detection from SED fitting (<3 means that it is not detected); (13) morphological type following the visual criteria of Kartaltepe et al. (2010) (objects with a * have been already classified in the same paper). We remind that the coordinates of our targets, their stellar masses, SFRs and Hα (Paβ) flux measurements can be retrieved from Calabrò et al. (2018).