Notes. Columns 1–4 correspond to the QSO2 identifier (full SDSS name can be found in Bessiere et al. 2012), RA, Dec, and spectroscopic redshift from SDSS. Columns 5 and 6 correspond to the seeing FWHM of the spectroscopic observations used here, measured from stars in the acquisition images, and to the spatial scale. Columns 7 and 8 list the extinction-corrected [OIII] luminosities from Kong & Ho (2018), with the uncorrected [OIII] luminosities from Reyes et al. (2008) within parentheses, and the bolometric luminosities, derived from the extinction-corrected [OIII] luminosities using the factor of 454 from Lamastra et al. (2009). Column 9 corresponds to the radio luminosity, calculated using the integrated flux at 1.4 GHz from either the FIRST or NVSS surveys, assuming a spectral index of α = –0.75 when unknown. When the object is undetected in both surveys, an upper limit is given. Columns 10 indicates whether the inclusion of a young stellar population (YSP) with age < 100 Myr was necessary for modeling the stellar spectral features, following Bessiere et al. (2017). Columns 11 and 12 indicate whether there is evidence of mergers or interactions in the optical images, and the different stages of these interactions, as reported in Bessiere et al. (2012): (1) the quasar host is part of a galaxy pair showing signatures of tidal interaction, (2) other signs of morphological disturbance, (3) system with multiple nuclei (within 10 kpc between them), and (4) isolated galaxy. Column 13 lists the value of the parameter from Ramos Almeida et al. (2013), that measures the excess in the number of galaxies around the QSO2 as compared with the average number of background galaxies.