Notes. Number of objects classified in the found distributions as a function of both α_OX (i.e., SR or HR) and log U (LE or HE) as calculated by HCM-TEFF-IR assuming models with f_e = 99.9% including dust grains. The table includes the overall sample, and different categories as a function of their optical classification and the classes defined by Spoon et al. (2022) from their IR spectrum (i.e., 1A: hot-dust-dominated spectrum typical of AGNs, 1B: Optical Seyferts, and 2A-3B: ULIRG mainly in interaction). For all spectral types, either the SRHE or HRLE class always contains the largest number of objects (indicated in boldface). The last column show the median bolometric luminosity for the different AGN type subsamples estimated from the [Ne V] 14.3 μm line derived by Spinoglio et al. (2024).