Left panel: example of fit of the SDSS optical – UV and Spitzer IR spectra (black lines). The thick blue line is the fit performed with two black-bodies (whose temperatures, T_warm and T_hot, are reported in the plot) using the four WISE data points (red points) for the IR emission, and KERRBB for the disk emission (dashed red line with a shaded blue area representing the confidence interval for the spectrum peak – ∼0.05 dex). The thick red line is the fit performed with two parabolas and two black-bodies (whose temperatures, T₁ and T₂, are reported on the plot; see text for details) to describe the Spitzer emission, and KERRBB for the disk emission. Both the integrated luminosities ( and ) are reported on the plot (in erg s⁻¹). Archival photometric data (2MASS, NED, GALEX) are shown with gray dots. Right panel: comparison between and for the sources with Spitzer IR data. The average uncertainty from the fit is shown in the plot. The best-fit equation is reported along with the 1–2σ data dispersion (shaded blue areas) and the 1:1 line (dashed black line).