SED modeling of the sources NGC 5548 (left panel) and MRK 509 (right panel). The red line is the modeling of KD 18 (disk + Corona) and the blue line is the modeling adopted in this work (disk + Galaxy). As KERRBB, the AGNSED modeling is degenerate and by changing some of its parameters (i.e., BH mass, spin, Eddington ratio, X-ray corona size) appropriately, it is possible to reproduce the same SED (keeping the corona slopes constant as reported in KD 18): on the plot, we report some AGNSED BH mass solutions (in solar masses) for different spin values, along with the spectrum peak position (frequency and luminosity, in Hz and erg s⁻¹ respectively).