Fig. A.8.

Fit of the source MRK 590. Prominent host-galaxy emission required in the fitting procedure. For a satisfactory fit, the AD emission has to be cut at around Log ν/Hz ∼ 15 (i.e., the AD size is smaller than 106Rg as implemented in KERRBB). In the range Log ν/Hz = 14.9 − 15, the Balmer continuum can describe the rise of spectroscopic data (not represented for clarity). For this source, the peak is not visible but we used the curvature at smaller frequencies to obtain an estimate of the position.
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