Inferred SED for the best-fit model of the nuclear spectrum of NGC 5427 (model A: M_BH = 5 × 10⁷ M_⊙, an Eddington fraction of 0.1, a hard X-ray scale factor of 0.2 and log U = −1.3). The vertical scaling factor applies at the inner edge of the model NLR. Note the absence of an intermediate Compton component between 16 < log ν< 18. Such a component would arise naturally in Compton-heated optically-thin photoionised gas close to the ionising source. For comparison, we also show the other models which give a reasonable fit to the observed nuclear spectrum. Model B has the parameters M_BH = 5 × 10⁷ M_⊙, an Eddington fraction of 0.1 and a hard X-ray scale factor of 0.25 and log U = −1.5, and model C has M_BH = 10⁸ M_⊙, an Eddington fraction of 0.05 and a hard X-ray scale factor of 0.2 and log U = −2.0. The line fluxes for these are given in detail in Table 2.