Best-fit modelling of the SDSS 2004 spectrum (left). Data are shown as solid black line along with the full best-fit model in red, and separate models for the various spectral components in different colours (see legend). A slight 1st-degree polynomial (dashed black line) is fitted to the weak AGN continuum, while no BLR components are detected. Zoom over the spectral window 6250 − 6900 Å around the Hα line, clearly showing the total absence of a broad Hα component (right).