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Fig. 3.

image

Spectrum of Mrk 1018 at different epochs once the contribution of the host galaxy has been subtracted from the spectrum of the nucleus. The flux density of the SDSS spectrum has been divided by a factor of 1.55 for comparison with the other spectra, which are affected differently by slit loss. Narrow lines appear broader in the FORS2 spectrum due to the lower spectral resolution.

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