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Broad emission line profiles in AGN can be characterized by their line-width ratios FWHM/σline. The broad optical and UV emission line profiles — observed in the spectra of Active Galactic Nuclei (AGN) — follow systematic trends in a FWHM/σline vs. FWHM diagram. We tried to model these observed characteristics by multiple combinations of different line profile types in a simple way. Finally, we were able to explain all observed trends of the different emission lines in a simple and unique way by Lorentzian profiles that are broadened by rotation. Combinations of other line profiles were less unambiguous and/or could be excluded. To the different emission line regions belong individual turbulent velocities: they range from 400 to 2 900 km s. The observed rotational velocities range from 1 000 to 6 000 km s. For the computation of the central black hole masses in AGN on basis of their emission line widths one has first to correct for the contribution of the turbulence onto the widths of the line profile. Otherwise black hole masses are overestimated by a factor of two to ten without correction for the turbulent velocity fraction on the line profile width. Especially the broad UV emission lines have to be corrected for this effect as they are more heavily affected by the additional turbulence component in comparison to the optical lines.

The shape of broad-line profiles as diagnostic tool for structure and kinematics of the BLR in AGN