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Broad emission lines are emitted in the surroundings of supermassive blackholes in the centers of active galactic nuclei (AGN). This region is spatiallynot resolved. We intend to get information on the structure and geometry ofthis broad emitting line region (BLR) based on line profile observations. Wemodel the rotational and turbulent velocities in the line-emitting regionsbased on observed full-width at half maximum line values (FWHM) and{\sigma}_{line} of the variable broad emission lines in four nearby AGN: NGC3783, NGC 7469, NGC 5548, and 3C 390.3. On the basis of these velocities, weestimate the height of the line-emitting regions above the midplane in contextwith their distances from the center. The H{\beta} lines are emitted in a moreflattened configuration above the midplane in comparison to the highly ionizedlines. The H{\beta} lines originate at heights of 0.7 to 1.6 light-days and atdistances of 1.4 to 24 light-days with height/distance (H/R) ratios of only0.07 to 0.5. The highly ionized lines originate at smaller radii than theH{\beta} lines and/or at greater distances above the midplane with H/R valuesof 0.2 to 1.7. In total, the emission lines do not originate in a thinatmosphere of an accretion disk but rather at very extended regions above anaccretion disk. The observed geometries of the line-emitting regions resemblethe geometries of accretion disk wind models. Furthermore, the angle of thecentral opening cone (generated by the emitting regions of the highly ionizedlines) is small for those galaxies with slow rotational velocities andincreases with the rotation velocity of the central region. The derivedgeometries of the line-emitting regions of all four AGN are consistent with thegeometries that are predicted in outflowing disk wind models.

Vertical broad-line region structure in nearby active galactic nuclei