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Broad‐Line Clouds in Active Galactic Nuclei

The equivalent width (i.e., relative strength) of the broad HB emission line in Seyfert I galaxies is shown to depend on the velocity width of the lines, being very weak for objects with narrow lines. The equivalent width of the FeII A4570 blend, on the other hand, is independent of velocity width. Simple calculations show that the decrease in equivalent width of HP is due to either slightly higher densities or slightly larger optical depths in the partially ionized zones of the broad-line clouds of the narrowerline Seyfert I galaxies. HB is collisionally suppressed at much lower densities or optical depths than the optical FeII lines are. The correlation of HB emissivity with cloud velocity provides strong support for the radiative acceleration models developed by Mathews and Blumenthal. It is suggested that the recent IUE satellite observations of low CIII]Al909/CIVA1549 ratios in Seyfert I galaxies (compared with high red shift quasars) are due to higher densities rather than high ionization parameters. It is predicted that this ratio should be higher in objects lacking strong FeII emission, such as radio galaxies.