The Virial Factor f of the Hβ Broad Line for NGC 5548 and NGC 4151

The variability of virial factor f is investigated for two active galactic nuclei, NGC 5548 and NGC 4151, which had been previously reverberation mapped (RM) over 20 times in the past 30 yr. Using four velocity tracers from the broad H β width at half-maximum (FWHM _H _β ) or the line dispersion from the mean or rms spectra, f for each RM epoch is calculated. Significant correlations are found between f and observational parameters, such as the broad-line widths, the Eddington ratios, and the line profile shapes. For NGC 5548, $f\propto {{\rm{FWHM}}}_{{\rm{mean}}}^{-0.70\pm 0.13}$ and for NGC 4151, $f\propto {{\rm{FWHM}}}_{{\rm{mean}}}^{-3.31\pm 0.59}$. This suggests that a variable f should be included to weight the virial supermassive black hole mass. Using a simple model of thick-disk broad-line regions (BLRs), we show that changes in mean inclination can explain f variation. The inclination range is 14 $\mathop{.}\limits^{\unicode{x000b0}}$ 1−40 $\mathop{.}\limits^{\unicode{x000b0}}$ 6 for NGC 5548 and 14 $\mathop{.}\limits^{\unicode{x000b0}}$ 0−55 $\mathop{.}\limits^{\unicode{x000b0}}$ 1 for NGC 4151. Modeling the light curves of f with a damped random walk process yields mean timescales of 638 and 668 days, consistent with BLR dynamical timescales within uncertainties. This indicates that f variations are linked to BLR dynamics, likely due to changes in geometry or inclination.

Abstract licence: CC BY

A person counts once a day per paper. We keep no cookie and no address: a reader is a hash that changes every day. Any month under five reads shows no number.