We present dynamical modeling of the broad line region (BLR) for a sample of five Seyfert 1 galaxies using reverberation mapping data taken by the Lick AGN Monitoring Project in 2008. By modeling the AGN continuum light curve and Hβ line profiles directly we are able to constrain the geometry and kinematics of the BLR and make a measurement of the black hole mass that does not depend upon the virial factor, f , needed in traditional reverberation mapping analysis. We find that the geometry of the BLR is generally a thick disk viewed close to face-on. While the Hβ emission is found to come preferentially from the far side of the BLR, the mean size of the BLR is consistent with the lags measured with cross-correlation analysis. The BLR kinematics are found to be consistent with either inflowing motions or elliptical orbits, often with some combination of the two. We measure black hole masses of log 10 (M BH /M ) = 6.62

Narrow-line Seyfert 1 galaxies (NLS1s) are arguably one of the key AGN subclasses in investigating the origin of the black hole mass -stellar velocity dispersion (M BH − σ * ) relation because of their high accretion rate and significantly low M BH . Currently, it is under discussion whether present-day NLS1s offset from the M BH − σ * relation. Using the directly measured stellar velocity dispersion of 93 NLS1s at z<0.1, and M BH estimates based on the updated mass estimators, we investigate the M BH − σ * relation of NLS1s in comparison with broad-line AGNs. We find no strong evidence that the NLS1s deviates from the M BH − σ * relation, which is defined by reverberation-mapped type 1 AGNs and quiescent galaxies. However, there is a clear trend of the offset with the host galaxy morphology, i.e., more inclined galaxies toward the line-of-sight have higher stellar velocity dispersion, suggesting that the rotational broadening plays a role in measuring stellar velocity dispersion based on the single-aperture spectra from the Sloan Digital Sky Survey. In addition, we provide the virial factor log f = 0.05 ± 0.12 (f = 1.12), for M BH estimators based on the FWHM of Hβ, by jointly fitting the M BH − σ * relation using quiescent galaxies and reverberation-mapped AGNs.

To investigate the validity of the assumption that quiescent galaxies and active galaxies follow the same black hole mass (M BH )-stellar velocity dispersion (σ * ) relation, as required for the calibration of M BH estimators for broad line AGNs, we determine and compare the M BH -σ * relations, respectively, for quiescent and active galaxies. For the quiescent galaxy sample, composed of 72 dynamical M BH measurements, we update σ * for 28 galaxies using homogeneous H-band measurements that are corrected for galaxy rotation. For active galaxies, we collect 25 reverberation-mapped AGNs and improve σ * measurement for two objects . Combining the two samples, we determine the virial factor f , first by scaling the active galaxy sample to the M BH -σ * relation of quiescent galaxies, and second by simultaneously fitting the quiescent and active galaxy samples, as f = 5.1 +1.5 −1.1 and f = 5.9 +2.1 −1.5 , respectively. The M BH -σ * relation of active galaxies appears to be shallower than that of quiescent galaxies. However, the discrepancy is caused by a difference in the accessible M BH distribution at given σ * , primarily due to the difficulty of measuring reliable stellar velocity dispersion for the host galaxies of luminous AGNs. Accounting for the selection effects, we find that active and quiescent galaxies are consistent with following intrinsically the same M BH -σ * relation.

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