We present inferences on the geometry and kinematics of the broad-H \beta line-emitting region in four active galactic nuclei monitored as a part of the fall 2010 reverberation mapping campaign at MDM Observatory led by the Ohio State University .
From modeling the continuum variability and response in emission-line profile changes as a function of time , we infer the geometry of the H \beta -emitting broad line regions to be thick disks that are close to face-on to the observer with kinematics that are well-described by either elliptical orbits or inflowing gas .
We measure the black hole mass to be \log _ { 10 } ( M _ { BH } ) ~ { } = ~ { } 7.25 ^ { +0.10 } _ { -0.10 } for Mrk 335 , 7.86 ^ { +0.20 } _ { -0.17 } for Mrk 1501 , 7.84 ^ { +0.14 } _ { -0.19 } for 3C 120 , and 6.92 ^ { +0.24 } _ { -0.23 } for PG 2130+099 .
These black hole mass measurements are not based on a particular assumed value of the virial scale factor f , allowing us to compute individual f factors for each target .
Our results nearly double the number of targets that have been modeled in this manner , and investigate the properties of a more diverse sample by including previously modeled objects .
We measure an average scale factor \bar { f } in the entire sample to be log _ { 10 } \bar { f } = 0.54 ~ { } \pm~ { } 0.17 when the line dispersion is used to characterize the line width , which is consistent with values derived using the normalization of the M _ { BH } – \sigma relation .
We find that the scale factor f for individual targets is likely correlated with the black hole mass , inclination angle , and opening angle of the broad line region but we do not find any correlation with the luminosity .