  We present inferences on the geometry and kinematics of the broad-Hbeta
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 Hbeta- 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
(MBH) = 7.25 (+/-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 f in
the entire sample to be log10(f) = 0.54 +/- 0.17 when the line dispersion is
used to characterize the line width, which is consistent with values derived
using the normalization of the MBH-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.
