The two-dimensional distribution and kinematics of the molecular , ionized , and highly ionized gas in the nuclear regions of Seyfert 1 galaxies have been measured using high spatial resolution ( \sim 0 ^ { \prime \prime } .09 ) near-infrared spectroscopy from NIRSPEC with adaptive optics on the Keck telescope .
Molecular hydrogen , H _ { 2 } , is detected in all nine Seyfert 1 galaxies and , in the majority of galaxies , has a spatially resolved flux distribution .
In contrast , the narrow component of the Br \gamma emission has a distribution consistent with that of the K -band continuum .
In general , the kinematics of the molecular hydrogen are consistent with thin disk rotation , with a velocity gradient of over 100 km s ^ { -1 } measured across the central 0 ^ { \prime \prime } .5 in three galaxies , and a similar gradient across the central 1 ^ { \prime \prime } .5 in an additional two galaxies .
The kinematics of Br \gamma are in agreement with the H _ { 2 } rotation , except that in all four cases the central 0 ^ { \prime \prime } .5 is either blue- or redshifted by more than 75 km s ^ { -1 } .
The highly ionized gas , measured with the [ Ca VIII ] and [ Si VII ] coronal lines , is spatially and kinematically consistent with Br \gamma in the central 0 ^ { \prime \prime } .5 .
In addition , the velocity dispersion of both the coronal and Br \gamma emission is greater than that of H _ { 2 } ( by 1.3-2.0 times ) , suggesting that both originate from gas that is located closer to the nucleus than the H _ { 2 } line emitting gas .
Dynamical models have been fitted to the two-dimensional H _ { 2 } kinematics , taking into account the stellar mass distribution , the emission line flux distribution , and the point spread function .
For NGC 3227 the modeling indicates a black hole mass of M _ { BH } =2.0 ^ { +1.0 } _ { -0.4 } \times 10 ^ { 7 } M _ { \odot } , and for NGC 4151 M _ { BH } =3.0 ^ { +0.75 } _ { -2.2 } \times 10 ^ { 7 } M _ { \odot } .
In NGC 7469 the best fit model gives M _ { BH } < 5.0 \times 10 ^ { 7 } M _ { \odot } .
In all three galaxies , modeling suggests a near face-on disk inclination angle , which is consistent with the unification theory of active galaxies .
The direct black hole mass estimates verify that masses determined from the technique of reverberation mapping are accurate to within a factor of three with no additional systematic errors .