We present modeling to explore the conditions of the broad-line emitting gas in two extreme Narrow-line Seyfert 1 galaxies , using the observational results described in the first paper of this series .
Photoionization modeling using Cloudy was conducted for the broad , blueshifted wind lines and the narrow , symmetric , rest-wavelength-centered disk lines separately .
A broad range of physical conditions were explored for the wind component , and a figure of merit was used to quantitatively evaluate the simulation results .
Of the three minima in the figure-of-merit parameter space , we favor the solution characterized by an X-ray weak continuum , elevated abundances , a small column density ( \log ( N _ { H } ) \approx 21.4 ) , relatively high ionization parameter ( \log ( U ) \approx - 1.2 – -0.2 ) , a wide range of densities ( \log ( n ) \approx 7 – 11 ) , and a covering fraction of \sim 0.15 .
The presence of low-ionization emission lines implies the disk component is optically thick to the continuum , and the Si iii ] /C iii ] ratio implies a density of 10 ^ { 10 } – 10 ^ { 10.25 } cm ^ { -3 } .
A low ionization parameter ( \log ( U ) = -3 ) is inferred for the intermediate-ionization lines , unless the continuum is “ filtered ” through the wind before illuminating the intermediate-line emitting gas , in which case \log ( U ) = -2.1 .
The location of the emission regions was inferred from the photoionization modeling and a simple “ toy ” dynamical model .
A large black hole mass ( 1.3 \times 10 ^ { 8 } M _ { \odot } ) radiating at 11 % of the Eddington luminosity is consistent with the kinematics of both the disk and wind lines , and an emission radius of \sim 10 ^ { 4 } R _ { S } is inferred for both .
We compare these results with previous work and discuss implications .