DOE OSTI2012
We present both phenomenological and more physical photoionization models of the Chandra/HETG spectra of the Seyfert-1 active galactic nucleus NGC 4051. We detect 40 absorption and emission lines, encompassing highly ionized charge states from O, Ne, Mg, Si, S, and the Fe L-shell and K-shell. Two independent photoionization packages, XSTAR and Cloudy, were both used to self-consistently model the continuum and line spectra. These fits detected three absorbing regions in this system with densities ranging from 10{sup 10} to 10{sup 11} cm{sup -3}. In particular, our XSTAR models require three components that have ionization parameters of log ({xi}) = 4.5, 3.3, and 1.0, and are located within the broad-line region at 70, 300, and 13000 R{sub g} , respectively, assuming a constant wind density. Larger radii are inferred for density profiles which decline with radius. The Cloudy models give a similar set of parameters with ionization parameters of log ({xi}) = 5.0, 3.6, and 2.2 located at 40, 200, and 3300 R{sub g} . We demonstrate that these regions are outflowing from the system, and carry a small fraction of material out of the system relative to the implied mass accretion rate. The data suggest that magnetic fields may be an important driving mechanism.
79 ASTRONOMY AND ASTROPHYSICS↗