Computer Science
Scientific paper
Jun 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009phdt.........3a&link_type=abstract
Proquest Dissertations And Theses 2009. Section 0043, Part 0606 244 pages; [Ph.D. dissertation].United States -- District of Co
Computer Science
X-Ray Absorption, Active Galactic Nuclei, Absorber Ionization
Scientific paper
I present the results of spectral analysis and modeling of nine Chandra and XMM-Newton X-ray observations of NGC 4151, spanning the period 2000-2007. The complex and highly variable spectrum is characterized by attenuation of the intrinsic power-law continuum by nested absorption components, which contribute both broadband curvature in the 1-5 keV continuum, and individual line absorption. Significant and variable narrow line emission and radiative recombination continua dominate energies below ~1.5 keV. The modeling process made extensive use of absorption tables produced by a newly-available Cloudy- XSPEC interface. Observed spectral evolution could not be explained entirely by simple changes in absorber ionization states in response to variations in the level of incident continuum, but required additional variations in absorber column densities. This fact implies transverse motion of the absorbers across the line of sight. The transverse velocity, coupled with observed absorber outflow determined from line energies, suggest a possible helical motion for the absorbers. Scattered incident continuum flux was also indicated. Model results predict that the absorbers may also serve as substantial emitters of observed soft X-ray narrow line emission. However, additional emission components, not represented by absorbers, were required. Narrow emission line modeling of a single observation required three separate components, two of which may be represented by model absorbers. A strong Fe Ka fluorescent line was present in all observations, with highly-variable equivalent width. While photoionization model results predicted contributions to Fe Ka line flux by all absorbers, the absorber contributions to emission were minor. High-energy feature analysis revealed the presence of an additional, highly-ionized absorber in at least one observation.
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