This book presents timely work on the nature of the physical
processes underpinning two of the basic characteristics of the gas
structure in the innermost region of Active Galactic Nuclei (AGN):
ionized outflows and emission line regions. In addition, it
describes physics-based methods for estimating the density of the
astrophysical plasma surrounding AGN. All numerical computations of
the photoionized gas employ the most advanced codes available
(CLOUDY and TITAN). Calculations of the radiative transfer are
based on the assumption of thermal and ionization equilibrium.
Promising preliminary examples of comparison with current
observations are included for several individual AGN. All of them
suggest that the absorbing/emitting gas should have a density on
the order of 1012 cm-3. Future observations will provide more
objects to verify these results, and will allow us to put
constraints on the launch radius of ionized outflows and therefore
on the mass loading and kinetic energy outflow rates. These rates,
in turn, are crucial to estimating whether the outflows have a
significant feedback impact on star formation and metal enrichment
in the interstellar medium of the host galaxy. In closing, the book
discusses a representative example of applying powerful
photoionization techniques to explain the complex physics of the
AGN environment.
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