  We analyze the hydrostatic effect of AGN radiation pressure on optically
thick gas in the host galaxy. We show that in luminous AGN, the radiation
pressure likely confines the ionized layer of the illuminated gas. Radiation
pressure confinement (RPC) has two main implications. First, the gas density
near the ionization front is 7x10^4 L_{i,45} r_{50}^{-2} cm^{-3}, where
L_{i,45} is the ionizing luminosity in units of 10^45 erg/s and r_{50} is the
distance of the gas from the nucleus in units of 50 pc. Second, as shown by
Dopita et al., the solution of the ionization structure within each slab is
unique, independent of the ambient pressure. We show that the RPC density vs.
distance relation is observed over a dynamical range of ~10^4 in distance, from
sub-pc to kpc from the nucleus, and a range of ~10^8 in gas density, from 10^3
to 10^11 cm^{-3}. This relation implies that the radiative force of luminous
AGN can compress giant molecular clouds in the host galaxy, and possibly affect
the star formation rate. The unique ionization structure in RPC includes a
highly ionized X-ray emitting surface, an intermediate layer which emits
coronal lines, and a lower ionization inner layer which emits optical lines.
This structure can explain the observed overlap of the extended X-ray and
optical narrow line emission in nearby AGN. We further support RPC by comparing
the predicted ratios of the narrow lines strength and narrow line widths with
available observations. We suggest a new method, based on the narrow line
widths, to estimate the black hole mass of low luminosity AGN.
