Activity driven by mass accretion onto supermassive black holes
differs in many ways from star-formation activity. The thermal and
non-thermal processes associated with the accretion disk and its
surroundings (e.g., corona) are at the origin of the "hard" ionizing
continuum detected in quasars and AGNs (e.g.,
Krolik 1999).
Material in the vicinity of the nucleus will bear the imprint of this strong
radiation field. The deep gravitational potential at the center of
these galaxies allows the presence of high-density
( 109
cm-3), high-velocity
(
2000 km
s-1) gas clouds in the
inner parsec of quasars and AGNs. This so-called broad-line region or
BLR is a powerful diagnostic of nuclear activity in galaxies. The
main signatures of the BLRs are broad recombination lines which are
unaffected by the effects of collisional de-excitation at high
densities. Two general methods have been used in the past to detect
BLRs in galaxies: direct spectroscopy and spectropolarimetry. This
last method relies on the presence of dust or electrons ("mirrors")
to scatter the BLR signature towards the line of sight (e.g.,
Antonucci 1993).
Direct spectroscopy searches for the presence of the
broad recombination lines at wavelengths where the effects of dust
extinction are reduced. As shown in Table 1 for
representative Galactic extinction (see, e.g.,
Cardelli, Clayton, &
Mathis 1989;
Draine & Lee 1984;
Draine 1989;
Lutz et al. 1996;
Lutz 1999),
great increase in sensitivity can in principle be obtained by observing at
longer wavelengths.
![]() | ![]() ![]() ![]() ![]() | NH(cm-2) @
![]() ![]() |
Ly![]() | 2.0 - 4.5 | 0.5 - 1.0 × 1021 |
V band 5500 Å | 1.2 | 1.7 × 1021 |
H![]() | 1.0 | 2.2 × 1021 |
J band 1.25 µm | 1/3 | 6.1 × 1021 |
H band 1.65 µm | 1/4.5 | 9.8 × 1021 |
K band 2.2 µm | 1/7 | 1.6 × 1022 |
L band 3.4 µm | 1/15 | 3.4 × 1022 |
M band 5.0 µm | 1/30 | 6.4 × 1022 |
N band 10 µm | 1/15 | 3.2 × 1022 |
12 µm | 1/30 | 6.2 × 1022 |
25 µm | 1/60 | 1.3 × 1023 |
60 µm | 1/400 | 8.6 × 1023 |
100 µm | 1/700 | 1.5 × 1024 |
In highly obscured objects with NH
1024
cm-2,
direct detection of the BLRs becomes very difficult and one has to
rely on spectropolarimetry to search for the presence of a BLR. The
obscuring screen may not be opaque in all directions, however. The
ionizing radiation field may be able to escape in certain directions
and ionize the surrounding material on scales beyond the obscuring
material. Distributed in the shallower portion of the gravitational
potential (~ 0.1 - 1 kpc), this "narrow-line region" or NLR is
another excellent probe of nuclear activity. The ionizing spectra of
all but the hottest O stars cut off near the He II edge (54.4 eV;
Dopita et al. 1995).
In contrast, the ionizing spectrum of AGNs
contains a relatively large fraction of high-energy photons (e.g.,
Elvis et al. 1994).
Optically thick gas clouds ionized by the hard
continuum of AGNs will present a stratified ionization structure with
(1) a highly ionized inner face (closest to the AGN), (2) a large
partially zone with characteristic fraction of ionized hydrogen
H+/H ~ 0.2 - 0.4 produced by the deposition of keV X-rays
(recall that the absorption cross sections of H0,
He0, and all
other ions decrease rapidly with increasing energy;
Osterbrock 1989),
and (3) a neutral zone facing away from the AGN. The fast free
electrons in the partly ionized zone will have a positive effect on
the strengths of low-ionization lines produced by collisional effects,
while the highly ionized conditions in the inner face will favor the
production of emission lines from ions with high ionization potentials
(e.g., Ferland &
Netzer 1983;
Ferland & Osterbrock
1986,
1987;
Binette, Wilson, &
Storchi-Bergmann 1996).
Based on these physical principles, one should choose narrow emission line diagnostics following ten basic rules or "Commandments" (a reminder of the 1700th anniversary of the adoption of Christianity as a national religion in Armenia):