6.2. The Narrow Line Region
The observations of narrow lines in high luminosity AGNs are not nearly as
good as those of the broad lines. In particular, it is difficult to
separate the broad and the narrow ultraviolet lines and there are no
reliable measurements of the
narrow CIV1549
and CIII]
1909
lines in quasars and Seyfert 1 galaxies. The
situation is likely to be improved with the HST observations but so far
the only
narrow ultraviolet lines that have been measured are in Seyfert 2 galaxies.
There are very good observations of optical narrow lines that can be
compared with the model predictions. The overall agreement is very good and
narrow line models, like the one shown in
Fig. 12, reproduce the relative
strength
of [OIII]5007,
[OII]
3727,
[OI]
6300 and
H
quite well. This is not the case
for [FeX]
6734,
and the line is observed to be much stronger than predicted. A
similar, although somewhat smaller discrepancy, occurs for the lines of
[NeV] and [FeVII].
Line profile observations (chapter 9) indicate a large density gradient in the NLR. The validity of the model in Fig. 12, where the density gradient is quite small, is thus questionable and the very high ionization lines may come from a much denser part of the NLR. Another, very different suggestion is that the high ionization lines come from the interstellar medium of the host galaxy.
Lower excitation spectra, such as in LINERs, cannot be explained by the relatively high ionization parameter model of Fig. 12. Such spectra are discussed in chapter 11.
The intensity of the narrow Balmer lines are easy to calculate. The
H
optical depth is not likely to be large, and the
H
/
H
ratio is closed to the Case B value. A comparison with the theoretical
L
intensity is
somewhat less
reliable. First, the line is likely to be collisionally excited by a
density dependent
amount. In addition, the typical NLR density is close to the critical
density of the 2-photon transition (~ 1.5 × 104
cm-3) and the relative population of the
hydrogen 2s and 2p levels may be different in different
clouds. Because of this the recombination
L
/
H
ratio can vary from about 23 (low density limit,
the 2s and 2p levels are not coupled) to 34 (high density
limit, the 2s to 2p
population ratio is 1:3). Combined with the collisional enhancement of
L
, the
overall expected range in the
L
/
H
ratio is about 25-100. Accurate modeling
is required for comparing this line ratio with the observations.