3 Results

In Fig. 3 we have plotted the $FWHM{\rm s}$ (corrected for the instrumental broadening) of each individual component, i.e. of each set of lines used to fit the blue and red spectra, as listed in Table 6 (Cols. 5 and 10, respectively). The good correlation found between the blue and red $FWHM{\rm s}$ gives confidence in the fitting analysis.

Figure 4 shows the log($\lambda 5007/{\rm H}\beta$) vs. log($\lambda 6583/{\rm H}\alpha$) and log($\lambda 5007/{\rm H}\beta$) vs. log($\lambda 6300/{\rm H}\alpha$) diagrams traditionally used to classify nuclear emission-line regions into H II regions, Liners or Seyfert 2s. We have delimited in the two diagrams three regions, each corresponding to one of these classes. In Figs. 4a and 4b we have plotted all objects for which line ratios are available in the literature and which are unambiguously classified as H II regions (crosses), Seyfert 2s (open circles) or Liners (open squares); we have also plotted the 61 observed objects suspected of having a "transition'' spectrum (filled circles): they fall, at least in one of the diagrams, in a "zone of avoidance'', i.e. outside the regions arbitrary assigned to the classical emission-line regions. In Figs. 4c and 4d, which are the same as 4a and 4b respectively, we have plotted the individual components used to fit the spectra, as given in Table 6.

 

Figure 3:  FWHM of all the individual line-components measured on the red spectra vs. the FWHM of the individual components measured on the blue spectra

 

Figure 4:  Diagnostic diagrams showing the log($\lambda 5007/{\rm H}\beta$) vs. log($\lambda 6583/{\rm H}\alpha$) - boxes a) and c) - and log($\lambda 5007/{\rm H}\beta$) vs. log($\lambda 6300/{\rm H}\alpha$) - boxes b) and d). H II regions are represented by crosses, Seyfert 2 galaxies by open circles, and Liners by open squares. In a) and b), filled circles represent "transition objects'', i.e. objects which, in at least one of the diagrams, fall outside the arbitrarily delimited regions assigned to H II regions, Seyfert 2s and Liners. In c) and d) we plotted the individual components. The symbols are the same as in the upper panels; open triangles represent objects which could not be classified ("?'' in Table 6)

It is apparent that most of the "transition objects'' belong to one of the three following categories:

1.

A few objects fall into the "zones of avoidance'' only because they have inaccurate published line ratios, appearing to be "normal'' when more accurate measurements are obtained; this is the case, for instance, for IRAS 04507+0358, KUG 0825+248, NGC 2989, CG 49 and Arp 107A.

2.

A few objects have Seyfert 2 spectra with abnormally weak [N II] lines. They constitute a rare but interesting class of objects which is further discussed below.

3.

Most "transition'' spectra turn out to be "composite'', due to the simultaneous presence on the slit of a H II region and a Seyfert 2 nebulosity. We have observed 70% of all the objects in an unbiased sample of galaxies displaying a "transition'' nuclear spectrum. Modeling of the data revealed that most of them have in fact a "composite'' spectrum, suggesting that genuine "transition objects'' do not exist at all. However, in a few cases such as NGC 3185, Mark 1291, IRAS 12474+4345S, Mark 266SW or IRAS 15184+0834, we cannot prove that the spectra are "composite''; the classification is ambiguous. Further studies are needed to find out the true nature of these "transition objects''.

Figure 5 is the histogram of the parameter log ($\lambda$6300/$\lambda$5007) for 159 Seyfert 2s and Liners after correction of the line fluxes for reddening, assuming that the intrinsic Balmer decrement is $\rm H\alpha$/$\rm H\beta$ = 3.1 (Osterbrock & Dahari 1983) (Binette et al. 1990, suggested an even higher value for the intrinsic Balmer decrement in AGNs: $\rm H\alpha$/$\rm H\beta$ = 3.4). The histogram has two main peaks showing a clear separation between strong [O III]$\lambda 5007/$ objects (Seyfert 2s) and weak [O III]$\lambda 5007/$ objects (Liners). Although our sample is heterogeneous and incomplete, this suggests that there is no continuity between the two classes of objects. Heckman (1980) originally defined Liners as objects with $\lambda 6300/\lambda 5007$ > 0.33; it seems that $\lambda 6300/\lambda 5007$ > 0.25 would be a more realistic definition, as the observed distribution of this ratio really shows a minimum centered around this value.

 

Figure 5:  Histogram of log($\lambda 6300/\lambda 5007$) for the 159 Seyfert 2 and Liners plotted in Fig. 4

According to Ho et al. (1997a), the separation between the two principal ionization sources (young stars vs. AGNs) and between the two AGN excitation classes (Seyfert 2 vs. Liners) does not have sharp, rigorously defined boundaries. Figure 4 shows that this is not the case. In fact, the three areas containing the H II regions, the Seyfert 2s and the Liners are clearly separated; almost every "transition object'' turns out to be "composite'' when observed with sufficient resolution.

Several authors had already suspected this to be the case. Kennicutt et al. (1989) and Ho et al. (1997c) have shown that the distribution of H II nuclei in the $\lambda 5007/{\rm H}\beta$ vs. $\lambda$6583/$\rm H\alpha$ plane parallels the disk H II region sequence, the most striking feature being a clear offset between the two classes of objects, the H II nuclei having larger $\lambda 6583/{\rm H}\alpha$ ratios for the same excitation; this effect could be due to the presence of a weak active nucleus in many of these galaxies. Binette (1985) also suggested that mixed cases of starburst and Liner spectra might be relatively common, providing a possible interpretation for objects which have an unusually strong $\lambda 6300/{\rm H}\alpha$ ratio compared to H II regions (NGC 3994, for example). Filippenko & Terlevich (1992) suggested that Liners with weak [O I] emission ($\lambda 6300/{\rm H}\alpha$ < 1/6) might be powered by hot main-sequence stars; however, Ho et al. (1993a) showed that these objects are most probably "composite''.

Ho et al. (1993b) reported the discovery of a non random trend in the dispersion of emission-line intensity ratios for Seyfert 2s. $\lambda 6300/{\rm H}\alpha$ and $\lambda 6583/{\rm H}\alpha$ were found to be correlated with $\lambda 5007/{\rm H}\beta$, suggesting the influence of a single underlying physical parameter - the hardness of the ionizing continuum. Our data do not show these correlations, which could be artifacts due to the inclusion in the sample of "composite'' spectra.

Examination of Fig. 4 shows that the points representative of Seyfert 2 galaxies are not distributed at random in the region assigned to them. Figure 6 is the histogram of the quantity log($\lambda 6583/{\rm H}\alpha$); it shows a sharp maximum at $\sim$ -0.05, with broad wings. Our sample of (131) Seyfert 2 galaxies is not complete in any sense and this could therefore be due to observational biases although this seems unlikely, as the $\lambda 6583/{\rm H}\alpha$ ratio is not used for finding Seyfert 2 galaxies. We have no explanation for this fact.

 

Figure 6:  Histogram of log($\lambda$6583/$\rm H\alpha$) for the 131 Seyfert 2 galaxies plotted in Fig. 4