| Issue |
A&A
Volume 563, March 2014
|
|
|---|---|---|
| Article Number | A119 | |
| Number of page(s) | 16 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/201321989 | |
| Published online | 19 March 2014 | |
Online material
Appendix A: Spectral modeling
In this appendix we report the result of modeling the objects where the BLR is not clearly visible in their spectra. For four galaxies, the spectra cover the [O I] spectral region, and these lines are bright enough to allow us to use them as templates. In these cases, we modeled the spectra with three different methods 1) by using the [O I] lines as templates and including a broad
 |
Fig. A.1
Modeling of the spectra of 4 objects without a readily visible BLR modeled with 3 different methods: by using the [O I] lines as templates and including a broad Hα component (left column), again with the [O I] template but adding a wing to the [N II] and narrow Hα lines (center column), by using as template the [S II] lines and including a BLR (right column). The original spectrum is in black, the contribution of the individual narrow lines in blue (their sum is in green), and in red are the residuals. The BLR component is in red. |
| Open with DEXTER | |
Hα component; 2) by using the [O I] template but adding a wing to the [N II] and narrow Hα lines and 3) by using the [S II] lines as template and including a BLR. For the eight remaining galaxies, the spectra do not cover the [O I] spectral region or these lines are not bright enough to be used as templates. In these cases we modeled the spectra with two different methods by using the [S II] lines as templates and 1) including a broad Hα component or 2) adding a wing to the [N II] and narrow Hα lines.
 |
Fig. A.2
Analysis of the spectra 8 objects without a clear BLR and not covering the [O I] region (or with faint [O I] lines). Each spectrum is modeled with 2 methods, always using the [S II] lines as templates and (left) including a broad Hα component (right) or adding a wing to the [N II] and narrow Hα lines. The original spectrum is in black, the contribution of the individual narrow lines in blue (their sum is in green), and the residuals in red. In red we also show either the BLR component or the wings’ contribution. |
| Open with DEXTER | |
© ESO, 2014
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