| Issue |
A&A
Volume 532, August 2011
|
|
|---|---|---|
| Article Number | A102 | |
| Number of page(s) | 20 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/201016409 | |
| Published online | 02 August 2011 | |
Online material
Appendix A: List of sources
In the following, we list the coordinates, redshifts, detection significances, count rates, column densities, and luminosities of the samples of Seyfert 1s (Table A.1), Seyfert 1.5s (A.2), Compton-thin Seyfert 2s (A.3), CT Seyfert 2s (A.4), and NLS1s (A.5) used for the stacking analysis.
Coordinates, redshifts, detection significances, count rates, column densities, and luminosities of the Seyfert 1s used for the stacking analysis.
Coordinates, redshifts, detection significances, count rates, column densities, and luminosities of the Seyfert 1.5s used for the stacking analysis.
Coordinates, redshifts, detection significances, count rates, column densities, and luminosities of the Seyfert 2s used for the stacking analysis.
Coordinates, redshifts, detection significances, count rates, column densities, and luminosities of the Compton-thick Seyfert 2s used for the stacking analysis.
Coordinates, redshifts, detection significances, count rates, column densities, and luminosities of the Narrow Lines Seyfert 1s used for the stacking analysis.
Appendix B: Spectra
In Fig. B.1, we show the average 17–250 keV spectra of Seyfert 1s, Seyfert 1.5s, Seyfert 2s, CT Seyfert 2s, and NLS1s. The parameters of the models used for the fit are reported in Table 3. In Fig. B.2, we show the average spectra of MOB and LOB Seyfert 2s. The parameters of the models are reported in Table 4.
 |
Fig. B.1
Spectra of different classes of AGN obtained using the pexrav model. We also show the contributions to the χ2 relative to the best fits. The results of the spectral analysis are reported in Table 3. |
| Open with DEXTER | |
 |
Fig. B.2
Spectra of MOB (left panel) and LOB (right panel) Seyfert 2s, the model used is a cutoff power law plus a reflection component from neutral matter (pexrav). The results of the analysis are reported in Table 4. |
| Open with DEXTER | |
© ESO, 2011
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