Free Access
Issue
A&A
Volume 567, July 2014
Article Number A142
Number of page(s) 15
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201322701
Published online 31 July 2014

Online material

Appendix A: X-ray spectral results

In Tables A.1 and A.2 we report the results of the spectral fitting described in Sect. 3 for our XMM-Newton/EPIC sample.

Table A.1

Results of the spectral fits of the XMM-Newton observations of our sample.

Table A.2

Results of the spectral fits of the XMM-Newton observations of our sample.

Appendix B: Notes on the individual sources

In the following we report the details on the emission lines added to the best fits. IC 4329a – II. A narrow (σ = 1 eV) emission feature is detected in the spectrum. The narrow line is found at  keV ( eV), and is likely to be Fe XXVI. NGC 4151 – I. The spectrum shows evidence of three narrow emission features at low energies. These features were fitted using Gaussian emission lines at  keV ( eV),  keV ( eV) and  keV ( eV). These lines are consistent with O VII, Ne IX, and Mg XI, respectively. NGC 4151 – II. Three narrow emission features at low energies are detected. The narrow lines were found to be at  keV ( eV),  keV ( eV), and  keV ( eV), and they are consistent with O VII, Ne IX, and Mg XI, respectively. NGC 4151 – III. Three narrow emission features at low energies are detected. The three lines are at  keV ( eV),  keV ( eV), and  keV ( eV), and they are consistent with O VII, Ne IX, and Mg XI, respectively. NGC 4151 – IV. Two narrow emission features at low energies are detected. The narrow features are found at  keV ( eV), and  keV ( eV), and they are consistent with O VII and Ne IX, respectively. NGC 4151 – V. Two narrow emission features at low energies are detected. The narrow features are located at  keV ( eV), and  keV ( eV), and they are consistent with O VII and Ne IX, respectively. NGC 4151 – VI. Two narrow emission features at  keV ( eV) and  keV ( eV) are detected. The two lines are consistent with O VII and Ne IX, respectively. NGC 4151 – VII. Five narrow emission features at low energies are detected. The energies of the narrow lines are  keV ( eV),  keV ( eV),  keV ( eV), keV ( eV), and keV ( eV). These lines are consistent with being due to O VII, Ne IX, Mg XI, Si XIII, and to Fe XXVI, respectively.

NGC 4151 – VIII. Three narrow emission features at low energies are detected. The narrow lines have energies of  keV ( eV),  keV ( eV), and  keV ( eV), and are consistent with O VII, Ne IX, and Si XIII, respectively. PG 0050+124 - I. The spectrum requires an additional line at keV, likely due to Fe XXVI, with an equivalent width EW = 106 ± 24 eV. PG 0050+124 - II. Besides the Fe XXVI line at keV (EW = 56 ± 13 eV), we found evidence of another unresolved ionised iron line (likely Fe XXV) at keV (). PG 1116+215 – I. Two lines at 6.7 keV () and 6.97 keV () are needed. The lines are consistent with being produced by emission of ionised iron (Fe XXV and Fe XXVI, respectively). PG 1116+215 – III. Two lines at 6.7 keV () and 6.97 keV () are needed. The two lines are consistent with being produced by emission of ionised iron (Fe XXV and Fe XXVI, respectively). PG 1126041 – I. Two emission lines at low energies were also needed. The lines are located at E = 0.56 ± 0.01 keV () and E = 0.90 ± 0.02 keV (), and are consistent with being due to O VII and Ne IX, respectively. PG 1126041 – II. Two emission lines at E = 0.60 ± 0.03 keV () and E = 0.89 ± 0.03 keV (EW ≤ 280 eV) are also needed. The lines are consistent with being due to O VII and Ne IX, respectively. PG 1126041 – III. The spectrum shows an additional emission line at E = 0.60 ± 0.02 keV (), consistent with the O VII line. PG 1126041 – IV. Two lines at low energy were also found. The line at E = 0.58 ± 0.01 keV (), is likely due to O VII emission, while that at E = 0.93 ± 0.02 keV () is consistent with being Ne IX. Another emission line at (EW=), consistent with being the He β form of Fe XXV, was also found. PG 1229+204. An emission line at E = 6.72 ± 0.05 keV (), consistent with being due to the He α state of Fe XXV, is required. PG 1440+356 – II . An emission line at E = 6.72 ± 0.09 keV () was detected, and is likely the He α form of Fe XXV. PG 1440+356 – III. The spectrum shows evidence of emission due to the He α form of Fe XXV at E = 6.73 ± 0.10 keV (EW = 106 ± 41 eV). PG 1440+356 – IV. We found evidence of an emission feature at E = 6.79 ± 0.07 keV (EW = 197 ± 48 eV), which is probably due to the Heα state of Fe XXV.


© ESO, 2014

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