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Journal Articles Astronomy and Astrophysics - A&A Year : 2013

Multiwavelength campaign on Mrk 509. XI. Reverberation of the Fe Kα line

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G. Ponti
  • Function : Author
M. Cappi
  • Function : Author
E. Costantini
  • Function : Author
S. Bianchi
J. S. Kaastra
  • Function : Author
B. de Marco
  • Function : Author
R. P. Fender
  • Function : Author
G. A. Kriss
  • Function : Author
K. C. Steenbrugge
  • Function : Author
N. Arav
  • Function : Author
E. Behar
  • Function : Author
G. Branduardi-Raymont
  • Function : Author
M. Dadina
  • Function : Author
J. Ebrero
  • Function : Author
P. Lubiński
  • Function : Author
M. Mehdipour
S. Paltani
C. Pinto
  • Function : Author
F. Tombesi
  • Function : Author

Abstract

Context. We report on a detailed study of the Fe K emission/absorption complex in the nearby, bright Seyfert 1 galaxy Mrk 509. The study is part of an extensive XMM-Newton monitoring consisting of 10 pointings (~60 ks each) about once every 4 days, and includes a reanalysis of previous XMM-Newton and Chandra observations.
Aims: We aim at understanding the origin and location of the Fe K emission and absorption regions.
Methods: We combine the results of time-resolved spectral analysis on both short and long time-scales including model-independent rms spectra.
Results: Mrk 509 shows a clear (EW = 58 ± 4 eV) neutral Fe Kα emission line that can be decomposed into a narrow (σ = 0.027 keV) component (found in the Chandra HETG data) plus a resolved (σ = 0.22 keV) component. We find the first successful measurement of a linear correlation between the intensity of the resolved line component and the 3-10 keV flux variations on time scales of years down to a few days. The Fe Kα reverberates the hard X-ray continuum without any measurable lag, suggesting that the region producing the resolved Fe Kα component is located within a few light days to a week (r ≲ 103rg) from the black hole (BH). The lack of a redshifted wing in the line poses a lower limit of ≥40 rg for its distance from the BH. The Fe Kα could thus be emitted from the inner regions of the BLR, i.e. within the ~80 light days indicated by the Hβ line measurements. In addition to these two neutral Fe Kα components, we confirm the detection of weak (EW ~ 8-20 eV) ionised Fe K emission. This ionised line can be modelled with either a blend of two narrow Fe xxv and Fe xxvi emission lines (possibly produced by scattering from distant material) or with a single relativistic line produced, in an ionised disc, down to a few rg from the BH. In the latter interpretation, the presence of an ionised standard α-disc, down to a few rg, is consistent with the source high Eddington ratio. Finally, we observe a weakening/disappearing of the medium- and high-velocity high-ionisation Fe K wind features found in previous XMM-Newton observations.
Conclusions: This campaign has made the first reverberation measurement of the resolved component of the Fe Kα line possible, from which we can infer a location for the bulk of its emission at a distance of r ~ 40-1000 rg from the BH.
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Dates and versions

insu-03617536 , version 1 (24-03-2022)

Licence

Attribution - CC BY 4.0

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G. Ponti, M. Cappi, E. Costantini, S. Bianchi, J. S. Kaastra, et al.. Multiwavelength campaign on Mrk 509. XI. Reverberation of the Fe Kα line. Astronomy and Astrophysics - A&A, 2013, 549, ⟨10.1051/0004-6361/201219450⟩. ⟨insu-03617536⟩
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