Super-Eddington QSO RX J0439.6−5311 – I. Origin of the soft X-ray excess and structure of the inner accretion flow
Jin, C.; Done, C.; Ward, M.
Professor Christine Done firstname.lastname@example.org
We report the results from a recent 133 ks XMM–Newton observation of a highly super-Eddington narrow-line Type-1 quasi-stellar object RX J0439.6−5311. This source has one of the steepest active galactic nuclei hard X-ray slopes, in addition to a prominent and smooth soft X-ray excess. Strong variations are found throughout the 0.3–10 keV energy range on all time-scales covered by the observation, with the soft excess mainly showing low-frequency (LF) variations below 0.1 mHz while the hard X-rays show stronger variability at higher frequencies. We perform a full set of spectral-timing analysis on the X-ray data, including a simultaneous modelling of the time-averaged spectra, frequency-dependent root-mean-square and covariance spectra, lag-frequency and lag-energy spectra. Especially, we find a significant time-lag signal in the LF band, which indicates that the soft X-rays lead the hard by ∼4 ks, with a broad continuum-like profile in the lag spectrum. Our analysis strongly supports the model where the soft X-ray excess is dominated by a separate low temperature, optically thick Comptonization component rather than relativistic reflection or a jet. This soft X-ray emitting region is several tens or hundreds of Rg away from the hot corona emitting hard X-rays, and is probably associated with a geometrically thick (‘puffed-up’) inner disc region.
Jin, C., Done, C., & Ward, M. (2017). Super-Eddington QSO RX J0439.6−5311 – I. Origin of the soft X-ray excess and structure of the inner accretion flow. Monthly Notices of the Royal Astronomical Society, 468(3), 3663-3681. https://doi.org/10.1093/mnras/stx718
|Journal Article Type||Article|
|Acceptance Date||Mar 21, 2017|
|Online Publication Date||Mar 23, 2017|
|Publication Date||Mar 23, 2017|
|Deposit Date||Jul 24, 2017|
|Publicly Available Date||Jul 26, 2017|
|Journal||Monthly Notices of the Royal Astronomical Society|
|Publisher||Royal Astronomical Society|
|Peer Reviewed||Peer Reviewed|
Published Journal Article
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2017. The Authors.<br /> Published by Oxford University Press on behalf of the Royal Astronomical Society.
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