Super-Eddington QSO RX J0439.6-5311 – II. Multiwavelength constraints on the global structure of the accretion flow

Jin, Chichuan; Done, Chris; Ward, M. J.; Gardner, Emma

doi:10.1093/mnras/stx1634

Cited by 53 publications

(78 citation statements)

References 133 publications

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“…Therefore, we can conclude that the UV variability is much weaker than the X-ray variability. This is very similar to that observed in several other super-Eddington NLS1s such as RX J0439.6-5311, whose optical/UV emission is also dominated by the disc emission, with MNRAS 500, 2475-2495 (2021) no intrinsic UV variability (Jin et al 2017b). But this is in contrast to some AGN with much lower Eddington ratios such as NGC 5548, where significant variability is observed in the UV/optical band, which is also correlated with the X-ray variability because of the Xray reprocessing (e.g.…”

Section: Exploring the Uv Variabilitysupporting

confidence: 88%

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Re-observing the NLS1 galaxy RE J1034+396 – II. New insights on the soft X-ray excess, QPO, and the analogy with GRS 1915+105

Jin

Done

Ward

2020

Monthly Notices of the Royal Astronomical Society

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The active galactic nucleus (AGN) RE J1034+396 displays the most significant X-ray Quasi-Periodic Oscillation (QPO) detected so far. We perform a detailed spectral-timing analysis of our recent simultaneous XMM-Newton, NuSTAR and Swift observations. We present the energy dependence of the QPO’s frequency, rms, coherence and phase lag, and model them together with the time-averaged spectra. Our study shows that four components are required to fit all the spectra. These components include an inner disc component (diskbb), two warm corona components (CompTT-1 and CompTT-2), and a hot corona component (nthComp). We find that diskbb, CompTT-2 (the hotter but less luminous component) and nthComp all contain the QPO signal, while CompTT-1 only exhibits stochastic variability. By fitting the lag spectrum, we find that the QPO in diskbb leads CompTT-2 by 679 s, and CompTT-2 leads nthComp by 180 s. By only varying the normalizations, these components can also produce good fits to the time-averaged and variability spectra obtained from previous observations when QPOs were present and absent. Our multi-wavelength study shows that the detectability of the QPO does not depend on the contemporaneous mass accretion rate. We do not detect a significant Iron Kα emission line, or any significant reflection hump. Finally, we show that the rms and lag spectra in the latest observation are very similar to the 67 Hz QPO observed in the micro-quasar GRS 1915+105. These new results support the physical analogy between these two sources. We speculate that the QPO in both sources is due to the expansion/contraction of the vertical structure in the inner disc.

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Section: Exploring the Uv Variabilitysupporting

confidence: 88%

“…This shows that the soft X-rays vary more at lower frequencies than the hard X-rays, suggesting that they originate from a more extended region (e.g. GD14; Jin, Done & Ward 2017b). The rms of the VLF variability (blue) continues this trend, but with even less variability observed above 2 keV.…”

Section: Frequency-differentiated Non-qpo Variability Spectramentioning

confidence: 76%

Re-observing the NLS1 galaxy RE J1034+396 – II. New insights on the soft X-ray excess, QPO, and the analogy with GRS 1915+105

Jin

Done

Ward

2020

Monthly Notices of the Royal Astronomical Society

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“…This would affect He II more than H I because the ionizing energy of He II is higher (see Figure 1), and so reduce the ratio between these two lines. This concept is discussed for super-Eddington AGN and shown as a cartoon in Jin et al (2017).…”

Section: Discussionmentioning

confidence: 99%

“…We extend this set of SEDs to even higher L/L Edd by including the single object RX J0439.6-5311 (Jin et al 2017). This is one of the most extreme Narrow Line Seyfert 1 galaxies (NLS1), and has an exquisitely well determined SED as there is very little interstellar extinction along this line of sight, so the continuum can be seen directly to 912Å in the rest frame (HST COS), and is visible again at 0.1 keV (ROSAT).…”

Section: Overview Of the Sedsmentioning

confidence: 99%

“…The mean equivalent widths for the four Eddington ratio groups, as measured from the sample described by Jin et al (2012a) and Jin et al (2017), are listed in the "obs" rows of Table 1. The uncertainties in the first three groups represents the ensemble average while the highest L/L Edd gives the measurement uncertainty in the single object.…”

Section: Comparison With Observationsmentioning

confidence: 99%

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State-of-the-art AGN SEDs for photoionization models: BLR predictions confront the observations

Ferland

Done

Jin

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The great power offered by photoionization models of active galactic nuclei emission line regions has long been mitigated by the fact that very little is known about the spectral energy distribution (SED) between the Lyman limit, where intervening absorption becomes a problem, and 0.3 keV, where soft X-ray observations become possible. The emission lines themselves can, to some degree, be used to probe the SED, but only in the broadest terms. This paper employs a new generation of theoretical SEDs that are internally self-consistent, energy conserving, and tested against observations, to infer properties of the emission-line regions. The SEDs are given as a function of the Eddington ratio, allowing emission-line correlations to be investigated on a fundamental basis. We apply the simplest possible tests, based on the foundations of photoionization theory, to investigate the implications for the geometry of the emission-line region. The SEDs become more far-ultraviolet bright as the Eddington ratio increases, so the equivalent widths of recombination lines should also become larger, an effect that we quantify. The observed lack of correlation between Eddington ratio and equivalent width shows that the cloud covering factor must decrease as Eddington ratio increases. This would be consistent with recent models proposing that the broad-line region is a failed dusty wind off the accretion disc.

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Accretion around black holes: The geometry and spectra

Liu

Qiao

2022

iScience

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Summary Observations of black hole X-ray binaries and active galactic nuclei indicate that the accretion flows around black holes are composed of hot and cold gas, which have been theoretically described in terms of either a hot geometrically thick corona lying above and below a cold geometrically thin disk or an inner advection dominated accretion flow connected to an outer thin disk. This article reviews the accretion flows around black holes, with an emphasis on the physics that determines the configuration of hot and cold accreting gas, and how the configuration varies with the accretion rate and thereby produces various luminosity and spectra.

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Super-Eddington QSO RX J0439.6-5311 – II. Multiwavelength constraints on the global structure of the accretion flow

Cited by 53 publications

References 133 publications

Re-observing the NLS1 galaxy RE J1034+396 – II. New insights on the soft X-ray excess, QPO, and the analogy with GRS 1915+105

Re-observing the NLS1 galaxy RE J1034+396 – II. New insights on the soft X-ray excess, QPO, and the analogy with GRS 1915+105

State-of-the-art AGN SEDs for photoionization models: BLR predictions confront the observations

Accretion around black holes: The geometry and spectra

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