Modelling the broad Fe Kα reverberation in the AGN NGC 4151

Cackett, E.; Zoghbi, Abderahmen; Reynolds, C. S.; Fabian, A. C.; Kara, Erin; Uttley, P.; Wilkins, D. R.

doi:10.1093/mnras/stt2424

Cited by 146 publications

(238 citation statements)

References 56 publications

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“…In Fig. 30 we show the lag-energy spectrum calculated over a range of different frequencies, and now follow the discussion in Cackett et al (2014) describing the behaviour. We start by looking at the lowest frequencies.…”

Section: 32mentioning

confidence: 82%

“…Black hole spin too has an effect on the lag-energy spectrum. The exact behaviour as each of these parameters is changed is demonstrated in detail in Cackett et al (2014), and we just briefly comment on each parameter here. For instance, increasing the height of the X-ray source will increase the overall path length between the direct and reprocessed emission, leading to longer lags.…”

Section: 32mentioning

confidence: 99%

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X-ray reverberation around accreting black holes

Uttley

Cackett

Fabian³

et al. 2014

Astron Astrophys Rev

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Luminous accreting stellar mass and supermassive black holes produce power-law continuum X-ray emission from a compact central corona. Reverberation time lags occur due to light travel time-delays between changes in the direct coronal emission and corresponding variations in its reflection from the accretion flow. Reverberation is detectable using light curves made in different X-ray energy bands, since the direct and reflected components have different spectral shapes. Larger, lower frequency, lags are also seen and are identified with propagation of fluctuations through the accretion flow and associated corona. We review the evidence for X-ray reverberation in active galactic nuclei and black hole X-ray binaries, showing how it can be best measured and how it may be modelled. The timescales and energy-dependence of the high frequency reverberation lags show that much of the signal is originating from very close to the black hole in some objects, within a few gravitational radii of the event horizon. We consider how these signals can be studied in the future to carry out X-ray reverberation mapping of the regions closest to black holes.

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Section: 32mentioning

confidence: 82%

Section: 32mentioning

confidence: 99%

X-ray reverberation around accreting black holes

Uttley

Cackett

Fabian³

et al. 2014

Astron Astrophys Rev

Self Cite

448

606

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“…This geometry has been adopted by many authors in the past when studying the variability properties of the X-ray reflection component (e.g. Gilfvanov et al 2000;Poutanen 2002 in the case Newtonian space-time, and Reynolds et al 1999;Miniutti & Fabian 2004;Niedžwiecki & Miyakawa 2010;Emmanoulopoulos et al 2014;Cackett et al 2014, who adopted a fully relativistically approach). From a physical point of view, the lamp-post geometry can account for the main features of the X-ray source if the latter is the site where an outflowing corona is accelerated for example, or where the shocks in an aborted jet collide (Ghisellini et al 2004).…”

Section: Summary Of Our Resultsmentioning

confidence: 99%

Signatures of X-ray reverberation in the power spectra of AGN

Papadakis

Pecháček

Dovčiak

et al. 2016

A&A

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Aims. We study the effects of X-ray reprocessing in the power spectra (PSDs) of active galactic nuclei (AGNs). Methods. We compute fully relativistic disc response functions in the case of lamp-post geometry using the full observed reflection spectrum for various X-ray source heights, disc inclination, and spin values of the central black hole. Since the observed PSD is equal to the product of the intrinsic power spectrum with the transfer function (i.e. the Fourier transform of the disc response function), we are able to predict the observed PSDs in the case of X-ray illumination of the inner disc.Results. The observed PSD should show a prominent dip at high frequencies and an oscillatory behaviour with a decreasing amplitude at higher frequencies. The reverberation echo features should be more prominent in energy bands where the reflection component is more pronounced. The frequency of the dip is independent of energy, and it is mainly determined by the black hole mass and the X-ray source height. The amplitude of the dip increases with increasing black hole spin and inclination angle, as long as the height of the lamp is smaller than ∼10 gravitational radii. Conclusions. The detection of the X-ray reverberation signals in the PSDs can provide further evidence for X-ray illumination of the inner disc in AGN. Our results are largely independent of the assumed geometry of the disc-corona system, as long as it does not change with time, and the disc response function is characterized by a sharp rise, a plateau, and a decline at longer times. Irrespective of the geometry, the frequency of the main dip should decrease with increasing mean time of the response function, and the amplitude of the dip should increase with increasing reflection fraction.

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“…The compactness of the corona has been observationally and independently confirmed via microlensing (e.g., Pooley et al 2007;Chartas et al 2009Chartas et al , 2016Dai et al 2010;Morgan et al 2008;Blackburne et al 2014Blackburne et al , 2015MacLeod et al 2015) and reverberation studies (Fabian et al 2009;De Marco et al 2011;Kara et al 2013Kara et al , 2016Cackett et al 2014;Emmanoulopoulos et al 2014;Uttley et al 2014). The reverberation studies in many cases constrain the distance between the corona and central black hole to lie in the range of 3 − 10r g .…”

Section: X-ray Observation and Data Analysismentioning

confidence: 91%

Measuring the Innermost Stable Circular Orbits of Supermassive Black Holes

Chartas

Krawczynski

Zalesky

et al. 2017

ApJ

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We present a promising new technique, the g-distribution method, for measuring the inclination angle (i), the innermost stable circular orbit (ISCO), and the spin of a supermassive black hole. The g-distribution method uses measurements of the energy shifts in the relativistic iron line emitted by the accretion disk of a supermassive black hole due to microlensing by stars in a foreground galaxy relative to the g-distribution shifts predicted from microlensing caustic calculations. We apply the method to the gravitationally lensed quasars RX J1131−1231 (z s = 0.658, z l = 0.295), QJ 0158−4325 (z s = 1.294, z l = 0.317), and SDSS 1004+4112 (z s = 1.734, z l = 0.68). For RX J1131−1231 our initial results indicate that r ISCO < ∼ 8.5 gravitational radii (r g ) and i > ∼ 76• . We detect two shifted Fe lines, in several observations, as predicted in our numerical simulations of caustic crossings. The current ∆E-distribution of RX J1131−1231 is sparsely sampled but further X-ray monitoring of RX J1131−1231 and other lensed quasars will provide improved constraints on the inclination angles, ISCO radii and spins of the black holes of distant quasars.

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Modelling the broad Fe Kα reverberation in the AGN NGC 4151

Cited by 146 publications

References 56 publications

X-ray reverberation around accreting black holes

X-ray reverberation around accreting black holes

Signatures of X-ray reverberation in the power spectra of AGN

Measuring the Innermost Stable Circular Orbits of Supermassive Black Holes

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