Broad iron L line and X-ray reverberation in 1H0707-495

Zoghbi, Abderahmen; Fabian, A. C.; Uttley, P.; Miniutti, G.; Gallo, Luigi; Reynolds, C. S.; Miller, J. M.; Ponti, G.

doi:10.1111/j.1365-2966.2009.15816.x

Cited by 242 publications

(334 citation statements)

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“…4 (left panel). All bands show the characteristic red-noise shape at high frequencies (although not clear from the figure, there is evidence for a break to a flatter slope at ∼ 1.4 × 10 −4 Hz, see Zoghbi et al 2010). However, the higher energies show a flatter PSD, showing that there is relatively more rapid variability at these energies.…”

Section: The Discrete Fourier Transform and Power Spectral Densitymentioning

confidence: 89%

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: The Discrete Fourier Transform and Power Spectral Densitymentioning

confidence: 89%

X-ray reverberation around accreting black holes

Uttley

Cackett

Fabian³

et al. 2014

Astron Astrophys Rev

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428

597

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“…Assuming that the lag timescale ∆t ∼ 2H/c = 2hRg/c, where H is the physical height of the lamppost and h = H/Rg is this in terms of gravitational radii, only constrains the product hM rather than each parameter separately. In 1H0707, the observed 30 s soft lag Zoghbi et al 2010; corresponds to an intrinsic 80 s light travel time after correcting for spectral dilution, which implies a lamppost height of 4Rg for a 2 × 10 6 M⊙ black hole (Kara et al 2013). However, the spectral data discussed above strongly require that the lamppost height is small from the strongly centrally peaked emissivity (e.g.…”

Section: Constraints From Relativistic Reflection Modelsmentioning

confidence: 99%

“…The line is smeared by the velocity structure of the wind, but without extreme relativistic effects it should be observable as a distinct feature rather than broadened into the red wing (Zoghbi et al 2010). However, if the clumps are embedded in a more highly ionized wind, then Compton scattering in the highly ionized phase will reduce the observed line flux.…”

Section: Alternative Models For the X-ray Spectra And Variability Of mentioning

confidence: 99%

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The mass and spin of the extreme Narrow Line Seyfert 1 Galaxy 1H 0707−495 and its implications for the trigger for relativistic jets

Done

Jin

2016

Mon. Not. R. Astron. Soc.

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Relativistic reflection models of the X-ray spectrum of the 'complex' Narrow Line Seyfert 1 (NLS1) 1H 0707-495 require a high spin, moderate inclination, low mass black hole. With these parameters fixed, the observed optical/UV emission directly determines the mass accretion rate through the outer disc and hence predicts the bolometric luminosity. This is 140 − 260× the Eddington limit. Such a disc should power a strong wind, and winds are generically expected to be clumpy. Changing inclination angle with respect to a clumpy wind structure gives a possible explanation for the otherwise puzzling difference between 'complex' NLS1 such as 1H 0707-495 and 'simple' ones like PG 1244+026. Lines of sight which intercept the wind show deep absorption features at iron from the hot phase of the wind, together with stochastic dips and complex absorption when the clumps occult the X-ray source (complex NLS1), whereas both these features are absent for more face-on inclination (simple NLS1). This geometry is quite different to the clean view of a flat disc which is assumed for the spin measurements in relativistic reflection models, so it is possible that even 1H 0707-495 has low spin. If so, this re-opens the simplest and hence very attractive possibility that high black hole spin is a necessary and sufficient condition to trigger highly relativistic (bulk Lorentz factor ∼ 10 − 15) jets.

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“…Measurements of BH spin (a key parameter to understand BH evolution) have been published for both Galactic BHs and AGN. The debate on the relativistic nature of these lines is however still hot, as some authors claim that they are, at least in AGN, simply an artifact of complex absorption (see [22,25]). While the two models are often degenerate below 10 keV, their extrapolations to higher energies are different, and easy to distinguish by NHXM.…”

Section: Strong Gravity Ef Fects Around Black Holes and Neutron Starsmentioning

confidence: 99%

The NHXM observatory

Tagliaferri

Hornstrup²,

Huovelin

et al. 2011

Exp Astron

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Exploration of the X-ray sky has established X-ray astronomy as a fundamental astrophysical discipline. While our knowledge of the sky below 10 keV has increased dramatically (∼8 orders of magnitude) by use of grazing incidence optics, we still await a similar improvement above 10 keV, where to date only collimated instruments have been used. Also ripe for exploration is the field of X-ray polarimetry, an unused fundamental tool to understand the physics and morphology of X-ray sources. Here we present a novel mission, the New Hard X-ray Mission (NHXM) that brings together for the first time simultaneous high-sensitivity, hard-X-ray imaging, broadband spectroscopy and polarimetry. NHXM will perform groundbreaking science in key scientific areas, including: black hole cosmic evolution, census and accretion physics; acceleration mechanism and non-thermal emission; physics of matter under extreme conditions. NHXM is designed specifically to address these topics via: broad 0.5-80 (120) keV band for imaging and spectroscopy; 20 arcsec (15 goal) Half Energy Width (HEW) angular resolution at 30 keV; sensitivity limits more than 3 orders of magnitude better than those available in present day instruments; broadband (2-35 keV) imaging polarimetry. In addition, NHXM has the ability to locate and actively monitor sources in different states of activity and to repoint within 1 to 2 h. This mission has been proposed to ESA in response to the Cosmic Vision M3 call. Its satellite configuration and payload subsystems were studied as part of previous national efforts permitting us to design a mature configuration that is compatible with a VEGA launch already by 2020.

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Broad iron L line and X-ray reverberation in 1H0707-495

Cited by 242 publications

References 58 publications

X-ray reverberation around accreting black holes

X-ray reverberation around accreting black holes

The mass and spin of the extreme Narrow Line Seyfert 1 Galaxy 1H 0707−495 and its implications for the trigger for relativistic jets

The NHXM observatory

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