A relativistic disc reflection model for 1H0419–577: Multi-epoch spectral analysis with<i>XMM–Newton</i>and<i>NuSTAR</i>

Jiang, Jiachen; Walton, D. J.; Fabian, A. C.; Parker, M. L.

doi:10.1093/mnras/sty3228

Cited by 28 publications

(15 citation statements)

References 75 publications

(83 reference statements)

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“…However, only upper limits of disc densities are achieved for sources with log(m BH ) > 8. This matches the previous analysis of another Seyfert 1 galaxy 1H 0419−577 where the mass of the central BH is estimated to be log(m BH ) ≈ 8 and a disc density of log(n e ) < 15.2 is obtained with 90% confidence (Jiang et al 2019a). Disc densities significantly higher than log(n e ) = 15 are found in AGN with log(m BH ) < 7.…”

Section: Disc Denstities In Seyfert 1 Galaxiessupporting

confidence: 90%

High Density Reflection Spectroscopy – II. The density of the inner black hole accretion disc in AGN

Jiang

Fabian

Dauser

et al. 2019

Monthly Notices of the Royal Astronomical Society

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109

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We present a high density disc reflection spectral analysis of a sample of 17 Seyfert 1 galaxies to study the inner disc densities at different black hole mass scales and accretion rates. All the available XMM-Newton observations in the archive are used. OM observations in the optical/UV band are used to estimate their accretion rates. We find that 65% of sources in our sample show a disc density significantly higher than n e = 10 15 cm −3 , which was assumed in previous reflection-based spectral analyses. The best-fit disc densities show an anti-correlation with black hole mass and mass accretion rate. High density disc reflection model can successfully explain the soft excess emission and significantly reduce inferred iron abundances. We also compare our black hole spin and disc inclination angle measurements with previous analyses.

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Section: Disc Denstities In Seyfert 1 Galaxiessupporting

confidence: 90%

High Density Reflection Spectroscopy – II. The density of the inner black hole accretion disc in AGN

Jiang

Fabian

Dauser

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

109

111

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“…Table 1 and Fig. 6 summarize the current reflection-based AGN spin measurements; this updates the compilations of Reynolds (2014) and Vasudevan et al (2016) applying the same "quality control criteria" and, in particular, includes the results obtained from the recent high-density reflection modelling of Jiang et al (2019). Taken together, these results suggest a mass dependence to the distribution of SMBH spins.…”

Section: The Spin Of Smbhs -Constraints On Black Hole Growth Over Cos...mentioning

confidence: 65%

Observational Constraints on Black Hole Spin

Reynolds

2020

Preprint

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The spin of a black hole is an important quantity to study, providing a window into the processes by which a black hole was born and grew. Further, spin can be a potent energy source for powering relativistic jets and energetic particle acceleration. In this review, I describe the techniques currently used to detect and measure the spins of black holes. It is shown that:• Two well understood techniques, X-ray reflection spectroscopy and thermal continuum fitting, can be used to measure the spins of black holes that are accreting at moderate rates. There is a rich set of other electromagnetic techniques allowing us to extend spin measurements to lower accretion rates. • Many accreting supermassive black holes are found to be rapidlyspinning, although a population of more slowly spinning black holes emerges at masses above M > 3 × 10 7 M as expected from recent structure formation models. • Many accreting stellar-mass black holes in X-ray binary systems are rapidly spinning and must have been born in this state. • The advent of gravitational wave astronomy has enabled the detection of spin effects in merging binary black holes. Most of the pre-merger black holes are found to be slowly spinning, a notable exception being an object that may itself be a merger product. • The stark difference in spins between the black hole X-ray binary and the binary black hole populations shows that there is a diversity of formation mechanisms.Given the array of new electromagnetic and gravitational wave capabilities currently being planned, the future of black hole spin studies is bright.

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“…Of course, a good constraint on the break radius and emissivity index is also obtained for a number of systems (both AGNs and binary systems), showing a steep inner index (q in > 3) and small break radius (R br < 6 R g 1 ), such as 1H0419-577 (Jiang et al 2019), 1H0707-495 (Fabian & Wilkins 2011;Fabian et al 2012), IRAS 13224-3809 (Fabian et al 2018), and Mrk 335 Wilkins & Gallo 2015), as well as for black hole binaries, such as XTE J1752-223 (García et al 2018b), Cyg X-1 , GRS 1915-105 (Miller et al 2013, and MAXI J1535-571 (Xu et al 2018). The steep emissivity profile is usually explained with an extremely compact corona locating close to the black hole, in which case a large fraction of the power-law emission will be focused towards the inner region as a result of light-bending effect (Miniutti & Fabian 2004;Dauser et al 2013).…”

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confidence: 97%

A detailed study on the reflection component for the black hole candidate MAXI J1836−194

Dong

García

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a detailed spectral analysis of the black hole candidate MAXI J1836-194. The source was caught in the intermediate state during its 2011 outburst by Suzaku and RXTE. We jointly fit the X-ray data from these two missions using the relxill model to study the reflection component, and a steep inner emissivity profile indicating a compact corona as the primary source is required in order to achieve a good fit. In addition, a reflection model with a lamp-post configuration (relxilllp), which is normally invoked to explain the steep emissivity profile, gives a worse fit and is excluded at 99% confidence level compared to relxill. We also explore the effect of the ionization gradient on the emissivity profile by fitting the data with two relativistic reflection components, and it is found that the inner emissivity flattens. These results may indicate that the ionization state of the disc is not constant. All the models above require a supersolar iron abundance higher than ∼ 4.5. However, we find that the high-density version of reflionx can describe the same spectra even with solar iron abundance well. A moderate rotating black hole (a * = 0.84-0.94) is consistently obtained by our models, which is in agreement with previously reported values.2 Yanting Dong et al. INTRODUCTIONGalactic X-ray binaries are believed to be powered by accretion onto stellar-mass black holes or neutron stars. The gases in accretion disc emit thermal radiation in UV/X-ray band (Shakura & Sunyaev 1973). Some fraction of the thermal photons from the disc are then inverse Compton scattered by energetic electrons in the hypothetically hot corona, producing a hard X-ray spectrum in the form of power-law, i.e. N(E) ∝ E −Γ . A fraction of the high-energy photons will irradiate the cold accretion disc, generating the so-called X-ray reflection component (Fabian et al. 1989). The main features of the reflection spectrum are the fluorescent Fe Kα emission line at energies of 6.4-6.97 keV (depend upon the ionization state of the disc) and the Compton hump at 20-30 keV (Young et al. 1999).The profile of the reflection spectrum will be smeared due to the effects of Doppler shift, special relativity, and general relativity if it comes from the inner region of the accretion disc (Fabian et al. 2000). Observationally, the most prominent effect is that the intrinsically narrow Fe Kα line is broadened and skewed to an asymmetric shape. The profile of the broad line, especially the red wing of the line, is directly linked to the inner radius of the accretion disc which is thought to be at the innermost stable circular orbit (ISCO), i.e. R in = R ISCO . Thus, by modelling the broad iron line, we can deduce the spin of the black hole based on the relation between the spin and the ISCO (Bardeen et al. 1972). However, the line profile is readily affected by the subtraction of continuum and other components. Therefore, Reynolds (2014) pointed out that a more accurate measurement of the spin can be achieved by modelling the full reflection spectrum. The spin...

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A relativistic disc reflection model for 1H0419–577: Multi-epoch spectral analysis withXMM–NewtonandNuSTAR

Cited by 28 publications

References 75 publications

High Density Reflection Spectroscopy – II. The density of the inner black hole accretion disc in AGN

High Density Reflection Spectroscopy – II. The density of the inner black hole accretion disc in AGN

Observational Constraints on Black Hole Spin

A detailed study on the reflection component for the black hole candidate MAXI J1836−194

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