No signatures of black hole spin in the X-ray spectrum of the Seyfert 1 galaxy Fairall 9

Yaqoob, T.; Turner, T. J.; Tatum, M. M.; Trevor, M.; Scholtes, A.

doi:10.1093/mnras/stw1824

Cited by 19 publications

(16 citation statements)

References 77 publications

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“…All these models assume a uniform density of the gas, and hence we refer to them as "smooth torus models". These models have also been widely used to fit the observed X-ray spectra of AGNs (Ikeda model: e.g., Awaki et al 2009;Eguchi et al 2011;Tazaki et al 2011Tazaki et al , 2013Kawamuro et al 2013Kawamuro et al , 2016aTanimoto et al 2016Tanimoto et al , 2018Oda et al 2017Oda et al , 2018Yamada et al 2018, MYTorus model: e.g., Yaqoob 2012Yaqoob et al 2015Yaqoob et al , 2016Koss et al 2013Koss et al , 2015Koss et al , 2016Koss et al , 2017Ricci et al 2014aRicci et al ,b, 2015Ricci et al , 2016aRicci et al ,b, 2017a,b, Torus model: e.g., Brightman & Nandra 2011bBrightman et al 2013Brightman et al , 2014Brightman et al , 2015Brightman et al , 2016Brightman et al , 2017Buchner et al 2014Buchner et al , 2015Gandhi et al 2014Gandhi et al , 2015Gandhi et al , 2017.…”

Section: Introductionmentioning

confidence: 99%

XCLUMPY: X-Ray Spectral Model from Clumpy Torus and Its Application to the Circinus Galaxy

Tanimoto

Ueda

Odaka

et al. 2019

ApJ

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We construct an X-ray spectral model from the clumpy torus in an active galactic nucleus (AGN), designated as "XCLUMPY", utilizing the Monte Carlo simulation for Astrophysics and Cosmology framework (MONACO: Odaka et al. 2011. The adopted geometry of the torus is the same as that in Nenkova et al. (2008a,b), who assume a power law distribution of clumps in the radial direction and a normal distribution in the elevation direction. We investigate the dependence of the X-ray continuum and Fe Kα fluorescence line profile on the torus parameters. Our model is compared with other torus models: MYTorus model (Murphy & Yaqoob 2009), Ikeda model (Ikeda et al. 2009), and CTorus model (Liu & Li 2014).As an example, we also present the results applied to the broadband X-ray spectra of the Circinus galaxy observed with XMM-Newton, Suzaku, and NuSTAR. Our model can well reproduce the data, yielding a hydrogen column density along the equatorial plane N Equ H = 9.08 +0.14 −0.08 × 10 24 cm −2 , a torus angular width σ = 14.7 +0.44 −0.39 degree, and a 2-10 keV luminosity log L 2−10 /erg s −1 = 42.8. These results are discussed in comparison with the observations in other wavelengths.

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Section: Introductionmentioning

confidence: 99%

XCLUMPY: X-Ray Spectral Model from Clumpy Torus and Its Application to the Circinus Galaxy

Tanimoto

Ueda

Odaka

et al. 2019

ApJ

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“…For a given column density of the reflecting medium, the shape of the reflection spectrum viewed along lines of sight that do not intercept the medium is not very sensitive to the exact geometry or orientation (e.g. see Liu & Li 2014;Yaqoob et al 2015Yaqoob et al , 2016. Thus, the faceon torus reflection spectrum could be representative of other physical scenarios, such as same-side reflection in a distribution of clouds.…”

Section: Mytorus Modelmentioning

confidence: 99%

New Constraints on the Geometry and Kinematics of Matter Surrounding the Accretion Flow in X-Ray Binaries from Chandra High-energy Transmission Grating X-Ray Spectroscopy

Tzanavaris

Yaqoob

2018

ApJ

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The narrow, neutral Fe Kα fluorescence emission line in X-ray binaries (XRBs) is a powerful probe of the geometry, kinematics and Fe abundance of matter around the accretion flow. In a recent study it has been claimed, using Chandra High-Energy Transmission Grating (HETG) spectra for a sample of XRBs, that the circumnuclear material is consistent with a solar-abundance, uniform, spherical distribution. It was also claimed that the Fe Kα line was unresolved in all cases by the HETG. However, these conclusions were based on ad hoc models that did not attempt to relate the global column density to the Fe Kα line emission. We revisit the sample and test a self-consistent model of a uniform, spherical X-ray reprocessor against HETG spectra from 56 observations of 14 Galactic XRBs. We find that the model is ruled out in 13/14 sources because a variable Fe abundance is required. In 2 sources a spherical distribution is viable but with non-solar Fe abundance. We also applied a solar-abundance Compton-thick reflection model, which can account for the spectra that are inconsistent with a spherical model, but spectra with a broader bandpass are required to better constrain model parameters. We also robustly measured the velocity width of the Fe Kα line and found full width half maximum values up to ∼ 5000 km s −1 . Only in some spectra was the Fe Kα line unresolved by the HETG.

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“…Among the selected observations, this spectrum covers the largest observable energy range, from 0.6−50 keV. The data reduction was performed as described in the Observation and Data Reduction section in Yaqoob et al (2016).…”

Section: Data Reductionmentioning

confidence: 99%

New Insights Into the Spectral Variability and Physical Conditions of the X-Ray Absorbers in NGC 4151

Couto

Kraemer

Turner

et al. 2016

ApJ

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We investigate the relationship between the long term X-ray spectral variability in the Seyfert 1.5 galaxy NGC 4151 and its intrinsic absorption, by comparing the 2014 simultaneous ultraviolet/XRay observations taken with Hubble STIS Echelle and Chandra HETGS with archival observations from Chandra, XMM-Newton and Suzaku. The observations are divided into "high" and "low" states, with the low states showing strong and unabsorbed extended emission at energies below 2 keV. Our X-ray model consists of a broken powerlaw, neutral reflection and the two dominant absorption components identified by Kraemer et al. (2005), hereafter KRA2005, X-High and D+Ea, which are present in all epochs. The model fittings suggest that the absorbers are very stable, with the principal changes in the intrinsic absorption resulting from variations in the ionization state of the gas as the ionizing continuum varies. However, the low states show evidence of larger column densities in one or both of the absorbers. Among plausible explanations for the column increase, we discuss the possibility of an expanding/contracting X-ray corona. As suggested by KRA2005, there seem to be contributions from magnetohydrodynamic (MHD) winds to the mass outflow. Along with the ultra fast outflow absorber identified by Tombesi et al. (2010), X-High is consistent with being magnetically driven. On the other hand, it is unlikely that D+Ea is part of the MHD flow, and it is possible that it is radiatively accelerated. These results suggest that at a sufficiently large radial distance there is a break point between MHD-dominated and radiatively driven outflows.

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No signatures of black hole spin in the X-ray spectrum of the Seyfert 1 galaxy Fairall 9

Cited by 19 publications

References 77 publications

XCLUMPY: X-Ray Spectral Model from Clumpy Torus and Its Application to the Circinus Galaxy

XCLUMPY: X-Ray Spectral Model from Clumpy Torus and Its Application to the Circinus Galaxy

New Constraints on the Geometry and Kinematics of Matter Surrounding the Accretion Flow in X-Ray Binaries from Chandra High-energy Transmission Grating X-Ray Spectroscopy

New Insights Into the Spectral Variability and Physical Conditions of the X-Ray Absorbers in NGC 4151

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