Long XMM observation of the narrow-line Seyfert 1 galaxy IRAS 13224−3809: rapid variability, high spin and a soft lag

Fabian, A. C.; Kara, Erin; Walton, D. J.; Wilkins, D. R.; Ross, R. R.; Lozanov, Kaloian D.; Uttley, P.; Gallo, L. C.; Zoghbi, Abderahmen; Miniutti, G.; Boller, Th.; Brandt, W. N.; Cackett, Edward M.; Chiang, Chia-Ying; Dwelly, T.; Malzac, J.; Miller, J. M.; Nardini, E.; Ponti, G.; Reis, R. C.; Reynolds, C. S.; Steiner, James F.; Tanaka, Yasuo; Young, Andrew J.

doi:10.1093/mnras/sts504

Cited by 126 publications

(127 citation statements)

References 36 publications

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“…Similar peaks at ∼ 1.1 keV are also recognized in Figure 3 of Ponti et al (2010) and Figure 11 of Fabian et al (2013) on the same target. The iron L-feature must be responsible for this RMS peak because they are in the same energy range.…”

Section: Interpretation Of the Root-mean-square Spectrasupporting

confidence: 74%

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Origin of the characteristic X-ray spectral variations of IRAS 13224−3809

Yamasaki

Mizumoto

Ebisawa

et al. 2016

Publications of the Astronomical Society of Japan

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The Narrow-line Seyfert 1 galaxy (NLS1) IRAS 13224−3809 is known to exhibit significant Xray spectral variation, a sharp spectral drop at ∼ 7 keV, strong soft excess emission, and a hint of iron L-edge feature, which is very similar to the NLS1 1H 0707−495. We have proposed the "Variable Double Partial Covering (VDPC) model" to explain the energy spectra and spectral variability of 1H 0707−495 (Mizumoto, Ebisawa and Sameshima 2014, PASJ, 66, 122). In this model, the observed flux/spectral variations below 10 keV within a ∼day are primarily caused by change of the partial covering fraction of patchy clouds composed by double absorption layers in the line of sight. In this paper, we apply the VDPC model to IRAS 13224−3809. Consequently, we have found that the VDPC model can explain the observed spectral variations of IRAS 13224-3809 in the 0.5-10 keV band. In particular, we can explain the observed Root Mean Square (RMS) spectra (energy dependence of the fractional flux variation) in the entire 0.5 -10 keV band. In addition to the well-known significant drop in the iron K-band, we have found intriguing iron L-peaks in the RMS spectra when the iron L-edge is particularly deep. This feature, which is also found in 1H 0707-495, is naturally explained with the VDPC model, such that the RMS variations increase at the energies where optical depths of the partial absorbers are large. The absorbers have a larger optical depth at the iron L-edge than in the adjacent energy bands, thus a characteristic iron L-peak appears. On the other hand, just below the iron K-edge, the optical depth is the lowest and the RMS spectrum has a broad dip.

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Section: Interpretation Of the Root-mean-square Spectrasupporting

confidence: 74%

“…Fabian et al 2013;Chiang et al 2015). This is because the particular spectral shape of the VDPC model (eq.2) has strong spectral troughs at iron L-and K-edges even with the solar abundance.…”

Section: Interpretation Of the Spectral Variationsmentioning

confidence: 99%

Origin of the characteristic X-ray spectral variations of IRAS 13224−3809

Yamasaki

Mizumoto

Ebisawa

et al. 2016

Publications of the Astronomical Society of Japan

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“…By decomposing the relativisticallyblurred reflection spectrum, most notably the prominent iron Kα line at 6.4 keV, into the contributions from successive radii in the accretion disc, find that the emissivity profile of the disc in the NLS1 galaxy 1H 0707−495 approximately takes the form of a twice broken power law, falling off steeply with index > 7 over the inner regions of the disc, then flattening to almost a constant between 5 ∼ 35 rg before falling off slightly steeper than r −3 over the outer part of the disc, the form that is expected theoretically for illumination of an accretion disc in the curved spacetime around a black hole by a coronal X-ray source (Miniutti et al 2003;Suebsuwong et al 2006). A similar emissivity profile, flattened between 5 ∼ 10 rg was found by Fabian et al (2013) for the accretion disc in the NLS1 galaxy IRAS 13224−3809. present a systematic analysis of the expected emissivity profiles for accretion discs illuminated by a range of point-like and extended coronae, derived from general relativistic ray tracing simulations.…”

Section: The Accretion Disc Emissivity Profilesupporting

confidence: 74%

Driving extreme variability: the evolving corona and evidence for jet launching in Markarian 335

Wilkins

Gallo

2015

Monthly Notices of the Royal Astronomical Society

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Variations in the X-ray emission from the narrow line Seyfert 1 galaxy, Markarian 335 (Mrk 335), are studied on both long and short timescales through observations made between 2006 and 2013 with XMM-Newton, Suzaku and NuSTAR. Changes in the geometry and energetics of the corona that give rise to this variability are inferred through measurements of the relativistically blurred reflection seen from the accretion disc. On long timescales, we find that during the high flux epochs the corona has expanded, covering the inner regions of the accretion disc out to a radius of 26 +10 −7 r g . The corona contracts to within 12 r g and 5 r g in the intermediate and low flux epochs, respectively. While the earlier high flux observation made in 2006 is consistent with a corona extending over the inner part of the accretion disc, a later high flux observation that year revealed that the X-ray source had become collimated into a verticallyextended jet-like corona and suggested relativistic motion of material upward. On short timescales, we find that an X-ray flare during a low flux epoch in 2013 corresponded to a reconfiguration from a slightly extended corona to one much more compact, within just 2 ∼ 3 r g of the black hole. There is evidence that during the flare itself, the spectrum softened and the corona became collimated and slightly extended vertically as if a jet-launching event was aborted. Understanding the evolution of the X-ray emitting corona may reveal the underlying mechanism by which the luminous X-ray sources in AGN are powered.

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“…The AGN are expected to be variable in the X-ray band, both in flux and spectral features (e.g. Nandra et al 2000;Fabian et al 2012;Parker et al 2014;Wilkins et al 2014Wilkins et al , 2015. However, as we are comparing the reflection measurements to radio measurements taken years apart from the X-ray observations, variability between the observations likely dominates the systematic errors.…”

Section: The Nustar Reflection Fraction Samplementioning

confidence: 99%

AGN Coronae through a Jet Perspective

King

Lohfink

Kara

2017

ApJ

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This paper presents an in depth look at the jet and coronal properties of 41 AGN. Utilizing the highest quality NuSTAR, XMM-Newton, and NVSS 1.4 GHz data, we find that the radio Eddington luminosity inversely scales with X-ray reflection fraction, and positively scales with the distance between the corona and the reflected regions in the disk. We next investigate a model fit to the data that predicts the corona is outflowing and propagates into the large scale jet. We find this model describes the data well and predicts the corona has mildly relativistic velocities, 0.04 < β < 0.40. We discuss our results in the context of disk-jet connections in AGN.

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Long XMM observation of the narrow-line Seyfert 1 galaxy IRAS 13224−3809: rapid variability, high spin and a soft lag

Cited by 126 publications

References 36 publications

Origin of the characteristic X-ray spectral variations of IRAS 13224−3809

Origin of the characteristic X-ray spectral variations of IRAS 13224−3809

Driving extreme variability: the evolving corona and evidence for jet launching in Markarian 335

AGN Coronae through a Jet Perspective

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