How the X-ray spectrum of a narrow-line Seyfert 1 galaxy may be reflection-dominated

Fabian, A. C.; Ballantyne, D. R.; Merloni, A.; Vaughan, S.; Iwasawa, K.; Boller, Th.

doi:10.1046/j.1365-8711.2002.05419.x

Cited by 149 publications

(180 citation statements)

References 25 publications

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“…Abundances up to 7 times Solar have been suggested (e.g. Fabian et al 2002). The same BLR model, but with the Fe abundance enhanced by a factor seven only reduces the O vii/Fe Kα luminosity ratio to about 4.5.…”

Section: The Contribution Of the Blr To The Fe Kα Linementioning

confidence: 85%

XMM-Newtonunveils the complex iron Kαregion of Mrk 279

Costantini¹,

Kaastra

Korista

et al. 2010

A&A

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We present the results of a ∼160 ks-long XMM-Newton observation of the Seyfert 1 galaxy Mrk 279. The spectrum shows evidence of both broad and narrow emission features. The Fe Kα line may be equally well explained by a single broad Gaussian (FWHM ∼ 10 000 km s −1 ) or by two components: an unresolved core plus a very broad profile (FWHM ∼ 14 000 km s −1 ). For the first time we quantified, via the "locally optimally emitting cloud" model, the contribution of the broad line region (BLR) to the absolute luminosity of the broad component of the Fe Kα at 6.4 keV. We find that the contribution of the BLR is only ∼3%. In the two-line component scenario, we also evaluated the contribution of the highly ionized gas component, which produces the Fe xxvi line in the iron K region. This contribution to the narrow core of the Fe Kα line is marginal <0.1%. Most of the luminosity of the unresolved, component of Fe Kα may come from the obscuring torus, while the very-broad associated component may come from the accretion disk. However, models of reflection by cold gas are difficult to test because of the limited energy band. The Fe xxvi line at 6.9 keV is consistent to be produced in a high column density (N H ∼ 10 23 cm −2 ), extremely ionized (log ξ ∼ 5.5−7) gas. This gas may be a highly ionized outer layer of the torus.

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Section: The Contribution Of the Blr To The Fe Kα Linementioning

confidence: 85%

XMM-Newtonunveils the complex iron Kαregion of Mrk 279

Costantini¹,

Kaastra

Korista

et al. 2010

A&A

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“…There are no archival radio observations of the host of XMMSL1 J0740-85 but from the above analysis Laor 1991;Fabian et al 2002), with fixed emissivity index = 3, inner radius = 4.5 GM/c 2 , outer radius = 100 GM/c 2 and inclination = 45 • , ( f ) ionized absorption (zxipcf; Reeves et al 2008) with equivalent column density, ionization state and covering fraction, (g) C-statistic/number of degrees of freedom. Notes.…”

Section: Discussionmentioning

confidence: 99%

XMMSL1 J074008.2-853927: a tidal disruption event with thermal and non-thermal components

Saxton

Read

Komossa

et al. 2017

A&A

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Aims. We study X-ray bright tidal disruption events (TDE), close to the peak of their emission, with the intention of understanding the evolution of their light curves and spectra. Methods. Candidate TDE are identified by searching for soft X-ray flares from non-active galaxies in recent XMM-Newton slew data. Results. In April 2014, X-ray emission was detected from the galaxy XMMSL1 J074008.2-853927 (a.k.a. 2MASX 07400785-8539307), a factor 20 times higher than an upper limit from 20 years earlier. Both the X-ray and UV flux subsequently fell, by factors of 70 and 12 respectively. The bolometric luminosity peaked at L bol ∼ 2 × 10 44 ergs s −1 with a spectrum that may be modelled with thermal emission in the UV band, a power-law with Γ ∼ 2 dominating in the X-ray band above 2 keV and a soft X-ray excess with an effective temperature of ∼86 eV. Rapid variability locates the X-ray emission to within <73 R g of the nuclear black hole. Radio emission of flux density ∼1 mJy, peaking at 1.5 GHz was detected 21 months after discovery. Optical spectra indicate that the galaxy, at a distance of 73 Mpc (z = 0.0173), underwent a starburst 2 Gyr ago and is now quiescent. We consider a tidal disruption event to be the most likely cause of the flare. If this proves to be correct then this is a very clean example of a disruption exhibiting both thermal and non-thermal radiation.

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“…Disk reflection models use these features to reproduce the emission from a photoionized accretion disk around a supermassive black hole (Ross & Fabian 1993Ballantyne et al 2001b). These models have been tested successfully in many objects (e.g., on five NLS1 by Ballantyne et al 2001a; on 1H 0707-495 by Fabian et al 2002; on MCG-6-30−15 by Ballantyne et al 2003; and on 34 sources by Crummy et al 2006, using the reflionx model from . Nevertheless, alternative models can also explain the soft-excess in some of these AGN (e.g., warm Comptonization in Ark 564 - Dewangan et al 2007, andPKS 0558-504 -Papadakis et al 2010;partial covering in 1H 0707-495 -Tanaka et al 2004;and MCG-6-30-15 -Miller et al 2008).…”

Section: Modelmentioning

confidence: 99%

Multiwavelength campaign on Mrk 509

Boissay

Paltani

Ponti

et al. 2014

A&A

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Active galactic nuclei (AGN) are the most luminous persistent objects in the universe. The X-ray domain is particularly important because the X-ray flux represents a significant fraction of the bolometric emission from such objects and probes the innermost regions of accretion disks, where most of this power is generated. An excess of X-ray emission below ∼2 keV, called soft-excess, is very common in Type 1 AGN spectra. The origin of this feature remains debated. Originally modeled with a blackbody, there are now several possibilities to model the soft-excess, including warm Comptonization and blurred ionized reflection. In this paper, we test ionized-reflection models on Mrk 509, a bright Seyfert 1 galaxy for which we have a unique data set, in order to determine whether it can be responsible for the strong soft-excess. We use ten simultaneous XMM-Newton and INTEGRAL observations performed every four days. We present here the results of the spectral analysis, the evolution of the parameters, and the variability properties of the X-ray emission. The application of blurred ionized-reflection models leads to a very strong reflection and an extreme geometry, but fails to reproduce the broad-band spectrum of Mrk 509. Two different scenarios for blurred ionized reflection are discussed: stable geometry and lamp-post configuration. In both cases we find that the model parameters do not follow the expected relations, indicating that the model is fine-tuned to fit the data without physical justification. A large, slow variation in the soft-excess without a counterpart in the hard X-rays could be explained by a change in ionization of the reflector. However, such a change does not naturally follow from the assumed geometrical configuration. Warm Comptonization remains the most probable origin of the soft-excess in this object. Nevertheless, it is possible that both ionized reflection and warm Comptonization mechanisms can explain the soft-excess in all objects, one dominating the other one, depending on the physical conditions of the disk and the corona.

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How the X-ray spectrum of a narrow-line Seyfert 1 galaxy may be reflection-dominated

Cited by 149 publications

References 25 publications

XMM-Newtonunveils the complex iron Kαregion of Mrk 279

XMM-Newtonunveils the complex iron Kαregion of Mrk 279

XMMSL1 J074008.2-853927: a tidal disruption event with thermal and non-thermal components

Multiwavelength campaign on Mrk 509

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