XMM-<i>Newton</i>unveils the complex iron K<i>α</i>region of Mrk 279

Costantini, E.; Kaastra, J. S.; Korista, K. T.; Ebrero, J.; Arav, Nahum; Kriss, G. A.; Steenbrugge, K. C.

doi:10.1051/0004-6361/200912555

Cited by 20 publications

(27 citation statements)

References 61 publications

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“…Though the data do not require inclusion of the Compton shoulder, the torus as the origin of the narrow lines is physically realistic as Mrk 530 is classified as a Seyfert 1.5, so we are observing the system at high inclination and seeing much of the torus. The scenario is consistent with observations of other sources like NGC 5506, an intermediate Seyfert with a complex Fe region (Bianchi & Matt 2002), and Mrk 279, a Seyfert 1 with ionised lines likely originating from the tours (Costantini et al 2010). A future mission like XARM, with Hitomi-like (Takahashi et al 2016) spectral resolution will advance this work.…”

Section: The Fe Kα Regionsupporting

confidence: 87%

Exploring the spectral variability of the Seyfert 1.5 galaxy Markarian 530 with Suzaku

Ehler

Gonzalez

Gallo

2018

Monthly Notices of the Royal Astronomical Society

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A 2012 Suzaku observation of the Seyfert 1.5 galaxy Markarian 530 was analysed and found to exhibit two distinct modes of variability, which were found to be independent from one another. Firstly, the spectrum undergoes a smooth transition from a soft to a hard spectrum. Secondly, the spectrum displays more rapid variability seemingly confined to a very narrow energy band (∼ 1 − 3 keV). Three physical models (blurred reflection, partial covering, and soft Comptonisation) were explored to characterise the average spectrum of the observation as well as the spectral state change. All three models were found to fit the average spectrum and the spectral changes equally well. The more rapid variability appears as two cycles of a sinusoidal function, but we cannot attribute this to periodic variability. The Fe Kα band exhibits a narrow 6.4 keV emission line consistent with an origin from the distant torus. In addition, features blueward of the neutral iron line are consistent with emission from He-like and H-like iron that could be originating from the highly ionised layer of the torus, but a broad Gaussian profile at ∼ 6.7 keV also fits the spectrum well.

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Section: The Fe Kα Regionsupporting

confidence: 87%

Exploring the spectral variability of the Seyfert 1.5 galaxy Markarian 530 with Suzaku

Ehler

Gonzalez

Gallo

2018

Monthly Notices of the Royal Astronomical Society

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“…Such lines are often observed both in Seyfert 1s and in Seyfert 2s, and are likely produced in a Comptonthin, photoionized material illuminated by the nuclear continuum (e.g. Bianchi & Matt 2002;Bianchi et al 2005;Costantini et al 2010).…”

Section: The Reprocessed Componentsmentioning

confidence: 99%

Multi-wavelength campaign on NCG 7469

Middei

Bianchi

Cappi

et al. 2018

A&A

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We conducted a multi-wavelength 6-month campaign to observe the Seyfert Galaxy NGC 7469, using the space-based observatories HST, Swift, XMM-Newton and NuSTAR. We report the results of the spectral analysis of the seven simultaneous XMM-Newton and NuSTAR observations. The source shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral Fe Kα emission line in all the spectra and weaker contributions from Fe Kβ, neutral Ni Kα, and ionized iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. In the joint analysis of XMM-Newton and NuSTAR data, a constant photon index is found (Γ = 1.78 ± 0.02) together with a high energy cut-off Ecut = 170−40+60 keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT = 45−12+15 keV and, assuming a spherical geometry, an optical depth τ = 2.6 ± 0.9. The reflection component is consistent with being constant and the reflection fraction is in the range R = 0.3−0.6. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a warm corona with an average kT = 0.67 ± 0.03 keV and a corresponding optical depth τ = 9.2 ± 0.2.

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“…Such emission lines from highly ionised ions are now observed often (Costantini et al 2010; e.g. for a compilation of sources, Bianchi et al 2009a,b;Fukazawa et al 2011), and they can arise from photo-ionised (Bianchi et al 2005;Bianchi & Matt 2002) or collisionally ionised plasma (Cappi et al 1999).…”

Section: The Ionised Fe K Emissionmentioning

confidence: 99%

Multiwavelength campaign on Mrk 509

Ponti

Cappi

Costantini

et al. 2012

A&A

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Context. We report on a detailed study of the Fe K emission/absorption complex in the nearby, bright Seyfert 1 galaxy Mrk 509. The study is part of an extensive XMM-Newton monitoring consisting of 10 pointings (∼60 ks each) about once every 4 days, and includes a reanalysis of previous XMM-Newton and Chandra observations. Aims. We aim at understanding the origin and location of the Fe K emission and absorption regions. Methods. We combine the results of time-resolved spectral analysis on both short and long time-scales including model-independent rms spectra. Results. Mrk 509 shows a clear (EW = 58±4 eV) neutral Fe Kα emission line that can be decomposed into a narrow (σ = 0.027 keV) component (found in the Chandra HETG data) plus a resolved (σ = 0.22 keV) component. We find the first successful measurement of a linear correlation between the intensity of the resolved line component and the 3-10 keV flux variations on time scales of years down to a few days. The Fe Kα reverberates the hard X-ray continuum without any measurable lag, suggesting that the region producing the resolved Fe Kα component is located within a few light days to a week (r < ∼ 10 3 r g ) from the black hole (BH). The lack of a redshifted wing in the line poses a lower limit of ≥40 r g for its distance from the BH. The Fe Kα could thus be emitted from the inner regions of the BLR, i.e. within the ∼80 light days indicated by the Hβ line measurements. In addition to these two neutral Fe Kα components, we confirm the detection of weak (EW ∼ 8-20 eV) ionised Fe K emission. This ionised line can be modelled with either a blend of two narrow Fe xxv and Fe xxvi emission lines (possibly produced by scattering from distant material) or with a single relativistic line produced, in an ionised disc, down to a few r g from the BH. In the latter interpretation, the presence of an ionised standard α-disc, down to a few r g , is consistent with the source high Eddington ratio. Finally, we observe a weakening/disappearing of the mediumand high-velocity high-ionisation Fe K wind features found in previous XMM-Newton observations. Conclusions. This campaign has made the first reverberation measurement of the resolved component of the Fe Kα line possible, from which we can infer a location for the bulk of its emission at a distance of r ∼ 40-1000 r g from the BH.

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XMM-Newtonunveils the complex iron Kαregion of Mrk 279

Cited by 20 publications

References 61 publications

Exploring the spectral variability of the Seyfert 1.5 galaxy Markarian 530 with Suzaku

Exploring the spectral variability of the Seyfert 1.5 galaxy Markarian 530 with Suzaku

Multi-wavelength campaign on NCG 7469

Multiwavelength campaign on Mrk 509

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