The first broad-band X-ray view of the narrow-line Seyfert 1 Ton S180

Matzeu, G. A.; Nardini, E.; Parker, M. L.; Reeves, J. N.; Braito, V.; Porquet, D.; Middei, R.; Kammoun, E. S.; Lusso, Elisabeta; Alston, W. N.; Giustini, M.; Lobban, A.; Joyce, Aoife; Igo, Z.; Ebrero, J.; Ballo, L.; Santos-Lleó, M.; Schartel, N.

doi:10.1093/mnras/staa2076

Cited by 27 publications

(23 citation statements)

References 100 publications

(117 reference statements)

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“…They are also consistent with those measured in XMM-Newton AGN samples (kT warm ∼ 0.3−1 keV, τ warm ∼ 10−20; e.g. Porquet et al 2004;Bianchi et al 2009) and in several individual X-ray broadband spectral analyses of AGN, such as: Mrk 509 (Petrucci et al 2013;Mehdipour et al 2015), Ark 120 (Matt et al 2014;Porquet et al 2018), HE 1143−1810 (Ursini et al 2020), NGC 4593 (Middei et al 2019), Mrk 359 (Middei et al 2020), TON S180 (Matzeu et al 2020), and ESO 511-G030 (Ghosh & Laha 2021). Very recent state-of-the-art simulations have been performed that show that a warm corona with such properties can indeed exist, until sufficient internal mechanical heating is present, and that warm and hot coronae can co-exist (Petrucci et al 2018(Petrucci et al , 2020Ballantyne 2020;Ballantyne & Xiang 2020).…”

Section: Summary and Discussionsupporting

confidence: 88%

“…We also find that both the cold disc and the warm corona can provide seed photons to the hot corona. Such a model, combining Comptonisation and relativistic reflection, has been proven to explain the X-ray broadband spectra of several other AGN, such as: Ark 120 (Porquet et al 2018), Fairall 9 (Lohfink et al 2016), Ton S180 (Matzeu et al 2020), and ESO 362-G18 (Xu et al 2021). In a forthcoming article, we will study the spectral energy distribution of Mrk 110 from optical-UV to hard X-ray excess, as done previously for the bare AGN Ark 120 (Porquet et al 2019).…”

Section: Summary and Discussionmentioning

confidence: 99%

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The first simultaneous X-ray broadband view of Mrk 110 with XMM-Newton and NuSTAR

Porquet

Reeves

Grosso

et al. 2021

A&A

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Context. Soft and hard X-ray excesses, compared to the continuum power-law shape between ∼2−10 keV, are common features observed in the spectra of active galactic nuclei (AGN) and are associated with the accretion disc-corona system around the supermassive black hole. However, the dominant process at work is still highly debated and has been proposed to be either relativistic reflection or Comptonisation. Such an investigation can be problematic for AGN that have significant intrinsic absorption, either cold or warm, which can severely distort the observed continuum. Therefore, AGN with no (or very weak) intrinsic absorption along the line-of-sight, called bare AGN, are the best targets for directly probing disc-corona systems. Aims. We aim to characterise the main X-ray spectral physical components from the bright bare broad-line Seyfert 1 AGN Mrk 110, as well as the physical process(es) at work in its disc-corona system viewed almost face-on. Methods. We perform the X-ray broadband spectral analysis thanks to two simultaneous XMM-Newton and NuSTAR observations performed on November 16−17, 2019, and April 5−6, 2020. We also use a deep NuSTAR observation obtained in January 2017 for the spectral analysis above 3 keV. Results. The broadband X-ray spectra of Mrk 110 are characterised by the presence of a prominent and absorption-free smooth soft X-ray excess, moderately broad O VII and Fe Kα emission lines, and a lack of a strong Compton hump. The continuum above ∼3 keV is very similar at both epochs, while some variability (stronger when brighter) is present for the soft X-ray excess. A combination of soft and hard Comptonisation by a warm and hot corona, respectively, plus mildly relativistic disc reflection reproduce the broadband X-ray continuum very well. The inferred warm corona temperature, kTwarm ∼ 0.3 keV, is similar to the values found in other sub-Eddington AGN, whereas the hot corona temperature, kThot ∼ 21−31 keV (depending mainly on the assumed hot corona geometry), is found to be in the lower range of the values measured in AGN.

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Section: Summary and Discussionsupporting

confidence: 88%

Section: Summary and Discussionmentioning

confidence: 99%

The first simultaneous X-ray broadband view of Mrk 110 with XMM-Newton and NuSTAR

Porquet

Reeves

Grosso

et al. 2021

A&A

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“…Although this is often not formally considered in detail in the literature, in the warm corona interpretation there should still be reflection from the standard disk outside of the warm corona. We therefore also test a hybrid model like Matzeu et al (2020) did, that includes a warm Comptonization component and a relativistic reflection component, both of which can contribute to the soft excess. Here we make use of the relxillCp model, which assumes both a Comptonization continuum and a fixed density of 10 15 cm −3 .…”

Section: Model C: Hybrid Modelmentioning

confidence: 99%

The Nature of Soft Excess in ESO 362-G18 Revealed by XMM-Newton and NuSTAR Spectroscopy

García

Walton

et al. 2021

ApJ

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We present a detailed spectral analysis of the joint XMM-Newton and NuSTAR observations of the active galactic nuclei (AGNs) in the Seyfert 1.5 Galaxy ESO 362-G18. The broadband (0.3-79 keV) spectrum shows the presence of a power-law continuum with a soft excess below 2 keV, iron Kα emission (∼6.4 keV), and a Compton hump (peaking at ∼20 keV). We find that the soft excess can be modeled by two different possible scenarios: a warm (kT e ∼ 0.2 keV) and optically thick (τ ∼ 34) Comptonizing corona, or with a relativistically blurred reflection off a high-density ( [ ]>n log cm 18.3 e 3) inner disk. These two models cannot be easily distinguished solely from their fit statistics. However, the low temperature (kT e ∼ 20 keV) and the thick optical depth (τ ∼ 5) of the hot corona required by the warm corona scenario are uncommon for AGNs. We also fit a "hybrid" model, which includes both disk reflection and a warm corona. Unsurprisingly, as this is the most complex of the models considered, this provides the best fit, and more reasonable coronal parameters. In this case, the majority of the soft excess flux arises in the warm corona component. However, based on recent simulations of warm coronae, it is not clear whether such a structure can really exist at the low accretion rates relevant for ESO 362-G18 ( m 0.015). This may therefore argue in favor of a scenario in which the soft excess is instead dominated by the relativistic reflection. Based on this model, we find that the data would require a compact hot corona (h ∼ 3 R Horizon ) around a rapidly spinning (a å > 0.927) black hole.Unified Astronomy Thesaurus concepts: Supermassive black holes (1663); X-ray astronomy (1810); Seyfert galaxies (1447); High energy astrophysics (739); Active galactic nuclei (16); Astrophysical black holes (98); Spectroscopy (1558); X-ray active galactic nuclei (2035)

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“…Two Comptonising components, one optically thick and warm (warm corona, wc) and the other optically thin and hot (hot corona, hc), have often been used to reproduce broadband AGN spectra (e.g. Porquet et al 2018;Middei et al 2018Middei et al , 2019bUrsini et al 2018Ursini et al , 2020Noda & Done 2018;Kubota & Done 2018;Petrucci et al 2018;Matzeu et al 2020), therefore we tested the so-called two-corona model on the present dataset. In Xspec, such a model appears as: redden× TBabs× const× ×[small BB + nthcomp wc +nthcomp hc +xillvercp].…”

Section: Broadband Data: Testing the Two-corona Modelmentioning

confidence: 99%

The soft excess of the NLS1 galaxy Mrk 359 studied with an XMM-Newton-NuSTAR monitoring campaign

Middei

Petrucci²,

Bianchi

et al. 2020

A&A

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Context. Joint XMM-Newton and NuSTAR multiple exposures allow us to disentangle the different emission components of active galactic nuclei (AGNs) and to study the evolution of their different spectral features. In this work, we present the timing and spectral properties of five simultaneous XMM-NewtonandNuSTAR observations of the Narrow Line Seyfert 1 galaxy Mrk 359. Aims. We aim to provide the first broadband spectral modeling of Mrk 359 describing its emission spectrum from the UV up to the hard X-rays. Methods. We performed temporal and spectral data analysis, characterising the amplitude and spectral changes of the Mrk 359 time series and computing the 2–10 keV normalised excess variance. The spectral broadband modelling assumes the standard hot Comptonising corona and reflection component, while for the soft excess we tested two different models: a warm, optically thick Comptonising corona (the two-corona model) and a reflection model in which the soft-excess is the result of a blurred reflected continuum and line emission (the reflection model). Results. High and low flux states were observed during the campaign. The former state has a softer spectral shape, while the latter shows a harder one. The photon index is in the 1.75–1.89 range, and only a lower limit to the hot-corona electron temperature can be found. A constant reflection component, likely associated with distant matter, is observed. Regarding the soft excess, we found that among the reflection models we tested, the one providing the better fit (reduced χ2 = 1.14) is the high-density one. However, a significantly better fit (reduced χ2 = 1.08) is found by modelling the soft excess with a warm Comptonisation model. Conclusions. The present analysis suggests the two-corona model as the best scenario for the optical-UV to X-ray emission spectrum of Mrk 359.

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The first broad-band X-ray view of the narrow-line Seyfert 1 Ton S180

Cited by 27 publications

References 100 publications

The first simultaneous X-ray broadband view of Mrk 110 with XMM-Newton and NuSTAR

The first simultaneous X-ray broadband view of Mrk 110 with XMM-Newton and NuSTAR

The Nature of Soft Excess in ESO 362-G18 Revealed by XMM-Newton and NuSTAR Spectroscopy

The soft excess of the NLS1 galaxy Mrk 359 studied with an XMM-Newton-NuSTAR monitoring campaign

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