Multi-wavelength campaign on NCG 7469

Middei, R.; Bianchi, S.; Cappi, M.; Petrucci, P.-O.; Ursini, F.; Arav, Nahum; Behar, E.; Branduardi‐Raymont, G.; Costantini, E.; Marco, Barbara De; Gesu, Laura Di; Ebrero, J.; Kaastra, J. S.; Kaspi, S.; Kriss, Gerard A.; Mao, Junjie; Mehdipour, M.; Paltani, S.; Peretz, U.; Ponti, G.

doi:10.1051/0004-6361/201832726

Cited by 37 publications

(30 citation statements)

References 66 publications

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“…In this framework, the lack of variation of the soft excess strength with M BH may be explained by bulk motion Comptonization, or by thermal Comptonization, provided that the accretion power released in the disk and in the corona vary in concert in such a way to produce the proper physical conditions with optical depth τ > 1 and kT ∼ 1 keV (e.g., Done et al 2012;Różańska et al 2015;Petrucci et al 2018). This conclusion is supported and strengthened by recent findings obtained applying physically motivated warm Comptonization models to fit high-quality broad-band spectra of different AGN, obtained from simultaneous long observations carried out by XMM-Newton and NuSTAR (e.g., Porquet et al 2018;Middei et al 2018;Ursini et al 2018) We conclude by summarizing the main findings of our work. Starting from a flux-limited sample of 89 type 1 AGN (59 BLS1s and 30 NLS1s), with BLS1s and NLS1s matched in X-ray luminosities, and with NLS1s with lower M BH on average and considerably larger λ Edd values than BLS1s, we defined a clean sample of 68 objects (46 BLS1s and 22 NLS1s) after excluding 13 BLS1s and 8 NLS1s severely affected by warm absorbers that hamper the proper characterization of the soft excess.…”

Section: Resultssupporting

confidence: 88%

The soft X-ray excess: NLS1s versus BLS1s

Gliozzi

Williams

2019

Monthly Notices of the Royal Astronomical Society

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The soft X-ray excess -the excess of X-rays below 2 keV with respect to the extrapolation of the hard X-ray spectral continuum model -is a very common feature among type 1 active galactic nuclei (AGN); yet the nature of the soft X-ray excess is still poorly understood and hotly debated. To shed some light on this issue, we have measured in a model-independent way the soft excess strength in a flux-limited sample of broad-line and narrow-line Seyfert 1 galaxies (BLS1s and NLS1s) that are matched in X-ray luminosity but different in terms of the black hole mass and the accretion rate values, with NLS1s being characterized by smaller M BH and larger m values. Our analysis, in agreement with previous studies carried out with different AGN samples, indicates that: 1) a soft excess is ubiquitously detected in both BLS1s and NLS1s; 2) the strength of the soft excess is significantly larger in the NLS1 sample, compared to the BLS1 sample; 3) combining the two samples, the strength of the soft excess appears to positively correlate with the photon index as well as with the accretion rate, whereas there is no correlation with the black hole mass. Importantly, our work also reveals the lack of an anticorrelation between the soft excess strength and the luminosity of the primary X-ray component, predicted by the absorption and reflection scenarios. Our findings suggest that the soft excess is consistent with being produced by a warm Comptonization component. Larger, more complete samples of NLS1s and BLS1s are needed to confirm these conclusions.

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Section: Resultssupporting

confidence: 88%

The soft X-ray excess: NLS1s versus BLS1s

Gliozzi

Williams

2019

Monthly Notices of the Royal Astronomical Society

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“…As already reported in XMM-Newton and NuSTAR simultaneous observations of other sources, the pn spectra are flatter than the NuSTAR spectra in the common bandpass 3-10 keV, with a difference in photon index of ∼0.1 (e.g. Cappi et al 2016;Fürst et al 2016;Middei et al 2018;Ponti et al 2018). In some cases the largest discrepancy was found in the 3-5 keV band, where NuSTAR measures a higher flux (e.g.…”

Section: Spectral Analysissupporting

confidence: 71%

“…Crummy et al 2006;Ponti et al 2006;Walton et al 2013;Jiang et al 2018;García et al 2019) and 'warm' Comptonization (see e.g. Magdziarz et al 1998;Mehdipour et al 2011;Done et al 2012;Petrucci et al 2013;Boissay et al 2014;Matt et al 2014;Middei et al 2018;Porquet et al 2018;Petrucci et al 2018;Ursini et al 2018;Middei et al 2019). In the latter hypothesis the optical-UV emission and soft X-ray excess could originate from the upper layer of the accretion disc, consisting of a warm (kT e ∼ 1 keV) optically thick (τ ∼ 10 − 20) slab-like corona (Różańska et al 2015;Petrucci et al 2018).…”

Section: Introductionmentioning

confidence: 99%

NuSTAR/XMM–Newton monitoring of the Seyfert 1 galaxy HE 1143-1810

Ursini¹,

Petrucci

Bianchi

et al. 2020

A&A

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Aims. We test the two-corona accretion scenario for active galactic nuclei in the case of the 'bare' Seyfert 1 galaxy HE 1143-1810. Methods. We perform a detailed study of the broad-band UV-X-ray spectral properties and of the short-term variability of HE 1143-1810. We present results of a joint XMM-Newton and NuSTAR monitoring of the source, consisting of 5 × 20 ks observations, each separated by 2 days, performed in December 2017. Results. The source is variable in flux among the different observations, and a correlation is observed between the UV and X-ray emission. Moderate spectral variability is observed in the soft band. The time-averaged X-ray spectrum exhibits a cut-off at ∼ 100 keV consistent with thermal Comptonization. We detect an iron Kα line consistent with being constant during the campaign and originating from a mildly ionized medium. The line is accompanied by a moderate, ionized reflection component. A soft excess is clearly present below 2 keV and is well described by thermal Comptonization in a 'warm' corona with a temperature of ∼ 0.5 keV and a Thomson optical depth of ∼ 17 − 18. For the hot hard X-ray emitting corona, we obtain a temperature of ∼ 20 keV and an optical depth of ∼ 4 assuming a spherical geometry. A fit assuming a jet-emitting disc (JED) for the hot corona also provides a nice description of the broad-band spectrum. In this case, the data are consistent with an accretion rate varying between ∼ 0.7 and ∼ 0.9 in Eddington units and a transition between the outer standard disc and the inner JED at ∼ 20 gravitational radii. Conclusions. The broad-band high-energy data agree with an accretion flow model consisting of two phases: an outer standard accretion disc with a warm upper layer, responsible for the optical-UV emission and the soft X-ray excess, and an inner slim JED playing the role of a hard X-ray emitting hot corona.

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“…Some of these features in this band may be directly attributed to the detector calibration uncertainties (e.g. Si K-edge 1.84 keV), and at the Au M-edge (∼2.4 keV) (see Kaastra et al 2011;Di Gesu et al 2015;Ursini et al 2015;Cappi et al 2016;Middei et al 2018a, for discussions and comparisons). We notice that modelling these features with Gaussian lines or The straight blue lines account for the average rates.…”

Section: Spectral and Timing Analysismentioning

confidence: 99%

A broadband X-ray view of the NLSy1 1E 0754.6+3928

Middei

Tombesi

Vagnetti

et al. 2020

A&A

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Context. The soft X-ray band of many active galactic nuclei (AGN) is affected by obscuration due to partially ionised matter crossing our line of sight. In this context, two past XMM-Newton observations (6 months apart) and a simultaneous NuSTAR-Swift (∼8 years later) exposure of the Narrow Line Seyfert 1 galaxy 1E 0754.6+392.8 revealed an intense and variable WA and hints of additional absorbers in the Fe Kα band. Aims. We aim at providing the first X-ray characterisation of this AGN discussing its broadband (0.3-79 keV) spectrum and temporal properties. Methods. We conduct a temporal and spectroscopic analysis on two ∼10 ks (net exposure) XMM-Newton snapshots performed in April and October 2006. We also study the high energy behaviour of 1E 0754.6+392.8 modelling its broadband spectrum using simultaneous Swift-NuSTAR data. Both phenomenological and physically motivated models are tested. Results. We find the presence of flux variability (∼150% and 30% for 0.3-2 and 2-10 keV bands, respectively) and spectral changes at months timescales (∆Γ ∼0.4). A reflection component that is consistent with being constant over years and arising from relatively cold material far from the central super massive black hole is detected. The main spectral feature shaping the 1E 0754.6+392.8 spectrum is a warm absorber. Such a component is persistent over the years and variability of its ionisation and column density is observed down on months in the ranges 3×10 22 cm −2 N H 7.2 × 10 22 cm −2 and 1.5 log(ξ/erg s −1 cm) 2.1. Despite the short exposures, we find possible evidence of two additional high-ionisation and high-velocity outflow components in absorption. Conclusions. Our analysis suggests the existence of a complex system of absorbers in 1E 0754.6+392.8. Longer exposures are mandatory in order to characterise, on more solid grounds, the absorbers in this AGN.

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Multi-wavelength campaign on NCG 7469

Cited by 37 publications

References 66 publications

The soft X-ray excess: NLS1s versus BLS1s

The soft X-ray excess: NLS1s versus BLS1s

NuSTAR/XMM–Newton monitoring of the Seyfert 1 galaxy HE 1143-1810

A broadband X-ray view of the NLSy1 1E 0754.6+3928

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