The high-energy view of Seyfert galaxies throughbroad-band monitoring campaigns

Francesco UrsiniINAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna

In collaboration with: P.-O. Petrucci, G. Matt, S. Bianchi, M. Cappi,B. De Marco, A. De Rosa, J. Malzac, A. Marinucci, R. Middei, G. Ponti,

A. Tortosa

10th Oct 2018AGN 13 - Beauty and the Beast

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The two-corona model

Petrucci et al. (2013)

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cold

hot coronawarm corona

reflection

softexcess

see also Magdiarz et al. (1998)2 / 14

The two-corona model

Petrucci et al. (2018)3 / 14

High-energy campaigns

Goals: Study the spectrum and variability of AGNs testingphysical models for the high-energy emission

Broad-band: XMM+NuSTAR (optical/UV to 80 keV)

Variability: 5× 20 ks observations

A classical Seyfert 1: NGC 4593

A broad-line radio galaxy: 3C 382

A highly accreting Seyfert 1: HE 1143-1810

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NGC 4593: a day time-scale monitoring

6.09.0

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Ursini et al. (2016)5 / 14

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variablesoft excess

Ursini et al. (2016)6 / 14

The average spectrum

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Middei et al., submitted

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Warm/hot coronae: correlated variability

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3C 382

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Ursini et al. (2018)9 / 14

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no Compton bump

Ursini et al. (2018)

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HE 1143-1810

789

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Ursini et al. (in prep.)11 / 14

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Summary

NGC 4593 3C 382 HE 1143-1810MBH 1× 107 M� 1× 109 M� 1× 107 M�Eddington ratio ∼ 0.1 ∼ 0.01 ∼ 1

hot coronaTemperature variable high low

∼ 30 to > 150 keV > 40 keV ∼ 20 keVOptical depth < 0.9 to ∼ 2 < 4 ∼ 4Geometry compact† compact†/ slim disc??

outflowing?warm corona

Temperature ∼ 0.12 keV ∼ 0.6 keV ∼ 0.5 keVOptical depth ∼ 35 to ∼ 45 ∼ 20 ∼ 20Geometry slab slab slab

reflectionComponents 2 (cold+ionized) none 1 (ionized)

† Covering factor ' 10%More to come: Mrk 359 (NLS1), archival data...

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Conclusions

The two-corona model provides a viable scenario in differenttypes of AGNs - see also campaigns with different strategieson Ark 120 (Porquet et al. 2018) and NGC 7469 (Middei etal. 2018)

A complex interplay is expected between the warm and hotcoronae.

I The warm corona provides the seed photons to the hot coronaI The hot corona illuminates the warm corona → reflection

features?

The existence of a warm corona implies the presence of strongmagnetic fields and/or outflows (Rozanska et al. 2015) →there could be a link with disc winds and/or radio jets!

Potential limitations: e.g. absorption/emission lines due tothe presence of the warm corona?

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Bibliography

Magdziarz et al., 1998, MNRAS, 301, 179: A spectral decomposition of thevariable optical, ultraviolet and X-ray continuum of NGC 5548

Middei et al., 2018, A&A, 615, A163: Multi-wavelength campaign on NCG7469. IV. The broad-band X-ray spectrum

Middei et al., submitted to MNRAS: High-energy monitoring of NGC 4593 II.Broadband spectral analysis: testing the two-corona model

Petrucci et al., 2013, A&A, 549, A73: Multiwavelength campaign on Mrk 509XII. Broad band spectral analysis.

Petrucci et al., 2018, A&A, 611, A59: Testing warm Comptonization models forthe origin of the soft X-ray excess in AGN

Porquet et al., 2018, A&A 609, A42: A deep X-ray view of the bare AGN Ark120. IV. XMM-Newton and NuSTAR spectra dominated by two temperature(warm, hot) Comptonization processes

Rozanska et al., 2015, A&A, 580, A77: The existence of warm and opticallythick dissipative coronae above accretion disks

Ursini et al., 2016, MNRAS, 463, 382: High-energy monitoring of NGC 4593with XMM-Newton and NuSTAR. X-ray spectral analysis

Ursini et al., 2018, MNRAS, 478, 2663: Radio/X-ray monitoring of thebroad-line radio galaxy 3C 382. High-energy view with XMM-Newton andNuSTAR