The high-energy view of Seyfert galaxies through broad-band monitoring campaigns Francesco Ursini INAF-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 2018 AGN 13 - Beauty and the Beast 1 / 14
The two-corona model Petrucci et al. (2013) kev 2 (Photons cm 2 s 1 kev 1 ) 10 3 0.01 0.1 warm corona soft excess hot corona cold reflection 10 3 0.01 0.1 1 10 100 1000 Energy (kev) 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 testing physical 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 4 / 14
NGC 4593: a day time-scale monitoring Hardness ratio Hardness ratio NGC 4593 XMM/pn and NuSTAR light curves and hardness ratios 18.0 XMM/pn 0.5 10 kev 15.0 12.0 9.0 6.0 0.45 XMM/pn 2 10 kev/0.5 2 kev 0.40 0.35 0.30 NuSTAR 3 50 kev 2.5 2.0 1.5 1.0 NuSTAR 10 50 kev/3 10 kev 0.6 0.4 0.2 0 1 10 5 2 10 5 3 10 5 Ursini et al. (2016) Time (s) 5 / 14
Counts s 1 kev 1 cm 2 10 2 10 3 10 4 10 5 XMM/pn and NuSTAR/FPMA data fitted with a power law Obs. 1 I Obs. 1 II Obs. 2 Obs. 3 Obs. 4 Obs. 5 Data/model ratio 10 6 2.0 1.5 1.0 variable soft excess 0.5 1 5 10 50 Ursini et al. (2016) Energy (kev) 6 / 14
The average spectrum warm corona kev 2 (Photons cm 2 s 1 kev 1 ) 10 3 0.01 hot corona cold reflection ionized reflection 10 3 0.01 0.1 1 10 100 1000 Energy (kev) Middei et al., submitted 7 / 14
Warm/hot coronae: correlated variability kev 2 (Photons cm 2 s 1 kev 1 ) 10 3 2 10 3 5 10 3 0.01 0.02 0.05 10 3 0.01 0.1 1 10 100 1000 Energy (kev) Middei et al., submitted 8 / 14
3C 382 XMM/pn and NuSTAR/FPMA+FPMB light curves and hardness ratios Hardness ratio Hardness ratio 15 14 13 12 11 5.5 5.0 4.5 4.0 0.40 0.38 0.36 0.34 2.8 2.4 2.0 1.6 1.2 1.0 0.8 0.6 0.5 0.4 0.3 0 20 40 Ursini et al. (2018) XMM/pn 0.5 2 kev XMM/pn 2 10 kev XMM/pn 2 10 kev/0.5 2 kev NuSTAR 3 10 kev NuSTAR 10 50 kev NuSTAR 10 50 kev/3 10 kev 0 20 40 0 20 40 Time (ks) 0 20 40 0 20 40 9 / 14
kev 2 (ph s 1 kev 1 cm 2 ) 10 2 10 3 Primary flux(3 10 kev) 3.6 3.4 3.2 ρ=0.72 p=0.17 no Compton bump 3.0 0.5 1.0 1.5 2.0 Soft excess flux(0.3 2 kev) 10 4 0.01 0.1 1 5 10 50 Ursini et al. (2018) Energy (kev) 10 / 14
HE 1143-1810 Hardness ratio 14 13 12 11 10 9 8 7 4.0 3.5 3.0 2.5 2.0 0.36 0.34 0.32 0.30 0.28 0.26 2.0 1.8 1.6 1.4 1.2 1.0 0.8 0.6 0.4 XMM/pn and NuSTAR/FPMA+FPMB light curves and hardness ratios XMM/pn 0.5 2 kev XMM/pn 2 10 kev XMM/pn 2 10 kev/0.5 2 kev NuSTAR 3 10 kev NuSTAR 10 50 kev Hardness ratio 0.6 NuSTAR 10 50 kev/3 10 kev 0.5 0.4 0.3 0 20 40 Ursini et al. (in prep.) 0 20 40 0 20 40 Time (ks) 0 20 40 0 20 40 11 / 14
kev 2 (Photons cm 2 s 1 kev 1 ) 10 4 10 3 0.01 0.01 0.1 1 10 100 Ursini et al. (in prep.) Energy (kev) 12 / 14
Summary NGC 4593 3C 382 HE 1143-1810 M BH 1 10 7 M 1 10 9 M 1 10 7 M Eddington ratio 0.1 0.01 1 hot corona Temperature variable high low 30 to > 150 kev > 40 kev 20 kev Optical depth < 0.9 to 2 < 4 4 Geometry compact compact / slim disc?? outflowing? warm corona Temperature 0.12 kev 0.6 kev 0.5 kev Optical depth 35 to 45 20 20 Geometry slab slab slab reflection Components 2 (cold+ionized) none 1 (ionized) Covering factor 10% More to come: Mrk 359 (NLS1), archival data... 13 / 14
Conclusions The two-corona model provides a viable scenario in different types of AGNs - see also campaigns with different strategies on Ark 120 (Porquet et al. 2018) and NGC 7469 (Middei et al. 2018) A complex interplay is expected between the warm and hot coronae. The warm corona provides the seed photons to the hot corona The hot corona illuminates the warm corona reflection features? The existence of a warm corona implies the presence of strong magnetic 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 to the presence of the warm corona? 14 / 14
Bibliography Magdziarz et al., 1998, MNRAS, 301, 179: A spectral decomposition of the variable optical, ultraviolet and X-ray continuum of NGC 5548 Middei et al., 2018, A&A, 615, A163: Multi-wavelength campaign on NCG 7469. 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 509 XII. Broad band spectral analysis. Petrucci et al., 2018, A&A, 611, A59: Testing warm Comptonization models for the 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 Ark 120. 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 optically thick dissipative coronae above accretion disks Ursini et al., 2016, MNRAS, 463, 382: High-energy monitoring of NGC 4593 with XMM-Newton and NuSTAR. X-ray spectral analysis Ursini et al., 2018, MNRAS, 478, 2663: Radio/X-ray monitoring of the broad-line radio galaxy 3C 382. High-energy view with XMM-Newton and NuSTAR