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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
1 / 14
The two-corona model
Petrucci et al. (2013)
10−3 0.01 0.1 1 10 100 1000
10
−3
0.0
10
.1
ke
V2 (
Ph
oto
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)
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
4 / 14
NGC 4593: a day time-scale monitoring
6.09.0
12.015.018.0
Cou
nts/
sNGC 4593 XMM/pn and NuSTAR light curves and hardness ratios
XMM/pn 0.5−10 keV
0.30
0.350.40
0.45
Har
dnes
s ra
tio XMM/pn 2−10 keV/0.5−2 keV
1.01.52.02.5
Cou
nts/
s
NuSTAR 3−50 keV
0.2
0.4
0.6
0 1×105 2×105 3×105
Har
dnes
s ra
tio
Time (s)
NuSTAR 10−50 keV/3−10 keV
Ursini et al. (2016)5 / 14
10ï6
10ï5
10ï4
10ï3
10ï2Co
unts
sï1 k
eVï1
cmï2
XMM/pn and NuSTAR/FPMA data fitted with a power lawObs. 1ïI
Obs. 1ïIIObs. 2Obs. 3Obs. 4Obs. 5
1.5
0.5
1.0
2.0
5 501 10
Dat
a/m
odel
ratio
Energy (keV)
1.5
0.5
1.0
2.0
5 501 10
Dat
a/m
odel
ratio
Energy (keV)
variablesoft excess
Ursini et al. (2016)6 / 14
The average spectrum
10−3 0.01 0.1 1 10 100 1000
10
−3
0.0
1
keV
2 (
Photo
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)
warm corona
hot corona
ionizedreflection
coldreflection
Middei et al., submitted
7 / 14
Warm/hot coronae: correlated variability
10−3 0.01 0.1 1 10 100 100010
−3
0.0
12×
10
−3
5×
10
−3
0.0
20.0
5
keV
2 (
Photo
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)Middei et al., submitted
10−3 0.01 0.1 1 10 100 100010
−3
0.0
12×
10
−3
5×
10
−3
0.0
20.0
5
keV
2 (
Photo
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)10−3 0.01 0.1 1 10 100 10001
0−
30.0
12×
10
−3
5×
10
−3
0.0
20.0
5
keV
2 (
Photo
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)10−3 0.01 0.1 1 10 100 10001
0−
30.0
12×
10
−3
5×
10
−3
0.0
20.0
5
keV
2 (
Photo
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)10−3 0.01 0.1 1 10 100 10001
0−
30.0
12×
10
−3
5×
10
−3
0.0
20.0
5
keV
2 (
Photo
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)10−3 0.01 0.1 1 10 100 10001
0−
30.0
12×
10
−3
5×
10
−3
0.0
20.0
5
keV
2 (
Photo
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)
8 / 14
3C 382
11
12
13
14
15
Co
un
ts/s
XMM/pn and NuSTAR/FPMA+FPMB light curves and hardness ratios
XMM/pn 0.5−2 keV
4.0
4.5
5.0
5.5
Co
un
ts/s
XMM/pn 2−10 keV
0.34
0.36
0.38
0.40
Ha
rd
ness
ra
tio XMM/pn 2−10 keV/0.5−2 keV
1.6
2.0
2.4
2.8
Co
un
ts/s
NuSTAR 3−10 keV
0.6
0.8
1.0
1.2
Co
un
ts/s
NuSTAR 10−50 keV
0.3
0.4
0.5
0 20 40
Ha
rd
ness
ra
tio
0 20 40 0 20 40
Time (ks)
NuSTAR 10−50 keV/3−10 keV
0 20 40 0 20 40
Ursini et al. (2018)9 / 14
10−4
10−3
10−2
5 500.01 0.1 1 10
keV
2 (
ph
s−
1 k
eV−
1 c
m−
2)
Energy (keV)
no Compton bump
Ursini et al. (2018)
3.0
3.2
3.4
3.6
0.5 1.0 1.5 2.0
ρ=0.72
p=0.17
Pri
mary
flu
x(3
−10 k
eV
)
Soft excess flux(0.3−2 keV)
10 / 14
HE 1143-1810
789
1011121314
Co
un
ts/s
XMM/pn and NuSTAR/FPMA+FPMB light curves and hardness ratios
XMM/pn 0.5−2 keV
2.0
2.5
3.0
3.5
4.0
Co
un
ts/s
XMM/pn 2−10 keV
0.26
0.28
0.30
0.32
0.34
0.36
Ha
rd
ness
ra
tio XMM/pn 2−10 keV/0.5−2 keV
1.0
1.2
1.4
1.6
1.8
2.0
Co
un
ts/s
NuSTAR 3−10 keV
0.4
0.6
0.8
Co
un
ts/s
NuSTAR 10−50 keV
0.3
0.4
0.5
0.6
0 20 40
Ha
rd
ness
ra
tio
0 20 40 0 20 40
Time (ks)
NuSTAR 10−50 keV/3−10 keV
0 20 40 0 20 40
Ursini et al. (in prep.)11 / 14
0.01 0.1 1 10 10010
−4
10
−3
0.0
1
keV
2 (
Photo
ns c
m−
2 s
−1 k
eV
−1)
Energy (keV)Ursini et al. (in prep.)
12 / 14
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...
13 / 14
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?
14 / 14
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