Broad-Line Radio Galaxies in the NuSTAR Era

Broad-Line Radio Galaxies in the NuSTAR Era
Anne M. Lohfink
with help from
Laura Brenneman (CfA), Andy Fabian (IoA), Svetlana Jorstad (BU), Alan
Marscher (BU), Jon Miller (UM), Richard Mushotzky (UMCP), Chris Reynolds
(UMCP), Francesco Tombesi (UMCP)
and the NuSTAR AGN Team
Broad-Line Radio Galaxies in the NuSTAR Era
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Broad-Line Radio Galaxies in the NuSTAR Era
2
tinuum
10−3
• Comptonization of disk photons in
corona → modeled power law con-
10−4
body (for AGN: UV)
ν Fν
0.01
• accretion disk: multi-color disk black
0.1
1
The Basics – X-ray Spectroscopy as a Key Tool I
0.1
1
10
100
Energy [keV]
Broad-Line Radio Galaxies in the NuSTAR Era
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Reflection – X-ray Spectroscopy as a Key Tool II
continuum photons will get scattered
from...
• ... the torus/outer accretion disk →
cold reflection
• ... the inner accretion disk → ionized
ν Fν
10−5 10−4 10−3 0.01 0.1
1
10
reflection
0.1
1
10
100
Energy [keV]
Broad-Line Radio Galaxies in the NuSTAR Era
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Advancing our Understanding
by Studying the X-ray Reflection Spectrum
Broad-Line Radio Galaxies in the NuSTAR Era
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10
1
ν Fν
10−5 10−4 10−3 0.01 0.1
0.1
1
10
100
Energy [keV]
Broad-Line Radio Galaxies in the NuSTAR Era
6
Begelman 2012, Kinney 2009
Chatterjee 2009, Lohfink 2013
Jet knot formation and disruption of inner accretion disk go alongside.
Broad-Line Radio Galaxies in the NuSTAR Era
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Observing Jet Formation
1)
2)
3)
4)
Broad-Line Radio Galaxies in the NuSTAR Era
111
000
000
111
000
111
0
1
0
1
8
→ Detection of recession of inner edge
of accretion disk.
→ First spin constraint of jetted AGN
+0.002
→ Spin is high (0.994−
0.003)!
Ratio
0.8 1 1.2
⇒ Use X-ray spectra of 3C120:
Ratio
Ratio
1 1.11.21.3 1 1.11.21.3
Observing Jet Formation II
0.5
1
2
5
10
Energy (keV)
⇒ Use Radio as Test:
Lohfink et al. 2013
Broad-Line Radio Galaxies in the NuSTAR Era
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Advancing our Understanding
using the hard X-ray band with NuSTAR
Broad-Line Radio Galaxies in the NuSTAR Era
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Measuring the Comptonization Parameters
Key Questions:
• properties of e−:
geometry, τ , kTe−
• Are the temperatures different
to radio-quiet AGN?
Energy [keV]
How?
Study spectra of a sample of objects from the UV to high X-ray energies.
Broad-Line Radio Galaxies in the NuSTAR Era
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The Sample
• 3C382 (with Swift)
(Ballantyne et al. 2014)
• 3C120 (with Swift & XMM)
(Lohfink et al. in prep)
• 3C390.3 (with Swift & Suzaku)
(Lohfink et al. in prep)
• Cyg A (with Swift)
(Reynolds et al. in prep)
• Cen A (with Swift & XMM)
(Fürst et al. in prep)
Results still preliminary!
Broad-Line Radio Galaxies in the NuSTAR Era
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The Coronal Temperature
4
Seyferts
BLRGs
3
2
1
0
75
125
175
225 unconstr.
⇒ Tentatively different distributions!
Broad-Line Radio Galaxies in the NuSTAR Era
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The Broad-band View
10−9
3C120
3C390.3
ν*F ν [ergs/s/cm2]
10−10
10−11
10−12
10−13
10−14
0.01
0.10
1.00
Energy [keV]
10.00
3C382
=> Corona is compact!
Broad-Line Radio Galaxies in the NuSTAR Era
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Variability of the continuum – 3C382
(Ballantyne et al. 2014)
→ Temperature flux dependent!?
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Summary
• Jet formation related to changes in the inner accretion disk.
• NuSTAR offers new dimension.
• Seyferts and BLRGs seem to have different coronal temperature distributions.
• Coronal temperature is variable and possibly flux dependent.
Outlook
• Finish analysis of remaining BLRGs.
• Model discrepancy of UV emission vs. X-ray modeling.
Broad-Line Radio Galaxies in the NuSTAR Era
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The End
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