broad-band x-ray variability of agns with suzaku y. terashima ehime univ. and the suzaku swg team
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Broad-Band X-ray Variability of AGNs with Suzaku
Y. TerashimaEhime Univ.
and
The Suzaku SWG team
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Outline
• The Suzaku Satellite
• Broad band X-ray spectral variability in – MCG-6-30-15– MCG-5-23-16– NGC 4051
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The Suzaku Satellite
Japan-US X-ray ObservatoryLaunched on July 10, 2005
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The Suzaku Satellite
Japan-US X-ray ObservatoryLaunched on July 10, 2005 Named after legendary red bird
Suzaku in Chinese myth
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The Four Guardians in Chinese Myth
Red Bird - Suzaku 朱雀[South]
White Tiger白虎[West]
Blue Dragon青龍 [East]
Black Turtle玄武 [North]
Infrared Images of inner walls of ancient tomb in Asuka, Japan
© National Research Institute for Cultural Properties
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The Suzaku Satellite
• Broad band coverage• Low background / High sensitivity at High E
Detection of faint hard sources or highly absorbed sources
Spectral variability on short time scales
A powerful new tool to study the central engine of AGNsAO-2 deadline Dec.1see http://www.astro.isas.jaxa.jp/suzaku
1 10 100Energy (keV)
NGC 2110 Okajima et al.
X-ray Imaging Spectrometer (CCD)
Hard X-ray Detector
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X-ray Spectral Components and Variability in AGNs
AGN spectral components - Compton refelection, Fe-K line etc.
Hard X-ray (>10 keV) essential for unambiguous interpretation ofcontinuum and broad Fe line
X-ray Variability Complex spectral variability
steeper slope at higher flux Intrinsic changes
l.o.s. absorption? multiple component s ?
Time resolved spectroscopy with Suzaku
X-raysource
reflection
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(1) MCG-6-30-15Miniutti, Fabian et al. 2006, PASJ in press(astro-ph/0609521)
Constant Reflection hump
Suzaku lightcurve
Factor >3 variability
PL + Strong Fe-K line and reflection hump
Broad Fe-K line from Kerr BH?
Smaller amplitude at higher E
High flux
Low flux
Net 300 ksec
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MCG-6-30-15High - Low Difference Spectrum
Pure power law (=2.2)
Fe line and reflection hump appear constant.
Broad line only mildly varied.
Light bending effect around a Kerr BH?
(Miniutti & Fabian 2004)
5 10 40Energy (keV)
Direct spectral fits to variable component
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(2) MCG-5-23-16Reeves et al. 2006, PASJ, in press
High flux = Red; Low flux = Blue; Reflection:Black
Continuum varied by ~40% over 220 ks duration
PL + Fe line + reflection
i=53+7/-9 deg Rin = 37+25/-10Rg=1.9 power law
Fe line
reflection
Narrow(<50 eV) + Diskline fit
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MCG-5-23-15High - Low Difference Spectrum
Variable component:
pure power law (=1.9) modified by absorption
Fe line and reflection hump
~ constant
Two component model
var. PL + cont reflection
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1
2
0 105 2x105 (s)
Time (s)
0.5-10 keVNet 86 ksec
(3) NGC 4051Terashima et al. in prep.
1/2-1/3 of historical average9x10-12 ergs s-1
Factor x7-8 flares
=2 PL
reflection
Smaller amplitude at higher E
Similar spec.
PL + Fe + reflection
C/S
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NGC 4051Difference Spectrum
=2.1+0.2/-0.1
Variable power law ~2.1Constant Fe+reflectionTwo comp. model
Const. narrow Fe line (<50 eV), sharp Fe-K edge:
Consistent w/ reprocessing & reverberation by distant matter
Variable absorption at <3 keV
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NGC 4051 in 2002Very low flux state with XMM-Newton
~1/2 of Suzaku flux
Highly absorbed component disappeared at the lowest flux state.
Presence of additional absorbed PL or variabiltiy of absorption column
Difference (Green - Blue)
NH = 1.5x1023 cm-2
1 5 10Energy (keV)
Haba et al. in prep.
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Summary
• Suzaku - new powerful observatory to study AGNsAO-2 due Dec. 1 (http://www.astro.isas.jaxa.jp/suzaku)
• ``Two component’’ behavior commonVariable PL - vicinity of BHConstant Fe line + reflection hump - G.R. effect or distant matte
r
• Time dependent absorption in NGC 4051
• Future: Mechanism of intrinsic variability
G.R. effect, energy release process
Nature of variable absorber - physics of ``torus’’ / ionized absorber
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NGC 4051