Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert...
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![Page 1: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/1.jpg)
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Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line
Structure in the Seyfert GalaxiesKen EBISAWA
Naoki ISO, Takehiro MIYAKAWA, Hajime INOUE
(JAXA/ISAS)
![Page 2: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/2.jpg)
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Contents of the Talk
1. Properties of the Seyfert Galaxies2. Variable Partial Covering Model3. Explanation of the Observed Properties4. Conclusion
![Page 3: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/3.jpg)
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1. Properties of the Seyfert Galaxies
a) Significant flux variationb) “Seemingly” broad iron-line featurec) Small variation in the iron energy band
![Page 4: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/4.jpg)
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1a. Significant flux-variation
Suzaku observations of NGC4051 and NGC3516 (0.2—12 keV, 1bin=512sec)
Significant and aperiodic variations in various time-scales
![Page 5: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/5.jpg)
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1b.“Seemingly” broad iron-line feature
• ASCA MCG-6-30-15
(Tanaka+ 1995)
• Looks like an iron K-line “broadened” by relativistic effects • Interpretation depends on the choice of models
![Page 6: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/6.jpg)
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1c. Small variation in the iron energy band
• MCG-6-30-15 with ASCAEnergy dependence of Root Mean Square (RMS) variation
• The RMS spectrum drops significantly at the iron K energy band (model independent result!)
(Matsumoto+ 2003)
〜 105 sec
〜 104 sec
![Page 7: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/7.jpg)
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Contents of the Talk
1. Properties of the Seyfert Galaxies2. Variable Partial Covering Model3. Explanation of the Observed Properties4. Conclusion
![Page 8: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/8.jpg)
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2. Variable Partial Covering Model• Several authors have proposed idea of partial
covering for MCG-6-30-15: e.g., Matsuoka+ (1990); McKernan and Yaqoob (1998); Miller, Turner and Reeves (2008, 2009)
• We have found “double partial covering” with two different warm absorbers can explain the Suzaku MCG-6-30-15 spectra (Miyakawa, Ebisawa and Inoue 2012)
![Page 9: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/9.jpg)
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Double partial covering
X-ray source
xspec notation: partcov(a) * exp(-NHs(x)) × partcov(a) exp(-NHs(x))
Partial covering by thick absorber with NH~1024.2cm-2 and x~101.6 and the partial covering fraction a
Partial covering by thin and more ionized absorber with NH~1022.1cm-2 and x~101.9 and the same partial covering fraction a
![Page 10: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/10.jpg)
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2. Variable Partial Covering Model• Observed spectral variation of MCG-6-30-15 is
mostly explained by only variation of the partial covering fraction (Miyakawa, Ebisawa and Inoue 2012, PASJ, 64, 140)
• Variable Partial Covering model can explain spectral variations of other 20 Seyfert galaxies observed with Suzaku (Iso, Ebisawa+ 2013 in prep.).
![Page 11: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/11.jpg)
11• Miyakawa, Ebisawa and Inoue (2012)
![Page 12: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/12.jpg)
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Outer disk reflection
Direct component
Heavily absorbed component
• Double Partial covering by absorbing clouds with thick core and thin envelope. • The continuum spectrum composed of the direct component, absorbed component,
and outer-disk reflection component• Observed spectral variation is mostly explained by only change of the covering
fraction α
2. Variable Partial Covering Model
![Page 13: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/13.jpg)
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direct component
Heavily absorbed
component
X-ray source
Ionized absorbers
Variable Partial Covering Model(Miyakawa, Ebisawa and Inoue 2012)
The X-ray luminosity of BH hardly variableGeometrical “covering fraction” is significantly variable
![Page 14: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/14.jpg)
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Variable Partial Covering Model(Miyakawa, Ebisawa and Inoue 2012)
The X-ray luminosity of BH hardly variableGeometrical “covering fraction” is significantly variable
Covering fraction varies
![Page 15: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/15.jpg)
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Covering fraction varies
Variable Partial Covering Model(Miyakawa, Ebisawa and Inoue 2012)
The X-ray luminosity of BH hardly variableGeometrical “covering fraction” is significantly variable
![Page 16: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/16.jpg)
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Variable Partial Covering Model(Miyakawa, Ebisawa and Inoue 2012)
The X-ray luminosity of BH hardly variableGeometrical “covering fraction” is significantly variable
Covering fraction varies
![Page 17: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/17.jpg)
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Variable Partial Covering Model(Miyakawa, Ebisawa and Inoue 2012)
The X-ray luminosity of BH hardly variableGeometrical “covering fraction” is significantly variable
Covering fraction varies
![Page 18: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/18.jpg)
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Variable Partial Covering Model(Miyakawa, Ebisawa and Inoue 2012)
The X-ray luminosity of BH hardly variableGeometrical “covering fraction” is significantly variable
Covering fraction varies
![Page 19: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/19.jpg)
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Covering fraction: Null
Variable Partial Covering Model(Miyakawa, Ebisawa and Inoue 2012)
The X-ray luminosity of BH hardly variableGeometrical “covering fraction” is significantly variable
![Page 20: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/20.jpg)
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Contents of the Talk
1. Properties of the Seyfert Galaxies2. Variable Partial Covering Model3. Explanation of the Observed Properties4. Conclusion
![Page 21: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/21.jpg)
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解析
Counting rate
Covering fraction
Flux variation of 21 Seyfert galaxies observed withSuaku, explained by only change of the covering fraction
3. Explanation of the Observed Propertiesa. Significant flux variation
![Page 22: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/22.jpg)
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Observed flux variations explained by “constant black hole luminosity and variable covering fraction”.
![Page 23: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/23.jpg)
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Example of other sourcesBlack:countig rateRed:covering fraction
![Page 24: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/24.jpg)
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Example of other sourcesBlack:countig rateRed:covering fraction
![Page 25: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/25.jpg)
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Example of other sourcesBlack:countig rateRed:covering fraction
![Page 26: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/26.jpg)
direct component
outer-reflection component
Heavily absorbed component
narrow ion line
The ionized iron-edge looks like a broad iron line feature
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3. Explanation of the Observed Propertiesb. “Seemingly” broad iron-line feature
Suzaku MCG-6-30-15Miyakawa, Ebisawa and Inoue (2012)
![Page 27: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/27.jpg)
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3. Explanation of the Observed Propertiesc. Small variation in the iron energy band
• In the Variable Partial Covering model, variations of the direct component and absorbed component cancel each other
• This is most effective at the iron energy band
![Page 28: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/28.jpg)
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3. Explanation of the Observed Propertiesc. Small variation in the iron energy band
• In the Variable Partial Covering model, variations of the direct component and absorbed component cancel each other
• This is most effective at the iron energy band
Iron linereflection
absorbed component
direct compoent
![Page 29: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/29.jpg)
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解析
• Observed Root Mean Square spectrum is explained by only variation of the covering fraction
3. Explanation of the Observed Propertiesc. Small variation in the iron energy band
Black:dataRed:model
![Page 30: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/30.jpg)
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Example of other sourcesBlack:dataRed:model
![Page 31: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/31.jpg)
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Example of other sourcesBlack:dataRed:model
![Page 32: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/32.jpg)
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Example of other sourcesBlack:dataRed:model
![Page 33: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/33.jpg)
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Contents of the Talk
1. Properties of the Seyfert Galaxies2. Variable Partial Covering Model3. Explanation of the Observed Properties4. Conclusion
![Page 34: Origin of the X-ray Spectral Variation and Seemingly Broad Iron Line Structure in the Seyfert Galaxies Ken EBISAWA Naoki ISO, Takehiro MIYAKAWA, Hajime.](https://reader036.fdocuments.us/reader036/viewer/2022062409/5697bfee1a28abf838cb95b6/html5/thumbnails/34.jpg)
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4. Conclusion
• We propose “Variable Partial Covering model” for Seyfert Galaxies, where X-ray luminosity of the black hole is hardly variable, and the observed spectral variation is primarily due to variation of the warm absorbers in the line of sight.
• In the Variable Partial Covering model, covering fraction is the primary parameter to describe the spectral variations.
• The Variable Partial Covering model successfully explains observed spectral variations of 21 Seyfert galaxies (including MCG-6-30-15) observed with Suzaku.