2009/03/13 超新星残骸ワークショップ @ 名古屋大学高等総合研究館 1F...
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Transcript of 2009/03/13 超新星残骸ワークショップ @ 名古屋大学高等総合研究館 1F...
白鳥座ループのシェルの観測+ Non-thermal SNR G330.2+1.0の観測
Shell Structure of the Cygnus Loop+ Non-thermal SNR G330.2+1.0
2009/03/13超新星残骸ワークショップ @ 名古屋大学高等総合研究館 1F カンファレンスホール
大阪大学 常深研究室 内田 裕之、常深 博、勝田 哲、木村 公、小杉 寛子
(H. Uchida, H. Tsunemi, S. Katsuda, M. Kimura, H. Kosugi)
Outline
• Cygnus Loop
– Southwest “Blowout” Region
– Abundance Inhomogeneity at the Northern Limb of the Loop
– Shell Structure along the Line of Sight
• Non-thermal SNR, G330.2+1.0
Cygnus Loop
• Location (l,b) = ( 74.0 ,-8.5 )
• Distance 540 pc (Blair et al. 2005)
• Age ~10,000 yr
• SN Type Core-collapse (Levenson et al. 1997; Tsunemi et al. 2007)
• Progenitor Star B0, 15M◎
(Levenson et al. 1998)
• Cavity ExplosionROSAT HRI
N
W
ROSAT HRI
XMM-Newton
Suzaku
Red: 0.3-0.5 keVGreen: 0.5-1.0Blue: 1.0-3.0
32 observations
9 observations
Summed Spectra of Cygnus Loop
LimbNorth PathSouth PathNorth PathSouth Path
C-band
C VI
N VI
O VIIO VIII
Fe-L
Ne IX
Ne X
Mg XI
Mg XII
Si XIII
Si XIII
S XVC-band
C VI
N VI
O VIIO VIII
Fe-L
Ne IX
Ne X
Mg XI
Mg XII
Si XIII
Si XIII
S XV
NXB
Suzaku XIS0+1+2+3
Outline
• Cygnus Loop
– Southwest “Blowout” Region
– Abundance Inhomogeneity at the Northern Limb of the Loop
– Shell Structure along the Line of Sight
• Non-thermal SNR, G330.2+1.0
Cygnus Loop南西領域の観測
South Blowout
South Blowout
Uyaniker et al. (2002) ― 電波の強度分布から南西に別の SNR の存在を示唆
→ ” blowout” の正体
The Effelsberg 100m Radio Telescope
extra SNR ?
Origin of the South “Blowout”
Aschenbach & Leahy (1999) - 南西方向の ISM 密度の薄さが“破れ”の起源
×
Center of the “extra SNR”(Uyaniker et al. 2002)
POS-8OBS_ID 0405490101date 2006/05/13exp. time 10ksPOS-9OBS_ID 0405490201date 2006/05/13Exp. time 10ks
XMM-Newton image
POS-8
POS-9
Observation of the South Blowout with XMM-Newton
Red: 0.2-0.5 keVGreen: 0.5-0.7 keVBlue: 0.7-10 keV
true color image POS-8
POS-9
• 観測領域を東西に2分割• さらに 5,000 photons / regionになるように円環に区切ってスペクトルを調べた
R=36’
R=95’
Spatially Resolved Spectral Analysis
• 各スペクトルは2温度の衝突電離非平衡モデル( VNEI)でよく合う
Two component VNEI model
Low kT component (~0.2keV)
High kT component (~0.4keV)
MOS1MOS2
Tsunemi et al.Uchida et al.
East pathWest path
Tsunemi et al. (2007)U
chid
a et al. (2008)
Emission Measure Distribution of Fe in the Cygnus Loop Ejecta
EM
(10
14cm
-5)
01
2
Distance from the Cygnus Loop Center (arcmin)0 50-50
高温成分の Feの EMは中心から外へ向けて減少しているFeの分布は CygnusLoop中心を通る Tsunemi et al.の結果と滑らかに繋がっている→高温成分は CygnusLoopのイジェクタ起源
West path
East path
R=36’
R=95’
Spatially Resolved Spectral Analysis
• 各スペクトルは2温度の衝突電離非平衡モデル( VNEI )でよく合う• 低温成分( ~0.2keV )は extra SNR からの放射だとすると温度が低すぎる• 低温成分は CygnusLoop のシェルからの放射と考えて矛盾はない• 2温度フィットの結果から、どの領域でも ISM 成分の寄与は小さい
CygnusLoop南西部のシェルは薄い
Two component VNEI model
Low kT component (~0.2keV)
High kT component (~0.4keV)
MOS1MOS2
SN explosion
Cavity Wall
Break of the Cavity Wall South Blowout
~10,000 yrs later...
No evidence in X-ray that the nature of the blowout region originated from the extra SNR
Origin of the Southwest “Blowout”
Outline
• Cygnus Loop
– Southwest “Blowout” Region
– Abundance Inhomogeneity at the Northern Limb of the Loop
– Shell Structure along the Line of Sight
• Non-thermal SNR, G330.2+1.0
originated from the large break of the cavity wall
Katsuda et al. 2008
Tsunemi et al. 2009
Uchida et al. 2009
Ne Abundance
Suzaku Observations of Limb Regions of the Cygnus Loop
C,N,O,Ne 等のアバンダンスを調べたところ、一部のリムの外縁部のみが ISM の組成に近い
←SNR center
XIS0+XIS1+XIS3XIS0+XIS1+XIS3
Single Component VNEI model
外縁部に行くほどアバンダンスが高くなっている領域がある
CygnusLoopcenter
Abundance-enhanced region; typically >0.5solar ~ISM abundance (Katsuda et al. 2008; Tsunemi et al. 2009; Uchida et al. 2009)
Abundance-enhanced Region at the Limb of the Cygnus Loop
The other limb regions show depleted abundances; typically <0.2solar (Leahy 2004; Miyata et al. 2007; Katsuda et al. 2008; etc.)
Lower Ambient Density
Interacting with Cloud(Levenson et al. 2005)
Interacting with Cloud(Levenson et al. 2002)
The Origin of the Abundance-enhanced Region
The Origin of the Abundance-enhanced Region
The blast waves in the abundance-enhanced are now proceeding into theoutside of the cavity wall and begin to interact with the surrounding ISM.
Outline
• Cygnus Loop
– Southwest “Blowout” Region
– Abundance Inhomogeneity at the Northern Limb of the Loop
– Shell Structure along the Line of Sight
• Non-thermal SNR, G330.2+1.0
originated from the large break of the cavity
derived from the breakout or the thinness of the cavity
低温成分の寄与の違い
視線方向のシェルの厚みを反映
low kT component - cavity material originhigh kT component - ejecta origin
RegionA
high kT component
low kT component
high kT component
low kT component
RegionB
Previous Study (Kimura et al. 2009)
Flu
x (c
ount
s cm
-2s-1
arcm
in-2)
Distance from center (arcmin)
Flux Distribution
flux of low-kT componentflux of high-kT componenttotal flux
Thin Shell Region
“Blowout” may exist here along the line of sight
Suzaku: 29 observationsXMM: 9 observations
~10,000 counts / region
949 box regions are obtained
Each spectrum is fitted bysingle component VNEI
ortwo component VNEI
Flux of each component is calculated
2D Flux Distribution Map
V shape structure(Leahy 2004)
0.2-3.0 keV Flux Distributions of Low- and High-kT Component
Low-kT component High-kT component
in unit of counts cm-2s-1arcmin-2
Rim-brightning
Low-kT component High-kT component
0.2-3.0 keV Flux Distributions of Low- and High-kT Component
in unit of counts cm-2s-1arcmin-2
Blowout region has the lowest flux
Low-flux region with radius ~30 arcmin
“Blowout” also exists in the middle west along the line of sight
Outline
• Cygnus Loop
– Southwest “Blowout” Region
– Abundance Inhomogeneity at the Northern Limb of the Loop
– Shell Structure along the Line of Sight
• Non-thermal SNR, G330.2+1.0
originated from the large break of the cavity
derived from the breakout or the thinness of the cavity
showed that the “blowout” also exists in the direction of our line of sight in the middle west of the Loop
Non-thermal SNR G330.2+1.0
Color Image: Chandra ACIS(0.5-10.0keV)Contour: MOST(843MHz)
Non-thermal emission was first detected with ASCA (Torii et al. 2006)Thermal emission are detected at the eastern limb (Park et al. 2008) Anti-correlation between the X-ray and radio intensities
Powerlaw Γ~2.3
Radio Intensity: LowX-ray Intensity: High
Radio Intensity: HighX-ray Intensity: Low
Easter LimbSouthwestern Limb
Powerlaw Γ~2.5
Thermal model ~0.7keV
Summary
• Cygnus Loop
– Southwest “Blowout” Region
– Abundance Inhomogeneity at the Northern Limb of the Loop
– Shell Structure along the Line of Sight
• Non-thermal SNR, G330.2+1.0
originated from the large break of the cavity
derived from the breakout or the thinness of the cavity
showed that the “blowout” also exists in the direction of our line of sight in the middle west of the Loop