白鳥座ループのシェルの観測 +non-thermal SNR G330.2

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)
N
W
ROSAT HRI
• Cavity Explosion
Suzaku
32 observations
XMM-Newton
9 observations
ROSAT HRI
Red: 0.3-0.5 keV
Green: 0.5-1.0
Blue: 1.0-3.0
Summed Spectra of Cygnus Loop
O VII
O VIII Ne IX
Suzaku XIS0+1+2+3
Ne X
N VI
C VI
Mg XI
Si XIII
Mg XII
Si XIII
S XV
C-band
Fe-L
Limb
North Path
South Path
NXB
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
Origin of the South “Blowout”
extra SNR ?
South Blowout
The Effelsberg 100m Radio Telescope
Aschenbach & Leahy (1999) －南西方向のISM密度の薄さが“破れ”の起源
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
Observation of the South Blowout with XMM-Newton
XMM-Newton image
POS-8
POS-9
POS-8
×
Center of the “extra SNR”
(Uyaniker et al. 2002)
OBS_ID
date
exp. time
0405490101
2006/05/13
10ks
POS-9
OBS_ID
date
Exp. time
0405490201
2006/05/13
10ks
true color image
POS-8
POS-9
Red:
Green:
Blue:
0.2-0.5 keV
0.5-0.7 keV
0.7-10 keV
• 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’
Spatially Resolved Spectral Analysis
Two component VNEI model
High kT component (~0.4keV)
MOS1
MOS2
Low kT component (~0.2keV)
R=95’
• 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
Tsunemi et al.
Uchida et al.
East path
West path
0
EM (1014cm-5)
1
2
Emission Measure Distribution of Fe in the Cygnus Loop Ejecta
-50
0
50
Distance from the Cygnus Loop Center (arcmin)
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
R=36’
Spatially Resolved Spectral Analysis
Two component VNEI model
High kT component (~0.4keV)
MOS1
MOS2
Low kT component (~0.2keV)
R=95’
•
•
•
•
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
Origin of the Southwest “Blowout”
Cavity Wall
SN explosion
~10,000 yrs later...
Break of the Cavity Wall
South Blowout
No evidence in X-ray that the nature of the blowout region originated from
the extra SNR
Outline
•
Cygnus Loop
–
Southwest “Blowout” Region
originated from the large break of the cavity wall
•
–
Abundance Inhomogeneity at the Northern Limb of the Loop
–
Shell Structure along the Line of Sight
Non-thermal SNR, G330.2+1.0
Suzaku Observations of Limb Regions of the Cygnus Loop
Single Component VNEI model
Katsuda et al. 2008
Ne Abundance
Uchida et al. 2009
XIS0+XIS1+XIS3
←SNR center
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
Tsunemi et al. 2009
CygnusLoop
center
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
Abundance-enhanced Region at the Limb of the Cygnus Loop
Abundance-enhanced region;
typically >0.5solar ~ISM abundance
(Katsuda et al. 2008; Tsunemi et al. 2009; Uchida et al. 2009)
The other limb regions show depleted abundances;
typically <0.2solar
(Leahy 2004; Miyata et al. 2007; Katsuda et al. 2008; etc.)
The Origin of the Abundance-enhanced Region
Interacting with Cloud
(Levenson et al. 2002)
Interacting with Cloud
(Levenson et al. 2005)
Lower Ambient Density
The Origin of the Abundance-enhanced Region
The blast waves in the abundance-enhanced are now proceeding into the
outside of the cavity wall and begin to interact with the surrounding ISM.
Outline
•
Cygnus Loop
–
Southwest “Blowout” Region
originated from the large break of the cavity
–
Abundance Inhomogeneity at the Northern Limb of the Loop
derived from the breakout or the thinness of the cavity
–
•
Shell Structure along the Line of Sight
Non-thermal SNR, G330.2+1.0
RegionB
low kT component
RegionA
低温成分の寄与の違い
視線方向のシェルの厚みを反映
high kT component
low kT component - cavity material origin
high kT component - ejecta origin
Previous Study (Kimura et al. 2009)
Flux (counts cm-2s-1arcmin-2)
Flux Distribution
Thin Shell Region
Distance from center (arcmin)
flux of low-kT component
flux of high-kT component
total flux
“Blowout” may exist here along the line of sight
Suzaku:
XMM:
29 observations
9 observations
~10,000 counts / region
949 box regions are obtained
Each spectrum is fitted by
single component VNEI
or
two component VNEI
Flux of each
component is
calculated
2D Flux
Distribution Map
0.2-3.0 keV Flux Distributions of Low- and High-kT Component
Rim-brightning
V shape structure
(Leahy 2004)
in unit of counts cm-2s-1arcmin-2
Low-kT component
High-kT component
0.2-3.0 keV Flux Distributions of Low- and High-kT Component
Low-flux region with radius ~30 arcmin
“Blowout” also exists in the middle west along the line of sight
Blowout region has the lowest flux
in unit of counts cm-2s-1arcmin-2
Low-kT component
High-kT component
Outline
•
Cygnus Loop
–
Southwest “Blowout” Region
originated from the large break of the cavity
–
Abundance Inhomogeneity at the Northern Limb of the Loop
derived from the breakout or the thinness of the cavity
–
Shell Structure along the Line of Sight
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
Non-thermal SNR G330.2+1.0
Southwestern Limb
Easter Limb
Thermal model
~0.7keV
Powerlaw Γ~2.3
Powerlaw Γ~2.5
Radio Intensity: High
X-ray Intensity: Low
Radio Intensity: Low
X-ray Intensity: High
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
Summary
•
Cygnus Loop
–
Southwest “Blowout” Region
originated from the large break of the cavity
–
Abundance Inhomogeneity at the Northern Limb of the Loop
derived from the breakout or the thinness of the cavity
–
Shell Structure along the Line of Sight
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

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