白鳥座ループのシェルの観測 + Non-thermal SNR G330. 2+1 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 Non-thermal SNR, G330.2+1.0 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 Explosion N W ROSAT HRI

32 observations 9 observations Suzaku ROSAT HRI 32 observations 9 observations XMM-Newton Red:　 0.3-0.5 keV Green: 0.5-1.0 Blue: 1.0-3.0

Summed Spectra of Cygnus Loop Limb North Path South Path C - band C VI N VI O VII O VIII Fe L Ne IX X Mg XI Mg XII Si XIII S XV Suzaku XIS0+1+2+3 NXB

Outline Cygnus Loop Non-thermal SNR, G330.2+1.0 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” 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 Aschenbach & Leahy (1999)　－　南西方向のISM密度の薄さが“破れ”の起源

Observation of the South Blowout with XMM-Newton POS-8 OBS_ID 0405490101 date　　 2006/05/13 exp. time 10ks POS-9 OBS_ID 0405490201 date 2006/05/13 Exp. time 10ks XMM-Newton image × Center of the “extra SNR” (Uyaniker et al. 2002)

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 true color image 　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 true color image POS-8 POS-9 Red: 0.2-0.5 keV Green: 0.5-0.7 keV Blue: 0.7-10 keV

Spatially Resolved Spectral Analysis Two component VNEI model Low kT component (~0.2keV) High kT component (~0.4keV) MOS1 MOS2 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

Emission Measure Distribution of Fe in the Cygnus Loop Ejecta Tsunemi et al. Uchida et al. East path West path 2 Tsunemi et al. (2007) EM (1014cm-5) 1 East path Uchida et al. (2008) West path -50 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

Spatially Resolved Spectral Analysis Two component VNEI model Low kT component (~0.2keV) High kT component (~0.4keV) MOS1 MOS2 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” ~10,000 yrs later... No evidence in X-ray that the nature of the blowout region originated from the extra SNR

Outline Cygnus Loop Non-thermal SNR, G330.2+1.0 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

Single Component VNEI model Suzaku Observations of Limb Regions of the Cygnus Loop Katsuda et al. 2008 Tsunemi et al. 2009 Uchida et al. 2009 Ne Abundance XIS0+XIS1+XIS3 Single Component VNEI model ←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

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 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 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 Lower Ambient Density Interacting with Cloud (Levenson et al. 2005) (Levenson et al. 2002)

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 Non-thermal SNR, G330.2+1.0 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

low kT component - cavity material origin RegionB 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 low kT component - cavity material origin high kT component - ejecta origin

“Blowout” may exist here along the line of sight Previous Study (Kimura et al. 2009) Flux Distribution Thin Shell Region Flux (counts cm-2s-1arcmin-2) 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

949 box regions are obtained Suzaku: 29 observations XMM: 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 Non-thermal SNR, G330.2+1.0 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 Southwestern Limb Easter Limb Color Image: Chandra ACIS(0.5-10.0keV) Contour: MOST(843MHz) 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 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 Non-thermal SNR, G330.2+1.0 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