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