特別推進研究研究会・宇宙線研究所共同利用研究会「高エネルギーガンマ線でみる極限宇宙2013」2013年9月4日(火) 東京大学 柏キャンパス

NANTEN2 と Suzaku 衛星による若いTeVガンマ線SNRの研究	
佐野 栄俊 （Hidetoshi SANO; 名大理 D3）

共同研究者： 福田達哉，吉池智史，鳥居和史，早川貴敬，山本宏昭，立原研悟，犬塚修一郎，福井康雄 (名大理)，田中孝明 (京大理)，松本浩典 (名大KMI)，内山泰伸 (立教大理)，井上剛志, 山崎了 (青山学院大理)，河村晶子，水野範和 (NAOJ)，水野亮(名大STE)，西村淳，大西利和 (大阪府立大理)， 他NANTENチーム	

SNR as Cosmic-ray Accelerator 	
n

2	/21	

SNRにおける	 Cosmic-Rays (CRs) の加速は, ほぼ揺るぎないものに (e.g., Fermi results)→しかし, 本当に Knee energy 付近まで CRs は加速されているのか？

By S. Funk (MPI)	
n

若く(~2000yr) TeVガンマ線で明るいSNRが, 現段階ではこの鍵を握る最有力ターゲット

3	/21	Four TeV Gamma-ray SNRs	n

年齢2000年程度の4つのTeVガンマ線SNRs→ どの天体もISM (Interstellar Medium) との相互作用が確認
RX J1713.7–3946	

Aharonian+07	

RX J0852.0–4622	

Arribas+11	

視直径: ~1 deg.	
~2 deg.	
年齢: ~1600 yr	
~1700−4300 yr	
ISM: rich CO + cold HI	 rich HI + little CO	
X-rays: pure synchrotron 	 pure synchrotron ?	
n

HESS J1731–347	

Abramowski+11	

RCW 86	

Aharonian+09	

~0.5 deg.	
~0.5 deg.	
~3600−7200 yr	
~1800 yr	rich CO + HI cavity	rich HI + little CO	pure synchrotron 	 thermal + non-thermal	

これらの高エネルギー放射起源や効率の良い CRs 加速と, ISMが密接に関係

Four TeV Gamma-ray SNRs	n

4	/21	

RXJ1713, Vela Jr. HESSJ1731 のTeV γ線とISMの相関

Wp nF∝ 2d

Wp ...... Total energy in accelerated protons
n ........ Target ISM proton density
d ........ Distance to the SNR↑ e.g., RXJ1713 (Fukui, Sano et al. 2012) 高度に非一様なISM分布
CRs proton の加速効率は ~0.1 % (~1048 erg)n

しかしながら, この空間分解能で議論できるのは視直径の大きなSNRに限られる.
→ CTA時代まで待つか, いま我々が他にできることは?

5	/21	

Shock-cloud interaction	n

SNR shock waves と ISM の相互作用 (Shock-cloud interaction)⇒ ISM clump 周辺で乱流励起 + 磁場増幅
⇒ 観測的には clump 周辺のX線増光として確認できる
ISM密度	

磁場強度	Inoue+12	

高空間分解能 / 高統計のX線データ	 ＋	 SNR と相互作用する	 ISM	 	 	 	 	 	 	 	 	 	 	  CR electron acceleration についての知見を深める

RXJ1713: Morphology (pc scale correlation)	
n

6	/21	

TeV ガンマ線 SNRの中でも最も重要なターゲットの１つ⇒ Rich CO + Cold HIとの相互作用, Pure Synchrotron X-rays, 視直径 ~1 deg.
NANTEN2 CO ……… HPBW ~1.5−3 arcmin
Suzaku X-rays ………. HPD ~2 arcmin
ATCA & Parkes HI ….. HPBW ~2.2 arcmin

Sano+13a arXiv: 1304.7722

images: Suzaku 1–5 keV mosaics, contours: 12CO(J=2–1) integrated intensity (two velocity ranges)	

RXJ1713: Morphology (sub pc scale anti-correlation)	
n

17 clumps 全てで, CO と X-ray の anti-correlation がみえている7	/21	

RXJ1713: Schematic image	

8	/21	

9	/21	

X-ray Spectroscopy: Regions and Models	↑ Image: Suzaku XIS (1—5 keV) mosaic
Solid boxes: source regions
Dashed boxes: background regions
Typical X-ray spectra ↗
and best fit parameters →nnRegion	

NH (X-ray)	

North	

0.6 −0.2	 ×1022 cm-2	+0.1+0.06−0.05	×1022 cm-2	Center	0.50

South	

0.89±0.09 ×1022 cm-2	

Γ	2.1±0.1	
2.7±0.1	
2.7±0.1	

Source grid size 2’−8’,	  計315領域からスペクトルを抽出 (FI CCDs only).	 	 	 → Absorbing column density NH (X-ray) の relativistic error < 30 % となるように調整.
Absorbed power-low model で fitting (at least ~100 counts / bin).
Sano+13b in prep.

X-ray Spectroscopy: Spatial and spectral characterization	 10	/21	Sano+13b in prep.
○ Maps of the Best-fit parameters(a) absorbing column NH(X-ray)(b) photon index Γ(c) absorption-corrected X-ray flux (3−10 keV)(contours indicate the smoothed XIS 1−5 keV image)○ Relative error (90% confidence level)
NH(X-ray)… ~14 % (max 30%)
Γ …………. ~6 % (max 13%)
Flux………. ~7 % (max 23%)

Absorbing column & Visual extinction 	11	/21	

Sano+13b in prep.
↖↑Maps of NH(X-ray) and visual extinction(Dobashi+05)← Correlation plot
- correlation coefficient: ~0.83- NH(X-rays) (cm−2) = 3.0×1021・Av (mag.)cf. NH (cm−2) = 2.5×1021・Av (mag.) (Jenkins & Savage+74)nn

NH(X-rays) ~0.4−1.4×1022 cm-2 の範囲で変化→ Cassam-Chenai+04の傾向とconsistentNH(X-rays) と Visual Extinction の非常に良い相関Absorbing column − Foreground component	

12	/21	

○ Foreground component NH, local(H2+HI) is identified
by Moriguchi+05 with NANTEN and ROSAT data.
○ ISM proton column density estimation□ NH (H2+HI) = 2×N(H2) + NH(HI).
□ N(H2) (cm−2) = XCO (cm−2 (K km s−1)−1)
×W(CO) (K km s−1).
□ XCO = 2 × 1020 (cm−2 (K km s−1)−1) (Bertsch+93).
nForeground (local) ISM による吸収量を推定,NH(X-ray) から差し引く (=SNRとの相互作用分).
→ X-ray shell に沿った構造が明らかになった.
Sano+13b in prep.

X-ray Flux & ISM proton column density	

13	/21	

← Image: absorption-corrected X-ray flux (3−10 keV)
Contours: ISM proton column density NH(H2+HI)↓ Correlation plot between the Flux and NH(H2+HI)(a) whole, (b) East and (c) West region.
Correlation coefficient: ~0.54 (whole region)

nn
n

ISMは西側で clumpy, 東側では diffuse に分布.
ISM の多い領域で X-ray enhance (特に西側)
弱いながらも NH(H2+HI) と flux は相関

Sano+13b in prep.

14	/21	

Photon index & ISM proton column density	

← Image: Photon index ΓContours: ISM proton column density NH(H2+HI)↓ Correlation plot between the Γ and NH(H2+HI)(a) whole, (b) East and (c) West region.

nn

SNR 全体に渡って, photon index Γ の小さな領域がいくつか存在している.
ISM rich な西側は NH(H2+HI) と Γ が反相関,東側では, 両者の顕著な相関は見られない

Sano+13b in prep.

Discussion: Efficient cosmic-ray acceleration	nWe interpret the photon index variation as difference of cut-off energy ε0.
→ The cutoff-energy become large (small) when the value of photon index is small (large).
The cutoff-energy ε0 is expressed as (Zirakashvili & Aharonian 07),ε 0 = 0.55 × (vs / 3000 km s-1 )2 η −1 keV.
where vs is shock velocity, η is the degree of magnetic field fluctuations (gyro-factor).
Here, the shock velocity in the dense clump became vs,clump = vs,ambient (nambient/nclump)0.5,
where the ambient gas density nambient = 1 cm−3 and clump density nclump = 102−103 cm−3.

n

In the west region: clumpy and rich ISM(shock waves will be stalled + strong turbulence)⇒ small shock speed and small η (η~1; Uchiyama+07)
In the east region: diffuse and poor ISM(shock waves will be little decelerated)⇒ large shock speed and large ηTherefore, photon index Γ can be small in both regions.
However, the flux excess cannot describe only this scenario.

15	/21	

Discussion: Efficient cosmic-ray acceleration	
n

We interpret the photon index variation as difference of cut-off energy ε0.
→ The cutoff-energy become large (small) when the value of photon index is small (large).
The cutoff-energy ε0 is expressed as (Zirakashvili & Aharonian 07),ε 0 = 0.55 × (vs / 3000 km s-1 )2 η −1 keV.
where vs is shock velocity, η is the degree of magnetic field fluctuations (gyro-factor).
Here, the shock velocity in the dense clump became vs,clump = vs,ambient (nambient/nclump)0.5,
where the ambient gas density nambient = 1 cm−3 and clump density nclump = 102−103 cm−3.

n

In the west region: clumpy and rich ISM(shock waves will be stalled + strong turbulence)⇒ small shock speed and small η (η~1; Uchiyama+07)
In the east region: diffuse and poor ISM(shock waves will be little decelerated)⇒ large shock speed and large η
Therefore, photon index Γ can be small in both regions.
However, the flux excess cannot describe only this scenario.
→ Perhaps the additional particle acceleration mechanism
is working in the ISM rich and clumpy region (e.g., Hoshino+12)16	/21	

Summary 	

17	/21	n

X-ray spectroscopy for the young TeV γ-ray SNR RXJ1713− We reveal the NH(X-ray), Γ and flux maps (+comparing with the ISM)n

Efficient cosmic-ray acceleration− We can describe the photon index variation as difference of the cut-off energy.
− The additional particle acceleration mechanism is working in the ISM rich and clumpy region.
− The interacting ISM with SNR is crucial play a role to understanding the efficient CR acceleration.
(NANTEN/NANTEN2 CO and Suzaku X-ray datasets make a very strong combination!)n

CTA will provide more detail information (high angular resolution images, photon index distribution,etc…) and reveal the relationship between the efficient CR acceleration and the ISM distribution.

Image courtesy G. Perez, SMM, IAC.	

Future work (1)	18	/21	

RXJ1713 の X-ray filamentary structure と ISM n− MHD 計算の磁場増幅 scale は, ~0.05 pc (Inoue+12).
− RXJ1713 で確認されているX線の	 short time variability (~0.05 pc: Uchiyama+07)

Uchiyama+07	




○ COについては, すでに ~0.15 pc の分解能でデータ取得⇒ ALMAで ~0.05 pc へ迫る	CO image with Mopra	

(Sano in prep.)	

19	/21	

Future work (2)	他のガンマ線 SNR と ISM の相互作用 n− RXJ1713 の結果の普遍性を探る (HESS J1731, RCW86 etc..)− Thermal X-rays や	 Hard X-rays と ISM の関係は？ (ASTRO-H SXS, HXI に期待)

Preliminary 	

Contours: CO 1-0 (Fukuda+13 submitted to ApJ) 	

RCW86 X-ray image+NANTEN2 CO contours	20	/21	

Future work (3)	Interacting ISM としての HI の重要性n− RXJ1713 SE-rim の cold HI や, Vela Jr. の HI シェルも重要な ISM 構成要素→ SNR と相互作用する ISM の大半を占めたり, 100 個/cc を超えるものも存在

X-ray : Blue	HI : Green	

CO: Red	RXJ1713 East (Sano+13b in prep.)

Vela Jr. (Sano+13c in prep.)

多くのSNRについて付随する HI を特定, 物理量を明らかにしていくことが肝要21	/21