Who accelerate cosmic rays Koyama et al.(1995) Discovery of sync. X-rays from the shell of SN 1006 Koyama et al. (1997)：Sync. X-rays Aharonian et al. (2004)： 　　　　　　　　　　　　VHE gamma-rays SNR RXJ 1713-3946 is an accelerator! スペクトルからは磁場強度のみ、構造までみたければ … 高空間分解能観測　：Chandra (0.5 arcsec) 偏光観測　：将来の観測機器に期待

1.4. Spectral Fitting Non-thermal! spectrum Hard No line SRCUT model 0.5 1 5 10 (keV) power-law exponential cutoff Sync. emission from electrons nrolloff = 5x1017Hz B 10mG Emax 100TeV 2 Reynolds & Keohane (1999) a = 0.57 @1GHz (fixed) (Allen et al. 2001) nrolloff = 2.6 (1.9 – 3.3) x 1017 Hz Flux = 1.8 x10-12 ergs cm-2s-1

1.5. Many young historical SNRs have thin filaments with sync. X-rays Cas A(SN1680) Kepler(SN1604) Tycho(SN1572) SN1006 RCW 86 (SN184) (Bamba et al. 2005)

Chandra: Thin Filaments (Bamba et al.) In this region, electron returns back (small: quick, large: slow) The Efficiency of Particle　 Acceleration NR: High ER: Low？ A ping-pong ball gets speed (energy) by a rally　in a moving wall Efficiency particle acceleration Thermal plasma shock

The scale length vs. radius 2 5 10 50 Radius of SNR (pc) 10-2 10-1 1 Scale length (pc) downstream upstream R/10 30 Dor C RCW 86 Cas A SN 1006 Tycho R/1000 Kepler The scale length is ~ % of the radius.

perpendicular B or parallel B ? Why are filaments so thin? ….. Small diffusion in direction to shock normal! perpendicular B or parallel B ? Diffusion only occurs along the B perpendicular! ordered or turbulent B ? turbulent → strongly scattered 　 → hardly go downstream → staying long around shocks turbulent B high effic. (equipartition) First quantitative image ! shock Emax of electron 30-40 TeV The angle: > 85 deg. The strength: 10 – 80 mG up down

９０° Magnetic field Up Stream Shock Front Electron Trajectory Down Stream

another scenario very strong parallel B (Berezhko et al. 2004) Strong B makes the gyro radius small → diffusion becomes small B ~ 100 – 400 mG shock up down Turbulent magnetic field (Bohm limit) Very efficient acceleration (equipartition) Anyway, First estimation of magnetic field structure

未知の超新星残骸探査 硬X線探査 今までのSNR探査: 電波中心 (265個: Green et al. 2006) SN1006 1GHzでの表面輝度 (10-22W m-2Hz-1sr-1) SN1006 0.1 1 10 銀河面からの距離 |b| (degree) 電波サーベイは銀河面近くで弱い SN1006型は電波で暗い 硬X線探査

ASCAによる無バイアス銀河面探査 探査領域: 硬X線無バイアス探査としては |l| < 45o, |b| < 0.4o おそらく最大･最高感度探査 複数の未同定宇宙線加速SNR候補を発見 G11.0+0.0 G25.5+0.0 G26.6-0.1 Bamba et al. (2003b) このようなSNR … ~20個?

ASCA Galactic Plane Survey

2. HESS sources New accelerator candidates? :XIS Mapping Sgr A* HESS J1837-069 HESS J1834-087 HESS J1825-137 HESS J1813-178 HESS J1804-216 HESS J1640-465 HESS J1614-518 HESS J1616-508 Aharonian et al. 2005 New accelerator candidates? :XIS Mapping

HESS + New SNRs

(1) RXJ1713.7-3946/ＳＮ1006　: Hard Tail　 Prepared by T.Takahashi, J.Hiraga, K. Nakazawa、 Y.Uchiyama Hard band ACIS-I 3-5 keV True TeV emitter  ASCA GIS Synchrotron X-ray Uchiyama et al. Aharonian et al. SN1006 Γ~ 2.7 : the standard acceleration theory. RXJ 1713.7 G~2.3 : hard to explain

Target list Name ext. flux* counterpart? viewing 1303-632 10 none (HESS J…) (‘) 1303-632 10 none 1614-518 12 9 none - Oct.3 1616-508 11 17 PSR J1617-5055? - Oct.3 1640-465 2 19 G338.3-0.0 1804-216 13 16 G8.7-0.1 - Oct.19 1813-178 3 12 W33? 1825-137 10 9 PSR1826-1334? - Oct.24 1834-087 12 13 G23.3-0.3 1837-069 4 9 AX J1838.0-0655 ● *: 10-12 ergs/cm2/s above 200 GeV

Assumption: RX J1713 and HESS sources have same spectra Who are they? XIS spectra and image detection with HXD? Assumption: RX J1713 and HESS sources have same spectra Name F2-10 keV 1614-518 5x10-12 1616-508 10x10-12 1804-216 9x10-12 1825-137 5x10-12 detectable with XIS 50ks ASCA survey: 2x10-12ergs cm-2s-1 with 50ks or strong upper limit… If they are not RX J1713s. Then dark accelerator !?

Suzaku will catch the nature of TeV unID sources 2.5. Suzaku observation of HESS unID sources HESS J1616-508 HESS J1804-216 pos. of HESS J1804 (cal source) (cal source) 2 – 7 keV 2 – 7 keV strong upper limit ! (Matumoto et al.2006 ) dim counterpart ? (Bamba et al. 2006) Suzaku will catch the nature of TeV unID sources

Their nature is still unknown, but wide band obs. will solve it ! 2.6. One possible scenario for TeV unID sources: Emission from SNRs in various phases young SNRs (Yamazaki et al. astro-ph/0601704) large shock speed both e and p are accelerated strong synchrotron X-rays old SNRs small shock speed electrons are deccelerated no emission TeV unIDs are old SNRs colliding with MCs? Their nature is still unknown, but wide band obs. will solve it ! SNRs colliding with MCs amount of targets strong p0 decay

FTeV/FX ratio target FTeV/FX Crab (PWN) ~2.7e-3 RX J1713 (SNR) ~0.06 HESS J1804-216 ~8 HESS J1616-508 >55? HESS unID sourcesは 本当にproton acceleratorかもしれない!