X 1970 1980 1990 2000 2010 2020 AstroE

日本のX線天文衛星 1970 1980 1990 2000 2010 2020 はくちょう てんま ぎんが あすか Astro-E (Failed) すざく Astro-H IXO

「すざく」のデータ例: Cen-A Emission line due to ionized Fe atom. PIN Diodes Intensity of Radiation 100 Absorption due to interstellar gas surrounding the black hole GSO/BGO phoswich counters 10 X-ray CCD Camera 1 Deconvolved spectrum Hard X-ray Detector • By the HXD team for the press release

「すざく」で観測したCyg X-1のlow/hard state 降着円盤成分：Diskbb 逆コンプトン成分：compps 鉄輝線：Gaussian 0. 1 1 10 Energy (ke. V) 1000

Low/Hard状態の降着円盤 Hot plasma: patchy structure Inner disk radius 330 km 250 km 200 km 75 km Reflection fraction: Seed accretion disk does not intrude deeply into the hot corona. Disk line (i=45 deg, emissivity ∝ r -3) -disk is largely retreated from 3 rs in the low/hard state.

宇宙線とは? 宇宙を飛び交う超高E粒子 u. CR ~ 1 e. V/cc c. f. CMB stellar light magnetic field turbulence thermal energy 0. 3 e. V/cc < 0. 3 e. V/cc 0. 01 e. V/cc G = 2. 7 knee=1015. 5 e. V 銀河の基本構成要素! G = 3. 1 宇宙線加速現場・機構は 発見以来 100年近くたった現在も ankle=1018. 5 e. V 謎のまま (Cronin 1999)

Hillas Diagram (1984) maximum E knee

衝撃波の基礎：terminology 実験室系: outer region (u 1 = 0) shock front (us) inner region (u 2) 超新星爆発 衝撃波静止系: shock front (us = 0) upstream region (uu = us) downstream region (ud)

加速器の探し方 電子 electrons: -> synchrotron emission in radio (Ge. V electron) 　synchrotron emission in X-rays (Te. V electron) Inverse compton emission in g-rays (Te. V electron) 陽子 protons: -> g-rays via p 0 decay(Ge. V-Te. V protons) X-rays IC sync. E 2 d. F/DE X線・γ線が 最適 g-rays p 0 電子 陽子 Energy

超新星残骸での宇宙線加速　観測的証拠 synchrotron X-ray Te. V gamma-ray RXJ 1713 -3946 SN 1006 Discovered by ASCA (Koyama+95) Discovered by HESS (Aharonian+04) 超新星残骸衝撃波面は宇宙線加速現場!

Te. V gamma-ray observations HESS: new generation Te. V g-ray telescope @ Namibia Imaging Atmospheric Cherenkov Telescopes using chrenkov lights from photon showers http: //www. mpi-hd. mpg. de/hfm/HESS. html Te. Vガンマ線帯域では世界で初めて 銀河面無バイアス探査を実施

新天体!? new sources! ~50 sources 現在~50天体 HESS team, 2009

They have no counterpart ! On the Galactic plane Some are diffuse Te. V emission ->They should be accelerators Galactic sources However, Are they really “dark”? they have no CP! What are their They areorigin not ? X-ray follow-ups known are essential PSRs, PWNe known SNRs known SF regions “HESS un. ID sources” “dark particle accelerators” (Aharonian et al. 2006)

Te. V un. ID source list (http: //tevcat. uchicago. edu/) Suzaku obs. HESS J 1303 -631 HESS J 1427 -608 HESS J 1614 -518 HESS J 1616 -508 HESS J 1626 -490 HESS J 1632 -478 HESS J 1634 -472 HESS J 1702 -420 HESS J 1708 -410 HESS J 1731 -347 HESS J 1741 -302 HESS J 1745 -303 HESS J 1747 -281 HESS J 1804 -216 HESS J 1813 -178 HESS J 1825 -137 HESS J 1834 -087 HESS J 1837 -069 HESS J 1841 -055 HESS J 1843 -033 HESS J 1857 -026 HESS J 1858+020 Te. V J 2032+4130 O O O HESS HESS J 1640 -465 J 1718 -385 J 1809 -193 J 1833 -105 J 1846 -029 J 1912+101 J 1923+141 J 1848 -018 Suzaku obs. O O ØThe number is still increasing. ØAbout half of Te. V un. IDs are observed with Suzaku. ØNow it is time to start systematic study. ØCategorize with X-ray feature

Group 1. Compact(+surrounding diffuse) sources HESS J 1837 -069 (Anada+08) HESS J 1809 -193 (Anada+08) HESS J 1825 -137 (Uchiyama+09) Spectra are very hard (Gamma ~ 1 – 2) Compact source; 1837 has pulsation (70 ms) They should be pulsars and pulsar wind nebulae We have many samples of PWN candidates

Group 2. Nothing found on the Te. V peak -> dark particle accelerators HESSJ 1616 -508 (Matsumoto+07) Suzaku HESS J 1702 -420 (Fujinaga+ in prep. ) upper-limit ! FTe. V/FX > 55 FTe. V/FX > 32 HESS J 1804 -216 (Bamba+07) Suzaku HESS un. ID compact sources FTe. V/FX > 13 Origin is still unknown real dark particle accelerator ?

Terada, Y. et al. 2008, PASJ, 60, 387