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CANGAROO グループ

CANGAROO グループ. 吉越　貴紀 宇宙線研究所共同利用研究成果発表会 ２００４年１２月１７日. University of Adelaide Australian National University Ibaraki University Ibaraki Prefectural University Konan University Kyoto University STE Lab, Nagoya University National Astronomical Observatory of Japan. Kitasato University

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CANGAROO グループ

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  1. CANGAROOグループ 吉越　貴紀 宇宙線研究所共同利用研究成果発表会 ２００４年１２月１７日

  2. University of Adelaide Australian National University Ibaraki University Ibaraki Prefectural University Konan University Kyoto University STE Lab, Nagoya University National Astronomical Observatory of Japan Kitasato University Shinshu University Institute of Space and Astronautical Science Tokai University ICRR, University of Tokyo Yamagata University Yamanashi Gakuin University CANGAROO-III Team

  3. Woomera, 2004 March 2004年3月から4台の10m望遠鏡による100GeV領域ガンマ線のステレオ観測を開始。 平成15年度でCOE経費終了⇒平成16年度以降の観測運転・維持改良経費＆一号機の改修費が必要 T2 T4 T3 T1

  4. CANGAROO-III event samples T2 T4 T1 T3

  5. いただいた研究費 • 今年は大変お世話になりました。 • 来年もよろしくお願いします。

  6. 最近の発表論文 • Detection of Sub-TeV Gamma Rays from the Galactic Center Direction by CANGAROO-II, Tsuchiya, Enomoto, Ksenofontov, Mori, et al., ApJL 606, L115 (2004) • A Search for TeV Gamma-Ray Emission from the PSR B1259-63/SS2883 Binary System with the CANGAROO-II 10 Meter Telescope, Kawachi, Naito, Patterson, Edwards, et al.,ApJ 607, 949 (2004) • Detection of Gamma-Rays around 1 TeV from RX J0852.0-4622 by CANGAROO-II, Katagiri, Enomoto, Ksenofontov, Mori, et al., ApJL, accepted

  7. The Galactic Center • CANGAROO 10m result Gamma-ray signal (ON-OFF) Also detected by the Whipple group [ApJ 607, 949 (2004)] and the H.E.S.S. group [astro-ph/0408145] Tsuchiya et al., ApJ 606, L115 (2004)

  8. Emission from the Galactic Center • Possible mechanisms • Acceleration in SNR (Sgr A East): not favored by H.E.S.S. observation • Sgr A* accretion disk • Dark matter annihilation Dark matter annihilation p-p in the accretion disk + absorption Horns, astro-ph/0408192 Aharonian & Neronov, astro-ph/0408303

  9. Pulsar binary B1259-63/SS2883 Kawachi et al. ApJ 607, 949(2004) U.L. in 2000 H.E.S.S. preliminary (2004)

  10. SNR RX J0852.0-4622 (G266.2-1.2) ASCAhard X-ray 2o ROSAT soft X-ray (0.4<E<2.0keV) 8o Vela SNR Maximum flux Non-thermal Flux (photons/sec/keV) X-ray spectrum very similar to RX J1713 TeV gamma-rays are expected ! 1 5 10 Energy (keV)

  11. SNR RX J0852.0-4622 ApJL, Accepted! • CANGAROO-II (2002-2003, 98 hr) • 6σ detection (12 % Crab @ 1 TeV)

  12. ステレオトリガーシステム • これまでのステレオイベントは、オフラインで時間合せをしたもの（各望遠鏡でトリガー） • ステレオトリガー: any 2 telescopes の coincidence • ミューオンイベントの除去 　　　→低バックグランド 　　　→エネルギー閾値を下げられる • 2004 年 12 月より稼動を開始→性能を調査中

  13. Outline • When each telescope is triggered, “local hit” signal is generated. • Local hit signal is sent to the Global Trigger System via light fibers • GTS receives local hit signals and delays each local signals. • Delay time is updating along with telescope direction. • If any 2 of 3 signals are within the coincidence window, “Global hit” signal is generated and increments event numbers. • GTS sends global hit signal and event number to every telescopes via light fibers • When receiving global hit signal, DAQ system is triggered and records data Variable delay gate generator Coincidence Window Event number Event number to T1-4 Local hit from T2-4 (6) Global hit to T2-4 (2) (3) (5) Global Trigger System

  14. H.E.S.S. completed in Dec.2003 Four 12m telescopes (2 completed) in Namibia, Africa Max Planck Inst., Heidelberg, etc.

  15. Hofmann, Gamma2004 (Heidelberg, July 2004)

  16. Hofmann, Gamma2004 SN 1006 Situation is similar on PSR 1706 & Vela

  17. Hofmann, Gamma2004 Confirmed as a source!

  18. H.E.S.S.の結果を受けて • 最近の結果（CANGAROO-II, 7/10m）について、H.E.S.S.と矛盾するものは再検討を開始 • SN1006: 較正にバグ→影響を調査中 • PSR1706: フラックスが下がる可能性 • CANGAROO-IIIのステレオシステムで再観測し、良質のデータでフラックスを確認 • SN1006（39時間）、PSR1706（36時間）のデータは取得済み→解析中 • 10月にNGC253、11～12月にCrabを観測 • 独立解析＆クロスチェックの体制作りを開始

  19. 4-telescope stereo observations (since 2004 March) Also we have a similar Off time for almost targets. Wobble mode was applied to PKS2155(point source) and Crab(2003). Stereo data analysis is underway… Wobble mode (HEGRA)

  20. The Crab Nebula • CANGAROO-III (Dec. 2003) • Two Telescopes Very Preliminary Integral Flux (cm-2 s-1) 1 10 Energy (TeV) θ2 (deg.2)

  21. Cen A • Kabuki, Ph.D., to be submitted • CANGAROO-III (Mar.-Apr. 2004) • 2σ upperlimits (~ 5% Crab) Very Preliminary Crab level

  22. Ohishi, Ph.D., to be submitted Galactic Diffuse Emission ~ 9 hr ~ 11 hr Very Preliminary

  23. CANGAROOの今後 • 平成15年度に完成した4台の10m望遠鏡によるステレオ観測を継続して行い、性能の理解に努める。 • H.E.S.S.とCANGAROO-I,IIで結果が矛盾する天体の観測、解析を、当面の最優先課題とする。 • 南天で有利な銀河系内天体の観測、特に宇宙線の起源天体として有力な超新星残骸を系統的に観測し、ガンマ線天体の検出数を統計的な議論を行える例数まで引き上げる。 • 望遠鏡は保守･改修･改良が必要であり、観測旅費も確保していかなければならない。→科研費など • より感度の高い次世代大型ガンマ線望遠鏡のための開発研究を行い、世界の大型計画に対抗していく。

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