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TeV gamma-ray observation of RCW86 with the CANGAROO-II telescope

TeV gamma-ray observation of RCW86 with the CANGAROO-II telescope. Contents The CANGAROO telescope Motivation Observation Analysis Result Summary. WATANABE Shio (Kyoto university) for the CANGAROO Collaboration. 28 th ICRC Tsukuba, 3 August 2003.

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TeV gamma-ray observation of RCW86 with the CANGAROO-II telescope

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  1. TeV gamma-ray observation of RCW86 with the CANGAROO-II telescope • Contents • The CANGAROO telescope • Motivation • Observation • Analysis • Result • Summary WATANABE Shio (Kyoto university) for the CANGAROO Collaboration 28th ICRC Tsukuba, 3 August 2003

  2. Collaboration of Australia and Nippon for a GAmma Ray Observatory in the Outback Site: Woomera, South Australia • 31°06’ S • 136°47’ E • 160m a.s.l. University of Adelaide Australian National University Ibaraki University Ibaraki Prefectural University of Health Science Institute for Cosmic Ray Research, U. Tokyo Institute of Space and Astronautical Science Kitasato University Konan University Kyoto University National Astronomical Observatory of Japan Osaka City University Shinshu University STE Laboratory, Nagoya University Tokai University Tokyo Institute of Technology Yamagata University Yamanashi Gakuin University Australian Institutes : 2& Japanese Institutes : 15

  3. —— dE 4 2 B2 dtSynch.3 2 =— sT C gmax — —— dE 4 2 dtI.C. 3 =— sT C gmaxUphoton TeV gamma-ray from SNRs • Inverse Compton scattering • 0 decay RX J1713.7-3946 SN1006 NE rim スペクトルの形に 違い Enomoto et al. 2002 =5e13 Synchrotron Naito 1999 • p vs. matter 0 

  4. RCW86 SW shell Observed Low temperature High temperature Non-thermal Bamba et al. 2000 0.5 1 2 5 10[keV] Supernova Remnant RCW86 • Type-II SNR • Diameter 0.8 deg. • Distance 2.5 kpc • Age ~2000 yr Red: 0.7 - 2 keV Blue: 2 - 10 keV SW shell Image byASCA Bamba et al. 2000

  5. Multi wavelength spectrum Synchrotron emissionSN100610 RCW86 SW-shell SN1006 NE-rim Inverse Compton scattering (estimated) SN1006 CANGAROO-II 10m Hara et al.2001 X-ray (ASCA) B < 15µG Radio Detectable for CANGAROO-II Synchrotron

  6. Observation with CANGAROO Strongest emission (E>2.0 keV) • R.A. = 220.19 • Dec.=-62.67 (obs.@zenith~ 32deg.) 2001 (March, April, May)  Suffering from light pollution 2002 (March, April)

  7. Estimation of Threshold Energy Energy threshold [events] Generated all Detected Monte Carlo simulation • Gamma-ray • photon index=2.5 • 150 GeV – 15 TeV • Observation zenith angle 32 – 40 degree (relatively large) High energy threshold Eth 900GeV [TeV]

  8. Imaging method ADC>500(5.4 p.e) & T4a  shower event  calculate Image Parameter

  9. Preliminary Result Signal a<15 deg. Normalize a>30 deg. Energy < 1 TeV (ADC<5000ch) Energy > 1 TeV (ADC>5000ch) Cosmic ray Index=2.7 Excess events -72±12 (0.6 s) Excess events 577±125(4.6 s) No excess below 1 TeV  inverse Compton scattering ?

  10. Summary • Supernova remnantRCW86 (emitting synchrotron X-ray) was observed with the CANGAROO-II telescope. • Preliminarily, we found gamma-ray like events ~4 sigma level (@Energy > 1 TeV). • We need more data to confirm this result. • In this year, we took additional data. • More data (~65 hours) • High quality (Stereo observation; Enomoto OG2.5-6) • High Signal/Noise ratio • Lower energy region

  11. Observation in 2003

  12. X-ray Observation by Chandra High resolution imaging detector RCW86 SW shellby Chandra 0.5-1 keV 1-2 keV2-8 keV Soft and hard regions are completely resolved. Hard filament Non-thermal Thermal Soft Rho et al., 2002 Soft band(<2 keV): Diffusive Hard band(>2 keV): Filament

  13. Nearby Molecular Cloud Red: thermal X-ray (ROSAT) Contour: molecular cloud

  14. Multi wavelength spectrum Cosmic ray Index=2.7 RCW86 SW-shell SN1006 NE-rim SN1006 CANGAROO-II 10m Hara et al.2001 X-ray (ASCA) Radio Inverse Compton scattering (estimated) Synchrotron

  15. Energy dependence of Alpha distribution Signal a<15 Normalize a>30 Energy < 1 TeV 2 TeV - 1 - 2 TeV 117±73 events 1.6 s -72±12 events 0.6 s 424 ±98 events 4.3 s

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