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Poster GA:10. International Symposium on High Energy Gamma-Ray Astronomy, June 26-30, Heidelberg. Status of the CANGAROO-III Project. Masaki Mori ICRR, University of Tokyo. CANGAROO collaboration. C ollaboration of A ustralia and N ippon for a Ga mma R ay O bservatory in the O utback.

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Status of the CANGAROO-III Project

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status of the cangaroo iii project

Poster GA:10

International Symposium on High Energy Gamma-Ray Astronomy, June 26-30, Heidelberg

Status of the CANGAROO-III Project

Masaki Mori

ICRR, University of Tokyo

cangaroo collaboration
CANGAROO collaboration
  • Collaboration of Australia and Nippon for a Gamma Ray Observatory in the Outback
  • Institute for Cosmic Ray Research, U. Tokyo
  • University of Adelaide
  • Australian National University
  • Ibaraki University
  • Ibaraki Prefectural University of Health Science
  • Institute of Space and Astronautical Science
  • Institute of Physical and Chemical Research (RIKEN)
  • Kanagawa University
  • Konan University
  • Kyoto University
  • National Astronomical Observatory of Japan
  • Osaka City University
  • STE Laboratory, Nagoya University
  • Tokai University
  • Tokyo Institute of Technology
  • Yamagata University
  • Yamanashi Gakuin University
cangaroo ii 7m telescope
CANGAROO-II 7m telescope
  • In operation since May 1999
  • Observation 1999/2000PSR1706-44 29hRXJ1713.7-3946 23hPKS2005-489 23hPKS2155-304 58hPKS0548-322 19hCrab 63hVela 10h
  • Data analysis underway - results will be coming soon!
cangaroo iii
  • Array of four 10m telescopes in Woomera, South Australia to be operated by 2004
the first 10m telescope 2
The first 10m telescope -2
  • Upgraded from 7m in March 2000
point image size
Point image size

(A. Kawachi, M. Ohishi and J. Kushida)

552ch imaging camera
552ch imaging camera
  • 3FOV
  • R4124UV(Hamamatsu)
  • 0.115 pixel
  • Lightguide
32 channel vme adc
32 channel VME ADC
  • VME-9U, A24/A32, D16
  • Features:・12 bit ・4ch/pC ・Min. 50ns gate・150ns internal delay
observations in 2000
Observations in 2000
  • March: Vela pulsar / PSR1259-63
  • April: SN1006
  • May: SN1006
  • June: PSR1706-44
  • …analysis using, and development of, unified software package in progress
  • FY2000: production of the 2nd telescope
  • FY2001: installation of the 2nd telescope /start of stereo observation /production of the 3rd telescope
  • FY2002: installation of the 3rd telescope /production of the 4th telescope
  • FY2003: installation of the 4th telescope /start of observation by the full array
work in progress
Work in progress
  • Refinement of mirror optical quality
  • Wider FOV camera with individually HV-controlled PMTs
  • Front-end electronics in VME-9U
  • Faster data readout
  • Pattern trigger circuit using PLD
  • Flexible, centralized telescope control
  • Total monitor system (calibration light source, environment etc.)
camera design
Camera design
  • 4.2 FOV
  • 427 pixels
  • 3/4” PMT(Hamamatsu R3478UV, TTS 0.36ns)

(C. Ito)

  • VME-based・Discriminator /scaler・TDC・ADC・Trigger・CPU(Solaris or VxWorks)
telescope separation study
Telescope separation study
  • 80~120m is not a bad choice

(R. Enomoto)

☆ Figure of merit = E-2.5(effective area)/(angular resolution)

possible layout of the array
Possible layout of the array

31°06’ S

136°47’ E

160m a.s.l.

(J. Patterson)

sensitivity in stereo mode
Sensitivity in stereo mode

(Simulation assuming [optimistic] g & m rejection power of 100, and timing rejection power of 2)

and in 2004
And in 2004…

(S. Hara)