1 Status of the CANGAROO-III Project Masaki Mori ICRR, University of Tokyo International Symposium on High Energy Gamma-Ray Astronomy, June 26-30, Heidelberg Poster GA:10

2 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

3 CANGAROO-II 7m telescope In operation since May 1999 Observation 1999/2000 PSR h RXJ h PKS h PKS h PKS h Crab63h Vela10h Data analysis underway - results will be coming soon!

4 CANGAROO-III Array of four 10m telescopes in Woomera, South Australia to be operated by 2004

5 The first 10m telescope -1 (As of May 2000)

6 The first 10m telescope -2 Upgraded from 7m in March m telescope (1999)10m telescope (2000) Focal length8m 80cm CFRP mirrors60 (30m 2 )114 (57m 2 ) Number of PMTs512 (1/2 ” )552 (1/2 ” ) Readout electronicsTDCTDC & ADC Point image size 0.15  (FWHM)0.20  (FWHM)

7 10m reflector

8 Point image size (A. Kawachi, M. Ohishi and J. Kushida)

9 552ch imaging camera 3  FOV R4124UV (Hamamatsu)  pixel Lightguide

10 32 channel VME ADC VME-9U, A24/A32, D16 Features: ・ 12 bit ・ 4ch/pC ・ Min. 50ns gate ・ 150ns internal delay

11 Observations in 2000 March: Vela pulsar / PSR April: SN1006 May: SN1006 June: PSR …analysis using, and development of, unified software package in progress

12 Schedule FY2000: production of the 2 nd telescope FY2001: installation of the 2 nd telescope / start of stereo observation / production of the 3 rd telescope FY2002: installation of the 3 rd telescope / production of the 4 th telescope FY2003: installation of the 4 th telescope / start of observation by the full array

13 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.)

14 Camera design 4.2  FOV 427 pixels 3/4 ” PMT (Hamamatsu R3478UV, TTS 0.36ns) (C. Ito)

15 Electronics VME-based ・ Discriminator /scaler ・ TDC ・ ADC ・ Trigger ・ CPU (Solaris or VxWorks)

16 Telescope separation study 80~120m is not a bad choice ☆ Figure of merit = E -2.5  (effective area)/  (angular resolution) (R. Enomoto)

17 Possible layout of the array 31°06 ’ S 136°47 ’ E 160m a.s.l. (J. Patterson)

18 Sensitivity in stereo mode (Simulation assuming [optimistic]  &  rejection power of 100, and timing rejection power of 2)

19 And in 2004 … (S. Hara) CANGAROO Website