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Future plans and world trend

Future plans and world trend . Masaki Mori Future plan meeting November 8, 2004. “Towards a Major Cherenkov Detectors” workshops. Paris (1992) Calgary (1993) Tokyo (1994) Padova (1995) Kruger Park (1997) Snowbird (1999). "Towards a Network of Atmospheric Cherenkov Detectors".

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Future plans and world trend

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  1. Future plans and world trend Masaki Mori Future plan meeting November 8, 2004

  2. “Towards a Major Cherenkov Detectors” workshops • Paris (1992) • Calgary (1993) • Tokyo (1994) • Padova (1995) • Kruger Park (1997) • Snowbird (1999) "Towards a Network of Atmospheric Cherenkov Detectors"

  3. The conference will cover the following topics: • Status of VHE astrophysics in 2005: new instruments and observations. • From shower images to astrophysical imaging. • Multi-wavelength observations and phenomenology of high-energy gamma-ray sources. • New projects in ground-based high-energy astrophysics. • Instrumentation and calibration for Cherenkov telescopes; inter-calibration with space instruments. • Data archiving and formatting and link with mainstream astrophysics.

  4. 5@5 Max Planck Inst. for Nuclear Physics 50m2 mirror area 5 telescopes (4 in 100m grid and 1 at center) at 5000m a.s.l. 3.2 camera, 721 pixels 5 GeV threshold Next-generation projects • ECO-1000 • Max Planck Inst. for Physics • 35m, 1000m2 mirror area • <5 camera, >2000 pixels • 5 GeV threshold Merck et al. ICRC2003 Aharonian et al. 2001 APh 15, 335

  5. ECO-1000 • European Cherenkov Observatory • Mirror surface 1000m2 • Initiative: MAGIC people • Eth < 8 GeV in 2009/2010 Astro-ph/0403180

  6. H.E.S.S. Phase 2 • 28m telescope at the center of H.E.S.S. telescopes • Future: 10m-class stereo system in Atacama? A. Konopelko, Heidelberg colloquium, July 2004

  7. Small Telescope ARrays (STAR) • Many (>144) small telescopes • Mirror 2.5m, camera 15cm (MCP?) • U. Purdue / U. Washington (Buckley et al.) Gamma2004

  8. SuperCANGAROO ? As of June 2003 • “Strawman” design parameters • <10 GeV energy threthold 10 times more area x 2 times QE • 30m, f=30m (F/1.0), parabola • Field-of-view ~10  survey mode • Short barrel preferred to keep long focal length  new optical design necessary • 0.1 -class pixel camera with advanced photon sensors • Stereo observation is essential

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