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"

4. 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.

5. Next-generation projects
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
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 APh 15, 335

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

7. 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

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

9. ? SuperCANGAROO “Strawman” design parameters
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