Conclusions

Jotted down by Bob Fosbury - not complete!

• Passive cooling heritage: Tim Hawarden and the ESA EDISON proposal
• Going to space shifts the sky background ~ 5µm longward (Stockman)
• The influence of the bright (16m) guiding stars on camera performance - probably OK
• Note the ALMA-NGST synergy: similar sensitivity to enshrouded objects at high z
• Importance of segment structure for success of coronography
• High-z galaxies are the driver for optical imaging
• The DRM is weighted towards imaging
• Stockman's concerns:
  • Can we really operate 8K x 8K?
  • Moderate/high resolution spectroscopy may be best done from the ground
  • Need to look at emission line equivalent widths for high-z galaxies as justification for high-R spectroscopy
• Tuning the wavelength response of the HgCdTe arrays for optimum noise performance
• Heat dissipation of Op-Amps close to detector?
• Use as much multiplexing as possible
• Have made measurements of the PRF: charge leaks to neighbouring pixel
• Measured background (continuum?) between the OH lines at 1440 photons/s/m²/arcsec²/µm (Paranal)
• ESO's TIMI-2 detector dissipates around 200mW - but due to required frequent readouts
• AO at 20µm (Q) is relatively easy because r₀ is so big
• OWL spectroscopy competes with NGST to around 5µm