Attending: Tom, Tomo, Toki, Brian, Kris, Shaul, Karl, Qi

Notes by : Qi

• Attitude Control and Reconstruction Requirements (Wrap up)
  • Tentative baseline: control = 1' (3 sigma) over 1 spin period; reconstruction = 1“ (3 sigma)
  • Last week's presentation from Jacques: Attitude control requirements (Jacques)
  • Last week's images from Kris: | | | |
  • Kris' update for this week
• Telescope I+T (Tomo and Bill)
  • Tomo's slides
  • Receiver, Bill Jones
• Instrument I+T (Bill J.)

• Attitude Control and Reconstruction Requirements (Wrap up)
  • The discussion was from last week: based on cross scan sampling, Jacques argued that increasing precession period T_prec is an potential solution, in order to achieve better sky coverage
  • Kris did not agree
  • Kris's updates:
    • figures show the high-resolution (highest frequency beam) hits number of sky coverage, assuming precession angle 30 deg and spin spin angle 65 deg.
    • Two cases were studied, fast (48 hrs) and slow (7 hrs)
    • it's shown that hits are dense on the edge of “donuts”, and coarse in the middle
      • for slow precession, the distinction between edges and inner parts is more obvious
    • color is in log scale, red is much more dense than blue
    • color scales in slow and fast are not same; the maxium in 48 hrs is a factor of ~4 compared to 7 hrs
    • Kris's conclusion: short (fast) precession is better
  • Shaul: 1 arcmin in 3 sigma in single spin rate is based on fast precession
  • Kris: many motions of PICO are much faster than Planck, we need to be careful. Someone studing WMAP pagers is a good thing to do.
  • Shaul: we need to be careful, star tracker; In optical astronomy, they don’t scan fast, so it’s trivial for them.