Pointing accuracy Clause Samples

Pointing accuracy. The overall instrument (including telescope) needs several highly accurate metrology sub-systems. Knowledge of the origin and propagation of phase and positional errors along the optical path is critical to fringe visibility and interferogram reconstruction. Further discussion is given in section 5.4, and it is clear that minimising these errors will be a major operational challenge. The requirements for the pointing and tracking (drift) accuracy depend on the science aims, observing efficiency desired and the ultimate angular resolution to be achieved. To generate a requirement assume that at the shortest wavelength (25µm) the normalised coupling (thus observing efficiency) due to pointing error in one-dimension be greater than 90% over long integrations. ▇▇▇▇▇▇▇▇▇ (▇▇▇▇▇▇▇▇▇ 1998) considers the case of a perfectly pointed telescope, for which the point source coupling, or aperture efficiency, is limited by the illumination edge taper and the secondary blockage (▇▇▇▇▇▇▇▇▇ equation 8.8). A telescope pointing error of θ manifests as a beam waist offset of δ = Fθ at the focal plane, where F is the focal ratio of the telescope optics. Figure 4 shows the fractional loss of signal due a RMS pointing offset (▇▇▇▇▇▇▇▇▇ equation 4.30) assuming a F/10 telescope illuminated with Gaussian beam with 10dB edge taper.
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