Dependence of Image Quality on Sky Position
Two sets of figures have been prepared. The first is a
table of pupil maps
,one cell for each sky position. Within each cell for which we
took measurements are two images: a representation of the wavefront error on
the pupil, and a reconstructed K' image from the wavefront.
The second set of figures is a table of
sky maps
sky maps
, one cell for each Zernicke
coefficient. These show how each coefficient varies as the
telescope pointing is changed.
The
total wavefront error
as a function of sky position shows a maximum in
the northeast of about one micron RMS; the minimum is at the
East 30 position but the overall aberration doesn't change much over most
of the southern half of the sky.