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Fig. 4 shows one of the objects used in the simulation, a
coloured cluster of 27 stars. The object's intensity distribution was
convolved with the interference function of the interferometer and then
multiplied with the diffraction function, both functions being converted to
intensities. The optical path differences were found, using 3 wavelengths,
with initial wavefront errors of the order of . The Strehl
ratio, i.e. the peak intensity in the image of a point source, relative
to the case of perfect phasing, gives an idea of the phasing
performance. It reaches 30% with 2200 photons detected during
the phasing cycle and 80% with photons.
The successive frames of Fig. 6 from left to right depict changes
in the full combined image during the phasing steps for the same object.
The field and object size restriction with densified-pupil imaging often
implies that the object is unresolved or little resolved by the smallest
baselines.
Although the simplified routines which we used in the simulations did
not include all the features which appeared necessary, the resulting
imaging quality approached the theoretical limits on the source shapes
used, typical of resolved stellar and galactic objects. Even better results
should therefore be expected with future refined versions of the
algorithm.
Figure 6:
Simulated phasing sequence on galaxy M51, in presence of
photon noise. The galaxy is shown in the top-left frame, followed by the
interference function of the interferometer and the convolution of the
object with the interference function. The object is unresolved by the
smallest baselines, its components have different colours and phasing is
achieved with 250,000 photons. Successive frames depict changes in the
full combined image during the phasing steps. The last frame, at bottom
right, is the final step of the phasing process, where a Strehl ratio of
0.80 was achieved.
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Next: Limiting magnitude
Up: A hierarchical phasing algorithm
Previous: Phasing and path difference
Ettore Pedretti
4/20/1999