The correction of the influence of phase corrugation in the pupil plane is a fundamental issue in achieving high dynamic range imaging .
In this paper , we investigate an instrumental setup which consists in applying interferometric techniques on a single telescope , by filtering and dividing the pupil with an array of single-mode fibers .
We developed a new algorithm , which makes use of the fact that we have a redundant interferometric array , to completely disentangle the astronomical object from the atmospheric perturbations ( phase and scintillation ) .
This self-calibrating algorithm can also be applied to any – diluted or not – redundant interferometric setup .
On an 8 meter telescope observing at a wavelength of 630 nm , our simulations show that a single mode pupil remapping system could achieve , at a few resolution elements from the central star , a raw dynamic range up to 10 ^ { 6 } ; depending on the brightness of the source .
The self calibration algorithm proved to be very efficient , allowing image reconstruction of faint sources ( mag = 15 ) even though the signal-to-noise ratio of individual spatial frequencies are of the order of 0.1 .
We finally note that the instrument could be more sensitive by combining this setup with an adaptive optics system .
The dynamic range would however be limited by the noise of the small , high frequency , displacements of the deformable mirror .