Interferometric imaging with arrays of large optical telescopes in the multi-speckle mode

Details Interferometric imaging with arrays of large optical telescopes in the multi-speckle mode Interferometric imaging with arrays of large optical telescopes in the multi-speckle mode

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...279..322r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 279, no. 1, p. 322-334

Astronomy and Astrophysics

Astrophysics

5

Arrays, Astronomical Interferometry, Astronomical Models, Computerized Simulation, Image Processing, Image Reconstruction, Imaging Techniques, Mathematical Models, Speckle Interferometry, Spectrum Analysis, Extremely High Frequencies, Millimeter Waves, Radio Interferometers, Submillimeter Waves

Scientific paper

We present a method for interferometric imaging with arrays of large optical telescopes in the multi-speckle mode. The raw data were produced by simulating light propagation in the atmosphere, various pupil functions similar to the pupil function of the European Southern Observatory (ESO) Very Large Telescope Interferometer (four 8-m telescopes), earth rotation, and photon noise. The generated data sets consist of up to 48,000 interferograms per experiment with 100 to 80,000 photoevents per interferogram. Since a Fried parameter r0 smaller than the telescope diameter was chosen, multi-speckle long-baseline interferograms were obtained which consist of many speckles with interference fringes in each speckle. This experimental condition is called the multi-speckle mode, which is typical for interferometric imaging with large telescopes at optical wavelengths. From the various data sets diffraction-limited images were reconstructed by the speckle masking method (bispectral analysis) and the iterative building block method. Image reconstruction is possible without the use of non-redundant masks since speckle masking is a generalization of phase closure imaging to highly redundant arrays (or large optical telescopes). The reconstructed images show the dependence of the signal-to-noise ratio on photon noise and other parameters. The proposed method can also be applied to radio interferometric data (especially, mm- or or sub-mm-observations).

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