Physics – Optics
Scientific paper
Jul 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990spie.1236..364b&link_type=abstract
IN: Advanced technology optical telescopes IV; Proceedings of the Meeting, Tucson, AZ, Feb. 12-16, 1990. Part 1 (A91-23201 08-89
Physics
Optics
3
Gratings (Spectra), Image Contrast, Radio Interferometers, Speckle Interferometry, Telescopes, Adaptive Optics, Image Resolution, Infrared Imagery, Signal To Noise Ratios, Visible Spectrum
Scientific paper
The factors contributing to fringe contrast decrease for telescopes working near their diffraction limits are summarized. These factors include variations with time, such as atmospheric variations, vibrations, pathlength drift, and fringe tracking noise; and variations accross the pupil; variation with wavelength and factors relating to polarization effects; unequal beam intensities; detector resolution; and pupil transfer geometry. The effects on multispeckle images are also considered. The resulting error budget for the Very Large Telescope Interferometer (VLTI) is derived. It is concluded that the total random error in the fringe contrast is 4.2. The total calibratable systematic error amounts to 34 percent (27 percent due to the instrument, 9 percent due to the atmosphere).
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