Optical processor for the very large array /VLA/ radiotelescope - Encoding-dependent errors

Details Optical processor for the very large array /VLA/ radiotelescope - Encoding-dependent errors Optical processor for the very large array /VLA/ radiotelescope - Encoding-dependent errors

Jan 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980spie..231...66f&link_type=abstract

In: 1980 International Optical Computing Conference, Washington, DC, April 8-11, 1980, Proceedings. Book 1. (A81-37755 17-35) Be

Computer Science

Antenna Arrays, Error Analysis, Fourier Transformation, Optical Data Processing, Radio Telescopes, Signal Encoding, Very Large Array (Vla), Light Scattering, Noise Reduction, Optical Correction Procedure, Signal To Noise Ratios, Sky Brightness, Transmittance, Visibility

Scientific paper

An optical Fourier transform processor converts visibility data at its input to a sky brightness function at its output. Scattered light and spurious terms resulting from the method of encoding the complex visibility function as a real-valued and nonnegative transmittance result in errors in the processor output. In this paper, the degree to which each of these undesired terms degrades the signal-to-noise ratio of the output for different encoding methods and classes of images is discussed. Alternative methods of encoding the input that greatly reduce the errors are suggested. Two particularly powerful methods of minimizing noise are 'complementary weighting' and 'bias equalization'. Two data dependent parameters are found to be most important: (1) the ratio of the mean-squared visibility magnitude to the square of its maximum, and (2) the ratio of the squared maximum of the brightness function to its mean squared value.

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