A. Glindemann, R. G. Lane, and J. C. Dainty, "Estimation of binary star parameters by model fitting the bispectrum phase," J. Opt. Soc. Am. A 9, 543-548 (1992)
The analysis of binary stars has to date been one of the major successes of speckle interferometry. A new technique for estimating the parameters of a binary star is presented. Unlike earlier methods, the system does not require the measurement of a reference star to compensate for the speckle transfer function. The algorithm relies on model fitting to the bispectrum phase and can obtain the separation, position angle, and relative brightness of the two components.
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Additionally to the full data set with 600 events/frame, the results with the reduced data are presented by taking every second and every fourth photon. It is apparent that for a lower number of photons a higher number of subplanes (Subpl.) is required. Rel. Br., Relative brightness; Sep., separation; Orient., orientation.
The data are the averages over reconstructions with 44, 60, and 80 subplanes of the bispectrum. Rel. Br., Relative brightness; Sep., separation; Orient., orientation.
The data are the averages over reconstructions with 44, 60, and 80 subplanes of the bispectrum. Rel. Br., Relative brightness; Sep., separation; Orient., orientation.
Additionally to the full data set with 600 events/frame, the results with the reduced data are presented by taking every second and every fourth photon. It is apparent that for a lower number of photons a higher number of subplanes (Subpl.) is required. Rel. Br., Relative brightness; Sep., separation; Orient., orientation.
The data are the averages over reconstructions with 44, 60, and 80 subplanes of the bispectrum. Rel. Br., Relative brightness; Sep., separation; Orient., orientation.
The data are the averages over reconstructions with 44, 60, and 80 subplanes of the bispectrum. Rel. Br., Relative brightness; Sep., separation; Orient., orientation.