Binary-star intensity ratios by the fork algorithm
- 1 October 1988
- journal article
- Published by Optica Publishing Group in Optics Letters
- Vol. 13 (10), 907-909
- https://doi.org/10.1364/ol.13.000907
Abstract
The fork algorithm for accurately estimating the intensity ratio of binary stars from speckle interferometry data is presented. For brighter stars simulation results suggest that the fork algorithm can attain a signal-to-noise ratio roughly 10 times greater than that of other algorithms, such as triple correlation and shift-and-add. The results of the application of the algorithm to Capella (Alpha Aurigae) data are described.Keywords
This publication has 7 references indexed in Scilit:
- ICCD speckle observations of binary stars. II - Measurements during 1982-1985 from the Kitt Peak 4 M telescopeThe Astronomical Journal, 1987
- Images From Astronomical Speckle Data: Weighted Shift-And-Add AnalysisOptical Engineering, 1986
- The true nodal quadrant of CapellaPublications of the Astronomical Society of the Pacific, 1983
- Direct derivation of intensity and phase statistics of speckle produced by a weak scatterer from the random sinusoid modelJournal of the Optical Society of America, 1981
- Towards true imaging by wideband speckle interferometryOptics Communications, 1980
- Estimation of spatial power spectra in speckle interferometryJournal of the Optical Society of America, 1979
- Modified astronomical speckle interferometry “speckle masking”Optics Communications, 1977