Titlebook: Data Analysis in Astronomy III; V. Gesù,L. Scarsi,M. C. Maccarone Book 1989 Springer Science+Business Media New York 1989 astronomy.astrop

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The Rayleigh Statistic in the Case of Weak Signals — Applications and Pitfalls with respect to an adjacent OFF-source region is still acceptable after a claimed periodic sinusoidal signal have been subtracted from the ON-source region. This is mainly due to the large effects of Rayleigh fluctuations. It is also shown that most of the present estimators of the signal strength

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Moving Regression: A Tool for the Statistical and Astrometrical Analyses of Solar Observationsing into account the physical constraints. After some statistical considerations, the results obtained with different sizes of window are analysed. Graphical comparisons are carried out on the estimators obtained by the usual method and by the new one for the 1978, 1979 and 1980 compaigns. They show

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Maximum Entropy Image Processing in Gamma-Ray Astronomyte experiments to date with real imaging capabilities have been NASA’s SAS-2 and ESA’s COS-B. At lower energies (1-30 MeV) only balloon experiments have so far had imaging capabilities (e.g. the MPE Compton Telescope). Much of the scientific analysis of such data can be done without actually generat

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Search for Bursts of Gamma-Ray Emission from the Crab Pulsar in the Cos-B Data by Adaptive Cluster A for short bursts of gamma-ray emission from the source. As a result, two clusters of 3 and 6 photon arrival times within 264 s and 1813s respectively were found with the corresponding residual phases having close correlation with the peaks of the Crab pulsed emission. The comparison with a similar

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Statistical Restoration of Astronomical Imagesty and h(,) is the point spread function (psf)-However, when we consider discrete samples on a rectangular grid, the intensity measured at each pixel (i,j) is given by.where ε. represents the external contribution, in our case background and random noise. The main problem in the restoration of astro