A DIRECT RESTORATION METHOD FOR SPECTRAL AND IMAGE-ANALYSIS

Physical constraints to directly control the output restoration are in troduced in each iteration of solving the spectral or image formation equation. For the purpose of increasing the restoration sensitivity an d the capability of smoothing noises, the fitting technique is used to reform the resolved equation. Our reconstruction results for Monte Ca rlo samples and observation data from space high energy astronomy show that, in comparison with traditional restorations, the direct method has high sensitivity, high resolution ability and capability of effect ively reducing the effect of statistical fluctuation in data and can b e used in the case of poor statistics. This method is model independen t and has the capability to simultaneously represent both the extended and discrete features in object.