Restoration problem
As we seen in Restoration Methods section, restoration problems can be modelled with the following equation:
g = K * f + b + w
g = K * f + b + w
| f is the astronomical object | K is the PSF |
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K * f is the blurred image |
b + w is the background + noise |
g = K * f + b + w |
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Examples of reconstruction of g, based on different methods
Lucy-Richardson/Expectation-maximization (LR-EM) method :