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A deconvolution-based algorithm for crowded field photometry with unknown point spread function

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Figure

Fig. 1. Synthetic images used to check the PSF recovery and photo- photo-metric accuracy versus crowding
Fig. 2. Difference between the reconstructed PSF and the exact one, as a function of crowding
Fig. 5. Standard deviation of the PSF residuals (in logarithmic scale) versus logarithm of peak intensity (see text)
Fig. 7. Zoom on a Mira star in the halo of the radio galaxy NGC 5128 (Centaurus A), selected from Rejkuba et al
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