Analysis of the Bayesian Cramér-Rao lower bound in astrometry - Studying the impact of prior information in the location of an object

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Fig. 1

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Relationship between the classical MCR (from Eqs. (B.2) and (24)), and the BCR (from Eq. (27)) lower bounds as a function of pixel size for three different S/N regimes and two FWHM for the case of σ_priori = 0.5 arcsec. As can be seen σ_BCR ≤ σ_MCR in all regimes.

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