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Restoration of interferometric images. IV. An algorithm for super-resolution of stellar systems

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Academic year: 2021

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Fig. 1. Upper-left panel: the object; upper-right: the reconstruction af- af-ter 1000 OS-EM iaf-terations (first step); lower-left: the mask obtained with a thresholding of the previous reconstruction (50% of the maxi-mum value); lower-right: the restorat
Fig. 2. One-pupil AO-corrected K-band PSFs: ideal case (left), on-axis case (middle), and 15 o ff -axis case (right)
Fig. 4. Example of application of the two-step algorithm. The object is a binary consisting of two stars with angular separation 1 4 λ/B (B = maximum baseline of LBT) and with the same magnitude m = 12;
Table 1. Summary of the results obtained in the case where the mag- mag-nitude di ff erence between the two stars is zero – monolithic case
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