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Fig. 2.


Upper images: collapsed data cubes of all observed frames for the detected binary candidates; 2M1510 (left), 2M1547 (middle), and 2M2022 (right). Lower images: corresponding relevant point source reference used in the fitting procedure of the astrometric measurements. Special care is taken for 2M1510 where we find no suitable standard reference star to match the PSF of the BD binary components, and thus an unresolved 2D Gaussian function is fitted to the entire system which is further explained in Sect. 3.4.1. For 2M1547 we note a third point source in the upper left part of the image which we do not include in our analysis since it was weak and appeared artefact-like in our original data reduction that did not correct for atmospheric dispersion. Derived astrometric parameters and photometry for each individual object are seen in Table 2. The scaling in each individual image is chosen to better highlight the individual components. North is up and east is to the left in the figures.

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