science frame and annulus, we computed a reference frame of the stellar residuals using the best linear combination of the 80 most correlated frames for which the [self-subtraction of mock point sources, [modeled]{} using the observed PSF]{}, was at maximum 20%. These parameters were selected from internal tests for the analysis of the consortium data. Negative synthetic companions [@Marois2010b; @Bonnefoy2011] [modeled]{} from the observed unsaturated PSF were inserted in the pre-processed data at the location of the detected point sources. We then processed the data assuming the TLOCI coefficients computed for the analysis without the synthetic companions. The [subpixel]{} position and the flux of the modeled images were optimized to minimize the image residuals within a disk of radius 1.5 full width at half maximum (FWHM) centered on the measured companions [@Galicher2011a]. The error bars include the variations in the stellar flux during the sequence (estimated from the fluctuations of the stellar residuals, 0.009 mag for the $K1$ band) and the accuracy of the fitting procedure. The error term related to the variations in the PSF could not be estimated because no IRDIS PSF was recorded after the sequence (Sect. \[sec:obs\]). The astrometry of the three detected companions (Table \[tab:photometryastrometry\]) 