in parallel, with IRDIS observing in the $K12$ filter pair [$\lambda_{K1}$=2.110 $\muup$m and $\lambda_{K2}$=2.251 $\muup$m, $R$$\sim$20, @Vigan2010] and IFS in the $YJH$ bands [0.95–1.65 $\muup$m, $R$$\sim$33, @Claudi2008]. The observing conditions were good and stable (wind speed $\sim$6–10 m/s, see Table \[tab:obs\]). The star was imaged with an apodized pupil Lyot coronagraph [@Soummer2005] of diameter 185 mas [@Boccaletti2008c]. At the beginning and the end of the sequence, [we acquired two dedicated calibrations. First, we recorded]{} for flux calibration purposes unsaturated images of the star out of the coronagraphic mask and inserting a neutral density filter of average transmission $\sim$1/100[^4] in the optical path. [Then, we]{} obtained coronagraphic images with four crosswise faint replicas of the star artificially generated using the deformable mirror [@Langlois2013] to measure the star location [for frame registering (Sect. \[sec:datareduc\]).]{} After the observation, we measured sky backgrounds. However, because of a hardware issue, the second unsaturated PSF image and the sky background images for IRDIS were not recorded properly. As a consequence, we used for the sky subtraction the closest [sky backgrounds (taken the previous night)]{} obtained with the same filter and coronagraph configuration [as]{} our observations and scaled them to the DIT and the background measured at 