imaging [ADI, @Marois2006a], subtraction of [a radial profile from the data]{}, Locally Optimized Combination of Images [LOCI, @Lafreniere2007a], Template-LOCI [TLOCI, @Marois2014], and principal component analysis [PCA, see @Soummer2012; @Amara2012]. [We also considered reference differential imaging (RDI) in order to obtain unbiased views of the disk morphology. [To build]{} the RDI reference, we [scaled in intensity the images of another star]{} without any disk features obtained in the same observing mode during the previous night. The quasi-static speckle pattern did not vary significantly between the two sequences, allowing for efficient rejection of the stellar residuals.]{} We show in Figs. \[fig:ifsim\] and \[fig:irdisim\] the median-collapsed IFS and IRDIS images obtained with this method and with classical ADI and in Fig. \[fig:irdisimfov\] the full field of view of the IRDIS classical-ADI image. [Regions inside the magenta circles in Figs. \[fig:ifsim\] and \[fig:irdisim\] were found to be dominated by the stellar residuals using the chromaticity of the stellar residuals.]{}

![image](./figs/f3){width="11.5cm"}

Three point sources are detected in the IRDIS field (Fig. \[fig:irdisimfov\]). Their photometry and astrometry were measured [using the TLOCI algorithm]{} applied to each spectral band separately. We divided each science frame into annuli of 1.5 full width at half maximum. Then, for each 