First row: left and middle: reduced SPHERE DPI Q_φ and U_φ images. Colour scale and stretch are the same for both images. North is up and east to the left. We have some residual signals in U_φ close to the centre of the image which can be explained by imperfect centring of the coronagraphic data or by multiple scattering in the inner disk. First row: right: Q_φ scaled with the square of the separation from the central star to account for the r² dependency of the scattered light flux (see Sect. 3.3). Second row: SPHERE ADI images of the system reduced with three different algorithms (simple ADI, PCA, and TLOCI). In all cases, the H2- and H3-band images were combined to increase the signal. Third and fourth row: left and middle: NACO H- and K_s-band Q_φ and U_φ images re-reduced by our team. Ring 2 and Gap 2 are clearly detected in K_s band. Third and fourth row: right: r²-scaled Q_φ NACO image analogous to the corresponding SPHERE image.