mag/arcsec$^2$ was [performed]{} using the 2MASS stellar magnitudes [$J$=7.279, $H$=6.587, and $K$=5.843, @Cutri2003] and the ratio of the maximum to the total flux of the measured [unsaturated non-coronagraphic PSF]{}. With this normalization choice, [the profiles provide information on the scattering efficiency of the dust grains with the wavelength [see @Quanz2012]]{}. We did not include the error on the photometric calibration. The noise levels (horizontal dashed lines) were estimated at large separation from the star.

[We note]{} [the similar overall shapes of the profiles of]{} the spectral bands with bumps associated to the two spiral arms at the same locations. Since the spiral pattern is not centrosymmetric (the opening angle of S1 decreases abruptly by $\sim$15$^{\circ}$ at the location of [its bright blob feature]{}, cf. Figs. \[fig:ifsim\] and \[fig:irdisim\]), the locations of the bumps are not centrosymmetric. The S/N of the disk detection drops quickly exterior to the spiral arms. The IFS radial profiles also show a sharp increase [($\sim$2.5 mag)]{} from the $Y$ to the $H$ bands, which suggests an increasing efficiency of the scattering with the wavelength. An increasing trend (although less significant) was also seen in the polarized-light radial profiles from the $R$ to the $J$ bands presented 