Simulated scene of the PDS70 system, with the PDS70 star and the PDS70 b and c protoplanets. Top-left: Spectrum of the protoplanets. Bottom-left: Spectrum of the star. They are both degraded by the LSF of the instrument as well as multiplied by a telluric absorption spectrum modeling the effect of the Earth atmosphere. Right: Spectrally integrated image of all the monochromatic images. Stellar and planetary fluxes are spread by the FSF of the instrument resulting in the masking of the planets because of their very low contrast compared to the star. The random noise is negligible compared with the stellar nuisance.