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tokens: after the observing sequence because of a slight saturation of the off-axis PSF obtained before the observation. An example of the output of this technique is shown in Fig 2 . Fig. 2 38th IFS spectral channel (1.63 m) with planets HR 8799 de obtained with KLIP reduction. A second approach, where ADI and SDI were used together, was then implemented. The single exposures in each of the 32 spectral datacubes were averaged. The PSF library used for the PCA fitting taking all frames into account, both along the temporal and spectral dimensions, where the PSF has moved by more than a separation criteria . In this scheme, the library is constructed using the frames spatially rescaled according to their respective wavelength. Various tests showed that a value of FWHM gives good results in terms of S/N for the detection of the planets. To account for the flux losses induced by the speckle subtraction algorithm, forward modeling is performed via the off-axis PSF of the above-mentioned star as a model for the PSF of the planet. The model is projected on the same PCA modes as the science data, and the flux loss is measured as the attenuation of the flux for the model before and after projection on the PCA modes. The fluxes of the planets are measured in the final spectral channels with aperture photometry in an aperture of diameter 0.8 (4 pixels). The flux is finally corrected for the flux loss estimated using the forward modeling. The error bars on the photometry were measured in the same way as for the IRDIS data described in Sect. 3.2 , except that we did not consider the flux variation during the exposure, as one of the two PSFs is slightly saturated. With this approach, we obtained eight spectral extractions from four independent pipelines. For each planet, a final estimate of the flux ratio between the star and planet was obtained by computing the median of the results. Astrometric measurements for planets HR 8799 de measured from the IFS are shown in Table 5 .The error budget is presented in Table 6 . The error bars are compatible with the expected ones for these targets, following the simulations of Zurlo et al. (2014) . Fig. 3 Contrastand off-axis PSFs curves for the IRDIFS_EXT data set. The 5 contrast for the two instruments are plotted as a function of the angular separation. The off-axis PSF of the star is represented as a black continuous line. Planets around HR 8799 are also shown as photometric points, the error bars are inside the dimension of the dots. The dotted vertical line indicates the coronagraph IWA. Fig. 4 Mass limits deduced from the contrast curves for the IRDIS and IFS instruments. An age of 30 Myr is assumed.Two different models are represented: the “hot-start models” BT-SETTL models, and the “warm-start models” from Spiegel Burrows (2012) . The separations where a possible planet f is expected to be (from Goździewski Migaszewski 2014 ) are shown as dashed black lines. The 5 contrast curves of IRDIS and IFS for the IRDIFS_EXT