Fig. 4
Spectral energy distribution for 51 Eri b constructed from our YJ-, YH-IFS spectra and IRDIS photometry in H23, BB_H, and K12. Channels used as reference for classical SDI were removed as they are biased. In addition to the SPHERE data we plot the two GPI spectra in the J and H band, respectively. The flux in the J band is consistent between the two SPHERE spectra, but significantly different compared to GPI. Uncertainties are given as 1σ and are assumed to be Gaussian.
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