Extended Data Fig. 1: Reduction of the NIRCam eclipse observation of 55 Cnc e.

a, The relative eclipse depths derived by fitting to the relative light curves obtained by dividing the spectroscopic light curves by the white-light curve (WLC). The spectrum is consistent between the analyses and we adopt the SPARTA analysis for model interpretation. b, The SPARTA analysis in comparison with the eclipse depths derived by direct fitting to the spectroscopic light curves (minus respective while-light (WL) depth). Direct fitting results in considerably noisier spectra, whereas the overall shape is approximately consistent with the SPARTA analysis. c, Relative spectroscopic light curves in the SPARTA analysis. The vertical dashed lines denote the phases in which the planet is eclipsed by the star. d, Comparison between the scatters of the light curves and the uncertainties of binned data for the relative spectroscopic light curves from the SPARTA analysis. All error bars correspond to 1σ.