Extended Data Fig. 2: Reduction of the MIRI eclipse observation of 55 Cnc e.

a, Drift of the trace along the spectral (x) and spatial (y) directions during the observation, binned to 1-min intervals. b, Wavelength-dependent coefficients for linear decorrelation against the drift in the x and y directions, calculated with and without masking the in-eclipse data. c, Raw spectroscopic light curves and best-fit models, binned to 2-min intervals for easier visualization, after trimming the first 30 min of data. d, Systematics-corrected spectroscopic light curves and eclipse models, binned to 10-min intervals. e, Comparison between the Eureka! and SPARTA eclipse depth spectra. The spectrum is consistent between the analyses and the Eureka! analysis has smaller final uncertainties (owing to less scatter in binned light curves) and is thus adopted for model interpretation. All error bars correspond to 1σ.