Extended Data Fig. 7: Measured properties of the planetary absorption signature as a function of time.
From: Nightside condensation of iron in an ultrahot giant exoplanet
Data from epoch 1 (orange), epoch 2 (green) and both epochs combined (binned by 2; black curve with 1σ uncertainty in dark grey) are shown. They result from Gaussian fits to the planetary absorption signal in the residual maps of Fig. 2b and Extended Data Figs. 5b and e. A factor of (Rp/R⁎)2/(1−ΔF/F(t)) was applied to the residual maps before the fit, where ΔF/F(t) is the model light curve used to extract the Doppler shadow. a, Radial velocity of the planetary signal (called the planet ‘shimmer’) in the planet rest frame. The light grey region shows the FWHM associated with each point. b, The FWHM of the signal. The weighted mean (horizontal dashed line) is 8.6 ± 0.7 km s−1. Horizontal dotted lines indicate the standard deviation of the values. c, Amplitude of the shimmer representing the differential transit depth. The weighted mean is 494 ± 27 ppm. The hatched area in all panels represents the overlap between the Doppler shadow and the planetary signal; data between −0.2 h and +0.7 h from mid-transit are excluded from the analysis. Error bars in all panels correspond to 1σ uncertainties.
