Fig. B.5
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Combined transit depth in ppm using the three HST/WFC3 G141 transit observations and corrected transit depth using stellar contamination models from Zhang et al. (2018) (purple), Wakeford et al. (2019) (blue), and Morris et al. (2018) (green). The latter (in green) and the raw extracted spectrum (in black) are almost similar because the stellar contribution of Morris et al. (2018) is flat in the HST/WFC3 NIR wavelength range.
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