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Fig. 8


Peak cross-correlation of the time-averaged spectrum of each order with the PHOENIX template spectrum broadened to the rotation velocity of the star. In the four datasets shown, the peak cross-correlation strength averages between 0.85 and 0.90, indicating that the template retrieves the stellar spectrum at high efficiency, and therefore is an accurate model of the planet’s reflection spectrum. The cross-correlation is only performed at wavelengths between 450 nm to 650 nm, because the disappearance of the continuum at short wavelengths (hence a break-down of the continuum-normalization needed to perform this cross-correlation) and the presence of tellurics at longer wavelengths cause the correlation of the template with the stellar spectrum to be degraded.

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