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Fig. 7


Upper panel: combined cross-correlation function of a spectral order of the second UVES night. For illustrative purposes, the planet’s spectrum was injected into these data at ϵ = 1 ×10−3 to show the slanted cross-correlation peak around − 80 km s−1 due to the changing radial velocity of the planet during the observations. The vertical structure at 0 km s−1 is caused by residual correlation with remnants of the stellar spectrum. Lower panel: same data but with the residual stellar structure at 0 km s−1 masked out. This will prevent it from contaminating non-zero radial-velocities when co-adding the individual cross-correlations at the rest-frame of the planet.

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