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.