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Fig. C.1.

image

Left panel: wavelength solutions used for the 2010 data of α Cen B, for spectral order 38. As we can see, those wavelength solutions are not stable on the edges of order 38. Top right panel: RV measured on the 4999.51 Å Ti line that falls on pixel 3800 of order 38 (red vertical dashed line in the left panel). In green, we show the RVs as measured when using the wavelength solutions shown on the left panel. In red we show the RVs derived when using a unique wavelength solution. As we can see, the non-stability of the wavelength solutions on the right edge of spectral order 38 induces night-to-night RV offsets of ∼15 m s−1, which is mitigated when using a unique wavelength solution. Bottom right panel: correlation between the RV of the 4999.51 Å Ti line and the RV derived using all the spectral lines. As we can see, the correlation is significantly stronger when we use the RVs derived using a unique wavelength solution.

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