Top: Radial velocities without and with the correction for blaze variation, smoothed using a 30 day moving average to mitigate stellar activity signals due to the Sun’s rotation (in blue and orange, respectively). The red and purple dots corresponds to the best-fitted linear model of the Mg2 activity index to those two different time-series. Middle: Radial velocity residuals after subtracting the best Mg2 activity index linear model. The vertical lines highlight the change of the broken solar feed fibre, the change of the TH-AR HC lamp used for wavelength solution and the change of the detector cryostat (see legend). The green region highlights a period when the flux of the TH-AR HC lamp was larger than 2.5 times it nominal value (see Fig. 1). Bottom: Radial velocity residuals after subtracting a linear model including the Mg2 activity index, two offsets for the broken fibre and the cryostat change and a scaling factor for the AR1 to TH ratio.