data has better sampling coverage in general for these targets. The MIKE velocities run from 2003 August 13$^{\rm{th}}$ until 2009 July 7$^{\rm{th}}$ (BJD 2452864.57934 - 2455019.6938), covering a baseline of six years that overlaps with the HARPS baseline but not the CORALIE data.

CORALIE
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The analysis of CORALIE data involves the normal echelle reduction steps, such as debiasing the images using CCD bias frames, order location and tracing using polynomial fitting methods and aperture order filtering, pixel-to-pixel sensitivity correction (flatfielding) by building a normalised master flatfield image and dividing out the master flatfield from the other images, scattered-light removal by measuring the contribution to the total light profile in the inter-order regions, order extraction using a profile fitting method ([@marsh89]), and finally building a precise 2D wavelength solution that is good to $\sim$2.5 overall precision ([@jordan14]; [@brahm16]). The final steps in the analysis include cross-correlating the individual spectra with a binary mask (either G2, K0, K5, or M2 depending on the spectral type of the star, see [@baranne96] and [@pepe02]) and fitting the cross-correlation function (CCF) with a gaussian to measure the radial velocity, along with the width of the CCF to generate realistic uncertainties. The instrumental drift is 