Notes. Zero-points are stated as Δυ_ZP = υ_γ,ref − υ_γVELOCE. N_stars is the number of stars used to determine Δυ_ZP, N_clusters the number of epochs used for the reference, with some stars contributing multiple epochs. Most zero-point offsets are of order ±1 km s⁻¹ or less, and we recover the zero-point change between Coralie07 and Coralie14 to within ~5 m s⁻¹, cf. Table 2, despite this analysis being based on high-amplitude variable stars. The adopted uncertainty $e_{\mathrm{\Delta }{v}_{\mathrm{Z}\mathrm{P}}}$ is the standard median error unless only a single star was used to determine the zero-point, in which case a generous uncertainty of kms⁻¹ was adopted. The offset for Anderson et al. (2016a) applies only to the Hamilton spectrograph data set. Coralie observations by Pont et al. (1997) used an instrument version prior to Coralie07 and feature a significantly different zero-point than Coralie07 and Coralie14. For Gaia DR3 RVs, we state the result based on template fitting, see Sect. 5.4.1.