Example template fits to literature data of stars with VELOCE RVs. Two parameters are fitted: the mean offset Δυ_γ and the phase offset Δϕ. The RV curve shapes and amplitudes are fixed by the VELOCE best fit models. From left to right: FN Aql observations by Barnes et al. (2005) closely fit to the VELOCE template; AX Cir observations by Lloyd Evans (1980) are sufficient to achieve a good template fit; BZ Cyg observations by Gorynya et al. (1992) show some scatter but the template fit is reliable thanks to dense phase sampling; even just seven VELOCE observations of R Mus allow for a precise template fit.