Radial velocities, best-fit model, and residuals for the HD 80869 system. This figure is structured and generated in the same way as Fig. B.1 (see the caption of that figure for more details). The main difference is that in this case we add, in the third row, the GLSP of the planetary model sampled at 10 000 times, evenly spread over the time span of our observations (modelHS). This allows us to visualize the harmonic content of this highly eccentric orbit and better understand the GLSP of our RV data.