Top: best-fit model of our preliminary RV analysis over-plotted on the RV data of HD15337 after removing the instrumental offset due to the change of the fibres on June 1,2015. Second row: phase plot showing the RV signals of TOI-402.01 (left) and TOI-402.02 (right). The best-fit model is shown in black, and the orbital parameters and mass of the detected planets can be found in the title of the two subplots. Third row: RV residuals after fitting our best model. The rms of the residuals of 2.17 m s⁻¹ is significantly higher than the average photon noise error of 0.9 m s⁻¹. Bottom: GLS periodogram of the RV residuals showing no significant signals. Although no signal is seen, the fact that the rms of the residuals is much higher than the photon noise errors indicates that there is still significant activity signal in the residuals.