Phase-folded radial velocities for planet b (top) and c (bottom). The points are colour-coded as in Fig. 2 (blue for SOPHIE and purple for HIRES). In the photodynamical model the contribution to RV signal coming from individual planets cannot be separated. Therefore, these figures are constructed by fitting a two-Keplerian model to the photodynamical MAP model radial velocities, and subtracting the individual contribution of each planet from the data. The uncertainties include the MAP jitter value.