The top panel shows the radial velocity time series collected using Keck/HIRES between 2015 June 24 and October 03. The red line shows the best fit Keplerian, assuming a circular orbit. The blue dashed line shows the best fit Keplerian allowing for eccentricity to vary. While the eccentric solution has higher likelihood than the circular solution ﹩\mathrm{ln}{ \mathcal L }﹩ = −85.3 vs. −80.1, it comes at the expense of more free parameters. We adopt the circular solution as our system parameters. The bottom panels show the RVs folded on the ephemerides of planet b and c. In these plots, the contribution of the other planet as well as the contribution from the trend (parametrized by γ and ﹩{dv}/{dt}﹩) has been removed.