Combined Keplerian orbit model for the planets and Gaussian process (GP) stellar noise fit. The best-fit kernel priors were found using the Kepler photometry in Figure 1 before application to the radial velocities (RVs). (a) RV vs. time as observed by HIRES and HARPS-North (pre and post CCD upgrade) are plotted with 1σ uncertainties. The blue line represents the total model of the planets and the GP regressions, with the gray region showing 1σ uncertainties. (b) Residuals of the model subtracted from the RVs. (c) The phase-folded RVs for Kepler-102d with the best-fit semiamplitude model overplotted. The red points are phase-folded weighted-mean RVs and their uncertainties. (d) Same as (c) but for Kepler-102e.