Fig. 3
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Posterior distribution for the orbital periods in the two-planet model from the analysis of the CCF RVs (top) and TM RVs (bottom). The posteriors are shown normalised by the ESS per histogram bin (so the maximum possible value in the abscissa is 1). The prior is log-uniform from 1 day to the time span of the data, which is marked with a dashed line.
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