(WF), and the S-index, $H\alpha$, $H\beta$, $H\gamma$, and the sodium doublet NaD activity indicators. [@Astudillo-Defru2017b] details how these spectroscopic activity indicators were derived. Each GLSP is shown in Fig. \[fig:GLSP\] along with a false alarm probability (FAP) that was computed via bootstrapping with replacement using $10^4$ iterations and normalizing each periodogram by its standard deviation.

Each of the GLSPs of the HARPS and PFS RV time series is dominated by noise and aliases arising from the respective WF. For example, the HARPS WF contains a forest of peaks with comparable FAP from $\sim 8$ days and extending out towards long periodicities. Similarly the GLSP of the PFS WF reveals a series of broad peaks for periodicities $\gtrsim 1$ day. These features, particularly those from the PFS WF, have clear manifestations in the GLSPs of their respective RV and activity indicator time series, thereby complicating the robust identification of periodocities in the data. However, strong peaks at the orbital period of L 168-9 b ($\sim 1.4$ days) are discernible in both RV time series at FAP $\sim 0.4\%$ and $\sim 0.3\%$ with HARPS and PFS respectively. This periodicity is not apparent in any of the ancillary activity indicators time series as 