expected for a signal originating from an orbiting planet.

In addition to the signal from L 168-9 b, the HARPS RVs exhibit some power close to [$P_{\text{rot}}$]{} and its second harmonic [$P_{\text{rot}}$]{}$/3$. Although the FAPs of these periodicities over the full frequency domain are large, they each appear locally as strong periodicities as most of the power in the HARPS RVs exists at $\lesssim 5$ days. The GLSP of the PFS RVs is much more difficult to interpret at periodicities in the vicinity of [$P_{\text{rot}}$]{} and its first and second harmonics due to strong aliases from the PFS WF. Due to these effects it is difficult to discern from the available PFS activity indices (i.e. S-index and $H\alpha$) whether or not a coherent activity signal is seen with PFS. Although each of the HARPS and PFS RV time series are significantly affected by sampling aliases, we do see evidence for L 168-9 b and rotationally modulated stellar activity in the RVs we endeavor to mitigate with our adopted model discussed in Sect. \[subsec:model\].

Radial velocity + transit model {#subsec:model}
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Guided by the periodicities in the HARPS and PFS RV time series, we proceeded to fit a model to the 