photometric signal with a period near 30 days is whether it was affected by moonlight. To check on this possibility, we searched for modulations in the WASP data of several stars of similar brightness within the surrounding 10 arcmin field, but did not find any 30-d signals similar to the one that was seen for L 168-9. In any case, the star location is far from the ecliptic, and moonlight contamination is not expected. Furthermore, the modulation was sometimes seen at the 15-d first harmonic, which would not be expected for moonlight. We can therefore be confident that the 30-d periodicity in the WASP data arises from L 168-9. The $R^\prime_{HK}$ from HARPS spectra supports the obtained photometric rotation period, as $log(R^\prime_{HK})=-4.562\pm0.043$ (active star) translates into [$P_{\text{rot}}$]{} $=22\pm 2$ days using the $R^\prime_{HK}$vs.[$P_{\text{rot}}$]{} relationship from [@Astudillo2017a].

![image](figures/TESS_phot_detrend_small.pdf)

Radial Velocity Periodogram Analysis {#subsec:kep}
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A first identification of significant periodicities in the HARPS and PFS RV time series is required in order to develop an accurate model of the observed RV variations. In a manner similar to our analysis of the WASP photometry, we computed the GLSP of the following HARPS and PFS spectroscopic time series: the RVs, the window functions 