were bracketed with spectra of rapidly rotating B stars taken through the iodine cell, for reconstruction of the spectral line spread function and wavelength calibration for the template observations.

The PFS observations of L 168-9 presented here are part of the Magellan TESS Survey (MTS) that will follow up $\sim$30 super-Earths and sub-Neptunes discovered by TESS in the next three years using PFS (Teske et al. in prep.). The goal of MTS is to conduct a statistically robust survey to understand the formation and evolution of super-Earths and sub-Neptunes. The observation schedules of all MTS targets, including L 168-9, can be found on the ExoFOP-TESS website.[^10]

Analysis {#sec:analysis}
========

![image](figures/WASP_gpv2.png)

Photometric rotation period {#subsec:rotation}
---------------------------

![*Left column*: Generalized Lomb-Scargle periodograms of the HARPS and PFS RV time series, window functions, and the S-index, $H\alpha$, $H\beta$, $H\gamma$, and sodium doublet activity indicators. The vertical dotted lines highlight the locations of the L 168-9 b orbital period, the stellar rotation period, and its first two harmonics. *Right column*: the false alarm probabilities computed from bootstrapping with replacement.[]{data-label="fig:GLSP"}](figures/periodogramsv2.png){width="0.98\hsize"}

Knowledge of the stellar rotation period helps to disentangle spurious RV signals arising from rotation and true RV signals due to orbital motion [e.g., @Queloz2001; 