@Cloutier2017b]. L 168-9 was photometrically monitored by WASP between May 2010 and December 2014 within five observing seasons each lasting approximately 200 days in duration. The photometric precision, observing cadence, and baselines within the WASP fields are sufficient to detect quasi-periodic (QP) photometric variations of L 168-9 due to active regions on the stellar surface rotating in and out of view at the stellar rotation period [$P_{\text{rot}}$]{}[.]{} The WASP photometry of L 168-9 is shown in Fig. \[fig:WASPphot\] along with the generalized Lomb-Scargle periodogram [GLSP; @Zechmeister2009] of the photometry in each of the five WASP observing seasons. It is clear from the GLSPs that a strong periodicity exists within the data whose timescale is often $\sim 30$ days except for within the second WASP season wherein the dominant periodicity appears at the first harmonic of [$P_{\text{rot}}$]{} $\sim 15$ days.

Given periodicities significantly detected in the WASP photometry, we proceeded to measure the photometric rotation period of L 168-9 [$P_{\text{rot}}$]{} with each WASP camera and in each WASP field[^11] in which L 168-9 was observed. As the photometric variations appear to vary nearly periodically, we modeled the photometry with a Gaussian process (GP) regression model and adopted a QP covariance kernel 