with a new large format CCD with $9\mu m$ pixels and switched to a narrower slit for its regular operation mode to boost the resolution from 80[,]{}000 to 130[,]{}000. The PFS spectra are reduced and analyzed with a custom IDL pipeline that is capable of delivering RVs with $<$1 m/s precision [@Butler:1996].

We followed up L 168-9 with PFS on the 6.5 m Magellan II Clay telescope at Las Campanas Observatory in Chile from October 13–26, and then on December 16 and 21 in 2018. Observations were conducted on 15 nights, with multiple exposures per night. There were a total of 76 exposures of 20 minutes each. We typically took 2–6 exposures per night over a range of timescales, to increase the total SNR per epoch and also to average out the stellar and instrumental jitter. Each exposure had a typical SNR of 28 per pixel near the peak of the blaze function, or 56 per resolution element. The radial velocity dispersion is 4.61 m/s and the median RV uncertainty per exposure is about 1.8 m/s. Five consecutive 20-minute iodine-free exposures were obtained to allow for the construction of a stellar spectral template in order to extract the RVs. These 