stars as potential sources of the TESS detection, so we can assume the planet orbits L 168-9. Given the limits placed on nearby companions by the Gemini-South data, if there were a close companion it would have to be fainter by $\sim 5$ magnitudes than the primary star, meaning the planet radius correction factor would be at most $$R_{p,corr} = R_{p}\times \sqrt{1 + 10^{-0.4\Delta m}} = R_{p}\times1.005.$$

This is smaller than the derived planet radius uncertainty (Table \[tab:results\]).

Radial velocity {#sec:rv}
---------------

### HARPS

The *High Accuracy Radial velocity Planet Searcher* [HARPS @Mayor2003] is an echelle spectrograph mounted on the 3.6m telescope at La Silla Observatory, Chile. The light is spread over two CCDs (pixel size 15 $\mu m$) by a science fiber and a calibration fiber. The calibration fiber can be illuminated with the calibration lamp for the best radial velocity precision, or it can be placed on sky for moderate precision. HARPS is stabilized in pressure and temperature, and has a resolving power of 115[,]{}000. The achievable precision in radial velocity of better than 1 $m/s$.

We began monitoring L 168-9 with HARPS on September 29, 2018, soon after the TESS alert. We elected not to use the 