Imaging {#sec:image}
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The relatively large 21pixels of TESS can lead to photometric contamination from nearby sources. These must be accounted for to rule out astrophysical false positives, such as background eclipsing binaries, and to correct the estimated planetary radius, initially derived from the diluted transit in a blended light curve [@ziegler18]. Without this correction, the interpreted planet radius can be underestimated [e.g., @ciardi2015; @Teske2018].

### SOAR {#subsubsec:soar}

![SOAR speckle results of L 168-9. Black points represent the I-band contrast obtained at a given separation of the star. The solid black line shows the $5 \sigma$ detection limit curve.[]{data-label="fig:soar"}](figures/TIC234994474I-cz20180925_2.pdf)

We searched for close companions to L 168-9 with speckle imaging on the 4.1-m Southern Astrophysical Research telescope [SOAR, @tokovinin18] installed in Cerro Pachón, Chile, on 2018 September 25 UT using the I-band ($\lambda_{cen}=824\ nm$, full width at half maximum$=170\ nm$) centered approximately on the TESS passband. Further details of the TESS SOAR survey are published in [@Ziegler2019].

Figure \[fig:soar\] shows the 5$\sigma$ detection sensitivity. No nearby stars ($\rho < 1 \farcs 6$) to L 168-9 were detected within the sensitivity limits of SOAR.

### Gemini-South {#subsubsec:gemini}

![DSSI/Gemini-S detection limit curves of L 168-9 in the 692 nm (top) and 880 