the empirical relations of @Mann:2019 gives $M = 0.62 \pm 0.03 M_\odot$. With these values of the mass and radius, the stellar mean density is $\rho = 4.04 \pm 0.49$ g cm$^{-3}$. We also tested to fit the SED using BT-Settl theoretical grid of stellar model [@Allard2014], where we obtained a consistent result.

We searched for infrared (IR) excess in [*WISE*]{} data using the Virtual Observatory SED Analyser [VOSA, @Bayo:2008], which could point for the presence of debris disks. For that we computed the excess significance parameter [$\chi_\lambda$, @Beichman:2006; @Moor:2006], where $\chi_\lambda \ge 3$ represents a robust detection of IR excess. We obtained $\chi_\lambda = 0.70$ in the W$_3$ band, ruling out the presence of a debris disk around L 168-9.

Observations
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The first hint of a planetary companion orbiting L 168-9 came from analyzing TESS data. After the Data Validation Report was released to the community, a follow-up campaign started with several instruments and by different teams to check on whether the transit-like signal seen by TESS originated from a planet, as opposed to a stellar binary or other source. The follow-up observations included supplementary time series photometry aiming to detect additional transits, seeing-limited and high-resolution imaging to 