$G$ magnitude from [*Gaia*]{}. Together, the available photometry spans the full stellar SED over the wavelength range 0.35–22 $\mu$m (see Figure \[fig:sed\]).

We performed a fit using NextGen stellar atmosphere models [@Hauschildt1999], with the effective temperature ($T_{\rm eff}$) and surface gravity ($\log g$) constrained on the ranges reported in the TESS Input Catalog [@StassunTIC:2018], while the metallicity \[Fe/H\] was fixed to a typical M-dwarf metallicity of -0.5. We fixed the extinction ($A_V$) to be zero, considering proximity of the star, the degrees-of-freedom of the fit is 10. The resulting fit (Figure \[fig:sed\]) has a $\chi^2$ of 42.3 ($\chi^2_{red}$=4.2), with $T_{\rm eff} = 3800 \pm 70$ K. The relatively high $\chi^2$ is likely due to systematics, as the stellar atmosphere model is not perfect. We artificially increased the observational uncertainty estimates until $\chi^2_{red}=1$ was achieved. Integrating the (unreddened) model SED gives the bolometric flux at Earth of $F_{\rm bol} = 3.41 \pm 0.12 \times 10^{-9}$ erg s$^{-1}$ cm$^{-2}$. Taking the $F_{\rm bol}$ and $T_{\rm eff}$ together with the [*Gaia*]{} DR2 parallax, adjusted by $+0.08$ mas to account for the systematic offset reported by @StassunTorres:2018, gives the stellar radius as $R = 0.600 \pm 0.022$ R$_\odot$. Finally, estimating the stellar mass from 