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EBLM J0113+31 is moderately bright (V=10.1), metal-poor ([Fe/H]$\approx-0.3$)G0V star with a much fainter M dwarf companion on a wide, eccentric orbit(=14.3 d). We have used near-infrared spectroscopy obtained with the SPIRouspectrograph to measure the semi-amplitude of the M dwarf's spectroscopicorbit, and high-precision photometry of the eclipse and transit from the CHEOPSand TESS space missions to measure the geometry of this binary system. From thecombined analysis of these data together with previously published observationswe obtain the following model-independent masses and radii: $M_1 = 1.029 \pm0.025 M_{\odot}$, $M_2 = 0.197 \pm 0.003 M_{\odot}$, $R_1 = 1.417 \pm 0.014R_{\odot}$, $R_2 = 0.215 \pm 0.002 R_{\odot}$. Using $R_1$ and the parallaxfrom Gaia EDR3 we find that this star's angular diameter is $\theta = 0.0745\pm 0.0007$ mas. The apparent bolometric flux of the G0V star corrected forboth extinction and the contribution from the M dwarf ($<0.2$ per cent) is${\mathcal F}_{\oplus,0} = (2.62\pm 0.05)\times10^{-9}$ erg.cm$^{-2}$.s$^{-1}$.Hence, this G0V star has an effective temperature $T_{\rm eff,1} = 6124{\rm\,K}\pm 40{\rm \,K\,(rnd.)} \pm 10 {\rm \,K\,(sys.)}$. EBLM J0113+31 is an idealbenchmark star that can be used for "end-to-end" tests of the stellarparameters measured by large-scale spectroscopic surveys, or stellar parametersderived from asteroseismology with PLATO. The techniques developed here can beapplied to many other eclipsing binaries in order to create a network of suchbenchmark stars.

monthly notices of the royal astronomical society

Fundamental effective temperature measurements for eclipsing binary  stars -- III. SPIRou near-infrared spectroscopy and CHEOPS photometry of the  benchmark G0V star EBLM J0113+31