EBLM J0113+31 CHEOPS light curves

We have used near-infrared spectroscopy obtained with the SPIRou spectrograph to measure the semi-amplitude of the M dwarf's spectroscopic orbit, and high-precision photometry of the eclipse and transit from the CHEOPS and TESS space missions to measure the geometry of this binary system.

From the combined analysis of these data together with previously published observations, we obtain the following model-independent masses and radii: M_1_=1.029+/-0.025M_{sun}_, M_2_=0.197+/-0.003M_{sun}_, R_1_=1.417+/-0.014R_{sun}_, R_2_=0.215+/-0.002R_{sun}_. Using R_1_ and the parallax from Gaia EDR3 we find that this star's angular diameter is {theta}=0.0745+/-0.0007mas. The apparent bolometric flux of the G0V star corrected for both extinction and the contribution from the M dwarf (<0.2 per cent) is F_{Earth}_=(2.62+/-0.05)x10^-9^erg/cm^2^/s.