  I describe the selection and initial characterisation of 20 eclipsing binary
stars that are suitable for calibration and testing of stellar models and data
analysis algorithms used by the PLATO mission and spectroscopic surveys. The
binary stars selected are F-/G-type dwarf stars with M-type dwarf companions
that contribute less than 2% of the flux at optical wavelengths. The light
curves typically show well-defined total eclipses with very little variability
between the eclipses. I have used near-infrared spectra obtained by the APOGEE
survey to measure the spectroscopic orbit for both stars in HD22064. Combined
with an analysis of the TESS light curve, I derive the following masses and
radii: $M_1 = 1.35 \pm 0.03 M_{\odot}$, $M_2 = 0.58 \pm 0.01 M_{\odot}$, $R_1 =
1.554 \pm 0.014 R_{\odot}$, $R_2 = 0.595 \pm 0.008 R_{\odot}$. Using $R_1$ and
the parallax from Gaia EDR3, I find that the primary star's angular diameter is
$\theta = 0.1035 \pm 0.0009 $ mas. The apparent bolometric flux of the primary
star is ${\mathcal F}_{\oplus,0} = (7.51\pm 0.09)\times10^{-9}$ erg cm$^{-2}$
s$^{-1}$. Hence, this F2V star has an effective temperature $T_{\rm eff,1} =
6763{\rm\,K} \pm 39{\rm \,K}$. HD22064 is an ideal benchmark star that can be
used for "end-to-end" tests of the stellar parameters measured by large-scale
spectroscopic surveys, or stellar parameters derived from asteroseismology with
PLATO. The techniques described here for HD22064 can be applied to the other
eclipsing binaries in the sample in order to create an all-sky network of such
benchmark stars.
