  V1022 Cas has been known as a spectroscopic binary for a century. It was
found to be eclipsing based on photometry from the Hipparcos satellite, and an
astrometric orbit was recently obtained from near-infrared interferometry. We
present the first high-precision measurement of the radii of the stars based on
light curves obtained by the TESS satellite. Combined with published radial
velocities from high-resolution spectra, we measure the masses of the stars to
be 1.626 +/- 0.001 Msun and 1.609 +/- 0.001 Msun, and the radii to be 2.591 +/-
0.026 Rsun and 2.472 +/- 0.027 Rsun. The 12.16-d orbit is eccentric and the
stars rotate sub-synchronously, so the system is tidally unevolved. A good
match to these masses and radii, and published temperatures of the stars, is
found for several sets of theoretical stellar evolutionary models, for a solar
metallicity and an age of approximately 2 Gyr. Four separate distance
determinations to the system are available, and are in good agreement. The
distances are based on surface brightness calibrations, theoretical bolometric
corrections, the Gaia parallax, and the angular size of the astrometric orbit.
A detailed spectroscopic analysis of the system to measure chemical abundances
and more precise temperatures would be helpful.
