  We aim to measure very precise and accurate model-independent masses and
distances of detached binary stars. Precise masses at the $< 1$% level are
necessary to test and calibrate stellar interior and evolution models, while
precise and independent orbital parallaxes are essential to check for the next
Gaia data releases. We combined RV measurements with interferometric
observations to determine orbital and physical parameters of ten double-lined
spectroscopic systems. We report new relative astrometry from VLTI/GRAVITY and,
for some systems, new VLT/UVES spectra to determine the radial velocities of
each component. We measured the distance of ten binary systems and the mass of
their components with a precision as high as 0.03% (average level 0.2%). They
are combined with other stellar parameters (effective temperatures, radii, flux
ratios, etc.) to fit stellar isochrones and determine their evolution stage and
age. We also compared our orbital parallaxes with Gaia and showed that half of
the stars are beyond $1\sigma$ with our orbital parallaxes; although, their
RUWE is below the frequently used cutoff of 1.4 for reliable Gaia astrometry.
By fitting the telluric features in the GRAVITY spectra, we also estimated the
accuracy of the wavelength calibration to be $\sim 0.02$% in high and medium
spectral resolution modes. We demonstrate that combining spectroscopic and
interferometric observations of binary stars provides extremely precise and
accurate dynamical masses and orbital parallaxes. As they are detached
binaries, they can be used as benchmark stars to calibrate stellar evolution
models and test the Gaia parallaxes.
