  The orbital motion of non-contact double-lined spectroscopic binaries (SB2),
with periods of a few tens of days to several years, holds unique accurate
informations on individual stellar masses, that only long-term monitoring can
unlock. The combination of radial velocity measurements from high-resolution
spectrographs and astrometric measurements from high-precision interferometers
allows the derivation of SB2 components masses down to the percent precision.
Since 2010, we observed a large sample of SB2 with the SOPHIE spectrograph at
the Observatoire de Haute-Provence, aiming at the derivation of orbital
elements with sufficient accuracy to obtain masses of components with relative
errors as low as 1$\%$ when the astrometric measurements of the Gaia satellite
will be taken into account. In this paper we present the results from six years
of observations of 14 SB2 systems with periods ranging from 33 to 4185 days.
Using the TODMOR algorithm we computed radial velocities from the spectra, and
then derived the orbital elements of these binary systems. The minimum masses
of the 28 stellar components are then obtained with a sample average accuracy
of 1.0$\pm$0.2$\,\%$. Combining the radial velocities with existing
interferometric measurements, we derived the masses of the primary and
secondary components of HIP 61100, HIP 95995 and HIP 101382 with relative
errors for components (A,B) of respectively (2.0, 1.7)$\,\%$, (3.7, 3.7)$\,\%$,
and (0.2, 0.1)$\,\%$. Using the Cesam2k stellar evolution code, we could
constrain the initial He-abundance, age and metallicity for HIP 61100 and HIP
95995.
