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 .