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The orbital motion of non-contact double-lined spectroscopic binaries (SB2),with periods of a few tens of days to several years, holds unique accurateinformations on individual stellar masses, that only long-term monitoring canunlock. The combination of radial velocity measurements from high-resolutionspectrographs and astrometric measurements from high-precision interferometersallows the derivation of SB2 components masses down to the percent precision.Since 2010, we observed a large sample of SB2 with the SOPHIE spectrograph atthe Observatoire de Haute-Provence, aiming at the derivation of orbitalelements with sufficient accuracy to obtain masses of components with relativeerrors as low as 1$\%$ when the astrometric measurements of the Gaia satellitewill be taken into account. In this paper we present the results from six yearsof observations of 14 SB2 systems with periods ranging from 33 to 4185 days.Using the TODMOR algorithm we computed radial velocities from the spectra, andthen derived the orbital elements of these binary systems. The minimum massesof the 28 stellar components are then obtained with a sample average accuracyof 1.0$\pm$0.2$\,\%$. Combining the radial velocities with existinginterferometric measurements, we derived the masses of the primary andsecondary components of HIP 61100, HIP 95995 and HIP 101382 with relativeerrors for components (A,B) of respectively (2.0, 1.7)$\,\%$, (3.7, 3.7)$\,\%$,and (0.2, 0.1)$\,\%$. Using the Cesam2k stellar evolution code, we couldconstrain the initial He-abundance, age and metallicity for HIP 61100 and HIP95995.

Masses of the components of SB2 binaries observed with Gaia. IV. Accurate SB2 orbits for 14 binaries, and masses of 3 binaries