  Double-lined spectroscopic binaries (SB2s) are one of the main sources of
stellar masses, as additional observations are only needed to give the
inclinations of the orbital planes in order to obtain the individual masses of
the components. For this reason, we are observing a selection of SB2s using the
SOPHIE spectrograph at the Haute-Provence observatory in order to precisely
determine their orbital elements. Our objective is to finally obtain masses
with an accuracy of the order of one percent by combining our radial velocity
(RV) measurements and the astrometric measurements that will come from the Gaia
satellite. We present here the RVs and the re-determined orbits of 10 SB2s. In
order to verify the masses we will derive from Gaia, we obtained
interferometric measurements of the ESO VLTI for one of these SB2s. Adding the
interferometric or speckle measurements already published by us or by others
for 4 other stars, we finally obtain the masses of the components of 5 binary
stars, with masses ranging from 0.51 to 2.2 solar masses, including
main-sequence dwarfs and some more evolved stars whose location in the HR
diagram has been estimated.
