  Brown-dwarfs are substellar objects with masses intermediate between planets
and stars within about 13-80Mjup. While isolated BDs are most likely produced
by gravitational collapse in molecular clouds down to masses of a few Mjup, a
non-negligible fraction of low-mass companions might be formed through the
planet formation channel in protoplanetary disks. The upper mass limit of
objects formed within disks is still observationally unknown, the main reason
being the strong dearth of BD companions at orbital periods shorter than 10
years, a.k.a. the BD desert. To address this question, we aim at determining
the best statistics of secondary companions within the 10-100Mjup range and
within 10 au from the primary star, while minimising observational bias. We
made an extensive use of the RV surveys of FGK stars below 60pc distance to the
Sun and in the northern hemisphere performed with the SOPHIE spectrograph at
the Observatoire de Haute-Provence. We derived the Keplerian solutions of the
RV variations of 54 sources. Public astrometric data of the Hipparcos and Gaia
missions allowed constraining the mass of the companion for most sources. We
introduce GASTON, a new method to derive inclination combining RVs Keplerian
and astrometric excess noise from Gaia DR1. We report the discovery of 12 new
BD candidates. For 5 of them, additional astrometric data led to revise their
mass in the M-dwarf regime. Among the 7 remaining objects, 4 are confirmed BD
companions, and 3 others are likely in this mass regime. We also report the
detection of 42 M-dwarfs within 90Mjup-0.52Msun. The resulting Msin(i)-P
distribution of BD candidates shows a clear drop in the detection rate below
80-day orbital period. Above that limit, the BD desert reveals rather wet, with
a uniform distribution of the Msin(i). We derive a minimum BD-detection
frequency around Solar-like stars of 2.0+/-0.5%.
