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Mass is one of the most important parameters for determining the true natureof an astronomical object. Yet, many published exoplanets lack a measurement oftheir true mass, in particular those detected thanks to radial velocity (RV)variations of their host star. For those, only the minimum mass, or $m\sin i$,is known, owing to the insensitivity of RVs to the inclination of the detectedorbit compared to the plane-of-the-sky. The mass that is given in database isgenerally that of an assumed edge-on system ($\sim$90$^\circ$), but many otherinclinations are possible, even extreme values closer to 0$^\circ$ (face-on).In such case, the mass of the published object could be strongly underestimatedby up to two orders of magnitude. In the present study, we use GASTON, a toolrecently developed in Kiefer et al. (2019) & Kiefer (2019) to take advantage ofthe voluminous Gaia astrometric database, in order to constrain the inclinationand true mass of several hundreds of published exoplanet candidates. We find 9exoplanet candidates in the stellar or brown dwarf (BD) domain, among which 6were never characterized. We show that 30 Ari B b, HD 141937 b, HD 148427 b, HD6718 b, HIP 65891 b, and HD 16760 b have masses larger than 13.5 M$_\text{J}$at 3-$\sigma$. We also confirm the planetary nature of 27 exoplanets amongwhich HD 10180 c, d and g. Studying the orbital periods, eccentricities andhost-star metallicities in the BD domain, we found distributions with respectto true masses consistent with other publications. The distribution of orbitalperiods shows of a void of BD detections below $\sim$100 days, whileeccentricity and metallicity distributions agree with a transition between BDssimilar to planets and BDs similar to stars about 40-50 M$_\text{J}$.

Determining the true mass of radial-velocity exoplanets with Gaia: 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets