The observed scarcity of brown dwarfs in close orbits (within 10AU) around solar-type stars has posed significant questions about the origins of these substellar companions. These questions not only pertain to brown dwarfs but also impact our broader under- standing of planetary formation processes. However, to resolve these formation mechanisms, accurate observational constraints are essential. Notably, most of the brown dwarfs have been discovered by radial velocity surveys, but this method introduces uncertainties due to its inability to determine the orbital inclination, leaving the true mass-and thus their true nature-unresolved. This highlights the crucial role of astrometric data, helping us distinguish between genuine brown dwarfs and stars. This study aims to refine the mass estimates of massive companions to solar-type stars, mostly discovered through radial velocity measurements and subsequently validated using Gaia DR3 astrometry, to gain a clearer understanding of their true mass and occurrence rates. We selected a sample of 31 sources with substellar companion candidates validated by Gaia DR3 and with available radial velocities. Using the Gaia DR3 solutions as prior information, we performed an MCMC fit with the available radial velocity measurements to integrate these two sources of data and thus obtain an estimate of their true mass. Combining radial velocity measurements with Gaia DR3 data led to more precise mass estimations, leading us to reclassify several systems initially labeled as brown dwarfs as low-mass stars. Out of the 32 analyzed companions, 18 were confirmed as sub- stellar, 12 are determined to be stars, and 2 have inconclusive results with the current data. Importantly, using these updated masses, we reevaluated the occurrence rate of brown dwarf companions (13-80M_Jup_) on close orbits (<10AU) in the CORALIE sample, determining an upper limit of 0.08^+0.03^_-0.02^%.

Cone search capability for table J/A+A/680/A16/stars (List of studied stars)