Thanks to the high precision of Gaia observations, numerous stellar companions have been investigated over the past decade, particularly through astrometric techniques. Long-period companions have been detected and characterized through long-term radial velocity surveys. In this work, we re-analyze a small sample of targets using a combined approach that integrates radial velocity data with astrometry. By merging Hipparcos and Gaia astrometry, specifically through the proper motion anomaly method, with radial velocity measurements, we are able to tightly constrain orbital inclinations and accurately determine the true masses of long-period companions. Additionally, we compare our results with the sensitivity curve, a tool that identifies the range of companion masses capable of inducing astrometric signals as a function of orbital separation and stellar mass. This comparison serves as a validation of our results and as to gain new information about the planetary system. Our revised analysis reveals that some targets previously classified as brown dwarfs or low-mass stars have, in fact, a planetary nature.