Binary stars are essential astrophysical test-beds. As the components of binary systems are formed from the same material and at the same time, they share fundamental properties such as their age and initial composition. Among the different types of binary systems, eclipsing binaries give the most stringent constraints about the stars, such as the stellar mass and radius. In this project, spectroscopic observations from Las Cumbres Observatory (LCO) are combined with high-precision photometry from NASA TESS and ESA Gaia to obtain radial velocity and multi-wavelength light curves of a peculiar binary system. This is an eclipsing, double-lined binary system, which hosts an oscillating red giant star and a second visible companion. We construct a well-constrained binary model and determine precise dynamical masses for both components. The giant's oscillations, present in the TESS photometry, allow for a direct comparison between asteroseismic and dynamical estimates of the star's mass and radius. This binary, which is located on the southern PLATO field, represents a rare and valuable benchmark system for validating asteroseismic scaling relations and testing stellar evolution models in the red giant phase.