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Oscillating red-giant stars in binary systems are an ideal testbed forinvestigating the structure and evolution of stars in the advanced phases ofevolution. With 83 known red giants in binary systems, of which only ~40 havedetermined global seismic parameters and orbital parameters, the sample issmall compared to the numerous known oscillating stars. The detection ofred-giant binary systems is typically obtained from the signature of stellarbinarity in space photometry. The time base of such data biases the detectiontowards systems with shorter periods and orbits of insufficient size to allow ared giant to fully extend as it evolves up the red-giant branch. Consequently,the sample shows an excess of H-shell burning giants while containing very fewstars in the He-core burning phase. From the ninth catalogue of spectroscopicbinary orbits (SB9), we identified candidate systems hosting a red-giantprimary component. Searching space photometry from the NASA missions Kepler,K2, and TESS (Transiting Exoplanet Survey Satellite) as well as the BRITE(BRIght Target Explorer) constellation mission, we find 99 systems, which werepreviously unknown to host an oscillating giant component. The revised searchstrategy allowed us to extend the range of orbital periods of systems hostingoscillating giants up to 26000days. Such wide orbits allow a rich population ofHe-core burning primaries, which are required for a complete view of stellarevolution from binary studies. Tripling the size of the sample of knownoscillating red-giant stars in binary systems is an important step towards anensemble approach for seismology and tidal studies. While for non-eclipsingbinaries the inclination is unknown, such a seismically well-characterizedsample will be a treasure trove in combination with Gaia astrometric orbits forbinary~systems.

99 oscillating red-giant stars in binary systems with NASA TESS and NASA Kepler identified from the SB9-Catalogue