  Much of the exoplanet discovery efforts over the next several years are
largely tasked with finding candidates for the upcoming Ariel mission. This is
a role that TESS is well-suited for. Radial velocity follow-up is needed to
confirm the planetary nature of these systems, as many of its planet candidates
turn out to be eclipsing binary systems with small stellar secondaries. Focused
Doppler follow-up to obtain these radial velocities is expensive. The Gaia
mission's radial velocity measurements on its target stars are not adequately
precise for a general search for orbiting planetary companions. While the RV
data has yielded thousands of spectroscopic binary systems, only an extreme
minority of these reach into the planetary-mass regime. Nonetheless, they do
detect eclipsing binary systems that can masquerade as transiting hot Jupiters.
In this work, we compare the Gaia DR3 Non-Single Stars catalogue to the current
planet candidate list from TESS and determine several of these candidate
planetary systems are actually eclipsing binaries. We find $\sim130$ eclipsing
binaries among the TOI and EPIC lists that do not appear to be in the
literature, including the previously statistically validated planet K2-256 b.
This work illustrates the usefulness of \textit{Gaia} to exoplanet validation
efforts and will help guide follow-up efforts for discovering new transiting
planets for the Ariel mission by avoiding misdirecting valuable telescope time.
