  The effect of stellar multiplicity on the formation and evolution of
planetary systems is complex. At a demographic level, campaigns with both
high-resolution imaging and radial velocity observations indicate that planet
formation is strongly disrupted by close binaries, while being relatively
unaffected by wide companions. However, the magnitude and distance-limited
nature of those tools mean that large ranges of mass ratios and separations
remain largely unexplored. The Early Data Release 3 (EDR3) from the Gaia
Mission includes radial velocity measurements of over 6.5 million targets,
which we employ to explore the effect of binary companions within a statistical
framework called paired. These companions present as a source of excess radial
velocity noise in the Gaia catalog, when compared to the typical noise for
stars of similar spectral type and magnitude. Within this framework, we examine
the evidence for stellar multiplicity among the stars surveyed by NASA's Kepler
and TESS missions. We use radial velocity errors published in Gaia EDR3 to
estimate the probability of an unresolved stellar companion for a large subset
of the Kepler and TESS Input Catalog stars, where possible benchmarking our
inferred radial velocity semi-amplitudes against the those from ground-based
radial velocity surveys. We determine that we are typically sensitive out to
several AU and mass ratios $>0.1$, dependent upon the stellar magnitude. We aim
for paired to be a useful community tool for the exploration of the effects of
binarity on planets at a population level, and for efficient identification of
false-positive transit candidates.
