  In this paper, we determine the detectability of eclipsing binary star
companions from eclipse timing variations using the Kepler mission dataset.
Extensive and precise stellar time-series photometry from space-based missions
enable searches for binary star companions. However, due to the large datasets
and computational resources involved, these searches would benefit from
guidance from detection simulations. Our simulations start with and benefit
from the use of empirical Kepler mission data, into which we inject third
bodies to predict the resulting timing of binary star eclipses. We find that
the orbital eccentricity of the third body and the orbital period of the host
binary star are the key factors in detecting companions. Target brightness is
also likely to be a factor in detecting companions. Detectable third body
masses and periods can be efficiently bound using just two equations. Our
results enable the setting of realistic expectations when planning searches for
eclipsing binary star planetary and brown dwarf companions. Our results also
suggest the brown dwarf desert is real rather than observational selection.
