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The origin of warm Jupiters (gas giant planets with periods between 10 and200 days) is an open question in exoplanet formation and evolution. Weinvestigate a particular migration theory in which a warm Jupiter is coupled toa perturbing companion planet that excites secular eccentricity oscillations inthe warm Jupiter, leading to periodic close stellar passages that can tidallyshrink and circularize its orbit. If such companions exist in warm Jupitersystems, they are likely to be massive and close-in, making them potentiallydetectable. We generate a set of warm Jupiter-perturber populations capable ofengaging in high-eccentricity tidal migration and calculate the detectabilityof the perturbers through a variety of observational metrics. We show that asmall percentage of these perturbers should be detectable in the Kepler lightcurves, but most should be detectable with precise radial velocity measurementsover a 3-month baseline and Gaia astrometry. We find these results to be robustto the assumptions made for the perturber parameter distributions. If ahigh-precision radial velocity search for companions to warm Jupiters does notfind evidence of a significant number of massive companions over a 3-monthbaseline, it will suggest that perturber-coupled high-eccentricity migration isnot the predominant delivery method for warm Jupiters.

Observable Predictions from Perturber-coupled High-eccentricity Tidal Migration of Warm Jupiters