We test the high-eccentricity tidal migration scenario for Kepler-419b , a member of the eccentric warm Jupiter class of planets whose origin is debated .
Kepler-419 currently hosts two known planets ( b , c ) .
However , in its current configuration , planet c can not excite the eccentricity of planet b enough to undergo high-eccentricity tidal migration .
We investigate whether the presence of an undiscovered fourth body could explain the orbit of Kepler-419b .
We explore the parameter space of this potential third giant planet using a suite of N-body simulations with a range of initial conditions .
From the results of these simulations , coupled with observational constraints , we can rule out this mechanism for much of the parameter space of initial object d conditions .
However , for a small range of parameters ( masses between 0.5 and 7 m _ { Jup } , semi-major axes between 4 and 7.5 AU , eccentricities between 0.18 and 0.35 , and mutual inclinations near 0 ^ { \circ } ) an undiscovered object d could periodically excite the eccentricity of Kepler-419b without destabilizing the system over 1 Gyr while producing currently undetectable radial velocity and transit timing variation signals .