Understanding the relationship between long-period giant planets and multiple smaller short-period planets is critical for formulating a complete picture of planet formation .
This work characterizes three such systems .
We present Kepler-65 , a system with an eccentric ( e = 0.28 \pm 0.07 ) giant planet companion discovered via radial velocities ( RVs ) exterior to a compact , multiply-transiting system of sub-Neptune planets .
We also use precision RVs to improve mass and radius constraints on two other systems with similar architectures , Kepler-25 and Kepler-68 .
In Kepler-68 we propose a second exterior giant planet candidate .
Finally , we consider the implications of these systems for planet formation models , particularly that the moderate eccentricity in Kepler-65 ’ s exterior giant planet did not disrupt its inner system .