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We establish the three-dimensional architecture of the Kepler-419 (previouslyKOI-1474) system to be eccentric yet with a low mutual inclination. Kepler-419bis a warm Jupiter at semi-major axis a = 0.370 +0.007/-0.006 AU with a largeeccentricity e=0.85 +0.08/-0.07 measured via the "photoeccentric effect." Itexhibits transit timing variations induced by the non-transiting Kepler-419c,which we uniquely constrain to be a moderately eccentric (e=0.184 +/- 0.002),hierarchically-separated (a=1.68 +/- 0.03 AU) giant planet (7.3 +/- 0.4 MJup).We combine sixteen quarters of Kepler photometry, radial-velocity (RV)measurements from the HIgh Resolution Echelle Spectrometer (HIRES) on Keck, andimproved stellar parameters that we derive from spectroscopy andasteroseismology. From the RVs, we measure the mass of inner planet to be2.5+/-0.3MJup and confirm its photometrically-measured eccentricity, refiningthe value to e=0.83+/-0.01. The RV acceleration is consistent with theproperties of the outer planet derived from TTVs. We find that, despite theirsizable eccentricities, the planets are coplanar to within 9 +8/-6 degrees, andtherefore the inner planet's large eccentricity and close-in orbit are unlikelyto be the result of Kozai migration. Moreover, even over many secular cycles,the inner planet's periapse is most likely never small enough for tidalcircularization. Finally, we present and measure a transit time and impactparameter from four simultaneous ground-based light curves from 1m-classtelescopes, demonstrating the feasibility of ground-based follow-up of Keplergiant planets exhibiting large TTVs.

Large eccentricity, low mutual inclination: the three-dimensional architecture of a hierarchical system of giant planets