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We present the discovery of Kepler-129 d ($P_{d}=7.2^{+0.4}_{-0.3}$ yr,$m\sin i_{d}=8.3^{+1.1}_{-0.7}\ \rm M_{Jup}$, $ e_{d}=0.15^{+0.07}_{-0.05} $)based on six years of radial velocity (RV) observations from Keck/HIRES.Kepler-129 also hosts two transiting sub-Neptunes: Kepler-129 b ($P_{b}=15.79$days, $r_{b}=2.40\pm{0.04}\ \rm{R_{\oplus}}$) and Kepler-129 c ($P_{c}=82.20$days, $r_{c}=2.52\pm{0.07}\ \rm{R_{\oplus}}$) for which we measure masses of$m_{b}<20\ \rm{M_{\oplus}}$ and $m_{c}=43^{+13}_{-12}\ \rm{M_{\oplus}}$.Kepler-129 is an hierarchical system consisting of two tightly-packed innerplanets and an external companion whose mass is close to the deuterium burninglimit. In such a system, two inner planets precess around the orbital normal ofthe outer companion, causing their inclinations to oscillate with time. Basedon an asteroseismic analysis of Kepler data, we find tentative evidence thatKepler-129 b and c are misaligned with stellar spin axis by $\gtrsim 38$ deg,which could be torqued by Kepler-129 d if it is inclined by $\gtrsim 19$ degrelative to inner planets. Using N-body simulations, we provide additionalconstraints on the mutual inclination between Kepler-129 d and inner planets byestimating the fraction of time during which two inner planets both transit.The probability that two planets both transit decreases as their misalignmentwith Kepler-129 d increases. We also find a more massive Kepler-129 c enablesthe two inner planets to become strongly coupled and more resistant toperturbations from Kepler-129 d. The unusually high mass of Kepler-129 cprovides a valuable benchmark for both planetary dynamics and interiorstructure, since the best-fit mass is consistent with this $\rm{2.5\R_{\oplus}}$ planet having a rocky surface.

Long Period Jovian Tilts the Orbits of Two sub-Neptunes Relative to Stellar Spin Axis in Kepler-129