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We investigate the origins of Kepler-419, a peculiar system hosting twonearly coplanar and highly eccentric gas giants with apsidal orientationslibrating around anti-alignment, and use this system to place constraints onthe properties of their birth protoplanetary disk. We follow the proposal byPetrovich, Wu, & Ali-Dib (2019) that these planets have been placed on theseorbits as a natural result of the precessional effects of a dissipating massivedisk and extend it by using direct N-body simulations and models for theevolution of the gas disks, including photoevaporation. Based on a parameterspace exploration, we find that in order to reproduce the system the initialdisk mass had to be at least 95 M_Jup and dissipate on a timescale of at least10^4 yr. This mass is consistent with the upper end of the observed disk massesdistribution, and the dissipation timescale is consistent with photoevaporationmodels. We study the properties of such disks using simplified 1D thin diskmodels and show that they are gravitationally stable, indicating that the twoplanets must have formed via core accretion and thus prone to disk migration.We hence finally investigate the sensitivity of this mechanism to the outerplanet's semi major axis, and find that the nearby 7:1, 8:1, and 9:1mean-motion resonances can completely quench this mechanism, while even higherorder resonances can also significantly affect the system. Assuming the twoplanets avoid these high order resonances and/or close encounters, the dynamicsseems to be rather insensitive to planet c semi major axis, and thus orbitalmigration driven by the disk.

Constraining protoplanetary disks with exoplanetary dynamics: Kepler-419 as an example