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CoRoT-9b is one of the rare long-period (P=95.3 days) transiting giantplanets with a measured mass known to date. We present a new analysis of theCoRoT-9 system based on five years of radial-velocity (RV) monitoring withHARPS and three new space-based transits observed with CoRoT and Spitzer.Combining our new data with already published measurements we redetermine theCoRoT-9 system parameters and find good agreement with the published values. Weuncover a higher significance for the small but non-zero eccentricity ofCoRoT-9b ($e=0.133^{+0.042}_{-0.037}$) and find no evidence for additionalplanets in the system. We use simulations of planet-planet scattering to showthat the eccentricity of CoRoT-9b may have been generated by an instability inwhich a $\sim 50~M_\oplus$ planet was ejected from the system. This scatteringwould not have produced a spin-orbit misalignment, so we predict that CoRoT-9borbit should lie within a few degrees of the initial plane of theprotoplanetary disk. As a consequence, any significant stellar obliquity wouldindicate that the disk was primordially tilted.

A deeper view of the CoRoT-9 planetary system. A small non-zero eccentricity for CoRoT-9b likely generated by planet-planet scattering