Radial velocity curves of {nu} Oct

We also describe a significant revision to the previously published RVs and the full set of 1437 RVs now encompasses nearly 13 yr. The sensitive orbital dynamics allow us to constrain the 3D architecture with a broad prior probability distribution on the mutual inclination, which with posterior samples obtained from an N-body Markov chain Monte Carlo is found to be 152.5^+0.7^_-0.6_{deg}. None of these samples are dynamically stable beyond 10^6^yr.

However, a grid search around the best-fitting solution finds a region that has many models stable for 10^7^yr, and includes one model within 1{sigma} that is stable for at least 10^8^yr. The planet's exceptional nature demands robust independent verification and makes the theoretical understanding of its formation a worthy challenge.