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We report 1212 radial-velocity (RV) measurements obtained in the years2009-2013 using an iodine cell for the spectroscopic binary nu Octantis(K1III/IV). This system (a_bin~2.6 au, P~1050 days) is conjectured to have aJovian planet with a semi-major axis half that of the binary host. The extremegeometry only permits long-term stability if the planet is in a retrogradeorbit. Whilst the reality of the planet (P~415 days) remains uncertain, otherscenarios (stellar variability or apsidal motion caused by a yet unobservedthird star) continue to appear substantially less credible based on CCFbisectors, line-depth ratios and many other independent details. If thisevidence is validated but the planet is disproved, the claims of other planetsusing RVs will be seriously challenged.  We also describe a significant revision to the previously published RVs andthe full set of 1437 RVs now encompasses nearly 13 years. The sensitive orbitaldynamics allow us to constrain the three-dimensional architecture with a broadprior probability distribution on the mutual inclination, which with posteriorsamples obtained from an N-body Markov chain Monte Carlo is found to be 158.4+/- 1.2 deg. None of these samples are dynamically stable beyond 1 Myr.However, a grid search around the best-fitting solution finds a region that hasmany models stable for 10 Myr, and includes one model within 1-sigma that isstable for at least 100 Myr. The planet's exceptional nature demands robustindependent verification and makes the theoretical understanding of itsformation a worthy challenge.

The conjectured S-type retrograde planet in nu Octantis: more evidence including four years of iodine-cell radial velocities