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We present results of a Bayesian analysis of radial velocity data for the star HIP 5158, confirming the presence of two companions and also constraining their orbital parameters. Assuming Keplerian orbits, the two‐companion model is found to be e 48  times more probable than the one‐planet model, although the orbital parameters of the second companion are only weakly constrained. The derived orbital periods are 345.6 ± 2.0 and 9017.8 ± 3180.7 d, respectively, and the corresponding eccentricities are 0.54 ± 0.04 and 0.14 ± 0.10. The limits on planetary mass ( m  sin  i ) and semimajor axis are (1.44 ± 0.14 M  J , 0.89 ± 0.01 au) and (15.04 ± 10.55 M  J , 7.70 ± 1.88 au), respectively. Owing to the large uncertainty on the mass of the second companion, we are unable to determine whether it is a planet or a brown dwarf. The remaining ‘noise’ (stellar jitter) unaccounted for by the model is 2.28 ± 0.31 m s −1 . We also analysed a three‐companion model, but found it to be e 8  times less probable than the two‐companion model.

Bayesian evidence for two companions orbiting HIP 5158