GJ 4276 radial velocity curve

The RV variations of GJ 4276 are best explained by the presence of a planetary companion with a minimum mass of m_b_sini~16M_{sun}_ on a P_b_=13.35-day orbit. The analysis of the activity indicators and spectral diagnostics exclude stellar induced RV perturbations and prove the planetary interpretation of the RV signal.

We show that a circular single-planet solution can be excluded by means of a likelihood ratio test. Instead, we find that the RV variations can either be explained by an eccentric orbit or interpreted as a pair of planets on circular orbits near a period ratio of 2:1. Although the eccentric single-planet solution is slightly preferred, our statistical analysis indicates that none of these two scenarios can be rejected with high confidence using the RV time series obtained so far.