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We carry out a new analysis of the published radial velocity data for theplanet-hosting star HD82943. We include the recent Keck/HIRES measurements aswell as the aged but much more numerous CORALIE data. We find that the CORALIEradial velocity measurements are polluted by a systematic annual variationwhich affected the robustness of many previous results. We show that afterpurging this variation, the residuals still contain a clear signature of anadditional $\sim 1100$ days periodicity. The latter variation leavessignificant hints in all three independent radial velocity subsets that weanalysed: the CORALIE data, the Keck data acquired prior to a hardware upgrade,and the Keck data taken after the upgrade.  We mainly treat this variation as a signature of a third planet in thesystem, although we cannot rule out other interpretations, such as long-termstellar activity. We find it easy to naturally obtain a stable three-planetradial-velocity fit close to the three-planet mean-motion resonance 1:2:5, withthe two main planets (those in the 1:2 resonance) in an aligned apsidalcorotation. The dynamical status of the third planet is still uncertain: it mayreside in as well as slightly out of the 5:2 resonance. We obtain the value of$\sim 1075$ days for its orbital period and of $\sim 0.3 M_{\rm Jup}$ for itsminimum mass, while the eccentric parameters are uncertain.

Possible solution to the riddle of HD 82943 multiplanet system: the three-planet resonance 1:2:5?