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We present evidence for a new two-planet system around the giant starHD202696 (= HIP105056, BD+26 4118). The discovery is based on public HIRESradial velocity measurements taken at Keck Observatory between July 2007 andSeptember 2014. We estimate a stellar mass of 1.91$^{+0.09}_{-0.14}M_\odot$ forHD202696, which is located close to the base of the red giant branch. Atwo-planet self-consistent dynamical modeling MCMC scheme of the radialvelocity data followed by a long-term stability test suggests planetary orbitalperiods of $P_{\rm b}$ = 517.8$_{-3.9}^{+8.9}$ days and $P_{\rm c}$ =946.6$_{-20.9}^{+20.7}$ days, eccentricities of $e_{\rm b}$ =0.011$_{-0.011}^{+0.078}$ and $e_{\rm c}$ = 0.028$_{-0.012}^{+0.065}$ , andminimum dynamical masses of $m_{\rm b}$ =2.00$_{-0.10}^{+0.22}$\,$M_{\mathrm{Jup}}$ and $m_{\rm c}$ =1.86$_{-0.23}^{+0.18}$,$M_{\mathrm{Jup}}$, respectively. Our stable MCMCsamples are consistent with orbital configurations predominantly in a meanperiod ratio of 11:6 and its close-by high order mean-motion commensurabilitieswith low eccentricities. For the majority of the stable configurations we findan aligned or anti-aligned apsidal libration (i.e.\ $\Delta\omega$ libratingaround 0$^\circ$ or 180$^\circ$), suggesting that the HD202696 system is likelydominated by secular perturbations near the high-order 11:6 mean-motionresonance. The HD202696 system is yet another Jovian mass pair around anintermediate mass star with a period ratio below the 2:1 mean motion resonance.Therefore, the HD202696 system is an important discovery, which may shed lighton the primordial disk-planet properties needed for giant planets to break thestrong 2:1 mean motion resonance and settle in more compact orbits.

Two Jovian planets around the giant star HD202696. A growing population of packed massive planetary pairs around massive stars?