Notes. Case A: orbital solution setting circular orbits and 8b:4c:2d:1e mean motion resonance. Case B: orbital solution setting circular orbits and 4b:2c:1d and 5d:2e mean motion resonances. Case C: orbital solution setting circular orbits and 4b:2c:1d and 3d:2e mean motion resonances. For each planet, the notations refer to the orbital period, inclination, longitude of the ascending node, eccentricity, argument of periapsis, time of periapsis passage, and semimajor axis. The error bars on the orbital parameters are at 1σ (see text). We also indicate the reduced χ² for the nominal orbital solution for each planet, and the mass and distance ranges assumed for the host star for the orbital fitting (Baines et al. 2012; van Leeuwen 2007). The semimajor axes are derived using Kepler’s third law assuming the fitted orbital periods and that the planet masses are negligible with respect to the mass of the host star.