The evolution of the planets’ semimajor axes (left panels) and eccentricities (right panels) for the corresponding best-fit (upper panels) and best-fit+1σ (lower panels) masses for 1 million orbits of the outer planet (L 98-59 d), and assuming initially circular orbits. The orbital elements do not experience drastic variations, and the system is dynamically stable for the duration of the integrations.