Eccentricity and period distributions of all giant planets that ever formed, regardless of their survival. This plot includes all planets with masses from 95 M_⊕, not only cold Jupiters. Insets show the corresponding empirical distribution functions. Upper left: eccentricity distribution for giants orbiting low-metallicity ([Fe/H] < 0.2, yellow) and high-metallicity ([Fe/H] > 0.2, blue) host stars. Planets with very low eccentricity are slightly more prevalent in low-metallicity systems. Upper right: period distributions of giant planets for different metallicities. A population of giants with very short periods exists only in the high-metallicity sample (p = 8 × 10⁻²). Lower left: eccentricity distributions of giant planets in cold Jupiter-hosting systems with and without super-Earth companions. Giants in systems without super-Earths have significantly higher eccentricities (p = 5 × 10⁻⁴). No super-Earths occur when a giant with e ≳ 0.7 exists. Lower right: period distributions of giants with and without super-Earths. The latter persist only in systems without short-period giants.