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Caption: Figure 2.
Orbital eccentricity (in e2) versus semimajor axis for the planet sample with eccentricities constrained to better than 40% for clarity (or if e < 0.1). Colors denote sub-Neptunes (1–4 R⊕, blue), sub-Saturns (4–8 R⊕, purple), and Jovians (8–16 R⊕, orange). Overlaid curves show theoretical formation channels from R. I. Dawson & J. A. Johnson (2018) for a fiducial planet of ∼6 R⊕ and ∼80 M⊕: high-eccentricity migration (red shaded region) and planet–planet scattering (gray dashed line, gray shaded region). The concentration of larger planets at high eccentricities and small semimajor axes is consistent with high-eccentricity migration.
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© 2026. The Author(s). Published by the American Astronomical Society.
