Age vs. semi-major axis of directly imaged planets. We selected young companions with planetary masses (except for HD 206893 B), M ≲ 13 M_J, planet-to-star mass ratios of $q\lesssim \frac{1}{25}$, and orbits smaller than ≈100 au. The locations of the giant planets in the Solar System are indicated with vertically dashed lines, and the gray areas from left to right are separated by the approximate locations of the H₂O and CO₂ ice lines of an A0-type star (Öberg et al. 2011). The semi-major axes were retrieved from whereistheplanet when available (Wang et al. 2021a), and from Wang et al. (2021b), Hinkley et al. (2023), Currie et al. (2023), and De Rosa et al. (2023) otherwise. The ages were adopted from Pecaut et al. (2012), Bell et al. (2015), Macintosh et al. (2015), Chauvin et al. (2017), Müller et al. (2018), Garufi et al. (2018), Zuckerman (2019), Miret-Roig et al. (2020), Brandt et al. (2021), and Hinkley et al. (2023). Systematic uncertainties on the ages (e.g., due to uncertain cluster membership) are not reflected by the error bars.