# List of exoplanets discovered via astrometry

Astrometry has been used to discover a handful number of exoplanets, mostly gas giants more massive than Jupiter. It is based on measuring a star's proper motion, and seeing how that position changes over time: a planet with a sufficiently large mass is able to gravitationally pull its host star, making its proper motion vary over large timescales. This cause a proper motion discrepancy between two observations (e.g. Hipparcos and Gaia). This list contains discoveries using this method, it does not contain exoplanets first detected by another method, but later detected using astrometry, e.g. Epsilon Indi Ab or Gamma Cephei Ab.

## List

This list contain only confirmed planets. Many candidate planets were decected via astrometry, including Gliese 65 Ab (which would be the nearest planet detected by this method, if confirmed), 9,698 candidates shown in a paper as well as many more detected via Hipparcos-Gaia astrometry in another studies.
| Name | Mass | Semi-major axis (AU) | Orbital period (years) | Eccentricity | Inclination (°) | Discovery year | Distance (ly) | Host star mass (M$_☉$) | Host star radius (R$_☉$) | Host star temperature (K) | Notes and references |
| EQ Pegasi Ab | 2.26±0.57 M$_J$ | 0.643±0.001 | 0.779±0.004 | 0.35±0.19 | 69.20±25.61 | 2022 | 20.428±0.004 | 0.436±0.001 | 0.409±0.016 | 3,491±35 | |
| Gaia-4 b | 11.80+0.73 −0.66 M$_J$ | | 1.565±0.004 | 0.338+0.026 −0.023 | 116.9+4.2 −4.4 | 2024 | 240.4 ± 0.3262 | 0.644+0.025 −0.023 | 0.624+0.014 −0.015 | 4,034±77 | |
| HD 11506 d | 12.8+0.6 −0.5 M$_J$ | 18.20+0.06 −0.09 | 72.6+0.7 −0.8 | 0.29+0.02 −0.03 | 90+6 −5 | 2022 | 167.0±0.2 | 1.22±0.02 | 1.06±0.01 | 5,833±28 | |
| HD 28185 c | 5.68+0.44 −0.36 M$_J$ | 8.54+0.21 −0.14 | 25.27+0.91 −0.61 | 0.15±0.04 | 73+10.0 −8.4 or 109.5+9.1 −12.0 | 2022 | 128.0±0.1 | 0.974±0.018 | 1.048±0.015 | 5,602±36 | Initially discovered as a brown dwarf, revealed to be an exoplanet by later studies. Planetary parameters taken from Feng et al. 2024, stellar parameters from Venner et al. 2024. |
| HD 75898 c | 8.49+0.65 −0.63 M$_J$ | 7.39+0.04 −0.05 | 18.39+0.12 −0.11 | 0.08±0.01 | 153+2 −3 | 2024 | 254.6±0.7 | 1.295±0.015 | 1.58±0.11 | 6,122±52 | |
| HD 118203 c | 11.0+1.3 −1.0 M$_J$ | 6.20±0.20 | 13.9+0.66 −0.63 | 0.257±0.034 | 95+15 −19 | 2024 | 330.2±0.5 | 1.353±0.006 | 1.993±0.065 | 5,872±20 | |
| HD 128717 b | 12.8 M$_J$ | 2.18 | 3.0 | | | 2024 | 240 ± 0.55 | 1.17+0.06 −0.16 | 1.275 | 6,158±115 | |
| HD 176051 b | 1.5±0.3 or 2.26 M$_J$ | 1.76 or 2.02 | 2.78±0.11 | | 115.8±8.2 | 2010 | 48.4±0.261 | 0.71 (B) or 1.07 (A) | 0.81 (B) or 1.06 (A) | 6,000 (A) | Orbiting either HD 176051 A or HD 176051 B, but more likely orbiting the latter. |
| HD 222237 b | 5.19±0.58 M$_J$ | 10.8+1.1 −1.0 | 40.8+5.8 −4.5 | 0.56±0.03 | 49.9+3.4 −2.8 | 2024 | 37.3 | 0.76±0.09 | 0.71±0.06 | 4,751±139 | |
| HIP 11696 b | 4–16 M$_J$ | 2.5–28 | | | | 2024 | 160.9±0.2 | 1.299±0.102 | 1.438±0.109 | 6,428±215 | |
| HIP 47110 b | 3–10 M$_J$ | 3–30 | | | | 2024 | 126.2±0.1 | 0.891±0.070 | 0.873±0.060 | 5,507±184 | |
| TVLM 513–46546 b | 0.347–0.418 M$_J$ | 0.279–0.307 | 0.61±0.014 | ~0 | ~80 | 2020 | 35.01±0.05 | 0.06–0.08 | 0.097–0.109 | 2,247±55 | |