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
[edit]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[1] as well as many more detected via Hipparcos-Gaia astrometry in another studies.[2][3]
| 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 MJ | 0.643±0.001 | 0.779±0.004 | 0.35±0.19 | 69.20±25.61 | 2022 | 20.428±0.004[4] | 0.436±0.001 | 0.409±0.016[5] | 3,491±35[5] | [6] |
| Gaia-4 b | 11.80+0.73 −0.66 MJ |
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 | [7] | |
| HD 11506 d | 12.8+0.6 −0.5 MJ |
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[8] | 1.22±0.02 | 1.06±0.01[9] | 5,833±28[9] | [10] |
| HD 28185 c | 5.68+0.44 −0.36 MJ |
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.[11][12] Planetary parameters taken from Feng et al. 2024,[12] stellar parameters from Venner et al. 2024.[11] |
| HD 75898 c | 8.49+0.65 −0.63 MJ |
7.39+0.04 −0.05 |
18.39+0.12 −0.11 |
0.08±0.01 | 153+2 −3 |
2024 | 254.6±0.7[13] | 1.295±0.015 | 1.58±0.11[14] | 6,122±52 | [10] |
| HD 118203 c | 11.0+1.3 −1.0 MJ |
6.20±0.20 | 13.9+0.66 −0.63 |
0.257±0.034 | 95+15 −19 |
2024 | 330.2±0.5[15] | 1.353±0.006[16] | 1.993±0.065[16] | 5,872±20[16] | [17] |
| HD 128717 b | 12.8 MJ | 2.18 | 3.0 | 2024 | 240 ± 0.55 | 1.17+0.06 −0.16 |
1.275 | 6,158±115 | [18] | ||
| HD 176051 b | 1.5±0.3 or 2.26 MJ | 1.76 or 2.02 | 2.78±0.11 | 115.8±8.2 | 2010 | 48.4±0.261[19] | 0.71 (B) or 1.07 (A) | 0.81 (B) or 1.06 (A)[20] | 6,000 (A)[21] | Orbiting either HD 176051 A or HD 176051 B, but more likely orbiting the latter.[22][23] | |
| HD 222237 b | 5.19±0.58 MJ | 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 | [24] |
| HIP 11696 b | 4–16 MJ | 2.5–28 | 2024 | 160.9±0.2[25] | 1.299±0.102[26] | 1.438±0.109[26] | 6,428±215[26] | [27] | |||
| HIP 47110 b | 3–10 MJ | 3–30 | 2024 | 126.2±0.1[28] | 0.891±0.070[26] | 0.873±0.060[26] | 5,507±184[26] | [27] | |||
| TVLM 513–46546 b | 0.347–0.418 MJ | 0.279–0.307 | 0.61±0.014 | ~0 | ~80 | 2020 | 35.01±0.05[29] | 0.06–0.08[30] | 0.097–0.109[30] | 2,247±55[31] | [32] |
See also
[edit]- Methods of detecting exoplanets#Astrometry
- Lists of exoplanets
- Astrometric binary
- List of directly imaged exoplanets
- List of exoplanets detected by radial velocity
- List of exoplanets detected by microlensing
- List of transiting exoplanets
- List of exoplanets detected by timing
- List of exoplanets discovered in 2024
References
[edit]- ^ Kiefer, Flavien; Lagrange, Anne-Marie; Rubini, Pascal; Philipot, Florian (2024-09-27). "Searching for substellar companion candidates with Gaia. II. A catalog of 9,698 planet candidate solar-type hosts". arXiv:2409.16993 [astro-ph.EP].
- ^ Kervella, Pierre; et al. (March 2019). "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly". Astronomy & Astrophysics. 623: 23. arXiv:1811.08902. Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. S2CID 119491061. A72.
- ^ Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022-01-01). "Stellar and substellar companions from Gaia EDR3. Proper-motion anomaly and resolved common proper-motion pairs". Astronomy and Astrophysics. 657: A7. arXiv:2109.10912. Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. ISSN 0004-6361.
- ^ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Mann, Andrew W.; et al. (May 2015). "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius". The Astrophysical Journal. 804 (1): 38. arXiv:1501.01635. Bibcode:2015ApJ...804...64M. doi:10.1088/0004-637X/804/1/64. S2CID 19269312. 64.
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- ^ a b Venner, Alexander; An, Qier; et al. (October 2024). "HD 28185 Revisited: An outer planet, instead of a brown dwarf, on a saturn-like orbit". Monthly Notices of the Royal Astronomical Society. 535 (1): 90–106. arXiv:2410.14218. Bibcode:2024MNRAS.535...90V. doi:10.1093/mnras/stae2336.
- ^ a b Feng, Fabo; Xiao, Guang-Yao; Jones, Hugh R. A.; Jenkins, James S.; Pena, Pablo; Sun, Qinghui (2024-12-19). "Lessons learned from the detection of wide companions by radial velocity and astrometry". arXiv:2412.14542 [astro-ph.EP].
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- ^ Ment, Kristo; et al. (October 2018). "Radial Velocities from the N2K Project: Six New Cold Gas Giant Planets Orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810". The Astronomical Journal. 156 (5). 213. arXiv:1809.01228. Bibcode:2018AJ....156..213M. doi:10.3847/1538-3881/aae1f5. S2CID 119243619.
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