This is a list of extrasolar planets that have been directly observed, sorted by observed separations. This method works best for young planets that emit infrared light and are far from the glare of the star. Currently, this list includes both directly imaged planets and imaged planetary-mass companions (objects that orbit a star but formed through a binary-star-formation process, not a planet-formation process). This list does not include free-floating planetary-mass objects in star-forming regions or young associations, which are also referred to as rogue planets.
The data given for each planet is taken from the latest published paper on the planet to have that data. In many cases it is not possible to have an exact value, and an estimated range is instead provided. The lightest, coldest, and oldest planet directly imaged is Proxima Centauri c, which has seven times Earth's mass, an effective temperature of 39 K, and an age of about 4.8 Ga. This list includes the four members of the multi-planet system that orbit HR 8799.
Exoplanets have been discovered using several different methods for collecting or combining direct images to isolate planets from the background light of their star. Non-Redundant Aperture Masking Interferometry is a method of combining the views of multiple telescopes into a single image, while the other methods are algorithms for combining multiple direct images taken from the same telescope.
Although listed in the table below, the identities of Candidate 1, FW Tau b, LkCa 15 b, LkCa 15 c, and HD 100546 b are disputed. They may not actually be true exoplanets. † There is no consensus whether these companions of stars should be considered sub-brown dwarfs or planets Check https://exoplanetarchive.ipac.caltech.edu/docs/imaging.html to see more directly imaged planets. It contains an updated table of all of them.
Star | Exoplanet | Image | Mass (MJ) | Radius (RJ) | Period (yr) | Observed separation (AU) | Eccentricity | Distance to Earth (ly) | Year of discovery | Imaging technique | Ref(s). |
---|---|---|---|---|---|---|---|---|---|---|---|
WISE J0336-0143 | WISE J0336-0143 B† | 4-12.5 | 5-9 | 0.97+0.05 −0.09 | 33 | 2023 | source substraction | [1] | |||
Alpha Centauri | Candidate 1 (?) | 0.11±0.05 | 0.459±0.17 | ~1 | 1.1 | 4.37 | 2021 | ||||
CFBDSIR J145829+101343 | CFBDSIR J145829+101343 b | 10.5±4.5 | 27.5±7.5 | 2.6±0.3 | 2011 | Direct imaging | |||||
HD 206893 | HD 206893 c | 12.7+1.2 −1.0 | 1.46+0.18 −0.06 | 5.7 | 3.53+0.08 −0.06 | 0.41±0.03 | 133 | 2023 | interferometry | [2] | |
HD 206893 B† | 28.0+2.2 −2.1 | 1.25±0.02 | 26 | 9.6+0.4 −0.3 | 0.14±0.05 | 2017 | ADI, PCA | [3] [2] | |||
WISE 1217+1626 | WISE 1217+1626 A b | 22±2 | 0.934±0.029 | 130-210 | 8.0±1.3 | 2012 | Direct imaging | [4] | |||
AF Leporis | AF Lep b | 2-5.5 | 20.6 | 8 | 0.47 | 87 | 2023 | Direct imaging | [5] [6] [7] | ||
Beta Pictoris | Beta Pictoris b | 12.7±0.3 | 1.5±0.2 | 22.47+3.77 −2.26 | 9 | 0.08+0.09 −0.05 | 63.4±0.1 | 2008 | RSDI | [8] [9] [10] [11] | |
51 Eridani | 51 Eridani b | 2.6 | 1.0 | ? | 13 | ? | 96 | 2014 | ADI, KLIP | [12] | |
WISE J1711+3500 | WISE J1711+3500 B | 8.7-22 | 280-430 | 15±2 | 62 | 2012 | laser AO | [4] | |||
HR 8799 | HR 8799 e | 7.0 | 1.3 | 49 | 14.5 | 0.14 | 128 | 2010 | ADI, LOCI | ||
HR 8799 d | 7.0 | 1.3 | 100 | 24.5 | 0.09 | 128 | 2008 | ADI, LOCI | |||
HR 8799 c | 7.0 | 1.3 | 189 | 37.4 | 0.24 | 128 | 2008 | ADI, LOCI | |||
HR 8799 b | 5.0 | 1.2 | 474 | 69.2 | 0.17 | 128 | 2008 | ADI, LOCI | |||
LkCa 15 | LkCa 15 b | 14.7±2.1 | 2015 | Direct imaging | |||||||
LkCa 15 c | 18.6±2.5 | 2015 | Direct imaging | ||||||||
2M J044144 | 2M J044144 b† | 5–10 | 15 | 456 | 2010 | Direct imaging | |||||
29 Cygni | HIP 99770 b | 13.9-16.1 | 1.05 | 51.0 | 16.9 | 0.25 | 130.9 | 2022 | ALOCI | [13] | |
HIP 21152 | HIP 21152 b | 24+6 −4 | 60.3 | 17+5 −4 | 0.36+0.37 −0.25 | 2022 | Direct imaging | ||||
HR 2562 | HR 2562 b | 30±15 | 1.11±0.11 | 20.3±0.3 | 2016 | Direct imaging | |||||
PDS 70 | PDS 70 b | ? | ? | 21 | 370 | 2018 | ADI, TLOCI | ||||
PDS 70 c | ? | ? | 35 | 370 | 2019 | SDI | |||||
HIP 81208 C | HIP 81208 Cb† | 14.8±0.4 | ~285 | 23 | 485 | 2023 | [14] | ||||
PZ Telescopii | PZ Telescopii b | 27+25 −9 | 120.5 | 27+14 −4 | 0.52+0.36 −0.32 | 2010 | Direct imaging, radial velocity | ||||
HD 169142 | HD 169142 b | 1-4 | 37.2 | 115 | 2019/2023 | pseudo-ADI, PDI, ASDI, ADI | [15] [16] | ||||
2M1207 | 2M1207b † | 4.2 | 1.5 | 1620 | 40.6 | 0.37 | 170 | 2004 | Direct imaging | ||
59 Virginis | Gliese 504 b† | 4+4.5 −1 | ? | ? | 43.5 | ? | 57.27 | 2013 | ADI, LOCI | ||
2MASS J01225093-2439505 | 2MASS J01225093-2439505 b | 24.5±2.5 | 1.0 | 52 | 2013 | Direct imaging | |||||
KR Muscae | HD 100546 b | 8.50±4.00 | 6.9+2.7 −2.9 | 53±2 | 2014 | Direct imaging | |||||
Kappa Andromedae | Kappa Andromedae b | 13+12 −2 | ? | 242–900 | 55 | 0.69–0.85 | 168.0 | 2013 | ADI, LOCI | ||
HD 95086 | HD 95086 b | 5.0 | ? | ? | 56 | ? | 295 | 2013 | ADI, LOCI | ||
2MASS J01033563-5515561(AB) | 2MASS J0103 AB b† | 12-14 | 84 | 154 | 2013 | AO | [17] | ||||
HIP 65426 | HIP 65426 b | 6-12 | 1.5 | 600 | 92 | 363 | 2017 | ADI, TLOCI | [18] [19] | ||
AB Aurigae | AB Aurigae b | 9-12 | 2.75 | ? | 93 | 0.19-0.60 | 508 | 2022 | ADI/RSDI, ALOCI | [20] | |
MWC 758 | MWC 758 c | 100 | 2023 | Direct imaging | |||||||
GQ Lupi | GQ Lupi b | 31±10 | 4.6±1.4 | 100 | 2004 | Direct imaging | |||||
VHS 1256-1257 | VHS 1256 b † | 11.2 | 3900 | 102 | 40 | 2015 | Direct imaging | ||||
YSES 2 | YSES 2 b | 6.3+1.6 −0.9 | 115 | 359 | 2021 | reference star image substraction | [21] | ||||
2MASS J04372171+2651014 | 2M0437 b | 3-5 | 118 | 418 | 2021 | AO | [22] | ||||
ROXs 42B | ROXs 42Bb | 9±3 | 2.5 | 1968.3 | 157 | Unknown | 440±16 | 2013 | Direct imaging | [23] | |
2MASS J02192210-3925225 | 2MASS J02192210-3925225 b | 13.9±1.1 | 1.44±0.03 | 160 | 2015 | Direct imaging | |||||
TYC 8998-760-1 | TYC 8998-760-1 b † | 14±3 | 160 | 309 | 2020 | imaging + coronagraph | [24] | ||||
TYC 8998-760-1 c | 6±1 | 320 | 2020 | [25] | |||||||
CFHTWIR-Oph 98 | CFHTWIR-Oph 98 b | 7.8+0.7 −0.8 | 1.86±0.05 | ~22000 | 200±6 | 2021 | Direct imaging | ||||
CHXR 73 | CHXR 73 b | 12.569+8.379 −5.237 | 210 | 2006 | Direct imaging | ||||||
ROXs 12 | ROXs 12 b | 16±4 | 214 | 0.83 | 2013 | Direct imaging | |||||
2MASS J22362452+4751425 | 2M2236+4751 b† | 11-14 | 230 | 205 | 2017 | AO | [26] | ||||
Mu2 Scorpii | Mu2 Scorpii b | 14.4±0.8 | 242.4 | 0.56 | 2022 | Direct imaging | |||||
Ophiuchi 11 | Ophiuchi 11 b | 21±3 | 20,000 | 243±55 | 2006 | Direct imaging | |||||
AB Pictoris | AB Pictoris b† | 10-14 | 260 | 164 | 2005 | imaging+ coronagraph | [27] [28] | ||||
GSC 6214-00210 | GSC 6214-00210 b† | 14 ± 2 | 320 | 355 | 2008 | [29] | |||||
FW Tauri | FW Tauri b† | 10±4 or star [30] | ? | ~12,000 [31] | 330 | ? | 472.93 [32] | 2013 | Direct imaging | [33] [34] | |
DH Tauri | DH Tauri b† | 11±3 | 2.7±0.8 | 330 | 441 | 2005/2014 | Coronagraph, AO | [35] [36] | |||
1RXS J1609 | 1RXS 1609 b† | 8–14 | 1.7 | 6518 | 331.1 | 0.08 | 470 | 2008/2010 | Direct imaging | ||
HIP 79098 AB | HIP 79098 AB b | 20.5±4.5 | 345±6 | 2019 | Direct imaging | ||||||
CT Chamaeleontis | CT Chamaeleontis b | 17±6 | 2.20+0.81 −0.60 | 440 | 2007 | Direct imaging | |||||
HD 203030 | HD 203030 B | 11+4 −3 | 487 | 128 | 2006 | SDI | [37] | ||||
b Centauri | b Centauri b | 10.9±1.6 | 556 | 330 | 2021 | coronagraph+ classical angular differential imaging | [38] | ||||
HD 106906 | HD 106906 b† | 11±2 | ? | ? | 650 | ? | 300 | 2013 | ADI | ||
USco CTIO 108 | USco CTIO 108 b | 14+2 −8 | 670 | 2008 | Direct imaging | ||||||
HIP 78530 | HIP 78530 b | 23±1 | 740±60 | 2010 | Direct imaging | ||||||
HN Pegasi | HN Pegasi b | 21.9987±9.42803 | 1.05066+0.136197 −0.0583702 | 773±13 | 2006 | Direct imaging | |||||
FU Tauri | FU Tauri b | 16 | 800 | 2008 | Direct imaging | ||||||
SR 12 | SR 12(AB) c† | 11 | 980 | 337 | 2011 | [39] | |||||
2MASS J05581644–4501559 | 0558 B | 6-12 | 1,043 | 88 | 2024 | Direct imaging | [40] | ||||
DT Virginis | Ross 458(AB) c† | 8.5 | 1.8 | 33,081 | 1,167.7 | 0.17 | 38 [41] | 2011 | Direct imaging | ||
BD+60 1417 | BD+60 1417b† | 15±5 | 1.31±0.06 | 1,662 | 144±13 | 2021 | Direct imaging | [42] | |||
SE 70 | S Ori 68 | 5 | 1,700 | 1,290 | 2006 | Direct imaging | [43] | ||||
2MASS J0249-0557AB | 2MASS J0249-0557c† | 11.6+1.3 −1.0 | 1,950 | 159 | 2018 | Direct imaging | [44] | ||||
GU Piscium | GU Piscium b† | 11±2 | 163,000 | 2,000 | 155 | 2014 | Direct imaging | ||||
LOri 167 | LOri 167B | 8+5 −1 | 2,000 | 1,300 | 2007 | Direct imaging | [45] | ||||
WD 0806-661 | WD 0806-661 B† | 7–9 | ? | ? | 2,500 | ? | 62 | 2011 | Direct imaging | ||
USco1621 A | USco1621 b | 16±2 | 2,880±20 | 2019 | Direct imaging | ||||||
USco1556 A | USco1556 b | 15±2 | 3,500±40 | 2019 | Direct imaging | ||||||
L 34-26 | COCONUTS-2b† | 6.3+1.5 −1.9 | 1.1±0.03 | ~1,100,000 | 6,471 | 35.51±0.01 | 2021/2011 | Direct imaging | [46] | ||
TYC 9486-927-1 | 2MASS J2126–8140 | 13.3±1.7 | ? | ~900,000 | 6,684 | ? | 80.72±13.86 | 2016/2006 | Direct imaging | [47] | |
GJ 900 | CW2335+0142 | 10.5 | 12,000 | 68 | 2024 | Direct imaging | [48] |
2M1207, 2M1207A or 2MASS J12073346–3932539 is a brown dwarf located in the constellation Centaurus; a companion object, 2M1207b, may be the first extrasolar planetary-mass companion to be directly imaged, and is the first discovered orbiting a brown dwarf.
AB Pictoris is a K-type main-sequence star, located 163.5 light-years away in the southern constellation of Pictor. It has been identified as a member of the young Tucana–Horologium association. The star has been classified as a BY Draconis variable, indicating it has an active chromosphere. It is an X-ray source and displays emission lines in its spectrum.
Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.
Gliese 176 is a small star with an orbiting exoplanet in the constellation of Taurus. With an apparent visual magnitude of 9.95, it is too faint to be visible to the naked eye. It is located at a distance of 30.9 light years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 26.4 km/s.
VHS J125601.92–125723.9 is a young triple brown dwarf system located in the constellation Corvus approximately 69.0 light-years from the Sun. The system consists of the equal-mass binary VHS J1256–1257AB and the distant planetary-mass companion VHS 1256–1257 b. In 2022, a continuous radio emission from the radiation belts surrounding VHS J1256–1257 was detected.
A circumplanetary disk is a torus, pancake or ring-shaped accumulation of matter composed of gas, dust, planetesimals, asteroids or collision fragments in orbit around a planet. They are reservoirs of material out of which moons may form. Such a disk can manifest itself in various ways.
HD 7449 is a binary star system about 126 light-years way. The primary star, HD 7449 A, is a main-sequence star belonging to the spectral class F9.5. It is younger than the Sun. The primary star is slightly depleted of heavy elements, having 80% of solar abundance.
HD 121056, or HIP 67851, is an aging giant star with a pair of orbiting exoplanets located in the southern constellation of Centaurus. This star is dimly visible to the naked eye with an apparent visual magnitude of 6.17. It is located at a distance of 209 light years from the Sun, based on parallax measurements, and is drifting further away with a radial velocity of 5.6 km/s.