List of directly imaged exoplanets

Motion interpolation of seven images of the HR 8799 system taken from the W. M. Keck Observatory over seven years, featuring four exoplanets

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 coldest and oldest planet directly imaged are Epsilon Indi Ab and 14 Herculis c, which have six times Jupiter's mass, an effective temperature of 275 K, an age of about 3.5 Ga and eight times Jupiter's mass, an effective temperature of 275 K, an age of about 4.6 Ga, respectively. This list includes the four members of the multi-planet system that orbit HR 8799.

It is unlikely or at least unclear if objects on a wide orbit (≥100 AU) formed in circumstellar disks and these objects are therefore more often referred as planetary-mass companions.[1][2][3] Only in rare cases, such as for HD 106906 b, the formation of the object in the disk is seen plausible.

Key

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.

  • ADI = Angular Differential Imaging
  • KLIP = Karhunen–Loève Image Processing
  • LOCI = Locally Optimized Combination of Images
  • NRM = Non-Redundant Aperture Masking Interferometry
  • RSDI = Reference Star Differential Imaging
  • SDI = Spectral Differential Imaging
  • TLOCI = Template Locally Optimized Combination of Images

Exoplanets

Although listed in the table below, the identities of Candidate 1, FW Tau b, 2MASS J044144 b, 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 Imaging confirmation Year of discovery Year of first image Imaging technique Ref(s).
WISE 0146+4234 WISE 0146+4234 B† 10 ±4 10 0.93+0.12
−0.16 		63 2015 AO
WISE J0336-0143 WISE J0336-0143 B† 4-12.5 5-9 0.97+0.05
−0.09 		33 2023 source subtraction [4]
Alpha Centauri A Alpha Centauri Ab (?) 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±0.3 104 ± 8 2011 2011 2010 Direct imaging [5][6]
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 [7]
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 [8][7]
WISE 1217+1626 WISE 1217+1626 A b 22 ± 2 0.934 ± 0.029 130-210 8.0 ± 1.3 30.4 ± 1.0 2012 2012 Direct imaging [9]
AF Leporis AF Lep b 2-5.5 20.6 8 0.47 87 2023 Direct imaging [10][11][12]
Beta Pictoris Beta Pictoris b 12.7±0.3 1.46±0.01 22.47+3.77
−2.26 		10.018+0.082
−0.076 		0.08+0.09
−0.05 		63.4±0.1 2010 2008 2003 RSDI [13][14][15][16][17][18][19]
LP 852-7 WD 1202–232 b 1-7 50 11.47 34 2024 PSF-subtraction [20]
51 Eridani 51 Eridani b 9.1+4.9
−3.3 		1.11+0.16
−0.14 		32+17
−9 		12+4
−2 		0.45+0.10
−0.15 		96.0 ± 1.0 2015 2015 2014 ADI, KLIP [21][22][23][24]
HR 8799 HR 8799 e 9.6+1.9
−1.8 		1.17+0.13
−0.11 		49 14.5 0.14 133.3 ± 0.2 2010 2010 2009 ADI, LOCI [25][26][27]
HR 8799 d 9.2 ± 0.1 1.2 ± 0.1 100 24.5 0.09 133.3 ± 0.2 2008 2008 2008 ADI, LOCI [28][29]
HR 8799 c 8.5 ± 0.4 1.2 ± 0.1 189 37.4 0.24 133.3 ± 0.2 2008 2008 2004/
2007 		ADI, LOCI [28][29]
HR 8799 b 6.0 ± 0.3 1.2 ± 0.1 474 69.2 0.17 133.3 ± 0.2 2008 2008 2004/
2007 		ADI, LOCI [28][29]
2M J044144 2M J044144 b† 9.8 ± 1.8 15 ± 0.6 400 ± 10 2010 2010 2008 Direct imaging [30][31]
WISE 1711+3500 WISE 1711+3500 B 8.1-26 280-430 15 ± 2 75 ± 3 2012 2012 laser AO [9]
29 Cygni HIP 99770 b 13.9-16.1 1.05 51.0 16.9 0.25 130.9 2022 ALOCI [32]
HIP 21152 HIP 21152 b 24+6
−4 		60.3 17+5
−4 		0.36+0.37
−0.25 		141 2022 Direct imaging [33]
14 Herculis 14 Herculis c 7.9+1.6
−1.2 		1.03 ± 0.01 143 ± 3 20.0+12.0
−4.9 		0.52+0.16
−0.12 		58.38 ± 0.03 2025 2006 (RV) 2024 coronagraph [34][35][36]
HR 2562 HR 2562 b 8-18.5 1.11±0.11 20.3±0.3 111 2016 Direct imaging [37]
PDS 70 PDS 70 b 6+6
−4 		1.96+0.20
−0.17 		123.5+9.8
−4.9 		20.7+1.4
−1.2 		0.16+0.12
−0.01 		366.6 ± 0.8 2018 2018 2012/
2016 		ADI, TLOCI [38][39][40]
PDS 70 c 9+9
−6 		1.98+0.39
−0.31 		191.5+15.8
−31.5 		33.9+1.7
−2.1 		0.042+0.027
−0.030 		366.6 ± 0.8 2019 2019 2016/
2018 		SDI [41][39][40]
HIP 81208 C HIP 81208 Cb† 14.8±0.4 ~285 23 485 2023 [42]
PZ Telescopii PZ Telescopii b 27+25
−9 		2.42+0.28
−0.34 		120.5 27+14
−4 		0.52+0.36
−0.32 		154.1 ± 0.2 2010 2010 2007/
2009 		Direct imaging, radial velocity [43][44][45][46]
Epsilon Indi A Epsilon Indi Ab 5.75-6.91 1.08[a] 180+32
−31 		28.4+10
−7.2 		0.40 12 2024 2018 (RV) coronagraphic images [47][48]
LAWD 83 WD 2105–82 b 1-2 243 34.62 52.7 2024 PSF-subtraction [20]
HD 169142 HD 169142 b 1-4 37.2 115 2023 2019 pseudo-ADI, PDI, ASDI, ADI [49][50]
59 Virginis Gliese 504 b† 1-17 1.08+0.04
−0.03 		43.5 57.4 ± 0.1 2013 2013 2011 ADI, LOCI [51][52]
2M1207 2M1207b † 5.5 ± 0.5 1.13 >2029 ≥49.8 ± 1.1 211 ± 2 2005 2004 2004 Direct imaging [53][54][55]
CE Antliae TWA 7b 0.3 550 52 111.2 ± 0.1 2025 2024 Direct imaging [56]
2MASS J01225093-2439505 2MASS J01225093-2439505 b 24.5±2.5 1.0 52 110 2013 Direct imaging
KR Muscae HD 100546 b 1.65-25 3.4 53 ± 2 353 ± 1 2013 2011 Direct imaging [57][58][59]
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
Delorme 1 (AB) Delorme 1 (AB) b† 12-14 84 154 2013 AO [60][61]
HIP 65426 HIP 65426 b 6-12 1.5 600 92 363 2017 ADI, TLOCI [62][63]
AB Aurigae AB Aurigae b 9-20 <2.75 93 0.19-0.60 509 ± 3 2022 2022 2007/
2016 		ADI/RSDI, ALOCI [64][65]
MWC 758 MWC 758 c 100 508 2023 Direct imaging
VHS 1256-1257 VHS 1256 b † 11.2 3900 102 40 2015 Direct imaging
GQ Lupi GQ Lupi b 1–36 3.7 114 ± 33 495 ± 4 2005 2004 1994/
1999 		Direct imaging [66][67][68]
YSES 2 YSES 2 b 6.3+1.6
−0.9 		115 359 2021 reference star image subtraction [69]
2MASS J04372171+2651014 2M0437 b 3-5 118 418 2021 AO [70]
ROXs 42B ROXs 42Bb 10+8
−4 		2.10 ± 0.35 1968 157 440 ± 16 2013 2005 2005/
2011 		Speckle Imaging & Direct imaging [71][72][73][74]
2MASS J02192210-3925225 2MASS J02192210-3925225 b 13.9±1.1 1.44±0.03 160 131 2015 Direct imaging [75]
TYC 8998-760-1 TYC 8998-760-1 b † 14±3 160 309 2020 imaging + coronagraph [76]
TYC 8998-760-1 c 6±1 320 2020 [77]
NIRISS-NGC1333-10 NIRISS-NGC1333-10 B ~15 164 978 2024 direct imaging +slitless spectroscopy [78]
AB Pictoris AB Pictoris b† 10±1 1.57 - 1.8 190 163.5 ± 0.1 2005 2005 2003 Imaging+ coronagraph [79][80][81]
CFHTWIR-Oph 98 CFHTWIR-Oph 98 b 7.8+0.7
−0.8 		1.86±0.05 ~22000 200±6 447 2021 Direct imaging
CHXR 73 CHXR 73 b 12.6+8.4
−5.2 		210 620 ± 20 2006 2005 Direct imaging [82]
ROXs 12 ROXs 12 b 16±4 214 0.83 452 2013 Direct imaging
2MASS J22362452+4751425 2M2236+4751 b† 11-14 230 205 2017 AO [83]
Mu2 Scorpii Mu2 Scorpii b†l 14.4±0.8 242.4 0.56 474 2022 Direct imaging
Ophiuchi 11 Ophiuchi 11 b 21 ± 3 20000 243 ± 55 430 ± 20 2006 2006 2005 Direct imaging [84][85][86]
GSC 6214-00210 GSC 6214-00210 b† 17 ± 3 1.91 ± 0.07 320 355 2011 2008 2007 NRM [87][88][89][86][90]
FW Tauri FW Tauri b† 10±4

or star[91]

~12000[92] 330 ? 472.93[93] 2013 Direct imaging [94][95]
DH Tauri DH Tauri b† 11 ± 3 2.7 ± 0.8 330 441 ± 4 2005 2004 1999 Coronagraph, AO [96][97]
1RXS J1609 1RXS 1609 b† 14+2
−3 		1.7 6518 331.1 0.08 450 ± 1 2010 2008 2008 Direct imaging [98][99][86]
HIP 79098 AB HIP 79098 AB b 20.5±4.5 345±6 500 2019 Direct imaging
HD 203030 HD 203030 B 11+4
−3 		1.27+0.06
−0.04 		487 128.2 ± 0.3 2006 2006 2002 SDI [100][101]
CT Chamaeleontis CT Chamaeleontis b† 17±6 2.20+0.81
−0.60 		507 625 ± 3 2008 2007 2006 Direct imaging [102]
b Centauri b Centauri b 10.9±1.6 556 330 2021 coronagraph+ classical angular differential imaging [103]
HD 106906 HD 106906 b† 11±2 650 300 2013 ADI
USco CTIO 108 USco CTIO 108 b 16±2 670 473 ± 6 2007 2007 Direct imaging [104][86]
2MASS J23225240-6151114 2MASS J23225299-6151275 12.6-13.3[105] 705 138.4 2014 Direct imaging [106][107]
FU Tauri FU Tauri b 19 ± 4 3.2 ± 0.3 719 429 ± 8 2009 2008 2007 Direct imaging [108][109]
2M1006(ABC) 2M1006(ABC) b 3-5 730 ± 10 444 2025 2018 Direct imaging (candidate) [110]
HIP 78530 HIP 78530 b 28 ± 10 1.83+0.16
−0.14 		12000 740 ± 60 445.8+4.87
−4.77 		2011 2010 2000/
2008 		Direct imaging [111][112]
HN Pegasi HN Pegasi b 22 ± 9.4 1.05+0.14
−0.06 		795 ± 15.0 59.14 ± 0.04 2007 2006 2006 Direct imaging [113]
SR 12 SR 12(AB) c† 11 ± 3 2.38+0.27
−0.32 		980 370 ± 20 2011 2011 1998/
2002 		Direct imaging [114][90][2]
2MASS J05581644–4501559 0558 B 6-12 1043 88 2024 Direct imaging [115]
Ross 458 Ross 458(AB) c† 27 ± 4 1.45 ± 0.06 33081 1167.7 0.17 37.53 ± 0.05 2010 2010 ≥2005/
2009 		Direct imaging [116][117][118]
BD+60 1417 BD+60 1417b† 13.47±5.67 1.31±0.06 1662 144±13 2021 Direct imaging [119]
SE 70 S Ori 68 5 1700 ± 300 1290 2006 2001 Direct imaging [120]
UPM J1040-3551 CWISE J104053.42–355029.7 3 or 31 1700 82.5 2024 Direct imaging [121][122]
2MASS J0249-0557AB 2MASS J0249-0557c† 11.6+1.3
−1.0 		1950 159 2018 Direct imaging [3]
GU Piscium GU Piscium b† 11±2 163000 2000 155 2014 Direct imaging
LOri 167 LOri 167B 8+5
−1 		2000 1300 2007 1999 Direct imaging [123]
GSC 00568-01752 SDSS J2249+0044AB 12.5±0.2 (for single object) 2264 146.7 2024 2010 Direct imaging [124][125][105]
WD 0806-661 WD 0806-661 B† 7–9 1.17 ± 0.07 2500 62.73 ± 0.02 2011 2011 2004 Direct imaging [126][127][128]
USco1621 A USco1621 b 16±2 2880 ±20 452 2019 Direct imaging [129]
USco1556 A USco1556 b 15±2 3500 ±40 461 2019 Direct imaging [129]
L 34-26 COCONUTS-2b† 6.3+1.5
−1.9 		1.1±0.03 ~1100000 6471 35.51±0.01 2021 2011 Direct imaging [130]
TYC 9486-927-1 2MASS J2126–8140 13.3±1.7 ~900000 6684 ? 80.72±13.86 2016 Direct imaging [131]
GJ 900 CW2335+0142 10.5 12000 68 2024 Direct imaging [121]
BD+29 5007 2MASS J2351+3010 11.9+0.40
−0.20 		22106 77.12 2024 2016 2015 Direct imaging [132][133][125][105]

See also

Notes

  1. ^ Calculated, using the Stefan-Boltzmann law and the planet's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K:

References

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