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|<ref name="Franson Bowler Zhou Pearce 2023 p. L19">{{cite journal | last1=Franson | first1=Kyle | last2=Bowler | first2=Brendan P. | last3=Zhou | first3=Yifan | last4=Pearce | first4=Tim D. | last5=Bardalez Gagliuffi | first5=Daniella C. | last6=Biddle | first6=Lauren I. | last7=Brandt | first7=Timothy D. | last8=Crepp | first8=Justin R. | last9=Dupuy | first9=Trent J. | last10=Faherty | first10=Jacqueline | last11=Jensen-Clem | first11=Rebecca | last12=Morgan | first12=Marvin | last13=Sanghi | first13=Aniket | last14=Theissen | first14=Christopher A. | last15=Tran | first15=Quang H. | last16=Wolf | first16=Trevor N. | title=Astrometric Accelerations as Dynamical Beacons: A Giant Planet Imaged inside the Debris Disk of the Young Star AF Lep | journal=The Astrophysical Journal Letters | publisher=American Astronomical Society | volume=950 | issue=2 | date=2023 | bibcode=2023ApJ...950L..19F | arxiv=2302.05420 | doi=10.3847/2041-8213/acd6f6 | s2cid=256808203 | page=L19 | doi-access=free }}</ref><ref>{{Cite journal |last1=Mesa |first1=D. |last2=Gratton |first2=R. |last3=Kervella |first3=P. |last4=Bonavita |first4=M. |last5=Desidera |first5=S. |last6=D'Orazi |first6=V. |last7=Marino |first7=S. |last8=Zurlo |first8=A. |last9=Rigliaco |first9=E. |date=2023-02-13 |title=AF Lep b: The lowest-mass planet detected by coupling astrometric and direct imaging data |journal=Astronomy & Astrophysics |volume=672 |pages=A93 |doi=10.1051/0004-6361/202345865 |arxiv=2302.06213 |bibcode=2023A&A...672A..93M }}</ref><ref>{{Cite journal |last1=De Rosa |first1=Robert J. |last2=Nielsen |first2=Eric L. |last3=Wahhaj |first3=Zahed |last4=Ruffio |first4=Jean-Baptise |last5=Kalas |first5=Paul G. |last6=Peck |first6=Anne E. |last7=Hirsch |first7=Lea A. |last8=Roberson |first8=William |date=2023-02-13 |title=Direct imaging discovery of a super-Jovian around the young Sun-like star AF Leporis |journal=Astronomy & Astrophysics |volume=672 |pages=A94 |doi=10.1051/0004-6361/202345877 |arxiv=2302.06332 |bibcode=2023A&A...672A..94D }}</ref>
|<ref name="Franson Bowler Zhou Pearce 2023 p. L19">{{cite journal | last1=Franson | first1=Kyle | last2=Bowler | first2=Brendan P. | last3=Zhou | first3=Yifan | last4=Pearce | first4=Tim D. | last5=Bardalez Gagliuffi | first5=Daniella C. | last6=Biddle | first6=Lauren I. | last7=Brandt | first7=Timothy D. | last8=Crepp | first8=Justin R. | last9=Dupuy | first9=Trent J. | last10=Faherty | first10=Jacqueline | last11=Jensen-Clem | first11=Rebecca | last12=Morgan | first12=Marvin | last13=Sanghi | first13=Aniket | last14=Theissen | first14=Christopher A. | last15=Tran | first15=Quang H. | last16=Wolf | first16=Trevor N. | title=Astrometric Accelerations as Dynamical Beacons: A Giant Planet Imaged inside the Debris Disk of the Young Star AF Lep | journal=The Astrophysical Journal Letters | publisher=American Astronomical Society | volume=950 | issue=2 | date=2023 | bibcode=2023ApJ...950L..19F | arxiv=2302.05420 | doi=10.3847/2041-8213/acd6f6 | s2cid=256808203 | page=L19 | doi-access=free }}</ref><ref>{{Cite journal |last1=Mesa |first1=D. |last2=Gratton |first2=R. |last3=Kervella |first3=P. |last4=Bonavita |first4=M. |last5=Desidera |first5=S. |last6=D'Orazi |first6=V. |last7=Marino |first7=S. |last8=Zurlo |first8=A. |last9=Rigliaco |first9=E. |date=2023-02-13 |title=AF Lep b: The lowest-mass planet detected by coupling astrometric and direct imaging data |journal=Astronomy & Astrophysics |volume=672 |pages=A93 |doi=10.1051/0004-6361/202345865 |arxiv=2302.06213 |bibcode=2023A&A...672A..93M }}</ref><ref>{{Cite journal |last1=De Rosa |first1=Robert J. |last2=Nielsen |first2=Eric L. |last3=Wahhaj |first3=Zahed |last4=Ruffio |first4=Jean-Baptise |last5=Kalas |first5=Paul G. |last6=Peck |first6=Anne E. |last7=Hirsch |first7=Lea A. |last8=Roberson |first8=William |date=2023-02-13 |title=Direct imaging discovery of a super-Jovian around the young Sun-like star AF Leporis |journal=Astronomy & Astrophysics |volume=672 |pages=A94 |doi=10.1051/0004-6361/202345877 |arxiv=2302.06332 |bibcode=2023A&A...672A..94D }}</ref>
|-
![[Epsilon Indi]]
|[[Epsilon Indi Ab]]
| style="background-color: black;" |[[File:Epsilon Indi Ab (MIRI Image).png|50x50px]]
|2-4
|
|29.93
|8.8
|0.48
|12
|2018 (RV), 2024 (images)
|coronographic images
|<ref>{{Cite web |last=information@eso.org |title=Webb images cold exoplanet 12 light-years away {{!}} ESA/Webb |url=https://esawebb.org/news/weic2421/ |access-date=2024-07-24 |website=esawebb.org |language=en}}</ref>
|-
|-
! scope="row" | [[Beta Pictoris]]
! scope="row" | [[Beta Pictoris]]

Revision as of 16:25, 24 July 2024

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 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.

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 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 [4]
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 [5]
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 [6][5]
WISE 1217+1626 WISE 1217+1626 A b 22±2 0.934±0.029 130-210 8.0±1.3 2012 Direct imaging [7]
AF Leporis AF Lep b 2-5.5 20.6 8 0.47 87 2023 Direct imaging [8][9][10]
Epsilon Indi Epsilon Indi Ab 2-4 29.93 8.8 0.48 12 2018 (RV), 2024 (images) coronographic images [11]
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 [12][13][14][15]
51 Eridani 51 Eridani b 2.6 1.0 ? 13 ? 96 2014 ADI, KLIP [16]
WISE 1711+3500 WISE 1711+3500 B 8.7-22 280-430 15±2 62 2012 laser AO [7]
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
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 [17]
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 [18]
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 [19][20]
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 [21]
HIP 65426 HIP 65426 b 6-12 1.5 600 92 363 2017 ADI, TLOCI [22][23]
AB Aurigae AB Aurigae b 9-12 2.75 ? 93 0.19-0.60 508 2022 ADI/RSDI, ALOCI [24]
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 [25]
2MASS J04372171+2651014 2M0437 b 3-5 118 418 2021 AO [26]
ROXs 42B ROXs 42Bb 9±3 2.5 1968.3 157 Un­known 440±16 2013 Direct imaging [27]
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 [28]
TYC 8998-760-1 c 6±1 320 2020 [29]
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 [30]
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 [31][32]
GSC 6214-00210 GSC 6214-00210 b† 14 ± 2 320 355 2008 [33]
FW Tauri FW Tauri b† 10±4

or star[34]

? ~12,000[35] 330 ? 472.93[36] 2013 Direct imaging [37][38]
DH Tauri DH Tauri b† 11±3 2.7±0.8 330 441 2005/2014 Coronagraph, AO [39][40]
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 [41]
b Centauri b Centauri b 10.9±1.6 556 330 2021 coronagraph+ classical angular differential imaging [42]
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 [2]
2MASS J05581644–4501559 0558 B 6-12 1,043 88 2024 Direct imaging [43]
DT Virginis Ross 458(AB) c† 8.5 1.8 33,081 1,167.7 0.17 38[44] 2011 Direct imaging
BD+60 1417 BD+60 1417b† 15±5 1.31±0.06 1,662 144±13 2021 Direct imaging [45]
SE 70 S Ori 68 5 1,700 1,290 2006 Direct imaging [46]
2MASS J0249-0557AB 2MASS J0249-0557c† 11.6+1.3
−1.0 		1,950 159 2018 Direct imaging [3]
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 [47]
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 [48]
TYC 9486-927-1 2MASS J2126–8140 13.3±1.7 ? ~900,000 6,684 ? 80.72±13.86 2016/2006 Direct imaging [49]
GJ 900 CW2335+0142 10.5 12,000 68 2024 Direct imaging [50]

See also

References

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