List of directly imaged 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.

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

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 is Epsilon Indi Ab, which has six times Jupiter's mass, an effective temperature of 275 K, and an age of about 3.5 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 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	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		30.4	2012	Direct imaging	[7]
AF Leporis	AF Lep b		2-5.5		20.6	8	0.47	87	2023	Direct imaging	[8][9][10]
Beta Pictoris	Beta Pictoris b		12.7±0.3	1.46±0.01[11]	22.47+3.77 −2.26	9	0.08+0.09 −0.05	63.4±0.1	2008	RSDI	[12][13][14][15]
LP 852-7	WD 1202–232 b		1-7		50	11.47		34	2024 (unconfirmed)	PSF-subtraction	[16]
51 Eridani	51 Eridani b		2.6	1.0	?	13	?	96	2014	ADI, KLIP	[17]
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	[18]
HIP 21152	HIP 21152 b		24+6 −4		60.3	17+5 −4	0.36+0.37 −0.25	141	2022	Direct imaging	[19]
HR 2562	HR 2562 b		8-18.5	1.11±0.11		20.3±0.3		111	2016	Direct imaging	[20]
PDS 70	PDS 70 b		3.2+3.3 −1.6	2.72+0.39 −0.34		21		370	2018	ADI, TLOCI
	PDS 70 c		7.5+4.7 −4.2	2.04+1.22 −0.89		35		370	2019	SDI
HIP 81208 C	HIP 81208 Cb†		14.8±0.4		~285	23		485	2023		[21]
PZ Telescopii	PZ Telescopii b		27+25 −9		120.5	27+14 −4	0.52+0.36 −0.32	154	2010	Direct imaging, radial velocity
Epsilon Indi A	Epsilon Indi Ab		5.75-6.91	1.08[a]	180+32 −31	28.4+10 −7.2	0.40	12	2018 (RV), 2024 (images)	coronagraphic images	[22][23]
LAWD 83	WD 2105–82 b		1-2		243	34.62		52.7	2024 (unconfirmed)	PSF-subtraction	[16]
HD 169142	HD 169142 b		1-4			37.2		115	2019/2023	pseudo-ADI, PDI, ASDI, ADI	[24][25]
2M1207	2M1207b †		4.2	1.11	1620	40.6	0.37	170	2004	Direct imaging
59 Virginis	Gliese 504 b†		4+4.5 −1	0.96		43.5		57.27	2013	ADI, LOCI
2MASS J01225093-2439505	2MASS J01225093-2439505 b		24.5±2.5	1.0		52		110	2013	Direct imaging
KR Muscae	HD 100546 b		8.50±4.00			53±2		353	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
Delorme 1 (AB)	Delorme 1 (AB) b†		12-14			84		154	2013	AO	[26][27]
HIP 65426	HIP 65426 b		6-12	1.5	600	92		363	2017	ADI, TLOCI	[28][29]
AB Aurigae	AB Aurigae b		9-12	2.75	?	93	0.19-0.60	508	2022	ADI/RSDI, ALOCI	[30]
MWC 758	MWC 758 c					100		508	2023	Direct imaging
GQ Lupi	GQ Lupi b		1–36	3		100		495	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 subtraction	[31]
2MASS J04372171+2651014	2M0437 b		3-5			118		418	2021	AO	[32]
ROXs 42B	ROXs 42Bb		9±3	2.83±0.01	1968.3	157	Un­known	440±16	2013	Direct imaging	[33]
2MASS J02192210-3925225	2MASS J02192210-3925225 b		13.9±1.1	1.44±0.03		160		131	2015	Direct imaging	[34]
TYC 8998-760-1	TYC 8998-760-1 b †		14±3			160		309	2020	imaging + coronagraph	[35]
	TYC 8998-760-1 c		6±1			320			2020		[36]
NIRISS-NGC1333-10	NIRISS-NGC1333-10 B		~15			164		978	2024	direct imaging +slitless spectroscopy	[37]
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		12.569+8.379 −5.237			210		620	2006	Direct imaging
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	[38]
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		20,000	243±55		400	2006	Direct imaging
AB Pictoris	AB Pictoris b†		10±1[39]	1.75		260		164	2005	imaging+ coronagraph	[40][41]
GSC 6214-00210	GSC 6214-00210 b†		14 ± 2			320		355	2008/2011		[42]
FW Tauri	FW Tauri b†		10±4 or star[43]		~12,000[44]	330	?	472.93[45]	2013	Direct imaging	[46][47]
DH Tauri	DH Tauri b†		11±3	2.7±0.8		330		441	2005/2014	Coronagraph, AO	[48][49]
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		500	2019	Direct imaging
CT Chamaeleontis	CT Chamaeleontis b†		17±6	2.20+0.81 −0.60		440		625	2007	Direct imaging
HD 203030	HD 203030 B		11+4 −3			487		128	2006	SDI	[50]
b Centauri	b Centauri b		10.9±1.6			556		330	2021	coronagraph+ classical angular differential imaging	[51]
HD 106906	HD 106906 b†		11±2			650		300	2013	ADI
USco CTIO 108	USco CTIO 108 b		14+2 −8			670		473	2008	Direct imaging
2MASS J23225240-6151114	2MASS J23225299-6151275		12.6-13.3[52]			705		138.4	2014	Direct imaging	[53][54]
HIP 78530	HIP 78530 b		23±1			740±60		446	2010	Direct imaging
HN Pegasi	HN Pegasi b		22±9.4	1.05+0.14 −0.06		773±13		59	2006	Direct imaging
FU Tauri	FU Tauri b		16			800		429	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	[55]
Ross 458	Ross 458(AB) c†		8.5	1.8	33,081	1,167.7	0.17	38[56]	2011	Direct imaging
BD+60 1417	BD+60 1417b†		13.47±5.67	1.31±0.06		1,662		144±13	2021	Direct imaging	[57]
SE 70	S Ori 68		5			1,700		1,290	2006	Direct imaging	[58]
UPM J1040-3551	CWISE J104053.42–355029.7		3 or 31			1,700		82.5	2024	Direct imaging	[59][60]
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	[61]
GSC 00568-01752	SDSS J2249+0044AB		12.5±0.2 (for single object)			2264		146.7	2010/2024	Direct imaging	[62][63][52]
WD 0806-661	WD 0806-661 B†		7–9			2,500		62	2011	Direct imaging
USco1621 A	USco1621 b		16±2			2,880±20		452	2019	Direct imaging	[64]
USco1556 A	USco1556 b		15±2			3,500±40		461	2019	Direct imaging	[64]
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	[65]
TYC 9486-927-1	2MASS J2126–8140		13.3±1.7		~900,000	6,684	?	80.72±13.86	2016/2006	Direct imaging	[66]
GJ 900	CW2335+0142		10.5			12,000		68	2024	Direct imaging	[59]
BD+29 5007	2MASS J2351+3010		11.9+0.40 −0.20			22,106		77.12	2015 (age+mass)/ 2016 (co-movement)/ 2024 (both)	Direct imaging	[67][68][63][52]

See also

• Lists of exoplanets
• List of largest exoplanets
• List of nearest exoplanets
• List of nearest terrestrial exoplanet candidates
• List of potentially habitable exoplanets
• List of stars with resolved images

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:$${\displaystyle {\sqrt {{\biggl (}{\frac {5,772}{275}}{\biggr )}^{4}\cdot 10^{-7.2}}}=0.1106\ R_{\odot }.}$$

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External links

• "Candidates detected by imaging". Extrasolar Planets Encyclopaedia. 1995. Retrieved 2 March 2011.
• "Exoplanets Data Explorer". Retrieved 2 March 2011.
• https://www.eso.org/public/images/potw1624a/ - Retrieved 2016-06-16